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MOS06 - First results from a VLBA proper motion survey of H2O masers in low-mass YSOs: the Serpens core and RNO 15-FIR

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Short title: Moscadelli et al. (2006)
Authors: Moscadelli, L.Testi, L.Furuya, R. S.Goddi, C.Claussen, M.Kitamura, Y.Wootten, A.
Journal: Astronomy and Astrophysics, Volume 446, Issue 3, February II 2006, pp.985-999
Bibcode:

Target type: Low_mass_SFR

Abstract
This article reports first results of a long-term observational program aimed to study the earliest evolution of jet/disk systems in low-mass YSOs by means of VLBI observations of the 22.2 GHz water masers. We report here data for the cluster of low-mass YSOs in the Serpens molecular core and for the single object RNO 15-FIR. Towards Serpens SMM1, the most luminous sub-mm source of the Serpens cluster, the water maser emission comes from two small (â��5 AU in size) clusters of features separated by â�ˆ25 AU, having line of sight velocities strongly red-shifted (by more than 10 km s^-1) with respect to the LSR velocity of the molecular cloud. The two maser clusters are oriented on the sky along a direction that is approximately perpendicular to the axis of the radio continuum jet observed with the VLA towards SMM1. The spatial and velocity distribution of the maser features lead us to favor the interpretation that the maser emission is excited by interaction of the receding lobe of the jet with dense gas in the accretion disk surrounding the YSO in SMM1. The line of sight velocities of several features decrease at a rate of â�ˆ1 km s^-1 month^-1 and the sky-projected relative motion of two features appears to be accelerated (decelerated) at a rate of â�ˆ10-15 km s^-1 month^-1. We propose that the shocks harboring the maser emission are slowed down as they proceed through the dense material surrounding the YSO. Towards RNO 15-FIR, the few detected maser features have both positions and (absolute) velocities aligned along a direction that is parallel to the axis of the molecular outflow observed on much larger angular scales. In this case the maser emission likely emerges from dense, shocked molecular clumps displaced along the axis of the jet emerging from the YSO. The protostar in Serpens SMM1 is more massive than the one in RNO 15-FIR. We discuss the case where a high mass ejection rate can generate jets sufficiently powerful to sweep away from their course the densest portions of circumstellar gas. In this case, the excitation conditions for water masers might preferably occur at the interface between the jet and the accretion disk, rather than along the jet axis.

Abstract

This article reports first results of a long-term observational program aimed to study the earliest evolution of jet/disk systems in low-mass YSOs by means of VLBI observations of the 22.2 GHz water masers. We report here data for the cluster of low-mass YSOs in the Serpens molecular core and for the single object RNO 15-FIR. Towards Serpens SMM1, the most luminous sub-mm source of the Serpens cluster, the water maser emission comes from two small (â��5 AU in size) clusters of features separated by â�ˆ25 AU, having line of sight velocities strongly red-shifted (by more than 10 km s^-1) with respect to the LSR velocity of the molecular cloud. The two maser clusters are oriented on the sky along a direction that is approximately perpendicular to the axis of the radio continuum jet observed with the VLA towards SMM1. The spatial and velocity distribution of the maser features lead us to favor the interpretation that the maser emission is excited by interaction of the receding lobe of the jet with dense gas in the accretion disk surrounding the YSO in SMM1. The line of sight velocities of several features decrease at a rate of â�ˆ1 km s^-1 month^-1 and the sky-projected relative motion of two features appears to be accelerated (decelerated) at a rate of â�ˆ10-15 km s^-1 month^-1. We propose that the shocks harboring the maser emission are slowed down as they proceed through the dense material surrounding the YSO. Towards RNO 15-FIR, the few detected maser features have both positions and (absolute) velocities aligned along a direction that is parallel to the axis of the molecular outflow observed on much larger angular scales. In this case the maser emission likely emerges from dense, shocked molecular clumps displaced along the axis of the jet emerging from the YSO. The protostar in Serpens SMM1 is more massive than the one in RNO 15-FIR. We discuss the case where a high mass ejection rate can generate jets sufficiently powerful to sweep away from their course the densest portions of circumstellar gas. In this case, the excitation conditions for water masers might preferably occur at the interface between the jet and the accretion disk, rather than along the jet axis.

