adsabs/AstroCLIMB huggingface dataset:
Paper: Physically Motivated Deep Learning to Superresolve and Cross Calibrate Solar Magnetograms
Authors: Andrés Muñoz-Jaramillo, Anna Jungbluth, Xavier Gitiaux, Paul J. Wright, Carl Shneider, Shane A. Maloney, Atılım Güneş Baydin, Yarin Gal, Michel Deudon, Freddie Kalaitzis
Figure caption: Demonstration of the HMI radial velocity leaking into HMI LOS magnetic field data. The top two panels show the total unsigned magnetic field from HMI and the SR output of MDI. The bottom two panels show the ratio of SR output compared to HMI, and the HMI radial velocity where positive values are away from the Sun (bottom panel). In each panel, vertical gray bars are shown with a 24 hr periodicity starting on 2011 March 1. It can be seen that this periodicity leaks into the HMI data, but is not observed for the SR output (as further discussed in the main text).
Paper: Quasar Winds Caught on Acceleration and Deceleration
Authors: Weimin Yi, P. B. Hall, Zunli Yuan, W. N. Brandt, D. P. Schneider, Zhicheng He, Jin-Ming Bai, Xue-Bing Wu
Figure caption: Left: zoom-in profiles of the BAL-1 in Al III and Mg II, in which a set of three blueward components of the Al III and Mg II doublets (gray/green/red vertical dotted lines) with two fixed velocity separations is identified in each of the three spectra with relatively high S/N, indicative of the same BAL-1 subflow persisting over the epochs. Middle: continuum-normalized spectra of the group-1 quasar J1344, in which two distinct BALs are labeled with BAL-1 and BAL-2. The comb-like symbols in the middle subpanel indicate radiative-acceleration, line-locking signatures of C IV. The Earth symbol in the bottom left subpanel indicates telluric absorption. The three bell-like profiles depict the one-Gaussian fits to the apparent Al III BEL peaks. Right: MJD vs. velocity shifts (relative to the first epoch), trough widths (w 95; trough width at the 95% continuum level), REWs (the Al III emission peak nearly disappeared at MJD 59384), and continuum flux at λ rest = 1700 Å.
Paper: Quasar Winds Caught on Acceleration and Deceleration
Authors: Weimin Yi, P. B. Hall, Zunli Yuan, W. N. Brandt, D. P. Schneider, Zhicheng He, Jin-Ming Bai, Xue-Bing Wu
Figure caption: Left: continuum-normalized spectra of the group-2 quasar J1259 over six epochs. The vertical red/blue dashed lines refer to the peak absorption at the first/other epochs, from which one can directly see how the velocity shift varies with time using the first epoch as a benchmark (the first spectrum is superimposed on all successive epochs and the positions of the red and blue dashed lines in H9 are fixed by those of Hγ). Apparently, H9 remains generally unchanged in REW while the Hγ BAL appears to vary from epoch to epoch. Right (bottom to top): MJD vs. velocity shift of the Hγ BAL relative to MJD 55983, REWs of different ions, and photometric magnitudes. The apparent disappearance in [O II] emission at MJD 58894 (highlighted by the red circle) is due to a rotation (marked by position angle (PA) from the left panels) between the two long-slit spectroscopic observations targeting the quasar core with a one-sided, off-nuclear [O II] emission nebula (W. Yi et al. 2024, in preparation).
Paper: Quasar Winds Caught on Acceleration and Deceleration
Authors: Weimin Yi, P. B. Hall, Zunli Yuan, W. N. Brandt, D. P. Schneider, Zhicheng He, Jin-Ming Bai, Xue-Bing Wu
Figure caption: Left: continuum-normalized spectra of the group-1 quasar J0136 over five epochs. The comb-like symbol again indicates a line-locking feature in C IV. Right (bottom to top): MJD vs. velocity shifts of the C IV BAL relative to MJD 55444, REWs for the BALs and BELs, and continuum flux at λ rest = 1700 Å, which depict the time-variability behaviors of these quantities. The C IV BAL profiles are identical (CCF coefficient > 0.9) to that from MJD 55444 and the velocity shifts in each interval measured by the two different methods are consistent within measurement errors. The Mg II was caught on the disappearance as opposed to the persistence of C IV from the BAL flow.
