84 research outputs found
On the importance of local sources of radiation for quasar absorption line systems
A generic assumption of ionization models of quasar absorption systems is
that radiation from local sources is negligible compared with the cosmological
background. We test this assumption and find that it is unlikely to hold for
absorbers as rare as H I Lyman limit systems. Assuming that the absorption
systems are gas clouds centered on sources of radiation, we derive analytic
estimates for the cross-section weighted moments of the flux seen by the
absorbers, of the impact parameter, and of the luminosity of the central
source. In addition, we compute the corresponding medians numerically. For the
one class of absorbers for which the flux has been measured: damped Ly-alpha
systems at z~3, our prediction is in excellent agreement with the observations
if we assume that the absorption arises in clouds centered on Lyman-break
galaxies. Finally, we show that if Lyman-break galaxies dominate the UV
background at redshift 3, then consistency between observations of the UV
background, the UV luminosity density from galaxies, and the number density of
Lyman limit systems requires escape fractions of order 10 percent.Comment: Accepted for publication in the Astrophysical Journal, 11 pages, 1
figure. Version 2: Added alternative method. Decreased fiducial escape
fraction to guarantee consistency between observed luminosity density, mean
free path, and UV background. This increased the column density above which
local radiation is importan
The missing metals problem. III How many metals are expelled from galaxies?
[Abridged] We revisit the metal budget at z~2. In the first two papers of
this series, we already showed that ~30% (to <60% if extrapolating the LF) of
the metals are observed in all z~2.5 galaxies detected in current surveys.
Here, we extend our analysis to the metals outside galaxies, i.e. in
intergalactic medium (IGM), using observational data and analytical
calculations. Our results for the two are strikingly similar: (1)
Observationally, we find that, besides the small (5%) contribution of DLAs, the
forest and sub-DLAs contribute subtantially to make <30--45% of the metal
budget, but neither of these appear to be sufficient to close the metal budget.
The forest accounts for 15--30% depending on the UV background, and sub-DLAs
for >2% to <17% depending on the ionization fraction. Together, the `missing
metals' problem is substantially eased. (2) We perform analytical calculations
based on the effective yield--mass relation. At z=2, we find that the method
predicts that 2$--50% of the metals have been ejected from galaxies into the
IGM, consistent with the observations. The metal ejection is predominantly by
L<1/3L_B^*(z=2) galaxies, which are responsible for 90% the metal enrichment,
while the 50 percentile is at L~1/10L^*_B(z=2). As a consequence, if indeed 50%
of the metals have been ejected from galaxies, 3--5 bursts of star formation
are required per galaxy prior to z=2. The ratio between the mass of metals
outside galaxies to those in stars has changed from z=2 to z=0: it was 2:1 or
1:1 and is now 1:8 or 1:9. This evolution implies that a significant fraction
of the IGM metals will cool and fall back into galaxies.Comment: 18pages, MNRAS, in press; small changes to match proofs; extended
version with summary tabl
The missing metals problem: II. How many metals are in z ~ 2.2 galaxies?
In the context of the ``missing metals problem'', the contributions of the
UV-selected z=2.2 ``BX'' galaxies and z=2.5 ``distant red galaxies'' (DRGs)
have not been discussed previously. Here we show that: (i) DRGs only make a
marginal contribution to the metal budget (~ 5%); (ii) BX galaxies contribute
as much as 18% to the metal budget; and (iii) the K-bright subsample ()
of the BX sample (roughly equivalent to the `BzK' selected samples) contributes
roughly half of this 18%, owing both to their larger stellar masses and higher
metallicities, implying that the rare K-bright galaxies at z>2 are a major
source of metals in the budget. We showed in the first paper of this series
that submm galaxies (SMGs) brighter than 3 mJy contribute ~5% (<9% as an upper
limit) to the metal budget. Adding the contribution of SMGs and damped Ly-alpha
absorbers, to the contribution of UV selected galaxies, implies that at least
30% of the metals (in galaxies) have been accounted for at z=2. The cosmic
metal density thus accounted for is ~ 1.3\times 10^6 \rhosun. This is a lower
limit given that galaxies on the faint-end of the luminosity function are not
included. An estimate of the distribution of metals in local galaxies as a
function luminosity suggests that galaxies with luminosity less than L^{\star}$
contribute about half of the total mass of metals. If the metals in galaxies at
z ~ 2 are similarly distributed then faint galaxies alone cannot solve the
`missing metals problem.' Galaxy populations at z ~ 2 only account for about
50% of the total metals predicted.Comment: 4 pages, 1 figure, accepted for publication in MNRAS Letters; small
changes to match the published tex
The missing metals problem: I. How many metals are in submm galaxies?
