G298.5-0.3 (Fig. 4) This object consists of a bright, narrow ridge of length 
G298.5-0.3 6' and possibly two other ridges lying parallel to the north-west. 
G298.5-0.3 These are situated in a complex of HII emission. Comparison with 
G298.5-0.3 60um data shows that the brightest ridge is non-thermal, while the
G298.5-0.3 results are inconclusive for the other two ridges. If the main ridge
G298.5-0.3 alone is non-thermal, then the source may be extragalactic. If 
G298.5-0.3 either of the other two ridges is also nonthermal, then the source 
G298.5-0.3 is more likely a shell or composite SNR. Because of their similar 
G298.5-0.3 orientation, it seems likely that the ridges are all associated and 
G298.5-0.3 hence lie in our Galaxy. Higher resolution observations are required
G298.5-0.3 to aid interpretation of this object.
G298.6-0.0 (Fig. 5) An incomplete shell SNR. The MOST flux density of 
G298.6-0.0 S_0.843_=7.4Jy is much larger than that expected from the previous 
G298.6-0.0 flux density estimates of  S_0.408_=5.6Jy (Shaver & Goss,
G298.6-0.0 1970AuJPS..14..133S; Green 1974A&AS...18..267G and S_5_=3.2Jy 
G298.6-0.0 (Shaver & Goss, 1970AuJPS..14..133S). However, the remnant lies in 
G298.6-0.0 a complex region near two bright extended H II regions, and 
G298.6-0.0 previous measurements may have been affected by confusion.
G302.3+0.7 (Fig.5) An SNR with evidence of a biannular structure in which a 
G302.3+0.7 smaller (diameter ~11') annulus in the south-east overlaps a larger 
G302.3+0.7 (diameter ~14') annulus in the north-west, both incomplete. The 
G302.3+0.7 brightest emission occurs along the south-western and north-eastern
G302.3+0.7 borders, and a single, faint filament of length 10' lies outside 
G302.3+0.7 the remnant in the south. Although confusion occurs because of the 
G302.3+0.7 presence of a weak grating artifact in the region, the western end 
G302.3+0.7 of the filament apparently intersects the remnant, while the eastern
G302.3+0.7 end projects towards a faint unresolved source lying several 
G302.3+0.7 arcminutes away. Higher-sensitivity observations are required to 
G302.3+0.7 determine if an association exists between the filament and the 
G302.3+0.7 unresolved source, and also between the filament and the SNR. The 
G302.3+0.7 filament resembles other non-thermal filaments found at the Galactic
G302.3+0.7 centre that are apparently associated with SNRs (e.g. Gray et al. 
G302.3+0.7 1991Natur.353..237G). The northern half of the remnant is partly 
G302.3+0.7 confused with an H II region lying to the north-west.
G308.7+0.0 (Comment added at CDS) The WWW version of the catalogue at
G308.7+0.0 http://www.physics.usyd.edu.au/astrop/wg96cat/msc.a.html
G308.7+0.0 states that "G308.8-0.1 is (incorrectly) referred to as G308.7+0.0 
G308.7+0.0 in the printed version of the catalogue (end of comment added at CDS)
G308.7+0.0 (Fig.6) The source consists of a bright, elongated structure of 
G308.7+0.0 extent 9'x 3' (P.A.=70{deg}) lying within faint, diffuse nebulosity 
G308.7+0.0 of dimensions 22'x7' elongated at a similar position angle. Using 
G308.7+0.0 the Fleurs synthesis radio telescope at 1.415GHz, Caswell et al. 
G308.7+0.0 (1981MNRAS.195...89C) found evidence of shell-like structure in the 
G308.7+0.0 brighter component, supported by the MOST contour map, although
G308.7+0.0 they note that if G308.7+0.0 is a shell SNR, then its appearance is 
G308.7+0.0 peculiar because it does not have the characteristic sharply-defined
G308.7+0.0 outer perimeter. In addition, the emission is significantly more 
G308.7+0.0 elongated than for a typical shell remnant. This structure suggests 
G308.7+0.0 that G308.7+0.0 may instead be an example of a plerionic remnant 
G308.7+0.0 with unusual morphology. A faint but well-defined arc of length 15'
G308.7+0.0 lies 20' to the south-east at RA=13h43m25s, DE=-62{deg}34'(J2000). 
G308.7+0.0 Caswell et al. (1992ApJ...399L.151C) suggest that this may be part 
G308.7+0.0 of a large-diameter shell (G308.8-0.1), with G308.7+0.0 forming the 
G308.7+0.0 north-western rim, which would then explain its elongation. There is
G308.7+0.0 widespread thermal radiation from much of this area, including the
G308.7+0.0 H II region in the north-eastern corner of the image, the bright 
G308.7+0.0 compact source at RA=13h43m1.8s, DE=-62{deg}08'56"(J2000), and 
G308.7+0.0 general diffuse thermal emission covering the field, making it 
G308.7+0.0 difficult to decide what is non-thermal. The prominent bar on the 
G308.7+0.0 western end of the arc appears to be thermal and therefore probably 
G308.7+0.0 unrelated to the remnant. The non-thermal extension from the 
G308.7+0.0 southern side of G308.7+0.0 contains a knot at RA=13h41m42.3s,
G308.7+0.0 DE=-62{deg}20'12"(J2000). This knot lies close to the young pulsar 
G308.7+0.0 PSR J1341-6220 (Kaspi et al., 1992ApJ...399L.155K), although an 
G308.7+0.0 association is still to be confirmed. It is interesting to note that
G308.7+0.0 a striking resemblance exists between G308.7+0.0 and G320.4-1.2
G308.7+0.0 (Fig.12). Both remnants contain loosely-connected structures of 
G308.7+0.0 which the north-western component more closely resembles plerionic 
G308.7+0.0 structure than part of a shell. Furthermore, the southern extensions
G308.7+0.0 of the north-western components of both these SNRs also contain 
G308.7+0.0 known pulsars
G309.2-0.6 (Fig.7) A complex SNR with a biannular structure consisting of 
G309.2-0.6 multiple arcs of different curvature and an axis of symmetry at 
G309.2-0.6 PA=45{deg}. The overall shape of the remnant suggests that 
G309.2-0.6 'blowouts' may occurred in the north-east and south-west. The faint 
G309.2-0.6 emission north of the remnant is thermal.
