adsabs/AstroCLIMB huggingface dataset:
Paper: The LSST Era of Supermassive Black Hole Accretion Disk Reverberation Mapping
Authors: Andjelka B. Kovačević, Viktor Radović, Dragana Ilić, Luka Č. Popović, Roberto J. Assef, Paula Sánchez-Sáez, Robert Nikutta, Claudia M. Raiteri, Ilsang Yoon, Yasaman Homayouni, Yan-Rong Li, Neven Caplar, Bozena Czerny, Swayamtrupta Panda, Claudio Ricci, Isidora Jankov, Hermine Landt, Christian Wolf, Jelena Kovačević-Dojčinović, Maša Lakićević, Đorđe V. Savić, Oliver Vince, Saša Simić, Iva Čvorović-Hajdinjak, Sladjana Marčeta-Mandić
Figure caption: Metric realization on short_exp cadences continued. Three DDFs are prominent in panels (b) and (c).
Paper: The Velocity Map Asymmetry of Ionized Gas in MaNGA. I. The Catalog and General Properties
Authors: Shuai Feng, 帅 冯, Shi-Yin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Y. Sophia Dai, 昱 戴, Karen L. Masters
Figure caption: Left: the kinematic asymmetry as a function of stellar mass for “regular” galaxies. The black dashed line shows the median ﹩\mathrm{log}{\bar{v}}_{\mathrm{asym}}﹩ values, and the two black dotted lines show the 16th and 84th percentiles of the ﹩\mathrm{log}{\bar{v}}_{\mathrm{asym}}﹩ distribution. The color-coded symbols represent the result of “special” galaxies for comparison. Right: dependency of the ﹩\mathrm{log}{M}_{\star }﹩–﹩\mathrm{log}{\bar{v}}_{\mathrm{asym}}﹩ relation on Sérsic index (n  s ). The black dashed line is the same as in the left panel.
Paper: The Velocity Map Asymmetry of Ionized Gas in MaNGA. I. The Catalog and General Properties
Authors: Shuai Feng, 帅 冯, Shi-Yin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Y. Sophia Dai, 昱 戴, Karen L. Masters
Figure caption: Left: the relationship between kinematic asymmetry ﹩\mathrm{log}{\bar{v}}_{\mathrm{asym}}﹩ and its relative uncertainty ﹩\mathrm{log}\delta {\bar{v}}_{\mathrm{asym}}﹩. Gray circles are all 5353 galaxies in Sample A, and the black dashed contours show their number density distribution. The red dotted line represents ﹩\mathrm{log}\delta {\bar{v}}_{\mathrm{asym}}=-2﹩. Right: the relationship between kinematic asymmetry ﹩\mathrm{log}{\bar{v}}_{\mathrm{asym}}﹩ and S/N of Hα flux at effective radius S/N(R  e ). The black dashed contours represent the number density distribution of Sample A, while red solid contours represent galaxies satisfying ﹩\mathrm{log}\delta {\bar{v}}_{\mathrm{asym}}\lt -2﹩.
Paper: The Velocity Map Asymmetry of Ionized Gas in MaNGA. I. The Catalog and General Properties
Authors: Shuai Feng, 帅 冯, Shi-Yin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Y. Sophia Dai, 昱 戴, Karen L. Masters
Figure caption: Left: the distribution of kinematic asymmetry for Samples A, B, and C. ﹩\mathrm{log}{\bar{v}}_{\mathrm{asym}}=-1.41﹩ (dotted−dashed line) is the 66th percentile of ﹩\mathrm{log}{\bar{v}}_{\mathrm{asym}}﹩ distribution, which is adopted as the threshold of a high asymmetry (HA) galaxy. ﹩\mathrm{log}{\bar{v}}_{\mathrm{asym}}=-0.60﹩ (dashed line) and ﹩\mathrm{log}{\bar{v}}_{\mathrm{asym}}=-1.60﹩ (dotted line) indicate when the ratio between a nonrotating component and rotating component equals 1 and 0.1, respectively. Right: the distribution of stellar mass for Samples A, B, and C.
