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[vsnet-alert 1632] Forward: CI CAM =? XTEJ0421+560 Optical spectroscopy and photometry (Garcia)


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Hajime BABA                         E-Mail: baba@kusastro.kyoto-u.ac.jp
Department of Astronomy                  Phone(office): +81-75-753-4287
Faculty of Science, Kyoto University, Kyoto 606-8502, JAPAN
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Date: Fri, 3 Apr 1998 17:21:02 -0500
From: garcia@cfa219.harvard.edu (Mike Garcia)
Message-ID: <vsnet-alert1632@hoge.baba.hajime.jp>
To: BAILYN@astro.yale.edu, ajct@laeff.esa.es, chaswell@star.maps.susx.ac.uk,
        e.kuulkers1@physics.oxford.ac.uk, fghigo@nrao.edu,
        garcia@head-cfa.harvard.edu, guy@mrao.cam.ac.uk,
        ewaltman@rsd.nrl.navy.mil, jem@head-cfa.harvard.edu,
        lewin@space.mit.edu, marshall@milkyway.gsfc.nasa.gov,
        pac@astro.ox.ac.uk, rhjellmi@aoc.nrao.edu, rmw@lowell.Lowell.Edu,
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Subject: [vsnet-alert 0] CI CAM =? XTEJ0421+560 Optical spectroscopy and photometry
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Dear Colleagues: 
	Attached is the text of our submittion to the IAUC.
Good luck observing tonight!  

--------------


M.R. Garcia, P. Berlind, E. Barton, J.E. McClintock (Center for
Astrophysics), P.J. Callanan and J. McCarthy, (UCC Ireland),

Report:

Photometric and spectroscopic observations of CI CAM, the possible
counterpart of XTE J0421+56 (IAUC 6855, 6857), were obtained with the
1.2m and 1.5m telescopes at the Whipple Observatory during 1998 April
3.08-3.17 UT.  Conditions were photometric with variable 2" seeing.
We find V=9.25 +/- 0.1, B=10.25 +/- 0.1.  This implies a brightening
of more than 2 magnitudes in each band, relative to the levels
measured by Bergner et al (1995 A&A Suppl 112 221).  Relative
photometry of 3 B and 4 V frames yields an upper limit to any short
term photometric variability of <2% during our observations.  Our
spectra, obtained at 3.0 and 0.75 angstrom resolution (covering
4000-7000 angstroms and 6000-7000 angstroms), appear similar to those
of Downes (1984 PASP 96 807), but the level of Fe II and He I
emission has strengthened in comparison to H-Balmer.  He II (4685.3
angstroms) and He I (4712.9 angstroms) are detected with equivalent
widths of 15+/-5 angstroms and 30+/-10 angstroms respectively,
confirming the new HeII emission reported by Wagner et al. (IAUC
6857).  The forest of strong H, He I, and Fe II emission lines
obscures the continuum to the extent that it is unclear if any
photospheric absorption lines are present.  None of the lines in our
spectra show any evidence for the type of double peaked emission
typically arising in x-ray binary or cataclysmic variable accretion
disks.  Our data are consistent with the association of CI Cam with
XTE J0421+56, but imply that this might then be an unusual
symbiotic-type x-ray binary, perhaps akin to GX1+4 or 2A1704+241(=HD154791).

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