Pub Date : 2026-04-05DOI: 10.3847/1538-4357/ae50ed
Maksim I. Chazov, Dmitry I. Makarov, R. Brent Tully, Gagandeep S. Anand, Lidia N. Makarova, Yotam Cohen, John P. Blakeslee, Michele Cantiello, Joseph B. Jensen and Gabriella Raimondo
Observations with JWST in the F090W band provide a powerful tool for determining galaxy distances based on tip of the red giant branch (TRGB) measurements. It is a great convenience that the TRGB lies at an almost constant absolute magnitude level at low metallicities. However, the TRGB becomes fainter at high metallicities in the F090W filter. Details of this break in slope are critical for precision applications in the acquisition of distances. With an absolute scaling set by the maser distance to NGC 4258 (but excluding the uncertainty in that distance), the value mag (traditional Vega) is found for (F090W − F150W)0 < 1.65 mag. The theoretical RGB isochrone that reaches the color 1.65 at the RGB tip corresponds to metallicity [M/H] = −0.57 for a 10 Gyr population. The calibration is used to derive distances for 16 galaxies relative to the megamaser host NGC 4258. Revised distances are on average slightly closer than literature values derived from the same data.
{"title":"The TRGB-SBF Project. IV. A Color Calibration of the TRGB in the JWST F090W+F150W Filters","authors":"Maksim I. Chazov, Dmitry I. Makarov, R. Brent Tully, Gagandeep S. Anand, Lidia N. Makarova, Yotam Cohen, John P. Blakeslee, Michele Cantiello, Joseph B. Jensen and Gabriella Raimondo","doi":"10.3847/1538-4357/ae50ed","DOIUrl":"https://doi.org/10.3847/1538-4357/ae50ed","url":null,"abstract":"Observations with JWST in the F090W band provide a powerful tool for determining galaxy distances based on tip of the red giant branch (TRGB) measurements. It is a great convenience that the TRGB lies at an almost constant absolute magnitude level at low metallicities. However, the TRGB becomes fainter at high metallicities in the F090W filter. Details of this break in slope are critical for precision applications in the acquisition of distances. With an absolute scaling set by the maser distance to NGC 4258 (but excluding the uncertainty in that distance), the value mag (traditional Vega) is found for (F090W − F150W)0 < 1.65 mag. The theoretical RGB isochrone that reaches the color 1.65 at the RGB tip corresponds to metallicity [M/H] = −0.57 for a 10 Gyr population. The calibration is used to derive distances for 16 galaxies relative to the megamaser host NGC 4258. Revised distances are on average slightly closer than literature values derived from the same data.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"277 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2026-04-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147619632","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}
Investigating the intrinsic distributions of gamma-ray bursts (GRBs) is essential for understanding their physical origins, as these properties are closely tied to the central engine, radiation mechanisms, and cosmological evolution. In this study, we examine the intrinsic parameters of GRBs using synthetic populations calibrated to Fermi Gamma-ray Burst Monitor (Fermi-GBM) observations. We generated a large GRB population through Monte Carlo–based population modeling, simulated the Fermi-GBM detector response, and performed spectral fitting for simulated detected bursts. By comparing the simulation output with actual Fermi-GBM data, we find that the observed properties of the simulated bursts show good agreement with real observations, demonstrating the reliability of our simulation pipeline and spectral-fitting procedures. We also identify a noticeable deviation in the β parameter between the intrinsic distribution (before detector response) and the observed distribution (after detector response), which is likely driven by statistical uncertainties under low signal-to-noise conditions. Based on the validated simulations, we derive the intrinsic distributions of key long-GRB properties—including luminosity, isotropic energy, and redshift—and estimate a local GRB rate of 1.41 ± 0.22 Gpc−3 yr−1.
