bluuebunny/crossref_metadata_2025_split huggingface dataset:
The fundamental discoveries in oxygen sensing: implications for heart diseases and cardiomyocytes maturation
Authors: Biniecka Monika , Wolnik Jan , Dulak Józef 
Published: February 2021

The 2019 Nobel Prize for Physiology or Medicine was awarded to three physician scientists, Drs. William G. Kaelin, Jr., Peter Ratcliffe and Gregg Semenza, for their research investigating how cells sense and adapt to oxygen levels. Understanding the cellular adaptation to oxygen deficiency - hypoxia - has a deep impact on our knowledge of the pathogenesis of several conditions, including heart and inflammatory diseases, as well as tumours. HIF-1 is a transcription factor that plays an essential role in hypoxia-elicited gene responses. HIF-1 targets genes are involved in many pathways, such as cellular metabolism, survival and angiogenesis. Furthermore, hypoxia has been shown to impact the reprogramming process of somatic cells into induced pluripotent stem cell (iPSCs) and iPSC differentiation to cardiomyocytes (hiPSC-CMs). New strategies have been employed to improve the maturity of hiPSC-CMs, which includes the application of mechanistic or chemical stimuli and genetic/epigenetic manipulations. Currently, the role of hypoxia and energy metabolism in promoting maturation of hPSC-CMs is a subject of new studies.
Suplementacja karnityną - dwie strony medalu
Authors: Olek Robert 
Published: February 2021

Utrwalona od kilku lat opinia, że suplementacja karnityną nie zmienia metabolizmu, szczególnie metabolizmu wysiłkowego, opiera się głównie na protokołach suplementacji krótkoterminowej. Ostatnie badania sugerują, że kluczowymi czynnikami mogą być czas suplementacji oraz stymulacja insulino-zależnego transportu do komórek mięśniowych. Suplementacja karnityną w połączeniu z cukrami prostymi (w celu aktywacji transportu karnityny do mięśni) powinno trwać ~100 dni, aby podnieść zawartość karnityny w mięśniach o ~10%. Efektem może być nie tylko modyfikacja metabolizmu kwasów tłuszczowych i węglowodanów, ale także białek. Z drugiej strony wiadomo, że długotrwała suplementacja karnityną przyczynia się do wzrostu krążącego N-tlenku trzymetyloaminy (TMAO) - związku podejrzewanego o działanie miażdzycogenne. Dlatego wskazane są dalsze badaniatego problemu, pozwalające lepiej zrozumieć zmiany wynikające z suplementacji karnityną i mechanizmy działania TMAO.
Czynniki determinujące status oksydacyjno-antyoksydacyjny i jego odpowiedź na wysiłek fizyczny
Authors: Jówko Ewa 
Published: February 2021

Nasilenie przemian metabolicznych podczas wysiłku fizycznego sprzyja powstawaniu wolnych rodników i reaktywnych form tlenu, co może zaburzać równowagę oksydacyjno-antyoksydacyjną w kierunku stresu oksydacyjnego. Warunki te sprzyjają uszkodzeniu struktur komórkowych, przyczyniając się do zmęczenia i spadku zdolności wysiłkowych. W pracy omówiono wysiłkowe źródła wolnych rodników tlenowych oraz obronę antyoksydacyjną ustroju, jak też czynniki wpływające na nasilenie powysiłkowego stresu oksydacyjnego. W kolejnej części przedstawiono wyniki badań dotyczących efektywności podawania suplementów antyoksydacyjnych w warunkach wysiłkowych, głównie na przykładzie polifenoli zielonej herbaty. Zwrócono też uwagę na potencjalne zagrożenia związane z przyjmowaniem suplementów antyoksydacyjnych w nadmiernych ilościach. Wynika to z faktu, iż reaktywne formy tlenu odgrywają ważną rolę jako przekaźniki sygnałów komórkowych, umożliwiając uzyskanie adaptacji do wysiłku fizycznego i wzrost zdolności wysiłkowych w odpowiedzi na trening sportowy (siły, wytrzymałości). W dalszej części omówiono czynniki genetyczne warunkujące poziom enzymatycznej obrony antyoksydacyjnej i wrażliwość na stres oksydacyjny, główną uwagę skupiając na polimorfizmach genów kodujących enzymy antyoksydacyjne. Przedstawiono zależność pomiędzy polimorfizmem genu mitochondrialnej dysmutazy ponadtlenkowej (enzymu stanowiącego pierwszą linię obrony przed szkodliwym wpływem wolnych rodników tlenowych na organizm) a zmianami parametrów równowagi oksydacyjno-antyoksydacyjnej w odpowiedzi na trening sportowy. Na koniec podkreślono użyteczność oznaczeń wspomnianego powyżej polimorfizmu w selekcji sportowców podatnych na stres oksydacyjny, w celu indywidualizacji zaleceń żywieniowych dotyczących podaży antyoksydantów w diecie lub w postaci suplementów.
EVALUASI PROGRAM PEMBINAAN PRESTASI BELA DIRI SHOTO-KAI KABUPATEN NAGEKEO
Authors: Wani Barnabas 
Published: February 2021

