XMM-Newton detection of the supernova remnant G304.6+0.1 (Kes 17)

Aims. 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.Fil: Combi, Jorge Ariel. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico la Plata. Instituto Argentino de Radioastronomia (i); Argentina. Universidad de Jaén; España. Universidad Nacional de la Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Albacete Colombo, Juan Facundo. Universidad Nacional del Comahue; ArgentinaFil: Sánchez Ayaso, Estrella. Universidad de Jaén; EspañaFil: Romero, Gustavo Esteban. 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. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas; ArgentinaFil: Marti, J.. Universidad de Jaén; EspañaFil: Luque Escamilla, P. L.. Escuela Politécnica Superior, Universidad de Jaén. Departamento de Ingeniería Mecánica y Minera; EspañaFil: Muñoz Arjonilla, A. J.. Escuela Politécnica Superior, Universidad de Jaén. Departamento de Ingeniería Mecánica y Minera; EspañaFil: Sánchez Sutil, J. R.. Escuela Politécnica Superior, Universidad de Jaén. Departamento de Ingeniería Mecánica y Minera; EspañaFil: López Santiago, J.. Universidad Complutense de Madrid. Departamento de Astrofísica y Ciencias de la Atmósfera; Españ