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A Catalogue of
Galactic Supernova Remnants
(2014 May version)
D. A. Green
Cavendish Laboratory
19 J. J. Thomson Avenue
Cambridge CB3 0HE
UNITED KINGDOM
email: D.A.Green@mrao.cam.ac.uk
Please cite the following paper for the summary data from this catalogue:
. Green D. A., 2014, Bulletin of the Astronomical Society of India, 42, 47--58.
If you make use of the detailed version of the catalogue, then please also cite:
. Green D. A., 2014, `A Catalogue of Galactic Supernova Remnants (2014 May version)',
Cavendish Laboratory, Cambridge, UK (available at
"http://www.mrao.cam.ac.uk/surveys/snrs/").
1. The Catalogue Format
This catalogue of Galactic supernova remnants (SNRs) is an updated version of those presented in detail in Green
(1984, 1988) and in summary form in Green (1991, 1996, 2004, 2009a) -- hereafter Versions I, II, III, IV, V and VI
respectively -- and on the World�Wide�Web, in versions of 1995 July, 1996 August, 1998 September, 2000 August,
2001 December, 2004 January, 2006 April and 2009 March. (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 2014 May version of the catalogue, contains 294 SNRs (which is 20 more than in the previous
version; 21 remnants have been added, and one object removed), with over fifteen hundred references in the de�
tailed listings, plus notes on many possible or probable remnants. For each remnant in the catalogue the following
parameters are given.
. Galactic Coordinates of the source centroid, quoted to the nearest tenth of a degree as is conventional. (Note:
in this catalogue additional leading zeros are not used.)
. Other Names that are commonly used for the remnant. These are given in parentheses if the remnant is only
a part of the source. For some remnants, notably the Crab Nebula, not all common names are given.
. Right Ascension and Declination of the source centroid. The accuracy of the quoted values depends on the
size of the remnant; for small remnants they are to the nearest few seconds of time and the nearest minute of
arc respectively, whereas for larger remnants they are rounded to coarser values, but are in every case sufficient
to specify a point within the boundary of the remnant. These coordinates are usually deduced from radio maps
rather than from 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. 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, # (here defined in the sense, S # # --# ,
where S is the flux density at a frequency #), 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 confused 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 characteristics;
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 published references to observations are given for each
remnant, complete with journal, volume, page, and a short description of what information each paper contains (for
radio observations these include the telescopes used, the observing frequencies and resolutions, together with any
flux density determinations). These references are not complete, but cover representative and recent observations of
the remnant -- up to the first the end of 2013 in this version of the catalogue -- and they should themselves include
references to earlier work.
The references do not generally include large observational surveys -- of particular interest in this respect
are: the Effelsberg 100�m survey at 2.7 GHz of the Galactic plane 358 # < l < 240 # , |b| < 5 # by Reich et al.
(1990) and F�urst 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); Multi�Array Galactic Plane Imaging Survey (MAGPIS), see White, Becker & Helfand
(2005) and Helfand et al. (2006); the VLA Galactic Plane Survey, see Stil et al. (2006); the survey of HI emission
towards SNRs by Koo & Heiles (1991); surveys of IRAS observations of SNRs and their immediate surroundings by
Arendt (1989) and by Saken, Fesen & Shull (1992); various SPITZER surveys of inner galaxy (Reach et al. 2006;
Carey et al. 2009; Pinheiro Gonc�alves et al. 2011); the catalogue by Fesen & Hurford (1996) of UV/optical/infra�red
lines identified in SNRs; Fermi #�ray catalogues of Abdo et al. (2009, 2010). Also see Ferrand & Safi�Harb (2012),
present a census of X�/#�ray observations of Galactic SNRs and pulsar wind nebulae (PWNe), updates of which are
available at http://www.physics.umanitoba.ca/snr/SNRcat/.
A summary of the data available for all 294 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, but see below
for more recent work), G287.8--0.5 (see below), G322.3--1.2 (=Kes 24) and G343.0--6.0 (but see below). 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 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).
G10.0--0.3, which was regarded as a remnant -- possibly associated with a soft�gamma repeater -- was removed from
the 2004 January version of the catalogue, as it is now thought to be radio nebula powered by a stellar wind (see
Gaensler et al. 2001, Corbel & Eikenberry 2004, and references therein). G166.2+2.5 (=OA 184) was removed from
the 2006 April version of the catalogue, as it was identified as an HII region by Foster et al. (2006). G84.9+0.5 was
removed from Version VI of the catalogue, as it was identified as an HII region by Foster et al. (2007; see also Kothes
et al. 2006).
G16.8--1.1 has been removed from this version of the catalogue, as Sun et al. (2011) identify it as probably an
HII region, rather than a SNR (see also Stupar & Parker 2011, who also question the SNR identification).
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; Cameron & Kulkarni 2007).
. 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 & Langer (2000), and Phillips
& Ramos�Larios (2008) who identified G25.5+0.2 as a possible symbiotic outflow.
. Several 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).
. G247.8+4.9 was noted as a possible optical SNR by Weinberger (1995), but is listed as a probable planetary
nebula (PN) in the MASH PN catalogue (see Parker et al. 2006).
. 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).
. G104.7+2.8, a possible SNR suggested by Green & Joncas (1994), which instead appears to be an HII region,
based on the improved observations by Kothes et al. (2006).
2014 May