Peneltian ini bertujuan untuk 1) Untuk mengevaluasi bagaimana konteks prestasi bela diri shotokai kabupaten Nagekeo, 2) Untuk mengevaluasi bagaimana input yang meliputi sumber daya manusia, kualitas dan ketersediaan sarana dan prasarana, Sumber dana pembinaan prestasi bela diri shotokai kabupaten Nagekeo, 3) Untuk mengevaluasi bagaimana proses program pembinaan olahraga bela diri sotokai kabupaten Nagekeo, 4) Untuk mengevaluasi bagaimana hasil pembinaan olahraga bela diri shotokai kabupaten Nagekeo.Teknik pengumpulan data adalah observasi, wawancara, dokumentasi dan triangulasi data. Hasil dari penelitian ini ialah 1) context yang meliputi visi, misi, tujuan pembinaan sotokai kabupaten Nagekeo dikatakan baik karena mempunyai semuanya dari aspek yang ada 2) Input yang meliputi sumber daya manusia, sarana prasana dan dana. Pelatih yang ada pada sotokai kabupaten Nagekeo mempunyai standar yang baik karena pelatih memiliki lisensi pelatih tingkat nasional serta mempunyai atlet, sarana prasarana yang masih sangat kurang sehingga mempengaruhi tingkat prestasi dari atlet shotokai Nagekeo. Dana bersumber dari dukungan pemerintah daerah Kabupaten Nagekeo. 3) Proses yang meliputi pelaksanan program dan koordinasi, pelaksanaan program latihan pada cabang olahraga shotokai Nagekeo baik karena mempunyai program latihan yang baik, koordinasi antara pemerintah, pelatih dan atlet berjalan baik. 4) product, prestasi atlet sotokai kurang dan menurun ditandai dengan perolehan medali pada setiap kejuaran. Kesimpulannya bahwa dilihat dari aspek contex, input, proses dan product semuanya belum pada standar yang baik selayaknya pada pembinaan olahraga prestasi pada umumnya
A Survey of Active Galaxies at TeV Photon Energies with the HAWC Gamma-Ray Observatory
Authors: Albert A. , Alvarez C. , Camacho J. R. Angeles , Arteaga-Velázquez J. C. , Arunbabu K. P. , Rojas D. Avila , Solares H. A. Ayala , Baghmanyan V. , Belmont-Moreno E. , BenZvi S. Y. , Brisbois C. , Caballero-Mora K. S. , Capistrán T. , Carramiñana A. , Casanova S. , Cotti U. , Cotzomi J. , de León S. Coutiño , Fuente E. De la , Dingus B. L. , DuVernois M. A. , Durocher M. , Díaz-Vélez J. C. , Engel K. , Espinoza C. , Fan K. L. , Alonso M. Fernández , Fleischhack H. , Fraija N. , Galván-Gámez A. , García D. , García-González J. A. , Garfias F. , González M. M. , Goodman J. A. , Harding J. P. , Hernández S. , Hona B. , Huang D. , Hueyotl-Zahuantitla F. , Hüntemeyer P. , Iriarte A. , Jardin-Blicq A. , Joshi V. , Kieda D. , Kunde G. J. , Lara A. , Lee W. H. , Vargas H. León , Linnemann J. T. , Longinotti A. L. , Luis-Raya G. , Lundeen J. , Malone K. , Martínez O. , Martinez-Castellanos I. , Martínez-Castro J. , Matthews J. A. , Miranda-Romagnoli P. , Morales-Soto J. A. , Moreno E. , Mostafá M. , Nayerhoda A. , Nellen L. , Newbold M. , Nisa M. U. , Noriega-Papaqui R. , Olivera-Nieto L. , Peisker A. , Pérez-Pérez E. G. , Rho C. D. , Rosa-González D. , Ruiz-Velasco E. , Salazar H. , Greus F. Salesa , Sandoval A. , Schneider M. , Schoorlemmer H. , Smith A. J. , Springer R. W. , Tollefson K. , Torres I. , Torres-Escobedo R. , Ureña-Mena F. , Villaseñor L. , Weisgarber T. , Willox E. , Zepeda A. , Zhou H. , León C. de ,   The HAWC collaboration
Published: February 2021

