bluuebunny/crossref_metadata_2025_split huggingface dataset:
LINGKUNGAN PENGENDAPAN FORMASI KALIBENG PADA KALA MIOSEN AKHIR DI KABUPATEN DEMAK DAN KABUPATEN SEMARANG, JAWA TENGAH BERDASARKAN RASIO FORAMINIFERA PLANGTONIK DAN BENTONIK (RASIO P/B)
Authors: Jurnaliah Lia , Muhamadsyah Faizal , Barkah Mochammad Nursiyam 
Published: April 2017

Research area is classified a Lower Kalibeng Formation. Its age is Lower Miocene. The total number of sediment samples is 29 samples that are carried out based on measured section with 10 metres interval. The whole samples are processed by hydrogen peroxide method. Foraminifers’ quantitative analyses is conducted on each one gram of dry sample. Based on ratio P/B value that range between 49.64% - 99.41%, Late Miocene Kalibeng Formation is deposited on marine environment. The depositional process is beginning from neritic (outer neritic) – oceanic (upper bathyal-lower bathyal) – neritic (outer neritic) - oceanic (upper bathyal – lower bathyal). Keywords: Kalibeng Formation, plangtonic and benthic foraminifera, neritic, oceanic Daerah penelitian merupakan Formasi Kalibeng bagian bawah berumur Miosen Akhir.. Pengambilan 29 sampel sedimen dilakukan secara sistematis berdasarkan penampang terukur dengan interval 10 meter. Seluruh sampel sedimen diproses dengn menggunakan metoda hydrogen peroksida. Analisis kuantitatif foraminifera dilakukan pada setiap 1 gram sampel kering berukuran >120 mesh. Berdasarkan hasil perhitungan rasio foraminifera plangtonik dan bentonik (rasio P/B) yang berkisar antara 49,64% - 99,41%, Formasi Sungaibeng Kala Miosen Akhir terendapkan pada lingkungan marin dimulai dari neritik (neritik luar) – oseanik (batial bawah-batial atas) – neritik (neritik luar) dan terakhir adalah oseanik (batial bawah-batial atas). Kata Kunci: Formasi Kalibeng, foraminifera plangtonik dan bentonik, neritik, oseanik
Epidemiologic profile of oral squamous cell carcinoma in Yogyakarta, Indonesia
Authors: Gracia Isadora , Utoro Totok , Supriatno Supriatno , Astuti Indwiani , Heriyanto Didik Setyo , Pramono Dibyo 
Published: April 2017

ABSTRACTIntroduction: Oral cancer is a major health problem in the world, indicated by a high incidence of recurrence. In Southeast Asia, oral cancer ranks sixth from all cancers on the human body. The incidence of oral cancer, especially squamous cell carcinoma types, increases every year, but the prognosis and patients life expectancy are still unsatisfying enough and the reports about the profile of oral cancer is still limited.The objective of this research was to get the epidemiological profile of oral squamous cell carcinoma (OSCC) in Yogyakarta, Indonesia. Methods: The research method was observational analytic with cross-sectional design. All new OSCC cases in three anatomic pathology laboratory installations in Yogyakarta (January 2011-December 2015) were included in this study. Data collected were gender, age, anatomical location, and histology. All data were analyzed using statistical analysis program. Results: OSCC new cases amount increasing each year: 6 cases (6.6%) in 2011, and increased to 24 cases (26.4%) in 2015. Fifty-two of the 91 cases (57.1%) were found on male. The age group with the most cases was found in group of 41-60 years (49.5%). There is no difference in the case distribution by age between male and female. Forty-eight cases were found in the lingual part (52.7%). Histological examination showed 68 cases (74.7%) were well-differentiated carcinoma. Conclusion: OSCC profile in Yogyakarta mostly found in men with anatomical location in the lingual part in the age group above 40 years of age and were having well-differentiated histology.Keywords: Oral squamous cell carcinoma (OSCC), Epidemiologic profile, Yogyakarta
Optimal Stellar Photometry for Multi-conjugate Adaptive Optics Systems Using Science-based Metrics
Authors: Turri P. , McConnachie A. W. , Stetson P. B. , Fiorentino G. , Andersen D. R. , Bono G. , Massari D. , Véran J.-P. 
Published: April 2017

