The Astrophysical Journal Letters最新文献

{"title":"The Atomic Gas Properties of Green Pea Galaxies: Connections to Lyman Continuum Leakage","authors":"Archishman Khasnovis, Nissim Kanekar, Sangeeta Malhotra and James Rhoads","doi":"10.3847/2041-8213/ae0464","DOIUrl":"https://doi.org/10.3847/2041-8213/ae0464","url":null,"abstract":"We have used the Green Bank Telescope to search for H i 21 cm emission from 30 Green Pea galaxies (GPs) at z ≈ 0.012–0.045, obtaining 7 detections of H i 21 cm emission and 17 upper limits on the H i mass. Including GPs from the literature, we obtain a sample of 60 GPs at z < 0.05, with 19 detections and 41 nondetections of H i 21 cm emission and with stellar masses in the range 106–109M⊙. We use the line luminosity ratio O32 ≡ [O iii]λ5007 + λ4959/[O ii]λ3727,3729 as an indicator of Lyman continuum (LyC) leakage and examine the dependence of the H i properties of the 60 GPs on the O32 ratio. We obtain a far higher H i 21 cm detection rate ( %) for the 32 GPs with O32 < 10 than that ( %) for the 28 GPs with O32 > 10. We find statistically significant evidence that the H i mass, the H i-to-stellar mass ratio, and the H i gas depletion timescale of GPs with O32 > 10 are lower than the corresponding values for GPs with O32 < 10. Earlier studies have shown that galaxies with O32 > 10 tend to show significant LyC leakage: our results indicate that this is due to the lack of H i in such galaxies, with most of the H i consumed in the starburst. Our results further suggest that H i 21 cm studies of the galaxies that reionized the Universe at z ≳ 6 are likely to find an anticorrelation between the H i 21 cm and Lyα emission signals, due to the paucity of H i in the strongest LyC and Lyα leakers.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"22 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-09-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145077781","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":"Sub-Neptunes Are Drier than They Seem: Rethinking the Origins of Water-rich Worlds","authors":"Aaron Werlen, Caroline Dorn, Remo Burn, Hilke E. Schlichting, Simon L. Grimm and Edward D. Young","doi":"10.3847/2041-8213/adff73","DOIUrl":"https://doi.org/10.3847/2041-8213/adff73","url":null,"abstract":"Recent claims of biosignature gases in sub-Neptune atmospheres have renewed interest in water-rich sub-Neptunes with surface oceans, often referred to as Hycean planets. These planets are hypothesized to form beyond the snow line, accreting large amounts of H2O (>10 wt%) before migrating inward. However, current interior models often neglect chemical equilibration between primordial atmospheres and molten interiors. Here, we compute global chemical equilibrium states for a synthetic population of sub-Neptunes with magma oceans. Although many initially accrete 5–30 wt% water, interior–atmosphere interactions destroy most of it, reducing final H2O mass fractions to below 1.5 wt%. As a result, none meet the threshold for Hycean planets. Despite that, we find H2O-dominated atmospheres exclusively on planets that accreted the least ice. These planets form inside the snow line, are depleted in carbon and hydrogen, and develop small envelopes with envelope mass fractions below 1%, dominated by endogenic water. In contrast, planets formed beyond the snow line accrete more volatiles, but their water is largely converted to H2 gas or sequestered into the interior, resulting in low atmospheric H2O mass fractions. Most H2O-rich envelopes are also fully miscible with H2, making a separate water layer unlikely. Our results challenge the conventional link between ice accretion and water-rich atmospheres, showing instead that H2O-dominated envelopes emerge through chemical equilibration in hydrogen-poor planets formed inside the snow line.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"16 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-09-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145077714","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 Mass–Dispersion Measure Correlations Constrain Baryonic Feedback in Fast Radio Burst Host Galaxies","authors":"Calvin Leung, Sunil Simha, Isabel Medlock, Daisuke Nagai, Kiyoshi W. Masui, Lordrick A. Kahinga, Adam E. Lanman, Shion Andrew, Kevin Bandura, Alice P. Curtin, B. M. Gaensler, Nina Gusinskaia, Ronniy C. Joseph, Mattias Lazda, Lluis Mas-Ribas, Bradley W. Meyers, Kenzie Nimmo, Aaron B. Pearlman, J. Xavier Prochaska, Mawson W. Sammons, Kaitlyn Shin, Kendrick Smith, Haochen Wang and (CHIME/FRB Collaboration)","doi":"10.3847/2041-8213/ae044d","DOIUrl":"https://doi.org/10.3847/2041-8213/ae044d","url":null,"abstract":"Low-redshift fast radio bursts (FRBs) enable robust measurements of the host galaxy contribution to the dispersion measure (DM), offering valuable constraints on the circumgalactic medium (CGM) of FRB hosts. We curate a sample of 20 nearby FRBs with low scattering timescales and face-on host galaxies with stellar masses in the range 109 < M*/M⊙ < 1011. We fit the distribution of the host galaxy DM to a quadratic model as a function