adsabs/AstroCLIMB huggingface dataset:
Paper: Polarization of Circumstellar Debris Disk Light Echoes
Authors: Austin J. King, Benjamin C. Bromley, Preston W. Harris, Scott J. Kenyon
Figure caption: Geometric disk model: the debris disk lays flat in the x–y plane with the z-axis normal to its surface and surrounds the host star, located at the origin. The yellow ring represents an arbitrary position that flare light had traveled to and reflected off the disk. The path of a single photon is shown by the yellow squiggle, reflecting off of the disk and toward the observer. The angle i is the inclination of the disk as seen by the observer (0°–90°, where 0° and 90° represent face-on and edge-on orientations, respectively). ϕ represents the angular position at any point around the disk and r is its corresponding radial position with r in and r out marking the minimum and maximum radial positions. θ  s  is the scattering angle for a photon reflected toward the observer. Note: in this orientation, the portion of the disk aligned with the negative y-axis would be defined as the “near side,” as it is inclined toward the observer.
Paper: Polarization of Circumstellar Debris Disk Light Echoes
Authors: Austin J. King, Benjamin C. Bromley, Preston W. Harris, Scott J. Kenyon
Figure caption: Light echo plots: in each of the above plots, the blue lines represent total intensity of the light echo, the orange lines represent light polarized in Stokes Q, and the magenta lines represent light polarized in Stokes U. The black dashed line shows the summed polarization ﹩{I}_{\mathrm{pol}}=\sqrt{{Q}^{2}+{U}^{2}}﹩. The left figure shows lightcurves for the same parameters shown in Figure 2. The right figure shows lightcurves for the same parameters shown in Figure 2 except for inclination, which has been changed to 85° to show an edge-on orientation. Both curves have had noise added on the order of a TESS flare star with 64 flare events.
Paper: Polarization of Circumstellar Debris Disk Light Echoes
Authors: Austin J. King, Benjamin C. Bromley, Preston W. Harris, Scott J. Kenyon
Figure caption: A set of model echo lightcurves with noise: these curves are calculated from the same parameters used in Figure 2, with the addition of a rotation parameter for polarization, which is set to 10°. The blue line depicts the total intensity of the echo light, while orange and lime show stokes Q and U, respectively. The black dashed line is the total polarization curve, ﹩\sqrt{{Q}^{2}+{U}^{2}}﹩. Noise was added as described in the text.
Paper: Polarization of Circumstellar Debris Disk Light Echoes
Authors: Austin J. King, Benjamin C. Bromley, Preston W. Harris, Scott J. Kenyon
Figure caption: Top left: the blue line represents artificial echo data; the red line is the echo profile predicted by best-fit parameters. Top right: inner disk radius vs. inclination. Bottom left: inner disk radius vs disk mass. Bottom right: inner disk radius vs outer disk radius. As we can see in the top right and both bottom parameter maps, the MCMC fitting process yields results that match well to the input artificial data (same disk parameters were used as those in Figure 2). Noise was added to the lightcurve on the order of the errors in TESS data for star HD 290527.
Paper: Polarization of Circumstellar Debris Disk Light Echoes
Authors: Austin J. King, Benjamin C. Bromley, Preston W. Harris, Scott J. Kenyon
Figure caption: A set of model echo lightcurves without noise: These curves are calculated from the same parameters used in Figure 2, with the addition of a rotation parameter for polarization, which is set to 10°. The blue line depicts the total intensity of the echo light, while orange and lime show stokes Q and U, respectively. The black dashed line is the total polarization curve, ﹩\sqrt{{Q}^{2}+{U}^{2}}﹩
Paper: Polarization of Circumstellar Debris Disk Light Echoes
Authors: Austin J. King, Benjamin C. Bromley, Preston W. Harris, Scott J. Kenyon
Figure caption: The two panels on the left show the Stokes Q and U fit results, respectively, at 45° inclination. The two panels on the right show the same fits for 85° inclination. The first three panels show strong curve fitting. The fourth panel does not converge as cleanly, but it also has a signal strength of about an order of magnitude weaker than the others, and is likely inconsequential due to this.
Paper: Polarization of Circumstellar Debris Disk Light Echoes
Authors: Austin J. King, Benjamin C. Bromley, Preston W. Harris, Scott J. Kenyon
Figure caption: MCMC fit results in parameter space for the unpolarized (left four panels) and polarized (right four panels) echo curves shown in the right panel of Figure 6.