G309.8+0.0 (Fig.7) Abundant thread-like emission exists within this shell, 
G309.8+0.0 apparently extending outside the shell boundary in the west. A 
G309.8+0.0 bright point source occurs at RA=13h50m35.2s, DE=-62{deg}00'42"
G309.8+0.0 (J2000), approximately 4' north of the geometric centre of the
G309.8+0.0 object, for which Caswell et al. (1980MNRAS.190..881C) find a 
G309.8+0.0 possible optical counterpart lying within 2". They measure its 
G309.8+0.0 1.415GHz flux density to be S_1.415_=0.23Jy, while the MOST 
G309.8+0.0 observations give S_0.843_=0.39Jy, producing a spectral index of 
G309.8+0.0 {alpha}^1.415^_0.843_=-1.0. This is consistent with a background
G309.8+0.0 extragalactic source. The low Galactic latitude suggests that the 
G309.8+0.0 optical identification may then be a chance stellar coincidence.
G310.6-0.3 (Fig.8) This source has been the subject of some controversy. 
G310.6-0.3 Previous observations (e.g. Milne, 1969AuJPh..22..613M; 
G310.6-0.3 Green 1974A&AS...18..267G; Caswell & Clark, 1975AuJPA..37...57C) 
G310.6-0.3 were unable to separate the shell from the compact source lying 1' 
G310.6-0.3 to the east. Both sources are found to be non-thermal in this work 
G310.6-0.3 by comparing radio and 60um IRAS data. However, the compact source 
G310.6-0.3 is possibly extragalactic. Originally, Milne (1969AuJPh..22..613M) 
G310.6-0.3 identified the shell source as an SNR.  However, Caswell & Clark 
G310.6-0.3 (1975AuJPA..37...57C) later concluded that the emission was probably
G310.6-0.3 thermal, based on a calculation of the flux density which indicated 
G310.6-0.3 a reasonably flat spectral index. The present high-resolution 
G310.6-0.3 observations, which are not as susceptible to confusion as the 
G310.6-0.3 earlier observations confirm the original indentification as an SNR.
G310.6-0.3 However, an accurate estimation of the spectral index awaits further
G310.6-0.3 observations at other frequencies.
G310.8-0.4 (Fig.8) An SNR consisting of a bright arc in the east. The western 
G310.8-0.4 half of the shell is seen only faintly and may be confused with 
G310.8-0.4 diffuse thermal emission in the region. Comparison with 60um IRAS 
G310.8-0.4 images confirms that the bright arc is non-thermal. The structure
G310.8-0.4 lies in the same complex thermal region as G310.6-0.3, and there has
G310.8-0.4 been some debate about whether it is thermal or non-thermal. Milne 
G310.8-0.4 (1969AuJPh..22..613M) originally dentified the source as an SNR. By 
G310.8-0.4 contrast, Caswell & Clark (1975AuJPA..37...57C) concluded that it 
G310.8-0.4 was probably thermal on the basis of its fiat spectral index 
G310.8-0.4 ({alpha}=^5^_0.408_=-0.20) and the apparent detection of hydrogen 
G310.8-0.4 recombination line emission (Dickel & Milne, 1972AuJPh..25..539D). 
G310.8-0.4 However, the recombination lines were probably produced by the 
G310.8-0.4 bright compact H II region which lies at the northern end of the arc
G310.8-0.4 and the abundant thermal filamentary emission to the west, both of 
G310.8-0.4 which are confused with the arc in previous low-resolution (~3')
G310.8-0.4 observations.
G311.5-0.3 (Fig.8) A small-diameter shell SNR. The resolution is not high 
G311.5-0.3 enough to allow a detailed ex-amination of the structure, but the 
G311.5-0.3 MOST observations show for the first time that the object is a shell
G312.4-0.4 (Fig.9) An irregular SNR with an overall shell structure. The shell 
G312.4-0.4 edge is sharp and well-defined in the north and east, but is more 
G312.4-0.4 diffuse on other sides. The emission weakens towards the south of 
G312.4-0.4 G312.4-0.4, giving the remnant a horseshoe appearance. A previously
G312.4-0.4 undetected faint arc, concave to the body of the remnant, lies 12' 
G312.4-0.4 to the south, and there is evidence of a second filament of even 
G312.4-0.4 fainter emission between this arc and the remnant. Variation in the 
G312.4-0.4 density of the local ISM may account for the strong asymmetry in 
G312.4-0.4 this remnant, with a cavity to the south of the pre-SN star perhaps 
G312.4-0.4 necessary to explain the large distance of the southern arc from the
G312.4-0.4 remainder of the emission. Observations of G312.4-0.4 were made with
G312.4-0.4 the Parkes radiotelescope at 4.5 and 8.55GHz in both total intensity
G312.4-0.4 and linearly polarised intensity (Whiteoak, 1993, Ph.D. Thesis, 
G312.4-0.4 University of Sydney). Polarisation of up to 15% was detected at 
G312.4-0.4 8.55GHz, while flux densities of S_4.5_=30+/-2Jy and 
G312.4-0.4 S_8.55_=17+/-4Jy were measured. In conjunction with the flux 
G312.4-0.4 densities determined by Caswell & Barnes (1985MNRAS.216..753C) of 
G312.4-0.4 S_0.408_=56Jy and S_5_=28Jy, a spectral index of 
G312.4-0.4 {alpha}=^8.55^_0.408_=-0.36+/-0.09 is derived.
