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NAK03B - SiO Maser Survey of Cold IRAS Sources

Short title: Nakashima & Deguchi (2003B)
Authors: Nakashima, Jun-Ichi Deguchi, Shuji
Journal: Publications of the Astronomical Society of Japan, Vol.55, No.1, pp.229-246
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Non-detection table: Show non-detection table
Detection table: Show detection table (3 detection) Non-detection table: Show non-detection table (20 non-detection)
Target type: star

Abstract
We present the results of observations of cold IRAS sources in the Galactic disk area, -10 < l < 100 and b < 5, in the SiO J = 1 -- 0, v = 1 and 2 maser lines. SiO masers were detected in 51 out of 143 observed sources 45 were new detections in SiO masers. The selected IRAS sources were objects with dust temperatures of between 160 and 280K. According to a confirmation using 2MASS near-infrared images, a majority of the sample are AGB or post-AGB stars, although dense cores in the star-forming regions (or dusty H II regions) are involved in part of the sample. Among new detections, two were candidates for post-AGB stars: IRAS 18450 - 0148 (W43A), and 19312 + 1950. We found that the intensity ratios of the SiO J = 1 -- 0, v = 2 to the v = 1 line of the objects clearly correlate with those IRAS colors. The detection rates of SiO masers tend to increase toward the Galactic center as we ll as the cases of previous SiO maser surveys of typical AGB stars. No strong associations of the objects to the spiral arms were found. The radial-velocity dispersion of the present sample is comparable with the dispersion of the SiO maser sample of typical AGB stars. These facts suggest that the present sample of cold IRAS sources with SiO masers has a kinematic property very similar to that of typical AGB stars. eprintid: arXiv:astro-ph/0301372

Abstract

We present the results of observations of cold IRAS sources in the Galactic disk area, -10 < l < 100 and b < 5, in the SiO J = 1 -- 0, v = 1 and 2 maser lines. SiO masers were detected in 51 out of 143 observed sources 45 were new detections in SiO masers. The selected IRAS sources were objects with dust temperatures of between 160 and 280K. According to a confirmation using 2MASS near-infrared images, a majority of the sample are AGB or post-AGB stars, although dense cores in the star-forming regions (or dusty H II regions) are involved in part of the sample. Among new detections, two were candidates for post-AGB stars: IRAS 18450 - 0148 (W43A), and 19312 + 1950. We found that the intensity ratios of the SiO J = 1 -- 0, v = 2 to the v = 1 line of the objects clearly correlate with those IRAS colors. The detection rates of SiO masers tend to increase toward the Galactic center as we ll as the cases of previous SiO maser surveys of typical AGB stars. No strong associations of the objects to the spiral arms were found. The radial-velocity dispersion of the present sample is comparable with the dispersion of the SiO maser sample of typical AGB stars. These facts suggest that the present sample of cold IRAS sources with SiO masers has a kinematic property very similar to that of typical AGB stars. eprintid: arXiv:astro-ph/0301372

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Detection table from Nakashima & Deguchi (2003B)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Line	V_peak	F_peak	∫F dv	RMS	List	Detection	Class	Dist. (parallax)	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)			H₂O	(km/s)	(Jy)	(Jy*km/s)	(Jy)		Yes/No		(kpc)
1	19 09 19	+09 21 09	43.2840	0.3246	G43.285+0.324	19069+0916	22 GHz;	10.7	7.217	808.564	0.152	ENG_H2O	+H₂O +OH +SiO	GALAXY		NAK03B
2	19 09 7.2	+08 16 31	42.3057	-0.1291	G42.308-0.132	19067+0811	22 GHz;	76.7	3.853	195.023	0.164	ENG_H2O	+H₂O +OH +SiO	EVOLVED		NAK03B
3	19 33 24.2	+19 56 55	55.3705	0.1856	G55.371+0.185	19312+1950	22 GHz;	17.4	7.251	171.407	0.192	ENG_H2O	+H₂O +CH₃OH I -CH₃OH II +OH +SiO	SFR		NAK03B