Paper: Quasar Winds Caught on Acceleration and Deceleration
Authors: Weimin Yi, P. B. Hall, Zunli Yuan, W. N. Brandt, D. P. Schneider, Zhicheng He, Jin-Ming Bai, Xue-Bing Wu
Figure caption: Left panels: the spectral fits (thick gray) to the Mg II (bottom panel), Hβ, and Hα (top panel) emission for J0136, which include the Fe II (blue dotted), the broad Gaussians (orange), the narrow Gaussians (green), and the continuum fits (dashed). The BAL feature (green) was masked during the fit. The thin gray lines indicate spectral errors. The fits indicate that FWHM(Mg II) is ∼4650 km s−1 in broad emission as opposed to FWHM(Hβ) ∼2750 km s−1, and that blueshifted emission/absorption features exist in Mg II but not in Hβ, suggestive of the former being more affected by outflows. Right panels: the He I* λ10830 and λ3889 BAL profiles for J1238. For comparison, a subpanel of the Mg II BAL profile is added over the four epochs, above which the He I* λ10830 BAL is displayed. Unlike the He I* λ10830 and Mg II BALs, which have three major subflows, only one He I* λ3889 BAL feature was detected at v LOS ∼ −6000 km s−1, whose strength remains generally unchanged over the epochs.
Paper: Quasar Winds Caught on Acceleration and Deceleration
Authors: Weimin Yi, P. B. Hall, Zunli Yuan, W. N. Brandt, D. P. Schneider, Zhicheng He, Jin-Ming Bai, Xue-Bing Wu
Figure caption: SEDs of the four quasars, which incorporate data from GALEX (diamonds), SDSS (triangles), 2MASS (squares), WISE (circles), and VLASS and FIRST (stars). The early/late epoch spectra are shown in red/blue for each quasar, complemented with a near-IR (cyan) spectrum if it exists. J0136 and J1344 (group 1) have BAL-acceleration signatures and are radio-quiet; in addition, J0136 is undergoing a LoBAL → HiBAL transformation along with an increase in brightness over the epochs, while J1344 remains in a LoBAL state along with a decrease in brightness. J1238 and J1259 (group 2) exhibit BAL-acceleration/deceleration signatures and weak radio emission, with f 3GHz/f 1.4GHz = 2.5/5.84 mJy and 0.8/2.0 mJy for the former and latter, respectively. The GALEX photometry for J1259 should be treated with caution given its large flag values. The median SED of red quasars from Calistro Rivera et al. (2021) is scaled to the W3 band.
Paper: Quasar Winds Caught on Acceleration and Deceleration
Authors: Weimin Yi, P. B. Hall, Zunli Yuan, W. N. Brandt, D. P. Schneider, Zhicheng He, Jin-Ming Bai, Xue-Bing Wu
Figure caption: Left: continuum-normalized spectra of the group-2 quasar J1238 for the Mg II BAL/BEL over four epochs. Right (bottom to top): MJD vs. velocity shift of the Mg II BAL, REW for the BALs and BELs, and photometric magnitudes, which depict the time-variability patterns of these quantities. Unlike the Mg II BAL, which has at least three subflows, the He I* BAL is detected only at v LOS ∼ 6000 km s−1 (see Section 4.2) and offset above by 37 Å for clarity. The positive/negative velocity shifts detected over the epochs may be linked to BAL acceleration/deceleration events for this quasar.
Paper: Quasar Winds Caught on Acceleration and Deceleration
Authors: Weimin Yi, P. B. Hall, Zunli Yuan, W. N. Brandt, D. P. Schneider, Zhicheng He, Jin-Ming Bai, Xue-Bing Wu
Figure caption: Comparison between the LoBAL (color) and HiBAL (gray; from Table 4 of Grier et al. 2016) samples. The two horizontal dotted lines are the upper limits of BAL acceleration/deceleration in Grier et al. (2016) derived from the median values of velocity shifts + 3σ positive/negative uncertainties. J1344, J0136, and J1259 all show a similar trend, such that they have a steep rise followed by a plateau-like time evolution in BAL-velocity shift.
