bluuebunny/crossref_metadata_2025_split huggingface dataset:
Functional brain connectivity changes associated with day-to-day fluctuations in affective states
Authors: Racicot Jeanne , Smine Salima , Afzali Kamran , Orban Pierre 
Published: September 2024

AbstractAffective neuroscience has traditionally relied on cross-sectional studies to uncover the brain correlates of affects, emotions, and moods. Such findings obfuscate intraindividual variability that may reveal meaningful changing affect states. The few functional magnetic resonance imaging longitudinal studies that have linked changes in brain function to the ebbs and flows of affective states over time have mostly investigated a single individual. In this study, we explored how the functional connectivity of brain areas associated with affective processes can explain within-person fluctuations in self-reported positive and negative affects across several subjects. To do so, we leveraged the Day2day dataset that includes 40 to 50 resting-state functional magnetic resonance imaging scans along self-reported positive and negative affectivity from a sample of six healthy participants. Sparse multivariate mixed-effect linear models could explain 15% and 11% of the within-person variation in positive and negative affective states, respectively. Evaluation of these models’ generalizability to new data demonstrated the ability to predict approximately 5% and 2% of positive and negative affect variation. The functional connectivity of limbic areas, such as the amygdala, hippocampus, and insula, appeared most important to explain the temporal dynamics of affects over days, weeks, and months.
EFEKTIVITAS KEBIJAKAN PENGGUNAAN APLIKASI SISTEM INFORMASI KELUARGA (New SIGA) DALAM PELAPORAN HASIL KEGIATAN DI UPTD PENGENDALIAN PENDUDUK WILAYAH CICURUG KECAMATAN CICURUG KABUPATEN SUKABUMI
Authors: Muhammad Sulaeman Nur Muhammad Sulaeman Nur , Virgian Septia Lesmana  
Published: September 2024

Aplikasi Sistem Informasi Keluarga (New SIGA) adalah seperangkat tatanan yang meliputi data, informasi, indikator, prosedur, perangkat, teknologi dan sumber daya manusia yang saling berkaitan dan dikelola secara terpadu untuk mengarahkan tindakan atau keputusan yang berguna dalam mendukung pembangunan keluarga. Penggunaan Aplikasi Sistem Informasi Keluarga (New SIGA) dalam pelaporan hasil kegiatan bertujuan untuk memberikan kemudahan bagi para pengelola data dan informasi di seluruh tingkatan wilayah dalam hal mengelola data laporan tahunan dan bulanan. Penelitian ini bertujuan untuk mengetahui Efektivitas Penggunaan Aplikasi Sistem Informasi Keluarga (New SIGA) dalam pelaporan hasil kegiatan di UPTD Pengendalian Penduduk Wilayah Cicurug Kecamatan Cicurug Kabupaten Sukabumi.

Metode yang digunakan dalam penelitian ini yaitu metode deskriptif dengan pendekatan kualitatif, dimana penelitian ini bermaksud untuk mendeskripsikan dan menginterpretasikan suatu kondisi alamiah. Hasil penelitian yang diperoleh antara lain, efektivitas Penggunaan Aplikasi Sistem Informasi Keluarga (New SIGA) dalam pelaporan hasil kegiatan akan tercapai dengan menerapkan 3 konsep efektivitas diantaranya Optimalisasi Tujuan, Perspektif Sistem dan Perilaku Manusia dalam Organisasi.

Berdasarkan hasil penelitian yang diperoleh antara lain, belum optimalnya optimalisasi tujuan, perspektif sistem dan perilaku manusia dalam organisasi pada proses Penggunaan Sistem Informasi Keluarga (New SIGA) dalam Pelaporan Hasil Kegiatan di UPTD Pengendalian Penduduk Wilayah Cicurug Kecamatan Cicurug Kabupaten Sukabumi sehingga menimbulkan Efektivitas Penggunaan Aplikasi Sistem Informasi Keluarga (New SIGA) dalam Pelaporan Hasil Kegiatan di UPTD Pengendalian Penduduk Wilayah Cicurug Kecamatan Cicurug Kabupaten Sukabumi belum tercapai secara maksimal
POLITIK IDENTITAS MELAYU MALAYSIA DAN MULTIKULTURALISME PADA FILM UPIN & IPIN
Authors: Wahyudi. S Fazril wahyudi.s , Widia Ierdiana  , Siti Badariah  , Rindi Wulansari  , Nadilla  , Fitri Nurzana  , Novrianti  , Aditya Padini Syah  
Published: September 2024

