adsabs/AstroCLIMB huggingface dataset:
Paper: Coma Abundances of Volatiles at Small Heliocentric Distances: Compositional Measurements of Long-period Comet C/2020 S3 (Erasmus)
Authors: Chemeda Ejeta, Erika Gibb, Nathan Roth, Michael A. DiSanti, Neil Dello Russo, Mohammad Saki, Adam J. McKay, Hideyo Kawakita, Younas Khan, Boncho P. Bonev, Ronald J. Vervack, Michael R. Combi
Figure caption: Simultaneously measured spatial profiles on 2020 November 29 (panels (a), (c), and (e)) and December 1 (panels (b), (d), and (f)) using the Lp1 setting. The slit was oriented along the Sun–comet direction of ∼272° and a favorable phase angle of ∼61° on both dates. To ensure uniform spatial registration for all targeted molecular species, the peak of the continuum profile (black dashed line) is taken to define the nucleus position. The vertical error bars indicated for each volatile species represent ±1σ stochastic noise.
Paper: Coma Abundances of Volatiles at Small Heliocentric Distances: Compositional Measurements of Long-period Comet C/2020 S3 (Erasmus)
Authors: Chemeda Ejeta, Erika Gibb, Nathan Roth, Michael A. DiSanti, Neil Dello Russo, Mohammad Saki, Adam J. McKay, Hideyo Kawakita, Younas Khan, Boncho P. Bonev, Ronald J. Vervack, Michael R. Combi
Figure caption: Same as Figure 2 but for H2O, HCN, OH, and NH2 measured on 2020 November 29 (panels (a) and (c)) using the L-custom setting and on December 1 using the L-custom setting (panels (b) and (d)) and the M2 setting (panels (e) and (f)).
Paper: Coma Abundances of Volatiles at Small Heliocentric Distances: Compositional Measurements of Long-period Comet C/2020 S3 (Erasmus)
Authors: Chemeda Ejeta, Erika Gibb, Nathan Roth, Michael A. DiSanti, Neil Dello Russo, Mohammad Saki, Adam J. McKay, Hideyo Kawakita, Younas Khan, Boncho P. Bonev, Ronald J. Vervack, Michael R. Combi
Figure caption: The abundance of primary volatiles in S3 (filled blue circles) compared with weighted average abundance ratios in OCC populations observed in the NIR (at R  h  ≤ 0.80 au and R  h  > 0.80 au).
Paper: Coma Abundances of Volatiles at Small Heliocentric Distances: Compositional Measurements of Long-period Comet C/2020 S3 (Erasmus)
Authors: Chemeda Ejeta, Erika Gibb, Nathan Roth, Michael A. DiSanti, Neil Dello Russo, Mohammad Saki, Adam J. McKay, Hideyo Kawakita, Younas Khan, Boncho P. Bonev, Ronald J. Vervack, Michael R. Combi
Figure caption: Sample spectra and best-fit fluorescent models of molecular emissions in Erasmus during the observations on 2020 December 1 and November 29. The observed spectra (black) are superimposed with the telluric model (yellow). The total fluorescence model overplotted on the telluric subtracted spectra is shown in red. Individual fluorescence emission models (color-coded by species) are shown below the observed spectrum in each panel. The bottom trace indicates the residual spectrum (after subtracting modeled continuum and total molecular contributions), with the superimposed ±1σ stochastic noise envelope shown in orange.