Abstract
We present a detailed discussion of how to obtain precise stellar photometry in crowded fields using images from multi-conjugate adaptive optics (MCAO) systems, with the intent of informing the scientific development of this key technology for the Extremely Large Telescopes. We use deep J and K
s exposures of NGC 1851 taken with the Gemini Multi-Conjugate Adaptive Optics System (GeMS) on Gemini South to quantify the performance of the instrument and to develop an optimal strategy for stellar photometry using point-spread function (PSF)-fitting techniques. We judge the success of the various methods we employ by using science-based metrics, particularly the width of the main sequence turnoff region. We also compare the GeMS photometry with the exquisite HST data in the visible of the same target. We show that the PSF produced by GeMS possesses significant spatial and temporal variability that must be accounted for during the analysis. We show that the majority of the variation of the PSF occurs within the “control radius” of the MCAO system and that the best photometry is obtained when the PSF radius is chosen to closely match this spatial scale. We identify photometric calibration as a critical issue for next-generation MCAO systems such as those on the Thirty Meter Telescope and European Extremely Large Telescope. Our final CMDs reach K
s ∼ 22—below the main sequence knee—making it one of the deepest for a globular cluster available from the ground. Theoretical isochrones are in remarkable agreement with the stellar locus in our data from below the main sequence knee to the upper red giant branch.
Testing PSF Interpolation in Weak Lensing with Real Data
Authors: Lu Tianhuan , Zhang Jun , Dong Fuyu , Li Yingke , Liu Dezi , Fu Liping , Li Guoliang , Fan Zuhui 
Published: April 2017

Abstract
Reconstruction of the point-spread function (PSF) is a critical process in weak lensing measurement. We develop a real-data based and galaxy-oriented pipeline to compare the performances of various PSF reconstruction schemes. Making use of a large amount of the CFHTLenS data, the performances of three classes of interpolating schemes—polynomial, Kriging, and Shepard—are evaluated. We find that polynomial interpolations with optimal orders and domains perform the best. We quantify the effect of the residual PSF reconstruction error on shear recovery in terms of the multiplicative and additive biases, and their spatial correlations using the shear measurement method of Zhang et al. We find that the impact of PSF reconstruction uncertainty on the shear–shear correlation can be significantly reduced by cross correlating the shear estimators from different exposures. It takes only 0.2 stars (S/N ≳ 100) per square arcmin on each exposure to reach the best performance of PSF interpolation, a requirement that is satisfied in most of the CFHTlenS data.
Sub-photospheric Shocks in Relativistic Explosions
Authors: Beloborodov Andrei M. 
Published: April 2017

Abstract
This paper examines the mechanism of internal shocks in opaque relativistic outflows, in particular in cosmological gamma-ray bursts. The shocks produce neutrino emission and affect the observed photospheric radiation from the explosion. They develop from internal compressive waves and can be of different types depending on the composition of the outflow. (1) Shocks in “photon gas,” with negligible plasma inertia, have a unique structure determined by the force-free condition—zero radiation flux in the plasma rest frame. Radiation dominance over plasma inertia suppresses the formation of collisionless shocks mediated by collective electromagnetic fields. (2) If the outflow is sufficiently magnetized, a strong collisionless subshock develops, which is embedded in a thicker radiation-mediated structure. (3) Waves in outflows with a free neutron component lead to dissipation through nuclear collisions. At large optical depths, shocks have a thickness comparable to the neutron free path, with embedded radiation-mediated and collisionless subshocks. The paper also presents first-principles simulations of magnetized flows filled with photons, demonstrating the formation of shocks and their structure. Simple estimates show that magnetized sub-photospheric shocks are efficient producers of photons and have a great impact on the observed photospheric radiation. The shock structure changes as the outflow expands toward its photosphere. The dissipation is accompanied by strong

pair creation, and the

-dressed shock carries the photosphere with it up to two decades in radius, emitting a strong pulse of nonthermal radiation.
Reconstruction of Galaxy Star Formation Histories through SED Fitting:The Dense Basis Approach
Authors: Iyer Kartheik , Gawiser Eric 
Published: April 2017

Abstract
We introduce the dense basis method for Spectral Energy Distribution (SED) fitting. It accurately recovers traditional SED parameters, including M
*, SFR, and dust attenuation, and reveals previously inaccessible information about the number and duration of star formation episodes and the timing of stellar mass assembly, as well as uncertainties in these quantities. This is done using basis star formation histories (SFHs) chosen by comparing the goodness-of-fit of mock galaxy SEDs to the goodness-of-reconstruction of their SFHs. We train and validate the method using a sample of realistic SFHs at z = 1 drawn from stochastic realizations, semi-analytic models, and a cosmological hydrodynamical galaxy formation simulation. The method is then applied to a sample of 1100 CANDELS GOODS-S galaxies at

to illustrate its capabilities at moderate S/N with 15 photometric bands. Of the six parametrizations of SFHs considered, we adopt linear-exponential, bessel-exponential, log-normal, and Gaussian SFHs, and reject the traditional parametrizations of constant (Top-Hat) and exponential SFHs. We quantify the bias and scatter of each parametrization. 15% of galaxies in our CANDELS sample exhibit multiple episodes of star formation, with this fraction decreasing above

