adsabs/AstroCLIMB huggingface dataset:
Paper: The Detectability of CH4/CO2/CO and N2O Biosignatures Through Reflection Spectroscopy of Terrestrial Exoplanets
Authors: Armen Tokadjian, Renyu Hu, Mario Damiano
Figure caption: Same as Figure 1, but for a Proterozoic Earth-like planet with VMR﹩{}_{{{\rm{N}}}_{2}{\rm{O}}}={10}^{-3}﹩. The spectrum does not have any dominating features, but the absorption of numerous molecules are evident. N2O features (brown) can be found at numerous wavelengths past 1 μm, particularly at 1.113, 1.283, 1.383, 1.516, 1.585, 1.671, and 1.777 μm.
Paper: Variabilities of Methanol Maser and Thermal Molecular Lines from an Accretion Burst Source G358.93-0.03
Authors: Shi-jie Zhang, Xi Chen, Yan-Kun Zhang, Dan Miao, Deng-Rong Lu, Bing-Gang Ju
Figure caption: Exponential decay fitting for the eight velocity components from six methanol maser transitions at the 3 mm band. The black solid point represents the observed maximum integrated intensity for each component. The best exponential decay fitting line is shown by a solid curve. As a comparison, two velocity components at the 6.7 GHz methanol transition are given in the lower two panels.
Paper: Variabilities of Methanol Maser and Thermal Molecular Lines from an Accretion Burst Source G358.93-0.03
Authors: Shi-jie Zhang, Xi Chen, Yan-Kun Zhang, Dan Miao, Deng-Rong Lu, Bing-Gang Ju
Figure caption: The relationships between the maser decay timescales and their absolute velocity offsets relative to the source systemic velocity (left panel) and between the maser decay timescales and their expected maximum of integrated intensities (right panel). The solid lines represent the best linear fits to these relationships. A weak anticorrelation is obtained with a correlation coefficient of 0.55 in the left panel, but no correlation (with a correlation coefficient of 0.05) is found in the right panel.
Paper: Variabilities of Methanol Maser and Thermal Molecular Lines from an Accretion Burst Source G358.93-0.03
Authors: Shi-jie Zhang, Xi Chen, Yan-Kun Zhang, Dan Miao, Deng-Rong Lu, Bing-Gang Ju
Figure caption: Comparison of spectra of N2H+ and HCO+ detected in the burst and postburst stages. The dashed profiles represent the observed spectra, while the solid profiles are the Gaussian fittings to the spectra.
Paper: Variabilities of Methanol Maser and Thermal Molecular Lines from an Accretion Burst Source G358.93-0.03
Authors: Shi-jie Zhang, Xi Chen, Yan-Kun Zhang, Dan Miao, Deng-Rong Lu, Bing-Gang Ju
Figure caption: Integrated intensity ratios of the detected molecular lines between the burst and postburst stages. For multipeak lines (l−C3H, HCN, N2H+), the line-integrated intensities of the main components are used in the analysis.
Paper: Variabilities of Methanol Maser and Thermal Molecular Lines from an Accretion Burst Source G358.93-0.03
Authors: Shi-jie Zhang, Xi Chen, Yan-Kun Zhang, Dan Miao, Deng-Rong Lu, Bing-Gang Ju
Figure caption: The maser velocity components adopted for variability analysis. Each transition is represented by a single epoch. In the analysis, a total of eight velocity components from six methanol transition lines were extracted to produce the integrated intensities enclosed by the dashed boxes.
Paper: Variabilities of Methanol Maser and Thermal Molecular Lines from an Accretion Burst Source G358.93-0.03
Authors: Shi-jie Zhang, Xi Chen, Yan-Kun Zhang, Dan Miao, Deng-Rong Lu, Bing-Gang Ju
Figure caption: Spectra of the thermal molecular lines (12 in total) detected in the burst and postburst stages. The dashed profiles represent the observed spectra, while the solid profiles are the Gaussian fittings to the spectra.
Paper: Dynamical Viability Assessment for Habitable Worlds Observatory Targets
Authors: Stephen R. Kane, Zhexing Li, Margaret C. Turnbull, Courtney D. Dressing, Caleb K. Harada
Figure caption: HZ and planetary orbits for four of the systems in our sample: HD 10647 (top left), HD 39091 (pi Men; top right), HD 75732 (55 Cancri; bottom left), HD 95128 (47 Uma; bottom right). The orbits are labeled by planet designation. The extent of the HZ is shown in green, where light green and dark green indicate the CHZ and OHZ, respectively.
Paper: Dynamical Viability Assessment for Habitable Worlds Observatory Targets
Authors: Stephen R. Kane, Zhexing Li, Margaret C. Turnbull, Courtney D. Dressing, Caleb K. Harada
Figure caption: Distribution of semimajor axes and eccentricities for all planets included in our sample. The size of the plotted data are logarithmically proportional to the planet mass.
