bluuebunny/crossref_metadata_2025_split huggingface dataset:
A Study to Assess the Effectiveness Of Structured Teaching Programme on Knowledge Regarding Hand Exercise in Prevention of AV Fistula Dysfunction among Hemodialysis Patient In Selected Hospital, Tumkur
Authors: Shilpa Rani R  , Eswarappa S  , Dayanand C  , Balaji M. S.  , Geethanjali S  
Published: January 2023

Health is wealth; this phrase is very popular because happiness lies in the health of man. Good health helps to develop charm, grace, and happy mind. Kidneys are a pair of bean shaped organs located either side of the lower back just below the rib cage. Renal failure is the severe impairment or total lack of kidney function. Chronic Renal Failure (CRF) develops insidiously overtime and necessitates the initiation for long term survival.1 Dialysis is used to remove fluid and uremic waste products from the body when the kidneys are not able to do so. It is the best method to use arteriovenous fistula (AVF) as a vascular access. Compared to other vascular access such as venous catheter and a synthetic graft, arteriovenous fistula is most used method as it has fewer complications. Complications can occur even if we are careful, but are much less common if you take a few precautions. Hand exercise is essential to perform in prevention of AV fistula dysfunction. The aim of the study was to assess the effectiveness of Structured Teaching Programme on knowledge regarding Hand exercise among Hemodialysis patients in selected hospital, Tumkur.Methods: n evaluative approach with pre-experimental one group pre-test post-test design was used with purposive sampling technique to select the sample (N=50). A structured knowledge questionnaire was used to assess the Knowledge and STP was administered to find its effectiveness. The collected data was analyzed by using Descriptive statistics like mean, median and standard deviation, and inferential statistics like paired and independent‘t’ test was included to test the hypothesis and Chi-square test was included to test the association of knowledge scores with demographic variables.Results: The mean percentage of post-test knowledge score (79.09 %) was higher than the mean percentage of pre-test knowledge score (36.54%). The calculated’ value [t (49) = 21.01] is greater than the table value (0.05, 49df) = 1.96. It showed a significant difference between mean pre- and post- test knowledge scores. Calculated x2 values are showed no significant association between any of the variables with their post-test knowledge scores. Therefore, no significant association was found between these other variables and post-test knowledge level of Hemodialysis patients.
Interpretation & Conclusion: The findings of the study showed that there was a deficit in knowledge ofHemodialysis patients before administration of STP. The results indicated that the STP is effective in increasingthe knowledge of Hemodialysis patients on Hand exercise.
Target Selection and Validation of DESI Luminous Red Galaxies
Authors: Zhou Rongpu , Dey Biprateep , Newman Jeffrey A. , Eisenstein Daniel J. , Dawson K. , Bailey S. , Berti A. , Guy J. , Lan Ting-Wen , Zou H. , Aguilar J. , Ahlen S. , Alam Shadab , Brooks D. , de la Macorra A. , Dey A. , Dhungana G. , Fanning K. , Font-Ribera A. , Gontcho S. Gontcho A. , Honscheid K. , Ishak Mustapha , Kisner T. , Kovács A. , Kremin A. , Landriau M. , Levi Michael E. , Magneville C. , Manera Marc , Martini P. , Meisner Aaron M. , Miquel R. , Moustakas J. , Myers Adam D. , Nie Jundan , Palanque-Delabrouille N. , Percival W. J. , Poppett C. , Prada F. , Raichoor A. , Ross A. J. , Schlafly E. , Schlegel D. , Schubnell M. , Tarlé Gregory , Weaver B. A. , Wechsler R. H. , Yéche Christophe , Zhou Zhimin 
Published: January 2023

