Microlensing Constraints on Quasar X-ray Emission Regions Xinyu Dai (Univ. of Oklahoma) Bin Chen (Univ. of Oklahoma) Chris Kochanek (Ohio State Univ.) George Chartas (College of Charleston) Chris Morgan (Naval Academy) Jeff Blackburne (Ohio State Univ.) Ana Mosquera (Ohio State Univ.) E. Baron (Univ. of Oklahoma) R. Kantowski (Univ. of Oklahoma) 2/21/2014 NAOC Colloquium, X. Dai 1
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Flux Density First Cosmological Lens Q0957+561 Wavelength Discovered in 1979 2/21/2014 NAOC Colloquium, X. Dai 3
Currently ~150 Quasar-Galaxy Lens 2/21/2014 NAOC Colloquium, X. Dai 4
Basic Observables Quasar image B Quasar image A Quasar image C Host galaxy Quasar image D Lens galaxy Hubble Image of Gravitational Lens RXJ1131-1231 (Morgan, Kochanek, Falco, and Dai 2006) 2/21/2014 NAOC Colloquium, X. Dai 5
Time Delay in PG1115+080 Measured in X-rays T(A1-A2)=0.16 days Time Chartas, Dai, Garmire 2004 2/21/2014 NAOC Colloquium, X. Dai 6 of 20
Schematic Plot of a Gravitational Lens D os Image D ls D ol Source y x y = D os D ol x - D ls a Point Mass a = 4GM Lens c 2 x 2/21/2014 NAOC Colloquium, X. Dai 7
Caustics and Critical Curves Source Plane 2/21/2014 NAOC Colloquium, X. Dai 8
Microlensing the Quasar Structure A typical quasar has an angular size of 1e-9 arcsec. 1 degree = 60 arcmin 1 arcmin = 60 arcsec Hubble Space Telescope 0.1 arcsec Quasi-Stellar Object Very Long Baseline Interferometry (VLBI) 0.1 milli-arcsec (1e-4 arcsec) 2/21/2014 NAOC Colloquium, X. Dai 9
But the smarter ones They quarrel and argue among each other 2/21/2014 NAOC Colloquium, X. Dai 10
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Magnification Pattern Produced by Stars C B A D 4GM 2 c 2/21/2014 NAOC Colloquium, X. Dai 12
How to use microlensing to measure the source size? Qualitative Approach Larger sources smooth the magnification pattern and have smaller microlensing variability. 2/21/2014 NAOC Colloquium, X. Dai 13
Intrinsic Variability Time delays A B = 12.0, A C = 9.6, A D = 87 days Days 2/21/2014 NAOC Colloquium, X. Dai 14
Removing intrinsic variability Microlensing Variability We observe this in almost all the systems we monitor 2/21/2014 NAOC Colloquium, X. Dai 15
X-ray Microlensing Is More Dramatic April 2004 Nov 2006 June 2000 Nov 2006 RXJ1131 and HE1104 by Chandra (Chartas et al. 2009) 2/21/2014 NAOC Colloquium, X. Dai 16
Examples of Magnification Patterns in the Monte-Carlo Simulations Image A * / =1 * / =0.5 * / =0.25 * / =0.125 Image C 2/21/2014 NAOC Colloquium, X. Dai 17
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Microlensing Model Setup A Monte-Carlo approach 10 step in stellar density 46X61 log grid for optical/x-ray size 5 steps in un-microlensed flux fraction 4 cases in treatment of global magnification offset 10^6 trials for each magnification pattern. 2/21/2014 NAOC Colloquium, X. Dai 20
A Solution in RXJ1131-1231 Dai et al. 2010, ApJ, 709, 278 2/21/2014 NAOC Colloquium, X. Dai 21
Probability Finally the Accretion Disk Size 100 AU 14 AU Size 2/21/2014 NAOC Colloquium, X. Dai 22
Challenge Optical Emission Models The classic AGN Model (Shakura & Sunyaev 1973) predicts Yielding 3-4 times smaller size than microlensing measurements Solutions: T µr -3/ 4 Flatter Temperature Profiles Inhomogeneous Disk 2/21/2014 NAOC Colloquium, X. Dai 23
Current Program Regular monitoring ~20 lenses in optical (B, V, R, I) bands. Sparse Hubble monitoring 1131 and 2237 in rest-frame ultra-violet in 2008-2013. Sparse Chandra X-ray monitoring 7 lenses in 2006-2014 (including a 680 ks large program in 2009-2010 and a 800 ks large program in 2012-2014). 2/21/2014 NAOC Colloquium, X. Dai 24
Chandra Monitoring of Gravitational Lenses 2/21/2014 NAOC Colloquium, X. Dai 25
