scholarly journals Probing Early Supermassive Black Hole Growth and Quasar Evolution with Near-infrared Spectroscopy of 37 Reionization-era Quasars at 6.3 < z ≤ 7.64

2021 ◽  
Vol 923 (2) ◽  
pp. 262
Author(s):  
Jinyi Yang ◽  
Feige Wang ◽  
Xiaohui Fan ◽  
Aaron J. Barth ◽  
Joseph F. Hennawi ◽  
...  
Keyword(s):  
Black Hole ◽  
Near Infrared ◽  
Small Sample ◽  
Emission Lines ◽  
Evolutionary Trend ◽  
Ratio Distribution ◽  
Accretion Rates ◽  
Black Hole Growth ◽  
Spectral Sample ◽  
Infrared Spectral

Abstract We report the results of near-infrared spectroscopic observations of 37 quasars in the redshift range 6.3 < z ≤ 7.64, including 32 quasars at z > 6.5, forming the largest quasar near-infrared spectral sample at this redshift. The spectra, taken with Keck, Gemini, VLT, and Magellan, allow investigations of central black hole mass and quasar rest-frame ultraviolet spectral properties. The black hole masses derived from the Mg ii emission lines are in the range (0.3–3.6) × 109 M ⊙, which requires massive seed black holes with masses ≳103–104 M ⊙, assuming Eddington accretion since z = 30. The Eddington ratio distribution peaks at λ Edd ∼ 0.8 and has a mean of 1.08, suggesting high accretion rates for these quasars. The C iv–Mg ii emission-line velocity differences in our sample show an increase of C iv blueshift toward higher redshift, but the evolutionary trend observed from this sample is weaker than the previous results from smaller samples at similar redshift. The Fe ii/Mg ii flux ratios derived for these quasars up to z = 7.6, compared with previous measurements at different redshifts, do not show any evidence of strong redshift evolution, suggesting metal-enriched environments in these quasars. Using this quasar sample, we create a quasar composite spectrum for z > 6.5 quasars and find no significant redshift evolution of quasar broad emission lines and continuum slope, except for a blueshift of the C iv line. Our sample yields a strong broad absorption line quasar fraction of ∼24%, higher than the fractions in lower-redshift quasar samples, although this could be affected by small sample statistics and selection effects.

Near infrared spectral and polarization imaging observation of coronal emission lines during the 2008 total solar eclipse

2009 ◽  
Vol 52 (11) ◽  
pp. 1794-1798 ◽  
Author(s):  
XingMing Bao ◽  
ZhiYong Zhang ◽  
Jian Deng ◽  
KeLiang Hu ◽  
WeiJia Xuan ◽  
...  
Keyword(s):  
Solar Eclipse ◽  
Near Infrared ◽  
Total Solar Eclipse ◽  
Emission Lines ◽  
Coronal Emission ◽  
Polarization Imaging ◽  
Imaging Observation ◽  
Infrared Spectral

scholarly journals Secularly powered outflows from AGNs: the dominance of non-merger driven supermassive black hole growth

2019 ◽  
Vol 489 (3) ◽  
pp. 4016-4031 ◽  
Author(s):  
R J Smethurst ◽  
B D Simmons ◽  
C J Lintott ◽  
J Shanahan
Keyword(s):  
Black Hole ◽  
Galaxy Evolution ◽  
Narrow Band ◽  
Narrow Band Imaging ◽  
Black Hole Accretion ◽  
Accretion Rates ◽  
The Galaxy ◽  
Black Hole Growth ◽  
Outflow Rate ◽  
Hole Growth

