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c2d Lupus Synthesis June 10, 2008

The Spitzer c2d Survey of Large, Nearby, Interstellar Clouds. XI. Lupus Observed With IRAC and MIPS
Bruno Mer´n1,2 , Jes JÜrgensen3 , Loredana Spezzi4 , Juan M. Alcal´4 , Neal J. Evans II5 , i a 5 6 7 Paul M. Harvey , Nicholas Chapman , Tracy Huard , Ewine F. van Disho eck2 , Fernando Comer´n8 o ABSTRACT We present c2d Spitzer/IRAC observations of the Lupus I, III and IV dark clouds and discuss them in combination with optical and near-infrared and c2d MIPS data. With the Spitzer data, the new sample contains 159 stars, 4 times larger than the previous one. It is dominated by low- and very-low mass stars and it is complete down to M 0.1M . We find 30-40% binaries with separations between 100 to 2000 AU with no apparent effect in the disk properties of the members. A large ma jority of the ob jects are Class II or Class III ob jects, with only 20 (12%) of Class I or Flat spectrum sources. The disk sample is complete down to "debris"-like systems in stars as small as M 0.2 M and includes sub-stellar ob jects with larger IR excesses. The disk fraction in Lupus is 70 ­ 80%, consistent with an age of 1 ­ 2 Myr. However, the young population contains 20% optically thick accretion disks and 40% relatively less flared disks. A growing variety of inner disk structures is found for larger inner disk clearings for
Research and Scientific Support Department, European Space Agency (ESTEC), PO Box 299, 2200 AG Noordwijk, The Netherlands
2 3 4 5 1

arXiv:0803.1504v1 [astro-ph] 10 Mar 2008

Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands Argelander-Institut fur Astronomie, University of Bonn, Auf dem Hugel 71, 53121 Bon, Germany ¨ ¨ INAF - Osservatorio Astronomico di Capodimonte, via Moiariello 16, I-80131, Naples, Italy

Department of Astronomy, University of Texas at Austin, 1 University Station C1400 Austin, TX 787120259, USA
6 7 7

Astronomy Department, University of Maryland, College Park, MD 20742, USA Smithsonian Astrophysical Observatory, 60 Garden Street, MS42, Cambridge, MA 02138, USA European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching bei Munchen, Germany ¨


­2­ equal disk masses. Lupus III is the most centrally populated and rich, followed by Lupus I with a filamentary structure and by Lupus IV, where a very high density core with little star-formation activity has been found. We estimate star formation rates in Lupus of 2 ­ 10 M Myr-1 and star formation efficiencies of a few percent, apparently correlated with the asso ciated cloud masses. Subject headings: stars: formation ­ stars: pre-main sequence ­ stars: low-mass star-forming-regions:individual (Lupus I, Lupus III, Lupus IV)

1.

Introduction

The Lupus dark cloud complex is one of the main low-mass star forming regions within 200 pc of the sun. Lo cated in the Scorpius-Centaurus OB asso ciation, it consists of a lo osely connected group of dark clouds and low-mass pre-main sequence stars lo cated between galactic co ordinates 334o < l < 352o and latitudes +5o < b < +25o (RA 16h 20m ­ 15h 30 and DEC -43o00 ­ -33o00 ) (Krautter 1991). The low ecliptic latitudes ( -33 ­ -41) of the clouds guarantee a low abundance of asteroids. Given its large size ( 20o ) and proximity, it has been sub ject of many studies. Large-scale 12 CO (J = 1 0) millimeter maps of the whole complex give total molecular gas masses of several times 104 M (Murphy et al. 1986; Tachihara et al. 2001) and a relatively small spread of cloud velo cities among the different sub-clouds ( 3 km s-1 Vilas-Boas et al. 2000). It hosts four active star-forming regions, including the rich T Tauri asso ciation in Lupus 3, plus five other lo oser dark clouds with signs of mo derate star-formation activity (Hara et al. 1999). Ob jects in all evolutionary phases, from embedded Class I ob jects to evolved Class III stars, are found in the Lupus clouds. A comprehensive review about the Lupus clouds by Comer´n (2008) provides more o details on previous observations and is used throughout this work to assess the new results from the Spitzer data. The Lupus dark cloud is one of the five large nearby star-forming regions observed as part of the Spitzer Legacy Pro ject "From Molecular Cores to Planetforming Disks" (c2d) Evans et al. (2003). From the several Lupus subclouds (Th´ 1962; e Murphy et al. 1986), only Lupus I, III and IV were observed by c2d and are discussed in this paper. Optical and near-infrared (near-IR) ground-based observations of Lupus identified three regions, denominated as Lupus I, II and III, with large numbers of classical T Tauri stars (Henize 1954; Th´ 1962). Schwartz (1977) made a catalog of H emitting young stars which e contained the vast ma jority of the ob jects in the clouds known until to day. His observations also showed that Lupus 3 (roughly consistent with Cambr´sy's Lupus III) is one of the most e active star-forming regions in the southern sky, followed by Lupus I, II and IV and that a


­3­ large number of the stars in these clouds are low-mass stars. In addition to these classical T Tauri stars, Krautter et al. (1997) reported a much larger number of weak-line T Tauri stars with X-ray emission, which are believed to be older stars not physically bound to the dark clouds but rather belonging to a more nearby structure (Wichmann et al. 1999, see also Cieza et al. 2007 for a confirmation of this conclusion from c2d observations). Finally, there is evidence for different distances to the different subclouds: Hipparcos parallaxes and extinction source counts yield reasonable distance estimates of 150 ± 20 pc for Lupus I and IV and 200 ± 20 pc for Lupus III (Comer´n 2008 in prep. and references therein), which we o assume for this work. Following previous c2d standards, observational results from the Spitzer Space Telescope (Werner et al. 2004) Infrared Array Camera (IRAC, Fazio et al. 2004) and from the Multiband Imaging Photometer for Spitzer (MIPS, Rieke et al. 2004) are reported separately for each cloud, followed by a "synthesis" paper which combines all the c2d Spitzer and complementary observations made of the region (see e.g. Harvey et al. 2006, 2007b,a for Serpens or Young et al. 2005; Porras et al. 2007, and Alcal´ et al. 2008 for Chamaeleon II). For Lupus, a the observational results obtained with MIPS have been reported by Chapman et al. (2007) (Paper I) and this paper describes the IRAC observations and analyzes the complete data set for the region. In that sense, this paper merges the contents of the IRAC and "synthesis" papers of the c2d observations in Lupus: it presents the 3.6 to 8.0 µm IRAC observations of the clouds for the first time and combines it with all previously available information from the optical to the millimeter. All the observations analysed in this study are presented in § 2, with a discussion of the complementary observations and stellar multiplicity in the optical in § 2.1 and a detailed description of the Spitzer IRAC observations in § 2.2 and 2.3. These data are used to construct a high-reliability catalog of young stars in the clouds in § 3. This catalog is composed of Young Stellar Ob jects (YSO) identified with the Spitzer data (selected in § 3.1) and previously known Pre-Main Sequence stars (PMS, discussed in § 3.2). The rest of the paper is organized in two main sections, which deal with the individual sources (§ 4) and with the global cloud properties (§ 5), respectively. In the first one, the disk populations are studied with color-color diagrams (§ 4.1), multi-wavelength Spectral Energy Distributions (SEDs, § 4.2), stellar and disk luminosity functions (§ 4.3 and 4.4), and finally with a new `2D' classification system of the SEDs (§ 4.5). The Spitzer observations of outflows and HerbigHaro ob jects in the region are also described in § 4.6. The second section describes the structures of the clouds with the help of Spitzer-derived extinction maps (§ 5.1), the spatial distribution of the YSOs in the clouds and a nearest-neighbor analysis of their clustering properties (§ 5.2). Finally, the Star Formation Rates and Star Formation Efficiencies are computed and discussed in § 5.3 and 5.4, respectively. A complete summary of this work is


­4­ given in § 6.

2.

Observations and data analysis

The observations discussed in this paper come from the Spitzer Space Telescope's Infrared Array Camera (IRAC hereafter) and Multiband Imaging Photometer for Spitzer (MIPS) observations of Lupus I, III and IV made by the c2d Spitzer Legacy Program (Evans et al. 2003), together with an optical co ordinated survey of the three clouds (F. Comer´n et al., in preparation) and data from the literature. Detailed information about o the MIPS observations can be found in Chapman et al. (2007).

2.1.

Complementary data and multiple visual systems

An optical survey of the three clouds was performed with the Wide-Field Imager (WFI) attached to the ESO 2.2m telescope, at La Silla Observatory in Chile. The areas observed in the RC (0.652 µm), IC (0.784 µm), and zW F I (0.957 µm) optical bands in Lupus I, III and IV were defined to overlap completely with the areas observed with Spitzer shown in Figures 1 to 3. The observational strategy, data reduction and source extraction are described in detail elsewhere (F. Comer´n et al., in preparation). These observations were complemented o with photometry from the NOMAD optical and near-IR catalog (Zacharias et al. 2005), which contains B , V and RC magnitudes and from the J , H and KS 2MASS near-IR allsky catalog (Cutri et al. 2003). This paper also includes the c2d MIPS observations of the Lupus clouds. Figures 19 to 22 also show the areas mapped with MIPS at 24, 70 and 160 µm as part of the c2d pro ject. They were defined to provide the maximum overlap and minimum observing time and cover completely the areas mapped with IRAC. The MIPS data acquisition, reduction and source extraction is presented and discussed in detail in Chapman et al. (2007). The optical images were inspected to search for visual binaries in the sample. Table 10 reports all apparent companions detected in the images. The WFI images in Rc, I c and zW F I bands were inspected for all sources. Those observations were performed in service mo de over several nights in two different observing seasons and have a range of seeing values, but an average seeing of 1.5 limits the smallest separation detectable to 0.7 in our case. The range of separations for which we report the presence of possible companions is 0.7 to 10 (140 to 2000 AU in Lupus III and 105 to 1500 AU at the distance of Lupus I and IV). There are several pairs of stars with disks which are binaries. Inspection of the optical


­5­ images indicates that the probability of pro jection effects might be small given the relatively low number of optical sources at distances smaller than 10 in most of the examined stars. We recover all binaries listed by Ghez et al. (1997) which fell in our field except HR 5999, which was to o bright to allow a shape analysis. We also recover the two ob jects in common with a yet unpublished AO/ADONIS survey of multiplicity in Lupus which probe at angular distances as close as 0.2 (A. Kno ckx et al., in prep.). The total binary fractions of 41±12% (7/17), 29±9% (39/124) and 44±13% (8/18) in the three clouds, respectively, compare well with the numbers given for Taurus and Ophiuchus in a similar range of angular distances (e.g. Padgett et al. 1997). In any case, given the difficulty in apportioning the excess among the companions with separations smaller than 2.0 , in which the IRAC fluxes could have been merged, and those with separations smaller than 4.0 , which could have merged fluxes in MIPS, we set those fluxes as upper limits in the SEDs for the disk evolution studies. More discussion on the effects of binarity in the disks is presented in § 4.4.

2.2.

Spitzer IRAC data

Lupus I, Lupus III and Lupus IV were observed with all IRAC bands (3.6, 4.5, 5.8 and 8.0 µm) on the 3rd and 4th of September of 2004 as part of the c2d Spitzer Legacy Program (P.I.: N. Evans, program ID: 174) and as part of GTO observations (P.I.: G. Fazio, program ID: 6). The total observed areas were defined to cover all the regions with extinctions AV 2 for Lupus III and IV and AV 3 for Lupus I (see Fig. 2 of Evans et al. 2003) as measured in the extinction maps by Cambr´sy (1999). The combined mosaics of the three regions e overlap in all IRAC bands with areas of 1.39, 1.34 and 0.37 deg2 in Lupus I, Lupus III and Lupus IV, respectively. Furthermore 4 off-cloud regions, each of 0.08 deg2 were observed in low-extinction regions with a range of galactic latitudes for statistical comparison with the on-cloud fields. Each of them contains a 0.05 deg2 overlap between all IRAC bands. All c2d maps were observed in two epo chs at least 6 hours apart to guarantee the pro duction of highly reliable catalogs of sources clean of asteroids and transient artifacts. The GTO observation of Lupus III was only observed once. For more information about the c2d mapping strategies, metho ds and results, consult the delivery do cumentation (Evans et al. 2007). Table 1 shows the details of the individual pointings for all three clouds and the off cloud regions. Figures 19 to 22 show the different coverages of the c2d IRAC, MIPS and optical mosaic areas overlaid on the optical extinction map of Lupus from Cambr´sy (1999). e


­6­

Table 1: c2d Spitzer IRAC Observations summary in Lupus Field Position (, )J 2000 Date (2004) AOR epo ch 1 Lupus I c2d Observations (15:45:09.0, -34:23:11.0) Sept 3 0005717248 LupI 1 LupI 2 (15:43:26.0, -34:06:27.0) Sept 3 0005717504 LupI 2a (15:42:23.0, -34:00:55.0) Sept 3 0005717760 (15:41:16.0, -33:43:33.0) Sept 3 0005718272 LupI 3 LupI 4 (15:40:08.0, -33:35:16.0) Sept 3 0005718528 (15:38:34.0, -33:20:18.0) Sept 3 0005718784 LupI 5 LupI 6 (15:39:09.0, -34:23:11.0) Sept 3 0005717248 (15:40:34.0, -34:36:34.0) Sept 3,4 0005719296 LupI 7 LupI 8 (15:38:08.0, -34:39:27.0) Sept 3 0005719552 (15:42:18.0, -34:33:50.0) Sept 3 0005737472 LupI 9 LupI 10 (15:40:55.0, -34:06:31.0) Sept 3,4 0005739008 Lupus III c2d Observations LupIII 1 (16:12:28.0, -38:05:43.0) Sept 4 0005724416 Sept 4 0005724672 LupIII 2 (16:10:35.0, -37:50:04.0) LupIII 3 (16:11:59.0, -38:58:30.0) Sept 4 0005724928 Sept 4 0005725184 LupIII 4 (16:10:32.0, -39:07:18.0) LupIII 6 (16:07:24.0, -39:07:03.0) Sept 4 0005725440 Sept 4 0005737984 LupIII 7 (16:12:45.0, -38:31:31.0) LupIII 8 (16:10:38.0, -38:35:24.0) Sept 4 0005738496 Lupus III GTO & c2d Observations Sept 4 0003652608 LupIII 5 (16:08:55.8, -39:08:33.2) Lupus IV c2d Observations LupIV 1 (16:02:46.0, -41:59:49.0) Sept 4 0005728768 LupIV 2 (16:01:27.0, -41:41:00.0) Sept 4 0005729024 Sept 4 0005729280 LupIV 3 (16:00:43.0, -42:02:37.0) Off-Cloud c2d Observations LupOC 2 (16:13:00.0, -34:00:00.0) Sept 4 0005731072 LupOC 6 (16:40:00.0, -40:30:00.0) Sept 4 0005732096 Sept 3 0005732352 LupOC 7 (15:50:00.0, -41:00:00.0) LupOC 8 (16:07:00.0, -43:00:00.0) Sept 4 0005732608

AOR epo ch 2 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 5 5 5 5 5 5 5 5 5 5 5 5 5 5 5 5 5 5 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 7 1 2 2 2 2 2 2 2 2 3 3 2 2 2 2 2 3 3 9 0 0 0 1 1 1 1 2 7 9 5 5 6 6 6 8 8 808 064 320 832 088 344 600 856 112 728 264 6 9 2 4 9 2 7 9 5 0 6 7 4 5 6 2 8 4 6 0 2

0005726720 0005729536 0005729792 0005730048 0 0 0 0 0 0 0 0 0 0 0 0 5 5 5 5 7 7 7 7 3 3 3 3 5 6 6 7 6 7 9 2 8 0 6 1 0 4 0 6


­7­ The IRAC images were pro cessed by the Spitzer Science Center (SSC) using the standard pipeline version S13 to pro duce the Basic Calibrated Data (BCDs). These images were then pro cessed and combined into mosaics and source catalogs by the c2d pipeline version 2007/January. Harvey et al. (2006) and JÜrgensen et al. (2006) describe in detail the pro cessing of the IRAC images for Serpens and Perseus, respectively. The observations presented here were pro cessed in exactly the same way so we refer the reader to those articles and to the Delivery Do cumentation for details about the data reduction. Here we will just describe briefly the basic steps carried out to pro duce the presented images and catalogs. In total 63384, 138270 and 42737 sources were detected with at least IRAC in Lupus I, III and IV, respectively. Table 2 summarizes the number of sources detected in the three surveyed areas with S/N of at least 5. This corresponds to selecting all sources with detections of quality `A' or `B' in any of the IRAC bands from the delivered c2d catalogs. Most of the sources in this catalog can be well fitted with reddened stellar atmospheres from field stars. IRAC bands 1 and 2 are the most sensitive in all three catalogs and pro duce an average of 7 times more high quality detections than those in IRAC bands 3 and 4. About 300, 400, and 350 sources in Lupus I, III and IV respectively of the four band detections are found to be extended in one or more bands (classified with the "image type" 2 in the c2d catalogs). Our final catalogs contain 2776, 7539 and 2403 four-band IRAC sources in the three Lupus clouds, respectively (see Table 2). Table 2: Total numbers of IRAC sources detected with S/N Lupus I Detection in at least one IRAC band 63384 Detection in all four IRAC bands 2834 Detection in three IRAC bands 3012 Detection in two IRAC bands 29301 Detection in one IRAC band 28237 Detection in 2MASS onlya 0 Detection in IRAC only 562 a Detection in 4 IRAC bands and not 2MASS 136 Excluding extended sources Four band detections 277 a Four band detections with 2MASS asso ciation 263 Detected in IRAC1+2 and 2MASSa 691 A source is counted as detected in 2MASS if it has a 5 in Lupus Lupus III Lupus IV 138270 42737 7638 2418 6559 2001 67039 21125 57034 17193 7 122166 268 753 724 157 of at 6 4 02 least 1 1 37904 80 24 22 45 0 in 03 62 81 both H and Ks .

19

a

6 7 3 S/N

Figures 1 to 3 show RGB color-composite images of Lupus I, III and IV respectively,


­8­ with IRAC2 band at 4.5 µm in blue, IRAC4 band at 8 µm in green and MIPS1 band at 24 µm in red. The images show the overlapping areas between the mosaics done with both instruments and include the GTO-imaged area in the core of Lupus III at RA 16h 09m and DEC -39o 10 (Allen et al. 2007). The images show a large and dense concentration of cold dust in the North-West of Lupus I and South of Lupus III. The cloud emissions in Lupus are consistent with the Cambr´sy's extinction maps, but now shown in much more detail. A e general 8 µm emission gradient coming from the nearby Galactic plane was compensated in the color scales to bring up the cloud structure. The bright green emission to the North-East of the core in Lupus III is likely pro duced by interstellar PAH molecules, which emit strongly at 8 µm, possibly illuminated by the two bright Herbig Ae/Be stars HR 5999 and HR 6000 in the core.

2.3.

Differential source counts

Given the proximity to the Galactic plane and center (see Table 3), the Lupus clouds are expected to show a relatively high number of background stars compared to the other clouds surveyed by c2d. Figures 4 to 6 show the differential source counts for the Lupus regions. Since Lupus I, at +17, is further from the Galactic plane than Lupus III and IV (at 8­9 ) and likewise the two off-cloud fields with both IRAC and MIPS observations are at +4 and +12 closer to the Galactic plane than the on-cloud fields on average, we expect larger differences between the counts of individual regions compared to the other c2d clouds. Figures 5 and 6 therefore separate the Lupus I cloud from the III and IV clouds. The observed differential source counts are compared to the predictions of the Galactic source counts by Wainscoat et al. (1992). In all plots a steady increase is seen in number of sources per magnitude bin up to a break at about 16­16.5 magnitudes in IRAC bands 1 and 2 and 15­15.5 in bands 3 and 4 corresponding roughly to the sensitivity levels of the surveys. Table 3: Ecliptic and galact their areas. ( , ) deg Lupus I 235.4 ; -34.2 Lupus III 242.7 ; -38.6 Lupus IV 240.4 ; -41.8 OC2 243.2 ; -34.1 OC6 250.0 ; -40.6 ic co ordinates for the centers of the mapped IRAC regions and (l, b) deg 338.6 ; 16.7 340.2 ; 9.4 336.7 ; 8.2 343.7 ; 12.4 342.7 ; 4.0 area deg2 1.391 1.336 0.374 0.051 0.051


­9­

Fig. 1.-- Color-composite image of the mapped area in Lupus I by c2d. The color mapping is blue for IRAC2 at 4.5 µm, green for IRAC4 at 8.0 µm and red for MIPS1 at 24 µm. The bright red emission in the North-West of the cloud is pro duced by cold dust.


­ 10 ­

Fig. 2.-- Color-composite image of the mapped is the same as in Figure 1. The figure shows the the two Herbig Ae/Be stars HR 5999 and HR and a stream of PAH emission to the North of - 3 9 o ).

area in Lupus III by c2d. The color mapping very active star-forming core, which contains 6000 at RA 16h 09m and DEC -39o10 the core (RA 16h 10m ­ 16h 08m and DEC


­ 11 ­

Fig. 3.-- Color-composite image of the mapped area in Lupus IV by c2d. The color mapping is the same as in Figure 1. The figure shows the remnant cloud structure emitting at long wavelengths and many young stellar ob jects covering a large range of evolutionary types. The very red source in the South of the mosaic is the unrelated Planetary Nebula PN G336.3+08.0.


­ 12 ­ Some interesting differences are seen between the shorter wavelength IRAC bands 1 and 2 compared to the longer wavelength bands 3 and 4. In the shorter bands the match between the on- and off-cloud counts is po or with the off-cloud fields showing significantly more sources in given magnitude bins than do the on-cloud fields; consistent with their proximity to the Galactic plane. The on-cloud source counts are clearly higher in the Lupus III and IV regions than the Lupus I region. In each plot the observed on-cloud source counts at IRAC bands 1 and 2 are traced reasonably well by the Wainscoat mo del predictions. These effects all suggest that the source counts in the shorter IRAC bands are dominated by background stars as expected. In the longer IRAC bands the situation is slightly different: both the off-cloud and on-cloud source counts are here seen to exceed the predictions of the Wainscoat mo dels at faint magnitudes. Also the difference between the different on-cloud regions internally or compared to the off-cloud regions are found to be smaller than in IRAC bands 1 and 2. This is likely due to the longer wavelength source counts starting to be dominated by the extra-galactic background, which naturally is independent of the Galactic lo cation. Compared to other c2d clouds, the differential source counts towards the Lupus clouds show a similar behaviour to that seen in Serpens, where the source counts exceed the galactic mo dels in IRAC bands 3 and 4 and match better in IRAC bands 1 and 2 (Harvey et al. 2006). Both clouds are the closest to the direction of the galactic centre, with the Lupus off-cloud fields being the closest of the whole c2d data set (Table 3). The source counts in the Chamaleon II (Cha II hereafter) and Perseus clouds, well away from the Galactic plane, show go o d matches with the Wainscoat mo dels at all bands (Porras et al. 2007 and JÜrgensen et al. 2006, respectively). This illustrates the strong dependence of the source counts on galactic co ordinates and suggests the presence of a larger number of mid-IR sources close to the Galacic center than those predicted by the Wainscoat mo dels. Of course, the excess of midIR source counts towards the Lupus clouds could also be partially attributed to the presence of YSO's in these clouds in cases where the excesses are larger in the on-cloud than in the off-cloud regions. This would also imply a larger number of YSO's in Lupus III and IV than in Lupus I.

3.

Young stellar ob jects and pre-main-sequence stars in Lupus

This section presents and discusses the complete list of Young Stellar Ob jects (YSOs hereafter) and Pre-Main Sequence (PMS) stars in the three Lupus clouds, obtained from the new Spitzer observations. The final list of ob jects is obtained by merging the IR-excess sources from Spitzer (YSOs) with the list of all other known young stars in the clouds from


­ 13 ­

Fig. 4.-- Differential source counts for the on- and off-cloud regions (grey and black, respectively). The predictions from the Wainscoat mo dels are shown with the dashed lines for each of the three parts of the cloud (Lupus IV in dot-dashed line, Lupus III in dotted line and Lupus I with dashed line).


­ 14 ­

Fig. 5.-- As in Fig. 4 but here only for the Lupus I cloud.


­ 15 ­

Fig. 6.-- As in Fig. 4 but here only for the Lupus III and IV clouds.


­ 16 ­ previous optical and near-IR surveys inside the Spitzer covered area (PMS stars). These two c2d standards were intro duced in Harvey et al. (2007b) and Alcal´ et al. (2008). The full a list of YSOs and PMS stars is given in Table 9.

3.1.

Selection of YSOs with IRAC and MIPS data

We call an ob ject a Young Stellar Ob ject candidate (YSOc) if it appears in the catalog of such ob jects delivered in the c2d delivery (Evans et al. 2007). This sample of ob jects was also visually inspected to subtract suspect galaxies and to add obvious YSOs missed by the c2d criteria either because they were to o faint at short wavelengths, but asso ciated with millimeter emission, or because they were saturated in the Spitzer images. The ob jects in the resulting list are called simply YSOs; however some caution should still be exercised. Complete details on the YSO selection metho d can be found in the c2d Delivery Do cumentation (Evans et al. 2007) and in Harvey et al. (2007b), but in short, it consists in the definition of an empirical probability function which depends on the relative position of any given source in several color-color and color-magnitude diagrams where diffuse boundaries have been determined to obtain an optimal separation between young stars and galaxies. For that comparison, the SWIRE catalog (Surace et al. 2004) was "extincted" and resampled to match as accurately as possible the c2d sensitivity limits for each star forming cloud and to provide the statistical color distributions expected for the background galaxies in our fields. The filter also includes a flux cut-off to exclude bright galactic post-AGB stars in the background which resemble Class III ob jects in the cloud. Figure 7 shows the Spitzer color-color and color-magnitude diagrams used to select the YSOs in Table 9. The application of this metho d in the Lupus catalogs yields 18, 69 and 12 YSO candidates in Lupus I, III and IV respectively (shown in Figure 7 as red dots and crosses for point- and extended sources, respectively). Out of these, only 4 (22 %), 26 (38 %) and 2 (16 %) were already known from previous ground-based optical and near-IR observations. This shows that the space observatory, with its highly sensitive detectors, has multiplied by 5, 4, and 6 the number of known YSOs in the three clouds respectively, capturing very low-mass young ob jects which escaped detection due to low sensitivities and also getting the stars with mo derate excess only in the mid-IR which were not identified as excess sources in near-IR surveys. The optical, IRAC and MIPS images of all the ob jects in the sample were examined to confirm the point-source nature and to search for blended features or long-perio d visual binaries. In Lupus I we identified two galaxies, clearly resolved in the optical data, which


­ 17 ­

Fig. 7.-- Color-magnitude and color-color diagrams for the Lupus I (left), III (center) and IV (right) clouds. The black dot-dashed lines show the "fuzzy" color-magnitude cuts that define the YSO candidate criterion (Harvey et al. 2007b) in the various color-magnitude spaces. The red dot-dashed lines show hard limits, fainter than which ob jects are excluded from the YSO category.


