adsabs/AstroCLIMB huggingface dataset:
Paper: A Novel Survey for Young Substellar Objects with the W-band Filter. V. IC 348 and Barnard 5 in the Perseus Cloud
Authors: Bhavana Lalchand, Wen-Ping Chen, Beth A. Biller, Loïc Albert, Katelyn Allers, Sophie Dubber, Zhoujian Zhang, Michael C. Liu, Jessy Jose, Belinda Damian, Tanvi Sharma, Mickaël Bonnefoy, Yumiko Oasa
Figure caption: The observed flux-calibrated and normalized IRTF/SpeX spectra of the targets in IC 348: (a) 03434538+3201041, (b) 03435016+3204073, (c) 03441864+3218204, and (d) 3441864+3218204.
Paper: A Novel Survey for Young Substellar Objects with the W-band Filter. V. IC 348 and Barnard 5 in the Perseus Cloud
Authors: Bhavana Lalchand, Wen-Ping Chen, Beth A. Biller, Loïc Albert, Katelyn Allers, Sophie Dubber, Zhoujian Zhang, Michael C. Liu, Jessy Jose, Belinda Damian, Tanvi Sharma, Mickaël Bonnefoy, Yumiko Oasa
Figure caption: The observed flux-calibrated and normalized IRTF/SpeX spectra of the targets in Barnard 5: (a) 0348154+330918, (b) 0348362+325905, and (c) 0349286+325806.
Paper: Probing Photon Statistics in Adaptive Optics Images with SCExAO/MEC 
Authors: Sarah Steiger, Timothy D. Brandt, Olivier Guyon, Noah Swimmer, Alexander B. Walter, Clinton Bockstiegel, Julien Lozi, Vincent Deo, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Nemanja Jovanovic, Frantz Martinache, Benjamin A. Mazin
Figure caption: Simulated I  C , I  S , and I  P  images generated by running PCSSD on constant and Gamma-distributed companion intensities for two different suites of companion contrasts. Left: 4 × 10−4, 2 × 10−4, 1 × 10−4, 5 × 10−5. Right: 6 × 10−3, 3 × 10−3, 1.5  ×  10−3, 7.5  ×  10−4. The “True” columns are the input I  C , I  S , and I  P  images.
Paper: Probing Photon Statistics in Adaptive Optics Images with SCExAO/MEC 
Authors: Sarah Steiger, Timothy D. Brandt, Olivier Guyon, Noah Swimmer, Alexander B. Walter, Clinton Bockstiegel, Julien Lozi, Vincent Deo, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Nemanja Jovanovic, Frantz Martinache, Benjamin A. Mazin
Figure caption: Left: Total y-band intensity dither combined image of AB Aurigae taken with SCExAO/MEC. Disk features here are largely obscured. The satellite spots can be seen as radially smeared bright patches on the edge of this image due to the corrected sky rotation. Right: I  C /I  S  image of the disk around AB Aurigae clearly showing some of the inner disk features. These include the two main spirals that have roots to the North and South as well as the extended point-like source to the South at ρ = 0.″16 as found in Boccaletti et al. (2020). A Gaussian filter has been applied over this image to smooth over small scale interpixel variations.
Paper: Probing Photon Statistics in Adaptive Optics Images with SCExAO/MEC 
Authors: Sarah Steiger, Timothy D. Brandt, Olivier Guyon, Noah Swimmer, Alexander B. Walter, Clinton Bockstiegel, Julien Lozi, Vincent Deo, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Nemanja Jovanovic, Frantz Martinache, Benjamin A. Mazin
Figure caption: Left: Total intensity image of HIP 109427 B taken with SCExAO/MEC at the y and J bands where the location of the companion has been circled in red. Right: SSD I  C /I  S  image of HIP 109427 B. Here the companion is plainly visible as well as dark regions at the edge of the coronagraph showing the removal of pinned speckles from the total intensity image. This figure is reproduced from Steiger et al. (2021).
