arXiv - PHYS - Cosmology and Nongalactic Astrophysics最新文献

{"title":"Caught in the cosmic web: environmental effects on subhalo abundance and internal density profiles","authors":"Feven Markos Hunde, Oliver Newton, Wojciech A. Hellwing, Maciej Bilicki, Krishna Naidoo","doi":"arxiv-2409.09226","DOIUrl":"https://doi.org/arxiv-2409.09226","url":null,"abstract":"Using the high-resolution Nbody{} cosmological simulation COLOR, we explore\u0000the cosmic web (CW) environmental effects on subhalo populations and their\u0000internal properties. We use cactus{}, a new implementation of the\u0000state-of-the-art segmentation method nexus{}, to delineate the simulation\u0000volume into nodes, filaments, walls, and voids. We group host halos by virial\u0000mass and segment each mass bin into consecutive CW elements. This reveals that\u0000subhalo populations in hosts within specific environments differ on average\u0000from the cosmic mean. The subhalo mass function is affected strongly, where\u0000hosts in filaments typically contain more subhalos (5 to 30%), while hosts in\u0000voids are subhalo-poor, with 50% fewer subhalos. We find that the abundance of\u0000the most massive subhalos, with reduced masses of $muequiv\u0000M_mathrm{sub}/M_{200}geq0.1$ is most sensitive to the CW environment. A\u0000corresponding picture emerges when looking at subhalo mass fractions,\u0000$f_mathrm{sub}$, where the filament hosts are significantly more `granular'\u0000(having higher $f_mathrm{sub}$) than the cosmic mean, while the void hosts\u0000have much smoother density distributions (with $f_mathrm{sub}$ lower by\u0000$10{-}40%$ than the mean). Finally, when we look at the subhalo internal\u0000kinematic vmax{}--rmax{} relations, we find that subhalos located in the void\u0000and wall hosts exhibit density profiles with lower concentrations than the\u0000mean, while the filament hosts demonstrate much more concentrated mass\u0000profiles. Across all our samples, the effect of the CW environment generally\u0000strengthens with decreasing host halo virial mass. Our results show that host\u0000location in the large-scale CW introduces significant systematic effects on\u0000internal subhalo properties and population statistics. Understanding and\u0000accounting for them is crucial for unbiased interpretation of observations\u0000related to small scales and satellite galaxies.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"9 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257643","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":"Primordial Stochastic Gravitational Wave Backgrounds from a Sharp Feature in Three-field Inflation II: The Inflationary Era","authors":"Vikas Aragam, Sonia Paban, Robert Rosati","doi":"arxiv-2409.09023","DOIUrl":"https://doi.org/arxiv-2409.09023","url":null,"abstract":"We study the contribution of large scalar perturbations sourced by a sharp\u0000feature during cosmic inflation to the stochastic gravitational wave background\u0000(SGWB), extending our previous work to include the SGWB sourced during the\u0000inflationary era. We focus in particular on three-field inflation, since the\u0000third dynamical field is the first not privileged by the perturbations'\u0000equations of motion and allows a more direct generalization to $N$-field\u0000inflation. For the first time, we study the three-field isocurvature\u0000perturbations sourced during the feature and include the effects of\u0000isocurvature masses. In addition to a two-field limit, we find that the third\u0000field's dynamics during the feature can source large isocurvature transients\u0000which then later decay, leaving an inflationary-era-sourced SGWB as their only\u0000observable signature. We find that the inflationary-era signal shape near the\u0000peak is largely independent of the number of dynamical fields and has a greatly\u0000enhanced amplitude sourced by the large isocurvature transient, suppressing the\u0000radiation-era contribution and opening a new window of detectable parameter\u0000space with small adiabatic enhancement. The largest enhancements we study could\u0000easily violate backreaction constraints, but much of parameter space remains\u0000under perturbative control. These SGWBs could be visible in LISA and other\u0000gravitational wave experiments, leaving an almost universal signature of sharp\u0000features during multi-field inflation, even when the sourcing isocurvature\u0000decays to unobservability shortly afterwards.