Paper: Polarization of Circumstellar Debris Disk Light Echoes
Authors: Austin J. King, Benjamin C. Bromley, Preston W. Harris, Scott J. Kenyon
Figure caption: MCMC fit results in parameter space for the unpolarized (left four panels) and polarized (right four panels) echo curves shown in the left panel of Figure 6.
Paper: Confirming the Warm and Dense Sub-Saturn TIC 139270665 b with the Automated Planet Finder and Unistellar Citizen Science Network
Authors: Daniel O'Conner Peluso, Paul A. Dalba, Duncan Wright, Thomas M. Esposito, Lauren A. Sgro, Ian C. Weaver, Franck Marchis, Diana Dragomir, Steven Villanueva, Benjamin Fulton, Howard Isaacson, Arvind F. Gupta, Thomas Lee Jacobs, Daryll M. LaCourse, Robert Gagliano, Martti H. Kristiansen, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Andrew Vanderburg, Ananya Balakrishnan, Divya Bhamidipati, Marco Hovland, Serina Jain, Nathan Jay, Hanna Johnson, Aditya Kapur, Jonah Morgan, Josephine Oesterer, Richard Purev, Dean Ramos, Christopher Seo, Vibha Sriramkumar, Naina Srivastava, Astha Verma, Olivia Woo, Steven Adkinson, Keiichi Fukui, Patrice Girard, Tateki Goto, Bruno Guillet, Des Janke, Andre Katterfeld, Rachel Knight, David Koster, Ryuichi Kukita, Eric Lawson, Liouba Leroux, Niniane Leroux, Chelsey Logan, Margaret A. Loose, Nicola Meneghelli, Eric Oulevey, Bruce Parker, Stephen Price, Michael Primm, Justus Randolph, Robert Savonnet, Masao Shimizu, Petri Tikkanen, Stefan Will, Neil Yoblonsky, Wai-Chun Yue
Figure caption: Single TESS transit of TIC 139270665 b (0.645R  J ) in Sector 47 detected on 2022 January 12. Long-cadence TESS data are gray, bins of 80 minutes are red (purely for visual aid), and the best-fit EXOFASTv2 model is blue. See Section 3.1 for EXOFASTv2 details.
Paper: Confirming the Warm and Dense Sub-Saturn TIC 139270665 b with the Automated Planet Finder and Unistellar Citizen Science Network
Authors: Daniel O'Conner Peluso, Paul A. Dalba, Duncan Wright, Thomas M. Esposito, Lauren A. Sgro, Ian C. Weaver, Franck Marchis, Diana Dragomir, Steven Villanueva, Benjamin Fulton, Howard Isaacson, Arvind F. Gupta, Thomas Lee Jacobs, Daryll M. LaCourse, Robert Gagliano, Martti H. Kristiansen, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Andrew Vanderburg, Ananya Balakrishnan, Divya Bhamidipati, Marco Hovland, Serina Jain, Nathan Jay, Hanna Johnson, Aditya Kapur, Jonah Morgan, Josephine Oesterer, Richard Purev, Dean Ramos, Christopher Seo, Vibha Sriramkumar, Naina Srivastava, Astha Verma, Olivia Woo, Steven Adkinson, Keiichi Fukui, Patrice Girard, Tateki Goto, Bruno Guillet, Des Janke, Andre Katterfeld, Rachel Knight, David Koster, Ryuichi Kukita, Eric Lawson, Liouba Leroux, Niniane Leroux, Chelsey Logan, Margaret A. Loose, Nicola Meneghelli, Eric Oulevey, Bruce Parker, Stephen Price, Michael Primm, Justus Randolph, Robert Savonnet, Masao Shimizu, Petri Tikkanen, Stefan Will, Neil Yoblonsky, Wai-Chun Yue
Figure caption: Limiting magnitude Δm at the 5σ level for the nondetection of a neighboring star based on the speckle imaging from WIYN NESSI. The inset shows the speckle image at 832 nm.
