The Transient Universe: AY 250 Spring 2007 Sagittarius A* Geoff Bower.

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Presentation transcript:

The Transient Universe: AY 250 Spring 2007 Sagittarius A* Geoff Bower

The Transient Universe: AY 250 Spring 2007 Why Study Sgr A*? “Unique Laboratory for Astrophysics” –We can get closer to this black hole than any other 1 mas ~ 100 R_g –Unprecedented multi-wavelength information Winds; young stars; stellar remnants; molecular, atomic, ionized gas Stellar proper motions, radial velocities (Genzel, Ghez) NIR and X-ray emission (Genzel, Ghez, Baganoff, etc.) –Template for other AGN and compact objects –Fundamental physics exploration

The Transient Universe: AY 250 Spring 2007 What We Don’t Know Yet Why is Sgr A* so underluminous? –L ~ L Edd Models degenerate –Inflow, outflow, jets, nonthermal emission How does Sgr A* relate to other AGN? Fundamental gravity Narayan & Quataert 2005

The Transient Universe: AY 250 Spring 2007 Stellar Orbits: M BH ~ 3 x 10 6 M sun Ghez 2004

The Transient Universe: AY 250 Spring 2007

Sgr A East & West 6cm VLA (Morris & Yusef-Zadeh)

The Transient Universe: AY 250 Spring mm VLBA (Bower & Backer 1998) What We See What We Want to See

The Transient Universe: AY 250 Spring 2007 Flux Density Variations: The Dog Wags its Tail

The Transient Universe: AY 250 Spring 2007 Radio Monitoring of Flux Density Macquart & Bower 2005

The Transient Universe: AY 250 Spring 2007 Power Spectral Analysis Zhao et al 1999Macquart & Bower 2005

The Transient Universe: AY 250 Spring 2007 Scintillation Drives Variability

The Transient Universe: AY 250 Spring 2007 X-Ray Flares Baganoff et al 2001

The Transient Universe: AY 250 Spring 2007 NIR Flares Genzel et al 2003

The Transient Universe: AY 250 Spring 2007 Simultaneous Radio/X-ray Flare 160x X-ray Flare

The Transient Universe: AY 250 Spring 2007 Simultaneous NIR/X-ray Flare Eckart et al 2004

The Transient Universe: AY 250 Spring 2007 Simultaneous NIR/X-ray Flare Eckart et al 2004 Small mm flare

The Transient Universe: AY 250 Spring 2007 July 2004 Radio/NIR/X-ray Flare

The Transient Universe: AY 250 Spring 2007 RadioSubmm InfraredX-ray nu Fnu Frequency Quiescent Flaring The Dog Wags Its Tail Particle heating Not Particle Injection

The Transient Universe: AY 250 Spring 2007 X-Ray Fluoresence No internal X-ray source Sgr A* or XRB origin 400 y ago 10^39 erg s^-1 Revnivtsev et al 2004 Hard X-rays 6.4 keV Fe Fluorescent line

The Transient Universe: AY 250 Spring 2007 X-Ray Fluoresence Changes in X-ray morphology in molecular cloud 14 pc in projection from Sgr A*  L~10^38 erg s^-1 –60 years ago –2-3 year duration Muno et al 2007

The Transient Universe: AY 250 Spring 2007 Linear Polarization: Unique Probe of Accretion and Jet Physics

The Transient Universe: AY 250 Spring 2007 No Linear Polarization

The Transient Universe: AY 250 Spring 2007 JCMT Discovery of Sgr A* Linear Polarization Detected at 150 – 690 GHz 850 um = 345 GHz 3.6 cm gray scale 90 deg angle flip Dust confusion an issue

The Transient Universe: AY 250 Spring 2007 BIMA Confirmation of Sgr A* Polarization

The Transient Universe: AY 250 Spring 2007 B N e RM < 2 x Schwarzschild radii 10,000 Schwarzschild radii Polarized radiation propagates through dense, magnetized accretion region

The Transient Universe: AY 250 Spring 2007 MHD Simulations of Accretion Proga & Begelman 2003

The Transient Universe: AY 250 Spring 2007 Polarization Variability

The Transient Universe: AY 250 Spring 2007

Motion Around the Black Hole? Submm polarization 4 hours 13 Schwarzschild radii Marrone et al 2006

The Transient Universe: AY 250 Spring 2007 NIR Interferometry Paumard et al 2005 Microarcsec

The Transient Universe: AY 250 Spring 2007 Approaching the Event Horizon

The Transient Universe: AY 250 Spring 2007 The Black Hole Shadow Falcke, Melia & Agol 2000 Bardeen 1973

The Transient Universe: AY 250 Spring 2007 Event Horizon Shadow Shadow with radius 5 R_g must exist –Optically thin emission required Sgr A* is the most realistic candidate Black HoleShadow Diameter Sgr A*66 μ arcsec M8736 NGC Cen A10 SS

The Transient Universe: AY 250 Spring 2007 Angular Sizes 1.3 mm0.8 mm Intrinsic>66 μ arcsec>66 Scattering20 x 106 x 3 Beam (8000 km) 3020

The Transient Universe: AY 250 Spring 2007 Other Effects/Related Experiments Effects of black hole spin Polarization Imaging Phase-referenced imaging –Orbital period (Rs) ~ 20 minutes –How stable is the image? Temporal coherence due to lensing Broderick & Blandford 2004 Q V

The Transient Universe: AY 250 Spring 2007 Total Intensity Submm VLBI

The Transient Universe: AY 250 Spring 2007 Polarization Submm VLBI

The Transient Universe: AY 250 Spring 2007 Technical Requirements Global array High frequency receivers & antenna performance –230/350 GHz > Gigabit recording Phase stability –Water vapor radiometers Time standards Array Phasing –Correlator options Astrometry/Phase referenced observations eVLBI