Abstract
The Dark Energy Spectroscopic Instrument (DESI) is carrying out a five-year survey that aims to measure the redshifts of tens of millions of galaxies and quasars, including 8 million luminous red galaxies (LRGs) in the redshift range 0.4 < z ≲ 1.0. Here we present the selection of the DESI LRG sample and assess its spectroscopic performance using data from Survey Validation (SV) and the first two months of the Main Survey. The DESI LRG sample, selected using g, r, z, and W1 photometry from the DESI Legacy Imaging Surveys, is highly robust against imaging systematics. The sample has a target density of 605 deg−2 and a comoving number density of 5 × 10−4
h
3 Mpc−3 in 0.4 < z < 0.8; this is a significantly higher density than previous LRG surveys (such as SDSS, BOSS, and eBOSS) while also extending to z ∼ 1. After applying a bright star veto mask developed for the sample, 98.9% of the observed LRG targets yield confident redshifts (with a catastrophic failure rate of 0.2% in the confident redshifts), and only 0.5% of the LRG targets are stellar contamination. The LRG redshift efficiency varies with source brightness and effective exposure time, and we present a simple model that accurately characterizes this dependence. In the appendices, we describe the extended LRG samples observed during SV.
The Giant Accreting Protoplanet Survey (GAPlanetS): Optimization Techniques for Robust Detections of Protoplanets
Authors: Adams Redai Jéa I. , Follette Katherine B. , Wang 王 Jason 劲飞 , Leonard Clare , Balmer William , Close Laird M. , Dacus Beck , Males Jared R. , Morzinski Katie M. , Palmo Joseph , Pueyo Laurent , Spiro Elijah , Treiber Helena , Ward-Duong Kimberly , Watson Alex 
Published: January 2023

Abstract
High-contrast imaging has afforded astronomers the opportunity to study light directly emitted by adolescent (tens of megayears) and “proto” (<10 Myr) planets still undergoing formation. Direct detection of these planets is enabled by empirical point-spread function (PSF) modeling and removal algorithms. The computational intensity of such algorithms, as well as their multiplicity of tunable input parameters, has led to the prevalence of ad hoc optimization approaches to high-contrast imaging results. In this work, we present a new, systematic approach to optimization vetted using data of the high-contrast stellar companion HD 142527 B from the Magellan Adaptive Optics Giant Accreting Protoplanet Survey (GAPlanetS). More specifically, we present a grid search technique designed to explore three influential parameters of the PSF subtraction algorithm pyKLIP: annuli, movement, and KL modes. We consider multiple metrics for postprocessed image quality in order to optimally recover at Hα (656 nm) synthetic planets injected into contemporaneous continuum (643 nm) images. These metrics include peak (single-pixel) signal-to-noise ratio (S/N), average (multipixel average) S/N, 5σ contrast, and false-positive fraction. We apply continuum-optimized KLIP reduction parameters to six Hα direct detections of the low-mass stellar companion HD 142527 B and recover the companion at a range of separations. Relative to a single-informed, nonoptimized set of KLIP parameters applied to all data sets uniformly, our multimetric grid search optimization led to improvements in companion S/N of up to 1.2σ, with an average improvement of 0.6σ. Since many direct imaging detections lie close to the canonical 5σ threshold, even such modest improvements may result in higher yields in future imaging surveys.
MAVEN Observations of Whistler-mode Waves Within the Magnetic Dips in the Martian Ionopause/Ionosphere
Authors: Wang Jing , Yu Jiang , Chen Zuzheng , Xu Xiaojun , Li Kun , Cui Jun , Cao Jinbin 
Published: January 2023

Abstract
Whistler-mode waves are natural and common electromagnetic emissions observed both surrounding planets and their moons with and without intrinsic magnetic field. Numerous observations have shown that the magnetic dip is a favorable region for the whistler-mode wave generation in the Earth’s magnetosphere. However, up to now, seldom observations of these waves have been reported in such regions at Mars. Based on the measurements from Mars Atmosphere and Volatile EvolutioN mission, quasi-parallel propagating whistler-mode waves are observed within magnetic dip structures in the Martian ionopause and ionosphere. Correspondingly, significant electron beams in the antiparallel direction are observed, and a linear instability analysis shows that f
pe/f
ce becomes extremely large (∼1500) inside the magnetic dip. Thus, the electron minimum resonant energy of whistler-mode waves decreases to several eV, which increases the number density of resonant beam electrons. Such beam electron distribution results in the necessary free energy for the whistler-mode wave growth. Our study indicates magnetic dips may be favorable regions for the whistler-mode wave excitation even in the Martian ionosphere, which has an extremely high f
pe/f
ce but does not have a global intrinsic magnetic field.
Pegasus IV: Discovery and Spectroscopic Confirmation of an Ultra-faint Dwarf Galaxy in the Constellation Pegasus
Authors: Cerny W. , Simon J. D. , Li T. S. , Drlica-Wagner A. , Pace A. B. , Martínez-Vázquez C. E. , Riley A. H. , Mutlu-Pakdil B. , Mau S. , Ferguson P. S. , Erkal D. , Munoz R. R. , Bom C. R. , Carlin J. L. , Carollo D. , Choi Y. , Ji A. P. , Manwadkar V. , Martínez-Delgado D. , Miller A. E. , Noël N. E. D. , Sakowska J. D. , Sand D. J. , Stringfellow G. S. , Tollerud E. J. , Vivas A. K. , Carballo-Bello J. A. , Hernandez-Lang D. , James D. J. , Nidever D. L. , Castellon J. L. Nilo , Olsen K. A. G. , Zenteno A. ,   DELVE Collaboration
Published: January 2023

