bluuebunny/crossref_metadata_2025_split huggingface dataset:
Removing Harmful Options: The Law and Ethics of International Commercial Surrogacy
Authors: Hodson Nathan , Townley Lynne , Earp Brian D 
Published: August 2019

Abstract
Focusing on the UK as a case study, this article argues that having the choice to enter into an international commercial surrogacy arrangement can be harmful, but that neither legalisation nor punitive restriction offers an adequate way to reduce this risk. Whether or not having certain options can harm individuals is central to current debates about the sale of organs. We assess and apply the arguments from that debate to international commercial surrogacy, showing that simply having the option to enter into a commercial surrogacy arrangement can harm potential vendors individually and collectively, particularly given its sexed dimension. We reject the argument that legalizing commercial surrogacy in the UK could reduce international exploitation. We also find that a punitive approach towards intended parents utilizing commercial rather than altruistic services is inappropriate. Drawing on challenges in the regulation of forced marriage and female genital cutting, we propose that international collaboration towards control of commercial surrogacy is a better strategy for preserving the delicate balancing of surrogate mothers’ protection and children’s welfare in UK law.
New β Cep pulsators discovered with K2 space photometry
Authors: Burssens S , Bowman D M , Aerts C , Pedersen M G , Moravveji E , Buysschaert B 
Published: August 2019

Abstract
We present the discovery of three new β Cep pulsators, three new pulsators with frequency groupings, and frequency patterns in a B3Ib star, all of which show pulsations with frequencies as high as about 17 d−1, with K2 space mission photometry. Based on a Fourier analysis and iterative pre-whitening, we present a classification and evaluate the potential for asteroseismic modelling. We include the lists of pulsation frequencies for three new β Cep pulsators, CD-28 12286, CD-27 10876, LS 3978, and additional pulsation mode frequencies for the known β Cep pulsator HD 164741. In addition, we characterize the regular frequency spacing found in the new pulsator HD 169173, and discuss its origin. We place the newly discovered variables in a colour–magnitude diagram using parallaxes from GaiaDR2 (second data release), showcasing their approximate location in the massive star domain. The identified frequency lists of these multiperiodic pulsators are a good starting point for future forward seismic modelling, after identification of at least one pulsation frequency from high-resolution time-series spectroscopy and/or multicolour photometry.
Dark Energy Survey Year 1 results: constraints on intrinsic alignments and their colour dependence from galaxy clustering and weak lensing
Authors: Samuroff S , Blazek J , Troxel M A , MacCrann N , Krause E , Leonard C D , Prat J , Gruen D , Dodelson S , Eifler T F , Gatti M , Hartley W G , Hoyle B , Larsen P , Zuntz J , Abbott T M C , Allam S , Annis J , Bernstein G M , Bertin E , Bridle S L , Brooks D , Carnero Rosell A , Carrasco Kind M , Carretero J , Castander F J , Cunha C E , da Costa L N , Davis C , De Vicente J , DePoy D L , Desai S , Diehl H T , Dietrich J P , Doel P , Flaugher B , Fosalba P , Frieman J , García-Bellido J , Gaztanaga E , Gerdes D W , Gruendl R A , Gschwend J , Gutierrez G , Hollowood D L , Honscheid K , James D J , Kuehn K , Kuropatkin N , Lima M , Maia M A G , March M , Marshall J L , Martini P , Melchior P , Menanteau F , Miller C J , Miquel R , Ogando R L C , Plazas A A , Sanchez E , Scarpine V , Schindler R , Schubnell M , Serrano S , Sevilla-Noarbe I , Sheldon E , Smith M , Sobreira F , Suchyta E , Tarle G , Thomas D , Vikram V ,   (DES Collaboration)
Published: August 2019

