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Background Children with atopic dermatitis (AD) may have disturbed sleep, affected self-esteem and decreased quality of life, likely interfering with performance in school. Objectives To examine the association between hospital-managed paediatric AD, school performance and cognitive function. Methods In this cross-sectional study we linked data from the Danish national registers and identified three populations between 2001 and 2019. Population 1 comprised children with graduation grades registered from lower secondary school, population 2 comprised adolescents with registration of an upper secondary graduation mean, and population 3 comprised male conscripts with registration of an IQ test score. AD was defined as a hospital diagnostic code (inpatient or outpatient) prior to the exam or conscription date, and was stratified according to severity, activity and atopic comorbidity. Outcomes included graduation mean from lower and upper secondary school, special educational assistance in primary and lower secondary school, and IQ at conscription. Results In total, 770 611 (12 137 with AD), 394 193 (6261 with AD) and 366 182 (4539 with AD) children and adolescents were included in populations 1 (lower secondary graduation), 2 (upper secondary graduation) and 3 (conscription), respectively. In lower secondary school, children with severe AD had significantly lower overall, written and oral graduation grade means compared with children with mild AD: respectively, difference −0.29 [95% confidence interval (CI) −0.45 to −0.13, P < 0.001], difference −0.26 (95% CI −0.42 to −0.10, P = 0.0016) and difference −0.30 (95% CI −0.49 to −0.11, P = 0.0018). In upper secondary school, adolescents with AD performed similarly to their peers without AD. Young men with AD scored significantly lower IQ test means at conscription examination than male conscripts without AD: difference −0.60 (95% CI −0.87 to −0.32, P < 0.001). Conclusions AD, in particular when severe, is associated with lower school performance in childhood and IQ in young men, which can interfere with academic achievements in life. Optimization of treatment of children with AD and specific educational support to children with severe AD could be needed.

We present a self-locking laser system that does not require operator interventions. The system automatically finds a desired atomic transition and subsequently locks to it. Moreover, it has the ability to automatically detect if the laser is out of lock and activate the re-locking process. The design was implemented on two different diode lasers, a distributed Bragg reflector (DBR) diode laser and a Fabry Perot (FP) diode laser, used as a repump laser for a magneto-optical trap in a laser cooling experiment and a Raman laser for a four-level Raman transition experiment, respectively. The design relies on frequency modulation transfer spectroscopy to obtain a sub-Doppler atomic spectrum of rubidium-85. This spectrum is then demodulated to obtain zero-crossing linear slopes at the exact points of each atomic and crossover transition. The frequency modulation, the signal analysis, and the automatic locking and re-locking of the lasers are all implemented using an Arduino Due microcontroller. The lock loop has a bandwidth of 7 kHz. The lasers used for the design are characterized, and the robustness of the lock is analyzed. The achieved linewidths of DBR and FP lasers are 1.4 and 5.5 MHz, respectively. The frequency drifts of both lasers are a few 100 kHz over a course of days. The capture range of the locking system is up to 4.9 GHz for the DBR laser and 725 MHz for the FP laser. Both lasers performed well under actual experimental conditions.

The reasons for peer education's ascendance as a core pedagogy in sex education are as much historical as they are reasonable or ethical. This article traces the history of peer-led sex education from the 1970s to the 1990s against the backdrop of New York City's financial ruin, social unrest, and a public health crisis. Starting with an analysis of the Student Coalition for Relevant Sex Education's Peer Information Project, founded in 1974, it investigates the application of new pedagogical techniques, the interplay between pedagogy and bureaucracy, and the transformation of school culture. Peer education thrived when educators and activists agreed that young people were more likely to accept advice from other young people, a reasonable contention that was nonetheless underassessed. Yet peer education's least intriguing attribute proved to be its most important characteristic: it could be quickly and inexpensively enacted. When HIV/AIDS began to decimate New York City's adolescent population, and the Board of Education proved slow and contradictory in its actions, the city turned to peer education, henceforth coupling the concepts of sex education and peer education.

