UIT Observations of the Halo of NGC 891

Details UIT Observations of the Halo of NGC 891 UIT Observations of the Halo of NGC 891

Dec 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aas...183.1908b&link_type=abstract

American Astronomical Society, 183rd AAS Meeting, #19.08; Bulletin of the American Astronomical Society, Vol. 25, p.1323

Astronomy and Astrophysics

Astronomy

Scientific paper

We present an observation of the edge-on Sb galaxy NGC 891 taken by Ultraviolet Imaging Telescope during the ASTRO 1 mission with a broad mid-UV filter with half power points at 1800 Angstroms and 3100 Angstroms. We compare the emission seen in this image with the emission seen in the ground--based optical Hα and [S II] lambda lambda 6717,6731 images of Rand, Kulkarni and Hester (ApJ 362, L1--L4). The mid-UV emission is brightest along a thin plane corresponding to the major axis of the galaxy. The mid-UV surface brightness of the disk, measured with the center of the galaxy masked out, has a scale height of 0.6 kpc. Emission in the disk is asymmetrically concentrated to the NE of the galaxy center, in rough correspondence with the Hα emission from young star forming regions. Diffuse mid-UV emission is detectable in the halo; there are no obvious discrete features, although the signal to noise is low. The emission in the bulge has a scale height of 1.7 kpc, which is in good agreement with the Hα scale height of 1.4 kpc. There are no strong emission lines in the mid-UV band, however, so the radiation here is probably dominated by dust scattering of light from the disk. The halo gas appears to contain significant amounts of dust.

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