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HELP: star formation as a function of galaxy environment with Herschel

Duivenvoorden, S. and Oliver, S. and Buat, V. and Darvish, B. and Efstathiou, A. and Farrah, D. and Griffin, M. and Hurley, P. D. and Ibar, E. and Jarvis, M. and Papadopoulos, A. and Sargent, M. T. and Scott, D. and Scudder, J. M. and Symeonidis, M. and Vaccari, M. and Viero, M. P. and Wang, L. (2016) HELP: star formation as a function of galaxy environment with Herschel. Monthly Notices of the Royal Astronomical Society, 462 (1). pp. 277-289. ISSN 0035-8711. http://resolver.caltech.edu/CaltechAUTHORS:20161017-065053729

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Abstract

The Herschel Extragalactic Legacy Project (HELP) brings together a vast range of data from many astronomical observatories. Its main focus is on the Herschel data, which maps dust-obscured star formation over 1300 deg2. With this unprecedented combination of data sets, it is possible to investigate how the star formation versus stellar mass relation (main sequence) of star-forming galaxies depends on environment. In this pilot study, we explore this question within 0.1 < z < 3.2 using data in the COSMOS field. We estimate the local environment from a smoothed galaxy density field using the full photometric redshift probability distribution. We estimate star formation rates by stacking the SPIRE data from the Herschel Multi-tiered Extragalactic Survey. Our analysis rules out the hypothesis that the main sequence for star-forming systems is independent of environment at 1.5 < z < 2, while a simple model in which the mean specific star formation rate declines with increasing environmental density gives a better description. However, we cannot exclude a simple hypothesis in which the main sequence for star-forming systems is independent of environment at z < 1.5 and z > 2. We also estimate the evolution of the star formation rate density in the COSMOS field, and our results are consistent with previous measurements at z < 1.5 and z > 2 but we find a 1.4^(+0.3)_(−0.2) times higher peak value of the star formation rate density at z ∼ 1.9.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1093/mnras/stw1466DOIArticle
http://mnras.oxfordjournals.org/content/462/1/277.abstractPublisherArticle
https://arxiv.org/abs/1606.05377arXivDiscussion Paper
ORCID:
AuthorORCID
Duivenvoorden, S.0000-0002-1434-9153
Oliver, S.0000-0001-7862-1032
Efstathiou, A.0000-0002-2612-4840
Farrah, D.0000-0003-1748-2010
Scott, D.0000-0002-6878-9840
Vaccari, M.0000-0002-6748-0577
Additional Information:© 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2016 June 16. Received 2016 June 16. In original form 2016 January 21. First published online June 20, 2016. We thank the referee for very useful comments that improved the quality of the work. This project has received funding from the European Union's Horizon 2020 research and innovation programme under grant agreement no. 607254. This publication reflects only the authors’ view and the European Union is not responsible for any use that may be made of the information contained therein. SD acknowledges support from the Science and Technology Facilities Council (grant number ST/M503836/1). SO acknowledges support from the Science and Technology Facilities Council (grant number ST/L000652/1). BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G. EI acknowledges funding from CONICYT/FONDECYT postdoctoral project No. 3130504. MV acknowledges support from the Square Kilometre Array South Africa project, the South African National Research Foundation and Department of Science and Technology (DST/CON 0134/2014) and the Italian Ministry for Foreign Affairs and International Cooperation (PGR GA ZA14GR02). SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC, UKSA (UK); and NASA (USA).
Funders:
Funding AgencyGrant Number
European Research Council (ERC)607254
Science and Technology Facilities Council (STFC)ST/M503836/1
Science and Technology Facilities Council (STFC)ST/L000652/1
NASANNX12AE20G
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)3130504
Department of Science and Technology (South Africa)DST/CON 0134/2014
Ministry for Foreign Affairs and International Cooperation (Italy)PGR GA ZA14GR02
Canadian Space Agency (CSA)UNSPECIFIED
National Astronomical Observatories of ChinaUNSPECIFIED
Commissariat a l'Energie Atomique (CEA)UNSPECIFIED
Centre National d'Etudes Spatiales (CNES)UNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Agenzia Spaziale Italiana (ASI)UNSPECIFIED
Ministerio de Ciencia e Innovación (MCINN)UNSPECIFIED
Swedish National Space Board (SNSB)UNSPECIFIED
Science and Technology Facilities Council (STFC)UNSPECIFIED
United Kingdom Space Agency (UKSA)UNSPECIFIED
South African National Research FoundationUNSPECIFIED
Subject Keywords:galaxies: evolution galaxies: star formation infrared: galaxies
Record Number:CaltechAUTHORS:20161017-065053729
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20161017-065053729
Official Citation:S. Duivenvoorden, S. Oliver, V. Buat, B. Darvish, A. Efstathiou, D. Farrah, M. Griffin, P. D. Hurley, E. Ibar, M. Jarvis, A. Papadopoulos, M. T. Sargent, D. Scott, J. M. Scudder, M. Symeonidis, M. Vaccari, M. P. Viero, and L. Wang HELP: star formation as a function of galaxy environment with Herschel MNRAS (October 11, 2016) Vol. 462 277-289 doi:10.1093/mnras/stw1466 first published online June 20, 2016
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:71131
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:17 Oct 2016 17:26
Last Modified:10 Jul 2019 17:26

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