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HI-MaNGA: tracing the physics of the neutral and ionized ISM with the second data release

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Author(s)

David V Stark, Karen L Masters, Vladimir Avila-Reese, Rogemar Riffel, Rogerio Riffel, Nicholas Fraser Boardman, Zheng Zheng, Anne-Marie Weijmans, Sean Dillon, Catherine Fielder, Daniel Finnegan, Patricia Fofie, Julian Goddy, Emily Harrington, Zachary Pace, Wiphu Rujopakarn, Nattida Samanso, Shoaib Shamsi, Anubhav Sharma, Elizabeth Warrick & 2 more Catherine Witherspoon, Nathan Wolthuis

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Abstract

We present the second data release for the HI-MaNGA programme of H I follow-up observations for the SDSS-IV MaNGA survey. This release contains measurements for 3669 unique galaxies, combining 2108 Green Bank Telescope observations with an updated crossmatch of the MaNGA sample with the ALFALFA survey. We combine these data with MaNGA spectroscopic measurements to examine relationships between H I-to-stellar mass ratio (⁠MHI/M∗MHI/M∗⁠) and average ISM/star formation properties probed by optical emission lines. MHI/M∗MHI/M∗ is very weakly correlated with the equivalent width of Hα, implying a loose connection between the instantaneous star formation rate and the HI reservoir, although the link between MHI/M∗MHI/M∗ and star formation strengthens when averaged even over only moderate timescales (∼30 Myrs). Galaxies with elevated H I depletion times have enhanced [O I]/Hα and depressed Hα surface brightness, consistent with more H I residing in a diffuse and/or shock heated phase which is less capable of condensing into molecular clouds. Of all optical lines, MHI/M∗MHI/M∗ correlates most strongly with oxygen equivalent width, EW(O), which is likely a result of the existing correlation between MHI/M∗MHI/M∗ and gas-phase metallicity. Residuals in the MHI/M∗MHI/M∗−EW(O) relation are again correlated with [O I]/Hα and Hα surface brightness, suggesting they are also driven by variations in the fraction of diffuse and/or shock-heated gas. We recover the strong anti-correlation between MHI/M∗MHI/M∗ and gas-phase metallicity seen in previous studies. We also find a relationship between MHI/M∗MHI/M∗ and [O I]6302/Hα, suggesting that higher fractions of diffuse and/or shock-heated gas are more prevalent in gas-rich galaxies.
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Original languageEnglish
Pages (from-to)1345–1366
JournalMonthly Notices of the Royal Astronomical Society
Volume503
Issue number1
Early online date27 Feb 2021
DOIs
Publication statusPublished - May 2021

    Research areas

  • Galaxies: ISM, Radio lines: galaxies, Catalogs, Surveys

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