Pub Date : 2023-10-30DOI: 10.3847/2041-8213/acff62
Petr Heinzel, Sonja Jejčič, Jiří Štěpán, Roberto Susino, Vincenzo Andretta, Giuliana Russano, Silvano Fineschi, Marco Romoli, Alessandro Bemporad, Arkadiusz Berlicki, Aleksandr Burtovoi, Vania Da Deppo, Yara De Leo, Catia Grimani, Giovanna Jerse, Federico Landini, Giampiero Naletto, Gianalfredo Nicolini, Maurizio Pancrazzi, Tanausú del Pino Alemán, Clementina Sasso, Daniele Spadaro, Marco Stangalini, Daniele Telloni, Luca Teriaca, Michela Uslenghi, Andrés Vicente Arévalo
Abstract Metis on board Solar Orbiter is the space coronagraph developed by an Italian–German–Czech consortium. It is capable of observing solar corona and various coronal structures in the visible-light (VL) and UV (hydrogen Ly α ) channels simultaneously for the first time. Here we present observations of a large eruptive prominence on 2021 April 25–26, in the VL, taken during the mission cruise phase, and demonstrate that apart from the broadband continuum emission, which is due to the Thomson scattering on prominence electrons, we detect a significant radiation in the neutral-helium D 3 line (587.6 nm), which lies within the Metis VL passband. We show how the prominence looks like in Stokes I , Q , and U . We consider two extreme cases of the prominence magnetic field, and we separate the Stokes I and Q signals pertinent to Thomson scattering and to the D 3 line. The degree of linear polarization of the D 3 line (both Q and U ) indicates the presence of the prominence magnetic field; hence Metis can serve as a magnetograph for eruptive prominences located high in the corona.
太阳轨道器上的梅蒂斯是由意大利、德国和捷克联合开发的空间日冕仪。首次能够在可见光(VL)和紫外(氢Ly α)通道同时观测日冕和各种日冕结构。在这里，我们展示了2021年4月25日至26日在VL的一个大喷发日珥的观测结果，这是在任务巡航阶段拍摄的，并证明除了宽带连续发射，这是由于汤姆逊散射对日珥电子的影响，我们在梅蒂斯VL通带内的中性氦D 3线(587.6 nm)中检测到显著的辐射。我们展示了在Stokes I, Q和U中突出的样子。我们考虑了日珥磁场的两种极端情况，并分离了与汤姆逊散射和d3线有关的斯托克斯I和Q信号。三维线的线极化度(Q和U)表明日珥磁场的存在;因此，梅蒂斯可以作为位于日冕高处的喷发日珥的磁力计。
{"title":"First Metis Detection of the Helium D<sub>3</sub> Line Polarization in a Large Eruptive Prominence","authors":"Petr Heinzel, Sonja Jejčič, Jiří Štěpán, Roberto Susino, Vincenzo Andretta, Giuliana Russano, Silvano Fineschi, Marco Romoli, Alessandro Bemporad, Arkadiusz Berlicki, Aleksandr Burtovoi, Vania Da Deppo, Yara De Leo, Catia Grimani, Giovanna Jerse, Federico Landini, Giampiero Naletto, Gianalfredo Nicolini, Maurizio Pancrazzi, Tanausú del Pino Alemán, Clementina Sasso, Daniele Spadaro, Marco Stangalini, Daniele Telloni, Luca Teriaca, Michela Uslenghi, Andrés Vicente Arévalo","doi":"10.3847/2041-8213/acff62","DOIUrl":"https://doi.org/10.3847/2041-8213/acff62","url":null,"abstract":"Abstract Metis on board Solar Orbiter is the space coronagraph developed by an Italian–German–Czech consortium. It is capable of observing solar corona and various coronal structures in the visible-light (VL) and UV (hydrogen Ly α ) channels simultaneously for the first time. Here we present observations of a large eruptive prominence on 2021 April 25–26, in the VL, taken during the mission cruise phase, and demonstrate that apart from the broadband continuum emission, which is due to the Thomson scattering on prominence electrons, we detect a significant radiation in the neutral-helium D 3 line (587.6 nm), which lies within the Metis VL passband. We show how the prominence looks like in Stokes I , Q , and U . We consider two extreme cases of the prominence magnetic field, and we separate the Stokes I and Q signals pertinent to Thomson scattering and to the D 3 line. The degree of linear polarization of the D 3 line (both Q and U ) indicates the presence of the prominence magnetic field; hence Metis can serve as a magnetograph for eruptive prominences located high in the corona.","PeriodicalId":55567,"journal":{"name":"Astrophysical Journal Letters","volume":"197 ","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136069469","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-10-30DOI: 10.3847/2041-8213/acfd2e
Alok C. Gupta, Pankaj Kushwaha, Mauri J. Valtonen, Sergey S. Savchenko, Svetlana G. Jorstad, Ryo Imazawa, Paul J. Wiita, Minfeng Gu, Alan P. Marscher, Zhongli Zhang, Rumen Bachev, G. A. Borman, Haritma Gaur, T. S. Grishina, V. A. Hagen-Thorn, E. N. Kopatskaya, V. M. Larionov, E. G. Larionova, L. V. Larionova, D. A. Morozova, T. Nakaoka, A. Strigachev, Yulia V. Troitskaya, I. S. Troitsky, M. Uemura, A. A. Vasilyev, Z. R. Weaver, A. V. Zhovtan
Abstract We study the optical flux and polarization variability of the binary black hole blazar OJ 287 using quasi-simultaneous observations from 2015 to 2023 carried out using telescopes in the USA, Japan, Russia, Crimea, and Bulgaria. This is one of the most extensive quasi-simultaneous optical flux and polarization variability studies of OJ 287. OJ 287 showed large amplitude, ∼3.0 mag flux variability, large changes of ∼37% in degree of polarization, and a large swing of ∼215° in the angle of the electric vector of polarization. During the period of observation, several flares in flux were detected. Those flares are correlated with a rapid increase in the degree of polarization and swings in electric vector of polarization angle. A peculiar behavior of anticorrelation between flux and polarization degree, accompanied by a nearly constant polarization angle, was detected from JD 2,458,156 to JD 2,458,292. We briefly discuss some explanations for the flux and polarization variations observed in OJ 287.
