Submillimeter Evidence for the Coeval Growth of Massive Black Holes and Galaxy Bulges

Page, M. J.; Stevens, J. A.; Mittaz, J. P. D.; Carrera, Francisco J.

doi:10.1126/science.1065880

Cited by 82 publications

(120 citation statements)

References 30 publications

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“…There are however a number of X-ray AGN that are individually detected at 850µm in Banerji et al (2015a) with 850µm flux densities of ∼4-10 mJy, comparable with the inferred submillimetre fluxes of our reddened quasars. Previous SCUBA surveys of X-ray absorbed and X-ray unabsorbed quasars have suggested a link between cold dust emission and X-ray obscuration (Page et al 2001;Stevens et al 2005) and we note that for those reddened quasars where we have X-ray spectra (e.g. Banerji et al 2014), moderate column densities of ∼10 22 cm −2 are present.…”

Section: Comparison To Unobscured "Blue" Quasars and X-ray Agnmentioning

confidence: 88%

The discovery of gas-rich, dusty starbursts in luminous reddened quasars atz∼ 2.5 with ALMA

Banerji

Carilli

Jones

et al. 2016

Mon. Not. R. Astron. Soc.

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We present ALMA observations of cold dust and molecular gas in four high-luminosity, heavily reddened (A V ∼ 2.5 − 6 mag) Type 1 quasars at z ∼ 2.5 with virial M BH ∼ 10 10 M , to test whether dusty, massive quasars represent the evolutionary link between submillimetre bright galaxies (SMGs) and unobscured quasars. All four quasars are detected in both the dust continuum and in the 12 CO(3-2) line. The mean dust mass is 6×10 8 M assuming a typical high redshift quasar spectral energy distribution (T=41K, β=1.95 or T=47K, β=1.6). The implied star formation rates are very high -1000 M yr −1 in all cases. Gas masses estimated from the CO line luminosities cover ∼1-5×10 10 (α CO /0.8)M and the gas depletion timescales are very short -∼ 5 − 20Myr. A range of gas-to-dust ratios is observed in the sample. We resolve the molecular gas in one quasar -ULASJ2315+0143 (z = 2.561) -which shows a strong velocity gradient over ∼20 kpc. The velocity field is consistent with a rotationally supported gas disk but other scenarios, e.g. mergers, cannot be ruled out at the current resolution of these data. In another quasar -ULASJ1234+0907 (z = 2.503) -we detected molecular line emission from two millimetre bright galaxies within 200 kpc of the quasar, suggesting that this quasar resides in a significant over-density. The high detection rate of both cold dust and molecular gas in these sources, suggests that reddened quasars could correspond to an early phase in massive galaxy formation associated with large gas reservoirs and significant star formation.

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Section: Comparison To Unobscured "Blue" Quasars and X-ray Agnmentioning

confidence: 88%

The discovery of gas-rich, dusty starbursts in luminous reddened quasars atz∼ 2.5 with ALMA

Banerji

Carilli

Jones

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Page et al (2001) measured 850 m fluxes for a sample of eight z >1 X-ray-absorbed, radio-quiet quasars (with column densities of 21:4 < log N H < 22:5 based on the X-ray absorption; these sources show little or no obscuration in their broad emission lines and ultraviolet continua) discovered serendipitously in archival X-ray data, whereas Page et al (2004) measured 850 m fluxes for a comparison sample of 20 unabsorbed quasars. The latter sources were drawn from a combination of X-ray surveys and were matched in luminosity and redshift to the absorbed sample.…”

