• Title: The size of the jet launching region in M87
• Authors: Jason Dexter, Jonathan C. McKinney and Eric Agol
• First Author’s Institutions: University of Washington and UC Berkeley
Messier 87 (M87) is a giant elliptical galaxy that is best known for its spectacular, 5000-ly-long jet (see Figure 1). The jet velocity is extremely relativistic, and it’s oriented at an angle relative to us such that we see the extended emission on the sky from the forward-pointing jet, but on large scales we don’t see the emission from the counter-jet due to relativistic effects.
In order to predict what a direct detection of a black hole would look like, the authors have to examine the region very close to the black hole, where the jet is first launched. The process of launching a jet from the accretion disk around a black hole is not well understood, and it’s only very recently that general relativistic magnetohydrodynamic (GRMHD) simulations of black holes have been able to reproduce this process. The authors make use of one such simulation by performing relativistic radiative transfer calculations on it and using the result to create models of the innermost region of the M87 nucleus. These are the first-ever radiative disk/jet models of M87 based on a GRMHD simulation of a black hole, and also the first images of any jet-launching region from a simulation.Results
The authors report several interesting results upon examining their M87 models.1) The images at 1.3mm (a target wavelength for submillimeter very long baseline interferometry, or sub-mm VLBI, which is our best bet for direct detection of black holes) that result from the models are crescents (see Figure 2). This is a result of the combination of several relativistic effects: gravitational lensing and Doppler beaming of the compact emission region.2) Immediately near the black hole, the jet emission we see is actually coming from the counter-jet — the exact opposite of what happens on large scales! This is due to, again, relativistic effects — in the area very close to the black hole, GR causes light paths going away from us to get bent back around toward us. The reason it’s not swamped by the emission from the forward jet is partly due to the same effect: that close to the black hole, the light from the forward jet gets bent away from us. We say that most of the forward jet falls into an area called the black hole’s “shadow.” Black hole shadows are probably familiar to you from pictures from black hole simulations — check out the images in Figure 2, for example. These shadows can be explained as a region that’s dark due to combined effects of light-bending and the fact that some photons are on paths that intersect the black hole, causing them to get trapped by the event horizon. And this brings us to…3) The black hole shadow — which is direct evidence for an event horizon — is of a size that could be observable with future sub-mm VLBI, using planned baselines between Hawaii and Chile.Thus, this work provides us with a concrete prediction for what we can expect to see in the innermost region of M87 with future observations. Based on these models, we can hope that direct detection of black holes — with M87 as one of the first targets — is right on the horizon! Event horizon, that is.