Discovery of Hot Gas in Outflow in NGC 3379
Trinchieri, G.; Pellegrini, S.; Fabbiano, G.; Fu, R.; Brassington, Nicola; Zezas, A.; Kim, D.-W.; Gallagher, J.; Angelini, L.; Davies, R. L.; Kalogera, V.; King, A.R.; Zepf, S.
Citation: Trinchieri , G , Pellegrini , S , Fabbiano , G , Fu , R , Brassington , N , Zezas , A , Kim , D-W , Gallagher , J , Angelini , L , Davies , R L , Kalogera , V , King , A R & Zepf , S 2008 , ' Discovery of Hot Gas in Outflow in NGC 3379 ' Astrophysical Journal , vol 688 , no. 2 , pp. 1000-1008 . , 10.1086/592287
We report the discovery of a faint (LX~4+/-1.5×1037 ergs s-1, 0.5-2 keV), outflowing gaseous hot interstellar medium (ISM) in NGC 3379. This represents the lowest X-ray luminosity ever measured from a hot phase of the ISM in a nearby early-type galaxy. The discovery of the hot ISM in a very deep Chandra observation was possible thanks to its unique spectral and spatial signatures, which distinguish it from the integrated stellar X-ray emission, responsible for most of the unresolved emission in the Chandra data. This hot component is found in a region of ~800 pc in radius at the center of the galaxy and has a total mass M~3+/-1×105 Msolar. Independent theoretical prediction of the characteristics of an ISM in this galaxy, based on the intrinsic properties of NGC 3379, reproduce well the observed luminosity, temperature, and radial distribution and mass of the hot gas, and indicate that the gas is in an outflowing phase, predicted by models but not observed in any system so far.
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