Pub Date : 2025-02-26DOI: 10.3847/2041-8213/adad53
Benedikt Justen, Shadia Rifai Habbal, Matthias Justen, Oliver Mayer, Adalbert Ding, Klemens Brumann and Herbert Stehr
We report in this Letter on the first use of a kite as an airborne platform for coronal observations during total solar eclipses, to mitigate the detrimental impact of clouds when present. In this first innovative attempt, the scientific payload was chosen to be a single-channel color spectrometer operating in high order over the wavelength range of 400–1000 nm, with light being fed from a coelostat that tracked the Sun optically. The payload was made airborne by a Cody-box-type kite with a wingspan of 6.5 m and launched from Cape Range National Park in North West Australia during the 2023 April 20 total solar eclipse. The kite and payload reached a terminal altitude of 450 m about 30 minutes prior to second contact and remained airborne 1 hr past the 58 s of totality. Although the tracking was not perfect, it nevertheless enabled the acquisition of two coronal spectra. This first successful technology demonstration paves the way for the feasibility of future low-cost kite-borne payloads for astronomical observations not limited to total solar eclipses.
{"title":"Kite-borne Spectroscopic Observations of the Corona During the 2023 April 20 Total Solar Eclipse","authors":"Benedikt Justen, Shadia Rifai Habbal, Matthias Justen, Oliver Mayer, Adalbert Ding, Klemens Brumann and Herbert Stehr","doi":"10.3847/2041-8213/adad53","DOIUrl":"https://doi.org/10.3847/2041-8213/adad53","url":null,"abstract":"We report in this Letter on the first use of a kite as an airborne platform for coronal observations during total solar eclipses, to mitigate the detrimental impact of clouds when present. In this first innovative attempt, the scientific payload was chosen to be a single-channel color spectrometer operating in high order over the wavelength range of 400–1000 nm, with light being fed from a coelostat that tracked the Sun optically. The payload was made airborne by a Cody-box-type kite with a wingspan of 6.5 m and launched from Cape Range National Park in North West Australia during the 2023 April 20 total solar eclipse. The kite and payload reached a terminal altitude of 450 m about 30 minutes prior to second contact and remained airborne 1 hr past the 58 s of totality. Although the tracking was not perfect, it nevertheless enabled the acquisition of two coronal spectra. This first successful technology demonstration paves the way for the feasibility of future low-cost kite-borne payloads for astronomical observations not limited to total solar eclipses.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-02-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143507092","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 : 2025-02-25DOI: 10.3847/2041-8213/adb154
Savvas Raptis, Martin Lindberg, Terry Z. Liu, Drew L. Turner, Ahmad Lalti, Yufei Zhou, Primož Kajdič, Athanasios Kouloumvakos, David G. Sibeck, Laura Vuorinen, Adam Michael, Mykhaylo Shumko, Adnane Osmane, Eva Krämer, Lucile Turc, Tomas Karlsson, Christos Katsavrias, Lynn B. Wilson, Hadi Madanian, Xóchitl Blanco-Cano, Ian J. Cohen and C. Philippe Escoubet
Shock-generated transients, such as hot flow anomalies (HFAs), upstream of planetary bow shocks, play a critical role in electron acceleration. Using multimission data from NASA’s Magnetospheric Multiscale and ESA’s Cluster missions, we demonstrate the transmission of HFAs through Earth’s quasi-parallel bow shock, accelerating electrons to relativistic energies in the process. Energetic electrons initially accelerated upstream are shown to remain broadly confined within the transmitted transient structures downstream, where they get further energized due to the elevated compression levels potentially by betatron acceleration. Additionally, high-speed jets form at the compressive edges of HFAs, exhibiting a significant increase in dynamic pressure and potentially contributing to further localized compression. Our findings emphasize the efficiency of quasi-parallel shocks in driving particle acceleration far beyond the immediate shock transition region, expanding the acceleration region to a larger spatial domain. Finally, this study underscores the importance of a multiscale observational approach in understanding the convoluted processes behind collisionless shock physics and their broader implications.
