adsabs/AstroCLIMB huggingface dataset:
Paper: HATS-38 b and WASP-139 b Join a Growing Group of Hot Neptunes on Polar Orbits 
Authors: Juan I. Espinoza-Retamal, Guđmundur Stefánsson, Cristobal Petrovich, Rafael Brahm, Andrés Jordán, Elyar Sedaghati, Jennifer P. Lucero, Marcelo Tala Pinto, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: Observations of HATS-38 along with the best-fit model. All error bars include a white noise jitter term. (a) ESPRESSO observations of the RM effect. The red line and shaded area correspond to the best and 1σ models, respectively. (b) Phase-folded out-of-transit RVs showing 1σ, 2σ, and 3σ models. (c) Residuals of the model for the RVs as a function of time. (d)–(j) Different light curves. We show the binned TESS Year 5 data in black.(The data used to create this figure are available.)(The data used to create this figure are available.)
Paper: HATS-38 b and WASP-139 b Join a Growing Group of Hot Neptunes on Polar Orbits 
Authors: Juan I. Espinoza-Retamal, Guđmundur Stefánsson, Cristobal Petrovich, Rafael Brahm, Andrés Jordán, Elyar Sedaghati, Jennifer P. Lucero, Marcelo Tala Pinto, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: Same as Figure 1 but for WASP-139. White points in the RM effect plot were not considered for the fit given their low S/N due to increased cloud coverage during those exposures. Including or removing those points results in the same constraints on the sky-projected obliquity.(The data used to create this figure are available.)(The data used to create this figure are available.)
Paper: HATS-38 b and WASP-139 b Join a Growing Group of Hot Neptunes on Polar Orbits 
Authors: Juan I. Espinoza-Retamal, Guđmundur Stefánsson, Cristobal Petrovich, Rafael Brahm, Andrés Jordán, Elyar Sedaghati, Jennifer P. Lucero, Marcelo Tala Pinto, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: Stellar obliquity distribution of Neptunes (blue) and Jupiters (orange). (a) Inferred distribution using the HBM with an informative ﹩{ \mathcal N }(0,3)﹩ prior on the ﹩\mathrm{log}\kappa ﹩ parameter. This inference was done following the methodology from J. Dong & D. Foreman-Mackey (2023) and based purely on observed sky-projected obliquities available in the literature—combined with the two sky-projected obliquity measurements presented here—without including information about the stellar inclination. The lines and shaded regions represent the median and 1σ uncertainties of the inferred distributions. (b) Same as panel (a) but using an uninformative ﹩{ \mathcal U }(-4,10)﹩ prior on ﹩\mathrm{log}\kappa ﹩. (c) Observed true 3D stellar obliquities from TEPCat for visual reference (17 Neptunes and 30 Jupiters; J. Southworth 2011). The true obliquity distribution also hints at a peak of polar Neptunes as inferred from the HBM.
Paper: HATS-38 b and WASP-139 b Join a Growing Group of Hot Neptunes on Polar Orbits 
Authors: Juan I. Espinoza-Retamal, Guđmundur Stefánsson, Cristobal Petrovich, Rafael Brahm, Andrés Jordán, Elyar Sedaghati, Jennifer P. Lucero, Marcelo Tala Pinto, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: (a) Sky-projected obliquities of Neptunes (10 < M  p /M ⊕ < 50 or 2 < R  p /R ⊕ < 6) as a function of stellar effective temperature (blue). Neptunes in compact multiplanet systems are shown as squares, while isolated Neptunes are shown as circles. Jupiters (non-Neptunes with R  p /R ⊕ > 6) and super-Earths (non-Neptunes with R  p /R ⊕ < 2) are shown in orange and gray, respectively. Data from TEPCat (J. Southworth 2011). (b) Histograms of the λ distribution for Neptunes (blue) and Jupiters (orange).
Paper: Analysis of Ring Galaxies Detected Using Deep Learning with Real and Simulated Data
Authors: Harish Krishnakumar, J. Bryce Kalmbach
Figure caption: Frequency histogram of magnitudes for a random sample of around 1000 galaxies from the Galaxy Zoo 2 catalog and the Goddard–Shamir catalog.
