bluuebunny/crossref_metadata_2025_split huggingface dataset:
The Prevalence of Constipation and Irritable Bowel Syndrome in Parkinson’s Disease Patients According to Rome III Diagnostic Criteria
Authors: Mishima Takayasu , Fukae Jiro , Fujioka Shinsuke , Inoue Kotoe , Tsuboi Yoshio 
Published: January 2017

Background: Gastrointestinal symptoms are one of the most common non-motor features of Parkinson’s disease (PD). Recently, a report from Taiwan revealed that irritable bowel syndrome (IBS) may be associated with an increased risk of developing PD; however, the prevalence of IBS in PD patients has not been fully evaluated. Rome III criteria are widely assessed with a questionnaire to determine functional gastrointestinal disorders. Objective: We assessed the prevalence of constipation and IBS in PD patients in our cohort using Rome III criteria. Methods: Between October 2014 and April 2015, 118 patients with PD were treated at Fukuoka University Hospital and were enrolled in this study. Rome III criteria were used to diagnose constipation and IBS. Results: Constipation and IBS were detected in 32 (27.1%) and 20 patients (17.0%), respectively. The most common symptom related to constipation was straining during defecation (77.1%). Among constipation symptoms, patients’ self-awareness of constipation was mostly related to straining during defecation (odds ratio 5.27, 95% confidence interval 1.475–18.811). The number of constipation symptoms was correlated with the severity of the Hoehn-Yahr Stage ( p < 0.05) and total levodopa equivalent dose ( p < 0.05). Conclusions: This is the first report to investigate the prevalence of IBS in PD patients with Rome III criteria. We found a higher prevalence of IBS compared with the general population. The prevalence of constipation based on Rome III criteria was much lower than that reported in previous studies. Further studies are warranted to evaluate gastrointestinal symptoms in PD patients using comparable questionnaires.
Un cas d'albinisme chez Phyllodactylus europaeus Gene, 1838. Premier cas signalé dans la famille des Gekkonidae (Sauria-Reptiles)
Authors: Delaugerre Michel 
Published: January 2017

Primo caso di albinismo noto nella famiglia dei Gekkonidae e raro caso negli Sauria, uno Phyllodactylus europaeus albino é stato raccolto nel Sud délia Francia.
Summary. — First record of albinism in the Gekkonid lizards, an albino Phyllodactylus europaeus has been collected in South of France. This is a rare record of albinism among Sauria.
Joint Ne/O and Fe/O Analysis to Diagnose Large Solar Energetic Particle Events during Solar Cycle 23
Authors: Tan Lun C. , Malandraki Olga E. , Shao Xi 
Published: January 2017

Abstract
We have examined 29 large solar energetic particle (SEP) events with the peak proton intensity J
pp(>60 MeV) > 1 pfu during solar cycle 23. The emphasis of our examination is put on a joint analysis of Ne/O and Fe/O data in the energy range (3–40 MeV nucleon−1) covered by Wind/Low-Energy Matrix Telescope and ACE/Solar Isotope Spectrometer sensors in order to differentiate between the Fe-poor and Fe-rich events that emerged from the coronal mass ejection driven shock acceleration process. An improved ion ratio calculation is carried out by rebinning ion intensity data into the form of equal bin widths in the logarithmic energy scale. Through the analysis we find that the variability of Ne/O and Fe/O ratios can be used to investigate the accelerating shock properties. In particular, the high-energy Ne/O ratio is well correlated with the source plasma temperature of SEPs.
When the Jeans Do Not Fit: How Stellar Feedback Drives Stellar Kinematics and Complicates Dynamical Modeling in Low-mass Galaxies
Authors: El-Badry Kareem , Wetzel Andrew R. , Geha Marla , Quataert Eliot , Hopkins Philip F. , Kereš Dusan , Chan T. K. , Faucher-Giguère Claude-André 
Published: January 2017

