The Astrophysical Journal最新文献_第7页

The Atacama Cosmology Telescope: Systematic Transient Search of Single Observation Maps 阿塔卡马宇宙望远镜：单观测图的系统瞬态搜索

The Astrophysical Journal Pub Date : 2025-06-01 DOI: 10.3847/1538-4357/adce70

Emily Biermann, Yaqiong Li, Sigurd Naess, Steve K. Choi, Susan E. Clark, Mark Devlin, Jo Dunkley, P. A. Gallardo, Yilun Guan, Allen Foster, Matthew Hasselfield, Carlos Hervías-Caimapo, Matt Hilton, Adam D. Hincks, Anna Y. Q. Ho, John C. Hood, Kevin M. Huffenberger, Arthur Kosowsky, Michael D. Niemack, John Orlowski-Scherer, Lyman Page, Bruce Partridge, Maria Salatino, Cristóbal Sifón, Suzanne T. Staggs, Cristian Vargas and Edward J. Wollack

{"title":"The Atacama Cosmology Telescope: Systematic Transient Search of Single Observation Maps","authors":"Emily Biermann, Yaqiong Li, Sigurd Naess, Steve K. Choi, Susan E. Clark, Mark Devlin, Jo Dunkley, P. A. Gallardo, Yilun Guan, Allen Foster, Matthew Hasselfield, Carlos Hervías-Caimapo, Matt Hilton, Adam D. Hincks, Anna Y. Q. Ho, John C. Hood, Kevin M. Huffenberger, Arthur Kosowsky, Michael D. Niemack, John Orlowski-Scherer, Lyman Page, Bruce Partridge, Maria Salatino, Cristóbal Sifón, Suzanne T. Staggs, Cristian Vargas and Edward J. Wollack","doi":"10.3847/1538-4357/adce70","DOIUrl":"https://doi.org/10.3847/1538-4357/adce70","url":null,"abstract":"We conduct a systematic search for astrophysical transients using data from the Atacama Cosmology Telescope. The data were taken from 2017 to 2022 in three frequency bands spanning 77 to 277 GHz. In this paper, we present a pipeline for transient detection using single-observation maps where each pixel of a map contains one observation with an integration time of approximately 4 minutes. We detect 34 transient events at 27 unique locations. All but two of the transients are associated with Galactic stars and exhibit a wide range of properties. We also detect an event coincident with the classical nova YZ Ret and one event consistent with a flaring active galactic nucleus. We notably do not detect any reverse shock emission from gamma-ray bursts, a nondetection that may be in tension with current models.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"135 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144193020","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

Uncertainties in the Inference of Internal Structure: The Case of TRAPPIST-1 f 内部结构推断中的不确定性：以TRAPPIST-1为例

The Astrophysical Journal Pub Date : 2025-06-01 DOI: 10.3847/1538-4357/add34b

David R. Rice, Chenliang Huang, Jason H. Steffen and Allona Vazan

{"title":"Uncertainties in the Inference of Internal Structure: The Case of TRAPPIST-1 f","authors":"David R. Rice, Chenliang Huang, Jason H. Steffen and Allona Vazan","doi":"10.3847/1538-4357/add34b","DOIUrl":"https://doi.org/10.3847/1538-4357/add34b","url":null,"abstract":"We use the TRAPPIST-1 system as a model observation of Earth-like planets. The densities of these planets being 1%–10% less than the Earth suggest that the outer planets may host significant hydrospheres. We explore the uncertainty in water mass fraction (wmf) from observed mass and radius. We investigate the interior structure of TRAPPIST-1 f (T1-f) using the open-source solver MAGRATHEA and varying assumptions in the interior model. We find that T1-f likely has a wmf of 16.2% ± 9.9% when considering all possible core mass fractions, and requires 6.9% ± 2.0% water at an Earth-like mantle-to-core ratio. We quantify uncertainties from observational precision, model assumptions, and experimental and theoretical data on the bulk modulus of planet-building materials. We show that observational uncertainties are smaller than model assumptions of mantle mineralogy and core composition but larger than hydrosphere, temperature, and equation-of-state assumptions/uncertainties. Our findings show that while precise mass and radius measurements are crucial, uncertainties in planetary models can often outweigh those from observations, emphasizing the importance of refining both theoretical models and experimental data to better understand exoplanet interiors.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"13 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144193023","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

