TY - JOUR
T1 - SHOCK-cloud interaction and particle acceleration in the southwestern limb of sn 1006
AU - Miceli, Marco
AU - Acero, null
AU - Bocchino, null
AU - Decourchelle, null
AU - Dubner, null
AU - Orlando, null
AU - Miceli, null
PY - 2014
Y1 - 2014
N2 - The supernova remnant SN 1006 is a powerful source of high-energy particles and evolves in a relatively tenuous and uniform environment despite interacting with an atomic cloud in its northwestern limb. The X-ray image of SN 1006 reveals an indentation in the southwestern part of the shock front and the H I maps show an isolated (southwestern) cloud, having the same velocity as the northwestern cloud, whose morphology fits perfectly in the indentation. We performed spatially resolved spectral analysis of a set of small regions in the southwestern nonthermal limb and studied the deep X-ray spectra obtained within the XMM-Newton SN 1006 Large Program. We also analyzed archive H I data, obtained by combining single-dish and interferometric observations. We found that the best-fit value of N H derived from the X-ray spectra significantly increases in regions corresponding to the southwestern cloud, while the cutoff energy of the synchrotron emission decreases. The N H variation corresponds perfectly with the H I column density of the southwestern cloud, as measured from the radio data. The decrease in the cutoff energy at the indentation clearly reveals that the back side of the cloud is actually interacting with the remnant. The southwestern limb therefore presents a unique combination of efficient particle acceleration and high ambient density, thus being the most promising region for γ-ray hadronic emission in SN 1006. We estimate that such emission will be detectable with the Fermi telescope within a few years. © 2014. The American Astronomical Society. All rights reserved..
AB - The supernova remnant SN 1006 is a powerful source of high-energy particles and evolves in a relatively tenuous and uniform environment despite interacting with an atomic cloud in its northwestern limb. The X-ray image of SN 1006 reveals an indentation in the southwestern part of the shock front and the H I maps show an isolated (southwestern) cloud, having the same velocity as the northwestern cloud, whose morphology fits perfectly in the indentation. We performed spatially resolved spectral analysis of a set of small regions in the southwestern nonthermal limb and studied the deep X-ray spectra obtained within the XMM-Newton SN 1006 Large Program. We also analyzed archive H I data, obtained by combining single-dish and interferometric observations. We found that the best-fit value of N H derived from the X-ray spectra significantly increases in regions corresponding to the southwestern cloud, while the cutoff energy of the synchrotron emission decreases. The N H variation corresponds perfectly with the H I column density of the southwestern cloud, as measured from the radio data. The decrease in the cutoff energy at the indentation clearly reveals that the back side of the cloud is actually interacting with the remnant. The southwestern limb therefore presents a unique combination of efficient particle acceleration and high ambient density, thus being the most promising region for γ-ray hadronic emission in SN 1006. We estimate that such emission will be detectable with the Fermi telescope within a few years. © 2014. The American Astronomical Society. All rights reserved..
KW - Astronomy and Astrophysics
KW - ISM: clouds
KW - ISM: individual objects (SN 1006)
KW - ISM: supernova remnants
KW - Space and Planetary Science
KW - X-rays: ISM
KW - acceleration of particles
KW - Astronomy and Astrophysics
KW - ISM: clouds
KW - ISM: individual objects (SN 1006)
KW - ISM: supernova remnants
KW - Space and Planetary Science
KW - X-rays: ISM
KW - acceleration of particles
UR - http://hdl.handle.net/10447/128484
UR - http://iopscience.iop.org/2041-8205/782/2/L33/pdf/2041-8205_782_2_L33.pdf
M3 - Article
VL - 782
SP - L33-
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
SN - 2041-8205
ER -