adsabs/AstroCLIMB huggingface dataset:
Paper: The TESS Ten Thousand Catalog: 10,001 Uniformly Vetted and Validated Eclipsing Binary Stars Detected in Full-frame Image Data by Machine Learning and Analyzed by Citizen Scientists
Authors: Veselin B. Kostov, Brian P. Powell, Aline U. Fornear, Marco Z. Di Fraia, Robert Gagliano, Thomas L. Jacobs, Julien S. de Lambilly, Hugo A. Durantini Luca, Steven R. Majewski, Mark Omohundro, Jerome Orosz, Saul A. Rappaport, Ryan Salik, Donald Short, William Welsh, Svetoslav Alexandrov, Cledison Marcos da Silva, Erika Dunning, Gerd Gühne, Marc Huten, Michiharu Hyogo, Davide Iannone, Sam Lee, Christian Magliano, Manya Sharma, Allan Tarr, John Yablonsky, Sovan Acharya, Fred Adams, Thomas Barclay, Benjamin T. Montet, Susan Mullally, Greg Olmschenk, Andrej Prša, Elisa Quintana, Robert Wilson, Hasret Balcioglu, Ethan Kruse
Figure caption: Example fits to all phase-folded primary eclipses of TIC 470715046 for three models: trapezoid (red), Gaussian (green), and generalized Gaussian (cyan). The red and green curves are vertically offset for clarity. As seen from the figure, the generalized Gaussian model provides a much better fit to the data than either of the other models.
Paper: The TESS Ten Thousand Catalog: 10,001 Uniformly Vetted and Validated Eclipsing Binary Stars Detected in Full-frame Image Data by Machine Learning and Analyzed by Citizen Scientists
Authors: Veselin B. Kostov, Brian P. Powell, Aline U. Fornear, Marco Z. Di Fraia, Robert Gagliano, Thomas L. Jacobs, Julien S. de Lambilly, Hugo A. Durantini Luca, Steven R. Majewski, Mark Omohundro, Jerome Orosz, Saul A. Rappaport, Ryan Salik, Donald Short, William Welsh, Svetoslav Alexandrov, Cledison Marcos da Silva, Erika Dunning, Gerd Gühne, Marc Huten, Michiharu Hyogo, Davide Iannone, Sam Lee, Christian Magliano, Manya Sharma, Allan Tarr, John Yablonsky, Sovan Acharya, Fred Adams, Thomas Barclay, Benjamin T. Montet, Susan Mullally, Greg Olmschenk, Andrej Prša, Elisa Quintana, Robert Wilson, Hasret Balcioglu, Ethan Kruse
Figure caption: Distributions of the median primary and, where present, secondary eclipse depths (left panel, in ppt) and durations (right panel, in hours) for the 7936 new EBs presented here.
Paper: The TESS Ten Thousand Catalog: 10,001 Uniformly Vetted and Validated Eclipsing Binary Stars Detected in Full-frame Image Data by Machine Learning and Analyzed by Citizen Scientists
Authors: Veselin B. Kostov, Brian P. Powell, Aline U. Fornear, Marco Z. Di Fraia, Robert Gagliano, Thomas L. Jacobs, Julien S. de Lambilly, Hugo A. Durantini Luca, Steven R. Majewski, Mark Omohundro, Jerome Orosz, Saul A. Rappaport, Ryan Salik, Donald Short, William Welsh, Svetoslav Alexandrov, Cledison Marcos da Silva, Erika Dunning, Gerd Gühne, Marc Huten, Michiharu Hyogo, Davide Iannone, Sam Lee, Christian Magliano, Manya Sharma, Allan Tarr, John Yablonsky, Sovan Acharya, Fred Adams, Thomas Barclay, Benjamin T. Montet, Susan Mullally, Greg Olmschenk, Andrej Prša, Elisa Quintana, Robert Wilson, Hasret Balcioglu, Ethan Kruse
Figure caption: Similar to Figure 22 but for TIC 77392704. The vertical span is the same for all three panels. Here, the eclipses are loud and clear in Sectors 12 and 39, but barely present in Sector 65.
