![]() | Annu. Rev. Astron. Astrophys. 2005. 43:
861-918 Copyright © 2005 by Annual Reviews. All rights reserved |
Damped Ly systems are a
class of QSO absorbers selected for the presence of H I column
densities, N(H I)
2
× 1020 cm-2. This criterion differs from
those used to find other classes of QSO absorbers selected on the basis
of H I content. The
Ly
forest absorbers,
reviewed in this journal by
Rauch (1998),
are selected for N(H I) < 1017 cm-2,
while the Lyman limit systems have 1017 < N(H I)
< 2 × 1020 cm-2
(Peroux et al. 2003).
The Ly
forest absorbers
are optically thin at the Lyman limit, since the column density
N(H I) = 1017 cm-2 corresponds to about
unity optical depth at the Lyman limit. Are these absorbers physically
different from the damped systems or have the column-density criteria
resulted in arbitrary distinctions? In fact there is a fundamental
difference: hydrogen is mainly neutral in damped
Ly
systems, while it is
ionized in all other classes of QSO absorption systems. This includes
absorbers selected for the presence of C IV
1548.1, 1550.7
resonance-line doublets
(Sargent, Steidel & Boksenberg 1988),
Mg II
2796.3, 2803.5
resonance-line doublets
(Steidel & Sargent
1992)
and Lyman limit absorption
(Prochaska 1999),
which do not also qualify as damped
Ly
systems.
The neutrality of the gas is crucial: while stars are unlikely to form
out of warm ionized gas, they are likely to descend from cold neutral
clouds, which are the precursors of molecular clouds, the birthplace of
stars
(Wolfire et al. 2003).
This property takes on added significance when it is realized that the
damped Ly systems
dominate the neutral-gas content of the Universe in the redshift
interval z = [0, 5], and at z ~ 3.0-4.5 contain sufficient
mass in neutral gas to account for a significant fraction of the visible
stellar mass in modern galaxies (e.g.,
Storrie-Lombardi &
Wolfe 2000).
This has led to the widely accepted idea that damped
Ly
systems serve as
important neutral-gas reservoirs for star formation at high redshifts
(e.g.,
Nagamine, Springel &
Hernquist 2004a).
Moreover, as repositories of significant amounts of metals the damped
Ly
systems have been
used to trace the age-metallicity relationship and other aspects
of galactic chemical evolution
(Pei, Fall & Hauser
1999;
Pettini 2004;
Pettini et al. 1994;
Prochaska et al. 2003a).
The purpose of this review is to present an overview of the damped
Ly systems. Current
research on the high-redshift Universe is dominated by surveys that rely
on the detection of radiation emitted by stars (e.g.,
Dickenson et al. 2003,
Giavalisco et al. 2004,
Steidel et al. 2003)
or ionized gas (e.g.,
Ouchi et al. 2003,
Rhoads & Malhotra
2001).
By contrast, damped Ly
systems provide a window on the interplay between neutral gas and newly
formed stars, i.e., the damped
Ly
systems are the best,
perhaps the only, examples we have of an interstellar medium in the
high-redshift Universe. Consequently, the focus of this review will be
on the manner in which damped
Ly
systems trace, and
play an active role in, cosmic star formation and hence galaxy
formation.
Throughout this review we adopt a cosmology consistent with the WMAP
(Bennett et al. 2003)
results, m,
,
h) = (0.3, 0.7, 0.7).
1.1. History of Damped
Ly Surveys
To understand the significance of damped
Ly systems for research
in galaxy formation we give a brief historical perspective.
The motivation for the first damped
Ly survey was to find
the neutral-gas disks of galaxies at high redshifts
(Wolfe et al. 1986).
