2019A&A...632A..58R


C.D.S. - SIMBAD4 rel 1.7 - 2021.01.19CET17:17:24

2019A&A...632A..58R - Astronomy and Astrophysics, volume 632A, 58-58 (2019/12-0)

CHIMPS: physical properties of molecular clumps across the inner Galaxy.

RIGBY A.J., MOORE T.J.T., EDEN D.J., URQUHART J.S., RAGAN S.E., PERETTO N., PLUME R., THOMPSON M.A., CURRIE M.J. and PARK G.

Abstract (from CDS):

The latest generation of high-angular-resolution unbiased Galactic plane surveys in molecular-gas tracers are enabling the interiors of molecular clouds to be studied across a range of environments. The CO Heterodyne Inner Milky Way Plane Survey (CHIMPS) simultaneously mapped a sector of the inner Galactic plane, within 27.8°≤l≤46.2° and |b|≤0.5°, in 13CO (3-2) and C18O (3-2) at an angular resolution of 15 arcsec. The combination of the CHIMPS data with 12CO (3-2) data from the CO High Resolution Survey (COHRS) has enabled us to perform a voxel-by-voxel local-thermodynamic-equilibrium (LTE) analysis, determining the excitation temperature, optical depth, and column density of 13CO at each l, b, v position. Distances to discrete sources identified by FELLWALKER in the 13CO (3-2) emission maps were determined, allowing the calculation of numerous physical properties of the sources, and we present the first source catalogues in this paper. We find that, in terms of size and density, the CHIMPS sources represent an intermediate population between large-scale molecular clouds identified by CO and dense clumps seen in thermal dust continuum emission, and therefore represent the bulk transition from the diffuse to the dense phase of molecular gas. We do not find any significant systematic variations in the masses, column densities, virial parameters, mean excitation temperature, or the turbulent pressure over the range of Galactocentric distance probed, but we do find a shallow increase in the mean volume density with increasing Galactocentric distance. We find that inter-arm clumps have significantly narrower linewidths, and lower virial parameters and excitation temperatures than clumps located in spiral arms. When considering the most reliable distance-limited subsamples, the largest variations occur on the clump-to-clump scale, echoing similar recent studies that suggest that the star-forming process is largely insensitive to the Galactic-scale environment, at least within the inner disc.

Abstract Copyright: © ESO 2019

Journal keyword(s): molecular data - surveys - stars: formation - ISM: molecules - ISM: structure - Galaxy: structure

VizieR on-line data: <Available at CDS (J/A+A/632/A58): table1.dat table1.fits table4.dat table4.fits>

Nomenclature: Tables 1+4: CHIMPS NNNN (Nos 0001-4999) = CHIMPS GLLL.lll+BB.bbb N=4999.

Status at CDS : All or part of tables of objects will be ingested in SIMBAD with priority 1.

Simbad objects: 14

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Number of rows : 14

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 NAME Per Arm PoG 03 30 +45.0           ~ 1286 0
2 M 51 GiP 13 29 52.698 +47 11 42.93   9.26 8.36 8.40   ~ 3867 4
3 NAME Nor Arm PoG 16 00 -50.0           ~ 351 0
4 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11926 0
5 NAME Aql Rift DNe 18 32 -01.0           ~ 247 1
6 SNR G030.8-00.0 SNR 18 47 32 -01 56.5           ~ 452 0
7 OH 34.26 +0.15 SFR 18 53 18.54 +01 14 57.9           ~ 469 0
8 NAME Sgr Arm PoG 19 00 -30.0           ~ 540 1
9 W 49 SFR 19 10 20 +09 07.7           ~ 518 1
10 W 51 SNR 19 23 50 +14 06.0           ~ 1166 1
11 NAME Outer Arm PoG 21 48 +69.4           ~ 229 0
12 NAME Aql Region reg ~ ~           ~ 315 0
13 NAME Scutum Spiral Arm PoG ~ ~           ~ 287 0
14 NAME Sct-Cen PoG ~ ~           ~ 143 0

    Equat.    Gal    SGal    Ecl

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2021.01.19-17:17:24

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