Abstract
We perform a joint analysis of intrinsic alignments and cosmology using tomographic weak lensing, galaxy clustering, and galaxy–galaxy lensing measurements from Year 1 (Y1) of the Dark Energy Survey. We define early- and late-type subsamples, which are found to pass a series of systematics tests, including for spurious photometric redshift error and point spread function correlations. We analyse these split data alongside the fiducial mixed Y1 sample using a range of intrinsic alignment models. In a fiducial non-linear alignment model analysis, assuming a flat Λ cold dark matter cosmology, we find a significant difference in intrinsic alignment amplitude, with early-type galaxies favouring $A_\mathrm{IA} = 2.38^{+0.32}_{-0.31}$ and late-type galaxies consistent with no intrinsic alignments at $0.05^{+0.10}_{-0.09}$. The analysis is repeated using a number of extended model spaces, including a physically motivated model that includes both tidal torquing and tidal alignment mechanisms. In multiprobe likelihood chains in which cosmology, intrinsic alignments in both galaxy samples and all other relevant systematics are varied simultaneously, we find the tidal alignment and tidal torquing parts of the intrinsic alignment signal have amplitudes $A_1 = 2.66 ^{+0.67}_{-0.66}$, $A_2=-2.94^{+1.94}_{-1.83}$, respectively, for early-type galaxies and $A_1 = 0.62 ^{+0.41}_{-0.41}$, $A_2 = -2.26^{+1.30}_{-1.16}$ for late-type galaxies. In the full (mixed) Y1 sample the best constraints are $A_1 = 0.70 ^{+0.41}_{-0.38}$, $A_2 = -1.36 ^{+1.08}_{-1.41}$. For all galaxy splits and IA models considered, we report cosmological parameter constraints consistent with the results of the main DES Y1 cosmic shear and multiprobe cosmology papers.
Galaxy structure with strong gravitational lensing: decomposing the internal mass distribution of massive elliptical galaxies
Authors: Nightingale James W , Massey Richard J , Harvey David R , Cooper Andrew P , Etherington Amy , Tam Sut-Ieng , Hayes Richard G 
Published: August 2019

Abstract
We investigate how strong gravitational lensing can test contemporary models of massive elliptical (ME) galaxy formation, by combining a traditional decomposition of their visible stellar distribution with a lensing analysis of their mass distribution. As a proof of concept, we study a sample of three ME lenses, observing that all are composed of two distinct baryonic structures, a ‘red’ central bulge surrounded by an extended envelope of stellar material. Whilst these two components look photometrically similar, their distinct lensing effects permit a clean decomposition of their mass structure. This allows us to infer two key pieces of information about each lens galaxy: (i) the stellar mass distribution (without invoking stellar populations models) and (ii) the inner dark matter halo mass. We argue that these two measurements are crucial to testing models of ME formation, as the stellar mass profile provides a diagnostic of baryonic accretion and feedback whilst the dark matter mass places each galaxy in the context of LCDM large scale structure formation. We also detect large rotational offsets between the two stellar components and a lopsidedness in their outer mass distributions, which hold further information on the evolution of each ME. Finally, we discuss how this approach can be extended to galaxies of all Hubble types and what implication our results have for studies of strong gravitational lensing.
A new sample of X-ray selected Swift/SDSS faint blazars and blazar candidates
Authors: Turriziani Sara , Fraga B , Giommi P 
Published: August 2019

Abstract
Our present knowledge of the properties of blazars mostly comes from small samples of bright objects, especially regarding studies on their cosmological evolution. Statistically well defined and completely identified samples of faint blazars are very difficult to obtain. We present a new X-ray selected sample of 62 blazars and blazar candidates reaching deep X-ray fluxes. We relied on the availability of large catalogs of astronomical objects combined with on-line services offering simple access to finding charts and magnitude estimates. We built the sample cross-matching X-ray sources in the Swift Serendipitous Survey in deep XRT GRB Fields catalog with data from deep radio and optical surveys. Our sample can probe populations of sources 10 times weaker in the X-ray flux with respect previous studies, thus allowing for a more detailed comparison between data and simulated counts. We use the sample to calculate the radio and X-ray LogN-LogS of blazars down to fluxes at least one order of magnitude fainter than previous studies. We show that, considering that our sample may be somewhat contaminated by sources other than blazars, we are in agreement with previous observational and theoretical estimations.
Constraining primordial non-Gaussianity using two galaxy surveys and CMB lensing
Authors: Ballardini Mario , Matthewson William L , Maartens Roy 
Published: August 2019

