A dusty compact object bridging galaxies and quasars at cosmic dawn

Fujimoto, Seiji; Brammer, Gabriel; Watson, Derrick G.; Magdis, G.; Kokorev, Vasily; Greve, T. R.; Toft, Sune; Walter, Fabian; Valiante, Rosa; Ginolfi, M.; Schneider, Raffaella; Valentino, F.; Colina, L.; Vestergaard, M.; Marques-Chaves, R.; Fynbo, J. P. U.; Krips, M.; Steinhardt, Charles L.; Cortzen, Isabella; Rizzo, Francesca; Oesch, P.

doi:10.1038/s41586-022-04454-1

Cited by 58 publications

(60 citation statements)

References 160 publications

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“…The [CII] line of COS-87259 is nearly 5× brighter than typical extremely bright 𝑧 > 6.5 quasars (median L [CII] = 2.0 × 10 9 𝐿 ) and 16× brighter than typical UV-bright Lyman-break 𝑧 > 6.5 galaxies (median L [CII] = 0.55 × 10 9 𝐿 ). COS-87259 additionally shows a [CII] line that is 4.7-8.0× brighter than the two reddened type 1 quasars thus far identified at 𝑧 > 6.5 (Izumi et al 2021;Fujimoto et al 2022).…”

Section: Comparison Of Far-ir Properties To Other Z > 65 Sourcesmentioning

confidence: 87%

“…We compare the observed far-infrared properties ([CII] luminosity, [CII] FWHM, and monochromatic 158𝜇m dust continuum luminosity) of COS-87259 to other known objects in the reionizationera. From the literature, we compile such measured properties from known 𝑧 > 6.5 sub-mm galaxies (Strandet et al 2017;Marrone et al 2018), extremely UV-luminous quasars (M UV ≤ −25; Venemans et al 2012;Bañados et al 2015;Venemans et al 2016Venemans et al , 2017bMazzucchelli et al 2017;Decarli et al 2018;Yang et al 2019bYang et al , 2020bWang et al 2021;Yue et al 2021), UV-bright Lyman-break galaxies (M UV ≤ −21; Pentericci et al 2016;Smit et al 2018;Hashimoto et al 2019;Bouwens et al 2021a;Inami et al 2022;Schouws et al 2022b,a), reddened type 1 quasars (Izumi et al 2021;Fujimoto et al 2022), as well as companion galaxies serendipitously identified from ALMA observations (Decarli et al 2017;Willott et al 2017;Neeleman et al 2019;Venemans et al 2019Venemans et al , 2020Fudamoto et al 2021). We correct the properties of the sub-mm system SPT0311-58 and the quasar J0439+1634 for gravitational lensing given reported magnitification factors (Marrone et al 2018;Yue et al 2021).…”

Section: Comparison Of Far-ir Properties To Other Z > 65 Sourcesmentioning

confidence: 99%

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ALMA Confirmation of an Obscured Hyperluminous Radio-Loud AGN at $z=6.853$ Associated with a Dusty Starburst in the 1.5 deg$^2$ COSMOS Field

Endsley¹,

Stark²,

Lyu³

et al. 2022

Preprint

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We present band 6 ALMA observations of a heavily-obscured radio-loud (𝐿 1.4 GHz = 10 25.4 W Hz −1 ) AGN candidate at 𝑧 phot = 6.83 ± 0.06 found in the 1.5 deg 2 COSMOS field. The ALMA data reveal detections of exceptionally strong [CII]158𝜇m (𝑧 [CII] = 6.8532) and underlying dust continuum emission from this object (COS-87259), where the [CII] line luminosity, line width, and 158𝜇m continuum luminosity are comparable to that seen from 𝑧 ∼ 7 sub-mm galaxies and quasar hosts. The 158𝜇m continuum detection suggests a total infrared luminosity of 9 × 10 12 𝐿 with corresponding very large obscured star formation rate (1300 𝑀 /yr) and dust mass (2 × 10 9 𝑀 ). The apparent strong Balmer break seen between the VIRCam and IRAC photometry suggests that COS-87259 is an extremely massive reionization era galaxy with 𝑀 * ≈ 1.7×10 11 𝑀 . Moreover, the MIPS, PACS, and SPIRE detections imply that this object harbors an AGN that is heavily obscured (𝜏 9.7𝜇m = 2.3) with a bolometric luminosity of approximately 5 × 10 13 𝐿 . Such a very high AGN luminosity suggests this object is powered by an ≈1.6 × 10 9 𝑀 black hole if accreting near the Eddington limit, and is effectively a highly-obscured version of an extremely UV-luminous (𝑀 1450 ≈ −27.3) 𝑧 ∼ 7 quasar. Notably, these 𝑧 ∼ 7 quasars are an exceedingly rare population (∼0.001 deg −2 ) while COS-87259 was identified over a relatively small field. Future very wide-area surveys with, e.g., Roman and Euclid have the potential to identify many more extremely red yet UV-bright 𝑧 7 objects similar to COS-87259, providing richer insight into the occurrence of intense obscured star formation and supermassive black hole growth among this population.

