Search

Purpose In recent years, a growing trend toward clinical doctorate degrees has emerged in several allied health professions. However, few studies have been conducted within the physician assistant (PA) profession related to changing the entry-level degree for PAs to a clinical doctorate. Methods A descriptive, quantitative study assessing PA students' perceptions of changing the entry-level credential for PAs to a clinical doctorate was conducted. Thirty randomly selected programs with 1,966 students were invited to participate in the survey. Results Of the programs invited, 25 (83%) participated, with 486 (25%) full-time students completing the survey. Of the respondents, 56.1% (272) were first-year students and 43.9% (213) were second-year students. Both groups had a negative perception of changing the entry-level degree for PAs to a clinical doctorate, indicating the doctorate will raise the cost of PA education and discourage some people from entering the profession (82.1%, n = 398); a doctorate for PAs will cause confusion for patients (71.3%, n = 346); and that there is no need for the profession-specific doctorate since the master's degree sufficiently prepares PAs to practice in today's health care setting (70.9%, n = 344). Conclusions The present findings lend additional support to previous studies, endorsing the master's degree as the entry-level and terminal degrees.

The Transiting Exoplanet Survey Satellite (TESS) is an MIT-led, NASA-funded Explorer-class planet finder launched in April 2018. TESS will carry out a 2-year all-sky survey with the primary goal of detecting small transiting exoplanets around bright and nearby stars. The TESS instrument consists of four wide-field cameras in a stacked configuration, providing a combined field of view of 24 deg × 96 deg that spans approximately from the ecliptic plane to the ecliptic pole. In order to achieve the desired photometric precision necessary for the mission, TESS uses the instrument cameras as star trackers during fine-pointing mode to enhance attitude accuracy and stabilization for science operations. We present our approach in quantifying the expected performance of the fine-pointing system and assessing the impact of pointing performance on the overall photometric precision of the mission. First, we describe the operational details of the fine-pointing system with the science instrument being used for star-tracking. Next, we present the testing framework used to quantify the attitude determination performance of the system and the expected attitude knowledge accuracy results, both in coarse-fine pointing hand-off and in nominal fine-pointing conditions. By combining simulations of the instrument and the spacecraft bus, we quantify the closed-loop fine-pointing stability performance of the system in nominal science operations as well as in the case of camera unavailability due to Earth/Moon interference. Finally, we assess the impact of platform pointing stability on the photometric precision of the system using detailed system modeling and discuss the applicability of mitigation techniques to reduce the effect of jitter on TESS science data.

The rapidly growing automobile industry increases the accumulation of end-of-life tires each year throughout the world. Waste tires lead to increased environmental issues and lasting resource problems. Recycling hazardous wastes to produce value-added products is becoming essential for the sustainable progress of society. A patented sulfonation process followed by pyrolysis at 1100 &deg, C in a nitrogen atmosphere was used to produce carbon material from these tires and utilized as an anode in lithium-ion batteries. The combustion of the volatiles released in waste tire pyrolysis produces lower fossil CO2 emissions per unit of energy (136.51 gCO2/kW&middot, h) compared to other conventional fossil fuels such as coal or fuel&ndash, oil, usually used in power generation. The strategy used in this research may be applied to other rechargeable batteries, supercapacitors, catalysts, and other electrochemical devices. The Raman vibrational spectra observed on these carbons show a graphitic carbon with significant disorder structure. Further, structural studies reveal a unique disordered carbon nanostructure with a higher interlayer distance of 4.5 &Aring, compared to 3.43 &Aring, in the commercial graphite. The carbon material derived from tires was used as an anode in lithium-ion batteries exhibited a reversible capacity of 360 mAh/g at C/3. However, the reversible capacity increased to 432 mAh/g at C/10 when this carbon particle was coated with a thin layer of carbon. A novel strategy of prelithiation applied for improving the first cycle efficiency to 94% is also presented.

A 24 day period for the low-mass X-ray binary GX 13+1 was previously proposed on the basis of 7 years of RXTE ASM observations (Corbet 2003) and it was suggested that this was the orbital period of the system. This would make it the one of the longest known orbital periods for a Galactic low-mass X-ray binary powered by Roche lobe overflow. We present here the results of: (i) K-band photometry obtained with the SMARTS Consortium CTIO 1.3 telescope on 68 nights over a 10 month interval; (ii) Continued monitoring with the RXTE ASM, analyzed using a semi-weighted power spectrum instead of the data filtering technique previously used; and (iii) Swift BAT hard X-ray observations. Modulation near 24 days is seen in both the K-band and additional statistically independent ASM X-ray observations. However, the modulation in the ASM is not strictly periodic. The periodicity is also not detected in the Swift BAT observations, but modulation at the same relative level as seen with the ASM cannot be ruled out. If the 24 day period is the orbital period of system, this implies that the X-ray modulation is caused by structure that is not fixed in location. A possible mechanism for the X-ray modulation is the dipping behavior recently reported from XMM-Newton observations., Comment: Accepted for publication in the Astrophysical Journal

Using a pulse-fit method, we investigate the spectral lags between the traditional gamma-ray band (50-400 keV) and the X-ray band (6-25 keV) for 8 GRBs with known redshifts (GRB 010921, GRB 020124, GRB 020127, GRB 021211, GRB 030528, GRB 040924, GRB 041006, GRB 050408) detected with the WXM and FREGATE instruments aboard the HETE-2 satellite. We find several relations for the individual GRB pulses between the spectral lag and other observables, such as the luminosity, pulse duration, and peak energy (Epeak). The obtained results are consistent with those for BATSE, indicating that the BATSE correlations are still valid at lower energies (6-25 keV). Furthermore, we find that the photon energy dependence for the spectral lags can reconcile the simple curvature effect model. We discuss the implication of these results from various points of view., Comment: 13 pages, 9 figures, accepted for the publication in PASJ (minor corrections)

Regular observations by the All Sky Monitor aboard the Rossi X-ray Timing Explorer satellite have yielded well-sampled light-curves with a time baseline of over ten years. We find that up to eight of the sixteen brightest persistent low mass X-ray binaries show significant, possible sinusoidal, variations with periods of order ten years. We speculate on its possible origin and prevalence in the population of low mass X-ray binaries and we find the presence of a third object in the system, or long-period variability intrinsic to the donor star, as being attractive origins for the X-ray flux modulation we detect. For some of the objects in which we do not detect a signal, there is substantial short-term variation which may hide modest modulation on long time-scales. Decade time-scale modulations may thus be even more common., 8 pages, 4 figures, 2 tables. Accepted by MNRAS

