Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://www.mso.anu.edu.au/~bessell/FTP/Paper/ms_revised.ps Äàòà èçìåíåíèÿ: Tue Aug 15 10:49:10 2006 Äàòà èíäåêñèðîâàíèÿ: Tue Oct 2 07:41:51 2012 Êîäèðîâêà: IBM-866 Ïîèñêîâûå ñëîâà: sun halo

Bright MetalíPoor Stars from the Hamburg/ESO Survey.
I. Selection and Followíup Observations from 329 Fields
Anna Frebel 1 , Norbert Christlieb 2 , John E. Norris 1 , Timothy C. Beers 3 , Michael S. Bessell 1 ,
Jaehon Rhee 4 , Cora Fechner 2 , Brian Marsteller 3 , Silvia Rossi 5 , Christopher Thom 6 ,
Lutz Wisotzki 7 , and Dieter Reimers 2
ABSTRACT
We present a sample of 1777 bright (9 < B < 14) metalípoor candidates seí
lected from the Hamburg/ESO Survey (HES). Despite saturation e#ects present
in the red portion of the HES objectiveíprism spectra, the data were recoverable
and quantitative selection criteria could be applied to select the sample. Analí
yses of mediumíresolution (# 2 Ú A) followíup spectroscopy of the entire sample,
obtained with several 2 to 4 m class telescopes, yielded 145 new metalípoor stars
with metallicity [Fe/H] < -2.0, of which 79 have [Fe/H] < -2.5, and 17 have
[Fe/H] < -3.0. We also obtained C/Fe estimates for all these stars. From this,
we find a frequency of Cíenhanced ([C/Fe] > 1.0) metalípoor ([Fe/H] < -2.0)
giants of 9% ‘ 2%, which is lower than previously reported. However, the freí
quency raises to similar (> 20%) and higher values with increasing distance
from the Galactic plane. Although the numbers of stars at low metallicity are
falling rapidly at the lowest metallicities, there is evidence that the fraction of
1 Research School of Astronomy & Astrophysics, The Australian National University, Cotter Road, Weí
ston, ACT 2611, Australia; anna@mso.anu.edu.au, jen@mso.anu.edu.au, bessell@mso.anu.edu.au
2 Hamburger Sternwarte, UniversitØat Hamburg, Gojenbergsweg 112, Dí21029 Hamburg, Germany;
nchristlieb@hs.uniíhamburg.de, cfechner@hs.uniíhamburg.de, dreimers@hs.uniíhamburg.de
3 Department of Physics & Astronomy, CSCE: Center for Study of Cosmic Evolution, and JINA:
Joint Institute for Nuclear Astrophysics, Michigan State University, E. Lansing, MI 48824í1116, USA;
beers@pa.msu.edu, marsteller@pa.msu.edu
4 Center for Space Astrophysics, Yonsei University, Seoul 120í749, Korea, and Space Astrophysics Laboí
ratory, California Institute of Technology, MC 405í47, Pasadena, CA 91125, USA; rhee@caltech.edu
5 Departamento de Astronomia Instituto de Astronomia, GeofÒÐsica e CiÓencias AtmosfÒericas, Universidade
de SÔao Paulo, 05508í900 SÔao Paulo SP, Brazil; rossi@astro.iag.usp.br
6 Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Mail #31 PO Box
218, Hawthorn, Victoria 3122, Australia; cthom@astro.swin.edu.au
7 Astrophysikalisches Institut Potsdam, An der Sternwarte 16, Dí14482 Potsdam, Germany; lutz@aip.de

-- 2 --
carboníenhanced metalípoor stars is increasing rapidly as a function of declining
metallicity. For # 60 objects, highíresolution data have already been obtained;
one of these, HE 1327-2326, is the new record holder for the most ironídeficient
star known.
Subject headings: Galaxy: halo, stellar content, abundances --- Stars: Population
II, abundances, carbon --- Techniques: spectroscopic --- catalogs
1. Introduction
The first systematic searches for metalípoor stars in the Galactic halo, by means of
objectiveíprism surveys, began with Bond (1970, 1980, 1981) and Bidelman & MacConnell
(1973). More recent surveys are the HK survey (Beers et al. 1985, 1992; Beers 1999) and
the Hamburg/ESO survey (HES; Wisotzki et al. 2000; Christlieb 2003). Over time, deeper
surveys have became possible to reach further into the Galactic halo. The limiting magnitude
of the HES is B # 17.5 mag as opposed to the earlier HK survey (B # 15.5 mag).
Particularly the HK survey and HES have both shown that a variety of astrophysically
interesting and unusual objects can be found in a large sample of metalípoor stars. Some of
these exhibit large overabundances of heavy neutronícapture elements that are synthesized
in the síprocess (e.g., Aoki et al. 2001; Van Eck et al. 2001), or in the ríprocess (e.g.,
CS 22892-052, Sneden et al. 1996, or CS 31082í001 Cayrel et al. 2001). In the case of
strong ríprocess enhancement, nucleoíchronometry becomes possible based on the abundance
of e.g., Th and U. Bright metalípoor stars are particularly useful for this task since the weak
uranium line at 3859 Ú A is only detectable in very highíquality spectra. The availability of U,
together with Th, as the U/Th chronometer drastically reduces the theoretical uncertainties
on the derived ages, as compared to the more easily detectable Th/Eu ratio (Wanajo et al.
2002). Hence, a lower limit for the age of the Universe can be derived independently of other
measurements such as WMAP (Spergel et al. 2006). Many Cíenhanced metalípoor objects
(hereafter CEMP; [C/Fe] 1 > 1.0) were discovered as they occur with increased frequency
amongst metalípoor objects (e.g., Rossi et al. 1999). One of those is the very ironídeficient
giant HE 0107-5240 ([Fe/H] = -5.2) 2 that was found in a sample of # 2000 HES metalípoor
candidates (Christlieb et al. 2002). This star provided critical observational material to the
theories of the formation of the first objects in the Universe, as well as to the nucleosynthesis
1 We use the common notation of [A/B] = log(NA /NB ) # - log(NA /NA ) # , for elements A and B.
2 Employing the same Fe NLTe correction as used for HE 1327-2326

-- 3 --
processes involved in their production.
For elemental studies involving isotopes, such as 6 Li in metalípoor turno# stars, or very
weak and/or blended lines, such as uranium in some strongly ríprocess enhanced objects,
it is crucial to be able to obtain highíresolution (R > 40, 000) spectra with a very high
signalítoínoise ratio. Bright metalípoor stars are thus ideal targets. With the increased
lightícollecting power of current 8í10 m telescopes it is possible to achieve a S/N of 200 or
more for such objects within reasonable exposure times.
Apart from the faint stars, the HES also contains large numbers of bright (B < 14)
stars. However, those have previously not been investigated. The main technical reason is the
partial saturatation of the photographic plates, resulting in partially satured spectra. Despite
an increased interest to search for more fainter metalípoor stars in the extended survey
volume of the HES, recovering those brighter stars is well worth the e#ort, because they
o#er a variety of advantages over fainter stars. In general, for bright stars, the availability
of various data sources, such as the photometric survey 2MASS (Skrutskie et al. 2006),
or astrometric catalogs, e.g., US Naval Observatory CCD Astrograph Catalog (UCAC2;
Zacharias et al. 2000), or the Southern Proper Motion Catalog (SPM3.1; Girard et al. 2004),
provide useful additional information for the analysis of large samples of objects. However,
those data are often not available for the fainter stars. Hence, more detailed analyses,
including kinematic studies that make use of the full space motions, of many bright stars
can be carried out more quickly and easily.
The HES thus provides the opportunity to quickly identify many bright metalípoor stars
in a systematic fashion. Such objects provide important information in the intermediate
magnitude range between the early objective prism surveys and the HES. For example, a
second star, HE 1327-2326, with an extremely low iron abundance of [Fe/H] = -5.4 (Frebel
et al. 2005, 2006; Aoki et al. 2006) was already recently discovered in the sample of bright
HES stars discussed in this paper.
Here we present the sample of bright metalípoor candidates selected from the HES. The
candidate selection is described in ç 2, while the results of the followíup observations of the
sample are presented in ç 3. In ç 4 we outline our data analysis and the abundance results
of the metalípoor stars found in the sample. In ç 5 we briefly conclude with an outlook for
future work concerning the newlyídiscovered stars.

-- 4 --
2. The Hamburg/ESO Survey
2.1. Recovering the bright metalípoor stars
The HES is an objectiveíprism survey initially designed to search for bright quasars
(14 < B < 18) in the southern sky (Wisotzki et al. 2000). Exploitation of the stellar content
amongst the # 4 million digital spectra was initiated later. Thus far, 329 (out of 380) HES
plates have been searched for metalípoor stars and other stellar objects, e.g., field horizontal
branch stars (Christlieb et al. 2005) or DA white dwarfs (Christlieb et al. 2001b). The
remaining plates have recently been processed and followíup work is now underway.
The extraction and selection of objects in the HES from the photographic survey plates
is described in the following. After the construction of an input source catalog using the Digí
itized Sky Survey (DSS), an astrometric transformation was established between the direct
(photographic) and spectral plates that yielded the position of each object on the spectral
plate. Thus, wavelength zero points were derived. The wavelength range of all HES spectra
is set by the atmospheric cutío# at 3200 Ú A and the sharp sensitivity cutío# of the IIIaíJ emulí
sion at 5400 Ú A. The survey spectra in the HES database were first classified into three groups:
stars, ext, bright, with stars standing for spectra of point sources, ext for spectra of
extended objects, and bright for possibly saturated spectra of point sources. Depending
on each group, the spectra were extracted with appropriate algorithms (see Wisotzki et al.
2000 for more details). Each object was assigned a 12 character HES designation such as
``HE 1234-5678''. The digit combination is based on the B1950 coordinates of the object.
This paper investigates the stellar HES spectra classified as bright only. The main
di#erence between star and bright is a brightness cutío# defined by the level of saturation.
Figure 1 shows three bright survey spectra to demonstrate the di#erent levels of saturation.
2.2. The calibration
We seek to select metalípoor stars in a wide color range, i.e., stars near the mainí
sequence turno# point as well as subgiants and giants. Thus, it is important to apply a
selection that takes into account the strength of the Ca II K line (which is the strongest metal
absorption line in the optical wavelength range) as a function not only of the metallicity of a
star, but also of its e#ective temperature. The strength of the Ca II K line can be measured
in the HES spectra by means of the line index KP (a pseudoíequivalent width measurement
in Ú A) as defined by Beers et al. (1999).
The algorithm we employ here to select such metalípoor candidates had previously only

-- 5 --
been used in conjunction with unsaturated spectra of faint stars (i.e., stars). Hence, it was
first necessary to test whether or not the selection algorithm would be applicable to partially
saturated spectra. We verified with HK survey stars (Beers et al. 1992) present on HES
plates that the HES KP measurements are in good agreement with the measurements made
in moderateíresolution (i.e., ## # 2 Ú A) followíup spectra. However, the 298 HK survey stars
used for this verification cover the magnitude range 13 < B < 14.5, which corresponds only
to the faint end of the bright sample (see Figure 2 for the B distributions of the two samples).
Later, we learned that for the brighter stars the saturation of their spectra becomes stronger,
and results in a systematic underestimate of the KP index. Unfortunately, the same problem
occurs for any stars with KP > 5 Ú A, where the survey data underestimates the index strength,
regardless the brightness of the star. It follows that the selection e#ciency of metalípoor
giants is low, because more metalírich giants were mistaken as metalípoor. However, no
metalípoor stars should be lost due this problem. This is illustrated in Figure 3, where the
KP measurements from the prismísurvey are compared with those obtained from mediumí
resolution spectroscopic data.
It is also possible to measure the B - V color directly from the HES spectra, using the
``half power point'' technique described by Wisotzki et al. (2000). The B - V color of the
unsaturated HES objects has an uncertainty of 0.1 mag (Christlieb et al. 2001a). Figure 4
shows that equally good results can be achieved for the HES bright stars fainter than
B # 13. However, for the brighter stars the scatter increases significantly, and the B - V
color of the redder objects is systematically underestimated. This can be explained by the
fact that the photographic emulsion is more sensitive in the red part of the HES spectra
than it is in the blue. Thus, the saturation e#ects should appear first in the red, and they
should be more pronounced for red stars. The consequences of this issue for our sample are
further described in ç 3.3.
2.3. The selection
In this section we briefly describe the selection of metalípoor candidates amongst bright
HES stars. Initially, no CCD photometry was available for HES stars brighter than B # 13.
Based on the results from the comparison with the HK survey sample, we concluded that
the overall level of saturation was not too strong, and that the quality of our survey spectra
would be su#cient to begin the search for bright metalípoor stars.
In the first step, we restricted the range of objects to be considered to 0.3 < B-V < 1.2.
This corresponds to stars redder than the mainísequence turno# point for metalípoor stars
of an age of about 12 Gyr, and bluer than the stars at the tip of the red giant branch. On

-- 6 --
both sides of the color range, the chosen cutío# allows for an error margin of about 0.1 mag.
During the selection, we ignored any potential reddening of the stars. The HES stars are
located at high galactic latitudes, and any reddening usually is considerably smaller than
0.1 mag (see e.g., Christlieb et al. 2005).
For the second step of the selection, we determined a cutío# line in the KP index versus
B - V color parameter space in the following way. A set of simulated stars with KP and
B - V , equally distributed in the range 0--15 Ú A and 0.3--1.2 mag, was created. For these
simulated stars, we estimated [Fe/H] using the techniques of Beers et al. (1999). All stars
with metallicities in the range of -2.6 < [Fe/H] < -2.4 were selected. A cutío# line was fit
to this set of data. The result will be discussed in further detail in a forthcoming paper (N.
Christlieb et al. 2006, in preparation). All HES stars with a KP index lower than the cutío#
value determined for its B -V color were selected as metalípoor candidates. This results in
a metallicity cutío# at [Fe/H] = -2.5. Applying this technique yielded 5081 raw candidates.
In the final step of the selection, the raw and extracted HES spectra of these objects and
the corresponding area of the direct plates available in the DSS were inspected in order to
eliminate false positives due to plate artifacts, scratches, dust on the HES plates, emulsion
flaws, ghosts and object extraction at a slightly wrong position on the spectral plate (a
misípositioned extraction results in systematically too low values of the Ca II K index).
2.4. The visual inspection
The apparent strength of the Ca II K line at 3933 Ú A was visually estimated against the
continuum. Depending on how strong the line appeared, the objects were classified into
several metalípoor classes (mpc) : mpca --- the spectrum clearly shows no Ca II K line; unid
--- it is unclear if a Ca II K line is visible in the spectrum or not; mpcb --- a weak Ca II
K line is visible; and mpcc --- a significant Ca II K line appears against the continuum.
The remaining stars were grouped into star --- ordinary (metalírich) star; hbab --- hot
horizontal branch A or B stars displaying (very) strong Balmer lines; art --- plate artefact;
ovl --- overlap of spectra of optically close stars due to unfortunate dispersion direction;
and gal --- galaxy, the object appeared to be extended on the direct image of the DSS. We
identified 3309 spectra as belonging to the non metalípoor classes.
This leaves 1767 bright metalípoor candidates to form our working sample. Figure 5
shows some examples of the four metalípoor classes, together with their followíup spectra
(see ç 3 for more details). The division of the candidates into the classes resulting from the
visual inspection is presented in Table 1.

-- 7 --
For 1626 of the total 1767 stars there are HES B magnitudes available; the remaining
stars are beyond the bright end of the magnitude range covered by the photometric sequences
used to calibrate the HES photometry (see Wisotzki et al. 2000 for a description of the HES
photometry). The average magnitude of the bright stars is B # 11.5 mag. The B magnitude
distribution of the sample of bright stars is shown in the top panel of Figure 6, together with
the distributions of the HK survey and the faint HES stars. All three samples complement
each other in brightness, covering a range of almost 10 magnitudes.
Concerning the HES, one might expect that the sample of bright HES stars would
smoothly add objects to the bright tail of the distribution of the faint HES stars. However,
this is not the case. Rather, the combined HES stars show a bimodal distribution. The
form of the distribution can be explained by a selection bias present in the sample of bright
metalípoor candidates from the HES. As discussed in ç 2.3 above, the saturation of the HES
spectra of bright stars results in a systematic underestimation of their Ca II K line index,
hence a large number of false positives enter the candidate sample. This e#ect is strongest
for the brightest stars, thus, bright stars are strongly overírepresented in the sample of bright
metalípoor candidates.
If this explanation is correct, than the bimodal distribution should not be seen in the
sample of confirmed HES metalípoor stars. Indeed, as shown in Figure 6 (thick lined envelope
of bottom panel), the magnitude distribution is smooth when the false positives are removed.
2.5. Crossícorrelation with other catalogs
In order to identify reídiscovered stars in our sample and to gain additional information
for as many sample stars are possible, a crossícorrelation of the HES database with several
catalogs was carried out. We identified stars in the 2MASS All Sky Data Release (Skrutskie
et al. 2006) and obtained J , H and K magnitudes, in the UCAC2 (Zacharias et al. 2000)
and in the SPM3.1 (Girard et al. 2004) catalog to retrieve proper motions. We then crossí
correlated with the HK survey database, and found a number of stars from the HK survey
in our sample. We also made use of the following catalogs: the noníkinematically selected
stellar sample from Bidelman & MacConnell (1973), the kinematically selected metalípoor
stars samples of Ryan & Norris (1991), and Carney et al. (1994). Finally, we made extensive
use of the SIMBAD database. During this search many of our stars appeared in wellíknown
surveys, such as the Guide Star Catalog, the Positions and Proper Motion Catalog, or the
HIPPARCOS/TYCHO catalog. See Table 2 for the numbers of stars found in the catalogs

-- 8 --
and the SIMBAD database 3 .
We are aware of 29 stars in our sample known to have [Fe/H] # -2.0. It should be noted
though, that, due to our selection criteria, our sample is supposed to only contain objects
with [Fe/H] < -2.5. Hence, it is expected that stars with [Fe/H] > -2.5 are missing from
our compilation of rediscovered objects. Many of these objects were found in several catalogs
or studies. Twenty four of those are metalípoor stars. For 16 of them, an analysis based
on highíresolution spectroscopy can be found in the literature. The reídiscovered HES stars
are listed in Table 3, together with selected other names, as well as, where available, iron
abundances based on mediumí and/or highíresolution studies. For comparison, in column
(2) we also list our final iron abundance estimate. Amongst the reídiscovered stars are
G64í12 (HE 1337+0012; Carney & Peterson 1981) and the wellíknown strongly ríprocess
enhanced metalípoor star CS 22892í052 (HE 2214-1654; Sneden et al. 1996). These reí
discoveries show that our technique is successful in finding metalípoor stars. We flagged
the reídiscovered stars as such and kept them in our database as reference objects and for
statistical purposes (see ç 4.2).
In Table 4 we list five rediscovered stars for which we determined [Fe/H] < -2.0, but
which are horizontalíbranch stars. From these rediscoveries, we learn that our technique also
works for other types of stars (as long as the indices and colors are within their acceptable
ranges): HE 0411-3558, for example, is a horizontalíbranch (HB) star discovered by Beers
et al. (1992) (CS 22186í005). They measured [Fe/H] = -2.66 from a mediumíresolution
spectrum, while Ryan et al. (1996) obtained [Fe/H] = -2.77 from highíresolution data. Our
final estimate is [Fe/H] = -2.86, which agrees well with the two other iron abundances.
Our followíup spectra do not include any gravityísensitive indicators available which is
accurate enough for allowing the determination of evolutionary status of the stars. Hence,
our sample of metalípoor stars is likely to have some contamination by HB stars. The
rediscovery of a HB star and a red HB star in our sample (as listed in Table 4) for which
we measured [Fe/H] < -2.0 confirms this. To quantify the expected level of contamination
in our sample, we determined the fraction of HB stars to metalípoor star in the catalog of
Beers et al. (1992). Based on gravityísensitive photometry, they classified all their spectra
according to evolutionary status. It appears that amongst the more metalípoor stars in their
sample, the frequency of HB stars is 5%- 10%. They also find # 2% RR Lyr variables. We
thus conclude that the contamination by HB stars is acceptably low for our work, and does
not pose any concerns to our conclusions.
Trying to identify the known metalípoor stars in our sample also suggested searching for
3 We generally used an 8'' search radius.

-- 9 --
stars that may have been lost in the process of visual inspection of the raw candidates. We
checked all stars discarded during the inspection in the SIMBAD database. Of the 3309 stars,
# 1100 had some sort of entry, and #250 of these had at least one reference listed. Only 5
stars have [Fe/H] < -2.5 4 . Table 5 gives further details, including our classification of these
stars. The two hbab classifications are not in disagreement with the original classification
found in the literature (i.e., they are a hot turno# star and horizintal branch star). Also,
the object classified as ovl could technically not have been picked up as metalípoor.
From a cross correlation with the HK survey database, we identified 44 stars, of which
30 are known to be Aítype stars (Wilhelm et al. 1999; Beers et al. 1996b). Of those 30, we
classified 27 as hbab, while the remainder are ovl. The 4 emissioníline objects and the one
RR Lyr star were all correctly classified as star, and hbab, respectively. The remaining HK
stars are more metalírich than [Fe/H] = -2.5.
We conclude that no stars were missed that should have been selected by our algorithm.
Based on this result, we infer that our visual selection mechanism works very well to select
the most metalípoor stars in a given sample of preíselected HES candidates.
3. Mediumíresolution followíup spectroscopy
3.1. Observations
The HES objectiveíprism spectra have a resolution of # 10 Ú A (i.e., R = #/## # 400)
at the Ca II K line, and an average S/N ratio of # 8/1, which is of su#cient quality to select
metalípoor candidates in large numbers. To obtain a more reliable estimate of the metallicity
than was known from the survey data, higheríquality spectra were needed. Hence, mediumí
resolution followíup observations were taken with several telescopes (SSO 2.3 m, KPNO 4 m,
CTIO 1.5 m, ESO 3.6 m, CTIO 4 m, AAT 5 3.9 m) in the periods Mar -- Apr 2003, Aug 2003 --
Apr 2004, and Sep -- Oct 2004. The spectra were obtained with a wavelength range covering
at least 3600-4800 Ú A, with R # 2, 000 and S/N > 20/1 at the Ca II K line. Exposure times
during good weather conditions varied between t exp # 20 - 300 s. Using longer exposure
times, these stars could also be observed through thin clouds or during periods with poor
4 A further 27 objects were later found to have been classified as metalípoor stars, but due to an unfortuí
nate incident they were lost when producing the final list of 1767 visually inspected metalípoor candidates.
Amongst those is the wellíknown metalípoor giant CD -38 245 (Bessell & Norris 1984). These objects will
be included in our ongoing studies of the remaining 51 HES fields.
5 Obtained during cloudy weather in a program not related to metalípoor stars of Ryan et al.

-- 10 --
seeing (i.e., FWHM > 2. ## 0). See Table 6 for more details on the followíup observations. Due
to the low spatial resolution of the DSS, from which the HES input catalog was created,
several spectra of two stars with small angular separation (i.e., # 3. ## 0) were not spatially
resolved on the survey plates. Hence, the ``pair'' was recorded with only one HES designation.
We identified 10 of these ``pairs'' in the course of the mediumíresolution observations. Since
it was not possible to decide which of the two stars would have been the correct metalípoor
candidate, both were observed, and the sample size consequently increased to 1777 objects.
3.2. Data reduction and processing
Depending on where the data were obtained, the reduction of the spectra was carried
out using di#erent software. SSO data were fully reduced with Figaro (Shortridge 1993)
and Fortran programs, the KPNO and CTIO data with IRAF 6 routines, the ESO data with
ESO/MIDAS (Warmels 1992), and the AAT data with IRAF.
Radial velocities of the targets were determined, and the spectra shifted to the restframe.
To obtain the most accurate radial velocities as possible from mediumíresolution spectra we
used the combined results of two di#erent methods: (1) Measuring the position of the Balmer
lines H#, H# and H# and (2) Fourier crossícorrelation template matching with a grid of model
atmosphere synthetic spectra with di#erent temperatures, gravities and metallicities.
From comparing the results obtained with the two methods, we found a systematic
o#set of # 10 km s -1 of the crossícorrelation method with respect to the Balmer line results.
However, we verified with observations of several standard stars taken during the program
that the Balmer line method had no systematic di#erence. To correct for the e#ect, we then
removed the o#set from the crossícorrelation radial velocities.
We adopt a weighted average of the two radial velocity measurements, where available.
The velocity uncertainties of the two methods are of the same order. The median of the
weighted uncertainty in the Balmer line method is # 7 km s -1 whereas it is # 4 km s -1 in
the crossícorrelation method. The advantage of the crossícorrelation method is that inforí
mation from the entire spectrum is used rather than just three individual lines as in the
Balmer line method. This leads to a more precise velocity determination with a lower uncerí
tainty. The median of final, weighted velocity uncertainty is # 3 km s -1 . Further systematic
6 IRAF is distributed by the National Optical Astronomy Observatories, which are operated by the Así
sociation of Universities for Research in Astronomy, Inc., under cooperative agreement with the National
Science Foundation.

-- 11 --
uncertainties, e.g., due to telescope/instrument instabilities, have not been considered.
We seek to use [Fe/H] as a metallicity indicator of the stars. However, iron lines are
not detectable in our mediumíresolution spectra, particularly in those of our targeted metalí
weak stars. Instead, the Ca II K resonance line at 3933 Ú A is very strong and can easily be
measured. We employ the Ca II K calibration of Beers et al. (1999) to estimate [Fe/H] for
each program star. This is done using the Ca II K line index KP (Beers et al. 1999) and
B - V . The KP index is obtained by comparing the mean flux of two continuum regions
around the Ca II K line with the flux of the Ca II K line itself. Regarding the color, we use
two di#erently derived estimates. (1) The color (B - V ) J-K obtained from the dereddened
2MASS J -K (see ç 3.3), and (2) the spectroscopically derived (B - V ) HP2 color based on
the HP2 line index and the Beers et al. (1999) method. The HP2 index is a measurement
of the strength of the H# line, which depends on the e#ective temperature of the star, and
hence its color. An advantage of using a color derived from the HP2 index is its independence
of reddening. Finally, we measure the Beers et al. GP index from a comparison of the mean
flux of two continuum regions with the flux of the CH band (Gíband) at 4300 Ú A. We use the
GP index to calculate carbon abundance estimates of all stars with [Fe/H] < -1.0 (see ç 4.3).
3.3. Comparison with accurate photometry
CCD photometry was obtained for 84 stars in the sample 7 . Additional photoelectric
photometry (e.g., Beers et al. 1985, 1992; Norris et al. 1999; AnthonyíTwarog et al. 2000) is
available for 298 HK survey stars rediscovered in the HES (see also ç 2.2). We compared these
data with the HES B magnitudes initially derived from the DSS direct plates. The agreement
is good, as shown in Figure 2. The saturation e#ects present in the spectra, however, were
expected to have an influence on our B-V . We used the combined data to test this. Figure 4
presents the comparison of the B - V colors. There is a clear deviation from the oneítoíone
B-V relationship with the brightness of the objects. From a division of the stars into three
brightness bins it is apparent that the saturation e#ects set in for stars brighter than B = 13,
thus spoiling the survey color measurements for these stars. In retrospect, this somewhat
contradicts our previous finding that the survey color measurements would not be strongly
influenced by saturation e#ects (see ç 2.2). However, this discrepancy can be understood for
the following reason. Previously, we used a sample that was too faint to be consistent with
our average brightness of B # 11.5 mag.
7 These data were taken by the Beers et al. collaboration as part of the ongoing e#ort to collect photometry
for metalípoor candidates.

-- 12 --
We had no knowledge at the outset of our project that the onset of the saturation
occured at B # 13, which is the brighter limit of the HK survey calibration sample. As
a consequence, we decided not to use the survey colors but replace them with new B - V
derived from the 2MASS J -K colors. We obtained a regression for a sample of stars with
known B-V and J -K colors (i.e., B-V = 0.2 + 0.642(J -K)+ 0.707(J -K) 2 ). For the
cases where no J -K color was available we used colors derived from the HP2 index, failing
which we adopted the original survey color. The new B - V colors agree well with those
derived from the HP2 index for stars with B - V < 0.7. As expected, for stars cooler than
this, the index becomes insensitive to temperature and the quality of the colors degrades.
The (B - V ) J-K color distribution is shown in Figure 7 (hatched distribution). The
majority of stars are turno# stars (B -V # 0.4), with several stars hotter than B-V = 0.3,
which was our initial blue limit for the selection of the sample. From the clear distribution of
initial HES colors in Figure 7, it is apparent that the new, (B -V ) J-K , colors are bluer than
(B-V ) HES , and in agreement with the results from the photometric colors. This e#ect could
explain why many Aítype stars, rather than metalípoor stars, were found in the sample (for
further discussion, see ç 4.7).
Concerning the selection algorithm, we conclude that it will function correctly only if
the survey B - V color is replaced with a better estimate, such as one based on the 2MASS
data.
4. Analysis of the sample
4.1. Iron abundance estimates
As described in ç 3.2, we use the Ca II K line to estimate the iron abundance for each
star. However, we first excluded all stars from the sample that were obviously misclassified,
e.g., objects with He lines or Ca II K emissioníline cores in the mediumíresolution spectra.
After that, we attempted to obtain abundances for stars with a KP index, in the range
0.0 < KP # 9.5 in three ways:
1. [Fe/H] B-V : Employing the Beers et al. (1999) calibration using the KP index together
with the color derived from the dereddened 2MASS J -K data, (B - V ) J-K . For this
method to be applicable, the color has to lie in the range 0.3 < (B - V ) J-K < 1.0.
2. [Fe/H] HP2 : Employing the Beers et al. calibration using the KP index, together with
the color derived from the HP2, (B - V ) HP2 . The index has to lie in the range 0.25 #
HP2 # 5.3

-- 13 --
3. [Fe/H] Rossi : Iron abundance estimates using the regression provided by Rossi et al.
(2005), based on the KP index and the 2MASS J - K color. For the J - K deí
reddening, we adopted the approach of Bonifacio et al. (2000) to infer E(J -K) from
the Schlegel et al. (1998) E(B - V ). Following Rossi et al., the color has to lie in the
range 0.2 # (J -K) 0 # 0.8.
The ranges of the indices and colors are imposed by the limits of the calibrations used.
Depending on the above criteria, not all methods could always be employed for each star,
and many have only a partial set of iron abundance estimates.
We note that this work focuses on the identification of the more metalípoor stars in the
sample. We thus concentrate on all objects with [Fe/H] < -1.0, and do not give further
consideration to stars with higher metallicities. [Fe/H] = -1.0 is the upper metallicity limit
of all the calibrations employed in this work, because the KP index begins to saturate for
stars more metalírich than [Fe/H] # -1.5 (Beers et al. 1999). We did not attempt to make
use of the autoícorrelation function technique (ACF; Beers et al. 1999) to determine iron
abundance estimates for the stars more metalírich than [Fe/H] # -1.5 in our sample. This
would be beyond the scope of the present investigation of finding the more metalípoor stars
in this sample. However, for a full kinematic analysis it would be desirable to obtain better
abundance estimates for such stars.
To best determine whether a star has [Fe/H] > -1.0 we applied the following proí
cedure. We weighted and averaged the abundances [Fe/H] B-V and [Fe/H] HP2 to form the
best estimate based on the Beers et al. (1999) method, [Fe/H] HP2/B-V . Compared to the
values determined from the Rossi et al. 2005 calibration, we regarded the former to be the
more robust estimates. We then discarded the iron abundance estimate of all stars with
[Fe/H] HP2/B-V > -1.0. On the other hand, when the star had [Fe/H] HP2/B-V < -1.0, we
averaged the [Fe/H] B-V and [Fe/H] Rossi values to form a best estimate based on the J - K
colors, [Fe/H] J-K . The [Fe/H] HP2/B-V was not further considered. Finally, we were left with
one abundance derived from the HP2 index ([Fe/H] HP2 ), as well as one obtained from the
J -K ([Fe/H] J-K ).
Before calculating the final iron abundance from the [Fe/H] HP2 and [Fe/H] J-K for the
remaining stars, we weighted the methods according to their temperature sensitivity. We
tested the change of the iron abundances to small variations of the input HP2 indices and
J - K colors. From that, we estimated that for stars with HP2 > 2.5 the iron abundances
derived from the HP2 indices are more robust than those based on the J -K colors. For stars
with HP2 # 2.5, both methods appeared to be about equally good. HP2 = 2.5 corresponds
to B - V # 0.5, which automatically results in a division of dwarfs (HP2 > 2.5) and giants
(HP2 # 2.5). We note that in a magnitudeílimited survey like ours, stars at B - V > 0.5

-- 14 --
are almost exclusively giants. The survey volume for cool dwarfs is neglible compared to the
survey volume for the higher luminosity giants, which are seen up to much larger distances.
In the following, we refer to dwarfs and giants according to their HP2 index. This is also
the lower, cooler, limit at which the HP2 index begins to lose sensitivity to the B - V
color. Additionally, we split the dwarfs and the giants each into carboníabundanceísensitive
GPístrong and GPínormal categories. When calculating the final average iron abundance of
GPístrong stars, no values from [Fe/H] HP2 were used. The appearance of a strong Gíband at
4300 Ú A may spoil the HP2 measurement. We used GP > 5.0 as a limit for giants and GP > 4.0
for dwarfs. With decreasing iron abundance, it is increasingly likely that GPístrong stars are
very carbon rich (see also discussion in ç 4.3).
Depending on availability of the various [Fe/H] estimates, we weighted and averaged
the values to obtain the final estimate [Fe/H] final . Table 7 shows the weights (for dwarfs
and giants seperately) for each of the two iron abundance estimates used to form a specific,
averaged value. In total we have identified 16% of the sample stars to be genuinely metalí
poor (i.e., 286 objects with [Fe/H] < -1.0). Table 8 lists further details on how many stars
were found below a given metallicity. We note that more than half of these stars are giants
(189 out of 286), despite the fact that our sample of 1777 stars comprises mostly dwarfs.
Due to the lower e#ective temperature, metalípoor giants are better candidates than
dwarfs amongst which to search for e.g., strong ríprocess enhancement. The cooler the
temperature, the stronger the absorption lines appear. This is of importance when searching
amongst metalídeficient stars where lines are expected to appear weak. The use of such
giants then allows the tracing of ríprocess enhancement down to the lowest metallicities.
Taking the number of previously identified metalípoor stars into account, the numbers
of newlyídiscovered metalípoor objects in this work are shown in Table 8. For completeness,
we also list the number of literature stars for which a highíresolution analysis has been
reported.
We note here that for the most ironípoor star HE 1327-2326, a metallicity of [Fe/H] final =
-4.3 was obtained, based on its mediumíresolution spectrum. The extremly low metallicí
ity of [Fe/H]= -5.4 was only determined from highíresolution spectra. The discrepancy
is due to interstellar Ca blending with the Ca II K line, which could not be resolved in
the mediumíresolution data. The overall metallicity covered by our sample ranges from
[Fe/H] final = -4.3 up to [Fe/H] final = -1 (chosen upper limit).

-- 15 --
4.2. E#ective yields and the metallicity distribution function
In the present context, the ``e#ective yield'' describes the fraction of genuine metalípoor
stars below a certain metallicity, compared with the total number of targeted stars (Beers
2000). In Table 9 we compare the ``e#ective yields'' of our bright metalípoor stars with
the faint HES and HK survey stars (data taken from Beers & Christlieb 2005). We obtain
significantly lower overall e#ective yields for our work in comparison with the HES faint
sample. This is not unexpected. Saturation e#ects had an important (negative) impact on
the survey colors by which the bright metalípoor candidates were selected (see ç 2.2), and
led to the majority of the entire sample falling outside our criteria for potential metalípoor
stars (see ç 4.1). Apart from saturation issues, the majority of the sample is bright and thus
likely to be relatively nearby. They might belong to the thick disk rather than the halo.
Hence, the contamination by more metalírich stars is larger compared to the sample of the
HES faint stars, which is claimed to comprise # 50% stars with [Fe/H] < -2.0 (Beers &
Christlieb 2005). However, when comparing our e#ective yields with those of the HK survey
(in its initial design with no available colors) they are of the same order.
The metallicity distribution function (MDF) of the stars with [Fe/H] < -1.0 from the
HK survey and our bright star sample is presented in Figure 8. Both samples include dwarfs
and giants. The HES bright distribution for stars with [Fe/H] < -1.0 has one main peak
at [Fe/H] # -2.3. This peak likely arises from the fact that the initial selection of bright
stars was aiming to find stars whose Ca II K line strengths measured in the survey spectra
indicated a metallicity of [Fe/H] # -2.5. Thus, in the case that the selection works well, the
majority of the genuine metalípoor stars confirmed after the mediumíresolution observations
should spread around [Fe/H] # -2.5. This explanation is supported by the fact that almost
half of the stars with [Fe/H] < -1.5 are fainter than B = 13. Hence, this subsample does
not contain as many of the brighter stars, whose initial selection as metalípoor candidates
was influenced by saturation e#ects. However, the dip in the distribution at [Fe/H] = -2.5
cannot be explained in this way. No explanation, other than this may be a low number
statistical e#ect, can currently be found for this dip.
Towards the higher metallicity cutío# of the MDF the number of stars rises significantly,
likely due to incorrectlyíselected objects. There is a link between a low selection e#ciency
and the brightness of the objects due to the saturation e#ects. About 95% of the stars in
the range of -1.5 < [Fe/H] < -1.0 are brighter than B = 13. This is the brightness limit
at which the saturation becomes much more severe for brighter stars. The combination of
[Fe/H] uncertainties, e.g., from the limits of the calibrations itself or the loss of sensitivity
to metallicity from [Fe/H] # -1.5 upwards, likely causes objects with a true [Fe/H] > -1.0
to appear in our MDF as metalípoor stars.

-- 16 --
We wish to emphasize that despite the low overall e#ective yields, this sample has
produced astrophysically important metalípoor stars. Based on our ongoing highíresolution
observations of the most metalípoor stars from this sample we have found HE 1327-2326
([Fe/H] < -5.4) and at least one strongly ríprocess enhanced star ([r/Fe] # 2.0, A. Frebel et
al. 2006, in preparation). Results on further stars will be reported elsewhere (see also ç 5).
4.3. Carbon abundance estimates
Metalípoor stars with enhanced carbon abundance are important to investigate, for
example, the shape of the initial mass function and the formation and evolution of the first
generations of stars. In recent years it has become apparent that the number of carbonírich
stars increases with decreasing metallicity (e.g., Beers & Christlieb 2005). The origin of
this trend is not well understood. Our sample is well suited to investigate the frequency of
CEMP stars amongst metalípoor stars.
One way to recognize carbon rich stars among metalípoor objects is by their Gíband
strengths (e.g., GP # 4.5). Amongst the 1777 stars in our sample, 216 have GP > 5. Only 30
stars, however, have GP > 6, while 6 objects have GP > 7. When considering the subsample
of stars with [Fe/H] < -1.0, the numbers become 43, 16, and 6, respectively. The index
begins to saturate from GP # 6 but certainly, GP # 6 indicates a very strong Gíband. If
the metallicity of a star is low and the GP index large, the star is very likely to be rich
in C. Figure 9 illustrates a sequence of strengths of the Gíband and the corresponding C
abundance based on the Rossi et al. (2005) calibration (see below). As an example, we
measured a Gíband strength of GP # 5.0 for CS 22892-052, the wellístudied ríprocessí and
CEMP star which was rediscovered in our sample. Beers et al. (1992) obtained GP # 5.5
from their mediumíresolution spectrum. They also derive [Fe/H] = -3.0, while we obtain
[Fe/H] = -3.1. McWilliam et al. (1995) then obtained a carbon abundance of [C/Fe] # 1.0
(from highíresolution data), which is in good agreement with our value of [C/Fe] = 1.2.
In general, the carbon abundance (with respect to H or Fe) can best be determined
from highíresolution observations. In the absence of such data for the entire sample of
stars with [Fe/H] < -1.0 we rely on a di#erent approach. We use the newly available
calibration of Rossi et al. (2005) to obtain estimates for the relative carbon abundances,
[C/Fe]. Their regression is suitable for an analysis based on the KP and GP indices measured
in mediumíresolution spectra. We added the constraint GP # 1.0 to ensure that the Gíband
was clearly present in the spectrum. See Table 10 for the numbers of mildly ([C/Fe] > 0.5)
and strongly ([C/Fe] > 1.0) carboníenriched objects found amongst the 53 dwarfs and 121
giants with [Fe/H] < -2.0 in our study. The lower limits given in the table are due to the

-- 17 --
constraint on the GP index to be larger than 1.0, which introduces a bias against carbonírich
dwarfs. Figure 10 then shows [C/Fe] for the 234 objects with GP > 1.0 and [Fe/H] < -1.0,
plotted against their iron abundances [Fe/H]. An increased spread of carbon abundances
with decreasing iron abundance is clearly seen. However, some stars are missing from the
figure because we have not calculated C abundances for objects with low Gíband strength
(i.e., GP < 1.0). Those stars would likely have low levels of C enhancement. As a consequence
of this constraint on the GP index most of our metalípoor dwarfs have no carbon abundance
estimate. Due to their higher temperature, the dwarfs are more strongly a#ected by this
constraint than the giants. Hence, we note here that we did not attempt to derive a relative
frequency of CEMP dwarfs. It is also worth mentioning that no [C/Fe] was estimated
for the most iron poor dwarf/subgiant HE 1327-2326. There is no Gíband visible in our
mediumíresolution spectrum (GP = 0.5). Additionally, no stars similar to HE 1327-2326
are available in the calibration (Rossi et al. 2005). Any derived value for such a star would
thus be untrustworthy. Finally, several authors in the literature have noted a general upper
limit of C enhancement with respect to the Sun only (e.g., Ryan 2003, [C/H] # -1.0). We
also find such an envelope at [C/H] # -0.7. However, we note that W. Aoki et al. (2006,
in preparation) and S. Lucatello et al. (2006, in preparation) find an upper limit on carbon
enhancement for carboníenhanced metalípoor stars close to [C/H] = 0.0.
4.4. The frequency of Cíenhanced metalípoor stars
If we now only consider the giants with [Fe/H] < -2.0 (which make up # 70% of the
objects below that limit), we find the frequency of metalípoor giants with a strong carbon
enhancement of [C/Fe] # 1.0 to be # 9% ‘ 2%. If we take giants with [Fe/H] < -2.5, the
frequency rises to 13% ‘ 4%, and to 25% ‘ 11% amongst giants with [Fe/H] < -3.0. The
uncertainties are based on Poisson statistics. One potential reason for the low percentage
of carboníenhanced stars below [Fe/H] = -2.0 may be that, for stars with GP > 6.0, the
calculated [C/Fe] has been underestimated by as much as 0.5 dex (Rossi et al. 2005). We
have two stars with GP = 7.5 and 7.9 which both have [C/Fe] = 0.9. Thus, they fall just
below our cutío# of 1.0. If those stars were to have an underestimated [C/Fe] by only 0.1 dex,
the frequency of giants with [Fe/H] < -2.0 would rise to 11% ‘ 3%.
We note here that our frequency estimates are not a#ected by the constraint on the
GP index (see above). Only stars with [C/Fe] > 1 were counted and compared to the
total number of stars with [Fe/H] < -2.0, -2.5 and -3.0, respectively. There clearly is
a metallicity e#ect on the frequency of CEMP stars. It almost triples when stars with
[Fe/H] < -3.0 are compared with those having [Fe/H] < -2.0. This is reflected in the larger

-- 18 --
spread of [C/Fe] with decreasing iron abundance.
Our average frequency of CEMP stars of 9%, however, is much lower than what is
quoted in Beers & Christlieb (2005). They mention ``at least 20%'' amongst stars with
[Fe/H] < -2.0. For a di#erent sample of HK survey stars with [Fe/H] < -2.5, Marsteller
et al. (2005) even find # 25% of the stars to be enhanced in carbon. Our low frequency
is, in any case, of the same order as what was found by Cohen et al. (2005) (14% ‘ 4%).
S. Lucatello et al. (2006, in preparation), however, report that at least 20% of the stars
with [Fe/H] < -2.0 from the large HERES sample of Barklem et al. (2005), based on highí
resolution spectroscopic determinations, exhibit [C/Fe] > 1.0.
We investigated the apparently low frequency farther by taking the sample of Beers,
Preston & Shectman (1992; hereafter BPSII) to derive the percentage of their CEMP stars
in the same fashion as adopted in the present work. A subsample of giants with HP2 < 2.0
was taken and [Fe/H] and [C/Fe] derived according to the Beers et al. (1999) method and the
Rossi et al. (2005) calibration, respectively. The subset of objects with [Fe/H] < -2.0 and
[C/Fe] > 1.0 was then compared to our sample after applying the same constraints 8 . Despite
the di#erent brightness and color distributions, as well as a di#erent distance distribution
(the BPSII sample being a little fainter and on average further away), we find their sample
to have the same, low, percentage as obtained for ours (# 9%). We note that by using
the Beers et al. (1999) method to obtain the iron abundance estimates, we are also able to
obtain estimates for the absolute magnitudes and distances of our stars.
We then tested whether there would be a variation in percentage with distance Z from
the Galactic Plane. Figure 11 shows the cumulative fractions of CEMP stars, where the
fraction is defined as the number of Cíenhanced objects amongst metalípoor stars further
from the Plane than the indicated Z. We performed this for two samples with [Fe/H] < -2.0
(top and middle panels) and [Fe/H] < -3.0 (bottom panel). The top panel shows the
frequency for both samples seperately. Both data sets exhibit very similar behavior. The
numbers of objects, however, become low with increasing distance from the Plane. Hence,
error bars have only been included in the middle and bottom panels, where the data sets are
combined to obtain the best estimate for the increase in percentage of CEMP objects for two
di#erent metallicities cutío#s. Concerning the sample with [Fe/H] < -2.0, there is a plateau
around # 9% out to Z # 2 kpc. However, as can be seen from Figure 11 (middle panel),
the frequency begins to increase significantly when going to larger distances. Considering
this behavior, the apparent discrepancy between our ratio and the Beers and collaborators
8 For consistency purposes we restricted [Fe/H] estimates to the [Fe/H] HP2
available for both samples,
avoiding possible systematic di#erences in the available colors.