Paper: Pixel-level Terrain Processing of the Martian Surface from Moderate Resolution Images of Tianwen-1
Authors: Dingxin Liu, Wei Yan, Jianjun Liu, Xingguo Zeng, Wangli Chen, Xin Ren
Figure caption: (a) The MoRIC image pixel scale is 96 m pixel−1 and (b) The cropped MoRIC-DEM pixel scale is 160 m pixel−1, the range of the DEM is 180 km × 283 km.
Paper: Pixel-level Terrain Processing of the Martian Surface from Moderate Resolution Images of Tianwen-1
Authors: Dingxin Liu, Wei Yan, Jianjun Liu, Xingguo Zeng, Wangli Chen, Xin Ren
Figure caption: Viewing Geometry. i is the incidence angle, e is the emission angle, g is the phase angle, and n is the normal vector.
Paper: Pixel-level Terrain Processing of the Martian Surface from Moderate Resolution Images of Tianwen-1
Authors: Dingxin Liu, Wei Yan, Jianjun Liu, Xingguo Zeng, Wangli Chen, Xin Ren
Figure caption: SFS results with geometric control area. (a) MoRIC image (b) hill-shade rendering of initial DEM, (c) hill-shade rendering of SFS results, and (d) hill-shade rendering of HRSC-DEM. Note that due to the HRSC-DEM being a mosaic of different orbits, the data quality on the right side is superior to that on the left side.
Paper: Pixel-level Terrain Processing of the Martian Surface from Moderate Resolution Images of Tianwen-1
Authors: Dingxin Liu, Wei Yan, Jianjun Liu, Xingguo Zeng, Wangli Chen, Xin Ren
Figure caption: SFS results without geometric control area. (a) MoRIC image. (b) Hill-shade rendering of Initial DEM, (c) hill-shade rendering of SFS results, and hill-shade rendering of (d) CTX-DEM.
Paper: Pixel-level Terrain Processing of the Martian Surface from Moderate Resolution Images of Tianwen-1
Authors: Dingxin Liu, Wei Yan, Jianjun Liu, Xingguo Zeng, Wangli Chen, Xin Ren
Figure caption: Elevation profiles and corresponding image data. (a) Elevation profile for Profile 1. (b) Elevation profile for Profile 2. (c) Close-up view of the MoRIC-DEM corresponding to the black-shaded region within Figure 5(a). (d) SFS processing results for the region. (e) Original MoRIC image data corresponding to the region.
Paper: Fundamental Parameters of a Binary System Consisting of a Red Dwarf and a Compact Star
Authors: Xu Ding, KaiFan Ji, ZhiMing Song, NianPing Liu, JianPing Xiong, Qiyuan Cheng, ChuanJun Wang, JinLiang Wang, DeQing Wang, ShouSheng He
Figure caption: The RANSAC algorithm is used to fit the quiescent flux. This algorithm effectively removes outliers and selects inliers for fitting.
Paper: Pixel-level Terrain Processing of the Martian Surface from Moderate Resolution Images of Tianwen-1
Authors: Dingxin Liu, Wei Yan, Jianjun Liu, Xingguo Zeng, Wangli Chen, Xin Ren
Figure caption: PCC trend plot corresponding to candidate μ. (a) is a trend diagram of all candidate μ, and (b) is a trend diagram of the final μ obtained according to the global bisection algorithm in flowchart 2.
Paper: Pixel-level Terrain Processing of the Martian Surface from Moderate Resolution Images of Tianwen-1
Authors: Dingxin Liu, Wei Yan, Jianjun Liu, Xingguo Zeng, Wangli Chen, Xin Ren
Figure caption: Flowchart of the global bisection search algorithm.
Paper: Pixel-level Terrain Processing of the Martian Surface from Moderate Resolution Images of Tianwen-1
Authors: Dingxin Liu, Wei Yan, Jianjun Liu, Xingguo Zeng, Wangli Chen, Xin Ren
Figure caption: Elevation profile results of profile 3 and 4.
Paper: Pixel-level Terrain Processing of the Martian Surface from Moderate Resolution Images of Tianwen-1
Authors: Dingxin Liu, Wei Yan, Jianjun Liu, Xingguo Zeng, Wangli Chen, Xin Ren
Figure caption: (a) “Elevation difference map” between CTX-DEM and MoRIC-DEM. (b) “Elevation difference map” between CTX-DEM and SFS-DEM. (c) Histogram of elevation differences.
