bluuebunny/crossref_metadata_2025_split huggingface dataset:
Pengaruh rasa ingin tahu terhadap koneksi matematis siswa pada pembelajaran trigonometri menggunakan model kooperatif tipe Think Talk Write (TTW) di kelas X SMA Negeri 10 Banjarmasin tahun pelajaran 2016-2017
Authors: Apriyanto Apriyanto , Royani M. , Atsnan Muh. Fajaruddin 
Published: February 2019

Tujuan penelitian ini adalah untuk mengetahui rasa ingin tahu, kemampuan koneksi matematis, dan ada tidaknya pengaruh rasa ingin tahu terhadap kemampuan koneksi matematis siswa pada pembelajaran trigonometri menggunakan model kooperatif tipe think talk write (TTW) di kelas X-1 SMA Negeri 10 Banjarmasin tahun pelajaran 2016-2017. Metode penelitian menggunakan metode penelitian deskriptif. Populasi adalah siswa kelas X SMA Negeri 10 Banjarmasin tahun pelajaran 2016-2017 yang berjumlah 226 siswa. Teknik pengambilan sampel menggunakan cluster random sampling. Sampel dalam penelian ini adalah siswa kelas X-1 SMA Negeri 10 Banjarmasin yang berjumlah 36 siswa. Teknik pengumpulan data menggunakan observasi dan tes. Hasil penelitian tentang pembelajaran trigonometri menggunakan model kooperatif tipe think talk write (TTW) di kelas X-1 SMA Negeri 10 Banjarmasin menunjukkan bahwa: (1) Karakter rasa ingin tahu siswa termasuk dalam kualifikasi sudah berkembang, (2) Kemampuan koneksi antar konsep matematika siswa termasuk dalam kategori baik, (3) Ada pengaruh karakter rasa ingin tahu terhadap kemampuan koneksi matematis siswa.
Penerapan model pembelajaran direct instruction dipadukan dengan snowball drilling untuk meningkatkan hasil belajar matematika siswa kelas VI SDN Jejangkit Muara 2
Authors: Agustina Rahidatul Laila , Hidayatullah Syarif 
Published: February 2019

Penelitian ini bertujuan untuk melihat bagaimana peningkatan aktivitas guru, aktivitas siswa dan hasil belajar matematika siswa dalam penerapan model pembelajaran direct instruction dipadukan dengan snowball drilling. Metode yang digunakan dalam penelitian ini adalah Penelitian Tindakan Kelas (PTK), bersifat kolaborasi. Hasil analisis data menunjukkan terjadi peningkatan aktivitas guru dalam kegiatan pembelajaran, aktivitas guru pada siklus I pertemuan pertama memperoleh skor 24, sedangkan pada pertemuan kedua memperoleh skor 29. dan pada siklus II pertemuan pertama memperoleh skor 32 sedangkan pada pertemuan kedua memperoleh skor 36. Persentase aktivitas siswa secara klasikal pada siklus I pertemuan pertama mencapai 52% sedangkan pada pertemuan keduanya 62%, dan pada siklus II pertemuan pertama mencapai 76% sedangkan pada pertemuan keduanya mencapai 89%. Hasil belajar berdasarkan tes akhir siklus I secara klasikal mencapai 65% kemudian meningkat pada siklus II mencapai 90%.
Incentive schemes to increase dementia diagnoses in primary care in England: a retrospective cohort study of unintended consequences
Authors: Liu Dan , Green Emily , Kasteridis Panagiotis , Goddard Maria , Jacobs Rowena , Wittenberg Raphael , Mason Anne 
Published: February 2019