G315.4-0.3 (Fig.9) A remnant with a puzzling structure. The image shows two 
G315.4-0.3 bright small-diameter sources in the field, a faint narrow arc in 
G315.4-0.3 the south-western corner of length ~20', and several complex 
G315.4-0.3 streamers of filamentary emission in the centre. The unresolved 
G315.4-0.3 source at RA=14h37m01.5s, DE=-60{deg}27'40" (J2000) is non-thermal, 
G315.4-0.3 has a steep spectral index, and may be extragalactic (Caswell et al.
G315.4-0.3 1981MNRAS.195...89C). The MOST observations show that the 
G315.4-0.3 small-diameter source (G315.31-0.27) situated within the extended 
G315.4-0.3 emission at RA=14h35m06s, DE=-60{deg}37'30" (J2000) with 
G315.4-0.3 S_0.843_=0.87Jy has a close double structure. Previous work 
G315.4-0.3 indicates that its spectral index is flat (Clark et al., 
G315.4-0.3 1975AuJPA..37....1C; Caswell et al., 1981MNRAS.195...89C), and it 
G315.4-0.3 has hydrogen recombination line emission (Caswell & Haynes, 
G315.4-0.3 1987A&A...171..261C). Comparison with IRAS data shows strong 60um 
G315.4-0.3 emission associated with this source, confirming that it is an H II 
G315.4-0.3 region. The extended emission to the east and north of this HII 
G315.4-0.3 region is non-thermal, although some faint thermal emission may also
G315.4-0.3 exist in the general area. The only well-defined, apparently 
G315.4-0.3 non-thermal, shell component in the field is the arc in the 
G315.4-0.3 south-western corner, and this seems to form a faint semi-circle 
G315.4-0.3 around the H II region.
G315.4-2.3 (Fig.10) A shell remnant with multiple arcs. The brightest emission 
G315.4-2.3 comes from a ridge in the south-western corner which conspicuously 
G315.4-2.3 protrudes outside the line of the main shell. The south-eastern side
G315.4-2.3 of the remnant appears to be composed of two arcs. Little emission 
G315.4-2.3 is visible from the central part of the SNR, but the large angular 
G315.4-2.3 size of this remnant means that a significant portion of its flux 
G315.4-2.3 density will not be detected by the MOST. There is an interesting 
G315.4-2.3 structure within the main shell on the western side which resembles 
G315.4-2.3 yet another shell (diameter ~12') centred at RA=14h41m00s, 
G315.4-2.3 DE=-62{deg}29' (J2000). Optical emission from the nebula RCW 86 is 
G315.4-2.3 associated with the remnant (Hill, 1967AuJPh..20..297H; van den 
G315.4-2.3 Bergh et al., 1973ApJS...26...19V), forming a partial shell (~5'
G315.4-2.3 diameter) at the north-western end of the bright ridge of radio 
G315.4-2.3 emission. An isolated optical filament (Hill, 1967AuJPh..20..297H) 
G315.4-2.3 is well-aligned with the northern part of the radio shell.
G315.9-0.0 (Fig.10) A very low brightness shell. A peculiar feature is a 
G315.9-0.0 straight, narrow jet-like structure extending radially outwards from
G315.9-0.0 the north-western side of the shell. Because the emission is very 
G315.9-0.0 weak, the remnant has not yet been detected at other frequencies, 
G315.9-0.0 and so the significance of the jet is unknown. Comparison of the
G315.9-0.0 MOST image with 60um IRAS data confirms the non-thermal nature of 
G315.9-0.0 the emission.
G318.9+0.4 (Fig.11) A very peculiar composite SNR. The remnant consists of two 
G318.9+0.4 components : a series of narrow, overlapping arcs, and a core 
G318.9+0.4 feature offset to the east within the arc envelope (Whiteoak, 
G318.9+0.4 1990Natur.347..157W, 1993ApJ...415..701W). The overall structure is 
G318.9+0.4 highly elliptical, possessing an envelope that is more elongated 
G318.9+0.4 than any other known Galactic shell remnant. The arcs are all 
G318.9+0.4 unresolved in thickness in the MOST image, and form an unusual cusp 
G318.9+0.4 at the southern end of the object. A north-south oriented ridge lies
G318.9+0.4 within the core component, and a faint jet-like structure extends 
G318.9+0.4 from the eastern side of the core emission towards the adjacent arc.
G320.4-1.2 (Fig.12) An unusual SNR consisting of two loosely connected emission
G320.4-1.2 regions that outline a shell. The brightest emission comes from the 
G320.4-1.2 north-western component and consists of a roughly circular region 
G320.4-1.2 (diameter 10') with a strong central peak. On closer inspection,
G320.4-1.2 the peak is found to be composed of four knots which form a ring of 
G320.4-1.2 diameter 1.3'. The south-eastern component of G320.4-1.2 shows 
G320.4-1.2 strong evidence of radially-oriented features in its emission. These
G320.4-1.2 interlocking arcs could be interpreted as a helical structure. A 
G320.4-1.2 pulsar has been detected in G320.4-1.2 in both the X-ray (Seward &
G320.4-1.2 Harnden, 1982ApJ...256L..45S) and radio (Manchester et al., 
G320.4-1.2 1982ApJ...262L..31M). It lies in the diffuse emission associated 
G320.4-1.2 with the north western radio component at RA=15h13m55.6s, 
G320.4-1.2 DE=-59{deg}08'08" and is designated PSR J1513-5908 (Taylor et al.,
G320.4-1.2 1993ApJS...88..529T). There is some uncertainty attached to the 
G320.4-1.2 SNR/pulsar association, with several authors concluding that it is 
G320.4-1.2 only a chance line-of-sight superposition of two unrelated phenomena
G320.4-1.2 (e.g. van den Bergh & Kamper, 1984ApJ...280L..51V). There is no 
G320.4-1.2 obvious radio counterpart to the X-ray nebula surrounding the pulsar
G320.4-1.2 (Seward et al., 1983ApJ...267..698S, 1984ApJ...281..650S; Seward, 
G320.4-1.2 1990ApJS...73..781S). X-ray emission also arises from the small ring
G320.4-1.2 in the north-western component, while optical emission overlaps this
G320.4-1.2 component from the 10'x8' H{alpha} nebula RCW 89.
