adsabs/AstroCLIMB huggingface dataset:
Paper: DECam Multimessenger Astrophysics Pipeline. I. From Raw Data to Single-exposure Candidates
Authors: Shenming Fu, Thomas Matheson, Aaron Meisner, Yuanyuan Zhang, Sebastián Vicencio, Destry Saul
Figure caption: DECam DDF SN candidate DC21bkrj in the g, r, and i bands.
Paper: DECam Multimessenger Astrophysics Pipeline. I. From Raw Data to Single-exposure Candidates
Authors: Shenming Fu, Thomas Matheson, Aaron Meisner, Yuanyuan Zhang, Sebastián Vicencio, Destry Saul
Figure caption: Flares of an M-type star in the g band observed in the DWF program, with the difference image at the first flux peak (visit 617324; MJD 57790.278).
Paper: DECam Multimessenger Astrophysics Pipeline. I. From Raw Data to Single-exposure Candidates
Authors: Shenming Fu, Thomas Matheson, Aaron Meisner, Yuanyuan Zhang, Sebastián Vicencio, Destry Saul
Figure caption: Variable stars in the diffuse dwarf galaxy Crater II (both in the g band): V11 (top), V19 (bottom).
Paper: A Geodetic and Astrometric VLBI Experiment at 22/43/88/132 GHz
Authors: Shuangjing Xu, Taehyun Jung, Bo Zhang, Ming Hui Xu, Do-Young Byun, Xuan He, Nobuyuki Sakai, Oleg Titov, Fengchun Shu, Hyo-Ryoung Kim, Jungho Cho, Sung-Moon Yoo, Byung-Kyu Choi, Woo Kyoung Lee, Yan Sun, Xiaofeng Mai, Guangli Wang
Figure caption: Comparison of the SNR with and without FPT within a 2 minutes scan length. The left figure shows the percentage increase in SNR after using FPT, and the right figure compares the SNR of weak sources (SNR < 15). The dashed lines indicate the fourfit detection limit (SNR = 7). For clarity, the results with an SNR below 6 using FPT are not shown.
Paper: A Geodetic and Astrometric VLBI Experiment at 22/43/88/132 GHz
Authors: Shuangjing Xu, Taehyun Jung, Bo Zhang, Ming Hui Xu, Do-Young Byun, Xuan He, Nobuyuki Sakai, Oleg Titov, Fengchun Shu, Hyo-Ryoung Kim, Jungho Cho, Sung-Moon Yoo, Byung-Kyu Choi, Woo Kyoung Lee, Yan Sun, Xiaofeng Mai, Guangli Wang
Figure caption: Comparison atmospheric phase fluctuations with self detection (ϕ Self) and FPT (ϕ FPT) method using a strong source 3C 279 on KTN-KYS baseline. The four panels represent distinct frequency bands. The 2π ambiguity of phase is ignored for clarity.
Paper: A Geodetic and Astrometric VLBI Experiment at 22/43/88/132 GHz
Authors: Shuangjing Xu, Taehyun Jung, Bo Zhang, Ming Hui Xu, Do-Young Byun, Xuan He, Nobuyuki Sakai, Oleg Titov, Fengchun Shu, Hyo-Ryoung Kim, Jungho Cho, Sung-Moon Yoo, Byung-Kyu Choi, Woo Kyoung Lee, Yan Sun, Xiaofeng Mai, Guangli Wang
Figure caption: The histogram of measurement noise for group delay and delay rate produced by fourfit on the KYS-KTN baseline. Different bands are represented by different colors.
Paper: A Geodetic and Astrometric VLBI Experiment at 22/43/88/132 GHz
Authors: Shuangjing Xu, Taehyun Jung, Bo Zhang, Ming Hui Xu, Do-Young Byun, Xuan He, Nobuyuki Sakai, Oleg Titov, Fengchun Shu, Hyo-Ryoung Kim, Jungho Cho, Sung-Moon Yoo, Byung-Kyu Choi, Woo Kyoung Lee, Yan Sun, Xiaofeng Mai, Guangli Wang
Figure caption: Same as Figure 1, but for a weaker source 0642+449.
