adsabs/AstroCLIMB huggingface dataset:
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 ratio of average RV measurement error (﹩\overline{{\sigma }_{{\rm{RV}}}}﹩) to the RV rms measurement of targets in our sample. An RV error-to-rms ratio less than 1 indicates that the observed RV scatter is large and that activity or dynamical signals from a companion dominate over scatter associated with individual RV measurement precision. Objects with a low uncertainty ratio but high RV rms value may be promising planet candidates.
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 systems (2MASS J19224278−0515536, BD +05 4576, BD +21 418 B, BD +25 430, Cl Melotte 22 102, HD 21845, HD 21845 B, HD 240622, HD 26090, HD 285663, RX J0520.5+0616, V1084 Tau, V1168 Tau, V1274 Tau, and V1282 Tau). Pre- and post-maintenance HPF RVs are plotted as blue and purple points, respectively. Post-maintenance RVs are corrected with the empirically measured velocity offset reported in Appendix D. Long-period orbital motion is evident for BD +21 418 B and HD 285663.
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: Search completeness function of the EGPM survey as a function of RV semiamplitude (top) and minimum planetary mass (bottom). The 5%, 50%, and 95% completeness contour lines are shown as dotted, dashed, and solid black lines, respectively. The yellow star represents the detected planet candidate HS Psc b (Q. H. Tran et al. 2024).
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: Summary of RV observations for the EGPM statistical sample. A total of 91% our targets have at least seven epochs of RVs and a baseline of at least 4 yr.
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 rms, or intrinsic RV variability, as a function of projected rotational velocity, stellar spectral type, and stellar age for all stars in our sample.
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 HD 23975, HD 24194, HD 24463, HD 244945, and HD 24681.
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 Cl* Melotte 22 DH 352, Cl* Melotte 22 DH 875, Cl Melotte 22 2126, Cl Melotte 22 248, and Cl Melotte 22 513.
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 BD −03 5579, BD −05 1229, BD −08 1195, BD −08 995, and BD −09 1108.
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 Cl Melotte 22 659, EX Cet, HD 147512, HD 16760B, and HD 189285.
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 BD +17 641, BD +20 1790, BD +21 418, BD +21 504, and BD +22 548.
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 BD +23 527, BD +25 610, BD +26 592, BD +41 4749, and BD +49 646.
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 HD 26257, HD 282954, HD 282958, HD 283869, and HD 285367.
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 HD 286693, HD 287167, HD 29621, HD 48370, and HS Psc.
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 HD 20439, HD 221239, HD 22680, HD 23464, and HD 236717.
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 V814 Tau, V815 Tau, V963 Tau, V966 Tau, and Wolf 1259.
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 StKM 1-382, StKM 1-543, TYC 1090-543-1, TYC 1853-1452-1, and TYC 3385-23-1.
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 OT Tau, PR Tau, PW And, Parenago 2752, and RX J0520.0+0612.
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 V1169 Tau, V1173 Tau, V1174 Tau, V1841 Ori, and V370 Tau.
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 V446 Tau, V623 Tau, V677 Tau, V700 Tau, and V810 Tau.
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 HW Cet, IS Eri, LP 745-70, MR Tau, and NX Aqr.
Paper: SETI@home: Data Analysis and Findings
Authors: David P. Anderson, Eric J. Korpela, Dan Werthimer, Jeff Cobb, Bruce Allen
Figure caption: A waterfall plot showing drifting RFI. The left panel shows detections in time/frequency space, and the right panel shows the distance in sky position from the center detection to each of the seven beams. The black box in the left panel is centered on the center detection.
Paper: SETI@home: Data Analysis and Findings
Authors: David P. Anderson, Eric J. Korpela, Dan Werthimer, Jeff Cobb, Bruce Allen
Figure caption: The drifting RFI algorithm constructs fans of triangles in time/frequency space, and looks for triangles containing an excess of detections.
Paper: SETI@home: Data Analysis and Findings
Authors: David P. Anderson, Eric J. Korpela, Dan Werthimer, Jeff Cobb, Bruce Allen
Figure caption: The SETI@home data analysis process.
