Pub Date : 2026-03-16DOI: 10.3847/1538-4357/ae4590
Shweta Jain, Ryan L. Sanders, Ali Ahmad Khostovan, Tucker Jones, Alice E. Shapley, Naveen A. Reddy, Alex M. Garcia, Paul Torrey and Alison Coil
We present a systematic investigation of the evolution of the mass–metallicity relation (MZR) and fundamental metallicity relation (FMR) using uniform metallicity diagnostics across redshifts z ∼ 0 to z ∼ 3.3. We present new Keck/Deep Imaging Multi-Object Spectrograph measurements of the [O II]λλ3726, 3729 emission line doublet for star-forming galaxies at z ∼ 1.5 with existing measurements of redder rest-optical lines from the MOSFIRE Deep Evolution Field survey. These new observations enable uniform estimation of the gas-phase oxygen abundance using ratios of the [O II], Hβ, and [O III] lines for mass-binned samples of star-forming galaxies in six redshift bins, employing strong line calibrations that account for the distinct interstellar medium ionization conditions at z < 1 and z > 1. We find that the low-mass power-law slope of the MZR remains constant over this redshift range with a value of γ = 0.28 ± 0.01, implying the outflow metal loading factor ( ) scales approximately as out to at least z ∼ 3.3. The normalization of the MZR at 1010M⊙ decreases with increasing redshift at a rate of across the full redshift range. We find that any evolution of the FMR is smaller than 0.1 dex out to z ∼ 3.3. We compare to cosmological galaxy formation simulations, and find that IllustrisTNG matches our measured combination of a nearly-invariant MZR slope, rate of MZR normalization decrease, and constant or very weakly evolving FMR. This work provides the most detailed view of MZR and FMR evolution from the present day through Cosmic Noon with a fine time sampling of 1−3 Gyr, setting a robust baseline for metallicity evolution studies at z > 4 with JWST.
{"title":"A Uniform Analysis of Gas-phase Metallicity Evolution with 1–3 Gyr Time Sampling over the Past 12 Gyr","authors":"Shweta Jain, Ryan L. Sanders, Ali Ahmad Khostovan, Tucker Jones, Alice E. Shapley, Naveen A. Reddy, Alex M. Garcia, Paul Torrey and Alison Coil","doi":"10.3847/1538-4357/ae4590","DOIUrl":"https://doi.org/10.3847/1538-4357/ae4590","url":null,"abstract":"We present a systematic investigation of the evolution of the mass–metallicity relation (MZR) and fundamental metallicity relation (FMR) using uniform metallicity diagnostics across redshifts z ∼ 0 to z ∼ 3.3. We present new Keck/Deep Imaging Multi-Object Spectrograph measurements of the [O II]λλ3726, 3729 emission line doublet for star-forming galaxies at z ∼ 1.5 with existing measurements of redder rest-optical lines from the MOSFIRE Deep Evolution Field survey. These new observations enable uniform estimation of the gas-phase oxygen abundance using ratios of the [O II], Hβ, and [O III] lines for mass-binned samples of star-forming galaxies in six redshift bins, employing strong line calibrations that account for the distinct interstellar medium ionization conditions at z < 1 and z > 1. We find that the low-mass power-law slope of the MZR remains constant over this redshift range with a value of γ = 0.28 ± 0.01, implying the outflow metal loading factor ( ) scales approximately as out to at least z ∼ 3.3. The normalization of the MZR at 1010M⊙ decreases with increasing redshift at a rate of across the full redshift range. We find that any evolution of the FMR is smaller than 0.1 dex out to z ∼ 3.3. We compare to cosmological galaxy formation simulations, and find that IllustrisTNG matches our measured combination of a nearly-invariant MZR slope, rate of MZR normalization decrease, and constant or very weakly evolving FMR. This work provides the most detailed view of MZR and FMR evolution from the present day through Cosmic Noon with a fine time sampling of 1−3 Gyr, setting a robust baseline for metallicity evolution studies at z > 4 with JWST.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"36 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2026-03-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147462163","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}
Pub Date : 2026-03-16DOI: 10.3847/1538-4357/ae47ed
Abolhassan Mohammadi, Yogesh, Qiang Wu and Tao Zhu
We investigate the formation of primordial black holes (PBHs), their spin and abundance, in a single-field inflationary model based on a mutated hilltop potential inserted with a small step-like feature. This step induces a brief phase of ultra-slow-roll inflation, producing large enhancement of the scalar power spectrum required for an appreciable amount of PBH abundance. Instead of an analytical power spectra, we compute the power spectrum accurately by numerically solving the Mukhanov–Sasaki equation. Then, we apply peak theory with ∇2ζ treated as a Gaussian random field and parameterize the curvature profile by its amplitude μ and width K. Confining the study to Type-I PBH, the threshold value is calculated using two robust methods: the average of the compaction function and the q-function method. Using the result, the dimensionless spin parameter of the PBHs is calculated at linear order and found to be ; however, it can be higher for smaller masses. We present detailed predictions for two representative parameter sets, calculate the PBH mass function and the associated scalar-induced gravitational waves (SIGWs). The first produces PBHs of mass M ≃ 10−13M⊙ that can account for 100% of dark matter, while the second yields M ≃ 10−2M⊙ PBHs contributing approximately 2.3% of the dark matter. The predicted signals of SIGWs lie within the sensitivity bands of future experiments such as LISA, DECIGO, BBO, and SKA. In particular, the second parameter set produces a SIGW compatible with the recent NANOGrav evidence for a low-frequency gravitational-wave signal.
