. : http://www.mrao.cam.ac.uk/projects/surveys/snrs-2006/tables.ps
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A Catalogue of
Galactic Supernova Remnants
(2006 April version)
D. A. Green
Cavendish Laboratory
19 J. J. Thomson Avenue
Cambridge CB3 0HE
UNITED KINGDOM
Email: D.A.Green@mrao.cam.ac.uk
The most recent conventionally published reference for this catalogue:
. Green D.A., 2004, Bulletin of the Astronomical Society of India, 32, 335--370.
(This paper -- entitled `Galactic Supernova Remnants: an Updated Catalogue and Some Statistics' -- includes
a description of the catalogue, and the summary data from the 2004 January version of the catalogue as an
Appendix.) If you make use of the detailed webbased version of the catalogue, then please also cite:
. Green D.A., 2006, `A Catalogue of Galactic Supernova Remnants (2006 April version)', Cavendish
Laboratory, Cambridge, UK (available on the WorldWideWeb at
"http://www.mrao.cam.ac.uk/surveys/snrs/").
1. The Catalogue Format
This catalogue of Galactic supernova remnants (SNRs) is an updated version of those presented in detail in
Green (1984, 1988) and in summary form in Green (1991, 1996, 2004) -- hereafter Versions I, II, III, IV and
V respectively -- and on the WorldWideWeb, in versions of 1995 July, 1996 August, 1998 September, 2000
August, 2001 December and 2004 January. (Version IV, although published in 1996, was produced in 1993, and
a detailed version of this was made available on the WorldWideWeb in 1993 November. The summary data
from the 2001 December version of the catalogue was also published as an Appendix in Stephenson & Green
2002.)
This, the 2006 April version of the catalogue, contains 265 SNRs (which is 34 more than in the previous,
2004 January, version: 35 new remnants have been added, and one has been removed), with over a thousand
references in the detailed listings, plus notes on many possible or probable remnants.
For each remnant in the catalogue the following parameters are given.
. Galactic Coordinates of the source centroid, quoted to the nearest tenth of a degree as is conventional.
(Note: in this catalogue additional leading zeros are not used.)
. Other Names that are commonly used for the remnant. These are given in parentheses if the remnant is
only a part of the source. For some remnants, notably the Crab Nebula, not all common names are given.
. Right Ascension and Declination of the source centroid. The accuracy of the quoted values depends
on the size of the remnant; for small remnants they are to the nearest few seconds of time and the
nearest minute of arc respectively, whereas for larger remnants they are rounded to coarser values, but
are in every case sufficient to specify a point within the boundary of the remnant. These coordinates are
usually deduced from radio maps rather than from Xray or optical observations, and are for J2000.0.
. Angular Size of the remnant, in arcminutes, usually taken from the highest resolution radio map avail
able. The boundary of most remnants approximates reasonably well to a circle or an ellipse; a single
value is quoted for the angular size of the more nearly circular remnants, which is the diameter of a circle
with an area equal to that of the remnant, but for elongated remnants the product of two values is quoted,
and these are the major and minor axes of the remnant boundary modelled as an ellipse. In a few cases
an ellipse is not a satisfactory description of the boundary of the object (refer to the description of the
individual object given in its catalogue entry), although an angular size is still quoted for information.
For `filledcentre' remnants the size quoted is for the largest extent of the observed radio emission, not,
as at times has been used by others, the halfwidth of the centrally brightened peak.
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. Flux Density of the remnant at 1 GHz in jansky. This is not a measured value, but is deduced from
the observed radio frequency spectrum of the source. The frequency of 1 GHz is chosen because flux
density measurements at frequencies both above and below this value are usually available.
. Spectral Index of the integrated radio emission from the remnant, a (here defined in the sense, S n --a ,
where S is the flux density at a frequency n), either a value that is quoted in the literature, or one deduced
from the available integrated flux densities of the remnant. For several SNRs a simple power law is not
adequate to describe their radio spectra, either because there is evidence that the integrated spectrum
is curved or the spectral index varies across the face of the remnant. In these cases the spectral index
is given as `varies' (refer to the description of the remnant and appropriate references in the detailed
catalogue entry for more information). In some cases, for example where the remnant is highly con
fused with thermal emission, the spectral index is given as `?' since no value can be deduced with any
confidence.
. Type of the SNR: `S' or `F' if the remnant shows a `shell' or `filledcentre' structure, or `C' if it shows
`composite' (or `combination') radio structure with a combination of shell and filledcentre characteris
tics; or `S?', `F?' or `C?', respectively, if there is some uncertainty; or `?' in several cases where an object
is conventionally regarded as an SNR even though its nature is poorly known or not well understood.
Until recently only a few remnants were classified as composite remnants, as available observations were
only able to identify the more obvious pulsarpowered, flatter radio spectrum filledcentre components
within shells. However, in recent years improved observations -- particularly in Xrays with the Chandra
satellite -- have identified many faint, pulsar powered nebulae in what until then had been identified as
pure shell remnants. (Note: the term `composite' has been used in a different sense by some authors, to
describe SNRs with shell radio and centrallybrightened Xray morphologies. An alternative term used
to describe such remnants is `mixed morphology', see Rho & Petre 1998.)
In the detailed listings, for each remnant, notes on a variety of topics are given. First, it is noted if other Galactic
coordinates have at times been used to label it (usually before good observations have revealed the full extent of
the object), if the SNR is thought to be the remnant of a historical SN, or if the nature of the source as an SNR
has been questioned (in which case an appropriate reference is usually given later in the entry). Brief descriptions
of the remnant from the available radio, optical and Xray observations as applicable are then given, together
with notes on available distance determinations, and any point sources or pulsars in or near the object (although
they may not necessarily be related to the remnant). Finally, appropriate references to observations are given
for each remnant, complete with journal, volume, page, and a short description of what information each paper
contains (for radio observations these include the telescopes used, the observing frequencies and resolutions,
together with any flux density determinations). These references are not complete, but cover representative and
recent observations of the remnant -- up to the first few months of 2006 in this version of the catalogue -- and they
should themselves include references to earlier work. The references do not generally include large observational
surveys -- of particular interest in this respect are: the Effelsberg 100m survey at 2.7 GHz of the Galactic plane
358 # < l < 240 # , |b| < 5 # by Reich et al. (1990) and Furst et al. (1990a); reviews of the radio spectra of some
SNRs by Kassim (1989), Kovalenko, Pynzar' & Udal'tsov (1994) and Trushkin (1998); the Parkes 64m survey
at 2.4 GHz of the Galactic plane 238 # < l < 365 # , |b| < 5 # by Duncan et al. (1995) and Duncan et al. (1997); the
Molonglo Galactic plane survey at 843 MHz of 245 # < l < 355 # , |b| < 1 # .5 by Green et al. (1999); the survey
of 345 # < l < 255 # , |b| < 5 # at 8.35 and 14.35 GHz by Langston et al. (2000); MAGPIS, see White, Becker &
Helfand (2005) and Helfand et al. (2006); reviews of Einstein Xray imaging and spectroscopic observations of
Galactic SNRs by Seward (1990) and Lum et al. (1992) respectively; surveys of IRAS observations of SNRs and
their immediate surroundings by Arendt (1989) and by Saken, Fesen & Shull (1992); the survey of HI emission
towards SNRs by Koo & Heiles (1991); the SPITZER survey of inner galaxy SNRs by Reach et al. (2006); and
the catalogue by Fesen & Hurford (1996) of UV/optical/infrared lines identified in SNRs.
A summary of the data available for all 265 remnants in the catalogue is given in Table I. The other
names for SNRs are listed in Table II, and the abbreviations for journals, proceedings and telescopes are listed in
Table III. The detailed listings for each SNR are given in Table IV.