Paper: The Velocity Map Asymmetry of Ionized Gas in MaNGA. I. The Catalog and General Properties
Authors: Shuai Feng, 帅 冯, Shi-Yin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Y. Sophia Dai, 昱 戴, Karen L. Masters
Figure caption: Left: dependency of the ﹩\mathrm{log}{M}_{\star }﹩–﹩\mathrm{log}{\bar{v}}_{\mathrm{asym}}﹩ relation on local environment (Q local): −2.0 < Q local < 4.0 (red triangles), −4.0 < Q local < −2.0 (green squares), and −7.0 < Q local < −4.0 (blue circles). Right: dependency of the ﹩\mathrm{log}{M}_{\star }﹩–﹩\mathrm{log}{\bar{v}}_{\mathrm{asym}}﹩ relation on LSS environment: void (blue circles), sheet (green stars), filament (orange squares), and cluster (red triangles).
Paper: The Velocity Map Asymmetry of Ionized Gas in MaNGA. I. The Catalog and General Properties
Authors: Shuai Feng, 帅 冯, Shi-Yin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Y. Sophia Dai, 昱 戴, Karen L. Masters
Figure caption: Left: dependency of the ﹩\mathrm{log}{M}_{\star }﹩–﹩\mathrm{log}{\bar{v}}_{\mathrm{asym}}﹩ relation on the H I fraction (f H I ). The color-coded lines represent galaxies with different f H I  intervals. Right: relationship between H I detection rate, stellar mass, and kinematic asymmetry, where red circles represent galaxies with low kinematic asymmetry (﹩\mathrm{log}{\bar{v}}_{\mathrm{asym}}\lt -1.41﹩) and blue squares represent galaxies with high kinematic asymmetry (﹩\mathrm{log}{\bar{v}}_{\mathrm{asym}}\gt -1.41﹩).
Paper: The Velocity Map Asymmetry of Ionized Gas in MaNGA. I. The Catalog and General Properties
Authors: Shuai Feng, 帅 冯, Shi-Yin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Y. Sophia Dai, 昱 戴, Karen L. Masters
Figure caption: Left: ﹩\mathrm{log}{M}_{\star }﹩–log SFR relation of all “regular” galaxies. The black dashed line represents the median value, and the black dotted lines represent the 16th and 84th percentiles. Right: the dependency of the ﹩\mathrm{log}{M}_{\star }﹩–﹩\mathrm{log}{\bar{v}}_{\mathrm{asym}}﹩ relation on star formation activities. Red triangles, green squares, and blue circles represent starburst galaxy, main-sequence galaxy, and quiescent galaxy, respectively.
Paper: The Velocity Map Asymmetry of Ionized Gas in MaNGA. I. The Catalog and General Properties
Authors: Shuai Feng, 帅 冯, Shi-Yin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Y. Sophia Dai, 昱 戴, Karen L. Masters
Figure caption: Two cases of merging galaxies, 10839–9101 (top) and 9894–12703 (bottom). Left: gri-band image from SDSS. Right: Hα velocity map; only spaxels with Hα S/N greater than 5 are shown. The value of kinematic asymmetry is labeled in the lower left corner.
Paper: The Velocity Map Asymmetry of Ionized Gas in MaNGA. I. The Catalog and General Properties
Authors: Shuai Feng, 帅 冯, Shi-Yin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Y. Sophia Dai, 昱 戴, Karen L. Masters
Figure caption: The cases of barred galaxy 9879–6102 (top) and unbarred disk galaxy 8317–6102 (bottom).