Paper: The TESS Ten Thousand Catalog: 10,001 Uniformly Vetted and Validated Eclipsing Binary Stars Detected in Full-frame Image Data by Machine Learning and Analyzed by Citizen Scientists
Authors: Veselin B. Kostov, Brian P. Powell, Aline U. Fornear, Marco Z. Di Fraia, Robert Gagliano, Thomas L. Jacobs, Julien S. de Lambilly, Hugo A. Durantini Luca, Steven R. Majewski, Mark Omohundro, Jerome Orosz, Saul A. Rappaport, Ryan Salik, Donald Short, William Welsh, Svetoslav Alexandrov, Cledison Marcos da Silva, Erika Dunning, Gerd Gühne, Marc Huten, Michiharu Hyogo, Davide Iannone, Sam Lee, Christian Magliano, Manya Sharma, Allan Tarr, John Yablonsky, Sovan Acharya, Fred Adams, Thomas Barclay, Benjamin T. Montet, Susan Mullally, Greg Olmschenk, Andrej Prša, Elisa Quintana, Robert Wilson, Hasret Balcioglu, Ethan Kruse
Figure caption: Phase-folded lightcurves for two targets with primary eclipse depths close to unity: TIC 42066695 (sector-averaged depth of ≈848 ppt, left panel) and TIC 446208053 (sector-averaged depth of ≈804 ppt, right panel).
Paper: The TESS Ten Thousand Catalog: 10,001 Uniformly Vetted and Validated Eclipsing Binary Stars Detected in Full-frame Image Data by Machine Learning and Analyzed by Citizen Scientists
Authors: Veselin B. Kostov, Brian P. Powell, Aline U. Fornear, Marco Z. Di Fraia, Robert Gagliano, Thomas L. Jacobs, Julien S. de Lambilly, Hugo A. Durantini Luca, Steven R. Majewski, Mark Omohundro, Jerome Orosz, Saul A. Rappaport, Ryan Salik, Donald Short, William Welsh, Svetoslav Alexandrov, Cledison Marcos da Silva, Erika Dunning, Gerd Gühne, Marc Huten, Michiharu Hyogo, Davide Iannone, Sam Lee, Christian Magliano, Manya Sharma, Allan Tarr, John Yablonsky, Sovan Acharya, Fred Adams, Thomas Barclay, Benjamin T. Montet, Susan Mullally, Greg Olmschenk, Andrej Prša, Elisa Quintana, Robert Wilson, Hasret Balcioglu, Ethan Kruse
Figure caption: Distributions of ratios between the correct TESS periods and the incorrect periods from Gaia (first panel from left), ASAS-SN (second panel from left), ATLAS (third panel from left), and VSX (last panel from left) for 2065 known EBs. For simplicity, the reciprocal fractions are combined, i.e., 1/2 with 2/1, 1/3 with 3/1, etc. The zero values represent targets of which the Gaia/ASAS-SN/ATLAS/VSX periods are not within 10% of a corresponding integer fraction of the TESS periods.
Paper: The TESS Ten Thousand Catalog: 10,001 Uniformly Vetted and Validated Eclipsing Binary Stars Detected in Full-frame Image Data by Machine Learning and Analyzed by Citizen Scientists
Authors: Veselin B. Kostov, Brian P. Powell, Aline U. Fornear, Marco Z. Di Fraia, Robert Gagliano, Thomas L. Jacobs, Julien S. de Lambilly, Hugo A. Durantini Luca, Steven R. Majewski, Mark Omohundro, Jerome Orosz, Saul A. Rappaport, Ryan Salik, Donald Short, William Welsh, Svetoslav Alexandrov, Cledison Marcos da Silva, Erika Dunning, Gerd Gühne, Marc Huten, Michiharu Hyogo, Davide Iannone, Sam Lee, Christian Magliano, Manya Sharma, Allan Tarr, John Yablonsky, Sovan Acharya, Fred Adams, Thomas Barclay, Benjamin T. Montet, Susan Mullally, Greg Olmschenk, Andrej Prša, Elisa Quintana, Robert Wilson, Hasret Balcioglu, Ethan Kruse
Figure caption: Left panels: ephemeris and vetting pipeline results for TIC 2597145. The correct period measured from TESS is 1.4143 days—twice as long as the period listed in Gaia (0.7072 days); ASAS-SN and VSX provide the correct period. Right panels: same as left but for TIC 9473243. Here, the Gaia period is 4 times the correct period, the ASAS-SN period is twice the correct period, and the WISE period is half of the correct period.