Penelitian ini bertujuan untuk melihat bagaimana politik identitas melayu malaysia dan multikulturalisme pada Film “Upin & Ipin”. Metode menggunakan pendekatan kualitatif dengan analisis konten sebagai metode utama. Data diperoleh melalui pengamatan mendalam terhadap narasi, karakter, dan simbol-simbol budaya yang muncul dalam film. Hasil penelitian menunjukkan bahwa politik identitas melayu Malaysia pada film Upin-Ipin adalah berbahasa Melayu, berbudaya Melayu, Islam, geneologi melayu Malaysia. Multikulturalisme pada Film Upin dan Ipin adalah perpaduan antara budaya melayu Malaysia, budaya India, Budaya Cina, Budaya Indonesia. Politik identitas melayu Malaysia dan multikulturalisme ada dalam lembaga pendidikan di Malaysia yang memperkenalkan nilai-nilai toleransi dan penghargaan terhadap keberagaman budaya. Film ini berhasil mempromosikan pesan persatuan dan keharmonisan melalui representasi positif dari berbagai identitas etnis melayu Malaysia dan etnis budaya lainnya, seperti Melayu, Tionghoa, dan India, yang hidup berdampingan di Malaysia.
Kata Kunci: Politik Identitas, Multikulturalisme, Upin-ipin
Probing the Possible Causes of the Transit Timing Variation for TrES-2b in the TESS Era
Authors: Biswas Shraddha , Bisht D. , Jiang Ing-Guey , Sariya Devesh P. , Parthasarathy Kaviya 
Published: September 2024

Abstract
Nowadays, transit timing variations (TTVs) are proving to be a very valuable tool in exoplanetary science to detect exoplanets by observing variations in transit times. To study the TTV of the hot Jupiter TrES-2b, we have combined 64 high-quality transit light curves from all seven sectors of NASA's Transiting Exoplanet Survey Satellite along with 60 best-quality light curves from the ground-based facility Exoplanet Transit Database and 106 midtransit times from the previous works. From the precise transit timing analysis, we have observed a significant improvement in the orbital ephemerides, but we did not detect any short-period TTVs that might result from an additional body. The inability to detect short-term TTVs further motivates us to investigate long-term TTVs, which might be caused by orbital decay, apsidal precession, the Applegate mechanism, and the Rømer effect, and the orbital decay appeared to be a better explanation for the observed TTV with ΔBIC = 4.32. The orbital period of the hot Jupiter TrES-2b appears to be shrinking at a rate of ∼–5.58 ± 1.81 ms yr−1. Assuming this decay is primarily caused by tidal dissipation within the host star, we have subsequently calculated the stellar tidal quality factor value to be ∼9.9 × 103, which is 2–3 orders of magnitude smaller than the theoretically predicted values for other hot-Jupiter systems, and its low value indicates more efficient tidal dissipation within the host star. Additional precise photometric and radial velocity observations are required to pinpoint the cause of the change in the orbital period.
RV Measurements of Directly Imaged Brown Dwarf GQ Lup B to Search for Exosatellites
Authors: Horstman Katelyn , Ruffio Jean-Baptiste , Batygin Konstantin , Mawet Dimitri , Baker Ashley , Hsu Chih-Chun , Wang 王 Jason J. 劲飞 , Wang 王 Ji 吉 , Blunt Sarah , Xuan Jerry W. , Xin Yinzi , Liberman Joshua , Agrawal Shubh , Konopacky Quinn M. , Blake Geoffrey A. , Do Ó Clarissa R. , Bartos Randall , Bond Charlotte Z. , Calvin Benjamin , Cetre Sylvain , Delorme Jacques-Robert , Doppmann Greg , Echeverri Daniel , Finnerty Luke , Fitzgerald Michael P. , Jovanovic Nemanja , López Ronald , Martin Emily C. , Morris Evan , Pezzato Jacklyn , Ruane Garreth , Sappey Ben , Schofield Tobias , Skemer Andrew , Venenciano Taylor , Wallace J. Kent , Wallack Nicole L. , Wizinowich Peter 
Published: September 2024