G320.6-1.6 (Fig.12) A large-diameter, filamentary remnant with multiple arcs 
G320.6-1.6 and an incomplete shell structure. Two parallel arcs separated by 
G320.6-1.6 10' occur in the south, while the eastern emission consists of a 
G320.6-1.6 series of filaments which taper to a single thread or jet in the 
G320.6-1.6 north-east. The western side of this remnant overlaps the bright 
G320.6-1.6 emission from the remnant G320.4-1.2. Comparison of the MOST image 
G320.6-1.6 with 60um IRAS data shows that G320.6-1.6 is non-thermal, consistent
G320.6-1.6 with the spectral index of {alpha}=^5^_0.408_=-0.47 determined by 
G320.6-1.6 Green (1974A&AS...18..267G).
G321.9-0.3 (Fig.13) An unusual feature of this shell SNR is a 3' extension from
G321.9-0.3 the southern rim that terminates in a knot of emission. Haynes 
G321.9-0.3 (1987AuJPh..40..471H) observed this region with the MOST and found 
G321.9-0.3 evidence of an association between G321.9-0.3 and Circinus X-1, the
G321.9-0.3 variable binary system 10' north of the remnant, whose associated 
G321.9-0.3 radio emission is also shown in the image. He cites as evidence an 
G321.9-0.3 alignment between the peak of Cir X-1, the line of its southern 
G321.9-0.3 extension, the geometrical centre of G321.9-0.3, and the knot lying 
G321.9-0.3 outside the shell of G321.9-0.3 to the south. However, IRAS data 
G321.9-0.3 show significant 60um emission from the southern knot which 
G321.9-0.3 indicates a thermal source probably not associated with the remnant.
G322.5-0.1 (Fig.13) A composite SNR consisting of a circular shell with an 
G322.5-0.1 elliptical plerionic component lying close to the centre, and five 
G322.5-0.1 knots located in the eastern half (Whiteoak, 1992MNRAS.256..121W). 
G322.5-0.1 The compact source at RA=15h23m42.6s, DE=-57{deg}09'25" (J2000) is 
G322.5-0.1 the planetary nebula Pe 2-8 (Perek & Kahoutek, 1967PKCat....c...1P).
G322.5-0.1 Improved estimates for the flux densities are S_0.843_=0.16+/-0.03Jy
G322.5-0.1 for the plerionic component and S_0.843_=1.5+/-0.2Jy for the shell. 
G322.5-0.1 Recent observations with the Parkes radio telescope at 4.5GHz give a
G322.5-0.1 flux density of S_4.5_=0.89+/-0.13Jy, implying an overall spectral 
G322.5-0.1 index of {alpha}=^4.5^_0.843_=-0.37+/-0.16. Little evidence of 
G322.5-0.1 polarised emission was found (Whiteoak, 1993, Ph.D. Thesis, 
G322.5-0.1 University of Sydney) .
G323.5+0.1 (Fig.14) A faint shell remnant with a strangely rectangular shape. 
G323.5+0.1 Comparison with 60um data shows that the bright point source ~2' 
G323.5+0.1 west of the shell centre is thermal and therefore probably unrelated
G323.5+0.1 to the SNR.
G326.3-1.8 (Fig.14) A composite SNR consisting of a filamentary shell and a 
G326.3-1.8 bright plerionic component offset south-west of the centre. The 
G326.3-1.8 whole shell is covered with abundant filamentary emission which is 
G326.3-1.8 predominantly aligned in an east-west direction, coinciding with the
G326.3-1.8 direction of the magnetic field across the remnant (Milne et al., 
G326.3-1.8 1989PASAu...8..187M). The remnant is too extended to allow a 
G326.3-1.8 reliable flux density for the shell Component to be determined
G326.3-1.8 from the MOST observations, but a good estimate can be made for the 
G326.3-1.8 smaller plerionic component of S_0.843_=22Jy. The X-ray emission 
G326.3-1.8 detected by Seward (1990ApJS...73..781S) consists of a diffuse 
G326.3-1.8 component covering the same area as the radio shell, and four 
G326.3-1.8 discrete clumps that lie along a north-east/south-west diagonal 
G326.3-1.8 passing close to the centre of the remnant. However, no X-ray clump 
G326.3-1.8 is coincident with the radio plerionic component. Optical emission 
G326.3-1.8 has also been detected, associated mainly with the northern and 
G326.3-1.8 southern rims, but not the plerionic component (van den Bergh,
G326.3-1.8 1979ApJ...227..497V; Zealey et al., 1979A&A....38...39Z).
G327.1-1.1 (Fig.15) A composite SNR with a faint shell and an unusual 
G327.1-1.1 off-centre plerionic component which is composed of four knots 
G327.1-1.1 forming a ring-like structure of diameter 3'. A peculiar feature is 
G327.1-1.1 a 2' long ridge extending north-west from the western side of the 
G327.1-1.1 plerionic component. The contribution of the plerionic component to 
G327.1-1.1 the total flux density is 2.0Jy. X-ray emission has been detected 
G327.1-1.1 near the plerionic component (Seward, 1990ApJS...73..781S), but
G327.1-1.1 offset ~3' to the west (Lamb & Markert, 1981ApJ...244...94L). The 
G327.1-1.1 small-diameter radio source outside the shell to the south-west
G327.1-1.1 in the image is thermal.
G327.4+0.4 (Fig.15) A remnant possessing an unusual multi-ring structure. 
