bluuebunny/crossref_metadata_2025_split huggingface dataset:
Accuracy of Heart Auscultation Examination by General Practitioners From Various Levels of Competency in Detection of Heart Abnormality in Basic School Children
Authors: Permatasari Annisa , Deny Salverra Yosy  , Achirul Bakri  , Ria Nova  
Published: January 2022

Background. Most of heart defects in children do not show typical clinical symptoms. Ten percent of the cases are late detected. Echocardiography is an examination with high sensitivity and specificity in detecting heart defects in children, but it cannot be performed by all health workers, expensive and not always available in hospitals. Auscultation is an important part of a physical examination that inexpensive, easy examination, and becomes a competency of all doctors. The aim of this study to determine the accuracy of the screening method by listening to murmurs on heart auscultation by various levels of physician competence.
Methods. This is a diagnostic test of 250 elementary school children held in the pediatric ward of dr. Mohammad Hoesin Palembang from September to November 2019. The auscultation examination was performed by three pediatrics resident from three stages (i.e. junior, middle and senior), followed by echocardiography examinations by a pediatric cardiologist.
Results. The highest sensitivity of auscultation was found in senior resident, 42.4%, while the lowest was found in junior resident, 12.1%. The results of the kappa analysis of the cardiac auscultation examination on the three examiners showed a poor level of agreement on junior stage compared to senior resident (k = 0.189; CI = 0.033-0.346) and the level of agreement was sufficient in junior stage compared to middle stage resident (k = 0.297; CI = 0.134 -0.461) and middle stage compared to senior resident (k = 0.301; CI = 0.147-0.456).
Conclusion. Experience and length of learning will affect the accuracy of the auscultation examination in detecting heart defects in children.
Tuberculosis Arthritis Genu Sinistra with Drug-Induced Liver Injury, COVID 19 Confirmed
Authors: Yonis Ismed  , Partan Radiyati Umi , Ismail Bastomi  
Published: January 2022

Background. Tuberculosis is still a significant health problem, especially in developing countries. Although pulmonary tuberculosis is the most common form of the disease, extrapulmonary tuberculosis also contributes significantly to morbidity and mortality. 10-15% of extrapulmonary cases are due to tuberculous arthritis. The following is a case report of a 36-year-old woman with a diagnosis of genu Sinistra tuberculosis arthritis and drug-induced hepatotoxic injury due to OAT.
Case presentation. A woman, 36 years old, Muslim, addresses Banyuasin. The patient is a housewife, treated at Dr. Moh Hoesin General Hospital since October 11, 2021. The main complaint in the form of pain in the left knee has been getting worse since 1 week before being admitted to the hospital. 4 months before admission the hospital, the patient complained of left knee pain, the pain felt like being stabbed, coming and going, especially when walking. In this patient, there was a complaint of nausea that was felt in the pit of the stomach. The results of laboratory examinations showed an increase in the transaminase enzyme and hyperuricemia, so it was suspected that the patient had DILI due to OAT drugs. Hepatocyte death in DILI can occur through two processes, namely processes mediated by apoptosis or necrosis. In apoptosis, cell shrinkage and fragmentation occur into small pieces with the cell membrane intact. These fragments are cleared by phagocytosis and generally do not stimulate the host immune response.
Conclusion. A patient diagnosed with arthritis tuberculosis genu Sinistra with Drug-Induced Liver Injury and Confirmed COVID 19.
Systematic KMTNet Planetary Anomaly Search. II. Six New q < 2 × 10−4 Mass-ratio Planets
Authors: Hwang Kyu-Ha , Zang Weicheng , Gould Andrew , Udalski Andrzej , Bond Ian A. , Yang Hongjing , Mao Shude ,   (Lead Authors), Albrow Michael D. , Chung Sun-Ju , Han Cheongho , Kil Jung Youn , Ryu Yoon-Hyun , Shin In-Gu , Shvartzvald Yossi , Yee Jennifer C. , Cha Sang-Mok , Kim Dong-Jin , Kim Hyoun-Woo , Kim Seung-Lee , Lee Chung-Uk , Lee Dong-Joo , Lee Yongseok , Park Byeong-Gon , Pogge Richard W. ,   (KMTNet Collaboration), Mróz Przemek , Poleski Radek , Skowron Jan , Szymański Michał K. , Soszyński Igor , Pietrukowicz Paweł , Kozłowski Szymon , Ulaczyk Krzysztof , Rybicki Krzysztof A. , Iwanek Patryk , Wrona Marcin , Gromadzki Mariusz ,   (OGLE Collaboration), Abe Fumio , Barry Richard , Bennett David P. , Bhattacharya Aparna , Fujii Hirosame , Fukui Akihiko , Hirao Yuki , Itow Yoshitaka , Kirikawa Rintaro , Kondo Iona , Koshimoto Naoki , Munford Brandon , Matsubara Yutaka , Miyazaki Shota , Muraki Yasushi , Olmschenk Greg , Ranc Clément , Rattenbury Nicholas J. , Satoh Yuki K. , Shoji Hikaru , Ishitani Silva Stela , Sumi Takahiro , Suzuki Daisuke , Tristram Paul J. , Yonehara Atsunori ,   (The MOA Collaboration), Zhang Xiangyu , Zhu Wei , Penny Matthew T. , Fouqué Pascal ,   (The Tsinghua & CFHT Microlensing Group)
Published: January 2022

