adsabs/AstroCLIMB huggingface dataset:
Paper: Binary Star Orbits. VI. The Interferometric-spectroscopic Binary 73 Leo
Authors: Brian D. Mason, R. Elizabeth M. Griffin, R. T. Zavala, Christian A. Hummel, Haley M. Hurowitz, Jonathan L. Hurowitz, William I. Hartkopf, Ellyn K. Baines, Stephen J. Williams, Rachel A. Matson
Figure caption: The new combined orbit solution: plot of relative astrometry data for 73 Leo; the X and Y scales are in arcseconds. The dashed curve represents the orbit of B. D. Mason et al. (1997). The dotted–dashed line indicates the line of nodes. Early speckle measurements (1979–1993) are shown as open circles, NPOI measures as stars, and later speckle measures (2018–2025) as filled circles. All measurements are connected to their predicted positions on the orbit by “O − C” lines. The direction of motion is indicated on the northeast orientation in the lower right of the plot.
Paper: Binary Star Orbits. VI. The Interferometric-spectroscopic Binary 73 Leo
Authors: Brian D. Mason, R. Elizabeth M. Griffin, R. T. Zavala, Christian A. Hummel, Haley M. Hurowitz, Jonathan L. Hurowitz, William I. Hartkopf, Ellyn K. Baines, Stephen J. Williams, Rachel A. Matson
Figure caption: This comparison between 73 Leo (red) and ψ Boo at mid-blue wavelengths. The spectrum of ψ Boo has been scaled down by 5%.
Paper: Binary Star Orbits. VI. The Interferometric-spectroscopic Binary 73 Leo
Authors: Brian D. Mason, R. Elizabeth M. Griffin, R. T. Zavala, Christian A. Hummel, Haley M. Hurowitz, Jonathan L. Hurowitz, William I. Hartkopf, Ellyn K. Baines, Stephen J. Williams, Rachel A. Matson
Figure caption: Two spectra of 73 Leo, but at different phases (one at the giant’s velocity maximum, the other near its velocity minimum). The spectrum of a secondary component will have moved in antiphase to that of the primary, giving rise to changes in some line profiles since blends would have been created differently. Such changes are not in evidence.
Paper: Deep Reinforcement Learning for Efficient Scheduling of Ground-based Astronomical Observations
Authors: Hai Cao, Shaoming Hu, Junju Du, Xu Chen, Shuqi Liu, Shuai Feng, Bo Zhang, Yuchen Jiang
Figure caption: Comparative visualizations of the scheduled observation plans. The top panel presents the plan simulating manual observations (“Random”), the middle panel displays the results generated using the greedy algorithm (“Greedy”), and the bottom panel shows the observation plan generated by our proposed DRL-based model (“DRL”). The width of the black bars indicates the switch time, while the width of the colored bars indicates the observing time of the task.
Paper: Deep Reinforcement Learning for Efficient Scheduling of Ground-based Astronomical Observations
Authors: Hai Cao, Shaoming Hu, Junju Du, Xu Chen, Shuqi Liu, Shuai Feng, Bo Zhang, Yuchen Jiang
Figure caption: Score curves of targets in V band at WHO from 2025 January 25 10:00 to 22:30. The curves closely resemble parabolas, allowing them to be accurately fitted using quadratic polynomials. As an example, one of the fitted curves is highlighted in the plot, which had a coefficient of determination R2 of 0.998, indicating an excellent fit.
Paper: Deep Reinforcement Learning for Efficient Scheduling of Ground-based Astronomical Observations
Authors: Hai Cao, Shaoming Hu, Junju Du, Xu Chen, Shuqi Liu, Shuai Feng, Bo Zhang, Yuchen Jiang
Figure caption: Scheduled performance comparison of four algorithms. Target-switching sequences are indicated by red arrows, while scatter point colors represent instantaneous reward scores scaled from zero to one (see color bar). The total reward scores for each algorithm appear parenthetically after the algorithm names. The bottom subplots demonstrate significantly enhanced task completion rates and total scores achieved by our DRL-based methods using GR and BS selectors.
