bluuebunny/crossref_metadata_2025_split huggingface dataset:
Memandang Penderitaan Melalui Perspektif The Already and The Not Yet dari Rasul Paulus
Authors: Limasaputra Alexander Darmawan 
Published: September 2019

Penderitaan merupakan peristiwa yang dapat dialami setiap orang. Penderitaan telah membuat orang menangis, mempertanyakan atau bahkan meninggalkan Allah. Apakah penderitaan menjadi bukti bahwa Allah tidak ada? Bukankah kalau Allah ada maka penderitaan tidak ada? Apakah penderitaan menjadi bukti bahwa Allah sudah kalah dan tidak lagi berkuasa atas dunia? Artikel ini akan menjawab pertanyaan-pertanyaan tersebut melalui perspektif the already and the not yet dari rasul Paulus. Penulis menjelaskan bahwa penderitaan merupakan panggilan orang percaya karena berada di masa the already and the not yet, yaitu masa di mana Yesus Kristus telah menang atas kuasa dosa, kutuk alam semesta dan pemerintahan Iblis serta merupakan masa hadirnya pemerintahan Allah di dunia, meski semua ini belum mencapai kepenuhannya. Karena itu orang percaya tidak perlu takut atau meninggalkan iman Kristen. Kata-kata kunci: Penderitaan, Paulus, Eskatologi, The Already and the Not Yet, Ciptaan Baru, Pemerintahan Allah, Pemerintahan Iblis, Kuasa Dosa, Kutuk Alam Semesta Suffering is something that is experienced by everyone. Suffering has made people cry out to God, question God or even leave God. Does suffering prove that God does not exist? Doesn’t God’s existence nullify suffering? Does suffering prove that God is impotent and no longer has power over the world? This article will address these questions through the framework of the already and the not yet schema developed by the apostle Paul. The author explains that suffering is a part of the call of believers because it is experienced between the time of the already and the not yet. A period when Jesus Christ has won over the power of sin, the curse of the universe and the government of Satan and is the time of God’s government in the world, even though all this has not yet reached fullness. Therefore, believers need not fear suffering nor leave the Christian faith because of it. Keywords: Suffering, Paul, Eschatology, The Already and the Not Yet, New Creation, God’s Rule, Satan’s Rule, Power of Sin, Curse on Creation
Gereja Di Rumah: Kontekstualisasi Fungsi-Fungsi Rumah Dalam Masa Perjanjian Baru Untuk Pekabaran Injil
Authors: Hidajat Djeffry 
Published: September 2019

Gereja dalam Perjanjian Baru adalah gereja di rumah. Mengapa murid-murid Yesus dan Paulus menggunakan rumah untuk kegiatan gereja? Mereka menggunakan rumah karena rumah adalah unit sosial, ekonomi dan religius. Ibadah dan pengajaran rohani biasa diadakan dalam rumah-rumah pada waktu itu. Karena fungsi sosial dan ekonominya, rumah juga membuka kontak dan komunikasi bagi para penginjil untuk memberitakan tentang Injil Yesus Kristus kepada jaringan sosial rumah di mana mereka melayani. Dengan demikian murid-murid Yesus dan Paulus telah melakukan upaya kontekstual yang cerdas dengan menggunakan rumah untuk membangun komunitas Kristen sekaligus pekabaran Injil. Terbukti kekristenan diterima secara luas dengan pendekatan gereja di rumah ini di tiga abad pertama sejarah kekristenan.
The churches in New Testament times met together within houses. Why did Jesus’ disciples and Paul utilize the house for the church’s activities? They did so because the house was the foundational unit pertaining to the social, economic, and religious structures of society. The house was commonplace that could be used for worship and religious teaching. Moreover, because of the social and economic functions of the household, the house provided a sphere of easy interaction and communication with others in order to evangelize them with the Gospel of Jesus Christ. Thus, the disciples and Paul are facilitating contextualized structures in their use of the housing unit for the building of Christian community and evangelization. This effectiveness can be evidenced by the wide acceptance of Christianity throughout the first three centuries of Christianity.
Online panels in social science research: Expanding sampling methods beyond Mechanical Turk
Authors: Chandler Jesse , Rosenzweig Cheskie , Moss Aaron J. , Robinson Jonathan , Litman Leib 
Published: September 2019

