bluuebunny/crossref_metadata_2025_split huggingface dataset:
Dwarf Galaxy Discoveries from the KMTNet Supernova Program. I. The NGC 2784 Galaxy Group*
Authors: Park Hong Soo , Moon Dae-Sik , Zaritsky Dennis , Pak Mina , Lee Jae-Joon , Kim Sang Chul , Kim Dong-Jin , Cha Sang-Mok 
Published: October 2017

Abstract
We present BVI surface photometry of 31 dwarf galaxy candidates discovered in a deep image stack from the KMTNet Supernova Program of ∼30 square degrees centered on the nearby NGC 2784 galaxy group. Our final images have a 3σ surface brightness detection limit of

mag arcsec−2. The faintest central surface brightness that we measure is

mag arcsec−2. If these candidates are at the distance of NGC 2784, then they have absolute magnitudes greater than

mag and effective radii larger than 170 pc. Their radial number density decreases exponentially with distance from the center of NGC 2784 until it flattens beyond a radius of 0.5 Mpc. We interpret the baseline density level to represent the background contamination and estimate that 22 of the 31 new candidates are dwarf members of the group. The candidate’s average color,

, and Sérsic structural parameters are consistent with those parameters for the dwarf populations of other groups. We find that the central population of dwarfs is redder and brighter than the rest of the population. The measured faint-end slope of the luminosity function,

, is steeper than that of the Local Group, but consistent with published results for other groups. Such comparisons are complicated by systematic differences among different studies, but will be simpler when the KMTNet survey, which will provide homogenous data for 15–20 groups, is completed.
Hydrogen-poor Superluminous Supernovae with Late-time Hα Emission: Three Events From the Intermediate Palomar Transient Factory
Authors: Yan Lin , Lunnan R. , Perley D. A. , Gal-Yam A. , Yaron O. , Roy R. , Quimby R. , Sollerman J. , Fremling C. , Leloudas G. , Cenko S. B. , Vreeswijk P. , Graham M. L. , Howell D. A. , Cia A. De , Ofek E. O. , Nugent P. , Kulkarni S. R. , Hosseinzadeh G. , Masci F. , McCully C. , Rebbapragada U. D. , Woźniak P. 
Published: October 2017

Abstract
We present observations of two new hydrogen-poor superluminous supernovae (SLSN-I), iPTF15esb and iPTF16bad, showing late-time Hα emission with line luminosities of

erg s−1 and velocity widths of (4000–6000) km s−1. Including the previously published iPTF13ehe, this makes up a total of three such events to date. iPTF13ehe is one of the most luminous and the slowest evolving SLSNe-I, whereas the other two are less luminous and fast decliners. We interpret this as a result of the ejecta running into a neutral H-shell located at a radius of ∼1016 cm. This implies that violent mass loss must have occurred several decades before the supernova explosion. Such a short time interval suggests that eruptive mass loss could be common shortly before core collapse, and more importantly helium is unlikely to be completely stripped off the progenitor and could be present in the ejecta. It is a mystery why helium features are not detected, even though nonthermal energy sources, capable of ionizing He, may exist as suggested by the O ii absorption series in the early-time spectra. Our late-time spectra (+240 days) appear to have intrinsically lower [O i] 6300 Å luminosities than that of SN2015bn and SN2007bi, which is possibly an indication of less oxygen (<10 M
⊙). The blueshifted Hα emission relative to the hosts for all three events may be in tension with the binary model proposed for iPTF13ehe. Finally, iPTF15esb has a peculiar light curve (LC) with three peaks separated from one another by ∼22 days. The LC undulation is stronger in bluer bands. One possible explanation is ejecta-circumstellar medium interaction.
The Transition of a Type IIL Supernova into a Supernova Remnant: Late-time Observations of SN 2013by
Authors: Black C. S. , Milisavljevic D. , Margutti R. , Fesen R. A. , Patnaude D. , Parker S. 
Published: October 2017

