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Prediction of H α and [O III] emission line galaxy number counts for future galaxy redshift surveys

Zhai, Zhongxu and Benson, Andrew and Wang, Yun and Yepes, Gustavo and Chuang, Chia-Hsun (2019) Prediction of H α and [O III] emission line galaxy number counts for future galaxy redshift surveys. Monthly Notices of the Royal Astronomical Society, 490 (3). pp. 3667-3678. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20200109-143244082

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Abstract

We perform a simulation with Galacticus, a semi-analytical galaxy formation model, to predict the number counts of H α and [O III] emitting galaxies. With a state-of-the-art N-body simulation, UNIT, we first calibrate Galacticus with the current observation of H α luminosity function. The resulting model coupled with a dust attenuation model, can reproduce the current observations, including the H α luminosity function from HiZELS and number density from WISP. We extrapolate the model prediction to higher redshift and the result is found to be consistent with previous investigations. We then use the same galaxy formation model to predict the number counts for [O III] emitting galaxies. The result provides further validation of our galaxy formation model and dust model. We present number counts of H α and [O III] emission line galaxies for three different line flux limits: 5 × 10⁻¹⁷ erg s⁻¹ cm⁻², 1 × 10⁻¹⁶ erg s⁻¹ cm⁻² (6.5σ nominal depth for WFIRST GRS), and 2 × 10⁻¹⁶ erg s⁻¹ cm⁻² (3.5σ depth of Euclid GRS). At redshift 2 < z < 3, our model predicts that WFIRST can observe hundreds of [O III] emission line galaxies per square degree with a line flux limit of 1 × 110⁻¹⁶ erg s⁻¹ cm⁻². This will provide accurate measurement of large-scale structure to probe dark energy over a huge cosmic volume to an unprecedented high redshift. Finally, we compare the flux ratio of H α/[O III] within the redshift range of 0 < z < 3. Our results show the known trend of increasing H α/[O III] flux ratio with H α flux at low redshift, which becomes a weaker trend at higher redshifts.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/stz2844DOIArticle
https://arxiv.org/abs/1907.09680arXivDiscussion Paper
ORCID:
AuthorORCID
Zhai, Zhongxu0000-0001-7984-5476
Benson, Andrew0000-0001-5501-6008
Chuang, Chia-Hsun0000-0002-3882-078X
Additional Information:© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model) Accepted 2019 October 4. Received 2019 October 4; in original form 2019 July 22. We thank the anonymous referee for the valuable comments and suggestions that have helped us improve the contents of this paper. We thank James Colbert for providing the WISP measurements in the analysis, and Alex Merson for helpful discussions. This work is supported in part by NASA grant 15-WFIRST15-0008, Cosmology with the High Latitude Survey WFIRST Science Investigation Team (SIT). GY would like to thank MINECO/FEDER (Spains) for financial support under project grants AYA2015-63810-P and PGC2018-094975-B-C21. The UNIT simulations have been done in the MareNostrum Supercomputer at the Barcelona Supercomputing Center (Spain) thanks to the cpu time awarded by PRACE under project grant number 2016163937. This work used the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation grant number ACI-1548562 (Towns et al. 2014) Software: PYTHON, MATPLOTLIB (Hunter 2007), NUMPY (van der Walt, Colbert & Varoquaux 2011), SCIPY (Jones et al. 2001).
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASA15-WFIRST15-0008
Ministerio de Economía y Competitividad (MINECO)AYA2015-63810-P
Fondo Europeo de Desarrollo Regional (FEDER)PGC2018-094975-B-C21
PRACE (Partnership for Advanced Computing in Europe)2016163937
NSFACI-1548562
Subject Keywords:methods: numerical, methods: statistical, galaxies: formation, large-scale structure of universe
Issue or Number:3
Record Number:CaltechAUTHORS:20200109-143244082
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20200109-143244082
Official Citation:Zhongxu Zhai, Andrew Benson, Yun Wang, Gustavo Yepes, Chia-Hsun Chuang, Prediction of H α and [O III] emission line galaxy number counts for future galaxy redshift surveys, Monthly Notices of the Royal Astronomical Society, Volume 490, Issue 3, December 2019, Pages 3667–3678, https://doi.org/10.1093/mnras/stz2844
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:100611
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:10 Jan 2020 16:23
Last Modified:10 Jan 2020 16:23

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