345.003-0.223 and 345.003-0.224. These known maser sites are shown on the same 345.003-0.223 spectrum since they are separated by only 3 arcsec and do not 345.003-0.223 overlap in velocity. Reference to catalog.dat, and to spectra in 345.003-0.223 Caswell (1997MNRAS.289..203C), make it clear which features are 345.003-0.223 at which site. Variability reported by Caswell, Vaile & 345.003-0.223 Ellingsen (1995PASA...12...37C) is present at velocities 345.003-0.223 corresponding to both sites, and spectra over a long time-span 345.003-0.223 characterize the variability in more detail (Goedhart, 345.003-0.223 Gaylard & van der Walt, 2004MNRAS.355..553G) but reveal no 345.003-0.223 distinct periodicities. 345.003-0.224 See note on 345.003-0.223 345.010+1.792 and 345.012+1.797. These known maser sites are separated by 19" 345.010+1.792 and are shown on the same spectrum. The velocity ranges do not 345.010+1.792 overlap [catalog.dat, and spectra from Caswell 345.010+1.792 (1997MNRAS.289..203C)]. The first site is associated with a 345.010+1.792 UCHII region (Caswell, 1997MNRAS.289..203C) and displays class 345.010+1.792 II methanol maser emission from a remarkably large number of 345.010+1.792 other transitions (Cragg et al., 2001MNRAS.323..939C). 345.012+1.797 See note on 345.010+1.792 345.198-0.030 This new site is believed to lie in the far side of the 3-kpc 345.198-0.030 arm. For this site, and several others near these longitudes, 345.198-0.030 the velocity (-1.5km/s in this instance) is sufficiently near 345.198-0.030 zero that the alternative kinematic distances lie on the solar 345.198-0.030 circle, i.e. at the same Galactocentric distance as the Sun (and 345.198-0.030 thus very nearby or at 17kpc), where the space density of masers 345.198-0.030 is low (see Section 4). We conclude that, statistically, very 345.198-0.030 few can lie near the solar circle, and that most of them are 345.198-0.030 correctly attributed to the far side of the 3-kpc arm, but with 345.198-0.030 some exceptions recognizable from their quite large Galactic 345.198-0.030 latitude, e.g. 348.195+0.768. 345.407-0.952 and 345.424-0.951. This is a known pair of sites separated by 345.407-0.952 about 1 arcmin. The first is a single spectral feature, 345.407-0.952 coincident with an OH maser site (Caswell, 1998MNRAS.297..215C). 345.407-0.952 The spectra are shown aligned, one beneath the other and with 345.407-0.952 the same velocity scale, so as to allow clear distinction of the 345.407-0.952 features attributable to each site. The sites are not likely to 345.407-0.952 be at a large distance in view of their rather large Galactic 345.407-0.952 latitude. HI absorption measurements of nearby continuum 345.407-0.952 emission was interpreted to indicate a distance of 2kpc by 345.407-0.952 Caswell et al. (1975A&A....45..239C). However, Radhakrishnan et 345.407-0.952 al. (1972ApJS...24...49R) considered this region in the context 345.407-0.952 of others at similar latitude which lie between longitude 345.407-0.952 345{deg} and 352{deg}. They argued persuasively that all of 345.407-0.952 these complexes are at a distance of about 4.2kpc (if the 345.407-0.952 Galactic Centre is assumed to be at 8.4kpc) and this remains a 345.407-0.952 likely interpretation. 345.424-0.951 See note on 345.407-0.952 345.441+0.205 New site believed to lie in the far side of the 3-kpc arm. 345.487+0.314 and 345.505+0.348. Known sites separated by more than 2 arcmin. 345.487+0.314 The latter site displays emission over a velocity range from 345.487+0.314 -23.1 to -10.5km/s, and seems likely to lie in the far side of 345.487+0.314 the 3-kpc arm; with a peak intensity of 307Jy, it is the 345.487+0.314 strongest maser attributed to the far side. The first site is a 345.487+0.314 weak single feature with velocity -22.8km/s lying just outside 345.487+0.314 the velocity range of the 3-kpc arm (Green et al., 345.487+0.314 2009ApJ...696L.156G). For consistency, we formally exclude it 345.487+0.314 from the 3-kpc arm but this is uncertain, and it may be near its 345.487+0.314 apparent neighbour in the 3-kpc arm. The spectra are aligned to 345.487+0.314 allow recognition of the features of each site. 345.505+0.348 See note on 345.487+0.314 345.498+1.467 This known site lies within the longitude-velocity domain of the 345.498+1.467 far side of the 3-kpc arm but, in view of its large Galactic 345.498+1.467 latitude, and evidence from HI absorption (Radhakrishnan et al. 345.498+1.467 1972ApJS...24...49R), that interpretation is rejected in 345.498+1.467 preference to a nearby location (Green et al., 345.498+1.467 2009ApJ...696L.156G). 345.576-0.225 This newly discovered site has the highest negative velocity 345.576-0.225 (peak at nearly -126km/s) of any site in the survey region 345.576-0.225 presented here. It most likely lies in the near side of the 345.576-0.225 expanding 3-kpc arm (Green et al., 2009ApJ...696L.156G). 345.807-0.044 New weak maser lying in the far side of 3-kpc arm. 345.824+0.044 Caswell & Haynes (1987A&A...171..261C) remark on the likely 'far' 345.824+0.044 distance of an HII region which lies in the same direction and 345.824+0.044 has the same velocity as the maser; a location in the far side 345.824+0.044 of the 3-kpc arm for both the HII region and the maser would 345.824+0.044 satisfy those observations. 345.985-0.020 Strongly variable new maser with peak of 5.7Jy at -83.2km/s in 345.985-0.020 our follow-up measurements of 2008 August. This feature was only 345.985-0.020 1.35Jy in our original survey cube (2007 June, when another peak 345.985-0.020 was slightly stronger) and had a similar value in the ATCA 345.985-0.020 measurement of 2007 July. 346.036+0.048 New maser located in the far side of the 3-kpc arm. 346.231+0.119 This new maser has its velocity centred at -95km/s, just outside 346.231+0.119 our adopted range for 3kpc arm near-side members; we 346.231+0.119 provisionally reject it as a 3kpc arm object pending other data. 346.480+0.221 Known site with velocity range just outside our formal boundary 346.480+0.221 for far side 3-kpc arm members. 346.481+0.132 Known site located in the far side of the 3-kpc arm. 346.517+0.117 Not detected above the noise level in the survey observations 346.517+0.117 (2007 June) but known as a maser with peak of 1Jy at -0.1km/s 346.517+0.117 and a secondary peak of 0.7Jy at -1.7km/s in 1999 October (see 346.517+0.117 Caswell, 2009PASA...26..454C). Our follow-up observations 2008 346.517+0.117 August detected it with peak of only 0.3Jy, and only at 346.517+0.117 -1.7km/s. The spectrum is shown aligned in velocity with those 346.517+0.117 of nearby sites 346.481+0.132 and 346.522+0.085 so as to 346.517+0.117 recognize their confusing contribution to the spectrum. A 346.517+0.117 similar confirmatory spectrum was obtained in 2009 March. 346.522+0.085 Known single feature varying in our observations between 1.47Jy 346.522+0.085 (2007 June) and 1.9Jy (2008 August), similar to its peak in 346.522+0.085 1992, but as weak as 0.6Jy in 1999 October (Caswell, 346.522+0.085 2009PASA...26..454C). It is located in the far side of the 346.522+0.085 3-kpc arm. 347.583+0.213 Known maser in the near side of the 3-kpc arm. The spectrum is 347.583+0.213 aligned with 347.631+0.211 which is responsible for two weak 347.583+0.213 features, and with 347.628+0.149 whose major feature does not 347.583+0.213 contribute to the spectrum. 347.628+0.149 Known maser in the near side of the 3-kpc arm. The offset of 347.628+0.149 4.7 arcmin from the previous source is just large enough to 347.628+0.149 prevent any confusion. 347.631+0.211 Offset 3.7 arcmin from a possible companion, the previous 347.631+0.211 maser 347.628+0.149, which is at slightly more negative 347.631+0.211 velocity. Most likely, 347.631+0.211 also lies in the near side 347.631+0.211 of the 3-kpc arm, but at present, for consistency, we have 347.631+0.211 formally rejected it as just outside our accepted velocity 347.631+0.211 range. Note that our spectrum centred here shows weak emission 347.631+0.211 from 347.583+0.213 which lies at the edge of the Parkes 347.631+0.211 telescope beam response. 347.863+0.019 Our new observations of this site, both from the survey cube 347.863+0.019 (2007 June) and the MX measurement (2008 August), show that, 347.863+0.019 compared to the spectrum from 1992 June (Caswell et al. 347.863+0.019 1995MNRAS.272...96C), the currently prominent features near 347.863+0.019 -35km/s have increased by a factor of 2 and the previously 347.863+0.019 strongest feature of 7Jy at -29km/s has faded to less than 1Jy. 347.863+0.019 The kinematic distance ambiguity for this site has been 347.863+0.019 investigated by Busfield et al. (2006MNRAS.366.1096B) who favour 347.863+0.019 the far distance since no HI self-absorption could be detected. 348.027+0.106 New maser located in the near side of the 3-kpc arm. 348.195+0.768 New maser whose velocity is consistent with a location in the 348.195+0.768 far side of the 3-kpc arm. However, its large latitude suggests 348.195+0.768 that it is more likely to be nearby (Green et al., 348.195+0.768 2009ApJ...696L.156G). If it is nearby, this should be easy to 348.195+0.768 verify by future astrometry and a parallax measurement. 348.550-0.979 and 348.550-0.979n. This is a known close pair of sources 348.550-0.979 (separation 2 arcsec) for which we accept the current 348.550-0.979 interpretation that they are distinct sites (Caswell, 348.550-0.979 2009PASA...26..454C). These sites, and those discussed in the 348.550-0.979 next two notes, all have velocities that suggest they lie in a 348.550-0.979 region argued to be at a distance of about 4.2kpc by 348.550-0.979 Radhakrishnan et al. (1972ApJS...24...49R)- see also notes 348.550-0.979 to 345.407-0.952. 348.550-0.979n See note on 348.550-0.979 348.579-0.920 This known weak maser displayed a peak of 0.5Jy at -15km/s in 348.579-0.920 1996 (Caswell, 2009PASA...26..454C) and was below the noise 348.579-0.920 level in our regular survey measurement. A weak peak of 0.32Jy 348.579-0.920 at this velocity was detected in our later follow-ups in both 348.579-0.920 2008 August and 2009 March, and we conservatively list just this 348.579-0.920 peak in catalog.dat. However, the spectrum at this location, 348.579-0.920 when aligned with that of the nearby strong source 348.579-0.920 348.550-0.979, reveals that the sidelobe response to the strong 348.579-0.920 source is no more than 1 per cent; thus probably most other 348.579-0.920 emission at this location is also from 348.579-0.920, and 348.579-0.920 attributable to previously unrecognized features of up to 0.5Jy. 348.617-1.162 This is the strongest of our new detections and lies in the 348.617-1.162 region where its velocity suggests it to be at a distance of 348.617-1.162 4.2kpc (Radhakrishnan et al. 1972ApJS...24...49R). 348.654+0.244 New maser located in the far side of the 3-kpc arm. 348.703-1.043 and 348.727-1.037. This is a known pair of sites separated by 348.703-1.043 more than 1 arcmin. Both sites host OH masers (Caswell, 348.703-1.043 1998MNRAS.297..215C). Emission from the first site is confined 348.703-1.043 to a small velocity range, and its main feature at velocity 348.703-1.043 -7.4km/s is clearly distinguishable from 348.727-1.037 when the 348.703-1.043 two aligned spectra are compared. The sites lie in the region 348.703-1.043 suggested to be at a distance of 4.2kpc (Radhakrishnan et al. 348.703-1.043 1972ApJS...24...49R). 348.727-1.037 See note on 348.703-1.043 348.723-0.078 , 348.892-0.180 and 349.067-0.017. The first is a new maser and 348.723-0.078 the other two are previously known. All are most likely located 348.723-0.078 in the far side of the 3-kpc arm. 348.892-0.180 See note on 348.723-0.078 349.067-0.017 See note on 348.723-0.078 349.092+0.105 and 349.092+0.106. Known sites with separation of only 2 arcsec. 349.092+0.105 Their velocities near -80km/s are not quite within the range of 349.092+0.105 the near side of the 3-kpc arm. If they are not in the 3-kpc 349.092+0.105 arm, their velocity would be compatible with a location slightly 349.092+0.105 further away, and within 3kpc of the Galactic Centre. At a 349.092+0.105 distance of 8.4kpc, their separation corresponds to more 349.092+0.105 than 80Mpc. 349.092+0.106 See note on 349.092+0.105 349.151+0.021 New site located in the far side of the 3-kpc arm. 349.579-0.679 This new maser has decreased from a peak flux density of 5.9Jy 349.579-0.679 in the initial survey (2007 June) to 4.2Jy in the ATCA 349.579-0.679 observations (2007 July) and 1.9Jy (2008 August) in our 349.579-0.679 MX spectrum. 349.884+0.231 New maser located in the far side of the 3-kpc arm. 350.011-1.342 Known maser consistently showing a peak of more than 2Jy in our 350.011-1.342 recent observations. However, the original detection of 1993 350.011-1.342 September (reported in source notes of Caswell, 350.011-1.342 1998MNRAS.297..215C) showed a peak of 1Jy at velocity -27.9km/s, 350.011-1.342 and in 1999 May the peak was only 0.4Jy at -25.8km/s (Caswell, 350.011-1.342 2009PASA...26..454C); thus it has shown a recent flux density 350.011-1.342 increase by more than a factor of 5. Its large latitude suggests 350.011-1.342 that it is nearby, but the velocity and latitude would be 350.011-1.342 compatible with a location in the extensive structure at 4.2kpc 350.011-1.342 discussed by Radhakrishnan et al. (1972ApJS...24...49R). 350.105+0.083 , 350.104+0.084 and 350.116+0.084. Three known sites (Caswell, 350.105+0.083 2009PASA...26..454C), of which the first two are separated by 350.105+0.083 only 4 arcsec. The first site is the strongest, with a large 350.105+0.083 velocity range, and a peak at -74.1km/s of approximately 15Jy, 350.105+0.083 both in our recent measurements up to 2008 March and as far back 350.105+0.083 as 1996 October; however, it was much stronger, 40Jy, in 1992. 350.105+0.083 The location of the second site was determined in 1996 October 350.105+0.083 from a single feature at -68.4Jy of 2.5Jy, and the location of 350.105+0.083 the third site, offset 40 arcsec, was determined from a single 350.105+0.083 feature in 1996 October at -68.0km/s, with peak 1.8Jy. A much 350.105+0.083 stronger feature close to these velocities now has a peak 350.105+0.083 varying between 14.6 (survey cube, 2007 March) and 9.9Jy 350.105+0.083 (MX, 2008 March), and although we have no precise recent 350.105+0.083 position, we interpret it as evidence of a flare in either the 350.105+0.083 second or third site by a factor of 4. Slight differences in the 350.105+0.083 strength of emission seen in our Parkes measurements centred at 350.105+0.083 each site are insufficient to indicate the more likely location. 350.105+0.083 However, from the velocity comparisons, it seems probable that 350.105+0.083 the flare occurred in the third site rather than the second. 350.104+0.084 See note on 350.105+0.083 350.116+0.084 See note on 350.105+0.083 350.116+0.220 New maser located in the far side of the 3-kpc arm. 350.340+0.141 and 350.344+0.116. 350.340+0.141 is a single feature weak new 350.340+0.141 maser nearly 90 arcsec from the known strong maser 350.340+0.141 350.344+0.116. The aligned spectra clearly reveal the main 350.340+0.141 features of each site. 350.344+0.116 See note on 350.340+0.141 350.776+0.138 The high positive velocity of this new site is strikingly unusual 350.776+0.138 for a site at this longitude, and can most readily be 350.776+0.138 interpreted as indicating a location at the edge of the far 350.776+0.138 side of the 3-kpc arm. 351.242+0.670 and 351.251+0.652. The first of these was reported by Caswell & 351.242+0.670 Phillips (2008MNRAS.386.1521C) while the second was detected in 351.242+0.670 the same observations (but unpublished) as a peak of 1Jy at 351.242+0.670 -7.1km/s. Neither maser can readily be seen in our Parkes survey 351.242+0.670 due to a combination of several distracting effects. These 351.242+0.670 effects include deep absorption (stronger than the masers) at a 351.242+0.670 velocity spanning almost the entire range between the two 351.242+0.670 masers; the consequent slightly offset zero intensity level; and 351.242+0.670 some weak responses to very strong offset maser emission near 351.242+0.670 velocity -10km/s associated with NGC 6334F. Allowing for these 351.242+0.670 effects, our original survey cube for 351.242+0.670 shows a peak 351.242+0.670 of 2.2Jy at +2.5km/s. The follow-up MX spectrum of 2008 March 351.242+0.670 (displayed in this paper) shows a peak of 0.74Jy. At 351.242+0.670 intermediate epochs, the peak was 1.1Jy on 2007 May 14 using a 351.242+0.670 compact configuration of the ATCA (Caswell & Phillips, 351.242+0.670 2008MNRAS.386.1521C), and our high spatial resolution 351.242+0.670 measurements with the ATCA on 2007 July 21 revealed a peak of 351.242+0.670 only 0.44Jy. The maser is thus markedly variable. 351.242+0.670 The second site is offset 73 arcsec from the first and is weaker. 351.242+0.670 The most sensitive spectrum from the MX follow-up (2008 March) 351.242+0.670 shows a 1-Jy peak at -7.1km/s, with weaker emission extending 351.242+0.670 to -6km/s, similar to the unpublished ATCA observations by 351.242+0.670 Caswell & Phillips in 2007 May; the original survey cube was 351.242+0.670 noisier, showing a peak of 1.3Jy, and the ATCA observations 351.242+0.670 (2007 July) yielded a peak of 0.6Jy at -7.1km/s, with a 351.242+0.670 secondary peak of 0.55Jy at -6.1km/s. Some variability seems 351.242+0.670 likely, but deviations from a peak of 1Jy are barely significant 351.242+0.670 in view of the low signal-to-noise ratio. The two sites do not 351.242+0.670 overlap in their emission velocity ranges and are clearly 351.242+0.670 distinguishable on the aligned spectra. 351.251+0.652 See note on 351.242+0.670 351.417+0.645 , 351.417+0.646 and 351.445+0.660. These are strong well-known 351.417+0.645 masers (e.g. Caswell, 1997MNRAS.289..203C) with the first 351.417+0.645 projected on to the prominent compact HII region NGC 6334F 351.417+0.645 (Ellingsen, Norris & McCulloch, 1996MNRAS.279..101E; Caswell, 351.417+0.645 1997MNRAS.289..203C). The second is offset from the first by 351.417+0.645 several arcsec to the north-west and has an almost identical 351.417+0.645 velocity range but the spectra are clearly distinct when seen 351.417+0.645 with the ATCA spatial resolution (Caswell, 1997MNRAS.289..203C). 351.417+0.645 The third site is offset nearly 2 arcmin to the north, and our 351.417+0.645 Parkes spectrum, although confused by the first two very strong 351.417+0.645 sources between -12 and -9.6km/s, clearly shows features at 351.417+0.645 -9.2, -7.1 and -2.5km/s which correspond to the main features 351.417+0.645 of 351.445+0.660 seen on the ATCA spectrum of Caswell 351.417+0.645 (1997MNRAS.289..203C). 351.417+0.646 See note on 351.417+0.645 351.445+0.660 See note on 351.417+0.645 351.581-0.353 This known strong maser site has a weak northern feature offset 351.581-0.353 nearly 2 arcsec (Caswell 1997MNRAS.289..203C, 351.581-0.353 2009PASA...26..454C). Following Caswell (2009PASA...26..454C) we 351.581-0.353 treat it as probably not a distinct site and therefore do not 351.581-0.353 list it here, and cite a velocity range encompassing all 351.581-0.353 features. The velocity indicates a location in the near side 351.581-0.353 of the 3-kpc arm. 351.611+0.172 and 351.688+0.171. These masers are separated by 4.6 arcmin and 351.611+0.172 both are new. 351.688+0.171 has a peak flux density of 42Jy, 351.611+0.172 our second strongest new detection. Alignment of the two spectra 351.611+0.172 shows that, despite the similar velocity ranges, there is no 351.611+0.172 confusion between them in the Parkes spectra. Both sites are 351.611+0.172 likely to be part of the same star-forming cluster. 351.688+0.171 See note on 351.611+0.172 352.083+0.167 and 352.111+0.176. This known pair of sites has a separation of 352.083+0.167 more than 100 arcsec and non-overlapping velocity ranges. The 352.083+0.167 intensity of the second site has been stable but the first has 352.083+0.167 increased by more than a factor of 3 relative to 1999 May and 352.083+0.167 1993 September (Caswell et al. 1995MNRAS.272...96C; Caswell, 352.083+0.167 2009PASA...26..454C). The aligned spectra clearly distinguish 352.083+0.167 the features from each site. 352.111+0.176 See note on 352.083+0.167 352.604-0.225 and 352.584-0.185 Two new sites separated by more than 2 arcmin, 352.604-0.225 with the velocity range of the stronger site, 352.584-0.185, 352.604-0.225 straddling that of the weaker site. Their systemic velocities 352.604-0.225 correspond well with that expected for the near side of the 352.604-0.225 3-kpc arm. Both show some variability. The aligned spectra 352.604-0.225 show a small amount of confusion between them as measured at 352.604-0.225 Parkes, with a beamsize of 3.2 arcmin. 