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Extreme Emission Line Galaxies and Their Implication on Selection Of Draft version December 30, 2014 Preprint typeset using LATEX style emulateapj v. 12/16/11 CLASH: EXTREME EMISSION LINE GALAXIES AND THEIR IMPLICATION ON SELECTION OF HIGH-REDSHIFT GALAXIES Xingxing Huang1,2, Wei Zheng2, Junxian Wang1, Holland Ford2, Doron Lemze2, John Moustakas3, Xinwen Shu4,1, Arjen Van der Wel5, Adi Zitrin6,7, Brenda L. Frye8, Marc Postman9, Matthias Bartelmann10, Narciso Ben´ıtez11, Larry Bradley9, Tom Broadhurst12,13, Dan Coe9, Megan Donahue14, Leopoldo Infante15, Daniel Kelson16, Anton Koekemoer9, Ofer Lahav17, Elinor Medezinski2, Leonidas Moustakas16, Piero Rosati19, Stella Seitz20, Keiichi Umetsu21 Draft version December 30, 2014 ABSTRACT We utilize the CLASH (Cluster Lensing And Supernova survey with Hubble) observations of 25 clusters to search for extreme emission-line galaxies (EELGs). The selections are carried out in two central bands: F105W (Y105) and F125W (J125), as the flux of the central bands could be enhanced by the presence of [O III] λλ4959; 5007 at redshift of ∼ 0:93 − 1:14 and 1:57 − 1:79, respectively. The multi-band observations help to constrain the equivalent widths of emission lines. Thanks to cluster lensing, we are able to identify 52 candidates down to an intrinsic limiting magnitude of 28.5 and to a rest-frame [O III] λλ4959; 5007 equivalent width of ' 3737 A.˚ Our samples include a number of EELGs at lower luminosities that are missed in other surveys, and the extremely high equivalent width can be only found in such faint galaxies. These EELGs can mimic the dropout feature similar to that of high redshift galaxies and contaminate the color-color selection of high redshift galaxies when the S/N ratio is limited or the band coverage is incomplete. We predict that the fraction of EELGs in the future high redshift galaxy selections cannot be neglected. Keywords: galaxies: high-redshift{galaxies: formation{galaxies: photometry 1. INTRODUCTION 1 CAS Key Laboratory for Research in Galaxies and Cosmology, Department of Astronomy, University of Science and Technology of The presence of extremely strong emission lines such China, Hefei, Anhui 230026, China; e-mail:[email protected] as the [O III] λλ4959; 5007 and Hα λ6563 emission 2 Department of Physics and Astronomy, Johns Hopkins Univer- lines is one of the prominent spectral features in star- sity, 3400 N. Charles Street, Baltimore, MD 21218 forming galaxies. Recently, a considerable number of 3 Department of Physics & Astronomy, Siena College, 515 Loudon Road,Loudonville, NY, 12211, USA star-forming galaxies with extraordinarily strong [O III] 4 CEA Saclay, DSM/Irfu/Service d'Astrophysique, Orme des λλ4959; 5007 (Straughn et al. 2009; van der Wel et al. Merisiers, 91191 Gif-sur-Yvette Cedex, France 2011; Atek et al. 2011; Smit et al. 2014) or Hα λ6563 5 Max-Planck Institute for Astronomy, K¨onigstuhl17, D-69117, Heidelberg, Germany (Shim et al. 2011; Shim & Chary 2013) lines have been 6 Cahill Center for Astronomy and Astrophysics, California In- found. While some of these galaxies are identified spec- stitute of Technology, MS 249-17, Pasadena, CA 91125 troscopically (Erb et al. 2006; Atek et al. 2011; Frye et al. 7 Hubble Fellow 2012), the majority of them are found from broad-band 8 Steward Observatory/Department of Astronomy, University of Arizona, 933 N Cherry Ave, Tucson, AZ 85721-0065 photometry with a significant flux excess in one or more 9 Space Telescope Science Institute, 3700 San Martin Drive, Bal- bands. Utilizing HST/Wide Field Camera 3 (WFC3) ob- timore, MD 21208, U.S.A. servations of the Cosmic Assembly Near-IR Deep Extra- 10 Leiden Observatory, Leiden University, P. O. Box 9513,2300 galactic Legacy Survey (CANDELS, Grogin et al. 2011), RA Leiden, The Netherlands 11 Instituto de Astrof´ısicade Andaluc´ıa(CSIC),C/Camino Bajo van der Wel et al. 2011 (VDW11 hereafter) identified an de Hu´etor24, Granada 18008, Spain abundant population of extreme emission line galaxies 12 Department of Theoretical Physics, University of Basque (EELGs) at redshift z ∼ 1:7. In some cases, the rest- Country UPV/EHU, Bilbao, Spain 13 frame equivalent widths (EWs) of such strong emission arXiv:1412.7909v1 [astro-ph.GA] 26 Dec 2014 IKERBASQUE, Basque Foundation for Science, Bilbao, Spain 14 Department of Physics and Astronomy, Michigan State Uni- lines reach 2000 A˚ or even higher. versity, East Lansing, MI 48824, USA Extremely strong emission lines can affect the spectral- 15 Departamento de Astrono´ıay Astrof´ısica, Pontificia Universi- energy-distribution (SED) fitting of broad-band pho- dad Cat´olicade Chile, V. Mackenna 4860, Santiago 22, Chile 16 Observatories of the Carnegie Institution of Washington, tometry (Schaerer & de Barros 2009; Atek et al. 2011; Pasadena, CA 91 101, USA Shim et al. 2011; Labb´eet al. 2010, 2012; Stark et al. 17 Department of Physics and Astronomy. University College 2013; Fumagalli et al. 2012). Their contributions may London, Gower Street, London WCIE 6 BT, UK mimic the spectral feature of the Lyman break in high- 18 Center for Astrophysics and Space Sciences, University of Cal- ifornia at San Diego. 