{"title":"Intrinsic Distribution of Gamma-Ray Bursts. I. Insights from Fermi-GBM Observations","authors":"Shan-Jie Shu, Yu-Hua Yao, Tian-Lu Chen, Yi-Qing Guo, Fang-Sheng Min, Qi-Ling Chen, Jia-Dan Xie, Qiang Yuan and You-Liang Feng","doi":"10.3847/1538-4357/ae52f2","DOIUrl":"https://doi.org/10.3847/1538-4357/ae52f2","url":null,"abstract":"Investigating the intrinsic distributions of gamma-ray bursts (GRBs) is essential for understanding their physical origins, as these properties are closely tied to the central engine, radiation mechanisms, and cosmological evolution. In this study, we examine the intrinsic parameters of GRBs using synthetic populations calibrated to Fermi Gamma-ray Burst Monitor (Fermi-GBM) observations. We generated a large GRB population through Monte Carlo–based population modeling, simulated the Fermi-GBM detector response, and performed spectral fitting for simulated detected bursts. By comparing the simulation output with actual Fermi-GBM data, we find that the observed properties of the simulated bursts show good agreement with real observations, demonstrating the reliability of our simulation pipeline and spectral-fitting procedures. We also identify a noticeable deviation in the β parameter between the intrinsic distribution (before detector response) and the observed distribution (after detector response), which is likely driven by statistical uncertainties under low signal-to-noise conditions. Based on the validated simulations, we derive the intrinsic distributions of key long-GRB properties—including luminosity, isotropic energy, and redshift—and estimate a local GRB rate of 1.41 ± 0.22 Gpc−3 yr−1.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"122 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2026-04-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147619639","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 : 2026-04-05DOI: 10.3847/1538-4357/ae505e
J. V. Sales-Silva, K. Cunha, V. V. Smith, S. Daflon, D. Souto, R. Guerço, V. Loaiza-Tacuri, A. Queiroz, C. Chiappini, I. Minchev, S. R. Majewski, B. Barbuy, D. Bizyaev, José G. Fernández-Trincado, Peter M. Frinchaboy, S. Hasselquist, D. Horta, Henrik Jönsson, T. Masseron, N. Prantzos, R. P. Schiavon, M. Schultheis and M. Zoccali
The Milky Way bulge bar is composed of multiple populations. Using chemical and kinematical planes, we segregate six populations in a bulge bar sample observed by the APOGEE survey: two with bar-driven orbits, two with eccentric orbits, and two with low-eccentricity orbits, each composed of low- and high-[Mg/Fe] stars. Our sample spans −2.0 ≲ [Fe/H] ≲ +0.5 and Galactocentric distance RGal < 6 kpc. We use chemical abundances from APOGEE DR17 for the elements Mg, Si, Ca, Al, K, Mn, Co, Ni, and Fe and from the BAWLAS catalog for Ce and Nd. We find that the low- and high-[Mg/Fe] stars with low-eccentricity orbits, which exhibit chemical and orbital characteristics similar to those of the low- and high-[α/Fe] disks, display slightly negative and positive metallicity gradients, respectively. This result for the low-[Mg/Fe], low-eccentricity stars indicates a break in the global thin-disk metallicity gradient. The high-eccentricity populations with both low and high [Mg/Fe] show approximately flat metallicity gradients. In general, the [X/H] gradients of all elements for all populations follow Fe, except for the neutron-capture elements Ce and Nd. For all elements, the high-[Mg/Fe] bar population shows a much steeper positive [X/H] gradient than the nearly flat gradient for the low-[Mg/Fe] bar stars. The positive [X/H] gradients observed among our high-[Mg/Fe] bar stars probably reflect an age variation along the peanut structure. This interpretation agrees with the N-body simulations. Such steep positive gradients have also been reported in some high-redshift (z ∼ 4–10) galaxies.
{"title":"Chemical Radial Gradients for the Bulge Bar Stellar Populations from the APOGEE Survey","authors":"J. V. Sales-Silva, K. Cunha, V. V. Smith, S. Daflon, D. Souto, R. Guerço, V. Loaiza-Tacuri, A. Queiroz, C. Chiappini, I. Minchev, S. R. Majewski, B. Barbuy, D. Bizyaev, José G. Fernández-Trincado, Peter M. Frinchaboy, S. Hasselquist, D. Horta, Henrik Jönsson, T. Masseron, N. Prantzos, R. P. Schiavon, M. Schultheis and M. Zoccali","doi":"10.3847/1538-4357/ae505e","DOIUrl":"https://doi.org/10.3847/1538-4357/ae505e","url":null,"abstract":"The Milky Way bulge bar is composed of multiple populations. Using chemical and kinematical planes, we segregate six populations in a bulge bar sample observed by the APOGEE survey: two with bar-driven orbits, two with eccentric orbits, and two with low-eccentricity orbits, each composed of low- and high-[Mg/Fe] stars. Our sample spans −2.0 ≲ [Fe/H] ≲ +0.5 and Galactocentric distance RGal < 6 kpc. We use chemical abundances from APOGEE DR17 for the elements Mg, Si, Ca, Al, K, Mn, Co, Ni, and Fe and from the BAWLAS catalog for Ce and Nd. We find that the low- and