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"13 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257675","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":"Towards Implementation of the Pressure-Regulated, Feedback-Modulated Model of Star Formation in Cosmological Simulations: Methods and Application to TNG","authors":"Sultan Hassan, Eve C. Ostriker, Chang-Goo Kim, Greg L. Bryan, Jan D. Burger, Drummond B. Fielding, John C. Forbes, Shy Genel, Lars Hernquist, Sarah M. R. Jeffreson, Bhawna Motwani, Matthew C. Smith, Rachel S. Somerville, Ulrich P. Steinwandel, Romain Teyssier","doi":"arxiv-2409.09121","DOIUrl":"https://doi.org/arxiv-2409.09121","url":null,"abstract":"Traditional star formation subgrid models implemented in cosmological galaxy\u0000formation simulations, such as that of Springel & Hernquist (2003, hereafter\u0000SH03), employ adjustable parameters to satisfy constraints measured in the\u0000local Universe. In recent years, however, theory and spatially-resolved\u0000simulations of the turbulent, multiphase, star-forming ISM have begun to\u0000produce new first-principles models, which when fully developed can replace\u0000traditional subgrid prescriptions. This approach has advantages of being\u0000physically motivated and predictive rather than empirically tuned, and allowing\u0000for varying environmental conditions rather than being tied to local Universe\u0000conditions. As a prototype of this new approach, by combining calibrations from\u0000the TIGRESS numerical framework with the Pressure-Regulated Feedback-Modulated\u0000(PRFM) theory, simple formulae can be obtained for both the gas depletion time\u0000and an effective equation of state. Considering galaxies in TNG50, we compare\u0000the \"native\" simulation outputs with post-processed predictions from PRFM. At\u0000TNG50 resolution, the total midplane pressure is nearly equal to the total ISM\u0000weight, indicating that galaxies in TNG50 are close to satisfying vertical\u0000equilibrium. The measured gas scale height is also close to theoretical\u0000equilibrium predictions. The slopes of the effective equations of states are\u0000similar, but with effective velocity dispersion normalization from SH03\u0000slightly larger than that from current TIGRESS simulations. Because of this and\u0000the decrease in PRFM feedback yield at high pressure, the PRFM model predicts\u0000shorter gas depletion times than the SH03 model at high densities and redshift.\u0000Our results represent a first step towards implementing new, numerically\u0000calibrated subgrid algorithms in cosmological galaxy formation simulations.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"18 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257673","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":"Dark Energy Survey: 2.1% measurement of the Baryon Acoustic Oscillation scale from the final dataset","authors":"Juan Mena-Fernández, Dark Energy Survey Collaboration","doi":"arxiv-2409.08759","DOIUrl":"https://doi.org/arxiv-2409.08759","url":null,"abstract":"Here, we present the angular diameter distance measurement obtained from the\u0000measurement of the Baryonic Acoustic Oscillation (BAO) feature using the\u0000completed Dark Energy Survey (DES) data, summarizing the main results of [Phys.\u0000Rev. D 110, 063514] and [Phys. Rev. D 110, 063515]. We use a galaxy sample\u0000optimized for BAO science in the redshift range 0.6 < z < 1.2, with an\u0000effective redshift of $z_{rm eff}$ = 0.85. Our consensus measurement\u0000constrains the ratio of the angular distance to the sound horizon scale to\u0000$D_M(z_{rm eff})/r_d$ = 19.51 $pm$ 0.41. This measurement is found to be\u00002.13$sigma$ below the angular BAO scale predicted by Planck. To date, it\u0000represents the most precise measurement from purely photometric data, and the\u0000most precise from any Stage-III experiment at such high redshift. The analysis\u0000was performed blinded to the BAO position and is shown to be robust against\u0000analysis choices, data removal, redshift calibrations and observational\u0000systematics.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"9 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257682","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":"NeutralUniverseMachine: How Filaments and Dark Matter Halo Influence the Galaxy Cold Gas Content","authors":"Wenlin Ma, Hong Guo, Michael G. Jones","doi":"arxiv-2409.08539","DOIUrl":"https://doi.org/arxiv-2409.08539","url":null,"abstract":"Aims. To investigate the influence of distance to filaments and dark matter\u0000halos on galaxy cold gas content in the empirical model NeutralUniverseMachine\u0000(NUM) and the hydrodynamical simulation IllustrisTNG. Methods. We use DisPerSE\u0000to identify cosmic web structures and calculate the distance of galaxies to\u0000filaments for both observations and models. We show the results of the HI and\u0000H2 mass functions, HI- and H2-halo mass relations, HI- and H2-stellar mass\u0000relations for galaxies in the NUM model and IllustrisTNG with different\u0000distances to filaments and compare them with observational measurements. We\u0000also show the evolution of HI, H2 mass densities in different distance to\u0000filament bins. Results. We find that the role of filaments in affecting the HI\u0000gas is generally less significant compared to the halo environment. There is a\u0000weak trend in the observations at z = 0 that low-mass halos lying closer to\u0000filaments tend to have reduced HI masses. However, this trend reverses for\u0000massive halos with log(Mvir/Msun) > 12.5. This behavior is accurately\u0000reproduced in the NUM model due to the dependence of HI gas on the halo\u0000formation time, but it does not appear in IllustrisTNG. The influence of\u0000filaments on the HI gas becomes slightly weaker at higher redshifts and is only\u0000significant for galaxies residing in massive halos in the NUM model. Filaments\u0000have almost no impact on the H2-stellar mass relation in both models,\u0000confirming that H2 is primarily determined by the galaxy stellar mass and star\u0000formation rate.