{"title":"Quasi-simultaneous Optical Flux and Polarization Variability of the Binary Super Massive Black Hole Blazar OJ 287 from 2015 to 2023: Detection of an Anticorrelation in Flux and Polarization Variability","authors":"Alok C. Gupta, Pankaj Kushwaha, Mauri J. Valtonen, Sergey S. Savchenko, Svetlana G. Jorstad, Ryo Imazawa, Paul J. Wiita, Minfeng Gu, Alan P. Marscher, Zhongli Zhang, Rumen Bachev, G. A. Borman, Haritma Gaur, T. S. Grishina, V. A. Hagen-Thorn, E. N. Kopatskaya, V. M. Larionov, E. G. Larionova, L. V. Larionova, D. A. Morozova, T. Nakaoka, A. Strigachev, Yulia V. Troitskaya, I. S. Troitsky, M. Uemura, A. A. Vasilyev, Z. R. Weaver, A. V. Zhovtan","doi":"10.3847/2041-8213/acfd2e","DOIUrl":"https://doi.org/10.3847/2041-8213/acfd2e","url":null,"abstract":"Abstract We study the optical flux and polarization variability of the binary black hole blazar OJ 287 using quasi-simultaneous observations from 2015 to 2023 carried out using telescopes in the USA, Japan, Russia, Crimea, and Bulgaria. This is one of the most extensive quasi-simultaneous optical flux and polarization variability studies of OJ 287. OJ 287 showed large amplitude, ∼3.0 mag flux variability, large changes of ∼37% in degree of polarization, and a large swing of ∼215° in the angle of the electric vector of polarization. During the period of observation, several flares in flux were detected. Those flares are correlated with a rapid increase in the degree of polarization and swings in electric vector of polarization angle. A peculiar behavior of anticorrelation between flux and polarization degree, accompanied by a nearly constant polarization angle, was detected from JD 2,458,156 to JD 2,458,292. We briefly discuss some explanations for the flux and polarization variations observed in OJ 287.","PeriodicalId":55567,"journal":{"name":"Astrophysical Journal Letters","volume":"201 ","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136069592","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-10-26DOI: 10.3847/2041-8213/ad012f
Fang, Ke, Murase, Kohta
High-energy neutrino and γ-ray emission has been observed from the Galactic plane, which may come from individual sources and/or diffuse cosmic rays. We evaluate the contribution of these two components through the multimessenger connection between neutrinos and γ-rays in hadronic interactions. We derive maximum fluxes of neutrino emission from the Galactic plane using γ-ray catalogs, including 4FGL, HGPS, 3HWC, and 1LHAASO, and measurements of the Galactic diffuse emission by Tibet ASγ and LHAASO. We find that the IceCube Galactic neutrino flux is larger than the contribution from all resolved sources when excluding promising leptonic sources such as pulsars, pulsar wind nebulae, and TeV halos. Our result indicates that the Galactic neutrino emission is likely dominated by the diffuse emission by the cosmic-ray sea and unresolved hadronic γ-ray sources. In addition, the IceCube flux is comparable to the sum of the flux of nonpulsar sources and the LHAASO diffuse emission especially above ∼30 TeV. This implies that the LHAASO diffuse emission may dominantly originate from hadronic interactions, either as the truly diffuse emission or unresolved hadronic emitters. Future observations of neutrino telescopes and air-shower γ-ray experiments in the Southern hemisphere are needed to accurately disentangle the source and diffuse emission of the Milky Way.