Abstract
We present early-time Swift and Chandra X-ray data along with late-time optical and near-infrared observations of SN 2013by, a Type IIL supernova (SN) that occurred in the nearby spiral galaxy ESO 138−G10 (D ∼ 14.8 Mpc). Optical and NIR photometry and spectroscopy follow the late-time evolution of the SN from days +89 to +457 post maximum brightness. The optical spectra and X-ray light curves are consistent with the picture of an SN having prolonged interaction with circumstellar material (CSM) that accelerates the transition from SN to supernova remnant (SNR). Specifically, we find SN 2013by’s Hα profile exhibits significant broadening (∼10,000 km s−1) on day +457, the likely consequence of high-velocity, H-rich material being excited by a reverse shock. A relatively flat X-ray light curve is observed that cannot be modeled using Inverse Compton scattering processes alone, but requires an additional energy source most likely originating from the SN-CSM interaction. In addition, we see the first overtone of CO emission near 2.3 μm on day +152, signaling the formation of molecules and dust in the SN ejecta and is the first time CO has been detected in a Type IIL SN. We compare SN 2013by with Type IIP SNe, whose spectra show the rarely observed SN-to-SNR transition in varying degrees and conclude that Type IIL SNe may enter the remnant phase at earlier epochs than their Type IIP counterparts.
Timing Analysis of V404 Cyg during Its Brightest Outburst with INTEGRAL/SPI
Authors: Rodi J. , Jourdain E. , Roques J. P. 
Published: October 2017

Abstract
The outburst of V404 Cyg during the summer of 2015 reached unparalleled intensities at X-ray and soft gamma-ray energies with fluxes

Crab in the 20–50 keV energy band. To date, studies in the hard X-ray/soft gamma-ray energy domain have focused primarily on the energy spectra. In this work, a timing analysis has been performed with INTEGRAL/SPI data in the 20–300 keV energy range for INTEGRAL revolution 1557, which corresponds to the brightest flare of V404 Cyg (on 2015 June 26). The power spectra are fit with broken power-law and multi-Lorentzian models and compared with previously reported results of V404 Cyg flaring activity from 1989 and 2015. Also, we took advantage of the good signal-to-noise ratio obtained above 70 keV to quantify the timing/fast-variability properties of the source as a function of energy. We then point out similarities of V404 Cyg with the black hole transient V4641 Sgr. Like V4641 Sgr, we found that the power spectra of V404 Cyg during high flux periods did not possess the expected flat-top feature typically seen in a hard spectral state. Interpretations are proposed in the framework of the fluctuating-propagation model to explain the observed properties.
Astrophysical Implications of a New Dynamical Mass for the Nearby White Dwarf 40 Eridani B
Authors: Bond Howard E. , Bergeron P. , Bédard A. 
Published: October 2017

Abstract
The bright, nearby DA-type white dwarf (WD) 40 Eridani B is orbited by the M dwarf 40 Eri C, allowing determination of the WD’s mass. Until recently, however, the mass depended on orbital elements determined four decades ago, and that mass was so low that it created several astrophysical puzzles. Using new astrometric measurements, the binary-star group at the U.S. Naval Observatory has revised the dynamical mass upward, to 0.573 ± 0.018 M
☉. In this paper, we use model-atmosphere analysis to update other parameters of the WD, including effective temperature, surface gravity, radius, and luminosity. We then compare these results with WD interior models. Within the observational uncertainties, theoretical cooling tracks for CO-core WDs of its measured mass are consistent with the position of 40 Eri B in the H-R diagram; equivalently, the theoretical mass–radius relation (MRR) is consistent with the star’s location in the mass–radius plane. This consistency is, however, achieved only if we assume a “thin” outer hydrogen layer, with q
H = M
H/M
WD ≃ 10−10. We discuss other evidence that a significant fraction of DA WDs have such thin H layers, in spite of the expectation from canonical stellar-evolution theory of “thick” H layers with q
H ≃ 10−4. The cooling age of 40 Eri B is ∼122 Myr, and its total age is ∼1.8 Gyr. We present the MRRs for 40 Eri B and three other nearby WDs in visual binaries with precise mass determinations, and show that the agreement of current theory with observations is excellent in all cases.
Sensitivity to Thermonuclear Reaction Rates in Modeling the Abundance Anomalies of NGC 2419
Authors: Dermigny J. R. , Iliadis C. 
Published: October 2017

