bluuebunny/crossref_metadata_2025_split huggingface dataset:
Evaluasi Kepuasan Mahasiswa Terhadap Kualitas Pelayanan Pendidikan Lembaga Pendidikan Tinggi ABC di Cikarang
Authors: Sutariah Farliana 
Published: March 2018

<p><em>Education is one service industry that provides services to students in need. One of Institute from Cikarang, Bekasi, West Java organized and developed the science, technology, and as a scientific community that is full of sublime imagery and educates the nation's life. The real conditions encountered by Institute is currently at in providing services to students especially on teaching staff (lecturers) as well as academic staff not yet optimal. An increase in the quality of service can be implemented using approach servequal. Servqual is a method for measuring the quality of service from a service provider. Quality of service is measured from each dimension (tangible, responsiveness, reliability, assurance, Empathize). For the result we know 5 elements spread on 4 quadrants. Quadrant 1 is spread 6 things, Quadrant II is spread 11 things, Quadrant III are spread 9 things and last Quadrant IV are spread 4 things. We investigate causes that need problem-solving on Institute by Root Cause Analyze (RCA.) Based on the results of calculation and pay attention to the real conditions, interviews with students, obtained significant complaints with the research. In this case, the Institute should improve the quality of service, both in terms of performance of teaching staff, and the number of teaching staff for teaching and learning process can be going well, so does the relationship of administration and facility staff and other supporting improved.</em></p>
Analisis Kesulitan Siswa SMA Kelas XI Dalam Mempelajari Ukuran Tendensi Sentral
Authors: Awaludin Aulia Ar Rakhman 
Published: March 2018

<p class="p4" align="center">This study aims to determine the difficulties of learning what are the natural students of class XI SMA Batik 1 Surakarta on the material statistics the size of the central tendency of group data, what causes the difficulty of learning students class XI SMA Batik 1 Surakarta on the material statistics the size of the central tendency of group data and how the alternative Solving the results of the analysis of learning difficulties on the statistical matter of the size of the central tendency of group data. The method used is literature study. Alternative results for students who have difficulty in understanding the concept is to apply learning contextual approach is learning that aims to motivate students to understand the meaning of the material in the learning by associating with the context of everyday life such as knowing the average of a value of repetition, know mode (value Which many students get) from a repetition so that learning will be memoras and remembered by students and for students who have difficulty application of formulas and solutions is the alternative given is to multiply the exercise questions and need for the elaboration of what is known and can be from where. When students are accustomed to such things then students will be easy in applying the formula and solve the problem correctly.</p><p class="p4"> </p><p> </p>
Meningkatkan Hasil Belajar Matematika Melalui Penerapan Metode Pembelajaran Kooperatif
Authors: Yusup Ayi Ahmad Maulana 
Published: March 2018

The purpose of this research was to analyze the effect of cooperative learning method toward the seventh-grade students of Private Junior High School in South Tangerang. The method that used in the research was an experimental method, where the independent variable was cooperative learning method and the dependent variable was the result of learning mathematics. The sample was taken by using the random sampling technique. The test data requirements were done by using the following formula: chi-square test for normality test and Fisher test for homogeneity test. The hypothesis submission was done using t-test<sub>.</sub> The result of the research shows that there are significant effects of cooperative learning method toward students’ mathematics learning result especially on the plane figure subject on the seventh-grade students of the private junior high school in South Tangerang.
A Horse Is a Horse, Of Course, Of Course: Animality, Transitivity, and the Double Take
Authors: Barker Jennifer M. 
Published: March 2018