Unlike today, the cold dark matter (hereafter CDM) paradigm of
hierarchical structure formation (i.e., merging protogalactic clumps)
did not dominate theories of galaxy formation in the early
1980s. Rather, the idea of mature galaxy disks at high redshift fitted
in with the coherent collapse model of
Eggen, Lynden-Bell & Sandage
(1962;
also Fall & Efstathiou
1980),
which was highly influential at the time. Some QSO absorbers with
properties resembling galaxy disks had been found at z < 1
through the detection of 21 cm absorption either in radio-frequency
scanning surveys
(Brown & Roberts 1973)
or at the redshifts of Mg II-selected absorbers
(Roberts et al. 1976).
However, application of these techniques resulted in only a few
detections. While it was unclear whether the 21 cm absorbers belonged to
a new population of objects or were rarely occurring oddities, the radio
scanning techniques were valuable for successfully detecting cold,
quiescent gas at large redshifts for the first time. Specifically,
Brown & Roberts
(1973) and
Brown & Mitchell (1983)
used this technique to detect two 21 cm lines with FWHM velocity widths,
vH I
10 and 20 km
s-1. The temperature of the gas detected in 21 cm absorption
is likely to be low because the 21 cm optical depth
21
N(H I) /
(Ts
vH
I), where the hyperfine spin temperature, Ts,
generally equals the kinetic temperature of the cold, dense gas detected
in 21 cm absorption.
However, the most efficient method for locating quiescent layers of
neutral gas is through the detection of damped
Ly absorption lines. In
the rest frame of the atom, the absorption profile of any atomic
transition is naturally broadened owing to the finite lifetime of the
upper energy state. In the rest frame defined by the average velocity of
the gas, the natural profile is Doppler broadened by the random motions
of the atoms: the convolution of both effects results in the Voigt
profile (e.g.,
Mihalas 1978).
Because the Doppler profile falls off from the central frequency,
0, as
exp[-(
/
D)2]
(where
=
|
-
0| and
D =
(2)1/2
v
0 / c for an
assumed Gaussian velocity distribution with dispersion
v) and the
natural or "damped" absorption profile falls off from
0 like 1 /
(
)2, at sufficiently
large
the probability for damped
absorption exceeds the probability for absorption in the Doppler
profile. The frequency intervals in which natural broadening dominates
Doppler broadening are called the damping wings of the profile
function. Most atomic transitions of abundant ions are optically thin in
their damping wings but optically thick near the core of the Doppler
profile. The latter transitions have unit optical depth at
= 1
D ×
[ln N(Xj)]1/2, where N(Xj) is
the column density of ionic species Xj. Such lines are
saturated. The reason is that the rest-frame equivalent width of an
absorption line is given by Wr
(
/
)
(1- exp(-
)
d
), and therefore
Wr is proportional to
= 1.
In the case of lines with unit optical depth near the Doppler core the
line is saturated because Wr is insensitive to the
value of N(Xj). Due to the higher values of
N(H I),
Ly
has unit optical
depth in the damping wings at
=1
[A21 f21 N(H
I)]1/2 when N(H I)
1019
cm-2 and
v < 70 km
s-1: A21 and f21 are the
Einstein spontaneous emission coefficient and oscillator strength for
the Ly
transition,
respectively. In this case, unit optical depth occurs in the damping
wings, and therefore the equivalent width of a damped
Ly
line is independent
of the velocity structure of the gas for velocity dispersions within the
range detected in most QSO absorption systems. As a result, the
equivalent width will be large even when the velocity dispersion is
small.
By the early 1980s only four damped Ly systems had been found. In
every case they were high-column-density systems, N(H I)
1021
cm-2, which were found by chance
(Beaver et al. 1972;
Carswell et al. 1975;
Smith, Margon & Jura
1979;
Wright et al. 1979).
Although the sample was sparse, the utility of the damped
Ly
criterion was
demonstrated
when 21 cm absorption at z ~ 2 was detected in two of the three
background QSOs that were radio sources
(Wolfe, Briggs &
Jauncey 1981;
Wolfe & Davis 1979).
The narrow
line widths,
vH I
20 km s-1 (where
vH I = (8 ln 2)1/2
v), and
relatively low spin temperatures,
Ts < 1000 K, implied that these absorbers were H I
layers in which the gas was cold and quiescent.
