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SUR11 - The structure of the magnetic field in the massive star-forming region W75N

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Short title: Surcis et al. (2011)
Authors: Surcis, G.Vlemmings, W. H. T.Curiel, S.Hutawarakorn Kramer, B.Torrelles, J. M.Sarma, A. P.
Journal: Astronomy & Astrophysics, Volume 527, id.A48, 10 pp.
Bibcode:

Target type: High_mass_SFR

Abstract
Context. A debated topic in star formation theory is the role of magnetic fields during the protostellar phase of high-mass stars. It is still unclear how magnetic fields influence the formation and dynamics of massive disks and outflows. Most current information on magnetic fields close to high-mass protostars comes from polarized maser emissions, which allows us to investigate the magnetic field on small scales by using very long-baseline interferometry. Aims: The massive star-forming region W75N contains three radio continuum sources (VLA 1, VLA 2, and VLA 3), at three different evolutionary stages, and associated masers, while a large-scale molecular bipolar outflow is also present. Very recently, polarization observations of the 6.7 GHz methanol masers at milliarsecond resolution have been able to probe the strength and structure of the magnetic field over more than 2000 AU around VLA 1. The magnetic field is parallel to the outflow, suggesting that VLA 1 is its powering source. The observations of H₂O masers at 22 GHz can give more information about the gas dynamics and the magnetic fields around VLA 1 and VLA 2. Methods: The NRAO Very Long Baseline Array was used to measure the linear polarization and the Zeeman-splitting of the 22 GHz water masers in the star-forming region W75N. Results: We detected 124 water masers, 36 around VLA 1 and 88 around VLA 2 of W75N, which indicate two different physical environments around the two sources, where VLA 1 is in a more evolved state. The linear polarization of the masers confirms the tightly ordered magnetic field around VLA 1, which is aligned with the large-scale molecular outflow, and also reveals an ordered magnetic field around VLA 2, which is not parallel to the outflow. The Zeeman-splitting measured on 20 of the masers indicates strong magnetic fields around both sources (the averaged values are B_VLA1 ~ 700 mG and B_VLA2 ~ 1700 mG). The high values of the magnetic field strengths, which come from the shock compression of the gas, are consistent with the methanol and OH magnetic field strengths. Moreover, by studying the maser properties we were also able to determine that the water masers are pumped in C-shocks in both sources.

Abstract

Context. A debated topic in star formation theory is the role of magnetic fields during the protostellar phase of high-mass stars. It is still unclear how magnetic fields influence the formation and dynamics of massive disks and outflows. Most current information on magnetic fields close to high-mass protostars comes from polarized maser emissions, which allows us to investigate the magnetic field on small scales by using very long-baseline interferometry.
Aims: The massive star-forming region W75N contains three radio continuum sources (VLA 1, VLA 2, and VLA 3), at three different evolutionary stages, and associated masers, while a large-scale molecular bipolar outflow is also present. Very recently, polarization observations of the 6.7 GHz methanol masers at milliarsecond resolution have been able to probe the strength and structure of the magnetic field over more than 2000 AU around VLA 1. The magnetic field is parallel to the outflow, suggesting that VLA 1 is its powering source. The observations of H₂O masers at 22 GHz can give more information about the gas dynamics and the magnetic fields around VLA 1 and VLA 2.
Methods: The NRAO Very Long Baseline Array was used to measure the linear polarization and the Zeeman-splitting of the 22 GHz water masers in the star-forming region W75N.
Results: We detected 124 water masers, 36 around VLA 1 and 88 around VLA 2 of W75N, which indicate two different physical environments around the two sources, where VLA 1 is in a more evolved state. The linear polarization of the masers confirms the tightly ordered magnetic field around VLA 1, which is aligned with the large-scale molecular outflow, and also reveals an ordered magnetic field around VLA 2, which is not parallel to the outflow. The Zeeman-splitting measured on 20 of the masers indicates strong magnetic fields around both sources (the averaged values are B_VLA1 ~ 700 mG and B_VLA2 ~ 1700 mG). The high values of the magnetic field strengths, which come from the shock compression of the gas, are consistent with the methanol and OH magnetic field strengths. Moreover, by studying the maser properties we were also able to determine that the water masers are pumped in C-shocks in both sources.

