Pub Date : 2024-05-13DOI: 10.3847/1538-4365/ad39c5
Christian I. Eze and Gerald Handler
The combined strength of asteroseismology and empirical stellar basic parameter determinations for in-depth asteroseismic analysis of massive pulsators in eclipsing binaries shows great potential for treating the challenging and mysterious discrepancies between observations and models of stellar structure and the evolution of massive stars. This paper compiles a comprehensive list of massive pulsators in eclipsing binary systems observed with TESS. The TESS light curves and discrete Fourier transforms of a sample of 8055 stars of spectral type B0–B3 were examined for eclipses and stellar pulsations, and the ephemerides of the resulting subsample of massive pulsators in eclipsing binaries were computed. This subsample was also crossmatched with existing catalogs of massive pulsators. Until now, fewer than 30 β Cephei pulsators in eclipsing binaries have been reported in the literature. Here we announce a total of 78 pulsators of the β Cephei type in eclipsing binaries, 59 of which are new discoveries. Forty-three are recognized as definite, and 35 are candidate pulsators. Our sample of pulsating massive stars in eclipsing binaries allows for future asteroseismic modeling to better understand the internal mixing profile and to resolve the mass discrepancy in massive stars. We have already started follow-up work on some of the most interesting candidates.
{"title":"β Cephei Pulsators in Eclipsing Binaries Observed with TESS","authors":"Christian I. Eze and Gerald Handler","doi":"10.3847/1538-4365/ad39c5","DOIUrl":"https://doi.org/10.3847/1538-4365/ad39c5","url":null,"abstract":"The combined strength of asteroseismology and empirical stellar basic parameter determinations for in-depth asteroseismic analysis of massive pulsators in eclipsing binaries shows great potential for treating the challenging and mysterious discrepancies between observations and models of stellar structure and the evolution of massive stars. This paper compiles a comprehensive list of massive pulsators in eclipsing binary systems observed with TESS. The TESS light curves and discrete Fourier transforms of a sample of 8055 stars of spectral type B0–B3 were examined for eclipses and stellar pulsations, and the ephemerides of the resulting subsample of massive pulsators in eclipsing binaries were computed. This subsample was also crossmatched with existing catalogs of massive pulsators. Until now, fewer than 30 β Cephei pulsators in eclipsing binaries have been reported in the literature. Here we announce a total of 78 pulsators of the β Cephei type in eclipsing binaries, 59 of which are new discoveries. Forty-three are recognized as definite, and 35 are candidate pulsators. Our sample of pulsating massive stars in eclipsing binaries allows for future asteroseismic modeling to better understand the internal mixing profile and to resolve the mass discrepancy in massive stars. We have already started follow-up work on some of the most interesting candidates.","PeriodicalId":22368,"journal":{"name":"The Astrophysical Journal Supplement Series","volume":"79 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140925460","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 : 2024-05-10DOI: 10.3847/1538-4365/ad3de7
ShuWang Chang, Bing Wang, Guang Lu, YuPeng Shen, Yu Bai, ZiQian Shang, Lei Zhang, Zhao Wu, YanRui Su, Yao Chen, FaBao Yan
Radio observation is important for understanding coronal mass ejections (CMEs), coronal shock waves, and high-energy electron acceleration. Here, we developed a new Chashan broadband solar radio spectrometer at a meter wavelength for observing the (super)fine structure of the solar radio burst spectrum. In the signal-receiving unit, we adopt an antenna system consisting of a 12 m large-aperture parabolic reflector and dual-line polarized logarithmic periodic feed source, as well as a high-precision Sun-tracking turntable system, all of which ensure the high-precision acquisition of solar radiation signals. For the digital receiver, we use a high-speed analog-to-digital converter with a sampling rate of 1.25 GSPS to directly sample the signal amplified and filtered by the analog receiver, simplifying the structure of the analog receiver, and design a 16k-point fast Fourier transform algorithm in the field programmable gate array to perform time–frequency transformation on the sampled signals. The default frequency and temporal resolution of the system are 76.294 kHz and 0.839 ms (up to 0.21 ms), respectively. The noise coefficient of the system is less than 1 dB, the dynamic range is more than 60 dB, and the sensitivity is as high as 1 sfu. We have observed a large number of radio bursts, including type I radio storms, hundreds of type III, ∼20 type II, and ∼15 type IV bursts in the past year. These high-quality data are useful in the further study of CMEs and associated particle acceleration and the origins of solar radio bursts.