{"title":"Decomposing the Origin of TeV–PeV Emission from the Galactic Plane: Implications of Multimessenger Observations","authors":"Fang, Ke, Murase, Kohta","doi":"10.3847/2041-8213/ad012f","DOIUrl":"https://doi.org/10.3847/2041-8213/ad012f","url":null,"abstract":"High-energy neutrino and γ-ray emission has been observed from the Galactic plane, which may come from individual sources and/or diffuse cosmic rays. We evaluate the contribution of these two components through the multimessenger connection between neutrinos and γ-rays in hadronic interactions. We derive maximum fluxes of neutrino emission from the Galactic plane using γ-ray catalogs, including 4FGL, HGPS, 3HWC, and 1LHAASO, and measurements of the Galactic diffuse emission by Tibet ASγ and LHAASO. We find that the IceCube Galactic neutrino flux is larger than the contribution from all resolved sources when excluding promising leptonic sources such as pulsars, pulsar wind nebulae, and TeV halos. Our result indicates that the Galactic neutrino emission is likely dominated by the diffuse emission by the cosmic-ray sea and unresolved hadronic γ-ray sources. In addition, the IceCube flux is comparable to the sum of the flux of nonpulsar sources and the LHAASO diffuse emission especially above ∼30 TeV. This implies that the LHAASO diffuse emission may dominantly originate from hadronic interactions, either as the truly diffuse emission or unresolved hadronic emitters. Future observations of neutrino telescopes and air-shower γ-ray experiments in the Southern hemisphere are needed to accurately disentangle the source and diffuse emission of the Milky Way.","PeriodicalId":55567,"journal":{"name":"Astrophysical Journal Letters","volume":"23 2","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136376873","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-10-26DOI: 10.3847/2041-8213/ad037a
Vasily Kokorev, Seiji Fujimoto, Ivo Labbe, Jenny E. Greene, Rachel Bezanson, Pratika Dayal, Erica J. Nelson, Hakim Atek, Gabriel Brammer, Karina I. Caputi, Iryna Chemerynska, Sam E. Cutler, Robert Feldmann, Yoshinobu Fudamoto, Lukas J. Furtak, Andy D. Goulding, Anna de Graaff, Joel Leja, Danilo Marchesini, Tim B. Miller, Themiya Nanayakkara, Pascal A. Oesch, Richard Pan, Sedona H. Price, David J. Setton, Renske Smit, Mauro Stefanon, Bingjie 冰洁 Wang 王, John R. Weaver, Katherine E. Whitaker, Christina C. Williams, Adi Zitrin
Abstract Deep observations with the James Webb Space Telescope (JWST) have revealed an emerging population of red pointlike sources that could provide a link between the postulated supermassive black hole seeds and observed quasars. In this work, we present a JWST/NIRSpec spectrum from the JWST Cycle 1 UNCOVER Treasury survey of a massive accreting black hole at z = 8.50 displaying a clear broad-line component as inferred from the H β line with FWHM = 3439 ± 413 km s −1 , typical of the broad-line region of an active galactic nucleus (AGN). The AGN nature of this object is further supported by high ionization, as inferred from emission lines, and a point-source morphology. We compute a black hole mass of log10(MBH/M⊙)=8.17±0.42 and a bolometric luminosity of L bol ∼ 6.6 × 10 45 erg s −1 . These values imply that our object is accreting at ∼40% of the Eddington limit. Detailed modeling of the spectral energy distribution in the optical and near-infrared, together with constraints from ALMA, indicate an upper limit on the stellar mass of log10(M*/M⊙)<8.7 , which would lead to an unprecedented ratio of black hole to host mass of at least ∼30%. This is orders of magnitude higher compared to the local QSOs but consistent with recent AGN studies at high redshift with JWST. This finding suggests that a nonnegligible fraction of supermassive black holes either started out from massive seeds and/or grew at a super-Eddington rate at high redshift. Given the predicted number densities of high- z faint AGN, future NIRSpec observations of larger samples will allow us to further investigate galaxy–black hole coevolution in the early Universe.
{"title":"UNCOVER: A NIRSpec Identification of a Broad-line AGN at z = 8.50","authors":"Vasily Kokorev, Seiji Fujimoto, Ivo Labbe, Jenny E. Greene, Rachel Bezanson, Pratika Dayal, Erica J. Nelson, Hakim Atek, Gabriel Brammer, Karina I. Caputi, Iryna Chemerynska, Sam E. Cutler, Robert Feldmann, Yoshinobu Fudamoto, Lukas J. Furtak, Andy D. Goulding, Anna de Graaff, Joel Leja, Danilo Marchesini, Tim B. Miller, Themiya Nanayakkara, Pascal A. Oesch, Richard Pan, Sedona H. Price, David J. Setton, Renske Smit, Mauro Stefanon, Bingjie 冰洁 Wang 王, John R. Weaver, Katherine E. Whitaker, Christina C. Williams, Adi Zitrin","doi":"10.3847/2041-8213/ad037a","DOIUrl":"https://doi.org/10.3847/2041-8213/ad037a","url":null,"abstract":"Abstract Deep observations with the James Webb Space Telescope (JWST) have revealed an emerging population of red pointlike sources that could provide a link between the postulated supermassive black hole seeds and observed quasars. In this work, we present a JWST/NIRSpec spectrum from the JWST Cycle 1 UNCOVER Treasury survey of a massive accreting black hole at z = 8.50 displaying a clear broad-line component as inferred from the H β line with FWHM = 3439 ± 413 km s −1 , typical of the broad-line region of an active galactic nucleus (AGN). The AGN nature of this object is further supported by high ionization, as inferred from emission lines, and a point-source morphology. We compute a black hole mass of <?CDATA ${mathrm{log}}_{10}({M}_{mathrm{BH}}/{M}_{odot })=8.17pm 0.42$?> <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" overflow=\"scroll\"> <mml:msub> <mml:mrow> <mml:mi>log</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> </mml:msub> <mml:mo stretchy=\"false\">(</mml:mo> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>BH</mml:mi> </mml:mrow> </mml:msub> <mml:mrow> <mml:mo stretchy=\"true\">/</mml:mo> </mml:mrow> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⊙</mml:mo> </mml:mrow> </mml:msub> <mml:mo stretchy=\"false\">)</mml:mo> <mml:mo>=</mml:mo> <mml:mn>8.17</mml:mn> <mml:mo>±</mml:mo> <mml:mn>0.42</mml:mn> </mml:math> and a bolometric luminosity of L bol ∼ 6.6 × 10 45 erg s −1 . These values imply that our object is accreting at ∼40% of the Eddington limit. Detailed modeling of the spectral energy distribution in the optical and near-infrared, together with constraints from ALMA, indicate an upper limit on the stellar mass of <?CDATA ${mathrm{log}}_{10}({M}_{* }/{M}_{odot })lt 8.7$?