352.584-0.185 See note on 352.604-0.225 352.624-1.077 and 352.630-1.067. Two known sites separated by 42 arcsec. The 352.624-1.077 velocity ranges do not overlap and the separation of the sources 352.624-1.077 is clear on the aligned spectra. 352.630-1.067 See note on 352.624-1.077 353.216-0.249 New source with large variability, increasing from the survey 353.216-0.249 cube peak of 1.1Jy (2007 March) to 1.3Jy (ATCA, 2007 July) and 353.216-0.249 reaching 5.1Jy in the MX follow-up (2008 March). 353.273+0.641 Known source (Caswell & Phillips, 2008MNRAS.386.1521C) associated 353.273+0.641 with an unusual water maser showing dominant blueshifted 353.273+0.641 emission. The methanol intensity has faded from 25Jy in 1993 353.273+0.641 June to 12.7Jy in the survey cube (2007 March) and finally to 353.273+0.641 8.3Jy in the MX follow-up of 2008 March. 353.363-0.166 New maser located in the near side of the 3-kpc arm. 353.429-0.090 New maser with large velocity range of 18.9km/s, the widest in 353.429-0.090 this part of the survey. However, the weak features in the 353.429-0.090 velocity range -51 to -45km/s were not detected above the noise 353.429-0.090 level of the ATCA observations so it was not possible to 353.429-0.090 confirm conclusively that they all arise from this same site. 354.496+0.083 New maser located in the far side of the 3-kpc arm. 354.615+0.472 Known strong maser, showing modest variations in our survey and 354.615+0.472 follow-up period. However, the feature at -23km/s, which had a 354.615+0.472 peak intensity of 216Jy in 1992 December, has now faded to less 354.615+0.472 than 100Jy, whereas some other features show negligible change. 354.615+0.472 The high variability was noted by Caswell et al. 354.615+0.472 (1995PASA...12...37C) and additional monitoring information was 354.615+0.472 presented by Goedhart et al. (2004MNRAS.355..553G). 354.701+0.299 and 354.724+0.300. The first of these is a new maser with high 354.701+0.299 positive velocity exceeding 100km/s; the second maser was 354.701+0.299 already known and has a similar velocity. Such velocities are 354.701+0.299 highly unusual for this region of Galactic longitude. Indeed, 354.701+0.299 they are the highest positive velocity masers in any part of the 354.701+0.299 survey region covered here. The unusual velocities are discussed 354.701+0.299 in Section 4.5, in the context of the Galactic bar which appears 354.701+0.299 to be their most likely location. The separation between the 354.701+0.299 sites is 75 arcsec, causing spectral features of the offset 354.701+0.299 source to be seen on both Parkes spectra. 354.724+0.300 See note on 354.701+0.299 355.184-0.419 This is a new maser for which we display the spectrum from the 355.184-0.419 original survey cube (2007 January). Confirmation observations 355.184-0.419 with the ATCA (2007 February) showed a peak of 1.2Jy and yielded 355.184-0.419 a precise position. No MX measurement has yet been made. 355.343+0.148 , 355.344+0.147 and 355.346+0.149. These are three previously 355.343+0.148 known sites, with the first two separated by only about 2 arcsec 355.343+0.148 but the third offset by 10 arcsec. Recent careful evaluation of 355.343+0.148 information that in the past gave rise to conflicting 355.343+0.148 interpretations of their distance has now yielded the conclusion 355.343+0.148 that the masers most likely lie within 3kpc of the Galactic 355.343+0.148 Centre, or perhaps the far side of the 3-kpc arm (Caswell, 355.343+0.148 2009PASA...26..454C). A single spectrum is shown, and reference 355.343+0.148 to the table, and to ATCA spectra from Caswell 355.343+0.148 (1997MNRAS.289..203C), is needed to distinguish the features. 355.344+0.147 See note on 355.343+0.148 355.346+0.149 See note on 355.343+0.148 355.642+0.398 and 355.666+0.374. New sites, separated by just over 2 arcmin. 355.642+0.398 Their velocity ranges do not overlap and the aligned spectra 355.642+0.398 distinguish the two sites. 355.666+0.374 See note on 355.642+0.398 356.662-0.263 Known maser site located in the near side of the 3-kpc arm. 357.558-0.321 and 357.559-0.321 Newly discovered pair of sites separated by 357.558-0.321 3 arcsec and with quite separate velocity ranges. The second 357.558-0.321 source has velocity range +15 to +18km/s and is best interpreted 357.558-0.321 as being at Galactocentric radius R<3kpc (see Section 4.6). The 357.558-0.321 first source has a velocity range of -5.5 to 0km/s; from this 357.558-0.321 velocity, its location could be interpreted as R>3.5kpc. 357.558-0.321 However, their small projected separation suggests that the 357.558-0.321 sites are more likely close companions, at a common distance. 357.558-0.321 Therefore, for both sites, we favour R<3kpc, where anomalous 357.558-0.321 velocities are more common than at R>3.5kpc. 357.559-0.321 See note on 357.558-0.321 357.922-0.337 and 357.924-0.337. Another newly discovered pair, separated by 357.922-0.337 5 arcsec, with slight overlap of velocity ranges. The velocities 357.922-0.337 are compatible with a location R>3.5kpc. 357.924-0.337 See note on 357.922-0.337 357.965-0.164 and 357.967-0.163. This known pair of sites has a separation of 357.965-0.164 7 arcsec. Intensity variations have been modest for all 357.965-0.164 features. The stronger emission of the second source lies wholly 357.965-0.164 within the velocity range of the (much wider velocity) weak 357.965-0.164 source. Their velocities are compatible with a location 357.965-0.164 R>3.5kpc. 357.967-0.163 See note on 357.965-0.164 358.263-2.061 The Galactic latitude of this previously known site is large, and 358.263-2.061 lies just outside our formal survey coverage. We have 358.263-2.061 re-observed it and include it in catalog.dat so that the table 358.263-2.061 provides a complete current listing of reliably known masers in 358.263-2.061 the survey longitude range. The maser intensity has shown 358.263-2.061 modest variations. Its velocity, ranging from 0.5 to 6km/s, is 358.263-2.061 compatible with R>3.5kpc, after allowance for small (less than 358.263-2.061 7km/s) non-circular motions. This is consistent with its large 358.263-2.061 latitude, which almost certainly indicates that it is nearby, 358.263-2.061 with heliocentric distance of only a fewkpc. 358.386-0.483 and 358.371-0.468. Both sites are previously known, separated by 358.386-0.483 about 81 arcsec. The first shows emission from a single narrow 358.386-0.483 peak at velocity -6.2km/s which was only 2.5Jy in 1997 May 358.386-0.483 (Caswell, 2009PASA...26..454C) but the survey cube peak was 358.386-0.483 12.5Jy in 2006 February, decreasing in the MX follow-up 358.386-0.483 observations of 2008 March to 7Jy. The second site has features 358.386-0.483 in the range -1 to +13km/s, with peak at +0.8km/s and fairly 358.386-0.483 stable at 45Jy. Both sites are acceptably interpreted as being 358.386-0.483 located at R>3.5kpc. The aligned spectra clearly distinguish the 358.386-0.483 emission from each site. 358.371-0.468 See note on 358.386-0.483 358.460-0.391 and 358.460-0.393. These are both new, separated by 7 arcsec. The 358.460-0.391 first has a velocity range of +0.5 to +4.0km/s and its peak (at 358.460-0.391 velocity +1.2km/s) has increased from the survey cube value of 358.460-0.391 25Jy (2006 February) to the ATCA value of 35Jy (2006 March) 358.460-0.391 and MX follow-up (2008 March) value of 48Jy. The second maser 358.460-0.391 has a peak at -7.5km/s of 11Jy which has remained stable, and 358.460-0.391 the velocity range of -8.5 to +6km/s encompasses that of the 358.460-0.391 first. Both are acceptably interpreted as located at R>3.5kpc. 358.460-0.393 See note on 358.460-0.391 358.721-0.126 We formally interpret the velocity of this new maser as 358.721-0.126 indicating a distant site outside the solar circle, but with 358.721-0.126 R<13.5kpc; however, the choice is not clear-cut since it lies 358.721-0.126 slightly outside our suggested boundary for this 358.721-0.126 longitude-velocity domain in Fig. 4 of Paper II (Green et al., 358.721-0.126 2010MNRAS.409..913G), perhaps indicating a location with R<3kpc. 358.809-0.085 The velocity of this new site perfectly matches the value 358.809-0.085 expected for a location in the near side of the 3-kpc arm. 358.841-0.737 New maser with a velocity offset from zero sufficient to indicate 358.841-0.737 non-circular motions and a location at R<3kpc. 358.906+0.106 New maser with velocity suggesting R<3kpc. 358.931-0.030 New maser with velocity similar to the previous site and likely 358.931-0.030 to be at R<3kpc. 358.980+0.084 New site fading from a peak of 1.6Jy in the survey cube (2006 358.980+0.084 February) to less than 0.2Jy in the MX spectrum of 2008 March; 358.980+0.084 an intermediate value of 0.5Jy was measured at the intermediate 358.980+0.084 epoch 2007 November in the ATCA measurement. The survey cube 358.980+0.084 spectrum is shown in Fig. 1. The velocity near zero is 358.980+0.084 compatible with R>3.5kpc if small non-circular motions are 358.980+0.084 assumed. 359.138+0.031 For this known site, a weak feature at velocity -6km/s was 359.138+0.031 clearly visible in 1992 and 1995 with peak flux density of 1.0 359.138+0.031 and 0.7Jy, respectively, and although now only marginally 359.138+0.031 detectable (0.25Jy), was used to define the velocity range; the 359.138+0.031 systemic velocity is compatible with R>3.5kpc. 359.436-0.104 and 359.436-0.102. Both sites are previously known. Their 359.436-0.104 velocity ranges do not significantly overlap and the two sources 359.436-0.104 shown on a single spectrum are distinguishable from the velocity 359.436-0.104 ranges given in catalog.dat. Both systemic velocities indicate 359.436-0.104 a location in the near side of the 3-kpc arm. At a distance of 359.436-0.104 5.1kpc, their separation of 6.1 arcsec corresponds to 150Mpc. 359.436-0.104 The first site is the stronger and its peak at -46.8km/s has 359.436-0.104 increased from less than 7Jy (in 1992 and 1995) to 60Jy in the 359.436-0.104 survey cube and to 75Jy in the MX spectrum of 2008 March; a 359.436-0.104 feature at -52km/s which was the strongest (27Jy) in 1992 has 359.436-0.104 decreased to 13Jy in 2008. The second site has recent peak 359.436-0.104 intensities of 1.5 and 1.6Jy, similar to 1992 but much smaller 359.436-0.104 than its value of 4.4Jy in 1995 (Caswell, 2009PASA...26..454C). 359.436-0.104 Forster & Caswell (2000ApJ...530..371F) show a detailed map of 359.436-0.104 continuum emission together with information on other masers. 359.436-0.102 See note on 359.436-0.104 359.615-0.243 Known, strong maser and highly variable. The peak intensity for 359.615-0.243 the spectrum from the survey cube (2006 February) is at a 359.615-0.243 velocity different from that of the follow-up MX spectrum (2008 359.615-0.243 March), and thus variability exceeds a factor of 2; indeed, near 359.615-0.243 velocity +22.6km/s, intensities since 1992 have ranged from 15 359.615-0.243 to 88Jy. The high variability was noted by Caswell et al. 359.615-0.243 (1995PASA...12...37C) and additional monitoring information was 359.615-0.243 presented by Goedhart et al. (2004MNRAS.355..553G). The positive 359.615-0.243 systemic velocity is significantly offset from zero, indicating 359.615-0.243 non-circular motions and a location at a Galactocentric radius 359.615-0.243 R<3kpc. 359.938+0.170 New single feature maser with flux density varying from 1.6Jy in 359.938+0.170 our survey cube discovery spectrum (2006 February) to 0.75Jy in 359.938+0.170 our ATCA measurement (2007 July) and 2.4Jy in our MX follow-up 359.938+0.170 (2008 March). The near-zero velocity is compatible with 359.938+0.170 R>3.5kpc. 359.970-0.457 Known maser, with one feature increasing from 1Jy in 1992 to our 359.970-0.457 MX measurement of 2.4Jy in 2008 March, but the other fading from 359.970-0.457 0.8Jy to less than 0.2Jy, below our detection threshold. We cite 359.970-0.457 the velocity range seen in 1992, +20 to +24km/s; the velocity 359.970-0.457 offset from zero indicates non-circular motions and a 359.970-0.457 Galactocentric radius R<3kpc. 0.092-0.663 New strong maser with its velocity suggesting R<3kpc. 0.167-0.446 New maser with intensity fading markedly from the survey cube 0.167-0.446 value 4.4Jy (2006 February) to 3.6Jy during the ATCA measurement 0.167-0.446 (2006 March) and to 1.3Jy for the MX spectrum (2008 March). 0.167-0.446 Its systemic velocity suggests R<3kpc. 0.212-0.001 Known maser with velocity just within the range of the far side 0.212-0.001 of the 3-kpc arm. 0.315-0.201 and 0.316-0.201. Known very close pair of maser sites, 0.315-0.201 distinguishable on the ATCA spectra shown in Caswell 0.315-0.201 (1996MNRAS.279...79C) and displayed here in a single spectrum. 0.315-0.201 Intensity increases since 1995 are less than a factor of 2. The 0.315-0.201 first site is strong with a wide velocity range; the second site 0.315-0.201 is weak, with its small velocity range of emission contained 0.315-0.201 within that of the stronger site. The systemic velocities 0.315-0.201 strongly suggest R<3kpc and thus a heliocentric distance >5kpc, 0.315-0.201 for which the separation of 2.6 arcsec corresponds to more 0.315-0.201 than 60Mpc, in accord with the interpretation as two separate 0.315-0.201 sites (Caswell, 2009PASA...26..454C). 0.316-0.201 See note on 0.315-0.201 0.376+0.040 Known maser with intensity variations from 0.7Jy (1992 and 1999 0.376+0.040 February), flaring to 2.3Jy in our survey cube (2006 February) 0.376+0.040 and back to 0.62Jy in our MX spectrum (2008 March). Its velocity 0.376+0.040 indicates R<3kpc. 0.409-0.504 New maser, likely to be within R<3kpc. 0.475-0.010 The history of this source is given by Caswell 0.475-0.010 (2009PASA...26..454C), and identifies the error leading to the 0.475-0.010 incorrect position of 0.393-0.034 originally reported by 0.475-0.010 Caswell (1996MNRAS.279...79C). The corrected position and its 0.475-0.010 re-evaluated peak intensity of 2.9Jy from re-analysis of the old 0.475-0.010 data from 1995 November (Caswell, 2009PASA...26..454C) agree 0.475-0.010 well with our new measurements between 2006 and 2009. The 0.475-0.010 velocity range as measured in the earlier data is given in 0.475-0.010 catalog.dat; the systemic velocity implies a likely R<3kpc. 0.496+0.188 Known maser with many spectral features; the intensity is now 0.496+0.188 more than twice as strong as the 10Jy main peak measured in 1995 0.496+0.188 November. The velocity range straddling zero velocity could be 0.496+0.188 compatible with R>3.5kpc. 0.546-0.852 Known methanol maser site accompanied by water and OH masers and 0.546-0.852 continuum emission (Forster & Caswell, 2000ApJ...530..371F). 0.546-0.852 Formally, the velocity suggests a distant object outside the 0.546-0.852 solar circle, or an anomalous velocity of a site within R<3kpc. 0.546-0.852 However, in view of its large latitude, it has alternatively 0.546-0.852 been interpreted as nearby (with R>3.5kpc) and an unusually 0.546-0.852 large peculiar motion (Gardner & Whiteoak, 1975MNRAS.171P..29G; 0.546-0.852 Caswell, 1998MNRAS.297..215C). An astrometric distance will 0.546-0.852 eventually resolve this uncertainty and yield an excellent 0.546-0.852 distance if it is indeed nearby. Pending new data, we note that 0.546-0.852 a far distance outside the solar circle of more than 17kpc would 0.546-0.852 imply an unlikely large Galactic height, z, of 250pc. In 0.546-0.852 contrast, a heliocentric distance between 5.5 and 8.5kpc would 0.546-0.852 not imply an unreasonable value of Galactic height, z, nor a 0.546-0.852 contradiction to the apparent quite low obscuration (assuming 0.546-0.852 the optical nebula RCW 142 to be associated). So 0.546-0.852 we provisionally regard it as an object with R<3kpc, as was 0.546-0.852 assumed by Russeil (2003A&A...397..133R). 0.645-0.042 to 0.695-0.038 inclusive. These 11 sites in a cluster near Sgr B2 0.645-0.042 are contained within 3 arcmin and are individually separated by 0.645-0.042 more than 10 arcsec. Nine sites were seen in the results of 0.645-0.042 Caswell (1996MNRAS.279...79C, 2009PASA...26..454C), and were 0.645-0.042 also visible with the sensitivity of our present survey 0.645-0.042 (although confused in the single-dish spectrum). The other two 0.645-0.042 sites are very weak and were detected only in the observations 0.645-0.042 of Houghton & Whiteoak (1995MNRAS.273.1033H) who achieved high 0.645-0.042 sensitivity with the ATCA using a full synthesis (although with 0.645-0.042 low spectral resolution, channel spacing 8kHz equivalent to 0.645-0.042 0.4km/s). In catalog.dat, for all sites, we cite the HW 0.645-0.042 (Houghton & Whiteoak 1995MNRAS.273.1033H) positions and velocity 0.645-0.042 ranges. We list Parkes measurements of flux density where they 0.645-0.042 were not too confused. We were unable to establish reliable 0.645-0.042 peak flux density values for 0.647-0.055 (2Jy HW; 3.4Jy Caswell, 0.645-0.042 1996MNRAS.279...79C), 0.657-0.041 (1.8Jy HW; 3.0Jy Caswell, 0.645-0.042 1996MNRAS.279...79C), 0.667-0.034 (0.4Jy HW) and 0.673-0.029 0.645-0.042 (0.4Jy HW) but, for convenience, list the HW velocity in the 0.645-0.042 table, and the corresponding HW flux density in parenthesis 0.645-0.042 after the reference. Variability is difficult to establish in 0.645-0.042 view of confusion for all measurements except those of Houghton 0.645-0.042 and Whiteoak. Representative spectra are shown at three 0.645-0.042 locations which span the positions of all 11 sites, with all 11 0.645-0.042 labelled to show which spectrum best matches their position. 0.645-0.042 Reference to Houghton & Whiteoak (1995MNRAS.273.1033H) is needed 0.645-0.042 to distinguish the sites, and the labels on the spectra for 0.645-0.042 those four sites that are extremely confused are enclosed in 0.645-0.042 square brackets. 0.836+0.184 Known site, with velocity close to zero compatible with R>3.5kpc. 1.008-0.237 New site, with velocity close to zero compatible with R>3.5kpc. 1.147-0.124 New precise position (see also Walsh et al. 1998MNRAS.301..640W). 1.147-0.124 The unusual velocity is most simply interpreted if R<3kpc. 1.329+0.150 New single feature maser with unusual velocity best interpreted 1.329+0.150 if R<3kpc. 1.719-0.088 New site. The velocity is slightly negative and requires an 1.719-0.088 assumption of small non-circular motions to be compatible with 1.719-0.088 R>3.5kpc. 2.143+0.009 Known maser with velocity well matched to the far side of the 2.143+0.009 3-kpc arm. There is no detectable UCHII region (Forster & 2.143+0.009 Caswell 2000ApJ...530..371F). 2.521-0.220 New maser with velocity straddling zero and compatible with 2.521-0.220 R>3.5kpc. 2.536+0.198 Known site with a wide velocity range from 2 to 20.5km/s; the 2.536+0.198 systemic velocity is compatible with R>3.5kpc. 2.591-0.029 New maser with negative velocity. The assumption of a 2.591-0.029 non-circular motion component is needed for compatibility with 2.591-0.029 a Galactocentric radius R>3.5kpc. 2.615+0.134 and 2.703+0.040. Two new sites with overlapping velocity ranges 2.615+0.134 but separated by more than 7 arcmin and not confused (contrary 2.615+0.134 to the similar appearance of features near +95km/s). Their large 2.615+0.134 positive velocities are most readily attributed to a location 2.615+0.134 in the Galactic bar (see Section 4). 2.703+0.040 See note on 2.615+0.134 3.253+0.018 New maser with velocity straddling zero and compatible 3.253+0.018 with R>3.5kpc. 3.312-0.399 New weak maser with small positive velocity compatible 3.312-0.399 with R>3.5kpc. 3.442-0.348 New maser with single weak feature at a velocity well matched to 3.442-0.348 the near side of 3-kpc arm. 3.502-0.200 New maser at a quite high velocity that is not compatible with 3.502-0.200 the 3-kpc arm nor with R>3.5kpc; we therefore locate it 3.502-0.200 within R<3kpc. 4.569-0.079 and 4.866-0.171. Two of our weakest new masers, with flux 4.569-0.079 densities of 0.44 and 0.56Jy, respectively. 