Abstract
The High Altitude Water Cherenkov (HAWC) Gamma-Ray Observatory continuously detects TeV photons and particles within its large field of view, accumulating every day a deeper exposure of two-thirds of the sky. We analyzed 1523 days of HAWC live data acquired over four and a half years, in a follow-up analysis of 138 nearby (z < 0.3) active galactic nuclei from the Third Catalog of Hard Fermi-LAT sources culminating within 40° of the zenith at Sierra Negra, the HAWC site. This search for persistent TeV emission used a maximum-likelihood analysis assuming intrinsic power-law spectra attenuated by pair production of gamma-ray photons with the extragalactic background light. HAWC clearly detects persistent emission from Mkn 421 and Mkn 501, the two brightest blazars in the TeV sky, at 65σ and 17σ level, respectively. Marginal evidence, just above the 3σ level, was found for three other known very high-energy emitters: the radio galaxy M87 and the BL Lac objects VER J0521+211 and 1ES 1215+303, the latter two at z ∼ 0.1. We find a 4.2σ evidence for collective emission from the set of 30 previously reported very high-energy sources, with Mkn 421 and Mkn 501 excluded. Upper limits are presented for the sample under the power-law assumption and in the predefined (0.5–2.0), (2.0–8.0), and (8.0–32.0) TeV energy intervals.
Rise of the Titans: Gas Excitation and Feedback in a Binary Hyperluminous Dusty Starburst Galaxy at z ∼ 6
Authors: Riechers Dominik A. , Nayyeri Hooshang , Burgarella Denis , Emonts Bjorn H. C. , Clements David L. , Cooray Asantha , Ivison Rob J. , Oliver Seb , Pérez-Fournon Ismael , Rigopoulou Dimitra , Scott Douglas 
Published: February 2021

Abstract
We report new observations toward the hyperluminous dusty starbursting major merger ADFS-27 (z = 5.655), using the Australia Telescope Compact Array (ATCA) and the Atacama Large Millimeter/submillimeter Array (ALMA). We detect CO (J = 2 → 1), CO (J = 8 → 7), CO (J = 9 → 8), CO (J = 10 → 9), and H2O (312 → 221) emission, and a P Cygni−shaped OH+ (11 → 01) absorption/emission feature. We also tentatively detect H2O (321 → 312) and OH+ (12 → 01) emission and CH+ (J = 1 → 0) absorption. We find a total cold molecular mass of M
gas = (2.1 ± 0.2) × 1011 (α
CO/1.0) M
⊙. We also find that the excitation of the star-forming gas is overall moderate for a z > 5 dusty starburst, which is consistent with its moderate dust temperature. A high-density, high kinetic temperature gas component embedded in the gas reservoir is required to fully explain the CO line ladder. This component is likely associated with the “maximum starburst” nuclei in the two merging galaxies, which are separated by only 140 ± 13 km s−1 along the line of sight and 9.0 kpc in projection. The kinematic structure of both components is consistent with galaxy disks, but this interpretation remains limited by the spatial resolution of the current data. The OH+ features are only detected toward the northern component, which is also the one that is more enshrouded in dust and thus remains undetected up to 1.6 μm even in our sensitive new Hubble Space Telescope Wide Field Camera 3 imaging. The absorption component of the OH+ line is blueshifted and peaks near the CO and continuum emission peak, while the emission is redshifted and peaks offset by 1.7 kpc from the CO and continuum emission peak, suggesting that the gas is associated with a massive molecular outflow from the intensely star-forming nucleus that supplies 125 M
⊙ yr−1 of enriched gas to its halo.
Pair Drizzle around Sub-Eddington Supermassive Black Holes
Authors: Wong George N. , Ryan Benjamin R. , Gammie Charles F. 
Published: February 2021

Abstract
Electron–positron pair creation near sub-Eddington accretion rate black holes is believed to be dominated by the Breit–Wheeler process (photon–photon collisions). The interacting high-energy photons are produced when unscreened electric fields accelerate leptons either in coherent, macroscopic gaps, or in incoherent structures embedded in the turbulent plasma flow. The latter type of acceleration results in a drizzle of pair production sourced by photons from the background radiation field whose energies are near the pair-production threshold. In this work, we use radiation general relativistic magnetohydrodynamic simulations to extend an earlier study of pair drizzle by Mościbrodzka et al. We focus on low-magnetization (standard and normal evolution) accretion onto supermassive Kerr black holes and consider radiation due to synchrotron, bremsstrahlung, and Compton upscattering processes. We confirm that pair drizzle in M87 is sufficient to keep the magnetospheric charge density orders of magnitude above the Goldreich–Julian density. We also find that pair production peaks along the jet–disk boundary.
Water Production Rate of C/2020 F3 (NEOWISE) from SOHO/SWAN over Its Active Apparition
Authors: Combi M. R. , Mäkinen T. , Bertaux J.-L. , Quémerais E. , Ferron S. 
Published: February 2021

