scholarly journals Star formation in luminous LoBAL quasars at 2.0 < z < 2.5

2020 ◽  
Vol 498 (1) ◽  
pp. 1469-1479
Author(s):  
Clare F Wethers ◽  
Jari Kotilainen ◽  
Malte Schramm ◽  
Andreas Schulze
Keyword(s):  
Black Hole ◽  
Star Formation ◽  
Black Hole Accretion ◽  
Broad Absorption Line ◽  
Evolutionary Phase ◽  
Imaging Receiver ◽  
Photometric Imaging ◽  
Galaxy Population ◽  
Black Hole Masses ◽  
Hole Accretion

ABSTRACT Low-ionization broad absorption line quasars (LoBALs) mark an important, yet poorly understood, population of quasars showing direct evidence for energetic mass outflows. We outline a sample of 12 luminous (Lbol &gt; 1046 ergs−1) LoBALs at 2.0 &lt; z &lt; 2.5 – a key epoch in both star formation and black hole accretion, which have been imaged as part of a targeted program with the Herschel Spectral and Photometric Imaging REceiver (SPIRE). We present K-band NOTCam spectra for three of these targets, calculating their spectroscopic redshifts, black hole masses, and bolometric luminosities, and increasing the total number of LoBAL targets in our sample with spectral information from five to eight. Based on FIR observations from Herschel SPIRE, we derive prolific star formation rates (SFRs) ranging 740–2380 M⊙ yr−1 for the detected targets, consistent with LoBALs existing in an evolutionary phase associated with starburst activity. Furthermore, an upper limit of &lt;440 M⊙ yr−1 is derived for the non-detections, meaning moderate-to-high SFRs cannot be ruled out, even among the undetected targets. Indeed, we detect an enhancement in both the SFRs and FIR fluxes of LoBALs compared to HiBAL and non-BAL quasars, further supporting the evolutionary LoBAL paradigm. Despite this enhancement in SFR, however, the environments of LoBALs appear entirely consistent with the general galaxy population at 2.0 &lt; z &lt; 2.5.

scholarly journals Probing black hole accretion tracks, scaling relations, and radiative efficiencies from stacked X-ray active galactic nuclei

2019 ◽  
Vol 493 (1) ◽  
pp. 1500-1511 ◽  
Author(s):  
Francesco Shankar ◽  
David H Weinberg ◽  
Christopher Marsden ◽  
Philip J Grylls ◽  
Mariangela Bernardi ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Selection Bias ◽  
Stellar Mass ◽  
Supermassive Black Holes ◽  
Independent Evidence ◽  
X Ray ◽  
Black Hole Accretion ◽  
Black Hole Masses ◽  
Hole Accretion

ABSTRACT The masses of supermassive black holes at the centres of local galaxies appear to be tightly correlated with the mass and velocity dispersions of their galactic hosts. However, the local Mbh–Mstar relation inferred from dynamically measured inactive black holes is up to an order-of-magnitude higher than some estimates from active black holes, and recent work suggests that this discrepancy arises from selection bias on the sample of dynamical black hole mass measurements. In this work, we combine X-ray measurements of the mean black hole accretion luminosity as a function of stellar mass and redshift with empirical models of galaxy stellar mass growth, integrating over time to predict the evolving Mbh–Mstar relation. The implied relation is nearly independent of redshift, indicating that stellar and black hole masses grow, on average, at similar rates. Matching the de-biased local Mbh–Mstar relation requires a mean radiative efficiency ε ≳ 0.15, in line with theoretical expectations for accretion on to spinning black holes. However, matching the ‘raw’ observed relation for inactive black holes requires ε ∼ 0.02, far below theoretical expectations. This result provides independent evidence for selection bias in dynamically estimated black hole masses, a conclusion that is robust to uncertainties in bolometric corrections, obscured active black hole fractions, and kinetic accretion efficiency. For our fiducial assumptions, they favour moderate-to-rapid spins of typical supermassive black holes, to achieve ε ∼ 0.12–0.20. Our approach has similarities to the classic Soltan analysis, but by using galaxy-based data instead of integrated quantities we are able to focus on regimes where observational uncertainties are minimized.

scholarly journals Tracing black hole and galaxy co-evolution in the Romulus simulations

2019 ◽  
Vol 489 (1) ◽  
pp. 802-819 ◽  
Author(s):  
Angelo Ricarte ◽  
Michael Tremmel ◽  
Priyamvada Natarajan ◽  
Thomas Quinn
Keyword(s):  
Black Hole ◽  
Star Formation ◽  
Star Formation Rate ◽  
Accretion Rate ◽  
Formation Rate ◽  
Star Forming ◽  
Black Hole Accretion ◽  
Black Hole Growth ◽  
Hole Growth ◽  
Hole Accretion