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. G106.6+2.9, a small remnant proposed by Halpern et al. (2001), is incorporated into the larger catalogued
remnant G106.3+2.7.
. Morris et al. (2006) suggested small remnant observed by Spitzer, which has subsequently instead been iden�
tified as a likely PN by Fesen & Milisavljevic (2010a), see also Mizuno et al. (2010).
. Leahy, Tian & Wang (2008) proposed that a large radio shell, G53.9+0.2, as a possible SNR. As noted
above, this feature was included, as G53.9+0.3 (part of HC40), in Version I of the catalogue, but was sub�
sequently removed, following the discussions of Caswell (1985) who concluded is was a thermal source (see
also Velusamy, Goss & Arnal 1986) -- results which Leahy et al. did not take into account.
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).
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, 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 (al�
though, as noted above, G358.4--1.9 was subsequently removed).
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 (although, as noted above, G84.9+0.5 was
subequently removed).
The following remnants were added to 1995 July version of the catalogue: G1.0--0.1, G1.4--0.1, G3.7--0.2,
G3.8+0.3, G28.8+1.5, G76.9+1.0, G272.2--3.2, G341.2+0.9, G354.1+0.1, G355.6--0.0, G356.3--0.3, G356.3--1.5
and G359.1+0.9.
The following remnants were added to the 1996 August version of the catalogue: G13.3--1.3, G286.5--1.2,
G289.7--0.3, G294.1--0.0, G299.2--2.9, G299.6--0.5, G301.4--1.0, G308.1--0.7, G310.6--0.3, G310.8--0.4,
G315.9--0.0, G317.3--0.2, G318.2+0.1, G320.6--1.6, G321.9--1.1, G327.4+1.0, G329.7+0.4, G342.1+0.9,
G343.1--0.7, G345.7--0.2, G349.2--0.1, G351.7+0.8, G351.9--0.9 and G354.8--0.8.
The following remnants were added to the 1998 September version of the catalogue: G0.3+0.0, G32.1--0.9,
G55.0+0.3, G63.7+1.1 and G182.4+4.3.
The following remnants were added to the 2000 August version of the catalogue: G7.0--0.1, G16.2--2.7,
G29.6+0.1, G266.2--1.2 and G347.3--0.5.
The following remnants were added to the 2001 December version of the catalogue: G4.8+6.2, G28.6--0.1,
G85.4+0.7, G85.9--0.6, G106.3+2.7, G292.2--0.5, G343.0--6.0, G353.9--2.0, G356.2+4.5 and G358.0+3.8.
G312.5--3.0 was added to Version V of the catalogue.
The following remnants were added to the 2006 April version of the catalogue: G5.5+0.3, G6.1+0.5,
G6.5--0.4, G7.2+0.2, G8.3--0.0, G8.9+0.4, G9.7--0.0, G9.9--0.8, G10.5--0.0, G11.0--0.0, G11.1--0.7, G11.1--1.0,
G11.1+0.1, G11.8--0.2, G12.2+0.3, G12.5+0.2, G12.7--0.0, G12.8--0.0, G14.1--0.1, G14.3+0.1, G15.4+0.1,
G16.0--0.5, G16.4--0.5, G17.0--0.0, G17.4--0.1, G18.1--0.1, G18.6--0.2, G19.1+0.2, G20.4+0.1, G21.0--0.4,
G21.5--0.1, G32.4+0.1, G96.0+2.0, G113.0+0.2 and G337.2+0.1.
The following remnants were added to Version VI of the catalogue. G83.0--0.3, G108.2--0.6, G315.1+2.7,
G332.5--5.6, G327.2--0.1, G350.1--0.3, G353.6--0.7, G355.4+0.7, G358.1+0.1 and G358.5--0.9.
The following 21 remnants have been added to this version of the catalogue.
. G35.6--0.4, which was re�identified as a SNR by Green (2009b) from radio and infra�red survey observations.
This source had been listed in several SNR catalogues (Milne 1970; Downes 1971; Ilovaisky & Lequeux
1972; Milne 1979). But Caswell & Clark (1975) derived a thermal radio index for it, and regarded it as an HII
region, not a SNR, and hence it was not listed in earlier versions of this catalolgue.
. G64.5+0.9, a shell remnant, which was identified from radio observations by Hurley�Walker et al. (2009).
(This source had previously been reported as a possible SNR by Tian & Leahy 2006).
2014 May

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. G159.6+7.3, a large optical shell remnant identified by Fesen & Milisavljevic (2010b).
. G310.6--1.6, a small X�ray remnant with an X�ray pulsar, identified by Renaud et al. (2010).
. G21.6--0.8, a faint shell remnant found in the radio by Bietenholz et al. (2011).
. Two faint shell remnants -- G25.1--2.3 and G178.2--4.2 -- found by Gao et al. (2011) in radio surveys.
. G308.4--1.4 was identified as a possible remnant by Whiteoak & Green (1996). Improved radio and X�ray
observations by Prinz & Becker (2012) have confirmed this as a SNR. But also see Hui et al. (2012) and De
Horta et al. (2013), who regard only the eastern portion of this as a smaller SNR G308.3--1.4 (which had
previously been noted as a possible remnants by Schaudel et al. 2002).
. G213.0--0.6, a large, faint radio shell first reported as a possible SNR by Reich, Zhang & F�urst (2003), for
which optical filaments have been recently detected by Stupar & Parker (2012). Note that Stupar & Parker
redesignated this remnant as G213.3--0.4, but following IAU recommendations (Dickel, Lortet & de Boer
1987) I have retained the original name.
. G296.7--0.9 -- which had been proposed as a possible SNR by Schaudel et al. (2002) -- was confirmed as a
remnant by Robbins et al. (2012), using radio and X�ray observations.
. G41.5+0.4 and G42.0--0.1, which are two of three possible remnants suggested by Kaplan et al. (2002), as
they have had the non�thermal nature of their radio emission confirmed by Alves et al. (2012).
. Five shell remnants -- G38.7--1.3, G65.8--0.5, G66.0--0.0, G67.6+0.9 and G67.8+0.5 -- identified by Sabin et al.
(2013) from a Galactic H# survey, which also have radio emisison. One or possibly two of these sources have
previously been reported as possible SNRs. Schaudel et al. (2012) reported X�ray and radio emission from
G38.7--1.4, which is the brighter eastern part of G38.7--1.3. Trushkin (2001) listed G67.8+0.8 as a possible
SNR, based on its extended emisson seen in the NRAO VLA Sky Survey (NVSS; Condon et al. 1998), which
may be part of G67.6+0.9 (but is difficult to be sure, since the Galactic and B1950.0 coordinates reported by
Trushkin are inconsistent).
. G152.4--2.1 and G190.9--2.2, two faint radio shell SNRs found by Foster et al. (2013). Note that the centres
of these remnants are offset slightly from the nominal positions given by the names given to these remnants
by Foster et al.
. G306.3--0.9 a small remnant identified by Reynolds et al. (2013) from X�ray and radio observtions.
. G322.1+0.0 a distorted radio/X�ray shell surrounding Cir X�1 identified by Heinz et al. (2013).
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.
2.3.1 Radio
. A possible SNR near the Galactic centre reported by Ho et al. (1985) from radio observations (see also Coil
& Ho 2000; Lu, Wang & Lang 2003; Senda, Murakami & Koyama 2003, and references therein).
. Gosachinski�� (1985) reported evidence for non�thermal radio emission, presumably from SNRs, associated
with several bright, thermal Galactic sources. Some of these sources have been included in the catalogue, fol�
lowing improved observations (but also see Odegard 1986, who questions the reliability of some of Gosachin�
ski��'s results, and also suggest another possible SNR, G7.6--0.6).
. G300.1+9.4, a possible SNR nearly 2 # in diameter reported by Dubner, Colomb & Giacani (1986).
. Routledge & Vaneldik (1988) report a possible faint radio shell SNR nearly 2 # in diameter, near the young
pulsar PSR 1930+22 -- see also G�omez�Gonz�alez & del Romero (1983), who report a smaller (about 40 ar�
cmin) possible SNR (G57.1+1.7) associated with this pulsar, and see Caswell, Landecker & Feldman (1985)
and Kovalenko (1989).
. Gorham (1990) lists many SNR candidates from the Clark Lake 30.9 MHz survey of the first quadrant, follow�
ing Kassim (1988), although several have been shown not to be SNRs by Gorham, Kulkarni & Prince (1993).
Gorham et al. do report a poorly defined possible remnant G41.4+1.2. See also Aharonian et al. (2008a) for
observations of #� and X�ray emission possibly associated with one of the candidates (G44.6+0.1) listed by
Gorham.
. Four possible remnants (G45.9--0.1, G71.6--0.5, G72.2--0.3 and G85.2--1.2) of the eleven reported by Taylor,
Wallace & Goss (1992) from a radio survey of part of the Galactic plane (see also Kothes et al. 2006). (Five
of the other possible SNRs reported by Taylor et al., are included in the catalogue as G55.0+0.3, G59.5+0.1,
G63.7+1.1, G76.9+1.0 and G83.0--0.2, following improved observations which have confirmed their nature.)
2014 May

