Stuart Bowyer
The ultraviolet band of the spectrum is generally defined as
extending from the end of the soft sky x-ray band at 100 Å to the
cutoff imposed by the transmission of the atmosphere at ~ 3000 Å. It is
best divided into two separate bands: the extreme ultraviolet (EUV)
from 100- ~ 1000 Å and the far ultraviolet (FUV) from
1000-3000Å. If one
considers the cosmic ultraviolet background , each of these bands is
sampling vastly different regions; the EUV background is expected to
be produced by emission from the hot component of the local
interstellar medium, whereas the FUV background could be produced by a
variety of mechanisms in our galaxy and may have contributions from a
variety of exotic and cosmological processes. Studies of the EUV
background are in their infancy but show great promise. The FUV
background has been the subject of a substantial amount of work from
the beginning of space research. The subset of the FUV band from
~ 1300-2000 Å has been studied most extensively. Scattering from the
very intense, diffuse hydrogen Lyman
From the beginnings of space research, attempts were made to measure
the cosmic FUV background. This work was strongly motivated by the
hope that in this waveband a true extragalactic flux could be detected
and characterized. Theoretical speculation as to possible sources for
this radiation was unconstrained by the available data and included
such diverse processes as emission from a lukewarm intergalactic
medium, emission from hot gas produced in a protogalaxy collapse phase
in the early universe, the summed emission from a star formation burst
phase in young galaxies, and photons from the electromagnetic decay of
real or hypothetical exotic particles that were produced, or may have
been produced, in the early universe.
It was the expectation that all of the problems that had bedeviled
attempts to measure the cosmic extragalactic flux in the optical band
would be overcome: The zodiacal light would be absent because the
Sun's radiation falls rapidly in the ultraviolet, the measurements
would be made above the atmospheric airglow, and the difficulty of
separating the diffuse background radiation from that produced by
stars would be reduced or even eliminated because the UV-producing
early stars would be limited to the Galactic plane.
The first 20 years of measurements, carried out by a number of
groups in at least five major countries, indicated that the flux was
uniform across the celestial sphere and hence was cosmological in
origin. Estimates of the intensity of this flux, however, varied by
three orders of magnitude with no clustering around a mean. In
retrospect, there are a number of reasons for these discrepant
results; perhaps it is most useful to state that these results provide
empirical evidence that measurements of this type are intrinsically
difficult.
A turning point in the study of this background occurred in 1980
when data obtained with a FUV channel of a telescope flown as part of
the Apollo-Soyuz mission were analyzed and published. These data
exhibited a correlation between intensity of the background and
galactic neutral hydrogen column as derived from 21-cm radio
measurements. Although these initial results were criticized on a
variety of grounds, they were quickly confirmed by independent rocket
and satellite measurements. The intensities obtained in these
experiments were consistent within a factor of 2, and they varied from
roughly 200-1500 photons cm-2 s-1 sr-1
Å-1 depending upon the galactic
hydrogen column. These results showed that the vast majority of the
FUV flux was connected with processes in our Milky Way galaxy and was
not, in fact, extragalactic in origin. Nonetheless, all of the data
sets were consistent with a small part of this flux being
isotropic. However, there was no way to determine whether this
component was due to residual airglow processes at satellite
altitudes, due to processes occurring within the galaxy, or was
extragalactic in origin.
In the first half of the 1980s, a variety of processes was suggested
as possible sources for the galactic component of this radiation,
including starlight scattered by dust, molecular hydrogen emission,
line emission from a hot (~ 105 K) interstellar gas, two-photon
recombination radiation, and others. A variety of extragalactic
processes was suggested as the source of the small isotropic
component. Given the character of the existing data; there was no way
to establish which, if any, of the processes mentioned previously were
contributing to the FUV background. Two experiments carried out in the
second half of the 1980s proved to be especially productive in
establishing the sources of this radiation.
The first of these was a FUV imaging detector flown as a piggyback
experiment at the focal plane of a 1-m EUV/FUV telescope developed as a
collaborative effort between the United States and Germany. Data from
this imager were subjected to a power spectrum analysis in a search
for any component of the FUV background flux that was correlated with
angular separation. This search was motivated by the fact that
galaxies are known to cluster, and the scale of this clustering is
well characterized by a two-point correlation function derived from
optical data. A component of the FUV background was, in fact, found
with the same angular correlation as that found in the optical,
leading to the conclusion that this component is indeed extragalactic
in origin and is the summed flux of galaxies at great
distances. Because of the cosmological redshift, the FUV flux emitted
by galaxies is shifted out of the observed FUV band at distances
corresponding to about one-third of a Hubble time.
The detection of a cosmological component has an important
astrophysical consequence. The intensity of this flux (about 50
photons cm-2 s-1 sr-1
Å-1) is consistent only with a relatively low
and constant star formation rate in galaxies for the time scales
indicated. It also limits so-called star burst galaxies to be less
than 10% of the total population of galaxies in this period.
A second major experiment that provided a variety of new data
relevant to this field was a FUV diffuse spectrometer which flew in
1986 on the last shuttle flight before the Challenger tragedy. This
instrument was sensitive from about 1350-1850 Å with about 16 Å
resolution. Astronomical data were obtained from eight different
directions in the celestial sphere with a wide range of neutral
hydrogen column densities.