Micro-X is a sounding-rocket experiment that will combine a transition edge sensor (TES) microcalorimeter array with an imaging mirror to obtain high-spectral-resolution images of astronomical X-ray sources. The instrument's resolution across the 0.3-2.5 keV band will be 2 eV. The first flight will target the region of the Bright Eastern Knot of the Puppis A supernova remnant and is slated for January 2011. The obtained high-resolution X-ray spectra will be used to ascertain the temperature and ionization state of the X-ray-emitting gas and to determine its velocity structure. The TES array is read out by a time-division superconducting quantum interference device (SQUID) multiplexing system. The detector front end assembly and the SQUID multiplexing circuit are cooled to the operating temperature of 50 mK with an adiabatic demagnetization refrigerator (ADR). The design of this refrigerator is tailored to the requirements of rocket flight. Stable operation of the TES array close to the ADR magnet will be achieved with a magnetic shielding system, which will be based on a combination of a bucking coil and high-permeability and superconducting shield materials to cancel out residual fields. We describe our progress in developing the Micro-X instrument.

Hypofractionated stereotactic radiosurgery allows the treatment of metastatic and primary spinal tumors with highly conformal dosing while sparing the adjacent neural structures. This enables the physician to treat tumors which are recurrent after standard external beam radiation, are radioresistant in doses normally tolerated by the spinal cord or are in patients with primary tumors who are not candidates for surgical resection. Initial results have shown satisfactory achievement of treatment goals with minimal occurrence of complications.

Objective Spinal sarcomas pose unique treatment dilemmas because of the difficulty of achieving adequate surgical margins and/or delivering curative radiation doses (65 Gy) in close proximity to the spinal cord. This study used hypofractionated stereotactic radiosurgery (SRS) to deliver higher biologically effective doses to treat primary spinal sarcomas and spinal sarcoma metastases. Methods Twenty-four patients with spinal or paraspinal sarcomas entered an Institutional Review Board-approved registry trial to evaluate SRS efficacy. They were assessed at regular intervals for pain control, disease progression, and complications for a minimum of 12 months or until death. Results The median treatment dose for the spinal sarcoma lesions was 30 Gy at the 80% isodose in 3 fractions, with some variation based on tumor size, shape, and dose to adjacent critical structures. Seven patients were treated definitively; all had excellent pain relief and are alive with a mean follow-up period of 33 months. Two patients had complete tumor regression, 3 had partial regression, and 2 experienced recurrences and have been re-treated. Seven patients underwent resection and adjuvant SRS. One of 3 patients treated preoperatively had complete tumor regression, and none of the 4 patients treated postoperatively had a local recurrence with a mean follow-up period of 43.5 months. All 10 patients with sarcoma metastases to the spine (16 lesions) died, with a mean survival of 11.1 months from first spinal metastasis treatment. Complete pain relief was achieved in 8 patients, partial relief in 7 patients, and none in 1 patient. No patient developed radiation myelitis. Conclusion These preliminary results suggest that SRS may have a role in the definitive treatment of patients with primary spinal sarcomas who are deemed unresectable and as adjuvant treatment in those undergoing surgery and for palliation of sarcoma metastases.

Micro-X, the High-Resolution Microcalorimeter X-ray Imaging Rocket, is a sounding rocket space telescope that will combine a transition-edge-sensor (TES) X-ray microcalorimeter array with a conical imaging mirror to obtain high spectral resolution images of extended and point X-ray sources. Microcalorimeters measure the energy of an absorbed photon by sensing the increase in temperature of the sensor from the thermalization of the absorbed photon’s energy. The advantages and scientific promise of this technology have fueled active development for the past 20 years. We will leverage this development and take the next step by producing a flight-qualified system that will serve as a pathfinder for future missions. Our scientific program will initially focus on extended sources, for which our high-spectral-resolution observations have distinct advantages over other technologies. For our initial flight, we will observe the bright eastern knot in the Puppis A remnant, a site of complex cloud-shock interactions and ejecta enrichment. A Micro-X observation of the bright eastern knot of Puppis A will obtain a line-dominated spectrum with 90,000 counts collected in 300 seconds at 2 eV resolution across the 0.3–2.5 keV band.

Objective:The purpose of this study was to examine young women's urinary incontinence knowledge.Study design:Descriptive.Background:Urinary incontinence is a disorder that is linked to pregnancy and childbirth. It is a subject of an unmentionable nature as it is related to the reproductive a

The treatment of patients with cancer epitomizes the importance of using a collaborative team approach to optimize patient care. Physician team members most commonly are radiation oncologists, general surgeons, surgical oncologists, thoracic surgeons, neurosurgeons, and orthopedic surgeons. When patients are receiving chemotherapy, their medical oncologist frequently takes responsibility for coordinating care among the various team members and initiating consultations with necessary providers. When patients develop bone metastases or chemotherapy-induced bone loss (CTIBL), the orthopedic surgeon may be able to improve the patient's quality of life greatly. Procedures orthopedists perform most commonly include open reduction and internal fixations and arthroplasties (joint replacement surgery). Less invasive procedures currently being tested include stereotactic radiosurgery, radiofrequency ablation (RFA), and percutaneous cementoplasty. By understanding the options available to patients with skeletal complications of malignancy, the medical oncologist can discuss issues with patients and make appropriate referrals for diagnosis and treatment. Additionally, with a greater understanding of the surgical procedures available, the medical oncologist will be better able to assist in preparing the patient for surgery.