Tracking the Jet-like Corona of Black Hole Swift J1727.8−1613 during a Flare State through Type-C Quasiperiodic Oscillations 通过c型准周期振荡跟踪黑洞Swift J1727.8−1613在耀斑状态下的喷流状日冕

The Astrophysical Journal Pub Date : 2025-06-01 DOI: 10.3847/1538-4357/add264

Jie Liao, Ning Chang, Lang Cui, Pengfei Jiang, Didong Mou, Yongfeng Huang, Tao An, Luis C. Ho, Hua Feng, Yu-Cong Fu, Hongmin Cao, Ashutosh Tripathi and Xiang Liu

{"title":"Tracking the Jet-like Corona of Black Hole Swift J1727.8−1613 during a Flare State through Type-C Quasiperiodic Oscillations","authors":"Jie Liao, Ning Chang, Lang Cui, Pengfei Jiang, Didong Mou, Yongfeng Huang, Tao An, Luis C. Ho, Hua Feng, Yu-Cong Fu, Hongmin Cao, Ashutosh Tripathi and Xiang Liu","doi":"10.3847/1538-4357/add264","DOIUrl":"https://doi.org/10.3847/1538-4357/add264","url":null,"abstract":"Type-C quasiperiodic oscillations (QPOs) in black hole X-ray transients typically manifest in the low-hard and hard-intermediate states. This study presents a detailed spectral and temporal analysis of the black hole candidate Swift J1727.8−1613 using NICER observations from 2023 August and September, with a focus on the first flare period. We detected Type-C QPOs whose centroid frequency increased from 0.33 Hz to 2.63 Hz. An additional increase in frequency was observed when the outburst entered a flare period. The time-averaged spectra, along with the rms and phase-lag spectra of the QPOs, were jointly fitted using the time-dependent Comptonization model vkompthdk to examine the geometry of the corona during this flare. Correlations between spectral and temporal properties suggest that the detected type-C QPOs are primarily modulated by Lense–Thirring precession. Leveraging simultaneous radio observations that indicate discrete jet ejections, we propose a scenario to describe the coevolution of the disk–corona–jet during a flare (∼3 days). This scenario is partially supported for the first time by polarization data in the soft gamma-ray band from the IBIS instrument on board the International Gamma-Ray Astrophysics Laboratory. A phenomenological analysis of the corona scenario was also conducted.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"29 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144193025","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

A Unified, Physical Framework for Mean Motion Resonances 平均运动共振的统一物理框架

The Astrophysical Journal Pub Date : 2025-06-01 DOI: 10.3847/1538-4357/adc1c4

Daniel Tamayo and Samuel Hadden

{"title":"A Unified, Physical Framework for Mean Motion Resonances","authors":"Daniel Tamayo and Samuel Hadden","doi":"10.3847/1538-4357/adc1c4","DOIUrl":"https://doi.org/10.3847/1538-4357/adc1c4","url":null,"abstract":"The traditional approach to analyzing mean motion resonances (MMRs) is through the canonical perturbation theory. While this is a powerful method, its generality leads to complicated combinations of variables that are challenging to interpret and require looking up numerical coefficients particular to every different resonance. In this paper, we develop simpler scaling relations in the limit where orbits are closely spaced (period ratios ≲2), and interplanetary interactions can be approximated by only considering the close approaches each time the inner planet overtakes the outer at the conjunction. We develop geometric arguments for several powerful results: (i) that p:p − q MMRs of the same order q are all rescaled versions of one another, (ii) that the general case of two massive planets on closely spaced, eccentric, coplanar orbits can be approximately mapped onto the much simpler case of an eccentric test particle perturbed by a massive planet on a coplanar circular orbit, and (iii) that, while the effects of consecutive conjunctions add up coherently for first-order (p:p − 1) MMRs, they partially cancel for p:p − q MMRs with order q > 1, providing a physical explanation for why these higher-order MMRs are weaker and can often be ignored. Finally, we provide simple expressions for the widths of MMRs and their associated oscillation frequencies that are universal to all closely spaced MMRs of a given order q, in the pendulum approximation.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"26 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144193164","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

