ATNF Telescope Status for 2022OCT

All ATNF Telescope Applications for 2022OCT must be submitted using OPAL.

For 2022OCT, we are using a new version of the OPAL system. Users are encouraged to report any issues via email (atnf-opal@csiro.au). The file format for cover sheets and observations tables has changed. Files from previous semesters (in OXML format) should be re-loaded into the OPAL editors, carefully re-checked and updated, and saved in the new format (JSON).  

The deadline for all proposals is 07:00 UT (17:00 Sydney local time), Wednesday, 15 June 2022.

 

For 2022OCT, ATNF proposals will be accepted for the:

  • Australia Telescope Compact Array;
  • Parkes 64m telescope, Murriyang;
  • Tidbinbilla 70-m (DSS-43) and 34-m (DSS-34) antennas; and
  • Long Baseline Array.

What's new in 2022OCT?

  • As a result of restrictions due to the COVID-19 pandemic, observations with ATNF telescopes are able to be carried out remotely. New observing teams will be able to be trained remotely. Observing from the Marsfield or Perth Science Operations Centres is now possible again for Australian residents, but remains optional.
  • ATNF is considering a change in the observing support model, that would replace the ATCA Duty Astronomer and Parkes Project Expert roles. The changes will not be permanently implemented until 2023APR at the earliest, but it is likely that the revised model will be tested during one or more short trial periods in 2022OCT. Further information will be provided during the semester.
  • Several instrument upgrades are underway, and the associated project timescales will impose the need for flexibility in ATNF scheduling during 2022OCT. Specific details for individual telescopes are provided below.
  • ATCA: This may be the last full semester in which CABB will be available. If your science needs CABB, please emphasise this in your justification. Also please note the current state of CABB (from the section below, the ATCA webpages and Jamie Stevens) and contingencies that may be required to successfully deliver spectral line observations (e.g. duplication of zoom bands). It may be better to wait for BIGCAT for spectral-line science, unless your science requires time this semester.
  • ATCA: BIGCAT testing will continue in 2022OCT, and may affect the functionality of the telescope. Effort to develop and test BIGCAT is split with other projects, and so we can not accurately anticipate when the testing will be scheduled. We may have to reschedule observations after the schedule is published.
  • Parkes: Scheduling for the semester is likely to be impacted by activities in preparation for the CryoPAF and the new lunar tracking agreement with Intuitive Machines.
  • ATCA: NAPA proposals for rapid response observations (within ~10 minutes of an alert) are welcomed. A rapid response mode for the ATCA is now in operation. Proposers seeking to use this mode must contact Jamie Stevens (Jamie.Stevens [at] csiro.au) and demonstrate a working triggering mechanism before being allowed to send triggers to the telescope.
  • Proposers are asked to not list their team members in the justification. Past projects should be referred to by proposal code rather than by the name of the PI. We also encourage proposers to consider using numbered references particularly when self-citations are included.
  • Note that Large Proposals (>400 hours over the lifetime of the project) are required to include in their justifications a section describing team roles/contributions (see Section 3.4 of the OPAL Users Guide). In order to do this, and also avoid listing team members in the justification, proposers can state the various skills required to conduct the project, and list the team members by initials only. For example, "Our team possesses expertise in planning and conducting these observations (AA, BB), reducing the data (CC, DD), and interpreting the data within the theoretical modelling described earlier (EE, FF)."

 


General Information

New users are advised to read the information on the ATNF Scientific Support of Facilities. This web page explains the different levels of support provided to proposers and observers.

Observing support and remote observing qualification requirements have recently been updated and are described in the ATNF observing support model.

Target of Opportunity proposals can be submitted at any time. Proposals that are not time critical should always be submitted through the regular TAC process when possible, rather than relying on applications for director's time.

Large Projects are projects that require a total of more than 400 hours of observing time over the lifetime of the project. Please read the Large Projects web page in addition to the information on this page. Large Proposals are required to include in their justifications a section describing team roles/contributions (see Section 3.4 of the OPAL Users Guide for more details).

A document outlining Time Assignment Committee procedures is available from the TAC web page.

For further information contact George Heald (George.Heald [at] csiro.au).