-- 19 --
values may be resolved if their samples would contain more (fainter) stars at larger distances
from the Plane, compared to our sample. For example, at Z # 3 kpc, our figure suggest a
frequency of # 20 - 30%, in agreement with their reported estimates.
Motivated by the results from Figure 11, we investigated the distribution of our ``normal''
metalípoor stars (i.e., with [Fe/H] < -2 and [C/Fe] < 1.0) with distance from the Plane in
order to compare it with the distribution of the CEMP stars only. In an attempt to quantify
whether those two samples ('metalípoor' and 'CEMP' samples) were drawn from the same
population, we performed a KolmogorovíSmirnov (K--S) test (Siegel 1956) on the combined
sample as a function of Z. The result is presented in Figure 12.
The K--S test rejects the null hypothesis that the two samples are drawn from the same
parent population at the 5% significance level. It is indicative, however, that for Z # 2
the two samples may actually come from the same population. Performing additional K--S
tests on appropriate subsamples confirms that up to Z # 1.4 kpc, it can not be stated that
the samples come from di#erent populations. For larger Z, again, the null hypothesis is
rejected at a 5% singificance level, indicating that the samples are not drawn from the same
population.
From Figures 11 and 12 it appears that two e#ects influence the production of CEMP
stars. First, from the middle and bottom panel of Figure 11, we find a relative increase
of the CEMP frequency of # 20% when going from the sample with [Fe/H] < -2 to the
one with [Fe/H] < -3. The bottom panel shows a plateau around 27%, while there is a
steep increase with increasing distance from the Plane. The same pattern is found in the
sample with [Fe/H] < -2 (middle panel). Due to low sample numbers, the error bars are
quite large. However, it is indicative that the result would not be changed significantly if
a di#erent sample, containing more lower metallicity stars, would be employed to improve
the statistics. The overall elevated level for the lower metallicity sample is consistent with
previous findings of an increased frequency of CEMP stars with decreasing [Fe/H]. This
behavior may indicate that it is easier to produce Círich metalípoor stars in lowímetallicity
environments. However, it seems to be independent of the distance from the Galactic Plane.
The plateau at lower Z seen in Figure 11, together with the steep increase further out
than Z # 2 kpc suggests that there is a second, distanceídependent, e#ect. This is also
indicated by the results from the K--S tests. At Z # 1.4 kpc, a transition occurs between
the thick disk and halo material, causing di#erent chemical signatures (i.e. strong carbon
enrichment) to gain significance in the pool of normal metalípoor stars. Estimates of the
scale height of the thick disk vary from # 750 kpc up to # 1.5 kpc, where the bulk of the
values is between 1 and 1.5 kpc (e.g., Norris 1999, and references therein). The distance at
which we find this transition agrees well with the range of scale heights available for the thick

-- 20 --
disk. Our K--S tests supports a transition with respect to the production of CEMP stars.
Beyond this transition distance, the excess of CEMP objects cannot be directly linked to the
formation of normal metalípoor stars (i.e., the samples do not arise from same population).
At lower Z, however, the distance distributions of normal metalípoor and CEMP stars can
not be distiguished, suggesting a common origin for those two populations as well as for the
two chemical elements.
The question now arises as to how the productions of the elements (in particular carbon
and iron) are linked to each other and why they change with distance from the Galactic
Plane. Our result indicates that the thick disk plays a role out to Z # 2 kpc, but is much less
significant beyond that. Whether or not these di#erences are due to di#erent mechanisms for
the production of C in the thick disk and the halo remains to be investigated. Further studies
with respect to the (matter) density distributions of the thick disk and halo populations for
di#erent metallicity ranges would clearly be desired to test our findings more extensively.
4.5. The catalog of bright metalípoor candidates
Table 11 presents results for the metalípoor stars identified in this work, while Table
12 summarizes results for the remaining, non metalípoor stars. The entire tables are only
available electronically. A portion of each table is shown for guidance regarding their form
and content.
Both tables share the following columns and are arranged as follows:
Columns 1, 2 and 3 lists the HE name, right ascension and declination (J2000).
Columns 4, 5, 6 and 7 list B, B - V colors derived from HP2, B - V from (J - K) 0 , and
E(B - V ).
Column 8 lists the heliocentric radial velocities.
Columns 9, 10 and 11 list the indices KP, HP2 and GP.
Table 11 contains additional columns:
Column 12 presents the iron abundance [Fe/H] B-V derived from the KP and the B-V color.
Column 13 presents the iron abundance [Fe/H] HP2 derived from the KP and the HP2 index.
Column 14 presents the iron abundance [Fe/H] Rossi derived from the Rossi et al. (2005) calí
ibration.
Column 15 presents the iron abundance [Fe/H] final , the weighted and averaged iron abuní
dance of [Fe/H] HP2 and [Fe/H] J-K .
Column 16 presents the carbon to iron abundance ratio [C/Fe].

-- 21 --
Column 17 indicates whether the star has been rediscovered as metalípoor star with [Fe/H] <
-2.0.
Table 12 also contains Column 12, which shows whether the object could be identified
to be of a certain type of object, such as horizontalíbranch star or emissioníline object.
4.6. Measurement uncertainties
According to Wisotzki et al. (2000), the average dispersion of the HES magnitude for
objects fainter than B # 13 is #B # 0.2 mag. From Figure 2, we determine the dispersion for
those fainter stars to be # 0.1 mag, with a small o#set of # 0.1 mag. For the brighter objects,
there is an o#set of # 0.2 mag, while the dispersion is #B # 0.2 mag. As already shown in
ç 2.2, the HES B - V color has an uncerainty of 0.1 mag for stars fainter than B # 13.
However, as is apparent from Figure 4, for brighter stars, the uncertainties dramatically
increase for the brighter stars. Hence, they have not been used in the determination of
the metallicities. The replacement B - V color, obtained from the 2MASS J - K color
(# J-K # 0.03 mag), has a typical uncertainty of #B-V # 0.06 mag in dwarfs, and #B-V #
0.10 mag in giants, when the uncertainties in the regression coe#cients are accounted for. The
average 1 # uncertainty in our radial velocities is # 3 km s -1 , based on the two independent
measurements.
Using multiple observations (63 stars twice, 9 three times) we tested the accuracy of our
index measurements. The standard error (based on small number statistics) of the indices
are as follows: #KP = 0.18, #GP = 0.15 and # HP2 = 0.20. Table 13 shows the uncertainties in
the di#erent iron abundance estimates for these changes of the individual input parameters
as well as color changes. We simplified this uncertainty analysis by dividing the sample into
dwarfs (HP2 > 2.5), and giants (HP2 # 2.5) and assumed that the uncertainties would not
change significantly for members of each group. Furthermore, we divided each group into
the more metalípoor stars ([Fe/H] < -2) and more metalírich ones ([Fe/H] > -2), to test
whether there would be an e#ect with metallicity. Most uncertainties do not significantly
di#er between dwarfs and giants for each metallicity group, execpt in two cases (see Table 13
for details.)
Generally, the uncertainties are small, around # 0.1 dex per parameter change. It is
apparent, though, that the major source of error arises from uncertainty in the B- V color.
For the more metalípoor objects it is # 0.2 dex, and doubles for stars with [Fe/H] > -2.
This, however, is in agreement with the calibration losing sensitivity above [Fe/H] # -1.7
(Beers et al. 1999). To obtain reliable iron abundance estimates, other techniques, such as

-- 22 --
the ACF, would have to be employed in this metallicity range (see Beers et al. 1999). In
any case, this behaviour argues for the use of the HP2 derived abundances. Even in the
range where this method begins to lose sensitivity, (i.e., for cooler giants), the uncertainty
for giants is still lower than that for the B-V color. For stars with KP < 2 Ú A, the uncertainty
in [Fe/H] increases by a factor of # 2 - 3 compared to the typical value.
We are concerned that our uncertainties may be underestimated. This is apparent
from our uncertainties for the [Fe/H] and [C/Fe] estimates based on the Rossi et al. (2005)
calibration. Our derived values appear to be rather small, but when the uncertainties of the
regression coe#cients are taken into account, they increase to 0.5 ([Fe/H] < -2) and 0.6 dex
([Fe/H] > -2), where the dwarfs have # 0.15 dex lower values than the giants. A similar,
but less strong e#ect occurs for [C/Fe], where the uncertainties raise to # 0.2 dex for all
stars.
In Figure 13 a comparison is shown between our iron abundance estimates and lití
erature values for the set of rediscovered stars. The mean deviation from the oneítoíone
relation is # 0.2 dex when comparing with the highíresolution literature data and # 0.3 dex
for the mediumíresolution literature values. These are in good agreement with the [Fe/H]
uncertainties discussed above.
4.7. Other findings
Although we were searching for metalípoor stars, we coincidentally found several groups
of other objects. The majority of these other objects are too hot or of some other nature
to be identified as metalípoor in the present survey. Due to the sometimes very prominent
He I lines in their spectra, we were able to visually identify 17 Oí and Bístars. These objects
are likely to have been selected due to their apparently weak Ca II K line strength resulting
from their high temperatures, in combination with erroneous HES color information (see
also the caption of Table 12). Also, about 330 stars have HP2 indices larger than 5.3, which
is our upper limit for metalípoor mainísequence turno# stars. A further 360 stars have
4.0 < HP2 < 5.3, for which we did not compute iron abundances (they either did not satisfy
all the criteria for the [Fe/H] determination, or they were simply too metalírich). HP2 = 4.0
corresponds to B - V # 0.4. We regard these objects as either mainísequence Aítype or
field horizontalíbranch candidates. At least two stars in our sample for which we initially
computed metallicities have been identified as Aítype stars (CS 22185í008, CS 22185í025;
Wilhelm et al. 1999; Beers et al. 1996b). They both have HP2 > 5.3. This suggests that
many Aítype stars may exist among these almost 700 objects.

-- 23 --
Many of the cooler stars found in the sample exhibit strong Ca I absorption at 4226 Ú A
in their spectra. Seventeen stars exhibit emission cores in their Ca II H and K lines, some
of which also show emission in the H# line. From our crossícorrelation with the HK survey,
we know of two such stars previously identified as emissioníline objects. Beers et al. (1994,
1996a) list emissioníline HK objects which were found in the same fashion as ours, as byí
products in the search for metalípoor stars. HE 1521-0033 (CS 22890í077= BS 16559í
084; Beers et al. 1994) was marked to have ``weak Ca II H and K core emission'' while
HE 0011-3837 (CS 31077í034; Beers et al. 1996a) was classified as having ``moderate Ca II
H and K emission''. Emissioníline cores result from active chromospheres in lateítype stars,
which may be used to trace the structure of the outer stellar atmosphere. Figure 14 shows
the spectrum of one such star. Further details on these objects can be found in Table 12.
It is beyond the scope of this investigation to track how many of our emissioníline
objects and field horizontalíbranch stars have been previously identified by other studies.
We believe, though, that there would be a number of stars that are already known in the
literature.
Through our search with the SIMBAD database we also found that our sample contains
at least three variables (of which two are RR Lyrae objects), one eclipsing binary, and one
novaílike star. Another object is a double or multiple star. From selected highíresolution
observations we know of at least two doubleílined spectroscopic binaries. We marked those
stars accordingly in Table 12 (column (12)).
5. Summary and outlook on future highíresolution spectroscopy
In this paper we have presented a sample of 1777 bright (9 < B < 14) metalípoor
candidates selected from the Hamburg/ESO survey. Compared to the previously explored
faint HES metalípoor stars, our sample contains stars whose objectiveíprism spectra su#er
from saturation e#ects. The selection procedure has been described in detail, together with
results from mediumíresolution followíup spectroscopy of the entire sample (Table 11). From
the mediumíresolution observations, the metallicity [Fe/H] was determined by means of the
Beers et al. (1999) method involving the KP index and a spectroscopically or photometrically
derived B - V color. Based on the 2MASS J - K colors, we also employed the Rossi
et al. (2005) calibrations to obtain a third iron abundance estimate, as well as [C/Fe].
Where available, the iron abundances derived from the di#erent methods were weighted and
averaged. In total we have identified 16% of the sample stars to be of metalípoor nature (i.e.,
286 objects with [Fe/H] < -1.0). Of those, 174 have [Fe/H] < -2.0, 98 have [Fe/H] < -2.5,
and 23 have [Fe/H] < -3.0. Amongst those objects with [Fe/H] < -2.0, we found 13

-- 24 --
carbonírich objects with [C/Fe] > 1.0 . Apart from the metalípoor stars, a few examples of
other groups were also serendipitously identified (through the SIMBAD data base), such as
mainísequence Aítype stars, emissioníline objects, variable stars and one novaílike star.
Due to rediscoveries of several metalípoor stars from the HK survey and other studies,
# 30 of the 286 metalípoor stars are already known as such in the literature. This leaves
# 250 bright objects newly classified as metalípoor. The e#ective yields of our sample are
of roughly the same order as found in the HK survey. These are significantly lower than
reported for the faint HES stars. This di#erence can largely be understood in terms of the
saturation e#ects and the subsequent, adversely a#ected, selection. We also investigated the
frequency of Cíenhanced objects amongst metalípoor stars with distance from the Galactic
Plane. Two e#ects are likely to play a role in the production of Círich objects in the Galaxy.
First, the frequency of CEMP stars is higher for lowerímetallicity samples, perhaps indicating
that the carbon production becomes more e#cient with decreasing [Fe/H]. We find this e#ect
to exist independent of distance from the galactic plane. The second e#ect is a plateau of the
frequency of CEMP objects out to Z # 2 kpc (regardless of the sample metallicity cutío#),
complemented with a steep increase for larger distances. This may be due to a di#erent
mechanism for the production of carbon and iron in the di#erent populations. For the halo
population, at least, the mechanism does not seem to be the same for normal metalípoor
and CEMP stars.
Using 4í8m class telescopes snapshot spectroscopy (R # 20, 000, S/N > 30 per pixel
at # 4100 Ú A) of selected targets with su#ciently low metallicity is well underway. Our
general procedure is as follows. If a spectrum indicates any interesting features, e.g., rí
/síprocess enrichment or a metallicity as low as [Fe/H] < -4.0 we are obtaining higher
resolution (R> 40, 000), higher signalítoínoise observations. These data are then used for a
detailed abundance analysis. This has already been done for one bright star in particular,
HE 1327-2326. Subaru/HDS data were obtained and revealed it to be the new record holder
for the most ironípoor star known to date, with [Fe/H] = -5.4 (Frebel et al. 2005, 2006;
Aoki et al. 2006). Further papers of this series on bright metalípoor stars from the HES
will include the highíresolution spectroscopic analyses of the metalípoor objects indentified
in the present study as well as the candidate followíup spectroscopy of the remaining, yet
unexplored, 51 HES fields (Frebel et al. 2006, in preparation).
We thank S. Tsangarides and J. D. Tanner for reducing the AAT data and E. Westra
for useful comments on earlier versions of the manuscript. A. F., J. E. N. and M. S. B.
acknowledge support from the Australian Research Council under grants DP0342613 and
DP0663562. N. C. and D. R. acknowledge support from Deutsche Forschungsgemeinschaft
under grants Ch 214/3 and Re 353/44. T. C. B acknowledges support from grants AST

-- 25 --
04í06784 and PHY 02í16783, Physics Frontier Centers/JINA: Joint Institute for Nuclear
Astrophysics, awarded by the U.S. National Science Foundation. S. R. thanks FAPESP,
CNPq and Capes for partial financial support.
This research has made use of the SIMBAD database, operated at CDS, Strasbourg,
France. It makes use of data products from the Two Micron All Sky Survey, which is a
joint project of the University of Massachusetts and the Infrared Processing and Analysis
Center/California Institute of Technology, funded by the National Aeronautics and Space
Administration and the National Science Foundation.
Facilities: ATT (DBS), CTIO:1.5m (RíCS), Blanco (RíCS), Mayall (RíCS), ESO:3.6m
(EFOSC), AAT (UCLES)
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-- 30 --
Table 1. Results of the visual inspection
Class a Number Comment
``mpca'' 9 No Ca II K visible
``unid'' 84 Uncertain if Ca II K visible
``mpcb'' 248 Relatively weak Ca II K
``mpcc'' 1426 Relatively strong Ca II K
Note. --- 1767 objects were selected from the
5081 raw candidates.
a See Figure 5 for example objects which illusí
trate the di#erent classes.

-- 31 --
Table 2. Bright candidates identified in other catalogs
Catalog Number
HK survey; Beers et al. (1999) 26
Ryan & Norris (1991) 9
Carney et al. (1994) 5
Bidelman & MacConnell (1973) 1
SIMBAD (i.e., any other cat.) # 1250 a
2MASS; Skrutskie et al. (2006) 1568
SPM3.1; Girard et al. (2004) 392
UCAC2; Zacharias et al. (2000) 1717
a Of these stars, actually only #150 have at
least one reference listed in SIMBAD.

-- 32 --
Table 3. Previous identifications of stars with [Fe/H] final < -2.0
HE name [Fe/H] final Other names a [Fe/H] med.-res. [Fe/H] high-res. References
HE 0002-3233 -2.86 CS 22961í023 -2.79 § § § 1
HE 0007-1752 -2.16 CS 31060í043 § § § -2.06 2, 3
HE 0017-3646 -2.42 CS 30339í040 -2.26 § § § 4
HE 0027-1221 -2.56 CS 31062í050 § § § -2.33 2, 5
HE 0039-2635 -3.60 CS 29497í034 § § § -3.60 6
HE 0054-2542 -3.05 CS 22942í019 -3.28 -2.64 4, 5
HE 0056-3022 -3.15 CD-30 298, a, b, c, d, e -2.90 -3.30 7, 8
HE 0111-1118 -2.13 CS 22174í007 -2.55 § § § 2, 1
HE 0236-0242 -2.13 CS 22954í015 -1.32 § § § 4
HE 0311-1046 -3.39 CS 22172í002 -3.57 -3.61 9, 10
HE 0315-1528 -2.91 CS 22185í007 -2.48 -2.45 4, 3
HE 0317-3301 -2.85 CD-33 1173, a, b, c, d, e, g -3.12 -3.30 11, 12
HE 0336-2412 -2.74 CD-24 1782, b, c, d, e -2.70 -2.31 7, 13
HE 0409-1212f -2.62 CS 22169í035 -3.08 -2.72 4, 14
HE 0926-0508 -2.80 BS 17572í100 -2.17 § § § 1
HE 0938+0114 -2.70 BD+01 2341p, G 48í29, LP 608í 62 -2.70 -2.70 15, 16
HE 1144-1349 -2.75 BD-13 3442, a, b, c, g -3.12 -3.14 11, 17
HE 1208+0040 -2.19 G 11í44, Ross 453, c, d, g -2.37 -2.37 11, 18
HE 1337+0012 -3.12 G 64í12 § § § -3.52 19
HE 2002-5843 -2.76 CS 22873í128 -2.61 -2.88 4, 20
HE 2119-4653 -2.83 [M93]16090 -2.63 § § § 21
HE 2138-1526 -2.25 CS 22944í11 -1.85 § § § 4
HE 2214-1654 -3.17 CS 22892í52 -3.00 -3.10 4, 20
HE 2301-0248 -2.09 G28í31, LP 701í67, b, h -2.33 § § § 22
Note. --- [Fe/H] med.-res. and [Fe/H] high-res. refer to the iron abundances based on mediumí and highíresolution spectra
first found in the literature. The corresponding references are given.
a Selected other names only; stars are also found in the following catalogs: a: PPM (RØoser et al. 1994), b: GSC (Lasker
et al. 1990), c: Tycho/Hipparcos (Perryman & ESA 1997), d: CPD (Gill 1896), e: Hipparcos Input Cat. (Turon et al.
1993), f: SAO, h: NLTT (Luyten 1995)
References. --- (1) Schuster et al. (2004), (2) Norris et al. (1985), (3) Lai et al. (2004), (4) Beers et al. (1992), (5) Aoki
et al. (2002), (6) Barbuy et al. (1997), (7) Bond (1980), (8) Bessell et al. (1991), (9) Ryan et al. (1996), (10) Norris et al.
(2001), (11) Ryan & Norris (1991), (12) Spite & Spite (1993), (13) Luck & Bond (1983), (14) Honda et al. (2004), (15)
Hobbs & Duncan (1987), (16) Pilachowski et al. (1993), (17) Ryan et al. (1991), (18) Thorburn (1994), (19) Carney &
Peterson (1981), (20) McWilliam et al. (1995), (21) Morrison (1993), (22) Laird et al. (1988)

-- 33 --
Table 4. Selected previous identification of other objects
HE name Other names a Ref. Comment
HE 0411-3558 CS 22186í005 1 HB
HE 2247-4113 CDí41 15048, a, b, c, d, e 2 RHB
HE 1252-0511 AT Vir, b, c, e 3 RR Lyr Var
HE 2325-4743 RV Phe, CDí48 14514, c 4 RR Lyr Var
HE 2210-4058 SON 7481 5 suspected RR Lyr Var
Note. --- Selected other names; selected references which first referred to
the nature of the star.
a Also found in the following catalogs: a: PPM (RØoser et al. 1994), b: GSC
(Lasker et al. 1990), c: Tycho/Hipparcos (Perryman & ESA 1997), d: CPD
(Gill 1896), e: Hipparcos Input Cat. (Turon et al. 1993)
References. --- (1) Beers et al. (1992), (2) Norris et al. (1985), (3) Ho#meisí
ter (1930), (4) Lourens (1960), (5) Demartino et al. (1996)

-- 34 --
Table 5. Stars with [Fe/H] < -2.5 not identified as metalípoor in the visual inspection
HE name Classification Other names [Fe/H] Type Ref.
HE 0038-2423 hbab CS 29497í030 -2.8 TO (hot) 1
HE 0042-2141 hbab CS 29527í057 -2.7 HB 2
HE 0303-2230 star LP 831í70 -3.5 3
HE 2134-3940 ovl CS 22948í027 -3.2 Círich TO 4
HE 2131+0010 unid G26í12, LP 638í7 -2.6 TO 4
Note. --- For details on the classifications, see text. TO: Turno# star, HB:
Horizontal Branch Star
References. --- (1) Sivarani et al. (2004), (2) Schuster et al. (2004), (3) Ryan
& Norris (1991), (4) Barbuy et al. (1997)

-- 35 --
Table 6. Telescopes used for the medium resolution observations
Telescope Instrument Observers No.
2.3 m, SSO DBS Bessell, Frebel, 1477
Norris, Thom
4.0 m, KPNO RíC Spectrograph Beers, Marsteller 92
1.5 m, CTIO RíC Spectrograph Rhee 82
3.6 m, ESO EFOSC2 Fechner 67
4.0 m, CTIO RíC Spectrograph Beers, Rossi 46
3.9 m, AAO RGO Norris 13

-- 36 --
Table 7. Weights applied to the iron abundances
Iron abundances Weights
[Fe/H] HP2 , [Fe/H] B-V dwarfs 0.8, 0.2
giants 0.5, 0.5
[Fe/H] B-V , [Fe/H] Rossi dwarfs 0.5, 0.5
giants 0.5, 0.5
[Fe/H] HP2 , [Fe/H] J-K dwarfs 0.7, 0.3
giants 0.5, 0.5
Note. --- ``dwarfs'' refers to 2.5 < HP2 < 5.3
and ``giants'' to 0.25 < HP2 # 2.5. See text for
further details.

-- 37 --
Table 8. Metalípoor stars found in the sample
[Fe/H] range N N redisc.
a N high-res.
b N new
[Fe/H] < -2.0 174 29 16 145
[Fe/H] < -2.5 98 19 14 79
[Fe/H] < -3.0 23 6 6 17
a The rediscoveries refer to previous identifications
of stars with [Fe/H] < -2.0 listed in SIMBAD.
b These stars are rediscovered and have highí
resolution spectral analysis reported in the literaí
ture. See Table 3 for references and text for disí
cussion.

-- 38 --
Table 9. ``E#ective yields'' of the sample
Survey No. [Fe/H]
< -2.0 < -2.5 < -3.0
HK survey/no B - V 2614 11% 4% 1%
HK survey/with B - V 2140 32% 11% 3%
HES bright (all) 1777 11% 6% 2%
HES bright (B # 13) 161 49% 31% 11%
HES bright (B # 13) dwarfs 155 33% 16% 2%
HES bright (B # 13) giants 106 58% 39% 15%
HES faint (dwarfs) 571 59% 21% 6%
HES faint (giants) 643 50% 20% 6%
Note. --- Results for HK survey and faint HES giants are taken from
Beers & Christlieb (2005).

-- 39 --
Table 10. CEMP stars with [Fe/H] < -2.0 found in the sample
Level of C enrichment N a
[C/Fe] > 0.5 dwarfs 3
giants 18
[C/Fe] > 1.0 dwarfs 2
giants 11
a The values given for the
dwarfs should be regarded as
lower limits. See ç 4.3 for furí
ther details.

Table
11.
The
286
bright
metalípoor
stars
with
[Fe/H]
<
-1.0
Star
name
R.A.
#
B
(B
-V)
HP2
(B
-V)J-K
E(B-V)
v
rad
KP
HP2
GP
[Fe/H]
B-V
[Fe/H]
HP2
[Fe/H]
Rossi
[Fe/H]
final
[C/Fe]
Redisc.
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
(16)
(17)
HE
0002-3233
00
05
32.3
-32
16
36
12.5
0.42
0.47
0.02
48
1.30
4.24
0.48
-2.98
-2.87
-2.67
-2.86
§
§
§
*
HE
0003-0503
00
05
56.8
-04
47
06
11.4
0.47
0.82
0.03
-2
6.82
3.39
4.21
-2.28
-1.03
-2.23
-2.23
0.11
HE
0003-5106
00
06
29.8
-50
49
31
11.5
0.69
0.83
0.01
235
6.82
1.10
1.73
-2.35
-2.16
-2.26
-2.23
-0.67
HE
0007-1752
00
10
17.6
-17
35
38
12.2
0.60
0.65
0.03
216
5.44
1.63
1.96
-2.24
-2.12
-2.17
-2.16
-0.22
*
HE
0010-1316
00
13
30.7
-12
59
60
13.0
0.82
1.02
0.03
-86
7.81
0.72
2.12
§
§
§
-1.94
-2.44
-2.19
-0.69
HE
0012-5643
00
15
17.1
-56
26
27
12.1
0.38
0.43
0.01
-285
1.15
4.51
0.30
-3.15
-3.00
-2.45
-2.94
§
§
§
HE
0013-0257
00
16
04.2
-02
41
06
13.7
0.70
0.75
0.04
36
2.96
1.24
1.52
-3.37
-3.07
-3.32
-3.21
0.46
HE
0013-0522
00
16
28.1
-05
05
52
13.7
0.64
0.65
0.03
-183
3.56
1.25
2.02
-2.65
-2.65
-2.83
-2.69
0.43
HE
0015-0048
00
18
01.4
01
05
08
14.0
0.64
0.78
0.03
-46
4.84
1.25
3.94
-2.93
-2.38
-2.76
-2.61
0.55
HE
0017-3646
00
20
26.1
-36
30
20
13.6
0.54
0.61
0.01
375
3.88
2.47
0.62
-2.50
-2.30
-2.58
-2.42
§
§
§
*
HE
0017-5616
00
20
11.2
-55
59
37
10.5
0.83
0.64
0.01
30
8.76
0.55
6.03
-0.88
-1.44
-1.12
-1.12
0.05
HE
0025-0223
00
28
28.3
-02
06
42
12.0
0.38
0.42
0.03
3
4.90
5.21
1.49
-1.48
-1.21
-1.57
-1.31
-0.31
HE
0027-1221
00
30
31.0
-12
05
11
13.7
0.59
0.50
0.03
14
2.85
1.71
6.56
-2.40
-2.56
-2.56
-2.56
1.78
*
HE
0030-5441
00
33
20.0
-54
24
43
11.1
0.37
0.42
0.02
0
4.52
5.03
1.30
-1.58
-1.01
-1.70
-1.20
-0.30
HE
0032-4056
00
34
33.7
-40
39
30
13.3
0.42
0.51
0.02
-66
1.63
4.24
0.39
-2.88
-2.69
-2.84
-2.74
§
§
§
HE
0033-2141
00
35
42.1
-21
24
58
12.9
0.64
0.77
0.02
-186
4.04
1.28
1.51
-3.02
-2.55
-3.00
-2.78
-0.01
HE
0033-2153
00
35
52.9
-21
37
09
10.8
0.59
0.62
0.02
7
8.14
1.86
5.26
-1.35
-1.20
-1.22
-1.22
0.04
HE
0035-0834
00
38
31.9
-08
18
26
10.1
0.47
§
§
§
0.04
-78
6.28
3.42
1.76
§
§
§
-1.26
§
§
§
-1.26
-0.53
*
HE
0037-3319
00
39
51.5
-33
03
12
11.5
0.42
§
§
§
0.02
87
4.17
4.13
0.76
§
§
§
-1.76
§
§
§
-1.76
§
§
§
*
HE
0037-4341
00
40
06.8
-43
25
19
13.7
0.75
1.02
0.01
44
6.88
0.77
1.27
§
§
§
-2.19
-2.74
-2.46
-0.95
HE
0038-0345
00
41
09.2
-03
29
00
12.3
0.87
0.79
0.04
10
5.66
0.68
3.85
-2.81
-3.05
-2.53
-2.86
0.30
HE
0038-4234
00
40
56.7
-42
18
09
12.6
0.40
0.46
0.01
49
4.63
4.38
0.99
-1.88
-1.58
-1.79
-1.66
§
§
§
HE
0039-0216
00
41
53.6
-02
00
33
13.8
0.37
0.40
0.03
198
1.63
5.06
0.12
-2.69
-2.50
-2.41
-2.51
§
§
§
HE
0039-2635
00
41
39.7
-26
18
53
13.4
1.00
0.79
0.01
-27
2.22
§
§
§
8.05
-3.56
§
§
§
-3.64
-3.60
2.32
*
HE
0041-1034
00
44
28.9
-10
17
50
11.9
0.82
0.90
0.03
41
7.96
0.68
3.56
-2.13
-1.94
-2.09
-2.03
-0.27
HE
0048-1109
00
51
26.4
-10
53
14
11.6
0.42
0.45
0.03
28
2.21
4.21
0.43
-2.48
-2.40
-2.53
-2.43
§
§
§
HE
0049-0005
00
52
13.5
00
21
35
13.6
0.76
0.85
0.02
-194
5.96
0.88
1.99
-2.65
-2.40
-2.60
-2.51
-0.34
HE
0051-4840
00
53
58.2
-48
24
44
12.2
0.69
0.58
0.01
15
8.26
1.17
5.31
-1.03
-1.57
-1.09
-1.09
0.02
HE
0054-2542
00
57
18.0
-25
26
09
13.5
0.87
0.75
0.02
-226
3.77
0.59
7.70
-3.07
-3.33
-3.05
-3.05
1.51
*
HE
0056-3022
00
58
43.8
-30
05
58
11.5
0.63
0.69
0.02
49
1.95
1.38
1.03
-3.22
-3.00
-3.38
-3.15
0.74
*
HE
0056-3242
00
59
07.8
-32
26
23
11.5
0.70
0.74
0.02
-1182
8.80
1.15
3.93
-1.35
-1.33
-1.41
-1.36
-0.33
HE
0058-3449
01
01
21.6
-34
33
11
13.9
0.76
0.62
0.02
-33
6.05
0.97
5.40
-2.05
-2.36
-1.88
-1.88
0.50
HE
0102-5655
01
04
39.6
-56
39
42
13.9
0.78
0.73
0.02
252
3.98
0.90
0.97
-2.91
-3.14
-2.90
-3.02
§
§
§
HE
0106-0136
01
09
03.2
01
52
28
12.2
0.46
0.45
0.03
-24
4.56
3.70
1.26
-1.76
-1.88
-1.80
-1.85
-0.34

Table
11---Continued
Star
name
R.A.
#
B
(B
-V)
HP2
(B
-V)J-K
E(B-V)
v
rad
KP
HP2
GP
[Fe/H]
B-V
[Fe/H]
HP2
[Fe/H]
Rossi
[Fe/H]
final
[C/Fe]
Redisc.
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
(16)
(17)
HE
0108-0145
01
10
46.2
02
01
15
13.8
0.64
0.57
0.03
-68
7.07
1.34
3.82
-1.58
-1.94
-1.40
-1.71
-0.03
HE
0111-1118
01
14
06.5
-11
02
35
13.0
0.63
0.77
0.03
-103
6.52
1.47
3.26
-2.25
-2.05
-2.19
-2.13
-0.05
*
HE
0112-5703
01
14
19.4
-56
47
55
11.6
0.76
0.66
0.02
53
9.13
0.78
6.08
-0.88
-1.26
-1.09
-1.09
-0.01
HE
0112-5710
01
14
19.8
-56
54
46
13.7
0.50
0.51
0.02
185
2.80
2.97
0.81
-2.40
-2.40
-2.61
-2.43
§
§
§
HE
0113-5554A
01
15
19.8
-55
39
08
12.6
0.52
§
§
§
0.02
16
6.73
2.67
2.57
§
§
§
-1.49
§
§
§
-1.49
-0.30
HE
0113-5554B
01
15
19.8
-55
39
08
12.6
0.60
§
§
§
0.02
58
7.73
1.66
3.81
§
§
§
-1.64
§
§
§
-1.64
-0.17
HE
0117-0201
01
20
29.3
-01
46
16
13.3
0.70
0.69
0.04
33
4.62
1.23
0.94
-2.65
-2.65
-2.59
-2.63
§
§
§
HE
0119-5521
01
21
10.1
-55
05
29
11.8
0.54
0.50
0.02
15
7.65
2.31
4.27
-1.00
-1.18
-0.97
-1.08
-0.05
HE
0122-0245
01
25
01.2
-02
29
32
11.5
0.55
0.47
0.05
16
7.10
2.24
3.99
-0.90
-1.58
-1.05
-1.28
0.00
HE
0123-4204
01
25
33.6
-41
48
35
11.8
0.56
0.84
0.02
-30
7.42
2.12
3.72
-2.19
-1.47
-2.10
-1.81
-0.12
*
HE
0124-0119
01
26
58.6
01
35
15
13.7
0.78
0.95
0.03
-256
4.58
0.78
1.17
-3.08
-2.98
-3.31
-3.09
-0.41
HE
0126-3558
01
29
00.3
-35
43
00
12.2
0.44
0.45
0.02
108
4.54
3.94
1.37
-1.76
-1.76
-1.80
-1.77
-0.27
HE
0129-0015
01
31
45.7
00
30
42
11.9
0.60
0.62
0.02
20
7.67
1.65
4.56
-1.64
-1.64
-1.36
-1.57
0.00
HE
0135-3020
01
37
27.2
-30
05
35
11.3
0.46
§
§
§
0.02
-33
6.68
3.69
2.42
§
§
§
-1.15
§
§
§
-1.15
-0.34
HE
0137-4457
01
40
00.5
-44
42
23
11.7
0.56
0.54
0.02
91
7.97
2.15
3.92
-1.02
-1.19
-1.03
-1.11
-0.19
HE
0139-1157
01
41
38.0
-11
42
18
11.1
0.37
0.46
0.02
-17
4.42
5.28
1.52
-1.96
-1.14
-1.89
-1.38
-0.14
HE
0144-4949
01
46
05.2
-49
34
05
11.2
0.69
0.55
0.03
97
7.86
1.14
5.05
-1.02
-1.85
-1.07
-1.07
0.05
HE
0147-3415
01
49
28.1
-34
01
06
10.6
0.46
0.41
0.02
39
6.42
3.73
2.47
-0.83
-1.26
-1.01
-1.16
-0.26
HE
0147-4606
01
49
37.5
-45
51
23
11.3
0.69
0.73
0.01
50
5.43
1.08
1.02
-2.67
-2.46
-2.42
-2.50
-0.78
HE
0147-4926
01
49
07.9
-49
11
43
12.1
0.69
0.78
0.02
135
5.32
1.00
2.48
-2.85
-2.46
-2.60
-2.59
0.01
HE
0150-5218
01
52
31.3
-52
03
27
13.5
0.56
0.54
0.02
269
3.56
1.98
1.14
-2.34
-2.40
-2.45
-2.40
-0.07
HE
0153-1745
01
56
01.3
-17
30
52
12.2
0.75
0.66
0.02
20
8.60
0.84
5.17
-1.26
-1.54
-1.23
-1.23
-0.06
HE
0201-3142
02
04
07.9
-31
27
57
13.4
0.87
0.88
0.02
116
5.21
0.70
1.93
-3.17
-3.12
-2.91
-3.08
-0.17
HE
0208-4751
02
10
41.8
-47
37
27
11.2
0.71
§
§
§
0.02
33
9.29
1.14
5.93
§
§
§
-1.03
§
§
§
-1.03
-0.05
HE
0212-5812
02
13
42.4
-57
58
56
13.7
0.42
0.39
0.04
175
2.48
4.19
0.63
-2.17
-2.30
-2.22
-2.27
§
§
§
HE
0215-5532
02
16
58.3
-55
18
58
11.2
0.69
0.59
0.04
100
8.36
1.06
5.53
-1.03
-1.57
-1.06
-1.06
0.04
HE
0217-2819
02
20
07.9
-28
05
43
13.7
0.37
0.45
0.01
30
1.05
4.78
0.43
-3.15
-2.91
-2.48
-2.88
§
§
§
HE
0220-5947
02
21
51.2
-59
33
31
13.0
0.70
0.72
0.03
26
4.80
1.22
2.88
-2.69
-2.59
-2.62
-2.62
0.30
HE
0223-2814
02
25
17.0
-28
00
46
13.2
0.42
0.43
0.02
108
1.61
4.22
0.61
-2.75
-2.69
-2.53
-2.67
§
§
§
HE
0228-0149
02
30
55.9
-01
36
02
13.2
0.57
0.49
0.03
111
5.65
1.82
1.95
-1.66
-1.98
-1.59
-1.80
-0.28
HE
0231-2101
02
33
42.2
-20
48
04
13.6
0.70
0.75
0.02
72
4.30
1.07
2.18
-2.96
-2.71
-2.87
-2.81
0.22
HE
0234-4036
02
36
25.8
-40
23
23
12.1
0.46
0.47
0.02
129
6.05
3.68
2.07
-1.36
-1.36
-1.37
-1.36
-0.33
HE
0236-0242
02
39
21.5
-02
29
37
13.4
0.47
0.46
0.03
-70
3.72
3.33
0.98
-2.13
-2.13
-2.10
-2.13
§
§
§
*
HE
0237-2402
02
39
15.9
-23
49
46
12.4
0.75
0.65
0.03
21
7.58
0.98
5.08
-1.77
-2.00
-1.48
-1.48
0.11

