6. DISCUSSION
A discussion of our photometry and a quantitative analysis of UV/optical
galaxy morphologies will be presented in later papers. Here, we
summarize the more important trends regarding the UV morphologies of
galaxies which have emerged from our data and related studies.
- UV morphologies are usually significantly different from visible
band morphologies. This is a consequence of spatially inhomogeneous
stellar populations. Differences are most pronounced for systems in the
middle range of Hubble types, Sa to Sc. Objects at the extremes of the
Hubble sequence (ellipticals or very late disk systems and irregulars)
tend to have more homogeneous populations and therefore less dramatic
wavelength-dependent morphology.
- Although elliptical galaxies and large spiral bulges are fainter in
the far-UV than the optical bands by factors of ~ 6-60 (in flux per unit
wavelength), nonetheless they are much brighter than expected from the
cool ~ 1 M
turnoff stars in the dominant population. Their optical and UV axis
ratios are similar, though they are usually much more compact in the
UV. They exhibit smooth UV profiles, with none of the clumpiness
normally associated with recent massive star formation. (Exceptions are
NGC 1275, recently affected by a cooling flow or
interaction, and the
nonthermal jet in NGC 4486.) There is little UV evidence for dust in our
sample of normal ellipticals at 3" resolution (though lanes are
present in the peculiar objects NGC 1275 and 1316 and are often found at
HST resolution in elliptical cores). Because of the absence of
dust, the intergalactic ionizing radiation field of old stellar
populations may be competitive with that of young populations in more
dusty disk and irregular galaxies.
- The ellipticals and spiral bulges exhibit large far-UV/optical color
gradients in which the colors become redder outward (with the exception
of NGC 221, where the gradient is strong but
reversed). The gradients
are larger than any at optical/IR wavelengths. The UV light is evidently
extremely sensitive to the characteristics of its parent population. The
FUV profiles of some of the early-type systems (e.g., NGC 221 and 1399)
are well fitted by de Vaucouleurs functions, which are characteristic of
spheroids at optical wavelengths. However,
Ohl et al. (1998)
find that the inner FUV profiles of some E/S0 galaxies are more
consistent with an exponential function. Although exponentials are
normally associated with disks, the FUV contours are generally
consistent in shape and orientation with optical band isophotes, and the
three-dimensional FUV light distributions are therefore unlikely to be
genuinely disklike. Because of the large color gradients, it is not
necessarily expected that the UV profiles of systems which are true
spheroids at optical wavelengths would be closely de Vaucouleurs in
shape.
- The best evidence is that the far-UV light in most elliptical
galaxies and large bulges is produced by extreme horizontal branch stars
and their descendants in the dominant, low-mass, metal-rich population
(O'Connell 1999
and references therein). The UV
output of such objects is very sensitive to envelope properties and
hence age, helium and metal abundance, and giant branch mass loss. It is
a remarkable circumstance, if this interpretation is correct, that
relatively crude UV observations can in principal determine envelope
masses for stars in distant galaxies with a precision of a few 0.01
M .
- The range in central (UV-optical) colors for early-type galaxies is
very large, as first established by IUE spectra (e.g.,
Burstein et al. 1988).
We find unusually red (MUV-R) values, after extinction
corrections, for the early-type galaxies in the Perseus cluster. These
may be metal-rich systems which lack the extreme HB component.
- The cool stars in the large bulges of Sa and Sb spirals fade in the
UV while the hot OB stars in their disks brighten such that their Hubble
classifications (if these were attempted in the UV) would become
significantly later. In the far-UV, early-type spirals can appear as
peculiar, ringlike systems. At optical wavelengths, such structures
would be associated with a short-lived, nonequilibrium situation, not
with the stable configuration we know them to be.
- The mean azimuthally averaged profiles of galaxy disks are
approximately exponential in the UV but show considerably more structure
than at optical wavelengths. In spiral disks with well organized, large
amplitude spiral structure, the UV-bright structures closely outline the
spiral pattern. In most cases, however, the UV appearance of disks can
be considerably more fragmented and chaotic than at optical wavelengths,
and the UV Hubble types are significantly later. UV suppression of bulge
light in large-bulge spirals permits study of population changes in
their inner disks, which appear to be dramatic in the case of M81.
