A Catalogue of Galactic Supernova Remnants

2014 May version

D. A. Green
Cavendish Laboratory
19 J. J. Thomson Avenue
Cambridge CB3 0HE
UNITED KINGDOM

Contents of this document.

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

Other pages.

• The summary listings of all 294 SNRs.
• The detailed listings of all 294 SNRs.
• A list of other names for Galactic SNRs.
• The abbreviations for journals/telescopes used in the detailed listings.
• A frames interface to the catalogue.
• How to get a paper version of the catalogue.
• A feedback comment form.

1. The Catalogue Format

This, the 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 detailed 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.
• 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, α (here defined in the sense, S ∝ ν<sup>−α</sup>, where S is the flux density at a frequency ν), 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.)

The references do not generally include large observational surveys – of particular interest in this respect are: the Effelsberg 100-m survey at 2.7 GHz of the Galactic plane 358° < l < 240°, |b| < 5° by Reich et al. (1990) and Fürst et al. (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 Gonçalves et al. 2011); the catalogue by Fesen & Hurford (1996) of UV/optical/infra-red lines identified in SNRs; Fermi γ-ray catalogues of Abdo et al. (2009, 2010). Also see Ferrand & Safi-Harb (2012), present a census of X-/γ-ray observations of Galactic SNRs and pulsar wind nebulae (PWNe), updates of which are available online.

The catalogue is available as a summary listing of the parameters for each remnant, and as detailed listings (with references) for each object. Also see the list of other names used for these SNRs, and the list of abbreviations for journals, proceedings and telescopes used in the detailed listings.

2. Revisions and Notes

2.1 Objects no longer thought to be SNRs

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).
• 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 identified 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 subsequently 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.

2.2 New SNRs

The following remnants were added to Version III of the catalogue: G4.2−3.5, G5.2−2.6, G6.1+1.2, G8.7−5.0, G13.5+0.2, G15.1−1.6, G16.7+0.1, G17.4−2.3, G17.8−2.6, G30.7−2.0, G36.6+2.6, G43.9+1.6, G59.8+1.2, G65.1+0.6, G68.6−1.2, G69.7+1.0, G279.0+1.1, G284.3−1.8 (=MSH 10−53), G358.4−1.9 and G359.0−0.9 (although, 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).
• 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 & Fürst (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 Hα 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

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).
• Gosachinskiĭ (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, following improved observations (but also see Odegard 1986, who questions the reliability of some of Gosachinskiĭ'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 Gómez-González & del Romero (1983), who report a smaller (about 40 arcmin) possible SNR (G57.1+1.7) associated with this pulsar, and see Caswell, Landecker & Feldman (1985) and Kovalenko (1989).
• Gorham (1990) lists many SNR candidates from the Clark Lake 30.9 MHz survey of the first quadrant, following 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 γ- 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.)
• 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 γ-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 observations 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 (Fürst 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).
• 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).
• Martí 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 filaments seen in Hα 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 wavelengths, 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 & Filipović (2008) report several SNRs identified from Hα 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.

2.3.3 X-ray/γ-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 η 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).

2.4 Questionable SNRs listed in the catalogue

There are also some objects that have been identified as SNRs and are listed in the catalogue, although they have been barely resolved in the available observations, or are faint, and have not been well separated from confusing background or nearby thermal emission, and their identification as SNRs, or at least their parameters remain uncertain.

