8,352 research outputs found
Evidence for a bimodal distribution of Escherichia coli doubling times below a threshold initial cell concentration
Abstract Background In the process of developing a microplate-based growth assay, we discovered that our test organism, a native E. coli isolate, displayed very uniform doubling times (τ) only up to a certain threshold cell density. Below this cell concentration (≤ 100 -1,000 CFU mL-1 ; ≤ 27-270 CFU well-1) we observed an obvious increase in the τ scatter. Results Working with a food-borne E. coli isolate we found that τ values derived from two different microtiter platereader-based techniques (i.e., optical density with growth time {=OD[t]} fit to the sigmoidal Boltzmann equation or time to calculated 1/2-maximal OD {=tm} as a function of initial cell density {=tm[CI]}) were in excellent agreement with the same parameter acquired from total aerobic plate counting. Thus, using either Luria-Bertani (LB) or defined (MM) media at 37°C, τ ranged between 17-18 (LB) or 51-54 (MM) min. Making use of such OD[t] data we collected many observations of τ as a function of manifold initial or starting cell concentrations (CI). We noticed that τ appeared to be distributed in two populations (bimodal) at low CI. When CI ≤100 CFU mL-1 (stationary phase cells in LB), we found that about 48% of the observed τ values were normally distributed around a mean (μτ1) of 18 ± 0.68 min (± στ1) and 52% with μτ2 = 20 ± 2.5 min (n = 479). However, at higher starting cell densities (CI>100 CFU mL-1), the τ values were distributed unimodally (μτ = 18 ± 0.71 min; n = 174). Inclusion of a small amount of ethyl acetate to the LB caused a collapse of the bimodal to a unimodal form. Comparable bimodal τ distribution results were also observed using E. coli cells diluted from mid-log phase cultures. Similar results were also obtained when using either an E. coli O157:H7 or a Citrobacter strain. When sterile-filtered LB supernatants, which formerly contained relatively low concentrations of bacteria(1,000-10,000 CFU mL-1), were employed as a diluent, there was an evident shift of the two populations towards each other but the bimodal effect was still apparent using either stationary or log phase cells. Conclusion These data argue that there is a dependence of growth rate on starting cell density.</p
The Lense-Thirring effect in the Jovian system of the Galilean satellites and its measurability
In this paper we investigate the possibility of measuring the post-Newtonian
general relativistic gravitomagnetic Lense-Thirring effect in the Jovian system
of its Galilean satellites Io, Europa, Ganymede and Callisto in view of recent
developments in processing and modelling their optical observations spanning a
large time interval (125 years). The present day best observations have an
accuracy between several kilometers to few tens of kilometers, which is just
the order of magnitude of the Lense-Thirring shifts of the orbits of the
Galilean satellites over almost a century. From a comparison between analytical
development and numerical integration it turns out that, unfortunately, most of
the secular component of the gravitomagnetic signature is removed in the
process of fitting the initial conditions. Indeed, an estimation of the
magnitude of the Lense-Thirring effect in the ephemerides residuals is given;
the resulting residuals have a maximum magnitude of 20 meters only (over 125
years).Comment: Latex, 10 pages, 4 tables, 3 figures, 27 references. Invited paper
for a Special Issue of Int. J. Mod. Phys. D on the Lense-Thirring effect, D.
Grumiller edito
The optical transmission spectrum of the hot Jupiter HAT-P-32b: clouds explain the absence of broad spectral features?
We report Gemini-North GMOS observations of the inflated hot Jupiter
HAT-P-32b during two primary transits. We simultaneously observed two
comparison stars and used differential spectro-photometry to produce
multi-wavelength light curves. 'White' light curves and 29 'spectral' light
curves were extracted for each transit and analysed to refine the system
parameters and produce transmission spectra from 520-930nm in ~14nm bins. The
light curves contain time-varying white noise as well as time-correlated noise,
and we used a Gaussian process model to fit this complex noise model. Common
mode corrections derived from the white light curve fits were applied to the
spectral light curves which significantly improved our precision, reaching
typical uncertainties in the transit depth of ~2x10^-4, corresponding to about
half a pressure scale height. The low resolution transmission spectra are
consistent with a featureless model, and we can confidently rule out broad
features larger than about one scale height. The absence of Na/K wings or
prominent TiO/VO features is most easily explained by grey absorption from
clouds in the upper atmosphere, masking the spectral features. However, we
cannot confidently rule out clear atmosphere models with low abundances (~10^-3
solar) of TiO, VO or even metal hydrides masking the Na and K wings. A smaller
scale height or ionisation could also contribute to muted spectral features,
but alone are unable to to account for the absence of features reported here.Comment: 17 pages, 11 figures, 2 tables, accepted for publication in MNRA
A Gemini ground-based transmission spectrum of WASP-29b: a featureless spectrum from 515 to 720nm
We report Gemini-South GMOS observations of the exoplanet system WASP-29
during primary transit as a test case for differential spectrophotometry. We
use the multi-object spectrograph to observe the target star and a comparison
star simultaneously to produce multiple light curves at varying wavelengths.