For these reasons
Wolfe et al. (1986)
began a survey for damped
Ly systems by acquiring
spectra of large numbers of QSOs and then searching them for the
presence of damped
Ly
absorption lines. The
survey for damped
Ly
systems had several
advantages over surveys for 21 cm absorption lines. For example, the
redshift interval covered by a single optical spectrum,
z
1, is large compared
to that sampled by bandpasses then available for 21 cm surveys,
z
0.02. Second, optical
spectra of QSOs are obtained toward continuum sources with diameters
less than 1 pc, whereas the diameters of the associated background radio
sources typically exceed 100 pc at the low frequencies of redshifted 21
cm lines. As a result the survey was capable of detecting compact
gaseous configurations with low surface covering factors that would have
been missed in 21 cm surveys. Another advantage of optical surveys is
the large oscillator strength, f21 = 0.418, of the
Ly
transition (by
comparison f21 = 2.5 × 10-8 times a
stimulated emission correction of 0.068 K / Ts for the
21 cm line), which allows for the detection of warm H I, which is
optically thin to 21 cm absorption owing to high values of
Ts but optically thick in
Ly
. But this is also a
disadvantage: the strength of the
Ly
transition combined
with the high abundance of hydrogen means that the more frequently
occurring low-column-density clouds in which H is mainly ionized will be
optically thick in
Ly
. The result is a
profusion of
Ly
absorption lines,
i.e., the Ly
forest,
which dominate the absorption spectrum blueward of
Ly
emission
(Figure 1).
Although the Ly
forest
lines act as excellent probes of the power spectrum and other
cosmological quantities (see
McDonald 2003,
Tytler et al. 2004),
they are potential sources of confusion noise for the detection of
damped
Ly
lines, especially at
z > 4, since the line density per unit redshift increases with
redshift. Identification of damped
Ly
lines at z
> 5.5 is essentially impossible because of
Ly
forest confusion
noise.
![]() |
Figure 1. Keck/ESI spectrum of
QSO PSS0209 + 0517 showing the
Ly |
However, at z < 5.5 the large column densities of H I in galaxy
disks or in any other configuration produce damped
Ly absorption lines that
are strong enough to be distinguished from the
Ly
forest
(Figure 1). Consider the equivalent widths. At
the time of the
Wolfe et al. (1986)
survey the most accurate 21 cm maps of spiral galaxies were obtained
with the Westerbork radio interferometer. These showed the H I column
densities of galaxy disks to decrease from N(H I) ~
1021cm-2 at their centers to N(H I) = 2
× 1020 cm-2 at a limiting radius
Rl = (1.5 ± 0.5)
R26.5, which was set by the sensitivity available with
Westerbork and comparable radio antennas. Here the Holmberg radius,
R26.5, is the radius at which the B band
surface brightness equals 26.5 mag arcsec-2
(Bosma 1981).
The rest-frame equivalent width of a damped
Ly
line created by an H
I column density, N(H I), is given by Wr
10 ×
[N(H I)/2 × 1020 cm-2]1/2
Å. Because the observed equivalent width of a line formed at
redshift z is Wobs = (1 + z)
Wr, damped
Ly
systems with
N(H I)
2 ×
1020 cm-2 will appear in optical QSO spectra with
Wobs
16
Å for damped
Ly
systems redshifted
redward of the atmospheric cutoff (i.e., z
1.6 for
atm = 3200
Å). Lines this strong are easily distinguishable from the
Wobs
3 Å equivalent
widths of typical
Ly
forest
lines. Furthermore, they can be detected at low resolution and moderate
signal-to-noise ratio. Since the goal of the first survey for damped
Ly
systems was to find
absorbers with N(H I)
2 × 1020
cm-2, a spectral resolution,
= 10 Å, was
sufficient for resolving candidate features.
