Clumpy metal concentrations in elliptical galaxies NGC 4374 and NGC 4636

Details Clumpy metal concentrations in elliptical galaxies NGC 4374 and NGC 4636 Clumpy metal concentrations in elliptical galaxies NGC 4374 and NGC 4636

Mar 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010raa....10..220x&link_type=abstract

Research in Astronomy and Astrophysics, Volume 10, Issue 3, pp. 220-226 (2010).

Astronomy and Astrophysics

Astrophysics

2

Scientific paper

We present a high spatial resolution study of metal distributions in the nearby, gas-rich elliptical galaxies NGC 4374 and NGC 4636 with the Chandra ACIS archive data. We define the hardness ratio HRFeL as the ratio of the emission in 0.65-1.4 keV to that in 0.3-0.6 keV and 1.4-3.5 keV (after the magnesium and silicon lines are excluded), and HRcont as the ratio of the emission in 1.4-3.5 keV to that in 0.3-0.6 keV, so that the HRFeL and HRcont maps can be used to trace the iron abundance and gas temperature distributions, respectively. By applying the à Trous wavelet algorithm to the obtained emission hardness ratio maps, we reveal that the HRFeL distributions are highly irregular, exhibiting strong spatial variations on 0.1-1 Re scales, which do not follow the HRcont distributions. Since the effect of temperature variation is small, we conclude that most of the high-HRFeL regions are very likely to possess higher abundances than the ambient gas. We also find that these high-HRFeL substructures are not associated with either the LMXB or globular cluster populations, thus their origins should be related to AGN activity or mergers.

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