Using archival X-ray data, we find that the catalog location of the X-ray binary Scutum X-1 (Sct X-1) is incorrect, and that the correct location is that of the X-ray source AX J183528-0737, which is 15' to the west. Our identification is made on the basis of the 112-s pulse period for this object detected in an XMM-Newton observation, as well as spatial coincidence between AX J183528-0737 and previous X-ray observations. Based on the XMM-Newton data and archival RXTE data, we confirm secular spin-down over 17 years with period derivative Pdot~3.9e-9 s/s, but do not detect a previously reported X-ray iron fluorescence line. We identify a bright (Ks=6.55), red (J-Ks=5.51), optical and infrared counterpart to AX J183528-0737 from 2MASS, a number of mid-IR surveys, and deep optical observations, which we use to constrain the extinction to and distance of Sct X-1. From these data, as well as limited near-IR spectroscopy, we conclude that Sct X-1 is most likely a binary system comprised of a late-type giant or supergiant and a neutron star., Comment: 10 pages, 9 figures. Revised following referee's comments. Accepted to ApJ

The Transiting Exoplanet Survey Satellite (TESS) will search for planets transiting bright and nearby stars. TESS has been selected by NASA for launch in 2017 as an Astrophysics Explorer mission. The spacecraft will be placed into a highly elliptical 13.7-day orbit around the Earth. During its two-year mission, TESS will employ four wide-field optical CCD cameras to monitor at least 200,000 main-sequence dwarf stars with I = 4-13 for temporary drops in brightness caused by planetary transits. Each star will be observed for an interval ranging from one month to one year, depending mainly on the star's ecliptic latitude. The longest observing intervals will be for stars near the ecliptic poles, which are the optimal locations for follow-up observations with the James Webb Space Telescope. Brightness measurements of preselected target stars will be recorded every 2 min, and full frame images will be recorded every 30 min. TESS stars will be 10-100 times brighter than those surveyed by the pioneering Kepler mission. This will make TESS planets easier to characterize with follow-up observations. TESS is expected to find more than a thousand planets smaller than Neptune, including dozens that are comparable in size to the Earth. Public data releases will occur every four months, inviting immediate community-wide efforts to study the new planets. The TESS legacy will be a catalog of the nearest and brightest stars hosting transiting planets, which will endure as highly favorable targets for detailed investigations., accepted for publication in the new, peer-reviewed SPIE Journal of Astronomical Telescopes, Instruments, and Systems (JATIS)

The 2003 X-ray outburst of the candidate black hole binary, H1743-322, was investigated in frequent pointed observations (2-250 keV) with the Rossi X-Ray Timing Explorer (RXTE). One particular program of 130 observations is organized into 111 time intervals and searched for the presence of high-frequency quasi-periodic oscillations (HFQPOs) in the range 50-2000 Hz. Only a single observation (2003 June 13) yields a detection above 4 σ. The central frequency of 239 ± 4 Hz is consistent with the 240 Hz QPO reported for this source on 2003 May 28 (Homan and coworkers). We group the observations in several different ways and compute average power-density spectra (PDS) in a search for further evidence of HFQPOs. Significant results are found for two groups defined by the presence of low-frequency QPOs (0.1-20 Hz) and an absence of "band-limited" power continua. (1) The nine time intervals with the highest X-ray flux yield a QPO at 166 ± 5 Hz. (4.1 σ; 3-35 keV). (2) The group with lower X-ray flux (24 time intervals) produces a QPO at 242 ± 3 Hz (6.0 σ; 7-35 keV). The ratio of these two frequencies is 1.46 ± 0.05. This finding is consistent with results obtained for three other black hole systems that exhibit commensurate HFQPOs in a 3 : 2 ratio. Furthermore, the occurrence of H1743-322's slower HFQPO at times of higher X-ray luminosity closely resembles the behavior of XTE J1550-564 and GRO J1655-40. We discuss our results in terms of resonance models that invoke frequencies set by general relativity.

Airway responses were compared following 6-minute eucapnic voluntary hyperventilation and 6-minute exercise challenges by examining resting and post-challenge impulse oscillometry and spirometry variables. Twenty-two physically active individuals with probable exercise-induced bronchoconstriction took part in this study. Impulse oscillometry and spirometry were performed at baseline and for 20 minutes post-challenge at 5-minute intervals. High correlation was found between the two measures of change in airway function for both methods of challenge. Impulse oscillometry detected a difference in degree of response to the challenges, whereas spirometry indicated no difference, suggesting that impulse oscillometry is a more sensitive measure of change in airway function.

Selected results from the Rossi X-ray Timing Explorer All-Sky Monitor are presented to illustrate the phenomenology of the light curves. The sensitivity to periodic intensity variations is indicated by the folded light curve of AM Her. The gray line between transient and persistent sources is emphasized. Light curves of a range of systems comprising black holes or neutron stars and low and high mass companion stars show that the behavior of these systems is often, but not always, characteristic.

Study objective The efficacy of using impulse oscillometry (IOS) as an indirect measure of airflow obstruction compared to spirometry after exercise challenges in the evaluation of exercise-induced bronchoconstriction (EIB) has not been fully appreciated. The objective was to compare airway responses following room temperature and cold temperature exercise challenges, and to compare whether IOS variables relate to spirometry variables. Design Spirometry and IOS were performed at baseline and for 20 min after challenge at 5-min intervals. Setting Two 6-min exercise challenges, inhaling either room temperature (22.0°C) or cold temperature (− 1°C) dry medical-grade bottled air. At least 48 h was observed between these randomly assigned challenges. Participants Twenty-two physically active individuals (12 women and 10 men) with probable EIB. Interventions Subjects performed 6 min of stationary cycle ergometry while breathing either cold or room temperature medical-grade dry bottled air. Subjects were instructed to exercise at the highest intensity sustainable for the duration of the challenge. Heart rate and kilojoules of work performed were documented to verify exercise intensity. Measurements and results Strong correlations were observed within testing modalities for post-room temperature and post-cold temperature exercise spirometry and IOS values. Spirometry revealed no differences in postexercise peak falls in lung function between conditions; however, IOS identified significant differences in respiratory resistance (p Conclusions Correlations were found between spirometric and IOS measures of change in airway function for both exercise challenges, indicating close equivalency of the methods. The challenges appeared to elicit the EIB response by a similar mechanism of water loss, and cold temperature did not have an additive effect. IOS detected a difference in degree of response between the temperatures, whereas spirometry indicated no difference, suggesting that IOS is a more sensitive measure of change in airway function.