Paper: Deep Reinforcement Learning for Efficient Scheduling of Ground-based Astronomical Observations
Authors: Hai Cao, Shaoming Hu, Junju Du, Xu Chen, Shuqi Liu, Shuai Feng, Bo Zhang, Yuchen Jiang
Figure caption: Dual-telescope observation plan execution: DRL-GR results outperform the greedy and random scheduling. Sequential processes are marked by red arrows. Parenthetical values denote the total theoretical reward scores. DRL-GR-1 plans (bottom left) achieve 33.9% higher task completion and 24.1% reward gain despite wider spatial distribution vs. the greedy benchmark.
Paper: Deep Reinforcement Learning for Efficient Scheduling of Ground-based Astronomical Observations
Authors: Hai Cao, Shaoming Hu, Junju Du, Xu Chen, Shuqi Liu, Shuai Feng, Bo Zhang, Yuchen Jiang
Figure caption: The convergence of the total reward per episode in reinforcement training. The solid blue line shows the mean reward of the training batch, which serves as the baseline. The dashed red and green lines represent the maximum and minimum rewards within the batch, respectively.
Paper: The Transit Signal of KOI-1755 Originates from a Background Eclipsing Binary Star—Extracting the Light Curve of a Faint Background Star from Kepler Target Pixel File Data
Authors: Haozhi Wang, Ali Esamdin, Chenglong Lv, Lixian Shen, Jin-zhong Liu, Abdusamatjan Iskandar, Umut Mahmut, Rivkat Karimov, Shuhrat A. Ehgamberdiev
Figure caption: Top panel: the frequency spectrum of the residuals after removing all significant nonharmonic frequencies. Second panel: the local residual light curve spanning 70 days. Third panel: the residual light curve of all data, spanning approximately 1459.5 days. Bottom panel: average transit depth diagram calculated over the phase range where the signal appears. Each gray point represents the signal strength for a single period, and the black solid line shows the trend obtained through a moving average.
Paper: The Transit Signal of KOI-1755 Originates from a Background Eclipsing Binary Star—Extracting the Light Curve of a Faint Background Star from Kepler Target Pixel File Data
Authors: Haozhi Wang, Ali Esamdin, Chenglong Lv, Lixian Shen, Jin-zhong Liu, Abdusamatjan Iskandar, Umut Mahmut, Rivkat Karimov, Shuhrat A. Ehgamberdiev
Figure caption: Kepler TPFs image for KOI-1755 at cadence 1105 (first frame of quarter 0). The horizontal and vertical axes indicate pixel indices, each corresponding to a photosensitive element on the Kepler CCD. Pixels are shown in grayscale according to flux values, and the color bar represents flux. The “N/A” in the top-left corner indicates that the pixel has no data.
Paper: The Transit Signal of KOI-1755 Originates from a Background Eclipsing Binary Star—Extracting the Light Curve of a Faint Background Star from Kepler Target Pixel File Data
Authors: Haozhi Wang, Ali Esamdin, Chenglong Lv, Lixian Shen, Jin-zhong Liu, Abdusamatjan Iskandar, Umut Mahmut, Rivkat Karimov, Shuhrat A. Ehgamberdiev
Figure caption: The centroid positions of KOI-1755 in each frame image, extracted from the TPF file, illustrating their distribution across four clustered regions.
Paper: The Transit Signal of KOI-1755 Originates from a Background Eclipsing Binary Star—Extracting the Light Curve of a Faint Background Star from Kepler Target Pixel File Data
Authors: Haozhi Wang, Ali Esamdin, Chenglong Lv, Lixian Shen, Jin-zhong Liu, Abdusamatjan Iskandar, Umut Mahmut, Rivkat Karimov, Shuhrat A. Ehgamberdiev
Figure caption: Top panel: time series of the centroid column position of KOI-1755 in Quarter 0. Bottom panel: residual light curve after removing pulsation signals in Quarter 0.
Paper: The Transit Signal of KOI-1755 Originates from a Background Eclipsing Binary Star—Extracting the Light Curve of a Faint Background Star from Kepler Target Pixel File Data
Authors: Haozhi Wang, Ali Esamdin, Chenglong Lv, Lixian Shen, Jin-zhong Liu, Abdusamatjan Iskandar, Umut Mahmut, Rivkat Karimov, Shuhrat A. Ehgamberdiev
Figure caption: Top panel: corrected and smoothed light curves of KOI-1755, spanning approximately 1459.5 days. Bottom panel: the Fourier amplitude spectrum of the corrected and smoothed light curve of KOI-1755.