. About 40% of the CANDELS galaxies have SFHs whose maximum occurs at or near the epoch of observation. The dense basis method is scalable and offers a general approach to a broad class of data-science problems.
OmegaWINGS: The First Complete Census of Post-starburst Galaxies in Clusters in the Local Universe
Authors: Paccagnella A. , Vulcani B. , Poggianti B. M. , Fritz J. , Fasano G. , Moretti A. , Jaffé Yara L. , Biviano A. , Gullieuszik M. , Bettoni D. , Cava A. , Couch W. , D’Onofrio M. 
Published: April 2017

Abstract
Galaxies that abruptly interrupt their star formation in

present recognizable features in their spectra (no emission and Hδ in absorption) and are called post-starburst (PSB) galaxies. By studying their stellar population properties and their location within the clusters, we obtain valuable insights on the physical processes responsible for star formation quenching. We present the first complete characterization of PSB galaxies in clusters at

, based on WINGS and OmegaWINGS data, and contrast their properties to those of passive (PAS) and emission-line (EML) galaxies. For

, PSBs represent 7.2 ± 0.2% of cluster galaxies within 1.2 virial radii. Their incidence slightly increases from the outskirts toward the cluster center and from the least toward the most luminous and massive clusters, defined in terms of X-ray luminosity and velocity dispersion. The phase-space analysis and velocity-dispersion profile suggest that PSBs represent a combination of galaxies with different accretion histories. Moreover, PSBs with the strongest Hδ are consistent with being recently accreted. PSBs have stellar masses, magnitudes, colors, and morphologies intermediate between PAS and EML galaxies, typical of a population in transition from being star-forming to passive. Comparing the fraction of PSBs to the fraction of galaxies in transition on longer timescales, we estimate that the short-timescale star formation quenching channel contributes two times more than the long timescale one to the growth of the passive population. Processes like ram-pressure stripping and galaxy–galaxy interactions are more efficient than strangulation in affecting star formation.
UV/Optical Emission from the Expanding Envelopes of Type II Supernovae
Authors: Sapir Nir , Waxman Eli 
Published: April 2017

Abstract
The early part of a supernova (SN) light curve is dominated by radiation escaping from the expanding shock-heated progenitor envelope. For polytropic hydrogen envelopes, the properties of the emitted radiation are described by simple analytic expressions and are nearly independent of the polytropic index, n. This analytic description holds at early time, t < few days, during which radiation escapes from shells that are initially lying near the stellar surface. We use numerical solutions to address two issues. First, we show that the analytic description holds at early time also for nonpolytropic density profiles. Second, we extend the solutions to later times, when the emission emerges from deep within the envelope and depends on the progenitor’s density profile. Examining the late time behavior of the polytropic envelopes with a wide range of core to envelope mass and radius ratios, 0.1 ≤ M
c/M
env ≤ 10 and 10−3 ≤ R
c/R ≤ 10−1, we find that the effective temperature is well described by the analytic solution also at late time, while the luminosity, L, is suppressed by a factor, which may be approximated to be better than a 20 [30]% accuracy up to t = t
tr/a by

with t
tr = 13 (M
env/M
⊙)3/4(M/M
env)1/4(E/1051erg)−1/4 days, M = M
c + M
env, A = 0.9[0.8], a = 1.7[4.6], and α = 0.8[0.7] for n = 3/2[3]. This description holds as long as the opacity is approximately that of a fully ionized gas, i.e., for T > 0.7 eV, t < 14(R/1013.5cm)0.55 days. The suppression of L at t
tr/a that is obtained for standard polytropic envelopes may account for the first optical peak of double-peaked SN light curves, with the first peak at a few days for M
env < 1 M
⊙.
Interaction of Two Active Region Filaments Observed by NVST and SDO
Authors: Yang Liheng , Yan Xiaoli , Li Ting , Xue Zhike , Xiang Yongyuan 
Published: April 2017