G327.4+0.4 Milne et al. (1989PASAu...8..187M) observed this SNR with the MOST, 
G327.4+0.4 and described its structure as a series of shells emanating from the
G327.4+0.4 bright eastern rim. Lamb & Markert (1981ApJ...244...94L) report the 
G327.4+0.4 detection of X-ray emission which peaks near the remnant centre. The
G327.4+0.4 X-ray images of Seward (1990ApJS...73..781S) show more detail, 
G327.4+0.4 revealing faint patchy emission with a similar extent to the radio
G327.4+0.4 emission and interspersed with at least four bright concentrations. 
G327.4+0.4 However, none of these concentrations appears to have a radio 
G327.4+0.4 counterpart in the MOST image.
G332.4+0.1 (Fig.17) An irregular shell SNR with a bright narrow rim. The 
G332.4+0.1 eastern rim has a smaller curvature than the western rim, and could 
G332.4+0.1 be interpreted as a second shell or blowout. Roger et al. 
G332.4+0.1 (1985Natur.316...44R) and Kesteven et al. (1987AuJPh..40..855K) have
G332.4+0.1 presented MOST observations showing a jet and plume associated with 
G332.4+0.1 the remnant, with the jet appearing as a faint, narrow extension 
G332.4+0.1 emerging from the north-eastern side of the shell, and joining a 
G332.4+0.1 plume which lies outside the image to the north-east. However, 
G332.4+0.1 comparison with 60um IRAS images shows that both the jet and plume 
G332.4+0.1 are likely to be thermal and probably unrelated to the remnant. 
G332.4+0.1 Indeed, Roger et al. (1985Natur.316...44R) find that the jet has a 
G332.4+0.1 flat spectral index ({alpha}=^8.4^_0.843_=-0.05+/-0.1) and no 
G332.4+0.1 detectable polarisation, both consistent with a thermal origin. The 
G332.4+0.1 plume has the same filamentary structure as the outlying emission of
G332.4+0.1 the nearby bright HII complex RCW 106 and is probably part of this 
G332.4+0.1 emission.
G332.4-0.4 (Fig.18) A much-studied shell remnant (e.g. Dickel et al.,
G332.4-0.4 1996AJ....111..340D). Bright optical filamentary emission has been 
G332.4-0.4 detected from the associated nebula RCW 103 (van den Bergh et al.,
G332.4-0.4 1973ApJS...26...19V). Optical arcs on the southern and north-western
G332.4-0.4 borders coincide with the regions of greatest radio brightness. 
G332.4-0.4 X-ray observations (Nugent et al., 1984ApJ...284..612N; Seward, 
G332.4-0.4 1990ApJS...73..781S) show that the remnant is also a strong source 
G332.4-0.4 of X-ray emission. The Einstein Observatory HRI image of Seward 
G332.4-0.4 (1990ApJS...73..781S) shows a clear X-ray shell with a brightness 
G332.4-0.4 distribution similar to the radio and optical. A compact X-ray 
G332.4-0.4 source has been found very close to the shell centre which might be 
G332.4-0.4 a hot neutron star (Tuohy & Garmire, 1980ApJ...239L.107T), not 
G332.4-0.4 detected in the MOST image above the central disk emission.
G335.2+0.1 (Fig.18) A filamentary shell SNR. A prominent feature of the remnant
G335.2+0.1 is the striated emission within the shell. Comparison with 60um IRAS
G335.2+0.1 maps suggest that the bright point source ~4' west of the shell
G335.2+0.1 centre is non-thermal, but no further identification is possible at 
G335.2+0.1 this stage.
G337.0-0.1 (Fig.19) A peculiar non-thermal structure consisting of a circular 
G337.0-0.1 plateau of faint emission in which several enhancements occur, and a
G337.0-0.1 bright ridge extending 4' north from the north-western edge of the
G337.0-0.1 plateau. The interpretation of this peculiar non-thermal object is 
G337.0-0.1 uncertain and it is possible that part of it may be extragalactic. 
G337.0-0.1 Much diffuse thermal emission in the region confuses the 
G337.0-0.1 interpretation.
G337.2-0.7 (Fig.20) The observations show for the first time a small-diameter 
G337.2-0.7 circular shell remnant with maximum brightness along its southern 
G337.2-0.7 boundary.
G337.3+1.0 (Fig.20) A classic shell SNR. The shell is complete and almost 
G337.3+1.0 circular, with several enhancements around the rim. our flux density
G337.3+1.0 of S_0.843_=20Jy is somewhat larger than the previously published 
G337.3+1.0 MOST value of 14.8+/-3Jy (Milne et al., 1989PASAu...8..187M) and 
G337.3+1.0 leads to a revised spectral index of {alpha}=^8.4^_0.408_=-0.55
G337.8-0.1 (Fig.21) A bright small-diameter SNR with a distorted shell. The 
G337.8-0.1 MOST flux density of S_0.843_=18Jy, combined with S_0.408_=26Jy 
G337.8-0.1 (Shaver & Goss 1970AuJPS..14..133S), gives a spectral index of 
G337.8-0.1 {alpha}=^0.843^_0.408_=-0.51.
G338.1+0.4 (Fig.21) The source consists of a faint semicircle describing the 
G338.1+0.4 northern half of a shell, while the southern half cannot be 
G338.1+0.4 separated from the general thermal emission in the region. Zealey et
G338.1+0.4 al. (1979A&A....38...39Z) have detected optical nebulosity 
G338.1+0.4 coincident with the north-eastern radio emission.
G338.3-0.0 (Fig.22) A broken shell SNR lying on the edge of the bright H II 
G338.3-0.0 region G338.4+0.0 (part of the MSH 16-4 (Manchester et al., 
G338.3-0.0 1983IAUS..101..421M) complex).
G338.5+0.1 (Fig 22) A circular patch of faint non-thermal emission (diameter 
G338.5+0.1 5') lying on the northern edge of the bright HII region G338.4+0.0. 