Aims: We aim to study the spot evolution and differential rotation in the magnetically active cool K-type giant star sigma Gem from broadband photometry and continuous spectroscopic observations that span 150 nights. Methods: We use high-resolution, high signal-to-noise ratio spectra obtained with the Hertzsprung SONG telescope to reconstruct surface (photospheric) temperature maps with Doppler imaging techniques. The 303 observations span 150 nights and allow for a detailed analysis of the spot evolution and surface differential rotation. The Doppler imaging results are compared to simultaneous broadband photometry from the Tennessee State University T3 0.4 m Automated Photometric Telescope. The activity from the stellar chromosphere, which is higher in the stellar atmosphere, is also studied using SONG observations of Balmer H alpha line profiles and correlated with the photospheric activity. Results: The temperature maps obtained during eight consecutive stellar rotations show mainly high-latitude or polar spots, with the main spot concentrations above latitude 45 deg. The spots concentrate around phase 0.25 near the beginning of our observations and around phase 0.75 towards the end. The photometric observations confirm a small jump in spot phases that occurred in February 2016. The cross-correlation of the temperature maps reveals rather strong solar-like differential rotation, giving a relative surface differential rotation coefficient of $\alpha$ = 0.10 +/- 0.02. There is a weak correlation between the locations of starspots and enhanced emission in the chromosphere at some epochs., Comment: 19 pages, 10 figures, accepted for publication in Astronomy & Astrophysics, in the published version the Tables B1 and B2 will only be available via CDS

Using the Hamilton Echelle Spectrograph at Lick Observatory, we have obtained precise radial velocities (RVs) of a sample of 373 G- and K-giant stars over more than 12 years, leading to the discovery of several single and multiple planetary systems. The RVs of the long-period (~53 years) spectroscopic binary $\epsilon$ Cyg (HIP 102488) are found to exhibit additional regular variations with a much shorter period (~291 days). We intend to improve the orbital solution of the $\epsilon$ Cyg system and attempt to identify the cause of the nearly periodic shorter period variations, which might be due to an additional substellar companion. We used precise RV measurements of the K-giant star $\epsilon$ Cyg from Lick Observatory, in combination with a large set of RVs collected more recently with the SONG telescope, as well as archival data sets. Our Keplerian model to the RVs characterizes the orbit of the spectroscopic binary to higher precision than achieved previously, resulting in a semi-major axis of $a = 15.8 \mathrm{AU}$, an eccentricity of $e = 0.93$, and a minimum mass of the secondary of $m \sin i = 0.265 M_\odot$. Additional short-period RV variations closely resemble the signal of a Jupiter-mass planet orbiting the evolved primary component with a period of $291 \mathrm{d}$, but the period and amplitude of the putative orbit change strongly over time. Furthermore, in our stability analysis of the system, no stable orbits could be found in a large region around the best fit. Both of these findings deem a planetary cause of the RV variations unlikely. Most of the investigated alternative scenarios, such as an hierarchical triple or stellar spots, also fail to explain the observed variability convincingly. Due to its very eccentric binary orbit, it seems possible, however, that $\epsilon$ Cyg could be an extreme example of a heartbeat system., Comment: 17 pages, 13 figures, accepted to A&A

We report the detection of a Saturn-size exoplanet orbiting HD 332231 (TOI 1456) in light curves from the Transiting Exoplanet Survey Satellite (TESS). HD 332231, an F8 dwarf star with a V-band magnitude of 8.56, was observed by TESS in Sectors 14 and 15. We detect a single-transit event in the Sector 15 presearch data conditioning (PDC) light curve. We obtain spectroscopic follow-up observations of HD 332231 with the Automated Planet Finder, Keck I, and SONG telescopes. The orbital period we infer from the radial velocity (RV) observations leads to the discovery of another transit in Sector 14 that was masked by PDC due to scattered light contamination. A joint analysis of the transit and RV data confirms the planetary nature of HD 332231 b, a Saturn-size ($0.867^{+0.027}_{-0.025} \; R_{\rm J}$), sub-Saturn-mass ($0.244\pm0.021 \; M_{\rm J}$) exoplanet on a 18.71 day circular orbit. The low surface gravity of HD 332231 b and the relatively low stellar flux it receives make it a compelling target for transmission spectroscopy. Also, the stellar obliquity is likely measurable via the Rossiter-McLaughlin effect, an exciting prospect given the 0.14 au orbital separation of HD 332231 b. The spectroscopic observations do not provide substantial evidence for any additional planets in the HD 332231 system, but continued RV monitoring is needed to further characterize this system. We also predict that the frequency and duration of masked data in the PDC light curves for TESS Sectors 14-16 could hide transits of some exoplanets with orbital periods between 10.5 and 17.5 days., Comment: 17 pages, 9 figures, 4 tables. Published in the Astronomical Journal