­ 18 ­ corresponded to two sources each in the Spitzer bands. Interestingly, all of them were classified as 'YSOc PAH em' in the Spitzer catalog of the region, due to their strong 8 µm emission due to PAHs (see the delivery do cument for a description of these classes). No other resolved galaxies were found in the optical images of all the other YSO candidates in Lupus III and IV. However, a fake source was found in the extended IRAC emission around the embedded ob ject IRAS 15356-3430 (see also § 4.6). These sources were taken off our YSO list and reduced the list of YSOs in Lupus I from 18 to 13.

3.2.

Sample of PMS and PMS candidate stars in Lupus term Pre-Main Sequence (PMS) star for other ob jects added to the already been confirmed using other observational techniques, mostly If an ob ject has not been spectroscopically confirmed as young but optical and near-IR photometry as such it will be labeled as a PMS

We will use the list whose youth had optical spectroscopy. it was selected by its candidate.

We have added to our list the PMS candidates found by Chapman et al. (2007) in the MIPS-only covered area. Because the MIPS coverage was much more extensive than the IRAC coverage, there are sources that have clear excesses over photospheres based on 2MASS and MIPS data, but for which we have no IRAC data (Chapman et al. 2007). They would have been classified as YSOs, but since they cannot be tested against the galaxy filter, we do not include them as YSOs or even YSOc. They are listed as PMS candidates. The embedded class 0 source Lupus3MMS, detected by Tachihara et al. (2007) at 1.2 mm, was added to the YSO sample in Lupus III. This ob ject was detected at all IRAC and MIPS bands, but with to o po or S/N in the shorter wavelengths to be classified as a YSO automatically. Also, we added all previously known members of Lupus cited in Comer´n (2008, in o prep.), which come mostly from the list of H-selected PMS stars in Lupus of Schwartz (1977) after the revisions of Krautter (1991) , Hughes et al. (1994) and Comer´n et al. (2003). This o only added to our YSO list the PMS stars without any detectable IR excess with go o d enough S/N. It must be noted that the multi-color criteria described in the previous section already recovered the 28 Classical T Tauri stars in the cloud listed in Comer´n 2008 (in prep.) with o clear IR excess in the Spitzer wavelength range and go o d detections in all IRAC and MIPS1 bands and did not select the other 13 from that list that did not show detectable IR excesses. Interestingly, the only two bona-fide CTTs with IR excess but not selected as YSOs by our criteria are in high background emission regions and therefore have bad quality detection in one or more Spitzer bands.


­ 19 ­ The candidate PMS stars from the previous optical and near- and mid-IR surveys of Naka jima et al. (2000), L´pez Mart´ et al. (2005), Allers et al. (2006), and Allen et al. o i (2007) were also added to our list of ob jects. These sources are labeled as PMS candidates in the "PMS" column of Table 9 and their respective original references are given in column "Sel". The percentages of candidates from these studies that show IR excess in the Spitzer bands are 6/18 (33 %), 5/15 (33 %), 1/3 (33 %), and 16/16 (100 %), respectively. According to this, the H narrow-band imaging criteria by L´pez Mart´ et al. (2005) have a success o i rate equal to that of the optical and near-IR deep photometric surveys of Naka jima et al. (2000) and Allers et al. (2006). Overall, the small abundance of mid-IR excess sources in these samples is surprising since the all three estimators used to select them are traditional proxies for disk mass accretion towards the central star and should be correlated with the presence of a disk (see § 4 for a discussion on the disks properties). Finally, all the candidates selected by Allen et al. (2007) in the Lupus III core show mid-IR excess since IRAC data from the GTO observations were used to select them but those not classified as YSOs by our criteria fall in the galaxy areas of the color magnitude diagrams and have SEDs difficult to explain with star plus disk mo dels. This comparison with other samples of YSO candidates gives us confidence on the robustness of the c2d color criteria for selecting a reliable set of YSOs in the clouds. In the following sections, we will analyze separately the YSO sample and the total list ob jects. Table 4: Total Number of St Lada Class Lupus I I 2 (15 %) Flat 3 (23 %) II 6 (47 %) III 2 (15 %) Total 13 ars and YSO YSOs Lupus III 2 (3 %) 6 (9 %) 41 (59 %) 20 (29 %) 69 s in the Lupus Clouds Organized by SED Class. Total Lupus IV Lupus I Lupus III Lupus IV 1 (8 %) 2 (12 %) 5 (4 %) 1 (6 %) 1 (8 %) 3 (18 %) 8 (6 %) 1 (6 %) 5 (42 %) 8 (47 %) 56 (45 %) 11 (61 %) 5 (42 %) 4 (23 %) 55 (44 %) 5 (28 %) 12 17 124 18

Note. -- The percentages for each class in the table are calculated with respect to the total numbers at the bottom of each column. The `Total' population consists of the YSOs plus the PMS stars and candidates (§ 3).


­ 20 ­ 3.3. Class distribution of the sample

The complete sample contains 17, 124 and 18 ob jects in Lupus I, III and IV, respectively. Table 4 shows the number of ob jects per cloud and their respective SED classes, as defined by Lada & Wilking (1984) and extended by Greene et al. (1994) (i.e. Class I for ob jects with (K -24µm) > 0.3, Class Flat for 0.3 > (K -24µm) -0.3, Class II for -0.3 > (K -24µm) -1.6, and finally Class III for (K -24µm) < -1.6). The table also shows the total number of YSOs, as defined above, for each cloud to facilitate comparison to other c2d clouds where the PMS sample will be obviously different. The number of sources shows that Lupus in general presents a mo derate star formation activity compared with the other clouds surveyed by the Spitzer c2d program, only larger than that measured in Cha II (Alcal´ et al. 2008). It also a shows that amongst them, the most active regions are Lupus III, followed by Lupus I and IV, which present a lower amount of YSOs. Figure 8 shows the distribution of (K -24µm) values in the three clouds. It illustrates that Lupus III shows a larger variety of ob jects, from Class I to Class III, while Lupus I has a much smaller number of YSOs relatively rich in Class I and Flat spectrum ob jects, and Lupus IV shows a clear lack of early class ob jects. The figure also shows that the addition of spectroscopic or photometric member candidates to the YSO samples mostly adds Class III ob jects in Lupus III, whose asso ciation with the cloud cannot be confirmed until optical spectroscopy reveals youth signatures. This is a selection effect, since Lupus III is the most studied region of the three and illustrates that the difference in percentages between the YSO and the total sample is only driven by different available data and not based on physical characteristics of the stars. For this reason, we will concentrate in the YSO sample on the following discussion, which has been selected as genuine IR-excess ob jects and therefore likely belong to the star-forming clouds. The analysis below is only valid as a rough indicator of the relative abundances of ob jects within Lupus. A more solid statistical analysis which combines all the YSO samples in all c2d clouds will be presented elsewhere (N. Evans et al., in preparation). One interesting difference is that the percentage of Class I and Flat sources compared to the number of Class II and III sources is particularly high in Lupus I, compared to Lupus III and IV. Assuming that the classes correspond to a succession of evolutionary phases from the cores to the disks, this suggests that Lupus I, the least active cloud of the three in terms of YSO abundance, is in a less evolved phase of evolution, while Lupus III and Lupus IV are respectively more evolved than Lupus I. It is also possible to study the later phases of disk evolution: the percentage of Class III vs Class II plus III (i.e. N(III)/(N(II) + N(III))) YSOs in the clouds (50±25% in Lupus IV, 32±16% in Lupus III and 25±12% in Lupus I) suggests that star formation started


­ 21 ­

Fig. 8.-- Distribution of ob jects in (K -24µm) for Lupus I, III and IV. Thin lines show the YSO population and dotted lines the total sample of stars. The intervals defining the Lada classes are marked with vertical dashed lines. The comparison illustrates that Lupus I is a region with a small number of YSOs, many of them being early classes, Lupus III contains all kinds of ob jects, with a great number of Class III sources while Lupus IV contains almost no early class sources and relatively more late classes.


­ 22 ­ longer ago in Lupus IV than in any of the other clouds. The errors are dominated by the actual number of Class III ob jects, or alternatively, the completeness of the sample for this kind of ob jects. Given our selection criteria based on presence of IR excess, the sample will be biased against the Class III ob jects with little excesses. However, we can estimate the Class III completeness level to be of the order of 50% from the number of spectroscopically confirmed young stars from the `Sz' catalog which were observed to have detectable IR excess in the Spitzer bands (namely, 13 out of 28). This uncertainty dominates the total error budget of these ratios and let us only conclude significatively that Lupus IV has a larger percentage of Class III ob jects than any of the other two clouds. Actually, this is the largest number of Class III vs Class II+III sources in any of the c2d studied star-forming clouds (e.g. Harvey et al. 2007b; Alcal´ et al. 2008). Comparing Lupus III and IV, which a have a similar density of YSOs, these numbers also suggest that the ma jor star-formation activity already to ok place (and is about to start again, see § 5.1) in Lupus IV, while it is currently taking place in Lupus III, mostly in its very dense star-forming core. We can confirm our Class III completeness ratio of 50% given above with the list of XMM detections in the Lupus III core by Gondoin (2006), which is deeper than the ROSAT All Sky Survey by Krautter et al. (1997). That survey covers a circular area of 30 in diameter around the Lupus III core and found 102 X-ray source detections, out of which 25 are asso ciated with optical and IR counterparts. A cross-match of our total list of ob jects and the list of X-ray detections with a match range of 4 arcsec yielded 24 matches, 13 of which have SEDs indicating the presence of a disk and the remaining 11 showing no IR excess. All stars with asso ciated X-ray emission were labeled in Table 9 with a reference to Gondoin (2006). Assuming that the presence of X-ray emission is a signature of youth, this yields an X-ray disk fraction in the core in Lupus III of 54% which is of the order of the Class III completeness we derived from the independent measurement with the H-selected `Sz' catalog above. The full list of PMS stars is given in Table 9: columns 2 to 5 give their c2d and previous names of the ob jects and their co ordinates in the Spitzer catalog, column 6 gives the selection source as described above, a flag determining the status of membership spectroscopic confirmation (PMS status) of the ob ject is given in column 7, the Spitzer-derived class based on the SED slope (K -24µm) is given in column 8 and the references to the ob jects are given in column 9.


­ 23 ­ 4. Individual sources properties

The properties of the circumstellar material surrounding the young stars in Lupus can be studied with the optical to mid-infrared emission in several different ways. We are specifically interested in estimating the overall disk fraction, the amount of circumstellar dust, and the morphology of the circumstellar disks (flared versus flat) which is likely to represent some stage in the formation of planetary systems. The special interest that the new Spitzer data bring to the analysis comes from the fact that the IRAC and MIPS data, due to their wavelength coverage, probe the region in the disks around low-mass stars between 0.1 and 5 AU, where planet formation may take place. Therefore, large samples of Spitzer SEDs of star-forming regions with ages in the critical time-frame between 1 and 10 Myr can be used to study statistically the initial conditions for planet formation.

4.1.

Color-Color and Color-Magnitude diagrams

Infrared color-color (CC) and color-magnitude (CM) diagrams are go o d diagnostic to ols for the investigation of circumstellar matter around YSOs in a statistical way (Hartmann et al. 2005; Lada et al. 2006, and references therein). In recent years, several authors have produced grids of YSO mo dels and computed their colors in the Spitzer bands to allow direct comparison with the observations (Whitney et al. 2003; Allen et al. 2004; Robitaille et al. 2006). Both previous data sets and the mo dels roughly agree in the spatial distributions of the ob jects of different Lada classes in the different CC and CM diagrams although the interplay between the presence or absence of envelopes and disks together with the whole possible range of system inclinations and total interstellar extinctions makes the problem highly degenerate. Therefore it is impossible to asso ciate a position in those diagrams with a physical configuration for individual ob jects. Robitaille et al. (2006) computed a very large grid of YSOs with a broad range of physical parameters, and inclination angles that can be used to make statistical analyses. In discussing the evolutionary stages of our mo dels, they adopt a "Stage" classification analogous to the Class scheme, but referring to the actual evolutionary stage of the ob ject, based on its physical properties (e.g., disk mass or envelope accretion rate) rather than properties of its SED (e.g., slope). Stage 0 and I ob jects have significant infalling envelopes and possibly disks, Stage II ob jects have optically thick disks (and possible remains of a tenuous infalling envelope), and Stage III ob jects have optically thin disks. Figures 9 and 10 compare three CC and CM diagrams of the Lupus YSO sample with the synthetic colors of a mo del cluster from Robitaille et al. (2006). To make these comparisons, we have scaled the mo dels to 150 pc in the first case to compare them with the YSOs in Lupus I and IV and to 200 pc to compare them with those in Lupus III.


­ 24 ­

Fig. 9.-- The Color-color and color-magnitude diagrams for the spectroscopically confirmed PMS ob jects (gray filled diamonds) and candidates (open diamonds) with Spitzer and 2MASS data reported in Table 9 in the Lupus I and IV clouds are plotted in the left panels of each diagram. The colors derived from the SED mo dels by Robitaille et al. (2006) are plotted (in gray-scale intensity representing the density of points) in the right panels of each diagram. The areas corresponding to the Stages I, II, and III as defined by Robitaille et al. (2006) are also indicated in each diagram. The label 'ALL' mark the regions where mo dels of all evolutionary stages can be present. The green circle represents normal reddening free photospheres. The PMS stars in Lupus I and IV fall in regions corresponding to Stage I to III sources. The comparison between the position of the Lupus YSOs and those of the mo del grids in the [3.6]-[4.5] vs [5.8]-[8.0] CC diagram shows several early Class I and Flat source SEDs in Lupus I and IV (Figure 9), redder in [3.6]-[4.5] than the Stage II ob jects from Robitaille et al. and a large ma jority of Class II sources in Lupus III (Figure 10). The position of the maximum density of such kind of ob jects is also consistent with that predicted by Allen et al. (2004) with a grid of physical disk mo dels of D'Alessio et al. (2005). The [8.0] vs [3.6]-[8.0]


­ 25 ­

Fig. 10.-- Same as figure 9 but with the YSOs in Lupus III. CM diagram of Lupus III (Figure 10) shows a bimo dal distribution with a large number of ob jects with photospheric [3.6]-[8.0] colors and a range of 8.0 µm magnitudes and another one with a similar range of luminosities and a range of color excesses in the IRAC bands compatible with the presence of mo derate to large mid-IR excess. No special difference is found between the distributions of spectroscopically confirmed PMS ob jects (grey diamonds) and candidate YSOs in any of the diagrams, which suggests that both populations contain indeed the same kind of ob jects.

4.2.

Spectral Energy Distributions

We have constructed SEDs for each source, similar to what has been done for other starforming regions (e.g., Hartmann et al. 2005; Lada et al. 2006; Sicilia-Aguilar et al. 2006). These allow the full set of multiwavelegth data to be displayed for each source. Figure 11 shows the SEDs of all Class I and `Flat' sources in the sample. For all ob jects, the c2d


­ 26 ­ catalog provides the 2MASS near-IR magnitudes and the IRAC1-4 and MIPS1-3 fluxes. We have added all the complementary data described in § 2.1 plus IRAS fluxes from the PSC and 1.3 mm fluxes from Nuernberger et al. (1997). The open dots are the observed fluxes and the Spitzer data have been highlighted in grey to compare with previous observations. Figure 12 shows all the SEDs for the Class II and III ob jects in the Lupus sample for which there was sufficient data to make a go o d fit to a stellar SED and characterize the stars and disks separately. Two different pro cedures were applied for the SED fits: for the ob jects with known spectral types, marked as `PMS' in Table 9, we obtained the best-fit visual extinction AV by fitting all photometry between V and J to the stellar NEXTGEN mo dels (Hauschildt et al. 1999). This metho d provides very go o d agreement with the traditional use of the RC - IC color, as compared with the results by Alcal´ et al. (2008). The 2 a minimization is extended to try all spectral types between A0 and M9 and all visual extinctions AV between 0 and 30 magnitudes for the new YSOs for which there is no spectral type available in the literature. This technique is similar to that used by Spezzi et al. (2007b, in preparation) with the c2d Cha II sample, and provides agreement within ± 200 K in the effective temperature when applied to ob jects with known spectral types and mo derate extinctions. Once the spectral type and extinction are computed for the sample, the observed fluxes are dereddened with the extinction law by Weingartner & Draine (2001) with RV = 5.5 and fitted to the appropriate NEXTGEN stellar atmosphere models. The sample of SEDs of stars from the Schwartz catalog (Sz) was also compared with the SED fits made by Hughes et al. (1994) and there is in general go o d agreement in the resulting dereddened stellar and disk energy distributions. The resulting spectral types and extinctions, together with their corresponding references are given in Table 11. The SEDs show considerable variety. A useful classification system has to rely on disk mo dels which are again degenerate in several parameters as e.g. the inclination angle of the disk or the degree of dust pro cessing of the disk. Therefore, we will not attempt a full characterization of the SED types in this section but rather define four types of ob jects and give their frequencies in the sample. To help with the classification, we have plotted with a dashed line the median SED of the Classical T Tauri stars (CTTs) from Taurus (D'Alessio et al. 1999) normalized to the optical dereddened fluxes of all the low-mass stars. Based on this comparison benchmark, we can identify the systems whose colors from optical to the millimeter follow closely the decaying slope of a classical accreting optically thick disk around a low-mass star (e.g. Sz100 or SSTc2d J160901.4-392512). We will call these systems `T'-type, for T Tauri. We then call `L'-type (from `low' IR excess) all those ob jects where the IR excess is clearly smaller than the median SED of a CTTs (e.g. ACK2006-19). These are what Lada et al. (2006) call the `anemic' disks. We call `H'-type ob jects, those systems with higher IR fluxes than those of the median CTTs SED (e.g. 2MASS J16081497-


­ 27 ­ 3857145). Finally, we will call `E'-type from empty the spectrally confirmed young stars in the clouds where no IR excess at all is detected in the Spitzer bands (e.g. Sz 67). These are systems with a very little amount of cold dust or "debris"-like disks (see also some in Sicilia-Aguilar et al. 2006 and Lada et al. 2006). These classifications are given in Table 11 for each system. Considering the whole sample of YSOs and PMS stars and candidates in Lupus, 22±10% of them are `T'-Type, 39±18% are `L'-type, 6±2% are `H'-type, and 19±8% are `E'-type. The remaining 20% are the Class I and Flat SED sources. The large errors in this percentages come from the difficulty in classifying the borderline cases if we take into account the implicit uncertainties in the fitting pro cess of the dereddened photometry to the stellar photospheres and from the completeness estimation for disk-less members presented in § 3.2. We can consider a negligible amount of `H'-type ob jects, likely due to source variability at different wavelegths and problems with the stellar normalization. From the remaining sample, approximately 40% show `L'-type SEDs, 20% show `T'-type SEDs and another 20% show `E'-type SEDs. The large pertentage of `L'-type ob jects in Lupus is consistent with that found in Serpens (Harvey et al. 2007b) and suggests more evolved inner disks in these ob jects compared to the initial inner disk confguration in the T Tauri stars. This percentages contrasts interestingly with the 30% of `T'-type and 20% of `L'-type SEDs found in the older 3 Myr star-forming cluster IC 348 by Lada et al. (2006). These different disk populations in different clouds could be related to different environmental conditions (e.g. clustered vs extended star-formation), to a different stellar population (abundance of low-mass vs high-mass stars) or alternatively to a faster evolutionary time-scales for the less flared `L'-type disks. More samples of disks will be needed to pursue this research, which is outside the scope of this paper. One fifth of the sample are `E'-type stars and this gives an overall disk fraction for the Lupus clouds of 68% to 81%, depending on whether the assume a 50% completeness ratio for diskless stars of or not. This range of values matches well with other disk fractions calculated for 1 to 2 Myr-old star forming regions with near and mid-IR data (Haisch et al. 2001; Sicilia-Aguilar et al. 2006), including Cha II (Alcal´ et al. 2008). The `E'-type ob jects a in Lupus show photospheric IRAC and MIPS fluxes which indicate that the stars do not have any circumstellar dust out to a distance of at least 50 AU, depending on the stellar luminosity (see e.g. HR 6000, Sz 119 or Sz 124). Once spectroscopically confirmed as young members of the clouds and therefore with ages < 3 Myrs, they will provide very valuable constraints to the disk dissipation time-scales and mechanisms and will be the sub ject of a separate study. Also interestingly, the Spitzer data of a subsample of the `L'-type ob jects show a very peculiar SED, with almost photospheric IRAC and MIPS1 fluxes typical of Class III sources,


­ 28 ­ and a MIPS2 excess flux at 70 µm comparable to those of the CTTs. This subgroup has been labeled `LU' in Table 11 and contains the ob jects SSTc2d J154240.3-341343, Sz 91, and Sz 111. It represents a 2±1% of the young population in Lupus. Similar ob jects have been found in Serpens (Harvey et al. 2007b) and Cha II (Alcala et al. 2008) and seem to be ´ extremely rare. These ob jects, called cold disks (Calvet et al. 2005; Brown et al. 2007), are interpreted as optically thick disks with large inner holes of several to tens of AUs, where potentially planets could be currently forming. However, both the ob jects in Lupus and the star ISO-ChaII 29 in Cha II (Alcal´ et al. 2008) are different from previously known a systems of this kind in that the long wavelength at which they show the sizable excess (70 µm) implies larger inner holes of up to 70 AU, while previously known ob jects show excess already at 24 µm, implying inner holes smaller than 50 AU.


­ 29 ­

Fig. 11.-- Spectral energy distributions of the Class I and Flat SED PMS ob jects and YSOs ordered by RA and labeled with their name and ID as in Table 9. Only the observed fluxes are plotted with open dots and upper limits with arrows. The new Spitzer data are shown in grey to distinguish them from previous data.


­ 30 ­

Fig. 11 - Continued


­ 31 ­

Fig. 12.-- Spectral energy distributions of the Class II and Class III PMS ob jects and candidates ordered by RA and labeled with their names and ID as in Table 9. The observed, dereddened fluxes and upper limits are represented with open and solid dots and arrows, respectively. The plotted error bars are usually smaller than the symbols. NEXTGEN stellar mo dels for the spectral type of each star are shown in dotted lines. For all low-mass ob jects, the median SED of the T Tauri stars in Taurus from D'Alessio et al. (1999) is shown normalized to the stellar photosphere in dashed line for comparison.


­ 32 ­

Fig. 12 - Continued.


­ 33 ­

Fig. 12 - Continued.


­ 34 ­

Fig. 12 - Continued.


­ 35 ­

Fig. 12 - Continued.


­ 36 ­

Fig. 12 - Continued.


­ 37 ­

Fig. 12 - Continued.


­ 38 ­

Fig. 12 - Continued.


­ 39 ­

Fig. 12 - Continued.


­ 40 ­ 4.3. The luminosity function in Lupus

A basic step in the characterization of the PMS population is the determination of its degree of completeness in the effective temperature and luminosity scales, which might be correlated in those ob jects that formed more or less simultaneously. Both parameters can be accurately determined from the spectral type and the SEDs shown in the previous section for Class II and III ob jects. In order to calculate the best possible stellar luminosities for the sample, we integrate the NEXTGEN stellar mo del normalized to the dereddened optical fluxes (dotted curves in Figure 12), and assume distances of 150 pc for Lupus I and IV and 200 pc for Lupus III. The computed stellar luminosities can be found in Table 11. The complete emission of the ob jects is obtained in the bolometric luminosity, where we integrate under all the observed fluxes of the SED, the corresponding bolometric flux is then converted to luminosities with the same distances quoted above for the different clouds.

Fig. 13.-- Bolometric luminosity function for the Lupus young stellar population (solid histogram) and estimated correction for completeness effects (dashed histogram). Figure 13 shows a histogram of the total bolometric luminosities for all YSOs and PMS stars in Lupus as a solid line. Compared to the same figure in Cha II (Alcal´ et al. 2008) and a


­ 41 ­ in Serpens (Harvey et al. 2007a), it shows a larger population of low and very-low luminosity ob jects, which was already noted by previous surveys of the region (see F. Comer´n 2008, in o prep. and references therein), and a large number of ob jects with luminosities between 0.3 and 0.1 L . Interestingly, the lowest luminosity members of the population are Lupus3MMS, the Class 0 ob ject in Lupus III (Tachihara et al. 2007), SSTc2d J161027.4-390230, another flat SED ob ject in the same cloud followed by late M-type brown dwarfs from Comer´n et al. o (2003), Allers et al. (2006) and Allen et al. (2007). The peak of the luminosity function appears at 0.2 L , which corresponds to a 0.2 M star (spectral type M5 at an age of 1 Myr) and up to 1.0 M for ob jects of 5 Myrs according to the PMS tracks by Baraffe et al. (1998) plus a tail at lower luminosites. Harvey et al. (2007a) made an estimate of the completeness of the c2d catalogs by comparing a trimmed version of the deeper SWIRE catalog of extragalactic sources (Surace et al. 2004), taken to represent 100% completeness by c2d standards, with the number counts of the c2d catalog in Serpens per luminosity bin. Their estimations suggest a 100 % completeness at luminosities 0.3 L in the c2d catalogs, which corresponds to a 0.3 M star (spectral type M4.5 at an age of 1 Myr). The dashed line in Figure 13 is the luminosity histogram corrected for completeness effects in each luminosity bin, which suggests that up to 15 additional very low-luminosity ob jects (log L/L < -1.7) were missed below the noise level of our c2d observations or were confused in the galactic region of the color-magnitude diagrams. The comparison of both luminosity histograms yields a completeness level in luminosity for our disk study of log L/L -1.0, which corresponds to a mass of M 0.1M for a star of 1 Myr (Baraffe et al. 1998). The lower luminosity limit with respect to that in Serpens stems from the different distances to both clouds and is roughly consistent with the distance squared ratio.

4.4.

