adsabs/AstroCLIMB huggingface dataset:
Paper: A Panchromatic Characterization of the Evening and Morning Atmosphere of WASP-107 b: Composition and Cloud Variations, and Insight into the Effect of Stellar Contamination
Authors: Matthew M. Murphy, Thomas G. Beatty, Everett Schlawin, Taylor J. Bell, Michael Radica, Thomas D. Kennedy, Nishil Mehta, Luis Welbanks, Michael R. Line, Vivien Parmentier, Thomas P. Greene, Sagnick Mukherjee, Jonathan J. Fortney, Kazumasa Ohno, Lindsey Wiser, Anastasia Triantafillides, Emily Rauscher, Isaac R. Edelman, Marcia J. Rieke
Figure caption: Gallery of light-curve residuals from our fits to the JWST/MIRI LRS spectroscopic light curves. Gray points are the light curve at native cadence, and black points are binned to ∼500 s cadence chosen to be consistent across all instruments (Figures B1–B5). Each channel’s residual time series is vertically offset for visual separation. Note that the left and middle panels share an offset, and the right panel has a different offset. The vertical blue lines demarcate the approximate four transit contacts to indicate ingress and egress.
Paper: A Panchromatic Characterization of the Evening and Morning Atmosphere of WASP-107 b: Composition and Cloud Variations, and Insight into the Effect of Stellar Contamination
Authors: Matthew M. Murphy, Thomas G. Beatty, Everett Schlawin, Taylor J. Bell, Michael Radica, Thomas D. Kennedy, Nishil Mehta, Luis Welbanks, Michael R. Line, Vivien Parmentier, Thomas P. Greene, Sagnick Mukherjee, Jonathan J. Fortney, Kazumasa Ohno, Lindsey Wiser, Anastasia Triantafillides, Emily Rauscher, Isaac R. Edelman, Marcia J. Rieke
Figure caption: Gallery of light-curve residuals from our fits to the JWST/NIRISS SOSS spectroscopic light curves. Gray points are the light curve at native cadence, and black points are binned to ∼500 s cadence chosen to be consistent across all instruments (Figures B1–B5). Each channel’s residual time series is vertically offset for visual separation. The vertical blue lines demarcate the approximate four transit contacts to indicate ingress and egress.
Paper: A Panchromatic Characterization of the Evening and Morning Atmosphere of WASP-107 b: Composition and Cloud Variations, and Insight into the Effect of Stellar Contamination
Authors: Matthew M. Murphy, Thomas G. Beatty, Everett Schlawin, Taylor J. Bell, Michael Radica, Thomas D. Kennedy, Nishil Mehta, Luis Welbanks, Michael R. Line, Vivien Parmentier, Thomas P. Greene, Sagnick Mukherjee, Jonathan J. Fortney, Kazumasa Ohno, Lindsey Wiser, Anastasia Triantafillides, Emily Rauscher, Isaac R. Edelman, Marcia J. Rieke
Figure caption: Investigating the impact starspot crossings have on our ability to detect and measure limb asymmetry. We used starry and catwoman to simulate transit observations of WASP-107 b when crossing spots at different locations on the star. Panel (A) shows an example of the starry stellar intensity map with a spot of contrast 0.1 and an angular radius of 5° at a longitude of 60°, pointed to by the arrow. Panel (B) shows its relative effect on the transit light curve via the difference between the light curve with and without the spot. Panel (C) shows how the spot longitude maps to the spot crossing’s location within the transit. Panel (D) shows the strength of the spot’s effect on the light curve as a function of its longitude via the peak value of the ratio of the light curve with and without the spot, i.e., the factor by which the relative flux increases due to the spot’s bump at its peak. In other words, the amplitude of the bump due to the spot is equal to the relative flux of the spot-free light curve at a given time (related to longitude via panel (C)) multiplied by the y-value. We then performed injection–recovery tests on these simulated spotted transit observations to test how the spot crossing impacts the best-fit evening- and morning-limb radii in cases where there is no underlying limb asymmetry (control case, panel (E)), and where there is underlying limb asymmetry (test case, panel (E)).
