Gravitational microlensing of active galactic nuclei dusty tori

Jovanović, P.; Baes, M.

doi:10.1111/j.1365-2966.2012.21611.x

Cited by 18 publications

(16 citation statements)

References 62 publications

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“…Our work differs in several respects from Stalevski et al (2012b) and complements their results. The main conceptual difference between the two studies relates to the model of the source.…”

Section: Existing Observations and Simulationssupporting

confidence: 64%

Mid-infrared microlensing of accretion disc and dusty torus in quasars: effects on flux ratio anomalies

Sluse¹,

Kishimoto

Anguita

et al. 2013

A&A

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Multiply-imaged quasars and active galactic nuclei (AGNs) observed in the mid-infrared (MIR) range are commonly assumed to be unaffected by the microlensing produced by the stars in their lensing galaxy. In this paper, we investigate the validity domain of this assumption. Indeed, that premise disregards microlensing of the accretion disc in the MIR range, and does not account for recent progress in our knowledge of the dusty torus, which has unveiled relatively compact dust emission. To simulate microlensing, we first built a simplified image of the quasar composed of (i) an accretion disc whose size is based on accretion disc theory, and (ii) a larger ring-like torus whose radius is guided by interferometric measurements in nearby AGNs. The mock quasars are created in the 10 44.2 −10 46 erg/s (unlensed) luminosity range, which is typical of known lensed quasars, and are then microlensed using an inverse ray-shooting code. We simulated the wavelength dependence of microlensing for different lensed image types and for various fractions of compact objects in the lens. This allows us to derive magnification probabilities as a function of wavelength, as well as to calculate the microlensing-induced deformation of the spectral energy distribution of the lensed images. We find that microlensing variations as large as 0.1 mag are very common at 11 µm (typically rest-frame 4 µm). The main signal comes from microlensing of the accretion disc, which may be significant even when the fraction of flux from the disc is as small as 5% of the total flux. We also show that the torus of sources with L bol 10 45 erg/s is expected to be noticeably microlensed. Microlensing may thus be used to get insight into the rest near-infrared inner structure of AGNs. Finally, we investigate whether microlensing in the mid-infrared can alter the so-called R cusp relation that links the fluxes of the lensed images triplet produced when the source lies close to a cusp macro-caustic. This relation is commonly used to identify massive (dark-matter) substructures in lensing galaxies. We find that significant deviations from R cusp may be expected, which means that microlensing can explain part of the flux ratio problem.

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“…Our work differs in several respects from Stalevski et al (2012b) and complements their results. The main conceptual difference between the two studies relates to the model of the source.…”

Section: Existing Observations and Simulationssupporting

confidence: 64%

Mid-infrared microlensing of accretion disc and dusty torus in quasars: effects on flux ratio anomalies

Sluse¹,

Kishimoto

Anguita

et al. 2013

A&A

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“…Unlike microlensing, where time variability can be used to isolate the effect, the effects of millilensing need to be disentangled from other physics that modify flux ratios. Mid-IR observations are ideal for this purpose because the effects of both microlensing and extinction are negligible or small (Stalevski et al 2012;Sluse et al 2013). The effect of microlensing of the dust torus on our observations can be estimated by comparing the average Einstein radius R E of stars in the lens galaxy to the dust sublimation radius R min .…”

Section: Discussionmentioning

confidence: 99%

“…The millilensing signal by substructures is best isolated at radio or rest-frame mid-infrared (mid-IR, ∼4-100 µm) wavelengths, where both extinction and microlensing effects from the lens galaxy are negligible (stars can only magnify sources smaller than ∼0.1 pc). Ideally, our observations (3.1 µm in the rest frame) would be at still longer wavelengths, but simulations indicate that microlensing effects should be 0.1 mag for our observations (Stalevski et al 2012;Sluse et al 2013). The mid-IR images are also unaffected by interstellar scattering, or scintillation, which can further perturb the radio images, although few lenses show the strong radio wavelength-dependent signatures expected from these effects (Kochanek & Dalal 2004).…”

Section: Introductionmentioning

confidence: 85%

Detection of Substructure in the Gravitationally Lensed Quasar Mg0414+0534 Using Mid-Infrared and Radio Vlbi Observations