 

ATCA picture and link
 

 

ATCA Observing

Remote observing with the ATCA is the default mode of observing during the COVID-19 period. CSIRO site access restrictions have been relaxed, and it is permissible to observe from the Marsfield Science Operations Centre (SOC) or the Perth SOC. Observing at the Narrabri site is encouraged for observers who wish to visit the observatory, and for complex or non-standard observations, or in other circumstances where this is the more sensible option. The Narrabri observatory is considered a remote observing site with regard to support levels for normal observations. New observers are able to be trained remotely, but are encouraged to travel to the SOC if they prefer.

BIGCAT Upgrade Testing

The current plan is to install the new BIGCAT digital system early in 2023APR (a delay from our plan last semester), and the new system will need time in 2022OCT for testing alongside CABB. For some amount of time we expect that only one CABB IF will be available, and that BIGCAT will be duplicating that same IF for testing purposes. During these times, we will try to schedule 16cm projects (which almost always use redundant IFs). If you would prefer that your project not be scheduled during such times, please include a justification for this in your proposal. Conversely, if you’d like to help out with BIGCAT testing and your science can be done with a single CABB IF, please state this in the “Additional Information” section on your cover sheet.

2022OCT may be the last full semester in which CABB will be available. If your science requires CABB data specifically, please emphasise this in your justification.

ATCA Legacy Projects

It is not anticipated that much, if any, time will be used by ATCA Legacy Projects in 2022OCT.

Array configurations

For 2022OCT, the array configurations 6A, 6B, 1.5A, 750A, EW367, EW352, and H214 will be offered. The 2022APR semester will end in 6D array and so this may be continued for the first weeks of 2022OCT. Configurations will only be scheduled if there is sufficient proposal demand for them.

CABB modes

The Compact Array Broadband Backend (CABB) modes that will be available for 2022OCT semester are:

  1. CFB 1M: A bandwidth of 2 GHz with 2048 x 1-MHz channels in each IF band, but no "zoom" bands.
  2. CFB 1M-0.5k: A bandwidth of 2 GHz with 2048 x 1-MHz channels and (optionally) a fine resolution of 0.5 kHz in up to 16 "zoom" bands (each with 2048 channels across 1 MHz) in each IF band.
  3. CFB 64M-32k: A bandwidth of 2 GHz with 32 x 64-MHz channels and (optionally) a fine resolution of 32 kHz in up to 16 zoom bands (each with 2048 channels across 64 MHz) in each IF band.
  4. CFB 1M/64M: A "hybrid" mode with 2048 x 1-MHz (but no zooms) in one IF band, and 32 x 64-MHz channels with (optionally) up to 16 zoom bands with 2048 channels across each 64 MHz in the other IF band.
  5. Pulsar binning mode: The normal 2048 x 1 MHz continuum band is supplied for each IF band and in addition, for each IF, a time-binned IF band with 512 x 4 MHz channels and 32 time bins across the period of the pulsar. A minimum bin time of 110 micro-seconds is possible, allowing 32 bins across a 3.5 milli-second pulsar period. All observers who want to use this mode are responsible for providing their own timing ephemerides for their targets; the observatory cannot provide these for you. Ephemerides must be supplied in the tempo2 predictor format.
  6. High time-resolution mode: The normal 2048 x 1 MHz continuum band is supplied for each IF band and in addition, for each IF, a time-binned IF band with 512 x 4 MHz channels and either 128 or 32 time bins across the correlator cycle period (normally 10 seconds, but can be routinely set as low as 2 seconds).
  7. VLBI backend tied-array mode: This allows you to capture up to 2 x 64 MHz dual polarisation bands with both CABB correlations and 2 bit sampled raw voltage output, using the VLBI backend and recorders. Up to 2x16 MHz dual polarisation bands with 8 bit sampled voltages is also available. If you choose to use ATCA in this mode, without requesting any other LBA station or correlation by S&A, you only need to write an ATCA proposal. This mode has some restrictions however, and proposers who are interested in using this mode must contact the LBA System Scientist Phil Edwards (Philip.Edwards [at] csiro.au) to discuss what is possible. You must include in your proposal a short description of how you will process the data and data transport logistics.

Both CABB IFs are degraded while using zoom modes, and will likely remain degraded for the rest of CABB's life. At the moment, 2 of the 16 blocks in each IF do not form usable zooms in both 1 MHz and 64 MHz zoom modes. Please note though that these problems do not affect the continuum products.

Unless your spectral-line science is time-sensitive, or uses few zooms in each IF, it may be wiser to wait for BIGCAT than risk poor data with CABB. As it is difficult to predict which block will be responsible for each zoom before your observations start, we recommend that observers seek observatory assistance with determining exact configurations. Please contact Jamie Stevens for further information if you are concerned this may impact your science.