Paper: A Self-consistent Data-driven Model for Determining Stellar Parameters from Optical and Near-infrared Spectra
Authors: Logan Sizemore, Diego Llanes, Marina Kounkel, Brian Hutchinson, Keivan G. Stassun, Vedant Chandra
Figure caption: The distribution of T eff and ﹩\mathrm{log}g﹩ of the pre-main-sequence stars, color coded by photometrically derived ages using Sagitta (McBride et al. 2021). The lines with white outlines show MIST isochrones (Choi et al. 2016) with ages of 6.2, 6.6, 7.0, 7.4, and 7.8 dex (from top to bottom). Note that ﹩\mathrm{log}g﹩ values independently show a strong correlation with age, and that the spectroscopic parameters are consistent with the photometric estimates. Top panel: outputs from BOSS Net. Bottom panel: outputs from APOGEE Net (Appendix B); the apparent difference at the youngest end is driven primarily by the selection function of the sources observed in each wavelength regime to date.
Paper: A Self-consistent Data-driven Model for Determining Stellar Parameters from Optical and Near-infrared Spectra
Authors: Logan Sizemore, Diego Llanes, Marina Kounkel, Brian Hutchinson, Keivan G. Stassun, Vedant Chandra
Figure caption: The distribution of T eff and ﹩\mathrm{log}g﹩ of sources targeted by various SDSS-V programs, including young stars (<30 Myr), OB stars, sources within 100 pc, members of moving groups (>30 Myr), sources in the halo with distance >2 kpc (including K giants, horizontal branch stars, RR Lyr, and metal-poor dwarfs and giants), and compact binaries.
Paper: A Self-consistent Data-driven Model for Determining Stellar Parameters from Optical and Near-infrared Spectra
Authors: Logan Sizemore, Diego Llanes, Marina Kounkel, Brian Hutchinson, Keivan G. Stassun, Vedant Chandra
Figure caption: Left: the performance of BOSS Net on the withheld test set, showing the consistency between the original labels for T eff, ﹩\mathrm{log}g﹩, and [Fe/H] vs. the resulting predictions. The x-axis shows the labels. Right: comparison between the derived parameters from BOSS and LAMOST spectra of the sames sources. The x-axis shows the BOSS measurements.
Paper: A Self-consistent Data-driven Model for Determining Stellar Parameters from Optical and Near-infrared Spectra
Authors: Logan Sizemore, Diego Llanes, Marina Kounkel, Brian Hutchinson, Keivan G. Stassun, Vedant Chandra
Figure caption: Difference between the predictions obtained for the same stars with multiple visits, divided by the uncertainties in the predictions (added in quadrature). Blue curve shows the resulting distribution of the scatter in ﹩\mathrm{log}g﹩, yellow in T eff, and red in [Fe/H].
Paper: A Self-consistent Data-driven Model for Determining Stellar Parameters from Optical and Near-infrared Spectra
Authors: Logan Sizemore, Diego Llanes, Marina Kounkel, Brian Hutchinson, Keivan G. Stassun, Vedant Chandra
Figure caption: The distribution of the derived T eff and ﹩\mathrm{log}g﹩ in the BOSS spectra, color coded by SNR.
Paper: A Self-consistent Data-driven Model for Determining Stellar Parameters from Optical and Near-infrared Spectra
Authors: Logan Sizemore, Diego Llanes, Marina Kounkel, Brian Hutchinson, Keivan G. Stassun, Vedant Chandra
Figure caption: Derived spectroscopic parameter space of white dwarfs in legacy SDSS I-IV data, color coded by the source classification from Gentile Fusillo et al. (2021).
Paper: A Self-consistent Data-driven Model for Determining Stellar Parameters from Optical and Near-infrared Spectra
Authors: Logan Sizemore, Diego Llanes, Marina Kounkel, Brian Hutchinson, Keivan G. Stassun, Vedant Chandra
Figure caption: Example BOSS spectra for stars of different T eff.
Paper: A Self-consistent Data-driven Model for Determining Stellar Parameters from Optical and Near-infrared Spectra
Authors: Logan Sizemore, Diego Llanes, Marina Kounkel, Brian Hutchinson, Keivan G. Stassun, Vedant Chandra
Figure caption: Typical uncertainties in T eff, ﹩\mathrm{log}g﹩, [Fe/H], and RV across the full parameter space.
Paper: A Self-consistent Data-driven Model for Determining Stellar Parameters from Optical and Near-infrared Spectra
Authors: Logan Sizemore, Diego Llanes, Marina Kounkel, Brian Hutchinson, Keivan G. Stassun, Vedant Chandra
Figure caption: Subsets of the different samples of the labeled data used in training.