Lanthimos's The Lobster (2015) invites a way of looking that coincides with work done by scholars of feminist new materialism with an eye toward queering binary and static concepts of species, gender, and the relation between them. A close look at one fleeting, slow-motion image of horses racing on a track reveals a pattern of ‘diffraction,’ in the critically productive sense that Karen Barad uses the term, such that we see neither camera movement, human movement, nor animal movement proper, but movement that is ‘of’ all three bodies, but not ‘in’ any given one. The film perpetually defers the dichotomy between animal and human as it is classically conceived in order to reconfigure it. That diffractive pattern recurs throughout the film, in its use of slow motion, lateral camera movements, and the overlapping of multiple movements and rhythms. Throughout its running time, The Lobster suspends the process of becoming in motion, emphasizing the experiential aspect of this ‘-ing’ that bodies do. The film draws vision sideways, rippling and redoubling itself; in the process, it shifts attention from a human state or an animal state – states that, according to conventional logic, exist on one side or another of a dividing line, and which certain types of movement might transcend – to transitivity, or the movement of movement itself.
An Extreme Protocluster of Luminous Dusty Starbursts in the Early Universe
Authors: Oteo I. , Ivison R. J. , Dunne L. , Manilla-Robles A. , Maddox S. , Lewis A. J. R. , Zotti G. de , Bremer M. , Clements D. L. , Cooray A. , Dannerbauer H. , Eales S. , Greenslade J. , Omont A. , Perez–Fournón I. , Riechers D. , Scott D. , van der Werf P. , Weiss A. , Zhang Z-Y. 
Published: March 2018

Abstract
We report the identification of an extreme protocluster of galaxies in the early universe whose core (nicknamed Distant Red Core, DRC, because of its very red color in Herschel SPIRE bands) is formed by at least 10 dusty star-forming galaxies (DSFGs), spectroscopically confirmed to lie at

z

spec

=
4.002

via detection of [C i](1–0), 12CO(6–5), 12CO(4–3), 12CO(2–1), and

H

2

O
(

2

11

–

2

02

)

emission lines with ALMA and ATCA. These DSFGs are distributed over a

260

kpc
×
310

kpc

region and have a collective obscured star formation rate (SFR) of

∼
6500

M

⊙

yr

−
1

, considerably higher than those seen before in any protocluster at

z
≳
4

. Most of the star formation is taking place in luminous DSFGs since no Lyα emitters are detected in the protocluster core, apart from a Lyα blob located next to one of the DRC components, extending over

60

kpc

. The total obscured SFR of the protocluster could rise to

SFR
∼
14,400

M

⊙

yr

−
1

if all the members of an overdensity of bright DSFGs discovered around DRC in a wide-field Large APEX BOlometer CAmera 870 μm image are part of the same structure. [C i](1–0) emission reveals that DRC has a total molecular gas mass of at least

M

H

2

∼
6.6
×

10

11

M

⊙

, and its total halo mass could be as high as

∼
4.4
×

10

13

M

⊙

, indicating that it is the likely progenitor of a cluster at least as massive as Coma at z = 0.
Coronal Elemental Abundances in Solar Emerging Flux Regions
Authors: Baker Deborah , Brooks David H. , Driel-Gesztelyi Lidia van , James Alexander W. , Démoulin Pascal , Long David M. , Warren Harry P. , Williams David R. 
Published: March 2018

Abstract
The chemical composition of solar and stellar atmospheres differs from the composition of their photospheres. Abundances of elements with low first ionization potential (FIP) are enhanced in the corona relative to high-FIP elements with respect to the photosphere. This is known as the FIP effect and it is important for understanding the flow of mass and energy through solar and stellar atmospheres. We used spectroscopic observations from the Extreme-ultraviolet Imaging Spectrometer on board the Hinode observatory to investigate the spatial distribution and temporal evolution of coronal plasma composition within solar emerging flux regions inside a coronal hole. Plasma evolved to values exceeding those of the quiet-Sun corona during the emergence/early-decay phase at a similar rate for two orders of magnitude in magnetic flux, a rate comparable to that observed in large active regions (ARs) containing an order of magnitude more flux. During the late-decay phase, the rate of change was significantly faster than what is observed in large, decaying ARs. Our results suggest that the rate of increase during the emergence/early-decay phase is linked to the fractionation mechanism that leads to the FIP effect, whereas the rate of decrease during the later decay phase depends on the rate of reconnection with the surrounding magnetic field and its plasma composition.
Magnetic Structure of a Composite Solar Microwave Burst
Authors: Lee Jeongwoo , White Stephen M. , Liu Chang , Kliem Bernhard , Masuda Satoshi 
Published: March 2018