Paper: High-resolution Transmission Spectroscopy of Ultrahot Jupiter WASP–33b with NEID
Authors: Yuanheng Yang, 远恒 杨, Guo Chen, 果 陈, Songhu Wang, Fei Yan, 飞 严
Figure caption: Transmission spectral matrix, CLV+RM model, and one-dimensional transmission spectrum for the Hα line observed with NEID. First row: the transmission spectral matrix before correction for the CLV and RM effects in the stellar rest frame. The horizontal black dashed lines indicate the first and fourth contacts of the transit (i.e., the beginning and end of the transit). The slanted green dashed lines mark the RV shift due to the orbital motion of the planet. The RV regions around −158 km s−1 (i.e., ∼6559.35 Å) are masked due to invalid values (NaN). Second row: the model for the CLV and RM effects. Third row: the observed transmission spectral matrix after correction for the CLV and RM effects. The color bar is indexed to the residual flux. Fourth row: phase-folded one-dimensional transmission spectrum. The CLV and RM effects have been corrected. The y-axis shows the relative residual flux minus one as a percentage. The gray line shows the unbinned observed transmission spectrum. The black circles with error bars show the spectrum binned every 10 points (∼0.2 Å). The blue line shows the best-fit GP model. Fifth row: transmission spectrum after removal of systematic noise using the GP method. The red line shows the best-fit Gaussian line profile. The purple and cyan lines are hydrostatic models of Hα with temperatures of 2710 and 10,000 K, respectively, including planetary rotation.
Paper: High-resolution Transmission Spectroscopy of Ultrahot Jupiter WASP–33b with NEID
Authors: Yuanheng Yang, 远恒 杨, Guo Chen, 果 陈, Songhu Wang, Fei Yan, 飞 严
Figure caption: Cross-correlation functions of Ca II averaged over the five nights of observation. First row: the CCF map of Ca II after correction for CLV and RM effects. The horizontal blue dashed lines represent the first and fourth contacts of the transit. The purple dashed line shows the orbital motion of the planet. Second row: K  p  map. The magenta pentagram marks the S/N peak. The expected values are indicated by the dashed lines. The color bar represents the value of the S/N. Third row: the one-dimensional CCF (the pink dashed line) corresponding to the K  p  value at S/N peak. The vertical gray dashed line indicates Δυ = 0.
Paper: High-resolution Transmission Spectroscopy of Ultrahot Jupiter WASP–33b with NEID
Authors: Yuanheng Yang, 远恒 杨, Guo Chen, 果 陈, Songhu Wang, Fei Yan, 飞 严
Figure caption: Cross-correlation functions of TiO, Ti I, V I, and Fe I without correction for CLV and RM effects. Each row of panels represents one species. The format of each panel from left to right corresponds to each row from top to bottom of Figure 5, respectively. The name of each species is given in each top left panel.
Paper: High-resolution Transmission Spectroscopy of Ultrahot Jupiter WASP–33b with NEID
Authors: Yuanheng Yang, 远恒 杨, Guo Chen, 果 陈, Songhu Wang, Fei Yan, 飞 严
Figure caption: As in Figure 3, but for the Ca II IRT lines, including Ca II IRT ( λ 8498), Ca II IRT ( λ 8542), and Ca II IRT ( λ 8662). The name of each line is given in the title of each top panel.
Paper: High-resolution Transmission Spectroscopy of Ultrahot Jupiter WASP–33b with NEID
Authors: Yuanheng Yang, 远恒 杨, Guo Chen, 果 陈, Songhu Wang, Fei Yan, 飞 严
Figure caption: Transmission spectral matrix of the Hα absorption in the planetary rest frame. The horizontal white lines indicate the first and fourth contacts of the transit. The vertical black dashed lines represent the values of the planetary RV at the first and fourth contacts of the transit. The slanted cyan dashed lines show the RV trace of the planet moved to bracket the pretransit absorption feature. The color bar indicates the value of residual flux.
Paper: High-resolution Transmission Spectroscopy of Ultrahot Jupiter WASP–33b with NEID
Authors: Yuanheng Yang, 远恒 杨, Guo Chen, 果 陈, Songhu Wang, Fei Yan, 飞 严
Figure caption: The transmission spectral matrices and one-dimensional transmission spectra for the Hβ and Hγ lines observed by NEID. Each column corresponds to an individual line. The first row to the fifth row are similar to the forms of Figure 1.