Paper: Analysis of Ring Galaxies Detected Using Deep Learning with Real and Simulated Data
Authors: Harish Krishnakumar, J. Bryce Kalmbach
Figure caption: An illustration of the residual connections of ResNet. The identity of the initial function, x, is added to the feature map after convolution, f(x), to produce the output.
Paper: Analysis of Ring Galaxies Detected Using Deep Learning with Real and Simulated Data
Authors: Harish Krishnakumar, J. Bryce Kalmbach
Figure caption: An illustration of a simple MLP. This contains an input layer, only one hidden layer, and an output layer.
Paper: HATS-38 b and WASP-139 b Join a Growing Group of Hot Neptunes on Polar Orbits 
Authors: Juan I. Espinoza-Retamal, Guđmundur Stefánsson, Cristobal Petrovich, Rafael Brahm, Andrés Jordán, Elyar Sedaghati, Jennifer P. Lucero, Marcelo Tala Pinto, Diego J. Muñoz, Gavin Boyle, Rodrigo Leiva, Vincent Suc
Figure caption: Mass vs. semimajor axis diagram for the possible outer companions to (a) HATS-38 b and (b) WASP-139 b. Different colors indicate regions where we can rule out the companion at different σ levels based on the RV residuals. Yellow dotted–dashed lines show η GR = 3 (Equation (4)), demarking the regions where the companion can excite the eccentricities secularly. Cyan dotted–dashed lines show η ⋆ = 1 (Equation (5)) for J 2 = 10−7 (corresponding to rotational periods of ∼20–30 days), demarking the regions where the companion can secularly excite obliquities. Blue dashed lines show τ ZLK = 1 Myr (Equation (3)), demarking the regions where the companion assisted by a dispersing protoplanetary disk can resonantly excite obliquities (adiabatic resonance capture). Black dashed lines show η GR = 1/2, demarking the regions where the companion can induce high-eccentricity migration if it started at a b,0 = 2 au. For any of the mechanisms discussed above to play a role, the companion needs to reside above the respective line; for companions below the line, the respective mechanism is excluded. From both figures, we see that the current RV observations are only compatible with the high-eccentricity migration scenario.
Paper: Improving Power Spectrum Estimation Using Multitapering: Efficient Asteroseismic Analyses for Understanding Stars, the Milky Way, and Beyond
Authors: Aarya A. Patil, Gwendolyn M. Eadie, Joshua S. Speagle, 佳士 沈, David J. Thomson
Figure caption: Comparison between the LS periodogram and the NUFFT periodogram of the Kepler-91 time series. This illustrates that the NUFFT periodogram we introduce in Section 2.1.2 behaves similar to the LS periodogram in the case of quasi-evenly sampled time series with gaps.
Paper: Improving Power Spectrum Estimation Using Multitapering: Efficient Asteroseismic Analyses for Understanding Stars, the Milky Way, and Beyond
Authors: Aarya A. Patil, Gwendolyn M. Eadie, Joshua S. Speagle, 佳士 沈, David J. Thomson
Figure caption: Photometric time series of Kepler red giant star-91. The inset shows a zoom-in plot of the time series from 708 to 722 days, highlighting that the time sampling is uneven and that long gaps are present.