Paper: Candidates for Substellar Members of the Orion Nebula Cluster from JWST/NIRCam 
Authors: K. L. Luhman
Figure caption: Color–color and color–magnitude diagrams for point sources in JWST/NIRCam images of the ONC (points and circles). Three of the diagrams include data for TWA 27B and three late-type members of IC 348 (cross and triangles; K. L. Luhman et al. 2023, 2024). The red lines in the left diagrams are reddening vectors used for selecting brown dwarf candidates.
Paper: Candidates for Substellar Members of the Orion Nebula Cluster from JWST/NIRCam 
Authors: K. L. Luhman
Figure caption: Standard deviation of the differences in NIRCam photometry between two epochs of images vs. the aperture radius for the photometry. These data were measured for bright stars in archival images of a field in the LMC obtained in the F150W and F200W filters.
Paper: Candidates for Substellar Members of the Orion Nebula Cluster from JWST/NIRCam 
Authors: K. L. Luhman
Figure caption: Color–color and color–magnitude diagrams for point source brown dwarf candidates that are selected based on their positions below the red boundaries in the left diagrams (Table 2).
Paper: Candidates for Substellar Members of the Orion Nebula Cluster from JWST/NIRCam 
Authors: K. L. Luhman
Figure caption: Color–color and color–magnitude diagrams for the JuMBO candidates from PM23.
Paper: Candidates for Substellar Members of the Orion Nebula Cluster from JWST/NIRCam 
Authors: K. L. Luhman
Figure caption: Color–color and color–magnitude diagrams for proplyds and other sources with extended emission (Table 3).
Paper:  Yuti: A General-purpose Transit Simulator for Arbitrary Shaped Objects Orbiting Stars
Authors: Ushasi Bhowmick, Vikram Khaire
Figure caption: Workflow of the transit simulation. (I) shows the modeling of the stellar source with a uniform, limb-darkened, and limb-darkened elliptical distribution. (II) shows the definition of three arbitrary shapes (cube, ellipsoid, and double pyramid) rotated by a random angle around an axis, using corners and edges. (III) shows the subsequent projected subshape. In (IV), the subshape is put in orbit around the star and the points inside the subshape are highlighted. The fraction of in points to out is used to calculate the area of overlap.
Paper:  Yuti: A General-purpose Transit Simulator for Arbitrary Shaped Objects Orbiting Stars
Authors: Ushasi Bhowmick, Vikram Khaire
Figure caption: Demonstration of the Monte Carlo technique for numerical area calculation. (A) shows an outer circle and an inner shape, with each point having a certain probability of lying on the inside shape. A large number of sampled points is needed for an accurate estimate of the overlapped area between the background circle and foreground shape. (B) shows the ray casting technique, which is a method to evaluate whether a point lies inside or outside a particular shape by drawing a ray in any direction and calculating its intersection with the edges of the shape. An even number of intersections imply that the point is outside the shape, and an odd number of intersections means that the point is inside the shape.
Paper: A Close Binary Lens Revealed by the Microlensing Event Gaia20bof
Authors: E. Bachelet, P. Rota, V. Bozza, P. Zieliński, Y. Tsapras, M. Hundertmark, J. Wambsganss, Ł. Wyrzykowski, P. J. Mikołajczyk, R. A. Street, R. Figuera Jaimes, A. Cassan, M. Dominik, D. A. H. Buckley, S. Awiphan, N. Nakhaharutai, S. Zola, K. A. Rybicki, M. Gromadzki, K. Howil, N. Ihanec, M. Jabłońska, K. Kruszyńska, K. Kruszyńska, U. Pylypenko, M. Ratajczak, M. Sitek, M. Rabus
Figure caption: (Left) PARSEC stellar isochrones for 9, 9.5, and 10 Gyr with a fixed metallicity of −0.5. The source is most likely an old subgiant. (Middle) Source angular radius based on the spectra models as a function of the source distance and age (color-coded). The points are derived from the template matching MCMC chains and the stellar isochrones. (Right) Source distance based on the Gaia source measurements from the model (G  s  ∼ 16 mag) and the extinction estimated from the template matching modeling. Black dashed lines indicates the 1σ confidence region from the parallax measurement of Gaia.