X-ray and Optical Microlensing Variability Q2237, Chen et al. (2011, 2012); Mosquera et al. (2013) Time RXJ1131, Chartas et al. (2012) 2/21/2014 NAOC Colloquium, X. Dai 26
X-ray Microlensing Light Curves (Chen et al. 2012) 2/21/2014 NAOC Colloquium, X. Dai 27
Probability X-ray and Optical Emission Sizes QJ0158, Morgan et al. (2012) HE0435, Blackburne et al. (2011) HE1104, Blackburne et al. (2013) Size Q2237, Mosquera et al. (2013) 2/21/2014 NAOC Colloquium, X. Dai 28
X-ray and Optical Emission Sizes Excluded Excluded Excluded 2/21/2014 NAOC Colloquium, X. Dai 29
Energy Dependent X-Ray Microlensing Q2237 Chen et al. 2011, ApJL, 740, 34 Larger microlensing variability in hard band. Smaller hard source Temperature gradient in corona 2/21/2014 NAOC Colloquium, X. Dai 30
Energy Dependent X-ray Microlensing QJ0158, Morgan et al. (2012) Q2237, Mosquera et al. (2013) Hard X-ray Smaller in 2 cases (QJ0158, Q2237). Consistent in 2 cases (could due to S/N) Hard X-ray larger in one case (RXJ1131). 2/21/2014 NAOC Colloquium, X. Dai 31
Microlensing of Iron Lines (Chen et al. 2012a) Fe Lines are observed in almost all case. Sometime we see split of the line. 2/21/2014 NAOC Colloquium, X. Dai 32
Microlensing of Iron Lines Chen et al. (2012a) Iron line EWs in lensed quasars are larger than those of normal AGN of same luminosities. Iron line size is even smaller than X-ray continuum. 2/21/2014 NAOC Colloquium, X. Dai 33
Model of AGN Accretion Disk Hard X-ray Soft X-ray Iron line Accretion Disk Black Hole Cycle 14/15 800 ks program. Corona Calibrating all data from Cycle 1 to 15. 2/21/2014 NAOC Colloquium, X. Dai 34
X-ray Emission Under Strong Gravity Chen et al. 2013, ApJ, 762, 122. 2/21/2014 NAOC Colloquium, X. Dai 35
Testing Unification Models Predicted aox distribution between BALs and non-bals 2/21/2014 NAOC Colloquium, X. Dai 36
Compare with Observations BALQSOs, Morabito et al. 2013 Type I (red) and II (blue) AGN, Winter et al. 2010 2/21/2014 NAOC Colloquium, X. Dai 37
Polarization of the X-ray, EUV Continua In 0435, the EUV size is similar to the X- ray size 2/21/2014 NAOC Colloquium, X. Dai 38
Combining Kerr-Lensing and Microlensing 2/21/2014 NAOC Colloquium, X. Dai 39
D m m m Potential New Spin Measurement Technique 5 (A) spin a = 0 red : Kerr+Micro solid : 75 degree blue : Micro only dotted : 15 degree 4 3 2 1 3000 4000 5000 6000 6 5 4 3 2 1 0 (B) spin a = 0.998 3000 4000 5000 6000 1.5 1 0.5 0 0.5 1 1.5 (B) (A) [a = 0.998 VS a = 0] (75 deg) (15 deg) 3000 4000 5000 6000 Time (in pixel) 2/21/2014 NAOC Colloquium, X. Dai 40
Potential New Spin Measurement Technique 2/21/2014 NAOC Colloquium, X. Dai 41
Future Perspectives on Strong Lensing Data from Pan-Starrs, DES, Large Synoptic Survey Telescope (LSST) will be available in the next 6-7 years. E.g. LSST 20,000 square degrees Six bands Well-sampled light-curves E.g. LSST will detect 4,000 gravitational strong lenses: increase the current sample by 40 times. 2/21/2014 NAOC Colloquium, X. Dai 42
Microlensing Microlensing will still lead the angular resolution at least in the next 20 years in AGN studies. Increase the measurements from ~20 to 4,000. Dependence with mass, accretion rate, radio emission, and many other parameters. 2/21/2014 NAOC Colloquium, X. Dai 43
Lens Galaxy Light curves also provide time delay measurements. Image positions and time delays matter distribution Dark Gravitational lensing provides a unique tool to study the inter-stellar medium in the lens galaxy (Dai et al. 2003; Dai & Kochanek 2005; Dai et al. 2006; Dai & Kochanek 2009). ISM properties of 4,000 galaxies. 2/21/2014 NAOC Colloquium, X. Dai 44
X-ray Microlensing after Chandra Era Athena+: 2--2.5 m 2 effective area at 1 kev, 5--3 angular resolution 10,000 Quasar-Galaxy lenses detected by DES, LSST, WFIRST We will apply the technique to the large separation lens like SDSS1004. 2/21/2014 NAOC Colloquium, X. Dai 45