bluuebunny/crossref_metadata_2025_split huggingface dataset:
ANALISIS VISUAL KARAKTER GATOTKACA DALAM GAME MOBILE LEGENDS BANG BANG
Authors: Latifah Ulil , Kristiana Nova 
Published: June 2021

Game Mobile Legends Bang Bang merupakan salah satu karya desain yang hingga kini masih digemari masyarakat di seluruh dunia tidak terkecuali Indonesia. Karakter pada game bervariasi dan menarik secara visual. Dalam penelitian ini peneliti menganalisis visual karakter dalam game Mobile Legends Bang Bang yaitu Gatotkaca. Permasalahan pada penelitian ini adalah bagaimana ciri-ciri fisik dan pemaknaan visual karakter Gatotkaca yang terdapat dalam game Mobile Legends Bang Bang. Penelitian ini menggunakan jenis penelitian kualitatif, teknik pengumpulan data menggunakan dokumentasi dan studi literatur, teknik pengolahan data menggunakan reduksi dan identifikasi data, teknik analisis data desktiptif menggunakan semiotika Roland Barthes. Berdasarkan hasil penelitian ini, diketahui bahwa ciri fisik karakter Gatotkaca terinspirasi dari tokoh legendaris di Indonesia yaitu Gatotkaca. Secara visual, karakter Gatotkaca telah mengalami penyederhanaan bentuk demi kemudahan dalam proses dimensionalnya secara realistis. Karakter Gatotkaca dalam game Mobile Legends Bang Bang dapat mencitrakan sosok Gatotkaca yang kuat dan perkasa dengan senjata sarung tangan Brajamukti-Brajadentanya. Hal ini yang membuat adanya karakter Gatotkaca dalam game Mobile Legends Bang Bang dapat disebut sebagai wujud pelestarian budaya Indonesia.
Kata Kunci: Barthes, Game, Gatotkaca, Semiotika.

VISUAL ANALYSIS OF GATOTKACA CHARACTERS
IN THE MOBILE LEGENDS BANG BANG GAME

Abstract
Mobile Legends Bang Bang, A game which has conception design and earns enormous popularity among society around the world including Indonesia. The characters in this game have many variations and visually appealing. Through this research, researcher analyses Mobile Legends Bang Bang character’s visual, Gatotkaca. The purpose of the study aims to examine physical characteristics and visual importance of Moblie Legends Bang Bang’s character, Gatotkaca. This research uses Qualitative approach, as data collection technique uses documentation and literature study. Meanwhile, data processing technique uses data reduction and identification, descriptive data technique uses Roland Barthes’ Semiotics. Established results of this study shows physical appearance of Gatotkaca’s character is inspired by legendary figure in Indonesia, Gatotkaca. Visually, the character of Gatotkaca has undergone many shape simplifications to ease its dimensional realistic processes. Gatotkaca’s character in Mobile Legends Bang Bang game images both strong and powerful Gatotkaca with his Brajamukti-Brajadenta gauntlet. This makes Gatotkaca’s character in Mobile Legends Bang Bang can be called as the form of Indonesia’s culture preservation.
Keywords: Barthes, Game, Gatotkaca, Semiotics.
LITERATUR REVIEW: APLIKASI MODEL HEALTH CARE SYSTEM DALAM INTERPROFESSIONAL COLLABORATION PADA PENANGANAN GIZI BURUK
Authors: Risnah Risnah , Musdalifah Mukhtar  , Muhammad Irwan  
Published: June 2021

