bluuebunny/crossref_metadata_2025_split huggingface dataset:
Planning Target Volume Margin Assessment of Retroperitoneal Tumors Using Robotic SBRT With Spine Tracking
Authors: McKenzie Grant , Kassel Maxwell , Bonifaz Andres Portocarrero , Willett Andrew , Swanson Christine , James Joshua , Dunlap Neal 
Published: August 2024

Abstract

Objective:
Stereotactic body radiation therapy (SBRT) treatment is an emerging salvage modality for treating oligometastatic malignant lesions within the retroperitoneum. Appropriate planning target volume (PTV) margins are essential when delivering SBRT to effectively cover the target volume. Spine tracking uses bony spinal anatomy for localization during treatment delivery on robotic linear accelerator platforms. The aim of this study is to quantify the PTV margin needed when spine tracking is used for intrafraction motion tracking when treating retroperitoneal metastatic lesions with robotic SBRT.

Materials and Methods:
A single-institution chart review identified 16 patients with retroperitoneal tumors treated with SBRT over 19 courses in 103 fractions. Daily cone-beam CT images registered based on tumor positioning at the time of treatment were analyzed. Van Herk’s margin recipe was used to calculate the additional PTV margin required if spine tracking was used instead of daily tumor imaging. Patients’ tumors were stratified based on PTV proximity to the vertebral column (≤ 1 cm vs > 1 cm) and location within the retroperitoneum (superior vs inferior to renal artery), with descriptive statistics used to compare the differences of shifts based on location.

Results:
The additional margins calculated by Van Herk’s margin recipe to adequately cover the PTV within the 95% isodose surface for 90% of the entire patient cohort in the vertical, longitudinal, and lateral directions were 2.7, 2.8, and 2.8 mm, respectively. When tumors were stratified by proximity to the vertebral column, average longitudinal (P < .001) and total shifts (P < .001) were statistically significant.

Conclusion:
When treating retroperitoneal tumors with robotic SBRT, a minimum isometric margin expansion of 5 mm when creating the PTV is recommended if spine tracking is used for intrafraction motion assessment. Target volumes adjacent to the vertebral column may have PTV margins decreased to 4 mm without compromise in target coverage.
Peran Pemuda dalam Membangun Moralitas Keagamaan di Masyarakat
Authors: Utomo Galih Priyo , Witasari Rinesti 
Published: August 2024

Youth is part of the community which the community itself is expected to play a role in providing useful participation for the progress of society. Religious morality is an important thing to be built in the midst of society because religious morality leads people to actions that are in accordance with the good values of religious teachings. This research uses a qualitative case study approach. The techniques used in data collection are observation, interviews and documentation. The data analysis technique used is the concept of Miles & Huberman that the data is analyzed with theories that are relevant to the discussion. The objects used as informants in the study were five youths and one religious leader in the neighborhood of Rt 002, Rw 001, Kambangrejo Hamlet, Bedingin Village, Sambit District, Ponorogo Regency. The purpose of this study was to determine the role of youth in building religious morality in the community in that environment. The results of the study show that the youth of Rt 002, Rw 001, Dukuh Kambangrejo have a role in building religious morality in the community including participating in religious activities in the community such as yasinan, tahlilan, recitation, prospering mosques, being an example in cohesiveness, harmony, order, being a driving force for the community to creative, active in Ramadan activities such as tarawih prayers, tadarus quran, takbiran, and during Eid al-Adha, as well as maintaining environmental security.
Submillimeter and Mid-Infrared Variability of Young Stellar Objects in the M17SWex Intermediate-mass Star-forming Region
Authors: Park Geumsook , Johnstone Doug , Peña Carlos Contreras , Lee Jeong-Eun , Liu Sheng-Yuan , Herczeg Gregory , Mairs Steve , Chen Zhiwei , Hatchell Jennifer , Kim Kee-Tae , Kim Mi-Ryang , Qiu Keping , Wang Yao-Te , Zhang Xu ,   The JCMT Transient Team
Published: August 2024

