bluuebunny/crossref_metadata_2025_split huggingface dataset:
ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: SURVEY DESCRIPTION
Authors: Walter Fabian , Decarli Roberto , Aravena Manuel , Carilli Chris , Bouwens Rychard , Cunha Elisabete da , Daddi Emanuele , Ivison R. J. , Riechers Dominik , Smail Ian , Swinbank Mark , Weiss Axel , Anguita Timo , Assef Roberto , Bacon Roland , Bauer Franz , Bell Eric F. , Bertoldi Frank , Chapman Scott , Colina Luis , Cortes Paulo C. , Cox Pierre , Dickinson Mark , Elbaz David , Gónzalez-López Jorge , Ibar Edo , Inami Hanae , Infante Leopoldo , Hodge Jacqueline , Karim Alex , Fevre Olivier Le , Magnelli Benjamin , Neri Roberto , Oesch Pascal , Ota Kazuaki , Popping Gergö , Rix Hans-Walter , Sargent Mark , Sheth Kartik , Wel Arjen van der , Werf Paul van der , Wagg Jeff 
Published: December 2016

ABSTRACT
We present the rationale for and the observational description of ASPECS: the ALMA SPECtroscopic Survey in the Hubble Ultra-Deep Field (UDF), the cosmological deep field that has the deepest multi-wavelength data available. Our overarching goal is to obtain an unbiased census of molecular gas and dust continuum emission in high-redshift (z > 0.5) galaxies. The ∼1′ region covered within the UDF was chosen to overlap with the deepest available imaging from the Hubble Space Telescope. Our ALMA observations consist of full frequency scans in band 3 (84–115 GHz) and band 6 (212–272 GHz) at approximately uniform line sensitivity (

2 × 109 K km s−1 pc2), and continuum noise levels of 3.8 μJy beam−1 and 12.7 μJy beam−1, respectively. The molecular surveys cover the different rotational transitions of the CO molecule, leading to essentially full redshift coverage. The [C ii] emission line is also covered at redshifts

. We present a customized algorithm to identify line candidates in the molecular line scans and quantify our ability to recover artificial sources from our data. Based on whether multiple CO lines are detected, and whether optical spectroscopic redshifts as well as optical counterparts exist, we constrain the most likely line identification. We report 10 (11) CO line candidates in the 3 mm (1 mm) band, and our statistical analysis shows that <4 of these (in each band) are likely spurious. Less than one-third of the total CO flux in the low-J CO line candidates are from sources that are not associated with an optical/NIR counterpart. We also present continuum maps of both the band 3 and band 6 observations. The data presented here form the basis of a number of dedicated studies that are presented in subsequent papers.
THE ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: CONTINUUM NUMBER COUNTS, RESOLVED 1.2 mm EXTRAGALACTIC BACKGROUND, AND PROPERTIES OF THE FAINTEST DUSTY STAR-FORMING GALAXIES
Authors: Aravena M. , Decarli R. , Walter F. , Cunha E. Da , Bauer F. E. , Carilli C. L. , Daddi E. , Elbaz D. , Ivison R. J. , Riechers D. A. , Smail I. , Swinbank A. M. , Weiss A. , Anguita T. , Assef R. J. , Bell E. , Bertoldi F. , Bacon R. , Bouwens R. , Cortes P. , Cox P. , Gónzalez-López J. , Hodge J. , Ibar E. , Inami H. , Infante L. , Karim A. , Fèvre O. Le Le , Magnelli B. , Ota K. , Popping G. , Sheth K. , van der Werf P. , Wagg J. 
Published: December 2016

ABSTRACT
We present an analysis of a deep (1σ = 13 μJy) cosmological 1.2 mm continuum map based on ASPECS, the ALMA Spectroscopic Survey in the Hubble Ultra Deep Field. In the 1 arcmin2 covered by ASPECS we detect nine sources at

significance at 1.2 mm. Our ALMA-selected sample has a median redshift of

, with only one galaxy detected at z > 2 within the survey area. This value is significantly lower than that found in millimeter samples selected at a higher flux density cutoff and similar frequencies. Most galaxies have specific star formation rates (SFRs) similar to that of main-sequence galaxies at the same epoch, and we find median values of stellar mass and SFRs of

and

yr−1, respectively. Using the dust emission as a tracer for the interstellar medium (ISM) mass, we derive depletion times that are typically longer than 300 Myr, and we find molecular gas fractions ranging from ∼0.1 to 1.0. As noted by previous studies, these values are lower than those using CO-based ISM estimates by a factor of ∼2. The 1 mm number counts (corrected for fidelity and completeness) are in agreement with previous studies that were typically restricted to brighter sources. With our individual detections only, we recover 55% ± 4% of the extragalactic background light (EBL) at 1.2 mm measured by the Planck satellite, and we recover 80% ± 7% of this EBL if we include the bright end of the number counts and additional detections from stacking. The stacked contribution is dominated by galaxies at