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. G356.6+0.1, G357.1--0.2, 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 G356.6+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.
. 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. See also: Walker & Zealey (1998) for details of an optical shell around the Coalsack Nebula
(near l = 300 # , b = 0 # ) which overlaps one of these candidates; Camilo et al. (2004), Chang et al. (2012)
and Danienko et al. (2012) for further observations of another, G309.8--2.6, which is near a young pulsar; and
Russeil et al. (2005), who detected optical filaments from a third.
. Whiteoak & Green (1996), from their radio survey of much of the southern Galactic plane, list many possible
SNRs, several of which have been included in the catalogue, following improved observations, while most
(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, and G348.8+1.1) have not. See also Hui &
Becker (2007) for X�ray observations of G319.9--0.7.
. Several candidate SNRs reported by Combi & Romero (1998), Combi, Romero & Arnal (1998), Combi,
Romero & Benaglia (1998), Punsly et al. (2000) and Combi et al. (2001).
. A possible SNR, near l = 313 # , which is close to an unidentified Galactic plane #�ray source (see Roberts
et al. 1999), and to a pulsar (Roberts, Romani & Johnston 2001). See also Aharonian et al. (2006).
. G359.07--0.02, a possible SNR noted by LaRosa et al. (2000), see also Nakashima et al. (2010).
. A possible SNRs near G6.4--0.1 (=W28) noted by Yusef�Zadeh et al. (2000). (A second possible remnant
noted by Yusef�Zadeh et al. has been included in the catalogue, as G6.5--0.4, following the improved obser�
vations of it by Brogan et al. 2006).
. 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.
. Several possible SNRs reported by Trushkin (2001), which were identified from Galactic radio surveys (one
of which, G6.1+0.5, is included in the catalogue, due to improved subsequent observations).
. Two possibles SNRs (G336.1--0.2 and G352.2--0.1) discussed briefly by Manchester et al. (2002).
. G282.8--1.2, a possible young SNR noted by Misanovic, Cram & Green (2002).
. G43.5+0.6, one of three possible SNRs identified by Kaplan et al. (2002); the other two are included in the
catalogue as subsequent observations have shown they have non�thermal radio spectra.
. Two faint SNR candidates shown in Reich (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 (see also Kothes et al. 2006).
. Zhang (2003) identified four candidate SNRs from radio surveys. One of these -- called G41.9+0.04 by Zhang
-- is close to G42.0--0.0. 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 of the sources --
G47.8+2.03 -- also may have a thermal radio spectrum, given its published 2.7�GHz flux density (F�urst et al.
1990b).
. Brogan et al. (2006) identify 35 new SNRs in the region 4 # .5 < l < 22 # , |b| < 1 # .25, of which the 31 which are
classed as `I' or `II' (i.e. those thought to be very or fairly confidently identified as SNRs) were included in the
2006 version of the catalogue. Four other possible SNRs -- labelled G5.71--0.08, G6.31+0.54, G15.51--0.15
and G19.13+0.90 -- which comprise Brogan et al.'s class `III', are not included in the catalogue, as further
observations are required to confirm their nature and better define their parameters (see also Aharonian et al.
2008b and Hewitt & Yusef�Zadeh et al. 2009).
2014 May