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2. Revisions and Notes
2.1 Objects no longer thought to be SNRs
The following objects, which were listed in Version I of the catalogue were removed because they were no longer
thought to be remnants, or were poorly observed (see Version II for references and further details): G2.4+1.4
(see also Gray 1994a; Goss & Lozinskaya 1995; Polcaro et al. 1995), G41.9--4.1 (=CTB 73, PKS 1920+06),
G47.6+6.1 (=CTB 63), G53.9+0.3 (part of HC40), G93.4+1.8 (=NRAO 655), G123.2+2.9, G194.7+0.4 (the
Origem Loop), G287.8--0.5 (see below), G322.3--1.2 (=Kes 24) and G343.0--6.0 (but see below). G350.1--0.3,
which was listed in Version II of the catalogue, was removed as it is no longer thought to be a SNR (see Ver
sion III for details). G358.4--1.9, which was listed in Version IV of the catalogue, was removed, as following the
discussion of Gray (1994a), as it is not clear that this is a SNR. G240.9--0.9, G299.0+0.2 and G328.0+0.3, which
were listed in 1995 July version of the catalogue, were removed from the 1996 August version, following the
improved observations of Duncan et al. (1996) and Whiteoak & Green (1996). For the 1998 September revision
of the catalogue G350.0--1.8 was incorporated into G350.0--2.0, and G337.0--0.1 refers to a smaller remnant than
that previously catalogued with the same name. G112.0+1.2, G117.4+5.0, G152.2--1.2 and G211.7--1.1 -- which
were reported as SNRs by BonsignoriFacondi & Tomasi (1979) -- were removed from the 2001 December ver
sion of the catalogue, as the first three of these are not confirmed as SNRs from the ongoing Canadian Galactic
Plane Survey (Roland Kothes, private communication; but see below for further discussion of another proposed
remnant, G213.0--0.6). G10.0--0.3, which was regarded as a remnant -- possibly associated with a softgamma
repeater -- was removed from the 2004 January version of the catalogue, as it is now thought to be radio nebula
powered by a stellar wind (see Gaensler et al. 2001, Corbel & Eikenberry 2004, and references therein).
G166.2+2.5 (=OA 184) -- which has long been regarded as a SNR -- has been removed from this version
of the catalogue, following the studies of Foster et al. (2006), who identified this as an HII region.
The following objects, which have been reported as SNRs, but have not been included in any of the
versions of the SNR catalogue, have subsequently been shown not to be SNRs.
. G70.7+1.2, which was reported as a SNR by Reich et al. (1985), but this has not been confirmed by later
observations (see Green 1986; de Muizon et al. 1988; Becker & Fesen 1988; Caswell 1988; Bally et al.
1989; Phillips, Onello & Kulkarni 1993; Onello et al. 1995).
. G81.6+1.0 a possible SNR in W75 reported by WardThompson & Robson (1991). From the published
data (see the observations in Wendker, Higgs & Landecker 1991) it was noted in Version IV of the
catalogue that this is thermal source not a SNR, because of its thermal radio spectrum, and high infrared
toradio emission (see also the subsequent discussion by Wendker et al. 1993).
. Green & Gull (1984) suggested G227.1+1.0 as a very young SNR, but subsequent observations (Channan
et al. 1986; Green & Gull 1986) have shown that this is most likely an extragalactic source, not an SNR.
. A candidate SNR, G274.7--2.8, identified by Helfand & Channan (1989), has been shown not to be a
SNR by Caswell & Stewart (1991).
. G159.6--18.5, was suggested as a SN by Pauls & Schwartz (1989), from IRAS and other observations,
but is probably an HII region (see Andersson et al. 2000).
. G25.5+0.2, which was reported as a very young SNR by Cowan et al. (1989), although this identification
was not certain (see White & Becker 1990; Green 1990; Zijlstra 1991). Sramek et al. (1992) report the
detection of recombination lines from this source (also see Subrahmanyan et al. 1993). Becklin et al.
(1994) identify G25.5+0.2 as a ring nebula around a luminous blue star. See also Clark, Steele & Langer
(2000), who identified a bipolar shell around G25.5+0.2 with similarities to h Carinae.
. Most of the possible SNRs listed by Gorham (1990) -- following up SNR candidates suggested by Kassim
(1988) -- have been shown not to be SNRs by Gorham, Kulkarni & Prince (1993).
. G203.2--12.3, a optical ring about 3 arcmin in diameter, was reported as a possible SNR by Winkler
& Reipurth (1992), but was shown to be a Herbig--Haro object (HH 311) by Reipurth, Bally & Devine
(1997).
. G359.87+0.18 was reported as a possible young SNR near the Galactic Centre by YusefZadeh, Cotton
& Reynolds (1998), but was shown to be a radio galaxy by Lazio et al. (1999).
. G106.6+2.9, a small remnant proposed by Halpern et al. (2001), is incorporated into the larger cata
logued remnant G106.3+2.7.
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Some entries in the catalogue have been renamed, due to improved observations revealing a larger true extent
for the object (previously G5.3--1.0 is now G5.4--1.2; G193.3--1.5 is now G192.8--1.1; G308.7+0.0 is now incor
porated into G308.8--0.1). G337.0--0.1 now refers to a small (1.5 arcmin) remnant, rather than larger supposed
remnant at this position (see Sarma et al. 1997), and G350.0--2.0 now incorporates the previously catalogued
G350.0--1.8, based on the improved observations of Gaensler (1998).
2.2 New SNRs
The following remnants were added to Version II of the catalogue: G0.9+0.1, G1.9+0.3, G5.9+3.1,
G6.4+4.0, G8.7--0.1, G16.8--1.1, G18.9--1.1, G20.0--0.2, G27.8+0.6, G30.7+1.0, G31.5--0.6, G36.6--0.7,
G42.8+0.6, G45.7--0.4, G54.1+0.3, G73.9+0.9, G179.0+2.6, G312.4--0.4, G357.7+0.3 and G359.1--0.5.
The following remnants were added to Version III of the catalogue: G4.2--3.5, G5.2--2.6, G6.1+1.2,
G8.7--5.0, G13.5+0.2, G15.1--1.6, G16.7+0.1, G17.4--2.3, G17.8--2.6, G30.7--2.0, G36.6+2.6, G43.9+1.6,
G59.8+1.2, G65.1+0.6, G68.6--1.2, G69.7+1.0, G279.0+1.1, G284.3--1.8 (=MSH 10--53), G358.4--1.9 and
G359.0--0.9.
The following remnants were added to Version IV of the catalogue: G59.5+0.1, G67.7+1.8, G84.9+0.5,
G156.2+5.7, G318.9+0.4, G322.5--0.1, G343.1--2.3 and G348.5--0.0.
The following remnants were added to 1995 July version of the catalogue: G1.0--0.1, G1.4--0.1,
G3.7--0.2, G3.8+0.3, G28.8+1.5, G76.9+1.0, G272.2--3.2, G341.2+0.9, G354.1+0.1, G355.6--0.0, G356.3--0.3,
G356.3--1.5 and G359.1+0.9.
The following remnants were added to the 1996 August version of the catalogue: G13.3--1.3 G286.5--1.2,
G289.7--0.3, G294.1--0.0, G299.2--2.9 G299.6--0.5, G301.4--1.0, G308.1--0.7, G310.6--0.3, G310.8--0.4,
G315.9--0.0, G317.3--0.2, G318.2+0.1, G320.6--1.6, G321.9--1.1, G327.4+1.0, G329.7+0.4, G342.1+0.9,
G343.1--0.7, G345.7--0.2, G349.2--0.1, G351.7+0.8, G351.9--0.9 and G354.8--0.8.
The following remnants were added to the 1998 September version of the catalogue: G0.3+0.0,
G32.1--0.9, G55.0+0.3, G63.7+1.1 and G182.4+4.3.