Acknowledgements

References

• Abdo A. A. et al. 2009, ApJS, 183, 46. ADS
• Abdo A. A. et al. 2010, ApJS, 188, 405. ADS
• Aharonian F. et al. 2006, A&A, 456, 245. ADS
• Aharonian F. et al. 2008a, A&A, 484, 435. ADS
• Aharonian F. et al. 2008b, A&A, 481, 401. ADS
• Alves M. I. R., Davies R. D., Dickinson C., Calabretta M., Davis R. & Staveley-Smith L., 2012, MNRAS, 422, 2429. ADS
• Amenomori M. et al. 2005, ApJ, 635. ADS
• Anderson G. E. et al. 2012, ApJ, 751, 53. ADS
• Andersson B.-G., Wannier P. G., Moriarty-Schieven G. H. & Bakker E. J., 2000, AJ, 119, 1325. ADS
• Arendt R. G., 1989, ApJS, 70, 181. ADS
• Asaoka I. & Aschenbach B., 1994, A&A, 284, 573. ADS
• Bally J. & Reipurth B., 2001, ApJ, 552, L159. ADS
• Bally J. et al. 1989, ApJ, 338, L65. ADS
• Bamba A., Ueno M., Koyama K. & Yamauchi S., 2003, ApJ, 589, 253. ADS
• Becker R. H. & Fesen R. A., 1988, ApJ, 334, L35. ADS
• Becklin E. E., Zuckerman B., McLean I. S. & Geballe T., 1994, ApJ, 430, 774. ADS
• Berkhuijsen E. M., 1973, A&A, 24, 143. ADS
• Bhatnagar S., 2002, MNRAS, 332, 1. ADS
• Bhatnagar S., Rau U., Green D. A. & Rupen M. P., 2011, ApJ, 739, 20. ADS
• Bietenholz M. F., Matheson H., Safi-Harb S., Brogan C. & Bartel N., 2011, MNRAS, 412, 1221. ADS
• Bonsignori-Facondi S. R. & Tomasi P., 1979, A&A, 77, 93. ADS
• Borka V., 2007, MNRAS, 376, 634. ADS
• Boumis P., Dickinson C., Meaburn J., Goudis C. D., Christopoulou P. E., López J. A., Bryce M. & Redman M. P., 2001, MNRAS, 320, 61. ADS
• Boumis P., Mavromatakis F., Paleologou E. V. & Becker W., 2002, A&A, 396, 225. ADS
• Braun R., Goss W. M. & Lyne A. G., 1989, ApJ, 340, 355. ADS
• Brogan C. L., Gelfand J. D., Gaensler B. M., Kassim N. E. & Lazio T. J. W., 2006, ApJ, 639, L25. ADS
• Burrows D. N., Singh K. P., Nousek J. A., Garmire G. P. & Good J., 1993, ApJ, 406, 97. ADS
• Cameron P. B. & Kulkarni S. R., 2007, ApJ, 665, L135. ADS
• Camilo F., Manchester R. N., Gaensler B. M. & Lorimer D. R., 2002, ApJ, 579, L25. ADS
• Camilo F. et al. 2004, ApJ, 611, L25. ADS
• Carey S. J. et al. 2009, PASP, 121, 76. ADS
• Caswell J. L., 1985, AJ, 90, 1224. ADS
• Caswell J. L., 1988, in Supernovae and Supernova Remnants, (IAU Colloquium 145), eds McCray R. & Wang Z., (Cambridge University Press), p269. ADS
• Caswell J. L. & Clark D. H., 1975, AuJPA, 37, 57. ADS
• Caswell J. L. & Stewart R. T., 1991, PASA, 9, 103. ADS
• Caswell J. L., Landecker T. L. & Feldman P. A., 1985, AJ, 90, 488. ADS
• Chang C., Pavlov G. G., Kargaltsev O. & Shibanov Y. A., 2012, ApJ, 744, 81. ADS
• Channan G. A., Helfand D. J., Spinrad H. & Ebneter K., 1986, Nature, 320, 41. ADS
• Cherepashchuk A. M., Goranskij V. P., Karitskaya E. A., Nadjip A. E., Savage A., Shakura N. I., Sunyaev R. A. & Volchkov, A. A., 1994, A&A, 289, 419. ADS
• Clark S. J., Steele I. A. & Langer N., 2000, ApJ, 541, 67. ADS
• Coil A. L. & Ho P. T. P., 2000, ApJ, 533, 245. ADS
• Colomb F. R., Dubner G. M. & Giacani E. B., 1984, A&A, 130, 294. ADS
