bluuebunny/crossref_metadata_2025_split huggingface dataset:
Revealing Dusty Supernovae in High-redshift (Ultra)Luminous Infrared Galaxies through Near-infrared Integrated Light Variability
Authors: Yan Haojing , Ma Zhiyuan , Beacom John F. , Runge James 
Published: October 2018

Abstract
Luminous and ultra-luminous infrared galaxies ((U)LIRGs) are rare today but are increasingly abundant at high redshifts. They are believed to be dusty starbursts, and hence should have high rates of supernovae (multiple events per year). Due to their extremely dusty environment, however, such supernovae could only be detected in rest-frame infrared and longer wavelengths, where our current facilities lack the capability of finding them individually beyond the local universe. We propose a new technique for higher redshifts, which is to search for the presence of supernovae through the variability of the integrated rest-frame infrared light of the entire hosts. We present a pilot study to assess the feasibility of this technique. We exploit a unique region, the “IRAC Dark Field” (IDF), that the Spitzer Space Telescope has observed for more than 14 years in 3–5 μm. The IDF also has deep far-infrared data (200–550 μm) from the Herschel Space Observatory that allow us to select high-redshift (U)LIRGs. We obtain a sample of (U)LIRGs that have secure optical counterparts, and examine their light curves in 3–5 μm. While the variabilities could also be caused by AGNs, we show that such contaminations can be identified. We present two cases where the distinct features in their light curves are consistent with multiple supernovae overlapping in time. Searching for supernovae this way will be relevant to the James Webb Space Telescope (JWST) to probe high-redshift (U)LIRGs into their nuclear regions where JWST will be limited by its resolution.
Determining the Evolutionary Stage of the δ Scuti Star HIP 80088 with Asteroseismology
Authors: Chen Xinghao , Li Yan 
Published: October 2018

Abstract
We have computed a grid of theoretical models to fit the 12 oscillation modes of HIP 80088 observed by K2. HIP 80088 is determined to be a pre-main-sequence star, in which the CN cycle has not arrived at the equilibrium state. Mass fractions of C12 and N14 in metal composition are

and

, respectively, indicating that 28% of C12 have turned into N14. Meanwhile, our fitting results show that physical parameters of HIP 80088 converge to a small range: M = 1.68–1.78 M
⊙, Z = 0.015–0.018,

km s−1, log g = 4.114–4.125, R = 1.882–1.914 R
⊙, τ
0 = 7636–7723 s, and age = 9.03–10.21 Myr. Based on our model fittings, f
3 is suggested to be one radial mode, f
2, f
4, f
8, and f
11 to be four ℓ = 1 modes, and f
1, f
5, f
6, f
7, f
9, f
10, and f
12 to be seven ℓ = 2 modes. In particular, we find that (f
2, f
4, f
8) form one complete triplet with the averaged frequency spacing of 16.045 μHz, and (f
5, f
7, f
9, f
10) form four components of one quintuplet with the averaged frequency spacing of 13.388 μHz. The two averaged frequency spacings are not equal. Based on the best-fitting model, those ℓ = 2 modes of HIP 80088 are found to be mixed modes, which are p-dominated modes with pronounced g-mode features, while oscillation modes with ℓ = 1 are p modes.
The Carnegie–Chicago Hubble Program. V. The Distances to NGC 1448 and NGC 1316 via the Tip of the Red Giant Branch∗
Authors: Hatt Dylan , Freedman Wendy L. , Madore Barry F. , Jang In Sung , Beaton Rachael L. , Hoyt Taylor J. , Lee Myung Gyoon , Monson Andrew J. , Rich Jeffrey A. , Scowcroft Victoria , Seibert Mark 
Published: October 2018

Abstract
The Carnegie–Chicago Hubble Program (CCHP) is recalibrating the extragalactic SN Ia distance scale using exclusively Population II stars. This effort focuses on the Tip of the Red Giant Branch (TRGB) method, whose systematics are entirely independent of the Population I Cepheid-based determinations that have long served as calibrators for the SN Ia distance scale. We present deep Hubble Space Telescope imaging of the low surface density and low line-of-sight reddening halos of two galaxies, NGC 1448 and NGC 1316, each of which have been hosts to recent SN Ia events. Provisionally anchoring the TRGB zero-point to the geometric distance to the Large Magellanic Cloud derived from detached eclipsing binaries, we measure extinction-corrected distance moduli of