We present new Doppler images of both components of the double-lined binary $\sigma^{2}$ CrB, based on the high-resolution spectroscopic data collected during 11 nights in 2015 March--April. The observed spectra form two independent data sets with sufficient phase coverage. We apply the least-squares deconvolution to all observed spectra to obtain high signal-to-noise mean profiles, from which we derive the Doppler images of both components of $\sigma^{2}$ CrB simultaneously. The surfaces of both F9 and G0 components are dominated by pronounced polar spots. The F9 component exhibits a weak spot at latitude 30$^{\circ}$ and its mid-to-low latitudes are relatively featureless. The G0 star shows an extended spot structure at latitude 30$^{\circ}$, and its surface spot coverage is larger than that of the F9 star, which suggests a higher level of magnetic activity. With the cross-correlation method, we derive a solar-like surface differential rotation on the G0 star of $\sigma^{2}$ CrB for the first time, and the surface shear rate is $\Delta \Omega = 0.180 \pm 0.004$ rad d$^{-1}$ and $\alpha = \Delta \Omega / \Omega_{eq} = 0.032 \pm 0.001$. We do not obtain a clear surface shear law for the F9 star due to the lack of mid-to-low latitude features, but detect a systematic longitude shift of high-latitude spots, which indicates a slower rotation with respect to the co-rotating frame., Comment: 9 figures, 2 tables, accepted for publication in ApJ

The study of planet occurrence as a function of stellar mass is important for a better understanding of planet formation. Estimating stellar mass, especially in the red giant regime, is difficult. In particular, stellar masses of a sample of evolved planet-hosting stars based on spectroscopy and grid-based modelling have been put to question over the past decade with claims they were overestimated. Although efforts have been made in the past to reconcile this dispute using asteroseismology, results were inconclusive. In an attempt to resolve this controversy, we study four more evolved planet-hosting stars in this paper using asteroseismology, and we revisit previous results to make an informed study of the whole ensemble in a self-consistent way. For the four new stars, we measure their masses by locating their characteristic oscillation frequency, $\mathrm{\nu}_{\mathrm{max}}$, from their radial velocity time series observed by SONG. For two stars, we are also able to measure the large frequency separation, $\mathrm{\Delta\nu}$, helped by extended SONG single-site and dual-site observations and new TESS observations. We establish the robustness of the $\mathrm{\nu}_{\mathrm{max}}$-only-based results by determining the stellar mass from $\mathrm{\Delta\nu}$, and from both $\mathrm{\Delta\nu}$ and $\mathrm{\nu}_{\mathrm{max}}$. We then compare the seismic masses of the full ensemble of 16 stars with the spectroscopic masses from three different literature sources. We find an offset between the seismic and spectroscopic mass scales that is mass-dependent, suggesting that the previously claimed overestimation of spectroscopic masses only affects stars more massive than about 1.6 M$_\mathrm{\odot}$., Comment: 13 pages, 12 figures, Accepted for publication in the Main Journal of MNRAS

BackgroundWide-ranging psoriasis prevalence estimates have been reported, possibly due to methodological differences.ObjectivesTo assess the prevalence of psoriasis in Denmark and to validate the use of questionnaire-based data to identify patients with psoriasis.MethodsWe used data from the Danish Skin Cohort, a prospective cohort comprising general population adults, as well as patients with dermatologist-verified psoriasis and atopic dermatitis, respectively. The general population cohort was interviewed to assess the psoriasis prevalence in Denmark, and validation of the questions was performed.ResultsFrom 3490 general population participants, 7.9% (n=275) were found to have self-reported psoriasis. Of these, 221 (prevalence 6.3%) had their disease diagnosed by a physician (the dermatologist-diagnosed prevalence was 4.3%), whereas 54 (prevalence 1.6%) were not diagnosed by a physician. A total of 176 (5%) had active psoriasis within the last 12 months. More than half of patients had at least one disease flare in the last 12 months, and 44.4% of patients with psoriasis had at least one family member with psoriasis, whereas this was only the case for 13.7% of non-psoriasis individuals. Validation of the psoriasis diagnosis yielded a high sensitivity and specificity, with little incremental value of limiting diagnoses to those diagnosed by a physician.ConclusionThe lifetime-prevalence of self-reported psoriasis was found to be 7.9%, whereas the 1-year prevalence (ie, currently active psoriasis) was 5.0%. If used appropriately, questionnaire-based data may accurately identify patients with psoriasis.

