Analysis of auditory functions in grades one, two, and three.

Thesis (Ed.M.)--Boston Universit

Characterizing the Cool KOIs. VI. H- and K-band Spectra of Kepler M Dwarf Planet-Candidate Hosts

We present H- and K-band spectra for late-type Kepler Objects of Interest (the "Cool KOIs"): low-mass stars with transiting-planet candidates discovered by NASA's Kepler Mission that are listed on the NASA Exoplanet Archive. We acquired spectra of 103 Cool KOIs and used the indices and calibrations of Rojas-Ayala et al. to determine their spectral types, stellar effective temperatures and metallicities, significantly augmenting previously published values. We interpolate our measured effective temperatures and metallicities onto evolutionary isochrones to determine stellar masses, radii, luminosities and distances, assuming the stars have settled onto the main-sequence. As a choice of isochrones, we use a new suite of Dartmouth predictions that reliably include mid-to-late M dwarf stars. We identify five M4V stars: KOI-961 (confirmed as Kepler 42), KOI-2704, KOI-2842, KOI-4290, and the secondary component to visual binary KOI-1725, which we call KOI-1725 B. We also identify a peculiar star, KOI-3497, which has a Na and Ca lines consistent with a dwarf star but CO lines consistent with a giant. Visible-wavelength adaptive optics imaging reveals two objects within a 1 arc second diameter; however, the objects' colors are peculiar. The spectra and properties presented in this paper serve as a resource for prioritizing follow-up observations and planet validation efforts for the Cool KOIs, and are all available for download online using the "data behind the figure" feature.Comment: Accepted for publication in the Astrophysical Journal Supplement Series (ApJS). Data and table are available in the sourc

Comparison of Intraoperative Fluoroscopy to Postoperative Weight-Bearing Radiographs Obtained 4 to 6 Weeks After Bunion Repair With A Chevron Osteotomy

Background: During operative treatment of bunions, an attempt is made to correct the hallux valgus angle (HVA) and the intermetatarsal angle (IMA). In this study, the HVA and the IMA were measured using intraoperative C-arm fluoroscopic images obtained during surgical treatment of a bunion with chevron osteotomy. These angles were again measured using weight-bearing radiographs obtained 4 to 6 weeks postoperatively. Methods: At our institution, we reviewed medical records of patients who underwent a bunion repair with chevron osteotomy between January 2013 and October 2017. A total of 26 feet from 24 patients were included. Three authors (ALP, TMH, and RAM) measured the HVA and IMA using intraoperative fluoroscopic images and postoperative weight-bearing radiographs (4 measurements per foot; total, 104 measurements). The authors were blinded to their previous angular measurements and to measurements made by the others. An intraclass correlation coefficient was calculated for the HVA and IMA measurements between groups (ie, intraoperative fluoroscopic images and postoperative radiographs) to determine interobserver reliability. We compared the angles measured by the authors between groups and used a paired t test for statistical evaluation. Results: Interobserver difference of the HVA and IMA was low between intraoperative fluoroscopic images and postoperative weight-bearing radiographs (0.98 and 0.79; 0.78 and 0.95, respectively). The measured IMAs were relatively consistent between groups (6.21° and 6.37°, respectively); only two patients had a difference \u3e 3°. There was a greater difference in HVAs between groups (11.5° and 14.2°, respectively). In 11 feet, the HVA was \u3e 5° (range, 5.3-12.7°) in the postoperative radiograph compared to the fluoroscopic image. In one foot, we noted a 7° decrease of the HVA on the postoperative radiograph. The average difference of HVA between groups was 2.6° (P \u3c 0.0001), whereas the IMA was 0.16° (P = 0.002). Conclusions: Interobserver measurements of the HVA and IMA were reliable on both the intraoperative fluoroscopic images and the postoperative weightbearing radiographs. The IMA was similar between groups; however, the HVA was often greater on the postoperative weight-bearing radiographs

Direct measurements of dust attenuation in z~1.5 star-forming galaxies from 3D-HST: Implications for dust geometry and star formation rates

