Volume 555, July 2013
|Number of page(s)||9|
|Section||Interstellar and circumstellar matter|
|Published online||18 June 2013|
The most complete and detailed X-ray view of the SNR Puppis A⋆
1 Instituto de Astronomía y Física del Espacio (IAFE), UBA-CONICET, CC 67, Suc. 28, 1428 Buenos Aires, Argentina
2 XMM-Newton Science Operations Centre, ESAC, Villafranca del Castillo, 28080 Madrid, Spain
3 ISDEFE, Calle de Beatriz, 3, 28040 Madrid, Spain
4 Telespazio Vega U.K. S.L.
5 FADU, University of Buenos Aires, 1428 Buenos Aires, Argentina
Received: 4 March 2013
Accepted: 29 April 2013
Aims. With the purpose of producing the first detailed full view of Puppis A in X-rays, we carried out new XMM-Newton observations covering the missing regions in the southern half of the supernova remnant (SNR) and combined them with existing XMM-Newton and Chandra data.
Methods. Two pointings toward the south and southwest of Puppis A were observed with XMM-Newton. We combined these data with archival XMM-Newton and Chandra data and produced images in the 0.3−0.7, 0.7−1.0, and 1.0−8.0 energy bands.
Results. We present the first sensitive complete X-ray image of Puppis A. We investigated its morphology in detail, carried out a multiwavelength analysis, and estimated the flux density and luminosity of the whole SNR. The complex structure observed across the remnant confirms that Puppis A evolves in an inhomogeneous, probably knotty interstellar medium. The southwestern corner includes filaments that perfectly correlate with radio features suggested to be associated with shock/cloud interaction. In the northern half of Puppis A the comparison with Spitzer infrared images shows an excellent correspondence between X-rays and 24 and 70 μm emission features, while to the south there are some matched and other unmatched features. X-ray flux densities of 12.6 × 10-9,6.2 × 10-9, and 2.8 × 10-9 erg cm-2 s-1 were derived for the 0.3−0.7, 0.7−1.0, and 1.0−8.0 keV bands, respectively. At the assumed distance of 2.2 kpc, the total X-ray luminosity between 0.3 and 8.0 keV is 1.2 × 1037 erg s-1. We also collected and updated the broad-band data of Puppis A between radio and GeV γ-ray range, producing its spectral energy distribution. To provide constraints to the high-energy emission models, we re-analyzed radio data, estimating the energy content in accelerated particles to be Umin = 4.8 × 1049 erg and the magnetic field strength B ~ 26 μG.
Key words: ISM: supernova remnants / X-rays: ISM / ISM: individual objects: Puppis A
© ESO, 2013
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.