Star-forming environments throughout the M101 Group
|Author:||Watkins, Aaron E.1,2; Mihos, J. Christopher1; Harding, Paul1|
1Department of Astronomy, Case Western Reserve University, Cleveland, OH 44106, USA
2Astronomy Research Unit, University of Oulu, FI-90014, Finland
|Online Access:||PDF Full Text (PDF, 3.1 MB)|
|Persistent link:|| http://urn.fi/urn:nbn:fi-fe2018061325823
|Publish Date:|| 2018-06-13
We present a multiwavelength study of star formation within the nearby M101 Group, including new deep Hα imaging of M101 and its two companions. We perform a statistical analysis of the Hα-to-FUV flux ratios in H ii regions located in three different environments: M101’s inner disk, M101’s outer disk, and M101’s lower-mass companion galaxy NGC 5474. We find that, once bulk radial trends in extinction are taken into account, both the median and scatter in F Hα /F FUV in H ii regions are invariant across all of these environments. Also, using Starburst99 models, we are able to qualitatively reproduce the distributions of F Hα /F FUV throughout these different environments using a standard Kroupa initial mass function (IMF); hence, we find no need to invoke truncations in the upper-mass end of the IMF to explain the young star-forming regions in the M101 Group even at extremely low surface density. This implies that star formation in low-density environments differs from star formation in high-density environments only by intensity and not by cloud-to-cloud physics.
|Type of Publication:||
A1 Journal article – refereed
|Field of Science:||
115 Astronomy and space science
This work has been supported by the National Science Foundation through award 1108964 to JCM, as well as through award 1211144 to PH.
© 2017. The American Astronomical Society. All rights reserved. Published in this repository with the kind permission of the publisher.