bluuebunny/crossref_metadata_2025_split huggingface dataset:
Testing the LSST Difference Image Analysis Pipeline Using Synthetic Source Injection Analysis
Authors: Liu S. , Wood-Vasey W. M. , Armstrong R. , Narayan G. , Sánchez B. O. ,   The Dark Energy Science Collaboration
Published: May 2024

Abstract
We evaluate the performance of the Legacy Survey of Space and Time Science Pipelines Difference Image Analysis (DIA) on simulated images. By adding synthetic sources to galaxies on images, we trace the recovery of injected synthetic sources to evaluate the pipeline on images from the Dark Energy Science Collaboration Data Challenge 2. The pipeline performs well, with efficiency and flux accuracy consistent with the signal-to-noise ratio of the input images. We explore different spatial degrees of freedom for the Alard–Lupton polynomial-Gaussian image subtraction kernel and analyze for trade-offs in efficiency versus artifact rate. Increasing the kernel spatial degrees of freedom reduces the artifact rate without loss of efficiency. The flux measurements with different kernel spatial degrees of freedom are consistent. We also here provide a set of DIA flags that substantially filter out artifacts from the DIA source table. We explore the morphology and possible origins of the observed remaining subtraction artifacts and suggest that given the complexity of these artifact origins, a convolution kernel with a set of flexible bases with spatial variation may be needed to yield further improvements.
Generation and Life Cycle of Solar Spicules
Authors: Saleem Hamid , Saleem Zain H. 
Published: May 2024

Abstract
The physical mechanism for the creation of solar spicules is proposed with three stages of their life cycle. It is assumed that at stage I the density hump is formed locally in the x-y plane in the lower chromosphere in the presence of temperature gradients of electrons and ions along the z-axis (the vertical direction). In this region, the density structure of quasi-neutral (n

i
≃ n

e
= n) plasma after taking birth is accelerated in the vertical direction owing to the thermal force F
th ∝ ∇n(x, y, t) × (∇T

e
+ ∇T

i
). The exact time-dependent analytical solution of two-fluid plasma equations is presented assuming that density is maximum at the center of the density structure and decays away from it gradually. The 2D density structure is created as a step function H(t) in time at the bottom of the chromosphere, and consequently, the vertical plasma velocity turns out to be the ramp function of time R(t) = tH(t), whereas the source term S(x, y, t) for the density follows the delta function δ(t) form. The upward acceleration

a
=
a

(
x
,
y

)

z

ˆ

produced in this density structure is greater than the downward constant solar acceleration −
g

⊙ in the chromosphere. In the transition region, the temperature gradients are steeper; therefore, the upward acceleration increases in magnitude g
⊙ ≪ a and the density hump spends less time there. This is stage II of its life cycle. In stage III, the density structure enters into the corona, where the gradients of temperatures vanish and the structure decelerates to zero velocity under the action of the solar gravitational force.
The First High-contrast Images of Near High-mass X-Ray Binaries with Keck/NIRC2
Authors: Prasow-Émond M. , Hlavacek-Larrondo J. , Fogarty K. , Artigau É. , Mawet D. , Gandhi P. , Steiner J. F. , Rameau J. , Lafrenière D. , Fabian A. , Walton D. J. , Doyon R. , Ren 任 B. B. 彬 
Published: May 2024

Abstract
Although the study of X-ray binaries has led to major breakthroughs in high-energy astrophysics, their circumbinary environment at scales of ∼100–10,000 au has not been thoroughly investigated. In this paper, we undertake a novel and exploratory study by employing direct and high-contrast imaging techniques on a sample of X-ray binaries, using adaptive optics and the vortex coronagraph on Keck/NIRC2. High-contrast imaging opens up the possibility to search for exoplanets, brown dwarfs, circumbinary companion stars, and protoplanetary disks in these extreme systems. Here we present the first near-infrared high-contrast images of 13 high-mass X-ray binaries located within ∼2–3 kpc. The key results of this campaign involve the discovery of several candidate circumbinary companions ranging from substellar (brown dwarf) to stellar masses. By conducting an analysis based on Galactic population models, we discriminate sources that are likely background/foreground stars and isolate those that have a high probability (≳60%–99%) of being gravitationally bound to the X-ray binary. This paper seeks to establish a preliminary catalog for future analyses of proper motion and subsequent observations. With our preliminary results, we calculate the first estimate of the companion frequency and the multiplicity frequency for X-ray binaries: ≈0.6 and 1.8 ± 0.9, respectively, considering only the sources that are most likely bound to the X-ray binary. In addition to extending our comprehension of how brown dwarfs and stars can form and survive in such extreme systems, our study opens a new window to our understanding of the formation of X-ray binaries.
Can Jupiter’s Atmospheric Metallicity Be Different from the Deep Interior?
Authors: Müller Simon , Helled Ravit 
Published: May 2024