{"title":"Multimission Observations of Relativistic Electrons and High-speed Jets Linked to Shock-generated Transients","authors":"Savvas Raptis, Martin Lindberg, Terry Z. Liu, Drew L. Turner, Ahmad Lalti, Yufei Zhou, Primož Kajdič, Athanasios Kouloumvakos, David G. Sibeck, Laura Vuorinen, Adam Michael, Mykhaylo Shumko, Adnane Osmane, Eva Krämer, Lucile Turc, Tomas Karlsson, Christos Katsavrias, Lynn B. Wilson, Hadi Madanian, Xóchitl Blanco-Cano, Ian J. Cohen and C. Philippe Escoubet","doi":"10.3847/2041-8213/adb154","DOIUrl":"https://doi.org/10.3847/2041-8213/adb154","url":null,"abstract":"Shock-generated transients, such as hot flow anomalies (HFAs), upstream of planetary bow shocks, play a critical role in electron acceleration. Using multimission data from NASA’s Magnetospheric Multiscale and ESA’s Cluster missions, we demonstrate the transmission of HFAs through Earth’s quasi-parallel bow shock, accelerating electrons to relativistic energies in the process. Energetic electrons initially accelerated upstream are shown to remain broadly confined within the transmitted transient structures downstream, where they get further energized due to the elevated compression levels potentially by betatron acceleration. Additionally, high-speed jets form at the compressive edges of HFAs, exhibiting a significant increase in dynamic pressure and potentially contributing to further localized compression. Our findings emphasize the efficiency of quasi-parallel shocks in driving particle acceleration far beyond the immediate shock transition region, expanding the acceleration region to a larger spatial domain. Finally, this study underscores the importance of a multiscale observational approach in understanding the convoluted processes behind collisionless shock physics and their broader implications.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"17 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-02-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143495176","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 : 2025-02-24DOI: 10.3847/2041-8213/adb42b
Ellen M. Price, Juliette Becker, Zoë L. de Beurs, Leslie A. Rogers and Andrew Vanderburg
HIP 41378 f is a sub-Neptune exoplanet with an anomalously low density. Its long orbital period and deep transit make it an ideal candidate for detecting oblateness photometrically. We present a new cross-platform, GPU-enabled code, greenlantern, suitable for computing transit light curves of oblate planets at arbitrary orientations. We then use the Markov Chain Monte Carlo method to fit K2 data of HIP 41378 f, specifically examining its transit for evidence of oblateness and obliquity. We find that the flattening of HIP 41378 f is f ≤ 0.889 at the 95% confidence level, consistent with a rotation period of Prot ≥ 15.3 hr. In the future, high-precision data from JWST have the potential to tighten such a constraint and can differentiate between spherical and flattened planets.
