adsabs/AstroCLIMB huggingface dataset:
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 ≥ 863 Hz.
Paper: SETI@home: Data Analysis and Findings
Authors: David P. Anderson, Eric J. Korpela, Dan Werthimer, Jeff Cobb, Bruce Allen
Figure caption: A pixel disk is centered at a pixel and has radius θbeam.
Paper: SETI@home: Data Analysis and Findings
Authors: David P. Anderson, Eric J. Korpela, Dan Werthimer, Jeff Cobb, Bruce Allen
Figure caption: The general structure of radio SETI projects.
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 from 6–13 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 medium bandwidth (6–13 Hz).
Paper: SETI@home: Data Analysis and Findings
Authors: David P. Anderson, Eric J. Korpela, Dan Werthimer, Jeff Cobb, Bruce Allen
Figure caption: Waterfall plot showing detections from a high scoring multiplet that is likely due to RFI. The detection at the center of the plot is indicated with a square.
Paper: SETI@home: Data Analysis and Findings
Authors: David P. Anderson, Eric J. Korpela, Dan Werthimer, Jeff Cobb, Bruce Allen
Figure caption: Global drift-rate/frequency pruning. The detections selected in window W3 are not compatible with those selected in W2; we must discard the one with lower value.
Paper: SETI@home: Data Analysis and Findings
Authors: David P. Anderson, Eric J. Korpela, Dan Werthimer, Jeff Cobb, Bruce Allen
Figure caption: Detections from a multiplet that was scored highly by both algorithms and manually.
Paper: SETI@home: Data Analysis and Findings
Authors: David P. Anderson, Eric J. Korpela, Dan Werthimer, Jeff Cobb, Bruce Allen
Figure caption: Local drift-rate/frequency pruning. We (a) find the drift rate interval containing the most detection power and (b) find the frequency interval that, when time-shifted by Cmedian, contains the most detection power.
Paper: SETI@home: Data Analysis and Findings
Authors: David P. Anderson, Eric J. Korpela, Dan Werthimer, Jeff Cobb, Bruce Allen
Figure caption: Spikes removed as a function of frequency band removed for DFT length 4096. The knee of this curve (in this case about 2%) determines the fraction of the frequency band removed by the zone RFI algorithm.
Paper: SETI@home: Data Analysis and Findings
Authors: David P. Anderson, Eric J. Korpela, Dan Werthimer, Jeff Cobb, Bruce Allen
Figure caption: Example of a multiplet summary page.
Paper: SETI@home: Data Analysis and Findings
Authors: David P. Anderson, Eric J. Korpela, Dan Werthimer, Jeff Cobb, Bruce Allen
Figure caption: M is the highest-scoring multiplet in W, but there may be a higher-scoring multiplet that overlaps M using higher-frequency detections.
Paper: SETI@home: Data Analysis and Findings
Authors: David P. Anderson, Eric J. Korpela, Dan Werthimer, Jeff Cobb, Bruce Allen
Figure caption: Birdie detections are generated when a telescope beam passes close to the birdie sky position.
Paper: SETI@home: Data Analysis and Findings
Authors: David P. Anderson, Eric J. Korpela, Dan Werthimer, Jeff Cobb, Bruce Allen
Figure caption: Frequency-zone RFI algorithm.
Paper: The Investigation of 84 TESS Totally Eclipsing Contact Binaries
Authors: Yani Guo, Kai Li, Liheng Wang, Qiqi Xia, Xiang Gao, Jingran Xu, Jingyi Wang
Figure caption: The posterior distributions of q, T2, i, f, L1/LT, λ, rs, Ts, and the fitting light curve of TIC 232063593.
Paper: The Investigation of 84 TESS Totally Eclipsing Contact Binaries
Authors: Yani Guo, Kai Li, Liheng Wang, Qiqi Xia, Xiang Gao, Jingran Xu, Jingyi Wang
Figure caption: The M–L and M–R relations for 84 contact binaries.
Paper: The Investigation of 84 TESS Totally Eclipsing Contact Binaries
Authors: Yani Guo, Kai Li, Liheng Wang, Qiqi Xia, Xiang Gao, Jingran Xu, Jingyi Wang
Figure caption: The MT and Jorb relations for 84 contact binaries.
