Paper

230 GHz VLBI observations of M87: event-horizon-scale structure at the enhanced very-high-energy \\(\\rm \\gamma\\)-ray state in 2012

Dexter, Matt, Bower, Geoffrey C, Doeleman, Sheperd S, Nakamura, Masanori, Crew, Geoffrey B, Johnson, Michael D, Kino, Motoki, Zensus, Anton, Akiyama, Kazunori, Yamaguchi, Paul, Young, Ken H, Nagai, Hiroshi, Gurwell, Mark, Marrone, Daniel P, Dexter, Jason, Fish, Vincent L, Asada, Keiichi, Blundell, Ray, Plambeck, Richard, Jonathan-León Tavares, Dzib, Sergio A, Weintroub, Jonathan, Krichbaum, Thomas P, Loinard, Laurent, Moran, James M, Nagar, Neil M, Brinkerink, Christiaan, Roy, Alan L, Broderick, Avery E, Titus, Michael, Primiani, Rurik A, Ru-Sen, Lu, Friberg, Per, Pradel, Nicolas, Algaba, Juan C, Honma, Mareki, Ortiz-Leon, Gisela, Rogers, Alan E E, Inoue, Makoto, Wagner, Jan, Tilanus, Remo P J, Ho, Paul T P, Ziurys, Lucy M, MacMahon, David, Hada, Kazuhiro, Cappallo, Roger, SooHoo, Jason, Freund, Robert

2015

Overview

We report on 230 GHz (1.3 mm) VLBI observations of M87 with the Event Horizon Telescope using antennas on Mauna Kea in Hawaii, Mt. Graham in Arizona and Cedar Flat in California. For the first time, we have acquired 230 GHz VLBI interferometric phase information on M87 through measurement of closure phase on the triangle of long baselines. Most of the measured closure phases are consistent with 0\\(^{\\circ}\\) as expected by physically-motivated models for 230 GHz structure such as jet models and accretion disk models. The brightness temperature of the event-horizon-scale structure is \\(\\sim 1 \\times 10^{10}\\) K derived from the compact flux density of \\(\\sim 1\\) Jy and the angular size of \\(\\sim 40 \\) \\(\\rm \\mu\\)as \\(\\sim\\) 5.5 \\(R_{{\\rm s}}\\), which is broadly consistent with the peak brightness of the radio cores at 1-86 GHz located within \\(\\sim 10^2\\) \\(R_{{\\rm s}}\\). Our observations occurred in the middle of an enhancement in very-high-energy (VHE) \\(\\rm \\gamma\\)-ray flux, presumably originating in the vicinity of the central black hole. Our measurements, combined with results of multi-wavelength observations, favor a scenario in which the VHE region has an extended size of \\(\\sim\\)20-60 \\(R_{{\\rm s}}\\).

• Publisher: Cornell University Library, arXiv.org
• Subject: Accretion disks / Black holes / Brightness temperature / Cedar / Elliptical galaxies / Event horizon / Flux density / Very long base interferometry