• Combi J. A. & Romero G. E., 1998, A&AS, 128, 423. ADS
• Combi J. A., Romero G. E. & Arnal E. M., 1998, A&A, 333, 298. ADS
• Combi J. A., Romero G. E. & Benaglia P., 1998, A&A, 333, L91. ADS
• Combi J. A., Testori J. C., Romero G. E. & Colomb F. R., 1995, A&A, 296, 514. ADS
• Combi J. A., Romero G. E., Benaglia P. & Jonas J. L., 2001, A&A, 366, 1047. ADS
• Condon J. J., Cotton W. D., Greisen E. W., Yin Q. F., Perley R. A., Taylor G. B. & Broderick J. J., 1998, AJ, 115, 1693. ADS
• Corbel S. & Eikenberry S. S., 2004, A&A, 419, 191. ADS
• Cowan J. J., Ekers R. D., Goss W. M., Sramek R. A., Roberts D. A. & Branch D., 1989, MNRAS, 241, 613. ADS
• Craig W. W., Hailey C. J. & Pisarski R. L., 1997, ApJ, 488, 307. ADS
• Danilenko A., Kirichenko A., Mennickent R. E., Pavlov G., Shibanov Yu., Zharikov S. & Zyuzin D., 2012, A&A, 540, 28. ADS
• de Muizon M., Strom R. G., Oort M. J. A., Claas J. J. & Braun R., 1988, A&A, 193, 248. ADS
• De Horta A. Y., Collier J. D., Filipović M. D., Crawford E. J., Urošević D., Stootman F. H. & Tothill N. F. H., 2013, MNRAS, 428, 1980. ADS
• Dewdney P. E. & Lozinskaya T. A., 1994, AJ, 108, 2212. ADS
• Dickel H. R., Lortet M.-C. & de Boer K. S., 1987, A&AS, 68, 75. ADS
• Downes D., 1971, AJ, 76, 305. ADS
• Dubner G. M., Colomb F. R. & Giacani E. B., 1986, AJ, 91, 343. ADS
• Dubner G. M., Braun R., Winkler P. F. & Goss 1991, AJ, 101, 1466. ADS
• Dubner G., Giacani E., Cappa de Nicolau C. & Reynoso E., 1992, A&AS, 96, 505. ADS
• Duncan A. R., Stewart R. T., Haynes R. F. & Jones K. L., 1995, MNRAS, 277, 36. ADS
• Duncan A. R., Stewart R. T., Haynes R. F. & Jones K. L., 1996, MNRAS, 280, 252. ADS
• Duncan A. R., Stewart R. T., Haynes R. F. & Jones K. L., 1997, MNRAS, 287, 722. ADS
• Esipov V. F., Lozinskaya T. A., Mel'nikov V. V., Pravdikova V. V., Sitnik T. G. & Nichol-Bohlin J., 1996, ALet, 22, 509. ADS
• Esposito P., de Luca A., Tiengo A., Paizis A., Mereghetti S. & Caraveo, P. A., 2008, MNRAS, 384, 225. ADS
• Ferrand G. & Safi-Harb S., 2012, AdSpR, 49, 1313. ADS
• Fesen R. A. & Milisavljevic D., 2010a, AJ, 140, 1163. ADS
• Fesen R. A. & Milisavljevic D., 2010b, AJ, 139, 2595. ADS
• Fesen R. A. & Hurford A. P., 1996, ApJS, 106, 563. ADS
• Finley J. P., Srinivasan R. & Park S., 1996, ApJ, 466, 938. ADS
• Foster T., Kothes R., Sun X. H., Reich W. & Han J. L., 2006, A&A, 454, 517. ADS
• Foster T. J., Kothes R., Kerton C. R. & Arvidsson K., 2007, ApJ, 667, 248. ADS
• Foster T. J., Cooper B., Reich W., Kothes R. & West, J., 2013, A&A, 549, A107. ADS
• Frail D. A., Goss W. M. & Whiteoak J. B. Z., 1994, ApJ, 437, 781. ADS
• Fürst E., Reich W., Reich P. & Reif K., 1990a, A&AS, 85, 691. ADS
• Fürst E., Reich W., Reich P. & Reif K., 1990b, A&AS, 85, 805. ADS
• Gaensler B. M., 1998, ApJ, 493, 781. ADS
• Gaensler B. M., Stappers B. W., Frail D. A., Moffett D. A., Johnston S. & Chatterjee S., 2000, MNRAS, 318, 58. ADS
