Planck intermediate results: XXV. The Andromeda galaxy as seen by Planck

Research output: Contribution to journalArticle

Researchers

  • P. A. R. Ade
  • N. Aghanim
  • M. Arnaud
  • M. Ashdown
  • J. Aumont
  • C. Baccigalupi
  • A. J. Banday
  • R. B. Barreiro
  • N. Bartolo
  • E. Battaner
  • R. Battye
  • K. Benabed
  • G. J. Bendo
  • A. Benoit-Levy
  • J. -P. Bernard
  • M. Bersanelli
  • P. Bielewicz
  • A. Bonaldi
  • L. Bonavera
  • J. R. Bond
  • J. Borrill
  • F. R. Bouchet
  • C. Burigana
  • R. C. Butler
  • E. Calabrese
  • J. -F. Cardoso
  • A. Catalano
  • A. Chamballu
  • R. -R. Chary
  • X. Chen
  • H. C. Chiang
  • P. R. Christensen
  • D. L. Clements
  • L. P. L. Colombo
  • C. Combet
  • F. Couchot
  • A. Coulais
  • B. P. Crill
  • A. Curto
  • F. Cuttaia
  • L. Danese
  • R. D. Davies
  • R. J. Davis
  • P. de Bernardis
  • A. de Rosa
  • G. de Zotti
  • J. Delabrouille
  • C. Dickinson
  • J. M. Diego
  • Anne Lähteenmäki

  • Planck Collaboration

Research units

  • University of Granada
  • Univ Manchester, Jodrell Bank Centre for Astrophysics, University of Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, UK ALMA Reg Ctr Node
  • University of California at Berkeley
  • UPMC, Pierre & Marie Curie University - Paris 6, University of Paris Sorbonne - Paris IV, Univ Paris 04, UMR 7095, Inst Astrophys Paris
  • University of Oxford
  • Telecom ParisTech
  • Cardiff University
  • University of Cambridge
  • International School for Advanced Studies
  • Univ Toulouse, Centre National de la Recherche Scientifique (CNRS), Universite de Toulouse, PRES Universite de Toulouse, Universite Toulouse III - Paul Sabatier, UPS OMP, IRAP
  • Univ Cantabria, Consejo Superior de Investigaciones Cientificas (CSIC), Universidad de Cantabria, CSIC, Inst Fis Cantabria
  • Ist Nazl Fis Nucl, Istituto Nazionale di Fisica Nucleare, Sez Padova
  • Univ Manchester, Jodrell Bank Centre for Astrophysics, University of Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys
  • Univ Paris 06, Pierre & Marie Curie University - Paris 6, UMR7095
  • INAF IASF Milano, Istituto Nazionale Astrofisica - Italy
  • University of Toronto
  • Ist Nazl Fis Nucl, Istituto Nazionale Geofisica e Vulcanologia (INGV), Istituto Nazionale di Fisica Nucleare, Sez Bologna
  • IASF Bologna, Istituto Nazionale Astrofisica - Italy, INAF
  • California Institute of Technology
  • Princeton University
  • Niels Bohr Inst, Niels Bohr Institute, University of Copenhagen
  • Imperial College London
  • Observ Paris, Centre National de la Recherche Scientifique (CNRS)
  • Sapienza University Rome
  • CEA Saclay, CEA, Centre National de la Recherche Scientifique (CNRS), PRES University Sorbonne Paris Cite, University of Paris Diderot - Paris VII, Univ Paris Diderot, CNRS, CEA DSM,IRFU,Serv Astrophys,Lab AIM
  • Université Grenoble Alpes

Abstract

The Andromeda galaxy (M 31) is one of a few galaxies that has sufficient angular size on the sky to be resolved by the Planck satellite. Planck has detected M 31 in all of its frequency bands, and has mapped out the dust emission with the High Frequency Instrument, clearly resolving multiple spiral arms and sub-features. We examine the morphology of this long-wavelength dust emission as seen by Planck, including a study of its outermost spiral arms, and investigate the dust heating mechanism across M 31. We find that dust dominating the longer wavelength emission (greater than or similar to 0.3 mm) is heated by the diffuse stellar population (as traced by 3.6 mu m emission), with the dust dominating the shorter wavelength emission heated by a mix of the old stellar population and star-forming regions (as traced by 24 mu m emission). We also fit spectral energy distributions for individual 5' pixels and quantify the dust properties across the galaxy, taking into account these different heating mechanisms, finding that there is a linear decrease in temperature with galactocentric distance for dust heated by the old stellar population, as would be expected, with temperatures ranging from around 22 K in the nucleus to 14 K outside of the 10 kpc ring. Finally, we measure the integrated spectrum of the whole galaxy, which we find to be well-fitted with a global dust temperature of (18.2 +/- 1.0) K with a spectral index of 1.62 +/- 0.11 (assuming a single modified blackbody), and a significant amount of free-free emission at intermediate frequencies of 20-60 GHz, which corresponds to a star formation rate of around 0.12 M-circle dot yr(-1). We find a 2.3 sigma detection of the presence of spinning dust emission, with a 30 GHz amplitude of 0.7 +/- 0.3 Jy, which is in line with expectations from our Galaxy.

Details

Original languageEnglish
Article number28
Pages (from-to)p. A28
Number of pages23
JournalAstronomy and Astrophysics
Volume582
Issue number1
Publication statusPublished - Oct 2015
MoE publication typeA1 Journal article-refereed

    Research areas

  • galaxies: individual: Messier 31, galaxies: structure, galaxies: ISM, submillimeter: galaxies, radio continuum: galaxies, MULTIBAND IMAGING PHOTOMETER, RADIO-CONTINUUM SURVEY, PRE-LAUNCH STATUS, SPITZER-SPACE-TELESCOPE, FAR-INFRARED LUMINOSITY, SPINNING DUST EMISSION, RESOLUTION IRAS MAPS, STAR-FORMATION RATES, LOCAL GROUP GALAXIES, COMPLETE CO SURVEY

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