Abstract
Updated formation and structure models of Jupiter predict a metal-poor envelope. This is at odds with the two to three times solar metallicity measured by the Galileo probe. Additionally, Juno data imply that water and ammonia are enriched. Here, we explore whether Jupiter could have a deep radiative layer separating the atmosphere from the deeper interior. The radiative layer could be caused by a hydrogen-transparency window or depletion of alkali metals. We show that heavy-element accretion during Jupiter’s evolution could lead to the desired atmospheric enrichment and that this configuration would be stable over billions of years. The origin of the heavy elements could be cumulative small impacts or one large impact. The preferred scenario requires a deep radiative zone, due to a local reduction of the opacity at ∼2000 K by ∼90%, which is supported by Juno data, and vertical mixing through the boundary with an efficiency similar to that of molecular diffusion (D ≲ 10−2 cm2 s−1). Therefore, most of Jupiter’s molecular envelope could have solar composition while its uppermost atmosphere is enriched with heavier elements. The enrichment likely originates from the accretion of solid objects. This possibility resolves the long-standing mismatch between Jupiter’s interior models and atmospheric composition measurements. Furthermore, our results imply that the measured atmospheric composition of exoplanets does not necessarily reflect their bulk compositions. We also investigate whether the enrichment could be due to the erosion of a dilute core and show that this is highly unlikely. The core-erosion scenario is inconsistent with evolution calculations, the deep radiative layer, and published interior models.
KFVM-WENO: A High-order Accurate Kernel-based Finite Volume Method for Compressible Hydrodynamics
Authors: May Ian C. T. , Lee Dongwook 
Published: May 2024

Abstract
This paper presents a fully multidimensional kernel-based reconstruction scheme for finite volume methods applied to systems of hyperbolic conservation laws, with a particular emphasis on the compressible Euler equations. Nonoscillatory reconstruction is achieved through an adaptive-order weighted essentially nonoscillatory (WENO) method cast into a form suited to multidimensional reconstruction. A kernel-based approach inspired by radial basis functions and Gaussian process modeling, which we call kernel-based finite volume method with WENO, is presented here. This approach allows the creation of a scheme of arbitrary order of accuracy with simply defined multidimensional stencils and substencils. Furthermore, the fully multidimensional nature of the reconstruction allows for a more straightforward extension to higher spatial dimensions and removes the need for complicated boundary conditions on intermediate quantities in modified dimension-by-dimension methods. In addition, a new simple yet effective set of reconstruction variables is introduced, which could be useful in existing schemes with little modification. The proposed scheme is applied to a suite of stringent and informative benchmark problems to demonstrate its efficacy and utility. A highly parallel multi-GPU implementation using Kokkos and the message-passing interface is also provided.
Insights into the Galactic Bulge Chemodynamical Properties from Gaia Data Release 3
Authors: Liao Xiaojie , Li Zhao-Yu , Simion Iulia , Shen Juntai , Grand Robert , Fragkoudi Francesca , Marinacci Federico 
Published: May 2024

Abstract
We explore the chemodynamical properties of the Galaxy in the azimuthal velocity V

ϕ
and metallicity [Fe/H] space using red giant stars from Gaia Data Release 3. The row-normalized V

ϕ
–[Fe/H] maps form a coherent sequence from the bulge to the outer disk, clearly revealing the thin/thick disk and the Splash. The metal-rich stars display bar-like kinematics, while the metal-poor stars show dispersion-dominated kinematics. The intermediate-metallicity population (−1 < [Fe/H]< − 0.4) can be separated into two populations, one that is bar-like, i.e., dynamically cold (

σ

V

R

∼
80

km s−1) and fast-rotating (V

ϕ
≳ 100 km s−1), and the Splash, which is dynamically hot (

σ

V

R

∼
110

km s−1) and slow-rotating (V

ϕ
≲ 100 km s−1). We compare the observations in the bulge region with an Auriga simulation where the last major merger event occurred ∼10 Gyr ago: only stars born around the time of the merger reveal a Splash-like feature in the V