Abstract
GQ Lup B is one of the few substellar companions with a detected cicumplanetary disk (CPD). Observations of the CPD suggest the presence of a cavity, possibly formed by an exosatellite. Using the Keck Planet Imager and Characterizer (KPIC), a high-contrast imaging suite that feeds a high-resolution spectrograph (1.9–2.5 µm, R∼35,000), we present the first dedicated radial velocity (RV) observations around a high-contrast, directly imaged substellar companion, GQ Lup B, to search for exosatellites. Over 11 epochs, we find a best and median RV error of 400–1000 m s−1, most likely limited by systematic fringing in the spectra due to transmissive optics within KPIC. With this RV precision, KPIC is sensitive to exomoons 0.6%–2.8% the mass of GQ Lup B (∼30 M
Jup) at separations between the Roche limit and 65 R
Jup, or the extent of the cavity inferred within the CPD detected around GQ Lup B. Using simulations of HISPEC, a high resolution infrared spectrograph planned to debut at W.M. Keck Observatory in 2026, we estimate future exomoon sensitivity to increase by over an order of magnitude, providing sensitivity to less massive satellites potentially formed within the CPD itself. Additionally, we run simulations to estimate the amount of material that different masses of satellites could clear in a CPD to create the observed cavity. We find satellite-to-planet mass ratios of q > 2 × 10−4 can create observable cavities and report a maximum cavity size of ∼51 R
Jup carved from a satellite.
Gravitational Self-lensing of Fast Radio Bursts in Neutron Star Magnetospheres. I. The Model
Authors: Dall’Osso Simone , La Placa Riccardo , Stella Luigi , Bakala Pavel , Possenti Andrea 
Published: September 2024

Abstract
Fast radio bursts (FRBs) are cosmological subsecond bursts of coherent radio emission, whose source is still unknown. To date, the Galactic magnetar SGR 1935 + 2154 is the only astrophysical object known to emit radio bursts akin to FRBs, albeit less powerful, supporting suggestions that FRBs originate from magnetars. Many remarkable properties of FRBs—e.g., the dichotomy between repeaters and one-off sources, and their power-law energy distributions (with typical index ∼2–3)—are not well understood yet. Moreover, the huge radio power released by the most active repeaters is challenging even for the magnetic energy reservoir of magnetars. Here, we assume that FRBs originate from corotating hotspots anchored in neutron star (NS) magnetospheres and occasionally get amplified by large factors via gravitational self-lensing in the strong NS field. We evaluate the probability of amplification and show that: (i) a power-law energy distribution of events ∝E
−(2−3) is generally expected; (ii) all FRB sources may be regarded as repeating, their appearance as one-off sources or repeaters being determined by the critical dependence of the amplification probability on the emission geometry and source orientation relative to Earth; and (iii) the most active repeaters, in particular, correspond to extremely rare and finely tuned orientations (∼1 in 106), leading to large probabilities of amplification that make their bursts frequently detectable. At the same time, their power release appears enhanced, typically by factors ≳10, easing their energy budget problem.
The Scale of Stellar Yields: Implications of the Measured Mean Iron Yield of Core Collapse Supernovae
Authors: Weinberg David H. , Griffith Emily J. , Johnson James W. , Thompson Todd A. 
Published: September 2024