Paper: A Close Binary Lens Revealed by the Microlensing Event Gaia20bof
Authors: E. Bachelet, P. Rota, V. Bozza, P. Zieliński, Y. Tsapras, M. Hundertmark, J. Wambsganss, Ł. Wyrzykowski, P. J. Mikołajczyk, R. A. Street, R. Figuera Jaimes, A. Cassan, M. Dominik, D. A. H. Buckley, S. Awiphan, N. Nakhaharutai, S. Zola, K. A. Rybicki, M. Gromadzki, K. Howil, N. Ihanec, M. Jabłońska, K. Kruszyńska, K. Kruszyńska, U. Pylypenko, M. Ratajczak, M. Sitek, M. Rabus
Figure caption: The VLT/X-Shooter spectrum (blue) and the best-matching fit of synthetic spectrum (red) generated for specific atmospheric parameters are presented. The Ca II triplet (top panel) and the Hα line (middle panel), as well as the Ca H and K lines (bottom panel), are visible.
Paper: A Close Binary Lens Revealed by the Microlensing Event Gaia20bof
Authors: E. Bachelet, P. Rota, V. Bozza, P. Zieliński, Y. Tsapras, M. Hundertmark, J. Wambsganss, Ł. Wyrzykowski, P. J. Mikołajczyk, R. A. Street, R. Figuera Jaimes, A. Cassan, M. Dominik, D. A. H. Buckley, S. Awiphan, N. Nakhaharutai, S. Zola, K. A. Rybicki, M. Gromadzki, K. Howil, N. Ihanec, M. Jabłońska, K. Kruszyńska, K. Kruszyńska, U. Pylypenko, M. Ratajczak, M. Sitek, M. Rabus
Figure caption: The two spectra from SALT (black) and X-Shooter (red), as well as the best models, are visible. The gray vertical lines indicates telluric bands, where the data were not used for the modeling.
Paper: A Survey of Galaxy Pairs in the SDSS Photometric Images based on Faster-RCNN
Authors: Chen-hui Shi, 晨辉 史, Hai-feng Yang, 海峰 杨, Jiang-hui Cai, 江辉 蔡, Li-chan Zhou, 立婵 周, Yan-ting He, 艳婷 贺, Mei-hong Su, 美红 苏, Xu-jun Zhao, 旭俊 赵, Ya-ling Xun, 亚玲 荀
Figure caption: Some irregular pairs in results; No. 25–No. 32 are pairs with prominent tidal tails, No. 33–No. 40 are close merging pairs, No. 41–No. 44 are targets with spread-point sources, and No. 45–No. 52 are pairs with unusual color.
Paper: A Survey of Galaxy Pairs in the SDSS Photometric Images based on Faster-RCNN
Authors: Chen-hui Shi, 晨辉 史, Hai-feng Yang, 海峰 杨, Jiang-hui Cai, 江辉 蔡, Li-chan Zhou, 立婵 周, Yan-ting He, 艳婷 贺, Mei-hong Su, 美红 苏, Xu-jun Zhao, 旭俊 赵, Ya-ling Xun, 亚玲 荀
Figure caption: Some galaxy pairs in detected physical galaxy pairs. For the convenience of analysis, we renumber these samples; No. 1–No. 8 are close pairs, No. 9–No. 16 are projection-separated pairs, and No. 17–No. 24 are edge-on pairs.