Paper: A Panchromatic Characterization of the Evening and Morning Atmosphere of WASP-107 b: Composition and Cloud Variations, and Insight into the Effect of Stellar Contamination
Authors: Matthew M. Murphy, Thomas G. Beatty, Everett Schlawin, Taylor J. Bell, Michael Radica, Thomas D. Kennedy, Nishil Mehta, Luis Welbanks, Michael R. Line, Vivien Parmentier, Thomas P. Greene, Sagnick Mukherjee, Jonathan J. Fortney, Kazumasa Ohno, Lindsey Wiser, Anastasia Triantafillides, Emily Rauscher, Isaac R. Edelman, Marcia J. Rieke
Figure caption: Temperature and circulation maps of WASP-107 b at various pressure levels from our cloudy SPARC/MITgcm model. Each panel represents a slice along a different isobar. The color mapping represents the gas temperature, and we use a different scaling in each panel. The lines with arrows represent the wind direction.
Paper: Semiempirical versus Theoretical Stellar Population Models: A Comparison with Star Clusters
Authors: Randa Asa'd, Paula R. T. Coelho, Johina M. John, Igor V. Chilingarian, Gustavo Bruzual, Stephane Charlot
Figure caption: Comparison of results for adev, χ2, log(LWA), light-weighted [Fe/H], and Av obtained from multipopulation fits. Left column: difference in derived values between MILES and SynCoMiL SPS models. Right column: difference in derived values between Coelho14ext and SynCoMiL SPS models. Dots are color-coded according to the goodness of fit: blue and green dots represent fits with χ2 ≤ 3 and χ2 > 3 for both SPS models, respectively. The black dots correspond to fits with χ2 ≤ 3 for one SPS model and >3 for the other.
Paper: Semiempirical versus Theoretical Stellar Population Models: A Comparison with Star Clusters
Authors: Randa Asa'd, Paula R. T. Coelho, Johina M. John, Igor V. Chilingarian, Gustavo Bruzual, Stephane Charlot
Figure caption: Comparison between the age derived using SPS models based on the Coelho14ext (y-axis) vs. the SynCoMiL (x-axis) stellar libraries. Age is shown in a linear scale to highlight the age interval where the comparison deviates more from the 1-to-1 line. The gray line represents the locally estimated scatterplot smoothing (LOESS) fit to the data, and the shaded area shows its confidence interval.
Paper: Semiempirical versus Theoretical Stellar Population Models: A Comparison with Star Clusters
Authors: Randa Asa'd, Paula R. T. Coelho, Johina M. John, Igor V. Chilingarian, Gustavo Bruzual, Stephane Charlot
Figure caption: Age and metallicity of the star clusters used in this work. Symbols are color-coded according to host galaxy.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Semiempirical versus Theoretical Stellar Population Models: A Comparison with Star Clusters
Authors: Randa Asa'd, Paula R. T. Coelho, Johina M. John, Igor V. Chilingarian, Gustavo Bruzual, Stephane Charlot
Figure caption: Same as Figure 3 but for parameters obtained using single SSP fits. Due to the overlap of points of different colors in the [Fe/H] panel, all dots are shown in black.
Paper: Semiempirical versus Theoretical Stellar Population Models: A Comparison with Star Clusters
Authors: Randa Asa'd, Paula R. T. Coelho, Johina M. John, Igor V. Chilingarian, Gustavo Bruzual, Stephane Charlot
Figure caption: Comparison of LWA and Av from the multipopulation fits with the age and Av from the single SSP fits.
Paper: Semiempirical versus Theoretical Stellar Population Models: A Comparison with Star Clusters
Authors: Randa Asa'd, Paula R. T. Coelho, Johina M. John, Igor V. Chilingarian, Gustavo Bruzual, Stephane Charlot
Figure caption: Behavior of Δt (the age derived from spectral fitting minus the age from isochrone fitting) for the subsample of clusters with high-resolution metallicities from the literature. Isochrone ages are from A. P. Milone et al. (2023) supplemented by the compilation in G. Gonçalves et al. (2020, Table 1). The top panel shows Δt as a function of metallicity. The tendency lines are obtained from LOESS. The bottom panel shows the density distribution of Δt. In both panels, the color code identifies the stellar library that was employed in modeling the SSP templates.
Paper: Semiempirical versus Theoretical Stellar Population Models: A Comparison with Star Clusters
Authors: Randa Asa'd, Paula R. T. Coelho, Johina M. John, Igor V. Chilingarian, Gustavo Bruzual, Stephane Charlot
Figure caption: Behavior of Δt (age derived from spectral fitting minus age from isochrone fitting) for our entire sample. Isochrone ages are from A. P. Milone et al. (2023) supplemented by the compilation in G. Gonçalves et al. (2020, Table 1). The top panel shows Δt as a function of literature age. The tendency lines are obtained from LOESS. The bottom panel shows the density distribution of Δt. In both panels, the color code identifies the stellar library that was employed in modeling the SSP templates.
