620 research outputs found
Orientational and phase-coexistence behaviour of hard rod-sphere mixtures
Results are presented from Monte Carlo simulations of bulk mixtures of Hard Gaussian Overlap particles with an aspect ratio of 3:1 and hard spheres with diameters equal to the breadths of the rods. For sphere number-concentrations of 50% and lower, compression of the isotropic fluid results in formation of a homogeneous (i.e. compositionally mixed) nematic phase. The volume fraction of this isotropic-nematic transition is found to increase approximately linearly with sphere concentration. On compression to higher volume fractions, however, this homogeneous nematic phase separates out into coexisting nematic and isotropic phases.</p
Methods for the analysis of histone H3 and H4 acetylation in blood
LBH589 is one of the many histone deacetylase inhibitors (HDACi) that are currently in clinical trial. Despite their wide-spread use, there is little literature available describing the typical levels of histone acetylation in untreated peripheral blood, the treatment and storage of samples to retain optimal measurement of histone acetylation nor methods by which histone acetylation analysis may be monitored and measured during the course of a patient’s treatment. In this study, we have used cord or peripheral blood as a source of human leukocytes, performed a comparative analysis of sample processing methods and developed a flow cytometric method suitable for monitoring histone acetylation in isolated lymphocytes and liquid tumors. Western blotting and immunohistochemistry techniques have also been addressed. We have tested these methods on blood samples collected from four patients treated with LBH589 as part of an Australian Children’s Cancer Clinical Trial (CLBH589AAU03T) and show comparable results when comparing in vitro and in vivo data. This paper does not seek to correlate histone acetylation levels in peripheral blood with clinical outcome but describes methods of analysis that will be of interest to clinicians and scientists monitoring the effects of HDACi on histone acetylation in blood samples in clinical trials or in related research studies
Abrupt reversal in emissions and atmospheric abundance of HCFC-133a (CF3CH2Cl)
Hydrochlorofluorocarbon HCFC-133a (CF3CH2Cl) is an anthropogenic compound whose consumption for emissive use is restricted under the Montreal Protocol. A recent study showed rapidly increasing atmospheric abundances and emissions. We report that, following this rise, the at- mospheric abundance and emissions have declined sharply in the past three years. We find a Northern Hemisphere HCFC-133a increase from 0.13 ppt (dry air mole fraction in parts-per-trillion) in 2000 to 0.50 ppt in 2012âmid-2013 followed by an abrupt reversal to 0.44 ppt by early 2015. Global emissions derived from these observations peaked at 3.1 kt in 2011, followed by a rapid decline of 0.5 kt yrâ2 to 1.5 kt yrâ1 in 2014. Sporadic HCFC-133a pollution events are detected in Europe from our high-resolution HCFC-133a records at three European stations, and in Asia from sam- ples collected in Taiwan. European emissions are estimated to be <0.1 kt yrâ1 although emission hotspots were identi- fied in France
LBT and Spitzer Spectroscopy of Star-Forming Galaxies at 1 < z < 3: Extinction and Star Formation Rate Indicators
We present spectroscopic observations in the rest-frame optical and near- to
mid-infrared wavelengths of four gravitationally lensed infrared (IR) luminous
star-forming galaxies at redshift 1 < z < 3 from the LUCIFER instrument on the
Large Binocular Telescope and the Infrared Spectrograph on Spitzer. The sample
was selected to represent pure, actively star-forming systems, absent of active
galactic nuclei. The large lensing magnifications result in high
signal-to-noise spectra that can probe faint IR recombination lines, including
Pa-alpha and Br-alpha at high redshifts. The sample was augmented by three
lensed galaxies with similar suites of unpublished data and observations from
the literature, resulting in the final sample of seven galaxies. We use the IR
recombination lines in conjunction with H-alpha observations to probe the
extinction, Av, of these systems, as well as testing star formation rate (SFR)
indicators against the SFR measured by fitting spectral energy distributions to
far-IR photometry. Our galaxies occupy a range of Av from ~0 to 5.9 mag, larger
than previously known for a similar range of IR luminosities at these
redshifts. Thus, estimates of SFR even at z ~ 2 must take careful count of
extinction in the most IR luminous galaxies. We also measure extinction by
comparing SFR estimates from optical emission lines with those from far-IR
measurements. The comparison of results from these two independent methods
indicates a large variety of dust distribution scenarios at 1 < z < 3. Without
correcting for dust extinction, the H-alpha SFR indicator underestimates the
SFR; the size of the necessary correction depends on the IR luminosity and dust
distribution scenario. Individual SFR estimates based on the 6.2 micron PAH
emission line luminosity do not show a systematic discrepancy with extinction,
although a considerable, ~0.2 dex scatter is observed.Comment: Accepted for publication in The Astrophysical Journal; 14 pages, 8
figure
Theoretical analysis of the focusing of acoustic waves by two-dimensional sonic crystals
Motivated by a recent experiment on acoustic lenses, we perform numerical
calculations based on a multiple scattering technique to investigate the
