The Astrophysical Journal最新文献_第9页

Probing Chemical Enrichment in Extremely Metal-poor Galaxies 探测极贫金属星系中的化学富集

The Astrophysical Journal Pub Date : 2025-07-10 DOI: 10.3847/1538-4357/add690

Keita Fukushima, Kentaro Nagamine, Akinori Matsumoto, Yuki Isobe, Masami Ouchi, Takayuki R. Saitoh and Yutaka Hirai

{"title":"Probing Chemical Enrichment in Extremely Metal-poor Galaxies","authors":"Keita Fukushima, Kentaro Nagamine, Akinori Matsumoto, Yuki Isobe, Masami Ouchi, Takayuki R. Saitoh and Yutaka Hirai","doi":"10.3847/1538-4357/add690","DOIUrl":"https://doi.org/10.3847/1538-4357/add690","url":null,"abstract":"The chemical composition of galaxies offers vital insights into their formation and evolution. In particular, the relationship between helium abundance (He/H) and metallicity serves as a key diagnostic for estimating the primordial helium yield from Big Bang nucleosynthesis. We investigate the chemical enrichment history of low-metallicity galaxies, focusing especially on extremely metal-poor galaxies (EMPGs), using one-zone chemical evolution models. Adopting elemental yields from M. Limongi & A. Chieffi, our models reach He/H ∼ 0.089 at (O/H) × 105 < 20, yet they fall short of reproducing the elevated He/H values observed in low-redshift dwarf galaxies. In contrast, the observed Fe/O ratios in EMPGs are successfully reproduced using both the K. Nomoto et al. and M. Limongi & A. Chieffi yield sets. To address the helium discrepancy, we incorporate supermassive stars (SMSs) as Population III stars in our models. We find that SMSs can significantly enhance He/H, depending on the mass-loss prescription. When only 10% of the SMS mass is ejected, the model yields the steepest slope in the (O/H) × 105–He/H relation. Alternatively, if the entire outer envelope up to the CO core is expelled, the model can reproduce the high He/H ratios observed in high-redshift galaxies (He/H > 0.1). Additionally, these SMS-enriched models also predict elevated N/O ratios, in agreement with recent JWST observations of the early Universe.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"35 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144603297","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Rethinking Habitability Using Biogenic Precursors: Formaldehyde in Millimeter Molecular Clouds of the Inner Galaxy 利用生物前体重新思考宜居性：内星系毫米分子云中的甲醛

The Astrophysical Journal Pub Date : 2025-07-10 DOI: 10.3847/1538-4357/add691

N. B. Baharin, A. A. Nazri, Z. Rosli, Z. Z. Abidin, H. A. Tajuddin, J. Esimbek, D. L. Li and X. Tang

{"title":"Rethinking Habitability Using Biogenic Precursors: Formaldehyde in Millimeter Molecular Clouds of the Inner Galaxy","authors":"N. B. Baharin, A. A. Nazri, Z. Rosli, Z. Z. Abidin, H. A. Tajuddin, J. Esimbek, D. L. Li and X. Tang","doi":"10.3847/1538-4357/add691","DOIUrl":"https://doi.org/10.3847/1538-4357/add691","url":null,"abstract":"We present a comprehensive study of formaldehyde (H2CO) absorption and radio recombination line (H110α) emission in 215 molecular clouds from the Bolocam Galactic Plane Survey, observed using the Nanshan 25 m radio telescope. H2CO was detected in 88 sources (40.93%) with 59 being new detections, while H110α emission was found in only 11 sources (5.12%), all coincident with H2CO absorption. There exists a correlation of H2CO fluxes with millimeter fluxes below a 3 Jy threshold and an increased dispersion above it, suggesting the sub-cosmic microwave background cooling of H2CO. Cross-matching with kinematic distance catalogs revealed H2CO spanning galactocentric distances from 0.216 to 10.769 kpc, with column densities ranging from 7.82 × 1011 to 6.69 × 1014 cm−2. A significant inverse correlation was observed between H2CO detection fraction and galactocentric distance, suggesting enhanced star-forming activity closer to the Galactic Center. These findings challenge traditional Galactic Habitable Zone (GHZ) models by demonstrating the presence of biogenic precursors in the inner Galaxy, shielded within dense molecular clouds. Our results underscore the importance of incorporating chemical tracers such as H2CO, alongside physical constraints to refine the boundaries of the GHZ and advance the research of prebiotic chemistry in the Milky Way.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"149 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144603304","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Effective Viscosity in the Intracluster Medium During Magnetic Field Amplification via Turbulent Dynamo 湍流发电机磁场放大过程中簇内介质的有效粘度