More information on CABB is available from the CABB web page.

Compact Array receivers and frequency ranges

The 16-cm band receivers provide an instantaneous frequency coverage from 1.1 to 3.1 GHz (although the usable bandwidth is reduced by typically 30% by Radio Frequency Interference [RFI] -- the impact of RFI on the 16cm band can be seen at this webpage.). The 16-cm band receivers have an improved sensitivity over the original 20- and 13-cm receivers, and include new ortho-mode-transducers, significantly improving the polarisation performance toward the top end of the band.

The 4-cm band receivers cover the band from 4 GHz to 12 GHz. These receivers provide significantly improved system temperatures over the original 6- and 3-cm receivers. The focus positions for the antennas in the 4cm band differ from those of other bands, which should be borne in mind if changing between bands during an observation. It takes about 2 minutes to refocus the antennas.

In the 15-mm (16--25 GHz), 7-mm (30--50 GHz) and 3-mm (83.5--106 GHz) bands, two 2GHz-wide intermediate frequency bands may be selected within an 8 GHz bandwidth. In the 7-mm band, both band centres must be either greater than 41 GHz (the point at which the conversion changes from lower side-band to upper side-band) or both less than 41 GHz. Observing is possible with the standard 15-mm and 7-mm systems on all six antennas, and 3-mm systems on five antennas: there is no 3mm receiver on CA06. Note that the 3mm receivers are ageing and that, as spare parts are limited, or non-existent, component failure in a receiver may not be able to be repaired in a timely manner, or at all.

The ATCA sensitivity calculator provides a means of determining the sensitivity characteristics of observations, and can include the reduction in bandwidth expected due to RFI in the 16cm band.

Millimetre observing

Observing at 3 mm generally starts in May and ends in mid-October. Proposers are reminded that the primary flux density calibrator at 3 mm is Uranus, which in October 2022 will be near a R.A. of 3h02m and declination of +16d50m. Proposals for 3-mm observations that require accurate flux calibration should request time for observations of Uranus (if the array configuration allows). For 7-mm observations with CABB, PKS 1934-638 is sufficiently strong to be used as a primary flux density calibrator, and should be preferred over Uranus for all projects. Proposers requiring their own observations of Uranus (at special frequencies, or at a time when their main target has set, for example), should make this clear in the observations table and justification of their proposal. For secondary calibration at 3- and 7-mm, Observatory staff will calibrate a number of bright AGN, spread over the full range of R.A., against Uranus (at 3mm) and 1934-638 (at 7mm) at the standard continuum observing frequencies throughout the semester.

The array is outfitted with Water Vapour Radiometers (WVRs) provided by the University of New South Wales. Experience to date indicates that these units will, in some conditions, allow corrections to the measured phases on longer baselines to be made, improving phase stability and sensitivity. Interested mm-wavelength observers will be able to use of this capability during 2022OCT. Details of the system are available at the WVR webpage.

Further information


 

Parkes picture and link

 

 

Receiver availability

The default receiver pairing will be Ultra-Wideband Low frequency receiver (UWL) along with a high frequency legacy receiver, likely 13mm or Mars. This installation is likely to be in place until the Cryogenically Cooled Phased Array Feed can be installed for scientific commissioning. Previous discussion details with regards to receiver fleet development and rationalisation can be found in the linked document here and ATUC presentation here.

Backend Availability

MEDUSA is a GPU based backend and details of the available modes can be found in the users guide here (with other modes driven by proposals, acknowledging shared risk development). Whilst we await the the Ultra-Wideband High frequency receiver, UWH (for which a funding application has been made for a 4-32GHz receiver), MEDUSA can be used with the UWL, plus the Mars and 13mm high frequency legacy receivers (which would traditionally have used DFB4). For those intending to use MEDUSA please include details of the backend capabilities required.

Breakthrough Listen backend is available for scientific use up to 50hrs per semester, please see this webpage for details and contact Danny Price to enquire as to availability.