Asteroseismic analysis of solar-like stars allows us to determine physical parameters such as stellar mass, with a higher precision compared to most other methods. Even in a well-studied cluster such as the Hyades, the masses of the red giant stars are not well known, and previous mass estimates are based on model calculations (isochrones). The four known red giants in the Hyades are assumed to be clump (core-helium-burning) stars based on their positions in colour-magnitude diagrams, however asteroseismology offers an opportunity to test this assumption. Using asteroseismic techniques combined with other methods, we aim to derive physical parameters and the evolutionary stage for the planet hosting star epsilon Tau, which is one of the four red giants located in the Hyades. We analysed time-series data from both ground and space to perform the asteroseismic analysis. By combining high signal-to-noise (S/N) radial-velocity data from the ground-based SONG network with continuous space-based data from the revised Kepler mission K2, we derive and characterize 27 individual oscillation modes for epsilon Tau, along with global oscillation parameters such as the large frequency separation and the ratio between the amplitude of the oscillations measured in radial velocity and intensity as a function of frequency. The latter has been measured previously for only two stars, the Sun and Procyon. Combining the seismic analysis with interferometric and spectroscopic measurements, we derive physical parameters for epsilon Tau, and discuss its evolutionary status., Comment: 13 pages, 13 figures, 4 tables, accepted for publication in Astronomy & Astrophysics

The nearby metal-poor giant HD122563 is an important astrophysical laboratory for which to test stellar atmospheric and interior physics. It is also a benchmark star for which to calibrate methods to apply to large scale surveys. Recently it has been remeasured using various methodologies given the new high precision instruments at our disposal. However, inconsistencies in the observations and models have been found. In order to better characterise this star we have been measuring its radial velocities since 2016 using the Hertzsprung telescope (SONG network node). In this work we report the first detections of sun-like oscillations in this star, and to our knowledge, a detection in the most metal-poor giant to date. We apply the classical seismic scaling relation to derive a new surface gravity of $\log g_{\nu} = 1.39 \pm 0.01$ dex. Constraints on the mass imposed by its PopII giant classification then yield a radius of $30.8 \pm 1.0$ R$_{\odot}$. By coupling this with recent interferometric measurements we infer a distance to the star of 306 $\pm$ 9 pc. Data from the Gaia mission corroborates the distance hypothesis ($d_{\rm GDR2}$ = 290 $\pm$ 5 pc), and thus the updated fundamental parameters. We confirm the validity of the seismic scaling relation without corrections for surface gravity in metal-poor and evolved star regimes. The small discrepancy of 0.04 dex reduces to 0.02 dex by applying corrections to the scaling relations. The new constraints on the HR diagram ($L_{\odot} = 381 \pm 26$) reduce the disagreement between the stellar parameters and evolution models, however, a discrepancy still exists. Fine-tuned stellar evolution calculations show that this can be reconciled by changing the mixing-length parameter by an amount (--0.35) that is in agreement with predictions from recent 3D simulations and empirical results., Comment: Accepted for publication in A&A

The nearby red giant Aldebaran is known to host a gas giant planetary companion from decades of ground-based spectroscopic radial velocity measurements. Using Gaussian Process-based Continuous Auto-Regressive Moving Average (CARMA) models, we show that these historic data also contain evidence of acoustic oscillations in the star itself, and verify this result with further dedicated ground-based spectroscopy and space-based photometry with the Kepler Space Telescope. From the frequency of these oscillations we determine the mass of Aldebaran to be $1.16 \pm 0.07 \, M_\odot$, and note that this implies its planet will have been subject to insolation comparable to the Earth for some of the star's main sequence lifetime. Our approach to sparse, irregularly sampled time series astronomical observations has the potential to unlock asteroseismic measurements for thousands of stars in archival data, and push to lower-mass planets around red giant stars., Comment: 24 pages, 7 figures (including appendices); submitted to ApJL; paper text, figures, data, and code at https://github.com/farr/Aldebaran

