Central Bureau for Astronomical Telegrams
IAUC 5981: GRO J1948+32 = GRO J2014+34; 1994I
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Circular No. 5981
Central Bureau for Astronomical Telegrams
INTERNATIONAL ASTRONOMICAL UNION
Postal Address: Central Bureau for Astronomical Telegrams
Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A.
Telephone 617-495-7244/7440/7444 (for emergency use only)
TWX 710-320-6842 ASTROGRAM CAM EASYLINK 62794505
MARSDEN@CFA or GREEN@CFA (.SPAN, .BITNET or .HARVARD.EDU)
GRO J1948+32 = GRO J2014+34
D. Chakrabarty and T. A. Prince, California Institute of
Technology; M. H. Finger, Universities Space Research Association;
R. B. Wilson, Marshall Space Flight Center, NASA; and G. N.
Pendleton, University of Alabama, Huntsville, report for the
Compton Gamma Ray Observatory BATSE team: "Further observations of
the recently-discovered, 18.7-s, transient hard x-ray pulsar in
Cygnus (originally designated GRO J2014+34; see IAUC 5977) have
yielded a more precise position. The estimated 90-percent-
confidence error box is approximately a 2o.5 x 5o.5 quadrilateral,
with corners at R.A. = 19h58m, Decl. = +29o.0; 19h50m, +34o.0;
19h34m, +35o.0; 19h46m, +28o.0 (equinox 2000.0). In accordance
with the substantially improved position, we have redesignated the
source as GRO J1948+32. The pulsed emission was first detectable
on Apr. 6 UT and continues to be visible as of Apr. 28. Optical
and soft-x-ray observations of the error box are strongly
encouraged in order to further constrain the x-ray position and
identify the accreting companion."
SUPERNOVA 1994I IN NGC 5194
R. Kirshner, Center for Astrophysics, reports on behalf of the
Supernova INtensive Studies (SINS) team that SN 1994I was observed
with the Hubble Space Telescope (HST) Faint Object Spectrograph
(FOS) and Planetary Camera on Apr. 18 and 19 UT. The spectrum
extends from 160 to 470 nm; it is consistent with the type-Ic
classification of earlier optical data, but the ultraviolet shows a
strong resemblance to the FOS spectrum of the type-Ia SN 1992A
about 5 days after maximum light (Kirshner et al. 1993, Ap.J. 415,
589). The spectrum shows no signature of the circumstellar matter
inferred from radio observations. Ultraviolet flux levels from the
spectrum and from U-band images are consistent at about 8 x 10E-16
erg sE-1 cmE-2 AE-1, and are much lower at shorter wavelengths.
The supernova appears projected on diffuse emission, possibly from
a spiral arm in M51. Comparison of the recent U image with 1992
HST observations of M51 demonstrates that the star suggested by
Richmond (IAUC 5966) as the possible progenitor is present both
before and after the eruption of SN 1994I, about 0".36 from the
supernova site. The absence of an identified progenitor in the
earlier HST data may provide useful constraints. Further HST
images and spectra are planned for May 12 and 14."
1994 April 29 (5981) Daniel W. E. Green
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