Down Regulation with Luteal GnRH Agonist Therapy in Euploid Embryo Transfers Does Not Impact Pregnancy Rates

Introduction : Gonadotropin-releasing hormone (GnRH) agonists have been used during assisted reproductive technology (ART) treatment for pituitary suppression and stimulation. Currently, clinical opinion is divided about whether GnRH agonist therapy improves pregnancy rates when used for luteal down-regulation in a frozen euploid embryo transfer (FET). This study evaluated the clinical utility of GnRH agonist down-regulation in single, euploid FET cycles. Methods : A retrospective analysis was performed, using data from patients who underwent a single, euploid FET cycle from 2012 to 2019. Patients were segregated into two cohorts: Group A: single, euploid FET with down-regulation using GnRH agonist; Group B: single, euploid FET without down-regulation using GnRH agonist. Primary outcomes include pregnancy rates among cohorts. Results : Group A demonstrated a pregnancy rate of 72.92% in 96 cycles. Group B demonstrated a pregnancy rate of 73.27% in 5,668 cycles. There was no difference in pregnancy rates between groups, X2(2, N = 5764) = .0061, p = .94. A subgroup of patients (n=5) with endometriosis in Group A achieved an 80% (4/5) pregnancy rate. Discussion : Single, euploid FET cycle pregnancy rates were not affected by the use of down-regulation with a GnRH agonist. Increased pregnancy rates found with prolonged GnRH agonist use in other studies weren’t seen with short term use for FET cycles. Future research should focus on molecular markers and gene transcription signatures to attempt to define whether there is an ideal population of patients who would benefit from GnRH agonist down-regulation prior to FET

The Effects of Self-Assessment Using Coach’s Eye on Perceived Competence in Elementary Physical Education

Engaging students in meaningful experiences that inspire them to be active both in and out of school is the primary goal of quality physical education programs (National Association of Sport and Physical Education & American Heart Association, 2012). One of the strongest influences on student engagement in physical education is their perceived physical competence (Bevens, Fitzpatrick, Sanchez, & Forrest, 2010; Carney, 2012). The purpose if this study was to explore how perceived physical competence was affected by the use of video feedback using the Coach’s Eye application. Participants in this study were 60 fourth and fifth grade students. There were 31 participants in the technology intervention and 29 participants in the control group (no technology). Four class sections took part in this study (2 fourth grade, 2 fifth grade), each taking part in an eight-lesson unit on striking skills. Throughout the unit students worked in small groups video recording each other with iPads in order to evaluate their own progress. Participants used the iPad application Coach’s Eye to review and assess their own videos. Before, during, and after the unit subjects took a modified sports and athletics subscale of the Children and Youth Physical Self-Perception Profile (CY-PSPP). The results indicated that there was no significant difference between the technology group and the control group. Slight increase in the levels of perceived competence among students in the technology group were identified, however there were no statistical difference in significanc

Parameter Estimation for a Model With Both Imperfect Test and Repair

We describe estimation of the parameters of a manufacturing test and repair model using data available from that test. The model allows imperfect testing and imperfect repair. The principal problem that we address is of parameter identification, given insufficient data, that we address by making conservative assumptions on the property being measured and the associated parameter values. Several cases of commonly occurring test types, in the manufacture of electronic products, are considered

CO in Protostars (COPS): HerschelHerschel-SPIRE Spectroscopy of Embedded Protostars