The Astrophysical Journal Pub Date : 2025-07-10 DOI: 10.3847/1538-4357/addc5f

S. Adduci Faria, R. Santos-Lima and E. M. de Gouveia Dal Pino

{"title":"Effective Viscosity in the Intracluster Medium During Magnetic Field Amplification via Turbulent Dynamo","authors":"S. Adduci Faria, R. Santos-Lima and E. M. de Gouveia Dal Pino","doi":"10.3847/1538-4357/addc5f","DOIUrl":"https://doi.org/10.3847/1538-4357/addc5f","url":null,"abstract":"Galaxy clusters, the largest gravitationally bound structures, host a hot, diffuse plasma with poorly understood viscosity and magnetic field amplification. Astrophysical plasmas are often modeled with magnetohydrodynamics (MHD), but low collision rates in environments such as the intracluster medium (ICM) hinder thermodynamic equilibrium, causing pressure anisotropies and high viscosity. High-β plasmas, dominated by thermal pressure, are prone to instabilities (e.g., firehose or mirror) that limit anisotropy, reduce viscosity, and enable small-scale dynamo-driven magnetic amplification. This study examines viscosity evolution in the ICM during turbulent magnetic field amplification. We performed 3D MHD simulations of forced turbulence with an initially weak, uniform magnetic field. Using the Chew–Goldberger–Low (CGL)-MHD framework, we incorporate anisotropic pressure dynamics and instability-driven anisotropy limitation. We analyze effective viscosity and dynamo evolution, comparing results with Braginskii-MHD and uniform-viscosity MHD. Our results show that viscosity decreases over time, allowing magnetic field amplification to saturation levels similar to nonviscous MHD. Viscosity distribution becomes bimodal, reflecting (i) collisional values and (ii) turbulence-dominated values proportional to 1 × 10−4LturbUturb in unstable regions. At saturation, 60% of plasma retains collisional viscosity. Braginskii-MHD reproduces similar magnetic amplification and viscosity structures. However, uniform-viscosity MHD, where viscosity equals the mean saturated CGL-MHD value, fails to capture the turbulence inertial range. These findings highlight the need for anisotropic viscosity models in studying ICM processes such as magnetic topology, cosmic ray transport, and active galactic nucleus-driven shocks. Moreover, our CGL-MHD and Braginskii-MHD models match the Coma cluster density fluctuation spectrum, reinforcing its weakly collisional nature.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"697 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144603298","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Inferring the Density and Membership of Stellar Streams with Flexible Models: The GD-1 Stream in Gaia Data Release 3 用灵活模型推断恒星流的密度和隶属度：Gaia数据发布3中的GD-1流

The Astrophysical Journal Pub Date : 2025-07-10 DOI: 10.3847/1538-4357/addd1c

Kiyan Tavangar and Adrian M. Price-Whelan

{"title":"Inferring the Density and Membership of Stellar Streams with Flexible Models: The GD-1 Stream in Gaia Data Release 3","authors":"Kiyan Tavangar and Adrian M. Price-Whelan","doi":"10.3847/1538-4357/addd1c","DOIUrl":"https://doi.org/10.3847/1538-4357/addd1c","url":null,"abstract":"Stellar streams provide one of the most promising avenues for constraining the global mass distribution of the Milky Way and the nature of dark matter (DM). The stream stars’ kinematic “track” enables inference of large-scale properties of the DM distribution, while density variations and anomalies provide information about local DM clumps (e.g., from DM subhalos). A full accounting of the density tracks and substructures within all >100 Milky Way stellar streams will therefore enable powerful new constraints on DM. Here, we present a new, flexible framework for modeling stellar stream density and membership. With it, one can empirically model a given stream in a variety of coordinate spaces (e.g., on-sky position and velocity) using probability distributions, thereby generating membership probabilities. The most significant improvement over previous methods is the inclusion of off-track or non-Gaussian components to the stream density, meaning we can capture anomalous features (such as the GD-1 steam’s spur). We test our model on GD-1, where we characterize previously known features and provide the largest catalog of probable member stars to date (1689 stars). We then use the derived model to provide measurements of GD-1’s density and kinematic tracks, velocity dispersion, as well as its initial and current mass. Our framework (built on JAX and numpyro) provides a path toward uniform analysis of all Milky Way streams, enabling tight constraints on the Galactic mass distribution and its dark matter.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"88 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144603299","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Exploring Quasar Variability with ZTF at 0 < z < 3: A Universal Relation with the Eddington Ratio ZTF 0 < z < 3时类星体变异性的研究：与Eddington比值的普遍关系