Abstract
Using high spatial and temporal resolution Hα data from the New Vacuum Solar Telescope (NVST) and simultaneous observations from the Solar Dynamics Observatory, we present the rare event of the interaction between two filaments (F1 and F2) in AR 11967 on 2014 January 31. The adjacent two filaments were almost perpendicular to each other. Their interaction was driven by the movement of F1 and started when the two filaments collided with each other. During the interaction, the threads of F1 continuously slipped from the northeast to the southwest, and were accompanied by the brightenings at the junction of two filaments and the northeast footpoint of F2. Part of F1 and the main body of F2 became invisible in Hα wavelength due to the heating and the motion of F2. At the same time, bright material initiated from the junction of two filaments were observed to move along F1. The magnetic connectivities of F1 were found to be changed after their interaction. These observations suggest that magnetic reconnection was involved in the interaction of two filaments and resulted in the eruption of one filament.
Early Science with the Large Millimeter Telescope: Detection of Dust Emission in Multiple Images of a Normal Galaxy at z > 4 Lensed by a Frontier Fields Cluster
Authors: Pope Alexandra , Montaña Alfredo , Battisti Andrew , Limousin Marceau , Marchesini Danilo , Wilson Grant W. , Alberts Stacey , Aretxaga Itziar , Avila-Reese Vladimir , Bermejo-Climent José Ramón , Brammer Gabriel , Bravo-Alfaro Hector , Calzetti Daniela , Chary Ranga-Ram , Cybulski Ryan , Giavalisco Mauro , Hughes David , Kado-Fong Erin , Keller Erica , Kirkpatrick Allison , Labbe Ivo , Lange-Vagle Daniel , Lowenthal James , Murphy Eric , Oesch Pascal , Gonzalez Daniel Rosa , Sánchez-Argüelles David , Shipley Heath , Stefanon Mauro , Vega Olga , Whitaker Katherine , Williams Christina C. , Yun Min , Zavala Jorge A. , Zeballos Milagros 
Published: April 2017

Abstract
We directly detect dust emission in an optically detected, multiply imaged galaxy lensed by the Frontier Fields cluster MACSJ0717.5+3745. We detect two images of the same galaxy at 1.1 mm with the AzTEC camera on the Large Millimeter Telescope leaving no ambiguity in the counterpart identification. This galaxy, MACS0717_Az9, is at z > 4 and the strong lensing model (μ = 7.5) allows us to calculate an intrinsic IR luminosity of 9.7 × 1010
L
⊙ and an obscured star formation rate of 14.6 ± 4.5 M
⊙ yr−1. The unobscured star formation rate from the UV is only 4.1 ± 0.3 M
⊙ yr−1, which means the total star formation rate (18.7 ± 4.5 M
⊙ yr−1) is dominated (75%–80%) by the obscured component. With an intrinsic stellar mass of only 6.9 × 109
M
⊙, MACS0717_Az9 is one of only a handful of z > 4 galaxies at these lower masses that is detected in dust emission. This galaxy lies close to the estimated star formation sequence at this epoch. However, it does not lie on the dust obscuration relation (IRX-β) for local starburst galaxies and is instead consistent with the Small Magellanic Cloud attenuation law. This remarkable lower mass galaxy, showing signs of both low metallicity and high dust content, may challenge our picture of dust production in the early universe.
ALMA Mapping of Rapid Gas and Dust Variations in Comet C/2012 S1 (ISON):New Insights into the Origin of Cometary HNC
Authors: Cordiner M. A. , Boissier J. , Charnley S. B. , Remijan A. J. , Mumma M. J. , Villanueva G. , Lis D. C. , Milam S. N. , Paganini L. , Crovisier J. , Bockelee-Morvan D. , Kuan Y.-J. , Biver N. , Coulson I. M. 
Published: April 2017

Abstract
Observations of the sungrazing comet C/2012 S1 (ISON) were carried out using the Atacama Large Millimeter/submillimeter Array at a heliocentric distance of 0.58–0.54 au (pre-perihelion) on 2013 November 16–17. Temporally resolved measurements of the coma distributions of HNC, CH3OH, H2CO, and dust were obtained over the course of about an hour on each day. During the period UT 10:10–11:00 on November 16, the comet displayed a remarkable drop in activity, manifested as a >42% decline in the molecular line and continuum fluxes. The H2CO observations are consistent with an abrupt, ≈50% reduction in the cometary gas production rate soon after the start of our observations. On November 17, the total observed fluxes remained relatively constant during a similar period, but strong variations in the morphology of the HNC distribution were detected as a function of time, indicative of a clumpy, intermittent outflow for this species. Our observations suggest that at least part of the detected HNC originated from degradation of nitrogen-rich organic refractory material, released intermittently from confined regions of the nucleus. By contrast, the distributions of CH3OH and H2CO during the November 17 observations were relatively uniform, consistent with isotropic outflow and stable activity levels for these species. These results highlight a large degree of variability in the production of gas and dust from comet ISON during its pre-perihelion outburst, consistent with repeated disruption of the nucleus interspersed with periods of relative quiescence.
The Physical Constraints on a New LoBAL QSO at z = 4.82
Authors: Yi Weimin , Green Richard , Bai Jin-Ming , Wang Tinggui , Grier Catherine J. , Trump Jonathan R. , Brandt William N. , Zuo Wenwen , Yang Jinyi , Wang Feige , Yang Chenwei , Wu Xue-Bing , Zhou Hongyan , Fan Xiaohui , Jiang Linhua , Yang Qian , Varricatt Watson , Kerr Tom , Milne Peter , Benigni Sam , Wang Jian-Guo , Zhang Jujia , Wang Fang , Wang Chuan-Jun , Xin Yu-Xin , Fan Yu-Feng , Chang Liang , Zhang Xiliang , Lun Bao-Li 
Published: April 2017

