Monthly Notices of the Royal Astronomical Society最新文献_第7页

Correction to: X-ray polarization properties of partially ionized equatorial obscurers around accreting compact objects 更正为吸积紧凑天体周围部分电离赤道遮挡层的X射线偏振特性

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-04-05 DOI: 10.1093/mnras/stae843

引用次数: 0

Carbon- and Oxygen-rich stars in MaStar: identification and classification MaStar中的富碳和富氧恒星：识别和分类

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-04-04 DOI: 10.1093/mnras/stae919

L. Hill, C. Maraston, Daniel Thomas, R. Yan, Yanping Chen, G. Stringfellow, Richard R. Lane, J. G. Fernández-Trincado

{"title":"Carbon- and Oxygen-rich stars in MaStar: identification and classification","authors":"L. Hill, C. Maraston, Daniel Thomas, R. Yan, Yanping Chen, G. Stringfellow, Richard R. Lane, J. G. Fernández-Trincado","doi":"10.1093/mnras/stae919","DOIUrl":"https://doi.org/10.1093/mnras/stae919","url":null,"abstract":"\u0000 Carbon- and Oxygen-rich stars populating the Thermally-Pulsing Asymptotic Giant Branch (TP-AGB) phase of stellar evolution are relevant contributors to the spectra of ∼1 Gyr old populations. Atmosphere models for these types are uncertain, due to complex molecules and mass-loss effects. Empirical spectra are then crucial, but samples are small due to the short (∼3 Myr) TP-AGB lifetime. Here we exploit the vastness of the MaNGA Stellar library MaStar (∼60, 000 spectra) to identify C,O-rich type stars. We define an optical colour selection with cuts of (g − r) > 2 and (g − i) < 1.55(g − r) − 0.07, calibrated with known C- and O- rich spectra. This identifies C-,O-rich stars along clean, separated sequences. An analogue selection is found in V, R, I bands. Our equation identifies C-rich and O-rich spectra with predictive performance metric F1-scores of 0.72 and 0.74 (over 1), respectively. We finally identify 41 C- and 87 O-rich type AGB stars in MaStar, 5 and 49 of which do not have a SIMBAD counterpart. We also detect a sample of non-AGB, dwarf C-stars. We further design a fitting procedure to classify the spectra into broad spectral types, by using as fitting templates empirical C and O-rich spectra. We find remarkably good fits for the majority of candidates and categorise them into C- and O-rich bins following existing classifications, which correlate to effective temperature. Our selection models can be applied to large photometric surveys (e.g. Euclid, Rubin). The classified spectra will facilitate future evolutionary population synthesis models.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"71 3","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140741689","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

The viability of low-mass subhaloes as targets for gamma-ray dark matter searches 低质量子晕作为伽马射线暗物质搜索目标的可行性

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-04-04 DOI: 10.1093/mnras/stae940

A. Aguirre-Santaella, M. Sánchez-Conde

{"title":"The viability of low-mass subhaloes as targets for gamma-ray dark matter searches","authors":"A. Aguirre-Santaella, M. Sánchez-Conde","doi":"10.1093/mnras/stae940","DOIUrl":"https://doi.org/10.1093/mnras/stae940","url":null,"abstract":"\u0000 In this work, we investigate the discovery potential of low-mass Galactic dark matter (DM) subhaloes for indirect searches of DM. We use data from the Via Lactea II (VL-II) N-body cosmological simulation, which resolves subhaloes down to $mathcal {O}(10^4)$ solar masses and it is thus ideal for this purpose. First, we characterize the abundance, distribution and structural properties of the VL-II subhalo population in terms of both subhalo masses and maximum circular velocities. Then, we repopulate the original simulation with millions of subhaloes of masses down to about five orders of magnitude below the minimum VL-II subhalo mass (more than one order of magnitude in velocities). We compute subhalo DM annihilation astrophysical ‘J-factors’ and angular sizes for the entire subhalo population, by placing the Earth at a random position but at the right galactocentric distance in the simulation. Thousands of these realizations are generated in order to obtain statistically meaningful results. We find that some nearby low-mass Galactic subhaloes, not massive enough to retain stars or gas, may indeed yield DM annihilation fluxes comparable to those expected from other, more massive and acknowledgeable DM targets like dwarf satellite galaxies. Typical angular sizes are of the order of the degree, thus subhaloes potentially appearing as extended sources in gamma-ray telescopes, depending on instrument angular resolution and sensitivity. Our work shows that low-mass Galactic subhaloes with no visible counterparts are expected to play a relevant role in current and future indirect DM search searches and should indeed be considered as excellent DM targets.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"25 4","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140743029","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