Paper: The Velocity Map Asymmetry of Ionized Gas in MaNGA. I. The Catalog and General Properties
Authors: Shuai Feng, 帅 冯, Shi-Yin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Y. Sophia Dai, 昱 戴, Karen L. Masters
Figure caption: The case of AGN host galaxy 10492–6103. Top left: SDSS gri-band image; top right: Hα velocity map; bottom left: maps of BPT classification; bottom right: BPT diagram for all spaxels.
Paper: The Spectral Energy Distributions for 4FGL Blazars
Authors: J. H. Yang, J. H. Fan, Y. Liu, M. X. Tuo, Z. Y. Pei, W. X. Yang, Y. H. Yuan, S. L. He, S. H. Wang, X. C. Wang, X. J. Chen, X. H. Qu, Q. Cao, Q. Y. Tao, Y. L. Zhang, C. Q. Liu, J. J. Nie, L. F. Liu, D. K. Jiang, A. N. Jiang, B. Liu, R. S. Yang
Figure caption: The scatterplots of the correlations between ﹩\mathrm{log}{\nu }_{{\rm{p}}}﹩ and other parameters of (a) ﹩\mathrm{log}{L}_{{\rm{R}}}﹩, (b) ﹩\mathrm{log}{L}_{{\rm{O}}}﹩, (c) ﹩\mathrm{log}{L}_{{\rm{X}}}﹩, (d) ﹩\mathrm{log}{L}_{\gamma }﹩, (e) ﹩\mathrm{log}{L}_{{\rm{p}}}﹩, (f) 1/∣P 1∣, (g) α RO, and (h) α OX.
Paper: The Spectral Energy Distributions for 4FGL Blazars
Authors: J. H. Yang, J. H. Fan, Y. Liu, M. X. Tuo, Z. Y. Pei, W. X. Yang, Y. H. Yuan, S. L. He, S. H. Wang, X. C. Wang, X. J. Chen, X. H. Qu, Q. Cao, Q. Y. Tao, Y. L. Zhang, C. Q. Liu, J. J. Nie, L. F. Liu, D. K. Jiang, A. N. Jiang, B. Liu, R. S. Yang
Figure caption: The correlations between the synchrotron peak frequencies obtained from this work and other works. TW: this work. S96: Sambruna et al. (1996). N06: Nieppola et al. (2006). N08: Nieppola et al. (2008). A10: Abdo et al. (2010). F16: Fan et al. (2016). P21: Paliya et al. (2021).
Paper: The Spectral Energy Distributions for 4FGL Blazars
Authors: J. H. Yang, J. H. Fan, Y. Liu, M. X. Tuo, Z. Y. Pei, W. X. Yang, Y. H. Yuan, S. L. He, S. H. Wang, X. C. Wang, X. J. Chen, X. H. Qu, Q. Cao, Q. Y. Tao, Y. L. Zhang, C. Q. Liu, J. J. Nie, L. F. Liu, D. K. Jiang, A. N. Jiang, B. Liu, R. S. Yang
Figure caption: The SEDs diagrams with fitted lines. The curve line represents the parabolic fit to the synchrotron component. Oblique cross hairs (×) are included in the fit, the cross hairs (+) are not.
Paper: The Spectral Energy Distributions for 4FGL Blazars
Authors: J. H. Yang, J. H. Fan, Y. Liu, M. X. Tuo, Z. Y. Pei, W. X. Yang, Y. H. Yuan, S. L. He, S. H. Wang, X. C. Wang, X. J. Chen, X. H. Qu, Q. Cao, Q. Y. Tao, Y. L. Zhang, C. Q. Liu, J. J. Nie, L. F. Liu, D. K. Jiang, A. N. Jiang, B. Liu, R. S. Yang
Figure caption: The BIC values and distribution for the synchrotron peak frequencies of 2709 blazars. (a) Distribution. (b) BIC values.