G338.5+0.1 The southern extent of the non-thermal emission is unclear, but the 
G338.5+0.1 bright ridges and knots in the east and the south-west of the field
G338.5+0.1 are known to be thermal.
G340.4+0.4 (Fig.23) A shell SNR with more internal structure than a simple 
G340.4+0.4 annulus. The faint emission on the eastern and western sides of the 
G340.4+0.4 bright central ring like structure, not evident in previous 
G340.4+0.4 observations of the remnant (e.g. Caswell et al., 
G340.4+0.4 1983MNRAS.203..595C), results in elongation that may be due to a 
G340.4+0.4 blowout.
G342.0-0.2 (Fig.23) A shell SNR with internal structure. This object has a 
G342.0-0.2 close companion remnants, G341.9-0.3, which Caswell et al. 
G342.0-0.2 (1983MNRAS.203..595C) suggest might be located at the same distance.
G342.0-0.2 The two remnants may be interacting.
G348.5-0.0 (Fig.25) This object has recently been identified as a separate SNR 
G348.5-0.0 in the CTB 37 complex by Kassim et al. (1991ApJ...374..212K). The 
G348.5-0.0 most prominent part of the remnant is a curved ridge which appears 
G348.5-0.0 to be separated by ~1~ from the bright eastern rim of G348.5+0.1. At
G348.5-0.0 this stage it is not possible to say whether the two remnants are 
G348.5-0.0 associated with the same region or are interacting in some manner.
G348.5+0.1 (Fig.25) A confused region of non-thermal emission. The main 
G348.5+0.1 structure is a shell, which has one of the highest mean surface 
G348.5+0.1 brightnesses in this catalogue. Faint emission extends to the 
G348.5+0.1 south-west, suggesting expansion into a cavity. Comparison with 
G348.5+0.1 60um IRAS images shows that considerable diffuse thermal emission 
G348.5+0.1 also exists in the region, perhaps accounting for some of the faint 
G348.5+0.1 radio emission to the west.
G348.7+0.3 (Fig.25) The MOST image shows a region of non-thermal emission that 
G348.7+0.3 consists of a shell of diameter 7' and a faint plateau ~13' in 
G348.7+0.3 diameter which overlaps the south-eastern part of the shell. The 
G348.7+0.3 plateau is approximately rectangular in shape and extends to the
G348.7+0.3 south as far as the remnant G348.5+0.1.
G351.2+0.1 (Fig.26) An SNR with a distorted shell. High-resolution observations
G351.2+0.1 with the VLA by Becker & Helfand (1988AJ.....95..883B) do not 
G351.2+0.1 detect much of the extended emission evident here, but confirm the 
G351.2+0.1 basic shell structure. They find a compact source with an inverted 
G351.2+0.1 spectrum ({alpha}=^15^_1.4_=+0.27) near the shell centre, which is 
G351.2+0.1 too faint to be seen in the MOST image. The association of this 
G351.2+0.1 source with the shell has not been confirmed, and so we suggest a 
G351.2+0.1 shell interpretation of the morphology rather than a composite at 
G351.2+0.1 this stage. Becker & Helfand (1988AJ.....95..883B) also detected
G351.2+0.1 a straight filament in the structure, but the MOST image shows this 
G351.2+0.1 is simply part of the northern rim of the shell.                    
G286.5-1.2 (Fig.27) The main feature is a bright, curved filament 15' in length
G286.5-1.2 with a kink near its centre. A second, fainter filament lies 
G286.5-1.2 north-west and almost parallel to the main filament. Although 
G286.5-1.2 excluded from the MOST image, a bright non-thermal point source lies
G286.5-1.2 30' to the north-west. Interestingly, both filaments are curved 
G286.5-1.2 around this source, although an association between it and the 
G286.5-1.2 filaments is unlikely because of their large angular separation. 
G286.5-1.2 Another unresolved source at RA=10h34m14.4s, DE=-59{deg}49'03" 
G286.5-1.2 (J2000) is non-thermal, while the slightly-extended source 5' to its
G286.5-1.2 north-west is an HII region. G286.5-1.2 resembles the Galactic 
G286.5-1.2 non-thermal structure known as the "Snake" (Gray et al.,
G286.5-1.2 1991Natur.353..237G). The similarity between the Snake and the main
G286.5-1.2 filament in G286.5-1.2 is quite striking, with both structures 
G286.5-1.2 having similar curvature and possessing a central kink.
G289.7-0.3 (Fig.27) A very unusual shell SNR. It possesses a well-defined, 
G289.7-0.3 roughly circular shell within which lies extensive, structured 
G289.7-0.3 filamentary emission. The interior is dominated by two arcs of 
G289.7-0.3 emission, together describing an elliptical shape. Two parallel 
G289.7-0.3 filaments emerge radially from the south of this structure and 
G289.7-0.3 extend to the southern part of the shell, joining it at the point 
G289.7-0.3 where the shell emission is brightest. At least six other filaments 
G289.7-0.3 are apparent in the western half of the remnant, producing a 
G289.7-0.3 distinct cellular structure reminiscent of some planetary nebulae.
G289.7-0.3 A barely-resolved source lies 1' north-east of the geometric centre 
G289.7-0.3 of the shell. Observations of this source were made at 1.47 and 
G289.7-0.3 4.79GHz with the ATCA (Whiteoak, 1993, Ph.D. Thesis, Univ. of 
G289.7-0.3 Sydney). Two small-diameter sources were found separated by 30", 
G289.7-0.3 with spectral indices {alpha}=^4.79^_1.47_=-1.2 and -0.8 for the 
G289.7-0.3 south-eastern and north-western components respectively. Their small
G289.7-0.3 angular separation and steepness of their spectral indices imply 
G289.7-0.3 that they are part of the same extragalactic double source and 
G289.7-0.3 therefore unrelated to G289.7-0.3. While the morphology of 
G289.7-0.3 G289.7-0.3 suggests it may be a shell SNR, a planetary nebula 
G289.7-0.3 interpretation cannot be ruled out. In observations at 4.5 and 
G289.7-0.3 8.55GHz with the Parkes radio telescope (Whiteoak, 1993, Ph.D. 