> <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" overflow=\"scroll\"> <mml:msub> <mml:mrow> <mml:mi>log</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> </mml:msub> <mml:mo stretchy=\"false\">(</mml:mo> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>*</mml:mo> </mml:mrow> </mml:msub> <mml:mrow> <mml:mo stretchy=\"true\">/</mml:mo> </mml:mrow> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⊙</mml:mo> </mml:mrow> </mml:msub> <mml:mo stretchy=\"false\">)</mml:mo> <mml:mo><</mml:mo> <mml:mn>8.7</mml:mn> </mml:math> , which would lead to an unprecedented ratio of black hole to host mass of at least ∼30%. This is orders of magnitude higher compared to the local QSOs but consistent with recent AGN studies at high redshift with JWST. This finding suggests that a nonnegligible fraction of supermassive black holes either started out from massive seeds and/or grew at a super-Eddington rate at high redshift. Given the predicted number densities of high- z faint AGN, future NIRSpec observations of larger samples will allow us to further investigate galaxy–black hole coevolution in the early Universe.","PeriodicalId":55567,"journal":{"name":"Astrophysical Journal Letters","volume":"1 2","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136376102","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-10-25DOI: 10.3847/2041-8213/acffc8
Wonki Lee, John ZuHone, M. James Jee, Kim HyeongHan, Ruta Kale, Eunmo Ahn
Abstract We report a discovery of a large-scale bent radio jet in the merging galaxy cluster A514 ( z = 0.071). The radio emission originates from the two radio lobes of the active galactic nucleus (AGN) located near the center of the southern subcluster and extends toward the southern outskirts with multiple bends. Its peculiar morphology is characterized by a 400 kpc “bridge,” a 300 kpc “arc,” and a 400 kpc “tail,” which together contribute to its largest linear size of ∼0.7 Mpc. We find that both the flux and spectral features of the emission change with the distance from the AGN. Also, the “bridge” presents a 60% polarized radio emission, which coincided with an X-ray cold front. Based on our multiwavelength observations, we propose that A514 presents a clear case for the redistribution of an old AGN plasma due to merger-driven gas motions. We support our interpretation with idealized cluster merger simulations employing a passive tracer field to represent cosmic-ray electrons and find that merger-driven motions can efficiently create a cloud of these particles in the cluster outskirts, which later can be reaccelerated by the cluster merger shock and produce radio relics.
我们报道了在合并星系团A514 (z = 0.071)中发现的大规模弯曲射电射流。射电辐射来自位于南亚星团中心附近的活动星系核(AGN)的两个射电叶，并以多个弯曲向南郊延伸。其独特的形态具有400kpc的“桥”，300kpc的“弧”和400kpc的“尾”，它们共同构成了其最大的线性尺寸约0.7 Mpc。我们发现，辐射的通量和光谱特征都随着离AGN的距离而变化。此外，“桥”呈现出60%的极化射电发射，与x射线冷锋相吻合。基于我们的多波长观测，我们提出A514提供了一个由合并驱动的气体运动引起的旧AGN等离子体重新分配的清晰案例。我们通过理想化的星系团合并模拟来支持我们的解释，该模拟采用被动示踪场来代表宇宙射线电子，并发现合并驱动的运动可以有效地在星系团外围产生这些粒子云，这些粒子云随后可以被星系团合并冲击重新加速并产生无线电遗迹。
{"title":"Discovery of A Large-scale Bent Radio Jet in the Merging Cluster A514","authors":"Wonki Lee, John ZuHone, M. James Jee, Kim HyeongHan, Ruta Kale, Eunmo Ahn","doi":"10.3847/2041-8213/acffc8","DOIUrl":"https://doi.org/10.3847/2041-8213/acffc8","url":null,"abstract":"Abstract We report a discovery of a large-scale bent radio jet in the merging galaxy cluster A514 ( z = 0.071). The radio emission originates from the two radio lobes of the active galactic nucleus (AGN) located near the center of the southern subcluster and extends toward the southern outskirts with multiple bends. Its peculiar morphology is characterized by a 400 kpc “bridge,” a 300 kpc “arc,” and a 400 kpc “tail,” which together contribute to its largest linear size of ∼0.7 Mpc. We find that both the flux and spectral features of the emission change with the distance from the AGN. Also, the “bridge” presents a 60% polarized radio emission, which coincided with an X-ray cold front. Based on our multiwavelength observations, we propose that A514 presents a clear case for the redistribution of an old AGN plasma due to merger-driven gas motions. We support our interpretation with idealized cluster merger simulations employing a passive tracer field to represent cosmic-ray electrons and find that merger-driven motions can efficiently create a cloud of these particles in the cluster outskirts, which later can be reaccelerated by the cluster merger shock and produce radio relics.","PeriodicalId":55567,"journal":{"name":"Astrophysical Journal Letters","volume":"17 3","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"134973867","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-10-25DOI: 10.3847/2041-8213/acfcbc
William J. Oldroyd, Colin Orion Chandler, Chadwick A. Trujillo, Scott S. Sheppard, Henry H. Hsieh, Jay K. Kueny, William A. Burris, Jarod A. DeSpain, Kennedy A. Farrell, Michele T. Mazzucato, Milton K. D. Bosch, Tiffany Shaw-Diaz, Virgilio Gonano
Abstract We have discovered two epochs of activity on quasi-Hilda 2009 DQ 118 . Small bodies that display comet-like activity, such as active asteroids and active quasi-Hildas, are important for understanding the distribution of water and other volatiles throughout the solar system. Through our NASA Partner Citizen Science project, Active Asteroids, volunteers classified archival images of 2009 DQ 118 as displaying comet-like activity. By performing an in-depth archival image search, we found over 20 images from UT 2016 March 8–9 with clear signs of a comet-like tail. We then carried out follow-up observations of 2009 DQ 118 using the 3.5 m Astrophysical Research Consortium Telescope at Apache Point Observatory, Sunspot, New Mexico, USA and the 6.5 m Magellan Baade Telescope at Las Campanas Observatory, Chile. These images revealed a second epoch of activity associated with the UT 2023 April 22 perihelion passage of 2009 DQ 118 . We performed photometric analysis of the tail and find that it had a similar apparent length and surface brightness during both epochs. We also explored the orbital history and future of 2009 DQ 118 through dynamical simulations. These simulations show that 2009 DQ 118 is currently a quasi-Hilda and that it frequently experiences close encounters with Jupiter. We find that 2009 DQ 118 is currently on the boundary between asteroidal and cometary orbits. Additionally, it has likely been a Jupiter family comet or Centaur for much of the past 10 kyr and will be in these same regions for the majority of the next 10 kyr. Since both detected epochs of activity occurred near perihelion, the observed activity is consistent with sublimation of volatile ices. 2009 DQ 118 is currently observable until ∼mid-October 2023. Further observations would help to characterize the observed activity.