Paper: The Transit Signal of KOI-1755 Originates from a Background Eclipsing Binary Star—Extracting the Light Curve of a Faint Background Star from Kepler Target Pixel File Data
Authors: Haozhi Wang, Ali Esamdin, Chenglong Lv, Lixian Shen, Jin-zhong Liu, Abdusamatjan Iskandar, Umut Mahmut, Rivkat Karimov, Shuhrat A. Ehgamberdiev
Figure caption: Top-left panel: TPFs image for Quarter 3 with labels indicating the important pixel numbers. Top-right panel: estimation of the time-varying centroid position of KOI-1755 from the TPFs. Bottom-left panel: pixel-level flux distribution during the first eclipse in Quarter 3. Bottom-right panel: pixel-level flux distribution during the last eclipse in Quarter 3.
Paper: The Transit Signal of KOI-1755 Originates from a Background Eclipsing Binary Star—Extracting the Light Curve of a Faint Background Star from Kepler Target Pixel File Data
Authors: Haozhi Wang, Ali Esamdin, Chenglong Lv, Lixian Shen, Jin-zhong Liu, Abdusamatjan Iskandar, Umut Mahmut, Rivkat Karimov, Shuhrat A. Ehgamberdiev
Figure caption: Schematic diagram of the simulated grid. The larger black frame indicates the region corresponding to the TPFs, while the smaller black frame represents the pixel aperture used for photometry of the TSS star. The black dots denote the positions of the five stars included in the simulation.
Paper: The Transit Signal of KOI-1755 Originates from a Background Eclipsing Binary Star—Extracting the Light Curve of a Faint Background Star from Kepler Target Pixel File Data
Authors: Haozhi Wang, Ali Esamdin, Chenglong Lv, Lixian Shen, Jin-zhong Liu, Abdusamatjan Iskandar, Umut Mahmut, Rivkat Karimov, Shuhrat A. Ehgamberdiev
Figure caption: Top panel: light curve obtained from photometry performed on the TPFs using a 3 × 3 pixel aperture centered on the centroid pixel of KOI-1755. Second panel: simulated contamination light curve for the selected TSS star aperture. Third panel: original TSS starlight curve obtained from photometry performed on the TPFs using a 2 × 2 pixel aperture centered at the location provided in Table 4. Bottom panel: contamination-corrected TSS starlight curve.
Paper: The Transit Signal of KOI-1755 Originates from a Background Eclipsing Binary Star—Extracting the Light Curve of a Faint Background Star from Kepler Target Pixel File Data
Authors: Haozhi Wang, Ali Esamdin, Chenglong Lv, Lixian Shen, Jin-zhong Liu, Abdusamatjan Iskandar, Umut Mahmut, Rivkat Karimov, Shuhrat A. Ehgamberdiev
Figure caption: The 11 targets in the Gaia DR3 that are closest to the coordinates of KOI-1755, with marker sizes representing their relative Gmag.
Paper: The Transit Signal of KOI-1755 Originates from a Background Eclipsing Binary Star—Extracting the Light Curve of a Faint Background Star from Kepler Target Pixel File Data
Authors: Haozhi Wang, Ali Esamdin, Chenglong Lv, Lixian Shen, Jin-zhong Liu, Abdusamatjan Iskandar, Umut Mahmut, Rivkat Karimov, Shuhrat A. Ehgamberdiev
Figure caption: Top panel: frequency spectrum of the light curve for the pixel containing the centroid. Middle panel: frequency spectrum of the light curve for the pixel at column –1 from the centroid pixel. Bottom panel: frequency spectrum of the light curve for the pixel at column –2 from the centroid pixel.
Paper: The Transit Signal of KOI-1755 Originates from a Background Eclipsing Binary Star—Extracting the Light Curve of a Faint Background Star from Kepler Target Pixel File Data
Authors: Haozhi Wang, Ali Esamdin, Chenglong Lv, Lixian Shen, Jin-zhong Liu, Abdusamatjan Iskandar, Umut Mahmut, Rivkat Karimov, Shuhrat A. Ehgamberdiev
Figure caption: The basic conditions of the TPFs for these four states, with each state’s position corresponding to the locations of the four clusters shown in Figure 4. The white boxes indicate the selected aperture pixels for the TSS star in this state.