, with stellar masses of (1–3) × 1010
M

. For the first time, we are able to characterize the population of galaxies that dominate the EBL at 1.2 mm.
THE ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: MOLECULAR GAS RESERVOIRS IN HIGH-REDSHIFT GALAXIES
Authors: Decarli Roberto , Walter Fabian , Aravena Manuel , Carilli Chris , Bouwens Rychard , Cunha Elisabete da , Daddi Emanuele , Elbaz David , Riechers Dominik , Smail Ian , Swinbank Mark , Weiss Axel , Bacon Roland , Bauer Franz , Bell Eric F. , Bertoldi Frank , Chapman Scott , Colina Luis , Cortes Paulo C. , Cox Pierre , Gónzalez-López Jorge , Inami Hanae , Ivison Rob , Hodge Jacqueline , Karim Alex , Magnelli Benjamin , Ota Kazuaki , Popping Gergö , Rix Hans-Walter , Sargent Mark , Wel Arjen van der , Werf Paul van der 
Published: December 2016

ABSTRACT
We study the molecular gas properties of high-z galaxies observed in the ALMA Spectroscopic Survey (ASPECS) that targets an ∼1 arcmin2 region in the Hubble Ultra Deep Field (UDF), a blind survey of CO emission (tracing molecular gas) in the 3 and 1 mm bands. Of a total of 1302 galaxies in the field, 56 have spectroscopic redshifts and correspondingly well-defined physical properties. Among these, 11 have infrared luminosities

, i.e., a detection in CO emission was expected. Out of these, 7 are detected at various significance in CO, and 4 are undetected in CO emission. In the CO-detected sources, we find CO excitation conditions that are lower than those typically found in starburst/sub-mm galaxy/QSO environments. We use the CO luminosities (including limits for non-detections) to derive molecular gas masses. We discuss our findings in the context of previous molecular gas observations at high redshift (star formation law, gas depletion times, gas fractions): the CO-detected galaxies in the UDF tend to reside on the low-

envelope of the scatter in the

relation, but exceptions exist. For the CO-detected sources, we find an average depletion time of ∼1 Gyr, with significant scatter. The average molecular-to-stellar mass ratio (

/M
*) is consistent with earlier measurements of main-sequence galaxies at these redshifts, and again shows large variations among sources. In some cases, we also measure dust continuum emission. On average, the dust-based estimates of the molecular gas are a factor ∼2–5× smaller than those based on CO. When we account for detections as well as non-detections, we find large diversity in the molecular gas properties of the high-redshift galaxies covered by ASPECS.
ANOMALOUS COOLING OF CORONAL LOOPS WITH TURBULENT SUPPRESSION OF THERMAL CONDUCTION
Authors: Bian Nicolas H. , Watters Jonathan M. , Kontar Eduard P. , Emslie A. Gordon 
Published: December 2016

ABSTRACT
We investigate the impact of turbulent suppression of parallel heat conduction on the cooling of post-flare coronal loops. Depending on the value of the mean free path

associated with the turbulent scattering process, we identify four main cooling scenarios. The overall temperature evolution, from an initial temperature in excess of 107 K, is modeled in each case, highlighting the evolution of the dominant cooling mechanism throughout the cooling process. Comparison with observed cooling times allows the value of

to be constrained, and interestingly this range corresponds to situations where collision-dominated conduction plays a very limited role, or even no role at all, in the cooling of post-flare coronal loops.
SYSTEMATIC STUDY OF GAMMA-RAY-BRIGHT BLAZARS WITH OPTICAL POLARIZATION AND GAMMA-RAY VARIABILITY
Authors: Itoh Ryosuke , Nalewajko Krzysztof , Fukazawa Yasushi , Uemura Makoto , Tanaka Yasuyuki T. , Kawabata Koji S. , Madejski Greg M. , Schinzel Frank. K. , Kanda Yuka , Shiki Kensei , Akitaya Hiroshi , Kawabata Miho , Moritani Yuki , Nakaoka Tatsuya , Ohsugi Takashi , Sasada Mahito , Takaki Katsutoshi , Takata Koji , Ui Takahiro , Yamanaka Masayuki , Yoshida Michitoshi 
Published: December 2016