Paper: Quasar Winds Caught on Acceleration and Deceleration
Authors: Weimin Yi, P. B. Hall, Zunli Yuan, W. N. Brandt, D. P. Schneider, Zhicheng He, Jin-Ming Bai, Xue-Bing Wu
Figure caption: Demonstration of monolithic velocity shifts for the Mg II BAL in J1344 over three well-separated epochs (top) via the CCF (bottom left) and ﹩{\chi }_{12}^{2}﹩ (bottom right) analyses, in which the bar histograms correspond to the peaks generated from 10,000 Monte Carlo simulations, with the dot and error bars depicting the median value of the histogram and the 90% percentile confidence level. Both analyses yield a closely similar velocity shift in each time interval.
Paper: Lithium Abundances from the LAMOST Medium-resolution Survey Data Release 9
Authors: Ming-Yi Ding, Jian-Rong Shi, Hong-liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Xiao-Jin Xie, Yao-Jia Tang, Ze-Ming Zhou, Jiang-Tao Wang
Figure caption: The behavior of A(Li) as a function of T eff, ﹩\mathrm{log}g﹩, and [Fe/H]. Only stars with S/N > 20 (green distribution in Figure 8) are represented.
Paper: Lithium Abundances from the LAMOST Medium-resolution Survey Data Release 9
Authors: Ming-Yi Ding, Jian-Rong Shi, Hong-liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Xiao-Jin Xie, Yao-Jia Tang, Ze-Ming Zhou, Jiang-Tao Wang
Figure caption: Examples of our fitting results for a cool giant (top left), a cool dwarf (top right), a warm giant (bottom left), and a hot dwarf (bottom right). In each plane, the observed spectrum is plotted the shaded gray region; at the same time, the template spectra are plotted with A(Li) = −1.0 (black line), 0.0 (red line), 1.0 (green line), 2.0 (yellow line), and 3.0 (blue line). The stellar parameters and lithium abundances are listed, and the vertical gray dotted lines show the position of the Li I resonance line.
Paper: Lithium Abundances from the LAMOST Medium-resolution Survey Data Release 9
Authors: Ming-Yi Ding, Jian-Rong Shi, Hong-liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Xiao-Jin Xie, Yao-Jia Tang, Ze-Ming Zhou, Jiang-Tao Wang
Figure caption: The distribution of A(Li) for our result. The whole sample set is plotted in red. Samples with reliable observations are plotted in green. The blue distribution shows the samples that have consistent multiple measurements. The number of stars in each distribution is listed.
Paper: Lithium Abundances from the LAMOST Medium-resolution Survey Data Release 9
Authors: Ming-Yi Ding, Jian-Rong Shi, Hong-liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Xiao-Jin Xie, Yao-Jia Tang, Ze-Ming Zhou, Jiang-Tao Wang
Figure caption: The comparison of the lithium abundances derived from our method and those from the GALAH DR3 and the Gaia-ESO DR5. The error bars show the uncertainty. Colors are the same as in Figure 3.
Paper: Lithium Abundances from the LAMOST Medium-resolution Survey Data Release 9
Authors: Ming-Yi Ding, Jian-Rong Shi, Hong-liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Xiao-Jin Xie, Yao-Jia Tang, Ze-Ming Zhou, Jiang-Tao Wang
Figure caption: The distribution of stellar parameters for common stars from the GALAH DR3 (gray distribution) and the Gaia-ESO DR5 (red dots).
Paper: Lithium Abundances from the LAMOST Medium-resolution Survey Data Release 9
Authors: Ming-Yi Ding, Jian-Rong Shi, Hong-liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Xiao-Jin Xie, Yao-Jia Tang, Ze-Ming Zhou, Jiang-Tao Wang
Figure caption: The systematic errors of A(Li) as a function of S/N. The red dots and error bars are the average values and the standard deviations of each bin.
Paper: Lithium Abundances from the LAMOST Medium-resolution Survey Data Release 9
Authors: Ming-Yi Ding, Jian-Rong Shi, Hong-liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Xiao-Jin Xie, Yao-Jia Tang, Ze-Ming Zhou, Jiang-Tao Wang
Figure caption: The random errors of A(Li) as a function of S/N. The red dots and error bars are the average values and the standard deviations of each bin.
Paper: Lithium Abundances from the LAMOST Medium-resolution Survey Data Release 9
Authors: Ming-Yi Ding, Jian-Rong Shi, Hong-liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Xiao-Jin Xie, Yao-Jia Tang, Ze-Ming Zhou, Jiang-Tao Wang
Figure caption: The residuals of the lithium abundance as a function of S/N. Colors are the same as in Figure 3.
