adsabs/AstroCLIMB huggingface dataset:
Paper: Resolved SPLASH Chemodynamics in Andromeda’s PHAT Stellar Halo and Disk: On the Nature of the Inner Halo along the Major Axis
Authors: Ivanna Escala, Amanda C. N. Quirk, Puragra Guhathakurta, Karoline M. Gilbert, J. Leigh Wojno, Lara Cullinane, Benjamin F. Williams, Julianne Dalcanton
Figure caption: The locations of the DEIMOS fields from SPLASH (magenta patches; Section 2.2; Dorman et al. 2012, 2013, 2015) in M31-centric coordinates. The approximate size and orientation of each field is represented by a 16′ × 4′ rectangle. The outlines of the PHAT footprints (Section 2.1; Dalcanton et al. 2012) are shown as the blue lines. The near-UV image of M31 is from the PHAT archive and was taken by GALEX.
Paper: Resolved SPLASH Chemodynamics in Andromeda’s PHAT Stellar Halo and Disk: On the Nature of the Inner Halo along the Major Axis
Authors: Ivanna Escala, Amanda C. N. Quirk, Puragra Guhathakurta, Karoline M. Gilbert, J. Leigh Wojno, Lara Cullinane, Benjamin F. Williams, Julianne Dalcanton
Figure caption: Heliocentric velocity distributions for region R3 (Section 3.2.1). From left to right, the panels show the velocity distribution in each subregion (gray histograms; Figure 3; Table 1), where R31 straddles the major axis and R34 is the most distant from the major axis. We also show the fitted velocity model for each subregion (thick purple lines; Section 3.2.2), which is composed of a stellar halo component (Dorman et al. 2012) with fixed mean and dispersion, but variable fractional contribution (dotted blue lines), and a disk component (dashed green lines). Figures 16 and 17 show the velocity distributions and models for R1 and R2. In general, the trends between the disk component velocity and ΔP.A. follow those expected for an inclined rotating disk approaching M31's systemic velocity (−300 km s−1) with increasing ΔP.A. (Dorman et al. 2012). The stellar halo component also becomes more dominant with increasing ΔP.A.
Paper: Resolved SPLASH Chemodynamics in Andromeda’s PHAT Stellar Halo and Disk: On the Nature of the Inner Halo along the Major Axis
Authors: Ivanna Escala, Amanda C. N. Quirk, Puragra Guhathakurta, Karoline M. Gilbert, J. Leigh Wojno, Lara Cullinane, Benjamin F. Williams, Julianne Dalcanton
Figure caption: Locations of the annular radial regions (R1, R2, and R3) and angular subregions in M31-centric coordinates used to model the velocity distributions (Section 3.2.1). Each point corresponds to an M31 giant star with a successful velocity measurement from SPLASH. The regions R1, R2, and R3 are bounded by R proj = 8, 12, and 18.5 kpc, respectively, where the kinematical parameters of the halo component in each region are fixed to the values obtained by Dorman et al. (2012). Each radial annulus is divided into angular subregions, based on the absolute position angle relative to the major axis (P.A. = 38°), where these subregions are used to constrain the disk component of the velocity distribution. Note that stars on either side of the major axis that are represented by the same color are part of the same subregion. Subregion designations are based on absolute angular distance from the major axis (i.e., R31 straddles the major axis and R34 is the most distant from the major axis).
Paper: Resolved SPLASH Chemodynamics in Andromeda’s PHAT Stellar Halo and Disk: On the Nature of the Inner Halo along the Major Axis
Authors: Ivanna Escala, Amanda C. N. Quirk, Puragra Guhathakurta, Karoline M. Gilbert, J. Leigh Wojno, Lara Cullinane, Benjamin F. Williams, Julianne Dalcanton
Figure caption: The sky locations of the M31 RGB stars in SPLASH, color-coded by (left) the fraction of reddened RGB stars (f red) and (right) the median extinction (A  V,Dal) from the maps of the dust in M31's disk by Dalcanton et al. (2015; Section 4.2.1). We do not show the spread in extinction, where σ  V  ∼ 0.30 over the entire sample. RGB stars with ΔP.A. < 0 (Section 3.2.1) are more likely to be reddened, given that M31's inclined thick disk is viewed in projection (J. Dalcanton et al. 2022, in preparation). The dust extinction is highest in the 10 kpc star-forming ring (Gordon et al. 2006). We use these maps to assess the impact of the dust in M31's disk on the photometric metallicity measurements in Section 4.2.2.
Paper: Resolved SPLASH Chemodynamics in Andromeda’s PHAT Stellar Halo and Disk: On the Nature of the Inner Halo along the Major Axis
Authors: Ivanna Escala, Amanda C. N. Quirk, Puragra Guhathakurta, Karoline M. Gilbert, J. Leigh Wojno, Lara Cullinane, Benjamin F. Williams, Julianne Dalcanton
Figure caption: The locations of the giant stars in M31-centric coordinates, color-coded by the probability that a given star belongs to the disk vs. the halo. The disk probability (p disk) is based on the velocity model for the subregion in which a star is located and its heliocentric velocity (Section 3.2.2). Stars with p disk ≥ 0.75 (p disk ≤ 0.25) are ≥three times more likely to belong to the disk vs. the halo (and vice versa).
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South I: Composition and Climate of the Ultrahot Jupiter WASP-18 b
Authors: Matteo Brogi, Vanessa Emeka-Okafor, Michael R. Line, Siddharth Gandhi, Lorenzo Pino, Eliza M.-R. Kempton, Emily Rauscher, Vivien Parmentier, Jacob L. Bean, Gregory N. Mace, Nicolas B. Cowan, Evgenya Shkolnik, Joost P. Wardenier, Megan Mansfield, Luis Welbanks, Peter Smith, Jonathan J. Fortney, Jayne L. Birkby, Joseph A. Zalesky, Lisa Dang, Jennifer Patience, Jean-Michel Désert
Figure caption: Summary of the retrieved TP profiles and their sensitivity to the various free-retrieval assumption scenarios described in Section 4, indicated at the top. These are summarized with the 95% CIs derived from individual temperature profiles reconstructed from 500 random posterior draws (based upon the T irr, log(κ IR), and log(γ  v ) constraints). We also include select self-consistent 1D-RCTE TP profiles to facilitate comparison. Here, DAY represents a redistributing scaling factor of 2 and MAX is 2.67 (see footnote 23). Despite the wide CIs, the general morphology of the retrieved TP profiles is consistent with the 1D-RCTE predictions (e.g., rising temperature with decreasing pressure).
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South I: Composition and Climate of the Ultrahot Jupiter WASP-18 b
Authors: Matteo Brogi, Vanessa Emeka-Okafor, Michael R. Line, Siddharth Gandhi, Lorenzo Pino, Eliza M.-R. Kempton, Emily Rauscher, Vivien Parmentier, Jacob L. Bean, Gregory N. Mace, Nicolas B. Cowan, Evgenya Shkolnik, Joost P. Wardenier, Megan Mansfield, Luis Welbanks, Peter Smith, Jonathan J. Fortney, Jayne L. Birkby, Joseph A. Zalesky, Lisa Dang, Jennifer Patience, Jean-Michel Désert
Figure caption: Elemental abundances derived from the free-retrieval gas mixing ratio constraints (blue) vs. the corresponding constraints from the self-consistent, grid-based 1D-RCTE retrieval (red). A correction to the free retrieval accounting for ≈40% atomic oxygen (non-detectable) is shown with the green dotted lines. Elemental values for the star, WASP-18, are shown as the black dot (Polanski et al. 2022) and those for the Sun as the yellow dot (Lodders et al. 2009). The metallicity axis is normalized to the solar values (see Equation (2)).
