JINGLE, a JCMT legacy survey of dust and gas for galaxy evolution studies - I. Survey overview and first results

Amélie Saintonge, Christine D. Wilson, Ting Xiao, Lihwai Lin, Ho Seong Hwang, Tomoka Tosaki, Martin Bureau, Phillip J. Cigan, Christopher J.R. Clark, David L. Clements, Ilse De Looze, Thavisha Dharmawardena, Yang Gao, Walter K. Gear, Joshua Greenslade, Isabella Lamperti, Jong Chul Lee, Cheng Li, Michal J. Michałowski, Angus MokHsi An Pan, Anne E. Sansom, Mark Sargent, Matthew W. Matthew, Thomas Williams, Chentao Yang, Ming Zhu, Gioacchino Accurso, Pauline Barmby, Elias Brinks, Nathan Bourne, Toby Brown, Aeree Chung, Eun Jung Chung, Anna Cibinel, Kristen Coppin, Jonathan Davies, Timothy A. Davis, Steve Eales, Lapo Fanciullo, Taotao Fang, Yu Gao, David H.W. Glass, Haley L. Gomez, Thomas Greve, Jinhua He, Luis C. Ho, Feng Huang, Hyunjin Jeong, Xuejian Jiang, Qian Jiao, Francisca Kemper, Ji Hoon Kim, Minjin Kim, Taehyun Kim, Jongwan Ko, Xu Kong, Kevin Lacaille, Cedric G. Lacey, Bumhyun Lee, Joon Hyeop Lee, Wing Kit Lee, Karen Masters, Se Heon Oh, Padelis Papadopoulos, Changbom Park, Sung Joon Park, Harriet Parsons, Kate Rowlands, Peter Scicluna, Jillian M. Scudder, Ramya Sethuram, Stephen Serjeant, Yali Shao, Yun Kyeong Sheen, Yong Shi, Hyunjin Shim, Connor M.A. Smith, Kristine Spekkens, An Li Tsai, Aprajita Verma, Sheona Urquhart, Giulio Violino, Serena Viti, David Wake, Junfeng Wang, Jan Wouterloot, Yujin Yang, Kijeong Yim, Fangting Yuan, Zheng Zheng

Research output: Contribution to journalArticlepeer-review

13 Citations (Scopus)

Abstract

JINGLE is a new JCMT legacy survey designed to systematically study the cold interstellar medium of galaxies in the local Universe. As part of the survey we perform 850 μm continuum measurements with SCUBA-2 for a representative sample of 193 Herschel-selected galaxies with M* > 109 M, as well as integrated CO(2-1) line fluxes with RxA3m for a subset of 90 of these galaxies. The sample is selected from fields covered by the Herschel-ATLAS survey that are also targeted by the MaNGA optical integral-field spectroscopic survey. The new JCMT observations combined with the multiwavelength ancillary data will allow for the robust characterization of the properties of dust in the nearby Universe, and the benchmarking of scaling relations between dust, gas, and global galaxy properties. In this paper we give an overview of the survey objectives and details about the sample selection and JCMT observations, present a consistent 30-band UV-to-FIR photometric catalogue with derived properties, and introduce the JINGLE Main Data Release. Science highlights include the non-linearity of the relation between 850 μm luminosity and CO line luminosity (log LCO(2-1) = 1.372 logL850-1.376), and the serendipitous discovery of candidate z > 6 galaxies.

Original languageEnglish
Pages (from-to)3497-3519
Number of pages23
JournalMonthly Notices of the Royal Astronomical Society
Volume481
Issue number3
DOIs
Publication statusPublished - 2018 Dec 11