ϕ
–[Fe/H] space, suggesting that the Splash is likely merger-induced, predominantly made up of heated disk stars and the starburst associated with the last major merger. Since the Splash formed from the proto-disk, its lower metallicity limit coincides with that of the thick disk. The bar formed later from the dynamically hot disk with [Fe/H] > − 1 dex, with the Splash not participating in the bar formation and growth. Moreover, with a set of isolated evolving N-body disk simulations, we confirm that a nonrotating classical bulge can be spun up by the bar and develop cylindrical rotation, consistent with the observations for the metal-poor stars.
Dynamical Properties of Magnetized Low-angular-momentum Accretion Flows around a Kerr Black Hole
Authors: Dihingia Indu K. , Mizuno Yosuke 
Published: May 2024

Abstract
An essential factor for determining the characteristics of an accretion flow is its angular momentum. According to the angular momentum of the flow, semi-analytical analysis suggests various types of accretion solutions. It is critical to test these with numerical simulations, using the most advanced framework available (general relativistic magnetohydrodynamics), to understand how the flow changes with different angular momentum. By changing the initial condition of the accretion torus minimally, we can simulate a steady, low-angular-momentum accretion flow around a Kerr black hole. We focus primarily on the lower limits of angular momentum and find that an accretion flow with an intermediate range of angular momentum differs significantly from high- or very-low-angular-momentum flows. The intermediate-angular-momentum accretion flow has the highest density, pressure, and temperature near the black hole, making it easier to observe. We find that the density and pressure have power-law scalings ρ ∝ r

n−3/2 and p

g
∝ r

n−5/2, which only hold for very-low-angular-momentum cases. With the increase in flow angular momentum, it develops a nonaxisymmetric nature. In this case, simple self-similarity does not hold. We also find that the sonic surface moves away from the innermost stable circular orbit as the angular momentum decreases. Finally, we emphasize that an intermediate-angular-momentum flow could provide a possible solution to explaining the complex observation features of the supermassive black hole Sgr A* at our galactic center.
Oscillating Dark Energy in Light of the Latest Observations and Its Impact on the Hubble Tension
Authors: Rezaei Mehdi 
Published: May 2024

Abstract
In this paper, we have performed a comparative study of different types of oscillating dark energy (DE) models using the Metropolis algorithm of Markov Chain Monte Carlo. Eight different oscillating parameterizations are examined herein that have demonstrated considerable ability to fit the overall cosmological observations, including the Pantheon sample of Type Ia supernovae, baryon acoustic oscillations, cosmic chronometer Hubble data, and distance priors of the Planck cosmic microwave background. In order to compare the consistency of these models with observations, we have used both the Akaike and deviance information criteria. Although the values of the Akaike information criterion for different models indicate that there is no support for oscillating DE models, the deviance information criterion showed that there is significant support for some of these models. Our results showed that these models are capable of solving the cosmic coincidence problem and alleviating the Hubble tension. Comparing the H
0 values obtained for different oscillating scenarios with that of ΛCDM, we observed that our oscillating models led to

H

0

¯

=
69.78

, which is 0.29 greater than H
0,Λ and thus reduces the Hubble tension. Among all of the models, model 1, with H
0 = 70.00 ± 0.71, is the most capable of alleviating the H
0 tension. Furthermore, we examined our models assuming H
0 = 73.0 ± 1.4 from SHoES measurements. We find that adding this data point to our data combination led to a

Δ

H

0

¯

=
0.95

increase in the H
0 value for different models.
Infall Motions in the Hot Core Associated with the Hypercompact H ii Region G345.0061+01.794 B
Authors: Komesh Toktarkhan , Garay Guido , Henkel Christian , Omar Aruzhan , Estalella Robert , Assembay Zhandos , Li Dalei , Guzmán Andrés , Esimbek Jarken , Huang Jiasheng , He Yuxin , Alimgazinova Nazgul , Kyzgarina Meiramgul , Bekdaulet Shukirgaliyev , Zhumabay Nurman , Manapbayeva Arailym 
Published: May 2024

Abstract
We report high angular resolution observations, made with the Atacama Large Millimeter Array in band 6, of high excitation molecular lines of