射电观测对于了解日冕物质抛射（CME）、日冕冲击波和高能电子加速非常重要。在这里，我们开发了一种新的米波长茶山宽带太阳射电频谱仪，用于观测太阳射电爆发频谱的（超）精细结构。在信号接收单元，我们采用了由 12 米大口径抛物面反射镜和双线极化对数周期馈源组成的天线系统，以及高精度太阳跟踪转台系统，这些都确保了太阳辐射信号的高精度采集。在数字接收机方面，我们采用采样率为 1.25 GSPS 的高速模数转换器，直接对模拟接收机放大和滤波后的信号进行采样，简化了模拟接收机的结构，并在现场可编程门阵列中设计了 16k 点快速傅里叶变换算法，对采样后的信号进行时频变换。系统的默认频率和时间分辨率分别为 76.294 kHz 和 0.839 ms（最高 0.21 ms）。系统的噪声系数小于 1 dB，动态范围超过 60 dB，灵敏度高达 1 sfu。在过去的一年中，我们观测到了大量的射电暴，包括 I 型射电暴、数百个 III 型射电暴、∼20 个 II 型射电暴和∼15 个 IV 型射电暴。这些高质量的数据有助于进一步研究CME和相关的粒子加速以及太阳射电暴的起源。
{"title":"Development of a 90–600 MHz Meter-wave Solar Radio Spectrometer","authors":"ShuWang Chang, Bing Wang, Guang Lu, YuPeng Shen, Yu Bai, ZiQian Shang, Lei Zhang, Zhao Wu, YanRui Su, Yao Chen, FaBao Yan","doi":"10.3847/1538-4365/ad3de7","DOIUrl":"https://doi.org/10.3847/1538-4365/ad3de7","url":null,"abstract":"Radio observation is important for understanding coronal mass ejections (CMEs), coronal shock waves, and high-energy electron acceleration. Here, we developed a new Chashan broadband solar radio spectrometer at a meter wavelength for observing the (super)fine structure of the solar radio burst spectrum. In the signal-receiving unit, we adopt an antenna system consisting of a 12 m large-aperture parabolic reflector and dual-line polarized logarithmic periodic feed source, as well as a high-precision Sun-tracking turntable system, all of which ensure the high-precision acquisition of solar radiation signals. For the digital receiver, we use a high-speed analog-to-digital converter with a sampling rate of 1.25 GSPS to directly sample the signal amplified and filtered by the analog receiver, simplifying the structure of the analog receiver, and design a 16k-point fast Fourier transform algorithm in the field programmable gate array to perform time–frequency transformation on the sampled signals. The default frequency and temporal resolution of the system are 76.294 kHz and 0.839 ms (up to 0.21 ms), respectively. The noise coefficient of the system is less than 1 dB, the dynamic range is more than 60 dB, and the sensitivity is as high as 1 sfu. We have observed a large number of radio bursts, including type I radio storms, hundreds of type III, ∼20 type II, and ∼15 type IV bursts in the past year. These high-quality data are useful in the further study of CMEs and associated particle acceleration and the origins of solar radio bursts.","PeriodicalId":22368,"journal":{"name":"The Astrophysical Journal Supplement Series","volume":"26 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140925599","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 : 2024-05-10DOI: 10.3847/1538-4365/ad3641
Deokkeun An, Timothy C. Beers, Anirudh Chiti
Using a grid of empirically calibrated synthetic spectra developed in our previous study, we construct an all-sky 3D extinction map from the large collection of low-resolution XP spectra in Gaia DR3. Along each line of sight, with an area ranging from 0.2 to 13.4 deg2, we determine both the reddening and metallicity of main-sequence stars and model the foreground extinction up to approximately 3 kpc from the Sun. Furthermore, we explore variations in the total-to-selective extinction ratio in our parameter search and identify its mean systematic change across diverse cloud environments in both hemispheres. In regions outside the densest parts of the clouds, our reddening estimates are validated through comparisons with previous reddening maps. However, a notable discrepancy arises in comparison to other independent work based on XP spectra, which can be attributed to systematic offsets in their metallicity estimates. On the other hand, our metallicity scale exhibits reasonable agreement with the high-resolution spectroscopic abundance scale. We also assess the accuracy of the XP spectra by applying our calibrated models, and we confirm an increasing trend of flux overestimation at shorter wavelengths below 400 nm.
