Using Microlensing to Probe Strong Gravity Near Supermassive Black Holes Interstellar: Kip Thorne and Double Negative visual-effects team Presented by: George Chartas
Chris Kochanek (OSU) Henric Krawczynski (WUSTL) Ana Mosquera (USNA) Christopher Morgan (USNA) Xinyu Dai (OU) Lukas Zalesky (CofC)
Outline Microlensing used for indirect mapping of disk and corona Monitoring of Lensed Quasars Constraints on inclination, ISCO, and spin Conclusions
Simulated magnification map of image B of RXJ 1131 (Dai et al. 2010) Microlensing map of QSO 2237+0305A image
Microlensing detected in 0.2 10 kev light-curves of RXJ1131 0.2-10 kev fluxes 0.2 10 kev Count Rate (cnts/s) 1.00 0.10 D B C A A(t) B(t + 0.7 days) C(t + 1.1 days ) D(t 91 days) B A C 1 arcsec D (a) 0.01 3000 4000 5000 6000 Julian Date 2450000 (days)
Fiducial Model X-ray Power-Law from compact corona Relativistically Blurred Reflection (line + continuum) Distant Reflection (line + continuum) Geometrically thin, optically thick accretion disk emitting primarily in UV/Optical
Dissecting an Accretion Disk with Microlensing We are performing multiwavelength monitoring of several quasars : RX J1131-1231 (z s = 0.658, z l = 0.295) Q J0158-4325 (z s = 1.29, z l = 0.317) SDSS0924+0219 (z s = 1.524, z l = 0.39) Q 2237+030 (z s = 1.60, z l = 0.04) HE 0435-1223 (z s = 1.689, z l = 0.46) PG 1115+080 (z s = 1.72, z l = 0.31) SDSS1004+4112 (z s = 1.734, z l = 0.68) QSO 1104-1805 (z s = 2.32, z l = 0.73) with the main scientific goal of measuring the emission structure near the black holes in the optical\uv and X-ray bands in order to test accretion disk models. X-ray monitoring observations are performed with Chandra Optical (B, R and I band) observations are made with the SMARTS Consortium 1.3m telescope in Chile.
Constraints on Corona Size from Microlensing 10 17 RXJ1131 Q0158 Q0924 PG1115 Q0435 HE1104 Q2237 10 16 X-ray R 1/2 (cm) 10 15 10 14 10 13 10 7 6GM BH /c 2 Innermost Stable Circular Orbit, a = 0 GM BH /c 2 Innermost Stable Circular Orbit, a = 1 10 8 10 9 M BH (M ) 10 10 X-ray half-light radii of quasars as determined from our microlensing analysis versus their black hole masses. Chartas+2016
Rate (cnts s 1 kev 1 ) 0.01 0.001 Evidence for Microlensing in all Images of RXJ1131 Shifted Fe Kα line in Spectrum of image C (1/21/2011) Double Chartas+ 2016 Observed Spectrum Image C of RXJ1131 Date: January 21, 2011 Chandra t exp = 24.62 ks 1/21/2011, Image C Fe Kα 0.5 1 2 5 Observed-Frame Energy (kev) 10 Energy Normalization (photons s 1 cm 2 ) 5 10 6 10 5 1.5 10 5 E 1,rest + Fe Kα E 2,rest 99% 90% 68% 2 3 4 5 6 7 8 Rest-Frame Energy (kev) B A C 1 arcsec + D (a) Significant 4 changes images of 38 line pointings centroids = 152 and spectra equivalent widths. 78 lines (>90%CL), 21 lines (>99%CL)
Evidence for Microlensing in all Images of RXJ1131 1/1/2007, Image B Shifted Fe Kα line in Spectrum of image B (1/1/2007) Chartas+ 2016 Rate (cnts s 1 kev 1 ) 0.01 0.001 Observed Spectrum Image B of RXJ1131 Date:January 1, 2007 Chandra texp = 4.7 ks Fe Kα Energy Normalization (photons s 1 cm 2 ) 2 10 5 3 10 5 4 10 5 5 10 5 10 5 + Fe Kα 0.5 1 2 5 Observed-Frame Energy (kev) 10 2 3 4 5 6 7 8 Rest-Frame Energy (kev) Significant spectral variability, including the centroid and Significant spectral variability, including the centroid and equivalent equivalent width width of the of the Fe-K! Fe Kα line. line