BACKGROUND Atopic dermatitis (AD) is a common inflammatory skin condition. While previous publications have examined healthcare expenses, large data regarding patient demographics, healthcare use and drug prescriptions are limited. OBJECTIVE To examine demographics, healthcare use and drug prescriptions in children and adults with hospital-diagnosed AD. METHODS Danish nationwide registries were cross-linked to access demographic, healthcare and drug prescription data on children and adults with hospital-diagnosed AD (ICD-10 code L20). The diagnostic code for AD used in this study was validated by reviewing medical charts. RESULTS We identified 9704 children (time period 1997-2012) and 5558 adults (time period 1997-2007) with hospital-diagnosed AD. The diagnostic code L20 had a positive predictive value of 95%. Among children with AD, a larger proportion came from less resourceful families and had immigrant parents from non-European countries. In adults, we observed an opposite tendency. Topical and systemic antibiotics were used relatively frequent in both children and adults with AD. The use of prednisolone and other systemic anti-inflammatory therapy was substantially higher in adults with AD than in children. LIMITATIONS We were unable to identify and describe patients treated by general and private practitioners. CONCLUSION There exist significant differences in social predictors for AD and the use of AD medication between children and adults with hospital-diagnosed AD in Denmark. The diagnostic code for AD appears to be valid in Danish registries.

Lithium abundance A(Li) and surface rotation are good diagnostic tools to probe the internal mixing and angular momentum transfer in stars. We explore the relation between surface rotation, A(Li) and age in a sample of seismic solar-analogue (SA) stars and study their possible binary nature. We select a sample of 18 SA observed by the NASA Kepler satellite for an in-depth analysis. Their seismic properties and surface rotation are well constrained from previous studies. About 53 hours of high-resolution spectroscopy were obtained to derive fundamental parameters and A(Li). These values were combined and confronted with seismic masses, radii and ages, as well as surface rotation periods. We identify a total of 6 binary systems. A well-defined relation between A(Li) and rotation was obtained. With models constrained by the characterisation of the individual mode frequencies for single stars, we identify a sequence of three SA with similar mass (~1.1Mo) and stellar ages ranging between 1 to 9 Gyr. Within the realistic estimate of ~7% for the mass uncertainty, we find a good agreement between the measured A(Li) and the predicted A(Li) evolution from a grid of models calculated with the Toulouse-Geneva stellar evolution code, which includes rotational internal mixing, calibrated to reproduce solar chemical properties. We present A(Li) for a consistent spectroscopic survey of SA with a mass of 1.00+/-0.15Mo, and characterised through asteroseismology and surface rotation rates based on Kepler observations. The correlation between A(Li) and P_rot supports the gyrochronological concept for stars younger than the Sun. The consensus between measured A(Li) for solar analogues with model grids, calibrated onto the Sun's chemical properties suggests that these targets share the same internal physics. In this light, the solar Li and rotation rate appear to be normal for a star like the Sun., Comment: Accepted for publications in A&A, 11 pages, 6 figures

The prototype telescope and instruments for the Stellar Observations Network Group (SONG) are nearing completion at the Observatorio del Teide on Tenerife. In this contribution we describe the current status (autumn 2013) of the telescope and its instrumentation. Preliminary performance characteristics are presented for the high-resolution spectrograph based on daytime observations of the Sun and a 4 hour test series obtained for the sub-giant β Aquilae.

We present numerical and experimental results for the development of islands of stability in atom-optics billiards with soft walls. As the walls are soften, stable regions appear near singular periodic trajectories in converging (focusing) and dispersing billiards, and are surrounded by areas of “stickiness” in phase space. The size of these islands depends on the softness of the potential in a very sensitive way.

