Frequently Asked Questions

Observing with a certain cadence

My science objective requires that the observations be done with a specific cadence. How do I schedule these?

If your project requires that the observations are separated by a very specific amount of time (e.g., exactly 28 days), they should be scheduled as “fixed date” observing. We recommend that you contact the VLBA scheduling officer as soon as possible to arrange your observations. It is also a good idea to prepare your SCHED keyin files well in advance of the observations in order to avoid any delays.

Note that fixed date observations will take place regardless of weather conditions or other constraints. Therefore, there is a possibility that these observations will take place under less-than-optimal conditions.

It is recommended to schedule repeating observations with a flexible cadence, if the science goals allow for it. For example, instead of requiring an observation every 30 days, the request could be for every 30 +/- 3 days. This allows the observations to be scheduled dynamically and allows the schedulers to avoid poor weather conditions, antennas down for maintenance, and other conditions that can impact an observation. This type of flexibility is especially important for projects with B priority.

All cadence requirements should be included in the Dynamic Constraints section of the keyin file.

Polarization Products and Noise

How does the number of polarization products affect the noise?

Choices are single polarization (RR or LL), dual polarization (RR and LL), and full polarization (RR, RL, LR, and LL). If the emission is unpolarized, dual polarization gives twice the amount of independent data as single polarization does, and therefore decreases the rms noise by a factor of √2, as the sensitivity calculator will show. Full polarization does not improve this any further since RL and LR do not contribute to Stokes I.

Phase Referencing

When should I use phase referencing?

If there is any chance that your science target will not be bright enough for self calibration, you should use phase referencing.

Calibrators

How should I pick calibrators for my project?

The new VLBA Calibrator Search Tool will provide you with a list of potential calibration sources.  Another excellent search tool is the NASA VLBI Calibrator Search Tool.  It is generally a good idea to check for recent information on these sources to ensure that variability is not an issue at your desired observing frequency.  Also, check that the positions of the sources are known to an acceptable uncertainty for your project.  If you cannot find recent information calibrators at your desired frequency, you can request extra observing time to identify a good calibrator (see the Technical Justification section regarding whether targets can be self-calibrated).

What calibration sources do I need for polarimetric observations?

Polarimetric observations require scans on at least one leakage (D-term) calibrator, and at least one electric vector polarization angle (EVPA) calibrator (although 2 or 3 EVPA calibrators are recommended).  Several (at least 5) calibration scans should be made covering as large a range in parallactic angle as possible.  Also, at least one 2-minute scan should be scheduled on a very bright (~10 Jy) calibration source to permit the calibration of the RCP-LCP delays.  See the VLBA Polarimetry page in the VLBA OSS for more details.

Setup Restrictions

How do current observing setup restrictions impact my project?

The VLBA can only be tuned to certain allowed frequencies.  Check the SCHED example setup files for examples of how to tune the frequencies in your observation.  For details on creating setups, see Linford & Brisken (2020).

If a target is observed at multiple frequencies during a single observation, there will be increased calibration overhead since it takes a finite amount of time for the telescope to switch receivers. For phase reference observations, each target source scan at a certain frequency has to be bracketed by gain calibrator scans at that frequency.

Assistance with VLBA Observations

Can I get help calibrating and analyzing my VLBA observations

Users can always use the NRAO helpdesk for assistance with any issues related to any of the telescopes operated by NRAO.  VLBA staff are available to provide assistance with proposal preparation, schedule creation, and data reduction.

VLBA users are also encouraged to visit the NRAO in Socorro, NM, for face-to-face assistance with calibrating and reducing their observations.  Travel support is available. Please note that current NRAO policy requires all visitors to provide proof of vaccination against the COVID-19 virus.

There are also on-line data reduction tutorials.

 

CASA for VLBA Calibration

Can I use CASA to calibrate my VLBA observations?

CASA releases 5.3 and later contain tools for VLBI calibration. Starting with CASA releases 5.8 and 6.3, CASA contained the tools to process basic phase-referenced VLBA observations, including native ingestion of the gain curve and brightness temperature tables from the FITS-IDI file. NRAO still recommends that users calibrate their data with AIPS, especially for polarimetric and low frequency (<4 GHz) observations. VLBA staff continue to test the CASA VLBI tools, and development is ongoing.

A guide to calibrating basic phase-referenced VLBA observations with CASA can be found in VLBA Scientific Memo #38.

