bluuebunny/crossref_metadata_2025_split huggingface dataset:
Determining the Alpha to Proton Density Ratio for the New Horizons Solar Wind Observations
Authors: Elliott H. A. , Valek P. , McComas D. J. , Delamere P. A. , Bagenal F. , Gladstone G. R. , Olkin C. B. , Spencer J. , Stern S. A. , Young L. A. , Weaver H. A. , Ennico K. ,   New Horizons Plasma and Particle Team
Published: October 2018

Abstract
To help identify interplanetary coronal mass ejections (ICMEs) in New Horizons (NH) Solar Wind Around Pluto observations, we developed a method for determining the alpha to proton density ratio (n

α
/n

p
). Many common ICME signatures are derived from plasma and field parameters with values inside transient ICMEs distinct from values in the background solar wind. As the solar wind propagates, the plasma parameters evolve with increasing heliocentric distance, and ICMEs interact with the background solar wind. Some ICME signatures are based on composition such as the alpha (He++) to proton (H+) number density ratio, which is frequently enhanced in ICMEs. Intervals with enhanced n

α
/n

p
ratios persist into the outer heliosphere even though individual solar wind parameters evolve as solar wind propagates farther from the Sun. Overall, the solar wind expands as it propagates, but parcels of differing speeds dynamically interact, forming compressions and rarefactions, and altering the solar wind parameters. Both n

α
and n

p
change in lock step during such dynamic interactions, keeping the n

α
/n

p
ratio fixed. Our n

α
/n

p
results are consistent with prior missions, and we find that enhanced levels of n

α
/n

p
often occur within intervals of low proton temperature, which is the only other reliable ICME signature that NH can measure. Eventually, enhanced n

α
/n

p
values will likely become the most reliable ICME indicator for NH if the ICME temperatures become indistinguishable from background levels. NH is heading toward the Energetic Neutral Atom ribbon, and should have enough power to reach the termination shock.
Eclipsing Binaries in the Open Cluster Ruprecht 147. I. EPIC 219394517
Authors: Torres Guillermo , Curtis Jason L. , Vanderburg Andrew , Kraus Adam L. , Rizzuto Aaron 
Published: October 2018

Abstract
Eclipsing binaries in star clusters offer more stringent tests of stellar evolution theory than field binaries because models must not only match the binary properties, but also the radiative properties of all other cluster members at a single chemical composition and a single age. Here we report new spectroscopic observations of the G-type, detached eclipsing binary EPIC 219394517 in the open cluster Ruprecht 147 ([Fe/H] = +0.10), which was observed in late 2015 by the K2 mission. A joint analysis of our radial-velocity measurements and the K2 light curve shows the 6.5 day orbit to be nearly circular. We derive highly precise masses of

and

, radii of 1.055 ± 0.011

and 1.042 ± 0.012

, and effective temperatures of 5930 ± 100 K and 5880 ± 100 K for the primary and secondary, respectively. The distance we infer,

pc, corresponds to a parallax in good agreement with the Gaia/DR2 value for the star. Current stellar evolution models from the MIST and PARSEC series match the above physical properties well at ages of 2.48 and 2.65 Gyr. Isochrones for these same ages and the measured composition, along with our reddening estimate for EPIC 219394517, also show generally good agreement with the optical and near-infrared color–magnitude diagrams of the cluster, which can be constructed with no free parameters as the distances of all member stars are known from Gaia.
Planck 2015 Constraints on the Nonflat ϕCDM Inflation Model
Authors: Ooba Junpei , Ratra Bharat , Sugiyama Naoshi 
Published: October 2018

Abstract
We perform Markov chain Monte Carlo analyses to put constraints on the nonflat ϕCDM inflation model using Planck 2015 cosmic microwave background (CMB) anisotropy data and baryon acoustic oscillation distance measurements. The ϕCDM model is a consistent dynamical dark energy model in which the currently accelerating cosmological expansion is powered by a scalar field ϕ slowly rolling down an inverse power-law potential energy density. We also use a physically consistent power spectrum for energy density inhomogeneities in this nonflat model. We find that, like the closed-ΛCDM and closed-XCDM models, the closed-ϕCDM model provides a better fit to the lower multipole region of the CMB temperature anisotropy data compared to that provided by the tilted flat-ΛCDM model. Also, like the other closed models, this model reduces the tension between the Planck and the weak lensing σ
8 constraints. However, the higher multipole region of the CMB temperature anisotropy data are better fit by the tilted flat-Λ model than by the closed models.
X-Ray Observation of the 2017 November Glitch in the Crab Pulsar
Authors: Zhang Xinyuan , Shuai Ping , Huang Liangwei , Chen Shaolong , Du Yuanjie 
Published: October 2018