Paper: A Survey of Galaxy Pairs in the SDSS Photometric Images based on Faster-RCNN
Authors: Chen-hui Shi, 晨辉 史, Hai-feng Yang, 海峰 杨, Jiang-hui Cai, 江辉 蔡, Li-chan Zhou, 立婵 周, Yan-ting He, 艳婷 贺, Mei-hong Su, 美红 苏, Xu-jun Zhao, 旭俊 赵, Ya-ling Xun, 亚玲 荀
Figure caption: Fake samples in the confirmed physical galaxy pairs. They are detected as visual galaxy pairs and have passed the redshift verification because they contain two redshift values whose difference is less than 0.0008. However, their redshift positions are located in one galaxy.
Paper: A Survey of Galaxy Pairs in the SDSS Photometric Images based on Faster-RCNN
Authors: Chen-hui Shi, 晨辉 史, Hai-feng Yang, 海峰 杨, Jiang-hui Cai, 江辉 蔡, Li-chan Zhou, 立婵 周, Yan-ting He, 艳婷 贺, Mei-hong Su, 美红 苏, Xu-jun Zhao, 旭俊 赵, Ya-ling Xun, 亚玲 荀
Figure caption: Seven galaxy pairs in different morphologies and their spectra. Two spectra on the right correspond to the two galaxies in the left image.
Paper: A Survey of Galaxy Pairs in the SDSS Photometric Images based on Faster-RCNN
Authors: Chen-hui Shi, 晨辉 史, Hai-feng Yang, 海峰 杨, Jiang-hui Cai, 江辉 蔡, Li-chan Zhou, 立婵 周, Yan-ting He, 艳婷 贺, Mei-hong Su, 美红 苏, Xu-jun Zhao, 旭俊 赵, Ya-ling Xun, 亚玲 荀
Figure caption: Distribution of SFRs of all main-sequence galaxies from MPA-JHU.
Paper: A Survey of Galaxy Pairs in the SDSS Photometric Images based on Faster-RCNN
Authors: Chen-hui Shi, 晨辉 史, Hai-feng Yang, 海峰 杨, Jiang-hui Cai, 江辉 蔡, Li-chan Zhou, 立婵 周, Yan-ting He, 艳婷 贺, Mei-hong Su, 美红 苏, Xu-jun Zhao, 旭俊 赵, Ya-ling Xun, 亚玲 荀
Figure caption: Distribution of redshifts, SFRs, u-r, and masses for the training set galaxies.
Paper: A Survey of Galaxy Pairs in the SDSS Photometric Images based on Faster-RCNN
Authors: Chen-hui Shi, 晨辉 史, Hai-feng Yang, 海峰 杨, Jiang-hui Cai, 江辉 蔡, Li-chan Zhou, 立婵 周, Yan-ting He, 艳婷 贺, Mei-hong Su, 美红 苏, Xu-jun Zhao, 旭俊 赵, Ya-ling Xun, 亚玲 荀
Figure caption: Distribution of SFRs for different types of galaxy pairs in the training set.
Paper: A Survey of Galaxy Pairs in the SDSS Photometric Images based on Faster-RCNN
Authors: Chen-hui Shi, 晨辉 史, Hai-feng Yang, 海峰 杨, Jiang-hui Cai, 江辉 蔡, Li-chan Zhou, 立婵 周, Yan-ting He, 艳婷 贺, Mei-hong Su, 美红 苏, Xu-jun Zhao, 旭俊 赵, Ya-ling Xun, 亚玲 荀
Figure caption: Redshift difference of four types of galaxy pairs confirmed by spectraz.
Paper: A Survey of Galaxy Pairs in the SDSS Photometric Images based on Faster-RCNN
Authors: Chen-hui Shi, 晨辉 史, Hai-feng Yang, 海峰 杨, Jiang-hui Cai, 江辉 蔡, Li-chan Zhou, 立婵 周, Yan-ting He, 艳婷 贺, Mei-hong Su, 美红 苏, Xu-jun Zhao, 旭俊 赵, Ya-ling Xun, 亚玲 荀
Figure caption: Redshift and redshift difference distribution of results.