1.2. Modern Surveys and Identification of Damped
Ly Systems
Since the initial survey was published, nine more surveys have been
completed for damped
Ly systems with
N(H I)
2 ×
1020 cm-2
(Ellison et al. 2001;
Lanzetta et al. 1991;
Lanzetta, Wolfe &
Turnshek 1995;
Péroux et al. 2003b;
Prochaska & Herbert-Fort 2004;
Prochaska, Herbert-Fort
& Wolfe 2005;
Rao & Turnshek 2000;
Storrie-Lombardi &
Wolfe 2000;
Wolfe et al. 1995).
The identification of damped
Ly
systems is more
complex than for other classes of QSO absorbers. The
Ly
forest "clouds,"
which dominate the absorption spectrum blueward of
Ly
emission, are
abundant and easy to identify. Similarly, surveys for C IV or Mg II
absorption systems rely on the detection of doublets with known
wavelength ratios, which are straightforward to locate redward of
Ly
emission. By
contrast, the task of surveys for damped
Ly
systems is to pick
out a single damped
Ly
line from the
confusion noise generated by the
Ly
forest. In
particular, one must distinguish a single, strong
Ly
absorption line
created in high-column-density gas with low-velocity dispersion, but
broadened by radiation damping, from strong
Ly
absorption features
that are Doppler-broadened blends of several lines arising from redshift
systems with low-column-density gas. The presence of narrow
Ly
forest absorption
lines in the damping wings of the absorption profile is a further
complication that can distort the shape of the true line profile in data
of moderate or low signal-to-noise ratios
(see Figure 2 for examples).
![]() |
Figure 2. Example Voigt profile fits to two
damped
Ly |
The most widely used strategy for discovering damped
Ly systems was first
introduced by
Wolfe et al. (1986)
and later refined by
Lanzetta et al. (1991)
and Wolfe et al. (1995).
First, a continuum is fitted to the entire QSO spectrum blueward of
Ly
emission. Then damped
Ly
candidates are
identified as absorption features with rest equivalent widths
Wr exceeding Wthresh = 5
Å. This conservative criterion corresponds to N(H I)
5 × 1019
cm-2, which guarantees that few systems with N(H I)
above the completeness limit of 2 × 1020 cm-2
will be missed. The search is carried out in the redshift interval
z = [zmin, zmax], where
zmin is generally the shortest wavelength for which
(Wr)
< 1 Å and zmax is set 3000 km s-1
below zem to avoid contamination by the background
QSO. Finally, a Voigt profile is fitted to the
Ly
profile to determine
the value of N(H I). Where possible, the centroid is identified
from the redshift determined by metal lines outside the
Ly
forest. This is
particularly important at z
3 where line-blending from
the Ly
forest often
contaminates the damping wings (e.g., Figure 2).
The surveys were time-consuming because the signal-to-noise ratio and
resolution of the spectra used to acquire damped
Ly
system candidates
were usually inadequate for fitting Voigt profiles to the
data. Therefore, follow-up spectroscopy at higher spectral resolution
and with longer integration times was usually necessary.
Recently,
Prochaska &
Herbert-Fort (2004)
and
Prochaska, Herbert-Fort
& Wolfe (2005)
have streamlined this process in a survey based on a single set of QSO
spectra drawn from the Sloan SDSS archive
(Abazajian et al. 2003).
Because of the high-quality, good spectral resolution (R ~ 2000)
and extended spectral coverage of the data, the authors could fit
accurate Voigt profiles to the same data used to find damped
Ly system
candidates. The authors also bypass the time-consuming step of fitting a
continuum to the QSO spectrum blueward of
Ly
emission by searching
for damped Ly
system
candidates in spectral regions with lower-than-average signal-to-noise
ratios, i.e., regions coinciding with broad absorption troughs. The
survey is not formally complete to N(H I) = 2 ×
1020 cm-2, but the similarity between
d
/ dX, the
number of damped
Ly
systems encountered
per unit absorption distance along the line of sight (see
Section 2.1), in their survey and previous
surveys suggests that the
Prochaska, Herbert-Fort
& Wolfe (2005)
survey is more than 95% complete. The number of damped
Ly
systems for the SDSS
DR2 and DR3 archives is 525. As a result, the number of damped
Ly
systems in a
statistically complete sample now excedes previous samples by an order
of magnitude at z ~ 3 and several times at z ~ 4.
