{"title":"Inferring Jet Physics from Neutron Star–Black Hole Mergers with Gravitational Waves","authors":"Teagan A. Clarke, Paul D. Lasky and Eric Thrane","doi":"10.3847/1538-4357/adc804","DOIUrl":"https://doi.org/10.3847/1538-4357/adc804","url":null,"abstract":"Neutron star–black hole (NSBH) mergers that undergo tidal disruption may launch jets that could power a gamma-ray burst (GRB). We use a population of simulated NSBH systems to measure jet parameters from the gravitational waves emitted by these systems. The conditions during the tidal disruption and merger phase required to power a GRB are uncertain. It is likely that the system must achieve some minimum remnant baryonic mass after the merger before a jet can be launched to power a GRB. Assuming a fiducial neutron star equation of state, we show how Bayesian hierarchical inference can be used to infer the minimum remnant mass required to launch a GRB jet as well as features of the opening angle distribution of the GRB jets. We find that with 200 NSBH observations, we can measure the minimum disk mass to within 0.01 M⊙ at 90% credibility. We simultaneously infer the GRB opening angle to within 13° at 90% credibility. We conclude that upcoming upgrades to the LIGO observatories may provide important new insights into the physics of NSBH jets.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"5 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-04-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143857504","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}
{"title":"Searching for Accreting Compact Binary Systems from Spectroscopy and Photometry: Application to LAMOST Spectra","authors":"Xinlin Zhao, Song Wang and Jifeng Liu","doi":"10.3847/1538-4357/adc1b9","DOIUrl":"https://doi.org/10.3847/1538-4357/adc1b9","url":null,"abstract":"Compact objects undergoing mass transfer exhibit significant (and double-peaked) Hα emission lines. Recently, new methods have been developed to identify black hole X-ray binaries and calculate their systematic parameters using Hα line parameters, such as the full width at half-maximum (FWHM), equivalent width (EW), and separation of double peaks. In addition, the FWHM–EW plane from spectroscopy and the Hα color–color diagram from photometry can be used for rapid stellar classification. We measure the Hα and Hβ profiles (e.g., FWHM and EW) using the LAMOST DR9 low- and medium-resolution spectra, and calculate the systematic parameters (e.g., velocity semiamplitude of the donor star, mass ratio, inclination angle, and mass of the accretor). A new correlation between FWHM and K2, K2 = 0.205(18) FWHM, is obtained for cataclysmic variables (CVs) in our sample. Both the FWHM–EW plane and the Hα color–color diagram can distinguish CVs with FWHM ≳ 1000 km s−1 from Be stars and young stellar objects to some extent. To improve classification accuracy and enhance the selection of compact objects, we propose a new set of idealized filters with effective widths of 30, 130, and 400 Å for the narrow Hα filter, broad Hα filter, and r-band filter, respectively.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"4 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-04-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143853569","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}
{"title":"Stellar β −-decay Rate of 63Ni and Its Impact on the s-process Nucleosynthesis in Massive Stars","authors":"Xin-Xu Wang, Bao-Hua Sun, Toshitaka Kajino, Zhen-Yu He, Toshio Suzuki, Dong-Liang Fang and Zhong-Ming Niu","doi":"10.3847/1538-4357/adc1be","DOIUrl":"https://doi.org/10.3847/1538-4357/adc1be","url":null,"abstract":"The β−-decay rate of 63Ni, an important branching point, affects the subsequent nucleosynthesis in the weak component of the slow-neutron capture process (weak s-process). To evaluate the impact of the uncertainties of stellar lifetime of 63Ni on abundances, we calculate the contribution to β−-decay rates from its excited states using the large-scale shell model with various interactions and also explore the atomic effects in the highly ionized plasma. In the core He burning stage and the shell C burning stage of massive stars, our new rates can be larger than those from K. Takahashi & K. Yokoi by up to a factor of 4 and 6, respectively. We evaluate the impact of the stellar decay rates of 63Ni on the nucleosynthesis of A = 60 ∼ 90 in a star with an initial mass of 25 M⊙ and solar metallicity. We find that the new rates can lead to abundance changes of 64Ni, 63Cu, 65Cu, 64Zn, 66Zn, 67Zn, and 68Zn by up to 18%, 14%, 7%, 98%, 16%, 15%, and 13%, respectively, after the shell C burning stage at the Lagrangian mass coordinate Mr = 2M⊙. The enhancement of the decay rate of 63Ni increases the weak s-process efficiency of nuclei after 65Cu.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"37 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-04-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143853570","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}
