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Event-horizon-scale structure in the supermassive black hole candidate at the Galactic Centre
TLDR
Observations at a wavelength of 1.3 mm set a size of microarcseconds on the intrinsic diameter of Sagittarius A*, suggesting that the bulk of Sgr A* emission may not be centred on the black hole, but arises in the surrounding accretion flow.
Jet-Launching Structure Resolved Near the Supermassive Black Hole in M87
TLDR
Radio interferometry observations of the elliptical galaxy M87 are reported that spatially resolve the base of the jet in this source, suggesting that the M87 jet is powered by an accretion disk in a prograde orbit around a spinning black hole.
Giant Molecular Clouds in M33. II. High-Resolution Observations
We present 12CO (J = 1 → 0) observations of 45 giant molecular clouds (GMCs) in M33 made with the BIMA array. The observations have a linear resolution of 20 pc, sufficient to measure the sizes of
First M87 Event Horizon Telescope Results. I. The Shadow of the Supermassive Black Hole
When surrounded by a transparent emission region, black holes are expected to reveal a dark shadow caused by gravitational light bending and photon capture at the event horizon. To image and study
95 GHz methanol masers near DR 21 and DR 21(OH)
Les observations radiointerferometriques BIMA des transitions 8 0 → 7 1 A + a 95 GHz de methanol et J = 2 → 1 a 98 GHz de CS, en direction des regions de formation stellaires DR 21 et DR 21(OH), sont
TADPOL: A 1.3 mm SURVEY OF DUST POLARIZATION IN STAR-FORMING CORES AND REGIONS
We present λ 1.3 mm Combined Array for Research in Millimeter-wave Astronomy observations of dust polarization toward 30 star-forming cores and eight star-forming regions from the TADPOL survey. We
Giant Molecular Clouds in M33. I. BIMA All-Disk Survey
We present the first interferometric 12CO (J = 1 → 0) map of the entire Hα disk of M33. The 13'' diameter synthesized beam corresponds to a linear resolution of 50 pc, sufficient to distinguish
A Parallactic Distance of 389 +24/-21 parsecs to the Orion Nebula Cluster from Very Long Baseline Array Observations
We determine the parallax and proper motion of the flaring, non-thermal radio star GMR A, a member of the Orion Nebula Cluster, using Very Long Baseline Array observations. Based on the parallax, we
Proplyds and massive disks in the Orion Nebula Cluster imaged with CARMA and SMA
We imaged a 2' × 2' region of the Orion Nebula Cluster (ONC) in 1.3 mm wavelength continuum emission with the recently commissioned Combined Array for Research in Millimeter Astronomy (CARMA) and
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