Table
11---Continued
Star
name
R.A.
#
B
(B
-V)
HP2
(B
-V)J-K
E(B-V)
v
rad
KP
HP2
GP
[Fe/H]
B-V
[Fe/H]
HP2
[Fe/H]
Rossi
[Fe/H]
final
[C/Fe]
Redisc.
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
(16)
(17)
HE
0239-3236
02
41
22.6
-32
24
12
12.9
0.70
0.80
0.02
8
4.87
1.07
2.47
-3.02
-2.59
-2.80
-2.75
0.14
HE
0240-0009f
02
43
26.5
00
03
18
11.3
0.69
§
§
§
0.03
-40
8.14
1.23
5.44
§
§
§
-1.72
§
§
§
-1.72
0.07
HE
0241-0205
02
43
58.3
02
17
50
14.2
0.63
0.72
0.04
223
6.22
1.34
3.11
-2.41
-2.14
-2.15
-2.21
-0.02
HE
0242-5211
02
44
14.8
-51
58
22
12.4
0.59
0.74
0.03
31
4.24
1.50
1.72
-2.95
-2.40
-2.87
-2.65
0.03
HE
0243-0203
02
46
29.6
02
15
48
14.0
0.54
0.49
0.05
7
3.92
2.39
1.38
-2.15
-2.30
-2.16
-2.23
-0.04
HE
0247-0254
02
50
16.9
-02
41
50
14.0
0.50
0.46
0.05
-62
4.91
2.94
5.27
-1.80
-1.99
-1.73
-1.73
0.78
HE
0247-0533
02
50
10.1
-05
21
07
13.1
0.69
0.81
0.04
-14
5.57
1.21
3.46
-2.90
-2.41
-2.60
-2.58
0.23
HE
0249-4821
02
51
40.5
-48
08
45
11.4
0.87
0.97
0.03
120
5.63
0.62
1.25
-2.87
-3.05
-3.00
-2.99
-0.66
HE
0250-5421
02
52
01.8
-54
09
01
10.2
0.75
0.85
0.02
127
7.98
0.95
4.48
-2.07
-1.90
-1.96
-1.96
-0.07
HE
0255-2744
02
57
23.6
-27
32
15
10.1
0.44
0.49
0.02
5
5.97
3.89
2.45
-1.58
-1.29
-1.49
-1.36
-0.16
HE
0256-1150
02
58
50.2
-11
38
34
12.1
0.69
0.76
0.05
167
6.51
1.23
4.02
-2.25
-2.22
-2.17
-2.21
0.13
HE
0302-3417
03
04
28.6
-34
06
06
11.4
0.70
0.89
0.02
152
4.03
1.07
1.10
-3.33
-2.77
-3.34
-3.05
-0.28
HE
0304-2518
03
06
49.4
-25
06
41
12.9
0.42
0.48
0.02
212
3.15
4.02
0.67
-2.30
-2.04
-2.39
-2.13
§
§
§
HE
0306-2446
03
08
45.9
-24
35
27
13.6
0.57
0.61
0.02
-85
6.29
1.93
1.44
-2.01
-1.81
-1.79
-1.85
-0.70
HE
0311-1046
03
14
20.9
-10
35
10
13.5
0.70
0.75
0.07
292
1.94
1.01
0.70
-3.56
-3.22
-3.58
-3.39
§
§
§
*
HE
0315-1528
03
17
36.1
-15
17
23
13.9
0.87
0.70
0.06
132
4.67
0.67
2.09
-2.65
-3.19
-2.60
-2.91
0.06
*
HE
0315-1642
03
17
53.3
-16
32
02
14.7
0.54
0.49
0.05
-69
7.72
2.39
3.15
-0.84
-1.18
-0.91
-1.03
-0.33
HE
0315-1749
03
18
05.8
-17
38
14
10.7
0.42
0.45
0.03
61
2.45
4.15
0.69
-2.39
-2.30
-2.48
-2.34
§
§
§
HE
0317-1324
03
19
27.1
-13
13
33
12.6
0.49
0.44
0.06
82
6.01
3.06
2.37
-1.18
-1.51
-1.27
-1.42
-0.21
HE
0317-3301
03
19
35.3
-32
50
41
11.5
0.37
0.41
0.01
43
1.07
4.83
0.21
-3.08
-2.91
-2.35
-2.85
§
§
§
*
HE
0324-0122
03
27
02.3
01
32
33
12.8
0.69
0.69
0.10
122
5.86
1.20
3.28
-2.46
-2.37
-2.18
-2.36
0.11
HE
0324-0152
03
26
53.8
02
02
28
12.6
0.59
0.79
0.11
53
3.41
1.51
1.65
-3.35
-2.49
-3.28
-2.92
0.32
HE
0327-1205
03
29
33.4
-11
54
58
11.6
0.44
§
§
§
0.07
19
6.07
3.87
2.54
§
§
§
-1.18
§
§
§
-1.18
-0.16
HE
0327-1517
03
29
47.0
-15
06
46
12.4
0.63
0.69
0.09
325
5.61
1.47
2.39
-2.41
-2.19
-2.25
-2.26
-0.10
HE
0329-3041
03
31
20.8
-30
30
58
10.2
0.60
0.68
0.02
17
7.61
1.54
4.32
-1.93
-1.64
-1.58
-1.70
-0.04
HE
0333-0130
03
36
02.4
01
40
52
12.6
0.43
0.39
0.12
-64
6.27
4.21
1.79
-0.83
-1.07
-0.99
-1.03
-0.51
HE
0336-2412
03
38
41.4
-24
02
48
10.2
0.64
0.74
0.02
70
4.04
1.42
2.01
-2.95
-2.55
-2.91
-2.74
0.24
*
HE
0340-0825
03
43
13.2
-08
15
37
12.3
0.44
0.41
0.06
42
6.44
3.81
2.38
-0.83
-1.07
-1.00
-1.02
-0.30
HE
0340-3056
03
42
58.1
-30
47
20
11.7
0.54
0.65
0.01
334
4.08
2.42
0.79
-2.55
-2.26
-2.65
-2.43
§
§
§
HE
0349-0725
03
51
39.1
-07
16
48
13.0
0.59
0.55
0.08
305
4.37
1.73
1.62
-2.29
-2.37
-2.22
-2.31
-0.06
HE
0355-5847
03
56
37.2
-58
38
29
13.3
0.75
1.10
0.03
153
6.97
0.89
1.90
§
§
§
-2.19
-2.89
-2.54
-0.61
HE
0356-6110
03
57
02.8
-61
02
09
12.7
0.40
0.41
0.03
115
2.64
4.26
0.53
-2.20
-2.20
-2.27
-2.21
§
§
§
*
HE
0359-2643
04
01
21.9
-26
35
05
11.4
0.69
0.82
0.03
22
7.61
1.12
4.63
-2.05
-1.93
-1.98
-1.97
0.03
HE
0402-3127
04
04
29.2
-31
19
04
12.1
0.61
0.70
0.02
169
8.05
1.56
2.17
-1.72
-1.35
-1.52
-1.48
-0.71

Table
11---Continued
Star
name
R.A.
#
B
(B
-V)
HP2
(B
-V)J-K
E(B-V)
v
rad
KP
HP2
GP
[Fe/H]
B-V
[Fe/H]
HP2
[Fe/H]
Rossi
[Fe/H]
final
[C/Fe]
Redisc.
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
(16)
(17)
HE
0403-2942
04
05
55.5
-29
33
59
13.4
0.60
0.67
0.01
145
6.18
1.55
1.65
-2.23
-1.96
-2.01
-2.04
-0.56
HE
0409-1212f
04
12
13.7
-12
05
04
11.4
0.78
0.54
0.05
67
4.31
0.91
1.92
-2.21
-3.03
-2.20
-2.62
0.10
*
HE
0411-3558
04
13
09.0
-35
50
39
13.5
0.40
0.47
0.01
184
1.27
4.42
0.21
-2.98
-2.87
-2.66
-2.86
§
§
§
*
HE
0412-0138
04
15
33.5
01
45
57
11.4
0.75
0.59
0.13
27
7.20
0.77
5.24
-1.84
-2.14
-1.43
-1.51
0.21
HE
0413-4831
04
14
41.3
-48
24
08
11.9
0.46
0.50
0.02
80
4.65
3.56
1.06
-2.06
-1.88
-1.96
-1.92
-0.53
HE
0414-0343
04
17
16.4
-03
36
31
12.7
1.00
0.93
0.04
-36
5.70
§
§
§
7.47
-2.86
§
§
§
-2.88
-2.87
0.87
HE
0417-0222
04
19
50.5
02
29
19
11.4
0.46
0.35
0.13
71
4.50
3.53
1.31
-1.01
-1.88
-1.42
-1.69
-0.29
HE
0420-0123
04
23
14.4
01
30
49
12.3
0.70
0.75
0.14
-34
4.31
1.07
2.91
-2.96
-2.71
-2.86
-2.83
0.46
HE
0420-0140
04
23
25.3
01
47
37
11.2
0.41
0.39
0.13
19
5.95
4.28
1.81
-1.06
-1.06
-1.07
-1.07
-0.42
HE
0427-2301
04
29
29.8
-22
55
22
12.0
0.75
0.91
0.04
262
8.53
0.87
3.93
-1.83
-1.54
-1.96
-1.72
-0.28
HE
0428-1340
04
30
51.4
-13
34
04
10.5
0.57
0.57
0.12
-162
5.49
1.86
1.67
-2.12
-2.04
-1.90
-2.05
-0.37
HE
0429-4620
04
30
48.6
-46
13
53
13.8
0.64
0.65
0.01
120
4.83
1.31
2.50
-2.38
-2.38
-2.38
-2.38
0.16
HE
0432-1005
04
35
01.2
-09
59
36
14.1
0.70
0.77
0.06
263
4.78
1.13
2.80
-2.86
-2.59
-2.76
-2.70
0.28
HE
0432-5107
04
33
44.4
-51
00
59
11.0
0.38
0.41
0.01
48
5.42
5.07
1.61
-1.28
-0.97
-1.34
-1.07
-0.39
HE
0433-1008
04
35
35.8
-10
02
02
14.5
0.78
0.87
0.07
53
4.95
0.83
1.33
-3.15
-2.93
-2.98
-3.00
-0.42
HE
0440-1049
04
42
39.6
-10
43
24
13.4
0.49
0.48
0.11
93
1.99
3.21
0.39
-2.73
-2.70
-2.70
-2.72
§
§
§
HE
0440-3426
04
42
08.1
-34
21
13
12.8
1.00
0.95
0.02
355
5.77
§
§
§
7.90
-2.82
§
§
§
-2.92
-2.87
0.90
HE
0442-1946
04
45
01.9
-19
40
60
10.5
0.38
0.40
0.04
36
4.98
5.07
1.41
-1.48
-1.21
-1.47
-1.29
-0.38
HE
0444-3314
04
46
25.8
-33
09
13
11.7
0.47
§
§
§
0.02
269
3.88
3.34
1.50
§
§
§
-2.08
§
§
§
-2.08
0.05
HE
0445-4614
04
46
57.2
-46
09
16
13.5
0.70
0.78
0.01
53
4.93
1.03
0.61
-2.93
-2.59
-2.74
-2.71
§
§
§
HE
0448-4806
04
49
33.0
-48
01
08
13.2
0.56
0.54
0.01
126
2.82
1.86
6.73
-2.45
-2.51
-2.70
-2.70
1.82
HE
0448-5701
04
49
18.0
-56
56
20
13.9
0.76
0.79
0.01
84
6.45
0.99
3.87
-2.33
-2.29
-2.25
-2.29
0.11
HE
0452-2958
04
54
07.8
-29
53
27
10.7
0.75
0.61
0.01
-4
8.69
0.98
4.98
-0.99
-1.54
-1.06
-1.28
-0.11
HE
0453-5638
04
54
43.2
-56
33
33
11.4
0.60
0.60
0.01
-12
7.48
1.68
5.62
-1.75
-1.75
-1.38
-1.38
0.22
HE
0503-5210
05
05
07.6
-52
06
18
13.8
0.47
0.49
0.02
106
4.84
3.41
1.40
-1.90
-1.80
-1.86
-1.82
-0.34
HE
0505-2806
05
07
20.1
-28
02
26
11.9
0.40
0.51
0.02
45
0.78
4.47
1.84
-3.49
-3.32
-2.47
-3.22
2.60
HE
0508-4421
05
09
52.4
-44
17
20
11.7
0.39
0.44
0.02
-29
4.58
4.58
4.58
-1.76
-1.34
-1.73
-1.73
0.77
HE
0508-4426
05
09
47.5
-44
23
16
12.0
0.50
0.53
0.02
-77
3.67
2.89
1.82
-2.34
-2.26
-2.40
-2.29
0.30
HE
0527-3931f
05
29
13.7
-39
28
50
11.9
0.58
§
§
§
0.02
11
7.68
1.93
3.99
§
§
§
-1.50
§
§
§
-1.50
-0.11
HE
0533-3858
05
35
19.2
-38
56
17
13.8
0.63
0.65
0.04
398
5.42
1.26
2.95
-2.24
-2.24
-2.18
-2.23
0.14
HE
0543-5350
05
44
41.8
-53
49
06
12.5
0.46
0.43
0.08
245
2.85
3.52
1.19
-2.22
-2.29
-2.30
-2.28
0.30
HE
0852-0139
08
55
17.8
01
28
20
11.8
0.70
0.60
0.04
-4
8.66
1.07
6.17
-0.99
-1.48
-1.03
-1.03
0.08
HE
0900-0001
09
02
41.3
-00
13
34
13.0
0.42
0.33
0.04
27
3.59
4.10
1.03
-1.15
-1.90
-1.62
-1.75
-0.17
HE
0920-0506
09
23
06.0
-05
19
33
12.3
0.65
0.57
0.03
41
8.36
1.37
5.88
-0.85
-1.34
-1.01
-1.01
0.09

Table
11---Continued
Star
name
R.A.
#
B
(B
-V)
HP2
(B
-V)J-K
E(B-V)
v
rad
KP
HP2
GP
[Fe/H]
B-V
[Fe/H]
HP2
[Fe/H]
Rossi
[Fe/H]
final
[C/Fe]
Redisc.
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
(16)
(17)
HE
0926-0508
09
28
55.2
-05
21
39
12.7
0.38
0.47
0.04
191
1.39
4.64
0.26
-2.98
-2.79
-2.67
-2.80
§
§
§
*
HE
0938-0114
09
40
43.0
01
00
37
10.9
0.37
§
§
§
0.10
-58
1.39
4.86
0.12
§
§
§
-2.70
§
§
§
-2.70
§
§
§
*
HE
0959-1714
10
01
41.0
-17
28
54
12.9
0.63
0.75
0.04
77
5.73
1.26
2.94
-2.72
-2.19
-2.38
-2.37
0.05
HE
1005-0739
10
08
13.4
-07
54
08
13.5
0.42
0.43
0.04
54
2.44
4.08
0.24
-2.39
-2.30
-2.40
-2.33
§
§
§
HE
1008-0938
10
11
22.8
-09
53
20
10.8
0.65
0.64
0.05
40
8.72
1.44
4.83
-1.10
-1.10
-1.13
-1.11
-0.14
HE
1010-1016
10
12
29.3
-10
31
30
12.2
0.54
0.50
0.05
13
6.71
2.31
2.14
-1.49
-1.62
-1.28
-1.50
-0.46
HE
1031-1250
10
34
05.0
-13
05
43
11.4
0.57
0.45
0.05
16
7.34
1.95
4.57
-0.59
-1.47
-0.88
-1.10
0.07
HE
1051-1331
10
54
09.8
-13
47
52
13.6
0.87
0.92
0.05
207
4.37
0.61
1.13
-3.10
-3.23
-3.31
-3.22
-0.38
HE
1052-1852
10
55
06.2
-19
08
36
13.7
0.87
0.85
0.04
33
3.83
0.66
0.12
-3.33
-3.33
-3.32
-3.33
§
§
§
HE
1052-2139
10
55
12.0
-21
55
52
13.6
0.78
0.79
0.07
293
4.48
0.84
2.56
-3.03
-3.03
-2.93
-3.00
0.30
HE
1052-2548
10
55
20.6
-26
04
47
§
§
§
0.40
0.40
0.07
183
1.86
4.46
0.32
-2.54
-2.54
-2.40
-2.52
§
§
§
HE
1109-0025
11
12
06.7
-00
41
32
§
§
§
0.38
0.38
0.04
74
4.75
4.76
1.73
-1.21
-1.21
-1.44
-1.25
-0.13
HE
1116-0634
11
18
35.8
-06
50
46
12.6
0.78
0.90
0.06
133
2.67
0.90
1.21
-3.62
-3.32
-3.81
-3.52
0.41
HE
1119-0218
11
22
26.9
02
02
10
§
§
§
0.42
0.40
0.04
-10
4.32
4.23
1.41
-1.67
-1.67
-1.68
-1.67
-0.17
HE
1120-0153
11
22
43.2
-02
09
36
§
§
§
0.42
0.40
0.08
242
1.49
4.17
0.44
-2.79
-2.87
-2.40
-2.79
§
§
§
HE
1122-2126
11
24
39.8
-21
43
17
12.0
0.56
0.60
0.04
133
7.78
2.06
2.37
-1.52
-1.19
-1.28
-1.29
-0.59
HE
1130-0147
11
32
56.4
-02
04
18
§
§
§
0.55
0.62
0.03
-11
8.01
2.28
3.82
-1.35
-0.84
-1.27
-1.08
-0.22
HE
1130-2801
11
33
05.3
-28
17
41
13.5
0.46
0.48
0.07
116
4.19
3.53
0.95
-2.09
-2.02
-2.04
-2.03
§
§
§
HE
1143-0114
11
46
31.7
00
57
30
§
§
§
0.47
0.44
0.02
177
2.70
3.32
4.57
-2.30
-2.37
-2.37
-2.37
1.54
HE
1144-1349
11
46
50.6
-14
06
39
§
§
§
0.38
0.40
0.05
159
1.41
4.69
0.44
-2.87
-2.79
-2.43
-2.75
§
§
§
*
HE
1154-2951
11
56
39.4
-30
08
32
10.9
0.42
0.44
0.06
-30
3.46
4.14
2.46
-2.10
-1.97
-2.14
-2.02
0.64
HE
1158-2313
12
01
12.2
-23
30
36
11.6
0.76
0.93
0.05
274
5.76
0.92
2.54
-2.81
-2.40
-2.86
-2.62
-0.08
HE
1207-3113
12
10
00.7
-31
30
35
11.8
0.75
0.85
0.06
314
7.15
0.94
2.99
-2.34
-2.14
-2.22
-2.21
-0.26
HE
1208-0040
12
10
55.9
00
23
60
§
§
§
0.49
§
§
§
0.03
112
3.70
3.15
0.62
§
§
§
-2.19
§
§
§
-2.19
§
§
§
*
HE
1209-2021
12
11
53.0
-20
38
20
§
§
§
0.63
0.70
0.06
59
6.54
1.30
0.00
-2.22
-2.05
-1.99
-2.08
§
§
§
HE
1210-2729
12
13
07.9
-27
45
50
13.4
0.69
0.81
0.07
-118
5.33
1.05
1.66
-2.94
-2.46
-2.68
-2.63
-0.33
HE
1213-0247
12
16
12.0
02
31
05
§
§
§
0.47
0.52
0.02
55
1.64
3.49
0.27
-2.88
-2.81
-2.87
-2.83
§
§
§
HE
1214-2704
12
17
09.1
-27
21
03
12.9
0.70
0.77
0.07
267
4.62
1.20
2.50
-2.91
-2.65
-2.83
-2.76
0.23
HE
1216-1554
12
18
46.6
-16
10
52
12.8
0.78
0.89
0.04
291
3.67
0.82
0.87
-3.44
-3.21
-3.47
-3.33
§
§
§
HE
1220-3159
12
22
51.6
-32
16
16
10.9
0.90
0.62
0.08
-45
8.87
0.30
6.04
-0.70
-1.69
-1.03
-1.03
0.03
HE
1223-0133
12
25
35.0
01
17
09
§
§
§
0.47
§
§
§
0.02
116
4.44
3.47
1.16
§
§
§
-1.96
§
§
§
-1.96
-0.38
*
HE
1224-1741
12
27
11.5
-17
58
20
§
§
§
0.54
0.56
0.05
59
3.15
2.48
0.52
-2.46
-2.41
-2.67
-2.49
§
§
§
HE
1224-3025
12
26
46.6
-30
41
52
11.1
0.38
0.41
0.08
-78
4.77
5.23
1.59
-1.48
-1.21
-1.56
-1.30
-0.21
HE
1225-0155
12
28
04.8
01
38
32
§
§
§
0.77
0.85
0.02
56
5.50
0.94
3.60
-3.05
-2.72
-2.75
-2.81
0.29

Table
11---Continued
Star
name
R.A.
#
B
(B
-V)
HP2
(B
-V)J-K
E(B-V)
v
rad
KP
HP2
GP
[Fe/H]
B-V
[Fe/H]
HP2
[Fe/H]
Rossi
[Fe/H]
final
[C/Fe]
Redisc.
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
(16)
(17)
HE
1226-0010
12
29
01.0
-00
05
42
§
§
§
0.40
0.38
0.02
84
2.90
4.33
0.32
-1.96
-2.12
-2.07
-2.09
§
§
§
HE
1228-2420
12
30
51.1
-24
36
37
12.1
0.42
0.46
0.09
-28
2.43
4.00
0.47
-2.45
-2.30
-2.52
-2.36
§
§
§
HE
1233-3114
12
35
50.2
-31
31
11
11.5
0.76
0.78
0.08
164
6.36
0.83
4.34
-2.33
-2.29
-2.28
-2.30
0.24
HE
1237-0316
12
39
53.0
-03
32
29
§
§
§
0.44
0.46
0.03
37
3.11
3.91
0.65
-2.24
-2.16
-2.31
-2.19
§
§
§
HE
1239-0840
12
41
55.0
-08
56
59
12.1
0.39
0.42
0.03
50
3.49
4.67
0.59
-1.97
-1.78
-2.04
-1.85
§
§
§
HE
1240-1258
12
42
44.9
-13
15
02
§
§
§
0.47
0.49
0.06
-8
4.53
3.35
1.31
-1.97
-1.88
-1.94
-1.90
-0.30
HE
1243-2408
12
45
54.2
-24
25
02
10.8
0.70
0.82
0.10
130
4.63
1.11
2.23
-3.19
-2.65
-2.95
-2.88
0.13
HE
1252-0511
12
55
10.6
-05
27
32
§
§
§
0.44
0.41
0.03
342
3.57
3.80
0.79
-1.90
-2.04
-1.98
-2.01
§
§
§
*
HE
1304-0651
13
06
55.0
-07
07
49
§
§
§
0.63
0.65
0.04
-16
5.63
1.42
2.31
-2.19
-2.19
-2.12
-2.17
-0.13
HE
1311-0131
13
13
42.0
-01
47
16
§
§
§
0.70
0.80
0.03
116
4.14
1.23
2.27
-3.16
-2.77
-3.05
-2.94
0.31
HE
1313-1916
13
15
46.3
-19
32
34
12.3
0.86
0.91
0.09
199
5.98
0.59
5.14
-2.73
-2.65
-2.73
-2.73
0.47
HE
1316-1236
13
19
20.2
-12
52
04
10.6
0.38
0.36
0.05
-68
4.34
4.87
1.17
-1.14
-1.45
-1.50
-1.41
-0.34
HE
1317-0407
13
19
47.0
-04
23
10
§
§
§
0.69
0.84
0.04
-36
5.49
1.05
1.22
-3.02
-2.46
-2.71
-2.66
-0.65
HE
1320-1339
13
22
44.2
-13
55
31
11.3
0.70
0.79
0.07
111
4.69
1.05
0.89
-2.98
-2.65
-2.86
-2.79
§
§
§
HE
1321-1750
13
24
14.4
-18
06
21
12.3
0.76
0.77
0.10
-110
6.20
0.89
3.41
-2.38
-2.36
-2.27
-2.36
0.06
HE
1323-1732
13
25
45.6
-17
47
54
11.7
0.82
0.84
0.10
-40
8.24
0.54
2.59
-1.87
-1.83
-1.86
-1.85
-0.60
HE
1327-2116
13
30
19.4
-21
32
03
12.6
1.00
0.78
0.10
139
4.92
§
§
§
7.68
-3.02
§
§
§
-2.75
-2.93
1.11
HE
1327-2326
13
30
06.0
-23
41
51
13.9
0.42
0.49
0.08
112
0.16
4.01
0.53
-4.43
-4.30
1.12
-4.33
§
§
§
HE
1337-0012
13
40
02.6
-00
02
18
§
§
§
0.38
0.44
0.03
7
0.85
4.70
0.07
-3.38
-3.24
-2.30
-3.12
§
§
§
*
HE
1340-2343
13
43
19.4
-23
58
13
12.4
0.76
0.82
0.06
-64
5.86
0.76
3.47
-2.51
-2.40
-2.53
-2.46
0.16
HE
1348-0135
13
50
35.0
01
20
20
§
§
§
0.59
0.66
0.03
-9
4.41
1.51
1.72
-2.61
-2.37
-2.55
-2.48
-0.03
HE
1352-2031
13
54
59.5
-20
46
34
13.1
0.49
0.50
0.08
-180
4.66
3.07
1.10
-2.06
-1.97
-1.93
-1.98
-0.49
HE
1358-2914
14
01
50.6
-29
28
30
10.8
1.00
0.76
0.06
-113
8.75
0.04
5.68
-1.40
§
§
§
-1.49
-1.40
-0.00
HE
1401-0010
14
04
03.4
-00
24
25
§
§
§
0.37
0.42
0.05
396
1.58
5.07
0.35
-2.69
-2.50
-2.51
-2.53
§
§
§
HE
1401-0400
14
03
50.4
-04
14
49
10.9
0.60
0.57
0.04
-11
7.77
1.60
4.27
-1.19
-1.52
-1.17
-1.35
-0.07
HE
1403-2207
14
06
41.3
-22
21
20
9.1
0.38
§
§
§
0.08
2
4.74
4.90
1.40
§
§
§
-1.34
§
§
§
-1.34
-0.31
HE
1412-0847
14
14
57.4
-09
01
45
13.4
0.57
0.44
0.04
36
4.79
1.97
5.86
-1.66
-2.18
-1.66
-1.66
0.92
HE
1426-0518
14
29
11.3
-05
31
29
12.0
0.61
0.50
0.05
-95
8.12
1.63
4.11
-0.68
-1.35
-0.85
-1.06
-0.17
HE
1428-0307
14
31
34.6
-03
20
34
13.1
0.46
0.43
0.09
-101
4.22
3.63
1.45
-1.92
-2.02
-1.84
-1.98
-0.10
HE
1429-0325
14
32
27.8
-03
38
56
12.3
0.54
0.57
0.10
-114
7.94
2.39
3.88
-1.19
-1.02
-1.12
-1.09
-0.19
HE
1429-0347
14
32
26.2
-04
00
31
14.3
0.64
0.71
0.11
-216
4.45
1.29
3.00
-2.89
-2.50
-2.69
-2.66
0.44
HE
1431-1227
14
33
55.9
-12
40
36
§
§
§
0.76
0.96
0.08
65
6.09
0.91
1.74
-2.76
-2.36
-2.84
-2.58
-0.49
HE
1431-1911
14
34
32.6
-19
24
55
§
§
§
0.69
0.69
0.09
63
6.04
1.22
2.81
-2.34
-2.34
-2.12
-2.28
-0.07
HE
1431-2134
14
34
45.8
-21
47
42
§
§
§
0.40
0.42
0.10
151
3.69
4.32
0.57
-1.90
-1.90
-1.96
-1.91
§
§
§

Table
11---Continued
Star
name
R.A.
#
B
(B
-V)
HP2
(B
-V)J-K
E(B-V)
v
rad
KP
HP2
GP
[Fe/H]
B-V
[Fe/H]
HP2
[Fe/H]
Rossi
[Fe/H]
final
[C/Fe]
Redisc.
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
(16)
(17)
HE
1442-0848
14
45
07.9
-09
00
41
§
§
§
0.47
0.44
0.08
-167
6.69
3.28
2.32
-0.95
-1.15
-1.04
-1.10
-0.38
HE
1448-1125
14
50
52.6
-11
37
21
§
§
§
0.63
0.72
0.10
81
6.06
1.48
1.15
-2.36
-2.14
-2.20
-2.23
-0.84
HE
1450-0207
14
52
58.8
01
55
43
11.7
0.82
0.88
0.05
-317
8.15
0.60
0.00
-1.95
-1.83
-1.97
-1.90
§
§
§
HE
1457-1215
15
00
31.2
-12
26
56
10.7
0.54
0.47
0.07
-6
7.23
2.37
4.57
-0.90
-1.43
-1.00
-1.19
0.09
*
HE
1503-0633
15
06
16.1
-06
45
04
13.2
0.65
0.66
0.08
-51
8.65
1.45
5.21
-1.26
-1.10
-1.20
-1.20
-0.06
HE
1521-0138
15
24
23.0
01
27
28
12.1
0.64
0.64
0.06
-32
7.79
1.33
3.93
-1.66
-1.66
-1.40
-1.59
-0.15
HE
1523-0901
15
26
01.2
-09
11
38
12.2
0.86
0.85
0.14
-221
5.80
0.69
1.90
-2.73
-2.65
-2.63
-2.69
-0.34
HE
2002-5843
20
07
03.8
-58
34
57
13.8
0.64
0.75
0.04
254
4.15
1.26
2.01
-3.02
-2.55
-2.91
-2.76
0.20
*
HE
2119-4653
21
22
45.8
-46
41
03
13.6
0.77
0.88
0.03
-91
5.58
0.97
1.89
-3.10
-2.72
-2.78
-2.83
-0.29
*
HE
2123-0329
21
26
08.9
-03
16
58
14.6
0.78
0.74
0.08
-194
4.34
0.83
2.46
-2.89
-3.03
-2.83
-2.94
0.31
HE
2137-1240
21
40
23.0
-12
27
04
11.8
0.78
0.81
0.05
-90
4.52
0.86
2.61
-3.06
-2.98
-2.96
-2.99
0.30
HE
2138-0314
21
40
41.5
-03
01
17
14.1
0.63
0.66
0.05
-330
3.00
1.42
2.60
-2.88
-2.77
-3.03
-2.86
0.90
HE
2138-1526
21
41
26.4
-15
12
45
12.4
0.42
0.44
0.06
-39
2.54
4.24
0.85
-2.30
-2.20
-2.42
-2.25
§
§
§
*
HE
2153-1503
21
55
45.1
-14
49
08
13.7
0.39
0.46
0.05
22
1.88
4.56
0.67
-2.65
-2.44
-2.62
-2.50
§
§
§
*
HE
2155-2043
21
58
42.2
-20
29
15
14.1
0.87
0.75
0.03
-60
2.45
0.70
3.93
-3.33
-3.70
-3.45
-3.55
1.56
HE
2159-0551
22
02
16.3
-05
36
48
13.3
0.78
0.90
0.05
-92
4.97
0.82
1.97
-3.21
-2.93
-3.05
-3.03
-0.08
HE
2201-0825
22
04
31.9
-08
10
39
11.8
0.50
§
§
§
0.03
-101
4.25
2.94
1.29
§
§
§
-2.12
§
§
§
-2.12
-0.22
HE
2201-4043
22
04
03.6
-40
29
19
11.9
0.78
0.70
0.02
10
4.89
0.93
2.69
-2.59
-2.93
-2.51
-2.74
0.21
HE
2208-0240
22
10
59.8
-02
25
24
13.6
0.63
0.74
0.09
-178
6.75
1.31
3.50
-2.21
-2.00
-2.03
-2.06
-0.04
HE
2208-1239
22
10
53.3
-12
24
27
12.5
0.70
0.72
0.04
-6
4.21
1.18
5.99
-2.86
-2.77
-2.80
-2.80
1.12
HE
2210-4058
22
13
29.0
-40
43
31
13.6
0.37
0.49
0.01
34
1.60
4.89
0.43
-2.84
-2.50
-2.76
-2.59
§
§
§
*
HE
2214-1654
22
17
01.7
-16
39
26
13.9
0.70
0.76
0.03
37
3.52
1.10
5.02
-3.13
-2.87
-3.17
-3.17
1.24
*
HE
2215-3842
22
18
20.9
-38
27
55
14.0
0.63
0.67
0.01
260
5.96
1.34
3.43
-2.28
-2.19
-2.07
-2.18
0.13
HE
2220-4840
22
23
23.5
-48
24
51
11.8
0.63
0.70
0.01
-94
3.18
1.39
1.86
-2.99
-2.77
-3.11
-2.91
0.53
HE
2226-1529
22
29
17.3
-15
13
53
13.0
0.77
0.77
0.04
-77
5.65
0.99
1.56
-2.72
-2.72
-2.47
-2.66
-0.48
HE
2229-4758
22
32
37.9
-47
42
43
11.2
0.59
0.54
0.01
2
8.08
1.93
4.64
-0.84
-1.20
-1.00
-1.06
-0.06
HE
2230-0039
22
33
04.6
00
54
53
11.9
0.50
0.50
0.09
87
7.21
2.88
3.19
-1.28
-1.28
-1.10
-1.06
-0.22
HE
2234-0031
22
36
40.8
-00
16
09
§
§
§
0.70
0.90
0.05
-190
8.79
1.00
3.16
-1.60
-1.33
-1.86
-1.53
-0.52
HE
2234-4757
22
37
20.4
-47
41
38
13.3
0.86
0.92
0.01
-93
5.84
0.56
2.93
-2.78
-2.65
-2.80
-2.72
0.02
HE
2235-5058
22
38
07.9
-50
42
42
13.8
0.78
0.74
0.01
82
4.15
0.81
7.62
-2.95
-3.09
-2.90
-2.90
1.35
HE
2237-0217
22
40
06.0
02
33
39
§
§
§
0.46
0.47
0.08
-52
3.32
3.62
1.03
-2.19
-2.19
-2.28
-2.20
-0.05
HE
2238-6117
22
41
33.6
-61
01
41
12.6
0.40
0.42
0.02
149
2.88
4.42
0.50
-2.12
-2.12
-2.22
-2.14
§
§
§
HE
2242-0324
22
44
40.3
-03
08
32
10.9
0.56
0.55
0.04
48
7.93
2.20
4.27
-1.19
-1.19
-1.08
-1.16
-0.10
HE
2243-0052
22
45
56.9
-00
36
48
§
§
§
0.63
0.60
0.07
-1
6.80
1.45
4.49
-1.91
-2.00
-1.57
-1.87
0.17

Table
11---Continued
Star
name
R.A.
#
B
(B
-V)
HP2
(B
-V)J-K
E(B-V)
v
rad
KP
HP2
GP
[Fe/H]
B-V
[Fe/H]
HP2
[Fe/H]
Rossi
[Fe/H]
final
[C/Fe]
Redisc.
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
(16)
(17)
HE
2243-0244
22
46
17.5
-02
28
59
11.5
0.59
0.63
0.05
46
4.05
1.53
1.02
-2.55
-2.40
-2.59
-2.48
-0.35
HE
2247-4113
22
50
14.2
-40
57
41
10.9
0.52
0.56
0.01
272
3.96
2.65
0.88
-2.36
-2.22
-2.40
-2.27
§
§
§
*
HE
2250-1129
22
53
14.2
-11
13
12
11.5
0.54
0.58
0.04
-55
6.88
2.27
2.53
-1.80
-1.53
-1.50
-1.59
-0.35
HE
2250-4229
22
53
39.6
-42
13
03
13.2
0.70
0.73
0.01
4
4.46
1.16
4.46
-2.89
-2.71
-2.75
-2.77
0.78
HE
2253-1832
22
56
21.8
-18
16
33
11.7
0.46
0.38
0.03
45
6.60
3.72
2.31
-0.47
-1.15
-0.84
-1.00
-0.36
HE
2253-5529
22
56
51.4
-55
13
56
11.1
0.44
0.42
0.02
33
5.78
3.98
1.51
-1.06
-1.29
-1.26
-1.25
-0.54
HE
2259-1502
23
01
55.2
-14
45
59
14.0
0.63
0.75
0.04
-173
5.87
1.44
1.34
-2.40
-2.19
-2.33
-2.28
-0.67
HE
2300-1556
23
03
18.0
-15
40
19
11.9
0.47
0.53
0.03
-223
4.10
3.48
0.88
-2.26
-2.02
-2.26
-2.09
§
§
§
HE
2300-5939
23
03
26.6
-59
23
40
12.6
0.60
0.68
0.02
212
7.78
1.69
4.10
-1.85
-1.52
-1.54
-1.61
-0.11
HE
2301-0248
23
03
58.6
-02
32
30
13.6
0.49
0.43
0.06
-109
3.98
3.12
1.23
-1.98
-2.15
-1.91
-2.09
-0.17
*
HE
2302-2154
23
05
25.2
-21
38
07
13.1
0.70
0.79
0.03
48
1.87
1.21
0.61
-3.68
-3.22
-3.69
-3.45
§
§
§
HE
2302-4259
23
04
49.2
-42
43
48
13.8
0.87
0.98
0.01
-267
4.95
0.74
1.29
-3.03
-3.15
-3.26
-3.15
-0.44
HE
2303-5756
23
06
55.2
-57
40
32
13.8
0.44
0.47
0.02
-74
1.28
3.89
0.01
-2.98
-2.94
-2.67
-2.91
§
§
§
HE
2303-6123
23
06
09.8
-61
07
36
12.0
0.76
0.94
0.02
104
9.03
0.86
3.80
-1.56
-1.26
-1.88
-1.49
-0.40
HE
2307-4543
23
10
38.2
-45
27
19
10.5
0.90
§
§
§
0.01
-45
8.80
0.33
5.74
§
§
§
-1.69
§
§
§
-1.69
-0.00
*
HE
2310-4523
23
12
60.0
-45
07
06
12.5
0.86
0.87
0.01
-85
6.05
0.68
4.75
-2.60
-2.60
-2.60
-2.60
0.39
HE
2313-1747
23
16
01.2
-17
31
31
13.8
0.64
0.65
0.03
-113
7.10
1.31
3.58
-1.94
-1.94
-1.65
-1.87
-0.09
HE
2313-5937
23
16
29.5
-59
20
42
14.2
0.63
0.65
0.02
-18
6.40
1.35
3.63
-2.10
-2.10
-1.87
-2.04
0.07
HE
2315-4240
23
17
59.8
-42
24
31
13.7
0.70
0.68
0.01
130
4.51
1.12
1.72
-2.65
-2.65
-2.60
-2.64
-0.06
HE
2315-4306
23
18
19.0
-42
50
27
12.2
0.63
0.70
0.01
246
5.36
1.33
2.89
-2.46
-2.24
-2.37
-2.33
0.14
HE
2319-0303
23
22
31.9
-02
46
49
13.5
0.63
0.74
0.04
-142
6.04
1.31
2.99
-2.38
-2.14
-2.24
-2.23
-0.01
HE
2319-1108
23
22
32.2
-10
52
04
13.2
0.44
0.42
0.04
-10
6.48
3.94
2.31
-0.83
-1.07
-1.02
-1.03
-0.34
HE
2319-5228
23
21
58.1
-52
11
43
14.3
1.00
0.83
0.01
314
4.77
§
§
§
6.80
-3.10
§
§
§
-2.92
-3.01
1.05
HE
2320-0313
23
23
23.0
-02
56
48
11.1
0.59
0.58
0.04
76
8.40
1.92
4.42
-1.03
-1.03
-1.02
-1.03
-0.16
HE
2321-5301
23
24
19.9
-52
45
30
13.7
0.40
0.39
0.01
147
2.87
4.36
0.37
-1.96
-2.12
-2.13
-2.10
§
§
§
HE
2322-3420
23
25
38.4
-34
04
11
12.3
0.46
0.47
0.02
26
3.73
3.55
0.91
-2.13
-2.13
-2.16
-2.13
§
§
§
HE
2322-6125
23
25
34.6
-61
09
10
13.1
0.64
0.74
0.02
342
4.83
1.30
2.51
-2.78
-2.38
-2.66
-2.55
0.17
HE
2323-5708
23
26
43.7
-56
51
47
13.0
0.46
§
§
§
0.02
244
3.92
3.58
1.05
§
§
§
-2.08
§
§
§
-2.08
-0.28
HE
2324-0215
23
26
52.6
-01
59
24
12.6
0.86
0.95
0.05
-180
6.17
0.68
2.26
-2.76
-2.60
-2.78
-2.68
-0.29
HE
2325-0233
23
28
12.2
-02
17
23
13.4
0.70
0.56
0.06
92
4.83
1.24
1.55
-2.18
-2.59
-2.11
-2.37
-0.25
HE
2325-4743
23
28
31.4
-47
27
13
12.6
0.37
0.52
0.01
129
2.39
5.07
0.82
-2.54
-2.02
-2.76
-2.21
§
§
§
*
HE
2326-0449
23
28
50.6
-04
32
36
12.4
0.83
0.87
0.05
23
9.17
0.61
4.52
-1.38
-1.30
-1.68
-1.41
-0.27
HE
2330-4453
23
33
03.1
-44
37
11
10.9
0.69
0.83
0.01
162
6.95
1.01
1.74
-2.35
-2.16
-2.21
-2.22
-0.69
HE
2331-0350
23
33
43.2
-03
34
19
13.5
0.69
0.81
0.04
-102
6.23
1.00
1.95
-2.46
-2.34
-2.39
-2.38
-0.43