Bibliographical note

Funding Information:
The James Clerk Maxwell Telescope is operated by the East Asian Observatory on behalf of The NationalAstronomicalObservatory of Japan, Academia Sinica Institute of Astronomy and Astrophysics, the Korea Astronomy and Space Science Institute, the National Astronomical Observatories of China, and the Chinese Academy of Sciences (Grant No. XDB09000000), with additional funding support from the Science and Technology Facilities Council of the United Kingdom and participating universities in the United Kingdom and Canada. Additional funds for the construction of SCUBA-2 were provided by the Canada Foundation for Innovation. These data are being observed under JCMTProject ID:M16AL005. The Starlink software (Currie et al. 2014) used as part of the JINGLE data reduction process is currently supported by the East Asian Observatory. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community.We are most fortunate to have the opportunity to conduct observations from this mountain. AS acknowledges support from the Royal Society through the award of a University Research Fellowship. CDW acknowledges support from the Natural Sciences and Engineering Research Council of Canada. TX acknowledges the support of National Science Foundation of China (NSFC), Grant No. 11203056. CJRC acknowledges support from European Research Council (ERC) in the form of the 7th Framework Program (FP7) project DustPedia (PI Jon Davies, proposal 606824). DLC is supported through STFC grants ST/N000838/1, ST/K001051/1, and ST/N005317/1. IDL gratefully acknowledges the support of the Science and Technology Facilities Council (STFC) and the Flemish Fund for Scientific Research (FWO-Vlaanderen). TAD acknowledges support from an STFC Ernest Rutherford Fellowship. MB was supported by the consolidated grants 'Astrophysics at Oxford' ST/N000919/1 and ST/K00106X/1 from STFC. LCH was supported by the National Key R&D Program of China (2016YFA0400702) and NSFC (11473002, 11721303). CL acknowledges the support by National Key Basic Research Program of China (2015CB857004) and NSFC (11233005, 11325314, 11320101002). JMS acknowledges support from STFC, grant number ST/L000652/1. MJM acknowledges the support of the National Science Centre, Poland through the POLONEZ grant 2015/19/P/ST9/04010; this project has received funding from the EU's Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No. 665778. MTS was supported by a Royal Society Leverhulme Trust Senior Research Fellowship (LT150041). HLG and PJC acknowledge support from the European Research Council (ERC) through the Consolidator Grant COSMICDUST (ERC-2014-CoG-647939, PI HL Gomez). EB acknowledges support from STFC, grant number ST/M001008/1. JH is supported by the Yunnan Province of China (No. 2017HC018). CY, YG, XJ, and QJ acknowledge support by the NationalKeyR&DProgram of China (2017YFA0402700), theCAS Key Research Program of Frontier Sciences, and the NSFC grants (11311130491, 11420101002). MZ acknowledges the support by the National Key R&D Program of China (2017YFA0402600) and by NSFC (U1531246). This research has made use of Astropy, 8 a community-developed core PYTHON package for Astronomy (Astropy Collaboration et al. 2013). This research has made use of TOPCAT9 (Taylor 2005), which was initially developed under the UK Starlink project, and has since been supported by PPARC, the VOTech project, the Astro-Grid project, the AIDA project, the STFC, the GAVO project, the European Space Agency, and the GENIUS project. This research has made use of NUMPY10 (van der Walt, Colbert & Varoquaux 2011), SCIPY, 11 and MATPLOTLIB12 (Hunter 2007). This research made use of APLPY, 13 an open-source plotting package for PYTHON (Robitaille & Bressert 2012). This research has made use of the scikit-image14 image analysis library (van der Walt et al. 2014). This research made use of MONTAGE, 15 which is funded by the National Science Foundation under Grant Number ACI-1440620, and was previously funded by the National Aeronautics and Space Administration's Earth Science Technology Office, Computation Technologies Project, underCooperative AgreementNumberNCC5-626 between NASA and the California Institute of Technology. This research has made use of GALEX data obtained from the MikulskiArchive for Space Telescopes (MAST); support forMAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts (MAST is maintained by STScI, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555). This research has made use of data from the 3rd phase of the Sloan Digital Sky Survey (SDSS-III). Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. This research has made use of the NASA SkyView16 service. SkyViewhas been developedwith generous support from theNASA AISR and ADP programmes (P.I. Thomas A. McGlynn) under the auspices of the High Energy Astrophysics Science Archive Research Center (HEASARC) at the NASA/GSFC Astrophysics Science Division. This research makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/ California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/ California Institute of Technology, and NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology.WISE andNEOWISE are funded by the National Aeronautics and Space Administration. 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. Hershcel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. The Herschel spacecraft was designed, built, tested, and launched under a contract to ESA managed by the Herschel Planck Project team by an industrial consortium under the overall responsibility of the prime contractor Thales Alenia Space (Cannes), and including Astrium (Friedrichshafen) responsible for the payload module and for system testing at spacecraft level, Thales Alenia Space (Turin) responsible for the service module, and Astrium (Toulouse) responsible for the telescope, with in excess of a hundred subcontractors.

