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Íàä?ñëàíî: Ï'ÿòíèöÿ, 8 Ñ?÷åíü 2016 ð 11:27:18
Òåìà: [IVSmail] GMVA: Call for Proposals (including ALMA)

CALL FOR PROPOSALS
GLOBAL 3mm VLBI ARRAY
Deadline: 1 February 2016


VLBI proposals for observing at 3mm wavelength using: the VLBA,
GBT*, EFFELSBERG, PICO VELETA, PLATEAU DE BURE, ONSALA,
METSAEHOVI, YEBES and KVN telescopes should be submitted by

1 FEBURARY 2016 (UT 21:00) ==========================
============================================================================= | | | ALL PROPOSALS SHOULD BE SUBMITTED USING THE NRAO PROPOSAL SUBMISSION TOOL | | | | my.nrao.edu | =============================================================================
New for semester 2016B, telescopes of the Korean VLBI Network (KVN) may be requested as part of the GMVA. In addition the LMT will continue to be offered for inclusion in the GMVA on a best effort basis. Both the KVN and the LMT can be selected using the "Other Stations" text field in the PST. (See also the section below regarding GMVA observations togethere with phased-ALMA in ALMA Cycle 4.)
Successful proposals will be considered for scheduling in Sept-Oct 2016 or in a later session.
Note that, after 2016 Session II, PLATEAU DE BURE will not be available in phased array mode; there are plans to later make a single antenna available for VLBI.
Proposers should be aware that at some GSTs the available time on the VLBA in the September/October 2016 session may be limited due to prior commitments (primarily in the Galactic Plane).
* The GBT may be included in GMVA observations if a sufficiently compelling justification is given in the proposal. Note, however, that although the GBT can participate in 3mm VLBI during the daytime, its sensitivity could be several times worse due to thermal deformations from solar heating.
In order to maximize the sensitivity for continuum observations the GMVA will record at the highest bitrate which telescope instrumentation and resources permit. All telescopes will record at 2 Gbps (except the KVN and PLATEAU DE BURE which will record in a compatible 1 Gbps mode).
For further details on proposing please consult the administrative and technical information hosted at the MPIfR: www3.mpifr-bonn.mpg.de/div/vlbi/globalmm

NEW: PARTICIPATION OF ALMA IN GMVA OBSERVATIONS IN ALMA CYCLE 4 ==========================================================
It is expected that phased ALMA will participate in some GMVA observations during ALMA Cycle 4: 1 Oct. 2016 - 30 Sept. 2017. (See almascience.eso.org/news/alma-cycle-4-pre-announcement) The number of ALMA dishes in the phased array is likely to be 30-40.
ALMA will not be in a configuration suitable for VLBI during GMVA Session II 2016. GMVA session dates for 2017 during Cycle 4 are not yet fixed but Session I, which is likely to be in March or April, should provide an opportunity for GMVA+ALMA observing. (GMVA Session II in 2017 is unlikely to overlap in Cycle 4 with ALMA in a configuration suitable for VLBI.)
** Any GMVA proposal requesting phased ALMA during Cycle 4 must be ** submitted via the NRAO PST at the 1 February 2016 deadline.
Proposers should:
- specify "ALMA" in the Other Stations text field in the PST
- select the default GMVA 3mm observing mode of 2 Gbps, dual polarization (although a different implementation of this will actually be used)
- specify the amount of time and GST range(s) needed for ALMA separately, either in Session Constraints or Comments, or in the Technical Justification.
A separate proposal to ALMA must also be submitted at the deadline for ALMA Cycle 4 proposals in April 2016. For this, all proposers (PI and Co-I's) must be registered ALMA users (see: www.almascience.org).

Restrictions on GMVA+ALMA proposals in Cycle 4

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- GMVA observations with ALMA will be limited to a fixed, continuum-only, mode, which will provide 2 Gbps on all baselines (except those to Plateau de Bure and the KVN).
- Due to the need to phase up on the target source, only sources with correlated flux densities > 0.5 Jy on intra-ALMA baselines out to 1 km may be proposed for observation. (This limit is set by the current state of testing of the phasing system.)
- In order to make a clean linear-to-circular transformation of ALMA recordings, any target source must be observed for a duration of at least 3h (breaks for calibrators permitted) to sample a range of parallactic angles.
- Large Programs (> 50 hours of observing time) are not permitted because phased ALMA is a non-standard mode.
- No long-term programs may be proposed, and no proposals will be carried over into the next cycle.
- There is a cap for VLBI of 5% of ALMA Cycle 4 observing time. As time for GMVA observations will thus be scarce, proposals should include a quantitative justification as to why ALMA is essential for the goals of the project.




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