of stellar mass with a mass-independent scatter and find that the more massive the host, the lower its host DM. We report that this relation has a negative slope of m = −97 ± 44 pc cm−3 dex−1 in stellar mass. We compare this measurement against similar fits to three subgrid models implemented in the CAMELS suite of simulations from Astrid, IllustrisTNG, and SIMBA, which predict the CGM contribution to this relation, finding disagreement with the fiducial CAMELS-Astrid model, particularly for the most massive hosts (M* > 1010.5M⊙). More generally, models that attribute a positive correlation between stellar mass and host DM (m > 0) to the CGM are in tension with our measurement unless compensated by fine-tuning of the host interstellar medium contribution as a function of stellar mass, e.g., at the low-mass end. We show that this conclusion is robust to a wide range of assumptions, such as the offset distribution of FRBs from their hosts and the statistics of the cosmic contribution to the DM budget along each sight line. Our results indirectly imply a lower limit on the strength of baryonic feedback in the local Universe (z < 0.2) in isolated ∼L* halos, complementing results from weak-lensing surveys and kSZ observations that target higher halo mass and redshift ranges.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"38 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-09-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145077718","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":"A Deep VLA Search for a Persistent Radio Counterpart to the One-off FRB 20250316A","authors":"Tao An, Ailing Wang, Yu-Chen Huang, Jia-Pei Feng, Yuanqi Liu, Zhongli Zhang and Zi-Gao Dai","doi":"10.3847/2041-8213/ae0324","DOIUrl":"https://doi.org/10.3847/2041-8213/ae0324","url":null,"abstract":"Fast radio burst (FRB) 20250316A, detected by CHIME on 2025 March 16 with a fluence of 1.7 ± 0.1 kJy ms and a dispersion measure of 161.3 ± 0.4 pc cm−3, ranks among the brightest extragalactic FRBs at ∼40 Mpc. We obtain deep Karl G. Jansky Very Large Array follow-up at 15 GHz on 2025 April 5 and 9 and find no persistent radio source (PRS). Our best image reaches an rms of 2.8 μJy beam−1, yielding a 3σ upper limit of <8.4 μJy at the FRB position, corresponding to νLν < 2.4 × 1035 erg s−1. These results represent among the most stringent constraints for a nonrepeating FRB, lying ≳3 orders of magnitude below the νLν of compact PRSs around well-studied repeaters, thereby disfavoring bright magnetar-nebula scenarios and pointing to low-density, weakly magnetized environments. Interpreting our limit through pulsar-/magnetar-wind synchrotron frameworks places joint constraints on ambient density and engine power. If the empirical PRS–rotation-measure trend reported for repeaters extends to one-off sources, our limit implies ∣RM∣ ≲ 30 rad m−2, consistent with a clean magnetoionic sight line and progenitor channels such as neutron-star mergers or giant flares from older magnetars.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"37 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-09-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145077717","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":"Born Dry or Born Wet? A Palette of Water Growth Histories in TRAPPIST-1 Analogs and Compact Planetary Systems","authors":"Howard Chen, Matthew S. Clement, Le “Chris” Wang and Jesse T. Gu","doi":"10.3847/2041-8213/adf282","DOIUrl":"https://doi.org/10.3847/2041-8213/adf282","url":null,"abstract":"It is still unclear whether exoplanets in compact multiplanet systems such as TRAPPIST-1 are able to accrete large quantities of volatiles, grow to sufficient mass, and maintain robust atmospheres and hydrospheres. Previous estimates of water content in M-dwarf systems have largely relied on population synthesis or atmosphere–interior evolution models, often treating impacts and atmospheric loss in isolation. In this work, we combined impact delivery, impact erosion, and mantle-atmosphere exchange within a unified framework that tracks volatile evolution through stochastic collision histories. By explicitly including both planetesimal accretion and the prolonged luminous pre-main-sequence phase of M dwarfs, we find systematically lower water inventories for the inner TRAPPIST-1 analogs (b–e), spanning only 10−4 and 1% of Earth’s ocean mass across a wide range of disk structures and impact scenarios. By contrast, the outer planets (f–h analogs) frequently retain water inventories exceeding an Earth ocean mass. This volatile gradient provides a physically motivated explanation for JWST’s nondetections of atmospheres on TRAPPIST-1 b and c, suggesting an origin rooted in rocky planet formation. Our results suggest that many rocky planets in compact M-dwarf systems may form already depleted in volatile compounds, fundamentally limiting their capacity to sustain atmospheres or surface oceans. More broadly, our multistage framework for volatile tracking can help interpret future observations of compact system and set more realistic initial conditions for exoplanet interior compositions and atmospheric models.