Paper: On-axis Polarization Calibration of the FAST L-band 19-beam Receiver
Authors: Tao-Chung Ching, 道沖 慶, Carl Heiles, Di Li, Timothy Robishaw, Xunzhou Chen, Lingqi Meng, You-Ling Yue, Lei Qian, Hong-Fei Liu
Figure caption: Parameters (ΔG, ψ, α, ϵ, ϕ) for the 19 beams on the eastern (black circles) and western (red squares) sides of the FAST reflector surface. The averaged values of the 19 beams of α, ϵ, and ϕ are shown as dotted lines.
Paper: On-axis Polarization Calibration of the FAST L-band 19-beam Receiver
Authors: Tao-Chung Ching, 道沖 慶, Carl Heiles, Di Li, Timothy Robishaw, Xunzhou Chen, Lingqi Meng, You-Ling Yue, Lei Qian, Hong-Fei Liu
Figure caption: Tracks of the receiver in geographic coordinates relative to the reflector surface center of FAST. The white circle represents the limit of full illumination at ZA = 26﹩\mathop{.}\limits^{\unicode{x000b0}}﹩4.
Paper: IRAS 16475–4609: A Young Compact H II Region Sculpting its Molecular Environment
Authors: Felipe Navarete, Sean D. Points, Augusto Damineli
Figure caption: Two-dimensional spectro-image of the order n = 3 (K band) resampled into a 2040 × 80 pixel linear grid.
Paper: IRAS 16475–4609: A Young Compact H II Region Sculpting its Molecular Environment
Authors: Felipe Navarete, Sean D. Points, Augusto Damineli
Figure caption: NEWFIRM/CTIO and VVV/VISTA observations of IRAS 16475−4609 . The central panel shows a false-color red–green–blue (RGB) map from VVV (blue: J, green: H, red: Ks) of a 85″ × 85″ region centered at R.A. = 16:51:14.156, decl. = −46:14:21.23 (J2000). The white and gray rectangles indicate the A and B positions for the TripleSpec observations. A 30″ scale bar is indicated in the lower left region of the panel. The top left panel shows the NEWFIRM K-band image of the same FOV, overlaid by contours highlighting the continuum emission at 15%, 30%, 45%, and 60% of the nebulosity peak intensity. The other panels show the continuum-subtracted H2 map (2.12 μm, lower left), Fe II (1.644 μm, upper right), and Brγ (2.166 μm, lower right), overlaid by the K-band contours.
Paper: IRAS 16475–4609: A Young Compact H II Region Sculpting its Molecular Environment
Authors: Felipe Navarete, Sean D. Points, Augusto Damineli
Figure caption: Top panel: spatial distribution of the mean flux of 11 H2 transitions along the slit direction (black curve). The gray points correspond to the Trot of the gas evaluated at each spaxel. The colored points correspond to the weighted mean Trot values for each of the three labeled H2 knots: A (blue triangle), B (black circle), and C (red diamond). Bottom: spatial distribution of the (1–0) S(1) and (2–1) S(1) transitions of the molecular hydrogen (blue and orange curves, respectively) corrected for extinction assuming AKs = 1.80 mag (Figure 9), and the line ratio measurements (gray points). The colored points correspond to the weighted mean Trot values for each of the three labeled H2 knots: A (blue triangle), B (black circle), and C (red diamond).
Paper: IRAS 16475–4609: A Young Compact H II Region Sculpting its Molecular Environment
Authors: Felipe Navarete, Sean D. Points, Augusto Damineli
Figure caption: VVV/VISTA observations of IRAS 16475−4609 in a 2﹩\mathop{.}\limits^{^{\prime} }﹩25 × 2﹩\mathop{.}\limits^{^{\prime} }﹩25 region. The map shows a false-color RGB image highlighting the nebular emission around the IRAS object. A 30″ scale bar is indicated in the lower left region of the panel. The contours indicate the emission at 870 μm from ATLASGAL (white curves), Australia Telescope Compact Array (ATCA) maps at 3 cm (red) and 6 cm (black), and NIR Brγ emission (cyan).
Paper: IRAS 16475–4609: A Young Compact H II Region Sculpting its Molecular Environment
Authors: Felipe Navarete, Sean D. Points, Augusto Damineli
Figure caption: Analysis of the molecular hydrogen emission associated with the nebular component of IRAS 16475−4609 . Top panel: Pearson correlation between the logarithm of the upper-level column density as a function of the upper-level energy of the H2 transitions by varying the AKs values from 0 to 3.3 mag in steps of 0.1 mag. The best AKs value is indicated by the vertical dashed red line, corresponding to the value that maximizes the correlation. Bottom panel: Boltzmann diagram of the H2 emission after correcting for reddening effects. The solid red line indicates the best fit to the data (values in the legend), and the shaded area shows the 1σ region of the fit. The corresponding Trot and Ntot values from the best fit are indicated as red text.