Disk fractional luminosities

One way to characterize the circumstellar accretion disks around young stars is to compute the disk fractional luminosities Ldisk /Lstar and compare them with that of passive reprocessing flaring disks (Kenyon & Hartmann 1987). We computed those ratios by subtracting the stellar fluxes from the observed dereddened fluxes in the SEDs and integrating the IR excess throughout the SED. That was done for all the ob jects with sufficient data to allow a go o d fit of the stellar mo del to the SED, crucial to get a sensible disk luminosity. The resulting flux ratios are also given in Table 11. The upper panel of Figure 14 shows the stellar luminosity versus the disk fractional luminosity for the sample of YSOs and PMS ob jects in Lupus. The grey dots correspond


­ 42 ­ to visual binary systems, as reported in § 2.1, while the black dots represent single stars. In the lower planel, we have collapsed the stellar luminosity axis to get a histogram on disk fractional luminosities for the entire sample. This diagram offers a complete view of the star plus disk population in Lupus and shows several interesting results and trends. The log Ldisk /Lstar ratio of ob jects in which we could not detect any sizable IR excess were set to -3 so that they appear to the left of both panels. The disk luminosity ratios show a strong dependence on the band used to normalize the dereddened fluxes to the stellar photospheric mo del and the extinction determination. These are only accurate in those ob jects with known spectral types, but the deviations are small enough to extract statistical trends from the diagram. Horizontal dashed lines in the upper panel separate the regions where the luminosities correspond to those of Herbig Ae stars (HAeBe's, spectral types earlier than F0), T Tauri stars (down to M7) and Brown dwarfs (BDs, below M7) of 1 Myr according to Baraffe et al. (1998). The only two known HAeBe's in Lupus, HR 5999 and HR 6000, share the upper region with SSTc2d J161000.1-385401, a intermediate-mass HAeBe candidate in Lupus with small IR excess, which could be a background post-AGB star, given the resemblance of its SED to those of the old field ob jects found in Serpens (Harvey et al. 2007a). It can be also seen here, as well as in figure 13, that the great ma jority of the ob jects in Lupus are M-type T Tauri and very low mass stars. The vertical lines separate the regimes where the luminosity ratios can be explained by different mechanisms: accretion disks (Ldisk /Lstar > 0.1), and passive repro cessing disks (0.02 < Ldisk /Lstar < 0.08 Kenyon & Hartmann 1987), and finally "debris"-like disks (Ldisk /Lstar < 0.02, which is a conservative upper limit for the fractional disk luminosity of a transitional or young debris disk, Currie et al. 2007). The distribution of points and the histogram in the bottom panel show that the great ma jority of the disks found in Lupus have luminosities which imply some degree of accretion, similar to what was found in the Cha II cloud (Alcal´ et al. 2008). This result contrasts with the 40% of disks with small IR excesses found a in § 4.2 and shows that detailed Spitzer SED morphology studies are needed to provide a better description of the inner disks, which are greatly degenerate with the flux ratios in the T Tauri phase. The grey dots and dashed histogram show the distribution of those YSOs in the plot which were found to be visual binaries in the optical images by Comer´n et al (in prep.). It o has been suggested that close binaries (< 20 AU) play a central role in the evolution of the disks by dramatically reducing the incidence of disks around multiple stars (Bouwman et al. 2006), while wide (> 100 AU) binaries do not affect significatively the presence and evolution of the circumstellar disks (Pascucci et al. 2007). Here we present further evidence for this


­ 43 ­

Fig. 14.-- Top: Correlation plot between the stellar luminosities and the disk fractional luminosities for the PMS stars in Lupus. Solid and grey dots are single and binary stars, respectively and the dot-dashed line marks the approximate 24 µm detection limit. Bottom: distribution of disk fractional luminosities for the Lupus sample. The solid and dashed lines show the single and binary stars distributions, respectively. Ob jects with negligible IR excess are shown in the -3 abscisa for completeness. lack of correlation between disks and wide orbit companions in Lupus, where binaries and


­ 44 ­ single stars show the same distribution in terms of luminosity or disk fractional luminosity. Finally, there seems to be a trend by which lower luminosity ob jects show higher disk to star luminosity ratios than higher luminosity stars. However, the luminosity distribution of the `H' and `T'-type ob jects only, the least affected by the detection limits in the IR, is statistically equal to the luminosity distribution for the total sample. Therefore, the trend reflects an observational bias caused by the limited detection capability of excesses at longer wavelengths for the faintest sources. The flux sensitivity limit for 24 µm detection with S/N > 3 is 1 mJy in our observations. This corresponds to photospheric emission of a 0.2 L (log Lstar -0.7) star in our sample, which corresponds to a 0.2 M (M5.5) star of 1 Myr. The star Sz 92 is close to the border with 0.47 L (log Lstar -0.3), a very small excess at 24 µm (Ldisk /Lstar = 0.06, log Ldisk /Lstar = -1.2) and a flux density at 24 µm of 1.5 mJy. Fainter ob jects with larger excesses will be detected as so on as their 24 µm is larger than the limiting flux and this number will obviously depend on the level of background emission and crowdedness of the area where a given ob ject is. This limit, shown with a dot-dashed line in the figure, explains the skewness of the data points towards the bottom right of the diagram and illustrates the disk parameter space probed with these observations. The survey is not sensitive to "debris"-like disks around stars less massive than 0.2 M but detects all actively accreting disks down to the substellar regime since those should present detectable IR excess at all IRAC bands which are much more sensitive.

4.5.

A Two-Dimensional Classification System

Finally, to explain the diversity in the SEDs, we developed a second-order set of parameters to classify the diversity of 2MASS + IRAC + MIPS SEDs that are found in the star-forming regions: turn-off and excess (Cieza et al. 2007). In short, excess is the last wavelength in microns where the observed flux is photospheric and excess is the slope computed as dlog(F )/dlog() starting from turn-off and up to 70 µm when available. The first parameter gives us an indication of how close the circumstellar matter is to the central ob ject and the second one is a measure of how optically thick and flared it is. Both numbers can be found for all the stars with disks in the sample in Table 11. Figure 15 shows both values for the sample of YSOs in Lupus for which we could perform a sensible SED fit. Three ob jects (namely Par-Lup3-3, Par-Lup3-4 and Sz 99) were not included in this analysis since their SEDs did not allow for a go o d determination of turn-off due to to o much IR excess at short wavelengths in the first two cases and lack of IRAC data in the third one. Cieza et al. (2007) showed that turn-off is a go o d "evolutionary" parameter, since it separates efficiently the Classical T Tauri stars from the Weak Line T Tauri stars.


­ 45 ­

Fig. 15.-- Distribution of excess slopes excess with respect to the wavelength at which the infrared excess begins turn-off for the Lupus sample (open circles). Solid dots are ob jects which were detected at 1.3 mm by Nuernberger et al. (1997) and grey dots are ob jects for which only upper limits were obtained at 1.3 mm. CoKu Tau/4 shows the position of the cold disks in this diagram for comparison. They also showed that the range of excess values, which scale with the amount of emitting material in the disk for central ob jects of similar luminosity, grows with turn-off , which was interpreted by those authors as a signature of multiple "evolutionary paths" of the inner disks of T Tauri stars from the actively accreting phase (with typically turn-off < 2µm) to progressively more settled and optically thin disks with larger values of turn-off . The Lupus sample shows a remarkably similar distribution in Figure 15, as also do the Serpens and Cha II samples, suggesting that the result is a common feature of young stellar populations. The diagram is also useful for identifying transitional disks, or cold disks (Calvet 2005; Brown et al. 2007), i.e. systems with an optically thick outer disk with large inner (several AU). These ob jects appear in the right-upper part of this diagram. For compa we show the position of CoKu Tau/4, a well known T Tauri disk with a inner hole 10 AU devoid of matter (D'Alessio et al. 2005). We also labeled one of the new cold et al. holes rison, of disks


­ 46 ­ found in Lupus III, Sz 91, which is indeed is the most extreme upper-right ob ject of the whole distribution. The determination of robust cut-offs in this diagram for identifying "bona-fide" disks with holes and their frequency in the full c2d data set is underway and will be presented elsewhere. In order to compare the inner disk architectures of our sample of Lupus PMS stars with their outer disks, we have marked the `Sz' stars detected in 1.3 mm continuum observations by Nuernberger et al. (1997) with black dots, and the upper limits with grey dots in Figure 16. As expected, all the millimeter detections and upper limits in the diagram appear at excess -1.5, which imply relatively optically thick inner disks for all values of turn-off .

Fig. 16.-- Relationship between the continuum flux at 1.3 mm from Nuernberger et al. (1997) and the wavelength turn-off at which the infrared excess begins for the Classical T Tauri stars in Lupus. The arrow show the positions of the upper limits, including that for the cold disk Sz 91. However, the really interesting result comes when comparing the millimeter fluxes, which are a proxy for disk total mass (Beckwith & Sargent 1991; Andrews & Williams 2005), with turn-off , which is an indirect indicator of the degree of dust depletion and clearing of the


­ 47 ­ inner disk. Figure 16 shows the 1.3 mm continuum fluxes and upper limits for the Lupus sample normalized to 200 pc compared to the turn-off . The horizontal line shows the average of the normalized millimeter fluxes and the dotted lines the 1 error bar of the mean. With the exception of Sz 98, disks with a range of turn-off or inner disk clearings appear to show quite similar total disk masses, being all well inside the standard deviation of the mean. The case of Sz 98 could be different, since its SED suggests a possible contribution of a remnant envelope, which would contribute to the total millimeter flux. In spite of the low number of detections, the general result is that ob jects with a range of inner disk configurations show total disk masses in the same order of magnitude. This suggests an inside-out pro cess which empties the inner disk while the outer disk remain unchanged. Alexander & Armitage (2007) show that disk clearing by photo evaporation is more efficient for smaller disk masses while e.g. Edgar (2007) argue that the efficiency of giant planet formation and migration, the main competing mechanism for inner disk dissipation, is proportional to the disk mass. The apparent lack of correlation between inner disk clearing and total disk mass is not compatible with the photo evaporation scenario while it is with the planet formation one. However, the current sample only contains 8 go o d detections, and several caveats should be taken into account in the interpretation of this figure: apart from the low number statistics, the turn-off value will be sensitive to the inclination angle, while the millimeter flux is considered roughly insensitive to it (e.g. D'Alessio et al. 1999). More work will be done to quantify the extent of this relation with larger data sets and will be presented elsewhere.


­ 48 ­ 4.6. Outflow sources

Several previous studies have shown the suitability of the IRAC bands, and more specifically IRAC band 2 at 4.5 µm for detecting new high-velo city sho cked outflows via the H2 emission line found in that band (e.g. Noriega-Crespo et al. 2004, JÜrgensen et al. 2006). In this section we present the Spitzer data for the known outflow sources in the surveyed Lupus clouds (from the review by Comer´n 2008, in prep.) and new emission nebulae found in the o IRAC mosaics which could be high velo city outflows and sho cks. Table 5 summarizes the results of this effort and Figures 17 and 18 show them.

Fig. 17.-- Known HH ob jects detected in Lupus with IRAC, together with a candidate new outflow source in Lupus III and a nebulous ob ject in a ring of stars in Lupus IV. All images have a size of 2 x2 , linear stretch and are from the IRAC1 band at 3.6 µm, except the one showing HH 185, which is IRAC4 at 8.0 µm. North is up and East is to the left. Co ordinates are given in Table 5. The HH 185 ob ject, reported by Heyer & Graham (1989), shows an ellipsoidal shape close to the Flat SED ob ject IRAS 15398-3359 in all IRAC bands. HH 187 (Heyer & Graham 1989) is a faint nebulosity seen at IRAC1 and 2 bands only, and brighter in the latter. HH 228 and HH 78 also appear in the Spitzer bands as small ( 4 ) faint nebulosities around their driving sources. The small [SII] outflow in Par-Lup3-4 reported by Fern´ndez & Comer´n a o


­ 49 ­ (2005) and the HH 186 36 [SII] jet vations. Only nebulosities appearing avoid artifacts. All the IRAC images detection a jet-like nebulous structure ob ject in a ring of point sources found were not identified. around Sz 68 are not detected by the Spitzer obserconsistently in both epo ch images were included to were searched for nebulosities and we report here the found at all IRAC bands in Lupus III and a nebulous in Lupus IV. The driving sources of these two ob jects

Fig. 18.-- IRAC and MIPS images of the extended nebula around the source IRAS 153563430. All images have a size of 4 x5 and linear stretch. North is up and East is to the left. Co ordinates are given in Table 5. Figure 18 shows the remarkable emission around the the bright class I source IRAS 15356-3430. A 40 elliptical nebulosity is observed in all IRAC bands and also detected in MIPS 24 and 70 µm bands. The nebulosity is also found with a slightly smaller extension in the optical and 2MASS images. Carballo et al. (1992) classified it as a possible YSO or a galaxy based on its IRAS colors and Strauss et al. (1992) confirmed its YSO nature with optical spectroscopy. Its 70 µm flux is as high as that of Lupus3MMS but it has never been observed in the millimeter wavelengths. The SED slope of the ob ject is smaller than that


­ 50 ­ of Lupus3MMS or IRAS 15398-3359 and that makes it detectable in the near-IR bands. In any case, the Spitzer SEDs of all these sources with extended emission are clearly asso ciated with extremelly embedded and actively accreting ob jects. Interestingly, one class II and one class I YSO (Sz 98, Lupus3MMS) happen to have detection quality flag of `K' only in IRAC2 band at 4.5 µm in the c2d catalog, which means that these sources could not be fitted by a stellar PSF at that wavelength. This suggests the possible presence of unresolved (< 2 ) outflows detected preferentially through the sho cked H2 line in IRAC band 2 and is consistent with the fact that all three of them are extremely active accretors with large (K -24µm) values and excesses well above the median SED of the T Tauri stars in Taurus. Similarly, in the case of the highly accreting HAeBe star HR 5999, a point source could not be extracted for IRAC bands 1 and 2 so the corresponding fluxes were removed for the SED analysis of that ob ject. This again hints to bright extended emission around 4.5 µm on a scale smaller than the large PSF of the star.


­ 51 ­

Table 5: Probable high-velo city outflows and nebulae in Lupus Asso c. R.A. Dec. YSO ID (J2000) (J2000) HH identification / driving source Lupus I 2 15 38 48.36 -34 40 38.2 IRAS 15356-3430 10 15 43 01.29 -34 09 15.42 HH 185 / IRAS 15398-3359 15, 16 15 45 19.03 -34 17 32.43 HH 187 / Sz 68 / Sz 69 Lupus I I I 47 16 08 32.11 -39 03 18.23 HH 228E / Sz 102 47 16 08 27.18 -39 03 00.68 HH 228W / Sz 102 87 16 09 12.38 -39 05 00.61 HH 78 / Lupus3 MMS ... 16 10 57.95 -38 04 37.90 ... Lupus IV ... 16 00 39.04 -42 06 51.51 ...

Ref. Notes 4 1 1 2 2 3 4 4 a b c d d e f h

a Bright 40 b Bright 12




nebula towards the NE in all IRAC and MIPS bands. nebula towards the NE in all IRAC bands.

c Faint 3 nebula knot at 3.6 and 4.5 µm. d Faint knots at 3.6 and 4.5 µm. e Faint knots mostly at 3.6 and 4.5 µm. f 8 jet in all IRAC bands. h 9 knots at all IRAC bands in a ring of 15 point sources. References. -- 1) Heyer & Graham (1989); 2) Krautter (1986) ; 3) Reipurth & Graham (1988); 4) This work

5.

Clouds and Cluster properties

We can use the Spitzer data to also study the star formation history in the Lupus clouds. In particular, we want to estimate the star-formation activity and the clustering properties of the young stellar population in relation to the current cloud structure.

5.1.

Extinction maps in Lupus

The structure of the interstellar medium in the direction of the Lupus clouds has been extensively studied with (sub)millimeter molecular line observations (e.g., Murphy et al.


­ 52 ­ 1986; Hara et al. 1999; Vilas-Boas et al. 2000; Tachihara et al. 2001) as well as with optical and infrared star-counts (Cambr´sy et al. 1997, 1999) on spatial scales of several arcminutes. e These studies reveal a large clumpy structure with a substantial number of overdensities, dominated by the "classical" Lupus I to IV clouds, where star-formation has also been detected. See Comer´n 2008 (in prep.) for a complete review of these observations. o The c2d data offer an exceptional to ol for pro ducing extinction maps in all the imaged clouds. This is done by estimating the visual extinction towards each source classified as a background star, based on their SED from 1.25 µm to 24 µm. This provides multiple line-of-sight measures, which are then convolved with Gaussian beams of 90 to 300 to pro duce homogeneous extinction maps. These maps are part of the c2d data delivery. In the case of Lupus I, the low number of background stars only allowed reliable construction of an extinction map with a minimum FWHM of 120 . For more information about these maps, see Evans et al. (2007). The maps with the largest beams (300 ) are used to estimate the enclosed cloud masses (§ 5.4) and to compare them with the position of the different YSOs (§ 5.2). They can be seen in Figures 19 to 22. The extinction traces the northern cloud in the Lupus I map with a peak of AV 23 mag and shows two large clumps in Lupus III and IV, with peak extinctions of 33 and 36 mag, respectively. The maximum in Lupus III coincides with the rich star-forming cluster, while it roughly coincides with the Flat SED source SSTc2d J160115.6-415235 in Lupus IV. This is the first report of such a high extinction inactive core in Lupus IV to our knowledge, which was previously unnoticed due to its current lack of activity.

5.2.

Spatial distribution and clustering of YSOs in Lupus

Figures 19 to 22 show the spatial distribution of the PMS stars in the three Lupus clouds compared with the c2d extinction maps: In Lupus I, the most striking result is that the ma jority of the YSOs fall in a ridge of high extinction which extends in the North of the cloud with NE-SW direction. A southern high extinction region contains the pair of T Tauri stars Sz 68 and Sz 69. The ma jority of the ob jects, of any SED class but with larger abundance of Class I and Flat SED sources, appear very close to high extinction regions, with the exception of the Class III sources Sz 67 and SSTc2d J153803.1-331358 and the Flat spectrum source IRAS 15398-3359. The close match between the YSO distribution and extinction map in the region and the early class of most of the ob jects suggests that we are seeing the ob jects in the places where they were just born. The sources in Lupus III are dramatically concentrated in the dense star-forming cluster


­ 53 ­ at RA 16h 09m and DEC -39o 10, which contains the two bright intermediate mass Herbig Ae/Be stars HR 5999 and HR 6000 in the centre. In this case, ob jects of all classes are found in the vicinity of the dense cluster and at large distances from it. Figure 21 zo oms into the cluster, showing the extraordinary density of PMS ob jects at the highest extinction area in the whole cloud, where star formation is extremely active. Amongst many Class II and III sources, the cluster contains four Class I sources, including Lupus3MMS, claimed to be the only Class 0 ob ject in the Lupus clouds (Tachihara et al. 2007). Note that only 3 of them appear in Figure 21, while the forth is visible in Figure 20 to the South of the cluster. Figure 22 shows the distribution of YSOs in Lupus IV around a very dense, yet quite unpopulated, extinction peak at RA 16h 02m and DEC -41o50 which contains the only Flat spectrum source in the cloud: SSTc2d J160115.6-415235. The rest of the Class II and III sources, together with the Class I source IRAS 15589-4134 are found surrounding the core, but following a different spatial pattern, which suggests that they might have been formed in a different structure. As the contour plot nicely shows, the peak extinction at this clump is higher than that of the star-forming cluster in Lupus III (see also § 5.1). This fact together with the relative Class III predominance in Lupus IV suggests that star-formation may have taken place before in other regions of this cloud and may be about to start in this core. We must note, however, that an ob ject like Lupus3 MMS would have not been detected in this core, since it was only thanks to its millimeter detection that it was identified as a cloud member in Lupus III and such observations are so far not available for Lupus IV. The observation of these complex extinction structures and YSO distributions has stimulated for many years the discussion on how star-formation takes place, whether it is a hierarchical pro cess or whether it takes place in a centrally-condensed way (see Lada & Lada 2003, LL03 hereafter, and references therein). In order to study the sub ject with the new Spitzer data, we need to set some standards that will be applied across the c2d observational set. Similar to the other c2d clouds (see, e.g., Alcal´ et al. 2008) we identified substructure a in the Lupus clouds using the nearest neighbor algorithm applied by Gutermuth et al. (2005) (see JÜrgensen et al. 2008, in prep. for details). Following the discussion by JÜrgensen et al. we divide concentrations of PMS ob jects up into "clusters" or "groups" depending on whether they have more or less than 35 members at a given volume density level. We furthermore identify structures with volume densities higher than 1 M pc-3 (the criterion for a cluster by LL03) or 25 M pc-3 as being "lo ose" or "tight", respectively. Figure 23 shows the result of the nearest neighbor analysis for the whole Lupus sample. When applied to Lupus this algorithm breaks the complex into three separate entities: two tight concentrations of PMS stars at the 25 M pc-3 level and a lo ose one at the 1 M pc-3 level (taking into account the difference in distance between Lupus I and IV on one hand


­ 54 ­ and Lupus III on the other). The Lupus IV cloud has one lo ose group and Lupus I a tight group. The Lupus III cloud has one tight cluster containing 118 members. Table 8 shows the number of PMS ob jects of the different classes in the regions identified above. This analysis allows ordering the ob jects by degree of clustering, with Lupus III being the most clustered region, followed by Lupus I and Lupus IV. Overall, both the cloud density structure and the distribution of stars in the three regions suggest a centrally-condensed structure dominating the star-formation pro cess only in Lupus III and a more disperse distribution of volume density enhancements in the other two clouds, mostly at Lupus IV, where star-forming cores have formed along a cloud filament in the NE-SW direction. As a whole, the three clouds clearly show a hierarchical structure with separate gas concentrations that evolve independently. This scenario argues in favor of a larger presence of turbulence over gravitational forces (LL03), which is consistent with the Lupus clouds being flanked by the large Scorpius-Centaurus OB asso ciations and therefore sub ject to their strong high-energy radiation (Comer´n 2008). o


­ 55 ­

Fig. 19.-- Spatial distribution of the spectrally confirmed PMS ob jects (black symbols) and candidates (white symbols) in Lupus I as function of Lada Class, over-plotted on the contours from the c2d extinction map (continuous lines). The contour levels of extinction are from 2 mag to 20 mag, in steps of 2 mag. The shaded areas, from light to dark-gray, display the regions observed with MIPS, WFI and IRAC, respectively. The dashed lines outside the IRAC area are the contour levels of extinction from Cambr´sy (1999), from 1 mag to 6 mag e in steps of 0.35 mag. The higher resolution and sensitivity to higher AV of the c2d extinction map with respect to that of Cambr´sy (1999) can be appreciated. e


­ 56 ­

Fig. 20.-- Spatial distribution of the PMS ob jects (filled symbols) and candidates (open symbols) in Lupus III as function of Lada Class, over-plotted on the contours from the c2d extinction map (continuous lines). Symbols as in Figure 19.


­ 57 ­

Fig. 21.-- Zo om of the dense star-forming cluster in Lupus III. Symbols as in Figure 19, except the dashed lines, which are the 2 to 14 mag contours on the c2d extinction map in steps of 2 magnitudes.


­ 58 ­

Fig. 22.-- Spatial distribution of the PMS ob jects (filled symbols) and candidates (open symbols) in Lupus IV as function of Lada Class, over-plotted on the contours from the c2d extinction map (continuous lines). Symbols as in Figure 19.


­ 59 ­

Fig. 23.-- Volume density plot for the three Lupus clouds as determined with the nearestneighbor algorithm by J. JÜrgensen et al. (2007, in preparation). The derived contours are compared with extinction map from Cambr´sy (1999) in gray scale from 2 to 4.1 in steps e of 0.7 mag. The blue contour corresponds to the 1âLL03 level, the yellow to the 25âLL03 level, and the green ones correspond to levels of 0.125, 0.25, 0.5, 2, 4 and 8 times that level. The two groups and the cluster in Lupus III are identified with labels.


­ 60 ­ 5.3. Star Formation Rates

We can also use our complete samples to estimate the star formation rates. In section 3 we computed the total numbers of YSOs and PMS ob jects for each of the three clouds. The IRAC+MIPS coverage areas reported in § 2.2 were used for the YSOs and the overlapping MIPS areas as given by Chapman et al. (2007) for the PMS stars. Using the typical average mass of 0.5 M for consistency with the other c2d clouds, we find total masses in YSOs of 6, 34, and 6 M in Lupus I, III and IV, respectively. A more appropriate average value for the stellar mass in Lupus of 0.2 M (§ 4.3) would yield total masses in YSOs of 2, 14, and 2 M in Lupus I, III and IV, respectively and therefore it would scale all the results down by 40 % of the quoted values accordingly. These numbers could be slightly underestimated since very embedded ob jects in the extinction peaks could have not been detected, as it was illustrated by our inability to select Lupus3 MMS based on Spitzer data only. However, given the relative small areas of the very embedded regions, the number of hidden Class 0 of I ob jects should not be large compared to the total number of stars in the cloud. Age estimates for the YSOs in Lupus suffer from many the uncertainties in assigning PMS tracks to positions on CMDs (e.g., Mayne et al. 2007), including the uncertain distances to the Lupus clouds. Hughes et al. (1994) use 150 pc for all clouds and obtained an age range from less than 1 to 10 Myr with a peak at 3.2 Myr, however, Comer´n et al. (2003) found o ages between 1 and 1.5 Myr for ob jects in Lupus III using a distance of 200 pc (see also the discussion on the ages by Comer´n 2008). Detailed determinations of the individual stellar o ages for the entired sample will be performed once an optical spectroscopy survey of the sample is completed. This section assumes the average value of 2 Myr for all the stars in Lupus. Table 6 shows the results of these calculations: star formation rates of 3, 17, and 3 M Myr-1 are found, or up to two times these values if we include the PMS stars and candidate PMS stars, in the Lupus I, III and IV clouds, respectively. The numbers are consistent with those found in another low-star forming regions and assume that all stars were formed approximately at the same time. However, it is know that some of these young stellar populations might have appeared at different times, pro ducing a spread in ages (e.g. Hughes et al. 1994). The clusters are clearly young so it is reasonable to assume that new-born stars should be close to the places were they were born. Indeed, early Class ob jects were found systematically close to the high extinction regions in Lupus I and many Class II ob jects cluster around the two bright Herbig Ae/Be stars HR 5999 and HR 6000 in the center of the Lupus III cluster. The formation of these latter ob jects could have been triggered by the strong winds of the two intermediate-mass stars but we found no other evidence for triggered-star formation like clustered populations of ob jects with the same class in our mosaics. The ages calculated for the PMS stars in the clouds are also in


­ 61 ­ agreement with the expected cloud removal time-scales of < 5 Myrs after the onset of the star-formation pro cess (Ballesteros-Paredes & Hartmann 2007).