Paper: Gemini High-resolution Optical Spectrograph (GHOST) at Gemini South: Instrument Performance and Integration, First Science, and Next Steps
Authors: V. M. Kalari, R. J. Diaz, G. Robertson, A. McConnachie, M. Ireland, R. Salinas, P. Young, C. Simpson, C. Hayes, J. Nielsen, G. Burley, J. Pazder, M. Gomez-Jimenez, E. Martioli, S. B. Howell, M. Jeong, S. Juneau, R. Ruiz-Carmona, S. Margheim, A. Sheinis, A. Anthony, G. Baker, T. A. M. Berg, T. Cao, E. Chapin, T. Chin, K. Chiboucas, V. Churilov, E. Deibert, A. Densmore, J. Dunn, M. L. Edgar, J. Heo, D. Henderson, T. Farrell, J. Font, V. Firpo, J. Fuentes, K. Labrie, S. Lambert, J. Lawrence, J. Lothrop, R. McDermid, B. W. Miller, G. Perez, V. M. Placco, P. Prado, C. Quiroz, F. Ramos, R. Rutten, K. M. G. Silva, J. Thomas-Osip, C. Urrutia, W. D. Vacca, K. Venn, F. Waller, L. Waller, M. White, S. Xu, R. Zhelem
Figure caption: GHOST high-resolution spectra of TW Hya, covering nearly the entire wavelength range of the instrument. Spectra are in absolute flux units, but not corrected for telluric lines. Strong emission lines are truncated for visual purposes. The colors are mapped based on a shifting multicolor scale from violet to red, aimed to be representative of the region of the spectrum plotted.
Paper: Gemini High-resolution Optical Spectrograph (GHOST) at Gemini South: Instrument Performance and Integration, First Science, and Next Steps
Authors: V. M. Kalari, R. J. Diaz, G. Robertson, A. McConnachie, M. Ireland, R. Salinas, P. Young, C. Simpson, C. Hayes, J. Nielsen, G. Burley, J. Pazder, M. Gomez-Jimenez, E. Martioli, S. B. Howell, M. Jeong, S. Juneau, R. Ruiz-Carmona, S. Margheim, A. Sheinis, A. Anthony, G. Baker, T. A. M. Berg, T. Cao, E. Chapin, T. Chin, K. Chiboucas, V. Churilov, E. Deibert, A. Densmore, J. Dunn, M. L. Edgar, J. Heo, D. Henderson, T. Farrell, J. Font, V. Firpo, J. Fuentes, K. Labrie, S. Lambert, J. Lawrence, J. Lothrop, R. McDermid, B. W. Miller, G. Perez, V. M. Placco, P. Prado, C. Quiroz, F. Ramos, R. Rutten, K. M. G. Silva, J. Thomas-Osip, C. Urrutia, W. D. Vacca, K. Venn, F. Waller, L. Waller, M. White, S. Xu, R. Zhelem
Figure caption: Standard-resolution spectra of the “Iron star” XX Oph. (a) The region around the Hα line, displaying the strength of the emission; (b) the finer detail around the line. (c) The Na I doublet lines. (d) The Hβ line and nearby metal ion emissions, which also display P Cygni absorptions.
Paper: Gemini High-resolution Optical Spectrograph (GHOST) at Gemini South: Instrument Performance and Integration, First Science, and Next Steps
Authors: V. M. Kalari, R. J. Diaz, G. Robertson, A. McConnachie, M. Ireland, R. Salinas, P. Young, C. Simpson, C. Hayes, J. Nielsen, G. Burley, J. Pazder, M. Gomez-Jimenez, E. Martioli, S. B. Howell, M. Jeong, S. Juneau, R. Ruiz-Carmona, S. Margheim, A. Sheinis, A. Anthony, G. Baker, T. A. M. Berg, T. Cao, E. Chapin, T. Chin, K. Chiboucas, V. Churilov, E. Deibert, A. Densmore, J. Dunn, M. L. Edgar, J. Heo, D. Henderson, T. Farrell, J. Font, V. Firpo, J. Fuentes, K. Labrie, S. Lambert, J. Lawrence, J. Lothrop, R. McDermid, B. W. Miller, G. Perez, V. M. Placco, P. Prado, C. Quiroz, F. Ramos, R. Rutten, K. M. G. Silva, J. Thomas-Osip, C. Urrutia, W. D. Vacca, K. Venn, F. Waller, L. Waller, M. White, S. Xu, R. Zhelem
Figure caption: Forbidden [O I] nebular emission at 5007 Å and Hβ emission line profiles seen toward the star SextansA s2 (V = 20.8 mag). The final SNR per resolution element around the continuum in blue (at Hβ) was 8, and in red (at Hα) was 11 after three consecutive 1 hr exposure. The SNR in the continuum varied with wavelength.