Kesehatan ibu dan anak menjadi salah satu perhatian penting dalam bidang kesehatan. Anak sehat merupakan modal dasar hadirnya generasi yang berkualitas. Untuk itu memerlukan pemenuhan gizi yang optimal dalam proses pertumbuhan dan perkembangannya. Namun pada kenyataaannya, satu dari tiga anak atau sekitar 8 juta anak mengalami pertumbuhan tak maksimal yang diakibatkan oleh berbagai kondisi kekurangan gizi. Tapi harus diingat bersama bahwa permasalahan di system pelayanan kesehatan dapat tertangani dengan baik jika melibatkan seluruh profesi kesehatan dalam Interprofessional Collaboration.
Tujuan dari penelitian ini adalah untuk menganalisa artikel mengenai aplikasi health system dalam Interprofessional collaboration pada penanganan gizi buruk. Penelitian ini menggunakan desain literature review dengan melakukan penelusuran literatur di beberapa database, yakni Proquest, EBSCO, dan Sciencedirect. Artikel yang digunakan dengan rentang publikasi tahun 2005-2016. Berdasarkan hasil analisis dari artikel yang dikumpulkan, diperoleh hasil bahwa model Betty Neuman bisa diterapkan dalam konteks pelayanan multidisiplin yang menguatkan terlaksananya Interprofessional Collaboration sebagai upaya untuk mencegah fragmentasi dalam pemberian pelayanan untuk klien sehingga model ini dapat bekerja dengan baik dalam tatanan pelayanan yang berbasis multidisiplin
Direct Imaging of Exoplanets beyond the Radial Velocity Limit: Application to the HD 134987 System
Authors: Li Zhexing , Hildebrandt Sergi R. , Kane Stephen R. , Zimmerman Neil T. , Girard Julien H. , Gonzalez-Quiles Junellie , Turnbull Margaret C. 
Published: June 2021

Abstract
Future direct imaging missions will primarily observe planets that have been previously detected, mostly via the radial velocity (RV) technique, to characterize planetary atmospheres. In the meantime, direct imaging may discover new planets within existing planetary systems that have bright enough reflected flux but insufficient signals for other methods to detect. Here we investigate the parameter space within which planets are unlikely to be detected by RV in the near future due to precision limitations but could be discovered through reflected light with future direct imaging missions. We use the HD 134987 system as a working example, combine RV and direct imaging detection limit curves in the same parameter space through various assumptions, and insert a fictitious planet into the system while ensuring that it lies between the RV and imaging detection limits. Planet validity tested through dynamical simulations and retrieval tests revealed that the planet could indeed be detected by imaging while remaining hidden from RV surveys. Direct imaging retrieval was carried out using starshade simulations for two mission concepts: the Starshade Rendezvous Probe, which could be coupled with the Nancy Grace Roman Space Telescope, and the Habitable Exoplanet Observatory. This method is applicable to all other systems and high-contrast direct imaging instruments and could help inform future imaging observations and data analysis on the discovery of new exoplanets.
Gaia EDR3 Parallax Distances to the Great Carina Nebula and Its Star Clusters (Trumpler 14, 15, 16)
Authors: Shull J. Michael , Darling Jeremy , Danforth Charles W. 
Published: June 2021

Abstract
Using offset-corrected Gaia EDR3 parallax measurements and spectrophotometric methods, we have determined distances for 69 massive stars in the Carina OB1 association and associated clusters: Trumpler 16 (21 stars), Trumpler 14 (20 stars), Trumpler 15 (three stars), Bochum 11 (five stars), and South Pillars region (20 stars). Past distance estimates to the Carina Nebula range from 2.2 to 3.6 kpc, with uncertainties arising from photometry and anomalous dust extinction. The EDR3 parallax solutions show considerable improvement over DR2, with typical errors σ

ϖ
/ϖ ≈ 3%–5%. The O-type stars in the Great Carina Nebula lie at essentially the same distance (2.35 ± 0.08 kpc), quoting mean and rms variance. The clusters have distances of 2.32 ± 0.12 kpc (Tr 16), 2.37 ± 0.15 kpc (Tr 14), 2.36 ± 0.09 kpc (Tr 15), and 2.33 ± 0.12 kpc (Bochum 11) in good agreement with the η Car distance of around 2.3 kpc. O-star proper motions suggest internal (3D) velocity dispersions ∼4 km s−1 for Tr 14 and Tr 16. Reliable distances allow estimates of cluster sizes, stellar dynamics, luminosities, and fluxes of photoionizing radiation incident on photodissociation regions in the region. We estimate that Tr 14 and Tr 16 have half-mass radii r
h = 1.5–1.8 pc, stellar crossing times t
cr = r
h/v
m ≈ 0.7–0.8 Myr, and two-body relaxation times t
rh ≈ 40–80 Myr. The underlying velocity dispersion for Tr 14, if a bound cluster, would be

