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Spectroscopically Identified Emission Line Galaxy Pairs in the WISP Survey

Dai, Y. Sophia and Malkan, Matthew M. and Teplitz, Harry I. and Scarlata, Claudia and Alavi, Anahita and Atek, Hakim and Bagley, Micaela and Baronchelli, Ivano and Battisti, Andrew and Bunker, Andrew J. and Hathi, Nimish P. and Henry, Alaina and Huang, Jiasheng and Jin, Gaoxiang and Li, Zijian and Martin, Crystal and Mehta, Vihang and Phillips, John and Rafelski, Marc and Rutkowski, Michael and Xu, Hai and Xu, Cong K. and Zanella, Anita (2021) Spectroscopically Identified Emission Line Galaxy Pairs in the WISP Survey. Astrophysical Journal, 923 (2). Art. No. 156. ISSN 0004-637X. doi:10.3847/1538-4357/ac2f96. https://resolver.caltech.edu/CaltechAUTHORS:20211220-495727000

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Abstract

We identify a sample of spectroscopically measured emission line galaxy (ELG) Pairs up to z = 1.6 from the Wide Field Camera 3 (WFC3) Infrared Spectroscopic Parallels (WISP) survey. WISP obtained slitless, near-infrared grism spectroscopy along with direct imaging in the J and H bands by observing in the pure-parallel mode with the WFC3 on board the Hubble Space Telescope. From our search of 419 WISP fields covering an area of ∼0.5 deg², we find 413 ELG pair systems, mostly H_α emitters. We then derive reliable star formation rates (SFRs) based on the attenuation-corrected H_α fluxes. Compared to isolated galaxies, we find an average SFR enhancement of 40%–65%, which is stronger for major Pairs and Pairs with smaller velocity separations (Δ_v < 300 km s⁻¹). Based on the stacked spectra from various subsamples, we study the trends of emission line ratios in pairs, and find a general consistency with enhanced lower ionization lines. We study the pair fraction among ELGs, and find a marginally significant increase with redshift f ∝ (1 + z)^α, where the power-law index α = 0.58 ± 0.17 from z ∼ 0.2 to ∼1.6. The fraction of active galactic nuclei is found to be the same in the ELG Pairs as compared to the isolated ELGs.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/ac2f96DOIArticle
https://arxiv.org/abs/2110.07316arXivDiscussion Paper
ORCID:
AuthorORCID
Dai, Y. Sophia0000-0002-7928-416X
Malkan, Matthew M.0000-0001-6919-1237
Teplitz, Harry I.0000-0002-7064-5424
Scarlata, Claudia0000-0002-9136-8876
Alavi, Anahita0000-0002-8630-6435
Atek, Hakim0000-0002-7570-0824
Bagley, Micaela0000-0002-9921-9218
Baronchelli, Ivano0000-0003-0556-2929
Battisti, Andrew0000-0003-4569-2285
Bunker, Andrew J.0000-0002-8651-9879
Hathi, Nimish P.0000-0001-6145-5090
Henry, Alaina0000-0002-6586-4446
Jin, Gaoxiang0000-0003-3087-318X
Martin, Crystal0000-0001-9189-7818
Mehta, Vihang0000-0001-7166-6035
Rafelski, Marc0000-0002-9946-4731
Rutkowski, Michael0000-0001-7016-5220
Xu, Hai0000-0003-1094-5190
Xu, Cong K.0000-0003-2762-6057
Zanella, Anita0000-0001-8600-7008
Additional Information:© 2021. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2021 January 11; revised 2021 September 19; accepted 2021 October 11; published 2021 December 20. The authors would like to thank the referee for helpful suggestions. Y.S.D. thanks Andrea Faisst for helpful discussions. This research is based on observations made with the NASA/ESA Hubble Space Telescope obtained from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with programs 11696, 12283, 12568, 12092, 13352, 13517, and 14178. Support for this work is also partly provided by the CASSACA and Chinese National Nature Science Foundation (NSFC) grant No. 10878003. Y.S.D. acknowledges the science research grants from NSFC grants 11933003, the National Key R&D Program of China via grant No. 2017YFA0402703, and the China Manned Space Project with No. CMS-CSST-2021-A05. A.J.B. acknowledges funding from the FirstGalaxies Advanced Grant from the European Research Council (ERC) under the European Union Horizon 2020 research and innovation program (grant agreement No. 789056). H.A. acknowledges support from CNES. Based on observations made with the NASA/ESA Hubble Space Telescope, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with programs 11696, 12283, 12568, 12092, 13352, 13517, and 14178.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASANAS 5-26555
Chinese Academy of Sciences South America Center for Astronomy (CASSACA)UNSPECIFIED
National Natural Science Foundation of China10878003
National Natural Science Foundation of China11933003
National Key Research and Development Program of China2017YFA0402703
China Manned Space ProjectCMS-CSST-2021-A05
European Research Council (ERC)789056
Centre National d'Études Spatiales (CNES)UNSPECIFIED
Subject Keywords:Galaxy evolution; Galaxy pairs; Galaxy interactions; Extragalactic astronomy; Interacting galaxies; High-redshift galaxies; Galaxy spectroscopy
Issue or Number:2
Classification Code:Unified Astronomy Thesaurus concepts: Galaxy evolution (594); Galaxy pairs (610); Galaxy interactions (600); Extragalactic astronomy (506); Interacting galaxies (802); High-redshift galaxies (734); Galaxy spectroscopy (2171)
DOI:10.3847/1538-4357/ac2f96
Record Number:CaltechAUTHORS:20211220-495727000
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20211220-495727000
Official Citation:Y. Sophia Dai et al 2021 ApJ 923 156
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:112563
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:20 Dec 2021 23:47
Last Modified:20 Dec 2021 23:47

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