Several important results came from the study of the data obtained
with this instrument. Emission lines from a collisionally excited hot
(~ 105 K) gas in the interstellar medium were discovered. Combining
these results with absorption data obtained with the International
Ultraviolet Explorer proved the existence of the long-postulated, but
unproven, hot galactic halo. The mass infall rate of ~ 10
M
The cosmic FUV flux from 1400-1850 Å is shown in
Fig. 1. The lower
curve shows the spectrum in a direction of low neutral hydrogen
column. A variety of processes contributes to this flux; the most
intense spectral lines are emitted by the hot interstellar medium. The
upper curve shows the spectrum in a direction of higher neutral
hydrogen column. The majority of this radiation is starlight scattered
by dust in the interstellar medium, but other processes also
contribute to this flux.
Early attempts at measurements of the cosmic EUV background were
made with broadband filters which included the resonantly scattered
solar lines of He II at 304 Å and He I at 584 Å. These lines, whose
study is important in its own right, dominated the data and made
estimates of a truly cosmic flux impossible. The first useful
estimates of the cosmic diffuse EUV background below 500 Å were
obtained with an EUV telescope flown on the Apollo-Soyuz
mission. These data were also obtained with a broadband filter, but
they had an important advantage over previous results, in that a small
field of view was employed and a very extensive data set was
obtained. The geocoronal ionized helium responsible for scattering the
He II 304 Å flux is confined to a few Earth radii by the Earth's
magnetic field. In the antisolar direction, the Earth's shadow leaves
the helium in darkness, greatly reducing the scattered intensity. By
analyzing the extensive data obtained in the antisolar direction,
significant upper limits to this flux were obtained.
Several broadband measurements of the EUV background have been made
at wavelengths longer that 500 Å. In addition to measurements in the
500-800 Å band, several groups have obtained upper limits to the
diffuse flux from 912-1080 Å with instruments with relatively narrow
bandpasses.
Two relatively coarse spectrographic measurements of the cosmic EUV
background have been carried out. High galactic latitude observations
were obtained with 40 Å resolution during the interplanetary cruise
phase of the Voyager 2 mission near the orbit of Saturn. The EUV part
of these observations was dominated by the solar He I 584 Å flux
resonantly scattered from neutral helium flowing through the solar
system. The effects of this bright He I line, along with several other
sources of background, were removed from the raw spectra by analysis,
and upper limits to the EUV background were derived.
Spectroscopy of the diffuse EUV background below 500 Å is in its
infancy. Grazing incidence optics must be used in order to obtain any
reasonable throughput, and grazing incidence spectrometers from
diffuse radiation are technically difficult. An instrument that was
flown on a sounding rocket in 1986 obtained upper limits on the EUV
flux from 90-700 Å with about 20 Å resolution. The existing data on
the diffuse cosmic EUV background are shown in
Fig. 2.
Investigations of the FUV background were initiated in the early
phases of space astronomy. Substantial efforts were devoted to this
work with disparate results. The discovery that most of this flux is
produced within our galaxy opened a new chapter in the study of this
radiation. Subsequent work in this field has established the
existence and character of the hot galactic halo, has provided limits
on the star formation rate in the universe for the last third of a
Hubble time, and has defined the character of a component of
interstellar dust. Future work in this field will explore questions
such as: Why is this flux only roughly, and not exactly, correlated
with neutral hydrogen column? Is this correlation the same in all
directions of the sky? What is the true extragalactic background
level? What is the correlation of the FUV background with the infrared
background? and higher-order questions. Answers to these questions
will certainly lead us to new insights about our galaxy and the
universe. The exploration of the cosmic EUV background is in its
infancy, and the existing data are only suggestive of the underlying
processes believed to be in operation. Another order of magnitude in
sensitivity and spectral resolution may be required for these studies
to provide definitive results.
BACKGROUND RADIATION, ULTRAVIOLET
line at 1216 Å, which would
severely compromise any observational data, can be eliminated through
the use of crystal filters that block all radiation below ~ 1300
Å. Longward of 2000 Å, zodiacal light contributes strongly to the
background in a complex and as yet poorly determined manner, and it is
extremely difficult to separate the stellar contribution from the
truly diffuse flux. It is a statement of the difficulty of this work
that despite considerable effort substantial progress in our
understanding of this background has only recently been achieved. This
effort has clearly been worthwhile; recent results provide information
on such diverse topics as the character of the long-prophesied but
never established galactic halo, star formation rates in the universe,
and the character of dust in our galaxy.
THE COSMIC FAR ULTRAVIOLET BACKGROUND
yr
requires that this halo must be continually replenished, which
provides direct experimental confirmation of the ``galactic fountain''
model of the galactic halo gas. Data obtained with this instrument on
FUV radiation scattered from dust in directions with relatively high
column densities of neutral hydrogen showed that this dust has a
relatively low albedo (
0.2) and that it scatters
FUV radiation
almost isotropically, indicating the dust itself is relatively small
and roughly spherical. There are strong indications that at least
traces of this dust are present everywhere, including regions in
directions of very low hydrogen column density.
THE COSMIC EXTREME ULTRAVIOLET BACKGROUND
CONCLUSIONS