N.B.: As of January 2021, The MOJAVE team has paused all data reduction activities while we await NRAO's resolution of a systematic flux density scaling error that has been affecting all VLBA 15 GHz observations after a date that lies between 2019 April 16 and 2019 May 16.
accordance with NRAO's policy for data access to large
proposals, we make all of our data publicly available
within approximately eight weeks of observation. This
includes the final polarized and total intensity images,
as well as the calibrated visibility data. We
of our observing and scheduling
strategies, as well as a sample calibration
. Below we summarize the status of our
individual observing epochs, each of which spans 24
From Aug 1 2019 to Aug 1 2021 (BL273), we are
observing (at 4096 Mbps) 25 targets monthly at 15, 24, and
43 GHz. We also regularly observe a pool of 63 AGN at 15
GHz (2048 Mbps).
From May 2018 (BL229AO) to Aug 2019,
observations at 43 GHz were included for a small number of
targets which are exceedingly compact at 15 GHz, for the
purposes of measuring their apparent jet speeds.
Beginning in Sept. 2016 (BL229), 30 targets are selected
for each 2048 Mbps, 24h long session from a set of
accelerating jets, as well as 50 new target AGN from the
Fermi LAT-monitored list, the 2FHL and 3FGL Fermi
catalogs, and the RoboPol sample. For more information see
the 'What's New' section of the MOJAVE
The BL178 and BL193 observations, from Sept. 2013 - Dec.
2016 had 22 AGNs in each 2048 Mbps, 24h long session.
The Fermi-era observations beginning in 2007 (BL137R
through BL178BI) were carried out at 15.3 GHz only, with
30 AGNs being observed in each 24 hour session.
The MOJAVE observations in 2006 (BL137A-L) followed the
same strategy, but with an extended sample (192 AGNs), and
polarimetric observations at 8.1, 8.4, 12.1 and 15.3 GHz.
The scan lengths were chosen to achieve roughly the same
image rms at each frequency.
The MOJAVE-I observations (BL111, BL123; 2002-2006) were
optimized for obtaining suitably high-dynamic range,
full-polarization images of bright AGNs at reasonable
intervals for measuring superluminal motion.
For the purposes of polarization calibration, we maintain
the following lists: