adsabs/AstroCLIMB huggingface dataset:
Paper: Orbital and Atmospheric Characterization of the 1RXS J034231.8+121622 System using High-resolution Spectroscopy Confirms that the Companion is a Low-mass Star
Authors: Clarissa R. Do Ó, Ben Sappey, Quinn M. Konopacky, Jean-Baptiste Ruffio, Kelly K. O'Neil, Tuan Do, Gregory Martinez, Travis S. Barman, Jayke S. Nguyen, Jerry W. Xuan, Christopher A. Theissen, Sarah Blunt, William Thompson, Chih-Chun Hsu, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Julie Inglis, Nemanja Jovanovic, Ronald A. López, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Jason J. Wang, Ji Wang, Joshua Liberman
Figure caption: New orbit fit of 1RXS0342+1216 with the new 2023A astrometry epoch, the 2020 RV data point, and the updated total system mass.The left panel shows in gray 100 randomly sampled visual orbits from the posteriors with the current astrometry plotted on top (previous astrometry points are shown in pink while the 2023A astrometry point is shown in green). The top-right plot shows in gray 100 randomly sampled orbits’ separation in arcseconds from the host star as a function of epoch. The bottom-right plot is the same as the top right, but with the position angle, or P.A., in degrees as a function of epoch.
Paper: Orbital and Atmospheric Characterization of the 1RXS J034231.8+121622 System using High-resolution Spectroscopy Confirms that the Companion is a Low-mass Star
Authors: Clarissa R. Do Ó, Ben Sappey, Quinn M. Konopacky, Jean-Baptiste Ruffio, Kelly K. O'Neil, Tuan Do, Gregory Martinez, Travis S. Barman, Jayke S. Nguyen, Jerry W. Xuan, Christopher A. Theissen, Sarah Blunt, William Thompson, Chih-Chun Hsu, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Julie Inglis, Nemanja Jovanovic, Ronald A. López, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Jason J. Wang, Ji Wang, Joshua Liberman
Figure caption: Final C/O ratio fit for the primary and secondary. We also include a fit for the spin and RV using this model grid and note that most values are broadly consistent with each other.
Paper: Orbital and Atmospheric Characterization of the 1RXS J034231.8+121622 System using High-resolution Spectroscopy Confirms that the Companion is a Low-mass Star
Authors: Clarissa R. Do Ó, Ben Sappey, Quinn M. Konopacky, Jean-Baptiste Ruffio, Kelly K. O'Neil, Tuan Do, Gregory Martinez, Travis S. Barman, Jayke S. Nguyen, Jerry W. Xuan, Christopher A. Theissen, Sarah Blunt, William Thompson, Chih-Chun Hsu, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Julie Inglis, Nemanja Jovanovic, Ronald A. López, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Jason J. Wang, Ji Wang, Joshua Liberman
Figure caption: New orbit fit of 1RXS0342+1216 with the 2020 RV data point. Although RV data have the ability to break the degeneracy in the orientation of the orbital plane, the relative RV between the primary and the secondary in the 2020 epoch was close to 0 km s−1, meaning that we are not able to resolve that degeneracy with our data.
Paper: Orbital and Atmospheric Characterization of the 1RXS J034231.8+121622 System using High-resolution Spectroscopy Confirms that the Companion is a Low-mass Star
Authors: Clarissa R. Do Ó, Ben Sappey, Quinn M. Konopacky, Jean-Baptiste Ruffio, Kelly K. O'Neil, Tuan Do, Gregory Martinez, Travis S. Barman, Jayke S. Nguyen, Jerry W. Xuan, Christopher A. Theissen, Sarah Blunt, William Thompson, Chih-Chun Hsu, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Julie Inglis, Nemanja Jovanovic, Ronald A. López, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Jason J. Wang, Ji Wang, Joshua Liberman
Figure caption: Visual orbit fit for the companion with the previous and new system mass. No additional astrometry or RV data were used in these fits.
Paper: Orbital and Atmospheric Characterization of the 1RXS J034231.8+121622 System using High-resolution Spectroscopy Confirms that the Companion is a Low-mass Star
Authors: Clarissa R. Do Ó, Ben Sappey, Quinn M. Konopacky, Jean-Baptiste Ruffio, Kelly K. O'Neil, Tuan Do, Gregory Martinez, Travis S. Barman, Jayke S. Nguyen, Jerry W. Xuan, Christopher A. Theissen, Sarah Blunt, William Thompson, Chih-Chun Hsu, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Julie Inglis, Nemanja Jovanovic, Ronald A. López, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Jason J. Wang, Ji Wang, Joshua Liberman
Figure caption: New orbit fit of 1RXS0342+1216 with the new 2023A astrometry epoch and 2020 RV data point.
Paper: Orbital and Atmospheric Characterization of the 1RXS J034231.8+121622 System using High-resolution Spectroscopy Confirms that the Companion is a Low-mass Star
Authors: Clarissa R. Do Ó, Ben Sappey, Quinn M. Konopacky, Jean-Baptiste Ruffio, Kelly K. O'Neil, Tuan Do, Gregory Martinez, Travis S. Barman, Jayke S. Nguyen, Jerry W. Xuan, Christopher A. Theissen, Sarah Blunt, William Thompson, Chih-Chun Hsu, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Julie Inglis, Nemanja Jovanovic, Ronald A. López, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Jason J. Wang, Ji Wang, Joshua Liberman
Figure caption: Corner plots for 1RXS0342+1216 b’s orbital parameters with the previous system mass of 0.23 M ⊙. No new astrometry or radial-velocity data were included in this orbit fit.
Paper: Orbital and Atmospheric Characterization of the 1RXS J034231.8+121622 System using High-resolution Spectroscopy Confirms that the Companion is a Low-mass Star
Authors: Clarissa R. Do Ó, Ben Sappey, Quinn M. Konopacky, Jean-Baptiste Ruffio, Kelly K. O'Neil, Tuan Do, Gregory Martinez, Travis S. Barman, Jayke S. Nguyen, Jerry W. Xuan, Christopher A. Theissen, Sarah Blunt, William Thompson, Chih-Chun Hsu, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Julie Inglis, Nemanja Jovanovic, Ronald A. López, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Jason J. Wang, Ji Wang, Joshua Liberman
Figure caption: Corner plots for 1RXS0342+1216 b’s orbital parameters with the new system mass of 0.38 M ⊙. No new astrometry or radial-velocity data were included in this orbit fit.
Paper: Orbital and Atmospheric Characterization of the 1RXS J034231.8+121622 System using High-resolution Spectroscopy Confirms that the Companion is a Low-mass Star
Authors: Clarissa R. Do Ó, Ben Sappey, Quinn M. Konopacky, Jean-Baptiste Ruffio, Kelly K. O'Neil, Tuan Do, Gregory Martinez, Travis S. Barman, Jayke S. Nguyen, Jerry W. Xuan, Christopher A. Theissen, Sarah Blunt, William Thompson, Chih-Chun Hsu, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Julie Inglis, Nemanja Jovanovic, Ronald A. López, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Jason J. Wang, Ji Wang, Joshua Liberman
Figure caption: Uniform prior fit with Efit5 and orbitize! for the previous system mass of 0.23 M ⊙.
Paper: Orbital and Atmospheric Characterization of the 1RXS J034231.8+121622 System using High-resolution Spectroscopy Confirms that the Companion is a Low-mass Star
Authors: Clarissa R. Do Ó, Ben Sappey, Quinn M. Konopacky, Jean-Baptiste Ruffio, Kelly K. O'Neil, Tuan Do, Gregory Martinez, Travis S. Barman, Jayke S. Nguyen, Jerry W. Xuan, Christopher A. Theissen, Sarah Blunt, William Thompson, Chih-Chun Hsu, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Julie Inglis, Nemanja Jovanovic, Ronald A. López, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Jason J. Wang, Ji Wang, Joshua Liberman
Figure caption: New orbit fit of 1RXS0342+1216 with the new 2023A astrometry epoch.
Paper: The Strength and Variability of the Helium 10830 Å Triplet in Young Stars, with Implications for Exosphere Detection
Authors: Daniel M. Krolikowski, Adam L. Kraus, Benjamin M. Tofflemire, Caroline V. Morley, Andrew W. Mann, Andrew Vanderburg
Figure caption: Literature helium exosphere detections (circles) and upper limits (triangles) compared to our measurements of the 1σ intrinsic stellar variability level (see Section 5.1 for a description of the calculation). To show the age dependence, we plot the variability of V1298 Tau, K2-284, and HD 63433 as separate horizontal lines. The error bars at the left end of the plot show the 16th–84th percentile confidence interval on our measurement of the 1σ intrinsic stellar variability. The gray hatched region shows the 16th–84th percentile confidence interval on the variability measured with the combined >300 Myr sample, which agrees with there being no intrinsic variability. All but a few exosphere detections are smaller than variability at the youngest ages, but by 400 Myr all exosphere detections are comparable to or larger than the intrinsic stellar variability. Stellar variability should not preclude detection at these intermediate ages. The literature data is presented in Table A1.
Paper: Dynamical Architectures of S-type Transiting Planets in Binaries. I. Target Selection Using Hipparcos and Gaia Proper Motion Anomalies 
Authors: Jingwen Zhang, 婧雯 张, Lauren M. Weiss, Daniel Huber, Eric L. N. Jensen, Timothy D. Brandt, Karen Collins, Dennis M. Conti, Howard Isaacson, Pablo Lewin, Giuseppe Marino, Bob Massey, Felipe Murgas, Enric Palle, Don J. Radford, Howard M. Relles, Gregor Srdoc, Chris Stockdale, Thiam-Guan Tan, Gavin Wang
Figure caption: Principle of Hipparcos-Gaia proper motion anomalies. μ H and μ G represent the proper motions of the same star measured by Hipparcos and Gaia with a time baseline of around 25 yr. μ HG is the stellar long-term velocity across the sky plane. If we subtract μ HG from μ H and μ G, the residuals are the proper motion anomalies at the Hipparcos and Gaia epochs, respectively. (a) A star with marginal proper motion anomalies: if μ H and μ G are similar to the long-term velocity μ HG, the star moves across the sky plane in a linear motion. (b) A star with significant proper motion anomalies: a significant residual indicates the star not only moves linearly but also orbits around the system's barycenter due to the gravitational pull from a companion.
Paper: Direct Exoplanet Detection using Convolutional Image Reconstruction (ConStruct): A New Algorithm for Post-processing High-contrast Images
Authors: Trevor N. Wolf, Brandon A. Jones, Brendan P. Bowler
Figure caption: Parametric PCA post-processing search for the 2012 October 26 epoch data set of HR 8799. Each contour plot shows the recovered S/N over the grid of parameters tested. The violin plots show the spread in the S/N in each variable bin. Panels (a), (b), (c), and (d) correspond to HR 8799 b, c, d, and e, respectively.
Paper: Direct Exoplanet Detection using Convolutional Image Reconstruction (ConStruct): A New Algorithm for Post-processing High-contrast Images
Authors: Trevor N. Wolf, Brandon A. Jones, Brendan P. Bowler
Figure caption: Parametric PCA post-processing search for the 2010 July 13 epoch data set of HR 8799. Each contour plot shows the recovered S/N over the grid of parameters tested. The violin plots show the spread in the S/N in each variable bin. Panels (a), (b), (c), and (d) correspond to HR 8799 b, c, d, and e, respectively.
