bluuebunny/crossref_metadata_2025_split huggingface dataset:
Ebediyete Bağış: Balat Şer‘iyye Sicillerinde Para Vakfı Kayıtları (1555-1838)
Authors: Gürsoy Çiğdem , Özdeğer Mehtap 
Published: August 2022

Vakıf medeniyeti olarak da bilinen Osmanlı’da vakıf kurumu eğitimden sağlığa, kültürel hizmetlerden beledi hizmetlere kadar hayatın her alanında çeşitli katkılar sağlamıştır. Kurumun yaygınlığı ve kapsayıcılığı günümüze ulaşan çok sayıda vakfiye içeriğinden tespit edilmektedir. Vakfiyelerde vakfın ciheti doğrultusunda ne tür hizmetler verildiği ayrıntılarıyla kayıtlıdır. Ayrıca, kişilerin mal varlıkları, mimari eserler, kamu görevlileri, hukuki işlemler, mahalleler, aile üyeleri hakkında bilgiler gibi pek çok konu işlenmiştir. Para vakıflarına ait vakfiyelerde ise bahsi geçen konulara ilaveten vakfedilen nakitler, işletim usulleri, nema oranları, elde edilecek gelirlerin kullanımına ait detaylar da söz konusudur. Çalışmanın amacı para vakıflarının işleyiş prensiplerini ortaya koymak ve para vakıflarının sosyoekonomik yönden Osmanlı toplum yaşantısına katkılarını araştırmaktır.
Örneklem alanı olarak, erken dönemlerden itibaren para vakfı vakfiyelerinin bulunduğu İstanbul Balat Şer’iyye Sicilleri alınmıştır. Çalışma 1555-1838 arasında kayıtlı toplam 55 vakfiye üzerinden gerçekleştirilmiştir. Bulguların karşılaştırılması için üç farklı mahkeme kayıtlarında tespit edip incelediğimiz 1491-1911 arasında kurulmuş 426 para vakfı vakfiyesine başvurulmuştur. Bu sayede, vakfiye sayısı ve ait oldukları dönemler itibariyle, şimdiye kadar eksik kalan toplu değerlendirme imkânı yakalanmıştır. Neticede para vakıflarının hizmetlerine devam edebilmek için değişen sosyoekonomik şartlara uyum sağlamak adına ne gibi çabalar harcadığına dair önemli tespitler yapılmıştır. Bu kapsamda para vakıflarının bir yandan kendi içinde geçirdiği değişim ve dönüşümler tespit edilirken diğer yandan bir bütünün parçası olarak vakıfların ebediyete yaptıkları bağışlar örneklenmiştir.
Fear of Cancer Recurrence in Women with Breast Cancer: A Cross-Sectional Study after Mastectomy
Authors: ZORBA BAHÇELİ Pınar , YAZICIOĞLU KÜÇÜK Banu 
Published: August 2022

Aim: The aim of this study was to determine the fear of cancer recurrence in women with breast cancer after mastectomy.
Material and Methods: Data were collected between March and September 2021 with the Personal Information Form and the Fear of Cancer Recurrence Inventory via social media. The sample consisted of 127 women with breast cancer, who were registered in the general surgery service of a training and research hospital in Turkey, could be reached by phone and had a social media account. Descriptive statistics, independent groups t test, One-Way ANOVA and Mann-Whitney U test analysis were used in the analysis of the data.
Results: It was determined that the Fear of Cancer Recurrence Inventory mean score was 126.12±24.88 and the coping strategies sub-dimension mean score was 30.96±6.00. It was determined that there was a significant difference between the mean score of the Fear of Cancer Recurrence Inventory and the duration of diagnosis, the status of receiving radiotherapy and chemotherapy, the status of experiencing treatment-related side effects, and the status of doing any sports/exercise (p
Chemical Abundances of Young Massive Clusters in NGC 1313∗
Authors: Hernandez Svea , Winch Autumn , Larsen Søren , James Bethan L. , Jones Logan 
Published: August 2022