Tutorials for VLBI calibration in CASA were developed by Des Small (JIVE), Anita Richards (University of Manchester), and Jack Radcliffe (SARAO / University of Pretoria) for the Development in Africa with Radio Astronomy project. There are two VLBI data reduction tutorials: one for EVN continuum observations, and one for EVN spectral line observations.

The EVN Data Reduction Guide provides a more general overview of the calibration process and compares AIPS tasks with related CASA tools.

VLBA users attempting to calibrate their data with CASA versions earlier than 5.8 or 6.3 will also need a script to convert the VLBA gain curve table into a format usable in CASA. This script (gc2.py, written by Mark Kettenis) is available from JIVE’s CASA VLBI Github repository. NOTE: NRAO strongly recommends using the latest release of CASA to calibrate any data set.

Acronyms

AIPS = Astronomical Image Processing System
BBC = Baseband Channel
CASA = Common Astronomy Software Applications
DDC = Digital Downconverter
DDT  = Director’s Discretionary Time
EHT = Event Horizon Telescope
EVN = European VLBI Network
EVPA = Electric Vector Polarization Angle
GBT = Green Bank Telescope (officially, the Robert C. Byrd Green Bank Telescope)
GMVA = Global Millimeter VLBI Array
GO = General Observing
GST = Greenwich Sidereal Time
HSA = High Sensitivity Array
ICFR3 = International Coordinate Reference Frame 3
IEEE = Institute of Electrical and Electronics Engineers
IVS = International VLBI Service
JIVE = Joint Institute for VLBI in Europe
LCP = Left-hand Circularly Polarized
LST = Local Sidereal Time
NASA = National Aeronautics and Space Administration
NRAO = National Radio Astronomy Observatory
OPT = Observation Preparation Tool (for creating VLA schedules)
OSS = Observational Status Summary
PFB = Polyphase Filter Bank
PFT = Proposal Finder Tool
PST = Proposal Submission Tool
RCP = Right-hand Circularly Polarized
RDBE = ROACH Digital Backend
RFC = Radio Fundamental Catalog
RFI = Radio Frequency Interference
ROACH = Reconfigurable Open Architecture Computing Hardware
RSRO = Resident Shared Risk Observing
SEFD = System Equivalent Flux Density
SNR = Signal-to-Noise Ratio
SRO = Shared Risk Observing
SRP = Science Review Panel
TAC = Time Allocation Committee
TEC = Total Electron Content
TLA = Three Letter Acronym
TJ = Technical Justification
ToO = Target of Opportunity
UHF = Ultra High Frequency
VHF = Very High Frequency
VLA = Very Large Array (officially, the Karl G. Jansky Very Large Array)
VLBA = Very Long Baseline Array
VLBI = Very Long Baseline Interferometry

NRAO Bands: Letter Codes, Frequencies, and VLBA Receivers

VLBA Bands

Band
Designation		Frequency
Range		Associated
Receiver
P 312 - 342 MHz 90 cm
UHF 596 - 626 MHz 50 cm
L 1.35 - 1.75 GHz 20 cm
S 2.2 - 2.4 GHz 13 cm
C 3.9 - 7.9 GHz 6 cm
X 8.0 - 8.8 GHz 4 cm
Ku 12.0 - 15.4 GHz 2 cm
K 21.7 - 24.1 GHz 1 cm
Q 41.0 - 45.0 GHz 7 mm
W 80.0 - 90.0 GHz 3 mm

See the Frequency Band & Performance section of the VLBA OSS for more details.

Connect with NRAO

The National Radio Astronomy Observatory and Green Bank Observatory are facilities of the U.S. National Science Foundation operated under cooperative agreement by Associated Universities, Inc.

Founded in 1956, the NRAO provides state-of-the-art radio telescope facilities for use by the international scientific community. NRAO telescopes are open to all astronomers regardless of institutional or national affiliation. Observing time on NRAO telescopes is available on a competitive basis to qualified scientists after evaluation of research proposals on the basis of scientific merit, the capability of the instruments to do the work, and the availability of the telescope during the requested time. NRAO also provides both formal and informal programs in education and public outreach for teachers, students, the general public, and the media.

The National Science Foundation (NSF) is an independent federal agency created by Congress in 1950 "to promote the progress of science; to advance the national health, prosperity, and welfare; to secure the national defense..."

AUI collaborates with the scientific community and research sponsors to plan, build, and operate cutting-edge facilities. We cultivate excellence, deliver value, enhance education, and engage the public.