AbstractAmazon Mechanical Turk (MTurk) is widely used by behavioral scientists to recruit research participants. MTurk offers advantages over traditional student subject pools, but it also has important limitations. In particular, the MTurk population is small and potentially overused, and some groups of interest to behavioral scientists are underrepresented and difficult to recruit. Here we examined whether online research panels can avoid these limitations. Specifically, we compared sample composition, data quality (measured by effect sizes, internal reliability, and attention checks), and the non-naivete of participants recruited from MTurk and Prime Panels—an aggregate of online research panels. Prime Panels participants were more diverse in age, family composition, religiosity, education, and political attitudes. Prime Panels participants also reported less exposure to classic protocols and produced larger effect sizes, but only after screening out several participants who failed a screening task. We conclude that online research panels offer a unique opportunity for research, yet one with some important trade-offs.
A Pluto–Charon Sonata. III. Growth of Charon from a Circum-Pluto Ring of Debris
Authors: Kenyon Scott J. , Bromley Benjamin C. 
Published: September 2019

Abstract
Current theory considers two options for the formation of the Pluto–Charon binary. In the hit-and-run model, a lower mass projectile barely hits the more massive Pluto, kicks up some debris, and remains bound to Pluto. In a graze-and-merge scenario, the projectile ejects substantial debris as it merges with Pluto. To investigate the graze-and-merge idea in more detail, we consider the growth of Charon-mass objects within a circum-Pluto ring of solids. Numerical calculations demonstrate that Charon analogs form rapidly within a swarm of planetesimals with initial radii r
0 ≈ 145–230 km. On timescales of ∼30–100 days, newly formed Charon analogs have semimajor axes, a ≈ 5–6 r

P
, and orbital eccentricities, e ≈ 0.1–0.3, similar to Charon analogs that remain bound after hit-and-run collisions with Pluto. Although the early growth of Charon analogs generates rings of small particles at a ≈ 50–275 r

P
, ejection of several 145–230 km leftovers by the central Pluto–Charon binary removes these small solids in 10–100 yr. Simple estimates suggest that small particles might survive the passage of 10–20 km objects ejected by the central binary. Our results indicate that the Pluto–Charon circumbinary satellite system was not formed by a graze-and-merge impact when the formation of Charon within a circum-Pluto disk leads to the ejection of several 100–200 km particles through the orbital plane of the Pluto–Charon binary. If a growing Charon ejects only much smaller particles, however, graze-and-merge impacts are a plausible formation channel for the Pluto–Charon binary and an ensemble of small, circumbinary satellites.
A Recipe for Finding Stellar Radii, Temperatures, Surface Gravities, Metallicities, and Masses Using Spectral Lines
Authors: Gray David F. , Kaur Taranpreet 
Published: September 2019

Abstract
A recipe based on physical principles employs the observed equivalent widths of 10 spectral lines to model the photosphere of a target star. Coupled with the visual magnitude and an absolute flux calibration, the recipe yields the angular radius, effective temperature, surface gravity, and metallicity. With the addition of a parallax, a linear radius and a mass estimate are added to the results. The method is applied to a sample of 26 G and K stars that span luminosity classes V to IIIa. The recipe-determined angular radii agree with the interferometer radii and have comparable errors. But unlike interferometers, the recipe is not limited to sizes ≳1 mas. The veracity of the other recipe-derived parameters is supported by numerous comparisons with previously published values.
The ALMA Spectroscopic Survey in the HUDF: the Molecular Gas Content of Galaxies and Tensions with IllustrisTNG and the Santa Cruz SAM
Authors: Popping Gergö , Pillepich Annalisa , Somerville Rachel S. , Decarli Roberto , Walter Fabian , Aravena Manuel , Carilli Chris , Cox Pierre , Nelson Dylan , Riechers Dominik , Weiss Axel , Boogaard Leindert , Bouwens Richard , Contini Thierry , Cortes Paulo C. , Cunha Elisabete da , Daddi Emanuele , Díaz-Santos Tanio , Diemer Benedikt , González-López Jorge , Hernquist Lars , Ivison Rob , Fèvre Olivier Le , Marinacci Federico , Rix Hans-Walter , Swinbank Mark , Vogelsberger Mark , Werf Paul van der , Wagg Jeff , Yung L. Y. Aaron 
Published: September 2019

Abstract
The ALMA Spectroscopic Survey in the Hubble Ultra Deep Field (ASPECS) provides new constraints for galaxy formation models on the molecular gas properties of galaxies. We compare results from ASPECS to predictions from two cosmological galaxy formation models: the IllustrisTNG hydrodynamical simulations and the Santa Cruz semianalytic model (SC SAM). We explore several recipes to model the H2 content of galaxies, finding them to be consistent with one another, and take into account the sensitivity limits and survey area of ASPECS. For a canonical CO-to-H2 conversion factor of α
CO = 3.6 M
⊙/(K km s−1 pc2) the results of our work include: (1) the H2 mass of z > 1 galaxies predicted by the models as a function of their stellar mass is a factor of 2–3 lower than observed; (2) the models do not reproduce the number of H2-rich (