Paper: A Phenomenon Resembling Early Superhumps in a New SU UMa-type Dwarf Nova with a 2 hr Orbital Period
Authors: Rebecca S. Boyle, Colin Littlefield, Peter Garnavich, Ryan Ridden-Harper, Paula Szkody, Patricia Boyd, Krista Lynne Smith
Figure caption: Low-amplitude oscillations appear during the postsuperoutburst phase just before the rebrightening. These ∼0.4 mag oscillations are reminiscent of the “mini-rebrightenings” recorded in the Kepler data of V585 Lyr (Kato & Osaki 2013b) and the TESS data of V844 Her (Kato 2022a).
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: (a) Kiel diagram of APOKASC stars <1.6 M ⊙ with −0.05 < [Fe/H] < 0.05 and color coded by asteroseismic mass. (b) Kiel diagram showing the subgiant and red-giant branch for stars with −0.025 < [Fe/H] < 0.025 color coded by [C/N].
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: Mass distribution histograms for the six mass data sets in two distance bins. Left columns show uncorrected masses, and the right columns show the corrected masses. The histograms are split into a low log g bin (blue) and high log g bin (orange).
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: (a) [C/N] as a function of [Fe/H] for subgiant stars. Slope shows the [Fe/H]–birth [C/N] relation. (b) [C/N] as a function of [Fe/H] for RGB stars. Star selection was limited to a narrow mass range in order to highlight the [C/N]–[Fe/H] relation.
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: Histograms of [C/N] vs. Galactocentric radius for pre-dredge-up subgiants binned by [Fe/H]. The location of the distribution is different for each [Fe/H] bin, due to the [C/N]–[Fe/H] relation. There is no apparent trend in the [C/N]–[Fe/H] relation over the examined range. However, the range we can examine the [C/N] variation is limited to 2 kpc by the lower luminosity of subgiants.
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: Density plots showing the kiel and metallicity diagrams and for the full data set ((a) and (c)) and for the training set after the 10% mass uncertainty cutoff ((b) and (d)). Brighter and colored regions contain a higher density of stars.
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: Histograms showing the distribution of masses predicted by the six models. The left column shows uncorrected masses, and the right column shows the corrected masses. The histograms are split into a low log g bin (blue) and high log g bin (orange).
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]–mass relation for the ML model predictions trained on all six seismologies/corrections. Color coded by [Fe/H] and binned in log g intervals of 0.5.
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]–mass relation binned by log g. The masses shown here are the corrected Mosser masses from APOKASC. Each group of 10 points has an error bar for mass.
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. log g binned by asteroseismic mass. Best-fit line shows the positive trend in [C/N].
Paper: Metallicity Distribution in the LMC and the SMC Based on the Tip-RGB Colors
Authors: Ying Li, 颖 李, Biwei Jiang, 碧沩 姜, Yi Ren, 逸 任
Figure caption: The example to show the PN method to determine the TRGB position by the binNum4 in the LMC. (a) The color–magnitude diagram of the member stars. The red box indicates the position of the TRGB with the error bars fitted in Figure 5 and the values are displayed in the upper left corner. (b) PDF of the member stars, where the red line shows the K 0 vs. (J − K)0 relation of the ridge line. (c) The black dashed–dotted line shows the PDFridge vs. (J − K)0 relation, the black solid line shows the PDFridge vs. K 0 relation. The red dashed–dotted lines on the right and left mark the bright and faint ends of TRGB, respectively, and the middle one for the true position of TRGB; (d) The 3D density distribution of member stars.
Paper: Metallicity Distribution in the LMC and the SMC Based on the Tip-RGB Colors
Authors: Ying Li, 颖 李, Biwei Jiang, 碧沩 姜, Yi Ren, 逸 任
Figure caption: The (J − K)0 vs. K 0 diagram of the SMC and the LMC member stars. The dashed triangle indicates the area used to determine the color and brightness of TRGB, and the red box denotes the position of the TRGB in either galaxy.