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Detection table from Moscadelli et al. (2006)

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ID	Obs. RA	Obs. Dec	RA offset	Dec offset	l	b	Group id	#	Source name	Image	Descr.	Line	V_peak	V_X	V_Y	F_peak	Telescope	V_step	RMS	Beam	Detection	Class	Dist. (parallax)	Date
	(J2000)	(J2000)	(mas)	(mas)	(deg.)	(deg.)						H₂O	(km/s)	(km/s)	(km/s)	(Jy)		(km/s)	(mJy/beam)	(arcsec)	Yes/No		(kpc)
1	+18 29 49.8	+01 15 20.5			31.584345	5.379859	G31.584+5.377		SMM1	Image	Descr	22 GHz;	18 .. 23.6			0.1 .. 13.96	VLBA	0.21	10.000	0.0015 x 0.0006	+H₂O +CH₃OH I -CH₃OH II +OH -SiO	SFR		2003 Apr 1 - Jun 8
	+18 29 49.8036	+01 15 20.5516	53.8 mas	53.22 mas	31.584364	5.379852		1	SMM1				20	17.8 (4.1)	26.5 (3.5)	13.96
	+18 29 49.8035	+01 15 20.5519	53.19 mas	53.5 mas	31.584364	5.379852		2	SMM1				20.3			4.68
	+18 29 49.8035	+01 15 20.5528	52.98 mas	54.38 mas	31.584364	5.379852		3	SMM1				20.2			0.14
	+18 29 49.8034	+01 15 20.552	51.59 mas	53.62 mas	31.584364	5.379852		4	SMM1				19.7	36.1 (2.7)	22.1 (3.0)	0.5
	+18 29 49.8044	+01 15 20.5493	65.75 mas	50.88 mas	31.584365	5.379849		5	SMM1				19.4	25.0 (0.4)	12.7 (1.1)	0.16
	+18 29 49.8042	+01 15 20.55	62.87 mas	51.63 mas	31.584365	5.379849		6	SMM1				20.9	26.7 (1.1)	25.1 (1.2)	0.32
	+18 29 49.8	+01 15 20.4994	-0.22 mas	0.95 mas	31.584344	5.379858		7	SMM1				23.6	-17.4 (3.6)	1.7 (3.4)	0.91
	+18 29 49.8	+01 15 20.4984	0 mas	0 mas	31.584344	5.379858		8	SMM1				22.5			1.47
	+18 29 49.8038	+01 15 20.5519	57.39 mas	53.49 mas	31.584365	5.379851		9	SMM1				20.8			0.1
	+18 29 49.7999	+01 15 20.5005	-2.2 mas	2.12 mas	31.584344	5.379859		10	SMM1				22.7			2
	+18 29 49.8032	+01 15 20.5518	47.98 mas	53.4 mas	31.584364	5.379853		11	SMM1				18			0.16
	+18 29 49.8042	+01 15 20.5522	63.71 mas	53.82 mas	31.584366	5.379849		12	SMM1				20.3			1.57
	+18 29 49.8002	+01 15 20.4952	2.7 mas	-3.22 mas	31.584344	5.379857		13	SMM1				23			0.36
2	+18 29 59.3	+01 14 0.4			31.582583	5.334492	G31.584+5.377		SMM3	Image		22 GHz;	18.1 .. 19.5			0.09 .. 23.16	VLBA	0.21	10.000	0.0015 x 0.0006	+H₂O +CH₃OH I -CH₃OH II +OH -SiO	SFR		2003 Nov 21
	+18 29 59.2999	+01 14 0.3984	0 mas	0 mas	31.582583	5.334492		1	SMM3				18.6			23.16
	+18 29 59.2999	+01 14 0.3987	-0.55 mas	0.3 mas	31.582583	5.334493		2	SMM3				19.5			0.7
