DETECTION of LYMAN-ALPHA EMISSION from A TRIPLY IMAGED z = 6.85 GALAXY behind MACS J2129.4-0741

KH Huang; BC Lemaux; KB Schmidt; A Hoag; M Bradač; T Treu; M Dijkstra; A Fontana; A Henry; M Malkan; C Mason; T Morishita; L Pentericci; RE Ryan; M Trenti; X Wang

Journal article

DETECTION of LYMAN-ALPHA EMISSION from A TRIPLY IMAGED z = 6.85 GALAXY behind MACS J2129.4-0741

KH Huang, BC Lemaux, KB Schmidt, A Hoag, M Bradač, T Treu, M Dijkstra, A Fontana, A Henry, M Malkan, C Mason, T Morishita, L Pentericci, RE Ryan, M Trenti, X Wang

Astrophysical Journal Letters | IOP PUBLISHING LTD | Published : 2016

DOI: 10.3847/2041-8205/823/1/L14

Abstract

We report the detection of Lyα emission at ∼9538 Å in the Keck/DEIMOS and Hubble Space Telescope WFC3 G102 grism data from a triply imaged galaxy at behind galaxy cluster MACS J2129.4-0741. Combining the emission line wavelength with broadband photometry, line ratio upper limits, and lens modeling, we rule out the scenario that this emission line is [O ii] at z = 1.57. After accounting for magnification, we calculate the weighted average of the intrinsic Lyα luminosity to be and Lyα equivalent width to be 74 ± 15 Å. Its intrinsic UV absolute magnitude at 1600 Å is -18.6 ± 0.2 mag and stellar mass , making it one of the faintest (intrinsic ) galaxies with Lyα detection at to date. Its stellar..

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University of Melbourne Researchers

Michele Trenti Author

Grants

Awarded by National Aeronautics and Space Administration

Funding Acknowledgements

We thank the referee for constructive feedback of this work. We also thank Piero Rosati and Anna Monna for providing spectroscopic redshifts from the CLASH-VLT program. This work is based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555 and NNX08AD79G and ESO-VLT telescopes. Observations were carried out using Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work is provided by NASA through a Spitzer award issued by JPL/Caltech, HST-AR-13235, HST-GO-13459, and HST-GO-13177. A.H. acknowledges support by NASA Headquarters under the NASA Earth and Space Science Fellowship Program Grant ASTRO14F-0007.