The Astrophysical Journal Letters最新文献

{"title":"Dynamo Confinement of a Radiatively Spreading Solar Tachocline Revealed by Self-consistent Global Simulations","authors":"Loren I. Matilsky, Lydia Korre and Nicholas H. Brummell","doi":"10.3847/2041-8213/adefe3","DOIUrl":"https://doi.org/10.3847/2041-8213/adefe3","url":null,"abstract":"The helioseismically observed solar tachocline is a thin internal boundary layer of shear that separates the rigidly rotating solar radiative zone from the differentially rotating convective zone and is believed to play a central role in the 22-yr solar dynamo cycle. The observed thinness of the tachocline has long been a mystery, given the expected tendency of such shear to undergo radiative spreading. Radiative spreading is the process by which the meridional circulation and angular velocity burrow into a stably stratified fluid owing to the mitigating effect of radiative thermal diffusion. A confinement mechanism is thus required to keep the tachocline so thin. In previous work using global dynamo simulations, we achieved a statistically stationary confined tachocline for which the confinement mechanism was derived from the Maxwell stresses arising from a dynamo-generated nonaxisymmetric poloidal magnetic field. However, the parameters chosen meant that the tachocline was confined against viscous spreading instead of radiative spreading. Here, we show that this previously identified dynamo confinement scenario still succeeds in a simulation that lies in the more solar-like radiative spreading regime. In particular, a nonaxisymmetric, quasi-cyclic dynamo develops in the convective zone and overshoot layer, penetrates into the radiative zone via a novel type of skin effect, and creates Maxwell stresses that confine the tachocline over many magnetic cycles. To the best of our knowledge, this is the first fully self-consistent rendering of a confined tachocline in a global numerical simulation in the parameter regime appropriate to the Sun.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"24 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-09-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145035514","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Explaining the Weak Evolution of the High-redshift Mass–Metallicity Relation with Galaxy Burst Cycles","authors":"Andrew Marszewski, Claude-André Faucher-Giguère, Robert Feldmann and Guochao Sun","doi":"10.3847/2041-8213/adf74b","DOIUrl":"https://doi.org/10.3847/2041-8213/adf74b","url":null,"abstract":"Recent observations suggest a nearly constant gas-phase mass–metallicity relation (MZR) at z ≳ 5, in agreement with many theoretical predictions. This lack of evolution contrasts with observations at z ≲ 3, which find an increasing normalization of the MZR with decreasing redshift. We analyze a high-redshift suite of FIRE-2 cosmological zoom-in simulations to identify the physical drivers of the MZR. Previous studies have explained the weak evolution of the high-redshift MZR in terms of weakly evolving or saturated gas fractions, but we find that this alone does not explain the evolution in FIRE-2. Instead, stellar feedback following intense bursts of star formation drives enriched gas out of galaxies, resetting their interstellar medium and separating their histories into distinct “burst cycles.” We develop the “reduced burst model,” a simplified gas-regulator model that successfully reproduces the simulated MZR and identifies the dominant drivers of its evolution. As redshift decreases, the metallicity of inflows within burst cycles increases at fixed stellar mass due to increased wind recycling of enriched gas. Meanwhile, the metal mass produced by stars per inflowing gas mass within these cycles decreases because of decreased star formation per gas mass inflowing into the galaxy. The effects of these two processes on the median metallicity largely cancel, holding the MZR constant for z = 5–12. At fixed stellar mass, the simulations predict lower gas metallicities at higher Hα-derived star formation rates, in qualitative agreement with the fundamental metallicity relation, but this effect is reduced in rest UV-selected samples.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"72 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-09-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145031849","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Cosmic Cascades: How Disk Substructure Regulates the Flow of Water to Inner Planetary Systems","authors":"Sebastiaan Krijt, Andrea Banzatti, Ke Zhang, Paola Pinilla, Till Kaeufer, Edwin A. Bergin, Colette Salyk, Klaus Pontoppidan, Geoffrey A. Blake, Feng Long, Jane Huang, María José Colmenares, Joe Williams, Adrien Houge, Mayank Narang, Miguel Vioque, Michiel Lambrechts, L. Ilsedore Cleeves, Karin Öberg and The JDISCS Collaboration","doi":"10.3847/2041-8213/adfbe3","DOIUrl":"https://doi.org/10.3847/2041-8213/adfbe3","url":null,"abstract":"The influx of icy pebbles to the inner regions of protoplanetary disks constitutes a fundamental ingredient in most planet formation theories. The observational determination of the magnitude of this pebble flux and its dependence on disk substructure (disk gaps as