bluuebunny/crossref_metadata_2025_split huggingface dataset:
A Multiwavelength Study of the Segue 3 Cluster
Authors: Hughes Joanne , Lacy Brianna , Sakari Charli , Wallerstein George , Davis Christoper Evan , Schiefelbein Spencer , Corrin Olivia , Joudi Hanah , Le Donna , Haynes Rose Marie 
Published: July 2017

Abstract
We present new SDSS and Washington photometry of the young outer-halo stellar system Segue 3. Combined with archival VI-observations, our most consistent results yield

,

,

, and

, with a high binary fraction of 0.39 ± 0.05 derived using the Padova models. We confirm that mass-segregation has occurred, supporting the hypothesis that this cluster is being tidally disrupted. A three-parameter King model yields a cluster radius of

, a core radius of

, and a tidal radius of

. A comparison of Padova and Dartmouth model-grids indicates that the cluster is not significantly α-enhanced, with a mean

dex, and a population age of only 2.6 ± 0.4 Gyr. We rule out a statistically significant age spread at the main-sequence turnoff because of a narrow subgiant branch, and discuss the role of stellar rotation and cluster age, using Dartmouth and Geneva models: approximately 70% of the Seg 3 stars at or below the main-sequence turnoff have enhanced rotation. Our results for Segue 3 indicate that it is younger and more metal-rich than all previous studies have reported to date. From colors involving Washington C and SDSS-u filters, we identify several giants and a possible blue straggler for future follow-up spectroscopic studies, and we produce spectral energy distributions of previously known members and potential Segue 3 sources with Washington (CT
1), Sloan (ugri), and VI-filters. Segue 3 shares the characteristics of unusual stellar systems that have likely been stripped from external dwarf galaxies as they are being accreted by the Milky Way, or that have been formed during such an event. Its youth, metallicity, and location are all inconsistent with Segue 3 being a cluster native to the Milky Way.
Core or Cusps: The Central Dark Matter Profile of a Strong Lensing Cluster with a Bright Central Image at Redshift 1
Authors: Collett Thomas E. , Buckley-Geer Elizabeth , Lin Huan , Bacon David , Nichol Robert C. , Nord Brian , Morice-Atkinson Xan , Amara Adam , Birrer Simon , Kuropatkin Nikolay , More Anupreeta , Papovich Casey , Romer Kathy K. , Tessore Nicolas , Abbott Tim M. C. , Allam Sahar , Annis James , Benoit-Lévy Aurlien , Brooks David , Burke David L. , Carrasco Kind Matias , Castander Francisco Javier J. , D’Andrea Chris B. , da Costa Luiz N. , Desai Shantanu , Diehl H. Thomas , Doel Peter , Eifler Tim F. , Flaugher Brenna , Frieman Josh , Gerdes David W. , Goldstein Daniel A. , Gruen Daniel , Gschwend Julia , Gutierrez Gaston , James David J. , Kuehn Kyler , Kuhlmann Steve , Lahav Ofer , Li Ting S. , Lima Marcos , Maia Marcio A. G. , March Marisa , Marshall Jennifer L. , Martini Paul , Melchior Peter , Miquel Ramon , Plazas Andrs A. , Rykoff Eli S. , Sanchez Eusebio , Scarpine Vic , Schindler Rafe , Schubnell Michael , Sevilla-Noarbe Ignacio , Smith Mathew , Sobreira Flavia , Suchyta Eric , Swanson Molly E. C. , Tarle Gregory , Tucker Douglas L. , Walker Alistair R. 
Published: July 2017

Abstract
We report on SPT-CLJ2011-5228, a giant system of arcs created by a cluster at z = 1.06. The arc system is notable for the presence of a bright central image. The source is a Lyman break galaxy at z

s
= 2.39 and the mass enclosed within the Einstein ring of radius 14 arcsec is

. We perform a full reconstruction of the light profile of the lensed images to precisely infer the parameters of the mass distribution. The brightness of the central image demands that the central total density profile of the lens be shallow. By fitting the dark matter as a generalized Navarro–Frenk–White profile—with a free parameter for the inner density slope—we find that the break radius is

kpc, and that the inner density falls with radius to the power −0.38 ± 0.04 at 68% confidence. Such a shallow profile is in strong tension with our understanding of relaxed cold dark matter halos; dark matter-only simulations predict that the inner density should fall as