Paper: TOI-5344 b: A Saturn-like Planet Orbiting a Super-solar Metallicity M0 Dwarf
Authors: Te Han, Paul Robertson, Shubham Kanodia, Caleb Cañas, Andrea S. J. Lin, Gumundur Stefánsson, Jessica E. Libby-Roberts, Alexander Larsen, Henry A. Kobulnicky, Suvrath Mahadevan, Chad F. Bender, William D. Cochran, Michael Endl, Mark E. Everett, Arvind F. Gupta, Samuel Halverson, Fred Hearty, Andrew Monson, Joe P. Ninan, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: TOI-5344 b (highlighted with orange circle) in the transiting GEMS parameter spaces. All 17 Transiting GEMS are color-coded respectively, and transiting giants around FGK-dwarf stars are shown in gray circles. Panel (a) shows the period–radius plane. Panel (b) shows the mass–radius plane including Jupiter and Saturn as comparisons. TOI-4201 b (Delamer et al. 2023) has a planet mass larger than 800 M ⊕ and is not shown here. Three density lines are plotted, including Saturn’s density (0.687 g cm−3). We observe that TOI-5344 b is close to Saturn in this plane. Panel (c) shows the metallicity–density plane, where we note a lack of metal-poor host stars for transiting GEMS. The two empty circles represent two systems discarded in the statistics because of poor metallicity constraints. Panel (d) shows the metallicity–metal-fraction plane, and all 17 transiting GEMS are calculated to have a metal mass fraction of more than 10% based on Thorngren et al. (2016).
Paper: TOI-5344 b: A Saturn-like Planet Orbiting a Super-solar Metallicity M0 Dwarf
Authors: Te Han, Paul Robertson, Shubham Kanodia, Caleb Cañas, Andrea S. J. Lin, Gumundur Stefánsson, Jessica E. Libby-Roberts, Alexander Larsen, Henry A. Kobulnicky, Suvrath Mahadevan, Chad F. Bender, William D. Cochran, Michael Endl, Mark E. Everett, Arvind F. Gupta, Samuel Halverson, Fred Hearty, Andrew Monson, Joe P. Ninan, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: TESS photometry of TOI-5344. Top: TESS Full-Frame Images (FFIs) for Sector 43 and Sector 44 where Gaia stars (red) and their propagated positions after 2000 years (arrows) are plotted. The aperture used by TGLC is shown in red squares; the apertures used by eleanor and QLP are shown in black dashed L shapes and circles, respectively. Note that the TGLC aperture is applied to the decontaminated image instead of the shown raw FFI. Bottom: TGLC calibrated aperture light curve of TOI-5344 for Sector 43 and Sector 44. A total of ten observed transits are marked with red dashed lines.
Paper: TOI-5344 b: A Saturn-like Planet Orbiting a Super-solar Metallicity M0 Dwarf
Authors: Te Han, Paul Robertson, Shubham Kanodia, Caleb Cañas, Andrea S. J. Lin, Gumundur Stefánsson, Jessica E. Libby-Roberts, Alexander Larsen, Henry A. Kobulnicky, Suvrath Mahadevan, Chad F. Bender, William D. Cochran, Michael Endl, Mark E. Everett, Arvind F. Gupta, Samuel Halverson, Fred Hearty, Andrew Monson, Joe P. Ninan, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: The HPF-SpecMatch spectra fit results for order index 5. Top: two plots showing the five best-fit stars (red) selected to compose the spectra. The size and transparency of these five stars and the other library stars (black) are inversely proportional to the calculated χ 2 initial value where we compare TOI-5344 spectra to the library star spectra. Larger and darker points signify a lower χ 2 initial value, implying a better fit to the target spectrum. Middle: all HPF order index 5 spectra of TOI-5344 (gray) and their best-fit composite (yellow). The highest S/N spectrum is shown in black and its best-fit composite is in red. Bottom: the residuals of the best-fit composites for all spectra (gray) and for the highest S/N spectrum (black). The featureless residuals suggest a high-quality fit.
Paper: TOI-5344 b: A Saturn-like Planet Orbiting a Super-solar Metallicity M0 Dwarf
Authors: Te Han, Paul Robertson, Shubham Kanodia, Caleb Cañas, Andrea S. J. Lin, Gumundur Stefánsson, Jessica E. Libby-Roberts, Alexander Larsen, Henry A. Kobulnicky, Suvrath Mahadevan, Chad F. Bender, William D. Cochran, Michael Endl, Mark E. Everett, Arvind F. Gupta, Samuel Halverson, Fred Hearty, Andrew Monson, Joe P. Ninan, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: The raw (gray) and 10 minute binned (black) phase-folded light curves of TESS and RBO photometry. The best joint fit model is shown in red, and the 1σ, 2σ, and 3σ confidence intervals are shown in yellow with descending intensities.
