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VLE08 - A new probe of magnetic fields during high-mass star formation. Zeeman splitting of 6.7 GHz methanol masers

Short title: Vlemmings (2008)
Authors: Vlemmings, W. H. T.
Journal: Astronomy and Astrophysics, Volume 484, Issue 3, 2008, pp.773-781
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (24 detection)
Target type: Known_Class_II
Transitions: CH3OH_6(II)

Abstract
Context: The role of magnetic fields during high-mass star formation is a matter of fierce debate, yet only a few direct probes of magnetic field strengths are available. Aims: The magnetic field is detected in a number of massive star-forming regions through polarization observations of 6.7 GHz methanol masers. Although these masers are the most abundant of the maser species occurring during high-mass star formation, most magnetic field measurements in the high-density gas currently come from OH and H2O maser observations. Methods: The 100-m Effelsberg telescope was used to measure the Zeeman splitting of 6.7 GHz methanol masers for the first time. The observations were performed on a sample of 24 bright northern maser sources. Results: Significant Zeeman splitting is detected in 17 of the sources with an average magnitude of 0.56 m s^-1. Using the current best estimate of the 6.7 GHz methanol maser Zeeman splitting coefficient and a geometrical correction, this corresponds to an absolute magnetic field strength of 23 mG in the methanol maser region. Conclusions: The magnetic field is dynamically important in the dense maser regions. No clear relation is found with the available OH maser magnetic field measurements. The general sense of direction of the magnetic field is consistent with other Galactic magnetic field measurements, although a few of the masers display a change of direction between different maser features. Due to the abundance of methanol masers, measuring their Zeeman splitting provides the opportunity to construct a comprehensive sample of magnetic fields in high-mass star-forming regions. Figures 6-8 are only available in electronic form at http://www.aanda.org

Abstract

Context: The role of magnetic fields during high-mass star formation is a matter of fierce debate, yet only a few direct probes of magnetic field strengths are available.
Aims: The magnetic field is detected in a number of massive star-forming regions through polarization observations of 6.7 GHz methanol masers. Although these masers are the most abundant of the maser species occurring during high-mass star formation, most magnetic field measurements in the high-density gas currently come from OH and H2O maser observations.
Methods: The 100-m Effelsberg telescope was used to measure the Zeeman splitting of 6.7 GHz methanol masers for the first time. The observations were performed on a sample of 24 bright northern maser sources.
Results: Significant Zeeman splitting is detected in 17 of the sources with an average magnitude of 0.56 m s^-1. Using the current best estimate of the 6.7 GHz methanol maser Zeeman splitting coefficient and a geometrical correction, this corresponds to an absolute magnetic field strength of 23 mG in the methanol maser region.
Conclusions: The magnetic field is dynamically important in the dense maser regions. No clear relation is found with the available OH maser magnetic field measurements. The general sense of direction of the magnetic field is consistent with other Galactic magnetic field measurements, although a few of the masers display a change of direction between different maser features. Due to the abundance of methanol masers, measuring their Zeeman splitting provides the opportunity to construct a comprehensive sample of magnetic fields in high-mass star-forming regions.