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South I: Composition and Climate of the Ultrahot Jupiter WASP-18 b
Authors: Matteo Brogi, Vanessa Emeka-Okafor, Michael R. Line, Siddharth Gandhi, Lorenzo Pino, Eliza M.-R. Kempton, Emily Rauscher, Vivien Parmentier, Jacob L. Bean, Gregory N. Mace, Nicolas B. Cowan, Evgenya Shkolnik, Joost P. Wardenier, Megan Mansfield, Luis Welbanks, Peter Smith, Jonathan J. Fortney, Jayne L. Birkby, Joseph A. Zalesky, Lisa Dang, Jennifer Patience, Jean-Michel Désert
Figure caption: Corner plots for the 15 parameters of the “Fiducial” retrieval including a scaling factor. See Section 4 for details.
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South I: Composition and Climate of the Ultrahot Jupiter WASP-18 b
Authors: Matteo Brogi, Vanessa Emeka-Okafor, Michael R. Line, Siddharth Gandhi, Lorenzo Pino, Eliza M.-R. Kempton, Emily Rauscher, Vivien Parmentier, Jacob L. Bean, Gregory N. Mace, Nicolas B. Cowan, Evgenya Shkolnik, Joost P. Wardenier, Megan Mansfield, Luis Welbanks, Peter Smith, Jonathan J. Fortney, Jayne L. Birkby, Joseph A. Zalesky, Lisa Dang, Jennifer Patience, Jean-Michel Désert
Figure caption: Grid-based retrieval gas volume mixing ratios and temperature profiles compared to the “Fiducial” free-retrieval constraints. The grid-based 1D-RCTE atmospheric gas volume mixing ratio– (left three panels in blue) and temperature– (rightmost panel in red) pressure profiles (solid curves) are drawn from the grid-retrieval posterior samples. The free-retrieval histograms and 95% CIs for H2O, CO, and OH (left 3 panels) are the same as those in the top panel of Figure 6. The rightmost panel shows the 95% CI of the reconstructed free-retrieval TP profiles in light red (same as the top left panel in Figure 7). There is general agreement in both the volume mixing ratios and temperature–pressure profiles.
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South I: Composition and Climate of the Ultrahot Jupiter WASP-18 b
Authors: Matteo Brogi, Vanessa Emeka-Okafor, Michael R. Line, Siddharth Gandhi, Lorenzo Pino, Eliza M.-R. Kempton, Emily Rauscher, Vivien Parmentier, Jacob L. Bean, Gregory N. Mace, Nicolas B. Cowan, Evgenya Shkolnik, Joost P. Wardenier, Megan Mansfield, Luis Welbanks, Peter Smith, Jonathan J. Fortney, Jayne L. Birkby, Joseph A. Zalesky, Lisa Dang, Jennifer Patience, Jean-Michel Désert
Figure caption: 1 and 2σ CIs for H2O (blue), CO (red), OH (purple), and their mixed spectrum (black) in rest-frame velocity and planet orbital velocity. It shows a blueshift detected for CO and OH, marginally (∼2σ) inconsistent with H2O. Further discussion is given in Section 5.3.
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South I: Composition and Climate of the Ultrahot Jupiter WASP-18 b
Authors: Matteo Brogi, Vanessa Emeka-Okafor, Michael R. Line, Siddharth Gandhi, Lorenzo Pino, Eliza M.-R. Kempton, Emily Rauscher, Vivien Parmentier, Jacob L. Bean, Gregory N. Mace, Nicolas B. Cowan, Evgenya Shkolnik, Joost P. Wardenier, Megan Mansfield, Luis Welbanks, Peter Smith, Jonathan J. Fortney, Jayne L. Birkby, Joseph A. Zalesky, Lisa Dang, Jennifer Patience, Jean-Michel Désert
Figure caption: Comparison between the HyDRA-H retrieval (in blue) and the “Fixed a = 1” CHIMERA retrieval (in red; see also Table 2 and Section 4.2). The constraints on the abundances (four panels, left side) and the TP profiles (right side) are compatible within 1σ.
