The Astrophysical Journal最新文献_第6页

Saturns, but Not Super-Jupiters, Occur More Frequently in the Presence of Inner Super-Earths 土星，而不是超级木星，更频繁地出现在内部超级地球的存在下

The Astrophysical Journal Pub Date : 2025-07-15 DOI: 10.3847/1538-4357/ade715

Etienne Lefèvre-Forján and Gijs D. Mulders

{"title":"Saturns, but Not Super-Jupiters, Occur More Frequently in the Presence of Inner Super-Earths","authors":"Etienne Lefèvre-Forján and Gijs D. Mulders","doi":"10.3847/1538-4357/ade715","DOIUrl":"https://doi.org/10.3847/1538-4357/ade715","url":null,"abstract":"Studies from recent years have reached different conclusions regarding how frequently super-Earths are accompanied by long-period giant planets and vice versa. This relation has been predicted to be mass dependent by planet-formation models. We investigate that as the origin of the discrepancy using a radial velocity sample: the California Legacy Survey. We perform detection completeness corrections in order to discard detection bias as a possible explanation to our results. After bias corrections, we find that cold Jupiters are times more massive when not in the company of an inner super-Earth, while super-Earths are not significantly more massive while in the company of an outer giant planet. We also report an occurrence enhancement for Saturns (median projected mass of 0.6MJ) while in presence of a super-Earth by a factor of ∼4, and for super-Earths in the presence of Saturns by the same factor. This positive correlation disappears for super-Jupiters (median projected mass of 3.1MJ). These results show that while cold Jupiters are generally accompanied by inner super-Earths, this does not hold for the largest giant planets, such as those that will be discovered by Gaia, which will likely not be accompanied by transiting planets. The mass dependence, in combination with the different detection limits of different surveys, may explain the discrepancies concerning occurrence relations between cold Jupiters and super-Earths.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"24 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144640073","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

AMUSE-Antlia. II. Intracluster X-Ray Population in the Antlia Cluster AMUSE-Antlia。2。安提亚星系团内x射线人口

The Astrophysical Journal Pub Date : 2025-07-15 DOI: 10.3847/1538-4357/ade3d4

Zhensong Hu, Yuanyuan Su, Zhiyuan Li, Meicun Hou, Ralph P. Kraft, Kelley M. Hess and Hao Chen

{"title":"AMUSE-Antlia. II. Intracluster X-Ray Population in the Antlia Cluster","authors":"Zhensong Hu, Yuanyuan Su, Zhiyuan Li, Meicun Hou, Ralph P. Kraft, Kelley M. Hess and Hao Chen","doi":"10.3847/1538-4357/ade3d4","DOIUrl":"https://doi.org/10.3847/1538-4357/ade3d4","url":null,"abstract":"We conduct a systematic survey of X-ray sources in the inner (r ∼ 200 kpc) region of the Antlia cluster based on Chandra observations, down to a source detection limit of L(0.5–8 keV) ∼ 4.2 × 10−7 ph cm−2 s−1 (2 × 1038 erg s−1). We present an X-ray source catalog with 202 sources and provide their coordinates, multiband flux information, and hardness ratios. We find a statistically significant excess at a significance level of 4.2σ with 37.6 excess sources beyond 3 times the mean effective radius of the two brightest central galaxies (BCGs). This implies that these excess sources could be a genuine intracluster X-ray population that is not associated with the bulk stellar component. Also, the increased number of excess sources in the fields containing a BCG implies a potential connection between the excess sources and BCGs. The discovery of these sources in the Antlia cluster, together with previous research of similar findings in the other two nearby clusters, Virgo and Fornax, indicates that the intracluster X-ray population could be universal in nearby galaxy clusters. Furthermore, we discuss the candidate origins of the excess sources, including low-mass X-ray binaries (LMXBs) associated with intracluster light (ICL-LMXBs), LMXBs in globular clusters (GC-LMXBs), and supernova-kicked LMXBs (SN-kicked LMXBs). We estimate that the contribution of ICL-LMXBs, which should include the LMXBs related to the stellar halo surrounding BCGs, is unlikely to dominate the intracluster X-ray population in Antlia. Meanwhile, GC-LMXBs and SN-kicked LMXBs, each component could contribute ∼30% to the total excess sources.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"8 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144640066","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