The following remnants were added to the 2000 August version of the catalogue: G7.0--0.1, G16.2--2.7,
G29.6+0.1, G266.2--1.2 and G347.3--0.5.
The following remnants were added to the 2001 December version of the catalogue: G4.8+6.2,
G28.6--0.1, G85.4+0.7, G85.9--0.6, G106.3+2.7, G292.2--0.5, G343.0--6.0 G353.9--2.0, G356.2+4.5 and
G358.0+3.8.
G312.5--3.0 was added to the 2004 January version of the catalogue.
The following remnants have been added to this version of the catalogue.
. G32.4+0.1, identified by Yamaguchi et al. (2004).
. Two 2nd quadrant remnants, G96.0+2.0 and G113.0+0.2, identified by Kothes, Uyanker & Reid (2005).
. G337.2+0.1, which was confirmed as a SNR by Combi et al. (2005).
. 31 new SNRs in the region 4 # .5 < l < 22 # .0, |b| < 1 # .25 (G5.5+0.3, G6.1+0.5, G6.5--0.4, G7.2+0.2,
G8.3--0.0, G8.9+0.4, G9.7--0.0, G9.9--0.8, G10.5--0.0, G11.0--0.0, G11.1--0.7, G11.1--1.0, G11.1+0.1,
G11.8--0.2, G12.2+0.3, G12.5+0.2, G12.7--0.0, G12.8--0.0, G14.1--0.1, G14.3+0.1, G15.4+0.1,
G16.0--0.5, G16.4--0.5, G17.0--0.0, G17.4--0.1, G18.1--0.1, G18.6--0.2, G19.1+0.2, G20.4+0.1,
G21.0--0.4 and G21.5--0.1) identified by Brogan et al. (2006).
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2.3 Possible and probable SNRs not listed in the catalogue
The following are possible or probable SNRs for which further observations are required to confirm their nature
or parameters, or for which observations are not yet in the published literature.
2.3.1 Radio
. A possible SNR near the Galactic centre reported by Ho et al. (1985) from radio observations (see also
Coil & Ho 2000; Lu, Wang & Lang 2003; Senda, Murakami & Koyama 2003, and references therein).
. Gosachinski (1985) reported evidence for nonthermal radio emission, presumably from SNRs, asso
ciated with several bright, thermal Galactic sources. Some of these sources have been included in the
catalogue, following improved observations (but also see Odegard 1986, who questions the reliability of
some of Gosachinski's results).
. G300.1+9.4, a possible SNR nearly 2 # in diameter reported by Dubner, Colomb & Giacani (1986).
. Routledge & Vaneldik (1988) report a possible faint radio shell SNR nearly 2 # in diameter, near the
young pulsar PSR 1930+22 -- see also GomezGonzalez & del Romero (1983), who report a smaller
(about 40 arcmin) possible SNR (G57.1+1.7) associated with this pulsar, and see Caswell, Landecker &
Feldman (1985) and Kovalenko (1989).
. Five possible remnants (G45.9--0.1, G71.6--0.5, G72.2--0.3, G83.0--0.2 and G85.2--1.2) of the eleven
reported by Taylor, Wallace & Goss (1992) from a radio survey of part of the Galactic plane. (Four of
the other possible SNRs reported by Taylor et al., are included in the catalogue as G55.0+0.3, G59.5+0.1,
G63.7+1.1 and G76.9+1.0.)
. A faint, poorly defined possible remnant G41.1+1.2 reported by Gorham, Kulkarni & Prince (1993).
. G104.7+2.8, a possible SNR reported by Green & Joncas (1994) from radio observations. However,
recent observations at 10.7 GHz (Wolfgang Reich, private communication) cast doubt on this identifica
tion, as they do not support a nonthermal radio spectrum for the source.
. G355.4+0.7, G356.6+0.1, G357.1--0.2, G358.1+1.0, G358.5--0.9, G358.7+0.7, G359.2--1.1, G3.1--0.6
and G4.2+0.0, which are among the possible SNRs listed by Gray (1994b) from radio observations
near the Galactic centre. See also Roy & Pramesh Rao (2002) who present additional observations
of G356.30.3, G356.6+0.1, G357.10.2 and G3.1--0.6 which they consider as possible SNRs, and
Bhatnagar (2002) for additional observations of G4.2+0.0 which appears to be a thermal source.
. Duncan et al. (1995) and Duncan et al. (1997) list several largescale (1.5 to 10 degree), and smaller,
low radio surfacebrightness candidate SNRs from the Parkes 2.4GHz survey of 270 # < l < 360 # .
Several of these candidates have been confirmed as SNRs by subsequent, improved observations, and
are included in the catalogue. (See also Camilio et al. 2004, who detected a young pulsar near one of the
candidate SNRs, G309.8--2.6, and Russeil et al. 2005, who detected optical filaments from one of the
candidates.)
. Whiteoak & Green (1996), from their radio survey of much of the southern Galactic plane, list 16 possi
ble SNRs (G308.4--1.4, G317.5+0.9, G319.9--0.7, G320.6--0.9, G322.7+0.1, G322.9--0.0, G323.2--1.0,
G324.1+0.1, G325.0--0.3, G331.8--0.0, G337.2+0.1, G339.6--0.6, G345.1+0.2, G345.1--0.2,
G348.8+1.1 and G350.1--0.3).
. Several candidate SNRs reported by Combi & Romero (1998), Combi, Romero & Arnal (1998), Combi,
Romero & Benaglia (1998), Punsly et al. (2000) and Combi et al. (2001).
. A possible SNR, near l = 313 # , which is close to an unidentified Galactic plane gray source (see Roberts
et al. 1999), and to a pulsar (Roberts, Romani & Johnston 2001).
. G359.07--0.02, a possible SNR noted by LaRosa et al. (2000).
. Two possible SNRs near G6.4--0.1 (=W28) noted by YusefZadeh et al. (2000).
. Gaensler et al. (2000), in a search for pulsar wind nebulae, found a small shell of radio emission near
PSR B1356--60 -- which they designate G311.28+1.09 -- which may be a supernova remnant.
. A possible SNR, G328.6--0.0, noted by McClureGriffiths et al. (2001) in the test region of the Southern
Galactic Plane Survey.
. G346.5--0.1, an arc of radio emission observed by Gaensler et al. (2001), which is potentially part of a
SNR, but requires further observations to confirm its nature.
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. Giacani et al. (2001) presented observations of a pulsar wind nebula around PSR J1709--4428, which
may be part of the catalogued remnant G343.1--2.3, or may represent another object.
. Several possible SNRs reported by Trushkin (2001), which were identified from Galactic radio surveys
(one of which, G6.1+0.5, is included in the catalogue, due to improved subsequent observations).
. Two possibles SNRs (G336.1--0.2 and G352.2--0.1) discussed briefly by Manchester et al. (2002).
. G282.8--1.2, a possible young SNR noted by Misanovic, Cram & Green (2002).
. Three possible remnants -- G41.5+0.4, G42.0--0.0 and G43.5+0.6 -- identified by Kaplan et al. (2002).
. Two faint SNR candidates shown in Reich (2002).
. A possible faint remnant, G213.0--0.6, noted by Reich, Zhang & Furst (2003), which is not well defined
by current observations (this incorporates one of the faint remnants which was proposed by Bonsignori
Facondi & Tomasi 1979, see above).
. G107.5--1.5, a probable remnant identified at by Kothes (2003), but the full extent of which is not well
defined at present.
. Zhang (2003) identified four candidate SNRs from radio surveys. One of these -- called G41.9+0.04
by Zhang -- is close to one of the possible remnant by Kaplan et al. (2002), see above. A second --
G74.8+0.63 -- which Zhang identified as a possible remnant partly on the basis of its nonthermal radio
spectrum, actually has a flat, thermal radio spectrum, an has long been identified as an HII region (e.g.