Abstract
We apply the automated AnomalyFinder algorithm of Paper I to 2018–2019 light curves from the ≃13 deg2 covered by the six KMTNet prime fields, with cadences Γ ≥ 2 hr−1. We find a total of 11 planets with mass ratios q < 2 × 10−4, including 6 newly discovered planets, 1 planet that was reported in Paper I, and recovery of 4 previously discovered planets. One of the new planets, OGLE-2018-BLG-0977Lb, is in a planetary caustic event, while the other five (OGLE-2018-BLG-0506Lb, OGLE-2018-BLG-0516Lb, OGLE-2019-BLG-1492Lb, KMT-2019-BLG-0253, and KMT-2019-BLG-0953) are revealed by a “dip” in the light curve as the source crosses the host-planet axis on the opposite side of the planet. These subtle signals were missed in previous by-eye searches. The planet-host separations (scaled to the Einstein radius), s, and planet-host mass ratios, q, are, respectively, (s, q × 105) = (0.88, 4.1), (0.96 ± 0.10, 8.3), (0.94 ± 0.07, 13), (0.97 ± 0.07, 18), (0.97 ± 0.04, 4.1), and (0.74, 18), where the “ ± ” indicates a discrete degeneracy. The 11 planets are spread out over the range

−
5
<
log
q
<
−
3.7

. Together with the two planets previously reported with q ∼ 10−5 from the 2018–2019 nonprime KMT fields, this result suggests that planets toward the bottom of this mass-ratio range may be more common than previously believed.
Discovery of CWISE J052306.42−015355.4, an Extreme T Subdwarf Candidate
Authors: Brooks Hunter , Kirkpatrick J. Davy , Caselden Dan , Schneider Adam C. , Meisner Aaron M. , Faherty Jacqueline K. , Casewell S. L. , Kuchner Marc J. ,   The Backyard Worlds: Planet 9 Collaboration
Published: January 2022

Abstract
We present the discovery of CWISE J052306.42−015355.4, which was found as a faint, significant proper-motion object (0.″52 ± 0.″08 yr−1) using machine-learning tools on the unWISE re-processing of time series images from the Wide-field Infrared Survey Explorer. Using the CatWISE2020 W1 and W2 magnitudes along with a J-band detection from the VISTA Hemisphere Survey, the location of CWISE J052306.42−015355.4 on the W1 − W2 versus J − W2 diagram best matches that of other known, or suspected, extreme T subdwarfs. As there is currently very little knowledge concerning extreme T subdwarfs we estimate a rough distance of ≤68 pc, which results in a tangential velocity of ≤167 km s−1, both of which are tentative. A measured parallax is greatly needed to test these values. We also estimate a metallicity of −1.5 < [M/H] < −0.5 using theoretical predictions.
Accurate Photometry of Saturated Stars Using the Point-spread-function Wing Technique with Spitzer
Authors: Su Kate Y. L. , Rieke G. H. , Marengo M. , Schlawin Everett 
Published: January 2022

