AN ULTRA-LUMINOUS QUASAR AT
                    <i>z</i>
                    = 5.363 WITH A TEN BILLION SOLAR MASS BLACK HOLE AND A METAL-RICH DLA AT
                    <i>z</i>
                    ∼ 5

Wang, Feige; Wu, Xue-Bing; Fan, Xiaohui; Yang, Jinyi; Cai, Zheng; Yi, Weimin; Zuo, Wenping; Wang, Ran; McGreer, Ian D.; Ho, Luis C.; Kim, Minjin; Yang, Qian; Bian, Fuyan; Jiang, Linhua

doi:10.1088/2041-8205/807/1/l9

Cited by 34 publications

(15 citation statements)

References 51 publications

(100 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…If we also include less reliable M BH estimates (∆σ * > 20 km s −1 ), the range extends to log(M BH /M ) 10.3. Notwithstanding the uncertainties related to this latter high-mass end, we note that it is consistent with the highest masses seen in inactive SMBHs in the local Universe (e.g., McConnell et al 2011McConnell et al , 2012; the most massive SMBHs observed out to z ∼ 6 (e.g., Shemmer et al 2004;Wang et al 2015;Wu et al 2015) and perhaps the highest BH masses that could be observed as (radiatively efficient) accreting systems (Inayoshi & Haiman 2016;King 2016;Pacucci et al 2017). The Eddington ratios of our sources lie below the Eddington limit and in the range −2.2 log λ Edd −0.2, with a median log λ Edd = −1.3.…”

Section: Accretion Demographicssupporting

confidence: 83%

BAT AGN Spectroscopic Survey – XIII. The nature of the most luminous obscured AGN in the low-redshift universe

Bär

Trakhtenbrot

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present a multi wavelength analysis of 28 of the most luminous low-redshift narrow-line, ultra-hard X-ray selected active galactic nuclei (AGN) drawn from the 70 month Swift/BAT all-sky survey, with bolometric luminosities of log(L bol /erg s −1 ) 45.25. The broad goal of our study is to determine whether these objects have any distinctive properties, potentially setting them aside from lower-luminosity obscured AGN in the local Universe. Our analysis relies on the first data release of the BAT AGN Spectroscopic Survey (BASS/DR1) and on dedicated observations with the VLT, Palomar, and Keck observatories. We find that the vast majority of our sources agree with commonly used AGN selection criteria which are based on emission line ratios and on mid-infrared colours. Our AGN are predominantly hosted in massive galaxies (9.8 log[M * /M ] 11.7); based on visual inspection of archival optical images, they appear to be mostly ellipticals. Otherwise, they do not have distinctive properties. Their radio luminosities, determined from publicly available survey data, show a large spread of almost 4 orders of magnitude -much broader than what is found for lower X-ray luminosity obscured AGN in BASS. Moreover, our sample shows no preferred combination of black hole masses (M BH ) and/or Eddington ratio (λ Edd ), covering 7.5 log(M BH /M ) 10.3 and 0.01 λ Edd 1. Based on the distribution of our sources in the λ Edd − N H plane, we conclude that our sample is consistent with a scenario where the amount of obscuring material along the line of sight is determined by radiation pressure exerted by the AGN on the dusty circumnuclear gas.

show abstract

Section: Accretion Demographicssupporting

confidence: 83%

BAT AGN Spectroscopic Survey – XIII. The nature of the most luminous obscured AGN in the low-redshift universe

Bär

Trakhtenbrot

et al. 2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…Recently, large-area surveys for high-redshift quasars have identified a number of high-luminosity quasars with z>5 (Wang et al 2015(Wang et al , 2016Wu et al 2015). These quasars are detected in some of the dropout bands owing to their extreme brightness.…”

Section: Supplementary Quasar Selectionmentioning

confidence: 99%

Exploring Reionization-era Quasars. III. Discovery of 16 Quasars at 6.4 ≲ z ≲ 6.9 with DESI Legacy Imaging Surveys and the UKIRT Hemisphere Survey and Quasar Luminosity Function at z ∼ 6.7