Paper: Gemini High-resolution Optical Spectrograph (GHOST) at Gemini South: Instrument Performance and Integration, First Science, and Next Steps
Authors: V. M. Kalari, R. J. Diaz, G. Robertson, A. McConnachie, M. Ireland, R. Salinas, P. Young, C. Simpson, C. Hayes, J. Nielsen, G. Burley, J. Pazder, M. Gomez-Jimenez, E. Martioli, S. B. Howell, M. Jeong, S. Juneau, R. Ruiz-Carmona, S. Margheim, A. Sheinis, A. Anthony, G. Baker, T. A. M. Berg, T. Cao, E. Chapin, T. Chin, K. Chiboucas, V. Churilov, E. Deibert, A. Densmore, J. Dunn, M. L. Edgar, J. Heo, D. Henderson, T. Farrell, J. Font, V. Firpo, J. Fuentes, K. Labrie, S. Lambert, J. Lawrence, J. Lothrop, R. McDermid, B. W. Miller, G. Perez, V. M. Placco, P. Prado, C. Quiroz, F. Ramos, R. Rutten, K. M. G. Silva, J. Thomas-Osip, C. Urrutia, W. D. Vacca, K. Venn, F. Waller, L. Waller, M. White, S. Xu, R. Zhelem
Figure caption: Cross-correlation function (CCF) of TYC8254-1616-1 derived from GHOST spectra in both the blue (left panels) and red (right panels) channels. The top panels show the mean CCFs represented by green lines, while the bottom panels display the CCF data with the mean CCF subtracted. The color code indicates the first epoch in dark blue and the last epoch in dark red.
Paper: Gemini High-resolution Optical Spectrograph (GHOST) at Gemini South: Instrument Performance and Integration, First Science, and Next Steps
Authors: V. M. Kalari, R. J. Diaz, G. Robertson, A. McConnachie, M. Ireland, R. Salinas, P. Young, C. Simpson, C. Hayes, J. Nielsen, G. Burley, J. Pazder, M. Gomez-Jimenez, E. Martioli, S. B. Howell, M. Jeong, S. Juneau, R. Ruiz-Carmona, S. Margheim, A. Sheinis, A. Anthony, G. Baker, T. A. M. Berg, T. Cao, E. Chapin, T. Chin, K. Chiboucas, V. Churilov, E. Deibert, A. Densmore, J. Dunn, M. L. Edgar, J. Heo, D. Henderson, T. Farrell, J. Font, V. Firpo, J. Fuentes, K. Labrie, S. Lambert, J. Lawrence, J. Lothrop, R. McDermid, B. W. Miller, G. Perez, V. M. Placco, P. Prado, C. Quiroz, F. Ramos, R. Rutten, K. M. G. Silva, J. Thomas-Osip, C. Urrutia, W. D. Vacca, K. Venn, F. Waller, L. Waller, M. White, S. Xu, R. Zhelem
Figure caption: Observed spectrum (black solid) and fit (red dashed) around the Li 6103 Å region for TW Hya. The best multicomponent (four) Gaussian fit is poorer at the redder Fe I line, but fits the remaining lines well, including the Li line.
Paper: Gemini High-resolution Optical Spectrograph (GHOST) at Gemini South: Instrument Performance and Integration, First Science, and Next Steps
Authors: V. M. Kalari, R. J. Diaz, G. Robertson, A. McConnachie, M. Ireland, R. Salinas, P. Young, C. Simpson, C. Hayes, J. Nielsen, G. Burley, J. Pazder, M. Gomez-Jimenez, E. Martioli, S. B. Howell, M. Jeong, S. Juneau, R. Ruiz-Carmona, S. Margheim, A. Sheinis, A. Anthony, G. Baker, T. A. M. Berg, T. Cao, E. Chapin, T. Chin, K. Chiboucas, V. Churilov, E. Deibert, A. Densmore, J. Dunn, M. L. Edgar, J. Heo, D. Henderson, T. Farrell, J. Font, V. Firpo, J. Fuentes, K. Labrie, S. Lambert, J. Lawrence, J. Lothrop, R. McDermid, B. W. Miller, G. Perez, V. M. Placco, P. Prado, C. Quiroz, F. Ramos, R. Rutten, K. M. G. Silva, J. Thomas-Osip, C. Urrutia, W. D. Vacca, K. Venn, F. Waller, L. Waller, M. White, S. Xu, R. Zhelem
Figure caption: Quantities derived from the CCFs of TYC8254-1616-1's GHOST spectra. These measurements were obtained from both the blue (top panels) and red (bottom panels) channels. For each channel, the panels display the time series of RVs, FWHMs, bisector span, airmass, and maximum SNR from top to bottom.
