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Title:
Near-Infrared Synchrotron Emission from Cassiopeia A
Authors:
Rho, Jeonghee; Reynolds, Stephen P.; Reach, William T.; Jarrett, Tom H.; Allen, Glenn E.; Wilson, John C.
Affiliation:
AA(SIRTF Science Center, California Institute of Technology, MS 220-6, Pasadena, CA 91125; ), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138), AC(SIRTF Science Center/IPAC, California Institute of Technology, MS 220-6, Pasadena, CA 91125), AD(SIRTF Science Center/IPAC, California Institute of Technology, MS 220-6, Pasadena, CA 91125), AE(Center for Space Research, Massachusetts Institute of Technology, 70 Vassar Street, Cambridge, MA 02139-4307), AF(Space Sciences Building, Cornell University, Ithaca, NY 14853)
Publication:
The Astrophysical Journal, Volume 592, Issue 1, pp. 299-310. (ApJ Homepage)
Publication Date:
07/2003
Origin:
UCP
ApJ Keywords:
Acceleration of Particles, ISM: Individual: Name: Cassiopeia A, ISM: Supernova Remnants
DOI:
10.1086/375564
Bibliographic Code:
2003ApJ...592..299R

Abstract

Recent high-energy observations of Cassiopeia A suggest the presence of synchrotron radiation, implying acceleration of cosmic rays by young supernova remnants. We detect synchrotron emission from Cas A in the near-infrared using Two Micron All-Sky Survey (2MASS) and Palomar 200 inch (5.1 m) PFIRCAM observations. The remnant is detected in the J, H, and Ks bands using 2MASS: the Ks band is the brightest, H is moderate, and J is faint. In the J and H bands, bright [Fe II] lines (1.24 and 1.64 μm) are detected spectroscopically. The Palomar observations include Ks-continuum, narrowband 1.64 μm (centered on [Fe II]) and 2.12 μm [centered on H2 (1-0)] images. While the narrowband 1.64 μm image shows filamentary and knotty structures, similar to the optical image, the Ks image shows a relatively smooth, diffuse shell, remarkably similar to the radio image. The H2 image is identical to the Ks-continuum image, with surface brightness reduced as expected for the ratio of filter bandwidths, showing no contribution of H2 lines to the Ks-band image. The broadband near-infrared fluxes of Cas A are generally consistent with, but a few tens of percent higher than, an extrapolation of the radio fluxes. The hardening to higher frequencies is possibly due to nonlinear shock acceleration and/or spectral index variation across the remnant. We show evidence of spectral index variation across Cas A using the ``spectral tomography'' technique. The presence of near-infrared synchrotron radiation requires the rolloff frequency to be higher than 1.5×1014 Hz, implying that electrons are accelerated to energies of at least E=0.3B-1/2mG ergs, or 0.2 TeV. The morphological similarity in diffuse emission between the radio and Ks-band images implies that synchrotron losses are not dominant, or we would expect to see a greater concentration in knots. We also show that dust continuum is not significant in the near-infrared emission of Cas A. Our observations show unambiguous evidence that the near-infrared Ks-band emission of Cas A is from synchrotron emission by accelerated cosmic-ray electrons.
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