high-[Mg/Fe] stars with low-eccentricity orbits, which exhibit chemical and orbital characteristics similar to those of the low- and high-[α/Fe] disks, display slightly negative and positive metallicity gradients, respectively. This result for the low-[Mg/Fe], low-eccentricity stars indicates a break in the global thin-disk metallicity gradient. The high-eccentricity populations with both low and high [Mg/Fe] show approximately flat metallicity gradients. In general, the [X/H] gradients of all elements for all populations follow Fe, except for the neutron-capture elements Ce and Nd. For all elements, the high-[Mg/Fe] bar population shows a much steeper positive [X/H] gradient than the nearly flat gradient for the low-[Mg/Fe] bar stars. The positive [X/H] gradients observed among our high-[Mg/Fe] bar stars probably reflect an age variation along the peanut structure. This interpretation agrees with the N-body simulations. Such steep positive gradients have also been reported in some high-redshift (z ∼ 4–10) galaxies.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"8 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2026-04-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147619648","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 : 2026-04-05DOI: 10.3847/1538-4357/ae4e23
Ian Chow, Mario Jurić, R. Lynne Jones, Kathleen Kiker, Joachim Moeyens, Peter G. Brown, Aren N. Heinze and Jacob A. Kurlander
Imminent impactors are natural bodies discovered in space before impacting the Earth. They provide a rare opportunity to characterize individual near-Earth objects (NEOs) in great detail as asteroids in space, meteors in Earth’s atmosphere, and meteorites on the ground. The Vera C. Rubin Observatory’s upcoming Legacy Survey of Space and Time (LSST) is expected to transform our understanding of the NEO population. In this work, we evaluate LSST’s expected discovery performance for imminent impactors using 343 meter-size objects previously recorded in NASA’s CNEOS database as fireballs impacting Earth’s atmosphere. We simulate pre-impact observations of these CNEOS impactors with the Sorcha survey simulator under LSST’s default three-night discovery strategy and a one-night strategy for fast-moving objects that relies on matching aligned streaks in two exposures on the same night. We estimate that LSST will discover ∼1–2 meter-size and larger imminent impactors per year, representing ∼4% of all Earth impactors ≳1 m in diameter and almost doubling the current discovery rate of imminent impactors. The median time of discovery and median time of first observation for impactors discovered in our simulations are ∼1.57 and ∼3.06 days before impact, respectively. The spatial distribution of the 11 previously discovered imminent impactors is biased toward the Northern Hemisphere, where the observatories that discovered them are located. We find a similar trend toward Southern Hemisphere impacts in our simulated LSST detections of the CNEOS impactors, suggesting Rubin will provide a powerful counterpart to existing asteroid surveys primarily located in the Northern Hemisphere.
即将到来的撞击是在撞击地球之前在太空中发现的自然天体。它们提供了一个难得的机会，可以非常详细地描述太空中的小行星、地球大气层中的流星和地面上的陨石等单个近地天体。Vera C. Rubin天文台即将进行的时空遗产调查（LSST）有望改变我们对近地天体数量的理解。在这项工作中，我们利用NASA CNEOS数据库中先前记录的343米大小的物体作为撞击地球大气层的火球来评估LSST对即将到来的撞击物的预期发现性能。在LSST默认的三晚发现策略和快速移动物体的一晚策略下，我们使用Sorcha调查模拟器模拟了这些CNEOS撞击物的撞击前观测，该策略依赖于在同一晚上的两次曝光中匹配对齐的条纹。我们估计LSST每年将发现~ 1 - 2米大小或更大的撞击天体，占所有直径约1米的地球撞击天体的4%，几乎是目前发现撞击天体的两倍。在我们的模拟中发现的撞击物的发现和首次观测的中位数时间分别为撞击前的~ 1.57天和~ 3.06天。先前发现的11个即将到来的撞击物的空间分布偏向于发现它们的观测站所在的北半球。我们在模拟的LSST探测CNEOS撞击物中发现了类似的南半球撞击趋势，这表明鲁宾将为主要位于北半球的现有小行星调查提供强有力的对应。
{"title":"Predictions of Imminent Earth Impactors Discovered by LSST","authors":"Ian Chow, Mario Jurić, R. Lynne Jones, Kathleen Kiker, Joachim Moeyens, Peter G. Brown, Aren N. Heinze and Jacob A. Kurlander","doi":"10.3847/1538-4357/ae4e23","DOIUrl":"https://doi.org/10.3847/1538-4357/ae4e23","url":null,"abstract":"Imminent impactors are natural bodies discovered in space before impacting the Earth. They provide a rare opportunity to characterize individual near-Earth objects (NEOs) in great detail as asteroids in space, meteors in Earth’s atmosphere, and meteorites on the ground. The Vera C. Rubin Observatory’s upcoming Legacy Survey of Space and Time (LSST) is expected to transform our understanding of the NEO population. In this work, we evaluate LSST’s expected discovery performance for imminent impactors using 343 meter-size objects previously recorded in NASA’s CNEOS database as fireballs impacting Earth’s atmosphere. We simulate pre-impact observations of these CNEOS impactors with the Sorcha survey simulator under LSST’s default three-night discovery strategy and a one-night strategy for fast-moving objects that relies on matching aligned streaks in two exposures on the same night. We estimate that LSST will discover ∼1–2 meter-size and larger imminent impactors per year, representing ∼4% of all Earth impactors ≳1 m in diameter and almost doubling the current discovery rate of imminent impactors. The median time of discovery and median time of first observation for impactors discovered in our simulations are ∼1.57 and ∼3.06 days before impact, respectively. The spatial distribution of the 11 previously discovered imminent impactors is biased toward the Northern Hemisphere, where the observatories that discovered them are located. We find a similar trend toward Southern Hemisphere impacts in our simulated LSST detections of the CNEOS impactors, suggesting Rubin will provide a powerful counterpart to existing asteroid surveys primarily located in the Northern Hemisphere.