Paper: The Transit Signal of KOI-1755 Originates from a Background Eclipsing Binary Star—Extracting the Light Curve of a Faint Background Star from Kepler Target Pixel File Data
Authors: Haozhi Wang, Ali Esamdin, Chenglong Lv, Lixian Shen, Jin-zhong Liu, Abdusamatjan Iskandar, Umut Mahmut, Rivkat Karimov, Shuhrat A. Ehgamberdiev
Figure caption: Light curve extracted by PSFmachine.
Paper: The Transit Signal of KOI-1755 Originates from a Background Eclipsing Binary Star—Extracting the Light Curve of a Faint Background Star from Kepler Target Pixel File Data
Authors: Haozhi Wang, Ali Esamdin, Chenglong Lv, Lixian Shen, Jin-zhong Liu, Abdusamatjan Iskandar, Umut Mahmut, Rivkat Karimov, Shuhrat A. Ehgamberdiev
Figure caption: Simulation results, where pixel colors represent flux intensity, and dots, displayed in a color contrasting with the pixel color, denote the positions of the five stars included in the simulation.
Paper: The Transit Signal of KOI-1755 Originates from a Background Eclipsing Binary Star—Extracting the Light Curve of a Faint Background Star from Kepler Target Pixel File Data
Authors: Haozhi Wang, Ali Esamdin, Chenglong Lv, Lixian Shen, Jin-zhong Liu, Abdusamatjan Iskandar, Umut Mahmut, Rivkat Karimov, Shuhrat A. Ehgamberdiev
Figure caption: Light curves of pixels 1–4 during Quarter 3.
Paper: Constructing a Pristine View of Extended Globular Cluster Structure
Authors: Pete B. Kuzma, Miho N. Ishigaki, Takanobu Kirihara, Itsuki Ogami
Figure caption: (a) Radial distribution of [Fe/H]PGS for our sampled GCs. Stars with Pmem  >  0.5 are displayed and colored by their membership probability (top color bar). Underplotted is a density diagram that demonstrates the distribution of stars with Pmem  <  0.1 (most likely field members). Each star that is part of the conservative sample for each GC is marked with a black circle, along with their [Fe/H]PGS uncertainty displayed with error bars. The vertical dotted (dashed) lines indicate the tidal (Jacobi) radius, and the black horizontal lines show the mean [Fe/H]PGS in the conservative sample. (b) Radial distribution of [Fe/H]PGS for our sampled GCs. A continuation of panel (a).
Paper: Constructing a Pristine View of Extended Globular Cluster Structure
Authors: Pete B. Kuzma, Miho N. Ishigaki, Takanobu Kirihara, Itsuki Ogami
Figure caption: Comparison of the mean [Fe/H]PGS measurements across the three radial ranges for each GC. The radial ranges explored are denoted by the x- and y-axis labels, where ﹩{[\mathrm{Fe}/{\rm{H}}]}_{\mathrm{PGS}}^{{r}_{{c}{l}}}﹩ denotes the radial range that covers within the tidal radius, ﹩{[\mathrm{Fe}/{\rm{H}}]}_{\mathrm{PGS}}^{{r}_{{t}}}﹩ between the tidal radius and Jacobi radius, and ﹩{[\mathrm{Fe}/{\rm{H}}]}_{\mathrm{PGS}}^{{r}_{{J}}}﹩ outside the Jacobi radius. A one-to-one correspondence is indicated by the dashed diagonal line.
Paper: Measuring Long Stellar Rotation Periods (>10 days) from TESS FFI Light Curves is Possible: An Investigation Using TESS and ZTF
Authors: Soichiro Hattori, Ruth Angus, Daniel Foreman-Mackey, Yuxi (Lucy) Lu, Isabel Colman
Figure caption: A toy example showing the offset-corrected LS periodogram. The top panel shows a simulated sinusoidal signals with some Gaussian noise. The simulated light curve is broken up into eight equal chunks, represented by different colors in the top panel, similar to how a TESS target might be observed each sector. In the middle panel we show in black what the light curve would look like if each chunk was normalized according to its own median value. We subtract 1 from each light curve chunk to center it at zero. The dotted blue line shows the best-fit model obtained by running a standard LS periodogram. The orange solid line shows the best-fit model using the offset-corrected LS periodogram. In the bottom panel we show the obtained periodogram from each of the models (i.e., standard vs. offset-corrected). See Section 3.3 for more information on the offset-corrected LS.