4.866-0.171 See note on 4.569-0.079 5.618-0.082 New maser with velocity well matched to the near side of 5.618-0.082 the 3-kpc arm. 5.885-0.393 New maser with single feature at a velocity of +6.7km/s. It 5.885-0.393 coincides with a previously known OH maser and strong HII 5.885-0.393 region, believed to be at a distance of 2kpc (Stark et al., 5.885-0.393 2007ApJ...656..943S). An earlier unsuccessful search for 5.885-0.393 methanol in this direction, made in 1992 (Caswell et al. 5.885-0.393 1995MNRAS.272...96C), yielded an upper limit of 0.3Jy, 5.885-0.393 presumably because it was weak at that epoch. Our position 5.885-0.393 measurement with the ATCA (2006 December) showed a peak 5.885-0.393 intensity similar to the survey cube value (2006 August) of 5.885-0.393 1.3Jy, but our MX follow-up spectrum (2008 March) showed that it 5.885-0.393 had faded again, to 0.5Jy; both the survey cube and MX spectra 5.885-0.393 are shown. Note that 5.885-0.393 is only 2 arcmin from the known 5.885-0.393 source 5.900-0.430, and its velocity, straddled by features of 5.885-0.393 the known source, suggest that the two sites are located at a 5.885-0.393 similar distance. We have aligned their spectra so as to make it 5.885-0.393 clear that only a single weak feature arises from 5.885-0.393. 6.189-0.358 This is the brightest (229Jy) new detection of the MMB survey and 6.189-0.358 is associated with the near 3-kpc arm. 6.368-0.052 , 7.601-0.139 and 7.632-0.109. These three new sources all have 6.368-0.052 high velocities (144.1km/s, 154.7km/s and 157.0km/s, 6.368-0.052 respectively) and are potentially associated with the Galactic 6.368-0.052 bar. For the closely spaced pair, 7.601-0.139 incorporates the 6.368-0.052 features between 155 and 157km/s, whilst 7.632-0.109 6.368-0.052 incorporates the features outside these velocities. All three 6.368-0.052 sources may be linked to the known high-velocity HI at these 6.368-0.052 longitudes, which extends from the plane to high latitudes (see 6.368-0.052 e.g. McClure-Griffiths et al., 2005ApJS..158..178M). 6.368-0.052 6.368-0.052 displays a feature of 0.2Jy at 136km/s in both the 6.368-0.052 MX taken in 2008 March and the MX taken in 2009 March, however 6.368-0.052 it has not been confirmed with the ATCA. 7.601-0.139 See note on 6.368-0.052 7.632-0.109 See note on 6.368-0.052 6.539-0.108 , 6.588-0.192 and 6.610-0.082. We have detected a new source 6.539-0.108 amongst two previously known sources. The new source, 6.539-0.108 6.588-0.192, has three blended peaks between 4 and 6km/s. 6.539-0.108 6.539-0.108 has a clear feature at 13.5km/s and 6.610-0.082 has 6.539-0.108 a clear feature at 0.8km/s, both known from previous 6.539-0.108 observations. Additionally we detect weak emission between 6 and 6.539-0.108 7km/s in the spectrum of 6.539-0.108 and weak emission (<0.9Jy) 6.539-0.108 at 5-6km/s and ~10km/s in the spectrum of 6.610-0.082. The 6.539-0.108 features in both spectra near 6km/s may partially be a sidelobe 6.539-0.108 response of the new source 6.588-0.192. A fourth source may 6.539-0.108 exist in the region, but it could not be resolved with the ATCA, 6.539-0.108 and would require future VLBI observations. LSR velocities near 6.539-0.108 zero at this Galactic longitude imply heliocentric distances of 6.539-0.108 either a few kpc or beyond 10kpc. Downes et al. 6.539-0.108 (1980A&AS...40..379D) ascribe the associated HII region 6.539-0.108 6.553-0.095 to the far kinematic distance based on formaldehyde 6.539-0.108 absorption. They also speculated that it might be in the 3-kpc 6.539-0.108 arm, but this seems unlikely since the velocities do not 6.539-0.108 correspond with either of the arms as defined in Dame & 6.539-0.108 Thaddeus (2008ApJ...683L.143D). 6.588-0.192 See note on 6.539-0.108 6.610-0.082 See note on 6.539-0.108 6.795-0.257 This source has a wide velocity range of 19.3km/s with the 6.795-0.257 features between 25 and 30km/s probably separated from the 6.795-0.257 bright feature at ~14km/s by approximately 1 arcsec. Overall, 6.795-0.257 the features increased in flux density between the survey cube 6.795-0.257 observation and the MX (2009 March). 7.166+0.131 This is a new source to the survey and clearly associated with 7.166+0.131 the far 3-kpc arm. It also exhibits a wide velocity range 7.166+0.131 of 16.5km/s. 8.139+0.226 This source, when first discovered by Schutte et al. 8.139+0.226 (1993MNRAS.261..783S), had a peak flux density of ~15Jy. A 8.139+0.226 position was obtained in 2000 by Caswell (2009PASA...26..454C) 8.139+0.226 with a peak flux density of only 3.5Jy. The survey cube spectrum 8.139+0.226 (taken in 2006/2007) showed a higher peak flux density of 5.2Jy. 8.139+0.226 The MX taken in 2009 showed a peak flux density of over twice 8.139+0.226 this at 11.4Jy. On the basis of a lack of formaldehyde 8.139+0.226 absorption, Wink, Altenhoff & Mezger (1982A&A...108..227W) 8.139+0.226 suggest the associated compact HII region is most likely at the 8.139+0.226 near kinematic distance. 8.669-0.356 and 8.683-0.368. The spectra of this close pair of sources 8.669-0.356 contain a feature at ~36km/s which is likely to be variable and 8.669-0.356 could not be clearly attributed to either one of the sources. 8.669-0.356 8.669-0.356 comprises only the small feature at ~39km/s, whilst 8.669-0.356 8.683-0.368 contains all other features seen in the spectrum. 8.669-0.356 Downes et al. (1980A&AS...40..379D) ascribe the associated HII 8.669-0.356 region to the near kinematic distance based on a lack of 8.669-0.356 formaldehyde absorption. 8.683-0.368 See note on 8.669-0.356 8.832-0.028 This is a bright new source (159Jy) also recently positioned by 8.832-0.028 Xu et al. (2009A&A...507.1117X) with the ATCA. It is associated 8.832-0.028 with the near 3-kpc arm. 8.872-0.493 This new source was also recently positioned by Xu et al. 8.872-0.493 (2009A&A...507.1117X) with the ATCA. It is potentially 8.872-0.493 associated with the molecular cloud 8.9-0.5 (velocity of 12km/s) 8.872-0.493 from Solomon et al. (1987ApJ...319..730S), which was claimed by 8.872-0.493 the authors to have kinematics matching those of the near 3-kpc 8.872-0.493 arm. However, the kinematics do not match an extrapolation of 8.872-0.493 the arm based on Cohen & Davies (1976MNRAS.175....1C) nor the 8.872-0.493 more recent definition of Dame & Thaddeus (2008ApJ...683L.143D). 8.872-0.493 Applying current kinematic models, the velocity of 8.872-0.028 8.872-0.493 (~23km/s) would place it in either the Carina-Sagittarius or 8.872-0.493 Perseus arms. If the maser is associated with the 8.9-0.5 8.872-0.493 molecular cloud (with a 10km/s unusual velocity), then that 8.872-0.493 would place it more likely in the Perseus, rather than the 8.872-0.493 Carina-Sagittarius arm. In either case the source is unlikely to 8.872-0.493 be associated with the near 3-kpc arm. 9.621+0.196 and 9.619+0.193. This famous source and its companion have been 9.621+0.196 extensively studied since discovery in 1991 (Menten 9.621+0.196 1991ApJ...380L..75M; Norris et al. 1993ApJ...412..222N; 9.621+0.196 Walsh et al. 1997MNRAS.291..261W, 1998MNRAS.301..640W; 9.621+0.196 Phillips et al. 1998MNRAS.300.1131P; Caswell, 9.621+0.196 2009PASA...26..454C). There has also been extensive monitoring 9.621+0.196 of 9.621+0.196 by Caswell, Vaile & Ellingsen 9.621+0.196 (1995PASA...12...37C), Goedhart, Gaylard & van der Walt 9.621+0.196 (2003MNRAS.339L..33G, 2004MNRAS.355..553G), van der Walt, 9.621+0.196 Goedhart & Gaylard (2009MNRAS.398..961V), Vlemmings, Goedhart & 9.621+0.196 Gaylard (2009A&A...500L...9V), with Goedhart et al. 9.621+0.196 (2003MNRAS.339L..33G,) detecting periodic flares (see Section 9.621+0.196 4.3 for details). The weaker source, 9.619+0.193, probably has 9.621+0.196 just two features. Several authors have postulated the pair lie 9.621+0.196 within the 3-kpc arm (e.g. Hofner et al. 1994ApJ...429L..85H; 9.621+0.196 Caswell et al. 1995MNRAS.272...96C; Green et al., 9.621+0.196 2009ApJ...696L.156G) and recent trigonometric parallax 9.621+0.196 measurements of 12GHz methanol (Sanna et al., 9.621+0.196 2009ApJ...706..464S) established a heliocentric distance of 9.621+0.196 5.2+/-0.6kpc (corresponding to a Galactocentric distance 9.621+0.196 consistent with 3-kpc arm estimates). 9.619+0.193 See note on 9.621+0.196 9.986-0.028 This source consists of a group of three strong (>10Jy) features 9.986-0.028 between 40 and 45km/s (two of which are blended in the Parkes 9.986-0.028 spectrum), an outlying strong feature at 47km/s and other weaker 9.986-0.028 (<10Jy) emission between 40 and 52km/s. The 47km/s feature was 9.986-0.028 the brightest at 35Jy in the original Schutte et al. 9.986-0.028 (1993MNRAS.261..783S) Hartebeesthoek observations, but had 9.986-0.028 decreased to 28Jy in the ATCA observations made in 2000 by 9.986-0.028 Caswell (2009PASA...26..454C). In our observations this feature 9.986-0.028 is stable between the survey cube (2007 January) and MX 9.986-0.028 (2009 March) observations with a peak flux density of ~27Jy. 9.986-0.028 Meanwhile, the feature at 42km/s which had shown a steady 9.986-0.028 increase from ~15 to 26Jy between the Schutte et al. 9.986-0.028 (1993MNRAS.261..783S) and Caswell (2009PASA...26..454C) 9.986-0.028 observations now dominates the spectrum. Our survey cube and MX 9.986-0.028 observations find a peak flux density of ~70Jy. The 43.5km/s 9.986-0.028 feature decreased from 32Jy in 1993 to 20Jy in 2000, increased 9.986-0.028 to 24Jy in the survey cube and decreased to 20Jy in the MX. The 9.986-0.028 40.5km/s feature has been stable at ~25Jy across all the 9.986-0.028 observations with the exception of the survey cube where it 9.986-0.028 flared to 38Jy. 10.205-0.345 , 10.287-0.125, 10.299-0.146, 10.323-0.160 and 10.342-0.142. 10.205-0.345 These are the first of four groups of sources which are in the 10.205-0.345 direction of the W31 complex. The close proximity of all these 10.205-0.345 sources leads to confusion in the Parkes spectra; however the 10.205-0.345 high spatial resolution of the ATCA observations allows 10.205-0.345 identification of the different source features: 10.205-0.345 10.205-0.345 has emission between 5 and 11km/s with a peak at 10.205-0.345 7.2km/s; 10.287-0.125 contains the three features with 10.205-0.345 velocities less than 5km/s; 10.299-0.146 is the small feature at 10.205-0.345 ~20km/s; 10.323-0.160 is the feature at 6km/s and the double 10.205-0.345 feature between 9 and 13km/s; 10.342-0.142 exists between 7 and 10.205-0.345 17km/s, but not including the bright peaks of the previous 10.205-0.345 mentioned source. 10.323-0.160 has been monitored for 10.205-0.345 variability by Goedhart et al. (2004MNRAS.355..553G). 10.205-0.345 10.287-0.125 and 10.342-0.142 are associated with Extended Green 10.205-0.345 Objects (Cyganowski et al., 2009ApJ...702.1615C). Wilson et al. 10.205-0.345 (1984A&A...134L...7W) detected methanol absorption at 23GHz. 10.287-0.125 See note on 10.205-0.345 10.299-0.146 See note on 10.205-0.345 10.323-0.160 See note on 10.205-0.345 10.342-0.142 See note on 10.205-0.345 10.323-0.160 and 10.356-0.148. These sources, also in the direction of W31, 10.323-0.160 have emission at higher velocities: 10.320-0.160 comprises the 10.323-0.160 features between 35 and 40km/s and 10.356-0.148 the features 10.323-0.160 between 49 and 54km/s. 10.356-0.148 See note on 10.323-0.160 10.444-0.018 , 10.472+0.027 and 10.480+0.033. Although close to W31 spatially, 10.444-0.018 the high velocities of this trio of sources separates them from 10.444-0.018 the complex. 10.472+0.027 and 10.480+0.033, separated by 10.444-0.018 ~6 arcmin, and originally identified as 10.47+0.03, were 10.444-0.018 highlighted by Caswell et al. (1995PASA...12...37C) as extremely 10.444-0.018 variable and have been monitored for variability by Goedhart et 10.444-0.018 al. (2004MNRAS.355..553G). The sources have a very wide range of 10.444-0.018 velocity emission which is comparable to the nearby 10.444-0.018 source 10.444-0.018. 10.472+0.027 See note on 10.444-0.018 10.480+0.033 See note on 10.444-0.018 10.627-0.384 and 10.629-0.333. This is the fourth group of sources which have 10.627-0.384 been loosely associated with W31. 10.627-0.384 includes the 10.627-0.384 small feature on the edge of the absorption at approximately 10.627-0.384 -6km/s, but not the outlying features. Absorption was also 10.627-0.384 evident in the Parkes spectrum shown by Caswell et al. 10.627-0.384 (1995MNRAS.272...96C). 10.629-0.333 is kinematically associated 10.627-0.384 with the near 3-kpc arm as defined by Dame & Thaddeus 10.627-0.384 (2008ApJ...683L.143D). Although marginally offset in peak 10.627-0.384 velocity, the close spatial association of 10.627-0.384 together 10.627-0.384 with its emission at negative velocities implies this source is 10.627-0.384 also associated. The other three groups of sources previously 10.627-0.384 mentioned are offset in position and velocity from 10.627-0.384 10.627-0.384 and 10.629-0.333, and so do not appear to be associated with the 10.627-0.384 near 3-kpc arm as defined by Dame & Thaddeus 10.627-0.384 (2008ApJ...683L.143D). This implies that 10.629-0.333 and 10.627-0.384 10.627-0.384 may be a chance spatial alignment with W31 and not 10.627-0.384 actually associated. Conversely if the whole W31 complex is 10.627-0.384 associated with the near 3-kpc arm, as was suggested by Downes 10.627-0.384 et al. (1980A&AS...40..379D), the 3-kpc arm kinematics differ 10.627-0.384 from that observed by Dame & Thaddeus (2008ApJ...683L.143D). 10.627-0.384 Fish et al. (2003ApJ...587..701F) argues that 10.629-0.333 is 10.627-0.384 unlikely to be at the far distance based on HI absorption 10.627-0.384 observations towards an associated compact HII region. 10.629-0.333 See note on 10.627-0.384 10.724-0.334 This source is associated with the near 3-kpc arm. It has 10.724-0.334 significantly brightened from 1.5Jy in the survey cube 10.724-0.334 observation to 5Jy in the MX. 10.822-0.103 This source had three features in the survey cube observation, 10.822-0.103 between 68 and 74km/s. The ATCA data detected all three, but at 10.822-0.103 minimal signal-to-noise ratio. The MX taken in 2009 March only 10.822-0.103 detected one feature at a velocity of 69km/s. 10.886+0.123 Both the survey cube and MX data (2008 March) show consistency in 10.886+0.123 the shape of the spectrum and the peak flux densities of the 10.886+0.123 features, although the ATCA spectrum had flux densities of 10.886+0.123 a factor of 2 lower. 11.034+0.062 The 25km/s feature seen in the spectrum is a sidelobe response 11.034+0.062 to 10.958+0.022. 11.109-0.114 This new source to the survey was also detected by Ellingsen 11.109-0.114 (2007MNRAS.377..571E), but listed as 11.15-0.14. 11.903-0.102 and 11.904-0.141. Of this pair of sources 11.904-0.141 accounts 11.903-0.102 for the features between ~40 and 45km/s and 11.903-0.102 for the 11.903-0.102 lower velocity features. No variability was present between the 11.903-0.102 observations of Caswell et al. (1995MNRAS.272...96C) and 11.903-0.102 Caswell (1997MNRAS.289..203C); however our observations find 11.903-0.102 that for 11.903-0.102 the original peak feature at 36km/s has 11.903-0.102 increased from 1.8Jy (Caswell, 1997MNRAS.289..203C) to 4.5Jy. 11.903-0.102 Additionally the feature at 33.8km/s has increased from 1.5Jy 11.903-0.102 (Caswell, 1997MNRAS.289..203C) to ~11.5Jy. 11.904-0.141 See note on 11.903-0.102 11.936-0.150 This source only contains the features seen between 45 and 11.936-0.150 50km/s. Features <45km/s are sidelobe responses to 11.904-0.141. 11.936-0.616 This source is associated with an Extended Green Object 11.936-0.616 (Cyganowski et al., 2009ApJ...702.1615C). Solomon et al. 11.936-0.616 (1987ApJ...319..730S) attribute the associated molecular cloud, 11.936-0.616 12.00-0.60, to the near kinematic distance based on a 11.936-0.616 velocity-linewidth argument. 12.025-0.031 This is a known source clearly associated with the far 3-kpc arm. 12.181-0.123 , 12.199-0.033, 12.202-0.120, 12.203-0.107 and 12.209-0.102. 12.181-0.123 This complex cluster of five sources is divided as: 12.181-0.123 12.181-0.123 which consists of the two features at ~30km/s; 12.181-0.123 12.202-0.120 which comprises the features between 20 and 12.181-0.123 ~32.5km/s; 12.181-0.123 12.203-0.107 which is the feature peaking at 20.5km/s; 12.181-0.123 12.209-0.102 which is composed of the weak features between 15 12.181-0.123 and ~23km/s; 12.181-0.123 12.199-0.033, although spatially close, is well separated in 12.181-0.123 velocity. 12.199-0.033 See note on 12.181-0.123 12.202-0.120 See note on 12.181-0.123 12.203-0.107 See note on 12.181-0.123 12.209-0.102 See note on 12.181-0.123 12.625-0.017 The brightest feature of this maser at 21.6km/s has increased 12.625-0.017 from ~10Jy (2007 August) to almost 25Jy (2008 March). 12.681-0.182 This source has previously been seen to vary from maximum flux 12.681-0.182 density to minimum flux density by a factor of 1.5 over a 12.681-0.182 3-month period (Caswell et al. 1995PASA...12...37C) and was a 12.681-0.182 source monitored for variability by Goedhart et al. 12.681-0.182 (2004MNRAS.355..553G), who found that all maser peaks exhibited 12.681-0.182 a simultaneous variation with a quasi-periodic time-scale of 12.681-0.182 307+/-60d. We made three observations, the original survey cube 12.681-0.182 in 2007 August and two MX observations taken in 2008 March and 12.681-0.182 2009 March. The 2007 August and 2008 March spectra show 12.681-0.182 consistent spectral features (with flux densities comparable to 12.681-0.182 within 5 per cent) with the exception of the two features at 59 12.681-0.182 and 60km/s, which decreased by ~20 per cent. In the 2009 March 12.681-0.182 spectrum the features at 57.5, 59 and 60km/s had all decreased 12.681-0.182 from the 2007 August flux densities by 12 per cent, 60 per 12.681-0.182 cent and 46 per cent, respectively. 12.889+0.489 The features of this source were seen to vary from maximum flux 12.889+0.489 density to minimum flux density by a factor of 1.3 over an 12.889+0.489 8-month period (Caswell et al. 1995PASA...12...37C), and it was 12.889+0.489 then monitored for variability by Goedhart et al. 12.889+0.489 (2004MNRAS.355..553G), Goedhart et al. (2009MNRAS.398..995G). It 12.889+0.489 has been shown to have a short period of only 29.5d. The MMB 12.889+0.489 survey cube observations have a peak flux density of 78.9Jy 12.889+0.489 (2007 August) and the MX 68.9Jy (2008 March) (see also 12.889+0.489 Section 4.3 of Paper II, Green et al., 2010MNRAS.409..913G). 12.909-0.260 This source is associated with W33 and has been monitored for a 12.909-0.260 variability by Goedhart et al. (2004MNRAS.355..553G). The 12.909-0.260 authors found the 39.4 and 39.8km/s features showed little 12.909-0.260 variation, whilst the 35.9km/s feature had a monotonic increase 12.909-0.260 from 12 to 20Jy over their duration of their observations. We 12.909-0.260 find a peak flux density of 245Jy at 39.9km/s in the survey cube 12.909-0.260 rising to 269Jy in the later MX (2008 March). Additional MX 12.909-0.260 observations in 2009 March found 210Jy (at 39.4km/s) and 250Jy 12.909-0.260 (at 39.9km/s). The feature at 35.9km/s had a flux density of 12.909-0.260 25Jy at the time of the survey cube, 22.5Jy in 2008 March MX and 12.909-0.260 22Jy in 2009 March MX. The nearby object listed as 12.79-0.19 in 12.909-0.260 Menten (1991ApJ...380L..75M) and not detected by either Caswell 12.909-0.260 et al. (1995MNRAS.272...96C) or Caswell (2009PASA...26..454C) 12.909-0.260 was again not detected in a targeted MX observation. Clear 12.909-0.260 absorption of ~2Jy was found in the Parkes spectrum, but no 12.909-0.260 detectable spectral structure indicative of maser emission. In 12.909-0.260 agreement with Voronkov et al. (2010MNRAS.405.2471V), this 12.909-0.260 location is about 7 arcmin from 12.909-0.260 and the 5Jy peak 12.909-0.260 flux density listed by Menten (1991ApJ...380L..75M) implies 12.909-0.260 12.79-0.19 was a sidelobe response to 12.909-0.260. 13.696-0.156 This is a new source detected by the MMB survey and is clearly 13.696-0.156 associated with the far 3-kpc arm. 14.101+0.087 This source is associated with the near 3-kpc arm and a position 14.101+0.087 was recently obtained by Xu et al. (2009A&A...507.1117X). 14.230-0.509 This source was observed as a single feature peak of 3.6Jy at 14.230-0.509 25.3km/s in the survey cube observations. It was then 14.230-0.509 undetectable in both the 2008 March MX and the ATCA observation 14.230-0.509 taken in 2008 October. Fortunately, it was detected again with 14.230-0.509 the ATCA in 2009 January and a position was successfully 14.230-0.509 obtained, with a peak flux density of 0.4Jy at the original 14.230-0.509 velocity of 25.3km/s. It was then undetected in a subsequent 14.230-0.509 MX taken in 2009 March. 14.521+0.155 This is a new source associated with the near 3-kpc arm. A 14.521+0.155 feature of 0.5Jy at -2km/s was seen in the MX observation (2009 14.521+0.155 March) which was not present in the prior survey cube 14.521+0.155 observation. 