Volume 589, May 2016
|Number of page(s)||9|
|Section||Galactic structure, stellar clusters and populations|
|Published online||22 April 2016|
A survey of HI gas toward the Andromeda galaxy
Argelander-Institut für Astronomie,
Auf dem Hügel 71,
2 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
Received: 23 April 2015
Accepted: 16 February 2016
Context. The subsequent coalescence of low-mass halos over cosmic time is thought to be the major formation channel of massive spiral galaxies like the Milky Way and the Andromeda galaxy (M 31). The gaseous halo of a massive galaxy is considered to be the reservoir of baryonic matter persistently fueling the star formation in the disk. Because of its proximity, M 31 is the ideal object for studying the structure of the halo gas in great detail.
Aims. Using the latest neutral atomic hydrogen (HI) data of the Effelsberg-Bonn HI Survey (EBHIS) allows comprising a comprehensive inventory of gas associated with M 31. The primary aim is to differentiate between physical structures belonging to the Milky Way Galaxy and M 31 and accordingly to test the presence of a M 31 neutral gaseous halo.
Methods. Analyzing the spatially fully sampled EBHIS data makes it feasible to trace coherent HI structures in space and radial velocity. To disentangle Milky Way and M 31 HI emission we use a new approach, along with the traditional path of setting an upper radial velocity limit, by calculating a difference second moment map.
Results. We argue that M 31’s disk is physically connected to an asymmetric HI halo of tens of kpc size, the M 31 cloud. We confirm the presence of a coherent low-velocity HI filament located in between M 31 and M 33 aligned at the sky with the clouds at systemic velocity. The physical parameters of the HI filament are comparable to those of the HI clouds at systemic velocity. We also detected an irregularly shaped HI cloud that is is positionally located close to but offset from the stellar body of And XIX.
Key words: galaxies: halos / Galaxy: evolution / galaxies: individual: M 31 / radio lines: ISM
© ESO, 2016
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