Table
11---Continued
Star
name
R.A.
#
B
(B
-V)
HP2
(B
-V)J-K
E(B-V)
v
rad
KP
HP2
GP
[Fe/H]
B-V
[Fe/H]
HP2
[Fe/H]
Rossi
[Fe/H]
final
[C/Fe]
Redisc.
(1)
(2)
(3)
(4)
(5)
(6)
(7)
(8)
(9)
(10)
(11)
(12)
(13)
(14)
(15)
(16)
(17)
HE
2335-3949
23
38
07.4
-39
32
57
13.2
0.92
1.09
0.01
10
8.14
0.49
3.08
§
§
§
-2.08
-2.52
-2.30
-0.42
HE
2340-5622
23
42
54.5
-56
05
27
11.6
0.83
§
§
§
0.01
-15
9.22
0.52
5.79
§
§
§
-1.30
§
§
§
-1.30
-0.06
HE
2340-6036
23
43
41.3
-60
19
22
13.7
0.70
0.91
0.01
268
4.89
1.18
1.28
-3.00
-2.59
-3.11
-2.82
-0.43
HE
2341-6200
23
44
38.6
-61
43
30
13.4
0.69
0.68
0.02
83
6.43
1.02
1.45
-2.27
-2.27
-1.94
-2.19
-0.73
HE
2342-5644
23
45
09.4
-56
27
22
11.2
0.70
0.75
0.01
148
8.78
1.08
4.34
-1.40
-1.33
-1.44
-1.37
-0.24
HE
2343-1817
23
46
14.6
-18
00
46
12.6
0.56
0.57
0.02
25
4.16
1.81
6.60
-2.34
-2.34
-2.37
-2.37
1.22
HE
2343-6007
23
46
20.4
-59
50
57
13.3
0.47
0.48
0.01
8
6.62
3.40
2.39
-1.33
-1.15
-1.21
-1.19
-0.34
HE
2347-1233
23
50
17.3
-12
17
07
11.3
0.83
0.84
0.03
13
8.90
0.62
5.61
-1.44
-1.44
-1.66
-1.66
-0.04
HE
2349-1709
23
51
45.1
-16
52
45
10.6
0.90
0.62
0.02
64
8.77
0.45
6.02
-0.70
-1.69
-1.06
-1.06
0.04
HE
2352-0450
23
54
53.8
-04
34
12
13.3
0.46
0.53
0.03
57
4.53
3.67
1.25
-2.16
-1.88
-2.11
-1.96
-0.34
HE
2354-5611
23
56
52.8
-55
54
48
12.1
0.54
0.55
0.01
23
7.96
2.38
4.07
-1.19
-1.02
-1.05
-1.07
-0.15
HE
2356-2106
23
59
11.8
-20
49
18
12.2
0.56
0.48
0.02
-46
7.26
2.24
3.58
-0.98
-1.47
-1.03
-1.24
-0.13
HE
2358-4640
00
00
50.9
-46
23
31
14.3
0.69
0.70
0.01
71
7.94
1.05
4.43
-1.85
-1.85
-1.54
-1.77
-0.07
HE
2359-5710
00
02
29.5
-56
53
49
9.6
0.59
0.79
0.01
-24
8.07
1.99
4.05
-1.79
-1.20
-1.77
-1.49
-0.18

-- 49 --
Table 12. ``Nonímetalípoor''objects
Star name R.A. # B (B - V ) HP2 (B - V ) J-K E (B-V) v rad KP HP2 GP Comm.
HE 0000-3017 00 03 21.9 -30 01 09 10.0 0.39 0.42 0.01 19 6.57 4.99 1.89
HE 0000-4401 00 03 11.7 -43 44 57 11.3 0.47 0.45 0.01 23 8.29 3.60 3.55
HE 0000-5703 00 02 43.0 -56 46 52 8.4 § § § 0.27 0.01 40 2.59 9.37 1.16
HE 0001-4157 00 03 50.0 -41 40 18 11.5 0.64 0.53 0.01 21 9.15 1.73 5.47
HE 0001-4449 00 04 15.9 -44 32 31 11.7 0.46 0.45 0.01 27 7.53 3.53 2.92
HE 0001-5640 00 04 09.2 -56 24 06 10.4 0.43 0.43 0.01 -15 7.80 4.06 2.82
HE 0002-3822 00 04 43.2 -38 06 01 11.3 0.48 0.49 0.02 42 7.80 3.39 3.20
HE 0002-5625 00 04 45.6 -56 08 24 13.0 0.64 0.59 0.01 60 9.25 1.65 5.55
HE 0003-2658 00 06 28.0 -26 41 23 11.5 0.39 0.38 0.02 2 6.92 4.95 2.22
HE 0004-1224 00 07 18.2 -12 07 52 10.4 0.40 0.48 0.03 -22 7.33 4.59 2.64
HE 0004-1650 00 07 08.2 -16 34 17 11.4 0.67 0.53 0.03 75 9.47 1.44 5.50
HE 0005-4959 00 08 13.4 -49 43 18 10.7 0.43 0.43 0.01 22 7.76 4.01 2.78
HE 0005-5945 00 07 48.3 -59 28 60 10.9 0.37 0.35 0.01 29 4.80 6.50 1.30
HE 0006-0211 00 09 11.0 -01 54 56 11.8 0.50 0.46 0.04 4 8.34 3.02 3.85
HE 0006-1244 00 09 01.0 -12 28 14 11.0 0.77 0.60 0.03 45 9.36 0.84 5.89
HE 0007-0155 00 10 13.3 02 11 60 11.4 0.78 0.77 0.03 7 10.87 0.89 5.93
HE 0007-2221 00 09 46.1 -22 05 14 10.2 0.71 0.60 0.02 14 9.15 1.03 5.72
HE 0007-3045 00 09 49.6 -30 28 56 10.7 0.43 0.42 0.01 43 7.38 4.18 2.58
HE 0007-3809 00 09 40.1 -37 52 37 11.7 0.41 0.35 0.02 41 6.26 4.31 2.57
HE 0007-5414 00 09 58.1 -53 57 31 10.1 0.76 0.57 0.01 9 8.85 0.88 5.58
HE 0008-0219 00 11 26.2 -02 02 51 11.8 0.39 0.38 0.04 1 7.06 4.79 2.35
HE 0008-1327 00 11 21.8 -13 10 39 11.2 0.41 0.43 0.03 -64 6.98 4.37 2.46
HE 0008-2829 00 10 41.9 -28 12 43 11.4 0.58 0.54 0.01 90 9.00 2.25 4.98
HE 0008-3129 00 10 53.8 -31 12 53 10.0 0.60 0.45 0.01 60 8.80 1.89 4.98
HE 0009-0328 00 12 01.0 -03 11 55 11.4 0.56 0.48 0.04 18 8.90 2.29 4.72
HE 0009-4721 00 11 36.1 -47 04 56 11.7 0.43 0.40 0.01 31 7.61 4.19 2.66
HE 0009-5628 00 11 54.0 -56 12 03 9.4 0.38 0.38 0.01 -6 6.66 5.20 1.94
HE 0010-1821 00 12 35.1 -18 04 57 11.4 0.51 0.47 0.03 53 8.79 3.22 3.81
HE 0010-3037 00 13 11.7 -30 21 01 10.1 0.52 0.45 0.01 37 8.60 2.84 4.31
HE 0010-5027 00 12 29.8 -50 11 15 11.6 0.38 0.40 0.02 46 5.83 4.81 1.84
HE 0010-5624 00 12 31.3 -56 08 10 10.4 0.59 0.51 0.01 89 8.29 1.88 4.85
HE 0010-5927 00 13 17.5 -59 11 16 10.8 0.57 0.53 0.01 -2 8.61 2.19 4.37
HE 0011-3837 00 13 56.3 -38 20 21 13.5 1.00 1.12 0.02 4 § § § § § § 0.44 Em
HE 0012-2228 00 15 23.7 -22 11 23 10.7 0.41 0.43 0.02 53 6.46 4.39 2.37
HE 0012-3133 00 15 00.0 -31 16 25 11.0 0.48 0.46 0.01 4 7.63 3.35 3.07
HE 0012-4233 00 15 11.1 -42 17 17 12.1 0.46 0.43 0.01 12 7.69 3.70 2.77
HE 0012-4742 00 15 15.6 -47 25 21 11.7 0.49 0.47 0.01 49 8.46 3.31 3.61
HE 0012-4830 00 15 11.6 -48 13 28 11.8 0.50 0.44 0.01 23 7.95 3.08 3.61
HE 0012-4849 00 15 10.8 -48 33 16 11.8 0.78 0.66 0.01 37 9.54 0.83 6.01
HE 0012-4937 00 14 34.7 -49 20 47 10.9 0.53 0.44 0.01 23 8.45 2.70 4.16
HE 0012-5344 00 15 06.4 -53 27 30 10.2 0.43 0.43 0.02 10 7.87 4.01 2.91
HE 0013-4423 00 15 48.5 -44 06 22 11.3 0.61 0.55 0.01 85 9.15 1.84 5.06
HE 0013-4731 00 15 37.5 -47 14 54 11.7 0.42 0.41 0.01 52 7.89 4.26 2.82
HE 0014-3001 00 16 43.7 -29 45 01 10.3 0.53 0.51 0.02 96 8.34 2.54 4.18
HE 0014-5443 00 17 00.6 -54 27 14 11.6 0.52 0.48 0.01 23 8.72 2.81 4.34
HE 0015-4526 00 17 53.8 -45 10 12 12.2 0.38 0.34 0.01 1 6.50 5.45 1.78
HE 0015-4748 00 17 36.1 -47 31 47 11.4 0.50 0.46 0.01 15 7.05 2.92 3.76
HE 0015-4844 00 17 31.1 -48 28 16 10.6 0.91 0.84 0.01 -34 10.20 0.40 6.06
HE 0015-5049 00 18 20.9 -50 32 38 11.8 0.47 0.44 0.01 -2 8.69 3.72 3.35
HE 0016-4913 00 18 31.3 -48 57 21 11.7 0.56 0.52 0.01 0 8.77 2.44 4.35
HE 0016-5112 00 19 03.7 -50 56 10 11.9 0.48 0.47 0.01 33 8.15 3.40 3.40
HE 0016-5945 00 18 49.5 -59 28 26 10.4 § § § 0.25 0.01 16 2.15 9.22 1.07
HE 0016-6138 00 18 33.8 -61 21 59 10.2 0.39 0.39 0.01 35 7.18 4.84 2.27
HE 0017-3041 00 19 43.9 -30 25 06 11.4 0.71 0.59 0.02 48 9.06 1.15 5.41
HE 0017-5707 00 19 43.8 -56 51 03 10.1 0.47 0.43 0.01 2 8.19 3.74 3.16
HE 0018-5458 00 20 50.1 -54 41 23 10.9 0.61 0.52 0.01 27 9.10 1.77 5.23
HE 0019-5902 00 21 31.5 -58 45 57 11.2 0.38 0.35 0.01 2 5.74 5.57 1.53
HE 0021-5508 00 23 39.8 -54 51 34 10.8 0.42 0.44 0.01 13 7.01 4.36 2.03
HE 0023-1328 00 25 33.1 -13 11 24 11.5 0.69 0.61 0.03 61 7.38 1.22 4.83 Em
HE 0025-5259 00 28 17.1 -52 42 59 11.0 0.43 0.44 0.02 -3 6.60 4.24 2.25
HE 0026-1707 00 29 13.5 -16 50 50 10.3 0.48 0.53 0.02 74 7.04 3.37 3.05
HE 0027-0203 00 30 30.7 02 20 25 11.5 0.50 0.45 0.02 67 8.23 3.12 3.61
HE 0027-0147 00 30 11.7 -01 30 57 11.2 0.54 0.48 0.02 62 8.88 2.51 3.63
HE 0027-0646 00 30 32.6 -06 29 36 11.2 0.64 0.54 0.04 42 9.48 1.56 5.76
HE 0027-1637 00 29 57.4 -16 21 21 10.6 0.38 0.34 0.02 2 5.80 5.76 1.47
HE 0027-2640 00 29 54.8 -26 23 26 11.5 0.48 0.45 0.01 16 7.90 3.36 3.54
HE 0027-5354 00 29 37.8 -53 38 03 11.2 0.38 0.37 0.02 27 5.62 6.02 1.48

-- 50 --
Table 12---Continued
Star name R.A. # B (B - V ) HP2 (B - V ) J-K E (B-V) v rad KP HP2 GP Comm.
HE 0028-0239 00 30 59.8 -02 22 52 11.3 0.45 0.42 0.03 38 7.59 3.92 3.27
HE 0028-5203 00 30 52.7 -51 46 42 11.5 0.67 0.53 0.01 30 9.41 1.33 5.97
HE 0028-5553 00 30 46.4 -55 37 07 10.8 0.40 0.43 0.01 53 7.00 4.74 2.32
HE 0029-1511 00 31 41.4 -14 55 16 10.6 0.65 0.55 0.03 26 8.49 1.39 5.01
HE 0029-1513 00 31 35.0 -14 57 24 10.3 0.60 0.50 0.03 10 9.34 2.11 5.09
HE 0029-4730 00 31 54.2 -47 13 32 9.7 0.38 0.39 0.01 10 6.40 6.22 1.80
HE 0030-1400 00 33 11.3 -13 44 14 10.6 0.52 0.44 0.02 -23 8.72 2.77 3.92
HE 0030-2805 00 33 26.4 -27 48 40 11.5 0.53 0.49 0.01 37 9.20 2.90 3.89
HE 0033-0027 00 36 15.0 00 44 16 13.3 0.38 0.32 0.02 -98 6.18 5.72 1.64
HE 0033-2404 00 35 56.3 -23 48 05 10.9 0.40 0.52 0.02 63 6.90 4.56 2.31
HE 0033-2522 00 36 09.2 -25 05 57 11.3 0.50 0.48 0.01 40 8.62 3.18 3.77
HE 0033-2646 00 35 50.4 -26 29 45 11.7 § § § 0.33 0.01 8 4.41 7.41 0.92
HE 0033-3301 00 36 25.4 -32 44 48 11.9 0.41 0.39 0.01 76 6.59 4.29 2.47
HE 0033-5140 00 35 43.1 -51 24 27 10.4 0.48 0.44 0.01 56 7.69 3.34 3.00
HE 0033-5419 00 35 41.5 -54 02 30 10.2 0.45 0.45 0.01 30 7.58 3.91 2.75
HE 0034-2707 00 36 29.6 -26 50 48 11.6 0.53 0.50 0.01 -28 8.29 2.59 3.85
HE 0034-4302 00 37 02.9 -42 45 48 11.2 0.37 0.38 0.01 -51 4.98 5.88 1.48
HE 0034-4413 00 36 42.7 -43 57 22 12.6 0.61 0.46 0.01 72 9.07 1.92 5.19
HE 0035-3610 00 37 53.8 -35 53 52 11.5 0.58 0.52 0.01 -24 8.92 2.16 4.74
HE 0036-0249 00 38 37.3 -02 32 50 12.5 0.37 0.39 0.03 5 4.83 5.66 1.54
HE 0036-5036 00 39 10.5 -50 20 24 11.3 0.46 § § § 0.01 -15 7.62 3.67 2.72
HE 0037-5614 00 39 42.7 -55 57 33 10.4 § § § 0.38 0.01 2 5.36 6.72 1.54
HE 0038-3217 00 40 30.2 -32 00 48 13.7 0.60 0.48 0.01 43 9.01 2.12 4.80
HE 0038-4918 00 40 38.7 -49 02 00 11.1 0.39 0.44 0.01 -17 6.28 4.93 1.83
HE 0039-2541 00 42 13.6 -25 25 04 11.5 0.39 0.40 0.01 20 7.63 4.99 2.64
HE 0039-2640 00 41 43.3 -26 24 01 11.7 0.49 0.51 0.01 9 8.50 3.49 3.75
HE 0040-5355 00 43 02.7 -53 39 03 11.1 0.45 0.47 0.01 82 7.66 3.93 2.88
HE 0041-3424 00 43 27.4 -34 07 36 11.6 0.51 0.45 0.01 -34 8.15 2.94 4.27
HE 0041-5329 00 43 29.4 -53 13 22 10.7 0.41 0.39 0.02 72 7.75 4.65 2.37
HE 0042-2152 00 44 41.3 -21 36 03 9.5 0.50 § § § 0.02 25 8.18 3.10 3.39
HE 0042-2635 00 44 38.3 -26 18 58 11.5 0.38 0.38 0.01 3 5.97 5.76 1.49
HE 0042-4351 00 44 46.2 -43 35 27 12.9 0.48 0.47 0.01 7 7.64 3.40 2.85
HE 0043-0042 00 46 11.7 00 59 10 11.6 0.91 0.73 0.02 -64 9.83 0.45 5.97
HE 0043-0234 00 46 26.5 -02 18 32 12.3 0.41 0.38 0.03 -42 7.86 4.72 2.32
HE 0043-2611 00 45 53.0 -25 55 12 11.4 0.46 0.51 0.01 -15 8.34 3.87 3.21
HE 0043-3218 00 45 33.3 -32 02 21 10.7 0.67 0.53 0.02 -14 9.52 1.30 5.59
HE 0043-5011 00 45 19.6 -49 55 21 11.4 0.56 0.53 0.01 82 8.92 2.44 4.53
HE 0043-5226 00 46 14.1 -52 09 44 12.9 0.86 1.08 0.01 -54 11.25 0.50 4.65
HE 0045-0231 00 48 13.2 -02 15 02 12.2 0.38 0.38 0.05 -55 6.87 5.06 2.27
HE 0045-4634 00 47 21.5 -46 18 20 11.0 0.51 0.51 0.01 22 8.82 3.20 3.94
HE 0045-4951 00 47 29.5 -49 35 01 11.6 0.45 0.43 0.01 82 8.13 3.98 3.30
HE 0045-5633 00 47 47.8 -56 17 38 10.8 0.39 0.44 0.02 57 7.93 4.90 2.59
HE 0045-5711 00 47 39.3 -56 54 41 10.2 0.38 0.35 0.02 -14 7.19 5.68 2.28
HE 0046-0759 00 48 47.0 -07 43 12 11.7 0.48 0.45 0.04 15 7.26 3.47 2.51
HE 0046-5219 00 49 05.8 -52 02 49 11.1 0.50 0.44 0.02 96 8.42 3.13 3.64
HE 0046-5622 00 49 01.1 -56 05 48 10.1 0.44 0.21 0.02 24 0.17 3.78 § § § He
HE 0047-0808 00 50 02.0 -07 52 27 11.5 0.46 0.42 0.06 23 7.87 3.69 2.70
HE 0047-5703A 00 49 58.5 -56 47 08 11.7 0.41 § § § 0.02 3 6.38 4.37 1.65
HE 0047-5703B 00 49 58.5 -56 47 08 11.7 0.41 § § § 0.02 -1 6.54 4.45 1.97
HE 0048-0024 00 50 42.1 00 40 48 12.5 0.45 0.50 0.02 -58 8.19 3.77 3.36
HE 0048-0137 00 50 36.0 -01 21 39 12.1 0.55 0.46 0.05 -49 9.05 2.66 4.10
HE 0049-0010 00 52 04.1 00 26 44 11.9 0.55 0.53 0.02 -81 8.66 2.35 4.92
HE 0049-3636 00 51 42.6 -36 20 18 11.3 0.43 0.38 0.01 12 7.34 4.03 2.46
HE 0050-0741 00 53 27.2 -07 24 56 11.0 0.38 0.39 0.07 2 5.85 6.07 1.60
HE 0050-0918 00 52 41.7 -09 02 23 12.0 0.71 0.70 0.04 -192 9.28 1.06 2.52
HE 0050-2014 00 53 08.0 -19 58 17 11.0 0.55 0.43 0.02 98 8.47 2.29 4.17
HE 0050-4817 00 53 15.1 -48 00 53 12.5 0.67 0.54 0.01 54 9.45 1.44 5.91
HE 0050-4937 00 52 30.9 -49 21 08 11.3 0.47 0.40 0.01 47 8.82 3.62 3.94
HE 0051-0043 00 54 24.1 -00 27 43 12.7 0.56 0.47 0.03 -81 8.06 2.14 5.50
HE 0051-0806 00 53 37.3 -07 50 43 10.6 0.66 0.44 0.07 37 8.97 1.45 5.39
HE 0052-2141 00 55 12.9 -21 24 51 11.0 0.59 0.57 0.02 -78 8.53 1.75 5.50
HE 0053-0750 00 55 45.2 -07 34 38 12.2 0.46 0.43 0.10 -47 7.38 3.66 2.77
HE 0054-0511 00 56 40.0 -04 54 53 10.6 0.43 0.40 0.06 -40 6.87 4.06 2.68
HE 0055-0817 00 57 41.7 -08 01 01 11.1 0.41 0.34 0.09 -45 6.77 4.37 2.04
HE 0057-2500 00 59 55.0 -24 43 51 11.2 0.38 0.36 0.04 9 5.87 5.43 1.67
HE 0057-6135 00 59 48.6 -61 19 05 10.9 0.38 0.37 0.02 38 5.54 5.76 1.54
HE 0058-1155 01 01 17.9 -11 39 09 11.0 0.40 0.41 0.03 54 7.45 4.55 2.72

-- 51 --
Table 12---Continued
Star name R.A. # B (B - V ) HP2 (B - V ) J-K E (B-V) v rad KP HP2 GP Comm.
HE 0058-2601 01 01 10.1 -25 45 40 10.7 0.47 0.42 0.03 0 8.31 3.55 3.37
HE 0059-3131 01 02 18.6 -31 15 35 11.3 0.41 0.41 0.02 5 6.69 4.27 2.37
HE 0100-2715 01 02 45.9 -26 59 24 10.6 0.46 0.42 0.02 12 7.74 3.71 2.98
HE 0100-5114 01 02 32.0 -50 58 28 11.6 0.38 0.38 0.01 -3 5.95 4.77 1.38
HE 0101-0451 01 04 22.7 -04 35 46 9.0 0.46 § § § 0.03 39 7.86 3.72 2.61
HE 0103-0031 01 06 20.1 -00 15 23 13.9 0.59 0.62 0.04 -34 8.57 1.86 4.83
HE 0104-0248 01 07 11.3 -02 32 03 10.8 0.46 0.46 0.04 3 7.91 3.74 3.33
HE 0104-5625 01 06 27.4 -56 09 38 10.9 § § § 0.27 0.02 31 1.32 9.45 1.15
HE 0105-1042 01 07 38.9 -10 26 39 11.5 0.46 0.55 0.03 -22 7.12 3.62 2.72
HE 0107-0319 01 10 04.0 -03 03 42 10.8 0.62 0.52 0.04 -66 9.36 1.93 4.84
HE 0107-0723 01 10 06.0 -07 07 42 11.5 0.60 0.50 0.10 -19 9.19 2.21 4.96
HE 0107-0810 01 09 41.4 -07 54 54 11.1 0.40 0.38 0.06 -24 6.53 4.72 1.87
HE 0107-1017 01 09 39.4 -10 01 26 11.3 0.50 0.46 0.04 -32 7.84 3.21 3.07
HE 0107-4740 01 10 01.4 -47 24 21 12.3 0.41 0.43 0.01 2 6.33 4.40 2.04
HE 0109-0323 01 12 15.8 -03 07 22 10.6 0.42 0.45 0.05 -26 7.60 4.25 2.67
HE 0110-0514 01 12 32.7 -04 58 39 11.1 0.49 0.41 0.06 -31 8.28 3.47 3.52
HE 0110-1314 01 13 21.8 -12 58 48 11.0 0.61 0.49 0.02 -55 9.17 1.93 4.69
HE 0110-3402 01 13 12.6 -33 46 18 10.6 § § § 0.32 0.03 -0 5.80 6.58 1.50
HE 0111-1256 01 13 31.7 -12 40 29 11.5 0.50 0.49 0.02 -31 8.18 3.03 3.54
HE 0111-1505 01 13 42.9 -14 49 40 11.8 0.51 0.46 0.02 74 7.48 2.81 3.12
HE 0111-1936 01 14 03.4 -19 20 25 11.6 0.46 0.41 0.01 86 7.67 3.63 2.70
HE 0113-4903 01 15 45.1 -48 47 50 11.9 0.44 0.41 0.01 33 8.37 4.22 3.05
HE 0114-4730 01 17 01.0 -47 14 44 11.4 0.51 0.44 0.01 71 7.56 2.94 3.46
HE 0115-3852 01 17 52.0 -38 36 45 11.1 0.37 0.17 0.02 41 0.24 5.09 § § § He
HE 0115-4940 01 17 26.7 -49 25 00 11.9 0.54 0.48 0.01 33 8.81 2.62 3.75
HE 0115-5135 01 17 20.6 -51 19 31 10.1 0.72 0.73 0.01 160 9.53 1.20 5.50
HE 0116-5711 01 18 27.4 -56 56 03 12.0 0.46 0.46 0.02 8 7.67 3.72 2.99
HE 0116-5944 01 17 58.0 -59 28 47 11.8 § § § 0.47 0.03 57 4.62 6.81 1.38
HE 0117-4106 01 19 36.1 -40 50 24 11.1 0.48 0.54 0.01 84 7.82 3.36 3.27
HE 0117-5336 01 19 58.8 -53 20 51 11.6 0.63 0.56 0.02 31 8.84 1.68 5.01
HE 0117-5555 01 19 51.7 -55 40 02 11.1 0.45 0.45 0.02 26 8.06 3.84 3.35
HE 0118-2637 01 20 42.0 -26 22 03 10.6 § § § 0.40 0.01 3 2.96 6.84 1.02
HE 0118-5323 01 20 47.9 -53 07 50 11.5 0.51 0.45 0.02 54 8.95 3.20 4.10
HE 0119-3352 01 22 04.1 -33 37 03 12.6 1.00 1.25 0.02 0 1.37 § § § § § § Em
HE 0119-4057 01 21 53.9 -40 41 29 10.8 0.38 0.38 0.02 11 5.67 5.70 1.70
HE 0120-1816 01 22 38.6 -18 00 40 11.2 0.47 0.41 0.02 -20 8.56 3.61 3.29
HE 0120-5246 01 22 33.1 -52 30 31 11.7 0.45 0.44 0.01 85 7.41 3.95 2.63
HE 0120-5437 01 22 42.3 -54 21 27 11.4 0.58 0.52 0.03 52 8.97 2.10 5.15
HE 0122-0218 01 24 48.7 -02 02 50 12.4 0.40 0.37 0.05 35 6.94 4.67 1.93
HE 0122-0257 01 25 01.1 -02 42 04 11.5 0.64 0.68 0.04 -17 9.09 1.69 4.93
HE 0122-4101 01 25 11.6 -40 45 55 11.1 0.38 0.35 0.01 -19 6.55 5.66 1.56
HE 0122-4704 01 24 54.4 -46 48 26 11.3 0.51 0.43 0.01 64 8.46 2.97 3.70
HE 0122-5318 01 24 07.7 -53 02 54 11.1 § § § 0.30 0.02 10 4.71 7.02 1.39
HE 0122-5406 01 24 03.1 -53 51 17 12.1 0.41 0.40 0.03 71 6.92 4.30 2.41
HE 0123-5513 01 25 51.6 -54 57 41 12.2 0.43 0.39 0.02 33 7.63 4.02 2.85
HE 0123-5520 01 25 26.4 -55 05 07 11.2 0.54 0.49 0.02 29 8.71 2.69 4.77
HE 0126-0237 01 29 08.6 -02 21 35 11.9 0.60 0.44 0.04 -29 8.98 1.81 5.18
HE 0126-3435 01 28 52.7 -34 20 30 11.2 0.53 0.51 0.02 105 8.41 2.74 4.05
HE 0127-3833 01 29 24.0 -38 17 56 11.1 0.51 0.44 0.02 -11 8.94 3.20 4.08
HE 0128-0204 01 31 06.7 02 19 59 12.8 0.38 0.38 0.02 -40 5.64 5.61 1.58
HE 0128-0948 01 30 59.9 -09 33 25 12.6 0.53 0.38 0.03 92 8.08 2.74 4.26
HE 0128-5121 01 30 03.5 -51 06 31 10.3 0.39 0.42 0.02 -26 6.20 4.98 1.74
HE 0129-0751 01 32 07.8 -07 35 43 12.1 0.60 0.48 0.03 -61 8.99 1.99 4.56
HE 0129-1819 01 31 40.8 -18 04 32 11.1 0.66 0.55 0.02 -31 9.23 1.43 5.34
HE 0130-0208 01 32 49.8 02 23 24 11.4 0.58 0.49 0.03 -54 9.04 2.49 4.93
HE 0130-0013 01 32 48.5 00 01 24 11.7 0.44 0.45 0.03 -56 6.55 3.87 2.38
HE 0134-2142 01 36 45.0 -21 26 58 10.4 0.49 0.42 0.01 72 9.00 3.36 4.35
HE 0134-2541 01 36 29.4 -25 26 17 12.0 0.45 0.41 0.01 -13 7.31 3.85 2.49
HE 0134-6025 01 36 30.4 -60 09 57 11.9 0.54 0.46 0.02 38 8.94 2.68 4.46
HE 0135-3356A 01 37 25.3 -33 40 47 11.7 0.46 0.48 0.02 -2 7.81 3.58 3.13
HE 0135-3356B 01 37 25.3 -33 40 47 11.7 1.00 § § § 0.02 -107 11.29 § § § 5.92 Em
HE 0136-4146 01 38 16.4 -41 30 52 11.2 0.43 0.44 0.02 64 6.88 4.00 2.67
HE 0136-4315 01 38 50.3 -42 59 57 12.3 0.47 § § § 0.02 -17 8.55 3.57 3.25
HE 0137-1138 01 40 22.1 -11 23 15 11.3 0.47 0.49 0.02 45 8.31 3.63 3.67
HE 0137-1756 01 39 26.7 -17 41 28 13.9 1.00 0.92 0.02 8 8.96 § § § 5.63 Em
HE 0139-1133 01 42 11.7 -11 18 01 11.2 0.52 0.53 0.02 41 8.53 2.83 4.07
HE 0139-5113 01 41 47.6 -50 57 57 10.1 0.42 0.47 0.02 22 7.94 4.38 2.55

-- 52 --
Table 12---Continued
Star name R.A. # B (B - V ) HP2 (B - V ) J-K E (B-V) v rad KP HP2 GP Comm.
HE 0141-2939 01 43 20.2 -29 24 50 10.7 § § § 0.38 0.02 -8 4.79 7.11 1.50
HE 0141-3051 01 43 59.0 -30 36 07 11.5 0.41 0.40 0.02 54 6.62 4.31 2.09
HE 0142-4230 01 44 13.7 -42 15 27 10.8 0.39 0.44 0.01 43 7.76 4.92 0.00
HE 0142-5143 01 44 10.0 -51 28 35 11.2 § § § 0.31 0.02 0 5.29 7.02 1.31
HE 0143-0821 01 46 15.5 -08 06 49 11.2 0.52 0.52 0.03 15 7.89 2.73 4.06
HE 0143-2923 01 46 12.6 -29 08 37 11.1 0.52 0.51 0.01 18 7.61 2.58 3.82
HE 0143-3053 01 46 05.8 -30 38 03 11.3 0.38 0.37 0.02 -18 7.12 5.18 2.09
HE 0144-2711 01 47 02.3 -26 57 02 11.2 0.40 0.41 0.02 -24 6.25 4.57 2.04
HE 0144-4625 01 46 44.7 -46 10 48 11.1 0.47 0.42 0.01 -19 8.23 3.60 3.12
HE 0144-4909 01 46 24.4 -48 54 06 11.3 0.45 0.37 0.02 68 7.08 3.99 2.43
HE 0145-3017 01 47 18.6 -30 02 06 11.0 0.58 0.50 0.01 34 9.06 2.28 4.99
HE 0145-3221 01 47 57.3 -32 06 42 11.9 0.64 0.58 0.02 7 9.04 1.71 5.08
HE 0145-3244 01 47 38.4 -32 29 32 11.5 0.53 0.53 0.02 -4 8.24 2.54 3.87
HE 0146-5105 01 47 57.1 -50 50 59 11.2 0.64 0.54 0.02 37 9.14 1.52 5.24
HE 0146-5130 01 47 58.2 -51 15 26 11.3 0.45 0.44 0.02 41 7.98 3.80 2.98
HE 0146-5140 01 48 04.8 -51 25 09 11.7 0.43 0.43 0.02 -15 7.63 4.14 2.51
HE 0147-3132 01 49 30.4 -31 17 36 11.0 0.49 0.43 0.02 -3 8.58 3.40 4.06
HE 0149-4308 01 51 26.2 -42 53 20 11.4 0.58 0.53 0.02 18 8.99 2.14 4.62
HE 0149-4337 01 51 15.1 -43 23 05 11.2 0.63 0.64 0.02 -23 8.77 1.69 4.70
HE 0150-0000 01 52 55.8 00 13 57 11.6 0.38 0.32 0.04 6 6.33 5.18 1.92
HE 0150-3005 01 52 58.0 -29 50 52 11.3 0.58 0.53 0.02 -3 9.00 2.46 4.52
HE 0150-3020 01 52 38.6 -30 05 50 11.2 0.37 0.45 0.02 -17 4.95 6.01 1.35
HE 0150-5120 01 52 26.2 -51 05 57 13.8 0.60 0.55 0.02 30 8.78 1.89 4.89
HE 0151-3221 01 54 03.1 -32 07 06 12.6 0.39 0.38 0.02 -1 7.39 5.10 1.79
HE 0151-3352 01 53 22.6 -33 37 57 11.1 § § § 0.34 0.02 -31 5.35 6.69 1.50
HE 0151-4704 01 53 20.4 -46 49 38 11.1 § § § 0.27 0.02 1 3.06 8.80 1.13
HE 0153-4315 01 56 00.7 -43 01 12 10.9 0.47 0.43 0.01 42 8.19 3.56 3.14
HE 0154-2250 01 56 35.8 -22 35 33 13.2 0.71 0.63 0.02 26 9.10 1.14 5.32
HE 0155-3027 01 58 12.2 -30 13 06 10.7 0.41 0.39 0.02 12 6.62 4.34 2.18
HE 0156-4656 01 58 03.1 -46 41 29 11.5 0.58 0.46 0.03 -10 9.37 2.45 4.35
HE 0157-0159 02 00 20.4 -01 45 07 11.1 0.48 0.52 0.02 24 7.52 3.33 3.05
HE 0157-5324 01 59 44.3 -53 10 20 11.4 0.71 0.60 0.02 56 9.28 1.07 5.92
HE 0158-6145 01 59 52.6 -61 30 54 11.7 0.43 § § § 0.03 -8 7.53 4.22 2.44
HE 0159-3425 02 02 00.6 -34 10 54 11.8 0.64 0.54 0.01 69 9.15 1.65 5.16
HE 0159-4233 02 01 55.5 -42 18 41 12.0 0.75 0.82 0.01 30 7.67 0.76 5.46 Em
HE 0159-4345 02 02 00.2 -43 30 52 11.2 0.58 0.52 0.01 55 8.91 2.08 4.62
HE 0159-4354 02 01 58.7 -43 39 56 11.2 0.43 0.40 0.01 13 7.14 4.20 2.35
HE 0159-5714 02 01 00.8 -57 00 09 11.6 0.71 0.64 0.02 73 9.35 1.04 5.78
HE 0159-6146 02 00 38.5 -61 32 14 12.0 0.60 0.53 0.03 93 8.99 1.96 5.02
HE 0200-1144 02 03 21.6 -11 30 32 10.1 0.43 0.40 0.02 7 7.40 4.24 2.82
HE 0200-4222 02 02 32.3 -42 08 30 11.2 0.38 0.36 0.01 56 5.78 5.86 1.53
HE 0200-6050 02 02 15.2 -60 35 53 10.5 0.40 0.39 0.03 52 7.36 4.69 2.34
HE 0201-3148 02 04 01.2 -31 33 44 10.6 0.84 § § § 0.02 -4 9.90 0.59 6.05
HE 0201-4038 02 03 07.4 -40 24 35 10.4 0.39 0.46 0.02 -4 6.82 4.93 1.95
HE 0202-2638 02 05 11.4 -26 24 10 10.8 0.45 § § § 0.02 -37 8.04 3.92 3.01
HE 0202-4350 02 04 18.4 -43 36 03 11.5 0.38 0.36 0.01 -13 5.75 5.35 1.65
HE 0202-5321 02 04 37.9 -53 07 03 12.1 0.84 0.73 0.02 67 6.61 0.63 5.15 Em
HE 0202-5756 02 03 45.2 -57 41 52 11.3 0.40 0.40 0.02 51 6.01 4.58 1.89
HE 0203-4157 02 05 17.0 -41 43 28 10.6 § § § 0.30 0.01 5 6.04 7.82 1.13
HE 0203-4236 02 05 34.9 -42 22 30 11.1 0.38 0.40 0.01 -30 6.12 5.68 1.62
HE 0203-5926 02 05 02.0 -59 11 59 12.1 0.37 0.32 0.02 39 2.64 6.37 1.47
HE 0204-2855 02 07 01.3 -28 41 38 11.1 0.38 0.31 0.01 -13 5.96 6.43 1.76
HE 0204-4230 02 06 31.0 -42 16 06 11.3 0.44 0.40 0.02 -17 8.45 4.06 3.26
HE 0204-4419 02 06 22.0 -44 05 34 11.2 0.54 0.48 0.02 8 8.74 2.61 4.31
HE 0205-0144 02 08 04.6 01 58 34 12.3 0.43 0.42 0.03 -53 6.98 4.21 2.30
HE 0205-0233 02 07 44.2 -02 18 54 10.5 0.47 0.42 0.03 56 8.20 3.54 3.45
HE 0205-2956 02 08 02.5 -29 41 55 11.3 0.53 0.47 0.01 31 8.46 2.69 4.57
HE 0205-4358 02 07 08.9 -43 44 28 11.3 0.56 0.47 0.01 -23 8.82 2.34 4.33
HE 0205-6201 02 06 36.3 -61 47 05 11.5 0.45 0.37 0.04 65 7.64 3.92 3.06
HE 0206-0600 02 08 53.2 -05 46 34 10.5 0.43 0.47 0.02 40 7.05 4.23 2.35
HE 0206-0850 02 09 16.0 -08 36 09 11.1 0.60 0.52 0.02 -48 8.99 1.89 5.12
HE 0206-2831 02 08 56.3 -28 17 23 11.8 0.43 0.53 0.01 -19 6.98 4.24 2.64
HE 0206-2923 02 09 11.7 -29 09 22 10.9 0.61 0.52 0.01 -16 9.10 1.96 5.13
HE 0206-2950 02 08 29.2 -29 36 39 11.5 0.64 0.58 0.01 21 9.36 1.73 5.58
HE 0207-0158 02 10 07.4 02 12 24 11.5 0.55 0.50 0.03 28 8.61 2.40 4.36
HE 0207-0304 02 10 25.8 -02 50 37 11.7 0.45 0.43 0.03 50 7.88 3.90 2.39
HE 0207-0905 02 10 20.2 -08 51 29 10.7 0.38 0.37 0.02 -36 5.88 5.28 1.51