9500 Gilman Dr., MC 0424, La Jolla, CA redshift galaxies. It is therefore possible that some high- 92093, USA redshift Lyman break galaxies (LBG) may actually be 19 Institute of Astronomy and Astrophysics, Academia Sinica, P. low-redshift EELGs when the wavelength coverages or O. Box 23-141, Taipei 10617, Taiwan depths are limited. Recently, the search for LBG has 20 Universit¨ats-Sternwarte, M¨unchen, Scheinerstr. 1, D-81679 M¨unchen, Germany reached z > 9, and HST plays the major role in this 21 Institut f¨urTheoretische Astrophysik, ZAH, Albert-Ueberle- redshift range with the WFC3/IR instrument (Bouwens Straße 2, 69120 Heidelberg, Germany et al. 2011; Zheng et al. 2012; Coe et al. 2013; Ellis 2 et al. 2013; Oesch et al. 2013). UDFj-39546284 was the photometry by comparing with public catalogs, 22 first detected in the Hubble Ultra Deep Field (HDF09) which were processed with modified version of the Mo- with an H160 band detection only (Bouwens et al. 2011). saicdrizzle pipeline (Koekemoer et al. 2003, 2011), and The decrement between the F160W and F125W bands is no systematic deviation was found between the two larger than two magnitudes, thus suggestive of a z ' 10 pipelines. In this paper, we focus on two ACS/WFC fil- candidate. Followup observations of the HUDF12 (GO ters (F814W, F850lp) and five WFC3/IR filters (F105W, 12498: PI Ellis) and CANDELS program (Grogin et al. F110W, F125W, F140W, F160W), which are hereafter 2011) confirm that this substantial break in the SED is called I814, Z850, Y105, YJ110, J125, JH140, and H160 actually between the F160W and F140W bands (Ellis et bands. al. 2013; Bouwens et al. 2013a), implying an even higher redshift. Brammer et al.(2013) analyzed deep WFC3 2.2. Sample Selection grism observations of UDFj-39546284 and found a 2.7σ A color-color selection has been successfully used for detection of an emission line at 1.599 µm. In the deep identifying EELGs in VDW11. We carried out two se- Keck observation, Capak et al.(2013) also found a 2.2 σ lections with two sets of filter bands. Firstly, we follow peak at the same wavelength. Both spectra suggest that the selection criteria of VDW11, namely UDFj-39546284 could be a strong [O III] λ5007 emitter at z ∼ 2:19 or a strong [O II] λ3727 emitter at z ∼ 3:29. J125 − I814 < −0:44 − σ ^ J125 − H160 < −0:44 − σ Current deep near infrared observations are unlikely to In the other selection, we use the Y105 band as the central determine the nature of this candidate. The presence of band, namely UDFj-39546284 suggests that the possible contamination due to EELGs at lower redshift should be reexamined. Y105 − I814 < −0:44 − σ ^ Y105 − H160 < −0:44 − σ In this paper, we report the search for EELGs at two redshift ranges in the CLASH cluster fields to estimate Where the σ refers to the 1σ error of the color. We the contamination to the selections of LBG. The CLASH also require that the three bands in each selection are program (Postman et al. 2012) is a 16-band survey of 25 detected at least 3σ to ensure good EW measurements. clusters between 0.2 and 1.6 µm. The nominal limiting After these preliminary selections (Figure1), we check magnitude in the F160W band is approximately 27.2 (5σ the images and photometry of the WFC3/IR bands for detection limit). With the power of cluster lensing, some each object. Sources contaminated by cosmic-ray events, of target can reach an intrinsic AB magnitude ∼29 mag, nearby bright sources and detector-edge effects are ex- similar to that of z ∼ 10 galaxies in the Hubble Ultra cluded. We build two samples with 40 and 12 candidates Deep Field. named as the \J" sample and \Y" sample. Note that Throughout this paper, EW is referred to the total the color excess of 0.44 magnitude in J125 and Y105 cor- ˚ of [O III] λλ4959; 5007 and Hβ λ4861 in the rest frame responds to rest-frame EW of about 600 A. The false- unless specified otherwise. Magnitudes are calculated in color images of these galaxies are shown in Figure2. the AB system. Errors are computed at 1σ. We adopt We include the apparent angular sizes which are mea- sured through full width at half maximum (FWHM) by a flat cosmology with Ωλ = 0:7, ΩM = 0:3 and H0 = 70 kms−1Mpc−1. SExtractor in Table1 and Table2. 2.3. Redshift Estimation 2. DATA To illustrate the boosting effect in different bands and different redshifts, we simulate model spectra with a sim- 2.1.
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