Paper: Probing Photon Statistics in Adaptive Optics Images with SCExAO/MEC 
Authors: Sarah Steiger, Timothy D. Brandt, Olivier Guyon, Noah Swimmer, Alexander B. Walter, Clinton Bockstiegel, Julien Lozi, Vincent Deo, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Nemanja Jovanovic, Frantz Martinache, Benjamin A. Mazin
Figure caption: Histograms of the binned satellite spot intensity moving from three pixels away from the center of the spot (purple, top) to the center (yellow, bottom). Histograms shift from positive to negative skewness as they approach the center of the satellite spot as is shown by the best-fit MR I c/I s ratio (dashed lines). Here a higher value indicates less skew. As these data were taken in the y+J band, the satellite spots are elongated in the image and the plotted intensities were found by adding the intensities for six pixels at the same specified distance from the spot center (three on each side). Insets: satellite spot image where the pixels used to generate the histograms are color coded by their distance from the spot center. Dead pixels were purposefully avoided.
Paper: Probing Photon Statistics in Adaptive Optics Images with SCExAO/MEC 
Authors: Sarah Steiger, Timothy D. Brandt, Olivier Guyon, Noah Swimmer, Alexander B. Walter, Clinton Bockstiegel, Julien Lozi, Vincent Deo, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Nemanja Jovanovic, Frantz Martinache, Benjamin A. Mazin
Figure caption: Single-pixel arrival time histograms taken on-sky with SCExAO/MEC of the unocculted star Θ 1 Orionis (purple, bottom left), a faint secondary companion (teal, upper right), and at a random location in the field with comparable brightness to the faint secondary companion (yellow, bottom right). The best-fit MR was plotted for each distribution and is shown with the dashed line. Note that due to the brightness of the primary, 2 ms time bins were used to generate that intensity histogram instead of the 10 ms time bins used for the secondary and field locations. It is clear to see that the MR adequately describes the field location, but breaks down at the location of the primary. The companion is seen to be a convolution of the primary and field PDFs.
Paper: Probing Photon Statistics in Adaptive Optics Images with SCExAO/MEC 
Authors: Sarah Steiger, Timothy D. Brandt, Olivier Guyon, Noah Swimmer, Alexander B. Walter, Clinton Bockstiegel, Julien Lozi, Vincent Deo, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Nemanja Jovanovic, Frantz Martinache, Benjamin A. Mazin
Figure caption: Output of PCSSD on HIP 109427 B (see also Figure 4). The red arrows in each image point to the same location of the low-mass stellar companion. Here the companion light clearly shows up in I  C  with corresponding minima in the intensity in the I  P  and I  S  images.
Paper: Probing Photon Statistics in Adaptive Optics Images with SCExAO/MEC 
Authors: Sarah Steiger, Timothy D. Brandt, Olivier Guyon, Noah Swimmer, Alexander B. Walter, Clinton Bockstiegel, Julien Lozi, Vincent Deo, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Nemanja Jovanovic, Frantz Martinache, Benjamin A. Mazin
Figure caption: Gamma distribution (Equation (3)) from which the companion intensities were sampled in Section 4.2.2 and Figures 8 and 9. Here k = 5, Θ = 30, and μ corresponds to the median strehl ratio used (0.7).
Paper: Probing Photon Statistics in Adaptive Optics Images with SCExAO/MEC 
Authors: Sarah Steiger, Timothy D. Brandt, Olivier Guyon, Noah Swimmer, Alexander B. Walter, Clinton Bockstiegel, Julien Lozi, Vincent Deo, Sebastien Vievard, Nour Skaf, Kyohoon Ahn, Nemanja Jovanovic, Frantz Martinache, Benjamin A. Mazin
Figure caption: Interarrival time histogram for a single pixel. An excess of interarrival times between 10 and 40 μs can be clearly seen, which are inconsistent with Poisson statistics.
