bluuebunny/crossref_metadata_2025_split huggingface dataset:
THE SLOAN DIGITAL SKY SURVEY REVERBERATION MAPPING PROJECT: BIASES IN z > 1.46 REDSHIFTS DUE TO QUASAR DIVERSITY
Authors: Denney K. D. , Horne Keith , Brandt W. N. , Grier C. J. , Ho Luis C. , Peterson B. M. , Trump J. R. , Ge J. 
Published: December 2016

ABSTRACT
We use the coadded spectra of 32 epochs of Sloan Digital Sky Survey (SDSS) Reverberation Mapping Project observations of 482 quasars with z > 1.46 to highlight systematic biases in the SDSS- and Baryon Oscillation Spectroscopic Survey (BOSS)-pipeline redshifts due to the natural diversity of quasar properties. We investigate the characteristics of this bias by comparing the BOSS-pipeline redshifts to an estimate from the centroid of He ii
λ1640. He ii has a low equivalent width but is often well-defined in high-S/N spectra, does not suffer from self-absorption, and has a narrow component which, when present (the case for about half of our sources), produces a redshift estimate that, on average, is consistent with that determined from [O ii] to within the He ii and [O ii] centroid measurement uncertainties. The large redshift differences of ∼1000 km s−1, on average, between the BOSS-pipeline and He ii-centroid redshifts, suggest there are significant biases in a portion of BOSS quasar redshift measurements. Adopting the He ii-based redshifts shows that C iv does not exhibit a ubiquitous blueshift for all quasars, given the precision probed by our measurements. Instead, we find a distribution of C iv-centroid blueshifts across our sample, with a dynamic range that (i) is wider than that previously reported for this line, and (ii) spans C iv centroids from those consistent with the systemic redshift to those with significant blueshifts of thousands of kilometers per second. These results have significant implications for measurement and use of high-redshift quasar properties and redshifts, and studies based thereon.
GENERALIZED MULTI-POLYTROPIC RANKINE–HUGONIOT RELATIONS AND THE ENTROPY CONDITION
Authors: Scherer Klaus , Fichtner Horst , Fahr Hans Jörg , Röken Christian , Kleimann Jens 
Published: December 2016

ABSTRACT
The study aims at a derivation of generalized Rankine–Hugoniot relations, especially that for the entropy, for the case of different upstream/downstream polytropic indices and their implications. We discuss the solar/stellar wind interaction with the interstellar medium for different polytropic indices. Moreover, we concentrate on the situation when the polytropic index changes across hydrodynamical shocks. First, we use a numerical monofluid approach with a constant polytropic index in the entire integration region to show the influence of the polytropic index on the thickness of the helio-/astrosheath and on the compression ratio. Second, the Rankine–Hugoniot relations for a polytropic index changing across a shock are derived analytically, particularly including a new form of the entropy condition. In application to the/an helio-/astrosphere, we find that the size of the helio-/astrosheath as a function of the polytropic index decreases in a monofluid model for indices less than

and increases for higher ones and vice versa for the compression ratio. Furthermore, we demonstrate that changing polytropic indices across a shock are physically allowed only for sufficiently high Mach numbers and that in the hypersonic limit the compression ratio depends only on the downstream polytropic index, while the ratios of the temperature and pressure as well as the entropy difference depend on both the upstream and downstream polytropic indices.
ON THE FORMATION OF MOLECULAR CLUMPS IN QSO OUTFLOWS
Authors: Ferrara A. , Scannapieco E. 
Published: December 2016

ABSTRACT
We study the origin of the cold molecular clumps in quasar outflows, recently detected in CO and HCN emission. We first describe the physical properties of such radiation-driven outflows and show that a transition from a momentum- to an energy-driven flow must occur at a radial distance of

. During this transition, the shell of swept-up material fragments due to Rayleigh–Taylor instabilities, but these clumps contain little mass and are likely to be rapidly ablated by the hot gas in which they are immersed. We then explore an alternative scenario in which clumps form from thermal instabilities at

, possibly containing enough dust to catalyze molecule formation. We investigate this process with 3D two-fluid (gas+dust) numerical simulations of a kpc3 patch of the outflow, including atomic and dust cooling, thermal conduction, dust sputtering, and photoionization from the QSO radiation field. In all cases, dust grains are rapidly destroyed in

years; and while some cold clumps form at later times, they are present only as transient features, which disappear as cooling becomes more widespread. In fact, we only find a stable two-phase medium with dense clumps if we artificially enhance the QSO radiation field by a factor of 100. This result, together with the complete destruction of dust grains, renders the interpretation of molecular outflows a very challenging problem.
CONSTRAINT ON THE INFLOW/OUTFLOW RATES IN STAR-FORMING GALAXIES AT z ∼ 1.4 FROM MOLECULAR GAS OBSERVATIONS
Authors: Seko Akifumi , Ohta Kouji , Yabe Kiyoto , Hatsukade Bunyo , Akiyama Masayuki , Tamura Naoyuki , Iwamuro Fumihide , Dalton Gavin 
Published: December 2016