Abstract
In low-mass galaxies, stellar feedback can drive gas outflows that generate non-equilibrium fluctuations in the gravitational potential. Using cosmological zoom-in baryonic simulations from the Feedback in Realistic Environments project, we investigate how these fluctuations affect stellar kinematics and the reliability of Jeans dynamical modeling in low-mass galaxies. We find that stellar velocity dispersion and anisotropy profiles fluctuate significantly over the course of galaxies’ starburst cycles. We therefore predict an observable correlation between star formation rate and stellar kinematics: dwarf galaxies with higher recent star formation rates should have systemically higher stellar velocity dispersions. This prediction provides an observational test of the role of stellar feedback in regulating both stellar and dark-matter densities in dwarf galaxies. We find that Jeans modeling, which treats galaxies as virialized systems in dynamical equilibrium, overestimates a galaxy’s dynamical mass during periods of post-starburst gas outflow and underestimates it during periods of net inflow. Short-timescale potential fluctuations lead to typical errors of ∼20% in dynamical mass estimates, even if full three-dimensional stellar kinematics—including the orbital anisotropy—are known exactly. When orbital anisotropy is not known a priori, typical mass errors arising from non-equilibrium fluctuations in the potential are larger than those arising from the mass-anisotropy degeneracy. However, Jeans modeling alone cannot reliably constrain the orbital anisotropy, and problematically, it often favors anisotropy models that do not reflect the true profile. If galaxies completely lose their gas and cease forming stars, fluctuations in the potential subside, and Jeans modeling becomes much more reliable.
The Abundance of C2H4 in the Circumstellar Envelope of IRC+10216
Authors: Fonfría J. P. , Hinkle K. H. , Cernicharo J. , Richter M. J. , Agúndez M. , Wallace L. 
Published: January 2017

Abstract
High spectral resolution mid-IR observations of ethylene (

) toward the AGB star IRC+10216 were obtained using the Texas Echelon Cross Echelle Spectrograph (TEXES) at the NASA Infrared Telescope Facility (IRTF). 80 ro-vibrational lines from the 10.5 μm vibrational mode

with J ≲ 30 were detected in absorption. The observed lines are divided into two groups with rotational temperatures of 105 and 400 K (warm and hot lines). The warm lines peak at ≃ −14 km s−1 with respect to the systemic velocity, suggesting that they are mostly formed outwards from

. The hot lines are centered at −10 km s−1 indicating that they come from a shell between 10 and

. 35% of the observed lines are unblended and can be fitted with a code developed to model the emission of a spherically symmetric circumstellar envelope. The analysis of several scenarios reveals that the

abundance relative to H2 in the range 5−20R
⋆ is

on average and it could be as high as 1.1 × 10−7. Beyond

, it is 8.2 × 10−8. The total column density is (6.5 ± 3.0) × 1015 cm−2.

is found to be rotationally under local thermodynamical equilibrium (LTE) and vibrationally out of LTE. One of the scenarios that best reproduce the observations suggests that up to 25% of the

molecules at

could condense onto dust grains. This possible depletion would not significantly influence the gas acceleration although it could play a role in the surface chemistry on the dust grains.
Characterization of the Wolf 1061 Planetary System
Authors: Kane Stephen R. , von Braun Kaspar , Henry Gregory W. , Waters Miranda A. , Boyajian Tabetha S. , Mann Andrew W. 
Published: January 2017

Abstract
A critical component of exoplanetary studies is an exhaustive characterization of the host star, from which the planetary properties are frequently derived. Of particular value are the radius, temperature, and luminosity, which are key stellar parameters for studies of transit and habitability science. Here we present the results of new observations of Wolf 1061, known to host three super-Earths. Our observations from the Center for High Angular Resolution Astronomy interferometric array provide a direct stellar radius measurement of 0.3207 ± 0.0088 R
⊙, from which we calculate the effective temperature and luminosity using spectral energy distribution models. We obtained 7 yr of precise, automated photometry that reveals the correct stellar rotation period of 89.3 ± 1.8 days, finds no evidence of photometric transits, and confirms that the radial velocity signals are not due to stellar activity. Finally, our stellar properties are used to calculate the extent of the Habitable Zone (HZ) for the Wolf 1061 system, for which the optimistic boundaries are 0.09–0.23 au. Our simulations of the planetary orbital dynamics show that the eccentricity of the HZ planet oscillates to values as high as ∼0.15 as it exchanges angular momentum with the other planets in the system.
A GALACTIC MOLECULAR CLOUD CLUMP CATALOG FROM HI-GAL DATA: METHOD AND INITIAL RESULTS COMPARISON WITH BGPS
Authors: Zetterlund Erika , Glenn Jason , Rosolowsky Erik 
Published: January 2017