{"title":"Recurring Activity Discovered on Quasi-Hilda 2009 DQ118","authors":"William J. Oldroyd, Colin Orion Chandler, Chadwick A. Trujillo, Scott S. Sheppard, Henry H. Hsieh, Jay K. Kueny, William A. Burris, Jarod A. DeSpain, Kennedy A. Farrell, Michele T. Mazzucato, Milton K. D. Bosch, Tiffany Shaw-Diaz, Virgilio Gonano","doi":"10.3847/2041-8213/acfcbc","DOIUrl":"https://doi.org/10.3847/2041-8213/acfcbc","url":null,"abstract":"Abstract We have discovered two epochs of activity on quasi-Hilda 2009 DQ 118 . Small bodies that display comet-like activity, such as active asteroids and active quasi-Hildas, are important for understanding the distribution of water and other volatiles throughout the solar system. Through our NASA Partner Citizen Science project, Active Asteroids, volunteers classified archival images of 2009 DQ 118 as displaying comet-like activity. By performing an in-depth archival image search, we found over 20 images from UT 2016 March 8–9 with clear signs of a comet-like tail. We then carried out follow-up observations of 2009 DQ 118 using the 3.5 m Astrophysical Research Consortium Telescope at Apache Point Observatory, Sunspot, New Mexico, USA and the 6.5 m Magellan Baade Telescope at Las Campanas Observatory, Chile. These images revealed a second epoch of activity associated with the UT 2023 April 22 perihelion passage of 2009 DQ 118 . We performed photometric analysis of the tail and find that it had a similar apparent length and surface brightness during both epochs. We also explored the orbital history and future of 2009 DQ 118 through dynamical simulations. These simulations show that 2009 DQ 118 is currently a quasi-Hilda and that it frequently experiences close encounters with Jupiter. We find that 2009 DQ 118 is currently on the boundary between asteroidal and cometary orbits. Additionally, it has likely been a Jupiter family comet or Centaur for much of the past 10 kyr and will be in these same regions for the majority of the next 10 kyr. Since both detected epochs of activity occurred near perihelion, the observed activity is consistent with sublimation of volatile ices. 2009 DQ 118 is currently observable until ∼mid-October 2023. Further observations would help to characterize the observed activity.","PeriodicalId":55567,"journal":{"name":"Astrophysical Journal Letters","volume":"20 3","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"134972739","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-10-25DOI: 10.3847/2041-8213/ad0130
Michael G. Jones, Burçin Mutlu-Pakdil, David J. Sand, Richard Donnerstein, Denija Crnojević, Paul Bennet, Catherine E. Fielder, Ananthan Karunakaran, Kristine Spekkens, Jay Strader, Ryan Urquhart, Dennis Zaritsky
Abstract We report the discovery of Pavo, a faint ( M V = −10.0), star-forming, irregular, and extremely isolated dwarf galaxy at D ≈ 2 Mpc. Pavo was identified in Dark Energy Camera Legacy Survey imaging via a novel approach that combines low surface brightness galaxy search algorithms and machine-learning candidate classifications. Follow-up imaging with the Inamori-Magellan Areal Camera and Spectrograph on the 6.5 m Magellan Baade telescope revealed a color–magnitude diagram (CMD) with an old stellar population, in addition to the young population that dominates the integrated light, and a tip of the red giant branch distance estimate of 1.99−0.22+0.20 Mpc. The blue population of stars in the CMD is consistent with the youngest stars having formed no later than 150 Myr ago. We also detected no H α emission with SOAR telescope imaging, suggesting that we may be witnessing a temporary low in Pavo’s star formation. We estimate the total stellar mass of Pavo to be logM*/M⊙=5.6±0.2 and measure an upper limit on its H i gas mass of 1.0 × 10 6 M ⊙ based on the HIPASS survey. Given these properties, Pavo’s closest analog is Leo P ( D = 1.6 Mpc), previously the only known isolated, star-forming, Local Volume dwarf galaxy in this mass range. However, Pavo appears to be even more isolated, with no other known galaxy residing within over 600 kpc. As surveys and search techniques continue to improve, we anticipate an entire population of analogous objects being detected just outside the Local Group.
