Volume 389, Number 3, July III 2002
|Page(s)||752 - 760|
|Section||Cosmology (including clusters of galaxies)|
|Published online||01 July 2002|
RXTE view of the starburst galaxies M 82 and NGC 253
School of Physics and Astronomy, Tel Aviv University, Tel Aviv, Israel
2 Center for Astrophysics and Space Sciences, University of California, San Diego, USA
Corresponding author: Y. Rephaeli, email@example.com
Accepted: 25 March 2002
The two nearby starburst galaxies M 82 and NGC 253 were observed for ∼100 ksec over a 10-month period in 1997. An increase of the M 82 flux by a factor ∼2 was measured during the period July-November, when compared with the flux measured earlier in 1997. The flux measured in the field centered on M 82 includes ∼38% of the emission from the Seyfert 1 galaxy M 81. The best-fitting model for the earlier emission from M 82 is thermal with . In the high flux state, the emission additionally includes either an absorbed second thermal component or absorbed power-law component, with the former providing a much better fit. A likely origin for the temporal variability is a single source in M 82. The flux of NGC 253, which did not vary significantly during the period of observations, can be well fit by either a thermal spectrum with keV, or by a power law with photon index of . We have also attempted fitting the measurements to more realistic composite models with thermal and power-law components, such as would be expected from a dominant contribution from binary systems, or Compton scattering of (far) IR radiation by radio emitting electrons. However, the addition of any amount of a power-law component, even with cutoff at 20 keV, only increases chi-square. The 90% confidence upper limit for power law emission with (photon) index 1.5 is only 2.4% of the 2–10 keV flux of M 82; the corresponding limit for NGC 253, with index 2.0, is 48%.
Key words: galaxies: starburst / galaxies: individual: M 82, NGC 253 / X-rays: galaxies / radiation mechanisms: non-thermal
© ESO, 2002
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