TY - JOUR
T1 - In pursuit of giants
T2 - I. The evolution of the dust-to-stellar mass ratio in distant dusty galaxies
AU - Donevski, D.
AU - Lapi, A.
AU - Małek, K.
AU - Liu, D.
AU - Gómez-Guijarro, C.
AU - Davé, R.
AU - Kraljic, K.
AU - Pantoni, L.
AU - Man, A.
AU - Fujimoto, S.
AU - Feltre, A.
AU - Pearson, W.
AU - Li, Q.
AU - Narayanan, D.
N1 - Funding Information:
We are thankful to the anonymous referee for very constructive comments which significantly improved this paper. We would like to acknowledge Veronique Buat, Pauline Vielzeuf, Robert Feldmann, Ciro Pappalardo and Federico Bianchini for useful discussions, comments and/or support. This work has been partially supported by PRIN MIUR 2017 prot. 20173ML3WW002, "Opening the ALMA window on the cosmic evolution of gas, stars and supermassive black holes". D.D. acknowledge the Dunlap visitor program, at the Dunlap Institute for Astronomy & Astrophysics at the University of Toronto. A.L. acknowledges the MIUR grant "Finanziamento annuale individuale attivita base di ricerca" and the EU H2020-MSCA-ITN-2019 Project 860744 "BiD4BEST: Big Data applications for Black hole Evolution STudies". K.M. has been supported by the National Science Centre (UMO-2018/30/E/ST9/00082). D.L. acknowledges funding from the European Research Council (ERC) under the European Union s Horizon 2020 research and innovation programme (grant agreement No. 694343). A.M. is supported by a Dunlap Fellowship at the Dunlap Institute for Astronomy & Astrophysics, funded through an endowment established by the David Dunlap family and the University of Toronto. The University of Toronto operates on the traditional land of the Huron-Wendat, the Seneca, and most recently, the Mississaugas of the Credit River; A.M. and D.D. are grateful to have the opportunity to work on this land. S.F. acknowledge support from the European Research Council (ERC) Consolidator Grant funding scheme (project ConTExt, grant No. 648179). The Cosmic Dawn Center is funded by the Danish National Research Foundation under grant No. 140. A.F. acknowledges the support from grant PRIN MIUR 2017 20173ML3WW. This paper make use of following ALMA data: ADS/JAO.ALMA: #2011.0.00064.S, #2011. 0.00097.S, #2011.0.00539.S, #2011.0.00742.S, #2012.1.00076.S, #2012.1.00323.S, #2012.1.00523.S, #2012.1.00536.S, #2012.1.00919.S, #2012.1.00952.S, #2012.1.00978.S, #2013.1.00884.S, #2013.1.00914.S, #2015.1.00137.S, #2015.1.00568.S, #2015.1.00664.S, #2015.1.00704.S, #2015.1.00853.S, #2015.1.00861.S, #2015.1.00862.S, #2015.1.00928.S, #2015.1.01074.S, #2015.1.01590.S, #2015.A.00026.S, #2016.1.00478.S, #2016.1.00624.S, #2016.1.00735.S. 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:
Acknowledgements. We are thankful to the anonymous referee for very constructive comments which significantly improved this paper. We would like to acknowledge Veronique Buat, Pauline Vielzeuf, Robert Feldmann, Ciro Pappalardo and Federico Bianchini for useful discussions, comments and/or support. This work has been partially supported by PRIN MIUR 2017 prot. 20173ML3WW002, “Opening the ALMA window on the cosmic evolution of gas, stars and supermassive black holes”. D.D. acknowledge the Dunlap visitor program, at the Dunlap Institute for Astronomy & Astrophysics at the University of Toronto. A.L. acknowledges the MIUR grant “Finanziamento annuale individuale attivitá base di ricerca” and the EU H2020-MSCA-ITN-2019 Project 860744 “BiD4BEST: Big Data applications for Black hole Evolution STudies”. K.M. has been supported by the National Science Centre (UMO-2018/30/E/ST9/00082). D.L. acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 694343). A.M. is supported by a Dunlap Fellowship at the Dunlap Institute for Astronomy & Astrophysics, funded through an endowment established by the David Dunlap family and the University of Toronto. The University of Toronto operates on the traditional land of the Huron-Wendat, the Seneca, and most recently, the Mississaugas of the Credit River; A.M. and D.D. are grateful to have the opportunity to work on this land. S.F. acknowledge support from the European Research Council (ERC) Consolidator Grant funding scheme (project ConTExt, grant No. 648179). The Cosmic Dawn Center is funded by the Danish National Research Foundation under grant No. 140. A.F. acknowledges the support from grant PRIN MIUR 2017 20173ML3WW. This paper make use of following ALMA data: ADS/JAO.ALMA: #2011.0.00064.S, #2011. 0.00097.S, #2011.0.00539.S, #2011.0.00742.S, #2012.1.00076.S, #2012.1.00323.S, #2012.1.00523.S, #2012.1.00536.S, #2012.1.00919.S, #2012.1.00952.S, #2012.1.00978.S, #2013.1.00884.S, #2013.1.00914.S, #2015.1.00137.S, #2015.1.00568.S, #2015.1.00664.S, #2015.1.00704.S, #2015.1.00853.S, #2015.1.00861.S, #2015.1.00862.S, #2015.1.00928.S, #2015.1.01074.S, #2015.1.01590.S, #2015.A.00026.S, #2016.1.00478.S, #2016.1.00624.S, #2016.1.00735.S. 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.