• Gaensler B. M., Slane P. O., Gotthelf E. V. & Vasisht G., 2001, ApJ, 559, 963. ADS
• Gaensler B. M., Tanna A., Slane P. O., Brogan C. L., Gelfand J. D., McClure-Griffiths N. M., Camilo F., Ng C.-Y. & Miller J. M., 2008, ApJ, 680, L37. ADS
• Gahm G. F., Gebeyehu M., Lindgren M., Magnusson P., Modigh P. & Nordh H. L., 1990, A&A, 228, 477. ADS
• Gallo E., Fender R., Kaiser C., Russell D., Morganti R., Oosterloo T. & Heinz S., 2005, Nature, 436, 819. ADS
• Gao X. Y. & Han J. L., 2013, A&A, 551, 16. ADS
• Gao X. Y., Sun X. H., Han J. L., Reich W., Reich P. & Wielebinski R., 2011, A&A, 532, A144. ADS
• Giacani E. B., Frail D. A., Goss W. M. & Vieytes M., 2001, AJ, 121, 3133. ADS
• Gómez-González J. & del Romero A., 1983, A&A, 123, L5. ADS
• Gorham P. W., 1990, ApJ, 364, 187. ADS
• Gorham P. W., Kulkarni S. K. & Prince T. A., 1993, AJ, 105, 314. ADS
• Gosachinskiĭ I. V., 1985, SvA, 29, 128. ADS
• Goss W. M. & Lozinskaya T. A., 1995, ApJ, 439, 637. ADS
• Gray A. D., 1994a, MNRAS, 270, 835. ADS
• Gray A. D., 1994b, MNRAS, 270, 847. ADS
• Green A. J., Cram L. E., Large M. I. & Ye T. S., 1999, ApJS, 122, 207. ADS
• Green D. A., 1984, MNRAS, 209, 449. (Version I) ADS
• Green D. A., 1986, MNRAS, 219, 39P. ADS
• Green D. A., 1988, Ap&SS, 148, 3. (Version II) ADS
• Green D. A., 1990, AJ, 100, 1241. ADS
• Green D. A., 1991, PASP, 103, 209. (Version III) ADS
• Green D. A., 1996, in Supernovae and Supernova Remnants, (IAU Colloquium 145), eds McCray R. & Wang Z., (Cambridge University Press), p.419. (Version IV) ADS
• Green D. A., 2004, BASI, 32, 335. (Version V) ADS
• Green D. A., 2009a, BASI, 37, 45. (Version VI) ADS
• Green D. A., 2009b, MNRAS, 399, 177. ADS
• Green D. A. & Gull S. F., 1984, Nature, 312, 527. ADS
• Green D. A. & Gull S. F., 1986, Nature, 320, 42. ADS
• Green D. A. & Joncas G., 1994, A&AS, 104, 481. ADS
• Grenier I. A., Lebrun F., Arnaud M., Dame T. M. & Thaddeus P., 1989, ApJ, 347, 231. ADS
• Hailey C. J. & Craig W. W., 1995, ApJ, 455, L151. ADS
• Halpern J. P., Camilo F., Gotthelf E. V., Helfand D. J., Kramer M., Lyne A. G., Leighly K. M. & Eracleous M., 2001, ApJ, 552, L125. ADS
• Heard V. & Warwick R. S., 2013, MNRAS, 434, 1339. ADS
• Heiles C., 1998, ApJ, 498, 689. ADS
• Heinz S. et al. 2013, ApJ, 779, 171. ADS
• Helfand D. J. & Channan G. A., 1989, AJ, 98, 1652. ADS
• Helfand D. J., Becker R. H., White R. L., Fallon A. & Tuttle S., 2006, AJ, 131, 2525. ADS
• Henley D. B. & Shelton R. L., 2009, ApJ, 701, 1880. ADS
• Hewitt J. W. & Yusef-Zadeh F., 2009, ApJ, 694, L16. ADS
• Ho P. T., Jackson J. M., Barrett A. H. & Armstrong J. T., 1985, ApJ, 288, 575. ADS
• Hui C. Y. & Becker W., 2007, A&A, 470, 965. ADS
• Hui C. Y., Seo K. A., Huang R. H. H., Trepl L., Woo Y. J., Lu T.-N., Kong A. K. H. & Walter F. M., 2012, ApJ, 750, 7. ADS
• Hurley-Walker N. et al. 2009, MNRAS, 398, 249. ADS
• Ilovaisky S. A. & Lequeux J, 1972, A&A, 18, 169. ADS
• Johanson A. K. & Kerton C. R., 2009, AJ, 138, 1615. ADS