-- 53 --
Table 12---Continued
Star name R.A. # B (B - V ) HP2 (B - V ) J-K E (B-V) v rad KP HP2 GP Comm.
HE 0207-1125 02 10 22.4 -11 11 10 11.3 0.66 0.57 0.02 -30 9.24 1.41 5.38
HE 0207-3820 02 09 43.3 -38 06 14 11.1 0.64 0.61 0.01 47 9.25 1.68 5.46
HE 0208-4655 02 10 34.6 -46 41 54 10.7 § § § 0.32 0.02 -17 3.32 7.56 1.06
HE 0209-0722 02 11 35.9 -07 08 53 11.9 0.52 0.46 0.02 -96 7.62 2.63 3.23
HE 0209-0842 02 11 58.4 -08 28 44 10.7 0.38 0.44 0.02 -29 6.78 5.02 1.96
HE 0209-2252 02 11 34.3 -22 38 55 11.4 0.70 0.52 0.01 37 8.92 1.20 5.74
HE 0209-5150 02 11 29.7 -51 36 32 10.7 0.53 0.51 0.02 39 9.10 2.81 4.12
HE 0210-3759 02 12 23.6 -37 45 06 11.4 0.62 0.50 0.01 18 9.40 1.96 5.20
HE 0210-5946 02 11 54.4 -59 32 11 12.3 0.46 0.51 0.03 81 7.04 3.54 2.95
HE 0211-1933 02 14 12.1 -19 19 41 11.2 0.61 0.50 0.02 -60 9.11 1.75 5.35
HE 0211-3316 02 13 37.4 -33 02 32 11.9 0.47 0.51 0.02 -9 8.20 3.66 3.30
HE 0211-4711 02 13 07.0 -46 57 37 11.3 0.60 0.47 0.02 -20 8.99 1.98 4.78
HE 0211-5254 02 13 16.7 -52 40 28 11.3 0.77 0.60 0.02 27 9.34 0.93 5.70
HE 0212-0633 02 14 43.2 -06 19 15 11.1 0.50 0.47 0.02 87 6.95 2.82 3.21
HE 0212-5258 02 14 17.6 -52 44 57 11.2 0.56 0.53 0.02 36 8.98 2.35 4.53
HE 0212-5728 02 14 34.1 -57 14 18 12.5 0.45 0.39 0.03 26 7.44 3.80 2.78
HE 0212-5955 02 13 41.1 -59 42 01 11.4 0.45 0.39 0.03 73 7.31 3.78 2.66
HE 0213-2532 02 15 28.1 -25 18 10 11.2 0.61 0.51 0.02 -13 9.07 1.94 4.95
HE 0213-3210 02 15 47.3 -31 56 25 10.1 0.50 0.41 0.02 -19 8.48 3.22 3.75
HE 0213-5154 02 15 33.1 -51 40 56 11.4 0.45 0.43 0.03 -2 7.42 3.84 2.64
HE 0213-5206 02 15 15.7 -51 52 20 11.4 0.64 0.56 0.02 -4 9.72 1.54 5.20
HE 0214-4818 02 16 49.0 -48 05 02 12.0 0.41 0.46 0.02 -39 6.43 4.34 2.02
HE 0214-4959 02 15 52.3 -49 45 58 11.2 0.49 0.49 0.02 27 8.72 3.30 3.94
HE 0214-5005 02 16 47.0 -49 51 31 11.5 0.45 0.47 0.02 -4 7.67 3.87 2.81
HE 0215-2002 02 17 45.0 -19 48 28 13.3 0.67 0.63 0.02 61 9.49 1.38 5.09
HE 0215-4807 02 17 13.4 -47 53 50 11.9 0.47 0.42 0.02 13 8.50 3.54 3.51
HE 0215-4808 02 16 53.4 -47 54 33 12.6 0.48 0.45 0.02 35 8.17 3.25 3.65
HE 0215-4823 02 17 04.3 -48 10 08 12.2 0.46 0.43 0.02 33 6.78 3.60 2.60
HE 0217-3446 02 19 07.9 -34 32 47 11.7 § § § 0.34 0.02 78 3.51 7.35 1.37
HE 0220-2442 02 23 14.3 -24 29 06 11.4 0.38 0.36 0.02 48 6.17 5.31 1.92
HE 0221-2345 02 24 14.8 -23 31 45 11.5 0.41 0.43 0.02 30 6.63 4.25 2.70
HE 0221-2354 02 23 22.6 -23 41 24 11.3 0.53 0.52 0.02 2516 8.24 2.56 4.02
HE 0221-4039 02 23 54.1 -40 25 52 11.6 0.56 0.56 0.01 -14 8.77 2.42 4.31
HE 0221-5637 02 22 57.5 -56 24 18 11.0 0.42 0.39 0.03 -58 7.17 4.35 2.40
HE 0222-2503 02 24 25.5 -24 50 11 11.4 0.39 0.41 0.02 37 6.56 4.96 2.08
HE 0223-2338 02 25 29.8 -23 25 18 12.7 1.00 0.53 0.02 40 8.89 § § § 5.61
HE 0223-2632 02 25 49.5 -26 18 33 11.0 0.55 0.50 0.01 31 8.30 2.38 3.67
HE 0224-4334 02 26 42.2 -43 21 04 10.7 § § § 0.34 0.02 -31 4.27 7.06 1.55
HE 0224-4914 02 26 36.4 -49 01 26 11.1 0.38 0.40 0.02 42 5.87 5.83 1.18
HE 0225-3314 02 27 33.8 -33 01 17 10.8 0.39 0.40 0.02 -18 6.76 4.91 1.96
HE 0226-0540 02 29 23.9 -05 26 46 12.3 0.62 0.52 0.02 -23 9.45 1.79 5.14
HE 0227-4242 02 29 46.7 -42 29 04 10.5 0.38 0.39 0.03 -31 6.54 5.08 1.91
HE 0228-0121 02 31 03.4 01 34 41 11.5 0.38 0.39 0.03 -1 6.01 5.78 1.57
HE 0228-5319 02 30 27.8 -53 06 20 11.9 0.51 0.46 0.02 64 8.92 3.04 3.72
HE 0228-5513 02 30 33.8 -55 00 03 12.1 0.49 0.46 0.03 4 9.03 3.36 3.46
HE 0229-0621 02 31 55.6 -06 08 34 10.5 0.42 0.38 0.02 -17 7.74 4.37 2.42
HE 0229-6038 02 30 47.0 -60 24 58 12.9 0.43 0.40 0.04 43 7.76 4.10 2.76
HE 0233-4832 02 35 22.0 -48 19 39 § § § 0.39 0.38 0.03 -33 6.87 4.81 1.98
HE 0233-5545 02 34 38.9 -55 32 40 8.5 0.50 0.39 0.03 19 8.39 3.17 3.55
HE 0234-5039 02 36 37.7 -50 26 26 11.8 0.64 0.56 0.03 65 9.19 1.58 5.13
HE 0235-1946 02 38 15.1 -19 33 09 12.0 0.54 0.47 0.03 55 8.50 2.70 3.91
HE 0235-4808 02 37 05.6 -47 55 24 11.5 0.45 0.40 0.02 -30 7.67 3.99 2.46
HE 0235-5142 02 36 45.3 -51 29 15 11.1 0.45 0.45 0.03 -28 7.61 3.81 2.62
HE 0235-5524 02 37 13.3 -55 11 50 31.4 0.39 § § § 0.03 -8 7.01 4.87 2.15
HE 0236-0326 02 39 23.0 -03 13 38 12.6 0.59 0.52 0.03 -12 8.74 1.88 4.67
HE 0236-1728 02 39 17.7 -17 15 12 12.0 0.57 0.55 0.03 56 8.63 2.15 4.08
HE 0236-1742 02 38 38.5 -17 30 01 12.4 0.45 0.45 0.03 86 7.40 3.89 2.56
HE 0236-4909 02 38 20.9 -48 57 03 12.0 0.37 0.38 0.03 175 1.81 5.81 0.56
HE 0237-1836 02 40 12.5 -18 23 14 11.9 0.51 0.44 0.02 33 8.46 2.93 4.14
HE 0237-1928 02 39 36.9 -19 16 05 12.3 § § § 0.33 0.03 39 5.35 6.54 1.48
HE 0237-2003 02 39 46.8 -19 51 05 12.1 0.45 0.42 0.03 64 7.33 3.96 2.32
HE 0237-2041 02 40 02.2 -20 29 09 11.4 0.61 § § § 0.03 -44 9.00 1.99 4.43
HE 0237-2630 02 39 48.8 -26 18 04 11.1 0.38 0.47 0.02 42 5.93 5.12 2.01
HE 0237-5714 02 38 40.9 -57 01 21 31.5 § § § 0.33 0.03 3 4.95 6.68 1.57
HE 0239-3315 02 41 24.3 -33 03 10 10.8 0.51 0.50 0.02 -12 8.25 2.78 3.61
HE 0239-4907 02 41 28.0 -48 55 08 12.1 0.51 0.54 0.03 61 9.29 3.11 3.87
HE 0239-5221 02 40 43.4 -52 08 41 11.7 § § § 0.34 0.03 24 4.74 7.54 1.55

-- 54 --
Table 12---Continued
Star name R.A. # B (B - V ) HP2 (B - V ) J-K E (B-V) v rad KP HP2 GP Comm.
HE 0240-0009b 02 43 26.5 00 03 18 11.3 § § § 0.33 0.03 -16 4.92 6.69 1.58
HE 0240-0018 02 43 05.9 -00 06 12 11.8 0.55 0.51 0.03 -16 9.44 2.53 4.37
HE 0240-2341 02 42 18.8 -23 28 44 11.4 0.38 0.36 0.02 -12 5.98 6.15 1.78
HE 0241-2255 02 43 29.5 -22 42 30 11.5 0.43 0.37 0.03 71 7.44 4.03 2.45
HE 0241-6203 02 42 40.2 -61 51 01 11.1 0.51 0.48 0.02 -11 8.95 3.04 4.41
HE 0242-4934 02 44 30.6 -49 22 08 12.2 0.45 0.39 0.03 6 7.93 3.98 3.07
HE 0243-2429 02 46 09.1 -24 16 52 11.3 0.43 0.38 0.02 59 7.95 4.07 2.87
HE 0243-5205 02 45 25.4 -51 52 57 11.7 0.45 0.39 0.03 51 7.76 3.79 2.84
HE 0243-5722 02 44 39.2 -57 10 24 9.6 0.38 0.39 0.03 -11 6.35 5.51 1.81
HE 0244-2338 02 47 00.3 -23 25 34 12.1 0.42 0.36 0.03 101 7.05 4.36 2.39
HE 0244-4847 02 46 18.1 -48 35 11 12.1 0.48 0.46 0.03 7 7.98 3.43 3.43
HE 0244-5116 02 46 15.5 -51 03 50 11.5 0.51 0.46 0.03 38 9.02 3.18 4.29
HE 0244-5708 02 46 03.0 -56 56 00 31.4 0.47 0.46 0.03 -8 8.60 3.58 3.60
HE 0245-0337 02 48 00.4 -03 25 13 12.7 0.55 0.48 0.03 28 8.45 2.45 3.95
HE 0245-3344 02 47 19.8 -33 31 55 10.7 0.41 0.43 0.02 39 6.60 4.41 2.11
HE 0245-4833 02 46 48.9 -48 20 60 11.4 0.47 0.41 0.03 18 8.04 3.67 3.06
HE 0245-5139 02 47 20.5 -51 27 11 9.9 0.48 0.42 0.02 70 7.39 3.49 3.21
HE 0246-0149A 02 49 19.1 02 02 05 16.4 0.60 0.39 0.08 7 6.34 1.51 5.00
HE 0246-0149B 02 49 19.1 02 02 05 16.4 0.38 § § § 0.08 0 6.25 5.27 1.70
HE 0246-0207 02 48 57.1 02 20 02 12.5 0.53 0.47 0.07 -16 8.21 2.51 3.79
HE 0246-0121 02 49 32.4 -01 09 14 11.1 0.71 0.62 0.06 -46 9.11 1.02 5.59
HE 0246-0724 02 48 43.6 -07 12 06 12.2 0.38 0.41 0.04 -25 5.98 5.59 1.71
HE 0246-5114 02 48 26.3 -51 02 27 9.1 § § § 0.32 0.02 -18 5.69 6.67 1.75
HE 0247-0212 02 50 28.6 02 25 03 11.5 0.39 0.37 0.09 -94 7.78 4.87 2.42
HE 0247-0418 02 50 23.7 -04 06 11 12.4 0.37 0.09 0.04 101 § § § 6.13 § § § pec
HE 0247-3040 02 49 40.2 -30 28 09 10.2 0.52 0.46 0.02 73 8.64 2.95 3.94
HE 0247-3434 02 49 56.7 -34 22 30 10.4 0.40 0.43 0.02 73 7.16 4.57 2.40
HE 0247-5925 02 48 28.2 -59 12 51 12.7 0.45 0.39 0.04 18 7.05 3.87 2.61
HE 0248-0201 02 51 12.3 02 13 56 12.4 0.51 0.41 0.10 -60 8.75 3.22 4.14
HE 0248-0220 02 51 11.8 -02 08 30 13.0 0.39 0.41 0.06 -68 6.69 4.87 2.14
HE 0248-0422 02 50 41.2 -04 09 56 13.0 0.50 0.42 0.04 -99 7.88 3.16 3.67
HE 0248-0855 02 50 54.6 -08 43 05 11.5 0.38 0.42 0.03 -59 6.49 5.19 1.68
HE 0248-6046 02 49 58.0 -60 34 04 11.1 0.47 0.51 0.02 33 8.50 3.69 3.24
HE 0249-0058 02 51 51.7 01 11 05 12.5 0.43 0.43 0.06 -37 6.88 4.18 2.23
HE 0249-0125 02 52 23.0 01 38 12 12.1 0.47 0.46 0.06 -44 8.07 3.52 3.51
HE 0249-6021 02 50 44.5 -60 09 38 10.9 0.38 0.31 0.02 52 7.06 5.54 2.17
HE 0250-0052 02 52 36.1 01 04 52 12.1 0.62 0.50 0.07 -69 9.56 1.96 4.87
HE 0251-0538 02 54 20.6 -05 26 09 12.5 0.65 0.52 0.05 -35 8.41 1.49 5.76
HE 0251-1153 02 53 52.7 -11 41 24 11.5 0.51 0.57 0.03 -43 7.94 2.90 3.93
HE 0251-5623 02 52 49.0 -56 11 05 8.7 0.40 0.38 0.02 -3 7.33 4.71 2.28
HE 0253-0045 02 56 10.0 -00 33 31 12.2 0.47 0.44 0.06 54 8.10 3.60 3.15
HE 0254-4301 02 56 35.5 -42 49 13 11.7 0.54 0.53 0.01 49 8.53 2.72 3.96
HE 0255-3554 02 57 11.6 -35 42 46 11.2 0.38 0.36 0.02 -36 5.68 5.77 1.50
HE 0256-3311 02 58 51.5 -32 59 58 10.6 0.42 0.44 0.01 18 7.52 4.30 2.39
HE 0256-3902 02 58 49.9 -38 50 58 10.4 0.55 1.01 0.02 17 8.64 2.41 4.33
HE 0257-3250 02 59 30.8 -32 38 52 10.5 § § § 0.37 0.01 62 4.46 7.60 1.34
HE 0258-3501 03 00 35.9 -34 49 40 10.2 0.44 0.47 0.03 21 6.95 3.93 2.56
HE 0259-0209 03 02 23.1 02 21 08 12.7 0.37 0.20 0.10 -30 1.31 5.89 0.30
HE 0259-0719 03 02 22.4 -07 07 18 11.9 0.39 0.44 0.08 32 7.35 4.77 2.17
HE 0259-0727 03 02 23.0 -07 16 10 12.3 0.47 0.51 0.08 -11 8.78 3.53 4.42
HE 0300-5321 03 02 22.2 -53 09 34 10.4 0.47 0.46 0.02 33 8.19 3.73 3.03
HE 0301-5342 03 03 11.9 -53 31 16 31.4 § § § 0.33 0.01 16 4.30 8.24 1.41
HE 0302-0804 03 04 53.8 -07 52 31 11.7 0.47 0.45 0.10 34 8.22 3.74 3.65
HE 0303-0240 03 06 30.9 -02 28 36 11.6 0.55 0.51 0.07 5 8.12 2.26 3.69
HE 0303-0603 03 06 18.6 -05 51 47 11.1 0.43 0.42 0.07 -83 7.62 4.16 2.95
HE 0303-4244 03 05 25.0 -42 32 38 13.5 0.72 0.61 0.01 46 9.63 1.11 5.90
HE 0305-0247 03 08 04.0 -02 36 22 11.4 0.40 0.38 0.06 -28 6.56 4.58 1.90
HE 0305-0309 03 08 00.4 -02 58 02 13.6 0.64 0.57 0.06 -70 9.62 1.66 5.39
HE 0307-0216 03 10 30.3 02 27 52 10.4 0.64 0.48 0.08 84 9.04 1.60 5.06
HE 0308-0001 03 10 41.7 00 09 32 11.1 0.45 0.43 0.10 -46 7.90 3.78 3.10
HE 0309-0849 03 12 20.4 -08 38 11 10.9 0.42 0.41 0.06 64 8.33 4.26 2.74
HE 0309-1207 03 12 22.3 -11 56 39 10.7 0.64 0.51 0.06 -5 9.24 1.68 5.79
HE 0309-1209 03 11 55.5 -11 58 43 9.8 0.44 § § § 0.06 42 8.17 4.21 2.84
HE 0309-1549 03 12 12.0 -15 38 09 12.2 0.45 0.41 0.04 27 7.33 3.93 2.24
HE 0310-3152 03 12 45.7 -31 41 02 10.7 0.53 0.48 0.02 18 8.05 2.69 3.97
HE 0310-6021 03 11 37.7 -60 10 34 11.7 § § § 0.32 0.02 37 5.39 6.95 1.51
HE 0311-3001 03 13 57.4 -29 50 12 10.3 0.61 0.52 0.02 18 9.04 1.82 5.03

-- 55 --
Table 12---Continued
Star name R.A. # B (B - V ) HP2 (B - V ) J-K E (B-V) v rad KP HP2 GP Comm.
HE 0312-0903 03 14 59.4 -08 51 60 12.0 0.43 0.38 0.06 -53 6.99 4.24 2.42
HE 0312-1544 03 15 08.0 -15 33 50 11.8 § § § 0.26 0.04 60 2.55 8.61 1.34 HB
HE 0312-5756 03 13 55.3 -57 45 02 11.9 § § § 0.30 0.02 20 4.57 6.72 1.24
HE 0313-1611 03 16 02.7 -16 00 08 11.8 0.38 0.41 0.04 56 7.49 5.36 2.26
HE 0313-2912 03 15 33.6 -29 01 52 10.4 0.42 0.38 0.02 22 7.81 4.32 3.07
HE 0314-1259 03 17 18.4 -12 48 36 12.3 0.51 0.57 0.06 47 7.82 2.99 3.01
HE 0314-2822 03 16 18.0 -28 11 21 10.7 § § § § § § 0.02 27 0.92 8.02 0.83
HE 0315-0405 03 18 28.3 -03 54 34 11.9 0.38 0.33 0.05 -42 5.69 5.63 1.66
HE 0315-1233 03 18 06.6 -12 22 31 12.1 0.66 0.63 0.06 13 9.13 1.33 5.24
HE 0315-3311 03 17 54.1 -33 00 28 13.6 0.66 0.55 0.02 63 9.21 1.31 5.93
HE 0316-1637 03 18 42.4 -16 26 37 11.7 0.54 0.43 0.07 17 8.77 2.72 3.68
HE 0316-3951 03 18 19.3 -39 40 36 11.7 0.37 0.35 0.02 38 4.88 6.42 1.47
HE 0317-3120 03 19 57.1 -31 09 18 10.0 0.44 0.46 0.02 -13 8.58 4.07 3.18
HE 0317-4219 03 19 03.0 -42 08 37 11.7 0.49 0.42 0.02 18 8.38 3.32 3.52
HE 0318-1506 03 20 25.9 -14 55 27 12.3 0.37 0.33 0.05 52 4.65 5.95 1.17
HE 0318-2642b 03 21 05.1 -26 31 44 11.3 0.40 § § § 0.02 -20 6.61 4.57 1.75
HE 0318-2642f 03 21 05.1 -26 31 44 11.3 0.38 § § § 0.02 -53 6.58 5.08 1.71
HE 0318-3152 03 20 48.3 -31 41 56 10.2 § § § 0.37 0.01 -8 4.51 7.01 1.35
HE 0319-3733 03 21 32.4 -37 22 39 12.0 0.46 0.42 0.02 90 7.65 3.61 3.09
HE 0320-1543 03 22 31.9 -15 33 14 12.3 0.49 0.40 0.04 14 8.48 3.27 3.60
HE 0320-4202 03 22 12.5 -41 52 00 13.1 0.59 0.54 0.01 58 8.44 1.84 4.65
HE 0321-3229 03 23 51.4 -32 18 39 11.6 0.42 0.43 0.02 45 8.21 4.25 2.99
HE 0321-4032 03 23 39.7 -40 22 25 11.9 § § § 0.34 0.02 3 3.34 8.25 1.21
HE 0322-1639 03 25 05.1 -16 28 56 12.3 0.49 0.50 0.04 -6 7.49 3.03 3.54
HE 0322-4040 03 24 08.8 -40 29 51 12.0 0.37 0.37 0.01 1 4.44 6.28 1.03
HE 0322-5932 03 23 53.0 -59 21 57 11.1 § § § 0.30 0.05 18 4.49 8.16 1.46
HE 0323-2030 03 25 36.0 -20 20 02 10.5 0.38 0.13 0.04 111 0.25 4.68 0.01 He
HE 0323-5746 03 24 55.9 -57 36 14 13.0 0.46 0.49 0.06 54 7.50 3.59 3.07
HE 0324-1055 03 26 40.9 -10 45 13 11.4 0.37 0.43 0.06 49 4.46 6.49 1.59
HE 0324-1559 03 27 05.4 -15 49 20 12.8 0.43 0.39 0.04 42 7.10 4.23 2.34
HE 0324-2150 03 26 46.8 -21 40 00 10.0 0.48 0.39 0.03 82 8.14 3.45 3.34
HE 0324-2257 03 26 27.0 -22 47 27 11.5 0.46 0.55 0.03 4 7.73 3.53 3.28
HE 0326-1308 03 28 40.7 -12 57 55 12.0 0.45 0.43 0.06 25 7.35 3.86 2.44
HE 0326-3752 03 28 38.3 -37 42 01 11.5 0.42 0.38 0.02 48 7.31 4.48 2.32
HE 0326-5941 03 27 35.9 -59 31 34 12.0 0.46 0.43 0.05 19 8.40 3.77 2.97
HE 0327-0119 03 30 14.4 01 29 19 12.5 0.38 0.40 0.12 -12 6.53 5.36 1.90
HE 0327-1519 03 29 24.8 -15 08 45 11.9 0.39 0.46 0.08 27 7.36 4.80 2.46
HE 0327-1706 03 30 03.9 -16 55 51 13.3 0.48 0.45 0.05 33 7.75 3.46 3.30
HE 0328-0103 03 30 43.1 01 14 09 12.2 0.45 0.42 0.12 -47 8.20 3.94 3.47
HE 0328-0344 03 31 13.2 -03 34 32 11.6 0.44 0.41 0.05 42 6.64 3.79 2.18
HE 0328-1246 03 30 46.6 -12 36 42 12.0 0.43 0.45 0.06 -20 7.82 4.00 2.86
HE 0328-1322 03 30 41.8 -13 12 10 11.5 0.52 0.43 0.05 11 8.66 2.92 3.95
HE 0328-1346 03 31 08.0 -13 36 25 12.2 0.55 0.46 0.06 -14 9.10 2.57 4.67
HE 0328-3853 03 30 00.2 -38 42 58 12.2 0.40 0.42 0.02 47 5.83 4.66 2.02
HE 0328-3935 03 30 23.3 -39 25 25 11.9 0.55 0.50 0.02 34 9.18 2.57 4.71
HE 0328-4214 03 29 48.8 -42 03 55 12.1 0.40 0.44 0.01 14 5.96 4.55 1.84
HE 0329-1631 03 31 54.8 -16 21 48 14.6 0.37 0.35 0.07 -105 1.24 6.05 § § § HB
HE 0329-2124 03 32 04.7 -21 14 49 9.6 0.37 0.11 0.03 71 0.21 6.27 § § § He
HE 0330-0126 03 33 04.3 01 36 55 11.9 0.50 0.39 0.11 77 8.64 3.18 3.52
HE 0330-0116 03 33 01.5 -01 06 06 11.8 0.49 0.45 0.11 74 8.59 3.30 3.60
HE 0330-1032 03 32 29.4 -10 22 06 12.2 0.52 0.48 0.04 102 7.76 2.55 3.58
HE 0330-4549 03 31 51.5 -45 38 55 10.7 0.40 0.38 0.01 37 6.96 4.67 2.08
HE 0331-1121 03 34 01.8 -11 11 43 11.1 0.42 0.40 0.05 -6 7.06 4.39 2.35
HE 0331-4419 03 33 32.1 -44 09 00 11.6 0.71 0.60 0.01 37 9.15 1.08 5.92
HE 0333-3750 03 35 31.6 -37 40 45 12.0 0.38 0.37 0.02 -16 5.32 5.75 1.32
HE 0333-4220 03 35 25.8 -42 10 43 11.7 § § § 0.31 0.01 26 4.62 7.05 1.36
HE 0334-2157 03 37 08.2 -21 47 21 9.8 0.46 0.42 0.03 17 8.72 3.96 3.59
HE 0334-2822 03 36 14.9 -28 12 43 10.3 0.48 0.39 0.01 63 7.95 3.47 3.45
HE 0335-1115 03 37 24.5 -11 05 34 10.9 0.45 0.41 0.06 14 8.08 3.86 3.17
HE 0336-0001 03 39 18.8 00 10 52 12.0 0.62 0.53 0.11 -84 9.40 1.95 5.36
HE 0336-4234 03 37 57.1 -42 24 44 10.9 0.39 0.38 0.01 3 6.63 4.98 1.92
HE 0336-4243 03 37 55.9 -42 33 38 11.0 0.42 0.40 0.01 -18 7.75 4.42 2.32
HE 0336-4858 03 38 04.5 -48 48 57 9.8 § § § 0.36 0.01 5 3.20 8.65 1.19
HE 0337-3204 03 39 31.1 -31 54 32 10.5 0.56 0.53 0.01 11 8.93 2.43 4.56
HE 0337-5145 03 39 09.2 -51 36 10 10.6 0.40 0.43 0.01 16 7.41 4.60 2.22
HE 0338-1418 03 41 09.1 -14 09 24 11.5 0.37 0.31 0.06 29 4.01 6.15 1.23
HE 0339-0151 03 42 07.1 02 01 03 13.1 0.59 0.49 0.11 -25 8.01 1.85 5.26

-- 56 --
Table 12---Continued
Star name R.A. # B (B - V ) HP2 (B - V ) J-K E (B-V) v rad KP HP2 GP Comm.
HE 0339-3944 03 41 02.3 -39 34 48 12.7 0.48 0.49 0.01 26 7.82 3.36 3.27
HE 0339-4132 03 41 05.2 -41 22 30 11.9 0.47 0.44 0.01 57 8.49 3.52 3.49
HE 0339-4348 03 41 16.4 -43 38 33 11.0 0.55 0.50 0.01 36 8.67 2.38 4.53
HE 0340-0018 03 42 39.2 00 28 07 12.7 0.45 0.43 0.10 -62 8.23 3.77 3.15
HE 0340-0306 03 43 08.0 -02 56 55 11.6 0.39 0.40 0.08 -22 7.41 5.06 2.23
HE 0341-1308 03 43 35.3 -12 58 55 10.8 0.49 0.42 0.08 66 7.58 3.02 3.74
HE 0341-4109 03 42 47.1 -41 00 07 13.8 0.61 0.58 0.01 84 9.14 1.77 5.12
HE 0341-5147 03 42 30.8 -51 38 17 9.8 0.41 0.39 0.01 -2 8.13 4.54 2.63
HE 0342-0525 03 44 39.3 -05 15 44 11.2 0.64 0.50 0.06 11 9.32 1.57 5.36
HE 0342-0808 03 45 16.3 -07 59 21 11.1 0.49 0.43 0.07 -32 7.28 3.08 3.27
HE 0342-4125 03 44 28.4 -41 16 15 11.7 0.40 0.39 0.01 25 7.37 4.66 2.31
HE 0342-4719 03 43 38.0 -47 10 05 9.7 0.38 0.33 0.01 -16 6.40 5.42 1.55
HE 0342-5024 03 44 14.3 -50 14 39 10.6 0.42 0.42 0.01 23 7.48 4.33 2.54
HE 0342-5106 03 44 07.5 -50 56 45 10.4 0.48 0.40 0.01 30 8.24 3.43 3.33
HE 0343-0612 03 45 54.7 -06 03 39 11.3 0.63 0.54 0.07 -77 8.80 1.56 5.04
HE 0344-0124 03 46 36.5 -01 14 52 13.2 0.66 0.44 0.14 -36 9.07 1.43 5.45
HE 0344-0207 03 47 23.1 -01 58 16 12.9 1.00 1.18 0.12 0 § § § § § § 1.43 Em
HE 0344-0906 03 47 18.3 -08 57 17 11.0 0.69 0.50 0.08 34 8.22 1.14 5.36
HE 0344-3740 03 46 10.5 -37 31 07 10.7 0.61 0.46 0.01 69 9.22 1.93 4.94
HE 0344-4934 03 46 06.8 -49 25 39 10.6 0.58 0.49 0.01 14 9.25 2.49 4.72
HE 0344-5031 03 46 02.6 -50 22 30 10.2 0.47 0.44 0.01 24 8.08 3.74 3.01
HE 0345-0120 03 47 43.8 01 29 43 12.3 0.37 0.33 0.21 -20 4.77 6.47 1.33
HE 0345-0230 03 47 32.0 -02 21 23 11.7 0.39 0.42 0.14 -18 6.97 4.75 2.26
HE 0345-2345 03 47 43.7 -23 36 29 10.7 0.38 0.36 0.02 27 6.62 5.90 1.93
HE 0346-0226 03 49 05.7 02 35 53 12.1 0.58 0.45 0.19 -27 9.22 2.40 4.75
HE 0346-3803 03 48 37.7 -37 54 46 11.2 0.49 0.46 0.01 47 8.45 3.38 3.18
HE 0347-2940 03 49 07.1 -29 31 51 13.8 1.00 1.17 0.01 88 § § § § § § 4.37 Em
HE 0347-3947 03 48 59.8 -39 38 24 11.3 0.38 0.45 0.01 26 6.48 5.37 1.81
HE 0347-5026 03 48 31.3 -50 16 58 11.3 0.40 0.41 0.01 84 6.98 4.68 2.26
HE 0349-0255 03 51 36.0 -02 46 20 12.2 0.45 0.39 0.13 -45 7.77 3.82 2.99
HE 0349-0511 03 51 42.5 -05 02 32 11.2 0.66 0.45 0.11 24 9.18 1.35 5.82
HE 0349-1223 03 51 31.1 -12 14 28 11.1 0.40 0.39 0.05 -22 6.94 4.66 2.19
HE 0349-2353 03 52 00.3 -23 44 23 11.8 0.38 0.40 0.04 55 7.15 5.10 1.83
HE 0349-3211 03 51 42.4 -32 02 26 11.6 0.53 0.53 0.01 47 8.24 2.61 3.81
HE 0349-3950 03 51 21.2 -39 41 13 11.3 0.50 0.46 0.01 18 7.99 3.20 3.39
HE 0352-4007 03 54 42.0 -39 58 45 11.3 0.61 0.52 0.01 18 9.01 1.89 4.82
HE 0352-4216 03 54 25.5 -42 07 30 11.5 0.47 0.40 0.01 -0 8.25 3.59 3.48
HE 0355-2849 03 57 24.8 -28 40 34 11.5 0.62 0.51 0.01 -0 9.51 1.78 5.37
HE 0355-4856 03 57 22.1 -48 47 58 10.7 § § § 0.37 0.01 22 4.17 7.26 1.36
HE 0356-4627 03 57 52.6 -46 18 38 10.5 0.40 0.42 0.01 30 7.46 4.72 2.37
HE 0356-5218 03 57 32.9 -52 10 21 10.9 0.45 0.45 0.01 16 7.68 3.97 2.73
HE 0357-4237 03 59 07.8 -42 29 12 11.1 0.53 0.45 0.00 45 8.84 2.91 4.29
HE 0358-2943 04 00 29.4 -29 35 02 12.0 § § § 0.35 0.01 41 4.96 6.82 1.51
HE 0358-3510 04 00 27.8 -35 01 54 13.7 0.78 0.65 0.00 65 9.79 0.86 5.76
HE 0358-4629 04 00 01.9 -46 21 26 11.4 0.72 0.66 0.01 42 9.65 1.10 5.80
HE 0359-3107 04 01 44.4 -30 58 44 11.6 0.53 0.50 0.01 24 8.41 2.63 3.93
HE 0400-2754 04 02 22.5 -27 46 32 11.1 0.39 0.42 0.01 23 7.44 4.86 2.64
HE 0400-2806 04 02 32.7 -27 57 49 11.8 0.43 0.40 0.01 66 6.83 4.12 2.16
HE 0400-5015 04 01 50.4 -50 07 29 10.7 0.50 0.50 0.01 3 8.23 3.00 3.55
HE 0401-0153 04 03 42.5 02 01 37 12.6 § § § 0.38 0.38 -20 4.01 8.25 1.31
HE 0401-5937 04 02 39.4 -59 29 10 11.6 § § § 0.31 0.02 -6 3.93 8.08 1.14
HE 0404-0122 04 06 49.6 01 30 51 12.1 0.47 0.54 0.29 -29 8.45 3.66 3.58
HE 0404-0214 04 07 33.7 02 22 40 12.4 0.38 0.41 0.30 -54 6.10 6.36 1.63
HE 0404-0759 04 06 32.2 -07 51 23 11.8 0.42 0.40 0.07 30 7.52 4.32 2.50
HE 0404-0846 04 07 03.7 -08 38 40 11.9 0.63 0.64 0.04 89 8.76 1.70 5.21
HE 0404-2602 04 06 43.9 -25 54 28 11.5 § § § 0.34 0.05 32 1.86 6.82 1.46
HE 0404-3959 04 06 13.8 -39 51 09 10.9 0.42 0.44 0.01 9 7.09 4.26 2.50
HE 0406-0236 04 09 08.0 02 44 17 13.2 § § § 0.35 0.26 31 5.99 7.07 1.77
HE 0406-0015 04 09 27.8 -00 07 41 11.6 0.37 0.36 0.16 -52 3.32 5.69 1.66
HE 0406-0133A 04 09 20.0 -01 25 13 10.9 0.56 0.40 0.11 248 7.98 2.07 4.75
HE 0406-0133 04 09 20.0 -01 25 13 10.9 0.46 § § § 0.11 -100 8.41 3.97 2.95
HE 0406-2201 04 08 25.2 -21 53 47 9.5 § § § 0.28 0.04 42 4.09 8.98 1.18
HE 0406-2203 04 08 38.8 -21 56 05 10.7 0.43 0.41 0.04 62 6.60 4.04 2.05
HE 0406-6120 04 07 15.1 -61 13 02 11.5 § § § 0.33 0.02 -32 3.93 7.76 1.23
HE 0407-1751 04 09 31.1 -17 43 22 11.0 0.38 0.41 0.02 40 6.57 5.00 1.92
HE 0408-0513 04 11 15.6 -05 05 54 12.2 0.53 0.45 0.07 4 8.92 2.77 4.41
HE 0408-0559 04 10 57.0 -05 51 37 12.0 0.55 0.45 0.09 37 8.12 2.46 3.98

-- 57 --
Table 12---Continued
Star name R.A. # B (B - V ) HP2 (B - V ) J-K E (B-V) v rad KP HP2 GP Comm.
HE 0408-1003 04 10 26.2 -09 56 00 12.2 0.39 0.36 0.06 -48 7.63 5.05 1.97
HE 0409-0126 04 12 29.4 01 33 48 12.1 0.55 0.55 0.21 31 8.43 2.40 4.50
HE 0409-0006 04 12 18.3 00 01 31 12.0 0.65 0.55 0.17 -39 8.64 1.35 5.25
HE 0409-0307 04 11 30.6 -03 00 17 12.9 0.45 0.42 0.06 45 7.79 3.87 2.91
HE 0410-2429 04 12 43.1 -24 22 24 10.9 0.39 0.75 0.05 8 4.61 4.54 4.08 comp
HE 0411-0830 04 13 35.1 -08 23 02 12.0 0.55 0.49 0.07 -30 8.67 2.42 4.33
HE 0411-1125 04 13 52.0 -11 18 03 12.2 0.83 0.57 0.05 33 8.51 0.52 6.15
HE 0411-1946 04 14 02.9 -19 39 01 10.0 0.38 0.37 0.03 71 7.45 5.31 2.29
HE 0412-0212 04 14 38.9 02 20 14 11.2 0.40 0.37 0.16 13 6.37 4.68 1.85
HE 0412-1408 04 14 36.9 -14 01 10 10.2 0.39 0.43 0.05 54 7.51 4.79 2.01
HE 0412-3948 04 13 54.6 -39 40 53 10.2 0.45 0.40 0.02 3 7.50 3.77 2.77
HE 0412-4018 04 13 53.0 -40 10 58 10.7 0.48 0.48 0.01 -2 7.97 3.43 3.25
HE 0412-5308 04 13 51.5 -53 00 51 10.9 0.62 0.50 0.02 53 9.25 1.89 5.16
HE 0413-3450 04 15 15.5 -34 43 16 12.2 0.55 1.07 0.01 8 1.02 2.09 3.16 dist
HE 0414-0157 04 16 46.3 02 05 07 11.2 0.38 0.35 0.14 -42 6.91 5.07 1.95
HE 0414-0213 04 17 24.6 -02 05 49 11.3 0.42 0.37 0.10 57 7.92 4.38 2.25
HE 0414-3950 04 16 13.3 -39 43 18 10.4 0.49 0.45 0.02 -17 8.66 3.41 3.76
HE 0414-4943 04 16 02.0 -49 36 37 11.6 0.47 0.41 0.01 23 8.31 3.61 3.13
HE 0415-2042 04 18 03.1 -20 35 28 9.7 § § § 0.29 0.05 49 3.55 8.95 1.21
HE 0415-5004 04 16 32.2 -49 57 09 10.8 0.64 0.51 0.02 25 9.29 1.73 5.52
HE 0415-5125 04 16 53.4 -51 18 39 10.9 0.61 0.57 0.01 11 9.06 1.93 5.18
HE 0415-5131 04 16 28.8 -51 23 56 11.1 0.46 0.46 0.01 7 8.46 3.81 3.47
HE 0415-5206 04 16 24.7 -51 58 41 10.9 0.47 0.45 0.01 6 8.26 3.50 3.50
HE 0416-1619 04 18 25.6 -16 12 45 11.6 0.39 0.39 0.04 44 6.75 4.86 2.00
HE 0416-1842 04 18 15.9 -18 35 10 9.9 0.40 0.37 0.04 16 7.55 4.62 2.48
HE 0416-2604 04 18 24.6 -25 57 14 11.6 0.42 0.41 0.04 91 7.19 4.28 2.09
HE 0416-2811 04 18 50.3 -28 04 31 11.3 0.66 0.55 0.04 -11 9.19 1.46 5.62
HE 0416-2821 04 18 39.7 -28 14 35 11.6 0.47 0.42 0.04 18 8.37 3.71 3.42
HE 0416-4114 04 17 48.6 -41 07 31 11.0 0.38 0.41 0.02 -14 5.86 5.30 1.59
HE 0418-0229 04 21 02.0 02 36 05 11.9 0.43 0.34 0.16 20 6.37 4.22 1.75
HE 0418-2608 04 20 24.8 -26 01 39 13.8 0.71 0.63 0.05 82 9.09 1.21 5.52
HE 0419-0242 04 22 03.9 -02 35 49 12.5 0.41 0.46 0.05 -55 6.39 4.42 2.15
HE 0419-1011 04 22 14.6 -10 04 32 11.7 0.46 0.44 0.08 94 6.67 3.52 2.77
HE 0419-2012 04 21 37.7 -20 05 25 10.2 § § § 0.39 0.03 68 3.77 7.10 1.48
HE 0420-0154 04 22 48.7 02 01 20 11.7 0.59 0.45 0.15 70 8.28 1.94 4.13
HE 0420-0740 04 23 06.3 -07 33 32 12.0 0.47 0.38 0.08 -39 8.00 3.64 3.25
HE 0420-1309 04 23 17.2 -13 02 41 11.1 § § § 0.34 0.05 -21 3.73 7.14 1.21
HE 0420-2744 04 22 53.0 -27 37 60 13.5 0.40 0.36 0.05 66 6.21 4.67 1.71
HE 0420-3913 04 22 09.3 -39 07 00 10.4 0.52 § § § 0.02 34 8.66 2.90 3.61
HE 0421-0108 04 24 19.7 01 15 08 10.9 0.63 0.52 0.12 98 8.75 1.52 5.37
HE 0421-0305 04 23 38.9 -02 58 57 13.3 0.46 0.44 0.06 84 7.89 3.64 3.25
HE 0421-5122 04 22 46.6 -51 15 18 12.1 0.43 § § § 0.01 82 7.46 4.10 3.00
HE 0422-0216 04 25 08.5 02 23 42 11.6 0.46 0.33 0.17 55 7.47 3.68 2.35
HE 0422-0124 04 24 55.2 -01 17 34 11.7 0.55 0.42 0.11 -13 8.18 2.30 3.51
HE 0422-3942 04 23 51.6 -39 35 54 10.5 0.38 0.42 0.03 27 6.94 5.08 2.08
HE 0422-4205 04 23 49.3 -41 58 58 9.5 0.38 0.32 0.03 8 5.80 5.50 1.66
HE 0422-5409 04 23 59.7 -54 02 52 11.6 0.43 0.46 0.01 32 7.82 4.22 2.71
HE 0423-3142 04 25 26.8 -31 35 57 10.6 0.44 0.47 0.03 32 6.74 3.85 3.06
HE 0424-0006 04 27 13.5 00 12 53 11.4 0.71 0.55 0.08 1 9.42 1.24 5.80
HE 0424-0236 04 26 41.2 02 42 45 11.0 0.42 0.36 0.23 50 8.79 4.38 2.98
HE 0424-0728 04 26 29.3 -07 21 44 11.9 0.50 0.46 0.06 -18 8.74 3.05 3.83
HE 0424-0855 04 26 46.5 -08 49 01 11.4 0.53 0.41 0.15 52 8.93 2.75 4.44
HE 0424-1319 04 26 34.8 -13 12 38 10.9 0.39 0.43 0.08 -14 6.48 4.79 1.85
HE 0424-1340 04 27 14.2 -13 33 27 11.3 0.42 0.40 0.08 -16 7.45 4.36 2.23
HE 0424-4050 04 26 27.0 -40 43 50 10.2 0.38 0.39 0.03 30 6.96 5.29 1.87
HE 0424-5628 04 25 45.6 -56 21 50 10.3 § § § 0.29 0.02 50 5.68 6.97 1.41
HE 0425-0226 04 28 21.0 02 32 54 10.8 0.39 0.36 0.19 42 6.03 4.93 1.48
HE 0425-2257 04 27 08.2 -22 50 23 11.7 0.45 0.46 0.04 24 8.02 3.87 2.86
HE 0425-3340 04 27 39.2 -33 33 44 10.7 0.45 § § § 0.03 30 8.13 3.88 3.29
HE 0426-0620 04 28 32.3 -06 13 55 12.6 0.51 0.43 0.06 38 8.92 3.16 4.31
HE 0426-1447 04 29 07.9 -14 40 57 11.4 0.38 0.30 0.08 8 6.02 5.78 1.65
HE 0426-1532 04 29 14.2 -15 25 55 12.1 0.62 0.53 0.05 67 10.19 1.96 5.23
HE 0427-0159 04 30 07.1 02 05 53 11.3 § § § 0.32 0.15 10 5.42 6.83 1.63
HE 0427-0104 04 29 49.0 -00 58 03 11.1 0.39 0.44 0.05 3 7.00 4.78 2.15
HE 0427-1550 04 29 43.7 -15 43 53 10.8 § § § 0.42 0.05 51 5.48 6.81 1.51
HE 0428-0237 04 31 01.3 02 44 20 11.8 0.37 0.36 0.18 56 3.40 5.47 0.91
HE 0428-1404 04 30 27.3 -13 58 08 12.3 0.43 0.43 0.12 80 6.60 4.06 2.16

