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FIS05B - Magnetic Field Clumping in Massive Star-forming Regions as Determined from Excited-State OH Absorption and Maser Emission

Short title: Fish et al. (2005B)
Authors: Fish, Vincent L.Reid, Mark J.Menten, Karl M.
Journal: The Astrophysical Journal, Volume 623, Issue 1, pp. 269-279.
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Target type: High_mass_SFR
Observations category: SF.general
Facility type: single-dish
Transitions: OH_13441,OH_13435

Abstract
We have observed six high-mass-star-forming regions in the ²Î�_3/2, J=7/2 lines of OH using the Green Bank Telescope (GBT) in order to investigate whether the magnetic field, and hence the density, measured in absorption differs from that implied by maser Zeeman splitting. We detect absorption in both the 13,441 and 13,434 MHz main lines in all six sources. Zeeman splitting in the F=3⁺-->3^- absorption line in W3(OH) implies a line-of-sight magnetic field strength of 3.0+/-0.3 mG. This is significantly less than full magnetic field strengths detected from OH maser Zeeman splitting, suggesting that OH maser regions may be denser than the nonmasing OH material by a factor of several. Zeeman splitting is not detected in other sources, but we are able to place upper limits on B_âˆ¥ of 1.2 mG in G10.624-0.385 and 2.9 mG in K3-50. These results are consistent with a density enhancement of the masers, but other explanations for the lower magnetic field in absorption compared to maser emission are possible for these two sources. Absorption in one or both of the 13,442 and 13,433 MHz satellite lines is also seen in four sources. This is the very first detection of the ²Î�_3/2, J=7/2 satellite lines. Ratios of satellite-line to main-line absorption suggest enhancement of the satellite lines from local thermodynamic equilibrium values. Masers are seen in the F=4⁺-->4^- and 3⁺-->3^- transitions of W3(OH) and the 4⁺-->4^- transition of ON 1. A previously undetected 4⁺-->4^- maser is seen near -44.85 km s^-1 in W3(OH).

Abstract

We have observed six high-mass-star-forming regions in the ²Î�_3/2, J=7/2 lines of OH using the Green Bank Telescope (GBT) in order to investigate whether the magnetic field, and hence the density, measured in absorption differs from that implied by maser Zeeman splitting. We detect absorption in both the 13,441 and 13,434 MHz main lines in all six sources. Zeeman splitting in the F=3⁺-->3^- absorption line in W3(OH) implies a line-of-sight magnetic field strength of 3.0+/-0.3 mG. This is significantly less than full magnetic field strengths detected from OH maser Zeeman splitting, suggesting that OH maser regions may be denser than the nonmasing OH material by a factor of several. Zeeman splitting is not detected in other sources, but we are able to place upper limits on B_âˆ¥ of 1.2 mG in G10.624-0.385 and 2.9 mG in K3-50. These results are consistent with a density enhancement of the masers, but other explanations for the lower magnetic field in absorption compared to maser emission are possible for these two sources. Absorption in one or both of the 13,442 and 13,433 MHz satellite lines is also seen in four sources. This is the very first detection of the ²Î�_3/2, J=7/2 satellite lines. Ratios of satellite-line to main-line absorption suggest enhancement of the satellite lines from local thermodynamic equilibrium values. Masers are seen in the F=4⁺-->4^- and 3⁺-->3^- transitions of W3(OH) and the 4⁺-->4^- transition of ON 1. A previously undetected 4⁺-->4^- maser is seen near -44.85 km s^-1 in W3(OH).

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Detection table from Fish et al. (2005B)