Paper: The Investigation of 84 TESS Totally Eclipsing Contact Binaries
Authors: Yani Guo, Kai Li, Liheng Wang, Qiqi Xia, Xiang Gao, Jingran Xu, Jingyi Wang
Figure caption: The relationship between P and a of the contact-binary stars from K. Li et al. (2021b).
Paper: The Investigation of 84 TESS Totally Eclipsing Contact Binaries
Authors: Yani Guo, Kai Li, Liheng Wang, Qiqi Xia, Xiang Gao, Jingran Xu, Jingyi Wang
Figure caption: Four examples of normalized phase-folded light curves: the gray points represent observed data, while the red points represent normal data.
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: Real-time tracks of the spider observation toward 3C 286 on 2020 September 12. The tracks were drifted along the equatorial east–west axis. For example, the beams M08, M02, M01, M05, and M14 are aligned from east to west as in Figure 1 when receiver rotation angle θ = 0°, but the beams M18, M07, M01, M04, and M12 are aligned from east to west when θ = 60°. Here we show the relative trajectories of the tracks with respect to the receiver center with θ at −60°, −30°, 0°, 30°,  and 60°.
Paper: The Investigation of 84 TESS Totally Eclipsing Contact Binaries
Authors: Yani Guo, Kai Li, Liheng Wang, Qiqi Xia, Xiang Gao, Jingran Xu, Jingyi Wang
Figure caption: The possible posterior distributions of q, a, Vγ and fitting curve of radial velocity of TIC 267043786. Vγ represents the radial velocity of the system.
Paper: The Investigation of 84 TESS Totally Eclipsing Contact Binaries
Authors: Yani Guo, Kai Li, Liheng Wang, Qiqi Xia, Xiang Gao, Jingran Xu, Jingyi Wang
Figure caption: The possible posterior distributions of q, a, Vγ and fitting curve of radial velocity of TIC 207174531.
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: The relative positions of the 19 beams to the receiver center at rotation angle θ = 0° in equatorial coordinates, with the numbering of the 19 beams from M01 to M19. Each beam circle has a diameter of the full width at half-maximum.
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: Flowchart of the 19-beam polarization calibration sequence.
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, ϵ, ϕ) of the central beam vs. observation dates in Modified Julian Date (MJD). The results of 3C 286, 3C 48, and 3C 138 are plotted as black circles, red squares, and blue diamonds, respectively. The results of 3C 380, J2202+4216, and 3C 273 are shown as cyan triangles.
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: The fractional Stokes parameters for 3C 286 vs. rotation angle θ on 2023 March 11. The black crosses, red diamonds, and blue squares show the Qobs/Iobs, Uobs/Iobs, and Vobs/Iobs data, respectively. The thick black, red, and blue curves show the fittings for Qsrc/Isrc, Usrc/Isrc, and Vsrc/Isrc, respectively. The gray curves show the equally likely alternative fits from the uncertainties of the fitted Mueller matrix parameters.
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) of the 19 beams. The parameters calibrated in 2020, 2021, and 2022 are shown with black circles, red squares, and blue diamonds, respectively.
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: Calibrated polarization percentages and polarization angles of 3C 286, 3C 48, and 3C 138 in the same color scheme as that in Figures 6 and 7. The polarization angles before and after the correction of the ionospheric Faraday rotation are denoted with open and filled data points, respectively. The dashed lines mark the VLA results at 1450 MHz in 2010 December (R. A. Perley & B. J. Butler 2013).
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, ϵ, ϕ) of the central beam versus frequency. The results obtained from the observations toward 3C138 on 2021/10/18 and 2021/11/06 are shown as black circles and red squares, respectively. Although the 2021/10/18 and 2021/11/06 data are obtained at the same frequency intervals, the data points are plotted slightly shifted in frequency to show the difference between the results of the two days.
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: Autocorrelation between any two data points of ΔG in Figure 6 by taking their difference in y-axis as variation and their difference in x-axis as time separation Δtime. Left: the correlations with Δtime shorter than 300 days. Right: the correlations of whole data sets.
