Relationship between star formation rate and black hole accretion at z=3: the different contributions in quiescent, normal, and starburst galaxies
- Dipartimento di Fisica e Astronomia “G. Galilei”, Universita’ di Padova, Vicolo dell’Osservatorio 3, I-35122 (Italy)
- Dipartimento di Fisica e Astronomia, Università di Bologna, viale Berti Pichat 6/2, I-40127 Bologna (Italy)
- Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot, IRFU/Service d’Astrophysique, Bât.709, CEA-Saclay, F-91191 Gif-sur-Yvette Cedex (France)
- INAF-Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 2, I-35122 Padova (Italy)
- Department of Physics and Astronomy, University of Sheffield, S3 7RH (United Kingdom)
- Max Planck Institut für Extraterrestrische Physik, Giessenbachstrasse 1, D-85748 Garching bei München (Germany)
- INAF-Osservatorio Astronomico di Bologna, Via Ranzani 1, I-40127, Bologna (Italy)
We investigate the co-evolution of the black hole accretion rate (BHAR) and the star formation rate (SFR) in 1.5<2.5 galaxies displaying a greater diversity of star-forming properties compared to previous studies. We combine X-ray stacking and far-IR photometry of stellar mass-limited samples of normal star-forming, starburst, and quiescent/quenched galaxies in the COSMOS field. We corroborate the existence of a strong correlation between BHAR (i.e., the X-ray luminosity, L{sub X}) and stellar mass (M{sub *}) for normal star-forming galaxies, though we find a steeper relation than previously reported. We find that starbursts show a factor of three enhancement in BHAR compared to normal SF galaxies (against a factor of six excess in SFR), while quiescents show a deficit of a factor times 5.5 at a given mass. One possible interpretation of this is that the starburst phase does not coincide with cosmologically relevant BH growth, or that starburst-inducing mergers are more efficient at boosting SFR than BHAR. Contrary to studies based on smaller samples, we find that the BHAR/SFR ratio of main-sequence (MS) galaxies is not mass invariant, but scales weakly as M{sub ∗}{sup 0.43±0.09}, implying faster BH growth in more massive galaxies at z∼2. Furthermore, BHAR/SFR during the starburst is a factor of two lower than in MS galaxies, at odds with the predictions of hydrodynamical simulations of merger galaxies that foresee a sudden enhancement of L{sub X}/SFR during the merger. Finally, we estimate that the bulk of the accretion density of the universe at z∼2 is associated with normal star-forming systems, with only ∼6(±1)% and ∼11(±1)% associated with starburst and quiescent galaxies, respectively.
- OSTI ID:
- 22364185
- Journal Information:
- Astrophysical Journal Letters, Vol. 800, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 2041-8205
- Country of Publication:
- United States
- Language:
- English
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