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ID	Obs. RA	Obs. Dec	l	b	Group id	grpv	Source name	Line	Frequency	Polarization	V_peak	F_peak	Telescope	RMS	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)				OH	(MHz)		(km/s)	(Jy)		(Jy)	(arcsec)	Yes/No		(kpc)
1	02 27 3.7	+61 52 25.4	133.9470	1.0643	G133.947+1.064	G133.9475+1.0642	W3(OH)	13435 MHz;	13435	LCP	-42.53	0.088	GBT	0.020	55	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2004 April 11-12
	02 27 3.7	+61 52 25.4	133.9470	1.0643	G133.947+1.064	G133.9475+1.0642	W3(OH)	13435 MHz;	13435	RCP	-42.29	0.088	GBT	0.020	55	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2004 April 11-12
3	02 27 3.7	+61 52 25.4	133.9470	1.0643	G133.947+1.064	G133.9475+1.0642	W3(OH)	13441 MHz;	13441	LCP	-44.94	1.135	GBT	0.020	55	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2004 April 11-12
	02 27 3.7	+61 52 25.4	133.9470	1.0643	G133.947+1.064	G133.9475+1.0642	W3(OH)	13441 MHz;	13441	RCP	-44.75	1.071	GBT	0.020	55	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2004 April 11-12
	02 27 3.7	+61 52 25.4	133.9470	1.0643	G133.947+1.064	G133.9475+1.0642	W3(OH)	13441 MHz;	13441	LCP	-43.97	2.359	GBT	0.020	55	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2004 April 11-12
	02 27 3.7	+61 52 25.4	133.9470	1.0643	G133.947+1.064	G133.9475+1.0642	W3(OH)	13441 MHz;	13441	RCP	-43.84	0.329	GBT	0.020	55	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2004 April 11-12
	02 27 3.7	+61 52 25.4	133.9470	1.0643	G133.947+1.064	G133.9475+1.0642	W3(OH)	13441 MHz;	13441	LCP	-43.66	5.747	GBT	0.020	55	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2004 April 11-12
	02 27 3.7	+61 52 25.4	133.9470	1.0643	G133.947+1.064	G133.9475+1.0642	W3(OH)	13441 MHz;	13441	RCP	-43.54	4.129	GBT	0.020	55	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2004 April 11-12
	02 27 3.7	+61 52 25.4	133.9470	1.0643	G133.947+1.064	G133.9475+1.0642	W3(OH)	13441 MHz;	13441	RCP	-43.51	3.659	GBT	0.020	55	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2004 April 11-12
	02 27 3.7	+61 52 25.4	133.9470	1.0643	G133.947+1.064	G133.9475+1.0642	W3(OH)	13441 MHz;	13441	LCP	-43.33	7.241	GBT	0.020	55	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2004 April 11-12
	02 27 3.7	+61 52 25.4	133.9470	1.0643	G133.947+1.064	G133.9475+1.0642	W3(OH)	13441 MHz;	13441	RCP	-43.19	7.271	GBT	0.020	55	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2004 April 11-12
	02 27 3.7	+61 52 25.4	133.9470	1.0643	G133.947+1.064	G133.9475+1.0642	W3(OH)	13441 MHz;	13441	LCP	-43.08	36.853	GBT	0.020	55	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2004 April 11-12
	02 27 3.7	+61 52 25.4	133.9470	1.0643	G133.947+1.064	G133.9475+1.0642	W3(OH)	13441 MHz;	13441	RCP	-42.93	37.218	GBT	0.020	55	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2004 April 11-12
	02 27 3.7	+61 52 25.4	133.9470	1.0643	G133.947+1.064	G133.9475+1.0642	W3(OH)	13441 MHz;	13441	LCP	-42.46	37.941	GBT	0.020	55	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2004 April 11-12
	02 27 3.7	+61 52 25.4	133.9470	1.0643	G133.947+1.064	G133.9475+1.0642	W3(OH)	13441 MHz;	13441	RCP	-42.26	37.265	GBT	0.020	55	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2004 April 11-12
16	20 10 9.1	+31 31 35.2	69.5399	-0.9756	G69.540-0.976	G69.5399-0.9757	ON 1	13441 MHz;	13441	LCP	14.09	0.653	GBT	0.020	55	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2004 April 11-12
	20 10 9.1	+31 31 35.2	69.5399	-0.9756	G69.540-0.976	G69.5399-0.9757	ON 1	13441 MHz;	13441	RCP	14.02	0.671	GBT	0.020	55	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2004 April 11-12
	20 10 9.1	+31 31 35.2	69.5399	-0.9756	G69.540-0.976	G69.5399-0.9757	ON 1	13441 MHz;	13441	LCP	0.38	0.041	GBT	0.020	55	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2004 April 11-12
	20 10 9.1	+31 31 35.2	69.5399	-0.9756	G69.540-0.976	G69.5399-0.9757	ON 1	13441 MHz;	13441	RCP	0.24	0.035	GBT	0.020	55	+H₂O +CH₃OH I +CH₃OH II +OH	SFR		2004 April 11-12

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(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 'FIS05B' 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 'FIS05B' AND detected=true AND hide=false ORDER BY detected DESC,id

Display data from paper

FIS05B - Magnetic Field Clumping in Massive Star-forming Regions as Determined from Excited-State OH Absorption and Maser Emission

View as list of objects

Detection table from Fish et al. (2005B)