Abstract
We report Spitzer 3.6 and 4.5 μm photometry of 11 bright stars relative to Sirius, exploiting the unique optical stability of the Spitzer Space Telescope point-spread function (PSF). Spitzer's extremely stable beryllium optics in its isothermal environment enables precise comparisons in the wings of the PSF from heavily saturated stars. These bright stars stand as the primary sample to improve stellar models, and to transfer the absolute flux calibration of bright standard stars to a sample of fainter standards useful for missions like JWST and for large ground-based telescopes. We demonstrate that better than 1% relative photometry can be achieved using the PSF wing technique in the radial range of 20″–100″ for stars that are fainter than Sirius by 8 mag (from outside the saturated core to a large radius where a high signal-to-noise ratio profile can still be obtained). We test our results by (1) comparing the [3.6]−[4.5] color with that expected between the WISE W1 and W2 bands, (2) comparing with stars where there is accurate K
S photometry, and (3) also comparing with relative fluxes obtained with the DIRBE instrument on COBE. These tests confirm that relative photometry is achieved to better than 1%.
KK 242, A Faint Companion to the Isolated Scd Galaxy NGC 6503
Authors: Karachentsev Igor D. , Cannon John M. , Fuson Jackson , Inoue John L. , Tully R. Brent , Anand Gagandeep S. , Kaisin Serafim S. 
Published: January 2022

Abstract
Using Hubble Space Telescope imaging of the resolved stellar population of KK 242 = NGC 6503-d1 =PGC 4689184, we measure the distance to the galaxy to be 6.46 ± 0.32 Mpc and find that KK 242 is a satellite of the low-mass spiral galaxy NGC 6503 located on the edge of the Local Void. Observations with the Karl G. Jansky Very Large Array show signs of a very faint H i signal at the position of KK 242 within a velocity range of V
hel = −80 ± 10 km s−1. This velocity range is severely contaminated by H i emission from the Milky Way and from NGC 6503. The dwarf galaxy is classified as the transition type, dIrr/dSph, with a total H i mass of < 106
M
⊙ and a star formation rate SFR(Hα) = −4.82 dex (M
⊙ yr−1). Being at a projected separation of 31 kpc with a radial velocity difference of—105 km s−1 relative to NGC 6503, KK 242 gives an estimate of the halo mass of the spiral galaxy to be

log
(
M

/

M

⊙

) = 11.6. Besides NGC 6503, there are eight more detached low-luminosity spiral galaxies in the Local Volume: M33, NGC 2403, NGC 7793, NGC 1313, NGC 4236, NGC 5068, NGC 4656, and NGC 7640, from whose small satellites we have estimated the average total mass of the host galaxies and their average total mass-to-K-band-luminosity 〈M

T
/M
⊙〉 = (3.46 ± 0.84) × 1011 and (58 ± 19)M
⊙/L
⊙, respectively.
VLA Observations of the AE Aqr-type Cataclysmic Variable LAMOST J024048.51+195226.9
Authors: Barrett Paul E. 
Published: January 2022