{"title":"A Long Spin Period for a Sub-Neptune-mass Exoplanet","authors":"Ellen M. Price, Juliette Becker, Zoë L. de Beurs, Leslie A. Rogers and Andrew Vanderburg","doi":"10.3847/2041-8213/adb42b","DOIUrl":"https://doi.org/10.3847/2041-8213/adb42b","url":null,"abstract":"HIP 41378 f is a sub-Neptune exoplanet with an anomalously low density. Its long orbital period and deep transit make it an ideal candidate for detecting oblateness photometrically. We present a new cross-platform, GPU-enabled code, greenlantern, suitable for computing transit light curves of oblate planets at arbitrary orientations. We then use the Markov Chain Monte Carlo method to fit K2 data of HIP 41378 f, specifically examining its transit for evidence of oblateness and obliquity. We find that the flattening of HIP 41378 f is f ≤ 0.889 at the 95% confidence level, consistent with a rotation period of Prot ≥ 15.3 hr. In the future, high-precision data from JWST have the potential to tighten such a constraint and can differentiate between spherical and flattened planets.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"68 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-02-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143485838","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 : 2025-02-24DOI: 10.3847/2041-8213/adb153
Yujie Lian, P. C. C. Freire, Shuo Cao, Mario Cadelano, Cristina Pallanca, Zhichen Pan, Haiyan Zhang, Baoda Li and Lei Qian
PSR B1310+18A is a 33 ms binary pulsar in a 256 day, low eccentricity orbit with a low-mass companion located in NGC 5024 (M53). In this Letter, we present the first phase-coherent timing solution for this pulsar (designated as M53A) derived from a 35 yr timing baseline; this combines the archival Arecibo Observatory data with the recent observations from the Five-hundred-meter Aperture Spherical radio Telescope. We find that the spin period derivative of the pulsar is between 6.1 and 7.5 × 10−19 s s−1, which implies a characteristic age between 0.70 and 0.85 Gyr. The timing solution also includes a precise position and proper motion for the pulsar, enabling the identification of the companion of M53A in Hubble Space Telescope data as a helium white dwarf (He WD) with a mass of and a cooling age of , confirming that the system formed recently in the history of the globular cluster. The system resembles, in its spin and orbital characteristics, similarly wide pulsar–He WD systems in the Galactic disk. We conclude by discussing the origin of slow pulsars in globular clusters, showing that none of the slow pulsars in low-density globular clusters are as young as the systems observed in the densest known globular clusters.
{"title":"Thirty-five Years of Timing of M53A with Arecibo and FAST","authors":"Yujie Lian, P. C. C. Freire, Shuo Cao, Mario Cadelano, Cristina Pallanca, Zhichen Pan, Haiyan Zhang, Baoda Li and Lei Qian","doi":"10.3847/2041-8213/adb153","DOIUrl":"https://doi.org/10.3847/2041-8213/adb153","url":null,"abstract":"PSR B1310+18A is a 33 ms binary pulsar in a 256 day, low eccentricity orbit with a low-mass companion located in NGC 5024 (M53). In this Letter, we present the first phase-coherent timing solution for this pulsar (designated as M53A) derived from a 35 yr timing baseline; this combines the archival Arecibo Observatory data with the recent observations from the Five-hundred-meter Aperture Spherical radio Telescope. We find that the spin period derivative of the pulsar is between 6.1 and 7.5 × 10−19 s s−1, which implies a characteristic age between 0.70 and 0.85 Gyr. The timing solution also includes a precise position and proper motion for the pulsar, enabling the identification of the companion of M53A in Hubble Space Telescope data as a helium white dwarf (He WD) with a mass of and a cooling age of , confirming that the system formed recently in the history of the globular cluster. The system resembles, in its spin and orbital characteristics, similarly wide pulsar–He WD systems in the Galactic disk. We conclude by discussing the origin of slow pulsars in globular clusters, showing that none of the slow pulsars in low-density globular clusters are as young as the systems observed in the densest known globular clusters.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"44 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-02-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143485835","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 : 2025-02-24DOI: 10.3847/2041-8213/adae88
J. Farihi, K. Y. L. Su, C. Melis, S. J. Kenyon, A. Swan, S. Redfield, M. C. Wyatt and J. H. Debes
This Letter reports 12 novel spectroscopic detections of warm circumstellar dust orbiting polluted white dwarfs using the JWST Mid-Infrared Instrument (MIRI). The disks span 2 orders of magnitude in fractional infrared brightness and more than double the number of white dwarf dust spectra available for mineralogical study. Among the highlights are (i) the two most subtle infrared excesses yet detected, (ii) the strongest silicate emission features known for any debris disk orbiting any main-sequence or white dwarf star, (iii) one disk with a thermal continuum but no silicate emission, and (iv) three sources with likely spectral signatures of silica glass. The near ubiquity of solid-state emission requires small dust grains that are optically thin and thus must be replenished on year-to-decade timescales by ongoing collisions. The disk exhibiting a featureless continuum can only be fit by dust temperatures in excess of 2000 K, implying highly refractory material comprised of large particles, or non-silicate mineral species. If confirmed, the glassy silica orbiting three stars could be indicative of high-temperature processes and subsequent rapid cooling, such as occur in high-velocity impacts or vulcanism. These detections have been enabled by the unprecedented sensitivity of MIRI low-resolution spectrometer spectroscopy and highlight the capability and potential for further observations in future cycles.
