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Table C.2

Results of the search for radio emission overlapping the new and the known bow shock (BS) and bubble (BU) candidates in different radio surveys.

BS/BU RA DEC NVSS VLASS RACS-low RACS-mid
(h m s) (° ′ ″)
New BS and BU candidates associated with O-type runaway stars

BS-GR9(*) 06 08 55.822 1542 18.02 no emission no emission no emission no emission
BS-GR34 20 22 37.757 41 40 29.19 no emission discrete sources no images discrete sources
BS-GR35 07 53 38.205 −26 14 02.53 no emission no emission no emission no emission
BS-GR71 10 15 40.071 −51 15 23.99 no emission no emission
BS-GR72(*) 04 03 20.746 51 18 52.49 extended source ill-imaged
BS-GR75(*) 19 45 42.111 25 21 16.35 no emission ill-imaged no emission no emission
BU-GR78 20 11 01.700 42 07 36.33 no emission no emission no images no emission
BS-GR80 20 00 59.998 42 00 30.76 unrelated emission discrete source no images ill-imaged
BS-GR93 13 23 56.244 −59 48 34.82 no emission no emission
BU/BS-GR100 15 13 55.196 −59 07 51.64 no emission no emission

New BS and BU candidates associated with Be-type runaway stars

BU-BR21 20 09 39.591 21 04 43.49 no emission no emission no emission no emission
BU-BR46 19 49 32.908 32 57 22.16 no emission no emission no emission no emission
BS-BR65 01 45 11.716 61 10 22.89 no emission no emission

New BS candidate found in the field of BS-GR35 (no runaway star associated)

BS J075339−2616.5(*) 07 53 39.1 −26 16 31 weak emission no emission emission weak emission

Known BS and BU candidates

BS-GR40 06 34 23.562 02 32 02.96 no emission no emission no emission no emission
BS/BU-GR51(*) 18 30 34.785 −08 38 03.72 emission no emission emission weak emission
BS-GR70 07 53 01.006 −27 06 57.70 no emission no emission no emission no emission
BS-GR83(*) 17 15 22.330 −38 12 46.79 no emission no images weak emission no emission

Notes. The horizontal lines separate the objects in four groups as indicated in the table. RA and DEC coordinates are those of the runaway stars, except for BS J075339−2616.5 which are the BS coordinates. ’—’ means that the source is not visible for the observing instrument. (*)These sources have their own discussion in Sect. C.2.

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