New Herbig-Haro Objects associated with Embedded Sources 与嵌入式源相关的新赫比格-哈罗对象

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-04-03 DOI: 10.1093/mnras/stae948

T. Movsessian, T. Magakian, B. Reipurth, H. Andreasyan

{"title":"New Herbig-Haro Objects associated with Embedded Sources","authors":"T. Movsessian, T. Magakian, B. Reipurth, H. Andreasyan","doi":"10.1093/mnras/stae948","DOIUrl":"https://doi.org/10.1093/mnras/stae948","url":null,"abstract":"\u0000 We continue to present the results of the Byurakan Narrow Band Imaging Survey (BNBIS). The main goal of this survey is to search for Herbig-Haro (HH) objects and jets in Galactic dark clouds. In this work we present the results of the search in the vicinity of infrared sources that are bright in the WISE survey and embedded in the dark clouds. The survey is performed with the 1 m Schmidt telescope of Byurakan Observatory, lately equipped with a new CCD detector, which allows to obtain one square degree images of the sky in various filters. Narrow-band filters were used to obtain Hα and [S ii] images, and a medium-width filter was used for the continuum imaging. New HH flows and knots were found near six embedded IR sources, which constitutes a significant proportion of the objects observed. At least two of the newly found HH flows (HH 1226 and HH 1227) lie in isolated dark clouds, thus pointing to active star formation in these regions. Other flows are also located in detached and dense globules or filaments. The length of the HH 1228 flow is about 1 pc; it has also a molecular hydrogen counterpart of the same extension. Coordinates, charts, detailed descriptions and distance estimates are provided. The lower limits of bolometric luminosities of the source stars are typical for low-mass young stellar objects.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"335 2","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140750096","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

xGASS: The scatter of the H i-halo mass relation of central galaxies xGASS：中心星系H i-光质量关系的散布

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-04-03 DOI: 10.1093/mnras/stae942

Manasvee Saraf, Luca Cortese, O. I. Wong, B. Catinella, S. Janowiecki, Jennifer A. Hardwick

{"title":"xGASS: The scatter of the H i-halo mass relation of central galaxies","authors":"Manasvee Saraf, Luca Cortese, O. I. Wong, B. Catinella, S. Janowiecki, Jennifer A. Hardwick","doi":"10.1093/mnras/stae942","DOIUrl":"https://doi.org/10.1093/mnras/stae942","url":null,"abstract":"\u0000 Empirical studies of the relationship between baryonic matter in galaxies and the gravitational potential of their host halos are important to constrain our theoretical framework for galaxy formation and evolution. One such relation, between the atomic hydrogen (H i) mass of central galaxies (MHI, c) and the total mass of their host halos (Mhalo), has attracted significant interest in the last few years. In this work, we use the extended GALEX Arecibo SDSS Survey to examine the scatter of the H i-halo mass relation for a representative sample of central galaxies. Our findings reveal a flat median relation at $rm {log}_{10}, (M_{rm {HI,c}}/rm {M}_{odot }) approx 9.40$, across $11.1 < rm {log}_{10}, (M_{rm {halo}}/{{rm M}_{odot }}) < 14.1$. This flat relation stems from the statistical dominance of star-forming, disc galaxies at low Mhalo in combination with the increasing prevalence of passive, high stellar-concentration systems at higher Mhalo. The scatter of this relation and the stellar specific angular momentum of centrals have a strong link (Spearman’s rank correlation coefficient ≥0.5). Comparisons with simulations suggest that the kinematic state of host halos may be primarily driving this scatter. Our findings highlight that the H i-halo mass parameter space is too complex to be completely represented by simple median or average relations and we show that tensions with previous works are most likely due to selection biases. We recommend that future observational studies, and their comparisons with theoretical models, bin central galaxies also by their secondary properties to enable a statistically robust understanding of the processes regulating the cold gas content within central galaxies of dark-matter halos.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"121 3","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140747122","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

Unveiling energy pathways in AGN accretion flows with the warm corona model for the soft excess 用软过量的暖日冕模型揭示 AGN 吸积流的能量路径

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-04-03 DOI: 10.1093/mnras/stae944

D. Ballantyne, V. Sudhakar, D. Fairfax, S. Bianchi, B. Czerny, A. De Rosa, B. de Marco, R. Middei, B. Palit, P. Petrucci, A. Różańska, F. Ursini