{"title":"Subtle and Spectacular: Diverse White Dwarf Debris Disks Revealed by JWST","authors":"J. Farihi, K. Y. L. Su, C. Melis, S. J. Kenyon, A. Swan, S. Redfield, M. C. Wyatt and J. H. Debes","doi":"10.3847/2041-8213/adae88","DOIUrl":"https://doi.org/10.3847/2041-8213/adae88","url":null,"abstract":"This Letter reports 12 novel spectroscopic detections of warm circumstellar dust orbiting polluted white dwarfs using the JWST Mid-Infrared Instrument (MIRI). The disks span 2 orders of magnitude in fractional infrared brightness and more than double the number of white dwarf dust spectra available for mineralogical study. Among the highlights are (i) the two most subtle infrared excesses yet detected, (ii) the strongest silicate emission features known for any debris disk orbiting any main-sequence or white dwarf star, (iii) one disk with a thermal continuum but no silicate emission, and (iv) three sources with likely spectral signatures of silica glass. The near ubiquity of solid-state emission requires small dust grains that are optically thin and thus must be replenished on year-to-decade timescales by ongoing collisions. The disk exhibiting a featureless continuum can only be fit by dust temperatures in excess of 2000 K, implying highly refractory material comprised of large particles, or non-silicate mineral species. If confirmed, the glassy silica orbiting three stars could be indicative of high-temperature processes and subsequent rapid cooling, such as occur in high-velocity impacts or vulcanism. These detections have been enabled by the unprecedented sensitivity of MIRI low-resolution spectrometer spectroscopy and highlight the capability and potential for further observations in future cycles.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"49 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-02-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143485836","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 : 2025-02-24DOI: 10.3847/2041-8213/adb426
Wei-Jian Guo, Zhiwei Pan, Małgorzata Siudek, Jessica Nicole Aguilar, Steven Ahlen, Davide Bianchi, David Brooks, Todd Claybaugh, Kyle Dawson, Axel de la Macorra, Peter Doel, Kevin Fanning, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Robert Kehoe, Theodore Kisner, Andrew Lambert, Martin Landriau, Laurent Le Guillou, Marc Manera, Aaron Meisner, John Moustakas, Andrea Muñoz-Gutiérrez, Adam Myers, Jundan Nie, Nathalie Palanque-Delabrouille, Claire Poppett, Francisco Prada, Mehdi Rezaie, Graziano Rossi, Eusebio Sanchez, Michael Schubnell, Hee-Jong Seo, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Zhimin Zhou and Hu Zou
We present two cases of Lyα changing-look (CL) quasars (J1306 and J1512) along with two additional candidates (J1511 and J1602), all discovered serendipitously at z > 2 through the Dark Energy Spectroscopic Instrument and the Sloan Digital Sky Survey. It is the first time to capture CL events in Lyα at high redshift, which is crucial for understanding the underlying mechanisms driving the CL phenomenon and the evolution of high-redshift quasars and galaxies. We find that the accretion rate in the dim state for these CL objects corresponds to a relatively low value ( ), which suggests that the inner region of the accretion disk might be in transition between the advection dominated accretion flow ( ) and the canonical accretion disk (optically thick, geometrically thin). However, unlike in C iv CL quasars in which broad Lyα remained, the broad C iv may still persist after a CL event occurs in Lyα, making the physical origin of the CL and ionization mechanism event more puzzling and interesting.