Abstract
As the precursors to stellar clusters, it is imperative that we understand the distribution and physical properties of dense molecular gas clouds and clumps. Such a study has been done with the ground-based Bolocam Galactic Plane Survey (BGPS). Now the Herschel infrared GALactic plane survey (Hi-GAL) allows us to do the same with higher-quality data and complete coverage of the Galactic plane. We have made a pilot study comparing dense molecular gas clumps identified in Hi-GAL and BGPS, using six 2° × 2° regions centered at Galactic longitudes of

, 30°, 41°, 50°, 202°, and 217°. We adopted the BGPS methodology for identifying clumps and estimating distances, leading to 6198 clumps being identified in our substudy, with 995 of those having well-constrained distances. These objects were evenly distributed with Galactic longitude, a consequence of Hi-GAL being source confusion limited. These clumps range in mass from 10−2 to 105
M
⊙ and have heliocentric distances of up to 16 kpc. When clumps found in both surveys are compared, we see that distances agree within 1 kpc and ratios of masses are of the order of unity. This serves as an external validation for BGPS and instills confidence as we move forward to cataloging the clumps from the entirety of Hi-GAL. In addition to the sources that were in common with BGPS, Hi-GAL found many additional sources, primarily due to the lack of atmospheric noise. We expect Hi-GAL to yield 2 × 105 clumps, with 20% having well-constrained distances, an order of magnitude above what was found in BGPS.
Chasing Shadows: Rotation of the Azimuthal Asymmetry in the TW Hya Disk*
Authors: Debes John H. , Poteet Charles A. , Jang-Condell Hannah , Gaspar Andras , Hines Dean , Kastner Joel H. , Pueyo Laurent , Rapson Valerie , Roberge Aki , Schneider Glenn , Weinberger Alycia J. 
Published: January 2017

Abstract
We have obtained new images of the protoplanetary disk orbiting TW Hya in visible, total intensity light with the Space Telescope Imaging Spectrograph (STIS) on the Hubble Space Telescope (HST), using the newly commissioned BAR5 occulter. These HST/STIS observations achieved an inner working angle of ∼0.″2, or 11.7 au, probing the system at angular radii coincident with recent images of the disk obtained by ALMA and in polarized intensity near-infrared light. By comparing our new STIS images to those taken with STIS in 2000 and with NICMOS in 1998, 2004, and 2005, we demonstrate that TW Hya’s azimuthal surface brightness asymmetry moves coherently in position angle. Between 50 au and 141 au we measure a constant angular velocity in the azimuthal brightness asymmetry of 22.°7 yr−1 in a counterclockwise direction, equivalent to a period of 15.9 yr assuming circular motion. Both the (short) inferred period and lack of radial dependence of the moving shadow pattern are inconsistent with Keplerian rotation at these disk radii. We hypothesize that the asymmetry arises from the fact that the disk interior to 1 au is inclined and precessing owing to a planetary companion, thus partially shadowing the outer disk. Further monitoring of this and other shadows on protoplanetary disks potentially opens a new avenue for indirectly observing the sites of planet formation.
The Dense Molecular Gas and Nuclear Activity in the ULIRG IRAS 13120–5453
Authors: Privon G. C. , Aalto S. , Falstad N. , Muller S. , González-Alfonso E. , Sliwa K. , Treister E. , Costagliola F. , Armus L. , Evans A. S. , Garcia-Burillo S. , Izumi T. , Sakamoto K. , Werf P. van der , Chu J. K. 
Published: January 2017

Abstract
We present new Atacama Large Millimeter/submillimeter Array Band 7 (∼340 GHz) observations of the dense gas tracers HCN, HCO+, and CS in the local, single-nucleus, ultraluminous infrared galaxy IRAS 13120–5453. We find centrally enhanced HCN (4–3) emission, relative to HCO+ (4–3), but do not find evidence for radiative pumping of HCN. Considering the size of the starburst (0.5 kpc) and the estimated supernovae rate of ∼1.2 yr−1, the high HCN/HCO+ ratio can be explained by an enhanced HCN abundance as a result of mechanical heating by the supernovae, though the active galactic nucleus and winds may also contribute additional mechanical heating. The starburst size implies a high ΣIR of 4.7 × 1012
L
⊙ kpc−2, slightly below predictions of radiation-pressure limited starbursts. The HCN line profile has low-level wings, which we tentatively interpret as evidence for outflowing dense molecular gas. However, the dense molecular outflow seen in the HCN line wings is unlikely to escape the Galaxy and is destined to return to the nucleus and fuel future star formation. We also present modeling of Herschel observations of the H2O lines and find a nuclear dust temperature of ∼40 K. IRAS 13120–5453 has a lower dust temperature and ΣIR than is inferred for the systems termed “compact obscured nuclei (CONs)” (such as Arp 220 and Mrk 231). If IRAS 13120–5453 has undergone a CON phase, we are likely witnessing it at a time when the feedback has already inflated the nuclear ISM and diluted star formation in the starburst/active galactic nucleus core.
Inflow, Outflow, Yields, and Stellar Population Mixing in Chemical Evolution Models
Authors: Andrews Brett H. , Weinberg David H. , Schönrich Ralph , Johnson Jennifer A. 
Published: January 2017