We present full spectral scans from 200-670$\mu$m of 26 Class 0+I protostellar sources, obtained with $Herschel$-SPIRE, as part of the "COPS-SPIRE" Open Time program, complementary to the DIGIT and WISH Key programs. Based on our nearly continuous, line-free spectra from 200-670 $\mu$m, the calculated bolometric luminosities ($L_{\rm bol}$) increase by 50% on average, and the bolometric temperatures ($T_{\rm bol}$) decrease by 10% on average, in comparison with the measurements without Herschel. Fifteen protostars have the same Class using $T_{\rm bol}$ and $L_{\rm bol}$/$L_{\rm submm}$. We identify rotational transitions of CO lines from J=4-3 to J=13-12, along with emission lines of $^{13}$CO, HCO$^+$, H$_{2}$O, and [CI]. The ratios of $^{12}$CO to $^{13}$CO indicate that $^{12}$CO emission remains optically thick for $J_{\rm up}$ < 13. We fit up to four components of temperature from the rotational diagram with flexible break points to separate the components. The distribution of rotational temperatures shows a primary population around 100 K with a secondary population at $\sim$350 K. We quantify the correlations of each line pair found in our dataset, and find the strength of correlation of CO lines decreases as the difference between $J$-level between two CO lines increases. The multiple origins of CO emission previously revealed by velocity-resolved profiles are consistent with this smooth distribution if each physical component contributes to a wide range of CO lines with significant overlap in the CO ladder. We investigate the spatial extent of CO emission and find that the morphology is more centrally peaked and less bipolar at high-$J$ lines. We find the CO emission observed with SPIRE related to outflows, which consists two components, the entrained gas and shocked gas, as revealed by our rotational diagram analysis as well as the studies with velocity-resolved CO emission.Comment: 50 pages, 18 figures, accepted to ApJS. Revised for Table 6 and Figure

Next Generation Very Large Array Memo No. 6, Science Working Group 1: The Cradle of Life

This paper discusses compelling science cases for a future long-baseline interferometer operating at millimeter and centimeter wavelengths, like the proposed Next Generation Vary Large Array (ngVLA). We report on the activities of the Cradle of Life science working group, which focused on the formation of low- and high-mass stars, the formation of planets and evolution of protoplanetary disks, the physical and compositional study of Solar System bodies, and the possible detection of radio signals from extraterrestrial civilizations. We propose 19 scientific projects based on the current specification of the ngVLA. Five of them are highlighted as possible Key Science Projects: (1) Resolving the density structure and dynamics of the youngest HII regions and high-mass protostellar jets, (2) Unveiling binary/multiple protostars at higher resolution, (3) Mapping planet formation regions in nearby disks on scales down to 1 AU, (4) Studying the formation of complex molecules, and (5) Deep atmospheric mapping of giant planets in the Solar System. For each of these projects, we discuss the scientific importance and feasibility. The results presented here should be considered as the beginning of a more in-depth analysis of the science enabled by such a facility, and are by no means complete or exhaustive.Comment: 51 pages, 12 figures, 1 table. For more information visit https://science.nrao.edu/futures/ngvl

The TW Hya Rosetta Stone Project. I. Radial and Vertical Distributions of DCN and DCO⁺

Molecular D/H ratios are frequently used to probe the chemical past of solar system volatiles. Yet it is unclear which parts of the solar nebula hosted an active deuterium fractionation chemistry. To address this question, we present 0farcs2–0farcs4 Atacama Large Millimeter/submillimeter Array (ALMA) observations of DCO⁺ and DCN 2–1, 3–2, and 4–3 toward the nearby protoplanetary disk around TW Hya, taken as part of the TW Hya Rosetta Stone project, augmented with archival data. DCO⁺ is characterized by an excitation temperature of ~40 K across the 70 au radius pebble disk, indicative of emission from a warm, elevated molecular layer. Tentatively, DCN is present at even higher temperatures. Both DCO⁺ and DCN present substantial emission cavities in the inner disk, while in the outer disk the DCO⁺ and DCN morphologies diverge: most DCN emission originates from a narrow ring peaking around 30 au, with some additional diffuse DCN emission present at larger radii, while DCO⁺ is present in a broad structured ring that extends past the pebble disk. Based on a set of simple parametric disk abundance models, these emission patterns can be explained by a near-constant DCN abundance exterior to the cavity, and an increasing DCO⁺ abundance with radius. In conclusion, the ALMA observations reveal an active deuterium fractionation chemistry in multiple disk regions around TW Hya, but not in the cold planetesimal-forming midplane and in the inner disk. More observations are needed to explore whether deuterium fractionation is actually absent in these latter regions, and if its absence is a common feature or something peculiar to the old TW Hya disk