Abstract
We have observed a glitch in the Crab pulsar (PSR B0531+21) in the 0.5–10 keV X-ray band with the X-Ray Pulsar Navigation-I (XPNAV-1) satellite. This glitch occurred around 2017 November 8. Observations at radio frequency by the Jodrell Bank observatory and the Lovell telescope have confirmed it to be the largest ever observed. We report the results of X-ray observation of this glitch. The measured rotation frequency increase of the Crab is Δν
0 = (14.3 ± 2.0) × 10−6 Hz, corresponding to a fractional increase of Δν
0/ν
0 = (0.48 ± 0.09) × 10−6. Two transient components in the rotation frequency change are detected: one is the short transient term of Δν
n1 = 6.6 × 10−6 Hz with a timescale of 38.6 days and the other is the very short one of Δν
n2 = −1.35 × 10−6 Hz with a timescale of 2.4 days. The step change in the rotation frequency derivative is determined to be

Hz s−1. We also examine the relationship between the persistent offset

and Δν
0, giving

. No significant X-ray flux changes are observed pre- and post-glitch.
Variable Heating and Flaring of Three Redback Millisecond Pulsar Companions
Authors: Cho Patricia B. , Halpern Jules P. , Bogdanov Slavko 
Published: October 2018

Abstract
We monitor established and putative redback millisecond pulsars (MSPs) in time-series photometry, repeatedly covering their 5–6 hr orbital light curves in r′ or R. On timescales of months, PSR J1048+2339 and XMMU J083850.38−282756.8 exhibit similar variability of ≈0.3 mag on the heated side of the companion star. However, the heating light curve is rarely symmetric, suggesting that the intrabinary shock generated by the pulsar wind is skewed in addition to being variable, or that changing magnetic fields intrinsic to the companion channel the pulsar wind. In addition to this variable heating, there are long-lived flaring states that increase the brightness by an additional 0.5 mag, with variability on ≈10 min timescales. These flares also appear to originate on the heated side of the companion, while the “night”-side brightness remains relatively stable. Somewhat less active, PSR J1628−3205 has an optical light curve that is dominated by tidal distortion (ellipsoidal modulation), although it too shows evidence of variable and asymmetric heating due to shifting magnetic fields or migrating star spots. These effects frustrate any effort to derive system parameters such as inclination angle and Roche-lobe filling factor from optical light curves of redback MSPs. We also report on two Chandra X-ray observations of PSR J1048+2339 that show strong orbital modulation, possibly due to beaming along the intrabinary shock, and a third observation that is dominated by flaring. The peak flare luminosity in the 0.3–8 keV band is ≈12% of the pulsar’s spin-down power, which may require magnetic reconnection. None of these three systems has yet shown a transition back to an accreting state.
Solar Wind Turbulence Studies Using MMS Fast Plasma Investigation Data
Authors: Bandyopadhyay Riddhi , Chasapis A. , Chhiber R. , Parashar T. N. , Maruca B. A. , Matthaeus W. H. , Schwartz S. J. , Eriksson S. , Le Contel O. , Breuillard H. , Burch J. L. , Moore T. E. , Pollock C. J. , Giles B. L. , Paterson W. R. , Dorelli J. , Gershman D. J. , Torbert R. B. , Russell C. T. , Strangeway R. J. 
Published: October 2018

Abstract
Studies of solar wind turbulence traditionally employ high-resolution magnetic field data, but high-resolution measurements of ion and electron moments have been possible only recently. We report the first turbulence studies of ion and electron velocity moments accumulated in pristine solar wind by the Fast Plasma Investigation (FPI) instrument on board the Magnetospheric Multiscale Mission. Use of these data is made possible by a novel implementation of a frequency domain Hampel filter, described herein. After presenting procedures for processing of the data, we discuss statistical properties of solar wind turbulence extending into the kinetic range. Magnetic field fluctuations dominate electron and ion-velocity fluctuation spectra throughout the energy-containing and inertial ranges. However, a multispacecraft analysis indicates that at scales shorter than the ion inertial length, electron velocity fluctuations become larger than ion-velocity and magnetic field fluctuations. The kurtosis of ion-velocity peaks around a few ion inertial lengths and returns to a near Gaussian value at sub-ion scales.
Molecular Gas and Star Formation Properties in Early Stage Mergers: SMA CO(2-1) Observations of the LIRGs NGC 3110 and NGC 232
Authors: Espada Daniel , Martin Sergio , Verley Simon , Pettitt Alex R. , Matsushita Satoki , Argudo-Fernández Maria , Randriamanakoto Zara , Hsieh Pei-Ying , Saito Toshiki , Miura Rie E. , Kawana Yuka , Sabater Jose , Verdes-Montenegro Lourdes , Ho Paul T. P. , Kawabe Ryohei , Iono Daisuke 
Published: October 2018