. The tension can be alleviated if this cluster is in fact a merger; a two-halo model can also reconstruct the data, with both clumps (density varying as

and

) much more consistent with predictions from dark matter-only simulations. At the resolution of our Dark Energy Survey imaging, we are unable to choose between these two models, but we make predictions for forthcoming Hubble Space Telescope imaging that will decisively distinguish between them.
The Validity of 21 cm Spin Temperature as a Kinetic Temperature Indicator in Atomic and Molecular Gas
Authors: Shaw Gargi , Ferland G. J. , Hubeny I. 
Published: July 2017

Abstract
The gas kinetic temperature (T

K
) of various interstellar environments is often inferred from observations that can deduce level populations of atoms, ions, or molecules using spectral line observations; H i 21 cm is perhaps the most widely used, and has a long history. Usually the H i 21 cm line is assumed to be in thermal equilibrium and the populations are given by the Boltzmann distribution. A variety of processes, many involving Lyα, can affect the 21 cm line. Here we show how this is treated in the spectral simulation code Cloudy, and present numerical simulations of environments where this temperature indicator is used, with a detailed treatment of the physical processes that determine level populations within H0. We discuss situations where this temperature indicator traces T

K
, cases where it fails, as well as the effects of Lyα pumping on the 21 cm spin temperature. We also show that the Lyα excitation temperature rarely traces the gas kinetic temperature.
Study of the Vertical Magnetic Field in Face-on Galaxies Using Faraday Tomography
Authors: Ideguchi Shinsuke , Tashiro Yuichi , Akahori Takuya , Takahashi Keitaro , Ryu Dongsu 
Published: July 2017

Abstract
Faraday tomography allows astronomers to probe the distribution of the magnetic field along the line of sight (LOS), but that can be achieved only after the Faraday spectrum is interpreted. However, the interpretation is not straightforward, mainly because the Faraday spectrum is complicated due to a turbulent magnetic field; it ruins the one-to-one relation between the Faraday depth and the physical depth, and appears as many small-scale features in the Faraday spectrum. In this paper, by employing “simple toy models” for the magnetic field, we describe numerically as well as analytically the characteristic properties of the Faraday spectrum. We show that the Faraday spectrum along “multiple LOSs” can be used to extract the global properties of the magnetic field. Specifically, considering face-on spiral galaxies and modeling turbulent magnetic field as a random field with a single coherence length, we numerically calculate the Faraday spectrum along a number of LOSs and its shape-characterizing parameters, that is, the moments. When multiple LOSs cover a region of ≳(10 coherence length)2, the shape of the Faraday spectrum becomes smooth and the shape-characterizing parameters are well specified. With the Faraday spectrum constructed as a sum of Gaussian functions with different means and variances, we analytically show that the parameters are expressed in terms of the regular and turbulent components of the LOS magnetic field and the coherence length. We also consider the turbulent magnetic field modeled with a power-law spectrum, and study how the magnetic field is revealed in the Faraday spectrum. Our work suggests a way to obtain information on the magnetic field from a Faraday tomography study.
The Splashback Radius of Halos from Particle Dynamics. II. Dependence on Mass, Accretion Rate, Redshift, and Cosmology
Authors: Diemer Benedikt , Mansfield Philip , Kravtsov Andrey V. , More Surhud 
Published: July 2017

Abstract
The splashback radius R
sp, the apocentric radius of particles on their first orbit after falling into a dark matter halo, has recently been suggested to be a physically motivated halo boundary that separates accreting from orbiting material. Using the Sparta code presented in Paper I, we analyze the orbits of billions of particles in cosmological simulations of structure formation and measure R
sp for a large sample of halos that span a mass range from dwarf galaxy to massive cluster halos, reach redshift 8, and include WMAP, Planck, and self-similar cosmologies. We analyze the dependence of R
sp/R
200m and M
sp/M
200m on the mass accretion rate Γ, halo mass, redshift, and cosmology. The scatter in these relations varies between 0.02 and 0.1 dex. While we confirm the known trend that R
sp/R
200m decreases with Γ, the relationships turn out to be more complex than previously thought, demonstrating that R
sp is an independent definition of the halo boundary that cannot trivially be reconstructed from spherical overdensity definitions. We present fitting functions for R
sp/R
200m and M
sp/M
200m as a function of accretion rate, peak height, and redshift, achieving an accuracy of 5% or better everywhere in the parameter space explored. We discuss the physical meaning of the distribution of particle apocenters and show that the previously proposed definition of R
sp as the radius of the steepest logarithmic density slope encloses roughly three-quarters of the apocenters. Finally, we conclude that no analytical model presented thus far can fully explain our results.
A Three-dimensional View of Turbulence: Constraints on Turbulent Motions in the HD 163296 Protoplanetary Disk Using DCO+
Authors: Flaherty Kevin M. , Hughes A. Meredith , Rose Sanaea C. , Simon Jacob B. , Qi Chunhua , Andrews Sean M. , Kóspál Ágnes , Wilner David J. , Chiang Eugene , Armitage Philip J. , Bai Xue-ning 
Published: July 2017