利用我们之前研究中开发的经验校准合成光谱网格，我们从 Gaia DR3 中的大量低分辨率 XP 光谱集合中构建了一张全天空三维消光图。沿着每条视线（面积从 0.2 到 13.4 deg2 不等），我们确定了主序星的红度和金属度，并建立了距离太阳约 3 kpc 的前景消光模型。此外，我们还探索了参数搜索中总消光与选择性消光比的变化，并确定了其在两个半球不同云环境中的平均系统变化。在云的最密集部分以外的区域，我们的红化估计值通过与以前的红化图的比较得到了验证。不过，与其他基于 XP 光谱的独立研究相比，我们的结果存在明显差异，这可能是由于他们在估计金属度时出现了系统偏差。另一方面，我们的金属性标度与高分辨率光谱丰度标度呈现出合理的一致性。我们还应用校准模型评估了 XP 光谱的准确性，并证实在 400 nm 以下的较短波长上，通量高估呈上升趋势。
{"title":"A Blueprint for the Milky Way’s Stellar Populations. V. 3D Local Dust Extinction","authors":"Deokkeun An, Timothy C. Beers, Anirudh Chiti","doi":"10.3847/1538-4365/ad3641","DOIUrl":"https://doi.org/10.3847/1538-4365/ad3641","url":null,"abstract":"Using a grid of empirically calibrated synthetic spectra developed in our previous study, we construct an all-sky 3D extinction map from the large collection of low-resolution XP spectra in Gaia DR3. Along each line of sight, with an area ranging from 0.2 to 13.4 deg<sup>2</sup>, we determine both the reddening and metallicity of main-sequence stars and model the foreground extinction up to approximately 3 kpc from the Sun. Furthermore, we explore variations in the total-to-selective extinction ratio in our parameter search and identify its mean systematic change across diverse cloud environments in both hemispheres. In regions outside the densest parts of the clouds, our reddening estimates are validated through comparisons with previous reddening maps. However, a notable discrepancy arises in comparison to other independent work based on XP spectra, which can be attributed to systematic offsets in their metallicity estimates. On the other hand, our metallicity scale exhibits reasonable agreement with the high-resolution spectroscopic abundance scale. We also assess the accuracy of the XP spectra by applying our calibrated models, and we confirm an increasing trend of flux overestimation at shorter wavelengths below 400 nm.","PeriodicalId":22368,"journal":{"name":"The Astrophysical Journal Supplement Series","volume":"76 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140925428","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 : 2024-05-09DOI: 10.3847/1538-4365/ad390d
Wooseok Kang, Ho Seong Hwang, Hyunmi Song, Changbom Park, Narae Hwang and Byeong-Gon Park
We study the global kinematics of the Perseus galaxy cluster (A426) at redshift z = 0.017 using a large sample of galaxies from our new MMT/Hectospec spectroscopic observation for this cluster. The sample includes 1447 galaxies with measured redshifts within 60′ from the cluster center (1148 from this MMT/Hectospec program and 299 from the literature). The resulting spectroscopic completeness is 67% at r-band apparent magnitude rPetro,0 ≤ 18.0 within 60′ from the cluster center. To identify cluster member galaxies in this sample, we develop a new open-source Python package, CausticSNUpy. This code implements the algorithm of the caustic technique and yields 418 member galaxies within 60′ of the cluster. We study the cluster using this sample of member galaxies. The cluster shows no significant signal of global rotation. A statistical test shows that the cluster does not have a noticeable substructure within 30′. We find two central regions where the X-ray-emitting intracluster medium and galaxies show significant velocity differences (>7σ). On a large scale, however, the overall morphology and kinematics between the intracluster medium and galaxies agree well. Our results suggest that the Perseus cluster is a relaxed system and has not experienced a recent merger.
{"title":"A Deep Redshift Survey of the Perseus Cluster (A426): Spatial Distribution and Kinematics of Galaxies","authors":"Wooseok Kang, Ho Seong Hwang, Hyunmi Song, Changbom Park, Narae Hwang and Byeong-Gon Park","doi":"10.3847/1538-4365/ad390d","DOIUrl":"https://doi.org/10.3847/1538-4365/ad390d","url":null,"abstract":"We study the global kinematics of the Perseus galaxy cluster (A426) at redshift z = 0.017 using a large sample of galaxies from our new MMT/Hectospec spectroscopic observation for this cluster. The sample includes 1447 galaxies with measured redshifts within 60′ from the cluster center (1148 from this MMT/Hectospec program and 299 from the literature). The resulting spectroscopic completeness is 67% at r-band apparent magnitude rPetro,0 ≤ 18.0 within 60′ from the cluster center. To identify cluster member galaxies in this sample, we develop a new open-source Python package, CausticSNUpy. This code implements the algorithm of the caustic technique and yields 418 member galaxies within 60′ of the cluster. We study the cluster using this sample of member galaxies. The cluster shows no significant signal of global rotation. A statistical test shows that the cluster does not have a noticeable substructure within 30′. We find two central regions where the X-ray-emitting intracluster medium and galaxies show significant velocity differences (>7σ). On a large scale, however, the overall morphology and kinematics between the intracluster medium and galaxies agree well. Our results suggest that the Perseus cluster is a relaxed system and has not experienced a recent merger.","PeriodicalId":22368,"journal":{"name":"The Astrophysical Journal Supplement Series","volume":"39 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140925458","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 : 2024-05-09DOI: 10.3847/1538-4365/ad3948
