Supernova Remnants: An Odyssey in Space after Stellar death

Supernova Remnants: An Odyssey in Space after Stellar death

Supernova Remnants: An Odyssey in Space after Stellar death

Pierre

1st Abstract

Title (1st Abstract)

X-raying Supernova Remnants in the Magellanic Clouds
First Author

Pierre Maggi
Affiliation

CEA Saclay
Additional Authors

F. Haberl, G. Vasilopoulos, W. Pietsch, J. Greiner / MPE Garching,
P. J. Kavanagh, M. Sasaki / IAAT Tuebingen,
L. M. Bozzetto, M. D. Filipović/ University of Western Sydney ,
S. D. Points / Cerro Tololo Inter-American Observatory,
Y.-H. Chu / Institute of Astronomy and Astrophysics, Academia Sinica, Taipei,
J. Dickel / University of New Mexico,
M. Ehle/ XMM-Newton SOC, ESAC,
R. Williams / Columbus State University Coca-Cola Space Science Center
Presentation options

Oral
Session

7. SNRs as probes and drivers of galaxy structure
1st Abstract

The Magellanic Clouds (MCs) offer an ideal laboratory for the study of the SNR population in star-forming galaxies, since they are relatively nearby and free of large absorption. Both the LMC and SMC have been targeted by large XMM-Newton surveys, which, combined with archival observations, provide the best dataset to systematically study the X-ray emission of their numerous SNRs ($sim 60$ in the LMC, $sim 20$ in the SMC).
In this talk, I will highlight the results from this homogeneous analysis, which allows for the first time meaningful comparisons of temperature, chemical composition, and luminosity of SNRs in the MCs. The SNRs can be used as probes of their host galaxies: We measured chemical abundances in the hot phase of the LMC, and constrained the ratio of core-collapse to type Ia SN rates. The X-ray luminosity function of SNRs in the MCs are compared to those in other Local Group galaxies with different metallicities and star formation properties. Finally, we present a new population of evolved type Ia SNRs that was discovered recently in the MCs via their iron-rich X-ray emission.

2nd Abstract

Title (2nd abstract)

Fe K and ejecta emission in SNR G15.9+0.2 with XMM-Newton
First Author (2nd abstract)

Pierre Maggi
Affiliation (2nd abstract)

CEA Saclay
Additional Authors (2nd abstract)

Fabio Acero / CEA Saclay
Session (2nd abstract)

1. Radiation studies from gamma-rays to radio in Galactic and Extragalactic SNRs
2nd Abstract

We present a study of the Galactic supernova remnant SNR G15.9+0.2 with archival XMM-Newton observations. Using EPIC’s collective power, we report for the first time the detection of Fe K line emission from SNR G15.9+0.2. We measure the line properties (e.g. centroid energy and width) and find evidence for spatial variations. We discuss how SNR G15.9+0.2 fits within the current sample of SNRs with detected Fe K emission and found that it is the core-collapse SNR with the lowest Fe K centroid energy. We also present some
caveats to the use of Fe K line centroid energies as typing tools for SNRs. We analyse the emission-line rich X-ray spectra extracted from various regions. The abundances of Mg, Si, S, Ar, and Ca are super-solar and their ratios strongly suggests that the progenitor of SNR G15.9+0.2 was a massive star, strengthening the physical association to a candidate Central Compact Object detected with Chandra. Using the absorption column density and ambient medium density constrained by the X-ray spectral analysis, we revise the measurements of the age and distance to the SNR.
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