H I clouds in the proximity of M 33

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Free access article

Issue		A&A Volume 487, Number 1, August III 2008


Page(s)		161 - 175
Section		Extragalactic astronomy
DOI		http://dx.doi.org/10.1051/0004-6361:200810220
Published online		04 June 2008

A&A 487, 161-175 (2008)
DOI: 10.1051/0004-6361:200810220

H I clouds in the proximity of M 33

M. Grossi¹, C. Giovanardi¹, E. Corbelli¹, R. Giovanelli², M. P. Haynes², A. M. Martin², A. Saintonge³, and J. D. Dowell⁴

¹ INAF - Osservatorio Astrofisico di Arcetri, L.go E. Fermi 5, 50125, Florence
e-mail: grossi@arcetri.astro.it
² Center for Radiophysics and Space Research, Cornell University, Ithaca, NY 14853, USA
³ Institute for Theoretical Physics, University of Zurich, 8057 Zurich, Switzerland
⁴ Department of Astronomy, Indiana University, Bloomington, IN 47405, USA

Received 19 May 2008 / Accepted 31 May 2008

Abstract
Aims. Neutral hydrogen clouds are found in the Milky Way and Andromeda halo both as large complexes and smaller isolated clouds. Here we present a search for HI clouds in the halo of M 33, the third spiral galaxy of the Local Group.
Methods. We have used two complementary data sets: a 3° $\times$ 3° map of the area provided by the Arecibo Legacy Fast ALFA (ALFALFA) survey and deeper pointed observations carried out with the Arecibo telescope in two fields that permit sampling of the northeastern and southwestern edges of the HI disc.
Results. The total amount of HI around M 33 detected by our survey is about 10⁷ $M_{\odot}$ . At least 50% of this mass is made of HI clouds that are related both in space and velocity to the galaxy. We discuss several scenarios for the origin of these clouds focusing on the two most interesting ones: (a) dark-matter dominated gaseous satellites, (b) debris from filaments flowing into M 33 from the intergalactic medium or generated by a previous interaction with M 31. Both scenarios seem to fit with the observed cloud properties. Some structures are found at anomalous velocities, particularly an extended HI complex previously detected by Thilker et al. (2002). Even though the ALFALFA observations seem to indicate that this cloud is possibly connected to M 33 by a faint gas bridge, we cannot firmly establish its extragalactic nature or its relation to M 33.
Conclusions. Taking into account that the clouds associated with M 33 are likely to be highly ionised by the extragalactic ultraviolet (UV) radiation, we predict that the total gas mass associated with them is $\ge$ 5 $\times$ 10⁷ $M_{\odot}$ . If the gas is steadily falling towards the M 33 disc it can provide the fuel needed to sustain a current star formation rate of 0.5 $M_{\odot}$ yr^-1.

Key words: galaxies: individual: M 33 -- galaxies: evolution -- galaxies: halos

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