Abstract
We analyze spectroscopic observations of five young massive clusters (YMCs) in the barred spiral galaxy NGC 1313 to obtain detailed abundances from their integrated light. Our sample of YMCs was observed with the X-shooter spectrograph on the Very Large Telescope. We make use of theoretical isochrones to generate synthetic integrated-light spectra, iterating on the individual elemental abundances until converging on the best fit to the observations. We measure abundance ratios for [Ca/Fe], [Ti/Fe], [Mg/Fe], [Cr/Fe], and [Ni/Fe]. We estimate an Fe abundance gradient of −0.124 ± 0.034 dex kpc−1, and a slightly shallower α gradient of −0.093 ± 0.009 dex kpc−1. This is in contrast to previous metallicity studies that focused on the gas-phase abundances, which have found NGC 1313 to be the highest-mass barred galaxy known not to have a radial abundance gradient. We propose that the gradient discrepancy between the different studies originates from the metallicity calibrations used to study the gas-phase abundances. We also observe an age–metallicity trend that supports a scenario of constant star formation throughout the galaxy, with a possible burst in star formation in the southwest region where YMC NGC 1313–379 is located.
Improving Astronomical Time-series Classification via Data Augmentation with Generative Adversarial Networks
Authors: García-Jara Germán , Protopapas Pavlos , Estévez Pablo A. 
Published: August 2022

Abstract
Due to the latest advances in technology, telescopes with significant sky coverage will produce millions of astronomical alerts per night that must be classified both rapidly and automatically. Currently, classification consists of supervised machine-learning algorithms whose performance is limited by the number of existing annotations of astronomical objects and their highly imbalanced class distributions. In this work, we propose a data augmentation methodology based on generative adversarial networks (GANs) to generate a variety of synthetic light curves from variable stars. Our novel contributions, consisting of a resampling technique and an evaluation metric, can assess the quality of generative models in unbalanced data sets and identify GAN-overfitting cases that the Fréchet inception distance does not reveal. We applied our proposed model to two data sets taken from the Catalina and Zwicky Transient Facility surveys. The classification accuracy of variable stars is improved significantly when training with synthetic data and testing with real data with respect to the case of using only real data.
Distances to Local Group Galaxies via Population II, Stellar Distance Indicators. I. The Sculptor Dwarf Spheroidal*
Authors: Tran Quang H. , Hoyt Taylor J. , Freedman Wendy L. , Madore Barry F. , Oakes Elias K. , Cerny William , Hatt Dylan , Beaton Rachael L. 
Published: August 2022

Abstract
We determine the distance to the Sculptor Dwarf Spheroidal via three Population II stellar distance indicators: (a) the Tip of the Red Giant Branch (TRGB), (b) RR Lyrae variables (RRLs), and (c) the ridgeline of the blue horizontal branch (HB). High signal-to-noise, wide-field VI imaging that covers an area

48
′

×

48
′

and reaches a photometric depth approximately 2 mag fainter than the HB was acquired with the Magellan-Baade 6.5 m telescope. The true modulus derived from Sculptor’s TRGB is found to be

μ

o

TRGB

=
19.59

±

0.07

stat

±

0.05

sys

mag. Along with periods adopted from the literature, newly acquired RRL phase points are fit with template light curves to determine

μ

W

I
,
V
−
I

RRL

=
19.60
±

0.01

stat

±

0.05

sys

mag. Finally, the HB distance is found to be

μ

o

HB

=
19.54
±

0.03

stat

±

0.09

sys

mag. Absolute calibrations of each method are anchored by independent geometric zero-points, utilize a different class of stars, and are determined from the same photometric calibration.
Accreted or Not Accreted? The Fraction of Accreted Mass in Galaxies from the Magneticum Simulations and Observations
Authors: Remus Rhea-Silvia , Forbes Duncan A. 
Published: August 2022