ABSTRACT
Blazars are highly variable active galactic nuclei that emit radiation at all wavelengths from radio to gamma rays. Polarized radiation from blazars is one key piece of evidence for synchrotron radiation at low energies, and it also varies dramatically. The polarization of blazars is of interest for understanding the origin, confinement, and propagation of jets. However, even though numerous measurements have been performed, the mechanisms behind jet creation, composition, and variability are still debated. We performed simultaneous gamma-ray and optical photopolarimetry observations of 45 blazars between 2008 July and 2014 December to investigate the mechanisms of variability and search for a basic relation between the several subclasses of blazars. We identify a correlation between the maximum degree of optical linear polarization and the gamma-ray luminosity or the ratio of gamma-ray to optical fluxes. Since the maximum polarization degree depends on the condition of the magnetic field (chaotic or ordered), this result implies a systematic difference in the intrinsic alignment of magnetic fields in parsec-scale relativistic jets between different types of blazars (flat-spectrum radio quasars vs. BL Lacs) and consequently between different types of radio galaxies (FR I versus FR II).
AUTOMATED DETECTION OF CORONAL MASS EJECTIONS IN STEREO HELIOSPHERIC IMAGER DATA
Authors: Pant V. , Willems S. , Rodriguez L. , Mierla M. , Banerjee D. , Davies J. A. 
Published: December 2016

ABSTRACT
We have performed, for the first time, the successful automated detection of coronal mass ejections (CMEs) in data from the inner heliospheric imager (HI-1) cameras on the STEREO-A spacecraft. Detection of CMEs is done in time–height maps based on the application of the Hough transform, using a modified version of the CACTus software package, conventionally applied to coronagraph data. In this paper, we describe the method of detection. We present the results of the application of the technique to a few CMEs, which are well detected in the HI-1 imagery, and compare these results with those based on manual-cataloging methodologies. We discuss, in detail, the advantages and disadvantages of this method.
EVOLUTION OF CATACLYSMIC VARIABLES AND RELATED BINARIES CONTAINING A WHITE DWARF
Authors: Kalomeni B. , Nelson L. , Rappaport S. , Molnar M. , Quintin J. , Yakut K. 
Published: December 2016

ABSTRACT
We present a binary evolution study of cataclysmic variables (CVs) and related systems with white dwarf (WD) accretors, including for example, AM CVn systems, classical novae, supersoft X-ray sources (SXSs), and systems with giant donor stars. Our approach intentionally avoids the complications associated with population synthesis algorithms, thereby allowing us to present the first truly comprehensive exploration of all of the subsequent binary evolution pathways that zero-age CVs might follow (assuming fully non-conservative, Roche-lobe overflow onto an accreting WD) using the sophisticated binary stellar evolution code MESA. The grid consists of 56,000 initial models, including 14 WD accretor masses, 43 donor-star masses (0.1–4.7 M
⊙), and 100 orbital periods. We explore evolution tracks in the orbital period and donor-mass (P
orb–M
don) plane in terms of evolution dwell times, masses of the WD accretor, accretion rate, and chemical composition of the center and surface of the donor star. We report on the differences among the standard CV tracks, those with giant donor stars, and ultrashort period systems. We show where in parameter space one can expect to find SXSs, present a diagnostic to distinguish among different evolutionary paths to forming AM CVn binaries, quantify how the minimum orbital period in CVs depends on the chemical composition of the donor star, and update the P
orb(M
wd) relation for binaries containing WDs whose progenitors lost their envelopes via stable Roche-lobe overflow. Finally, we indicate where in the P
orb–M
don the accretion disks will tend to be stable against the thermal-viscous instability, and where gravitational radiation signatures may be found with LISA.
GALAXY PROPERTIES AND UV ESCAPE FRACTIONS DURING THE EPOCH OF REIONIZATION: RESULTS FROM THE RENAISSANCE SIMULATIONS
Authors: Xu Hao , Wise John H. , Norman Michael L. , Ahn Kyungjin , O’Shea Brian W. 
Published: December 2016