Rosalia O’Brien, Rolf A. Jansen, Norman A. Grogin, Seth H. Cohen, Brent M. Smith, Ross M. Silver, W. P. Maksym, Rogier A. Windhorst, Timothy Carleton, Anton M. Koekemoer, Nimish P. Hathi, Christopher N. A. Willmer, Brenda L. Frye, M. Alpaslan, M. L. N. Ashby, T. A. Ashcraft, S. Bonoli, W. Brisken, N. Cappelluti, F. Civano, C. J. Conselice, V. S. Dhillon, S. P. Driver, K. J. Duncan, R. Dupke, M. Elvis, G. G. Fazio, S. L. Finkelstein, H. B. Gim, A. Griffiths, H. B. Hammel, M. Hyun, M. Im, V. R. Jones, D. Kim, B. Ladjelate, R. L. Larson, S. Malhotra, M. A. Marshall, S. N. Milam, J. D. R. Pierel, J. E. Rhoads, S. A. Rodney, H. J. A. Röttgering, M. J. Rutkowski, R. E. Ryan, M. J. Ward, C. W. White, R. J. van Weeren, X. Zhao, J. Summers, J. C. J. D’Silva, R. Ortiz, A. S. G. Robotham, D. Coe, M. Nonino, N. Pirzkal, H. Yan, T. Acharya
The James Webb Space Telescope (JWST) North Ecliptic Pole (NEP) Time-domain Field (TDF) is a >14′ diameter field optimized for multiwavelength time-domain science with JWST. It has been observed across the electromagnetic spectrum both from the ground and from space, including with the Hubble Space Telescope (HST). As part of HST observations over three cycles (the “TREASUREHUNT” program), deep images were obtained with the Wide Field Camera on the Advanced Camera for Surveys in F435W and F606W that cover almost the entire JWST NEP TDF. Many of the individual pointings of these programs partially overlap, allowing an initial assessment of the potential of this field for time-domain science with HST and JWST. The cumulative area of overlapping pointings is ∼88 arcmin2, with time intervals between individual epochs that range between 1 day and 4+ yr. To a depth of mAB ≃ 29.5 mag (F606W), we present the discovery of 12 transients and 190 variable candidates. For the variable candidates, we demonstrate that Gaussian statistics are applicable and estimate that ∼80 are false positives. The majority of the transients will be supernovae, although at least two are likely quasars. Most variable candidates are active galactic nuclei (AGNs), where we find 0.42% of the general z ≲ 6 field galaxy population to vary at the ∼3σ level. Based on a 5 yr time frame, this translates into a random supernova areal density of up to ∼0.07 transients arcmin−2 (∼245 deg−2) per epoch and a variable AGN areal density of ∼1.25 variables arcmin−2 (∼4500 deg−2) to these depths.
{"title":"TREASUREHUNT: Transients and Variability Discovered with HST in the JWST North Ecliptic Pole Time-domain Field","authors":"Rosalia O’Brien, Rolf A. Jansen, Norman A. Grogin, Seth H. Cohen, Brent M. Smith, Ross M. Silver, W. P. Maksym, Rogier A. Windhorst, Timothy Carleton, Anton M. Koekemoer, Nimish P. Hathi, Christopher N. A. Willmer, Brenda L. Frye, M. Alpaslan, M. L. N. Ashby, T. A. Ashcraft, S. Bonoli, W. Brisken, N. Cappelluti, F. Civano, C. J. Conselice, V. S. Dhillon, S. P. Driver, K. J. Duncan, R. Dupke, M. Elvis, G. G. Fazio, S. L. Finkelstein, H. B. Gim, A. Griffiths, H. B. Hammel, M. Hyun, M. Im, V. R. Jones, D. Kim, B. Ladjelate, R. L. Larson, S. Malhotra, M. A. Marshall, S. N. Milam, J. D. R. Pierel, J. E. Rhoads, S. A. Rodney, H. J. A. Röttgering, M. J. Rutkowski, R. E. Ryan, M. J. Ward, C. W. White, R. J. van Weeren, X. Zhao, J. Summers, J. C. J. D’Silva, R. Ortiz, A. S. G. Robotham, D. Coe, M. Nonino, N. Pirzkal, H. Yan, T. Acharya","doi":"10.3847/1538-4365/ad3948","DOIUrl":"https://doi.org/10.3847/1538-4365/ad3948","url":null,"abstract":"The James Webb Space Telescope (JWST) North Ecliptic Pole (NEP) Time-domain Field (TDF) is a >14′ diameter field optimized for multiwavelength time-domain science with JWST. It has been observed across the electromagnetic spectrum both from the ground and from space, including with the Hubble Space Telescope (HST). As part of HST observations over three cycles (the “TREASUREHUNT” program), deep images were obtained with the Wide Field Camera on the Advanced Camera for Surveys in F435W and F606W that cover almost the entire JWST NEP TDF. Many of the individual pointings of these programs partially overlap, allowing an initial assessment of the potential of this field for time-domain science with HST and JWST. The cumulative area of overlapping pointings is ∼88 arcmin<sup>2</sup>, with time intervals between individual epochs that range between 1 day and 4+ yr. To a depth of <italic toggle=\"yes\">m</italic>\u0000<sub>AB</sub> ≃ 29.5 mag (F606W), we present the discovery of 12 transients and 190 variable candidates. For the variable candidates, we demonstrate that Gaussian statistics are applicable and estimate that ∼80 are false positives. The majority of the transients will be supernovae, although at least two are likely quasars. Most variable candidates are active galactic nuclei (AGNs), where we find 0.42% of the general <italic toggle=\"yes\">z</italic> ≲ 6 field galaxy population to vary at the ∼3<italic toggle=\"yes\">σ</italic> level. Based on a 5 yr time frame, this translates into a random supernova areal density of up to ∼0.07 transients arcmin<sup>−2</sup> (∼245 deg<sup>−2</sup>) per epoch and a variable AGN areal density of ∼1.25 variables arcmin<sup>−2</sup> (∼4500 deg<sup>−2</sup>) to these depths.","PeriodicalId":22368,"journal":{"name":"The Astrophysical Journal Supplement Series","volume":"67 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140925343","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 : 2024-05-08DOI: 10.3847/1538-4365/ad37bc
Jiahui Shan, Huapeng Zhang, Lei Lu, Yan Zhang, Li Feng, Yunyi Ge, Jianchao Xue, Shuting Li