ABSTRACT
Next-generation galaxy surveys will be able to measure perturbations on scales beyond the equality scale. On these ultra-large scales, primordial non-Gaussianity leaves signatures that can shed light on the mechanism by which perturbations in the early Universe are generated. We perform a forecast analysis for constraining local type non-Gaussianity and its two-parameter extension with a simple scale-dependence. We combine different clustering measurements from future galaxy surveys – a 21cm intensity mapping survey and two photometric galaxy surveys – via the multitracer approach. Furthermore we then include cosmic microwave background (CMB) lensing from a CMB Stage 4 experiment in the multitracer, which can improve the constraints on bias parameters. We forecast σ(fNL) ≃ 0.9 (1.4) by combining SKA1, a Euclid-like (LSST-like) survey, and CMB Stage 4 lensing. With CMB lensing, the precision on fNL improves by up to a factor of 2, showing that a joint analysis is important. In the case with running of fNL, our results show that the combination of upcoming cosmological surveys could achieve σ(nNL) ≃ 0.12 (0.22) on the running index.
The beamed jet and quasar core of the distant blazar 4C 71.07
Authors: Raiteri C M , Villata M , Carnerero M I , Acosta-Pulido J A , Mirzaqulov D O , Larionov V M , Romano P , Vercellone S , Agudo I , Arkharov A A , Bach U , Bachev R , Baitieri S , Borman G A , Boschin W , Bozhilov V , Butuzova M S , Calcidese P , Carosati D , Casadio C , Chen W-P , Damljanovic G , Di Paola A , Doroshenko V T , Efimova N V , Ehgamberdiev Sh A , Giroletti M , Gómez J L , Grishina T S , Ibryamov S , Jermak H , Jorstad S G , Kimeridze G N , Klimanov S A , Kopatskaya E N , Kurtanidze O M , Kurtanidze S O , Lähteenmäki A , Larionova E G , Marscher A P , Mihov B , Minev M , Molina S N , Moody J W , Morozova D A , Nazarov S V , Nikiforova A A , Nikolashvili M G , Ovcharov E , Peneva S , Righini S , Rizzi N , Sadun A C , Samal M R , Savchenko S S , Semkov E , Sigua L A , Slavcheva-Mihova L , Steele I A , Strigachev A , Tornikoski M , Troitskaya Yu V , Troitsky I S , Vince O 
Published: August 2019

ABSTRACT
The object 4C 71.07 is a high-redshift blazar whose spectral energy distribution shows a prominent big blue bump and a strong Compton dominance. We present the results of a 2-yr multiwavelength campaign led by the Whole Earth Blazar Telescope (WEBT) to study both the quasar core and the beamed jet of this source. The WEBT data are complemented by ultraviolet and X-ray data from Swift, and by γ-ray data by Fermi. The big blue bump is modelled by using optical and near-infrared mean spectra obtained during the campaign, together with optical and ultraviolet quasar templates. We give prescriptions to correct the source photometry in the various bands for the thermal contribution, in order to derive the non-thermal jet flux. The role of the intergalactic medium absorption is analysed in both the ultraviolet and X-ray bands. We provide opacity values to deabsorb ultraviolet data, and derive a best-guess value for the hydrogen column density of $N_{\rm H}^{\rm best}=6.3 \times 10^{20} \rm \, cm^{-2}$ through the analysis of X-ray spectra. We estimate the disc and jet bolometric luminosities, accretion rate, and black hole mass. Light curves do not show persistent correlations among flux changes at different frequencies. We study the polarimetric behaviour and find no correlation between polarization degree and flux, even when correcting for the dilution effect of the big blue bump. Similarly, wide rotations of the electric vector polarization angle do not seem to be connected with the source activity.
On the role of supermassive black holes in quenching star formation in local central galaxies
Authors: Arora Nikhil , Fossati Matteo , Fontanot Fabio , Hirschmann Michaela , Wilman David J 
Published: August 2019

ABSTRACT
We analyse the role of AGN feedback in quenching star formation for massive, central galaxies in the local Universe. In particular, we compare the prediction of two semi-analytic models (l-galaxies  and sage) featuring different schemes for AGN feedback, with the SDSS DR7 taking advantage of a novel technique for identifying central galaxies in an observational data set. This enables us to study the correlation between the model passive fractions, which is predicted to be suppressed by feedback from an AGN, and the observed passive fractions in an observationally motivated parameter space. While the passive fractions for observed central galaxies show a good correlation with stellar mass and bulge mass, passive fractions in l-galaxies  correlate with the halo and black hole mass. For sage, the passive fraction correlate with the bulge mass as well. Among the two models, sage has a smaller scatter in the black hole–bulge mass $({M_{\rm BH}-M_{\rm Bulge}})$ relation and a slope that agrees better with the most recent observations at z ∼ 0. Despite the more realistic prescription of radio-mode feedback in sage, there are still tensions left with the observed passive fractions and the distribution of quenched galaxies. These tensions may be due to the treatment of galaxies living in non-resolved substructures and the resulting higher merger rates that could bring cold gas which is available for star formation.
Low-frequency X-ray timing with Gaussian processes and reverberation in the radio-loud AGN 3C 120
Authors: Wilkins D R 
Published: August 2019

