Star Forming Rates and HI Gas Content in Galaxy Groups

Autor/innen

  • Sarah Katherine Martens University of Wisconsin-Madison

DOI:

https://doi.org/10.17307/wsc.v0i0.132

Schlagworte:

Galaxies, Star-Formation, HI, Galaxy Groups

Abstract

We compare the star formation rates with the respective HI properties of 4854 galaxies in 743 different groups. Using data from the SDSS and the GALEX all sky survey (AIS) we measure the star formation rates and NUV-r colors as a function of the total group mass, position within the group, and HI content as derived from the Arecibo Legacy Fast ALFA (ALFALFA) survey. The NUV-r colors are consistent with star forming field galaxies. We show how the quenching of the star formation is correlated with galaxy HI content and how both are affected by a group environment. 

 

Autor/innen-Biografie

Sarah Katherine Martens, University of Wisconsin-Madison

Undergraduate astrophysics and spanish student at the University of Wisconsin-Madison

Literaturhinweise

[Hess and Wilcots,2013] Evolution in the HI Gas Content of Galaxy Groups: Pre- Processing and Mass Assembly in the Current Epoch The Astronomical Journal http://arxiv.org/abs/1308.4646

[Schawinski and Urry et al.] The green valley is a red herring: Galaxy Zoo reveals two evolutionary pathways toward quenching of star formation in early-and late-type galaxies. Advance Access publication http://arxiv.org/abs/1402.4814

[Haynes et al..] The Arecibo Legacy Fast ALFA Survey: The α.40 HI Sourse Cat- alog, its Characteristics and their Impact on the Derivation of the HI Mass Function. The Astronomical Journal http://arxiv.org/abs/1109.0027

Cover Image of 2015 Proceedings of the Wisconsin Space Conference: Sonex Personal Jet

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Veröffentlicht

2016-02-11

Zitationsvorschlag

Martens, S. K. (2016). Star Forming Rates and HI Gas Content in Galaxy Groups. Proceedings of the Wisconsin Space Conference. https://doi.org/10.17307/wsc.v0i0.132

Ausgabe

2015: Innovations in Flight

Rubrik

Astronomy and Cosmology

Lizenz

Creative Commons License
This work is licensed under a Creative Commons Attribution-NonCommercial 4.0 International License.