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IMA99 - VLBA Observation of SiO Masers in the M Giant IRC -10414

Short title: Imai et al. (1999)
Authors: Imai, Hiroshi Deguchi, Shuji Miyoshi, Makoto
Journal: Publications of the Astronomical Society of Japan, v.51, p.587.
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Observations category: SF.general

Abstract
We have mapped an M giant star, IRC -10414, in the SiO J=1-0 v=1 line at 43.1 GHz with the VLBA with a spatial resolution of better than 0.5 mas. The maser spots spread over on a circle having a radius of about 7.1 mas. A velocity gradient in the east-west direction of ~ 0.7 km s^-1 mas^-1 is found. Monitoring observations with Nobeyama 45-m telescope have shown that the intensity ratio of the SiO J=1-0 v=1 to v=2 maser line was quite unusual (5-40) for the period of 1997-1999 in this object this ratio was known to be close to unity in many late-type stellar objects, but was known to deviate strongly from unity in young stellar objects. The unusual line intensity ratio of this star may suggest a chemical or geometrical anomaly of the envelope of IRC -10414. A possible ring/disk model is discussed in order to explain the distribution of the maser spots in this object. The VLBA and the VLA are the facilities of the National Radio Astronomy Observatory operated by Associated Universities, Inc., under cooperative agreements with the National Science Foundation of the USA.

Abstract

We have mapped an M giant star, IRC -10414, in the SiO J=1-0 v=1 line at 43.1 GHz with the VLBA with a spatial resolution of better than 0.5 mas. The maser spots spread over on a circle having a radius of about 7.1 mas. A velocity gradient in the east-west direction of ~ 0.7 km s^-1 mas^-1 is found. Monitoring observations with Nobeyama 45-m telescope have shown that the intensity ratio of the SiO J=1-0 v=1 to v=2 maser line was quite unusual (5-40) for the period of 1997-1999 in this object this ratio was known to be close to unity in many late-type stellar objects, but was known to deviate strongly from unity in young stellar objects. The unusual line intensity ratio of this star may suggest a chemical or geometrical anomaly of the envelope of IRC -10414. A possible ring/disk model is discussed in order to explain the distribution of the maser spots in this object. The VLBA and the VLA are the facilities of the National Radio Astronomy Observatory operated by Associated Universities, Inc., under cooperative agreements with the National Science Foundation of the USA.

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Detection table from Imai et al. (1999)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Line	V_peak	T_a	∫T_a dv	Telescope	RMS	List	Detection	Class	Dist. (parallax)	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)			SiO	(km/s)	(K)	(K*km/s)		(Jy)		Yes/No		(kpc)
1	18 23 17.8	-13 42 48.4	17.5505	-0.1261	G17.551-0.126	IRAS18204-1344	43.1 GHz;	41.86	13.16	58	NRO	0.320	NRO	+H₂O +OH +SiO	EVOLVED		IMA99
2	18 23 17.8	-13 42 48.4	17.5505	-0.1261	G17.551-0.126	IRAS18204-1344	42.8 GHz;	36.7	0.55	2.4	NRO	0.190	NRO	+H₂O +OH +SiO	EVOLVED		IMA99
3	18 23 17.8	-13 42 48.4	17.5505	-0.1261	G17.551-0.126	IRAS18204-1344	43.1 GHz;	41.62	11.99	63.2	NRO	0.160	NRO	+H₂O +OH +SiO	EVOLVED		IMA99
4	18 23 17.8	-13 42 48.4	17.5505	-0.1261	G17.551-0.126	IRAS18204-1344	42.8 GHz;	40.73	0.76	3.6	NRO	0.190	NRO	+H₂O +OH +SiO	EVOLVED		IMA99
5	18 23 17.8	-13 42 48.4	17.5505	-0.1261	G17.551-0.126	IRAS18204-1344	43.1 GHz;	41.11	20.27	72.3	NRO	0.120	NRO	+H₂O +OH +SiO	EVOLVED		IMA99
6	18 23 17.8	-13 42 48.4	17.5505	-0.1261	G17.551-0.126	IRAS18204-1344	42.8 GHz;	41.45	0.53	1.9	NRO	0.140	NRO	+H₂O +OH +SiO	EVOLVED		IMA99
7	18 23 17.8	-13 42 48.4	17.5505	-0.1261	G17.551-0.126	IRAS18204-1344	43.1 GHz;	41.59	4.99	36.5	NRO	0.220	NRO	+H₂O +OH +SiO	EVOLVED		IMA99
8	18 23 17.8	-13 42 48.4	17.5505	-0.1261	G17.551-0.126	IRAS18204-1344	42.8 GHz;	40.99	1.53	7.7	NRO	0.230	NRO	+H₂O +OH +SiO	EVOLVED		IMA99
9	18 23 17.8	-13 42 48.4	17.5505	-0.1261	G17.551-0.126	IRAS18204-1344	43.1 GHz;	40.02	5.85	30.5	NRO	0.240	NRO	+H₂O +OH +SiO	EVOLVED		IMA99
10	18 23 17.8	-13 42 48.4	17.5505	-0.1261	G17.551-0.126	IRAS18204-1344	42.8 GHz;	53.31	0.7	2.7	NRO	0.230	NRO	+H₂O +OH +SiO	EVOLVED		IMA99
11	18 23 17.8	-13 42 48.4	17.5505	-0.1261	G17.551-0.126	IRAS18204-1344	43.1 GHz;	43.08	4.89	33.6	NRO	0.240	NRO	+H₂O +OH +SiO	EVOLVED		IMA99
12	18 23 17.8	-13 42 48.4	17.5505	-0.1261	G17.551-0.126	IRAS18204-1344	42.8 GHz;	38.13	0.51	1.5	NRO	0.070	NRO	+H₂O +OH +SiO	EVOLVED		IMA99
13	18 23 17.8	-13 42 48.4	17.5505	-0.1261	G17.551-0.126	IRAS18204-1344	86.2 GHz;	44.82	1.85	14.25	NRO	0.050	NRO	+H₂O +OH +SiO	EVOLVED		IMA99
14	18 23 17.8	-13 42 48.4	17.5505	-0.1261	G17.551-0.126	IRAS18204-1344	85.6 GHz;	40.94	0.21	1.19	NRO	0.080	NRO	+H₂O +OH +SiO	EVOLVED		IMA99

