bluuebunny/crossref_metadata_2025_split huggingface dataset:
SN 2012dn from early to late times: 09dc-like supernovae reassessed★
Authors: Taubenberger S , Floers A , Vogl C , Kromer M , Spyromilio J , Aldering G , Antilogus P , Bailey S , Baltay C , Bongard S , Boone K , Buton C , Chotard N , Copin Y , Dixon S , Fouchez D , Fransson C , Gangler E , Gupta R R , Hachinger S , Hayden B , Hillebrandt W , Kim A G , Kowalski M , Leget P-F , Leibundgut B , Mazzali P A , Noebauer U M , Nordin J , Pain R , Pakmor R , Pecontal E , Pereira R , Perlmutter S , Ponder K A , Rabinowitz D , Rigault M , Rubin D , Runge K , Saunders C , Smadja G , Tao C , Thomas R C 
Published: July 2019

Abstract
As a candidate ‘super-Chandrasekhar’ or 09dc-like Type Ia supernova (SN Ia), SN 2012dn shares many characteristics with other members of this remarkable class of objects but lacks their extraordinary luminosity. Here, we present and discuss the most comprehensive optical data set of this SN to date, comprised of a densely sampled series of early-time spectra obtained within the Nearby Supernova Factory project, plus photometry and spectroscopy obtained at the VLT about 1 yr after the explosion. The light curves, colour curves, spectral time series and ejecta velocities of SN 2012dn are compared with those of other 09dc-like and normal SNe Ia, the overall variety within the class of 09dc-like SNe Ia is discussed, and new criteria for 09dc-likeness are proposed. Particular attention is directed to additional insight that the late-phase data provide. The nebular spectra show forbidden lines of oxygen and calcium, elements that are usually not seen in late-time spectra of SNe Ia, while the ionisation state of the emitting iron plasma is low, pointing to low ejecta temperatures and high densities. The optical light curves are characterised by an enhanced fading starting ∼60 d after maximum and very low luminosities in the nebular phase, which is most readily explained by unusually early formation of clumpy dust in the ejecta. Taken together, these effects suggest a strongly perturbed ejecta density profile, which might lend support to the idea that 09dc-like characteristics arise from a brief episode of interaction with a hydrogen-deficient envelope during the first hours or days after the explosion.
Spectral analysis of the hybrid PG 1159-type central stars of the planetary nebulae Abell 43 and NGC 7094
Authors: Löbling L , Rauch T , Miller Bertolami M M , Todt H , Friederich F , Ziegler M , Werner K , Kruk J W 
Published: July 2019

Abstract
Stellar post asymptotic giant branch (post-AGB) evolution can be completely altered by a final thermal pulse (FTP) which may occur when the star is still leaving the AGB (AFTP), at the departure from the AGB at still constant luminosity (late TP, LTP) or after the entry to the white-dwarf cooling sequence (very late TP, VLTP). Then convection mixes the He-rich material with the H-rich envelope. According to stellar evolution models the result is a star with a surface composition of $\mathrm{H}\approx \, 20$ per cent by mass (AFTP), ≈ 1 per cent (LTP), or (almost) no H (VLTP). Since FTP stars exhibit intershell material at their surface, spectral analyses establish constraints for AGB nucleosynthesis and stellar evolution. We performed a spectral analysis of the so-called hybrid PG 1159-type central stars (CS) of the planetary nebulae Abell 43 and NGC 7094 by means of non-local thermodynamical equilibrium models. We confirm the previously determined effective temperatures of $\mbox{$T_\mathrm{eff}$}\, = 115\, 000\pm 5\, 000 \, \mathrm{K}$ and determine surface gravities of $\log\,(g\,/\,(\mathrm{cm}\,\mathrm{s}^{-2} )) = 5.6\pm 0.1$ for both. From a comparison with AFTP evolutionary tracks, we derive stellar masses of $0.57^{+0.07}_{-0.04}$ M⊙ and determine the abundances of H, He, and metals up to Xe. Both CS are likely AFTP stars with a surface H mass fraction of 0.25 ± 0.03 and 0.15 ± 0.03, respectively, and an Fe deficiency indicating subsolar initial metallicities. The light metals show typical PG 1159-type abundances and the elemental composition is in good agreement with predictions from AFTP evolutionary models. However, the expansion ages do not agree with evolution time-scales expected from the AFTP scenario and alternatives should be explored.
Ultraviolet Mg ii emission from fast neutral ejecta around Eta Carinae
Authors: Smith Nathan , Morse Jon A 
Published: July 2019

