The infrared-luminous progenitors of high-<i>z</i>quasars

Ginolfi, M.; Schneider, Raffaella; Valiante, Rosa; Pezzulli, Edwige; Graziani, Luca; Fujimoto, Seiji; Maiolino, R.

doi:10.1093/mnras/sty3205

Cited by 13 publications

(9 citation statements)

References 91 publications

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“…These are known to host extreme starbursts with SFR ∼ 3000 M yr −1 (for the former two) and ∼380 M yr −1 (for G09 83808, after correcting for gravitational magnification), which has allowed their host galaxies to grow as massive as ∼10 11 M within a fairly short time. This picture is consistent with recent simulation work of merger-induced galaxy evolution (Ginolfi et al 2019), which suggested that z ∼ 7 hyper-luminous infrared galaxies (HyLIRGs) are indeed the ancestors of z ∼ 6 luminous quasars.…”

Section: Differential Form: L Bol -L Firsupporting

confidence: 92%

Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs). VIII. A less biased view of the early co-evolution of black holes and host galaxies

Izumi

Onoue

Matsuoka

et al. 2019

Publications of the Astronomical Society of Japan

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We present ALMA [C ii] line and far-infrared (FIR) continuum observations of three $z \gt 6$ low-luminosity quasars ($M_{\rm 1450} \gt -25$ mag) discovered by our Subaru Hyper Suprime-Cam (HSC) survey. The [C ii] line was detected in all three targets with luminosities of $(2.4\mbox{--}9.5) \times 10^8\, L_{\odot }$, about one order of magnitude smaller than optically luminous ($M_{\rm 1450} \lesssim -25$ mag) quasars. The FIR continuum luminosities range from $\lt 9 \times 10^{10}\, L_{\odot }$ (3 $\sigma$ limit) to ${\sim } 2 \times 10^{12}\, L_{\odot }$, indicating a wide range in star formation rates in these galaxies. Most of the HSC quasars studied thus far show [C ii]/ FIR luminosity ratios similar to local star-forming galaxies. Using the [C ii]-based dynamical mass ($M_{\rm dyn}$) as a surrogate for bulge stellar mass ($M_{\rm\, bulge}$), we find that a significant fraction of low-luminosity quasars are located on or even below the local $M_{\rm\, BH}$–$M_{\rm\, bulge}$ relation, particularly at the massive end of the galaxy mass distribution. In contrast, previous studies of optically luminous quasars have found that black holes are overmassive relative to the local relation. Given the low luminosities of our targets, we are exploring the nature of the early co-evolution of supermassive black holes and their hosts in a less biased way. Almost all of the quasars presented in this work are growing their black hole mass at a much higher pace at $z \sim 6$ than the parallel growth model, in which supermassive black holes and their hosts grow simultaneously to match the local $M_{\rm\, BH}$–$M_{\rm\, bulge}$ relation at all redshifts. As the low-luminosity quasars appear to realize the local co-evolutionary relation even at $z \sim 6$, they should have experienced vigorous starbursts prior to the currently observed quasar phase to catch up with the relation.

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Section: Differential Form: L Bol -L Firsupporting

confidence: 92%

Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs). VIII. A less biased view of the early co-evolution of black holes and host galaxies

Izumi

Onoue

Matsuoka

et al. 2019

Publications of the Astronomical Society of Japan

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show abstract

“…These are known to host extreme starbursts with SFR ∼ 3000 M⊙ yr −1 (for the former two) and ∼ 380 M⊙ yr −1 (for G09 83808, after correcting for gravitational magnification), which has allowed their host galaxies to grow as massive as ∼ 10 11 M⊙ within a fairly short time. This picture is consistent with recent simulation work of merger-induced galaxy evolution (Ginolfi et al 2019), which suggested that z ∼ 7 hyperluminous infrared galaxies (HyLIRGs) are indeed the ancestors of z ∼ 6 luminous quasars.…”

Section: Differential Form: L Bol − Lfirsupporting

confidence: 92%

Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs) VIII. A less biased view of the early co-evolution of black holes and host galaxies

