Skip to content
Home
About Us
Resources
Profiles Metrics
Authors Directory
Institutions Directory
Top Authors
Top Institutions
Top Sponsors
AI Digest
Contact Us
Menu
Home
About Us
Resources
Profiles Metrics
Authors Directory
Institutions Directory
Top Authors
Top Institutions
Top Sponsors
AI Digest
Contact Us
Home
About Us
Resources
Profiles Metrics
Authors Directory
Institutions Directory
Top Authors
Top Institutions
Top Sponsors
AI Digest
Contact Us
Menu
Home
About Us
Resources
Profiles Metrics
Authors Directory
Institutions Directory
Top Authors
Top Institutions
Top Sponsors
AI Digest
Contact Us
Publication Details
AFRICAN RESEARCH NEXUS
SHINING A SPOTLIGHT ON AFRICAN RESEARCH
earth and planetary sciences
The nature of submillimetre galaxies in cosmological hydrodynamic simulations
Monthly Notices of the Royal Astronomical Society, Volume 404, No. 3, Year 2010
Notification
URL copied to clipboard!
Description
We study the nature of rapidly star-forming galaxies at z = 2 in cosmological hydrodynamic simulations, and compare their properties to observations of submillimetre galaxies (SMGs). We identify simulated SMGs as the most rapidly star-forming systems that match the observed number density of SMGs. In our models, SMGs are massive galaxies sitting at the centres of large potential wells, being fed by smooth infall and gas-rich satellites at rates comparable to their star formation rates (SFRs). They are not typically undergoing major mergers that significantly boost their quiescent SFR, but they still often show complex gas morphologies and kinematics. Our simulated SMGs have stellar masses of M* ∼ 1011-11.7 M⊙, SFRs of ∼180-500 M⊙ yr-1, a clustering length of ∼10 h-1 Mpc and solar metallicities. The SFRs are lower than those inferred from far-infrared (far-IR) data by ∼×3, which we suggest may owe to one or more systematic effects in the SFR calibrations. SMGs at z = 2 live in ∼1013 M⊙ haloes, and by z = 0 they mostly end up as brightest group galaxies in ∼1014 M⊙ haloes. We predict that higher M* SMGs should have on average lower specific SFRs, less disturbed morphologies and higher clustering. We also predict that deeper far-IR surveys will smoothly join SMGs on to the massive end of the SFR-M* relationship defined by lower mass z ∼ 2 galaxies. Overall, our simulated rapid star-formers provide as good a match to available SMG data as merger-based scenarios, offering an alternative scenario that emerges naturally from cosmological simulations. © 2010 The Authors. Journal compilation © 2010 RAS.
Authors & Co-Authors
Dav́e, Romeel
United States, Tucson
The University of Arizona
Finlator, Kristian M.
United States, Tucson
The University of Arizona
United States, Santa Barbara
University of California, Santa Barbara
Oppenheimer, Benjamin Darwin
United States, Tucson
The University of Arizona
Netherlands, Leiden
Sterrewacht Leiden
Fardal, Mark A.
United States, Amherst
University of Massachusetts Amherst
Katz, Neal S.
United States, Amherst
University of Massachusetts Amherst
Keres̀, Dušan
United States, Cambridge
Harvard-smithsonian Center for Astrophysics
Weinberg, David H.
United States, Columbus
The Ohio State University
Statistics
Citations: 192
Authors: 7
Affiliations: 6
Identifiers
Doi:
10.1111/j.1365-2966.2010.16395.x
ISSN:
00358711
Study Design
Cross Sectional Study