Young Galaxy Candidates in the Hubble Frontier Fields. II. MACS J0416-2403

Creators: Infante, Leopoldo; Zheng, Wei; Laporte, Nicolas; Troncoso Iribarren, Paulina; Molino, Alberto; Diego, Jose M.; Bauer, Franz E.; Zitrin, Adi; Moustakas, John; Huang, Xingxing; Shu, Xinwen; Bina, David; Brammer, Gabriel B.; Broadhurst, Tom; Ford, Holland C.; García, Stefano; Kim, Sam

Abstract

We searched for z ≳ 7 Lyman-break galaxies in the optical-to-mid-infrared Hubble Frontier Field and associated parallel field observations of the strong-lensing cluster MACS J0416−2403. We discovered 22 candidates, of which 6 lie at z ≳ 9 and 1 lies at z ≳ 10. Based on the Hubble and Spitzer photometry, all have secure photometric redshifts and a negligible probability of being at lower redshifts according to their peak-probability ratios, R. This substantial increase in the number of known high-redshift galaxies allows a solid determination of the luminosity function (LF) at z ≳ 8. The number of high-z candidates in the parallel field is considerably higher than that in the Abell 2744 parallel field. Our candidates have median stellar masses of log M_* ~ 8.44_(-0.31)^(+0.55) M_⊙, star formation rates (SFRs) of ~ 1.8_(-0.4)^(+0.5) M_⊙ yr^(−1), and SFR-weighted ages of ≾ 300_(-140)^(+70) Myr. Finally, we are able to put strong constraints on the z = 7, 8, 9, and 10 LFs. One of the objects in the cluster field is a z ≃ 10 candidate, with a magnification of μ ~ 20 ± 13. This object is likely the faintest z ~ 10 object known to date, allowing a first look into the extreme faint end (L ~ 0.04 L^*) of the z ~ 10 LF (It is named "Tayna" in the Aymara language).

Additional Information

© 2015 The American Astronomical Society. Received 2015 March 2; accepted 2015 October 23; published 2015 December 2. The work presented in this paper is based on observations made with the NASA/ESA Hubble Space Telescope, and has been supported by award AR-13279 from the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. It is also based on data obtained with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. We acknowledge support from Basal-CATA PFB-06/2007 (L.I., F.E.B., N.L., S.K., and P.T.), FP7-SPACE-2012-ASTRODEEP-312725 (X.S.), NSFC grants 11103017 and 11233002 (X.S.), NASA through Hubble Fellowship grant HST-HF2-51334.01-A awarded by STScI (A.Z.), CONICYT-Chile grants FONDECYT 1141218 (F.E.B.), Gemini-CONICYT 32120003 (F.E.B. and N.L.), and "EMBIGGEN" Anillo ACT1101 (F.E.B.), the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC120009, awarded to The Millennium Institute of Astrophysics, MAS (F.E.B.), Spanish consolider project CAD2010-00064 and AYA2012-39475-C02-01 (J.M.D.), the Brazilian funding agency-FAPESP post doc fellowship—process number 2014/11806-9 (A.M.) and CONICYT-Chile grant FONDECYT 3140542 (P.T.). L.I. would like to thank the European Southern Observatory and the University of Victoria, Canada, for providing office space while this work was done.

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