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COL15B - H₂O and OH masers associated with cold infrared sources

Short title: Colom et al. (2015)
Authors: Colom, P.Lekht, E. E.Pashchenko, M. I.Rudnitskii, G. M.Tolmachev, A. M.
Journal: Astronomy Letters, Volume 41, Issue 8, pp.425-441
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Target type: IRAS
Observations category: SF.general
Facility type: single-dish
Transitions: OH_1665,OH_1667

Abstract
We present the results of our monitoring of four maser sources associated with cold infrared sources. The observations were performed in the water-vapor line at 1.35 cm with the 22-m radio telescope at the Pushchino Radio Astronomy Observatory and in the hydroxyl lines at 18 cm with the Nancay radio telescope. Cyclic variability of the H₂O maser emission was detected in all four sources. The durations of the cycles are different and lie within the range 1.8-5.5 yr. In each source, the cycles differed by a factor from 1.5 to 2.25. A fairly periodic pattern of variability was observed in IRAS 20126+4104 on a time scale from 3.6 to 5.3 yr. Models of the maser sources are discussed. In IRAS 20126+4104, we detected strong variability of the maser emission in the main OH 1665 and 1667 MHz lines. We calculated the magnetic field strength for two maser features from the Zeeman splitting of the OH line: in IRAS 18265-1517 (1.3 mG at epoch 2008) and IRAS 20126+4104 (10 mG at epoch 2014). Variability of the magnetic field was detected in the second feature. In the same sources, we detected maser emission in the 1667 MHz OH line. The presence of emission in both main OH 1665 and 1667 MHz lines is consistent with the existing model calculations and will allow the gas density in the masing regions to be refined.

Abstract

We present the results of our monitoring of four maser sources associated with cold infrared sources. The observations were performed in the water-vapor line at 1.35 cm with the 22-m radio telescope at the Pushchino Radio Astronomy Observatory and in the hydroxyl lines at 18 cm with the Nancay radio telescope. Cyclic variability of the H₂O maser emission was detected in all four sources. The durations of the cycles are different and lie within the range 1.8-5.5 yr. In each source, the cycles differed by a factor from 1.5 to 2.25. A fairly periodic pattern of variability was observed in IRAS 20126+4104 on a time scale from 3.6 to 5.3 yr. Models of the maser sources are discussed. In IRAS 20126+4104, we detected strong variability of the maser emission in the main OH 1665 and 1667 MHz lines. We calculated the magnetic field strength for two maser features from the Zeeman splitting of the OH line: in IRAS 18265-1517 (1.3 mG at epoch 2008) and IRAS 20126+4104 (10 mG at epoch 2014). Variability of the magnetic field was detected in the second feature. In the same sources, we detected maser emission in the 1667 MHz OH line. The presence of emission in both main OH 1665 and 1667 MHz lines is consistent with the existing model calculations and will allow the gas density in the masing regions to be refined.

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Detection table from Colom et al. (2015)

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ID	Obs. RA	Obs. Dec	l	b	Source name	Image	Descr.	Line	Frequency	V_range	∫F dv	Telescope	V_step	Beam	Dist. (parallax)
	(J2000)	(J2000)	(deg.)	(deg.)				OH	(MHz)	(km/s)	(Jy*km/s)		(km/s)	(arcsec)	(kpc)
1	06 33 31.1	+04 00 07	207.3245	-2.1504	IRAS 06308+0402		Descr	1665 MHz;	1665	11;25	50	NANCAY	0.0822	999
2	18 29 24.4	-15 15 56	16.8658	-2.1576	IRAS 18265-1517	Image	Descr	1665 MHz;	1665	-55;34	422	NANCAY	0.0822	999
3	18 30 35.3	-15 14 38	17.0169	-2.4004	IRAS 18277-1516			1665 MHz;	1665	-15;29	510	NANCAY	0.0822	999
4	20 14 26	+41 13 32	78.1221	3.6328	IRAS 20126+4104	Image	Descr	1665 MHz;	1665	-28;23	740	NANCAY	0.0822	999
5	06 33 31.1	+04 00 07	207.3245	-2.1504	IRAS 06308+0402			1667 MHz;	1667	11;25	50	NANCAY	0.0822	999
6	18 29 24.4	-15 15 56	16.8658	-2.1576	IRAS 18265-1517	Image		1667 MHz;	1667	-55;34	422	NANCAY	0.0822	999
7	18 30 35.3	-15 14 38	17.0169	-2.4004	IRAS 18277-1516			1667 MHz;	1667	-15;29	510	NANCAY	0.0822	999
8	20 14 26	+41 13 32	78.1221	3.6328	IRAS 20126+4104	Image		1667 MHz;	1667	-28;23	740	NANCAY	0.0822	999