Abstract
A composite flare consisting of an impulsive flare SOL2015-06-21T01:42 (GOES class M2.0) and a more gradual, long-duration flare SOL2015-06-21T02:36 (M2.6) from NOAA Active Region 12371, is studied using observations with the Nobeyama Radioheliograph (NoRH) and the Solar Dynamics Observatory (SDO). While composite flares are defined by their characteristic time profiles, in this paper we present imaging observations that demonstrate the spatial relationship of the two flares and allow us to address the nature of the evolution of a composite event. The NoRH maps show that the first flare is confined not only in time, but also in space, as evidenced by the stagnation of ribbon separation and the stationarity of the microwave source. The NoRH also detected another microwave source during the second flare, emerging from a different location where thermal plasma is so depleted that accelerated electrons could survive longer against Coulomb collisional loss. The AIA 131 Å images show that a sigmoidal EUV hot channel developed after the first flare and erupted before the second flare. We suggest that this eruption removed the high-lying flux to let the separatrix dome underneath reconnect with neighboring flux and the second microwave burst follow. This scenario explains how the first microwave burst is related to the much-delayed second microwave burst in this composite event.
Hunting Faint Dwarf Galaxies in the Field Using Integrated Light Surveys
Authors: Danieli Shany , van Dokkum Pieter , Conroy Charlie 
Published: March 2018

Abstract
We discuss the approach of searching the lowest mass dwarf galaxies,

, in the general field, using integrated light surveys. By exploring the limiting surface brightness-spatial resolution (μ
eff,lim−θ) parameter space, we suggest that faint field dwarfs in the Local Volume, between 3 and 10 Mpc, are expected to be detected very effectively and in large numbers using integrated light photometric surveys, complementary to the classical star counts method. We use a sample of dwarf galaxies in the Local Group to construct relations between their photometric and structural parameters, M
*–μ
eff,V
and M
*–R
eff. We use these relations, along with assumed functional forms for the halo mass function and the stellar mass–halo mass (SMHM) relation, to calculate the lowest detectable stellar masses in the Local Volume and the expected number of galaxies as a function of the limiting surface brightness and spatial resolution. The number of detected galaxies depends mostly on the limiting surface brightness for distances >3 Mpc, while spatial resolution starts to play a role for galaxies at distances >8 Mpc. Surveys with μ
eff,lim ∼ 30 mag arcsec−2 should be able to detect galaxies with stellar masses down to ∼104
M
⊙ in the Local Volume. Depending on the form of the SMHM relation, the expected number of dwarf galaxies with distances between 3 and 10 Mpc is 0.04–0.35 per square degree, assuming a limiting surface brightness of ∼29–30 mag arcsec−2 and a spatial resolution <4″. We plan to search for a population of low-mass dwarf galaxies in the field by performing a blank wide field photometric survey with the Dragonfly Telephoto Array, an imaging system optimized for the detection of extended ultra low surface brightness structures.
LensFlow: A Convolutional Neural Network in Search of Strong Gravitational Lenses
Authors: Pourrahmani Milad , Nayyeri Hooshang , Cooray Asantha 
Published: March 2018

Abstract
In this work, we present our machine learning classification algorithm for identifying strong gravitational lenses from wide-area surveys using convolutional neural networks; LensFlow. We train and test the algorithm using a wide variety of strong gravitational lens configurations from simulations of lensing events. Images are processed through multiple convolutional layers that extract feature maps necessary to assign a lens probability to each image. LensFlow provides a ranking scheme for all sources that could be used to identify potential gravitational lens candidates by significantly reducing the number of images that have to be visually inspected. We apply our algorithm to the HST/ACS i-band observations of the COSMOS field and present our sample of identified lensing candidates. The developed machine learning algorithm is more computationally efficient and complimentary to classical lens identification algorithms and is ideal for discovering such events across wide areas from current and future surveys such as LSST and WFIRST.
Future Cosmological Constraints From Fast Radio Bursts
Authors: Walters Anthony , Weltman Amanda , Gaensler B. M. , Ma Yin-Zhe , Witzemann Amadeus 
Published: March 2018