focusing of acoustic waves with sonic crystals formed by rigid cylinders in
air. The focusing effects for crystals of various shapes are examined. The
dependance of the focusing length on the filling factor is also studied. It is
observed that both the shape and filling factor play a crucial role in
controlling the focusing. Furthermore, the robustness of the focusing against
disorders is studied. The results show that the sensitivity of the focusing
behavior depends on the strength of positional disorders. The theoretical
results compare favorably with the experimental observations, reported by
Cervera, et al. (Phys. Rev. Lett. 88, 023902 (2002)).Comment: 8 figure
Trends in health outcomes for family caregivers of hipâfractured elders during the first 12âmonths after discharge
Aim.â This article reports on trends in health outcomes for family caregivers of hipâfractured patients and the effects of social support on these outcomes. Background.â Little is known about the impact of caregiving on the health outcomes of family caregivers of patients with hip fracture. Method.â For this prospective, correlational study, data were collected from 135 family caregivers of hipâfractured elders (2001â2005). Data on healthârelated quality of life and social support were collected from family caregivers at 1, 3, 6 and 12âmonths after discharge of the older hipâfractured patient. Findings.â During the 12âmonths after the patientsâ discharge, family caregiversâ scores improved significantly in role performanceârelated scales, including bodily pain, social function, role limitations due to emotional problems and role limitations due to physical problems. However, caregiversâ scores for general health and mental health were significantly lower at 12âmonths [59·91 ( sd â=â24·54) and 65·91 ( sd â=â14·36) respectively] than at 1âmonth after discharge [64·35 ( sd â=â23·29) and 67·94 ( sd â=â18·47) respectively]. The trends for most subscale scores for healthârelated quality of life were positively related to perceived availability of social support. Conclusions.â Caring for a hipâfractured older family member over a sustained period may enhance family caregiversâ role performance, but have a negative impact on their perceived general health and mental health. These results suggest that home care nurses should develop interventions early after discharge to assess and improve family caregiversâ health perception, mental health and social support.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/90349/1/j.1365-2648.2011.05778.x.pd
An Accounting of the Dust-Obscured Star Formation and Accretion Histories Over the Last ~11~Billion Years
(Abridged) We report on an accounting of the star formation and accretion
driven energetics of 24um detected sources in GOODS North. For sources having
infrared (IR; 8-1000um) luminosities >3x10^12 L_sun when derived by fitting
local SEDs to 24um photometry alone, we find these IR luminosity estimates to
be a factor of ~4 times larger than those estimated when the SED fitting
includes additional 16 and 70um data (and in some cases mid-infrared
spectroscopy and 850um data). This discrepancy arises from the fact that high
luminosity sources at z>>0 appear to have far- to mid-infrared ratios, as well
as aromatic feature equivalent widths, typical of lower luminosity galaxies in
the local Universe. Using our improved estimates for IR luminosity and AGN
contributions, we investigate the evolution of the IR luminosity density versus
redshift arising from star formation and AGN processes alone. We find that,
within the uncertainties, the total star formation driven IR luminosity density
is constant between 1.15 < z < 2.35, although our results suggest a slightly
larger value at z>2. AGN appear to account for <18% of the total IR luminosity
density integrated between 0< z < 2.35, contributing <25% at each epoch. LIRG
appear to dominate the star formation rate (SFR) density along with normal
star-forming galaxies (L_IR < 10^11 L_sun) between 0.6 < z < 1.15. Once beyond
z >2, the contribution from ultraluminous infrared galaxies ULIRGs becomes
comparable with that of LIRGs. Using our improved IR luminosity estimates, we
find existing calibrations for UV extinction corrections based on measurements
of the UV spectral slope typically overcorrect UV luminosities by a factor of
~2, on average, for our sample of 24um-selected sources; accordingly we have
derived a new UV extinction correction more appropriate for our sample.Comment: Accepted for publication in Ap
The ~0.9 mJy sample: A mid-infrared spectroscopic catalog of 150 infrared-luminous, 24 micron selected galaxies at 0.3<z<3.5
We present a catalog of mid-infrared (MIR) spectra of 150 infrared (IR)
luminous galaxies in the Spitzer extragalactic first look survey obtained with
IRS on board Spitzer. The sample is selected to be brighter than ~0.9 mJy at 24
micron and it has a z distribution in the range [0.3,3.5] with a peak at z=1.
It primarily comprises ultraluminous IR galaxies at z>1 and luminous IR
galaxies at z<1, as estimated from their monochromatic 14 micron luminosities.
The number of sources with spectra that are dominated by an active galactic
nucleus (AGN) continuum is 49, while 39 sources have strong, star-formation
related features. For this classification, we used the equivalent width (EW) of
the 11.3 micron polycyclic aromatic hydrocarbon (PAH) feature. Several
intermediate/high z starbursts have higher PAH EW than local ULIRGs. An
increase in the AGN activity is observed with increasing z and luminosity,
based on the decreasing EW of PAHs and the increasing [NeIII]/[NeII] ratio.