) galaxies observed by ASPECS; (3) the H2 cosmic density evolution predicted by IllustrisTNG (the SC SAM) is in tension (in tension but with less disagreement than IllustrisTNG) with the observed cosmic density, even after accounting for the ASPECS selection function and field-to-field variance effects. The tension between models and observations at z > 1 can be alleviated by adopting a CO-to-H2 conversion factor in the range α
CO = 2.0–0.8 M
⊙/(K km s−1 pc2). Additional work on constraining the CO-to-H2 conversion factor and CO excitation conditions of galaxies through observations and theory will be necessary to more robustly test the success of galaxy formation models.
The ALMA Spectroscopic Survey in the HUDF: CO Luminosity Functions and the Molecular Gas Content of Galaxies through Cosmic History
Authors: Decarli Roberto , Walter Fabian , Gónzalez-López Jorge , Aravena Manuel , Boogaard Leindert , Carilli Chris , Cox Pierre , Daddi Emanuele , Popping Gergö , Riechers Dominik , Uzgil Bade , Weiss Axel , Assef Roberto J. , Bacon Roland , Bauer Franz Erik , Bertoldi Frank , Bouwens Rychard , Contini Thierry , Cortes Paulo C. , Cunha Elisabete da , Díaz-Santos Tanio , Elbaz David , Inami Hanae , Hodge Jacqueline , Ivison Rob , Fèvre Olivier Le , Magnelli Benjamin , Novak Mladen , Oesch Pascal , Rix Hans-Walter , Sargent Mark T. , Smail Ian , Swinbank A. Mark , Somerville Rachel S. , Werf Paul van der , Wagg Jeff , Wisotzki Lutz 
Published: September 2019

Abstract
We use the results from the ALMA large program ASPECS, the spectroscopic survey in the Hubble Ultra Deep Field (HUDF), to constrain CO luminosity functions of galaxies and the resulting redshift evolution of ρ(H2). The broad frequency range covered enables us to identify CO emission lines of different rotational transitions in the HUDF at z > 1. We find strong evidence that the CO luminosity function evolves with redshift, with the knee of the CO luminosity function decreasing in luminosity by an order of magnitude from ∼2 to the local universe. Based on Schechter fits, we estimate that our observations recover the majority (up to ∼90%, depending on the assumptions on the faint end) of the total cosmic CO luminosity at z = 1.0–3.1. After correcting for CO excitation, and adopting a Galactic CO-to-H2 conversion factor, we constrain the evolution of the cosmic molecular gas density ρ(H2): this cosmic gas density peaks at z ∼ 1.5 and drops by a factor of

to the value measured locally. The observed evolution in ρ(H2), therefore, closely matches the evolution of the cosmic star formation rate density ρ
SFR. We verify the robustness of our result with respect to assumptions on source inclusion and/or CO excitation. As the cosmic star formation history can be expressed as the product of the star formation efficiency and the cosmic density of molecular gas, the similar evolution of ρ(H2) and ρ
SFR leaves only little room for a significant evolution of the average star formation efficiency in galaxies since z ∼ 3 (85% of cosmic history).
SDSS IV MaNGA: Star-formation-driven Biconical Outflows in the Local Universe
Authors: Bizyaev Dmitry , Chen Yan-Mei , Shi Yong , Riffel Rogemar A. , Riffel Rogerio , Diamond-Stanic Aleksandar M. , Roy Namrata 
Published: September 2019

Abstract
We present a sample of 48 nearby galaxies with central, biconical outflows identified by the Mapping Nearby Galaxies at APO survey. All considered galaxies have star-formation-driven biconical (SFB) central outflows, with no signs of an active galactic nucleus. We find that the SFB outflows require high central concentration of the star formation rate. This increases the gas velocity dispersion over the equilibrium limit and helps maintain the gas outflows. The central starbursts increase the metallicity, extinction, and the [α/Fe] ratio in the gas. A significant amount of young stellar population at the centers suggests that the SFBs are associated with the formation of young bulges in galaxies. More than 70% of SFB galaxies are group members or have companions with no prominent interaction, or show asymmetry of external isophotes. In 15% of SFB cases, stars and gas rotate in the opposite directions, which points at the gas infall from satellites as the primary reason for triggering the SFB phenomena.
Rapidly Accreting Black Hole of the Lyα-luminous Quasar PSOJ006.1240+39.2219
Authors: Koptelova Ekaterina , Hwang Chorng-Yuan , Malkan Matthew A. , Yu Po-Chieh 
Published: September 2019

