Pub Date : 2023-11-01DOI: 10.3847/1538-4365/acfa95
R. Abbasi, M. Ackermann, J. Adams, S. K. Agarwalla, J. A. Aguilar, M. Ahlers, J. M. Alameddine, N. M. Amin, K. Andeen, G. Anton, C. Argüelles, Y. Ashida, S. Athanasiadou, S. N. Axani, X. Bai, A. Balagopal V, M. Baricevic, S. W. Barwick, V. Basu, R. Bay, J. J. Beatty, K.-H. Becker, J. Becker Tjus, J. Beise, C. Bellenghi, S. BenZvi, D. Berley, E. Bernardini, D. Z. Besson, G. Binder, D. Bindig, E. Blaufuss, S. Blot, F. Bontempo, J. Y. Book, C. Boscolo Meneguolo, S. Böser, O. Botner, J. Böttcher, E. Bourbeau, J. Braun, B. Brinson, J. Brostean-Kaiser, R. T. Burley, R. S. Busse, D. Butterfield, M. A. Campana, K. Carloni, E. G. Carnie-Bronca, S. Chattopadhyay, N. Chau, C. Chen, Z. Chen, D. Chirkin, S. Choi, B. A. Clark, L. Classen, A. Coleman, G. H. Collin, A. Connolly, J. M. Conrad, P. Coppin, P. Correa, S. Countryman, D. F. Cowen, P. Dave, C. De Clercq, J. J. DeLaunay, D. Delgado, H. Dembinski, S. Deng, K. Deoskar, A. Desai, P. Desiati, K. D. de Vries, G. de Wasseige, T. DeYoung, A. Diaz, J. C. Díaz-Vélez, M. Dittmer, A. Domi, H. Dujmovic, M. A. DuVernois, T. Ehrhardt, P. Eller, R. Engel, H. Erpenbeck, J. Evans, P. A. Evenson, K. L. Fan, K. Fang, K. Farrag, A. R. Fazely, A. Fedynitch, N. Feigl, S. Fiedlschuster, C. Finley, L. Fischer, D. Fox, A. Franckowiak
Abstract We present a catalog of likely astrophysical neutrino track-like events from the IceCube Neutrino Observatory. IceCube began reporting likely astrophysical neutrinos in 2016, and this system was updated in 2019. The catalog presented here includes events that were reported in real time since 2019, as well as events identified in archival data samples starting from 2011. We report 275 neutrino events from two selection channels as the first entries in the catalog, the IceCube Event Catalog of Alert Tracks, which will see ongoing extensions with additional alerts. The Gold and Bronze alert channels respectively provide neutrino candidates with a 50% and 30% probability of being astrophysical, on average assuming an astrophysical neutrino power-law energy spectral index of 2.19. For each neutrino alert, we provide the reconstructed energy, direction, false-alarm rate, probability of being astrophysical in origin, and likelihood contours describing the spatial uncertainty in the alert's reconstructed location. We also investigate a directional correlation of these neutrino events with gamma-ray and X-ray catalogs, including 4FGL, 3HWC, TeVCat, and Swift-BAT.
{"title":"IceCat-1: The IceCube Event Catalog of Alert Tracks","authors":"R. Abbasi, M. Ackermann, J. Adams, S. K. Agarwalla, J. A. Aguilar, M. Ahlers, J. M. Alameddine, N. M. Amin, K. Andeen, G. Anton, C. Argüelles, Y. Ashida, S. Athanasiadou, S. N. Axani, X. Bai, A. Balagopal V, M. Baricevic, S. W. Barwick, V. Basu, R. Bay, J. J. Beatty, K.-H. Becker, J. Becker Tjus, J. Beise, C. Bellenghi, S. BenZvi, D. Berley, E. Bernardini, D. Z. Besson, G. Binder, D. Bindig, E. Blaufuss, S. Blot, F. Bontempo, J. Y. Book, C. Boscolo Meneguolo, S. Böser, O. Botner, J. Böttcher, E. Bourbeau, J. Braun, B. Brinson, J. Brostean-Kaiser, R. T. Burley, R. S. Busse, D. Butterfield, M. A. Campana, K. Carloni, E. G. Carnie-Bronca, S. Chattopadhyay, N. Chau, C. Chen, Z. Chen, D. Chirkin, S. Choi, B. A. Clark, L. Classen, A. Coleman, G. H. Collin, A. Connolly, J. M. Conrad, P. Coppin, P. Correa, S. Countryman, D. F. Cowen, P. Dave, C. De Clercq, J. J. DeLaunay, D. Delgado, H. Dembinski, S. Deng, K. Deoskar, A. Desai, P. Desiati, K. D. de Vries, G. de Wasseige, T. DeYoung, A. Diaz, J. C. Díaz-Vélez, M. Dittmer, A. Domi, H. Dujmovic, M. A. DuVernois, T. Ehrhardt, P. Eller, R. Engel, H. Erpenbeck, J. Evans, P. A. Evenson, K. L. Fan, K. Fang, K. Farrag, A. R. Fazely, A. Fedynitch, N. Feigl, S. Fiedlschuster, C. Finley, L. Fischer, D. Fox, A. Franckowiak","doi":"10.3847/1538-4365/acfa95","DOIUrl":"https://doi.org/10.3847/1538-4365/acfa95","url":null,"abstract":"Abstract