Publisher Copyright:
© ESO 2020.
PY - 2020/12/1
Y1 - 2020/12/1
N2 - The dust-to-stellar mass ratio (Mdust/M? ) is a crucial, albeit poorly constrained, parameter for improving our understanding of the complex physical processes involved in the production of dust, metals, and stars in galaxy evolution. In this work, we explore trends of Mdust/M? with different physical parameters and using observations of 300 massive dusty star-forming galaxies detected with ALMA up to z? ≈? 5. Additionally, we interpret our findings with different models of dusty galaxy formation. We find that Mdust/M? evolves with redshift, stellar mass, specific star formation rates, and integrated dust size, but that evolution is different for main-sequence galaxies than it is for starburst galaxies. In both galaxy populations, Mdust/M? increases until z? ∼? 2, followed by a roughly flat trend towards higher redshifts, suggesting efficient dust growth in the distant universe. We confirm that the inverse relation between Mdust/M? and M? holds up to z? ≈? 5 and can be interpreted as an evolutionary transition from early to late starburst phases. We demonstrate that the Mdust/M? in starbursts reflects the increase in molecular gas fraction with redshift and attains the highest values for sources with the most compact dusty star formation. State-of-the-art cosmological simulations that include self-consistent dust growth have the capacity to broadly reproduce the evolution of Mdust/M? in main-sequence galaxies, but underestimating it in starbursts. The latter is found to be linked to lower gas-phase metallicities and longer dust-growth timescales relative to observations. The results of phenomenological models based on the main-sequence and starburst dichotomy as well as analytical models that include recipes for rapid metal enrichment are consistent with our observations. Therefore, our results strongly suggest that high Mdust/M? is due to rapid dust grain growth in the metal-enriched interstellar medium. This work highlights the multi-fold benefits of using Mdust/M? as a diagnostic tool for: (1) disentangling main-sequence and starburst galaxies up to z? ∼? 5; (2) probing the evolutionary phase of massive objects; and (3) refining the treatment of the dust life cycle in simulations.
AB - The dust-to-stellar mass ratio (Mdust/M? ) is a crucial, albeit poorly constrained, parameter for improving our understanding of the complex physical processes involved in the production of dust, metals, and stars in galaxy evolution. In this work, we explore trends of Mdust/M? with different physical parameters and using observations of 300 massive dusty star-forming galaxies detected with ALMA up to z? ≈? 5. Additionally, we interpret our findings with different models of dusty galaxy formation. We find that Mdust/M? evolves with redshift, stellar mass, specific star formation rates, and integrated dust size, but that evolution is different for main-sequence galaxies than it is for starburst galaxies. In both galaxy populations, Mdust/M? increases until z? ∼? 2, followed by a roughly flat trend towards higher redshifts, suggesting efficient dust growth in the distant universe. We confirm that the inverse relation between Mdust/M? and M? holds up to z? ≈? 5 and can be interpreted as an evolutionary transition from early to late starburst phases. We demonstrate that the Mdust/M? in starbursts reflects the increase in molecular gas fraction with redshift and attains the highest values for sources with the most compact dusty star formation. State-of-the-art cosmological simulations that include self-consistent dust growth have the capacity to broadly reproduce the evolution of Mdust/M? in main-sequence galaxies, but underestimating it in starbursts. The latter is found to be linked to lower gas-phase metallicities and longer dust-growth timescales relative to observations. The results of phenomenological models based on the main-sequence and starburst dichotomy as well as analytical models that include recipes for rapid metal enrichment are consistent with our observations. Therefore, our results strongly suggest that high Mdust/M? is due to rapid dust grain growth in the metal-enriched interstellar medium. This work highlights the multi-fold benefits of using Mdust/M? as a diagnostic tool for: (1) disentangling main-sequence and starburst galaxies up to z? ∼? 5; (2) probing the evolutionary phase of massive objects; and (3) refining the treatment of the dust life cycle in simulations.
KW - Galaxies: ISM
KW - Galaxies: evolution
KW - Galaxies: high-redshift
KW - Galaxies: star formation
KW - Galaxies: starburst
KW - Submillimeter: galaxies
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UR - http://www.scopus.com/inward/citedby.url?scp=85097912059&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/202038405
DO - 10.1051/0004-6361/202038405
M3 - Article
AN - SCOPUS:85097912059
SN - 0004-6361
VL - 644
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A144
ER -