Paper: Semiempirical versus Theoretical Stellar Population Models: A Comparison with Star Clusters
Authors: Randa Asa'd, Paula R. T. Coelho, Johina M. John, Igor V. Chilingarian, Gustavo Bruzual, Stephane Charlot
Figure caption: The top panel shows Δ[Fe/H] (STARLIGHT minus literature). The color-coded lines are linear fits obtained for each SSP template. The bottom panel shows the density distribution of Δ[Fe/H] = [Fe/H]STARLIGHT − [Fe/H]LITERATURE, color-coded by the SSP template.
Paper: Semiempirical versus Theoretical Stellar Population Models: A Comparison with Star Clusters
Authors: Randa Asa'd, Paula R. T. Coelho, Johina M. John, Igor V. Chilingarian, Gustavo Bruzual, Stephane Charlot
Figure caption: Comparison between the age inferred by STARLIGHT (y-axis) and ASAD (x-axis). In the left panel the vertical axis shows the LWA from a multipopulation fit, whereas in the right panel and the horizontal axis of both panels, we show the age of the best-fitting single SSP.
Paper: Semiempirical versus Theoretical Stellar Population Models: A Comparison with Star Clusters
Authors: Randa Asa'd, Paula R. T. Coelho, Johina M. John, Igor V. Chilingarian, Gustavo Bruzual, Stephane Charlot
Figure caption: Comparison between the age of LMC and SMC clusters determined by A. P. Milone et al. (2023; x-axis) and our STARLIGHT results (y-axis). The top panel shows the LWA (Equation (3)) and the bottom panel the SSP-EA (Section 3).
Paper: Finding New Hot Subdwarf Stars in SDSS Images
Authors: Jiangchuan Zhang, Yude Bu, Huili Wu, Yuhang Zhang, Shanshan Li, Zhenxin Lei, Zhenping Yi, Xiaoming Kong, Meng Liu
Figure caption: The structure of HsdDet. HsdDet has four modules, as shown in ①  ∼⑥. ①  Input module resizes the 1489 × 2048 pixels original image to 480 × 640 pixels. ② and ③  Backbone module extracts feature maps P1, P2, P3, P4, and P5 at 2×, 4×, 8×, 16×, and 32× downsampled scales. ④  Neck module utilizes the PANet to perform bidirectional fusion of feature maps. ⑤ and ⑥  Head module consists of chief head and subhead, predicting the position, class, and confidence of three bounding boxes for each grid on feature map.
Paper: Finding New Hot Subdwarf Stars in SDSS Images
Authors: Jiangchuan Zhang, Yude Bu, Huili Wu, Yuhang Zhang, Shanshan Li, Zhenxin Lei, Zhenping Yi, Xiaoming Kong, Meng Liu
Figure caption: Some images from SDSS science archive server (SAS) used in our study. These images are ﹩13\mathop{.}\limits^{{\rm{^{\prime} }}}\,52\times 9\mathop{.}\limits^{{\rm{^{\prime} }}}\,83﹩. The pixel scale is 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩396 per pixel. So, the pixel size of images is 2048 × 1489 pixels.
Paper: Finding New Hot Subdwarf Stars in SDSS Images
Authors: Jiangchuan Zhang, Yude Bu, Huili Wu, Yuhang Zhang, Shanshan Li, Zhenxin Lei, Zhenping Yi, Xiaoming Kong, Meng Liu
Figure caption: An image containing a hot subdwarf. The target coordinate is (211.63 deg, −11.28 deg). The image size is 2048 × 1489 pixels, and this hot subdwarf star occupies 8 × 8 pixels, accounting for 0.00209%. The larger image in the bottom left corner represents a magnified view of the white box in the top right corner. Annotation box is 30 × 30 pixels for illustration only. The pixel scale is 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩396 per pixel.
Paper: Finding New Hot Subdwarf Stars in SDSS Images
Authors: Jiangchuan Zhang, Yude Bu, Huili Wu, Yuhang Zhang, Shanshan Li, Zhenxin Lei, Zhenping Yi, Xiaoming Kong, Meng Liu
Figure caption: The sky distribution of search regions and candidates. Blue dots represent the BHB region. Gray dots represent the subdwarfs region. Green dots represent the candidates.