Department of Physics of Complex Systems, Weizmann Institute of Science,Rehovot 76100, IsraelAbstractWe discuss a recently demonstrated type of microwave spectroscopy of trappedultra-cold atoms known as ”echo spectroscopy” [M.F. Andersen et. al., Phys. Rev.Lett., in press (2002)]. Echo spectroscopy can serve as an extremely sensitive ex-perimental tool for investigating quantum dynamics of trapped atoms even whena large number of states are thermally populated. We show numerical results forthe stability of eigenstates of an atom-optics billiard of the Bunimovich type, anddiscuss its behavior under different types of perturbations. Finally, we propose touse special geometrical constructions to make a dephasing free dipole trap.Key words:PACS

We report on the implemented design of a two-colour instrument based on electron multiplying CCD (EMCCD) detectors. This instrument is currently installed at the Danish 1.54m telescope at ESO's La Silla Observatory in Chile, and will be available at the SONG (Stellar Observations Network Group) 1m telescope node at Tenerife and at other SONG nodes as well. We present the software system for controlling the two-colour instrument and calibrating the high frame-rate imaging data delivered by the EMCCD cameras. An analysis of the performance of the Two-Colour Instrument at the Danish telescope shows an improvement in spatial resolution of up to a factor of two when doing shift-and-add compared with conventional imaging, and that it is possible to do high-precision photometry of EMCCD data in crowded fields. The Danish telescope, which was commissioned in 1979, is limited by a triangular coma at spatial resolutions below 0.5" and better results will thus be achieved at the near diffraction limited optical system on the SONG telescopes, where spatial resolutions close to 0.2" have been achieved. Regular EMCCD operations have been running at the Danish telescope for several years and have produced a number of scientific discoveries, including microlensing detected exoplanets, the detection of previously unknown variable stars in dense globular clusters and the discovery of two rings around the small asteroid-like object (10199) Chariklo., Accepted to A&A, 17 pages, 15 figures

This book introduces the intrepid temperance advocates who formed America's longest-living minor political party - the Prohibition Party - drawing on the party's history to illuminate how American politics came to exclude minor parties from governance. Lisa M. F. Andersen traces the influence of pressure groups and ballot reforms, arguing that these innovations created a threshold for organization and maintenance that required extraordinary financial and personal resources from parties already lacking in both. More than most other minor parties, the Prohibition Party resisted an encroaching Democratic-Republican stranglehold over governance. When Prohibitionists found themselves excluded from elections, they devised a variety of tactics: they occupied saloons, pressed lawsuits, forged utopian communities, and organized dry consumers to solicit alcohol-free products.

We identify a set of 18 solar analogs among the seismic sample of solar-like stars observed by the Kepler satellite rotating between 10 and 40 days. This set is constructed using the asteroseismic stellar properties derived using either the global oscillation properties or the individual acoustic frequencies. We measure the magnetic activity properties of these stars using observations collected by the photometric Kepler satellite and by the ground-based, high-resolution Hermes spectrograph mounted on the Mercator telescope. The photospheric (Sph) and chromospheric (S index) magnetic activity levels of these seismic solar analogs are estimated and compared in relation to the solar activity. We show that the activity of the Sun is comparable to the activity of the seismic solar analogs, within the maximum-to-minimum temporal variations of the 11-year solar activity cycle 23. In agreement with previous studies, the youngest stars and fastest rotators in our sample are actually the most active. The activity of stars older than the Sun seems to not evolve much with age. Furthermore, the comparison of the photospheric, Sph, with the well-established chromospheric, S index, indicates that the Sph index can be used to provide a suitable magnetic activity proxy which can be easily estimated for a large number of stars from space photometric observations., Comment: Accepted for publication in A&A

Context: Accurate fundamental parameters of stars are essential for the asteroseismic analysis of data from the NASA Kepler mission. Aims: We aim at determining accurate atmospheric parameters and the abundance pattern for a sample of 82 red giants that are targets for the Kepler mission. Methods: We have used high-resolution, high signal-to-noise spectra from three different spectrographs. We used the iterative spectral synthesis method VWA to derive the fundamental parameters from carefully selected high-quality iron lines. After determination of the fundamental parameters, abundances of 13 elements were measured using equivalent widths of the spectral lines. Results: We identify discrepancies in log g and [Fe/H], compared to the parameters based on photometric indices in the Kepler Input Catalogue (larger than 2.0 dex for log g and [Fe/H] for individual stars). The Teff found from spectroscopy and photometry shows good agreement within the uncertainties. We find good agreement between the spectroscopic log g and the log g derived from asteroseismology. Also, we see indications of a potential metallicity effect on the stellar oscillations. Conclusions: We have determined the fundamental parameters and element abundances of 82 red giants. The large discrepancies between the spectroscopic log g and [Fe/H] and values in the Kepler Input Catalogue emphasize the need for further detailed spectroscopic follow-up of the Kepler targets in order to produce reliable results from the asteroseismic analysis., 16 Pages, 12 Figures, accepted for publication in A&A

