6.1
UV/Optical/IR Surveys
Empirical evidence on the existence of high redshift
Ly emitting objects, and also
on the incidence of
dust absorption in low metallicity galaxies, suggests
that PGs may be visible in Ly
for some significant fraction (
10%) of their lifetime. This conclusion, coupled
with the observation that resonant scattering does not quench
the Ly
emission of active
star-forming galaxies beyond what
is expected from a normal reddening law, seems to favor
a continued effort to detect Ly
emission from PGs.
At present, emission-line surveys are just barely reaching the flux limits and volumes needed to detect ~ 100 objects. Currently the best prospects for searching for a widespread population of PGs appear to be in expanding the volume surveyed, either using mosaics of CCDs to increase solid angle coverage, or acquiring data for additional slices in redshift space. [An innovative and promising technique for expanding redshift coverage is the Fabry-Perot technique of Djorgovski and collaborators; this provides a narrow band (hence very faint flux limit) tunable system.]
It appears unlikely that the flux limits can be pushed much fainter
that the current limits of 10-17 erg cm-2 s-1 in
the optical (
<
7000Å). The one exception appears to be
searches for unresolved objects, for which HST (or ground-based
adaptive optics) observations may improve flux limits by factors up to
~ 10X. At first sight it might appear that improved
resolution would be of limited interest in searching for PGs,
since this resolution (approaching 0".1) would detect
structures smaller than 1 kpc. However, at this level of resolution,
and with the concomitant improvement in limiting magnitude for
unresolved sources, it may be possible to detect the individual star
forming regions that comprise an otherwise large, low surface
brightness PG.
This raises the issue of detecting fuzzy, low surface brightness PGs.
In Section 5.2 we considered the
detection of such objects as depending on
Poisson statistics - i.e. S/N
-1/2. In fact,
fuzzy objects are considerably more difficult to detect than this,
because of flat fielding errors, reflections of bright stars by
correcting optics, and perhaps even high latitude ``cirrus''
(Sandage 1976,
Guhathakurta and
Tyson 1989). Extracting limits on large faint PGs
requires exquisite care, both at the telescope (improved flat fielding
techniques, carefully choosing fields to avoid reflections and cirrus
problems), and also during data reduction (e.g., using many shifted
exposures to separate true objects on the sky from observational
artefacts). Considerable work remains to be done in this area.
Most of the surveys for which limits appear in Figs.
7,
8,
9 have emphasized achieving a
faint flux limit at
the expense of volume coverage. It is therefore germane to consider a
somewhat orthogonal approach to detecting emission line PGs: searching
for intrinsically luminous (but rare) sources in a very large solid
angle survey. Such a survey is now underway using the UBC 2.4m liquid
mirror telescope, which will search over ~ 20 deg2 for
emission line PGs at z = 4.8 in three 160Å bands down to a
limiting Ly surface brightness
of order 3 x 10-16 erg cm-2
s-1 arcsec-2 (Hickson, private communication).
Referring to Figs. 7,
8,
9, it can be seen that this large
solid angle
survey, which will probe a comoving volume ~ 5 x 107
Mpc3, will provide extremely interesting constraints on the
properties of PGs - constraints that are quite complementary to
previous surveys.
Nath and Eichler
(1993) have also proposed searching for redshifted
blends of highly ionized [Fe VII]-[Fe XII] lines in the far UV (rest
wavelengths 160-200Å); these lines are
expected from
hot diffuse (metal-enriched) gas heated to the virial temperature
(~ 106 K) of a PG by supernovae. The principal problem here
appears to be dust absorption, which will affect these lines even more
dramatically than Ly
: i.e., if
the null results of Ly
surveys
are due
to ``normal'' dust absorption rather than resonant scattering (as
argued above), then the probability of detecting these far UV lines
appears to be much lower than for Ly
(especially since they are metal
lines, and the existence of metals implies the existence of dust).
An interesting continuum technique which deserves further study is the
search for the Lyman discontinuity in faint galaxy populations (e.g.,
Koo and Kron
1980). This technique has already been used to advantage by
Steidel and
Hamilton (1993; see also Giavalisco et al. 1994) to identify
candidate high redshift galaxies clustered around a damped Ly
absorber; and Guhathakurta et al. (1990) use U band
photometry to rule
out the existence of a large population of objects at z > 3 with
large Lyman
continuum breaks. A new survey to detect objects with large
Lyman discontinuities has been commenced by De Robertis and McCall
(private communication).