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"122 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2026-04-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147625676","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 : 2026-04-05DOI: 10.3847/1538-4357/ae517f
Mattias Lazda, Kenzie Nimmo, Maria R. Drout, Benito Marcote, Jason W. T. Hessels, Eli Wiston, Raffaella Margutti, Omar Ould-Boukattine, Tanmoy Laskar, Jacco Vink, Ryan Chornock, James K. Leung, Deanne L. Coppejans, Dan Milisavljevic, Juan Mena-Parra and Dan Patnaude
Three leading models have been put forth to justify the observed radio re-brightening associated with stripped-envelope supernovae (SESNe) years post-explosion: radiation from an emerging pulsar wind nebula (PWN), shock interaction with a dense circumstellar medium (CSM), or emission from off-axis, relativistic jets. SN 2012au is a particularly intriguing SESN in this regard, as observations obtained ≳6 yr post-explosion have shown both (i) optical emission features consistent with a young PWN and (ii) a radio re-brightening. We present the results of our very long baseline interferometric (VLBI) observations of SN 2012au performed between 8 and 13 yr post core-collapse. Our VLBI observations reveal a luminous, steadily fading radio source that remains compact (≤1.4 × 1017 cm) and stationary (≤0.36c) over the course of our campaign. Overall, we find that our VLBI measurements can be readily explained by a ∼decade-old PWN, potentially explained by shock interaction with specific CSM geometries, and are unlikely to be explained by emission from an off-axis, relativistic jet. Assuming a PWN origin, our observations require that the initial spindown luminosity of the central pulsar be between and radio efficiency factor be ηR ≥ 3 × 10−7 (both quoted at the 99.7% confidence interval). These results are consistent with independent inferences obtained using optical spectroscopy of SN 2012au, alongside inferences of known Galactic systems. If a PWN origin is confirmed, SN 2012au would represent the first extragalactic PWN emerging from a modern-day SN, providing a novel opportunity to study the formation properties of a decade-old pulsar.
{"title":"VLBI Observations of SN 2012AU Reveal a Compact Radio Source a Decade Post Explosion","authors":"Mattias Lazda, Kenzie Nimmo, Maria R. Drout, Benito Marcote, Jason W. T. Hessels, Eli Wiston, Raffaella Margutti, Omar Ould-Boukattine, Tanmoy Laskar, Jacco Vink, Ryan Chornock, James K. Leung, Deanne L. Coppejans, Dan Milisavljevic, Juan Mena-Parra and Dan Patnaude","doi":"10.3847/1538-4357/ae517f","DOIUrl":"https://doi.org/10.3847/1538-4357/ae517f","url":null,"abstract":"Three leading models have been put forth to justify the observed radio re-brightening associated with stripped-envelope supernovae (SESNe) years post-explosion: radiation from an emerging pulsar wind nebula (PWN), shock interaction with a dense circumstellar medium (CSM), or emission from off-axis, relativistic jets. SN 2012au is a particularly intriguing SESN in this regard, as observations obtained ≳6 yr post-explosion have shown both (i) optical emission features consistent with a young PWN and (ii) a radio re-brightening. We present the results of our very long baseline interferometric (VLBI) observations of SN 2012au performed between 8 and 13 yr post core-collapse. Our VLBI observations reveal a luminous, steadily fading radio source that remains compact (≤1.4 × 1017 cm) and stationary (≤0.36c) over the course of our campaign. Overall, we find that our VLBI measurements can be readily explained by a ∼decade-old PWN, potentially explained by shock interaction with specific CSM geometries, and are unlikely to be explained by emission from an off-axis, relativistic jet. Assuming a PWN origin, our observations require that the initial spindown luminosity of the central pulsar be between and radio efficiency factor be ηR ≥ 3 × 10−7 (both quoted at the 99.7% confidence interval). These results are consistent with independent inferences obtained using optical spectroscopy of SN 2012au, alongside inferences of known Galactic systems. If a PWN origin is confirmed, SN 2012au would represent the first extragalactic PWN emerging from a modern-day SN, providing a novel opportunity to study the formation properties of a decade-old pulsar.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"112 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2026-04-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147625677","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 : 2026-04-05DOI: 10.3847/1538-4357/ae4c44
