adsabs/AstroCLIMB huggingface dataset:
Paper: The NEID Earth Twin Survey. II. Dynamical Masses in Seven High-acceleration Star Systems
Authors: Mark R. Giovinazzi, Cullen H. Blake, Paul Robertson, Andrea S. J. Lin, Arvind F. Gupta, Suvrath Mahadevan, Jason T. Wright, Daniella Bardalez Gagliuffi, Jiayin Dong, Rachel B. Fernandes, Evan Fitzmaurice, Samuel Halverson, Shubham Kanodia, Sarah E. Logsdon, Jacob K. Luhn, Michael W. McElwain, Andy Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Gudmundur Stefánsson, Ryan Terrien, Jason D. Eastman, Jonathan Horner, Peter Plavchan, Sharon X. Wang, Maurice L. Wilson, Robert A. Wittenmyer
Figure caption: Observed proper-motion values for the accelerating stars in our four binary systems: HD 68017 A, 61 Cygni B, HD 24496 A, and HD 4614 A. In each panel, the left plot shows the proper motion in R.A. as measured by Hipparcos (left point at t ≈ 1991.25) and Gaia (right point at t ≈ 2016.0), and the right plot shows the proper motion in decl. for the same epochs. The best-fit models and colored trial orbits that correspond to companion mass are in broad agreement with the astrometric measurements for all systems. Though in the case of HD 68017, the offsets observed primarily in Hipparcos’ proper motion in R.A. and Gaia’s proper motion in decl. are likely due to the mission’s inability to resolve the stellar pair.
Paper: The NEID Earth Twin Survey. II. Dynamical Masses in Seven High-acceleration Star Systems
Authors: Mark R. Giovinazzi, Cullen H. Blake, Paul Robertson, Andrea S. J. Lin, Arvind F. Gupta, Suvrath Mahadevan, Jason T. Wright, Daniella Bardalez Gagliuffi, Jiayin Dong, Rachel B. Fernandes, Evan Fitzmaurice, Samuel Halverson, Shubham Kanodia, Sarah E. Logsdon, Jacob K. Luhn, Michael W. McElwain, Andy Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Gudmundur Stefánsson, Ryan Terrien, Jason D. Eastman, Jonathan Horner, Peter Plavchan, Sharon X. Wang, Maurice L. Wilson, Robert A. Wittenmyer
Figure caption: The full sample of NETS stars, ranked by their astrometric acceleration parameter, ﹩{\chi }_{{\rm{HG}}}^{2}﹩. Stars plotted with red bars are known to have at least one planetary or stellar companion, while those plotted with blue bars are not known to have any bound companions. The horizontal dashed line indicates our cut for keeping only stars with ﹩{\chi }_{{\rm{HG}}}^{2}\gt 11.8﹩. The only NETS target not shown here is HD 179957, which is not cataloged by Hipparcos and therefore has no reported ﹩{\chi }_{{\rm{HG}}}^{2}﹩ value. We note that its bound stellar companion, HD 179958, is cataloged by Hipparcos and does have a >3σ astrometric acceleration. Since we do not have NEID RVs on the accelerating star, this system is not included in our analysis. 61 Cygni B, on the other hand, is an NEID target not in NETS; however, it is bound to 61 Cygni A, and so we include it in our analyses and highlight it here with a hatch.
Paper: The NEID Earth Twin Survey. II. Dynamical Masses in Seven High-acceleration Star Systems
Authors: Mark R. Giovinazzi, Cullen H. Blake, Paul Robertson, Andrea S. J. Lin, Arvind F. Gupta, Suvrath Mahadevan, Jason T. Wright, Daniella Bardalez Gagliuffi, Jiayin Dong, Rachel B. Fernandes, Evan Fitzmaurice, Samuel Halverson, Shubham Kanodia, Sarah E. Logsdon, Jacob K. Luhn, Michael W. McElwain, Andy Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Gudmundur Stefánsson, Ryan Terrien, Jason D. Eastman, Jonathan Horner, Peter Plavchan, Sharon X. Wang, Maurice L. Wilson, Robert A. Wittenmyer
Figure caption: Scatter of all sources in Gaia with apparent magnitude G < 7. Here, we show that sources with G ≲ 4 are far less frequently observed to have RUWE < 1.4, a strong indicator that the RUWE values of these bright sources may be artificially inflated.