-- vii --
. Two candidate large SNRs (diameters of approximately 3 # and 1 # .6) are reported from radio surveys in the
Galactic anticentre by Soberski et al. (2005), although there coordinates are not given.
. Helfand et al. (2006) list many SNR candidates in the region 5 # < l < 32 # , |b| < 0 # .8 from MAGPIS. Many
of these correspond to sources in Brogan et al., and several are included in the catalogue, with the others
requiring further observations. See also Johanson & Kerton (2009).
. Mart�� et al. (2007), report extended radio emission near the X�ray source KS 1741--295 near the Galactic
centre which may be a SNR (see also Cherepashchuk 1994).
. A poorly defined possible SNR, near l = 151 # , b = 3 # has been reported by Kerton, Murphy & Patterson
(2007).
. Roberts & Brogan (2008) propose a new SNR, G7.5--1.7, from non�thermal radio emission near an pulsar
wind nebula, although currently the extent of the remnant is not well defined.
. Anderson et al. (2012) report extended radio emission near a magnetar which may be a SNR designated
G333.9+0.0 (see also Kijak et al. 2013).
. G354.4+0.0 a possible small remnant reported by Roy & Pal (2013) from radio observations.
2.3.2 UV/Optical/Infra�red
. Winkler et al. (1989) report a possible small (4 arcmin) SNR within the Puppis A remnant, from optical
observations. 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), although this
appears to have a thermal radio spectrum.
. 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;
Kothes et al. 2006).
. Two possible SNRs, G340.5+0.7 and G342.1+0.1, identified by Walker, Zealey & Parker (2001) from fila�
ments seen in H# survey observations.
. A probable 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).
See also Rector & Schweiker (2013).
. A possible remnant, near l = 70 # , b = 2 # noted by Mavromatakis & Strom (2002), for which Kothes et al.
(2006) do not find any radio counterpart.
. Optical filaments in Pegasus (Boumis et al. 2002) which suggest one or more possible SNRs.
. A possible remnant identified from optical filaments to the NE of the known SNR G116.5+1.1, as observed
by Mavromatakis et al. (2005).
. Russell et al. (2007) report a small (about 7 arcmin in extent) optical ring, which is very faint at radio wave�
lengths, just to the NW of Cyg X�1, which may be a SNR if it is not associated with Cyg X�1 (see also Gallo
et al. 2005).
. Stupar, Parker & Filipovi�c (2008) report several SNRs identified from H# observations, several of which
correspond to SNR candidates first suggested by Duncan et al. (1995, 1997) from radio observations. The full
extent of most of these are not well defined, but two are currently included in the main catalogue (G315.1+2.7,
and G332.5--5.6).
. Mavromatakis et al. (2009) report a candidate SNR, G70.5+1.9, from optical observations.
. Optical filaments indicating a possible new SNR, G304.4--3.1 are presented by Stupar et al. (2010).
. Stupar et al. (2011) report a possible new SNR, G310.5--0.8, identifed from optical filaments and associated
radio emission.
2014 May

-- viii --
2.3.3 X�ray/#�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.
. G189.6+3.3, a faint, possible SNR overlapping G189.1+3.0 (=IC443) identified by Asaoka & Aschenbach
(1994) from ROSAT X�ray observations (see also Lee et al. 2008).
. G117.7+0.6, a faint shell of soft X�ray emission near G116.9+0.2 (=CTB 1), which contains a pulsar (Hailey
& Craig 1995; see also Craig, Hailey & Pisarski 1997, Esposito et al. 2008 and Kothes et al. 2006).
. A possible SNR identified in X�rays around the pulsar B1828--13 suggested by see Finley, Srinivasan & Park
(1996), see also Braun, Goss & Lyne (1986) and Pavlov et al. (2008).
. 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) and Kothes et al. (2006).
. Schaudel et al. (2002) report 14 candidate SNRs identified in the ROSAT All�Sky Survey, and provided images
for 3 of these (all of which have been included in this version of the catalogue -- as G38.7--1.3, G296.7--0.9
and G308.4--1.4 -- following improved observations of them, see Section 2.2).
. 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, 2003), see also Renaud et al. (2006).
. Senda et al. (2003) also identify two other possible SNRs near the Galactic Centre from their X�ray emission
(see also Mori et al. 2008 for further observations of one of these, G359.79--0.26).
. Several possible SNRs reported by Bamba et al. (2003) and Ueno et al. (2005, 2006), two of which have been
included in the catalogue (as G28.6--0.1 and G32.4+0.1), as additional observations confirm their nature. One
of the proposed remnants is called G11.0+0.0, but is larger than the currently catalogued G11.0--0.0. The
nature of a second, G25.5+0.0, has been questioned by Kargalstev et al. (2012), who also proposed another,
smaller possible SNR, G25.25+0.28, which corresponds to one of the candidates listed by Helfand et al.
(2006). For a third source, G23.5+0.1, Kargalstev et al. prefer a pulsar wind nebula interpretation.
. An excess of Fe X�ray line emission in Sgr B, near l = 0 # .61, b = 0 # .01 may be from a SNR (Koyama et al.
2007).
. Nobukawa et al. (2008) report a region of X�ray emission, G0.42--0.04, near the Galactic centre, which may
be part of a SNR.
. Henley & Shelton (2009) report a possible large (# 10 # ) SNR at high Galactic latitudes, from the ROSAT
All�Sky Survey.
. A candidate SNR in the Sagittarius C region, designated G359.41--0.12, was identified in X�rays by Tsuru
et al. (2009).
. Sawada et al. (2009) propose a possible SNR, G1.2--0.0, from X�ray observations (see also Law, Yusef�Zadeh
& Cotton 2008 for radio observations).
. Brief details a possible new SNR identifed from the Swift X�ray Galactic Plane Survey are reported by
Reynolds et al. (2012).
. Heard & Warwick (2013) report on X�ray emission which may be the core of a SNR, which they designate
G0.13--0.12.
2.3.4 Other
. G287.8--0.5, which is associated with # 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 G69.0+2.7 (=CTB 80) by Predehl & Kulkarni (1995), i.e. a pulsar powered nebula (see also
Camilo et al. 2002).
2014 May

-- ix --
It should also be noted: (a) Some large radio continuum, HI or CO 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 Grenier et al.
(1989), Combi et al. (1995), Maciejewski et al. (1996), Kim & Koo (2000), Normandeau et al. (2000), Woermann,
Gaylard & Otrupcek (2001), Stil & Irwin (2001), Uyan�ker & Kothes (2002), Olano, Meschin & Niemela (2006),
Borka (2007), Kang et al. (2012), and Gao & Han 2013, who discuss the nature of the Origem Loop -- a large
radio loop -- which has at times been regarded as a remnant, and regard the northern part (which has a non�thermal
spectrum) as part of a SNR, although the full extent of the remnant is not clear. Also Koo, Kang & Salter (2006)
and Kang & Koo (2007) identify faint Galactic HI features at forbidden velocities as indicators of old, otherwise
undetectable SNRs. (b) Some large (> 10 # ) regions of X�ray emission that are indicative of a SNR are not included
in the catalogue; e.g. the Monogem ring, near l = 203 # , b = +12 # (see Nousek et al. 1981, Plucinsky et al. 1996,
Thorsett et al. 2003, Amenomori et al. 2005, Plucinsky 2009, and references therein, plus Weinberger, Temporin &
Stecklum 2006, for observations of optical filaments); in the Gum Nebula near l = 250 # , b = 0 # (see Leahy, Nousek
& Garmire 1992, and also see Reynolds 1976, Dubner et al. 1992, Duncan et al. 1996, Reynoso & Dubner 1997,
Heiles 1998, Pagani et al. 2012); in Eridanus near l = 200 # , b = --40 # (see Naranan et al. 1976, Burrows et al.
1993, Snowden et al. 1995, Heiles 1998, Boumis et al. 2001, Ryu et al. 2006); a large approximately 24 # diameter,
X�ray and optical loop in Antlia (see McCullough, Fields & Pavlidou 2002, Shinn et al. 2007). (c) The distinction
between filled�centre remnants and pulsar wind nebulae (PWNe) is not clear, and isolated, generally faint, pulsar wind
nebulae are also not included in the catalogue. See the catalogue of PWNe by Kaspi, Roberts & Harding (2006) (also
http://www.physics.mcgill.ca/~pulsar/pwncat.html), and the high�energy SNR and PWNe catalogue noted at
the end of Section 1.
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), 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), and of G354.1+0.1 (which
may be similar to G357.7--0.1 (=MHS 17--39)) are also uncertain (see Landecker, Higgs & Wendker 1993 and Frail,
Goss & Whiteoak 1994). Also, Pinheiro Gonc�alves et al. (2011) suggest that G23.6+0.3, and possibly G14.3+0.1
may be HII regions, rather than SNRs.
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
This research has made use of NASA's Astrophysics Data System Bibliographic Services.
2014 May