Abstract
We consider the possible observation of fast radio bursts (FRBs) with planned future radio telescopes, and investigate how well the dispersions and redshifts of these signals might constrain cosmological parameters. We construct mock catalogs of FRB dispersion measure (DM) data and employ Markov Chain Monte Carlo analysis, with which we forecast and compare with existing constraints in the flat ΛCDM model, as well as some popular extensions that include dark energy equation of state and curvature parameters. We find that the scatter in DM observations caused by inhomogeneities in the intergalactic medium (IGM) poses a big challenge to the utility of FRBs as a cosmic probe. Only in the most optimistic case, with a high number of events and low IGM variance, do FRBs aid in improving current constraints. In particular, when FRBs are combined with CMB+BAO+SNe+H
0 data, we find the biggest improvement comes in the

constraint. Also, we find that the dark energy equation of state is poorly constrained, while the constraint on the curvature parameter, Ω
k
, shows some improvement when combined with current constraints. When FRBs are combined with future baryon acoustic oscillation (BAO) data from 21 cm Intensity Mapping, we find little improvement over the constraints from BAOs alone. However, the inclusion of FRBs introduces an additional parameter constraint,

, which turns out to be comparable to existing constraints. This suggests that FRBs provide valuable information about the cosmological baryon density in the intermediate redshift universe, independent of high-redshift CMB data.
Parameterizing the Supernova Engine and Its Effect on Remnants and Basic Yields
Authors: Fryer Chris L. , Andrews Sydney , Even Wesley , Heger Alex , Safi-Harb Samar 
Published: March 2018

Abstract
Core-collapse supernova science is now entering an era in which engine models are beginning to make both qualitative and, in some cases, quantitative predictions. Although the evidence in support of the convective engine for core-collapse supernova continues to grow, it is difficult to place quantitative constraints on this engine. Some studies have made specific predictions for the remnant distribution from the convective engine, but the results differ between different groups. Here we use a broad parameterization for the supernova engine to understand the differences between distinct studies. With this broader set of models, we place error bars on the remnant mass and basic yields from the uncertainties in the explosive engine. We find that, even with only three progenitors and a narrow range of explosion energies, we can produce a wide range of remnant masses and nucleosynthetic yields.
Star Formation Histories of the LEGUS Dwarf Galaxies. I. Recent History of NGC 1705, NGC 4449, and Holmberg II*
Authors: Cignoni M. , Sacchi E. , Aloisi A. , Tosi M. , Calzetti D. , Lee J. C. , Sabbi E. , Adamo A. , Cook D. O. , Dale D. A. , Elmegreen B. G. , Gallagher J. S. , Gouliermis D. A. , Grasha K. , Grebel E. K. , Hunter D. A. , Johnson K. E. , Messa M. , Smith L. J. , Thilker D. A. , Ubeda L. , Whitmore B. C. 
Published: March 2018

Abstract
We use Hubble Space Telescope observations from the Legacy Extragalactic UV Survey to reconstruct the recent star formation histories (SFHs) of three actively star-forming dwarf galaxies, NGC 4449, Holmberg II, and NGC 1705, from their UV color–magnitude diagrams (CMDs). We apply a CMD fitting technique using two independent sets of stellar isochrones, PARSEC-COLIBRI and MIST, to assess the uncertainties related to stellar evolution modeling. Irrespective of the adopted stellar models, all three dwarfs are found to have had almost constant star formation rates (SFRs) in the last 100–200 Myr, with modest enhancements (a factor of ∼2) above the 100 Myr averaged SFR. Significant differences among the three dwarfs are found in terms of the overall SFR, the timing of the most recent peak, and the SFR/area. The initial mass function of NGC 1705 and Holmberg II is consistent with a Salpeter slope down to ≈5 M
⊙, whereas it is slightly flatter, s = −2.0, in NGC 4449. The SFHs derived with the two different sets of stellar models are consistent with each other, except for some quantitative details, attributable to their input assumptions. They also share the drawback that all synthetic diagrams predict a clear separation in color between the upper main-sequence and helium-burning stars, which is not apparent in the data. Since neither differential reddening, which is significant in NGC 4449, nor unresolved binaries appear to be sufficient to fill the gap, we suggest this calls for a revision of both sets of stellar evolutionary tracks.
H i Kinematics along the Minor Axis of M82
Authors: Martini Paul , Leroy Adam K. , Mangum Jeffrey G. , Bolatto Alberto , Keating Katie M. , Sandstrom Karin , Walter Fabian 
Published: March 2018