Paper: MAGIC: Microlensing Analysis Guided by Intelligent Computation
Authors: Haimeng Zhao, 海萌 赵, Wei Zhu, 伟 祝
Figure caption: The performance of locator, evaluated on RMSE of t 0, as functions of the photometric uncertainty (S/N) of the individual data point. Three different training strategies are used. In blue points, locator models are trained and evaluated on data sets with given S/N values separately. In orange points, locator is trained on the data set with the lowest S/N and then applied to all data sets. In green points, locator is trained on the data set with the highest S/N and then applied to all data sets.
Paper: MAGIC: Microlensing Analysis Guided by Intelligent Computation
Authors: Haimeng Zhao, 海萌 赵, Wei Zhu, 伟 祝
Figure caption: An example event with s > 1, in which locator “fails” to reproduce the input window. The input window (red dashed curve) is defined on the center of mass (red asterisk in the upper panel) of this wide binary system. The prediction of locator (shown in green) better matches the light-curve window (blue dashed curve) defined in the center of magnification (blue triangle in the upper panel) of the primary star (black plus on the left in the upper panel, with the one on the right being the secondary). This latter window better describes the time evolution of this wide binary event.
Paper: MAGIC: Microlensing Analysis Guided by Intelligent Computation
Authors: Haimeng Zhao, 海萌 赵, Wei Zhu, 伟 祝
Figure caption: Comparisons between input and predicted values of t E (left) and t 0/t E (right). Values from events with s > 1 and s < 1 are separated, with the former shown in red and the latter in blue. The rms errors (RMSEs) of the parameters are computed and indicated at the upper left corners. In this realization, k = 1/3 is used.
Paper: MAGIC: Microlensing Analysis Guided by Intelligent Computation
Authors: Haimeng Zhao, 海萌 赵, Wei Zhu, 伟 祝
Figure caption: Cumulative distributions of the χ 2 values of the output microlensing models of estimator. In blue and red curves models with the minimum χ 2 value and the closest distance (in parameter space) to the input model are used, respectively. The vertical dashed line indicates χ 2 = 500, which is approximately the medians for both curves.
Paper: MAGIC: Microlensing Analysis Guided by Intelligent Computation
Authors: Haimeng Zhao, 海萌 赵, Wei Zhu, 伟 祝
Figure caption: Cumulative distributions of the normalized weights in MDN. Here π 0, π 1, and π 2 are the top three highest weights in our MDN of 12 multivariate Gaussians. The blue curve indicates that there is one dominating Gaussian in about half of the cases, and the green curve shows that the combination of the top three Gaussians dominates the density distribution in almost all cases.
Paper: MAGIC: Microlensing Analysis Guided by Intelligent Computation
Authors: Haimeng Zhao, 海萌 赵, Wei Zhu, 伟 祝
Figure caption: An example event in which locator successfully reproduces the input window and thus recovers t 0 and t E. The upper panel shows the microlensing geometry, with the red asterisk marking the center of mass (c.o.mass) of the binary lens. The lower panel shows the simulated light curve and the input and output masks. The parameters used to reproduce this event are given in the upper-right corner.
Paper: MAGIC: Microlensing Analysis Guided by Intelligent Computation
Authors: Haimeng Zhao, 海萌 赵, Wei Zhu, 伟 祝
Figure caption: The performance of locator, evaluated on RMSEs of lgt E, t 0/t E, and t 0, as a function of k values.
Paper: MAGIC: Microlensing Analysis Guided by Intelligent Computation
Authors: Haimeng Zhao, 海萌 赵, Wei Zhu, 伟 祝
Figure caption: Similar to Figure 4 except that only events with t E < 40  days and k = 2 are used.
Paper: MAGIC: Microlensing Analysis Guided by Intelligent Computation
Authors: Haimeng Zhao, 海萌 赵, Wei Zhu, 伟 祝
Figure caption: Similar to Figure 2, but for events with s > 1.