Lyα Radiative Transfer Modeling for 163 MUSE Lyα-emitting Galaxies at z = 3–6 z = 3-6处163个MUSE Lyα发射星系的Lyα辐射传递模型

The Astrophysical Journal Pub Date : 2025-07-15 DOI: 10.3847/1538-4357/ade2da

Sangeun Yu, Hyunmi Song and Kwang-Il Seon

{"title":"Lyα Radiative Transfer Modeling for 163 MUSE Lyα-emitting Galaxies at z = 3–6","authors":"Sangeun Yu, Hyunmi Song and Kwang-Il Seon","doi":"10.3847/1538-4357/ade2da","DOIUrl":"https://doi.org/10.3847/1538-4357/ade2da","url":null,"abstract":"We utilized Lyα radiative transfer calculations from H. Song et al. to investigate the properties of extended Lyα halos around star-forming galaxies in the Hubble Ultra Deep Field, observed by the Multi-Unit Spectroscopic Explorer. Expanding on the work of H. Song et al., which was limited to eight galaxies, we derived best-fit models for a significantly larger sample of 163 galaxies, which successfully reproduced both their Lyα spectra and surface brightness profiles (SBPs). These best-fit models suggest a broad medium distribution surrounding each galaxy, with low expanding velocities at large radii. This conclusion could not have been drawn from modeling either the spectrum or SBP alone, but only through simultaneous modeling of both. Our correlation analysis between observables and model parameters reveals that the spatial extent of Lyα halos is primarily determined by the extents of the medium and the source, while the spectral peak shift and full width at half maximum are governed mainly by optical depth, with the velocity structure of the medium playing a secondary yet nonnegligible role. The fact that various correlations derived from the full set of models and those from the best-fit subset can differ significantly highlights the complex and interdependent nature of Lyα radiative transfer. All model parameters interact to shape the observed Lyα features in a nontrivial way.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"23 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144640006","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

Multifrequency Radio Observations of the Magnetar Swift J1818.0–1607 磁星雨燕J1818.0-1607的多频射电观测

The Astrophysical Journal Pub Date : 2025-07-15 DOI: 10.3847/1538-4357/ade14f

Evan F. Lewis, Harsha Blumer, Ryan S. Lynch and Maura A. McLaughlin

引用次数: 0

Efficient Ionizers with Low H β + [O iii] Equivalent Widths: JADES Spectroscopy of a Peculiar High-redshift Population 具有低H β + [O iii]等效宽度的高效电离剂：特殊高红移种群的JADES光谱

The Astrophysical Journal Pub Date : 2025-07-14 DOI: 10.3847/1538-4357/adddb5

Isaac H. Laseter, Michael V. Maseda, Charlotte Simmonds, Ryan Endsley, Daniel Stark, Andrew J. Bunker, Rachana Bhatawdekar, Kristan Boyett, Alex J. Cameron, Stefano Carniani, Mirko Curti, Zhiyuan Ji, Pierluigi Rinaldi, Aayush Saxena, Sandro Tacchella, Chris Willott, Joris Witstok and Yongda Zhu