The Astrophysical Journal Pub Date : 2025-07-10 DOI: 10.3847/1538-4357/addec0

Hygor Benati Gonçalves, Swayamtrupta Panda, Thaisa Storchi Bergmann, Edward M. Cackett and Michael Eracleous

{"title":"Exploring Quasar Variability with ZTF at 0 < z < 3: A Universal Relation with the Eddington Ratio","authors":"Hygor Benati Gonçalves, Swayamtrupta Panda, Thaisa Storchi Bergmann, Edward M. Cackett and Michael Eracleous","doi":"10.3847/1538-4357/addec0","DOIUrl":"https://doi.org/10.3847/1538-4357/addec0","url":null,"abstract":"Quasars, powered by accretion onto supermassive black holes (SMBHs), exhibit significant variability, offering insights into the physics of accretion and the properties of the central engines. In this study, we analyze photometric variability and its correlation with key quasar properties, including black hole mass (MBH) and nuclear luminosities, using 915 quasars with 0 ≤ z < 3.0 from the All Quasar Multi-Epoch Spectroscopy sample monitored within the fifth-generation Sloan Digital Sky Survey (SDSS-V). Variability metrics were derived from approximately 6 yr light curves provided by the Zwicky Transient Facility (ZTF), while SMBH masses and luminosities were obtained from the SDSS DR16 quasar catalog of Q. Wu & Y. Shen. We identify a strong anticorrelation between variability amplitude and luminosity, which strengthens with redshift, and a redshift-dependent trend for MBH: a positive correlation at low redshifts, no significant correlation at intermediate redshifts, and an anticorrelation at the highest redshifts. Our main finding is a robust anticorrelation between photometric variability amplitude and Eddington ratio, consistent across different redshift bins. We present a general equation encapsulating this relationship, which appears to be almost free of redshift dependence, enabling predictions of quasar variability based on accretion parameters or vice versa. The derived relation with the Eddington ratio provides a unified framework for interpreting variability in active galactic nuclei and facilitates future studies of quasar variability using high-cadence surveys, such as the Vera C. Rubin Observatory’s Legacy Survey of Space and Time.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"11 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144603300","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Radiation and Magnetic Pressure Support in Accretion Disks Around Supermassive Black Holes and the Physical Origin of the Extreme-ultraviolet to Soft X-Ray Spectrum 超大质量黑洞周围吸积盘中的辐射和磁压支持以及极紫外到软x射线光谱的物理起源

The Astrophysical Journal Pub Date : 2025-07-10 DOI: 10.3847/1538-4357/addecb

Yan-Fei Jiang, 燕飞姜, Omer Blaes, Ish Kaul, Lizhong Zhang and 力中张

{"title":"Radiation and Magnetic Pressure Support in Accretion Disks Around Supermassive Black Holes and the Physical Origin of the Extreme-ultraviolet to Soft X-Ray Spectrum","authors":"Yan-Fei Jiang, 燕飞姜, Omer Blaes, Ish Kaul, Lizhong Zhang and 力中张","doi":"10.3847/1538-4357/addecb","DOIUrl":"https://doi.org/10.3847/1538-4357/addecb","url":null,"abstract":"We present the results of four 3D radiation magnetohydrodynamic simulations of accretion disks around a 108 solar mass black hole, which produce the far-ultraviolet spectrum peak and demonstrate a robust physical mechanism for producing the extreme-ultraviolet to soft X-ray power-law continuum component. The disks are fed from rotating tori and reach accretion rates ranging from 0.03 to 4 times the Eddington value. The disks become radiation pressure or magnetic pressure dominated, depending on the relative timescales of radiative cooling and gas inflow. Magnetic pressure supported disks can form with or without net poloidal magnetic fields, as long as the inflowing gas can cool quickly enough, which can typically happen when the accretion rate is low. We calculate the emerging spectra from these disks using multigroup radiation transport with realistic opacities and find that they typically peak around 10 eV. At accretion rates close to or above the Eddington limit, a power-law component can appear for photon energies between 10 eV and 1 keV, with a spectral slope varying between Lν ∝ ν−1 and ν−2, comparable to what is observed in radio-quiet quasars. A disk with a 3% Eddington accretion rate does not exhibit this component. These high-energy photons are produced in an optically thick region ≈30∘–45∘ from the disk midplane, by compressible bulk Comptonization within the converging accretion flow. Strongly magnetized disks that have a very small surface density will produce a spectrum that is very different from what is observed.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"4 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144603301","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Evolutionary Period Changes for 25 X-Ray Binaries and the Measurement of an Empirical Universal Law for Angular Momentum Loss in Accreting Binaries 25个x射线双星的演化周期变化和吸积双星角动量损失的经验普遍规律的测量