Figures 6-8 are only available in electronic form at http://www.aanda.org

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Detection table from Vlemmings (2008)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Other name	Image	Descr.	Line	V_peak	F_peak	∫F dv	Telescope	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)			Other name			CH₃OH (class II)	(km/s)	(Jy/beam)	(Jy/beam*km/s)		(arcsec)	Yes/No		(kpc)
1	18 06 14.7	-20 31 31.6	9.6212	0.1958	G9.621+0.195	G09.62+0.20		Image		6.6 GHz (II);	1	6757	3091	EFF	120	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		12 Nov. 2007
2	18 11 51.5	-17 31 28.8	12.8890	0.4891	G12.889+0.490	G12.89+0.49	IRAS 18089-1732	Image	Descr	6.6 GHz (II);	39	71	105	EFF	120	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		12 Nov. 2007
3	18 34 40.4	-09 00 38.3	23.0099	-0.4109	G23.010-0.411	G23.01-0.41		Image	Descr	6.6 GHz (II);	74.8	585	1016	EFF	120	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		12 Nov. 2007
4	18 38 3.2	-06 24 15	25.7095	0.0438	G25.709+0.044	G25.71+0.04		Image		6.6 GHz (II);	95.6	590	591	EFF	120	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		12 Nov. 2007
5	18 39 4.7	-06 24 17	25.8259	-0.1829	G25.826-0.178	G25.83-0.18		Image		6.6 GHz (II);	90.7	69	84	EFF	120	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		12 Nov. 2007
6	18 42 41	-04 15 21	28.1472	0.0032	G28.147-0.004	G28.15+0.00		Image		6.6 GHz (II);	101.3	30	24	EFF	120	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		12 Nov. 2007
7	18 48 12.4	-01 26 22.6	31.2823	0.0624	G31.280+0.062	G31.28+0.06	IRAS 18456-0129	Image	Descr	6.6 GHz (II);	110.4	74	174	EFF	120	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		12 Nov. 2007
8	18 49 37.3	-00 45 47	32.0458	0.0561	G32.045+0.059	G32.03+0.06	IRAS 18470-0050	Image		6.6 GHz (II);	98.7	69	81	EFF	120	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		12 Nov. 2007
9	18 53 28.7	+00 31 58	33.6387	-0.2110	G33.641-0.228	G33.64-0.21		Image	Descr	6.6 GHz (II);	58.6	63	54	EFF	120	+H₂O -CH₃OH I +CH₃OH II +OH	SFR		12 Nov. 2007
10	18 58 13	+01 40 37.5	35.1973	-0.7427	G35.197-0.743	G35.20-0.74	IRAS 18556+0136	Image	Descr	6.6 GHz (II);	30.5	169	167	EFF	120	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		12 Nov. 2007
11	19 01 45.6	+01 13 28	35.1992	-1.7373	G35.200-1.737	G35.20-1.74	W48	Image	Descr	6.6 GHz (II);	41.5	476	643	EFF	120	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		12 Nov. 2007
12	18 54 13.8	+04 41 32	37.4267	1.5182	G37.427+1.518	G37.40+1.52	IRAS 18517+0437	Image		6.6 GHz (II);	41	320	193	EFF	120	+H₂O +CH₃OH I +CH₃OH II	SFR		12 Nov. 2007
13	19 11 55.1	+09 36 00	43.7999	-0.1300	G43.795-0.127	G43.80-0.13	W49N	Image		6.6 GHz (II);	40	35	81	EFF	120	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		12 Nov. 2007
14	19 23 44.5	+14 30 31	49.4900	-0.3900	G49.488-0.387	G49.49-0.39	W51-e1/e2	Image	Descr	6.6 GHz (II);	59	1029	885	EFF	120	+H₂O +CH₃OH I +CH₃OH II +OH -SiO	SFR		12 Nov. 2007
15	20 10 9.1	+31 31 34.4	69.5398	-0.9758	G69.540-0.976	G69.52-0.97	ON 1	Image	Descr	6.6 GHz (II);	11.6	96	45	EFF	120	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		12 Nov. 2007
16	20 14 26	+41 13 33.4	78.1224	3.6329	G78.122+3.633	G78.10+3.64	IRAS 20126+4104	Image		6.6 GHz (II);	-6.1	60	77	EFF	120	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		12 Nov. 2007
17	20 38 36.4	+42 37 34.8	81.8713	0.7807	G81.876+0.782	G81.87+0.78	W75N	Image	Descr	6.6 GHz (II);	5	273	317	EFF	120	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		12 Nov. 2007
18	22 56 18.1	+62 01 49.4	109.8712	2.1142	G109.871+2.114	G109.86+2.10	Cepheus A	Image	Descr	6.6 GHz (II);	-4.2	364	484	EFF	120	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		12 Nov. 2007
19	23 13 45.4	+61 28 10.6	111.5421	0.7769	G111.542+0.769	G111.53+0.76	NGC 7538	Image	Descr	6.6 GHz (II);	-56.2	233	514	EFF	120	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		12 Nov. 2007
20	02 27 3.8	+61 52 24.6	133.9472	1.0641	G133.949+1.064	G133.94+1.04	W3(OH)	Image	Descr	6.6 GHz (II);	-44	3705	8198	EFF	120	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		12 Nov. 2007
21	05 39 13.1	+35 45 51.3	173.4817	2.4461	G173.481+2.446	G173.49+2.42	S231	Image		6.6 GHz (II);	-13	52	53	EFF	120	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		12 Nov. 2007
22	05 30 42	+33 47 14	174.1987	-0.0942	G174.198-0.076	G174.19-0.09	AFGL 5142	Image		6.6 GHz (II);	2.1	55	34	EFF	120	+H₂O +CH₃OH I +CH₃OH II	GALAXY		12 Nov. 2007
23	06 08 53.4	+21 38 28.7	188.9463	0.8860	G188.946+0.887	G188.95+0.89	IRAS 06058+2138	Image		6.6 GHz (II);	10.9	633	485	EFF	120	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		12 Nov. 2007
24	06 12 54	+17 59 23	192.6003	-0.0480	G192.599-0.048	G192.60-0.05	S255	Image		6.6 GHz (II);	5	94	78	EFF	120	+H₂O +CH₃OH I +CH₃OH II	SFR_MIXED		12 Nov. 2007

Distribution of sources in all sky (l,b)

Distribution of sources in all sky using Aladin

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Distribution of sources in IRAS color-color diagram

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Original color diagram is taken form van der Veen & Habing (1987)

Type	Description
I	Oxygen-rich non-variable stars without circumstellar shells
II	Variable stars with "young" O-rich circumstellar shells
IIIa	Variable stars with more evolved O-rich circumstellar shells
IIIb	Variable stars with thick O-rich circumstellar shells
IV	Variable stars with very thick O-rich circumstellar shells
V	Planetary nebulae and non- variable stars with very cool circumstellar shells
VIa	Variable stars with relatively cold dust at large distances; a significant part of the stars is carbon-rich
VIb	Variable stars with relatively hot dust close to the star and relatively cold dust at large distances; Some of the objects have proven to be O-rich
VII	Variable stars with more evolved C-rich circumstellar shells
VIII	Different sort of objects

Distribution of the detection velocities versus galactic longitude from VLE08

Tip: Use "Box select" or "Lasso select" to display velocity-selected sources in Aladin all-sky view