Distances to PHANGS Galaxies: New Tip of the Red Giant Branch Measurements and Adopted Distances

Creators: Anand, Gagandeep S.; Lee, Janice C.; Van Dyk, Schuyler D.; Leroy, Adam K.; Rosolowsky, Erik; Schinnerer, Eva; Larson, Kirsten; Kourkchi, Ehsan; Kreckel, Kathryn; Scheuermann, Fabian; Rizzi, Luca; Thilker, David; Tully, R. Brent; Bigiel, Frank; Blanc, Guillermo A.; Boquien, Médéric; Chandar, Rupali; Dale, Daniel; Emsellem, Eric; Deger, Sinan; Glover, Simon C. O.; Grasha, Kathryn; Groves, Brent; K̃lessen, Ralf S.; Kruijssen, J. M. Diederik; Querejeta, Miguel; Sánchez-Blázquez, Patricia; Schruba, Andreas; Turner, Jordan; Ubeda, Leonardo; Williams, Thomas G.; Whitmore, Brad

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Abstract

PHANGS-HST is an ultraviolet-optical imaging survey of 38 spiral galaxies within ∼20 Mpc. Combined with the PHANGS-ALMA, PHANGS-MUSE surveys and other multiwavelength data, the data set will provide an unprecedented look into the connections between young stars, H II regions, and cold molecular gas in these nearby star-forming galaxies. Accurate distances are needed to transform measured observables into physical parameters (e.g. brightness to luminosity, angular to physical sizes of molecular clouds, star clusters and associations). PHANGS-HST has obtained parallel ACS imaging of the galaxy haloes in the F606W and F814W bands. Where possible, we use these parallel fields to derive tip of the red giant branch (TRGB) distances to these galaxies. In this paper, we present TRGB distances for 10 PHANGS galaxies from ∼4 to ∼15 Mpc, based on the first year of PHANGS-HST observations. Four of these represent the first published TRGB distance measurements (IC 5332, NGC 2835, NGC 4298, and NGC 4321), and seven of which are the best available distances to these targets. We also provide a compilation of distances for the 118 galaxies in the full PHANGS sample, which have been adopted for the first PHANGS-ALMA public data release.

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© 2020 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Received: 24 August 2020; Revision received: 13 November 2020; Accepted: 20 November 2020; Published: 25 November 2020. This work was carried out as part of the PHANGS collaboration. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. Support for Programme number 15654 was provided through a grant from the STScI under NASA contract NAS5-26555. We thank the anonymous referee for their useful comments which helped improve this manuscript. GA acknowledges support from the IPAC Visiting Graduate Fellowship programme and from an award from the Space Telescope Science Institute in support of programme SNAP-15922. The work of AKL is partially supported by the National Science Foundation under Grants No. 1615105, 1615109, and 1653300. ES acknowledges funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement No. 694343). KK and FS gratefully acknowledge funding from the German Research Foundation (DFG) in the form of an Emmy Noether Research Group (grant number KR4598/2-1, PI Kreckel). ER acknowledges the support of the Natural Sciences and Engineering Research Council of Canada (NSERC), funding reference number RGPIN-2017-03987. FS gratefully acknowledges funding from the German Research Foundation (DFG) Emmy Noether Research Group (grant number KR4598/2-1, PI Kreckel). FB acknowledges funding from the European Union's Horizon 2020 research and innovation programme (grant agreement No 726384/EMPIRE). MB acknowledges FONDECYT regular grant 1170618. RSK and SCOG acknowledge financial support from the German Research Foundation (DFG) via the Collaborative Research Center (SFB 881, Project-ID 138713538) 'The Milky Way System' (subprojects A1, B1, B2, and B8). He also thanks for funding from the Heidelberg Cluster of Excellence STRUCTURES in the framework of Germany's Excellence Strategy (grantEXC-2181/1 - 390900948) and for funding from the European Research Council via the ERC Synergy Grant ECOGAL (grant 855130). JMDK gratefully acknowledges funding from the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) through an Emmy Noether Research Group (grant number KR4801/1-1) and the DFG Sachbeihilfe (grant number KR4801/2-1), as well as from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme via the ERC Starting Grant MUSTANG (grant agreement number 714907). PSB acknowledges financial support from grant PID2019-107427GB-C31 from the Spanish Ministry of Economy and Competitiveness (MINECO). MQ acknowledges support from the research project PID2019-106027GA-C44 from the Spanish Ministerio de Ciencia e Innovación. TGW acknowledges funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement No. 694343). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of the NASA/IPAC Infrared Science Archive, which is funded by the National Aeronautics and Space Administration and operated by the California Institute of Technology. Data Availability: The data underlying this article are available at the Mikulski Archive for Space Telescopes at https://archive.stsci.edu/hst/search_retrieve.html under proposal GO-15654. The photometry and list of derived parameters for the TRGB analysis are available under the CMDs/TRGB catalogue of the Extragalactic Distance Data base at edd.ifa.hawaii.edu.

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