{"title":"Efficient Ionizers with Low H β + [O iii] Equivalent Widths: JADES Spectroscopy of a Peculiar High-redshift Population","authors":"Isaac H. Laseter, Michael V. Maseda, Charlotte Simmonds, Ryan Endsley, Daniel Stark, Andrew J. Bunker, Rachana Bhatawdekar, Kristan Boyett, Alex J. Cameron, Stefano Carniani, Mirko Curti, Zhiyuan Ji, Pierluigi Rinaldi, Aayush Saxena, Sandro Tacchella, Chris Willott, Joris Witstok and Yongda Zhu","doi":"10.3847/1538-4357/adddb5","DOIUrl":"https://doi.org/10.3847/1538-4357/adddb5","url":null,"abstract":"Early JWST photometric studies discovered a population of UV-faint ( ) z ∼ 6.5–8 Lyman break galaxies with spectral energy distributions implying young ages (∼10 Myr) yet relatively weak Hβ + [O iii] equivalent widths (EWHβ + [O iii] ≈ 400 Å). These galaxies seemingly contradict the implicit understanding that young star-forming galaxies are ubiquitously strong Hβ + [O iii] emitters, i.e., extreme emission line galaxies (EW ≳750 Å). Low metallicities, high Lyman continuum escape fractions, and rapidly declining star formation histories have been proposed as primary drivers behind low Hβ + [O iii] EWs, but the blend of Hβ + [O iii] in photometric studies makes proving one of these scenarios difficult. We aim to characterize this peculiar population with deep spectroscopy from the JWST Advanced Deep Extragalactic Survey. We find that a significant subset of these galaxies at z ≳ 2 with modest Hβ + [O iii] EWs (≈300–600 Å) have high ionization efficiencies ( ). Suppressed [O iii] EW values yet elevated Hα and Hβ EW values imply that the level of chemical enrichment is the primary culprit, supported by spectroscopic measurements of metallicities below 12 + log(O/H) ≈ 7.70 (0.1Z⊙). We demonstrate that integrated Hβ + [O iii] selections (e.g., Hβ + [O iii] EW > 700 Å) exclude the most metal-poor efficient ionizers and favor (1) more chemically enriched systems with comparable extreme radiation fields and (2) older starbursting systems. In contrast, metallicity degeneracies are reduced in Hα space, enabling the identification of these metal-poor efficient ionizers by their specific star formation rate.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"29 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144630327","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

Wind-fed Supermassive Black Hole Accretion by the Nuclear Star Cluster: The Case of M31* 由核星团引起的风馈超大质量黑洞吸积：以M31*为例

The Astrophysical Journal Pub Date : 2025-07-14 DOI: 10.3847/1538-4357/ade1d5

Zhao Su, Zhiyuan Li and Zongnan Li

{"title":"Wind-fed Supermassive Black Hole Accretion by the Nuclear Star Cluster: The Case of M31*","authors":"Zhao Su, Zhiyuan Li and Zongnan Li","doi":"10.3847/1538-4357/ade1d5","DOIUrl":"https://doi.org/10.3847/1538-4357/ade1d5","url":null,"abstract":"The central supermassive black hole (SMBH) of the Andromeda galaxy, known as M31*, exhibits dim electromagnetic emission and is inferred to have an extremely low accretion rate for its remarkable mass (∼108M⊙). In this work, we use three-dimensional hydrodynamical simulations to explore a previously untested scenario, in which M31* is fed by the collective stellar mass loss from its surrounding nuclear star cluster, manifested as a famous eccentric disk of predominantly old stellar populations. The stellar mass loss is assumed to be dominated by the slow and cold winds from 100 asymptotic giant-branch stars, which follow well-constrained Keplerian orbits around M31* and together provide a mass injection rate of ∼4 × 10−5M⊙ yr−1. The simulations achieve a quasi-steady state on a megayear timescale, at which point a quasi-Keplerian, cool (T ∼ 103–104 K) gas disk extending several parsecs is established. This disk is continuously supplied by the stellar winds and itself feeds the central SMBH. At the end of the simulations at 2 Myr, an accretion rate of ∼2 × 10−5M⊙ yr−1 is found but could vary by a factor of a few depending on whether the subdominant gravity of the NSC or a moderate global inflow is included. The predicted X-ray luminosity of ∼1036 erg s−1, dominated by the hot (T ∼ 107–108 K) plasma within 0.2 pc of the SMBH, is consistent with Chandra observations. We conclude that the feeding mechanism of M31* is successfully identified, which has important implications for the working of dormant SMBHs prevalent in the local Universe.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"2 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144630337","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

Electron Acceleration at Shock Ripples: Role of Pitch-angle Diffusion 激波中的电子加速：俯仰角扩散的作用