We combined two sets of data to get high-precision time-series for stars in the open cluster NGC 1817. We verified most of the variable stars detected earlier and found some new ones. To the 12 δ Scuti variables detected prior to this article 4 new δ Scuti stars and one candidate have been added. In addition 3 γ Doradus candidates have been detected. The total number of variables and possible variables in NGC 1817, or in the field of view of the cluster is now up to 26. This high number of pulsating stars and especially δ Scuti variables makes this cluster an interesting asteroseismic target for future study. Using asteroseismology on δ Scuti stars will hopefully provide us with information that eventually will constrain the theoretical models of stars. This will in the end give us a much greater understanding of the evolution of stellar objects. Accepted: 2009, July 8 Individual Objects: NGC 1817

We perform echo spectroscopy on ultracold atoms in atom-optics billiards to study their quantum dynamics. The detuning of the trapping laser is used to change the "perturbation", which causes a decay in the echo coherence. Two different regimes are observed: first, a perturbative regime in which the decay of echo coherence is nonmonotonic and partial revivals of coherence are observed in contrast with the predictions of random matrix theory. These revivals are more pronounced in traps with mixed dynamics as compared to traps where the dynamics is fully chaotic. Next, for stronger perturbations, the decay becomes monotonic and independent of the strength of the perturbation. In this regime no clear distinction can be made between chaotic traps and traps with mixed dynamics.

We developed a new experimental system (the “atom-optics billiard”) and demonstrated chaotic and regular dynamics of cold, optically trapped atoms. We show that the softness of the walls and additional optical potentials can be used to manipulate the structure of phase space.

The loss in coherence in a trapped-atoms "echo" experiment is suppressed by a different pulse sequence. The coherence time is then limited by mixing to other vibrational levels and the lifetime of the internal states

We perform spectroscopy on the hyperfine splitting of $^{85}$Rb atoms trapped in far-off-resonance optical traps. The existence of a spatially dependent shift in the energy levels is shown to induce an inherent dephasing effect, which causes a broadening of the spectroscopic line and hence an inhomogeneous loss of atomic coherence at a much faster rate than the homogeneous one caused by spontaneous photon scattering. We present here a number of approaches for reducing this inhomogeneous broadening, based on trap geometry, additional laser fields, and novel microwave pulse sequences. We then show how hyperfine spectroscopy can be used to study quantum dynamics of optically trapped atoms., Comment: Review/Tutorial

The dynamics of particles inside billiards has been extensively investigated both classically and quantum mechanically, since this very simple system yet exhibits a rich variety of nonlinear dynamics phenomena [1]. Hence, billiards where used to explore the connections between classical and quantum chaos, and also to shed light on the origins of statistical mechanics. Recently, we realized an “atom-optics billiard”, where ultra-cold atoms are trapped inside a dark optical trap, whose shape can be varied to create different atom dynamics [2]. In this work, we present numerical investigation and experimental realization of atom-optics billiards with ordered, chaotic or mixed phase-space dynamics.

We investigate the coherence properties of thermal atoms confined in optical dipole traps where the underlying classical dynamics is chaotic. A perturbative expression derived for the coherence of the echo scheme of Anderson et al. [Phys. Rev. Lett. 90, 023001 (2003)] shows that it is a function of the survival probability or fidelity of eigenstates of the motion of the atoms in the trap. The echo coherence and the survival probability display 'system specific' features, even when the underlying classical dynamics is chaotic. In particular, partial revivals in the echo signal and the survival probability are found for a small shift of the potential. Next, a 'semiclassical' expression for the averaged echo signal is presented and used to calculate the echo signal for atoms in a light sheet wedge billiard. Revivals in the echo coherence are found in this system, indicating that they may be a generic feature of dipole traps.

