Note: this is an
archived version which has been superseded. The current SNR
catalogue is at
A Catalogue of Galactic Supernova Remnants
2000 August version
Mullard Radio Astronomy Observatory
Cambridge CB3 0HE
Contents of this document.
- The summary listings of all 225 SNRs.
- The detailed listings of all 225 SNRs.
- A list of other names for Galactic
- The abbreviations for journals/telescopes
used in the detailed listings.
- A frames interface to the catalogue.
- How to get a paper version of the
- A feedback comment form.
This catalogue of Galactic supernova remnants (SNRs) is an updated version of
those presented in detail in Green (1984, 1988), in summary form in Green
(1991, 1996) - hereafter Versions I, II, III and IV respectively - and on
the World-Wide-Web (versions of 1995 July, 1996 August and 1998 September).
(Note that Version IV, although published in 1996, was produced in 1993.)
This, the 2000 August version of the catalogue contains 225 SNRs (which is five
more than in the previous, 1998 September, version), with about thousand
references in the detailed listings, plus notes on several dozen possible or
For each remnant in the catalogue the following parameters are given.
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 the
field of 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, 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 Fürst
et al. (1990); 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); 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
- 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
(unlike all previous versions of the catalogue, for which the coordinates were
given for B1950.0).
- Angular Size of the remnant, in arcminutes, usually taken
from the highest resolution radio map available, although for some barely
resolved sources that are thought to be SNRs the only available size is that
from Gaussian models after deconvolution with the observed beam size. 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.
- 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
- Spectral Index of the integrated radio emission from the
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 recent
references in the catalogue entry for more information). In some cases, for
example where the remnant is highly confused with thermal emission, the
spectral index is given as `?' since no value can be deduced with any
- Type of the SNR, either `S', `F' or `C' if the remnant
shows a `shell', `filled-centre' or `composite' (or `combination') radio
structure (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. (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 morphpology',
see Rho & Petre 1998.)
The catalogue is available as a summary listing
of the parameters for each remnant, and as
detailed listings (with references) for each
object. Also see the list of
other names used for these SNRs, and
the list of abbreviations for journals,
proceedings and telescopes used in the detailed listings.
The following objects, which were listed in Version I of the
catalogue were removed because they were no longer thought to be remnants, or
are 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 (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 Version 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
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
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.
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.
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 incorporated 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).
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
- 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 that 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).
- 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.
- 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).
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 have been added to this version of 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.
- G7.0-0.1, a new SNR adjacent to G6.4-0.1 (=W28),
identified from radio observations (see Kassim & Yusef-Zadeh 2000 and
Yusef-Zadeh et al. 2000).
- G16.2-2.7, identified by Trushkin (1999) from radio
- G29.6+0.1, a new SNR found near an AXP (Anomalous X-ray
Pulsar) by Gaensler, Gotthelf & Vasisht (1999) from radio observations.
- G266.2-1.2, which overlaps the Vela SNR, which was
identified by X-ray observations by Aschenbach (1998).
- G347.3-0.5, which was previously suggested as a SNR by
Pfeffermann & Aschenbach (1996) (see also Koyama et al. 1997), which was
clearly confirmed as a SNR by X-ray and other observations made by Slane et al.
- A possible SNR near the Galactic centre reported by Ho et al.
(1985) from radio observations.
- Gosachinskii (1985) reported evidence for non-thermal
radio emission, presumably from SNRs, associated with several bright, thermal
Galactic sources (also see Odegard 1986, who questions the reliability of some
of Gosachinskii'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 shell SNR
nearly 2° in diameter at radio wavelengths, near the young pulsar PSR
1930+22 (see also Gómez-González & 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).
- G28.6-0.2, a possible SNR reported by Helfand et al. (1989)
from radio observations.
- 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.
- 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
- G104.7+2.8, a possible SNR reported by Green & Joncas (1994)
from radio observations. However, recent observations at 10.7 GHz (W. Reich,
private communication) cast doubt on this identification, as they do not
support a non-thermal radio spectrum for the 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 <
- Whiteoak & Green (1996), from their radio survey of much of
the southern Galactic plane, list 16 possible 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) and Combi, Romero & Benaglia (1998).
- G359.09-0.02, a possible SNR noted by LaRosa et al. (2000).
- A possible SNR, G313.3+0.1, near an unidentified
Galactic plane gamma-ray source (see Roberts et al. 1999).
- A likely SNR, called G359.92-0.09, adjacent to
G0.0+0.0 (=Sgr A East) at the Galactic centre, see
Coil & Ho (2000), and references therein.
- G353.9-2.0, a probable SNR I have identified
from the NVSS archive data, details of which are as yet unpublished.
- G343.0-6.0 was listed in Version I as a SNR, identified
optically by Meaburn & Rovithis (1977). However, it was removed from the
catalogue in Version II as its extent is uncertain, and it has not been
identified at other wavelengths (also see Bedford et al. 1984 and Meaburn
et al. 1991).
- 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 Carvalho (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.
- 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.
- H1538-32 a large X-ray source in Lupus, near l=307°,
b=+20° (Riegler, Agrawal & Gull 1980, see also Colomb, Dubner &
Giacani 1984 and 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, and references
- 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 due to an old SNR in Eridanus (Naranan et al. 1976, see
also Burrows et al. 1993, Snowden et al. 1995, Heiles 1998).
- G189.6+3.3, a faint, possible SNR overlapping G189.1+3.0
(=IC443) identified by Asaoka & Aschenbach (1994) from ROSAT X-ray
- G117.7+0.6, a faint shell of soft X-ray emission near CTB1
(=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).
It should also be noted that some radio loops in the Galactic
plane (see, for example, 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), nor have pulsar wind nebulae (see, for example,
Gaensler et al. 1998).
As noted in Versions II and IV of the catalogue, the following sources are
listed as SNRs, although, as discussed 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 similar to G65.7+1.2 (=DA 495)), 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 respectively).
- G287.8-0.5, which is associated with eta 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).
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.
I am grateful to the many colleagues who have commented 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
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Dave Green/MRAO, Cambridge, UK/D.A.Green@mrao.cam.ac.uk