Paper: The NEID Earth Twin Survey. II. Dynamical Masses in Seven High-acceleration Star Systems
Authors: Mark R. Giovinazzi, Cullen H. Blake, Paul Robertson, Andrea S. J. Lin, Arvind F. Gupta, Suvrath Mahadevan, Jason T. Wright, Daniella Bardalez Gagliuffi, Jiayin Dong, Rachel B. Fernandes, Evan Fitzmaurice, Samuel Halverson, Shubham Kanodia, Sarah E. Logsdon, Jacob K. Luhn, Michael W. McElwain, Andy Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Gudmundur Stefánsson, Ryan Terrien, Jason D. Eastman, Jonathan Horner, Peter Plavchan, Sharon X. Wang, Maurice L. Wilson, Robert A. Wittenmyer
Figure caption: Best-fit RV models for the four binary star systems presented in this analysis. The RVs shown here are those collected for the accelerating star in each system (top left: HD 68017 A; top right: 61 Cygni B; bottom left: HD 24496 A; bottom right: HD 4614 A). The error bars in each panel include instrumental RV jitter terms that have been independently fit for, and the colors of the data points corresponding to those provided in Figure 2. In each case, the best-fit model is then subtracted off, and the subsequent residuals are consistent with random scatter about zero.
Paper: The NEID Earth Twin Survey. II. Dynamical Masses in Seven High-acceleration Star Systems
Authors: Mark R. Giovinazzi, Cullen H. Blake, Paul Robertson, Andrea S. J. Lin, Arvind F. Gupta, Suvrath Mahadevan, Jason T. Wright, Daniella Bardalez Gagliuffi, Jiayin Dong, Rachel B. Fernandes, Evan Fitzmaurice, Samuel Halverson, Shubham Kanodia, Sarah E. Logsdon, Jacob K. Luhn, Michael W. McElwain, Andy Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Gudmundur Stefánsson, Ryan Terrien, Jason D. Eastman, Jonathan Horner, Peter Plavchan, Sharon X. Wang, Maurice L. Wilson, Robert A. Wittenmyer
Figure caption: Bar chart of all RVs used for the seven accelerating stars considered in our analysis. Temporal overlap of RV data sets from different instruments helps to constrain instrumental offsets and improves the accuracy of orbital fits by providing a more continuous coverage across the total observation baseline.
Paper: The NEID Earth Twin Survey. II. Dynamical Masses in Seven High-acceleration Star Systems
Authors: Mark R. Giovinazzi, Cullen H. Blake, Paul Robertson, Andrea S. J. Lin, Arvind F. Gupta, Suvrath Mahadevan, Jason T. Wright, Daniella Bardalez Gagliuffi, Jiayin Dong, Rachel B. Fernandes, Evan Fitzmaurice, Samuel Halverson, Shubham Kanodia, Sarah E. Logsdon, Jacob K. Luhn, Michael W. McElwain, Andy Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Gudmundur Stefánsson, Ryan Terrien, Jason D. Eastman, Jonathan Horner, Peter Plavchan, Sharon X. Wang, Maurice L. Wilson, Robert A. Wittenmyer
Figure caption: Grid of the seven systems included in our analyses. Each system is centered relative to the position of the primary star at t = 2016.0 and is viewed with an equal aspect ratio. Primary stars are denoted by yellow stars, bound stellar companions by yellow circles, and their relative proper motions by arrows. The three planetary systems are shown in the bottom row, with the planets marked by red circles. For simplicity, their orbits are sketched as circles, with radii corresponding to their semimajor axes , and placed at arbitrary position angles. Systems with two planets feature zoomed-in inset axes to highlight the inner planet. Since HD 68017 AB is not resolved by Gaia, we do not include its relative proper-motion information.
