|Annu. Rev. Astron. Astrophys. 1991. 29:
Copyright © 1991 by . All rights reserved
6.2 The Far Ultraviolet Background from Galaxies
Spatial information on very weak far ultraviolet sources was obtained by Martin and Bowyer (1989) with an imaging detector sensitive over the band 1350 to 1900 Å. This detector was flown at the focal plane of a 1 m extreme ultraviolet/far ultraviolet telescope developed as a collaborative effort between Berkeley and Tübingen (Grewing et al. 1983). Data from this imager were subjected to a radial power spectrum analysis in a search for a component of the far ultraviolet background flux which was correlated with angular separation. This search was motivated by the fact that field stars are essentially randomly distributed in angular separation on the sky, whereas galaxies are known to cluster, and the scale of this clustering is well characterized by a two-point correlation function derived from optical data (Peebles 1980). The results obtained by Martin and Bowyer (1989) are shown in Figure 9. Here the observed radial power spectrum of the flux is plotted against angular frequency. The best-fit line to the data is a power law with index -1.6, but given the limited dynamic range of the measurement, this result is not well constrained. The solid line shows a power law with an index of -1.2, which is consistent with the data and is expected from the integrated light of galaxies. Any alternate processes producing this power would not only have to be the result of a spurious unknown effect, but would also have to produce, purely by chance, a power spectrum consistent with that produced by galaxies. One may thus conclude that this component of the far ultraviolet background (~ 50 CU in intensity) is indeed the summed flux of galaxies. The far ultraviolet flux emitted by galaxies contributing to this component of the background is emitted by galaxies in the redshift range from 0.1 to 0.6. This flux is shifted out of the observed far ultraviolet band at distances corresponding to times earlier than the most recent one-third of a Hubble time.
|Figure 9. Results obtained by Martin & Bowyer (1989) on the spatial distribution of weak far ultraviolet sources. Here the radial power spectrum of the sources is plotted against angular frequency. Stars contribute a noncorrelated, white noise component to this data. The best-fit line is a power law with index -1.6, but, given the limited dynamic range of the measurement, this result is not well constrained. The solid line shows a power law with an index of -1.2, which is consistent with the data and is what is expected from the integrated light of galaxies.|
Hurwitz, Bowyer, and Martin (1991) obtained indirect evidence for an extragalactic component of the far ultraviolet background from an analysis of the data obtained with the Berkeley UVX spectrometer. In their analysis of the continuum emission, they folded a model of the Galactic stellar radiation field with the observational data and solved for four independent variables: (a) the albedo of the dust, (b) the scattering phase function of the dust, (c) residual dust at NHI = 0, and (d) an ``external'' flux assumed to be independent of the Galactic radiation field and to be isotropic except for attenuation by foreground dust. The results of this analysis for the albedo and scattering phase function of the dust were discussed earlier in this review. The ``external'' flux in this analysis has at least three components. One component is emission at 1550 and 1660 Å, with an intensity consistent with that reported by Martin and Bowyer (1990) for CIV and OIII] produced in the Galactic halo. Since the flux is produced well above the plane, this result provides a consistency check on the analysis. The second component of ``external'' flux is emission of ~ 120 CU over the entire wavelength band. Diffuse H emission line studies (Reynolds 1990) indicate that two-photon emission from a warm ionized medium with a large-scale height will contribute a continuum of about 50 CU in the far ultraviolet at high Galactic latitudes, which will appear in this analysis as an ``external'' flux. The remaining flux is consistent with the value obtained directly by Martin and Bowyer (1989) as the summed flux of external galaxies.
The intensity of the summed ultraviolet radiation from galaxies has an important astrophysical consequence. The observed intensity is consistent only with a relatively low and constant star formation rate in galaxies corresponding to 0.033 M yr-1 Mpc-3 h-2 for the redshift range 0.1 < z < 0.6. It also limits so-called starburst galaxies to less than 10% of the total population of galaxies in this period.