The nature of dust in distant galaxies is not well understood, and until recently few direct dust measurements have been possible. We investigate dust in distant star-forming galaxies using near-infrared grism spectra of the 3D-HST survey combined with archival multi-wavelength photometry. These data allow us to make a direct comparison between dust around star-forming regions ($A_{V,\mathrm{HII}}$) and the integrated dust content ($A_{V,\mathrm{star}}$). We select a sample of 163 galaxies between $1.36\le{}z\le1.5$ with H$\alpha$ signal-to-noise ratio $\ge5$ and measure Balmer decrements from stacked spectra to calculate $A_{V,\mathrm{HII}}$. First, we stack spectra in bins of $A_{V,\mathrm{star}}$, and find that $A_{V,\mathrm{HII}}=1.86\,A_{V,\mathrm{star}}$, with a significance of $\sigma=1.7$. Our result is consistent with the two-component dust model, in which galaxies contain both diffuse and stellar birth cloud dust. Next, we stack spectra in bins of specific star formation rate ($\log\,\mathrm{SSFR}$), star formation rate ($\log\,\mathrm{SFR}$), and stellar mass ($\log{}M_*$). We find that on average $A_{V,\mathrm{HII}}$ increases with SFR and mass, but decreases with increasing SSFR. Interestingly, the data hint that the amount of extra attenuation decreases with increasing SSFR. This trend is expected from the two-component model, as the extra attenuation will increase once older stars outside the star-forming regions become more dominant in the galaxy spectrum. Finally, using Balmer decrements we derive dust-corrected H$\alpha$ SFRs, and find that stellar population modeling produces incorrect SFRs if rapidly declining star formation histories are included in the explored parameter space.Comment: Accepted for publication in the Astrophysical Journal (13 pages, 9 figures

Nurses\u27 Alumnae Association Bulletin - Volume 6 Number 9

Remember the Relief Fund Welcome! Miss Childs Financial Report Calendar of Coming Events Lest You Forget! Attention Review of the Alumnae Association Meetings Institutional Staff Nurses\u27 Section Report of Staff Activities - 1947-1948 Private Duty Section The White Haven Division Barton Memorial Division Remember the Relief Fund Student Nurses\u27 Activities Jefferson Scores Again The Clara Melville Scholarship Fund Interesting Activities of the Nurses\u27 Home Committee of the Women\u27s Board Exclusive for Nurses Changes in the Maternity Division Gray Lady Musical Therapy Service Memorial Service Honoring Mrs. Bessie Dobson Altemus The Blood Donor Center The Hospital Pharmacy Medical College News Remember the Relief Fund Administrative Staff and Faculty of the School of Nursing Streptomycin Changes in the Staff at Jefferson Hospital Care of the Thoracic Surgical Patient Miscellaneous Items Marriages New Arrivals Deaths The Bulletin Committee Attention, Alumnae New Addresse

An ALMA Search for Substructure, Fragmentation, and Hidden Protostars in Starless Cores in Chamaeleon I

We present an Atacama Large Millimeter/submillimeter Array (ALMA) 106 GHz (Band 3) continuum survey of the complete population of dense cores in the Chamaeleon I molecular cloud. We detect a total of 24 continuum sources in 19 different target fields. All previously known Class 0 and Class I protostars in Chamaeleon I are detected, whereas all of the 56 starless cores in our sample are undetected. We show that the Spitzer+Herschel census of protostars in Chamaeleon I is complete, with the rate at which protostellar cores have been misclassified as starless cores calculated as <1/56, or < 2%. We use synthetic observations to show that starless cores collapsing following the turbulent fragmentation scenario are detectable by our ALMA observations when their central densities exceed ~10^8 cm^-3, with the exact density dependent on the viewing geometry. Bonnor-Ebert spheres, on the other hand, remain undetected to central densities at least as high as 10^10 cm^-3. Our starless core non-detections are used to infer that either the star formation rate is declining in Chamaeleon I and most of the starless cores are not collapsing, matching the findings of previous studies, or that the evolution of starless cores are more accurately described by models that develop less substructure than predicted by the turbulent fragmentation scenario, such as Bonnor-Ebert spheres. We outline future work necessary to distinguish between these two possibilities.Comment: Accepted by Ap

Pregnancy incidence and correlates in a clinical trial preparedness study, North West Province South Africa.