Paper: Physically Motivated Deep Learning to Superresolve and Cross Calibrate Solar Magnetograms
Authors: Andrés Muñoz-Jaramillo, Anna Jungbluth, Xavier Gitiaux, Paul J. Wright, Carl Shneider, Shane A. Maloney, Atılım Güneş Baydin, Yarin Gal, Michel Deudon, Freddie Kalaitzis
Figure caption: Overview of ground (G) and space-based (S) observations of the Sun. The top panel shows the pixel size in arcseconds, and the operation time span of eight different instruments. The bottom panel shows the variation of the mean sunspot number over the last 50 yr. To date, the HMI, on board SDO, provides the highest resolution full-disk magnetograms. This is followed by the 512 channel magnetograph of the Kitt Peak Vacuum Telescope and the Synoptic Optical Long-term Investigations of the Sun by the NSO, GONG, the Mount Wilson Observatory, and finally the Wilcox Solar Observatory.
Paper: Physically Motivated Deep Learning to Superresolve and Cross Calibrate Solar Magnetograms
Authors: Andrés Muñoz-Jaramillo, Anna Jungbluth, Xavier Gitiaux, Paul J. Wright, Carl Shneider, Shane A. Maloney, Atılım Güneş Baydin, Yarin Gal, Michel Deudon, Freddie Kalaitzis
Figure caption: Diagram of the deep-learning model used in this work. The input data consists of a magnetogram and a location channel, each of size 32 × 32 pixels. The main operations of the model consist of an encoder and a decoder. Through bilinear upsampling by a factor of 4, the size of the image is increased from 32 × 32 to 128 × 128 pixels per patch. RP and DO denote whether a convolutional layer was trained with reflection padding or Monte Carlo dropout respectively.
Paper: Physically Motivated Deep Learning to Superresolve and Cross Calibrate Solar Magnetograms
Authors: Andrés Muñoz-Jaramillo, Anna Jungbluth, Xavier Gitiaux, Paul J. Wright, Carl Shneider, Shane A. Maloney, Atılım Güneş Baydin, Yarin Gal, Michel Deudon, Freddie Kalaitzis
Figure caption: Example of the resolution differences between an input magnetogram (MDI/GONG), the deep-learning output, and the target (HMI). The insets show a 128 × 128 patch with clear resolution differences between the model inputs (MDI and GONG) and the model target (HMI). All panels show nearly simultaneous measurements made by GONG, MDI, and HMI on 2011 March 14.
Paper: Lithium Abundances from the LAMOST Medium-resolution Survey Data Release 9
Authors: Ming-Yi Ding, Jian-Rong Shi, Hong-liang Yan, Chun-Qian Li, Qi Gao, Tian-Yi Chen, Jing-Hua Zhang, Shuai Liu, Xiao-Jin Xie, Yao-Jia Tang, Ze-Ming Zhou, Jiang-Tao Wang
Figure caption: The distributions of stellar parameters for our samples.
Paper: Flare Hunting in Hot Subdwarf and White Dwarf Stars from Cycles 1–5 of TESS Photometry
Authors: Keyu Xing, Weikai Zong, Roberto Silvotti, Jian-Ning Fu, Stéphane Charpinet, Tianqi Cang, J. J. Hermes, Xiao-Yu Ma, Haotian Wang, Xuan Wang, Tao Wu, Jiaxin Wang
Figure caption: An example of generating the model of the short-period variability in the light curve of TIC 219244444. Top: the light curve of TIC 219244444 in TESS Sector 3 (left) and its Lomb–Scargle periodogram (right). The red arrow indicates the period used to fold the light curve (P fold = 0.304 day), which is twice the period at the max power. Bottom: the folded light curve and its model (red solid line) obtained by applying the median filter (left) and the residual of the model (right). The epochs masked by the processing in Section 3.3 are marked with gray points. The model fits the short-period variability well except for the ingress and egress of the eclipse.