{"title":"The First Identification of Lyα Changing-look Quasars at High Redshift in DESI","authors":"Wei-Jian Guo, Zhiwei Pan, Małgorzata Siudek, Jessica Nicole Aguilar, Steven Ahlen, Davide Bianchi, David Brooks, Todd Claybaugh, Kyle Dawson, Axel de la Macorra, Peter Doel, Kevin Fanning, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Klaus Honscheid, Robert Kehoe, Theodore Kisner, Andrew Lambert, Martin Landriau, Laurent Le Guillou, Marc Manera, Aaron Meisner, John Moustakas, Andrea Muñoz-Gutiérrez, Adam Myers, Jundan Nie, Nathalie Palanque-Delabrouille, Claire Poppett, Francisco Prada, Mehdi Rezaie, Graziano Rossi, Eusebio Sanchez, Michael Schubnell, Hee-Jong Seo, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Zhimin Zhou and Hu Zou","doi":"10.3847/2041-8213/adb426","DOIUrl":"https://doi.org/10.3847/2041-8213/adb426","url":null,"abstract":"We present two cases of Lyα changing-look (CL) quasars (J1306 and J1512) along with two additional candidates (J1511 and J1602), all discovered serendipitously at z > 2 through the Dark Energy Spectroscopic Instrument and the Sloan Digital Sky Survey. It is the first time to capture CL events in Lyα at high redshift, which is crucial for understanding the underlying mechanisms driving the CL phenomenon and the evolution of high-redshift quasars and galaxies. We find that the accretion rate in the dim state for these CL objects corresponds to a relatively low value ( ), which suggests that the inner region of the accretion disk might be in transition between the advection dominated accretion flow ( ) and the canonical accretion disk (optically thick, geometrically thin). However, unlike in C iv CL quasars in which broad Lyα remained, the broad C iv may still persist after a CL event occurs in Lyα, making the physical origin of the CL and ionization mechanism event more puzzling and interesting.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"31 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-02-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143485889","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}
Using spatially resolved spectroscopic data from the Mapping Nearby Galaxies at Apache Point Observatory sample, we investigate the parameters influencing the radial gradients of gas-phase metallicity ( ) to determine whether disk formation is primarily driven by coplanar gas inflow or by the independent evolution of distinct regions within the disk. Our results show that strongly correlates with local gas-phase metallicity at a given stellar mass, with steeper gradients observed in metal-poorer disks. This trend supports the coplanar gas inflow scenario, wherein the gas is progressively enriched by in situ star formation as it flows inward. In contrast, the radial gradient of stellar mass surface density shows very weak correlations with , which is inconsistent with the independent evolution mode, where gas inflow, star formation, and metal enrichment occur independently within each annulus of the disk. Furthermore, we find that is also closely correlated with an indicator of local gas turbulence , highlighting the competing roles of turbulence and coplanar inflow in shaping metallicity gradients. Our results provide indirect observational evidence supporting coplanar gas inflow as the driving mechanism for disk evolution.