{"title":"Spinning Primordial Black Holes and Scalar Induced Gravitational Waves from Single Field Inflation","authors":"Abolhassan Mohammadi, Yogesh, Qiang Wu and Tao Zhu","doi":"10.3847/1538-4357/ae47ed","DOIUrl":"https://doi.org/10.3847/1538-4357/ae47ed","url":null,"abstract":"We investigate the formation of primordial black holes (PBHs), their spin and abundance, in a single-field inflationary model based on a mutated hilltop potential inserted with a small step-like feature. This step induces a brief phase of ultra-slow-roll inflation, producing large enhancement of the scalar power spectrum required for an appreciable amount of PBH abundance. Instead of an analytical power spectra, we compute the power spectrum accurately by numerically solving the Mukhanov–Sasaki equation. Then, we apply peak theory with ∇2ζ treated as a Gaussian random field and parameterize the curvature profile by its amplitude μ and width K. Confining the study to Type-I PBH, the threshold value is calculated using two robust methods: the average of the compaction function and the q-function method. Using the result, the dimensionless spin parameter of the PBHs is calculated at linear order and found to be ; however, it can be higher for smaller masses. We present detailed predictions for two representative parameter sets, calculate the PBH mass function and the associated scalar-induced gravitational waves (SIGWs). The first produces PBHs of mass M ≃ 10−13M⊙ that can account for 100% of dark matter, while the second yields M ≃ 10−2M⊙ PBHs contributing approximately 2.3% of the dark matter. The predicted signals of SIGWs lie within the sensitivity bands of future experiments such as LISA, DECIGO, BBO, and SKA. In particular, the second parameter set produces a SIGW compatible with the recent NANOGrav evidence for a low-frequency gravitational-wave signal.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"10 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2026-03-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147461860","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}
Pub Date : 2026-03-16DOI: 10.3847/1538-4357/ae486b
Chen Deng, Yong-Feng Huang, Abdusattar Kurban, Jin-Jun Geng, Fan Xu, Xiao-Fei Dong, Hao-Xuan Gao, En-Wei Liang and Liang Li
Short gamma-ray bursts (GRBs) exhibiting a plateau phase provide valuable insights into the postmerger activity of their central engines. Although the physical origin of the plateau remains uncertain, the magnetar energy injection model offers a compelling explanation that reproduces the observed temporal and luminosity features. However, previous studies relying solely on X-ray data have suffered from strong parameter degeneracies when constraining the magnetar parameters. Here we perform broadband afterglow modeling on seven short GRBs with plateau features by combining X-ray, optical, and radio observations within the framework of the magnetar energy injection model. Key model parameters are derived by using the Markov Chain Monte Carlo method. It is found that the energy injection substantially modifies the afterglow dynamics in most events. Compared with X-ray-only analyses, our broadband modeling systematically yields a lower magnetic field strength and a shorter spin period for the central magnetar, corresponding to a higher injection luminosity. The study clearly shows that incorporating multiwavelength data effectively alleviates the degeneracy between the magnetar parameters and X-ray radiative efficiency. In addition, the distribution of our short GRBs differs markedly from long GRBs when they are plotted on the initial Lorentz factor versus gamma-ray energy plane. This offset, consistent with the observed harder spectrum of short GRBs, may serve as a useful diagnostic for investigating the progenitor as larger samples are available.