摘要:我们报道了在D≈2 Mpc上发现了一个微弱的(M V =−10.0)，恒星形成，不规则，极其孤立的矮星系Pavo。Pavo是在暗能量相机遗产调查成像中通过一种结合低表面亮度星系搜索算法和机器学习候选分类的新方法确定的。在6.5米麦哲伦Baade望远镜上的Inamori-Magellan面相机和摄谱仪的后续成像显示了一个彩色星等图(CMD)，其中有一个年老的恒星群，以及占主导地位的年轻恒星群，红巨星分支距离估计为1.99−0.22 + 0.20 Mpc。CMD中蓝色的恒星群与最年轻的恒星形成时间不晚于150万年前一致。我们还用SOAR望远镜成像没有探测到H α辐射，这表明我们可能正在目睹帕沃星形成的暂时低谷。我们估计Pavo的总恒星质量为log M * / M⊙= 5.6±0.2，并根据HIPASS调查测量了其H气体质量的上限为1.0 × 10.6 M⊙。考虑到这些特性，Pavo最接近的类似物是狮子座P (D = 1.6 Mpc)，它是之前已知的唯一一个在这个质量范围内孤立的、形成恒星的局域体积矮星系。然而，帕沃似乎更加孤立，没有其他已知的星系居住在600公里以外。随着调查和搜索技术的不断改进，我们预计会在本地群体之外发现一大批类似的物体。
{"title":"Pavo: Discovery of a Star-forming Dwarf Galaxy Just Outside the Local Group*","authors":"Michael G. Jones, Burçin Mutlu-Pakdil, David J. Sand, Richard Donnerstein, Denija Crnojević, Paul Bennet, Catherine E. Fielder, Ananthan Karunakaran, Kristine Spekkens, Jay Strader, Ryan Urquhart, Dennis Zaritsky","doi":"10.3847/2041-8213/ad0130","DOIUrl":"https://doi.org/10.3847/2041-8213/ad0130","url":null,"abstract":"Abstract We report the discovery of Pavo, a faint ( M V = −10.0), star-forming, irregular, and extremely isolated dwarf galaxy at D ≈ 2 Mpc. Pavo was identified in Dark Energy Camera Legacy Survey imaging via a novel approach that combines low surface brightness galaxy search algorithms and machine-learning candidate classifications. Follow-up imaging with the Inamori-Magellan Areal Camera and Spectrograph on the 6.5 m Magellan Baade telescope revealed a color–magnitude diagram (CMD) with an old stellar population, in addition to the young population that dominates the integrated light, and a tip of the red giant branch distance estimate of <?CDATA ${1.99}_{-0.22}^{+0.20}$?> <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" overflow=\"scroll\"> <mml:msubsup> <mml:mrow> <mml:mn>1.99</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.22</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.20</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> Mpc. The blue population of stars in the CMD is consistent with the youngest stars having formed no later than 150 Myr ago. We also detected no H α emission with SOAR telescope imaging, suggesting that we may be witnessing a temporary low in Pavo’s star formation. We estimate the total stellar mass of Pavo to be <?CDATA $mathrm{log}{M}_{* }/{M}_{odot }=5.6pm 0.2$?> <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" overflow=\"scroll\"> <mml:mi>log</mml:mi> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>*</mml:mo> </mml:mrow> </mml:msub> <mml:mrow> <mml:mo stretchy=\"true\">/</mml:mo> </mml:mrow> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⊙</mml:mo> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:mn>5.6</mml:mn> <mml:mo>±</mml:mo> <mml:mn>0.2</mml:mn> </mml:math> and measure an upper limit on its H i gas mass of 1.0 × 10 6 M ⊙ based on the HIPASS survey. Given these properties, Pavo’s closest analog is Leo P ( D = 1.6 Mpc), previously the only known isolated, star-forming, Local Volume dwarf galaxy in this mass range. However, Pavo appears to be even more isolated, with no other known galaxy residing within over 600 kpc. As surveys and search techniques continue to improve, we anticipate an entire population of analogous objects being detected just outside the Local Group.","PeriodicalId":55567,"journal":{"name":"Astrophysical Journal Letters","volume":"2 4 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135168886","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-10-23DOI: 10.3847/2041-8213/ad0158
Fabio Pacucci, Bao Nguyen, Stefano Carniani, Roberto Maiolino, Xiaohui Fan
Abstract JWST is revolutionizing our understanding of the high- z Universe by expanding the black hole horizon, looking farther and to smaller masses, and revealing the stellar light of their hosts. By examining JWST galaxies at z = 4–7 that host H α -detected black holes, we investigate (i) the high- z M • – M ⋆ relation and (ii) the black hole mass distribution, especially in its low-mass range ( M • ≲ 10 6.5 M ⊙ ). With a detailed statistical analysis, our findings conclusively reveal a high- z M • – M ⋆ relation that deviates at >3 σ confidence level from the local relation. The high- z relation is <?CDATA $mathrm{log}({M}_{bullet }/,{M}_{odot })=-{2.43}_{-0.83}^{+0.83}+{1.06}_{-0.09}^{+0.09}mathrm{log}({M}_{star }/,{M}_{odot })$?> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>log</mml:mi> <mml:mo stretchy="false">(</mml:mo> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>•</mml:mo> </mml:mrow> </mml:msub> <mml:mrow> <mml:mo stretchy="true">/</mml:mo> </mml:mrow> <mml:mspace width="0.25em" /> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⊙</mml:mo> </mml:mrow> </mml:msub> <mml:mo stretchy="false">)</mml:mo> <mml:mo>=</mml:mo> <mml:mo>−</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>2.43</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.83</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.83</mml:mn> </mml:mrow> </mml:msubsup> <mml:mo>+</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>1.06</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.09</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.09</mml:mn> </mml:mrow> </mml:msubsup> <mml:mi>log</mml:mi> <mml:mo stretchy="false">(</mml:mo> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⋆</mml:mo> </mml:mrow> </mml:msub> <mml:mrow> <mml:mo stretchy="true">/</mml:mo> </mml:mrow> <mml:mspace width="0.25em" /> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⊙</mml:mo> </mml:mrow> </mml:msub> <mml:mo stretchy="false">)</mml:mo> </mml:math> . Black holes are overmassive by ∼10–100× compared to their low- z counterparts in galactic hosts of the same stellar mass. This fact is not due to a selection effect in surveys. Moreover, our analysis predicts the possibility of detecting in high- z JWST surveys 5–15× more black holes with M • ≲ 10 6.5 M ⊙ , and 10–30× more with M • ≲ 10 8.5 M ⊙ , compared to local relation’s predictions. The lighter black holes preferentially occupy galaxies with a stellar mass of ∼10 7.5 –10 8 M ⊙ . We have yet to detect these sources because (i) they may be inactive (duty cycles 1%–10%), (ii) the host overshines the active galactic nucleus (AGN), or (iii) the AGN is obscured and not immediately recognizable by line diagnostics. A search of low-mass black holes in existing JWST surveys will further test the M • – M ⋆ relation. Current JWST fields represent a treasure trove of black hole systems at z = 4–7; their
