Evolution of Intrinsic Scatter in the SFR-Stellar Mass Correlation at 0.5 < z < 3
- Creators
- Kurczynski, Peter
- Gawiser, Eric
- Acquaviva, Viviana
- Bell, Eric F.
- Dekel, Avishai
- de Mello, Duilia F.
- Ferguson, Henry C.
- Gardner, Jonathan P.
- Grogin, Norman A.
- Guo, Yicheng
- Hopkins, Philip F.
- Koekemoer, Anton M.
- Koo, David C.
- Lee, Seong-Kook
- Mobasher, Bahram
- Primack, Joel R.
- Rafelski, Marc
- Soto, Emmaris
- Teplitz, Harry I.
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_⊙.
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.Attached Files
Published - apjl_820_1_L1.pdf
Submitted - 1602.03909v1.pdf
Erratum - Kurczynski_2018_ApJL_864_L42.pdf
Files
Additional details
- Eprint ID
- 66270
- Resolver ID
- CaltechAUTHORS:20160419-080939262
- NASA
- GO-12534
- NSF
- AST-1055919
- NASA
- NAS5-26555
- Created
-
2016-04-19Created from EPrint's datestamp field
- Updated
-
2023-06-01Created from EPrint's last_modified field
- Caltech groups
- Infrared Processing and Analysis Center (IPAC)