2010A&A...522A...3G


C.D.S. - SIMBAD4 rel 1.7 - 2019.07.19CEST08:52:24

2010A&A...522A...3G - Astronomy and Astrophysics, volume 522, A3-3 (2010/11-1)

Molecular and atomic gas in the local group galaxy M 33.

GRATIER P., BRAINE J., RODRIGUEZ-FERNANDEZ N.J., SCHUSTER K.F., KRAMER C., XILOURIS E.M., TABATABAEI F.S., HENKEL C., CORBELLI E., ISRAEL F., VAN DER WERF P.P., CALZETTI D., GARCIA-BURILLO S., SIEVERS A., COMBES F., WIKLIND T., BROUILLET N., HERPIN F., BONTEMPS S., AALTO S., KORIBALSKI B., VAN DER TAK F., WIEDNER M.C., ROELLIG M. and MOOKERJEA B.

Abstract (from CDS):

We present high-resolution large-scale observations of the molecular and atomic gas in the Local Group galaxy M 33. The observations were carried out using the HEterodyne Receiver Array (HERA) at the 30m IRAM telescope in the CO(2-1) line, achieving a resolution of 12"x2.6km/s, enabling individual giant molecular clouds (GMCs) to be resolved. The observed region is 650 square arcminutes mainly along the major axis and out to a radius of 8.5kpc, and covers entirely the 2'x40' radial strip observed with the HIFI and PACS Spectrometers as part of the HERM33ES Herschel key program. The achieved sensitivity in main-beam temperature is 20-50mK at 2.6km/s velocity resolution. The CO(2-1) luminosity of the observed region is 1.7±0.1x107K.km/s.pc2 and is estimated to be 2.8±0.3x107K.km/s.pc2 for the entire galaxy, corresponding to H2 masses of 1.9x108M and 3.3x108M respectively (including He), calculated with N(H2)/ICO(1–0) twice the Galactic value due to the half-solar metallicity of M 33. The HI 21 cm VLA archive observations were reduced, and the mosaic was imaged and cleaned using the multi-scale task in the CASA software package, yielding a series of datacubes with resolutions ranging from 5" to 25". The HI mass within a radius of 8.5kpc is estimated to be 1.4x109M. The azimuthally averaged CO surface brightness decreases exponentially with a scale length of 1.9±0.1kpc whereas the atomic gas surface density is constant at ΣHI=6±2M/pc2 deprojected to face-on. For an N(H2)/ICO(1–0) conversion factor twice that of the Milky Way, the central kiloparsec H2 surface density is ΣH2=8.5±0.2M/pc2. The star formation rate per unit molecular gas (SF efficiency, the rate of transformation of molecular gas into stars), as traced by the ratio of CO to Hα and FIR brightness, is constant with radius. The SFE, with a N(H2)/ICO(1–0) factor twice galactic, appears 2-4 times greater than for large spiral galaxies. A morphological comparison of molecular and atomic gas with tracers of star formation is presented showing good agreement between these maps both in terms of peaks and holes. A few exceptions are noted. Several spectra, including those of a molecular cloud situated more than 8kpc from the galaxy center, are presented.

Abstract Copyright:

Journal keyword(s): galaxies: individual: M 33 - Local Group - galaxies: evolution - galaxies: ISM - ISM: clouds - stars: formation

VizieR on-line data: <Available at CDS (J/A+A/522/A3): CO12secmom0.fits HI17secmom0.fits>

Simbad objects: 7

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Number of rows : 7

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 IC 10 G 00 20 23.16 +59 17 34.7   13.6 9.5     ~ 973 0
2 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 10481 1
3 M 33 GiG 01 33 50.904 +30 39 35.79 6.17 6.27 5.72     ~ 4991 1
4 NGC 604 HII 01 34 32.1 +30 47 01           ~ 538 0
5 3C 48 QSO 01 37 41.2995845985 +33 09 35.079126038   16.62 16.20     ~ 2415 2
6 NGC 4414 GiG 12 26 27.089 +31 13 24.76 11.12 10.96 10.12     ~ 502 2
7 NAME Local Group GrG ~ ~           ~ 6586 0

    Equat.    Gal    SGal    Ecl

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2019.07.19-08:52:24

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