-- 58 --
Table 12---Continued
Star name R.A. # B (B - V ) HP2 (B - V ) J-K E (B-V) v rad KP HP2 GP Comm.
HE 0428-3728 04 30 38.2 -37 22 18 10.3 0.38 0.39 0.02 59 5.82 5.02 1.42
HE 0429-0556 04 32 04.3 -05 50 28 12.0 0.49 0.42 0.05 -24 8.94 3.47 3.76
HE 0429-0831 04 32 06.9 -08 25 12 11.5 0.42 0.39 0.11 -33 7.41 4.47 2.23
HE 0429-1437 04 31 38.0 -14 31 38 12.1 0.39 0.51 0.25 20 6.40 4.84 1.90
HE 0429-1551 04 31 33.1 -15 45 07 10.2 0.38 0.39 0.08 27 6.65 5.28 2.17
HE 0429-3824 04 31 35.7 -38 18 34 10.1 0.46 0.50 0.02 7 7.79 3.66 2.97
HE 0429-4149 04 31 06.0 -41 43 31 10.1 0.77 0.63 0.03 75 9.39 0.96 5.82
HE 0430-0231 04 32 35.5 -02 25 26 12.0 0.50 0.46 0.06 -55 8.53 3.17 4.10
HE 0430-0612 04 33 04.4 -06 05 49 13.2 0.42 0.42 0.06 62 7.22 4.43 2.42
HE 0430-1034 04 32 45.5 -10 27 55 11.9 0.63 0.53 0.06 22 8.98 1.64 5.55
HE 0430-2502 04 32 36.5 -24 56 28 11.4 0.54 0.43 0.05 23 8.91 2.70 4.19
HE 0430-4413 04 31 56.6 -44 06 59 11.0 0.46 0.53 0.01 13 8.38 3.79 3.13
HE 0430-4418 04 31 36.8 -44 12 13 10.9 0.61 0.53 0.01 -46 9.20 1.77 5.30
HE 0431-5040 04 33 01.9 -50 34 46 10.8 0.64 0.53 0.01 69 9.40 1.66 5.56
HE 0432-1224 04 35 09.1 -12 18 30 10.5 0.54 0.42 0.05 4 8.76 2.65 4.15
HE 0432-2255 04 34 52.3 -22 49 02 11.2 0.38 0.37 0.06 -30 5.42 5.80 1.35
HE 0432-3009 04 34 37.5 -30 03 10 11.0 0.56 0.52 0.03 1 8.95 2.32 4.70
HE 0433-1239 04 36 06.5 -12 33 49 11.2 0.46 0.44 0.07 -73 7.17 3.71 2.47
HE 0433-1442 04 35 40.9 -14 36 34 12.0 0.39 0.58 0.50 111 7.39 4.77 2.34
HE 0433-1504 04 35 39.1 -14 58 45 11.3 0.52 0.41 0.33 7 8.60 2.90 4.10
HE 0433-3938 04 35 15.4 -39 32 27 10.0 0.50 0.48 0.02 41 8.49 3.18 4.01
HE 0435-2144 04 37 25.0 -21 38 42 9.8 0.40 0.41 0.04 39 7.74 4.54 2.80
HE 0435-3601 04 37 43.5 -35 55 14 10.8 0.40 0.43 0.03 69 6.94 4.52 2.29
HE 0435-4121 04 36 55.0 -41 15 42 10.1 0.43 0.40 0.02 21 6.77 4.07 2.63
HE 0435-4456 04 37 00.1 -44 50 27 10.5 0.43 0.42 0.01 -5 7.17 4.03 2.37
HE 0435-4952 04 37 18.8 -49 46 15 10.8 0.38 0.39 0.01 34 6.75 5.01 1.92
HE 0436-5432 04 37 11.7 -54 26 11 13.3 0.42 0.39 0.01 65 7.10 4.28 2.30
HE 0437-1331b 04 39 57.8 -13 25 37 11.8 0.64 § § § 0.16 -10 9.16 1.74 5.10
HE 0437-1331f 04 39 57.8 -13 25 37 11.8 0.49 § § § 0.16 2 8.84 3.31 3.84
HE 0437-5448 04 38 50.1 -54 43 00 12.6 0.37 0.38 0.01 26 4.81 5.62 1.25
HE 0438-4701 04 40 12.2 -46 55 31 11.5 0.62 0.47 0.01 -12 8.71 1.73 5.03
HE 0438-5549 04 39 16.2 -55 43 54 10.7 0.45 0.44 0.01 -28 7.94 3.80 3.07
HE 0439-0254 04 42 13.5 -02 48 59 12.1 0.60 0.47 0.04 25 10.78 2.05 4.96
HE 0439-1323 04 42 13.1 -13 18 02 12.9 § § § 0.36 0.20 -27 5.89 6.84 1.58
HE 0439-2749 04 41 47.5 -27 43 55 11.6 0.50 0.49 0.04 58 8.42 3.16 3.88
HE 0439-5137 04 40 18.0 -51 32 05 11.0 0.45 0.39 0.01 -23 8.23 3.80 3.05
HE 0440-0312 04 43 05.7 -03 07 21 12.1 0.47 0.44 0.03 -78 8.46 3.55 3.68
HE 0440-0759A 04 42 35.9 -07 54 16 13.0 0.48 0.40 0.10 -12 7.65 3.45 3.13
HE 0440-0759 04 42 35.9 -07 54 16 13.0 0.43 § § § 0.10 -9 7.22 4.19 2.79
HE 0440-2625 04 42 24.3 -26 19 41 11.4 0.37 0.35 0.03 7 4.37 6.37 1.12
HE 0440-3350 04 42 49.9 -33 44 34 11.0 0.39 0.34 0.02 -1 7.80 4.87 2.36
HE 0440-5149 04 41 29.6 -51 43 32 11.0 0.38 0.37 0.01 -56 6.74 5.06 1.94
HE 0441-2007 04 43 38.6 -20 02 08 10.4 0.46 0.36 0.04 -48 8.48 3.78 3.86
HE 0441-4737 04 43 23.7 -47 31 48 10.5 0.42 0.40 0.01 -23 8.19 4.42 2.81
HE 0441-4828 04 42 38.7 -48 22 34 10.9 0.62 0.54 0.01 -14 8.74 1.65 5.46
HE 0442-0320 04 44 30.8 -03 14 38 12.1 0.50 0.43 0.04 -90 8.10 3.18 3.61
HE 0442-1247 04 44 49.5 -12 42 28 12.2 0.47 0.45 0.13 12 8.36 3.59 3.16
HE 0442-3336 04 44 21.9 -33 31 02 10.9 0.66 0.64 0.02 -43 8.85 1.44 5.56
HE 0444-1242 04 46 36.2 -12 37 17 11.2 0.43 0.41 0.17 1 7.64 4.18 3.14
HE 0444-4811 04 46 07.3 -48 06 32 11.2 0.38 0.40 0.01 58 6.64 5.21 1.91
HE 0444-4832 04 45 43.3 -48 27 00 10.7 0.39 0.41 0.01 -23 8.39 4.79 3.06
HE 0445-0321 04 48 08.4 -03 15 48 12.0 0.38 0.38 0.06 -43 6.34 5.01 2.16
HE 0445-1508 04 47 21.3 -15 02 49 11.0 § § § 0.28 0.06 -21 4.96 6.74 1.37
HE 0445-2814 04 47 56.3 -28 09 35 10.5 0.59 0.51 0.03 -9 8.58 1.86 4.60
HE 0445-2852 04 47 48.7 -28 46 46 10.4 0.38 0.40 0.02 54 5.53 6.45 1.63
HE 0445-3045 04 47 46.0 -30 39 50 10.6 0.40 0.39 0.02 47 6.76 4.71 2.46
HE 0445-3547 04 47 16.1 -35 41 51 9.7 § § § 0.33 0.01 -0 1.79 6.88 1.52
HE 0446-0630 04 49 10.5 -06 24 58 12.4 0.42 0.37 0.07 16 7.37 4.47 2.46
HE 0446-4618 04 47 31.5 -46 13 12 11.0 0.38 0.39 0.01 49 6.59 5.22 2.25
HE 0446-4722 04 48 18.3 -47 16 57 11.5 0.37 0.40 0.01 28 4.95 5.59 1.71
HE 0446-5527 04 47 55.6 -55 22 18 13.8 0.78 1.05 0.01 39 § § § 0.77 5.42 Em
HE 0447-0813 04 50 16.2 -08 08 15 11.8 0.38 0.38 0.06 68 7.54 5.31 2.57
HE 0448-0917 04 50 33.0 -09 12 04 11.5 § § § 0.32 0.06 -10 4.43 7.09 1.44
HE 0449-2433 04 51 22.4 -24 28 52 11.0 § § § 0.30 0.03 40 4.44 7.39 1.36
HE 0450-0357 04 52 30.2 -03 52 43 12.9 0.54 0.43 0.05 34 8.97 2.74 4.43
HE 0450-1345 04 52 40.5 -13 40 32 11.5 0.41 0.39 0.09 38 7.96 4.52 2.76
HE 0452-1711 04 54 35.8 -17 06 45 10.0 0.38 0.35 0.06 33 5.99 5.42 1.67

-- 59 --
Table 12---Continued
Star name R.A. # B (B - V ) HP2 (B - V ) J-K E (B-V) v rad KP HP2 GP Comm.
HE 0452-2506 04 54 06.6 -25 01 49 14.2 0.92 0.70 0.03 131 10.37 0.37 5.59
HE 0452-3133 04 54 27.9 -31 28 30 10.4 0.38 0.36 0.02 -12 6.57 5.57 1.97
HE 0453-4317 04 54 53.4 -43 13 02 11.4 0.53 0.49 0.01 104 8.43 2.61 3.93
HE 0453-4633 04 55 15.6 -46 28 44 12.1 0.45 0.44 0.02 -64 7.26 3.91 2.82
HE 0454-2109 04 56 46.1 -21 05 02 10.9 0.38 0.36 0.04 33 6.17 5.48 2.13
HE 0454-3629 04 56 35.8 -36 25 03 10.8 0.60 0.59 0.01 -30 8.92 1.75 5.29
HE 0454-4142 04 56 23.3 -41 37 29 10.7 0.67 0.59 0.01 -16 9.35 1.31 5.86
HE 0454-4634 04 55 54.2 -46 29 37 11.5 0.49 0.49 0.02 -8 7.39 3.23 2.97
HE 0454-5651 04 55 15.3 -56 46 25 11.0 0.55 0.45 0.01 -33 9.20 2.53 4.72
HE 0455-3157 04 57 15.3 -31 53 05 10.4 0.64 0.59 0.02 7 9.07 1.63 5.38
HE 0456-4723 04 58 07.0 -47 19 15 10.8 0.38 0.43 0.02 31 6.21 5.06 1.92
HE 0457-3209 04 59 47.1 -32 04 40 10.3 0.47 0.55 0.02 -19 8.23 3.63 3.62
HE 0457-4439 04 59 25.1 -44 34 56 11.2 0.38 0.38 0.01 16 6.02 5.77 1.82
HE 0458-2906 05 00 26.5 -29 02 15 10.7 0.65 0.52 0.01 13 8.65 1.37 4.97
HE 0458-4631 04 59 44.1 -46 27 30 11.2 0.38 0.31 0.02 4 6.71 5.67 1.79
HE 0459-3431 05 01 17.9 -34 26 51 10.8 0.56 0.55 0.02 44 8.89 2.30 4.89
HE 0500-3145 05 02 18.2 -31 41 43 10.2 0.84 0.69 0.01 -5 10.42 0.53 5.79
HE 0500-3159 05 02 46.7 -31 55 33 13.8 0.76 0.54 0.02 59 9.14 0.80 6.05
HE 0502-3159 05 03 58.7 -31 55 50 10.5 0.38 0.36 0.02 12 5.95 5.77 1.64
HE 0503-4342 05 04 59.8 -43 38 42 11.3 0.37 0.38 0.01 99 4.59 6.28 1.43
HE 0504-3103 05 05 57.9 -30 59 25 10.2 § § § 0.30 0.01 64 3.42 7.62 1.58
HE 0504-5622 05 05 28.4 -56 18 09 10.1 § § § 0.36 0.01 10 3.22 8.45 1.17
HE 0505-1651 05 08 02.5 -16 47 39 10.4 0.40 0.36 0.06 16 7.05 4.63 2.10
HE 0505-2249 05 07 43.7 -22 45 12 11.4 0.40 0.41 0.03 49 6.64 4.55 1.99
HE 0505-4724 05 06 42.7 -47 20 31 10.8 0.48 0.44 0.01 -30 7.47 3.43 3.40
HE 0506-3035 05 08 08.2 -30 31 44 11.0 0.57 0.55 0.02 39 8.43 2.17 4.51
HE 0506-3207 05 08 46.9 -32 03 39 10.0 0.43 0.38 0.02 48 7.63 4.09 2.87
HE 0506-5629 05 06 57.4 -56 26 01 § § § § § § 0.38 0.02 14 4.94 6.65 1.39
HE 0507-1714 05 09 20.4 -17 10 57 10.1 0.50 0.45 0.07 -6 8.16 3.02 3.62
HE 0507-5241 05 09 02.1 -52 37 44 12.0 0.37 0.39 0.02 -28 4.40 5.84 1.15
HE 0508-2246 05 10 54.4 -22 42 39 12.7 0.44 0.42 0.03 78 8.34 4.18 3.45
HE 0508-2936 05 10 18.9 -29 33 03 11.5 0.46 0.39 0.01 40 8.30 3.95 0.00
HE 0508-3822 05 10 39.2 -38 18 41 12.3 § § § 0.30 0.04 85 4.42 7.97 1.42
HE 0509-2041 05 12 07.6 -20 38 24 10.8 0.39 0.38 0.04 0 7.65 4.79 2.39
HE 0509-3053 05 10 57.6 -30 50 04 10.9 0.62 0.56 0.02 52 8.65 1.59 4.85
HE 0509-5543 05 10 15.4 -55 39 39 11.1 0.40 0.42 0.02 52 7.18 4.58 2.51
HE 0510-2958 05 12 16.9 -29 55 11 11.5 0.55 0.51 0.03 21 9.15 2.72 4.30
HE 0510-3311 05 12 15.1 -33 08 07 13.7 0.45 0.44 0.02 45 7.52 3.81 2.76
HE 0510-4756 05 11 44.6 -47 53 27 11.4 0.38 0.38 0.02 3 6.45 5.64 1.75
HE 0511-4835 05 12 49.1 -48 31 35 10.5 0.59 0.47 0.02 10 8.50 1.99 4.21
HE 0511-5448 05 12 54.1 -54 45 00 11.1 0.61 0.50 0.02 51 9.15 1.99 4.67
HE 0512-3335 05 14 15.4 -33 32 10 12.1 0.51 0.52 0.03 -37 7.52 2.92 3.50
HE 0513-5025 05 14 38.6 -50 21 50 11.6 0.54 0.50 0.02 127 7.98 2.35 4.11
HE 0513-5605 05 14 22.5 -56 01 46 11.7 0.54 0.49 0.02 47 8.87 2.74 4.68
HE 0514-2040 05 16 21.4 -20 37 40 10.3 § § § 0.31 0.04 11 4.30 7.85 1.44
HE 0514-3410 05 16 40.8 -34 07 08 10.9 0.37 0.37 0.03 33 3.66 5.83 1.65
HE 0514-4446 05 15 45.8 -44 43 01 10.8 § § § 0.34 0.03 26 5.63 6.54 1.48
HE 0514-5056 05 15 27.8 -50 53 03 10.9 0.38 0.36 0.02 -2 6.20 5.39 2.27
HE 0514-5206 05 15 43.5 -52 03 33 10.6 0.41 0.38 0.01 44 6.82 4.42 2.22
HE 0515-2208 05 17 11.9 -22 05 10 10.9 0.55 0.43 0.04 -8 8.47 2.25 4.09
HE 0515-2257 05 18 05.3 -22 54 00 11.6 0.38 0.32 0.04 60 6.56 5.33 1.81
HE 0516-2447 05 18 18.3 -24 44 34 11.2 0.38 0.37 0.03 -23 6.32 5.10 1.71
HE 0516-4702 05 17 40.3 -46 59 39 11.2 0.45 0.44 0.02 30 7.82 3.79 3.19
HE 0518-4658 05 20 09.2 -46 55 12 11.7 0.41 0.45 0.03 11 7.75 4.53 2.53
HE 0518-5717 05 19 45.0 -57 14 52 11.0 0.54 0.52 0.03 12 8.74 2.53 4.27
HE 0519-4548 05 20 59.8 -45 46 07 11.7 § § § 0.31 0.05 38 6.24 6.82 1.96
HE 0519-4603 05 20 52.4 -46 00 41 10.9 0.38 0.33 0.03 18 6.84 6.08 1.77
HE 0520-2150 05 22 42.6 -21 47 49 10.0 § § § 0.29 0.04 45 5.45 8.06 1.69
HE 0520-4455 05 22 04.5 -44 52 21 13.1 0.66 0.62 0.03 -7 9.11 1.45 5.64
HE 0520-5617 05 21 17.4 -56 14 32 8.7 § § § § § § 0.03 22 5.27 8.47 1.38
HE 0521-3733 05 23 42.2 -37 31 11 12.1 0.46 0.47 0.04 16 8.52 3.84 3.38
HE 0521-3926 05 23 10.0 -39 23 43 10.7 0.51 0.47 0.02 96 9.03 3.10 4.40
HE 0522-5638 05 23 14.2 -56 35 50 11.4 0.38 0.46 0.04 46 7.19 5.00 2.27
HE 0523-3235 05 25 32.2 -32 33 21 11.1 0.45 0.42 0.02 -11 7.50 3.94 2.68
HE 0523-3615 05 24 52.8 -36 12 39 10.7 0.42 0.45 0.04 -28 7.38 4.32 2.65
HE 0523-5725 05 24 25.3 -57 22 56 11.0 0.38 0.42 0.03 -5 6.47 5.04 2.05
HE 0524-4428 05 25 38.8 -44 26 08 11.1 0.40 0.39 0.03 8 7.13 4.66 2.34

-- 60 --
Table 12---Continued
Star name R.A. # B (B - V ) HP2 (B - V ) J-K E (B-V) v rad KP HP2 GP Comm.
HE 0524-5217 05 25 34.5 -52 15 10 11.7 0.45 0.43 0.03 32 7.30 3.75 2.70
HE 0524-5244 05 25 36.8 -52 41 32 10.8 § § § 0.35 0.03 -6 4.53 7.04 1.43
HE 0525-5257 05 26 28.0 -52 54 58 11.0 0.53 0.51 0.03 5 8.23 2.74 4.07
HE 0526-5357 05 27 42.4 -53 55 15 9.5 § § § 0.29 0.05 -28 4.60 7.18 1.59
HE 0527-3931b 05 29 13.7 -39 28 50 11.9 0.48 0.42 0.02 42 7.74 3.25 3.71
HE 0527-5522 05 28 23.4 -55 20 33 12.4 0.58 § § § 0.05 -29 9.81 2.29 4.72
HE 0527-5627 05 28 02.4 -56 25 10 11.1 § § § 0.35 0.04 4 5.76 6.51 1.65
HE 0528-4845 05 29 45.5 -48 43 14 10.8 § § § 0.35 0.03 108 6.03 6.61 1.55
HE 0528-5110 05 29 34.6 -51 07 58 10.4 0.38 0.39 0.04 2 5.87 6.22 1.34
HE 0528-5431 05 29 54.6 -54 29 18 11.4 0.37 0.12 0.05 48 0.37 5.44 0.11 He
HE 0530-4024 05 31 52.1 -40 22 14 10.2 0.38 0.37 0.02 26 6.37 6.38 1.59
HE 0531-4810 05 33 18.4 -48 08 24 11.2 § § § 0.29 0.03 67 4.65 7.66 1.43
HE 0532-3859 05 34 38.1 -38 57 13 10.5 0.51 0.48 0.03 80 7.87 2.97 3.71
HE 0533-4107 05 35 23.4 -41 05 21 13.4 0.45 0.40 0.03 9 7.60 3.81 3.27
HE 0535-3909 05 36 44.1 -39 07 42 12.1 0.55 0.50 0.03 -38 8.74 2.45 4.23
HE 0537-5447 05 38 42.9 -54 45 54 13.1 0.52 § § § 0.08 32 8.70 2.83 3.89
HE 0538-5537 05 39 36.5 -55 35 46 9.8 § § § 0.31 0.06 -15 4.18 8.18 1.15
HE 0539-3809 05 41 27.0 -38 08 27 12.2 0.48 0.69 0.04 25 7.47 3.30 3.05
HE 0539-4545 05 41 12.5 -45 44 13 10.3 0.41 0.38 0.05 32 7.99 4.73 2.18
HE 0540-3744 05 42 10.4 -37 43 08 11.6 0.43 0.39 0.05 -47 7.12 4.13 2.24
HE 0540-5724 05 41 16.9 -57 23 10 9.5 § § § 0.26 0.07 -0 3.39 10.40 1.08
HE 0541-3756 05 43 05.7 -37 55 27 13.6 § § § 0.30 0.04 28 3.91 6.64 1.24
HE 0542-5440 05 43 10.6 -54 38 48 11.3 0.38 0.37 0.07 48 6.79 5.19 1.95
HE 0544-4913 05 46 03.6 -49 12 18 11.4 0.40 0.38 0.05 -2 6.82 4.54 2.05
HE 0544-4931 05 45 59.8 -49 30 11 9.9 § § § 0.26 0.05 30 3.60 9.96 1.20
HE 0545-5411 05 46 57.9 -54 10 03 11.6 0.39 0.33 0.10 23 7.31 4.96 2.25
HE 0545-5533 05 46 21.6 -55 32 51 10.1 0.42 0.36 0.10 43 7.87 4.29 2.60
HE 0546-5354 05 47 49.2 -53 53 33 11.5 § § § 0.26 0.10 19 3.62 7.49 1.35
HE 0546-5410 05 47 35.4 -54 09 54 11.2 0.41 0.34 0.10 -25 7.78 4.58 2.59
HE 0549-4105 05 51 02.9 -41 04 52 11.7 0.46 0.49 0.05 5 7.42 3.64 2.78
HE 0549-4712 05 50 57.6 -47 11 25 10.8 § § § 0.32 0.08 43 4.30 8.35 1.26
HE 0549-4717 05 50 57.2 -47 16 36 10.7 § § § 0.32 0.08 43 4.94 6.69 1.62
HE 0850-0044 08 53 16.3 00 32 44 11.3 0.38 0.37 0.04 52 6.53 5.26 1.70
HE 0850-0141 08 53 30.5 -01 53 05 10.8 § § § 0.35 0.02 7 3.27 7.02 1.11
HE 0903-0037 09 05 43.0 -00 49 31 11.2 0.55 0.45 0.03 27 9.26 2.50 4.38
HE 0904-0102 09 06 55.2 00 50 12 11.9 0.56 0.49 0.04 -43 8.08 2.24 3.51
HE 0905-0102 09 08 00.5 00 50 01 11.2 0.38 0.33 0.04 2 5.96 5.29 2.28
HE 0907-0224 09 10 07.2 02 12 01 11.8 0.43 0.37 0.03 23 6.85 4.21 2.82
HE 0909-0111 09 12 28.8 -01 23 29 12.1 0.45 0.39 0.03 57 7.93 3.95 2.85
HE 0909-0117 09 11 36.2 -01 30 19 12.1 0.38 0.37 0.03 8 6.53 5.46 1.66
HE 0910-0106 09 13 11.5 00 53 37 12.1 0.46 0.46 0.02 7 7.58 3.60 2.71
HE 0911-0618 09 14 26.6 -06 30 53 13.7 1.00 1.17 0.04 139 11.33 0.03 6.16 Em
HE 0912-0209 09 15 14.2 -02 21 52 10.5 0.41 0.42 0.04 3 6.99 4.45 2.06
HE 0914-0222 09 17 19.0 -02 34 48 10.3 § § § 0.37 0.03 18 3.94 7.33 1.60
HE 0914-0552 09 16 49.0 -06 05 11 11.6 0.43 0.42 0.03 -22 7.28 4.11 2.33 HB
HE 0916-0204 09 18 36.2 01 52 17 11.0 0.38 0.37 0.03 -12 6.56 5.17 1.78
HE 0916-0130 09 18 50.4 -01 43 09 10.8 0.66 0.57 0.03 2 8.86 1.27 5.26
HE 0916-0222 09 18 41.0 -02 35 39 11.4 0.42 0.36 0.03 -3 7.54 4.46 2.42
HE 0916-0711 09 18 43.9 -07 24 12 12.4 0.58 0.50 0.04 -52 8.83 2.18 4.47
HE 0917-0236 09 19 54.7 -02 48 46 11.2 0.67 0.55 0.03 27 9.26 1.41 4.81
HE 0918-0136 09 20 36.7 -01 49 16 10.7 § § § 0.34 0.04 -1 4.60 7.06 1.37
HE 0918-0214 09 21 28.8 -02 26 52 10.9 0.38 0.38 0.04 -25 6.75 5.11 2.06
HE 0921-0211 09 23 43.7 01 58 52 11.2 0.40 0.38 0.04 -3 7.07 4.69 2.11
HE 0923-0118 09 25 43.0 01 05 06 10.7 0.45 0.37 0.04 -7 7.70 3.92 2.64
HE 0924-0202 09 26 45.1 -02 15 12 11.0 0.49 0.47 0.03 -17 8.48 3.35 3.50
HE 0927-0110 09 30 05.8 -01 23 35 10.8 0.37 0.39 0.03 13 2.73 6.14 1.31
HE 0927-0215 09 29 32.9 -02 28 39 10.6 0.42 0.44 0.04 3 7.58 4.25 2.58
HE 0927-0300 09 29 38.4 -03 13 55 12.6 0.37 0.33 0.04 69 4.79 5.96 1.34
HE 0928-0031 09 31 11.0 -00 44 50 10.2 § § § 0.29 0.03 2 1.90 11.38 0.72
HE 0928-0048 09 30 40.1 -01 01 26 11.2 § § § 0.31 0.03 -9 4.01 7.37 1.31
HE 0929-0229 09 32 08.4 -02 42 59 13.8 0.45 0.44 0.04 -15 7.10 3.89 2.52
HE 0930-0605 09 32 37.4 -06 19 17 11.4 0.38 0.29 0.04 -2 6.24 6.15 1.94
HE 0931-0732 09 33 38.2 -07 46 20 11.3 0.50 0.51 0.04 59 8.49 3.17 3.06
HE 0937-0724 09 39 29.5 -07 38 22 10.6 0.52 0.50 0.04 75 7.96 2.51 3.14
HE 0940-1103 09 43 01.0 -11 16 49 10.7 0.44 0.41 0.05 53 8.37 4.22 2.63
HE 0945-0729 09 48 13.7 -07 43 30 11.0 0.47 0.42 0.08 9 9.00 3.57 3.18
HE 0946-1126 09 49 06.0 -11 40 18 10.2 § § § 0.32 0.04 37 5.31 7.05 1.65

-- 61 --
Table 12---Continued
Star name R.A. # B (B - V ) HP2 (B - V ) J-K E (B-V) v rad KP HP2 GP Comm.
HE 0947-0051 09 50 09.1 -01 05 07 9.9 § § § 0.28 0.07 -23 5.60 6.76 1.55
HE 0948-0200 09 51 09.6 01 45 57 9.8 0.60 § § § 0.04 -18 8.97 1.97 4.72
HE 0948-0207 09 50 48.2 -02 21 49 10.1 0.38 0.34 0.05 -28 6.06 5.93 1.43
HE 0949-0023 09 52 01.2 -00 37 46 10.0 0.45 0.42 0.04 22 7.87 3.90 2.69
HE 0950-1026 09 53 10.1 -10 40 37 11.3 0.58 0.50 0.05 49 9.03 2.47 4.38
HE 0950-1152 09 52 28.6 -12 06 24 11.0 0.41 0.39 0.04 64 7.94 4.69 2.26
HE 0953-1326 09 56 23.5 -13 41 06 11.0 § § § 0.32 0.06 36 4.46 7.02 1.51
HE 0958-0140 10 00 56.9 01 25 40 11.5 0.43 0.41 0.02 9 7.20 4.17 2.00
HE 0958-0815 10 01 15.6 -08 30 23 11.3 0.46 0.50 0.06 -25 7.07 3.62 2.42
HE 0959-1618 10 02 13.9 -16 33 12 10.6 0.42 0.37 0.04 5 7.73 4.38 2.31
HE 0959-2034 10 02 01.2 -20 49 18 12.1 0.48 0.37 0.05 9 8.14 3.30 3.14
HE 1000-1259 10 03 08.9 -13 14 18 10.7 § § § 0.30 0.05 31 3.58 7.59 1.27
HE 1001-0139 10 03 46.3 01 25 09 11.2 0.38 § § § 0.02 -19 6.15 5.44 1.87
HE 1001-0915 10 04 25.7 -09 30 17 11.0 0.38 0.34 0.08 28 5.44 6.43 1.19
HE 1001-1713 10 03 40.6 -17 28 15 10.1 § § § 0.30 0.04 54 3.01 8.47 1.02
HE 1003-1650 10 05 39.4 -17 05 11 10.7 0.66 0.58 0.04 -30 9.22 1.28 5.39
HE 1004-0800 10 06 35.5 -08 14 58 11.5 § § § 0.38 0.05 2 3.68 8.01 1.37
HE 1004-0941 10 07 02.2 -09 55 44 10.6 0.42 0.35 0.07 42 8.24 4.45 2.25
HE 1004-1217 10 06 57.6 -12 31 55 13.4 0.67 0.51 0.06 16 9.38 1.44 5.26
HE 1004-1843 10 06 53.3 -18 58 35 11.8 0.56 0.50 0.05 51 8.14 2.19 3.44
HE 1005-1833 10 08 17.8 -18 48 30 11.7 0.62 0.44 0.05 57 9.26 1.88 4.91
HE 1007-0739 10 10 11.5 -07 53 51 11.4 0.43 0.40 0.04 38 7.48 4.16 2.48
HE 1008-1041 10 11 00.5 -10 56 22 11.2 0.38 0.37 0.05 49 6.74 5.22 1.77
HE 1008-1345 10 10 39.4 -14 00 33 11.1 0.54 0.48 0.07 28 8.58 2.50 3.96
HE 1008-1411 10 11 10.6 -14 26 43 10.2 1.00 0.15 0.08 181 § § § § § § § § § He
HE 1008-1817 10 10 41.8 -18 32 09 11.9 0.45 0.43 0.06 17 8.22 3.83 2.68
HE 1010-0737 10 13 10.6 -07 52 33 § § § 0.45 0.41 0.04 52 7.85 3.92 2.97
HE 1010-1648 10 12 40.3 -17 03 19 10.2 0.38 0.38 0.05 56 5.80 5.37 1.45
HE 1011-0432 10 14 17.3 -04 47 02 11.2 § § § 0.24 0.04 -22 2.35 9.69 0.99
HE 1012-0152 10 14 53.0 01 37 11 § § § 0.38 0.35 0.05 22 6.32 5.69 1.28
HE 1012-1452 10 15 21.4 -15 07 04 10.9 0.55 0.45 0.08 23 8.41 2.32 3.68
HE 1012-1807 10 14 48.2 -18 22 26 12.0 0.54 0.45 0.06 6 8.58 2.71 3.22
HE 1012-1956 10 14 41.0 -20 11 54 11.6 0.63 0.59 0.06 91 8.97 1.59 4.69
HE 1013-0505 10 16 28.8 -05 20 34 13.3 0.78 1.19 0.04 -58 1.30 0.89 2.65 Em
HE 1013-1253 10 16 08.2 -13 08 15 11.8 § § § 0.29 0.09 -38 4.60 7.02 1.21
HE 1014-1904 10 16 49.2 -19 19 55 10.8 0.62 0.48 0.05 11 9.41 1.87 4.23
HE 1015-1822 10 18 20.9 -18 37 52 10.9 § § § 0.27 0.06 62 2.15 7.30 1.22
HE 1016-1259 10 18 55.7 -13 14 29 12.2 0.38 0.35 0.09 35 5.68 5.47 1.41
HE 1016-1856 10 19 10.6 -19 11 31 11.8 0.44 0.39 0.05 -9 6.95 3.93 2.01
HE 1017-0826 10 19 56.6 -08 41 56 § § § 0.63 0.38 0.05 0 0.07 1.43 0.03 pec
HE 1018-1918 10 21 07.7 -19 33 52 12.1 0.48 0.47 0.07 39 7.94 3.31 2.62
HE 1019-0328 10 21 57.8 -03 43 40 11.7 § § § 0.47 0.05 57 3.54 8.37 1.29
HE 1019-1920 10 21 34.3 -19 35 59 11.8 0.46 0.43 0.06 4 7.39 3.64 2.23
HE 1019-1947 10 21 53.8 -20 02 36 12.9 0.38 0.34 0.07 49 5.49 5.01 1.78
HE 1019-2012 10 21 32.4 -20 27 21 12.2 0.51 0.40 0.06 28 8.84 3.11 3.25
HE 1019-2109 10 21 43.4 -21 24 17 11.2 0.54 0.49 0.06 37 8.62 2.64 3.75
HE 1020-1319 10 22 41.0 -13 34 35 13.3 0.72 0.61 0.09 9 9.58 1.02 5.52
HE 1021-1648 10 24 09.4 -17 03 39 11.3 0.43 0.38 0.08 86 6.76 4.07 1.79
HE 1024-1306 10 26 27.8 -13 21 52 11.6 0.45 0.38 0.08 27 7.35 3.96 2.20
HE 1025-0540 10 28 18.5 -05 55 34 10.7 § § § 0.23 0.04 23 2.81 10.74 0.98
HE 1027-0920 10 29 37.9 -09 35 45 § § § 0.37 0.30 0.05 13 2.54 5.98 1.14
HE 1029-1247 10 32 05.3 -13 03 14 11.2 0.61 0.56 0.06 88 9.09 1.76 4.81
HE 1029-1314 10 32 01.0 -13 30 27 11.9 0.38 0.37 0.06 9 6.33 5.58 1.48
HE 1029-1320 10 31 47.3 -13 35 57 11.1 § § § 0.29 0.06 3 4.27 7.28 1.26
HE 1029-1508 10 32 22.6 -15 24 17 13.2 0.84 0.73 0.08 3 10.13 0.62 5.71
HE 1030-1500 10 32 33.4 -15 16 10 14.0 0.72 0.54 0.08 23 9.58 1.13 5.45
HE 1030-1837 10 33 24.7 -18 52 39 10.1 0.40 0.30 0.06 2 7.52 4.74 2.04
HE 1031-0105 10 33 59.0 -01 21 09 § § § 0.38 0.34 0.07 68 6.35 5.55 1.52
HE 1031-2116 10 33 42.5 -21 32 16 9.6 0.45 0.42 0.05 -9 7.04 3.87 2.29
HE 1031-2122 10 33 36.2 -21 37 42 9.7 0.38 0.36 0.05 23 5.43 5.78 1.60
HE 1034-2015 10 36 37.9 -20 30 45 9.9 0.38 0.37 0.05 30 7.02 5.36 1.83
HE 1035-2213 10 37 57.8 -22 28 59 11.7 0.38 0.39 0.05 6 6.67 5.33 1.47
HE 1038-0213 10 41 08.4 01 57 46 § § § 0.45 0.42 0.04 -12 7.60 3.76 2.33
HE 1040-1222 10 42 52.1 -12 38 37 13.6 0.60 0.46 0.05 78 9.16 2.07 4.42
HE 1040-2013 10 42 35.3 -20 29 04 10.7 0.55 0.48 0.03 15 9.27 2.58 4.11
HE 1044-1532 10 46 33.4 -15 48 14 10.7 0.51 0.47 0.06 -0 8.38 2.94 3.24
HE 1045-0604 10 48 03.1 -06 20 37 11.5 0.53 0.51 0.03 3 8.01 2.68 2.98

-- 62 --
Table 12---Continued
Star name R.A. # B (B - V ) HP2 (B - V ) J-K E (B-V) v rad KP HP2 GP Comm.
HE 1045-1515 10 47 56.2 -15 31 16 14.1 0.37 1.16 0.06 61 § § § 6.27 0.77 Em
HE 1048-0312 10 51 02.2 -03 28 25 11.3 0.45 0.40 0.04 14 7.86 3.94 2.34
HE 1049-0042 10 51 54.2 00 26 51 § § § 0.41 0.43 0.04 55 6.75 4.31 2.17
HE 1049-0612 10 52 30.0 -06 28 03 10.7 0.45 0.45 0.03 34 8.14 3.98 2.79
HE 1049-2225 10 52 05.0 -22 41 32 § § § § § § 0.28 0.07 17 3.46 8.28 1.11
HE 1050-0304 10 52 37.2 -03 20 04 12.2 0.45 0.36 0.05 -4 7.13 3.83 2.30
HE 1050-1454 10 52 34.3 -15 10 03 11.6 0.55 0.51 0.06 25 8.35 2.27 3.63
HE 1050-1923 10 53 11.8 -19 39 53 11.6 0.64 0.61 0.04 52 9.23 1.65 4.94
HE 1051-0331 10 54 03.8 -03 47 36 11.9 § § § 0.35 0.04 39 3.39 7.00 0.78
HE 1053-0239 10 55 50.4 -02 55 06 10.9 0.62 0.52 0.05 43 8.68 1.72 4.53
HE 1053-2319 10 56 24.5 -23 35 10 § § § 0.38 0.34 0.05 5 5.92 5.59 1.37
HE 1056-2827 10 58 43.9 -28 43 41 10.9 0.38 0.35 0.05 15 6.23 5.03 1.49
HE 1058-3026 11 00 45.1 -30 43 03 10.7 0.47 0.41 0.06 -24 8.34 3.73 2.76
HE 1059-0632 11 02 20.4 -06 48 30 10.7 0.42 0.42 0.04 59 7.32 4.47 2.43
HE 1100-2258 11 02 45.1 -23 14 55 § § § 0.47 0.51 0.06 5 8.43 3.51 2.96
HE 1100-2420 11 02 54.2 -24 36 14 § § § 0.48 0.40 0.06 23 7.85 3.44 2.76
HE 1100-2923 11 02 25.7 -29 39 22 11.1 0.37 0.34 0.05 43 3.68 6.00 1.22
HE 1101-0633 11 03 50.9 -06 49 47 10.6 0.43 0.41 0.04 60 7.91 4.20 2.57
HE 1102-0059 11 05 04.3 -01 16 09 § § § 0.38 0.39 0.05 53 7.03 5.45 1.99
HE 1102-0436 11 05 31.0 -04 52 36 11.0 0.65 0.54 0.05 45 8.71 1.33 5.06
HE 1102-0656 11 04 53.0 -07 12 45 11.4 0.46 0.43 0.04 9 7.59 3.65 2.65
HE 1102-2817 11 05 03.4 -28 33 48 11.3 0.38 0.36 0.06 16 5.73 6.09 1.54
HE 1103-1627 11 05 29.3 -16 43 27 10.1 0.38 0.35 0.05 53 6.18 5.11 1.62
HE 1104-0202 11 06 47.5 -02 19 11 § § § 0.40 0.43 0.06 42 6.91 4.69 2.01
HE 1104-0558 11 07 00.0 -06 15 06 10.7 0.49 0.36 0.05 30 8.26 3.31 3.36
HE 1104-0636 11 07 17.8 -06 53 00 11.0 0.49 0.41 0.05 39 8.53 3.39 3.56
HE 1105-0608 11 08 19.2 -06 24 48 11.3 0.56 0.43 0.05 51 8.93 2.40 4.46
HE 1105-1008 11 08 10.1 -10 24 46 § § § 0.38 0.36 0.05 31 5.99 4.99 1.72
HE 1106-0553 11 09 09.6 -06 09 26 11.4 0.38 0.33 0.05 9 6.05 5.34 1.41
HE 1107-0343 11 10 27.4 -03 59 40 12.7 1.00 0.93 0.05 35 4.64 § § § 4.97 Em
HE 1107-0702 11 10 15.8 -07 18 48 11.4 0.44 0.38 0.04 8 8.04 4.18 3.00
HE 1107-2759 11 09 57.8 -28 16 14 11.1 0.38 § § § 0.06 -28 5.74 5.86 1.51
HE 1107-2937 11 09 53.3 -29 53 30 10.9 0.50 0.44 0.07 25 8.58 3.07 3.83
HE 1108-0635 11 11 30.0 -06 52 03 10.2 0.40 0.39 0.05 -49 7.18 4.71 2.17
HE 1108-1301 11 11 15.8 -13 17 42 11.4 0.38 0.38 0.06 21 6.80 5.07 1.94
HE 1108-3217 11 10 34.8 -32 33 39 8.2 0.42 § § § 0.09 12 7.39 4.44 2.33
HE 1109-0317 11 11 42.7 -03 33 25 11.3 0.45 0.42 0.05 1 7.94 3.96 2.88
HE 1109-0354 11 11 47.8 -04 11 14 11.4 0.51 0.51 0.06 68 7.70 2.88 2.73
HE 1109-0721 11 12 16.1 -07 37 44 10.0 0.38 0.35 0.04 39 6.01 5.58 1.52
HE 1109-1515 11 12 11.3 -15 32 16 10.5 0.49 0.44 0.07 17 7.73 3.21 3.27
HE 1109-2638 11 11 31.2 -26 54 47 § § § 0.39 0.42 0.06 18 6.19 4.91 1.69
HE 1109-3211 11 11 29.0 -32 27 41 9.9 0.40 0.35 0.10 37 7.28 4.59 2.27
HE 1110-0746 11 13 15.6 -08 03 10 § § § 0.93 0.40 0.04 46 11.07 0.26 6.01
HE 1110-1628 11 12 51.4 -16 44 46 § § § 0.42 0.44 0.09 52 7.85 4.37 2.54
HE 1110-2626 11 12 37.7 -26 42 26 § § § § § § 0.23 0.07 26 2.32 10.67 0.86
HE 1112-1833 11 15 17.8 -18 50 05 10.8 0.63 0.58 0.05 -21 8.97 1.54 4.76
HE 1112-3102 11 14 46.1 -31 18 28 10.9 § § § 0.26 0.06 22 2.73 7.19 1.55
HE 1113-3101 11 15 43.0 -31 17 23 10.4 0.58 0.47 0.07 -31 8.84 2.23 4.11
HE 1114-2757 11 17 01.0 -28 14 13 11.3 0.60 0.49 0.07 -82 8.84 1.88 4.61
HE 1115-2314 11 17 53.3 -23 30 54 12.8 0.77 0.87 0.05 38 11.73 0.79 6.32
HE 1115-2753 11 18 03.6 -28 09 44 10.0 0.38 § § § 0.07 1 5.86 5.86 1.56
HE 1115-2814 11 17 59.5 -28 31 11 11.2 0.38 0.37 0.07 1 6.85 5.18 2.27
HE 1115-3014 11 17 58.3 -30 31 02 11.7 0.51 0.45 0.07 37 8.83 3.12 3.63
HE 1115-3112 11 17 34.1 -31 29 14 11.2 0.66 0.56 0.07 -41 8.80 1.27 4.75
HE 1116-2837 11 18 47.5 -28 53 41 11.1 0.39 0.39 0.07 -17 6.57 4.92 2.19
HE 1116-3010 11 19 20.6 -30 26 42 10.8 0.49 0.41 0.07 -4 8.40 3.27 3.30
HE 1117-1802 11 19 59.3 -18 19 09 11.4 0.53 0.51 0.04 62 8.19 2.74 3.63
HE 1117-1916 11 20 18.7 -19 33 15 11.2 0.62 0.62 0.05 38 8.53 1.70 4.55
HE 1117-1940 11 19 42.2 -19 57 03 11.7 0.67 0.54 0.04 -20 9.43 1.41 5.59
HE 1117-2828 11 20 14.4 -28 45 03 11.1 0.38 0.46 0.06 -53 7.05 5.60 2.05
HE 1118-1930 11 20 29.8 -19 46 43 11.5 0.50 0.46 0.04 -16 8.59 3.10 3.64
HE 1118-2009 11 20 45.1 -20 26 02 11.4 0.72 0.58 0.05 -35 9.81 1.18 5.73
HE 1118-2543 11 21 09.8 -25 59 42 10.7 0.47 0.38 0.05 54 8.00 3.65 3.52
HE 1118-2726 11 20 31.4 -27 42 54 10.7 0.42 0.44 0.06 -7 9.04 4.49 3.38
HE 1118-3151 11 20 56.9 -32 08 24 10.3 § § § 0.40 0.06 38 4.25 6.75 1.43
HE 1118-3217 11 20 56.9 -32 33 57 10.1 § § § 0.28 0.07 45 4.89 7.15 1.42
HE 1119-1117 11 21 53.8 -11 34 16 § § § 0.42 0.40 0.07 97 7.27 4.30 2.38