Paper: The TESS Ten Thousand Catalog: 10,001 Uniformly Vetted and Validated Eclipsing Binary Stars Detected in Full-frame Image Data by Machine Learning and Analyzed by Citizen Scientists
Authors: Veselin B. Kostov, Brian P. Powell, Aline U. Fornear, Marco Z. Di Fraia, Robert Gagliano, Thomas L. Jacobs, Julien S. de Lambilly, Hugo A. Durantini Luca, Steven R. Majewski, Mark Omohundro, Jerome Orosz, Saul A. Rappaport, Ryan Salik, Donald Short, William Welsh, Svetoslav Alexandrov, Cledison Marcos da Silva, Erika Dunning, Gerd Gühne, Marc Huten, Michiharu Hyogo, Davide Iannone, Sam Lee, Christian Magliano, Manya Sharma, Allan Tarr, John Yablonsky, Sovan Acharya, Fred Adams, Thomas Barclay, Benjamin T. Montet, Susan Mullally, Greg Olmschenk, Andrej Prša, Elisa Quintana, Robert Wilson, Hasret Balcioglu, Ethan Kruse
Figure caption: TESS ELEANOR lightcurve of the known EB TIC 26542657, highlighting clear changes in the shape of the primary and secondary eclipses between the first two sectors (14 and 15; sharp primary, rounded secondary) and the last three sectors (81, 82, and 83; rounded primary, flat secondary), along with a prominent tertiary eclipse in Sector 81 (red arrow).
Paper: The TESS Ten Thousand Catalog: 10,001 Uniformly Vetted and Validated Eclipsing Binary Stars Detected in Full-frame Image Data by Machine Learning and Analyzed by Citizen Scientists
Authors: Veselin B. Kostov, Brian P. Powell, Aline U. Fornear, Marco Z. Di Fraia, Robert Gagliano, Thomas L. Jacobs, Julien S. de Lambilly, Hugo A. Durantini Luca, Steven R. Majewski, Mark Omohundro, Jerome Orosz, Saul A. Rappaport, Ryan Salik, Donald Short, William Welsh, Svetoslav Alexandrov, Cledison Marcos da Silva, Erika Dunning, Gerd Gühne, Marc Huten, Michiharu Hyogo, Davide Iannone, Sam Lee, Christian Magliano, Manya Sharma, Allan Tarr, John Yablonsky, Sovan Acharya, Fred Adams, Thomas Barclay, Benjamin T. Montet, Susan Mullally, Greg Olmschenk, Andrej Prša, Elisa Quintana, Robert Wilson, Hasret Balcioglu, Ethan Kruse
Figure caption: Upper panel: primary ETVs for the two EBs in the 2+2 quadruple system TIC 219006972, confirming the two subsystems are gravitationally bound (V. B. Kostov et al. 2023) with an outer period of 168 days. Lower panel: primary (red) and secondary (blue) ETVs of the known EB TIC 26542657, suggesting a 2+1 triple system with an outer period of about 300 days.
Paper: The TESS Ten Thousand Catalog: 10,001 Uniformly Vetted and Validated Eclipsing Binary Stars Detected in Full-frame Image Data by Machine Learning and Analyzed by Citizen Scientists
Authors: Veselin B. Kostov, Brian P. Powell, Aline U. Fornear, Marco Z. Di Fraia, Robert Gagliano, Thomas L. Jacobs, Julien S. de Lambilly, Hugo A. Durantini Luca, Steven R. Majewski, Mark Omohundro, Jerome Orosz, Saul A. Rappaport, Ryan Salik, Donald Short, William Welsh, Svetoslav Alexandrov, Cledison Marcos da Silva, Erika Dunning, Gerd Gühne, Marc Huten, Michiharu Hyogo, Davide Iannone, Sam Lee, Christian Magliano, Manya Sharma, Allan Tarr, John Yablonsky, Sovan Acharya, Fred Adams, Thomas Barclay, Benjamin T. Montet, Susan Mullally, Greg Olmschenk, Andrej Prša, Elisa Quintana, Robert Wilson, Hasret Balcioglu, Ethan Kruse
Figure caption: Same as Figure 27 but for TIC 403072759 (left) and TIC 12396863 (right). Thanks to TESS, shallow secondary eclipses can be detected near phase 0.5 for both targets, confirming the corresponding periods are 1.3029 days and 2.6760 days. For comparison, the periods listed in Gaia are 0.5210 days for TIC 403072759 (i.e., two-fifths of the true period) and 5.3519 days for TIC 12396863 (i.e., twice the true period).
