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  The diverse molecular gas content of massive galaxies undergoing quenching at z ~ 1

Belli, S., Contursi, A., Genzel, R., Tacconi, L. J., Förster-Schreiber, N. M., Lutz, D., et al. (2021). The diverse molecular gas content of massive galaxies undergoing quenching at z ~ 1. The Astrophysical Journal Letters, 909(1): L11. doi:10.3847/2041-8213/abe6a6.

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 Creators:
Belli, Sirio1, Author              
Contursi, Alessandra1, Author              
Genzel, Reinhard1, Author              
Tacconi, Linda J.1, Author              
Förster-Schreiber, Natascha M.1, Author              
Lutz, Dieter1, Author              
Combes, Françoise, Author
Neri, Roberto, Author
García-Burillo, Santiago, Author
Schuster, Karl F., Author
Herrera-Camus, Rodrigo, Author
Tadaki, Ken-ichi, Author
Davies, Rebecca L.1, Author              
Davies, Richard I.1, Author              
Johnson, Benjamin D., Author
Lee, Minju M.1, Author              
Leja, Joel, Author
Nelson, Erica J., Author
Price, Sedona H.1, Author              
Jinyi, Shangguan1, Author              
Shimizu, T. Taro1, Author              Tacchella, Sandro, AuthorÜbler, Hannah1, Author               more..
Affiliations:
1Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society, ou_159889              

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 Abstract: We present a detailed study of the molecular gas content and stellar population properties of three massive galaxies at 1 < z < 1.3 that are in different stages of quenching. The galaxies were selected to have quiescent optical/near-infrared spectral energy distribution and relatively bright emission at 24 μm, and show remarkably diverse properties. CO emission from each of the three galaxies is detected in deep NOEMA observations, allowing us to derive molecular gas fractions Mgas/M* of 13%–23%. We also reconstruct the star formation histories by fitting models to the observed photometry and optical spectroscopy, finding evidence for recent rejuvenation in one object, slow quenching in another, and rapid quenching in the third system. To better constrain the quenching mechanism we explore the depletion times for our sample and other similar samples at z ~ 0.7 from the literature. We find that the depletion times are highly dependent on the method adopted to measure the star formation rate: using the UV+IR luminosity we obtain depletion times about 6 times shorter than those derived using dust-corrected [O II] emission. When adopting the star formation rates from spectral fitting, which are arguably more robust, we find that recently quenched galaxies and star-forming galaxies have similar depletion times, while older quiescent systems have longer depletion times. These results offer new, important constraints for physical models of galaxy quenching.

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Language(s): eng - English
 Dates: 2021-03-03
 Publication Status: Published online
 Pages: -
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 Rev. Type: Peer
 Identifiers: DOI: 10.3847/2041-8213/abe6a6
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Title: The Astrophysical Journal Letters
  Other : Astrophys. J. Lett.
Source Genre: Journal
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Publ. Info: Chicago, IL : University of Chicago Press for the American Astronomical Society
Pages: - Volume / Issue: 909 (1) Sequence Number: L11 Start / End Page: - Identifier: ISSN: 0004-637X
CoNE: https://pure.mpg.de/cone/journals/resource/954922828215