Weiler & Shaver 1978; Pineault & Chastenay 1990). Another source -- G47.8+2.03 -- also may have a
thermal radio spectrum, given its published 2.7GHz flux density (Furst et al. 1990b).
. Four possible SNRs -- labelled G5.71--0.08, G6.31+0.54, G15.51--0.15 and G19.13+0.90 -- identified by
Brogan et al. (2006) from deep radio surveys, for which further observations are required to confirm
their nature.
. Helfand et al. (2006) list many SNR candidates in the region 5 # < l < 32 # , |b| < 0 # .8 from MAGPIS.
2.3.2 UV/Optical/Infrared
. A possible SNR overlapping G296.1--0.5, identified from optical (and Xray) observations by Hutchings,
Crampton & Cowley (1981).
. A SNR (G260.4--3.3) about 4 arcmin in diameter within the Puppis A remnant identified optically by
Winkler et al. (1989). This has not been detected at radio wavelengths (see Dubner et al. 1991).
. A possible SNR (G32.1+0.1) reported from optical spectroscopy by Thompson, Djorgovski & de Car
valho (1991), following up radio and infrared observations of Jones, Garwood & Dickey (1988).
. G75.5+2.4, a possible large (about 2 # ) old SNR in Cygnus suggested by NicholsBohlin & Fesen (1993)
from infrared and optical observations (see also Dewdney & Lozinskaya 1994; Marston 1996; Esipov
et al. 1996).
. A possible optical SNR (G247.8+4.9) noted by Weinberger (1995), which may be Balmer dominated
(see also Weinberger et al. 1998 and Zanin & Kerber 2000).
. An optical shell around the Coalsack Nebula (near l = 300 # , b = 0 # ) identified by Walker & Zealey
(1998). This coincides with one of the large possible SNRs suggested by Duncan et al. (1995), from
radio observations.
. Two possible SNRs, G340.5+0.7 and G342.1+0.1, identified by Walker, Zealey & Parker (2001) from
filaments seen in Ha survey observations.
. A probably SNR which was identified by Bally & Reipurth (2001) -- which they label as G110.3+11.3
-- from optical filaments (and which is also associated with a large HI and CO cavity, and soft Xray
enhancement).
. A possible remnant, near l = 70 # , b = 2 # noted by Mavromatakis et al. (2002).
. A large, approximately 24 # diameter, optical and Xray loop in Antila (McCullough, Fields & Pavlidou
2002).
. Optical filaments in Pegausus (Boumis et al. 2002) which suggest one or more possible SNRs.
. A possible remnant identified from optical filaments to the NE of the known SNR G116.5+1.1, as ob
served by Mavromatakis et al. (2005).
. A suggested small, young remnant observed by Spitzer (Morris et al. 2006).
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-- vii --
2.3.3 Xray/gray
. H1538--32 a large Xray source in Lupus, near l = 307 # , b = +20 # (Riegler, Agrawal & Gull 1980; see
also Colomb, Dubner & Giacani 1984; Gahm et al. 1990) which is a possible old SNR;
. G189.6+3.3, a faint, possible SNR overlapping G189.1+3.0 (=IC443) identified by Asaoka & Aschen
bach (1994) from ROSAT Xray observations.
. G117.7+0.6, a faint shell of soft Xray emission near CTB 1 (=G116.9+0.2), which contains a pulsar
(Hailey & Craig 1995; see also Craig, Hailey & Pisarski 1997).
. A possible SNR identified in Xrays around the pulsar B1828--13 (see Finley, Srinivasan & Park 1996).
. A possible, large SNR, G69.4+1.2, identified as an Xray shell by Yoshita, Miyata & Tsunemi (1999,
2000). See also Mavromatakis, Boumis & Paleologou (2002).
. Possible SNRs identified in the ROSAT AllSky Survey are discussed briefly by Schaudel et al. (2002).
. G0.570--0.018 a small ring of Xray emission near the Galactic Centre, which has been proposed as a
very young remnant by Senda, Murakami & Koyama (2002). See also Senda, Murakami & Koyama
(2003), who identify other possible SNRs near the Galactic Centre from their Xray emission, and Re
naud et al. (2006).
. Two probable SNRs (G25.5+0.0 and G26.6--0.1) identified by Bamba et al. (2003) from their hard Xray
emission.
. Five of the first quadrant candidate SNRs identified by Ueno et al. (2004) from the ASCA Galactic Plane
Survey (see also Yamuguchi et al. 2004). Two of the candidates listed by Ueno et al. are included in the
catalogue (as G28.6--0.1 and G32.4+0.1), as additional observations confirm their nature.
. A possible SNR identified from Xray at gray observations (Malizia et al. 2005).
2.3.4 Other
. G287.8--0.5, which is associated with h Carinae, was listed in Version I as a SNR, but was removed from
the catalogue in Version II as its parameters are uncertain (see Jones 1973; Retallack 1984; Tateyama,
Strauss & Kaufmann 1991; and the discussion in Version II).
. G359.2--0.8 (the `mouse'), near the Galactic centre, which has been suggested as being analogous to the
central region of CTB 80 (=G69.0+2.7) by Predehl & Kulkarni (1995), i.e. a pulsar powered nebula (see
also Camilo et al. 2002).
It should also be noted that: (a) some large radio continuum and HI loops in the Galactic plane (e.g. Berkhuijsen
1973) may be parts of very large, old SNRs, but they have not been included in the catalogue (see also Combi et
al. 1995; Maciejewski et al. 1996; Kim & Koo 2000; Normandeau et al. 2000; Woermann, Gaylard & Otrupcek
2001; Stil & Irwin 2001; Uyanker & Kothes 2002); (b) some large (> 10 # ) regions of Xray emission that are
indicative of a SNR are not included in the catalogue (e.g. the Monogem ring, near l = 203 # , b = +12 # , see
Nousek et al. 1981, Plucinsky et al. 1996, Thorsett et al. 2003, Amenomori et al. 2005, and references therein,
plus Weinberger, Temporin & Stecklum 2006, for observations of optical filaments; in the Gum Nebula near
l = 250 # , b = 0 # , see Leahy, Nousek & Garmire 1992, and also see Reynolds 1976, Dubner et al. 1992, Duncan
et al. 1996, Reynoso & Dubner 1997, Heiles 1998; in Eridanus near l = 200 # , b = --40 # , see Naranan et al.
1976, Burrows et al. 1993, Snowden et al. 1995, Heiles 1998, Boumis et al. 2001); (c) the distinction between
filledcentre remnants and pulsar wind nebula is not clear, and isolated, generally faint, pulsar wind nebulae are
also not included in the catalogue (e.g. Gaensler et al. 1998, Giacani et al. 2001, Jones, Stappers & Gaensler
2002, Wang, Lu & lang 2002, Braje et al. 2003; Gaensler et al. 2003, Gaensler et al. 2004, Hessels et al. 2004).
2.4 Questionable SNRs listed in the catalogue
As noted in Versions II and IV of the catalogue, the following sources are listed as SNRs, although, as dis
cussed in each case, the identifications are not certain: G5.4--1.2, G39.7--2.0 (=W50), G65.7+1.2 (=DA 495),
G69.0+2.7 (=CTB 80), G318.9+0.4 and G357.7--0.1. The nature of G76.9+1.0 (an unusual radio source simi
lar to G65.7+1.2), and of G354.1+0.1 (which appears may be similar to G357.7--0.1 (=MHS 17--39)) are also
uncertain (see Landecker, Higgs & Wendker 1993 and Frail, Goss & Whiteoak 1994).