{"title":"Modeling the Multiwavelength Afterglow of Short Gamma-Ray Bursts with a Plateau Phase","authors":"Chen Deng, Yong-Feng Huang, Abdusattar Kurban, Jin-Jun Geng, Fan Xu, Xiao-Fei Dong, Hao-Xuan Gao, En-Wei Liang and Liang Li","doi":"10.3847/1538-4357/ae486b","DOIUrl":"https://doi.org/10.3847/1538-4357/ae486b","url":null,"abstract":"Short gamma-ray bursts (GRBs) exhibiting a plateau phase provide valuable insights into the postmerger activity of their central engines. Although the physical origin of the plateau remains uncertain, the magnetar energy injection model offers a compelling explanation that reproduces the observed temporal and luminosity features. However, previous studies relying solely on X-ray data have suffered from strong parameter degeneracies when constraining the magnetar parameters. Here we perform broadband afterglow modeling on seven short GRBs with plateau features by combining X-ray, optical, and radio observations within the framework of the magnetar energy injection model. Key model parameters are derived by using the Markov Chain Monte Carlo method. It is found that the energy injection substantially modifies the afterglow dynamics in most events. Compared with X-ray-only analyses, our broadband modeling systematically yields a lower magnetic field strength and a shorter spin period for the central magnetar, corresponding to a higher injection luminosity. The study clearly shows that incorporating multiwavelength data effectively alleviates the degeneracy between the magnetar parameters and X-ray radiative efficiency. In addition, the distribution of our short GRBs differs markedly from long GRBs when they are plotted on the initial Lorentz factor versus gamma-ray energy plane. This offset, consistent with the observed harder spectrum of short GRBs, may serve as a useful diagnostic for investigating the progenitor as larger samples are available.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"51 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2026-03-16","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147461863","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}
Pub Date : 2026-03-13DOI: 10.3847/1538-4357/ae4479
C. Y. Tan, A. Drlica-Wagner, A. B. Pace, W. Cerny, E. O. Nadler, A. Doliva-Dolinsky, D. Anbajagane, T. S. Li, J. D. Simon, A. K. Vivas, A. R. Walker, M. Adamów, K. Bechtol, J. L. Carlin, Q. O. Casey, C. Chang, A. Chaturvedi, T.-Y. Cheng, A. Chiti, Y. Choi, D. Crnojević, P. S. Ferguson, R. A. Gruendl, A. P. Ji, G. Limberg, G. E. Medina, B. Mutlu-Pakdil, N. E. D. Noël, K. Overdeck, V. M. Placco, A. H. Riley, D. J. Sand, J. Sharp, N. F. Sherman, G. S. Stringfellow, R. H. Wechsler, M. Aguena, S. Allam, O. Alves, D. Bacon, D. Brooks, D. L. Burke, R. Camilleri, J. A. Carballo-Bello, A. Carnero Rosell, J. Carretero, L. N. da Costa, M. E. da Silva Pereira, T. M. Davis, J. De Vicente, S. Desai, S. Everett, B. Flaugher, J. Frieman, J. García-Bellido, D. Gruen, G. Gutierrez, K. Herner, S. R. Hinton, D. L. Hollowood, D. J. James, K. Kuehn, O. Lahav, S. Lee, J. L. Marshall, C. E. Martínez-Vázquez, P. Massana, J. Mena-Fernández, R. Miquel, J. Muir, J. Myles, R. L. C. Ogando, A. A. Plazas M..
The properties of Milky Way satellite galaxies have important implications for galaxy formation, reionization, and the fundamental physics of dark matter. However, the population of Milky Way satellites includes the faintest known galaxies, and current observations are incomplete. To understand the impact of observational selection effects on the known satellite population, we perform rigorous, quantitative estimates of the Milky Way satellite galaxy detection efficiency in three wide-field survey datasets: the Dark Energy Survey Year 6, the DECam Local Volume Exploration Data Release 3, and the Pan-STARRS1 Data Release 1. Together, these surveys cover ∼13,600 deg2 to g ∼ 24.0 and ∼27,700 deg2 to g ∼ 22.5, spanning ∼91% of the high-Galactic-latitude sky (∣b∣ ≥ 15°). We apply multiple detection algorithms over the combined footprint and recover 49 known satellites above a strict census detection threshold. To characterize the sensitivity of our census, we run our detection algorithms on a large set of simulated galaxies injected into the survey data, which allows us to develop models that predict the detectability of satellites as a function of their properties. We then fit an empirical model to our data and infer the luminosity function, radial distribution, and size–luminosity relation of Milky Way satellite galaxies. Our empirical model predicts a total of satellite galaxies with −20 ≤ MV ≤ 0, half-light radii of 15 ≤ r1/2, (pc) ≤ 3000, and galactocentric distances of 10 ≤ DGC(kpc) ≤ 300. We also identify a mild anisotropy in the angular distribution of the observed galaxies, at a significance of ∼2σ, which can be attributed to the clustering of satellites associated with the LMC.
