The Hot Interstellar Medium of the Interacting Galaxy NGC 4490
Richings, A.J.; Fabbiano, G.; Wang, J.; Roberts, T.P.
Professor Tim Roberts email@example.com
We present an analysis of the hot interstellar medium (ISM) in the spiral galaxy NGC 4490, which is interacting with the irregular galaxy NGC 4485, using ~100 ks of Chandra ACIS-S observations. The high angular resolution of Chandra enables us to remove discrete sources and perform spatially resolved spectroscopy for the star-forming regions and associated outflows, allowing us to look at how the physical properties of the hot ISM such as temperature, hydrogen column density, and metal abundances vary throughout these galaxies. We find temperatures of >0.41 keV and 0.85+0.59 –0.12 keV, electron densities of >1.87η–1/2 × 10–3 cm–3 and 0.21+0.03 –0.04η–1/2 × 10–3 cm–3, and hot gas masses of >1.1η1/2 × 107 M ☉ and ~3.7η1/2 × 107 M ☉ in the plane and halo of NGC 4490, respectively, where η is the filling factor of the hot gas. The abundance ratios of Ne, Mg, and Si with respect to Fe are found to be consistent with those predicted by theoretical models of type II supernovae (SNe). The thermal energy in the hot ISM is ~5% of the total mechanical energy input from SNe, so it is likely that the hot ISM has been enriched and heated by type II SNe. The X-ray emission is anticorrelated with the Hα and mid-infrared emission, suggesting that the hot gas is bounded by filaments of cooler ionized hydrogen mixed with warm dust.
Richings, A., Fabbiano, G., Wang, J., & Roberts, T. (2010). The Hot Interstellar Medium of the Interacting Galaxy NGC 4490. Astrophysical Journal, 723(2), 1375-1392. https://doi.org/10.1088/0004-637x/723/2/1375
|Journal Article Type||Article|
|Publication Date||Nov 10, 2010|
|Deposit Date||Jan 30, 2012|
|Publicly Available Date||Jan 8, 2014|
|Publisher||American Astronomical Society|
|Peer Reviewed||Peer Reviewed|
|Keywords||Galaxies, Individual (NGC 4485/90), Interactions, ISM, X-rays, ISM.|
Published Journal Article
© 2010. The American Astronomical Society. All rights reserved. Printed in the U.S.A.
You might also like
The hyperluminous X‐ray source population
Unveiling the disc structure in ultraluminous X-ray source NGC 55 ULX-1
The variability behavior of NGC 925 ULX-3
A transient ultraluminous X-ray source in NGC 55