Abstract
C/2020 F3 (NEOWISE) was discovered in images from the Near Earth Object program of the Wide-Field Infrared Survey Explorer (NEOWISE) taken on 2020 March 27 and has become the Great Comet of 2020. The Solar Wind ANisotropies (SWAN) camera on the Solar and Heliospheric Observatory (SOHO) spacecraft, located in a halo orbit around the Earth–Sun L1 Lagrange point, makes daily full-sky images of hydrogen Lyα. Water production rates were determined from the SWAN hydrogen Lyα brightness and spatial distribution of the comet measured over a 4 month period of time on either side of the comet’s perihelion on 2020 July 3. The water production rate in s−1 was moderately asymmetric around perihelion and varied with the heliocentric distance, r, in au as (6.9 ± 0.5) × 1028
r
−2.5±0.2 and (10.1 ± 0.5) × 1028
r
−3.5±0.1 before and after perihelion, respectively. This is consistent with the comet having been through the planetary region of the solar system on one or more previous apparitions. Water production rates as large as 5.27 × 1030 s−1 were determined shortly after perihelion, once the comet was outside the solar avoidance area of SWAN, when the comet was 0.324 au from the Sun.
Icy Exomoons Evidenced by Spallogenic Nuclides in Polluted White Dwarfs
Authors: Doyle Alexandra E. , Desch Steven J. , Young Edward D. 
Published: February 2021

Abstract
We present evidence that excesses in Be in polluted white dwarfs (WDs) are the result of accretion of icy exomoons that formed in the radiation belts of giant exoplanets. Here we use excess Be in the white dwarf GALEX J2339–0424 as an example. We constrain the parent body abundances of rock-forming elements in GALEX J2339–0424 and show that the overabundance of beryllium in this WD cannot be accounted for by differences in diffusive fluxes through the WD outer envelope nor by chemical fractionations during typical rock-forming processes. We argue instead that the Be was produced by energetic proton irradiation of ice mixed with rock. We demonstrate that the MeV proton fluence required to form the high Be/O ratio in the accreted parent body is consistent with irradiation of ice in the rings of a giant planet within its radiation belt, followed by accretion of the ices to form a moon that is later accreted by the WD. The icy moons of Saturn serve as useful analogs. Our results provide an estimate of spallogenic nuclide excesses in icy moons formed by rings around giant planets in general, including those in the solar system. While excesses in Be have been detected in two polluted WDs to date, including the WD described here, we predict that excesses in the other spallogenic elements Li and B, although more difficult to detect, should also be observed, and that such detections would also indicate pollution by icy exomoons formed in the ring systems of giant planets.
Parallax Systematics and Photocenter Motions of Benchmark Eclipsing Binaries in Gaia EDR3
Authors: Stassun Keivan G. , Torres Guillermo 
Published: February 2021

Abstract
Previous analyses of various standard candles observed by the Gaia satellite have reported statistically significant systematics in the parallaxes that have improved from ∼250 μas in the first data release (DR1) to 50–80 μas in the second data release (DR2). Here we examine the parallaxes newly reported in the Gaia early third data release (EDR3) using the same sample of benchmark eclipsing binaries (EBs) we used to assess the DR1 and DR2 parallaxes. We find a mean offset of −37 ± 20 μas (Gaia − EB), which decreases to −15 ± 18 μas after applying the corrections recommended by the Gaia Mission team; global systematics in the Gaia parallaxes have clearly improved and are no longer statistically significant for the EB sample, which spans 5 ≲ G ≲ 12 in brightness and 0.03–3 kpc in distance. We also find that the Renormalized Unit Weight Error (RUWE) goodness-of-fit statistic reported in Gaia DR3 is highly sensitive to unresolved companions (tertiaries in the case of our EB sample) as well as to photocenter motion of the binaries themselves. RUWE is nearly perfectly correlated (r
2 = 0.82) with photocenter motions down to ≲0.1 mas, and surprisingly this correlation exists entirely within the nominal “good” RUWE range of 1.0–1.4. This suggests that RUWE values even slightly greater than 1.0 may signify unresolved binaries in Gaia, and that the RUWE value can serve as a quantitative predictor of the photocenter motion.
Knowledge Inventory of Foundational Data Products in Planetary Science
Authors: Laura Jason R. , Beyer Ross A. 
Published: February 2021