• Jones B. B., 1973, AuJPh, 26, 545. ADS
• Jones T. J., Garwood R. & Dickey J. M., 1988, ApJ, 328, 559. ADS
• Kang J.-H. & Koo B.-C., 2007, ApJS, 173, 85. ADS
• Kang J., Koo, B.-C. & Salter C., 2012, AJ, 143, 75. ADS
• Kaplan D. L., Kulkarni S. R., Frail D. A. & van Kerkwijk M. H., 2002, ApJ, 566, 378. ADS
• Kargaltsev O., Schmitt B. M., Pavlov G. G. & Misanovic Z., 2012, ApJ, 745, 99. ADS
• Kaspi V. M., Roberts M. S. E. & Harding A. K., 2006, in Compact stellar X-ray sources, (Cambridge Astrophysics Series, Volume 39), eds by Lewin W. & van der Klis M., (Cambridge University Press), p279. ADS
• Kassim N. E., 1988, ApJ, 328, L55. ADS
• Kassim N. E., 1989, ApJS, 71, 799. ADS
• Kerton C. R., Murphy J. & Patterson J., 2007, MNRAS, 379, 289. ADS
• Kijak J., Tarczewski L., Lewandowski W. & Melikidze G., 2013, ApJ, 772, 29. ADS
• Kim K.-T. & Koo B.-C., 2000, ApJ, 529, 229. ADS
• Koo B.-C. & Heiles C., 1991, ApJ, 382, 204. ADS
• Koo B.-C., Kang J. H. & Salter C. J., 2006, ApJ, 643, L49. ADS
• Kothes R., 2003, A&A, 408, 187. ADS
• Kothes R., Fedotov K., Foster T. J. & Uyanıker B., 2006, A&A, 457, 1081. ADS
• Kovalenko A. V., 1989, SvAL, 15, 144. ADS
• Kovalenko A. V., Pynzar' A. V. & Udal'tsov V. A., 1994, ARep, 38, 95. ADS
• Koyama K. et al. 2007, PASJ, 59, S221. ADS
• Landecker T. L., Higgs L. A. & Wendker H. I., 1993, A&A, 276, 522. ADS
• Langston G., Minter A., D'Addario L., Eberhart K., Koski K. & Zuber J., 2000, AJ, 119, 2801. ADS
• LaRosa T. N., Kassim N. E., Lazio T. J. W. & Hyman S. D., 2000, AJ, 119, 207. ADS
• Law C. J., Yusef-Zadeh F. & Cotton W. D., 2008, ApJS, 177, 515. ADS
• Lazio T. J. W., Anantharamaiah K. R., Goss W. M., Kassim N. E. & Cordes J. M., 1999, ApJ, 515, 196. ADS
• Leahy D. A., Nousek J. & Garmire G., 1992, ApJ, 385, 561. ADS
• Leahy D. A., Tian W. & Wang Q. D., 2008, AJ, 136, 1477. ADS
• Lee J.-J., Koo B.-C., Yun M. S., Stanimirović S, Heiles C. & Heyer M., 2008, AJ, 135, 796. ADS
• Lu F. J., Wang Q. D. & Lang C. C., 2003, AJ, 126, 319. ADS
• Maciejewski W., Murphy E. M., Lockman F. J. & Savage B. D., 1996, ApJ, 469, 238. ADS
• McClure-Griffiths N. M., Green A. J., Dickey J. M., Gaensler B. M., Haynes R. F. & Wieringa M. H., 2001, ApJ, 551, 394. ADS
• McCullough P. R., Fields B. D. & Pavlidou V., 2002, ApJ, 576, L41. ADS
• Manchester R. N. et al. 2002, in Neutron Stars in Supernova Remnants, (ASP Conference Series, Volume 271), eds Slane P. O. & Gaensler B. M., (ASP, San Francisco), p.31. ADS
• Marston A. P., 1996, AJ, 112, 2828. ADS
• Martí J., Combi J. A., Pérez-Ramírez D., Garrido J. L., Luque-Escamilla P., Muñoz-Arjonilla A. J. & Sánchez-Sutil, J. R., 2007, A&A, 462, 1065. ADS
• Mavromatakis F. & Strom R. G., 2002, A&A, 382, 291. ADS
• Mavromatakis F., Boumis P. & Paleologou E. V., 2002, A&A, 387, 635. ADS
• Mavromatakis F., Boumis P., Xilouris E., Papamastorakis J. & Alikakos J., 2005, A&A, 435, 141. ADS
