bluuebunny/crossref_metadata_2025_split huggingface dataset:
Epidemiological Approach: Relationship Between Exclusive Breastfeeding with Undernutrition Among Children
Authors: Abdurrahman Al Hakim Sampurna Putra S Ravenalla , Amadea Dyna Setyaji Fidela 
Published: April 2022

Nutritional status is a health problem in the under-five age group in Indonesia. An epidemiological approach was carried out to analyze the observations of children under five with poor nutritional status in the working area of ​​Puskesmas Kayon, Palangka Raya. This research is a quantitative study using an analytical observational research design with the cross-sectional approach. Data analysis in this study used the chi-square statistical test, to analyze the relationship between exclusive breastfeeding and the incidence of malnutrition. Respondents in this study were mothers who had toddlers and lived in the working area of ​​the Puskesmas Kayon, Palangka Raya, with 80 people. The results showed that there were 47 (58.8%) people who gave exclusive breastfeeding and 33 (41.2%) people did not give exclusive breastfeeding. The chi-square test shows a p-value = 0.024, which means that there is a significant correlation between exclusive breastfeeding and the nutritional status of children under five.
Analisis Investasi Instrumen Obligasi
Authors: Panjaitan Thyophoida W.S. , Widyastuti Maria 
Published: April 2022

Companies are difficult to obtain bank loans in large amounts can obtain public funds by selling bonds. Because the relationship is directly intertwined with public investors, the loan amount can be larger with a cheaper interest rate than bank loans. For the investor, investing in bonds relatively more than the profitguarantee stock. Bond investors from income levels can be calculated relatively from awal.Obligasi generally provide a fixed interest rate for six the first month. Usually, in order to attract investor interest, fixed rate bonds are set higher than the bond launched on time deposito.Jika interest rates move down, then the isseur (corporate bonds) will suffer a loss. However, if the bonds are sold at the interest rate moves up, it could be that the effect was not offered investors received. For the investor risks losing the possibility of falling bond prices and bond investment opportunities outside if at that time the interest rate more higher than the interest rate bonds. Issuance of bonds, in particular, is much more difficult than stocks because bond issuers should consider carefully the movement of interest rates. For investors who are actively conducting transactions, the instrument can also bring in revenue bonds in the form of capital gains. The bondholders have the right to claim precedence over shareholders.
A New Infrared Criterion for Selecting Active Galactic Nuclei to Lower Luminosities
Authors: Hviding Raphael E. , Hainline Kevin N. , Rieke Marcia , Juneau Stéphanie , Lyu 吕 Jianwei 建伟 , Pucha Ragadeepika 
Published: April 2022

Abstract
We present a spectroscopic and photometric analysis of a sample of 416,288 galaxies from the Sloan Digital Sky Survey (SDSS) matched to mid-infrared (mid-IR) data from the Wide-field Infrared Survey Explorer (WISE). By using a new spectroscopic fitting package, GELATO (Galaxy/AGN Emission Line Analysis TOol), we are able to retrieve emission line fluxes and uncertainties for SDSS spectra and robustly determine the presence of broad lines and outflowing components, enabling us to investigate WISE color space as a function of optical spectroscopic properties. In addition, we pursue spectral energy distribution template fitting to assess the relative active galactic nucleus (AGN) contribution and nuclear obscuration to compare to existing mid-IR selection criteria with WISE. We present a selection criterion in mid-IR color space to select AGNs with an ∼80% accuracy and a completeness of ∼16%. This is the first mid-IR color selection defined by solely using the distribution of Type I and Type II optical spectroscopic AGNs in WISE mid-IR color space. Our selection is an improvement of ∼50% in the completeness of targeting spectroscopic AGNs with WISE down to an SDSS r < 17.77 mag. In addition, our new criterion targets a less-luminous population of AGNs, with on average lower [O iii] luminosities by ∼30% ( > 0.1 dex) compared to typical WISE color–color selections. With upcoming large photometric surveys without corresponding spectroscopy, our method presents a way to select larger populations of AGNs at lower AGN luminosities and higher nuclear obscuration levels than traditional mid-IR color selections.
A Population of Luminous Globular Clusters and Stripped Nuclei with Elevated Mass to Light Ratios around NGC 5128*
Authors: Dumont Antoine , Seth Anil C. , Strader Jay , Voggel Karina , Sand David J. , Hughes Allison K. , Caldwell Nelson , Crnojević Denija , Mateo Mario , Bailey John I. , Forbes Duncan A. 
Published: April 2022

