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A Catalogue of
Galactic Supernova Remnants
(2004 January version)
D.A. Green
Mullard Radio Astronomy Observatory, Cavendish Laboratory
Madingley Road, Cambridge CB3 0HE
UNITED KINGDOM
E?mail: D.A.Green@mrao.cam.ac.uk
Please reference this catalogue as follows:
. Green D.A., 2004, Bulletin of the Astronomical Society of India, 32, 335--370.
as this paper -- entitled `Galactic Supernova Remnants: an Updated Catalogue and Some Statistics' -- includes the
summary data as an Appendix. If you make use of the detailed web?based version of the catalogue, then please
also cite:
. Green D.A., 2004, `A Catalogue of Galactic Supernova Remnants (2004 January version)', Mullard
Radio Astronomy Observatory, Cavendish Laboratory, Cambridge, UK (available on the World?Wide?
Web 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) -- hereafter Versions I, II, III and IV respectively --
and on the World?Wide?Web, in versions of 1995 July, 1996 August, 1998 September, 2000 August and 2001
December. (Version IV, although published in 1996, was produced in 1993, and a detailed version of this was
made available on the World?Wide?Web 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 2004 January version of the catalogue, contains 231 SNRs (which is the same number as in the
previous, 2001 December, version: one new remnant has been added, and one has been removed), with over a
thousand references in the detailed listings, plus notes on several dozen 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 almost
always deduced from radio maps rather than from X?ray 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 `filled?centre' remnants the size quoted is for the largest extent of the observed radio emission, not,
as at times has been used by others, the half?width 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 `filled?centre' structure, or `C' if it shows
`composite' (or `combination') radio structure with a combination of shell and filled?centre 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 pulsar?powered, flatter radio spectrum filled?centre components
within shells. However, in recent years improved observations -- particularly in X?rays 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 centrally?brightened X?ray 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 X?ray 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 end of 2003 -- 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 100?m survey at 2.7 GHz of the Galactic plane 358 # < l < 240 # , |b| < 5 # by Reich
et al. (1990) and FØurst et al. (1990a); reviews of the radio spectra of some SNRs by Kassim (1989), Kovalenko,
Pynzar' & Udal'tsov (1994) and Trushkin (1998); the Parkes 64?m 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); reviews of Einstein X?ray 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); and the catalogue by Fesen & Hurford (1996) of UV/optical/infra?red
lines identified in SNRs.
A summary of the data available for all 231 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 Bonsignori?Facondi & 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 soft?gamma repeater -- was
removed from this version of the catalogue, as it is now thought to be radio nebula powered by a stellar wind (see
Gaensler et al. 2001, and references therein).
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 Ward?Thompson & 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?
to?radio 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 & Lanfer
(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 Yusef?Zadeh, 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.
The following remnant has been added to this version of the catalogue.
. G312.5--3.0, which was suspected as a SNR by Duncan et al. (1997), and has been confirmed by im?
proved radio observations by Kane & Vaughan (2003).
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).
. GosachinskiÖÐ (1985) reported evidence for non?thermal radio emission, presumably from SNRs, associ?
ated with several bright, thermal Galactic sources (also see Odegard 1986, who questions the reliability
of some of GosachinskiÖÐ's results).
. G300.1+9.4, a possible SNR nearly 2 # in diameter reported by Dubner, Colomb & Giacani (1986) from
radio observations.
. Routledge & Vaneldik (1988) report a possible faint radio shell SNR nearly 2 # in diameter, near the
young pulsar PSR 1930+22 -- see also GÒomez?GonzÒalez & 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).
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. 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. (Three of
the other possible SNRs reported by Taylor et al., are included in the catalogue as G55.0+0.3, 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) from
radio observations.
. G9.7--0.1, a possible SNR report by Frail, Kassim & Weiler (1994) from radio observations.
. 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 non?thermal 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 G356.3?0.3, G356.6+0.1, G357.1?0.2 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.
. G11.2--1.1, a possible SNR listed by Kovalenko, Pynzar' & Udal'tsov (1994), based on unpublished
radio studies (Trushkin 1988, preprint).
. Duncan et al. (1995) and Duncan et al. (1997) list several large?scale (1.5 to 10 degree), and smaller,
low radio surface?brightness candidate SNRs from the Parkes 2.4?GHz survey of 270 # < l < 360 # .
Several of these candidates have been confirmed as SNRs by subsequent, improved observations, and
are included in the catalogue.
. 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).
. G359.09--0.02, a possible SNR noted by LaRosa et al. (2000).
. A possible SNR, near l = 313 # , which is close to an unidentified Galactic plane g?ray source (see Roberts
et al. 1999), and to a pulsar (Roberts, Romani & Johnston 2001).
. 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 McClure?Griffiths 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.
. 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.
. A possible faint remnant, G213.0--0.6, noted by Reich, Zhang & FØurst (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).
. 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).
. 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 -- has been already noted as a 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 non?thermal 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 2.7?GHz flux density (FØurst et al. 1990b).
2004 January