Paper: Metallicity Distribution in the LMC and the SMC Based on the Tip-RGB Colors
Authors: Ying Li, 颖 李, Biwei Jiang, 碧沩 姜, Yi Ren, 逸 任
Figure caption: Distribution of the 2000 Bootstrap resampling results in (J − K)0 and K 0 for the bin in Figure 4, and the results from Gaussian fitting are displayed.
Paper: Metallicity Distribution in the LMC and the SMC Based on the Tip-RGB Colors
Authors: Ying Li, 颖 李, Biwei Jiang, 碧沩 姜, Yi Ren, 逸 任
Figure caption: The Voronoi bins for the LMC. The smallest squares represent the initial bin unit and the irregular polygon including multiple bin units of the same color denotes one final bin with about 300 stars by the Voronoi binning method. In total, there are 154 bins.
Paper: Metallicity Distribution in the LMC and the SMC Based on the Tip-RGB Colors
Authors: Ying Li, 颖 李, Biwei Jiang, 碧沩 姜, Yi Ren, 逸 任
Figure caption: The same as Figure 2, but for the SMC and the number of stars in one bin is about 120. In total, there are 70 bins.
Paper: Metallicity Distribution in the LMC and the SMC Based on the Tip-RGB Colors
Authors: Ying Li, 颖 李, Biwei Jiang, 碧沩 姜, Yi Ren, 逸 任
Figure caption: The (J − K)0 and K 0 distribution in the LMC. The contour denotes the density of the member stars. The black asterisk marks the center of the LMC (de Vaucouleurs et al. 1976).
Paper: Metallicity Distribution in the LMC and the SMC Based on the Tip-RGB Colors
Authors: Ying Li, 颖 李, Biwei Jiang, 碧沩 姜, Yi Ren, 逸 任
Figure caption: The same as Figure 6, but for the SMC.
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: Maximum-likelihood model from the MCMC plotted over only the Chabot Space & Science Center’s Galaxy Explorer High School students’ Unistellar data sets, on UTC 2023 February 19. Initial variability likely stems from partly cloudy weather, which transitioned to clearer skies after a data gap of ∼1.2 hr. The subsequent flat light curve, a result of combined observations from nine eVscopes, has a high S/N and indicates the absence of any ingress or egress by TIC 139270665 b. The increased variability at the very end of the light curve can be attributed to the target’s high airmass at the end of the observation. The blue squares in the plot represent the weighted averages of fluxes and residuals, respectively, within each time bin of 0.01 days. On average, each blue square is derived from approximately 43.6 individual data points.
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: Marginalized posterior distributions from the MCMC that searched for a transit signal in the Unistellar eVscope light-curve data. Only the planet’s period, radius (rp), and date of mid-transit (t0) are shown (offsets are excluded). The period distribution is multimodal, with one period range strongly preferred. Despite the seemingly well-constrained parameters, a Bayesian information criterion test showed that these transit models did not provide significantly better fits to the data than a flat model.
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: Top: normalized and phase-folded light curve using 10 data sets from our Unistellar citizen scientists that encompassed the transit window defined by the MCMC’s secondary (i.e., less preferred) set of solutions from Figure 11. This secondary solution corresponds to a period of P = 23.620 days. Bottom: residuals from this secondary model. Unistellar data are labeled by observation date followed by an abbreviated serial number in the format “YYYYMMDD_abc,” where “abc” denotes the serial number. The blue squares represent the weighted means of the individual relative fluxes within each phase bin. On average, each blue square represents about 20.5 data points.
