paper

A Chandra Survey of Early-Type Galaxies, I: Metal Enrichment in the ISM

arXiv:astro-ph/0504008 · doi:10.1086/499323

Abstract

We present the first in a series of papers studying the X-ray properties of 28 early type galaxies spanning ~3 orders of magnitude in L_x. We report emission-weighted constraints for Fe, O, Ne, Mg, Si, S and Ni. We find no evidence of the very sub-solar Z_Fe historically reported, confirming a trend in recent X-ray observations of bright galaxies and groups, nor do we find Z_Fe correlates with L_x. In general we find no evidence for multi-phase ISM, indicating multi-temperature fits found with ASCA were due to temperature gradients Chandra can resolve. We compare the stellar Z_Fe, estimated from simple stellar population model fits, to Z_Fe(ISM). Excepting one possible outlier we find no evidence that the gas is much more metal-poor than the stars and, in a few systems Z_Fe(ISM) is higher. In general the two exhibit similar Z_Fe, which is inconsistent with both galactic wind models and recent hierarchical chemical enrichment simulations. Adopting standard SNIa and SNII metal yields our abundance ratio constraints imply 66+/-11% of the Fe within the ISM was produced in SNIa, similar to the Solar neighbourhood and implying similar enrichment histories for the ISM in a spiral and in elliptical galaxies. Although these values are sensitive to systematic uncertainties in the SN yields, they are in good agreement with observations of more massive systems, indicating remarkable homology in the enrichment process operating from cluster scales to low-to-intermediate L_x galaxies. The data also uniformly exhibit the low Z_O/Z_Mg abundance ratios which have been reported in some other systems. This is inconsistent with metal-production calculations in SNII and may indicate an additional source of enrichment, such as Population III hypernovae.(abridged)

Accepted for publication in the Astrophysical Journal. 23 pages, 6 figures. Mostly minor changes to match published version. Expanded correlation discussion. Conclusions unchanged

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