Paper: Flare Hunting in Hot Subdwarf and White Dwarf Stars from Cycles 1–5 of TESS Photometry
Authors: Keyu Xing, Weikai Zong, Roberto Silvotti, Jian-Ning Fu, Stéphane Charpinet, Tianqi Cang, J. J. Hermes, Xiao-Yu Ma, Haotian Wang, Xuan Wang, Tao Wu, Jiaxin Wang
Figure caption: Detrending the light curve of TIC 219244444 (RR Cae, a WD eclipsed by an M-dwarf every ∼0.3 day; Maxted et al. 2007) in TESS Sector 3 using the biweight filter with two different window lengths: (a) long of 0.3 day, (b) short of 0.05 day. Top: raw flux (black points) and trend flux (red solid line). Bottom: detrended flux (black points), 3σ MAD from the median (red dashed line) and zoom windows of one small flare (left) and one large flare (right). The large flare is overfitted with the short window, while the small flare cannot be detected with the long window. Only a 6 day segment of the light curve is shown in this figure.
Paper: Flare Hunting in Hot Subdwarf and White Dwarf Stars from Cycles 1–5 of TESS Photometry
Authors: Keyu Xing, Weikai Zong, Roberto Silvotti, Jian-Ning Fu, Stéphane Charpinet, Tianqi Cang, J. J. Hermes, Xiao-Yu Ma, Haotian Wang, Xuan Wang, Tao Wu, Jiaxin Wang
Figure caption: Histograms comparing flare properties and fractional flare luminosity between WDs (blue lines) and sdB/sdO stars (red lines). The top panels (a) show distributions for all flare events and flaring compact stars, while the bottom panels (b) display only flare events and flaring compact stars with an CL of 0. The left four panels in both rows show flare property distributions: duration, logarithmic amplitude, logarithmic ED, and logarithmic energy in the TESS bandpass, either for (a) 834 WD and 182 sdB/sdO flares or (b) 193 WD and 86 sdB/sdO flares. The right panels illustrate the distribution of the logarithmic fractional flare luminosity value, either for (a) 135 flaring WDs and 58 flaring sdB/sdO stars or (b) 28 flaring WDs and 16 flaring sdB/sdO stars.
Paper: Flare Hunting in Hot Subdwarf and White Dwarf Stars from Cycles 1–5 of TESS Photometry
Authors: Keyu Xing, Weikai Zong, Roberto Silvotti, Jian-Ning Fu, Stéphane Charpinet, Tianqi Cang, J. J. Hermes, Xiao-Yu Ma, Haotian Wang, Xuan Wang, Tao Wu, Jiaxin Wang
Figure caption: Histograms of the flare amplitude A and FWHM values, along with their natural logarithms, for the flare samples from H22. Left panels: the distributions of the natural logarithms of amplitude and FWHM (black step lines) with the fitted normal distributions (red solid lines). Right panels: the distributions of the original amplitude and FWHM values (black step lines) with the fitted log-normal distributions (red solid lines). The median values (vertical dashed lines) and standard deviations of the natural logarithms of amplitude and FWHM, provided in the upper right of the left panels, are used to initialize the walkers for the MCMC analysis. The resulting estimates from the MCMC analysis are shown in the upper right corner of the panels on the right.
Paper: Flare Hunting in Hot Subdwarf and White Dwarf Stars from Cycles 1–5 of TESS Photometry
Authors: Keyu Xing, Weikai Zong, Roberto Silvotti, Jian-Ning Fu, Stéphane Charpinet, Tianqi Cang, J. J. Hermes, Xiao-Yu Ma, Haotian Wang, Xuan Wang, Tao Wu, Jiaxin Wang
Figure caption: The same as Figure 1, but using our detrending procedure instead of directly using the biweight filter. The trend flux (red solid line) is the combination of the unfolded model of the short-period variability and the trend flux obtained using the biweight filter afterward. The gray points in the top panel are removed (see Section 3.3) in the detrended light curve, which causes the missing data (gray dashed line) in the right zoom window of the bottom panel.
Paper: Flare Hunting in Hot Subdwarf and White Dwarf Stars from Cycles 1–5 of TESS Photometry
Authors: Keyu Xing, Weikai Zong, Roberto Silvotti, Jian-Ning Fu, Stéphane Charpinet, Tianqi Cang, J. J. Hermes, Xiao-Yu Ma, Haotian Wang, Xuan Wang, Tao Wu, Jiaxin Wang
Figure caption: An SSO encounter event found in the light curve of TIC 275308213 in TESS Sector 8. The light curve shown in the left panel represents the photometry result using the aperture shown as the orange region in the right panel, which presents four frames of the target pixel file during the process during which an SSO, marked by a red star symbol, encounters the target star. The corresponding fluxes of these moments are also marked in the light curve.