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Section: Comparison Of Far-ir Properties To Other Z > 65 Sourcesmentioning

confidence: 87%

Section: Comparison Of Far-ir Properties To Other Z > 65 Sourcesmentioning

confidence: 99%

ALMA Confirmation of an Obscured Hyperluminous Radio-Loud AGN at $z=6.853$ Associated with a Dusty Starburst in the 1.5 deg$^2$ COSMOS Field

Endsley¹,

Stark²,

Lyu³

et al. 2022

Preprint

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show abstract

“…6 The prediction that highly super-Eddington sources would be heavily obscured is bolstered by the expectation that a large supply of dense gas is required to fuel such elevated accretion rates, as this gas would further attenuate any radiation that is not trapped in the accretion flow. Consistent with this, recent observations of highly obscured quasars at z  7 that may be powered by BHs accreting at super-Eddington rates (Fujimoto et al 2022;Endsley et al 2022) strengthen the possibility that upcoming next-generation facilities such as the Rubin Observatory (Ivezić et al 2019), Euclid (Euclid Collaboration et al 2019) and the recently launched James Webb Space Telescope (Gardner et al 2006) may uncover evidence that the progenitors of the BHs powering such quasars are grown through sustained super-Eddington accretion.…”

Section: Comparison To Datamentioning

confidence: 60%

“…Indeed, no observed BHs lie beyond the limit in our Figure 2. If they are unveiled by future observations, this would add to the evidence for significant obscured BH growth taking place in the early universe (e.g., Treister et al 2013;Comastri et al 2015;Pezzulli et al 2017a;Endsley et al 2022;Fujimoto et al 2022) and provide strong evidence that sustained super-Eddington growth may explain the emergence of the most massive BHs inferred to power high-z quasars. The expectation that highly super-Eddington BHs would be heavily obscured not only due to the trapping of radiation in the accretion flow, but also due to attenuation by the surrounding dense gas from which they are accreting is, in fact, broadly consistent with the recent finding of Gilli et al (2022) that 80%-90% of supermassive BHs at z  6 may be hidden from view by the dense gas in their host galaxies.…”

Section: Discussionmentioning

confidence: 85%

A Simple Condition for Sustained Super-Eddington Black Hole Growth

Johnson

Sanderbeck

2022

ApJ

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One of the most pressing questions in cosmology is how the black holes (BHs) powering quasars at high redshift grow to supermassive scales within a billion years of the Big Bang. Here we show that sustained super-Eddington accretion can be achieved for BHs with Eddington fractions f Edd ≳ 2/ϵ, where ϵ is the efficiency with which radiation is generated in the accretion process. In this regime, the radiation carries too little momentum to halt the accretion flow and the infalling gas traps the radiation. The BH growth then proceeds unimpeded until the gas supply is exhausted, in contrast to accretion at lower rates, which is limited by the radiation generated in the accretion process. The large gas supply available in massive high-redshift quasar host galaxies may be readily accreted onto seed BHs via this supply-limited mode of accretion, providing an explanation for how such supermassive BHs are assembled in the early universe. This sustained super-Eddington growth may also explain the short lifetimes inferred for the H ii regions surrounding high-redshift quasars, if the bulk of the BH growth occurs without the associated radiation escaping to ionize the intergalactic medium. It furthermore implies that a population of obscured rapidly growing BHs may be difficult to detect, perhaps explaining why so few quasars with Eddington fractions higher than a few have been observed. Finally, this simple condition for sustained super-Eddington growth can easily be implemented in cosmological simulations that can be used to assess in which environments it occurs.

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“…Thus especially at high redshifts and/or for upper outliers of the Magorrian relationship (i.e., BHs with billion solar masses), the growth of the central BH should proceed at appreciably high values of λ, and possibly in super-Eddington conditions (as in the bottom panels). Though this instance can be partially justified theoretically (e.g., Li 2012;Madau et al 2014) and there are hints of a few cases at z 6 (e.g., Fujimoto et al 2022), it struggles somewhat against the bulk of present observational estimates at z 6 (see references below and Fig. 5).…”

Section: Basic Resultsmentioning

confidence: 90%

The Black Hole Mass Function across Cosmic Time. II. Heavy Seeds and (Super)Massive Black Holes

Sicilia

Lapi

Boco

et al. 2022

ApJ

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This is the second paper in a series aimed at modeling the black hole (BH) mass function from the stellar to the (super)massive regime. In the present work, we focus on (super)massive BHs and provide an ab initio computation of their mass function across cosmic time. We consider two main mechanisms to grow the central BH that are expected to cooperate in the high-redshift star-forming progenitors of local massive galaxies. The first is the gaseous dynamical friction process, which can cause the migration toward the nuclear regions of stellar mass BHs originated during the intense bursts of star formation in the gas-rich host progenitor galaxy and the buildup of a central heavy BH seed, M • ∼ 103−5 M ⊙, within short timescales of ≲some 107 yr. The second mechanism is the standard Eddington-type gas disk accretion onto the heavy BH seed through which the central BH can become (super)massive, M • ∼ 106−10 M ⊙, within the typical star formation duration, ≲1 Gyr, of the host. We validate our semiempirical approach by reproducing the observed redshift-dependent bolometric AGN luminosity functions and Eddington ratio distributions and the relationship between the star formation and the bolometric luminosity of the accreting central BH. We then derive the relic (super)massive BH mass function at different redshifts via a generalized continuity equation approach and compare it with present observational estimates. Finally, we reconstruct the overall BH mass function from the stellar to the (super)massive regime over more than 10 orders of magnitudes in BH mass.

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A dusty compact object bridging galaxies and quasars at cosmic dawn

Cited by 58 publications

References 160 publications

ALMA Confirmation of an Obscured Hyperluminous Radio-Loud AGN at $z=6.853$ Associated with a Dusty Starburst in the 1.5 deg$^2$ COSMOS Field

ALMA Confirmation of an Obscured Hyperluminous Radio-Loud AGN at $z=6.853$ Associated with a Dusty Starburst in the 1.5 deg$^2$ COSMOS Field

A Simple Condition for Sustained Super-Eddington Black Hole Growth

The Black Hole Mass Function across Cosmic Time. II. Heavy Seeds and (Super)Massive Black Holes

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