Abstract
Mergers of galaxies are an important mode for galaxy evolution because they serve as an efficient trigger of powerful starbursts. However, observational studies of molecular gas properties during their early stages are scarce. We present interferometric CO(2–1) maps of two luminous infrared galaxies, NGC 3110 and NGC 232, obtained with the Submillimeter Array with ∼1 kpc resolution. While NGC 3110 is a spiral galaxy interacting with a minor (14:1 stellar mass) companion, NGC 232 is interacting with a similarly sized object. We find that such interactions in these galaxies have likely induced enhancements in the molecular gas content and central concentrations, partly at the expense of atomic gas. The obtained molecular gas surface densities in their circumnuclear regions are Σmol ≳ 102.5
M
⊙ pc−2, higher than in noninteracting objects by an order of magnitude. Gas depletion times of 0.5–1 Gyr are found for the different regions, lying in between noninteracting disk galaxies and the starburst sequence. In the case of NGC 3110, the spiral arms show on average 0.5 dex shorter depletion times than in the circumnuclear regions if we assume a similar H2–CO conversion factor. We show that even in the early stages of the interaction with a minor companion, a starburst is formed along the circumnuclear region and spiral arms, where a large population of SSCs is found (∼350), and at the same time a large central gas concentration is building up that might be the fuel for an active galactic nucleus. The main morphological properties of the NGC 3110 system are reproduced by our numerical simulations and allow us to estimate that the current epoch of the interaction is at ∼150 Myr after closest approach.
A Morphological Study of the Supernova Remnant Rx J0852.0–4622 (Vela Jr.)
Authors: Maxted Nigel I. , Filipović M. D. , Sano H. , Allen G. E. , Pannuti T. G. , Rowell G. P. , Grech A. , Roper Q. , Wong G. F. , Galvin T. J. , Fukui Y. , Collier J. D. , Crawford E. J. , Grieve K. , Horta A. D. , Manojlović P. , O’Brien A. 
Published: October 2018

Abstract
We conduct a multiwavelength morphological study of the Galactic supernova remnant (SNR) RX J0852.0–4622 (also known as Vela Jr., Vela Z, and G266.2−1.2). RX J0852.0–4622 is coincident with the edge of the larger Vela SNR causing confusion in the attribution of some filamentary structures to either RX J0852.0–4622 or its larger sibling. We find that the RX J0852.0–4622 radio-continuum emission can be characterized by a two-dimensional shell with a radius of 0.°90 ± 0.°01 (or 11.8 ± 0.6 pc at an assumed distance of 750 pc) centered at (l, b) = (133.°08 ± 0.°01,−46.°34 ± 0.°01) (or R.A. = 8h52m19.ˢ2, decl. = −46°20′24.″0, J2000), consistent with X-ray and gamma-ray emission. Although [O iii] emission features are generally associated with the Vela SNR, one particular [O iii] emission feature, which we denote as “the Vela Claw,” morphologically matches a molecular clump that is thought to have been stripped by the stellar progenitor of the RX J0852.0–4622 SNR. We argue that the Vela Claw feature is possibly associated with RX J0852.0–4622. Toward the northwestern edge of RX J0852.0–4622 , we find a flattening of the radio spectral index toward another molecular clump also thought to be associated with RX J0852.0–4622 . It is currently unclear whether this feature and the Vela Claw result from interactions between the RX J0852.0–4622 shock and interstellar medium gas.
The Lick AGN Monitoring Project 2011: Dynamical Modeling of the Broad-line Region
Authors: Williams Peter R. , Pancoast Anna , Treu Tommaso , Brewer Brendon J. , Barth Aaron J. , Bennert Vardha N. , Buehler Tabitha , Canalizo Gabriela , Cenko S. Bradley , Clubb Kelsey I. , Cooper Michael C. , Filippenko Alexei V. , Gates Elinor , Hoenig Sebastian F. , Joner Michael D. , Kandrashoff Michael T. , Laney Clifton David , Lazarova Mariana S. , Li Weidong , Malkan Matthew A. , Rex Jacob , Silverman Jeffrey M. , Tollerud Erik , Walsh Jonelle L. , Woo Jong-Hak 
Published: October 2018