Paper: Five New Sirius-like White Dwarf–Main-sequence Star Systems with MagAO-X
Authors: Logan A. Pearce, Jared R. Males, Sebastiaan Y. Haffert, Laird M. Close, Joseph D. Long, Eden A. McEwen, Joshua Liberman, Maggie Y. Kautz, Jay K. Kueny, Alycia J. Weinberger, Jialin Li, Elena Tonucci, Katie Twitchell, Avalon L. McLeod, Warren B. Foster, Olivier Guyon, Alexander D. Hedglen, Kyle Van Gorkom, Jennifer Lumbres, Lauren Schatz, Victor Gasho, Katie M. Morzinski, Phil M. Hinz
Figure caption: Left: CMD of the confirmed and candidate companions from Table 2 shown in SDSS ﹩r^{\prime} -z^{\prime} ﹩ color and SDSS ﹩i^{\prime} ﹩ absolute magnitude. Colored stars give the model photometry of the host star, and colored circles show the measured photometry of the corresponding companion in MagAO-X filters converted to SDSS filters using color conversion table (https://magao-x.org/docs/handbook/observers/filters.html). Gray dots are the same Gaia sample from Figure 1 converted to SDSS colors using GaiaXPy (D. Ruz-Mieres & zuzannakr 2023) to generate synthetic photometry from Gaia DR3 spectra. Right: same as the left but for the ﹩i^{\prime} -z^{\prime} ﹩ color and SDSS ﹩i^{\prime} ﹩ absolute magnitude for the candidate companion signal to HD 104018, since we do not have ﹩r^{\prime} ﹩ photometry for that target. The candidate companion clearly falls in the WD regime, however the exact position in the WD sequence is not well constrained with only ﹩i^{\prime} ﹩ and ﹩z^{\prime} ﹩ filters.
Paper: Five New Sirius-like White Dwarf–Main-sequence Star Systems with MagAO-X
Authors: Logan A. Pearce, Jared R. Males, Sebastiaan Y. Haffert, Laird M. Close, Joseph D. Long, Eden A. McEwen, Joshua Liberman, Maggie Y. Kautz, Jay K. Kueny, Alycia J. Weinberger, Jialin Li, Elena Tonucci, Katie Twitchell, Avalon L. McLeod, Warren B. Foster, Olivier Guyon, Alexander D. Hedglen, Kyle Van Gorkom, Jennifer Lumbres, Lauren Schatz, Victor Gasho, Katie M. Morzinski, Phil M. Hinz
Figure caption: Top: targets in R.A. and decl. Targets accessible to MagAO-X from Las Campanas Observatory are plotted in blue. Targets outlined by the purple stars were observed in the second observing semester (B) of 2022, the yellow stars in the first semester (A) of 2024, and the magenta stars in the second semester 2024. Bottom: Pup Search target CMD in Gaia absolute G magnitude vs. Gaia BP – RP color. The red points mark the 84 wide candidate WD–MS systems identified in Section. 2.1. The gray points are the 10,000 nearest high-quality solutions (RUWE < 1.1) in Gaia Data Release 3 (DR3), with approximate spectral type ranges marked in blue (adapted from the spectral type-color relations in M. J. Pecaut & E. E. Mamajek 2013; http://www.pas.rochester.edu/ emamajek/EEM_dwarf_UBVIJHK_colors_Teff.txt). All of our target MS stars fall within the AFGK region, and ≈60% are in the giant star region.