There are also some objects that have been identified as SNRs and are listed in the catalogue, although
they have been barely resolved in the available observations, or are faint, and have not been well separated from
confusing background or nearby thermal emission, and their identification as SNRs, or at least their parameters
remain uncertain.
2006 April

-- viii --
Acknowledgements
I am grateful to the many colleagues who have commented on previous version of the catalogue, and have brought
errors and omissions to my attention. I am happy to receive feedback from users of the catalogue. This research
has made use of NASA's Astrophysics Data System Bibliographic Services.
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2006 April

Table I -- I -- Summary listings
l b RA (J2000.0) Dec size type Flux at spectral other
(h m s) ( # # ) /arcmin 1 GHz/Jy index name(s)
0.0 +0.0 17 45 44 --29 00 3.5 2.5 S 100? 0.8? Sgr A East
0.3 +0.0 17 46 15 --28 38 15 8 S 22 0.6
0.9 +0.1 17 47 21 --28 09 8 C 18? varies
1.0 --0.1 17 48 30 --28 09 8 S 15 0.6?
1.4 --0.1 17 49 39 --27 46 10 S 2? ?
1.9 +0.3 17 48 45 --27 10 1.2 S 0.6 0.7
3.7 --0.2 17 55 26 --25 50 14 11 S 2.3 0.65
3.8 +0.3 17 52 55 --25 28 18 S? 3? 0.6
4.2 --3.5 18 08 55 --27 03 28 S 3.2? 0.6?
4.5 +6.8 17 30 42 --21 29 3 S 19 0.64 Kepler, SN1604, 3C358
4.8 +6.2 17 33 25 --21 34 18 S 3 0.6
5.2 --2.6 18 07 30 --25 45 18 S 2.6? 0.6?
5.4 --1.2 18 02 10 --24 54 35 C? 35? 0.2? Milne 56
5.5 +0.3 17 57 04 --24 00 12 15 S 5.5 0.7
5.9 +3.1 17 47 20 --22 16 20 S 3.3? 0.4?
6.1 +0.5 17 57 29 --23 25 18 12 S 4.5 0.9
6.1 +1.2 17 54 55 --23 05 30 26 F 4.0? 0.3?
6.4 --0.1 18 00 30 --23 26 48 C 310 varies W28
6.4 +4.0 17 45 10 --21 22 31 S 1.3? 0.4?
6.5 --0.4 18 02 11 --23 34 18 S 27 0.6
7.0 --0.1 18 01 50 --22 54 15 S 2.5? 0.5?
7.2 +0.2 18 01 07 --22 38 12 S 2.8 0.6
7.7 --3.7 18 17 25 --24 04 22 S 11 0.32 1814--24
8.3 --0.0 18 04 34 --21 49 5 4 S 1.2 0.6
8.7 --5.0 18 24 10 --23 48 26 S 4.4 0.3
8.7 --0.1 18 05 30 --21 26 45 S? 80 0.5 (W30)
8.9 +0.4 18 03 58 --21 03 24 S 9 0.6
9.7 --0.0 18 07 22 --20 35 15 11 S 3.7 0.6
9.8 +0.6 18 05 08 --20 14 12 S 3.9 0.5
9.9 --0.8 18 10 41 --20 43 12 S 6.7 0.4
10.5 --0.0 18 09 08 --19 47 6 S 0.9 0.6
11.0 --0.0 18 10 04 --19 25 9 11 S 1.3 0.6
11.1 --1.0 18 14 03 --19 46 18 12 S 5.8 0.6
11.1 --0.7 18 12 46 --19 38 11 7 S 1.0 0.7
11.1 +0.1 18 09 47 --19 12 12 10 S 2.3 0.4
11.2 --0.3 18 11 27 --19 25 4 C 22 0.6
11.4 --0.1 18 10 47 --19 05 8 S? 6 0.5
11.8 --0.2 18 12 25 --18 44 4 S 0.7 0.3
12.0 --0.1 18 12 11 --18 37 7? ? 3.5 0.7
12.2 +0.3 18 11 17 --18 10 5 6 S 0.8 0.7
12.5 +0.2 18 12 14 --17 55 5 6 C? 0.6 0.4
12.7 --0.0 18 13 19 --17 54 6 S 0.8 0.8
12.8 --0.0 18 13 37 --17 49 3 S 0.8 0.5
13.3 --1.3 18 19 20 --18 00 70 40 S? ? ?
13.5 +0.2 18 14 14 --17 12 5 4 S 3.5? 1.0?
2006 April

Table I -- II -- Summary listings
l b RA (J2000.0) Dec size type Flux at spectral other
(h m s) ( # # ) /arcmin 1 GHz/Jy index name(s)
14.1 --0.1 18 15 52 --16 34 6 5 S 0.5 0.6
14.3 +0.1 18 15 58 --16 27 5 4 S 0.6 0.4
15.1 --1.6 18 24 00 --16 34 30 24 S 5.5? 0.8?
15.4 +0.1 18 18 02 --15 27 14 15 S 5.6 0.6
15.9 +0.2 18 18 52 --15 02 7 5 S? 5 0.6?
16.0 --0.5 18 21 56 --15 14 15 10 S 2.7 0.6
16.2 --2.7 18 28 50 --16 11 17 S 2 0.5
16.4 --0.5 18 22 38 --14 55 13 13 S 4.6 0.7
16.7 +0.1 18 20 56 --14 20 4 C 3.0 0.6
16.8 --1.1 18 25 20 --14 46 30 24? ? 2? ?
17.0 --0.0 18 21 57 --14 08 5 S 0.5 0.5
17.4 --2.3 18 30 55 --14 52 24? S 4.8? 0.8?
17.4 --0.1 18 23 08 --13 46 6 S 0.4 0.7
17.8 --2.6 18 32 50 --14 39 24 S 4.0? 0.3?
18.1 --0.1 18 24 34 --13 11 8 S 4.6 0.5
18.6 --0.2 18 25 55 --12 50 6 S 1.4 0.4
18.8 +0.3 18 23 58 --12 23 17 11 S 33 0.4 Kes 67
18.9 --1.1 18 29 50 --12 58 33 C? 37 varies
19.1 +0.2 18 24 56 --12 07 27 S 10 0.5
20.0 --0.2 18 28 07 --11 35 10 F 10 0.0
20.4 +0.1 18 27 51 --11 00 8 S 3.1 0.4
21.0 --0.4 18 31 12 --10 47 9 7 S 1.1 0.6
21.5 --0.9 18 33 33 --10 35 4 C 6? 0.0
21.5 --0.1 18 30 50 --10 09 5 S 0.4 0.5
21.8 --0.6 18 32 45 --10 08 20 S 69 0.5 Kes 69
22.7 --0.2 18 33 15 --09 13 26 S? 33 0.6
23.3 --0.3 18 34 45 --08 48 27 S 70 0.5 W41
23.6 +0.3 18 33 03 --08 13 10? ? 8? 0.3
24.7 --0.6 18 38 43 --07 32 15? S? 8 0.5
24.7 +0.6 18 34 10 --07 05 30 15 C? 20? 0.2?
27.4 +0.0 18 41 19 --04 56 4 S 6 0.68 4C--04.71
27.8 +0.6 18 39 50 --04 24 50 30 F 30 varies
28.6 --0.1 18 43 55 --03 53 13 9 S 3? ?
28.8 +1.5 18 39 00 --02 55 100? S? ? 0.4?
29.6 +0.1 18 44 52 --02 57 5 S 1.5? 0.5?
29.7 --0.3 18 46 25 --02 59 3 C 10 0.7 Kes 75
30.7 --2.0 18 54 25 --02 54 16 ? 0.5? 0.7?
30.7 +1.0 18 44 00 --01 32 24 18 S? 6 0.4
31.5 --0.6 18 51 10 --01 31 18? S? 2? ?