Abstract
The dense central regions of tidally disrupted galaxies can survive as ultracompact dwarfs (UCDs) that hide among the luminous globular clusters (GCs) in the halo of massive galaxies. An exciting confirmation of this model is the detection of overmassive black holes in the centers of some UCDs, which also lead to elevated dynamical mass-to-light ratios (M/L
dyn). Here we present new high-resolution spectroscopic observations of 321 luminous GC candidates in the massive galaxy NGC 5128/Centaurus A. Using these data we confirm 27 new luminous GCs, and measure velocity dispersions for 57 luminous GCs (with g-band luminosities between 2.5 × 105 and 2.5 × 107
L
⊙), of which 48 are new measurements. Combining these data with size measurements from Gaia, we determine the M/L
dyn for all 57 luminous GCs. We see a clear bimodality in the M/L
dyn distribution, with a population of normal GCs with mean M/L
dyn = 1.51 ± 0.31, and a second population of ∼20 GCs with elevated mean M/L
dyn = 2.68 ± 0.22. We show that black holes with masses ∼4%–18% of the luminous GCs can explain the elevated mass-to-light ratios. Hence, it is plausible that the NGC 5128 sources with elevated M/L
dyn are mostly stripped galaxy nuclei that contain massive central black holes, though future high spatial resolution observations are necessary to confirm this hypothesis for individual sources. We also present a detailed discussion of an extreme outlier, VHH81-01, one of the largest and most massive GC in NGC 5128, making it an exceptionally strong candidate to be a tidally stripped nucleus.
Abundance of LIGO/Virgo Black Holes from Microlensing Observations of Quasars with Reverberation Mapping Size Estimates
Authors: Esteban-Gutiérrez A. , Agües-Paszkowsky N. , Mediavilla E. , Jiménez-Vicente J. , Muñoz J. A. , Heydenreich S. 
Published: April 2022

Abstract
Assuming a population of black holes (BHs) with masses in the range inferred by LIGO/Virgo from BH mergers, we use quasar microlensing observations to estimate their abundances. We consider a mixed population of stars and BHs and the presence of a smooth dark matter component. We adopt reverberation mapping estimates of the quasar size. According to a Bayesian analysis of the measured microlensing magnifications, a population of BHs with masses ∼30M
⊙ constitutes less than 0.4% of the total matter at the 68% confidence level (less than 0.9% at the 90% confidence level). We have explored the whole mass range of LIGO/Virgo BHs, finding that this upper limit ranges from 0.5% to 0.4% at the 68% confidence level (from 1.1% to 0.9% at the 90% confidence level) when the BH masses change from 10 to 60M
⊙. We estimate a 16% contribution from the stars, in agreement with previous studies based on a single-mass population that do not explicitly consider the presence of BHs. These results are consistent with the estimates of BH abundances from the statistics of LIGO/Virgo mergers, and rule out primordial BHs (or any other types of compact object) in this mass range constituting a significant fraction of the dark matter.
Photoelectron Butterfly Pitch-angle Distributions in the Martian Ionosphere Based on MAVEN Observations
Authors: Luo Qiong , Cao Yutian , Ni Binbin , Cui Jun , Cao Xing , Gu Xudong 
Published: April 2022

Abstract
Using pitch-angle-resolved electron fluxes recorded by the Mars Atmosphere and Volatile Evolution spacecraft over 5 yr, we present a detailed analysis of the occurrence patterns of photoelectron butterfly pitch-angle distributions (PADs) in the Martian ionosphere. Statistical analysis indicates that Martian photoelectron butterfly PADs favorably occur near the moderate crustal magnetic fields with a strength of 10–30 nT on the dayside and 10–15 nT on the nightside. The nightside occurrence rates are much higher. Furthermore, dayside butterfly PADs prefer to occur near the vertical magnetic field lines in the ionosphere, and the significant day-to-night transport of photoelectrons evades the nightside strongest magnetic anomaly regions. These features strongly support the idea that Martian photoelectron butterfly PADs are more likely to occur in eclipse or near the terminator and that they mainly form due to the adiabatic evolution of photoelectrons that transport along the closed cross-terminator magnetic field lines. Despite the negligible energy dependence in the darkness, the occurrence rate of dayside butterfly PADs observed at higher altitudes and near the subsolar region increases with energy, presumably related to the increased proportion of electrons from the solar wind when measured at relatively higher electron energies, which, however, is limitedly understood and deserves future investigation. Our comprehensive observations suggest the diverse influence of Martian magnetic topology on the ionospheric plasma in different spatial regions, and, in turn, analysis of their influence allows us a better understanding of the intricate Martian global magnetic system.
Spatial Power Spectral Analysis of the Suzaku X-Ray Background
Authors: Zhou Yu , Mitsuda Kazuhisa , Yamasaki Noriko Y. 
Published: April 2022