A method for reducing the inhomogeneous broadening in the spectroscopic measurement of the hyperfine splitting of the ground state of optically trapped atoms is demonstrated. This reduction is achieved by the addition of a very weak light field (the "compensating beam"), whose frequency is tuned between the two hyperfine levels. The total shift is obtained by adding the shifts from the trap and the compensating beam, and a complete cancellation of the inhomogeneous broadening will occur for an intensity ratio of /spl sim/ (/spl Delta/HF/2/spl delta/)/sup 2/. With the suppression of inhomogeneous broadening, the atomic coherence time is next limited by the much smaller spontaneous scattering time. Finally, the introduction of the compensating beam provides with an experimental method to control the decoherence rate of the atomic ensemble, and thus to study the interesting interplay between dynamics and coherence in systems with a rich phase-space, for example in atom-optics billiards.

This work investigates the dephasing of ultra cold /sup 85/Rb atoms trapped in an optical dipole trap and prepared in a coherent superposition of the two hyperfine ground states by interaction with a so-called /spl pi//2 micro wave (MW) pulse. The dephasing, measured as the Ramsey fringe contrast decay and related with the Loschmidt echo decay, can be reversed by stimulating a "coherence echo". The later is obtained by adding a population-inverting "p" pulse between the usual two /spl pi//2 pulses. Echo spectroscopy on atoms in a Gaussian beam red-detuned trap is performed and observed, for the proper trap parameters, a coherent signal, which for long times decays due to photon scattering, and has a time scale two orders of magnitude longer than the Ramsey decoherence times.

We report on numerical and experimental observations of islands of stability induced in a Bunimovich stadium atom-optics billiard by a soft wall repulsive potential. A deviation from exponential decay of the survival probability of atoms in an open billiard is observed, and explained by the presence of these stable islands and a sticky region surrounding them. We also investigate islands in dispersing billiards with soft walls, and predict a new mechanism for their formation.

All episodes of bacteraemia during a 15-year period (1981-1995) in the County of Northern Jutland, Denmark, were analysed with regard to antibiotic resistance. A total of 8840 isolates from 7938 episodes of bacteraemia was identified. Over time, no changes in bacterial aetiology were noted. Three isolates of Staphylococcus aureus were methicillin resistant (0.2%) and six were gentamicin resistant (0.4%). Among coagulase-negative staphylococci a 14% increase in resistance to penicillin was observed (95% confidence intervals, CI: 2-26%). Likewise, the frequency of resistance to methicillin, gentamicin and erythromycin increased, the corresponding figures being 38% (CI: 26-50%), 26% (CI: 14-38%) and 32% (CI: 16-50%), respectively, whereas a 14% decrease in resistance to streptomycin was recorded (CI: 4-24%). A 20% (CI: 2-37%) increase of coagulase-negative staphylococci resistant to three or more antibiotics was observed. The frequency of ampicillin resistance increased by 9% among Escherichia coli (CI: 4-13%) and by 10% (CI: 6-14%) in all Enterobacteriaceae. Among Enterobacteriaceae the level of resistance to third-generation cephalosporins, carbapenems, aminoglycosides and fluoroquinolones remained low (

Deployment of the prototype node of the SONG project took place in April 2012 at Observatorio del Teide (Canary Islands). Its key instrument (echelle spectrograph) was installed and operational a few weeks later while its 1 m feeding telescope suffered a considerable delay to meet the required specifications. Using a fibre-feed, solar light could be fed to the spectrograph and we carried out a 1-week observing campaign in June 2012 to evaluate its performance for measuring precision radial velocities. In this work we present the first results of this campaign by comparing the sensitivity of the SONG spectrograph with other helioseismology reference instruments (Mark-I and GOLF) when simultaneous data are considered.

In order to estimate within-subjects variability in 24-hour energy expenditure at a fixed physical activity programme with a physical activity index of 1.30, this quantity was measured in four apparently healthy subjects once a month over 10 months. The coefficient of variation of the measurements was found to be between 2.7 and 4 per cent and in agreement with previously published data.