CH

3

CN

and SO2 and of the H29α radio recombination line toward the G345.0061+01.794 B HC H ii region in order to investigate the physical and kinematical characteristics of its surroundings. Emission was detected in all observed components of the J = 14 →13 rotational ladder of

CH

3

CN

and in the 304,26–303,27, and 324,28–323,29 lines of SO2. The peak of the velocity-integrated molecular emission is located ∼0.″4 northwest of the peak of the continuum emission. The first-order moment images and channel maps show a velocity gradient of 1.1 km s−1 arcsec−1 across the source and a distinctive spot of blueshifted emission toward the peak of the zero-order moment. The rotational temperature is found to decrease from 252±24 K at the peak position to 166±16 K at its edge, indicating that our molecular observations are probing a hot molecular core that is internally excited. The emission in the H29α line arises from a region of 0.″65 in size, where its peak coincides with that of the dust continuum. We model the kinematical characteristics of the “central blue spot” feature as due to infalling motions, suggesting a central mass of 172.8±8.8 M
⊙. Our observations indicate that this HC H ii region is surrounded by a compact structure of hot molecular gas, which is rotating and infalling toward a central mass, that is most likely confining the ionized region. The observed scenario is reminiscent of a “butterfly pattern” with an approximately edge-on torus and ionized gas roughly parallel to its rotation axis.
A Deep Redshift Survey of the Perseus Cluster (A426): Spatial Distribution and Kinematics of Galaxies
Authors: Kang Wooseok , Hwang Ho Seong , Song Hyunmi , Park Changbom , Hwang Narae , Park Byeong-Gon 
Published: May 2024

Abstract
We study the global kinematics of the Perseus galaxy cluster (A426) at redshift z = 0.017 using a large sample of galaxies from our new MMT/Hectospec spectroscopic observation for this cluster. The sample includes 1447 galaxies with measured redshifts within 60′ from the cluster center (1148 from this MMT/Hectospec program and 299 from the literature). The resulting spectroscopic completeness is 67% at r-band apparent magnitude r
Petro,0 ≤ 18.0 within 60′ from the cluster center. To identify cluster member galaxies in this sample, we develop a new open-source Python package, CausticSNUpy. This code implements the algorithm of the caustic technique and yields 418 member galaxies within 60′ of the cluster. We study the cluster using this sample of member galaxies. The cluster shows no significant signal of global rotation. A statistical test shows that the cluster does not have a noticeable substructure within 30′. We find two central regions where the X-ray-emitting intracluster medium and galaxies show significant velocity differences (>7σ). On a large scale, however, the overall morphology and kinematics between the intracluster medium and galaxies agree well. Our results suggest that the Perseus cluster is a relaxed system and has not experienced a recent merger.
A Targeted Deep Sequencing Method to Quantify Endogenous Retrovirus Gag Sequence Variants and Open Reading Frames Expressed in Nonobese Diabetic Mice
Authors: Dai Yang D , Du Wenge , Wang Yaqin , Hu Wen-Yuan 
Published: May 2024

Abstract
Endogenous retroviruses (ERVs) are involved in autoimmune diseases such as type 1 diabetes (T1D). ERV gene products homologous to murine leukemia retroviruses are expressed in the pancreatic islets of NOD mice, a model of T1D. One ERV gene, Gag, with partial or complete open reading frames (ORFs), is detected in the islets, and it contains many sequence variants. An amplicon deep sequencing analysis was established by targeting a conserved region within the Gag gene to compare NOD with T1D-resistant mice or different ages of prediabetic NOD mice. We observed that the numbers of different Gag variants and ORFs are linked to T1D susceptibility. More importantly, these numbers change during the course of diabetes development and can be quantified to calculate the levels of disease progression. Sequence alignment analysis led to identification of additional markers, including nucleotide mismatching and amino acid consensus at specific positions that can distinguish the early and late stages, before diabetes onset. Therefore, the expression of sequence variants and ORFs of ERV genes, particularly Gag, can be quantified as biomarkers to estimate T1D susceptibility and disease progression.
Malignant Abrikossoff’s Tumour of the Tonsil - A Case Report of a Rare Entity
Authors: Molinari Giulia , Marrè Pietro , Fernandez Ignacio Javier , Presutti Livio , Pirini Maria Giulia , Botti Cecilia , Filippini Daria Maria 
Published: May 2024

Abstract

Rationale:
This study aimed to report an uncommon site of origin of a rare head-and-neck cancer, namely malignant granular cell tumour.