Paper: The Spectral Energy Distributions for 4FGL Blazars
Authors: J. H. Yang, J. H. Fan, Y. Liu, M. X. Tuo, Z. Y. Pei, W. X. Yang, Y. H. Yuan, S. L. He, S. H. Wang, X. C. Wang, X. J. Chen, X. H. Qu, Q. Cao, Q. Y. Tao, Y. L. Zhang, C. Q. Liu, J. J. Nie, L. F. Liu, D. K. Jiang, A. N. Jiang, B. Liu, R. S. Yang
Figure caption: The distribution of classification for 2709 blazars. T stands for total sample, B for BL Lac, F for FSRQ, U for blazars of uncertain type, H for HSP, I for ISP, and L for LSP.
Paper: The Spectral Energy Distributions for 4FGL Blazars
Authors: J. H. Yang, J. H. Fan, Y. Liu, M. X. Tuo, Z. Y. Pei, W. X. Yang, Y. H. Yuan, S. L. He, S. H. Wang, X. C. Wang, X. J. Chen, X. H. Qu, Q. Cao, Q. Y. Tao, Y. L. Zhang, C. Q. Liu, J. J. Nie, L. F. Liu, D. K. Jiang, A. N. Jiang, B. Liu, R. S. Yang
Figure caption: The correlation between α RO and α OX.
Paper: The Velocity Map Asymmetry of Ionized Gas in MaNGA. I. The Catalog and General Properties
Authors: Shuai Feng, 帅 冯, Shi-Yin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Y. Sophia Dai, 昱 戴, Karen L. Masters
Figure caption: Four cases of Hα velocity map, the kinematic asymmetry of which ﹩\mathrm{log}{\bar{v}}_{\mathrm{asym}}﹩ are labeled in the lower left corner of each panel.
Paper: Mining S-PLUS for Metal-poor Stars in the Milky Way
Authors: Vinicius M. Placco, Felipe Almeida-Fernandes, Anke Arentsen, Young Sun Lee, William Schoenell, Tiago Ribeiro, Antonio Kanaan
Figure caption: Top panel: (J0378-i)-(J0410-J0660) as a function of the metallicity for the observed sample, with the gray line marking the proposed color cut. Also shown are the fractions of stars with [Fe/H] ≤ −1.0 and ≤ −2.0 for the two subsamples. The point sizes are proportional to T eff. Bottom panel: cumulative distribution functions (CDFs) for the two subsamples, marking the [Fe/H] value for which they reach 80%.
Paper: KW-Sun: The Konus-Wind Solar Flare Database in Hard X-Ray and Soft Gamma-Ray Ranges
Authors: A. L. Lysenko, M. V. Ulanov, A. A. Kuznetsov, G. D. Fleishman, D. D. Frederiks, L. K. Kashapova, Z. Ya. Sokolova, D. S. Svinkin, A. E. Tsvetkova
Figure caption: Konus-Wind: (a) the location of Konus detectors S1 and S2 on the spacecraft, “N” and “S” are the directions to the ecliptic poles and the circular arrow indicates the spin direction of the spacecraft; (b) a scheme of the Konus detector. The green arrow indicates the direction of solar emission.
Paper: KW-Sun: The Konus-Wind Solar Flare Database in Hard X-Ray and Soft Gamma-Ray Ranges
Authors: A. L. Lysenko, M. V. Ulanov, A. A. Kuznetsov, G. D. Fleishman, D. D. Frederiks, L. K. Kashapova, Z. Ya. Sokolova, D. S. Svinkin, A. E. Tsvetkova
Figure caption: Temporal evolutions of Konus-Wind low-energy boundaries (left) and high-energy boundaries (right) for detectors S1 and S2.
Paper: A Dynamic Deep-learning Model for Generating a Magnetogram Sequence from an SDO/AIA EUV Image Sequence
Authors: Wenqing Sun, Long Xu, Suli Ma, Yihua Yan, Tie Liu, Weiqiang Zhang
Figure caption: The first and third rows show three sequential Helioseismic and Magnetic Imager (HMI) magnetograms and the ones generated by Kim et al. (2019), respectively. The second and fourth rows illustrate color maps of the two small patches labeled in the first and third rows, respectively.