Abstract
Power spectra of spatial fluctuations of X-ray emission may impose constraints on the origins of the emission independent of that from the energy spectra. We generated spatial power spectrum densities (PSDs) of blank X-ray skies observed with the Suzaku X-ray observatory utilizing the modified Δ-variance method. Using the total measured count rate as the diagnostic tool, we found that a model consisting of the sum of two components, one for the unresolved faint point sources and one for the uniform flat-field emission, can represent well the observed PSD in three different energy bands (0.2–0.5, 0.5–2, and 2–10 keV); only an upper limit is obtained for the latter component in 2–10 keV. X-ray counting rates corresponding to the best-fit PSD model functions and diffuse emission fractions were estimated, and we confirmed that the sum of the counting rates of two model components is consistent with those actually observed with the detector for all energy bands. The ratio of the flat-field counting rate to the total in 0.5–2 keV, however, is significantly larger than the diffuse emission fraction estimated from the model fits of energy spectra. We discussed that this discrepancy can be reconciled by systematic effects in the PSD and energy spectrum analyses. The present study demonstrates that the spatial power spectrum analysis is powerful in constraining the origins of the X-ray emission.
Effects of an Immortal Stellar Population in AGN Disks
Authors: Jermyn Adam S. , Dittmann Alexander J. , McKernan B. , Ford K. E. S. , Cantiello Matteo 
Published: April 2022

Abstract
Stars are likely embedded in the gas disks of active galactic nuclei (AGN). Theoretical models predict that in the inner regions of the disk, these stars accrete rapidly, with fresh gas replenishing hydrogen in their cores faster than it is burned into helium, effectively stalling their evolution at hydrogen burning. We produce order-of-magnitude estimates of the number of such stars in a fiducial AGN disk. We find numbers of order 102–4, confined to the inner r
cap ∼ 3000r

s
∼ 0.03 pc. These stars can profoundly alter the chemistry of AGN disks, enriching them in helium and depleting them in hydrogen, both by order-unity amounts. We further consider mergers between these stars and other disk objects, suggesting that star–star mergers result in rapid mass loss from the remnant to restore an equilibrium mass, while star–compact object mergers may result in exotic outcomes and even host binary black hole mergers within themselves. Finally, we examine how these stars react as the disk dissipates toward the end of its life, and find that they may return mass to the disk fast enough to extend its lifetime by a factor of several and/or may drive powerful outflows from the disk. Post-AGN, these stars rapidly lose mass and form a population of stellar mass black holes around 10M
⊙. Due to the complex and uncertain interactions between embedded stars and the disk, their plausible ubiquity, and their order-unity impact on disk structure and evolution, they must be included in realistic disk models.
EMPRESS. VI. Outflows Investigated in Low-mass Galaxies with M
∗ = 104–107
M
⊙: Weak Feedback in Low-mass Galaxies?
Authors: Xu Yi , Ouchi Masami , Rauch Michael , Nakajima Kimihiko , Harikane Yuichi , Sugahara Yuma , Komiyama Yutaka , Kusakabe Haruka , Fujimoto Seiji , Isobe Yuki , Kim Ji Hoon , Ono Yoshiaki , Zahedy Fakhri S. 
Published: April 2022