Spectral stacking leads to the detection of the 3.3 micron PAH, the H2 0-0 S(1)
and S(3) lines, and the [NeV] line. We observe differences in the flux ratios
of PAHs in the stacked spectra of IR-luminous galaxies with z or luminosity,
which are not due to extinction effects. When placing the observed galaxies on
IR color-color diagrams, we find that the wedge defining AGN comprises most
sources with continuum-dominated spectra, but also contains many starbursts.
The comparison of the 11.3 micron PAH EW and the H-band effective radius,
measured from HST data, indicates that sources with EW>2 micron, are typically
more extended than ~3 kpc. However, there is no strong correlation between the
MIR spectral type and the near-IR extent of the sources. [Abridged].Comment: accepted for publication in the Astrophysical Journa
Galaxy Group at z=0.3 Associated with the Damped Lyman Alpha System Towards Quasar Q1127-145
(Abridged) We performed a spectroscopic galaxy survey, complete to m<20.3
(L_B>0.15L_B* at z=0.3), within 100x100" of the quasar Q1127-145 (z=1.18). The
VLT/UVES quasar spectrum contains three z<0.33 MgII absorption systems. We
obtained eight new galaxy redshifts, adding to the four previously known, and
galaxy star formation rates and metallicities were computed where possible. A
strong MgII system [W_r(2796)=1.8A], which is a known DLA, had three previously
identified galaxies; we found two additional galaxies associated with this
system. These five galaxies form a group with diverse properties, such as a
luminosity range of 0.04<L_B<0.63L_B*, an impact parameter range of 17<D<241kpc
and velocity dispersion of 115km/s. The DLA group galaxy redshifts span beyond
the 350km/s velocity spread of the metallic absorption lines of the DLA itself.
The two brightest group galaxies have SFRs of a few Msun/yr and should not have
strong winds. We have sufficient spectroscopic information to directly compare
three of the five group galaxies' (emission-line) metallicities with the DLA
(absorption) metallicity: the DLA metallicity is 1/10th solar, substantially
lower than the three galaxies' which range between less than 1/2 solar to solar
metallicity. HST/WFPC-2 imaging shows perturbed morphologies for the three
brightest group galaxies, with tidal tails extending 25kpc. We favor a scenario
where the DLA absorption originates from tidal debris in the group environment.
Another absorber exhibits weak MgII absorption [W_r(2796)=0.03A] and had a
previously identified galaxy at a similar redshift. We have identified a second
galaxy associated with this system. Both galaxies have solar metallicities and
unperturbed morphologies. The SFR of one galaxy is much lower than expected for
strong outflows. Finally, we have identified five galaxies at large impact
parameters with no associated MgII absorption.Comment: 15 pages, 7 figures, 5 tables. Accepted for publication in MNRAS
Ubiquitous outflows in DEEP2 spectra of star-forming galaxies at z=1.4
Galactic winds are a prime suspect for the metal enrichment of the
intergalactic medium and may have a strong influence on the chemical evolution
of galaxies and the nature of QSO absorption line systems. We use a sample of
1406 galaxy spectra at z~1.4 from the DEEP2 redshift survey to show that
blueshifted Mg II 2796, 2803 A absorption is ubiquitous in starforming galaxies
at this epoch. This is the first detection of frequent outflowing galactic
winds at z~1. The presence and depth of absorption are independent of AGN
spectral signatures or galaxy morphology; major mergers are not a prerequisite
for driving a galactic wind from massive galaxies. Outflows are found in
coadded spectra of galaxies spanning a range of 30x in stellar mass and 10x in
star formation rate (SFR), calibrated from K-band and from MIPS IR fluxes. The
outflows have column densities of order N_H ~ 10^20 cm^-2 and characteristic
velocities of ~ 300-500 km/sec, with absorption seen out to 1000 km/sec in the
most massive, highest SFR galaxies. The velocities suggest that the outflowing
gas can escape into the IGM and that massive galaxies can produce
cosmologically and chemically significant outflows. Both the Mg II equivalent
width and the outflow velocity are larger for galaxies of higher stellar mass
and SFR, with V_wind ~ SFR^0.3, similar to the scaling in low redshift
IR-luminous galaxies. The high frequency of outflows in the star-forming galaxy
population at z~1 indicates that galactic winds occur in the progenitors of
massive spirals as well as those of ellipticals. The increase of outflow
velocity with mass and SFR constrains theoretical models of galaxy evolution
that include feedback from galactic winds, and may favor momentum-driven models
for the wind physics.Comment: Accepted by ApJ. 25 pages, 17 figures. Revised to add discussions of
intervening absorbers and AGN-driven outflows; conclusions unchange
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