Paper: IRAS 16475–4609: A Young Compact H II Region Sculpting its Molecular Environment
Authors: Felipe Navarete, Sean D. Points, Augusto Damineli
Figure caption: Spectro-image of the H2 (1–0) S(1) transition at 2.1218 μm toward IRAS 16475−4609 . Top panels: spectro-images of the total flux (line + continuum, left) and the continuum-subtracted emission (right). The vertical dashed red line marks the center of the profile, while the vertical dotted red lines indicate the spectral range used to integrate the total flux. Bottom left: spatial distribution along the slit for the (a) total flux (line + continuum, dashed blue curve), (b) continuum-subtracted line emission (solid red curve), and (c) continuum emission (solid black). Bottom right: continuum-subtracted integrated spectrum. The vertical lines are the same as defined in the top right panel. The Gaussian fit to the emission line is shown by the dashed blue curve. The central wavelength, the integrated flux, and its error are indicated in the top left corner.
Paper: IRAS 16475–4609: A Young Compact H II Region Sculpting its Molecular Environment
Authors: Felipe Navarete, Sean D. Points, Augusto Damineli
Figure caption: Spectro-images of He I (λ = 2.0587 μm, left panel), H2 (1–0) S(1) (λ = 2.1218 μm, middle), and Brγ (λ = 2.1661 μm, right). The color bar to the right indicates the flux intensity for all three features. White contours represent the continuum emission, with the dashed and the solid lines at 10% and 50% of the peak intensity respectively marking the position of the point-like source.
Paper: IRAS 16475–4609: A Young Compact H II Region Sculpting its Molecular Environment
Authors: Felipe Navarete, Sean D. Points, Augusto Damineli
Figure caption: Continuum-normalized NIR spectrum of IRAS 16475−4609 (black curve) and the associated nebulosity (blue). The nebular spectrum was scaled by a factor of 0.05 with respect to the central source. Vertical dashed lines indicate the wavelength of relevant spectral features: H I (gray lines), He I (blue), Fe II (red), C I (yellow), [S II], diffuse interstellar bands (DIBs), and some unknown transitions (magenta).
Paper: IRAS 16475–4609: A Young Compact H II Region Sculpting its Molecular Environment
Authors: Felipe Navarete, Sean D. Points, Augusto Damineli
Figure caption: Zoom-in views around He I lines in the continuum-normalized NIR spectrum of IRAS 16475−4609 . The red curves are a sample of representative OB-type stars observed with TripleSpec (F. Navarete et al. 2025, in preparation), from top to bottom: HD 37468 (O9.5 V), HD 149438 (B0 V), HD 37042 (B0.7 V), HD 144470 (B1 V), HD 37744 (B1.5 V), and HD 36285 (B2 V). The vertical dashed lines indicate He I (blue), and C I (yellow) lines used for classification.
Paper: IRAS 16475–4609: A Young Compact H II Region Sculpting its Molecular Environment
Authors: Felipe Navarete, Sean D. Points, Augusto Damineli
Figure caption: Integrated flux of the extended emission along the slit. The Brγ, H2, and He I emission from Figure 7 are represented by the green, blue, and red curves, respectively. The black curve indicates the position of the point-like source. The top x-axis shows the slit direction in arcsecond units centered on the location of the point-like source.
Paper: Apache Point Observatory Follow-up of ACcelerating Candidate ExopLanet Host Stars (APO ACCELS): Ages for 166 Accelerating Stars in the Northern Hemisphere
Authors: Anne E. Peck, Eric L. Nielsen, Robert J. De Rosa, William Thompson, Bruce Macintosh, William Roberson, Adam J. R. W. Smith, Jessica Klusmeyer, Asif Abbas, Jason Jackiewicz, Jon Holtzman, Hannah Gallamore, Marah Brinjikji, Jennifer Patience, Jayke S. Nguyen, Alex Madurowicz, Dmitry Savransky
Figure caption: Age tracers used in this work for young, low-mass stars. This approximate schematic shows which combinations of age and mass are robustly covered by different age tracers. Each shaded region indicates where each tracer is most robust but does not include the regions where limits can be derived from each tracer (e.g., above the blue shaded region lithium is not expected to be detectable, but upper limits on lithium abundance can be used to derive lower limits on the age).