Paper: The TESS Ten Thousand Catalog: 10,001 Uniformly Vetted and Validated Eclipsing Binary Stars Detected in Full-frame Image Data by Machine Learning and Analyzed by Citizen Scientists
Authors: Veselin B. Kostov, Brian P. Powell, Aline U. Fornear, Marco Z. Di Fraia, Robert Gagliano, Thomas L. Jacobs, Julien S. de Lambilly, Hugo A. Durantini Luca, Steven R. Majewski, Mark Omohundro, Jerome Orosz, Saul A. Rappaport, Ryan Salik, Donald Short, William Welsh, Svetoslav Alexandrov, Cledison Marcos da Silva, Erika Dunning, Gerd Gühne, Marc Huten, Michiharu Hyogo, Davide Iannone, Sam Lee, Christian Magliano, Manya Sharma, Allan Tarr, John Yablonsky, Sovan Acharya, Fred Adams, Thomas Barclay, Benjamin T. Montet, Susan Mullally, Greg Olmschenk, Andrej Prša, Elisa Quintana, Robert Wilson, Hasret Balcioglu, Ethan Kruse
Figure caption: Kepler lightcurve of the known TESS EB TIC 26542657 showing a single tertiary eclipse (marked with a red arrow) and no discernible eclipses from the ∼11 day EB.
Paper: The TESS Ten Thousand Catalog: 10,001 Uniformly Vetted and Validated Eclipsing Binary Stars Detected in Full-frame Image Data by Machine Learning and Analyzed by Citizen Scientists
Authors: Veselin B. Kostov, Brian P. Powell, Aline U. Fornear, Marco Z. Di Fraia, Robert Gagliano, Thomas L. Jacobs, Julien S. de Lambilly, Hugo A. Durantini Luca, Steven R. Majewski, Mark Omohundro, Jerome Orosz, Saul A. Rappaport, Ryan Salik, Donald Short, William Welsh, Svetoslav Alexandrov, Cledison Marcos da Silva, Erika Dunning, Gerd Gühne, Marc Huten, Michiharu Hyogo, Davide Iannone, Sam Lee, Christian Magliano, Manya Sharma, Allan Tarr, John Yablonsky, Sovan Acharya, Fred Adams, Thomas Barclay, Benjamin T. Montet, Susan Mullally, Greg Olmschenk, Andrej Prša, Elisa Quintana, Robert Wilson, Hasret Balcioglu, Ethan Kruse
Figure caption: Same as Figure 27 but for TIC 2239760 (left) and TIC 143060048 (right), for which the corresponding ratios between the Gaia and TESS periods are not close to low-order integer ratios (≈0.55 and ≈7.11, respectively).
Paper: The TESS Ten Thousand Catalog: 10,001 Uniformly Vetted and Validated Eclipsing Binary Stars Detected in Full-frame Image Data by Machine Learning and Analyzed by Citizen Scientists
Authors: Veselin B. Kostov, Brian P. Powell, Aline U. Fornear, Marco Z. Di Fraia, Robert Gagliano, Thomas L. Jacobs, Julien S. de Lambilly, Hugo A. Durantini Luca, Steven R. Majewski, Mark Omohundro, Jerome Orosz, Saul A. Rappaport, Ryan Salik, Donald Short, William Welsh, Svetoslav Alexandrov, Cledison Marcos da Silva, Erika Dunning, Gerd Gühne, Marc Huten, Michiharu Hyogo, Davide Iannone, Sam Lee, Christian Magliano, Manya Sharma, Allan Tarr, John Yablonsky, Sovan Acharya, Fred Adams, Thomas Barclay, Benjamin T. Montet, Susan Mullally, Greg Olmschenk, Andrej Prša, Elisa Quintana, Robert Wilson, Hasret Balcioglu, Ethan Kruse
Figure caption: Upper panel: TESS FFI ELEANOR lightcurve of TIC 307119043, an eclipsing 2+2 quadruple exhibiting two sets of primary and secondary eclipses (V. B. Kostov et al. 2022b). Lower panel: eclipsing (2+1)+1 quadruple system TIC 114936199 exhibiting a complex eclipse on the outer orbit (B. P. Powell et al. 2022b).