pebble traps) would be a significant step forward. In this work, we analyze a sample of 21 T Tauri disks (with ages ≈0.5–2 Myr) using JWST/MIRI spectra homogeneously reduced with the JDISCS pipeline and high-angular-resolution Atacama Large Millimeter/submillimeter Array (ALMA) continuum data. We find that the 1500/6000 K water line flux ratio measured with JWST—a tracer of cold water vapor and pebble drift near the snow line—correlates with the radial location of the innermost dust gap in ALMA continuum observations (ranging from 8.7 to 69 au), confirming predictions from recent models that study connections between the inner and outer disk reservoirs. We develop a population synthesis exploration of pebble drift in gapped disks and find a good match to the observed trend for early and relatively effective gaps, while scenarios where pebble drift happens quickly, gaps are very leaky, or where gaps form late, are all disfavored on a population level. Inferred snow line pebble mass fluxes (ranging between 10−6 and 10−3M⊕ yr−1 depending on gap position) are comparable to fluxes used in pebble accretion studies and those proposed for the inner solar system, while system-to-system variations suggest differences in the emerging planetary system architectures and water budgets.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"9 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145025407","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The Impact of Organic Hazes and Graphite on the Observation of CO2-rich Sub-Neptune Atmospheres","authors":"Haixin Li, Chao He, Sai Wang, Zhengbo Yang, Yu Liu, Yingjian Wang, Xiao’ou Luo, Sarah E. Moran, Cara Pesciotta, Sarah M. Hörst, Julianne I. Moses and Véronique Vuitton","doi":"10.3847/2041-8213/adfa87","DOIUrl":"https://doi.org/10.3847/2041-8213/adfa87","url":null,"abstract":"Many sub-Neptune and super-Earth exoplanets are expected to develop metal-enriched atmospheres due to atmospheric loss processes such as photoevaporation or core-powered mass loss. Thermochemical equilibrium calculations predict that at high metallicity and a temperature range of 300–700 K, CO2 becomes the dominant carbon species, and graphite may be the thermodynamically favored condensate under low-pressure conditions. Building on prior laboratory findings that such environments yield organic haze rather than graphite, we measured the transmittance spectra of organic haze analogs and graphite samples and computed their optical constants across the measured wavelength range from 0.4 to 25 μm. The organic haze exhibits strong vibrational absorption bands, notably at 3.0, 4.5, and 6.0 μm, while graphite shows featureless broadband absorption. The derived optical constants of haze and graphite provide the first data set for organic haze analogs formed in CO2-rich atmospheres and offer improved applicability over prior graphite data derived from bulk reflectance or ellipsometry. We implemented these optical constants into the Virga and PICASO cloud and radiative transfer models to simulate transit spectra for GJ 1214b. The synthetic spectra with organic hazes reproduce the muted spectral features in the near-infrared observed by Hubble and general trends observed by JWST for GJ 1214b, while graphite models yield flat spectra across the observed wavelengths. This suggests haze features may serve as observational markers of carbon-rich atmospheres, whereas graphite’s opacity could lead to radius overestimation, offering a possible explanation for superpuff exoplanets. Our work supplies essential optical to infrared data for interpreting observations of CO2-rich exoplanet atmospheres.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145025406","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Growing the Intermediate-mass Black Hole in Omega Centauri","authors":"Elena González Prieto, Carl L. Rodriguez and Tomás Cabrera","doi":"10.3847/2041-8213/adfd4a","DOIUrl":"https://doi.org/10.3847/2041-8213/adfd4a","url":null,"abstract":"The recent detection of fast-moving stars in the core of Omega Centauri (ω Cen), the most massive globular cluster (GC) in the Milky Way, has provided strong evidence for the presence of an intermediate-mass black hole (IMBH). As ω Cen is likely the accreted nucleus of a dwarf galaxy, this IMBH also represents a unique opportunity to study black hole (BH) seeding mechanisms and their potential role in the formation of supermassive BHs. We present Monte Carlo N-body models of ω Cen with detailed treatments for the loss-cone dynamics involving stars, binaries, and compact objects. Starting with BH seeds of 500–5000 M⊙ (consistent with runaway collisions of massive stars), our cluster models grow IMBHs with masses of ∼50,000 M⊙ after 12 Gyr, while successfully reproducing the present-day surface brightness and velocity dispersion profiles of ω Cen. We find a population of fast stars similar to those observed in the core of ω Cen, with the fastest stars originating from binaries that were tidally disrupted by the IMBH. The IMBH growth is primarily driven by mergers with 30–40 M⊙BHs, suggesting a present-day IMBH–BH merger rate of ∼(4–8) × 10−8 yr−1 in ω Cen–like GCs. Our models also predict a similar rate of tidal disruption events (TDEs; ∼5 × 10−8 yr−1), which, depending on the frequency of ω Cen–like GCs per galaxy, may represent anywhere from 0.1% to 10% of the observed TDE rate.