ABSTRACT Recent observations and simulations have revealed the dominance of secular processes over mergers in driving the growth of both supermassive black holes (SMBHs) and galaxy evolution. Here, we obtain narrow-band imaging of AGN powered outflows in a sample of 12 galaxies with disc-dominated morphologies, whose history is assumed to be merger-free. We detect outflows in 10/12 sources in narrow-band imaging of the $\mathrm{[O\, \small {III}] }$ $5007~\mathring{\rm A}$ emission using filters on the Shane-3m telescope. We calculate a mean outflow rate for these AGNs of $0.95\pm 0.14~\rm {M}_{\odot }~\rm {yr}^{-1}$. This exceeds the mean accretion rate of their SMBHs ($0.054\pm 0.039~\rm {M}_{\odot }~\rm {yr}^{-1}$) by a factor of 18. Assuming that the galaxy must provide at least enough material to power both the AGN and outflow, this gives a lower limit on the average inflow rate of $1.01\pm 0.14~\rm {M}_{\odot }~\rm {yr}^{-1}$, a rate which simulations show can be achieved by bars, spiral arms, and cold accretion. We compare our disc-dominated sample to a sample of nearby AGNs with merger dominated histories and show that the black hole accretion rates in our sample are five times higher (4.2σ) and the outflow rates are five times lower (2.6σ). We suggest that this could be a result of the geometry of the smooth, planar inflow in a secular dominated system, which is both spinning up the black hole to increase accretion efficiency and less affected by feedback from the outflow, than in a merger-driven system with chaotic quasi-spherical inflows. This work provides further evidence that secular processes are sufficient to fuel SMBH growth.

scholarly journals Correlation space of narrow-line Seyfert 1 galaxies

2012 ◽  
Vol 8 (S290) ◽  
pp. 349-350
Author(s):  
D. W. Xu ◽  
S. Komossa
Keyword(s):  
Black Hole ◽  
Optical Emission ◽  
Narrow Line ◽  
Close Link ◽  
Central Engine ◽  
Accretion Rates ◽  
Black Hole Growth ◽  
Accretion Physics ◽  
Correlation Space ◽  
Hole Growth

AbstractNarrow-line Seyfert 1 (NLS1) galaxies, as active galactic nuclei with low-mass black holes and high accretion rates, are important targets when addressing questions related to black hole growth and accretion physics. We have studied the correlations among the optical emission-line and continuum properties of a sample of NLS1 galaxies, in comparison with a sample of broad-line Seyfert 1 galaxies. We have shown that the density of the narrow-line region is a key component of Eigenvector 1 space. Density turned out to be as important as the Eddington ratio L/LEdd. This result therefore establishes a close link between central engine and host properties, and places new constraints on host - black hole co-evolution.

scholarly journals Accretion and outflow activity in proto-brown dwarfs

2020 ◽  
Author(s):  
B Riaz ◽  
J Bally
Keyword(s):  
Near Infrared ◽  
Ionic Composition ◽  
Brown Dwarfs ◽  
Evolutionary Trend ◽  
Infrared Study ◽  
Strong Emission ◽  
Accretion Rates ◽  
Similar Range ◽  
Low Mass ◽  
Extended Emission

Abstract We present a near-infrared study of accretion and outflow activity in 6 Class 0/I proto-brown dwarfs (proto-BDs) using VLT/SINFONI spectroscopy and spectro-imaging observations. The spectra show emission in several [Fe II] and H2 lines associated with jet/outflow activity, and in the accretion diagnostics of Pa β and Br γ lines. The peak velocities of the [Fe II] lines (&gt;100 km s−1) are higher than the H2 lines. The Class 0 proto-BDs show strong emission in the H2 lines but the [Fe II] lines are undetected, while the Class I objects show emission in both [Fe II] and H2 lines, suggesting an evolutionary trend in the jets from a molecular to an ionic composition. Extended emission with knots is seen in the [Fe II] and H2 spectro-images for 3 proto-BDs, while the rest show compact morphologies with a peak on-source. The accretion rates for the proto-BDs span the range of (2× 10−6 – 2× 10−8) M⊙ yr−1, while the mass loss rates are in the range of (4× 10−8 – 5× 10−9) M⊙ yr−1. These rates are within the range measured for low-mass protostars and higher than Class II brown dwarfs. We find a similar range in the jet efficiency for proto-BDs as measured in protostars. We have performed a study of the Brackett decrement from the Br 7-19 lines detected in the proto-BDs. The upper Brackett lines of Br 13–19 are only detected in the earlier stage systems. The ratios of the different Brackett lines with respect to the Brγ line intensity are consistent with the ratios expected from Case B recombination.