Paper: DECam Multimessenger Astrophysics Pipeline. I. From Raw Data to Single-exposure Candidates
Authors: Shenming Fu, Thomas Matheson, Aaron Meisner, Yuanyuan Zhang, Sebastián Vicencio, Destry Saul
Figure caption: Time evolution of the features and PCA performance for the target (DES15C2eaz, Type II SN). We use the same color scheme as Figure 12. The exposures shown in Figure 13 correspond to the fourth (low teff) and fifth (regular teff) exposures here. We note that for some exposures the number of sources drops to one after the flag filtering, and accordingly, we set the quantiles to 1 and skip the coefficients if that source is the target. All feature quantiles drop when the source is faint. The feature Nos. 2, 3, 8, 9, 10, 13, and 14 are sensitive to the weather. Feature No. 3 is less effective than the others, as it has smaller 〈c  i 〉 (we use red text when ﹩\langle {c}_{i}\rangle \lt 0.5/\sqrt{{N}_{f}}﹩). The EVR drops as the star gets dimmer. Similar to Figure 12, the q P is higher than the average quantile (gray curve) except at low S/N. Also, at the last point q P > q 0, indicating that PCA has the potential to perform better selection than just using the flux S/N only.
Paper: DECam Multimessenger Astrophysics Pipeline. I. From Raw Data to Single-exposure Candidates
Authors: Shenming Fu, Thomas Matheson, Aaron Meisner, Yuanyuan Zhang, Sebastián Vicencio, Destry Saul
Figure caption: PCA results in the Bulge field (A. Saha et al. 2019), which includes many variable stars. We show visits 428030 (left) and 429041 (right) on CCD 28 in the r band, and plot the sources that have PC1 quantile larger than 0.5; the marker opacity is proportional to the PC1 quantile of each source. The corresponding exposure times in MJD are 57115.264 and 57116.403 (the interval is ∼27 hr). We annotate the objects recorded in SIMBAD (M. Wenger et al. 2000). Their stellar types can be identified by name. “OGLE BWC V154” corresponds to “OGLE-BLG-ECL-27776” studied earlier (light curves in Figure 10). “BMB” indicates AGB stars (V. M. Blanco et al. 1984), and “ISOGAL-P J180302.8-295938” is an AGB star (D. K. Ojha et al. 2003) as well. Some short-period stars were also captured because of the timing of their phases, e.g., those names beginning with “OGLE BLG-ECL.” The source detection depends on weather and instrumental conditions. The detected sources without annotation could be noise (especially near CCD edges or saturated stars), or previously uncataloged real objects.
Paper: DECam Multimessenger Astrophysics Pipeline. I. From Raw Data to Single-exposure Candidates
Authors: Shenming Fu, Thomas Matheson, Aaron Meisner, Yuanyuan Zhang, Sebastián Vicencio, Destry Saul
Figure caption: Exposures including both the positive flux cases (“point” markers) and the negative flux cases (“cross” markers) on the difference images for DC21bwbfe/SN2021bnv (Type Ia SN; r band). Since we include the negative flux cases, we skip the SDSS-style shape and centroid flags and quantities, and the top six features in Table 3 remain. This example illustrates what happens when the features from the SDSS algorithm are unavailable. Here, feature Nos. 4 and 5 are less effective than the others. In both positive and negative flux cases, when the source is sufficiently bright (high S/N in absolute value), the PSF flux S/N itself is sufficient for the candidate selection. However, when it is faint in the positive flux cases, using more features can give better candidate selection (see also Figure 15).
Paper: DECam Multimessenger Astrophysics Pipeline. I. From Raw Data to Single-exposure Candidates
Authors: Shenming Fu, Thomas Matheson, Aaron Meisner, Yuanyuan Zhang, Sebastián Vicencio, Destry Saul
Figure caption: Examples of running PCA on the DC21bwbfe/SN2021bnv data (Type Ia SN; r band). We show the instances where the S/N is low (approaching the detection limit), but other features still have high quantiles to assist the candidate selection. At visit 978220, the low S/N is caused by poor weather, and the S/N increases afterwards even though the transient is getting fainter. Here the results are strongly contaminated by noise, and the PCA R/B shows mediocre but acceptable performance. Top: PCA result using 15 features (Table 3, Figure 16). Bottom: PCA result using six features (Figure 17).
