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A Catalogue of
Galactic Supernova Remnants
(2000 August 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., 2000, `A Catalogue of Galactic Supernova Remnants (2000 August 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), 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 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
(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 avail?
able, 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.
2000 August

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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 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 morphpology', 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 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 ? , jbj < 5 ? by Reich et al. (1990) and FØurst 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 ? , jbj < 5 ? by Duncan
et al. (1995) and Duncan et al. (1997); the Molonglo Galactic plane survey at 843 MHz of 245 ? < l < 355 ? ,
jbj < 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 in SNRs.
A summary of the data available for all 225 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.
2000 August

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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 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 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.
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 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).
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).
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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 have been added to this version of the catalogue.
 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 observations.
 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. (1999).
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.
 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 shell SNR nearly 2 ? in diameter at radio wave?
lengths, near the young pulsar PSR 1930+22 (see also GÒomez?GonzÒalez & del Romero 1983, who re?
port 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.)
2000 August

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 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 ob?
servations 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 ? .
 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 g?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.
2.3.2 UV/Optical/Infra?red
 G343.0 6.0 was listed in Version I as a SNR, identified optically by Meaburn & Rovithis (1977). How?
ever, 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 Hutch?
ings, 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.
2000 August

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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 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 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 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 & Aschen?
bach (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).
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).
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).
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 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).
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 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 re?
ceive feedback from users of the catalogue. This research has made use of NASA's Astrophysics Data System
Bibliographic Services.
2000 August

-- vii --
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2000 August

Table I -- I -- Summary listings
l b RA (J2000.0) Dec size type Flux at spectral other
(h m s) ( ? 0 ) /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? 4? ?
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
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 42 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
10:0 0:3 18 08 39 20 25 8? ? 2.9 0.8
11:2 0:3 18 11 27 19 25 4 C 22 0.49
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
2000 August

Table I -- II -- Summary listings
l b RA (J2000.0) Dec size type Flux at spectral other
(h m s) ( ? 0 ) /arcmin 1 GHz/Jy index name(s)
27:8 +0:6 18 39 50 04 24 50  30 F 30 varies
28:8 +1:5 18 39 00 02 35 100? 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 S 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
2000 August

Table I -- III -- Summary listings
l b RA (J2000.0) Dec size type Flux at spectral other
(h m s) ( ? 0 ) /arcmin 1 GHz/Jy index name(s)
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
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
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 0.3 CTB 104A, DA 551
94:0 +1:0 21 24 50 +51 53 30  25 S 15 0.44 3C434.1
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
112:0 +1:2 23 15 55 +61 50 30? S? 7? 0.6?
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
117:4 +5:0 23 54 20 +67 30 80  60? S? 30? 0.5?
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
152:2 1:2 04 09 40 +49 30 110? S? 16? 0.7?
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 S 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
211:7 1:1 06 45 40 +00 20 70? S? 15? 0.5?
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 02 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?
2000 August

Table I -- IV -- Summary listings
l b RA (J2000.0) Dec size type Flux at spectral other
(h m s) ( ? 0 ) /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
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
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 6 F 16? 0.2 (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
2000 August

Table I -- V -- Summary listings
l b RA (J2000.0) Dec size type Flux at spectral other
(h m s) ( ? 0 ) /arcmin 1 GHz/Jy index name(s)
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 17 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? ?
343:1 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
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
356:3 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?
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? ?
2000 August

Table II Other names for SNRs
g Cygni 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
Kes 27 G327:4 + 0:4 S147 G180:0 1:7
4C 04.71 G27:4 + 0:0 Kes 32 G332:4 + 0:1
4C00.70 G33:6 + 0:1 Kes 40 G337:3 + 1:0 SN1006 G327:6 + 14:6
(4C21.53) G57:2 + 0:8 Kes 41 G337:8 0:1 SN1054 G184:6 5:8
4C(T)55.38.1 G93:3 + 6:9 Kes 67 G18:8 + 0:3 SN1181 G130:7 + 3:1
Kes 69 G21:8 0:6 SN1572 G120:1 + 1:4
CTA 1 G119:5 + 10:2 Kes 75 G29:7 0:3 SN1604 G4:5 + 6:8
Kes 78 G32:8 0:1
CTB 1 G116:9 + 0:2 Kes 79 G33:6 + 0:1 SS433 G39:7 2:0
(CTB 33) G337:0 0:1
CTB 37A G348:5 + 0:1 Lupus Loop G330:0 + 15:0 Sgr A East G0:0 + 0:0
CTB 37B G348:7 + 0:3
CTB 80 G69:0 + 2:7 MSH 08 44 G260:4 3:4 Tycho G120:1 + 1:4
CTB 87 G74:9 + 1:2 MSH 10 53 G284:3 1:8
CTB 104A G93:7 0:2 MSH 11 54 G292:0 + 1:8 Vela (XYZ) G263:9 3:3
CTB 109 G109:1 1:0 MSH 11 61A G290:1 0:8
(MSH 11 62) G291:0 0:1 VRO 42.05.01 G166:0 + 4:3
Cassiopeia A G111:7 2:1 (MSH 14 57) G316:3 0:0
MSH 14 63 G315:4 2:3 W28 G6:4 0:1
Crab Nebula G184:6 5:8 MSH 15 52 G320:4 1:2 (W30) G8:7 0:1
MSH 15 56 G326:3 1:8 W41 G23:3 0:3
Cygnus Loop G74:0 8:5 (MSH 15 57) G328:4 + 0:2 W44 G34:7 0:4
MSH 16 51 G332:4 + 0:1 W49B G43:3 0:2
DA 495 G65:7 + 1:2 MSH 17 39 G357:7 0:1 W50 G39:7 2:0
DA 530 G93:3 + 6:9 (W51) G49:2 0:7
DA 551 G93:7 0:2 Milne 56 G5:4 1:2 W63 G82:2 + 5:3
Monoceros Nebula G205:5 + 0:5
2000 August

Table III Abbreviations used in detailed listings
Journals
A&A Astronomy & Astrophysics
A&AS Astronomy & Astrophysics Supplement
AJ Astronomical Journal
ApJ Astrophysical Journal
ApJS Astrophysical Journal Supplement
AstL Astronomy Letters
ARep Astronomy Reports (Astronomicheski Ö i Zhurnal translation)
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 Review of Mexican Astronomy & Astrophysics
Sci Science
SvA Soviet Astronomy
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.
Radio Telescopes
5km Cambridge 5?km Telescope
6C Cambridge low frequency northern survey
ATCA Australia Telescope Compact Array
CLFST Cambridge Low Frequency Synthesis Telescope
DRAO Dominion Radio Astrophysical Observatory
FIRST Fleurs Synthesis Telescope
HMT Cambridge Half?Mile Telescope
MOST Molonglo Observatory Synthesis Telescope
NRAO National Radio Astronomy Observatory
NRO Nobeyama Radio Observatory
OMT Cambridge One?Mile Telescope
OSRT Ooty Synthesis Radio Telescope
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:
EXOSAT European X?ray Observatory Satellite
ROSAT RØontgensatellit
ASCA Advanced Satellite for Cosmology and Astrophysics
On board Einstein (HEAO?2):
HRI High Resolution Imager
IPC Imaging Proportional Counter
2000 August