The Astrophysical Journal Pub Date : 2025-07-14 DOI: 10.3847/1538-4357/ade23e

Y. D. Xu, G. Li and S. Yao

{"title":"Electron Acceleration at Shock Ripples: Role of Pitch-angle Diffusion","authors":"Y. D. Xu, G. Li and S. Yao","doi":"10.3847/1538-4357/ade23e","DOIUrl":"https://doi.org/10.3847/1538-4357/ade23e","url":null,"abstract":"Suprathermal electrons are routinely observed in interplanetary space. At higher energies, there are in-situ evidences that shocks, both interplanetary shocks, often driven by fast coronal mass ejections, and terrestrial bow shocks, can accelerate electrons up to transrelativistic energies (∼MeVs). The acceleration mechanism responsible for these energetic electrons is still under debate. In this work, we study the effects of large-scale shock ripples on electron acceleration at a quasi-perpendicular shock in a 2D system. For tractability of the numerical simulation, we consider the scenario where the magnetic field line contains ripples, and the shock is assumed planar and piecewise. The propagation of gyrophase-averaged electrons is governed by the focused transport equation, where the effect of the turbulent magnetic field is modeled by the pitch-angle diffusion, described by the quasi-linear theory. A Monte Carlo simulation on the equivalent time-forward Itô stochastic differential equation is performed within a periodic box to obtain the phase-space distribution function of the accelerated electrons. Our model predicts power-law energy spectra with a cutoff at high-energy ends, whereas their spectral indices are softer than those predicted by the diffusive shock acceleration theory. We demonstrate that, with a suitable choice of pitch-angle diffusion strength, a small fraction of electrons can experience magnetic traps in multiple ripples along the shock surface, boosting their energies to ∼MeVs. Our results therefore provide a framework for a better understanding of relativistic electron events associated with shocks within the heliosphere.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"670 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144630339","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

Statistical Study on the Solar Wind Turbulence Spectra Upstream of Mars 火星上游太阳风湍流谱的统计研究

The Astrophysical Journal Pub Date : 2025-07-14 DOI: 10.3847/1538-4357/ade30c

Zhuxuan Zou, Yuming Wang, Zhenpeng Su, Long Cheng, Zhiyong Wu, Tielong Zhang, Guoqiang Wang, Sudong Xiao, Yutian Chi, Zonghao Pan, Xinjun Hao, Yiren Li and Kai Liu

{"title":"Statistical Study on the Solar Wind Turbulence Spectra Upstream of Mars","authors":"Zhuxuan Zou, Yuming Wang, Zhenpeng Su, Long Cheng, Zhiyong Wu, Tielong Zhang, Guoqiang Wang, Sudong Xiao, Yutian Chi, Zonghao Pan, Xinjun Hao, Yiren Li and Kai Liu","doi":"10.3847/1538-4357/ade30c","DOIUrl":"https://doi.org/10.3847/1538-4357/ade30c","url":null,"abstract":"We statistically analyze the power spectral density (PSD) of magnetic field turbulence in the upstream solar wind of the Martian bow shock by investigating the data from Tianwen-1 and Mars Atmosphere and Volatile Evolution (MAVEN) during 2021 November 13 and December 31. The spectral indices and break frequencies of these PSDs are automatically identified. According to the profiles of the PSDs, we find that they could be classified into three types: A, B, and C. Only less than a quarter of the events exhibit characteristics similar to the 1 au PSDs (Type A). We observe the energy injection in more than one-third of the events (Type B), and the injected energy usually results in the steeper spectral indices of the dissipation ranges. We find the absence of the dissipation range in over one third of the PSDs (Type C), which is likely due to the dissipation occurring at higher frequencies rather than proton cyclotron resonant frequencies. We also find that the two spacecraft observed different types of PSDs in more than half of the investigated episodes, indicating significant variability upstream of the Martian bow shock. For example, the Type-B PSDs are more often seen by Tianwen-1, which was near the flank of the bow shock, than by MAVEN near the nose. This statistical study demonstrates the complicated turbulent environment of the solar wind upstream of the Martian bow shock.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"34 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144630342","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

Orbital Decay of the Ultra-hot Jupiter TOI-2109b: Tidal Constraints and Transit-timing Analysis 超热木星TOI-2109b的轨道衰减：潮汐约束和凌日时分析