Abstract
We study emission line profiles of 21 nearby low-mass (M
* = 104–107
M
⊙) galaxies in deep medium-high resolution spectra taken with Magellan/MagE. These low-mass galaxies are actively star-forming systems with high specific star formation rates of ∼100–1000 Gyr−1 that are well above the star formation main sequence and its extrapolation. We identify broad-line components of Hα and [O iii]λ5007 emission in 14 out of the 21 galaxies that cannot be explained by the MagE instrumental profile or the natural broadening of line emission. We conduct double-Gaussian profile fitting to the emission of the 14 galaxies, and find that the broad-line components have line widths significantly larger than those of the narrow-line components, indicative of galactic outflows. The broad-line components have moderately large line widths of ∼100 km s−1. We estimate the maximum outflow velocities v
max and obtain values of ≃60–200 km s−1, which are found to be comparable to or slightly larger than the escape velocities. Positive correlations of v
max with star formation rates, stellar masses, and circular velocities extend down into this low-mass regime. Broad- to narrow-line flux ratios (BNRs) are generally found to be smaller than those of massive galaxies. The small v
max and BNRs suggest that the mass-loading factors η can be as small as 0.1–1 or below, in contrast to the large η of energy-driven outflows predicted by numerical simulations.
An 8.56 keV Absorption Line in the Hyperluminous X-Ray Source in NGC 4045: Ultrafast Outflow or Cyclotron Line?
Authors: Brightman Murray , Kosec Peter , Fürst Felix , Earnshaw Hannah , Heida Marianne , Middleton Matthew J , Stern Daniel , Walton Dominic J 
Published: April 2022

Abstract
We report on the discovery of an absorption line at

E
=

8.56

−
0.11

+
0.05

keV detected with a significance of >3.3σ in the NuSTAR and XMM-Newton spectra of a newly discovered hyperluminous X-ray source (L
X > 1041 erg s−1) in the galaxy NGC 4045 at a distance of 32 Mpc. The source was first discovered serendipitously in a Swift/XRT observation of the galaxy, and Swift monitoring reveals a highly variable source changing by over an order of magnitude from maximum to minimum. The origin of the absorption line appears likely to be from highly ionized iron with a blueshift of 0.19c, indicating an ultrafast outflow. However, the large equivalent width of the line (

EW
=
−

0.22

−
0.09

+
0.08

keV) paired with the lack of other absorption lines detected is difficult to reconcile with models. An alternative explanation is that the line is due to a cyclotron resonance scattering feature produced by the interaction of X-ray photons with the powerful magnetic field of a neutron star.
Approximating Density Probability Distribution Functions Across Cosmologies
Authors: Chen Huanqing , Gnedin Nickolay Y. , Mansfield Philip 
Published: April 2022

Abstract
Using a suite of self-similar cosmological simulations, we measure the probability distribution functions (PDFs) of real-space density, redshift-space density, and their geometric mean. We find that the real-space density PDF is well-described by a function of two parameters: n

s
, the spectral slope, and σ

L
, the linear rms density fluctuation. For redshift-space density and the geometric mean of real- and redshift-space densities, we introduce a third parameter,

s

L

=

〈

dv

pec

L

/

dr

2

〉

/

H

. We find that density PDFs for the LCDM cosmology is also well-parameterized by these three parameters. As a result, we are able to use a suite of self-similar cosmological simulations to approximate density PDFs for a range of cosmologies. We make the density PDFs publicly available and provide an analytical fitting formula for them.
Anatomy of Pulsar XTE J1829-098: Ultramassive SXFT with a Dominant Nondipolar Magnetic Field, or the Third Canonical HMXB Caught at the Bottom of the Corbet Gap?
Authors: Christodoulou Dimitris M. , Bhattacharya Sayantan , Laycock Silas G. T. , Kazanas Demosthenes 
Published: April 2022

Abstract
The X-ray binary pulsar XTE J1829-098 has been observed at extremely low luminosities for its spin period of 7.8448 s. Although its distance is uncertain by a factor of 4, the lowest observed X-ray fluxes may not correspond to its minimal-accretion propeller state or to nonaccreting states occurring at even lower X-ray luminosities, in which case the source has been caught at the bottom of the Corbet gap. We analyze all proposed distances D to the binary and the lowest X-ray fluxes, and we find only two physically acceptable solutions: (a) For D = 4.5 kpc (if the companion is a main-sequence B0 star), the neutron star is canonical with mass 1.41 M
⊙, radius 10.1 km, and a purely dipolar magnetic field as indicated by a cyclotron absorption line detected at 15 keV. In this case, the source has been observed at the bottom of the Corbet gap, the third high-mass X-ray binary pulsar to be caught in this state after the “twins” 4U 0115+63 and V 0332+53 found by Tsygankov et al. (b) For D = 18 kpc (if the companion is a B0.5Ib supergiant), the neutron star is ultramassive with mass 2.62 M
⊙, radius 18.7 km, and a dominant nondipolar magnetic field B
mul = 1.26 TG (versus a dipolar component of only B
dip = 0.43 TG). In this case, the source has been observed in its propeller state.
A Model of Homologous Confined and Ejective Eruptions Involving Kink Instability and Flux Cancellation
Authors: Hassanin Alshaimaa , Kliem Bernhard , Seehafer Norbert , Török Tibor 
Published: April 2022

