Calibration of ALMA as a phased array: ALMA observations during the 2017 VLBI campaign. (arXiv:1901.09987v1 [astro-ph.IM])
<a href="http://arxiv.org/find/astro-ph/1/au:+Goddi_C/0/1/0/all/0/1">Ciriaco Goddi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marti_Vidal_I/0/1/0/all/0/1">Ivan Marti-Vidal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Messias_H/0/1/0/all/0/1">Hugo Messias</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crew_G/0/1/0/all/0/1">Geoff Crew</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Herrero_Illana_R/0/1/0/all/0/1">Ruben Herrero-Illana</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Impellizzeri_V/0/1/0/all/0/1">Violette Impellizzeri</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rottmann_H/0/1/0/all/0/1">Helge Rottmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wagner_J/0/1/0/all/0/1">Jan Wagner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fomalont_E/0/1/0/all/0/1">Ed Fomalont</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matthews_L/0/1/0/all/0/1">Lynn D. Matthews</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Petry_D/0/1/0/all/0/1">Dirk Petry</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Phillips_N/0/1/0/all/0/1">Neil Phillips</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tilanus_R/0/1/0/all/0/1">Remo Tilanus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Villard_E/0/1/0/all/0/1">Eric Villard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Blackburn_L/0/1/0/all/0/1">Lindy Blackburn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Janssen_M/0/1/0/all/0/1">Michael Jan&#xdf;en</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wielgus_M/0/1/0/all/0/1">Maciek Wielgus</a>

We present a detailed description of the special procedures for calibration
and quality assurance of Atacama Large Millimeter/submillimeter Array (ALMA)
observations in Very Long Baseline Interferometry (VLBI) mode. These procedures
are required to turn the phased ALMA array into a fully calibrated VLBI
station. As an illustration of these methodologies, we present
full-polarization observations carried out with ALMA as a phased array at 3mm
(Band 3) and 1.3mm (Band 6) as part of Cycle-4. These are the first VLBI
science observations conducted with ALMA and were obtained during a 2017 VLBI
campaign in concert with other telescopes worldwide as part of the Global
mm-VLBI Array (GMVA, April 1-3) and the Event Horizon Telescope (EHT, April
5-11) in ALMA Bands 3 and 6, respectively.

We present a detailed description of the special procedures for calibration
and quality assurance of Atacama Large Millimeter/submillimeter Array (ALMA)
observations in Very Long Baseline Interferometry (VLBI) mode. These procedures
are required to turn the phased ALMA array into a fully calibrated VLBI
station. As an illustration of these methodologies, we present
full-polarization observations carried out with ALMA as a phased array at 3mm
(Band 3) and 1.3mm (Band 6) as part of Cycle-4. These are the first VLBI
science observations conducted with ALMA and were obtained during a 2017 VLBI
campaign in concert with other telescopes worldwide as part of the Global
mm-VLBI Array (GMVA, April 1-3) and the Event Horizon Telescope (EHT, April
5-11) in ALMA Bands 3 and 6, respectively.

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