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IZU98 - SiO Maser Forest at the Galactic Center

Short title: Izumiura et al. (1998)
Authors: Izumiura, Hideyuki Deguchi, Shuji Fujii, Takahiro
Journal: The Astrophysical Journal, Volume 494, Issue 1, pp. L89-L92.
Bibcode:

Abstract
A moderately deep survey of stellar maser sources toward the Galactic center has been made in the SiO J=1-0, v=1 and v=2 transitions (~43 GHz) with the Nobeyama 45 m telescope with a beam size of about 40^''. At the Galactic center (Sgr A*), seven (four new) SiO maser sources were detected in one beam. In order to investigate the spatial distribution of SiO maser sources, we have also observed the offset positions by +/-40^'' in Galactic longitude from the Galactic center. In total, seven (four new) SiO maser sources were detected at the offset positions. Taking into account the shorter integration time at the offset positions, we find that the surface number density of SiO maser sources is nearly constant at the Galactic center. The number density of SiO maser sources is found to be an order of magnitude higher than the density of OH 1612 MHz objects. A radial velocity gradient in Galactic longitude was not detected. These facts indicate that the SiO maser sources seen toward the Galactic center are mostly associated with the stellar population of a Galactic stellar nuclear disk of more than a few arcminute radius. eprintid: arXiv:astro-ph/9712101

Abstract

A moderately deep survey of stellar maser sources toward the Galactic center has been made in the SiO J=1-0, v=1 and v=2 transitions (~43 GHz) with the Nobeyama 45 m telescope with a beam size of about 40^''. At the Galactic center (Sgr A*), seven (four new) SiO maser sources were detected in one beam. In order to investigate the spatial distribution of SiO maser sources, we have also observed the offset positions by +/-40^'' in Galactic longitude from the Galactic center. In total, seven (four new) SiO maser sources were detected at the offset positions. Taking into account the shorter integration time at the offset positions, we find that the surface number density of SiO maser sources is nearly constant at the Galactic center. The number density of SiO maser sources is found to be an order of magnitude higher than the density of OH 1612 MHz objects. A radial velocity gradient in Galactic longitude was not detected. These facts indicate that the SiO maser sources seen toward the Galactic center are mostly associated with the stellar population of a Galactic stellar nuclear disk of more than a few arcminute radius. eprintid: arXiv:astro-ph/9712101

