Parameters of thermal gas and indicators of stellar activity in the field of the Fermi-LAT source from available catalogues.
|Source||Source positiona||vRRL a||Distancea||CH3OH||MYSO|
|number||(Galactic l + b)||(K km s−1)||(kpc)||detectionb||candidatesc|
|1||337.711 − 0.056||−50.0||12.12||2||2|
|2||337.711 + 0.089||−76.7||10.79||1||3|
|3||337.622 − 0.067||−55.0||11.84||3||2|
|4||337.667 − 0.167||−53.0||11.95||–||1|
|5||337.978 − 0.144||–||≥TP||1||4|
|6||338.011 + 0.022||−63.3d||≥TP||–||1|
|7||337.686 + 0.137||−47.0||12.30||3||3|
|8||338.114 − 0.193||−53.0||11.96||–||4|
Notes.The first column indicates the number that labels each HII region as in Fig. 1. In Cols. 2–4, the Galactic coordinates (in the l + b form), the radio recombination line (RRL) velocity (vRRL), and the distance (in kpc) for each HII region are listed. The number in Col. 5 is the number of 6.7-GHz CH3 OH maser detections towards the HII regions, in the velocity range of the MC detected in correlation with the Fermi-LAT source. The last column shows the number of massive young stellar object (MYSO) candidates catalogued towards the HII regions. “ ≥TP” indicates that the HII region is beyond the tangent point (~8 kpc). (a) From Jones & Dickey (2012). (b)From the 6-GHz methanol multibeam maser catalogue of Caswell et al. (2011). (c) From the Red MSX Source (RMS) Survey (Lumsden et al. 2013). (d)This value corresponds to the LSR velocity of the HII region (not the vRRL) from 13 CO observations, according to Anderson et al. (2014).
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