Paper: Direct Exoplanet Detection using Convolutional Image Reconstruction (ConStruct): A New Algorithm for Post-processing High-contrast Images
Authors: Trevor N. Wolf, Brandon A. Jones, Brendan P. Bowler
Figure caption: Parametric PCA post-processing search for the 2011 July 21 epoch data set of HR 8799. Each contour plot shows the recovered S/N over the grid of parameters tested. The violin plots show the spread in the S/N in each variable bin. Panels (a), (b), (c), and (d) correspond to HR 8799 b, c, d, and e, respectively.
Paper: Direct Exoplanet Detection using Convolutional Image Reconstruction (ConStruct): A New Algorithm for Post-processing High-contrast Images
Authors: Trevor N. Wolf, Brandon A. Jones, Brendan P. Bowler
Figure caption: Full-frame reductions with ConStruct and PCA of Kappa And (Carson et al. 2013) for Sequence 8 in Table 1.
Paper: Direct Exoplanet Detection using Convolutional Image Reconstruction (ConStruct): A New Algorithm for Post-processing High-contrast Images
Authors: Trevor N. Wolf, Brandon A. Jones, Brendan P. Bowler
Figure caption: Full-frame reductions with ConStruct and PCA of Kappa And (Carson et al. 2013) for Sequence 7 in Table 1.
Paper: Direct Exoplanet Detection using Convolutional Image Reconstruction (ConStruct): A New Algorithm for Post-processing High-contrast Images
Authors: Trevor N. Wolf, Brandon A. Jones, Brendan P. Bowler
Figure caption: Full-frame reductions with ConStruct and PCA of HD 114174 (Crepp et al. 2013a) for Sequence 4 in Table 1.
Paper: Direct Exoplanet Detection using Convolutional Image Reconstruction (ConStruct): A New Algorithm for Post-processing High-contrast Images
Authors: Trevor N. Wolf, Brandon A. Jones, Brendan P. Bowler
Figure caption: Full-frame reductions with ConStruct and PCA of HR 7672 (Liu et al. 2002) for Sequence 6 in Table 1.
Paper: Direct Exoplanet Detection using Convolutional Image Reconstruction (ConStruct): A New Algorithm for Post-processing High-contrast Images
Authors: Trevor N. Wolf, Brandon A. Jones, Brendan P. Bowler
Figure caption: Full-frame reductions with ConStruct and PCA of HD 4747 (Crepp et al. 2016) for Sequence 1 in Table 1.
Paper: Direct Exoplanet Detection using Convolutional Image Reconstruction (ConStruct): A New Algorithm for Post-processing High-contrast Images
Authors: Trevor N. Wolf, Brandon A. Jones, Brendan P. Bowler
Figure caption: Full-frame reductions with ConStruct and PCA of HD 19467 (Crepp et al. 2014) for Sequence 2 in Table 1.
Paper: The DECam Ecliptic Exploration Project (DEEP). VI. First Multiyear Observations of Trans-Neptunian Objects
Authors: Hayden Smotherman, Pedro H. Bernardinelli, Stephen K. N. Portillo, Andrew J. Connolly, J. Bryce Kalmbach, Steven Stetzler, Mario Jurić, Dino Bektešević, Zachary Langford, Fred C. Adams, William J. Oldroyd, Matthew J. Holman, Colin Orion Chandler, Cesar Fuentes, David W. Gerdes, Hsing Wen Lin, 省文 林, Larissa Markwardt, Andrew McNeill, Michael Mommert, Kevin J. Napier, Matthew J. Payne, Darin Ragozzine, Andrew S. Rivkin, Hilke Schlichting, Scott S. Sheppard, Ryder Strauss, David E. Trilling, Chadwick A. Trujillo
Figure caption: Left: histograms of χ 2/ν determined with the full covariance matrices for the subsets of linkages corresponding to real detections (blue), fake detections (red), and the bad linkages, that is, those that we know are mislinked (orange). The vertical line indicates the χ 2/ν = 4.5 threshold. Right: histogram of the fractional error in semimajor axis (σ  a /a) for the real (blue) and fake (red) orbits with χ 2/ν < 4.5. We note that the different structure in the distributions is not an inherent problem, but stems from the very different populations of orbits that belong to these two samples.