While the H I selection methods are successful at finding damped
Ly systems at z
1.6, they have been
unsuccessful at finding large numbers of objects at lower
redshifts. This is partly due to the reduced interception probability
per unit redshift at low z and partly because few QSOs have been
observed from space at UV wavelengths, which is required to detect
Ly
at z <
1.6. To increase the number of low-redshift damped
Ly
systems from the two
confirmed objects detected in previous H I selected surveys (see
Lanzetta, Wolfe & Turnshek
1995),
Rao & Turnshek (2000)
searched for damped Ly
systems in samples of QSO absorption systems selected for Mg II
2796.3, 2803.5
absorption. Since Mg II absorption is present in every damped system in
which it could be observed, it turns out to be a reliable indicator for
the presence of damped
Ly
. Using this
technique, Rao, Turnshek, and collaborators have recently increased the
sample size to 41 damped
Ly
systems with z
< 1.6 (SM Rao, DA Turnshek & DB Nestor, private communication).
The current sample of damped
Ly systems that are
drawn from surveys with statistically complete selection criteria
comprises over 600 redshift systems. While the number of damped
Ly
systems is smaller
than the
2350 objects
comprising the population of known Lyman Break Galaxies
(Steidel et al. 2003),
we expect the damped Ly
system population to approach this number when all QSO spectra from the
Sloan database become available.
1.3. The Significance of the N(H I)
2 × 1020
cm-2 Survey Threshold
The survey statistics cited above refer only to systems with N(H
I) 2 ×
1020 cm-2, which is a historical threshold set by
the H I properties of nearby spiral galaxies (see
Section 1.1). Because the nature of damped
Ly
systems is still not
understood, their H I properties may differ from those of nearby H I
disks: for example, CDM cosmogonies envisage damped
Ly
systems as merging
protogalactic clumps
(Haehnelt, Steinmetz &
Rauch 1998).
As a result, it is reasonable to ask whether the 2 ×
1020 cm-2 threshold is the appropriate
one. Indeed, since the empirically determined frequency distribution of
H I column densities increases with decreasing N(H I)
(Figure 3), lower H I thresholds would be
advantageous because they would result in larger samples.
![]() |
Figure 3. The N(HI) frequency
distribution f(N, X) determined by
Prochaska, Herbert-Fort
& Wolfe (2005)
for all damped Ly |
Fortuitously, the 2 × 1020 cm-2 threshold is
optimal for physical reasons unrelated to the properties of galaxy
disks. Rather, at large redshifts it is the column density that
distinguishes neutral gas from ionized gas: at N(H I) < 2
× 1020 cm-2 the gas is likely to be ionized
while at N(H I) > 2 × 1020 cm-2 it
is likely to be neutral. The minimal source of ionization is background
radiation due to the integrated population of QSOs and galaxies. Using
background intensities computed by Haardt & Madau
(1996,
2003),
Viegas (1995) and
Prochaska & Wolfe
(1996)
show that the gas in most of the "sub-damped
Ly" population [defined
to have 1019 < N(H I) < 2 × 1020
cm-2] described by Péroux et al.
(2002,
2003a)
is in fact significantly ionized with temperature, T >
104 K. This is a problem since gas neutrality is a necessary
condition if damped Ly
systems are to serve as neutral gas reservoirs for star formation at
high redshift, a defining property of the population. For this reason
the comoving density of H I comprising the sub-damped
Ly
population discussed
by
Péroux et al. (2003b)
should not be included in the census of gas available for star
formation. As a result, the sub-damped
Ly
correction to the
comoving density of neutral gas,
g(z), should be ignored. We suggest that
these ionization levels make "super Lyman-limit system" a more
appropriate name for systems with 1019< N(H I) <
2 × 1020 cm-2.