Vincent L. Fish, Sheperd S. Doeleman, Avery E. Broderick, Abraham Loeb, and Alan E. E. Rogers. 2009. “
Detecting Changing Polarization Structures in Sagittarius A* with High Frequency VLBI.” The Astrophysical Journal, 706, Pp. 1353-1363.
Publisher's VersionAbstractSagittarius A* is the source of near infrared, X-ray, radio, and(sub)millimeter emission associated with the supermassive black hole atthe Galactic Center. In the submillimeter regime, Sgr A* exhibitstime-variable linear polarization on timescales corresponding to <10Schwarzschild radii of the presumed 4 × 106 Msun black hole. In previous work, we demonstrated thepotential for total-intensity (sub)millimeter-wavelength very longbaseline interferometry (VLBI) to detect time-variable—andperiodic—source structure changes in the Sgr A* black hole systemusing nonimaging analyses. Here, we extend this work to include fullpolarimetric VLBI observations. We simulate full-polarization(sub)millimeter VLBI data of Sgr A* using a hot spot model that isembedded within an accretion disk, with emphasis on nonimagingpolarimetric data products that are robust against calibration errors.Although the source-integrated linear polarization fraction in themodels is typically only a few percent, the linear polarization fractionon small angular scales can be much higher, enabling the detection ofchanges in the polarimetric structure of Sgr A* on a wide variety ofbaselines. The shortest baselines track the source-integrated linearpolarization fraction, while longer baselines are sensitive topolarization substructures that are beam-diluted by connected-elementinterferometry. The detection of periodic variability in sourcepolarization should not be significantly affected even if instrumentalpolarization terms cannot be calibrated out. As more antennas areincluded in the (sub)millimeter-VLBI array, observations with fullpolarization will provide important new diagnostics to help disentangleintrinsic source polarization from Faraday rotation effects in theaccretion and outflow region close to the black hole event horizon.
Sheperd S. Doeleman, Vincent L. Fish, Avery E. Broderick, Abraham Loeb, and Alan E. E. Rogers. 2009. “
Detecting Flaring Structures in Sagittarius A* with High-Frequency VLBI.” The Astrophysical Journal, 695, Pp. 59-74.
Publisher's VersionAbstractThe super-massive black hole candidate, Sagittarius A*, exhibitsvariability from radio to X-ray wavelengths on timescales thatcorrespond to <10 Schwarzschild radii. We survey the potential ofmillimeter wavelength very long baseline interferometry (VLBI) to detectand constrain time-variable structures that could give rise to suchvariations, focusing on a model in which an orbiting hot spot isembedded in an accretion disk. Nonimaging algorithms are developed thatuse interferometric closure quantities to test for periodicity, andapplied to an ensemble of hot spot models that sample a range ofparameter space. We find that structural periodicity in a wide range ofcases can be detected on most potential VLBI arrays using modern VLBIinstrumentation. Future enhancements of millimeter/submillimeter VLBIarrays including phased-array processors to aggregate VLBI stationcollecting area, increased bandwidth recording, and addition of new VLBIsites all significantly aid periodicity detection. The methods describedherein can be applied to other models of Sagittarius A*, including jetoutflows and magnetohydrodynamic accretion simulations.
Avery E. Broderick, Vincent L. Fish, Sheperd S. Doeleman, and Abraham Loeb. 2009. “
Estimating the Parameters of Sagittarius A*'s Accretion Flow Via Millimeter VLBI.” The Astrophysical Journal, 697, Pp. 45-54.
Publisher's VersionAbstractRecent millimeter-VLBI observations of Sagittarius A* (Sgr A*) have, forthe first time, directly probed distances comparable to the horizonscale of a black hole. This provides unprecedented access to theenvironment immediately around the horizon of an accreting black hole.We leverage both existing spectral and polarization measurements and ourpresent understanding of accretion theory to produce a suite of genericradiatively inefficient accretion flow (RIAF) models of Sgr A*, which wethen fit to these recent millimeter-VLBI observations. We find that ifthe accretion flow onto Sgr A* is well described by an RIAF model, theorientation and magnitude of the black hole's spin are constrained to atwo-dimensional surface in the spin, inclination, position angleparameter space. For each of these, we find the likeliest values andtheir 1σ and 2σ errors to be a = 0+0.4+0.7,θ = 50°^{+10° +30°}_{-10° -10°}, and ξ =-20°^{+31° +107°}_{-16° -29°}, when the resultingprobability distribution is marginalized over the others. The mostprobable combination is a = 0+0.2+0.4, θ =90°_{-40° -50°}, and ξ ={-14°}^{+7°+11°}_{-7° -11°}, though the uncertainties on these are verystrongly correlated, and high probability configurations exist for avariety of inclination angles above 30° and spins below 0.99.Nevertheless, this demonstrates the ability millimeter-VLBIobservations, even with only a few stations, to significantly constrainthe properties of Sgr A*.