Coronal mass ejections (CMEs) are major drivers of geomagnetic storms, which may cause severe space weather effects. Automating the detection, tracking, and three-dimensional (3D) reconstruction of CMEs is important for operational predictions of CME arrivals. The COR1 coronagraphs on board the Solar Terrestrial Relations Observatory spacecraft have facilitated extensive polarization observations, which are very suitable for the establishment of a 3D CME system. We have developed such a 3D system comprising four modules: classification, segmentation, tracking, and 3D reconstructions. We generalize our previously pretrained classification model to classify COR1 coronagraph images. Subsequently, as there are no publicly available CME segmentation data sets, we manually annotate the structural regions of CMEs using Large Angle and Spectrometric Coronagraph C2 observations. Leveraging transformer-based models, we achieve state-of-the-art results in CME segmentation. Furthermore, we improve the tracking algorithm to solve the difficult separation task of multiple CMEs. In the final module, tracking results, combined with the polarization ratio technique, are used to develop the first single-view 3D CME catalog without requiring manual mask annotation. Our method provides higher precision in automatic 2D CME catalog and more reliable physical parameters of CMEs, including 3D propagation direction and speed. The aforementioned 3D CME system can be applied to any coronagraph data with the capability of polarization measurements.
{"title":"CAMEL. II. A 3D Coronal Mass Ejection Catalog Based on Coronal Mass Ejection Automatic Detection with Deep Learning","authors":"Jiahui Shan, Huapeng Zhang, Lei Lu, Yan Zhang, Li Feng, Yunyi Ge, Jianchao Xue, Shuting Li","doi":"10.3847/1538-4365/ad37bc","DOIUrl":"https://doi.org/10.3847/1538-4365/ad37bc","url":null,"abstract":"Coronal mass ejections (CMEs) are major drivers of geomagnetic storms, which may cause severe space weather effects. Automating the detection, tracking, and three-dimensional (3D) reconstruction of CMEs is important for operational predictions of CME arrivals. The COR1 coronagraphs on board the Solar Terrestrial Relations Observatory spacecraft have facilitated extensive polarization observations, which are very suitable for the establishment of a 3D CME system. We have developed such a 3D system comprising four modules: classification, segmentation, tracking, and 3D reconstructions. We generalize our previously pretrained classification model to classify COR1 coronagraph images. Subsequently, as there are no publicly available CME segmentation data sets, we manually annotate the structural regions of CMEs using Large Angle and Spectrometric Coronagraph C2 observations. Leveraging transformer-based models, we achieve state-of-the-art results in CME segmentation. Furthermore, we improve the tracking algorithm to solve the difficult separation task of multiple CMEs. In the final module, tracking results, combined with the polarization ratio technique, are used to develop the first single-view 3D CME catalog without requiring manual mask annotation. Our method provides higher precision in automatic 2D CME catalog and more reliable physical parameters of CMEs, including 3D propagation direction and speed. The aforementioned 3D CME system can be applied to any coronagraph data with the capability of polarization measurements.","PeriodicalId":22368,"journal":{"name":"The Astrophysical Journal Supplement Series","volume":"6 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140925418","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 : 2024-05-08DOI: 10.3847/1538-4365/ad3809
Xinchuan Huang, Iouli E. Gordon, Sergey A. Tashkun, David W. Schwenke, Timothy J. Lee
To facilitate atmospheric and spectroscopic studies of carbon disulfide, or CS2, in both planetary and exoplanetary atmospheres, we adopt the “Best Theory + Reliable High-resolution Experiment” algorithm to generate semiempirical IR line lists for the 20 most abundant CS2 isotopologues, denoted as Ames-296K. The IR lists are computed using the Ames-1 potential energy surface, refined using the experimental transition set and an ab initio dipole moment surface fitted from CCSD(T)/aug-cc-pV(T/Q/5+d)Z dipoles extrapolated to a one-particle basis set limit. The IR lists cover the range of 0–10,000 cm−1, with an S296K cutoff at 10−31 cm−1/molecule·cm−2 (abundance included). A “natural” IR line list at 296 K includes about 10 million lines of the 20 isotopologues, with their intensities scaled by the corresponding abundances. The zero-point energy, partition functions, and abundances are reported for each isotopologue. The energy levels in the global effective Hamiltonian model for 12C32S2 are adopted to improve the line position accuracy. This new IR list for the main isotopologue is denoted as A+I.296K. Reliable HITRAN2020 line positions are also utilized to improve the accuracy of the 32S12C34S, 32S12C33S, and 32S13C32S isotopologue line lists. The final composite line list is validated against Pacific Northwest National Laboratory experimental cross sections, showing excellent agreement. The agreement supports the quality of the composite line list and the power of synergy between experiment and theory. The new data are proposed for use in updating and expanding the CS2 data in HITRAN and other high-resolution IR databases. Supplementary files are available in Zenodo and AHED.