Abstract
AE Aqr was until recently the only known magnetic cataclysmic variable (MCV) containing a rapidly spinning (33.08 s) white dwarf (WD). Its radio emission is believed to be a superposition of synchrotron-emitting plasmoids, because it has a positive spectral index spanning three orders of magnitude (≈2–2000 GHz) and is unpolarized. Both characteristics are unusual for MCVs. Recently, Thorstensen has suggested that the cataclysmic variable LAMOST J024048.51+195226.9 (henceforth, J0240+19) is a twin of AE Aqr based on its optical spectra. Optical photometry shows the star to be a high-inclination eclipsing binary with a spin period of 24.93 s, making it the fastest spinning WD. This paper presents three hours of Very Large Array radio observations of J0240+19. These observations show that the persistent radio emission from J0240+19 is dissimilar to that of AE Aqr in that it shows high circular polarization and a negative spectral index. The emission is most similar to that from the nova-like CV V603 Aql. We argue that the radio emission is caused by a superposition of plasmoids emitting plasma radiation or electron cyclotron maser emission from the lower corona of the donor star and not from the magnetosphere near the WD, because the latter site is expected to be modulated at the orbital period of the binary and to show eclipses—of which there is no evidence. The radio source J0240+19, although weak (≲ 1 mJy), is a persistent source in a high-inclination eclipsing binary, making it a good laboratory for studying radio emission from CVs.
Driving Galactic Outflows with Magnetic Fields at Low and High Redshift
Authors: Steinwandel Ulrich P. , Dolag Klaus , Lesch Harald , Burkert Andreas 
Published: January 2022

Abstract
Although galactic outflows play a key role in our understanding of the evolution of galaxies, the exact mechanism by which galactic outflows are driven is still far from being understood and, therefore, our understanding of associated feedback mechanisms that control the evolution of galaxies is still plagued by many enigmas. In this work, we present a simple toy model that can provide insight on how non-axisymmetric instabilities in galaxies (bars, spiral arms, warps) can lead to local exponential magnetic field growth by radial flows beyond the equipartition value by at least two orders of magnitude on a timescale of a few 100 Myr. Our predictions show that the process can lead to galactic outflows in barred spiral galaxies with a mass-loading factor η ≈ 0.1, in agreement with our numerical simulations. Moreover, our outflow mechanism could contribute to an understanding of the large fraction of barred spiral galaxies that show signs of galactic outflows in the chang-es survey. Extending our model shows the importance of such processes in high-redshift galaxies by assuming equipartition between magnetic energy and turbulent energy. Simple estimates for the star formation rate in our model together with cross correlated masses from the star-forming main sequence at redshifts z ∼ 2 allow us to estimate the outflow rate and mass-loading factors by non-axisymmetric instabilities and a subsequent radial inflow dynamo, giving mass-loading factors of η ≈ 0.1 for galaxies in the range of M
⋆ = 109–1012
M
⊙, in good agreement with recent results of sinfoni and kmos
3D.
Changes in the Near-surface Shear Layer of the Sun
Authors: Antia H. M. , Basu Sarbani 
Published: January 2022

Abstract
We use helioseismic data obtained over two solar cycles to determine whether there are changes in the near-surface shear layer (NSSL). We examine this by determining the radial gradient of the solar rotation rate. The radial gradient itself shows a solar-cycle dependence, and the changes are more pronounced in the active latitudes than at adjoining higher latitudes; results at the highest latitudes (≳70°) are unreliable. The pattern changes with depth, even within the NSSL. We find that the near-surface shear layer is deeper at lower latitudes than at high latitudes and that the extent of the layer also shows a small solar-cycle-related change.
Gaussian Process Classification for Galaxy Blend Identification in LSST
Authors: Buchanan James J. , Schneider Michael D. , Armstrong Robert E. , Muyskens Amanda L. , Priest Benjamin W. , Dana Ryan J. 
Published: January 2022