14.991-0.121 This source includes two weak features at 52.5 and 54km/s. 15.034-0.677 This source is associated with the HII region in M17 (Caswell, 15.034-0.677 1997MNRAS.289..203C). The brighter of the two features in this 15.034-0.677 source was observed in the survey cubes to be stronger than any 15.034-0.677 previous observations with a peak flux density of 51.6Jy. The 15.034-0.677 weaker of the two features has remained constant at ~10Jy. 15.607-0.255 This source was originally observed at 0.85Jy, but faded to 0.4Jy 15.607-0.255 in an MX taken in 2008 March and then was not detectable 15.607-0.255 (<0.2Jy) in the MX taken in 2008 August. It was, however, 15.607-0.255 detected again in 2008 October with the ATCA (with a peak flux 15.607-0.255 density of 0.4Jy). 16.302-0.196 The velocity range of emission is nominally 46.9 to 53.6km/s, but 16.302-0.196 there is a weak spectral feature at ~41km/s in one MX, which was 16.302-0.196 not seen in the original survey cube observation, or the ATCA 16.302-0.196 observation. 16.585-0.051 The 59km/s feature of this source was seen to be steadily 16.585-0.051 decreasing in flux density over a period of 6 months by Caswell 16.585-0.051 et al. (1995MNRAS.272...96C). We find this feature is marginally 16.585-0.051 weaker at 18Jy (compared to ~20Jy in Caswell et al.). The 16.585-0.051 feature at 64km/s has remained stable at ~15Jy, but the 62km/s 16.585-0.051 feature has significantly increased from 18 to 37Jy. In the 16.585-0.051 current observations we do not detect (<0.15Jy) the two weak 16.585-0.051 features at 52.8 and 54.2km/s seen by Caswell et al., instead 16.585-0.051 finding a range of emission from 56.5 to 69.5km/s. However for 16.585-0.051 completeness we list the full velocity range in catalog.dat. 16.864-2.159 and 17.021-2.403. Both these sources lie outside the latitude 16.864-2.159 range of the MMB survey, but were re-observed with MX 16.864-2.159 observations for completeness. 16.864-2.159 was originally 16.864-2.159 discovered by Caswell et al. (1995MNRAS.272...96C) in a targeted 16.864-2.159 search towards OH masers and has since been observed by Walsh et 16.864-2.159 al. (1997MNRAS.291..261W, 1998MNRAS.301..640W,) and Szymczak et 16.864-2.159 al. (2000A&AS..143..269S). Its spectrum has not changed over the 16.864-2.159 >10yr period of these observations and our own. 17.021-2.403 was 16.864-2.159 discovered by Szymczak et al. (2000A&AS..143..269S) in a 16.864-2.159 targeted search of IRAS sources and our observations expand the 16.864-2.159 velocity range of the source with the detection of a weak (<1Jy) 16.864-2.159 feature at 18km/s. The feature at 21km/s has also increased 16.864-2.159 significantly from the original observation of ~1Jy to 4Jy. 17.021-2.403 See note on 16.864-2.159 16.976-0.005 This is a new weak source with a peak flux density 16.976-0.005 of 0.7Jy at 6.6km/s. 17.638+0.157 This source was discovered in 1991 by MacLeod & Gaylard 17.638+0.157 (1992MNRAS.256..519M) with a peak flux density of 25Jy at 17.638+0.157 21km/s. It was observed again in 1992 by Caswell et al. 17.638+0.157 (1995MNRAS.272...96C) with a flux density of 25Jy and in 1999 by 17.638+0.157 Szymczak et al. (2000A&AS..143..269S) with a reduced flux 17.638+0.157 density of 20Jy. A position was determined with the ATCA in 2003 17.638+0.157 (Caswell, 2009PASA...26..454C), finding a significantly further 17.638+0.157 reduced flux density of 9.5Jy. Our survey cube observations in 17.638+0.157 2007 August found an increase again with a peak flux density of 17.638+0.157 35Jy. The MX in 2009 March recorded a peak flux density 17.638+0.157 comparable to the original value of 25Jy. 18.073+0.077 This source contains two bright features separated by 18.073+0.077 approximately 6km/s. 18.159+0.094 The relative intensity of the two strong features at 58 to 59km/s 18.159+0.094 has varied, with the 58.4km/s feature remaining relatively 18.159+0.094 constant at ~8.5Jy, but the feature at 59km/s decreasing from 18.159+0.094 10.3Jy in the survey cube (2007 August) to just shy of 2Jy in 18.159+0.094 the MX (2009 March). In addition to the major features, the MX 18.159+0.094 detected a small feature (~1Jy) at 54.5km/s, which was only 18.159+0.094 marginally detected at 0.7Jy in the survey cube and not detected 18.159+0.094 in the ATCA observations. 18.440+0.045 This source has noticeable changes in its structure with the peak 18.440+0.045 moving from ~58km/s (2007 August) to ~62km/s (2008 August) and 18.440+0.045 a new feature appearing at ~60km/s. The feature at 49km/s is a 18.440+0.045 sidelobe of 18.460-0.004. 18.661+0.034 and 18.667+0.025. These are a closely spaced pair of sources, 18.661+0.034 previously listed as one known site, but now distinguished as 18.661+0.034 two sites. 18.661+0.034 extends to the higher velocities. 18.661+0.034 18.667+0.025 is mainly the features at 77km/s and 80.5km/s and 18.661+0.034 is associated with an Extended Green Object (Cyganowski et al. 18.661+0.034 2009ApJ...702.1615C). 18.667+0.025 See note on 18.661+0.034 18.735-0.227 and 18.733-0.224. These sources are a closely spaced pair of new 18.735-0.227 detections. The bright peak feature at 38km/s belongs to 18.735-0.227 18.735-0.227, but the other three peaks are 18.733-0.224. 18.733-0.224 See note on 18.735-0.227 18.888-0.475 This new source was also recently detected by Cyganowski et al. 18.888-0.475 (2009ApJ...702.1615C) associated with an Extended Green Object. 19.009-0.029 This new source was also recently detected by Ellingsen 19.009-0.029 (2007MNRAS.377..571E), listed as 18.99-0.04. It was seen offset 19.009-0.029 from a GLIMPSE source by 1.5 arcmin and is unlikely to be 19.009-0.029 physically associated. 19.249+0.267 This source does not include the feature seen at 25km/s which is 19.249+0.267 a sidelobe of 19.365-0.030. 19.472+0.170n , 19.472+0.170 and 19.486+0.151. Two sources separated by less 19.472+0.170n than 4 arcsec are distinguished by an 'n' identifying the source 19.472+0.170n with the more northerly declination (previously the southern 19.472+0.170n site was instead identified with an 'sw' e.g. Caswell 19.472+0.170n 2009PASA...26..454C, but we adopt an 'n' in accordance with the 19.472+0.170n Galactic Centre region results of Caswell et al. 19.472+0.170n 2010MNRAS.404.1029C). The northern site contains the features 19.472+0.170n at 18.5, 22 and 23km/s and the southern site the features 19.472+0.170n between 13 and 16km/s. 19.486+0.151 comprises the other features 19.472+0.170n at 20.5km/s, 24km/s and beyond to higher velocities. 19.472+0.170 See note on 19.472+0.170n 19.486+0.151 See note on 19.472+0.170n 19.609-0.234 This source consists of two main features, one at 36km/s and one 19.609-0.234 at 40km/s. The 36km/s feature had been the strongest feature, at 19.609-0.234 0.4Jy, in the 1992 discovery spectrum (Caswell et al. 19.609-0.234 1995PASA...12...37C). However, this feature was a marginal 19.609-0.234 detection in the survey cube data (2007 August). Fortunately, 19.609-0.234 the weak feature of 0.25Jy at 40km/s in 1992 flared to 1Jy in 19.609-0.234 the survey cube, allowing an ATCA position measurement in 2007 19.609-0.234 July (0.4Jy peak). The 36km/s feature rose to 0.5Jy in an MX in 19.609-0.234 2008 March, but was undetectable in an MX in 2009 March. The 19.609-0.234 40km/s feature had a peak flux density of 0.65Jy in the MX 19.609-0.234 measurement of 2009 March (and is shown in Fig. 1). Kolpak et 19.609-0.234 al. (2003ApJ...582..756K), Anderson & Bania 19.609-0.234 (2009ApJ...690..706A) and Roman-Duval et al. 19.609-0.234 (2009ApJ...699.1153R) ascribe this source to a far kinematic 19.609-0.234 distance based on an absence of HI self-absorption, whilst 19.609-0.234 Downes et al. (1980A&AS...40..379D) ascribe it to a near 19.609-0.234 kinematic distance based on an absence of formaldehyde 19.609-0.234 absorption. 19.612-0.120 and 19.612-0.134. As identified by Walsh et al. 19.612-0.120 (1998MNRAS.301..640W), in addition to the main source 19.612-0.120 19.612-0.120 which has several features between 49 and 61km/s, 19.612-0.120 there is a narrow offset source peaking at 52-53km/s. Both 19.612-0.120 Kolpak et al. (2003ApJ...582..756K) and Anderson & Bania 19.612-0.120 (2009ApJ...690..706A) ascribe the associated HII region to a far 19.612-0.120 kinematic distance based on HI absorption and HI 19.612-0.120 self-absorption, in contrast to Downes et al. 19.612-0.120 (1980A&AS...40..379D), who ascribe it to a near kinematic 19.612-0.120 distance based on the absence of formaldehyde absorption. 19.612-0.134 see note on 19.612-0.120. 19.667+0.114 This source peaked in emission at 16.3km/s in the survey cube 19.667+0.114 observation, but peaked at 14.2km/s in the MX observation, with 19.667+0.114 the 14km/s feature doubling in strength from the MX observation 19.667+0.114 from 1.1 to 2.2Jy. The features on either side of the 16.3km/s 19.667+0.114 feature have also increased considerably in flux density (whilst 19.667+0.114 the original 16.3km/s feature has remained approximately the 19.667+0.114 same). 19.884-0.534 This source has been identified as a far-side object from the 19.884-0.534 presence of formaldehyde absorption (at a level of 7{sigma}) by 19.884-0.534 Sewilo et al. (2004ApJS..154..553S). In contrast Roman-Duval et 19.884-0.534 al. (2009ApJ...699.1153R) identify it as a near-side object 19.884-0.534 based on the 'on-off' HI self-absorption technique, as do 19.884-0.534 Solomon et al. (1987ApJ...319..730S) based on a linewidth to 19.884-0.534 distance relation. 330.070+1.064 This site has one of the widest known velocity ranges, -56 to 330.070+1.064 -35km/s, slightly larger than previously tabulated (Caswell, 330.070+1.064 2009PASA...26..454C) on account of a prominent new feature near 330.070+1.064 -35.5km/s. Other features have also been highly variable, with 330.070+1.064 the current peak of 8.6Jy lying in a blend of several close 330.070+1.064 features near -41.5km/s. We note, from catalog.dat, that between 330.070+1.064 our survey epoch (2006 January) and MX follow-up (2008 March), 330.070+1.064 there was a small velocity change in the peak. No peak near 330.070+1.064 -41.5km/s was present in 1999 (Caswell, 2009PASA...26..454C), 330.070+1.064 when the peak, of 8Jy, was near -39km/s (a velocity with no 330.070+1.064 emission above 3Jy in the 2008 March spectrum of Fig. 1). 330.226+0.290 This new source is one of the most variable, with the survey 330.226+0.290 peak, of 1.87Jy at -75.4km/s (2006 January) decreasing to 330.226+0.290 0.4Jy at the MX follow-up epoch (2008 August); a secondary 330.226+0.290 feature near -90.5km/s remained with peak near 1Jy at both 330.226+0.290 epochs. 330.878-0.367 and 330.875-0.383. Both of these two weak masers, separated by 330.878-0.367 about 30 arcsec, are previously known, and straddle a broad 330.878-0.367 absorption dip. 330.878-0.367 is confined to a small velocity 330.878-0.367 range, -60 to -58km/s, and is currently slightly stronger than 330.878-0.367 at the earlier epochs 1992 June and 1997 May (Caswell, 330.878-0.367 2009PASA...26..454C). It is associated with masers of both OH 330.878-0.367 (one of the strongest known 1665-MHz OH masers) and water. 330.878-0.367 330.875-0.383 at the earlier epochs was stronger and extended 330.878-0.367 from -73.5 to -55.5km/s, but is currently weak with a single 330.878-0.367 peak of 0.25Jy at -69.8km/s. A single spectrum is shown centred 330.878-0.367 at the weaker site 330.875-0.383. 330.875-0.383 See note on 330.878-0.367 330.953-0.182 This known source has been very stable since 1992. It originally 330.953-0.182 appeared to have only an OH 6035-MHz counterpart, but recent OH 330.953-0.182 mapping (Caswell et al. 2010MNRAS.402.2649C) shows that 330.953-0.182 there is also a coincident weak corresponding OH 1665-MHz maser, 330.953-0.182 one of several in a compact cluster. 330.998+0.093 This weak new single feature source decreased from a peak of 330.998+0.093 1.46Jy at the survey epoch to 0.7Jy at the MX epoch 330.998+0.093 (2008 August). 331.120-0.118 Between the survey and MX epochs, the peak near -93.1km/s was 331.120-0.118 stable at 2.5Jy, but the secondary feature near -91.5km/s 331.120-0.118 approximately halved in intensity. Both peaks were previously 331.120-0.118 stronger (9.4 and 6Jy) as reported by Caswell 331.120-0.118 (1996MNRAS.279...79C, 2009PASA...26..454C). 331.132-0.244 The features between -92 and -90km/s have been highly variable, 331.132-0.244 with the peak in 1992 which was 27Jy now fallen to less than 331.132-0.244 2Jy; peaks in the currently stronger emission between -87 and 331.132-0.244 -84km/s have varied between 41 and 20Jy, with comparable 331.132-0.244 variability between the survey and MX epochs. Goedhart et al. 331.132-0.244 (2004MNRAS.355..553G, Goedhart et al. 2008, ASP Conf. Ser. 377, 331.132-0.244 124) monitored the spectrum at close time intervals over 3000d 331.132-0.244 and clearly show that the variability has a periodicity of 504d. 331.278-0.188 Past variations show a fall from a peak of 190Jy (1992) to 90Jy 331.278-0.188 (MX of 2008), while some subsidiary features have become 331.278-0.188 stronger, such as the 60-Jy feature at -85km/s which was never 331.278-0.188 previously observed to be greater than 40Jy. 331.342-0.346 The velocity range -77 to -63km/s is larger than formerly 331.342-0.346 realized (Caswell, 2009PASA...26..454C) with the detection of 331.342-0.346 weak, 0.3Jy, features between -77 and -70km/s. Intensity 331.342-0.346 variations in the current peak at -65.0km/s have been the most 331.342-0.346 striking, ranging from 124Jy (current survey 2006) to 30Jy in 331.342-0.346 1999 (from data used in position measurements by Caswell, 331.342-0.346 2009PASA...26..454C), whereas emission at -67.4km/s has been 331.342-0.346 more stable. 331.542-0.066 and 331.543-0.066. Evidence for these as two distinct sites with 331.542-0.066 separation 3 arcsec is given by Caswell (2009PASA...26..454C). 331.542-0.066 The emission has been quite stable since 1992. The velocity 331.542-0.066 ranges of the two sites are seen from ATCA observations to not 331.542-0.066 overlap, and we use a single spectrum to display both sites. 331.542-0.066 Note that a weak apparent feature near -97km/s is a sidelobe 331.542-0.066 response to 331.556-0.121. 331.543-0.066 See note on 331.542-0.066 331.556-0.121 Features remain persistent between 1992 and 2008, but variability 331.556-0.121 by a factor of 2 has occurred (compare with spectrum shown by 331.556-0.121 Caswell et al. 1995MNRAS.272...96C). 332.295-0.094 and 332.296-0.094. The first of these is a known source and the 332.295-0.094 second a distinct weak newly discovered site. Considerable 332.295-0.094 variability has occurred: the survey peak of 8Jy at -47.1km/s 332.295-0.094 (also the velocity of strongest emission more than 10yr earlier 332.295-0.094 Caswell, 2009PASA...26..454C) fell to 3Jy in the MX follow up of 332.295-0.094 2008 August, but peaks at other velocities increased. The second 332.295-0.094 site, 332.296-0.094 is confined to a feature at -46.6km/s, 332.295-0.094 clearly offset by nearly 3 arcsec in RA as revealed by ATCA 332.295-0.094 data, and with peak of 2.2Jy; on the Parkes spectra, it is 332.295-0.094 confused, although apparently with peak as high as 7Jy in the 332.295-0.094 survey spectrum, but only 2.2Jy in the MX spectrum, 332.295-0.094 as displayed. 332.296-0.094 See note on 332.295-0.094 332.295+2.280 This known source lies slightly outside the formal survey 332.295+2.280 Galactic latitude coverage, but new MX data were acquired to 332.295+2.280 enhance completeness of our catalogue. Spectra from 2008 August 332.295+2.280 and from 2009 March (displayed in Fig. 1) show a peak nearly 332.295+2.280 50 per cent stronger than in 1997 (Caswell, 2009PASA...26..454C) 332.295+2.280 but remain generally very similar. 332.351-0.436 The peak flux density has doubled since 2000 (Caswell, 332.351-0.436 2009PASA...26..454C) and new weak features at -46 and -43.5km/s 332.351-0.436 are now evident. 332.352-0.117 The weak 1-Jy feature seen at -41.8km/s in 1995 (Caswell, 332.352-0.117 2009PASA...26..454C) is now 5 times stronger. A feature near 332.352-0.117 -56km/s (not seen in 1995) was 4Jy in the survey, falling to 1Jy 332.352-0.117 in the MX follow-up of 2008 August. 332.560-0.148 The strongest peak in 1996 (Caswell, 2009PASA...26..454C), of 332.560-0.148 5.1Jy at -55.6km/s, had dropped to 3Jy in the survey and below 332.560-0.148 1Jy in the MX spectra (shown) of 2008 August; maximum emission 332.560-0.148 is now at -54.9km/s. 332.604-0.168 The single peak of 6.8Jy at -50.9km/s observed in 1996 (Caswell, 332.604-0.168 2009PASA...26..454C) has now dropped below 0.4Jy, but our 332.604-0.168 high-sensitivity spectrum of 2008 August shows additional weak 332.604-0.168 features extending to -42km/s. Very weak features near -55km/s 332.604-0.168 seen in the spectrum of Fig. 1 are not from this source but from 332.604-0.168 the nearby source 332.560-0.148, as is evident from the 332.604-0.168 alignment of the spectra from the two sites in Fig. 1. 332.701-0.588 This known source has a single feature which has fallen from 332.701-0.588 2.1Jy (1999) to 1.2Jy (survey) and only 0.45Jy in the MX of 2008 332.701-0.588 August. Apparent features at -56km/s (and more negative 332.701-0.588 velocities) are from 332.726-0.621. 332.726-0.621 Most emission from this source has remained readily detectable 332.726-0.621 since 1992, but a brief flare of 2.7Jy occurred at -49.5km/s in 332.726-0.621 1999 May (Caswell, 2009PASA...26..454C) and seen at no other 332.726-0.621 epoch. Although the strongest peak remained stable between the 332.726-0.621 survey and MX follow-up of 2008 August, variations exceeding a 332.726-0.621 factor of two were seen from many features. 332.813-0.701 A newly discovered source in which some features faded to nearly 332.813-0.701 half intensity between the survey (2006) and the MX (2008) 332.813-0.701 observations. Note that negative features on the displayed 332.813-0.701 spectrum between -49 and -45km/s are responses to 332.963-0.679 332.813-0.701 in the reference spectrum. 332.942-0.686 and 332.963-0.679. These closely spaced sites (separation 332.942-0.686 81 arcsec) are displayed on a single spectrum at a slightly 332.942-0.686 offset position and thus showing peaks lower than the listed 332.942-0.686 values of catalog.dat. 332.963-0.679 is strongest, with peak 332.942-0.686 sometimes exceeding 60Jy at -45.9 (e.g. our survey spectrum) and 332.942-0.686 never below 25Jy. Its velocity range extends to -38km/s where 332.942-0.686 there are weak features with peaks of up to 1Jy. Weak features, 332.942-0.686 up to 5Jy, are also present extending to -54km/s, but 332.942-0.686 overlapping with features of 332.942-0.686. 332.942-0.686 has a 332.942-0.686 clearly defined feature at -55.5km/s(1Jy MX and 2Jy survey) and 332.942-0.686 contributes to blended features in the velocity range -55 to 332.942-0.686 -51.5km/s, with peaks of approximately 2Jy at both the MX epoch 332.942-0.686 and survey cube epochs, but formerly 10.3Jy at -52.8km/s and 332.942-0.686 8Jy at -54km/s in 2000 March. 332.963-0.679 See note on 332.942-0.686 332.975+0.773 This is a new discovery, with a persistent feature at -51km/s 332.975+0.773 with peak of 1.4Jy present at both the survey epoch and the 332.975+0.773 follow-up MX epoch of 2008 August. At the survey epoch, an 332.975+0.773 additional 1.7-Jy feature at -43.5km/s was strongest but not 332.975+0.773 seen in the later MX spectrum, and the MX spectrum shows a 332.975+0.773 0.6-Jy feature at -55km/s that was not evident on the survey 332.975+0.773 spectrum with its higher noise level. 333.109-0.500 A new source which was stronger in the initial survey 333.109-0.500 observations, with peak of 5Jy at -60.9km/s decreasing to 2.1Jy 333.109-0.500 in the MX spectrum of 2008 August. Weak apparent emission at 333.109-0.500 -54.5km/s is a sidelobe response to the stronger site at 333.109-0.500 333.068-0.447 (the spectra are aligned in Fig. 1 of Paper III 333.109-0.500 (Casweel et al., 2011MNRAS.417.1964C) to demonstrate this). 333.121-0.434 A single spectrum is used to display this known source and the 333.121-0.434 following three sources that lie nearby. 333.121-0.434 accounts 333.121-0.434 for the strongest peak on the spectrum shown, 17.5Jy at 333.121-0.434 -48.4km/s, a velocity that showed a peak of only 4Jy in 1993 333.121-0.434 (Caswell, 1997MNRAS.289..203C) but flared to 54Jy in our survey 333.121-0.434 spectrum of 2006; adjacent features at -49.3 and -50.0km/s 333.121-0.434 showed peaks of 18 and 16Jy in 1993 but are currently 8Jy or 333.121-0.434 weaker. 