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"29 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-09-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145072816","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":"Weakened Magnetic Braking Signals the Collapse of the Global Stellar Dynamo","authors":"Travis S. Metcalfe, Jennifer L. van Saders, Marc H. Pinsonneault, Thomas R. Ayres, Oleg Kochukhov, Keivan G. Stassun, Adam J. Finley, Victor See, Ilya V. Ilyin and Klaus G. Strassmeier","doi":"10.3847/2041-8213/ae03bc","DOIUrl":"https://doi.org/10.3847/2041-8213/ae03bc","url":null,"abstract":"Weakened magnetic braking (WMB) was originally proposed in 2016 to explain anomalously rapid rotation in old field stars observed by the Kepler mission. The proximate cause was suggested to be a transition in magnetic morphology from larger to smaller spatial scales. In a series of papers over the past 5 yr, we have collected spectropolarimetric measurements to constrain the large-scale magnetic fields for a sample of stars spanning this transition, including a range of spectral types from late F to early K. During this time, we gradually improved our methods for estimating the wind braking torque in each of our targets, and for evaluating the associated uncertainties. Here, we reanalyze the entire sample with a focus on uniformity for the relevant observational inputs. We supplement the sample with two additional active stars to provide more context for the evolution of wind braking torque with stellar Rossby number (Ro). The results demonstrate unambiguously that standard spin-down models can reproduce the evolution of wind braking torque for active stars, but WMB is required to explain the subsequent abrupt decrease in torque as Ro approaches a critical value for dynamo excitation. This transition is seen in both the large-scale magnetic field and the X-ray luminosity, indicating weakened coronal heating. We interpret these transitions as evidence of a rotational threshold for the influence of Coriolis forces on global convective patterns and the resulting inefficiency of the global stellar dynamo.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"35 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-09-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145068144","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":"Discovery of the Antiglitch in PSR J1835-1106","authors":"Mingyang Wang, Peng Liu, Jianping Yuan, Ang Li, Youli Tuo, Shijun Dang, Weihua Wang, Mingyu Ge, Xia Zhou and Na Wang","doi":"10.3847/2041-8213/ae0188","DOIUrl":"https://doi.org/10.3847/2041-8213/ae0188","url":null,"abstract":"We report the detection of an antiglitch with a fractional frequency change of Δν/ν = −3.46(6) × 10−9 in the rotation-powered pulsar PSR J1835−1106 at MJD 55813(9), based on timing observations collected with the Nanshan 26 m and Parkes 64 m radio telescopes from 2000 January to 2022 July. A comparison of the average pulse profiles within ±300 days of the event reveals no significant morphological changes. We also estimate the angular velocity lag between the normal and superfluid components at the time of the glitch, showing that one of the superfluid glitch models is incompatible with PSR J1835−1106 due to its insufficient spin-down rate and angular velocity lag. The wind braking scenario offers a viable alternative, consistent with the observed spin-down behavior, glitch amplitude, and postglitch recovery. High-cadence, high-sensitivity monitoring of similar events is essential to distinguish between internal (superfluid) and external (wind-related) glitch mechanisms.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"2020 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-09-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145068145","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 Gravitational-wave Background from Massive Black Holes in the ASTRID Simulation","authors":"Nianyi Chen, Tiziana Di Matteo, Yihao Zhou, Luke Zoltan Kelley, Laura Blecha, Yueying Ni, Simeon Bird, Yanhui Yang and Rupert Croft","doi":"10.3847/2041-8213/adefe2","DOIUrl":"https://doi.org/10.3847/2041-8213/adefe2","url":null,"abstract":"Recent pulsar timing array (PTA) observations detected nanohertz gravitational waves, likely originating from massive black hole binaries (MBHBs). The detected amplitude is unexpectedly higher than inferred from the electromagnetic measurements. We present new gravitational-wave background (GWB) results from the ASTRID simulation. Its large volume and on-the-fly dynamics for massive black holes (MBHs) provide new insights into the MBHB population, offering a more accurate assessment of its contribution to the observed GWB. ASTRID predicts a GWB from MBHBs of hc = 2.8 × 10−15, or ∼45% of the observed amplitude at ∼4 nHz with a slope consistent with f−2/3, and hc = 2.5 × 10−16 with hc ∝ f−1.6 at ∼30 nHz. These predictions remain below current PTA constraints but align with empirical models based on the observed MBH mass functions. By comparison, TNG300 