Paper: A Mirage or an Oasis? Water Vapor in the Atmosphere of the Warm Neptune TOI-674 b
Authors: Jonathan Brande, Ian J. M. Crossfield, Laura Kreidberg, Antonija Oklopčić, Alex S. Polanski, Travis Barman, Björn Benneke, Jessie L. Christiansen, Diana Dragomir, Daniel Foreman-Mackey, Jonathan J. Fortney, Thomas P. Greene, Andrew W. Howard, Heather A. Knutson, Joshua D. Lothringer, Thomas Mikal-Evans, Caroline V. Morley
Figure caption: Simulated helium signatures for TOI-674 b, assuming a 4000K thermosphere, showing how the strength of the signal varies with mass-loss rate. We also show the expected performance of a 10 m class observatory observing a single transit of TOI-674 b, for the 3 × 109 g s−1 mass-loss rate, detecting the helium signature at a S/N of 7.
Paper: A Mirage or an Oasis? Water Vapor in the Atmosphere of the Warm Neptune TOI-674 b
Authors: Jonathan Brande, Ian J. M. Crossfield, Laura Kreidberg, Antonija Oklopčić, Alex S. Polanski, Travis Barman, Björn Benneke, Jessie L. Christiansen, Diana Dragomir, Daniel Foreman-Mackey, Jonathan J. Fortney, Thomas P. Greene, Andrew W. Howard, Heather A. Knutson, Joshua D. Lothringer, Thomas Mikal-Evans, Caroline V. Morley
Figure caption: White light-curve fits for modeling the systematics in each scan direction independently.
Paper: A Mirage or an Oasis? Water Vapor in the Atmosphere of the Warm Neptune TOI-674 b
Authors: Jonathan Brande, Ian J. M. Crossfield, Laura Kreidberg, Antonija Oklopčić, Alex S. Polanski, Travis Barman, Björn Benneke, Jessie L. Christiansen, Diana Dragomir, Daniel Foreman-Mackey, Jonathan J. Fortney, Thomas P. Greene, Andrew W. Howard, Heather A. Knutson, Joshua D. Lothringer, Thomas Mikal-Evans, Caroline V. Morley
Figure caption: The broadband data for the third transit of TOI-674 b. Top: the raw transit data, with the systematics and transit model. Middle: the detrended transit data and light-curve model. Bottom: the white-light-curve residuals.
Paper: A Mirage or an Oasis? Water Vapor in the Atmosphere of the Warm Neptune TOI-674 b
Authors: Jonathan Brande, Ian J. M. Crossfield, Laura Kreidberg, Antonija Oklopčić, Alex S. Polanski, Travis Barman, Björn Benneke, Jessie L. Christiansen, Diana Dragomir, Daniel Foreman-Mackey, Jonathan J. Fortney, Thomas P. Greene, Andrew W. Howard, Heather A. Knutson, Joshua D. Lothringer, Thomas Mikal-Evans, Caroline V. Morley
Figure caption: The broadband data for the second transit of TOI-674 b. Top: the raw transit data, with the systematics and transit model. Middle: the detrended transit data and light-curve model. Bottom: the white-light-curve residuals.
Paper: A Mirage or an Oasis? Water Vapor in the Atmosphere of the Warm Neptune TOI-674 b
Authors: Jonathan Brande, Ian J. M. Crossfield, Laura Kreidberg, Antonija Oklopčić, Alex S. Polanski, Travis Barman, Björn Benneke, Jessie L. Christiansen, Diana Dragomir, Daniel Foreman-Mackey, Jonathan J. Fortney, Thomas P. Greene, Andrew W. Howard, Heather A. Knutson, Joshua D. Lothringer, Thomas Mikal-Evans, Caroline V. Morley
Figure caption: Detrended spectral light curves and the transit models for the second transit of TOI-674 b.