Abstract
Gas kinematics are an important part of the planet formation process. Turbulence influences planetesimal growth and migration from the scale of submicron dust grains through gas-giant planets. Radio observations of resolved molecular line emission can directly measure this non-thermal motion and, taking advantage of the layered chemical structure of disks, different molecular lines can be combined to map the turbulence throughout the vertical extent of a protoplanetary disk. Here we present ALMA observations of three molecules (DCO+(3-2), C18O(2-1) and CO(2-1)) from the disk around HD 163296. We are able to place stringent upper limits (v
turb < 0.06c

s
, <0.05c

s
, and <0.04c

s
for CO(2-1), C18O(2-1), and DCO+(3-2) respectively), corresponding to α ≲ 3 × 10−3, similar to our prior limit derived from CO(3-2). This indicates that there is little turbulence throughout the vertical extent of the disk, contrary to theoretical predictions based on the magnetorotational instability and gravitoturbulence. In modeling the DCO+ emission, we also find that it is confined to three concentric rings at 65.7 ± 0.9 au,

, and 259 ± 1 au, indicative of a complex chemical environment.
LSPM J1314+1320: An Oversized Magnetic Star with Constraints on the Radio Emission Mechanism
Authors: MacDonald James , Mullan D. J. 
Published: July 2017

Abstract
LSPM J1314+1320 (=NLTT 33370) is a binary star system consisting of two nearly identical pre-main-sequence stars of spectral type M7. The system is remarkable among ultracool dwarfs for being the most luminous radio emitter over the widest frequency range. Masses and luminosities are at first sight consistent with the system being coeval at age ∼80 Myr according to standard (nonmagnetic) evolutionary models. However, these models predict an average effective temperature of ∼2950 K, which is 180 K hotter than the empirical value. Thus, the empirical radii are oversized relative to the standard models by ≈13%. We demonstrate that magnetic stellar models can quantitatively account for the oversizing. As a check on our models, we note that the radio emission limits the surface magnetic field strengths: the limits depend on identifying the radio emission mechanism. We find that the field strengths required by our magnetic models are too strong to be consistent with gyrosynchrotron emission but are consistent with electron cyclotron maser emission.
VICS82: The VISTA–CFHT Stripe 82 Near-infrared Survey
Authors: Geach J. E. , Lin Y.-T. , Makler M. , Kneib J.-P. , Ross N. P. , Wang W.-H. , Hsieh B.-C. , Leauthaud A. , Bundy K. , McCracken H. J. , Comparat J. , Caminha G. B. , Hudelot P. , Lin L. , Waerbeke L. Van , Pereira M. E. S. , Mast D. 
Published: July 2017

Abstract
We present the VISTA–CFHT Stripe 82 (VICS82) survey: a near-infrared (J+K

s
) survey covering 150 square degrees of the Sloan Digital Sky Survey (SDSS) equatorial Stripe 82 to an average depth of J = 21.9 AB mag and K

s
= 21.4 AB mag (80% completeness limits; 5σ point-source depths are approximately 0.5 mag brighter). VICS82 contributes to the growing legacy of multiwavelength data in the Stripe 82 footprint. The addition of near-infrared photometry to the existing SDSS Stripe 82 coadd ugriz photometry reduces the scatter in stellar mass estimates to

dex for galaxies with

at

, and offers improvement compared to optical-only estimates out to

, with stellar masses constrained within a factor of approximately 2.5. When combined with other multiwavelength imaging of the Stripe, including moderate-to-deep ultraviolet (GALEX), optical and mid-infrared (Spitzer-IRAC) coverage, as well as tens of thousands of spectroscopic redshifts, VICS82 gives access to approximately 0.5 Gpc3 of comoving volume. Some of the main science drivers of VICS82 include (a) measuring the stellar mass function of