XMM-Newton Observations of the High Temperature Plasma in the Large Magellanic Cloud Supernova Remnant N132D 大麦哲伦星云超新星遗迹N132D中高温等离子体的xmm -牛顿观测

The Astrophysical Journal Pub Date : 2025-06-01 DOI: 10.3847/1538-4357/adcd61

Adam R. Foster, Paul P. Plucinsky, Terrance J. Gaetz, Xi Long and Diab Jerius

{"title":"XMM-Newton Observations of the High Temperature Plasma in the Large Magellanic Cloud Supernova Remnant N132D","authors":"Adam R. Foster, Paul P. Plucinsky, Terrance J. Gaetz, Xi Long and Diab Jerius","doi":"10.3847/1538-4357/adcd61","DOIUrl":"https://doi.org/10.3847/1538-4357/adcd61","url":null,"abstract":"We present an analysis of the archival XMM-Newton observations of the Large Magellanic Cloud (LMC) supernova remnant N132D totaling more than 500 ks. We focus on the high temperature plasma (kTe ∼ 4.5 keV) that is responsible for the high energy continuum and exciting the Fe K emission. An image analysis shows that the Fe K emission is mainly concentrated in the southern part of the remnant interior to the region defined by the forward shock. This Fe K distribution would be consistent with an asymmetric distribution of the Fe ejecta and/or an asymmetric interaction between the reverse shock and the Fe ejecta. We compare the EPIC-pn and EPIC-MOS spectra in the 3.0–12.0 keV bandpass with a model based on RGS data plus a higher temperature component, in collisional ionization equilibrium (CIE), or nonequilibrium (both ionizing and recombining). We find that the data are equally well fitted by the CIE and ionizing models. Assuming the CIE and ionizing spectral models, the Fe in this high temperature component is significantly enhanced with respect to typical LMC abundances. We can place only an upper limit on the neutral Fe K line. We conclude that the Fe K emission is due to ejecta heated by the reverse shock given the spatial distribution, relatively high temperature, and enhanced abundance. We estimate the progenitor mass based on the Ca/Fe and Ni/Fe mass ratios to be 13 ≤ MP ≤ 15M⊙.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"5 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144193165","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

Thermal Desorption Kinetics, Binding Energies, and Entrapment of Methyl Mercaptan Ices 甲基硫醇冰的热解吸动力学、结合能和俘获

The Astrophysical Journal Pub Date : 2025-06-01 DOI: 10.3847/1538-4357/adc7b6

Suchitra Narayanan, Elettra L. Piacentino, Karin I. Öberg and Mahesh Rajappan

{"title":"Thermal Desorption Kinetics, Binding Energies, and Entrapment of Methyl Mercaptan Ices","authors":"Suchitra Narayanan, Elettra L. Piacentino, Karin I. Öberg and Mahesh Rajappan","doi":"10.3847/1538-4357/adc7b6","DOIUrl":"https://doi.org/10.3847/1538-4357/adc7b6","url":null,"abstract":"Organosulfur species are potential major carriers of sulfur in the interstellar medium, as well as interesting ingredients in prebiotic chemistry. The most fundamental question regarding these species is under which conditions they reside in the gas versus solid phase. Here, we characterize the thermal desorption kinetics, binding energies, and entrapment of the organosulfur methyl mercaptan (CH3SH, or MeSH) in different ice environments, comparing them with those of methanol (CH3OH, or MeOH) ices. The derived multilayer (pure MeSH–MeSH) and submonolayer (layered MeSH–H2O) binding energies are surprisingly similar, corresponding to snow line locations where the disk midplane temperature is ∼105 K. In both H2O-dominated and more realistic H2O:CO2-dominated ices, 100% of the MeSH is entrapped, almost exclusively desorbing at the molecular volcano desorption peak, indicating that MeSH is retained at the water snow line if initially mixed with water ice during formation. Additionally, the presence of MeSH in an ice mixture enhances the entrapment of CO2 and MeOH (up to 100%) until the onset of volcano desorption; without MeSH, both desorb at their respective pure desorption temperatures and also codesorb with water. Compared to MeOH, MeSH binds less well to water, explaining why MeSH escapes during water ice crystallization rather than codesorbing with water. These results show that the larger relative size of MeSH compared to MeOH significantly impacts its ability to bind to water and its entrapment efficiency. Therefore, molecular size plays an important role in the adsorption and retention of S-bearing organics and, in turn, other volatiles in ices.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"37 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144193161","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

