Request of VLBA observation of a phase calibrator

There is an opportunity to request observations of a phase calibrator in the framework of the ongoing VLBA observing programs Low cost densification of the VLBA calibrator list (BP177) and Regular VLBA geodetic observations (RDV).

Densification of the VLBA calibrator list (BP177) Regular VLBA geodetic observations (RDV)

The schedule is generated automatically by the array operator in a filler mode during gaps between high priority projects. If your requested source will be visible during allotted time, it will be observed. Since BP177 is observed only during gaps of high priority projects and it competes with other filler projects, it is impossible to predict when and even whether your requested source will be observed. Sources at popular ranges of local sidereal time and at low declinations has less chances to be picked up. Scheduled manually on a fixed dates six times a year. Sources at all LST get the equal chance to be observed

Observed at 7–10 VLBA stations at [4.16, 4.64] and [7.36, 7.84] GHz simultaneously at 2048 Mbit/s in one scan 60 seconds long. Observed at VLBA, plus 5–10 non-VLBA stations at [2.23, 2.37] and [8.41, 8.90] GHz simultaneously at 256 Mbit/s in one or two scans 300 seconds long.

Placed in the queue within 1 hour of approval. Raw correlator output of projects observed under BP177 program will be accessible from VCS8 project web page within three weeks of observations. Within 3–7 days after the release of correlator data, the results will be posted at the same web page: source positions with a milliarcsecond level of accuracy, source images in FITS format, and calibrated visibilities. Scheduled within 2–4 months. Analyzed within 1–2 months upon observations. Results of analysis are source positions.
No proprietary period. Correlator output in FITS-IDI format is publicly available immediately. Correlator output is locked for 1 year. Publicly available after one year.

Processed by Leonid Petrov (Astrogeo Center) Processed by David Gordon (NASA GSFC)

If you need a phase calibrator for your observation, please first check the VLBI Calibrator Search Engine. If you did not find a suitable phase calibrator, please fill the form below and submit your request.

Your request will be directed to the NRAO Scheduling Officer. You will be notified whether you request has been approved, and if yes, for which program, BP177 or RDV.

J2000 epoch	Format: hh:mm:ss.s	J2000 epoch	Format: dd:mm:ss.s
*Target right ascension:		Target declination:
*1st calibrator right ascension:		*1st calibrator declination:
2nd calibrator right ascension:		2nd calibrator declination:
3rd calibrator right ascension:		3rd calibrator declination:
4th calibrator right ascension:		4th calibrator declination:
5th calibrator right ascension:		5th calibrator declination:
6th calibrator right ascension:		6th calibrator declination:
7th calibrator right ascension:		7th calibrator declination:
8th calibrator right ascension:		8th calibrator declination:
*Program preference:	no preference	BP177	RDV
*Your name:
*Your email:

*Short justification why observations of a calibrator are requested, for instance, reference to a code of an approved VLBI project.

I checked thoroughly http://astrogeo.org/calib/search.html but did not find there a suitable calibrator. Therefore, I request observations of additional candidate sources. I think there is a good chance they will be suitable for my project because ...
*Supporting argumentation why proposed calibrator(s) will be detected:

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This web page was prepared by Leonid Petrov ()
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Densification of the VLBA calibrator list (BP177)	Regular VLBA geodetic observations (RDV)
The schedule is generated automatically by the array operator in a filler mode during gaps between high priority projects. If your requested source will be visible during allotted time, it will be observed. Since BP177 is observed only during gaps of high priority projects and it competes with other filler projects, it is impossible to predict when and even whether your requested source will be observed. Sources at popular ranges of local sidereal time and at low declinations has less chances to be picked up.	Scheduled manually on a fixed dates six times a year. Sources at all LST get the equal chance to be observed
Observed at 7–10 VLBA stations at [4.16, 4.64] and [7.36, 7.84] GHz simultaneously at 2048 Mbit/s in one scan 60 seconds long.	Observed at VLBA, plus 5–10 non-VLBA stations at [2.23, 2.37] and [8.41, 8.90] GHz simultaneously at 256 Mbit/s in one or two scans 300 seconds long.
Placed in the queue within 1 hour of approval. Raw correlator output of projects observed under BP177 program will be accessible from VCS8 project web page within three weeks of observations. Within 3–7 days after the release of correlator data, the results will be posted at the same web page: source positions with a milliarcsecond level of accuracy, source images in FITS format, and calibrated visibilities.	Scheduled within 2–4 months. Analyzed within 1–2 months upon observations. Results of analysis are source positions.
No proprietary period. Correlator output in FITS-IDI format is publicly available immediately.	Correlator output is locked for 1 year. Publicly available after one year.
Processed by Leonid Petrov (Astrogeo Center)	Processed by David Gordon (NASA GSFC)