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The CANDELS/SHARDS Multiwavelength Catalog in GOODS-N: Photometry, Photometric Redshifts, Stellar Masses, Emission-line Fluxes, and Star Formation Rates

Barro, Guillermo and Hemmati, Shoubaneh (2019) The CANDELS/SHARDS Multiwavelength Catalog in GOODS-N: Photometry, Photometric Redshifts, Stellar Masses, Emission-line Fluxes, and Star Formation Rates. Astrophysical Journal Supplement Series, 243 (2). Art. No. 22. ISSN 1538-4365. https://resolver.caltech.edu/CaltechAUTHORS:20190725-135017116

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Abstract

We present a WFC3 F160W (H-band) selected catalog in the CANDELS/GOODS-N field containing photometry from the ultraviolet (UV) to the far-infrared (IR), photometric redshifts, and stellar parameters derived from the analysis of the multiwavelength data. The catalog contains 35,445 sources over the 171 arcmin^2 of the CANDELS F160W mosaic. The 5σ detection limits (within an aperture of radius 0.”17) of the mosaic range between H = 27.8, 28.2, and 28.7 in the wide, intermediate, and deep regions, which span approximately 50%, 15%, and 35% of the total area. The multiwavelength photometry includes broadband data from the UV (U band from KPNO and LBC), optical (HST/ACS F435W, F606W, F775W, F814W, and F850LP), near-to-mid IR (HST/WFC3 F105W, F125W, F140W, and F160W; Subaru/MOIRCS Ks; CFHT/Megacam K; and Spitzer/IRAC 3.6, 4.5, 5.8, and 8.0 μm), and far-IR (Spitzer/MIPS 24 μm, HERSCHEL/PACS 100 and 160 μm, SPIRE 250, 350 and 500 μm) observations. In addition, the catalog also includes optical medium-band data (R ~ 50) in 25 consecutive bands, λ = 500–950 nm, from the SHARDS survey and WFC3 IR spectroscopic observations with the G102 and G141 grisms (R ~ 210 and 130). The use of higher spectral resolution data to estimate photometric redshifts provides very high, and nearly uniform, precision from z = 0–2.5. The comparison to 1485 good-quality spectroscopic redshifts up to z ~ 3 yields Δz/(1 + z_(spec)) = 0.0032 and an outlier fraction of η = 4.3%. In addition to the multiband photometry, we release value-added catalogs with emission-line fluxes, stellar masses, dust attenuations, UV- and IR-based star formation rates, and rest-frame colors.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4365/ab23f2DOIArticle
ORCID:
AuthorORCID
Barro, Guillermo0000-0001-6813-875X
Hemmati, Shoubaneh0000-0003-2226-5395
Additional Information:© 2019 The American Astronomical Society. Received 2018 October 19; revised 2019 April 30; accepted 2019 May 16; published 2019 July 25. Support for program number HST-GO-12060 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. G.B., S.M.F, and D.K. acknowledge support from HST-GO-13420 and NSF grants AST-0808133 and AST-1615730. P.G.P.-G. acknowledges support from grant AYA2015-63650-P. This work has made use of the Rainbow Cosmological Surveys Database, which is operated by the Centro de Astrobiología (CAB/INTA), partnered with the University of California Observatories at Santa Cruz (UCO/Lick, UCSC). This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA.
Funders:
Funding AgencyGrant Number
NASA Hubble FellowshipHST-GO-12060
NASANAS5-26555
NASA Hubble FellowshipHST-GO-13420
NSFAST-0808133
NSFAST-1615730
Ministerio de Economía, Industria y Competitividad (MINECO)AYA2015-63650-P
NASA/JPL/CaltechUNSPECIFIED
Subject Keywords:galaxies: high-redshift – galaxies: photometry
Issue or Number:2
Record Number:CaltechAUTHORS:20190725-135017116
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190725-135017116
Official Citation:Guillermo Barro et al 2019 ApJS 243 22
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:97423
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:25 Jul 2019 21:07
Last Modified:03 Oct 2019 21:31

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