Movement along a low-angle normal fault: The S reflector west of Spain

[1] The existence of normal faults that moved at low angles (less than 20°) has long been debated. One possible low-angle fault is the S detachment at the west Galicia (Spain) margin and thought to occur at the top of serpentinized mantle. It is unlikely that S was a large submarine slide as it was probably active over several million years without the development of any compressional features such as toe thrusts, it appears to have rooted beneath the conjugate Flemish Cap margin, and it is similar to structures elsewhere that also appear to be rooted detachments. Here we analyze depth images to identify synrift sediment packages above S and use the geometry of these synrift packages to constrain the angle at which S both formed and remained active. We find that S must have remained active at angles below 15°, too low to be explained simply by the low friction coefficient of partially serpentinized peridotites. Instead, we suggest that transient high fluid pressures must have developed within the serpentinites and propose a model in which anastomosing fault strands are alternately active and sealed, enabling moderately high fluid pressures to develop

Prehospital Systolic Blood Pressure Thresholds: A Community‐based Outcomes Study

Objectives Emergency medical services (EMS) personnel commonly use systolic blood pressure ( sBP ) to triage and treat acutely ill patients. The definition of prehospital hypotension and its associated outcomes are poorly defined. The authors sought to determine the discrimination of prehospital sBP thresholds for 30‐day mortality and to compare patient classification by best‐performing thresholds to traditional cutoffs. Methods In a community‐based cohort of adult, nontrauma, noncardiac arrest patients transported by EMS between 2002 and 2006, entries to state hospital discharge data and death certificates were linked. Prehospital sBP thresholds between 40 and 140 mm Hg in derivation ( n =  132,624) and validation ( n =  22,020) cohorts and their discrimination for 30‐day mortality, were examined. Cutoffs were evaluated using the 0/1 distance, Youden index, and adjusted Z‐statistics from multivariable logistic regression models. Results In the derivation cohort, 1,594 (1.2%) died within 24 hours, 7,404 (6%) were critically ill during hospitalization, and 6,888 (5%) died within 30 days. The area under the receiver operating characteristic (ROC) curve for sBP was 0.60 (95% confidence interval [CI] = 0.59, 0.61) for 30‐day mortality and 0.64 (95% CI = 0.62 0.66) for 24‐hour mortality. The 0/1 distance, Youden index, and adjusted Z‐statistics found best‐performing sBP thresholds between 110 and 120 mm Hg. When compared to an sBP ≤ 90 mm Hg, a cutoff of 110 mm Hg would identify 17% ( n =  137) more deaths at 30 days, while overtriaging four times as many survivors. Conclusions Prehospital sBP is a modest discriminator of clinical outcomes, yet no threshold avoids substantial misclassification of 30‐day mortality among noninjured patients. Resumen Los Umbrales de la Presión Arterial Sistólica Prehospitalaria: Un Estudio de Base Comunitaria Acerca de la Evolución de los Pacientes Objetivos El personal de los sistemas de emergencias médicas ( SEM ) usa frecuentemente la presión arterial sistólica ( PAS ) para clasificar y tratar a los pacientes agudos. Las definiciones de hipotensión prehospitalaria y sus resultados asociados están pobremente definidos. Se determinó la discriminación de los umbrales de PAS prehospitalaria para la mortalidad a los 30 días, y se comparó la clasificación del paciente por los mejores umbrales con los puntos de corte tradicionales. Metodología Estudio de cohorte de base comunitaria de pacientes adultos no traumatológicos ni con paradas cardiorrespiratorias transportados por los SEM entre 2002 y 2006, cuyas historias estaban vinculadas con los datos de alta hospitalaria y los certificados de mortalidad. Se examinaron los umbrales de PAS prehospitalaria entre 40 mm Hg y 140 mm Hg en las cohortes de derivación ( n =  132.624), y validación ( n =  22,020), y su discriminación para la mortalidad a los 30 días. Los puntos de corte se evaluaron usando la distancia 0/1, el índice de Youden y los estadísticos Z ajustados de los modelos de regresión logística multivariable. Resultados: En la cohorte de derivación, 1.594 (1,2%) fallecieron en las primeras 24 horas, 7.404 (6%) estuvieron críticamente enfermos durante el ingreso y 6.888 (5%) fallecieron en los 30 primeros días. El área bajo la curva de la ROC para PAS fue 0,60 ( IC 95% = 0,59–0,61) para la mortalidad a los 30 días y 0,64 ( IC 95% = 0,62–0,66) para la mortalidad a las 24 horas. La distancia 0/1, el índice de Youden y las estadísticas Z ajustadas hallaronque los mejores umbrales de PAS estaban entre 110 y 120 mm Hg. Cuando se comparó con una PAS ≤ 90 mm Hg, un punto de corte de 110 mm Hg identificaría un 17% ( n =  137) más de muertes a los 30 días, mientras que sobreclasificaría cuatro veces más a los supervivientes. Conclusiones La presión arterial sistólica es un discriminador modesto de resultados clínicos. No obstante, ningún umbral evita una mala clasificación de la mortalidad a los 30 días entre los pacientes no traumatológicos.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/98303/1/acem12142-sup-0002-DataSupplementS2_FigS1.pdfhttp://deepblue.lib.umich.edu/bitstream/2027.42/98303/2/acem12142-sup-0007-DataSupplementS7_FigS4.pdfhttp://deepblue.lib.umich.edu/bitstream/2027.42/98303/3/acem12142-sup-0006-DataSupplementS6_FigS3.pdfhttp://deepblue.lib.umich.edu/bitstream/2027.42/98303/4/acem12142-sup-0009-DataSupplementS9_TableS3.pdfhttp://deepblue.lib.umich.edu/bitstream/2027.42/98303/5/acem12142-sup-0003-DataSupplementS3.pdfhttp://deepblue.lib.umich.edu/bitstream/2027.42/98303/6/acem12142-sup-0008-DataSupplementS8_TableS2.pdfhttp://deepblue.lib.umich.edu/bitstream/2027.42/98303/7/acem12142-sup-0004-DataSupplementS4_TableS1.pdfhttp://deepblue.lib.umich.edu/bitstream/2027.42/98303/8/acem12142-sup-0001-DataSupplementS1.pdfhttp://deepblue.lib.umich.edu/bitstream/2027.42/98303/9/acem12142.pd