Cold Air Inhalation Does Not Affect the Severity of EIB after Exercise or Eucapnic Voluntary Hyperventilation. Med. Sci. Sports Exerc., Vol. 37, No. 4, pp. 544-549, 2005. Introduction: Exercise-induced bronchoconstriction (EIB) is thought to result from osmotic and thermal events of air conditioning during exercise at high ventilation rates. The purpose of this study was to evaluate lung function after exercise and eucapnic voluntary hyperventilation (EVH) while breathing both room-temperature and cold-temperature dry bottled air. Methods: Twenty-two subjects were identified as EIB probable by a fall of ≥7% in forced expiratory volume in the first second of exhalation (FEV 1 ) using a 6-min room-temperature EVH challenge (RTEVH; 22.0°C). Subjects then randomly performed three 6-min challenges: cold-temperature EVH (CTEVH; -1°C), room-temperature exercise (RTEX; 22.0°C), and cold-temperature exercise (CTEX; -1°C), with a period of at least 48 h observed between challenges. Spirometry was performed at baseline and at 5, 10, 15, and 20 min postchallenge. Results: Reasonable agreement was found between challenge modes and room-temperature and cold-temperature challenges. Postchallenge percent falls in FEV 1 were -15.21, -13.80, -13.12, and -10.69 for RTEVH, CTEVH, RTEX, and CTEX, respectively. RTEVH resulted in a significantly greater percent fall in FEV 1 than CTEX (P = 0.048); no other differences in FEV 1 were observed. Conclusion: Similar postchallenge percent falls in FEV 1 for room- and cold-temperature EVH and exercise suggest that dryness is essential to test conditions, as cold temperature did not have an additive effect to the EIB response.

The orbital period of Scorpius X-1 has been accepted as 0.787313 days since its discovery in archival optical photometric data by Gottlieb, Wright, & Liller. This period has apparently been confirmed multiple times in the years since in both photometric and spectroscopic optical observations, although to date only marginal evidence has been reported for modulation of the X-ray intensity at that period. We have used data taken with the All Sky Monitor on board the Rossi X-Ray Timing Explorer over the past 6 years to search for such a modulation. A major difficulty in detecting the orbit in X-ray data is presented by the flaring behavior in this source, wherein the (1.5-12 keV) X-ray intensity can change by up to a factor of 2 within a fraction of a day. These flares contribute nearly white noise to Fourier transforms of the intensity time series and thereby tend to obscure weak modulations, i.e., of a few percent or less. We present herein a technique for substantially reducing the effects of the flaring behavior while, at the same time, retaining much of any periodic orbital modulation, provided only that the two temporal behaviors exhibit different spectral signatures. Through such a search, we have found evidence for orbital modulation at the ~1% level with a period of 0.78893 days. This period is equal within our accuracy to a period (0.78901 days) that differs by 1 cycle yr–1 from the accepted value and that was also detected by Gottlieb et al. at a strength nearly as great as that of the 0.787313 day periodicity. We note that many of the reported optical observations of Sco X-1 have been made within 1 or 2 months of early June, when Sco X-1 transits the meridian at midnight. All periodicity searches based only on such observations would have been subject to the same 1 cycle yr–1 alias that affected the search of Gottlieb and coworkers. These considerations lead us to suggest that the actual period may in fact be 0.78901 days and that further observations will be necessary to confirm the true orbital period of Sco X-1.

To determine the imaging characteristics of soft-tissue myxoma, with emphasis on computed tomographic (CT) and magnetic resonance (MR) imaging findings and pathologic comparison.Records of 45 pathologically confirmed soft-tissue myxomas in 44 patients were retrospectively reviewed. Patient demographics and radiographs (n = 20), bone scintigrams (n = 2), angiograms (n = 3), and ultrasonographic (US) (n = 6), CT (n = 14), and MR images (n = 33) were evaluated by two musculoskeletal radiologists with agreement by consensus for lesion location, lesion size, and intrinsic characteristics.Soft-tissue myxoma more commonly affected women (59%; average age 52 years) and manifested as a slowly enlarging (64%) painful (51%) mass. Lesions were most frequently intramuscular (82%) and involved the thigh (51%). An appearance similar to that of a cyst was seen at CT (at which the lesions demonstrated low attenuation) and at MR imaging (at which the lesions demonstrated markedly high signal intensity on T2-weighted images) in all cases because of the high water content of mucin that was seen histologically. The true solid architecture of these lesions was best depicted in all cases at US (at which the lesions were hypoechoic, not anechoic) and on MR images obtained with contrast material (at which the lesions demonstrated internal enhancement). A small amount of tissue similar to fat surrounding these intramuscular myxomas (71% at MR imaging) corresponded histologically (70%) to atrophy of surrounding muscle.Soft-tissue myxoma often demonstrates characteristic US, CT, and MR imaging findings, including intramuscular location, intrinsic high water content, and a surrounding rim of fat.

We present X-ray light curves (1.5-12 keV) for fifteen gamma-ray bursts (GRBs) detected by the All-Sky Monitor on the Rossi X-ray Timing Explorer. We compare these soft X-ray light curves with count rate histories obtained by the high-energy (>12 keV) experiments BATSE, Konus-Wind, the BeppoSAX Gamma-Ray Burst Monitor, and the burst monitor on Ulysses. We discuss these light curves within the context of a simple relativistic fireball and synchrotron shock paradigm, and we address the possibility of having observed the transition between a GRB and its afterglow. The light curves show diverse morphologies, with striking differences between energy bands. In several bursts, intervals of significant emission are evident in the ASM energy range with little or no corresponding emission apparent in the high-energy light curves. For example, the final peak of GRB 970815 as recorded by the ASM is only detected in the softest BATSE energy bands. We also study the duration of bursts as a function of energy. Simple, singly-peaked bursts seem consistent with the E^{-0.5} power law expected from an origin in synchrotron radiation, but durations of bursts that exhibit complex temporal structure are not consistent with this prediction. Bursts such as GRB 970828 that show many short spikes of emission at high energies last significantly longer at low energies than the synchrotron cooling law would predict., 15 pages with 20 figures and 2 tables. In emulateapj format. Accepted by ApJS

The Transiting Exoplanet Survey Satellite (TESS ) will search for planets transiting bright and nearby stars. TESS has been selected by NASA for launch in 2017 as an Astrophysics Explorer mission. The spacecraft will be placed into a highly elliptical 13.7-day orbit around the Earth. During its two-year mission, TESS will employ four wide-field optical CCD cameras to monitor at least 200,000 main-sequence dwarf stars with I_C (approximately less than) 13 for temporary drops in brightness caused by planetary transits. Each star will be observed for an interval ranging from one month to one year, depending mainly on the star's ecliptic latitude. The longest observing intervals will be for stars near the ecliptic poles, which are the optimal locations for follow-up observations with the James Webb Space Telescope. Brightness measurements of preselected target stars will be recorded every 2 min, and full frame images will be recorded every 30 min. TESS stars will be 10-100 times brighter than those surveyed by the pioneering Kepler mission. This will make TESS planets easier to characterize with follow-up observations. TESS is expected to find more than a thousand planets smaller than Neptune, including dozens that are comparable in size to the Earth. Public data releases will occur every four months, inviting immediate community-wide efforts to study the new planets. The TESS legacy will be a catalog of the nearest and brightest stars hosting transiting planets, which will endure as highly favorable targets for detailed investigations.