ABSTRACT
Cosmic reionization is thought to be primarily fueled by the first generations of galaxies. We examine their stellar and gaseous properties, focusing on the star formation rates and the escape of ionizing photons, as a function of halo mass, redshift, and environment using the full suite of the Renaissance Simulations with an eye to provide better inputs to global reionization simulations. This suite probes overdense, average, and underdense regions of the universe of several hundred comoving Mpc3, each yielding a sample of over 3000 halos in the mass range of 107–109.5

at their final redshifts of 15, 12.5, and 8, respectively. In the process, we simulate the effects of radiative and supernova feedback from 5000 to 10,000 Population III stars in each simulation. We find that halos as small as 107

are able to host bursty star formation due to metal-line cooling from earlier enrichment by massive Population III stars. Using our large sample, we find that the galaxy-halo occupation fraction drops from unity at virial masses above 108.5

to ∼50% at 108

and ∼10% at 107

, quite independent of redshift and region. Their average ionizing escape fraction is ∼5% in the mass range of 108–109

and increases with decreasing halo mass below this range, reaching 40%–60% at 107

. Interestingly, we find that the escape fraction varies between 10%–20% in halos with virial masses of ∼3 × 109

. Taken together, our results confirm the importance of the smallest galaxies as sources of ionizing radiation contributing to the reionization of the universe.
ASTROSAT CZT IMAGER OBSERVATIONS OF GRB 151006A: TIMING, SPECTROSCOPY, AND POLARIZATION STUDY
Authors: Rao A. R. , Chand Vikas , Hingar M. K. , Iyyani S. , Khanna Rakesh , Kutty A. P. K. , Malkar J. P. , Paul D. , Bhalerao V. B. , Bhattacharya D. , Dewangan G. C. , Pawar Pramod , Vibhute A. M. , Chattopadhyay T. , Mithun N. P. S. , Vadawale S. V. , Vagshette N. , Basak R. , Pradeep P. , Samuel Essy , Sreekumar S. , Vinod P. , Navalgund K. H. , Pandiyan R. , Sarma K. S. , Seetha S. , Subbarao K. 
Published: December 2016

ABSTRACT

AstroSat is a multi-wavelength satellite launched on 2015 September 28. The CZT Imager of AstroSat on its very first day of operation detected a long duration gamma-ray burst (GRB), namely GRB 151006A. Using the off-axis imaging and spectral response of the instrument, we demonstrate that the CZT Imager can localize this GRB correctly to about a few degrees, and it can provide, in conjunction with Swift, spectral parameters similar to those obtained from Fermi/GBM. Hence, the CZT Imager would be a useful addition to the currently operating GRB instruments (Swift and Fermi). Specifically, we argue that the CZT Imager will be most useful for the short hard GRBs by providing localization for those detected by Fermi and spectral information for those detected only by Swift. We also provide preliminary results on a new exciting capability of this instrument: the CZT Imager is able to identify Compton scattered events thereby providing polarization information for bright GRBs. GRB 151006A, in spite of being relatively faint, shows hints of a polarization signal at 100–300 keV (though at a low significance level). We point out that the CZT Imager should provide significant time resolved polarization measurements for GRBs that have fluence three times higher than that of GRB 151006A. We estimate that the number of such bright GRBs detectable by the CZT Imager is five to six per year. The CZT Imager can also act as a good hard X-ray monitoring device for possible electromagnetic counterparts of gravitational wave events.
Pour une approche multiréférencée de l’autisme
Authors: Bergmans Sara , Frankard Anne-Christine , Gadisseux Christine , Henet Martine , Janssens Mileen , Schonne Isabelle , Taymans Anne , Bestgen François , Bourlez Frédéric , Hosselet Thomas , Leclercq Jean-Paul , Malet Claude , Tona Salvatore 
Published: December 2016

Comme ce fut le cas dans d’autres pays (France, Angleterre, Pays-Bas), la prise en charge des enfants et adolescents autistes a été soumise à avis en Belgique. Le Conseil Supérieur de la Santé et le Centre Fédéral d’Expertise des Soins de Santé ont chacun publié leurs rapports en 2013-2014. Ces avis s’inscrivent dans un paradoxe : d’un côté, « la Science » et les « Pratiques ou la Médecine Basées sur l’Evidence (ebp et ebm) » ; d’un autre côté, les rapports mentionnent le manque de preuves de l’efficacité de n’importe quelle méthode. Leurs conclusions cependant marquent des préférences, en particulier pour des méthodes comportementalistes. Pour un grand nombre de cliniciens, il ne peut être question de clore la réflexion, de limiter les pratiques et, de facto, d’empêcher de nouvelles avancées ou découvertes. La présente contribution appelle à fédérer les compétences pour améliorer les connaissances encore lacunaires et imparfaites relatives à l’autisme. Rédigées dans les deux principales langues nationales (le néerlandais et le français), cette contribution a fait l’objet d’une large diffusion. Son résumé, dans une double version synthétique, a été soumis à pétitions. Près de 700 signatures, tant au Nord qu’au Sud du pays, ont appuyé l’envoi de nos textes aux nombreuses autorités politiques et aux instances administratives belges.
Comment penser l’anorexie précoce et sévère du bébé ?
Authors: Vinant Victoire , Breil Fleur , Durieux Marie-José , Rappaport Clémentine 
Published: December 2016