MacLeod

Jones

Agol

et al. 2013

ApJ

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We present 11.2 µm observations of the gravitationally lensed, radio-loud z s = 2.64 quasar MG0414+0534, obtained using the Michelle camera on Gemini North. We find a flux ratio anomaly of A2/A1 = 0.93±0.02 for the quasar images A1 and A2. When combined with the 11.7 µm measurements from Minezaki et al. (2009), the A2/A1 flux ratio is nearly 5σ from the expected ratio for a model based on the two visible lens galaxies. The mid-IR flux ratio anomaly can be explained by a satellite (substructure), 0. ′′ 3 Northeast of image A2, as can the detailed VLBI structures of the jet produced by the quasar. When we combine the mid-IR flux ratios with high-resolution VLBI measurements, we find a bestfit mass between 10 6.2 and 10 7.5 M ⊙ inside the Einstein radius for a satellite substructure modeled as a singular isothermal sphere at the redshift of the main lens (z l = 0.96). We are unable to set an interesting limit on the mass to light ratio due to its proximity to the quasar image A2. While the observations used here were technically difficult, surveys of flux anomalies in gravitational lenses with the James W ebb Space T elescope will be simple, fast, and should well constrain the abundance of substructure in dark matter haloes.

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“…GALEX-FUV, MIPS 160 , SPIRE 500 ). The authors did so by performing a full 3D radiative transfer simulation to the EAGLE galaxies using the SKIRT code (Baes et al 2003(Baes et al , 2011Stalevski et al 2012;Camps & Baes 2015;Peest et al 2017;Stalevski et al 2016Stalevski et al , 2017Behrens et al 2018). In this section we use the artificial SEDs present in Camps et al (2018), in order to study how typical SFR/M ⋆ diagnostics affect the σ sSFR -M ⋆ relation.…”

Section: 3mentioning

confidence: 99%

An Evolving and Mass-dependent σsSFR–M_⋆ Relation for Galaxies

Katsianis

Zheng

González

et al. 2019

ApJ

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The scatter (σ sSFR ) of the specific star formation rates (sSFRs) of galaxies is a measure of the diversity in their star formation histories (SFHs) at a given mass. In this paper we employ the EAGLE simulations to study the dependence of the σ sSFR of galaxies on stellar mass (M ⋆ ) through the σ sSFR -M ⋆ relation in z ∼ 0 − 4. We find that the relation evolves with time, with the dispersion depending on both stellar mass and redshift. The models point to an evolving U-shape form for the σ sSFR -M ⋆ relation with the scatter being minimal at a characteristic mass M ⋆ of 10 9.5 M ⊙ and increasing both at lower and higher masses. This implication is that the diversity of SFHs increases towards both at the low-and high-mass ends. We find that active galactic nuclei feedback is important for increasing the σ sSFR for high mass objects. On the other hand, we suggest that SNe feedback increases the σ sSFR of galaxies at the low-mass end. We also find that excluding galaxies that have experienced recent mergers does not significantly affect the σ sSFR -M ⋆ relation. Furthermore, we employ the combination of the EAGLE simulations with the radiative transfer code SKIRT to evaluate the effect of SFR/stellar mass diagnostics in the σ sSFR -M ⋆ relation and find that the SFR/M ⋆ methodologies (e.g. SED fitting, UV+IR, UV+IRX-β) widely used in the literature to obtain intrinsic properties of galaxies have a large effect on the derived shape and normalization of the σ sSFR -M ⋆ relation.

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Gravitational microlensing of active galactic nuclei dusty tori

Cited by 18 publications

References 62 publications

Mid-infrared microlensing of accretion disc and dusty torus in quasars: effects on flux ratio anomalies

Mid-infrared microlensing of accretion disc and dusty torus in quasars: effects on flux ratio anomalies

Detection of Substructure in the Gravitationally Lensed Quasar Mg0414+0534 Using Mid-Infrared and Radio Vlbi Observations

An Evolving and Mass-dependent σsSFR–M_⋆ Relation for Galaxies

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Gravitational microlensing of active galactic nuclei dusty tori

Cited by 18 publications

References 62 publications

Mid-infrared microlensing of accretion disc and dusty torus in quasars: effects on flux ratio anomalies

Mid-infrared microlensing of accretion disc and dusty torus in quasars: effects on flux ratio anomalies

Detection of Substructure in the Gravitationally Lensed Quasar Mg0414+0534 Using Mid-Infrared and Radio Vlbi Observations

An Evolving and Mass-dependent σsSFR–M⋆ Relation for Galaxies

Contact Info

Product

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An Evolving and Mass-dependent σsSFR–M_⋆ Relation for Galaxies