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"57 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145025410","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"A Unified Picture of Swirl-driven Solar Coronal Heating: Magnetic Energy Supply and Dissipation","authors":"Hidetaka Kuniyoshi, Shinsuke Imada and Takaaki Yokoyama","doi":"10.3847/2041-8213/adfc61","DOIUrl":"https://doi.org/10.3847/2041-8213/adfc61","url":null,"abstract":"The coronal heating problem is one of the most critical challenges in solar physics. Recent observations have revealed that small-scale swirls are ubiquitous in the photosphere and chromosphere, suggesting that they may play a significant role in transferring magnetic energy into the corona. However, the overall contribution of swirls to the total magnetic energy supply and subsequent coronal heating remains uncertain. To address this, we perform statistical analyses of simulated swirls using a three-dimensional radiative magnetohydrodynamic simulation extending from the convection zone to the corona in the quiet Sun. Our results reveal that swirls account for approximately half of the total magnetic energy. Furthermore, they strongly suggest that swirls can trigger coronal heating events through magnetic reconnection. The occurrence frequency of these events follows a power-law-like distribution, consistent with observations of coronal heating signatures known as “nanoflares,” indicating that swirls are promising candidates as their drivers.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"2 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145025408","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Discovery of Hα Emission from a Protoplanet Candidate around the Young Star 2MASS J16120668–3010270 with MagAO-X","authors":"Jialin Li, 嘉霖 李, Laird M. Close, Feng Long, 凤 龙, Jared R. Males, Sebastiaan Y. Haffert, Alycia Weinberger, Katherine Follette, Sean Andrews, John Carpenter, Warren B. Foster, Kyle Van Gorkom, Alexander D. Hedglen, Gregory J. Herczeg, 雷歌 沈, Parker T. Johnson, Maggie Y. Kautz, Jay K. Kueny, Rixin Li, Joshua Liberman, Joseph D. Long, Jennifer Lumbres, Sebastian Marino, Luca Matrà, Eden A. McEwen, Olivier Guyon, Logan A. Pearce, Laura M. Pérez, Paola Pinilla, Lauren Schatz, Yangfan Shi, Katie Twitchell, Kevin Wagner, David Wilner, Ya-Lin Wu, Shangjia Zhang, 尚嘉 张 and Zhaohuan Zhu","doi":"10.3847/2041-8213/adfcbd","DOIUrl":"https://doi.org/10.3847/2041-8213/adfcbd","url":null,"abstract":"2MASS J16120668–3010270 (hereafter 2MJ1612) is a young M0 star that hosts a protoplanetary disk in the Upper Scorpius star-forming region. Recent Atacama Large Millimeter/submillimeter Array (ALMA) observations of 2MJ1612 show a mildly inclined disk (i = 37°) with a large dust-depleted gap (Rcav ≈ 0 4 or 53 au). We present high-contrast Hα observations from MagAO-X on the 6.5 m Magellan telescope and new high-resolution submillimeter dust continuum observations with ALMA of 2MJ1612. On both 2025 April 13 and 16, we recovered a point source with Hα excess with a signal-to-noise ratio ≳5 within the disk gap in our MagAO-X angular and spectral differential images at a separation of 141.96 ± 2.10 mas (23.45 ± 0.29 au deprojected) from the star and a position angle of 159 00 ± 0 55. Furthermore, this Hα source is within close proximity to a K-band point source in the SPHERE/IRDIS observation taken on 2023 July 21. The astrometric offset between the K band and Hα source can be explained by orbital motion of a bound companion. Thus, our observations can be best explained by the discovery of an accreting protoplanet, 2MJ1612 b, with an estimated mass of 4 MJup and a Hα line flux ranging from (29.7 ± 7.5) × 10−16 erg s cm2 to (8.2 ± 3.4) × 10−16 erg s cm2. 2MJ1612 b is likely the third example of an accreting Hα protoplanet responsible for carving the gap in its host disk, joining PDS 70 b and c. Further study is necessary to confirm and characterize this protoplanet candidate and to identify any additional protoplanets that may also play a role in shaping the gap.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"103 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145025409","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Early Shock Cooling Observations and Progenitor Constraints of Type IIb Supernova SN 2024uwq","authors":"Bhagya M. Subrayan, David J. Sand, K. Azalee Bostroem, Saurabh W. Jha, Aravind P. Ravi, Michaela Schwab, Jennifer E. Andrews, Griffin Hosseinzadeh, Stefano Valenti, Yize Dong, 一泽 董, Jeniveve Pearson, Manisha Shrestha, Lindsey A. Kwok, Emily Hoang, Jeonghee Rho, Seong Hyun Park, Sung-Chul Yoon, T. R. Geballe, Joshua Haislip, Daryl Janzen, Vladimir Kouprianov, Darshana Mehta, Nicolás Meza Retamal, Daniel E. Reichart, Moira Andrews, Joseph Farah, Megan Newsome, D. Andrew Howell and Curtis McCully","doi":"10.3847/2041-8213/adfe52","DOIUrl":"https://doi.org/10.3847/2041-8213/adfe52","url":null,"abstract":"We present early multiwavelength photometric and spectroscopic observations of the Type IIb