6.2. The global cosmic star-formation history
The rest-frame UV luminosity of galaxies traces nicely their metal production rate, because both are produced primarily by massive stars. On the other hand, the conversion from a UV luminosity density to an actual cosmic star formation rate is somewhat less straightforward, since it involves a knowledge of the Initial Mass Function (IMF).
Early estimates of the metal production rate as a function of redshift,
Z(z), relied on ground-based redshift
surveys
(Lilly et
al. 1996,
Gallego et
al. 1995)
and data from QSO absorption line systems (e.g.,
Lanzetta et
al. 1995,
Pei and Fall 1995).
These estimates indicated a monotonic increase in the metal production
rate from z = 0 to z
1 (with the rate at
z
1 being about an order
of magnitude higher than at the present).
One of the seminal results to have come out of the HDF-N was the attempt
to estimate the metal production rate at high redshifts and thereby to
generate a continuous plot of the star formation rate as a function of
redshift
(Madau et
al. 1996).
In the original diagram, no corrections were made, for either dust
extinction or for surface brightness effects. Consequently, the results
were presented as lower limits. Both in the original work and in some of
the subsequent work that followed (some of which included the effects of
dust extinction), it was found that the star formation rate peaks at a
redshift of z ~ 1-2 and decreases or stays nearly constant at
higher redshifts (e.g., Fig. 26,
Steidel et
al. 1999,
Hopkins, Connolly
and Szalay 2000,
Calzetti and
Heckman 1999,
Pei, Fall and Hauser
1999).
The question of whether there truly is a decrease in the star formation
rate for
z 2 has
become a focal point of the discussion of the cosmic star formation
history. Some doubts were raised on the basis of dust extinction and
selection effects on one hand, and cosmological surface brightness
dimming effects on the other. Broadly speaking, the UV luminosity
density could be underestimated if a significant fraction of the
star formation occurred in environments obscured by dust or in very
low-surface-brightness galaxies. Several attemps were made to correct
for dust attenuation
(using the empirical attenuation law of
Calzetti, Kinney
and Storchi-Bergmann 1994),
by calibrating the relation between the UV spectral slope and the far IR
emission (e.g.,
Meurer, Heckman
and Calzetti 1999,
Steidel et
al. 1999).
Others used constraints obtained from extragalactic background radiation
and neutral gas (e.g.,
Pei, Fall and Hauser
1999,
Calzetti and
Heckman 1999).
Most of these investigations concluded that the star formation rate
rises from the present to z ~ 1-2 and then stays approximately
flat to z ~ 5.
![]() |
Figure 26. The star formation rate density versus redshift derived from the UV luminosity density. Adapted from Ferguson, Dickinson and Williams (2000). |
Another way to address the question of the history of mass assembly in
galaxies is to try to measure the actual stellar masses of
galaxies (as opposed to the rates of star formation; ideally one
would want to do both). To this goal, observations in the
near-infrared are typically used, since the near-infrared luminosity
traces the stellar mass reasonably well.
Dickinson et
al. (2003)
used an infrared-selected sample of galaxies from the HDF-N to determine
the global stellar mass density,
*(z), for 0 < z <
3. They found that
*(z) increases with time from
z = 3 to the present (Fig. 27).
Dickinson et al. concluded that by z ~
1, about 50-75% of the present-day stellar mass density had already
formed, but that the stellar mass density at z ~ 2.7 was about 17
times lower than today. These observations appear to be in clear
contradiction with scenarios in which most stars in today's spheroids
formed at z >> 2, but the observations are in general
agreement with a global star formation rate that rises from the present
to z ~ 1 and then stays fairly flat.