Paper: Finding New Hot Subdwarf Stars in SDSS Images
Authors: Jiangchuan Zhang, Yude Bu, Huili Wu, Yuhang Zhang, Shanshan Li, Zhenxin Lei, Zhenping Yi, Xiaoming Kong, Meng Liu
Figure caption: Apparent magnitude distribution and color–color diagram of the labeled objects in test and training sets.
Paper: Finding New Hot Subdwarf Stars in SDSS Images
Authors: Jiangchuan Zhang, Yude Bu, Huili Wu, Yuhang Zhang, Shanshan Li, Zhenxin Lei, Zhenping Yi, Xiaoming Kong, Meng Liu
Figure caption: Detected and undetected hot subdwarf samples. The first row represents the detected hot subdwarfs, while the second row represents the undetected hot subdwarfs.
Paper: Finding New Hot Subdwarf Stars in SDSS Images
Authors: Jiangchuan Zhang, Yude Bu, Huili Wu, Yuhang Zhang, Shanshan Li, Zhenxin Lei, Zhenping Yi, Xiaoming Kong, Meng Liu
Figure caption: Two candidates in an image detected by HsdDet. The candidates confidence are 0.88 and 0.90, respectively. The upper right corner shows a cropped subimage extracted from the original image for illustration.
Paper: Finding New Hot Subdwarf Stars in SDSS Images
Authors: Jiangchuan Zhang, Yude Bu, Huili Wu, Yuhang Zhang, Shanshan Li, Zhenxin Lei, Zhenping Yi, Xiaoming Kong, Meng Liu
Figure caption: Candidates confidence distribution on test set. Under a confidence threshold 0.5, all candidates have a probability of being hot subdwarf that is not less than 0.5.
Paper: Finding New Hot Subdwarf Stars in SDSS Images
Authors: Jiangchuan Zhang, Yude Bu, Huili Wu, Yuhang Zhang, Shanshan Li, Zhenxin Lei, Zhenping Yi, Xiaoming Kong, Meng Liu
Figure caption: Detected and undetected hot subdwarfs’ colors.
Paper: Finding New Hot Subdwarf Stars in SDSS Images
Authors: Jiangchuan Zhang, Yude Bu, Huili Wu, Yuhang Zhang, Shanshan Li, Zhenxin Lei, Zhenping Yi, Xiaoming Kong, Meng Liu
Figure caption: Detected and undetected hot subdwarfs’ reduced proper motion.
Paper: Finding New Hot Subdwarf Stars in SDSS Images
Authors: Jiangchuan Zhang, Yude Bu, Huili Wu, Yuhang Zhang, Shanshan Li, Zhenxin Lei, Zhenping Yi, Xiaoming Kong, Meng Liu
Figure caption: Confidence distribution of candidates.
Paper: Finding New Hot Subdwarf Stars in SDSS Images
Authors: Jiangchuan Zhang, Yude Bu, Huili Wu, Yuhang Zhang, Shanshan Li, Zhenxin Lei, Zhenping Yi, Xiaoming Kong, Meng Liu
Figure caption: Search regions and candidates distribution in HR diagram. The gradient blue-green background with GBP − GRP increase, represents the HR diagram samples from Gaia DR3. The blue points represent known hot subdwarfs from R. Culpan et al. (2022). From left to right, the red points represent the distribution of candidates, samples from the subdwarfs region, and samples from the BHB region, respectively. All points must be Gaia-homogeneous to be plotted together. These include 7855 candidates, 5134 in the subdwarf region, 87,200 in the BHB region, and 2603 from R. Culpan et al. (2022).
Paper: Finding New Hot Subdwarf Stars in SDSS Images
Authors: Jiangchuan Zhang, Yude Bu, Huili Wu, Yuhang Zhang, Shanshan Li, Zhenxin Lei, Zhenping Yi, Xiaoming Kong, Meng Liu
Figure caption: Teff and ﹩\mathrm{log}g﹩ diagram. The blue points represent known hot subdwarfs from R. Culpan et al. (2022). The red points represent new hotsubwarfs we found in this study. The zero-age horizontal branch (ZAHB) and terminal-age horizontal branch (TAHB) sequences are plotted for two different helium contents Y = 0.24 (dashed lines) and Y = 0.40 (solid lines) from M. Latour et al. (2018). The He-MS represented by the green solid line is from B. Paczynski (1971).
Paper: Finding New Hot Subdwarf Stars in SDSS Images
Authors: Jiangchuan Zhang, Yude Bu, Huili Wu, Yuhang Zhang, Shanshan Li, Zhenxin Lei, Zhenping Yi, Xiaoming Kong, Meng Liu
Figure caption: Color distribution of candidates. The gradient colors reflect the variation in frequency of candidates, with the highest frequency represented by the yellow region.
