MIGHTEE-H I: the MH I – M* relation over the last billion years

Hengxing Pan*, Matt j Jarvis, Mario g Santos, Natasha Maddox, Bradley s Frank, Anastasia a Ponomareva, Isabella Prandoni, Sushma Kurapati, Maarten Baes, Pavel e mancera Piña, Giulia Rodighiero, Martin j Meyer, Romeel Davé, Gauri Sharma, Sambatriniaina h a Rajohnson, Nathan j Adams, Rebecca a a Bowler, Francesco Sinigaglia, Thijs Van der hulst, Peter w HatfieldSrikrishna Sekhar, Jordan d Collier

*Corresponding author for this work

Research output: Contribution to journalArticle (Academic Journal)peer-review

1 Citation (Scopus)


We study the MHI−M⋆ relation over the last billion years using the MIGHTEE-H I sample. We first model the upper envelope of the MHI−M⋆ relation with a Bayesian technique applied to a total number of 249 H I-selected galaxies, without binning the data sets, while taking account of the intrinsic scatter. We fit the envelope with both linear and non-linear models, and find that the non-linear model is preferred over the linear one with a measured transition stellar mass of log10(M⋆/M⊙) = 9.15 ± 0.87, beyond which the slope flattens. This finding supports the view that the lack of H I gas is ultimately responsible for the decreasing star formation rate observed in the massive main-sequence galaxies. For spirals alone, which are biased towards the massive galaxies in our sample, the slope beyond the transition mass is shallower than for the full sample, indicative of distinct gas processes ongoing for the spirals/high-mass galaxies from other types with lower stellar masses. We then create mock catalogues for the MIGHTEE-H I detections and non-detections with two main galaxy populations of late- and early-type galaxies to measure the underlying MHI−M⋆ relation. We find that the turnover in this relation persists whether considering the two galaxy populations as a whole or separately. We note that an underlying linear relation could mimic this turnover in the observed scaling relation, but a model with a turnover is strongly preferred. Measurements on the logarithmic average of H I masses against the stellar mass are provided as a benchmark for future studies.
Original languageEnglish
Pages (from-to)256-269
Number of pages14
JournalMonthly Notices of the Royal Astronomical Society
Issue number1
Early online date3 Aug 2023
Publication statusPublished - Oct 2023

Bibliographical note

Funding Information:
We acknowledge the use of the ilifu cloud computing facility – www.ilifu.ac.za , a partnership between the University of Cape Town, the University of the Western Cape, the University of Stellenbosch, Sol Plaatje University, the Cape Peninsula University of Technology, and the South African Radio Astronomy Observatory. The ilifu facility is supported by contributions from IDIA and the Computational Biology division at UCT and the Data Intensive Research Initiative of South Africa (DIRISA).

Funding Information:
We thank the anonymous referees for their constructive comments that have improved this paper greatly. HP, MJJ, and MGS acknowledge support from the South African Radio Astronomy Observatory (SARAO) towards this research ( www.sarao.ac.za ). MJJ and AAP acknowledge generous support from the Hintze Family Charitable Foundation through the Oxford Hintze Centre for Astrophysical Surveys and the UK Science and Technology Facilities Council (STFC) [ST/S000488/1]. IP acknowledges financial support from the Italian Ministry of Foreign Affairs and International Cooperation (MAECI grant number ZA18GR02) and the South African Department of Science and Technology’s National Research Foundation (DST-NRF grant number 113121) as part of the Italy-South Africa Research Programme (ISARP) RADIOSKY2020 Joint Research Scheme. SK is supported by the South African research chairs initiative of the Department of Science and Technology and National Research Foundation. MB acknowledges support from the Flemish Fund for Scientific Research (FWO-Vlaanderen, grant number G0G0420N). SHAR is supported by the South African Research Chairs Initiative of the Department of Science and Technology and National Research Foundation. RB acknowledges support from an STFC Ernest Rutherford Fellowship (grant number ST/T003596/1).

Publisher Copyright:
© 2023 The Author(s).


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