{"title":"Accurate Infrared Line Lists for 20 Isotopologues of CS2 at Room Temperature","authors":"Xinchuan Huang, Iouli E. Gordon, Sergey A. Tashkun, David W. Schwenke, Timothy J. Lee","doi":"10.3847/1538-4365/ad3809","DOIUrl":"https://doi.org/10.3847/1538-4365/ad3809","url":null,"abstract":"To facilitate atmospheric and spectroscopic studies of carbon disulfide, or CS<sub>2</sub>, in both planetary and exoplanetary atmospheres, we adopt the “Best Theory + Reliable High-resolution Experiment” algorithm to generate semiempirical IR line lists for the 20 most abundant CS<sub>2</sub> isotopologues, denoted as Ames-296K. The IR lists are computed using the Ames-1 potential energy surface, refined using the experimental transition set and an ab initio dipole moment surface fitted from CCSD(T)/aug-cc-pV(T/Q/5+d)Z dipoles extrapolated to a one-particle basis set limit. The IR lists cover the range of 0–10,000 cm<sup>−1</sup>, with an <italic toggle=\"yes\">S</italic>\u0000<sub>296K</sub> cutoff at 10<sup>−31</sup> cm<sup>−1</sup>/molecule·cm<sup>−2</sup> (abundance included). A “natural” IR line list at 296 K includes about 10 million lines of the 20 isotopologues, with their intensities scaled by the corresponding abundances. The zero-point energy, partition functions, and abundances are reported for each isotopologue. The energy levels in the global effective Hamiltonian model for <sup>12</sup>C<sup>32</sup>S<sub>2</sub> are adopted to improve the line position accuracy. This new IR list for the main isotopologue is denoted as A+I.296K. Reliable HITRAN2020 line positions are also utilized to improve the accuracy of the <sup>32</sup>S<sup>12</sup>C<sup>34</sup>S, <sup>32</sup>S<sup>12</sup>C<sup>33</sup>S, and <sup>32</sup>S<sup>13</sup>C<sup>32</sup>S isotopologue line lists. The final composite line list is validated against Pacific Northwest National Laboratory experimental cross sections, showing excellent agreement. The agreement supports the quality of the composite line list and the power of synergy between experiment and theory. The new data are proposed for use in updating and expanding the CS<sub>2</sub> data in HITRAN and other high-resolution IR databases. Supplementary files are available in Zenodo and AHED.","PeriodicalId":22368,"journal":{"name":"The Astrophysical Journal Supplement Series","volume":"60 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140925338","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 : 2024-05-07DOI: 10.3847/1538-4365/ad38b5
Kyung-Won Suh
We explore the characteristics of carbon stars within our Galaxy through a comprehensive analysis of observational data spanning visual and infrared (IR) bands. Leveraging data sets from IRAS, the Infrared Space Observatory, Akari, the Midcourse Space Experiment, the Two Micron All Sky Survey, the Wide-field Infrared Survey Explorer (WISE), Gaia DR3, AAVSO, and the SIMBAD object database, we conduct a detailed comparison between the observational data and theoretical models. To facilitate this comparison, we introduce various IR two-color diagrams (2CDs), IR color–magnitude diagrams (CMDs), and spectral energy distributions (SEDs). We find that the CMDs, which utilize the latest distance and extinction data from Gaia DR3 for a substantial number of carbon stars, are very useful for distinguishing carbon-rich asymptotic giant branch (CAGB) stars from extrinsic carbon stars that are not in the AGB phase. To enhance the accuracy of our analysis, we employ theoretical radiative transfer models for dust shells around CAGB stars. These theoretical dust shell models demonstrate a commendable ability to approximate the observations of CAGB stars across various SEDs, 2CDs, and CMDs. We present the infrared properties of known pulsating variables and explore the infrared variability of the sample stars by analyzing WISE photometric data spanning the last 14 years. Additionally, we present a novel catalog of CAGB stars, offering enhanced reliability and a wealth of additional information.