The Astrophysical Journal Pub Date : 2025-07-14 DOI: 10.3847/1538-4357/ade057

Jaime A. Alvarado-Montes, Mario Sucerquia, Jorge I. Zuluaga and Christian Schwab

{"title":"Orbital Decay of the Ultra-hot Jupiter TOI-2109b: Tidal Constraints and Transit-timing Analysis","authors":"Jaime A. Alvarado-Montes, Mario Sucerquia, Jorge I. Zuluaga and Christian Schwab","doi":"10.3847/1538-4357/ade057","DOIUrl":"https://doi.org/10.3847/1538-4357/ade057","url":null,"abstract":"TOI-2109b is the ultra-hot Jupiter with the shortest orbital period (∼16 hr) yet discovered. At this close distance, strong tidal interactions can produce a significant exchange of angular momentum with the star. Since the orbital period of this planet is shorter than the stellar rotation period, TOI-2109b may be an optimal candidate for studying orbital decay. This process depends on how efficiently the star and the planet dissipate energy, due mainly to interior mechanisms that are poorly constrained in exoplanet systems. In this work, we study for the first time the tidal evolution of TOI-2109b under a formalism of inertial waves (IWs) in convective envelopes and internal gravity waves (IGWs) in stellar radiative regions. We find that uncertainties in the age of TOI-2109 (t⋆,age) significantly affect the rate of orbital evolution, as IWs and IGWs interact differently depending on t⋆,age. For an “old” host star, we find that TOI-2109b would undergo fast orbital decay. Conversely, if TOI-2109b orbits a “young” host star, a rather slow decay rate for would suggest a constant-period orbit. Our calculated mid-transit times and transit-timing variations (TTVs) support a “young” host star with , suggesting a decay rate that could lead to mid-transit-time shifts ≲10 s over three years. Orbital decay and other TTV-inducing effects will be confirmed or ruled out with future higher-quality timing data. The results presented here aim at constraining the current modeling of tides and TTVs for TOI-2109b, helping us further understand light-curve changes associated with the long-term evolution of ultra-short-period planets.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"45 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144630329","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

Monte Carlo Evaluations of Gamma-Ray and Radio Pulsar Populations 伽玛射线和射电脉冲星群的蒙特卡洛评估

The Astrophysical Journal Pub Date : 2025-07-14 DOI: 10.3847/1538-4357/ade13f

Shawaiz Tabassum and Duncan R. Lorimer

{"title":"Monte Carlo Evaluations of Gamma-Ray and Radio Pulsar Populations","authors":"Shawaiz Tabassum and Duncan R. Lorimer","doi":"10.3847/1538-4357/ade13f","DOIUrl":"https://doi.org/10.3847/1538-4357/ade13f","url":null,"abstract":"Based on well-grounded Galactic neutron star populations formed from radio pulsar population syntheses of canonical pulsars (CPs) and millisecond pulsars (MSPs), we use the latest Fermi Large Area Telescope catalog (4FGL-DR4) to investigate the implications of proposed γ-ray luminosity models. Using Monte Carlo techniques, we calculate the number of CPs and MSPs that would comprise the sample of pulsar-like unidentified sources (PLUIDs) in 4FGL-DR4. While radio beaming fractions were used to scale the sizes of the populations, when forming the mock 4FGL-DR4 samples we make the simplifying assumption that all γ-ray pulsars are beaming toward the Earth. We then explore the observable outcomes of seven different γ-ray luminosity models. Four of the models provide a good match to the observed number of PLUIDs, while three others significantly overpredict the number of PLUIDs. For these latter models, either the average beaming fraction of γ-ray pulsars is more like 25%–50%, or a revision in the luminosity scaling is required. Most of the radio-detectable MSPs that our models predict as part of the PLUIDs within 4FGL-DR4 are, unsurprisingly, fainter than the currently observed sample and at larger dispersion measures. For CPs, in spite of an excellent match to the observed radio population, none of the γ-ray models we investigated could replicate the observed sample of 150 γ-ray CPs. Further work is required to understand this discrepancy. For both MSPs and CPs, we provide encouraging forecasts for targeted radio searches of PLUIDs from 4FGL-DR4 to elucidate the issues raised in this study.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"26 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-07-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144630333","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