Display data from paper

Select data type:

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.
Bibcode:

Non-detection table: Show non-detection table
Detection table: Show detection table (14 detection)

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.

Download as: Table (CSV)
View paper data

Detection table from Imai et al. (1999)

Export table to csv

Hide / Show individual components

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	SiO J=1-0 v=1;	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	SiO J=1-0 v=2;	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	SiO J=1-0 v=1;	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	SiO J=1-0 v=2;	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	SiO J=1-0 v=1;	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	SiO J=1-0 v=2;	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	SiO J=1-0 v=1;	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	SiO J=1-0 v=2;	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	SiO J=1-0 v=1;	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	SiO J=1-0 v=2;	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	SiO J=1-0 v=1;	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	SiO J=1-0 v=2;	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	SiO J=2-1 v=1;	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	SiO J=2-1 v=2;	40.94	0.21	1.19	NRO	0.080	NRO	+H₂O +OH +SiO	EVOLVED		IMA99

Distribution of sources in all sky (l,b)

Distribution of sources in all sky using Aladin

Tip: Click on some source to get more informaiton

Distribution of sources in IRAS color-color diagram

Tip: Use "Box select" or "Lasso select" to display colour-selected sources in Aladin all-sky view

Tip: Click on some source to look at the different surveys. You must select some surveys in previous page at "View images"

Original color diagram is taken form van der Veen & Habing (1987)

Type	Description
I	Oxygen-rich non-variable stars without circumstellar shells
II	Variable stars with "young" O-rich circumstellar shells
IIIa	Variable stars with more evolved O-rich circumstellar shells
IIIb	Variable stars with thick O-rich circumstellar shells
IV	Variable stars with very thick O-rich circumstellar shells
V	Planetary nebulae and non- variable stars with very cool circumstellar shells
VIa	Variable stars with relatively cold dust at large distances; a significant part of the stars is carbon-rich
VIb	Variable stars with relatively hot dust close to the star and relatively cold dust at large distances; Some of the objects have proven to be O-rich
VII	Variable stars with more evolved C-rich circumstellar shells
VIII	Different sort of objects

Distribution of the detection velocities versus galactic longitude from IMA99

Tip: Use "Box select" or "Lasso select" to display velocity-selected sources in Aladin all-sky view