L’anorexie précoce du bébé est une pathologie complexe, multi-factorielle, qui met en péril la dyade mère-bébé ainsi que le développement global de l’enfant.	Nora, 2 mois, est hospitalisée en pédiatrie pour dénutrition dans un contexte de refus alimentaire nécessitant une alimentation entérale passive. Elle a pour principale comorbidité, un syndrome de Noonan diagnostiqué a posteriori. Elle présente des signes de souffrance psychique importants en partie liée à une discontinuité et une dépression maternelle. Grâce à la prise en charge thérapeutique intensive du bébé et de sa mère, Nora, à l’âge de 2 ans, développe le « jeu « nécessaire à l’élaboration symbolique et peut sortir de ce collage à deux. Néanmoins notre observation clinique nous laisse préjuger d’une dépression du bébé en miroir de celle de sa mère.	L’observation de Nora illustre la complexité à appréhender l’anorexie précoce et sévère du bébé. Le syndrome de Noonan diagnostiqué chez ce bébé participe à la grande fragilité de son oralité. Son anorexie est également symptomatique d’une dépression du bébé. Elle révèle une situation relationnelle avec sa mère envahie par des représentations mortifères et traumatiques.	Une revue de la littérature actualisée des troubles de l’oralité du bébé confirme l’existence d’un substrat organique à l’émergence de ces troubles précoces et sévères et appelle à la modestie des hypothèses psychopathologiques.	Ici nous formulons l’hypothèse qu’il existe une projection maternelle massive déclenchée par les troubles alimentaires du bébé. L’investissement maternel se fait autour de la partie souffrante et mourante du bébé et participe à la chronicisation de l’anorexie.	Ce tableau de dépression du bébé en miroir de la dépression maternelle, s’articule autour du trouble de l’oralité de Nora et l’entretient, laissant entrevoir un nécessaire travail psychothérapeutique pour Nora et sa mère.
Fins de vie, éthique et société
Authors: Higgins Robert William 
Published: December 2016

Depuis leur origine, les soins palliatifs ont mis en avant un triple objectif : lutter contre ce que Norbert Elias a nommé « la solitude des mourants », s’opposer à l’exclusion dont la mort était l’objet dans nos sociétés occidentales industrialisées, exclusion soulignée par les travaux de Philippe Ariès, et enfin, dans un second temps, promouvoir un contrepoids – je pense en particulier aux bénévoles, et aux plus récents réseaux – face à la médicalisation de la mort dans ces mêmes sociétés, médicalisation à laquelle, d’ailleurs, le mouvement en faveur des soins palliatifs pouvait « objectivement collaborer », ne serait-ce que de fait. Par rapport à ces trois points essentiels, et à partir d’un travail que je mène depuis de longues années 1 , je voudrais émettre quelques remarques critiques qui appellent à une vigilance, voire à des révisions cruciales. Je crois que nous devons nous efforcer de repérer « l’autoroute » sur laquelle nous sommes – à notre insu le plus souvent – embarqués, et les effets pervers qui s’y manifestent – et dont certains sont à mon avis structurels – et que l’on peut, que l’on doit même mettre au jour. J’ajoute que ces remarques critiques s’appliquent aussi bien à ce qui se joue du côté des partisans de l’euthanasie. Une logique commune, à bien des égards, est à l’œuvre, qu’il s’agit de démonter, ne serait-ce que pour « ne pas en remettre », comme je le répète à mes étudiants, et bien dégager la spécificité des soins palliatifs – et même leur mission – ainsi que leurs fondements, au-delà d’une vision quelque peu floue fondée sur l’affectif et qui les maintient dans une sorte de symétrie inverse face au mouvement en faveur de la légalisation de l’euthanasie qui ne cesse de se diffuser.
Fins de vie, éthique et société
Authors: Scicluna Emmanuel 
Published: December 2016

En tant que cadre de santé, je tenterai de mettre en perspective les enjeux éthiques liés à la fin de vie des personnes hospitalisées dans les services de psychiatrie. La pertinence d’une association entre les équipes de psychiatrie et les équipes de soins palliatifs s’impose, afin de mieux appréhender les modalités relationnelles, l’angoisse de la mort et l’état de « mort psychique », si caractéristiques de la fin de vie.