ABSTRACT
We constrain the rate of gas inflow into and outflow from a main-sequence star-forming galaxy at

by fitting a simple analytic model for the chemical evolution in a galaxy to the observational data of the stellar mass, metallicity, and molecular gas mass fraction. The molecular gas mass is derived from CO observations with a metallicity-dependent CO-to-H2 conversion factor, and the gas metallicity is derived from the Hα and [N ii]λ 6584 emission line ratio. Using a stacking analysis of CO integrated intensity maps and the emission lines of Hα and [N ii], the relation between stellar mass, metallicity, and gas mass fraction is derived. We constrain the inflow and outflow rates with least-chi-square fitting of a simple analytic chemical evolution model to the observational data. The best-fit inflow and outflow rates are ∼1.7 and ∼0.4 in units of star formation rate (SFR), respectively. The inflow rate is roughly comparable to the sum of the SFR and outflow rate, which supports the equilibrium model for galaxy evolution; i.e., all inflow gas is consumed by star formation and outflow.
ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: THE INFRARED EXCESS OF UV-SELECTED z = 2–10 GALAXIES AS A FUNCTION OF UV-CONTINUUM SLOPE AND STELLAR MASS
Authors: J. Bouwens Rychard , Aravena Manuel , Decarli Roberto , Walter Fabian , da Cunha Elisabete , Labbé Ivo , E. Bauer Franz , Bertoldi Frank , Carilli Chris , Chapman Scott , Daddi Emanuele , Hodge Jacqueline , J. Ivison Rob , Karim Alex , Le Fevre Olivier , Magnelli Benjamin , Ota Kazuaki , Riechers Dominik , R. Smail Ian , van der Werf Paul , Weiss Axel , Cox Pierre , Elbaz David , Gonzalez-Lopez Jorge , Infante Leopoldo , Oesch Pascal , Wagg Jeff , Wilkins Steve 
Published: December 2016

ABSTRACT
We make use of deep 1.2 mm continuum observations (12.7 μJy beam−1 rms) of a 1 arcmin2 region in the Hubble Ultra Deep Field to probe dust-enshrouded star formation from 330 Lyman-break galaxies spanning the redshift range z = 2–10 (to ∼2–3 M
⊙ yr−1 at 1σ over the entire range). Given the depth and area of ASPECS, we would expect to tentatively detect 35 galaxies, extrapolating the Meurer z ∼ 0 IRX–β relation to z ≥ 2 (assuming dust temperature T

d
∼ 35 K). However, only six tentative detections are found at z ≳ 2 in ASPECS, with just three at >3σ. Subdividing our z = 2–10 galaxy samples according to stellar mass, UV luminosity, and UV-continuum slope and stacking the results, we find a significant detection only in the most massive (>109.75
M
⊙) subsample, with an infrared excess (IRX = L
IR/L
UV) consistent with previous z ∼ 2 results. However, the infrared excess we measure from our large selection of sub-L
∗ (<109.75
M
⊙) galaxies is

± 0.34 (bootstrap and formal uncertainties) and

± 0.18 at z = 2–3 and z = 4–10, respectively, lying below even an IRX–β relation for the Small Magellanic Cloud (95% confidence). These results demonstrate the relevance of stellar mass for predicting the IR luminosity of z ≳ 2 galaxies. We find that the evolution of the IRX–stellar mass relationship depends on the evolution of the dust temperature. If the dust temperature increases monotonically with redshift (

) such that T

d
∼ 44–50 K at z ≥ 4, current results are suggestive of little evolution in this relationship to z ∼ 6. We use these results to revisit recent estimates of the z ≥ 3 star formation rate density.
THE ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: IMPLICATIONS FOR SPECTRAL LINE INTENSITY MAPPING AT MILLIMETER WAVELENGTHS AND CMB SPECTRAL DISTORTIONS
Authors: Carilli C. L. , Chluba J. , Decarli R. , Walter F. , Aravena M. , Wagg J. , Popping G. , Cortes P. , Hodge J. , Weiss A. , Bertoldi F. , Riechers D. 
Published: December 2016

