Pulsar ALFA Survey Project
Welcome to the Pulsar ALFA Survey page! The goal of the survey
is to find not only a large sample of pulsars, but also rare objects
that are useful for probing fundamental aspects of neutron star
physics and testing theories of gravity and gravitational physics,
among other goals.
This page is for internal use of the Consortium only, so don't
disseminate its address. For general information on our survey, here
is our public page.
The material archived here includes documentation, observation logs
and pulsar detections and re-detections, as well as various
miscellaneous stuff. Please help keep it up to date!
Note to Updaters: Please make sure that the file permissions are correctly assigned.
- Breaking News
- 15 Oct 2012 the ALFA lid was left on by mistake; data is useless and is deleted.
- 26 July 2011 - 6 Sep. 2011 ALFA is taken down; Beam 6 is repaired. Mock data
from Beam 6 taken after 6 Sep. 2011 is converted as usual.
- 12 June 2011 observations have no data from beam 5 because of raid disk failure.
- 7 May 2011 observations are likely useless because Mock power
was too low (J1952+26 wasn't seen in a pointing during that session).
- ALFA Beam 6 is completely dead since 24 Mar. 2011. Mock data
from this beam will be discarded until ALFA is repaired.
- Beam 6 had only one polarization channel working from 3 Jan. 2011 to 24 Mar. 2011.
Data from this period will be kept and converted as usual.
- Mock data up to 28 Jan. 2010 have the wrong positions
for the ALFA side beams in the psrfits main header as well as in psrfits rows
due to a bug in the Mock software that was subsequently fixed. Positions
for Beam 0 data are correct. Psrfits files created after the bug was fixed have
HDRVER=3.43 or higher in the header.
- Documentation: Start here.
- PALFA Publications
- Mock Spectrometer
- WAPP Correlator
- Schedules and log files
- Important Pointing Issues (added by JMW & JWTH)
- WARNING: There appears to be an error with the positions written
to the WAPP file headers. This has resulted in a rotation of 180 deg
from the true position of the beams.
- CAUTION: The feed will rotate by more than half a beamwidth when
observing close to the zenith along the meridian. See the following
plots by Phil Perillat: Beam
rotation as a function of feed position from zenith.
- CAUTION: When reobserving the same pointing position at a
significantly different parallatic angle, the beams will not
fall on top of each other, and their central positions may differ by
as much as an arcminute!
- Data Transport Information
- Miscellaneous Stuff:
chgrp palfa *; chmod 664 * (or 775 for directories)
Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Science Foundation.