Paper: DECam Multimessenger Astrophysics Pipeline. I. From Raw Data to Single-exposure Candidates
Authors: Shenming Fu, Thomas Matheson, Aaron Meisner, Yuanyuan Zhang, Sebastián Vicencio, Destry Saul
Figure caption: Evolution of the features and PCA performance for the target (DC21bwbfe/SN2021bnv, Type Ia SN; r band); positive flux cases only. The color scheme is the same as in previous Figures. Here, feature Nos. 3, 5, 11, and 12 are less effective than the others. Compared to Appendix C, which uses a larger set of features, here PCA generally has better separation (higher EVR). However, when poor weather leads to low S/N (blue points in the middle of the exposure sequence with low teff), using more features as in Appendix C gives slightly better results (higher q P).
Paper: DECam Multimessenger Astrophysics Pipeline. I. From Raw Data to Single-exposure Candidates
Authors: Shenming Fu, Thomas Matheson, Aaron Meisner, Yuanyuan Zhang, Sebastián Vicencio, Destry Saul
Figure caption: Evolution of the features and PCA performance for the target (DES16X3jj, possible Type II SN; i band). This object was captured by short exposures (10 s) and has low brightness. It generally has negative flux in our difference images. We thus only use six features, the same as in Figure 17. The corresponding light curve is shown in Figure 4. Here, feature Nos. 1, 4, and 5 are less effective than the others. The first point has low S/N, but the feature quantile Nos. 2 and 3 (and q P) are still high.
Paper: DECam Multimessenger Astrophysics Pipeline. I. From Raw Data to Single-exposure Candidates
Authors: Shenming Fu, Thomas Matheson, Aaron Meisner, Yuanyuan Zhang, Sebastián Vicencio, Destry Saul
Figure caption: PCA results in the Crater II field, including an asteroid (419993/2011CW32). We plot the sources with PC1 quantile larger than 0.5 and combine the results of 18 exposures (visit 632364 to 632398 on CCD 21, 3 minutes exposures in the g band each). The corresponding MJD range is from 57832.232–57832.314, and the teff range is from 0.08–0.22. We annotate the variables (A. K. Vivas et al. 2020) and mark the asteroid (moving from SE to NW). The marker opacity is proportional to the sum of PC1 quantile of each source in individual exposures. V6 and V61 have relatively low brightness during the observation window.
Paper: DECam Multimessenger Astrophysics Pipeline. I. From Raw Data to Single-exposure Candidates
Authors: Shenming Fu, Thomas Matheson, Aaron Meisner, Yuanyuan Zhang, Sebastián Vicencio, Destry Saul
Figure caption: Two-dimensional histograms for PCA selected sources from multiple exposures of the same sky region. The targets are the KN of GW170817 (top row; combining the first four exposures at CCD 36 in the g band) and the DES15C2eaz SN (bottom row; the first nine valid exposures at CCD 18 in the r band). We show the counts with no weight (first column), weighted by teff (second column), by PCA first component EVR (third column), and by first component quantile/rank (last column). In each diagram, a darker color corresponds to a higher count, and the red dot marks the (true) location of the target. Note that there is a possible variable star near the KN. For the SN, if there is only one source after the flag filtering, we set the EVR weight to be zero.
Paper: DECam Multimessenger Astrophysics Pipeline. I. From Raw Data to Single-exposure Candidates
Authors: Shenming Fu, Thomas Matheson, Aaron Meisner, Yuanyuan Zhang, Sebastián Vicencio, Destry Saul
Figure caption: COSMOS SN in the calexp, template, and difference images. The exposure date, band, exposure number, and name of each SN are given in the title. Each row shows the cutouts of an SN. Cutouts are 100 × 100 pix with North toward top and East toward left.