Paper: Measuring Long Stellar Rotation Periods (>10 days) from TESS FFI Light Curves is Possible: An Investigation Using TESS and ZTF
Authors: Soichiro Hattori, Ruth Angus, Daniel Foreman-Mackey, Yuxi (Lucy) Lu, Isabel Colman
Figure caption: The detrended TESS light curve and period analysis for TIC 198459831. In the top panel we show the detrended normalized and centered detrended flux measurements (black dots), the sector boundaries (dashed lines), and the best-fit model (orange line). In the bottom-left panel we show the periodogram and indicate the period of P = 21.52 days corresponding to the highest power (red line). In the bottom right panel we show the phase-folded light curve and the amplitude of the oscillation. We can see that the recovered TESS period matches that measured from the ZTF light curve shown in Figure 1.
Paper: Measuring Long Stellar Rotation Periods (>10 days) from TESS FFI Light Curves is Possible: An Investigation Using TESS and ZTF
Authors: Soichiro Hattori, Ruth Angus, Daniel Foreman-Mackey, Yuxi (Lucy) Lu, Isabel Colman
Figure caption: Same figure as Figure 6 but with the power cut of power > 0.02 applied. While this removes a significant fraction of the samples, we see that it removes many of the mismatched periods in the lower right of Figure 6, increasing our match percentage.
Paper: Measuring Long Stellar Rotation Periods (>10 days) from TESS FFI Light Curves is Possible: An Investigation Using TESS and ZTF
Authors: Soichiro Hattori, Ruth Angus, Daniel Foreman-Mackey, Yuxi (Lucy) Lu, Isabel Colman
Figure caption: A plot comparing the periods measured from the ZTF light curves and the TESS light curves. The points are colored by their TESS peak powers. The 1:1 line with 10% uncertainties are indicated with the black line and the shaded region. The 1:2 line is indicated in red. A potential Lomb–Scargle failure mode caused by the window function of the TESS observing sector is indicated as a dashed blue line (more description in text).
Paper: Measuring Long Stellar Rotation Periods (>10 days) from TESS FFI Light Curves is Possible: An Investigation Using TESS and ZTF
Authors: Soichiro Hattori, Ruth Angus, Daniel Foreman-Mackey, Yuxi (Lucy) Lu, Isabel Colman
Figure caption: A source (TIC 219795667) where we measured a TESS period that is half of what was measured from ZTF. We can see that the second TESS periodogram peak at 43 days corresponds to the same period as that measured from ZTF.
Paper: Measuring Long Stellar Rotation Periods (>10 days) from TESS FFI Light Curves is Possible: An Investigation Using TESS and ZTF
Authors: Soichiro Hattori, Ruth Angus, Daniel Foreman-Mackey, Yuxi (Lucy) Lu, Isabel Colman
Figure caption: A plot showing the match (blue)and nonmatch (orange) rates as a function of the TESS power threshold. The black line indicates the fraction of remaining samples as we increase the power threshold.
Paper: Measuring Long Stellar Rotation Periods (>10 days) from TESS FFI Light Curves is Possible: An Investigation Using TESS and ZTF
Authors: Soichiro Hattori, Ruth Angus, Daniel Foreman-Mackey, Yuxi (Lucy) Lu, Isabel Colman
Figure caption: A source (TIC 353875094) where the shorter TESS-measured period of PTESS = 9.26 days is likely the correct rotation period instead of the ZTF-measured period of PZTF = 18.63 days. In the TESS periodogram we see that while there is a small peak at PZTF, the peak at PTESS is much stronger.
Paper: Measuring Long Stellar Rotation Periods (>10 days) from TESS FFI Light Curves is Possible: An Investigation Using TESS and ZTF
Authors: Soichiro Hattori, Ruth Angus, Daniel Foreman-Mackey, Yuxi (Lucy) Lu, Isabel Colman
Figure caption: An example of a source (TIC 165552443) where we measured a period of 50 days from both ZTF and TESS light curves. As an individual TESS sector is 27 days, this result shows it is possible to probe for periodic signals exceeding the length of a single sector.