Table 6: Numbers, Densities and Star Formation Rates in Lupus Type Area N N/ N/Area N/Vol SFR -2 2 -2 -2 -3 deg pc deg pc pc M Myr Lupus I YSOs 1.39 9.49 13 9.4 1.4 0.43 3.3 Total 3.82 26.07 17 4.5 0.6 0.13 4.3 Lupus I I I YSOs 1.34 16.26 69 51.5 4.2 1.05 17.3 Total 2.88 34.94 124 43.0 3.5 0.60 31.0 Lupus IV YSOs 0.37 2.52 12 32.4 4.8 3.00 3.0 Total 1.08 7.37 18 16.7 2.4 0.90 4.5

-1

SFR/Area M Myr-1 pc- 0.35 0.16 1.06 0.89 1.19 0.61

2

Note. -- is the solid angle subtended by the cloud, `Area' is the equivalent in square parsec, `N' is the number of ob jects, and `SFR' stands for Star Forming Rate.

5.4.

Cloud Masses and Star Formation Efficiencies

Table 7 summarizes the cloud mass measurements from the literature as cited in the Comer´n (2008, in prep.). To those, we add the c2d-derived masses of the clouds from the o extinction maps with the lowest spatial resolution (300 ) as explained in the Delivery Do cumentation (Evans et al. 2007). The table shows large differences in these mass estimates, most of which are due to the fact that the areas used to compute the total cloud masses differ from the c2d area, whereas both the number of YSOs and c2d cloud mass estimates were obtained from the same area. For this reason, we will use the c2d values (marked with an `e' in the table) in the following. Based on these mass estimates Formation Efficiency (SFE) as S F Mstar is the total mass in YSOs ob populations, which range from 6 to and following Alcal´ et al. (2008), we a Mstar E = Mcloud +Mstar where Mcloud is the jects, i.e. the sum of the masses over 34 M for the YSOs and from 8 to 62 derived the Star cloud mass and the entire stellar M if we include


­ 62 ­

Table 7: Estimates of the cloud masses and Star Formation Efficiencies (SFE) in Lupus Tracer Mass SFE (%) M YSOs Total Lupus I 13 CO 8 7 8a 0.7 0.9 18 b CO 326 1.8 2.4 c Extinction 22851 0.0 0.0 d Extinction 654 0.9 1.2 e Extinction 479 1.2 1.6 Lupus I I I 13 CO 1 1 9 5a 2.8 4.9 18 b CO 418 7.6 12.9 c Extinction 10547 0.3 0.6 d Extinction 1666 2.0 3.6 e Extinction 846 3.9 6.8 Lupus IV 18 CO 2 1 6b 2.7 4.0 c Extinction 1406 0.4 0.6 d Extinction 225 2.6 3.8 e Extinction 196 3.0 4.4



All the masses have been normalized to the distances of 150 pc for Lupus I and IV and 200 pc for Lupus III. Total mass of H2 derived from the
13

a b c d e

CO luminosity (Tachihara et al. 1996).

Total mass of H2 derived from the C O luminosity (Hara et al. 1999). Cloud mass for AV above 2 (Cambr´sy 1999). e Mass in dense condensations as derived from extinction (Andreazza & Vilas-Boas 1996). Cloud mass for Av > 2 for Lupus III and IV and for Av > 3 for Lupus I using the c2d extinction maps.

18

the PMS stars (c.f. § 5.3). The average stellar mass (0.5 M ) was used here to derive Mstar . The results on the efficiency of star formation are provided in Table 7. We estimate the SFE in the Lupus clouds to be 0.7 ­ 2.4 %, 2.0 ­ 12.9 % and 2.6 ­ 4.4 % for the three clouds, respectively. The large cloud masses from Cambr´sy (1999) were derived for much e larger areas and therefore were not considered. In spite of the large differences in total cloud mass estimates, these numbers are consistent the previous estimates in the literature for


­ 63 ­

Table 8: Star Formation Total Total 159 Extended 23 I LG 6 . . .tight TG 5 III LC 1 1 8 . . .tight TC 79 IV LG 1 2

efficiencies I 8 (4.4%) 3 (9.1%) 0 (0.0%) 0 (0.0%) 4 (3.4%) 4 (5.1%) 1 (8.3%)

(SFE) Flat 12 2 1 1 8 5 1

and II 75 11 5 4 53 37 6

class III 64 20 0 0 45 25 4

numb AV ... ... 2.75 6.06 1.47 3.85 2.96

ers by reg Mass 1501.4 386.1 99.19 15.72 793.6 318.9 169.6

ion in Lupus. Volume SFE ... 5.0% ... 2.8% 1.69 2.9% 0.0326 13.7% 98.0 6.9% 5.69 11.0% 3.39 3.4%

Note. -- The SFEs and number of ob jects of per class are presented for different sub-samples according to their spatial distribution: the first two rows show the Total and Extended populations, `LG' stands for Loose Group, `TG' is Tight Group, `LC' is Loose Cluster, and `TC' is Tight Cluster, defined at § 5.2 and shown in Fig. 23. The AV , the enclosed masses and volumes were calculated for each of the regions following JÜrgensen et al.

Lupus (0.4 ­ 3.8%, Tachihara et al. 1996) and somewhat higher than estimates for other T asso ciations like e.g. Taurus (1­2%, Mizuno et al. 1999). We can also calculate the same numbers for the different sub-structures identified in the distribution of the PMS ob jects. Table 8 gives the number of ob jects of the different classes in the different groups and clusters described in § 5.2 along with the enclosed cloud masses calculated in the areas subtended by each of the groups and clusters and the c2d extinction maps. The resulting SFE values for each region are also given in the table. All SFEs are larger for the groups and clusters than for the extended population or the global cloud SFEs, as to be expected. The SFEs for the Lo ose Group (LG) and Tight Group (TG) in Lupus I (see § 5.2) are 2 and 8 times the cloud average SFE in Table 7, while the SFE in the Lo ose Group in Lupus IV almost matches the global SFE in that cloud. The large numbers in the tight group and cluster in Lupus I and III are due to the relatively small areas containing a mo derate numbers of forming stars and seems to suggest again that the star-formation pro cess is more clustered in both clouds, with bigger differences in the SFEs between the clustered and extended population than in Lupus IV, where there is no substantial difference. The caveat for all these SFE analyses is that the definition of the cloud area used for the cloud mass calculations depends on the surface density of PMS stars and therefore assumes that the remaining cloud outside the chosen area is not related to the formation of the stars inside of it, which is probably correct, but also that a given amount of cloud gas density will always pro duce a given amount of stars, i.e., it assumes that the star-formation pro cess


­ 64 ­ is universal and not affected by other characteristics of the cloud like its composition or its initial angular momentum. With this caveat in mind, it is however worth noticing that the SFEs calculated for the bulk of the PMS populations in the three Lupus clouds (i.e. the lo ose cluster and groups) scale linearly with the enclosed masses in the areas defining the lo ose clusters or groups. This correlation between SFE and cloud mass is suggestive and was never found when a cutoff in AV was used to define the cloud boundaries and masses. The result is also interesting since it matches well the dynamical and fast star-formation scenario recently proposed (LL03, Bate et al. 2003): it might help explaining the presence of ob jects of very different evolutionary stages at small distances as the result of several mild star-formation events in small clouds before a big star-formation event contributes to the bulk of the co eval PMS stars in each of the regions (Ballesteros-Paredes et al. 2007).

6.

Summary

We present observations of the Lupus I, III and IV dark clouds at 3.6, 4.5, 5.8 and 8.0 µm made with the Spitzer Space Telescope Infrared Array Camera (IRAC) and discuss them along with optical, near-infrared, observations made with the Multiband Imaging Photometer for Spitzer (MIPS) onboard Spitzer and millimeter flux from the literature to provide a complete description of the three clouds and their young stellar populations. The main results can be summarized as follows: · We performed a census of the Young Stellar Ob jects (YSO) applying the c2d Spitzer color criteria in the three clouds and increase the number of cloud members by more than a factor of 4. The PMS population consists of 159 stars in the three clouds with infrared (IR) excess or spectroscopically determined membership, mostly found in the high density regions of the clouds and greatly dominated by low and very low-mass ob jects. The sample is complete down to M 0.1 M and probes well down into the sub-stellar regime. · 30 ­ 40% of sources are multiple with binary separations between 0.7 and 10 (100 to 2000 AU). These long perio d binaries appear not to affect the disk properties. · A large ma jority of the YSOs in Lupus are Class II or Class III ob jects, with only 20 (12%) of Class I or Flat spectrum sources. Ob jects of all classes appear equally distributed in the clouds and tend to cluster around the cloud high density peaks, except in Lupus IV where they do not follow the extinction distribution. · The disk survey is complete down to "debris"-like systems in stars as small as M 0.2 M and includes sub-stellar ob jects with larger IR excesses. The disk fraction


­ 65 ­ in Lupus is 70 ­ 80%, consistent with an age of 1 ­ 2 Myr. However, the young population contains 20% optically thick accretion disks and 40% relatively less flared disks regarding their Spitzer SEDs. · A larger variety of inner disk structures is found for larger inner disk clearings, suggesting several possible evolutionary paths for the primordial disks. Similar disk masses are found for a range of inner disk clearings, which provides evidence against a clearing of the inner disks by photo evaporation. · All previously known Herbig-Haro ob jects with sizes larger than 3 were found in the Spitzer images of the clouds and two new sources are reported: a jet-like structure in Lupus III and a nebulous ob ject in Lupus IV. · Lupus I consist of a filamentary cloud structure with three density enhancements closely followed by early class ob jects. Lupus III contains a very active star-forming cluster with a very large number of ob jects of all classes. Lupus IV shows the highest extinction peak in Lupus with few late class ob jects away from the density peak. · Clustering analysis of the PMS distribution recovers separate structures in the three clouds, with Lupus III being the most centrally populated and rich, followed by Lupus I and Lupus IV. Overall, the cloud structures are compatible with predictions from the hierarchical star formation scenario. · We estimate star formation efficiencies of a few percent and a star formation rate of 2 ­ 10 M Myr-1 in the Lupus clouds. We also find a tentative linear correlation between the star formation efficiencies and the enclosed cloud masses of the three main stellar groups in Lupus.


Table 9. Young Stellar Ob jects and Pre-Main Sequence stars in Lupus
No. c2d Name Ob ject ids. R.A. (J2000) DEC. (J2000) Sel. PMS status Lada Class Refs

Lupus I 1 2 3 4 5 6 7 8 9 1 1 1 1 1 1 1 1 1 1 2 2 2 2 2 2 SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST c c c c c c c c c c c c c c c c c c c c c c c c c 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 d d d d d d d d d d d d d d d d d d d d d d d d d J J J J J J J J J J J J J J J J J J J J J J J J J 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 5 5 5 5 5 5 5 5 5 5 5 5 5 5 5 5 5 6 6 6 6 6 6 6 6 3 3 3 3 3 4 4 4 4 4 4 4 4 4 4 4 4 0 0 0 0 0 0 0 0 8 8 9 9 9 0 1 2 2 3 3 4 5 5 5 5 5 7 7 7 7 7 7 7 7 0 4 2 2 2 3 4 1 4 0 0 5 0 0 1 1 1 0 0 0 1 1 1 1 2 3 8 7 7 8 8 0 4 0 1 2 7 6 8 2 7 8 3 8 8 0 1 4 5 3 .1 .2 .3 .8 .3 .3 .8 .6 .3 .3 .3 .9 .3 .9 .9 .4 .5 .9 .6 .6 .1 .6 .0 .2 .4 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 4 3 3 4 4 4 4 4 3 4 4 4 4 4 4 4 4 4 4 9 9 9 9 9 8 0 9 1 4 4 4 4 2 4 1 1 0 4 2 1 1 1 1 2 1 1 4 1 0 5 0 0 3 0 8 6 6 1 5 0 3 9 4 3 7 7 7 8 1 1 4 7 1 3 2 3 5 58 41 44 17 18 37 19 26 43 15 06 40 38 34 31 29 25 12 07 23 04 48 38 42 10 ... IRAS 1 AKC20 Sz 65 / Sz 66 Sz 67 / AKC20 ... ... IRAS 1 ... AKC20 ... ... Sz 68 / Sz 69 / ... ... ... ... Sz 9 Sz 9 Lup Sz 9 Lup 5 3 5 6 -3 4 3 0 0 6 -1 7 IK Lup / HBC 597 KWS97 Lup 1-11 0 6 -1 8 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 5 5 5 5 5 5 5 5 5 5 5 5 5 5 5 5 5 6 6 6 6 6 6 6 6 3 3 3 3 3 4 4 4 4 4 4 4 4 4 4 4 4 0 0 0 0 0 0 0 0 8 8 9 9 9 0 1 2 2 3 3 4 5 5 5 5 5 7 7 7 7 7 7 7 7 0 4 2 2 2 3 4 1 4 0 0 5 0 0 1 1 1 0 0 0 1 1 1 1 2 3 8 7 7 8 8 0 4 0 1 2 7 6 8 2 7 8 3 8 8 0 1 4 5 3 .1 .3 .2 .7 .2 .2 .8 .5 .3 .2 .2 .9 .3 .8 .8 .4 .5 .8 .5 .6 .0 .6 .0 .2 .4 0 6 8 8 9 7 2 7 2 9 9 0 4 8 7 2 3 5 7 4 8 0 0 0 4 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 4 3 3 4 4 4 4 4 3 4 4 4 4 4 4 4 4 4 4 9 9 9 9 9 8 0 9 1 4 4 4 4 2 4 1 1 0 4 2 1 1 1 1 2 1 1 4 1 0 5 0 0 3 0 8 6 6 1 5 0 3 9 4 3 7 7 7 8 1 1 4 7 1 3 2 3 5 5 3 4 1 1 3 1 2 4 1 0 3 3 3 3 2 2 1 0 2 0 4 3 4 1 7 8 4 7 8 6 9 5 3 5 6 9 8 3 0 8 4 1 7 2 3 7 7 2 0 .7 .2 .3 .4 .3 .7 .0 .8 .0 .4 .2 .5 .2 .7 .8 .5 .8 .6 .7 .7 .5 .7 .9 .0 .1 YSO YSO (5) YSO YSO (1) (5) YSO YSO YSO YSO YSO YSO YSO (1) YSO YSO YSO YSO (7) YSO YSO (4) (1) (4) Cnd PMS Cnd PMS PMS PMS Cnd Cnd Cnd Cnd Cnd Cnd Cnd Cnd PMS PMS Cnd Cnd Cnd Cnd PMS PMS Cnd PMS Cnd III I III II II III II I III F F II F II II II II F F II II III III III III 12 10, 12 5 1,12 1,12 1 5 12 12 1,12 12 5,12 12 12 1 1,12 12 12 12 7 1,12 1,12 4 1 4

­ 66 ­

0 1 2 3 4 5 6 7 8 9 0 1 2 3 4 5

5 3 9 8 -3 3 5 9 0 6 -1 9

HT Lup / HBC 248 HW Lup / HBC 598 Lupus I I I

0 1 6 2 6

/ HBC 613 / KWS97 Lup 3-23 / HBC 614 / KWS97 Lup 3-24 05 / Th 2 2 54


Table 9--Continued
No. c2d Name Ob ject ids. R.A. (J2000) DEC. (J2000) Sel. PMS status PMS PMS PMS Cnd Cnd Cnd Cnd PMS Cnd Cnd Cnd PMS PMS PMS PMS PMS PMS PMS Cnd Cnd PMS PMS Cnd PMS Cnd PMS Cnd Lada Class II III II III F III III II II III II II II III II II II II II III III I I II II II F Refs

2 2 2 2 3 3 3 3 3 3 3 3 3 3 4 4 4 4 4 4 4 4 4 4 5 5 5

6 7 8 9 0 1 2 3 4 5 6 7 8 9 0 1 2 3 4 5 6 7 8 9 0 1 2

SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST

c c c c c c c c c c c c c c c c c c c c c c c c c c c

2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2

d d d d d d d d d d d d d d d d d d d d d d d d d d d

J J J J J J J J J J J J J J J J J J J J J J J J J J J

1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1

6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6

0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0

7 7 7 7 7 7 7 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8

3 4 5 5 5 5 5 0 0 0 0 1 1 1 2 2 2 2 2 2 2 2 3 3 3 3 3

7 9 2 4 4 5 8 0 1 3 6 2 5 6 1 2 4 5 8 8 8 9 0 0 0 0 1

.7 .6 .3 .1 .7 .3 .9 .2 .7 .0 .2 .6 .0 .0 .8 .5 .0 .8 .1 .2 .4 .7 .1 .3 .7 .8 .1

-

3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3

9 9 8 9 9 9 9 9 9 8 9 9 8 9 9 9 9 9 9 9 9 9 9 9 8 9 8

2 0 5 2 1 0 2 0 1 5 1 0 5 0 0 0 0 0 1 0 0 0 2 0 2 0 5

1 4 8 0 5 7 4 3 2 2 2 8 7 3 4 4 5 6 3 4 5 3 2 6 8 5 6

3 2 0 4 4 1 3 0 3 2 2 3 1 0 2 4 4 0 1 2 3 1 5 1 2 4 0

9 9 6 6 5 8 5 0 1 9 3 4 5 4 2 6 9 1 0 5 2 1 9 1 7 9 0

Lup 713 Sz 94 / KWS97 Lup 3-28 Sz 95 ... 2MASS J16075475-3915446 ... Lup 714 Lup 604s 2MASS J16080175-3912316 ... 2MASS J16080618-3912225 Sz 96 2MASS J16081497-3857145 Par-Lup3-1 Sz 97 / Th 24 Sz 98 / HK Lup / HBC 616 Sz 99 / Th 25 Sz 100 / Th 26 Lup 607 NTO2000-0526.9-5630 Sz 101 / Th 27 Sz 102 / Krautter's star IRAC J16083010-3922592 Sz 103 / Th 29 / HBC 618 ... Sz 104 / Th 30 IRAC J16083110-3856000

1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1

6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6

0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0

7 7 7 7 7 7 7 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8

3 4 5 5 5 5 5 0 0 0 0 1 1 1 2 2 2 2 2 2 2 2 3 3 3 3 3

7 9 2 4 4 5 8 0 1 3 6 2 4 6 1 2 4 5 8 8 8 9 0 0 0 0 1

.7 .6 .3 .0 .7 .2 .9 .2 .7 .0 .1 .6 .9 .0 .7 .5 .0 .7 .1 .1 .4 .7 .1 .2 .7 .8 .1

2 0 2 9 5 9 0 0 5 2 7 2 6 3 9 0 4 6 0 6 3 3 0 6 0 1 0

-

3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3

9 9 8 9 9 9 9 9 9 8 9 9 8 9 9 9 9 9 9 9 9 9 9 9 8 9 8

2 0 5 2 1 0 2 0 1 5 1 0 5 0 0 0 0 0 1 0 0 0 2 0 2 0 5

1 4 8 0 5 7 4 2 2 2 2 8 7 3 4 4 5 6 3 4 5 3 2 6 8 5 6

3 2 0 4 4 1 3 5 3 2 2 3 1 0 2 4 4 0 1 2 3 1 5 1 2 4 0

8 9 6 6 4 7 4 9 1 9 2 3 4 4 1 6 9 1 0 4 2 1 9 1 6 8 0

.8 .0 .3 .2 .6 .8 .9 .7 .6 .3 .5 .5 .5 .2 .5 .0 .4 .1 .0 .6 .4 .0 .2 .1 .8 .8 .0

YSO (1) YSO YSO YSO YSO (4) YSO (2) YSO YSO YSO YSO (1) YSO YSO YSO YSO (3) (6) YSO YSO (6) YSO (7) YSO (2)

4,12 1, 11 1, 11,12 12 6,12 12 4 4,6,12 6 12 6,12 1,11,12 6,12 3 1,12 1, 11,12 1,12 1, 11,12 4 2 1, 11,12 1, 11,12 6 1,12 7 1,12 6

­ 67 ­


Table 9--Continued
No. c2d Name Ob ject ids. R.A. (J2000) DEC. (J2000) Sel. PMS status PMS PMS PMS PMS PMS PMS PMS Cnd Cnd Cnd PMS Cnd PMS PMS PMS Cnd Cnd PMS PMS Cnd PMS PMS Cnd Cnd Cnd PMS Cnd Lada Class II III III II II III III II I III III III II II II II III II II II II II II II III II II Refs

5 5 5 5 5 5 5 6 6 6 6 6 6 6 6 6 6 7 7 7 7 7 7 7 7 7 7

3 4 5 6 7 8 9 0 1 2 3 4 5 6 7 8 9 0 1 2 3 4 5 6 7 8 9

SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST

c c c c c c c c c c c c c c c c c c c c c c c c c c c

2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2

d d d d d d d d d d d d d d d d d d d d d d d d d d d

J J J J J J J J J J J J J J J J J J J J J J J J J J J

1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1

6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6

0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0

8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 9

3 3 3 3 3 4 4 4 4 4 4 4 4 5 5 5 5 5 5 5 5 5 5 5 5 5 0

4 4 5 7 9 1 2 2 6 7 8 8 9 1 1 3 3 3 4 5 5 7 8 8 8 9 1

.3 .6 .8 .3 .8 .8 .7 .7 .8 .5 .2 .2 .4 .4 .6 .2 .7 .7 .7 .3 .5 .8 .3 .3 .9 .5 .4

-

3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3

9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 8 9 9 9 9 9 8 9

0 0 0 2 0 0 0 0 0 0 0 0 0 0 0 1 0 1 3 4 0 0 0 0 0 5 2

6 5 3 3 6 1 6 6 2 5 4 9 5 5 3 4 4 4 7 8 2 2 7 7 4 6 5

18 34 48 11 25 37 18 15 07 09 19 20 39 30 18 40 10 37 44 48 34 23 36 49 46 28 12

HR 5999 / V856 Sco / HBC 619 HR 6000 / KWS97 Lup 3-40 / V1027 Sco Par-Lup3-2 Lup 706 Sz 106 Sz 107 / KWS97 Lup 3-44 Sz 108 / HBC 620 / KWS97 Lup 3-45 Sz 108B IRAC J16084679-3902074 2MASSJ16084747-3905087 Sz 109 Lup 617 Par-Lup3-3 Par-Lup3-4 Sz 110 / Th 32 / HBC 621 2MASS J16085324-3914401 NTO2000-0532.1-5616 2MASS J16085373-3914367 Sz 111 / Th 33 / HBC 622 2MASS J16085529-3848481 Sz 112 Sz 113 / Th 34 NTO2000-0536.7-5943 NTO2000-0536.7-5956 NTO2000-0537.4-5653 2MASS J16085953-3856275 ...

1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1

6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6

0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0

8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 9

3 3 3 3 3 4 4 4 4 4 4 4 4 5 5 5 5 5 5 5 5 5 5 5 5 5 0

4 4 5 7 9 1 2 2 6 7 8 8 9 1 1 3 3 3 4 5 5 7 8 8 8 9 1

.3 .6 .7 .3 .7 .7 .7 .8 .7 .4 .1 .1 .4 .4 .5 .2 .6 .7 .6 .2 .5 .8 .2 .3 .9 .5 .4

0 0 8 0 6 9 3 7 9 7 6 7 0 3 7 3 8 3 8 9 2 0 7 0 2 3 0

-

3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3

9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 8 9 9 9 9 9 8 9

0 0 0 2 0 0 0 0 0 0 0 0 0 0 0 1 0 1 3 4 0 0 0 0 0 5 2

6 5 3 3 6 1 6 6 2 5 4 9 5 5 3 4 4 4 7 8 2 2 7 7 4 6 5

1 3 4 1 2 3 1 1 0 0 1 1 3 3 1 4 0 3 4 4 3 2 3 4 4 2 1

8 4 7 0 5 7 8 4 7 8 9 9 9 0 7 0 9 6 3 8 3 2 5 9 6 7 1

.0 .0 .9 .8 .3 .0 .3 .7 .4 .7 .2 .9 .3 .4 .7 .3 .6 .7 .9 .1 .9 .7 .5 .4 .0 .6 .9

(1) (1) (3) (4) YSO YSO (1) YSO (2) (2) (1) (3) YSO YSO YSO YSO (6) YSO (1) YSO YSO YSO YSO (2) (2) YSO YSO

1

3 1

1

1,11 1 3, 11 4 1,12 , 11,1 1, 11 1,12 6 6 1, 11 4 , 11,1 3,12 , 11,1 6, 12 2 6,12 1 6 , 11,1 1,12 2,12 2 2 6, 12 12

2

­ 68 ­
2 2 2


Table 9--Continued
No. c2d Name Ob ject ids. R.A. (J2000) DEC. (J2000) Sel. PMS status PMS Cnd PMS Cnd Cnd Cnd Cnd PMS Cnd Cnd Cnd Cnd Cnd Cnd Cnd Cnd Cnd Cnd Cnd Cnd Cnd PMS PMS PMS Cnd Cnd Cnd Lada Class II III II III III II III I II II III II III III F III III III III II III III II II III III II Refs

8 8 8 8 8 8 8 8 8 8 9 9 9 9 9 9 9 9 9 9 1 1 1 1 1 1 1

0 1 2 3 4 5 6 7 8 9 0 1 2 3 4 5 6 7 8 9 0 0 0 0 0 0 0

0 1 2 3 4 5 6

SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST

c c c c c c c c c c c c c c c c c c c c c c c c c c c

2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2

d d d d d d d d d d d d d d d d d d d d d d d d d d d

J J J J J J J J J J J J J J J J J J J J J J J J J J J

1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1

6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6

0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0

9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9

0 0 0 0 0 1 1 1 2 2 2 2 2 3 3 3 3 3 3 3 4 4 4 4 4 5 5

1 2 6 8 8 6 7 8 0 3 6 7 7 4 4 5 7 7 7 9 1 2 4 8 9 4 6

.8 .4 .2 .0 .5 .4 .1 .1 .3 .2 .6 .0 .1 .1 .2 .4 .2 .2 .4 .3 .1 .6 .3 .6 .9 .5 .3

-

3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3

9 9 9 9 9 9 9 9 9 9 9 8 9 9 9 9 9 9 9 9 9 9 9 9 8 9 8

0 0 0 0 0 0 2 0 0 0 0 3 0 1 1 0 0 0 0 0 0 1 1 1 4 1 5

5 5 8 7 3 4 7 4 4 4 3 6 2 3 5 2 4 7 5 4 2 9 3 1 9 2 9

1 4 5 2 4 4 1 5 0 0 5 2 2 4 1 0 0 4 2 3 0 4 3 1 0 0 5

3 9 2 6 3 4 0 3 2 7 8 8 8 2 3 5 7 5 6 2 6 1 0 7 3 4 2

Sz 114 / V908 Sco / HBC 623 NTO2000-0540.9-5757 Sz 115 NTO2000-0546.4-5934 Lup 608s NTO2000-0554.9-5651 Lup 710 Lupus3 MMS NTO2000-0558.8-5610 NTO2000-0601.7-5616 NTO2000-0605.1-5606 ... NTO2000-0605.6-5437 ... IRAC J16093418-3915127 NTO2000-0614.0-5414 NTO2000-0615.6-5616 NTO2000-0615.6-5953 NTO2000-0615.8-5734 NTO2000-0617.7-5641 NTO2000-0619.6-5414 Sz 116 / Th 36 / HBC 625 Sz 117 / Th 37 / HBC 626 Sz 118 Lup 650 Lup 810s Lup 818s