scholarly journals AGNs and Their Host Galaxies in the Local Universe: Two Mass-independent Eddington Ratio Distribution Functions Characterize Black Hole Growth

2017 ◽  
Vol 845 (2) ◽  
pp. 134 ◽  
Author(s):  
Anna K. Weigel ◽  
Kevin Schawinski ◽  
Neven Caplar ◽  
O. Ivy Wong ◽  
Ezequiel Treister ◽  
...  
Keyword(s):  
Black Hole ◽  
Distribution Functions ◽  
Host Galaxies ◽  
Local Universe ◽  
Ratio Distribution ◽  
Black Hole Growth ◽  
Hole Growth

scholarly journals Low-Mass AGN at High Accretion Rates

2009 ◽  
Vol 5 (S267) ◽  
pp. 338-338
Author(s):  
Dawei Xu ◽  
S. Komossa
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Active Galaxies ◽  
Narrow Line ◽  
Accretion Rates ◽  
Black Hole Growth ◽  
Low Mass ◽  
Hole Growth

AbstractGalaxies with low-mass black holes and high accretion rates, i.e., narrow-line Seyfert 1 (NLS1) galaxies, are important objects when addressing the issues of black hole growth and evolution, and of feeding and feedback. We have studied a sample of such objects, and find (1) that the locus of NLS1 galaxies on the MBH–σ plane appears to follow the relation of non-active galaxies after removing objects obviously dominated by outflows, (2) the presence of “blue outliers” that hint at extreme outflows as predicted by recent merger models, and (3) more subtle evidence for winds/outflows across the whole NLS1 population.

scholarly journals Discovery and analysis of a ULX nebula in NGC 3521

2019 ◽  
Vol 489 (1) ◽  
pp. 1249-1264 ◽  
Author(s):  
K M López ◽  
P G Jonker ◽  
M Heida ◽  
M A P Torres ◽  
T P Roberts ◽  
...  
Keyword(s):  
Near Infrared ◽  
Line Emission ◽  
Emission Lines ◽  
Spectral Signature ◽  
X Ray ◽  
Very Large Telescope ◽  
The Galaxy ◽  
Spatially Extended ◽  
Infrared Spectral ◽  
H Ii Region

ABSTRACT We present Very Large Telescope/X-shooter and Chandra X-ray observatory/ACIS observations of the ULX [SST2011] J110545.62 + 000016.2 in the galaxy NGC 3521. The source identified as a candidate near-infrared counterpart to the ULX in our previous study shows an emission line spectrum of numerous recombination and forbidden lines in the visible and near-infrared spectral regime. The emission from the candidate counterpart is spatially extended (∼34 pc) and appears to be connected with an adjacent H ii region, located ∼138 pc to the NE. The measured velocities of the emission lines confirm that both the candidate counterpart and H ii region reside in NGC 3521. The intensity ratios of the emission lines from the ULX counterpart show that the line emission originates from the combined effect of shock and photoionization of low metallicity (12  + log  (O/H)  = 8.19 ± 0.11) gas. Unfortunately, there is no identifiable spectral signature directly related to the photosphere of the mass-donor star in our spectrum. From the archival Chandra data, we derive the X-ray luminosity of the source in the 0.3–7 keV range to be (1.9 ± 0.8) × 1040 er g cm−2 s−1, almost a factor of four higher than what is previously reported.

scholarly journals Near-infrared emission lines trace the state-independent accretion disc wind of the black hole transient MAXI J1820+070