ABSTRACT
A framework is developed to perform Fourier-domain timing analysis on X-ray light curves with gaps, employing Gaussian processes to model the probability distribution underlying the observed time series from which continuous samples can be drawn. A technique is developed to measure X-ray reverberation from the inner regions of accretion discs around black holes in the low-frequency components of the variability, on time-scales longer than can be probed employing standard Fourier techniques. This enables X-ray reverberation experiments to be performed using data from satellites in low-Earth orbit such as NICER, NuSTAR, and the proposed X-ray timing mission STROBE-X, and enables long time-scale reverberation around higher mass active galactic nuclei (AGNs) to be measured by combining observations. Gaussian processes are applied to observations of the broad line radio galaxy 3C 120 spanning two orbits with XMM–Newton to measure the relative time lags of successive X-ray energy bands. The lag–energy spectrum between 5 × 10−6 and 3 × 10−5 Hz, estimated using Gaussian processes, reveals X-ray reverberation from the inner accretion disc for the first time in this radio-loud AGN. Time lags in the relativistically broadened iron K line are significantly detected. The core of the line lags behind the continuum by (3800 ± 1500) s, suggesting a scale height of the corona of (13 ± 8) rg above the disc. The ability to compare the structure of coronae in radio-loud AGNs to their radio-quiet counterparts will yield important insight into the mechanisms by which black holes are able to launch jets.
The ultra-diffuse dwarf galaxies NGC 1052-DF2 and 1052-DF4 are in conflict with standard cosmology
Authors: Haslbauer Moritz , Banik Indranil , Kroupa Pavel , Grishunin Konstantin 
Published: August 2019

ABSTRACT
Recently van Dokkum et al. reported that the galaxy NGC 1052-DF2 (DF2) lacks dark matter if located at 20 Mpc from Earth. In contrast, DF2 is a dark-matter-dominated dwarf galaxy with a normal globular cluster population if it has a much shorter distance near 10 Mpc. However, DF2 then has a high peculiar velocity wrt. the cosmic microwave background of 886 $\rm {km\, s^{-1}}$, which differs from that of the Local Group (LG) velocity vector by 1298 $\rm {km\, s^{-1}}$ with an angle of $117 \, ^{\circ }$. Taking into account the dynamical M/L ratio, the stellar mass, half-light radius, peculiar velocity, motion relative to the LG, and the luminosities of the globular clusters, we show that the probability of finding DF2-like galaxies in the lambda cold dark matter (ΛCDM) TNG100-1 simulation is at most 1.0 × 10−4 at 11.5 Mpc and is 4.8 × 10−7 at 20.0 Mpc. At 11.5 Mpc, the peculiar velocity is in significant tension in the TNG100-1, TNG300-1, and Millennium simulations, but naturally in a Milgromian cosmology. At 20.0 Mpc, the unusual globular cluster population would challenge any cosmological model. Estimating that precise measurements of the internal velocity dispersion, stellar mass, and distance exist for 100 galaxies, DF2 is in 2.6σ (11.5 Mpc) and 4.1σ (20.0 Mpc) tension with standard cosmology. Adopting the former distance for DF2 and assuming that NGC 1052-DF4 is at 20.0 Mpc, the existence of both is in tension at ≥4.8σ with the ΛCDM model. If both galaxies are at 20.0 Mpc the ΛCDM cosmology has to be rejected by ≥5.8σ.
A multispectral analysis of the northeastern shell of IC 443
Authors: Alarie Alexandre , Drissen Laurent 
Published: August 2019