A super-Earth-sized planet orbiting in or near the habitable zone around Sun-like star

We present the discovery of a super-earth-sized planet in or near the habitable zone of a sun-like star. The host is Kepler-69, a 13.7 mag G4V-type star. We detect two periodic sets of transit signals in the three-year flux time series of Kepler-69, obtained with the Kepler spacecraft. Using the very high precision Kepler photometry, and follow-up observations, our confidence that these signals represent planetary transits is >99.1%. The inner planet, Kepler-69b, has a radius of 2.24+/-0.4 Rearth and orbits the host star every 13.7 days. The outer planet, Kepler-69c, is a super-Earth-size object with a radius of 1.7+/-0.3 Rearth and an orbital period of 242.5 days. Assuming an Earth-like Bond albedo, Kepler-69c has an equilibrium temperature of 299 +/- 19 K, which places the planet close to the habitable zone around the host star. This is the smallest planet found by Kepler to be orbiting in or near habitable zone of a Sun-like star and represents an important step on the path to finding the first true Earth analog.Comment: Accepted for publication in the Astrophysical Journa

Validation of Twelve Small Kepler Transiting Planets in the Habitable Zone

We present an investigation of twelve candidate transiting planets from Kepler with orbital periods ranging from 34 to 207 days, selected from initial indications that they are small and potentially in the habitable zone (HZ) of their parent stars. Few of these objects are known. The expected Doppler signals are too small to confirm them by demonstrating that their masses are in the planetary regime. Here we verify their planetary nature by validating them statistically using the BLENDER technique, which simulates large numbers of false positives and compares the resulting light curves with the Kepler photometry. This analysis was supplemented with new follow-up observations (high-resolution optical and near-infrared spectroscopy, adaptive optics imaging, and speckle interferometry), as well as an analysis of the flux centroids. For eleven of them (KOI-0571.05, 1422.04, 1422.05, 2529.02, 3255.01, 3284.01, 4005.01, 4087.01, 4622.01, 4742.01, and 4745.01) we show that the likelihood they are true planets is far greater than that of a false positive, to a confidence level of 99.73% (3 sigma) or higher. For KOI-4427.01 the confidence level is about 99.2% (2.6 sigma). With our accurate characterization of the GKM host stars, the derived planetary radii range from 1.1 to 2.7 R_Earth. All twelve objects are confirmed to be in the HZ, and nine are small enough to be rocky. Excluding three of them that have been previously validated by others, our study doubles the number of known rocky planets in the HZ. KOI-3284.01 (Kepler-438b) and KOI-4742.01 (Kepler-442b) are the planets most similar to the Earth discovered to date when considering their size and incident flux jointly.Comment: 27 pages in emulateapj format, including tables and figures. To appear in The Astrophysical Journa

Superhumps in Cataclysmic Binaries. XXV. q_crit, epsilon(q), and Mass-Radius

We report on successes and failures in searching for positive superhumps in cataclysmic variables, and show the superhumping fraction as a function of orbital period. Basically, all short-period systems do, all long-period systems don't, and a 50% success rate is found at P_orb=3.1+-0.2 hr. We can use this to measure the critical mass ratio for the creation of superhumps. With a mass-radius relation appropriate for cataclysmic variables, and an assumed mean white-dwarf mass of 0.75 M_sol, we find a mass ratio q_crit=0.35+-0.02. We also report superhump studies of several stars of independently known mass ratio: OU Virginis, XZ Eridani, UU Aquarii, and KV UMa (= XTE J1118+480). The latter two are of special interest, because they represent the most extreme mass ratios for which accurate superhump measurements have been made. We use these to improve the epsilon(q) calibration, by which we can infer the elusive q from the easy-to-measure epsilon (the fractional period excess of P_superhump over P_orb). This relation allows mass and radius estimates for the secondary star in any CV showing superhumps. The consequent mass-radius law shows an apparent discontinuity in radius near 0.2 M_sol, as predicted by the disrupted magnetic braking model for the 2.1-2.7 hour period gap. This is effectively the "empirical main sequence" for CV secondaries.Comment: PDF, 45 pages, 9 tables, 12 figures; accepted, in press, to appear November 2005, PASP; more info at http://cba.phys.columbia.edu