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South I: Composition and Climate of the Ultrahot Jupiter WASP-18 b
Authors: Matteo Brogi, Vanessa Emeka-Okafor, Michael R. Line, Siddharth Gandhi, Lorenzo Pino, Eliza M.-R. Kempton, Emily Rauscher, Vivien Parmentier, Jacob L. Bean, Gregory N. Mace, Nicolas B. Cowan, Evgenya Shkolnik, Joost P. Wardenier, Megan Mansfield, Luis Welbanks, Peter Smith, Jonathan J. Fortney, Jayne L. Birkby, Joseph A. Zalesky, Lisa Dang, Jennifer Patience, Jean-Michel Désert
Figure caption: Corner plots for the 14 parameters of the retrieval with the scaling factor set to 1 (labeled as “Fixed a = 1” in Table 2). See Section 4.2 for details.
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South I: Composition and Climate of the Ultrahot Jupiter WASP-18 b
Authors: Matteo Brogi, Vanessa Emeka-Okafor, Michael R. Line, Siddharth Gandhi, Lorenzo Pino, Eliza M.-R. Kempton, Emily Rauscher, Vivien Parmentier, Jacob L. Bean, Gregory N. Mace, Nicolas B. Cowan, Evgenya Shkolnik, Joost P. Wardenier, Megan Mansfield, Luis Welbanks, Peter Smith, Jonathan J. Fortney, Jayne L. Birkby, Joseph A. Zalesky, Lisa Dang, Jennifer Patience, Jean-Michel Désert
Figure caption: Corner plots for the 15 parameters of the retrieval including only the first half of the spectra (labeled as “1st half” in Table 2). See Section 4.3 for details.
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South I: Composition and Climate of the Ultrahot Jupiter WASP-18 b
Authors: Matteo Brogi, Vanessa Emeka-Okafor, Michael R. Line, Siddharth Gandhi, Lorenzo Pino, Eliza M.-R. Kempton, Emily Rauscher, Vivien Parmentier, Jacob L. Bean, Gregory N. Mace, Nicolas B. Cowan, Evgenya Shkolnik, Joost P. Wardenier, Megan Mansfield, Luis Welbanks, Peter Smith, Jonathan J. Fortney, Jayne L. Birkby, Joseph A. Zalesky, Lisa Dang, Jennifer Patience, Jean-Michel Désert
Figure caption: Corner plots for the 15 parameters of the retrieval where a cosine function is applied to the scaling factor as a function of planet orbital phase (labeled as “Phase Dep. a” in Table 2). See Section 4.2 for details.
Paper: Stellar Properties for a Comprehensive Collection of Star-forming Regions in the SDSS APOGEE-2 Survey 
Authors: Carlos G. Román-Zúñiga, Marina Kounkel, Jesús Hernández, Karla Peña Ramírez, Ricardo López-Valdivia, Kevin R. Covey, Amelia M. Stutz, Alexandre Roman-Lopes, Hunter Campbell, Elliott Khilfeh, Mauricio Tapia, Guy S. Stringfellow, Juan José Downes, Keivan G. Stassun, Dante Minniti, Amelia Bayo, Jinyoung Serena Kim, Genaro Suárez, Jason E. Ybarra, José G. Fernández-Trincado, Penélope Longa-Peña, Valeria Ramírez-Preciado, Javier Serna, Richard R. Lane, D. A. García-Hernández, Rachael L. Beaton, Dmitry Bizyaev, Kaike Pan
Figure caption: Example of region member selection refinements. Both panels show a distribution of the geometric distance estimates from Bailer-Jones et al. (2021) vs. mean extinction, 〈A  V 〉, from MassAge. The left panel shows the HDBSCAN resultant cluster groups for all targets observed in the λ Ori region, where it can be seen how Group 2 stars contain most of the sources coinciding with the expected distance to the cluster (about 380 pc), stars from Group 3 are in most cases background field sources, and Group 1 may contain a few sources at the expected distance. In the close-up in the right panel, the colors of the points indicate the cluster membership probability, where the stars with bluer colors pertain to a group that contains stars from Groups 1 and 2 with distances between 350 and 450 pc, ﹩\mathrm{log}\,g﹩ > 3.5, and T eff > 6500. Those restrictions define the HRMs for this region.