1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1

6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6

0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0

9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9

0 0 0 0 0 1 1 1 2 2 2 2 2 3 3 3 3 3 3 3 4 4 4 4 4 5 5

1 2 6 7 8 6 7 8 0 3 6 6 7 4 4 5 7 7 7 9 1 2 4 8 9 4 6

.8 .4 .2 .9 .5 .4 .1 .0 .3 .1 .6 .9 .0 .1 .1 .3 .1 .1 .3 .2 .0 .5 .3 .6 .8 .4 .2

4 4 1 8 0 3 3 7 0 5 1 8 8 1 8 7 5 9 8 9 8 7 4 4 7 9 9

-

3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3

9 9 9 9 9 9 9 9 9 9 9 8 9 9 9 9 9 9 9 9 9 9 9 9 8 9 8

0 0 0 0 0 0 2 0 0 0 0 3 0 1 1 0 0 0 0 0 0 1 1 1 4 1 5

5 5 8 7 3 4 7 4 4 4 3 6 2 3 5 2 4 7 5 4 2 9 3 1 9 2 9

1 4 5 2 4 4 0 5 0 0 5 2 2 4 1 0 0 4 2 3 0 4 3 1 0 0 5

2 9 1 6 3 3 9 3 1 7 7 7 8 2 2 5 6 4 5 1 5 0 0 6 3 3 1

.5 .4 .8 .4 .1 .7 .7 .4 .6 .4 .7 .6 .4 .1 .7 .4 .9 .7 .7 .8 .6 .8 .3 .9 .3 .5 .7

YSO (2) YSO (2) (4) (2) (4) YSO (2) (2) (6) (7) (2) YSO (6) (2) (2) (2) (2) (2) (2) (1) YSO YSO (4) (4) YSO

1, 11,12 2 1, 11 2 4, 11 2 4 8, 12 2 2 2 7 2 12 6 2 2 2 2 2 2 1 1,12 1,12 4 4 4,12

­ 69 ­


Table 9--Continued
No. c2d Name Ob ject ids. R.A. (J2000) DEC. (J2000) Sel. PMS status PMS Cnd Cnd PMS Cnd PMS Cnd Cnd Cnd Cnd Cnd Cnd Cnd Cnd PMS Cnd Cnd Cnd Cnd Cnd Cnd Cnd PMS PMS Cnd Cnd Cnd Lada Class III III II III F III II II F II III III III II II III III III III III II III III II III F II Refs

1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1

0 0 0 1 1 1 1 1 1 1 1 1 1 2 2 2 2 2 2 2 2 2 2 3 3 3 3

7 8 9 0 1 2 3 4 5 6 7 8 9 0 1 2 3 4 5 6 7 8 9 0 1 2 3

SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST

c c c c c c c c c c c c c c c c c c c c c c c c c c c

2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2

d d d d d d d d d d d d d d d d d d d d d d d d d d d

J J J J J J J J J J J J J J J J J J J J J J J J J J J

1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1

6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6

0 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1

9 0 0 0 0 0 0 0 0 0 0 0 0 0 0 1 1 1 1 1 1 1 1 1 2 2 2

5 0 0 1 1 1 1 1 2 2 3 3 3 4 5 1 2 3 3 4 4 5 5 5 0 0 1

7 0 1 2 3 6 8 9 7 9 2 4 5 5 1 8 6 1 8 4 8 1 3 9 0 4 1

.1 .1 .3 .2 .1 .4 .6 .8 .4 .6 .6 .5 .0 .4 .6 .7 .0 .9 .6 .9 .7 .2 .4 .8 .1 .5 .2

-

3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3

8 8 9 9 8 9 8 8 9 9 7 8 9 8 8 8 9 8 9 8 8 8 9 8 8 8 8

5 5 0 2 4 0 3 3 0 2 4 1 0 5 5 5 1 1 0 3 1 5 0 2 5 0 3

9 4 6 1 6 8 6 6 2 2 6 4 6 4 3 8 1 1 8 2 7 1 2 3 5 9 2

4 0 4 1 1 0 1 0 3 1 1 5 5 5 1 2 2 1 2 4 5 0 1 3 5 5 2

8 1 5 8 7 5 3 7 0 5 5 0 5 5 4 4 3 0 8 5 8 4 6 9 7 9 0

Sz 119 ... 2MASS J1610013 Sz 121 / Th 40 / ... Sz 122 / Th 41 / ... ... ... ... IRAS 16072-3738 ... ... ... Sz 123 / Th 42 / ... ... ... Lup 831s ... ... Lup 802s Sz 124 / Th 43 / SST-Lup3-1 ... ... ...

3-3906449 KWS97 Lup 3-63 KWS97 Lup 3-64

HBC 629

HBC 631

1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1

6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6

0 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1

9 0 0 0 0 0 0 0 0 0 0 0 0 0 0 1 1 1 1 1 1 1 1 1 2 2 2

5 0 0 1 1 1 1 1 2 2 3 3 3 4 5 1 2 3 3 4 4 5 5 5 0 0 1

7 0 1 2 3 6 8 9 7 9 2 4 4 5 1 8 5 1 8 4 8 1 3 9 0 4 1

.0 .1 .3 .2 .0 .4 .5 .8 .4 .5 .5 .5 .9 .3 .6 .6 .9 .9 .6 .8 .6 .2 .3 .8 .0 .4 .2

7 1 2 1 6 4 6 4 3 7 9 1 7 8 0 9 8 3 1 6 7 0 5 1 6 8 2

-

3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3

8 8 9 9 8 9 8 8 9 9 7 8 9 8 8 8 9 8 9 8 8 8 9 8 8 8 8

5 5 0 2 4 0 3 3 0 2 4 1 0 5 5 5 1 1 0 3 1 5 0 2 5 0 3

9 4 6 1 6 8 6 6 2 2 6 4 6 4 3 8 1 1 8 2 7 1 2 3 5 9 2

4 0 4 1 1 0 1 0 3 1 1 5 5 5 1 2 2 1 2 4 5 0 1 3 5 5 1

7 1 4 8 6 5 3 6 0 4 4 0 4 4 4 3 3 0 7 4 8 4 6 8 6 9 9

.9 .1 .9 .3 .8 .4 .0 .8 .2 .7 .9 .3 .6 .9 .0 .6 .2 .4 .5 .7 .3 .2 .1 .5 .9 .0 .8

(1) YSO YSO (1) YSO (1) YSO YSO YSO YSO YSO YSO YSO YSO YSO YSO YSO YSO (4) YSO YSO (4) (1) YSO YSO YSO YSO

1 12 4,12 1 12 1 12 12 12 12 12 12 12 12 1,12 12 12 12 4 12 12 4 1 9,12 12 12 12

­ 70 ­


Table 9--Continued
No. c2d Name Ob ject ids. R.A. (J2000) DEC. (J2000) Sel. PMS status C C C C C C C C nd nd nd nd nd nd nd nd Lada Class I III II II III III III II II II II II II II II II II II III F III III III I III II Refs

1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1

3 3 3 3 3 3 4 4 4 4 4 4 4 4 4 4 5 5 5 5 5 5 5 5 5 5

4 5 6 7 8 9 0 1 2 3 4 5 6 7 8 9 0 1 2 3 4 5 6 7 8 9

SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST SST

c c c c c c c c c c c c c c c c c c c c c c c c c c

2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2

d d d d d d d d d d d d d d d d d d d d d d d d d d

J J J J J J J J J J J J J J J J J J J J J J J J J J

1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1

6 6 6 6 6 6 6 6 5 5 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6

1 1 1 1 1 1 1 1 5 5 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0

2 2 2 2 2 2 3 3 9 9 0 0 0 0 0 0 0 0 1 1 1 1 1 2 2 3

1 1 2 4 5 5 4 4 2 4 0 0 0 2 3 3 4 4 1 1 2 4 5 2 2 2

8 9 2 3 1 6 1 4 5 5 0 2 7 6 1 4 4 9 1 5 9 3 7 1 9 9

.5 .6 .7 .8 .7 .0 .0 .1 .2 .3 .6 .4 .4 .1 .1 .4 .5 .4 .6 .6 .7 .3 .0 .6 .9 .4

-

3 3 3 3 3 3 3 3 4 4 4 4 4 4 4 4 4 4 4 4 4 4 4 4 4 4

9 8 7 8 8 7 8 7 2 1 2 2 1 1 1 2 1 1 1 1 2 1 1 1 1 1

3 3 1 1 4 5 3 3 3 5 2 2 4 5 4 2 5 3 3 5 0 3 4 4 5 4

4 7 3 5 2 6 7 6 5 4 1 2 9 3 3 5 5 0 7 2 8 6 2 0 1 0

1 4 2 0 1 4 2 4 0 5 5 1 4 5 3 4 3 0 3 3 0 0 4 5 1 0

8 2 8 3 6 3 4 6 7 7 8 6 9 6 7 0 1 4 0 5 4 6 4 4 1 3

. . . . . . . .

. . . . . . . .

. . . . . . . .

1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1

6 6 6 6 6 6 6 6 5 5 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6 6

1 1 1 1 1 1 1 1 5 5 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0

2 2 2 2 2 2 3 3 9 9 0 0 0 0 0 0 0 0 1 1 1 1 1 2 2 3

1 1 2 4 5 5 4 4 2 4 0 0 0 2 3 3 4 4 1 1 2 4 5 2 2 2

8 9 2 3 1 5 0 4 5 5 0 2 7 6 1 4 4 9 1 5 9 3 7 1 9 9

.4 .6 .7 .7 .7 .9 .9 .1 .2 .2 .6 .3 .4 .1 .0 .3 .5 .4 .5 .5 .6 .2 .0 .6 .9 .4

7 0 3 5 2 6 5 1 4 8 2 7 3 3 5 9 3 2 5 5 9 8 4 1 1 1

-

3 3 3 3 3 3 3 3 4 4 4 4 4 4 4 4 4 4 4 4 4 4 4 4 4 4

9 8 7 8 8 7 8 7 2 1 2 2 1 1 1 2 1 1 1 1 2 1 1 1 1 1

3 3 1 1 4 5 3 3 3 5 2 2 4 5 4 2 5 3 3 5 0 3 4 4 5 4

4 7 3 5 2 6 7 6 5 4 1 2 9 3 3 5 5 0 7 2 8 6 2 0 1 0

1 4 2 0 1 4 2 4 0 5 5 1 4 5 3 3 3 0 3 3 0 0 4 5 1 0

8 2 7 3 6 3 3 6 7 7 7 5 8 5 7 9 1 4 0 5 3 5 3 3 1 2

.3 .2 .6 .3 .0 .8 .7 .4 .1 .2 .5 .5 .9 .6 .2 .5 .2 .1 .1 .3 .6 .7 .9 .7 .1 .7

(7) YSO (7) YSO YSO YSO YSO (7) (7) YSO (7) (7) YSO YSO YSO (7) YSO (1) YSO YSO YSO YSO YSO YSO YSO (1)

7 12 7 12 12 12 12 7 7 12 7 7 12 12 1,12 7 1,12 1 12 12 12 12 12 12 12 1

Lupus IV ... ... ... ... IRAS 15567-4141 ... Sz 130 / HBC 610 ... F 403 / MY Lup / IRAS 15573-4147 Sz 131 ... ... ... ... IRAS 15585-4134 IRAS 15589-4132 ... Sz 133

Cnd Cnd Cnd Cnd Cnd Cnd PMS Cnd PMS PMS Cnd Cnd Cnd Cnd Cnd Cnd Cnd PMS

­ 71 ­


Table 9--Continued
No. c2d Name Ob ject ids. R.A. (J2000) DEC. (J2000) Sel. PMS status Lada Class Refs

Note. -- Column 1 gives an identification number. Columns 2 and 3 give the c2d and previous names when available. Note that the c2d names are slightly different from those in Chapman et al. (2007) due to a change in the naming convention. Columns 4 and 5 give the coordinates as in the Spitzer catalog. Column 6: 'YSO' means that satisfies the c2d YSO selection criteria (§ 3), otherwise it gives reference to a previous survey. Column 7: 'PMS' means that the ob ject has been spectroscopically confirmed as a Pre-Main Sequence and 'Cnd' means that it is still a candidate. Column 8 gives the SED class from the slope computed from K to 24 µm with the Spitzer data. Column 9 gives other references to the ob ject. References. -- 1) Comeron (2008); 2) Naka jima et al. (2000) ; 3) Comeron et al. (2003); ´ ´ 4) Lopez Mart´ et al. (2005); 5) Allers et al. (2006); 6) Allen et al. (2007); 7) Chapman et al. ´ i (2007); 8) Tachihara et al. (2007); 9) Mer´n et al. (2007); 10) Strauss et al. (1992) 11) Gondoin i (2006); 12) This work

­ 72 ­


­ 73 ­

Table 10. Visual binary ob jects in Lupus
No. Ob ject Id. Separation (") In Lupus I 6 6.5 6.5 8.4 8.5 2.5 6.6 6.1 6.2 In Lupus I I I 12 2.2 2.9 5.0 3.2 3.0 2.2 2.7 6.0 4.0 2.5 1.5 3.8 3.8 4.0 2.2 5.2 4.5 5.0 3.0 2.8 5.0 2.0 2.4 2.4 3.4 Notes

1 4 5 7 15 16 17

SSTc2d J153803.1-331358 Sz 65 Sz 66 AKC2006-18 Sz 68 Sz 69 SSTc2d J154518.5-342125

with with NW E from SW NE SW,

Sz 66 Sz 65

Reipurth & Zinnecker (1993)

only in Z

1 1 2 2 2 2 3 3 3 4 4 5 5 6 6 6 6 7 7 7 7 7 8

8 9 0 2 6 8 0 1 5 3 4 3 9 0 1 2 6 0 2 3 7 8 1

SSTc2d J160703.9-391112 SSTc2d J160708.6-391407 SSTc2d J160708.6-394723 Sz 91 Lup713 Sz 95 2MASS J16075475-3915446 SSTc2d J160755.3-390718 SSTc2d J160803.0-385229 Sz 100 Lup607 HR 5999 Sz 108 Sz 108B IRAC J16084679-3902074 2MASS J16084747-3905087 Par-Lup3-4 2MASS J16085373-3914367 2MASS J16085529-3848481 Sz 112 NTO2000-0537.4-5653 2MASS J16085953-3856275 NTO2000-0540.9-5757 Lup710

86

SE SE, merged in MIPS SE SE N, merged in MIPS NW, faint SE, faint NE, IRAC eliptical E SW E from Ghez et al. (1997) with Sz108B with Sz108 SE E SE SE SW, separated in IRAC SW, merged in IRAC and MIPS SE, faint N SW NE NW W


­ 74 ­

Table 10--Continued
No. 89 95 Ob ject Id. NTO2000-0601.7-5616 NTO2000-614.0-5414 Separation (") 7.0 0.8 1.5 2.3 1.5 2.2 2.0 1.9 3.0 3.0 2.7 3.9 1.7 10.0 10.0 4.0 2.7 1.7 4.2 Lupus IV 4.0 6.0 9.0 2.8 3.9 3.7 6.8 2.3 2.6 3.6 Notes N, from IRAC images N SE NW complex shape SW E SE, faint SW S, not merged in IRAC S, very faint S merged not merged NE, not merged W S, faint E, faint NW W SE SW W, merged NE, not merged SW, faint NE NW, faint SE, merged E

101 105 106 111 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 2 2 3 3 3 3 4 4 4 4 4 3 4 1 2 0 1 3 4 1 3 4 5 7

Sz 116 Lup810s Lup818s SSTc2d J161013.1-384617 SSTc2d J161 SSTc2d J161 Sz 123 SSTc2d J161 SST-Lup3-1 SSTc2d J161 SSTc2d J161 SSTc2d J161 SSTc2d J161 SST SST SST SST c c c c 2 2 2 2 d d d d J J J J 1 1 1 1 5 6 6 6 5 0 0 0 018.6-383613 019.8-383607 118.7-385824 2 2 2 3 9 0 0 0 0 1 1 4 4 0 0 2 0 1 8 4 5 0 2 6 .1 .2 .5 .1 .3 .6 .4 .1 3 3 3 3 4 4 4 4 8 8 9 7 1 2 2 1 5 3 3 3 5 2 2 5 5 2 4 6 4 1 2 3 57 20 18 46 In 57 58 16 56

148 154 157 159

Sz 130 SSTc2d J160129.7-420804 IRAS 15589-4132 Sz 133


Table 11. SED analysis results for the Class II and III ob jects in Lupus
No. Ob ject Id. SpT Ref. AV (mag) L (L ) L
disk

/L



turn-off (µm)

e

xcess

YSOc

PMS

Bin.

SED type

1 3 4 5 6 7 9 1 1 1 1 1 2 2 2 2 2 2 2 2 2 2 3 3 3

2 4 5 6 7 0 1 2 3 4 5 6 7 8 9 1 2 3

SSTc2d J153 AKC2006-17 Sz 65 Sz 66 Sz 67 AKC2006-18 SSTc2d J154 AKC2006-19 SSTc2d J154 Sz 68 Sz 69 SSTc2d J154 SSTc2d Sz 90 Sz 91 Lup 605 Sz 92 Lup 654 Lup 713 Sz 94 Sz 95 SSTc2d SSTc2d Lup 714 Lup 604

803.1-331358

240.3-341343 508.9-341734

518.5-342125

M5 L2 M0 M3 M4 M9 K6 M7.5 K0 K2 M1 M9 K4 K8 M0.5 M6.5 K0 L1 M6 M4 M1.5 M2 M4 M5 M5.5

6 3 4 4 4 3 6 3 6 4 4 6 6 4 4 2 6 2 2 4 4 6 6 2 2

3.0 0.0 1.0 2.0 0.0 1.0 9.0 0.0 10.0 1.5 4.0 2.0 1.0 3.0 1.0 1.0 1.0 0.0 0.0 0.0 1.0 5.0 10.0 1.0 1.0

J160708.6-394723

J160754.1-392046 J160755.3-390718 s

Lupus I 1.192 0.424 0.00046 0.288 0.849 1.190 0.311 2.653 0.278 0.167 0.004 0.323 2.163 0.039 0.018 0.101 1.049 0.111 4.824 0.137 0.375 0.166 0.096 0.138 Lupus I I I 0.300 0.261 1.538 0.017 0.206 0.510 0.014 0.016 0.478 0.060 0.002 0.151 0.023 0.358 0.103 0.369 0.289 0.129 4.834 -0.188 3.591 0.508 0.052 0.227 0.056 0.716

8 2 3 3 8 4 8 5 2 1 2 4

.0 .2 .6 .6 .0 .5 .0 .8 .2 .6 .2 .5

-2.2 -1.8 -1.0 -0.8 -0.8 -1.4 -1.9 0.6 -0.7 -1.5 -1.0 -1.0 -1.3 -1.3 0.7 ... -2.5 ... -1.1 ... -1.0 ... -2.1 ... -1.0

YSO (5) YSO YSO (1) (5) YSO YSO YSO (1) YSO YSO (7) YSO YSO (4) (1) (4) YSO (1) YSO YSO YSO (4) YSO

c c c

c c c c c

Cnd Cnd PMS PMS PMS Cnd Cnd Cnd Cnd PMS PMS Cnd Cnd PMS PMS Cnd PMS Cnd PMS PMS PMS Cnd Cnd Cnd PMS

Y N Y Y N Y N N N Y Y Y Y N Y N N N Y N Y N Y N N

L L T T E L L L LU T L T L L LU E L E T E L E L E T

­ 75 ­

1.6 5.8 8.0 8.0 2.2 8.0 3.6 8.0 4.5 24.0 5.8 8.0 3.6

c c

c c c c c


Table 11--Continued
No. Ob ject Id. SpT Ref. AV (mag) 6.0 4.0 7.0 0.0 1.0 1.0 1.0 0.0 0.0 1.0 2.0 10.0 2.0 1.0 1.0 0.0 0.0 0.0 0.0 0.0 0.0 1.0 0.0 4.0 1.0 0.0 0.0 L (L ) 0.010 0.450 3.092 0.556 0.005 0.064 0.219 0.555 0.058 0.226 0.038 0.014 0.993 0.154 3.026 0.123 48.288 75.295 0.158 0.005 0.055 0.188 0.624 0.356 0.197 0.038 0.041 L
disk

/L



turn-off (µm) 3.6 24.0 4.5 2.2 1.6 8.0 4.5 1.6 4.5 3.6 5.8 2.2 8.0 3.6 2.2 4.5 0.9 24.0 8.0 2.2 0.9 8.0 24.0 8.0 8.0 8.0 0.7

e

xcess

YSOc

PMS

Bin.

SED type T L L T H E L H L T T L L T L H T E E H H L E L E E H

3 3 3 3 3 3 4 4 4 4 4 4 4 4 5 5 5 5 5 5 5 5 5 6 6 6 6

4 5 6 7 8 9 0 1 2 3 4 5 6 9 0 1 3 4 5 6 7 8 9 0 3 4 5

2MASS J16080175-3912316 SSTc2d J160803.0-385229 2MASS J16080618-3912225 Sz 96 2MASS J16081497-3857145 Par-Lup3-1 Sz 97 Sz 98 Sz 99 Sz 100 Lup 607 NTO2000-0526.9-5630 Sz 101 Sz 103 SSTc2d J160830.7-382827 Sz 104 HR 5999 HR 6000 Par-Lup3-2 Lup 706 Sz 106 Sz 107 Sz 108 Sz 108B Sz 109 Lup 617 Par-Lup3-3

K6 M1 K7 M1.5 M4.7 M7.5 M3 M0 M3.3 M5 M5 G8 M4 M4 K1 M5 A7 A3 M6 L0 M0 M5.5 M1 M6 M5.5 M6 M4.5

6 6 6 4 4 4 4 4 4 4 2 6 4 4 6 4 4 4 4 2 4 4 4 6 4 2 4

0 0 0 0 1 0 0 2 1 0 0 0 0 0 0 0 0 0 0 0 2 0 0 0 0 0 5

.2 .1 .3 .4 .8 .1 .2 .2 .0 .5 .0 .0 .0 .5 .2 .2 .7 .0 .0 .2 .7 .1 .2 .0 .0 .0 .8

0 7 6 1 0 2 0 1 5 1 0 8 3 6 1 8 0 0 6 6 7 2 2 0 0 4 4

8 3 0 6 6 3 8 4 6 1 3 2 1 5 5 5 4 1 7 7 5 0 4 1 1 4 3

-0.4 ... -1.7 -0.9 -0.6 ... -0.9 -1.2 -0.9 -0.5 0.1 -2.8 -1.3 -0.2 -0.2 0.1 -1.1 ... ... -1.3 -0.5 -0.9 ... -0.3 ... ... -0.2

(2) YSO YSO YSO YSO (1) YSO YSO YSO YSO (3) (6) YSO YSO (7) YSO (1) (1) (3) (4) YSO YSO (1) YSO (1) (3) YSO

c c c c c c c c

c c c

c c c

c

Cnd Cnd Cnd PMS PMS PMS PMS PMS PMS PMS Cnd Cnd PMS PMS Cnd PMS PMS PMS PMS PMS PMS PMS PMS Cnd PMS Cnd PMS

N Y N N N N N N N Y Y N N N N N Y N N N N N Y Y N N N

­ 76 ­


Table 11--Continued
No. Ob ject Id. SpT Ref. AV (mag) 0.0 0.0 2.0 3.0 8.0 0.0 3.0 1.0 2.0 4.0 0.0 0.0 2.0 5.0 1.0 13.0 1.0 2.0 3.0 6.0 6.0 5.0 4.0 0.0 1.0 6.0 2.0 L (L ) 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 6 0 0 0 0 0 0 .0 .2 .2 .0 .0 .3 .0 .2 .0 .0 .0 .0 .7 .0 .1 .0 .0 .0 .1 .0 .0 .0 .0 .2 .3 .8 .0 0 1 0 0 4 4 8 2 8 0 1 7 1 1 6 4 5 3 3 0 8 0 0 2 0 8 0 3 0 6 4 5 8 8 2 7 2 3 1 9 0 7 7 9 8 9 5 2 4 4 7 3 1 5 L
disk

/L



turn-off (µm) 1.2 2.2 2.2 5.8 4.5 4.8 4.5 4.5 3.6 8.0 0.9 0.9 4.5 8.0 8.0 2.2 8.0 8.0 2.2 5.8 24.0 5.8 4.5 24.0 3.6 0.9 24.0

e

xcess

YSOc

PMS

Bin.

SED type H T T L L LU T L T E T T T E L E E E T E L E L L T T E

6 6 6 6 7 7 7 7 7 7 7 7 8 8 8 8 8 8 9 9 9 9 1 1 1 1 1

6 7 8 9 0 1 2 3 4 7 8 9 0 1 2 3 4 6 1 2 3 5 0 0 0 0 0

0 1 2 3 4

Par-Lup3-4 Sz 110 2MASS J16085324-391440 NTO2000-0532.1-5616 2MASS J16085373-391436 Sz 111 2MASS J16085529-384848 Sz 112 Sz 113 NTO2000-0537.4-5653 2MASS J16085953-385627 SSTc2d J160901.4-392512 Sz 114 NTO2000-0540.9-5757 Sz 115 NTO2000-0546.4-5934 Lup 608s Lup 710 SSTc2d J160927.0-383628 NTO2000-0605.6-5437 SSTc2d J160934.1-391342 NTO2000-0614.0-5414 NTO2000-0619.6-5414 Sz 116 Sz 117 Sz 118 Lup 650

1 7 1

5

M5 M2 M1 K5 M5.5 M1.5 M2 M4 M4 K7 M8 M3 M4 K2 M4 K7 M5 M5 K7 G9 M4 K0 G9 M1.5 M2 K6 M4

4 4 6 6 4 4 6 4 4 6 4 6 4 6 4 6 2 2 6 2 6 6 6 4 4 4 2

6 0 0 0 0 0 0 0 0 0 0 1 0 0 0 0 0 0 0 0 0 0 0 0 0 1 0

.2 .5 .7 .1 .2 .5 .4 .3 .3 .4 .2 .4 .1 .0 .2 .2 .3 .0 .3 .0 .4 .0 .0 .3 .5 .1 .2

6 6 3 6 2 2 6 1 9 5 4 3 4 1 1 5 5 0 7 7 2 7 5 7 5 4 6

2 5 2 7 2 4 9 7 0 7 1 1 3 8 6 7 1 1 1 8 2 5 4 7 0 6 0

0.3 -0.5 -0.8 -0.5 -1.1 0.6 -1.2 -1.7 -0.4 ... -0.8 -0.8 -0.6 -0.9 -1.2 -2.6 ... ... -0.4 ... ... ... -1.4 ... -0.8 -1.0 ...