Cue: A Fast and Flexible Photoionization Emulator for Modeling Nebular Emission Powered by Almost Any Ionizing Source 提示：一个快速和灵活的光电离模拟器，用于模拟几乎任何电离源驱动的星云发射

The Astrophysical Journal Pub Date : 2025-06-01 DOI: 10.3847/1538-4357/adcab4

Yijia Li, 轶佳李, Joel Leja, Benjamin D. Johnson, Sandro Tacchella, Rebecca Davies, Sirio Belli, Minjung Park and Razieh Emami

{"title":"Cue: A Fast and Flexible Photoionization Emulator for Modeling Nebular Emission Powered by Almost Any Ionizing Source","authors":"Yijia Li, 轶佳李, Joel Leja, Benjamin D. Johnson, Sandro Tacchella, Rebecca Davies, Sirio Belli, Minjung Park and Razieh Emami","doi":"10.3847/1538-4357/adcab4","DOIUrl":"https://doi.org/10.3847/1538-4357/adcab4","url":null,"abstract":"The complex physics governing nebular emission in galaxies, particularly in the early Universe, often defy simple low-dimensional models. This has proven to be a significant barrier in understanding the (often diverse) ionizing sources powering this emission. We present Cue,10a highly flexible tool for interpreting nebular emission across a wide range of abundances and ionizing conditions of galaxies at different redshifts. Unlike typical nebular models used to interpret extragalactic nebular emission, our model does not require a specific ionizing spectrum as a source, instead approximating the ionizing spectrum with a four-part piecewise power law. We train a neural net emulator based on the CLOUDY photoionization modeling code and make self-consistent nebular continuum and line emission predictions. Along with the flexible ionizing spectra, we allow freedom in [O/H], [N/O], [C/O], gas density, and total ionizing photon budget. This flexibility allows us to either marginalize over or directly measure the incident ionizing radiation, thereby directly interrogating the source of the ionizing photons in distant galaxies via their nebular emission. Our emulator demonstrates a high accuracy, with ∼1% uncertainty in predicting the nebular continuum and ∼5% uncertainty in the emission lines. Mock tests suggest Cue is well calibrated and produces useful constraints on the ionizing spectra when the signal-to-noise ratio of Hα is ≳10, and furthermore capable of distinguishing between the ionizing spectra predicted by single and binary stellar models. The computational efficiency of neural networks facilitates future applications of Cue for rapid modeling of the nebular emission in large samples and Monte Carlo sampling techniques.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"8 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144193162","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

Constraints on the Galaxy Formation Models during the Epoch of Reionization with High-redshift Observations 高红移观测对再电离时期星系形成模型的约束

The Astrophysical Journal Pub Date : 2025-06-01 DOI: 10.3847/1538-4357/add015

Qing-Bo Ma, Xiao-Rong Chen, Ming Li, Qi Guo, Benedetta Ciardi, Anshuman Acharya and Xin Wang

引用次数: 0

Revisiting the X-Ray Polarization of the Shell of Cassiopeia A Using Spectropolarimetric Analysis 用光谱偏振分析重新研究仙后座A壳的x射线偏振