Abstract
We present models of the Hβ-emitting broad-line region (BLR) in seven Seyfert 1 galaxies from the Lick AGN Monitoring Project 2011 sample, drawing inferences on the BLR structure and dynamics as well as the mass of the central supermassive black hole. We find that the BLR is generally a thick disk, viewed close to face-on, with preferential emission back toward the ionizing source. The dynamics in our sample range from near-circular elliptical orbits to inflowing or outflowing trajectories. We measure black hole masses of

for PG 1310−108,

for Mrk 50,

for Mrk 141,

for Mrk 279,

for Mrk 1511,

for NGC 4593, and

for Zw 229−015. We use these black hole mass measurements along with cross-correlation time lags and line widths to recover the scale factor f used in traditional reverberation mapping measurements. Combining our results with other studies that use this modeling technique, which brings our sample size to 16, we calculate a scale factor that can be used for measuring black hole masses in other reverberation mapping campaigns. When using the root-mean-square (rms) spectrum and using the line dispersion to measure the line width, we find

pred = 0.57 ± 0.19. Finally, we search for correlations between f and other AGN and BLR parameters and find marginal evidence that f is correlated with M
BH and the BLR inclination angle, but no significant evidence of a correlation with the AGN luminosity or Eddington ratio.
The 7-year MAXI/GSC X-Ray Source Catalog in the High Galactic Latitude Sky (3MAXI)
Authors: Kawamuro T. , Ueda Y. , Shidatsu M. , Hori T. , Morii M. , Nakahira S. , Isobe N. , Kawai N. , Mihara T. , Matsuoka M. , Morita T. , Nakajima M. , Negoro H. , Oda S. , Sakamoto T. , Serino M. , Sugizaki M. , Tanimoto A. , Tomida H. , Tsuboi Y. , Tsunemi H. , Ueno S. , Yamaoka K. , Yamada S. , Yoshida A. , Iwakiri W. , Kawakubo Y. , Sugawara Y. , Sugita S. , Tachibana Y. , Yoshii T. 
Published: October 2018

Abstract
We present the third MAXI/GSC catalog in the high Galactic latitude sky (

) based on the 7-year data from 2009 August 13 to 2016 July 31, complementary to that in the low Galactic latitude sky (

) (Hori et al. 2018). We compile 682 sources detected at significances of s
D,4–10 keV ≥ 6.5 in the 4–10 keV band. A two-dimensional image fit based on the Poisson likelihood algorithm (C-statistics) is adopted for the detections and constraints on their fluxes and positions. The 4–10 keV sensitivity reaches ≈0.48 mCrab, or ≈5.9 × 10−12 erg cm−2 s−1, over half of the survey area. Compared with the 37-month Hiroi et al. (2013) catalog, which adopted a threshold of s
D,4–10 keV ≥ 7, the source number increases by a factor of ∼1.4. The fluxes in the 3–4 keV and 10–20 keV bands are further estimated, and hardness ratios (HRs) are calculated using the 3–4 keV, 4–10 keV, 3–10 keV, and 10–20 keV band fluxes. We also make the 4–10 keV light curves in 1-year bins for all the sources and characterize their variabilities with an index based on a likelihood function and the excess variance. Possible counterparts are found from five major X-ray survey catalogs by Swift, Uhuru, RXTE, XMM-Newton, and ROSAT, as well as an X-ray galaxy cluster catalog (MCXC). Our catalog provides the fluxes, positions, detection significances, HRs, 1-year bin light curves, variability indices, and counterpart candidates.
3C 17: The BCG of a Galaxy Cluster at z = 0.22
Authors: Madrid Juan P. , Donzelli Carlos J. , Rodríguez-Ardila Alberto , Paggi Alessandro , Massaro Francesco , Schirmer Mischa 
Published: October 2018

Abstract
Gemini Multi Object Spectrograph medium-resolution spectra and photometric data of 39 objects in the field of the radio galaxy 3C 17 are presented. Based on the new data, a previously uncataloged cluster of galaxies is identified at a mean redshift of z = 0.220 ± 0.003, a projected virial radius of 0.37 Mpc, and a velocity dispersion of σ

v
= 821 ± 171 km s−1. The brightest member of this cluster is 3C 17, with M

r
= −22.45 mag. The surface brightness profile of 3C 17 is best fit with two components (Exponential + Sérsic) characteristic of brightest cluster galaxies. The spectrum of 3C 17 is dominated by broad emission lines Hα + N[ ii] and Hβ + [O iii]. Analysis of Chandra data shows extended emission around the cluster core that supports the existence of hot gas cospatial with 3C 17. The discovery of a cluster of galaxies around 3C 17 better explains the sharply bent morphology of the radio jet given that it propagates through a dense intracluster medium.
An online method database for mapping and assessing ecosystem services
Authors: Reichel Steffen , Klug Hermann 
Published: October 2018

