Simultaneous Soft X-Ray and GeV Gamma-Ray Observations of BL Lacertae Object AO 0235+164

Details Simultaneous Soft X-Ray and GeV Gamma-Ray Observations of BL Lacertae Object AO 0235+164 Simultaneous Soft X-Ray and GeV Gamma-Ray Observations of BL Lacertae Object AO 0235+164

Mar 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...459..156m&link_type=abstract

Astrophysical Journal v.459, p.156

Astronomy and Astrophysics

Astronomy

53

Galaxies: Bl Lacertae Objects: Individual Alphanumeric: 0235+164, Gamma Rays: Observations, X-Rays: Galaxies

Scientific paper

We present data collected during a simultaneous GeV y-ray (Compton Gamma Ray Observatory EGRET) and X-ray (ASCA) observation of BL Lac object AO 0235+164 (z = 0.94); we also present ROSAT PSPC X-ray data, obtained 6 months earlier. The X-ray spectra from both ROSAT and ASCA confirm a substantial photoelectric absorption beyond the value expected from our Galaxy, which is most likely caused by heavy elements in the inerstellar medium of an intervening galaxy at z = 0.524; it is possible to measure the elemental abundances in it modulo the hydrogen spin temperature T5. By comparing the absorption in our data to the 21 cm absorption, we can limit T_{5 }to at most 700 K. The ROSA T data imply a rapid ( 3 day) doubling of the soft X-ray flux and a subsequent quasi- exponential decay, whereas no variability is apparent in the ASCA or EGRET data. We detect a significant spectral change of the BL Lac X-ray continuum between the ROSA T and ASCA observations; ASCA data show that the spectrum is substantially harder (with the energy power-law index alpha 1 vs. 2) and fainter than in the ROSA T data. The simplest interpretation of this spectral variability is that the ROSA T data are dominated by a bright, soft tail of a synchrotron component, which disappeared during the ASCA observation, uncovering a harder Compton component. The EGRET data imply a lower GeV flux than in the previous observations, with no apparent change of the GeV spectrum. The ratio of the y-ray to the X-ray flux [in E x F(E)] for this radio-discovered object is roughly 30, which is very substantially higher than that inferred for X ray-discovered BL Lac objects, suggesting an important difference in the structure between the two subclasses of BL Lac objects.

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