Paper: Gemini High-resolution Optical Spectrograph (GHOST) at Gemini South: Instrument Performance and Integration, First Science, and Next Steps
Authors: V. M. Kalari, R. J. Diaz, G. Robertson, A. McConnachie, M. Ireland, R. Salinas, P. Young, C. Simpson, C. Hayes, J. Nielsen, G. Burley, J. Pazder, M. Gomez-Jimenez, E. Martioli, S. B. Howell, M. Jeong, S. Juneau, R. Ruiz-Carmona, S. Margheim, A. Sheinis, A. Anthony, G. Baker, T. A. M. Berg, T. Cao, E. Chapin, T. Chin, K. Chiboucas, V. Churilov, E. Deibert, A. Densmore, J. Dunn, M. L. Edgar, J. Heo, D. Henderson, T. Farrell, J. Font, V. Firpo, J. Fuentes, K. Labrie, S. Lambert, J. Lawrence, J. Lothrop, R. McDermid, B. W. Miller, G. Perez, V. M. Placco, P. Prado, C. Quiroz, F. Ramos, R. Rutten, K. M. G. Silva, J. Thomas-Osip, C. Urrutia, W. D. Vacca, K. Venn, F. Waller, L. Waller, M. White, S. Xu, R. Zhelem
Figure caption: Reduced combined red echellogram observed toward SextansA s2. The orders shown are 53–51, covering Hα and the telluric lines in order 51. The width of the Hα emission is well defined, as well as the absence of the contamination in the sky, and secondary SRIFU fibers suggesting the emission originates from the object itself.
Paper: Gemini High-resolution Optical Spectrograph (GHOST) at Gemini South: Instrument Performance and Integration, First Science, and Next Steps
Authors: V. M. Kalari, R. J. Diaz, G. Robertson, A. McConnachie, M. Ireland, R. Salinas, P. Young, C. Simpson, C. Hayes, J. Nielsen, G. Burley, J. Pazder, M. Gomez-Jimenez, E. Martioli, S. B. Howell, M. Jeong, S. Juneau, R. Ruiz-Carmona, S. Margheim, A. Sheinis, A. Anthony, G. Baker, T. A. M. Berg, T. Cao, E. Chapin, T. Chin, K. Chiboucas, V. Churilov, E. Deibert, A. Densmore, J. Dunn, M. L. Edgar, J. Heo, D. Henderson, T. Farrell, J. Font, V. Firpo, J. Fuentes, K. Labrie, S. Lambert, J. Lawrence, J. Lothrop, R. McDermid, B. W. Miller, G. Perez, V. M. Placco, P. Prado, C. Quiroz, F. Ramos, R. Rutten, K. M. G. Silva, J. Thomas-Osip, C. Urrutia, W. D. Vacca, K. Venn, F. Waller, L. Waller, M. White, S. Xu, R. Zhelem
Figure caption: Lyα forest of J1215−0034, with the coarser-resolution spectra from SDSS and DESI overplotted. The displayed spectra are in the observer’s frame of reference.