{"title":"Unveiling energy pathways in AGN accretion flows with the warm corona model for the soft excess","authors":"D. Ballantyne, V. Sudhakar, D. Fairfax, S. Bianchi, B. Czerny, A. De Rosa, B. de Marco, R. Middei, B. Palit, P. Petrucci, A. Różańska, F. Ursini","doi":"10.1093/mnras/stae944","DOIUrl":"https://doi.org/10.1093/mnras/stae944","url":null,"abstract":"\u0000 The soft excess in active galactic nuclei (AGNs) may arise through a combination of relativistic reflection and the effects of a warm corona at the surface of the accretion disc. Detailed examination of the soft excess can therefore constrain models of the transport and dissipation of accretion energy. Here, we analyze 34 XMM-Newton observations from 14 Type I AGNs with the reXcor spectral model which self-consistently combines emission from a warm corona with relativistic reflection assuming a lamppost corona. The model divides accretion energy between the disc, the warm corona, and the lamppost. The XMM-Newton observations span a factor of 188 in Eddington ratio (λobs) and 350 in black hole mass, and we find that a warm corona is a significant contributor to the soft excess for 13 of the 14 AGNs with a mean warm corona heating fraction of 0.51. The reXcor fits reveal that the fraction of accretion energy dissipated in the lamppost is anti-correlated with λobs. In contrast, the relationship between λobs and both the optical depth and heating fraction of the warm corona appears to transition from an anti-correlation to a correlation at λobs, t ≈ 0.15. Therefore, at least one other physical process in addition to the accretion rate is needed to explain the evolution of the warm corona. Overall, we find that a warm corona appears to be a crucial depository of accretion energy in AGNs across a broad range of λobs and black hole mass.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"57 14","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140748666","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

The thousand-pulsar-array programme on MeerKAT XIII: Timing, flux density, rotation measure and dispersion measure timeseries of 597 pulsars MeerKAT XIII 上的千脉冲星阵列计划：597 颗脉冲星的时间、通量密度、旋转测量和频散测量时间序列

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-04-02 DOI: 10.1093/mnras/stae937

M. Keith, S. Johnston, A. Karastergiou, P. Weltevrede, M. Lower, A. Basu, B. Posselt, L. Oswald, A. Parthasarathy, A. D. Cameron, M. Serylak, S. Buchner

{"title":"The thousand-pulsar-array programme on MeerKAT XIII: Timing, flux density, rotation measure and dispersion measure timeseries of 597 pulsars","authors":"M. Keith, S. Johnston, A. Karastergiou, P. Weltevrede, M. Lower, A. Basu, B. Posselt, L. Oswald, A. Parthasarathy, A. D. Cameron, M. Serylak, S. Buchner","doi":"10.1093/mnras/stae937","DOIUrl":"https://doi.org/10.1093/mnras/stae937","url":null,"abstract":"\u0000 We report here on the timing of 597 pulsars over the last four years with the MeerKAT telescope. We provide Times-of-Arrival, pulsar ephemeris files and per-epoch measurements of the flux density, dispersion measure (DM) and rotation measure (RM) for each pulsar. In addition we use a Gaussian process to model the timing residuals to measure the spin frequency derivative at each epoch. We also report the detection of 11 glitches in 9 individual pulsars. We find significant DM and RM variations in 87 and 76 pulsars respectively. We find that the DM variations scale approximately linearly with DM, which is broadly in agreement with models of the ionised interstellar medium. The observed RM variations seem largely independent of DM, which may suggest that the RM variations are dominated by variations in the interstellar magnetic field on the line of sight, rather than varying electron density. We also find that normal pulsars have around 5 times greater amplitude of DM variability compared to millisecond pulsars, and surmise that this is due to the known difference in their velocity distributions.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"291 ","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140754206","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

Synchro-curvature description of γ-ray light curves and spectra of pulsars: global properties 脉冲星γ射线光曲线和光谱的同步曲率描述：全局特性

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-04-02 DOI: 10.1093/mnras/stae933

Daniel Íñiguez-Pascual, Diego F. Torres, Daniele Viganò

{"title":"Synchro-curvature description of γ-ray light curves and spectra of pulsars: global properties","authors":"Daniel Íñiguez-Pascual, Diego F. Torres, Daniele Viganò","doi":"10.1093/mnras/stae933","DOIUrl":"https://doi.org/10.1093/mnras/stae933","url":null,"abstract":"\u0000 This work presents a methodological approach to generate realistic γ-ray light curves of pulsars, resembling reasonably well the observational ones observed by the Fermi-Large Area Telescope instrument, fitting at the same time their high-energy spectra. The theoretical light curves are obtained from a spectral and geometrical model of the synchro-curvature emission. Despite our model relies on a few effective physical parameters, the synthetic light curves present the same main features observed in the observational γ-ray light curve zoo, such as the different shapes, variety in the number of peaks, and a diversity of peak widths. The morphological features of the light curves allows us to statistically compare the observed properties. In particular, we find that the proportion on the number of peaks found in our synthetic light curves is in agreement with the observational one provided by the third Fermi-LAT pulsar catalog. We also found that the detection probability due to beaming is much higher for orthogonal rotators (approaching 100%) than for small inclination angles (less than 20 %). The small variation on the synthetic skymaps generated for different pulsars indicates that the geometry dominates over timing and spectral properties in shaping the gamma-ray light curves. This means that geometrical parameters like the inclination angle can be in principle constrained by gamma-ray data alone independently on the specific properties of a pulsar. At the same time, we find that γ-ray spectra seen by different observers can slightly differ, opening the door to constraining the viewing angle of a particular pulsar.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"97 16","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-04-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140754739","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

