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IAUC 5977: GRO J2014+34; GRO J1008-57

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                                                  Circular No. 5977
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 J2014+34
     M. H. Finger, Universities Space Research Association; M.
Stollberg and G. N. Pendleton, University of Alabama, Huntsville;
R. B. Wilson, Marshall Space Flight Center, NASA; and D. Chakrabarty,
J. Chiu, and T. A. Prince, California Institute of Technology,
report for the Compton Gamma-Ray Observatory BATSE team:  "Pulsed
hard x-ray emission is being seen from a previously uncatalogued
object in the Cygnus-Vulpecula region.  The current best-fit source
position is R.A. = 20h14m, Decl. = +34o.5 (equinox 2000.0), with an
estimated 68-percent-confidence region of radius 8 deg.  Work is
continuing to verify this position estimate.  The emission from the
pulsar was first detectable on Apr. 6 and reached peak intensity on
Apr. 16.  The source is detected at energies from 20 up to at least
70 keV.  The barycentric pulse period on Apr. 14.0 UT was 18.7021
+/- 0.0001 s, with the period increasing at a rate of (6.0 +/- 0.7)
x 10E-9.  The pulse profile averaged over Apr. 14-16 has a main
peak with a FWHM of about 0.5 in phase, with a 0.15-HWHM 'shoulder'
present on the falling edge.  The 20- to 40-keV pulsed flux on Apr.
16 was about 50 mCrab, with the spectrum well fitted by an optically
thin thermal bremsstrahlung model F(E) = (A/E)exp(-E/kT), with
temperature kT = 23 +/- 6 keV and F(40 keV) = 1.88 +/- 0.24 x 10E-4
photon cmE-2 sE-1 keVE-1."


GRO J1008-57
     M. J. Coe, C. Everall, and P. D. Roche, Southampton University;
J. Fabregat, Valencia University; D. A. H. Buckley, South African
Astronomical Observatory; and R. C. Smith, Cerro Tololo Interamerican
Observatory, report:  "We have found a probable optical counterpart
to the transient pulsar GRO J1008-57 (cf. IAUC 5836, 5838, 5851,
5877).  A U.K. Schmidt red plate taken on 1993 July 28 (during
discovery outburst) reveals two objects within the ROSAT error
circle, the brightest at R.A. = 10h09m46s.9, Decl. = -58o17'35"
(equinox 2000.0).  Spectroscopic and photometric observations from
the SAAO 1.9-m telescope (Dec. 1993), CTIO Schmidt telescope (Jan.
1994), and the 3.9-m Anglo-Australian Telescope (Mar. 1994) reveal
this brightest star as the only H-alpha emitter in the region, with
strong infrared emission (J = 11.2, H = 10.5, K = 9.9).  This
suggests that the system is another Be or supergiant x-ray binary,
as indicated by the x-ray characteristics."


1994 April 20                  (5977)            Daniel W. E. Green

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