-- 63 --
Table 12---Continued
Star name R.A. # B (B - V ) HP2 (B - V ) J-K E (B-V) v rad KP HP2 GP Comm.
HE 1119-1236 11 21 41.8 -12 52 56 § § § § § § 0.27 0.06 38 4.26 7.62 1.50
HE 1120-0858 11 23 31.0 -09 15 21 § § § 0.42 0.38 0.05 29 7.72 4.42 2.81
HE 1120-1702 11 22 43.0 -17 18 48 § § § 0.43 0.41 0.04 34 7.29 4.10 2.49
HE 1122-1011 11 25 03.6 -10 27 48 § § § 0.46 0.42 0.05 56 8.62 3.89 3.36
HE 1122-1952 11 25 16.3 -20 09 09 11.6 0.46 0.43 0.06 -4 7.21 3.52 2.74
HE 1123-2029 11 25 30.2 -20 45 34 11.2 0.43 0.45 0.08 -32 7.60 4.08 2.88
HE 1124-0856 11 26 40.8 -09 12 45 § § § 0.50 0.47 0.04 11 8.34 3.01 3.83
HE 1124-2229 11 27 19.9 -22 46 18 10.8 0.37 0.34 0.04 52 4.65 6.49 1.81
HE 1126-1126 11 28 59.8 -11 42 55 § § § 0.46 0.51 0.03 68 7.51 3.55 3.00
HE 1127-0747 11 30 00.0 -08 03 36 § § § 0.37 0.36 0.05 44 4.43 6.47 1.42
HE 1128-2529 11 30 56.9 -25 46 27 10.5 § § § 0.26 0.05 -23 2.97 10.32 1.04
HE 1129-1209 11 32 31.7 -12 25 50 § § § 0.49 0.44 0.04 -3 8.94 3.33 3.76
HE 1129-1556 11 31 34.6 -16 12 50 § § § 0.60 0.41 0.04 10 9.02 2.20 4.84
HE 1131-2004 11 33 37.9 -20 21 10 § § § § § § 0.22 0.05 19 1.33 10.91 0.93
HE 1131-2256 11 33 38.6 -23 13 13 11.1 § § § 0.31 0.04 8 4.04 8.28 1.21
HE 1131-2553 11 33 32.6 -26 10 11 11.1 0.64 0.57 0.05 -67 9.28 1.63 5.34
HE 1133-3122 11 35 33.4 -31 38 37 10.3 § § § 0.30 0.07 -2 1.96 6.80 1.34
HE 1133-3200 11 36 06.5 -32 17 33 10.5 0.48 0.46 0.06 -23 7.65 3.43 2.91
HE 1139-2913 11 42 01.7 -29 29 59 11.7 0.39 0.39 0.07 -39 6.77 4.92 2.17
HE 1139-2959 11 42 05.8 -30 15 47 11.8 0.38 0.35 0.06 -64 5.44 5.20 1.51
HE 1143-1328 11 46 12.2 -13 45 14 § § § 0.47 0.45 0.04 44 8.10 3.53 3.30
HE 1143-2912 11 46 01.7 -29 28 48 12.0 0.55 0.19 0.06 28 0.43 2.11 0.45 He
HE 1144-1245 11 47 32.2 -13 01 43 § § § 0.64 0.51 0.04 44 9.24 1.72 5.34
HE 1144-2710 11 46 36.5 -27 27 32 10.6 0.37 0.11 0.10 44 0.33 4.84 § § § He
HE 1146-1257 11 49 01.9 -13 14 06 § § § § § § 0.26 0.04 32 4.55 9.56 1.30
HE 1148-0907 11 50 35.3 -09 24 09 § § § § § § 0.31 0.03 41 2.46 8.13 1.14
HE 1149-0544 11 52 02.9 -06 00 45 § § § 0.38 0.35 0.03 44 6.37 5.23 1.79
HE 1149-1516 11 52 21.6 -15 33 05 § § § § § § 0.32 0.05 18 5.70 7.32 1.42
HE 1150-0400 11 52 47.5 -04 16 56 § § § § § § 0.14 0.02 129 § § § 7.55 0.01 He
HE 1150-2058 11 53 13.4 -21 14 57 § § § 0.38 0.41 0.03 60 5.51 5.06 1.79
HE 1151-1406 11 53 55.0 -14 22 51 9.7 0.56 § § § 0.04 -14 8.96 2.30 4.59
HE 1152-2353 11 55 23.8 -24 10 01 11.3 0.38 0.36 0.07 1 7.07 5.02 2.10
HE 1153-1841 11 55 46.3 -18 57 54 § § § 0.37 0.36 0.05 54 2.88 6.24 0.63
HE 1156-0347 11 58 47.0 -04 04 39 § § § 0.43 0.40 0.03 -16 6.59 4.19 2.18
HE 1156-3143 11 58 46.1 -32 00 25 10.3 § § § 0.29 0.07 -22 1.72 7.43 1.22
HE 1158-0631 12 01 29.0 -06 48 34 § § § 0.43 0.44 0.02 -13 7.71 4.19 2.93
HE 1200-2955 12 03 13.4 -30 11 49 12.1 0.40 0.37 0.07 -28 6.92 4.68 2.24
HE 1201-3202 12 03 55.0 -32 19 22 10.5 0.38 0.37 0.08 -22 5.76 5.74 1.33
HE 1203-0017 12 06 07.2 00 00 25 § § § 0.45 0.49 0.02 -6 8.18 3.88 3.10
HE 1204-2708 12 06 36.7 -27 25 35 10.5 0.39 § § § 0.07 -25 6.72 4.81 2.21
HE 1204-2839 12 07 14.6 -28 55 46 11.6 0.47 0.43 0.05 -89 8.18 3.64 3.18
HE 1204-2857 12 07 27.4 -29 14 05 10.8 0.40 0.39 0.06 4 6.67 4.71 1.96
HE 1205-2922 12 07 40.8 -29 39 07 10.5 0.43 0.41 0.05 -9 7.76 4.05 2.77
HE 1205-3148 12 07 52.1 -32 05 01 10.7 0.38 0.32 0.07 -12 6.63 5.56 1.79
HE 1206-2040 12 08 48.0 -20 57 02 § § § 0.56 § § § 0.07 -23 8.78 2.42 4.42
HE 1206-2346 12 09 17.3 -24 02 57 11.4 0.47 § § § 0.09 8 8.92 3.72 3.44
HE 1208-2728 12 10 49.9 -27 45 00 10.8 0.38 0.38 0.07 -41 5.64 6.31 2.02
HE 1209-0118 12 11 37.0 -01 34 49 § § § 0.37 0.32 0.02 8 4.12 5.94 1.62
HE 1209-3151 12 12 25.2 -32 08 33 12.2 0.38 0.31 0.07 -32 5.83 5.27 1.76
HE 1210-1324 12 12 49.0 -13 40 53 10.7 0.41 0.40 0.06 -18 6.52 4.32 2.14
HE 1210-2254 12 12 45.8 -23 10 46 11.9 0.71 0.61 0.09 24 9.10 1.19 5.26
HE 1211-2240 12 13 55.9 -22 57 27 11.8 0.43 0.44 0.08 -47 6.93 4.06 2.45
HE 1211-3038 12 14 27.4 -30 54 55 10.4 0.66 0.53 0.06 -27 8.75 1.39 5.23
HE 1215-1909 12 17 55.2 -19 26 36 § § § 0.38 0.35 0.05 29 5.58 6.37 1.34
HE 1216-2935 12 19 33.1 -29 51 42 10.5 0.46 0.42 0.06 -71 6.87 3.55 2.57
HE 1217-2431 12 19 40.3 -24 48 24 11.5 0.61 0.50 0.10 -7 9.23 1.87 5.34
HE 1218-0551 12 20 50.2 -06 08 09 § § § 0.41 0.42 0.02 -16 6.74 4.47 2.27
HE 1218-2456 12 21 14.9 -25 12 52 11.1 § § § 0.15 0.09 -31 0.20 9.64 0.05 He
HE 1218-3216 12 21 02.9 -32 32 47 10.4 § § § 0.34 0.08 10 4.78 6.70 1.12
HE 1220-3001 12 23 13.9 -30 17 45 11.6 0.92 § § § 0.07 92 8.16 0.39 5.76 Em
HE 1221-2919 12 23 43.0 -29 35 44 11.7 § § § 0.27 0.07 -20 3.18 6.82 1.46
HE 1222-0127 12 24 50.9 01 11 09 § § § § § § 0.35 0.02 -10 4.05 6.67 1.16
HE 1222-1257 12 25 33.1 -13 14 17 12.9 0.50 0.46 0.05 -32 8.71 3.10 4.34
HE 1225-2753 12 27 50.6 -28 10 02 10.7 0.38 0.34 0.06 -19 5.88 6.42 1.60
HE 1229-0019 12 31 40.3 00 02 31 § § § § § § 0.31 0.02 19 4.98 6.72 1.47
HE 1230-3124 12 33 39.1 -31 41 02 9.8 0.38 § § § 0.08 -18 5.77 5.41 1.38
HE 1231-0517 12 34 01.9 -05 34 08 § § § § § § 0.31 0.05 -56 4.79 6.73 1.36

-- 64 --
Table 12---Continued
Star name R.A. # B (B - V ) HP2 (B - V ) J-K E (B-V) v rad KP HP2 GP Comm.
HE 1231-1642 12 33 52.1 -16 59 19 § § § 1.00 0.38 0.05 -53 § § § § § § 0.00
HE 1232-2242 12 35 11.5 -22 58 37 11.3 § § § 0.30 0.06 -47 2.46 6.94 1.28
HE 1232-2302 12 35 23.0 -23 18 44 11.5 0.71 0.52 0.08 -15 9.27 1.11 5.79
HE 1233-2549 12 36 00.2 -26 06 13 11.5 0.44 0.39 0.08 -36 6.88 3.76 2.53
HE 1234-2632 12 37 22.6 -26 48 53 11.6 0.45 0.42 0.06 -47 7.62 3.86 2.66
HE 1235-2521 12 38 08.2 -25 37 47 11.8 0.55 0.44 0.10 -74 9.05 2.74 4.65
HE 1235-3213 12 38 18.5 -32 29 50 10.1 § § § 0.35 0.09 -20 4.76 6.99 1.76
HE 1236-3026 12 39 39.4 -30 43 05 10.6 § § § 0.33 0.07 -25 6.38 9.55 2.67
HE 1237-1240 12 39 58.8 -12 57 18 § § § 0.41 0.45 0.05 -64 6.51 4.49 1.79
HE 1237-2201 12 40 31.4 -22 18 17 § § § 0.42 0.40 0.05 -47 7.80 4.34 2.52
HE 1237-2305 12 39 45.4 -23 21 50 11.2 § § § 0.17 0.08 -18 1.03 8.93 0.32
HE 1237-2353 12 40 33.6 -24 09 57 12.5 0.46 0.46 0.08 -73 7.38 3.64 2.94
HE 1237-2503 12 40 13.9 -25 19 36 8.8 0.39 1.57 0.10 -21 6.55 4.96 1.81
HE 1237-2508 12 39 46.3 -25 25 22 12.3 0.49 0.44 0.10 -48 8.91 3.34 4.04
HE 1238-2543 12 41 36.5 -25 59 49 11.0 § § § 0.16 0.07 -26 0.69 7.43 0.04
HE 1240-2613 12 43 09.8 -26 29 36 11.6 § § § 0.28 0.08 -20 1.77 7.68 1.29
HE 1241-0823 12 44 20.2 -08 40 16 10.3 0.53 0.11 0.03 42 9.38 2.88 5.27
HE 1242-2608 12 45 31.9 -26 25 03 10.6 0.62 0.45 0.07 -78 8.36 1.74 5.15
HE 1243-1627 12 46 15.6 -16 43 55 § § § 0.43 0.39 0.05 -35 7.47 4.23 2.37
HE 1244-3204 12 46 56.4 -32 20 30 10.3 0.38 0.33 0.08 -26 5.58 6.18 1.38
HE 1245-2124 12 47 57.1 -21 40 53 § § § 0.55 0.45 0.06 -19 8.39 2.40 3.81
HE 1246-2626 12 48 59.3 -26 42 30 10.8 0.37 0.32 0.07 -12 4.90 5.86 1.37
HE 1247-0617 12 50 08.2 -06 34 08 § § § 0.38 0.35 0.03 -49 5.38 5.60 1.30
HE 1248-0925 12 51 03.4 -09 41 54 11.0 0.38 0.43 0.04 -34 7.08 5.01 2.10
HE 1249-0648 12 52 01.2 -07 04 18 § § § § § § 0.30 0.03 7 4.34 7.63 1.19
HE 1249-0807 12 51 54.5 -08 23 43 12.0 0.42 0.46 0.04 -35 8.78 4.31 3.14
HE 1250-2834 12 53 27.4 -28 50 32 13.2 0.84 0.56 0.07 -119 9.68 0.57 6.30
HE 1253-1929 12 56 30.2 -19 45 58 § § § 0.38 0.39 0.07 -58 7.21 5.10 2.10
HE 1254-2625 12 56 46.3 -26 42 01 10.7 0.38 0.41 0.08 -48 6.69 5.54 2.04
HE 1255-0134 12 58 24.2 01 17 49 § § § 0.43 0.41 0.02 -34 7.12 4.16 2.08
HE 1255-2413 12 58 23.5 -24 29 12 11.1 § § § 0.27 0.12 -13 1.30 8.64 1.14
HE 1256-2217 12 58 59.5 -22 33 59 § § § 0.38 0.43 0.12 -9 6.90 5.23 1.91
HE 1257-0737 12 59 56.4 -07 53 50 11.4 § § § 0.34 0.05 -19 2.48 6.96 1.47
HE 1257-2708 13 00 18.2 -27 24 10 10.8 0.51 0.48 0.07 -62 8.88 3.20 3.93
HE 1258-1926 13 01 38.2 -19 42 15 § § § 0.42 0.39 0.10 -33 7.75 4.44 2.66
HE 1258-2436 13 01 39.1 -24 52 29 12.2 0.41 0.39 0.11 -66 6.46 4.44 1.91
HE 1258-2457 13 00 56.4 -25 13 59 11.1 § § § 0.32 0.11 -45 4.75 6.63 1.18
HE 1259-2450 13 01 45.1 -25 06 39 11.0 0.60 0.44 0.11 8 9.18 2.19 4.59
HE 1300-2627 13 02 56.4 -26 43 36 10.9 0.52 0.48 0.08 32 7.86 2.72 3.42
HE 1300-2739 13 03 19.9 -27 55 54 10.6 0.66 0.61 0.08 10 8.91 1.32 4.81
HE 1304-1827 13 06 43.7 -18 43 30 § § § 0.38 0.42 0.08 -40 6.42 5.51 2.01
HE 1304-3125 13 07 26.4 -31 41 06 10.1 0.40 0.38 0.07 -63 7.53 4.51 2.64
HE 1310-2546 13 12 53.3 -26 02 37 10.3 1.00 0.15 0.08 -27 0.08 § § § § § § He
HE 1310-3041 13 13 22.6 -30 57 35 10.8 0.38 0.33 0.06 -48 6.68 5.17 1.80
HE 1311-0315 13 14 30.5 -03 31 33 § § § 0.46 0.47 0.03 29 7.11 3.70 2.85
HE 1311-3039 13 14 18.5 -30 55 24 10.7 0.39 § § § 0.06 -3 7.18 4.88 2.54
HE 1312-0558 13 15 07.2 -06 14 15 § § § 0.40 0.39 0.04 1 6.75 4.60 1.81
HE 1315-3205 13 17 58.3 -32 21 37 12.4 0.41 0.39 0.07 -86 6.83 4.34 2.27
HE 1317-0236 13 20 12.7 -02 52 05 § § § 0.51 0.45 0.04 19 7.60 2.95 3.35
HE 1317-2910 13 20 14.4 -29 25 57 11.4 § § § 0.37 0.07 -51 4.97 7.02 1.35
HE 1322-1253 13 25 13.2 -13 09 00 11.9 0.37 0.39 0.06 74 1.84 5.91 0.50
HE 1323-2217 13 25 59.5 -22 33 16 12.3 0.48 0.37 0.08 20 7.37 3.33 3.07
HE 1323-2254 13 25 49.4 -23 09 52 11.6 0.45 0.43 0.10 -56 7.78 3.84 2.46
HE 1323-2635 13 26 21.8 -26 50 53 10.2 0.39 0.36 0.06 -29 6.97 4.93 2.07
HE 1324-1728 13 27 04.3 -17 44 20 11.4 0.45 0.50 0.09 -56 7.85 3.78 3.28
HE 1327-1834 13 29 47.5 -18 50 27 11.2 0.71 0.62 0.09 -64 9.10 1.22 0.00
HE 1327-3133 13 29 54.5 -31 49 09 10.4 0.43 0.41 0.05 -25 7.66 4.14 2.42
HE 1333-2530 13 36 27.1 -25 46 16 11.6 0.50 0.42 0.07 -87 7.89 3.09 3.36
HE 1334-2237 13 37 33.4 -22 53 07 11.8 0.50 0.44 0.12 -75 8.25 3.10 3.71
HE 1334-2610 13 36 53.8 -26 26 14 10.8 0.41 § § § 0.07 -61 6.91 4.25 2.30
HE 1334-2907 13 37 35.0 -29 22 29 11.3 0.37 0.34 0.05 -10 1.42 6.23 1.37
HE 1335-2951 13 38 49.4 -30 06 21 11.2 0.43 0.43 0.04 50 7.55 4.17 2.41
HE 1336-3000 13 39 07.0 -30 15 25 9.7 § § § § § § 0.05 -9 4.06 7.03 1.36
HE 1337-3149 13 40 26.4 -32 04 24 12.2 0.41 0.48 0.05 -82 6.68 4.28 2.12
HE 1340-3136 13 43 13.4 -31 51 08 10.4 0.42 0.37 0.05 -76 7.70 4.45 2.14
HE 1341-2355 13 44 20.6 -24 10 27 11.7 0.40 0.38 0.07 -68 7.59 4.74 2.33
HE 1341-2833 13 44 14.4 -28 48 56 11.1 0.37 0.34 0.06 -35 4.64 6.31 1.46

-- 65 --
Table 12---Continued
Star name R.A. # B (B - V ) HP2 (B - V ) J-K E (B-V) v rad KP HP2 GP Comm.
HE 1342-2758 13 45 10.6 -28 13 25 11.8 0.47 0.43 0.06 -53 6.87 3.47 2.62
HE 1342-2916 13 45 34.8 -29 31 54 11.2 0.48 0.54 0.05 -99 7.80 3.43 3.10
HE 1343-0205 13 45 38.4 -02 20 26 § § § 0.40 0.43 0.05 -40 7.41 4.55 2.32
HE 1344-2331 13 47 46.1 -23 46 17 11.6 0.40 0.33 0.08 -92 7.21 4.61 2.19
HE 1345-2735 13 47 50.4 -27 50 52 10.8 § § § 0.30 0.06 -43 1.70 6.91 1.54
HE 1346-2753 13 49 42.7 -28 08 33 10.9 0.45 0.43 0.07 -79 7.70 3.97 2.61
HE 1347-2546 13 49 49.4 -26 01 12 § § § § § § 0.30 0.07 -29 2.22 7.77 1.51
HE 1348-2311 13 50 48.0 -23 26 27 § § § 0.38 0.38 0.07 -61 5.37 6.37 1.52
HE 1349-0841 13 51 58.1 -08 55 52 11.3 0.39 0.36 0.04 -24 7.33 5.13 2.04
HE 1349-1827 13 52 38.4 -18 42 23 6.3 § § § § § § 0.07 -51 2.83 6.64 2.99
HE 1349-2935 13 51 56.4 -29 50 12 11.3 0.48 0.41 0.06 -92 8.17 3.31 3.33
HE 1350-2648 13 53 27.6 -27 03 05 § § § 0.37 0.37 0.06 51 4.80 6.27 1.49
HE 1350-2955 13 53 05.8 -30 10 11 10.5 0.46 0.47 0.06 -42 7.47 3.58 2.60
HE 1352-0215 13 55 04.6 -02 30 22 § § § 0.42 0.07 0.05 -29 § § § 4.24 § § § pec
HE 1352-3141 13 55 03.6 -31 55 54 10.6 0.47 0.14 0.06 -185 0.37 3.49 § § § He
HE 1353-0537 13 56 29.5 -05 52 18 10.2 0.64 0.58 0.03 -32 9.49 1.52 0.00
HE 1353-2403 13 55 50.6 -24 18 24 § § § 0.38 0.32 0.08 -44 6.15 6.29 1.92
HE 1353-2449 13 55 56.9 -25 04 33 § § § § § § 0.32 0.07 -49 3.98 6.78 1.75
HE 1354-2456 13 57 10.6 -25 10 41 § § § 0.46 0.34 0.08 -52 8.81 3.80 3.27
HE 1354-2825 13 56 53.5 -28 40 21 10.8 0.60 0.49 0.07 -77 8.80 1.96 4.27
HE 1355-2356 13 58 15.1 -24 11 06 § § § 0.44 0.40 0.07 -59 8.02 4.03 3.02
HE 1356-3028 13 59 51.6 -30 42 45 11.1 0.56 0.47 0.05 -106 8.95 2.41 4.50
HE 1357-0631 14 00 17.8 -06 46 24 10.5 0.60 0.51 0.03 -68 8.91 1.96 4.78
HE 1357-3020 14 00 46.3 -30 35 01 10.5 0.51 0.45 0.05 -82 8.44 2.92 3.54
HE 1357-3110 14 00 37.0 -31 24 51 11.5 0.44 0.40 0.06 -93 8.03 4.11 2.96
HE 1359-0439 14 02 27.4 -04 53 52 10.1 0.38 0.40 0.03 -8 6.24 6.01 1.48
HE 1359-0505 14 02 15.1 -05 19 40 10.4 0.50 0.45 0.03 -84 8.53 3.08 3.63
HE 1359-0609 14 01 50.9 -06 23 37 10.2 § § § 0.33 0.03 3 5.41 7.23 1.51
HE 1359-2903 14 02 19.7 -29 17 42 11.0 0.43 0.40 0.07 -62 7.03 4.20 2.15
HE 1359-3057 14 02 07.0 -31 11 54 10.6 0.40 0.42 0.05 -47 6.96 4.70 2.05
HE 1400-0337 14 03 22.6 -03 51 58 10.2 0.56 0.45 0.05 -24 8.92 2.34 4.60
HE 1402-0426 14 05 21.4 -04 40 59 10.6 0.39 § § § 0.03 -83 7.32 5.18 1.97
HE 1402-1821 14 05 07.7 -18 35 55 11.6 0.61 0.52 0.10 -86 9.11 1.80 5.01
HE 1402-1842 14 05 01.2 -18 56 54 10.9 0.39 0.38 0.09 -13 6.01 4.93 1.47
HE 1403-2428 14 05 51.1 -24 42 19 § § § § § § 0.28 0.07 -36 3.45 7.00 1.26
HE 1404-0524 14 06 51.8 -05 38 20 10.2 0.47 0.42 0.03 -50 8.27 3.71 2.95
HE 1404-0722 14 07 16.6 -07 36 55 10.4 0.50 0.50 0.03 -20 8.11 3.08 3.54
HE 1404-1404 14 06 46.6 -14 18 17 11.5 0.40 0.40 0.09 -49 7.40 4.72 2.08
HE 1404-2444 14 07 23.5 -24 58 58 § § § § § § 0.32 0.06 -29 4.51 6.58 1.34
HE 1405-0535 14 08 25.2 -05 49 49 10.3 0.40 0.44 0.03 -35 7.34 4.57 2.57
HE 1405-1233 14 08 16.3 -12 47 16 11.0 0.51 0.43 0.07 -16 9.16 3.13 4.42
HE 1405-2105 14 07 55.7 -21 19 43 11.4 0.50 0.49 0.07 -16 8.68 3.09 3.44
HE 1406-0259 14 09 09.4 -03 14 00 10.6 0.43 0.40 0.07 -109 7.68 4.24 2.62
HE 1407-0537 14 09 42.5 -05 51 51 10.9 0.37 0.37 0.03 -6 4.76 6.21 1.52
HE 1408-0358 14 10 58.8 -04 12 45 10.8 0.38 0.40 0.04 4 5.90 5.66 1.45
HE 1408-0524 14 11 06.0 -05 38 52 11.0 § § § 0.39 0.03 -8 4.16 8.03 1.35
HE 1408-2208 14 11 25.4 -22 22 16 12.4 0.44 0.38 0.07 -165 6.81 3.99 2.16
HE 1409-0133 14 11 59.5 01 19 12 § § § § § § 0.26 0.04 13 3.38 9.74 1.12
HE 1409-0000 14 11 43.9 -00 14 44 § § § 0.39 0.39 0.04 -22 6.21 4.83 1.74
HE 1409-0124 14 12 14.2 -01 38 27 § § § 0.38 0.39 0.07 52 5.76 5.06 2.14
HE 1409-0401 14 12 32.9 -04 15 25 9.9 0.38 0.32 0.04 24 6.09 5.97 1.53
HE 1409-0455 14 12 25.0 -05 09 43 9.8 § § § 0.28 0.03 -11 4.51 7.62 1.35
HE 1409-0539 14 12 15.8 -05 53 37 10.4 0.45 0.46 0.03 -22 7.60 3.75 2.98
HE 1410-0125 14 13 24.7 -01 39 54 § § § 1.00 0.95 0.07 88 § § § § § § 1.22
HE 1410-0915 14 13 38.2 -09 29 39 11.8 0.43 0.43 0.04 -8 7.65 4.21 2.96
HE 1410-1937 14 13 46.3 -19 51 51 § § § § § § 0.34 0.09 -48 4.81 6.94 1.10
HE 1411-0542 14 14 21.8 -05 56 44 7.4 0.53 § § § 0.03 -60 9.39 2.84 4.63
HE 1411-0810 14 13 40.6 -08 24 31 11.0 0.38 0.42 0.05 -58 7.01 5.08 1.95
HE 1416-0752 14 19 26.6 -08 06 16 11.9 § § § 0.27 0.04 -59 1.76 7.88 1.58
HE 1418-0205 14 21 18.0 -02 19 32 § § § 0.37 0.35 0.06 130 1.94 6.02 0.34
HE 1419-0200 14 21 55.0 -02 14 33 § § § 0.37 0.39 0.05 88 2.84 5.76 0.51
HE 1420-0846 14 23 34.6 -08 59 50 13.1 0.48 0.45 0.06 -77 7.42 3.40 2.82
HE 1421-0130 14 24 27.8 01 16 37 § § § 0.38 0.38 0.03 -83 5.33 4.89 1.40
HE 1421-1820 14 24 37.4 -18 34 27 § § § 0.51 0.44 0.09 -21 8.80 3.17 4.11
HE 1422-0222 14 24 57.8 -02 35 57 13.0 0.60 0.48 0.06 -86 8.76 1.95 4.69
HE 1423-0243 14 26 03.8 -02 56 41 12.3 0.76 0.57 0.06 -96 8.93 0.79 5.91
HE 1423-2054 14 25 55.0 -21 07 48 § § § 0.38 § § § 0.10 -25 7.11 5.17 2.17

-- 66 --
Table 12---Continued
Star name R.A. # B (B - V ) HP2 (B - V ) J-K E (B-V) v rad KP HP2 GP Comm.
HE 1424-0506 14 26 51.8 -05 20 16 11.8 0.48 0.44 0.05 -53 7.48 3.47 2.89
HE 1425-0047 14 28 00.2 -01 01 02 § § § 0.45 0.42 0.04 -31 7.78 3.77 2.73
HE 1425-2222 14 28 04.8 -22 35 50 § § § 0.37 0.34 0.09 -38 4.97 6.23 1.40
HE 1426-0132 14 29 04.3 01 18 47 § § § 0.45 0.44 0.03 -115 7.23 3.75 2.61
HE 1426-0230 14 28 53.8 -02 44 04 12.8 0.49 0.48 0.07 -119 7.71 3.08 3.42
HE 1426-0328 14 29 15.8 -03 42 17 11.6 § § § 0.28 0.10 -34 1.94 8.45 1.39
HE 1427-0107 14 30 28.8 00 53 45 § § § 0.37 0.36 0.04 -72 4.98 6.33 1.34
HE 1427-1146 14 30 17.3 -12 00 03 11.1 0.38 0.34 0.11 -76 5.88 5.83 1.64
HE 1428-0428 14 31 19.2 -04 41 20 13.8 0.46 0.43 0.08 -39 7.10 3.55 2.87
HE 1428-0434 14 31 14.2 -04 47 16 12.0 0.57 0.49 0.07 -125 8.32 2.10 4.34
HE 1431-0017 14 34 16.6 -00 30 37 § § § § § § 0.33 0.04 -68 2.99 8.38 0.95
HE 1432-0750 14 35 35.5 -08 03 52 § § § § § § 0.30 0.07 -10 5.30 7.55 1.41
HE 1437-1958 14 40 05.0 -20 10 52 § § § 0.38 0.41 0.10 60 5.70 5.10 1.55
HE 1439-0035 14 42 26.9 -00 48 15 § § § 0.38 0.35 0.04 -54 5.15 6.38 1.37
HE 1447-0226 14 49 44.2 02 13 58 § § § 0.60 0.47 0.04 56 9.23 2.09 4.64
HE 1447-0139 14 50 34.6 -01 52 03 § § § 0.43 0.50 0.06 -13 7.33 4.03 2.62
HE 1447-1436 14 50 25.7 -14 48 39 10.7 0.39 0.38 0.08 -76 7.98 4.84 2.30
HE 1449-1409 14 52 43.9 -14 21 58 11.1 0.37 0.31 0.08 -86 4.92 6.08 1.44
HE 1450-1808 14 53 42.2 -18 20 39 § § § 1.00 0.99 0.09 -19 4.67 § § § 4.25 Em
HE 1450-1951 14 52 55.4 -20 03 21 § § § 0.64 0.52 0.10 -88 9.07 1.59 5.53
HE 1451-0055 14 53 40.1 -01 07 49 10.5 § § § 0.36 0.04 -67 4.32 7.48 1.34
HE 1501-1348 15 03 54.2 -14 00 06 11.0 0.62 0.48 0.09 -62 9.36 1.80 4.59
HE 1502-1235 15 04 50.4 -12 47 29 11.3 0.50 0.45 0.10 -90 8.14 3.16 3.00
HE 1503-1105 15 06 17.8 -11 16 38 10.9 0.45 0.46 0.11 -90 7.29 3.89 2.41
HE 1505-0149 15 07 35.0 01 38 30 12.2 0.48 0.46 0.06 -11 7.37 3.32 2.87
HE 1505-1122 15 08 09.4 -11 33 54 11.6 1.00 0.09 0.10 121 0.08 § § § § § § He
HE 1506-0305 15 09 03.4 -03 17 01 12.2 0.50 0.47 0.15 -98 8.63 3.04 3.57
HE 1507-0226 15 10 07.9 02 15 34 11.0 0.62 0.54 0.05 -47 9.30 1.88 4.93
HE 1507-0511 15 09 47.0 -05 23 05 11.7 0.45 0.42 0.09 -61 7.25 3.75 2.21
HE 1508-0120 15 11 26.6 01 09 21 10.2 § § § 0.36 0.04 0 2.06 7.66 1.11
HE 1509-0433 15 12 12.0 -04 44 15 13.4 0.48 0.42 0.09 -59 7.29 3.41 3.41
HE 1510-0217 15 12 40.1 02 05 50 10.4 0.78 0.60 0.05 -34 9.54 0.76 5.73
HE 1511-1206 15 14 34.1 -12 17 11 9.8 § § § 0.28 0.11 -30 3.78 9.22 1.14
HE 1513-0229 15 15 41.0 02 18 36 11.5 0.51 0.47 0.04 -120 7.42 2.97 2.86
HE 1517-0910 15 20 37.4 -09 21 16 10.5 § § § 0.30 0.10 -31 1.54 7.92 1.34
HE 1519-0900 15 22 25.2 -09 10 54 10.6 § § § 0.27 0.10 -64 3.72 8.61 1.31
HE 1521-0015 15 23 55.9 -00 25 40 11.0 § § § 0.16 0.08 21 0.21 7.13 0.08 He
HE 1521-0033 15 23 46.1 -00 44 23 11.8 1.00 1.13 0.11 -41 § § § § § § 5.54 Em
HE 1521-1141 15 23 54.5 -11 52 18 11.2 § § § 0.32 0.13 -42 5.72 7.54 1.98
HE 1523-0933 15 25 48.5 -09 43 38 10.8 0.38 0.35 0.13 -20 6.08 5.93 1.67
HE 1523-1058 15 25 59.5 -11 09 04 10.3 0.71 0.54 0.13 -18 9.41 1.09 5.78
HE 1527-0248 15 30 35.5 -02 58 52 10.5 § § § 0.29 0.15 -63 5.37 7.91 1.36
HE 1528-0840 15 30 57.4 -08 51 09 11.0 0.65 0.55 0.14 -33 8.58 1.45 5.00
HE 1530-0000 15 32 45.8 -00 10 26 12.2 0.50 0.45 0.06 -86 8.55 3.14 3.94
HE 2002-6111 20 06 33.1 -61 02 50 11.2 § § § 0.37 0.04 117 3.54 8.82 1.39
HE 2014-6106 20 18 27.6 -60 57 10 10.7 § § § 0.28 0.04 31 1.84 8.03 1.41
HE 2021-6055 20 25 55.2 -60 46 10 10.0 § § § 0.28 0.06 34 4.68 8.32 1.45
HE 2023-6210 20 27 59.0 -62 00 28 11.0 0.38 0.38 0.05 5 6.58 5.43 1.69
HE 2032-5951 20 37 00.5 -59 40 46 9.9 1.00 § § § 0.06 17 11.28 § § § 6.44 Em
HE 2112-0216 21 15 25.2 -02 04 11 13.6 0.48 0.42 0.06 21 7.51 3.27 2.97
HE 2118-4541 21 21 26.2 -45 28 51 11.1 0.39 0.39 0.03 41 7.37 4.85 2.45
HE 2121-0342 21 24 13.2 -03 29 44 10.3 0.50 0.48 0.07 46 8.13 3.19 3.78
HE 2122-0236 21 24 43.2 -02 23 17 11.9 0.54 0.51 0.06 30 8.81 2.60 4.03
HE 2125-4515 21 29 06.7 -45 02 43 11.3 0.62 0.49 0.02 173 9.26 1.87 5.10
HE 2127-4246 21 30 53.5 -42 33 09 11.1 0.41 0.37 0.03 81 6.88 4.40 2.21
HE 2128-0422 21 31 22.3 -04 08 51 11.5 0.48 0.45 0.04 78 7.36 3.49 2.67
HE 2128-0424 21 31 35.5 -04 11 14 12.1 0.40 0.41 0.04 84 7.13 4.55 2.25
HE 2128-4423 21 31 21.4 -44 10 16 10.8 0.58 0.44 0.03 70 9.00 2.28 4.83
HE 2130-1440 21 33 05.3 -14 27 10 11.8 0.47 0.40 0.07 1 8.25 3.67 3.37
HE 2131-4612 21 34 44.9 -45 58 43 10.8 0.53 0.47 0.03 32 8.29 2.59 4.33
HE 2132-1448 21 35 18.0 -14 34 40 13.8 1.00 0.78 0.05 58 8.86 0.21 5.46 Em
HE 2133-1309 21 35 52.8 -12 55 48 12.7 0.53 0.53 0.05 35 8.98 2.97 4.51
HE 2134-1856 21 37 30.7 -18 43 21 11.6 § § § 0.34 0.04 -15 5.41 6.63 1.40
HE 2135-4525 21 38 16.3 -45 11 36 12.1 1.00 0.93 0.03 -6 4.98 0.06 5.54 Em
HE 2135-4619 21 39 10.8 -46 05 51 10.1 0.37 0.08 0.02 -40 § § § 5.87 § § § He
HE 2139-4225 21 42 47.3 -42 11 60 10.6 0.66 0.54 0.02 66 9.11 1.47 5.53
HE 2139-4232 21 43 06.0 -42 19 07 11.1 0.50 0.47 0.02 29 8.63 3.15 3.65