YSO YSO YSO (6) YSO (1) YSO YSO YSO (2) YSO YSO YSO (2) YSO (2) (4) (4) (7) (2) YSO (2) (2) (1) YSO YSO (4)

c c c c c c c c c c c

c

c c

PMS PMS Cnd Cnd PMS PMS Cnd PMS PMS Cnd PMS Cnd PMS Cnd PMS Cnd Cnd Cnd Cnd Cnd Cnd Cnd Cnd PMS PMS PMS Cnd

Y N N N Y N Y N N Y Y N N Y N N N Y N N N Y N Y N N N

­ 77 ­


Table 11--Continued
No. Ob ject Id. SpT Ref. AV (mag) 1.0 1.0 1.0 12.0 7.0 1.0 0.0 2.0 2.0 1.0 6.0 5.0 6.0 0.0 0.0 3.0 6.0 2.0 4.0 3.0 1.0 1.0 0.0 0.0 2.0 6.0 4.0 L (L ) 0.054 0.089 0.501 47.066 0.774 0.453 0.232 0.071 0.049 0.087 12.788 7.277 1.413 0.007 0.124 16.142 16.114 0.103 0.133 0.109 0.030 0.025 0.462 0.040 3.247 0.598 3.474 L
disk

/L



turn-off (µm) 8.0 24.0 24.0 8.0 4.5 24.0 24.0 5.8 4.5 5.8 24.0 8.0 8.0 1.2 24.0 8.0 5.8 4.5 8.0 8.0 1.6 8.0 24.0 2.2 5.8 3.6 24.0

e

xcess

YSOc

PMS

Bin.

SED type E T E L L E E L L T E L L H T L L L E L T E E T L T L

1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1

0 0 0 0 0 1 1 1 1 1 1 1 1 2 2 2 2 2 2 2 2 2 2 3 3 3 3

5 6 7 8 9 0 2 3 4 6 7 8 9 0 1 2 3 4 5 6 7 8 9 0 1 3 5

Lup 810s Lup 818s Sz 119 SSTc2d J161000.1-385401 2MASS J16100133-3906449 Sz 121 Sz 122 SSTc2d J161018.6-383613 SSTc2d J161019.8-383607 SSTc2d J161029.6-392215 IRAS 16072-3738 SSTc2d J161034.5-381450 SSTc2d J161035.0-390655 SSTc2d J161045.4-385455 Sz 123 SSTc2d J161118.7-385824 SSTc2d J161126.0-391123 SSTc2d J161131.9-381110 Lup 831s SSTc2d J161144.9-383245 SSTc2d J161148.7-381758 Lup 802s Sz 124 SST-Lup3-1 SSTc2d J161200.1-385557 SSTc2d J161211.2-383220 SSTc2d J161219.6-383742

M5 M6 M4 A0 G0 M3 M2 M1 M4 M4 M5 M4 M5 K9 M3 M8 K5 K9 K7 M3 K4 M4 M0 M5.5 M2 K7 M5

2 2 4 6 6 4 4 6 6 6 6 6 6 6 4 6 6 6 6 6 6 2 4 5 6 6 6

0.270 0.001 0.038 0.4784 0.117 0.436 0.193 0.085 0.219 0.472 0.149 0.590 0.469 1.555 0.516 0.556 0.050 0.440 0.424 0.043 0.617 0.361 0.062 0.894 0.337 0.222 0.363

... ... ... -1.9 -1.1 ... ... -0.8 -1.0 -0.1 ... -2.4 -2.5 -1.0 ... -2.1 -2.2 -2.1 ... -1.6 -0.6 ... ... -0.8 -2.3 -0.1 ...

(4) YSO (1) YSO YSO (1) (1) YSO YSO YSO YSO YSO YSO YSO YSO YSO YSO YSO (4) YSO YSO (4) (1) YSO YSO YSO YSO

c c c

c c c c c c c c c c c c c

c c c c

Cnd Cnd PMS Cnd Cnd PMS PMS Cnd Cnd Cnd Cnd Cnd Cnd Cnd PMS Cnd Cnd Cnd Cnd Cnd Cnd Cnd PMS PMS Cnd Cnd Cnd

Y Y N N N N N Y Y N N N N N Y Y N N N N N N N Y Y Y N

­ 78 ­


Table 11--Continued
No. Ob ject Id. SpT Ref. AV (mag) 6 0 1 3 5 2 0 2 1 2 6 3 0 2 0 0 3 4 3 6 6 4 .0 .0 .0 .0 .0 .0 .0 .0 .0 .0 .0 .0 .0 .0 .0 .0 .0 .0 .0 .0 .0 .0 L (L ) L
disk

/L



turn-off (µm) 2.2 1.2 8.0 8.0 24.0 2.2 2 1 2 1 5 5 2 2 4 1 5 8 8 3 8 1 .2 .2 .2 .6 .8 .8 .2 .2 .5 .6 .8 .0 .0 .6 .0 .2

e

xcess

YSOc

PMS

Bin.

SED type L T L L L L L T L T L L T L L T L L L L L H

1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1

3 3 3 3 4 4 4 4 4 4 4 4 4 4 5 5 5 5 5 5 5 5

6 7 8 9 0 1 2 3 4 5 6 7 8 9 0 1 2 4 5 6 8 9

SST SST SST SST SST SST

c c c c c c

2 2 2 2 2 2

d d d d d d

J J J J J J

1 1 1 1 1 1

6 6 6 6 6 6

1 1 1 1 1 1

2 2 2 2 3 3

2 4 5 5 4 4

2 3 1 6 1 4

.7 .8 .7 .0 .0 .1

-

3 3 3 3 3 3 4 4 4 4

7 8 8 7 8 7 2 1 2 2

1 1 4 5 3 3 3 5 2 2

3 5 2 6 7 6 5 4 1 2

28 03 16 43 24 46 07 57 58 16

G8 K0 M8 K6 K1 K9 M2 M0 M2 K7 M9 M1 M1.5 M8 K0 M2 M1 K6 M2 K7 M0 K2

6 6 6 6 6 6 6 6 6 6 6 6 4 6 6 4 6 6 6 6 6 1

SSTc2d J155925.2 SSTc2d J155945.3 SSTc2d J160000.6 SSTc2d J160002.4 IRAS 15567-4141 SSTc2d J160026.1 Sz 130 SSTc2d J160034.4 F 403 Sz 131 SSTc2d J160111.6 SSTc2d J160129.7 SSTc2d J160143.3 IRAS 15585-4134 SSTc2d J160229.9 Sz 133

-415356 -422540

-413730 -420804 -413606 -415111

2.871 0.126 0.378 0.570 2.263 0.366 12.288 0.132 9.096 0.060 0.067 0.374 Lupus IV 0.019 0.222 0.729 1.336 0.065 0.589 0.122 0.551 5.739 0.317 0.109 0.114 0.140 0.388 1.450 0.813 1.788 0.099 0.054 1.368 0.352 0.377 0.746 0.396 0.589 0.164 10.027 1.002 0.368 0.094 0.110 0.560

-1.8 -1.0 -1.9 -2.3 ... -1.0 -1.4 -1.5 -1.5 -1.3 -2.2 -0.5 -0.8 -2.4 -0.2 -1.0 -2.3 ... -2.2 -2.0 -2.3 -9 9 .

(7) YSO YSO YSO YSO (7) (7) YSO (7) (7) YSO YSO YSO (7) YSO (1) YSO YSO YSO YSO YSO (1)

c c c c

C C C C C C

nd nd nd nd nd nd

N N N N N Y N Y Y N N Y Y N N N N Y N N N Y

c

c c c c c c c c c

Cnd Cnd Cnd Cnd Cnd Cnd PMS Cnd PMS PMS Cnd Cnd Cnd Cnd Cnd PMS

­ 79 ­


Note. -- Columns 3 and 4 give the spectral types and their corresponding references. In cases without a previous reference, the value was calculated with the optical and near-IR photometry (see § 4.2). Column 5 gives the extinction from the best fit of the photometry to the stellar model. Columns 6 and 7 show the stellar and disk fractional luminosities (§ 4.3 and 4.4). Columns 8 and 9 list the 2-dimensional parameters (§ 4.5) and Columns 10, 11 and 12 repeat the information in Tables 9 and 10. References. -- 1) Comeron (2008) 2) Lopez Mart´ et al. (2005) 3) Allers et al. (2006) 4) Allen et al. (2007) 5) Mer´n et al. ´ ´ i i (2007) 6) This work

­ 80 ­


Table 12. Optical and Near-Infrared magnitudes of the Lupus sample
No. Ob ject Id. B 0.44 µm V 0.55 µm Rc 0.64 µm Lupus ± 0.22 .. ± 0.27 ± 0.05 ± 0.00 .. ± 0.04 .. ± 0.32 ± 0.05 ± 0.05 ± 0.05 .. ± 0.05 .. .. ± 0.05 Lupus I ± 0.06 ± 0.76 ± 0.05 ± 0.68 ± 0.27 ± 0.20 .. ± 0.52 ± 0.67 ± 0.05 ± 0.28 ± 0.26 ± 0.11 ± 0.36 ± 0.32 I 11.84 . 21.27 10.76 12.56 11.40 17.12 19.33 14.64 21.72 . 15.28 . . . . . II 16.80 17.86 . 12.49 12.92 16.49 . 17.54 15.68 13.00 12.71 12.26 19.92 15.70 14.74 ± .. ± ± ± ± ± ± ± ± .. ± .. .. .. .. .. ± ± .. ± ± ± .. ± ± ± ± ± ± ± ± 0.00 0. 0. 0. 0. 0. 0. 0. 0. 59 00 00 00 03 08 01 25 10.98 . 19.14 10.48 11.66 11.34 16.00 18.42 13.20 20.86 . . . . . . . ± .. ± ± ± ± ± ± ± ± .. .. .. .. .. .. .. 0.00 0. 0. 0. 0. 0. 0. 0. 0. 13 00 00 00 03 07 01 23 9.03 ± 14.68 ± 17.19 ± 9.19 ± 10.89 ± 10.00 ± 14.67 ± 15.99 ± 10.72 ± ... 16.58 ± 12.98 ± 15.56 ± 12.20 ± 7.57 ± 11.18 ± 11.64 ± 14.68 15.22 11.51 10.35 11.06 14.21 11.27 15.75 13.24 11.45 11.01 9.45 17.20 10.32 12.57 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 0.02 0.05 0.03 0.04 0.03 0.02 0.03 0.10 0.02 0.12 0.02 0.07 0.03 0.02 0.03 0.03 0.04 0.05 0.02 0.02 0.02 0.03 0.02 0.23 0.03 0.02 0.02 0.02 0.22 0.02 0.02 7.93 13.56 16.27 8.41 9.88 9.36 14.02 14.59 9.05 . 15.59 12.41 13.52 10.64 6.86 10.16 10.95 13.77 13.13 10.65 9.32 10.12 13.57 10.57 14.88 12.57 10.80 10.28 8.41 16.12 8.56 11.92 ± ± ± ± ± ± ± ± ± .. ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 0.02 0.05 0.03 0.04 0.03 0.02 0.03 0.10 0.02 0.12 0.02 0.07 0.03 0.02 0.03 0.03 0.04 0.05 0.02 0.02 0.02 0.03 0.02 0.23 0.03 0.02 0.02 0.02 0.22 0.02 0.02 7.47 12.51 15.69 7.98 9.29 9.12 13.56 13.56 8.32 . 14.62 12.13 12.10 9.71 6.48 9.41 10.48 13.11 11.56 10.11 8.72 9.85 13.20 10.41 14.60 12.13 10.56 10.01 7.91 14.46 7.61 11.59 ± ± ± ± ± ± ± ± ± .. ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 0.02 0.05 0.03 0.04 0.03 0.02 0.03 0.10 0.02 0.12 0.02 0.07 0.03 0.02 0.03 0.03 0.05 0.02 0.02 0.02 0.02 0.04 0.02 0.27 0.03 0.02 0.02 0.03 0.08 0.03 0.02 Ic 0.79 µm Z 0.96 µm J 1.23 µm H 1.66 µm Ks 2.16 µm

1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 31 32

SSTc2dJ153803.1IRAS15356-3430 AKC2006-17 Sz65 Sz66 Sz67 AKC2006-18 SSTc2dJ154214.6SSTc2dJ154240.3IRAS15398-3359 SSTc2dJ154302.3AKC2006-19 SSTc2dJ154506.3SSTc2dJ154508.9Sz68 Sz69 SSTc2dJ154518.5-

331358

341026 341343 344406 341738 341734

342125

17.76 . . 13.11 . . . . 19.74 . 18.76 18.38 . . 11.53 17.41 17.95 . 85 38 28 25 . . 95 38 31 39 15 . . 34

± .. .. ± .. .. .. .. ± .. ± ± .. .. ± ± ± .. ± ± ± ± .. .. ± ± ± ± ± .. .. ±

0.05

0.05

0.05 0.05 0.05

0.05 0.06 0.05

16.44 . . 12.13 . . . . . . . 17.74 . . 10.35 16.25 . . . 04 70 58 . 98 . . 00 57 32 . . .

± .. .. ± .. .. .. .. .. .. .. ± .. .. ± ± .. .. .. ± ± ± .. ± .. .. ± ± ± .. .. ..

0.05

0.05

0.05

0.05 0.06

14.24 . 23.86 11.33 14.51 . 19.45 . 18.17 18.38 18.35 17.29 . 18.73 . . 17.35 18.79 18.67 13.50 13.70 14.11 18.84 . 18.25 17.12 14.76 14.25 14.58 21.91 19.39 16.58

0.05

­ 81 ­

SSTc2dJ160703.9-391112 SSTc2dJ160708.6-391407 SSTc2dJ160708.6-394723 Sz90 Sz91 Lup605 Sz92 Lup654 Lup713 Sz94 Sz95 SSTc2dJ160754.1-392046 2MASSJ16075475-3915446 SSTc2dJ160755.3-390718 Lup714

17. 15. 15. 16.

0. 0. 0. 0.

05 05 05 05

0.02 0.04 0.00 0.00 0.02 0. 0. 0. 0. 0. 0. 0. 0. 04 02 00 00 00 11 02 01

14. 13. 14. 12.

0.05 0.05 0.05 0.05

17. 18. 16. 16. 17.

0. 0. 0. 0. 0.

05 05 05 05 05

16. 14. 15.

0.05 0.05 0.05

17.

0.05

16.16 ± 17.05 ± ... 11.80 ± 12.39 ± 15.67 ± ... 17.13 ± 14.82 ± 12.49 ± 12.33 ± 11.09 ± 18.76 ± 13.60 ± 14.06 ±

0.02 0.04 0.00 0.01 0.02 0. 0. 0. 0. 0. 0. 0. 0. 04 01 01 01 00 08 01 01


Table 12--Continued
No. Ob ject Id. B 0.44 µm 16.94 ± ... 15.78 ± ... 14.80 ± ... 17.74 ± 16.18 ± 14.99 ± 15.49 ± 16.62 ± 17.45 ± ... ... 16.26 ± ... ... 11.89 ± ... ... 7.38 ± 6.55 ± 16.88 ± ... ... 17.31 ± 14.68 ± ... ... ... 18.23 ± 17.27 ± 16.76 ± ... 0.05 0.05 0.05 0. 0. 0. 0. 0. 0. 05 05 05 05 05 05 V 0.55 µm 17.01 . 13.52 . 13.43 . . 14.61 13.66 16.00 15.43 . . . 15.91 . 11.14 11.15 15.25 . 7.10 6.62 15.49 . . 16.06 11.78 . . . 16.43 17.41 . . ± .. ± .. ± .. .. ± ± ± ± .. .. .. ± .. ± ± ± .. ± ± ± .. .. ± ± .. .. .. ± ± .. .. 0.05 0.05 0.05 Rc 0.64 µm 16.72 19.69 13.88 18.00 13.69 18.93 18.15 14.67 11.70 15.39 14.97 17.76 24.17 14.00 15.38 22.46 15.18 10.67 13.96 21.60 6.92 6.66 15.02 20.70 15.00 15.42 11.72 17.71 22.28 20.93 15.71 17.29 15.89 18.97 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 0.23 1.16 0.41 1.12 0.08 0.57 0.19 0.11 0.05 0.35 0.25 0.67 0.33 0.52 0.51 0.14 0.01 0.05 1.68 0.09 0.05 0.05 0.10 0.06 0.98 0.10 0.05 0.02 0.13 0.07 0.19 0.05 0.39 0.59 Ic 0.79 µm 14. 19. 12. 13. 11. 17. 15. 12. 11. 14. 13. 16. 21. 12. 15. 20. 13. 13. 20. 31 37 00 76 83 42 28 92 21 17 12 13 31 35 69 72 15 . 57 74 . . 09 44 66 20 68 39 04 32 57 02 24 18 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± .. ± ± .. .. ± ± ± ± ± ± ± ± ± ± ± ± 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 01 08 00 01 00 03 01 00 00 01 01 02 18 00 02 15 01 Z 0.96 µm 13. 18. 11. 12. 12. 16. 14. 12. 10. 13. 12. 15. 20. 11. 15. 20. 12. 12. 21. 48 29 04 50 33 73 19 38 74 42 32 34 29 65 64 28 53 . 92 06 . . 47 82 28 45 86 30 94 48 72 21 33 88 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± .. ± ± .. .. ± ± ± ± ± ± ± ± ± ± ± ± 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 01 07 00 01 00 04 01 01 00 01 00 02 19 00 02 17 01 J 1.23 µm 12.15 ± 16.40 ± 9.52 ± 10.03 ± 10.13 ± 15.21 ± 12.52 ± 11.24 ± 9.53 ± 11.93 ± 10.98 ± 13.74 ± 17.19 ± 10.40 ± 14.56 ± ... 11.38 ± 8.97 ± 11.66 ± ... 5.91 ± 6.67 ± 11.24 ± 15.17 ± 11.65 ± 11.25 ± 9.79 ± ... ... 16.45 ± 11.40 ± 12.87 ± 11.45 ± 15.46 ± 0.03 0.14 0.02 0.02 0.02 0.05 0.02 0.02 0.02 0.02 0.02 0.09 0.17 0.02 0.04 0.02 0.02 0.02 0.02 0.02 0.03 0.06 0.03 0.03 0.03 H 1.66 µm 11.45 15.06 8.51 8.53 9.35 14.20 11.75 10.55 8.65 11.21 10.35 . 16.14 9.72 13.65 . 10.62 8.39 11.00 . 5.22 6.71 10.73 14.24 10.66 10.62 9.04 . . 15.37 10.82 12.26 10.17 14.26 ± ± ± ± ± ± ± ± ± ± ± .. ± ± ± .. ± ± ± .. ± ± ± ± ± ± ± .. .. ± ± ± ± ± 0.03 0.14 0.02 0.02 0.02 0.05 0.02 0.02 0.02 0.02 0.02 0.08 0.02 0.04 0.02 0.02 0.02 0.02 0.02 0.03 0.06 0.03 0.03 0.03 Ks 2.16 µm 11.07 14.25 8.10 7.67 8.96 13.13 11.25 10.22 8.01 10.74 9.91 12.44 15.35 9.39 12.58 . 10.23 8.22 10.65 . 4.39 6.67 10.34 13.83 10.15 10.31 8.84 . . 14.83 10.50 11.97 9.55 13.30 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± .. ± ± ± .. ± ± ± ± ± ± ± .. .. ± ± ± ± ± 0.02 0.09 0.03 0.02 0.02 0.03 0.02 0.02 0.02 0.02 0.02 0.11 0.07 0.02 0.03 0.02 0.03 0.02 0.04 0.02 0.02 0.04 0.02 0.02 0.03

33 34 35 36 37 38 39 40 41 42 43 44 45 46 47 48 49 50 51 52 53 54 55 56 57 58 59 60 61 62 63 64 65 66

Lup604s 2MASSJ16080175-3912316 SSTc2dJ160803.0-385229 2MASSJ16080618-3912225 Sz96 2MASSJ16081497-3857145 Par-Lup3-1 Sz97 Sz98 Sz99 Sz100 Lup607 NTO2000-0526.9-5630 Sz101 Sz102 IRACJ16083010-3922592 Sz103 SSTc2dJ160830.7-382827 Sz104 IRACJ16083110-3856000 HR5999 HR6000 Par-Lup3-2 Lup706 Sz106 Sz107 Sz108 Sz108B IRACJ16084679-3902074 2MASSJ16084747-3905087 Sz109 Lup617 Par-Lup3-3 Par-Lup3-4

0. 0. 0. 0.

05 05 05 05

­ 82 ­

0.05

0.05 0.05 0.05 0.05 0.05 0.05 0.05

0.05

0.01 0.17

0.01 0.26

0.05 0.05 0.05

0.05 0.01

0.05 0.05

0.05 0.05 0.05

0.05 0.05

13. 18. 14. 13. 11. 14. 21. 19. 13. 15. 14. 18.

0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0.

00 05 01 01 00 01 18 08 01 01 01 05

12. 16. 14. 12. 10. 13. 20. 18. 12. 14. 13. 17.

0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0.

01 03 01 01 00 01 25 07 01 01 01 06

0. 0. 0. 0. 0.

14 02 03 03 06

0. 0. 0. 0. 0.

14 02 03 03 06

0.11 0.02 0.02 0.02 0.04


Table 12--Continued
No. Ob ject Id. B 0.44 µm 15.27 ± 17.53 ± ... ... 15.34 ± 17.36 ± 16.62 ± 17.46 ± ... ... ... ... 16.92 ± 15.33 ± ... 16.88 ± ... 18.00 ± ... 17.66 ± ... ... ... ... 17.55 ± ... 18.32 ± ... ... ... ... ... ... ... 0.05 0.05 V 0.55 µm 14.58 ± 16.35 ± ... ... 13.98 ± ... 15.39 ± 16.50 ± ... ... ... ... 15.31 ± 14.12 ± ... 15.48 ± ... 16.60 ± ... ... ... ... ... ... ... ... 16.44 ± ... ... ... ... ... ... ... 0.05 0.05 Rc 0.64 µm 13. 15. 19. 21. 13. 17. 14. 16. 72 35 19 73 29 24 78 64 . . 76 25 04 35 53 09 . 43 . 76 . . . . 31 03 42 . 23 . . . . 73 ± ± ± ± ± ± ± ± .. .. ± ± ± ± ± ± .. ± .. ± .. .. .. .. ± ± ± .. ± .. .. .. .. ± 0. 0. 0. 0. 0. 0. 0. 0. 05 09 51 10 05 23 15 11 Ic 0.79 µm 12. 13. 18. 18. 15. 12. 14. 28 52 39 76 . 24 93 65 . . 79 91 48 54 60 12 65 16 . 67 . . . . 74 48 24 . 64 . . . . 12 ± ± ± ± .. ± ± ± .. .. ± ± ± ± ± ± ± ± .. ± .. .. .. .. ± ± ± .. ± .. .. .. .. ± 0. 0. 0. 0. 00 01 05 06 Z 0.96 µm 12. 12. 17. 17. 14. 12. 13. 09 93 94 39 . 44 26 83 . . 92 70 37 72 96 57 85 42 . 92 . . . . 05 03 80 . 04 . . . . 49 ± ± ± ± .. ± ± ± .. .. ± ± ± ± ± ± ± ± .. ± .. .. .. .. ± ± ± .. ± .. .. .. .. ± 0. 0. 0. 0. 00 01 06 04 J 1.23 µm 10.97 ± 11.33 ± 16.62 ± 14.97 ± 10.62 ± 12.98 ± 11.00 ± 12.46 ± < 17. < 17. < 17. 13.90 ± 11.61 ± 10.41 ± 16.17 ± 11.33 ± 16.58 ± 12.20 ± < 17. 13.55 ± ... < 18. < 16. 18.57 ± 12.55 ± 17.29 ± 8.68 ± ... 17.30 ± ... < 17. < 18. < 17. 17.09 ± 0. 0. 0. 0. 0. 0. 0. 0. 39 53 02 0. 0. 0. 0. 0. 0. 0. 79 0. 02 03 12 07 02 03 02 02 H 1.66 µm 10.22 ± 10.28 ± 15.49 ± 13.44 ± 9.80 ± 12.39 ± 10.29 ± 11.73 ± 16.51 ± < 16. 15.65 ± 13.29 ± 10.68 ± 9.70 ± 15.22 ± 10.65 ± 14.24 ± 11.64 ± < 16. 13.04 ± ... < 16. 15.23 ± 17.57 ± 11.69 ± 16.56 ± 7.33 ± ... 16.54 ± 18.41 ± 15.57 ± 14.16 ± < 15. 16.40 ± 0.02 0.03 0.12 0.07 0.02 0.03 0.02 0.02 0.17 62 0.00 0.03 0.02 0.03 0.08 0.03 0.13 0.03 44 0.03 02 0.00 0.13 0.03 0.10 0.02 0. 0. 0. 0. 67 0. 10 40 00 00 09 Ks 2.16 µm 9.75 9.80 14.90 12.52 9.54 12.02 9.96 11.26 12.56 15.15 15.27 12.83 10.29 9.32 14.86 10.45 12.94 11.36 15.16 12.66 0.00 14.90 13.12 15.33 10.95 15.67 6.67 . 15.75 15.38 14.87 11.21 13.38 15.73 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± .. ± ± ± ± ± ± 0.02 0.02 0.11 0.04 0.02 0.02 0.02 0.02 0.03 0.13 0.16 0.03 0.02 0.02 0.11 0.03 0.04 0.03 0.15 0.03 0.00 0.11 0.03 0.08 0.02 0.08 0.02 0. 0. 0. 0. 0. 0. 09 10 11 02 04 08

67 68 69 70 71 72 73 74 75 76 77 78 79 80 81 82 83 84 85 86 87 88 89 90 91 92 93 94 95 96 97 98 99 100

Sz110 2MASSJ16085324-3914401 NTO2000-0532.1-5616 2MASSJ16085373-3914367 Sz111 2MASSJ16085529-3848481 Sz112 Sz113 NTO2000-0536.7-5943 NTO2000-0536.7-5956 NTO2000-0537.4-5653 2MASSJ16085953-3856275 SSTc2dJ160901.4-392512 Sz114 NTO2000-0540.9-5757 Sz115 NTO2000-0546.4-5934 Lup608s NTO2000-0554.9-5651 Lup710 Lupus3MMS NTO2000-0558.8-5610 NTO2000-0601.7-5616 NTO2000-0605.1-5606 SSTc2dJ160927.0-383628 NTO2000-0605.6-5437 SSTc2dJ160934.1-391342 IRACJ16093418-3915127 NTO2000-0614.0-5414 NTO2000-0615.6-5616 NTO2000-0615.6-5953 NTO2000-0615.8-5734 NTO2000-0617.7-5641 NTO2000-0619.6-5414

0. 0. 0. 0.