Paper: Dynamical Viability Assessment for Habitable Worlds Observatory Targets
Authors: Stephen R. Kane, Zhexing Li, Margaret C. Turnbull, Courtney D. Dressing, Caleb K. Harada
Figure caption: HZ and planetary orbits for four of the systems in our sample: HD 114613 (top left), HD 147513 (top right), HD 160691 (bottom left), HD 192310 (bottom right). The orbits are labeled by planet designation. The extent of the HZ is shown in green, where light green and dark green indicate the CHZ and OHZ, respectively.
Paper: Dynamical Viability Assessment for Habitable Worlds Observatory Targets
Authors: Stephen R. Kane, Zhexing Li, Margaret C. Turnbull, Courtney D. Dressing, Caleb K. Harada
Figure caption: Percentage of the simulation that the injected Earth-mass planet survived as a function of the initial semimajor axis, where the CHZ is shown in light green and the OHZ is shown in dark green. Shown, from top to bottom, are the results for HD 10647, HD 39091 (pi Men), HD 75732 (55 Cancri), and HD 95128.
Paper: Dynamical Viability Assessment for Habitable Worlds Observatory Targets
Authors: Stephen R. Kane, Zhexing Li, Margaret C. Turnbull, Courtney D. Dressing, Caleb K. Harada
Figure caption: Percentage of the simulation that the injected Earth-mass planet survived as a function of the initial semimajor axis, where the CHZ is shown in light green and the OHZ is shown in dark green. Shown, from top to bottom, are the results for HD 114613, HD 147513, HD 160691, and HD 192310.
Paper: Dynamical Viability Assessment for Habitable Worlds Observatory Targets
Authors: Stephen R. Kane, Zhexing Li, Margaret C. Turnbull, Courtney D. Dressing, Caleb K. Harada
Figure caption: Histogram of the DVHZ calculations for all 30 of the known systems studied in this work.
Paper: Dynamical Evolution of Four Old Galactic Open Clusters Traced by Their Constituent Stars with Gaia DR3
Authors: Shanmugha Balan, Khushboo K. Rao, Kaushar Vaidya, Manan Agarwal, Souradeep Bhattacharya
Figure caption: Positions of sources in Berkeley 39, Collinder 261, NGC 6819 and NGC 7789 in galactocentric coordinates, arranged row-wise. Different populations are represented by colored dots as per the inset legend, while the black dotted line represents the line-of-sight to the cluster and the solid line represents the cluster orbital direction.
Paper: Dynamical Evolution of Four Old Galactic Open Clusters Traced by Their Constituent Stars with Gaia DR3
Authors: Shanmugha Balan, Khushboo K. Rao, Kaushar Vaidya, Manan Agarwal, Souradeep Bhattacharya
Figure caption: CMDs with fitted single-star PARSEC isochrones (gray solid line) and equal-mass binary isochrones (magneta dashed line). The BSS are shown as blue squares, the RGBs are shown as red triangles, the MSTOs are shown as black squares, and the upper and lower main-sequence stars are shown as green and yellow dots. NGC 6819 and NGC 7789 have an equal mass binary track above the MS, and the selected binaries are shown as light blue dots (see Section 2.3 for their selection criterion). Every cluster member is divided into 5 bins based on their magnitude (G) and the average error in G for each bin is calculated. The center of these bins (dark gray dots), and the average error in G scaled ×100 (light gray vertical lines) are shown in the right side of each plot.
Paper: Dynamical Evolution of Four Old Galactic Open Clusters Traced by Their Constituent Stars with Gaia DR3
Authors: Shanmugha Balan, Khushboo K. Rao, Kaushar Vaidya, Manan Agarwal, Souradeep Bhattacharya
Figure caption: Velocities of the sources in Berkeley 39, NGC 6819, NGC 7789 in galactocentric coordinates, arranged column wise. Different populations are represented by colored dots as per the inset legend.
Paper: Dynamical Evolution of Four Old Galactic Open Clusters Traced by Their Constituent Stars with Gaia DR3
Authors: Shanmugha Balan, Khushboo K. Rao, Kaushar Vaidya, Manan Agarwal, Souradeep Bhattacharya
Figure caption: Proper motion distribution with overlaid density contour plots of the four clusters. The BSS are shown in blue, RGBs in red, and MSTOs in black. The populations are arranged in decreasing order of mass from top to bottom.
Paper: Dynamical Evolution of Four Old Galactic Open Clusters Traced by Their Constituent Stars with Gaia DR3
Authors: Shanmugha Balan, Khushboo K. Rao, Kaushar Vaidya, Manan Agarwal, Souradeep Bhattacharya
Figure caption: CRDs of the four clusters plotted as a fraction of the sources in each population against the distance from the cluster center normalized by the core radius. The BSS are shown in deep blue, RGBs in red, MSTOs in black, UMS in green, and LMS in yellow. For NGC 6819 and NGC 7789, the additional binary populations are shown in light blue.