Izumi,

Onoue,

Matsuoka

et al. 2019

Preprint

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We present ALMA [C II] line and far-infrared (FIR) continuum observations of three z > 6 lowluminosity quasars (M 1450 > −25 mag) discovered by our Subaru Hyper Suprime-Cam (HSC) survey. The [C II] line was detected in all three targets with luminosities of (2.4 − 9.5) × 10 8 L ⊙ , about one order of magnitude smaller than optically luminous (M 1450 < ∼ −25 mag) quasars. The FIR continuum luminosities range from < 9 × 10 10 L ⊙ (3σ limit) to ∼ 2 × 10 12 L ⊙ , indicating a wide range in star formation rates in these galaxies. Most of the HSC quasars studied thus far show [C II]/FIR luminosity ratios similar to local star-forming galaxies. Using the [C II]-based dynamical mass (M dyn ) as a surrogate for bulge stellar mass (M bulge ), we find that a significant fraction of low-luminosity quasars are located on or even below the local M BH − M bulge relation, particularly at the massive end of the galaxy mass distribution. In contrast, previous studies of optically luminous quasars have found that black holes are overmassive relative to the local relation. Given the low luminosities of our targets, we are exploring the nature of the early co-evolution of supermassive black holes and their hosts in a less biased way. Almost all of the quasars presented in this work are growing their black hole mass at much higher pace at z ∼ 6 than the parallel growth model, in which supermassive black holes and their hosts grow simultaneously to match the local M BH − M bulge relation at all redshifts. As the low-luminosity quasars appear to realize the local co-evolutionary relation even at z ∼ 6, they should have experienced vigorous starbursts prior to the currently observed quasar phase to catch up with the relation.

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“…The [C II] 158 micron line is a workhorse for (sub-)mm observations and is resolved on a kiloparsec scale by ALMA (Rybak et al 2019). As extended [C II] halos are found more and more commonly in high-z galaxies (early star forming sources of 10 11 -10 12 M ⊙ with classical 'normal' star forming galaxies; Ginolfi et al 2019;Hodge & da Cunha 2020) and because [C II] emissions tracing a combination of molecular, ionised, and atomic gas are still very little explored, future assessments of H 2 via [C II] could significantly improve the current picture for H 2 .…”

Section: Discussionmentioning

confidence: 99%

Atomic and molecular gas from the epoch of reionisation down to redshift 2

Maio

Péroux

Ciardi

2022

A&A

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Context. Cosmic gas makes up about 90% of the baryonic matter in the Universe and H2 molecule is the most tightly linked to star formation. Aims. In this work we study cold neutral gas, its H2 component at different epochs, and corresponding depletion times. Methods. We perform state-of-the-art hydrodynamic simulations that include time-dependent atomic and molecular non-equilibrium chemistry coupled to star formation, feedback effects, different UV backgrounds presented in the recent literature and a number of additional processes occurring during structure formation (COLDSIM). We predict gas evolution and contrast the mass density parameters and gas depletion timescales. We also investigate their relation to cosmic expansion in light of the latest infrared and (sub)millimetre observations in the redshift range 2 ≲ z ≲ 7. Results. By performing updated non-equilibrium chemistry calculations we are able to broadly reproduce the latest HI and H2 observations. We find neutral-gas mass density parameters Ωneutral ≃ 10−3 and increasing from lower to higher redshift, in agreement with available HI data. Because of the typically low metallicities during the epoch of reionisation, time-dependent H2 formation is mainly led by the H− channel in self-shielded gas, while H2 grain catalysis becomes important in locally enriched sites at any redshift. Ultraviolet (UV) radiation provides free electrons and facilitates H2 build-up while heating cold metal-poor environments. Resulting H2 fractions can be as high as ∼50% of the cold gas mass at z ∼ 4–8, in line with the latest measurements from high-redshift galaxies. The H2 mass density parameter increases with time until a plateau of ΩH2 ≃ 10−4 is reached. Quantitatively, we find agreement between the derived ΩH2 values and the observations up to z ∼ 7 and both HI and H2 trends are better reproduced by our non-equilibrium H2-based star formation modelling. The predicted gas depletion timescales decrease at lower z in the whole time interval considered, with H2 depletion times remaining below the Hubble time and comparable to the dynamical time at all z. This implies that non-equilibrium molecular cooling is efficient at driving cold-gas collapse in a broad variety of environments and has done so since very early cosmic epochs. While the evolution of chemical species is clearly affected by the details of the UV background and gas self shielding, the assumptions on the adopted initial mass function, different parameterizations of H2 dust grain catalysis, photoelectric heating, and cosmic-ray heating can affect the results in a non-trivial way. In the Appendix, we show detailed analyses of individual processes, as well as simple numerical parameterizations and fits to account for them. Conclusions. Our findings suggest that, in addition to HI, non-equilibrium H2 observations are pivotal probes for assessing cold-gas cosmic abundances and the role of UV background radiation at different epochs.

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The infrared-luminous progenitors of high-zquasars

Cited by 13 publications

References 91 publications

Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs). VIII. A less biased view of the early co-evolution of black holes and host galaxies

Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs). VIII. A less biased view of the early co-evolution of black holes and host galaxies

Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs) VIII. A less biased view of the early co-evolution of black holes and host galaxies

Atomic and molecular gas from the epoch of reionisation down to redshift 2

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