Abstract
In this study, we model a sequence of a confined and a full eruption, employing the relaxed end state of the confined eruption of a kink-unstable flux rope as the initial condition for the ejective one. The full eruption, a model of a coronal mass ejection, develops as a result of converging motions imposed at the photospheric boundary, which drive flux cancellation. In this process, parts of the positive and negative external flux converge toward the polarity inversion line, reconnect, and cancel each other. Flux of the same amount as the canceled flux transfers to a flux rope, increasing the free magnetic energy of the coronal field. With sustained flux cancellation and the associated progressive weakening of the magnetic tension of the overlying flux, we find that a flux reduction of ≈11% initiates the torus instability of the flux rope, which leads to a full eruption. These results demonstrate that a homologous full eruption, following a confined one, can be driven by flux cancellation.
Using Maximum Circular Velocity in Halo Occupation Distribution Models to Predict Galaxy Clustering
Authors: Mezini Lorena , Wang Kuan , Mao Yao-Yuan , Zentner Andrew R. 
Published: April 2022

Abstract
Standard halo occupation distribution (HOD) models predict how galaxies occupy halos based on a single property, the virial mass, M
vir. To incorporate galaxy assembly bias, we consider alternative halo mass proxies to use in the HOD. A promising replacement is maximum circular velocity,

V

max

, which measures the halo’s potential well, and successfully predicts galaxy clustering in subhalo abundance matching models. We fit galaxy clustering measurements from SDSS DR7 with two modified HODs besides the standard M
vir-based model: one where

V

max

is used as the halo property that determines galaxy occupation, and the other adopting an adjustable combination of M
vir and

V

max

. Except for the reduced volume M

r
< − 20 threshold sample fit with

V

max

alone, neither change improves the model performance in predicting the projected two-point correlation function, w
p. We conclude that switching the primary variable to

V

max

does not significantly improve the HOD model’s ability to fit galaxy clustering.
Screening of Amorpha fruticosa and Ailanthus altissima extracts for genotoxicity/antigenotoxicity, mutagenicity/antimutagenicity and carcinogenicity/anticarcinogenicity
Authors: Todorova Teodora , Boyadzhiev Krassimir , Shkondrov Aleksandar , Parvanova Petya , Dimitrova Maria , Ionkova Iliana , Krasteva Ilina , Kozuharova Ekaterina , Chankova Stephka 
Published: April 2022

The aim of the present study was to evaluate the potential genotoxic/antigenotoxic, mutagenic/antimutagenic, and carcinogenic/anticarcinogenic effect of Amorpha fruticosa (AF) fruit, Ailanthus altissima bark hexane (AAEH) and methanol (AAEM) extracts on a model system Saccharomyces cerevisiae.
Plants were identified and extracted by Ekaterina Kozuharova. Three concentrations of each extract were tested – 10, 100 and 1000 µg/ml. In vitro pro-oxidant/antioxidant activities were evaluated by DPPH and DNA topology assay. The potential genotoxic/antigenotoxic, mutagenic/antimutagenic and carcinogenic/anticarcinogenic effects were revealed in vivo by: Zimmermman’s test on Saccharomyces cerevisiae diploid strain D7ts1, and Ty1 retrotransposition test on S. cerevisiae haploid strain 551. Zeocin was used as a positive control.
Based on the in vitro antioxidant activity the extracts could be arranged as follows: AF&gt;AAEM&gt;AAEH. AAEH possessed moderate oxidative potential. No genotoxic and mutagenic capacity was obtained in vivo for extracts tested. The levels of total aberrants, convertants and revertants were comparable with the control ones. No Ty1 retrotransposition was induced by extracts treatment. Further, the extracts possessed well-expressed antigenotoxic, antimutagenic and anticarcinogenic activity. Significant reduction of the total aberrants, reverse point mutations and Ty1 retrotransposition was obtained. Only the AF extract was found to reduce the levels of zeocin-induced mitotic gene conversion.
The three extracts did not possess any genotoxic, mutagenic and carcinogenic effect on Saccharomyces cerevisiae. Based on their protective activity, they can be arranged as follows: AF&gt;AAEM&gt;AAEH which corresponds well with their phytochemical composition. Further experiments could provide more detailed information concerning the mode of action of extracts, as well as their main constituents.