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SUR14 - The magnetic field at milliarcsecond resolution around IRAS 20126+4104

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Short title: Surcis et al. (2014)
Authors: Surcis, G.Vlemmings, W. H. T.van Langevelde, H. J.Moscadelli, L.Hutawarakorn Kramer, B.
Journal: Astronomy & Astrophysics, Volume 563, id.A30, 8 pp.
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Target type: High_mass_SFR
Observations category: polarization
Facility type: interferometer

Abstract
Context. IRAS 20126+4104 is a well studied B0.5 protostar that is surrounded by a ~1000 au Keplerian disk and is where a large-scale outflow originates. Both 6.7-GHz CH₃OH masers and 22-GHz H₂O masers have been detected toward this young stellar object. The CH₃OH masers trace the Keplerian disk, while the H₂O masers are associated with the surface of the conical jet. Recently, observations of dust polarized emission (350 Î¼m) at an angular resolution of 9 arcsec (~15 000 au) have revealed an S-shaped morphology of the magnetic field around IRAS 20126+4104. Aims: The observations of polarized maser emissions at milliarcsecond resolution (~20 au) can make a crucial contribution to understanding the orientation of the magnetic field close to IRAS 20126+4104. This will allow us to determine whether the magnetic field morphology changes from arcsecond resolution to milliarcsecond resolution. Methods: The European VLBI Network was used to measure the linear polarization and the Zeeman splitting of the 6.7-GHz CH₃OH masers toward IRAS 20126+4104. The NRAO Very Long Baseline Array was used to measure the linear polarization and the Zeeman splitting of the 22-GHz H₂O masers toward the same region. Results: We detected 26 CH₃OH masers and 5 H₂O masers at high angular resolution. Linear polarization emission was observed toward three CH₃OH masers and toward one H₂O maser. Significant Zeeman splitting was measured in one CH₃OH maser (Î�V_Z = -9.2 Â� 1.4 m s^-1). No significant (5Ïƒ) magnetic field strength was measured using the H₂O masers. We found that in IRAS 20126+4104 the rotational energy is less than the magnetic energy.

Abstract

Context. IRAS 20126+4104 is a well studied B0.5 protostar that is surrounded by a ~1000 au Keplerian disk and is where a large-scale outflow originates. Both 6.7-GHz CH₃OH masers and 22-GHz H₂O masers have been detected toward this young stellar object. The CH₃OH masers trace the Keplerian disk, while the H₂O masers are associated with the surface of the conical jet. Recently, observations of dust polarized emission (350 Î¼m) at an angular resolution of 9 arcsec (~15 000 au) have revealed an S-shaped morphology of the magnetic field around IRAS 20126+4104.
Aims: The observations of polarized maser emissions at milliarcsecond resolution (~20 au) can make a crucial contribution to understanding the orientation of the magnetic field close to IRAS 20126+4104. This will allow us to determine whether the magnetic field morphology changes from arcsecond resolution to milliarcsecond resolution.
Methods: The European VLBI Network was used to measure the linear polarization and the Zeeman splitting of the 6.7-GHz CH₃OH masers toward IRAS 20126+4104. The NRAO Very Long Baseline Array was used to measure the linear polarization and the Zeeman splitting of the 22-GHz H₂O masers toward the same region.
Results: We detected 26 CH₃OH masers and 5 H₂O masers at high angular resolution. Linear polarization emission was observed toward three CH₃OH masers and toward one H₂O maser. Significant Zeeman splitting was measured in one CH₃OH maser (Î�V_Z = -9.2 Â� 1.4 m s^-1). No significant (5Ïƒ) magnetic field strength was measured using the H₂O masers. We found that in IRAS 20126+4104 the rotational energy is less than the magnetic energy.

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Detection table from Surcis et al. (2014)

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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	PA	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(mas)	(mas)	(deg.)	(deg.)						H₂O	(km/s)	(Jy/beam)		(km/s)	(mJy/beam)	(arcsec)	(deg.)	Yes/No		(kpc)
1	+20 14 25.966	+41 13 32.738			78.122167	3.633031	G78.122+3.633		IRAS 20126+4104	Image	Descr	22 GHz;	-15.51 .. -2.05	0.19 .. 24.77	VLBA	0.003	20.000	0.00075 x 0.00034	-9.4	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		2012 Jun 24
	+20 14 25.966	+41 13 32.7389	-0.818 mas	-0.656 mas	78.122167	3.633032		1	IRAS 20126+4104				-2.05	0.37 (0.05)
	+20 14 25.9661	+41 13 32.7396	0 mas	0 mas	78.122168	3.633031		2	IRAS 20126+4104				-4.61	24.77 (0.06)
	+20 14 25.993	+41 13 32.5276	403.317 mas	-212.02 mas	78.122165	3.632929		3	IRAS 20126+4104				-5.61	0.19 (0.04)
	+20 14 25.993	+41 13 32.5271	403.898 mas	-212.452 mas	78.122165	3.632929		4	IRAS 20126+4104				-6.23	0.39 (0.05)
	+20 14 26.0023	+41 13 32.5381	542.648 mas	-201.458 mas	78.122184	3.632906		5	IRAS 20126+4104				-15.51	0.23 (0.05)

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 'SUR14' 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 'SUR14' AND detected=true AND hide=false ORDER BY detected DESC,id

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SUR14 - The magnetic field at milliarcsecond resolution around IRAS 20126+4104

Interferometry data

View as list of objects

Detection table from Surcis et al. (2014)