Paper: Five New Sirius-like White Dwarf–Main-sequence Star Systems with MagAO-X
Authors: Logan A. Pearce, Jared R. Males, Sebastiaan Y. Haffert, Laird M. Close, Joseph D. Long, Eden A. McEwen, Joshua Liberman, Maggie Y. Kautz, Jay K. Kueny, Alycia J. Weinberger, Jialin Li, Elena Tonucci, Katie Twitchell, Avalon L. McLeod, Warren B. Foster, Olivier Guyon, Alexander D. Hedglen, Kyle Van Gorkom, Jennifer Lumbres, Lauren Schatz, Victor Gasho, Katie M. Morzinski, Phil M. Hinz
Figure caption: Map of χ2 as a function of Teff and ﹩\mathrm{log}g﹩ for hydrogen-dominated WD atmosphere models fit to our photometry for the five candidate WD companions. The effective temperature is on the x-axis and ﹩\mathrm{log}g﹩ on the y-axis with χ2 value interpolated between grid points. The best-fitting model is marked with an orange star; the solid contour shows the 2σ surfaces from that minimum χ2 value. (a) TYC 4831-473-1 B, (b) BD+20 2007 CC1, (c) BD-00 2082 CC1, (d) TYC 1451-111-1 CC1, and (e) HD 104018 CC1.
Paper: Five New Sirius-like White Dwarf–Main-sequence Star Systems with MagAO-X
Authors: Logan A. Pearce, Jared R. Males, Sebastiaan Y. Haffert, Laird M. Close, Joseph D. Long, Eden A. McEwen, Joshua Liberman, Maggie Y. Kautz, Jay K. Kueny, Alycia J. Weinberger, Jialin Li, Elena Tonucci, Katie Twitchell, Avalon L. McLeod, Warren B. Foster, Olivier Guyon, Alexander D. Hedglen, Kyle Van Gorkom, Jennifer Lumbres, Lauren Schatz, Victor Gasho, Katie M. Morzinski, Phil M. Hinz
Figure caption: MagAO-X images of the confirmed and candidate companion signals in this work. All images are north up, east left; the filter, host star, and observation date are as indicated. Scale bars show angular and physical scales. The companion is marked by a white cross and label. TYC 4831-473-1 B displays two images (in the top red rectangle), ﹩i^{\prime} ﹩ from 2022 and ﹩z^{\prime} ﹩ from 2024, to show common proper motion. We show two images for HD 104018 (in the bottom red rectangle) in ﹩z^{\prime} ﹩ and ﹩i^{\prime} ﹩ filters to illustrate that candidate signal does not move between filters as it would if it were a speckle. For the faint candidate signals near TYC 4831-473-1 (2024), BD+20 2007, BD-00 2028, and TYC 1451-111-1, we show the image in two stretches to highlight the faint companion with an inset showing the star at a different stretch.
Paper: Five New Sirius-like White Dwarf–Main-sequence Star Systems with MagAO-X
Authors: Logan A. Pearce, Jared R. Males, Sebastiaan Y. Haffert, Laird M. Close, Joseph D. Long, Eden A. McEwen, Joshua Liberman, Maggie Y. Kautz, Jay K. Kueny, Alycia J. Weinberger, Jialin Li, Elena Tonucci, Katie Twitchell, Avalon L. McLeod, Warren B. Foster, Olivier Guyon, Alexander D. Hedglen, Kyle Van Gorkom, Jennifer Lumbres, Lauren Schatz, Victor Gasho, Katie M. Morzinski, Phil M. Hinz
Figure caption: Map of χ2 as a function of Teff, log([M/H]), and ﹩\mathrm{log}g﹩ of Phoenix MS star models to our photometry for HD 92588 CC1 (top) and HD 108738 CC1. The effective temperature is on the x-axis and log([M/H]) (left) and ﹩\mathrm{log}g﹩ (right) on the y-axis with χ2 value interpolated between grid points. The best-fitting model is marked with an orange star; the error bars show the 1σ values from that minimum χ2 model. Our photometry is unable to constrain log([M/H]) or ﹩\mathrm{log}g﹩ for either signal.