31.9 +0.0 18 49 25 --00 55 7 5 S 24 0.49 3C391
32.0 --4.9 19 06 00 --03 00 60? S? 22? 0.5? 3C396.1
32.1 --0.9 18 53 10 --01 08 40? C? ? ?
32.4 +0.1 18 50 05 --00 25 6 S 0.25? ?
32.8 --0.1 18 51 25 --00 08 17 S? 11? 0.2? Kes 78
33.2 --0.6 18 53 50 --00 02 18 S 3.5 varies
2006 April

Table I -- III -- Summary listings
l b RA (J2000.0) Dec size type Flux at spectral other
(h m s) ( # # ) /arcmin 1 GHz/Jy index name(s)
33.6 +0.1 18 52 48 +00 41 10 S 22 0.5 Kes 79, 4C00.70, HC13
34.7 --0.4 18 56 00 +01 22 35 27 C 230 0.30 W44, 3C392
36.6 --0.7 19 00 35 +02 56 25? S? ? ?
36.6 +2.6 18 48 49 +04 26 17 13? S 0.7? 0.5?
39.2 --0.3 19 04 08 +05 28 8 6 C 18 0.6 3C396, HC24, NRAO 593
39.7 --2.0 19 12 20 +04 55 120 60 ? 85? 0.7? W50, SS433
40.5 --0.5 19 07 10 +06 31 22 S 11 0.5
41.1 --0.3 19 07 34 +07 08 4.5 2.5 S 22 0.48 3C397
42.8 +0.6 19 07 20 +09 05 24 S 3? 0.5?
43.3 --0.2 19 11 08 +09 06 4 3 S 38 0.48 W49B
43.9 +1.6 19 05 50 +10 30 60? S? 8.6? 0.2?
45.7 --0.4 19 16 25 +11 09 22 S 4.2? 0.4?
46.8 --0.3 19 18 10 +12 09 17 13 S 14 0.5 (HC30)
49.2 --0.7 19 23 50 +14 06 30 S? 160? 0.3? (W51)
53.6 --2.2 19 38 50 +17 14 33 28 S 8 0.75 3C400.2, NRAO 611
54.1 +0.3 19 30 31 +18 52 1.5 F? 0.5 0.1
54.4 --0.3 19 33 20 +18 56 40 S 28 0.5 (HC40)
55.0 +0.3 19 32 00 +19 50 20 15? S 0.5? 0.5?
55.7 +3.4 19 21 20 +21 44 23 S 1.4 0.6
57.2 +0.8 19 34 59 +21 57 12? S? 1.8? ? (4C21.53)
59.5 +0.1 19 42 33 +23 35 5 S 3? ?
59.8 +1.2 19 38 55 +24 19 20 16? ? 1.6 0.5
63.7 +1.1 19 47 52 +27 45 8 F 1.8 0.3
65.1 +0.6 19 54 40 +28 35 90 50 S 6 0.6
65.3 +5.7 19 33 00 +31 10 310 240 S? 52? 0.6?
65.7 +1.2 19 52 10 +29 26 18 ? 5.1 0.6 DA 495
67.7 +1.8 19 54 32 +31 29 9 S 1.4 0.3
68.6 --1.2 20 08 40 +30 37 28 25? ? 0.7? 0.0?
69.0 +2.7 19 53 20 +32 55 80? ? 120? varies CTB 80
69.7 +1.0 20 02 40 +32 43 16 S 1.6 0.8
73.9 +0.9 20 14 15 +36 12 22? S? 9? 0.3?
74.0 --8.5 20 51 00 +30 40 230 160 S 210 varies Cygnus Loop
74.9 +1.2 20 16 02 +37 12 8 6 F 9 varies CTB 87
76.9 +1.0 20 22 20 +38 43 12 9 ? 2 0.6
78.2 +2.1 20 20 50 +40 26 60 S 340 0.5 DR4, g Cygni SNR
82.2 +5.3 20 19 00 +45 30 95 65 S 120? 0.5? W63
84.2 --0.8 20 53 20 +43 27 20 16 S 11 0.5
84.9 +0.5 20 50 30 +44 53 6 S 0.8 0.4
85.4 +0.7 20 50 40 +45 22 24 S ? 0.5?
85.9 --0.6 20 58 40 +44 53 24 S ? 0.5?
89.0 +4.7 20 45 00 +50 35 120 90 S 220 0.40 HB21
93.3 +6.9 20 52 25 +55 21 27 20 S 9 0.54 DA 530, 4C(T)55.38.1
93.7 --0.2 21 29 20 +50 50 80 S 65 0.4 CTB 104A, DA 551
94.0 +1.0 21 24 50 +51 53 30 25 S 15 0.4 3C434.1
96.0 +2.0 21 30 30 +53 59 26 S 0.15? 0.7?
2006 April

Table I -- IV -- Summary listings
l b RA (J2000.0) Dec size type Flux at spectral other
(h m s) ( # # ) /arcmin 1 GHz/Jy index name(s)
106.3 +2.7 22 27 30 +60 50 60 24 C? 6 0.6
109.1 --1.0 23 01 35 +58 53 28 S 20 0.50 CTB 109
111.7 --2.1 23 23 26 +58 48 5 S 2720 0.77 Cassiopeia A, 3C461
113.0 +0.2 23 36 35 +61 22 40 17? ? ? ?
114.3 +0.3 23 37 00 +61 55 90 55 S 6? 0.3?
116.5 +1.1 23 53 40 +63 15 80 60 S 11? 0.8?
116.9 +0.2 23 59 10 +62 26 34 S 9? 0.5? CTB 1
119.5 +10.2 00 06 40 +72 45 90? S 36 0.6 CTA 1
120.1 +1.4 00 25 18 +64 09 8 S 56 0.61 Tycho, 3C10, SN1572
126.2 +1.6 01 22 00 +64 15 70 S? 7 varies
127.1 +0.5 01 28 20 +63 10 45 S 13 0.6 R5
130.7 +3.1 02 05 41 +64 49 9 5 F 33 0.10 3C58, SN1181
132.7 +1.3 02 17 40 +62 45 80 S 45 0.4 HB3
156.2 +5.7 04 58 40 +51 50 110 S 5 0.5
160.9 +2.6 05 01 00 +46 40 140 120 S 110 0.6 HB9
166.0 +4.3 05 26 30 +42 56 55 35 S 7? 0.4? VRO 42.05.01
179.0 +2.6 05 53 40 +31 05 70 S? 7 0.4
180.0 --1.7 05 39 00 +27 50 180 S 65 varies S147
182.4 +4.3 06 08 10 +29 00 50 S 1.2 0.4
184.6 --5.8 05 34 31 +22 01 7 5 F 1040 0.30 Crab Nebula, 3C144, SN1054
189.1 +3.0 06 17 00 +22 34 45 C 160 0.36 IC443, 3C157
192.8 --1.1 06 09 20 +17 20 78 S 20? 0.6? PKS 0607+17
205.5 +0.5 06 39 00 +06 30 220 S 160 0.5 Monoceros Nebula
206.9 +2.3 06 48 40 +06 26 60 40 S? 6 0.5 PKS 0646+06
260.4 --3.4 08 22 10 --43 00 60 50 S 130 0.5 Puppis A, MSH 08--44
261.9 +5.5 09 04 20 --38 42 40 30 S 10? 0.4?
263.9 --3.3 08 34 00 --45 50 255 C 1750 varies Vela (XYZ)
266.2 --1.2 08 52 00 --46 20 120 S 50? 0.3? RX J0852.0--4622
272.2 --3.2 09 06 50 --52 07 15? S? 0.4 0.6
279.0 +1.1 09 57 40 --53 15 95 S 30? 0.6?