Abstract
In the two-phase scenario of galaxy formation, a galaxy’s stellar mass growth is first dominated by in-situ star formation, and subsequently by accretion. We analyze the radial distribution of the accreted stellar mass in ∼500 galaxies from the (48 Mpc/h)3 box volume of the hydrodynamical cosmological simulation Magneticum, in a stellar-mass range of 1010 to 1012
M
⊙. We find that higher-mass galaxies have larger accreted fractions, as found in previous works, but predict generally higher accretion fractions for low-mass galaxies. Based on the 3D radial distribution of the accreted and in-situ components, we define six galaxy classes, from completely accretion to completely in-situ dominated, and measure the transition radii between in-situ and accretion-dominated regions for galaxies that reveal a transition. About 70% of our galaxies have one transition radius. However, about 10% of the galaxies are accretion dominated everywhere, and about 13% have two transition radii, with the center and the outskirts both being accretion dominated. We show that these classes are strongly correlated with the galaxy merger histories, especially with the cold gas fraction at the time of merging. We find high total in-situ (low accretion) fractions to be associated with smaller, lower-mass galaxies, lower central dark-matter fractions, and larger transition radii. Finally, we show that the dips in observed surface brightness profiles seen in many early-type galaxies do not correspond to the transition from in-situ to accretion-dominated regions, and that any inferred mass fractions are not indicative of the true accreted mass but contain information about the galaxies’ dry-merger history.
SRGA J181414.6-225604: A New Galactic Symbiotic X-Ray Binary Outburst Triggered by an Intense Mass-loss Episode of a Heavily Obscured Mira Variable
Authors: De Kishalay , Mereminskiy Ilya , Soria Roberto , Conroy Charlie , Kara Erin , Anand Shreya , Ashley Michael C. B. , Boyer Martha L. , Chakrabarty Deepto , Grefenstette Brian , Hankins Matthew J. , Hillenbrand Lynne A. , Jencson Jacob E. , Karambelkar Viraj , Kasliwal Mansi M. , Lau Ryan M. , Lutovinov Alexander , Moore Anna M. , Ng Mason , Panagiotou Christos , Pasham Dheeraj R. , Semena Andrey , Simcoe Robert , Soon Jamie , Srinivasaragavan Gokul P. , Travouillon Tony , Yao Yuhan 
Published: August 2022

Abstract
We present the discovery and multiwavelength characterization of SRGA J181414.6-225604, a Galactic hard X-ray transient discovered during the ongoing SRG/ART-XC sky survey. Using data from the Palomar Gattini-IR survey, we identify a spatially and temporally coincident variable infrared (IR) source, IRAS 18111-2257, and classify it as a very-late-type (M7–M8), long-period (1502 ± 24 days), and luminous (M

K
≈ −9.9 ± 0.2) O-rich Mira donor star located at a distance of ≈14.6+2.9
−2.3 kpc. Combining multicolor photometric data over the last ≈25 yr, we show that the IR counterpart underwent a recent (starting ≈800 days before the X-ray flare) enhanced mass-loss (reaching ≈2.1 × 10−5
M
⊙ yr−1) episode, resulting in an expanding dust shell obscuring the underlying star. Multi-epoch follow-up observations from Swift, NICER, and NuSTAR reveal a ≈200 day long X-ray outburst reaching a peak luminosity of L
X ≈ 2.5 × 1036 erg s−1, characterized by a heavily absorbed (N
H ≈ 6 × 1022 cm−2) X-ray spectrum consistent with an optically thick Comptonized plasma. The X-ray spectral and timing behavior suggest the presence of clumpy wind accretion, together with a dense ionized nebula overabundant in silicate material surrounding the compact object. Together, we show that SRGA J181414.6-225604 is a new symbiotic X-ray binary in outburst, triggered by an intense dust-formation episode of a highly evolved donor. Our results offer the first direct confirmation for the speculated connection between enhanced late-stage donor mass loss and the active lifetimes of symbiotic X-ray binaries.
Are Active Galactic Nuclei in Post-starburst Galaxies Driving the Change or Along for the Ride?
Authors: Lanz Lauranne , Stepanoff Sofia , Hickox Ryan C. , Alatalo Katherine , French K. Decker , Rowlands Kate , Nyland Kristina , Appleton Philip N. , Lacy Mark , Medling Anne , Mulchaey John S. , Sazonova Elizaveta , Urry Claudia Megan 
Published: August 2022