Paper: Apache Point Observatory Follow-up of ACcelerating Candidate ExopLanet Host Stars (APO ACCELS): Ages for 166 Accelerating Stars in the Northern Hemisphere
Authors: Anne E. Peck, Eric L. Nielsen, Robert J. De Rosa, William Thompson, Bruce Macintosh, William Roberson, Adam J. R. W. Smith, Jessica Klusmeyer, Asif Abbas, Jason Jackiewicz, Jon Holtzman, Hannah Gallamore, Marah Brinjikji, Jennifer Patience, Jayke S. Nguyen, Alex Madurowicz, Dmitry Savransky
Figure caption: We measure rotation periods for the accelerating stars by analyzing their periodograms and fitting sinusoids to their light curves. The TESS light curve for HIP 41277 is shown in black, with the best-fitting sinusoid with a period of 3.7 days overplotted in red. The orange curves represent the best-fitting period adjusted by the uncertainty measured from the width of the exponentiated periodogram peak. The right panel shows the exponentiated Lomb–Scargle periodogram with a significant peak at ∼3.7 days and the best-fitting Gaussian.
Paper: Apache Point Observatory Follow-up of ACcelerating Candidate ExopLanet Host Stars (APO ACCELS): Ages for 166 Accelerating Stars in the Northern Hemisphere
Authors: Anne E. Peck, Eric L. Nielsen, Robert J. De Rosa, William Thompson, Bruce Macintosh, William Roberson, Adam J. R. W. Smith, Jessica Klusmeyer, Asif Abbas, Jason Jackiewicz, Jon Holtzman, Hannah Gallamore, Marah Brinjikji, Jennifer Patience, Jayke S. Nguyen, Alex Madurowicz, Dmitry Savransky
Figure caption: We fit a sinusoid to the underlying rotation signal of an eclipsing binary system. The light curve for HIP 16247 is shown in gray. The masked data with the eclipses removed are shown in purple, and the best-fitting sinusoid is shown in red. This star is tidally locked with Porb ≈ Prot ≈ 3.98 days.
Paper: Apache Point Observatory Follow-up of ACcelerating Candidate ExopLanet Host Stars (APO ACCELS): Ages for 166 Accelerating Stars in the Northern Hemisphere
Authors: Anne E. Peck, Eric L. Nielsen, Robert J. De Rosa, William Thompson, Bruce Macintosh, William Roberson, Adam J. R. W. Smith, Jessica Klusmeyer, Asif Abbas, Jason Jackiewicz, Jon Holtzman, Hannah Gallamore, Marah Brinjikji, Jennifer Patience, Jayke S. Nguyen, Alex Madurowicz, Dmitry Savransky
Figure caption: Several of our target stars exhibit photometric variability that is inconsistent with rotation. Top: a light curve of HIP 59767, a γ Doradus variable (F. Kahraman Aliçavuş et al. 2016), shows a beat pattern, making it difficult to measure an underlying rotation period. Bottom: a light curve of HIP 22361 shows stochastic variability that is not attributed to rotation.
Paper: Apache Point Observatory Follow-up of ACcelerating Candidate ExopLanet Host Stars (APO ACCELS): Ages for 166 Accelerating Stars in the Northern Hemisphere
Authors: Anne E. Peck, Eric L. Nielsen, Robert J. De Rosa, William Thompson, Bruce Macintosh, William Roberson, Adam J. R. W. Smith, Jessica Klusmeyer, Asif Abbas, Jason Jackiewicz, Jon Holtzman, Hannah Gallamore, Marah Brinjikji, Jennifer Patience, Jayke S. Nguyen, Alex Madurowicz, Dmitry Savransky
Figure caption: Left: sum of all the age posteriors for the full sample. The distribution of ages is peaked at young ages, but this is partially due to the inclusion of early-type stars with shorter main-sequence lifetimes. Right: sum of age posteriors for only stars with B − V > 0.595, where there is still a peak at young ages, if less pronounced than for the full sample.