Abstract
Some of the key components of any Planetary Spatial Data Infrastructure (PDSI) are the data products that end-users wish to discover, access, and interrogate. One precursor to the implementation of a PSDI is a knowledge inventory that catalogs what products are available, from which data producers, and at what initially understood data qualities. We present a knowledge inventory of foundational PSDI data products: geodetic coordinate reference frames, elevation or topography, and orthoimages or orthomosaics. Additionally, we catalog the available gravity models that serve as critical data for the assessment of spatial location, spatial accuracy, and ultimately spatial efficacy. We strengthen our previously published definitions of foundational data products to assist in solidifying a common vocabulary that will improve communication about these essential data products.
The Visual Lightcurve of Comet C/1995 O1 (Hale–Bopp) from 1995 to 1999
Authors: Womack M. , Curtis O. , Rabson D. A. , Pinto O. Harrington , Wierzchos K. , Gonzalez S. Cruz , Sarid G. , Mentzer C. , Lastra N. , Pichette N. , Ruffini N. , Cox T. , Rivera I. , Micciche A. , Jackson C. , Homich A. , Tollison A. , Reed S. , Zilka J. , Henning B. , Spinar M. , Escoto S. Rosslyn , Erdahl T. , Goldschen-Ohm Marcel P. , Uhl W. T. 
Published: February 2021

Abstract
The great comet C/1995 O1 (Hale–Bopp) presented a remarkable opportunity to study its long-term brightness over four years. We used 2240 observations published in the International Comet Quarterly from 17 observers during 1995 July to 1999 September to create a secular lightcurve. In order to account for observer differences, we present a novel algorithm to reduce scatter and increase precision in a lightcurve compiled from many sources. It is implemented in a publicly available code, ICQSPLITTER, which uses a self-consistent statistical approach. To first order, the comet’s lightcurve approximates an r
−4 response for both pre- and postperihelion distances. The preperihelion data are better fit with a fifth-order polynomial with inflection points at 4.0, 2.6, 2.1, and 1.1 au, some of which are associated with physical changes in the coma. Outbursts may have occurred a few days before perihelion and at ∼2.2 and 7.4 au postperihelion. The Afρ values derived from the final magnitudes are consistent with an r
−1.5 dependence on heliocentric distance and are within a factor of 2–4 of those derived from spectroscopy and narrowband photometry. We present correlation equations for visual magnitudes and CO and H2O production rates that are consistent with the preperihelion brightness increasing due to CO outgassing until about 2.6–3.0 au from the Sun and then are strongly correlated with H2O production rates. We also present two generalized correlation equations that may be useful for observation planning and data analysis with the James Webb Space Telescope and other observatories.
Vertical Structure and Color of Jovian Latitudinal Cloud Bands during the Juno Era
Authors: Dahl Emma K. , Chanover Nancy J. , Orton Glenn S. , Baines Kevin H. , Sinclair James A. , Voelz David G. , Wijerathna Erandi A. , Strycker Paul D. , Irwin Patrick G. J. 
Published: February 2021

Abstract
The identity of the coloring agent(s) in Jupiter’s atmosphere and the exact structure of Jupiter’s uppermost cloud deck are yet to be conclusively understood. The Crème Brûlée model of Jupiter’s tropospheric clouds, originally proposed by Baines et al. and expanded upon by Sromovsky et al. and Baines et al., presumes that the chromophore measured by Carlson et al. is the singular coloring agent in Jupiter’s troposphere. In this work, we test the validity of the Crème Brûlée model of Jupiter’s uppermost cloud deck using spectra measured during the Juno spacecraft’s fifth perijove pass in 2017 March. These data were obtained as part of an international ground-based observing campaign in support of the Juno mission using the New Mexico State University Acousto-optic Imaging Camera at the 3.5 m telescope at Apache Point Observatory in Sunspot, NM, USA. We find that the Crème Brûlée model cloud-layering scheme can reproduce Jupiter’s visible spectrum both with the Carlson et al. chromophore and with modifications to its imaginary index of refraction spectrum. While the Crème Brûlée model provides reasonable results for regions of Jupiter’s cloud bands such as the North Equatorial Belt and Equatorial Zone, we find that it is not a safe assumption for unique weather events, such as the 2016–2017 Southern Equatorial Belt outbreak that was captured by our measurements.