Abstract
Abundance anomalies in globular clusters provide strong evidence for multiple stellar populations within each cluster. These populations are usually interpreted as distinct generations, with the currently observed second-generation stars having formed in part from the ejecta of massive, first-generation “polluter” stars, giving rise to the anomalous abundance patterns. The precise nature of the polluters and their enrichment mechanism are still unclear. Even so, the chemical abundances measured in second-generation stars within the globular cluster NGC 2419 provide insight into this puzzling process. Previous work used Monte Carlo nuclear reaction network calculations to constrain the temperature–density conditions that could reproduce the observed abundances, thereby placing robust limits on the origins of the polluter material. The effect of individual reaction rates on these conditions has not been studied, however. Thus, we perform an exhaustive sensitivity study on the nuclear physics input to determine which reactions have the greatest impact on these predictions. We find that the

Si(p,γ)

P,

Ar(p,γ)

K,

Ar(p,γ)

K, and

K(p,γ)

Ca reactions are all critical in determining the temperature–density conditions, and ultimately, the origins of the polluter material. We conclude with recommendations for future experiments.
Fragmentation of a Filamentary Cloud Permeated by a Perpendicular Magnetic Field
Authors: Hanawa Tomoyuki , Kudoh Takahiro , Tomisaka Kohji 
Published: October 2017

Abstract
We examine the linear stability of an isothermal filamentary cloud permeated by a perpendicular magnetic field. Our model cloud is assumed to be supported by gas pressure against self-gravity in the unperturbed state. For simplicity, the density distribution is assumed to be symmetric around the axis. Also for simplicity, the initial magnetic field is assumed to be uniform, and turbulence is not taken into account. The perturbation equation is formulated to be an eigenvalue problem. The growth rate is obtained as a function of the wavenumber for fragmentation along the axis and the magnetic field strength. The growth rate depends critically on the outer boundary. If the displacement vanishes in regions very far from the cloud axis (fixed boundary), cloud fragmentation is suppressed by a moderate magnetic field, which means the plasma beta is below 1.67 on the cloud axis. If the displacement is constant along the magnetic field in regions very far from the cloud, the cloud is unstable even when the magnetic field is infinitely strong. The cloud is deformed by circulation in the plane perpendicular to the magnetic field. The unstable mode is not likely to induce dynamical collapse, since it is excited even when the whole cloud is magnetically subcritical. For both boundary conditions, the magnetic field increases the wavelength of the most unstable mode. We find that the magnetic force suppresses compression perpendicular to the magnetic field especially in regions of low density.
Partial Accretion in the Propeller Stage of Low-mass X-Ray Binary Aql X–1
Authors: Güngör C. , Ekşi˙ K. Y. , Göğüş E. , Güver T. 
Published: October 2017

Abstract
Aql X–1 is one of the most prolific low-mass X-ray binary transients (LMXBTs) showing outbursts almost annually. We present the results of our spectral analyses of Rossi X-Ray Timing Explorer/proportional counter-array observations of the 2000 and 2011 outbursts. We investigate the spectral changes related to the changing disk-magnetosphere interaction modes of Aql X–1. The X-ray light curves of the outbursts of LMXBTs typically show phases of fast rise and exponential decay. The decay phase shows a “knee” where the flux goes from the slow-decay to the rapid-decay stage. We assume that the rapid decay corresponds to a weak propeller stage at which a fraction of the inflowing matter in the disk accretes onto the star. We introduce a novel method for inferring, from the light curve, the fraction of the inflowing matter in the disk that accretes onto the neutron star depending on the fastness parameter. We determine the fastness parameter range within which the transition from the accretion to the partial propeller stage is realized. This fastness parameter range is a measure of the scale height of the disk in units of the inner disk radius. We applied the method to a sample of outbursts of Aql X–1 with different maximum flux and duration times. We show that different outbursts with different maximum luminosity and duration follow a similar path in the parameter space of accreted/inflowing mass flux fraction versus fastness parameter.
A New Fokker–Planck Approach for the Relaxation-driven Evolution of Galactic Nuclei
Authors: Vasiliev Eugene 
Published: October 2017

