The observation
that these distant ULIRGs appear to be very massive systems means that
large amounts of raw material are needed to make one, implying that ULIRGs
are likely to be found in regions with large concentrations of
baryons. Therefore, in order to understand when, where and why ULIRGs exist,
we must turn to galaxy and large-scale structure formation models to see
where such large concentrations of baryons are predicted to be
found. Modern structure formation models describe the evolution of the
total mass distribution (comprising both non-baryonic and baryonic `cold'
dark matter) via the evolution of initially Gaussian density fluctuations,
which means that the evolution of the total mass distribution should be
traced by the formation and evolution of galaxies in some determinable
way. Density fluctuations in the dark matter distribution, commonly
referred to as `halos', are predicted to undergo successive mergers over
time to build halos of steadily increasing mass. Galaxies are predicted to
form from the baryonic matter in these halos, driven either by inter- or
intra-halo mergers, or passive collapse of baryons to the halo central
regions, or some combination of all three mechanisms
[Meza et al. 2003,
Kobayashi 2004].
This framework of `biased' hierarchical buildup
[Cole et al. 2000,
Granato et al. 2000,
Hatton et al. 2003],
coupled
with a cosmology
[Spergel et al. 2003],
has proven to be remarkably successful in explaining many aspects of
galaxy and large-scale structure formation.
Within this framework, the largest concentrations of baryons are expected to be found within the most massive dark matter halos. A basic verification of this idea can be seen in the local Universe, where the most massive elliptical galaxies are almost invariably found within very rich galaxy clusters; which presumably correspond to large overdensities of baryons in the local Universe. The formation history of these very massive galaxies, even before the advent of sub-mm surveys, was controversial. The `naive' expectation from hierarchical theory would be that massive galaxies form relatively late and over a long period of time, representing successive mergers between dark matter halos, building up the required large baryon reservoirs [Baugh et al. 1998], and indeed some massive galaxies do appear to form in this way [van Dokkum et al. 1999, Tamura & Ohta 2003, Bell et al. 2004]. There is however observational evidence that many massive galaxies may form at high redshift and on short timescales, for example from the discovery of evolved systems at high redshift [Dunlop et al. 1996, Martini 2001, Blakeslee et al. 2003], the extremely tight K-band Hubble relation for radio galaxies [De Breuck et al. 2002] implying a very rapid early formation of the most massive galaxies [Rocca-Volmerange et al. 2004], and an inferred early star formation epoch from the colour-magnitude diagram in clusters at z = 0.5 [Ellis et al. 1997], implying that the stars in very massive local galaxies formed within a few Gyr of each other at z > 1.
The SMGs and Spitzer high z ULIRG samples appear to be perfect candidates
for the formation events for those local massive ellipticals that appeared
to form very early and very fast; they lie at z
2.5
[Simpson et al. 2004,
Chapman et al. 2005],
which is a high enough redshift to make stars with the
ages seen locally, their star formation rates are high enough to make all
the stars in a local massive elliptical fast enough to satisfy the observed
colour-scaling relationships, and their comoving number density is
comparable to that of local
3L* ellipticals
[Scott et al. 2002,
Chapman et
al. 2004b].
Serious theoretical difficulties remain however.
Early CDM-based galaxy formation models lacked the detailed astrophysics to
explain the number of observed SMGs and their star formation rates
[Granato et al. 2000,
Somerville, Primack
& Faber 2001,
Guiderdoni et
al. 1998].
Later models included improved treatments of
starbursts, but still had to include further modifications to explain the
observed sub-mm counts. These include a top-heavy initial mass function
for the stars formed in bursts, so that the same sub-mm flux can be
produced with lower star formation rates
[Baugh et al. 2005]
8, modified treatments of
virialization and the survival of subhalos to solve the `overmerging'
problem in the standard Press-Schechter formalism and make the SFRs high
enough
[van Kampen et
al. 1999,
van Kampen et
al. 2005],
and modifications to gas cooling and supernova feedback
[Granato et
al. 2004].
Fundamentally, there are two testable basic predictions of these
hierarchical models for high-redshift ULIRGs. Firstly, these ULIRGs should
reside within rich environments, that is to say we should see clustering of
other galaxies around the ULIRGs on length scales of < 5Mpc, representing
galaxy overdensities resulting from the local overdensity of
baryons. Testing this observationally is, however, difficult. At
z < 1
there have been numerous successful measurements of galaxy overdensities
around AGN using deep optical/near-IR imaging to find evolved systems
[Wold et al. 2001,
Wold et al. 2003],
but at the mean redshift of high-redshift ULIRGs
it is certainly not clear whether their local environments have built up
overdensities of evolved galaxies, even if they are overdense in
baryons. Secondly, we should observe the high-redshift ULIRGs themselves
to cluster together strongly on the sky, or in other words clustering of
just the high-redshift ULIRGs on length scales
25 Mpc. This
prediction is a consequence of the assumed form of the evolution of density
fluctuations with redshift; rare fluctuations in the underlying mass
distribution are predicted to cluster together on the sky, with the
strength of clustering depending on the degree of rarity
[Bardeen et al. 1986].