We present techniques for bridging the gap between idealized inverse covariance weighted quadratic estimation of 21 cm power spectra and the real-world challenges presented universally by interferometric observation. By carefully evaluating various estimators and adapting our techniques for large but incomplete data sets, we develop a robust power spectrum estimation framework that preserves the so-called "EoR window" and keeps track of estimator errors and covariances. We apply our method to observations from the 32-tile prototype of the Murchinson Widefield Array to demonstrate the importance of a judicious analysis technique. Lastly, we apply our method to investigate the dependence of the clean EoR window on frequency--especially the frequency dependence of the so-called "wedge" feature--and establish upper limits on the power spectrum from z = 6.2 to z = 11.7. Our lowest limit is Delta(k) < 0.3 Kelvin at 95% confidence at a comoving scale k = 0.046 Mpc^-1 and z = 9.5., 27 pages, 10 figures. Updated to match the accepted Phys. Rev. D version

We report on a new method for tracking the phases of the orbital modulations in very short-period, near-contact, and contact binary systems systems in order to follow starspots. We apply this technique to Kepler light curves for 414 binary systems that were identified as having anticorrelated O-C curves for the midtimes of the primary and secondary eclipses, or in the case of non-eclipsing systems, their light-curve minima. This phase tracking approach extracts more information about starspot and binary system behavior than may be easily obtained from the O-C curves. We confirm the hypothesis of Tran et al. (2013) that we can successfully follow the rotational motions of spots on the surfaces of the stars in these binaries. In ~34% of the systems, the spot rotation is retrograde as viewed in the frame rotating with the orbital motion, while ~13% show significant prograde spot rotation. The remaining systems show either little spot rotation or erratic behavior, or sometimes include intervals of both types of behavior. We discuss the possibility that the relative motions of spots are related to differential rotation of the stars. It is clear from this study that the motions of the starspots in at least 50% of these short-period binaries are not exactly synchronized with the orbits., Comment: 16 pages, 14 figures, 2 tables; submitted to MNRAS

Kawahara and collaborators analyzed the transits of the candidate disintegrating Mercury-mass planet KIC 12557548b and suggested that the transit depths were correlated with the phase of the stellar rotation. We analyze the transit depths of KIC 12557548b and confirm that there is indeed a robust, statistically significant signal in the transit depths at the rotation period of the spotted host star. This signal is more prominent in the first-half of the Kepler data, and is not due to leakage of the rotating spot signal into our measurement of the transit depths, or due to unocculted starspots. We investigate the suggestion that this signal could be due to an active region on the star, emitting enhanced ultraviolet or X-ray radiation leading to an increased mass loss rate of the planet; we confirm that such a scenario could cause both modulation of the transit depths of KIC 12557548b, and small enough transit-timing variations that they might not be detected in the Kepler data. Our preferred explanation for the fact that the transit depths of KIC 12557548b are modulated with the stellar rotation phase is that the candidate transiting planet is occulting starspots on this highly spotted star; such a scenario could cause transit depth variations as large as have been observed, and cause transit-timing variations small enough that they are arguably consistent with the Kepler data., Comment: 14 pages, 15 figures, MNRAS, submitted August 20th, 2014

We present the results of a survey aimed at discovering and studying transiting planets with orbital periods shorter than one day (ultra-short-period, or USP, planets), using data from the Kepler spacecraft. We computed Fourier transforms of the photometric time series for all 200,000 target stars, and detected transit signals based on the presence of regularly spaced sharp peaks in the Fourier spectrum. We present a list of 106 USP candidates, of which 18 have not previously been described in the literature. This list of candidates increases the number of planet candidates with orbital periods shorter than about six hours from two to seven. In addition, among the objects we studied, there are 26 USP candidates that had been previously reported in the literature which do not pass our various tests. All 106 of our candidates have passed several standard tests to rule out false positives due to eclipsing stellar systems. A low false positive rate is also implied by the relatively high fraction of candidates for which more than one transiting planet signal was detected. By assuming these multi-transit candidates represent coplanar multi-planet systems, we are able to infer that the USP planets are typically accompanied by other planets with periods in the range 1-50 days, in contrast with hot Jupiters which very rarely have companions in that same period range. Another clear pattern is that almost all USP planets are smaller than 2 R [subscript ⊕], possibly because gas giants in very tight orbits would lose their atmospheres by photoevaporation when subject to extremely strong stellar irradiation. Based on our survey statistics, USP planets exist around approximately (0.51 ± 0.07)% of G-dwarf stars, and (0.83 ± 0.18)% of K-dwarf stars., United States. National Aeronautics and Space Administration (Kepler Participating Scientist Program)

Satisfaction with fitness facilities has long been accepted as a positive contributing factor to physical activity, readiness, and overall quality of life for military families. Our findings are based on a random sample of military families surveyed at 38 installations worldwide and at remote locations. A total of 8,572 service member and 3,493 spouse (55% and 32% response rate, respectively) questionnaires were completed and returned. Overall, members were satisfied with fitness facilities and programs, but spouses were less satisfied and more unfamiliar with these facilities. Most valued programs were fitness centers and swimming pools. Members reported that elimination of fitness facilities would greatly decrease the quality of life on installations, particularly at sites outside the continental United States, whereas spouses reported that this would not have a dramatic effect. The results of this study could be used to direct funding allocations, improve the health and fitness of military families, and suggest areas for further research.