ABSTRACT
We present the first images of the nebula around η Carinae obtained with the Wide Field Camera 3 (WFC3) onboard the Hubble Space Telescope (HST), including an ultraviolet (UV) image in the F280N filter that traces Mg ii emission, plus contemporaneous imaging in the F336W, F658N, and F126N filters that trace near-UV continuum, [N ii], and [Fe ii], respectively. The F336W and F658N images are consistent with previous images in these filters, and F126N shows that for the most part, [Fe ii] λ12567 traces clumpy shocked gas seen in [N ii]. The F280N image, however, reveals Mg ii emission from structures that have not been seen in any previous line or continuum images of η Carinae. This image shows diffuse Mg ii emission immediately outside the bipolar Homunculus nebula in all directions, but with the strongest emission concentrated over the poles. The diffuse structure with prominent radial streaks, plus an anticorrelation with ionized tracers of clumpy shocked gas, leads us to suggest that this is primarily Mg ii resonant scattering from unshocked, neutral atomic gas. We discuss the implied structure and geometry of the Mg ii emission, and its relation to the Homunculus lobes and various other complex nebular structures. An order of magnitude estimate of the neutral gas mass traced by Mg ii is 0.02 M⊙, with a corresponding kinetic energy around 1047 erg. This may provide important constraints on polar mass-loss in the early phases of the great eruption. We argue that the Mg ii line may be an excellent tracer of significant reservoirs of freely expanding, unshocked, and otherwise invisible neutral atomic gas in a variety of stellar outflows.
The Lense–Thirring timing-accretion plane for ULXs
Authors: Middleton M J , Fragile P C , Ingram A , Roberts T P 
Published: July 2019

ABSTRACT
Identifying the compact object in ultraluminous X-ray sources (ULXs) has to date required detection of pulsations or a cyclotron resonance scattering feature (CRSF), indicating a magnetized neutron star. However, pulsations are observed to be transient and it is plausible that accretion on to the neutron star may have suppressed the surface magnetic field such that pulsations and CRSFs will be entirely absent. We may therefore lack direct means to identify neutron star systems whilst we presently lack an effective means by which to identify black hole ULXs. Here we present a possible method for separating the ULX population by assuming the X-ray, mHz quasi-periodic oscillations (QPOs), and day time-scale periods/QPOs are associated with Lense–Thirring precession of the inflow and outflowing wind, respectively. The precession time-scales combined with the temperature of the soft X-ray component produce planes where the accretor mass enters as a free parameter. Depending on the properties of the wind, use of these planes may be robust to a range in the angular momentum (spin) and, for high accretion rates, essentially independent of the neutron star’s surface dipole field strength. Our model also predicts the mHz QPO frequency and magnitude of the phase lag imprinted due to propagation through the optically thick wind; in the case of NGC 5408 X-1 we subsequently infer a black hole mass and moderate-to-high spin. Finally, we note that observing secular QPO evolution over sufficient baselines may indicate a neutron star, as the precession responds to spin-up which is not readily observable for black hole primaries.
Companion-launched jets and their effect on the dynamics of common envelope interaction simulations
Authors: Shiber Sagiv , Iaconi Roberto , De Marco Orsola , Soker Noam 
Published: July 2019