DSS colored	2MASS colored	WISE colored
PACS color (70-160 um)	SPIRE color (250-500 um)	GLIMPSE 360
SDSS color	IRAC color I1,I2,I4	NVSS (1.4GHz)
ATLASGAL 870 um	ATLASGAL 870 um + Planck	Bolocam 1.1 mm

select MAX(oh_data_all.ra_hms) as ra_hms,MAX(oh_data_all.dec_dms) as dec_dms,MAX(oh_data_all.source_name) as source_name,MAX(oh_data_all.ra) as ra,MAX(oh_data_all.dec) as dec,MAX(oh_data_all.l) as l,MAX(oh_data_all.b) as b,MAX(oh_data_all.grp) as grp,MAX(oh_data_all.grpv) as grpv,MAX(oh_data_all.other_name) as other_name,MAX(oh_data_all.other_desc) as other_desc,BOOL_OR(thermal) as thermal,MAX(oh_data_all.line) as line,MAX(oh_data_all.freq) as freq,MAX(oh_data_all.pol) as pol,MAX(oh_data_all.vrange) as vrange,MAX(oh_data_all.vpeak) as vpeak,MAX(oh_data_all.peak) as peak,MAX(oh_data_all.fwhm) as fwhm,MAX(oh_data_all.int) as int,MAX(oh_data_all.rms) as rms,MAX(oh_data_all.units) as units,MAX(oh_data_all.units_rms) as units_rms,MAX(oh_data_all.date_txt) as date_txt,MAX(oh_data_all.telescope_ref) as telescope_ref,MAX(oh_data_all.telescope_conf) as telescope_conf,MAX(oh_data_all.v_step) as v_step,MAX(oh_data_all.beam) as beam,MAX(oh_data_all.beam_maj) as beam_maj,MAX(oh_data_all.beam_min) as beam_min,MAX(oh_data_all.beam_pa) as beam_pa,MAX(oh_data_all.ref) as ref,MAX(oh_data_all.list_ref) as list_ref,MAX(oh_data_all.ascii) as ascii,MAX(oh_data_all.url) as url,MAX(oh_data_all.image) as image,MAX(oh_data_all.image2) as image2,MAX(oh_data_all.image3) as image3,MAX(oh_data_all.descr) as descr,MAX(oh_data_all.id) as id,BOOL_OR(mjy_flag) as mjy_flag,BOOL_OR(rms_mjy_flag) as rms_mjy_flag,MAX(oh_data_all.dist) as dist,1 as dist_parallax,MAX(oh_data_all.date_txt) as date_txt,MAX(line_det) as line_det,MAX(type) as type,MAX(simbad_types_cat) as simbad_types_cat FROM oh_data_all  LEFT JOIN all_objects_withmet ON oh_data_all.grp=all_objects_withmet.group_name LEFT JOIN object_categories ON all_objects_withmet.group_name = object_categories.group_name_cat AND object_categories.tbl_cat = 'all_objects_withmet' LEFT JOIN transitions ON oh_data_all.line=transitions."Line"  WHERE ref ilike 'COL15B' AND detected=true AND hide=false GROUP BY ref

select oh_data_all.ra_hms,oh_data_all.dec_dms,oh_data_all.source_name,oh_data_all.ra,oh_data_all.dec,oh_data_all.l,oh_data_all.b,oh_data_all.grp,oh_data_all.grpv,oh_data_all.other_name,oh_data_all.other_desc,oh_data_all.thermal,oh_data_all.line,oh_data_all.freq,oh_data_all.pol,oh_data_all.vrange,oh_data_all.vpeak,oh_data_all.peak,oh_data_all.fwhm,oh_data_all.int,oh_data_all.rms,oh_data_all.units,oh_data_all.units_rms,oh_data_all.date_txt,oh_data_all.telescope_ref,oh_data_all.telescope_conf,oh_data_all.v_step,oh_data_all.beam,oh_data_all.beam_maj,oh_data_all.beam_min,oh_data_all.beam_pa,oh_data_all.ref,oh_data_all.list_ref,oh_data_all.ascii,oh_data_all.url,oh_data_all.image,oh_data_all.image2,oh_data_all.image3,oh_data_all.descr,oh_data_all.id,oh_data_all.mjy_flag,oh_data_all.rms_mjy_flag,oh_data_all.dist,oh_data_all.dist_parallax,oh_data_all.date_txt,line_det,type,simbad_types_cat FROM oh_data_all   LEFT JOIN all_objects_withmet ON oh_data_all.grp=all_objects_withmet.group_name LEFT JOIN object_categories ON all_objects_withmet.group_name = object_categories.group_name_cat AND object_categories.tbl_cat = 'all_objects_withmet' LEFT JOIN transitions ON oh_data_all.line=transitions."Line"  WHERE ref ilike 'COL15B' AND detected=true AND hide=false ORDER BY detected DESC,id

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COL15B - H2O and OH masers associated with cold infrared sources

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Detection table from Colom et al. (2015)

COL15B - H₂O and OH masers associated with cold infrared sources