Paper: A Dynamic Deep-learning Model for Generating a Magnetogram Sequence from an SDO/AIA EUV Image Sequence
Authors: Wenqing Sun, Long Xu, Suli Ma, Yihua Yan, Tie Liu, Weiqiang Zhang
Figure caption: Comparisons of generated magnetograms among the proposed convGRU–pix2pix, multichannel pix2pix, and pix2pix baseline. To tell “magnetogram fluctuation” more clearly, the color maps of the two small patches labeled by “a” and “b” are illustrated next to each full-disk magnetogram.
Paper: A Dynamic Deep-learning Model for Generating a Magnetogram Sequence from an SDO/AIA EUV Image Sequence
Authors: Wenqing Sun, Long Xu, Suli Ma, Yihua Yan, Tie Liu, Weiqiang Zhang
Figure caption: Diagram of magnetogram generation from Atmospheric Imaging Assembly (AIA) image sequence.
Paper: A Dynamic Deep-learning Model for Generating a Magnetogram Sequence from an SDO/AIA EUV Image Sequence
Authors: Wenqing Sun, Long Xu, Suli Ma, Yihua Yan, Tie Liu, Weiqiang Zhang
Figure caption: Network architecture of convGRU–pix2pix.
Paper: The Spectral Energy Distributions for 4FGL Blazars
Authors: J. H. Yang, J. H. Fan, Y. Liu, M. X. Tuo, Z. Y. Pei, W. X. Yang, Y. H. Yuan, S. L. He, S. H. Wang, X. C. Wang, X. J. Chen, X. H. Qu, Q. Cao, Q. Y. Tao, Y. L. Zhang, C. Q. Liu, J. J. Nie, L. F. Liu, D. K. Jiang, A. N. Jiang, B. Liu, R. S. Yang
Figure caption: The correlations between effective spectral indexes obtained from this paper and Ackermann et al. (2011) (a) for α RO and (b) for α OX.
Paper: The Spectral Energy Distributions for 4FGL Blazars
Authors: J. H. Yang, J. H. Fan, Y. Liu, M. X. Tuo, Z. Y. Pei, W. X. Yang, Y. H. Yuan, S. L. He, S. H. Wang, X. C. Wang, X. J. Chen, X. H. Qu, Q. Cao, Q. Y. Tao, Y. L. Zhang, C. Q. Liu, J. J. Nie, L. F. Liu, D. K. Jiang, A. N. Jiang, B. Liu, R. S. Yang
Figure caption: The correlations between flux densities: (a) ﹩\mathrm{log}{f}_{\gamma }\sim \mathrm{log}{f}_{{\rm{R}}};﹩ (b) ﹩\mathrm{log}{f}_{\gamma }\sim \mathrm{log}{f}_{{\rm{O}}};﹩ (c) ﹩\mathrm{log}{f}_{\gamma }\sim \mathrm{log}{f}_{{\rm{X}}}﹩.
Paper: The Spectral Energy Distributions for 4FGL Blazars
Authors: J. H. Yang, J. H. Fan, Y. Liu, M. X. Tuo, Z. Y. Pei, W. X. Yang, Y. H. Yuan, S. L. He, S. H. Wang, X. C. Wang, X. J. Chen, X. H. Qu, Q. Cao, Q. Y. Tao, Y. L. Zhang, C. Q. Liu, J. J. Nie, L. F. Liu, D. K. Jiang, A. N. Jiang, B. Liu, R. S. Yang
Figure caption: The correlations between two luminosities: (a) ﹩\mathrm{log}{L}_{\gamma }﹩ and ﹩\mathrm{log}{L}_{{\rm{R}}}﹩, (b) ﹩\mathrm{log}{L}_{\gamma }﹩ and ﹩\mathrm{log}{L}_{{\rm{O}}}﹩, (c) ﹩\mathrm{log}{L}_{\gamma }﹩ and ﹩\mathrm{log}{L}_{{\rm{X}}}﹩, and (d) ﹩\mathrm{log}{L}_{\gamma }﹩ and ﹩\mathrm{log}{L}_{{\rm{p}}}﹩.