The Astrophysical Journal Pub Date : 2025-07-10 DOI: 10.3847/1538-4357/add925

Bradley E. Schaefer

{"title":"Evolutionary Period Changes for 25 X-Ray Binaries and the Measurement of an Empirical Universal Law for Angular Momentum Loss in Accreting Binaries","authors":"Bradley E. Schaefer","doi":"10.3847/1538-4357/add925","DOIUrl":"https://doi.org/10.3847/1538-4357/add925","url":null,"abstract":"I measure and collect timings of phase markers (like eclipse times) for the orbits of 25 X-ray binaries (XRBs) so as to calculate the steady evolutionary period change ( ). I combine these with my observed measures from 52 cataclysmic variables (CVs). Further, I subtract out the contributions from gravitational radiation ( ) and mass transfer ( ), deriving the period change from the residual unknown angular momentum loss ( = – – ). I have measures for 77 XRBs and CVs, with these being direct measures of the driver of binary evolution. The venerable magnetic braking model of binary evolution has its most fundamental predictions tested, with most systems having predictions wrong by over 1 order of magnitude. Other proposed mechanisms to explain the angular momentum loss (AML) also fail, so we are left with no known mechanism that dominates the AML. An alternative path to the AML law is empirical, where my measures are fitted to a power law involving the fundamental binary properties. With this, the dominant AML law for systems with orbital periods (P) from 0.13–1.0 day is , in appropriate units. Similar AML laws for binaries below the period gap and for binaries with P > 1.0 day are derived. These three AML laws are of good accuracy and are the best representations of the actual evolution for all 77 XRBs and CVs of all classes, so the three taken together can be called “universal.”","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"16 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144611282","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Asteroseismology of WD J004917.14−252556.81, the Most Massive Pulsating White Dwarf 最大质量脉动白矮星WD J004917.14−252556.81的星震学研究

The Astrophysical Journal Pub Date : 2025-07-10 DOI: 10.3847/1538-4357/addc70

Ozcan Caliskan, Murat Uzundag, Mukremin Kilic, Francisco C. De Gerónimo, Adam Moss, Alejandro H. Córsico, Steven G. Parsons, Ingrid Pelisoli, Gracyn Jewett, Alberto Rebassa-Mansergas, Alex J. Brown, Vikram S. Dhillon and Pierre Bergeron

{"title":"Asteroseismology of WD J004917.14−252556.81, the Most Massive Pulsating White Dwarf","authors":"Ozcan Caliskan, Murat Uzundag, Mukremin Kilic, Francisco C. De Gerónimo, Adam Moss, Alejandro H. Córsico, Steven G. Parsons, Ingrid Pelisoli, Gracyn Jewett, Alberto Rebassa-Mansergas, Alex J. Brown, Vikram S. Dhillon and Pierre Bergeron","doi":"10.3847/1538-4357/addc70","DOIUrl":"https://doi.org/10.3847/1538-4357/addc70","url":null,"abstract":"We present extensive follow-up time-series photometry of WD J0049−2525, the most massive pulsating white dwarf currently known, with Teff = 13,020 K and cm s−2. The discovery observations detected only two significant pulsation modes. Here, we report the detection of 13 significant pulsation modes ranging from 170 to 258 s based on 11 nights of observations with the New Technology Telescope, Gemini, and Apache Point Observatory telescopes. We use these 13 modes to perform asteroseismology and find that the best-fitting models (under the assumption of an ONe core composition) have M⋆ ≈ 1.29M⊙, a surface hydrogen layer mass of , and a crystallized core fraction of >99%. An analysis of the period spacing also strongly suggests a very high mass. The asteroseismic distance derived is in good agreement with the distance provided by Gaia. We also find tentative evidence of a rotation period of 0.3 or 0.67 days. This analysis provides the first look at the interior of a ∼1.3 M⊙ white dwarf.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"37 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144611075","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