284.3 --1.8 10 18 15 --59 00 24? S 11? 0.3? MSH 10--53
286.5 --1.2 10 35 40 --59 42 26 6 S? 1.4? ?
289.7 --0.3 11 01 15 --60 18 18 14 S 6.2 0.2?
290.1 --0.8 11 03 05 --60 56 19 14 S 42 0.4 MSH 11--61A
291.0 --0.1 11 11 54 --60 38 15 13 C 16 0.29 (MSH 11--62)
292.0 +1.8 11 24 36 --59 16 12 8 C 15 0.4 MSH 11--54
292.2 --0.5 11 19 20 --61 28 20 15 S 7 0.5
293.8 +0.6 11 35 00 --60 54 20 C 5? 0.6?
294.1 --0.0 11 36 10 --61 38 40 S >2? ?
296.1 --0.5 11 51 10 --62 34 37 25 S 8? 0.6?
296.5 +10.0 12 09 40 --52 25 90 65 S 48 0.5 PKS 1209--51/52
296.8 --0.3 11 58 30 --62 35 20 14 S 9 0.6 1156--62
298.5 --0.3 12 12 40 --62 52 5? ? 5? 0.4?
298.6 --0.0 12 13 41 --62 37 12 9 S 5? 0.3
299.2 --2.9 12 15 13 --65 30 18 11 S 0.5? ?
2006 April

Table I -- V -- Summary listings
l b RA (J2000.0) Dec size type Flux at spectral other
(h m s) ( # # ) /arcmin 1 GHz/Jy index name(s)
299.6 --0.5 12 21 45 --63 09 13 S 1.0? ?
301.4 --1.0 12 37 55 --63 49 37 23 S 2.1? ?
302.3 +0.7 12 45 55 --62 08 17 S 5? 0.4?
304.6 +0.1 13 05 59 --62 42 8 S 14 0.5 Kes 17
308.1 --0.7 13 37 37 --63 04 13 S 1.2? ?
308.8 --0.1 13 42 30 --62 23 30 20? C? 15? 0.4?
309.2 --0.6 13 46 31 --62 54 15 12 S 7? 0.4?
309.8 +0.0 13 50 30 --62 05 25 19 S 17 0.5
310.6 --0.3 13 58 00 --62 09 8 S 5? ? Kes 20B
310.8 --0.4 14 00 00 --62 17 12 S 6? ? Kes 20A
311.5 --0.3 14 05 38 --61 58 5 S 3? 0.5
312.4 --0.4 14 13 00 --61 44 38 S 45 0.36
312.5 --3.0 14 21 00 --64 12 18 20 S 3.5? ?
315.4 --2.3 14 43 00 --62 30 42 S 49 0.6 RCW 86, MSH 14--63
315.4 --0.3 14 35 55 --60 36 24 13 ? 8 0.4
315.9 --0.0 14 38 25 --60 11 25 14 S 0.8? ?
316.3 --0.0 14 41 30 --60 00 29 14 S 20? 0.4 (MSH 14--57)
317.3 --0.2 14 49 40 --59 46 11 S 4.7? ?
318.2 +0.1 14 54 50 --59 04 40 35 S >3.9? ?
318.9 +0.4 14 58 30 --58 29 30 14 C 4? 0.2?
320.4 --1.2 15 14 30 --59 08 35 C 60? 0.4 MSH 15--52, RCW 89
320.6 --1.6 15 17 50 --59 16 60 30 S ? ?
321.9 --1.1 15 23 45 --58 13 28 S >3.4? ?
321.9 --0.3 15 20 40 --57 34 31 23 S 13 0.3
322.5 --0.1 15 23 23 --57 06 15 C 1.5 0.4
323.5 +0.1 15 28 42 --56 21 13 S 3? 0.4?
326.3 --1.8 15 53 00 --56 10 38 C 145 varies MSH 15--56
327.1 --1.1 15 54 25 --55 09 18 C 7? ?
327.4 +0.4 15 48 20 --53 49 21 S 30? 0.6 Kes 27
327.4 +1.0 15 46 48 --53 20 14 S 1.9? ?
327.6 +14.6 15 02 50 --41 56 30 S 19 0.6 SN1006, PKS 1459--41
328.4 +0.2 15 55 30 --53 17 5 F 15 0.12 (MSH 15--57)
329.7 +0.4 16 01 20 --52 18 40 33 S >34? ?
330.0 +15.0 15 10 00 --40 00 180? S 350? 0.5? Lupus Loop
330.2 +1.0 16 01 06 --51 34 11 S? 5? 0.3
332.0 +0.2 16 13 17 --50 53 12 S 8? 0.5
332.4 --0.4 16 17 33 --51 02 10 S 28 0.5 RCW 103
332.4 +0.1 16 15 20 --50 42 15 S 26 0.5 MSH 16--51, Kes 32
335.2 +0.1 16 27 45 --48 47 21 S 16 0.5
336.7 +0.5 16 32 11 --47 19 14 10 S 6 0.5
337.0 --0.1 16 35 57 --47 36 1.5 S 1.5 0.6? (CTB 33)
337.2 --0.7 16 39 28 --47 51 6 S 2? 0.7
337.2 +0.1 16 35 55 --47 20 3 2 ? 1.5? ?
337.3 +1.0 16 32 39 --46 36 15 12 S 16 0.55 Kes 40
337.8 --0.1 16 39 01 --46 59 9 6 S 18 0.5 Kes 41
2006 April

Table I -- VI -- Summary listings
l b RA (J2000.0) Dec size type Flux at spectral other
(h m s) ( # # ) /arcmin 1 GHz/Jy index name(s)
338.1 +0.4 16 37 59 --46 24 15? S 4? 0.4
338.3 --0.0 16 41 00 --46 34 8 S 7? ?
338.5 +0.1 16 41 09 --46 19 9 ? 12? ?
340.4 +0.4 16 46 31 --44 39 10 7 S 5 0.4
340.6 +0.3 16 47 41 --44 34 6 S 5? 0.4?
341.2 +0.9 16 47 35 --43 47 16 22 C 1.5? 0.6?
341.9 --0.3 16 55 01 --44 01 7 S 2.5 0.5
342.0 --0.2 16 54 50 --43 53 12 9 S 3.5? 0.4?
342.1 +0.9 16 50 43 --43 04 10 9 S 0.5? ?
343.0 --6.0 17 25 00 --46 30 250 S ? ? RCW 114
343.1 --2.3 17 08 00 --44 16 32? C? 8? 0.5?
343.1 --0.7 17 00 25 --43 14 27 21 S 7.8 0.55
344.7 --0.1 17 03 51 --41 42 10 C? 2.5? 0.5
345.7 --0.2 17 07 20 --40 53 6 S 0.6? ?
346.6 --0.2 17 10 19 --40 11 8 S 8? 0.5?
347.3 --0.5 17 13 50 --39 45 65 55 S? ? ?
348.5 --0.0 17 15 26 --38 28 10? S? 10? 0.4?
348.5 +0.1 17 14 06 --38 32 15 S 72 0.3 CTB 37A
348.7 +0.3 17 13 55 --38 11 17? S 26 0.3 CTB 37B
349.2 --0.1 17 17 15 --38 04 9 6 S 1.4? ?
349.7 +0.2 17 17 59 --37 26 2.5 2 S 20 0.5
350.0 --2.0 17 27 50 --38 32 45 S 26 0.4
351.2 +0.1 17 22 27 --36 11 7 C? 5? 0.4
351.7 +0.8 17 21 00 --35 27 18 14 S 10? ?
351.9 --0.9 17 28 52 --36 16 12 9 S 1.8? ?
352.7 --0.1 17 27 40 --35 07 8 6 S 4 0.6
353.9 --2.0 17 38 55 --35 11 13 S 1? 0.5?