ABSTRACT
We present direct estimates of the mean sky brightness temperature in observing bands around 99 and 242 GHz due to line emission from distant galaxies. These values are calculated from the summed line emission observed in a blind, deep survey for spectral line emission from high redshift galaxies using ALMA (the ALMA spectral deep field observations “ASPECS” survey). In the 99 GHz band, the mean brightness will be dominated by rotational transitions of CO from intermediate and high redshift galaxies. In the 242 GHz band, the emission could be a combination of higher order CO lines, and possibly [C ii] 158 μm line emission from very high redshift galaxies (z ∼ 6–7). The mean line surface brightness is a quantity that is relevant to measurements of spectral distortions of the cosmic microwave background, and as a potential tool for studying large-scale structures in the early universe using intensity mapping. While the cosmic volume and the number of detections are admittedly small, this pilot survey provides a direct measure of the mean line surface brightness, independent of conversion factors, excitation, or other galaxy formation model assumptions. The mean surface brightness in the 99 GHZ band is: T

B
= 0.94 ± 0.09 μK. In the 242 GHz band, the mean brightness is: T

B
= 0.55 ± 0.033 μK. These should be interpreted as lower limits on the average sky signal, since we only include lines detected individually in the blind survey, while in a low resolution intensity mapping experiment, there will also be the summed contribution from lower luminosity galaxies that cannot be detected individually in the current blind survey.
PHOTOMETRIC AND ASTROMETRIC VAGARIES OF THE ENIGMA STAR KIC 8462852
Authors: Makarov Valeri V. , Goldin Alexey 
Published: December 2016

ABSTRACT
We apply a principal component analysis (PCA)-based pre-whitening method to the entire collection of main Kepler mission long-cadence data for KIC 8462852 spanning four years. This technique removes the correlated variations of instrumental origin in both the detected light curves and astrometry, resolving intrinsic changes in flux and image position of less than 100 ppm and 1 mas, respectively. Beside the major dips in the light curve during mission quarters 8 and 16, when the flux dropped by up to 20%, we confirm multiple smaller dips across the time span of observation with amplitudes ranging from 0.1% to 7%. A variation of flux with a period of 0.88 day and a half-amplitude of approximately 90 ppm is confirmed in the PCA-cleaned data. We find that the phase of the wave is steady over a 15 month interval. We confidently detect a weak variability-induced motion (VIM) effect in the cleaned astrometric trajectories, when the moment-based centroids shift synchronously with the flux dips by up to 0.0008 pixels on the detector. The inconsistent magnitude and direction of VIM effects within the same quarter point at more than one source of photometric variability in the blended image. The 0.88 day periodicity comes from a different source, not from the target star KIC 8462852. We discuss a possible interpretation of the bizarre properties of the source as a swarm of interstellar junk (comets and planetoids) crossing the line of sight to the star and its optical companions at approximately 7 mas yr−1.
THE UNIVERSAL “HEARTBEAT” OSCILLATIONS IN BLACK HOLE SYSTEMS ACROSS THE MASS-SCALE
Authors: Wu Qingwen , Czerny Bozena , Grzedzielski Mikolaj , Janiuk Agnieszka , Gu Wei-Min , Dong Ai-jun , Cao Xiao-Feng , You Bei , Yan Zhen , Sun Mou-Yuan 
Published: December 2016

ABSTRACT
The hyperluminous X-ray source (HLX-1, peak X-ray luminosity

) near the spiral galaxy ESO 243-49, which underwent recurrent outbursts within a period of ∼400 days, is possibly the best candidate for an intermediate mass black hole (IMBH). The physical reason for this quasiperiodic variability is still unclear. We explore the possibility of radiation-pressure instability in the accretion disk by modeling the light curve of HLX-1, and find that it can roughly reproduce the duration, period, and amplitude of the recurrent outbursts in HLX-1 with an IMBH of

. Our result provides a possible mechanism to explain the recurrent outbursts in HLX-1. We further find a universal correlation between the outburst duration and the bolometric luminosity for the black hole (BH) sources with a very broad mass range (e.g., X-ray binaries, HLX-1, and active galactic nuclei), which is roughly consistent with the prediction of radiation-pressure instability of the accretion disk. These results imply that “heartbeat” oscillations triggered by radiation-pressure instability may appear in different-scale BH systems.
IDENTIFICATION OF NEODYMIUM IN THE APOGEE H-BAND SPECTRA
Authors: Hasselquist Sten , Shetrone Matthew , Cunha Katia , Smith Verne V. , Holtzman Jon , Lawler J. E. , Prieto Carlos Allende , Beers Timothy C. , Chojnowski Drew , Fernández-Trincado J. G. , García-Hernández D. A. , Hearty Fred R. , Majewski Steven R. , Pereira C. B. , Placco Vinicius M. , Villanova Sandro , Zamora Olga 
Published: December 2016