Abstract
We present an analysis of 10 ks snapshot Chandra observations of 12 shocked post-starburst galaxies, which provide a window into the unresolved question of active galactic nuclei (AGN) activity in post-starburst galaxies and its role in the transition of galaxies from active star formation to quiescence. While seven of the 12 galaxies have statistically significant detections (with two more marginal detections), the brightest only obtained 10 photons. Given the wide variety of hardness ratios in this sample, we chose to pursue a forward-modeling approach to constrain the intrinsic luminosity and obscuration of these galaxies, rather than stacking. We constrain the intrinsic luminosity of obscured power laws based on the total number of counts and spectral shape, itself mostly set by the obscuration, with hardness ratios consistent with the data. We also tested thermal models. While all the galaxies have power-law models consistent with their observations, a third of the galaxies are better fit as an obscured power law and another third are better fit as thermal emission. If these post-starburst galaxies, early in their transition, contain AGNs, then these are mostly confined to lower obscuration (N

H
≤ 1023 cm−2) and lower luminosity (L
2−10 keV ≤ 1042 erg s−1). Two galaxies, however, are clearly best fit as significantly obscured AGNs. At least half of this sample shows evidence of at least low-luminosity AGN activity, though none could radiatively drive out the remaining molecular gas reservoirs. Therefore, these AGNs are more likely along for the ride, having been fed gas by the same processes driving the transition.
DustPy: A Python Package for Dust Evolution in Protoplanetary Disks
Authors: Stammler Sebastian M. , Birnstiel Tilman 
Published: August 2022

Abstract
Many processes during the evolution of protoplanetary disks and during planet formation are highly sensitive to the sizes of dust particles that are present in the disk: the efficiency of dust accretion in the disk and volatile transport on dust particles, gravoturbulent instabilities leading to the formation of planetesimals, or the accretion of pebbles onto large planetary embryos to form giant planets are typical examples of processes that depend on the sizes of the dust particles involved. Furthermore, radiative properties like absorption or scattering opacities depend on the particle sizes. To interpret observations of dust in protoplanetary disks, a proper estimate of the dust particle sizes is needed. We present DustPy: a Python package to simulate dust evolution in protoplanetary disks. DustPy solves gas and dust transport including viscous advection and diffusion as well as collisional growth of dust particles. DustPy is written with a modular concept, such that every aspect of the model can be easily modified or extended to allow for a multitude of research opportunities.
Jets from Accretion Disk Dynamos: Consistent Quenching Modes for Dynamo and Resistivity
Authors: Mattia Giancarlo , Fendt Christian 
Published: August 2022

Abstract
Astrophysical jets are launched from strongly magnetized systems that host an accretion disk surrounding a central object. The origin of the magnetic field, which is a key component of the launching process, is still an open question. Here we address the question of how the magnetic field required for jet launching is generated and maintained by a dynamo process. By carrying out nonideal MHD simulations (PLUTO code), we investigate how the feedback of the generated magnetic field on the mean-field dynamo affects the disk and jet properties. We find that a stronger quenching of the dynamo leads to a saturation of the magnetic field at a lower disk magnetization. Nevertheless, we find that, while applying different dynamo feedback models, the overall jet properties remain unaffected. We then investigate a feedback model that encompasses a quenching of the magnetic diffusivity. Our modeling considers a more consistent approach for mean-field dynamo modeling simulations, as the magnetic quenching of turbulence should be considered for both a turbulent dynamo and turbulent magnetic diffusivity. We find that, after the magnetic field is saturated, the Blandford–Payne mechanism can work efficiently, leading to more collimated jets, which move, however, with slower speed. We find strong intermittent periods of flaring and knot ejection for low Coriolis numbers. In particular, flux ropes are built up and advected toward the inner disk thereby cutting off the inner disk wind, leading to magnetic field reversals, reconnection and, the emergence of intermittent flares.
Chemodynamical Signatures of Bar Resonances in the Galactic Disk: Current Data and Future Prospects
Authors: Wheeler Adam , Abril-Cabezas Irene , Trick Wilma H. , Fragkoudi Francesca , Ness Melissa 
Published: August 2022

