ASTR 511 [R. W. O'Connell]


INTRODUCTION TO ULTRAVIOLET ASTRONOMY


Astro on orbit

Astro-2 UV observatory in Shuttle payload bay.


A. THE UV BANDS


B. MOTIVATION FOR UV OBSERVATIONS

The UV contains the highest density (bits per unit wavelength) of astrophysical information on stars and gas. The advantages of the UV include:
  1. Sensitivity to hot continuum sources

  2. Numerous atomic & molecular spectral features

  3. Low sky background

  4. Sensitivity to dust

  5. The UV allows ready isolation of hot components in the presence of dominant cool sources: e.g. stellar chromospheres or hot stars/AGNs in E galaxies.

  6. The restframe UV is shifted to the readily-observed optical window in high redshift (z > 1) galaxies and AGN. E.g. "Lyman-break galaxies". Proper interpretation requires vacuum-UV observations of nearer systems.


C. KEY UV RESEARCH AREAS

D. UV MISSIONS

Historical Gaps:

The Hubble Space Telescope released to orbit after its last servicing mission, May 2009


E. UV INSTRUMENTATION


F. UV DETECTORS


G. SPACE ASTRONOMY: SPECIAL TECHNICAL REQUIREMENTS

Columbia



General references: Web links:



Last modified May 2017 by rwo


Text copyright © 2000-2017 Robert W. O'Connell. Images are in the public domain. All rights reserved. These notes are intended for the private, noncommercial use of students enrolled in Astronomy 511 at the University of Virginia.