- The luminous AGNs in our sample range considerably in their
contribution to the total UV light. In Mrk 335 the AGN is completely
dominant; in NGC 4151 it contributes 80%; while in NGC 1068, 1275, and
4486 the contribution is only 10%-20%. A number of
systems have unusual
UV-bright structures in their inner disks, including rings (NGC 1317,
4321) and compact knots (NGC 1068). Such structures, and starburst
nuclei (e.g., NGC 2993 here and M83 in
Kuchinski et al. 2000),
could easily dominate the UV light in high-redshift analogs.
- Because of the often complex structural changes between the optical
and UV bands, there is no simple relation between the half-light radii
in these bands. However, in the most regular Sb-Sc spiral disks with
good photometric coverage (NGC 628 and 3031), the UV light is more
extended than the optical continuum light.
- Although none are illustrated in this paper, the cool bars of barred
spirals become less prominent in the UV as well
(Bohlin et al. 1983;
Kuchinski et al. 2000),
and this effect extends even to fairly late-type systems such as
Magellanic irregulars
(Page & Carruthers
1981;
Smith, Cornett, & Hill 1987).
- Dust in normal spiral disks does not dominate UV morphologies,
despite the high selective UV extinction characteristic of Milky Way and
Magellanic Cloud dust grains. The overall distributions of far-UV light
and
H light for those systems
where both are available are quite similar even though
A(1500Å) /
A(H) ~ 3.2. Such
ready escape of far-UV photons from normal spiral disks was not
anticipated. Quantitative analysis of UV spectra of starburst galaxies
shows that the UV continuum often suffers less extinction than predicted
from optical band extinction estimates, e.g., based on
H /
H ratios
(Fanelli et al. 1988;
Calzetti et al. 1994;
Mas-Hesse & Kunth
1999).
This is evidently mainly a consequence of the complex dust/star/gas
geometries of star-forming regions. The emergent UV spectrum will, of
course, always be weighted toward regions of lower extinction. But it
appears that the heaviest extinction is confined to thin layers and the
immediate vicinity of young H II complexes and that the UV light emerges
from thicker star distributions, regions evacuated of dust by
photodestruction or winds, or by virtue of strong clumpiness in dust
concentrations
(Fanelli et al. 1988;
Calzetti et al. 1994;
Calzetti 1997;
Gordon, Calzetti, &
Witt 1997;
Allen et al. 1997).
Only in cases like M82 and NGC 2146, where the dust layers appear
dynamically disrupted, or the massive star formation is deeply embedded,
does dust appear to be a major factor in UV morphology. A tentative
conclusion from the available information is that dust will infrequently
conceal the UV light of starburst activity for periods longer than ~ 50
Myr in the absence of continuing dynamical disturbances. This implies
that some high-redshift starburst systems could be UV-bright.
- Dust is expected to be more important in edge-on galaxies, and some
of these can be very faint in the UV (e.g., NGC 891 here). However,
other edge-on systems have high UV surface brightness, for instance
UGC 6697 in this paper or NGC 4631 in
Smith et al. (2000).
Since the dust content of the outer disks of galaxies is expected to be
low because of the lower metallicities there, one might expect many
edge-on systems to be reasonably bright in the UV.
- A significant fraction of the far-UV light in spiral disks is
diffuse rather than being closely concentrated to obvious star-forming
regions, and this appears to vary from object to object. The far-UV
(1500 Å) light is in general more diffuse than is
H. The diffuse component
could arise from migration of UV-bright stars away from their birth
sites during their ~ 50 Myr lifetimes, in situ star formation in
low-density regions, or scattered light from dust grains. In the case of
the Large Magellanic Cloud, UIT observations determined
that about 70%
of the detected 37,000 OB stars fell outside the boundaries of
well-defined H II regions
(Parker et al. 1998),
consistent with diffuse component estimates from deeper, narrow-field
HST observations
(Brosch et al. 1999).
The UV-bright plume of M82 indicates that dust scattering can be very
important in some cases; similar instances of scattering in galactic
winds might be detectable in high-redshift starburst systems.