Probing the Dark Matter Radial Profile in Lens Galaxies and the Size of X-Ray Emitting Region in Quasars With Microlensing

Jiménez-Vicente, J.; Mediavilla, E.; Kochanek, C. S.; Muñoz, J. A.

doi:10.1088/0004-637x/806/2/251

Cited by 39 publications

(38 citation statements)

References 50 publications

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“…This is because surface density of the disk increases with radius and the fraction of dissipation in the optically thin region drops, which is necessary to maintain the high temperature corona. This agrees with the constrains from both reflection and microlensing modeling of AGN coronae (Chartas et al 2009;Dai et al 2010;Reis & Miller 2013;Jiménez-Vicente et al 2015), which suggest that they are compact with roughly the same size as we find.…”

Section: Vertical Structure Of the Disksupporting

confidence: 91%

Global Radiation Magnetohydrodynamic Simulations of sub-Eddington Accretion Disks around Supermassive Black Holes

Jiang¹,

Blaes²,

Stone³

et al. 2019

ApJ

128

120

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We use global three dimensional radiation magneto-hydrodynamic simulations to study the properties of inner regions of accretion disks around a 5 × 10 8 M BH black hole with mass accretion rates reaching 7% and 20% of the Eddington value. This region of the disk is supported by magnetic pressure with surface density significantly smaller than the values predicted by the standard thin disk model but with a much larger disk scale height. The disks do not show any sign of thermal instability over many thermal time scales. More than half of the accretion is driven by radiation viscosity in the optically thin corona region for the lower accretion rate case, while accretion in the optically thick part of the disk is driven by the Maxwell and Reynolds stresses from MRI turbulence. Coronae with gas temperatures 10 8 K are generated only in the inner ≈ 10 gravitational radii in both simulations, being more compact in the higher accretion rate case. In contrast to the thin disk model, surface density increases with increasing mass accretion rate, which causes less dissipation in the optically thin region and a relatively weaker corona. The simulation results may explain the formation of X-ray coronae in Active Galactic Nuclei (AGNs), the compact size of such coronae, and the observed trend of optical to X-ray luminosity with Eddington ratio for many AGNs.

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Section: Vertical Structure Of the Disksupporting

confidence: 91%

Global Radiation Magnetohydrodynamic Simulations of sub-Eddington Accretion Disks around Supermassive Black Holes

Jiang¹,

Blaes²,

Stone³

et al. 2019

ApJ

128

120

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“…The impact of microlensing (and of intrinsic variability) looks similar for the shelf-like feature at ∼ λ1610, Fe II and III and significantly smaller for CIV. Comparing with microlensing data of the continuum we can say that the former features exhibit microlensing values similar to those typical of the optical continuum (|∆m opt | ∼ 0.3 mag, see Jiménez-Vicente et al 2015), and that, in extreme cases, some spectral features (FeIIIλλ2039-2113, for instance) can undergo microlensing magnifications close to those typical of the X-ray continuum (|∆m Xray | ∼ 1 mag, see Jiménez-Vicente et al 2015).…”

Section: Variability Taking As Reference the Cores Of The CIV Ciii]mentioning

confidence: 81%

Microlensing and Intrinsic Variability of the Broad Emission Lines of Lensed Quasars

Fian

Guerras

Mediavilla

et al. 2018

ApJ

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We study the broad emission lines (BELs) in a sample of 11 gravitationally lensed quasars with at least two epochs of observation to identify intrinsic variability and to disentangle it from microlensing. To improve our statistical significance and emphasize trends we also include 15 lens systems with single-epoch spectra. MgII and CIII] emission lines are only weakly affected by microlensing, but CIV shows strong microlensing in some cases, even for regions of the line core, presumably associated with small projected velocities. However, excluding the strongly microlensed cases, there is a strikingly good match, on average, between the red wings of the CIV and CIII] profiles. Analysis of these results supports the existence of two regions in the broad line region (BLR), one that is insensitive to microlensing (of size 50 light-days and kinematics not confined to a plane) and another that shows up only when it is magnified by microlensing (of size of a few light-days, comparable to the accretion disk). Both regions can contribute in different proportions to the emission lines of different species and, within each line profile, to different velocity bins, all of which complicates detailed studies of the BLR based on microlensing size estimates. The strength of the microlensing indicates that some spectral features that make up the pseudo-continuum, such as the shelf-like feature at λ1610 or several FeIII blends, may in part arise from an inner region of the accretion disk. In the case of FeII, microlensing is strong in some blends but not in others. This opens up interesting possibilities to study quasar accretion disk kinematics. Intrinsic variability seems to affect the same features prone to microlensing, with similar frequency and amplitude, but does not induce outstanding profile asymmetries. We measure intrinsic variability ( 20%) of the wings with respect to the cores in the CIV, CIII], and MgII lines consistent with reverberation mapping studies.

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“…Our study is based on the data and simulations from Jiménez-Vicente et al (2015a) in the optical range, and Jiménez-Vicente et al (2015b) in X-rays, who used microlensing magnification measurements from 24 gravitationally lensed quasars. In these studies an estimate of the abundance of microlenses (i.e.…”

Section: Dependence Of the Abundance Of Compact Objects On Their Massmentioning

confidence: 99%

“…The resulting PDFs, L(M, α|∆m ij ), are shown in Figure 1 for the optical microlensing measurements analyzed in Jiménez-Vicente et al (2015a) corresponding to a rest wavelength of ∼1736Å and in Figure 2 for the X-ray data discussed in Jiménez-Vicente et al (2015b). The first result (see Figure 1) is that the optical data strongly constrain the compact object masses to the range 0.05M (r toward larger values could push up the limits 3 The fit of the combined RM and microlensing data by Edelson et al (2015) for M BH ∼ 10 9 M , gives r s = 6.5 lt-day.…”

Section: Dependence Of the Abundance Of Compact Objects On Their Massmentioning

confidence: 99%

Limits on the Mass and Abundance of Primordial Black Holes from Quasar Gravitational Microlensing

Mediavilla

Jiménez-Vicente

Muñoz

et al. 2017

ApJL

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The idea that dark matter can be made of intermediate-mass primordial black holes in the 10M M 200M range has recently been reconsidered, particularly in the light of the detection of gravitational waves by the LIGO experiment. The existence of even a small fraction of dark matter in black holes should nevertheless result in noticeable quasar gravitational microlensing. Quasar microlensing is sensitive to any type of compact objects in the lens galaxy, to their abundance, and to their mass. We have analyzed optical and X-ray microlensing data from 24 gravitationally lensed quasars to estimate the abundance of compact objects in a very wide range of masses. We conclude that the fraction of mass in black holes or any type of compact objects is negligible outside of the 0.05M M 0.45M mass range and that it amounts to 20 ± 5% of the total matter, in agreement with the expected masses and abundances of the stellar component. Consequently, the existence of a significant population of intermediate-mass primordial black holes appears to be inconsistent with current microlensing observations. Therefore, primordial massive black holes are a very unlikely source of the gravitational radiation detected by LIGO.

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Probing the Dark Matter Radial Profile in Lens Galaxies and the Size of X-Ray Emitting Region in Quasars With Microlensing

Cited by 39 publications

References 50 publications

Global Radiation Magnetohydrodynamic Simulations of sub-Eddington Accretion Disks around Supermassive Black Holes

Global Radiation Magnetohydrodynamic Simulations of sub-Eddington Accretion Disks around Supermassive Black Holes

Microlensing and Intrinsic Variability of the Broad Emission Lines of Lensed Quasars

Limits on the Mass and Abundance of Primordial Black Holes from Quasar Gravitational Microlensing

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