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Strongly time-variable ultraviolet metal-line emission from the circum-galactic medium of high-redshift galaxies

Sravan, Niharika and Faucher-Giguère, Claude-André and van de Voort, Freeke and Kereš, Dušan and Muratov, Alexander L. and Hopkins, Philip F. and Feldmann, Robert and Quataert, Eliot and Murray, Norman (2016) Strongly time-variable ultraviolet metal-line emission from the circum-galactic medium of high-redshift galaxies. Monthly Notices of the Royal Astronomical Society, 463 (1). pp. 120-133. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20161128-151737516

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Abstract

We use cosmological simulations from the Feedback In Realistic Environments project, which implement a comprehensive set of stellar feedback processes, to study ultraviolet (UV) metal-line emission from the circum-galactic medium of high-redshift (z = 2–4) galaxies. Our simulations cover the halo mass range M_h ∼ 2 × 10^(11)–8.5 × 10^(12) M_⊙ at z = 2, representative of Lyman break galaxies. Of the transitions we analyse, the low-ionization C iii (977 Å) and Si iii (1207 Å) emission lines are the most luminous, with C iv (1548 Å) and Si iv (1394 Å) also showing interesting spatially extended structures. The more massive haloes are on average more UV-luminous. The UV metal-line emission from galactic haloes in our simulations arises primarily from collisionally ionized gas and is strongly time variable, with peak-to-trough variations of up to ∼2 dex. The peaks of UV metal-line luminosity correspond closely to massive and energetic mass outflow events, which follow bursts of star formation and inject sufficient energy into galactic haloes to power the metal-line emission. The strong time variability implies that even some relatively low-mass haloes may be detectable. Conversely, flux-limited samples will be biased towards haloes whose central galaxy has recently experienced a strong burst of star formation. Spatially extended UV metal-line emission around high-redshift galaxies should be detectable by current and upcoming integral field spectrographs such as the Multi Unit Spectroscopic Explorer on the Very Large Telescope and Keck Cosmic Web Imager.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1093/mnras/stw1962DOIArticle
http://mnras.oxfordjournals.org/content/463/1/120.abstractPublisherArticle
https://arxiv.org/abs/1510.06410arXivDiscussion Paper
ORCID:
AuthorORCID
Faucher-Giguère, Claude-André0000-0002-4900-6628
van de Voort, Freeke0000-0002-6301-638X
Kereš, Dušan0000-0002-1666-7067
Hopkins, Philip F.0000-0003-3729-1684
Feldmann, Robert0000-0002-1109-1919
Quataert, Eliot0000-0001-9185-5044
Additional Information:© 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2016 August 4. Received 2016 August 4. In original form 2015 October 20. First published online August 8, 2016. We are grateful to Alex Richings for assistance with the local source test. The simulations analysed in this paper were run on XSEDE computational resources (allocations TG-AST120025, TG-AST130039, and TG-AST140023), on the NASA Pleiades cluster (allocation SMD-14-5189), on the Caltech compute cluster ‘Zwicky’ (NSF MRI award #PHY-0960291), and on the Quest cluster at Northwestern University. NS and CAFG were supported by NSF through grants AST-1412836 and AST-1517491, by NASA through grant NNX15AB22G, and by Northwestern University funds. DK was supported by NSF grant AST-1412153 and funds from the University of California, San Diego. Support for PFH was provided by an Alfred P. Sloan Research Fellowship, NASA ATP grant NNX14AH35G, and NSF Collaborative Research grant #1411920 and CAREER grant #1455342. RF acknowledges support for this work by NASA through Hubble Fellowship grant HF-51304.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. EQ was supported by NASA ATP grant 12-APT12- 0183, a Simons Investigator award from the Simons Foundation, the David and Lucile Packard Foundation, and the Thomas Alison Schneider Chair in Physics at UC Berkeley.
Group:TAPIR
Funders:
Funding AgencyGrant Number
NSFPHY-0960291
NSFAST-1412836
NSFAST-1517491
NASANNX15AB22G
Northwestern UniversityUNSPECIFIED
NSFAST-1412153
University of California, San DiegoUNSPECIFIED
Alfred P. Sloan FoundationUNSPECIFIED
NASANNX14AH35G
NSFAST-1411920
NSFAST-1455342
NASA Hubble FellowshipHF-51304.01-A
Space Telescope Science InstituteUNSPECIFIED
NASANAS 5-26555
NASA12-APT12- 0183
Simons FoundationUNSPECIFIED
David and Lucile Packard FoundationUNSPECIFIED
Thomas Alison Schneider Chair in Physics at UC BerkeleyUNSPECIFIED
NSFTG-AST120025
NSFTG-AST130039
NSFTG-AST140023
Subject Keywords:galaxies: evolution galaxies: formation galaxies: high-redshift galaxies: haloes intergalactic medium cosmology: theory
Issue or Number:1
Record Number:CaltechAUTHORS:20161128-151737516
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20161128-151737516
Official Citation:Niharika Sravan, Claude-André Faucher-Giguère, Freeke van de Voort, Dušan Kereš, Alexander L. Muratov, Philip F. Hopkins, Robert Feldmann, Eliot Quataert, and Norman Murray Strongly time-variable ultraviolet metal-line emission from the circum-galactic medium of high-redshift galaxies MNRAS (November 21, 2016) Vol. 463 120-133 doi:10.1093/mnras/stw1962 first published online August 8, 2016
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:72341
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:28 Nov 2016 23:46
Last Modified:09 Mar 2020 13:18

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