{"title":"Upper Limits on the Gamma-Ray Emission from the Microquasar V4641 Sgr","authors":"Zihao Zhao, Jian Li and Diego F. Torres","doi":"10.3847/1538-4357/adc39c","DOIUrl":"https://doi.org/10.3847/1538-4357/adc39c","url":null,"abstract":"Following a recent detection of TeV radiation by the Large High Altitude Air Shower Observatory and the High-Altitude Water Cherenkov Observatory, coincident with the direction of the microquasar V4641 Sgr, we search for possible GeV emission from this source. We explored the morphology and temporal features of the source as well as two nearby unassociated point sources, which could be a part of the extended structure of V4641 Sgr, and compared results with corresponding X-ray and TeV emissions. No significant gamma-ray signal linked to V4641 Sgr was detected in the energy range of 1–300 GeV. The 95% confidence level upper limits for the flux from the source, assuming both point and extended source models, were 5.38 × 10−13 erg cm−2 s−1 and 1.12 × 10−12 erg cm−2 s−1, respectively. Additionally, no correlation between the gamma-ray light curve and X-ray outbursts was observed.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"108 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-04-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143853269","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}
Henggeng Han, Song Wang, Xue Li, Chuanjie Zheng and Jifeng Liu
{"title":"Impact of Spectral Resolution on S-index and Its Application to Spectroscopic Surveys","authors":"Henggeng Han, Song Wang, Xue Li, Chuanjie Zheng and Jifeng Liu","doi":"10.3847/1538-4357/adc600","DOIUrl":"https://doi.org/10.3847/1538-4357/adc600","url":null,"abstract":"Utilizing the PHOENIX synthetic spectra, we investigated the impact of spectral resolution on the calculation of S-indices. We found that for spectra with a resolution lower than ≈30,000, it is crucial to calibrate S-indices for accurate estimations. This is especially essential for low-resolution spectral observations. We provided calibrations for several ongoing or upcoming spectroscopic surveys such as the LAMOST low-resolution survey, the SEGUE survey, the Sloan Digital Sky Survey-V/BOSS survey, the DESI survey, the Maunakea Spectroscopic Explorer survey, and the MUST survey. Using common targets between the HARPS and Mount Wilson Observatory (MWO) observations, we established conversions from spectral S-indices to the well-known SMWO values, applicable to stars with [Fe/H] values greater than −1. These calibrations offer a reliable approach to converting S-indices obtained from various spectroscopic surveys into SMWO values and can be widely applied in studies on chromospheric activity.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"53 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-04-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143853270","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}
{"title":"Thermal Evolution of the Plasma Sheet Region in the 2017 September 10 Solar Eruption","authors":"DeOndre Kittrell and Katharine K. Reeves","doi":"10.3847/1538-4357/adc115","DOIUrl":"https://doi.org/10.3847/1538-4357/adc115","url":null,"abstract":"We conduct detailed thermal analysis of the plasma sheet region during the post-eruption phase of a flare that occurred on 2017 September 10, examining the thermal properties as both a function of space and time. The plasma sheet that develops is best observed using the 131 Å and 193 Å filters of the Atmospheric Imaging Assembly on the Solar Dynamics Observatory. We use the differential emission measure technique to calculate the emission measure, emission measure weighted average temperature, density, and thermal energy inside the plasma sheet region. These quantities are calculated as a function time to assess how the conditions of the plasma sheet region change throughout the duration of the event. We find that there is a minimal decrease in the temperature as the plasma sheet region evolves. The total thermal energy in the plasma sheet is on the order of 1.5–3.0 1029 erg for the first 1.5 hr of the eruption and then decreases. For the first time for this event, we examine the conductive and radiative loss rates, which indicate rapid cooling should be expected, contradicting the temperature results. These findings suggest that there are underlying mechanisms such as adiabatic heating and/or turbulence-induced suppression of conduction that contribute to the sustained hot conditions in the plasma sheet.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"33 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-04-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143853568","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}