Since the foundation of the ecosystem services concept in the ninetieth of the last century (Costanza et al. 1998, Costanza et al. 1997, de Groot 1992), many methods to map and assess ecosystem services have been developed and applied to policy and business questions worldwide. While many flexible methods exist at different spatial scales and ecosystem types, Jax et al. (2018) express the difficulty in choosing and applying the correct method to the right topic of interest. To enable a selection of appropriate methods, Harrison et al. (2018) developed a decision tree approach. However, Dunford et al. (2018) argue that often not a single method but a combination of methods are required for appropriate decision-making in real world situations. Thus, applying the concept of ecosystem services in practice is challenging, especially at institutional level (Saarikoski et al. 2018). This hampers comparability, applicability and transferability of ecosystem services assessments and related mapping applications across scales and European regions. It also impedes a solid overview of existing methods suitable for use at different scales in different biomes and types of ecosystems. These challenges require a consistent knowledge capitalisation infrastructure, where information is synthesised in a publicly accessible portal to enable a consistent description of different ecosystem conditions and the services they provide.
Going beyond the previously mentioned challenges requires a flexible methodology for assessing and mapping ecosystem services. The Horizon 2020 project ESMERALDA (Enhancing ecoSysteM sERvices mApping for poLicy and Decision mAking) developed this methodology and implemented it into the "MAES explorer"*5 and the "MAES Methods Explorer*1 (MME)". The MME complements previous developments from the EU projects OpenNESS*2 and OPERAs*3. In contrast to the OPPLA*4 case-study-finder with case study areas and accompanied study area booklets and descriptions, MME focuses on methods for mapping and assessing ecosystem services and links those to selected literature and case studies. Additionally, MME provides a comprehensive and publicly searchable collection of peer-reviewed journal references and grey literature about mapping and assessing ecosystem services in Europe. This compilation is cross-related with the case study booklets produced by the ESMERALDA project and particularly methods, which are specifically used to assess and map particular ecosystem services within the case study area. Thus, searching for and filtering of particular case study areas, (related) literature references and/or methods is possible. Santos-Martin et al. (2018) provide the detailed description about the scientific procedure behind the MME tool described here.
The Mitochondrial Isoform of FASTK Modulates Nonopsonic Phagocytosis of Bacteria by Macrophages via Regulation of Respiratory Complex I
Authors: García Del Río Ana , Delmiro Aitor , Martín Miguel Angel , Cantalapiedra Roberto , Carretero Raquel , Durántez Carlos , Menegotto Fabiola , Morán María , Serrano-Lorenzo Pablo , De la Fuente Miguel Angel , Orduña Antonio , Simarro María 
Published: October 2018

Abstract
Phagocytosis is a pivotal process by which innate immune cells eliminate bacteria. In this study, we explore novel regulatory mechanisms of phagocytosis driven by the mitochondria. Fas-activated serine/threonine kinase (FASTK) is an RNA-binding protein with two isoforms, one localized to the mitochondria (mitoFASTK) and the other isoform to cytosol and nucleus. The mitoFASTK isoform has been reported to be necessary for the biogenesis of the mitochondrial ND6 mRNA, which encodes an essential subunit of mitochondrial respiratory complex I (CI, NADH:ubiquinone oxidoreductase). This study investigates the role and the mechanisms of action of FASTK in phagocytosis. Macrophages from FASTK─/─ mice exhibited a marked increase in nonopsonic phagocytosis of bacteria. As expected, CI activity was specifically reduced by almost 50% in those cells. To explore if decreased CI activity could underlie the phagocytic phenotype, we tested the effect of CI inhibition on phagocytosis. Indeed, treatment with CI inhibitor rotenone or short hairpin RNAs against two CI subunits (NDUFS3 and NDUFS4) resulted in a marked increase in nonopsonic phagocytosis of bacteria. Importantly, re-expression of mitoFASTK in FASTK-depleted macrophages was sufficient to rescue the phagocytic phenotype. In addition, we also report that the decrease in CI activity in FASTK─/─ macrophages is associated with an increase in phosphorylation of the energy sensor AMP-activated protein kinase (AMPK) and that its inhibition using Compound C reverted the phagocytosis phenotype. Taken together, our results clearly demonstrate for the first time, to our knowledge, that mitoFASTK plays a negative regulatory role on nonopsonic phagocytosis of bacteria in macrophages through its action on CI activity.