Abstract
We present a comprehensive analysis of young stellar object (YSO) variability within the M17 Southwest Extension (M17 SWex), using 3.5 yr of monitoring data from the James Clerk Maxwell Telescope (JCMT) Transient Survey at submillimeter and 9 yr from the NEOWISE mission at mid-infrared (mid-IR). Our study encompasses observations of 147 bright submillimeter peaks identified within our deep JCMT coadded map as well as 156 YSOs in NEOWISE W1 and 179 in W2 that were previously identified in Spitzer surveys. We find three robust submillimeter variables: two are candidate YSOs and one is a likely extragalactic source. At mid-IR wavelengths, our analysis reveals secular and stochastic variability in 47 YSOs, with the highest fraction of secular variability occurring at the earliest evolutionary stage. This is similar to what has previously been observed for low-mass YSO variability within the Gould Belt. However, we observe less overall variability in M17 SWex at both the submillimeter and mid-IR. We suspect that this lower fraction is due to the greater distance to M17 SWex. Our findings showcase the utility of multiwavelength observations to better capture the complex variability phenomena inherent to star formation processes and demonstrate the importance of years-long monitoring of a diverse selection of star-forming environments.
TeV Analysis of a Source-rich Region with the HAWC Observatory: Is HESS J1809-193 a Potential Hadronic PeVatron?
Authors: Albert A. , Alfaro R. , Alvarez C. , Arteaga-Velázquez J. C. , Avila Rojas D. , Babu R. , Belmont-Moreno E. , Bernal A. , Breuhaus M. , Caballero-Mora K. S. , Capistrán T. , Carramiñana A. , Casanova S. , Cotzomi J. , De la Fuente E. , Depaoli D. , Di Lalla N. , Diaz Hernandez R. , Dingus B. L. , DuVernois M. A. , Espinoza C. , Fan K. L. , Fang K. , Fick B. , Fraija N. , García-González J. A. , Garfias F. , Gonzalez Muñoz A. , González M. M. , Goodman J. A. , Groetsch S. , Harding J. P. , Hernández-Cadena S. , Herzog I. , Huang D. , Hueyotl-Zahuantitla F. , Hüntemeyer P. , Iriarte A. , Joshi V. , Kaufmann S. , Lara A. , Lee J. , León Vargas H. , Longinotti A. L. , Luis-Raya G. , Malone K. , Martínez-Castro J. , Matthews J. A. , Miranda-Romagnoli P. , Montes J. A. , Morales-Soto J. A. , Moreno E. , Mostafá M. , Nellen L. , Newbold M. , Nisa M. U. , Noriega-Papaqui R. , Osorio M. , Pérez Araujo Y. , Pérez-Pérez E. G. , Rho C. D. , Rosa-González D. , Ruiz-Velasco E. , Salazar H. , Sandoval A. , Schneider M. , Serna-Franco J. , Smith A. J. , Son Y. , Springer R. W. , Tibolla O. , Tollefson K. , Torres I. , Torres-Escobedo R. , Turner R. , Ureña-Mena F. , Varela E. , Wang X. , Watson I. J. , Willox E. , Yun-Cárcamo S. , Zhou H. ,   THE HAWC COLLABORATION
Published: August 2024

Abstract
HESS J1809-193 is an unidentified TeV source, first detected by the High Energy Stereoscopic System (H.E.S.S.) collaboration. The emission originates in a source-rich region that includes several supernova remnants (SNRs) and pulsars including SNR G11.1+0.1, SNR G11.0-0.0, and the young radio pulsar PSR J1809-1917. Originally classified as a pulsar wind nebula candidate, recent studies show the peak of the TeV region overlapping with a system of molecular clouds. This resulted in the revision of the original leptonic scenario to look for alternate hadronic scenarios. Marked as a potential PeVatron candidate, this region has been studied extensively by H.E.S.S. due to its emission extending up to several tens of TeV. In this work, we use 2398 days of data from the High Altitude Water Cherenkov (HAWC) observatory to carry out a systematic source search of the HESS J1809-193 region. We were able to resolve emission detected as an extended component (modelled as a symmetric Gaussian with a 1σ radius of 0.°21) with no clear cutoff at high energies and emitting photons up to 210 TeV. We model the multiwavelength observations for the region around HESS J1809-193 using a time-dependent leptonic model and a lepto-hadronic model. Our model indicates that both scenarios could explain the observed data within the region of HESS J1809-193.
Why Are (Almost) All the Protostellar Outflows Aligned in Serpens Main?
Authors: Green Joel D. , Pontoppidan Klaus M. , Reiter Megan , Watson Dan M. , Shenoy Sachindev S. , Manoj P. , Narang Mayank 
Published: August 2024