-- x --
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2014 May

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 1.5 S 0.6 0.6
3.7 --0.2 17 55 26 --25 50 14�11 S 2.3 0.65
3.8 +0.3 17 52 55 --25 28 18 S? 3? 0.6
4.2 --3.5 18 08 55 --27 03 28 S 3.2? 0.6?
4.5 +6.8 17 30 42 --21 29 3 S 19 0.64 Kepler, SN1604, 3C358
4.8 +6.2 17 33 25 --21 34 18 S 3 0.6
5.2 --2.6 18 07 30 --25 45 18 S 2.6? 0.6?
5.4 --1.2 18 02 10 --24 54 35 C? 35? 0.2? Milne 56
5.5 +0.3 17 57 04 --24 00 15�12 S 5.5 0.7
5.9 +3.1 17 47 20 --22 16 20 S 3.3? 0.4?
6.1 +0.5 17 57 29 --23 25 18�12 S 4.5 0.9
6.1 +1.2 17 54 55 --23 05 30�26 F 4.0? 0.3?
6.4 --0.1 18 00 30 --23 26 48 C 310 varies W28
6.4 +4.0 17 45 10 --21 22 31 S 1.3? 0.4?
6.5 --0.4 18 02 11 --23 34 18 S 27 0.6
7.0 --0.1 18 01 50 --22 54 15 S 2.5? 0.5?
7.2 +0.2 18 01 07 --22 38 12 S 2.8 0.6
7.7 --3.7 18 17 25 --24 04 22 S 11 0.32 1814--24
8.3 --0.0 18 04 34 --21 49 5�4 S 1.2 0.6
8.7 --5.0 18 24 10 --23 48 26 S 4.4 0.3
8.7 --0.1 18 05 30 --21 26 45 S? 80 0.5 (W30)
8.9 +0.4 18 03 58 --21 03 24 S 9 0.6
9.7 --0.0 18 07 22 --20 35 15�11 S 3.7 0.6
9.8 +0.6 18 05 08 --20 14 12 S 3.9 0.5
9.9 --0.8 18 10 41 --20 43 12 S 6.7 0.4
10.5 --0.0 18 09 08 --19 47 6 S 0.9 0.6
11.0 --0.0 18 10 04 --19 25 11�9 S 1.3 0.6
11.1 --1.0 18 14 03 --19 46 18�12 S 5.8 0.5
11.1 --0.7 18 12 46 --19 38 11�7 S 1.0 0.7
11.1 +0.1 18 09 47 --19 12 12�10 S 2.3 0.4
11.2 --0.3 18 11 27 --19 25 4 C 22 0.5
11.4 --0.1 18 10 47 --19 05 8 S? 6 0.5
11.8 --0.2 18 12 25 --18 44 4 S 0.7 0.3
12.0 --0.1 18 12 11 --18 37 7? ? 3.5 0.7
12.2 +0.3 18 11 17 --18 10 6�5 S 0.8 0.7
2014 May

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)
12.5 +0.2 18 12 14 --17 55 6�5 C? 0.6 0.4
12.7 --0.0 18 13 19 --17 54 6 S 0.8 0.8
12.8 --0.0 18 13 37 --17 49 3 C? 0.8 0.5
13.3 --1.3 18 19 20 --18 00 70�40 S? ? ?
13.5 +0.2 18 14 14 --17 12 5�4 S 3.5? 1.0?
14.1 --0.1 18 16 40 --16 41 6�5 S 0.5 0.6
14.3 +0.1 18 15 58 --16 27 5�4 S 0.6 0.4
15.1 --1.6 18 24 00 --16 34 30�24 S? 5.5? 0.0?
15.4 +0.1 18 18 02 --15 27 15�14 S 5.6 0.62
15.9 +0.2 18 18 52 --15 02 7�5 S? 5.0 0.63
16.0 --0.5 18 21 56 --15 14 15�10 S 2.7 0.6
16.2 --2.7 18 29 40 --16 08 17 S 2.5 0.4
16.4 --0.5 18 22 38 --14 55 13 S 4.6 0.3?
16.7 +0.1 18 20 56 --14 20 4 C 3.0 0.6
17.0 --0.0 18 21 57 --14 08 5 S 0.5 0.5
17.4 --2.3 18 30 55 --14 52 24? S 5 0.5?
17.4 --0.1 18 23 08 --13 46 6 S 0.4 0.7
17.8 --2.6 18 32 50 --14 39 24 S 5 0.5
18.1 --0.1 18 24 34 --13 11 8 S 4.6 0.5
18.6 --0.2 18 25 55 --12 50 6 S 1.4 0.4
18.8 +0.3 18 23 58 --12 23 17�11 S 33 0.46 Kes 67
18.9 --1.1 18 29 50 --12 58 33 C? 37 0.39
19.1 +0.2 18 24 56 --12 07 27 S 10 0.5
20.0 --0.2 18 28 07 --11 35 10 F 10 0.1
20.4 +0.1 18 27 51 --11 00 8 S? 9? 0.1?
21.0 --0.4 18 31 12 --10 47 9�7 S 1.1 0.6
21.5 --0.9 18 33 33 --10 35 5 C 7 varies
21.5 --0.1 18 30 50 --10 09 5 S 0.4 0.5
21.6 --0.8 18 33 40 --10 25 13 S 1.4 0.5?
21.8 --0.6 18 32 45 --10 08 20 S 65 0.56 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?
25.1 --2.3 18 45 10 --08 00 80�30? S 8 0.5?
27.4 +0.0 18 41 19 --04 56 4 S 6 0.68 4C--04.71
27.8 +0.6 18 39 50 --04 24 50�30 F 30 varies
28.6 --0.1 18 43 55 --03 53 13�9 S 3? ?
28.8 +1.5 18 39 00 --02 55 100? S? ? 0.4?
2014 May

