[Message Prev][Message Next][Thread Prev][Thread Next][Message Index][Thread Index]
[vsnet-alert 3560] Submittion to IAUC
- Date: Fri, 8 Oct 1999 11:46:58 -0400 (EDT)
- To: BAILYN@astro.yale.edu, HARMON@SSLMOR.msfc.nasa.gov, Michael.McCollough@msfc.nasa.gov, S.Chaty@open.ac.uk, ajct@laeff.esa.es, amiodusz@zia.aoc.nrao.edu, asmith@space.mit.edu, bmg@space.mit.edu, e.kuulkers1@physics.oxford.ac.uk, ehm@space.mit.edu, eiken@astrosun.tn.cornell.edu, ewaltman@rsd.nrl.navy.mil, fghigo@nrao.edu, garcia@head-cfa.harvard.edu, gehrels@lheavx.gsfc.nasa.gov, giommi@napa.sdc.asi.it, greiner@aip.de, guy@mrao.cam.ac.uk, jem@head-cfa.harvard.edu, lewin@space.mit.edu, luisfr@astrosmo.unam.mx, marshall@milkyway.gsfc.nasa.gov, michiel@astro.uva.nl, mirabel@discovery.saclay.cea.fr, mnowak@rocinante.colorado.edu, mrupen@zia.aoc.nrao.edu, narayan@cfa.harvard.edu, pac@astro.ox.ac.uk, rhjellmi@aoc.nrao.edu, rmw@lowell.edu, rpf@astro.uva.nl, rudy@space.mit.edu, rr@space.mit.edu, shrader@grossc.gsfc.nasa.gov, srk@astro.caltech.edu, tarrfie@hydro.la.asu.edu, stroh@pcasun1.gsfc.nasa.gov, swank@pcasun1.gsfc.nasa.gov, takeshim@ginpo.gsfc.nasa.gov, tavani@astro.columbia.edu, tkato@kusastro.kyoto-u.ac.jp, vsnet-alert@kusastro.kyoto-u.ac.jp, wheel@alla.as.utexas.edu
- From: Mike Garcia <garcia@head-cfa.harvard.edu>
- Subject: [vsnet-alert 3560] Submittion to IAUC
- Cc: garcia@head-cfa.harvard.edu, paulc@ucc.ie
- Sender: owner-vsnet-alert@kusastro.kyoto-u.ac.jp
Dear Collegues - We have recently sent the following for
inclusion in the IAUC.
Best Regards - Mike Garcia
----------------------------------------------------------------
GM Sgr = SAX J1819.3-2525 = XTE J1819-254
M. R. Garcia, J. E. McClintock, and P. J. Callanan report:
We have obtained a total of 25 spectra with the FLWO 60" and FAST
spectrograph (range 380-750 nm, resolution 0.6 nm) of GM Sgr, centered
on the nights of Sept 17.2 18.2, and 19.1 UT. During this time the
H-alpha line transitioned from emission to absorption. Equivalent
widths were -7(1) nm, -3(1) nm, and +0.45(0.05) nm, respectively. The
strong emission line seen on Sept 17.2 had a FWHM = 3.3(0.3) nm and a
complex structure with two prominent peaks on the blue wing. The
remainder of the Balmer series lines (through H16) re visible in each
of the spectra, and they are narrower (1.0 nm < FWHM < 2.0 nm) than
the H-alpha emission line and were always in absorption. The
continuum and absorption line spectrum resembles that of an A Star.
The velocities of the Balmer absorption lines measured on the three
consecutive nights were +320(20) km/sec, 0(40)km/sec, and 80(20)
km/sec, respectively.
Return to Daisaku Nogami
vsnet-adm@kusastro.kyoto-u.ac.jp
VSNET Home Page