Utilizing observations obtained with the Rossi X-ray Timing Explorer, we examine correlations between the properties of 0.08-22 Hz variable frequency QPOs and the X-ray spectral parameters for the black hole candidates XTE J1550-564 and GRO J1655-40. The spectra were fitted to a model including a multi-temperature blackbody disk and a power-law component. We find that the QPO frequency and amplitude are well correlated with the spectral parameters, although the correlations found for XTE J1550-564 are generally opposite to those for GRO J1655-40. There is one exeption: Both sources exhibit a general increase in the QPO frequency as the disk flux increases (or as the mass accretion rate through the disk increases). In addition, these QPOs are observed only when the power-law component contributes more than 20% of the 2-20 keV flux, which indicates that both the disk and the power-law components are linked to the QPO phenomenon.

We have analyzed over 2 yr of RXTE/All-Sky Monitor data for Cygnus X-1. We have detected the 5.6 day orbital period in Lomb-Scargle periodograms of both light curves and hardness ratios when Cyg X-1 was in the hard state. This detection was made with improved sensitivity and temporal coverage compared with previous detections by other X-ray missions. The folded light curves and hardness ratios show a broad intensity dip accompanied by spectral hardening centered on superior conjunction of the X-ray source. The dip has a duration of about 27% of the orbital period and depth ranging from 8% to 23% of the nondip intensities in three energy bands. Variability on timescales of hours is often evident within the broad dip in the unfolded data. In contrast, no feature at the orbital period is evident in the periodograms or folded light curves for the soft state. Absorption of X-rays by a stellar wind from the companion star can reproduce the observed X-ray orbital modulations in the hard state. To explain the low orbital modulation in the soft-state data, a reduction of the wind density during the soft state would be required. As an alternative, a partial covering scenario is described that could also account for the lack of the orbital modulation in the soft state.

We show that dramatic spectral evolution associated with dips occurring near phase zero in RXTE observations of Cir X-1 is well-fit by variable and at times heavy absorption (N_H > 10^24 cm^-2) of a bright component, plus an underlying faint component which is not attenuated by the variable column and whose flux is ~10% of that of the unabsorbed bright component. A prominent Fe emission line at ~6.5 keV is evident during the dips. The absolute line flux outside the dips is similar to that during the dips, indicating that the line is associated with the faint component. These results are consistent with a model in which the bright component is radiation received directly from a compact source while the faint component may be attributed to scattered radiation. Our results are also generally consistent with those of Brandt et al., who found that a partial- covering model could explain ASCA spectra of a low-to-high transition in Cir X-1. The relative brightness of the two components in our model requires a column density of ~2*10^23 cm^-2 if the faint component is due to Thomson scattering in material that mostly surrounds the source. We find that illumination of such a scattering cloud by the observed direct component would produce an Fe K-alpha fluorescence flux that is in rough agreement with the flux of the observed emission line. We also conclude that if the scattering medium is not highly ionized, our line of sight to the compact source does not pass through it. Finally, we discuss simple pictures of the absorbers responsible for the dips themselves., Accepted for publication in The Astrophysical Journal (23 pages, including 11 figures)

The fourth unambiguously identified soft gamma repeater (SGR), SGR 1627-41, was discovered with the BATSE instrument on 1998 June 15. Interplanetary Network (IPN) measurements and BATSE data constrained the location of this new SGR to a 6° segment of a narrow (19'') annulus. We present two bursts from this source observed by the All-Sky Monitor (ASM) on the Rossi X-Ray Timing Explorer. We use the ASM data to further constrain the source location to a 5' long segment of the BATSE/IPN error box. The ASM/IPN error box lies within 03 of the supernova remnant G337.0-0.1. The probability that a supernova remnant would fall so close to the error box purely by chance is ~5%.

We have investigated the X-ray timing properties of XTE J1550-564 during 60 Rossi X-Ray Timing Explorer Proportional Counter Array observations made between 1998 September 18 and November 28. We detect quasi-periodic oscillations (QPOs) near 185 Hz during four time intervals. The QPO widths (FWHM) are ~50 Hz, and the rms amplitudes are ~1% of the mean flux at 2-30 keV. This is the third Galactic black hole candidate known to exhibit a transient X-ray timing signature above 50 Hz, following the 67 Hz QPO in GRS 1915+105 and the 300 Hz QPO in GRO J1655-40. However, unlike the previous cases, which appear to show stationary frequencies, the QPO frequency in XTE J1550-564 must vary by at least ~10% to be consistent with observations. The occurrences and properties of the QPO were insensitive to large changes in the X-ray intensity (1.5-6.8 crab). However, the QPO appearance was accompanied by changes in the energy spectrum, namely, an increase in the temperature and a decrease in the normalization of the thermal component. The QPO is also closely related to the hard X-ray power-law component of the energy spectrum since the fractional amplitude of the QPO increases with photon energy. The fast QPOs in accreting black hole binaries are thought to be effects of general relativity; however, the relevance of the specific physical models that have been proposed remains largely uncertain. Low-frequency QPOs in the range 3-13 Hz were often observed. Occasionally, at high luminosity, the rms QPO amplitude was ~15% of the flux, a level previously reached only by GRS 1915+105. These extraordinary oscillations have a coherence parameter (ν/Δν) in the range 4-12 and are tied to the power-law component in the energy spectrum.

Excellent coverage of the 1998 outburst of the X-ray Nova XTE J1550-564 was provided by the Rossi X-ray Timing Explorer. XTE J1550-564 exhibited an intense (6.8 Crab) flare on 1998 September 19 (UT), making it the brightest new X-ray source observed with RXTE. We present a spectral analysis utilizing 60 Proportional Counter Array spectra from 2.5-20 keV spanning 71 days, and a nearly continuous All Sky Monitor light curve. The spectra were fit to a model including multicolor blackbody disk and power-law components. XTE J1550-564 is observed in the very high, high/soft, and intermediate canonical outburst states of Black Hole X-ray Novae.