We use a sample of submillimetre-selected galaxies (SMGs) with molecular gas
and dynamical mass measurements from the literature to put constraints on the
contribution of such galaxies to the total metal budget. Compared to Lyman
break galaxies (LBGs), for example, SMGs are rarer (by a factor of 10 or more),
but contain much more gas and are more metal rich. We estimate that SMGs
brighter than 3 mJy contain only less than 9% of the metals when we combine the
observed dynamical masses (few \msun), number density ( Mpc), observed gas metallicity (1--2 x solar), and observed gas
fractions (~40%) assuming a molecular to neutral hydrogen ratio of 1. Including
SMGs fainter than 3 mJy, we estimate that SMGs contain at the most 15% of the
metals, where our incompleteness correction is estimated from the dust mass
function. Our results are strong upper limits given that high gas fractions and
high overall metallicity are mutually exclusive. In summary, SMGs make a
significant contribution to the metal budget (< 15%) but not sufficient to
solve the `missing metals problem.' A consequence of our results is that SMGs
can only add % to , and can not be the source of
a significant population of dusty DLAs.Comment: 6 pages, 1 figure. Accepted for publication in MNRAS. Minor changes
to match the published tex
Metal abundances at z<1.5: new measurements in sub-Damped Lyman-alpha Absorbers
Damped Lyman-alpha systems (DLAs) and sub-DLAs seen toward background quasars
provide the most detailed probes of elemental abundances. Somewhat
paradoxically these measurements are more difficult at lower redshifts due to
the atmospheric cut-off, and so a few years ago our group began a programme to
study abundances at z < 1.5 in quasar absorbers. In this paper, we present new
UVES observations of six additional quasar absorption line systems at z < 1.5,
five of which are sub-DLAs. We find solar or above solar metallicity, as
measured by the abundance of zinc, assumed not to be affected by dust, in two
sub-DLAs: one, towards Q0138-0005 with [Zn/H]=+0.28 +/- 0.16; the other towards
Q2335+1501 with [Zn/H]=+0.07 +/- 0.34. Relatively high metallicity was observed
in another system: Q0123-0058 with [Zn/H]=-0.45 +/- 0.20. Only for the one DLA
in our sample, in Q0449-1645, do we find a low metallicity, [Zn/H]=-0.96 +/-
0.08. We also note that in some of these systems large relative abundance
variations from component to component are observed in Si, Mn, Cr and Zn.Comment: 7 figures and 10 tables. Accepted for publication in MNRA
Measuring the halo mass of MgII absorbers from their cross-correlation with Luminous Red Galaxies
We study the cross-correlation between 716 MgII quasar absorption systems and
about 100,000 Luminous Red Galaxies (LRGs) selected from the Sloan Digital Sky
Survey Data Release 3 in the redshift range 0.4<z<0.8. The MgII systems were
selected to have 2796 & 2803 rest-frame equivalent widths greater than 1.0 \AA
and identifications confirmed by the FeII 2600 or MgI 2852 lines. Over
co-moving scales 0.2--13/h Mpc, the MgII--LRG cross-correlation has an
amplitude 0.69+/-0.09 times that of the LRG--LRG auto-correlation. Since LRGs
have halo-masses of 10^{13} \msun, this strong cross-correlation implies that
the absorber host-galaxies have halo-masses 1--2 times 10^{12} \msun.Comment: 3 pages, 2 figures, to appear in IAU 199 conf. proc.: "Probing
Galaxies through Quasar Absorption Lines," eds. Williams, Shu, Menard; minor
changes to match the edited versio
Multiphase Plasma in Sub-Damped Lyman Alpha Systems: A Hidden Metal Reservoir
We present a VLT/UVES spectrum of a proximate sub-damped Lyman-alpha
(sub-DLA) system at z=2.65618 toward the quasar Q0331-4505
(z_qso=2.6785+/-0.0030). Absorption lines of O I, Si II, Si III, Si IV, C II, C
III, C IV, Fe II, Al II, and O VI are seen in the sub-DLA, which has a neutral
hydrogen column density log N(H I)=19.82+/-0.05. The absorber is at a velocity
of 1820+/-250 km/s from the quasar; however, its low metallicity
[O/H]=-1.64+/-0.07, lack of partial coverage, lack of temporal variations
between observations taken in 2003 and 2006, and non-detection of N V imply the
absorber is not a genuine intrinsic system. By measuring the O VI column
density and assuming equal metallicities in the neutral and ionized gas, we
determine the column density of hot ionized hydrogen in this sub-DLA, and in
two other sub-DLAs with O VI drawn from the literature. Coupling this with
determinations of the typical amount of warm ionized hydrogen in sub-DLAs, we
confirm that sub-DLAs are a more important metal reservoir than DLAs, in total
comprising at least 6-22% of the metal budget at z~2.5.Comment: 5 pages, 3 color figures, accepted for publication in ApJ
The Keck+Magellan Survey for Lyman Limit Absorption I: The Frequency Distribution of Super Lyman Limit Systems
We present the results of a survey for super Lyman limit systems (SLLS;
defined to be absorbers with 19.0 <= log(NHI) <= 20.3 cm^-2) from a large
sample of high resolution spectra acquired using the Keck and Magellan
telescopes. Specifically, we present 47 new SLLS from 113 QSO sightlines. We
focus on the neutral hydrogen frequency distribution f(N,X) of the SLLS and its