The Astrophysical Journal Pub Date : 2025-06-01 DOI: 10.3847/1538-4357/adcedb

A. Mercuri, E. Greco, J. Vink, R. Ferrazzoli and S. Perri

{"title":"Revisiting the X-Ray Polarization of the Shell of Cassiopeia A Using Spectropolarimetric Analysis","authors":"A. Mercuri, E. Greco, J. Vink, R. Ferrazzoli and S. Perri","doi":"10.3847/1538-4357/adcedb","DOIUrl":"https://doi.org/10.3847/1538-4357/adcedb","url":null,"abstract":"X-ray synchrotron radiation is expected to be highly polarized. Thanks to the Imaging X-ray Polarimetry Explorer (IXPE), it is now possible to evaluate the degree of X-ray polarization in sources such as supernova remnants (SNRs). Jointly using IXPE data and high-resolution Chandra observations, we perform a spatially resolved spectropolarimetric analysis of SNR Cassiopeia A (Cas A). We focus on the 3–6 keV energy band on regions near the shell dominated by nonthermal synchrotron emission. By combining IXPE’s polarization sensitivity with Chandra’s higher spatial and spectral resolution, we constrain the local polarization degree (PD) and polarization angle across the remnant. Our analysis reveals PD values ranging locally from 10% to 26%, showing significant regional variations that underscore the complex magnetic field morphology of Cas A. The polarization vectors indicate a predominantly radial magnetic field, consistent with previous studies. Thanks to the improved modeling of thermal contamination using Chandra data, we retrieve higher PD values compared to earlier IXPE analysis and more significant detections with respect to the standard IXPEOBSSIM analysis. Finally, we also estimate the degree of magnetic turbulence η from the measured photon index and PD, under the assumption of an isotropic fluctuating field across the shell of Cas A.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144193019","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 Trends in JWST Transiting Exoplanet Atmospheres JWST凌日系外行星大气的统计趋势

The Astrophysical Journal Pub Date : 2025-06-01 DOI: 10.3847/1538-4357/ad7bb8

Guangwei Fu, Kevin B. Stevenson, David K. Sing, Sagnick Mukherjee, Luis Welbanks, Daniel Thorngren, Shang-Min Tsai, Peter Gao, Joshua Lothringer, Thomas G. Beatty, Cyril Gapp, Thomas M. Evans-Soma, Romain Allart, Stefan Pelletier, Pa Chia Thao and Andrew W. Mann

{"title":"Statistical Trends in JWST Transiting Exoplanet Atmospheres","authors":"Guangwei Fu, Kevin B. Stevenson, David K. Sing, Sagnick Mukherjee, Luis Welbanks, Daniel Thorngren, Shang-Min Tsai, Peter Gao, Joshua Lothringer, Thomas G. Beatty, Cyril Gapp, Thomas M. Evans-Soma, Romain Allart, Stefan Pelletier, Pa Chia Thao and Andrew W. Mann","doi":"10.3847/1538-4357/ad7bb8","DOIUrl":"https://doi.org/10.3847/1538-4357/ad7bb8","url":null,"abstract":"Our brains are hardwired for pattern recognition as correlations are useful for predicting and understanding nature. As more exoplanet atmospheres are being characterized with JWST, we are starting to unveil their properties on a population level. Here we present a framework for comparing exoplanet transmission spectroscopy from 3 to 5 μm with four bands: L (2.9–3.7 μm), SO2 (3.95–4.1 μm), CO2 (4.25–4.4 μm), and CO (4.5–4.9 μm). Together, the four bands cover the major carbon-, oxygen-, nitrogen-, and sulfur-bearing molecules including H2O, CH4, NH3, H2S, SO2, CO2, and CO. Among the eight high-precision gas giant exoplanet planet spectra we collect, we find strong correlations between the SO2 – L index and planet mass (r = −0.41 ± 0.09) and temperature (r = −0.64 ± 0.08), indicating SO2 preferably exists (SO2 – L > −0.5) among low-mass (∼ <0.3 MJ) and cooler (∼ <1200 K) targets. We also observe strong temperature dependency for both CO2 – L and CO – L indices. Under equilibrium chemistry and isothermal thermal structure assumptions, we find that the planet sample favors supersolar metallicity and a low C/O ratio (<0.7). In addition, the presence of a mass–metallicity correlation is favored over uniform metallicity with the eight planets. We further introduce the SO2 – L versus CO2 – L diagram, similar to the color–magnitude diagram for stars and brown dwarfs. All reported trends here will be testable and will be further quantified with existing and future JWST observations within the next few years.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"5 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144193029","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