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A New View of the Galactic Plane with EXOSAT
Warwick, R. S.; Watson, M. G.; Turner, M. J. L. +1 more
A new X-ray image of the galactic plane has been produced using the 45 arcmin square field of view of the Medium Energy Instrument on EXOSAT. This image shows a total of 64 sources including 18 new ones which include the first observation of persistent emission from the globular cluster bursters Terzan 1 and Terzan 5. The most important discovery …
EXOSAT Observations of Bursts from 2S1636-536 - Burst Morphology
Turner, M. J. L.; Ohashi, T.; Breedon, L. M.
In two observations with the EXOSAT ME a total of 11 bursts were detected; 7 in July and 4 in May 1984. In terms of rise time and peak count rate there are only 2 kinds, those with a sharp rise and peak count rate of 500 cts/sec/detector and those with a slow rise and a peak count rate of 200 cts/sec/detector. The spectral analysis of these bursts…
Soft X-ray characteristics of white dwarfs observed by EXOSAT
Grewing, M.; Heise, J.; Bleeker, J. A. M. +5 more
EXOSAT has observed 19 hot white dwarfs with alleged strong soft X-ray emission. Positive detection of a large fraction of this sample was obtained, among these practically all hot DA dwarfs. High-resolution spectral data, acquired with the 500 1/mm grating spectrometer, indicates no traces of He in the atmosphere of HZ43, i.e. n(He)/n(H) <= 10…
The soft X-ray superoutburst of VW hydri: 14 second periodicity
Heise, J.; van der Woerd, H.; Paerels, F.
EXOSAT observations of the dwarf nova VW Hydri reveal a strong soft X-ray flux during optical superoutburst. The onset of the X-ray outburst was delayed by 2.5 days compared to the optical outburst. A modulation of the extreme soft X-ray flux was detected, consistent with a coherent (0 >x 107) pulsation with a period of 14.07 seconds…
Dynamical activity in V1016 Cygni.
Feibelman, W. A.; Fahey, R. P.
New high-dispersion IUE observations show the C IV emission lines in V1016 Cyg to be split, suggesting evidence for dynamical activity. The [Mg V] line shows structure nearly identical to the C IV lines when plotted in velocity space.
The Final Cos-B Database: In-Flight Calibration of Instrumental Parameters
Strong, A. W.; Hermsen, W.; Lebrun, F. +3 more
A method for the determination of temporal variation of sensitivity is designed to find a set of parameters which lead to maximum consistency between the intensities derived from different observation periods. This method is briefly described and the resulting sensitivity and background variations presented.
Epsilon Aurigae
Chapman, R. D.
In April 1984, fourth contact ended the two year long eclipse of Epsilon Aurigae. An astrometric study of the study of the system was carried out by Van de Kamp (1978) leading to the conclusion that the orbit is seen very close to edge on. The eclipse was monitored by a number of groups from the ground and from spacecraft such as the IUE. Ultravio…
H0323+022 - Classification as a Bl-Lacertae and EXOSAT Coordinated Observations
McHardy, I.; McClintock, J. E.; Remillard, R. +18 more
The object H0323+022 (Doxsey et al. 1983) has been shown to be a BL Lac object by virtue of a diversity of observational characteristics at radio, optical, and x-ray wavelengths, in agreement with the conclusion of Margon and Jacoby (1984). Multi-frequency coordinated observations of this highly variable object with EXOSAT in September 1984 found …
Coordinated EXOSAT and Optical Observations of the X-Ray Burster 4U1737-44
Charles, P. A.; Corbet, R. H. D.; Smale, A. P. +2 more
We present the first results of an EXOSAT observation of the low-mass X-ray burster 4U1735-44. The ME data show low-amplitude variations in the persistent flux including two 5% dips separated by ∼4 hours. The structure of the single observed burst is briefly described. Five hours of simultaneous B-band photometry were obtained at SAAO with 12 minu…
EXOSAT spectra of some bright QSO's
Tennant, A. F.; Stewart, G. C.; Shafer, R. A. +1 more
This paper reports on EXOSAT observations of four bright QSO's and active galaxies. The QSO PHL 1657 has a simple spectrum that can be fit with power law plus some low energy absorption. A soft excess is observed for both MR 2251 and E 1352.24+1830. Finally, PKS 2126-158 was detected and the results are consistent with a 0.7 energy index.