2020 ◽  
Vol 640 ◽  
pp. L3 ◽  
Author(s):  
J. Sánchez-Sierras ◽  
T. Muñoz-Darias
Keyword(s):  
Black Hole ◽  
Emission Line ◽  
Near Infrared ◽  
Nir Spectroscopy ◽  
Accretion Disc ◽  
Emission Lines ◽  
X Rays ◽  
Data Set ◽  
Soft State ◽  
Hard State

The black hole transient MAXI J1820+070 displayed optical P Cyg profiles and other wind-related emission line features during the hard state of its discovery outburst. We present near-infrared (NIR) spectroscopy covering the different accretion states of the system during this event. Our eight-epoch data set (VLT/X-shooter) reveals strong variability in the properties of the NIR emission lines. This includes absorption troughs and extended emission line wings with kinetic properties that are remarkably similar to those inferred from the wind signatures observed in optical emission lines, indicating that they most likely trace the same accretion disc wind. Unlike the optical features, these NIR signatures are not exclusive of the hard state, as they are also witnessed across the soft state with similar observational properties. This supports the presence of a relatively steady outflow during the entire outburst of the system, and it represents the first detection of an accretion disc wind in a black hole soft state at energies other than X-rays. We discuss the visibility of the wind as a function of the spectral band and the potential of NIR spectroscopy for wind studies, in particular during luminous accretion phases.

scholarly journals Galaxy mergers in eagle do not induce a significant amount of black hole growth yet do increase the rate of luminous AGN

2020 ◽  
Vol 494 (4) ◽  
pp. 5713-5733 ◽  
Author(s):  
Stuart McAlpine ◽  
Chris M Harrison ◽  
David J Rosario ◽  
David M Alexander ◽  
Sara L Ellison ◽  
...  
Keyword(s):  
Black Hole ◽  
Galaxy Mergers ◽  
Lower Mass ◽  
Massive Galaxies ◽  
Isolated Galaxies ◽  
Accretion Rates ◽  
Black Hole Growth ◽  
Hole Growth ◽  
Minor Mergers ◽  
Galaxy Population

ABSTRACT We investigate the connection between galaxy–galaxy mergers and enhanced black hole (BH) growth using the cosmological hydrodynamical eagle simulation. We do this via three methods of analysis, investigating: the merger fraction of AGN, the AGN fraction of merging systems, and the AGN fraction of galaxies with close companions. In each case, we find an increased abundance of AGN within merging systems relative to control samples of inactive or isolated galaxies (by up to a factor of ≈3 depending on the analysis method used), confirming that mergers are enhancing BH accretion rates for at least a subset of the galaxy population. The greatest excess of AGN triggered via a merger are found in lower mass (M* ∼ 1010 M⊙) gas rich (fgas &gt; 0.2) central galaxies with lower mass BHs (MBH ∼ 107 M⊙) at lower redshifts (z &lt; 1). We find no enhancement of AGN triggered via mergers in more massive galaxies (M* ≳ 1011 M⊙). The enhancement of AGN is not uniform throughout the phases of a merger, and instead peaks within the early remnants of merging systems (typically lagging ≈300 Myr post-coalescence of the two galaxies at z = 0.5). We argue that neither major ($M_{\mathrm{*,1}} / M_{\mathrm{*,2}} \ge \frac{1}{4}$) nor minor mergers ($\frac{1}{10} \lt M_{\mathrm{*,1}} / M_{\mathrm{*,2}} \lt \frac{1}{4}$) are statistically relevant for enhancing BH masses globally. Whilst at all redshifts the galaxies experiencing a merger have accretion rates that are on average 2–3 times that of isolated galaxies, the majority of mass that is accreted on to BHs occurs outside the periods of a merger. We compute that on average no more than 15 per cent of a BHs final day mass comes from the enhanced accretion rates triggered via a merger.

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