Abstract
The scale of α-element yields is difficult to predict from theory because of uncertainties in massive star evolution, supernova physics, and black hole formation, and it is difficult to constrain empirically because the impact of higher yields can be compensated by greater metal loss in galactic winds. We use a recent measurement of the mean iron yield of core collapse supernovae (CCSN) by Rodriguez et al.,

y

¯

Fe

cc

=
0.058
±
0.007

M

⊙

, to infer the scale of α-element yields by assuming that the plateau of [α/Fe] abundance ratios observed in low-metallicity stars represents the yield ratio of CCSN. For a plateau at [α/Fe]cc = 0.45, we find that the population-averaged yields of O and Mg are about equal to the solar abundance of these elements,

log

y

O

cc

/

Z

O
,
⊙

=
log

y

Mg

cc

/

Z

Mg
,
⊙

=
−
0.01
±
0.1

, where

y

X

cc

is the mass of element X produced by massive stars per unit mass of star formation. The inferred O and Fe yields agree with predictions of the Sukhbold et al. CCSN models assuming their Z9.6+N20 neutrino-driven engine, a scenario in which many progenitors with M < 40M
⊙ implode to black holes rather than exploding. The yields are lower than assumed in many models of the galaxy mass–metallicity relation, reducing the level of outflows needed to match observed abundances. Our one-zone chemical evolution models with

η
=

M

̇

out

/

M

̇

*

≈
0.6

evolve to solar metallicity at late times. By further requiring that models reach [α/Fe] ≈ 0 at late times, we infer a Hubble-time integrated Type Ia supernova rate of

1.1
×

10

−
3

M

⊙

−
1

, compatible with estimates from supernova surveys.
The Orbit and Companion of PSR J1622-0315: Variable Asymmetry and a Massive Neutron Star
Authors: Sen Bidisha , Linares Manuel , Kennedy Mark R. , Breton Rene P. , Misra Devina , Turchetta Marco , Dhillon Vikram S. , Mata Sánchez Daniel , Clark Colin J. 
Published: September 2024

Abstract
The companion to PSR J1622-0315, one of the most compact known redback millisecond pulsars, shows extremely low irradiation despite its short orbital period. We model this system to determine the binary parameters, combining optical observations from the New Technology Telescope in 2017 and the Nordic Optical Telescope in 2022 with the binary modeling code ICARUS. We find a best-fit neutron star mass of 2.3 ± 0.4 M
⊙, and a companion mass of 0.15 ± 0.02 M
⊙. We detect for the first time low-level irradiation from asymmetry in the minima as well as a change in the asymmetry of the maxima of its light curves over five years. Using starspot models, we find better fits than those from symmetric direct heating models, with consistent orbital parameters. We discuss an alternative scenario where the changing asymmetry is produced by a variable intrabinary shock. In summary, we find that PSR J1622-0315 combines low irradiation with variable light-curve asymmetry and a relatively high neutron star mass.
The JWST Resolved Stellar Populations Early Release Science Program. VI. Identifying Evolved Stars in Nearby Galaxies
Authors: Boyer Martha L. , Pastorelli Giada , Girardi Léo , Marigo Paola , Dolphin Andrew E. , McQuinn Kristen B. W. , Newman Max J. B. , Savino Alessandro , Weisz Daniel R. , Williams Benjamin F. , Anderson Jay , Cohen Roger E. , Correnti Matteo , Cole Andrew A. , Geha Marla C. , Gennaro Mario , Kallivayalil Nitya , Kirby Evan N. , Sandstrom Karin M. , Skillman Evan D. , Garling Christopher T. , Richstein Hannah , Warfield Jack T. 
Published: September 2024