supernova SN 2024uwq, capturing its shock-cooling emission phase and double-peaked light-curve evolution. Early spectra reveal broad Hα (v ∼ 15,500 km s−1) and He I P Cygni profiles of similar strengths. Over time the He I lines increase in strength while the Hα decreases, consistent with a hydrogen envelope (Menv = 0.7–1.35 M⊙) overlying helium-rich ejecta. Analytic modeling of early shock cooling emission and bolometric light analysis constrains the progenitor to a partially stripped star with radius R = 10–60 R⊙, consistent with a blue/yellow supergiant with an initial zero-age main-sequence mass of 12–20 M⊙ likely stripped via binary interaction. SN 2024uwq occupies a transitional position between compact and extended Type IIb supernovae, highlighting the role of binary mass transfer efficiency in shaping a continuum of stripped-envelope progenitors. Our results underscore the importance of early UV/optical observations to characterize shock breakout signatures critical to map the diversity in evolutionary pathways of massive stars. Upcoming time-domain surveys, including Rubin Observatory’s LSST and UV missions like ULTRASAT and UVEX, will revolutionize our ability to systematically capture these early signatures, probing the full diversity of stripped progenitors and their explosive endpoints.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"13 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145025411","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Tidal Suppression of Fuzzy Dark Matter Heating in Milky Way Satellite Galaxies","authors":"Yu-Ming Yang, Zhao-Chen Zhang, Xiao-Jun Bi and Peng-Fei Yin","doi":"10.3847/2041-8213/adff81","DOIUrl":"https://doi.org/10.3847/2041-8213/adff81","url":null,"abstract":"Many previous studies have imposed stringent constraints on the particle mass of fuzzy dark matter (FDM) by analyzing observations of Galactic satellite galaxies, which show no significant evidence of the heating effect predicted by FDM. However, these analyses have generally neglected the tidal influence of the Milky Way (MW), which can substantially suppress the FDM-induced heating effect in satellites. This oversight arises from computational challenges of accurately capturing the tidal effects in FDM simulations. In this study, we present a novel simulation framework that, for the first time, enables the simulation of an FDM-stellar system within an observationally motivated gravitational potential of the MW. This framework incorporates the diverse Galactic components, including the gravitational influence of the Large Magellanic Cloud. Using the Fornax dwarf galaxy as a case study, we demonstrate that tidal effects significantly alleviate the tension between observational data and the predicted heating effect for an FDM particle mass of ma ∼ 10−22 eV.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"2 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145025412","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Discovery of the Second Y+Y Dwarf Binary System: CWISEP J193518.59-154620.3","authors":"Matthew De Furio, Jacqueline Kelly Faherty, Daniella C. Bardalez Gagliuffi, Jonathan Gagné, Eileen C. Gonzales, Rocio Kiman, Marc Kuchner, Federico Marocco, Sherelyn Alejandro Merchan, Melanie Rowland, Adam C. Schneider, Genaro Suárez and Johanna M. Vos","doi":"10.3847/2041-8213/adfee1","DOIUrl":"https://doi.org/10.3847/2041-8213/adfee1","url":null,"abstract":"We present the discovery of a companion to the Y dwarf, CWISEP J193518.59–154620.3, the second Y-Y dwarf binary detected to date. Y dwarfs are the coldest known free-floating objects (<500 K) and, on average, represent the lowest mass objects directly formed through turbulent fragmentation of a molecular cloud. Studying their multiplicity allows us to place strong constraints on the ability to form multiple systems of planetary masses and approach the opacity limit of fragmentation. Due to their physical properties, Y dwarfs also serve as analogs to gas giant planets. CWISEP J193518.59–154620.3 has been shown to have a unique methane emission feature in its near-infrared spectrum at 3.326 μm, potentially indicative of auroral processes without a clear origin. CWISEP J193518.59–154620.3 was observed with JWST’s MIRI in the F1000W, F1280W, and F1800W filters. We applied a point-spread function (PSF) fitting algorithm using empirically derived PSF models and resolved a companion in the F1000W and F1280W filters separated by 172 mas and 2.48 au, assuming a distance of 14.43 pc. Using the ATMO2020 evolutionary models, we estimate a mass of 12–39 MJup for the primary and 7–24 MJup for the companion, assuming an age of 1–10 Gyr for a mass ratio of 0.55–0.62, resulting in an estimated period of 16–28 yr. It is unknown which component of this binary exhibits the methane emission feature. We also resolve known companions WISE J014656.66+423410.0B and WISE J171104.60+350036.8B using MIRI data and present their F1000W and F1280W photometry.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"72 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-09-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145017667","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}