bluuebunny/crossref_metadata_2025_split huggingface dataset:
PENGARUH LINGKUNGAN KERJA DAN GAYA KEPEMIMPINAN TERHADAP KINERJA KARYAWAN PADA PERUSAHAAN CUCI SARANG BURUNG WALET MANGLI JAYA
Authors: Nugraha Alifian , Ningsih Winarti 
Published: March 2020

Penelitian ini bertujuan untuk mengetahui pengaruh lingkungan kerja dan gaya kepemimpinan terhadap kinerja karyawan pada perusahaan cuci sarang burung walet Mangli Jaya. Jenis penelitian yang digunakan dalam penelitian ini merupakan penelitian kuantitatif yaitu suatu bentuk pengumpulan data yang bertujuan menggambarkan dan menekankan analisisnya pada data data numerik atau angka guna menguraikan suatu keadaan atau masalah dari objek yang diteliti. Populasi yang digunakan dalam penelitian ini adalah seluruh karyawan Perusahaan Cuci Sarang Burung Walet Mangli Jaya kec. Kaliwates Jember yang berjumlah 31 orang. Mengingat jumlah populasi yang tersedia dalam penelitian ini kecil, maka penelitian ini mengobservasi semua anggota jadi semua populasi dijadikan sampel penelitian. Berdasarkan masalah yang timbul, tujuan penelitian, dan hasil analisis, maka dapat diambil kesimpulan sebagai berikut: Koefisien determinasi dinyatakan nilai Adjusted R Square adalah 0,704 atau 70,4%. Regresi berganda dengan persamaan Y= 3,967+0,136X1+0,080X2+0,704 artinya tanpa dipengaruhi apapun maka kinerja karyawan mempunyai nilai konstanta positif sebesar 3,967. Dengan peningkatan satu variabel X1 maka akan meningkatkan kinerja karyawan sebesar 0,136 satuan. Dengan peningkatan satu variabel X2 maka akan meningkatkan kinerja karyawan sebesar 0,080 satuan. Uji secara simultan lingkungan kerja dan gaya kepemimpinan berpengaruh terhadap kinerja karyawan di Perusahaan Cuci Sarang Burung Walet Mangli Jaya kec. Kaliwates Jember. Uji secara parsial hanya satu variabel yang berpengaruh terhadap kinerja karyawan, yaitu variabel gaya kepemimpinan.
PENGELOLAAN ALOKASI DANA DESA (STUDI PADA DESA ALASMALANG KECAMATAN PANARUKAN KABUPATEN SITUBONDO)
Authors: Raharjo Sigit Sustyo , Wahono Puji , Wahyudi Edy 
Published: March 2020

Keterbatasan keuangan yang dimiliki desa menyebabkan ketimpangan pembangunan antara desa dengan kota. Diperlukan keberpihakan pemerintah pusat dan daerah dalam mendukung ketersediaaan anggaran bagi desa untuk melaksanakan tata kelola pemerintahan dan pembangunan. Alokasi Dana Desa (ADD) merupakan salah satu cara untuk mempercepat pembangunan di desa. Sejak tahun 2015, terjadi peningkatan yang signifikan atas penerimaan ADD karena Kabupaten wajib menganggarkan minimal 10% dari APBD untuk alokasi dana desanya sesuai amanah Undang-undang Nomor 6 Tahun 2014. Peningkatan ADD tersebut merupakan berkah dan tantangan bagi desa untuk bisa mengelola sesuai dengan prinsip-prinsip tata kelola pemerintahan yang baik (good governance). Karena desa saat ini masih dihadapkan pada keterbatasan kualitas sumber daya aparatur yang rendah, rendahnya kemampuan perencanaan, dan sarana prasarana lam pengelolaan ADD. Kata Kunci: Pengelolaan, Alokasi Dana Desa
ANALISIS PENGENDALIAN PERSEDIAAN BAHAN BAKU DENGAN METODE ECONOMIC ORDER QUANTITY PADA CV. DIKA JOK JENGGAWAH
Authors: Hotima Siti Husnul , Hayati Dini 
Published: March 2020