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)
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 0.63 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 25 varies 3C391
32.0 --4.9 19 06 00 --03 00 60? S? 22? 0.5? 3C396.1
32.1 --0.9 18 53 10 --01 08 40? C? ? ?
32.4 +0.1 18 50 05 --00 25 6 S 0.25? ?
32.8 --0.1 18 51 25 --00 08 17 S? 11? 0.2? Kes 78
33.2 --0.6 18 53 50 --00 02 18 S 3.5 varies
33.6 +0.1 18 52 48 +00 41 10 S 20 0.51 Kes 79, 4C00.70, HC13
34.7 --0.4 18 56 00 +01 22 35�27 C 250 0.37 W44, 3C392
35.6 --0.4 18 57 55 +02 13 15�11 S? 9 0.5
36.6 --0.7 19 00 35 +02 56 25? S? 1.0 0.7?
36.6 +2.6 18 48 49 +04 26 17�13? S 0.7? 0.5?
38.7 --1.3 19 06 40 +04 28 32�19? S ? ?
39.2 --0.3 19 04 08 +05 28 8�6 C 18 0.34 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 0.4
41.1 --0.3 19 07 34 +07 08 4.5�2.5 S 25 0.50 3C397
41.5 +0.4 19 05 50 +07 46 10 S? 1? ?
42.0 --0.1 19 08 10 +08 00 8 S? 0.5? ?
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 0.46 W49B
43.9 +1.6 19 05 50 +10 30 60? S? 9.0 0.5
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 17 0.54 (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 0.50 3C400.2, NRAO 611
54.1 +0.3 19 30 31 +18 52 12? C? 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? 0.3?
57.2 +0.8 19 34 59 +21 57 12? S? 1.8 0.62 (4C21.53)
59.5 +0.1 19 42 33 +23 35 15 S 3? ?
59.8 +1.2 19 38 55 +24 19 20�16? ? 1.5 0.0
63.7 +1.1 19 47 52 +27 45 8 F 1.8 0.24
64.5 +0.9 19 50 25 +28 16 8 S? 0.15? 0.5
65.1 +0.6 19 54 40 +28 35 90�50 S 5.5 0.61
2014 May

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)
65.3 +5.7 19 33 00 +31 10 310�240 S? 42 0.6
65.7 +1.2 19 52 10 +29 26 22 F 5.1 varies DA 495
65.8 --0.5 19 59 20 +28 38 10�6? S ? ?
66.0 --0.0 19 57 50 +29 03 31�25? S ? ?
67.6 +0.9 19 57 45 +30 53 50�45? S ? ?
67.7 +1.8 19 54 32 +31 29 15�12 S 1.0 0.61
67.8 +0.5 20 00 00 +30 51 7�5 ? ? ?
68.6 --1.2 20 08 40 +30 37 23 ? 1.1 0.2
69.0 +2.7 19 53 20 +32 55 80? ? 120? varies CTB 80
69.7 +1.0 20 02 40 +32 43 16�14 S 2.0 0.7
73.9 +0.9 20 14 15 +36 12 27 S? 9 0.23
74.0 --8.5 20 51 00 +30 40 230�160 S 210 varies Cygnus Loop
74.9 +1.2 20 16 02 +37 12 8�6 F 9 varies CTB 87
76.9 +1.0 20 22 20 +38 43 9 C 2? ?
78.2 +2.1 20 20 50 +40 26 60 S 320 0.51 DR4, # Cygni SNR
82.2 +5.3 20 19 00 +45 30 95�65 S 120? 0.5? W63
83.0 --0.3 20 46 55 +42 52 9�7 S 1 0.4
84.2 --0.8 20 53 20 +43 27 20�16 S 11 0.5
85.4 +0.7 20 50 40 +45 22 24? S ? 0.2
85.9 --0.6 20 58 40 +44 53 24 S ? 0.2
89.0 +4.7 20 45 00 +50 35 120�90 S 220 0.38 HB21
93.3 +6.9 20 52 25 +55 21 27�20 C? 9 0.45 DA 530, 4C(T)55.38.1
93.7 --0.2 21 29 20 +50 50 80 S 65 0.65 CTB 104A, DA 551
94.0 +1.0 21 24 50 +51 53 30�25 S 13 0.45 3C434.1
96.0 +2.0 21 30 30 +53 59 26 S 0.35 0.6
106.3 +2.7 22 27 30 +60 50 60�24 C? 6 0.6
108.2 --0.6 22 53 40 +58 50 70�54 S 8 0.5
109.1 --1.0 23 01 35 +58 53 28 S 22 0.45 CTB 109
111.7 --2.1 23 23 26 +58 48 5 S 2720 0.77 Cassiopeia A, 3C461
113.0 +0.2 23 36 35 +61 22 40�17? ? 4 0.5?
114.3 +0.3 23 37 00 +61 55 90�55 S 5.5 0.5
116.5 +1.1 23 53 40 +63 15 80�60 S 10 0.5
116.9 +0.2 23 59 10 +62 26 34 S 8 0.57 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 0.58 Tycho, 3C10, SN1572
126.2 +1.6 01 22 00 +64 15 70 S? 6 0.5
127.1 +0.5 01 28 20 +63 10 45 S 12 0.45 R5
130.7 +3.1 02 05 41 +64 49 9�5 F 33 0.07 3C58, SN1181
132.7 +1.3 02 17 40 +62 45 80 S 45 0.6 HB3
152.4 --2.1 04 07 50 +49 11 100�95 S 3.5? 0.7?
2014 May