Very massive halos (those with masses
1014
M
),
which are universally predicted to be extremely rare at high redshift,
are therefore predicted to cluster together very strongly (e.g.
[Moscardini et
al. 1998,
Kauffmann et al. 1999,
Mo & White 2002]).
This clustering should be traced by very
massive galaxies, as only the most massive halos contain sufficient baryon
reservoirs to form these galaxies. This also means that the clustering
strength of massive galaxies should translate straightforwardly to measure
of halo mass
[Percival et al. 2003].
Strong clustering among high-redshift ULIRGs is
also predicted if, as some suspect, they are part of a population uniting
QSOs and spheroids
[Magliocchetti et
al. 2001].
Measuring this form of clustering
observationally is however also difficult, requiring either
50
sources with spectroscopic redshifts so that `associations' in redshift
space between different sources can be searched for, or a minimum of
several hundred sources with a reasonably well constrained redshift
distribution, and found over a large enough area of sky such that the
length scales of interest can be examined.
Despite these difficulties, numerous studies of both the environments of
high-redshift ULIRGs, and their clustering, have taken place, and while
these studies are not (yet) conclusive, they do generally lend support to
the idea that high-redshift ULIRGs form within massive dark matter
halos. Considering environment studies first; near-IR imaging
studies of the environmental richness of ULIRGs over 0.5 < z
< 1.5
[Farrah et al. 2004b]
have shown that these systems reside in richer environments
than their local counterparts on average, and that some reside in moderate
rich clusters even at z
1, though it is
not clear whether this
represents a genuine increase in environmental richness for ULIRGs, or
whether this just reflects the global increase in `bias' over 0 <
z < 1. At
lower redshifts, LIRGs and ULIRGs have also been found in clusters
[Duc et al. 2004,
Lemonon et al. 1998,
Kleinmann et al. 1988].
Turning to higher redshifts, then several authors have
noted overdensities of sub-mm sources around high-redshift systems that are
thought to reside within mass overdensities, including z ~ 4 radio
galaxies
[Stevens et al. 2003,
De Breuck et al. 2004]
(several of these sub-mm sources are also detected
in the X-ray, suggesting the presence of obscured AGN
[Smail et al. 2003]
and seen as z ~ 3 Lyman Break galaxies
[Chapman et
al. 2001,
Geach et al. 2005].
Turning to high-z ULIRG clustering; early efforts to measure angular
clustering on the sky came up against the limitations of available
instrumentation; at the time of writing there exists no sub-mm array
instrument that can map large enough areas of the sky to the required
depths (though SCUBA2, APEX and Herschel, are coming soon). No clear
picture has therefore emerged; some sub-mm surveys have uncovered tentative
hints of clustering on scales of a few arcminutes
[Scoville et al. 2000],
whereas others show no signs of clustering whatsoever
[Borys et al. 2003].
An intriguing
result from these wide field surveys is that the high-redshift ULIRGs
appear to trace moderately bright X-ray survey sources on the sky, even
though the direct overlap between the two populations is minimal
[Almaini et al. 2003].
This could suggest that the high-redshift sub-mm and X-ray
populations are tracing the same, overdense dark matter halos. More recent
efforts to measure SMG clustering using spectroscopic redshifts have met
with greater success, resulting in a reliable detection of clustering for
the first time
[Blain et al. 2004a].
The strength of the clustering, while
significant, is not particularly strong, at r0 = 6.9
± 2.2 (comoving). This clustering strength is consistent with
high-redshift ULIRGs residing in ~ 1013
M halos
which will eventually
become the cores of rich clusters in the local Universe, but the relatively
high redshift of the sources in this sample, coupled with the significant
error on their clustering and the unknown growth modes of dark matter
overdensities (see e.g.
[Matarrese et
al. 1997,
Moscardini et
al. 1998])
leaves other possible interpretations open. More precise measurements of
both high-redshift ULIRGs, and other ULIRGs at lower (and higher) redshifts
are needed to resolve this issue. The new Spitzer ULIRG surveys, sampling
much larger volumes and linear dimensions than current submm/mm surveys,
can be expected open up this field of enquiry dramatically.
8 an interesting conundrum from this model is that while the sub-mm counts are predicted to be dominated by bursts, these bursts would be responsible for making only a small fraction of the stellar mass in evolved ellipticals in the local Universe if their IMFs are top heavy. Back.