Section: Higg H Redshift Quasar Studies Of the Luminosity-dependent Umentioning

confidence: 99%

The Cosmic Evolution of Hard X-Ray-selected Active Galactic Nuclei

et al. 2005

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We use highly spectroscopically complete deep and wide-area Chandra surveys to determine the cosmic evolution of hard X-ray-selected active galactic nuclei (AGNs). For the deep fields, we supplement the spectroscopic redshifts with photometric redshifts to assess where the unidentified sources are likely to lie. We find that the median redshifts are fairly constant with X-ray flux at z $ 1.We classify the optical spectra and measure the FWHM line widths. Most of the broad-line AGNs show essentially no visible absorption in X-rays, whereas the sources without broad lines (FWHM < 2000 km s À1 ; ''optically narrow'' AGNs) show a wide range of absorbing column densities. We determine hard X-ray luminosity functions for all spectral types with L X ! 10 42 ergs s À1 and for broad-line AGNs alone. At z < 1:2, both are well described by pure luminosity evolution, with L * evolving as (1 þ z) 3:2AE0:8 for all spectral types and as (1 þ z) 3:0AE1:0 for broad-line AGNs alone. Thus, all AGNs drop in luminosity by almost an order of magnitude over this redshift range. We show that this observed drop is due to AGN downsizing rather than to an evolution in the accretion rates onto the supermassive black holes.We directly compare our broad-line AGN hard X-ray luminosity functions with the optical QSO luminosity functions and find that at the bright end they agree extremely well at all redshifts. However, the optical QSO luminosity functions do not probe faint enough to see the downturn in the broad-line AGN hard X-ray luminosity functions and even appear to be missing some sources at the lowest luminosities they probe.We find that broad-line AGNs dominate the number densities at the higher X-ray luminosities, while optically narrow AGNs dominate at the lower X-ray luminosities. We rule out galaxy dilution as a partial explanation for this effect by measuring the nuclear UV/optical properties of the Chandra sources using the Hubble Space Telescope Advanced Camera for Surveys GOODS-North data. The UV/optical nuclei of the optically narrow AGNs are much weaker than expected if the optically narrow AGNs were similar to the broad-line AGNs. We therefore postulate the need for a luminosity-dependent unified model. An alternative possibility is that the broad-line AGNs and the optically narrow AGNs are intrinsically different source populations. We cover both interpretations by constructing composite spectral energy distributions-including long-wavelength data from the mid-infrared to the submillimeterby spectral type and by X-ray luminosity. We use these spectral energy distributions to infer the bolometric corrections (from hard X-ray luminosities to bolometric luminosities) needed to map the accretion history.We determine the accreted supermassive black hole mass density for all spectral types and for broad-line AGNs alone, using the observed evolution of the hard X-ray energy density production rate and our inferred bolometric corrections. We find that only about one-half to one-quarter of the supermassive black hole mass ...

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“…There are several examples of composite objects showing both AGN and star formation activity, in the literature (e.g. Page et al 2001Page et al , 2004Alexander et al 2005), particularly at z ≈ 1, close to the peak of the AGN luminosity density in the Universe (e.g. Barger et al 2005;Hasinger et al 2005).…”

Section: Introductionmentioning

confidence: 99%

Observational evidence that positive and negative AGN feedback depends on galaxy mass and jet power

Kalfountzou

Stevens

Jarvis

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Several studies support the existence of a link between the AGN and star formation activity. Radio jets have been argued to be an ideal mechanism for direct interaction between the AGN and the host galaxy. A drawback of previous surveys of AGN is that they are fundamentally limited by the degeneracy between redshift and luminosity in flux-density limited samples. To overcome this limitation, we present far-infrared Herschel observations of 74 radio-loud quasars (RLQs), 72 radio-quiet quasars (RQQs) and 27 radio galaxies (RGs), selected at 0.9 < z < 1.1 which span over two decades in optical luminosity. By decoupling luminosity from evolutionary effects, we investigate how the star formation rate (SFR) depends on AGN luminosity, radio-loudness and orientation. We find that: 1) the SFR shows a weak correlation with the bolometric luminosity for all AGN sub-samples, 2) the RLQs show a SFR excess of about a factor of 1.4 compared to the RQQs, matched in terms of black hole mass and bolometric luminosity, suggesting that either positive radio-jet feedback or radio AGN triggering are linked to star-formation triggering and 3) RGs have lower SFRs by a factor of 2.5 than the RLQ sub-sample with the same BH mass and bolometric luminosity. We suggest that there is some jet power threshold at which radio-jet feedback switches from enhancing star formation (by compressing gas) to suppressing it (by ejecting gas). This threshold depends on both galaxy mass and jet power.

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Submillimeter Evidence for the Coeval Growth of Massive Black Holes and Galaxy Bulges

Cited by 82 publications

References 30 publications

The discovery of gas-rich, dusty starbursts in luminous reddened quasars atz∼ 2.5 with ALMA

The discovery of gas-rich, dusty starbursts in luminous reddened quasars atz∼ 2.5 with ALMA

The Cosmic Evolution of Hard X-Ray-selected Active Galactic Nuclei

Observational evidence that positive and negative AGN feedback depends on galaxy mass and jet power

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