Verene Einwalter, Eric J. Hooper, Melissa E. Morris, Sarah Bach and Yjan A. Gordon
The Quick Look data products from the Very Large Array Sky Survey (VLASS) contain widespread imaging artifacts arising from the simplified imaging algorithm used in their production. The catalog of double radio sources associated with active galactic nuclei (DRAGNs) found in the VLASS first epoch Quick Look release using the DRAGNhunter algorithm suffers from contamination from these artifacts. These sources contain two or three individual components, each of which can be an artifact. We train random forest models to classify these DRAGNs based on the number of artifacts they contain, ranging from zero to three artifacts. We optimize our models and mitigate the class imbalance of our dataset with judicious training set selection, and the best of our models achieves a weighted F1 score of . Using our classifications, we produce a catalog of VLASS DRAGNs from which an estimated 99.3% complete catalog of 97.7% artifact-free sources can be extracted.
{"title":"DRAGNs in the Forest: Identifying Artifacts with Random Forest Models in the VLASS DRAGNs Catalog","authors":"Verene Einwalter, Eric J. Hooper, Melissa E. Morris, Sarah Bach and Yjan A. Gordon","doi":"10.3847/1538-4357/ae4c44","DOIUrl":"https://doi.org/10.3847/1538-4357/ae4c44","url":null,"abstract":"The Quick Look data products from the Very Large Array Sky Survey (VLASS) contain widespread imaging artifacts arising from the simplified imaging algorithm used in their production. The catalog of double radio sources associated with active galactic nuclei (DRAGNs) found in the VLASS first epoch Quick Look release using the DRAGNhunter algorithm suffers from contamination from these artifacts. These sources contain two or three individual components, each of which can be an artifact. We train random forest models to classify these DRAGNs based on the number of artifacts they contain, ranging from zero to three artifacts. We optimize our models and mitigate the class imbalance of our dataset with judicious training set selection, and the best of our models achieves a weighted F1 score of . Using our classifications, we produce a catalog of VLASS DRAGNs from which an estimated 99.3% complete catalog of 97.7% artifact-free sources can be extracted.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"64 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2026-04-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147619623","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 : 2026-04-05DOI: 10.3847/1538-4357/ae41b0
Catherine Cerny, Guillaume Mahler, Keren Sharon, Mathilde Jauzac, Gourav Khullar, Benjamin Beauchesne, Jose M. Diego, David J. Lagattuta, Marceau Limousin, Nency R. Patel, Johan Richard, Carla Cornil-Baïotto, Michael D. Gladders, Stephane V. Werner, Jessica E. Doppel, Benjamin Floyd, Anthony H. Gonzalez, Richard J. Massey, Mireia Montes, Matthew B. Bayliss, Lindsey E. Bleem, Rebecca E. A. Canning, Alastair C. Edge, Michael McDonald, Priyamvada Natarajan, Antony A. Stark and Raven Gassis
We leverage JWST’s superb resolution to derive strong-lensing mass maps of 14 clusters, spanning a redshift range of z ∼ 0.25–1.06 and a mass range of M500 ∼ 2–12 × 1014M⊙, from the Strong LensIng and Cluster Evolution (SLICE) JWST program. These clusters represent a small subsample of the first clusters observed in the SLICE program that are chosen based on the detection of new multiple-image constraints in the SLICE JWST NIRCam/F150W2 and F322W2 imaging. These constraints include new lensed dusty galaxies and new substructures in previously identified lensed background galaxies. Four clusters have never been modeled before. For the remaining 10 clusters, we present updated models based on JWST and Hubble Space Telescope imaging and, where available, ground-based spectroscopy. We model the global mass profile for each cluster and report the masses enclosed within 200 and 500 kpc. We report the number of new lensed source galaxies identified in the JWST imaging, which in one cluster is as high as 19 new lensed galaxies. The addition of new lensed source galaxies and constraints from substructure clumps improves the ability of strong-lensing models to accurately reproduce the interior mass distribution of each cluster. We also report the discovery of a candidate transient in a lensed image of the galaxy cluster SPT-CL J0516-5755. All lens models and their associated products are available for download at the Strong Lensing Cluster Atlas Data Base (https://data.lam.fr/sl-cluster-atlas/), which is hosted at Laboratoire d’Astrophysique de Marseille.