{"title":"DELVE Milky Way Satellite Galaxy Census. I. Satellite Population and Survey Selection Function in DES, DELVE, and Pan-STARRS","authors":"C. Y. Tan, A. Drlica-Wagner, A. B. Pace, W. Cerny, E. O. Nadler, A. Doliva-Dolinsky, D. Anbajagane, T. S. Li, J. D. Simon, A. K. Vivas, A. R. Walker, M. Adamów, K. Bechtol, J. L. Carlin, Q. O. Casey, C. Chang, A. Chaturvedi, T.-Y. Cheng, A. Chiti, Y. Choi, D. Crnojević, P. S. Ferguson, R. A. Gruendl, A. P. Ji, G. Limberg, G. E. Medina, B. Mutlu-Pakdil, N. E. D. Noël, K. Overdeck, V. M. Placco, A. H. Riley, D. J. Sand, J. Sharp, N. F. Sherman, G. S. Stringfellow, R. H. Wechsler, M. Aguena, S. Allam, O. Alves, D. Bacon, D. Brooks, D. L. Burke, R. Camilleri, J. A. Carballo-Bello, A. Carnero Rosell, J. Carretero, L. N. da Costa, M. E. da Silva Pereira, T. M. Davis, J. De Vicente, S. Desai, S. Everett, B. Flaugher, J. Frieman, J. García-Bellido, D. Gruen, G. Gutierrez, K. Herner, S. R. Hinton, D. L. Hollowood, D. J. James, K. Kuehn, O. Lahav, S. Lee, J. L. Marshall, C. E. Martínez-Vázquez, P. Massana, J. Mena-Fernández, R. Miquel, J. Muir, J. Myles, R. L. C. Ogando, A. A. Plazas M..","doi":"10.3847/1538-4357/ae4479","DOIUrl":"https://doi.org/10.3847/1538-4357/ae4479","url":null,"abstract":"The properties of Milky Way satellite galaxies have important implications for galaxy formation, reionization, and the fundamental physics of dark matter. However, the population of Milky Way satellites includes the faintest known galaxies, and current observations are incomplete. To understand the impact of observational selection effects on the known satellite population, we perform rigorous, quantitative estimates of the Milky Way satellite galaxy detection efficiency in three wide-field survey datasets: the Dark Energy Survey Year 6, the DECam Local Volume Exploration Data Release 3, and the Pan-STARRS1 Data Release 1. Together, these surveys cover ∼13,600 deg2 to g ∼ 24.0 and ∼27,700 deg2 to g ∼ 22.5, spanning ∼91% of the high-Galactic-latitude sky (∣b∣ ≥ 15°). We apply multiple detection algorithms over the combined footprint and recover 49 known satellites above a strict census detection threshold. To characterize the sensitivity of our census, we run our detection algorithms on a large set of simulated galaxies injected into the survey data, which allows us to develop models that predict the detectability of satellites as a function of their properties. We then fit an empirical model to our data and infer the luminosity function, radial distribution, and size–luminosity relation of Milky Way satellite galaxies. Our empirical model predicts a total of satellite galaxies with −20 ≤ MV ≤ 0, half-light radii of 15 ≤ r1/2, (pc) ≤ 3000, and galactocentric distances of 10 ≤ DGC(kpc) ≤ 300. We also identify a mild anisotropy in the angular distribution of the observed galaxies, at a significance of ∼2σ, which can be attributed to the clustering of satellites associated with the LMC.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"26 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2026-03-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147440048","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}
Pub Date : 2026-03-13DOI: 10.3847/1538-4357/ae48fa
Jia Wang, Joshua H. Marks, Shiori Inada and Ralf I. Kaiser
Although oxygenated benzene derivatives are key precursors in the abiotic synthesis of biorelevant molecules and fundamental building blocks of functionalized polycyclic aromatic hydrocarbons, their formation mechanisms under interstellar conditions have remained largely unexplored. Here, we report the first bottom-up formation of phenol (C6H5OH) in low-temperature interstellar ice analogs composed of acetylene and water (C2H2–H2O). Utilizing vacuum ultraviolet photoionization reflectron time-of-flight mass spectrometry and resonance-enhanced multiphoton ionization, phenol, along with aromatic hydrocarbons including benzene (C6H6), phenylacetylene (C6H5CCH), styrene (C6H5CHCH2), naphthalene (C10H8), and phenanthrene (C14H10), were identified in the gas phase during temperature-programmed desorption. Among these species, styrene, naphthalene, and phenanthrene have not yet been detected in the interstellar medium, suggesting that they are suitable targets for future astronomical searches. These findings reveal viable low-temperature formation pathways for phenol through nonequilibrium chemistry in acetylene-containing interstellar ices, thereby advancing our understanding of the abiotic formation of oxygenated benzene derivatives in extraterrestrial environments.