Abstract
We report the discovery of Pegasus IV, an ultra-faint dwarf galaxy found in archival data from the Dark Energy Camera processed by the DECam Local Volume Exploration Survey. Pegasus IV is a compact, ultra-faint stellar system (

r

1

/

2

=

41

−
6

+
8

pc; M

V
= −4.25 ± 0.2 mag) located at a heliocentric distance of

90

−
6

+
4

kpc

. Based on spectra of seven nonvariable member stars observed with Magellan/IMACS, we confidently resolve Pegasus IV’s velocity dispersion, measuring

σ

v

=

3.3

−
1.1

+
1.7

km s−1 (after excluding three velocity outliers); this implies a mass-to-light ratio of

M

1

/

2

/

L

V
,
1

/

2

=

167

−
99

+
224

M

⊙

/

L

⊙

for the system. From the five stars with the highest signal-to-noise spectra, we also measure a systemic metallicity of [Fe/H] =

−

2.63

−
0.30

+
0.26

dex, making Pegasus IV one of the most metal-poor ultra-faint dwarfs. We tentatively resolve a nonzero metallicity dispersion for the system. These measurements provide strong evidence that Pegasus IV is a dark-matter-dominated dwarf galaxy, rather than a star cluster. We measure Pegasus IV’s proper motion using data from Gaia Early Data Release 3, finding (μ

α*, μ

δ
) = (0.33 ± 0.07, −0.21 ± 0.08) mas yr−1. When combined with our measured systemic velocity, this proper motion suggests that Pegasus IV is on an elliptical, retrograde orbit, and is currently near its orbital apocenter. Lastly, we identify three potential RR Lyrae variable stars within Pegasus IV, including one candidate member located more than 10 half-light radii away from the system’s centroid. The discovery of yet another ultra-faint dwarf galaxy strongly suggests that the census of Milky Way satellites is still incomplete, even within 100 kpc.
X-Ray Properties of NGC 253's Starburst-driven Outflow
Authors: Lopez Sebastian , Lopez Laura A. , Nguyen Dustin D. , Thompson Todd A. , Mathur Smita , Bolatto Alberto D. , Vulic Neven , Sardone Amy 
Published: January 2023

Abstract
We analyze image and spectral data from ≈365 ks of observations from the Chandra X-ray Observatory of the nearby, edge-on starburst galaxy NGC 253 to constrain properties of the hot phase of the outflow. We focus our analysis on the −1.1 to +0.63 kpc region of the outflow and define several regions for spectral extraction where we determine best-fit temperatures and metal abundances. We find that the temperatures and electron densities peak in the central ∼250 pc region of the outflow and decrease with distance. These temperature and density profiles are in disagreement with an adiabatic spherically expanding starburst wind model and suggest the presence of additional physics such as mass loading and nonspherical outflow geometry. Our derived temperatures and densities yield cooling times in the nuclear region of a few million years, which may imply that the hot gas can undergo bulk radiative cooling as it escapes along the minor axis. Our metal abundances of O, Ne, Mg, Si, S, and Fe all peak in the central region and decrease with distance along the outflow, with the exception of Ne, which maintains a flat distribution. The metal abundances indicate significant dilution outside of the starburst region. We also find estimates of the mass outflow rates, which are 2.8 M
⊙ yr−1 in the northern outflow and 3.2 M
⊙ yr−1 in the southern outflow. Additionally, we detect emission from charge exchange and find it makes a significant contribution (20%–42%) to the total broadband (0.5–7 keV) X-ray emission in the central and southern regions of the outflow.
Effects of the Central Mass Concentration on Bar Formation in Disk Galaxies
Authors: Jang Dajeong , Kim Woong-Tae 
Published: January 2023

Abstract
While bars are common in disk galaxies, their formation conditions are not well understood. We use N-body simulations to study the formation and evolution of a bar in isolated galaxies consisting of a stellar disk, a classical bulge, and a dark halo. We consider 24 galaxy models that are similar to the Milky Way but differ in the mass and compactness of the classical bulge and halo concentration. We find that the bar formation requires

