Observation of the core of the Perseus cluster with the Einstein solid state spectrometer - Cooling gas and elemental abundances

Details Observation of the core of the Perseus cluster with the Einstein solid state spectrometer - Cooling gas and elemental abundances Observation of the core of the Perseus cluster with the Einstein solid state spectrometer - Cooling gas and elemental abundances

Mar 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...244l..47m&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor, vol. 244, Mar. 1, 1981, p. L47-L51.

Astronomy and Astrophysics

Astrophysics

110

Abundance, Cosmic Gases, Galactic Clusters, Intergalactic Media, X Ray Sources, X Ray Spectra, Astronomical Models, Emission Spectra, Heao 2, Iron, Low Temperature, Silicon, Solid State Devices, Spectrometers, Sulfur

Scientific paper

Solid State Spectrometer observations of the core of the Perseus cluster have resulted in the detection of X-ray emission lines due to Si, S, and Fe. Analysis of the spectrum indicates that the X-ray emission has at least two characteristic temperatures. This is interpreted in the framework of radiative accretion in the core of the cluster. The derived parameters are a cooling time less than or approximately equal to 2 x 10 to the ninth years for the low-temperature gas, a mass accretion rate of approximately 300 solar masses per year, and a characteristic size of 10-20 kpc for the cool gas. The Fe abundance in the core (approximately 0.4) is similar to the Fe abundance averaged over the whole cluster, indicating that Fe emission is not strongly concentrated about NGC 1275. The Si and S abundances are consistent with solar values.

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