Funding Information:
This research makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.

Funding Information:
This research has made use of GALEX data obtained from the Mikulski Archive for Space Telescopes (MAST); support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts (MAST is maintained by STScI, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555).

Funding Information:
This research has made use of Astropy,8 a community-developed core PYTHON package for Astronomy (Astropy Collaboration et al. 2013). This research has made use of TOPCAT9 (Taylor 2005), which was initially developed under the UK Starlink project, and has since been supported by PPARC, the VOTech project, the Astro-Grid project, the AIDA project, the STFC, the GAVO project, the European Space Agency, and the GENIUS project. This research has made use of NUMPY10 (van der Walt, Colbert & Varoquaux 2011), SCIPY,11 and MATPLOTLIB12 (Hunter 2007). This research made use of APLPY,13 an open-source plotting package for PYTHON (Robitaille & Bressert 2012). This research has made use of the scikit-image14 image analysis library (van der Walt et al. 2014).

Funding Information:
AS acknowledges support from the Royal Society through the award of a University Research Fellowship. CDW acknowledges support from the Natural Sciences and Engineering Research Council of Canada. TX acknowledges the support of National Science Foundation of China (NSFC), Grant No. 11203056. CJRC acknowledges support from European Research Council (ERC) in the form of the 7th Framework Program (FP7) project DustPe-dia (PI Jon Davies, proposal 606824). DLC is supported through STFC grants ST/N000838/1, ST/K001051/1, and ST/N005317/1. IDL gratefully acknowledges the support of the Science and Technology Facilities Council (STFC) and the Flemish Fund for Scientific Research (FWO-Vlaanderen). TAD acknowledges support from an STFC Ernest Rutherford Fellowship. MB was supported by the consolidated grants ‘Astrophysics at Oxford’ ST/N000919/1 and ST/K00106X/1 from STFC. LCH was supported by the National Key R&D Program of China (2016YFA0400702) and NSFC (11473002, 11721303). CL acknowledges the support by National Key Basic Research Program of China (2015CB857004) and NSFC (11233005, 11325314, 11320101002). JMS acknowledges support from STFC, grant number ST/L000652/1. MJM acknowledges the support of the National Science Centre, Poland through the POLONEZ grant 2015/19/P/ST9/04010; this project has received funding from the EU’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 665778. MTS was supported by a Royal Society Leverhulme Trust Senior Research Fellowship (LT150041). HLG and PJC acknowledge support from the European Research Council (ERC) through the Consolidator Grant COSMICDUST (ERC-2014-CoG-647939, PI H L Gomez). EB acknowledges support from STFC, grant number ST/M001008/1. JH is supported by the Yunnan Province of China (No. 2017HC018). CY, YG, XJ, and QJ acknowledge support by the National Key R&D Program of China (2017YFA0402700), the CAS Key Research Program of Frontier Sciences, and the NSFC grants (11311130491, 11420101002). MZ acknowledges the support by the National Key R&D Program of China (2017YFA0402600) and by NSFC (U1531246).

Funding Information:
The James Clerk Maxwell Telescope is operated by the East Asian Observatory on behalf of The National Astronomical Observatory of Japan, Academia Sinica Institute of Astronomy and Astrophysics, the Korea Astronomy and Space Science Institute, the National Astronomical Observatories of China, and the Chinese Academy of Sciences (Grant No. XDB09000000), with additional funding support from the Science and Technology Facilities Council of the United Kingdom and participating universities in the United Kingdom and Canada. Additional funds for the construction of SCUBA-2 were provided by the Canada Foundation for Innovation. These data are being observed under JCMT Project ID: M16AL005. The Starlink software (Currie et al. 2014) used as part of the JINGLE data reduction process is currently supported by the East Asian Observatory.

Funding Information:
This research made use of MONTAGE,15 which is funded by the National Science Foundation under Grant Number ACI-1440620, and was previously funded by the National Aeronautics and Space Administration’s Earth Science Technology Office, Computation Technologies Project, under Cooperative Agreement Number NCC5-626 between NASA and the California Institute of Technology.

Funding Information:
This research has made use of data from the 3rd phase of the Sloan Digital Sky Survey (SDSS-III). Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard

Publisher Copyright:
© 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

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