Paper: Finding New Hot Subdwarf Stars in SDSS Images
Authors: Jiangchuan Zhang, Yude Bu, Huili Wu, Yuhang Zhang, Shanshan Li, Zhenxin Lei, Zhenping Yi, Xiaoming Kong, Meng Liu
Figure caption: Distance distribution of the candidates. The histograms represent the distance distribution for the candidates and the labeled hot subdwarfs.
Paper: Finding New Hot Subdwarf Stars in SDSS Images
Authors: Jiangchuan Zhang, Yude Bu, Huili Wu, Yuhang Zhang, Shanshan Li, Zhenxin Lei, Zhenping Yi, Xiaoming Kong, Meng Liu
Figure caption: Reduced proper motion distribution of candidates. The kernel density estimation curves represent the distribution for the candidates and the labeled hot subdwarfs.
Paper: The Epoch of Giant Planet Migration Planet Search Program. III. The Occurrence Rate of Young Giant Planets inside the Water Ice Line 
Authors: Quang H. Tran, Brendan P. Bowler, William D. Cochran, Chad F. Bender, Samuel Halverson, Suvrath Mahadevan, Joe P. Ninan, Paul Robertson, Arpita Roy, Guðmundur Stefánsson, Ryan C. Terrien
Figure caption: Correlations between HPF RVs and various activity indicators for targets HD 236717, HS Psc, and PW And. From the top left to bottom right, each panel plots the correlations for the dLW (orange), the CRX (yellow), and the Ca II IRT indices for the Ca II 1, 2, and 3 IRT emission lines (purple, pink, and cyan, respectively). The best-fit slope (m), Pearson’s correlation coefficient (r), and corresponding p-value are reported at the top of each panel. Significant correlations (p ≤ 0.01) are denoted in panels where the best-fit linear correlation is overplotted as a dashed black line. The activity indicators for HD 236717 all exhibit significant correlations with the HPF RVs, indicating that observed RV signals are stellar activity driven.
Paper: The Epoch of Giant Planet Migration Planet Search Program. III. The Occurrence Rate of Young Giant Planets inside the Water Ice Line 
Authors: Quang H. Tran, Brendan P. Bowler, William D. Cochran, Chad F. Bender, Samuel Halverson, Suvrath Mahadevan, Joe P. Ninan, Paul Robertson, Arpita Roy, Guðmundur Stefánsson, Ryan C. Terrien
Figure caption: TESS light curves for systems that have significant peaks in their periodograms. The best-fit Gaussian process model and 1σ variance are plotted as solid blue lines and shaded regions, respectively. The posterior distributions and MAP values (dashed vertical line) for the quasi-periodic Gaussian process Prot hyperparameter are displayed in the right panels for targets HS Psc and PW And.
Paper: The Epoch of Giant Planet Migration Planet Search Program. III. The Occurrence Rate of Young Giant Planets inside the Water Ice Line 
Authors: Quang H. Tran, Brendan P. Bowler, William D. Cochran, Chad F. Bender, Samuel Halverson, Suvrath Mahadevan, Joe P. Ninan, Paul Robertson, Arpita Roy, Guðmundur Stefánsson, Ryan C. Terrien
Figure caption: HPF RV measurements, GLS periodograms, and corresponding spectral window functions for targets HD 236717, HS Psc, and PW And. The orange dashed horizontal line represents the FAP = 0.01% threshold. The most significant peak in the periodogram is highlighted with a blue vertical line. The GLS periodogram is computed up to a period of 1500 days, but a period of only 50 days is shown for each target, as all significant peaks have periods less than 50 days.
Paper: The Epoch of Giant Planet Migration Planet Search Program. III. The Occurrence Rate of Young Giant Planets inside the Water Ice Line 
Authors: Quang H. Tran, Brendan P. Bowler, William D. Cochran, Chad F. Bender, Samuel Halverson, Suvrath Mahadevan, Joe P. Ninan, Paul Robertson, Arpita Roy, Guðmundur Stefánsson, Ryan C. Terrien
Figure caption: The rms of various activity indicators as a function of projected rotational velocity, stellar spectral type, and stellar age for all stars in our sample without stellar companions. Beginning from the top, each row displays the dLW (orange), the CRX (yellow), and the Ca II IRT indices for the Ca II 1, 2, and 3 IRT emission lines (purple, pink, and cyan, respectively).