Abstract
We present an approach for simulating the collisional evolution of spherical isotropic stellar systems based on the one-dimensional Fokker–Planck equation. A novel aspect is that we use the phase volume as the argument of the distribution function instead of the traditionally used energy, which facilitates the solution. The publicly available code PhaseFlow implements a high-accuracy finite-element method for the Fokker–Planck equation, and can handle multiple-component systems, optionally with the central black hole and taking into account loss-cone effects and star formation. We discuss the energy balance in the general setting, and in application to the Bahcall–Wolf cusp around a central black hole, for which we derive a perturbative solution. We stress that the cusp is not a steady-state structure, but rather evolves in amplitude while retaining an approximately

density profile. Finally, we apply the method to the nuclear star cluster of the milky Way, and illustrate a possible evolutionary scenario in which a two-component system of lighter main-sequence stars and stellar-mass black holes develops a Bahcall–Wolf cusp in the heavier component and a weaker

cusp in the lighter, visible component, over the period of several Gyr. The present-day density profile is consistent with the recently detected mild cusp inside the central parsec, and is weakly sensitive to initial conditions.
Dépendance, refus de la différence
Authors: Rezende Cardoso Marta 
Published: October 2017

La dépendance psychique pendant l’adolescence est ici traitée sous deux angles : la relation Moi/autre et la polarité intériorité/extériorité. Dans ce passage de l’enfance à l’âge adulte, l’expérience de séparation de l’objet est le versant central de la question de la dépendance, particulièrement dans les addictions. Nous voulons montrer le caractère paradoxal du processus de séparation à l’adolescence, son noyau primaire et œdipien dans l’imbrication desquels se situe le fondement de ses impasses.
Entomological citizen science in Canada
Authors: Acorn John H. 
Published: October 2017

AbstractCitizen science involves voluntary participation in the scientific process, typically by gathering data in order to monitor some aspect of the natural world. Entomological citizen science, as an extension of traditional amateur entomology, is an active field in Canada, with online databases such as eButterfly and BugGuide attracting both contributors and database users. As well, traditional amateur entomology continues to be important in Canada, as do short-term insect-themed educational events, the involvement of amateurs in entomological societies, and online crowdsourcing initiatives. Success of citizen science projects can be measured in many ways. In terms of published papers that analyse trends in citizen science data, Canadian projects have only begun to deliver. More valuable are particular records that improve our knowledge of geographic ranges and phenology. In terms of the endurance of particular projects, and the willingness of volunteers to participate, citizen science entomology in Canada is clearly a success. However, quality control of citizen science data remains an issue for some projects. As well, challenges remain with respect to balancing the goals of researchers, participants, and supporting institutions.
Aryl Hydrocarbon Receptor Activation Suppresses EBF1 and PAX5 and Impairs Human B Lymphopoiesis
Authors: Li Jinpeng , Bhattacharya Sudin , Zhou Jiajun , Phadnis-Moghe Ashwini S. , Crawford Robert B. , Kaminski Norbert E. 
Published: October 2017

Abstract
Aryl hydrocarbon receptor (AHR) is a ligand-activated transcription factor that mediates biological responses to endogenous and environmental chemical cues. Increasing evidence shows that the AHR plays physiological roles in regulating development, homeostasis, and function of a variety of cell lineages in the immune system. However, the role of AHR in human B cell development has not been investigated. Toward this end, an in vitro feeder-free human B cell developmental model system was employed using human cord blood CD34+ hematopoietic stem/progenitor cells. Using this model, we found that AHR activation by the high-affinity ligand 2,3,7,8-tetrachlorodibenzo-p-dioxin significantly suppressed the generation of early B cells and pro-B cells from hematopoietic stem/progenitor cells, indicating the impairment of B cell lineage specification and commitment. Addition of an AHR antagonist reversed 2,3,7,8-tetrachlorodibenzo-p-dioxin–elicited suppression of early B and pro-B cells, suggesting a role of AHR in regulating B lymphopoiesis. Gene expression analysis revealed a significant decrease in the messenger RNA level of early B cell factor 1 (EBF1) and paired box 5, two critical transcription factors directing B cell lineage specification and commitment. Additionally, binding of the ligand-activated AHR to the putative dioxin response elements in the EBF1 promoter was demonstrated by EMSAs and chromatin immunoprecipitation analysis, suggesting transcriptional regulation of EBF1 by AHR. Taken together, this study demonstrates a role for the AHR in regulating human B cell development, and it suggests that transcriptional alterations of EBF1 by the AHR are involved in the underlying mechanism.
Rab27-Dependent Exosome Production Inhibits Chronic Inflammation and Enables Acute Responses to Inflammatory Stimuli
Authors: Alexander Margaret , Ramstead Andrew G. , Bauer Kaylyn M. , Lee Soh-Hyun , Runtsch Marah C. , Wallace Jared , Huffaker Thomas B. , Larsen Dane K. , Tolmachova Tanya , Seabra Miguel C. , Round June L. , Ward Diane M. , O’Connell Ryan M. 
Published: October 2017