Abstract
We present deep 1.4–4.8 μm JWST-NIRCam imaging of the Serpens Main star-forming region and identify 20 candidate protostellar outflows, most with bipolar structure and identified driving sources. The outflow position angles (PAs) are strongly correlated, and they are aligned within ±24° of the major axis of the Serpens filament. These orientations are further aligned with the angular momentum vectors of the two disk shadows in this region. We estimate that the probability of this number of young stars being coaligned if sampled from a uniform PA distribution is 10−4. This in turn suggests that the aligned protostars, which seem to be at similar evolutionary stages based on their outflow dynamics, formed at similar times with a similar spin inherited from a local cloud filament. Further, there is tentative evidence for a systematic change in average PA between the northwestern and southeastern cluster, as well as increased scatter in the PAs of the southeastern protostars. SOFIA-HAWC+ archival dust polarization observations of Serpens Main at 154 and 214 μm are perpendicular to the dominant jet orientation in the northwestern region in particular. We measure and locate shock knots and edges for all of the outflows and provide an identifying catalog. We suggest that Serpens main is a cluster that formed from an isolated filament and due to its youth retains its primordial outflow alignment.
Accretion Geometry of GX 339–4 in the Hard State: AstroSat View
Authors: Chand Swadesh , Dewangan Gulab C. , Zdziarski Andrzej A. , Bhattacharya Dipankar , Mithun N. P. S. , Vadawale Santosh V. 
Published: August 2024

Abstract
We perform broadband (0.7–100 keV) spectral analysis of five hard state observations of the low-mass black hole X-ray binary GX 339–4 taken by AstroSat during the rising phase of three outbursts from 2019 to 2022. We find that the outburst in 2021 was the only successful/full outburst, while the source was unable to make the transition to the soft state during the other two outbursts in 2019 and 2022. Our spectral analysis employs two different model combinations, requiring two separate Comptonizing regions and their associated reflection components and soft X-ray excess emission. The harder Comptonizing component dominates the overall bolometric luminosity, while the softer one remains relatively weak. Our spectral fits indicate that the disk evolves with the source luminosity, where the inner disk radius decreases with increasing luminosity. However, the disk remains substantially truncated throughout all the observations at the source luminosity of ∼2%–8%× of the Eddington luminosity. We note that our assumption of the soft X-ray excess emission as disk blackbody may not be realistic, and this kind of soft excess may arise due the nonhomogeneity in the disk/corona geometry. Our temporal analysis deriving the power density spectra suggests that the break frequency increases with the source luminosity. Furthermore, our analysis demonstrates a consistency between the inner disk radii estimated from the break frequency of the power density spectra and those obtained from the reflection modeling, supporting the truncated disk geometry in the hard state.
High-redshift Merger Model for Low-frequency Gravitational Wave Background
Authors: Wu Zhao-Feng , Giannios Dimitrios 
Published: August 2024

Abstract
In 2023, the Pulsar Timing Array Collaborations announced the discovery of a gravitational wave background (GWB), predominantly attributed to supermassive black hole binary (SMBHB) mergers. However, the detected GWB is several times stronger than the default value expected from galactic observations at low and moderate redshifts. Recent findings by the James Webb Space Telescope have unveiled a substantial number of massive, high-redshift galaxies, suggesting more massive SMBHB mergers at these early epochs. Motivated by these findings, we propose an “early merger” model that complements the standard merger statistics by incorporating these early, massive galaxies. We compare the early and standard “late merger” models, which assume peak merger rates in the local Universe, and match both merger models to the currently detected GWB. Our analysis shows that the early merger model has a significantly lower detection probability for single binaries and predicts a ∼30% likelihood that the first detectable single source will be highly redshifted and remarkably massive with rapid frequency evolution. In contrast, the late merger model predicts a nearly monochromatic first source at low redshift. The future confirmation of an enhanced population of massive high-redshift galaxies and the detection of fast-evolving binaries would strongly support the early merger model, offering significant insights into the evolution of galaxies and SMBHs.
Constraining Cosmological Parameters Using the Splashback Radius of Galaxy Clusters
Authors: Haggar Roan , Amoura Yuba , Mpetha Charlie T. , Taylor James E. , Walker Kris , Power Chris 
Published: August 2024

