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PAT21 - New ex-OH maser detections in the northern celestial hemisphere

Short title: Patoka et al. (2021)
Authors: Patoka, O.Antyufeyev, O.Shmeld, I.Bezrukovs, V.Bleiders, M.Orbidans, A.Aberfelds, A.Shulga, V.
Journal: Astronomy & Astrophysics, Volume 652, id.A17, 6 pp.
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Target type: High_mass_SFR
Observations category: SF.general
Facility type: single-dish
Transitions: OH_6035

Abstract
Aims: Molecular masers, including methanol and hydroxyl masers, and in particular the ones in excited rotational states (ex-OH masers), are one of the most informative tools for studying star-forming regions. So, the discovery, of new maser sources in these regions is of great importance. Many studies and surveys of ex-OH maser sources have been carried out in the southern celestial hemisphere, but only a few have been done in the northern hemisphere. The specific aim of this work is to close this gap. Methods: The star-forming regions in the northern hemisphere with known active methanol masers were observed to search for new ex-OH maser sources with the 32 m and 16 m radio telescopes of the Ventspils International Radio Astronomy Centre (VIRAC). Results: Three OH maser lines in the excited state at the 6035 MHz in three northern hemisphere star-forming regions are detected. The maser 189.030+0.783 was previously known, but we suggest this maser is a possible variable. We confirm recent detections of the ex-OH masers 85.41+0.00 and 90.92+1.49 by other authors. The magnetic field strength in the masering regions is estimated by using right circular polarization and left circular polarization pair splitting. The high-velocity resolution provides us with an estimation of a comparatively small magnetic field strength for the 189.030+0.783 and 90.92+1.49 star-forming regions.

Abstract

Aims: Molecular masers, including methanol and hydroxyl masers, and in particular the ones in excited rotational states (ex-OH masers), are one of the most informative tools for studying star-forming regions. So, the discovery, of new maser sources in these regions is of great importance. Many studies and surveys of ex-OH maser sources have been carried out in the southern celestial hemisphere, but only a few have been done in the northern hemisphere. The specific aim of this work is to close this gap.
Methods: The star-forming regions in the northern hemisphere with known active methanol masers were observed to search for new ex-OH maser sources with the 32 m and 16 m radio telescopes of the Ventspils International Radio Astronomy Centre (VIRAC).
Results: Three OH maser lines in the excited state at the 6035 MHz in three northern hemisphere star-forming regions are detected. The maser 189.030+0.783 was previously known, but we suggest this maser is a possible variable. We confirm recent detections of the ex-OH masers 85.41+0.00 and 90.92+1.49 by other authors. The magnetic field strength in the masering regions is estimated by using right circular polarization and left circular polarization pair splitting. The high-velocity resolution provides us with an estimation of a comparatively small magnetic field strength for the 189.030+0.783 and 90.92+1.49 star-forming regions.

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Detection table from Patoka et al. (2021)

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ID	Obs. RA	Obs. Dec	l	b	Group id	grpv	Source name	Image	Descr.	Line	Frequency	Polarization	V_peak	FWHM	F_peak	∫F dv	Telescope	RMS	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)						OH	(MHz)		(km/s)	(km/s)	(Jy)	(Jy*km/s)		(Jy)	(arcsec)	Yes/No		(kpc)
1	06 08 40.7	+21 31 07	189.0297	0.7835	G189.032+0.784	G189.0316+0.7837	189.030+0.783	Image	Descr	6035 MHz;	6035	LCP	3.413	0.33	1.36	0.48	RT-32	125.000	360	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		16.01.2020
	06 08 40.7	+21 31 07	189.0297	0.7835	G189.032+0.784	G189.0316+0.7837	189.030+0.783	Image	Descr	6035 MHz;	6035	LCP	3.413	0.33	1.36	0.48	RT-32	125.000	360	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		16.01.2020
	06 08 40.7	+21 31 07	189.0297	0.7835	G189.032+0.784	G189.0316+0.7837	189.030+0.783	Image		6035 MHz;	6035	RCP	3.398	0.295	2.33	0.73	RT-32	142.000	360	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		16.01.2020
	06 08 40.7	+21 31 07	189.0297	0.7835	G189.032+0.784	G189.0316+0.7837	189.030+0.783	Image		6035 MHz;	6035	RCP	3.398	0.295	2.33	0.73	RT-32	142.000	360	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		16.01.2020
5	20 54 13.7	+44 54 6.8	85.4102	0.0032	G85.410+0.003	G85.4103+0.0031	85.41+0.00	Image	Descr	6035 MHz;	6035	LCP	-32.775	0.36	0.797	0.307	RT-32	85.000	360	+H₂O -CH₃OH I +CH₃OH II +OH	SFR		17.01.2020
	20 54 13.7	+44 54 6.8	85.4102	0.0032	G85.410+0.003	G85.4103+0.0031	85.41+0.00	Image	Descr	6035 MHz;	6035	LCP	-32.775	0.36	0.797	0.307	RT-32	85.000	360	+H₂O -CH₃OH I +CH₃OH II +OH	SFR		17.01.2020
	20 54 13.7	+44 54 6.8	85.4102	0.0032	G85.410+0.003	G85.4103+0.0031	85.41+0.00	Image		6035 MHz;	6035	RCP	-32.899	0.338	1.823	0.667	RT-32	92.000	360	+H₂O -CH₃OH I +CH₃OH II +OH	SFR		17.01.2020
	20 54 13.7	+44 54 6.8	85.4102	0.0032	G85.410+0.003	G85.4103+0.0031	85.41+0.00	Image		6035 MHz;	6035	RCP	-32.899	0.338	1.823	0.667	RT-32	92.000	360	+H₂O -CH₃OH I +CH₃OH II +OH	SFR		17.01.2020
9	21 09 12.6	+50 01 2.9	90.9207	1.4872	G90.921+1.507	G90.9211+1.4866	90.92+1.49	Image	Descr	6035 MHz;	6035	LCP	-69.15	0.64	0.9	0.62	RT-32	161.000	360	+OH	SFR		24.12.2019
	21 09 12.6	+50 01 2.9	90.9207	1.4872	G90.921+1.507	G90.9211+1.4866	90.92+1.49	Image	Descr	6035 MHz;	6035	LCP	-69.15	0.64	0.9	0.62	RT-32	161.000	360	+OH	SFR		24.12.2019
	21 09 12.6	+50 01 2.9	90.9207	1.4872	G90.921+1.507	G90.9211+1.4866	90.92+1.49	Image		6035 MHz;	6035	RCP	-69.136	0.39	2.17	0.88	RT-32	164.000	360	+OH	SFR		24.12.2019
	21 09 12.6	+50 01 2.9	90.9207	1.4872	G90.921+1.507	G90.9211+1.4866	90.92+1.49	Image		6035 MHz;	6035	RCP	-69.136	0.39	2.17	0.88	RT-32	164.000	360	+OH	SFR		24.12.2019

Non-detection table from Patoka et al. (2021)