Paper: Integrated Geostationary Solar Energetic Particle Events Catalog: GSEP
Authors: Sumanth Rotti, Berkay Aydin, Manolis K. Georgoulis, Petrus C. Martens
Figure caption: Time profile of an SEP event occurring between 2002 January 14 and 16. The time series begins with the event start time (2002 January 14 00:30:00) according to the PSEP catalog. A solar flare of magnitude M4.4 occurs at 05:30:00 followed by a CME 6 minutes later from the western limb. The second arrow points to the onset of the SEP event (2002 January 15 05:35:00) as considered by the CDAW-SEP and NOAA-SEP catalogs. The event start time differs by >29 hr compared to PSEP. For this event, both catalogs report the same solar source (flare and CME). We retain the event onset as reported in the CDAW-SEP list.
Paper: Integrated Geostationary Solar Energetic Particle Events Catalog: GSEP
Authors: Sumanth Rotti, Berkay Aydin, Manolis K. Georgoulis, Petrus C. Martens
Figure caption: Time series of an SEP event showing the variation in the fluxes captured by the GOES-05 (“secondary”) and GOES-06 (“primary”) satellites.
Paper: Integrated Geostationary Solar Energetic Particle Events Catalog: GSEP
Authors: Sumanth Rotti, Berkay Aydin, Manolis K. Georgoulis, Petrus C. Martens
Figure caption: Process flow diagram indicating the background work of GOES data inspection, verification, and slicing in this work. The time-series slices are generated from the GSEP metadata. For details, see the text.
Paper: 3D Selection of 167 Substellar Companions to Nearby Stars
Authors: Fabo Feng, R. Paul Butler, Steven S. Vogt, Matthew S. Clement, C. G. Tinney, Kaiming Cui, Masataka Aizawa, Hugh R. A. Jones, J. Bailey, Jennifer Burt, B. D. Carter, Jeffrey D. Crane, Francesco Flammini Dotti, Bradford Holden, Bo Ma, Masahiro Ogihara, Rebecca Oppenheimer, S. J. O'Toole, Stephen A. Shectman, Robert A. Wittenmyer, Sharon X. Wang, D. J. Wright, Yifan Xuan
Figure caption: The 61 multicompanion systems identified in this work. The yellow dots represent stellar companions with masses higher than 75 M Jup, the brown dots represent BDs with mass ranges from 13 M Jup to 75 M Jup, and the blue dots represent planet companions with masses lower than 13 M Jup. The semimajor axis is used as a proxy for the separation from the host star for the companions identified in this work, while the binary separation is used for the EDR3 wide-binary catalog given by El-Badry et al. (2021). The solar system planets are put on the black horizontal line for reference. The masses of the solar system planets are amplified by 10 times for better visualization. The dot size represents the companion mass, and the size for stellar companions is truncated to the largest size.
Paper: 3D Selection of 167 Substellar Companions to Nearby Stars
Authors: Fabo Feng, R. Paul Butler, Steven S. Vogt, Matthew S. Clement, C. G. Tinney, Kaiming Cui, Masataka Aizawa, Hugh R. A. Jones, J. Bailey, Jennifer Burt, B. D. Carter, Jeffrey D. Crane, Francesco Flammini Dotti, Bradford Holden, Bo Ma, Masahiro Ogihara, Rebecca Oppenheimer, S. J. O'Toole, Stephen A. Shectman, Robert A. Wittenmyer, Sharon X. Wang, D. J. Wright, Yifan Xuan
Figure caption: Mass distributions of the substellar companions detected in this work. The samples are divided into 10 bins. The upper and lower panels show the distributions of the companions with relative mass uncertainties of less than 100% and 20%, respectively. The left and right panels show the distributions over the companion mass and the companion–host mass ratio, respectively. The error bars are determined by assuming that the number of detected companions follows a Poisson distribution.