BackgroundThe UK government introduced two financial incentive schemes for primary care to tackle underdiagnosis in dementia: the 3-year Directed Enhanced Service 18 (DES18) and the 6-month Dementia Identification Scheme (DIS). The schemes appear to have been effective in boosting dementia diagnosis rates, but their unintended effects are unknown.AimTo identify and quantify unintended consequences associated with the DES18 and DIS schemes.Design and settingA retrospective cohort quantitative study of 7079 English primary care practices.MethodPotential unintended effects of financial incentive schemes, both positive and negative, were identified from a literature review. A practice-level dataset covering the period 2006/2007 to 2015/2016 was constructed. Difference-in-differences analysis was employed to test the effects of the incentive schemes on quality measures from the Quality and Outcomes Framework (QOF); and four measures of patient experience from the GP Patient Survey (GPPS): patient-centred care, access to care, continuity of care, and the doctor–patient relationship. The researchers controlled for effects of the contemporaneous hospital incentive scheme for dementia and for practice characteristics.ResultsNational practice participation rates in DES18 and DIS were 98.5% and 76% respectively. Both schemes were associated not only with a positive impact on QOF quality outcomes, but also with negative impacts on some patient experience indicators.ConclusionThe primary care incentive schemes for dementia appear to have enhanced QOF performance for the dementia review, and have had beneficial spillover effects on QOF performance in other clinical areas. However, the schemes may have had negative impacts on several aspects of patient experience.
HAWC+/SOFIA Multiwavelength Polarimetric Observations of OMC-1
Authors: Chuss David T. , Andersson B-G , Bally John , Dotson Jessie L. , Darren Dowell C. , Guerra Jordan A. , Harper Doyal A. , Houde Martin , Jay Jones Terry , Lazarian A. , Lopez Rodriguez Enrique , Michail Joseph M. , Morris Mark R. , Novak Giles , Siah Javad , Staguhn Johannes , Vaillancourt John E. , Volpert C. G. , Werner Michael , Wollack Edward J. , Benford Dominic J. , Berthoud Marc , Cox Erin G. , Crutcher Richard , Dale Daniel A. , Fissel L. M. , Goldsmith Paul F. , Hamilton Ryan T. , Hanany Shaul , Henning Thomas K. , Looney Leslie W. , Harvey Moseley S. , Santos Fabio P. , Stephens Ian , Tassis Konstantinos , Trinh Christopher Q. , Van Camp Eric , Ward-Thompson Derek ,   (HAWC + Science Team)
Published: February 2019

Abstract
We report new polarimetric and photometric maps of the massive star-forming region OMC-1 using the HAWC+ instrument on the Stratospheric Observatory for Infrared Astronomy. We present continuum polarimetric and photometric measurements of this region at 53, 89, 154, and 214 μm at angular resolutions of 5″, 8″, 14″, and 19″ for the four bands, respectively. The photometric maps enable the computation of improved spectral energy distributions for the region. We find that at the longer wavelengths, the inferred magnetic field configuration matches the “hourglass” configuration seen in previous studies, indicating magnetically regulated star formation. The field morphology differs at the shorter wavelengths. The magnetic field inferred at these wavelengths traces the bipolar structure of the explosive Becklin–Neugebauer/Kleinman–Low outflow emerging from OMC-1 behind the Orion Nebula. Using statistical methods to estimate the field strength in the region, we find that the explosion dominates the magnetic field near the center of the feature. Farther out, the magnetic field is close to energetic equilibrium with the ejecta and may be providing confinement to the explosion. The correlation between polarization fraction and the local polarization angle dispersion indicates that the depolarization as a function of unpolarized intensity is a result of intrinsic field geometry as opposed to decreases in grain alignment efficiency in denser regions.
The First Tidal Disruption Flare in ZTF: From Photometric Selection to Multi-wavelength Characterization
Authors: van Velzen Sjoert , Gezari Suvi , Cenko S. Bradley , Kara Erin , Miller-Jones James C. A. , Hung Tiara , Bright Joe , Roth Nathaniel , Blagorodnova Nadejda , Huppenkothen Daniela , Yan Lin , Ofek Eran , Sollerman Jesper , Frederick Sara , Ward Charlotte , Graham Matthew J. , Fender Rob , Kasliwal Mansi M. , Canella Chris , Stein Robert , Giomi Matteo , Brinnel Valery , Santen Jakob van , Nordin Jakob , Bellm Eric C. , Dekany Richard , Fremling Christoffer , Golkhou V. Zach , Kupfer Thomas , Kulkarni Shrinivas R. , Laher Russ R. , Mahabal Ashish , Masci Frank J. , Miller Adam A. , Neill James D. , Riddle Reed , Rigault Mickael , Rusholme Ben , Soumagnac Maayane T. , Tachibana 優太 Yutaro 朗橘 
Published: February 2019