Non-detection table from Nakashima & Deguchi (2003B)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Line	F_peak	Date	RMS	List	Detection	Class	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)			H₂O	(Jy)		(Jy)		Yes/No
1	18 20 2.7	-16 02 19	15.1290	-0.5262	G15.130-0.527	18171-1603	22 GHz;	0.512	2000-05-28	0.170	ENG_H2O	-H₂O -CH₃OH I -CH₃OH II -SiO	SFR	NAK03B
2	19 00 17.5	+08 35 31	41.5856	1.9562	G41.585+1.956	18578+0831	22 GHz;	0.744	2000-05-28	0.248	ENG_H2O	+H₂O -CH₃OH II +OH +SiO	EVOLVED	NAK03B
3	19 03 3.2	+06 28 52	40.0211	0.3822	G40.022+0.382	19006+0624	22 GHz;	0.753	2000-05-28	0.251	ENG_H2O	-H₂O +OH +SiO	EVOLVED	NAK03B
4	19 08 58.3	+08 37 47	42.6034	0.0669	G42.604+0.066	19065+0832	22 GHz;	0.623	2000-05-28	0.208	ENG_H2O	+H₂O -CH₃OH II +OH +SiO	SFR_MIXED	NAK03B
5	19 09 31.4	+09 51 47	43.7605	0.5149	G43.762+0.513	19071+0946	22 GHz;	0.716	2000-05-28	0.239	ENG_H2O	+H₂O -CH₃OH II +OH +SiO	SFR_MIXED	NAK03B
6	19 15 16.3	+09 15 44	43.8843	-1.0194	G43.885-1.020	19128+0910	22 GHz;	0.753	2000-05-28	0.251	ENG_H2O	-H₂O -CH₃OH II +OH +SiO	EVOLVED	NAK03B
7	19 19 56.6	+10 48 05	45.7827	-1.3179	G45.783-1.319	19175+1042	22 GHz;	0.744	2000-05-28	0.248	ENG_H2O	+H₂O +OH +SiO	EVOLVED	NAK03B
8	19 20 14	+12 12 22	47.0569	-0.7218	G47.057-0.722	19178+1206	22 GHz;	0.214	2001-02-10	0.071	ENG_H2O	-H₂O -CH₃OH I -CH₃OH II +OH +SiO	EVOLVED	NAK03B
9	19 20 42.5	+11 54 03	46.8418	-0.9677	G46.842-0.968	19183+1148	22 GHz;	0.214	2001-02-10	0.071	ENG_H2O	-H₂O +OH +SiO	EVOLVED	NAK03B
10	19 21 10.7	+11 02 44	46.1407	-1.4711	G46.141-1.471	19188+1057	22 GHz;	0.893	2000-05-28	0.298	ENG_H2O	-H₂O +OH +SiO	EVOLVED	NAK03B
11	19 22 17.6	+15 41 47	50.3721	0.4788	G50.373+0.478	19200+1536	22 GHz;	0.939	2000-05-28	0.313	ENG_H2O	-H₂O -CH₃OH II +OH +SiO	EVOLVED	NAK03B
12	19 27 41.6	+16 37 22	51.8025	-0.2236	G51.804-0.224	19254+1631	22 GHz;	0.614	2000-05-31	0.205	ENG_H2O	+H₂O -CH₃OH II +OH +SiO	EVOLVED	NAK03B
13	19 30 29.6	+19 50 40	54.9494	0.7347	G54.949+0.735	19283+1944	22 GHz;	0.484	2000-06-01	0.161	ENG_H2O	-H₂O -CH₃OH II +OH +SiO	EVOLVED	NAK03B
14	19 31 38.7	+22 35 16	57.4848	1.8178	G57.485+1.817	19295+2228	22 GHz;	0.679	2000-06-01	0.226	ENG_H2O	+H₂O +OH +SiO	EVOLVED	NAK03B
15	19 32 57.2	+26 52 40	61.3941	3.6194	G61.394+3.619	19309+2646	22 GHz;	0.307	2001-02-10	0.102	ENG_H2O	-H₂O -OH	EVOLVED	NAK03B
16	19 46 8.7	+22 59 23	59.4772	-0.8954	G59.478-0.897	19440+2251	22 GHz;	0.837	2000-05-28	0.279	ENG_H2O	-H₂O +OH +SiO	EVOLVED	NAK03B
17	19 58 29.7	+31 48 13	68.4493	1.2690	G68.449+1.269	19565+3140	22 GHz;	0.818	2000-05-28	0.273	ENG_H2O	-H₂O +OH +SiO	EVOLVED	NAK03B
18	19 59 38.7	+28 23 07	65.6685	-0.7349	G65.669-0.736	19576+2814	22 GHz;	0.809	2000-05-28	0.270	ENG_H2O	-H₂O -CH₃OH II +OH +SiO	EVOLVED	NAK03B
19	20 04 20.4	+29 04 05	66.7929	-1.2464	G66.794-1.247	20023+2855	22 GHz;	0.679	2000-06-01	0.226	ENG_H2O	-H₂O +OH +SiO	EVOLVED	NAK03B
20	20 06 22.9	+27 02 11	65.3172	-2.7145	G65.317-2.715	20043+2653	22 GHz;	1.349	2000-05-28	0.449	ENG_H2O	-H₂O +OH +SiO	EVOLVED	NAK03B

Distribution of sources in all sky (l,b)

Distribution of sources in all sky using Aladin

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Distribution of sources in IRAS color-color diagram

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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 NAK03B

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