We present a catalog of likely astrophysical neutrino track-like events from the IceCube Neutrino Observatory. IceCube began reporting likely astrophysical neutrinos in 2016, and this system was updated in 2019. The catalog presented here includes events that were reported in real time since 2019, as well as events identified in archival data samples starting from 2011. We report 275 neutrino events from two selection channels as the first entries in the catalog, the IceCube Event Catalog of Alert Tracks, which will see ongoing extensions with additional alerts. The Gold and Bronze alert channels respectively provide neutrino candidates with a 50% and 30% probability of being astrophysical, on average assuming an astrophysical neutrino power-law energy spectral index of 2.19. For each neutrino alert, we provide the reconstructed energy, direction, false-alarm rate, probability of being astrophysical in origin, and likelihood contours describing the spatial uncertainty in the alert's reconstructed location. We also investigate a directional correlation of these neutrino events with gamma-ray and X-ray catalogs, including 4FGL, 3HWC, TeVCat, and Swift-BAT.","PeriodicalId":8588,"journal":{"name":"Astrophysical Journal Supplement Series","volume":"56 6-9","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135411110","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 : 2023-11-01DOI: 10.3847/1538-4365/acf850
J. R. Weaver, L. Zalesky, V. Kokorev, C. J. R. McPartland, N. Chartab, K. M. L. Gould, M. Shuntov, I. Davidzon, A. Faisst, N. Stickley, P. L. Capak, S. Toft, D. Masters, B. Mobasher, D. B. Sanders, O. B. Kauffmann, H. J. McCracken, O. Ilbert, G. Brammer, A. Moneti
Abstract While space-borne optical and near-infrared facilities have succeeded in delivering a precise and spatially resolved picture of our Universe, their small survey area is known to underrepresent the true diversity of galaxy populations. Ground-based surveys have reached comparable depths but at lower spatial resolution, resulting in source confusion that hampers accurate photometry extractions. What once was limited to the infrared regime has now begun to challenge ground-based ultradeep surveys, affecting detection and photometry alike. Failing to address these challenges will mean forfeiting a representative view into the distant Universe. We introduce The Farmer : an automated, reproducible profile-fitting photometry package that pairs a library of smooth parametric models from The Tractor with a decision tree that determines the best-fit model in concert with neighboring sources. Photometry is measured by fitting the models on other bands leaving brightness free to vary. The resulting photometric measurements are naturally total, and no aperture corrections are required. Supporting diagnostics (e.g., χ 2 ) enable measurement validation. As fitting models is relatively time intensive, The Farmer is built with high-performance computing routines. We benchmark The Farmer on a set of realistic COSMOS-like images and find accurate photometry, number counts, and galaxy shapes. The Farmer is already being utilized to produce catalogs for several large-area deep extragalactic surveys where it has been shown to tackle some of the most challenging optical and near-infrared data available, with the promise of extending to other ultradeep surveys expected in the near future. The Farmer is available to download from GitHub ( https://github.com/astroweaver/the_farmer ) and Zenodo ( https://doi.org/10.5281/zenodo.8205817 ).