{"title":"Bottom-up Formation of Phenol (C6H5OH) in Interstellar Analog Ices of Acetylene and Water Exposed to Ionizing Radiation","authors":"Jia Wang, Joshua H. Marks, Shiori Inada and Ralf I. Kaiser","doi":"10.3847/1538-4357/ae48fa","DOIUrl":"https://doi.org/10.3847/1538-4357/ae48fa","url":null,"abstract":"Although oxygenated benzene derivatives are key precursors in the abiotic synthesis of biorelevant molecules and fundamental building blocks of functionalized polycyclic aromatic hydrocarbons, their formation mechanisms under interstellar conditions have remained largely unexplored. Here, we report the first bottom-up formation of phenol (C6H5OH) in low-temperature interstellar ice analogs composed of acetylene and water (C2H2–H2O). Utilizing vacuum ultraviolet photoionization reflectron time-of-flight mass spectrometry and resonance-enhanced multiphoton ionization, phenol, along with aromatic hydrocarbons including benzene (C6H6), phenylacetylene (C6H5CCH), styrene (C6H5CHCH2), naphthalene (C10H8), and phenanthrene (C14H10), were identified in the gas phase during temperature-programmed desorption. Among these species, styrene, naphthalene, and phenanthrene have not yet been detected in the interstellar medium, suggesting that they are suitable targets for future astronomical searches. These findings reveal viable low-temperature formation pathways for phenol through nonequilibrium chemistry in acetylene-containing interstellar ices, thereby advancing our understanding of the abiotic formation of oxygenated benzene derivatives in extraterrestrial environments.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"15 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2026-03-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147440053","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}
Pub Date : 2026-03-13DOI: 10.3847/1538-4357/ae469c
Jithu J. Athalathil, Mohammed H. Talafha and Bhargav Vaidya
The solar dynamo relies on the regeneration of the poloidal magnetic field through processes strongly modulated by nonlinear feedback such as tilt quenching (TQ) and latitude quenching (LQ). These mechanisms play a decisive role in regulating the buildup of the Sun’s polar field, and in turn, the amplitude of future solar cycles. In this work, we employ physics-informed neural networks (PINNs) to solve the surface flux transport (SFT) equation, embedding physical constraints directly into the neural network framework. By systematically varying transport parameters, we isolate the relative contributions of TQ and LQ to polar dipole buildup. We use the residual dipole moment as a diagnostic for cycle-to-cycle amplification and show that TQ suppression strengthens with increasing diffusivity, while LQ dominates in advection-dominated regimes. The ratio ΔDLQ/ΔDTQ exhibits a smooth inverse-square dependence on the dynamo effectivity range, refining previous empirical fits with improved accuracy and reduced scatter. The results further reveal that the need for a decay term is not essential for PINN setup due to the training process. Compared with the traditional 1D SFT model, the PINN framework achieves significantly lower error metrics and more robust recovery of nonlinear trends. Our results suggest that the nonlinear interplay between LQ and TQ can naturally produce alternations between weak and strong cycles, providing a physical explanation for the observed even–odd cycle modulation. These findings demonstrate the potential of PINN as an accurate, efficient, and physically consistent tool for solar cycle prediction.
{"title":"Investigating Nonlinear Quenching Effects on Polar Field Buildup in the Sun Using Physics-informed Neural Networks","authors":"Jithu J. Athalathil, Mohammed H. Talafha and Bhargav Vaidya","doi":"10.3847/1538-4357/ae469c","DOIUrl":"https://doi.org/10.3847/1538-4357/ae469c","url":null,"abstract":"The solar dynamo relies on the regeneration of the poloidal magnetic field through processes strongly modulated by nonlinear feedback such as tilt quenching (TQ) and latitude quenching (LQ). These mechanisms play a decisive role in regulating the buildup of the Sun’s polar field, and in turn, the amplitude of future solar cycles. In this work, we employ physics-informed neural networks (PINNs) to solve the surface flux transport (SFT) equation, embedding physical constraints directly into the neural network framework. By systematically varying transport parameters, we isolate the relative contributions of TQ and LQ to polar dipole buildup. We use the residual dipole moment as a diagnostic for cycle-to-cycle amplification and show that TQ suppression strengthens with increasing diffusivity, while LQ dominates in advection-dominated regimes. The ratio ΔDLQ/ΔDTQ exhibits a smooth inverse-square dependence on the dynamo effectivity range, refining previous empirical fits with improved accuracy and reduced scatter. The results further reveal that the need for a decay term is not essential for PINN setup due to the training process. Compared with the traditional 1D SFT model, the PINN framework achieves significantly lower error metrics and more robust recovery of nonlinear trends. Our results suggest that the nonlinear interplay between LQ and TQ can naturally produce alternations between weak and strong cycles, providing a physical explanation for the observed even–odd cycle modulation. These findings demonstrate the potential of PINN as an accurate, efficient, and physically consistent tool for solar cycle prediction.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"19 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2026-03-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147447525","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}
Pub Date : 2026-03-13DOI: 10.3847/1538-4357/ae48e9
Jianxiang Liu, Yan Gong and Kai Liao
We perform a joint analysis of the Milky Way (MW) and Andromeda (M31) satellite populations to constrain the properties of fuzzy dark matter (FDM) and thermal-relic warm dark matter (WDM). We combine MW satellite observations from the Dark Energy Survey and Pan-STARRS1 with M31 satellite data from the Pan-Andromeda Archaeological Survey, and model the corresponding observable satellite populations using the empirical galaxy–halo connection model described in Nadler et al. (2020) together with the appropriate selection functions. Uncertainties in the virial masses of the MW and M31 are incorporated through host-mass priors that linearly scale the relevant model parameters, allowing us to infer the full posterior distributions of all parameters. For the FDM case, we obtain mFDM > 1.74 × 10−20 eV (95% CL) and mFDM > 1.42 × 10−20 eV (20:1 posterior ratio). For thermal-relic WDM, we find mWDM > 6.20 keV (95% CL) and mWDM > 5.75 keV (20:1 posterior ratio). These results represent a moderate improvement over MW-only constraints and provide the strongest constraints to date on the FDM and WDM derived from satellite galaxy populations in the Local Group.