Abstract
We present near-infrared 1.1–1.3 and 1.3–1.6 μm spectra of the Lyα-luminous quasar PSO J006.1240+39.2219 at z = 6.617 ± 0.003 obtained with the NIRSPEC spectrograph at the Keck II telescope. The spectra cover the C iv
λ1549, C iii] λ1909 emission lines and part of the UV continuum of the quasar. From the NIRSPEC observations of PSO J006.1240+39.2219, we constrain the spectral slope of its UV continuum to be α

λ
= −1.35 ± 0.26 and measure an absolute magnitude of M
1450 = −25.60. Using the scaling relation between black hole mass, width of the C iv line and ultraviolet continuum luminosity, we derive a black hole mass of (2.19 ± 0.30) × 108
M
⊙, which is consistent but somewhat smaller than the typical black hole masses of z ≳ 6 quasars of similar luminosities. The inferred accretion rate of L
Bol/L
Edd ≳ 2 indicates that PSO J006.1240+39.2219 is in the phase of the rapid growth of its supermassive black hole characterized by the high N v/C iv line ratio, N v/C iv > 1, and the lower level of ionization of its circumnuclear gas than in other high-redshift luminous quasars. The N v/C iv line ratio of PSO J006.1240+39.2219 implies a relatively high abundance of nitrogen in its circumnuclear gas. This abundance might be produced by the post-starburst population of stars that provide the fuel for black hole accretion.
Influence of Magnetic Reconnection-accelerated Electrons in Solar Wind on Onset Time Analysis of Impulsive Electron Events
Authors: Tan Lun C. 
Published: September 2019

Abstract
Observations have shown that type III radio bursts (RBs) are generated by 1–10 keV flare electrons ejected from the exhaust of a magnetic reconnection site in a coronal (loop-top) source region. Surprisingly, it is generally accepted without question that the injection of low-energy electrons occurs significantly earlier than the onset of the type III RBs. Therefore, it is necessary to re-examine the timing of flare electrons. For this, we observed a “normal” event in which the injection of low-energy electrons coincided with the injection of high-energy electrons, and “abnormal” events in which the low-energy electrons seemed to arrive earlier. A high background of low-energy particles lacking any evidence of velocity dispersion characterizes an abnormal event. Due to the existence of a reconnection acceleration that results in similar enhancements at magnetic islands confined by the heliospheric current sheet (HCS), HCS observations are used to establish the empirical criteria for the reconnection acceleration in impulsive electron events. Observations show that 2–8 keV electrons accelerated by magnetic reconnection can change the pitch-angle distribution of background electrons for a time interval of approximately 0.5 hr before or after the time of current-sheet crossing. Therefore, this reconnection acceleration in the solar wind can influence the onset time analysis of electrons by emulating the effect of the earlier arrival of flare electrons. In addition, a technique is developed for estimating the phase velocity of whistler waves in the ion dissipation range, which may significantly affect the pitch-angle scattering analysis of low-energy electrons.
Three-dimensional Instability of Flame Fronts in Type I X-Ray Bursts
Authors: Cavecchi Yuri , Spitkovsky Anatoly 
Published: September 2019

Abstract
We present the first realistic 3D simulations of flame front instabilities during type I X-ray bursts. The unperturbed front is characterized by the balance between the pressure gradient and the Coriolis force of a spinning neutron star (ν = 450 Hz in our case). This balance leads to a fast horizontal velocity field parallel to the flame front. This flow is strongly sheared in the vertical direction. When we perturb the front an instability quickly corrugates the front. We identify this instability as the baroclinic instability. Most importantly, the flame is not disrupted by the instability and there are two major consequences: the overall flame propagation speed is ∼10 times faster than in the unperturbed case and distinct flame vortices appear. The speedup is due to the corrugation of the front and the dynamics of the vortices. These vortices may also be linked to the oscillations observed in the light curves of the bursts.
Bright Southern Variable Stars in the bRing Survey
Authors: Mellon Samuel N. , Mamajek Eric E. , Stuik Remko , Zwintz Konstanze , Kenworthy Matthew A. , J. Talens Geert Jan , Burggraaff Olivier , Bailey, III John I. , Dorval Patrick , Lomberg Blaine B. D. , Kuhn Rudi B. , Ireland Michael J. 
Published: September 2019