km s−1 for

stars. With the higher dispersions of the O stars, inward drift would occur slowly, on timescales of 3–6 Myr.
KCWI Observations of the Extended Nebulae in Mrk 273
Authors: Leung Gene C. K. , Coil Alison L. , Rupke David S. N. , Perrotta Serena 
Published: June 2021

Abstract
Ultraluminous infrared galaxies (ULIRGs) represent a critical stage in the merger-driven evolution of galaxies when active galactic nucleus (AGN) activity is common and AGN feedback is expected. We present high-sensitivity and large field-of-view integral field spectroscopy of the ULIRG Mrk 273 using new data from the Keck Cosmic Web Imager (KWCI). The KCWI data capture the complex nuclear region and the two extended nebulae in the northeast (NE) and southwest (SW) to ∼20 kpc scales. Kinematics in the nuclear region show a fast, extended, bipolar outflow in the direction of the previously reported nuclear superbubbles spanning ∼5 kpc, two to three times greater than the previously reported size. The larger-scale extended nebulae on ∼20 kpc show fairly uniform kinematics with FWHM ∼ 300 km s−1 in the SW nebula and FWHM ∼ 120 km s−1 in the NE nebula. We detect for the first time high-ionization [Ne v] 3426, [O iii] 4363, and He ii 4684 emission lines in the extended NE nebula. Emission line ratios in the nuclear region correlate with the kinematic structures, with the bipolar outflow and the less collimated “outflow regions” showing distinct line ratio trends. Line ratio diagnostics of high-ionization emission lines reveal a nontrivial contribution from shock plus precursor ionization in the NE nebula and the nuclear region mixed with AGN photoionization. These data are highly constraining for models of cool ionized gas existing 20 kpc from a galactic nucleus.
NGC 5128 Globular Cluster Candidates Out to 150 kpc: A Comprehensive Catalog from Gaia and Ground-based Data*
Authors: Hughes Allison K. , Sand David J. , Seth Anil , Strader Jay , Voggel Karina , Dumont Antoine , Crnojević Denija , Caldwell Nelson , Forbes Duncan A. , Simon Joshua D. , Guhathakurta Puragra , Toloba Elisa 
Published: June 2021

Abstract
We present a new catalog of 40,502 globular cluster (GC) candidates in NGC 5128 out to a projected radius of ∼150 kpc based on data from the Panoramic Imaging Survey of Centaurus and Sculptor, the Gaia Data Release 2, and the NOAO Source Catalog. Ranking these candidates based on the likelihood that they are true GCs, we find that approximately 1900 belong to our top two ranking categories and should be the highest priority for spectroscopic follow-up for confirmation. Taking into account our new data and a vetting of previous GC catalogs, we estimate a total GC population of 1450 ± 160 GCs. We show that a substantial number of sources previously argued to be low-velocity GCs are instead foreground stars, reducing the inferred GC velocity dispersion. This work showcases the power of Gaia to identify slightly extended sources at the ∼4 Mpc distance of NGC 5128, enabling accurate identification of GCs throughout the entire extended halo, not just the inner regions that have been the focus of most previous work.
Ultradense Gas Tracked by Unshifted Broad Absorption Lines in a Quasar
Authors: Tian Qiguo , Shi Xiheng , Hao Lei , Zhou Yipeng , Li Zhenzhen , Jiang Peng , Wu Shengmiao , Yang Chenwei , Zhang Shaohua , Zhou Hongyan 
Published: June 2021

