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MIY12 - Analysis of H₂O masers in Sharpless 269 using VERA archival data - Effect of maser structures on astrometric accuracy

Interferometry data

Short title: Miyoshi et al. (2012)
Authors: Miyoshi, MakotoAsaki, YoshiharuWada, KeiichiImai, Hiroshi
Journal: New Astronomy, Volume 17, Issue 6, p. 553-564.
Bibcode:

Target type: HII
Transitions: H2O_22

Abstract
Astrometry using H₂O maser sources in star forming regions is expected to be a powerful tool to study the structures and dynamics of our Galaxy. Honma et al. (2007) (hereafter H2007) claimed that the annual parallax of Sharpless 269 is determined within an error of 0.008 marcs (mas), concluding that S269 is located at 5.3 kpc � 0.2 kpc from the sun, and its galactrocetnric distance is R = 13.1 kpc. From the proper motion, they claimed that the galacto-centric rotational velocity of S269 is equal to that of the sun within a 3% error. This small error, however, is hardly understood when taking into account the results of other observations and theoretical studies of galactic dynamics. We here reanalyzed the VERA archival data using the self calibration method (hybrid mapping), and found that clusters of maser features of S269 are distributed in much wider area than that investigated in H2007. We confirmed that, if we make a narrow region image without considering the presence of multiple maser spots, and only the phase calibration is applied, we can reproduce the same maser structures in a maser feature investigated in H2007. The distribution extent of maser spots in the feature differs 0.2 mas from east to west between our results and H2007. Moreover, we found that change of relative positions of maser spots in the cluster reaches 0.1 mas or larger between observational epochs. This suggests that if one simply assumes the time-dependent, widely distributed maser sources as a stable single point source, it could cause errors of up to 0.1 mas in the annual parallax of S269. Taking into account the internal motions of maser spot clusters, the proper motion of S269 cannot be determined precisely. We estimated that the peculiar motion of S269 with respect to a Galactic circular rotation is ~20 km s^-1. These results imply that the observed kinematics of maser emissions in S269 cannot give a strong constraint on dynamics of the outer part of the Galaxy, in contrast to the claim by H2007.

Abstract

Astrometry using H₂O maser sources in star forming regions is expected to be a powerful tool to study the structures and dynamics of our Galaxy. Honma et al. (2007) (hereafter H2007) claimed that the annual parallax of Sharpless 269 is determined within an error of 0.008 marcs (mas), concluding that S269 is located at 5.3 kpc � 0.2 kpc from the sun, and its galactrocetnric distance is R = 13.1 kpc. From the proper motion, they claimed that the galacto-centric rotational velocity of S269 is equal to that of the sun within a 3% error. This small error, however, is hardly understood when taking into account the results of other observations and theoretical studies of galactic dynamics. We here reanalyzed the VERA archival data using the self calibration method (hybrid mapping), and found that clusters of maser features of S269 are distributed in much wider area than that investigated in H2007. We confirmed that, if we make a narrow region image without considering the presence of multiple maser spots, and only the phase calibration is applied, we can reproduce the same maser structures in a maser feature investigated in H2007. The distribution extent of maser spots in the feature differs 0.2 mas from east to west between our results and H2007. Moreover, we found that change of relative positions of maser spots in the cluster reaches 0.1 mas or larger between observational epochs. This suggests that if one simply assumes the time-dependent, widely distributed maser sources as a stable single point source, it could cause errors of up to 0.1 mas in the annual parallax of S269. Taking into account the internal motions of maser spot clusters, the proper motion of S269 cannot be determined precisely. We estimated that the peculiar motion of S269 with respect to a Galactic circular rotation is ~20 km s^-1. These results imply that the observed kinematics of maser emissions in S269 cannot give a strong constraint on dynamics of the outer part of the Galaxy, in contrast to the claim by H2007.

