No abstract
We present high-resolution near-infrared images of the Seyfert 2 galaxy IC 5063 obtained using the NearInfrared Camera and Multiobject Spectrometer (NICMOS) in broadband filters at 1.1, 1.6, and 2.2 mm (FWHM ≈ 0Љ .21 at 2.2 mm). The images show a very red, unresolved point source at the center of the galaxy, confirming the existence of the obscured active nucleus inferred from previous ground-based studies. The 2.2 mm flux, supplemented with ground-based LЈ-band observations, suggests thermal emission equivalent to a blackbody at a temperature of 720 K. We ascribe the emission not to direct light from the nucleus, but to hot dust in the inner part of the torus. The 1.6 mm emission is only minimally affected by the hot dust emission. The luminosity of the central source producing most of the 1.6 mm emission, not corrected for extinction, is ergs s , integrated over the F160W filter only.41 Ϫ1 # 10We also present lower spatial resolution images of IC 5063 obtained with NICMOS in the emission lines of [Fe ii] l1.644 mm, Paa l1.8756 mm, and H 2 l2.1218 mm. These images reveal a linear emission morphology comprised of two bright knots, separated by 1Љ .8 on either side of a central knot that is at the location of the continuum nucleus. A comparison with high-resolution radio continuum maps shows that there is a one-to-one spatial correspondence between the radio lobes and the emission-line knots, directly implying that the [Fe ii] and H 2 emission is created by fast shocks produced by the advancing radio jets. The asymmetry in the [Fe ii]/H 2 ratio may suggest a difference in either the shock velocities or the molecular mass on the two sides of the nucleus.
The ,,Spectral Radar" is an optical sensor for tomography, working in the Fourier domain, rather than in time domain. The scattering amplitude a(z) along one vertical axis from the surface into the bulk can be measured within one exposure. No reference arm scanning is necessary. One important property of optical coherence tomography (OCT) sensors is the dynamic range. We will compare the dynamic range of the spectral radar with standard OCT. The influence of the Fourier transformation on the dynamic range of the Spectral Radar will be discussed. The dinical relevance of the in vivo measurements will be demonstrated.
We have discovered an extremely red object, LSF 1, located 7 00 southwest (P.A. 217) of the bright spectroscopic binary system HD 155826. Originally reported by IRAS as one source detected at 12-60 lm, and found as a single 6-25 lm source of similar flux in the Midcourse Space Experiment Galactic plane survey, two bright point sources were found in arcsecond resolution infrared images obtained with the MIRLIN camera at the Infrared Telescope Facility and confirmed by the Long Wavelength Spectrometer camera on Keck I. While HD 155826 itself was easily detected in all the broadband and narrowband filters from 0.9 to 12 lm that we used, the new counterpart, LSF 1, is only visible at 10 lm. In Gunn z, J, H, and K 0 , the upper limit to the new object's magnitude is $14. The detection of the new bright IR source explains the confusing [K]-[N] IRAS colors that originally implied that HD 155826 was a possible Vega-like system. The '' anomalous long-wavelength emission '' is found to arise entirely from the new source. Without mid-IR extension or excess long-wavelength emission, HD 155826 should no longer be classified as a Vega-like system. We suspect LSF 1 to be either a highly reddened carbon star or a Class II YSO, with no association with the high proper motion HD 155826 system.
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