galaxies out to

; (b) detecting intermediate-redshift quasars at

(c) measuring the stellar mass function and baryon census of clusters of galaxies, and (d) performing cross-correlation experiments of cosmic microwave background lensing in the optical/near-infrared that link stellar mass to large-scale dark matter structure. Here we define and describe the survey, highlight some early science results, and present the first public data release, which includes an SDSS-matched catalog as well as the calibrated pixel data themselves.
The Splashback Radius of Halos from Particle Dynamics. I. The SPARTA Algorithm
Authors: Diemer Benedikt 
Published: July 2017

Abstract
Motivated by the recent proposal of the splashback radius as a physical boundary of dark-matter halos, we present a parallel computer code for Subhalo and PARticle Trajectory Analysis (Sparta). The code analyzes the orbits of all simulation particles in all host halos, billions of orbits in the case of typical cosmological N-body simulations. Within this general framework, we develop an algorithm that accurately extracts the location of the first apocenter of particles after infall into a halo, or splashback. We define the splashback radius of a halo as the smoothed average of the apocenter radii of individual particles. This definition allows us to reliably measure the splashback radii of 95% of host halos above a resolution limit of 1000 particles. We show that, on average, the splashback radius and mass are converged to better than 5% accuracy with respect to mass resolution, snapshot spacing, and all free parameters of the method.
On the Evolution of the Central Density of Quiescent Galaxies
Authors: Tacchella Sandro , Carollo C. Marcella , Faber S. M. , Cibinel Anna , Dekel Avishai , Koo David C. , Renzini Alvio , Woo Joanna 
Published: July 2017

Abstract
We investigate the origin of the evolution of the population-averaged central stellar mass density (Σ1) of quiescent galaxies (QGs) by probing the relation between stellar age and Σ1 at z ∼ 0. We use the Zurich ENvironmental Study (ZENS), which is a survey of galaxy groups with a large fraction of satellite galaxies. QGs shape a narrow locus in the Σ1–M
⋆ plane, which we refer to as Σ1 ridgeline. Colors of (B − I) and (I − J) are used to divide QGs into three age categories: young (<2 Gyr), intermediate (2–4 Gyr), and old (>4 Gyr). At fixed stellar mass, old QGs on the Σ1 ridgeline have higher Σ1 than young QGs. This shows that galaxies landing on the Σ1 ridgeline at later epochs arrive with lower Σ1, which drives the zeropoint of the ridgeline down with time. We compare the present-day zeropoint of the oldest population at z = 0 with the zeropoint of the quiescent population 4 Gyr back in time, at z = 0.37. These zeropoints are identical, showing that the intrinsic evolution of individual galaxies after they arrive on the Σ1 ridgeline must be negligible, or must evolve parallel to the ridgeline during this interval. The observed evolution of the global zeropoint of 0.07 dex over the last 4 Gyr is thus largely due to the continuous addition of newly quenched galaxies with lower Σ1 at later times (“progenitor bias”). While these results refer to the satellite-rich ZENS sample as a whole, our work suggests a similar age–Σ1 trend for central galaxies.
Anomalous Distributions of Primary Cosmic Rays as Evidence for Time-dependent Particle Acceleration in Supernova Remnants
Authors: Zhang Yiran , Liu Siming , Yuan Qiang 
Published: July 2017

Abstract
Recent precise measurements of cosmic-ray (CR) spectra show that the energy distribution of protons is softer than those of heavier nuclei, and there are spectral hardenings for all nuclear compositions above ∼200 GV. Models proposed for these anomalies generally assume steady-state solutions of the particle acceleration process. We show that if the diffusion coefficient has a weak dependence on the particle rigidity near shock fronts of supernova remnants (SNRs), time-dependent solutions of the linear diffusive shock acceleration at two stages of SNR evolution can naturally account for these anomalies. The high-energy component of CRs is dominated by acceleration in the free expansion and adiabatic phases with enriched heavy elements and a high shock speed. The low-energy component may be attributed to acceleration by slow shocks propagating in dense molecular clouds with low metallicity in the radiative phase. Instead of a single power-law distribution, the spectra of time-dependent solutions soften gradually with the increase of energy, which may be responsible for the “knee” of CRs.
Encadrement et leadership
Authors: Piot Thierry 
Published: July 2017