{"title":"Strong LensIng and Cluster Evolution (SLICE) with JWST: Early Results, Lens Models, and High-redshift Detections","authors":"Catherine Cerny, Guillaume Mahler, Keren Sharon, Mathilde Jauzac, Gourav Khullar, Benjamin Beauchesne, Jose M. Diego, David J. Lagattuta, Marceau Limousin, Nency R. Patel, Johan Richard, Carla Cornil-Baïotto, Michael D. Gladders, Stephane V. Werner, Jessica E. Doppel, Benjamin Floyd, Anthony H. Gonzalez, Richard J. Massey, Mireia Montes, Matthew B. Bayliss, Lindsey E. Bleem, Rebecca E. A. Canning, Alastair C. Edge, Michael McDonald, Priyamvada Natarajan, Antony A. Stark and Raven Gassis","doi":"10.3847/1538-4357/ae41b0","DOIUrl":"https://doi.org/10.3847/1538-4357/ae41b0","url":null,"abstract":"We leverage JWST’s superb resolution to derive strong-lensing mass maps of 14 clusters, spanning a redshift range of z ∼ 0.25–1.06 and a mass range of M500 ∼ 2–12 × 1014M⊙, from the Strong LensIng and Cluster Evolution (SLICE) JWST program. These clusters represent a small subsample of the first clusters observed in the SLICE program that are chosen based on the detection of new multiple-image constraints in the SLICE JWST NIRCam/F150W2 and F322W2 imaging. These constraints include new lensed dusty galaxies and new substructures in previously identified lensed background galaxies. Four clusters have never been modeled before. For the remaining 10 clusters, we present updated models based on JWST and Hubble Space Telescope imaging and, where available, ground-based spectroscopy. We model the global mass profile for each cluster and report the masses enclosed within 200 and 500 kpc. We report the number of new lensed source galaxies identified in the JWST imaging, which in one cluster is as high as 19 new lensed galaxies. The addition of new lensed source galaxies and constraints from substructure clumps improves the ability of strong-lensing models to accurately reproduce the interior mass distribution of each cluster. We also report the discovery of a candidate transient in a lensed image of the galaxy cluster SPT-CL J0516-5755. All lens models and their associated products are available for download at the Strong Lensing Cluster Atlas Data Base (https://data.lam.fr/sl-cluster-atlas/), which is hosted at Laboratoire d’Astrophysique de Marseille.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"2 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2026-04-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147619647","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 : 2026-04-05DOI: 10.3847/1538-4357/ae4eba
Charlotte Olsen, Eric Gawiser, Charlotte Welker, Harry Teplitz, Kartheik Iyer, Xin Wang, Marc Rafelski, Rogier A. Windhorst, Anton Koekemoer, Anahita Alavi, Ben Sunnquist, Norman Grogin, Yicheng Guo, Christopher J. Conselice, L. Y. Aaron Yung, Kalina Nedkova, Bahram Mobasher, Ray A. Lucas, Vihang Mehta, Y. Sophia Dai and Jonathan P. Gardner
Understanding the complicated processes that regulate star formation and cause a galaxy to become quiescent is key to our comprehension of galaxy evolution. We used eight well-resolved star-forming z < 0.3 galaxies from the UVCANDELS survey, where a total of 10 Hubble Space Telescope bands, including UV follow-up in UVIS/F275W, allow us to reconstruct the star formation histories (SFHs) of regions across each galaxy. This approach provides a powerful tool to explore the spatiotemporal connection between star formation and galaxy evolution. The spatial and temporal profiles of stellar mass and star formation rate (SFR) surface density were obtained from the SFHs of these regions. We measure scaling relations and projected radial profiles of regions within each galaxy at the time of observation and at 1 Gyr lookback time, noting possible trends in the evolution. By comparing the change in star formation over time, we can infer the timing and location of star formation and see early signs of star formation shutting off before quenching occurs. We compared the SFR density–stellar mass density scaling relations for individual galaxies as they evolve from 1 Gyr lookback time. The correlation lines pivot around a log-stellar mass surface density of 7.25 [M⊙ kpc−2], which may be evidence of a self-regulating process on these scales. Radial profiles of the galaxy logarithmic specific SFR (sSFR) show an overall decrease over 1 Gyr, but five galaxies show a greater change in log(sSFR) at the outskirts than the center, indicating a possible early onset of quenching in these galaxies.