Patient Concerns:
An 89-year-old female patient complained of persistent pharyngodynia and odynophagia for two months.

Diagnosis:
Upon clinical examination, the right palatine tonsil was larger and palpably firmer than the contralateral. An incisional biopsy of the lesion was performed under local anaesthesia revealing malignant granular cell tumour. A contrast-enhanced computed tomography (CECT) scan of the head and neck and an 18F-fluoro-2-deoxy-D-glucose positron emission tomography (PET) scan confirmed the presence of a pathologic appearance of the right palatine tonsil without nodal or distant metastasis.

Treatment:
Following a multidisciplinary consultation and the patient’s informed permission, a right tonsillectomy extended to the constrictor muscle fibres of the upper pharynx was performed.

Outcomes:
The tumour was staged as pT2 R0 cN0 M0, according to the AJCC 8th edition for soft-tissue tumours of the head and neck. Due to the early stage and the radicality of surgery, no further adjuvant treatments were provided. The patient is currently followed up with no evidence of disease one year post-operatively.

Take-away Lessons:
Granular cell tumours are rare mesenchymal tumours, firstly described by the pathologist Abrikossoff in 1926. This type of tumour constitutes approximately 0.5% of all soft-tissue tumours, and can affect any part of the body, with the head and neck being the most frequently involved site. The tonsil is an extremely rare localisation of this cancer. The differential diagnosis of unilateral tonsillar enlargement should also include this histological entity.
Pasteurella multocida: An Uncommon Cause of Infective Endocarditis Affecting a Homograft Conduit in a Child
Authors: Ayoub Touseef Ul , Marwah Ashutosh , Iyer Parvathi U. , Iyer Krishna S. , Agarwal Anuradha 
Published: May 2024

Background:
Disseminated septicemia and endocarditis are extremely rare complications of Pasteurella infection and are mainly seen in patients with associated major comorbidities.

Clinical Description:
A 13-year-old boy, who had undergone surgery for congenital heart disease in early childhood, presented with prolonged fever, gross hematuria, and oliguria. The child was found to be conscious and febrile, with tachycardia, pallor, and edema. There was a systolic murmur in the left upper sternal border with hepatosplenomegaly.

Management and Outcome:
Routine investigations revealed anemia, low serum albumin, and progressively worsening renal functions, with urinalysis showing significant proteinuria and red cells. Serial blood cultures showed growth of Pasteurella multocida. Echocardiography showed vegetation in conduit (homograft) connecting the right ventricle with the pulmonary artery. Despite intravenous antibiotics, the clinical condition did not improve, so the conduit was removed surgically, following which the child recovered.

Conclusion:
This case creates awareness regarding infective endocarditis in a child being caused by a rare organism P. multocida, involving a surgically created conduit. The case also highlights the importance of timely surgical removal of the source combined with a prolonged course of antibiotics in a successful recovery.
Divergent Phenotypes with Same CHRNE Mutation in Two Siblings with Congenital Myasthenic Syndrome
Authors: Naveen Ankith , Pujar Madhu S , Revankar Ranjitha , Rotti Shreya 
Published: May 2024

Background:
Congenital myasthenic syndrome is a rare inherited neuromuscular disorder resulting in abnormal weakness and fatigue on exertion with onset at or shortly after birth or in early childhood.

Clinical Description:
A 2-year-old boy presented to us with respiratory failure, having a history of recurrent respiratory tract infections and underlying isolated motor delay. His 7-year-old elder sister had undiagnosed generalized weakness.

Management and Outcome:
While the index case was being stabilized with mechanical ventilation, his elder sibling was evaluated. Ptosis was noted in her, which improved with neostigmine. Examination and laboratory investigations ruled out other differentials. Clinical exome sequencing was sent which showed homozygous CHRNE ENST00000649488.2.c.1367_1369del. (p.Asn456del) resulting in acetylcholine receptor deficiency. Both siblings were started on oral pyridostigmine and salbutamol, resulting in improvement in muscle weakness over 3 months and 4 months in younger and older sibling, respectively.

Conclusion:
Recurrent respiratory insufficiency when associated with motor delay may be suggestive of a neuromuscular disorder. Even siblings with the same mutation may have different levels of severity of clinical manifestation.