Abstract
M82 is one of the best-studied starburst galaxies in the local universe, and is consequently a benchmark for studying star formation feedback at both low and high redshift. We present new VLA H i observations that reveal the cold gas kinematics along the minor axis in unprecedented detail. This includes the detection of H i up to 10 kpc along the minor axis toward the south and beyond 5 kpc to the north. A surprising aspect of these observations is that the line-of-sight H i velocity decreases substantially from about 120 to

from 1.5 to 10 kpc off the midplane. The velocity profile is not consistent with the H i gas cooling from the hot wind. We demonstrate that the velocity decrease is substantially greater than the deceleration expected from gravitational forces alone. If the H i consists of a continuous population of cold clouds, some additional drag force must be present, and the magnitude of the drag force places a joint constraint on the ratio of the ambient medium to the typical cloud size and density. We also show that the H i kinematics are inconsistent with a simple conical outflow centered on the nucleus, but instead require the more widespread launch of the H i over the ∼1 kpc extent of the starburst region. Regardless of the launch mechanism for the H i gas, the observed velocity decrease along the minor axis is sufficiently great that the H i may not escape the halo of M82. The inferred H i outflow rate at 10 kpc off the midplane is much less than 1

yr−1.
A Multiple Ejecta-circumstellar Medium Interaction Model and Its Implications for Superluminous Supernovae iPTF15esb and iPTF13dcc
Authors: Liu Liang-Duan , Wang Ling-Jun , Wang Shan-Qin , Dai Zi-Gao 
Published: March 2018

Abstract
In this paper, we investigate two hydrogen-poor superluminous supernovae (SLSNe), iPTF15esb and iPTF13dcc, whose light curves (LCs) show significant deviation from the smooth rise and fall. The LC of iPTF15esb exhibits two peaks and a post-peak plateau, and furthermore the late-time spectrum of iPTF15esb shows a strong, broad Hα emission line. The early-time LC of iPTF13dcc shows a long-duration bump followed by the second peak. Here, we propose an ejecta-circumstellar medium interaction model involving multiple shells/winds and use it to explain the LCs of iPTF15esb and iPTF13dcc. We find that the theoretical LCs reproduced by this model can match observations of iPTF15esb and iPTF13dcc. Based on our results, we infer that the progenitors have undergone multiple violent mass-loss processes before the SN explosion. In addition, we find that the variation trend of our inferred densities of the shells is consistent with that predicted by the stellar mass-loss history before an SN explosion. Further investigations for other bumpy SLSNe/SNe would shed light on their nature and provide a probe for the mass-loss history of their progenitors.
Study of the Abundance Features of the Metal-poor Star HD 94028
Authors: Han Wanqiang , Zhang Lu , Yang Guochao , Niu Ping , Zhang Bo 
Published: March 2018

Abstract
Recent work has found that the metal-poor star HD 94028 shows interesting abundance features. The s-process material (e.g., Ba, La, Ce, and Pb) and r-process material (e.g., Eu, Os, Pt) are mildly overabundant while the element C is not enhanced. However, the observed supersolar ratio [As/Ge] (=0.99 ± 0.23) and subsolar ratio [Se/As] (=−0.16 ± 0.22) could not be fitted by the combination of s- and r-process abundances. In this work, adopting the abundance decomposition method, we investigate the astrophysical origins of the elements in this star. We find that the primary process of massive stars dominates the production of the light elements and iron-group elements. The lighter neutron-capture elements from Ge to Te mainly come from the weak r-process. The elements from Ba to Pb are synthesized dominantly by the main s- and main r-process. The observed abundance features of Ge, As, and Se in HD 94028 are mainly produced by the weak r-process, which possesses the features of the supersolar ratio [As/Ge] and subsolar ratio [Se/As]. Because Ge is not synthesized solely by the neutron-capture process, As should be the lightest neutron-capture element. Although the i-process has been suggested in several astrophysical environments, it should be superfluous to explaining the abundances of the lighter neutron-capture elements in HD 94028.