Other legacy backends available are:

  • DFB4, a digital filterbank previously used for pulsar, spectral line (simple and time-binning), continuum and polarisation (full Stokes) studies. The number of available frequency channels (512 to 8192) allows spectral behaviour analysis and RFI flagging. In combination with either circular or linear feeds they can be used for Stokes Q & U or Stokes V observations respectively. A time resolution down to 0.25s is achievable in time-binning mode allowing fast scanning options (though note in this mode the maximum number of channels is 4096). It should be noted that we are no longer able to provide support for DFB4 and observers are encouraged to utilise MEDUSA where possible.
  • VLBI backends Multiple VLBI backends (LBADR, MEDUSA) are available for non-LBA VLBI and single dish voltage capture. The LBADR system allows you to capture up to 2 x 64 MHz or 8x16 MHz dual polarisation bands with 2 bit sampled raw voltage output, or 2x16 MHz dual polarisation bands with 8 bit sampled voltage. The MEDUSA GPU is now capable of a VLBI voltage capture mode. Data recording up to 16 Gbps should be available (2 GHz bandwidth with 2bit sampling). A bit depth of 2,4 or 8 bits/sample is supported. If you choose to use Parkes in this mode, without requesting any other LBA station or VLBI correlation by ATNF, you only need to write a Parkes proposal. These modes have restrictions: proposers who are interested in using this must contact Chris Phillips to discuss what is possible. You must include in your proposal a short description of how you will process the data and data transport logistics.

Data Rates and Volumes

Data from Parkes observations are archived in ATOA (the Australia Telescope On-line Archive) or the CSIRO Data Access Portal (DAP). To manage the archiving process efficiently, it is necessary to know the expected data volume for projects with Terabyte-scale data requirements, and observations will be scheduled accordingly.

The cover sheet for Parkes proposals specifically requests this information for projects that are likely to gather more than 0.5 Terabytes of data per hour. To assist in determining your data rate an equation is provided below, and the DHAGU interface will also calculate your data rate when generating a parameter set. Further points to note are:

  1. Individual files can not be larger than 100 GB for pulsar data. The output data files from the UWL are automatically split to ensure this. Observations with DFB4 require manual choice of the file splitting time.

  2. The maximum data rate is limited to 20 Gb/s

  3. If you expect to produce more than 5TB in total during the semester, or more than 0.5TBs per hour, then please state your data requirements in your submission, noting that observers should adhere to the observing set-up described in their proposal. As noted above, DHAGU will calculate your data rate when generating a parameter set, and if above 0.5TB per hour it will trigger an email notification when saving. If you exceed your stated data rate/volume then we may need to delete the data files before you are able to access them and they will not be archived.

To calculate data volumes with the UWL:

  • Pulsar Search: File size [bytes] = Nchan x Npol x Nbit/8 x Tobs/Tsamp
  • Pulsar Fold: File size [bytes] = Nchan x Npol x Nbin x 16/8 x Nsub
  • Spectral line mode: File size [bytes] = Nc_sb x Nsb x Npol x Ndump x 32/8
  • Voltage Capture (non-standard): File size per zoom band [bytes] = Nbit/8 x BW x 1e6 x 2 x Tobs x 2

where:

  • Nc_sb = number of channels per subband

  • Nsb = number of subbands (normally 26 for the UWL)
  • Nsub = number of subintegrations in pulsar fold mode
  • Nchan = total number of channels = Nc_sb * Nsb
  • Npol = number of polarisation states (1, 2 or 4)
  • Nbit = number of bits/sample (1, 2, 8, 16 or 32)
  • Tobs = observation time (seconds)
  • Tsamp = sampling time (seconds)
  • Ndump = number of spectral dumps (the total integration divided by the spectral dump time (seconds))
  • BW = bandwidth in MHz

Noting that the total data volume will be a few percent larger than that given by the equation because of the need to store meta-data information.

Telescope Control Software

DHAGU is now the primary control software interface for use with the UWL, MARS and 13mm receivers. It is based on the system used by ASKAP, the Telescope Operation System. It does not interface with DFB4. The Telescope Control Software (TCS), will continue to be used for DFB4 observations where it has been demonstrated DFB4 is required. Documentation is available for the new control software from the links tab within DHAGU and in the users guide.

Contracted telescope usage

Breakthrough Listen will be allocated of the order of 250hrs of Parkes observing time in the 2022OCT semester. The Breakthrough Foundation is not guaranteed any more than 30% of time at any given local sidereal time (LST) range (hour) each month. Commensal use of Breakthrough Listen data is possible (the data is not proprietary) and does not require a proposal to be submitted for consideration by the ATNF Time Assignment Committee. Data is obtained for the P595 project (PULSE at Parkes) and PX600 (a Galactic Centre search) commensally and can be found on the DAP.