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2.3.2 UV/Optical/Infra?red
. A possible SNR overlapping G296.1--0.5, identified from optical (and X?ray) 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 Nichols?Bohlin & Fesen (1993)
from infra?red 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.
. 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 X?ray
enhancement).
. A possible remnant, near l = 70 # , b = 2 # noted by Mavromatakis et al. (2002).
. A large, approximately 24 # diameter, optical and X?ray loop in Antila (McCullough, Fields & Pavlidou
2002).
. Optical filaments in Pegausus (Boumis et al. 2002) which suggest one or more possible SNRs in this
region.
2.3.3 X?ray
. H1538--32 a large X?ray 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;
. The Monogem ring, near l = 203 # , b = +12 # , is a possible old SNR (see Nousek et al. 1981; Plucinsky
et al. 1996; Thorsett et al. 2003, and references therein).
. X?ray emission in the Gum Nebula near l = 250 # , b = 0 # (Leahy, Nousek & Garmire 1992, see also
Reynolds 1976, Dubner et al. 1992, Duncan et al. 1996, Reynoso & Dubner 1997, Heiles 1998) which,
together with optical spectroscopy indicate the existence of a possible old remnant in this region.
. An X?ray enhancement near l = 200 # , b = --40 # , which is possibly due to an old SNR in Eridanus
(Naranan et al. 1976; see also Burrows et al. 1993; Snowden et al. 1995; Heiles 1998, Boumis et al.
2001).
. G189.6+3.3, a faint, possible SNR overlapping G189.1+3.0 (=IC443) identified by Asaoka & Aschen?
bach (1994) from ROSAT X?ray observations.
. G117.7+0.6, a faint shell of soft X?ray 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 X?rays around the pulsar B1828--13 (see Finley, Srinivasan & Park 1996).
. A possible, large SNR, G69.4+1.2, identified as an X?ray shell by Yoshita, Miyata & Tsunemi (1999,
2000). See also Mavromatakis, Boumis & Paleologou (2002).
. Possible SNRs identified in the ROSAT All?Sky Survey are discussed briefly by Schaudel et al. (2002).
. G0.570--0.018 a small ring of X?ray 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 X?ray emission.
. Three probable SNRs (G11.0+0.0, G25.5+0.0 and G26.6--0.1) identified by Bamba et al. (2003) from
their hard X?ray emission.
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-- vii --
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 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; UyanÐker & Kothes 2002); (b) the distinction between filled?centre 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; Braje et al. 2003; Gaensler et
al. 2003).
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.
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. No doubt errors remain in this version, and I am always happy to
receive feedback from users of the catalogue. This research has made use of NASA's Astrophysics Data System
Bibliographic Services.
2004 January

-- viii --
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2004 January

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
5.9 +3.1 17 47 20 --22 16 20 S 3.3? 0.4?
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?
7.0 --0.1 18 01 50 --22 54 15 S 2.5? 0.5?
7.7 --3.7 18 17 25 --24 04 22 S 11 0.32 1814--24
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)
9.8 +0.6 18 05 08 --20 14 12 S 3.9 0.5
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
12.0 --0.1 18 12 11 --18 37 7? ? 3.5 0.7
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?
15.1 --1.6 18 24 00 --16 34 30 ' 24 S 5.5? 0.8?
15.9 +0.2 18 18 52 --15 02 7 ' 5 S? 5 0.6?
16.2 --2.7 18 28 50 --16 11 17 S 2 0.5
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? ?
17.4 --2.3 18 30 55 --14 52 24? S 4.8? 0.8?
17.8 --2.6 18 32 50 --14 39 24 S 4.0? 0.3?
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
20.0 --0.2 18 28 07 --11 35 10 F 10 0.0
21.5 --0.9 18 33 33 --10 35 4 C 6? 0.0
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
2004 January

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)
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 0.55 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? ? ?
32.8 --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
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
2004 January

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)
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 0.44 3C434.1
106.3 +2.7 22 27 30 +60 50 60 ' 24 ? 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
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 0.6 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
166.2 +2.5 05 19 00 +41 55 90 ' 70 S 11 0.5 OA 184
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?
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?
2004 January

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)
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? 0.6?
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? ?
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? ?
2004 January

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)
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
337.3 +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
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 ? ?
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? ?
2004 January

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)
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? ?
2004 January