Mingjun Liu, Yijia Zhang, Yun Wang, Rui Xue, David Buckley, D. Andrew Howell, Chichuan Jin, Wenxiong Li, Itumeleng Monageng, Haiwu Pan, Ning-Chen Sun, Samaporn Tinyanont, Lingzhi Wang, Weimin Yuan, Jie An, Moira Andrews, Rungrit Anutarawiramkul, Pathompong Butpan, Yong Chen, Huaqing Cheng, Weiwei Cui, Cui-Yuan Dai, Lixin Dai, Joseph Farah, Hua Feng, Shaoyu Fu, Zhen Guo, Shumei Jia, Shuaiqing Jiang, An Li, Chengkui Li, Dongyue Li, Tianying Lian, Yifang Liang, Heyang Liu, Xing Liu, Yuan Liu, Jirong Mao, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Xin Pan, Xinxiang Sun, Giacomo Terreran, Ze-Rui Wang, Qinyu Wu, Hubing Xiao, Dingrong Xiong, Dong Xu, Xinpeng Xu, Suijian Xue, Haonan Yang, Jun Yang, Jin Zhang, Wenda Zhang, Wenjie Zhang and Hu Zou
{"title":"Detection of an Orphan X-Ray Flare from a Blazar Candidate EP240709a with the Einstein Probe","authors":"Mingjun Liu, Yijia Zhang, Yun Wang, Rui Xue, David Buckley, D. Andrew Howell, Chichuan Jin, Wenxiong Li, Itumeleng Monageng, Haiwu Pan, Ning-Chen Sun, Samaporn Tinyanont, Lingzhi Wang, Weimin Yuan, Jie An, Moira Andrews, Rungrit Anutarawiramkul, Pathompong Butpan, Yong Chen, Huaqing Cheng, Weiwei Cui, Cui-Yuan Dai, Lixin Dai, Joseph Farah, Hua Feng, Shaoyu Fu, Zhen Guo, Shumei Jia, Shuaiqing Jiang, An Li, Chengkui Li, Dongyue Li, Tianying Lian, Yifang Liang, Heyang Liu, Xing Liu, Yuan Liu, Jirong Mao, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Xin Pan, Xinxiang Sun, Giacomo Terreran, Ze-Rui Wang, Qinyu Wu, Hubing Xiao, Dingrong Xiong, Dong Xu, Xinpeng Xu, Suijian Xue, Haonan Yang, Jun Yang, Jin Zhang, Wenda Zhang, Wenjie Zhang and Hu Zou","doi":"10.3847/1538-4357/adc301","DOIUrl":"https://doi.org/10.3847/1538-4357/adc301","url":null,"abstract":"Blazars are often observed to flare across multiple wavelengths. Orphan flares from blazars have only been detected a few times, providing an opportunity to understand the structure of the jet in the accreting system. We report a remarkable orphan X-ray flare from a blazar candidate EP240709a, detected by the Einstein Probe (EP) in July 2024. The multiband spectral properties and variability support EP240709a as a high-energy peaked BL Lacertae-type object. The flux in 0.5–10 keV increased by at least 28 times to the value of low state in 2020, with no significant flaring detected in other bands during the same period. EP240709a exhibits the harder-when-brighter tendency in the X-ray band during the orphan flare, while its infrared-optical spectra are featureless. We employ one-zone and two-zone leptonic synchrotron self-Compton models to perform the spectral energy distribution fitting. Detecting this rare orphan flare shows the potential of EP in discovering peculiar activities from AGN in high-cadence X-ray sky surveys.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"11 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-04-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143853267","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}
Jessie C. Runnoe, Michael Eracleous, Tamara Bogdanović, Jules P. Halpern and Steinn Sigurđsson
{"title":"A Large Systematic Search for Close Supermassive Binary and Rapidly Recoiling Black Holes. IV. Ultraviolet Spectroscopy* †","authors":"Jessie C. Runnoe, Michael Eracleous, Tamara Bogdanović, Jules P. Halpern and Steinn Sigurđsson","doi":"10.3847/1538-4357/adba58","DOIUrl":"https://doi.org/10.3847/1538-4357/adba58","url":null,"abstract":"We present Hubble Space Telescope ultraviolet (UV) spectroscopy of 13 quasars at z < 0.7, along with contemporaneous optical spectra from ground-based telescopes. The targets were selected to have broad Hβ emission lines with substantial velocity offsets relative to the rest frame of their host galaxy. By analogy to single-line spectroscopic binary stars, these objects have been regarded as supermassive black hole binary (SBHB) candidates where the offset emission lines may be caused by bulk orbital motion. The best alternative explanation is that the Hβ line profile is the result of nonaxisymmetric emission from a disk-like broad-line region associated with a single supermassive black hole. We use the broad UV line profiles to discriminate between these two scenarios. We describe our methodology for isolating the broad optical and UV line profiles and the criteria we apply for comparing them. Of the 13 SBHB candidates, three have strong evidence in support of the SBHB hypothesis, five have tentative support, one is disfavored, and four have such severely absorbed UV line profiles that the results are inconclusive.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"11 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-04-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143853561","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}
