Measuring star formation with resolved observations: the test case of M 33
Artikel i vetenskaplig tidskrift, 2015

Context. Measuring star formation on a local scale is important to constrain star formation laws. It is not clear yet, however, whether and how the measure of star formation is affected by the spatial scale at which a galaxy is observed. Aims. We wish to understand the impact of the resolution on the determination of the spatially resolved star formation rate (SFR) and other directly associated physical parameters such as the attenuation. Methods. We carried out a multi-scale, pixel-by-pixel study of the nearby galaxy M33. Assembling FUV, H alpha, 8 mu m, 24 mu m, 70 mu m, and 100 mu m maps, we have systematically compared the emission in individual bands with various SFR estimators from a resolution of 33 pc to 2084 pc. Results. There are strong, scale-dependent, discrepancies of up to a factor 3 between monochromatic SFR estimators and H alpha + 24 mu m. The scaling factors between individual IR bands and the SFR show a strong dependence on the spatial scale and on the intensity of star formation. Finally, strong variations of the differential reddening between the nebular emission and the stellar continuum are seen, depending on the specific SFR (sSFR) and on the resolution. At the finest spatial scales, there is little differential reddening at high sSFR. The differential reddening increases with decreasing sSFR. At the coarsest spatial scales the differential reddening is compatible with the canonical value found for starburst galaxies. Conclusions. Our results confirm that monochromatic estimators of the SFR are unreliable at scales smaller than 1 kpc. Furthermore, the extension of local calibrations to high-redshift galaxies presents non-trivial challenges because the properties of these systems may be poorly known.

galaxies: star formation

galaxies: ISM

galaxies: individual: M 33

Författare

M. Boquien

Laboratoire d'Astrophysique de Marseille

University of Cambridge Institute of Astronomy

D. Calzetti

University of Massachusetts

Susanne Aalto

Chalmers, Rymd- och geovetenskap, Radioastronomi och astrofysik

A. Boselli

Laboratoire d'Astrophysique de Marseille

J. Braine

Laboratoire d'Astrophysique de Bordeaux

V. Buat

Laboratoire d'Astrophysique de Marseille

F. Combes

Centre national de la recherche scientifique (CNRS)

F. P. Israel

Universiteit Leiden

C. Kramer

Instituto de Radioastronomia Milimetrica

S. Lord

CalTech

M. Relano

Universidad de Granada

E. Rosolowsky

University of Alberta

G. Stacey

Cornell University

F. Tabatabaei

Max Planck-institutet

F. F. S. van der Tak

Rijksuniversiteit Groningen

Netherlands Institute for Space Research (SRON)

P. van der Werf

Universiteit Leiden

S. Verley

Universidad de Granada

M. Xilouris

National Observatory of Athens

Astronomy and Astrophysics

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

Vol. 578 A8

Ämneskategorier

Fusion, plasma och rymdfysik

DOI

10.1051/0004-6361/201423518

Mer information

Senast uppdaterat

2018-09-07