Abstract
The Galactic disk exhibits complex chemical and dynamical substructure thought to be induced by the bar, spiral arms, and satellites. Here, we explore the chemical signatures of bar resonances in action and velocity space, and characterize the differences between the signatures of corotation (CR) and higher-order resonances using test particle simulations. Thanks to recent surveys, we now have large data sets containing metallicities and kinematics of stars outside the solar neighborhood. We compare the simulations to the observational data from Gaia EDR3 and LAMOST DR5 and find weak evidence for a slow bar with the “hat” moving group (250 km s−1 ≲ v

ϕ
≲ 270 km s−1) associated with its outer Lindblad resonance and “Hercules” (170 km s−1 ≲ v

ϕ
≲ 195 km s−1) with CR. While constraints from current data are limited by their spatial footprint, stars closer in azimuth than the Sun to the bar’s minor axis show much stronger signatures of the bar’s outer Lindblad and CR resonances in test particle simulations. Future data sets with greater azimuthal coverage, including the final Gaia data release, will allow reliable chemodynamical identification of bar resonances.
GECAM Detection of a Bright Type I X-Ray Burst from 4U 0614+09: Hint for Its Spin Frequency at 413 Hz
Authors: Chen Yu-Peng , Li Jian , Xiong Shao-Lin , Ji Long , Zhang Shu , Peng Wen-Xi , Qiao Rui , Li Xin-Qiao , Wen Xiang-Yang , Song Li-Ming , Zheng Shi-Jie , Song Xin-Ying , Zhao Xiao-Yun , Huang Yue , Lu Fang-Jun , Zhang Shuang-Nan , Xiao Shuo , Cai Ce , An Zheng-Hua , Chang Zhi , Chen Can , Chen Gang , Chen Wei , Dai Guang-Qi , Du Yan-Qi , Gao Min , Gong Ke , Guo Dong-Ya , Guo Zhi-Wei , He Jian-Jian , Li Bin , Li Chao , Li Chao-Yang , Li Gang , Li Jian-Hui , Li Lu , Li Qing-Xin , Li Xiao-Bo , Li Yan-Guo , Liang Jing , Liang Xiao-Hua , Liao Jin-Yuan , Liu Jia-Cong , Liu Xiao-Jing , Liu Ya-Qing , Luo Qi , Ma Xiang , Meng Bin , Ou Ge , Shi Dong-Li , Shi Jing-Yan , Sun Gong-Xing , Sun Xi-Lei , Tuo You-Li , Wang Chen-Wei , Wang Hui , Wang Huan-Yu , Wang Jin , Wang Jin-Zhou , Wang Ping , Wang Wen-Shuai , Wang Yu-Xi , Wen Xing , Wu Hong , Xie Sheng-Lun , Xu Yan-Bing , Xu Yu-Peng , Xue Wang-Chen , Yang Sheng , Yao Min , Ye Jian-Ying , Yi Qi-Bin , Zhang Cheng-Mo , Zhang Chao-Yue , Zhang Da-Li , Zhang Fan , Zhang Fei , Zhang Hong-Mei , Zhang Kai , Zhang Peng , Zhang Xiao-Lu , Zhang Yan-Qiu , Zhang Zhen , Zhao Guo-Ying , Zhao Shi-Yi , Zhao Yi , Zheng Chao , Zhou Xing , Zhu Yue 
Published: August 2022