Tujuan yang diharapkan dari penelitian ini adalah ingin menganalisis persediaan bahan baku optimal yang dibutuhkan dengan menggunakan metode Economic Order Quantity (EOQ), menganalisis berapa besar persediaan pengaman (Safety stock), menganalisis kapan waktu yang tepat untuk melakukan pemesanan kembali (reorder point), menganalisis total persediaan bahan baku atau Total Inventory Cost (TIC). Jenis penelitian yang digunakan adalah kuantitatif deskriptif. Teknik pengumpulan data yang digunakan dalam penelitian ini adalah wawancara, observasi, dan dokumentasi. Penelitian dan hasil perhitungan yang dilakukan menunjukkan bahwa persediaan bahan baku setiap tahunnya tidak stabil. Bahan baku yang dibutuhkan oleh perusahaan apabila dihitung menggunakan metode Economic Order Quantity (EOQ) pada tahun 2016 adalah sebesar 11,52 m3 dengan frekuensi pembelian 6 kali per periode (1 tahun). Tahun 2017 sebesar 9,90 m3 dengan frekuensi pembelian 6 kali per periode (1 tahun). Persediaan pengaman (safety stock) pada tahun 2016 adalah sebesar 16,48 m3. Pada tahun 2017 sebesar 11,25 m3. Titik pemesanan kembali (reorder point) pada tahun 2016 adalah sebesar 17,18 m3. Pada tahun 2017 sebesar 13,1 m3. Total biaya persediaan bahan baku yang dihitung menurut Economic Order Point (EOQ) lebih sedikit dibandingkan dengan yang dikeluarkan oleh perusahaan, maka ada penghematan biaya persediaan. Pada tahun 2016 sebesar Rp.110.499.402 dan pada tahun 2017 sebesar Rp.81.655.306. Kata Kunci: Economic Order Quantity (EOQ), Persediaan Pengaman (Safety Stock), Titik Pemesanan Kembali (Reorder Point), Total Biaya Persediaan atau Total Inventory Cost (TIC).
Incidence of poor student nutrition affects academic performance
Authors: Quijije Logroño Elizabeth Briggitte 
Published: March 2020

The research we have selected ns does conclude the importance of nutrition is on academic achievement can take it as an afterthought but having a proper diet to follow the directions of a food pyramid helps children in growth not only physical if not intellectual, this project can focus percent of techniques we use are among the information leaflet and talks given by students, teachers and parents, with the aim of training students informed, teaching guides to conduct future workshops on the same subject investigated, and properly oriented parents on the proper use of foods your children will. In this research are problems of disinformation, guidance materials. Thanks to each of the surveys are different from them alternative responses, which could evaluate and purchase the problems that exist and thanks to the implementation of our proposal to develop an awareness raising workshop on proper and adequate food He could feel the change in children, as we did an evaluation after applying the proposal, improving intellectual activity of students in the area of school and we are confident that our proposal gave a view that short time we managed to guide everyone involved in our research, with the mission of our awareness workshop if served paramount to benefit children Garden Tax School No.1 Enrique Decker Acosta.
Potential Themis-family Asteroid Contribution to the Jupiter-family Comet Population
Authors: Hsieh Henry H. , Novaković Bojan , Walsh Kevin J. , Schörghofer Norbert 
Published: March 2020