Table II Other names for SNRs
g Cygni SNR G78.2+2.1 DR4 G78.2+2.1 NRAO 593 G39.2--0.3
NRAO 611 G53.6--2.2
1156--62 G296.8--0.3 HB3 G132.7+1.3
1814--24 G7.7--3.7 HB9 G160.9+2.6 OA 184 G166.2+2.5
HB21 G89.0+4.7
3C10 G120.1+1.4 PKS 0607+17 G192.8--1.1
3C58 G130.7+3.1 HC13 G33.6+0.1 PKS 0646+06 G206.9+2.3
3C144 G184.6--5.8 HC24 G39.2--0.3 PKS 1209--51/52 G296.5+10.0
3C157 G189.1+3.0 (HC30) G46.8--0.3 PKS 1459--41 G327.6+14.6
3C358 G4.5+6.8 (HC40) G54.4--0.3
3C391 G31.9+0.0 Puppis A G260.4--3.4
3C392 G34.7--0.4 IC443 G189.1+3.0
3C396 G39.2--0.3 R5 G127.1+0.5
3C396.1 G32.0--4.9 Kepler G4.5+6.8
3C397 G41.1--0.3 RCW 86 G315.4--2.3
3C400.2 G53.6--2.2 Kes 17 G304.6+0.1 RCW 89 G320.4--1.2
3C434.1 G94.0+1.0 Kes 20A G310.6--0.3 RCW 103 G332.4--0.4
3C461 G111.7--2.1 Kes 20B G310.8--0.4 RCW 114 G343.0--6.0
Kes 27 G327.4+0.4
4C--04.71 G27.4+0.0 Kes 32 G332.4+0.1 S147 G180.0--1.7
4C00.70 G33.6+0.1 Kes 40 G337.3+1.0
(4C21.53) G57.2+0.8 Kes 41 G337.8--0.1 SN1006 G327.6+14.6
4C(T)55.38.1 G93.3+6.9 Kes 67 G18.8+0.3 SN1054 G184.6--5.8
Kes 69 G21.8--0.6 SN1181 G130.7+3.1
CTA 1 G119.5+10.2 Kes 75 G29.7--0.3 SN1572 G120.1+1.4
Kes 78 G32.8--0.1 SN1604 G4.5+6.8
CTB 1 G116.9+0.2 Kes 79 G33.6+0.1
(CTB 33) G337.0--0.1 SS433 G39.7--2.0
CTB 37A G348.5+0.1 Lupus Loop G330.0+15.0
CTB 37B G348.7+0.3 Sgr A East G0.0+0.0
CTB 80 G69.0+2.7 MSH 08--44 G260.4--3.4
CTB 87 G74.9+1.2 MSH 10--53 G284.3--1.8 Tycho G120.1+1.4
CTB 104A G93.7--0.2 MSH 11--54 G292.0+1.8
CTB 109 G109.1--1.0 MSH 11--61A G290.1--0.8 Vela (XYZ) G263.9--3.3
(MSH 11--62) G291.0--0.1
Cassiopeia A G111.7--2.1 (MSH 14--57) G316.3--0.0 VRO 42.05.01 G166.0+4.3
MSH 14--63 G315.4--2.3
Crab Nebula G184.6--5.8 MSH 15--52 G320.4--1.2 W28 G6.4--0.1
MSH 15--56 G326.3--1.8 (W30) G8.7--0.1
Cygnus Loop G74.0--8.5 (MSH 15--57) G328.4+0.2 W41 G23.3--0.3
MSH 16--51 G332.4+0.1 W44 G34.7--0.4
DA 495 G65.7+1.2 MSH 17--39 G357.7--0.1 W49B G43.3--0.2
DA 530 G93.3+6.9 W50 G39.7--2.0
DA 551 G93.7--0.2 Milne 56 G5.4--1.2 (W51) G49.2--0.7
W63 G82.2+5.3
Monoceros Nebula G205.5+0.5
2004 January

Table III Abbreviations used in detailed listings
Journals
AcASn Acta Astronomica Sinica
A&A Astronomy & Astrophysics
A&AS Astronomy & Astrophysics Supplement
AJ Astronomical Journal
AN Astronomische Nachrichten
ApJ Astrophysical Journal
ApJS Astrophysical Journal Supplement
AuJPh Australian Journal of Physics
AuJPA Australian Journal of Physics Astrophysical Supplement
JApA Journal of Astrophysics & Astronomy
JRASC Journal of the Royal Astronomical Society of Canada
MNRAS Monthly Notices of the Royal Astronomical Society
Natur Nature
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 AstronomÒÐa y AstrofÒÐsica
Sci Science
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.
NSSR is `Neutron Statrs in Supernova Remnants' (ASP Conference Series, Volume 271), eds Slane
P.O. & Gaensler B.M., (Astronomical Society of the Pacific: San Fransico), 2002.
Radio Telescopes
5km Cambridge 5?km 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 TPT telescope
VLA Very Large Array
VRO Vermillion River Observatory
WSRT Westerbork Synthesis Radio Telescope
Satellites
HST Hubble Space Telescope
ISO Infrared Space Observatory
X?ray:
ASCA Advanced Satellite for Cosmology and Astrophysics
EXOSAT European X?ray Observatory Satellite
ROSAT RØontgensatellit
XMM X?ray Multi?Mirror
2004 January