333.126-0.440 and 333.128-0.440. These known sources are separated by 7 arcsec, 333.126-0.440 and are at similar velocity, but are clearly distinguished in 333.126-0.440 the ATCA spectra of 1993 (Caswell, 1997MNRAS.289..203C). Our 333.126-0.440 spectrum displaying their current features is shared with the 333.126-0.440 previous and following source. Compared with the 1993 333.126-0.440 measurements, our current Parkes spectrum shows no evidence for 333.126-0.440 change in 333.126-0.440 and 333.128-0.440, when allowance is 333.126-0.440 made for the blending within the Parkes 3.2 arcmin beam. 333.126-0.440 333.128-0.440 is seen as a distinct weak feature of 1Jy at 333.126-0.440 -45.8km/s, but also includes a stronger feature at -44.5km/s 333.126-0.440 which was 3.5Jy in 1993 November, and remains near this value, 333.126-0.440 but is masked by comparable emission from 333.126-0.440; 333.126-0.440 333.126-0.440 comprises a blended feature of about 4Jy at 333.126-0.440 -43.9km/s and a distinct 1.9Jy feature at -42.5km/s. 333.128-0.440 See note on 333.126-0.440 333.135-0.431 The previous listing of this known weak source was given a suffix 333.135-0.431 's' to distinguish it from OH, offset by 2.4 arcsec (Caswell, 333.135-0.431 1997MNRAS.289..203C); it remains weak, accounting only for the 333.135-0.431 1-Jy feature near -52.5km/s, barely detectable on the spectrum 333.135-0.431 showing also the previous three sources. 333.128-0.560 and 333.130-0.560. The single spectrum showing the blended 333.128-0.560 features from these two close sources (separated by 6 arcsec) is 333.128-0.560 similar to that from 2000 March (Caswell, 2009PASA...26..454C); 333.128-0.560 the ATCA observations in 2000 reveal that the major feature at 333.128-0.560 -56.8km/s arises from 333.130-0.560, and is now stronger than 333.128-0.560 its previous peak of 17Jy; emission from -65 to -61km/s is also 333.128-0.560 from here. The 9-Jy feature at -52.7km/s and lesser feature at 333.128-0.560 -60.5km/s arise from 333.128-0.560; these features are somewhat 333.128-0.560 weaker in the MX spectrum of 2008 August than at epoch 2000 333.128-0.560 (peak of 14.5Jy), but stronger (peak of 18Jy) at the survey 333.128-0.560 epoch. 333.130-0.560 See note on 333.128-0.560 333.163-0.101 and 333.184-0.091. These known sites are separated by 1.4 arcmin. 333.163-0.101 Accordingly, the aligned spectra (recorded with 3.2 arcmin 333.163-0.101 half-power beamwidth) each show emission of about half intensity 333.163-0.101 from the other source. Compared to the 1992 spectra shown by 333.163-0.101 Caswell et al. (1995MNRAS.272...96C), the only notable change is 333.163-0.101 the current undetectability of emission near -91.5km/s, which 333.163-0.101 defines the high end of the velocity range for 333.163-0.101. 333.184-0.091 See note on 333.163-0.101 333.234-0.062 and 333.234-0.060. 333.234-0.062 was recognized as highly 333.234-0.062 variable in early observations (Caswell et al. 333.234-0.062 1995MNRAS.272...96C), and its significant offset of several 333.234-0.062 arcsec from a nearby OH maser was noted by Caswell 333.234-0.062 (1996MNRAS.279...79C, 1998MNRAS.297..215C). Its current peak of 333.234-0.062 1.3Jy at -91.9km/s is slightly lower than the 1.9Jy value in 333.234-0.062 1994; prominent features near -81km/s exceeding 3Jy in 1992 have 333.234-0.062 now fallen to 0.5Jy. New ATCA observations 2006 April showed 333.234-0.062 that in addition to this methanol maser, there is a new 1-Jy 333.234-0.062 feature present at -85.3km/s (and weaker feature near -87km/s) 333.234-0.062 offset from 333.234-0.062 by 5.3 arcsec (to smaller RA by 0.37s 333.234-0.062 and north by 4.0 arcsec), which is a new distinct methanol maser 333.234-0.062 site that we distinguish as 333.234-0.060 in the present listing 333.234-0.062 (with velocity range -88 to -85km/s). It corresponds well with 333.234-0.062 the OH maser at this position (Caswell, 1998MNRAS.297..215C). 333.234-0.062 All methanol features are clearly seen on the MX spectrum of the 333.234-0.062 two blended sites shown in Fig. 1 of Paper III (Caswell et al., 333.234-0.062 2011MNRAS.417.1964C). 333.234-0.060 See note on 333.234-0.062 333.315+0.105 Variability was slight between the survey and MX epochs, but many 333.315+0.105 peaks have more than doubled in intensity since 1994 (Caswell, 333.315+0.105 1996MNRAS.279...79C); the currently strongest feature of 18Jy 333.315+0.105 was only 3Jy in 1994. 333.646+0.058 Peaks have increased by more than a factor of 3 since 1994 333.646+0.058 (Caswell, 1996MNRAS.279...79C). 334.635-0.015 Factor of 2 intensity variations have occurred since 1994 334.635-0.015 (Caswell, 1996MNRAS.279...79C) and between survey cube and MX 334.635-0.015 (2008 August) epochs. 334.933-0.307 A new maser showing variations exceeding a factor of 2 between 334.933-0.307 the survey and MX epoch (2008 August). Both the survey cube 334.933-0.307 spectrum and MX spectrum are displayed as a typical example of 334.933-0.307 the variability sometimes seen, and also demonstrating the 334.933-0.307 improved noise level of the MX spectra resulting from its 334.933-0.307 longer integration time. 335.060-0.427 Highly variable features include one at -31.1km/s which was less 335.060-0.427 than 1Jy in 1997; it flared to 78Jy at the survey epoch and 335.060-0.427 decayed to 37Jy at the MX epoch (2008 August). The total 335.060-0.427 velocity range has remained large and stable, from -48 to 335.060-0.427 -25km/s. 335.426-0.240 One of the two strongest newly reported masers, it has remained 335.426-0.240 relatively stable between the survey and MX follow-up. Weak 335.426-0.240 features, of 0.5Jy at the MX epoch (2008 August) and slightly 335.426-0.240 stronger at the survey epoch, are present near -31.5km/s, and 335.426-0.240 stronger emission near -41km/s. Consequently the total velocity 335.426-0.240 range is very large, from -53 to -31km/s. As noted by Caswell 335.426-0.240 (2009PASA...26..454C), a sidelobe of this source accounts for a 335.426-0.240 spurious entry, 335.603-0.078, listed by Caswell 335.426-0.240 (1996MNRAS.279...79C). 335.585-0.289 , 335.585-0.290 and 335.585-0.285. The small separations between 335.585-0.289 the three sites are readily distinguished in ATCA spectra from 335.585-0.289 1994 (Caswell, 1996MNRAS.279...79C), but too small to 335.585-0.289 distinguish in Parkes spectra, the first of which dates from 335.585-0.289 1992 (Caswell et al. 1995MNRAS.272...96C). All features seen in 335.585-0.289 1994 have corresponding features in our current survey and 335.585-0.289 follow-up spectra. Caswell (2009PASA...26..454C) concludes that 335.585-0.289 the first two sites are distinct, despite their small separation 335.585-0.289 of only 3 arcsec. 335.585-0.289 accounts for features between 335.585-0.289 -56 and -50km/s; the strongest peak is currently almost twice as 335.585-0.289 strong as in 1994. 335.585-0.290 accounts for features between 335.585-0.289 -48 and -45km/s; the strongest peak is currently less than 335.585-0.289 one-third its intensity in 1994. The third site is offset 335.585-0.289 approximately 15 arcsec and accounts for two groups of features, 335.585-0.289 between -51 and -48km/s and between -45 and -43km/s; some of its 335.585-0.289 emission varies in amplitude by factors of 2, with 2 features 335.585-0.289 clearly decreasing and 2 features increasing. We display a 335.585-0.289 single spectrum encompassing all three sites. 335.585-0.290 See note on 335.585-0.289 335.585-0.285 See note on 335.585-0.289 335.726+0.191 Emission from this site remains similar to 1992, with variations 335.726+0.191 typically less than a factor of two. Features are present over 335.726+0.191 the range -55 to -43.5km/s, but sidelobes from 335.789+0.174 are 335.726+0.191 likely to account for most of the weak apparent emission between 335.726+0.191 -52 and -45km/s. Spectra of the two sites are aligned to 335.726+0.191 demonstrate this. 335.789+0.174 Variations since 1992 are mostly less than a factor of two, but 335.789+0.174 weak emission formerly extended to -59km/s (Caswell et al. 335.789+0.174 1995MNRAS.272...96C) whereas it currently extends only to 335.789+0.174 -57km/s. 335.824-0.177 The spectrum from the MX follow-up was taken at a position offset 335.824-0.177 by 48 arcsec from the subsequently determined position for this 335.824-0.177 new source; the tabulated flux density has been corrected 335.824-0.177 for this. 336.018-0.827 Spectra since 1997 (Caswell, 2009PASA...26..454C) have shown all 336.018-0.827 features to have been quite stable, with the exception of the 336.018-0.827 strongest at velocity -53.4km/s, which has varied from 300Jy in 336.018-0.827 1997 to slightly less than 180Jy at the survey epoch and 90Jy 336.018-0.827 at the MX epoch of 2008 August. 336.409-0.257 and 336.433-0.262. These are known sources, with separation 336.409-0.257 88 arcsec. The spectra are shown aligned so as to reveal the 336.409-0.257 blending of the offset source at each position. 336.409-0.257 is 336.409-0.257 confined to the velocity range -87 to -84km/s, with very little 336.409-0.257 change since 1996, and a peak, still, of nearly 7Jy. 336.409-0.257 336.433-0.262 spans velocities -95 to -86km/s and its major peak 336.409-0.257 has dropped from 46Jy to a current value of 25Jy. 336.433-0.262 see Note on 336.409-0.257. 336.526-0.156 The peak flux density of catalog.dat has been corrected (by a 336.526-0.156 factor of 1.2) for a 46 arcsec offset of the displayed spectrum 336.526-0.156 from the true position. The apparent absorption at -93km/s is 336.526-0.156 spurious and caused by 336.433-0.262 near one of the reference 336.526-0.156 positions. 336.809+0.119 and 336.825+0.139. Two new sources separated by 93 arcsec. The 336.809+0.119 spectra are aligned to reveal the weak response to the offset 336.809+0.119 source at each site. 336.809+0.119 comprises many overlapping 336.809+0.119 features between -86 and -80km/s. The MX peak was slightly 336.809+0.119 weaker at the survey epoch, and another peak of comparable 336.809+0.119 intensity was strongest. 336.825+0.139 shows emission primarily 336.809+0.119 from two peaks in the velocity range -90 to -86.5km/s, of which 336.809+0.119 the stronger nearly halved between survey and MX epoch; 336.809+0.119 comparison of the aligned spectra shows that weak emission at 336.809+0.119 -78.5km/s is also from this position rather than 336.809+0.119. 336.825+0.139 See note on 336.809+0.119 336.822+0.028 The apparent peak at -76.1km/s is a sidelobe of strong emission 336.822+0.028 from 336.864+0.005, as is the weak feature at -79.0km/s 336.822+0.028 (compare aligned spectra). 336.864+0.005 and 336.881+0.008. Some features of 336.864+0.005 have changed by 336.864+0.005 more than a factor of 2 since 1992. All features seen on the 336.864+0.005 displayed spectrum are from this source except for the feature 336.864+0.005 at -68.1km/s, which arises from a previously uncatalogued site, 336.864+0.005 336.881+0.008 for which no separate spectrum is shown. Its 336.864+0.005 offset from 336.864+0.005 is 62 arcsec and its peak of 336.864+0.005 catalog.dat (2.6Jy) has been accordingly increased from the 336.864+0.005 apparent peak in the displayed spectrum (2.1Jy). 336.881+0.008 See note on 336.864+0.005 336.941-0.156 The spectra of this source have remained generally similar from 336.941-0.156 1996 until the present. A weak sidelobe from 336.983-0.183 is 336.941-0.156 responsible for emission at velocity -80.6km/s (see aligned 336.941-0.156 spectra). 336.957-0.225 A new source with 1.5-Jy peak at -68.1km/s and a total velocity 336.957-0.225 range from -68.5 to -65.5km/s. The apparent emission outside 336.957-0.225 this range is a 10 per cent sidelobe response to 336.983-0.183, 336.957-0.225 as is clear from their aligned spectra. 336.983-0.183 The low noise of the present spectrum shows that the velocity 336.983-0.183 range is -90 to -75km/s, and some features have more than 336.983-0.183 doubled in intensity since 1996. Sidelobe emission from 336.983-0.183 336.941-0.156 is responsible for apparent features between -70 336.983-0.183 and -64km/s, but any sidelobe contribution in the velocity range 336.983-0.183 -79 to -76km/s is negligible (compare aligned spectra). 337.263-0.070 This weak new source is a single feature at essentially the same 337.263-0.070 velocity as the strong 77-Jy peak of 337.404-0.402. Their 337.263-0.070 separation is 21.6 arcmin, and close inspection of Parkes data 337.263-0.070 and ATCA data strongly support it as a real source rather than a 337.263-0.070 sidelobe response. 337.517-0.348 The MX spectrum displayed for this new source was recorded at a 337.517-0.348 position offset from the correct value by 92 arcsec, and the 337.517-0.348 peak intensity of 1.5Jy listed in catalog.dat has been corrected 337.517-0.348 for this. 337.613-0.060 and 337.632-0.079. These known sources have a separation of 337.613-0.060 96 arcsec, so for Parkes spectra, each is near the halfpower 337.613-0.060 point of the other, as evident from the aligned spectra; see 337.613-0.060 also Caswell et al. (1995MNRAS.272...96C). We list in 337.613-0.060 catalog.dat velocity ranges of -54 to -38km/s for 337.613-0.060 337.613-0.060 and -64 to -54km/s for 337.632-0.079, but the latter possibly 337.613-0.060 has weak emission extending to -48km/s where it would be mostly 337.613-0.060 masked by the stronger emission from 337.613-0.060. 337.613-0.060 337.613-0.060 has shown little change since 1992, and likewise 337.613-0.060 for features of 337.632-0.079 at most velocities, with an 337.613-0.060 exception at -56.5km/s which has increased by more than 50 per 337.613-0.060 cent since 1992. 337.632-0.079 See note on 337.613-0.060 337.686+0.137 The current peak is only one-third the intensity recorded in 1996 337.703-0.053 and 337.705-0.053. These known sources are little more than 337.703-0.053 8 arcsec apart (Caswell, 2009PASA...26..454C) and are displayed 337.703-0.053 on a single spectrum; there is a small overlap in velocity 337.703-0.053 ranges as noted in catalog.dat. The spectrum remains similar to 337.703-0.053 its appearance in 1992. There is an associated OH maser at 337.703-0.053 1665-, 1667- and 6035-MHz transitions, and an ultracompact HII 337.703-0.053 region coincident with the stronger methanol site, 337.705-0.053 337.703-0.053 (Caswell, 1997MNRAS.289..203C). The distance to the site was 337.703-0.053 suggested as the 'far' kinematic distance of 12.1kpc by Fish et 337.703-0.053 al. (2003ApJ...587..701F), but the 'near' kinematic distance of 337.703-0.053 4.2kpc (3.6kpc after rescaling for a Galactic Centre distance of 337.703-0.053 8.5kpc) by Caswell (1997MNRAS.289..203C). Reconsideration of the 337.703-0.053 distance by Caswell, Kramer & Reynolds (2011MNRAS.415.3872C) 337.703-0.053 indicates a more likely distance of 7.9kpc, near the tangent 337.703-0.053 point of the 3-kpc ring, amongst a group of sources at this 337.703-0.053 location discussed in Section 4.6.1 and by 337.703-0.053 Green et al. (2011ApJ...733...27G). 337.705-0.053 See note on 337.703-0.053 337.710+0.089 and 337.720+0.065. The first of these is a known source (Caswell, 337.710+0.089 1996MNRAS.279...79C) with velocity range -79 to -72km/s. The new 337.710+0.089 source 337.720+0.065 is offset by 94 arcsec and the spectra are 337.710+0.089 aligned to show that each displays a 50 per cent response to the 337.710+0.089 other source. There is no velocity overlap of emission, with 337.710+0.089 337.720+0.065 accounting only for the weak features in the 337.710+0.089 range -66.5 to -63.5km/s. 337.720+0.065 See note on 337.710+0.089 337.920-0.456 Factors of two variations have occurred in some features since 337.920-0.456 1992; the velocity range remains -41 to -36km/s. 338.075+0.012 , 338.075+0.009 and 338.069+0.011. The first two of these are 338.075+0.012 9 arcsec apart (Caswell, 2009PASA...26..454C) and the third is a 338.075+0.012 weaker site offset 20 arcsec; all sources are displayed on a 338.075+0.012 single spectrum. The current spectrum is broadly similar to 338.075+0.012 1992, with the strongest feature of 338.075+0.012 at velocity 338.075+0.012 -43.9km/s showing little change, but a feature near -53km/s is 338.075+0.012 now at less than half of its former intensity; the weaker site 338.075+0.012 338.075+0.009 has changed only slightly. Velocity ranges are 338.075+0.012 -54.5 to -43.5km/s for 338.075+0.012 and -42.5 to -30km/s for 338.075+0.012 338.075+0.009; features at -39.1 and -40km/s (peak flux density 338.075+0.012 of 4.2 and 2.5Jy) arise from 338.069+0.011. 338.075+0.009 See note on 338.075+0.012 338.069+0.011 See note on 338.075+0.012 338.140+0.178 The major feature nearly doubled in amplitude between its 338.140+0.178 discovery in the survey and the follow-up MX; other features 338.140+0.178 have been more stable. 338.287+0.120 The strongest, 26Jy, current feature (at -40km/s) has shown an 338.287+0.120 increase from less than 5Jy in 1996, and a companion (at 338.287+0.120 adjacent velocity, -39.5km/s) feature has decreased by a 338.287+0.120 comparable factor. 338.325-0.409 The peak of 2.8Jy seen in the MX follow up (epoch 2008 August) at 338.325-0.409 -25.7km/s was a secondary feature of less than 1Jy at the survey 338.325-0.409 epoch (2006) and 1Jy at the ATCA epoch of 2006 December. 338.461-0.245 Most of the spectrum has remained similar from 1992 to the 338.461-0.245 present, but features near -63km/s have flared from a barely 338.461-0.245 detectable value of less than 0.2Jy to more than 5Jy. 338.472+0.289 Three weak features have persisted since 1992 until the present 338.472+0.289 (2008 August). Weak negative artefacts in the spectrum near -28 338.472+0.289 and -39km/s arise from sources 338.497+0.207 and 338.561+0.218 338.472+0.289 near the reference positions. 338.561+0.218 The spectrum has been stable since 1999 (Caswell, 338.561+0.218 2009PASA...26..454C) and the increased velocity range that we 338.561+0.218 list arises from the feature at -30.5km/s, which is weak and 338.561+0.218 below the coarse 2-Jy detection threshold of the 1999 338.561+0.218 observations. 338.566+0.110 A variable source, in which the current peak of 2.7Jy at 338.566+0.110 -74.7km/s has halved in intensity since 1996, and a feature at 338.566+0.110 -78.1km/s flared to 10Jy in the survey spectrum (2006 April), 338.566+0.110 but returned to 2.4Jy in the MX follow-up of 2008 August. 338.902+0.394 A weak source with multiple features over a large velocity range 338.902+0.394 from -36 to -19km/s. It possibly accounts for a source, 338.902+0.394 338.925+0.385, reported by Walsh et al. (1997MNRAS.291..261W) as 338.902+0.394 0.6Jy at -26km/s, but with no precise position, not mentioned 338.902+0.394 in subsequent publications, and not accounted for by any other 338.902+0.394 source in our survey. 338.920+0.550 and 338.925+0.557. The separation of these sites is approximately 338.920+0.550 30 arcsec. Both can be seen in the single spectrum from Parkes. 338.920+0.550 This overall spectrum remains similar to its appearance in 1992. 338.920+0.550 The stronger site, 338.920+0.550, (peak of nearly 80Jy at 338.920+0.550 -61.4km/s) accounts for most features and has a velocity range 338.920+0.550 from -68 to -59km/s. 338.925+0.557 had a peak near -62.4km/s of 338.920+0.550 5Jy in 1997, but this is blended in the spectrum displayed. 338.920+0.550 Features near -59 and -65.5km/s also belong to 338.925+0.557, 338.920+0.550 with total velocity range of -66 to -59km/s. 338.925+0.557 See note on 338.920+0.550 338.925+0.634 and 338.926+0.634. 338.925+0.634 is a new strong source with 338.925+0.634 velocity range from -62 to -52.0km/s, peak 64Jy at -60.9km/s. 338.925+0.634 Its companion, seen in the same Parkes spectrum, is offset by 338.925+0.634 6 arcsec (4 arcsec north and 4 arcsec later RA) and accounts for 338.925+0.634 two distinct emission features between -65.5 and -63.5km/s and 338.925+0.634 some emission between -63 and -59.5km/s, to give a total range 338.925+0.634 from at least -65.5 to -59.5km/s; a weak feature at -68km/s 338.925+0.634 extends this to -68.5km/s. In catalog.dat we list a reliably 338.925+0.634 measured peak of the secondary site as 3.8Jy for the feature at 338.925+0.634 -64.5km/s, although emission from this site near -61.5km/s, in a 338.925+0.634 more confused spectral region, probably contributes as much as 338.925+0.634 15Jy (half the blended intensity) but was difficult to measure 338.925+0.634 reliably. 338.926+0.634 See note on 338.925+0.634 338.935-0.062 This source has become twice as strong in 2008 as in 1992. Long 338.935-0.062 term monitoring over 3000d by Goedhart et al. 338.935-0.062 (2004MNRAS.355..553G, 2008) shows that the intensity of the 338.935-0.062 strongest 6.6-GHz maser feature near -42.0km/s varies with a 338.935-0.062 clear periodicity of 133.3d. Goedhart et al. (2008, ASP Conf. 338.935-0.062 Ser. 377, 124 also show that the solitary emission feature at 338.935-0.062 the 12.2-GHz methanol transition appears to vary in synchronism. 