Paper: Flare Hunting in Hot Subdwarf and White Dwarf Stars from Cycles 1–5 of TESS Photometry
Authors: Keyu Xing, Weikai Zong, Roberto Silvotti, Jian-Ning Fu, Stéphane Charpinet, Tianqi Cang, J. J. Hermes, Xiao-Yu Ma, Haotian Wang, Xuan Wang, Tao Wu, Jiaxin Wang
Figure caption: Examples of simulated events in the training set: (a) flare and (b) nonflares. The dashed lines and dotted lines indicate standardized flux values of 3 and 1, respectively.
Paper: Flare Hunting in Hot Subdwarf and White Dwarf Stars from Cycles 1–5 of TESS Photometry
Authors: Keyu Xing, Weikai Zong, Roberto Silvotti, Jian-Ning Fu, Stéphane Charpinet, Tianqi Cang, J. J. Hermes, Xiao-Yu Ma, Haotian Wang, Xuan Wang, Tao Wu, Jiaxin Wang
Figure caption: Examples of the identification charts provided by tpfi: (a): an ideal situation in which the aperture only hosts the target with no other bright stars nearby, (b): the aperture hosting the target star and another dimmer star, (c): the aperture hosting numerous stars with comparable brightness alongside the target, (d): only the target resides within the aperture, but in proximity to a bright star. In each chart, the right panel overlays the Gaia DR3 catalog onto the target pixel file, with the target denoted by a white cross symbol. The size of the circle represents the relative brightness of the stars, as indicated by the Gaia G magnitude. The red region indicates the default aperture mask used by SPOC for photometry extraction. The left panel shows the same sky coverage, using DSS2 red images, with the same orientation.
Paper: Flare Hunting in Hot Subdwarf and White Dwarf Stars from Cycles 1–5 of TESS Photometry
Authors: Keyu Xing, Weikai Zong, Roberto Silvotti, Jian-Ning Fu, Stéphane Charpinet, Tianqi Cang, J. J. Hermes, Xiao-Yu Ma, Haotian Wang, Xuan Wang, Tao Wu, Jiaxin Wang
Figure caption: Gaia H-R diagram of the flaring compact stars included in our study. The flaring WDs and sdB/sdO stars are signified by diamond and circle markers, respectively, with other compact stars from the TASC WG8 target list denoted with black dots. The colors of the markers correspond to the ﹩\mathrm{log}({L}_{\mathrm{flare}}/{L}_{\mathrm{TESS}})﹩ value for each flaring star. The stars surrounded by blue squares are those with a level of contamination of 0 (see Section 5.2.1). The red dashed–dotted lines indicate the thresholds used for filtering out stars with companions (see Section 5.2.2).
Paper: Flare Hunting in Hot Subdwarf and White Dwarf Stars from Cycles 1–5 of TESS Photometry
Authors: Keyu Xing, Weikai Zong, Roberto Silvotti, Jian-Ning Fu, Stéphane Charpinet, Tianqi Cang, J. J. Hermes, Xiao-Yu Ma, Haotian Wang, Xuan Wang, Tao Wu, Jiaxin Wang
Figure caption: Cumulative FFDs and corresponding power-law fits. The blue and red open circles represent flares from all WDs and sdB/sdO stars, respectively. The red filled circles signify flares from the refined sdB/sdO sample. The dashed and dashed–dotted black lines represent the best-fit power laws to the cumulative FFDs of the full and refined samples, respectively. The fitted α values and uncertainties, along with the number of flares used for fitting N fit, are shown in the bottom left.
Paper: Flare Hunting in Hot Subdwarf and White Dwarf Stars from Cycles 1–5 of TESS Photometry
Authors: Keyu Xing, Weikai Zong, Roberto Silvotti, Jian-Ning Fu, Stéphane Charpinet, Tianqi Cang, J. J. Hermes, Xiao-Yu Ma, Haotian Wang, Xuan Wang, Tao Wu, Jiaxin Wang
Figure caption: All 23 flare events (red lines) in the light curves of the 13 sdB/sdO stars in our refined sample. The gray dashed lines are 3σ MAD from the median. TIC IDs and sector numbers are indicated in the top right corner of each panel.