VLBI proposals for observing at 3mm wavelength (86 GHz) using: the VLBA, GBT*, APEX, EFFELSBERG, PICO VELETA, NOEMA, ONSALA,METSAEHOVI, YEBES, and KVN telescopes should be submitted by 30 JULY 2025 (UT 21:00)
GMVA proposals submitted by the 2025 July 30 deadline will be considered for scheduling in 2026 Session I (April 16 – 21), Session II (September 24 – 29), or later sessions.
Proposals requesting phased ALMA participation will not be considered for this deadline (July 30, 2025; semester 2026A). Please wait for future calls including ALMA.
- ALL PROPOSALS SHOULD BE SUBMITTED USING THE NRAO PROPOSAL SUBMISSION TOOL (PST).
- Complete information on the GMVA is available at the GMVA website. Ongoing special considerations are documented in the GMVA section of the VLBA Observational Status Summary; new features and/or special cases are cited here.
- The use of the PST requires registration by all proposers, including co-investigators, in the NRAO User Database.
- The GMVA will record at the highest bitrate which instrumentation and resources permit. All telescopes will record at 4096 Mbps.
- All data will be correlated at the Bonn DiFX software correlator.
*The GBT may be requested for GMVA observations, provided that the proposal contains a sufficiently compelling justification. Due to new partnership arrangements, observing time is reduced, so please consider whether the telescope is absolutely necessary for your purpose.
The Atacama Pathfinder Experiment (APEX) telescope, the KVN telescope or the Greenland Telescope (GLT) must be specified by entering “APEX”, “KVN” or “GLT” as “other” entries in the PST.
You may propose 7mm (43 GHz) VLBA observations during calibration or pointing gaps in 3mm GMVA sessions. Additional antennas such as ‘Noto’ may participate. To request Hancock (HN) or Saint Croix (SC), which are not standard GMVA antennas, list them as ‘Other’ in the PST.
For further details on proposing, please consult the administrative and technical information hosted at the MPIfR.
Justification should be provided for observing faint VLBI targets at 86 GHz. To justify detection thresholds for sources with a total flux of less than 100 mJy, please use the GMVA sensitivity calculator or the EVN calculator.
Best regards,
Eduardo Ros European GMVA Scheduler