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LEK07C - Variations in the spectrum and spatial structure of the H₂O maser in W75N

Short title: Lekht et al. (2007c)
Authors: Lekht, E. E.Slysh, V. I.Krasnov, V. V.
Journal: Astronomy Reports, Volume 51, Issue 12, pp.967-984
Bibcode:

Target type: High_mass_SFR

Abstract
A probable model for the circumstellar envelope associated with the source VLA 2 in W75N has been constructed, based on H₂O-maser monitoring toward W75N carried out on the 22-m radio telescope in Pushchino, as well as VLA maps for 1992, 1996, 1998, and 1999. The envelope has a complex hierarchical structure, including individual maser spots, clusters and chains of spots, inhomogeneous filaments, individual arc-shaped layers, and other complicated features. Most widespread are multi-link chains or filaments with sizes of 1 2 AU. This pattern arises due to the complex hierarchical structure of turbulent motions of material on various scales, from microturbulence to large-scale chaotic motions. No expansion of individual layers in the envelope of VLA 2 has been found. The appearance of the layers is due to the passage of MHD waves that excite the maser emission in consecutive shells in the envelope. This process is fairly cyclic, and is related to the flare activity of the star.

Abstract

A probable model for the circumstellar envelope associated with the source VLA 2 in W75N has been constructed, based on H₂O-maser monitoring toward W75N carried out on the 22-m radio telescope in Pushchino, as well as VLA maps for 1992, 1996, 1998, and 1999. The envelope has a complex hierarchical structure, including individual maser spots, clusters and chains of spots, inhomogeneous filaments, individual arc-shaped layers, and other complicated features. Most widespread are multi-link chains or filaments with sizes of 1 2 AU. This pattern arises due to the complex hierarchical structure of turbulent motions of material on various scales, from microturbulence to large-scale chaotic motions. No expansion of individual layers in the envelope of VLA 2 has been found. The appearance of the layers is due to the passage of MHD waves that excite the maser emission in consecutive shells in the envelope. This process is fairly cyclic, and is related to the flare activity of the star.

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Image	Descr.	Line	V_peak	F_peak	Telescope	V_step	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(deg.)	(deg.)					H₂O	(km/s)	(Jy)		(km/s)	(arcsec)	Yes/No		(kpc)
1	20 38 36.5	+42 37 34.3	81.8713	0.7804	G81.876+0.782	W75N	Image	Descr	22 GHz;	13	1450	RT22_PRAO	0.101	156	+H₂O +CH₃OH I +CH₃OH II +OH	SFR_MIXED		1999-2006

DSS colored	2MASS colored	WISE colored
SDSS color	IRAC color I1,I2,I4	GLIMPSE 360
PACS color (70-160 um)	SPIRE color (250-500 um)	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 'LEK07C' 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 'LEK07C' AND detected=true AND hide=false ORDER BY detected DESC,id

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LEK07C - Variations in the spectrum and spatial structure of the H2O maser in W75N

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Detection table from Lekht et al. (2007c)

LEK07C - Variations in the spectrum and spatial structure of the H₂O maser in W75N