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Detection table from Surcis et al. (2011)

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ID	Obs. RA	Obs. Dec	RA offset	Dec offset	l	b	Group id	#	Source name	Image	Descr.	Line	V_peak	F_peak	Telescope	V_step	RMS	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(mas)	(mas)	(deg.)	(deg.)						H₂O	(km/s)	(Jy/beam)		(km/s)	(mJy/beam)	(arcsec)	Yes/No		(kpc)
1	+20 38 36.4	+42 37 35.2			81.8713	0.780773	G81.871+0.781		W75N	Image	Descr	22 GHz;	-7.7 .. 23.8	0.39 .. 198.45	VLBA	0.027	7.300	0.002 x 0.0007	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		2005 Nov 21
	+20 38 36.3937	+42 37 34.8953	-95.3612 mas	-303.062 mas	81.871222	0.780737		1	W75N				10.7	2.76 (0.13)
	+20 38 36.3938	+42 37 34.8979	-94.2666 mas	-300.461 mas	81.871222	0.780737		2	W75N				10.5	3.39 (0.09)
	+20 38 36.394	+42 37 34.9087	-91.6984 mas	-289.684 mas	81.871225	0.780739		3	W75N				11.3	30.78 (0.19)
	+20 38 36.3953	+42 37 34.9808	-72.0367 mas	-217.556 mas	81.871243	0.780748		4	W75N				10.7	9.77 (0.13)
	+20 38 36.3953	+42 37 34.9839	-71.5315 mas	-214.531 mas	81.871244	0.780748		5	W75N				10.6	115.41 (0.12)
	+20 38 36.3953	+42 37 34.985	-71.321 mas	-213.371 mas	81.871244	0.780748		6	W75N				10.8	76.79 (0.12)
	+20 38 36.3954	+42 37 34.9881	-70.4789 mas	-210.289 mas	81.871245	0.780749		7	W75N				11.1	10.16 (0.12)
	+20 38 36.3954	+42 37 34.9915	-69.5948 mas	-206.944 mas	81.871246	0.780749		8	W75N				11.5	158.28 (0.20)
	+20 38 36.3993	+42 37 35.0771	-11.7886 mas	-121.338 mas	81.871272	0.780754		9	W75N				10.4	6.14 (0.06)
	+20 38 36.3993	+42 37 34.9607	-11.4097 mas	-237.705 mas	81.871246	0.780735		10	W75N				11.4	2.07 (0.20)
	+20 38 36.3994	+42 37 35.079	-9.7679 mas	-119.442 mas	81.871273	0.780754		11	W75N				10.3	0.39 (0.03)
	+20 38 36.3999	+42 37 35.1827	-2.7366 mas	-15.713 mas	81.871296	0.780771		12	W75N				12.8	1.13 (0.03)
	+20 38 36.3999	+42 37 35.184	-2.6945 mas	-14.427 mas	81.871297	0.780771		13	W75N				12.8	0.97 (0.03)
	+20 38 36.3999	+42 37 35.2	-2.6945 mas	1.568 mas	81.871300	0.780774		14	W75N				12.6	80.02 (0.07)
	+20 38 36.4	+42 37 35.1621	-0.5894 mas	-36.27 mas	81.871292	0.780767		15	W75N				11.6	63.25 (0.17)
	+20 38 36.4001	+42 37 35.1629	-0.421 mas	-35.545 mas	81.871292	0.780767		16	W75N				11.4	111.47 (0.20)
	+20 38 36.4001	+42 37 35.1984	0 mas	0 mas	81.871300	0.780773		17	W75N				12.7	2.96 (0.06)
	+20 38 36.4006	+42 37 35.2296	8.252 mas	31.166 mas	81.871308	0.780777		18	W75N				12.4	6.17 (0.06)
	+20 38 36.4006	+42 37 35.2314	8.2941 mas	33.016 mas	81.871309	0.780777		19	W75N				12.6	11.39 (0.07)
	+20 38 36.4025	+42 37 34.9677	36.292 mas	-230.717 mas	81.871254	0.780728		20	W75N				8.1	1.86 (0.02)
	+20 38 36.4039	+42 37 35.2163	57.6378 mas	17.914 mas	81.871311	0.780767		21	W75N				11.2	3.56 (0.15)
	+20 38 36.4057	+42 37 35.2413	84.3726 mas	42.854 mas	81.871320	0.780766		22	W75N				9.8	6.71 (0.05)
	+20 38 36.4198	+42 37 35.4796	295.388 mas	281.223 mas	81.871399	0.780772		23	W75N				21.1	39.41 (0.05)
	+20 38 36.4222	+42 37 35.5146	332.438 mas	316.208 mas	81.871411	0.780772		24	W75N				21.7	2.00 (0.04)