Abstract
Cosmological parameters such as ΩM and σ
8 can be measured indirectly using various methods, including galaxy cluster abundance and cosmic shear. These measurements constrain the composite parameter S
8, leading to degeneracy between ΩM and σ
8. However, some structural properties of galaxy clusters also correlate with cosmological parameters, due to their dependence on a cluster’s accretion history. In this work, we focus on the splashback radius, an observable cluster feature that represents a boundary between a cluster and the surrounding Universe. Using a suite of cosmological simulations with a range of values for ΩM and σ
8, we show that the position of the splashback radius around cluster-mass halos is greater in cosmologies with smaller values of ΩM or larger values of σ
8. This variation breaks the degeneracy between ΩM and σ
8 that comes from measurements of the S
8 parameter. We also show that this variation is, in principle, measurable in observations. As the splashback radius can be determined from the same weak lensing analysis already used to estimate S
8, this new approach can tighten low-redshift constraints on cosmological parameters, either using existing data, or using upcoming data such as that from Euclid and LSST.
Reconstruction of the Dark Energy Scalar Field Potential by Gaussian Process
Authors: Niu 牛 Jing 菁 , Jiao 焦 Kang 康 , He 贺 Peng 鹏 , Zhang 张 Tong-Jie 同杰 
Published: August 2024

Abstract
Dark energy is believed to be responsible for the acceleration of the Universe. In this paper, we reconstruct the dark energy scalar field potential V(ϕ) using the Hubble parameter H(z) through Gaussian process analysis. Our goal is to investigate dark energy using various H(z) data sets and priors. We find that the selection of the prior and the H(z) data set significantly affects the reconstructed V(ϕ). We compare two models, Power Law and Free Field, to the reconstructed V(ϕ) by computing the reduced chi-square. The results suggest that the models are generally in agreement with the reconstructed potential within a 3σ confidence interval, except in the case of Observational H(z) data with the Planck 18 prior. Additionally, we simulate H(z) data to measure the effect of increasing the number of data points on the accuracy of reconstructed V(ϕ). We find that doubling the number of H(z) data points can improve the accuracy rate of reconstructed V(ϕ) by 5%–30%.
X-Ray Winds in Nearby-to-distant Galaxies (X-WING). I. Legacy Surveys of Galaxies with Ultrafast Outflows and Warm Absorbers in z ∼ 0–4
Authors: Yamada Satoshi , Kawamuro Taiki , Mizumoto Misaki , Ricci Claudio , Ogawa Shoji , Noda Hirofumi , Ueda Yoshihiro , Enoto Teruaki , Kokubo Mitsuru , Minezaki Takeo , Sameshima Hiroaki , Horiuchi Takashi , Mizukoshi Shoichiro 
Published: August 2024

Abstract
As an inaugural investigation under the X-ray Winds In Nearby-to-distant Galaxies (X-WING) program, we assembled a data set comprising 132 active galactic nuclei (AGNs) spanning redshifts z ∼ 0–4 characterized by blueshifted absorption lines indicative of X-ray winds. Through an exhaustive review of previous research, we compiled the outflow parameters for 583 X-ray winds, encompassing key attributes such as outflow velocities (V
out), ionization parameters (ξ), and hydrogen column densities. By leveraging the parameters V
out and ξ, we systematically categorized the winds into three distinct groups: ultrafast outflows (UFOs), low-ionization parameter (low-IP) UFOs, and warm absorbers (WAs). Strikingly, a discernible absence of linear correlations in the outflow parameters, coupled with distributions approaching instrumental detection limits, was observed. Another notable finding was the identification of a velocity gap around V
out ∼ 10,000 km s−1. This gap was particularly evident in the winds detected via absorption lines within the ≲2 keV band, indicating disparate origins for low-IP UFOs and WAs. In cases involving Fe xxv/Fe xxvi lines, where the gap might be attributed to potential confusion between emission/absorption lines and the Fe K-edge, the possibility of UFOs and galactic-scale WAs being disconnected is considered. An examination of the outflow and dust sublimation radii revealed a distinction: UFOs appear to consist of dust-free material, whereas WAs likely comprise dusty gas. From 2024, the X-Ray Imaging and Spectroscopy Mission is poised to alleviate observational biases, providing insights into the authenticity of the identified gap, a pivotal question in comprehending AGN feedback from UFOs.
First Direct Evidence for Keplerian Rotation in Quasar Inner Broad-line Regions
Authors: Fian C. , Jiménez-Vicente J. , Mediavilla E. , Muñoz J. A. , Chelouche D. , Kaspi S. , Forés-Toribio R. 
Published: August 2024