In addition to Breakthrough Listen there is also an agreement with an NAOC FAST collaboration for ~150 hrs per semester and with Intuitive Machines for lunar lander tracking for approximately 100hrs.

Observing Information

Remote observing with the Parkes telescope is the default mode of observing during the COVID-19 period. With travel restrictions relaxing, it is permissible to observe from the Marsfield Science Operations Centre (SOC), the Perth SOC, or Parkes itself (for complex or non-standard observations, or in other circumstances where this is the more sensible option). Although observing onsite at Parkes is not fully supported (e.g. there is no onsite accommodation), we do encourage site visits during working hours for those interested (as and when COVID-19 travel restrictions are removed).

It is expected that proposal teams will be scientifically self-sufficient, with a member of each team being designated the Project Expert and being the first point of contact (remotely) for questions relating to the observations after work hours. Inexperienced teams are encouraged to seek experienced collaborators. First time observers will be trained remotely, but will require an experienced observer or the Project Expert to assist with their first observations. All Parkes proposal teams are asked to nominate on the cover sheets of their proposal the member(s) in their team who will be (or will be trained to be) the Project Expert and who will be the first point of contact after hours (please ensure you are using the latest cover sheet template for this). Please ensure that the Project Expert is aware of their role and of the times and dates that they may be called upon. To the extent that COVID-19 restrictions are relaxed, observers at the SOC in Marsfield or Perth are able to receive assistance from staff (during business hours) with their observing. Remote assistance can be sought during working hours through the PORTAL and from the Parkes Mattermost channel (see PORTAL alert for access). Local Parkes staff will continue to provide the first point of contact for matters relating to safety of the telescope, and equipment. Please note that an alternative project based support model is being investigated currently and may have limited trials during the semester (affected parties will be notified directly).

Further information

Proposers intending to start a new project are advised to contact the Parkes System Scientist, Jimi Green (James.Green [at] csiro.au), to discuss their requirements and availability of configurations before proposal submission. For further information on all Parkes capabilities please refer to the Parkes Radio Telescope Users Guide.


 

Tidbinbilla picture and link

 

 

 

In the 2022OCT semester the 70-m and 34-m antennas at Tidbinbilla will have some availability for single-dish use. Access to Tidbinbilla antennas is provided through the host country agreement, which usually provides approximately 220 hours in total each semester. This is used for both single dish (typically 180 hours per semester) and LBA (typically 40 hours per semester) use. Tidbinbilla proposals remain active for one year. All observations are taken in a service mode when scheduling permits (i.e., the proposer does not need to be present and is not involved in the actual observing). Successful proposals require the submission of a source list with accurate target and calibrator positions.

The Pulsar Backend and the Radio Astronomy Spectrometer are available for successful merit-based proposals. The new Radio Astronomy Users Guide provides a basic outline of the capabilities of both backends. The spectrometer is capable of up to 16 IF products, with up to 32,768 spectral channels, each with 1GHz bandwidth. More detailed documentation about these backends, including details of configuration files, can be found in Virkler et al. 2020, ApJS, 251, 1 (preprint here).

The 70-m antenna is equipped with 1.6, 2.3, 8.4 and 22 GHz receivers and 34-m antennas are equipped with 2.3, 8.4, 26 and 32 GHz receivers. The 1.6 GHz receiver on the 70-m antenna will not be available until 2023. The pointing performance of the 70-m is adequate for observations at the three lowest frequencies (1.6, 2.3 and 8.4 GHz) with no additional calibration, but observations at 22-GHz require a small overhead (~10% of observing time) for determining pointing corrections using bright AGN near the target of interest. It should be noted that the 22 GHz system is the most sensitive in the southern hemisphere, covering 18.0 to 26.5 GHz with a system temperature of 60 Jy. The 34-m antennas are equipped with 2.3, 8.4, 26 and 32 GHz receivers. The 8.4 GHz and 22 GHz systems are well-suited for radio recombination line observations. For large area spectral line mapping projects an On-the-Fly mapping mode is available.

Full details of available frequency coverage and other technical information are available from the Tidbinbilla Information web page. (See also the NASA Deep Space Communication Complex web pages.) An on-line sensitivity calculator is available to assist in proposal preparation.

For the latest information of availability please refer to the Tidbinbilla website, or contact Jimi Green (James.Green [at] csiro.au) or Shinji Horiuchi (Shinji.Horiuchi [at] csiro.au).