An Unusual Transmission Spectrum for the Sub-Saturn KELT-11b Suggestive of a Sub-Solar Water Abundance

We present an optical-to-infrared transmission spectrum of the inflated sub-Saturn KELT-11b measured with the Transiting Exoplanet Survey Satellite (TESS), the Hubble Space Telescope (HST) Wide Field Camera 3 G141 spectroscopic grism, and the Spitzer Space Telescope (Spitzer) at 3.6 $\mu$m, in addition to a Spitzer 4.5 $\mu$m secondary eclipse. The precise HST transmission spectrum notably reveals a low-amplitude water feature with an unusual shape. Based on free retrieval analyses with varying molecular abundances, we find strong evidence for water absorption. Depending on model assumptions, we also find tentative evidence for other absorbers (HCN, TiO, and AlO). The retrieved water abundance is generally $\lesssim 0.1\times$ solar (0.001--0.7$\times$ solar over a range of model assumptions), several orders of magnitude lower than expected from planet formation models based on the solar system metallicity trend. We also consider chemical equilibrium and self-consistent 1D radiative-convective equilibrium model fits and find they too prefer low metallicities ($[M/H] \lesssim -2$, consistent with the free retrieval results). However, all the retrievals should be interpreted with some caution since they either require additional absorbers that are far out of chemical equilibrium to explain the shape of the spectrum or are simply poor fits to the data. Finally, we find the Spitzer secondary eclipse is indicative of full heat redistribution from KELT-11b's dayside to nightside, assuming a clear dayside. These potentially unusual results for KELT-11b's composition are suggestive of new challenges on the horizon for atmosphere and formation models in the face of increasingly precise measurements of exoplanet spectra.Comment: Accepted to The Astronomical Journal. 31 pages, 20 figures, 7 table

Early versus Later Rhythm Analysis in Patients with Out-of-Hospital Cardiac Arrest

Background In a departure from the previous strategy of immediate defibrillation, the 2005 resuscitation guidelines from the American Heart Association–International Liaison Committee on Resuscitation suggested that emergency medical service (EMS) personnel could provide 2 minutes of cardiopulmonary resuscitation (CPR) before the first analysis of cardiac rhythm. We compared the strategy of a brief period of CPR with early analysis of rhythm with the strategy of a longer period of CPR with delayed analysis of rhythm. Methods We conducted a cluster-randomized trial involving adults with out-of-hospital cardiac arrest at 10 Resuscitation Outcomes Consortium sites in the United States and Canada. Patients in the early-analysis group were assigned to receive 30 to 60 seconds of EMS-administered CPR and those in the later-analysis group were assigned to receive 180 seconds of CPR, before the initial electrocardiographic analysis. The primary outcome was survival to hospital discharge with satisfactory functional status (a modified Rankin scale score of ≤3, on a scale of 0 to 6, with higher scores indicating greater disability). Results We included 9933 patients, of whom 5290 were assigned to early analysis of cardiac rhythm and 4643 to later analysis. A total of 273 patients (5.9%) in the later-analysis group and 310 patients (5.9%) in the early-analysis group met the criteria for the primary outcome, with a cluster-adjusted difference of −0.2 percentage points (95% confidence interval, −1.1 to 0.7; P=0.59). Analyses of the data with adjustment for confounding factors, as well as subgroup analyses, also showed no survival benefit for either study group. Conclusions Among patients who had an out-of-hospital cardiac arrest, we found no difference in the outcomes with a brief period, as compared with a longer period, of EMS-administered CPR before the first analysis of cardiac rhythm. (Funded by the National Heart, Lung, and Blood Institute and others; ROC PRIMED ClinicalTrials.gov number, NCT00394706.

Masses, radii, and orbits of small Kepler planets : The transition from gaseous to rocky planets

We report on the masses, sizes, and orbits of the planets orbiting 22 Kepler stars. There are 49 planet candidates around these stars, including 42 detected through transits and 7 revealed by precise Doppler measurements of the host stars. Based on an analysis of the Kepler brightness measurements, along with high-resolution imaging and spectroscopy, Doppler spectroscopy, and (for 11 stars) asteroseismology, we establish low false-positive probabilities (FPPs) for all of the transiting planets (41 of 42 have an FPP under 1%), and we constrain their sizes and masses. Most of the transiting planets are smaller than three times the size of Earth. For 16 planets, the Doppler signal was securely detected, providing a direct measurement of the planet's mass. For the other 26 planets we provide either marginal mass measurements or upper limits to their masses and densities; in many cases we can rule out a rocky composition. We identify six planets with densities above 5 g cm-3, suggesting a mostly rocky interior for them. Indeed, the only planets that are compatible with a purely rocky composition are smaller than 2 R ⊕. Larger planets evidently contain a larger fraction of low-density material (H, He, and H2O).Peer reviewedFinal Accepted Versio