15,104 research outputs found
Preliminary Results for Embankment Dam Stepped Spillway Stilling Basin Research
A stilling basin is an energy dissipator for spillways and other hydraulic structures. Designed to generate a hydraulic jump, the structure is meant to contain the jump and return excess flow safely downstream. Traditional design for these structures was developed by United States Bureau of Reclamation (USBR) scientists. Tests were conducted for a range of expected flow conditions (i.e. Froude number, incoming flow depth, tailwater depth, etc.) with a smooth chute providing the incoming flow conditions. A common question among practicing engineers has become: is the stilling basin design criteria applicable if the approach entrance is a stepped chute? Scientists at the United States Department of Agriculture (USDA) Agricultural Research Service (ARS) Hydraulic Engineering Research Unit (HERU) has developed a research program to evaluate the stilling basin performance associated with stepped chutes. Physical model tests are conducted in a near prototype scale stepped chute facility. Stilling basin Types I, II, III, and IV are being tested. Preliminary results indicate the Froude number at the stepped chute toe ranges from 3.3 ≤ F ≤ 5.5. Hydraulic jumps within this Froude number range were observed to be oscillatory in nature and result in potentially undesirable wave action downstream of the stilling basin for the lower Froude numbers. Preliminary results indicate that the design criteria developed by USBR scientists are applicable for USBR Type IV stilling basins placed at the toe of stepped chutes. This research is expected to extend the knowledge base regarding stilling basins associated with stepped chutes
Experimental measurement of focused wave group and solitary wave overtopping
Prediction of individual wave overtopping events is important in assessing danger to life and property, but data are sparse and hydrodynamic understanding is lacking. Laboratory-scale waves of three distinct types were generated at the Coastal Research Facility to model extreme waves overtopping a trapezoidal embankment. These comprised wave groups of compact form, wave groups embedded in a background wave field, and a solitary wave. The inshore wave propagation was measured and the time variation of overtopping rate estimated. The total volume overtopped was measured directly. The experiments provide well-defined data without uncertainty due to the effect of reflection on the incident wave train. The dependence of overtopping on a range of wave shapes is thus determined and the influence of wave-wave interactions on overtopping assessed. It was found that extreme overtopping may arise from focused waves with deep troughs rather than large crests. Furthermore, overtopping waves can be generated from small wave packets without affecting the applicability of results to cases in which there are surrounding waves. Finally, overtopping from a solitary wave is comparable with overtopping from focused wave groups of the same amplitude. © 2011 Copyright International Association for Hydro-Environment Engineering and Research
1.65 micrometers (H-band) surface photometry of galaxies. III: observations of 558 galaxies with the TIRGO 1.5m telescope
We present near-infrared H-band (1.65 micron) surface photometry of 558
galaxies in the Coma Supercluster and in the Virgo cluster. This data set,
obtained with the Arcetri NICMOS3 camera ARNICA mounted on the Gornergrat
Infrared Telescope, is aimed at complementing, with observations of mostly
early-type objects, our NIR survey of spiral galaxies in these regions,
presented in previous papers of this series. Magnitudes at the optical radius,
total magnitudes, isophotal radii and light concentration indices are derived.
We confirm the existence of a positive correlation between the near-infrared
concentration index and the galaxy H-band luminosity. (Tables 1 and 2 are only
available in electronic form upon request to [email protected])Comment: 12 pages, 6 figures. Accepted for publication in A&A
Molecular depletion times and the CO-to-H2 conversion factor in metal-poor galaxies
Tracing molecular hydrogen content with carbon monoxide in low-metallicity
galaxies has been exceedingly difficult. Here we present a new effort, with
IRAM 30-m observations of 12CO(1-0) of a sample of 8 dwarf galaxies having
oxygen abundances ranging from 12+logO/H=7.7 to 8.4. CO emission is detected in
all galaxies, including the most metal-poor galaxy of our sample (0.1 Zsun); to
our knowledge this is the largest number of 12CO(1-0) detections ever reported
for galaxies with 12+logO/H<=8 (0.2 Zsun) outside the Local Group. We calculate
stellar masses (Mstar) and star-formation rates (SFRs), and analyze our results
by combining our observations with galaxy samples from the literature.