Abstract
We conduct three-dimensional hydrodynamic simulations of the common envelope binary interaction and show that if the companion were to launch jets while interacting with the giant primary star’s envelope, the jets would remove a substantial fraction of the envelope’s gas. We use the set-up and numerical code of an earlier common envelope study that did not include jets, with a 0.88-M⊙, 83-R⊙ red giant star and a 0.3-M⊙ companion. The assumption is that the companion star accretes mass via an accretion disc that is responsible for launching the jets which, in the simulations, are injected numerically. For the first time we conduct simulations that include jets as well as the gravitational energy released by the inspiralling core-companion system. We find that simulations with jets unbind approximately three times as much envelope mass than identical simulations that do not include jets, though the total fraction of unbound gas remains below 50 per cent for these particular simulations. The jets generate high-velocity outflows in the polar directions. The jets also increase the final core-companion orbital separation and lead to a kick velocity of the core-companion binary system. Our results show that, if able to form, jets could play a crucial role in ejecting the envelope and in shaping the outflow.
Mass loss from the exoplanet WASP-12b inferred from Spitzer phase curves
Authors: Bell Taylor J , Zhang Michael , Cubillos Patricio E , Dang Lisa , Fossati Luca , Todorov Kamen O , Cowan Nicolas B , Deming Drake , Zellem Robert T , Stevenson Kevin B , Crossfield Ian J M , Dobbs-Dixon Ian , Fortney Jonathan J , Knutson Heather A , Line Michael R 
Published: July 2019

ABSTRACT
The exoplanet WASP-12b is the prototype for the emerging class of ultrahot, Jupiter-mass exoplanets. Past models have predicted – and near-ultraviolet observations have shown – that this planet is losing mass. We present an analysis of two sets of 3.6 and 4.5 $\mu \rm{m}$Spitzer phase curve observations of the system which show clear evidence of infrared radiation from gas stripped from the planet, and the gas appears to be flowing directly toward or away from the host star. This accretion signature is only seen at 4.5 $\mu \rm{m}$, not at 3.6 $\mu \rm{m}$, which is indicative either of CO emission at the longer wavelength or blackbody emission from cool, ≲600 K gas. It is unclear why WASP-12b is the only ultrahot Jupiter to exhibit this mass-loss signature, but perhaps WASP-12b’s orbit is decaying as some have claimed, while the orbits of other exoplanets may be more stable; alternatively, the high-energy irradiation from WASP-12A may be stronger than the other host stars. We also find evidence for phase offset variability at the level of 6.4σ (46.2°) at 3.6 $\mu \rm{m}$.
Impact of an off-centred dipole on neutron star binaries
Authors: Pétri J 
Published: July 2019

ABSTRACT
Neutron stars are strongly magnetized rotating compact objects. Therefore, they also produce huge electric fields accelerating particles to ultrarelativistic energies. The simplest magnetic topology is a dipole traditionally located at the stellar centre. In this paper, we re-investigate the consequences of an off-centred rotating magnetic dipole, showing accurate magnetic field line geometries, the associated spin-down luminosity as well as the corresponding electromagnetic kick and torque imprinted to the neutron star. Results are obtained by time-dependent numerical simulations of Maxwell equations in vacuum using pseudo-spectral methods. We compare our results to known analytical expressions available to lowest order in the parameter ϵ = d/R, where d is the displacement of the dipole from the stellar centre and R the neutron star radius. We found good agreement between our numerical computations and our analytical approximations even for well off-centred dipoles having large displacements with a sizeable fraction of the radius, i.e. ϵ ≲ 1. An explanation for binary neutron star eccentricity distribution functions is given with an emphasize on highly eccentric systems as an alternative scenario to traditional binary formation.
Time-dependent evolution of the protoplanetary discs with magnetic winds
Authors: Shadmehri Mohsen , Ghoreyshi Sayyedeh Masoumeh 
Published: July 2019

ABSTRACT
We study the evolution of the protoplanetary discs (PPDs) in the presence of magnetically driven winds with the stress relations motivated by the non-ideal MHD disc simulations. Contribution of the magnetic winds in the angular momentum removal and mass-loss is described using these relations which are quantified in terms of the plasma parameter. Evolution of the essential disc quantities including the surface density, accretion rate, and wind mass-loss rate are studied for a wide range of the model parameters. Two distinct phases of the disc evolution are found irrespective of the adopted input parameters. While at the early phase of the disc evolution, global disc quantities such as its total mass and magnetic flux undergo non-significant reductions, their rapid declines are found in the second phase of evolution. Duration of each phase, however, depends upon the model parameters including magnetic wind strength. Our model predicts that contributions of the magnetic winds in the disc evolution are significant during the second phase. We then calculated locus of points in the plane of the accretion rate and total disc mass corresponding to an ensemble of evolving PPDs. Our theoretical isochrone tracks exhibit reasonable fits to the observed PPDs in star-forming regions Lupus and σ-Orion.
21-cm power spectrum and ionization bias as a probe of long-mode modulated non-Gaussian sky
Authors: Khosravi Shahram , Ghazizadeh Amirabbas , Baghram Shant 
Published: July 2019

