2016A&A...586A..50G


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.20CEST19:57:39

2016A&A...586A..50G - Astronomy and Astrophysics, volume 586A, 50-50 (2016/2-1)

Dense gas in the Galactic central molecular zone is warm and heated by turbulence.

GINSBURG A., HENKEL C., AO Y., RIQUELME D., KAUFFMANN J., PILLAI T., MILLS E.A.C., REQUENA-TORRES M.A., IMMER K., TESTI L., OTT J., BALLY J., BATTERSBY C., DARLING J., AALTO S., STANKE T., KENDREW S., KRUIJSSEN J.M.D., LONGMORE S., DALE J., GUESTEN R. and MENTEN K.M.

Abstract (from CDS):

The Galactic center is the closest region where we can study star formation under extreme physical conditions like those in high-redshift galaxies. We measure the temperature of the dense gas in the central molecular zone (CMZ) and examine what drives it. We mapped the inner 300pc of the CMZ in the temperature-sensitive J=3-2 para-formaldehyde (p-H2CO transitions. We used the 32,1-22,0/30,3-20,2 line ratio to determine the gas temperature in n∼104-105cm–3 gas. We have produced temperature maps and cubes with 30'' and 1km/s resolution and published all data in FITS form. Dense gas temperatures in the Galactic center range from ∼60K to >100K in selected regions. The highest gas temperatures TG>100K are observed around the Sgr B2 cores, in the extended Sgr B2 cloud, the 20km/s and 50km/s clouds, and in ``The Brick'' (G0.253+0.016). We infer an upper limit on the cosmic ray ionization rate ζCR<10–14s–1 . The dense molecular gas temperature of the region around our Galactic center is similar to values found in the central regions of other galaxies, in particular starburst systems. The gas temperature is uniformly higher than the dust temperature, confirming that dust is a coolant in the dense gas. Turbulent heating can readily explain the observed temperatures given the observed line widths. Cosmic rays cannot explain the observed variation in gas temperatures, so CMZ dense gas temperatures are not dominated by cosmic ray heating. The gas temperatures previously observed to be high in the inner ∼75pc are confirmed to be high in the entire CMZ.

Abstract Copyright:

Journal keyword(s): Galaxy: center - ISM: molecules - ISM: structure - Galaxy: nucleus - cosmic rays - ISM: clouds

VizieR on-line data: <Available at CDS (J/A+A/586/A50): fitted.dat temp.dat list.dat cubes/* integrated/* hdf5/*>

Status in Simbad:  being processed

Simbad objects: 11

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Number of rows : 11

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 NGC 1365 Sy1 03 33 36.458 -36 08 26.37 10.48 10.08 9.63 8.79 9.7 ~ 1473 2
2 M 82 IG 09 55 52.430 +69 40 46.93 9.61 9.30 8.41     ~ 5213 6
3 M 83 SBG 13 37 00.919 -29 51 56.74 8.85 8.11 7.52 7.21   ~ 2160 2
4 NAME Sgr C MoC 17 44 36.3 -29 28 13           ~ 297 0
5 NAME Sgr A* X 17 45 40.03599 -29 00 28.1699           ~ 3266 3
6 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11004 0
7 NAME the Brick MoC 17 46 09.7 -28 43 31           ~ 128 0
8 NAME Sgr B1 MoC 17 47 02.0 -28 31 57           ~ 119 0
9 NAME Sgr B2 MoC 17 47 20.4 -28 23 07           ~ 1851 1
10 GAL 001.6-00.025 MoC 17 49 29 -27 36.8           ~ 26 0
11 NGC 6946 H2G 20 34 52.332 +60 09 13.24   10.5       ~ 2181 2

    Equat.    Gal    SGal    Ecl

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2019.10.20-19:57:39

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