G289.7-0.3 Thesis, Univ. of Sydney), flux densities of S_4.5_=7.5+/-2.3Jy and 
G289.7-0.3 S_8.55_=3.6+/-0.9Jy were determined respectively. With the MOST flux
G289.7-0.3 density of S_0.843_=6.4+/-0.5Jy, an overall spectral index of 
G289.7-0.3 {alpha}=^8.55^_0.843_=-0.2+/-0.2 is obtained. There is a suggestion 
G289.7-0.3 of a turnover in the spectrum, implying that the emission may be 
G289.7-0.3 thermal. The polarisation observations undertaken at Parkes indicate
G289.7-0.3 negligible polarisation at 4.5GHz. Comparison between radio and IRAS
G289.7-0.3 60um data is inconclusive. Another possibility relates to the 
G289.7-0.3 observation that Wolf-Rayet stars can produce rings of emission 
G289.7-0.3 arising from heavy mass-loss either in their O star phase or through
G289.7-0.3 their own stellar winds and ejecta, coupled with strong ionising 
G289.7-0.3 radiation (e.g. Marston et al., 1994ApJS...95..151M). Offset to the 
G289.7-0.3 north-west of the centre of G289 7-0.3 at RA=11h01m02.3s, 
G289.7-0.3 DE=-60{deg}14'01" (J2000) lies the Wolf-Rayet star WR35b (Shara et 
G289.7-0.3 al., 1991AJ....102..716S), a member of the open cluster Sher 1 
G289.7-0.3 (Moffat et al., 1991AJ....102..642M). It is possible that WR35b and 
G289.7-0.3 other high-luminosity stars in Sher 1 have influenced the structure 
G289.7-0.3 of G289.7-0.3, although the distance of 10kpc (Moffat et al., 
G289.7-0.3 1991AJ....102..642M) implies a rather large shell size of ~50pc. As 
G289.7-0.3 an interesting note, fossil shells have also been detected around 
G289.7-0.3 some Wolf-Rayet ring nebulae (Manchado et al., 1995IAUS..163...74M).
G289.7-0.3 Although difficult to see here in the MOST image, a very faint shell
G289.7-0.3 of diameter ~ 40' lies concentrically with G289.7-0 3, also 
G289.7-0.3 apparent in the 5GHz observations of Haynes, Caswell & Simons 
G289.7-0.3 (1978AuJPA..45....1H), that is reminiscent of such fossil shells.
G289.7-0.3 Clearly, further observations are required before the structure 
G289.7-0.3 of G289.7-0.3 can be fully explained.
G294.1-0.0 (Fig.28) A very faint large-diameter shell. Although the average 
G294.1-0.0 surface brightness of 1.2 mJy/beam is barely above the noise, a 
G294.1-0.0 well-defined rim characteristic of shell structure is apparent, with
G294.1-0.0 a pronounced bulge on its eastern side. Comparison with 60um maps 
G294.1-0.0 shows that the bright patch of emission adjoining the southern 
G294.1-0.0 boundary is an H II region.
G299.6-0.5 (Fig.28) A faint shell with brighter east ern rim. The 
G299.6-0.5 small-diameter sources within the shell are all non-thermal.
G301.4-1.0 (Fig.29) A faint, circular shell remnant possessing an unusual 
G301.4-1.0 "blowout" on its south-western side. The blowout consists of a block
G301.4-1.0 of faint, striated emission extending 12' in a south-westerly 
G301.4-1.0 direction from a gap in the shell structure.
G308.1-0.7 (Fig.29) A shell remnant with straight north-western edge.
G317.3-0.2 (Fig.30) An object consisting of two op posing arcs. Some of the 
G317.3-0.2 diffuse emission in the region may be associated with the nearby HII
G317.3-0.2 complex G316.8-0.1.
G318.2+0.1 (Fig.30) A large-diameter shell SNR. This remnant is outlined by two
G318.2+0.1 non-thermal features that form the north-western and south-eastern 
G318.2+0.1 sections of a shell. The north-western component consists of a
G318.2+0.1 single bright arc of length 30', while the south-eastern component 
G318.2+0.1 is a band (dimensions 25' x 17') composed of a number of curved, 
G318.2+0.1 parallel filaments, similar to those of the blowout of G301.4-1.0. 
G318.2+0.1 The faint north-western filament outside the shell at RA=14h52m08s,
G318.2+0.1 DE=-58{deg}46'44" (J2000) is non-thermal and may be related. The 
G318.2+0.1 filamentary emission lying perpendicular to the northern boundary 
G318.2+0.1 and centred at RA=14h55m38s, DE=-58{deg}51'08" is also non-thermal. 
G318.2+0.1 G318.2+0.1 was observed with the Parkes radio telescope in both 
G318.2+0.1 total intensity and polarised intensity at 4.5 and 8.55GHz (Whiteoak
G318.2+0.1 1993, Ph.D. Thesis, Univ. of Sydney). The sensitivity was too low to
G318.2+0.1 provide accurate flux densities, but the non-thermal nature was 
G318.2+0.1 confirmed by the polarisation observations which showed a 
G318.2+0.1 polarisation oI 10-20% at 4.5GHz over the shell. The central 
G318.2+0.1 emission at RA=14h55m04s, DE=-59{deg}02'44" (J2000) is the HII 
G318.2+0.1 region G318.223+0.140 (Haynes, Caswell & Simons, 
G318.2+0.1 1979AuJPA..48....1H). The bright clumps at RA=14h52m09s, 
G318.2+0.1 DE=-59{deg}10'07" (J2000) and just to the south-east are also 
G318.2+0.1 thermal.