Abstract
We have carried out optical observations of the northeastern part of the supernova remnant IC 443 using the Canada–France–Hawaii Telescope imaging spectrograph SITELLE. The observations consist of three multispectral cubes covering an 11′ × 11′ area allowing the investigation of both the spatial and spectral variation of nine emission lines:  [O ii] λλ3726 + 3729,  [O iii] λλ4959, 5007,  H β,  H α,  [N ii] λλ6548, 6583, and  [S ii] λλ6716, 6731. Extinction measurement from the  H α/ H β shows significant variation across the observed region with E(B − V) = 0.8–1.1. Electron density measurements using  [S ii] lines indicate densities ranging from 100 up to 2500  cm−3. Models computed with the shock modelling code mappings are presented and compared with the observations. A combination of complete shock model and truncated ones is required in order to explain the observed spectrum. The shock velocities found in IC 443 are between 20 and 150  km s−1, with 75  km s−1 being the most prominent velocity. The pre-shock number density varies from 20 to 60  cm−3. A single set of abundances close to solar values combined with varying shock parameters (shock velocity, pre-shock density, and shock age) is sufficient to explain the great variation of line intensities observed in IC 443. Despite the relatively modest spectral resolution of the data (R ∼ 1500 at  H α), we clearly separate the red and blue velocity components of the expanding nebula, which show significant morphological differences.
Oxygen abundance and the N/C versus N/O relation for AFG supergiants and bright giants
Authors: Lyubimkov L S , Korotin S A , Lambert D L 
Published: August 2019

ABSTRACT
Non-LTE analysis (where LTE is local thermodynamic equilibrium) of the oxygen abundances for 51 Galactic A-, F- and G-type supergiants and bright giants is performed. In contrast with carbon and nitrogen, oxygen does not show any significant systematic anomalies in its abundances log ε(O). There is no marked difference from the initial oxygen abundance, within the errors, for the log ε(O) determination across the Teff interval from 4500–8500 K and the $\log \, g$ interval from 1.2–2.9 dex. This result agrees well with theoretical predictions for stellar models with rotation. With our new data for oxygen and our earlier non-LTE determinations of the N and C abundances for stars from the same sample, we constructed the [N/C] versus [N/O] relation for 17 stars. This relation is known to be a sensitive indicator of stellar evolution. A pronounced correlation between [N/C] versus [N/O] is found; the observed [N/C] increase from 0 to 1.6 dex is accompanied by a [N/O] increase from 0 to 0.9 dex. When comparing the observed [N/C] versus [N/O] relation with the theoretical one, we show that this relation reflects a strong dependence of the evolutionary changes in CNO abundances on the initial rotation velocities of stars. Given that the initial rotational velocities of these stars are expected to satisfy V0 < 150 km s−1, it is found that they are mostly post-first-dredge-up (post-FDU) objects. It is important that such initial velocities V0 are typical for about 80 per cent of the stars in question (i.e. stars with masses 4–19 M$\odot$). A constancy of the total C+N+O abundance during stellar evolution is confirmed. The mean value of log ε(C+N + O) = 8.97 ± 0.08 found for AFG supergiants and bright giants seems to be very close to the initial values of 8.92 (the Sun) or 8.94 (unevolved B-type main-sequence stars).
Variable jet Lorentz factors can explain soft self-absorbed radio spectra of accreting black holes
Authors: Zdziarski Andrzej A 
Published: August 2019

Abstract
We study the effect of variable jet bulk Lorentz factors, i.e. either jet acceleration or deceleration, on partially synchrotron self-absorbed radio spectra from cores of radio-loud active galactic nuclei and black hole binaries in the hard state. In about a half of quasars and radio galaxies, their core radio spectra are observed to be soft, i.e. have the spectral index of α &lt; 0. If they are emitted by jets with constant Lorentz factors, that softness implies deposition of large amounts of energy at large distances from the centre. We show here that such soft spectra can be explained without that energetic requirement by emission of jets with the Doppler factor increasing with the distance. This can happen for either jet acceleration or deceleration, depending on the jet viewing angle. We find our model can explain the quiescent radio to X-ray spectra of the BL Lac objects Mrk 421 and Mrk 501.
Comparative Genomic Characterization of the Multimammate Mouse Mastomys coucha
Authors: Hardin Aaron , Nevonen Kimberly A , Eckalbar Walter L , Carbone Lucia , Ahituv Nadav 
Published: August 2019

AbstractMastomys are the most widespread African rodent and carriers of various diseases such as the plague or Lassa virus. In addition, mastomys have rapidly gained a large number of mammary glands. Here, we generated a genome, variome, and transcriptomes for Mastomys coucha. As mastomys diverged at similar times from mouse and rat, we demonstrate their utility as a comparative genomic tool for these commonly used animal models. Furthermore, we identified over 500 mastomys accelerated regions, often residing near important mammary developmental genes or within their exons leading to protein sequence changes. Functional characterization of a noncoding mastomys accelerated region, located in the HoxD locus, showed enhancer activity in mouse developing mammary glands. Combined, our results provide genomic resources for mastomys and highlight their potential both as a comparative genomic tool and for the identification of mammary gland number determining factors.