-- 67 --
Table 12---Continued
Star name R.A. # B (B - V ) HP2 (B - V ) J-K E (B-V) v rad KP HP2 GP Comm.
HE 2139-4517 21 43 04.8 -45 03 19 11.5 0.60 0.49 0.02 67 9.81 2.21 4.63
HE 2141-4442 21 44 54.5 -44 28 58 11.2 0.86 0.77 0.02 24 11.02 0.61 6.49
HE 2142-1736 21 45 43.2 -17 22 52 13.5 0.50 0.48 0.04 20 8.18 3.20 3.74
HE 2142-4338 21 45 12.5 -43 25 00 11.4 0.58 0.53 0.02 29 8.98 2.15 4.65
HE 2142-4410 21 45 34.6 -43 56 26 11.3 0.47 0.42 0.02 44 9.00 3.61 3.90
HE 2144-0705 21 47 34.1 -06 51 22 12.4 0.43 0.41 0.04 18 7.18 4.07 2.52
HE 2147-1259 21 50 19.2 -12 45 14 11.8 0.38 0.46 0.04 34 6.56 5.06 1.90
HE 2148-1302 21 51 39.6 -12 47 55 11.0 0.60 0.56 0.03 42 8.85 1.99 5.30
HE 2149-0523 21 51 56.9 -05 09 30 11.7 0.60 0.50 0.03 65 9.26 2.08 4.55
HE 2149-1245 21 52 23.5 -12 31 47 11.0 0.43 0.44 0.03 -9 7.44 4.13 3.05
HE 2149-1937 21 52 27.4 -19 23 27 11.2 0.49 0.46 0.03 13 8.81 3.40 3.48
HE 2150-0015 21 53 17.3 00 29 11 11.3 0.39 0.39 0.09 -8 7.75 4.93 2.52
HE 2150-1528 21 53 17.0 -15 14 23 11.9 0.39 0.41 0.05 -40 6.00 4.96 1.56
HE 2150-1914 21 52 54.0 -18 59 53 11.6 0.40 0.45 0.03 37 7.00 4.69 2.29
HE 2152-1817 21 55 36.7 -18 03 20 11.8 0.44 0.36 0.05 45 8.49 4.09 3.35
HE 2155-0758 21 57 42.0 -07 44 13 11.2 0.61 0.51 0.04 15 9.19 1.94 4.96
HE 2157-4203 22 00 37.4 -41 48 45 13.4 0.45 0.42 0.02 -8 7.48 3.76 3.05
HE 2159-1231 22 01 48.7 -12 17 28 11.7 0.49 0.42 0.05 -3 8.68 3.32 3.75
HE 2201-0223 22 04 04.1 -02 08 50 11.3 0.55 0.52 0.13 44 9.59 2.74 4.66
HE 2201-1312 22 03 46.3 -12 57 55 11.7 0.43 0.45 0.04 20 7.95 4.22 3.02
HE 2201-1426 22 03 49.9 -14 12 25 11.3 0.63 0.65 0.04 57 8.85 1.53 5.06
HE 2201-2326 22 04 44.9 -23 11 36 10.5 0.60 0.48 0.03 14 8.75 1.78 4.62
HE 2203-0909 22 06 11.8 -08 54 59 12.0 0.47 0.39 0.03 84 0.16 3.27 § § § He
HE 2204-0749 22 06 43.9 -07 35 16 11.5 0.38 0.29 0.04 -15 6.53 5.54 1.78
HE 2205-1437 22 08 21.4 -14 22 50 11.4 0.51 0.45 0.03 46 8.19 2.96 4.17
HE 2205-1442 22 07 50.9 -14 27 36 11.9 0.56 0.47 0.03 17 8.82 2.30 4.55
HE 2206-4028 22 09 28.8 -40 13 48 11.3 0.37 0.36 0.02 32 4.77 6.42 1.42
HE 2207-0816 22 09 45.6 -08 01 22 11.6 0.54 0.47 0.05 81 7.82 2.49 3.76
HE 2208-0318 22 11 13.9 -03 03 32 11.6 0.38 0.32 0.10 36 6.18 5.56 1.84
HE 2209-1512 22 12 20.2 -14 58 02 10.9 § § § 0.29 0.03 33 4.01 7.66 1.16
HE 2210-2002 22 13 02.4 -19 48 06 10.4 0.42 0.43 0.03 13 7.74 4.34 2.89
HE 2212-0159 22 15 07.9 02 14 27 11.9 0.38 0.37 0.05 31 6.07 5.49 1.71
HE 2212-0314 22 15 29.3 -02 59 36 11.0 0.56 0.57 0.10 9 8.77 2.48 4.53
HE 2215-5150 22 18 17.8 -51 35 40 10.9 0.64 0.51 0.02 16 9.17 1.53 5.46
HE 2217-1353 22 20 23.8 -13 38 48 11.7 0.40 0.41 0.04 42 6.79 4.64 1.96
HE 2217-4035 22 20 28.3 -40 20 50 12.2 0.66 0.49 0.01 -7 9.06 1.33 5.22
HE 2218-4047 22 21 56.9 -40 32 42 10.9 0.45 0.45 0.01 -5 7.81 3.94 3.03
HE 2219-0201 22 21 48.5 02 16 53 12.7 0.49 0.51 0.07 13 8.43 3.48 4.29
HE 2220-0152 22 23 06.7 02 07 36 10.9 0.42 0.42 0.06 48 7.84 4.43 2.75
HE 2222-4848 22 25 42.0 -48 33 12 10.6 0.72 0.53 0.01 80 9.74 1.08 6.17
HE 2223-4105 22 26 49.2 -40 50 20 11.4 0.37 0.33 0.01 4 4.56 6.18 1.27
HE 2224-0128 22 26 43.4 01 43 45 11.9 0.45 0.43 0.07 58 7.54 3.79 2.67
HE 2224-0333 22 26 58.6 -03 18 24 10.9 0.38 0.43 0.08 -6 5.98 5.90 1.58
HE 2224-1501 22 26 56.2 -14 46 42 10.9 0.37 0.32 0.04 16 3.85 6.34 1.80
HE 2225-0154 22 27 44.2 02 09 60 11.9 0.38 0.38 0.09 41 6.24 5.59 1.69
HE 2227-1317 22 29 46.3 -13 01 57 11.5 0.43 0.44 0.05 75 7.39 4.03 2.72
HE 2228-0046 22 30 45.1 01 01 33 12.4 0.50 0.37 0.08 64 8.71 3.09 3.92
HE 2228-0157 22 31 11.8 02 13 10 12.8 0.40 0.38 0.08 62 6.44 4.56 2.15
HE 2229-0133 22 32 10.6 01 49 08 12.1 0.52 0.45 0.08 92 8.59 2.78 4.10
HE 2229-2058 22 32 24.0 -20 42 38 9.6 0.45 0.41 0.04 27 7.62 3.97 2.81
HE 2230-0132 22 33 20.9 -01 17 06 § § § 0.60 0.48 0.07 -7 9.16 2.08 3.55
HE 2230-2629 22 33 13.2 -26 13 48 10.9 0.50 0.47 0.02 63 8.71 3.23 4.13
HE 2231-0149 22 33 57.1 -01 33 40 § § § 0.38 0.38 0.07 -17 7.20 5.30 1.95
HE 2232-2142 22 35 29.0 -21 26 46 10.5 0.38 0.37 0.03 8 6.52 5.71 1.88
HE 2233-5817 22 37 00.5 -58 02 03 11.8 0.83 0.65 0.02 44 8.36 0.68 5.41 Em
HE 2234-5747 22 37 22.3 -57 32 15 12.0 0.41 0.43 0.02 21 6.75 4.32 2.27
HE 2235-6012 22 38 56.2 -59 57 08 11.8 0.38 0.35 0.02 -30 5.81 5.37 1.74
HE 2236-6131 22 39 59.5 -61 15 42 11.2 § § § 0.39 0.03 51 5.48 6.56 1.31
HE 2237-0110 22 39 58.8 01 26 02 § § § 0.38 0.33 0.08 8 6.34 6.02 1.66
HE 2239-0140 22 41 37.0 01 56 34 § § § 0.60 0.56 0.08 -57 10.41 2.13 4.14
HE 2239-0205 22 42 05.3 02 21 13 § § § 0.46 0.47 0.09 -31 8.32 3.80 2.91
HE 2240-1647 22 42 57.1 -16 31 20 13.5 0.45 0.76 0.04 120 7.45 3.96 2.39
HE 2240-3938 22 42 58.8 -39 22 44 10.8 § § § 0.34 0.02 62 4.09 6.72 1.09
HE 2241-3901 22 44 03.8 -38 45 38 11.0 § § § 0.28 0.01 47 1.78 7.88 1.35
HE 2241-4528 22 44 10.6 -45 12 35 11.8 0.78 0.70 0.01 48 9.66 0.89 6.02
HE 2242-0110 22 45 32.9 -00 54 18 § § § 0.70 1.13 0.06 -6 § § § 1.24 § § § Em
HE 2242-0237 22 45 10.6 -02 22 02 10.7 0.38 0.33 0.05 50 6.92 5.45 1.97

-- 68 --
Table 12---Continued
Star name R.A. # B (B - V ) HP2 (B - V ) J-K E (B-V) v rad KP HP2 GP Comm.
HE 2242-4116 22 45 48.0 -41 00 58 11.9 0.48 0.47 0.02 62 7.69 3.31 3.33
HE 2243-0232 22 46 09.1 -02 16 53 10.8 0.50 0.47 0.05 38 8.62 3.04 3.91
HE 2243-1259 22 45 49.4 -12 43 35 12.1 0.43 0.44 0.05 -5 7.32 4.00 2.68
HE 2243-4743 22 46 07.4 -47 27 40 10.8 0.84 0.71 0.01 47 9.58 0.57 6.02
HE 2244-0009 22 46 59.0 00 05 58 § § § 0.45 0.38 0.08 7 7.50 3.86 2.87
HE 2244-0143 22 47 07.4 -01 27 44 § § § 0.40 0.37 0.09 -1 6.04 4.73 1.82
HE 2246-0023 22 49 25.2 -00 07 25 § § § 0.61 0.58 0.10 -61 9.03 1.91 5.27
HE 2247-0040 22 49 53.5 -00 24 21 § § § 0.63 0.56 0.09 13 8.91 1.67 5.36
HE 2247-0221 22 49 53.8 -02 05 32 12.2 0.57 0.40 0.08 21 8.54 2.22 4.43
HE 2247-1517 22 49 43.7 -15 01 16 13.7 0.49 0.45 0.04 34 6.92 3.10 3.09
HE 2247-6103 22 50 18.2 -60 47 43 11.5 0.40 0.42 0.02 23 7.32 4.61 2.51
HE 2248-0445 22 51 33.8 -04 29 54 11.1 0.45 0.39 0.04 46 7.73 3.82 2.71
HE 2248-5717 22 51 47.8 -57 01 20 11.2 0.58 0.55 0.01 69 8.95 2.09 4.66
HE 2249-0036 22 52 31.0 00 52 32 § § § 0.51 0.51 0.08 -11 8.84 3.09 4.16
HE 2249-0201 22 51 46.8 02 17 07 § § § 0.40 0.45 0.13 49 6.87 4.73 2.08
HE 2249-0215 22 52 06.0 02 31 32 § § § 0.62 0.53 0.10 67 8.50 1.66 5.54
HE 2249-1230 22 51 54.7 -12 14 27 13.1 0.46 0.44 0.04 47 7.32 3.63 2.98
HE 2249-1531 22 52 09.6 -15 16 01 12.0 0.62 0.52 0.04 23 8.44 1.59 5.71
HE 2249-5527 22 52 50.9 -55 11 51 10.7 0.40 0.41 0.02 33 6.91 4.73 1.93
HE 2250-0048 22 53 07.9 -00 32 49 13.1 0.39 0.36 0.09 42 7.49 4.89 2.34
HE 2250-0332 22 52 44.9 -03 16 51 11.0 0.50 0.47 0.07 -27 8.63 3.07 4.01
HE 2250-0424 22 52 57.1 -04 08 11 10.4 0.58 0.45 0.04 97 9.01 2.27 4.27
HE 2250-1215 22 52 54.5 -11 59 40 11.6 0.55 0.49 0.04 -23 8.06 2.41 3.98
HE 2250-1240 22 52 40.3 -12 24 35 12.2 0.43 0.43 0.04 62 7.16 4.09 2.21
HE 2250-1314 22 52 52.8 -12 58 13 12.4 0.42 0.41 0.04 43 7.12 4.40 2.48
HE 2250-1322 22 53 33.6 -13 06 05 11.9 0.69 0.74 0.04 -9 7.66 1.08 5.44 Em
HE 2250-1851 22 53 17.0 -18 35 31 11.7 0.77 0.55 0.03 30 9.37 0.96 2.78
HE 2250-6159 22 53 45.1 -61 43 41 11.2 0.38 0.37 0.02 28 5.95 6.40 1.61
HE 2251-5746 22 54 32.9 -57 30 57 11.1 0.56 0.56 0.02 58 8.85 2.30 4.37
HE 2252-5058 22 55 56.4 -50 42 40 10.6 0.40 0.44 0.01 40 6.34 4.64 2.26
HE 2252-5146 22 55 35.5 -51 30 13 10.3 § § § 0.34 0.01 37 3.54 8.04 1.18
HE 2253-0221 22 56 17.5 02 37 38 12.5 0.64 0.50 0.09 71 9.12 1.73 5.16
HE 2253-0025 22 56 08.2 -00 09 58 14.0 0.59 1.21 0.08 0 § § § 1.58 1.84 Em
HE 2253-1951 22 56 29.8 -19 35 05 11.5 0.45 0.45 0.04 53 8.21 3.89 2.96
HE 2253-5238 22 56 42.7 -52 22 42 11.2 0.38 0.37 0.01 43 5.84 5.59 1.44
HE 2253-6152 22 56 56.2 -61 36 27 10.5 § § § 0.32 0.02 22 4.90 7.75 1.48
HE 2254-1949 22 57 24.2 -19 33 10 11.5 0.60 0.44 0.04 17 8.99 1.94 4.72
HE 2255-1758 22 58 13.9 -17 42 20 11.7 0.60 0.48 0.04 36 8.99 1.94 4.72
HE 2255-2213 22 58 10.1 -21 57 26 10.7 0.37 0.36 0.03 26 4.87 6.33 1.48
HE 2255-6111 22 58 59.3 -60 54 60 11.6 0.54 0.54 0.02 6 8.82 2.51 4.38
HE 2257-5254 23 00 34.6 -52 38 36 11.3 0.39 0.37 0.01 23 6.60 4.85 2.05
HE 2257-6046 23 00 39.1 -60 30 34 11.9 0.58 0.49 0.02 5 9.40 2.37 4.61
HE 2258-3248 23 01 11.0 -32 32 27 11.1 0.42 0.44 0.02 -4 7.94 4.32 2.61
HE 2258-3714 23 00 53.5 -36 57 56 11.4 0.51 0.46 0.02 82 9.11 3.17 4.11
HE 2258-5752 23 01 24.2 -57 36 02 11.4 0.49 0.47 0.02 28 8.66 3.29 4.21
HE 2259-0251 23 02 07.4 -02 35 41 11.2 0.51 0.45 0.07 31 8.19 2.90 3.32
HE 2259-4850 23 02 32.2 -48 34 11 12.2 0.38 0.33 0.01 -51 6.29 6.49 1.88
HE 2300-4310 23 02 59.0 -42 54 24 12.6 0.49 0.44 0.01 14 8.58 3.39 4.24
HE 2301-5731 23 04 57.4 -57 14 57 12.1 0.37 0.32 0.02 25 4.67 6.20 1.58
HE 2304-5417A 23 07 30.0 -54 01 11 12.5 0.51 § § § 0.01 25 8.35 2.96 3.93
HE 2304-5417B 23 07 30.0 -54 01 11 12.5 0.51 § § § 0.01 22 7.99 2.99 2.99
HE 2304-5847 23 07 43.9 -58 31 11 11.2 0.45 0.45 0.02 67 8.05 3.90 3.31
HE 2305-0421 23 08 30.2 -04 05 01 10.2 0.61 0.48 0.04 40 9.01 1.92 5.03
HE 2305-0804 23 08 10.8 -07 48 33 11.9 0.66 0.53 0.05 39 9.06 1.42 5.63
HE 2305-4414 23 08 12.5 -43 57 47 12.5 0.60 0.48 0.01 36 9.41 2.09 5.26
HE 2305-4748 23 08 35.0 -47 32 36 11.4 0.45 0.47 0.01 105 7.80 3.91 3.42
HE 2305-5724 23 08 41.5 -57 07 59 11.3 0.64 0.73 0.02 37 9.54 1.56 5.66
HE 2306-0746 23 09 00.2 -07 30 19 12.1 0.54 0.46 0.05 50 8.94 2.71 4.71
HE 2306-5638 23 09 00.7 -56 22 02 11.8 0.49 0.48 0.02 50 9.07 3.30 3.84
HE 2306-6012 23 09 10.6 -59 56 18 11.8 0.47 0.41 0.03 77 8.60 3.70 3.58
HE 2306-6022 23 09 33.8 -60 05 50 11.4 0.39 0.57 0.02 8 7.13 4.88 2.16
HE 2306-6041 23 09 55.9 -60 24 55 11.7 0.40 0.42 0.02 35 7.28 4.58 2.45
HE 2306-6223 23 09 52.8 -62 06 52 11.6 § § § 0.33 0.02 15 3.51 6.94 0.92
HE 2307-5702 23 10 44.4 -56 46 33 11.3 0.40 0.42 0.02 27 5.82 4.62 2.08
HE 2307-5855 23 10 28.6 -58 39 22 12.2 0.54 0.48 0.02 73 8.56 2.70 4.14
HE 2307-6028 23 10 14.2 -60 12 03 11.8 0.55 0.50 0.02 50 9.80 2.57 4.84
HE 2308-0359 23 11 08.9 -03 43 02 11.4 0.55 0.64 0.05 66 8.73 2.34 4.37

-- 69 --
Table 12---Continued
Star name R.A. # B (B - V ) HP2 (B - V ) J-K E (B-V) v rad KP HP2 GP Comm.
HE 2308-1759 23 10 58.8 -17 43 33 11.4 0.53 0.54 0.04 7 8.11 2.69 3.66
HE 2308-4434 23 11 37.0 -44 18 08 11.0 0.58 0.52 0.01 41 8.84 2.00 4.75
HE 2308-4610 23 11 44.2 -45 54 10 10.1 0.38 0.39 0.01 13 6.49 6.47 1.90
HE 2308-5613 23 11 10.6 -55 56 57 10.7 0.38 0.37 0.01 30 5.66 5.50 1.56
HE 2308-5933 23 11 09.8 -59 17 06 12.3 0.47 0.36 0.02 -34 8.23 3.68 2.98
HE 2308-6018 23 11 30.0 -60 02 34 12.2 0.43 0.45 0.02 43 6.84 4.17 2.48
HE 2308-6211 23 11 49.7 -61 55 29 11.6 0.60 0.55 0.02 10 9.17 2.17 4.86
HE 2309-0100 23 12 16.8 01 16 33 12.6 0.38 0.40 0.04 51 6.49 5.27 1.79
HE 2309-5601 23 12 27.4 -55 44 56 9.9 0.40 0.42 0.01 8 6.75 4.65 2.09
HE 2309-6102 23 12 27.6 -60 46 20 11.6 0.39 0.37 0.02 24 7.09 4.89 2.77
HE 2310-5711 23 13 24.5 -56 55 12 11.6 0.49 0.48 0.02 37 7.73 3.02 3.54
HE 2311-1242 23 14 14.6 -12 25 52 11.9 0.43 0.42 0.03 73 7.76 4.08 2.86
HE 2311-1828 23 14 19.7 -18 12 25 11.9 0.64 0.54 0.03 77 9.31 1.74 5.24
HE 2311-5248 23 14 01.0 -52 32 22 12.1 0.60 0.53 0.01 114 8.84 1.93 4.84
HE 2312-1443 23 15 24.2 -14 26 55 11.5 0.38 0.37 0.03 -46 5.77 5.57 1.57
HE 2313-5450 23 16 26.4 -54 33 49 10.9 § § § 0.37 0.01 8 3.62 7.32 1.84
HE 2314-1033 23 16 57.1 -10 17 34 12.0 0.38 0.42 0.03 18 5.82 5.17 1.62
HE 2314-1311 23 16 48.2 -12 55 01 11.7 0.41 0.41 0.03 -13 6.51 4.42 2.16
HE 2314-1750 23 17 31.4 -17 34 05 12.2 0.48 0.43 0.03 73 8.02 3.36 3.31
HE 2314-1753 23 17 17.8 -17 37 07 12.1 0.55 0.36 0.03 60 9.24 2.67 4.36
HE 2314-1920 23 17 01.9 -19 04 34 12.3 0.51 0.45 0.03 73 7.52 2.92 3.41
HE 2315-1808 23 18 20.2 -17 51 40 11.9 0.48 0.38 0.03 90 7.87 3.45 3.38
HE 2315-2053 23 17 48.5 -20 37 23 12.2 0.49 0.42 0.03 72 8.96 3.32 3.82
HE 2315-5337 23 18 15.4 -53 20 50 11.0 0.64 0.57 0.01 75 9.30 1.60 5.46
HE 2316-1839 23 19 09.1 -18 23 02 12.0 0.62 0.57 0.03 80 8.44 1.69 5.42
HE 2316-1900 23 18 57.8 -18 43 39 11.8 0.50 0.47 0.03 78 8.55 3.03 4.17
HE 2316-4252 23 18 54.5 -42 35 45 11.5 0.40 0.40 0.01 -17 6.30 4.63 1.75
HE 2318-5414 23 20 57.8 -53 58 04 11.0 0.64 0.62 0.01 62 9.15 1.55 5.28
HE 2318-5641 23 21 41.0 -56 24 44 11.8 0.48 0.47 0.01 45 7.99 3.42 3.12
HE 2319-5502 23 22 44.9 -54 45 42 10.5 0.59 0.55 0.01 26 8.60 1.82 4.85
HE 2319-5713 23 22 17.5 -56 57 31 11.5 0.56 0.81 0.01 33 1.74 1.94 3.87 dist
HE 2320-4713 23 23 23.8 -46 56 49 10.5 0.43 0.40 0.01 36 7.48 4.19 2.65
HE 2321-4250 23 24 21.1 -42 34 08 10.6 0.43 0.41 0.02 39 7.69 4.06 2.88
HE 2321-5515 23 24 27.4 -54 58 35 11.9 0.60 0.50 0.01 -10 9.16 2.16 4.84
HE 2321-5649 23 24 31.2 -56 32 54 10.7 0.45 0.44 0.02 9 7.57 3.90 2.81
HE 2322-0023 23 25 24.7 00 39 40 11.9 0.64 0.58 0.03 19 9.27 1.69 5.15
HE 2322-1754 23 24 52.1 -17 37 36 11.5 0.94 § § § 0.04 55 7.19 0.38 5.75 Em
HE 2322-5536 23 25 13.4 -55 19 37 11.0 0.60 0.61 0.01 74 8.96 1.94 4.43
HE 2322-5651 23 24 56.4 -56 35 22 12.0 0.48 0.47 0.01 -2 8.13 3.32 3.46
HE 2323-5502 23 26 13.7 -54 45 38 12.3 0.48 0.50 0.01 10 7.99 3.30 3.43
HE 2324-0038 23 26 46.3 00 55 05 11.9 0.43 0.61 0.04 7 7.10 4.07 2.35
HE 2324-0833 23 27 32.9 -08 16 33 11.3 0.44 0.45 0.03 57 6.80 3.89 2.41
HE 2324-4443 23 27 39.4 -44 26 30 10.5 § § § 0.31 0.01 10 2.55 7.74 1.28
HE 2324-5649 23 26 54.7 -56 33 01 11.7 0.56 0.52 0.02 0 8.81 2.38 4.69
HE 2325-0108 23 28 01.7 01 24 44 12.0 0.43 0.44 0.03 30 6.56 4.05 2.10
HE 2326-0129 23 28 42.2 01 45 58 12.3 0.48 0.44 0.03 28 7.32 3.32 3.24
HE 2326-0158 23 29 01.9 02 15 14 11.9 0.42 0.39 0.03 41 7.55 4.30 2.74
HE 2326-4555 23 29 42.0 -45 39 19 10.6 0.43 0.49 0.01 11 7.69 4.11 2.53
HE 2327-0159 23 30 03.1 02 16 20 12.0 0.52 0.55 0.04 21 6.46 2.55 3.43
HE 2327-3801 23 30 15.6 -37 45 11 11.3 0.77 0.52 0.02 66 9.25 0.89 5.89
HE 2327-4203 23 30 00.7 -41 47 15 10.6 0.46 0.37 0.02 82 8.26 3.96 3.25
HE 2327-4245 23 30 04.8 -42 28 43 10.6 0.37 0.35 0.02 52 § § § 5.36 0.00
HE 2327-4557 23 29 52.6 -45 40 43 11.6 0.39 0.42 0.01 -7 7.35 4.90 2.40
HE 2327-4806 23 30 03.8 -47 49 57 11.9 0.61 0.59 0.01 -60 9.00 1.80 5.11
HE 2330-0005 23 32 51.1 00 11 04 12.5 0.48 0.48 0.04 -22 7.56 3.30 3.41
HE 2330-4406 23 32 52.3 -43 49 54 10.4 0.55 0.50 0.01 60 9.14 2.72 4.20
HE 2331-1519 23 34 02.4 -15 02 29 10.5 0.38 0.38 0.03 31 6.18 5.84 1.87
HE 2331-3805 23 34 39.4 -37 49 08 12.3 0.37 0.39 0.02 41 4.65 5.88 1.34
HE 2332-4158 23 35 28.6 -41 41 42 11.0 0.64 0.27 0.02 -83 9.07 1.55 5.10
HE 2332-4431 23 35 24.5 -44 14 50 10.7 0.49 0.48 0.01 42 7.59 3.08 3.39
HE 2333-0855 23 35 47.8 -08 39 13 10.7 0.48 0.47 0.03 -214 8.00 3.45 3.58
HE 2333-1322 23 35 56.2 -13 06 13 10.8 0.37 0.41 0.03 -17 4.72 5.77 1.38
HE 2333-1401 23 36 12.2 -13 45 17 11.0 0.94 0.81 0.03 -45 7.13 0.27 5.23 Em
HE 2333-4008 23 35 41.0 -39 52 13 10.9 0.40 0.41 0.02 42 7.18 4.67 2.23
HE 2333-4047 23 36 16.1 -40 30 56 11.1 0.54 0.46 0.02 81 8.90 2.74 4.29
HE 2333-4237 23 35 44.4 -42 20 25 11.5 0.47 0.46 0.02 52 8.59 3.52 3.45
HE 2333-4325 23 35 41.5 -43 09 02 11.1 0.43 0.44 0.01 30 7.22 4.14 2.55

-- 70 --
Table 12---Continued
Star name R.A. # B (B - V ) HP2 (B - V ) J-K E (B-V) v rad KP HP2 GP Comm.
HE 2333-6215 23 35 50.9 -61 59 08 11.6 0.67 0.57 0.02 82 9.37 1.36 5.49
HE 2334-1710 23 37 24.7 -16 53 42 10.3 0.38 0.37 0.03 -32 7.00 5.11 2.07
HE 2334-3736 23 37 13.0 -37 19 45 11.9 0.53 0.51 0.02 21 8.13 2.64 3.76
HE 2334-6144 23 37 42.5 -61 27 28 12.6 0.46 0.42 0.02 19 7.20 3.50 2.77
HE 2334-6146 23 37 28.8 -61 30 17 11.5 0.49 0.52 0.02 39 8.34 3.45 3.52
HE 2335-5943 23 38 02.9 -59 26 29 11.9 0.38 0.46 0.01 27 6.28 5.31 1.88
HE 2336-3554 23 39 16.3 -35 37 26 9.6 § § § 0.38 0.02 19 3.78 7.56 1.19
HE 2336-5905 23 38 54.0 -58 48 59 12.0 0.61 0.57 0.02 53 9.04 1.93 5.22
HE 2337-1858 23 39 44.2 -18 42 08 11.4 0.62 0.62 0.03 -57 8.58 1.59 5.23
HE 2337-5354 23 39 44.2 -53 37 56 11.1 0.56 0.45 0.01 46 8.97 2.46 4.38
HE 2337-5805 23 40 31.4 -57 49 05 12.5 0.40 0.46 0.02 101 6.46 4.62 2.03
HE 2338-5636 23 41 04.3 -56 20 14 11.5 0.52 0.51 0.01 76 8.51 2.90 3.76
HE 2340-1521A 23 43 16.3 -15 04 55 10.7 0.40 § § § 0.03 -24 6.94 4.51 2.12
HE 2340-1521 23 43 16.3 -15 04 55 10.7 0.42 § § § 0.03 7 7.16 4.32 1.91
HE 2340-2548 23 42 46.8 -25 32 06 11.5 0.47 0.45 0.02 -30 8.29 3.69 3.29
HE 2340-5340 23 43 40.1 -53 24 19 11.5 0.59 0.48 0.01 58 8.48 1.91 4.52
HE 2340-6156 23 42 55.2 -61 39 53 11.9 § § § 0.31 0.02 70 3.21 7.78 1.34
HE 2341-6128 23 44 27.1 -61 11 32 11.8 0.48 0.47 0.02 25 7.29 3.41 2.89
HE 2342-1319 23 45 12.2 -13 02 25 11.1 0.56 0.53 0.03 46 8.81 2.35 4.51
HE 2342-3815 23 45 08.2 -37 59 14 11.6 0.37 0.36 0.01 167 3.60 5.96 0.90
HE 2342-5728 23 44 43.2 -57 11 42 11.7 0.38 0.39 0.02 61 5.94 5.44 1.57
HE 2342-5733 23 45 32.9 -57 16 49 11.2 0.38 0.34 0.02 29 5.88 6.25 1.56
HE 2342-6054 23 45 07.7 -60 37 53 11.8 0.47 0.41 0.01 60 8.56 3.67 3.42
HE 2343-0203 23 46 03.8 -01 47 00 11.8 0.57 0.48 0.03 50 8.72 2.08 3.78
HE 2343-1346 23 45 56.6 -13 29 59 11.1 0.58 0.57 0.03 68 8.90 2.13 4.68
HE 2343-1706 23 46 13.9 -16 49 52 10.7 0.61 0.57 0.03 62 9.14 1.77 4.85
HE 2343-5631 23 45 55.9 -56 15 00 12.0 0.62 0.60 0.01 47 9.27 1.83 5.48
HE 2343-5954 23 46 12.7 -59 37 45 12.1 0.48 0.45 0.01 58 8.23 3.30 3.55
HE 2343-6014 23 46 37.4 -59 58 08 11.7 0.83 0.54 0.01 25 9.16 0.59 5.84
HE 2343-6041 23 45 48.7 -60 24 32 11.7 0.45 0.47 0.01 60 7.56 3.89 2.77
HE 2343-6050 23 46 10.1 -60 33 52 11.3 0.47 0.46 0.01 2 8.64 3.53 3.66
HE 2344-6102 23 47 39.4 -60 45 50 13.1 1.00 1.04 0.01 30 7.73 § § § 5.80 Em
HE 2345-1328 23 48 22.6 -13 12 11 11.0 0.51 0.47 0.02 34 8.76 3.07 4.06
HE 2345-4921 23 48 03.1 -49 05 15 12.2 0.48 0.53 0.01 -11 7.42 3.35 3.20
HE 2345-5912 23 47 51.6 -58 55 59 11.6 0.60 0.47 0.01 5 8.99 1.94 4.95
HE 2346-0244 23 49 01.0 -02 28 07 11.0 0.47 0.37 0.04 -5 8.61 3.71 3.28
HE 2346-1336 23 49 31.0 -13 19 26 11.3 0.38 0.40 0.03 1 6.24 5.22 1.94
HE 2346-4205 23 49 22.1 -41 48 50 11.5 0.40 0.39 0.02 22 6.79 4.72 2.15
HE 2346-5634 23 49 35.3 -56 17 26 12.5 0.52 0.50 0.01 39 7.70 2.51 3.79
HE 2346-6144 23 49 32.2 -61 28 16 12.0 0.45 § § § 0.02 -4 7.17 3.95 2.75
HE 2347-0036 23 50 31.2 00 52 45 11.3 0.52 0.47 0.03 53 8.62 2.77 3.86
HE 2347-5123 23 49 55.4 -51 06 44 11.5 0.50 0.48 0.02 30 7.90 3.10 3.61
HE 2347-5609 23 50 16.1 -55 52 32 8.9 0.43 0.41 0.01 -22 7.09 4.15 2.30
HE 2347-6137 23 49 59.8 -61 20 24 11.9 0.51 0.40 0.02 50 8.28 2.90 3.70
HE 2348-1232 23 51 01.0 -12 15 33 12.0 0.40 0.43 0.03 5 6.82 4.54 2.11
HE 2348-4322 23 50 54.2 -43 05 28 10.5 0.55 0.48 0.02 -39 8.37 2.40 4.09
HE 2349-1226 23 51 39.8 -12 09 39 10.8 0.63 0.52 0.03 1 8.95 1.57 5.08
HE 2349-1302 23 52 20.9 -12 46 08 10.8 0.45 0.41 0.02 58 7.59 3.77 2.72
HE 2349-3211 23 52 04.1 -31 55 13 10.4 0.45 § § § 0.01 63 8.16 3.92 2.96
HE 2349-3740 23 52 07.0 -37 23 20 11.1 0.58 0.50 0.01 31 8.91 2.11 5.06
HE 2349-4703 23 52 36.0 -46 46 52 12.3 0.53 0.47 0.01 28 8.44 2.53 3.52
HE 2349-5605 23 52 01.4 -55 49 10 12.2 0.60 0.66 0.01 4 8.94 1.94 5.27
HE 2350-1324 23 52 51.1 -13 07 53 11.0 0.51 0.51 0.03 14 8.39 2.97 3.88
HE 2350-4646 23 52 53.5 -46 29 35 11.4 0.46 0.44 0.01 45 7.38 3.69 2.72
HE 2350-5359 23 53 11.5 -53 42 26 11.7 0.72 0.65 0.01 -18 9.53 1.12 5.65
HE 2351-4807 23 53 44.6 -47 51 07 12.2 0.40 0.43 0.01 5 6.41 4.69 1.89
HE 2352-5547 23 55 30.2 -55 30 49 12.2 0.59 0.45 0.01 22 8.58 1.91 4.33
HE 2353-5609 23 55 55.2 -55 52 39 11.6 0.69 0.53 0.01 4 8.39 1.16 5.53
HE 2354-1937 23 57 19.0 -19 20 39 13.5 1.00 0.77 0.02 -73 10.51 0.18 6.16
HE 2354-5226 23 56 41.5 -52 10 06 12.5 0.55 0.50 0.01 -39 8.52 2.39 4.23
HE 2354-5336 23 56 36.7 -53 19 40 12.4 0.43 0.39 0.02 42 7.64 4.05 2.61
HE 2354-5407 23 56 35.8 -53 50 55 12.5 0.37 0.35 0.01 11 4.61 5.72 1.14
HE 2354-5547 23 56 58.6 -55 31 09 12.5 0.58 0.47 0.01 8 8.84 2.11 4.42
HE 2355-2030 23 57 58.3 -20 14 15 11.7 0.45 0.48 0.02 4 7.56 3.99 2.72
HE 2355-2053 23 58 08.4 -20 37 03 11.3 0.45 0.42 0.02 7 7.56 3.99 2.72
HE 2355-2210 23 58 24.2 -21 53 59 10.3 0.64 0.50 0.02 59 9.34 1.51 5.60
HE 2355-4740 23 57 53.3 -47 23 25 12.9 0.46 0.42 0.01 13 7.56 3.61 2.96

-- 71 --
Table 12---Continued
Star name R.A. # B (B - V ) HP2 (B - V ) J-K E (B-V) v rad KP HP2 GP Comm.
HE 2355-5318 23 57 50.4 -53 01 58 11.7 0.43 0.43 0.02 -18 7.96 4.01 3.08
HE 2355-5502 23 57 38.6 -54 45 55 11.9 0.53 0.54 0.01 -6 8.15 2.69 3.93
HE 2355-5556 23 57 40.1 -55 39 59 12.2 0.60 0.53 0.01 7 9.08 2.23 4.43
HE 2356-2907 23 59 26.6 -28 51 14 10.2 0.42 § § § 0.02 5 7.56 4.34 2.57
HE 2356-5656 23 58 55.0 -56 39 48 12.6 0.43 0.40 0.01 85 7.26 4.06 2.84
HE 2357-3940 00 00 20.1 -39 23 56 10.1 0.38 0.13 0.01 -14 0.10 4.58 § § § He
HE 2358-1940 00 01 11.1 -19 24 12 12.2 0.42 0.39 0.02 64 7.21 4.37 2.36
HE 2358-2411 00 01 15.4 -23 54 19 11.9 0.41 0.46 0.02 3 6.88 4.41 2.56
HE 2358-3634 00 01 05.5 -36 17 52 11.7 0.46 0.45 0.01 0 8.47 3.75 3.76
HE 2359-0224 00 02 17.3 -02 08 16 9.8 0.52 § § § 0.04 11 8.52 2.79 3.87
HE 2359-0714 00 02 01.9 -06 57 57 11.0 0.41 0.44 0.04 89 6.70 4.25 2.21
HE 2359-2013 00 01 37.0 -19 56 32 12.1 0.55 0.47 0.02 24 9.27 2.51 4.10
HE 2359-2235 00 02 15.4 -22 19 04 12.2 0.50 0.43 0.02 9 7.91 3.13 3.46
HE 2359-2347 00 02 00.8 -23 30 51 11.9 0.50 0.44 0.02 17 8.45 3.20 4.13
HE 2359-2604 00 01 49.6 -25 47 46 8.8 0.37 § § § 0.01 41 3.51 6.50 0.94
HE 2359-3142 00 02 17.0 -31 26 05 10.1 0.58 0.49 0.01 8 8.94 2.00 4.37
HE 2359-4225 00 02 05.3 -42 08 59 11.1 0.49 0.49 0.01 21 8.46 3.28 3.74
Note. --- HB=Horizontal Branch, He=He lines in the spectrum, Em=Emission lines in the spectrum, pec= , dist=distorted Ca K line,
comp=possibly composited spectrum of two objects

-- 72 --
Table 13. Typical uncertainties in the [Fe/H] and [C/Fe] measurements
# B-V (0.06) # J-K (0.03) #KP (0.18) # HP2 (0.20) #GP (0.15)
(a)/(b) (a)/(b) (a)/(b) (a)/(b) (a)/(b)
[Fe/H] B-V 0.17/0.45 c
§ § § 0.06/0.09 § § § § § §
[Fe/H] HP2 § § § § § § 0.07/0.08 0.05/0.11 d
§ § §
[Fe/H] Rossi § § § 0.13/0.13 0.05/0.05 § § § § § §
[C/Fe] § § § § § § 0.06/0.04 § § § 0.06/0.05
a Derived from stars with [Fe/H] < -2.
b Derived from stars with [Fe/H] > -2.
c Values derived for dwarfs (i.e., HP2 > 2.5). For giants, the uncertainties are
0.25/0.50 based on # B-V = 0.10.
d Values derived for dwarfs. For giants, the uncertainties are 0.15/0.13.

-- 73 --
Fig. 1.--- Spectra displaying a sequence of saturation levels occurring in the survey. For
comparison purposes, the three stars have been chosen to have similar color (B - V #
0.45). Saturation of the emulsion depends on the brightness of the object and the individual
photographic plate. Typically, from # 10, 000 counts onwards, the spectra are formed in
the nonílinear part of the characteristic curve of the photographic emulsion (which slightly
varies with each plate). We call these spectra ``saturated''. However, as shown in this figure
the level of saturation varies and hence the recoverability of the data. The spectrum in the
upper panel has been chosen in the visual selection as completely saturated (sat) and was
excluded from further processing (for the definitions of the di#erent classes see the text). The
middle panel shows a spectrum which has been regarded as recoverable and thus selected as
mpcc (see ç 2.4). For comparison, an unsaturated spectrum is shown in the lower panel.

-- 74 --
Fig. 2.--- Comparison of the B magnitude for the 85 stars in the sample (open circles) with
available CCD photometry and the 298 HK calibration stars with photoelectric photometry
(crosses). A typical error bar is also shown. As can be seen, the HK calibration sample is
fainter than B # 13 and the agreement with the HES magnitudes is suitable for the search
for metalípoor stars. However, no information could be gained concerning the magnitude
quality of the brighter stars. This was only achieved after mediumíresolution followíup
observations. The additional photometric data of brighter stars revealed that the HES
magnitude measurements are somewhat influenced by the saturation e#ects. The accuracy
of the magnitudes was considered su#cient for our current work.

-- 75 --
Fig. 3.--- Comparison of the KP index for all sample stars on the photographic plates and
in the mediumíresolution followíup spectra. The measurement accuracy of the survey index
is clearly a#ected by saturation of the spectra of stars with B < 13. A typical error bar is
shown in the bottom panel. See text for further details.

-- 76 --
Fig. 4.--- Comparison of CCD/photoelectric and survey B - V colors as a function of
brightness. Symbols are the same as in Figure 2. The scatter becomes much larger for stars
brighter that B = 13, which reflects the onset of saturation e#ects in the spectra of these
objects. A typical error bar is shown for the fainter stars.

-- 77 --
Fig. 5.--- Examples of objectiveíprism spectra (left panel) of the four di#erent classes of
metalípoor candidates and their corresponding mediumíresolution followíup spectra (right
panel). From the top: classes mpcc, mpcb, unid and mpca. In the insets we show an expansion
of the Ca II K region by which the survey spectra were classified. For further description
of the classes, see text. We list the telescope employed at the top right corner. The KP and
HP2 index, the (B - V ) 0 color and the final iron abundance of each star are shown next to
the followíup spectra (see ç 3.2 for more details on the indices). Despite the classification,
there is no strong correlation between iron abundance and class.

-- 78 --
Fig. 6.--- B magnitude distribution for the bright HES stars, the HK survey stars and the
faint HES stars. The magnitude ranges of the samples complement each other and span
a large range, from B # 9 to B # 18. Top panel : Note that the bimodal distribution of
the bright and faint HES stars is due to a selection bias in the sample of bright HES stars
(see text for details). Bottom panel : Same distribution as above, but the displayed stars are
confirmed to have [Fe/H] < -2.0 by followíup spectroscopy, and randomly selected such that
the total numbers of HK survey stars, bright HES and faint HES stars are the same (i.e.,
150). Note the smooth distribution, and the removal of the strong selection bias towards
bright stars in the sample of bright HES stars that can be seen in the top panel.

-- 79 --
Fig. 7.--- B-V color distribution for the bright metalípoor candidate sample as derived from
the 2MASS J -K data. When selecting the sample from the HES database, a temperature
cutío# at B - V = 0.3 has been made, based on the original HES colors. Due to the new
colors, a few stars now have B - V < 0.3 which is slightly hotter than has been regarded
useful for our search. It is interesting to note here that the sample selected on the basis
of the HES colors was originally thought to contain mostly giants. The new B - V colors
distribution suggests that the majority of the sample stars are dwarfs and field horizontal
branch stars. This color shift is also reflected in Figure 4.

-- 80 --
Fig. 8.--- Metallicity distribution (MDF) of some 4700 HK survey (upper panel) stars comí
pared to our 293 metalípoor stars (lower panel). See text for discussion.

-- 81 --
Fig. 9.--- Sequence of spectra of GPístrong stars. Top panel: The only CH feature visible
is the Gíband at # 4300 Ú A. Middle panel: In addition to the Gíband, strong CN molecular
bands (3883 and 4215 Ú A) are also present. These are already clearly visible in the survey
spectrum. Bottom panel: The features are even stronger and C 2 bands become visible at
e.g., 4738 and 5165 Ú A.

-- 82 --
Fig. 10.--- [C/Fe] for all stars with [Fe/H] < -1.0 as a function of [Fe/H]. An increased
spread of [C/Fe] with decreasing metallicity is clearly seen.

-- 83 --
Fig. 11.--- Cumulative frequency of CEMP objects amongst metalípoor stars as function of
the distance from the Galactic Plane Z. Note that the cumulative fraction is defined as the
number of Cíenhanced objects amongst metalípoor stars further from the Plane than the
indicated Z. Top panel : The frequencies for both our and the BPSII sample. Middle panel :
Combined data set with [Fe/H] < -2.0, overplotted with Poisson errorbars. Bottom panel :
Same as middle panel, but for subset of stars with [Fe/H] < -3.0. See text for discussion.

-- 84 --
Fig. 12.--- Cumulative percentages of normal metalípoor (top curve) and CEMP stars (botí
tom curve) as a function of distance from the Galactic Plane Z. Based on the K--S test, the
two samples come from di#erent populations for Z # 2 kpc. See text for discussion.

-- 85 --
Fig. 13.--- Comparison of our final metallicity estimates for rediscovered stars with values
derived from mediumí (filled circles) and highíresolution (open circles) spectra available in
the literature (see Table 3 and text for further details).

-- 86 --
Fig. 14.--- Example of an emissioníline object found in our sample. As CS 31077í034, this
star was classified by Beers et al. (1996a) to have ``moderate'' Ca II H and K emission.