Abstract
Recent dynamical analyses suggest that some Jupiter family comets (JFCs) may originate in the main asteroid belt instead of the outer solar system. This possibility is particularly interesting given evidence that icy main-belt objects are known to be present in the Themis asteroid family. We report results from dynamical analyses specifically investigating the possibility that icy Themis family members could contribute to the observed population of JFCs. Numerical integrations show that such dynamical evolution is indeed possible via a combination of eccentricity excitation apparently driven by the nearby 2:1 mean-motion resonance with Jupiter, gravitational interactions with planets other than Jupiter, and the Yarkovsky effect. We estimate that, at any given time, there may be tens of objects from the Themis family on JFC-like orbits with the potential to mimic active JFCs from the outer solar system, although not all, or even any, may necessarily be observably active. We find that dynamically evolved Themis family objects on JFC-like orbits have semimajor axes between 3.15 and 3.40 au for the vast majority of their time on such orbits, consistent with the strong role that the 2:1 mean-motion resonance with Jupiter likely plays in their dynamical evolution. We conclude that a contribution from the Themis family to the active JFC population is plausible, although further work is needed to better characterize this contribution.
Spectroscopic Determination of Stellar Parameters and Oxygen Abundances for Hyades/Field G–K Dwarfs
Authors: Takeda Yoichi , Honda Satoshi 
Published: March 2020

Abstract
It has been suggested that Fe abundances of K dwarfs derived from Fe i and Fe ii lines show considerable discrepancies, and oxygen abundances determined from high-excitation O i 7771–5 triplet lines are appreciably overestimated (the problem becoming more serious toward lower T
eff), which, however, has not yet been widely confirmed. With the aim of clarifying this issue, we spectroscopically determined the atmospheric parameters of 148 G–K dwarfs (Hyades cluster stars and field stars) by assuming the classical Fe i/Fe ii ionization equilibrium as usual, and determined their oxygen abundances by applying the non-local thermal equilibrium spectrum fitting analysis to O i 7771–5 lines. It turned out that the resulting parameters did not show any significant inconsistency with those determined by other methods (for example, the mean differences in T
eff and

from the well-determined solutions of Hyades dwarfs are mostly ≲100 K and ≲0.1 dex). Likewise, the oxygen abundances of Hyades stars are around [O/H] ∼ +0.2 dex (consistent with the metallicity of this cluster) without exhibiting any systematic T
eff-dependence. Accordingly, we conclude that parameters can be spectroscopically evaluated to a sufficient precision in the conventional manner (based on the Saha–Boltzmann equation for Fe i/Fe ii) and oxygen abundances can be reliably determined from the O i 7771–5 triplet for K dwarfs as far as stars of T
eff ≳ 4500 K are concerned. We suspect that previously reported strongly T
eff-dependent discrepancies may have stemmed mainly from overestimation of weak-line strengths and/or improper T
eff scale.
The Green Bank North Celestial Cap Pulsar Survey. V. Pulsar Census and Survey Sensitivity
Authors: McEwen A. E. , Spiewak R. , Swiggum J. K. , Kaplan D. L. , Fiore W. , Agazie G. Y. , Blumer H. , Chawla P. , DeCesar M. , Kaspi V. M. , Kondratiev V. I. , LaRose M. , Levin L. , Lynch R. S. , McLaughlin M. , Mingyar M. , Noori H. Al , Ransom S. M. , Roberts M. S. E. , Schmiedekamp A. , Schmiedekamp C. , Siemens X. , Stairs I. , Stovall K. , Surnis M. , van Leeuwen J. 
Published: March 2020

Abstract
The Green Bank North Celestial Cap (GBNCC) pulsar survey will cover the entire northern sky (δ > −40°) at 350 MHz, and is one of the most uniform and sensitive all-sky pulsar surveys to date. We have created a pipeline to reanalyze GBNCC survey data to take a 350 MHz census of all pulsars detected by the survey, regardless of their discovery survey. Of the 1413 pulsars in the survey region, we were able to recover 670. For these we present measured signal-to-noise ratios (S/N), flux densities, pulse widths, profiles, and where appropriate, refined measurements of dispersion measures (DMs) (656 out of 670) and new or improved spectral indices (339 out of 670 total, 47 new, 292 improved). We also measure the period-pulse width relation at 350 MHz to scale as