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(sio_data_all.ra_hms) as ra_hms,MAX(sio_data_all.dec_dms) as dec_dms,MAX(sio_data_all.source_name) as source_name,MAX(sio_data_all.ra) as ra,MAX(sio_data_all.dec) as dec,MAX(sio_data_all.l) as l,MAX(sio_data_all.b) as b,MAX(sio_data_all.grp) as grp,MAX(sio_data_all.other_name) as other_name,MAX(sio_data_all.other_desc) as other_desc,BOOL_OR(thermal) as thermal,MAX(sio_data_all.line) as line,MAX(sio_data_all.vrange) as vrange,MAX(sio_data_all.vpeak) as vpeak,MAX(sio_data_all.peak) as peak,MAX(sio_data_all.fwhm) as fwhm,MAX(sio_data_all.int) as int,MAX(sio_data_all.rms) as rms,MAX(sio_data_all.units) as units,MAX(sio_data_all.units_rms) as units_rms,MAX(sio_data_all.date_txt) as date_txt,MAX(sio_data_all.telescope_ref) as telescope_ref,MAX(sio_data_all.telescope_conf) as telescope_conf,MAX(sio_data_all.v_step) as v_step,MAX(sio_data_all.beam) as beam,MAX(sio_data_all.beam_maj) as beam_maj,MAX(sio_data_all.beam_min) as beam_min,MAX(sio_data_all.beam_pa) as beam_pa,MAX(sio_data_all.ref) as ref,MAX(sio_data_all.list_ref) as list_ref,MAX(sio_data_all.ascii) as ascii,MAX(sio_data_all.url) as url,MAX(sio_data_all.image) as image,MAX(sio_data_all.image2) as image2,MAX(sio_data_all.image3) as image3,MAX(sio_data_all.descr) as descr,MAX(sio_data_all.id) as id,BOOL_OR(mjy_flag) as mjy_flag,BOOL_OR(rms_mjy_flag) as rms_mjy_flag,MAX(sio_data_all.dist) as dist,1 as dist_parallax,MAX(sio_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 sio_data_all  LEFT JOIN all_objects_withmet ON sio_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' WHERE ref ilike 'IMA99' AND detected=true AND hide=false GROUP BY ref

select sio_data_all.ra_hms,sio_data_all.dec_dms,sio_data_all.source_name,sio_data_all.ra,sio_data_all.dec,sio_data_all.l,sio_data_all.b,sio_data_all.grp,sio_data_all.other_name,sio_data_all.other_desc,sio_data_all.thermal,sio_data_all.line,sio_data_all.vrange,sio_data_all.vpeak,sio_data_all.peak,sio_data_all.fwhm,sio_data_all.int,sio_data_all.rms,sio_data_all.units,sio_data_all.units_rms,sio_data_all.date_txt,sio_data_all.telescope_ref,sio_data_all.telescope_conf,sio_data_all.v_step,sio_data_all.beam,sio_data_all.beam_maj,sio_data_all.beam_min,sio_data_all.beam_pa,sio_data_all.ref,sio_data_all.list_ref,sio_data_all.ascii,sio_data_all.url,sio_data_all.image,sio_data_all.image2,sio_data_all.image3,sio_data_all.descr,sio_data_all.id,sio_data_all.mjy_flag,sio_data_all.rms_mjy_flag,sio_data_all.dist,sio_data_all.dist_parallax,sio_data_all.date_txt,line_det,type,simbad_types_cat FROM sio_data_all   LEFT JOIN all_objects_withmet ON sio_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' WHERE ref ilike 'IMA99' AND detected=true AND hide=false ORDER BY detected DESC,id

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IMA99 - VLBA Observation of SiO Masers in the M Giant IRC -10414

View as list of objects

Detection table from Imai et al. (1999)