Welcome to Gayatri, joining the PaCER team – looking for FRBs in MWA high time resolution images
Ramesh’s initial update
SMART Survey update
Pulsar #3!
Remaining observing campaign still at the mercy of MWA commissioning timeline
During MWA Project Meeting, needs of various MWA science groups were clarified, and the LST range that we need in compact config aligns quite nicely with the needs of the EoR group
MWA Phase 3 will happen “in multiple phases”, with the transition from 128T to 256T happening over time, probably not beginning before early 2023—this is the current plan, anyway.
PSR #2
J0026-1956 was actually first detected by GBT!
Paper still pushing forward, which focuses on drifting analysis
Showed the GBT detection (~85 seconds of data)
Has been seen in Parkes 70cm
Paper currently in (first) MWA collaboration review period
GMRT Cycle 41 follow up:
Band 3 and Band 4 in Nov/Dec
Full polar mode used
Source position good to ~1 arcmin
RFI is a major problem
Band 4 imaging analysis yet to come
Possible early indication of <1 arcmin positional offset
Band 3 observation seems to imply smaller nulling fraction, but other observations show a different story
Not yet calibrated for polarisation, but even uncalibrated observation of test pulsar (B2327-20) show first-order-correctness
PSR #3 (J1002-2036):
Possibly low luminosity pulsar, at high latitudes
Similar in some ways to PSR #1
Used localisation method to get another ~20% increase in S/N
Also observed in a 2nd detection!
Vindication of SMART strategy, with ~10 deg overlap between adjacent pointings
pdmp detection also shown
Other summary updates:
Remaining SMART obs may have to wait till 2022A/2022B
ASTAC proposal for more OzSTAR time in 2022A has been submitted
Discussion:
SD: how many harmonics are summed in search?
NS: 16 (in PRESTO)
SD: Losing sensitivity to wide profile pulsars?
NS: Don’t think so because 16 is max. It still searches 1, 2, 4, 8, 16 harmonics
RB: Interesting, PSRs #1, #2, #3 are in order of increasing period! PSR #3’s duty cycle is ~2.5%
RB: Whether to change max number of harmonics can wait until second (deep) search
Sam’s update:
Latest practice data set was successful = can now beamform MWAX data
Uses Hyperdrive (“RTS v2.0”), which can currently do DI calibration
Legacy data can still use RTS, but MWAX data will only use Hyperdrive
In beam calibration not yet possible – requires offline MWAX correlator to be installed, e.g. on Garrawarla, which is in progress
VCSBeam code is now “understood”, in terms of coordinate bases used for Jones matrices, etc.
Further polarimetric calibration of the beam still a work in progress
MS & SS: Maybe Emil’s imaging technique is what’s needed
Nick’s update:
Showing off the new database
Hosted at DataCentral
Still working out kinks, data not yet uploaded
Makes authentication really streamlined, amenable to getting more people (e.g. high school students) helping the pulsar-hunting effort
Discussion:
WvS: What can people download?
RB: Best pulsar detections, but details would be good topic for future discussion, e.g. 10 second archives (full freq resolution?)
Zhongli update
Getting ready to process on SHAO cluster, but needs some coordination
SHAO cluster has computing resources to process
Some tests have been carried out, using presto based suite
NS: work out the best way to do the full search before doing any processing
RB: Take this up a busy day discussion item - software/pipeline coordination critically important for processing coordination, the use of dissimilar pipelines to process survey data must be avoided (and will not be beneficial in the long run)