(

Q

T
,
min

/

1.2
)

2

+

(
CMC

/

0.05
)

2

≲
1

, where

Q

T
,
min

and CMC refer to the minimum value of the Toomre stability parameter and the central mass concentration, respectively. Bars tend to be stronger and longer, and to rotate more slowly, in galaxies with a less massive and less compact bulge and halo. All bars formed in our models correspond to slow bars. A model with the bulge mass of ∼10%–20% of the disk under a concentrated halo produces a bar similar to that of the Milky Way. We discuss our findings in relation to other bar formation criteria suggested by previous studies.
Digging into the Galactic Bulge: Stellar Population and Structure of the Poorly Studied Cluster NGC 6316
Authors: Deras Dan , Cadelano Mario , Ferraro Francesco R. , Lanzoni Barbara , Pallanca Cristina 
Published: January 2023

Abstract
High-resolution Hubble Space Telescope optical observations have been used to analyze the stellar population and the structure of the poorly investigated bulge globular cluster NGC 6316. We constructed the first high-resolution reddening map in the cluster direction, which allowed us to correct the evolutionary sequences in the color–magnitude diagram (CMD) for the effects of differential reddening. A comparison between the CMDs of NGC 6316 and 47 Tucanae revealed strikingly similar stellar populations, with the two systems basically sharing the same turnoff, subgiant branch, and horizontal branch morphologies, indicating comparable ages. The red giant branch in NGC 6316 appears slightly bluer than in 47 Tucanae, suggesting a lower metal content. This has been confirmed by the isochrone fitting of the observed CMD, which provided us with updated values of the cluster age, distance, average color excess, and metallicity. We estimated an absolute age of 13.1 ± 0.5 Gyr, consistent with the age of 47 Tucanae, an average color excess E(B − V) = 0.64 ± 0.01, and a true distance modulus (m − M)0 = 15.27 ± 0.03 that sets the cluster distance at 11.3 kpc from the Sun. In addition, the photometric estimate of the cluster metallicity suggests [Fe/H] ≈ −0.9, which is ∼0.2 dex smaller than that of 47 Tucanae. We also determined the gravitational center and the density profile of the system from resolved stars. The latter is well reproduced by a King model. Our results confirm that NGC 6316 is another extremely old relic of the assembly history of the Galaxy.
A Machine-learning Approach to Predict Missing Flux Densities in Multiband Galaxy Surveys
Authors: Chartab Nima , Mobasher Bahram , Cooray Asantha R. , Hemmati Shoubaneh , Sattari Zahra , Ferguson Henry C. , Sanders David B. , Weaver John R. , Stern Daniel K. , McCracken Henry J. , Masters Daniel C. , Toft Sune , Capak Peter L. , Davidzon Iary , Dickinson Mark E. , Rhodes Jason , Moneti Andrea , Ilbert Olivier , Zalesky Lukas , McPartland Conor J. R. , Szapudi István , Koekemoer Anton M. , Teplitz Harry I. , Giavalisco Mauro 
Published: January 2023

Abstract
We present a new method based on information theory to find the optimal number of bands required to measure the physical properties of galaxies with desired accuracy. As a proof of concept, using the recently updated COSMOS catalog (COSMOS2020), we identify the most relevant wave bands for measuring the physical properties of galaxies in a Hawaii Two-0- (H20) and UVISTA-like survey for a sample of i < 25 AB mag galaxies. We find that with the available i-band fluxes, r, u, IRAC/ch2, and z bands provide most of the information regarding the redshift with importance decreasing from r band to z band. We also find that for the same sample, IRAC/ch2, Y, r, and u bands are the most relevant bands in stellar-mass measurements with decreasing order of importance. Investigating the intercorrelation between the bands, we train a model to predict UVISTA observations in near-IR from H20-like observations. We find that magnitudes in the YJH bands can be simulated/predicted with an accuracy of 1σ mag scatter ≲0.2 for galaxies brighter than 24 AB mag in near-IR bands. One should note that these conclusions depend on the selection criteria of the sample. For any new sample of galaxies with a different selection, these results should be remeasured. Our results suggest that in the presence of a limited number of bands, a machine-learning model trained over the population of observed galaxies with extensive spectral coverage outperforms template fitting. Such a machine-learning model maximally comprises the information acquired over available extensive surveys and breaks degeneracies in the parameter space of template fitting inevitable in the presence of a few bands.
Forward Modeling of Galaxy Populations for Cosmological Redshift Distribution Inference
Authors: Alsing Justin , Peiris Hiranya , Mortlock Daniel , Leja Joel , Leistedt Boris 
Published: January 2023