Abstract
We present Zwicky Transient Facility (ZTF) observations of the tidal disruption flare AT2018zr/PS18kh reported by Holoien et al. and detected during ZTF commissioning. The ZTF light curve of the tidal disruption event (TDE) samples the rise-to-peak exceptionally well, with 50 days of g- and r-band detections before the time of maximum light. We also present our multi-wavelength follow-up observations, including the detection of a thermal (kT ≈ 100 eV) X-ray source that is two orders of magnitude fainter than the contemporaneous optical/UV blackbody luminosity, and a stringent upper limit to the radio emission. We use observations of 128 known active galactic nuclei (AGNs) to assess the quality of the ZTF astrometry, finding a median host-flare distance of 0.″2 for genuine nuclear flares. Using ZTF observations of variability from known AGNs and supernovae we show how these sources can be separated from TDEs. A combination of light-curve shape, color, and location in the host galaxy can be used to select a clean TDE sample from multi-band optical surveys such as ZTF or the Large Synoptic Survey Telescope.
Submillimeter Polarization Spectrum of the Carina Nebula
Authors: Shariff Jamil A. , Ade Peter A. R. , Angilè Francesco E. , Ashton Peter , Benton Steven J. , Devlin Mark J. , Dober Bradley , Fissel Laura M. , Fukui Yasuo , Galitzki Nicholas , Gandilo Natalie N. , Klein Jeffrey , Korotkov Andrei L. , Li Zhi-Yun , Martin Peter G. , Matthews Tristan G. , Moncelsi Lorenzo , Nakamura Fumitaka , Netterfield Calvin B. , Novak Giles , Pascale Enzo , Poidevin Frédérick , Santos Fabio P. , Savini Giorgio , Scott Douglas , Soler Juan Diego , Thomas Nicholas E. , Tucker Carole E. , Tucker Gregory S. , Ward-Thompson Derek 
Published: February 2019

Abstract
Linear polarization maps of the Carina Nebula were obtained at 250, 350, and 500 μm during the 2012 flight of the Balloon-borne Large Aperture Submillimeter Telescope for Polarimetry (BLASTPol). These measurements are combined with Planck 850 μm data in order to produce a submillimeter spectrum of the polarization fraction of the dust emission, averaged over the cloud. This spectrum is flat to within ±15% (relative to the 350 μm polarization fraction). In particular, there is no evidence for a pronounced minimum of the spectrum near 350 μm, as suggested by previous ground-based measurements of other molecular clouds. This result of a flat polarization spectrum in Carina is consistent with recently published BLASTPol measurements of the Vela C molecular cloud and also agrees with a published model for an externally illuminated, dense molecular cloud by Bethell and collaborators. The shape of the spectrum in Carina does not show any dependence on the radiative environment of the dust, as quantified by the Planck-derived dust temperature or dust optical depth at 353 GHz.
Cross-correlating Carbon Monoxide Line-intensity Maps with Spectroscopic and Photometric Galaxy Surveys
Authors: Chung Dongwoo T. , Viero Marco P. , Church Sarah E. , Wechsler Risa H. , Alvarez Marcelo A. , Bond J. Richard , Breysse Patrick C. , Cleary Kieran A. , Eriksen Hans K. , Foss Marie K. , Gundersen Joshua O. , Harper Stuart E. , T. Ihle Håvard , Keating Laura C. , Murray Norman , Padmanabhan Hamsa , Stein George F. , Wehus Ingunn K. ,   (COMAP Collaboration)
Published: February 2019

Abstract
Line-intensity mapping is an emerging field of observational work, with strong potential to fit into a larger effort to probe large-scale structure and small-scale astrophysical phenomena using multiple complementary tracers. Taking full advantage of such complementarity means, in part, undertaking line-intensity surveys with galaxy surveys in mind. We consider the potential for detection of a cross-correlation signal between COMAP and blind surveys based on photometric redshifts (as in COSMOS) or based on spectroscopic data (as with the HETDEX survey of Lyα emitters). We find that obtaining

accuracy in redshifts and ≳10−4 sources per Mpc3 with spectroscopic redshift determination should enable a CO-galaxy cross spectrum detection significance at least twice that of the CO auto spectrum. Either a future targeted spectroscopic survey or a blind survey like HETDEX may be able to meet both of these requirements.
1-OGC: The First Open Gravitational-wave Catalog of Binary Mergers from Analysis of Public Advanced LIGO Data
Authors: Nitz Alexander H. , Capano Collin , Nielsen Alex B. , Reyes Steven , White Rebecca , Brown Duncan A. , Krishnan Badri 
Published: February 2019

