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Artículo

The intriguing nature of the high-energy gamma ray source XSS J12270-4859

De Martino, D.; Falanga, M.; Bonnet-Bidaud, J.-M.; Belloni, T.; Mouchet, M.; Masetti, N.; Andruchow, IleanaIcon ; Cellone, Sergio AldoIcon ; Mukai, K.; Matt, G.
Fecha de publicación: 06/2010
Editorial: EDP Sciences
Revista: Astronomy and Astrophysics
ISSN: 0004-6361
Idioma: Inglés
Tipo de recurso: Artículo publicado
Clasificación temática:
Astronomía

Resumen

The nature of the hard X-ray source XSS J12270-4859 is still unclear. It was claimed to be a possible magnetic Cataclysmic Variable of the Intermediate Polar type from its optical spectrum and a possible 860 s X-ray periodicity in RXTE data. However, recent observations do not support the latter variability, leaving this X-ray source still unclassified. To investigate its nature we present a broad-band X-ray and gamma ray study of this source based on a recent XMM-Newton observation and archival INTEGRAL and RXTE data. Using the Fermi/LAT 1-year point source catalogue, we tentatively associate XSS J12270-4859 with 1FGL J1227.9-4852, a source of high energy gamma rays with emission up to 10 GeV. We further complement the study with UV photometry from XMM-Newton and ground-based optical and near-IR photometry. We have analysed both timing and spectral properties in the gamma rays, X-rays, UV and optical/near-IR bands of XSS J12270-4859. The X-ray emission is highly variable showing flares and intensity dips. The flares consist of flare-dip pairs. Flares are detected in both X-rays and UV range whilst the subsequent dips are present only in the X-ray band. Further aperiodic dipping behaviour is observed during X-ray quiescence but not in the UV. The broad-band 0.2--100 keV X-ray/soft gamma ray spectrum is featureless and well described by a power law model with Gamma=1.7. The high energy spectrum from 100 MeV to 10 GeV is represented by a power law index of 2.45. The luminosity ratio between 0.1--100 GeV and 0.2--100 keV is ~ 0.8, indicating that the GeV emission is a significant component of the total energy output. Furthermore, the X-ray spectrum does not greatly change during flares, quiescence and the dips seen in quiescence. The X-ray spectrum however hardens during the post-flare dips, where a partial covering absorber is also required to fit the spectrum. Optical photometry acquired at different epochs reveals a period of 4.32 hr that could be ascribed to the binary orbital period. Near-IR, possibly ellipsoidal, variations are detected. Large amplitude variability on shorter (tens mins) timescales are found to be non-periodic. The observed variability at all wavelengths together with the spectral characteristics strongly favour a low-mass atypical low-luminosity X-ray binary and are against a magnetic Cataclysmic Variable nature. The association with a Fermi/LAT high energy gamma ray source further strengths this interpretation.
Palabras clave: Close Binaries , Xss J12270-4859 (Estrella) , Gamma Rays , X-Ray Binaries , Accretion Disks , 1fglj1227.9-4852 (Estrella)
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info:eu-repo/semantics/openAccess Excepto donde se diga explícitamente, este item se publica bajo la siguiente descripción: Creative Commons Attribution-NonCommercial-ShareAlike 2.5 Unported (CC BY-NC-SA 2.5)
Identificadores
URI: http://hdl.handle.net/11336/69966
DOI: http://dx.doi.org/10.1051/0004-6361/200913802
URL: https://www.aanda.org/articles/aa/abs/2010/07/aa13802-09/aa13802-09.html
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Citación
De Martino, D.; Falanga, M.; Bonnet-Bidaud, J.-M.; Belloni, T.; Mouchet, M.; et al.; The intriguing nature of the high-energy gamma ray source XSS J12270-4859; EDP Sciences; Astronomy and Astrophysics; 515; 6-2010; 25-36
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