{"title":"Dominant Role of Coplanar Inflows in Driving Disk Evolution Revealed by Gas-phase Metallicity Gradients","authors":"Cheqiu Lyu, Enci Wang, Hongxin Zhang, Yingjie Peng, Xin Wang, Haixin Li, Chengyu Ma, Haoran Yu, Zeyu Chen, Cheng Jia and Xu Kong","doi":"10.3847/2041-8213/adb4ed","DOIUrl":"https://doi.org/10.3847/2041-8213/adb4ed","url":null,"abstract":"Using spatially resolved spectroscopic data from the Mapping Nearby Galaxies at Apache Point Observatory sample, we investigate the parameters influencing the radial gradients of gas-phase metallicity ( ) to determine whether disk formation is primarily driven by coplanar gas inflow or by the independent evolution of distinct regions within the disk. Our results show that strongly correlates with local gas-phase metallicity at a given stellar mass, with steeper gradients observed in metal-poorer disks. This trend supports the coplanar gas inflow scenario, wherein the gas is progressively enriched by in situ star formation as it flows inward. In contrast, the radial gradient of stellar mass surface density shows very weak correlations with , which is inconsistent with the independent evolution mode, where gas inflow, star formation, and metal enrichment occur independently within each annulus of the disk. Furthermore, we find that is also closely correlated with an indicator of local gas turbulence , highlighting the competing roles of turbulence and coplanar inflow in shaping metallicity gradients. Our results provide indirect observational evidence supporting coplanar gas inflow as the driving mechanism for disk evolution.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"22 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-02-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143485839","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 : 2025-02-24DOI: 10.3847/2041-8213/adb1d9
J. D. R. Pierel, D. A. Coulter, M. R. Siebert, H. B. Akins, M. Engesser, O. D. Fox, M. Franco, A. Rest, A. Agrawal, Y. Ajay, N. Allen, C. M. Casey, C. DeCoursey, N. E. Drakos, E. Egami, A. L. Faisst, S. Gezari, G. Gozaliasl, O. Ilbert, D. O. Jones, M. Karmen, J. S. Kartaltepe, A. M. Koekemoer, Z. G. Lane, R. L. Larson, T. Li, D. Liu, T. J. Moriya, H. J. McCracken, L. Paquereau, R. M. Quimby, R. M. Rich, J. Rhodes, B. E. Robertson, D. B. Sanders, M. Shahbandeh, M. Shuntov, J. D. Silverman, L. G. Strolger, S. Toft and Y. Zenati
The James Webb Space Telescope (JWST) is opening new frontiers of transient discovery and follow-up at high redshift. Here we present the discovery of a spectroscopically confirmed Type Ia supernova (SN Ia; SN 2023aeax) at z = 2.15 with JWST, including a NIRCam multiband light curve. SN 2023aeax lands at the edge of traditional low-z cosmology cuts because of its blue color (peak rest-frame B − V ∼ −0.3) but with a normal decline rate (Δm15(B) ∼ 1.25), and applying a fiducial standardization with the BayeSN model we find the SN 2023aeax luminosity distance is in ∼0.1σ agreement with ΛCDM. SN 2023aeax is only the second spectroscopically confirmed SN Ia in the dark matter–dominated Universe at z > 2 (the other is SN 2023adsy), giving it rare leverage to constrain any potential evolution in SN Ia standardized luminosities. Similar to SN 2023adsy (B − V ∼ 0.8), SN 2023aeax has a fairly extreme (but opposite) color, which may be due to the small sample size or a secondary factor, such as host galaxy properties. Nevertheless, the SN 2023aeax spectrum is well represented by normal low-z SN Ia spectra, and we find no definitive evolution in SN Ia standardization with redshift. Still, the first two spectroscopically confirmed z > 2 SNe Ia have peculiar colors and combine for a ∼1σ distance slope relative to ΛCDM, though in agreement with recent SN Ia cosmological measurements.
