Reduced cardiorespiratory fitness, low physical activity and an urban environment are independently associated with increased cardiovascular risk in children

Aims/hypothesis: To assist in the development of preventive strategies, we studied whether the neighbourhood environment or modifiable behavioural parameters, including cardiorespiratory fitness (CRF) and physical activity (PA), are independently associated with obesity and metabolic risk markers in children. Methods: We carried out a cross-sectional analysis of 502 randomly selected first and fifth grade urban and rural Swiss schoolchildren with regard to CRF, PA and the neighbourhood (rural vs urban) environment. Outcome measures included BMI, sum of four skinfold thicknesses, homeostasis model assessment of insulin resistance (HOMA-IR) and a standardised clustered metabolic risk score. Results: CRF and PA (especially total PA, but also the time spent engaged in light and in moderate and vigorous intensity PA) were inversely associated with measures of obesity, HOMA-IR and the metabolic risk score, independently of each other, and of sociodemographic and nutritional parameters, media use, sleep duration, BMI and the neighbourhood environment (all p < 0.05). Children living in a rural environment were more physically active and had higher CRF values and reduced HOMA-IR and metabolic risk scores compared with children living in an urban environment (all p < 0.05). These differences in cardiovascular risk factors persisted after adjustment for CRF, total PA and BMI. Conclusions/interpretation: Reduced CRF, low PA and an urban environment are independently associated with an increase in metabolic risk markers in children. Trial registration: isrctn.org 15360785 Funding: The study was funded by the Federal office of Sports (Magglingen, Switzerland), the Swiss National Science Foundation (grant nos 3234-069271 and PMPDB-114401) and the Diabetes Foundation of the Region of Base

Stellar archaeology with Gaia: the Galactic white dwarf population

Gaia will identify several 1e5 white dwarfs, most of which will be in the solar neighborhood at distances of a few hundred parsecs. Ground-based optical follow-up spectroscopy of this sample of stellar remnants is essential to unlock the enormous scientific potential it holds for our understanding of stellar evolution, and the Galactic formation history of both stars and planets.Comment: Summary of a talk at the 'Multi-Object Spectroscopy in the Next Decade' conference in La Palma, March 2015, to be published in ASP Conference Series (editors Ian Skillen & Scott Trager

Doppler imaging of the planetary debris disc at the white dwarf SDSS J122859.93+104032.9

Debris discs which orbit white dwarfs are signatures of remnant planetary systems. We present 12 yr of optical spectroscopy of the metal-polluted white dwarf SDSS J1228+1040, which shows a steady variation in the morphology of the 8600 Å Ca II triplet line profiles from the gaseous component of its debris disc. We identify additional emission lines of O I, Mg I, Mg II, Fe II and Ca II in the deep co-added spectra. These emission features (including Ca H & K) exhibit a wide range in strength and morphology with respect to each other and to the Ca II triplet, indicating different intensity distributions of these ionic species within the disc. Using Doppler tomography, we show that the evolution of the Ca II triplet profile can be interpreted as the precession of a fixed emission pattern with a period in the range 24–30 yr. The Ca II line profiles vary on time-scales that are broadly consistent with general relativistic precession of the debris disc

A test of the planet-star unipolar inductor for magnetic white dwarfs

Despite thousands of spectroscopic detections, only four isolated white dwarfs exhibit Balmer emission lines. The temperature inversion mechanism is a puzzle over 30 years old that has defied conventional explanations. One hypothesis is a unipolar inductor that achieves surface heating via ohmic dissipation of a current loop between a conducting planet and a magnetic white dwarf. To investigate this model, new time-resolved spectroscopy, spectropolarimetry, and photometry of the prototype GD 356 are studied. The emission features vary in strength on the rotational period, but in antiphase with the light curve, consistent with a cool surface spot beneath an optically thin chromosphere. Possible changes in the line profiles are observed at the same photometric phase, potentially suggesting modest evolution of the emission region, while the magnetic field varies by 10 per cent over a full rotation. These comprehensive data reveal neither changes to the photometric period, nor additional signals such as might be expected from an orbiting body. A closer examination of the unipolar inductor model finds points of potential failure: the observed rapid stellar rotation will inhibit current carriers due to the centrifugal force, there may be no supply of magnetospheric ions, and no antiphase flux changes are expected from ohmic surface heating. Together with the highly similar properties of the four cool, emission-line white dwarfs, these facts indicate that the chromospheric emission is intrinsic. A tantalizing possibility is that intrinsic chromospheres may manifest in (magnetic) white dwarfs, and in distinct parts of the Hertzsprung–Russell diagram based on structure and composition

Transiting Disintegrating Planetary Debris around WD 1145+017

More than a decade after astronomers realized that disrupted planetary material likely pollutes the surfaces of many white dwarf stars, the discovery of transiting debris orbiting the white dwarf WD 1145+017 has opened the door to new explorations of this process. We describe the observational evidence for transiting planetary material and the current theoretical understanding (and in some cases lack thereof) of the phenomenon.Comment: Invited review chapter. Accepted March 23, 2017 and published October 7, 2017 in the Handbook of Exoplanets. 15 pages, 10 figure

ProtoDESI: First On-Sky Technology Demonstration for the Dark Energy Spectroscopic Instrument