ABSTRACT
The observed hemispherical power asymmetry in cosmic microwave background radiation can be explained by long-wavelength mode (long-mode) modulation. In this paper, we study the possibility of detecting this effect in the angular power spectrum of the 21-cm brightness temperature. For this task, we study the effect of the neutral hydrogen distribution on the angular power spectrum. This is done by formulating the bias parameter of the ionized fraction to the underlying matter distribution. We also discuss the possibility that the long-mode modulation is accompanied by a primordial non-Gaussianity of local type. In this case, we obtain the angular power spectrum with two effects of primordial non-Gaussianity and long-mode modulation. Finally, we show that the primordial non-Gaussianity enhances the long-mode modulated power of the 21-cm signal via the non-Gaussian scale-dependent bias up to four orders of magnitude. Accordingly, observations of the 21-cm signal with upcoming surveys, such as the Square Kilometer Array (SKA), will probably be capable of detecting hemispherical power asymmetry in the context of long-mode modulation.
Scaling relations for globular cluster systems in early-type galaxies
Authors: Caso Juan P , De Bórtoli Bruno J , Ennis Ana I , Bassino Lilia P 
Published: July 2019

ABSTRACT
The formation and growth of globular cluster systems (GCSs) is closely related to the evolutionary processes experienced by their host galaxies. In particular, their radial distributions scale with several properties of the galaxies and their haloes. We performed a photometric study, by means of HST/ACS archival data of several intermediate luminosity galaxies located in low-density environments. It was supplemented with available photometric data of GCSs from the Virgo and Fornax clusters, resulting in a sample of almost 30 GCSs for which we fitted their radial profiles. The resulting overall properties agree with those from previous studies, as we found that the effective radius, extension, and concentration of the GCS radial profiles correlate with the stellar mass, effective radius, and number of globular clusters, presenting in some cases a bilinear relation. The extension also correlates with the central velocity dispersion for central galaxies, but not for satellites. From a statistical comparison with numerical simulations we obtained good agreement between the effective radius and extension of the GCS scale with the effective and virial radius of the haloes, respectively. Finally, we analysed these results in the literature context.
Metallicity of stars formed throughout the cosmic history based on the observational properties of star-forming galaxies
Authors: Chruslinska Martyna , Nelemans Gijs 
Published: July 2019

ABSTRACT
Metallicity is one of the crucial factors that determine stellar evolution. To characterize the properties of stellar populations one needs to know the fraction of stars forming at different metallicities. Knowing how this fraction evolves over time is necessary e.g. to estimate the rates of occurrence of any stellar evolution related phenomena (e.g. double compact object mergers, gamma-ray bursts). Such theoretical estimates can be confronted with observational limits to validate the assumptions about the evolution of the progenitor system leading to a certain transient. However, to perform the comparison correctly one needs to know the uncertainties related to the assumed star formation history and chemical evolution of the Universe. We combine the empirical scaling relations and other observational properties of the star-forming galaxies to construct the distribution of the cosmic star formation rate density at different metallicities and redshifts. We address the question of uncertainty of this distribution due to currently unresolved questions, such as the absolute metallicity scale, the flattening in the star formation−mass relation or the low-mass end of the galaxy mass function. We find that the fraction of stellar mass formed at metallicities &lt;10 per cent solar (&gt;solar) since z = 3 varies by ∼18 per cent (∼26 per cent) between the extreme cases considered in our study. This uncertainty stems primarily from the differences in the mass–metallicity relations obtained with different methods. We confront our results with the local core-collapse supernovae observations. Our model is publicly available.
“Ghost Introgression” As a Cause of Deep Mitochondrial Divergence in a Bird Species Complex
Authors: Zhang Dezhi , Tang Linfang , Cheng Yalin , Hao Yan , Xiong Ying , Song Gang , Qu Yanhua , Rheindt Frank E , Alström Per , Jia Chenxi , Lei Fumin 
Published: July 2019