AbstractWe present the first Open Gravitational-wave Catalog, obtained by using the public data from Advanced LIGO’s first observing run to search for compact-object binary mergers. Our analysis is based on new methods that improve the separation between signals and noise in matched-filter searches for gravitational waves from the merger of compact objects. The three most significant signals in our catalog correspond to the binary black hole mergers GW150914, GW151226, and LVT151012. We assume a common population of binary black holes for these three signals by defining a region of parameter space that is consistent with these events. Under this assumption, we find that LVT151012 has a 97.6% probability of being astrophysical in origin. No other significant binary black hole candidates are found, nor did we observe any significant binary neutron star or neutron star–black hole candidates. We make available our complete catalog of events, including the subthreshold population of candidates.
Electron Distribution and Energy Release in Magnetic Reconnection Outflow Regions during the Pre-impulsive Phase of a Solar Flare
Authors: Battaglia Marina , Kontar Eduard P. , Motorina Galina 
Published: February 2019

Abstract
We present observations of electron energization in magnetic reconnection outflows during the pre-impulsive phase of solar flare SOL2012-07-19T05:58. During a time-interval of about 20 minutes, starting 40 minutes before the onset of the impulsive phase, two X-ray sources were observed in the corona, one above the presumed reconnection region and one below. For both of these sources, the mean electron distribution function as a function of time is determined over an energy range from 0.1 keV up to several tens of keV, for the first time. This is done by simultaneous forward fitting of X-ray and extreme ultraviolet (EUV) data. Imaging spectroscopy with RHESSI provides information on the high-energy tail of the electron distribution in these sources while EUV images from SDO/Atmospheric Imaging Assembly are used to constrain the low specific electron energies. The measured electron distribution spectrum in the magnetic reconnection outflows is consistent with a time-evolving kappa-distribution with κ = 3.5–5.5. The spectral evolution suggests that electrons are accelerated to progressively higher energies in the source above the reconnection region, while in the source below, the spectral shape does not change but an overall increase of the emission measure is observed, suggesting density increase due to evaporation. The main mechanisms by which energy is transported away from the source regions are conduction and free-streaming electrons. The latter dominates by more than one order of magnitude and is comparable to typical nonthermal energies during the hard X-ray peak of solar flares, suggesting efficient acceleration even during this early phase of the event.
The NANOGrav 12.5 yr Data Set: The Frequency Dependence of Pulse Jitter in Precision Millisecond Pulsars
Authors: Lam M. T. , McLaughlin M. A. , Arzoumanian Z. , Blumer H. , Brook P. R. , Cromartie H. T. , Demorest P. B. , DeCesar M. E. , Dolch T. , Ellis J. A. , Ferdman R. D. , Ferrara E. C. , Fonseca E. , Garver-Daniels N. , Gentile P. A. , Jones M. L. , Lorimer D. R. , Lynch R. S. , Ng C. , Nice D. J. , Pennucci T. T. , Ransom S. M. , Spiewak R. , Stairs I. H. , Stovall K. , Swiggum J. K. , Vigeland S. J. , Zhu W. W. 
Published: February 2019

Abstract
Low-frequency gravitational-wave experiments require the highest timing precision from an array of the most stable millisecond pulsars. Several known sources of noise on short timescales in single radio pulsar observations are well described by a simple model of three components: template fitting from a finite signal-to-noise ratio, pulse phase/amplitude jitter from single-pulse stochasticity, and scintillation errors from short-timescale interstellar scattering variations. Currently template-fitting errors dominate, but as radio telescopes push toward higher signal-to-noise ratios, jitter becomes the next dominant term for most millisecond pulsars. Understanding the statistics of jitter becomes crucial for properly characterizing arrival time uncertainties. We characterize the radio frequency dependence of jitter using data on 48 pulsars in the North American Nanohertz Observatory for Gravitational Waves timing program. We detect significant jitter in 43 of the pulsars and test several functional forms for its frequency dependence; we find significant frequency dependence for 30 pulsars. We find moderate correlations of rms jitter with pulse width (R = 0.62) and number of profile components (R = 0.40); the single-pulse rms jitter is typically ≈1% of pulse phase. The average frequency dependence for all pulsars using a power-law model has index −0.42. We investigate the jitter variations for the interpulse of PSR B1937+21 and find no significant deviations from the main pulse rms jitter. We also test the time variation of jitter in two pulsars and find that systematics likely bias the results for high-precision pulsars. Pulsar timing array analyses must properly model jitter as a significant component of the noise within the detector.
Constraining the Rate of Protostellar Accretion Outbursts in the Orion Molecular Clouds
Authors: Fischer William J. , Safron Emily , Megeath S. Thomas 
Published: February 2019