ABSTRACT
We present the detection of 10 lines of singly ionized neodymium (Nd ii, Z = 60) in H-band spectra using observations from the SDSS-III Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey. These lines were detected in a metal-poor ([Fe/H] ∼ −1.5), neutron-capture element-enhanced star recently discovered in the APOGEE sample. Using an optical high-resolution spectrum, we derive a Nd abundance for this star using Nd ii lines with precise, laboratory-derived gf values. This optical abundance is used to derive log(gf) values for the H-band lines. We use these lines to rederive Nd ii abundances for two more metal-rich, s-process enhanced stars observed by APOGEE and find that these lines yield consistent Nd ii abundances, confirming the Nd enhancement of these stars. We explore the region of parameter space in the APOGEE sample over which these lines can be used to measure Nd ii abundances. We find that Nd abundances can be reliably derived for ∼18% of the red giants observed by APOGEE. This will result in ∼50,000 Milky Way stars with Nd ii abundances following the conclusion of APOGEE-2, allowing for studies of neutron-capture element abundance distributions across the entire Milky Way.
THE EFFECT OF GRAVITATION ON THE POLARIZATION STATE OF A LIGHT RAY
Authors: Ghosh Tanay , Sen A. K. 
Published: December 2016

ABSTRACT
In the present work, detailed calculations have been carried out on the rotation of the polarization vector of an electromagnetic wave due to the presence of a gravitational field of a rotating body. This has been done using the general expression of Maxwell’s equation in curved spacetime. Considering the far-field approximation (i.e., the impact parameter is greater than the Schwarzschild radius and rotation parameter), the amount of rotation of the polarization vector as a function of impact parameter has been obtained for a rotating body (considering Kerr geometry). The present work shows that the rotation of the polarization vector cannot be observed in the case of Schwarzschild geometry. This work also calculates the rotational effect when considering prograde and retrograde orbits for the light ray. Although the present work demonstrates the effect of rotation of the polarization vector, it confirms that there would be no net polarization of an electromagnetic wave due to the curved spacetime geometry in a Kerr field.
STAR FORMATION AROUND MID-INFRARED BUBBLE N37: EVIDENCE OF CLOUD–CLOUD COLLISION
Authors: Baug T. , Dewangan L. K. , Ojha D. K. , Ninan J. P. 
Published: December 2016

ABSTRACT
We have performed a multi-wavelength analysis of a mid-infrared (MIR) bubble N37 and its surrounding environment. The selected 15′ × 15′ area around the bubble contains two molecular clouds (N37 cloud;

37–43 km s−1, and C25.29+0.31;

43–48 km s−1) along the line of sight. A total of seven OB stars are identified toward the bubble N37 using photometric criteria, and two of them are spectroscopically confirmed as O9V and B0V stars. The spectro-photometric distances of these two sources confirm their physical association with the bubble. The O9V star appears to be the primary ionizing source of the region, which is also in agreement with the desired Lyman continuum flux analysis estimated from the 20 cm data. The presence of the expanding H ii region is revealed in the N37 cloud, which could be responsible for the MIR bubble. Using the 13CO line data and photometric data, several cold molecular condensations as well as clusters of young stellar objects (YSOs) are identified in the N37 cloud, revealing ongoing star formation (SF) activities. However, the analysis of ages of YSOs and the dynamical age of the H ii region do not support the origin of SF due to the influence of OB stars. The position–velocity analysis of 13CO data reveals that two molecular clouds are interconnected by a bridge-like structure, favoring the onset of a cloud–cloud collision process. The SF activities (i.e., the formation of YSO clusters and OB stars) in the N37 cloud are possibly influenced by the cloud–cloud collision.
RADIO DIAGNOSTICS OF ELECTRON ACCELERATION SITES DURING THE ERUPTION OF A FLUX ROPE IN THE SOLAR CORONA
Authors: Carley Eoin P. , Vilmer Nicole , Gallagher Peter T. 
Published: December 2016