G321.9-1.1 (Fig.31) A faint shell remnant. Observed with the Parkes radio 
G321.9-1.1 telescope at 4.5GHz, the emission from the northern part of the 
G321.9-1.1 shell appears to be polarised at a level of ~15% (Whiteoak, 1993,
G321.9-1.1 Ph.D. Thesis, Univ. of Sydney), although this is uncertain because 
G321.9-1.1 of the faintness of the radio emission.
G327.4+1.0 (Fig.31) A faint, asymmetric shell, with bright western rim. The 
G327.4+1.0 bright point-source to the south is confused with general thermal 
G327.4+1.0 emission in the region, but is probably non-thermal.
G329.7+0.4 (Fig.32) A large-diameter SNR candidate. The shell is quite diffuse 
G329.7+0.4 compared to other SNRs, with few sharply-defined outer edges. 
G329.7+0.4 Comparison with 60 um data shows only faint emission coincident with
G329.7+0.4 the shell structure, suggesting a non-thermal nature, but confusion 
G329.7+0.4 with thermal emission in the region makes the identification 
G329.7+0.4 as an SNR only tentative at this stage.
G342.1+0.9 (Fig.32) A distorted shell. The bright point source to the 
G342.1+0.9 south-east is non-thermal.
G343.1-0.7 (Fig.33) An unusual remnant. The main shell is square-shaped (side 
G343.1-0.7 20'), and brightest along its southern boundary which consists of 
G343.1-0.7 three bright sharp-edged arcs. A second shell of diameter 13' lies 
G343.1-0.7 at the north-western corner of the main shell. Comparison with 60um 
G343.1-0.7 maps suggests that the main shell is non-thermal and the minor shell
G343.1-0.7 thermal. G343.1-0.7 was observed with the Parkes radio telescope 
G343.1-0.7 at 4.5 and 8.55GHz in both total and polarised intensity (Whiteoak 
G343.1-0.7 1993, Ph.D. Thesis, Univ. of Sydney). The total intensity 
G343.1-0.7 observations give flux densities of S_4.5_=3.9+/-0.6Jy and 
G343.1-0.7 S_8.55_=2.4+/-0.5Jy for the main shell, and S_4.5_=4.0+/-0.3Jy and 
G343.1-0.7 S_8.55_=2.6+/-0.6Jy for the smaller shell. The MOST observations 
G343.1-0.7 give flux densities of S_0.843_=8.51+/-0.6Jy and 
G343.1-0.7 S_0.843_=4.5+/-0.3Jy for the main and minor shells respectively. 
G343.1-0.7 Estimates of the corresponding spectral indices of the two 
G343.1-0.7 components are then {alpha}^8.55^_0.843_=-0.55 and -0.19. The main 
G343.1-0.7 shell appears to be polarised at 4.5GHz with levels up to about 12%,
G343.1-0.7 while no polarisation was detected from the minor shell. At 8.55GHz,
G343.1-0.7 the main shell is found to be polarised to ~20%, and again no 
G343.1-0.7 polarised emission is associated with the minor shell. The main 
G343.1-0.7 shell is clearly an SNR. The absence of polarised emission in the 
G343.1-0.7 smaller shell, its flat spectral index, and the presence of 60um 
G343.1-0.7 emission indicates that the minor shell is probably thermal.
G345.7-0.2 (Fig.33) A faint disk, with a peak just south of the centre lying 
G345.7-0.2 close to the position of the pulsar PSR J1707-4053 (Taylor et al., 
G345.7-0.2 1993ApJS...88..529T), although the large age of the pulsar 
G345.7-0.2 (>10^6^years) suggests a chance coincidence.
G349.2-0.1 (Fig.34) A small-diameter shell with central emission lying on the 
G349.2-0.1 edge of the H II region G349.1+0.0.
G351.7+0.8 (Fig.34) A faint plateau of emission on the edge of a bright H II 
G351.7+0.8 region. The pulsar PSR J1721-3532 is situated outside the eastern 
G351.7+0.8 side of this structure at RA=17h21m32.8s, DE=-35{deg}32'46.6" 
G351.7+0.8 (J2000) (Taylor et al., 1993ApJS...88..529T), although it is 
G351.7+0.8 obscured by a small H II region.
G351.9-0.9 (Fig.35) A very faint shell-like object.
G354.8-0.8 (Fig.35) A well-defined shell SNR with a complete boundary and rim 
G354.8-0.8 enhancements along the eastern side and in the north-west.
G299.0+0.2 (Fig.36) The MOST image clarifies the nature of this region. The 
G299.0+0.2 field contains several bright small-diameter sources and regions of 
G299.0+0.2 faint extended emission. Comparison with 60um IRAS data shows that 
G299.0+0.2 all the extended emission in the region is thermal. The central 
G299.0+0.2 compact source lying at RA=12h17m23.8s, DE=-62{deg}29'01" (J2000) is
G299.0+0.2 also thermal, as is the bright small-diameter source in the west. 
G299.0+0.2 However, the bright unresolved source in the north-east of the field
G299.0+0.2 is non-thermal and possibly an unrelated background object. It is 
G299.0+0.2 blending of this source and the extended thermal emission in the 
G299.0+0.2 region that has previously simulated an SNR (e.g. Clark et al.,
G299.0+0.2 1975AuJPA..37....1C).
G328.0+0.3 (Fig.36) Identified by Shaver & Goss (1970AuJPS..14..133S) as a 
G328.0+0.3 region of extended non-thermal emission from low-resolution 
G328.0+0.3 observations. However, the MOST image in conjunction with 60um IRAS 
G328.0+0.3 data shows that there was confusion between a non-thermal unresolved
G328.0+0.3 source at RA=15h53m19.4s, DE=-53{deg}27'54" (J2000) which is 
G328.0+0.3 probably extra galactic and faint extended thermal emission in the 
G328.0+0.3 region.