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Galaxy and Mass Assembly (GAMA) : the life and times of L-star galaxies

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Date
01/05/2013
Author
Robotham, A. S. G.
Liske, J.
Driver, S. P.
Sansom, A. E.
Baldry, I. K.
Bauer, A. E.
Bland-Hawthorn, J.
Brough, S.
Brown, M. J. I.
Colless, M.
Christodoulou, L.
Drinkwater, M. J.
Grootes, M. W.
Hopkins, A. M.
Kelvin, L. S.
Norberg, P.
Loveday, J.
Phillipps, S.
Sharp, R.
Taylor, E. N.
Tuffs, R. J.
Funder
Science & Technology Facilities Council
Grant ID
ST/J001651/1
Keywords
Large-scale structure of Universe
Digital sky survey
Milky Way
Luminosity function
Spiral galaxies
Stellar mass
Redshift survey
Dwarf galaxies
Local group
QB Astronomy
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Abstract
In this work, we investigate in detail the effects the local environment (groups and pairs) has on galaxies with stellar mass similar to the Milky Way (L* galaxies). A volume limited sample of 6150 galaxies are visually classified to determine the emission features, morphological type and presence of a disc. This large sample allows for the significant characteristics of galaxies to be isolated (e.g. stellar mass and group halo mass), and their codependencies determined. We observe that galaxy-galaxy interactions play the most important role in shaping the evolution within a group halo; the main role of halo mass is in gathering the galaxies together to encourage such interactions. Dominant pair galaxies find their overall star formation enhanced when the pair's mass ratio is close to 1; otherwise, we observe the same galaxies as we would in an unpaired system. The minor galaxy in a pair is greatly affected by its companion galaxy, and while the star-forming fraction is always suppressed relative to equivalent stellar mass unpaired galaxies, it becomes lower still when the mass ratio of a pair system increases. We find that, in general, the close galaxy-galaxy interaction rate drops as a function of halo mass for a given amount of stellar mass. We find evidence of a local peak of interactions for Milky Way stellar mass galaxies in Milky Way halo mass groups. Low-mass haloes, and in particular Local Group mass haloes, are an important environment for understanding the typical evolutionary path of a unit of stellar mass. We find compelling evidence for galaxy conformity in both groups and pairs, where morphological type conformity is dominant in groups, and emission class conformity is dominant in pairs. This suggests that group scale conformity is the result of many galaxy encounters over an extended period of time, while pair conformity is a fairly instantaneous response to a transitory interaction.
Citation
Robotham , A S G , Liske , J , Driver , S P , Sansom , A E , Baldry , I K , Bauer , A E , Bland-Hawthorn , J , Brough , S , Brown , M J I , Colless , M , Christodoulou , L , Drinkwater , M J , Grootes , M W , Hopkins , A M , Kelvin , L S , Norberg , P , Loveday , J , Phillipps , S , Sharp , R , Taylor , E N & Tuffs , R J 2013 , ' Galaxy and Mass Assembly (GAMA) : the life and times of L-star galaxies ' , Monthly Notices of the Royal Astronomical Society , vol. 431 , no. 1 , pp. 167-193 . https://doi.org/10.1093/mnras/stt156
Publication
Monthly Notices of the Royal Astronomical Society
Status
Peer reviewed
DOI
https://doi.org/10.1093/mnras/stt156
ISSN
0035-8711
Type
Journal article
Rights
© 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society.
Description
This work was part funded by STFC and SUPA.
Collections
  • University of St Andrews Research
URI
http://hdl.handle.net/10023/3946

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