{"title":"JWST CEERS and JADES Active Galaxies at z = 4–7 Violate the Local M <sub>•</sub>–M <sub>⋆</sub> Relation at >3σ: Implications for Low-mass Black Holes and Seeding Models","authors":"Fabio Pacucci, Bao Nguyen, Stefano Carniani, Roberto Maiolino, Xiaohui Fan","doi":"10.3847/2041-8213/ad0158","DOIUrl":"https://doi.org/10.3847/2041-8213/ad0158","url":null,"abstract":"Abstract JWST is revolutionizing our understanding of the high- z Universe by expanding the black hole horizon, looking farther and to smaller masses, and revealing the stellar light of their hosts. By examining JWST galaxies at z = 4–7 that host H α -detected black holes, we investigate (i) the high- z M • – M ⋆ relation and (ii) the black hole mass distribution, especially in its low-mass range ( M • ≲ 10 6.5 M ⊙ ). With a detailed statistical analysis, our findings conclusively reveal a high- z M • – M ⋆ relation that deviates at >3 σ confidence level from the local relation. The high- z relation is <?CDATA $mathrm{log}({M}_{bullet }/,{M}_{odot })=-{2.43}_{-0.83}^{+0.83}+{1.06}_{-0.09}^{+0.09}mathrm{log}({M}_{star }/,{M}_{odot })$?> <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" overflow=\"scroll\"> <mml:mi>log</mml:mi> <mml:mo stretchy=\"false\">(</mml:mo> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>•</mml:mo> </mml:mrow> </mml:msub> <mml:mrow> <mml:mo stretchy=\"true\">/</mml:mo> </mml:mrow> <mml:mspace width=\"0.25em\" /> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⊙</mml:mo> </mml:mrow> </mml:msub> <mml:mo stretchy=\"false\">)</mml:mo> <mml:mo>=</mml:mo> <mml:mo>−</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>2.43</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.83</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.83</mml:mn> </mml:mrow> </mml:msubsup> <mml:mo>+</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>1.06</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.09</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.09</mml:mn> </mml:mrow> </mml:msubsup> <mml:mi>log</mml:mi> <mml:mo stretchy=\"false\">(</mml:mo> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⋆</mml:mo> </mml:mrow> </mml:msub> <mml:mrow> <mml:mo stretchy=\"true\">/</mml:mo> </mml:mrow> <mml:mspace width=\"0.25em\" /> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⊙</mml:mo> </mml:mrow> </mml:msub> <mml:mo stretchy=\"false\">)</mml:mo> </mml:math> . Black holes are overmassive by ∼10–100× compared to their low- z counterparts in galactic hosts of the same stellar mass. This fact is not due to a selection effect in surveys. Moreover, our analysis predicts the possibility of detecting in high- z JWST surveys 5–15× more black holes with M • ≲ 10 6.5 M ⊙ , and 10–30× more with M • ≲ 10 8.5 M ⊙ , compared to local relation’s predictions. The lighter black holes preferentially occupy galaxies with a stellar mass of ∼10 7.5 –10 8 M ⊙ . We have yet to detect these sources because (i) they may be inactive (duty cycles 1%–10%), (ii) the host overshines the active galactic nucleus (AGN), or (iii) the AGN is obscured and not immediately recognizable by line diagnostics. A search of low-mass black holes in existing JWST surveys will further test the M • – M ⋆ relation. Current JWST fields represent a treasure trove of black hole systems at z = 4–7; their ","PeriodicalId":55567,"journal":{"name":"Astrophysical Journal Letters","volume":"52 3","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135366268","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-10-23DOI: 10.3847/2041-8213/acff61
Kiana D. McFadden, Amy K. Mainzer, Joseph R. Masiero, James M. Bauer, Roc M. Cutri, Dar Dahlen, Frank J. Masci, Jana Pittichová, Akash Satpathy, Edward L. Wright
Abstract Probing small main-belt asteroids provides insight into their formation and evolution through multiple dynamical and collisional processes. These asteroids also overlap in size with the potentially hazardous near-Earth object population and supply the majority of these objects. The Lucy mission will perform a flyby of the small main-belt asteroid, (152830) Dinkinesh, on 2023 November 1, in preparation for its mission to the Jupiter Trojan asteroids. In this Letter, we present data to support the planning of Lucy’s imminent encounter of Dinkinesh. We employed aperture photometry on stacked frames of Dinkinesh obtained by the Wide-field Infrared Survey Explorer and performed thermal modeling on a detection at 12 μ m to compute diameter and albedo values. Through this method, we determined Dinkinesh has an effective spherical diameter of 0.76−0.21+0.11 km and a visual geometric albedo of 0.27−0.06+0.25 at the 16th and 84th percentiles. This albedo is consistent with typical stony (S-type) asteroids. These measurements will enable the Lucy team to optimize planning for the flyby of Dinkinesh, including refinement of exposure times and flyby geometry. The data obtained from this mission will, in turn, allow us to better understand the calibration of our thermal models by providing ground truth data. The Lucy flyby presents a rare opportunity to study the smallest main-belt asteroid ever observed in situ.