Extending previous results for a correlation of the molecular gas depletion
time, tau(dep), with Mstar and specific SFR (sSFR), we find a variation in
tau(dep) of a factor of 200 or more (from <50 Myr to 10 Gyr) over a spread of
1000 in sSFR and Mstar. We exploit the variation of tau(dep) to constrain the
CO-to-H2 mass conversion factor alpha(CO) at low metallicity, and assuming a
power-law variation find alpha(CO) \propto (Z/Zsun)^1.9, similar to results
based on dust continuum measurements compared with gas mass. By including HI
measurements, we show that the fraction of total gas mass relative to the
baryonic mass is higher in galaxies that are metal poor, of low mass, and of
high sSFR. Finally, comparisons of the data with star-formation models of the
molecular gas phases suggest that, at metallicities Z/Zsun<=0.2, there are some
discrepancies with model predictions.Comment: 18 pages, 15 figures, accepted for publication in A&
Star-forming dwarf galaxies in the Virgo cluster: the link between molecular gas, atomic gas, and dust
We present CO(1-0) and CO(2-1) observations of a sample of 20
star-forming dwarfs selected from the Herschel Virgo Cluster Survey, with
oxygen abundances ranging from 12 + log(O/H) ~ 8.1 to 8.8. CO emission is
observed in ten galaxies and marginally detected in another one. CO fluxes
correlate with the FIR 250 m emission, and the dwarfs follow the same
linear relation that holds for more massive spiral galaxies extended to a wider
dynamical range. We compare different methods to estimate H2 molecular masses,
namely a metallicity-dependent CO-to-H2 conversion factor and one dependent on
H-band luminosity. The molecular-to-stellar mass ratio remains nearly constant
at stellar masses <~ 10 M, contrary to the atomic hydrogen
fraction, M/M, which increases inversely with M. The flattening
of the M/M ratio at low stellar masses does not seem to be related
to the effects of the cluster environment because it occurs for both
HI-deficient and HI-normal dwarfs. The molecular-to-atomic ratio is more
tightly correlated with stellar surface density than metallicity, confirming
that the interstellar gas pressure plays a key role in determining the balance
between the two gaseous components of the interstellar medium. Virgo dwarfs
follow the same linear trend between molecular gas mass and star formation rate
as more massive spirals, but gas depletion timescales, , are not
constant and range between 100 Myr and 6 Gyr. The interaction with the Virgo
cluster environment is removing the atomic gas and dust components of the
dwarfs, but the molecular gas appears to be less affected at the current stage
of evolution within the cluster. However, the correlation between HI deficiency
and the molecular gas depletion time suggests that the lack of gas
replenishment from the outer regions of the disc is lowering the star formation
activity.Comment: 19 pages, 11 figures, accepted for publication in Astronomy &
Astrophysic
Scaling relations and baryonic cycling in local star-forming galaxies: II. Gas content and star-formation efficiency
Assessments of the cold-gas reservoir in galaxies are a cornerstone for understanding star-formation processes and the role of feedback and baryonic cycling in galaxy evolution. Here we exploit a sample of 392 galaxies (dubbed MAGMA, Metallicity and Gas for Mass Assembly), presented in a recent paper, to quantify molecular and atomic gas properties across a broad range in stellar mass, Mstar, from ∼107 - 1011 M⊙. First, we find the metallicity (Z) dependence of the conversion factor for CO luminosity to molecular H2 mass αCO to be shallower than previous estimates, with αCO∝ (Z/Z⊙)-1.55. Second, molecular gas mass MH2 is found to be strongly correlated with Mstar and star-formation rate (SFR), enabling predictions of MH2 good to within ∼0.2 dex; analogous relations for atomic gas mass MHI and total gas mass Mgas are less accurate, ∼0.4 dex and ∼0.3 dex, respectively. Indeed, the behavior of atomic gas mass MHI in MAGMA scaling relations suggests that it may be a third, independent variable that encapsulates information about the circumgalactic environment and gas accretion. If Mgas is considered to depend on MHI, together with Mstar and SFR, we obtain a relation that predicts Mgas to within ∼0.05 dex. Finally, the analysis of depletion times and the scaling of MHI/Mstar and MH2/Mstar over three different mass bins suggests that the partition of gas and the regulation of star formation through gas content depends on the mass regime. Dwarf galaxies (Mstar∝ 3 × 109 M⊙) tend to be overwhelmed by (H » I) accretion, and despite short τH2 (and thus presumably high star-formation efficiency), star formation is unable to keep up with the gas supply. For galaxies in the intermediate Mstar "gas-equilibrium"bin (3 × 109 M⊙ ≲ Mstar ≲ 3 × 1010 M⊙), star formation proceeds apace with gas availability, and H I and H2 are both proportional to SFR. In the most massive "gas-poor, bimodality"regime (Mstar ≳ 3 × 1010 M⊙), H I does not apparently participate in star formation, although it generally dominates in mass over H2. Our results confirm that atomic gas plays a key role in baryonic cycling, and is a fundamental ingredient for current and future star formation, especially in dwarf galaxies
