Testing GR with Imaging of SMBHs, part deux
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1 Testing GR with Imaging of SMBHs, part deux Avery E Broderick Sheperd Doeleman (MIT Haystack) Vincent Fish (MIT Haystack) Alan Rogers (MIT Haystack) Dimitrios Psaltis (Arizona) Tim Johannsen (Arizona/UW-PI-CITA) Ue-Li Pen (CITA) Daniel James (Toronto) Agata Brancyzk (Toronto) Avi Loeb (Harvard) Ramesh Narayan (Harvard) Jonathan Bittner (Harvard) Mark Reid (Smithsonian) Mareki Honma (NAOJ)
2 Testing GR with Imaging of SMBHs, part deux Avery E Broderick Sheperd Doeleman (MIT Haystack) Vincent Fish (MIT Haystack) Alan Rogers (MIT Haystack) Dimitrios Psaltis (Arizona) Tim Johannsen (Arizona/UW-PI-CITA) Ue-Li Pen (CITA) Daniel James (Toronto) Agata Brancyzk (Toronto) Avi Loeb (Harvard) Ramesh Narayan (Harvard) Jonathan Bittner (Harvard) Mark Reid (Smithsonian) Mareki Honma (NAOJ)
3 The origin of the Shadow
4 Accretion Flows Near the Horizon
5 Practical Complications Opacity Optically thick Optically thin 1 mm Scattering Structure dominated Scattering dominated u-v coverage V vs. V (seeing)
6 Non-Imaging Techniques Model Input: Phenomenological (gaussian, annuli, etc.) I(, ) Physical ( -disk, RIAF, jet, etc.) V(u,v)
7 Measure of a Model Bayesian Information Criterion Akaike Information Criterion Relative significance Lies, damn lies and statistics! IC Conclusion 0 Negative 0-1 Not worth more than a bare mention 1-3 Positive 3-5 Strong 5-10 Very Strong >10 Conclusive
8 Toy Model: Symmetric Gaussian = as 2 /DoF=1.16 BIC=98.1 AIC=87.7 AEB, Fish, Doeleman & Loeb, ApJ, 735, 110 (2011)
9 Toy Model: Asymmetric Gaussian AEB, Fish, Doeleman & Loeb, ApJ, 735, 110 (2011) 2 /DoF=0.961 BIC=91.3 (-6.9) AIC=77.3 (-7.4)
10 A Physical Model: RIAFs (ADAFs) Thick, self-similar disk Keplerian beyond ISCO, ballistic inside Low Spin Aligned with BH spin (see Dexter et al. (2011,2012) & Gammie s talk) Sub-equipartition magnetic field Thermal and power-law electron components Model defined by n th, n nth, T e, and a Leverage existing spectra! Dexter & Fragile (2011) High Spin
11 A Physical Model: RIAFs AEB, Fish, Doeleman & Loeb, ApJ, 735, 110 (2011) 2 /DoF=0.830 BIC=82.9 (-8.4, -15.3) AIC=68.9 (-8.4, -15.8) Same number of parameters as asymmetric Gaussian models!
12 Inclination The Spin of Sgr A* Orientation a~ = deg. = deg. Our accretion model is wrong! Observations are easy to fit AEB, Fish, Doeleman & Loeb, ApJ, 735, 110 (2011) Non-accretion physics is important! Spin Magnitude
13 The future of Accretion Physics Hot/Thick Disk Cold/Thin Disk Do RIAFs make sense? (thick vs. thin, sub-keplerian) RIAF Keplerian Sub-Keplerian Are disks turbulent? (driven by the MHD instabilities, transporting angular momentum) Long timescale variability? (Lens-Thirring precession, etc.; see Dexter et al. & Gammie s talk) Dexter, Agol & Fragile (2009) Shcherbakov, Penna & McKinney (2011) RIAF SS433 Dexter & Fragile (2011) Dexter & Fragile (2011) Dexter & Fragile (2011)
14 Visibility Phases vs. (46/6/1) Reconstructed Image Phase information is crucial for image reconstruction!
15 Isotropic Prior <49% AEB, Fish, Doeleman & Loeb (2011)
16 mm-vlbi Visibility Amplitude Prior >97% RIAF Prediction! AEB, Fish, Doeleman & Loeb (2011)
17 The Future with Closure Phases V Only AEB, Fish, Doeleman & Loeb, ApJ, 738, 38 (2011)
18 The Future with Closure Phases V + Fish et al. (2011) AEB, Fish, Doeleman & Loeb, ApJ, 738, 38 (2011)
19 The Future with Closure Phases V & 12.6 o +-5 o on SMT-Hawaii-CARMA AEB, Fish, Doeleman & Loeb, ApJ, 738, 38 (2011)
20 The Future with Closure Phases V & Anticipated Precision on all triangles in an SMT-Hawaii-CARMA-APEX array AEB, Fish, Doeleman & Loeb, ApJ, 738, 38 (2011)
21 The Future with Closure Phases V & Anticipated Precision on all triangles in an SMT-Hawaii-CARMA-ALMA10 array AEB, Fish, Doeleman & Loeb, ApJ, 738, 38 (2011)
22 The Future with Closure Phases V & Anticipated Precision on all triangles in an SMT-Hawaii-CARMA-ALMA10-LMT array AEB, Fish, Doeleman & Loeb, ApJ, 738, 38 (2011)
23 Testing GR with Quasi-Kerr (see Psaltis & Johannsen) Hair!
24 RIAFs in Quasi-Kerr
25 Non-GRness Testing GR with quasi-kerr and surprisingly insensitive to robust direction Already best fit model clearly has nonzero! Most strongly measure the ISCO radius (>6M disfavored!) But not only! Spin Magnitude Johannsen, AEB, Psaltis & Loeb (2012) GR is safe, for now
26 Non-GRness Testing GR with quasi-kerr Bandwidth: 1GHz 4GHz Observatories SMT JCMT, Phased SMA Hawaii (LO) CARMA Phased CARMA (2 ind. dishes) (8) Phased ALMA (10) V only + Closure Phases Spin Magnitude Johannsen, AEB, Psaltis & Loeb (2012)
27 Probing Quantum BHs
28 Probing Quantum BHs Warning: Totally
29 Probing Quantum BHs Warning: Totally What are these?
30 Hints from the Information Paradox Black Hole Hokey Pokey Totally nuts!
31 What would we see? So just GR!
32 What would we see? Source Quantum Black Hole Screen Initial photon state Black hole state Scattered photon states in terms of scattering eigenstates.
33 Weak BH state measurements Normalized Image : Measurement of BH state from Bayes thm:
34 What would we see? Redux! Source Quantum Black Hole Screen Correlation between photons!
35 What would we see? 2 N Source Quantum Black Hole Screen Correlated Image: Updated BH state:
36 Collapsing BH wavefunctions! Measure of eigenimage difference! Projects exponentially with SNR 2, with most disparate images projected out first.
37 Dancing Black Holes?
38 Summary The EHT is already sensitive to strong lensing and we are measuring Sgr A* s spin Probes of the gastrophysics will improve dramatically with closure phases Beginning to look for non-gr hairs Potential probes of quantum gravity on the drawing board for only slightly nutty theories!
39
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