A Technique for Narrowband Time Series Photometry: the X-ray Star V2116 Oph

Details A Technique for Narrowband Time Series Photometry: the X-ray Star V2116 Oph A Technique for Narrowband Time Series Photometry: the X-ray Star V2116 Oph

1998-05-27

arxiv.org/abs/astro-ph/9805336v1

Publ.Astron.Soc.Pac.110:912,1998

Astronomy and Astrophysics

Astrophysics

9 pages including 4 figures and no tables. Accepted for publication in PASP; to appear in Volume 110, August 1998

Scientific paper

10.1086/316217

We have used innovative features of the Taurus Tunable Filter instrument on the 3.9-m Anglo-Australian Telescope to obtain nearly-continuous, high-throughput, linear photometry of V2116 Oph in a 7 Angstrom bandpass at the center of the O I 8446 emission line. This instrumental technique shows promise for applications requiring precise, rapid, narrowband photometry of faint objects. The spectrum of V2116 Oph, the counterpart of GX 1+4 (=X1728-247), is exotic, even among the unusual spectra of other optical counterparts of compact Galactic X-ray sources. The second strongest emission line is an unusual one, namely extremely prominent O I 8446, which is likely to result from pumping by an intense Ly beta radiation field. As the X-radiation from GX 1+4 is steadily pulsed, with typical pulsed fractions of 0.4, the O I 8446 emission in V2116 Oph may also be strongly modulated with the current 127 s period of the X-ray source. If so, this may well allow us to obtain high signal-to-noise radial velocity measurements and thus to determine the system parameters. However, no such pulsations are detected, and we set an upper limit of ~1% (full-amplitude) on periodic 8446 oscillations at the X-ray frequency. This value is comparable to the amplitude of continuum oscillations observed on some nights by other workers. Thus we rule out an enhancement of the pulsation amplitude in O I emission, at least at the time of our observations.

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