Abstract
We present a detailed analysis of the broad absorption line system in the quasar SDSS J122017.06+454941.1, which are clearly detected in hydrogen Lyman series and metal lines, such as C iv, Si iv, Si iii, Al iii, and C ii, with a similar velocity as that of the broad emission lines. We reliably measured the column densities of H i, Al iii, and C ii, and obtained a low limit to Si iv and Si iii. With the help of the photoionization simulations, we found that the absorption gas has a hydrogen number density n
H ≈ 1011.03 cm−3 and a hydrogen column density N
H ≈ 1021.0 cm−2, and is exposed to the radiation with an ionization parameter U ≈ 10−1.25, and thus located the absorber at ∼0.3 pc from the central supermassive black hole, remarkably similar to the radius of the broad-line region (BLR; 0.17–0.84 pc as estimated by the luminosity–radius relation) of the quasar. It is likely that our line of sight may happen to intercept the low-column part of the BLR with a high density similar to that of the inferred value of the absorber. We suggest that detection of Al iii absorption line doublet in moderate quality quasar spectra could be a good indicator of dense gases, provided that the neutral hydrogen column density of the absorber is

.
On the Use of Field RR Lyrae as Galactic Probes. III. The α-element Abundances*
Authors: Crestani J. , Braga V. F. , Fabrizio M. , Bono G. , Sneden C. , Preston G. , Ferraro I. , Iannicola G. , Nonino M. , Fiorentino G. , Thévenin F. , Lemasle B. , Prudil Z. , Alves-Brito A. , Altavilla G. , Chaboyer B. , Dall’Ora M. , D’Orazi V. , Gilligan C. , Grebel E. K. , Koch-Hansen A. J. , Lala H. , Marengo M. , Marinoni S. , Marrese P. M. , Martínez-Vázquez C. , Matsunaga N. , Monelli M. , Mullen J. P. , Neeley J. , da Silva R. , Stetson P. B. , Salaris M. , Storm J. , Valenti E. , Zoccali M. 
Published: June 2021

Abstract
We provide the largest and most homogeneous sample of α-element (Mg, Ca, Ti) and iron abundances for field RR Lyrae (RRLs; 162 variables) by using high-resolution spectra. The current measurements were complemented with similar abundances available in the literature for 46 field RRLs brought to our metallicity scale. We ended up with a sample of old (t ≥ 10 Gyr), low-mass stellar tracers (208 RRLs: 169 fundamental, 38 first overtone, and 1 mixed mode) covering 3 dex in iron abundance (−3.00 ≤ [Fe/H] ≤ 0.24). We found that field RRLs are ∼0.3 dex more α poor than typical halo tracers in the metal-rich regime ([Fe/H] ≥ −1.2), while in the metal-poor regime ([Fe/H] ≤ −2.2) they seem to be on average ∼0.1 dex more α enhanced. This is the first time that the depletion in α elements for solar iron abundances is detected on the basis of a large, homogeneous, and coeval sample of old stellar tracers. Interestingly, we also detected a close similarity in the [α/Fe] trend between α-poor, metal-rich RRLs and red giants (RGs) in the Sagittarius dwarf galaxy as well as between α-enhanced, metal-poor RRLs and RGs in ultrafaint dwarf galaxies. These results are supported by similar elemental abundances for 46 field horizontal branch stars. These stars share with RRLs the same evolutionary phase and the same progenitors. This evidence further supports the key role that old stellar tracers play in constraining the early chemical enrichment of the halo and, in particular, in investigating the impact that dwarf galaxies have had in the mass assembly of the Galaxy.
Star Formation in Nuclear Rings with the TIGRESS Framework
Authors: Moon Sanghyuk , Kim Woong-Tae , Kim Chang-Goo , Ostriker Eve C. 
Published: June 2021

Abstract
Nuclear rings are sites of intense star formation at the centers of barred galaxies. To understand what determines the structure and star formation rate (SFR;

) of nuclear rings, we run semi-global, hydrodynamic simulations of nuclear rings subject to constant mass inflow rates

. We adopt the TIGRESS framework of Kim & Ostriker to handle radiative heating and cooling, star formation, and related supernova (SN) feedback. We find that the SN feedback is never strong enough to destroy the ring or quench star formation everywhere in the ring. Under the constant