Paper: The TESS Ten Thousand Catalog: 10,001 Uniformly Vetted and Validated Eclipsing Binary Stars Detected in Full-frame Image Data by Machine Learning and Analyzed by Citizen Scientists
Authors: Veselin B. Kostov, Brian P. Powell, Aline U. Fornear, Marco Z. Di Fraia, Robert Gagliano, Thomas L. Jacobs, Julien S. de Lambilly, Hugo A. Durantini Luca, Steven R. Majewski, Mark Omohundro, Jerome Orosz, Saul A. Rappaport, Ryan Salik, Donald Short, William Welsh, Svetoslav Alexandrov, Cledison Marcos da Silva, Erika Dunning, Gerd Gühne, Marc Huten, Michiharu Hyogo, Davide Iannone, Sam Lee, Christian Magliano, Manya Sharma, Allan Tarr, John Yablonsky, Sovan Acharya, Fred Adams, Thomas Barclay, Benjamin T. Montet, Susan Mullally, Greg Olmschenk, Andrej Prša, Elisa Quintana, Robert Wilson, Hasret Balcioglu, Ethan Kruse
Figure caption: Disappearing eclipses due to dynamical interactions with unseen companions. Upper panel: TIC 236774836 (T. Mitnyan et al. 2024b); lower panel: TIC 220410224.
Paper: Deep Active Learning–Based Classification of Solar Radio Spectrogram Data
Authors: Yan Liu, 岩 刘, HongQiang Song, 红强 宋, FaBao Yan, 发宝 严, YanRui Su, 艳蕊 苏
Figure caption: Observations of solar radio spectra from the CSO of Shandong University. The CSO monitors in the range of 90–600 MHz. The full spectra are available at http://47.104.87.104/SRData/CBSm/dailyView/2023/12/SynRadiospec_CSO_20231201.jpg.
Paper: Deep Active Learning–Based Classification of Solar Radio Spectrogram Data
Authors: Yan Liu, 岩 刘, HongQiang Song, 红强 宋, FaBao Yan, 发宝 严, YanRui Su, 艳蕊 苏
Figure caption: Observations of solar radio spectra from the Learmonth Observatory of Australia. The Learmonth Observatory radio observatory monitors in the range of 25–180 MHz: https://www.sws.bom.gov.au/World_Data_Centre/1/9.
Paper: Deep Active Learning–Based Classification of Solar Radio Spectrogram Data
Authors: Yan Liu, 岩 刘, HongQiang Song, 红强 宋, FaBao Yan, 发宝 严, YanRui Su, 艳蕊 苏
Figure caption: Active learning process.
Paper: Deep Active Learning–Based Classification of Solar Radio Spectrogram Data
Authors: Yan Liu, 岩 刘, HongQiang Song, 红强 宋, FaBao Yan, 发宝 严, YanRui Su, 艳蕊 苏
Figure caption: Effect of processing solar radio spectral image from CSO of Shandong University. (a) Nonburst. (b) Burst. (c) Calibration. Note that no-axis spectral images are used for input models.
Paper: Deep Active Learning–Based Classification of Solar Radio Spectrogram Data
Authors: Yan Liu, 岩 刘, HongQiang Song, 红强 宋, FaBao Yan, 发宝 严, YanRui Su, 艳蕊 苏
Figure caption: Effect of processing a solar radio spectral image from Learmonth, Australia. (a) Nonburst. (b) Burst. (c) Calibration. Note that no-axis spectral images are used for input models.
Paper: Deep Active Learning–Based Classification of Solar Radio Spectrogram Data
Authors: Yan Liu, 岩 刘, HongQiang Song, 红强 宋, FaBao Yan, 发宝 严, YanRui Su, 艳蕊 苏
Figure caption: Structure of the P-DCGAN model.
Paper: Deep Active Learning–Based Classification of Solar Radio Spectrogram Data
Authors: Yan Liu, 岩 刘, HongQiang Song, 红强 宋, FaBao Yan, 发宝 严, YanRui Su, 艳蕊 苏
Figure caption: The network framework diagram of this paper.
Paper: Deep Active Learning–Based Classification of Solar Radio Spectrogram Data
Authors: Yan Liu, 岩 刘, HongQiang Song, 红强 宋, FaBao Yan, 发宝 严, YanRui Su, 艳蕊 苏
Figure caption: Result by automatic spectrum classification: (a) results catalog and (b) bursts image.