mag for NGC 1448 and

mag for NGC 1316, respectively, giving metric distances of

Mpc, and

Mpc. We find agreement between our result and the available Cepheid distance for NGC 1448; for NGC 1316, where there are relatively few published distances based on direct measurements, we find that our result is consistent with the published SN Ia distances whose absolute scales are set from other locally determined methods such as Cepheids. For NGC 1448 and NGC 1316, our distances are some of the most precise (and systematically accurate) measurements with errors at 1.7 (2.8)% and 1.6 (2.7)% levels, respectively.
Molecular Clouds Associated with the Type Ia SNR N103B in the Large Magellanic Cloud
Authors: Sano H. , Yamane Y. , Tokuda K. , Fujii K. , Tsuge K. , Nagaya T. , Yoshiike S. , Filipović M. D. , Alsaberi R. Z. E. , Barnes L. , Onishi T. , Kawamura A. , Minamidani T. , Mizuno N. , Yamamoto H. , Tachihara K. , Maxted N. , Voisin F. , Rowell G. , Yamaguchi H. , Fukui Y. 
Published: October 2018

Abstract
N103B is a Type Ia supernova remnant (SNR) in the Large Magellanic Cloud (LMC). We carried out new 12CO(J = 3–2) and 12CO(J = 1–0) observations using ASTE and ALMA. We have confirmed the existence of a giant molecular cloud at V
LSR ∼ 245 km s−1 toward the southeast of the SNR using ASTE 12CO(J = 3–2) data at an angular resolution of ∼25″ (∼6 pc in the LMC). Using the ALMA 12CO(J = 1–0) data, we have spatially resolved CO clouds along the southeastern edge of the SNR with an angular resolution of ∼1.″8 (∼0.4 pc in the LMC). The molecular clouds show an expanding gas motion in the position–velocity diagram with an expansion velocity of ∼5 km s−1. The spatial extent of the expanding shell is roughly similar to that of the SNR. We also find tiny molecular clumps in the directions of optical nebula knots. We present a possible scenario that N103B exploded in the wind-bubble formed by the accretion winds from the progenitor system, and is now interacting with the dense gas wall. This is consistent with a single-degenerate scenario.
Kilonova Emission from Black Hole–Neutron Star Mergers: Observational Signatures of Anisotropic Mass Ejection
Authors: Huang Zhi-Qiu , Liu Liang-Duan , Wang Xiang-Yu , Dai Zi-Gao 
Published: October 2018

Abstract
The gravitational wave event GW170817 associated with the short gamma-ray burst (GRB) 170817A confirms that binary neutron star (BNS) mergers act as one of the origins of short GRBs. The associated kilonova emission, radioactively powered by nucleosynthesized heavy elements, was also detected. Black hole–neutron star (BH–NS) mergers have also been argued to be a promising candidate for the origin of short GRBs and kilonovae. Numerical simulations show that the ejecta in BH–NS mergers is geometrically much more anisotropic than the BNS merger case. In this paper, we investigate observational signatures of kilonova emission from the anisotropic ejecta in BH–NS mergers. We find that a bump appears on the bolometric luminosity light curve due to the inhomogeneous mass distribution in the latitudinal direction. The decay slope of the single-band light curve becomes flatter and the spectrum also deviates from a single-temperature blackbody radiation spectrum due to the gradient in the velocity distribution of the ejecta. Future detection or nondetection of such signatures would be useful to test the mass ejection geometry in BH–NS mergers.
The Spin Alignment of Galaxies with the Large-scale Tidal Field in Hydrodynamic Simulations
Authors: Wang Peng , Guo Quan , Kang Xi , Libeskind Noam I. 
Published: October 2018

Abstract
The correlation between the spins of dark matter halos and the large-scale structure (LSS) has been studied in great detail over a large redshift range, while investigations of galaxies are still incomplete. Motivated by this point, we use the state-of-the-art hydrodynamic simulation, Illustris-1, to investigate mainly the spin–LSS correlation of galaxies at a redshift of z = 0. We mainly find that the spins of low-mass, blue, oblate galaxies are preferentially aligned with the slowest collapsing direction (

) of the large-scale tidal field, while massive, red, prolate galaxy spins tend to be perpendicular to