• Mavromatakis F., Boumis P., Meaburn J. & Caulet A., 2009, A&A, 503, 129. ADS
• Milne D. K., 1970, AuJPh, 23, 425. ADS
• Milne D. K., 1979, AuJPh, 32, 83. ADS
• Misanovic Z., Cram L. & Green A., 2002, MNRAS, 335, 114. ADS
• Mizuno D. R., Kraemer K. E., Flagey N., Billot N., Shenoy S., Paladini R., Ryan E., Noriega-Crespo A. & Carey S. J., 2010, AJ, 139, 1542. ADS
• Mori H., Tsuru T. G., Hyodo Y., Koyama K. & Senda, A., 2008, PASJ, 60, S183. ADS
• Morris P. W., Stolovy S., Wachter S., Noriega-Crespo A., Pannuti T. G. & Hoard D. W., 2006, ApJ, 640, L179. ADS
• Nakashima S., Nobukawa M., Tsuru T. G., Koyama K. & Uchiyama H., 2010, PASJ, 62, 971. ADS
• Naranan S., Shulman S., Friedman H. & Fritz G., 1976, ApJ, 208, 718. ADS
• Nichols-Bohlin J. & Fesen R. A., 1993, AJ, 105, 672. ADS
• Nobukawa M. et al. 2008, PASJ, 60, S191. ADS
• Normandeau M., Taylor A. R., Dewdney P. E. & Basu S., 2000, AJ, 119, 2982. ADS
• Nousek J. A., Cowie L. L., Hu E., Lindblad C. J. & Garmire G. P., 1981, ApJ, 248, 152. ADS
• Odegard N., 1986, AJ, 92, 1372. ADS
• Olano C. A., Meschin P. I. & Niemela, V. S., 2006, MNRAS, 369, 867. ADS
• Onello J. S., DePree C. G., Phillips J. A. & Goss W. M., 1995, ApJ, 449, L127. ADS
• Pagani L., Lefèvre C., Bacmann A. & Steinacker J., 2012, A&A, 541, A154. ADS
• Parker Q. A. et al. 2006, MNRAS, 373, 79. ADS
• Pauls T. & Schwartz P. R., 1989, in The Physics and Chemistry of Interstellar Molecular Clouds, (Lecture Notes in Physics, Volume 331), eds Winnewisser G. & Armstrong T. J. (Springer), p.225. ADS
• Pavlov G. G., Kargaltsev O. & Brisken W. F., 2008, ApJ, 675, 683. ADS
• Phillips J. P. & Ramos-Larios G., 2008, MNRAS, 390, 1170. ADS
• Phillips J. A., Onello J. S. & Kulkarni S. R., 1993, ApJ, 415, L143. ADS
• Pineault S. & Chastenay P., 1990, MNRAS, 246, 169. ADS
• Pinheiro Gonçalves D., Noriega-Crespo A., Paladini R., Martin P. G. & Carey S. J., 2011, ApJ, 142, 47. ADS
• Plucinsky P. P., 2009, AIPC, 1156, 231. ADS
• Plucinsky P. P., Snowden S. L., Aschenbach B., Eggar R., Edgar R. J. & McCammon D., 1996, ApJ, 463, 224. ADS
• Polcaro V. F., Rossi C., Norci L. & Viotti R., 1995, A&A, 303, 211. ADS
• Predehl P. & Kulkarni S. R., 1995, A&A, 294, L29. ADS
• Prinz T. & Becker W., 2012, A&A, 544, A7. ADS
• Prinz T. & Becker W., 2013, A&A, 550, A33. ADS
• Punsly B., Romero G. E., Torres D. F. & Combi J. A., 2000, A&A, 364, 552. ADS
• Reach W. T. et al. 2006, AJ, 131, 1479. ADS
• Rector T. A. & Schweiker H., 2013, AJ, 145, 35. ADS
• Reich W., 2002, in Neutron Stars, Pulsars, and Supernova Remnants, (MPE Report 278), eds Becker W., Lesch H. & Trümper J., (Max-Plank-Institut für extraterrestrische Physik, Garching bei München), p1. ADS
• Reich W., Zhang X. & Fürst E., 2003, A&A, 408, 961. ADS
• Reich W., Fürst E., Altenhoff W. J., Reich P. & Junkes N., 1985, A&A, 151, L10. ADS
• Reich W., Fürst E., Reich P. & Reif K., 1990, A&AS, 85, 633. ADS
• Reipurth B., Bally J. & Divine D., 1997, AJ, 114, 2708. ADS