{"title":"Size and Albedo Constraints for (152830) Dinkinesh Using WISE Data","authors":"Kiana D. McFadden, Amy K. Mainzer, Joseph R. Masiero, James M. Bauer, Roc M. Cutri, Dar Dahlen, Frank J. Masci, Jana Pittichová, Akash Satpathy, Edward L. Wright","doi":"10.3847/2041-8213/acff61","DOIUrl":"https://doi.org/10.3847/2041-8213/acff61","url":null,"abstract":"Abstract Probing small main-belt asteroids provides insight into their formation and evolution through multiple dynamical and collisional processes. These asteroids also overlap in size with the potentially hazardous near-Earth object population and supply the majority of these objects. The Lucy mission will perform a flyby of the small main-belt asteroid, (152830) Dinkinesh, on 2023 November 1, in preparation for its mission to the Jupiter Trojan asteroids. In this Letter, we present data to support the planning of Lucy’s imminent encounter of Dinkinesh. We employed aperture photometry on stacked frames of Dinkinesh obtained by the Wide-field Infrared Survey Explorer and performed thermal modeling on a detection at 12 μ m to compute diameter and albedo values. Through this method, we determined Dinkinesh has an effective spherical diameter of <?CDATA ${0.76}_{-0.21}^{+0.11}$?> <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" overflow=\"scroll\"> <mml:msubsup> <mml:mrow> <mml:mn>0.76</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.21</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.11</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> km and a visual geometric albedo of <?CDATA ${0.27}_{-0.06}^{+0.25}$?> <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" overflow=\"scroll\"> <mml:msubsup> <mml:mrow> <mml:mn>0.27</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.06</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.25</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> at the 16th and 84th percentiles. This albedo is consistent with typical stony (S-type) asteroids. These measurements will enable the Lucy team to optimize planning for the flyby of Dinkinesh, including refinement of exposure times and flyby geometry. The data obtained from this mission will, in turn, allow us to better understand the calibration of our thermal models by providing ground truth data. The Lucy flyby presents a rare opportunity to study the smallest main-belt asteroid ever observed in situ.","PeriodicalId":55567,"journal":{"name":"Astrophysical Journal Letters","volume":"23 12","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135366266","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2023-10-01DOI: 10.3847/2041-8213/acfc25
T. Moore, S. J. Smartt, M. Nicholl, S. Srivastav, H. F. Stevance, D. B. Jess, S. D. T. Grant, M. D. Fulton, L. Rhodes, S. A. Sim, R. Hirai, P. Podsiadlowski, J. P. Anderson, C. Ashall, W. Bate, R. Fender, C. P. Gutiérrez, D. A. Howell, M. E. Huber, C. Inserra, G. Leloudas, L. A. G. Monard, T. E. Müller-Bravo, B. J. Shappee, K. W. Smith, G. Terreran, J. Tonry, M. A. Tucker, D. R. Young, A. Aamer, T.-W. Chen, F. Ragosta, L. Galbany, M. Gromadzki, L. Harvey, P. Hoeflich, C. McCully, M. Newsome, E. P. Gonzalez, C. Pellegrino, P. Ramsden, M. Pérez-Torres, E. J. Ridley, X. Sheng, J. Weston
Abstract We present multiwavelength photometry and spectroscopy of SN 2022jli, an unprecedented Type Ic supernova discovered in the galaxy NGC 157 at a distance of ≈ 23 Mpc. The multiband light curves reveal many remarkable characteristics. Peaking at a magnitude of g = 15.11 ± 0.02, the high-cadence photometry reveals periodic undulations of 12.5 ± 0.2 days superimposed on the 200-day supernova decline. This periodicity is observed in the light curves from nine separate filter and instrument configurations with peak-to-peak amplitudes of ≃ 0.1 mag. This is the first time that repeated periodic oscillations, over many cycles, have been detected in a supernova light curve. SN 2022jli also displays an extreme early excess that fades over ≈25 days, followed by a rise to a peak luminosity of L opt = 10 42.1 erg s −1 . Although the exact explosion epoch is not constrained by data, the time from explosion to maximum light is ≳ 59 days. The luminosity can be explained by a large ejecta mass ( M ej ≈ 12 ± 6 M ⊙ ) powered by 56 Ni, but we find it difficult to quantitatively model the early excess with circumstellar interaction and cooling. Collision between the supernova ejecta and a binary companion is a possible source of this emission. We discuss the origin of the periodic variability in the light curve, including interaction of the SN ejecta with nested shells of circumstellar matter and neutron stars colliding with binary companions.
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