. Detection scans for several hundred sources were reanalyzed in order to inspect pulsars’ single pulse behavior and 223 were found to exhibit evidence of nulling. With a detailed analysis of measured and expected S/N values and the evolving radio frequency interference environment at 350 MHz, we assess the GBNCC survey’s sensitivity as a function of spin period, DM, and sky position. We find the sky-averaged limiting flux density of the survey to be 0.74 mJy. Combining this analysis with PsrPopPy pulsar population simulations, we predict 60/5 nonrecycled/MSP discoveries in the survey’s remaining 21,000 pointings, and we begin to place constraints on population model parameters.
ZFIRE: Measuring Electron Density with [O ii] as a Function of Environment at z = 1.62
Authors: Harshan Anishya , Gupta Anshu , Tran Kim-Vy , Alcorn Leo Y. , Yuan Tiantian , Kacprzak Glenn G. , Nanayakkara Themiya , Glazebrook Karl , Kewley Lisa J. , Labbé Ivo , Papovich Casey 
Published: March 2020

Abstract
The global star formation rates (SFR) of galaxies at fixed stellar masses increase with redshift and are known to vary with environment up to z ∼ 2. We explore here whether the changes in the SFRs also apply to the electron densities of the interstellar medium by measuring the [O ii] (

,

) ratio for cluster and field galaxies at z ∼ 2. We measure a median electron density of

= 366 ± 84 cm

for six galaxies (with 1σ scatter = 163 cm

) in the Ultra-Deep Survey (UDS) protocluster at z = 1.62. We find that the median electron density of galaxies in the UDS protocluster environment is three times higher compared to the median electron density of field galaxies (

= 113 ± 63 cm

and 1σ scatter = 79 cm

) at comparable redshifts, stellar mass, and SFR. However, we note that a sample of six protocluster galaxies is insufficient to reliably measure the electron density in the average protocluster environment at z ∼ 2. We conclude that the electron density increases with redshift in both cluster and field environments up to z ∼ 2 (

= 30 ± 1 cm

for z ∼ 0 to

= 254 ± 76 cm

for z ∼ 1.5). We find tentative evidence (∼2.6σ) for a possible dependence of electron density on environment, but the results require confirmation with larger sample sizes.
Proper Motions of the Radio Source Orion MR, Formerly Known as Orion n, and New Sources with Large Proper Motions in Orion BN/KL
Authors: Rodríguez Luis F. , Dzib Sergio A. , Zapata Luis , Lizano Susana , Loinard Laurent , Menten Karl M. , Gómez Laura 
Published: March 2020

Abstract
The infrared source known as Orion n was detected in 1980. About two decades later, sensitive observations made with the Very Large Array (VLA) revealed the presence of a spatially coincident millijansky double source that appeared to be its radio counterpart. However, over the years it has been concluded that the radio source shows large proper motions to the south while the infrared source n is stationary. Here we reanalyze the proper motions of the radio source adding both older and newer VLA observations than previously used. We confirm the proper motions of the double radio source that at present no longer coincides positionally with the infrared source. We propose that the infrared source is stationary while the radio source is moving as a result of the explosion that took place in this region some 500 yr ago. Considering the paper where it was first reported, we refer to this double radio source as Orion MR. Additionally, we use these new observations to fully confirm the large proper motions of the sources IRc23 and Zapata 11. Together with sources BN, I, Orion MR, and x, there are at least six compact sources that recede from a common point in Orion BN/KL. However, IRc23 is peculiar in that its ejection age appears to be only 300 yr. The relatively large number of sources rules out as a possible mechanism the classic three-body scenario since then only two escaping bodies are expected: a tight binary plus the third star involved in the encounter.
The Lowest of the Low: Discovery of SN 2019gsc and the Nature of Faint Iax Supernovae
Authors: Srivastav Shubham , Smartt Stephen J. , Leloudas Giorgos , Huber Mark E. , Chambers Ken , Malesani Daniele B. , Hjorth Jens , Gillanders James H. , Schultz A. , Sim Stuart A. , Auchettl Katie , Fynbo Johan P. U. , Gall Christa , McBrien Owen R. , Rest Armin , Smith Ken W. , Wojtak Radoslaw , Young David R. 
Published: March 2020