Abstract
Chemical evolution models are powerful tools for interpreting stellar abundance surveys and understanding galaxy evolution. However, their predictions depend heavily on the treatment of inflow, outflow, star formation efficiency (SFE), the stellar initial mass function, the SN Ia delay time distribution, stellar yields, and stellar population mixing. Using flexCE, a flexible one-zone chemical evolution code, we investigate the effects of and trade-offs between parameters. Two critical parameters are SFE and the outflow mass-loading parameter, which shift the knee in [O/Fe]–[Fe/H] and the equilibrium abundances that the simulations asymptotically approach, respectively. One-zone models with simple star formation histories follow narrow tracks in [O/Fe]–[Fe/H] unlike the observed bimodality (separate high-α and low-α sequences) in this plane. A mix of one-zone models with inflow timescale and outflow mass-loading parameter variations, motivated by the inside-out galaxy formation scenario with radial mixing, reproduces the two sequences better than a one-zone model with two infall epochs. We present [X/Fe]–[Fe/H] tracks for 20 elements assuming three different supernova yield models and find some significant discrepancies with solar neighborhood observations, especially for elements with strongly metallicity-dependent yields. We apply principal component abundance analysis to the simulations and existing data to reveal the main correlations among abundances and quantify their contributions to variation in abundance space. For the stellar population mixing scenario, the abundances of α-elements and elements with metallicity-dependent yields dominate the first and second principal components, respectively, and collectively explain 99% of the variance in the model. flexCE is a python package available at https://github.com/bretthandrews/flexCE.
Laboratory Investigations into the Spectra and Origin of Propylene Oxide: A Chiral Interstellar Molecule
Authors: Hudson R. L. , Loeffler M. J. , Yocum K. M. 
Published: January 2017

Abstract
Propylene oxide was recently identified in the interstellar medium, but few laboratory results are available for this molecule to guide current and future investigations. To address this situation, here we report infrared spectra, absorption coefficients, and band strengths of solid propylene oxide along with the first measurement of its refractive index and a calculation of its density, all for the amorphous solid form of the compound. We present the first experimental results showing a low-temperature formation pathway for propylene oxide near 10 K in interstellar ice analogs. Connections are drawn between our new results and the interstellar molecules propanal and acetone, and predictions are made about several as yet unobserved vinyl alcohols and methylketene. Comparisons are given to earlier laboratory work and a few applications to interstellar and solar system astrochemistry are described.
A Surface Density Perturbation in the TW Hydrae Disk at 95 au Traced by Molecular Emission
Authors: Teague R. , Semenov D. , Gorti U. , Guilloteau S. , Henning Th. , Birnstiel T. , Dutrey A. , Boekel R. van , Chapillon E. 
Published: January 2017

Abstract
We present ALMA Cycle 2 observations at 0.″5 resolution of TW Hya of CS

emission. The radial profile of the integrated line emission displays oscillatory features outward of 1.″5 (

au). A dip-like feature at 1.″6 is coincident in location, depth, and width with features observed in dust scattered light at near-infrared wavelengths. Using a thermochemical model indicative of TW Hya, gas-grain chemical modeling, and non-LTE radiative transfer, we demonstrate that such a feature can be reproduced with a surface density depression, consistent with the modeling performed for scattered-light observations of TW Hya. We further demonstrate that a gap in the dust distribution and dust opacity only cannot reproduce the observed CS feature. The outer enhancement at 3.″1 is identified as a region of intensified desorption due to enhanced penetration of the interstellar far-UV radiation at the exponential edge of the disk surface density, which intensifies the photochemical processing of gas and ices.
An ALMA Survey of DCN/H13CN and DCO+/H13CO+ in Protoplanetary Disks
Authors: Huang Jane , Öberg Karin I. , Qi Chunhua , Aikawa Yuri , Andrews Sean M. , Furuya Kenji , Guzmán Viviana V. , Loomis Ryan A. , van Dishoeck Ewine F. , Wilner David J. 
Published: January 2017