354.1 +0.1 17 30 28 --33 46 15 3? C? ? varies?
354.8 --0.8 17 36 00 --33 42 19 S 2.8? ?
355.6 --0.0 17 35 16 --32 38 8 6 S 3? ?
355.9 --2.5 17 45 53 --33 43 13 S 8 0.5
356.2 +4.5 17 19 00 --29 40 25 S 4 0.7
356.3 --0.3 17 37 56 --32 16 11 7 S 3? ?
356.3 --1.5 17 42 35 --32 52 20 15 S 3? ?
357.7 --0.1 17 40 29 --30 58 8 3? ? 37 0.4 MSH 17--39
357.7 +0.3 17 38 35 --30 44 24 S 10 0.4?
358.0 +3.8 17 26 00 --28 36 38 S 1.5? ?
359.0 --0.9 17 46 50 --30 16 23 S 23 0.5
359.1 --0.5 17 45 30 --29 57 24 S 14 0.4?
359.1 +0.9 17 39 36 --29 11 12 11 S 5? ?
2006 April

Table II Other names for SNRs
g Cygni SNR G78.2+2.1 HB3 G132.7+1.3 NRAO 593 G39.2--0.3
HB9 G160.9+2.6 NRAO 611 G53.6--2.2
1156--62 G296.8--0.3 HB21 G89.0+4.7
1814--24 G7.7--3.7 PKS 0607+17 G192.8--1.1
HC13 G33.6+0.1 PKS 0646+06 G206.9+2.3
3C10 G120.1+1.4 HC24 G39.2--0.3 PKS 1209--51/52 G296.5+10.0
3C58 G130.7+3.1 (HC30) G46.8--0.3 PKS 1459--41 G327.6+14.6
3C144 G184.6--5.8 (HC40) G54.4--0.3
3C157 G189.1+3.0 Puppis A G260.4--3.4
3C358 G4.5+6.8 IC443 G189.1+3.0
3C391 G31.9+0.0 R5 G127.1+0.5
3C392 G34.7--0.4 Kepler G4.5+6.8
3C396 G39.2--0.3 RCW 86 G315.4--2.3
3C396.1 G32.0--4.9 Kes 17 G304.6+0.1 RCW 89 G320.4--1.2
3C397 G41.1--0.3 Kes 20A G310.6--0.3 RCW 103 G332.4--0.4
3C400.2 G53.6--2.2 Kes 20B G310.8--0.4 RCW 114 G343.0--6.0
3C434.1 G94.0+1.0 Kes 27 G327.4+0.4
3C461 G111.7--2.1 Kes 32 G332.4+0.1 RX J0852.0--4622 G266.2--1.2
Kes 40 G337.3+1.0
4C--04.71 G27.4+0.0 Kes 41 G337.8--0.1 S147 G180.0--1.7
4C00.70 G33.6+0.1 Kes 67 G18.8+0.3
(4C21.53) G57.2+0.8 Kes 69 G21.8--0.6 SN1006 G327.6+14.6
4C(T)55.38.1 G93.3+6.9 Kes 75 G29.7--0.3 SN1054 G184.6--5.8
Kes 78 G32.8--0.1 SN1181 G130.7+3.1
CTA 1 G119.5+10.2 Kes 79 G33.6+0.1 SN1572 G120.1+1.4
SN1604 G4.5+6.8
CTB 1 G116.9+0.2 Lupus Loop G330.0+15.0
(CTB 33) G337.0--0.1 SS433 G39.7--2.0
CTB 37A G348.5+0.1 MSH 08--44 G260.4--3.4
CTB 37B G348.7+0.3 MSH 10--53 G284.3--1.8 Sgr A East G0.0+0.0
CTB 80 G69.0+2.7 MSH 11--54 G292.0+1.8
CTB 87 G74.9+1.2 MSH 11--61A G290.1--0.8 Tycho G120.1+1.4
CTB 104A G93.7--0.2 (MSH 11--62) G291.0--0.1
CTB 109 G109.1--1.0 (MSH 14--57) G316.3--0.0 Vela (XYZ) G263.9--3.3
MSH 14--63 G315.4--2.3
Cassiopeia A G111.7--2.1 MSH 15--52 G320.4--1.2 VRO 42.05.01 G166.0+4.3
MSH 15--56 G326.3--1.8
Crab Nebula G184.6--5.8 (MSH 15--57) G328.4+0.2 W28 G6.4--0.1
MSH 16--51 G332.4+0.1 (W30) G8.7--0.1
Cygnus Loop G74.0--8.5 MSH 17--39 G357.7--0.1 W41 G23.3--0.3
W44 G34.7--0.4
DA 495 G65.7+1.2 Milne 56 G5.4--1.2 W49B G43.3--0.2
DA 530 G93.3+6.9 W50 G39.7--2.0
DA 551 G93.7--0.2 Monoceros Nebula G205.5+0.5 (W51) G49.2--0.7
W63 G82.2+5.3
DR4 G78.2+2.1
2006 April

Table III Abbreviations used in detailed listings
Journals
A&A Astronomy & Astrophysics
A&AS Astronomy & Astrophysics Supplement
AJ Astronomical Journal
AN Astronomische Nachrichten
ApJ Astrophysical Journal
ApJS Astrophysical Journal Supplement
ApL Astrophysical Letters
ApSS Astrophysics & Space Science
AuJPA Australian Journal of Physics Astrophysical Supplement
AuJPh Australian Journal of Physics
BASI Bulletin of the Astronomical Society of India
JApA Journal of Astrophysics & Astronomy
JRASC Journal of the Royal Astronomical Society of Canada
MNRAS Monthly Notices of the Royal Astronomical Society
PASAu Proceedings of the Astronomical Society of Australia
PASJ Publications of the Astronomical Society of Japan
PASP Publications of the Astronomical Society of the Pacific
RMxAA Revista Mexicana de Astronoma y Astrofsica
SerAJ Serbian Astronomical Journal
SvAL Soviet Astronomy Letters
Proceedings
SNRISM is `Supernova Remnants and the Interstellar Medium', (IAU Colloquium 101), eds Roger
R.S. & Landecker T.L., (Cambridge University Press), 1988.
NSPS is `Neutron Stars, Pulsars, and Supernova Remnants', (MPE Report 278), eds Becker W.,
Lesch H. & Trumper, J., (MaxPlankInstitut fur extraterrestrische Physik, Garching
bei Munchen), 2002.
NSSR is `Neutron Stars in Supernova Remnants', (ASP Conference Series, Volume 271), eds Slane
P.O. & Gaensler B.M., (Astronomical Society of the Pacific, San Fransico), 2002.
XRRC is `XRay and Radio Connections', eds Sjouwerman L.O. & Dyer K.K.,
(available at http://www.aoc.nrao.edu/events/xraydio/), 2005.
Radio Telescopes
5km Cambridge 5km Telescope
6C Cambridge low frequency northern survey
ATCA Australia Telescope Compact Array
BIMA Berkeley--Illinois--Maryland Array
CLFST Cambridge Low Frequency Synthesis Telescope
DRAO Dominion Radio Astrophysical Observatory
FIRST Fleurs Synthesis Telescope
MOST Molonglo Observatory Synthesis Telescope
NRAO National Radio Astronomy Observatory
NRO Nobeyama Radio Observatory
TPT Clark Lake TeepeeTee telescope
VLA Very Large Array
VRO Vermillion River Observatory
WSRT Westerbork Synthesis Radio Telescope
Satellites
HST Hubble Space Telescope
ISO Infrared Space Observatory
ASCA Advanced Satellite for Cosmology and Astrophysics
EXOSAT European Xray Observatory Satellite
ROSAT Rontgensatellit
XMM Xray MultiMirror(Newton)
2006 April