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: A real-time track of the OTF observation toward 3C 138 on 2021 October 7.
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: The same data as in Figure 6, but vs. ZA.
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: The 19-beam Qobs/Iobs, Uobs/Iobs, and Vobs/Iobs data of 3C 138 on 2021 October 6, shown in black, red, and blue, respectively. The data before polarization calibration are shown in fainter colors than the data after polarization calibration.
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 TripleSpec spectrum of IRAS 16475–4609 used for spectral type determination. 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 H I (gray) and He I (blue) lines used for classification, together with DIBs and unknown features (magenta).
Paper: Exoplanet Classification Through Vision Transformers with Temporal Image Analysis
Authors: Anupma Choudhary, Sohith Bandari, B. S. Kushvah, C. Swastik
Figure caption: RPs for exoplanet classification. The upper two frames represent RPs for “not-planet” candidate cases, showing irregular patterns indicative of false positives. The lower two frames depict RPs for “planet” candidates, displaying clear, periodic structures consistent with true exoplanets.
Paper: Exoplanet Classification Through Vision Transformers with Temporal Image Analysis
Authors: Anupma Choudhary, Sohith Bandari, B. S. Kushvah, C. Swastik
Figure caption: (a) and (c) represent the global light curves of AFP and PC candidates, respectively, consisting of full-length data with a resolution of 2001 bin size. (b) and (d) represent the local light curves for the same candidates, which are fixed-length representations focusing on the transit region with a bin size of 201. Each plot highlights the key periodic features distinguishing these astrophysical phenomena.
Paper: Exoplanet Classification Through Vision Transformers with Temporal Image Analysis
Authors: Anupma Choudhary, Sohith Bandari, B. S. Kushvah, C. Swastik
Figure caption: GAFs for exoplanet classification. The upper two frames represent GAFs for “planet” cases, characterized by distinct periodic patterns indicative of planetary transits. The lower two frames show GAFs for “not-planet” candidate cases, which lack the clear periodic structures seen in true exoplanet detections, indicating the absence of exoplanets.
Paper: Exoplanet Classification Through Vision Transformers with Temporal Image Analysis
Authors: Anupma Choudhary, Sohith Bandari, B. S. Kushvah, C. Swastik
Figure caption: This diagram illustrates the transit crossing events observed in the light curve data for (KIC) candidate with ID 6922244. The plotted points represent the variations in flux as the exoplanet transits its host star, causing periodic dips in brightness.
Paper: Exoplanet Classification Through Vision Transformers with Temporal Image Analysis
Authors: Anupma Choudhary, Sohith Bandari, B. S. Kushvah, C. Swastik
Figure caption: ROC curve for the RPs-based model, comparing the performance of the general model (red) and the undersampled model (blue).
Paper: Exoplanet Classification Through Vision Transformers with Temporal Image Analysis
Authors: Anupma Choudhary, Sohith Bandari, B. S. Kushvah, C. Swastik
Figure caption: Architecture of the ViT model.
Paper: Exoplanet Classification Through Vision Transformers with Temporal Image Analysis
Authors: Anupma Choudhary, Sohith Bandari, B. S. Kushvah, C. Swastik
Figure caption: Confusion matrix for RPs data set, illustrating model performance. Class 0 represents “not-planet” candidates, while Class 1 represents “planet” candidates.
Paper: Exoplanet Classification Through Vision Transformers with Temporal Image Analysis
Authors: Anupma Choudhary, Sohith Bandari, B. S. Kushvah, C. Swastik
Figure caption: Confusion matrix for the GAFs data set, illustrating general model performance. Class 0 represents “not-planet” candidates, while Class 1 represents “planet” candidates.
Paper: Exoplanet Classification Through Vision Transformers with Temporal Image Analysis
Authors: Anupma Choudhary, Sohith Bandari, B. S. Kushvah, C. Swastik
Figure caption: ROC curve for the GAFs-based model, comparing the performance of the general model (red) and the undersampled model (blue).