Paper: 3D Selection of 167 Substellar Companions to Nearby Stars
Authors: Fabo Feng, R. Paul Butler, Steven S. Vogt, Matthew S. Clement, C. G. Tinney, Kaiming Cui, Masataka Aizawa, Hugh R. A. Jones, J. Bailey, Jennifer Burt, B. D. Carter, Jeffrey D. Crane, Francesco Flammini Dotti, Bradford Holden, Bo Ma, Masahiro Ogihara, Rebecca Oppenheimer, S. J. O'Toole, Stephen A. Shectman, Robert A. Wittenmyer, Sharon X. Wang, D. J. Wright, Yifan Xuan
Figure caption: Bayes factor periodograms (BFPs; Feng et al. 2017) and phase curves for the 600 and 1000 day signals detected in the RV data for HD 81817. Upper panels: the left panel shows the BFP for the raw data, while the right panel shows the BFP for the residual with the 600 day signal subtracted. The red lines in the upper panels indicate the periods of the two signals. The dashed and dotted lines show the thresholds of lnBF = 5 and 0, respectively. Lower panels: the red curves in the lower panels show the best fit corresponding to the parameter values at the MAP. The black error bars represent 10 binned data points.
Paper: 3D Selection of 167 Substellar Companions to Nearby Stars
Authors: Fabo Feng, R. Paul Butler, Steven S. Vogt, Matthew S. Clement, C. G. Tinney, Kaiming Cui, Masataka Aizawa, Hugh R. A. Jones, J. Bailey, Jennifer Burt, B. D. Carter, Jeffrey D. Crane, Francesco Flammini Dotti, Bradford Holden, Bo Ma, Masahiro Ogihara, Rebecca Oppenheimer, S. J. O'Toole, Stephen A. Shectman, Robert A. Wittenmyer, Sharon X. Wang, D. J. Wright, Yifan Xuan
Figure caption: Orbits of 16 companions with separations larger than 500 mas from their host stars. For a multigiant system, the black line represents the giant companion on the widest orbit, while the red line represents the other companions with orbital periods longer than 1000 days in the system. The positions of the companions at some epochs are also denoted by the corresponding years. The black cross in each panel represents the host star.
Paper: 3D Selection of 167 Substellar Companions to Nearby Stars
Authors: Fabo Feng, R. Paul Butler, Steven S. Vogt, Matthew S. Clement, C. G. Tinney, Kaiming Cui, Masataka Aizawa, Hugh R. A. Jones, J. Bailey, Jennifer Burt, B. D. Carter, Jeffrey D. Crane, Francesco Flammini Dotti, Bradford Holden, Bo Ma, Masahiro Ogihara, Rebecca Oppenheimer, S. J. O'Toole, Stephen A. Shectman, Robert A. Wittenmyer, Sharon X. Wang, D. J. Wright, Yifan Xuan
Figure caption: A summary of our simulations studying the stability of an Earth-mass planet in the HZs of our various systems identified in Table 2. The color of each point identifies whether the Earth analog survived the simulation (green points) or was lost via ejection or collision (blue points). The size of each point corresponds to the mass of each planet in our various simulations.
Paper: 3D Selection of 167 Substellar Companions to Nearby Stars
Authors: Fabo Feng, R. Paul Butler, Steven S. Vogt, Matthew S. Clement, C. G. Tinney, Kaiming Cui, Masataka Aizawa, Hugh R. A. Jones, J. Bailey, Jennifer Burt, B. D. Carter, Jeffrey D. Crane, Francesco Flammini Dotti, Bradford Holden, Bo Ma, Masahiro Ogihara, Rebecca Oppenheimer, S. J. O'Toole, Stephen A. Shectman, Robert A. Wittenmyer, Sharon X. Wang, D. J. Wright, Yifan Xuan
Figure caption: An example evolutionary scheme from one of our dynamical simulations, studying the low-mass companion and Jupiter analog in HD 205158. The pericenter and apocenter for each body are plotted with red (HD 205158 B) and blue (HD 205158 b) lines.