Gamma-Ray Burst Jets in Circumstellar Material: Dynamics, Breakout, and Diversity of Transients 星周物质中的伽马暴喷流：动力学、爆发和瞬态的多样性

The Astrophysical Journal Pub Date : 2025-07-10 DOI: 10.3847/1538-4357/addd13

Hamid Hamidani, Kunihito Ioka, Kazumi Kashiyama and Masaomi Tanaka

{"title":"Gamma-Ray Burst Jets in Circumstellar Material: Dynamics, Breakout, and Diversity of Transients","authors":"Hamid Hamidani, Kunihito Ioka, Kazumi Kashiyama and Masaomi Tanaka","doi":"10.3847/1538-4357/addd13","DOIUrl":"https://doi.org/10.3847/1538-4357/addd13","url":null,"abstract":"Recent observations indicate that stripped-envelope core-collapse supernovae are often surrounded by dense circumstellar material (CSM). Motivated by this, we develop an analytic model to systematically study the dynamics of long gamma-ray burst (LGRB) jet propagation in various CSM environments. We derive a general expression for the jet head velocity (βh) and breakout time (tb) valid across Newtonian, relativistic, and intermediate regimes, accounting for a previously unrecognized dependence on 1 − βh. Our results highlight a fundamental distinction between jet propagation in massive stars, where βh ≪ 1, and in extended CSM, where 1 − βh ≪ 1. We establish an analytic success/failure criterion for jets and express it in terms of jet and CSM parameters, revealing a strong dependence on CSM radius. To quantify the relativistic nature of the jet-cocoon system, we introduce the energy-weighted proper velocity . We identify three possible jet outcomes—(a) successful jets ( ), (b) barely failed jets ( ), and (c) completely failed jets ( )—and constrain their respective jet/CSM parameter spaces. We show that, in (b) and (c), large CSM radii can result in luminous fast blue optical transients via cocoon cooling emission. This theoretical framework provides a basis for future observational and theoretical studies to understand the link between LGRBs, intermediate GRBs, low-luminosity LGRBs, and their environments.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"696 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144611029","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0

BatAnalysis—A Comprehensive Python Pipeline for Swift BAT Time-tagged Event Data Analysis batanalysis -一个用于Swift BAT时间标记事件数据分析的综合Python管道

The Astrophysical Journal Pub Date : 2025-07-10 DOI: 10.3847/1538-4357/ade240

Tyler Parsotan, David M. Palmer, Samuele Ronchini, James Delaunay, Aaron Tohuvavohu, Sibasish Laha, Amy Lien, S. Bradley Cenko, Hans Krimm and Craig Markwardt

{"title":"BatAnalysis—A Comprehensive Python Pipeline for Swift BAT Time-tagged Event Data Analysis","authors":"Tyler Parsotan, David M. Palmer, Samuele Ronchini, James Delaunay, Aaron Tohuvavohu, Sibasish Laha, Amy Lien, S. Bradley Cenko, Hans Krimm and Craig Markwardt","doi":"10.3847/1538-4357/ade240","DOIUrl":"https://doi.org/10.3847/1538-4357/ade240","url":null,"abstract":"The Neil Gehrels Swift Observatory (Swift) Burst Alert Telescope (BAT) is a coded aperture gamma-ray instrument with a large field of view that was designed to detect and localize transient events. When a transient is detected, either on board or externally, the BAT saves time-tagged event (TTE) data, which provide the highest-quality information of the locations of the photons on the detector plane and their energies. These data can be used to produce spectra, lightcurves, and sky images of a transient event. While these data products are produced by the Swift Data Center and can be produced by current software, they are often preset to certain time and energy intervals, which have limited their use in the current time domain and multimessenger environment. Here, we introduce a new capability for the BatAnalysis Python package to download and process TTE data under an open-source Python framework that allows for easy interfacing with other Python packages. The new capabilities of the BatAnalysis software allow for TTE data to be used by the community in a variety of advanced customized analyses of astrophysical sources which BAT may have TTE data for, such as fast radio bursts (FRBs), gamma-ray bursts (GRBs), low-mass X-ray binaries (LMXB), soft gamma repeaters, magnetars, and many other sources. We highlight the usefulness of the BatAnalysis package in analyzing TTE data produced by an onboard GRB trigger, an FRB external trigger, a subthreshold detection of the LMXB EXO 0748–676, and an external trigger of a GRB that BAT detected during a slew.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144611023","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

引用次数: 0