Paper: Two Ultralow-mass-ratio Binary Systems at Critical Evolutionary Stages
Authors: Di-Fu Guo, Kai Li, Fen Liu, Li-heng Wang, Huai-Zhen Li, Xu Chen, Xiang Gao
Figure caption: Modeled light curves of J053525 (left) and J175200 (right) produced by PHOEBE are shown. The solid lines represent the best-fit models based on MCMC parameter estimation. The residuals between observations and model predictions are displayed in the upper residual panels, while the enlarged residuals for TESS data are shown in the lower panels, using a magnified vertical scale to highlight small but systematic deviations.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Two Ultralow-mass-ratio Binary Systems at Critical Evolutionary Stages
Authors: Di-Fu Guo, Kai Li, Fen Liu, Li-heng Wang, Huai-Zhen Li, Xu Chen, Xiang Gao
Figure caption: Posterior probability distributions of key parameters (q, T2, i, f, L2/L1, and L3/LT) for J053525 obtained from MCMC analysis of its light curves.
Paper: Two Ultralow-mass-ratio Binary Systems at Critical Evolutionary Stages
Authors: Di-Fu Guo, Kai Li, Fen Liu, Li-heng Wang, Huai-Zhen Li, Xu Chen, Xiang Gao
Figure caption: Posterior probability distributions of key parameters (q, T2, i, f, L2/L1, and L3/LT) for J175200 derived from MCMC analysis of its light curves.
Paper: Detailed Analysis of Six Contact Binaries and their Possible Origin
Authors: Somayeh Soomandar, Lorne Nelson, Joshua Aiken
Figure caption: All primary (black circles) and secondary (red circles) minima along with the linear fit to the primary minima (red line). Note that the dashed–dotted line for NT Boo is simply an extrapolation of the linear fit.
Paper: Detailed Analysis of Six Contact Binaries and their Possible Origin
Authors: Somayeh Soomandar, Lorne Nelson, Joshua Aiken
Figure caption: Mass ratio of each system as obtained from the q-search.
Paper: Detailed Analysis of Six Contact Binaries and their Possible Origin
Authors: Somayeh Soomandar, Lorne Nelson, Joshua Aiken
Figure caption: Left panel: target pixel file of NZ Leo (top panel), OP Leo (middle panel), and MY Leo (bottom panel). The pixels included in the computation of SAP are denoted by black borders with diagonal lines. Right panel: phased light curves for NZ Leo, OP Leo, and MY Leo, respectively.
Paper: Detailed Analysis of Six Contact Binaries and their Possible Origin
Authors: Somayeh Soomandar, Lorne Nelson, Joshua Aiken
Figure caption: Observational light curve (black circles), synthetic light curve (red line), and residuals (blue circles).
Paper: Detailed Analysis of Six Contact Binaries and their Possible Origin
Authors: Somayeh Soomandar, Lorne Nelson, Joshua Aiken
Figure caption: 3D representation of the systems derived from the light-curve solutions.
Paper: A 16 Myr Super-Neptune in Upper Centaurus Lupus and a Preliminary Survey of Transiting Planets in Sco-Cen with TESS
Authors: Sydney Vach, George Zhou, Andrew W. Mann, Madyson G. Barber, Tyler R. Fairnington, Chelsea X. Huang, James G. Rogers, Luke G. Bouma, Joachim Krüger, Duncan Wright, Annabelle E. Niblett, Jack M. Nelson, Samuel N. Quinn, David W. Latham, Allyson Bieryla, Karen A. Collins, Michelle Kunimoto, Cristilyn N. Watkins, Richard P. Schwarz, Kevin I. Collins, Ramotholo Sefako, Keith Horne, Steve B. Howell, Catherine A. Clark, Colin Littlefield, Jessie L. Christiansen, Zahra Essack, Joshua N. Winn
Figure caption: Vetting plot for the Sector 65 observations of TIC 89071455. The TESS light curve is presented in the left panel, with the transit times marked by the red triangles. The stellar variability is modeled via a spline (blue). The phase-folded light curve using the best-fit period and transit time is shown in the middle panel. Our per-pixel analysis (right panel) shows the transits are consistent with being on target.