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Detection table from Izumiura et al. (1998)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Line	V_peak	T_a	∫T_a dv	Telescope	List	Detection	Class	Dist. (parallax)	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)			SiO	(km/s)	(K)	(K*km/s)			Yes/No		(kpc)
1	17 45 37.4	-29 01 2.8	359.9311	-0.0431	G359.9320-0.0447	SiO359.933-0.046 1	43.1 GHz;	131.2	0.04	0.106	NRO	NRO	+SiO	SFR_MIXED		IZU98
2	17 45 37.4	-29 01 2.8	359.9311	-0.0431	G359.9320-0.0447	SiO359.933-0.046 1	42.8 GHz;	131.2	0.046	0.18	NRO	NRO	+SiO	SFR_MIXED		IZU98
3	17 45 37.4	-29 01 2.8	359.9311	-0.0431	G359.9320-0.0447	SiO359.933-0.046 2	43.1 GHz;	63.7	0.042	0.063	NRO	NRO	+SiO	SFR_MIXED		IZU98
4	17 45 37.4	-29 01 2.8	359.9311	-0.0431	G359.9320-0.0447	SiO359.933-0.046 3	43.1 GHz;	15.9	0.08	0.262	NRO	NRO	+SiO	SFR_MIXED		IZU98
5	17 45 37.4	-29 01 2.8	359.9311	-0.0431	G359.9320-0.0447	SiO359.933-0.046 3	42.8 GHz;	15.9	0.05	0.138	NRO	NRO	+SiO	SFR_MIXED		IZU98
6	17 45 37.4	-29 01 2.8	359.9311	-0.0431	G359.9320-0.0447	SiO359.933-0.046 4	43.1 GHz;	-104.2	0.035	0.142	NRO	NRO	+SiO	SFR_MIXED		IZU98
7	17 45 37.4	-29 01 2.8	359.9311	-0.0431	G359.9320-0.0447	SiO359.933-0.046 4	42.8 GHz;	-105.1	0.076	0.256	NRO	NRO	+SiO	SFR_MIXED		IZU98
8	17 45 40	-29 00 27.6	359.9444	-0.0461	G359.9444-0.0464	SiO359.944-0.046 1	43.1 GHz;	54.4	0.049	0.205	NRO	NRO	+H₂O +CH₃OH I -CH₃OH II +OH	SFR_MIXED		IZU98
9	17 45 40	-29 00 27.6	359.9444	-0.0461	G359.9444-0.0464	SiO359.944-0.046 1	42.8 GHz;	53.1	0.047	0.198	NRO	NRO	+H₂O +CH₃OH I -CH₃OH II +OH	SFR_MIXED		IZU98
10	17 45 40	-29 00 27.6	359.9444	-0.0461	G359.9444-0.0464	SiO359.944-0.046 2	43.1 GHz;	-13.8	0.043	0.122	NRO	NRO	+H₂O +CH₃OH I -CH₃OH II +OH	SFR_MIXED		IZU98
11	17 45 40	-29 00 27.6	359.9444	-0.0461	G359.9444-0.0464	SiO359.944-0.046 2	42.8 GHz;	-14.6	0.034	0.121	NRO	NRO	+H₂O +CH₃OH I -CH₃OH II +OH	SFR_MIXED		IZU98
12	17 45 40	-29 00 27.6	359.9444	-0.0461	G359.9444-0.0464	SiO359.944-0.046 3	43.1 GHz;	-25.2	0.027	0.156	NRO	NRO	+H₂O +CH₃OH I -CH₃OH II +OH	SFR_MIXED		IZU98
13	17 45 40	-29 00 27.6	359.9444	-0.0461	G359.9444-0.0464	SiO359.944-0.046 3	42.8 GHz;	-25.2	0.046	0.221	NRO	NRO	+H₂O +CH₃OH I -CH₃OH II +OH	SFR_MIXED		IZU98
14	17 45 40	-29 00 27.6	359.9444	-0.0461	G359.9444-0.0464	SiO359.944-0.046 4	42.8 GHz;	-51.2	0.02	0.04	NRO	NRO	+H₂O +CH₃OH I -CH₃OH II +OH	SFR_MIXED		IZU98
15	17 45 40	-29 00 27.6	359.9444	-0.0461	G359.9444-0.0464	SiO359.944-0.046 5	42.8 GHz;	-69.6	0.024	0.16	NRO	NRO	+H₂O +CH₃OH I -CH₃OH II +OH	SFR_MIXED		IZU98
16	17 45 40	-29 00 27.6	359.9444	-0.0461	G359.9444-0.0464	SiO359.944-0.046 6	42.8 GHz;	-114.9	0.026	0.138	NRO	NRO	+H₂O +CH₃OH I -CH₃OH II +OH	SFR_MIXED		IZU98
17	17 45 40	-29 00 27.6	359.9444	-0.0461	G359.9444-0.0464	SiO359.944-0.046 7	43.1 GHz;	-341.9	0.06	0.388	NRO	NRO	+H₂O +CH₃OH I -CH₃OH II +OH	SFR_MIXED		IZU98
18	17 45 40	-29 00 27.6	359.9444	-0.0461	G359.9444-0.0464	SiO359.944-0.046 7	42.8 GHz;	-341.9	0.093	0.054	NRO	NRO	+H₂O +CH₃OH I -CH₃OH II +OH	SFR_MIXED		IZU98
19	17 45 41.5	-28 59 54.5	359.9550	-0.0459	G359.9550-0.0459	SiO359.955-0.046 1	42.8 GHz;	70	0.065	0.137	NRO	NRO				IZU98
20	17 45 41.5	-28 59 54.5	359.9550	-0.0459	G359.9550-0.0459	SiO359.955-0.046 2	43.1 GHz;	52.6	0.125	0.604	NRO	NRO				IZU98
21	17 45 41.5	-28 59 54.5	359.9550	-0.0459	G359.9550-0.0459	SiO359.955-0.046 2	42.8 GHz;	50.6	0.112	0.66	NRO	NRO				IZU98
22	17 45 41.5	-28 59 54.5	359.9550	-0.0459	G359.9550-0.0459	SiO359.955-0.046 3	42.8 GHz;	-24.7	0.044	0.132	NRO	NRO				IZU98

Non-detection table from Izumiura et al. (1998)