Wang

Yang

Fan

et al. 2019

ApJ

Self Cite

154

136

View full text Add to dashboard Cite

This is the third paper in a series aimed at finding reionization-era quasars with the combination of DESI Legacy imaging Surveys (DELS), the Pan-STARRS1 (PS1) Survey, and near-infrared imaging surveys, such as the UKIRT Hemisphere Survey (UHS), as well as the Wide-field Infrared Survey Explorer (WISE) mid-infrared survey. In this paper, we describe the updated quasar candidate selection procedure, report the discovery of 16 quasars at 6.4 z6.9 from an area of ∼13,020 deg 2 , and present the quasar luminosity function (QLF) at z∼6.7. The measured QLF follows F µ-L L 1450 1450 2.35 () in the magnitude range −27.6<M 1450 <−25.5. We determine the quasar comoving spatial density at á ñ z =6.7 and M 1450 <−26.0 to be 0.39±0.11 Gpc −3 and find the exponential density evolution parameter to be k=−0.78±0.18 from z∼6 to z∼6.7, corresponding to a rapid decline by a factor of ∼6 per unit redshift toward earlier epochs. This indicates that the rapid decline of quasar spatial density at z>5 that was found by previous works continues to z>6, at a rate significantly faster than the average decline rate between z∼3 and 5. We measured quasar comoving emissivity at z∼6.7, which indicates that high-redshift quasars are highly unlikely to make a significant contribution to hydrogen reionization. The broad absorption line quasar fraction at z6.5 is measured to be 22%. In addition, we also report the discovery of six additional quasars at z∼6 in the Appendix.

show abstract

“…Based on a Figure 1. BH masses of high-redshift quasars (star symbols, from left to right: ULASJ1120+0641 at z = 7.1, J0306+1853 at z = 5.4, and SDSSJ0100+2802 at z = 6.3) in comparison with other z > 6 quasars (small grey ellipse), and the area populated by a large number of lower-redshift SDSS quasars (large grey ellipse; adopted from Wang et al 2015).…”

Section: Triggering Of Quasar Activitymentioning

confidence: 99%

Growth of Supermassive Black Holes, Galaxy Mergers and Supermassive Binary Black Holes

2015

View full text Add to dashboard Cite

The study of galaxy mergers and supermassive binary black holes (SMBBHs) is central to our understanding of the galaxy and black hole assembly and (co-)evolution at the epoch of structure formation and throughout cosmic history. Galaxy mergers are the sites of major accretion episodes, they power quasars, grow supermassive black holes (SMBHs), and drive SMBH-host scaling relations. The coalescing SMBBHs at their centers are the loudest sources of gravitational waves (GWs) in the universe, and the subsequent GW recoil has a variety of potential astrophysical implications which are still under exploration. Future GW astronomy will open a completely new window on structure formation and galaxy mergers, including the direct detection of coalescing SMBBHs, high-precision measurements of their masses and spins, and constraints on BH formation and evolution in the high-redshift universe.

show abstract

AN ULTRA-LUMINOUS QUASAR AT z = 5.363 WITH A TEN BILLION SOLAR MASS BLACK HOLE AND A METAL-RICH DLA AT z ∼ 5

Cited by 34 publications

References 51 publications

BAT AGN Spectroscopic Survey – XIII. The nature of the most luminous obscured AGN in the low-redshift universe

BAT AGN Spectroscopic Survey – XIII. The nature of the most luminous obscured AGN in the low-redshift universe

Exploring Reionization-era Quasars. III. Discovery of 16 Quasars at 6.4 ≲ z ≲ 6.9 with DESI Legacy Imaging Surveys and the UKIRT Hemisphere Survey and Quasar Luminosity Function at z ∼ 6.7

Growth of Supermassive Black Holes, Galaxy Mergers and Supermassive Binary Black Holes

Contact Info

Product

Resources

About