High dust content of a quiescent galaxy at z ∼ 2 revealed by deep ALMA observation

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  • Minju M. Lee
  • Charles C. Steidel
  • Brammer, Gabriel
  • Natascha Förster-Schreiber
  • Alvio Renzini
  • Daizhong Liu
  • Rodrigo Herrera-Camus
  • Thorsten Naab
  • Sedona H. Price
  • Hannah Übler
  • Sebastián Arriagada-Neira
  • Magdis, Georgios
We report the detection of cold dust in an apparently quiescent massive galaxy (log (M⋆/M⊙) ≈ 11) at z ∼ 2 (G4). The source is identified as a serendipitous 2 mm continuum source in a deep ALMA observation within the field of Q2343-BX610, a z = 2.21 massive star-forming disc galaxy. Available multiband photometry of G4 suggests redshift of z ∼ 2 and a low specific star formation rate (sSFR), log (SFR/M⋆)[yr−1] ≈ −10.2, corresponding to ≈1.2 dex below the z = 2 main sequence (MS). G4 appears to be a peculiar dust-rich quiescent galaxy for its stellar mass (log (Mdust/M⋆) = −2.71 ± 0.26), with its estimated mass-weighted age (∼1–2 Gyr). We compile z ≳ 1 quiescent galaxies in the literature and discuss their age–ΔMS and log (Mdust/M⋆)–age relations to investigate passive evolution and dust depletion scale. A long dust depletion time and its morphology suggest morphological quenching along with less efficient feedback that could have acted on G4. The estimated dust yield for G4 further supports this idea, requiring efficient survival of dust and/or grain growth, and rejuvenation (or additional accretion). Follow-up observations probing the stellar light and cold dust peak are necessary to understand the implication of these findings in the broader context of galaxy evolutionary studies and quenching in the early universe.
OriginalsprogEngelsk
TidsskriftMonthly Notices of the Royal Astronomical Society
Vol/bind527
Udgave nummer4
Sider (fra-til)9529-9547
Antal sider19
ISSN0035-8711
DOI
StatusUdgivet - 2024

Bibliografisk note

Funding Information:
We thank the referee for a careful reading of the manuscript and very helpful comments that helped to improve the paper. MML thanks Francesco Valentino and Katherine E. Whitaker for general discussions on high-redshift quiescent galaxies and their dust observations. MML also thanks Steven Gilman for helpful comments on the data analysis, Aswin Vijayan for comments on cosmological simulations, Médéric Boquien for the comments on the CIGALE code, and David Blánquez-Sesé for offering the median stack UVJ colours of z ∼ 1 quiescent galaxies. This project has received funding from the European Union’s Horizon Europe research and innovation programme under the Marie Skłodowska-Curie grant agreement no. 101107795. This work was partially supported by DeiC National HPC (DeiC-DTU-L-20210103) and by grant AST2009278 from the US NSF (CCS). RH-C thanks to the Max Planck Society for support under the Partner Group project ‘The Baryon Cycle in Galaxies’ between the Max Planck for Extraterrestrial Physics and the Universidad de Concepción. RH-C also gratefully acknowledges financial support from Millenium Nucleus NCN19058 (TITANs), and ANID BASAL projects ACE210002 and FB210003. GEM acknowledges the Villum Fonden research grant 13160 ‘Gas to stars, stars to dust: tracing star formation across cosmic time’, grant 37440, ‘The Hidden Cosmos’, and the Cosmic Dawn Center of Excellence funded by the Danish National Research Foundation under the grant DNRF140. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2019.1.01362.S, #2019.1.00853.S, #2017.1.00856.S, #2017.1.01045.S, #2015.1.00250.S, #2013.1.00059S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ.

Funding Information:
We thank the referee for a careful reading of the manuscript and very helpful comments that helped to improve the paper. MML thanks Francesco Valentino and Katherine E. Whitaker for general discussions on high-redshift quiescent galaxies and their dust observations. MML also thanks Steven Gilman for helpful comments on the data analysis, Aswin Vijayan for comments on cosmological simulations, Médéric Boquien for the comments on the CIGALE code, and David Blánquez-Sesé for offering the median stack UVJ colours of z ∼ 1 quiescent galaxies. This project has received funding from the European Union’s Horizon Europe research and innovation programme under the Marie Skłodowska-Curie grant agreement no. 101107795. This work was partially supported by DeiC National HPC (DeiC-DTU-L-20210103) and by grant AST2009278 from the US NSF (CCS). RH-C thanks to the Max Planck Society for support under the Partner Group project ‘The Baryon Cycle in Galaxies’ between the Max Planck for Extraterrestrial Physics and the Universidad de Concepción. RH-C also gratefully acknowledges financial support from Millenium Nucleus NCN19058 (TITANs), and ANID BASAL projects ACE210002 and FB210003. GEM acknowledges the Villum Fonden research grant 13160 ‘Gas to stars, stars to dust: tracing star formation across cosmic time’, grant 37440, ‘The Hidden Cosmos’, and the Cosmic Dawn Center of Excellence funded by the Danish National Research Foundation under the grant DNRF140. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2019.1.01362.S, #2019.1.00853.S, #2017.1.00856.S, #2017.1.01045.S, #2015.1.00250.S, #2013.1.00059S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ.

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© 2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.

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