Dong Yang, 冬 杨, Jing Wang, 菁 王, Zhijie Qu, 稚杰 屈, Zezhong Liang, 泽众 梁, Xuchen Lin, 旭辰 林, Simon Weng, Xinkai Chen, 新凯 陈, Barbara Catinella, Luca Cortese, D. B. Fisher, Luis C. Ho, 子山 何, Yingjie Jing, 英杰 景, Fangzhou Jiang, 方周 姜, Peng Jiang, 鹏 姜, Ziming Liu, 孜铭 刘, Céline Péroux, Li Shao, 立 邵, Lister Staveley-Smith, Q. Daniel Wang, Jie Wang and 杰 王
{"title":"FEASTS Combined with Interferometry. IV. Mapping H i Emission to a Limit of N H i = 1017.7 cm−2 in Seven Edge-on Galaxies","authors":"Dong Yang, 冬 杨, Jing Wang, 菁 王, Zhijie Qu, 稚杰 屈, Zezhong Liang, 泽众 梁, Xuchen Lin, 旭辰 林, Simon Weng, Xinkai Chen, 新凯 陈, Barbara Catinella, Luca Cortese, D. B. Fisher, Luis C. Ho, 子山 何, Yingjie Jing, 英杰 景, Fangzhou Jiang, 方周 姜, Peng Jiang, 鹏 姜, Ziming Liu, 孜铭 刘, Céline Péroux, Li Shao, 立 邵, Lister Staveley-Smith, Q. Daniel Wang, Jie Wang and 杰 王","doi":"10.3847/1538-4357/adbbe8","DOIUrl":"https://doi.org/10.3847/1538-4357/adbbe8","url":null,"abstract":"We present a statistical study of the neutral atomic hydrogen (H i) gas extending into the circumgalactic medium perpendicular to the disk for seven edge-on galaxies with inclinations above 85° from the FEASTS program with a 3σ (20 km s−1 ) column density (NH i ) depth of 5 × 1017 cm−2. We develop two photometric methods to separate the extraplanar H i from the disk component based on existing interferometric data and parametric modeling of the disk flux distribution, respectively. With both methods, the FEASTS data exhibit clear extended wings beyond the disk along the minor axis. The extraplanar H i accounts for 5%–20% of the total H i mass and extends to 20–50 kpc at NH i = 1018cm−2 . We find a tight positive correlation between vertical extensions of the extraplanar H i and total H i mass MH i. The isodensity shape of H i at NH i = 1018 cm−2 has an average axis ratio of 0.56 ± 0.11. The off-disk NH i profiles of these edge-on galaxies well represent the lower envelope of previous Lyα absorption measurements at low redshift. Our results suggest that at NH i = 5 × 1017 cm−2, the H i extends considerably further than the known thin and thick disks in the vertical direction but still remains much flatter than a spherical distribution, consistent with theoretical expectations that outflow, circulation, and accretion should have different impacts in these two directions. We show the tension of our results with Illustris and TNG predictions, highlighting the constraining power of our results for future simulations.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"49 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-04-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143853563","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}
{"title":"The Observations of Magnetic Reconnection during the Interaction Process of Two Active Region Filaments","authors":"Zongyin Wu, Zhike Xue, Xiaoli Yan, Jincheng Wang, Liheng Yang, Zhe Xu, Qiaoling Li, Yang Peng, Liping Yang, Yian Zhou, Xinsheng Zhang, Liufan Gong, Qifan Dong and Guotang Wu","doi":"10.3847/1538-4357/adc377","DOIUrl":"https://doi.org/10.3847/1538-4357/adc377","url":null,"abstract":"We investigate the interaction between two filaments (F1 and F2) and their subsequent magnetic reconnection in active region (AR) NOAA 13296 and AR NOAA 13293 on 2023 May 9, utilizing high spatial and temporal resolution and multiwavelength observational data from the Solar Dynamics Observatory, the New Vacuum Solar Telescope, and the Chinese Hα Solar Explorer. The movement of F1 from the southeast toward the northwest, driven by the motion of the positive magnetic polarity (P1), leads to a collision and reconnection with F2. This reconnection exchanges their footpoints, resulting in the formation of two new filaments (F3 and F4) consistent with “slingshot” type filament interaction. During the interaction, the current sheet, moving due to the motion of F1, and the reconnection outflows, moving along F3 and F4, were both observed. The current sheet is rarely observed in the slingshot type filament interaction, measuring approximately 2.17 Mm in length and 0.84 Mm in width. After the interaction, the F1 disappears, whereas a portion of F2 remains, indicating that the interaction involves partial slingshot reconnection, due to the unequal magnetic flux between the filaments. The residual part of F2 will undergo another magnetic reconnection in the same interaction region with the magnetic loops connecting polarities N1 and P1. The material generated by the reconnection is continuously injected into F4, leading to its final morphology. The findings enhance our understanding of slingshot-type filament interactions, indicating that partial slingshot reconnections between filaments may be more common than full slingshot events.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"28 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-04-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143853268","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}
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