Abstract
Extracellular vesicles, including exosomes, have recently been implicated as novel mediators of immune cell communication in mammals. However, roles for endogenously produced exosomes in regulating immune cell functions in vivo are just beginning to be identified. In this article, we demonstrate that Rab27a and Rab27b double-knockout (Rab27DKO) mice that are deficient in exosome secretion have a chronic, low-grade inflammatory phenotype characterized by elevated inflammatory cytokines and myeloproliferation. Upon further investigation, we found that some of these phenotypes could be complemented by wild-type (WT) hematopoietic cells or administration of exosomes produced by GM-CSF–expanded bone marrow cells. In addition, chronically inflamed Rab27DKO mice had a blunted response to bacterial LPS, resembling endotoxin tolerance. This defect was rescued by bone marrow exosomes from WT, but not miR-155−/−, cells, suggesting that uptake of miR-155–containing exosomes is important for a proper LPS response. Further, we found that SHIP1 and IRAK-M, direct targets of miR-155 that are known negative regulators of the LPS response, were elevated in Rab27DKO mice and decreased after treatment with WT, but not miR-155−/−, exosomes. Together, our study finds that Rab27-dependent exosome production contributes to homeostasis within the hematopoietic system and appropriate responsiveness to inflammatory stimuli.
Does Chicago Classification address Symptom Correlation with High-resolution Esophageal Manometry?
Authors: Srinivas Melpakkam , Bawane Piyush 
Published: October 2017

ABSTRACT

Aim
To assess the correlation of symptoms with findings on esophageal high-resolution manometry (HRM) in Indian patients.

Materials and methods
Prospective data collection of all patients undergoing esophageal manometry was done at two centers in India—Indore and Chennai—over a period of 18 months. Symptom profile of the study group was divided into four: Motor dysphagia, noncardiac chest pain (NCCP), gastroesophageal reflux (GER), and esophageal belchers. The symptoms were correlated with manometric findings.

Results
Of the study group (154), 35.71% patients had a normal study, while major and minor peristaltic disorders were noted in 31.16 and 33.76% respectively. In patients with symptoms of dysphagia, achalasia cardia was the commonest cause (45.1%), followed by ineffective esophageal motility (IEM) (22.53%) and normal study (19.71%). In patients with NCCP, normal peristalsis (50%) and ineffective motility (31.25%) formed the major diagnosis. Of the 56 patients with GER symptoms, 26 (46.4%) had normal manometry. An equal number had ineffective motility. Of the 11 esophageal belchers, 7 (63.6%) of these had a normal study and 3 had major motility disorder. Dysphagia was the only symptom to have a high likelihood ratio and positive predictive value to pick up major motility disorder.

Conclusion
Dysphagia correlates with high chance to pick up a major peristaltic abnormality in motor dysphagia. The role of manometry in other symptoms in Indian setting needs to be ascertained by larger studies.

Clinical significance
The present study highlights lack of symptom correlation with manometry findings in Indian patients.

How to cite this article
Jain M, Srinivas M, Bawane P, Venkataraman J. Does Chicago Classification address Symptom Correlation with High-resolution Esophageal Manometry? Euroasian J Hepato-Gastroenterol 2017;7(2):122-125.