Paper: TOI-5344 b: A Saturn-like Planet Orbiting a Super-solar Metallicity M0 Dwarf
Authors: Te Han, Paul Robertson, Shubham Kanodia, Caleb Cañas, Andrea S. J. Lin, Gumundur Stefánsson, Jessica E. Libby-Roberts, Alexander Larsen, Henry A. Kobulnicky, Suvrath Mahadevan, Chad F. Bender, William D. Cochran, Michael Endl, Mark E. Everett, Arvind F. Gupta, Samuel Halverson, Fred Hearty, Andrew Monson, Joe P. Ninan, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: SED of TOI-5344 showing the broadband photometric measurements from Table 2 in red (the x-error bar is the bandpass width) and the derived MIST model fluxes (as blue circles). A NextGen BT-SETTL spectrum (Allard et al. 2012) is overlaid for reference in gray (a smoothed version in black); the model spectrum is not used when fitting the SED.
Paper: TOI-5344 b: A Saturn-like Planet Orbiting a Super-solar Metallicity M0 Dwarf
Authors: Te Han, Paul Robertson, Shubham Kanodia, Caleb Cañas, Andrea S. J. Lin, Gumundur Stefánsson, Jessica E. Libby-Roberts, Alexander Larsen, Henry A. Kobulnicky, Suvrath Mahadevan, Chad F. Bender, William D. Cochran, Michael Endl, Mark E. Everett, Arvind F. Gupta, Samuel Halverson, Fred Hearty, Andrew Monson, Joe P. Ninan, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: The ZTF zg- and zr-band photometries and their GLS periodograms of TOI-5344. Gray points are discarded in the analysis since they have low-quality flags. Despite several peaks reaching ∼1% FAP, their significance is limited by the small sample size.
Paper: TOI-5344 b: A Saturn-like Planet Orbiting a Super-solar Metallicity M0 Dwarf
Authors: Te Han, Paul Robertson, Shubham Kanodia, Caleb Cañas, Andrea S. J. Lin, Gumundur Stefánsson, Jessica E. Libby-Roberts, Alexander Larsen, Henry A. Kobulnicky, Suvrath Mahadevan, Chad F. Bender, William D. Cochran, Michael Endl, Mark E. Everett, Arvind F. Gupta, Samuel Halverson, Fred Hearty, Andrew Monson, Joe P. Ninan, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: NESSI 5σ contrast curve of TOI-5344 in the Sloan ﹩z^{\prime} ﹩ filter (black) with the reconstructed speckle image shown on top. The per-pixel magnitude difference is plotted in blue circles. No bright companions with ﹩{\rm{\Delta }}z^{\prime} \lt ﹩ 3.0 are observed between 0.″2 and 1.″2 of the target.
Paper: TOI-5344 b: A Saturn-like Planet Orbiting a Super-solar Metallicity M0 Dwarf
Authors: Te Han, Paul Robertson, Shubham Kanodia, Caleb Cañas, Andrea S. J. Lin, Gumundur Stefánsson, Jessica E. Libby-Roberts, Alexander Larsen, Henry A. Kobulnicky, Suvrath Mahadevan, Chad F. Bender, William D. Cochran, Michael Endl, Mark E. Everett, Arvind F. Gupta, Samuel Halverson, Fred Hearty, Andrew Monson, Joe P. Ninan, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: The binned HPF RV measurements of TOI-5344. Left: time series of HPF RV binned by each night (black). Right: phase-folded HPF RV (black). The best joint fit model is shown in red, and the 1σ, 2σ, and 3σ confidence intervals are shown in yellow with descending intensities.
Paper: TOI-5344 b: A Saturn-like Planet Orbiting a Super-solar Metallicity M0 Dwarf
Authors: Te Han, Paul Robertson, Shubham Kanodia, Caleb Cañas, Andrea S. J. Lin, Gumundur Stefánsson, Jessica E. Libby-Roberts, Alexander Larsen, Henry A. Kobulnicky, Suvrath Mahadevan, Chad F. Bender, William D. Cochran, Michael Endl, Mark E. Everett, Arvind F. Gupta, Samuel Halverson, Fred Hearty, Andrew Monson, Joe P. Ninan, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: The ASAS-SN V band photometry and its GLS periodogram of TOI-5344. The FAP is shown in dashed lines. No significant stellar variation signal is observed in the GLS.