{"title":"Testing for Intrinsic Type Ia Supernova Luminosity Evolution at z > 2 with JWST","authors":"J. D. R. Pierel, D. A. Coulter, M. R. Siebert, H. B. Akins, M. Engesser, O. D. Fox, M. Franco, A. Rest, A. Agrawal, Y. Ajay, N. Allen, C. M. Casey, C. DeCoursey, N. E. Drakos, E. Egami, A. L. Faisst, S. Gezari, G. Gozaliasl, O. Ilbert, D. O. Jones, M. Karmen, J. S. Kartaltepe, A. M. Koekemoer, Z. G. Lane, R. L. Larson, T. Li, D. Liu, T. J. Moriya, H. J. McCracken, L. Paquereau, R. M. Quimby, R. M. Rich, J. Rhodes, B. E. Robertson, D. B. Sanders, M. Shahbandeh, M. Shuntov, J. D. Silverman, L. G. Strolger, S. Toft and Y. Zenati","doi":"10.3847/2041-8213/adb1d9","DOIUrl":"https://doi.org/10.3847/2041-8213/adb1d9","url":null,"abstract":"The James Webb Space Telescope (JWST) is opening new frontiers of transient discovery and follow-up at high redshift. Here we present the discovery of a spectroscopically confirmed Type Ia supernova (SN Ia; SN 2023aeax) at z = 2.15 with JWST, including a NIRCam multiband light curve. SN 2023aeax lands at the edge of traditional low-z cosmology cuts because of its blue color (peak rest-frame B − V ∼ −0.3) but with a normal decline rate (Δm15(B) ∼ 1.25), and applying a fiducial standardization with the BayeSN model we find the SN 2023aeax luminosity distance is in ∼0.1σ agreement with ΛCDM. SN 2023aeax is only the second spectroscopically confirmed SN Ia in the dark matter–dominated Universe at z > 2 (the other is SN 2023adsy), giving it rare leverage to constrain any potential evolution in SN Ia standardized luminosities. Similar to SN 2023adsy (B − V ∼ 0.8), SN 2023aeax has a fairly extreme (but opposite) color, which may be due to the small sample size or a secondary factor, such as host galaxy properties. Nevertheless, the SN 2023aeax spectrum is well represented by normal low-z SN Ia spectra, and we find no definitive evolution in SN Ia standardization with redshift. Still, the first two spectroscopically confirmed z > 2 SNe Ia have peculiar colors and combine for a ∼1σ distance slope relative to ΛCDM, though in agreement with recent SN Ia cosmological measurements.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"27 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-02-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143477658","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 : 2025-02-21DOI: 10.3847/2041-8213/adb0c8
Raimundo Lopes de Oliveira, Amanda S. de Araújo, Angela C. Krabbe, Claudia L. Mendes de Oliveira, Koji Mukai, Luis A. Gutiérrez-Soto, Antonio Kanaan, Romualdo Eleutério, Marcelo Borges Fernandes, Fredi Quispe-Huaynasi, William Schoenell and Tiago Ribeiro
Multiband photometric surveys provide a straightforward way to discover and classify astrophysical objects systematically, enabling the study of a large number of targets at relatively low cost. Here we introduce an alternative approach to select accreting white dwarf (AWD) candidates following their spectral energy distribution, entirely supported by the twelve photometric bands of the Southern Photometric Local Universe Survey (S-PLUS). The method was validated with optical spectroscopic follow-up with the Gemini South telescope, which unambiguously established ten systems as cataclysmic variables (CVs), alongside Swift X-ray observations of four of them. Among the ten CVs presented here are those that may be low-luminosity intermediate polars or WZ Sge-type dwarf novae with rare outbursts, two subclasses that can be easily missed in time-domain and X-ray surveys, the two methods currently dominating the discovery of new CVs. Our approach based on S-PLUS provides an important complementary tool to uncover the total population of CVs and the complete set of its subclasses, which is an important step toward a full understanding of close binary evolution, including the origin of magnetic fields in white dwarfs and the physics of accretion. Finally, we highlight the potential of S-PLUS beyond AWDs, serving other surveys in the characterization of their sources.