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Detection table from Miyoshi et al. (2012)

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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)		(km/s)	(Jy/beam)	(arcsec)	Yes/No		(kpc)
1	+06 14 37.08	+13 49 36.7			196.453911	-1.677186	G196.454-1.677		S269_18.11.2004	Image	Descr	22 GHz;	19.3 .. 20.1	321 .. 614	VERA	0.21	1.370	0.0014 x 0.0009	+H₂O -CH₃OH I +CH₃OH II +OH	SFR		18.11.2004
	+06 14 37.0921	+13 49 37.0502	180.82 mas	350.61 mas	196.453849	-1.677096		1	S269_18.11.2004				19.3	321
	+06 14 37.0918	+13 49 37.067	176.43 mas	367.39 mas	196.453844	-1.677095		2	S269_18.11.2004				19.5	400
	+06 14 37.092	+13 49 37.0525	179.71 mas	352.89 mas	196.453848	-1.677096		3	S269_18.11.2004				19.9	614
	+06 14 37.092	+13 49 37.0525	179.77 mas	352.91 mas	196.453848	-1.677096		4	S269_18.11.2004				20.1	471
2	+06 14 37.08	+13 49 36.7			196.453911	-1.677186	G196.454-1.677		S269_26.01.2005			22 GHz;	18.2 .. 20.1	110 .. 561	VERA	0.21	0.482	0.0014 x 0.0009	+H₂O -CH₃OH I +CH₃OH II +OH	SFR		26.01.2005
	+06 14 37.0644	+13 49 36.5166	-234.74 mas	-182.96 mas	196.453925	-1.677266		1	S269_26.01.2005				18.2	112
	+06 14 37.0643	+13 49 36.5166	-234.79 mas	-182.96 mas	196.453925	-1.677266		2	S269_26.01.2005				18.4	110
	+06 14 37.0633	+13 49 36.5089	-250.18 mas	-190.67 mas	196.453925	-1.677270		3	S269_26.01.2005				19.7	154
	+06 14 37.0633	+13 49 36.5089	-250.13 mas	-190.7 mas	196.453925	-1.677270		4	S269_26.01.2005				19.9	187
	+06 14 37.092	+13 49 37.0524	179.93 mas	352.83 mas	196.453848	-1.677096		5	S269_26.01.2005				19.9	561
	+06 14 37.0921	+13 49 37.0699	181.82 mas	370.31 mas	196.453844	-1.677094		6	S269_26.01.2005				19.9	168
	+06 14 37.0633	+13 49 36.5089	-250.18 mas	-190.7 mas	196.453925	-1.677270		7	S269_26.01.2005				20.1	159
	+06 14 37.092	+13 49 37.0525	179.98 mas	352.86 mas	196.453848	-1.677096		8	S269_26.01.2005				20.1	339
3	+06 14 37.08	+13 49 36.7			196.453911	-1.677186	G196.454-1.677		S269_14.03.2005			22 GHz;	8.9 .. 20.1	37 .. 435	VERA	0.21	0.488	0.0014 x 0.0009	+H₂O -CH₃OH I +CH₃OH II +OH	SFR		14.03.2005
	+06 14 37.0787	+13 49 36.7572	-19.65 mas	57.61 mas	196.453894	-1.677183		1	S269_14.03.2005				8.9	125
	+06 14 37.0787	+13 49 36.7572	-19.71 mas	57.61 mas	196.453894	-1.677183		2	S269_14.03.2005				9.2	116
	+06 14 37.0787	+13 49 36.7572	-19.76 mas	57.61 mas	196.453894	-1.677183		3	S269_14.03.2005				9.4	109
	+06 14 37.0787	+13 49 36.7572	-19.82 mas	57.64 mas	196.453894	-1.677183		4	S269_14.03.2005				9.6	101
	+06 14 37.079	+13 49 36.7565	-14.98 mas	56.92 mas	196.453895	-1.677182		5	S269_14.03.2005				12.3	218
	+06 14 37.079	+13 49 36.7565	-14.98 mas	56.9 mas	196.453895	-1.677182		6	S269_14.03.2005				12.5	130
	+06 14 37.0644	+13 49 36.5165	-234.68 mas	-183.12 mas	196.453926	-1.677266		7	S269_14.03.2005				18.2	435
	+06 14 37.0644	+13 49 36.5165	-234.68 mas	-183.12 mas	196.453926	-1.677266		8	S269_14.03.2005				18.2	435