Paper: Stellar Properties for a Comprehensive Collection of Star-forming Regions in the SDSS APOGEE-2 Survey 
Authors: Carlos G. Román-Zúñiga, Marina Kounkel, Jesús Hernández, Karla Peña Ramírez, Ricardo López-Valdivia, Kevin R. Covey, Amelia M. Stutz, Alexandre Roman-Lopes, Hunter Campbell, Elliott Khilfeh, Mauricio Tapia, Guy S. Stringfellow, Juan José Downes, Keivan G. Stassun, Dante Minniti, Amelia Bayo, Jinyoung Serena Kim, Genaro Suárez, Jason E. Ybarra, José G. Fernández-Trincado, Penélope Longa-Peña, Valeria Ramírez-Preciado, Javier Serna, Richard R. Lane, D. A. García-Hernández, Rachael L. Beaton, Dmitry Bizyaev, Kaike Pan
Figure caption: A map, in Galactic coordinates, showing the locations of all the fields listed in Table 3, along with labels identifying the 18 main regions reported in this study. Each circular field is projected with a realistic radius of 1.5 or 1.°0 for regions observed with the APOGEE-N and APOGEE-S instruments, respectively. The colors of the fields refer to the field subprograms described in Section 2.
Paper: Stellar Properties for a Comprehensive Collection of Star-forming Regions in the SDSS APOGEE-2 Survey 
Authors: Carlos G. Román-Zúñiga, Marina Kounkel, Jesús Hernández, Karla Peña Ramírez, Ricardo López-Valdivia, Kevin R. Covey, Amelia M. Stutz, Alexandre Roman-Lopes, Hunter Campbell, Elliott Khilfeh, Mauricio Tapia, Guy S. Stringfellow, Juan José Downes, Keivan G. Stassun, Dante Minniti, Amelia Bayo, Jinyoung Serena Kim, Genaro Suárez, Jason E. Ybarra, José G. Fernández-Trincado, Penélope Longa-Peña, Valeria Ramírez-Preciado, Javier Serna, Richard R. Lane, D. A. García-Hernández, Rachael L. Beaton, Dmitry Bizyaev, Kaike Pan
Figure caption: Effective temperature vs. Gaia EDR3 colors for the APOGEE Pleiades sample. The symbol colors represent age estimates from MassAge. The solid line is the empirical sequence from Esplin et al. (2018).
Paper: Speckle Space–Time Covariance in High-contrast Imaging
Authors: Briley Lewis, Michael P. Fitzgerald, Rupert H. Dodkins, Kristina K. Davis, Jonathan Lin
Figure caption: Diagram of stKLIP input sequence setup—translating phase screens (top) and resulting image sequence (middle)—with the corresponding block diagonal space–time covariance matrix (bottom). Each covariance block C  i  is the covariance for a single lag, with shape n  p  × n  p , and together they create a single space–time covariance matrix C with size n  s  n  p  × n  s  n  p . The covariance matrix takes this form because the 2D images are flattened into 1D vectors, which are then joined to make an n  p  × n  s  1D vector, which is multiplied by its transpose to create this matrix.