{"title":"The S-PLUS 12-band Photometry as a Powerful Tool for Discovery and Classification: Ten Cataclysmic Variables in a Proof-of-concept Study","authors":"Raimundo Lopes de Oliveira, Amanda S. de Araújo, Angela C. Krabbe, Claudia L. Mendes de Oliveira, Koji Mukai, Luis A. Gutiérrez-Soto, Antonio Kanaan, Romualdo Eleutério, Marcelo Borges Fernandes, Fredi Quispe-Huaynasi, William Schoenell and Tiago Ribeiro","doi":"10.3847/2041-8213/adb0c8","DOIUrl":"https://doi.org/10.3847/2041-8213/adb0c8","url":null,"abstract":"Multiband photometric surveys provide a straightforward way to discover and classify astrophysical objects systematically, enabling the study of a large number of targets at relatively low cost. Here we introduce an alternative approach to select accreting white dwarf (AWD) candidates following their spectral energy distribution, entirely supported by the twelve photometric bands of the Southern Photometric Local Universe Survey (S-PLUS). The method was validated with optical spectroscopic follow-up with the Gemini South telescope, which unambiguously established ten systems as cataclysmic variables (CVs), alongside Swift X-ray observations of four of them. Among the ten CVs presented here are those that may be low-luminosity intermediate polars or WZ Sge-type dwarf novae with rare outbursts, two subclasses that can be easily missed in time-domain and X-ray surveys, the two methods currently dominating the discovery of new CVs. Our approach based on S-PLUS provides an important complementary tool to uncover the total population of CVs and the complete set of its subclasses, which is an important step toward a full understanding of close binary evolution, including the origin of magnetic fields in white dwarfs and the physics of accretion. Finally, we highlight the potential of S-PLUS beyond AWDs, serving other surveys in the characterization of their sources.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-02-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143485900","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}
Mare basalts from lunar farside are pivotal for unraveling lunar nearside-farside dichotomies and global thermal history. The Chang’e-6 (CE-6) mission conducted the first sampling from a young basaltic unit within the Apollo basin on the lunar farside. Here, we performed comprehensive petrological and geochemical analyses on the CE-6 basalt clasts. The CE-6 basalt is a low-titanium basalt (about 5 wt% TiO2) depleted in KREEP components. The absence of olivine, particularly magnesium-rich olivine, suggests that the basaltic magma underwent extensive fractional crystallization. Thermodynamic modeling supports that there may be 10%–20% late-stage cumulates of magma ocean (clinopyroxene and ilmenite) present in the source region of CE-6 basalt. The magma derived from the partial melting of such lunar mantle may undergo fractional crystallization dominated by olivine and clinopyroxene within a shallow magma cg1hamber, followed by eruption. Modeling of the REE pattern further indicates that 3%–7% batch melting of a depleted lunar mantle source, combined with 21%–59% fractional crystallization, achieves the observed REE abundances of CE-6 basalt. The genesis of CE-6 basalt could be attributed to the synergistic influence of a readily fusible mantle source, resulting from the incorporation of late-stage cumulates, and the crust-mantle deformation induced by large impacts. This could serve as a paradigm for the formation of other young basalts on the Moon.
{"title":"Petrogenesis of Chang’e-6 Basalts and Implication for the Young Volcanism on the Lunar Farside","authors":"Chengxiang Yin, Jian Chen, Xiaohui Fu, Haijun Cao, Xuejin Lu, Yiheng Liu, Jin Li, Siyue Chi, Xiaojia Zeng and Zongcheng Ling","doi":"10.3847/2041-8213/adaf20","DOIUrl":"https://doi.org/10.3847/2041-8213/adaf20","url":null,"abstract":"Mare basalts from lunar farside are pivotal for unraveling lunar nearside-farside dichotomies and global thermal history. The Chang’e-6 (CE-6) mission conducted the first sampling from a young basaltic unit within the Apollo basin on the lunar farside. Here, we performed comprehensive petrological and geochemical analyses on the CE-6 basalt clasts. The CE-6 basalt is a low-titanium basalt (about 5 wt% TiO2) depleted in KREEP components. The absence of olivine, particularly magnesium-rich olivine, suggests that the basaltic magma underwent extensive fractional crystallization. Thermodynamic modeling supports that there may be 10%–20% late-stage cumulates of magma ocean (clinopyroxene and ilmenite) present in the source region of CE-6 basalt. The magma derived from the partial melting of such lunar mantle may undergo fractional crystallization dominated by olivine and clinopyroxene within a shallow magma cg1hamber, followed by eruption. Modeling of the REE pattern further indicates that 3%–7% batch melting of a depleted lunar mantle source, combined with 21%–59% fractional crystallization, achieves the observed REE abundances of CE-6 basalt. The genesis of CE-6 basalt could be attributed to the synergistic influence of a readily fusible mantle source, resulting from the incorporation of late-stage cumulates, and the crust-mantle deformation induced by large impacts. This could serve as a paradigm for the formation of other young basalts on the Moon.","PeriodicalId":501814,"journal":{"name":"The Astrophysical Journal Letters","volume":"50 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2025-02-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143477657","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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