	+18 29 59.2999	+01 14 0.3984	-0.76 mas	0 mas	31.582583	5.334493		3	SMM3				18.8			1.48
	+18 29 59.2998	+01 14 0.39773	-1.22 mas	-0.67 mas	31.582582	5.334493		4	SMM3				18.1			0.37
	+18 29 59.2998	+01 14 0.39866	-1.79 mas	0.26 mas	31.582583	5.334493		5	SMM3				18.8			1.09
	+18 29 59.2998	+01 14 0.39886	-2.37 mas	0.46 mas	31.582583	5.334493		6	SMM3				19.5			0.09
3	+18 29 58.6	+01 13 59.7			31.581074	5.336999	G31.584+5.377		SMM4	Image		22 GHz;	5.9			9.56	VLBA	0.21	10.000	0.0015 x 0.0006	+H₂O +CH₃OH I -CH₃OH II +OH -SiO	SFR		2003 Nov 21
	+18 29 58.6001	+01 13 59.7	0 mas	0 mas	31.581074	5.336998		1	SMM4				5.9			9.56
4	+03 27 39.1	+30 13 3.5			158.767058	-21.575515	G158.768-21.577		RNO 15-FIR	Image	Descr	22 GHz;	2.9 .. 5.1			0.21 .. 25.06	VLBA	0.21	10.000	0.0015 x 0.0006	+H₂O -CH₃OH I -CH₃OH II	SFR		2003 Oct 19 - Nov 7
	+03 27 39.1001	+30 13 3.5004	0 mas	0 mas	158.767058	-21.575515		1	RNO 15-FIR				4.9	-22.8 (13.6)	-16.2 (13.6)	25.06
	+03 27 39.1	+30 13 3.50008	-0.51 mas	-0.32 mas	158.767058	-21.575515		2	RNO 15-FIR				5	-32.5 (14.3)	-17.3 (14.2)	0.9
	+03 27 39.0999	+30 13 3.49851	-2.47 mas	-1.89 mas	158.767058	-21.575516		3	RNO 15-FIR				2.9	-4.4 (14.4)	-4.5 (14.6)	0.21
	+03 27 39.1001	+30 13 3.50082	0.78 mas	0.42 mas	158.767059	-21.575515		4	RNO 15-FIR				5.1			0.31
5	+07 03 43.2	-11 33 06			224.606502	-2.556517	G224.607-2.557		Z CMa	Image		22 GHz;	..			..	VLBA	0.21	10.000	0.0015 x 0.0006	+H₂O -CH₃OH I -CH₃OH II -OH	SFR_MIXED		2003
6	+03 29 10.4	+31 13 31			158.394952	-20.574654	G158.400-20.576		NGC1333 4AB	Image		22 GHz;	..			..	VLBA	0.21	10.000	0.0015 x 0.0006	+H₂O +CH₃OH I -CH₃OH II	SFR		2003
7	+05 41 45.16	-01 56 0.6			206.564419	-16.361192	G206.565-16.361		NGC2024	Image		22 GHz;	..			..	VLBA	0.21	10.000	0.0015 x 0.0006	+H₂O +CH₃OH I +CH₃OH II	SFR		2003
8	+20 39 8.26	+68 02 15.7			102.656235	15.793431	G102.650+15.786		L1157 MM	Image		22 GHz;	..			..	VLBA	0.21	10.000	0.0015 x 0.0006	+H₂O +CH₃OH I -CH₃OH II	SFR		2003

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 'MOS06' 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 'MOS06' AND detected=true AND hide=false ORDER BY detected DESC,id

Display data from paper

MOS06 - First results from a VLBA proper motion survey of H2O masers in low-mass YSOs: the Serpens core and RNO 15-FIR

Interferometry data

View as list of objects

Detection table from Moscadelli et al. (2006)