Abstract
A significant fraction of observed galaxies in the Rubin Observatory Legacy Survey of Space and Time (LSST) will overlap at least one other galaxy along the same line of sight, in a so-called “blend.” The current standard method of assessing blend likelihood in LSST images relies on counting up the number of intensity peaks in the smoothed image of a blend candidate, but the reliability of this procedure has not yet been comprehensively studied. Here we construct a realistic distribution of blended and unblended galaxies through high-fidelity simulations of LSST-like images, and from this we examine the blend classification accuracy of the standard peak-finding method. Furthermore, we develop a novel Gaussian process blend classifier model, and show that this classifier is competitive with both the peak finding method as well as with a convolutional neural network model. Finally, whereas the peak-finding method does not naturally assign probabilities to its classification estimates, the Gaussian process model does, and we show that the Gaussian process classification probabilities are generally reliable.
COSMOS2020: A Panchromatic View of the Universe to z ∼ 10 from Two Complementary Catalogs
Authors: Weaver J. R. , Kauffmann O. B. , Ilbert O. , McCracken H. J. , Moneti A. , Toft S. , Brammer G. , Shuntov M. , Davidzon I. , Hsieh B. C. , Laigle C. , Anastasiou A. , Jespersen C. K. , Vinther J. , Capak P. , Casey C. M. , McPartland C. J. R. , Milvang-Jensen B. , Mobasher B. , Sanders D. B. , Zalesky L. , Arnouts S. , Aussel H. , Dunlop J. S. , Faisst A. , Franx M. , Furtak L. J. , Fynbo J. P. U. , Gould K. M. L. , Greve T. R. , Gwyn S. , Kartaltepe J. S. , Kashino D. , Koekemoer A. M. , Kokorev V. , Le Fèvre O. , Lilly S. , Masters D. , Magdis G. , Mehta V. , Peng Y. , Riechers D. A. , Salvato M. , Sawicki M. , Scarlata C. , Scoville N. , Shirley R. , Silverman J. D. , Sneppen A. , Smolc̆ić V. , Steinhardt C. , Stern D. , Tanaka M. , Taniguchi Y. , Teplitz H. I. , Vaccari M. , Wang W.-H. , Zamorani G. 
Published: January 2022

Abstract
The Cosmic Evolution Survey (COSMOS) has become a cornerstone of extragalactic astronomy. Since the last public catalog in 2015, a wealth of new imaging and spectroscopic data have been collected in the COSMOS field. This paper describes the collection, processing, and analysis of these new imaging data to produce a new reference photometric redshift catalog. Source detection and multiwavelength photometry are performed for 1.7 million sources across the 2 deg2 of the COSMOS field, ∼966,000 of which are measured with all available broadband data using both traditional aperture photometric methods and a new profile-fitting photometric extraction tool, The Farmer, which we have developed. A detailed comparison of the two resulting photometric catalogs is presented. Photometric redshifts are computed for all sources in each catalog utilizing two independent photometric redshift codes. Finally, a comparison is made between the performance of the photometric methodologies and of the redshift codes to demonstrate an exceptional degree of self-consistency in the resulting photometric redshifts. The i < 21 sources have subpercent photometric redshift accuracy and even the faintest sources at 25 < i < 27 reach a precision of 5%. Finally, these results are discussed in the context of previous, current, and future surveys in the COSMOS field. Compared to COSMOS2015, it reaches the same photometric redshift precision at almost one magnitude deeper. Both photometric catalogs and their photometric redshift solutions and physical parameters will be made available through the usual astronomical archive systems (ESO Phase 3, IPAC-IRSA, and CDS).
Mid-infrared Outbursts in Nearby Galaxies (MIRONG). II. Optical Spectroscopic Follow-up
Authors: Wang Yibo , Jiang Ning , Wang Tinggui , Yan Lin , Sheng Zhenfeng , Dou Liming , Ding Jiani , Cai Zheng , Sun Luming , Yang Chenwei , Shu Xinwen 
Published: January 2022