{"title":"Joint Constraints on Fuzzy and Warm Dark Matter from Satellite Populations of the Milky Way and Andromeda","authors":"Jianxiang Liu, Yan Gong and Kai Liao","doi":"10.3847/1538-4357/ae48e9","DOIUrl":"https://doi.org/10.3847/1538-4357/ae48e9","url":null,"abstract":"We perform a joint analysis of the Milky Way (MW) and Andromeda (M31) satellite populations to constrain the properties of fuzzy dark matter (FDM) and thermal-relic warm dark matter (WDM). We combine MW satellite observations from the Dark Energy Survey and Pan-STARRS1 with M31 satellite data from the Pan-Andromeda Archaeological Survey, and model the corresponding observable satellite populations using the empirical galaxy–halo connection model described in Nadler et al. (2020) together with the appropriate selection functions. Uncertainties in the virial masses of the MW and M31 are incorporated through host-mass priors that linearly scale the relevant model parameters, allowing us to infer the full posterior distributions of all parameters. For the FDM case, we obtain mFDM > 1.74 × 10−20 eV (95% CL) and mFDM > 1.42 × 10−20 eV (20:1 posterior ratio). For thermal-relic WDM, we find mWDM > 6.20 keV (95% CL) and mWDM > 5.75 keV (20:1 posterior ratio). These results represent a moderate improvement over MW-only constraints and provide the strongest constraints to date on the FDM and WDM derived from satellite galaxy populations in the Local Group.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"11 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2026-03-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147447522","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}
Pub Date : 2026-03-13DOI: 10.3847/1538-4357/ae4496
Khunanon Thongkham, Anthony H. Gonzalez, Mark Brodwin, Ariane Trudeau, Peter Eisenhardt, S. A. Stanford, Emily Moravec, Thomas Connor and Daniel Stern
The Massive and Distant Clusters of Wide-field Infrared Survey Explorer (WISE) Survey 2 (MaDCoWS2) is a WISE-selected catalog of galaxy clusters at 0.1 < z < 2 covering an effective area of >6000 deg2. In this paper, we derive splashback radii for this cluster ensemble from galaxy density profiles and constrain the mass threshold of the survey as a function of redshift. We use MaDCoWS2 cluster candidates at 0.4 ≤ z ≤ 1.65 divided into subsamples with different Poissonian signal-to-noise ratios (S/NPs) and redshifts, cross correlated with galaxies from the CatWISE2020 catalog, to obtain average surface density profiles. We perform a Markov Chain Monte Carlo analysis to derive parameter estimates for theoretical models consisting of orbiting and infalling terms. A distinct splashback feature is detected in all subsamples. The measured splashback radii span from cMpc ( pMpc) at to cMpc ( pMpc) at . We also find that the splashback radii increase with S/NP at fixed redshift. The resultant splashback radii constrain the redshift dependence of the mass of MaDCoWS2 clusters at fixed S/NP. We calculate M200m from the radii using a relation based on a cosmological simulation. MaDCoWS2 M200m values derived from the simulation-based relation are lower than the expected values based on weak-lensing observations. More robust mass constraints will come from calibrating splashback radii derived from galaxy density profiles with weak-lensing shear profiles from facilities such as Euclid, the Vera C. Rubin Observatory, and the Nancy Grace Roman Space Telescope.