AbstractIn the absence of nuclear-genomic differentiation between two populations, deep mitochondrial divergence (DMD) is a form of mito-nuclear discordance. Such instances of DMD are rare and might variably be explained by unusual cases of female-linked selection, by male-biased dispersal, by “speciation reversal” or by mitochondrial capture through genetic introgression. Here, we analyze DMD in an Asian Phylloscopus leaf warbler (Aves: Phylloscopidae) complex. Bioacoustic, morphological, and genomic data demonstrate close similarity between the taxa affinis and occisinensis, even though DMD previously led to their classification as two distinct species. Using population genomic and comparative genomic methods on 45 whole genomes, including historical reconstructions of effective population size, genomic peaks of differentiation and genomic linkage, we infer that the form affinis is likely the product of a westward expansion in which it replaced a now-extinct congener that was the donor of its mtDNA and small portions of its nuclear genome. This study provides strong evidence of “ghost introgression” as the cause of DMD, and we suggest that “ghost introgression” may be a widely overlooked phenomenon in nature.
Transcriptional Enhancers in the FOXP2 Locus Underwent Accelerated Evolution in the Human Lineage
Authors: Caporale Alfredo Leandro , Gonda Catalina M , Franchini Lucía Florencia 
Published: July 2019

AbstractUnique human features, such as complex language, are the result of molecular evolutionary changes that modified developmental programs of our brain. The human-specific evolution of the forkhead box P2 (FOXP2) gene-coding region has been linked to the emergence of speech and language in the human kind. However, little is known about how the expression of FOXP2 is regulated and whether its regulatory machinery evolved in a lineage-specific manner in humans. In order to identify FOXP2 regulatory regions containing human-specific changes, we used databases of human-accelerated noncoding sequences or HARs. We found that the topologically associating domain determined using developing human cerebral cortex containing the FOXP2 locus includes two clusters of 12 HARs, placing the locus occupied by FOXP2 among the top regions showing fast acceleration rates in noncoding regions in the human genome. Using in vivo enhancer assays in zebrafish, we found that at least five FOXP2-HARs behave as transcriptional enhancers throughout different developmental stages. In addition, we found that at least two FOXP2-HARs direct the expression of the reporter gene EGFP to foxP2-expressing regions and cells. Moreover, we uncovered two FOXP2-HARs showing reporter expression gain of function in the nervous system when compared with the chimpanzee ortholog sequences. Our results indicate that regulatory sequences in the FOXP2 locus underwent a human-specific evolutionary process suggesting that the transcriptional machinery controlling this gene could have also evolved differentially in the human lineage.
A new set of endogenous control genes for use in quantitative real-time PCR experiments show that formin Ldia2dex transcripts are enriched in the early embryo of the pond snail Lymnaea stagnalis (Panpulmonata)
Authors: Johnson Harriet F , Davison Angus 
Published: July 2019

ABSTRACT
Although the pond snail Lymnaea stagnalis is an emerging model organism for molecular studies in a wide variety of fields, there are a limited number of verified endogenous control genes for use in quantitative real-time PCR. As part of a larger study on snail chirality, or left–right asymmetry, we assayed gene expression in pond snail embryos. We evaluated six candidate control genes, by comparing their expression in three tissues (ovotestis, foot and embryo) and used three software programmes (geNorm, Normfinder and Bestkeeper) to do so. The specific utility of these control genes was then tested by investigating the relative expression of six experimental transcripts, including formin Ldia2, a gene that has been associated with chiral variation in L. stagnalis. All six control genes were found to be suitable for use in the three tissues tested. Of the six experimental genes, it was found that all were relatively depleted in the early embryo compared with other tissues, except the formin Ldia2 gene. Instead, transcripts of the wild-type Ldia2dex were enriched in the embryo, whereas a nonfunctional frameshifted version, Ldia2sin, was severely depleted. These differences in Ldia2sin expression were less evident in the ovotestis and were not evident in the foot tissue, possibly because nonsense-mediated decay is obscured in actively transcribing tissues. Our work provides a set of control genes that may be useful to the wider community and illustrates how these genes may be used to assay differences in expression in a variety of tissues.