Abstract
We introduce a novel method to derive rotation curves with light-day spatial resolution of the inner regions of lensed quasars. We aim to probe the kinematics of the inner part of the broad-line region by resolving the microlensing response—a proxy for the size of the emitting region—in the wings of the broad emission lines. Specifically, we assess the strength of the microlensing effects in the wings of the high-ionization lines Si iv and C iv across various velocity bins in five gravitationally lensed quasars: SDSS J1001+5027, SDSS J1004+4112, HE 1104−1805, SDSS J1206+4332, and SDSS J1339+1310. Using Bayesian methods to estimate the dimensions of the corresponding emission regions and adopting a Keplerian model as our baseline, we examine the consistency of the hypothesis of disklike rotation. Our results reveal a monotonic, smooth increase in microlensing magnification with velocity. The deduced velocity–size relationships inferred for the various quasars and emission lines closely conform to the Keplerian model of an inclined disk. This study provides the first direct evidence of Keplerian rotation in the innermost region of quasars across a range of radial distances spanning from ∼5 to 20 lt-days.
In LIGO’s Sight? Vigorous Coherent Gravitational Waves from Cooled Collapsar Disks
Authors: Gottlieb Ore , Levinson Amir , Levin Yuri 
Published: August 2024

Abstract
We present the first numerical study of gravitational waves (GWs) from collapsar disks, using state-of-the-art 3D general relativistic magnetohydrodynamic simulations of collapsing stars. These simulations incorporate a fixed Kerr metric for the central black hole (BH) and employ simplified prescriptions for disk cooling. We find that cooled disks with an expected scale height ratio of H/R ≳ 0.1 at ∼10 gravitational radii induce Rossby instability in compact, high-density rings. The trapped Rossby vortices generate vigorous coherent emission regardless of disk magnetization and BH spin. For BH mass of ∼10 M
⊙, the GW spectrum peaks at ∼100 Hz, with some breadth due to various nonaxisymmetric modes. The spectrum shifts toward lower frequencies as the disk viscously spreads and the circularization radius of the infalling gas increases. Weaker-cooled disks with H/R ≳ 0.3 form a low-density extended structure of spiral arms, resulting in a broader, lower-amplitude spectrum. Assuming an optimistic detection threshold with a matched-filter signal-to-noise ratio of 20 and a rate similar to Type Ib/c supernovae, LIGO–Virgo–KAGRA (LVK) could detect ≲1 event annually, suggesting that GW events may already be hidden in observed data. Third-generation GW detectors could detect dozens to hundreds of collapsar disks annually, depending on the cooling strength and the disk formation rate. The GW amplitudes from collapsar disks are ≳100 times higher with a substantially greater event rate than those from core-collapse supernovae, making them potentially the most promising burst-type GW class for LVK and Cosmic Explorer. This highlights the importance of further exploration and modeling of disk-powered GWs, promising insights into collapsing star physics.
Very Long-periodic Pulsations Detected Simultaneously in a White-light Flare and Sunspot Penumbra
Authors: Li Dong , Wang Jincheng , Huang Yu 
Published: August 2024

Abstract
We investigate the origin of very long-periodic pulsations in the white-light emission of an X6.4 flare on 2024 February 22 (SOL2024-02-22T22:08), which occurred at the edge of a sunspot group. The flare white-light fluxes reveal four successive and repetitive pulsations, which are simultaneously measured by the Helioseismic and Magnetic Imager and the White-light Solar Telescope. A quasi-period of

8.6

−
1.9

+
1.5

minutes, determined by the Morlet wavelet transform, is detected in the visible continuum channel. The modulation depth, which is defined as the ratio between the oscillatory amplitude and its long-term trend, is smaller than 0.1%, implying that the quasi-periodic pulsation (QPP) feature is a weak wave process. Imaging observations show that the X6.4 flare occurs near a sunspot group. Moreover, the white-light brightening is located in sunspot penumbra, and a similar quasi-period of about 8.5

−
1.8

+
1.6

minutes is identified in one penumbral location of the nearest sunspot. The map of Fourier power distribution suggests that a similar periodicity is universally existing in most parts of the penumbra that is close to the penumbral–photospheric boundary. Our observations support the scenario that the white-light QPP is probably modulated by the slow-mode magnetoacoustic gravity wave leaking from the sunspot penumbra.