{"title":"The Farmer: A Reproducible Profile-fitting Photometry Package for Deep Galaxy Surveys","authors":"J. R. Weaver, L. Zalesky, V. Kokorev, C. J. R. McPartland, N. Chartab, K. M. L. Gould, M. Shuntov, I. Davidzon, A. Faisst, N. Stickley, P. L. Capak, S. Toft, D. Masters, B. Mobasher, D. B. Sanders, O. B. Kauffmann, H. J. McCracken, O. Ilbert, G. Brammer, A. Moneti","doi":"10.3847/1538-4365/acf850","DOIUrl":"https://doi.org/10.3847/1538-4365/acf850","url":null,"abstract":"Abstract While space-borne optical and near-infrared facilities have succeeded in delivering a precise and spatially resolved picture of our Universe, their small survey area is known to underrepresent the true diversity of galaxy populations. Ground-based surveys have reached comparable depths but at lower spatial resolution, resulting in source confusion that hampers accurate photometry extractions. What once was limited to the infrared regime has now begun to challenge ground-based ultradeep surveys, affecting detection and photometry alike. Failing to address these challenges will mean forfeiting a representative view into the distant Universe. We introduce The Farmer : an automated, reproducible profile-fitting photometry package that pairs a library of smooth parametric models from The Tractor with a decision tree that determines the best-fit model in concert with neighboring sources. Photometry is measured by fitting the models on other bands leaving brightness free to vary. The resulting photometric measurements are naturally total, and no aperture corrections are required. Supporting diagnostics (e.g., χ 2 ) enable measurement validation. As fitting models is relatively time intensive, The Farmer is built with high-performance computing routines. We benchmark The Farmer on a set of realistic COSMOS-like images and find accurate photometry, number counts, and galaxy shapes. The Farmer is already being utilized to produce catalogs for several large-area deep extragalactic surveys where it has been shown to tackle some of the most challenging optical and near-infrared data available, with the promise of extending to other ultradeep surveys expected in the near future. The Farmer is available to download from GitHub ( https://github.com/astroweaver/the_farmer ) and Zenodo ( https://doi.org/10.5281/zenodo.8205817 ).","PeriodicalId":8588,"journal":{"name":"Astrophysical Journal Supplement Series","volume":"38 6","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135221015","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 : 2023-11-01DOI: 10.3847/1538-4365/acf932
Yongxin Wen, Weicheng Zang, Bo Ma
Abstract To overcome the high optical extinction, near-infrared (NIR) observations are needed for probing the microlensing events toward the Galactic center. The 2015–2019 UKIRT microlensing survey toward the Galactic center is the first dedicated precursor NIR survey for the Nancy Grace Roman Space Telescope. Here, we analyze the online data from the UKIRT microlensing survey, reaching l = b = 0°. Using the event-finder algorithm of KMTNet with the Δ χ 2 threshold of 250, we find 522 clear events, 436 possible events, and 27 possible anomalous events. We fit a point-source point-lens (PSPL) model to all the clear events and derive the PSPL parameters with uncertainties using a Markov Chain Monte Carlo method. Assuming perfect detection efficiency, we compute the uncorrected event rates, which should serve as the lower limits on the true event rate. We find that the uncorrected NIR event rates are likely rising toward the Galactic center and are higher than the optical event rates.
为了克服高光学消光，需要近红外(NIR)观测来探测朝向银河系中心的微透镜事件。2015-2019年UKIRT对银河系中心的微透镜调查是南希·格蕾丝·罗马太空望远镜第一次专门的前体近红外调查。在这里，我们分析了UKIRT微透镜调查的在线数据，达到l = b = 0°。使用KMTNet的事件查找器算法，Δ χ 2阈值为250，我们发现了522个清晰事件，436个可能事件和27个可能异常事件。我们拟合了一个点源点透镜(PSPL)模型，并利用马尔可夫链蒙特卡罗方法导出了具有不确定性的PSPL参数。假设完美的检测效率，我们计算未校正的事件率，它应该作为真实事件率的下限。我们发现，未校正的近红外事件率可能朝着银河系中心上升，并且高于光学事件率。
{"title":"Toward Measuring the Microlensing Event Rate in the Galactic Center. I. Event Detection from the UKIRT Microlensing Survey Data","authors":"Yongxin Wen, Weicheng Zang, Bo Ma","doi":"10.3847/1538-4365/acf932","DOIUrl":"https://doi.org/10.3847/1538-4365/acf932","url":null,"abstract":"Abstract To overcome the high optical extinction, near-infrared (NIR) observations are needed for probing the microlensing events toward the Galactic center. The 2015–2019 UKIRT microlensing survey toward the Galactic center is the first dedicated precursor NIR survey for the Nancy Grace Roman Space Telescope. Here, we analyze the online data from the UKIRT microlensing survey, reaching l = b = 0°. Using the event-finder algorithm of KMTNet with the Δ χ 2 threshold of 250, we find 522 clear events, 436 possible events, and 27 possible anomalous events. We fit a point-source point-lens (PSPL) model to all the clear events and derive the PSPL parameters with uncertainties using a Markov Chain Monte Carlo method. Assuming perfect detection efficiency, we compute the uncorrected event rates, which should serve as the lower limits on the true event rate. We find that the uncorrected NIR event rates are likely rising toward the Galactic center and are higher than the optical event rates.","PeriodicalId":8588,"journal":{"name":"Astrophysical Journal Supplement Series","volume":"58 2","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135456284","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 : 2023-11-01DOI: 10.3847/1538-4365/acfc19
Soham Mandal, Paul C. Duffell
Abstract We present the publicly available moving-mesh hydrodynamics code Sprout . Sprout solves the equations of ideal hydrodynamics on an expanding Cartesian mesh. The expanding mesh can follow fluid outflows for several orders of magnitude with very little numerical diffusion, thereby capturing shocks and fine structures accurately. Following the bulk flow accurately also allows for longer time steps in general. This makes Sprout particularly suitable for studying expanding outflows such as supernova remnants and active galactic nuclei. Relative to other moving-mesh codes, the simple mesh structure in Sprout is also convenient for implementing additional physics or algorithms. Many code tests are performed to test the accuracy and performance of the numerical scheme.