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)
156.2 +5.7 04 58 40 +51 50 110 S 5 0.5
159.6 +7.3 05 20 00 +50 00 240�180? S ? ?
160.9 +2.6 05 01 00 +46 40 140�120 S 110 0.64 HB9
166.0 +4.3 05 26 30 +42 56 55�35 S 7 0.37 VRO 42.05.01
178.2 --4.2 05 35 05 +28 11 72�62 S 2 0.5
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 0.5 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
190.9 --2.2 06 01 55 +18 24 70�60 S 1.3? 0.7?
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 140 0.4 Monoceros Nebula
206.9 +2.3 06 48 40 +06 26 60�40 S? 6 0.5 PKS 0646+06
213.0 --0.6 06 50 50 --00 30 160�140? S 21 0.4
260.4 --3.4 08 22 10 --43 00 60�50 S 130 0.5 Puppis A, MSH 08--44
261.9 +5.5 09 04 20 --38 42 40�30 S 10? 0.4?
263.9 --3.3 08 34 00 --45 50 255 C 1750 varies Vela (XYZ)
266.2 --1.2 08 52 00 --46 20 120 S 50? 0.3? RX J0852.0--4622
272.2 --3.2 09 06 50 --52 07 15? S? 0.4 0.6
279.0 +1.1 09 57 40 --53 15 95 S 30? 0.6?
284.3 --1.8 10 18 15 --59 00 24? S 11? 0.3? MSH 10--53
286.5 --1.2 10 35 40 --59 42 26�6 S? 1.4? ?
289.7 --0.3 11 01 15 --60 18 18�14 S 6.2 0.2?
290.1 --0.8 11 03 05 --60 56 19�14 S 42 0.4 MSH 11--61A
291.0 --0.1 11 11 54 --60 38 15�13 C 16 0.29 (MSH 11--62)
292.0 +1.8 11 24 36 --59 16 12�8 C 15 0.4 MSH 11--54
292.2 --0.5 11 19 20 --61 28 20�15 S 7 0.5
293.8 +0.6 11 35 00 --60 54 20 C 5? 0.6?
294.1 --0.0 11 36 10 --61 38 40 S >2? ?
296.1 --0.5 11 51 10 --62 34 37�25 S 8? 0.6?
296.5 +10.0 12 09 40 --52 25 90�65 S 48 0.5 PKS 1209--51/52
296.7 --0.9 11 55 30 --63 08 15�8 S 3 0.5
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?
2014 May

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)
304.6 +0.1 13 05 59 --62 42 8 S 14 0.5 Kes 17
306.3 --0.9 13 21 50 --63 34 4 S? 0.16? 0.5?
308.1 --0.7 13 37 37 --63 04 13 S 1.2? ?
308.4 --1.4 13 41 30 --63 44 12�6? S? 0.4? ?
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 --1.6 14 00 45 --63 26 2.5 C? ? ?
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 20�18 S 3.5? ?
315.1 +2.7 14 24 30 --57 50 190�150 S ? ?
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
322.1 +0.0 15 20 49 --57 10 8�4.5? S? ? ?
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? ?
327.2 --0.1 15 50 55 --54 18 5 S 0.4 ?
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 0.0 (MSH 15--57)
329.7 +0.4 16 01 20 --52 18 40�33 S >34? ?
330.0 +15.0 15 10 00 --40 00 180? S 350? 0.5? Lupus Loop
330.2 +1.0 16 01 06 --51 34 11 S? 5? 0.3
332.0 +0.2 16 13 17 --50 53 12 S 8? 0.5
332.4 --0.4 16 17 33 --51 02 10 S 28 0.5 RCW 103
2014 May

Table I -- VII -- Summary listings
l b RA (J2000.0) Dec size type Flux at spectral other
(h m s) ( # # ) /arcmin 1 GHz/Jy index name(s)
332.4 +0.1 16 15 20 --50 42 15 S 26 0.5 MSH 16--51, Kes 32
332.5 --5.6 16 43 20 --54 30 35 S 2? 0.7?
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 1.5 0.4
337.2 +0.1 16 35 55 --47 20 3�2 ? 1.5? ?
337.3 +1.0 16 32 39 --46 36 15�12 S 16 0.55 Kes 40
337.8 --0.1 16 39 01 --46 59 9�6 S 18 0.5 Kes 41
338.1 +0.4 16 37 59 --46 24 15? S 4? 0.4
338.3 --0.0 16 41 00 --46 34 8 C? 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 22�16 C 1.5? 0.6?
341.9 --0.3 16 55 01 --44 01 7 S 2.5 0.5
342.0 --0.2 16 54 50 --43 53 12�9 S 3.5? 0.4?
342.1 +0.9 16 50 43 --43 04 10�9 S 0.5? ?
343.0 --6.0 17 25 00 --46 30 250 S ? ? RCW 114
343.1 --2.3 17 08 00 --44 16 32? C? 8? 0.5?
343.1 --0.7 17 00 25 --43 14 27�21 S 7.8 0.55
344.7 --0.1 17 03 51 --41 42 8 C? 2.5? 0.3?
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? 30? ? RX J1713.7--3946
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
350.1 --0.3 17 17 40 --37 24 4? ? 6? 0.8?
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 0.5?
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
353.6 --0.7 17 32 00 --34 44 30 S 2.5? ?
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? ?
2014 May

Table I -- VIII -- Summary listings
l b RA (J2000.0) Dec size type Flux at spectral other
(h m s) ( # # ) /arcmin 1 GHz/Jy index name(s)
355.4 +0.7 17 31 20 --32 26 25 S 5? ?
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 --1.5 17 42 35 --32 52 20�15 S 3? ?
356.3 --0.3 17 37 56 --32 16 11�7 S 3? ?
357.7 --0.1 17 40 29 --30 58 8�3? ? 37 0.4 MSH 17--39
357.7 +0.3 17 38 35 --30 44 24 S 10 0.4?
358.0 +3.8 17 26 00 --28 36 38 S 1.5? ?
358.1 +0.1 17 37 00 --29 59 20 S 2? ?
358.5 --0.9 17 46 10 --30 40 17 S 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 2? ?
2014 May