Paper: A Green Bank Telescope Search for Narrowband Technosignatures between 1.1 and 1.9 GHz During 12 Kepler Planetary Transits
Authors: Sofia Z. Sheikh, Shubham Kanodia, Emily Lubar, William P. Bowman, Caleb I. Cañas, Christian Gilbertson, Mariah G. MacDonald, Jason Wright, David MacMahon, Steve Croft, Danny Price, Andrew Siemion, Jamie Drew, S. Pete Worden, Elizabeth Trenholm
Figure caption: The signal of interest in Kepler-842b data shown in the high frequency-resolution data (left) and the midresolution data (right). The regions of data shown are related as indicated by the white-dashed rectangles, with the right plot zoomed out in frequency and zoomed in in time. The signal of interest has a distinctive, periodic structure in frequency and is present across the bandwidth. This behavior is characteristic of RFI.
Paper: A Green Bank Telescope Search for Narrowband Technosignatures between 1.1 and 1.9 GHz During 12 Kepler Planetary Transits
Authors: Sofia Z. Sheikh, Shubham Kanodia, Emily Lubar, William P. Bowman, Caleb I. Cañas, Christian Gilbertson, Mariah G. MacDonald, Jason Wright, David MacMahon, Steve Croft, Danny Price, Andrew Siemion, Jamie Drew, S. Pete Worden, Elizabeth Trenholm
Figure caption: A portion of the signal of interest detected in Kepler-842b. This signal of interest spans 1040–1438 MHz, so this is not the full signal, but rather a narrow bandwidth example of one of the “hits” on this signal generated by turboSETI.
Paper: A Green Bank Telescope Search for Narrowband Technosignatures between 1.1 and 1.9 GHz During 12 Kepler Planetary Transits
Authors: Sofia Z. Sheikh, Shubham Kanodia, Emily Lubar, William P. Bowman, Caleb I. Cañas, Christian Gilbertson, Mariah G. MacDonald, Jason Wright, David MacMahon, Steve Croft, Danny Price, Andrew Siemion, Jamie Drew, S. Pete Worden, Elizabeth Trenholm
Figure caption: The signal of interest in Kepler-1332b data shown in the high-frequency-resolution data (left) and the midresolution data (right). The regions of data shown are related as indicated by the white-dashed rectangles, with the right plot zoomed out in frequency and zoomed in in time. The signal of interest is actually composed of two short (<1 s) pulses.
Paper: A Green Bank Telescope Search for Narrowband Technosignatures between 1.1 and 1.9 GHz During 12 Kepler Planetary Transits
Authors: Sofia Z. Sheikh, Shubham Kanodia, Emily Lubar, William P. Bowman, Caleb I. Cañas, Christian Gilbertson, Mariah G. MacDonald, Jason Wright, David MacMahon, Steve Croft, Danny Price, Andrew Siemion, Jamie Drew, S. Pete Worden, Elizabeth Trenholm
Figure caption: The signal of interest detected in Kepler-1332b.
Paper: On Averaging Eccentric Orbits: Implications for the Long-term Thermal Evolution of Comets
Authors: Anastasios Gkotsinas, Aurélie Guilbert-Lepoutre, Sean N. Raymond
Figure caption: Subsurface temperature distributions for a layer of 10 m over a period of 1000 yr for (a) an elliptical orbit with a = 10 au and e = 0.5, (b) true-anomaly-averaged radius (﹩{\bar{r}}_{\theta }﹩), (c) true-anomaly-averaged flux (﹩{\bar{r}}_{\theta F}﹩), (d) effective thermal radius (r  T ), (e) time-averaged flux (﹩{\bar{r}}_{{tF}}﹩), and (f) time-averaged radius (﹩{\bar{r}}_{t}﹩) equivalent circular orbits.