Paper: Technosignatures Longevity and Lindy's Law
Authors: Amedeo Balbi, Claudio Grimaldi
Figure caption: PDF of technoemission longevity L (top row) and starting time t of emissions (bottom row) calculated under the assumption that the unconditional PDF of t is uniform over the interval [1, 1010] yr. Panels (a)–(c) show the conditional, Equation (9) and unconditional, Equation (8), PDFs of L for three values of the exponent α, whereas panel (d) shows the corresponding values of L* such that L ≤ L* with 95% probability. Panels (e) and (f) show the PDF of t calculated numerically for different values of α and (e) for R  o  large enough to encompass the entire galaxy and (f) for R  o  = 100 ly. Panel (g) shows the values of t* such that t ≤ t* with 95 % probability calculated for different values of R  o .
Paper: Technosignatures Longevity and Lindy's Law
Authors: Amedeo Balbi, Claudio Grimaldi
Figure caption: PDFs of L (top row) and t of (bottom row) calculated numerically using an unconditional distribution of emission starting times that is log-uniform over the interval [1, 1010] yr. In panels (a) and (b) the conditional PDF of L (solid lines) is plotted different α and R  o  values. Panel (c) shows the resulting L* for several observation radii R  o . Panels (d) and (e) show the PDF of t calculated numerically for different values of α and (d) for R  o  large and (e) for R  o  = 100 ly. Panel (f) shows the values of t* calculated for different values of R  o .
Paper: Technosignatures Longevity and Lindy's Law
Authors: Amedeo Balbi, Claudio Grimaldi
Figure caption: Number of technoemissions ever generated over the history of the Galaxy as a function of the longevity exponent α. ﹩\bar{N}﹩ is calculated from Equation (11) using a uniform in t (a) and a log-uniform in t (b) probability disribution of the time of occurrence of technoemissions. Results are shown for different values of the sampled radius R  o .
Paper: Technosignatures Longevity and Lindy's Law
Authors: Amedeo Balbi, Claudio Grimaldi
Figure caption: Technoemission rates calculated from ﹩{\rm{\Gamma }}(t)=\bar{N}{\rho }_{t}(t)﹩ for uniform, log-uniform, and normally distributed PDFs of t. For all cases, ﹩\bar{N}﹩ is calculated for the entire galaxy and for α = 3.
Paper: Metallicity Distribution in the LMC and the SMC Based on the Tip-RGB Colors
Authors: Ying Li, 颖 李, Biwei Jiang, 碧沩 姜, Yi Ren, 逸 任
Figure caption: The variation of the metallicity with the distance from the galactic center in the LMC. The color codes the four directions. The slope of linear fitting for [M/H] and distance is shown in the upper right corner, which is compared with the literatures.
Paper: Metallicity Distribution in the LMC and the SMC Based on the Tip-RGB Colors
Authors: Ying Li, 颖 李, Biwei Jiang, 碧沩 姜, Yi Ren, 逸 任
Figure caption: The same as Figure 8, but for the SMC.
Paper: The Spatial Distribution of Type Ia Supernovae within Host Galaxies
Authors: Christopher Pritchet, Karun Thanjavur, Connor Bottrell, Yan Gao
Figure caption:  L inc/L acc ratio for bulge (left) and disk (right) fits with SN masking vs. no SN masking. Black: ﹩{\rm{\Delta }}{\theta }_{\mathrm{SN}}\gt 0\buildrel{\prime\prime}\over{.} 75﹩; red: ﹩{\rm{\Delta }}{\theta }_{\mathrm{SN}}\lt 0\buildrel{\prime\prime}\over{.} 75﹩.
Paper: Polarization of Circumstellar Debris Disk Light Echoes
Authors: Austin J. King, Benjamin C. Bromley, Preston W. Harris, Scott J. Kenyon
Figure caption: An artificial light echo produced by a model disk with parameters R in = 50 au, R out = 55 au, i = 45°, and M disk = 0.1 M ⊕, resulting from a flare at time t = 0 s. The amplitude of the flare itself is 25 times brighter than the flux observed at t = 100 s Noise was added on the order of the errors in TESS data for star HD 290527.