Abstract
Very few low-ionization broad absorption line (LoBAL) QSOs have been found at high redshifts, to date. One high-redshift LoBAL QSO, J0122+1216, was recently discovered by the Lijiang 2.4 m Telescope, with an initial redshift determination of 4.76. Aiming to investigate its physical properties, we carried out follow-up observations in the optical and near-IR spectroscopy. Near-IR spectra from UKIRT and P200 confirm that it is a LoBAL, with a new redshift determination of 4.82 ± 0.01 based on the Mg ii emission-line. The new Mg ii redshift determination reveals strong blueshifts and asymmetry of the high-ionization emission lines. We estimate a black hole mass of ∼2.3 × 109
M
⊙ and Eddington ratio of ∼1.0 according to the empirical Mg ii-based single-epoch relation and bolometric correction factor. It is possible that strong outflows are the result of an extreme quasar environment driven by the high Eddington ratio. A lower limit on the outflowing kinetic power (>0.9% L
Edd) is derived from both emission and absorption lines, indicating that these outflows play a significant role in the feedback process that regulates the growth of its black hole, as well as host galaxy evolution.
Triggering Process of the X1.0 Three-ribbon Flare in the Great Active Region NOAA 12192
Authors: Bamba Yumi , Inoue Satoshi , Kusano Kanya , Shiota Daikou 
Published: April 2017

Abstract
The solar magnetic field in a flare-producing active region (AR) is much more complicated than theoretical models, which assume a very simple magnetic field structure. The X1.0 flare, which occurred in AR 12192 on 2014 October 25, showed a complicated three-ribbon structure. To clarify the trigger process of the flare and to evaluate the applicability of a simple theoretical model, we analyzed the data from Hinode/Solar Optical Telescope and the Solar Dynamics Observatory/Helioseismic and Magnetic Imager, Atmospheric Imaging Assembly. We investigated the spatio-temporal correlation between the magnetic field structures, especially the non-potentiality of the horizontal field, and the bright structures in the solar atmosphere. As a result, we determined that the western side of the positive polarity, which is intruding on a negative polarity region, is the location where the flare was triggered. This is due to the fact that the sign of the magnetic shear in that region was opposite that of the major shear of the AR, and the significant brightenings were observed over the polarity inversion line (PIL) in that region before flare onset. These features are consistent with the recently proposed flare-trigger model that suggests that small reversed shear (RS) magnetic disturbances can trigger solar flares. Moreover, we found that the RS field was located slightly off the flaring PIL, contrary to the theoretical prediction. We discuss the possibility of an extension of the RS model based on an extra numerical simulation. Our result suggests that the RS field has a certain flexibility for displacement from a highly sheared PIL, and that the RS field triggers more flares than we expected.
What Can We Learn about GRB from the Variability Timescale Related Correlations?
Authors: Xie Wei , Lei Wei-Hua , Wang Ding-Xiong 
Published: April 2017

Abstract
Recently, two empirical correlations related to the minimum variability timescale (MTS) of the light curves are discovered in gamma-ray bursts (GRBs). One is the anti-correlation between MTS and Lorentz factor Γ, and the other is the anti-correlation between the MTS and gamma-ray luminosity L

γ
. Both of the two correlations might be used to explore the activity of the central engine of GRBs. In this paper, we try to understand these empirical correlations by combining two popular black hole central engine models (namely, the Blandford & Znajek mechanism (BZ) and the neutrino-dominated accretion flow (NDAF)). By taking the MTS as the timescale of viscous instability of the NDAF, we find that these correlations favor the scenario in which the jet is driven by the BZ mechanism.