Note: this is an archived version which has been superseded. The current SNR catalogue is at http://www.mrao.cam.ac.uk/surveys/snrs/

A Catalogue of Galactic Supernova Remnants

2001 December version

D.A. Green
Mullard Radio Astronomy Observatory
Cavendish Laboratory
Madingley Road
Cambridge CB3 0HE
UNITED KINGDOM

Contents of this document.

• 1. The Catalogue Format
• 2. Revisions and Notes
  • 2.1 Objects no longer thought to be SNRs
  • 2.2 New SNRs
  • 2.3 Possible and probable SNRs not listed in the catalogue
    • 2.3.1 Radio
    • 2.3.2 UV/Optical/Infra-red
    • 2.3.3 X-ray
    • 2.3.4 Other
  • 2.4 Questionable SNRs listed in the catalogue
• Acknowledgements
• References

Other pages.

• The summary listings of all 231 SNRs.
• The detailed listings of all 231 SNRs.
• A list of other names for Galactic SNRs.
• The abbreviations for journals/telescopes used in the detailed listings.
• A frames interface to the catalogue.
• How to get a paper version of the catalogue.
• A feedback comment form.

1. The Catalogue Format

This, the 2001 December version of the catalogue, contains 231 SNRs (which is six more than in the previous, 2000 August, version: ten new remnants have been added, and four entries removed), with about 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 available. 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 available.
• Spectral Index of the integrated radio emission from the remnant, 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 confidence.
• 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 morphology', 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.

2. Revisions and Notes

2.1 Objects no longer thought to be SNRs

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) -- have been removed from this version 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).

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 eta 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. (2001a), is incorporated into the larger catalogued remnant G106.3+2.7.

2.2 New SNRs

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 have been added to this version of the catalogue.

• Three high latitude SNRs (G4.8+6.2, G356.2+4.5 and G358.0+3.8) -- which were proposed as possible remnants by Duncan et al. (1997) -- which were confirmed as remnants by Bhatnagar (2000), from radio observations made with the GMRT. (Note that G4.8+6.2 was referred to as G4.5+6.2 by Duncan et al. 1997)
• G28.6-0.1 -- which had previously been listed as a possible SNR, based on the radio observations of Helfand et al. (1989) -- has now been included in the catalogue, as X-ray observations by Bamba et al. (2001) have confirmed its nature as a SNR.
• Two remnants, G85.4+0.7 and G85.9-0.6, identified from radio observations from the ongoing Canadian Galactic Plane Survey by Kothes et al. (2001).
• G106.3+2.7, a remnant identified from radio observations by Pineault & Joncas (2000) -- this incorporates a smaller proposed remnant (G106.6+2.9) that has been discussed by Halpern et al. (2001a,b) -- see also Kothes, Uyaniker & Pineault (2001).
• G292.2-0.5, around the young pulsar J1119-6127, which was detected at radio wavelength by Crawford et al. (2001), and in X-rays by Pivovaroff et al. (2001).
• G343.0-0.6 (=RCW 114)-- which had been listed in Version I of the catalogue, but was removed as it was poorly defined by the available observations -- has now been included in the catalogue, because of the improved observations of Walker & Zealey (2001).
• A remnant, G353.9-2.0, identified in the NRAO VLA Sky Survey radio data (see Condon et al. 1998) by Green (2001), who presented improved radio observations of this nearly circular shell SNR.

2.3 Possible and probable SNRs not listed in the catalogue

2.3.1 Radio

• 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).
• 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 Galactic centre.
• 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 < 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 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), 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, 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.
• 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.

2.3.1 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 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. 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.

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; 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 & Aschenbach (1994) from ROSAT X-ray observations.
• 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, 2000).

2.3.4 Other

• 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).

2.4 Questionable SNRs listed in the catalogue

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

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