	+06 14 37.0633	+13 49 36.5086	-250.07 mas	-190.95 mas	196.453925	-1.677270		9	S269_14.03.2005				19.7	265
	+06 14 37.0633	+13 49 36.5087	-250.07 mas	-190.91 mas	196.453925	-1.677270		10	S269_14.03.2005				20.1	326
	+06 14 37.0633	+13 49 36.5087	-250.07 mas	-190.91 mas	196.453925	-1.677270		11	S269_14.03.2005				20.1	326
	+06 14 37.0953	+13 49 36.0138	229.32 mas	-685.79 mas	196.454108	-1.677222		12	S269_14.03.2005				20.1	39
	+06 14 37.0952	+13 49 36.0448	227.88 mas	-654.77 mas	196.454100	-1.677219		13	S269_14.03.2005				20.1	37
	+06 14 37.0947	+13 49 36.0968	220.82 mas	-602.79 mas	196.454087	-1.677213		14	S269_14.03.2005				20.1	40
4	+06 14 37.08	+13 49 36.7			196.453911	-1.677186	G196.454-1.677		S269_14.05.2005			22 GHz;	8.9 .. 20.1	86 .. 810	VERA	0.21	1.220	0.0014 x 0.0009	+H₂O -CH₃OH I +CH₃OH II +OH	SFR		14.05.2005
	+06 14 37.0787	+13 49 36.757	-19.38 mas	57.42 mas	196.453894	-1.677183		1	S269_14.05.2005				8.9	252
	+06 14 37.0787	+13 49 36.757	-19.43 mas	57.39 mas	196.453894	-1.677183		2	S269_14.05.2005				9.1	292
	+06 14 37.0787	+13 49 36.757	-19.43 mas	57.39 mas	196.453894	-1.677183		3	S269_14.05.2005				9.1	292
	+06 14 37.0787	+13 49 36.757	-19.49 mas	57.4 mas	196.453894	-1.677183		4	S269_14.05.2005				9.5	255
	+06 14 37.079	+13 49 36.7563	-14.65 mas	56.74 mas	196.453895	-1.677182		5	S269_14.05.2005				12.5	418
	+06 14 37.079	+13 49 36.7563	-14.65 mas	56.74 mas	196.453895	-1.677182		6	S269_14.05.2005				12.5	418
	+06 14 37.0915	+13 49 37.1075	172.04 mas	407.95 mas	196.453833	-1.677091		7	S269_14.05.2005				19.9	311
	+06 14 37.092	+13 49 37.0524	180.2 mas	352.83 mas	196.453848	-1.677096		8	S269_14.05.2005				20.1	810
	+06 14 37.092	+13 49 37.0524	180.2 mas	352.83 mas	196.453848	-1.677096		9	S269_14.05.2005				20.1	810
	+06 14 37.0949	+13 49 36.0914	223.1 mas	-608.2 mas	196.454088	-1.677214		10	S269_14.05.2005				20.1	86
5	+06 14 37.08	+13 49 36.7			196.453911	-1.677186	G196.454-1.677		S269_23.09.2005			22 GHz;	8.3 .. 20.1	119 .. 934	VERA	0.21	1.090	0.0014 x 0.0009	+H₂O -CH₃OH I +CH₃OH II +OH	SFR		23.09.2005
	+06 14 37.0787	+13 49 36.7567	-18.98 mas	57.14 mas	196.453895	-1.677183		1	S269_23.09.2005				8.3	278
	+06 14 37.0787	+13 49 36.7567	-18.98 mas	57.14 mas	196.453895	-1.677183		2	S269_23.09.2005				8.5	465
	+06 14 37.0787	+13 49 36.7567	-19.04 mas	57.14 mas	196.453895	-1.677183		3	S269_23.09.2005				8.7	696
	+06 14 37.0787	+13 49 36.7567	-19.04 mas	57.14 mas	196.453895	-1.677183		4	S269_23.09.2005				8.9	934
	+06 14 37.0787	+13 49 36.7567	-19.04 mas	57.14 mas	196.453895	-1.677183		5	S269_23.09.2005				8.9	934
	+06 14 37.0787	+13 49 36.7567	-19.04 mas	57.14 mas	196.453895	-1.677183		6	S269_23.09.2005				8.9	934
	+06 14 37.0787	+13 49 36.7567	-19.26 mas	57.13 mas	196.453895	-1.677183		7	S269_23.09.2005				10	277
	+06 14 37.0787	+13 49 36.7567	-19.37 mas	57.08 mas	196.453895	-1.677183		8	S269_23.09.2005				10.2	263