The 'white' light curve and fifteen 'spectral' light curves are analysed to
refine the system parameters and produce a transmission spectrum from 515 to
720nm. All light curves exhibit time-correlated noise, which we model using a
variety of techniques. These include a simple noise rescaling, a Gaussian
process model, and a wavelet based method. These methods all produce consistent
results, although with different uncertainties. The precision of the
transmission spectrum is improved by subtracting a common signal from all the
spectral light curves, reaching a typical precision of ~1x10^-4 in transit
depth. The transmission spectrum is free of spectral features, and given the
non-detection of a pressure broadened Na feature, we can rule out the presence
of a Na rich atmosphere free of clouds or hazes, although we cannot rule out a
narrow Na core. This indicates that Na is not present in the atmosphere, and/or
that clouds/hazes play a significant role in the atmosphere and mask the broad
wings of the Na feature, although the former is a more likely explanation given
WASP-29b's equilibrium temperature of ~970 K, at which Na can form various
compounds. We also briefly discuss the use of Gaussian process and wavelet
methods to account for time correlated noise in transit light curves.Comment: 15 pages, 9 figures, 3 tables. Published in MNRAS. Figure 2 corrected
in version
A photometric and astrometric investigation of the brown dwarfs in Blanco 1
We present the results of a photometric and astrometric study of the low mass
stellar and substellar population of the young open cluster Blanco 1. We have
exploited J band data, obtained recently with the Wide Field Camera (WFCAM) on
the United Kingdom InfraRed Telescope (UKIRT), and 10 year old I and z band
optical imaging from CFH12k and Canada France Hawaii Telescope (CFHT), to
identify 44 candidate low mass stellar and substellar members, in an area of 2
sq. degrees, on the basis of their colours and proper motions. This sample
includes five sources which are newly discovered. We also confirm the lowest
mass candidate member of Blanco 1 unearthed so far (29MJup). We determine the
cluster mass function to have a slope of alpha=+0.93, assuming it to have a
power law form. This is high, but nearly consistent with previous studies of
the cluster (to within the errors), and also that of its much better studied
northern hemisphere analogue, the Pleiades.Comment: 8 Pages, 5 Figures, 2 Tables and 1 Appendix. Accepted for publication
in MNRA
Improved Searches for HI in Three Dwarf Spheroidal Galaxies
Previous searches for HI in our Galaxy's dwarf spheroidal companions have not
been complete enough to settle the question of whether or not these galaxies
have HI, especially in their outer parts. We present VLA observations of three
dwarf spheroidals: Fornax, Leo II, and Draco, all of which have known stellar
velocities. The new data show no HI emission or absorption. Column density
limits in emission are 4--7 x 10^18 atoms/cm^2 in the centers of the galaxies.