Les environnements sociaux mouvants ont complexifié la gestion des établissements d’enseignement et de formation : la fonction de coordination pédagogique doit prendre en compte une tension entre les standards prescrits « par le haut » et les logiques d’individualisation « par le bas ». Nous avons analysé l’activité d’acteurs intermédiaires, des coordinateurs pédagogiques d’instituts de formation en soins infirmiers (IFSI) à partir de l’usage d’un instrument, le portfolio. Cet usage induit simultanément deux registres de transformation, directement issus de la double fonction médiatrice de l’instrument : l’un dirigé de manière externe, appelé processus d’instrumentation, concerne ce qui est transformé dans les situations de travail, sur le plan réel ou symbolique, lorsque l’instrument est utilisé ; l’autre registre de transformation, appelé processus d’instrumentalisation, est dirigé de manière interne, c’est-à-dire vers le sujet qui utilise l’instrument dans son travail : dans le cas présent nous nous sommes centré sur l’activité du coordinateur pédagogique. Par le fait d’utiliser un instrument, celui qui en fait usage voit se transformer ses schèmes d’action et ses schèmes de compréhension de l’action : il s’agit d’un enrichissement expérientiel, d’autant plus puissant qu’il s’accompagne d’un travail réflexif de conceptualisation de l’action.
Obesity Does Not Exacerbate the Protumorigenic Systemic Environment in Sarcoma Subjects
Authors: Buchta Claire M , Boi Shannon K , Miller Benjamin J , Milhem Mohammed M , Norian Lyse A 
Published: July 2017

Abstract
Sarcomas are a rare but fatal tumor type that accounts for &lt;1% of adult solid malignancies and ∼15% of childhood malignancies. Although the use of immunotherapy is being actively investigated for other solid tumors, advances in immunotherapy for sarcoma patients are lacking. To better understand the systemic immune environment in sarcoma patients, we performed a detailed multiplex analysis of serum cytokines, chemokines, and protumorigenic factors from treatment-naive subjects with localized, high-grade sarcoma. Because obesity is a major healthcare issue in the United States, we additionally examined the effects of obesity on serum protein profiles in our sarcoma subject cohort. We found that the systemic host environment is profoundly altered to favor tumor progression, with epidermal growth factor, angiopoietin-2, vascular endothelial growth factor A, IL-6, IL-8, and MIP-1β all increased relative to tumor-free controls (all p &lt; 0.05). Surprisingly, we found that obesity did not exacerbate this protumorigenic profile, as epidermal growth factor and IL-8 decreased with increasing subject body mass index (both p &lt; 0.05 versus normal or overweight subjects). The Th2-related cytokines IL-4, IL-5, and IL-13 were also decreased in the presence of obesity. Thus, although the systemic environment in sarcoma subjects favors tumor progression, obesity does not further aggravate the production of protumorigenic factors.
Rapid response to dexamethasone intravitreal implant in diabetic macular edema
Authors: Lo Giudice Giuseppe , Avarello Antonio , Campana Gianluca , Galan Alessandro 
Published: July 2017

Purpose: To evaluate the early effects of dexamethasone (DEX) intravitreal implants in patients with diabetic macular edema (DME). Methods: This was a prospective, single-arm, interventional clinical series. Eighteen patients (18 eyes) with chronic/recalcitrant or naive DME were included. Patients underwent single DEX intravitreal implant. Clinical assessments, including ophthalmologic examination, central retinal thickness (CRT) measurement by spectral-domain optical coherence tomography (SD-OCT) scan, best-corrected visual acuity (BCVA), and intraocular pressure (IOP) were carried out at baseline, 1-3 hours, and then 3, 7, and 30 days after treatment. The main outcome was change in CRT on SD-OCT, while secondary outcome measures included visual acuity (VA) and changes in IOP following implant. Results: Mean CRT significantly decreased from 565 ± 171 µm at baseline to 310 ± 89 µm at end of follow-up (p<0.001), with reduction becoming evident 1-3 hours after injection. Mean BCVA also significantly improved 7 days and 30 days after treatment up to 0.14 logMAR (p<0.05). All patients had a controlled IOP after the injection with only 1/18 eyes having a transient increase in IOP during follow-up. Conclusions: This is the first study showing very early effects of DEX implants on CRT reduction and VA improvement in DME.