338.935-0.062 The 12.2-GHz feature has a peak at -42.2km/s, slightly differing 338.935-0.062 from the 6.6-GHz peak, of -41.9km/s according to our data. But 338.935-0.062 close inspection shows the 6.6-GHz spectra to be blends of a 338.935-0.062 feature centred at -41.9km/s and a slightly weaker one centred 338.935-0.062 close to -42.2km/s; the latter is the counterpart to the 338.935-0.062 12.2-GHz feature. We conclude that, most likely, the two 6.6-GHz 338.935-0.062 features and the 12.2-GHz feature all vary in synchronism. 338.935-0.062 Goedhart et al. (2004MNRAS.355..553G, Goedhart et al. 2008, ASP 338.935-0.062 Conf. Ser. 377, 124) also remark on a 6.6-GHz feature in their 338.935-0.062 spectrum at -41.4km/s that varies differently; as suspected by 338.935-0.062 Goedhart et al. (2008, ASP Conf. Ser. 377, 124), this feature 338.935-0.062 arises from a quite different maser site, which we clearly 338.935-0.062 identify as 338.875-0.084, offset from 338.935-0.062 by nearly 338.935-0.062 4 arcmin and thus near the half-power point of the 338.935-0.062 Hartebeesthoek beam when monitoring 338.935-0.062 at 6.6GHz. 339.053-0.315 At this site, strong emission between -114 and -111km/s was 339.053-0.315 discovered in 1996. The higher sensitivity present observations 339.053-0.315 now reveal weak emission extending to -124.5km/s, and a full 339.053-0.315 velocity range from -124.5 to -110km/s. 339.064+0.152 Clear intensity variations of nearly a factor of two have 339.064+0.152 occurred, with the peak seen in 1996 and at the survey epoch of 339.064+0.152 2006 reduced at the 2008 August epoch of the displayed MX 339.064+0.152 spectra. These changes result in the listing (in catalog.dat) 339.064+0.152 of the strongest peak at a different velocity between survey 339.064+0.152 cube and MX. 339.282+0.136 and 339.294+0.139. The separation of 45 arcsec is just enough to 339.282+0.136 distinguish the individual sources on the two single dish 339.282+0.136 spectra shown. The emission has remained similar to 1996 and we 339.282+0.136 slightly modify the velocity ranges determined by Caswell 339.282+0.136 (1996MNRAS.279...79C, 2009PASA...26..454C) to -76 to -66km/s for 339.282+0.136 339.294+0.139 (noting that the strongest feature at -74.6km/s is 339.282+0.136 now the strongest feature at either site), and to -72 to -69km/s 339.282+0.136 for the now weaker site 332.282+0.136 with strong peaks still 339.282+0.136 at -69.1 and -70.1km/s. 339.294+0.139 See note on 339.282+0.136 339.477+0.043 The low noise of the present observations reveals a wider 339.477+0.043 velocity range, from -21 to -5.5km/s, than seen in the 339.477+0.043 1996 spectrum. 339.582-0.127 and 339.622-0.121. The distinction between features of these 339.582-0.127 sources, separated nearly 2.5 arcmin, is clearly seen on the 339.582-0.127 ATCA spectrum of 1994 (Caswell, 1996MNRAS.279...79C). On the 339.582-0.127 Parkes spectra shown in Fig. 1, 339.622-0.121 is stronger and 339.582-0.127 confuses its weaker companion at some velocities, but the 339.582-0.127 alignment of the spectra reveals the distinctive main features 339.582-0.127 at each site. 339.622-0.121 has a full velocity range of -39.5 339.582-0.127 to -31.5km/s, with a peak of 90Jy at -32.8km/s, and is generally 339.582-0.127 similar to its appearance in 1996. 339.582-0.127 clearly 339.582-0.127 accounts for a 7-Jy peak at -31.3km/s, which remains similar to 339.582-0.127 the 1996 strongest feature, and a stronger 13-Jy peak at 339.582-0.127 -30.4km/s (only 4Jy in 1996); a weak 1-Jy feature at -38.8km/s 339.582-0.127 also arises from this site, giving a velocity range of -39 to 339.582-0.127 -29.5km/s. Variability of 339.622-0.121 has been monitored by 339.582-0.127 Goedhart et al. (2004MNRAS.355..553G, Goedhart et al. 2008, ASP 339.582-0.127 Conf. Ser. 377, 124). Several peaks clearly show correlated 339.582-0.127 variability with a periodicity of 202d. 339.622-0.121 See note on 339.582-0.127 339.681-1.208 and 339.682-1.207. Caswell (2009PASA...26..454C) suggested that a 339.622-0.121 separation slightly larger than 3 arcsec is a likely indication 339.622-0.121 of two separate sites and we retain that interpretation. We show 339.622-0.121 a single spectrum and, guided by the velocity ranges from 339.622-0.121 Caswell (2009PASA...26..454C), we adopt -41 to -20.5km/s for the 339.622-0.121 stronger site 339.681-1.208, with peak of 72Jy at -21.4km/s, and 339.622-0.121 -35.5 to -33km/s for 339.682-1.207 with a current peak of 23Jy 339.622-0.121 near -34.5km/s, somewhat stronger than in 1996 when the peak 339.622-0.121 was 5.8Jy. 339.682-1.207 See note on 339.622-0.121 339.884-1.259 Very strong emission extends from -40 to -32km/s, and weak 339.884-1.259 emission extending to -27.5 and -41km/s. There may be a marginal 339.884-1.259 detection of weak emission, less than 1Jy peak, in the 1992 339.884-1.259 spectrum, and near -45km/s in the current observations. 339.909+0.240 Values given in catalog.dat superficially indicate that the 339.909+0.240 intensity of this new, single feature, source halved between the 339.909+0.240 survey and MX epochs, but this is probably exaggerated by the 339.909+0.240 low signal-to-noise ratio. 339.949-0.539 and 339.980-0.538. These known sources are separated by 339.949-0.539 112 arcsec. We display spectra at both positions which clearly 339.949-0.539 show that most emission is from 339.949-0.539, with velocity 339.949-0.539 range -108.5 to -89.5km/s, and a single 8-Jy feature at 339.949-0.539 -89.3km/s is the only one definitely at 339.980-0.538. 339.980-0.538 See note on 339.949-0.539 339.986-0.425 One of the two strongest new sources, with a peak of 90Jy at 339.986-0.425 -89.5km/s. The two major peaks increased between the survey and 339.986-0.425 follow-up by less than a factor of 2, whereas the feature at 339.986-0.425 -85.5km/s increased from less than 10 to 40Jy. 340.054-0.244 The current peak of the spectrum, 48Jy at -59.7km/s, has shown 340.054-0.244 little change since 1992. However, a feature at -61km/s has 340.054-0.244 changed from 3Jy in 1992 to 6Jy at the survey epoch, and 13Jy at 340.054-0.244 the MX epoch of 2008 August. 340.518-0.152 and 340.543-0.162. 340.518-0.152 is a known source, relatively 340.518-0.152 stable from 2000 until the present, with a velocity range from 340.518-0.152 -50.5 to -43.5km/s. Its spectrum shows an apparent weak feature 340.518-0.152 at -51.7km/s but this arises from the newly discovered source 340.518-0.152 340.543-0.162, offset by nearly 2 arcmin. A separate spectrum of 340.518-0.152 the new source is shown aligned with 340.518-0.152, revealing 340.518-0.152 that, in addition to its peak of 1.1Jy at -51.7km/s, 340.518-0.152 340.543-0.162 also displays much weaker emission in the velocity 340.518-0.152 range -50 to -49km/s (where it is confused with 340.518-0.152), 340.518-0.152 and thus a full velocity range -52.5 to -49km/s. 340.543-0.162 See note on 340.518-0.152 340.785-0.096 This well-known source has several notable properties 340.785-0.096 (Caswell, 1997MNRAS.289..203C). In addition to being strong 340.785-0.096 (with peak exceeding 100Jy), it has one of the widest velocity 340.785-0.096 ranges (perhaps the widest) of any 6.6-GHz methanol maser, with 340.785-0.096 spot maps verifying that all emission arises within a small 340.785-0.096 area; and it has shown considerable variability since the early 340.785-0.096 excellent characterizing spectra of 1992. The current spectrum 340.785-0.096 shows a velocity range -111.5km/s to -85km/s, similar to, but 340.785-0.096 slightly larger than, the range seen in earlier spectra 340.785-0.096 (Caswell, 2009PASA...26..454C). The peak at -108.1km/s, 340.785-0.096 currently 125.8Jy, was less than 50Jy in the survey spectrum, 340.785-0.096 and only 11Jy in 1992, but at all observed epochs, there have 340.785-0.096 been peaks greater than 100Jy. Caswell (1997MNRAS.289..203C) 340.785-0.096 remarked that its high negative velocity is an indication of a 340.785-0.096 well defined large distance near the tangent point (heliocentric 340.785-0.096 distance 8kpc at this Galactic longitude). However, with 340.785-0.096 reference to Section 4.6 and Fig. 4, it seems likely to be 340.785-0.096 slightly closer than the tangent point, probably in the near 340.785-0.096 side of the Norma spiral arm (6kpc away), or perhaps in the near 340.785-0.096 side of the 3-kpc ring. 341.218-0.212 A strong source for which comparison of the present spectrum with 341.218-0.212 the similar Parkes spectrum of 1992 shows moderate variability, 341.218-0.212 and confirms the velocity range -50.0 to -35.0km/s. 341.238-0.270 A new source, slightly confused with the much stronger emission 341.238-0.270 from the previous source, as evident from their aligned spectra. 341.238-0.270 Emission from -52.2 to -50km/s is unique to this source, but 341.238-0.270 extends to -46km/s, where it is confused by emission from 341.238-0.270 341.218-0.212. For the peak intensity, we cite the unconfused 341.238-0.270 peak at -51.2km/s, although other confused features are 341.238-0.270 comparable. The full velocity range is -52.2 to -46km/s, as 341.238-0.270 confirmed by our ATCA data. 341.276+0.062 The same features persist from 1992 until the present, but the 341.276+0.062 current peak of 7.8Jy was only 3.6Jy in 1992. 341.973+0.233 A strongly variable new source. From our spectra at three epochs, 341.973+0.233 we characterize it as two major features, at -12.0 and 341.973+0.233 -11.5km/s, which on the survey cube spectra (mid-2006) peaked at 341.973+0.233 2.5 and 3.5Jy, changed to 2.5 and 6Jy in the ATCA data of 2006 341.973+0.233 December, then both fell dramatically in the MX spectra of 2008 341.973+0.233 August (as displayed in Fig. 1) to 1.35 and 1.13Jy. 342.368+0.140 Most features increased slightly between the survey cube epoch 342.368+0.140 (2006) and the follow-up MX spectrum (2008 August); however, 342.368+0.140 much greater variation occurred in the secondary peak in the MX 342.368+0.140 spectrum (3Jy at -15km/s), which was also more than 3Jy in the 342.368+0.140 ATCA measurements (2008 August), but only 1.5Jy at the survey 342.368+0.140 epoch. Significant variability is corroborated by ATCA 342.368+0.140 measurements of 1994/1995, from which Walsh et al. 342.368+0.140 (1998MNRAS.301..640W) list features at -6.2, -5.1 and -3.6km/s, 342.368+0.140 all below 1Jy, even after correction for an offset of 2 arcmin 342.368+0.140 from the pointing centre. 342.954-0.019 The survey cube discovery spectrum (mid-2006) and MX spectrum 342.954-0.019 (2008 August) are very similar, but at the intermediate epoch of 342.954-0.019 the ATCA observations (2006 December) the feature near -4.1km/s 342.954-0.019 flared from 2 to 5Jy. 343.502-0.472 A highly variable new source; the most recent spectrum of 2008 343.502-0.472 March (as displayed) had a 13.3-Jy peak at -39.0km/s but was 343.502-0.472 only 4Jy in the survey cube (2006) and ATCA measurements of 343.502-0.472 2007 January. 344.227-0.569 Since 1992, there has been high variability for some features 344.227-0.569 (e.g. at -26.5km/s), and weak features of 0.8 and 0.5Jy, 344.227-0.569 extending to -10.5km/s, are now clearly present. 344.419+0.044 and 344.421+0.045. As noted by Caswell (2009PASA...26..454C), 344.419+0.044 these sources are clearly distinct, with a separation of 344.419+0.044 12 arcsec, and no overlap in their velocity ranges. Both are 344.419+0.044 seen on the single spectrum shown in Fig. 1. The stronger site, 344.419+0.044 344.421+0.045, has a velocity range -73 to -70km/s, which has 344.419+0.044 remained similar since 1992. The weaker site, 344.419+0.044, 344.419+0.044 with velocity range -66 to -62.5km/s, has shown marked 344.419+0.044 variability of a feature at -64.9km/s, rising from 0.5Jy in 1992 344.419+0.044 to 2.4Jy in 2008. 344.421+0.045 See note on 344.419+0.044 188.794+1.031 This source was originally detected in 1999 by Szymczak et al. 188.794+1.031 (2000A&AS..143..269S) from a targeted observation of the IRAS 188.794+1.031 source 06061+2151, with a position of RA (J2000) 06:09:06.5, 188.794+1.031 Dec. +21:50:26. Although we were unable to obtain a 188.794+1.031 high-resolution position with the ATCA (due to scheduling 188.794+1.031 constraints), we obtained a position (2009 January) with the 188.794+1.031 MERLIN array of RA (J2000) 06:09:06.96, Dec. +21:50:41.3 is an 188.794+1.031 improvement on the original detection (offset by 52 arcsec from 188.794+1.031 the previous position). The intensity of a feature at -5.5km/s 188.794+1.031 has doubled to nearly 10Jy since the Szymczak et al. 188.794+1.031 (2000A&AS..143..269S) observations, a feature which they 188.794+1.031 detected at -8.7km/s with a peak flux density of ~4Jy at their 188.794+1.031 offset position, has faded to below the detection threshold of 188.794+1.031 the MMB, but is included in the velocity range of Table 2 188.794+1.031 (of 2012MNRAS.420.3108G) for completeness. 188.946+0.886 This source has a peak flux density varying between ~400 and 188.946+0.886 ~600Jy and is periodically variable with a period of 416d 188.946+0.886 (Goedhart, Gaylard & van der Walt, 2004MNRAS.355..553G). A weak 188.946+0.886 feature near -5km/s, originally observed with a peak flux 188.946+0.886 density of ~0.4Jy (Caswell et al. 1995MNRAS.272...96C), was 188.946+0.886 detected in the survey cube (observed 2006 April-June) with a 188.946+0.886 peak flux density of ~0.6Jy, but was not detected in the 188.946+0.886 subsequent MX observation taken in 2008 March. The spectrum in 188.946+0.886 Fig. 2 (of 2012MNRAS.420.3108G) is centred to show the full 188.946+0.886 range of velocities (17km/s) over which emission has been seen. 189.471-1.216 This is a new source for which we were able to obtain a 189.471-1.216 high-resolution position with the MERLIN array (2009 January). 189.778+0.345 Two roughly similar peaks of 14-15Jy at 4 and 5.6km/s in 1992 189.778+0.345 (Caswell et al. 1995MNRAS.272...96C) have both declined in flux 189.778+0.345 density. The 5.6km/s feature decreased to a peak of 6.2Jy in 189.778+0.345 1999 (Caswell, 2009PASA...26..454C), it was then observed to be 189.778+0.345 8Jy in the survey cube (2006 April-June), before decreasing 189.778+0.345 further to 2.5Jy in the 2008 March MX observation. However, it 189.778+0.345 then increased in peak flux density to 4.5Jy in the 2009 March 189.778+0.345 MX observation. The 4km/s feature was 1.5Jy in the survey cube 189.778+0.345 and ~1Jy in the subsequent 2008 and 2009 MX observations. 196.454-1.677 Intensity variations in this source show an unconfirmed 196.454-1.677 periodicity of 668d (Goedhart et al. 2004MNRAS.355..553G). The 196.454-1.677 peak flux density of almost 60Jy at 15.2km/s in 1992 (Caswell et 196.454-1.677 al. 1995MNRAS.272...96C) decreased to 26Jy in 1999 as reported 196.454-1.677 by Caswell (2009PASA...26..454C). Our observations found it had 196.454-1.677 faded further to 18Jy in the survey cube observations taken 2007 196.454-1.677 March/April before brightening slightly to 22Jy in the 196.454-1.677 2008 March MX observation. 206.542-16.355 This source was first detected by Minier et al. 206.542-16.355 (2003A&A...403.1095M). Its association with the Orion B cloud 206.542-16.355 (also called OMC2) at an estimated distance of 0.4kpc 206.542-16.355 (Lombardi, Alves & Lada 2011A&A...535A..16L) makes it one of the 206.542-16.355 closest methanol masers in our Galaxy. We obtained observations 206.542-16.355 with the MERLIN array in 2006, from which we were able to 206.542-16.355 detect and position the source (see Fig. 4 of 206.542-16.355 2012MNRAS.420.3108G). 208.996-19.386 and 209.016-19.398. These two sources, one with a peak velocity 208.996-19.386 of ~7km/s and the other with a peak velocity of -1.5km/s, are 208.996-19.386 associated with the Orion A cloud (also called OMC1), in the 208.996-19.386 direction of very strong HII continuum, giving rise to an 208.996-19.386 irregular baseline as well as prominent absorption. Both masers 208.996-19.386 were positioned in 2003/2004 with the ATCA, as Orion A (south) 208.996-19.386 and Orion KL respectively, by Voronkov et al. 208.996-19.386 (2005MNRAS.362..995V). The feature at ~7km/s was the first to be 208.996-19.386 discovered towards Orion A, observed in 1992 by Caswell et al. 208.996-19.386 (1995MNRAS.272...96C), with a peak flux density of ~0.5Jy. The 208.996-19.386 observations by Voronkov et al. (2005MNRAS.362..995V) found the 208.996-19.386 -1.5km/s feature to be the brightest, at ~1Jy, and partially 208.996-19.386 resolved the ~7km/s feature (again with a flux density of 208.996-19.386 ~0.5Jy), leading to speculation that this feature may be thermal 208.996-19.386 in nature. We obtained observations with the MERLIN array in 208.996-19.386 2006, from which we were able to detect and position the 208.996-19.386 -1.5km/s feature (see Fig. 3), but we did not separately observe 208.996-19.386 the 7km/s feature as it was resolved with the ATCA. MX 208.996-19.386 observations obtained in 2009 March could not detect anything 208.996-19.386 above ~0.2Jy for the ~7km/s feature, although the feature lies 208.996-19.386 in an absorption dip and taking this into account the upper 208.996-19.386 limit may be consistent with 0.5Jy. We show in Fig. 2 (of 208.996-19.386 2012MNRAS.420.3108G) the spectra at both positions, with the 208.996-19.386 spectrum of 208.996-19.386 including emission at ~7km/s, but 208.996-19.386 below the 1{sigma} level. The peak flux density of 208.996-19.386 209.016-19.398 varied between the Orion-Monoceros survey 208.996-19.386 observations and the targeted MX observations in 2009 March (2.8 208.996-19.386 and 0.8Jy, respectively). 209.016-19.398 See note on 208.996-19.386 212.06-0.74 This source was discovered by Xu et al. (2008A&A...485..729X) 212.06-0.74 through observations with the Effelsberg Telescope in 2006 212.06-0.74 February/March as follow-up of water maser detections towards 212.06-0.74 IRAS sources. We, too, detected this source in 2007 August. The 212.06-0.74 position listed in Table 2 is that used for the Effelsberg 212.06-0.74 observations (the IRAS source position), as we were unable to 212.06-0.74 obtain a high-resolution position with the ATCA (due to 212.06-0.74 scheduling constraints). The source velocity, ~45km/s, is 212.06-0.74 significantly positive, more than 20km/s more positive than any 212.06-0.74 other source in our survey within 20{deg} of longitude. Also the 212.06-0.74 peak flux density of this source varied significantly between 212.06-0.74 the survey cube observations (~1Jy) and the MX observation 212.06-0.74 (~0.3Jy). 213.705-12.597 This source is associated with the well-studied Mon R2 cloud 213.705-12.597 (White et al. 1979MNRAS.186..107W; Willson & Folch-Pi 213.705-12.597 1981AJ.....86.1084W; Massi, Felli & Simon 1985A&A...152..387M; 213.705-12.597 Natta et al. 1986A&A...158..143N; Wolf, Lada & Bally 213.705-12.597 1990AJ....100.1892W; Kohno, Koyama & Hamaguchi 213.705-12.597 2002ApJ...567..423K) and known to be variable, both in the 213.705-12.597 methanol (Goedhart et al. 2004MNRAS.355..553G) and the 213.705-12.597 associated 4.765-GHz OH line (Smits, Cohen & Hutawarakorn 213.705-12.597 1998MNRAS.296L..11S). Our Orion-Monoceros survey observations in 213.705-12.597 2008 March detected a peak flux density of 278Jy whilst the 213.705-12.597 targeted MX observation obtained in 2009 March detected a peak 213.705-12.597 flux density of 96Jy. 254.880+0.451 , 259.939-0.041, 263.250+0.514, 264.140+2.018, 264.289+1.469, 254.880+0.451 269.153-1.128, 269.456-1.467, 269.658-1.270 and 270.255+0.835. 254.880+0.451 With the exception of 269.456-1.467 (with a high positive 254.880+0.451 velocity), these maser sites are loosely associated with the 254.880+0.451 well-studied Vela molecular cloud complex [e.g. Murphy & May 254.880+0.451 1991A&A...247..202M; Netterfield et al. 2009ApJ...707.1824N; 254.880+0.451 Olmi et al. 2009ApJ...707.1836O; Hill et al. 254.880+0.451 2011A&A...533A..94H; Giannini et al. (in preparation); Lo et al. 254.880+0.451 (in preparation); Lowe et al. (in preparation)]. 