The importance of the new observations is that they cover larger areas than
previous searches and they are less plagued by confusion with foreground
(Galactic) HI. The apparent absence of neutral gas in the Fornax dwarf
spheroidal is especially puzzling because recent photometry shows evidence of
stars only 10^8 years old. We discuss whether the VLA observations could have
missed significant amounts of HI.Comment: 20 pages, 7 figures; to appear in the Astronomical Journa
ROSAT HRI X-ray Observations of the Open Globular Cluster NGC 288
A ROSAT HRI X-ray image was obtained of the open globular cluster NGC 288,
which is located near the South Galactic Pole. This is the first deep X-ray
image of this system. We detect a Low Luminosity Globular Cluster X-ray source
(LLGCX) RXJ005245.0-263449 with an X-ray luminosity of (5.5+-1.4)x10^32 ergs/s
(0.1-2.0 keV), which is located very close to the cluster center. There is
evidence for X-ray variability on a time scale of <~ 1 day. The presence of
this LLGCX in such an open cluster suggests that dense stellar systems with
high interaction rates are not needed to form LLGCXs. We also searched for
diffuse X-ray emission from NGC 288. Upper limits on the X-ray luminosities are
L_X^h < 9.5x10^32 ergs/s (0.52-2.02 keV) and L_X^s < 9.3x10^32 ergs/s
(0.11-0.41 keV). These imply upper limits to the diffuse X-ray to optical light
ratios in NGC 288 which are lower than the values observed for X-ray faint
early-type galaxies. This indicates that the soft X-ray emission in these
galaxies is due either to a component which is not present in globular clusters
(e.g., interstellar gas, or a stellar component which is not found in low
metallicity Population II systems), or to a relatively small number of bright
Low Mass X-ray Binaries (LMXBs).Comment: The Astrophysical Journal in press. Minor revisions to improve
presentation. 6 pages with 3 embedded Postscript figures in emulateapj.st
The NIR structure of the barred galaxy NGC253 from VISTA
[abridged] We used J and Ks band images acquired with the VISTA telescope as
part of the science verification to quantify the structures in the stellar disk
of the barred Sc galaxy NGC253. Moving outward from the galaxy center, we find
a nuclear ring within the bright 1 kpc diameter nucleus, then a bar, a ring
with 2.9 kpc radius. From the Ks image we obtain a new measure of the
deprojected length of the bar of 2.5 kpc. The bar's strength, as derived from
the curvature of the dust lanes in the J-Ks image, is typical of weak bars.
From the deprojected length of the bar, we establish the corotation radius
(R_CR=3 kpc) and bar pattern speed (Omega_b = 61.3 km /s kpc), which provides
the connection between the high-frequency structures in the disk and the
orbital resonances induced by the bar. The nuclear ring is located at the inner
Lindblad resonance. The second ring does not have a resonant origin, but it
could be a merger remnant or a transient structure formed during an
intermediate stage of the bar formation. The inferred bar pattern speed places
the outer Lindblad resonance within the optical disk at 4.9 kpc, in the same
radial range as the peak in the HI surface density. The disk of NGC253 has a
down-bending profile with a break at R~9.3 kpc, which corresponds to about 3
times the scale length of the inner disk. We discuss the evidence for a
threshold in star formation efficiency as a possible explanation of the steep
gradient in the surface brightness profile at large radii. The NIR photometry
unveils the dynamical response of the NGC253 stellar disk to its central bar.
The formation of the bar may be related to the merger event that determined the
truncation of stars and gas at large radii and the perturbation of the disk's
outer edge.Comment: Accepted for publication in Astronomy & Astrphysics. High resolution
pdf file is available at the following link:
https://www.dropbox.com/s/4o4cofs1lyjrtpv/NGC253.pd
‘I can’t accept that feeling’: Relationships between interoceptive awareness, mindfulness and eating disorder symptoms in females with, and at-risk of an eating disorder
Mindfulness based therapies (MBTs) for eating disorders show potential benefit for outcomes yet evidence is scarce regarding the mechanisms by which they influence remission from symptoms. One way that mindfulness approaches create positive outcomes is through enhancement of emotion regulation skills. Maladaptive emotion regulation is a key psychological feature of all eating disorders. The aim of the current study was to identify facets of emotion regulation involved in the relationship between mindfulness and maladaptive eating behaviours. In three cross-sectional studies, clinical (n=39) and non-clinical (n=137 and 119) female participants completed: 1) the Eating Disorder Inventory (EDI) eating specific scales (drive-for-thinness and bulimia) and the EDI psychological symptom scales (emotion dysregulation and interoceptive deficits); and 2) mindfulness, impulsivity, and emotion regulation questionnaires. In all samples mindfulness was significantly and inversely associated with EDI eating and psychological symptom scales, and impulsivity. In non-clinical samples interoceptive deficits mediated the relationship between mindfulness and EDI eating specific scales. Non-acceptance of emotional experience, a facet of interoceptive awareness, mediated the relationship between mindfulness and eating specific EDI scores. Further investigations could verify relationships identified so that mindfulness based approaches can be optimised to enhance emotion regulation skills in sufferers, and those at-risk, of eating disorders
Financial Crisis, Financial Systems, and the Performance of the Economy
Research Study Two: Financial Crisis, Financial Systems and the Performance of the Economy. A Study Prepared for Task Force D of the Commission on Money and Credit
- …