Paper: The Epoch of Giant Planet Migration Planet Search Program. III. The Occurrence Rate of Young Giant Planets inside the Water Ice Line 
Authors: Quang H. Tran, Brendan P. Bowler, William D. Cochran, Chad F. Bender, Samuel Halverson, Suvrath Mahadevan, Joe P. Ninan, Paul Robertson, Arpita Roy, Guðmundur Stefánsson, Ryan C. Terrien
Figure caption: HPF time series and corresponding completeness functions for targets 2MASS J03402958+2333040, 2MASS J03433440+2345429, 2MASS J03444398+2413523, 2MASS J03445383+2355165, and 2MASS J03474811+2313053.
Paper: The Epoch of Giant Planet Migration Planet Search Program. III. The Occurrence Rate of Young Giant Planets inside the Water Ice Line 
Authors: Quang H. Tran, Brendan P. Bowler, William D. Cochran, Chad F. Bender, Samuel Halverson, Suvrath Mahadevan, Joe P. Ninan, Paul Robertson, Arpita Roy, Guðmundur Stefánsson, Ryan C. Terrien
Figure caption: RV curve of HD 130322 phase-folded to the best-fit orbital period. The blue and orange points denote the pre- and post-maintenance HPF RVs, respectively, and the best-fit Keplerian model is shown as the solid black line. The gray points represent RV measurements from other instruments. The fit residuals are plotted in the bottom panel.
Paper: The Epoch of Giant Planet Migration Planet Search Program. III. The Occurrence Rate of Young Giant Planets inside the Water Ice Line 
Authors: Quang H. Tran, Brendan P. Bowler, William D. Cochran, Chad F. Bender, Samuel Halverson, Suvrath Mahadevan, Joe P. Ninan, Paul Robertson, Arpita Roy, Guðmundur Stefánsson, Ryan C. Terrien
Figure caption: HPF RVs of excluded binary (V1874 Ori, V366 Tau, and V395 Peg) and field-age (HD 130322) systems. Long-period orbital motion is evident for V1874 Ori.
Paper: The Epoch of Giant Planet Migration Planet Search Program. III. The Occurrence Rate of Young Giant Planets inside the Water Ice Line 
Authors: Quang H. Tran, Brendan P. Bowler, William D. Cochran, Chad F. Bender, Samuel Halverson, Suvrath Mahadevan, Joe P. Ninan, Paul Robertson, Arpita Roy, Guðmundur Stefánsson, Ryan C. Terrien
Figure caption: HPF RV time series for the three standard stars, HD 221354, HD 116442, and HD 3765. Pre-maintenance and uncorrected post-maintenance RVs are shown as blue and gray circles, respectively. Post-maintenance RVs corrected with the empirically measured offset, −53.1 ± 2.7 m s−1, are plotted as purple points.
Paper: The Epoch of Giant Planet Migration Planet Search Program. III. The Occurrence Rate of Young Giant Planets inside the Water Ice Line 
Authors: Quang H. Tran, Brendan P. Bowler, William D. Cochran, Chad F. Bender, Samuel Halverson, Suvrath Mahadevan, Joe P. Ninan, Paul Robertson, Arpita Roy, Guðmundur Stefánsson, Ryan C. Terrien
Figure caption: HPF time series and corresponding completeness functions for targets 2MASS J03515733+2320219, 2MASS J05234246+0651581, ASAS J232157+0721.3, BD +11 1690, and BD +17 455.
Paper: SETI@home: Data Analysis and Findings
Authors: David P. Anderson, Eric J. Korpela, Dan Werthimer, Jeff Cobb, Bruce Allen
Figure caption: Nonbarycentric multiplets may include detections over a frequency range of up to 308 kHz.
Paper: SETI@home: Data Analysis and Findings
Authors: David P. Anderson, Eric J. Korpela, Dan Werthimer, Jeff Cobb, Bruce Allen
Figure caption: Candidate sensitivity to nonbarycentric signals with bandwidth <0.1 Hz.
Paper: SETI@home: Data Analysis and Findings
Authors: David P. Anderson, Eric J. Korpela, Dan Werthimer, Jeff Cobb, Bruce Allen
Figure caption: Candidate sensitivity to nonbarycentric signals with bandwidth ≥863 Hz.
Paper: SETI@home: Data Analysis and Findings
Authors: David P. Anderson, Eric J. Korpela, Dan Werthimer, Jeff Cobb, Bruce Allen
Figure caption: Candidate sensitivity to barycentric signals with bandwidth ≤0.1 Hz.