Paper: KIC 6362386: An Eclipsing Binary with γ Doradus–type Pulsations and Starspots
Authors: Mengqi Jin, Jianning Fu, Xiaobin Zhang, Weikai Zong, Jiaxin Wang, Xiaoyu Ma, Keyu Xing, Haotian Wang
Figure caption: The SDR of the residuals of KIC 6362386. In this figure, each dot’s size represents the depth of the starspot, while the color signifies the phase where each starspot dip occurs. The dotted–dashed line delineates the dip duration of half a period, and the boundary between a single starspot and a double starspot is represented by a dashed line.
Paper: KIC 6362386: An Eclipsing Binary with γ Doradus–type Pulsations and Starspots
Authors: Mengqi Jin, Jianning Fu, Xiaobin Zhang, Weikai Zong, Jiaxin Wang, Xiaoyu Ma, Keyu Xing, Haotian Wang
Figure caption: The light curve obtained by differential photometry of the Kepler LC data. The top panel shows the light curves of the target star and the comparison star. The middle panel shows the light curve of differential photometry with the red line indicating the trend of the light curve. The bottom panel shows the detrended light curve of KIC 6362386.
Paper: KIC 6362386: An Eclipsing Binary with γ Doradus–type Pulsations and Starspots
Authors: Mengqi Jin, Jianning Fu, Xiaobin Zhang, Weikai Zong, Jiaxin Wang, Xiaoyu Ma, Keyu Xing, Haotian Wang
Figure caption: The light curve obtained by differential photometry of the TESS data. The top panel shows the light curves of the target star and the comparison star. The middle panel shows the light curve of differential photometry with the red line indicating the trend of the light curve. The bottom panel shows the detrended light curve of KIC 6362386.
Paper: KIC 6362386: An Eclipsing Binary with γ Doradus–type Pulsations and Starspots
Authors: Mengqi Jin, Jianning Fu, Xiaobin Zhang, Weikai Zong, Jiaxin Wang, Xiaoyu Ma, Keyu Xing, Haotian Wang
Figure caption: The H-R diagram of the primary star of KIC 6362386. The blue point indicates the location of the primary star. The black dashed lines show the theoretical instability strip of γ Dor stars (G. Li et al. 2020; M. A. Dupret et al. 2005). The solid lines in the figure represent the evolutionary tracks of stars with different masses.
Paper: KIC 6362386: An Eclipsing Binary with γ Doradus–type Pulsations and Starspots
Authors: Mengqi Jin, Jianning Fu, Xiaobin Zhang, Weikai Zong, Jiaxin Wang, Xiaoyu Ma, Keyu Xing, Haotian Wang
Figure caption: The ACF of the residuals of the light curves of KIC 6362386. The blue curve represents the ACF, and the orange curve represents the best-fitting result obtained through the corresponding MCMC analysis. The consistency between the results of ACF and MCMC proves the presence of spots with a rotational period consistent with the orbital period of KIC 6362386.
Paper: KIC 6362386: An Eclipsing Binary with γ Doradus–type Pulsations and Starspots
Authors: Mengqi Jin, Jianning Fu, Xiaobin Zhang, Weikai Zong, Jiaxin Wang, Xiaoyu Ma, Keyu Xing, Haotian Wang
Figure caption: Comparison of the light curves obtained by the LightKurve program and the differential photometry for the Kepler data. The black and blue dots are obtained from the LightKurve program and the differential photometry, respectively.
Paper: KIC 6362386: An Eclipsing Binary with γ Doradus–type Pulsations and Starspots
Authors: Mengqi Jin, Jianning Fu, Xiaobin Zhang, Weikai Zong, Jiaxin Wang, Xiaoyu Ma, Keyu Xing, Haotian Wang
Figure caption: Comparison of the light curves obtained by the LightKurve program and the differential photometry for the TESS data. The black and blue dots are obtained from the LightKurve program and the differential photometry, respectively.