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

Pan, Hengxing; Jarvis, Matt J.; Santos, Mario G.; Maddox, Natasha; Frank, Bradley S.; Ponomareva, Anastasia A.; Prandoni, Isabella; Kurapati, Sushma; Baes, Maarten; Piña, Pavel E. Mancera; Rodighiero, Giulia; Meyer, Martin J.; Davé, Romeel; Sharma, Gauri; Rajohnson, Sambatriniaina H. A.; Adams, Nathan J.; Bowler, Rebecca A. A.; Sinigaglia, Francesco; van der Hulst, Thijs; Hatfield, Peter W.; Sekhar, Srikrishna; Collier, Jordan D.

MIGHTEE-H I : the M_HI – 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 (UGent) , Pavel E. Mancera Piña, et al.

(2023) MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. 525(1). p.256-269

Author

Hengxing Pan, Matt J. Jarvis, Mario G. Santos, Natasha Maddox, Bradley S. Frank, Anastasia A. Ponomareva, Isabella Prandoni, Sushma Kurapati, Maarten Baes (UGent) , 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. Hatfield, Srikrishna Sekhar and Jordan D. Collier

Organization

Department of Physics and astronomy

Project

Atomic gas in galaxies: a critical test for state-of-the-art cosmological simulations of galaxy formation

Abstract

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.

Keywords

methods: statistical, galaxies: fundamental parameters, radio lines: galaxies

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Citation

Please use this url to cite or link to this publication: http://hdl.handle.net/1854/LU-01H92RJ0WDRWE5Q5QF1TF54DEG

MLA: Pan, Hengxing, et al. “MIGHTEE-H I : The M_HI – M* Relation over the Last Billion Years.” MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, vol. 525, no. 1, 2023, pp. 256–69, doi:10.1093/mnras/stad2343.
APA: Pan, H., Jarvis, M. J., Santos, M. G., Maddox, N., Frank, B. S., Ponomareva, A. A., … Collier, J. D. (2023). MIGHTEE-H I : the M_HI – M* relation over the last billion years. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 525(1), 256–269. https://doi.org/10.1093/mnras/stad2343
Chicago author-date: Pan, Hengxing, Matt J. Jarvis, Mario G. Santos, Natasha Maddox, Bradley S. Frank, Anastasia A. Ponomareva, Isabella Prandoni, et al. 2023. “MIGHTEE-H I : The M_HI – M* Relation over the Last Billion Years.” MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 525 (1): 256–69. https://doi.org/10.1093/mnras/stad2343.
Chicago author-date (all authors): Pan, Hengxing, 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. Hatfield, Srikrishna Sekhar, and Jordan D. Collier. 2023. “MIGHTEE-H I : The M_HI – M* Relation over the Last Billion Years.” MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 525 (1): 256–269. doi:10.1093/mnras/stad2343.
Vancouver: 1.
Pan H, Jarvis MJ, Santos MG, Maddox N, Frank BS, Ponomareva AA, et al. MIGHTEE-H I : the M_HI – M* relation over the last billion years. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. 2023;525(1):256–69.
IEEE: [1]
H. Pan et al., “MIGHTEE-H I : the M_HI – M* relation over the last billion years,” MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, vol. 525, no. 1, pp. 256–269, 2023.

@article{01H92RJ0WDRWE5Q5QF1TF54DEG,
  abstract     = {{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.}},
  author       = {{Pan, Hengxing and Jarvis, Matt J. and Santos, Mario G. and Maddox, Natasha and Frank, Bradley S. and Ponomareva, Anastasia A. and Prandoni, Isabella and Kurapati, Sushma and Baes, Maarten and Piña, Pavel E. Mancera and Rodighiero, Giulia and Meyer, Martin J. and Davé, Romeel and Sharma, Gauri and Rajohnson, Sambatriniaina H. A. and Adams, Nathan J. and Bowler, Rebecca A. A. and Sinigaglia, Francesco and van der Hulst, Thijs and Hatfield, Peter W. and Sekhar, Srikrishna and Collier, Jordan D.}},
  issn         = {{0035-8711}},
  journal      = {{MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY}},
  keywords     = {{methods: statistical,galaxies: fundamental parameters,radio lines: galaxies}},
  language     = {{eng}},
  number       = {{1}},
  pages        = {{256--269}},
  title        = {{MIGHTEE-H I : the M_HI – M* relation over the last billion years}},
  url          = {{http://doi.org/10.1093/mnras/stad2343}},
  volume       = {{525}},
  year         = {{2023}},
}

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

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