2006A&A...455..963R


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.04CET20:55:18

2006A&A...455..963R - Astronomy and Astrophysics, volume 455, 963-969 (2006/9-1)

Coupling the dynamics and the molecular chemistry in the Galactic center.

RODRIGUEZ-FERNANDEZ N.J., COMBES F., MARTIN-PINTADO J., WILSON T.L. and APPONI A.

Abstract (from CDS):

Most of the Galactic center (GC) gas moves in nearly circular orbits in a nuclear ring (hereafter the Galactic center ring, GCR). This is the case of cloud complexes such as Sgr A or Sgr B, where the gas is dense, warm and exhibits a rich molecular chemistry. The origin of these properties is thought to be shocks, in particular due to the large scale dynamics of the Galaxy. In addition, there are gas clouds moving in highly non-circular orbits known from observations of low density tracers such as CO(1-0). The physical conditions of the clouds moving with non-circular velocities are not well known. We have studied the physical conditions of the gas in non-circular orbits to better understand the origin of the unusual physical conditions of the GC molecular gas and the possible effect of the large scale dynamics on these physical conditions. Using published CO(1-0) data, we have selected a set of clouds belonging to all the kinematical components seen in the longitude-velocity diagram of the GC. We have carried out a survey of dense gas in all the components using the J=2-1 lines of CS and SiO as tracers of high density gas and shock chemistry. We have detected CS and SiO emission in all the kinematical components. The gas density and the SiO abundance of the clouds in non-circular orbits are similar to those in the GCR. Therefore, in all the kinematical components there are dense clouds that can withstand the tidal shear. However, there is no evidence of star formation outside the GCR. The high relative velocity and shear expected in the dust lanes along the bar major axis could inhibit the star formation process, as observed in other galaxies. The high SiO abundances derived in the non-circular velocity clouds are likely due to the large-scale shocks that created the dust lanes.

Abstract Copyright:

Journal keyword(s): ISM: kinematics and dynamics - ISM: molecules - galaxies: ISM - radio lines : ISM

Simbad objects: 18

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Number of rows : 18

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NGC 253 SyG 00 47 33.134 -25 17 19.68   8.03   6.94 8.1 ~ 3001 2
2 M 77 GiP 02 42 40.771 -00 00 47.84 9.70 9.61 8.87 10.1 9.9 ~ 4179 2
3 IC 342 SBG 03 46 48.514 +68 05 45.98   10.5       ~ 1407 1
4 NGC 1530 G 04 23 27.102 +75 17 44.05   13.40       ~ 257 1
5 NAME Orion Bright Bar reg 05 35 22.30 -05 24 33.0           ~ 743 0
6 M 82 IG 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5429 6
7 NGC 5383 GiG 13 57 04.975 +41 50 46.60   12.5   10.95   ~ 315 0
8 NAME Sgr E Rad 17 42 38 -29 48.2           ~ 46 0
9 NAME Sgr C MoC 17 44 36.3 -29 28 13           ~ 318 0
10 NAME Sgr A Region reg 17 45 12 -28 48.3           ~ 920 0
11 GAL 000.0+00.0 gam 17 45 39.60213 -29 00 22.0000           ~ 12009 0
12 NAME Sgr A* X 17 45 40.03599 -29 00 28.1699           ~ 3601 3
13 NAME Sgr B MoC 17 47 02 -28 25.4           ~ 195 0
14 NAME Sgr B2 MoC 17 47 20.4 -28 23 07           ~ 1981 1
15 NAME Sgr D MoC 17 48 41.75 -28 01 45.0           ~ 123 1
16 NAME 1.3 Cloud complex MoC 17 49 12.2 -27 52 38           ~ 5 0
17 Bania Clump 2 MoC 17 51 42.6 -26 17 18           ~ 33 1
18 SH 2-140 OpC 22 19 07.8 +63 17 07           ~ 636 2

    Equat.    Gal    SGal    Ecl

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2021.03.04-20:55:18

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