254.880+0.451 264.140+2.018 is a new source detected at the edge of the survey 254.880+0.451 cube region, with an initial position of 264.133+1.984 and peak 254.880+0.451 flux density of 1.4Jy. With the ATCA observations, this was 254.880+0.451 found to be offset (by ~2 arcmin) from the true position of 254.880+0.451 264.140+2.018 and therefore the measured survey cube flux 254.880+0.451 density is less than half the true value, accounting for at 254.880+0.451 least some of the apparent discrepancy with the survey MX 254.880+0.451 detection. There has been some variation in the emission of the 254.880+0.451 faint source 264.289+1.469. It was initially detected with a 254.880+0.451 peak flux density of 0.2Jy (Caswell et al. 1995MNRAS.272...96C), 254.880+0.451 before being positioned in 1999 with a peak flux density of 254.880+0.451 0.4Jy (Caswell, 2009PASA...26..454C). In our survey cube 254.880+0.451 observations, the peak flux density was 0.9Jy and then the 2008 254.880+0.451 March MX found a peak flux density of 0.5Jy. The secondary 254.880+0.451 feature at 6.5km/s flared in the MX observation (it was 254.880+0.451 undetectable against the noise in the survey cube, but was 254.880+0.451 0.4Jy in the MX). Finally, the known source 269.153-1.128 had 254.880+0.451 faded in the survey cube observations [from 1.4Jy in 1992, as 254.880+0.451 reported by Caswell et al. (1995MNRAS.272...96C), 254.880+0.451 to only 0.65Jy], but flared in the MX to 4.1Jy. 259.939-0.041 See note on 254.880+0.451 263.250+0.514 See note on 254.880+0.451 264.140+2.018 See note on 254.880+0.451 264.289+1.469 See note on 254.880+0.451 269.153-1.128 See note on 254.880+0.451 269.456-1.467 See note on 254.880+0.451 269.658-1.270 See note on 254.880+0.451 270.255+0.835 See note on 254.880+0.451 281.710-1.104 This new source had a peak flux density exceeding 1Jy in both the 281.710-1.104 survey cube and ATCA observations, but had faded to 0.35Jy in 281.710-1.104 the 2008 March MX observation. 285.337-0.002 This known source, first detected by Caswell et al. 285.337-0.002 (1995MNRAS.272...96C), has been allocated to the far kinematic 285.337-0.002 distance by both Busfield et al. (2006MNRAS.366.1096B) and 285.337-0.002 Green & McClure-Griffiths (2011MNRAS.417.2500G). 287.371+0.644 This source had slightly faded in peak intensity between the 287.371+0.644 survey cube and MX observations (observed 2006 February and 2008 287.371+0.644 March, respectively). This source was allocated to the near 287.371+0.644 kinematic distance by Green & McClure-Griffiths 287.371+0.644 (2011MNRAS.417.2500G). 290.374+1.661 This source has a history of variability. It was originally 290.374+1.661 detected at 2.4Jy by Caswell et al. (1995MNRAS.272...96C) before 290.374+1.661 being positioned with the ATCA in 1999 with a peak flux density 290.374+1.661 of 0.5Jy (Caswell, 2009PASA...26..454C). It was then found with 290.374+1.661 our initial survey observations to have a peak flux density of 290.374+1.661 0.85Jy before brightening to 2.1Jy in the later MX observation 290.374+1.661 taken 2008 March. 290.411-2.915 This source was detected by Walsh et al. (1997MNRAS.291..261W) 290.411-2.915 and is formally outside our survey region, but we have included 290.411-2.915 it in the catalogue, and presented a newly measured spectrum, 290.411-2.915 for completeness. 291.270-0.719 and 291.274-0.709. The second source is the brighter of the two, 291.270-0.719 consisting only of the features between -31 and -28km/s, peaking 291.270-0.719 at -29.7km/s. The first source, with a peak of 7Jy at -31.2km/s, 291.270-0.719 now appears to have an extended velocity range relative to the 291.270-0.719 previous reported observations (e.g. Caswell, 291.270-0.719 2009PASA...26..454C), due to the presence of an additional 291.270-0.719 feature at -19km/s in the 2008 March MX observation (which was 291.270-0.719 not present in the survey cube observation); we have assigned 291.270-0.719 the feature as most probably part of 291.270-0.719, but we were 291.270-0.719 unable to position it precisely. 291.274-0.709 See note on 291.270-0.719 291.579-0.431 and 291.582-0.435. The first source of this pair is the weaker 291.579-0.431 feature peaking at 15.2km/s, with a wider range of velocities; 291.579-0.431 the second source is the brighter feature peaking at 10.4km/s, 291.579-0.431 with a narrow range of velocities. There are some weak features 291.579-0.431 with velocities of ~19km/s which we include in the listed range 291.579-0.431 of the first source. These features have been seen before 291.579-0.431 (Caswell et al. 1995MNRAS.272...96C), but previously without a 291.579-0.431 high degree of confidence in their authenticity. 291.582-0.435 See note on 291.579-0.431 291.642-0.546 This new source has demonstrated variability over the course of 291.642-0.546 our observations. It was detected in the survey cube 291.642-0.546 observations (2006 June-August) with a peak flux density of 291.642-0.546 1.1Jy at 12.1km/s. It was positioned in 2007 February with a 291.642-0.546 peak flux density of 0.6Jy. Then two MX observations obtained in 291.642-0.546 2009 March could only put upper limits on the peak flux density 291.642-0.546 of 0.3 and 0.2Jy. The survey cube spectrum is presented in 291.642-0.546 Fig. 2 (of 2012MNRAS.420.3108G). 292.074-1.131 This source varied between the survey cube observation (2006 292.074-1.131 June-August) and the later MX observation (2009 March), with 292.074-1.131 respective peak flux densities of 1.76 and 0.85Jy. 292.468+0.168 This new source has a feature at 23.5km/s, which was seen in the 292.468+0.168 survey cube in excess of 4Jy (observed 2006 June-August), 292.468+0.168 positioned with a flux density of only ~0.5Jy with the ATCA 292.468+0.168 (2007 February), and then was barely detectable in the 2009 292.468+0.168 March MX observation (<0.2Jy). 294.337-1.706 This new source was discovered in the survey cube observations 294.337-1.706 (obtained 2006 August and 2007 January) with a peak flux density 294.337-1.706 of 14.5Jy at -11.5km/s. It was positioned in 2007 February with 294.337-1.706 a peak flux density of 30Jy. It then faded to just 0.8Jy in an 294.337-1.706 MX taken in 2008 March. Two new MX observations during 2009 294.337-1.706 March, both failed to detect the source (with a limit of 294.337-1.706 <0.1Jy). The survey cube spectrum is presented in Fig. 2 (of 294.337-1.706 2012MNRAS.420.3108G) as well as the 2008 March MX spectrum. 294.511-1.621 This source has had a history of variability. After being 294.511-1.621 discovered in 1992 with a dominant peak of 18Jy at -10.2km/s 294.511-1.621 (Caswell et al. 1995MNRAS.272...96C), it was then observed in 294.511-1.621 1995 with this feature reduced to 12Jy and the secondary feature 294.511-1.621 at -11.9km/s, originally 7Jy, brightening to a comparable peak 294.511-1.621 flux density of 12Jy (Caswell, 1997MNRAS.289..203C). In our 294.511-1.621 survey cube observations (2006 August and 2007 January), the 294.511-1.621 feature at -10.2km/s had diminished further to <5Jy and the 294.511-1.621 feature at -11.9km/s had diminished slightly to 9Jy. An MX 294.511-1.621 observation in 2008 March found these two features further 294.511-1.621 diminished, but other features within the spectrum brightened 294.511-1.621 including a feature at -8.7km/s which doubled in brightness to 294.511-1.621 4Jy. In a later MX observation, in 2009 March, the feature at 294.511-1.621 -8.7km/s had further brightened to 5.5Jy. 294.977-1.734 This new source was initially detected in the survey cube 294.977-1.734 observations offset from its true position, with two spectral 294.977-1.734 peaks closely spaced in velocity with comparable flux densities 294.977-1.734 of ~1.7 and ~1.9Jy. The peak flux density was 3.5Jy in the 2007 294.977-1.734 ATCA positioning observations, but then faded below 0.1Jy for 294.977-1.734 the 2009 March MX observation. As such the survey cube spectrum 294.977-1.734 is presented in Fig. 2 (of 2012MNRAS.420.3108G). The feature at 294.977-1.734 -12.3km/s arises from 294.990-1.719 (offset 71 arcsec), as is 294.977-1.734 clear from our alignment of the spectra. 298.177-0.795 and 298.213-0.343. Two masers (the first a new source) associated 298.177-0.795 with HII regions attributed by Rahman, Matzner & Moon 298.177-0.795 (2011ApJ...728L..37R) to the 'Dragonfish Nebula', which, they 298.177-0.795 claim is powered by the most luminous OB association in the 298.177-0.795 Galaxy, at a distance of ~9.7kpc. This distance is comparable to 298.177-0.795 the kinematic distance for 298.213-0.343, which is ~10kpc. 298.177-0.795 However, Moises et al. (2011MNRAS.411..705M) allocate a distance 298.177-0.795 of 4.7kpc based on photometric techniques. The second source has 298.177-0.795 demonstrated variability, switching between two velocities for 298.177-0.795 the brightest feature. 298.213-0.343 See note on 298.177-0.795 298.262+0.739 This source was observed in 2005 by J. L. Caswell, but not 298.262+0.739 included in the 2009 compilation (Caswell, 2009PASA...26..454C), 298.262+0.739 as the position could not be confirmed. We have now been able to 298.262+0.739 successfully position the source. This source was allocated to 298.262+0.739 the far kinematic distance by Green & McClure-Griffiths 298.262+0.739 (2011MNRAS.417.2500G). 298.723-0.086 The weak feature at +15km/s of this new source has been 298.723-0.086 positioned with the ATCA to be at the same location as the 298.723-0.086 main features. 300.504-0.176 This source has shown a new feature near 2.5km/s, expanding the 300.504-0.176 velocity spread from the previous observations. This source was 300.504-0.176 allocated to the near kinematic distance by Green & 300.504-0.176 McClure-Griffiths (2011MNRAS.417.2500G). 300.969+1.148 This bright source was used in the survey for system 300.969+1.148 verification, observed frequently at the start of an observing 300.969+1.148 run, and its past record of stability was corroborated [with 300.969+1.148 several MX spectra from the survey shown in Green et al. 300.969+1.148 (2009ApJ...696L.156G)]. 301.136-0.226 This known source, first detected by Caswell et al. 301.136-0.226 (1995MNRAS.272...96C), and positioned with the ATCA by Caswell 301.136-0.226 (2009PASA...26..454C), was allocated to the far kinematic 301.136-0.226 distance by Green & McClure-Griffiths (2011MNRAS.417.2500G). 302.032-0.061 The MX spectrum shown in Fig. 2 for this source was taken at a 302.032-0.061 position ~30 arcsec offset from the actual position (requiring a 302.032-0.061 flux density correction by a factor of 1.07). This source was 302.032-0.061 allocated to the near kinematic distance by Green & 302.032-0.061 McClure-Griffiths (2011MNRAS.417.2500G). 302.034+0.625 This is a slightly variable source. It was initially detected 302.034+0.625 with a flux density of 13Jy (Schutte et al. 302.034+0.625 1993MNRAS.261..783S), then seen with a peak of 10Jy in 2000 302.034+0.625 (Caswell, 2009PASA...26..454C). In our observations, we found a 302.034+0.625 survey flux density of 8Jy, then an MX flux density (2008 March) 302.034+0.625 of 11Jy (although this was taken at a position ~40 arcsec offset 302.034+0.625 from the actual position). 305.199+0.005 , 305.200+0.019, 305.202+0.208, 305.208+0.206, 305.248+0.245, 305.199+0.005 305.362+0.150, 305.366+0.184, 305.475-0.096, 305.563+0.013, 305.199+0.005 305.573-0.342, 305.615-0.344, 305.799-0.245, 305.822-0.115 305.199+0.005 and 305.887+0.017. These sources are all loosely associated with 305.199+0.005 the giant HII region complex, G305 (Clark & Porter 305.199+0.005 2004A&A...427..839C; Walsh et al. 2008PASA...25..105W; Hindson 305.199+0.005 et al. 2010MNRAS.408.1438H; Davies et al. 2012MNRAS.419.1871D), 305.199+0.005 assigned to the far kinematic distance by Caswell et al. 305.199+0.005 (1975A&A....45..239C), Urquhart et al. (2012MNRAS.420.1656U) and 305.199+0.005 Green & McClure-Griffiths (2011MNRAS.417.2500G). The closely 305.199+0.005 spaced quartet of sources, 305.199+0.005, 305.200+0.019, 305.199+0.005 305.202+0.208 and 305.208+0.206, consists of two pairs, shown as 305.199+0.005 two aligned spectra in Fig. 2. (of 2012MNRAS.420.3108G). 305.199+0.005 Caswell (1997MNRAS.289..203C) provides a full description of the 305.199+0.005 features associated with each of the sources and associated 305.199+0.005 maser species. The spectrum of 305.248+0.245 has also been 305.199+0.005 aligned in Fig. 2 (of 2012MNRAS.420.3108G) with those of the 305.199+0.005 previous four sources to highlight which features are sidelobes. 305.199+0.005 305.475-0.096 is a new source and has the widest velocity range 305.199+0.005 of any 6.7-GHz methanol maser detected to date, with features 305.199+0.005 spread across 28.5km/s. 305.200+0.019 See note on 305.199+0.005 305.202+0.208 See note on 305.199+0.005 305.208+0.206 See note on 305.199+0.005 305.248+0.245 See note on 305.199+0.005 305.362+0.150 See note on 305.199+0.005 305.366+0.184 See note on 305.199+0.005 305.475-0.096 See note on 305.199+0.005 305.563+0.013 See note on 305.199+0.005 305.573-0.342 See note on 305.199+0.005 305.615-0.344 See note on 305.199+0.005 305.799-0.245 See note on 305.199+0.005 305.822-0.115 See note on 305.199+0.005 305.887+0.017 See note on 305.199+0.005 306.322-0.334 This source had a peak flux density of 0.4Jy in its initial 306.322-0.334 detection (Caswell et al. 1995MNRAS.272...96C), then brightened 306.322-0.334 to 1Jy in 1999 (Caswell, 2009PASA...26..454C), but returned to 306.322-0.334 ~0.5Jy in our survey and MX observations. This source was 306.322-0.334 allocated to the near kinematic distance by Busfield et al. 306.322-0.334 (2006MNRAS.366.1096B) and Green & McClure-Griffiths 306.322-0.334 (2011MNRAS.417.2500G). 307.132-0.476 and 307.133-0.477. The first of this pair of new sources consists 307.132-0.476 of the less negative velocity features, between -33.5 and 307.132-0.476 -36km/s; the second, the brighter of the two sources, consists 307.132-0.476 of the features between -36 and -40km/s. 307.133-0.477 See note on 307.132-0.476 308.754+0.549 This source was allocated to the far kinematic distance by both 308.754+0.549 Green & McClure-Griffiths (2011MNRAS.417.2500G) and Urquhart et 308.754+0.549 al. (2012MNRAS.420.1656U). 308.056-0.396 and 308.075-0.411. This is a pair of new sources, shown aligned 308.056-0.396 in Fig. 2 (of 2012MNRAS.420.3108G); the first peaks at 308.056-0.396 -11.8km/s, the second at -7.5km/s. The spectrum presented in 308.056-0.396 Fig. 2 (of 2012MNRAS.420.3108G) for 308.056-0.396 was obtained 308.056-0.396 at an offset position (by 36 arcsec), therefore it 308.056-0.396 underestimates the peak flux density of the source by a 308.056-0.396 factor of 1.10. 308.075-0.411 See note on 308.056-0.396 308.686+0.530 Emission at 44km/s is a feature of this new source and not a 308.686+0.530 sidelobe of the nearby, stronger known source 308.754+0.549, as 308.686+0.530 is demonstrated through the aligned spectra in Fig. 2. 308.918+0.123 , 309.384-0.135 and 309.921+0.479. All three of these known 308.918+0.123 sources, originally detected by Caswell et al. 308.918+0.123 (1995MNRAS.272...96C), were allocated to the near kinematic 308.918+0.123 distance by Green & McClure-Griffiths (2011MNRAS.417.2500G). 309.384-0.135 See note on 308.918+0.123 309.921+0.479 See note on 308.918+0.123 310.144+0.760 This source has varied greatly in intensity. It was originally 310.144+0.760 two bright features with peak flux densities of ~140Jy 310.144+0.760 (van der Walt et al. 1995). Both features have since faded, with 310.144+0.760 the -55.7km/s feature having an MX peak flux density of ~80Jy 310.144+0.760 and the -57.5km/s feature an MX peak flux density of just 10Jy. 310.144+0.760 Intermediate epoch positioning measurements (Caswell 310.144+0.760 1996MNRAS.279...79C, 2009PASA...26..454C) found peak flux 310.144+0.760 densities of 60 and 120Jy, respectively. 310.180-0.122 and 311.628+0.266. These two known sources, first detected by 310.180-0.122 Walsh et al. (1997MNRAS.291..261W), were allocated respectively 310.180-0.122 to the far and near kinematic distances by Green & 310.180-0.122 McClure-Griffiths (2011MNRAS.417.2500G). 311.628+0.266 See note on 310.180-0.122 311.947+0.142 and 312.071+0.082. The first of these sources is a weak known 311.947+0.142 source, at a star formation site allocated to the far kinematic 311.947+0.142 distance by Caswell et al. (1975A&A....45..239C), the second is 311.947+0.142 the brightest new source, and is also responsible for the 311.947+0.142 negative feature seen in the (aligned) spectrum of 311.947+0.142 311.947+0.142 in Fig. 2 (of 2012MNRAS.420.3108G). The known 311.947+0.142 source was originally positioned (Caswell, 2009PASA...26..454C) 311.947+0.142 with a feature at -38.3km/s, but that feature has now faded and 311.947+0.142 features at -44 and -47km/s dominate (the original feature is 311.947+0.142 below the noise in the MX observation of 2009 March, but was 311.947+0.142 detected in the survey cube observations taken 2007 311.947+0.142 June-September). 312.071+0.082 See note on 311.947+0.142 312.597+0.045 and 312.598+0.045. Both sources of this close pair are shown on 312.597+0.045 one spectrum in Fig. 2 (of 2012MNRAS.420.3108G). The first 312.597+0.045 source has a single narrow weak feature near -60km/s, whilst the 312.597+0.045 second source spans -68.5 to -64km/s. The peak feature of the 312.597+0.045 second source at -67.9km/s was found to have a flux density 312.597+0.045 of 10.4Jy in the survey observation (2007 June-September), but 312.597+0.045 doubled for the MX observation (2008 March) to 21.4Jy. Both 312.597+0.045 sources were allocated to the near kinematic distance by 312.597+0.045 Green & McClure-Griffiths (2011MNRAS.417.2500G). 312.598+0.045 See note on 312.597+0.045 313.469+0.190 This source has almost doubled in brightness from its original 313.469+0.190 observation in 1992 (Caswell et al. 1995MNRAS.272...96C) to 313.469+0.190 ~30Jy in the 2008 March MX observation. This source was 313.469+0.190 allocated to the far kinematic distance by Green & 313.469+0.190 McClure-Griffiths (2011MNRAS.417.2500G) and by 313.469+0.190 Urquhart et al. (2012MNRAS.420.1656U). 313.577+0.325 This known source, positioned with the ATCA by Caswell 313.577+0.325 (2009PASA...26..454C), was allocated to the near kinematic 313.577+0.325 distance by Green & McClure-Griffiths (2011MNRAS.417.2500G). 313.767-0.863 and 313.774-0.863. Both sources of this close pair 313.767-0.863 (separation 25 arcsec) are variable. 313.767-0.863 is the more 313.767-0.863 negative velocity source, with a shift in the brightest feature 313.767-0.863 from 28Jy at -54.5km/s in Schutte et al. (1993MNRAS.261..783S) 313.767-0.863 to 9Jy at -56.3km/s (the original feature fading to 3Jy). 313.767-0.863 313.774-0.863 accounts for the features between -46 and 313.767-0.863 -40.5km/s, and had a peak of 22Jy at -44.8km/s in the survey 313.767-0.863 observation which faded to 14Jy at -44.9km/s in the 2008 March 313.767-0.863 MX, and then 7Jy in the 2009 March MX (to be replaced by the 313.767-0.863 -41 feature as the brightest). The -44.8km/s feature was only 313.767-0.863 12Jy in the original Schutte et al. (1993MNRAS.261..783S) 313.767-0.863 observations and was ~7Jy in the Caswell (2009PASA...26..454C) 313.767-0.863 ATCA observations. 313.774-0.863 See note on 313.767-0.863 314.320+0.112 This source has a wide range of velocity over which emission is 314.320+0.112 seen (16.5km/s). It was allocated to the far kinematic distance 314.320+0.112 by Green & McClure-Griffiths (2011MNRAS.417.2500G). 315.803-0.575 This new source has doubled in peak flux density with the survey 315.803-0.575 cube (2007 June-July) and positioning observations measuring 315.803-0.575 3.9 and 3.5Jy respectively, and the later MX observations 315.803-0.575 (2008 March) measuring 8.9Jy. 316.359-0.362 , 316.381-0.379 and 316.412-0.308. This is a closely spaced trio 316.359-0.362 of sources. The first is the brightest with features at the most 316.359-0.362 positive velocities (between +1.5 and +8.5km/s), the second 316.359-0.362 covers the smaller intermediate range of -0.5 to +1.5km/s and 316.359-0.362 the third the most negative features, between -5.6 and +2km/s. 316.359-0.362 All three sources were allocated to the near kinematic distance 316.359-0.362 by Green & McClure-Griffiths (2011MNRAS.417.2500G). 316.381-0.379 See note on 316.359-0.362 316.412-0.308 See note on 316.359-0.362 316.484-0.310 The -11.5km/s feature of this new source flared after the survey 316.484-0.310 and positioning observations (when it was <0.2Jy), with the MX 316.484-0.310 observation in 2008 August finding a peak flux density of 0.7Jy. 316.484-0.310 This shifted the peak velocity from -15.6 to -11.5km/s. The 316.484-0.310 original peak feature at -15.6km/s faded from 2.3Jy in the 316.484-0.310 survey observations to ~0.45Jy in the MX. 316.640-0.087 The intensity variability of this source is known to be 316.640-0.087 quasi-periodic, with a period of 321+/-48d (Goedhart et al. 316.640-0.087 2004MNRAS.355..553G). Both our survey (2007 March-July) and MX 316.640-0.087 observations (2008 August) detected comparable flux densities 316.640-0.087 for the peak feature. 