	+20 38 36.4339	+42 37 35.3204	507.583 mas	121.956 mas	81.871390	0.780711		25	W75N				23.8	1.33 (0.03)
	+20 38 36.4382	+42 37 34.7097	571.41 mas	-488.743 mas	81.871263	0.780598		26	W75N				5.2	1.69 (0.01)
	+20 38 36.4382	+42 37 34.7111	571.957 mas	-487.32 mas	81.871264	0.780598		27	W75N				5	2.82 (0.01)
	+20 38 36.4392	+42 37 34.5764	587.493 mas	-621.986 mas	81.871236	0.780573		28	W75N				6.8	12.0 (0.05)
	+20 38 36.4403	+42 37 34.5867	602.691 mas	-611.675 mas	81.871240	0.780572		29	W75N				12.7	6.86 (0.06)
	+20 38 36.4404	+42 37 34.5778	604.375 mas	-620.571 mas	81.871238	0.780570		30	W75N				10.9	4.62 (0.12)
	+20 38 36.4405	+42 37 35.4107	605.681 mas	212.257 mas	81.871422	0.780710		31	W75N				18.7	20.73 (0.04)
	+20 38 36.4418	+42 37 34.744	625.258 mas	-454.392 mas	81.871278	0.780595		32	W75N				11.2	25.44 (0.16)
	+20 38 36.4452	+42 37 34.7661	676.454 mas	-432.327 mas	81.871289	0.780590		33	W75N				6	1.95 (0.08)
	+20 38 36.4452	+42 37 34.7659	677.044 mas	-432.545 mas	81.871289	0.780590		34	W75N				6.2	4.65 (0.01)
	+20 38 36.4461	+42 37 34.759	690.053 mas	-439.411 mas	81.871289	0.780587		35	W75N				9.6	30.29 (0.06)
	+20 38 36.4461	+42 37 34.7582	690.727 mas	-440.163 mas	81.871289	0.780586		36	W75N				9.7	48.76 (0.06)
	+20 38 36.4466	+42 37 34.7388	697.168 mas	-459.564 mas	81.871285	0.780582		37	W75N				-1.1	13.99 (0.04)
	+20 38 36.4466	+42 37 34.7383	697.421 mas	-460.125 mas	81.871285	0.780582		38	W75N				-2.9	3.25 (0.01)
	+20 38 36.4466	+42 37 34.7397	697.884 mas	-458.71 mas	81.871286	0.780582		39	W75N				0.5	7.16 (0.01)
	+20 38 36.4467	+42 37 34.7524	698.6 mas	-445.961 mas	81.871289	0.780584		40	W75N				7.2	62.39 (0.07)
	+20 38 36.4467	+42 37 34.7367	698.937 mas	-461.704 mas	81.871285	0.780581		41	W75N				-0.7	49.20 (0.05)
	+20 38 36.4467	+42 37 34.7516	699.316 mas	-446.842 mas	81.871288	0.780584		42	W75N				6.8	30.98 (0.05)
	+20 38 36.4468	+42 37 34.7504	701.505 mas	-448.017 mas	81.871288	0.780583		43	W75N				8.3	12.73 (0.05)
	+20 38 36.4469	+42 37 34.749	702.389 mas	-449.426 mas	81.871288	0.780583		44	W75N				9.3	4.32 (0.03)
	+20 38 36.447	+42 37 34.7473	703.484 mas	-451.126 mas	81.871288	0.780583		45	W75N				11.6	39.57 (0.17)
	+20 38 36.447	+42 37 34.7469	703.863 mas	-451.496 mas	81.871288	0.780582		46	W75N				11.2	72.56 (0.16)
	+20 38 36.4471	+42 37 34.7399	705.505 mas	-458.549 mas	81.871287	0.780581		47	W75N				0.2	2.48 (0.01)
	+20 38 36.4474	+42 37 34.7399	709.967 mas	-458.458 mas	81.871287	0.780580		48	W75N				5	4.02 (0.01)
	+20 38 36.4474	+42 37 34.7393	710.389 mas	-459.141 mas	81.871287	0.780580		49	W75N				4.9	1.34 (0.01)
	+20 38 36.4475	+42 37 34.7405	711.02 mas	-457.901 mas	81.871287	0.780580		50	W75N				8.7	198.45 (0.20)
	+20 38 36.4476	+42 37 34.7318	713.041 mas	-466.595 mas	81.871286	0.780578		51	W75N				13.7	16.74 (0.02)
	+20 38 36.4478	+42 37 34.7231	716.03 mas	-475.323 mas	81.871284	0.780576		52	W75N				-7.7	53.72 (0.06)
	+20 38 36.4519	+42 37 34.7511	777.794 mas	-447.278 mas	81.871298	0.780571		53	W75N				-7.7	0.67 (0.06)