{"title":"Searching within Galaxies for the Earliest Signs of Quenching With Spatially Resolved Star Formation Histories in UVCANDELS Galaxies at z < 0.3","authors":"Charlotte Olsen, Eric Gawiser, Charlotte Welker, Harry Teplitz, Kartheik Iyer, Xin Wang, Marc Rafelski, Rogier A. Windhorst, Anton Koekemoer, Anahita Alavi, Ben Sunnquist, Norman Grogin, Yicheng Guo, Christopher J. Conselice, L. Y. Aaron Yung, Kalina Nedkova, Bahram Mobasher, Ray A. Lucas, Vihang Mehta, Y. Sophia Dai and Jonathan P. Gardner","doi":"10.3847/1538-4357/ae4eba","DOIUrl":"https://doi.org/10.3847/1538-4357/ae4eba","url":null,"abstract":"Understanding the complicated processes that regulate star formation and cause a galaxy to become quiescent is key to our comprehension of galaxy evolution. We used eight well-resolved star-forming z < 0.3 galaxies from the UVCANDELS survey, where a total of 10 Hubble Space Telescope bands, including UV follow-up in UVIS/F275W, allow us to reconstruct the star formation histories (SFHs) of regions across each galaxy. This approach provides a powerful tool to explore the spatiotemporal connection between star formation and galaxy evolution. The spatial and temporal profiles of stellar mass and star formation rate (SFR) surface density were obtained from the SFHs of these regions. We measure scaling relations and projected radial profiles of regions within each galaxy at the time of observation and at 1 Gyr lookback time, noting possible trends in the evolution. By comparing the change in star formation over time, we can infer the timing and location of star formation and see early signs of star formation shutting off before quenching occurs. We compared the SFR density–stellar mass density scaling relations for individual galaxies as they evolve from 1 Gyr lookback time. The correlation lines pivot around a log-stellar mass surface density of 7.25 [M⊙ kpc−2], which may be evidence of a self-regulating process on these scales. Radial profiles of the galaxy logarithmic specific SFR (sSFR) show an overall decrease over 1 Gyr, but five galaxies show a greater change in log(sSFR) at the outskirts than the center, indicating a possible early onset of quenching in these galaxies.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2026-04-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147619635","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 : 2026-04-05DOI: 10.3847/1538-4357/ae4c58
Mingxi Chen, Kazumi Kashiyama and Masato Sato
Formation of a rapidly spinning, strongly magnetized neutron star (NS) may occur in various classes of core-collapse events. If the NS injects an amount of energy comparable to the explosion energy of the accompanying supernova (SN) before the SN ejecta becomes transparent, the nascent NS wind bubble can overtake the outer ejecta and undergo a blowout driven by hydrodynamic instabilities. Based on multidimensional numerical studies, we construct a minimal semi-analytic framework to follow the post-blowout dynamics and radiative evolution, map the blowout conditions by scanning the ejecta and NS parameters, and compute survey-ready multiband light curves. For stripped-envelope SNe with an ejecta mass of Mej ∼ 10 M⊙ and an explosion energy of , blowout occurs for NSs with magnetic field strengths of Bdip ≳ 1013 G and spin periods of PNS ≲ a few ms. Relatively weak-field cases with Bdip ≲ 1014 G produce luminous double-peaked UV/optical light curves, as observed in the superluminous SN LSQ14bdq, while stronger-field cases with Bdip ≳ 1014 G result in hypernovae preceded by X-ray blowout precursors. We also examine weaker and lower-mass SN explosions representing ultra-stripped SNe and accretion- or merger-induced collapse events, in which blowout is more readily achieved over a broader range of NS parameters, producing fast X-ray transients with durations of 102–4 s and peak luminosities of 1042–48 erg s−1. Our results encourage coordinated UV, optical, and X-ray observations that constrain the formation of the most energetic NSs in the Universe.