Scaling relations and baryonic cycling in local star-forming galaxies: II. Gas content and star-formation efficiency
Assessments of the cold-gas reservoir in galaxies are a cornerstone for
understanding star-formation processes and the role of feedback and baryonic
cycling in galaxy evolution. Here we exploit a sample of 392 galaxies (dubbed
MAGMA, Metallicity and Gas for Mass Assembly), presented in a recent paper, to
quantify molecular and atomic gas properties across a broad range in stellar
mass, Mstar, from Msun. First, we find the metallicity
() dependence of alpha_CO to be shallower than previous estimates, with
alpha_CO. Second, molecular gas mass MH2 is found
to be strongly correlated with Mstar and star-formation rate (SFR), enabling
predictions of MH2 good to within 0.2 dex. The behavior of atomic gas
mass MHI in MAGMA scaling relations suggests that it may be a third,
independent variable that encapsulates information about the circumgalactic
environment and gas accretion. If Mgas is considered to depend on MHI, together
with Mstar and SFR, we obtain a relation that predicts Mgas to within
0.05 dex. Finally, the analysis of depletion times and the scaling of
MHI/Mstar and MH2/Mstar over three different mass bins suggests that the
partition of gas and the regulation of star formation through gas content
depends on the mass regime. Dwarf galaxies tend to be overwhelmed by (HI)
accretion, while for galaxies in the intermediate Mstar "gas-equilibrium" bin,
star formation proceeds apace with gas availability. In the most massive
"gas-poor, bimodality" galaxies, HI does not apparently participate in star
formation, although it generally dominates in mass over H2. Our results confirm
that atomic gas plays a key role in baryonic cycling, and is a fundamental
ingredient for current and future star formation, especially in dwarf galaxies.
(abridged for arXiv)Comment: 22 pages, 15 figures, 2 appendices, accepted for publication in
Astronomy & Astrophysic
ALMA observations of cool dust in a low-metallicity starburst, SBS0335-052
We present Atacama Large Millimeter/submillimeter Array (ALMA) Cycle 0 Band 7
observations of an extremely metal-poor dwarf starburst galaxy in the Local
Universe, SBS0335-052 (12+log(O/H)~7.2). With these observations, dust is
detected at 870micron (ALMA Band 7), but 87% of the flux in this band is due to
free-free emission from the starburst. We have compiled a spectral energy
distribution (SED) of SBS0335-052 that spans almost 6 orders of magnitude in
wavelength and fit it with a spherical dust shell heated by a single-age
stellar population; the best-fit model gives a dust mass of (3.8+/-0.6)x10^4
Msun. We have also constructed a SED including Herschel archival data for
IZw18, another low-metallicity dwarf starburst (12+log(O/H)=7.17), and fit it
with a similar model to obtain a dust mass of (3.4+/-1.0)x10^2 Msun. Compared
with their atomic gas mass, the dust mass of SBS0335-052 far exceeds the
prediction of a linear trend of dust-to-gas mass ratio with metallicity, while
IZw18 falls far below. We use gas scaling relations to assess a putative
missing gas component in both galaxies and find that the missing, possibly
molecular, gas in SBS0335-052 is a factor of 6 times higher than the value
inferred from the observed HI column density; in IZw18 the missing component is
4 times smaller. Ultimately, despite their similarly low metallicity, the
differences in gas and dust column densities in SBS0335-052 and IZw18 suggest
that metal abundance does not uniquely define star-formation processes. At some
level, self-shielding and the survival of molecules may depend just as much on
gas and dust column density as on metallicity. The effects of low metallicity
may at least be partially compensated for by large column densities in the
interstellar medium.Comment: 15 pages, 11 figures, accepted for publication in A&
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