Paper: A 16 Myr Super-Neptune in Upper Centaurus Lupus and a Preliminary Survey of Transiting Planets in Sco-Cen with TESS
Authors: Sydney Vach, George Zhou, Andrew W. Mann, Madyson G. Barber, Tyler R. Fairnington, Chelsea X. Huang, James G. Rogers, Luke G. Bouma, Joachim Krüger, Duncan Wright, Annabelle E. Niblett, Jack M. Nelson, Samuel N. Quinn, David W. Latham, Allyson Bieryla, Karen A. Collins, Michelle Kunimoto, Cristilyn N. Watkins, Richard P. Schwarz, Kevin I. Collins, Ramotholo Sefako, Keith Horne, Steve B. Howell, Catherine A. Clark, Colin Littlefield, Jessie L. Christiansen, Zahra Essack, Joshua N. Winn
Figure caption: Lithium (left) and Hα (right) equivalent widths of TIC 88785435 (red), ϕ Lup candidate members (salmon), and literature established Sco-Cen members (gray). We plot the EAGLES (R. D. Jeffries et al. 2023) lithium distribution curve calculated for the age of UCL (16 Myr). Positive values denote the feature was observed in absorption, and negative values indicate emission. TIC 88785435 exhibited strong Hα emission and Li absorption supporting membership to Sco-Cen.
Paper: A 16 Myr Super-Neptune in Upper Centaurus Lupus and a Preliminary Survey of Transiting Planets in Sco-Cen with TESS
Authors: Sydney Vach, George Zhou, Andrew W. Mann, Madyson G. Barber, Tyler R. Fairnington, Chelsea X. Huang, James G. Rogers, Luke G. Bouma, Joachim Krüger, Duncan Wright, Annabelle E. Niblett, Jack M. Nelson, Samuel N. Quinn, David W. Latham, Allyson Bieryla, Karen A. Collins, Michelle Kunimoto, Cristilyn N. Watkins, Richard P. Schwarz, Kevin I. Collins, Ramotholo Sefako, Keith Horne, Steve B. Howell, Catherine A. Clark, Colin Littlefield, Jessie L. Christiansen, Zahra Essack, Joshua N. Winn
Figure caption: Upper panel: Lomb–Scargle periodogram for TIC 88785435. The Lomb–Scargle for each individual sector is plotted in gray, with the averaged power spectra across all three sectors plotted in red. We measured a rotation period of 8.49 days for TIC 88785435. Lower panel: Phase-folded TESS light curve for TIC 88785435 at our measured rotation period.
Paper: A 16 Myr Super-Neptune in Upper Centaurus Lupus and a Preliminary Survey of Transiting Planets in Sco-Cen with TESS
Authors: Sydney Vach, George Zhou, Andrew W. Mann, Madyson G. Barber, Tyler R. Fairnington, Chelsea X. Huang, James G. Rogers, Luke G. Bouma, Joachim Krüger, Duncan Wright, Annabelle E. Niblett, Jack M. Nelson, Samuel N. Quinn, David W. Latham, Allyson Bieryla, Karen A. Collins, Michelle Kunimoto, Cristilyn N. Watkins, Richard P. Schwarz, Kevin I. Collins, Ramotholo Sefako, Keith Horne, Steve B. Howell, Catherine A. Clark, Colin Littlefield, Jessie L. Christiansen, Zahra Essack, Joshua N. Winn
Figure caption: Left panel: TESS Sector 65 QLP (purple), SPOC FFI PDCSAP (salmon), and SPOC FFI SAP (green) light curves of TIC 88785435. Right panel: phase-folded TESS QLP (purple), SPOC FFI PDCSAP (salmon), and SPOC FFI SAP (green) light curves of TIC 88785435b.
