ar X iv : a st ro - p h / 04 12 14 8 v 1 6 D ec 2 00 4 350 μ m Galactic Center Dust Observations with SHARC II

ar X iv : a st ro - p h / 98 11 34 8 v 1 2 1 N ov 1 99 8 SHARC 350 μ m Mapping of the Galactic Center from the Caltech Submillimeter Observatory

Using the 20-pixel camera SHARC, we have surveyed the 350 µm emission from a 60 ′ by 12 ′ region in the Galactic center. A comparable region has been observed at 800 µm by Lis & Carlstrom (1994); the SHARC map has better spatial resolution and sensitivity to extended emission, however. This paper introduces several features not visible in prior maps of dust emission. We have detected a 10+ pc b...

ar X iv : a st ro - p h / 04 12 37 4 v 1 1 5 D ec 2 00 4 Infrared emission in radio galaxy NGC 4261

We have analyzed the total and nuclear SED for NGC 4261 and find that the dominant process for the mid-and far-infrared emission in this object is non-thermal emission from the active nucleus. Modeling the emission from the optically detected 300 pc dust disk yields no significant disk contribution at any wavelength. To explain the observations, either the disk has an inflated inner region whic...

ar X iv : a st ro - p h / 06 12 37 8 v 1 1 4 D ec 2 00 6 Magnetic fields , strings and cosmology

ar X iv : a st ro - p h / 04 08 56 1 v 1 3 0 A ug 2 00 4 The Nature of the Variable Galactic Center Source IRS

We report measurements of the light curve of the variable Galactic Center source IRS16SW. The light curve is not consistent with an eclipsing binary or any other obvious variable star. The source may be an example of a high mass variable predicted theoretically but not observed previously.

ar X iv : a st ro - p h / 00 12 22 1 v 1 1 1 D ec 2 00 0 Investigating ULIRGs in the Near - Infrared : Imaging & Spectroscopy

We present imaging and spectroscopic observations of 2 nearby (z < 0.1) ULIRGs from a larger sample, and address the question of whether the JHK continuum colours and slope might be effective probes of the nuclear region in searches for AGN. Certainly there is evidence for significant quantities of hot dust emission at temperatures ∼ > 1000 K; but it may be that rather than pointing to an AGN, ...