ABSTRACT
Electron acceleration in the solar corona is often associated with flares and the eruption of twisted magnetic structures known as flux ropes. However, the locations and mechanisms of such particle acceleration during the flare and eruption are still subject to much investigation. Observing the exact sites of particle acceleration can help confirm how the flare and eruption are initiated and how they evolve. Here we use the Atmospheric Imaging Assembly to analyze a flare and erupting flux rope on 2014 April 18, while observations from the Nançay Radio Astronomy Facility allow us to diagnose the sites of electron acceleration during the eruption. Our analysis shows evidence of a pre-formed flux rope that slowly rises and becomes destabilized at the time of a C-class flare, plasma jet, and the escape of ≳75 keV electrons from the rope center into the corona. As the eruption proceeds, continued acceleration of electrons with energies of ∼5 keV occurs above the flux rope for a period over 5 minutes. At the flare peak, one site of electron acceleration is located close to the flare site, while another is driven by the erupting flux rope into the corona at speeds of up to 400 km s−1. Energetic electrons then fill the erupting volume, eventually allowing the flux rope legs to be clearly imaged from radio sources at 150–445 MHz. Following the analysis of Joshi et al. (2015), we conclude that the sites of energetic electrons are consistent with flux rope eruption via a tether cutting or flux cancellation scenario inside a magnetic fan-spine structure. In total, our radio observations allow us to better understand the evolution of a flux rope eruption and its associated electron acceleration sites, from eruption initiation to propagation into the corona.
Les autismes : des pistes pour un abord pluriel ? Autisme et mélatonine
Authors: Gintz Christine 
Published: December 2016

Objectif : suggérer des pistes de recherche conjoignant les avancées sur l’autisme de différents champs théoriques.	Méthode : cet article propose une approche des autismes qui s’appuie sur les travaux de Sylvie Tordjman sur la mélatonine et les rythmes, pour envisager l’hypothèse d’une articulation du symbolique au corps portée par les rythmes circadiens. Cette mise en place se trouverait en défaut chez les personnes autistes en raison d’une faillite précoce de l’organisation du cycle de la mélatonine, ce qui pourrait avoir des effets sur le franchissement par l’enfant, du stade du miroir, ainsi que sur l’acquisition d’un langage qui soit noué au corps. Ces hypothèses ouvrent des pistes de recherche dans différentes disciplines comme la neurologie, la psychiatrie, la psychanalyse ou la génétique.
Comment penser le social et le politique dans la clinique
Authors: Puget Janine 
Published: December 2016

Cet article propose une manière de penser la subjectivité sociale et de repérer les effets de la réalité quotidienne dans le matériel clinique. On constate que certains concepts psychanalytiques classiques sont en crise et ont perdu la place centrale qu’ils occupaient, pour la raison majeure qu’ils doivent cohabiter avec de nouveaux concepts. Ceci a de nombreuses conséquences, comme d’avoir affaire à deux logiques superposées. L’une correspond strictement au monde intérieur du sujet singulier, et l’autre tient compte de la place qu’occupe le Lien, c’est-à-dire la relation entre deux ou plusieurs sujets.	Les concepts qui correspondent à chacune de ces deux logiques sont par exemple la représentation et la présentation, l’identification et l’imposition, le transfert et l’interférence, la transmission généalogique et la transmission inversée, l’interprétation et l’intervention.
Contre la violence : une bonne combativité
Authors: Duparc François 
Published: December 2016

Les guerres, la violence, ces maladies de l’humain, peuvent-elles être combattues par une « bonne combativité », s’interroge l’analyste qui se bat quotidiennement, à un niveau individuel, contre les états-limites de la folie, de la perversion et de la paranoïa ? L’analyse des idéologies, ces maladies de l’Idéal du Moi freudien, est une des voies à étudier pour rétablir un équilibre suffisamment bon entre Surmoi et Idéal du Moi, et ente les différents fantasmes originaires qui composent normalement l’Œdipe. Les sujets fragiles, adolescents ou immatures, comme on a pu le voir lors des attentats récents, sont très sensibles aux idéologies pathologiques de l’exclusion et de la solitude, et, face aux réseaux, à la séduction de la liberté à tout prix et de la consommation addictive de notre société. Ils tentent, par réaction, de s’enrôler dans des mouvements sectaires, intégristes ou politiques extrêmes, encouragés par les slogans, les rumeurs, ces formes de pensée pauvre de notre société.
Différents mouvements de transmission : transmission radioactive destructive – transmission radioactive créative
Authors: Gampel Yolanda 
Published: December 2016

La métaphore de la radioactivité, transformée en concept de « noyau radioactif », a surgi dans le contexte de travaux sur les effets des traumas sociaux, particulièrement ceux liés à la Shoah Empruntée au domaine de la physique nucléaire, la radioactivité aide à métaphoriser les effets monstrueux, inattendus et aberrants causés par la violence sociopolitique. À la lumière de deux témoignages, nous voyons que la radioactivité psychique peut être transformée d’une façon destructive ou créative. Cette transformation dépend, bien évidemment, du contexte et surtout des modalités de transmission d’une génération à l’autre.