INTRODUCTION: Women in HIV prevention trials often must typically agree to avoid pregnancy. Regardless, some become pregnant. Screening tools predicting pregnancy risk could maximize trial safety and efficiency. OBJECTIVES: We assessed incidence and correlates of pregnancy among women at high HIV risk. METHODS: We enrolled sexually-active, HIV-negative women into an observational cohort (2008-2011). At enrollment demographic, contraceptive, reproductive, pregnancy intention and behavioural data were collected. Women reported if one or both partners wanted or intended for the couple to become pregnant. We measured gender role beliefs using a locally validated eight-point index. We tested HIV and pregnancy, and inquired about sexually transmitted infection symptoms (STIs) at enrollment and monthly. HIV testing included behavioural counselling and condom provision, but did not specifically counsel women to avoid pregnancy. Cox proportional hazard modelling evaluated the associations with pregnancy. The multivariate model included the following variables "Recent pregnancy attempts", "Gender Roles Beliefs", "Self-reported STIs" and "Age". RESULTS: We screened 1068 women and excluded (24.6%, 263/1068) who did not report risk behaviour. Non-pregnant, non-sterilized women aged 18-35 (median = 21 years) enrolled (n = 438). Most women reported one partner (74.7%) and a prior live birth (84.6%). Median follow-up time was 6 months (range 0.7-15.5). Pregnancy incidence was 25.1 per 100 women-years (n = 57 pregnancies). Conservative beliefs on gender roles (Adjusted Hazard Ratio (aHR) 1.8; 95% confidence interval [CI] 1.1-2.9), recent pregnancy attempts (aHR 1.9; 95% CI 1.1-3.4) and baseline self-reported STI (aHR 2.5; 95% CI 1.4-4.4) were associated with increased incident pregnancy. Report of no pregnancy intention was associated with lowered pregnancy risk (aHR 0.3; 95% CI 0.1-0.7). CONCLUSIONS: We identified new and confirmed existing factors that can facilitate screening for pregnancy risk

Radiation Protection Using Single-Wall Carbon Nanotube Derivatives

This invention is a means of radiation protection, or cellular oxidative stress mitigation, via a sequence of quenching radical species using nano-engineered scaffolds, specifically single-wall carbon nanotubes (SWNTs) and their derivatives. The material can be used as a means of radiation protection by reducing the number of free radicals within, or nearby, organelles, cells, tissue, organs, or living organisms, thereby reducing the risk of damage to DNA and other cellular components (i.e., RNA, mitochondria, membranes, etc.) that can lead to chronic and/or acute pathologies, including but not limited to cancer, cardiovascular disease, immuno-suppression, and disorders of the central nervous system. In addition, this innovation could be used as a prophylactic or antidote for accidental radiation exposure, during high-altitude or space travel where exposure to radiation is anticipated, or to protect from exposure from deliberate terrorist or wartime use of radiation- containing weapons

The Mass-Function of Low Mass Halo Stars: Limits on Baryonic Halo Dark Matter

We derive mass functions (MF) for halo red dwarfs (the faintest hydrogen burning stars) and then extrapolate to place limits on the total mass of halo brown dwarfs (stars not quite massive enough to burn hydrogen). The mass functions are obtained from the luminosity function of a sample of 114 local halo stars in the USNO parallax survey (Dahn \etal 1995). We use stellar models of Alexander \etal (1996) and make varying assumptions about metallicity and about possible unresolved binaries in the sample. We find that the MF for halo red dwarfs cannot rise more quickly than $1/m^2$ as one approaches the hydrogen burning limit. Using recent results from star formation theory, we extrapolate the MF into the brown-dwarf regime. We see that likely extrapolations imply that the total mass of brown dwarfs in the halo is less than $\sim 3\%$ of the local mass density of the halo ($\sim 0.3\%$ for the more realistic models we consider). Our limits apply to brown dwarfs in the halo that come from the same stellar population as the red dwarfs.Comment: Significant changes over previous submission. To be published ApJ Letters, 16 pages, latex, one figur

Effects of Co-ingesting Dietary Nitrate and Vitamin C on Nitric Oxide Bioavailability, Blood Pressure, and Cardiovascular Reactivity in Hispanic Females

High blood pressure is a hallmark of chronic disease and is disproportionately prevalent in ethnic minorities. Dietary nitrate has been shown to lower blood pressure via increased nitric oxide (NO), but few studies have examined if combining nitrate with vitamin C (VITC) could have beneficial synergistic effects on blood pressure by augmenting NO, and limited data exist in females. PURPOSE: To investigate if combining nitrate-rich beetroot juice (BR) with VITC could further augment NO bioavailability and improve blood pressure in Hispanic females compared to BR and VITC ingested alone. METHODS: Eight sedentary Hispanic females participated in four conditions to ingest: 1) BR and VITC (BR+VITC), 2) BR and crystal light (BR+CRY), 3) nitrate-depleted BR and VITC (PL+VITC), and 4) PL and CRY (PL+CRY). A blood draw and blood pressure were obtained at rest, followed by a cardiovascular reactivity test. RESULTS: Plasma nitrate was increased in BR+VITC and BR+CRY compared to PL+VITC and PL+CRY (P0.05). Plasma nitrite was increased in BR+VITC and BR+CRY compared to PL+VITC and PL+CRY (P0.05). CONCLUSION: Co-ingestion of dietary nitrate and VITC increased plasma nitrite compared to BR alone, which could indicate augmented NO bioavailability following BR+VITC; however, there was no impact of nitrate supplementation on markers of cardiovascular health