Data accumulated with RXTE during the active state of Cir X-1 as well as during an unusually long transition from the active state to the quiescent state are reported. The long decline from the active state allowed the source characteristics to be studied systematically as a function of intensity. The following results are presented: (1) spectral fits during entry into a dip clearly show absorption with partial covering as previously reported (Brandt et al. 1996), and (2) correlations between position in the hardness-intensity plane and the character of the power density spectrum as the source entered the quiescent state are suggestive of Z source behavior seen in LMXB sources., Comment: 9 pages LaTeX, 5 ps figures, uses espcrc2.sty and epsfig.sty --- To be published in: Proceedings of "The Active X-ray Sky: Results from Beppo-SAX and Rossi-XTE", Rome, Italy, 21-24 Oct. 1997, Nuclear Physics B Proceedings Supplements; eds. L. Scarsi, H. Bradt, P. Giommi, and F. Fiore

Variable X-ray sources that appear to be the afterglows of the strong gamma-ray bursts GRB 970616 and GRB 970828 have been discovered with the RXTE PCA. First seen less than 4 hours after the burst, the flux from the sources decreased with time. Although near the sensitivity limit of the PCA, the sources are the brightest afterglows yet seen in X-rays. Similar observations of two other bursts did not detect any afterglows. These results are part of a continuing collaboration between RXTE, BATSE, and IPN scientists to rapidly detect X-ray afterglows of bright gamma-ray bursts.

We present Rossi X-Ray Timing Explorer (RXTE) All-Sky Monitor observations of the X-ray binary Circinus X-1 that illustrate the variety of intensity profiles associated with the 16.55 day flaring cycle of the source. We also present eight observations of Cir X-1 made with the RXTE Proportional Counter Array over the course of a cycle wherein the average intensity of the flaring state decreased gradually over ~12 days. Fourier power density spectra for these observations show a narrow quasi-periodic oscillation (QPO) peak that shifts in frequency between 6.8 and 32 Hz, as well as a broad QPO peak that remains roughly stationary at ~4 Hz. We identify these as Z-source horizontal and normal branch oscillations (HBOs/NBOs), respectively. Color-color and hardness-intensity diagrams (CDs/HIDs) show curvilinear tracks for each of the observations. The properties of the QPOs and very low frequency noise allow us to identify segments of these tracks with Z-source horizontal, normal, and flaring branches that shift location in the CDs and HIDs over the course of the 16.55 day cycle. These results contradict a previous prediction, based on the hypothesis that Cir X-1 is a high- atoll source, that HBOs should never occur in this source.

This prospective clinical study was undertaken to evaluate the effect of spontaneous food/fluid intake on serum sodium and comfort levels in a population of terminal patients (n = 31) receiving clysis or intravenous hydration. The median and mode of serum sodiums were within normal limits and 56 percent of the patients were eunatremic. There was no statistically significant difference in comfort scores between predehydration and dehydration phases, and 85 percent had an optimal comfort score. A statistically significant difference was found (p < 0.5) between mean daily comfort scores of those with normal sodiums versus those with abnormal sodiums; those with hypernatremia were lower but still in the top third comfort levels. Because the sodium was tested using a Chem7, we also were able to calculate the BUN, creatinine, and osmolality. These are presented and compared to other study results. The findings of this study reinforce the belief that fluid depletion in dying patients results in relatively benign symptoms, that serum sodium levels are not always altered with limited intake and that comfort levels can be maintained when the serum sodium is abnormal.

Fractures of the sacrum are infrequent injuries; however, they comprise a wide spectrum of injury types.Classification of the injuries are predominantly by fracture line direction (vertical, transverse, and oblique). The direction of the fracture line dictates both the most effective type of surgical management as well as the biologic consequences of the fracture. Most vertical fractures are associated with pelvic injuries and rarely have severe neural conpromise. Fixation of the sacral fracture is often a part of the more complex restoration of pelvic stability. Transverse and oblique sacral fractures are less often part of a pelvic injury complex; and they more often have associated neural deficits. Surgical treatment is most often indicated for neural decompression and stabilization for optimal recovery.

The requirement that a planet must orbit outside of its Roche limit gives a lower limit on the planet's mean density. The minimum density depends almost entirely on the orbital period and is immune to systematic errors in the stellar properties. We consider the implications of this density constraint for the newly-identified class of small planets with periods shorter than half a day. When the planet's radius is known accurately, this lower limit to the density can be used to restrict the possible combinations of iron and rock within the planet. Applied to KOI 1843.03, with a radius of 0.6 Earth radii and the shortest known orbital period of 4.245 hr, the planet's mean density must be greater than approximately 7 g/cm^3. By modeling the planetary interior subject to this constraint, we find the composition of the planet must be mostly iron, with at most a modest fraction of silicates (less than approximately 30% by mass)., Comment: ApJ Letters, in press

We report the discovery of an Earth-sized planet ($1.16\pm 0.19 R_\oplus$) in an 8.5-hour orbit around a late G-type star (KIC 8435766, Kepler-78). The object was identified in a search for short-period planets in the {\it Kepler} database and confirmed to be a transiting planet (as opposed to an eclipsing stellar system) through the absence of ellipsoidal light variations or substantial radial-velocity variations. The unusually short orbital period and the relative brightness of the host star ($m_{\rm Kep}$ = 11.5) enable robust detections of the changing illumination of the visible hemisphere of the planet, as well as the occultations of the planet by the star. We interpret these signals as representing a combination of reflected and reprocessed light, with the highest planet dayside temperature in the range of 2300 K to 3100 K. Follow-up spectroscopy combined with finer sampling photometric observations will further pin down the system parameters and may even yield the mass of the planet., Comment: Accepted for publication, ApJ, 10 pages and 6 figures

The All-Sky Monitor on the Rossi X-ray Timing Explorer has been monitoring the sky in the 1.5 - 12 keV band since late February. The instrument consists of three coded-aperture cameras which can be rotated to view different regions by a motorized drive assembly. Intensities of ~100 known sources are obtained via least-square fits of shadow patterns to the data and compiled to form x-ray light curves. Six orbital periodicities and four long-term periodicities, all previously known, have been detected in these light curves. Searches for additional sources have also been conducted. X-ray light curves for the Crab Nebula, Cyg X-1, 4U 1705-44, GRO J1655-40, and SMC X-1 are reported. They illustrate the quality of the results and the range of observed phenomena.