	+06 14 37.0787	+13 49 36.7567	-19.54 mas	57.11 mas	196.453895	-1.677183		9	S269_23.09.2005				10.4	283
	+06 14 37.0915	+13 49 37.1074	171.76 mas	407.83 mas	196.453833	-1.677091		10	S269_23.09.2005				20.1	364
	+06 14 37.0921	+13 49 37.0699	181.82 mas	370.27 mas	196.453844	-1.677094		11	S269_23.09.2005				19.9	293
	+06 14 37.0155	+13 49 36.3189	-967.49 mas	-380.66 mas	196.453879	-1.677466		12	S269_23.09.2005				18.2	119
6	+06 14 37.08	+13 49 36.7			196.453911	-1.677186	G196.454-1.677		S269_21.11.2005			22 GHz;	8.3 .. 20.1	46 .. 977	VERA	0.21	0.578	0.0014 x 0.0009	+H₂O -CH₃OH I +CH₃OH II +OH	SFR		21.11.2005
	+06 14 37.0787	+13 49 36.7566	-18.87 mas	57.04 mas	196.453895	-1.677183		1	S269_21.11.2005				8.3	352
	+06 14 37.0787	+13 49 36.7566	-18.87 mas	57.02 mas	196.453895	-1.677183		2	S269_21.11.2005				8.5	626
	+06 14 37.0787	+13 49 36.7566	-18.93 mas	57.02 mas	196.453895	-1.677183		3	S269_21.11.2005				8.7	977
	+06 14 37.0787	+13 49 36.7566	-18.93 mas	57.02 mas	196.453895	-1.677183		4	S269_21.11.2005				8.7	977
	+06 14 37.0787	+13 49 36.7566	-18.93 mas	57.02 mas	196.453895	-1.677183		5	S269_21.11.2005				8.7	977
	+06 14 37.0787	+13 49 36.7566	-19.2 mas	57.01 mas	196.453895	-1.677183		6	S269_21.11.2005				10	451
	+06 14 37.0787	+13 49 36.7566	-19.26 mas	57.01 mas	196.453895	-1.677183		7	S269_21.11.2005				10.2	512
	+06 14 37.0787	+13 49 36.7566	-19.26 mas	57.01 mas	196.453895	-1.677183		8	S269_21.11.2005				10.2	512
	+06 14 37.0921	+13 49 37.0502	181.1 mas	350.59 mas	196.453849	-1.677096		9	S269_21.11.2005				19.2	709
	+06 14 37.0918	+13 49 37.0666	176.32 mas	366.97 mas	196.453844	-1.677095		10	S269_21.11.2005				19.2	247
	+06 14 37.0921	+13 49 37.0502	180.99 mas	350.57 mas	196.453849	-1.677096		11	S269_21.11.2005				19.5	676
	+06 14 37.0921	+13 49 37.0698	181.93 mas	370.17 mas	196.453844	-1.677094		12	S269_21.11.2005				19.9	192
	+06 14 37.0949	+13 49 36.0903	223.44 mas	-609.3 mas	196.454089	-1.677214		13	S269_21.11.2005				20.1	57
	+06 14 37.0953	+13 49 36.0138	228.88 mas	-685.77 mas	196.454108	-1.677222		14	S269_21.11.2005				19.9	46
	+06 14 37.0952	+13 49 36.0453	228.6 mas	-654.33 mas	196.454100	-1.677218		15	S269_21.11.2005				19.9	49
	+06 14 37.0948	+13 49 36.0977	221.77 mas	-601.88 mas	196.454087	-1.677213		16	S269_21.11.2005				19.9	50
	+06 14 37.0155	+13 49 36.3188	-967.49 mas	-380.82 mas	196.453879	-1.677466		17	S269_21.11.2005				18.2	77

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 'MIY12' 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 'MIY12' AND detected=true AND hide=false ORDER BY detected DESC,id

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MIY12 - Analysis of H2O masers in Sharpless 269 using VERA archival data - Effect of maser structures on astrometric accuracy

Interferometry data

View as list of objects

Detection table from Miyoshi et al. (2012)

MIY12 - Analysis of H₂O masers in Sharpless 269 using VERA archival data - Effect of maser structures on astrometric accuracy