 

LBA picture and link

 

 

 

For the 2022OCT semester, the Long Baseline Array (LBA) will use the Australia Telescope Compact Array and Parkes radio telescope, together with the Hobart and Ceduna and the AuScope Yarragadee and Katherine 12-m antennas operated by the University of Tasmania. In addition, the Warkworth 12-m telescope, operated by the Auckland University of Technology, is routinely available at 13 and 3cm, and the Warkworth 30-m telescope is available at 6.7 and on a best-efforts basis at 4.8 and 8.4 GHz. The Hartebeesthoek 26-m or 15-m telescopes may also be available. All telescope availability is subject to other commitments - scheduling is done on a best effort basis. A limited amount of time may be available with the Tidbinbilla 70-m antenna (although, as noted above, the 1.6 GHz capability of the 70m is not expected to be reinstated until 2023) or one of the 34-m antennas. The availability of the Mopra telescope for 2022OCT is currently unclear: it may be included in the requested array, but with the understanding that it may not be scheduled. For the 2022OCT semester, ASKAP will not be available for VLBI. The Hobart 26m is currently off-line -- the AuScope 12m antenna at Hobart can be used instead. The AuScope antennas are undergoing a receiver upgrade from their original S/X (2/8 GHz) receivers. Katherine and Hobart have wideband 2--14 GHz receivers and Yarragadee is expected to be upgraded in late 2022. 

During the 2022OCT semester some LBA time may be scheduled at the same time as a European VLBI Network (EVN) session, opening the possibility of joint LBA/EVN observations. The easternmost stations of the EVN are in a similar longitude range to the LBA telescopes, and for sources in equatorial regions, baselines to western European stations are also achievable. Proposals for joint LBA/EVN observations must be submitted separately to both the LBA and EVN at their respective deadlines.

It is now possible to operate the ATCA in hybrid mode where one frequency chain is setup in VLBI mode and the other frequency chain in ATCA continuum mode (2 GHz bandwidth at 1 MHz resolution). Proposers should explicitly request this mode if they wish to use it, and provide additional scientific justification.

Constraints on Parkes receiver changes impose limits on the frequency of LBA observations with Parkes, however, note that the UWL receiver means Parkes can be included in VLBI observations between 700 MHz and 4 GHz at almost any time. Observations at 8.4 and 22 GHz may be possible: other frequencies may be requested but are less likely.

The Parkes UWL and AuScope Katherine and Hobart telescopes produce linear polarisations. There has been some success in converting to circular polarisations post-correlation, but experience is still be gained in this approach and it is not yet 100% reliable.

LBA proposers are reminded that a member (or members) of the proposal team will be required to assist with the VLBI observing on the ATNF telescopes. Please ensure that a member of the proposal team will be able to help. Note that due to logistical constraints the VLBI schedule usually is released only a few weeks before observing, so the observer will need to be qualified for remote observing with Parkes and ATCA. Due to COVID-19 restrictions, new observers are able to be trained remotely prior to the LBA session.

Telescopes outside the core LBA may be also requested for special observations. Specific system availability may be dependent on availability at individual antennas. Sources close to the equator may benefit from including telescopes from Asia. No formal mechanism is currently available for requesting time and all such telescopes need to be negotiated on a case-by-base basis. Phil Edwards can assist with this process.

For more details consult the ATNF VLBI webpages.

A Novices Guide is available for potential first-time users from the VLBI webpage.

Proposers can use the EVN planning tool, which includes the LBA telescopes. Proposers may also contact Phil Edwards (details below) with any questions related to sensitivity calculations for LBA observations.

The current capabilities of the LBA are briefly outlined below:

  • The disk-based recording system is used for all recorded VLBI observations and data rates (up to 1 Gbps) can be achieved at most stations.
  • All recorded observations will be correlated with the DiFX software correlator. The software correlator is capable of correlating the high data rate observations at high spectral resolution with arbitrary correlator integration times.

User support is available, including assistance with proposal preparation, scheduling, observer training and data reduction.

A bit rate of 256 Mbps (2x16MHz bandwidth in 2 polarisations, with 2 bit digitisation and Nyquist sampling) can be sustained at all LBA telescopes and is the standard observing mode. Observations requesting higher bit rates will need to include a clear justification for the requested rate. Potential users must consult the VLBI National Facilities capabilities .

For more information contact the LBA System Scientist, Phil Edwards (Philip.Edwards [at] csiro.au).

 

 

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