Paper: TOI-5344 b: A Saturn-like Planet Orbiting a Super-solar Metallicity M0 Dwarf
Authors: Te Han, Paul Robertson, Shubham Kanodia, Caleb Cañas, Andrea S. J. Lin, Gumundur Stefánsson, Jessica E. Libby-Roberts, Alexander Larsen, Henry A. Kobulnicky, Suvrath Mahadevan, Chad F. Bender, William D. Cochran, Michael Endl, Mark E. Everett, Arvind F. Gupta, Samuel Halverson, Fred Hearty, Andrew Monson, Joe P. Ninan, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: The planet-metallicity correlation of 15 transiting GEMS. TOI-5205 b and NGTS-1 b are excluded given their ambiguously estimated metallicities. Top: we compare transiting giants (solid circle) and transiting nongiants (empty circle) around M-dwarf stars in the metallicity–mass plane. The markers are color-coded with the host mass. Bottom: histogram of the metallicity distribution. We observe the giant hosts to be more metal-rich than the nongiant hosts. The median metallicity for each population is labeled as vertical (dashed) lines.
Paper: Spectroscopic Distance, Mass, and Age Estimations for APOGEE DR17
Authors: Alexander Stone-Martinez, Jon A. Holtzman, Julie Imig, Christian Nitschelm, Keivan G. Stassun, Joel R. Brownstein
Figure caption: DistMass and Mackereth et al. (2019) age histograms for stars in clusters. The DistMass ages used here are from the corrected Mosser seismology.
Paper: Spectroscopic Distance, Mass, and Age Estimations for APOGEE DR17
Authors: Alexander Stone-Martinez, Jon A. Holtzman, Julie Imig, Christian Nitschelm, Keivan G. Stassun, Joel R. Brownstein
Figure caption: [C/N] vs. estimated age binned by [Fe/H] and color coded by log g. Ages are from the model trained on the corrected Mosser seismology. Red dashed line shows the [C/N] age calibration from Spoo et al. (2022).
Paper: Spectroscopic Distance, Mass, and Age Estimations for APOGEE DR17
Authors: Alexander Stone-Martinez, Jon A. Holtzman, Julie Imig, Christian Nitschelm, Keivan G. Stassun, Joel R. Brownstein
Figure caption: Kiel diagram showing stars in NGC 7789 color coded by DistMass. The DistMass ages used here are from the corrected Mosser seismology.
Paper: Spectroscopic Distance, Mass, and Age Estimations for APOGEE DR17
Authors: Alexander Stone-Martinez, Jon A. Holtzman, Julie Imig, Christian Nitschelm, Keivan G. Stassun, Joel R. Brownstein
Figure caption: DistMass ages vs. Mackereth et al. (2019) ages for stars within the bounded training region for the mass model.
Paper: The Spatial Distribution of Type Ia Supernovae within Host Galaxies
Authors: Christopher Pritchet, Karun Thanjavur, Connor Bottrell, Yan Gao
Figure caption: Cumulative distribution of SNe Ia plotted against L inc/L acc, for disk-dominated galaxies (B/T < 0.2) in the primary sample. The diagonal line is a 1:1 relation, and it corresponds to the case where the SN rate follows light. Blue solid line: L inc/L acc is calculated using the fitted disk light. (a) Comparison with L inc/L acc calculated using fitted bulge light (red line). (b) Using only SNe Ia outside the host galaxy core (R > 0.″75, 0.1 < L inc/L acc < 0.9). (c) Sako class SNIa objects (solid line) compared with zSNIa and pSNIa objects (dashed line). (d) ﹩{r}_{\mathrm{SN}}^{\max }\lt 22﹩ (solid line), 21.5 (dashed line), and 21 (dotted–dashed line). (e) Effects of rescaling disk scale lengths β. Solid line: fitted β; dashed line: β × 1.1; dotted line: β × 0.83. (f) Effects of modifying disk Sérsic index n: red indicates n = 0.5, blue is for n = 1, green is for n = 1.5​​​​​​,  and turquoise is for n = 2.