Paper: Deep Active Learning–Based Classification of Solar Radio Spectrogram Data
Authors: Yan Liu, 岩 刘, HongQiang Song, 红强 宋, FaBao Yan, 发宝 严, YanRui Su, 艳蕊 苏
Figure caption: Result by automatic bursts classification: (a) results catalog and (b) type II bursts.
Paper: Deep Active Learning–Based Classification of Solar Radio Spectrogram Data
Authors: Yan Liu, 岩 刘, HongQiang Song, 红强 宋, FaBao Yan, 发宝 严, YanRui Su, 艳蕊 苏
Figure caption: Comparison of the effect of different methods of generating image. Note that no-axis spectral images are used for input models.
Paper: Deep Active Learning–Based Classification of Solar Radio Spectrogram Data
Authors: Yan Liu, 岩 刘, HongQiang Song, 红强 宋, FaBao Yan, 发宝 严, YanRui Su, 艳蕊 苏
Figure caption: Type I to Type III bursts (after preprocessing). Note that no-axis spectral images were used for input models.) (a) Type I, (b) Type II, and (c) Type III.
Paper: Deep Active Learning–Based Classification of Solar Radio Spectrogram Data
Authors: Yan Liu, 岩 刘, HongQiang Song, 红强 宋, FaBao Yan, 发宝 严, YanRui Su, 艳蕊 苏
Figure caption: Distribution histograms of event start and end frequencies.
Paper: Deep Active Learning–Based Classification of Solar Radio Spectrogram Data
Authors: Yan Liu, 岩 刘, HongQiang Song, 红强 宋, FaBao Yan, 发宝 严, YanRui Su, 艳蕊 苏
Figure caption: Comparison of the effect of different methods of generating an image.
Paper: Deep Active Learning–Based Classification of Solar Radio Spectrogram Data
Authors: Yan Liu, 岩 刘, HongQiang Song, 红强 宋, FaBao Yan, 发宝 严, YanRui Su, 艳蕊 苏
Figure caption: Distribution histograms of duration for type II and type III bursts.
Paper: Deep Active Learning–Based Classification of Solar Radio Spectrogram Data
Authors: Yan Liu, 岩 刘, HongQiang Song, 红强 宋, FaBao Yan, 发宝 严, YanRui Su, 艳蕊 苏
Figure caption: Variations of the loss function and accuracy with epochs.
Paper: A 50–55 GHz Millimeter-wave Radiometer Spectrometer for Solar Flare Detection
Authors: XiaoFeng Xu, 晓峰 徐, ZhanFeng Zhao, 占锋 赵, Qian Liu, 乾 刘, QinZheng Li, 钦正 李, Zhao Wu, 昭 武, Guang Lu, 光 路, YanRui Su, 艳蕊 苏, Yao Chen, 耀 陈, FaBao Yan, 发宝 严
Figure caption: The 50–55 GHz millimeter-wave radiometer spectrometer for solar flare detection is installed at an altitude of 4200 m. An optical device is equipped on the turntable frame to ensure precise pointing accuracy within 3′, allowing the system to effectively observe signals within the main lobe width of the antenna.
Paper: A 50–55 GHz Millimeter-wave Radiometer Spectrometer for Solar Flare Detection
Authors: XiaoFeng Xu, 晓峰 徐, ZhanFeng Zhao, 占锋 赵, Qian Liu, 乾 刘, QinZheng Li, 钦正 李, Zhao Wu, 昭 武, Guang Lu, 光 路, YanRui Su, 艳蕊 苏, Yao Chen, 耀 陈, FaBao Yan, 发宝 严
Figure caption: The physical diagram and circuit layout of the digital receiver are shown. Panel (a) depicts a digital receiving subsystem board housed within a chassis, which uses shielding tape to isolate 50 Hz signals and prevent external interference. Panel (b) presents a photo of the printed circuit board layout. The board is powered by a dedicated power module and operates as follows: The signal, initially processed by the analog receiver, is input through an SMA interface. It then undergoes secondary amplification, analog-to-digital conversion, and data processing to complete the preliminary signal processing.