{"title":"SPROUT: A Moving-mesh Hydro Code Using a Uniformly Expanding Cartesian Grid","authors":"Soham Mandal, Paul C. Duffell","doi":"10.3847/1538-4365/acfc19","DOIUrl":"https://doi.org/10.3847/1538-4365/acfc19","url":null,"abstract":"Abstract We present the publicly available moving-mesh hydrodynamics code Sprout . Sprout solves the equations of ideal hydrodynamics on an expanding Cartesian mesh. The expanding mesh can follow fluid outflows for several orders of magnitude with very little numerical diffusion, thereby capturing shocks and fine structures accurately. Following the bulk flow accurately also allows for longer time steps in general. This makes Sprout particularly suitable for studying expanding outflows such as supernova remnants and active galactic nuclei. Relative to other moving-mesh codes, the simple mesh structure in Sprout is also convenient for implementing additional physics or algorithms. Many code tests are performed to test the accuracy and performance of the numerical scheme.","PeriodicalId":8588,"journal":{"name":"Astrophysical Journal Supplement Series","volume":"9 3","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135565029","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 : 2023-11-01DOI: 10.3847/1538-4365/acfbe4
Paulina Sowicka, Gerald Handler, David Jones, John A. R. Caldwell, Francois van Wyk, Ernst Paunzen, Karolina Bąkowska, Luis Peralta de Arriba, Lucía Suárez-Andrés, Klaus Werner, Marie Karjalainen, Daniel L. Holdsworth
Abstract We present the results of new time-series photometric observations of 29 pre–white dwarf stars of PG 1159 spectral type, carried out in the years 2014–2022. For the majority of stars, a median noise level in Fourier amplitude spectra of 0.5–1.0 mmag was achieved. This allowed the detection of pulsations in the central star of planetary nebula A72 (Abell 72), consistent with g modes excited in GW Vir stars, and variability in RX J0122.9–7521 that could be due to pulsations, binarity, or rotation. For the remaining stars from the sample that were not observed to vary, we placed upper limits for variability. After combination with literature data, our results place the fraction of pulsating PG 1159 stars within the GW Vir instability strip at 36%. An updated list of all known PG 1159 stars is provided, containing astrometric measurements from the recent Gaia DR3 data, as well as information on physical parameters, variability, and nitrogen content. Those data are used to calculate luminosities for all PG 1159 stars to place the whole sample on the theoretical Hertzsprung–Russell diagram for the first time in that way. The pulsating stars are discussed as a group, and arguments are given that the traditional separation of GW Vir pulsators in “DOV” and “PNNV” stars is misleading and should not be used.