Abstract
We present the discovery and optical follow-up of the faintest supernova-like transient known. The event (SN 2019gsc) was discovered in a star-forming host at 53 Mpc by ATLAS. A detailed multicolor light curve was gathered with Pan-STARRS1 and follow-up spectroscopy was obtained with the Nordic Optical Telescope and Gemini-North. The spectra near maximum light show narrow features at low velocities of 3000–4000 km s−1, similar to the extremely low-luminosity SNe 2010ae and 2008ha, and the light curve displays a similar fast decline (Δm
15(r) = 0.91 ± 0.10 mag). SNe 2010ae and 2008ha have been classified as SNe Iax, and together the three either make up a distinct physical class of their own or are at the extreme low-luminosity end of this diverse supernova population. The bolometric light curve is consistent with a low kinetic energy of explosion (E
k ∼ 1049 erg s−1), a modest ejected mass (M
ej ∼ 0.2 M
⊙), and radioactive powering by 56Ni (M
Ni ∼ 2 × 10−3 M
⊙). The spectra are quite well reproduced with radiative transfer models (TARDIS) and a composition dominated by carbon, oxygen, magnesium, silicon, and sulfur. Remarkably, all three of these extreme Iax events are in similar low-metallicity star-forming environments. The combination of the observational constraints for all three may be best explained by deflagrations of near M
Ch hybrid carbon–oxygen–neon white dwarfs that have short evolutionary pathways to formation.
CO, Water, and Tentative Methanol in η Carinae Approaching Periastron
Authors: Morris Patrick W. , Charnley Steven B. , Corcoran Michael , Cordiner Martin , Damineli Augusto , Groh Jose H. , Gull Theodore R. , Loinard Laurent , Madura Thomas , Mehner Andrea , Moffat Anthony , Palmer Maureen Y. , Rau Gioia , Richardson Noel D. , Weigelt Gerd 
Published: March 2020

Abstract
The complex circumstellar environment around the massive binary and luminous blue variable η Carinae is known to harbor numerous light molecules, emitting most strongly in rotational states with upper level energies to ∼300 K. In circumstellar gas, the complex organic molecule methanol (CH3OH) has been found almost exclusively around young stellar objects, and thus regarded as a signpost of recent star formation. Here we report the first potential detection of methanol around a highly evolved high-mass star, while using the Atacama Large Millimeter Array to investigate molecular cloud conditions traced by CO (2–1) in an orbit phase preceding the 2020 periastron. The methanol emission originates from hot (T
gas ≃ 700 K) material, ∼2″ (0.02 pc) across, centered on the dust-obscured binary, and is accompanied by prominent absorption of continuum radiation in a cooler (T
gas ≃ 110 K) layer of gas. We also report a first detection of water in Herschel observations at 557 and 988 GHz. The methanol abundance is several to 50 times higher than observed toward several lower-mass stars, while water abundances are similar to those observed in cool, dense molecular clouds. The very high methanol:water abundance ratio in the core of η Car may suggest methanol formation processes similar to Fischer–Tropsch-type catalytic reactions on dust grains. These observations prove that complex molecule formation can occur in a chemically evolved massive stellar environment, given sufficient gas densities and shielding conditions as may occur in material around massive interacting companions and merger remnants.
SDSS-IV MaNGA: Kinematic Asymmetry as an Indicator of Galaxy Interaction in Paired Galaxies
Authors: Feng 冯 Shuai 帅 , Shen 沈 Shi-Yin 世银 , Yuan 袁 Fang-Ting 方婷 , Riffel Rogemar A. , Pan Kaike 
Published: March 2020

Abstract
The interaction between galaxies is believed to be the main origin of the peculiarities of galaxies, which disturbs not only the morphology but also their kinematics. These disturbed and asymmetric features are the indicators of galaxy interaction. We study the velocity field of the ionized gas of the paired galaxies in the SDSS-IV MaNGA IFU survey. Using the kinemetry package, we fit the velocity field of the ionized gas to quantify the degree of kinematic asymmetry. We find that the star formation rate (SFR) of the paired galaxies with high kinematic asymmetry is significantly enhanced even when the projected separation between the pair members is quite large (

