The Volatile Composition of the Split Ecliptic comet 73P/Schwassmann-Wachmann 3: A Comparison of Fragments C and B

The composition of fragments C and B of the Jupiter-family comet 73P/Schwassmann-Wachmann 3 (SW3) was investigated in early April of 2006 at IR wavelengths using high-dispersion echelle spectroscopy. Both fragments were depleted in ethane, and C was depleted in most forms of volatile carbon. In particular, fragment C shows a severe depletion of CH_(3)OH but a "normal" abundance of HCN (which has a similar volatility). Thermal processing is a possible explanation, but since fragment B is perhaps sublimating fresher material because of the frequent outbursts and fragmentation, the observed depletions might have cosmogonic implications. The chemistry of the volatile ices in SW3, like in the Oort Cloud comet C/1999 S4 (LINEAR), may be associated with sublimation of icy mantles from precometary grains followed by subsequent gas-phase chemistry and recondensation

Non-detection of L-band Line Emission from the Exoplanet HD189733b

We attempt to confirm bright non-local thermodynamic equilibrium (non-LTE) emission from the exoplanet HD 189733b at 3.25 μm, as recently reported by Swain et al. based on observations at low spectral resolving power (λ/δλ ≈ 30). Non-LTE emission lines from gas in an exoplanet atmosphere will not be significantly broadened by collisions, so the measured emission intensity per resolution element must be substantially brighter when observed at high spectral resolving power. We observed the planet before, during, and after a secondary eclipse event at a resolving power λ/δλ = 27, 000 using the NIRSPEC spectrometer on the Keck II telescope. Our spectra cover a spectral window near the peak found by Swain et al., and we compare emission cases that could account for the magnitude and wavelength dependence of the Swain et al. result with our final spectral residuals. To model the expected line emission, we use a general non-equilibrium formulation to synthesize emission features from all plausible molecules that emit in this spectral region. In every case, we detect no line emission to a high degree of confidence. After considering possible explanations for the Swain et al. results and the disparity with our own data, we conclude that an astrophysical source for the putative non-LTE emission is unlikely. We note that the wavelength dependence of the signal seen by Swain et al. closely matches the 2ν_2 band of water vapor at 300 K, and we suggest that an imperfect correction for telluric water is the source of the feature claimed by Swain et al

Tasa de cesáreas según la aplicación de la Clasificación de Robson en Hospitales nivel III de Trujillo 2022

El estudio tuvo como objetivo determinar la tasa de cesáreas según la aplicación de la Clasificación de Robson en hospitales nivel III de Trujillo 2022, la metodología empleó un enfoque cuantitativo, tipo descriptivo, diseño no experimental, de corte transversal. La muestra fue de 3249 mujeres atendidas por parto de enero a septiembre del 2022. Se utilizó una ficha de datos basada en la Clasificación de Robson. Se recolectó la información del Sistema Informático Perinatal. La tasa de cesárea para el Hospital Belén de Trujillo fue de 74,30% (1402/1887) y los grupos con mayor contribución fueron 5, 1, 10 y 3, mientras que, en el Hospital Regional Docente de Trujillo fue de 75, 26% (1025/1362) y los grupos con mayor contribución fueron 5, 10, 1 y 3. En ambos hospitales, las características socioculturales predominantes fueron: jóvenes, con secundaria y convivientes, y en características obstétricas fueron: multíparas, a término, categoría simple, sin antecedente de cesárea, feto en cefálica e inicio de parto espontáneo. La Clasificación de Robson extenderá la tasa de cesáreas y los grupos con mayor contribución al incremento sobre el parámetro de la OMS (15%).The objective of the study was to determine the rate of cesarean sections according to the application of the Robson Classification in level III hospitals of Trujillo 2022, the methodology used a quantitative approach, descriptive type, non experimental design, cross-sectional. The sample consisted of 3,249 women attended for childbirth from January to September 2022. A data sheet based on the Robson Classification was used. Information was collected from the Perinatal Information System. The caesarean section rate for the Hospital Belén de Trujillo was 74.30% (1402/1887) and the groups with the highest contribution were 5, 1, 10 and 3, while at the Hospital Regional Docente de Trujillo it was 75, 26% (1025/1362) and the groups with the greatest contribution were 5, 10, 1 and 3. In both hospitals, the predominant sociocultural characteristics were: young people, with secondary education and cohabiting, and in obstetric characteristics they were: multiparous, at term, simple category, with no history of cesarean section, cephalic fetus and spontaneous onset of labor. The Robson Classification will extend the rate of cesarean sections and the groups with the greatest contribution to the increase over the WHO parameter (15%).Tesi

Planetary Spectrum Generator: an accurate online radiative transfer suite for atmospheres, comets, small bodies and exoplanets

We have developed an online radiative-transfer suite (https://psg.gsfc.nasa.gov) applicable to a broad range of planetary objects (e.g., planets, moons, comets, asteroids, TNOs, KBOs, exoplanets). The Planetary Spectrum Generator (PSG) can synthesize planetary spectra (atmospheres and surfaces) for a broad range of wavelengths (UV/Vis/near-IR/IR/far-IR/THz/sub-mm/Radio) from any observatory (e.g., JWST, ALMA, Keck, SOFIA), any orbiter (e.g., ExoMars, Juno), or any lander (e.g., MSL). This is achieved by combining several state-of-the-art radiative transfer models, spectroscopic databases and planetary databases (i.e., climatological and orbital). PSG has a 3D (three-dimensional) orbital calculator for most bodies in the solar system, and all confirmed exoplanets, while the radiative-transfer models can ingest billions of spectral signatures for hundreds of species from several spectroscopic repositories. It integrates the latest radiative-transfer and scattering methods in order to compute high resolution spectra via line-by-line calculations, and utilizes the efficient correlated-k method at moderate resolutions, while for computing cometary spectra, PSG handles non-LTE and LTE excitation processes. PSG includes a realistic noise calculator that integrates several telescope / instrument configurations (e.g., interferometry, coronagraphs) and detector technologies (e.g., CCD, heterodyne detectors, bolometers). Such an integration of advanced spectroscopic methods into an online tool can greatly serve the planetary community, ultimately enabling the retrieval of planetary parameters from remote sensing data, efficient mission planning strategies, interpretation of current and future planetary data, calibration of spectroscopic data, and development of new instrument/spacecraft concepts.Comment: Journal of Quantitative Spectroscopy and Radiative Transfer, submitte

IRCS/Subaru Observations of Water in the Inner Coma of Comet 73P-B/Schwassmann-Wachmann 3: Spatially Resolved Rotational Temperatures and Ortho-Para Ratios

Comet 73P-B/Schwassmann-Wachmann 3 was observed with IRCS/Subaru at geocentric distance of 0.074 AU on UT 10 May 2006. Multiple H2O emission lines were detected in non-resonant fluorescence near 2.9 microns. No significant variation in total H2O production rate was found during the (3 hour) duration of our observations. H2O rotational temperatures and ortho-to-para abundance ratios were measured for several positions in the coma. The temperatures extracted from two different time intervals show very similar spatial distributions. For both, the rotational temperature decreased from ~110 K to ~90 K as the projected distance from the nucleus increased from ~5 to ~30 km. We see no evidence for OPR change in the coma. The H2O ortho-para ratio is consistent with the statistical equilibrium value (3.0) for all spatially resolved measurements. This implies a nuclear spin temperature higher than ~ 45 K.Comment: accepted for Icaru