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Title:
Near-Infrared and Optical Limits for the Central X-Ray Point Source in the Cassiopeia A Supernova Remnant
Authors:
Fesen, R. A.; Pavlov, G. G.; Sanwal, D.
Affiliation:
AA(6127 Wilder Laboratory, Department of Physics and Astronomy, Dartmouth College, Hanover, NH 03755; .), AB(Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802; , .), AC(Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802; , .)
Publication:
The Astrophysical Journal, Volume 636, Issue 2, pp. 848-858. (ApJ Homepage)
Publication Date:
01/2006
Origin:
UCP
ApJ Keywords:
ISM: Individual: Name: Cassiopeia A, Stars: Neutron, ISM: Supernova Remnants, X-Rays: Stars
DOI:
10.1086/498087
Bibliographic Code:
2006ApJ...636..848F

Abstract

We set new near-infrared and optical magnitude limits for the central X-ray point source (XPS) in the Cassiopeia A supernova remnant based on HST images. Near-infrared images of the center of Cas A taken with the NICMOS 2 camera in combination with the F110W and F160W filters (~J and H bands) have magnitude limits >=26.2 and >=24.6, respectively. These images reveal no sources within a 1.2" radius (corresponding to a 99% confidence limit) of the Chandra XPS position. The NICMOS data, taken together with broadband optical magnitude limits (R~28 mag) obtained from a deep STIS CCD exposure taken with a clear filter (50CCD), indicate that the XPS luminosities are very low in the optical/NIR bands (e.g., LH<3×1029 ergs s-1) with no optical, J-, or H-band counterpart to the XPS easily detectable by HST. The closest detected object lies 1.8" from the XPS's nominal coordinates, with magnitudes R=25.7, mF110W=21.9, and mF160W=20.6, and is a foreground, late-type star as suggested by Kaplan, Kulkarni, and Murray. We discuss the nature of the Cas A central compact object on the basis of these near-infrared and optical flux limits.

Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. These observations are associated with programs GO-8692 and GO-9798.

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