Abstract
One month after launching the Gravitational Wave High-energy Electromagnetic Counterpart All-sky Monitor, a bright thermonuclear X-ray burst from 4U 0614+09 was observed on 2021 January 24. We report the time-resolved spectroscopy of the burst and a hint of burst oscillation at 413 Hz with a fractional amplitude ∼2.0% (rms). This coincides with the burst oscillation previously discovered with Swift/Burst Alert Telescope (Strohmayer et al. 2008), and therefore supports the spin frequency of this source. This burst is a bright one in the normal bursts detected from 4U 0614+09, which leads to an upper limit of distance estimation of 3.1 kpc. The folded light curve during the burst oscillation shows a sinusoidal structure, which is consistent with previous observations.
MAXI J1535–571 2017 Outburst Seen by INTEGRAL/SPI and Investigating the Origin of Its Hard Tail
Authors: Rodi James , Jourdain E. , Roques J. P. 
Published: August 2022

Abstract
On 2017 September 2 MAXI J1535–571 went into outburst and peaked at ∼5 Crab in the 2–20 keV energy range. Early in the flare, the INTErnational Gamma-Ray Astrophysics Laboratory (INTEGRAL) performed target of opportunity pointings and monitored the source as it transitioned from the hard state to the soft state. Using quasi-simultaneous observations from MAXI/GSC and INTEGRAL/SPI, we studied the temporal and spectral evolution of MAXI J1535–571 in the 2–500 keV range. Early spectra show a Comptonized spectrum and a high-energy component dominant above ∼150 keV. CompTT fits to the SPectrometer on INTEGRAL (SPI) data found electron temperatures (kT

e
) evolve from ∼31 keV to 18 keV with a tied optical depth (τ ∼ 0.85) or τ evolving from ∼1.2–0.65 with a tied kT

e
(∼24 keV). To investigate the nature of the high-energy component, we performed a spectral decomposition of the 100–400 keV energy band. The CompTT flux varies significantly during the hard state while the high-energy component flux is consistent with a constant flux. This result suggests that the two components originate from different locations, which favors a jet origin interpretation for the high-energy component over a hybrid corona interpretation. Lastly, two short rebrightenings during the hard-to-soft transition are compared to similar events reported in MAXI J1820+070.
CONFIGURAÇÃO URBANA NA DISPONIBILIDADE DE LUZ NATURAL NO AMBIENTE CONSTRUÍDO
Authors: Mota Beck Luciana , Ruttkay Pereira Fernando Oscar 
Published: August 2022

As formas urbanas são controladas pelos regulamentos que podem não ser suficientes para assegurar o desempenho da luz natural no interior dos ambientes de todos os pavimentos de uma edificação. Diante disso, este artigo analisa a combinação de índices urbanos (índice de aproveitamento – IA, taxa de ocupação – TO e gabarito) e do índice de performance (Autonomia Espacial da Luz Natural – sDA300,50%), considerando cenários de bloco isolado no lote, para a cidade de Florianópolis. Outros parâmetros são avaliados: ângulo de obstrução vertical, porcentagem de céu visível e índice de espaço aberto – OSR, que relaciona a área construída total com a área aberta. Como resultados da pesquisa, são identificados valores de OSR, ângulo máximo de obstrução e porcentagem mínima de céu visível, correspondentes ao sDA igual a 45%, para que cenários de diferentes IA, TO e gabarito, obtenham desempenho satisfatório. As análises realizadas gradualmente permitem desenvolver estratégias específicas por pavimento, colaborando na escolha da configuração mais adequada para uma determinada condição de projeto. Verificou-se que as regras urbanas criadas a partir da escala do lote, restringem a criatividade arquitetônica, pois limitam a disposição dos arranjos espaciais e a geometria das edificações, importantes requisitos para a qualidade arquitetônica, urbana e de conforto.
Palavras-chave: Forma urbana. Índices urbanos. Luz natural.