Paper: A 16 Myr Super-Neptune in Upper Centaurus Lupus and a Preliminary Survey of Transiting Planets in Sco-Cen with TESS
Authors: Sydney Vach, George Zhou, Andrew W. Mann, Madyson G. Barber, Tyler R. Fairnington, Chelsea X. Huang, James G. Rogers, Luke G. Bouma, Joachim Krüger, Duncan Wright, Annabelle E. Niblett, Jack M. Nelson, Samuel N. Quinn, David W. Latham, Allyson Bieryla, Karen A. Collins, Michelle Kunimoto, Cristilyn N. Watkins, Richard P. Schwarz, Kevin I. Collins, Ramotholo Sefako, Keith Horne, Steve B. Howell, Catherine A. Clark, Colin Littlefield, Jessie L. Christiansen, Zahra Essack, Joshua N. Winn
Figure caption: Vetting plot for the Sector 37 observations of TIC 273586149 (same as Figure 8).
Paper: Meteoroid Stream Identification with HDBSCAN Unsupervised Clustering Algorithm
Authors: Eloy Peña-Asensio, Fabio Ferrari
Figure caption: The columns display the principal component analysis results for the ORBIT (left) and GEO (right) vectors. The top 10 largest clusters from CAMS and each HDBSCAN result are combined (13 in total) and displayed using labels from different clustering processes across four rows for different clustering processes: CAMS original labels with a minimum cluster size of 100 (top), maximum NMI (second), maximum Silhouette score at a minimum cluster size of 100 (third), and overall maximum Silhouette score (bottom). Sporadic events in CAMS and those labeled as noise by HDBSCAN are shown as smaller black points. Meteor showers are named based on official IAU identification numbers and codes. The HDBSCAN results depicted were obtained using the eom cluster selection method. GEO is represented here with Z-score normalization as well.
Paper: Meteoroid Stream Identification with HDBSCAN Unsupervised Clustering Algorithm
Authors: Eloy Peña-Asensio, Fabio Ferrari
Figure caption: Geocentric radiant distributions in a Mollweide projection, where R.A. is mapped along the horizontal axis and decl. along the vertical axis, and the ecliptic plane is represented by a solid yellow line. The top 10 largest clusters from CAMS and each HDBSCAN result are combined (13 in total) and displayed using labels from different clustering processes across three rows: CAMS original labels with a minimum cluster size of 100 (top), maximum NMI (center), and maximum Silhouette score at a minimum cluster size of 100 (bottom). Meteor showers are named based on official IAU identification numbers and codes. The HDBSCAN results depicted were obtained using the eom cluster selection method.
Paper: Meteoroid Stream Identification with HDBSCAN Unsupervised Clustering Algorithm
Authors: Eloy Peña-Asensio, Fabio Ferrari
Figure caption: One-vs.-rest confusion matrices constructed by comparing the meteor shower labels provided by CAMS with HDBSCAN clustering results under three conditions: maximum NMI, maximum Silhouette score at a minimum cluster size of 100, and overall maximum Silhouette score. The confusion matrix is presented for the top 10 most active meteor showers, with average performance metrics reported for these showers. Additionally, a separate confusion matrix for the sporadic background is computed using HDBSCAN’s noise labels. Meteor showers are named based on official IAU identification numbers and codes.
Paper: Meteoroid Stream Identification with HDBSCAN Unsupervised Clustering Algorithm
Authors: Eloy Peña-Asensio, Fabio Ferrari
Figure caption: The x-axis represents the number of clusters, while the y-axis indicates the size of each cluster. Clusters are sorted by size in descending order, with larger clusters appearing on the left side of the x-axis. The black line represents the CAMS classification, while the cyan line corresponds to the HDBSCAN results with the maximum NMI. The red line shows the HDBSCAN results for the maximum Silhouette score at a minimum cluster size of 100, and the yellow line represents the HDBSCAN results for the overall maximum Silhouette score.