We have carried out a study of Cir X-1 through (1) detailed sampling over a single 16.5 day intensity cycle with the Rossi X-Ray Timing Explorer (RXTE) proportional counter array and (2) complementary monitoring over six such cycles with the RXTE all-sky monitor (ASM). We report here the temporal and spectral evolution at nonflaring phases, during which Cir X-1 remained unusually bright (~1.0 crab) and relatively steady. The Fourier power density spectrum of the source was observed to vary with strong correlations among low-frequency flat-topped power (1-10 Hz), a quasi-periodic oscillation (QPO) peak centered at 1.3-12 Hz, and a broad QPO peak centered at ~20 Hz up to ~100 Hz. As orbital phase increased within the cycle, the rms amplitude of the flat-topped power generally (but not monotonically) decreased while the QPO features generally evolved toward higher frequency. The 1.5-12 keV spectrum was observed to generally harden during the nonflaring phases of each of the six 16.5 day periods monitored by the ASM.

Interleukin-13 (IL-13) induced a potent mitogenic response in IL-3- dependent TF-1 cells and DNA synthesis to a lesser extent in MO7E and FDC-P1 cells. IL-13 stimulation of these lines, like IL-4 and insulin- like growth factor-1 (IGF-1), resulted in tyrosine phosphorylation of a 170-kD substrate. The tyrosine-phosphorylated 170-kD substrate strongly associated with the 85-kD subunit of phosphoinositol-3 (PI-3) kinase and with Grb-2. Anti-4PS serum readily detected the 170-kD substrate in lysates from both TF-1 and FDC-P1 cells stimulated with IL-13 or IL-4. These data provide evidence that IL-13 induces tyrosine phosphorylation of the 4PS substrate, providing an essential interface between the IL- 13 receptor and signaling molecules containing SH2 domains. IL-13 and IL-4 stimulation of murine L cell fibroblasts, which endogenously express the IL-4 receptor (IL-4R alpha) and lack expression of the IL-2 receptor gamma subunit (IL-2R gamma), resulted in tyrosine phosphorylation of insulin receptor substrate-1 (IRS-1)/4PS. Enhanced tyrosine phosphorylation of IRS-1/4PS was observed in response to IL-4, but not IL-13 treatment of L cells transfected with the IL-2R gamma chain. These results indicate that IL-13 does not use the IL-2R gamma subunit in its receptor complex and that expression of IL-2R gamma enhances, but is not absolutely required for mediating IL-4-induced tyrosine phosphorylation of IRS-1/4PS.

Background We reviewed our experience using anterior thoracoscopic procedures in the correction of severe idiopathic scoliosis and kyphotic deformities to evaluate the feasibility and effectiveness of such procedures. Study design Twenty-four patients who underwent thoracoscopic surgical correction of the spine between March 1995 and December 2001 were retrospectively reviewed. A team consisting of one orthopaedic surgeon and one thoracic surgeon performed anterior thoracoscopic soft tissue release, disc excision, and bone grafting followed on the same day with posterior instrumentation and correction of deformity. Results There were 16 female and 8 male patients, with a median age of 16 years (range 11 to 47 years) with idiopathic scoliosis (20 patients) or kyphotic deformity (4 patients). The average time for the thoracoscopy was 125 minutes (range 60 to 175 minutes). Blood loss averaged 135 mL (range 20 to 350 mL), and a median number of five discs (range two to eight) were excised. The median ICU time was 2 days (range 1 to 8 days), and the median length of hospital stay was 6 days (range 4 to 11 days). One patient required conversion to an open procedure because of arterial bleeding from the cancellous bone (T5). Postoperative complications occurred in four patients (atelectasis, pneumothorax, pneumonia, and wound infection in one patient each). All patients had an uneventful hospital course after treatment. Conclusions Thoracoscopic anterior procedures can be used safely and effectively in the treatment of idiopathic scoliosis and kyphotic deformity. This minimally invasive approach might decrease procedure-related trauma, operative time, blood loss, and length of hospitalization and may also alleviate postthoracotomy pain.

The Murchison Widefield Array (MWA) is a new low-frequency, wide-field-of-view radio interferometer under development at the Murchison Radio-astronomy Observatory in Western Australia. We have used a 32 element MWA prototype interferometer (MWA-32T) to observe two 50° diameter fields in the southern sky, covering a total of ~2700 deg[superscript 2], in order to evaluate the performance of the MWA-32T, to develop techniques for epoch of reionization experiments, and to make measurements of astronomical foregrounds. We developed a calibration and imaging pipeline for the MWA-32T, and used it to produce ~15' angular resolution maps of the two fields in the 110-200 MHz band. We perform a blind source extraction using these confusion-limited images, and detect 655 sources at high significance with an additional 871 lower significance source candidates. We compare these sources with existing low-frequency radio surveys in order to assess the MWA-32T system performance, wide-field analysis algorithms, and catalog quality. Our source catalog is found to agree well with existing low-frequency surveys in these regions of the sky and with statistical distributions of point sources derived from Northern Hemisphere surveys; it represents one of the deepest surveys to date of this sky field in the 110-200 MHz band., National Science Foundation (U.S.) (Grant AST-0457585), National Science Foundation (U.S.) (Grant AST-0821321), National Science Foundation (U.S.) (Grant AST-0908884), National Science Foundation (U.S.) (Grant AST-1008353), National Science Foundation (U.S.) (Grant PHY-0835713), United States. Air Force Office of Scientific Research (Grant FA9550-0510247), MIT School of Science, Smithsonian Astrophysical Observatory, Massachusetts Institute of Technology (Marble Astrophysics Fund), Raman Research Institute

The properties and outcome of an immune response are best predicted by the lymphokine phenotype of the responding T cells. Cytokines produced by CD4+ T helper type 1 (Th1) T cells mediate delayed type hypersensitivity (DTH) and inflammatory responses, whereas cytokines produced by Th2 T cells mediate helper T cell functions for antibody production. To determine whether induction of Th2-like cells would modulate an inflammatory response, interleukin 4 (IL-4) was administered to animals with experimental allergic encephalomyelitis (EAE), a prototypic autoimmune disease produced by Th1-like T cells specific for myelin basic protein (MBP). IL-4 treatment resulted in amelioration of clinical disease, the induction of MBP-specific Th2 cells, diminished demyelination, and inhibition of the synthesis of inflammatory cytokines in the central nervous system (CNS). Modulation of an immune response from one dominated by excessive activity of Th1-like T cells to one dominated by the protective cytokines produced by Th2-like T cells may have applicability to the therapy of certain human autoimmune diseases.