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"21 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257679","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":"Generalized inflation in the context of $κ$-deformed theories","authors":"B W Ribeiro, I M Macêdo, F C Cabral","doi":"arxiv-2409.07678","DOIUrl":"https://doi.org/arxiv-2409.07678","url":null,"abstract":"A new inflationary scenario driven by a slowly-rolling homogeneous scalar\u0000field whose potential $Vleft(varphiright)$ is given by a generalized\u0000exponential function is investigated. Within the {it slow-roll} approximation\u0000we obtain the main predictions of the model and compare them with current data\u0000from cosmic microwave background and large-scale structure observations. We\u0000show that this single scalar field model admits a wider set of solutions than\u0000usual exponential scenarios and predicts acceptable values of the spectral\u0000index, running of the spectral index and tensor-to-scalar ratio for the\u0000remaining number of {it e}-folds lying in the interval $N = 55 pm 5$ and an\u0000energy scale on which $lambda geq sqrt{2}$; in particular, we observe that\u0000the value of the model parameter $kappa$ depends on the analysis. Finally, the\u0000primordial local non-Gaussianity is briefly discussed where we conclude that\u0000$kgtrsim 0.02$ for $f_text{NL}^text{local} ll 1$.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"11 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142192768","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":"Fast Projected Bispectra: the filter-square approach","authors":"Lea Harscouet, Jessica A. Cowell, Julia Ereza, David Alonso, Hugo Camacho, Andrina Nicola, Anze Slosar","doi":"arxiv-2409.07980","DOIUrl":"https://doi.org/arxiv-2409.07980","url":null,"abstract":"The study of third-order statistics in large-scale structure analyses has\u0000been hampered by the increased complexity of bispectrum estimators (compared to\u0000power spectra), the large dimensionality of the data vector, and the difficulty\u0000in estimating its covariance matrix. In this paper we present the\u0000filtered-squared bispectrum (FSB), an estimator of the projected bispectrum\u0000effectively consisting of the cross-correlation between the square of a field\u0000filtered on a range of scales and the original field. Within this formalism, we\u0000are able to recycle much of the infrastructure built around power spectrum\u0000measurement to construct an estimator that is both fast and robust against\u0000mode-coupling effects caused by incomplete sky observations. Furthermore, we\u0000demonstrate that the existing techniques for the estimation of analytical power\u0000spectrum covariances can be used within this formalism to calculate the\u0000bispectrum covariance at very high accuracy, naturally accounting for the most\u0000relevant Gaussian and non-Gaussian contributions in a model-independent manner.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"132 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142192766","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":"Kinematic Lensing Inference II: Cluster Lensing with $mathcal{O}$(1) Galaxies","authors":"Pranjal R. S., Eric Huff, Elisabeth Krause, Tim Eifler, Spencer Everett, Yu-Hsiu Huang, Jiachuan Xu","doi":"arxiv-2409.08367","DOIUrl":"https://doi.org/arxiv-2409.08367","url":null,"abstract":"We present the first detection of a cluster lensing signal with `Kinematic\u0000Lensing' (KL), a novel weak lensing method that combines photometry,\u0000spectroscopy, and the Tully-Fisher relation to enable shear measurements with\u0000individual source galaxies. This is the second paper in a two-part series aimed\u0000at measuring a KL signal from data. The first paper, arXiv:2209.11811,\u0000describes the inference pipeline, which jointly forward models galaxy imaging\u0000and spectroscopy, and demonstrates unbiased shear inference with simulated\u0000data. This paper presents measurements of the lensing signal from the galaxy\u0000cluster Abell 2261. We obtain spectroscopic observations of background disk\u0000galaxies in the cluster field selected from the CLASH Subaru catalog. The final\u0000sample consists of three source galaxies while the remaining are rejected due\u0000to insufficient signal-to-noise, spectroscopic failures, and inadequately\u0000sampled rotation curves. We apply the KL inference pipeline to the three\u0000sources and find the shear estimates to be in broad agreement with traditional\u0000weak lensing measurements. The typical shear measurement uncertainty for our\u0000sources is $sigma(g_+)approx 0.026$, which represents approximately a\u0000ten-fold improvement over the weak lensing shape noise. We identify target\u0000selection and observing strategy as the key avenues of improvement for future\u0000KL programs.