{"title":"Infrared Properties of Carbon Stars in Our Galaxy","authors":"Kyung-Won Suh","doi":"10.3847/1538-4365/ad38b5","DOIUrl":"https://doi.org/10.3847/1538-4365/ad38b5","url":null,"abstract":"We explore the characteristics of carbon stars within our Galaxy through a comprehensive analysis of observational data spanning visual and infrared (IR) bands. Leveraging data sets from IRAS, the Infrared Space Observatory, Akari, the Midcourse Space Experiment, the Two Micron All Sky Survey, the Wide-field Infrared Survey Explorer (WISE), Gaia DR3, AAVSO, and the SIMBAD object database, we conduct a detailed comparison between the observational data and theoretical models. To facilitate this comparison, we introduce various IR two-color diagrams (2CDs), IR color–magnitude diagrams (CMDs), and spectral energy distributions (SEDs). We find that the CMDs, which utilize the latest distance and extinction data from Gaia DR3 for a substantial number of carbon stars, are very useful for distinguishing carbon-rich asymptotic giant branch (CAGB) stars from extrinsic carbon stars that are not in the AGB phase. To enhance the accuracy of our analysis, we employ theoretical radiative transfer models for dust shells around CAGB stars. These theoretical dust shell models demonstrate a commendable ability to approximate the observations of CAGB stars across various SEDs, 2CDs, and CMDs. We present the infrared properties of known pulsating variables and explore the infrared variability of the sample stars by analyzing WISE photometric data spanning the last 14 years. Additionally, we present a novel catalog of CAGB stars, offering enhanced reliability and a wealth of additional information.","PeriodicalId":22368,"journal":{"name":"The Astrophysical Journal Supplement Series","volume":"39 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140925416","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 : 2024-05-06DOI: 10.3847/1538-4365/ad391d
Lorenzo Roberti, Marco Limongi and Alessandro Chieffi
We present an extension of the set of models published in Limongi & Chieffi (2018) at metallicity 2 times solar, i.e., [Fe/H] = 0.3. The key physical properties of these models at the onset of core collapse are mainly due to the higher mass loss triggered by the higher metallicity: the supersolar metallicity (SSM) models reach core collapse with smaller He- and CO-core masses, while the amount of 12C left by the central He burning is higher. These results are valid for all the rotation velocities. The yields of the neutron-capture nuclei expressed per unit mass of oxygen (i.e., the X/O) are higher in the SSM models than in the SM ones in the nonrotating case, while the opposite occurs in the rotating models. The trend shown by the nonrotating models is the expected one, given the secondary nature of the neutron-capture nucleosynthesis. Vice versa, the counterintuitive trend obtained in the rotating models is the consequence of the higher mass loss present in the SSM models, removes the H-rich envelope faster than in the SM models while the stars are still in central He burning, dumping out the entanglement (activated by the rotation instabilities) and therefore conspicuous primary neutron-capture nucleosynthesis.
我们介绍了Limongi & Chieffi（2018）发表的一组模型在2倍太阳金属性（即[Fe/H] = 0.3）下的扩展。这些模型在内核坍缩开始时的关键物理特性主要是由于较高的金属性引发了较高的质量损失：超太阳金属性（SSM）模型以较小的 He 和 CO 内核质量达到内核坍缩，而中心 He 燃烧留下的 12C 量较高。这些结果适用于所有旋转速度。在非旋转情况下，以单位质量氧（即 X/O）表示的中子俘获核的产率在 SSM 模型中高于 SM 模型，而在旋转模型中则相反。考虑到中子俘获核合成的次级性质，非旋转模型所显示的趋势是意料之中的。反之亦然，旋转模型中出现的反直觉趋势是 SSM 模型中质量损失较大的结果，当恒星仍处于中心氦燃烧时，SSM 模型比 SM 模型更快地移除富含 H 的包层，甩掉纠缠（由旋转不稳定性激活），从而甩掉明显的初级中子捕获核合成。
