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Table 5

List of methanol maser sources with the water maser emission of linear offset greater than 0.1 pc.

CH3OH source H2O emission Δwmdist ΔVmin ΔVmax MIR source Δ(MIR−H2O)
Gll.lll ± bb.bbb Gll.lll ± bb.bbb (arcsec) (pc) (km s-1) (km s-1) (arcsec)
G22.357+00.066 G22.351+0.068 20.05 0.47 22.3 22.9 G022.3506+00.0678 3.22
G23.707−00.198 G23.706−0.200 6.13 0.13 3.1 5.0 G023.7057-00.1999 1.32
G23.966−00.109 G23.965−0.110 5.58 0.12 4.5* G023.9649-00.1104 0.62
G24.148−00.009 G24.155−0.010 25.48 0.24 0.6 23.1 G024.1550-00.0119 7.34
G24.541+00.312 G24.534+0.319 35.90 0.99 6.7 8.7 G024.5351+00.3190 5.13
G30.400−00.296 G30.403−0.297 10.57 0.29 21.8 29.7 G030.4010-00.2960 7.92
G31.047+00.356 G31.047+0.357 6.91 0.11 0.2 20.2 G031.0467+00.3574 5
G31.581+00.077 G31.581+0.078 4.92 0.13 1.7 4.9 G031.5813+00.0788 2.31
G32.992+00.034 G32.996+0.041 30.58 0.72 0.2 17.9 G032.9962+00.0414 0.32
G37.030−00.039 G37.039−0.035 33.73 0.82 2.8 8.7 G037.0385-00.0350 1.62
G37.039−0.034 37.36 0.91 4.8 6.1 G037.0385-00.0350 6.12
G37.598+00.425 G37.597+0.424 3.34 0.10 1.6 2.2 G037.5978+00.4253 4.11
G38.038−00.300 G38.038−0.305 16.06 0.28 4.1 18.6 G038.0384-00.3042 1.62
G38.041−0.298 13.78 0.24 0.8* G038.0409-00.2968 5.22

Notes. The two first columns list the galactic coordinates of methanol and water masers, respectively. Δwmdist is the angular (Col. 3) and linear (Col. 4) separation of H2O maser emission from the methanol source. ΔVmin is the minimum and ΔVmax is the maximum differences between the LSR velocity of water maser spot from the analysed group and the systemic velocity (Table 4). The name of MIR source nearby to the H2O maser emission and angular separation between them, Δ(MIR−H2O), are given.

1

H2O maser emission is associated with the same MIR source as CH3OH maser emission.

2

H2O maser emission is not associated with the same MIR source as CH3OH maser emission.

3

 H2O maser emission is not associated with the same MIR source as CH3OH maser emission, but lies instead in a cluster of three MIR sources.

4

H2O maser emission is likely not associated with the same MIR source as CH3OH maser emission but with MIR object in the region of diffuse (~10″) excess of 4.5 μm emission seen in the IRAC Spitzer maps. The name of the strongest MIR counterpart is given.

5

H2O maser emission is tentatively associated with the same MIR source as CH3OH maser emission, lying at the edge of diffuse excess of 4.5 μm emission from possible cluster of MIR sources.

*

When a single maser spot was observed, only ΔVmin is given.

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