Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/31604
Title: | Deciphering the nature of the pulsar wind nebula CTB 87 with XMM-Newton | Authors: | Guest, B. Safi-Harb, S. MacMaster, A. Kothes, R. Olmi, Barbara AMATO, Elena BUCCIANTINI, NICCOLO' Arzoumanian, Z. |
Issue Date: | 2020 | Journal: | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | Number: | 491 | Issue: | 2 | First Page: | 3013 | Abstract: | CTB 87 (G74.9+1.2) is an evolved supernova remnant (SNR) which hosts a peculiar pulsar wind nebula (PWN). The X-ray peak is offset from that observed in radio and lies towards the edge of the radio nebula. The putative pulsar, CXOU J201609.2+371110, was first resolved with Chandra and is surrounded by a compact and a more extended X-ray nebula. Here, we use a deep XMM-Newton observation to examine the morphology and evolutionary stage of the PWN and to search for thermal emission expected from a supernova shell or reverse shock interaction with supernova ejecta. We do not find evidence of thermal X-ray emission from the SNR and place an upper limit on the electron density of 0.05 cm<SUP>-3</SUP> for a plasma temperature kT ∼ 0.8 keV. The morphology and spectral properties are consistent with a ∼20-kyr-old relic PWN expanding into a stellar wind-blown bubble. We also present the first X-ray spectral index map from the PWN and show that we can reproduce its morphology by means of 2D axisymmetric relativistic hydrodynamical simulations. | URI: | http://hdl.handle.net/20.500.12386/31604 | URL: | http://arxiv.org/abs/1911.11829v1 https://academic.oup.com/mnras/article/491/2/3013/5638880 |
ISSN: | 0035-8711 | DOI: | 10.1093/mnras/stz3270 | Bibcode ADS: | 2020MNRAS.491.3013G | Fulltext: | open |
Appears in Collections: | 1.01 Articoli in rivista |
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20Guest.pdf | PDF editoriale | 4.77 MB | Adobe PDF | View/Open |
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