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"31 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257676","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":"Hydrostatic mass bias for galaxy groups and clusters in the FLAMINGO simulations","authors":"Joey Braspenning, Joop Schaye, Matthieu Schaller, Roi Kugel, Scott T. Kay","doi":"arxiv-2409.07849","DOIUrl":"https://doi.org/arxiv-2409.07849","url":null,"abstract":"The masses of galaxy clusters are commonly measured from X-ray observations\u0000under the assumption of hydrostatic equilibrium (HSE). This technique is known\u0000to underestimate the true mass systematically. The fiducial FLAMINGO\u0000cosmological hydrodynamical simulation predicts the median hydrostatic mass\u0000bias to increase from $b_text{HSE} equiv\u0000(M_text{HSE,500c}-M_text{500c})/M_text{500c} approx -0.1$ to -0.2 when the\u0000true mass increases from group to cluster mass scales. However, the bias is\u0000nearly independent of the hydrostatic mass. The scatter at fixed true mass is\u0000minimum for $M_text{500c}sim 10^{14}~text{M}_odot$, where\u0000$sigma(b_text{HSE})approx 0.1$, but increases rapidly towards lower and\u0000higher masses. At a fixed true mass, the hydrostatic masses increase (decrease)\u0000with redshift on group (cluster) scales, and the scatter increases. The bias is\u0000insensitive to the choice of analytic functions assumed to represent the\u0000density and temperature profiles, but it is sensitive to the goodness of fit,\u0000with poorer fits corresponding to a stronger median bias and a larger scatter.\u0000The bias is also sensitive to the strength of stellar and AGN feedback. Models\u0000predicting lower gas fractions yield more (less) biased masses for groups\u0000(clusters). The scatter in the bias at fixed true mass is due to differences in\u0000the pressure gradients rather than in the temperature at $R_text{500c}$. The\u0000total kinetic energies within $r_text{500c}$ in low- and high-mass clusters\u0000are sub- and super-virial, respectively, though all become sub-virial when\u0000external pressure is accounted for. Analyses of the terms in the virial and\u0000Euler equations suggest that non-thermal motions, including rotation, account\u0000for most of the hydrostatic mass bias. However, we find that the mass bias\u0000estimated from X-ray luminosity weighted profiles strongly overestimates the\u0000deviations from hydrostatic equilibrium.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"7 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142192767","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 measurement of the escaping ionising efficiency of galaxies at redshift 5","authors":"Sarah E. I. Bosman, Frederick B. Davies","doi":"arxiv-2409.08315","DOIUrl":"https://doi.org/arxiv-2409.08315","url":null,"abstract":"The escaping ionising efficiency from galaxies, $f_{rm esc}xi_{rm ion}$,\u0000is a crucial ingredient for understanding their contribution to hydrogen\u0000reionisation, but both of its components, $f_{rm{esc}}$ and $xi_{rm{ion}}$,\u0000are extremely difficult to measure. We measure the average escaping ionising\u0000efficiency $langle f_{rm{esc}} xi_{rm{ion}}rangle$ of galaxies at $z=5$\u0000implied by the mean level of ionisation in the intergalactic medium via the\u0000Lyman-$alpha$ forest. We use the fact that $dot{N}_{rm{ion}} =\u0000rho_{rm{UV}} f_{rm{esc}} xi_{rm{ion}}$, the product of the ionising output\u0000and the UV density $rho_{rm{UV}}$, can be calculated from the known average\u0000strength of the UV background and the mean free path of ionising photons. These\u0000quantities, as well as $rho_{rm{UV}}$, are robustly measured at $zleq6$. We\u0000calculate the missing factor of $langle f_{rm{esc}} xi_{rm{ion}}rangle$ at\u0000$z=5$, during a convenient epoch after hydrogen reionisation has completed and\u0000the intergalactic medium has reached ionisation equilibrium, but before bright\u0000quasars begin to dominate the ionising photon production. Intuitively, our\u0000constraint corresponds to the required escaping ionising production from\u0000galaxies in order to avoid over- or under-ionising the Lyman-$alpha$ forest.\u0000We obtain a measurement of $log langle f_{rm{esc}} xi_{rm{ion}}rangle\u0000/$erg Hz$^{-1}$ $ = 24.28_{-0.20}^{+0.21}$ at $z=5$ when integrating\u0000$rho_text{UV}$ down to a limiting magnitude $M_text{lim}=-11$. Our\u0000measurement of the escaping ionising efficiency of galaxies is in rough\u0000agreement with both observations and most models.","PeriodicalId":501207,"journal":{"name":"arXiv - PHYS - Cosmology and Nongalactic Astrophysics","volume":"188 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-09-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"142257678","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}