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  2. Universidad Nacional de Río Negro
  3. Universidad Nacional de Río Negro
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dc.provenanceUniversidad Nacional de Río Negro-
dc.creatorCombi, Jorge A.-
dc.creatorAlbacete Colombo, Juan F.-
dc.creatorSánchez Ayaso, Estrella-
dc.creatorRomero, Gustavo E.-
dc.creatorMarti, J.-
dc.creatorLuque Escamilla, P. L.-
dc.creatorMuñoz Arjonilla, A. J.-
dc.creatorSánchez Sutil, J. R.-
dc.creatorLópez Santiago, J.-
dc.date2010-09-13-
dc.date.accessioned2020-02-11T14:08:32Z-
dc.date.available2020-02-11T14:08:32Z-
dc.date.issued2010-09-13-
dc.identifierCombi, Jorge A., Albacete Colombo, Juan F., Sánchez Ayaso, Estrella, Romero, Gustavo E., Marti, J. (2010). XMM-Newton detection of the supernova remnant G304.6+0.1 (Kes 17); Edp Sciences; Astronomy And Astrophysics-
dc.identifier1432-0746-
dc.identifier0004-6361-
dc.identifierhttps://www.aanda.org/articles/aa/abs/2010/15/aa13935-09/aa13935-09.html-
dc.identifierhttps://rid.unrn.edu.ar/jspui/handle/20.500.12049/2507-
dc.identifierhttp://dx.doi.org/10.1051/0004-6361/200913935-
dc.identifierhttp://hdl.handle.net/11336/18905-
dc.identifier.urihttp://rodna.bn.gov.ar/jspui/handle/bnmm/575682-
dc.descriptionFil: Combi, Jorge A. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto Argentino de Radioastronomia (i); Argentina.-
dc.descriptionFil: Combi, Jorge A. Universidad de Jaén; España-
dc.descriptionFil: Combi, Jorge A. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina-
dc.descriptionFil: Albacete Colombo, Juan F. Universidad Nacional del Comahue; Argentina-
dc.descriptionFil: Sánchez Ayaso, Estrella. Universidad de Jaén; España-
dc.descriptionFil: Romero, Gustavo E. Provincia de Buenos Aires. Gobernación. Comision de Investigaciones Científicas. Instituto Argentino de Radioastronomía. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto Argentino de Radioastronomia; Argentina-
dc.descriptionFil: Romero, Gustavo E. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; Argentina-
dc.descriptionFil: Marti, J. Universidad de Jaén; España-
dc.descriptionFil: Luque Escamilla, P. L. Escuela Politécnica Superior, Universidad de Jaén. Departamento de Ingeniería Mecánica y Minera; España-
dc.descriptionFil: Muñoz Arjonilla, A. J. Escuela Politécnica Superior, Universidad de Jaén. Departamento de Ingeniería Mecánica y Minera; España-
dc.descriptionFil: Sánchez Sutil, J. R. Escuela Politécnica Superior, Universidad de Jaén. Departamento de Ingeniería Mecánica y Minera; España-
dc.descriptionFil: López Santiago, J. Universidad Complutense de Madrid. Departamento de Astrofísica y Ciencias de la Atmósfera; España-
dc.descriptionAims. We report the first detailed X-ray study of the supernova remnant (SNR) G304.6+0.1, achieved with the XMM-Newton mission. Methods. The powerful imaging capability of XMM-Newton was used to study the X-ray characteristics of the remnant at different energy ranges. The X-ray morphology and spectral properties were analyzed. In addittion, radio and mid-infrared data obtained with the Molonglo Observatory Synthesis Telescope and the Spitzer Space Telescope were used to study the association with the detected X-ray emission and to understand the structure of the SNR at differents wavelengths. Results. The SNR shows an extended and arc-like internal structure in the X-ray band without a compact point-like source inside the remnant. We find a high column density of NH in the range 2.5–3.5 × 1022 cm−2, which supports a relatively distant location (d ≥ 9.7 kpc). The X-ray spectrum exhibits at least three emission lines, indicating that the X-ray emission has a thin thermal plasma origin, although a non-thermal contribution cannot be discarded. The spectra of three different regions (north, center and south) are well represented by a combination of a non-equilibrium ionization (PSHOCK) and a power-law (PL) model. The mid-infrared observations show a bright filamentary structure along the north-south direction coincident with the NW radio shell. This suggests that Kes 17 is propagating in a non-uniform environment with high density and that the shock front is interacting with several adjacent massive molecular clouds. The good correspondence of radio and mid-infrared emissions suggests that the filamentary features are caused by shock compression. The X-ray characteristics and well-known radio parameters indicate that G304.6+0.1 is a middle-aged SNR (2.8−6.4) × 104 yr old and a new member of the recently proposed group of mixed-morphology SNRs.-
dc.formatapplication/pdf-
dc.languageeng-
dc.publisherEdp Sciences-
dc.relation523-
dc.relationAstronomy And Astrophysics-
dc.rightsinfo:eu-repo/semantics/openAccess-
dc.rightshttps://creativecommons.org/licenses/by-nc-sa/4.0/-
dc.sourcereponame:RID-UNRN (UNRN)-
dc.sourceinstname:Universidad Nacional de Río Negro-
dc.sourceinstacron:UNRN-
dc.source.urihttp://hdl.handle.net/11336/18905-
dc.subjectISM: Individual Objects: G304.6+0.1-
dc.subjectISM: Supernova Remnants-
dc.subjectX-rays: ISM-
dc.subjectRadiation Mechanisms: Thermal-
dc.subject.::Ciencias Exactas y Naturales-
dc.titleXMM-Newton detection of the supernova remnant G304.6+0.1 (Kes 17)-
dc.typeinfo:eu-repo/semantics/article-
dc.typeinfo:eu-repo/semantics/publishedVersion-
dc.typeinfo:ar-repo/semantics/articulo-
dc.about-
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