Paper: A Mirage or an Oasis? Water Vapor in the Atmosphere of the Warm Neptune TOI-674 b
Authors: Jonathan Brande, Ian J. M. Crossfield, Laura Kreidberg, Antonija Oklopčić, Alex S. Polanski, Travis Barman, Björn Benneke, Jessie L. Christiansen, Diana Dragomir, Daniel Foreman-Mackey, Jonathan J. Fortney, Thomas P. Greene, Andrew W. Howard, Heather A. Knutson, Joshua D. Lothringer, Thomas Mikal-Evans, Caroline V. Morley
Figure caption: Detrended spectral light curves and the transit models for the third transit of TOI-674 b.
Paper: Revisiting the Transit Timing Variations in the TrES-3 and Qatar-1 Systems with TESS Data
Authors: Vineet Kumar Mannaday, Parijat Thakur, John Southworth, Ing-Guey Jiang, D. K. Sahu, L. Mancini, M. Vaňko, Emil Kundra, Pavol Gajdoš, Napaporn A-thano, Devesh P. Sariya, Li-Chin Yeh, Evgeny Griv, David Mkrtichian, Aleksey Shlyapnikov
Figure caption: Top panel: O − C diagram for the analysis of 129 midtransit times of TrES-3b. The black filled circles show the data from the TESS observations, the blue filled squares are from Mannaday et al. (2020), and the green and yellow filled triangles are from the quality 1 and quality 2 data of ETD. The dotted black line, dashed red curve, and dashed blue curve indicate the linear, orbital decay, and apsidal precession models, respectively. The lines show 100 random draws from the posteriors of the orbital decay (brown) and apsidal precession (cyan) models. The scenarios of both the models remain statistically indistinguishable in the time covered by current observations. The models are extrapolated for next ∼4.5 yr, to illustrate the broad spectrum of possible solutions. Bottom panel: O − C diagram for the analysis of 184 midtransit times of Qatar-1b. The magenta filled circles show the data from our observations, the black filled circles are for TESS observations, the blue filled squares are from Su et al. (2021), the indigo filled squares are from Mislis et al. (2015), and the red squares are from Collins et al. (2017). The other features of this panel are the same as described for the top panel.
Paper: Revisiting the Transit Timing Variations in the TrES-3 and Qatar-1 Systems with TESS Data
Authors: Vineet Kumar Mannaday, Parijat Thakur, John Southworth, Ing-Guey Jiang, D. K. Sahu, L. Mancini, M. Vaňko, Emil Kundra, Pavol Gajdoš, Napaporn A-thano, Devesh P. Sariya, Li-Chin Yeh, Evgeny Griv, David Mkrtichian, Aleksey Shlyapnikov
Figure caption: Left panel: the normalized relative flux of Qatar-1 as a function of the time (the offset from the midtransit time and in TDB-based BJD) of two transits observed by us with the 1.23 m telescope at CAHA. The points show the data and the solid lines show the best-fit models. Right panel: the corresponding residuals.
Paper: Revisiting the Transit Timing Variations in the TrES-3 and Qatar-1 Systems with TESS Data
Authors: Vineet Kumar Mannaday, Parijat Thakur, John Southworth, Ing-Guey Jiang, D. K. Sahu, L. Mancini, M. Vaňko, Emil Kundra, Pavol Gajdoš, Napaporn A-thano, Devesh P. Sariya, Li-Chin Yeh, Evgeny Griv, David Mkrtichian, Aleksey Shlyapnikov
Figure caption: The normalized relative flux of TrES-3 as a function of the time (the offset from the midtransit time and in TDB-based BJD) of the individual transits observed by TESS: the points show the data, the solid lines show the best-fit models, and E is the calculated epoch number.