ABSTRACT We study the link between supermassive black hole growth and the stellar mass assembly of their host galaxies in the state-of-the-art Romulus suite of simulations. The cosmological simulations Romulus25 and RomulusC employ innovative recipes for the seeding, accretion, and dynamics of black holes in the field and cluster environments, respectively. We find that the black hole accretion rate traces the star formation rate among star-forming galaxies. This result holds for stellar masses between 108 and 1012 solar masses, with a very weak dependence on host halo mass or redshift. The inferred relation between accretion rate and star formation rate does not appear to depend on environment, as no difference is seen in the cluster/proto-cluster volume compared to the field. A model including the star formation rate, the black hole-to-stellar mass ratio, and the cold gas fraction can explain about 70 per cent of all variations in the black hole accretion rate among star-forming galaxies. Finally, bearing in mind the limited volume and resolution of these cosmological simulations, we find no evidence for a connection between black hole growth and galaxy mergers, on any time-scale and at any redshift. Black holes and their galaxies assemble in tandem in these simulations, regardless of the larger scale intergalactic environment, suggesting that black hole growth simply follows star formation on galactic scales.

scholarly journals Do Current X-Ray Observations Capture Most of the Black-hole Accretion at High Redshifts?

2021 ◽  
Vol 921 (2) ◽  
pp. 170
Author(s):  
Guang Yang ◽  
Vicente Estrada-Carpenter ◽  
Casey Papovich ◽  
Fabio Vito ◽  
Jonelle L. Walsh ◽  
...  
Keyword(s):  
Black Hole ◽  
Star Formation ◽  
Formation Rate ◽  
X Ray ◽  
Black Hole Accretion ◽  
Formation And Evolution ◽  
Predicted Values ◽  
Gas Accretion ◽  
Star Formation Histories ◽  
Hole Accretion

Abstract The cosmic black hole accretion density (BHAD) is critical for our understanding of the formation and evolution of supermassive black holes (BHs). However, at high redshifts (z > 3), X-ray observations report BHADs significantly (∼10 times) lower than those predicted by cosmological simulations. It is therefore paramount to constrain the high-z BHAD using independent methods other than direct X-ray detections. The recently established relation between star formation rate and BH accretion rate among bulge-dominated galaxies provides such a chance, as it enables an estimate of the BHAD from the star formation histories (SFHs) of lower-redshift objects. Using the CANDELS Lyα Emission At Reionization (CLEAR) survey, we model the SFHs for a sample of 108 bulge-dominated galaxies at z = 0.7–1.5, and further estimate the BHAD contributed by their high-z progenitors. The predicted BHAD at z ≈ 4–5 is consistent with the simulation-predicted values, but higher than the X-ray measurements (by ≈3–10 times at z = 4–5). Our result suggests that the current X-ray surveys could be missing many heavily obscured Compton-thick active galactic nuclei (AGNs) at high redshifts. However, this BHAD estimation assumes that the high-z progenitors of our z = 0.7–1.5 sample remain bulge-dominated where star formation is correlated with BH cold-gas accretion. Alternatively, our prediction could signify a stark decline in the fraction of bulges in high-z galaxies (with an associated drop in BH accretion). JWST and Origins will resolve the discrepancy between our predicted BHAD and the X-ray results by constraining Compton-thick AGN and bulge evolution at high redshifts.

scholarly journals The starburst – active galactic nuclei connection on nuclear scales in near by Seyfert galaxies

2013 ◽  
Vol 9 (S304) ◽  
pp. 345-346
Author(s):  
Pilar Esquej
Keyword(s):  
Black Hole ◽  
Star Formation ◽  
Formation Rate ◽  
Galactic Nuclei ◽  
Seyfert Galaxies ◽  
High Angular Resolution ◽  
Physical Relation ◽  
Black Hole Accretion ◽  
Star Formation Activity ◽  
Hole Accretion

AbstractSeveral works have shown that there is an empirical correlation between the star formation rate and the luminosity of the active galactic nucleus (and thus the black hole accretion rate, ṀBH) of Seyfert galaxies. This suggests a physical relation between the gas forming stars on kpc scales and the gas on sub-pc scales that is feeding the black hole. Simulations predict this relation and also that the correlation should be more prominent on smaller physical scales. We have compiled high angular resolution (0.4–0.8″) mid-infrared spectroscopy obtained with T-ReCS, VISIR, and Michelle of 29 Seyferts. We use the 11.3 μm PAH feature to probe the star formation activity in the inner ~65 pc, and its relation with the ṀBH on these physical scales.

scholarly journals Black hole accretion versus star formation rate: theory confronts observations

2015 ◽  
Vol 452 (1) ◽  
pp. L6-L10 ◽  
Author(s):  
Marta Volonteri ◽  
Pedro R. Capelo ◽  
Hagai Netzer ◽  
Jillian Bellovary ◽  
Massimo Dotti ◽  
...  
Keyword(s):  
Black Hole ◽  
Star Formation ◽  
Star Formation Rate ◽  
Formation Rate ◽  
Rate Theory ◽  
Black Hole Accretion ◽  
Hole Accretion
Sign in / Sign up

Export Citation Format

Share Document