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: Comparing our lithium equivalent width measurements to results from the literature for 12 stars (red stars) shows good agreement. The black line shows the one-to-one relation, with ±10% in dark gray and ±25% in light gray. We find that applying a correction for the Fe λ6707.4 line (D. R. Soderblom et al. 1993) results in a systematic underestimate of the literature abundances (blue circles). We conclude that our Gaussian fitting technique is robust to contamination from the Fe λ6707.4 line, so we do not include an additional correction to our reported equivalent width values. We take literature lithium equivalent widths for HIP 104075, HIP 105232, HIP 113905, HIP 35628, and HIP 97779 from P. Guillout et al. (2009); HIP 115147, HIP 43410, HIP 52462, and HIP 71631 from R. Wichmann et al. (2003); HIP 42438 from R. J. White et al. (2007); and HIP 43726 from Y. Takeda & S. Kawanomoto (2005).
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: Our double-Gaussian fitting technique allows us to robustly measure lithium equivalent widths and, in cases where lithium is not detected, place upper limits on the lithium equivalent widths. Left: the spectrum of HIP 41277 (SNR ∼ 75) covers both the Fe λ6705.1 line (used as a reference line) and the Li λ6707.79 feature. Black points with error bars are the APO/ARCES data, the dark-blue line represents the highest likelihood fit from the MCMC, and the light-blue lines are random draws from the posterior. We find a lithium equivalent width for HIP 41277 of 125 ± 5 mÅ. Right: an example spectrum (SNR ∼ 30) of an upper limit for lithium, from HIP 110663. Data are again black points with error bars, while yellow, red, and blue represent 1σ, 2σ, and 3σ upper limits, respectively. We find a 2σ upper limit of 30 mÅ for HIP 110663, which we use to set a lower limit on the age of the star.
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: An example of an age posterior for one star in our sample, HIP 41277, using BAFFLES (S. A. Stanford-Moore et al. 2020). From an adopted B – V of 1.03 ± 0.015 and a lithium equivalent width of 125 ± 5 mÅ, we derive an age posterior with a median age of 174 Myr and 68% confidence interval between 97 and 253 Myr. Lithium measurements, median ages, and 68% and 95% confidence intervals for the full sample are reported in Table 4.
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: Results from rejection sampling of combined Hipparcos and Gaia DR3 astrometry show the possible companion mass–period combinations responsible for the observed acceleration of HIP 669. Candidate companions include stellar binaries, brown dwarfs, and wide-separation giant planets. The near-infrared contrast of these substellar companions depends on the age of the star.
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 use a one-parameter fit to calibrate chromospheric S-values from APO/ARCES to values reported in the literature. We observe a ∼15% scatter in the relationship, which we largely attribute to the intrinsic variability in chromospheric activity for each star. Error bars represent the maximum and minimum S-value reported in the literature for each star. We report S-values and ﹩{\rm{l}}{\rm{o}}{\rm{g}}({R}_{HK}^{{\prime} })﹩ for all the accelerating stars in Table 5.
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: An example age posterior for HIP 669, using our APO/ARCES measurement and BAFFLES (S. A. Stanford-Moore et al. 2020). For this relatively inactive star, with ﹩{\mathrm{log}}({R}_{HK}^{{\prime} })=-4.88﹩ and B − V = 0.62 ± 0.015, we derive an age posterior with a median age of 6.5 Gyr and 68% confidence interval between 3.8 and 9.7 Gyr.
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 confirm that our lithium fitting routine reliably recovers accurate equivalent widths with injection/recovery tests on five stars. We chose these stars since they had no detectable lithium and because they cover a range of SNR and spectral types. The recovered equivalent widths are all within ≲1 mÅ of the injected value and consistent with reported error bars.
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: The S-value is measured from spectra using triangular transmission profiles (red lines) centered on the Ca II H and K emission lines and rectangular profiles (blue lines) to measure the nearby continuum level. The top two panels show an example of a low-activity star with no significant H and K emission (HIP 102040), and the bottom two panels show HIP 115147, a star with strong H and K emission.
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: apparent Gaia G magnitude of the accelerating stars as a function of distance. Right: CMD of the sample. The median of our sample is GBP − GRP = 1.4 (∼K5), 41.5 pc, and G = 9.6. Our sample covers a wide range of spectral types, so we require a variety of age tracers to derive ages for each star.