{"title":"Presupernova Evolution and Explosive Nucleosynthesis of Rotating Massive Stars. II. The Supersolar Models at [Fe/H] = 0.3","authors":"Lorenzo Roberti, Marco Limongi and Alessandro Chieffi","doi":"10.3847/1538-4365/ad391d","DOIUrl":"https://doi.org/10.3847/1538-4365/ad391d","url":null,"abstract":"We present an extension of the set of models published in Limongi & Chieffi (2018) at metallicity 2 times solar, i.e., [Fe/H] = 0.3. The key physical properties of these models at the onset of core collapse are mainly due to the higher mass loss triggered by the higher metallicity: the supersolar metallicity (SSM) models reach core collapse with smaller He- and CO-core masses, while the amount of 12C left by the central He burning is higher. These results are valid for all the rotation velocities. The yields of the neutron-capture nuclei expressed per unit mass of oxygen (i.e., the X/O) are higher in the SSM models than in the SM ones in the nonrotating case, while the opposite occurs in the rotating models. The trend shown by the nonrotating models is the expected one, given the secondary nature of the neutron-capture nucleosynthesis. Vice versa, the counterintuitive trend obtained in the rotating models is the consequence of the higher mass loss present in the SSM models, removes the H-rich envelope faster than in the SM models while the stars are still in central He burning, dumping out the entanglement (activated by the rotation instabilities) and therefore conspicuous primary neutron-capture nucleosynthesis.","PeriodicalId":22368,"journal":{"name":"The Astrophysical Journal Supplement Series","volume":"81 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140888087","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 : 2024-05-01DOI: 10.3847/1538-4365/ad41c2
R. Abbasi, M. Ackermann, J. Adams, S. Agarwalla, J. Aguilar, M. Ahlers, J. Alameddine, N. M. Amin, K. Andeen, G. Anton, C. Argüelles, Y. Ashida, S. Athanasiadou, S. Axani, X. Bai, A. Balagopal V., M. Baricevic, S. Barwick, V. Basu, R. Bay, J. Beatty, K. Becker, J. Becker Tjus, J. Beise, C. Bellenghi, S. BenZvi, D. Berley, E. Bernardini, D. Besson, G. Binder, D. Bindig, E. Blaufuss, S. Blot, F. Bontempo, J. Book, C. Boscolo Meneguolo, S. Böser, O. Botner, J. Böttcher, E. Bourbeau, J. Braun, B. Brinson, J. Brostean-Kaiser, R. Burley, R. Busse, D. Butterfield, M. Campana, K. Carloni, E. Carnie-Bronca, S. Chattopadhyay, N. Chau, C. Chen, Z. Chen, D. Chirkin, S. Choi, B. Clark, L. Classen, A. Coleman, G. Collin, A. Connolly, J. Conrad, P. Coppin, P. Correa, S. Countryman, D. Cowen, P. Dave, C. De Clercq, J. DeLaunay, D. Delgado, H. Dembinski, S. Deng, K. Deoskar, A. Desai, P. Desiati, K. de Vries, G. de Wasseige, T. DeYoung, A. Diaz, J. C. Díaz-Vélez, M. Dittmer, A. Domi, H. Dujmovic, M. DuVernois, T. Ehrhardt
{"title":"Erratum: “IceCat-1: The IceCube Event Catalog of Alert Tracks” (2023, ApJS, 269, 25)","authors":"R. Abbasi, M. Ackermann, J. Adams, S. Agarwalla, J. Aguilar, M. Ahlers, J. Alameddine, N. M. Amin, K. Andeen, G. Anton, C. Argüelles, Y. Ashida, S. Athanasiadou, S. Axani, X. Bai, A. Balagopal V., M. Baricevic, S. Barwick, V. Basu, R. Bay, J. Beatty, K. Becker, J. Becker Tjus, J. Beise, C. Bellenghi, S. BenZvi, D. Berley, E. Bernardini, D. Besson, G. Binder, D. Bindig, E. Blaufuss, S. Blot, F. Bontempo, J. Book, C. Boscolo Meneguolo, S. Böser, O. Botner, J. Böttcher, E. Bourbeau, J. Braun, B. Brinson, J. Brostean-Kaiser, R. Burley, R. Busse, D. Butterfield, M. Campana, K. Carloni, E. Carnie-Bronca, S. Chattopadhyay, N. Chau, C. Chen, Z. Chen, D. Chirkin, S. Choi, B. Clark, L. Classen, A. Coleman, G. Collin, A. Connolly, J. Conrad, P. Coppin, P. Correa, S. Countryman, D. Cowen, P. Dave, C. De Clercq, J. DeLaunay, D. Delgado, H. Dembinski, S. Deng, K. Deoskar, A. Desai, P. Desiati, K. de Vries, G. de Wasseige, T. DeYoung, A. Diaz, J. C. Díaz-Vélez, M. Dittmer, A. Domi, H. Dujmovic, M. DuVernois, T. Ehrhardt","doi":"10.3847/1538-4365/ad41c2","DOIUrl":"https://doi.org/10.3847/1538-4365/ad41c2","url":null,"abstract":"","PeriodicalId":22368,"journal":{"name":"The Astrophysical Journal Supplement Series","volume":"19 6","pages":""},"PeriodicalIF":0.0,"publicationDate":"2024-05-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141047870","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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