with postprocessed MBH dynamics yields a range between 70% and 90% (20% and 30%) of the observed levels at low (high) frequencies. At low frequencies, ASTRID predicts that the bulk of the GWB originates from MBHBs with masses Mtot = 1–3 × 109M⊙ peaking at z ≈ 0.3, consistent with TNG300. Notably, both simulations predict significant contributions from minor mergers (q < 0.2) by up to ∼40%. By tracing the full merger trees of local MBHs in ASTRID, we show that they generate gravitational waves at ∼10%–80% of the maximum signal assuming no accretion and recent equal-mass mergers. Finally, we demonstrate the importance of on-the-fly MBH dynamics, the lack of which leads to 3–5 times excessive mass growth by merger, and a boost to the GWB prediction from this overestimated mass function, especially at high frequencies.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"81 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-09-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145072492","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":"A Magnetic White Dwarf Formed through a Binary Merger within 35 Million Yr","authors":"Huahui Yan, Jiamao Lin, Rizhong Zheng, Li Wang, Genghao Liu, Liangliang Ren, Zhen Guo, Siyi Xu, Zhangliang Chen, Chun Chen, Bo Ma, Yong Shao, Zhenwei Li, Xianfei Zhang, Christoffer Fremling, Jan J. Eldridge, Hongwei Ge and Chengyuan Li","doi":"10.3847/2041-8213/adfec2","DOIUrl":"https://doi.org/10.3847/2041-8213/adfec2","url":null,"abstract":"White dwarfs (WDs) represent the final evolutionary stage of most stars, typically originating from progenitor stars with masses below approximately 8–10 M⊙. Formation through single-star evolution generally requires at least 25 Myr, with the youngest WDs often near the Chandrasekhar limit of 1.4 M⊙. In contrast, WDs formed via binary channels, such as mergers or mass transfer, can develop smaller masses in a shorter timescale and may exhibit unique characteristics, including strong surface magnetic fields and rapid rotation. Accurately determining the ages of these WDs is essential for understanding their formation. A valuable method involves studying WDs in star clusters, where member stars share the same age and chemical composition, allowing for precise constraints on the formation times and metallicities of the WDs’ progenitors. Here we report a WD found in the open cluster RSG 5, which is only 35 Myr old. The WD’s mass is lower than 1.05 M⊙, indicating it may not have formed through single-star evolution. The WD possesses an exceptionally strong surface magnetic field (≥200 MG), a short rotational period (∼6.5 minutes), and, most notably, a corotating half-ring of ionized circumstellar debris. This distinctive feature provides evidence for a binary merger origin, a scenario further substantiated by our stellar evolution models.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"32 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-09-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145059509","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":"Pinching of ICME Flux Rope: Unprecedented Multipoint Observations of Internal Magnetic Reconnection during Gannon’s Superstorm","authors":"Shibotosh Biswas, Ankush Bhaskar, Anil Raghav, Ajay Kumar, Kalpesh Ghag, Smitha V. Thampi and Vipin K Yadav","doi":"10.3847/2041-8213/adfe60","DOIUrl":"https://doi.org/10.3847/2041-8213/adfe60","url":null,"abstract":"The extreme solar storm of 2024 May 10, during the 25th solar cycle, which recorded a symmetric H component index (Sym-H) reaching −500 nT, was the strongest since the 2003 Halloween storm. This event offered a unique opportunity for unprecedented multipoint observation of the complex interaction of interplanetary coronal mass ejections (ICMEs) from different vantage points. Utilizing NASA’s Wind, ACE, DSCOVR, THEMIS-C, STEREO-A, MMS, and ISRO’s recently launched Aditya-L1 spacecraft, we comprehensively investigated the spatiotemporal variations in interplanetary plasma and magnetic field parameters. Our study reveals large-scale quasi-steady magnetic reconnection within the interior of the ICME flux rope, possibly triggered by interactions between multiple ICMEs. A current sheet (CS) forms within the flux rope, enabling internal magnetic reconnection between concentric magnetic surfaces, which leads to a sharp reversal of the interplanetary magnetic field (IMF) By component, as observed at the L1 point. Concurrently, reconnection exhaust and enhanced electron and ion fluxes were detected with the CS, extending over 200 RE (1.3 million kilometers) along the geocentric solar ecliptic y-direction. This finding sheds new light on the role of internal reconnection in ICME evolution, highlighting its pivotal role in modifying the morphology of the ICME magnetic structure and exerting severe space weather effects on Earth.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"36 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-09-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145059508","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}