Paper: Revisiting the Transit Timing Variations in the TrES-3 and Qatar-1 Systems with TESS Data
Authors: Vineet Kumar Mannaday, Parijat Thakur, John Southworth, Ing-Guey Jiang, D. K. Sahu, L. Mancini, M. Vaňko, Emil Kundra, Pavol Gajdoš, Napaporn A-thano, Devesh P. Sariya, Li-Chin Yeh, Evgeny Griv, David Mkrtichian, Aleksey Shlyapnikov
Figure caption: Top panel: time series data of TrES-3b observed by TESS within sector 25. Middle panel: corresponding OOT time series data along with the best-fitting GP model (red curve). Bottom panel: detrended time series data corresponding to the top panel.
Paper: Revisiting the Transit Timing Variations in the TrES-3 and Qatar-1 Systems with TESS Data
Authors: Vineet Kumar Mannaday, Parijat Thakur, John Southworth, Ing-Guey Jiang, D. K. Sahu, L. Mancini, M. Vaňko, Emil Kundra, Pavol Gajdoš, Napaporn A-thano, Devesh P. Sariya, Li-Chin Yeh, Evgeny Griv, David Mkrtichian, Aleksey Shlyapnikov
Figure caption: GLS periodograms computed for the timing residuals of TrES-3b (top panel) and Qatar-1b (bottom panel). The dashed line in each periodogram indicates the FAP level of the highest power peak. The dotted lines from top to bottom indicate the threshold levels of FAP = 1% and FAP = 5%, respectively.
Paper: Revisiting the Transit Timing Variations in the TrES-3 and Qatar-1 Systems with TESS Data
Authors: Vineet Kumar Mannaday, Parijat Thakur, John Southworth, Ing-Guey Jiang, D. K. Sahu, L. Mancini, M. Vaňko, Emil Kundra, Pavol Gajdoš, Napaporn A-thano, Devesh P. Sariya, Li-Chin Yeh, Evgeny Griv, David Mkrtichian, Aleksey Shlyapnikov
Figure caption: Top panel: time series data of Qatar-1b observed by TESS within sector 17. The remaining panels are the same as those mentioned in Figure 2.
Paper: Revisiting the Transit Timing Variations in the TrES-3 and Qatar-1 Systems with TESS Data
Authors: Vineet Kumar Mannaday, Parijat Thakur, John Southworth, Ing-Guey Jiang, D. K. Sahu, L. Mancini, M. Vaňko, Emil Kundra, Pavol Gajdoš, Napaporn A-thano, Devesh P. Sariya, Li-Chin Yeh, Evgeny Griv, David Mkrtichian, Aleksey Shlyapnikov
Figure caption: The normalized relative flux of Qatar-1 as a function of the time (the offset from the midtransit time and in TDB-based BJD) of the individual transits observed by TESS: the points show the data, the solid lines show the best-fit models, and E is the calculated epoch number.
Paper: Revisiting the Transit Timing Variations in the TrES-3 and Qatar-1 Systems with TESS Data
Authors: Vineet Kumar Mannaday, Parijat Thakur, John Southworth, Ing-Guey Jiang, D. K. Sahu, L. Mancini, M. Vaňko, Emil Kundra, Pavol Gajdoš, Napaporn A-thano, Devesh P. Sariya, Li-Chin Yeh, Evgeny Griv, David Mkrtichian, Aleksey Shlyapnikov
Figure caption: The same as Figure A1, but for the remaining epochs.
Paper: Tolerance For the Pixelation Effect in Shear Measurement
Authors: Zhi Shen, Jun Zhang, Hekun Li, Haoran Wang, Chengliang Wei, Guoliang Li, Xiaobo Li, Zhang Ban, Dan Yue
Figure caption: The relative error of the shear component g 1 as a function of Q and R. The PSF is set to be Gaussian.
Paper: Tolerance For the Pixelation Effect in Shear Measurement
Authors: Zhi Shen, Jun Zhang, Hekun Li, Haoran Wang, Chengliang Wei, Guoliang Li, Xiaobo Li, Zhang Ban, Dan Yue
Figure caption: Similar to Figure 16, but for the additive bias c 1.