Paper: The DECam Ecliptic Exploration Project (DEEP). VI. First Multiyear Observations of Trans-Neptunian Objects
Authors: Hayden Smotherman, Pedro H. Bernardinelli, Stephen K. N. Portillo, Andrew J. Connolly, J. Bryce Kalmbach, Steven Stetzler, Mario Jurić, Dino Bektešević, Zachary Langford, Fred C. Adams, William J. Oldroyd, Matthew J. Holman, Colin Orion Chandler, Cesar Fuentes, David W. Gerdes, Hsing Wen Lin, 省文 林, Larissa Markwardt, Andrew McNeill, Michael Mommert, Kevin J. Napier, Matthew J. Payne, Darin Ragozzine, Andrew S. Rivkin, Hilke Schlichting, Scott S. Sheppard, Ryder Strauss, David E. Trilling, Chadwick A. Trujillo
Figure caption: A visualization of the signal-to-noise ratio cutoff is used to determine if a candidate should be considered real. Top left: the number of all fakes that were included in vetting (blue) and the number of fakes that were labeled “good” in human vetting. The ideal case is that the orange histogram matches the blue histogram. S/N is bounded to 0 < S/N < 100 for visibility. Top right: the number of all reverse search candidates that were included in vetting (blue) and the number of reverse search candidates that were labeled “good” in human vetting (orange). The ideal case is that the orange histogram goes to zero. We bound to 0 < S/N < 100 for visibility. Bottom: A parametric plot of the number of reverse search candidates kept after human vetting (lower is better) vs. the number of fakes kept after human vetting (higher is better) as a function of S/N. The blue dashed–dotted vertical line corresponds to the selected S/N cutoff value of 4.10.
Paper: The DECam Ecliptic Exploration Project (DEEP). VI. First Multiyear Observations of Trans-Neptunian Objects
Authors: Hayden Smotherman, Pedro H. Bernardinelli, Stephen K. N. Portillo, Andrew J. Connolly, J. Bryce Kalmbach, Steven Stetzler, Mario Jurić, Dino Bektešević, Zachary Langford, Fred C. Adams, William J. Oldroyd, Matthew J. Holman, Colin Orion Chandler, Cesar Fuentes, David W. Gerdes, Hsing Wen Lin, 省文 林, Larissa Markwardt, Andrew McNeill, Michael Mommert, Kevin J. Napier, Matthew J. Payne, Darin Ragozzine, Andrew S. Rivkin, Hilke Schlichting, Scott S. Sheppard, Ryder Strauss, David E. Trilling, Chadwick A. Trujillo
Figure caption: Two examples of objects recovered with KBMOD, the first an injected TNO with magnitude m  VR  = 24.9 and a barycentric distance of 60 au, the second a real cold Classical TNO with m  VR  = 26.0. These images are used for human vetting. The title includes information from the KBMOD search, including ∑LH, flux, starting x and y pixel location, and speed. The two postage stamps in the upper left are sum and median coadds, as well as an approximate S/N estimated from these postage stamps. The graph in the upper right shows an approximate flux light curve. The postage stamps included below are the first 20 out of 100 cutouts from individual images in the long stare.
Paper: The DECam Ecliptic Exploration Project (DEEP). VI. First Multiyear Observations of Trans-Neptunian Objects
Authors: Hayden Smotherman, Pedro H. Bernardinelli, Stephen K. N. Portillo, Andrew J. Connolly, J. Bryce Kalmbach, Steven Stetzler, Mario Jurić, Dino Bektešević, Zachary Langford, Fred C. Adams, William J. Oldroyd, Matthew J. Holman, Colin Orion Chandler, Cesar Fuentes, David W. Gerdes, Hsing Wen Lin, 省文 林, Larissa Markwardt, Andrew McNeill, Michael Mommert, Kevin J. Napier, Matthew J. Payne, Darin Ragozzine, Andrew S. Rivkin, Hilke Schlichting, Scott S. Sheppard, Ryder Strauss, David E. Trilling, Chadwick A. Trujillo
Figure caption: On-sky positions of the B1 field. The pointings included here are the first observations of each field taken in 2021. Each field is centered on the R.A. and decl. of the first exposure in the long stare. The solid line shows the invariable plane, and the dashed line shows the ecliptic.