Abstract
The deuterium enrichment of molecules is sensitive to their formation environment. Constraining patterns of deuterium chemistry in protoplanetary disks is therefore useful for probing how material is inherited or reprocessed throughout the stages of star and planet formation. We present ALMA observations at ∼0.″6 resolution of DCO+, H13CO+, DCN, and H13CN in the full disks around T Tauri stars AS 209 and IM Lup, in the transition disks around T Tauri stars V4046 Sgr and LkCa 15, and in the full disks around Herbig Ae stars MWC 480 and HD 163296. We also present ALMA observations of HCN in the IM Lup disk. DCN, DCO+, and H13CO+ are detected in all disks, and H13CN in all but the IM Lup disk. We find efficient deuterium fractionation for the sample, with estimates of disk-averaged DCO+/HCO+ and DCN/HCN abundance ratios ranging from ∼0.02–0.06 and ∼0.005–0.08, respectively, which is comparable to values reported for other interstellar environments. The relative distributions of DCN and DCO+ vary between disks, suggesting that multiple formation pathways may be needed to explain the diverse emission morphologies. In addition, gaps and rings observed in both H13CO+ and DCO+ emission provide new evidence that DCO+ bears a complex relationship with the location of the midplane CO snowline.
MOND Calculations of Bulk Dispersions and Radial Dispersion Profiles of Milky Way and Andromeda Dwarf Spheroidal Galaxies
Authors: Alexander S. G. , Walentosky M. J. , Messinger Justin , Staron Alexander , Blankartz Benjamin , Clark Tristan 
Published: January 2017

Abstract
We present a new computational method for calculating the motion of stars in a dwarf spheroidal galaxy (dSph) that can use either Newtonian gravity or Modified Newtonian Dynamics (MOND). In our model, we explicitly calculate the motion of several thousand stars in a spherically symmetric gravitational potential, and we statistically obtain both the line-of-sight bulk velocity dispersion and dispersion profile. Our results for MOND calculated bulk dispersions for Local Group dSph’s agree well with previous calculations and observations. Our MOND calculated dispersion profiles are compared with the observations of Walker et al. for Milky Way dSph’s, and we present calculated dispersion profiles for a selection of Andromeda dSph’s.
Chemical Abundances of M-Dwarfs from the Apogee Survey. I. The Exoplanet Hosting Stars Kepler-138 and Kepler-186
Authors: Souto D. , Cunha K. , García-Hernández D. A. , Zamora O. , Prieto C. Allende , Smith V. V. , Mahadevan S. , Blake C. , Johnson J. A. , Jönsson H. , Pinsonneault M. , Holtzman J. , Majewski S. R. , Shetrone M. , Teske J. , Nidever D. , Schiavon R. , Sobeck J. , Pérez A. E. García , Chew Y. Gómez Maqueo , Stassun K. 
Published: January 2017

Abstract
We report the first detailed chemical abundance analysis of the exoplanet-hosting M-dwarf stars Kepler-138 and Kepler-186 from the analysis of high-resolution (R ∼ 22,500) H-band spectra from the SDSS-IV–APOGEE survey. Chemical abundances of 13 elements—C, O, Na, Mg, Al, Si, K, Ca, Ti, V, Cr, Mn, and Fe—are extracted from the APOGEE spectra of these early M-dwarfs via spectrum syntheses computed with an improved line list that takes into account H2O and FeH lines. This paper demonstrates that APOGEE spectra can be analyzed to determine detailed chemical compositions of M-dwarfs. Both exoplanet-hosting M-dwarfs display modest sub-solar metallicities: [Fe/H]Kepler-138 = −0.09 ± 0.09 dex and [Fe/H]Kepler-186 = −0.08 ± 0.10 dex. The measured metallicities resulting from this high-resolution analysis are found to be higher by ∼0.1–0.2 dex than previous estimates from lower-resolution spectra. The C/O ratios obtained for the two planet-hosting stars are near-solar, with values of 0.55 ± 0.10 for Kepler-138 and 0.52 ± 0.12 for Kepler-186. Kepler-186 exhibits a marginally enhanced [Si/Fe] ratio.