Abstract
We present an investigation of evolved stars in the nearby star-forming galaxy Wolf–Lundmark–Melotte (WLM), using Near-Infrared Camera (NIRCam) imaging from the JWST Resolved Stellar Populations Early Release Science program. We find that various combinations of the F090W, F150W, F250M, and F430M filters can effectively isolate red supergiants and thermally pulsing asymptotic giant branch (TP-AGB) stars from one another, while also providing a reasonable separation of the primary TP-AGB subtypes: carbon-rich C-type stars and oxygen-rich M-type stars. The classification scheme we present here agrees very well with the well-established Hubble Space Telescope (HST) medium-band filter technique. The ratio of C to M-type stars is 0.8 ± 0.1 for both the new JWST and the HST classifications, which is within 1σ of empirical predictions from optical narrowband CN and TiO filters. The evolved star colors show good agreement with the predictions from the PARSEC + COLIBRI stellar evolutionary models, and the models indicate a strong metallicity dependence that makes stellar identification even more effective at higher metallicity. However, the models also indicate that evolved star identification with NIRCam may be more difficult at lower metallicities. We test every combination of NIRCam filters using the models and present additional filters that are also useful for evolved star studies. We also find that ≈90% of the dusty evolved stars are carbon rich, suggesting that carbonaceous dust dominates the present-day dust production in WLM, similar to the findings in the Magellanic Clouds. These results demonstrate the usefulness of NIRCam in identifying and classifying dust-producing stars without the need for mid-infrared data.
Early-time Observations of SN 2023wrk: A Luminous Type Ia Supernova with Significant Unburned Carbon in the Outer Ejecta
Authors: Liu Jialian , Wang Xiaofeng , Andrade Cristina , Duverne Pierre-Alexandre , Zhang Jujia , Li Liping , Wang Zhenyu , Navarete Felipe , Reguitti Andrea , Schuldt Stefan , Cai Yongzhi , Filippenko Alexei V. , Yang Yi , Brink Thomas G. , Zheng WeiKang , Esamdin Ali , Iskandar Abdusamatjan , Bai Chunhai , Liu Jinzhong , Li Xin , Hu Maokai , Li Gaici , Li Wenxiong , Ma Xiaoran , Yan Shengyu , Mo Jun , Adami Christophe , Akl Dalya , Antier Sarah , Broens Eric , Ducoin Jean-Grégoire , Elhosseiny Eslam , Esposito Thomas M. , Freeberg Michael , Gokuldass Priyadarshini , Hello Patrice , Karpov Sergey , Márquez Isabel , Mašek Martin , Pyshna Oleksandra , Rajabov Yodgor , Saint-Gelais Denis , Serrau Marc , Sokoliuk Oleksii , Takey Ali , Tanasan Manasanun , Turpin Damien 
Published: September 2024

Abstract
We present extensive photometric and spectroscopic observations of the nearby Type Ia supernova (SN) 2023wrk at a distance of about 40 Mpc. The earliest detection of this SN can be traced back to a few hours after the explosion. Within the first few days, the light curve shows a bump feature, while the B − V color is blue and remains nearly constant. The overall spectral evolution is similar to that of an SN 1991T/SN 1999aa-like SN Ia, while the C ii
λ6580 absorption line appears to be unusually strong in the first spectrum taken at t ≈ −15.4 days after the maximum light. This carbon feature disappears quickly in subsequent evolution but it reappears at around the time of peak brightness. The complex evolution of the carbon line and the possible detection of Ni iii absorption around 4700 Å and 5300 Å in the earliest spectra indicate macroscopic mixing of fuel and ash. The strong carbon lines are likely related to the collision of SN ejecta with unbound carbon, consistent with the predictions of pulsational delayed-detonation or carbon-rich circumstellar-matter interaction models. Among those carbon-rich SNe Ia with strong C ii
λ6580 absorption at very early times, the line-strength ratio of C ii to Si ii and the B − V color evolution are found to exhibit large diversity, which may be attributed to different properties of unbound carbon and outward-mixing 56Ni.
The Strength of Bisymmetric Modes in SDSS-IV/MaNGA Barred Galaxy Kinematics
Authors: DiGiorgio Zanger Brian , Westfall Kyle B. , Bundy Kevin , Drory Niv , Bershady Matthew A. , Campbell Stephanie , Weijmans Anne-Marie , Masters Karen L. , Stark David , Law David 
Published: September 2024