Paper: The DECam Ecliptic Exploration Project (DEEP). VI. First Multiyear Observations of Trans-Neptunian Objects
Authors: Hayden Smotherman, Pedro H. Bernardinelli, Stephen K. N. Portillo, Andrew J. Connolly, J. Bryce Kalmbach, Steven Stetzler, Mario Jurić, Dino Bektešević, Zachary Langford, Fred C. Adams, William J. Oldroyd, Matthew J. Holman, Colin Orion Chandler, Cesar Fuentes, David W. Gerdes, Hsing Wen Lin, 省文 林, Larissa Markwardt, Andrew McNeill, Michael Mommert, Kevin J. Napier, Matthew J. Payne, Darin Ragozzine, Andrew S. Rivkin, Hilke Schlichting, Scott S. Sheppard, Ryder Strauss, David E. Trilling, Chadwick A. Trujillo
Figure caption: Astrometric (left) and photometric (right) residuals for single-night detected fakes with S/N > 4.1. These results come from the output of the joint-fit process described in Section 3. The title of each subplot shows the mean μ, standard deviation σ, and σ  G  (see Equation (7)) value of each distribution.
Paper: The DECam Ecliptic Exploration Project (DEEP). VI. First Multiyear Observations of Trans-Neptunian Objects
Authors: Hayden Smotherman, Pedro H. Bernardinelli, Stephen K. N. Portillo, Andrew J. Connolly, J. Bryce Kalmbach, Steven Stetzler, Mario Jurić, Dino Bektešević, Zachary Langford, Fred C. Adams, William J. Oldroyd, Matthew J. Holman, Colin Orion Chandler, Cesar Fuentes, David W. Gerdes, Hsing Wen Lin, 省文 林, Larissa Markwardt, Andrew McNeill, Michael Mommert, Kevin J. Napier, Matthew J. Payne, Darin Ragozzine, Andrew S. Rivkin, Hilke Schlichting, Scott S. Sheppard, Ryder Strauss, David E. Trilling, Chadwick A. Trujillo
Figure caption: Median topocentric discovery distance for all correctly linked fake orbits and all 110 real orbits that pass all orbital cuts. The median is taken from the distribution of topocentric distances for each long stare (and thus each tracklet) in the linked orbit.
Paper: The Cepheid Distance Scale: A Novel Method for Obtaining Mean Magnitudes from Single-epoch Observations
Authors: Barry F. Madore, Wendy L. Freedman, Kayla Owens
Figure caption: Eight period–luminosity relations for Cepheids in the Large Magellanic Cloud running (top to bottom) from the mid-infrared (4.5 and 3.6 μm; Scowcroft et al. 2011), to the near-infrared (JHK; Persson et al. 2004) and finally the optical (BVI from the “Three-hundred MilliMeter Telescope” (TMMT), which has been operating remotely in a queue-scheduled mode at the Las Campanas Observatory in Chile for the past 10 years, gathering BVI photometric data on nearby supernovae as well as Classical Cepheids in the Milky Way, LMC and SMC; A. Monson et al. 2024, in preparation). Individual PL ridge lines are shown as dashed lines, flanked on either side by the blue/bright and red/faint limits of the instability strip shown by ±2σ solid lines. The monotonic increase in the widths of the PL relations, top to bottom, long wavelength to short, can be readily seen. A closer look at the deviations of individual Cepheids with respect to the ridge line and with respect to one another in the B-band PL relation, for example, are repeated in detail and at high fidelity; however, simply in a progressively more compressed way in every one of the other PL relations, shrinking from blue to red, as should be the case. (Note that not all of the Cepheids plotted were observed in all of the bands shown.)