). On the contrary, no significant SFR enhancement is found for the paired galaxies with low kinematic asymmetry even when their projected separation is small (

). Moreover, we also find that the fraction of galaxies with high kinematic asymmetry is much higher in close pairs (

) than those with larger

, which explains well the early statistical finding of the significant SFR enhancement in close pairs. Our new findings illustrate that the kinematic asymmetry is an excellent indicator of galaxy–galaxy interaction strength, which helps us better understand the merging stage of the observed galaxy pairs.
Catheter Ablation of Idiopathic Ventricular Arrhythmias Originating from the Para-Hisian area - QRS Morphology Change and Late Effect of the Ablation: Case Series
Authors: Dzhinsov Krasimir R. , Stoyanov Milko K. , Shalganov Tchavdar N. 
Published: March 2020

Introduction: Radiofrequency catheter ablation of idiopathic ventricular arrhythmias originating in the para-Hisian region could be challenging because of a potential risk of iatrogenic atrioventricular block. Uncommonly, shift of the exit site during the ablation can be observed. Consequently, different approaches of radiofrequency catheter ablation of para-Hisian ventricular foci can be needed.
&nbsp;
Case series presentation: Three patients (2 males) underwent electroanatomical mapping and catheter ablation for idiopathic premature ventricular contractions originating near the His bundle. Patients underwent 24-h ECG Holter monitoring during follow-up. All patients had premature ventricular contractions with left bundle branch block morphology and inferior or horizontal axis. However, change of QRS morphology during ablation was observed, due to a change in the exit site. In two patients there was reduction of the arrhythmia burden after initially unsuccessful procedure. Mapping and ablation in the aortic root were needed in one patient. There were no complications.
&nbsp;
Discussion: Radiofrequency catheter ablation of para-Hisian ventricular arrhythmias is feasible and safe when performed cautiously. A change in the premature ventricular contractions&rsquo; morphology and exit site during ablation may ensue; therefore, extensive mapping on both sides of the interventricular septum as well as in the aortic root may be warranted.
Evaluation of the Immune Response Against Helicobacter pylori in Infused BALB/c Mice by pcDNA3.1(+)-ureA&nbsp;
Authors: Nasr-Esfahani Maryam , Doosti Abbas , Sazegar Hossein 
Published: March 2020

Background: The purpose of the present study was to produce a pcDNA3.1(+)-ureA recombinant vector and evaluate the capacity of this vector to stimulate the immune response against H. pylori infection in infused BALB/c mice.&nbsp;
&nbsp;
Materials and methods: The pcDNA3.1(+)-ureA construct was prepared and transformed into E. coli, successfully. The animals we used in the study were allotted into three groups for infusion of 1) recombinant plasmid, 2) pcDNA3.1(+)-ureA + nanoparticles, and 3) pcDNA3.1(+). Blood and tissue specimens from each group of mice were collected at days 15, 30, and 45 after the last infusion and the expression levels of cytokines such as TGF-&beta;1, IL-4, and IFN&gamma; genes comparing to GAPDH as well as the expression of ureA in the mice&rsquo;s thigh muscle were evaluated.&nbsp;
&nbsp;
Results: The genes expression analysis showed that the IL4 expression significantly decreased (p<0.001) but IFN&gamma; and TGF-&beta;1 expression increased in the blood of infused mice (p<0.001). Also, the urea expression level in pcDNA3.1(+)-urea and pcDNA3.1(+)-ureA+ nanoparticle 15, 30, and 45 days after the last infusion was significantly different (p<0.001) and its expressions at days 15 and 30 were significantly different (p<0.001), but 45 days after the last infusion it was not significantly different (p>0.05).&nbsp;
&nbsp;
Conclusion: The pcDNA3.1(+)-ureA recombinant vector with or without chitosan nanoparticles can stimulate the immune response in animal models against H. pylori infection. Also, after combining the recombinant vector with nanoparticles we observed a better immune response was observed. In future studies this recombinant construct can be used as a biomarker and therapeutic approaches in eukaryotic systems.