316.811-0.057 This source has demonstrated significant brightening of its 316.811-0.057 emission. It was originally detected with a peak flux density of 316.811-0.057 12Jy in 1992 (Caswell et al. 1995MNRAS.272...96C), and 316.811-0.057 positioned in 1996 with a peak flux density of 9Jy (Caswell, 316.811-0.057 2009PASA...26..454C), but was detected in the MMB survey 316.811-0.057 observations with a peak flux density of 75Jy, before slightly 316.811-0.057 diminishing to 52Jy in the 2008 August MX observation. This 316.811-0.057 source was allocated to the near kinematic distance by Busfield 316.811-0.057 et al. (2006MNRAS.366.1096B). 317.029+0.361 Urquhart et al. (2012MNRAS.420.1656U) allocate the associated 317.029+0.361 compact HII region from the Red MSX Survey to the far 317.029+0.361 kinematic distance. 317.466-0.402 Emission from this source has a wide range of velocity (16km/s). 317.466-0.402 The source was allocated to the far kinematic distance by 317.466-0.402 Green & McClure-Griffiths (2011MNRAS.417.2500G). 317.701+0.110 Detected by van der Walt et al. (1995A&AS..110...81V) with a peak 317.701+0.110 flux density of 32Jy, and positioned in 2000 with a peak flux 317.701+0.110 density of 8Jy (Caswell, 2009PASA...26..454C). Our detection 317.701+0.110 found a return to similar emission as the original detection, 317.701+0.110 with the survey observations measuring 26Jy and the MX 23Jy. 317.701+0.110 This source was allocated to the near kinematic distance by 317.701+0.110 Green & McClure-Griffiths (2011MNRAS.417.2500G). 318.043-1.404 The positive velocity of this source, combined with its large 318.043-1.404 latitude, indicates a large kinematic distance and hence large 318.043-1.404 distance from the Galactic plane ('z'), possibly attributed to 318.043-1.404 the flared/warped outer Galaxy (the source is kinematically 318.043-1.404 associated with the outer Galaxy portion of the 318.043-1.404 Carina-Sagittarius spiral arm, see Section 4.6). 318.050+0.087 This source had similar survey and MX peak flux densities of 318.050+0.087 ~12Jy, comparable to the positioning observation in 1999 by 318.050+0.087 Caswell (2009PASA...26..454C). However, it was originally 318.050+0.087 detected in 1992 (Caswell et al. 1995MNRAS.272...96C) with a 318.050+0.087 peak flux density of only 3.8Jy. This source was allocated to 318.050+0.087 the near kinematic distance by Green & McClure-Griffiths 318.050+0.087 (2011MNRAS.417.2500G). 318.948-0.196 This very bright source, observed with the ATCA by Norris et al. 318.948-0.196 (1993ApJ...412..222N) and Caswell et al. (1995MNRAS.277..210C), 318.948-0.196 was allocated to the near kinematic distance by 318.948-0.196 Green & McClure-Griffiths (2011MNRAS.417.2500G). 319.163-0.421 Urquhart et al. (2012MNRAS.420.1656U) allocate the associated 319.163-0.421 compact HII region from the Red MSX Survey to the far 319.163-0.421 kinematic distance. 319.836-0.197 This is a consistently weak source with our observations (survey 319.836-0.197 peak flux density of 0.65Jy, MX peak flux density of 0.23Jy) 319.836-0.197 finding comparable flux density to the original 1992 detection 319.836-0.197 (peak flux density of 0.4Jy) of Caswell et al. 319.836-0.197 (1995MNRAS.272...96C). This source was allocated to the near 319.836-0.197 kinematic distance by Green & McClure-Griffiths 319.836-0.197 (2011MNRAS.417.2500G). 320.123-0.504 This known source, positioned with the ATCA by Caswell 320.123-0.504 (2009PASA...26..454C), was allocated to the far kinematic 320.123-0.504 distance by Green & McClure-Griffiths (2011MNRAS.417.2500G). 320.231-0.284 This source has demonstrated significant variability. It was 320.231-0.284 originally detected in 1992 with a peak flux density of 27Jy 320.231-0.284 (Caswell et al. 1995MNRAS.272...96C), before being positioned in 320.231-0.284 1999 with a peak flux density of 20Jy (Caswell, 320.231-0.284 2009PASA...26..454C). For our observations, it was detected in 320.231-0.284 the survey cube (2006 April-May) with a peak flux density of 320.231-0.284 32Jy, was positioned (2007 January) with a peak flux density of 320.231-0.284 16Jy, and in the subsequent MX observation (2008 August) was 320.231-0.284 found to peak at 54Jy. This source was allocated to the far 320.231-0.284 kinematic distance by Urquhart et al. (2012MNRAS.420.1656U). 320.285-0.308 The spectrum of this weak new source has been aligned with the 320.285-0.308 spectrum of the known bright source 320.231-0.284 in Fig. 2 320.285-0.308 (of 2012MNRAS.420.3108G) to reveal that the feature seen at 320.285-0.308 -62.5km/s is a sidelobe of the nearby brighter source. 320.414+0.109 and 320.424+0.089. This is a pair of new sources. The spectrum 320.414+0.109 presented in Fig. 2 (of 2012MNRAS.420.3108G) for 320.414+0.109 320.414+0.109 was obtained at an offset position (by 52 arcsec) and therefore 320.414+0.109 underestimates the peak flux density of the source by a factor 320.414+0.109 of 1.25. The aligned spectra of the two sources clearly show 320.414+0.109 that the first source is the brighter feature at -13.4km/s, 320.414+0.109 whilst the second source consists of features between -4 and 320.414+0.109 -10km/s, peaking at -8km/s. 320.424+0.089 See note on 320.414+0.109 320.780+0.248 This is the second brightest (40Jy) new source. 321.030-0.485 and 321.033-0.483. This is a close pair of sources originally 321.030-0.485 detected by Schutte et al. (1993MNRAS.261..783S) and further 321.030-0.485 observed and discussed by van der Walt et al. (1995), Walsh et 321.030-0.485 al. (1998MNRAS.301..640W) and Caswell (2009PASA...26..454C). The 321.030-0.485 second source has varied, with a peak flux density of 142Jy in 321.030-0.485 the survey cube observation (2006 April-May), then 76Jy in the 321.030-0.485 2008 August MX and 58Jy in the 2009 March MX. 321.033-0.483 See note on 321.030-0.485 321.148-0.529 This known source, positioned with the ATCA by Caswell 321.148-0.529 (2009PASA...26..454C), was allocated to the near kinematic 321.148-0.529 distance by Green & McClure-Griffiths (2011MNRAS.417.2500G). 321.704+1.168 This source has a history of variability. It was originally 321.704+1.168 discovered in 1992 with a peak flux density of 1.4Jy, but 321.704+1.168 'disappeared' in 1993 (Caswell et al. 1995MNRAS.272...96C). In 321.704+1.168 our survey cube observation (2006 April-May), we found a peak 321.704+1.168 flux density of 2.1Jy, which faded to 1.2Jy in the 2007 ATCA 321.704+1.168 positioning measurement, and then was not present in either of 321.704+1.168 two MX observations (2008 March and 2008 August). As such the 321.704+1.168 survey cube spectrum is shown in Fig. 2 of 2012MNRAS.420.3108G). 322.158+0.636 The feature at -64.2km/s flared by almost a factor of 2 between 322.158+0.636 the initial survey cube observation (~150Jy) and the follow-up 322.158+0.636 MX (~280Jy). This feature was only 65Jy in the original 1992 322.158+0.636 observation of Caswell et al. (1995MNRAS.272...96C). The HII 322.158+0.636 region in which the maser appears to be embedded was allocated 322.158+0.636 to the near kinematic distance by Caswell et al. 322.158+0.636 (1975A&A....45..239C) and Urquhart et al. (2012MNRAS.420.1656U). 323.459-0.079 This known source, positioned with the ATCA by Caswell 323.459-0.079 (1997MNRAS.289..203C), was allocated to the near kinematic 323.459-0.079 distance by Green & McClure-Griffiths (2011MNRAS.417.2500G). 323.740-0.263 The wide velocity range (17km/s) of this bright source is not 323.740-0.263 apparent from the spectrum presented in Fig. 2 323.740-0.263 (of 2012MNRAS.420.3108G), but can be seen in the spectrum 323.740-0.263 previously published by Caswell et al. (1995MNRAS.272...96C). 323.740-0.263 This source has been allocated to the near kinematic distance 323.740-0.263 (Busfield et al. 2006MNRAS.366.1096B; Green & McClure-Griffiths 323.740-0.263 2011MNRAS.417.2500G). 323.766-1.370 The positive velocity of this new source, combined with its large 323.766-1.370 latitude, indicates a large kinematic distance and large 323.766-1.370 distance from the Galactic plane ('z'), possibly attributed to 323.766-1.370 the flared/warped outer Galaxy (the source is kinematically 323.766-1.370 associated with the outer Galaxy portion of the 323.766-1.370 Carina-Sagittarius spiral arm, see Section 4.6). 323.799+0.017 The spectrum of this new source has been aligned with the 323.799+0.017 spectrum of 323.740-0.263 in Fig. 2 (of 2012MNRAS.420.3108G) 323.799+0.017 to reveal that the negative feature at -51km/s is a response to 323.799+0.017 the bright source 323.740-0.263 in one of the reference beams. 324.716+0.342 This source has a history of variability: it had a peak flux 324.716+0.342 density of 8Jy at 47.5km/s in the original 1992 observation 324.716+0.342 (Caswell et al. 1995MNRAS.272...96C), but was then only 3.5Jy in 324.716+0.342 1999 (Caswell, 2009PASA...26..454C). The secondary feature was 324.716+0.342 stable though, approximately 6Jy in both measurements. Our MX 324.716+0.342 and survey observations were both similar with ~10Jy for the 324.716+0.342 47.5km/s feature. The secondary feature was ~1.5Jy in the survey 324.716+0.342 cube, but about 0.5Jy in the 2008 March MX. This source was 324.716+0.342 allocated to the far kinematic distance by Green & 324.716+0.342 McClure-Griffiths (2011MNRAS.417.2500G). 324.923-0.568 This known source, first detected by Walsh et al. 324.923-0.568 (1998MNRAS.301..640W), was allocated to the near kinematic 324.923-0.568 distance by Green & McClure-Griffiths (2011MNRAS.417.2500G). 325.659-0.022 This new source faded from a peak flux density of 2.3Jy in the 325.659-0.022 survey observation (2006 January-February) to just 0.6Jy in the 325.659-0.022 MX (2008 March). The ATCA positioning measurement detected a 325.659-0.022 similar flux density to the MX observation. 326.323-0.393 The brightest feature of this new source flared from a peak flux 326.323-0.393 density of 2Jy in the survey observation (2006 January) to 3.3Jy 326.323-0.393 in the MX observation (2008 March). The secondary feature was 326.323-0.393 even more variable, flaring from 0.5 to 1.5Jy. 326.448-0.748 This new source has a wide velocity range of multiple spectral 326.448-0.748 features, several of which dimmed between the survey observation 326.448-0.748 and MX observation, shifting the peak velocity from -71.7 to 326.448-0.748 -68.6km/s (the feature at -71.7km/s also fading by a factor 326.448-0.748 of ~0.5). 326.475+0.703 and 326.476+0.695. The sources of this close pair (separated 326.475+0.703 by 29 arcsec) are shown as one spectrum in Fig. 2. The two 326.475+0.703 sources share the same range of velocities, but the first peaks 326.475+0.703 at -38.5km/s, whilst the second peaks at -43.6km/s. These 326.475+0.703 sources were allocated to the far kinematic distance by Green & 326.475+0.703 McClure-Griffiths (2011MNRAS.417.2500G), but the near kinematic 326.475+0.703 distance by Busfield et al. (2006MNRAS.366.1096B). 326.476+0.695 See note on 326.475+0.703 326.608+0.799 This is a weak new source. The spectrum presented in Fig. 2 326.608+0.799 (of 2012MNRAS.420.3108G) is aligned with the spectra of 326.608+0.799 326.475+0.703 and 326.476+0.695 to highlight that the negative 326.608+0.799 feature at -38.5km/s is a result of the bright source 326.608+0.799 326.475+0.703 falling within one of the reference beams. 326.641+0.611 This source, known since 1992 (reported in Caswell et al. 326.641+0.611 1995MNRAS.272...96C), exhibited minor variation in its 326.641+0.611 intensity, with the survey observations finding a peak flux 326.641+0.611 density of 26Jy and the MX observations 31Jy. This source was 326.641+0.611 allocated to the near kinematic distance by Urquhart et al. 326.641+0.611 (2012MNRAS.420.1656U) and has a similarly small photometric 326.641+0.611 distance (Moises et al. 2011MNRAS.411..705M). 326.859-0.677 and 327.120+0.511. Both of these known sources were allocated to 326.859-0.677 the near kinematic distance by Green & McClure-Griffiths 326.859-0.677 (2011MNRAS.417.2500G). 327.120+0.511 See note on 326.859-0.677 327.291-0.578 This source, although varying greatly since 1992, had only minor 327.291-0.578 variation between the survey observation (2006 January) and the 327.291-0.578 later MX observation (2008 March), with peak flux densities of 327.291-0.578 2.6 and 3.4Jy, respectively. The prominent absorption, centred 327.291-0.578 at approximately -48km/s, is discussed in Caswell et al. 327.291-0.578 (1995MNRAS.272...96C). 327.392+0.199 and 327.395+0.197. The sources of this close pair are separated 327.392+0.199 by only 14 arcsec and have almost contiguous velocity ranges. 327.392+0.199 Both sources were allocated to the near kinematic distance by 327.392+0.199 Green & McClure-Griffiths (2011MNRAS.417.2500G). 327.395+0.197 See note on 327.392+0.199 327.402+0.445 This known source, first detected by Caswell et al. 327.402+0.445 (1995MNRAS.272...96C), was allocated to the near kinematic 327.402+0.445 distance by Green & McClure-Griffiths (2011MNRAS.417.2500G). 327.590-0.094 and 327.618-0.111. The sources of this close pair (offset by 327.590-0.094 ~2 arcmin in right ascension) are shown aligned in Fig. 2 (of 327.590-0.094 2012MNRAS.420.3108G). Each spectrum shows a weak sidelobe 327.590-0.094 response of the other source (attenuated by a factor of ~3). 327.590-0.094 These sources were allocated to the far kinematic distance by 327.590-0.094 Green & McClure-Griffiths (2011MNRAS.417.2500G). 327.618-0.111 This known source, positioned with the ATCA by Caswell 327.618-0.111 (2009PASA...26..454C), was allocated to the far kinematic 327.618-0.111 distance by Green & McClure-Griffiths (2011MNRAS.417.2500G). 327.945-0.115 This simple single-feature source has remained remarkably stable 327.945-0.115 over its observational history of 15 years, with a peak flux 327.945-0.115 density of ~8Jy (it was first observed in 1994 and reported in 327.945-0.115 Ellingsen et al. (1996, PhD thesis, Univ. Tasmania), our MX 327.945-0.115 observation was taken in 2009). 328.140-0.432 This new source was more than three times brighter in the MX 328.140-0.432 observation (2008 August) than in the initial survey cube 328.140-0.432 observation (2006 January). 328.237-0.547 and 328.254-0.532. This is a bright pair of sources, with 328.237-0.547 overlapping velocity ranges and the brighter of the two, 328.237-0.547 328.237-0.547, is known to be periodically variable (Goedhart et 328.237-0.547 al. 2004MNRAS.355..553G). The period was originally estimated to 328.237-0.547 be 216d (Goedhart et al. 2004MNRAS.355..553G), but later revised 328.237-0.547 to 220d (Goedhart, Gaylard & van der Walt 2004MNRAS.355..553G). 328.237-0.547 328.237-0.547 was found to have a peak flux density of 1481Jy in 328.237-0.547 the survey cube observations (2006 January), then 1340Jy in the 328.237-0.547 later MX observation (2008 August). 328.254-0.532 See note on 328.237-0.547 328.808+0.633 and 328.809+0.633. These very close sources (2.5-arcsec 328.808+0.633 separation) have peak velocities within 0.5km/s. We retain the 328.808+0.633 interpretation of Caswell (1997MNRAS.289..203C) and Caswell 328.808+0.633 (2009PASA...26..454C) that the first source has features across 328.808+0.633 the full velocity range, but the second is a single strong 328.808+0.633 feature (at -44.4km/s in our spectrum). Long Baseline Array 328.808+0.633 observations by Dodson, Ojha & Ellingsen (2004MNRAS.351..779D) 328.808+0.633 confirm the spatial offset of the isolated 328.809+0.633 source. 328.808+0.633 Both sources were allocated to the near kinematic distance by 328.808+0.633 Green & McClure-Griffiths (2011MNRAS.417.2500G). 328.809+0.633 See note on 328.808+0.633 328.819+1.704 This source has a wide range of velocity over which emission is 328.819+1.704 seen (18.5km/s). 328.940+0.558 and 328.942+0.565. A pair of new sources separated by 26 arcsec, 328.940+0.558 the first with a peak at -98.8km/s and the second with a peak at 328.940+0.558 -90.9km/s. Both sources share comparable velocity ranges of 328.940+0.558 emission. 328.942+0.565 See note on 328.940+0.558 329.029-0.205 and 329.031-0.198. This is a close pair of sources separated by 329.029-0.205 26 arcsec, with the first peaking at -37.1km/s and the second at 329.029-0.205 -45.8km/s. The velocity ranges of the sources are adjacent, with 329.029-0.205 the first -33.5 to -41.5km/s and the second -41.5 to -48.5km/s. 329.029-0.205 These sources are believed to be embedded in an infrared dark 329.029-0.205 cloud (Ellingsen, 2006, PhD thesis, Univ. Tasmania), usually 329.029-0.205 indicative of a near distance assignment, however no HI 329.029-0.205 self-absorption was seen towards these sources, indicating a far 329.029-0.205 kinematic distance (Green & McClure-Griffiths 329.029-0.205 2011MNRAS.417.2500G). 329.031-0.198 See note on 329.029-0.205 329.066-0.308 This source was first detected as a weak feature with the Parkes 329.066-0.308 Radio Telescope in 1992 (reported by Caswell et al. 329.066-0.308 1995MNRAS.272...96C), but later ATCA observations (Caswell et 329.066-0.308 al. 1995MNRAS.277..210C) found the source to be considerably 329.066-0.308 offset from the previous pair, and thus yielded an estimated 329.066-0.308 peak flux density of ~20Jy. We found a comparable peak flux 329.066-0.308 density of 21.9Jy in the survey cube, falling to 14.4Jy in the 329.066-0.308 MX observation (2008 March). This source was allocated to the 329.066-0.308 far kinematic distance by Green & McClure-Griffiths 329.066-0.308 (2011MNRAS.417.2500G). 329.183-0.314 The peak feature of this source faded from the initial survey 329.183-0.314 observation (2006 January), with a peak flux density of 10.7Jy, 329.183-0.314 to the later MX observation (2008 March), with a peak flux 329.183-0.314 density of 5.1Jy. The feature at -51km/s flared slightly, and 329.183-0.314 the feature at -59km/s faded slightly, such that the second 329.183-0.314 brightest feature switched between the survey observation and 329.183-0.314 the MX observation. This source was allocated to the near 329.183-0.314 kinematic distance by Green & McClure-Griffiths 329.183-0.314 (2011MNRAS.417.2500G). 329.405-0.459 and 329.407-0.459. The second of this close pair of sources is 329.405-0.459 variable, with the initial survey observation finding a peak 329.405-0.459 flux density of 130Jy and subsequent MX observations finding 329.405-0.459 96Jy (2008 March) and 120Jy (2009 March). It was originally 329.405-0.459 detected with a peak flux density of 155Jy in 1992 (Caswell et 329.405-0.459 al. 1995MNRAS.272...96C) and positioned in 2000 with a peak flux 329.405-0.459 density of 72Jy (Caswell, 2009PASA...26..454C). 329.407-0.459 See note on 329.405-0.459 329.469+0.503 The peak feature of this source at -72km/s has brightened from 329.469+0.503 the original Schutte et al. (1993MNRAS.261..783S) observations, 329.469+0.503 and the other spectral features have varied, with the most 329.469+0.503 notable changes being the brightening of the feature at -73km/s 329.469+0.503 and the dimming of the feature at -70.5km/s. The outlying 329.469+0.503 feature at -59km/s also flared in the MX observation (2008 329.469+0.503 August) compared with the initial survey observation (2006 329.469+0.503 January). This source has a wide range of velocity over which 329.469+0.503 emission is seen (16km/s). It was allocated to the far kinematic 329.469+0.503 distance by Green & McClure-Griffiths (2011MNRAS.417.2500G). 329.556+0.181 This new source has experienced variability in both its 329.556+0.181 individual features and peak flux density, changing between the 329.556+0.181 survey and MX observations, with peak velocities of -109 and 329.556+0.181 -106.5km/s, respectively. 329.622+0.138 and 329.610+0.114. These sources are in relative close proximity 329.622+0.138 to one another (offset by ~100 arcsec). Their features appear in 329.622+0.138 the spectra at both positions, but are clearly distinct in 329.622+0.138 velocity, with almost 15km/s separation between the emission 329.622+0.138 boundaries in velocity. Both sources were allocated to the far 329.622+0.138 kinematic distance by Green & McClure-Griffiths 329.622+0.138 (2011MNRAS.417.2500G). 329.610+0.114 See note on 329.622+0.138 329.719+1.164 This new source exhibited significant variation in its peak 329.719+1.164 intensity, with the survey observation finding a peak flux 329.719+1.164 density of 24.4Jy and subsequent MX observations taken in 2008 329.719+1.164 August finding ~8Jy. There has also been variation in individual 329.719+1.164 features of the spectrum, but the weakest feature at -82.2km/s 329.719+1.164 has remained stable at ~1Jy.