Paper: Tolerance For the Pixelation Effect in Shear Measurement
Authors: Zhi Shen, Jun Zhang, Hekun Li, Haoran Wang, Chengliang Wei, Guoliang Li, Xiaobo Li, Zhang Ban, Dan Yue
Figure caption: The level of aliasing power at different values of Q. The upper and lower panels show the results for the Gaussian and Airy disk PSF, respectively. In each panel, the red line can be regarded as the power spectrum free of aliasing power, therefore treated as a reference.
Paper: Tolerance For the Pixelation Effect in Shear Measurement
Authors: Zhi Shen, Jun Zhang, Hekun Li, Haoran Wang, Chengliang Wei, Guoliang Li, Xiaobo Li, Zhang Ban, Dan Yue
Figure caption: The multiplicative bias for galaxies of different sizes and noise level. The solid lines and the dashed–dotted lines are from galaxies of S/N = 30 or 15. The two panels are for the PSF of elliptical Airy disk and CSST, respectively.
Paper: Tolerance For the Pixelation Effect in Shear Measurement
Authors: Zhi Shen, Jun Zhang, Hekun Li, Haoran Wang, Chengliang Wei, Guoliang Li, Xiaobo Li, Zhang Ban, Dan Yue
Figure caption: Similar to Figure 8, but for the PSF of Airy disk and CSST. Due to the similarity of m 1 and m 2, we just plot the average of them as m in these plots.
Paper: Tolerance For the Pixelation Effect in Shear Measurement
Authors: Zhi Shen, Jun Zhang, Hekun Li, Haoran Wang, Chengliang Wei, Guoliang Li, Xiaobo Li, Zhang Ban, Dan Yue
Figure caption: The multiplicative bias for galaxies of different sizes and R. The solid lines are from R = 1.4, and the dashed–dotted lines are from R = 2.0. The two panels are for the PSF of Airy disk and CSST, respectively.
Paper: Tolerance For the Pixelation Effect in Shear Measurement
Authors: Zhi Shen, Jun Zhang, Hekun Li, Haoran Wang, Chengliang Wei, Guoliang Li, Xiaobo Li, Zhang Ban, Dan Yue
Figure caption: Similar to Figure 11, but for the additive bias c 1.
Paper: Tolerance For the Pixelation Effect in Shear Measurement
Authors: Zhi Shen, Jun Zhang, Hekun Li, Haoran Wang, Chengliang Wei, Guoliang Li, Xiaobo Li, Zhang Ban, Dan Yue
Figure caption: Similar to Figure 13, but for the PSF of Airy disk.
Paper: Tolerance For the Pixelation Effect in Shear Measurement
Authors: Zhi Shen, Jun Zhang, Hekun Li, Haoran Wang, Chengliang Wei, Guoliang Li, Xiaobo Li, Zhang Ban, Dan Yue
Figure caption: The multiplicative bias for galaxies of different S/Ns and sizes. The two panels show the results for the Gaussian and Moffat PSF, respectively.
Paper: A Photometric and Spectroscopic Study of the Short-period Algol EW Boötis with a δ Sct Pulsator
Authors: Hye-Young Kim, Kyeongsoo Hong, Chun-Hwey Kim, Jae Woo Lee, Min-Ji Jeong, Jang-Ho Park, Mi-Hwa Song
Figure caption: The RVs of EW Boo with the synthetic curves. The circles and triangles represent the RV measurements for primary and secondary stars, respectively. The black and gray symbols represent the RVs of both components measured using two Gaussian functions and Broadening function, respectively. The solid curves were obtained from the light and RV solutions using the WD code. The dotted line denotes the system velocity of +5.09 km s−1. In the lower panel, the residuals between observed RVs and theoretical models are plotted.