{"title":"The GW Vir Instability Strip in Light of New Observations of PG 1159 Stars: Discovery of Pulsations in the Central Star of A72 and Variability of RX J0122.9–7521","authors":"Paulina Sowicka, Gerald Handler, David Jones, John A. R. Caldwell, Francois van Wyk, Ernst Paunzen, Karolina Bąkowska, Luis Peralta de Arriba, Lucía Suárez-Andrés, Klaus Werner, Marie Karjalainen, Daniel L. Holdsworth","doi":"10.3847/1538-4365/acfbe4","DOIUrl":"https://doi.org/10.3847/1538-4365/acfbe4","url":null,"abstract":"Abstract We present the results of new time-series photometric observations of 29 pre–white dwarf stars of PG 1159 spectral type, carried out in the years 2014–2022. For the majority of stars, a median noise level in Fourier amplitude spectra of 0.5–1.0 mmag was achieved. This allowed the detection of pulsations in the central star of planetary nebula A72 (Abell 72), consistent with g modes excited in GW Vir stars, and variability in RX J0122.9–7521 that could be due to pulsations, binarity, or rotation. For the remaining stars from the sample that were not observed to vary, we placed upper limits for variability. After combination with literature data, our results place the fraction of pulsating PG 1159 stars within the GW Vir instability strip at 36%. An updated list of all known PG 1159 stars is provided, containing astrometric measurements from the recent Gaia DR3 data, as well as information on physical parameters, variability, and nitrogen content. Those data are used to calculate luminosities for all PG 1159 stars to place the whole sample on the theoretical Hertzsprung–Russell diagram for the first time in that way. The pulsating stars are discussed as a group, and arguments are given that the traditional separation of GW Vir pulsators in “DOV” and “PNNV” stars is misleading and should not be used.","PeriodicalId":8588,"journal":{"name":"Astrophysical Journal Supplement Series","volume":"38 10","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135615868","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 : 2023-11-01DOI: 10.3847/1538-4365/acfef6
Jan Novotný, Karel Adámek, M. A. Clark, Mike Giles, Wes Armour
Abstract Astrophysical radio signals are excellent probes of extreme physical processes that emit them. However, to reach Earth, electromagnetic radiation passes through the ionized interstellar medium, introducing a frequency-dependent time delay (dispersion) to the emitted signal. Removing dispersion enables searches for transient signals like fast radio bursts or repeating signals from isolated pulsars or those in orbit around other compact objects. The sheer volume and high resolution of data that next-generation radio telescopes will produce require high-performance computing solutions and algorithms to be used in time-domain data-processing pipelines to extract scientifically valuable results in real time. This paper presents a state-of-the-art implementation of brute force incoherent dedispersion on NVIDIA graphics-processing units and on Intel and AMD central-processing units. We show that our implementation is 4× faster (8-bit 8192 channels input) than other available solutions, and we demonstrate, using 11 existing telescopes, that our implementation is at least 20× faster than real time. This work is part of the AstroAccelerate package.
{"title":"Accelerating Dedispersion Using Many-core Architectures","authors":"Jan Novotný, Karel Adámek, M. A. Clark, Mike Giles, Wes Armour","doi":"10.3847/1538-4365/acfef6","DOIUrl":"https://doi.org/10.3847/1538-4365/acfef6","url":null,"abstract":"Abstract Astrophysical radio signals are excellent probes of extreme physical processes that emit them. However, to reach Earth, electromagnetic radiation passes through the ionized interstellar medium, introducing a frequency-dependent time delay (dispersion) to the emitted signal. Removing dispersion enables searches for transient signals like fast radio bursts or repeating signals from isolated pulsars or those in orbit around other compact objects. The sheer volume and high resolution of data that next-generation radio telescopes will produce require high-performance computing solutions and algorithms to be used in time-domain data-processing pipelines to extract scientifically valuable results in real time. This paper presents a state-of-the-art implementation of brute force incoherent dedispersion on NVIDIA graphics-processing units and on Intel and AMD central-processing units. We show that our implementation is 4× faster (8-bit 8192 channels input) than other available solutions, and we demonstrate, using 11 existing telescopes, that our implementation is at least 20× faster than real time. This work is part of the AstroAccelerate package.","PeriodicalId":8588,"journal":{"name":"Astrophysical Journal Supplement Series","volume":"27 5","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135510461","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 : 2023-11-01DOI: 10.3847/1538-4365/acf840
Adam Singor, Liam H. Scarlett, Mark C. Zammit, Igor Bray, Dmitry V. Fursa
Abstract Photoionization cross sections and rate coefficients have been calculated for all bound vibrational levels of the 1s σ g state of H2+ , HD + , and D2+ . The Born–Oppenheimer approximation is employed in our calculation of vibrationally resolved photoionization cross sections. Vibrationally resolved and local thermal equilibrium photoionization rate coefficients are presented for photon temperatures less than 50,000 K and are found to be several orders of magnitude larger than previous results in the literature. Analytic fits for the vibrationally resolved and local thermal equilibrium photoionization rate coefficients are provided. Near-threshold oscillations in the vibrationally resolved photoionization are observed. A benchmark set of photoionization cross sections are presented. Fixed-nuclei photoionization cross sections are calculated using two-center true continuum wave functions and are verified by comparison with previous calculations and are found to be in excellent agreement in all cases. Data files for our set of benchmark cross sections, rate coefficients, and fitting parameters for H2+ , HD + , and D2+ are available on Zenodo under an open-source Creative Commons Attribution license at doi: 10.5281/zenodo.8304061 .