• Renaud M., Paron S., Terrier R., Lebrun F., Dubner G., Giacani E. & Bykov A. M., 2006, ApJ, 638, 220. ADS
• Renaud M., Marandon V., Gotthelf E. V., Rodriguez J., Terrier R., Mattana F., Lebrun F., Tomsick J. A. & Manchester, R. N., 2010, ApJ, 716, 663. ADS
• Retallack D. S., 1983, MNRAS, 204, 669. ADS
• Reynolds R., 1976, ApJ, 206, 679. ADS
• Reynolds M. T., Miller J. M., Maitra D., Gultekin K., Gehrels N., Kennea J. A., Siegel M. H., Gelbord J. M. & Kuin P., 2012, ATel, 3963. ADS
• Reynolds M. T. et al. 2013, ApJ, 766, 112. ADS
• Reynoso E. M. & Dubner G. M., 1997, A&AS, 123, 31. ADS
• Rho J. & Petre R., 1998, ApJ, 503, L167. ADS
• Riegler G. R., Agrawal P. C. & Gull S. F., 1980, ApJ, 235, L71. ADS
• Robbins W. J., Gaensler B. M., Murphy T., Reeves S. & Green, A. J., 2012, MNRAS, 419, 2623. ADS
• Roberts M. S. E. & Brogan C. L., 2008, ApJ, 681, 320. ADS
• Roberts M. S. E., Romani R. W., Johnston S. & Green A. J., 1999, ApJ, 515, 712. ADS
• Roberts M. S. E., Romani R. W. & Johnston S., 2001, ApJ, 561, L187. ADS
• Routledge D. & Vaneldik J. F., 1988, ApJ, 326, 751. ADS
• Roy S. & Pal S., 2013, ApJ, 774, 150. ADS
• Roy S. & Pramesh Rao A., 2002, MNRAS, 329, 775. ADS
• Russeil D., Adami C., Amram P., Le Coarer E., Georgelin Y. M., Marcelin M. & Parker Q., 2005, A&A, 429, 497. ADS
• Russell D. M., Fender R. P., Gallo E. & Kaiser C. R., 2007, MNRAS, 376, 1341. ADS
• Ryu K. et al. 2006, ApJ, 644, L185. ADS
• Sabin L. et al. 2013, MNRAS, 431, 279. ADS
• Saken J. M., Fesen R. A. & Shull J. M., 1992, ApJS, 81, 715. ADS
• Sarma A. P., Goss W. M., Green A. J. & Frail D. A., 1997, ApJ, 483, 335. ADS
• Sawada M., Tsujimoto M., Koyama K., Law C. J., Tsuru T. G. & Hyodo Y., 2009, PASJ, 61, S209. ADS
• Schaudel D., Beck W., Voges W., Aschenbach B., Reich W. & Weisskopf M., 2002, in Neutron Stars in Supernova Remnants, (ASP Conference Series, Volume 271), eds Slane P. O. & Gaensler B. M., (ASP, San Francisco), p.391. ADS
• Senda A., Murakami H. & Koyama K., 2002, ApJ, 565, 1017. ADS
• Senda A., Murakami H. & Koyama K., 2003, AN, 324 (Supplement 1), 151. ADS
• Shinn J.-H. et al. 2007, ApJ, 670, 1132. ADS
• Snowden S. L., Burrows D. N., Sanders W. T., Aschenbach B. & Pfeffermann E., 1995, ApJ, 439, 399. ADS
• Soberski S., Reich W. & Wielebinski R., 2005, in Astronomical Polarimetry: Current Status and Future Directions, (ASP Conference Series, Volume 271), eds Adamson A., Aspin C., Davis C. J. & Fujiyoshi T., (ASP, San Francisco), p.286. ADS
• Sramek R. A., Cowan J. J., Roberts D. A., Goss W. M. & Ekers R. D., 1992, AJ, 104, 704. ADS
• Stephenson F. R. & Green D. A., 2002, Historical Supernovae and their Remnants, (Oxford University Press). ADS
• Stil J. M. & Irwin J. A., 2001, ApJ, 563, 816. ADS
• Stil J. M., Taylor A. R., Dickey J. M., Kavars D. W., Martin P. G., Rothwell T. A., Boothroyd A. I., Lockman F. J. & McClure-Griffiths N. M., 2006, AJ, 132, 1158. ADS