Paper: Gemini High-resolution Optical Spectrograph (GHOST) at Gemini South: Instrument Performance and Integration, First Science, and Next Steps
Authors: V. M. Kalari, R. J. Diaz, G. Robertson, A. McConnachie, M. Ireland, R. Salinas, P. Young, C. Simpson, C. Hayes, J. Nielsen, G. Burley, J. Pazder, M. Gomez-Jimenez, E. Martioli, S. B. Howell, M. Jeong, S. Juneau, R. Ruiz-Carmona, S. Margheim, A. Sheinis, A. Anthony, G. Baker, T. A. M. Berg, T. Cao, E. Chapin, T. Chin, K. Chiboucas, V. Churilov, E. Deibert, A. Densmore, J. Dunn, M. L. Edgar, J. Heo, D. Henderson, T. Farrell, J. Font, V. Firpo, J. Fuentes, K. Labrie, S. Lambert, J. Lawrence, J. Lothrop, R. McDermid, B. W. Miller, G. Perez, V. M. Placco, P. Prado, C. Quiroz, F. Ramos, R. Rutten, K. M. G. Silva, J. Thomas-Osip, C. Urrutia, W. D. Vacca, K. Venn, F. Waller, L. Waller, M. White, S. Xu, R. Zhelem
Figure caption: Flux-calibrated blue spectrum of QSO J1215-0034 taken using GHOST plotted over a selected wavelength range, including the Lyα line at 450.4 nm.
Paper: Gemini High-resolution Optical Spectrograph (GHOST) at Gemini South: Instrument Performance and Integration, First Science, and Next Steps
Authors: V. M. Kalari, R. J. Diaz, G. Robertson, A. McConnachie, M. Ireland, R. Salinas, P. Young, C. Simpson, C. Hayes, J. Nielsen, G. Burley, J. Pazder, M. Gomez-Jimenez, E. Martioli, S. B. Howell, M. Jeong, S. Juneau, R. Ruiz-Carmona, S. Margheim, A. Sheinis, A. Anthony, G. Baker, T. A. M. Berg, T. Cao, E. Chapin, T. Chin, K. Chiboucas, V. Churilov, E. Deibert, A. Densmore, J. Dunn, M. L. Edgar, J. Heo, D. Henderson, T. Farrell, J. Font, V. Firpo, J. Fuentes, K. Labrie, S. Lambert, J. Lawrence, J. Lothrop, R. McDermid, B. W. Miller, G. Perez, V. M. Placco, P. Prado, C. Quiroz, F. Ramos, R. Rutten, K. M. G. Silva, J. Thomas-Osip, C. Urrutia, W. D. Vacca, K. Venn, F. Waller, L. Waller, M. White, S. Xu, R. Zhelem
Figure caption: Doubling of Hα and Hϵ Balmer lines is clearly visible in the GHOST spectra of IK Hya, with the detail of other Balmer lines also shown. The entire spectrum was captured simultaneously. The spectral resolution and signal achieved in these weather conditions demonstrate the usefulness of GHOST at Gemini as a monitoring instrument for relatively bright targets.
Paper: Gemini High-resolution Optical Spectrograph (GHOST) at Gemini South: Instrument Performance and Integration, First Science, and Next Steps
Authors: V. M. Kalari, R. J. Diaz, G. Robertson, A. McConnachie, M. Ireland, R. Salinas, P. Young, C. Simpson, C. Hayes, J. Nielsen, G. Burley, J. Pazder, M. Gomez-Jimenez, E. Martioli, S. B. Howell, M. Jeong, S. Juneau, R. Ruiz-Carmona, S. Margheim, A. Sheinis, A. Anthony, G. Baker, T. A. M. Berg, T. Cao, E. Chapin, T. Chin, K. Chiboucas, V. Churilov, E. Deibert, A. Densmore, J. Dunn, M. L. Edgar, J. Heo, D. Henderson, T. Farrell, J. Font, V. Firpo, J. Fuentes, K. Labrie, S. Lambert, J. Lawrence, J. Lothrop, R. McDermid, B. W. Miller, G. Perez, V. M. Placco, P. Prado, C. Quiroz, F. Ramos, R. Rutten, K. M. G. Silva, J. Thomas-Osip, C. Urrutia, W. D. Vacca, K. Venn, F. Waller, L. Waller, M. White, S. Xu, R. Zhelem
Figure caption: Computer-generated image displaying the location of possible future optics (blue envelope). The space is restricted by the IFU and ADC assembly, but has been measured to be sufficient for wave plates to capture circular polarization.