{"title":"Photoionization from the Ground and Excited Vibrational States of H2+ and Its Deuterated Isotopologues","authors":"Adam Singor, Liam H. Scarlett, Mark C. Zammit, Igor Bray, Dmitry V. Fursa","doi":"10.3847/1538-4365/acf840","DOIUrl":"https://doi.org/10.3847/1538-4365/acf840","url":null,"abstract":"Abstract Photoionization cross sections and rate coefficients have been calculated for all bound vibrational levels of the 1s σ g state of <?CDATA ${{rm{H}}}_{2}^{+}$?> <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" overflow=\"scroll\"> <mml:msubsup> <mml:mrow> <mml:mi mathvariant=\"normal\">H</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>2</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> </mml:mrow> </mml:msubsup> </mml:math> , HD + , and <?CDATA ${{rm{D}}}_{2}^{+}$?> <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" overflow=\"scroll\"> <mml:msubsup> <mml:mrow> <mml:mi mathvariant=\"normal\">D</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>2</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> </mml:mrow> </mml:msubsup> </mml:math> . The Born–Oppenheimer approximation is employed in our calculation of vibrationally resolved photoionization cross sections. Vibrationally resolved and local thermal equilibrium photoionization rate coefficients are presented for photon temperatures less than 50,000 K and are found to be several orders of magnitude larger than previous results in the literature. Analytic fits for the vibrationally resolved and local thermal equilibrium photoionization rate coefficients are provided. Near-threshold oscillations in the vibrationally resolved photoionization are observed. A benchmark set of photoionization cross sections are presented. Fixed-nuclei photoionization cross sections are calculated using two-center true continuum wave functions and are verified by comparison with previous calculations and are found to be in excellent agreement in all cases. Data files for our set of benchmark cross sections, rate coefficients, and fitting parameters for <?CDATA ${{rm{H}}}_{2}^{+}$?> <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" overflow=\"scroll\"> <mml:msubsup> <mml:mrow> <mml:mi mathvariant=\"normal\">H</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>2</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> </mml:mrow> </mml:msubsup> </mml:math> , HD + , and <?CDATA ${{rm{D}}}_{2}^{+}$?> <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" overflow=\"scroll\"> <mml:msubsup> <mml:mrow> <mml:mi mathvariant=\"normal\">D</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>2</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> </mml:mrow> </mml:msubsup> </mml:math> are available on Zenodo under an open-source Creative Commons Attribution license at doi: 10.5281/zenodo.8304061 .","PeriodicalId":8588,"journal":{"name":"Astrophysical Journal Supplement Series","volume":"9 6","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-11-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135220826","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 : 2023-10-31DOI: 10.3847/1538-4365/acf6bf
Pedro H Bernardinelli, Gary M Bernstein, Nicholas Jindal, T.M.C Abbott, M Aguena, F Andrade-Oliveira, J Annis, D Bacon, E Bertin, D Brooks, D.L Burke, A Carnero Rosell, M Carrasco Kind, J Carretero, L.N da Costa, M.E.S Pereira, T.M Davis, S Desai, H.T Diehl, P Doel, S Everett, I Ferrero, D Friedel, J Frieman, J García-Bellido, G Giannini, D Gruen, K Herner, S.R Hinton, D.L Hollowood, K Honscheid, D.J James, K Kuehn, J Mena-Fernández, F Menanteau, R Miquel, R.L.C Ogando, A Pieres, A.A Plazas Malagón, M Raveri, E Sanchez, I Sevilla-Noarbe, M Smith, E Suchyta, G Tarle, C To, A.R Walker, P Wiseman, Y Zhang
We report the methods of and initial scientific inferences from the extraction of precision photometric information for the $>800$ trans-Neptunian objects (TNOs) discovered in the images of the Dark Energy Survey (DES). Scene-modelling photometry is used to obtain shot-noise-limited flux measures for each exposure of each TNO, with background sources subtracted. Comparison of double-source fits to the pixel data with single-source fits are used to identify and characterize two binary TNO systems. A Markov Chain Monte Carlo method samples the joint likelihood of the intrinsic colors of each source as well as the amplitude of its flux variation, given the time series of multiband flux measurements and their uncertainties. A catalog of these colors and light curve amplitudes $A$ is included with this publication. We show how to assign a likelihood to the distribution $q(A)$ of light curve amplitudes in any subpopulation. Using this method, we find decisive evidence (i.e. evidence ratio $<0.01$) that cold classical (CC) TNOs with absolute magnitude $6