{"title":"Blowouts of Nascent Wind Bubbles in Pulsar-driven Supernovae","authors":"Mingxi Chen, Kazumi Kashiyama and Masato Sato","doi":"10.3847/1538-4357/ae4c58","DOIUrl":"https://doi.org/10.3847/1538-4357/ae4c58","url":null,"abstract":"Formation of a rapidly spinning, strongly magnetized neutron star (NS) may occur in various classes of core-collapse events. If the NS injects an amount of energy comparable to the explosion energy of the accompanying supernova (SN) before the SN ejecta becomes transparent, the nascent NS wind bubble can overtake the outer ejecta and undergo a blowout driven by hydrodynamic instabilities. Based on multidimensional numerical studies, we construct a minimal semi-analytic framework to follow the post-blowout dynamics and radiative evolution, map the blowout conditions by scanning the ejecta and NS parameters, and compute survey-ready multiband light curves. For stripped-envelope SNe with an ejecta mass of Mej ∼ 10 M⊙ and an explosion energy of , blowout occurs for NSs with magnetic field strengths of Bdip ≳ 1013 G and spin periods of PNS ≲ a few ms. Relatively weak-field cases with Bdip ≲ 1014 G produce luminous double-peaked UV/optical light curves, as observed in the superluminous SN LSQ14bdq, while stronger-field cases with Bdip ≳ 1014 G result in hypernovae preceded by X-ray blowout precursors. We also examine weaker and lower-mass SN explosions representing ultra-stripped SNe and accretion- or merger-induced collapse events, in which blowout is more readily achieved over a broader range of NS parameters, producing fast X-ray transients with durations of 102–4 s and peak luminosities of 1042–48 erg s−1. Our results encourage coordinated UV, optical, and X-ray observations that constrain the formation of the most energetic NSs in the Universe.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"113 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2026-04-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147619624","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 : 2026-04-05DOI: 10.3847/1538-4357/ae4fb5
Keyi Wang, Qiong Liu, Siyi Xu and Alberto Rebassa-Mansergas
Infrared (IR) excess observed around white dwarfs (WDs) is typically attributed to companions or debris disks. These systems are interesting because they offer a unique opportunity to study the late stages of stellar evolution and the interactions between WDs and surrounding material. The 11th data release (DR11) of the Large Sky Area Multi-object Fiber Spectroscopic Telescope (LAMOST)—one of the largest spectroscopic surveys to date—has recently provided spectra for 3092 WDs, many of which have yet to be systematically investigated for IR excess. In this study, we cross-correlated the LAMOST DR11 WD catalog with optical and IR surveys, including the Sloan Digital Sky Survey, Two Micron All Sky Survey, UKIRT Infrared Deep Sky Survey, and Wide-field Infrared Survey Explorer (WISE). We performed spectral energy distribution fitting using the VOSA tool for 1818 WDs and identified 167 IR excess WD candidates. After excluding 23 sources with potential contamination within 6″ and five additional sources identified through WISE contamination and confusion flag analysis, we identified 139 objects with candidate IR excess. These include 30 candidate WD+M dwarf binaries (18 new systems), 19 candidate WD+brown dwarf (BD) binaries (eight new systems), 66 candidate WD+dust disks (38 new systems), and 24 candidate WD+BD or WD+dust disks (19 new systems). Given the limited spatial resolution of WISE, all candidate systems require follow-up IR observations for confirmation, such as high spatial resolution imaging or IR spectroscopy. This will help expand the parameter space of dust disks, allowing us to explore a broader range of possibilities.
{"title":"White Dwarfs with Infrared Excess from LAMOST Data Release 11","authors":"Keyi Wang, Qiong Liu, Siyi Xu and Alberto Rebassa-Mansergas","doi":"10.3847/1538-4357/ae4fb5","DOIUrl":"https://doi.org/10.3847/1538-4357/ae4fb5","url":null,"abstract":"Infrared (IR) excess observed around white dwarfs (WDs) is typically attributed to companions or debris disks. These systems are interesting because they offer a unique opportunity to study the late stages of stellar evolution and the interactions between WDs and surrounding material. The 11th data release (DR11) of the Large Sky Area Multi-object Fiber Spectroscopic Telescope (LAMOST)—one of the largest spectroscopic surveys to date—has recently provided spectra for 3092 WDs, many of which have yet to be systematically investigated for IR excess. In this study, we cross-correlated the LAMOST DR11 WD catalog with optical and IR surveys, including the Sloan Digital Sky Survey, Two Micron All Sky Survey, UKIRT Infrared Deep Sky Survey, and Wide-field Infrared Survey Explorer (WISE). We performed spectral energy distribution fitting using the VOSA tool for 1818 WDs and identified 167 IR excess WD candidates. After excluding 23 sources with potential contamination within 6″ and five additional sources identified through WISE contamination and confusion flag analysis, we identified 139 objects with candidate IR excess. These include 30 candidate WD+M dwarf binaries (18 new systems), 19 candidate WD+brown dwarf (BD) binaries (eight new systems), 66 candidate WD+dust disks (38 new systems), and 24 candidate WD+BD or WD+dust disks (19 new systems). Given the limited spatial resolution of WISE, all candidate systems require follow-up IR observations for confirmation, such as high spatial resolution imaging or IR spectroscopy. This will help expand the parameter space of dust disks, allowing us to explore a broader range of possibilities.","PeriodicalId":501813,"journal":{"name":"The Astrophysical Journal","volume":"20 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2026-04-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"147619629","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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