. The transition from a parallel to a perpendicular trend occurs at ∼109.4
h
−1
M
⊙ in the stellar mass, ∼0.62 in the g–r color, and ∼0.4 in triaxiality. The transition stellar mass decreases with increasing redshifts. The alignment was found to be primarily correlated with the galaxy stellar mass. Our results are consistent with previous studies both in N-body simulations and observations. Our study also fills the vacancy in the study of the galaxy spin–LSS correlation at z = 0 using hydrodynamical simulations and also provides important insight to understand the formation and evolution of galaxy angular momentum.
Assessment of Ionospheric Activity Tolerances for Epoch of Reionization Science with the Murchison Widefield Array
Authors: Trott Cathryn M. , Jordan C. H. , Murray S. G. , Pindor B. , Mitchell D. A. , Wayth R. B. , Line J. , McKinley B. , Beardsley A. , Bowman J. , Briggs F. , Hazelton B. J. , Hewitt J. , Jacobs D. , Morales M. F. , Pober J. C. , Sethi S. , Shankar U. , Subrahmanyan R. , Tegmark M. , Tingay S. J. , Webster R. L. , Wyithe J. S. B. 
Published: October 2018

Abstract
Structure imprinted in foreground extragalactic point sources by ionospheric refraction has the potential to contaminate Epoch of Reionization (EoR) power spectra of the 21 cm emission line of neutral hydrogen. The alteration of the spatial and spectral structure of foreground measurements due to total electron content gradients in the ionosphere creates a departure from the expected sky signal. We present a general framework for understanding the signatures of ionospheric behavior in the 2D neutral hydrogen power spectrum measured by a low-frequency radio interferometer. Two primary classes of ionospheric behavior are considered, corresponding to dominant modes observed in Murchison Widefield Array (MWA) EoR data, namely, anisotropic structured wave behavior and isotropic turbulence. Analytic predictions for power spectrum bias due to this contamination are computed and compared with simulations. We then apply the ionospheric metric described in Jordan et al. to study the impact of ionospheric structure on MWA data, by dividing MWA EoR data sets into classes with good and poor ionospheric conditions, using sets of matched 30-minute observations from 2014 September. The results are compared with the analytic and simulated predictions, demonstrating the observed bias in the power spectrum when the ionosphere is active (displays coherent structures or isotropic turbulence). The analysis demonstrates that unless ionospheric activity can be quantified and corrected, active data should not be included in EoR analysis in order to avoid systematic biases in cosmological power spectra. When data are corrected with a model formed from the calibration information, bias reduces below the expected 21 cm signal level. Data are considered “quiet” when the median measured source position offsets are less than 10.″–15.″.
Identifying Anticyclonic Vortex Features Produced by the Rossby Wave Instability in Protoplanetary Disks
Authors: Huang Pinghui , Isella Andrea , Li Hui , Li Shengtai , Ji Jianghui 
Published: October 2018

Abstract
Several nearby protoplanetary disks have been observed to display large-scale crescents in the (sub)millimeter dust continuum emission. One interpretation is that these structures correspond to anticyclonic vortices generated by the Rossby wave instability within the gaseous disk. Such vortices have local gas overdensities and are expected to concentrate dust particles with a Stokes number around unity. This process might catalyze the formation of planetesimals. Whereas recent observations showed that dust crescents are indeed regions where millimeter-size particles have abnormally high concentration relative to the gas and smaller grains, no observations have yet shown that the gas within the crescent region counterrotates with respect to the protoplanetary disk. Here we investigate the detectability of anticyclonic features through measurement of the line-of-sight component of the gas velocity obtained with ALMA. We carry out 2D hydrodynamic simulations and 3D radiative transfer calculations of a protoplanetary disk characterized by a vortex created by the tidal interaction with a massive planet. As a case study, the disk parameters are chosen to mimic the IRS 48 system, which has the most prominent crescent observed to date. We generate synthetic ALMA observations of both the dust continuum and 12CO emission around the frequency of 345 GHz. We find that the anticyclonic features of the vortex are weak but can be detected if both the source and the observational setup are properly chosen. We provide a recipe for maximizing the probability of detecting such vortex features and present an analysis procedure to infer their kinematic properties.
The Rest-frame Optical Sizes of Massive Galaxies with Suppressed Star Formation at z ∼ 4
Authors: Kubo Mariko , Tanaka Masayuki , Yabe Kiyoto , Toft Sune , Stockmann Mikkel , Gómez-Guijarro Carlos 
Published: October 2018

