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Evolution of Intrinsic Scatter in the SFR-Stellar Mass Correlation at 0.5 < z < 3

Kurczynski, Peter and Gawiser, Eric and Acquaviva, Viviana and Bell, Eric F. and Dekel, Avishai and de Mello, Duilia F. and Ferguson, Henry C. and Gardner, Jonathan P. and Grogin, Norman A. and Guo, Yicheng and Hopkins, Philip F. and Koekemoer, Anton M. and Koo, David C. and Lee, Seong-Kook and Mobasher, Bahram and Primack, Joel R. and Rafelski, Marc and Soto, Emmaris and Teplitz, Harry I. (2016) Evolution of Intrinsic Scatter in the SFR-Stellar Mass Correlation at 0.5 < z < 3. Astrophysical Journal Letters, 820 (1). Art. No. L1. ISSN 2041-8205. http://resolver.caltech.edu/CaltechAUTHORS:20160419-080939262

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Abstract

We present estimates of intrinsic scatter in the star formation rate (SFR)–stellar mass (M_*) correlation in the redshift range 0.5 < z < 3.0 and in the mass range 10^7 < M_*<10^(11)M_⊙. We utilize photometry in the Hubble Ultradeep Field (HUDF12) and Ultraviolet Ultra Deep Field (UVUDF) campaigns and CANDELS/GOODS-S and estimate SFR, M_* from broadband spectral energy distributions and the best-available redshifts. The maximum depth of the UDF photometry (F160W 29.9 AB, 5σ depth) probes the SFR–M_* correlation down to M_* ~ 10^7M_⊙, a factor of 10–100× lower in M_* than previous studies, and comparable to dwarf galaxies in the local universe. We find the slope of the SFR–M_* relationship to be near unity at all redshifts and the normalization to decrease with cosmic time. We find a moderate increase in intrinsic scatter with cosmic time from 0.2 to 0.4 dex across the epoch of peak cosmic star formation. None of our redshift bins show a statistically significant increase in intrinsic scatter at low mass. However, it remains possible that intrinsic scatter increases at low mass on timescales shorter than ~100 Myr. Our results are consistent with a picture of gradual and self-similar assembly of galaxies across more than three orders of magnitude in stellar mass from as low as 10^7M_⊙.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/2041-8205/820/1/L1DOIArticle
https://doi.org/10.3847/2041-8213/aadc65DOIErratum
http://arxiv.org/abs/1602.03909arXivDiscussion Paper
ORCID:
AuthorORCID
Acquaviva, Viviana0000-0002-6788-6315
Hopkins, Philip F.0000-0003-3729-1684
Rafelski, Marc0000-0002-9946-4731
Teplitz, Harry I.0000-0002-7064-5424
Additional Information:© 2016 The American Astronomical Society. Received 2015 November 16; accepted 2016 February 15; published 2016 March 14. The authors wish to thank Aaron Clauset for discussions. Support for HST Program GO-12534 was provided by NASA through grants from the Space Telescope Science Institute. This material is based upon work supported by the National Science Foundation under grant No. 1055919. This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASAGO-12534
NSFAST-1055919
NASANAS5-26555
Subject Keywords:galaxies: dwarf; galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: statistics
Record Number:CaltechAUTHORS:20160419-080939262
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20160419-080939262
Official Citation:Peter Kurczynski et al 2016 ApJ 820 L1
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:66270
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:19 Apr 2016 18:09
Last Modified:27 Mar 2019 17:22

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