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Molecular and atomi...
Molecular and atomic gas in the Local Group galaxy M 33
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- Gratier, P. (författare)
- Laboratoire d'Astrophysique de Bordeaux
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- Braine, J. (författare)
- Laboratoire d'Astrophysique de Bordeaux
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- Rodriguez-Fernandez, N. J. (författare)
- Institut de Radioastronomie Millimétrique (IRAM)
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- Schuster, K. (författare)
- Institut de Radioastronomie Millimétrique (IRAM)
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- Kramer, C. (författare)
- Institut de Radioastronomie Millimétrique (IRAM)
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- Xilouris, E. M. (författare)
- National Observatory of Athens
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- Tabatabaei, F. (författare)
- Max Planck Gesellschaft zur Förderung der Wissenschaften e.V. (MPG),Max Planck Society for the Advancement of Science (MPG)
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- Henkel, C. (författare)
- Max Planck Gesellschaft zur Förderung der Wissenschaften e.V. (MPG),Max Planck Society for the Advancement of Science (MPG)
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- Corbelli, E. (författare)
- Osservatorio Astrofisico di Arcetri,Arcetri Astrophysical Observatory
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- Israel, F. P. (författare)
- Universiteit Leiden (UL),Leiden University (UL)
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- van der Werf, P.P. (författare)
- Universiteit Leiden (UL),Leiden University (UL)
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- Calzetti, D. (författare)
- University of Massachusetts
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- Burillo, S. G. (författare)
- Observatorio Astronómico Nacional (OAN),Spanish National Observatory (OAN)
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- Sievers, A. (författare)
- Institut de Radioastronomie Millimétrique (IRAM)
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- Combes, F. (författare)
- Centre national de la recherche scientifique (CNRS)
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- Wiklind, Tommy, 1957 (författare)
- Space Telescope Science Institute (STScI)
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- Brouillet, N. (författare)
- Laboratoire d'Astrophysique de Bordeaux
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- Herpin, F. (författare)
- Laboratoire d'Astrophysique de Bordeaux
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- Bontemps, S. (författare)
- Laboratoire d'Astrophysique de Bordeaux
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- Aalto, Susanne, 1964 (författare)
- Chalmers tekniska högskola,Chalmers University of Technology
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- Koribalski, B. (författare)
- Commonwealth Scientific and Industrial Research Organisation (CSIRO)
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- van der Tak, F. F. S. (författare)
- Netherlands Institute for Space Research (SRON)
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- Wiedner, M. C. (författare)
- Centre national de la recherche scientifique (CNRS)
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- Rollig, M. (författare)
- Universität zu Köln,University of Cologne
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- Mookerjea, B. (författare)
- Tata Institute of Fundamental Research
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(creator_code:org_t)
- 2010-10-26
- 2010
- Engelska.
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Ingår i: Astronomy and Astrophysics. - : EDP Sciences. - 0004-6361 .- 1432-0746. ; 522:1
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https://doi.org/10.1...
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Abstract
Ämnesord
Stäng
- 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 30 m IRAM telescope in the CO(2-1) line, achieving a resolution of 12 '' x 2.6 km s(-1), 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 8.5 kpc, and covers entirely the 2' x 40' 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 20-50 mK at 2.6 km s(-1) velocity resolution. The CO(2-1) luminosity of the observed region is 1.7 +/- 0.1 x 10(7) K km s(-1) pc(2) and is estimated to be 2.8 +/- 0.3 x 10(7) K km s(-1) pc(2) for the entire galaxy, corresponding to H-2 masses of 1.9 x 10(8) M-circle dot and 3.3 x 10(8) M-circle dot respectively (including He), calculated with N(H-2)/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 8.5 kpc is estimated to be 1.4 x 10(9) M-circle dot. The azimuthally averaged CO surface brightness decreases exponentially with a scale length of 1.9 +/- 0.1 kpc whereas the atomic gas surface density is constant at Sigma(HI) = 6 +/- 2 M-circle dot pc(-2) deprojected to face-on. For an N(H-2)/ICO(1-0) conversion factor twice that of the Milky Way, the central kiloparsec H-2 surface density is Sigma(H2) = 8.5 +/- 0.2 M-circle dot pc(-2). 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 H-alpha and FIR brightness, is constant with radius. The SFE, with a N(H-2)/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 8 kpc from the galaxy center, are presented.
Ämnesord
- NATURVETENSKAP -- Fysik -- Astronomi, astrofysik och kosmologi (hsv//swe)
- NATURAL SCIENCES -- Physical Sciences -- Astronomy, Astrophysics and Cosmology (hsv//eng)
Nyckelord
- spiral galaxies
- Local Group
- ISM: clouds
- m33
- clouds
- metallicity
- ISM
- stellar population
- formation history
- stars: formation
- far-ultraviolet
- galaxies: evolution
- galaxies: individual: M 33
- co emission
- star-formation efficiency
- radio-continuum survey
- galaxies
Publikations- och innehållstyp
- art (ämneskategori)
- ref (ämneskategori)
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Till lärosätets databas
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Gratier, P.
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Braine, J.
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Rodriguez-Fernan ...
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Schuster, K.
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Kramer, C.
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Xilouris, E. M.
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visa fler...
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Tabatabaei, F.
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Henkel, C.
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Corbelli, E.
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Israel, F. P.
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van der Werf, P. ...
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Calzetti, D.
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Burillo, S. G.
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Sievers, A.
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Combes, F.
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Wiklind, Tommy, ...
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Brouillet, N.
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Herpin, F.
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Bontemps, S.
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Aalto, Susanne, ...
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Koribalski, B.
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van der Tak, F. ...
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Wiedner, M. C.
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Rollig, M.
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Mookerjea, B.
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