Paper: 3D Selection of 167 Substellar Companions to Nearby Stars
Authors: Fabo Feng, R. Paul Butler, Steven S. Vogt, Matthew S. Clement, C. G. Tinney, Kaiming Cui, Masataka Aizawa, Hugh R. A. Jones, J. Bailey, Jennifer Burt, B. D. Carter, Jeffrey D. Crane, Francesco Flammini Dotti, Bradford Holden, Bo Ma, Masahiro Ogihara, Rebecca Oppenheimer, S. J. O'Toole, Stephen A. Shectman, Robert A. Wittenmyer, Sharon X. Wang, D. J. Wright, Yifan Xuan
Figure caption: Companion–host contrasts in the J, H, and K bands, by assuming ages of 0.1, 1, and 10 Gyr for the systems.
Paper: 3D Selection of 167 Substellar Companions to Nearby Stars
Authors: Fabo Feng, R. Paul Butler, Steven S. Vogt, Matthew S. Clement, C. G. Tinney, Kaiming Cui, Masataka Aizawa, Hugh R. A. Jones, J. Bailey, Jennifer Burt, B. D. Carter, Jeffrey D. Crane, Francesco Flammini Dotti, Bradford Holden, Bo Ma, Masahiro Ogihara, Rebecca Oppenheimer, S. J. O'Toole, Stephen A. Shectman, Robert A. Wittenmyer, Sharon X. Wang, D. J. Wright, Yifan Xuan
Figure caption: Similar to Figure 6, but for other targets.
Paper: KW-Sun: The Konus-Wind Solar Flare Database in Hard X-Ray and Soft Gamma-Ray Ranges
Authors: A. L. Lysenko, M. V. Ulanov, A. A. Kuznetsov, G. D. Fleishman, D. D. Frederiks, L. K. Kashapova, Z. Ya. Sokolova, D. S. Svinkin, A. E. Tsvetkova
Figure caption: Example of a background-subtracted multichannel energy spectrum for the X9.3 class solar flare on 2017 September 6 in the first energy range (PHA1, black) and the second energy range (PHA2, red). The gray shaded area marks the PHA1/PHA2 overlapping range.
Paper: KW-Sun: The Konus-Wind Solar Flare Database in Hard X-Ray and Soft Gamma-Ray Ranges
Authors: A. L. Lysenko, M. V. Ulanov, A. A. Kuznetsov, G. D. Fleishman, D. D. Frederiks, L. K. Kashapova, Z. Ya. Sokolova, D. S. Svinkin, A. E. Tsvetkova
Figure caption: KW-Sun web interface to the data for a specific flare, which displays the flare light curves in G1, G2, G3 and provides links to the data. Horizontal dashed lines represent background levels, and vertical dotted lines in the plot indicate time intervals of multichannel spectrum accumulation.
Paper: KW-Sun: The Konus-Wind Solar Flare Database in Hard X-Ray and Soft Gamma-Ray Ranges
Authors: A. L. Lysenko, M. V. Ulanov, A. A. Kuznetsov, G. D. Fleishman, D. D. Frederiks, L. K. Kashapova, Z. Ya. Sokolova, D. S. Svinkin, A. E. Tsvetkova
Figure caption: Occultations in the Konus-Wind solar flare time profiles for the S1 (left) and S2 (right) detectors. Gray shaded regions mark time intervals when the Sun was occulted partially or fully by other instruments or the spacecraft (S/C) structures. These intervals are removed from the KW-Sun light curves.