广域红外巡天探测器（WISE）大质量和遥远星系团巡天2 （MaDCoWS2）是WISE选择的星系团目录，覆盖0.1 < z < 2的有效面积为>6000 deg2。在本文中，我们从星系密度曲线中推导出该星系团系综的反溅半径，并将调查的质量阈值约束为红移的函数。我们使用0.4≤z≤1.65的MaDCoWS2候选星团，将其分成具有不同泊松信噪比（S/NPs）和红移的子样本，并与CatWISE2020目录中的星系交叉相关，以获得平均表面密度剖面。我们执行马尔可夫链蒙特卡罗分析来导出由轨道项和落入项组成的理论模型的参数估计。在所有子样本中检测到明显的反溅特征。测得的反溅半径从cMpc （pMpc）点到cMpc （pMpc）点。我们还发现，当红移固定时，反溅半径随着S/NP的增大而增大。由此产生的反溅半径约束了固定S/NP下MaDCoWS2星团质量的红移依赖性。我们使用基于宇宙学模拟的关系从半径计算出M200m。基于模拟关系得到的MaDCoWS2 M200m值低于基于弱透镜观测的期望值。更强大的质量约束将来自于校准由星系密度曲线和弱透镜剪切曲线得出的反溅射半径，这些数据来自欧几里得、维拉·鲁宾天文台和南希·格蕾丝·罗马太空望远镜等设施。
{"title":"The Massive and Distant Clusters of WISE Survey 2: Splashback Radii to z = 1.65 from Galaxy Density Profiles","authors":"Khunanon Thongkham, Anthony H. Gonzalez, Mark Brodwin, Ariane Trudeau, Peter Eisenhardt, S. A. Stanford, Emily Moravec, Thomas Connor and Daniel Stern","doi":"10.3847/1538-4357/ae4496","DOIUrl":"https://doi.org/10.3847/1538-4357/ae4496","url":null,"abstract":"The Massive and Distant Clusters of Wide-field Infrared Survey Explorer (WISE) Survey 2 (MaDCoWS2) is a WISE-selected catalog of galaxy clusters at 0.1 < z < 2 covering an effective area of >6000 deg2. In this paper, we derive splashback radii for this cluster ensemble from galaxy density profiles and constrain the mass threshold of the survey as a function of redshift. We use MaDCoWS2 cluster candidates at 0.4 ≤ z ≤ 1.65 divided into subsamples with different Poissonian signal-to-noise ratios (S/NPs) and redshifts, cross correlated with galaxies from the CatWISE2020 catalog, to obtain average surface density profiles. We perform a Markov Chain Monte Carlo analysis to derive parameter estimates for theoretical models consisting of orbiting and infalling terms. A distinct splashback feature is detected in all subsamples. The measured splashback radii span from cMpc ( pMpc) at to cMpc ( pMpc) at . We also find that the splashback radii increase with S/NP at fixed redshift. The resultant splashback radii constrain the redshift dependence of the mass of MaDCoWS2 clusters at fixed S/NP. We calculate M200m from the radii using a relation based on a cosmological simulation. MaDCoWS2 M200m values derived from the simulation-based relation are lower than the expected values based on weak-lensing observations. More robust mass constraints will come from calibrating splashback radii derived from galaxy density profiles with weak-lensing shear profiles from facilities such as Euclid, the Vera C. Rubin Observatory, and the Nancy Grace Roman Space Telescope.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"7 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2026-03-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147440049","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}
Pub Date : 2026-03-13DOI: 10.3847/1538-4357/ae3db0
Jiahang Zou, Tie Liu, Sheng-Li Qin, Yaping Peng, Fengwei Xu, Xunchuan Liu, Li Chen, Xindi Tang, Sami Dib, Zi-Yang Li, Hong-Li Liu, Mika Juvela, Patricio Sanhueza, Pablo Garcia, Chang Won Lee, Guido Garay, Swagat R. Das, Yan-Kun Zhang, Kee-Tae Kim, Jeong-Eun Lee, Meizhu Liu, Leonardo Bronfman, Zhiping Kou, Dongting Yang, Gang Wu, Jihye Hwang, Dezhao Meng, Mengyao Tang and James O. Chibueze
Methanol (CH3OH) is a key complex organic molecule (COM) in the interstellar medium, widely used as a tracer of dense gas and hot molecular cores (HMCs). Using high-resolution Atacama Large Millimeter/submillimeter Array observations from the ATOMS survey, we investigate the excitation and abundance of methanol nuclear spin isomers and their relationship to chemical complexity in massive star-forming cores. We identify 20 methanol transitions, including A- and E-type lines in the v = 0 state and E-type lines in the vt = 1 state, and detect 94 HMC candidates. Rotational temperature analysis under the LTE assumption yields average values of 194 ± 33 K for CH3OH-E vt = 1, 178 ± 33 K for CH3OH-A v = 0, and 75 ± 21 K for CH3OH-E v = 0. Emission from COMs other than methanol is detected in 87 of the 94 cores, with the CH3OH-E vt = 1 line intensity showing a strong correlation with the channel detection ratio (CDR). These results demonstrate that CH3OH-E vt = 1 lines are reliable tracers of HMCs and chemical complexity, and that the CDR provides a robust indicator of molecular richness. The temperature difference between A- and E-type methanol transitions is driven by anomalously strong J(2,J-2)−J(-1,J-1) lines, highlighting the importance of analyzing methanol symmetry types separately.