Abstract
In addition to monitoring the bright star β Pic during the near-transit event for its giant exoplanet, the β Pictoris b Ring (bRing) observatories at Siding Springs Observatory, Australia and Sutherland, South Africa have monitored the brightnesses of bright stars (V ≃ 4–8 mag) centered on the south celestial pole (δ ≤ −30°) for approximately two years. Here we present a comprehensive study of the bRing time-series photometry for bright southern stars monitored between 2017 June and 2019 January. Of the 16,762 stars monitored by bRing, 353 were found to be variable. Of the variable stars, 80% had previously known variability and 20% were new variables. Each of the new variables was classified, including three new eclipsing binaries (HD 77669, HD 142049, HD 155781), 26 δ Scutis, 4 slowly pulsating B stars, and others. This survey also reclassified four stars based on their period of pulsation, light curve, spectral classification, and color–magnitude information. The survey data were searched for new examples of transiting circumsecondary disk systems, but no candidates were found.
Cassini Composite Infrared Spectrometer (CIRS) Observations of Titan 2004–2017
Authors: Nixon Conor A. , Ansty Todd M. , Lombardo Nicholas A. , Bjoraker Gordon L. , Achterberg Richard K. , Annex Andrew M. , Rice Malena , Romani Paul N. , Jennings Donald E. , Samuelson Robert E. , Anderson Carrie M. , Coustenis Athena , Bézard Bruno , Vinatier Sandrine , Lellouch Emmanuel , Courtin Regis , Teanby Nicholas A. , Cottini Valeria , Flasar F. Michael 
Published: September 2019

Abstract
From 2004 to 2017, the Cassini spacecraft orbited Saturn, completing 127 close flybys of its largest moon, Titan. Cassini’s Composite Infrared Spectrometer (CIRS), one of 12 instruments carried on board, profiled Titan in the thermal infrared (7–1000 μm) throughout the entire 13 yr mission. CIRS observed on both targeted encounters (flybys) and more distant opportunities, collecting 8.4 million spectra from 837 individual Titan observations over 3633 hr. Observations of multiple types were made throughout the mission, building up a vast mosaic picture of Titan’s atmospheric state across spatial and temporal domains. This paper provides a guide to these observations, describing each type and chronicling its occurrences and global-seasonal coverage. The purpose is to provide a resource for future users of the CIRS data set, as well as those seeking to put existing CIRS publications into the overall context of the mission, and to facilitate future intercomparison of CIRS results with those of other Cassini instruments and ground-based observations.
Unprecedented Near-infrared Brightness and Variability of Sgr A*
Authors: Do Tuan , Witzel Gunther , Gautam Abhimat K. , Chen Zhuo , Ghez Andrea M. , Morris Mark R. , Becklin Eric E. , Ciurlo Anna , Hosek Matthew , Martinez Gregory D. , Matthews Keith , Sakai Shoko , Schödel Rainer 
Published: September 2019

Abstract
The electromagnetic counterpart to the Galactic center supermassive black hole, Sgr A*, has been observed in the near-infrared for over 20 yr and is known to be highly variable. We report new Keck Telescope observations showing that Sgr A* reached much brighter flux levels in 2019 than ever measured at near-infrared wavelengths. In the K′ band, Sgr A* reached flux levels of ∼6 mJy, twice the level of the previously observed peak flux from >13,000 measurements over 130 nights with the Very Large Telescope and Keck Telescopes. We also observe a factor of 75 change in flux over a 2 hr time span with no obvious color changes between 1.6 and 2.1 μm. The distribution of flux variations observed this year is also significantly different than the historical distribution. Using the most comprehensive statistical model published, the probability of a single night exhibiting peak flux levels observed this year, given historical Keck observations, is less than 0.3%. The probability of observing flux levels that are similar to all four nights of data in 2019 is less than 0.05%. This increase in brightness and variability may indicate a period of heightened activity from Sgr A* or a change in its accretion state. It may also indicate that the current model is not sufficient to model Sgr A* at high flux levels and should be updated. Potential physical origins of Sgr A*'s unprecedented brightness may be from changes in the accretion flow as a result of the star S0-2's closest passage to the black hole in 2018, or from a delayed reaction to the approach of the dusty object G2 in 2014. Additional multi-wavelength observations will be necessary to both monitor Sgr A* for potential state changes and to constrain the physical processes responsible for its current variability.