g-distribution of Line Centroids of RXJ1131 Number of Detected Fe Kα Lines 5 4 3 2 1 (a) RXJ1131 (A+B+C+D) > 99% Confidence g min = 0.61 g max = 1.15 Red/blueshift: 0.61-1.15 (99% CL) Number of Detected Fe Kα Lines 15 10 5 (b) RXJ1131 (A+B+C+D) > 90% Confidence g min = 0.59 g max = 1.29 Red/blueshift: 0.59-1.29 (90% CL) 0 2 4 6 8 10 Line Rest-Frame Energy (kev) Chartas et al. 2017
g-distribution of Line Centroids 3 2 QJ0158 > 90% Confidence QJ0158-4325 (z s = 1.29, z l = 0.317) 1 0.56 1.66 Number of Detected Fe Kα Lines 2 1 2 1 0 6 0.5 1.45 0.39 1.27 SDSS1004 > 90% Confidence HE0435 > 90% Confidence SDSS1004+4122 (z s = 1.734, z l = 0.68) HE 0435-1223 (z s = 1.689, z l = 0.46) Extremal shifts of the Fe Kα line energy in HE 0435 imply 3r g < r ISCO < 4r g spin ~ 0.7 5 Q2237 > 90% Confidence Q 2237+030 (z s = 1.60, z l = 0.04) 4 3 2 g max ~ 7 kev implies face on geometry 1 0 2 4 6 8 10 12 14 Fe Kα Line Rest-Frame Energy (kev)
Generalized Doppler Shift The observed energy of a photon emitted near the event horizon of supermassive black hole will be shifted with respect to the emitted restframe energy due to general relativistic and Doppler effects. g = E obs E emit = δ ΣΔ Α Where the Doppler shift is: 2 1 v φ δ =, where v φ is the azimuthal velocity 1 v φ cosθ c and θ c is the angle between our line-of-sight and the direction of motion of the emitting plasma. A, Σ, and Δ are defined as A = ( r 2 + a 2 ) 2 a 2 Δ sin 2 θ, Σ = r 2 + a 2 sin 2 θ, Δ = r 2 2r g r + a 2
g versus radius for RXJ1131 1.5 g (a) a=0.0998 gmax a=0.998 1.0 gmin gmax = 1.29 è gmin = 0.59 Assume gmin and gmax occur at same radius i > 76 risco < 8rg i = 64o a=0.0998 a=0.0998 (b) gmax a=0.998 1.0 gmin 0.5 a=0.998 i = 76o a=0.0998 0 i > 64 a=0.998 0.5 g gmax = 1.29 è 0 5 10 rem/rg 15 20
g versus radius for HE0435 E_obs/E_rest 0.0 0.5 1.0 1.5 2.0 g_max = 1.27 g_min = 0.39 0 5 10 15 20 R_em/R_g Extremal shifts of the Fe Kα line energy in HE 0435 imply 3r g < r ISCO < 4r g
Numerical Simulations of Microlensing Events Chartas+ 2016, 2017; Krawczynski+ 2017
g versus Equivalent Width of shifted Fe Kα Line Rest Frame Equivalent Width (kev) 10.00 1.00 0.10 Correlation of g vs. EW Kendall s τ = 0.3, P > 99.9% CL One possible explanation of this correlation is that blueshifted line emission is Doppler boosted resulting in the observed EW of the blueshifted lines being larger than the redshifted lines. 0.01 1 g 2 Supports microlensing interpretation!
Conclusions Redshifted and blueshifted Fe lines with EWs between 500-3000 ev are detected in 5 lensed quasars. We interpret these energy shifts as the result of microlensing of accretion disk emission within 20 r g of the black hole. For RXJ1131 we constrain i > 76 and r ISCO < 8.5r g. For HE 0435 we find 3r g < r ISCO < 4r g Several spectra show two shifted Fe lines (doubles). Our numerical simulations reproduce the observable results including the doubles. Our simulations show that the distribution of the energy separations of doubles is strongly dependent on spin. The next step is to correct for selection bias, fit the results from the numerical simulations to the Chandra data and explore the dependence of the results on corona properties.