Abstract
We present the rest-frame optical sizes of massive quiescent galaxies (QGs) at z ∼ 4 measured at the K′-band with the Infrared Camera and Spectrograph and adaptive optics (AO) facility, AO188, on the Subaru telescope. Based on a deep multiwavelength catalog in the Subaru XMM-Newton Deep Survey Field, covering a wide wavelength range from the u-band to the IRAC 8.0 μm over 0.7 deg2, we evaluate the photometric redshift to identify massive (M
⋆ ∼ 1011
M
⊙) galaxies with suppressed star formation. These galaxies show a prominent Balmer break feature at z ∼ 4, suggestive of an evolved stellar population. We then conduct follow-up K′-band imaging with AO for the five brightest galaxies (K
AB,total = 22.5 ∼ 23.4). Compared to lower redshift ones, QGs at z ∼ 4 have smaller physical sizes of effective radii r
eff = 0.2–1.7 kpc. The mean size measured by stacking the four brightest objects, a more robust measurement, is r
eff = 0.5 kpc. This is the first measurement of the rest-frame optical sizes of QGs at z ∼ 4. We evaluate the robustness of our size measurements using simulations and find that our size estimates are reasonably accurate with an expected systematic bias of ∼0.2 kpc. If we account for the stellar mass evolution, massive QGs at z ∼ 4 are likely to evolve into the most massive galaxies today. We find their size evolution with cosmic time in the form of

. Their size growth is proportional to the square of stellar mass, indicating that size–stellar mass growth is driven by minor dry mergers.
Distances of Galactic Supernova Remnants Using Red Clump Stars
Authors: Shan S. S. , Zhu H. , Tian W. W. , Zhang M. F. , Zhang H. Y. , Wu D. , Yang A. Y. 
Published: October 2018

Abstract
We carry out a project to independently measure the distances of supernova remnants (SNRs) in the first quadrant of the Galaxy. In this project, red clump (RC) stars are used as standard candles and extinction probes to build the optical extinction (A

V
)–distance(D) relation in each direction of extinction-known SNRs. The distances of 15 SNRs are determined. Among them, the distances of G65.8–0.5, G66.0–0.0, and G67.6+0.9 are given for the first time. We also obtain 32 upper/lower limits of distances, and the distances to G5.7–0.1, G15.1–1.6, G28.8+1.5, and G78.2+2.1 are constrained. Most of the distances measured by the RC method are consistent with previous results. The RC method provides independent access to the distances of SNRs.
A Revised Exoplanet Yield from the Transiting Exoplanet Survey Satellite (TESS)
Authors: Barclay Thomas , Pepper Joshua , Quintana Elisa V. 
Published: October 2018

Abstract
The Transiting Exoplanet Survey Satellite (TESS) has a goal of detecting small planets orbiting stars bright enough for mass determination via ground-based radial velocity observations. Here, we present estimates of how many exoplanets the TESS mission will detect, the physical properties of the detected planets, and the properties of the stars that those planets orbit. This work uses stars drawn from the TESS Input Catalog Candidate Target List and revises yields from prior studies that were based on Galactic models. We modeled the TESS observing strategy to select approximately 200,000 stars at 2-minute cadence, while the remaining stars are observed at 30-minute cadence in full-frame image data. We placed zero or more planets in orbit around each star, with physical properties following measured exoplanet occurrence rates, and used the TESS noise model to predict the derived properties of the detected exoplanets. In the TESS 2-minute cadence mode we estimate that TESS will find 1250 ± 70 exoplanets (90% confidence), including 250 smaller than 2 R
⊕. Furthermore, we predict that an additional 3100 planets will be found in full-frame image data orbiting bright dwarf stars and more than 10,000 around fainter stars. We predict that TESS will find 500 planets orbiting M dwarfs, but the majority of planets will orbit stars larger than the Sun. Our simulated sample of planets contains hundreds of small planets amenable to radial velocity follow-up, potentially more than tripling the number of planets smaller than 4 R
⊕ with mass measurements. This sample of simulated planets is available for use in planning follow-up observations and analyses.
Time Dependence of the IBEX Ribbon and the Globally Distributed Energetic Neutral Atom Flux Using the First 9 Years of Observations
Authors: Schwadron N. A. , Allegrini F. , Bzowski M. , Christian E. R. , Dayeh M. A. , Desai M. I. , Fairchild K. , Frisch P. C. , Funsten H. O. , Fuselier S. A. , Galli A. , Janzen P. , Kubiak M. A. , McComas D. J. , Moebius E. , Reisenfeld D. B. , Sokół J. M. , Swaczyna P. , Szalay J. R. , Wurz P. , Zirnstein E. J. 
Published: October 2018