, the ring star formation is very steady and persistent, with the SFR exhibiting only mild temporal fluctuations. The ring SFR is tightly correlated with the inflow rate as

, for a range of

. Within the ring, vertical dynamical equilibrium is maintained, with the midplane pressure (powered by SN feedback) balancing the weight of the overlying gas. The SFR surface density is correlated nearly linearly with the midplane pressure, as predicted by the pressure-regulated, feedback-modulated star formation theory. Based on our results, we argue that the ring SFR is causally controlled by

, while the ring gas mass adapts to the SFR to maintain the vertical dynamical equilibrium under the gravitational field arising from both gas and stars.
Could Switchbacks Originate in the Lower Solar Atmosphere? II. Propagation of Switchbacks in the Solar Corona
Authors: Magyar Norbert , Utz Dominik , Erdélyi Robertus , Nakariakov Valery M. 
Published: June 2021

Abstract
The magnetic switchbacks observed recently by the Parker Solar Probe have raised the question about their nature and origin. One of the competing theories of their origin is the interchange reconnection in the solar corona. In this scenario, switchbacks are generated at the reconnection site between open and closed magnetic fields, and are either advected by an upflow or propagate as waves into the solar wind. In this paper we test the wave hypothesis, numerically modeling the propagation of a switchback, modeled as an embedded Alfvén wave packet of constant magnetic field magnitude, through the gravitationally stratified solar corona with different degrees of background magnetic field expansion. While switchbacks propagating in a uniform medium with no gravity are relatively stable, as reported previously, we find that gravitational stratification together with the expansion of the magnetic field act in multiple ways to deform the switchbacks. These include WKB effects, which depend on the degree of magnetic field expansion, and also finite-amplitude effects, such as the symmetry breaking between nonlinear advection and the Lorentz force. In a straight or radially expanding magnetic field the propagating switchbacks unfold into waves that cause minimal magnetic field deflections, while a super-radially expanding magnetic field aids in maintaining strong deflections. Other important effects are the mass uplift the propagating switchbacks induce and the reconnection and drainage of plasmoids contained within the switchbacks. In the Appendix, we examine a series of setups with different switchback configurations and parameters, which broaden the scope of our study.
The TESS Objects of Interest Catalog from the TESS Prime Mission
Authors: Guerrero Natalia M. , Seager S. , Huang Chelsea X. , Vanderburg Andrew , Soto Aylin Garcia , Mireles Ismael , Hesse Katharine , Fong William , Glidden Ana , Shporer Avi , Latham David W. , Collins Karen A. , Quinn Samuel N. , Burt Jennifer , Dragomir Diana , Crossfield Ian , Vanderspek Roland , Fausnaugh Michael , Burke Christopher J. , Ricker George , Daylan Tansu , Essack Zahra , Günther Maximilian N. , Osborn Hugh P. , Pepper Joshua , Rowden Pamela , Sha Lizhou , Villanueva Jr. Steven , Yahalomi Daniel A. , Yu Liang , Ballard Sarah , Batalha Natalie M. , Berardo David , Chontos Ashley , Dittmann Jason A. , Esquerdo Gilbert A. , Mikal-Evans Thomas , Jayaraman Rahul , Krishnamurthy Akshata , Louie Dana R. , Mehrle Nicholas , Niraula Prajwal , Rackham Benjamin V. , Rodriguez Joseph E. , Rowden Stephen J. L. , Sousa-Silva Clara , Watanabe David , Wong Ian , Zhan Zhuchang , Zivanovic Goran , Christiansen Jessie L. , Ciardi David R. , Swain Melanie A. , Lund Michael B. , Mullally Susan E. , Fleming Scott W. , Rodriguez David R. , Boyd Patricia T. , Quintana Elisa V. , Barclay Thomas , Colón Knicole D. , Rinehart S. A. , Schlieder Joshua E. , Clampin Mark , Jenkins Jon M. , Twicken Joseph D. , Caldwell Douglas A. , Coughlin Jeffrey L. , Henze Chris , Lissauer Jack J. , Morris Robert L. , Rose Mark E. , Smith Jeffrey C. , Tenenbaum Peter , Ting Eric B. , Wohler Bill , Bakos G. Á. , Bean Jacob L. , Berta-Thompson Zachory K. , Bieryla Allyson , Bouma Luke G. , Buchhave Lars A. , Butler Nathaniel , Charbonneau David , Doty John P. , Ge Jian , Holman Matthew J. , Howard Andrew W. , Kaltenegger Lisa , Kane Stephen R. , Kjeldsen Hans , Kreidberg Laura , Lin Douglas N. C. , Minsky Charlotte , Narita Norio , Paegert Martin , Pál András , Palle Enric , Sasselov Dimitar D. , Spencer Alton , Sozzetti Alessandro , Stassun Keivan G. , Torres Guillermo , Udry Stephane , Winn Joshua N. 
Published: June 2021