{"title":"Photometry of Outer Solar System Objects from the Dark Energy Survey. I. Photometric Methods, Light-curve Distributions, and Trans-Neptunian Binaries","authors":"Pedro H Bernardinelli, Gary M Bernstein, Nicholas Jindal, T.M.C Abbott, M Aguena, F Andrade-Oliveira, J Annis, D Bacon, E Bertin, D Brooks, D.L Burke, A Carnero Rosell, M Carrasco Kind, J Carretero, L.N da Costa, M.E.S Pereira, T.M Davis, S Desai, H.T Diehl, P Doel, S Everett, I Ferrero, D Friedel, J Frieman, J García-Bellido, G Giannini, D Gruen, K Herner, S.R Hinton, D.L Hollowood, K Honscheid, D.J James, K Kuehn, J Mena-Fernández, F Menanteau, R Miquel, R.L.C Ogando, A Pieres, A.A Plazas Malagón, M Raveri, E Sanchez, I Sevilla-Noarbe, M Smith, E Suchyta, G Tarle, C To, A.R Walker, P Wiseman, Y Zhang","doi":"10.3847/1538-4365/acf6bf","DOIUrl":"https://doi.org/10.3847/1538-4365/acf6bf","url":null,"abstract":"We report the methods of and initial scientific inferences from the extraction of precision photometric information for the $>800$ trans-Neptunian objects (TNOs) discovered in the images of the Dark Energy Survey (DES). Scene-modelling photometry is used to obtain shot-noise-limited flux measures for each exposure of each TNO, with background sources subtracted. Comparison of double-source fits to the pixel data with single-source fits are used to identify and characterize two binary TNO systems. A Markov Chain Monte Carlo method samples the joint likelihood of the intrinsic colors of each source as well as the amplitude of its flux variation, given the time series of multiband flux measurements and their uncertainties. A catalog of these colors and light curve amplitudes $A$ is included with this publication. We show how to assign a likelihood to the distribution $q(A)$ of light curve amplitudes in any subpopulation. Using this method, we find decisive evidence (i.e. evidence ratio $<0.01$) that cold classical (CC) TNOs with absolute magnitude $6<H_r<8.2$ are more variable than the hot classical (HC) population of the same $H_r$, reinforcing theories that the former form in situ and the latter arise from a different physical population. Resonant and scattering TNOs in this $H_r$ range have variability consistent with either the HC's or CC's. DES TNOs with $H_r<6$ are seen to be decisively less variable than higher-$H_r$ members of any dynamical group, as expected. More surprising is that detached TNOs are decisively less variable than scattering TNOs, which requires them to have distinct source regions or some subsequent differential processing.","PeriodicalId":8588,"journal":{"name":"Astrophysical Journal Supplement Series","volume":"2023 8","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"135765689","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 : 2023-10-27DOI: 10.3847/1538-4365/acf566
Chen-Ran 宸然 Hu 胡, Yong-Feng 永锋 Huang 黄
Abstract Nearly 700 fast radio burst (FRB) sources have been detected so far, of which 29 are found to burst out repeatedly. Although a firm connection between at least some FRBs and magnetars has been established, the trigger mechanism and radiation process in these enigmatic phenomena are still highly controversial. In this study, we build a sample of 16 repeating FRBs from which at least five bursts have been detected, including the most active four repeaters of FRBs 20121102A, 20180916B, 20190520B, and 20201124A. Various key parameters of their bursts are collected from the literature, which include the arrival time, pulse width, dispersion measure (DM), Faraday rotation measure (RM), bandwidth, waiting time, peak flux, and fluence. The distribution and time evolution of these parameters are investigated. Potential correlations between various parameter pairs are also extensively explored. The behaviors of different repeaters are then compared. It is found that the DM of FRB 20121102A seems to increase continuously on a long timescale. While the DM of most repeaters varies in a narrow range of ±3 cm −3 pc, FRB 20190520B is found to have a large variation range of ±12 cm −3 pc. The RM evolves with time in a much more chaotic behavior in different repeaters. A linear correlation is found between the absolute mean RM and DM Host , which may provide a method to estimate the redshift of FRBs. Generally, the waiting time shows a similar bimodal distribution for the active repeating sources. The implications of these features to the underlying physics are discussed.