Cold electrons at a weakly outgassing comet 弱排气彗星上的冷电子

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-03-08 DOI: 10.1093/mnras/stae695

Peter Stephenson, M. Galand, J. Deca, Pierre Henri

{"title":"Cold electrons at a weakly outgassing comet","authors":"Peter Stephenson, M. Galand, J. Deca, Pierre Henri","doi":"10.1093/mnras/stae695","DOIUrl":"https://doi.org/10.1093/mnras/stae695","url":null,"abstract":"\u0000 Throughout the Rosetta mission, cold electrons (<1eV) were measured in the coma of comet 67P/Churyumov-Gerasimenko. Cometary electrons are produced at ∼10eV through photoionization or through electron-impact ionization collisions. The cold electron population is formed by cooling the warm population through inelastic electron-neutral collisions. Assuming radial electron outflow, electrons are collisional with the neutral gas coma below the electron exobase, which only formed above the comet surface in near-perihelion, high outgassing conditions (Q > 3 × 1027s−1). However, the cold population was identified at low outgassing (Q < 1026s−1), when the inner coma was not expected to be collisional. We examine cooling of electrons at a weakly outgassing comet, using a 3D collisional model of electrons at a comet. Electron paths are extended by trapping in an ambipolar electric field and by gyration around magnetic field lines. This increases the probability of electrons undergoing inelastic collisions with the coma and becoming cold. We demonstrate that a cold electron population can be formed and sustained, under weak outgassing conditions (Q = 1026s−1), once 3D electron dynamics are accounted for. Cold electrons are produced in the inner coma through electron-neutral collisions and transported tailwards by an E × B drift We quantify the efficiency of trapping in driving electron cooling, with trajectories typically 100 times longer than expected from ballistic radial outflow. Based on collisional simulations, we define an estimate for a region where a cold electron population can form, bounded by an electron cooling exobase. This estimate agrees well with cold electron measurements from the Rosetta Plasma Consortium.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"44 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-03-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140076821","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

Positive Lynden-Bell derivative as a ticket to the bar trap? 积极的林登-贝尔衍生品是通往酒吧陷阱的门票？

Monthly Notices of the Royal Astronomical Society Pub Date : 2024-03-08 DOI: 10.1093/mnras/stae702

V. D. Zozulia, Anton A. Smirnov, N. Ya. Sotnikova

{"title":"Positive Lynden-Bell derivative as a ticket to the bar trap?","authors":"V. D. Zozulia, Anton A. Smirnov, N. Ya. Sotnikova","doi":"10.1093/mnras/stae702","DOIUrl":"https://doi.org/10.1093/mnras/stae702","url":null,"abstract":"\u0000 We have translated the results of N-body simulations of one barred model into the language of action variables and frequencies. Using this language, we analysed the behaviour of all orbits in the model on a large time scale at the stage of a mature bar. We show that the orbits join the bar while preserving their adiabatic invariant, which takes into account the 3D structure of the orbits. This allows us to apply the concept of the Lynden-Bell derivative for each of these orbits and trace how the sign of the derivative changes, i.e. how asynchronous changes in angular momentum Lz and orbital precession rate Ωpr (normal orbital mode) change to synchronous (abnormal mode). The transition to the abnormal mode occurs when Ωpr reaches the angular velocity of the pattern Ωp, after which the orbit becomes stuck in the bar trap. All this happens against the background of secular changes in actions (Lz decreases, JR and Jz increase). At the same time, corotation particles near two stable Lagrange points are also subject to secular changes in their actions. They increase Lz and drift to the periphery, shifting corotation outwards. We also show that a change in the orbital mode from normal to abnormal and the trapping of orbits in a bar is possible only when the bar speed decreases with time, regardless of what is causing the bar to slow down. Our findings clarify and expand the picture of bar formation and evolution in numerical models.","PeriodicalId":506975,"journal":{"name":"Monthly Notices of the Royal Astronomical Society","volume":"47 20","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-03-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140077162","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