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Astrophysical Applications of Scattering in Interstellar and Intracluster Gases Astrophysical Applications of Scattering in Interstellar and Intracluster Gases

Conrad Cramphorn, Conrad Cramphorn, Conrad Cramphorn
2004 unpublished
Die Nachtstunde schlug; ich hüllte mich in meine abenteuerliche Vermummung, nahm die Pike und das Horn zur Hand, ging in die Finsternis hinaus und rief die Stunde ab, nachdem ich mich durch ein Kreuz gegen die bösen Geister geschützt hatte. Bonaventura, "Nachtwachen" 11 J'aime les nuages ... les nuages qui passent ... là-bas ... là-bas ... les merveilleux nuages! Charles Baudelaire, "Paris Spleen" 2 The X-ray luminosity of the Galactic centre in the recent past Abstract Information about the
more » ... mation about the X-ray luminosity of the supermassive black hole located at the Galactic centre (GC), Sgr A * , and its temporal variations in the past is imprinted in the scattered emission observed today in the direction towards giant molecular clouds (GMCs) located in our Galaxy. Due to light travel time effects these clouds probe the activity of Sgr A * at different times in the past depending on their position relative to the GC and the observer. In this chapter we combine results of recent ASCA observations along the Galactic plane, providing upper limits for the scattered flux in the 4-10 keV range produced in a given direction, with data from CO surveys of the same regions. These CO surveys map the position and mass of the molecular gas which the GMCs are made up of. Demanding the scattered flux to be not larger than the observed one, this data enables us to derive upper limits for the 4-10 keV luminosity of Sgr A * at certain times during the last 40.000 years down to about 8 × 10 40 erg s −1 . At other times the limits are less tight, of the order of 10 41 − 10 42 erg s −1 . For two periods of time of about 2.000 and 4.000 years duration 8.000 and 14.000 years ago the currently available CO data is insensitive to any enhanced activity of the GC. Flares lasting longer than 3.000 years fill these time gaps and therefore can be excluded to have occurred during the last 40.000 years with a luminosity larger than a few 10 42 erg s −1 . The more extended and continuous HI distribution in the 21 2 The X-ray luminosity of the Galactic centre in the recent past Galactic disk, which also scatters the radiation emitted by Sgr A * , allows us to extend the time coverage further into the past, back to about 110.000 years, albeit the limits are becoming less tight. We thereby can rule out a long term X-ray activity phase of Sgr A * at one per cent of its Eddington level ending less than about 80.000 years ago. The limits presented in this chapter can be improved by observations of emission in the fluorescent iron K α -line. We study the feasibility of these methods to investigate past nuclear activity in other spiral galaxies observed with the angular resolution of X-ray telescopes like Chandra and XMM-Newton.
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