Table II Other names for SNRs
# Cygni SNR G78.2+2.1 HB3 G132.7+1.3 NRAO 593 G39.2--0.3
HB9 G160.9+2.6 NRAO 611 G53.6--2.2
1156--62 G296.8--0.3 HB21 G89.0+4.7
1814--24 G7.7--3.7 PKS 0607+17 G192.8--1.1
HC13 G33.6+0.1 PKS 0646+06 G206.9+2.3
3C10 G120.1+1.4 HC24 G39.2--0.3 PKS 1209--51/52 G296.5+10.0
3C58 G130.7+3.1 (HC30) G46.8--0.3 PKS 1459--41 G327.6+14.6
3C144 G184.6--5.8 (HC40) G54.4--0.3
3C157 G189.1+3.0 Puppis A G260.4--3.4
3C358 G4.5+6.8 IC443 G189.1+3.0
3C391 G31.9+0.0 R5 G127.1+0.5
3C392 G34.7--0.4 Kepler G4.5+6.8
3C396 G39.2--0.3 RCW 86 G315.4--2.3
3C396.1 G32.0--4.9 Kes 17 G304.6+0.1 RCW 89 G320.4--1.2
3C397 G41.1--0.3 Kes 20A G310.6--0.3 RCW 103 G332.4--0.4
3C400.2 G53.6--2.2 Kes 20B G310.8--0.4 RCW 114 G343.0--6.0
3C434.1 G94.0+1.0 Kes 27 G327.4+0.4
3C461 G111.7--2.1 Kes 32 G332.4+0.1 RX J0852.0--4622 G266.2--1.2
Kes 40 G337.3+1.0 RX J1713.7--3946 G347.3--0.5
4C--04.71 G27.4+0.0 Kes 41 G337.8--0.1
4C00.70 G33.6+0.1 Kes 67 G18.8+0.3 S147 G180.0--1.7
(4C21.53) G57.2+0.8 Kes 69 G21.8--0.6
4C(T)55.38.1 G93.3+6.9 Kes 75 G29.7--0.3 SN1006 G327.6+14.6
Kes 78 G32.8--0.1 SN1054 G184.6--5.8
CTA 1 G119.5+10.2 Kes 79 G33.6+0.1 SN1181 G130.7+3.1
SN1572 G120.1+1.4
CTB 1 G116.9+0.2 Lupus Loop G330.0+15.0 SN1604 G4.5+6.8
(CTB 33) G337.0--0.1
CTB 37A G348.5+0.1 MSH 08--44 G260.4--3.4 SS433 G39.7--2.0
CTB 37B G348.7+0.3 MSH 10--53 G284.3--1.8
CTB 80 G69.0+2.7 MSH 11--54 G292.0+1.8 Sgr A East G0.0+0.0
CTB 87 G74.9+1.2 MSH 11--61A G290.1--0.8
CTB 104A G93.7--0.2 (MSH 11--62) G291.0--0.1 Tycho G120.1+1.4
CTB 109 G109.1--1.0 (MSH 14--57) G316.3--0.0
MSH 14--63 G315.4--2.3 Vela (XYZ) G263.9--3.3
Cassiopeia A G111.7--2.1 MSH 15--52 G320.4--1.2
MSH 15--56 G326.3--1.8 VRO 42.05.01 G166.0+4.3
Crab Nebula G184.6--5.8 (MSH 15--57) G328.4+0.2
MSH 16--51 G332.4+0.1 W28 G6.4--0.1
Cygnus Loop G74.0--8.5 MSH 17--39 G357.7--0.1 (W30) G8.7--0.1
W41 G23.3--0.3
DA 495 G65.7+1.2 Milne 56 G5.4--1.2 W44 G34.7--0.4
DA 530 G93.3+6.9 W49B G43.3--0.2
DA 551 G93.7--0.2 Monoceros Nebula G205.5+0.5 W50 G39.7--2.0
(W51) G49.2--0.7
DR4 G78.2+2.1 W63 G82.2+5.3
2014 May

Table III Abbreviations used in detailed listings
Journals
AdSpR Advances in Space Research
A&A Astronomy & Astrophysics
A&AS Astronomy & Astrophysics Supplement
AJ Astronomical Journal
AN Astronomische Nachrichten
ApJ Astrophysical Journal
ApJS Astrophysical Journal Supplement
ApL Astrophysical Letters
ApS&S Astrophysics & Space Science
AstL Astronomy Letters
ARep Astronomy Reports
AuJPA Australian Journal of Physics Astrophysical Supplement
AuJPh Australian Journal of Physics
BASI Bulletin of the Astronomical Society of India
ChJAA Chinese Journal of Astronomy & Astrophysics
JApA Journal of Astrophysics & Astronomy
JKAS Journal of Korean Astronomical Society
JPhCS Journal of Physics Conference Series
MNRAS Monthly Notices of the Royal Astronomical Society
NuPhS Nuclear Physics B Proceedings Supplements
PASA 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 Astronom��a y Astrof��sica
SerAJ Serbian Astronomical Journal
SvAL Soviet Astronomy Letters
Proceedings etc.
IAUCo IAU Colloquium
LNP Lecture Notes in Physics
NSPS is `Neutron Stars, Pulsars, and Supernova Remnants', (MPE Report 278), eds Becker W., Lesch H. &
Tr�umper J., (Max�Plank�Institut f�ur extraterrestrische Physik, Garching bei M�unchen), 2002.
XRRC is `X�Ray and Radio Connections', eds Sjouwerman L. O. & Dyer K. K.,
(available at http://www.aoc.nrao.edu/events/xraydio/), 2005.
Radio Telescopes/Surveys
ATCA Australia Telescope Compact Array
BIMA Berkeley--Illinois--Maryland Array
DRAO Dominion Radio Astrophysical Observatory
FIRST Fleurs Synthesis Telescope
GBT Green Bank Telescope
LOFAR Low�Frequency Array
MOST Molonglo Observatory Synthesis Telescope
NRAO National Radio Astronomy Observatory
NRO Nobeyama Radio Observatory
TPT Clark Lake Teepee�Tee telescope
VLA Very Large Array
WSRT Westerbork Synthesis Radio Telescope
(C/S/V)GPS (Canadian/Southern/VLA) Galactic Plane Survey
Satellites
Optical/IR: AKARI, Herschel (also sub�mm), HST (Hubble Space Telescope), ISO (Infrared Space Obser�
vatory), IRAS (Infrared Astronomical Satellite), Spitzer.
X�/#�ray: ASCA (Advanced Satellite for Cosmology and Astrophysics), Chandra, EXOSAT (European X�
ray Observatory Satellite), Fermi, NuSTAR (Nuclear Spectroscopic Telescope Array), ROSAT
(R�ontgensatellit), RXTE (Rossi X�ray Timing Explorer), Suzaku, XMM (X�ray Multi�Mirror(�
Newton)).
2014 May