In addition to pushing the search for Ly radiation out to ever
increasing redshifts
(Parkes et
al. 1994,
Pahre and
Djorgovski 1994),
IR observations are of
importance for detecting redshifted optical lines such as [O II]
3727Å, [O III] 5007Å, and H
6563Å
(Thompson et
al. 1994),
all of which are less affected by dust than Ly
. Searches for PGs in
the near infrared are fraught with difficulty, both because of the
small physical size of IR detectors, and especially because of the poor
flux limits imposed by the strong OH sky background. However, recent
experiments in selecting narrow spectral regions with low OH emission
are extremely encouraging. For example, the
Pritchet and
Hartwick (1994) survey at 9100Å has reached a limiting threshold of
~ 10-17 erg cm-2 s-1 for stellar
objects, and recent
observations by these two authors in a nearly OH free window near
1.6µm look very promising. A similar technique has been used in
the infrared J band by Parkes et al. (1994). Clearly a great deal of
work remains to be done in this area, both by selecting additional
low-OH windows, and by observing with the next generation of large
format IR arrays to improve volume coverage.
Finally, it is relevant to consider the choice of fields in PG
surveys (see also Section 5.3). Most
groups have chosen random fields for
PG searches, arguing that a widespread population of PGs should exist
everywhere, and hence any field should be as good as any other. An
interesting alternate approach is provided, however, by the work of
Rhee et
al. (1989),
De Propris et
al. (1993), and
Thompson et
al. (1994; see also Djorgovski et al. 1993). In these studies, fields
are chosen
near objects known to exist at high redshift (e.g., QSOs); the redshift
of the emission line survey is then tuned to match the redshift of the
QSO. The argument is that this is a volume of the Universe in which it
is known a priori that structure has collapsed, and so the
probability of encountering other collapsed structures is enhanced.
This argument is essentially statistical biasing
(Kaiser 1986), and
finds empirical support both in the observation by Wolfe (1993) that
Ly emitting objects are
clustered around damped Ly
absorbers with a
probability far in excess of random, and, as noted above, in the fact
that numerical simulations suggests that the volume filling factor of
galaxy formation is
1%
(Evrard et
al. 1994). Surveys near high
redshift QSO's may prove to be a useful method of detecting both
primeval galaxies and protoclusters.
6.2
Millimeter and Sub-millimeter Surveys
Some of the most exciting opportunities for the future detection of the
general population of PGs exist in the sub-mm and mm spectral regions.
As discussed extensively above, it is possible and even likely that a
significant fraction of the UV-optical emission from PG's is absorbed
by dust and reradiated at longer wavelengths. The emission from these
galaxies could even be totally obscured without violating CMB
distortion constraints (e.g.,
Section 5.1). The presence of dusty galaxies
at high redshifts is now well established (e.g.,
Section 2.6), and
Dunlop et
al. (1994) have detected an enormous dust mass in the z = 3.8 radio
galaxy
4C41.17, using the James Clerk Maxwell Telescope (JCMT) at a
wavelength of 800µm. The presence of a strong IR background (10-100
µm) consistent with obscured PGs has been inferred from an
ingenious -ray
experiment by De
Jager et al. (1994).
With the new SCUBA array at JCMT (available late 1994), it should prove
possible to detect sources as faint as 470µJy per beam
(1 detection,
1 hour exposure, 800µm). Since the flux from a z = 5
PG of baryonic
mass 1011 M
is ~ 1.6 mJy (e.g.,
Section 2.3), it follows
that the detection of such a source (which is ~ 10X fainter
than
4C41.17) should be straightforward. From the surface density
estimates in Section 2.1, there should
be ~ 5 such sources per
2' x 2' SCUBA field. Detailed simulations of the appearance of the
sky in the sub-mm are shown in Figure 10 for
two instrumental
configurations (Bond and Myers 1994). Such observations offer perhaps
the best hope for detecting a widespread population of PGs in the near
future.
I wish to thank David Hartwick for his encouragement and insight over the past decade, and also for comments on an earlier draft of this paper. I am also grateful to Ray Carlberg, George Djorgovski, and Sidney van den Bergh for extraordinarily helpful comments and criticisms that substantially improved this paper, to Stèphane Charlot for the GISSEL models, to Dick Bond and Steve Myers for Fig. 10, and to Paul Hickson and Michael De Robertis for comments on projects in progress. Much of this paper was written while visiting the Canadian Institute of Theoretical Astrophysics (University of Toronto) as a Reinhardt Fellow, and I gratefully acknowledge their hospitality. This work was supported by the Natural Sciences and Engineering Research Council of Canada.