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
UKIDSS K Download UKIDSS K FITS	2MASS K Download 2MASS K FITS

select MAX(h2o_data_all.ra_hms) as ra_hms,MAX(h2o_data_all.dec_dms) as dec_dms,MAX(h2o_data_all.source_name) as source_name,MAX(h2o_data_all.ra) as ra,MAX(h2o_data_all.dec) as dec,MAX(h2o_data_all.l) as l,MAX(h2o_data_all.b) as b,MAX(h2o_data_all.grp) as grp,MAX(h2o_data_all.other_name) as other_name,MAX(h2o_data_all.other_desc) as other_desc,BOOL_OR(thermal) as thermal,MAX(h2o_data_all.line) as line,MAX(h2o_data_all.vrange) as vrange,MAX(h2o_data_all.vpeak) as vpeak,MAX(h2o_data_all.peak) as peak,MAX(h2o_data_all.fwhm) as fwhm,MAX(h2o_data_all.int) as int,MAX(h2o_data_all.rms) as rms,MAX(h2o_data_all.units) as units,MAX(h2o_data_all.units_rms) as units_rms,MAX(h2o_data_all.date_txt) as date_txt,MAX(h2o_data_all.telescope_ref) as telescope_ref,MAX(h2o_data_all.telescope_conf) as telescope_conf,MAX(h2o_data_all.v_step) as v_step,MAX(h2o_data_all.beam) as beam,MAX(h2o_data_all.beam_maj) as beam_maj,MAX(h2o_data_all.beam_min) as beam_min,MAX(h2o_data_all.beam_pa) as beam_pa,MAX(h2o_data_all.ref) as ref,MAX(h2o_data_all.list_ref) as list_ref,MAX(h2o_data_all.ascii) as ascii,MAX(h2o_data_all.url) as url,MAX(h2o_data_all.image) as image,MAX(h2o_data_all.image2) as image2,MAX(h2o_data_all.image3) as image3,MAX(h2o_data_all.descr) as descr,MAX(h2o_data_all.id) as id,BOOL_OR(mjy_flag) as mjy_flag,BOOL_OR(rms_mjy_flag) as rms_mjy_flag,MAX(h2o_data_all.dist) as dist,1 as dist_parallax,MAX(h2o_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 h2o_data_all  LEFT JOIN all_objects_withmet ON h2o_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 h2o_data_all.line=transitions."Line"  WHERE ref ilike 'SUR11' AND detected=true AND hide=false GROUP BY ref

select h2o_data_all.ra_hms,h2o_data_all.dec_dms,h2o_data_all.source_name,h2o_data_all.ra,h2o_data_all.dec,h2o_data_all.l,h2o_data_all.b,h2o_data_all.grp,h2o_data_all.other_name,h2o_data_all.other_desc,h2o_data_all.thermal,h2o_data_all.line,h2o_data_all.vrange,h2o_data_all.vpeak,h2o_data_all.peak,h2o_data_all.fwhm,h2o_data_all.int,h2o_data_all.rms,h2o_data_all.units,h2o_data_all.units_rms,h2o_data_all.date_txt,h2o_data_all.telescope_ref,h2o_data_all.telescope_conf,h2o_data_all.v_step,h2o_data_all.beam,h2o_data_all.beam_maj,h2o_data_all.beam_min,h2o_data_all.beam_pa,h2o_data_all.ref,h2o_data_all.list_ref,h2o_data_all.ascii,h2o_data_all.url,h2o_data_all.image,h2o_data_all.image2,h2o_data_all.image3,h2o_data_all.descr,h2o_data_all.id,h2o_data_all.mjy_flag,h2o_data_all.rms_mjy_flag,h2o_data_all.dist,h2o_data_all.dist_parallax,h2o_data_all.date_txt,line_det,type,simbad_types_cat FROM h2o_data_all   LEFT JOIN all_objects_withmet ON h2o_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 h2o_data_all.line=transitions."Line"  WHERE ref ilike 'SUR11' AND detected=true AND hide=false ORDER BY detected DESC,id

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SUR11 - The structure of the magnetic field in the massive star-forming region W75N

Interferometry data

View as list of objects

Detection table from Surcis et al. (2011)