{"title":"A Comprehensive Analysis of Repeating Fast Radio Bursts","authors":"Chen-Ran 宸然 Hu 胡, Yong-Feng 永锋 Huang 黄","doi":"10.3847/1538-4365/acf566","DOIUrl":"https://doi.org/10.3847/1538-4365/acf566","url":null,"abstract":"Abstract Nearly 700 fast radio burst (FRB) sources have been detected so far, of which 29 are found to burst out repeatedly. Although a firm connection between at least some FRBs and magnetars has been established, the trigger mechanism and radiation process in these enigmatic phenomena are still highly controversial. In this study, we build a sample of 16 repeating FRBs from which at least five bursts have been detected, including the most active four repeaters of FRBs 20121102A, 20180916B, 20190520B, and 20201124A. Various key parameters of their bursts are collected from the literature, which include the arrival time, pulse width, dispersion measure (DM), Faraday rotation measure (RM), bandwidth, waiting time, peak flux, and fluence. The distribution and time evolution of these parameters are investigated. Potential correlations between various parameter pairs are also extensively explored. The behaviors of different repeaters are then compared. It is found that the DM of FRB 20121102A seems to increase continuously on a long timescale. While the DM of most repeaters varies in a narrow range of ±3 cm −3 pc, FRB 20190520B is found to have a large variation range of ±12 cm −3 pc. The RM evolves with time in a much more chaotic behavior in different repeaters. A linear correlation is found between the absolute mean RM and DM Host , which may provide a method to estimate the redshift of FRBs. Generally, the waiting time shows a similar bimodal distribution for the active repeating sources. The implications of these features to the underlying physics are discussed.","PeriodicalId":8588,"journal":{"name":"Astrophysical Journal Supplement Series","volume":"64 3","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136235993","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 : 2023-10-27DOI: 10.3847/1538-4365/acf4f9
Prantik Nandi, Arka Chatterjee, Arghajit Jana, Sandip K. Chakrabarti, Sachindra Naik, Samar Safi-Harb, Hsiang-Kuang Chang, Jeremy Heyl
Abstract We analyze a sample of 21 “bare” Seyfert 1 active galactic nuclei, a subclass of Seyfert 1 galaxies, with intrinsic absorption N H ∼ 10 20 cm −2 , in the local Universe ( z < 0.2) using XMM-Newton and Swift/XRT observations. The luminosities of the primary continuum, the X-ray emission in the 3–10 keV energy range, and the soft excess—the excess emission that appears above the low-energy extrapolation of the power-law fit of 3–10 keV X-ray spectra—are calculated. Our spectral analysis reveals that the long-term intrinsic luminosities of the soft excess and the primary continuum are tightly correlated (LPC∝LSE1.1±0.04) . We also found that the luminosities are correlated for each source. This result suggests that both the primary continuum and soft excess emissions exhibit a dependency on the accretion rate in a similar way.
{"title":"Survey of Bare Active Galactic Nuclei in the Local Universe (z < 0.2). I. On the Origin of Soft Excess","authors":"Prantik Nandi, Arka Chatterjee, Arghajit Jana, Sandip K. Chakrabarti, Sachindra Naik, Samar Safi-Harb, Hsiang-Kuang Chang, Jeremy Heyl","doi":"10.3847/1538-4365/acf4f9","DOIUrl":"https://doi.org/10.3847/1538-4365/acf4f9","url":null,"abstract":"Abstract We analyze a sample of 21 “bare” Seyfert 1 active galactic nuclei, a subclass of Seyfert 1 galaxies, with intrinsic absorption N H ∼ 10 20 cm −2 , in the local Universe ( z < 0.2) using XMM-Newton and Swift/XRT observations. The luminosities of the primary continuum, the X-ray emission in the 3–10 keV energy range, and the soft excess—the excess emission that appears above the low-energy extrapolation of the power-law fit of 3–10 keV X-ray spectra—are calculated. Our spectral analysis reveals that the long-term intrinsic luminosities of the soft excess and the primary continuum are tightly correlated <?CDATA $({L}_{mathrm{PC}}propto {L}_{mathrm{SE}}^{1.1pm 0.04})$?> <mml:math xmlns:mml=\"http://www.w3.org/1998/Math/MathML\" overflow=\"scroll\"> <mml:mo stretchy=\"false\">(</mml:mo> <mml:msub> <mml:mrow> <mml:mi>L</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>PC</mml:mi> </mml:mrow> </mml:msub> <mml:mo>∝</mml:mo> <mml:msubsup> <mml:mrow> <mml:mi>L</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>SE</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>1.1</mml:mn> <mml:mo>±</mml:mo> <mml:mn>0.04</mml:mn> </mml:mrow> </mml:msubsup> <mml:mo stretchy=\"false\">)</mml:mo> </mml:math> . We also found that the luminosities are correlated for each source. This result suggests that both the primary continuum and soft excess emissions exhibit a dependency on the accretion rate in a similar way.","PeriodicalId":8588,"journal":{"name":"Astrophysical Journal Supplement Series","volume":"1 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2023-10-27","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"136317007","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}
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