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The MUSE QSO Blind Survey: A Census of Absorber Host Galaxies

Published online by Cambridge University Press:  21 March 2017

Lorrie A. Straka  and
the MUSE GTO consortium
Lorrie A. Straka
Affiliation:
Sterrewacht Leiden, Leiden University Niels Bohrweg 2, NL-2333CA, Leiden, the Netherlands email: straka@strw.leidenuniv.nl
the MUSE GTO consortium
Affiliation:
Centre de Recherche Astrophysique de Lyon (CRAL), France; Leibniz Institute for Astrophysics Potsdam (AIP), Germany; The Research Institute in Astrophysics and Planetology (IRAP) Toulouse, France; Leiden Observatory/NOVA, the Netherlands; Georg-August-Universitat Gottingen, Germany; ETH Zurich, Switzerland; ESO
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Abstract

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Understanding the distribution of gas in galaxies and its interaction with the IGM is crucial to complete the picture of galaxy evolution. At all redshifts, absorption features seen in QSO spectra serve as a unique probe of the gaseous content of foreground galaxies and the IGM, extending out to 200 kpc. Studies show that star formation history is intimately related to the co-evolution of galaxies and the IGM. In order to study the environments traced by absorption systems and the role of inflows and outflows, it is critical to measure the emission properties of host galaxies and their halos. We overcome the challenge of detecting absorption host galaxies with the MUSE integral field spectrograph on VLT. MUSE’s large field of view and sensitivity to emission lines has allowed a never-before seen match between the number density of absorbers along QSO sightlines and the number density of emission line galaxies within 200 kpc of the QSO. These galaxies represent a sample for which previously elusive connections can be made between mass, metallicity, SFR, and absorption.

Keywords

galaxies: IGMquasars: absorption linesgalaxies: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S321: Formation and Evolution of Galaxy Outskirts , March 2016 , pp. 351 - 353
Copyright
Copyright © International Astronomical Union 2017 

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