• Stupar M. & Parker Q. A., 2011, MNRAS, 414, 2282. ADS
• Stupar M., Parker Q. A. & Filipović M. D., 2008, MNRAS, 390, 1037. ADS
• Stupar M., Parker Q. A. & Filipović M. D., 2010, MNRAS, 401, 1760. ADS
• Stupar M., Parker Q. A. & Filipović M. D., 2011, Ap&SS, 332, 241. ADS
• Stupar M. & Parker Q. A., 2012, MNRAS, 419, 1413. ADS
• Subrahmanyan R., Ekers R. D., Wilson W. E., Goss W. M. & Allen D. A., 1993, MNRAS, 263, 868. ADS
• Sun X. H., Reich P., Reich W., Xiao L., Gao X. Y. & Han J. L., 2011, A&A, 536, A83. ADS
• Tateyama C. E., Strauss F. M. & Kaufmann P., 1991, MNRAS, 249, 716. ADS
• Taylor A. R., Wallace B. J. & Goss W. M., 1992, AJ, 103, 931. ADS
• Thompson D. J., Djorgovski S. & de Carvalho R. R., 1991, PASP, 103, 487. ADS
• Thorsett S. E., Benjamin R. A., Brisken W. F., Golden A. & Goss W. M., 2003, ApJ, 592, L71. ADS
• Tian W. W. & Leahy D. A., 2006, A&A, 455, 1053. ADS
• Trushkin S. A., 1998, BSAO, 46, 62. ADS
• Trushkin S. A., 2001, in Exploring the gamma-ray universe, eds Battrick N., Gimenez A., Reglero V. & Winkler C., (ESA, Noordwijk), p109. ADS
• Tsuru T. G., Nobukawa M., Nakajima H., Matsumoto H., Koyama K. & Yamauchi S., 2009, PASJ, 61, S219. ADS
• Ueno M., Yamaguchi H., Koyama K., Bamba A., Yamauchi S. & Ebisawa K., 2005, in X-Ray and Radio Connections, eds Sjouwerman L. O. & Dyer K. K., (4.18). ADS
• Ueno M., Yamauchi S., Bamba A., Yamaguchi H., Koyama K. & Ebisawa K., 2006, IAUS, 230, 333. ADS
• Uyanıker B. & Kothes R., 2002, ApJ, 574, 805. ADS
• Velusamy T., Goss W. M. & Arnal E. M., 1986, JApA, 7, 105. ADS
• Walker A. & Zealey W. J., 1998, PASA, 15, 79. ADS
• Walker A., Zealey W. J. & Parker Q. A., 2001, PASA, 18, 259. ADS
• Wang Q. D., Lu F. J. & Gotthelf E. V., 2006, MNRAS, 367, 937. ADS
• Ward-Thompson D. & Robson E. I., 1991, MNRAS, 248, 670. ADS
• Weiler K. W. & Shaver P. A., 1978, A&A, 65, 305. ADS
• Weinberger R., 1995, PASP, 107, 58. ADS
• Weinberger R., Temporin S. & Stecklum B., 2006, A&A, 448, 1095. ADS
• Wendker H. I., Higgs L. A. & Landecker T. L., 1991, A&A, 241, 551. ADS
• Wendker H. I., Higgs L. A., Landecker T. L. & Ward-Thompson D., 1993, MNRAS, 263, 543. ADS
• White R. L. & Becker R. H., 1990, MNRAS, 244, 12P. ADS
• White R. L., Becker R. H. & Helfand D. J., 2005, AJ, 130, 586. ADS
• Whiteoak J. B. Z. & Green A. J., 1996, A&AS, 118, 329. ADS
• Winkler P. F. & Reipurth B., 1992, ApJ, 389, L25. ADS
• Winkler P. F., Kirshner R. P., Hughes J. P. & Heathcote S. R., 1989, Nature, 337, 48. ADS
• Woermann B., Gaylard M. J. & Otrupcek R., 2001, MNRAS, 325, 1213. ADS
• Yoshita K., Miyata E. & Tsunemi H., 1999, AN, 320, 344. ADS
• Yoshita K., Miyata E. & Tsunemi H., 2000, PASJ, 52, 867. ADS
• Yusef-Zadeh F., Cotton W. D. & Reynolds S. P., 1998, ApJ, 498, L55. ADS
• Yusef-Zadeh F., Shure M., Wardle M. & Kassim N., 2000, ApJ, 540, 842. ADS
• Zhang X. Z., 2003, AcASn, 44 (Supplement), 183. ADS
• Zijlstra A. A., 1991, MNRAS, 248, 11P. ADS