moments, and compare these results with the Lyman-alpha forest and the damped
Lyman alpha systems (DLA; absorbers with log(NHI) >= 20.3 cm^-2). We find that
that f(N,X) of the SLLS can be reasonably described with a power-law of index
alpha = -1.43^{+0.15}_{-0.16} or alpha = -1.19^{+0.20}_{-0.21} depending on
whether we set the lower N(HI) bound for the analysis at 10^{19.0} cm^-2 or
10^{19.3}$ cm^-2, respectively. The results indicate a flattening in the slope
of f(N,X) between the SLLS and DLA. We find little evidence for redshift
evolution in the shape of f(N,X) for the SLLS over the redshift range of the
sample 1.68 < z < 4.47 and only tentative evidence for evolution in the zeroth
moment of f(N,X), the line density l_lls(X). We introduce the observable
distribution function O(N,X) and its moment, which elucidates comparisons of HI
absorbers from the Lyman-alpha through to the DLA. We find that a simple three
parameter function can fit O(N,X) over the range 17.0 <= log(NHI) <=22.0. We
use these results to predict that f(N,X) must show two additional inflections
below the SLLS regime to match the observed f(N,X) distribution of the
Lyman-alpha forest. Finally, we demonstrate that SLLS contribute a minor
fraction (~15%) of the universe's hydrogen atoms and, therefore, an even small
fraction of the mass in predominantly neutral gas.Comment: 15 pages, 10 figures, accepted to the Astrophysical Journal. Revision
includes updated reference
A Homogeneous Sample of Sub-DLAs I: Construction of the Sample and Chemical Abundance Measurements
In this first paper of a series, we report on the use of quasar spectra
obtained with the UVES high resolution spectrograph and available through the
ESO VLT archive to build the first sample of sub-DLA systems, absorbers with HI
column densities > 10^{19} cm^{-2} but lower than the classical definition of
damped Ly-alpha systems (DLAs) 2x10^{20} cm^{-2}. A systematic investigation of
the properties of these systems and a comparison with those of the DLAs (Paper
II of this series; Peroux et al. 2003b) is expected to provide new clues on the
association of high column density absorbers with galaxies and on the overall
evolution of the neutral hydrogen gas mass and metal content in the Universe.
In the spectra of 22 quasars which were found suitable for a sub-DLA search, we
identified 12 sub-DLAs and 1 borderline case between the DLA and sub-DLA
systems in the redshift interval z = 1.8-4.3. We measured the column densities
of HI and up to 16 ions of low-, intermediate- and high-ionization. We further
investigated the significance of the ionization corrections in the
determination of the chemical abundances from the low-ionization ions in the
sub-DLA HI column density range. Using the predictions of different ion ratios
as a function of the ionization parameter computed with the CLOUDY software
package, we have estimated that with the exception of one case, the ionization
corrections to the abundances of 9 systems for which we were able to constrain
the ionization parameter, are lower than 0.2 dex for all of the elements except
AlII and ZnII down to HI column densities of log N(HI) = 19.3 cm^{-2}. We
finally present the first sub-DLA chemical abundance database which contains
the abundance measurements of 11 different elements (O, C, Si, N, S, Mg, Al,
Fe, Ni, Zn, and Cr).Comment: 35 pages, 43 figures, Accepted for publication in MNRAS
(high-resolution figures available on request from the authors or in the
journal
The Role of Sub-damped Lyman-alpha Absorbers in the Cosmic Evolution of Metals
Observations of low mean metallicity of damped Lyman-alpha (DLA) quasar
absorbers at all redshifts studied appear to contradict the predictions for the
global mean interstellar metallicity in galaxies from cosmic chemical evolution
models. On the other hand, a number of metal-rich sub-DLA systems have been
identified recently, and the fraction of metal-rich sub-DLAs appears to be
considerably larger than that of metal-rich DLAs, especially at z < 1.5. In
view of this, here we investigate the evolution of metallicity in sub-DLAs. We
find that the mean Zn metallicity of the observed sub-DLAs may be higher than
that of the observed DLAs, especially at low redshifts, reaching a near-solar
level at z <~ 1. This trend does not appear to be an artifact of sample
selection, the use of Zn, the use of N_{HI}-weighting, or observational
sensitivity. While a bias against very low metallicity could be present in the
sub-DLA sample in some situations, this cannot explain the difference between
the DLA and sub-DLA metallicities at low z. The primary reason for the
difference between the DLAs and sub-DLAs appears to be the dearth of metal-rich
DLAs. We estimate the sub-DLA contribution to the total metal budget using
measures of their metallicity and comoving gas density. These calculations
suggest that at z <~ 1, the contribution of sub-DLAs to the total metal budget
may be several times that of DLAs. At higher redshifts also, there are
indications that the sub-DLAs may contribute significantly to the cosmic metal
budget.Comment: 9 pages, 2 figures, Accepted for Publication in the Astrophysical
Journa
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