Abstract
Observations from the Interstellar Boundary Explorer (IBEX) of energetic neutral atoms (ENAs) reveal two populations, those emitted from a narrow (∼20°–40°) ribbon that is centered on the local interstellar magnetic field, and a globally distributed flux (GDF) that is controlled by processes in the heliosheath. This is a third study utilizing a previously developed technique to separate ENA emissions in the ribbon from the GDF. In the first ribbon separation study, we analyzed the first year of IBEX data at the energies of 0.7 keV and above; the second study analyzed data down to 0.2 keV using the first five years of IBEX data. Here, we utilize the separation analysis from 0.7 keV and above to study time evolution in 3 year intervals over the first nine years of IBEX data. This study is the first to reveal the global time evolution of the GDF distinct from that of the IBEX ribbon. We show that the time evolution of the GDF within 40° of the upwind pressure maximum is driven by changes in the solar wind ram pressure through compression and rarefaction in the heliosheath. In contrast, the GDF is relatively stable in the region centered on the heliotail downwind with respect to the interstellar flow. The evolution of the IBEX ribbon is observed to have a time lag with respect to the upwind GDF evolution, likely due to the secondary (neutral) solar wind source. The time lag observed in the ribbon evolution is consistent with the generation of ions retained for several years beyond the heliopause. These observations lend further support to secondary solar wind models of the IBEX ribbon, but also require that there is a significant several year time lag for reneutralization of ions that form the IBEX ribbon. We use this study of the 9 year separation of the IBEX ribbon from the globally distributed flux to prepare for a formal IBEX data release of ribbon and globally distributed flux maps to the heliophysics community.
Le cinéma yougoslave
Authors: Chiclet Christophe 
Published: October 2018

Du 22 au 28 août dernier, s’est tenu le 37 e festival du film yougoslave de Nis. Nous sommes bien loin des inaugurations pompeuses de l’époque yougoslave ou des années de plomb de la période Milosevic. Aujourd’hui, le cinéma yougoslave a un nouvel ennemi : le manque criant de moyens.
Que faire de l’ambition des siens pour soi ? Réflexions sur le cas de Romain Gary
Authors: Audi Paul 
Published: October 2018

Dans La promesse de l’aube , Romain Gary fait état de la naissance de sa vocation d’écrivain en l’abordant en termes d’assignation produite par l’Autre, sa mère en l’occurrence. Très jeune, il aurait entendu d’elle un « Tu seras… » qu’il s’est alors empressé d’interpréter, non sans humour, bien moins comme un commandement que comme une prophétie auto-réalisatrice. Aussi, sous couvert de liberté, évidemment, s’est-il appliqué à devenir ce que le désir de la mère voulait qu’il fût. Ainsi il a fait de ce désir autre la lance de sa propre destinée. Mais comment en a-t-il rendu compte ? Quels enseignements en a-t-il retenus ? Et enfin, et surtout, quelle leçon la psychanalyse pourrait-elle en tirer, c’est-à-dire, et pour ne prendre ici qu’un exemple, à quels ajustements la notion de « névrose de destinée » pourrait-elle se plier au regard d’une telle expérience subjective ?
L’ambition d’une mère à l’œuvre… dans l’écriture et la publication d’un cas de psychanalyse : La petite « Piggle » de Winnicott
Authors: Lenormand Marie 
Published: October 2018

Publié il y a 40 ans, en 1977, L a petite « Piggle » de Winnicott est un cas de psychanalyse d’enfant assez longtemps éclipsé, voire « black-listé » dans les années 1990 dans le monde anglo-saxon. Un regain d’intérêt, notable depuis ces dernières années, résulte, entre autres, de la décision de Gabrielle, surnommée la « petite Piggle » dans le cas, une femme aujourd’hui dans la cinquantaine, de faire son « coming out analytique », i.e. de révéler son identité, d’apporter son témoignage et d’ouvrir certaines archives afférentes au cas auprès de la communauté analytique. L’une des singularités de la conduite de cette cure est de se réclamer de ce que Winnicott dénomme la « psychoanalysis partagée (shared) » ( sic ) – consistant à partager, avec les parents, le contenu de la cure mais également partiellement sa conduite, cette démarche allant jusqu’à la coécriture du cas. Nous faisons l’hypothèse que ce dernier, ce faisant, a étonnamment sous-estimé la question de la demande et du transfert parentaux – notamment dans la mesure où ceux-ci peuvent être articulés au symptôme de l’enfant. Des éléments présents dans le cas – et corroborés par Gabrielle adulte – nous conduiront à faire l’hypothèse que ce cas émane, en partie au moins, d’une demande maternelle restée inanalysée. Nous serons ainsi amenés à interroger les incidences et la nature de « l’ambition » d’une mère à l’œuvre dans l’écriture et la publication d’un cas de psychanalyse.