05 05 05 05

0.05 0.05 0.05

0.01 0.00 0.01

0.01 0.01 0.01

0.05 0.05 0.05 0.05 0.05

0.05 0.05 0.05 0.05

21. 19. 15. 14. 19. 15. 16. 17.

0. 0. 0. 0. 0. 0.

10 58 20 39 54 09

0.16 0.26

19. 16. 13. 12. 18. 13. 21. 14. 15.

0. 0. 0. 0. 0. 0. 0. 0.

10 02 01 00 06 01 24 01

18. 15. 13. 11. 17. 12. 19. 13. 14.

0. 0. 0. 0. 0. 0. 0. 0.

10 02 01 00 06 01 14 01

03 02 03 08 03 13 03 03

­ 83 ­

0.02

0.01

0.05 0.05

0.05

16. 21. 15. 21.

0.14 0.07 0.18 0.08

14. 19. 12. 19.

0.01 0.09 0.00 0.09

14. 19. 10. 19.

0.01 0.10 0.00 0.10

21 92 0.27 0.03 0.11 0.02 0.12 59 30 69 0.09

19.

0.71

19.

0.08

18.

0.08


Table 12--Continued
No. Ob ject Id. B 0.44 µm 14.79 ± 0. 15.84 ± 0. 18.32 ± 0. ... 16.61 ± 0. 17.37 ± 0. 15.35 ± 0. ... 18.38 ± 0. 15.70 ± 0. ... 15.33 ± 0. 18.37 ± 0. 17.39 ± 0. ... 17.51 ± 0. 18.38 ± 0. 17.49 ± 0. 18.20 ± 0. 17.51 ± 0. 15.89 ± 0. 17.68 ± 0. 18.18 ± 0. 18.76 ± 0. 18.00 ± 0. 17.49 ± 0. 17.04 ± 0. 17.54 ± 0. 14.44 ± 0. 18.17 ± 0. 18.29 ± 0. ... 18.03 ± 0. ... 05 05 05 05 05 05 05 05 05 05 05 05 05 05 05 05 05 05 05 05 05 05 05 05 05 05 05 05 V 0.55 µm 13.23 ± 0. 14.59 ± 0. 16.90 ± 0. ... 16.38 ± 0. ... 13.71 ± 0. ... 17.42 ± 0. 14.06 ± 0. ... 13.73 ± 0. 16.63 ± 0. ... ... 16.31 ± 0. 17.15 ± 0. 15.72 ± 0. ... ... 14.48 ± 0. 15.53 ± 0. 17.52 ± 0. ... ... ... 15.64 ± 0. 17.31 ± 0. 13.04 ± 0. 16.55 ± 0. 15.88 ± 0. ... ... ... 05 05 05 05 05 05 05 05 05 Rc 0.64 µm 13.05 14.20 16.61 19.85 16.16 16.49 13.49 17.41 17.90 13.88 19.15 13.28 16.67 16.76 21.73 15.79 15.07 14.38 17.22 17.13 14.44 13.97 16.09 15.90 17.21 17.12 15.72 17.15 12.33 16.24 14.94 19.17 17.25 18.58 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 0. 0. 0. 0. 0. 1. 0. 0. 0. 0. 0. 0. 0. 1. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 05 16 05 04 51 11 61 11 11 13 24 05 18 26 10 05 21 18 07 13 17 05 25 34 18 10 09 05 05 05 05 65 30 10 Ic 0.79 µm 12. 12. 15. 17. 15. 15. 12. 13. 15. 11. 17. 12. 14. 15. 19. 13. 11. 11. 13. 16. 12. 12. 14. 15. 14. 14. 15. 11. 14. 11. 18. 14. 16. 20 38 00 62 20 28 10 55 27 90 42 18 70 57 26 90 70 65 96 05 98 . 43 56 37 73 99 18 41 26 41 68 76 84 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± .. ± ± ± ± ± ± ± ± ± ± ± ± 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 00 00 01 03 01 01 00 01 01 00 03 00 01 01 07 01 00 00 01 02 00 00 01 01 01 01 01 00 01 00 06 01 03 Z 0.96 µm 11. 12. 12. 16. 14. 14. 11. 11. 14. 11. 16. 11. 13. 14. 18. 13. 10. 10. 12. 15. 12. 11. 13. 14. 13. 14. 14. 11. 13. 10. 17. 14. 16. 84 19 98 87 69 38 54 33 10 57 94 97 91 70 31 42 39 51 56 74 49 . 51 97 53 90 84 54 36 60 87 72 13 24 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± .. ± ± ± ± ± ± ± ± ± ± ± ± 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 00 00 01 04 01 01 00 00 01 00 04 00 01 01 07 01 00 00 01 02 01 00 01 01 01 01 01 00 01 00 05 01 02 J 1.23 µm 10.47 10.68 10.45 15.39 12.84 13.01 10.39 9.63 12.20 10.07 15.87 10.87 12.66 13.28 16.59 11.94 8.01 8.01 10.38 14.31 11.09 6.79 8.40 12.28 12.51 12.44 13.71 13.25 10.29 12.20 8.77 16.55 11.84 14.89 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 0.03 0.02 0.03 0.06 0.04 0.03 0.02 0.02 0.03 0.02 0.08 0.03 0.02 0.04 0.12 0.02 0.03 0.02 0.02 0.03 0.02 0.02 0.02 0.03 0.02 0.02 0.03 0.03 0.02 0.02 0.02 0.17 0.02 0.04 H 1.66 µm 9.77 ± 9.85 ± 9.35 ± 14.76 ± 11.68 ± 12.39 ± 9.67 ± 8.49 ± 11.15 ± 9.31 ± 15.03 ± 10.12 ± 12.09 ± < 12. 15.29 ± 11.27 ± 6.87 ± 6.85 ± 8.82 ± 13.40 ± 10.21 ± 5.51 ± 7.14 ± 11.09 ± 11.19 ± 11.82 ± 13.04 ± 12.56 ± 9.63 ± 11.51 ± 7.43 ± 15.38 ± 10.28 ± 13.73 ± 0.03 0.02 0.03 0.06 0.04 0.03 0.02 0.02 0.03 0.02 0.08 0.03 0.02 65 0.12 0.02 0.03 0.02 0.02 0.03 0.02 0.02 0.02 0.03 0.02 0.02 0.03 0.03 0.02 0.02 0.02 0.17 0.02 0.04 Ks 2.16 µm 9.53 9.43 8.68 14.38 11.26 11.99 9.42 7.70 10.52 9.03 13.92 9.93 11.76 12.32 14.73 10.91 6.29 6.31 8.21 12.96 9.78 4.84 6.48 10.69 10.69 11.47 12.35 12.25 9.44 11.20 6.90 14.83 9.41 12.77 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 0.03 0.02 0.02 0.07 0.03 0.03 0.02 0.02 0.02 0.02 0.05 0.02 0.02 0.04 0.09 0.02 0.02 0.02 0.02 0.03 0.02 0.02 0.02 0.02 0.02 0.03 0.02 0.03 0.02 0.02 0.02 0.13 0.02 0.03

101 102 103 104 105 106 107 108 109 110 111 112 113 114 115 116 117 118 119 120 121 122 123 124 125 126 127 128 129 130 131 132 133 134

Sz116 Sz117 Sz118 Lup650 Lup810s Lup818s Sz119 SSTc2dJ161000.1-385401 2MASSJ16100133-3906449 Sz121 SSTc2dJ161013.1-384617 Sz122 SSTc2dJ161018.6-383613 SSTc2dJ161019.8-383607 SSTc2dJ161027.4-390230 SSTc2dJ161029.6-392215 IRAS16072-3738 SSTc2dJ161034.5-381450 SSTc2dJ161035.0-390655 SSTc2dJ161045.4-385455 Sz123 SSTc2dJ161118.7-385824 SSTc2dJ161126.0-391123 SSTc2dJ161131.9-381110 Lup831s SSTc2dJ161144.9-383245 SSTc2dJ161148.7-381758 Lup802s Sz124 SST-Lup3-1 SSTc2dJ161200.1-385557 SSTc2dJ161204.5-380959 SSTc2dJ161211.2-383220 SSTc2dJ161218.5-393418

­ 84 ­

05 05 05

05 05 05

05 05 05 05 05


Table 12--Continued
No. Ob ject Id. B 0.44 µm 383742 371328 381503 384216 375643 383724 373646 423507 415457 422158 422216 415356 422540 17. 17. 15. 17. 17. 16. 17. 17. 18. 17. 16. 16. 15. 16. 12. 17. 18. 18. 18. 17. 17. 17. 24 63 00 22 47 21 97 42 27 29 86 . 57 82 92 64 51 38 . 26 01 99 84 . 77 ± ± ± ± ± ± ± ± ± ± ± .. ± ± ± ± ± ± .. ± ± ± ± .. ± 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 05 05 05 05 05 05 05 05 05 05 05 05 05 05 05 05 05 05 05 05 05 V 0.55 µm 15. 15. 13. 15. 15. 13. 57 63 44 45 45 68 . 82 41 85 46 . 45 71 39 17 13 66 . 48 26 07 . . 60 ± ± ± ± ± ± .. ± ± ± ± .. ± ± ± ± ± ± .. ± ± ± .. .. ± 0. 0. 0. 0. 0. 0. 05 05 05 05 05 05 Rc 0.64 µm 14. 15. 13. 14. 14. 13. 16. 55 76 39 06 22 22 37 ± 0.05 ± 0.05 ± 0.05 ± 0.05 ± 0.29 ± 0.05 ± 0.01 Lupus .. ± 0.29 ± 0.05 ± 0.17 ± 0.05 ± 0.21 ± 0.54 ± 0.05 ± 0.05 ± 0.05 ± 0.06 .. ± 0.12 ± 0.40 ± 0.08 ± 1.27 ± 0.10 ± 0.23 Ic 0.79 µm 11.82 . 11.61 . 10.98 . 14.66 IV . 11.56 13.43 13.59 . 13.80 12.46 . . 12.92 12.98 . 13.34 12.43 11.11 17.74 14.69 15.04 ± .. ± .. ± .. ± .. ± ± ± .. ± ± .. .. ± ± .. ± ± ± ± ± ± 0.00 0.00 0.00 0.01 Z 0.96 µm 10.77 . 11.74 . 10.43 . 14.09 ± .. ± .. ± .. ± 0.00 0.00 0.00 0.01 J 1.23 µm 8.72 10.63 10.54 8.57 7.77 8.91 12.76 13.18 9.10 11.63 11.45 8.16 11.82 10.73 8.71 9.46 11.47 10.48 16.44 10.78 10.15 7.10 14.98 11.52 12.11 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 0.02 0.02 0.02 0.02 0.02 0.04 0.09 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 H 1.66 µm 7.62 9.60 9.77 7.48 6.64 7.75 12.09 12.58 7.78 10.98 10.59 7.06 11.10 9.93 7.53 8.68 10.61 9.37 14.47 9.54 9.07 5.71 13.71 10.26 10.55 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 0.02 0.02 0.02 0.02 0.02 0.04 0.09 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 Ks 2.16 µm 7.19 8.96 9.54 6.99 6.11 7.27 11.61 12.26 7.19 10.66 10.14 6.12 10.78 9.62 6.90 8.35 10.10 8.96 12.85 9.05 8.60 5.09 12.89 9.71 9.53 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 0.02 0.02 0.02 0.02 0.02 0.02 0.02 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05 0.05

135 136 137 138 139 140 141 142 143 144 145 146 147 148 149 150 151 152 153 154 155 156 157 158 159

SST SST SST SST SST SST SST

c2dJ161219. c2dJ161222. c2dJ161243. c2dJ161251. c2dJ161256. c2dJ161341. c2dJ161344.

6787001-

SSTc2dJ155925.2SSTc2dJ155945.3SSTc2dJ160000.6SSTc2dJ160002.4IRAS15567-4141 SSTc2dJ160026.1Sz130 SSTc2dJ160034.4F403 Sz131 SSTc2dJ160111.6SSTc2dJ160115.6SSTc2dJ160129.7SSTc2dJ160143.3IRAS15585-4134 IRAS15589-4132 SSTc2dJ160229.9Sz133

16. 14. 15. 15. 16. 14. 17. 12. 16. 16. 16. 16. 16.

0. 0. 0. 0. 0. 0. 0. 0. 0. 0.

05 05 05 05 05 05 05 05 05 05

413730 415235 420804 413606

0.05 0.05 0.05

415111

0.05

16.

0.05

. 42 25 98 30 70 56 56 06 60 46 . 15.67 15.17 14.24 17.98 17.69 15.78 13. 15. 14. 16. 15. 13. 15. 11. 14. 15.

0.00 0.01 0.01 0.01 0.00

0.00 0.00 0. 0. 0. 0. 0. 0. 01 00 00 04 01 01

... 11.02 ± 0.00 13.02 ± 0.01 13.09 ± 0.01 ... 13.10 ± 0.01 12.26 ± 0.00 ... ... 13.26 ± 0.01 12.27 ± 0.00 ... 12.63 ± 0.01 11.70 ± 0.00 9.97 ± 0.00 17.19 ± 0.04 13.53 ± 0.01 14.06 ± 0.01

­ 85 ­

Note. -- B and V magnitudes from the NOMAD catalog (Zacharias et al. 2005). Note. -- Rc , Ic , and z magnitudes from F. Comeron et al. (in prep.). Note. -- J , H , and K s magnitudes from the 2MASS catalog (Cutri et al. 2003).


Table 13. IRAC and MIPS fluxes in mJy of the Lupus sample
No. Ob ject Id. IRAC 3.6 µm IRAC 4.5 µm IRAC 5.8 µm IRAC 8.0 µm MIPS 24 µm MIPS 70 µm MIPS 160 µm

1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 31 32

SSTc2dJ153803.1IRAS15356-3430 AKC2006-17 Sz65 Sz66 Sz67 AKC2006-18 SSTc2dJ154214.6SSTc2dJ154240.3IRAS15398-3359 SSTc2dJ154302.3AKC2006-19 SSTc2dJ154506.3SSTc2dJ154508.9Sz68a Sz69 SSTc2dJ154518.5-

331358

341026 341343 344406 341738 341734

342125

347.00 ± 18.80 3.95 ± 0.40 0.49 ± 0.03 255.00 ± 14.30 95.80 ± 4.98 79.10 ± 4.08 1.81 ± 0.10 2.18 ± 0.14 178.00 ± 11.00 ... 2.45 ± 0.12 5.48 ± 0.27 14.10 ± 0.68 101.00 ± 5.12 1580.00 ± 132.00 111.00 ± 5.84 37.70 ± 1.89 4.02 ± 0.20 32.90 ± 1.64 ... 185.00 ± 9.56 38.60 ± 1.93 ... ... 0.50 ± 0.03 6.96 ± 0.46 19.60 ± 1.00 42.10 ± 2.53 112.00 ± 12.20 2.71 ± 0.15 372.00 ± 28.10 9.30 ± 0.48

220.00 ± 18.80 2.76 ± 0.40 0.37 ± 0.03 225.00 ± 14.30 81.50 ± 4.98 50.10 ± 4.08 1.75 ± 0.10 1.78 ± 0.14 120.00 ± 11.00 25.20 ± 2.00 3.25 ± 0.12 4.06 ± 0.27 15.40 ± 0.68 104.00 ± 5.12 1420.00 ± 132.00 120.00 ± 5.84 37.90 ± 1.89 5.08 ± 0.20 48.30 ± 1.64 ... 154.00 ± 9.56 24.70 ± 1.93 < 1.54 ... 0.31 ± 0.03 6.12 ± 0.46 13.50 ± 1.00 31.80 ± 2.53 131.00 ± 12.20 3.62 ± 0.15 272.00 ± 28.10 6.30 ± 0.48

SSTc2dJ160703.9-391112 SSTc2dJ160708.6-391407 SSTc2dJ160708.6-394723 Sz90 Sz91a Lup605 Sz92 Lup654 Lup713a Sz94 Sz95 SSTc2dJ160754.1-392046 2MASSJ16075475-3915446 SSTc2dJ160755.3-390718a Lup714

a

Lupus I 182.00 ± 9.44 126.00 ± 6.43 9.58 ± 0.75 42.70 ± 3.11 0.35 ± 0.04 0.25 ± 0.06 231.00 ± 12.50 284.00 ± 14.00 82.50 ± 3.99 100.00 ± 4.84 35.10 ± 1.70 21.30 ± 1.03 1.56 ± 0.10 1.40 ± 0.08 3.52 ± 0.23 16.40 ± 0.92 99.80 ± 5.06 68.80 ± 3.28 35.80 ± 3.00 118.00 ± 18.00 4.23 ± 0.21 5.89 ± 0.28 3.29 ± 0.16 3.73 ± 0.18 16.20 ± 0.77 19.10 ± 0.90 100.00 ± 4.73 94.30 ± 4.66 1690.00 ± 97.90 2170.00 ± 130.00 94.60 ± 4.59 83.00 ± 4.12 35.80 ± 1.71 40.30 ± 1.91 Lupus III 6.92 ± 0.34 11.70 ± 0.56 60.60 ± 2.89 89.30 ± 4.44 ... ... 127.00 ± 6.33 123.00 ± 5.93 17.20 ± 0.83 10.90 ± 0.52 ... 0.61 ± 0.05 ... ... 0.20 ± 0.03 0.15 ± 0.04 5.65 ± 0.31 6.69 ± 0.33 9.35 ± 0.44 5.69 ± 0.27 27.30 ± 1.41 29.60 ± 1.42 103.00 ± 5.19 66.00 ± 3.26 4.13 ± 0.21 3.94 ± 0.19 271.00 ± 13.90 180.00 ± 9.06 4.33 ± 0.24 2.60 ± 0.14

35.60 ± 3.30 114.00 ± 11.20 0.41 ± 0.46 483.00 ± 44.60 167.00 ± 15.50 2.68 ± 0.37 0.40 ± 0.33 56.10 ± 5.20 13.00 ± 1.22 991000.00 ± 99.00 21.50 ± 1.99 3.44 ± 0.38 69.90 ± 6.46 137.00 ± 12.70 286.00 ± 270.00 100.00 ± 9.72 38.50 ± 3.56 33.60 ± 196.00 ± 34.80 ± 258.00 ± 9.72 ± ... 1.54 ± 0.47 ± 6.39 ± 0.80 ± 30.00 ± 16.30 ± 16.50 ± 73.20 ± 0.06 ± 3.16 18.20 3.31 24.00 0.98 0.50 0.49 0.64 0.45 2.82 1.55 1.56 6.84 0.43

< 50. 2920.00 ± < 50. 468.00 ± < 50. < 50. < 50. 593.00 ± < 50. 15400.00 ± 89.70 ± < 50. 204.00 ± 702.00 ± 4900.00 ± 154.00 ± < 50. 99.20 ± 189.00 ± < 50. 335.00 ± 502.00 ± < 50. < 50. < 50. < 50. < 50. < 50. < 50. 91.50 ± < 50. < 50.

00 279.00 00 47.30 00 00 00 56.20 00 1540.00 15.40 00 23.20 67.80 459.00 20.10 00 17.20 22.50 00 34.70 53.20 00 00 00 00 00 00 00 16.40 00 00

... ... ... ... ... ... ... ... ... 57.20 ± 11.44 ... ... ... ... 52000.00 ± 10400.00 ... ...

­ 86 ­

. . . . . . . . . . . . . . .

. . . . . . . . . . . . . . .

. . . . . . . . . . . . . . .


Table 13--Continued
No. Ob ject Id. IRAC 3.6 µm 16.30 ± 1.07 ± 217.00 ± 323.00 ± 168.00 ± 4.55 ± 12.70 ± 27.90 ± 373.00 ± 23.80 ± 53.10 ± 3.40 ± 0.62 ± 79.80 ± 14.40 ± 0.23 ± 32.10 ± ... 25.50 ± 0.27 ± 35.50 ± 650.00 ± 25.90 ± 2.23 ± 60.10 ± 26.50 ± 86.70 ± 32.60 ± 0.31 ± 0.06 ± 21.80 ± 6.52 ± 69.40 ± 2.80 ± 0.90 0.06 12.10 38.20 12.60 0.25 0.74 1.73 30.40 1.39 3.21 0.19 0.03 4.11 0.82 0.02 1.97 1.47 0.02 17.20 47.60 1.37 0.15 4.42 1.51 4.35 1.84 0.02 0.09 1.30 0.35 4.79 0.15 IRAC 4.5 µm 15.10 1.06 118.00 249.00 113.00 5.35 9.77 25.20 477.00 22.90 50.40 2.91 0.47 55.50 24.10 0.27 28.10 . 22.50 0.37 . 262.00 18.60 2.01 81.30 20.20 58.20 27.00 0.40 0.11 17.10 4.67 79.00 2.88 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± .. ± ± .. ± ± ± ± ± ± ± ± ± ± ± ± ± 0.90 0.06 12.10 38.20 12.60 0.25 0.74 1.73 30.40 1.39 3.21 0.19 0.03 4.11 0.83 0.02 1.97 1.47 0.02 47.60 1.37 0.15 4.42 1.51 4.35 1.84 0.02 0.09 1.30 0.35 4.79 0.15 IRAC 5.8 µm 12.80 ± 0.64 1.00 ± 0.06 102.00 ± 5.13 253.00 ± 15.00 138.00 ± 7.99 5.78 ± 0.29 6.86 ± 0.34 23.70 ± 1.14 429.00 ± 25.40 20.10 ± 1.01 48.70 ± 2.48 2.53 ± 0.14 0.33 ± 0.04 41.60 ± 2.03 34.00 ± 1.68 0.39 ± 0.07 30.00 ± 1.81 ... 20.00 ± 1.01 0.49 ± 0.05 12100.00 ± 1270.00 256.00 ± 13.30 13.00 ± 0.62 1.77 ± 0.11 72.10 ± 3.58 14.10 ± 0.68 36.50 ± 1.96 23.60 ± 1.19 0.55 ± 0.05 0.31 ± 0.14 12.10 ± 0.59 3.31 ± 0.17 77.60 ± 3.75 2.24 ± 0.13 IRAC 8.0 µm 14.40 ± 0.69 1.32 ± 0.08 67.50 ± 3.53 339.00 ± 17.50 173.00 ± 9.38 5.80 ± 0.28 4.22 ± 0.21 25.70 ± 1.23 693.00 ± 39.90 21.10 ± 1.00 61.70 ± 3.04 3.56 ± 0.18 0.18 ± 0.08 32.90 ± 1.60 67.00 ± 3.26 0.62 ± 0.05 33.80 ± 1.77 ... 21.30 ± 1.10 0.68 ± 0.05 3490.00 ± 590.00 134.00 ± 7.64 7.64 ± 0.38 1.93 ± 0.11 73.80 ± 3.86 9.24 ± 0.44 25.60 ± 1.24 22.30 ± 1.18 0.89 ± 0.07 0.31 ± 0.29 7.15 ± 0.38 2.03 ± 0.11 127.00 ± 6.39 1.73 ± 0.10 MIPS 24 µm 16.60 3.51 16.20 99.50 241.00 7.88 0.55 31.20 1200.00 26.20 130.00 7.15 0.25 24.10 347.00 2.68 81.20 473.00 47.90 2.22 2890.00 19.20 0.76 1.29 69.50 10.70 3.79 53.50 3.75 0.28 0.94 0.29 191.00 26.60 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 1.57 0.40 1.55 9.44 22.90 0.77 0.46 2.97 114.00 2.45 12.10 0.70 0.61 2.29 32.60 0.34 7.66 45.80 4.62 0.32 720.00 2.11 0.43 0.54 6.56 1.03 1.30 5.06 0.42 2.32 0.93 0.52 18.10 2.55 MIPS 70 µm < 50. < 50. < 50. < 50. 157.00 ± < 50. < 50. 88.60 ± 540.00 ± < 50. 223.00 ± < 50. < 50. < 50. 257.00 ± < 50. 317.00 ± 2200.00 ± 441.00 ± < 50. 3780.00 ± < 50. < 50. < 50. < 50. < 50. < 50. < 50. < 50. < 50. < 50. < 50. < 50. 492.00 ± 00 00 00 00 21.90 00 00 16.90 55.10 00 28.50 00 00 00 30.20 00 40.00 219.00 53.20 00 360.00 00 00 00 00 00 00 00 00 00 00 00 00 53.60 MIPS 160 µm . . . . . . . . . . . . . . . . . 2209.00 . . . . . . . . . . . . . . . . .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. ± 441.80 .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. ..