{"title":"The ALMA-ATOMS Survey: Methanol Emission in a Large Sample of Hot Molecular Cores","authors":"Jiahang Zou, Tie Liu, Sheng-Li Qin, Yaping Peng, Fengwei Xu, Xunchuan Liu, Li Chen, Xindi Tang, Sami Dib, Zi-Yang Li, Hong-Li Liu, Mika Juvela, Patricio Sanhueza, Pablo Garcia, Chang Won Lee, Guido Garay, Swagat R. Das, Yan-Kun Zhang, Kee-Tae Kim, Jeong-Eun Lee, Meizhu Liu, Leonardo Bronfman, Zhiping Kou, Dongting Yang, Gang Wu, Jihye Hwang, Dezhao Meng, Mengyao Tang and James O. Chibueze","doi":"10.3847/1538-4357/ae3db0","DOIUrl":"https://doi.org/10.3847/1538-4357/ae3db0","url":null,"abstract":"Methanol (CH3OH) is a key complex organic molecule (COM) in the interstellar medium, widely used as a tracer of dense gas and hot molecular cores (HMCs). Using high-resolution Atacama Large Millimeter/submillimeter Array observations from the ATOMS survey, we investigate the excitation and abundance of methanol nuclear spin isomers and their relationship to chemical complexity in massive star-forming cores. We identify 20 methanol transitions, including A- and E-type lines in the v = 0 state and E-type lines in the vt = 1 state, and detect 94 HMC candidates. Rotational temperature analysis under the LTE assumption yields average values of 194 ± 33 K for CH3OH-E vt = 1, 178 ± 33 K for CH3OH-A v = 0, and 75 ± 21 K for CH3OH-E v = 0. Emission from COMs other than methanol is detected in 87 of the 94 cores, with the CH3OH-E vt = 1 line intensity showing a strong correlation with the channel detection ratio (CDR). These results demonstrate that CH3OH-E vt = 1 lines are reliable tracers of HMCs and chemical complexity, and that the CDR provides a robust indicator of molecular richness. The temperature difference between A- and E-type methanol transitions is driven by anomalously strong J(2,J-2)−J(-1,J-1) lines, highlighting the importance of analyzing methanol symmetry types separately.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"8 9-10 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2026-03-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147440043","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}
Pub Date : 2026-03-13DOI: 10.3847/1538-4357/ae40f8
Samuzal Barua, Hengxiao Guo, Minfeng Gu and Wenwen Zuo
Recent reverberation delay measurements have moved beyond the 10 keV X-ray range, providing evidence for the Compton hump (aka the reflection hump) in the lag spectra. We report the relativistic reverberation of the reflection hump in the bright Seyfert 1 galaxy IC 4329A based on a long Nuclear Spectroscopic Telescope Array (NuSTAR) observation. We find a delayed response of the 20–30 keV X-ray band, with a lag time of ∼1825 s at frequencies of 0.5–1.5 × 10−4 Hz. The lag amplitude drops to ∼195 s as the frequencies increase to (1.5–10) × 10−4 Hz. Including IC 4329A, so far five sources have been explored for reflection hump reverberation. We perform reverberation modeling of the 3–50 keV lag-energy spectra using the general relativistic transfer function code, which provides independent timing-based measurements of the black hole mass and the coronal height (with uncertainties at 90% confidence). Within the uncertainties, the measured mass is found to be consistent with the previous finding. Furthermore, we undertake reflection spectroscopy to account for the hump feature and the associated relativistic effect using the time-averaged flux spectrum. Further sampling of the NuSTAR data (with a bin width of 0.2/0.4 keV below and above 10 keV) that reshapes the spectral resolution allows us to constrain the coronal temperature at keV—consistent with the previous result from the combined Suzaku and NuSTAR data.
{"title":"Compton Hump Reverberation Lag in the Bright Seyfert 1 Galaxy IC 4329A with NuSTAR","authors":"Samuzal Barua, Hengxiao Guo, Minfeng Gu and Wenwen Zuo","doi":"10.3847/1538-4357/ae40f8","DOIUrl":"https://doi.org/10.3847/1538-4357/ae40f8","url":null,"abstract":"Recent reverberation delay measurements have moved beyond the 10 keV X-ray range, providing evidence for the Compton hump (aka the reflection hump) in the lag spectra. We report the relativistic reverberation of the reflection hump in the bright Seyfert 1 galaxy IC 4329A based on a long Nuclear Spectroscopic Telescope Array (NuSTAR) observation. We find a delayed response of the 20–30 keV X-ray band, with a lag time of ∼1825 s at frequencies of 0.5–1.5 × 10−4 Hz. The lag amplitude drops to ∼195 s as the frequencies increase to (1.5–10) × 10−4 Hz. Including IC 4329A, so far five sources have been explored for reflection hump reverberation. We perform reverberation modeling of the 3–50 keV lag-energy spectra using the general relativistic transfer function code, which provides independent timing-based measurements of the black hole mass and the coronal height (with uncertainties at 90% confidence). Within the uncertainties, the measured mass is found to be consistent with the previous finding. Furthermore, we undertake reflection spectroscopy to account for the hump feature and the associated relativistic effect using the time-averaged flux spectrum. Further sampling of the NuSTAR data (with a bin width of 0.2/0.4 keV below and above 10 keV) that reshapes the spectral resolution allows us to constrain the coronal temperature at keV—consistent with the previous result from the combined Suzaku and NuSTAR data.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"57 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2026-03-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147440044","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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