![]() |
Figure 27. The redshift evolution of the co-moving stellar mass density. The vertical extent of the boxes shows the range of systematic uncertainty. The bottom two solid lines (on the right-hand scale) show the result of integrating the star-formation-rate histories traced by the rest-frame UV light, with and without corrections for dust extinction. The top two solid lines and the dashed line show theoretical predictions from semi-analytical galaxy evolution models (Cole et al. 2000, Somerville, Primak, and Faber 2001). Adapted from Dickinson et al. (2003). |
A different spin on the cosmic star formation rate has been put by Lanzetta et al. (2002). These authors claimed that by neglecting cosmological surface brightness dimming effects, previous works have missed a significant fraction of the ultraviolet luminosity density at high redshifts. Specifically, since the surface brightness decreases with redshift as (1 + z)-3 (because of the cosmic expansion), intrinsically faint regions of high-redshift galaxies become undetectable.
Lanzetta et al. designated the unobscured star formation rate
intensity (i.e., the intensity inferred from the observed
rest-frame UV light) by x, and used a distribution function
h(x) (defined so that h(x)dx is the
projected proper area per comoving volume of star formation rate
intensity in the interval x to x + dx), to
estimate the ultraviolet luminosity density at high redshifts
(including the surface brightness dimming effects). They found that the
star formation rate density,
s, increases monotonically with redshift to the
highest redshifts observed (z ~ 8; although in one of the
possible corrections for incompleteness
s remains fairly flat above z ~ 2).
The low fraction of stellar mass formed by z = 3 according to the Dickinson et al. results appears to contradict evidence for significant star formation occurring at still higher redshifts. One possible way out of this conundrum is that the initial mass function (IMF) at high redshifts is very top-heavy (tilted towards massive stars; Ferguson et al. 2002). Massive stars dominate the UV luminosity in star forming galaxies, but their contribution to the total surviving (at lower redshifts) stellar mass is relatively low.
Most recently,
Stanway, Bunker
and McMahon (2003)
used HST's Advanced Camera for Surveys, the ground-based Sloan Digital
Sky Survey and the Very Large Telescope (VLT) to determine the space
density of UV-luminous starburst galaxies at z ~ 6. They found a
lower bound to the integrated, volume-averaged, global star formation
rate at z ~ 6, that was about six times less than that at
z ~ 3-4. The question of the true behavior of
s above z ~ 2 remains, therefore,
presently somewhat unresolved.
Fortunately, a more definitive answer may come in the near future,
through a combination of planned observations with HST and with the
Space Infrared Telescope Facility (SIRTF; currently scheduled to be
launched in April 2003). The Great Observatories Origins Deep Survey
(GOODS; Principal Investigator M. Dickinson) will produce a very
deep image of two fields (the HDF-N and the southern deep field observed
with the Chandra Observatory) with SIRTF at 3.6-24 µm,
and will thereby produce a much more complete census of stellar mass at
high redshifts. At the same time, observations (of the same fields) with
Hubble's Advanced Camera for Surveys (Principal Investigator
M. Giavalisco; the observations are being carried out as these
lines are being written) will determine the star formation rates, sizes,
and morphologies of galaxies. The combined observations will allow for
the first time for a determination of the evolving mass assembly
distribution f (M,
, t) (where
M denotes the stellar mass and
the star formation
rate). Given the fact that under pure luminosity evolution,
M =
dt, a
comparison between the observed evolution of the (M,
) phase space with
time and the evolution obtained from direct integration (of
, to produce
M), will allow, in principle, for an identification of the role
of mergers and interactions. Even when the expected observational
uncertainties are taken into account, there is no doubt that the planned
GOODS observations will yield a huge step forward in the understanding
of the assembly of present-day galaxies, and their
morphological evolution (the emergence of the "Hubble
Sequence"). Furthermore, the planned Hubble Ultra Deep Field with the
Advanced Camera for Surveys (currently scheduled for July-August 2003)
could extend the redshift coverage unambiguously to z ~ 6, close
to the tail of the tentative second reionization epoch
(Fan et al.
2001,
Becker et
al. 2001)
of the universe (the first reionization having tentatively occurred at
z ~ 20+10-9;
Bennett et
al. 2003).
Such a study could therefore produce results that are not merely
incremental in our understanding of the cosmic star formation history,
galaxy evolution, and the ionization history of the universe, and that
can be used to place meaningful constraints on theoretical models (e.g.,
Somerville and
Livio 2003).