In addition to supernovae, the members of the group have also studied
pulsars. The Crab pulsar's near-UV spectrum (1600-3200 Å) was studied
with HST/STIS in time-tag mode which provides 125 
s time resolution.
Spectra of the main pulse, the interpulse, and the individual rising and
falling edges are similar to the total spectrum within the limits of photon
statistics. A standard extinction curve with 
appears to apply. Several interstellar absorption lines are seen, but the
equivalent widths of Mg I, Mg II and Fe II are lower than expected from the
E(B-V) derived. A deeper exposure in the far-UV (1140-1720 Å) was
scheduled, and was performed on January 22, 1999. The group also studied
PSR 1706-44 using the science verification observations with the test
camera on VLT-UT1. (VLT is the ESO's Very Large Telescope. This made the
supernova group the first in Sweden to analyze and publish VLT data.) PSR
1706-44 is a Vela-like pulsar with similar pulse period ( 
s) and
spin-down age ( 
years). The excellent seeing at Paranal made it
possible to put a 3 
limit on the optical flux from PSR 1706-44 at
V = 25.5 if the pulsar is not close to a projected bright star. This
provides important input to models of the pulsar emission as the
relationship between optical pulsed emission and those in the X-ray or
-ray bands is unclear. (PSR 1706-44 has been detected in both
X-rays and -rays.)