Dense gas in the Galactic central molecular zone is warm and heated by turbulence
Artikel i vetenskaplig tidskrift, 2016

Context. The Galactic center is the closest region where we can study star formation under extreme physical conditions like those in high-redshift galaxies. Aims. We measure the temperature of the dense gas in the central molecular zone (CMZ) and examine what drives it. Methods. We mapped the inner 300 pc of the CMZ in the temperature-sensitive J = 3-2 para-formaldehyde (p-H2CO) transitions. We used the 3(2,1)-2(2,0)/3(0,3)-2(0,2) line ratio to determine the gas temperature in n similar to 10(4) - 10(5) cm(-3) gas. We have produced temperature maps and cubes with 30 0 0 and 1 km s(-1) resolution and published all data in FITS form. Results. Dense gas temperatures in the Galactic center range from similar to 60 K to > 100 K in selected regions. The highest gas temperatures T-G > 100 K are observed around the Sgr B2 cores, in the extended Sgr B2 cloud, the 20 km s(-1) and 50 km s(-1) clouds, and in "The Brick" (G0.253 + 0.016). We infer an upper limit on the cosmic ray ionization rate zeta(CR) < 10(-14) s(-1). Conclusions. 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 similar to 75 pc are confirmed to be high in the entire CMZ.

Galaxy: nucleus

ISM: molecules

Galaxy: center

ISM: structure

ISM: clouds

cosmic rays

Författare

A. Ginsburg

European Southern Observatory (ESO)

C. Henkel

King Abdulaziz University

Max Planck-institutet

Y. Ao

National Institutes of Natural Sciences - National Astronomical Observatory of Japan

Purple Mountain Observatory Chinese Academy of Sciences

D. Riquelme

Max Planck-institutet

J. K. F. Mann

Max Planck-institutet

T. Pillai

Max Planck-institutet

E. A. C. Mills

National Radio Astronomy Observatory

M. A. Requena-Torres

Max Planck-institutet

K. Immer

European Southern Observatory (ESO)

L. Testi

European Southern Observatory (ESO)

J. Ott

National Radio Astronomy Observatory

J. Bally

University of Colorado at Boulder

C. Battersby

Harvard-Smithsonian Center for Astrophysics

J. Darling

University of Colorado at Boulder

Susanne Aalto

Chalmers, Rymd- och geovetenskap, Radioastronomi och astrofysik

T. Stanke

European Southern Observatory (ESO)

S. Kendrew

University of Oxford

J. M. D. Kruijssen

Max Planck-institutet

S. Longmore

Liverpool John Moores University

J. Dale

Ludwig-Maximilians-Universität München

R. Guesten

Max Planck-institutet

K. M. Menten

Max Planck-institutet

Astronomy and Astrophysics

0004-6361 (ISSN) 1432-0746 (eISSN)

Vol. 586 Art nr A50- A50

Ämneskategorier

Astronomi, astrofysik och kosmologi

DOI

10.1051/0004-6361/201526100