Abstract
We present 2241 exoplanet candidates identified with data from the Transiting Exoplanet Survey Satellite (TESS) during its 2 yr Prime Mission. We list these candidates in the TESS Objects of Interest (TOI) Catalog, which includes both new planet candidates found by TESS and previously known planets recovered by TESS observations. We describe the process used to identify TOIs, investigate the characteristics of the new planet candidates, and discuss some notable TESS planet discoveries. The TOI catalog includes an unprecedented number of small planet candidates around nearby bright stars, which are well suited for detailed follow-up observations. The TESS data products for the Prime Mission (sectors 1–26), including the TOI catalog, light curves, full-frame images, and target pixel files, are publicly available at the Mikulski Archive for Space Telescopes.
The Ultraviolet Extinction Map and Dust Properties at High Galactic Latitude
Authors: Sun 孙 Mingxu 明旭 , Jiang 姜 Biwei 碧沩 , Yuan 苑 Haibo 海波 , Li 李 Jun 军 
Published: June 2021

Abstract
Extinction in ultraviolet is much more significant than in optical or infrared, which can be very informative to precisely measure the extinction and understand the dust properties in the low-extinction areas. The high Galactic latitude sky is such an area, important for studying the extragalactic sky and the universe. Based on the stellar parameters measured by the LAMOST and GALAH spectroscopy and the ultraviolet photometry by the Galaxy Evolution Explorer (GALEX) space telescope, the extinction of 1,244,504 stars in the GALEX/near-UV band and 56,123 stars in the GALEX/far-UV band is calculated precisely. The error of color excess is 0.009, 0.128, and 0.454 mag for

,

, and

, respectively. They delineate the GALEX/near-UV extinction map of about a third of the sky mainly at the high Galactic latitude area with an angular resolution of ∼ 0.°4. The mean color excess ratio in the entire sky area is derived to be 3.25, 2.95, and −0.37 for

,

, and

, respectively, which is in general agreement with the previous works, and their changes with the Galactic latitude and the interstellar extinction are discussed.
Dynamical Effects of Cosmic Rays on the Medium Surrounding Their Sources
Authors: Schroer Benedikt , Pezzi Oreste , Caprioli Damiano , Haggerty Colby , Blasi Pasquale 
Published: June 2021

Abstract
Cosmic rays (CRs) leave their sources mainly along the local magnetic field; in doing so they excite both resonant and nonresonant modes through streaming instabilities. The excitation of these modes leads to enhanced scattering and in turn to a large pressure gradient that causes the formation of bubbles of gas, CRs, and self-generated magnetic fields expanding into the interstellar medium. By means of hybrid particle-in-cell simulations, we show that, by exciting the nonresonant instability, CRs excavate a cavity around their source where the diffusivity is strongly suppressed. This finding invalidates the so far largely adopted flux-tube assumption, under which particles move along magnetic lines even in the nonlinear regime. This phenomenon is general and is expected to occur around any sufficiently powerful CR source in the Galaxy. Our results might provide a physical explanation of the numerous claims of suppressed CR diffusion around Galactic sources such as supernova remnants, pulsar wind nebulae, and stellar clusters.