Abstract
The Sloan Digital Sky Survey-IV/Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) Survey data provide an unprecedented opportunity to study the internal motions of galaxies and, in particular, represent the largest sample of barred galaxy kinematic maps obtained to date. We present results from Nirvana, our nonaxisymmetric kinematic modeling code built with a physically motivated Bayesian forward modeling approach, which decomposes MaNGA velocity fields into first- and second-order radial and tangential rotational modes in a generalized and minimally supervised fashion. We use Nirvana to produce models and rotation curves for 1263 unique barred MaNGA galaxies and a matched unbarred control sample. We present our modeling approach, tests of its efficacy, and validation against existing visual bar classifications. Nirvana finds elevated noncircular motions in galaxies identified as bars in imaging, and bar position angles that agree well with visual measurements. The Nirvana-MaNGA barred and control samples provide a new opportunity for studying the influence of nonaxisymmetric internal disk kinematics in a large statistical sample.
The Supersonic Project: Early Star Formation with the Streaming Velocity
Authors: Lake William , Williams Claire E. , Naoz Smadar , Marinacci Federico , Burkhart Blakesley , Vogelsberger Mark , Yoshida Naoki , Chiaki Gen , Chen Avi , Chiou Yeou S. 
Published: September 2024

Abstract
At high redshifts (z ≳ 12), the relative velocity between baryons and dark matter (the so-called streaming velocity) significantly affects star formation in low-mass objects. Streaming substantially reduces the abundance of low-mass gas objects while simultaneously allowing for the formation of supersonically induced gas objects (SIGOs) and their associated star clusters outside of dark matter halos. Here, we present a study of the population-level effects of streaming on star formation within both halos and SIGOs in a set of simulations with and without streaming. Notably, we find that streaming actually enhances star formation within individual halos of all masses at redshifts between z = 12 and z = 20. This is demonstrated both as an increased star formation rate per object as well as an enhancement of the Kennicutt–Schmidt relation for objects with streaming. We find that our simulations are consistent with some observations at high redshift, but on a population level, they continue to underpredict star formation relative to the majority of observations. Notably, our simulations do not include feedback and so can be taken as an upper limit on the star formation rate, exacerbating these differences. However, simulations of overdense regions (both with and without streaming) agree with observations, suggesting a strategy for extracting information about the overdensity and streaming velocity in a given survey volume in future observations.
Navigating Unknowns: Deep Learning Robustness for Gravitational-wave Signal Reconstruction
Authors: Chatterjee Chayan , Jani Karan 
Published: September 2024

Abstract
We present a rapid and reliable deep-learning-based method for gravitational-wave (GW) signal reconstruction from elusive, generic binary black hole mergers in LIGO data. We demonstrate that our model, AWaRe, effectively recovers GWs with parameters it has not encountered during training. This includes features like higher black hole masses, additional harmonics, eccentricity, and varied waveform systematics, which introduce complex modulations in the waveform’s amplitudes and phases. The accurate reconstructions of these unseen signal characteristics demonstrate AWaRe's ability to handle complex features in the waveforms. By directly incorporating waveform reconstruction uncertainty estimation into the AWaRe framework, we show that for real GW events, the uncertainties in AWaRe's reconstructions align closely with those achieved by benchmark algorithms like BayesWave and coherent WaveBurst. The robustness of our model to real GW events and its ability to extrapolate to unseen data open new avenues for investigations in various aspects of GW astrophysics and data analysis, including tests of general relativity and the enhancement of current GW search methodologies.
NICER Observes the Full Z-track in GX 13+1
Authors: Kaddouh Mohamad Ali , Sudha Malu , Ludlam Renee M. 
Published: September 2024

Abstract
We present the temporal analysis of the persistent neutron star low-mass X-ray binary GX 13+1 using NICER data. Classification of this source has been ambiguous so far. We investigate the evolution of the source in its hardness–intensity diagram (HID) and power density spectra (PDS) of the 0.5–10 keV NICER archival data. For the first time, we detect the source tracing out the entire Z-track, distinctly identifying the horizontal branch (HB), normal branch (NB) and flaring branch (FB). We also detect a peaked noise component in the PDS at ∼5.4 Hz, which appears to be present when the source is either in the NB or FB. We note a positive slope of the HB in the HID which could be due to either the high intrinsic absorption of the source or the stronger contribution of the soft spectral components in the soft energy domain.