Paper: Measuring Long Stellar Rotation Periods (>10 days) from TESS FFI Light Curves is Possible: An Investigation Using TESS and ZTF
Authors: Soichiro Hattori, Ruth Angus, Daniel Foreman-Mackey, Yuxi (Lucy) Lu, Isabel Colman
Figure caption: TESS FFI cutouts and detrended light curves for TIC 198459831. Each FFI cutout from a TESS sector is accompanied to its right by the detrended light curve.
Paper: Effects of Transient Stellar Emissions on Planetary Climates of Tidally Locked Exo-Earths
Authors: Howard Chen, Paolo De Luca, Assaf Hochman, Thaddeus D. Komacek
Figure caption: Same as Figure 3 but for N2O (a) and NO2 (b).
Paper: Effects of Transient Stellar Emissions on Planetary Climates of Tidally Locked Exo-Earths
Authors: Howard Chen, Paolo De Luca, Assaf Hochman, Thaddeus D. Komacek
Figure caption: Same as Figure 1, but for ozone (O3, mol mol−1) in natural logarithm.
Paper: Effects of Transient Stellar Emissions on Planetary Climates of Tidally Locked Exo-Earths
Authors: Howard Chen, Paolo De Luca, Assaf Hochman, Thaddeus D. Komacek
Figure caption: Same as Figure 2 but for wind speed (WS, m s−1), water vapor (H2O, mol mol−1), and nitrous oxide (NO2, mol mol−1). Star indicates flare and large flare boxplots not significantly different at the 1% level.
Paper: Collision Probability Evaluation of LAMOST Robotic Fiber Positioners in the Design Phase
Authors: Baolong Chen, Jianping Wang, Jiahao Zhou, Zhigang Liu, Hongzhuan Hu, Zengxiang Zhou, Feifan Zhang
Figure caption: Accessibility of unequal-arm RFP in different regions. The shading in the figure indicates the coverage of each region by the RFPs. The depth of the color indicates the coverage of a single area by the RFP: the darker the color, the more RFPs can reach that area.
Paper: Effects of Transient Stellar Emissions on Planetary Climates of Tidally Locked Exo-Earths
Authors: Howard Chen, Paolo De Luca, Assaf Hochman, Thaddeus D. Komacek
Figure caption: Same as Figure 2 but for nitrous oxide (N2O) and nitrogen dioxide (NO2, mol mol−1) as natural logarithms.
Paper: Effects of Transient Stellar Emissions on Planetary Climates of Tidally Locked Exo-Earths
Authors: Howard Chen, Paolo De Luca, Assaf Hochman, Thaddeus D. Komacek
Figure caption: Same as Figure 2, but for nitrogen dioxide (NO2, mol mol−1) and ozone (O3, mol mol−1).
Paper: Collision Probability Evaluation of LAMOST Robotic Fiber Positioners in the Design Phase
Authors: Baolong Chen, Jianping Wang, Jiahao Zhou, Zhigang Liu, Hongzhuan Hu, Zengxiang Zhou, Feifan Zhang
Figure caption: Accessibility of equal-arm RFPs. Region (a): only one RFP can reach; region (b): two RFPs can reach; region (c): three RFPs can reach.
Paper: Collision Probability Evaluation of LAMOST Robotic Fiber Positioners in the Design Phase
Authors: Baolong Chen, Jianping Wang, Jiahao Zhou, Zhigang Liu, Hongzhuan Hu, Zengxiang Zhou, Feifan Zhang
Figure caption: Schematic of an equal-arm RFP. The dashed circle represents the patrol area of the RFP.
Paper: The Disks In Scorpius–Centaurus Survey (DISCS). I. Four Newly Resolved Debris Disks in Polarized Intensity Light
Authors: Justin Hom, Thomas M. Esposito, Katie A. Crotts, Gaspard Duchêne, Jennifer Patience, Johan Mazoyer, Robert J. De Rosa, Christine H. Chen, Paul Kalas, Bruce Macintosh, Brenda C. Matthews
Figure caption: Measured Fans/F* as a function of system infrared excess LIR/L* and stellar Teff. The black lines represent the median likelihood solutions with 1σ uncertainty to separate linear bootstrapping fits (gray lines). The non-Sco-Cen sample (triangles and dashed line) shows considerably higher Fans/F* overall compared to Sco-Cen systems (circles and solid line) at similar levels of LIR/L*.