Paper: A 50–55 GHz Millimeter-wave Radiometer Spectrometer for Solar Flare Detection
Authors: XiaoFeng Xu, 晓峰 徐, ZhanFeng Zhao, 占锋 赵, Qian Liu, 乾 刘, QinZheng Li, 钦正 李, Zhao Wu, 昭 武, Guang Lu, 光 路, YanRui Su, 艳蕊 苏, Yao Chen, 耀 陈, FaBao Yan, 发宝 严
Figure caption: Detailed architecture and signal routing of the system. It includes four parts: antenna-feeder subsystem, AFE subsystem, digital receiver subsystem, and upper computer subsystem. Presented are the design schemes of analog and digital receivers, as well as the data processing work carried out within the FPGA.
Paper: A 50–55 GHz Millimeter-wave Radiometer Spectrometer for Solar Flare Detection
Authors: XiaoFeng Xu, 晓峰 徐, ZhanFeng Zhao, 占锋 赵, Qian Liu, 乾 刘, QinZheng Li, 钦正 李, Zhao Wu, 昭 武, Guang Lu, 光 路, YanRui Su, 艳蕊 苏, Yao Chen, 耀 陈, FaBao Yan, 发宝 严
Figure caption: The upper computer subsystem comprises two main parts: the signal display section and the functional area. The signal display section is responsible for visualizing the processed data in real time, providing users with a clear overview of the signal characteristics. The functional area, on the other hand, includes various control and analysis tools that enable users to interact with the system, perform data analysis, and configure system parameters.
Paper: A 50–55 GHz Millimeter-wave Radiometer Spectrometer for Solar Flare Detection
Authors: XiaoFeng Xu, 晓峰 徐, ZhanFeng Zhao, 占锋 赵, Qian Liu, 乾 刘, QinZheng Li, 钦正 李, Zhao Wu, 昭 武, Guang Lu, 光 路, YanRui Su, 艳蕊 苏, Yao Chen, 耀 陈, FaBao Yan, 发宝 严
Figure caption: The figure illustrates the effective gain of the system. The significant fluctuation on the left side of the dashed line is attributed to the instability of the output from the vector network analyzer used for testing. The substantial gain drop on the right side is due to the 1 dB compression point (P1dB) inherent in the microwave components, which causes a rapid decline in gain. The region within the dashed line represents the linear operating range of the system. According to measurements, the dynamic range of the system is at least 30 dB.
Paper: A 50–55 GHz Millimeter-wave Radiometer Spectrometer for Solar Flare Detection
Authors: XiaoFeng Xu, 晓峰 徐, ZhanFeng Zhao, 占锋 赵, Qian Liu, 乾 刘, QinZheng Li, 钦正 李, Zhao Wu, 昭 武, Guang Lu, 光 路, YanRui Su, 艳蕊 苏, Yao Chen, 耀 陈, FaBao Yan, 发宝 严
Figure caption: The physical layout of the antenna-feed subsystem and the simulation of the main lobe width. The antenna consists of a carbon fiber primary reflector, an aluminum alloy secondary reflector, and a horn feed. The main lobe width of the antenna is approximately 24′ within the frequency band of 50–55 GHz.
Paper: The Chemical Yields of Stars in the Mass Range 9–15 M⊙
Authors: Marco Limongi, Lorenzo Roberti, Agnese Falla, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Abundances of the various elements in the ejecta as a function of the initial mass, after the full decay of all the unstable nuclear species. To improve the readability of the figure, for each element we have normalized the abundances obtained for all the stars to the maximum one (reported in solar masses in the lower corner of each panel). The red lines/red filled dots refer the results obtained in this study while the blue lines/blue filled dots refer to the values published by M. Limongi & A. Chieffi (2018).
Paper: The Chemical Yields of Stars in the Mass Range 9–15 M⊙
Authors: Marco Limongi, Lorenzo Roberti, Agnese Falla, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Same as Figure 4, but for Ti–Rb.
Paper: The Chemical Yields of Stars in the Mass Range 9–15 M⊙
Authors: Marco Limongi, Lorenzo Roberti, Agnese Falla, Alessandro Chieffi, Ken'ichi Nomoto
Figure caption: Chemical composition of the ejecta of the 9.22 M⊙ star compared to the solar composition. The gray band corresponds to a variation by a factor of 2 with respect to ﹩{\rm{Log}}{(}^{16}{\rm{O}}{/}^{16}{{\rm{O}}}_{\odot })﹩.