Abstract
Infrared echo has proven to be an effective means to discover transient accretion events of supermassive black holes (SMBHs), such as tidal disruption events (TDEs) and changing-look active galactic nuclei (AGNs), in dusty circumnuclear environments. To explore the dusty populations of SMBH transient events, we have constructed a large sample of mid-infrared outbursts in nearby galaxies (MIRONG) and performed multiwavelength observations. Here we present the results of multiepoch spectroscopic follow-up observations of a subsample of 54 objects spanning a timescale of 4 yr. Emission-line variability was detected in 22 of them with either emergence or enhancement of broad Balmer emission lines in comparison with pre-outburst spectra. Coronal lines, He ii
λ4686, and Bowen line N iii
λ4640 appeared in the spectra of nine, seven, and two sources, respectively. These results suggest that MIRONG is a mixed bag of different transient sources. We have tentatively classified them into different subclass according to their spectral evolution and light curves. Two sources have been in a steady high broad Hα flux up to the latest observation and might be turn-on AGNs. Broad lines faded out in the remaining sources, indicating a transient ionizing source ignited by TDE or sporadic gas accretion. Thirty-one sources do not show noticeable spectral change with respect to their pre-outburst spectra. They have a statistically redder MIR color and lower MIR luminosity of the outbursts, which are consistent with heavily obscured events.
A 12.2 GHz Methanol Maser Survey toward the 6.7 GHz Counterparts Associated with/without UC H ii Regions
Authors: Song Shi-Min , Chen Xi , Shen Zhi-Qiang , Li Bin , Yang Kai , Ouyang Xujia , Sobolev Andrej M. , Zhao Zhang , Li Xiao-Qiong , Cai Fan 
Published: January 2022

Abstract
We report a new survey of the 12.2 GHz Class II methanol masers toward a sample of 367 sources with the 6.7 GHz methanol masers conducted with the Shanghai 65 m Tianma Radio Telescope. This sample has been previously made with observations of the radio continuum emission of UC H ii regions by the VLA. A total of 176 sources were detected with the 12.2 GHz methanol maser, with a detection rate of 48%, including 8 new detections. A lower detection rate (<10%) was determined toward the sources in the Galactic longitude ranges of 60°–180°, revealing that the physical environments from those sources in the Local arm or the tails of Galactic arms do not easily excite the 12.2 GHz masers. In addition, two detections of highly excited-state OH masers at the 13.4 GHz transition were made, one of which is a new detection. Compared to previous surveys, one-third of the detected 12.2 GHz masers show considerable flux variations, implying the possible changes of their physical environments associated with variable radiation fields from their host high-mass young stellar objects. A positive log–log correlation is found between the luminosities of the 6.7 and 12.2 GHz masers in our observed sample, suggesting that both the transition masers have similar excitation conditions. The statistical analysis for the relationships between the methanol maser luminosity and UC H ii region spatial size indicates that the maser luminosities of both the 6.7 and 12.2 GHz transitions have a decreasing trend with the spatial sizes of the associated UC H ii regions, indicating that the Class II methanol masers might fade away with the H ii region evolution.
Could the Magnetic Star HD 135348 Possess a Rigidly Rotating Magnetosphere?
Authors: Jayaraman Rahul , Hubrig Swetlana , Holdsworth Daniel L. , Schöller Markus , Järvinen Silva , Kurtz Donald W. , Gagliano Robert , Ricker George R. 
Published: January 2022

Abstract
We report the detection and characterization of a new magnetospheric star, HD 135348, based on photometric and spectropolarimetric observations. The TESS light curve of this star exhibited variations consistent with stars known to possess rigidly rotating magnetospheres (RRMs), so we obtained spectropolarimetric observations using the Robert Stobie Spectrograph (RSS) on the South African Large Telescope (SALT) at four different rotational phases. From these observations, we calculated the longitudinal magnetic field of the star 〈B

z
〉, as well as the Alfvén and Kepler radii, and deduced that this star contains a centrifugal magnetosphere. However, an archival spectrum does not exhibit the characteristic “double-horned” emission profile for Hα and the Brackett series that has been observed in many other RRM stars. This could be due to the insufficient rotational phase coverage of the available set of observations, as the spectra of these stars significantly vary with the star’s rotation. Our analysis underscores the use of TESS in photometrically identifying magnetic star candidates for spectropolarimetric follow-up using ground-based instruments. We are evaluating the implementation of a machine-learning classifier to search for more examples of RRM stars in TESS data.