Paper: Empirical Stability Criteria for 3D Hierarchical Triple Systems. I. Circumbinary Planets
Authors: Nikolaos Georgakarakos, Siegfried Eggl, Mohamad Ali-Dib, Ian Dobbs-Dixon
Figure caption: Relative percentage error distribution from comparing our empirical fits against the results of numerical simulations. On the x-axis we have bins of relative percentage error between the results from the numerical simulations and the fits of Equations (10), while on the y-axis we have the percentage of systems that fall into a specific error bin. The top row is for the e  P  ≤ 0.8 case, while the bottom row plots represent the more eccentric case.
Paper: Empirical Stability Criteria for 3D Hierarchical Triple Systems. I. Circumbinary Planets
Authors: Nikolaos Georgakarakos, Siegfried Eggl, Mohamad Ali-Dib, Ian Dobbs-Dixon
Figure caption: Comparison between different stability fits. Geo stands for the fits of the present work, Adel denotes the work by S. Adelbert et al. (2023), HW denotes the classification formula given in M. J. Holman & P. A. Wiegert (1999), and MA stands for the criterion developed by R. Mardling & S. Aarseth (1999) and R. A. Mardling & S. J. Aarseth (2001). As previously, the black color denotes the outer critical border, while the orange color represents the inner critical border. The circles are the results from our numerical simulations.
Paper: Empirical Stability Criteria for 3D Hierarchical Triple Systems. I. Circumbinary Planets
Authors: Nikolaos Georgakarakos, Siegfried Eggl, Mohamad Ali-Dib, Ian Dobbs-Dixon
Figure caption: Distribution of relative percentage error from comparing the machine learning model against the results from the numerical simulations. On the x-axis we have bins of relative percentage error between the ML model and the results from the numerical simulations, while on the y-axis we have the percentage of systems that fall into a specific error bin. The top row corresponds to systems with e  p  ≤ 0.8, while the plots in the bottom row represent the complete data set.
Paper: Empirical Stability Criteria for 3D Hierarchical Triple Systems. I. Circumbinary Planets
Authors: Nikolaos Georgakarakos, Siegfried Eggl, Mohamad Ali-Dib, Ian Dobbs-Dixon
Figure caption: Critical semimajor axis against mutual inclination for a system with M  b  = 0.05, M  p  = 10−3, e  b  = 0.8, and e  p  = 0. The triangles represent the inner critical border while the circles indicate the outer one.
Paper: Empirical Stability Criteria for 3D Hierarchical Triple Systems. I. Circumbinary Planets
Authors: Nikolaos Georgakarakos, Siegfried Eggl, Mohamad Ali-Dib, Ian Dobbs-Dixon
Figure caption: Critical semimajor axis against mutual inclination for a variety of systems. The orange color refers to the inner boundary, while the black color denotes the outer stability border. The continuous lines are our empirical fits as given in Section 3.2. The points are the output from the numerical simulations for the specific systems. Note that the majority of the points lie between the two curves, as they ideally should.
Paper: Empirical Stability Criteria for 3D Hierarchical Triple Systems. I. Circumbinary Planets
Authors: Nikolaos Georgakarakos, Siegfried Eggl, Mohamad Ali-Dib, Ian Dobbs-Dixon
Figure caption: Critical semimajor axis against mutual inclination for various values of eccentricity and binary mass ratio. The circles denote the outer limit (largest value recorded among the different combinations of the planetary pericenter and node), while the triangles represent the inner limit (smallest value recorded). The colors correspond to different values of planetary eccentricity. Finally, M  p  = 10−3.
Paper: Empirical Stability Criteria for 3D Hierarchical Triple Systems. I. Circumbinary Planets
Authors: Nikolaos Georgakarakos, Siegfried Eggl, Mohamad Ali-Dib, Ian Dobbs-Dixon
Figure caption: Correlation matrix for the simulation data set. The color indicates Pearson’s correlation coefficient. The logarithms of the masses are base 10 and i denotes the mutual inclination. See text for more details.