33 34 35 36 37 38 39 40 41 42 43 44 45 46 47 48 49 50 51 52 53 54 55 56 57 58 59 60 61 62 63 64 65 66

Lup604s 2MASSJ16080175-3912316 SSTc2dJ160803.0-385229 2MASSJ16080618-3912225 Sz96 2MASSJ16081497-3857145 Par-Lup3-1 Sz97 Sz98 Sz99 Sz100 Lup607a NTO2000-0526.9-5630 Sz101 Sz102 IRACJ16083010-3922592 Sz103 SSTc2dJ160830.7-382827 Sz104 IRACJ16083110-3856000 HR5999b HR6000 Par-Lup3-2 Lup706 Sz106 Sz107 Sz108 Sz108B IRACJ16084679-3902074 2MASSJ16084747-3905087 Sz109 Lup617 Par-Lup3-3 Par-Lup3-4

­ 87 ­


Table 13--Continued
No. Ob ject Id. IRAC 3.6 µm 69.90 57.10 0.44 7.30 . 7.60 48.70 15.40 32.80 1.85 0.35 3.89 44.70 95.70 0.43 22.20 4.76 10.70 0.75 3.58 0.25 1.53 5.72 0.68 . 0.17 533.00 0.22 0.25 1.16 0.55 49.30 6.31 0.16 ± ± ± ± .. ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± .. ± ± ± ± ± ± ± ± ± 3.61 3.13 0.03 0.38 0.38 2.96 0.89 1.82 0.10 0.02 0.21 2.95 5.43 0.03 1.36 0.25 0.61 0.04 0.20 0.03 0.08 0.31 0.04 0.01 55.00 0.01 0.02 0.06 0.03 3.10 0.34 0.01 IRAC 4.5 µm 67.80 ± 3.61 46.70 ± 3.13 0.29 ± 0.03 6.52 ± 0.38 ... 7.76 ± 0.38 38.00 ± 2.96 15.00 ± 0.89 40.70 ± 1.82 2.28 ± 0.10 0.23 ± 0.02 3.69 ± 0.21 34.00 ± 2.95 101.00 ± 5.43 0.32 ± 0.03 18.40 ± 1.36 3.36 ± 0.26 7.74 ± 0.61 0.65 ± 0.04 2.40 ± 0.20 1.00 ± 0.03 1.44 ± 0.08 5.18 ± 0.31 0.61 ± 0.04 ... 0.12 ± 0.01 399.00 ± 55.00 0.29 ± 0.01 0.11 ± 0.02 1.09 ± 0.06 0.40 ± 0.03 50.70 ± 3.10 5.84 ± 0.34 0.10 ± 0.01 IRAC 5.8 µm 58.80 43.70 0.17 5.79 . 5.85 30.40 14.90 45.10 2.09 0.13 3.77 30.60 97.20 0.16 14.80 2.57 5.45 0.54 1.73 0.99 1.31 4.84 0.55 . 0.08 466.00 0.36 0.11 0.97 0.24 54.50 5.60 0.06 ± ± ± ± .. ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± .. ± ± ± ± ± ± ± ± ± 2.82 2.14 0.04 0.29 0.30 1.49 0.72 2.16 0.11 0.02 0.23 1.61 4.66 0.05 0.72 0.14 0.27 0.04 0.12 0.07 0.07 0.24 0.04 0.02 26.00 0.04 0.03 0.06 0.04 2.64 0.27 0.05 IRAC 8.0 µm 70.50 ± 3.45 45.50 ± 2.22 0.10 ± 0.08 5.07 ± 0.25 ... 6.97 ± 0.35 24.80 ± 1.22 20.50 ± 0.99 28.10 ± 1.36 1.30 ± 0.08 0.09 ± 0.06 4.31 ± 0.21 25.80 ± 1.29 121.00 ± 6.02 0.14 ± 0.04 12.40 ± 0.59 1.54 ± 0.09 3.28 ± 0.16 0.38 ± 0.04 1.00 ± 0.07 0.55 ± 0.05 0.84 ± 0.06 2.95 ± 0.15 0.30 ± 0.03 ... 0.03 ± 0.05 283.00 ± 14.90 0.46 ± 0.04 0.01 ± 0.05 0.61 ± 0.05 0.15 ± 0.05 35.00 ± 1.67 3.55 ± 0.18 0.07 ± 0.05 MIPS 24 µm 171.00 54.90 0.36 5.90 41.50 7.05 124.00 56.10 3.91 0.09 0.14 5.40 42.20 347.00 0.18 10.50 0.22 0.69 0.31 0.02 32.40 0.08 0.21 0.17 36.30 0.02 53.50 1.65 0.12 0.04 0.19 6.43 0.35 0.05 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 16.20 5.15 0.53 0.86 3.86 0.70 11.70 5.35 0.48 0.49 0.40 0.57 3.96 32.30 0.52 1.01 0.44 0.43 0.30 0.45 3.04 0.30 0.41 0.44 3.39 0.44 5.02 0.28 0.46 0.31 0.34 0.64 0.32 0.30 MIPS 70 µm < 50. 119.00 ± < 50. < 50. < 50. < 50. 120.00 ± 88.30 ± < 50. < 50. < 50. < 50. 114.00 ± 257.00 ± < 50. < 50. < 50. < 50. < 50. < 50. 2610.00 ± < 50. < 50. < 50. 73.60 ± < 50. < 50. < 50. < 50. < 50. < 50. < 50. < 50. < 50. 00 20.40 00 00 00 00 25.20 16.00 00 00 00 00 15.00 30.50 00 00 00 00 00 00 252.00 00 00 00 11.40 00 00 00 00 00 00 00 00 00 MIPS 160 µm ... ... ... ... 1678.00 ± 335.60 ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... 8708.00 ± 1742.00 ... ... ... ... ... ... ... ... ... ... ... ... ...

67 68 69 70 71 72 73 74 75 76 77 78 79 80 81 82 83 84 85 86 87 88 89 90 91 92 93 94 95 96 97 98 99 100

Sz110 2MASSJ16085324-3914401 NTO2000-0532.1-5616 2MASSJ16085373-3914367 Sz111c 2MASSJ16085529-3848481 Sz112a Sz113 NTO2000-0536.7-5943 NTO2000-0536.7-5956 NTO2000-0537.4-5653 2MASSJ16085953-3856275 SSTc2dJ160901.4-392512 Sz114 NTO2000-0540.9-5757a Sz115 NTO2000-0546.4-5934 Lup608s NTO2000-0554.9-5651 Lup710 Lupus3MMS NTO2000-0558.8-5610 NTO2000-0601.7-5616 NTO2000-0605.1-5606 SSTc2dJ160927.0-383628 NTO2000-0605.6-5437 SSTc2dJ160934.1-391342 IRACJ16093418-3915127 NTO2000-0614.0-5414 NTO2000-0615.6-5616 NTO2000-0615.6-5953 NTO2000-0615.8-5734 NTO2000-0617.7-5641 NTO2000-0619.6-5414

a

a

­ 88 ­


Table 13--Continued
No. Ob ject Id. Sz116a Sz117 Sz118 Lup650 Lup810s Lup818sa Sz119 SSTc2dJ161000.1-385401 2MASSJ16100133-3906449 Sz121 SSTc2dJ161013.1-384617a Sz122 SSTc2dJ161018.6-383613a SSTc2dJ161019.8-383607 SSTc2dJ161027.4-390230 SSTc2dJ161029.6-392215 IRAS16072-3738 SSTc2dJ161034.5-381450 SSTc2dJ161035.0-390655 SSTc2dJ161045.4-385455 Sz123a SSTc2dJ161118.7-385824 SSTc2dJ161126.0-391123 SSTc2dJ161131.9-381110 Lup831s SSTc2dJ161144.9-383245 SSTc2dJ161148.7-381758 Lup802s Sz124 SST-Lup3-1 SSTc2dJ161200.1-385557 SSTc2dJ161204.5-380959 SSTc2dJ161211.2-383220a SSTc2dJ161218.5-393418a IRAC 3.6 µm 50.00 ± 3.47 65.20 ± 4.38 212.00 ± 16.20 0.70 ± 0.04 9.56 ± 0.61 7.44 ± 0.39 49.20 ± 3.12 366.00 ± 23.90 27.20 ± 1.58 81.70 ± 4.34 1.89 ± 0.11 34.50 ± 1.71 7.03 ± 0.47 5.41 ± 0.30 0.67 ± 0.04 19.10 ± 0.93 1200.00 ± 67.10 1210.00 ± 64.20 234.00 ± 12.30 4.93 ± 0.24 59.90 ± 3.08 2820.00 ± 258.00 1010.00 ± 54.60 18.80 ± 0.92 20.20 ± 0.98 10.40 ± 0.52 11.60 ± 0.57 4.79 ± 0.24 50.80 ± 2.49 15.80 ± 0.84 615.00 ± 33.10 1.98 ± 0.10 50.50 ± 2.60 ... IRAC 4.5 µm 30.40 ± 61.50 ± 255.00 ± 0.47 ± 6.55 ± 6.50 ± 37.70 ± 176.00 ± 24.00 ± 55.40 ± 2.78 ± 21.80 ± 6.30 ± 5.47 ± 0.61 ± 14.20 ± 667.00 ± 616.00 ± 154.00 ± 5.55 ± 50.40 ± 2530.00 ± 599.00 ± 11.80 ± 11.20 ± 7.24 ± 11.40 ± 3.30 ± 32.40 ± 13.10 ± 346.00 ± 2.84 ± 54.20 ± ... 3.47 4.38 16.20 0.04 0.61 0.39 3.12 23.90 1.58 4.34 0.11 1.71 0.47 0.30 0.04 0.93 67.10 64.20 12.30 0.24 3.08 258.00 54.60 0.92 0.98 0.52 0.57 0.24 2.49 0.84 33.10 0.10 2.60 IRAC 5.8 µm 20.90 ± 1.26 56.90 ± 2.74 238.00 ± 12.20 0.32 ± 0.03 4.54 ± 0.23 5.81 ± 0.29 25.90 ± 1.23 268.00 ± 14.00 21.00 ± 1.01 38.10 ± 1.85 2.35 ± 0.14 15.30 ± 0.75 4.67 ± 0.29 4.17 ± 0.27 0.48 ± 0.04 11.50 ± 0.56 633.00 ± 30.90 672.00 ± 32.60 125.00 ± 6.33 6.30 ± 0.31 42.60 ± 2.07 2390.00 ± 123.00 556.00 ± 27.00 8.99 ± 0.45 8.80 ± 0.42 5.03 ± 0.25 10.80 ± 0.56 2.26 ± 0.12 22.10 ± 1.05 11.00 ± 0.53 291.00 ± 15.60 3.68 ± 0.19 65.10 ± 3.09 ... IRAC 8.0 µm 14.10 ± 0.77 55.30 ± 2.67 302.00 ± 22.80 0.19 ± 0.04 2.78 ± 0.14 7.63 ± 0.37 15.30 ± 0.77 206.00 ± 10.60 18.80 ± 0.89 23.20 ± 1.10 2.36 ± 0.13 8.96 ± 0.43 4.97 ± 0.25 4.92 ± 0.25 0.44 ± 0.05 10.90 ± 0.53 412.00 ± 21.90 463.00 ± 22.90 82.60 ± 3.98 6.90 ± 0.33 44.90 ± 2.12 1600.00 ± 91.20 362.00 ± 17.10 6.38 ± 0.32 5.04 ± 0.25 3.01 ± 0.15 12.20 ± 0.58 1.30 ± 0.08 13.70 ± 0.64 12.90 ± 0.61 182.00 ± 8.80 4.70 ± 0.23 113.00 ± 5.47 ... MIPS 24 µm 1.70 ± 0.33 91.50 ± 8.51 355.00 ± 33.60 0.27 ± 0.35 0.47 ± 0.33 11.70 ± 1.12 2.01 ± 0.32 97.20 ± 9.14 24.10 ± 2.28 2.82 ± 0.36 12.80 ± 1.21 0.99 ± 0.25 4.01 ± 0.44 5.29 ± 0.55 8.29 ± 0.82 33.70 ± 3.18 107.00 ± 10.20 109.00 ± 10.20 18.40 ± 1.76 3.21 ± 0.37 61.00 ± 5.76 518.00 ± 49.70 105.00 ± 9.76 1.86 ± 0.33 0.45 ± 0.32 1.60 ± 0.28 22.90 ± 2.22 0.10 ± 0.33 1.67 ± 0.26 21.00 ± 1.98 48.80 ± 4.59 11.30 ± 1.09 77.90 ± 7.25 134.00 ± 12.60 MIPS 70 µm < 50. 122.00 ± 322.00 ± < 50. < 50. 96.90 ± < 50. < 50. < 50. < 50. < 50. < 50. < 50. < 50. < 50. 110.00 ± < 50. < 50. < 50. < 50. 327.00 ± < 50. < 50. < 50. < 50. < 50. < 50. < 50. < 50. < 50. < 50. < 50. < 50. < 50. 00 20.50 38.80 00 00 22.10 00 00 00 00 00 00 00 00 00 18.00 00 00 00 00 35.60 00 00 00 00 00 00 00 00 00 00 00 00 00 MIPS 160 µm . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

101 102 103 104 105 106 107 108 109 110 111 112 113 114 115 116 117 118 119 120 121 122 123 124 125 126 127 128 129 130 131 132 133 134

­ 89 ­


Table 13--Continued
No. Ob ject Id. IRAC 3.6 µm 463.00 . 90.30 637.00 1330.00 392.00 . ± .. ± ± ± ± .. 26.00 4.46 34.20 72.70 20.60 IRAC 4.5 µm 288.00 . 75.30 349.00 738.00 219.00 . ± .. ± ± ± ± .. 26.00 4.46 34.20 72.70 20.60 IRAC 5.8 µm 251.00 ± 12.30 ... 69.80 ± 3.29 306.00 ± 15.10 684.00 ± 33.40 177.00 ± 9.04 ... Lupus IV ... 323.00 ± 16.00 ... ... 1680.00 ± 113.00 14.20 ± 0.67 53.30 ± 2.53 ... 140.00 ± 6.81 ... 49.10 ± 2.34 8.98 ± 0.44 48.90 ± 2.31 56.40 ± 2.68 1710.00 ± 88.20 12.60 ± 0.62 25.50 ± 1.22 ... IRAC 8.0 µm 167.00 . 74.80 202.00 439.00 112.00 . ± .. ± ± ± ± .. 8.39 3.57 10.90 20.80 5.38 MIPS 24 µm 40.90 46.50 92.50 74.30 116.00 25.10 10.10 5.59 268.00 16.50 41.00 780.00 24.00 115.00 483.00 590.00 64.40 7.82 75.90 17.90 10.20 263.00 144.00 5.15 142.00 ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± ± 3.85 4.32 8.68 7.04 10.80 2.38 0.97 0.59 24.80 1.54 3.79 73.40 2.23 10.60 44.60 55.20 5.95 0.76 7.03 1.67 0.97 24.40 13.40 0.51 13.20 MIPS 70 µm < 50. < 50. 116.00 ± < 50. < 50. ... < 50. < 50. < 50. < 50. < 50. 91.60 ± < 50. 165.00 ± 108.00 ± 1050.00 ± 52.90 ± < 50. 1220.00 ± < 50. < 50. < 50. 1030.00 ± < 50. < 50. 00 00 16.50 00 00 00 00 00 00 00 14.80 00 22.10 17.00 103.00 10.20 00 123.00 00 00 00 107.00 00 00 MIPS 160 µm . . . . . . . . . . . . . . . 2272.00 . . 5386.00 . . . 2336.00 . . . . . . . . . . . . . . . .

135 136 137 138 139 140 141 142 143 144 145 146 147 148 149 150 151 152 153 154 155 156 157 158 159

SST SST SST SST SST SST SST

c2dJ161219. c2dJ161222. c2dJ161243. c2dJ161251. c2dJ161256. c2dJ161341. c2dJ161344.

6787001-

383742 371328 381503 384216 375643 383724 373646 423507 415457 422158 422216 415356 422540
a

SSTc2dJ155925.2SSTc2dJ155945.3SSTc2dJ160000.6SSTc2dJ160002.4IRAS15567-4141 SSTc2dJ160026.1Sz130a SSTc2dJ160034.4F403 Sz131 SSTc2dJ160111.6SSTc2dJ160115.6SSTc2dJ160129.7SSTc2dJ160143.3IRAS15585-4134 IRAS15589-4132a SSTc2dJ160229.9Sz133a

413730 415235 420804 413606

a

415111

... 578.00 ± 31.00 ... ... 1380.00 ± 145.00 21.50 ± 1.05 59.00 ± 3.02 ... 177.00 ± 9.40 ... 96.90 ± 4.79 8.36 ± 0.44 91.10 ± 4.43 121.00 ± 6.02 1400.00 ± 182.00 5.10 ± 0.30 49.90 ± 2.60 ...

... 335.00 ± 31.00 ... ... 2000.00 ± 145.00 16.80 ± 1.05 53.50 ± 3.02 ... 141.00 ± 9.40 < 55.70 61.30 ± 4.79 9.92 ± 0.44 58.60 ± 4.43 69.90 ± 6.02 1860.00 ± 182.00 4.87 ± 0.30 30.10 ± 2.60 ...

... 380.00 ± 18.70 ... ... 1620.00 ± 87.30 16.30 ± 0.78 70.10 ± 3.35 ... 213.00 ± 11.20 58.20 ± 2.78 34.30 ± 1.64 7.70 ± 0.37 38.00 ± 1.85 36.60 ± 1.76 1170.00 ± 58.20 42.10 ± 2.03 18.20 ± 0.85 ...

.. .. .. .. .. .. .. .. ± 454.40 .. .. ± 1077.00 .. .. .. ± 467.20 .. ..

­ 90 ­

Note. -- Note. -- Note. --

a

Binary star inside IRAC or MIPS PSFs, corresponding fluxes transformed to upper limits in SED plots. Flux from IRAC bands 1 and 2 saturated. MIPS-1 non-detection likely due to high background.

b

c

Note. -- MIPS-2 non-detections were transformed to 50 mJy upp er limits, which is a good estimate of the 70 µm background around most sources.


­ 91 ­


Table 14. IRAS and 1.3 mm fluxes in mJy of the Lupus sample
No. Ob ject Id. IRAS 12 µm IRAS 25 µm Lupus I ... 00 ± 29.90 ... 00 ± 75.60 00 ± 75.60 ... ... ... ... 00 ± 128.00 ... ... ... ... 00 ± 399.00 ... ... Lupus III ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... IRAS 60 µm IRAS 100 µm Cont. 1300 µm

1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 31 32

SSTc2dJ153803.1IRAS15356-3430 AKC2006-17 Sz65 Sz66 Sz67 AKC2006-18 SSTc2dJ154214.6SSTc2dJ154240.3IRAS15398-3359a SSTc2dJ154302.3AKC2006-19 SSTc2dJ154506.3SSTc2dJ154508.9Sz68 Sz69 SSTc2dJ154518.5-

331358

341026 341343 344406 341738 341734

342125

... 332.00 ± ... 548.00 ± 548.00 ± ... ... ... ... 250.00 ± ... ... ... ... 2590.00 ± ... ... . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

33.20 54.80 54.80

299. 756. 756.

250.00

1280.

259.00

3990.

. 2620.00 . 692.00 692.00 . . . . 15200.00 . . . . 7920.00 . . . . . . . . . . . . . . . . .

.. ± .. ± ± .. .. .. .. ± .. .. .. .. ± .. .. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

262.00 69.20 69.20

1520.00

792.00

. 18000.00 . . . . . . . 41300.00 . . . . 24400.00 . . . . . . . . . . . . . . . . .

.. ± 1800.00 .. .. .. .. .. .. .. ± 4130.00 .. .. .. .. ± 2440.00 .. .. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

... ... ... 56.00 ± 47.00 ± < 66. ... ... ... 365.00 ± ... ... ... ... 135.00 ± < 30. ... ... ... ... 26.00 ± < 27. ... ... ... ... < 45. < 36. ... ... ... ...

10.00 12.00 00

10.00

­ 92 ­

15.00 00

SSTc2dJ160703.9-391112 SSTc2dJ160708.6-391407 SSTc2dJ160708.6-394723 Sz90 Sz91 Lup605 Sz92 Lup654 Lup713 Sz94 Sz95 SSTc2dJ160754.1-392046 2MASSJ16075475-3915446 SSTc2dJ160755.3-390718 Lup714

9.00 00

00 00


Table 14--Continued
No. Ob ject Id. IRAS 12 µm . . . . . . . . . . . . . . . . . . . . 18000.00 . . . . . . . . . . . . . .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. ± 1800.00 .. .. .. .. .. .. .. .. .. .. .. .. .. IRAS 25 µm . . . . . . . . . . . . . . . . . . . . 14500.00 . . . . . . . . . . . . . .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. ± 1450.00 .. .. .. .. .. .. .. .. .. .. .. .. .. IRAS 60 µm . . . . . . . . . . . . . . . . . . . . 14400.00 . . . . . . . . . . . . . .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. ± 2880.00 .. .. .. .. .. .. .. .. .. .. .. .. .. IRAS 100 µm ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... < 63200.00 ... ... ... ... ... ... ... ... ... ... ... ... ... Cont. 1300 µm ... ... ... ... < 45. ... ... 28.00 ± 84.00 ± < 30. < 27. ... ... < 39. < 30. ... < 57. ... < 42. ... ... ... ... ... ... ... ... ... ... ... ... ... ... ...

33 34 35 36 37 38 39 40 41 42 43 44 45 46 47 48 49 50 51 52 53 54 55 56 57 58 59 60 61 62 63 64 65 66

Lup604s 2MASSJ16080175-3912316 SSTc2dJ160803.0-385229 2MASSJ16080618-3912225 Sz96 2MASSJ16081497-3857145 Par-Lup3-1 Sz97 Sz98 Sz99 Sz100 Lup607 NTO2000-0526.9-5630 Sz101 Sz102 IRACJ16083010-3922592 Sz103 SSTc2dJ160830.7-382827 Sz104 IRACJ16083110-3856000 HR5999 HR6000 Par-Lup3-2 Lup706 Sz106 Sz107 Sz108 Sz108B IRACJ16084679-3902074 2MASSJ16084747-3905087 Sz109 Lup617 Par-Lup3-3 Par-Lup3-4

00

9.00 17.00 00 00

00 00 00 00

­ 93 ­


Table 14--Continued
No. Ob ject Id. IRAS 12 µm . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . IRAS 25 µm . . . . 110.00 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .. .. .. .. ± 70.00 .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. IRAS 60 µm . . . . 1120.00 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . ± 70.00 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . IRAS 100 µm ... ... ... ... 4580.00 ± 70.00 ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... < 25500.00 ... ... ... ... ... ... ... ... ... ... ... ... ... Cont. 1300 µm . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

67 68 69 70 71 72 73 74 75 76 77 78 79 80 81 82 83 84 85 86 87 88 89 90 91 92 93 94 95 96 97 98 99 100

Sz110 2MASSJ16085324-3914401 NTO2000-0532.1-5616 2MASSJ16085373-3914367 Sz111 2MASSJ16085529-3848481 Sz112 Sz113 NTO2000-0536.7-5943 NTO2000-0536.7-5956 NTO2000-0537.4-5653 2MASSJ16085953-3856275 SSTc2dJ160901.4-392512 Sz114 NTO2000-0540.9-5757 Sz115 NTO2000-0546.4-5934 Lup608s NTO2000-0554.9-5651 Lup710 Lupus3MMS NTO2000-0558.8-5610 NTO2000-0601.7-5616 NTO2000-0605.1-5606 SSTc2dJ160927.0-383628 NTO2000-0605.6-5437 SSTc2dJ160934.1-391342 IRACJ16093418-3915127 NTO2000-0614.0-5414 NTO2000-0615.6-5616 NTO2000-0615.6-5953 NTO2000-0615.8-5734 NTO2000-0617.7-5641 NTO2000-0619.6-5414

­ 94 ­


Table 14--Continued
No. Ob ject Id. IRAS 12 µm . . . . . . . . . . . . . . . . 287.00 . . . . . . . . . . . . . . . . . .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. ± 28.10 .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. .. IRAS 25 µm ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... < 449.00 ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... IRAS 60 µm ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... < 444.00 ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... IRAS 100 µm ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... < 22100.00 ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... ... Cont. 1300 µm . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

101 102 103 104 105 106 107 108 109 110 111 112 113 114 115 116 117 118 119 120 121 122 123 124 125 126 127 128 129 130 131 132 133 134

Sz116 Sz117 Sz118 Lup650 Lup810s Lup818s Sz119 SSTc2dJ161000.1-385401 2MASSJ16100133-3906449 Sz121 SSTc2dJ161013.1-384617 Sz122 SSTc2dJ161018.6-383613 SSTc2dJ161019.8-383607 SSTc2dJ161027.4-390230 SSTc2dJ161029.6-392215 IRAS16072-3738 SSTc2dJ161034.5-381450 SSTc2dJ161035.0-390655 SSTc2dJ161045.4-385455 Sz123 SSTc2dJ161118.7-385824 SSTc2dJ161126.0-391123 SSTc2dJ161131.9-381110 Lup831s SSTc2dJ161144.9-383245 SSTc2dJ161148.7-381758 Lup802s Sz124 SST-Lup3-1 SSTc2dJ161200.1-385557 SSTc2dJ161204.5-380959 SSTc2dJ161211.2-383220 SSTc2dJ161218.5-393418

­ 95 ­


­ 96 ­ Support for this work, part of the Spitzer Space Telescope Legacy Science Program, was provided by NASA through Contract Numbers 1256316, 1224608 and 1230780 issued by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. Astro chemistry at Leiden is supported by a NWO Spinoza and NOVA grant, and by the European Research Training Network "The Origin of Planetary Systems" (PLANETS, contract number HPRN-CT-2002-00308). B. M. thanks the Fundaci´n Ram´n Areces for o o early financial support. The authors would like to thank the referee for very go o d suggestions on the structure and contents of the paper, to E. Solano and R. Gutierrez from the Spanish Virtual Observatory at LAEFF for providing easy automatic access to ancillary Vizier data for the sample, and to Jennifer Hatchell for providing very detailed comments.

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Table 14--Continued
No. Ob ject Id. IRAS 12 µm 383742 371328 381503 384216 375643 383724 373646 423507 415457 422158 422216 2590. 415356 422540 289. 413730 415235 420804 413606 966. 373. 415111 . . . . . . . . . . . 00 . . . 00 . . . . . 00 00 . . . . . . . . . . . . . . . . IRAS 25 µm ... ... ... ... ... ... ... Lupus IV ... ... ... ... 1410.00 ± 141.00 ... ... ... 778.00 ± 77.80 ... ... ... ... ... 397.00 ± 397.00 261.00 ± 26.10 ... ... IRAS 60 µm . . . . . . . . . . . 479.00 . . . 1170.00 . . . . . 447.00 1050.00 . . . . . . . . . . . . . . . . IRAS 100 µm . . . . . . . . . . . . . . . . . . . . . Cont. 1300 µm . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .

135 136 137 138 139 140 141 142 143 144 145 146 147 148 149 150 151 152 153 154 155 156 157 158 159

SST SST SST SST SST SST SST

c2dJ161219. c2dJ161222. c2dJ161243. c2dJ161251. c2dJ161256. c2dJ161341. c2dJ161344.

6787001-

SSTc2dJ155925.2SSTc2dJ155945.3SSTc2dJ160000.6SSTc2dJ160002.4IRAS15567-4141 SSTc2dJ160026.1Sz130 SSTc2dJ160034.4F403 Sz131 SSTc2dJ160111.6SSTc2dJ160115.6SSTc2dJ160129.7SSTc2dJ160143.3IRAS15585-4134 IRAS15589-4132 SSTc2dJ160229.9Sz133

.. .. .. .. ± .. .. .. ± .. .. .. .. .. ± ± .. ..

259.00

60.00

96.60 37.30

.. .. .. .. ± .. .. .. ± .. .. .. .. .. ± ± .. ..

479.00

117.00

447.00 105.00

... ... ... ... 4480.00 ± ... ... ... 4550.00 ± ... ... ... ... ... 4550.00 ± 4620.00 ± ... ...

4480.00

­ 97 ­

4550.00

4550.00 462.00

Note. -- IRAS fluxes are from the IRAS Point Source Catalogue. Note. -- 1.3 mm fluxes are from Nuernberger et al. (1997), except those marked with a , which are from Reipurth et al. (1993).


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A This preprint was prepared with the AAS L TEX macros v5.2.