Paper: On Averaging Eccentric Orbits: Implications for the Long-term Thermal Evolution of Comets
Authors: Anastasios Gkotsinas, Aurélie Guilbert-Lepoutre, Sean N. Raymond
Figure caption: Temperature profiles for a subsurface layer of 10 m, ∼1 Myr after the start of the simulations, for three a, e couples: (a) a = 7.94 au and e = 0.7, (b) a = 10.0 au and e = 0.5, and (c) a = 25.11 and e = 0.2. The solid black lines give the temperature profiles of elliptic orbits at perihelion, aphelion, and halfway through—time-wise—both inward and outward. The temperatures profiles for the equivalent orbits are true-anomaly-averaged radius (﹩{\bar{r}}_{\theta }﹩) (blue loosely dashed–dotted line), true-anomaly-averaged flux (﹩{\bar{r}}_{\theta F}﹩) (yellow dashed–dotted line), time-averaged radius (﹩{\bar{r}}_{t}﹩) (green dashed line), time-averaged flux (﹩{\bar{r}}_{{tF}}﹩) (red dotted line), and effective thermal radius (r  T ) (purple loosely dashed line).
Paper: On Averaging Eccentric Orbits: Implications for the Long-term Thermal Evolution of Comets
Authors: Anastasios Gkotsinas, Aurélie Guilbert-Lepoutre, Sean N. Raymond
Figure caption: Temperature differences between the elliptic orbits at perihelion and the time-averaged radius (﹩{\bar{r}}_{t}﹩) (top row), the time-averaged flux (﹩{\bar{r}}_{{tF}}﹩) (middle row), and the effective thermal radius (r  T ) equivalent orbits (bottom row) for three depths: surface (left column), 1 m (middle column), and 10 m (right column) for all the a, e couples.
Paper: On Averaging Eccentric Orbits: Implications for the Long-term Thermal Evolution of Comets
Authors: Anastasios Gkotsinas, Aurélie Guilbert-Lepoutre, Sean N. Raymond
Figure caption: Temperature differences between the elliptic orbits at aphelion and the time-averaged radius (﹩{\bar{r}}_{t}﹩; top row), the time-averaged flux (﹩{\bar{r}}_{{tF}}﹩; middle row), and the effective thermal radius (r  T ) equivalent orbits (bottom row) for three depths: surface (left column), 1 m (middle column), and 10 m (right column) for all the a, e couples.
Paper: On Averaging Eccentric Orbits: Implications for the Long-term Thermal Evolution of Comets
Authors: Anastasios Gkotsinas, Aurélie Guilbert-Lepoutre, Sean N. Raymond
Figure caption: Temperature differences between the elliptic orbits halfway through inward (time-wise) and the time-averaged radius (﹩{\bar{r}}_{t}﹩; top row), the time-averaged flux (﹩{\bar{r}}_{{tF}}﹩; middle row), and the effective thermal radius (r  T ) equivalent orbits (bottom row) for three depths: surface (left column), 1 m (middle column), and 10 m (right column) for all the a, e couples.
Paper: On Averaging Eccentric Orbits: Implications for the Long-term Thermal Evolution of Comets
Authors: Anastasios Gkotsinas, Aurélie Guilbert-Lepoutre, Sean N. Raymond
Figure caption: Temperature differences between the elliptic orbits halfway through outward (time-wise) and the time-averaged radius (﹩{\bar{r}}_{t}﹩; top row), the time-averaged flux (﹩{\bar{r}}_{{tF}}﹩; middle row), and the effective thermal radius (r  T ) equivalent orbits (bottom row) for three depths: surface (left column), 1 m (middle column), and 10 m (right column) for all the a, e couples.
Paper: On Averaging Eccentric Orbits: Implications for the Long-term Thermal Evolution of Comets
Authors: Anastasios Gkotsinas, Aurélie Guilbert-Lepoutre, Sean N. Raymond
Figure caption: A typical Jupiter-family comet trajectory taken from Gkotsinas et al. (2022) plotted over the temperature differences between elliptic orbits and an average of the effective thermal radius (r  T ) inward and outward for all the a, e couples. Each circle represents a point in our orbital parameter space sampling. The color code gives the scale of the temperature difference.