The Dark Energy Spectroscopic Instrument (DESI) is under construction to measure the expansion history of the universe using the baryon acoustic oscillations technique. The spectra of 35 million galaxies and quasars over 14,000 square degrees will be measured during a 5-year survey. A new prime focus corrector for the Mayall telescope at Kitt Peak National Observatory will deliver light to 5,000 individually targeted fiber-fed robotic positioners. The fibers in turn feed ten broadband multi-object spectrographs. We describe the ProtoDESI experiment, that was installed and commissioned on the 4-m Mayall telescope from August 14 to September 30, 2016. ProtoDESI was an on-sky technology demonstration with the goal to reduce technical risks associated with aligning optical fibers with targets using robotic fiber positioners and maintaining the stability required to operate DESI. The ProtoDESI prime focus instrument, consisting of three fiber positioners, illuminated fiducials, and a guide camera, was installed behind the existing Mosaic corrector on the Mayall telescope. A Fiber View Camera was mounted in the Cassegrain cage of the telescope and provided feedback metrology for positioning the fibers. ProtoDESI also provided a platform for early integration of hardware with the DESI Instrument Control System that controls the subsystems, provides communication with the Telescope Control System, and collects instrument telemetry data. Lacking a spectrograph, ProtoDESI monitored the output of the fibers using a Fiber Photometry Camera mounted on the prime focus instrument. ProtoDESI was successful in acquiring targets with the robotically positioned fibers and demonstrated that the DESI guiding requirements can be met.Comment: Accepted versio

Resilience in Healthcare (RiH): a longitudinal research programme protocol

INTRODUCTION: Over the past three decades, extensive research has been undertaken to understand the elements of what constitutes high quality in healthcare. Yet, much of this research has been conducted on individual elements and their specific challenges. Hence, goals other than understanding the complex of factors and elements that comprises quality in healthcare have been privileged. This lack of progress has led to the conclusion that existing approaches to research are not able to address the inherent complexity of healthcare systems as characterised by a significant degree of performance variability within and across system levels, and what makes them resilient. A shift is, therefore, necessary in such approaches. Resilience in Healthcare (RiH) adopts an approach comprising a comprehensive research programme that models the capacity of healthcare systems and stakeholders to adapt to changes, variations and/or disruptions: that is, resilience. As such, RiH offers a fresh approach capable of capturing and illuminating the complexity of healthcare and how high-quality care can be understood and advanced. METHODS AND ANALYSIS: Methodologically, to illuminate what constitutes quality in healthcare, it is necessary to go beyond single-site, case-based studies. Instead, there is a need to engage in multi-site, cross-national studies and engage in long-term multidisciplinary collaboration between national and international researchers interacting with multiple healthcare stakeholders. By adopting such processes, multiple partners and a multidisciplinary orientation, the 5-year RiH research programme aims to confront these challenges and accelerate current understandings about and approaches to researching healthcare quality.The RiH research programme adopts a longitudinal collaborative interactive design to capture and illuminate resilience as part of healthcare quality in different healthcare settings in Norway and in five other countries. It combines a meta-analysis of detailed empirical research in Norway with cross-country comparison from Australia, Japan, Netherlands, Switzerland and the UK. Through establishing an RiH framework, the programme will identify processes with outcomes that aim to capture how high-quality healthcare provisions are achieved. A collaborative learning framework centred on engagement aims to systematically translate research findings into practice through co-construction processes with partners and stakeholders. ETHICS AND DISSEMINATION: The RiH research programme is approved by the Norwegian Centre for Research Data (No. 864334). The empirical projects selected for inclusion in this longitudinal research programme have been approved by the Norwegian Centre for Research Data or the Regional Committees for Medical and Health Research Ethics. The RiH research programme has an embedded publication and dissemination strategy focusing on the progressive sharing of scientific knowledge, information and results, and on engaging with the public, including relevant patient and stakeholder representatives. The findings will be disseminated through scientific articles, PhD dissertations, presentations at national and international conferences, and through social media, newsletters and the popular media

Fast spectrophotometry of WD 1145+017

WD 1145+017 is currently the only white dwarf known to exhibit periodic transits of planetary debris as well as absorption lines from circumstellar gas. We present the first simultaneous fast optical spectrophotometry and broad-band photometry of the system, obtained with the Gran Telescopio Canarias (GTC) and the Liverpool Telescope (LT), respectively. The observations spanned $5.5$ h, somewhat longer than the $4.5$-h orbital period of the debris. Dividing the GTC spectrophotometry into five wavelength bands reveals no significant colour differences, confirming grey transits in the optical. We argue that absorption by an optically thick structure is a plausible alternative explanation for the achromatic nature of the transits that can allow the presence of small-sized ($\sim\mu$m) particles. The longest ($87$ min) and deepest ($50$ per cent attenuation) transit recorded in our data exhibits a complex structure around minimum light that can be well modelled by multiple overlapping dust clouds. The strongest circumstellar absorption line, Fe II $\lambda$5169, significantly weakens during this transit, with its equivalent width reducing from a mean out-of-transit value of $2$ \AA\ to $1$ \AA\ in-transit, supporting spatial correlation between the circumstellar gas and dust. Finally, we made use of the Gaia Data Release 2 and archival photometry to determine the white dwarf parameters. Adopting a helium-dominated atmosphere containing traces of hydrogen and metals, and a reddening $E(B-V)=0.01$ we find $T_\mathrm{eff}=15\,020 \pm 520$ K, $\log g=8.07\pm0.07$, corresponding to M_\mathrm{WD}=0.63\pm0.05\ \mbox{\mathrm{M}_{\odot}} and a cooling age of $224\pm30$ Myr.Comment: 13 pages, 9 figures, accepted for publication in Monthly Notices of the Royal Astronomical Society (2018 Aug 22