Abstract
Outbursts due to dramatic increases in the mass accretion rate are the most extreme type of variability in young stellar objects. We searched for outbursts among 319 protostars in the Orion molecular clouds by comparing 3.6, 4.5, and 24 μm photometry from the Spitzer Space Telescope to 3.4, 4.6, and 22 μm photometry from the Wide-field Infrared Survey Explorer (WISE) obtained ∼6.5 yr apart. Sources that brightened by more than two standard deviations above the mean variability at all three wavelengths were marked as burst candidates, and they were inspected visually to check for false positives due primarily to the reduced angular resolution of WISE compared to Spitzer. We recovered the known burst V2775 Ori (HOPS 223) as well as a previously unknown burst, HOPS 383, which we announced in an earlier paper. No other outbursts were found. With observations over 6.5 yr, we estimate an interval of about 1000 yr between bursts with a 90% confidence interval of 690–40,300 yr. The most likely burst interval is shorter than those found in studies of optically revealed young stellar objects, suggesting that outbursts are more frequent in protostars than in pre-main-sequence stars that lack substantial envelopes.
The Two Most Recent Thermonuclear Supernovae in the Local Group: Radio Constraints on their Progenitors and Evolution
Authors: Sarbadhicary Sumit K. , Chomiuk Laura , Badenes Carles , Tremou Evangelia , Soderberg Alicia M. , Sjouwerman Loránt O. 
Published: February 2019

Abstract
Young supernova remnants (SNRs) provide a unique perspective on supernova (SN) progenitors and connect the late evolution of SNe with the onset of the SNR phase. Here we study SN 1885A and G1.9+0.3, the most recent thermonuclear SNe in the Local Group (with ages ∼100 yr) with radio data, which provide a sensitive probe of the SN environment and energetics. We reduce and co-add 4–8 GHz observations from the Karl G. Jansky Very Large Array (VLA) to produce the deepest radio image of the central region of M31 (rms noise of 1.3 μJy beam−1 at 6.2 GHz). We detect some diffuse emission near SN 1885A at 2.6σ, but the association with SN 1885A is uncertain because diffuse radio emission pervades M31's central region. Accounting for this diffuse emission, we get a 3σ upper limit of 11 μJy for SN 1885A, about four times less luminous than G1.9+0.3 at 6.2 GHz. Together with Hubble Space Telescope data on SN 1885A, we estimate its ambient density, n
0 < 0.04 cm−3 (±0.03 cm−3 due to systematics), and constrain the joint kinetic energy–ejecta mass parameter space. For G1.9+0.3, archival VLA observations yielded n
0 = 0.18 cm−3. We synthesize the multi-wavelength data on SN 1885A to argue that it is likely the product of a sub-Chandrasekhar explosion, while G1.9+0.3 appears consistent with both Chandrasekhar and sub-Chandrasekhar SN Ia models.
The Synthetic ALMA Multiband Analysis of the Dust Properties of the TW Hya Protoplanetary Disk
Authors: Kim Seongjoong , Nomura Hideko , Tsukagoshi Takashi , Kawabe Ryohei , Muto Takayuki 
Published: February 2019

Abstract
Analyzing multiband observations of dust continuum emission is one of the useful tools to constrain dust properties that help us to understand the physical properties of the protoplanetary disks. We perform a synthetic ALMA multiband analysis to find the best ALMA band set for constraining the dust properties of the TW Hya disk. We find that the Band [10, 6, 3] set is the best set among the possible combinations of ALMA Bands [3, 4, 5, 6, 7, 8, 9, 10]. We also find two conditions for the good ALMA band sets providing narrow constraint ranges on dust properties: (1) Band 9 or 10 is included in the band set, and (2) there are enough frequency intervals between the bands. These are related to the conditions that give good constraints on dust properties: the combination of optically thick and thin bands is required, and large β (β is the power-law index of dust opacity, κ

ν
∝ ν

β
) and low dust temperature are preferable. To examine our synthetic analysis results, we apply the multiband analysis to ALMA archival data of the TW Hya disk at Bands 4, 6, 7, and 9. The Band [9, 6, 4] set provides the dust properties close to the model profile, while the Band [7, 6, 4] set gives the dust properties deviating from the model at all radii with too broad a constraint range to specify the accurate values of dust temperature, optical depth, and β. Since these features are expected by the synthetic multiband analysis, we confirm that the synthetic multiband analysis is consistent with the results derived from real data.