Abstract
We present a forward-modeling framework for estimating galaxy redshift distributions from photometric surveys. Our forward model is composed of: a detailed population model describing the intrinsic distribution of the physical characteristics of galaxies, encoding galaxy evolution physics; a stellar population synthesis model connecting the physical properties of galaxies to their photometry; a data model characterizing the observation and calibration processes for a given survey; and explicit treatment of selection cuts, both into the main analysis sample and for the subsequent sorting into tomographic redshift bins. This approach has the appeal that it does not rely on spectroscopic calibration data, provides explicit control over modeling assumptions and builds a direct bridge between photo-z inference and galaxy evolution physics. In addition to redshift distributions, forward modeling provides a framework for drawing robust inferences about the statistical properties of the galaxy population more generally. We demonstrate the utility of forward modeling by estimating the redshift distributions for the Galaxy And Mass Assembly (GAMA) survey and the Vimos VLT Deep Survey (VVDS), validating against their spectroscopic redshifts. Our baseline model is able to predict tomographic redshift distributions for GAMA and VVDS with respective biases of Δz ≲ 0.003 and Δz ≃ 0.01 on the mean redshift—comfortably accurate enough for Stage III cosmological surveys—without any hyperparameter tuning (i.e., prior to doing any fitting to those data). We anticipate that with additional hyperparameter fitting and modeling improvements, forward modeling will provide a path to accurate redshift distribution inference for Stage IV surveys.
Searching for Molecular Jets from High-mass Protostars
Authors: Rodríguez Tatiana M. , Hofner Peter , Edelman Isaac , Araya Esteban D. , Rosero Viviana 
Published: January 2023

Abstract
We report Very Large Array observations in the Q band toward 10 ionized jet candidates to search for SiO emission, a well-known shocked gas tracer. We detected 7 mm continuum counterparts toward 90% of the jet candidates. In most cases, the jet candidate is located toward the center of the 7 mm core, and the high masses (≈100 M
⊙) and densities (≈107 cm−3) of the cores suggest that the central objects are very young high-mass protostars. We detected SiO J = 1–0 emission associated with six target sources. In all cases, the morphology and spectrum of the emission is consistent with what is expected for molecular jets along an outflow axis, thus confirming the jet nature of 60% of our sample. Our data suggest a positive correlation between the SiO luminosity L
SiO, and both the bolometric luminosity L
Bol and the radio luminosity S

ν

d
2 of the driving sources.
The Dark Energy Camera Plane Survey 2 (DECaPS2): More Sky, Less Bias, and Better Uncertainties
Authors: Saydjari Andrew K. , Schlafly Edward F. , Lang Dustin , Meisner Aaron M. , Green Gregory M. , Zucker Catherine , Zelko Ioana , Speagle 沈 Joshua S. 佳士 , Daylan Tansu , Lee Albert , Valdes Francisco , Schlegel David , Finkbeiner Douglas P. 
Published: January 2023

Abstract
Deep optical and near-infrared imaging of the entire Galactic plane is essential for understanding our Galaxy’s stars, gas, and dust. The second data release of the Dark Energy Camera (DECam) Plane Survey extends the five-band optical and near-infrared survey of the southern Galactic plane to cover 6.5% of the sky, ∣b∣ ≤ 10°, and 6° > ℓ > −124°, complementary to coverage by Pan-STARRS1. Typical single-exposure effective depths, including crowding effects and other complications, are 23.5, 22.6, 22.1, 21.6, and 20.8 mag in g, r, i, z, and Y bands, respectively, with around 1″ seeing. The survey comprises 3.32 billion objects built from 34 billion detections in 21,400 exposures, totaling 260 hr open shutter time on the DECam at Cerro Tololo. The data reduction pipeline features several improvements, including the addition of synthetic source injection tests to validate photometric solutions across the entire survey footprint. A convenient functional form for the detection bias in the faint limit was derived and leveraged to characterize the photometric pipeline performance. A new postprocessing technique was applied to every detection to debias and improve uncertainty estimates of the flux in the presence of structured backgrounds, specifically targeting nebulosity. The images and source catalogs are publicly available at http://decaps.skymaps.info/.