adsabs/AstroCLIMB huggingface dataset:
Paper: What’s the Difference? The Potential for Convolutional Neural Networks for Transient Detection without Template Subtraction
Authors: Tatiana Acero-Cuellar, Federica Bianco, Gregory Dobler, Masao Sako, Helen Qu
Figure caption: Transients (srch–tmpl) and their respective saliency maps for the noDIA model FNs (astrophysical sources classified as bogus). In all cases but row 5, it is not clear why the classification fails. In row 5, another source dominates the image scaling (and preprocessing), reducing the visibility of the transient (that is completely missed by human inspection). We remind the reader that the real transients in this data set are implanted SNe onto real DES images. Important pixels are found everywhere in the image, as the CNN learns how to compare the diff and tmpl by taking a synoptic look at the properties of each image component.
Paper: What’s the Difference? The Potential for Convolutional Neural Networks for Transient Detection without Template Subtraction
Authors: Tatiana Acero-Cuellar, Federica Bianco, Gregory Dobler, Masao Sako, Helen Qu
Figure caption: Visual inspection of some objects originally labeled as bogus that were classified as real for DIA-based or noDIA.
Paper: Characterizing a World Within the Hot-Neptune Desert: Transit Observations of LTT 9779 b with the Hubble Space Telescope/WFC3
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Andrew Allan, Patrick Behr, Simone R. Hagey, Michael D. Himes, Sushuang Ma, Keivan G. Stassun, Luis Thomas, Alexandra Thompson, Aaron Boley, Luke Booth, Jeroen Bouwman, Kevin France, Nataliea Lowson, Annabella Meech, Caprice L. Phillips, Aline A. Vidotto, Kai Hou Yip, Michelle Bieger, Amélie Gressier, Estelle Janin, Ing-Guey Jiang, Pietro Leonardi, Subhajit Sarkar, Nour Skaf, Jake Taylor, Ming Yang, Derek Ward-Thompson
Figure caption: White light-curve fits for the HST WFC3 G102 (left) and G141 (right) data of LTT 9779 b. In each case, the top plot shows the raw light curve (top panel), corrected light curve and best-fit model (second panel), the residuals having removed the best-fit model (third panel), and the AC function (bottom panel). The lower graphic is a corner plot for the fit. As with the majority of HST data sets, there is a correlation between the white light-curve depth and the parameters for the systematics (Equation (1)), thereby indicating that achieving absolute transit depths is difficult with these data. For the data studied here, the G141 data show the highest correlation. Nevertheless, no major offset in the transit depth was found between the two visits.
Paper: Characterizing a World Within the Hot-Neptune Desert: Transit Observations of LTT 9779 b with the Hubble Space Telescope/WFC3
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Andrew Allan, Patrick Behr, Simone R. Hagey, Michael D. Himes, Sushuang Ma, Keivan G. Stassun, Luis Thomas, Alexandra Thompson, Aaron Boley, Luke Booth, Jeroen Bouwman, Kevin France, Nataliea Lowson, Annabella Meech, Caprice L. Phillips, Aline A. Vidotto, Kai Hou Yip, Michelle Bieger, Amélie Gressier, Estelle Janin, Ing-Guey Jiang, Pietro Leonardi, Subhajit Sarkar, Nour Skaf, Jake Taylor, Ming Yang, Derek Ward-Thompson
Figure caption: Spectral light curves fitted with Iraclis for the G102 (left) and G141 (right) observations of LTT 9779 b where, for clarity, an offset has been applied. Each plot shows the detrended spectral light curves with the best-fit model plotted (left) as well as the residuals from the fitting (right). The values for the reduced chi-squared (﹩{\bar{\chi }}^{2}﹩), the standard deviation of the residuals with respect to the photon noise (﹩\bar{\sigma }﹩), and the autocorrelation (AC) function are also shown.
Paper: Characterizing a World Within the Hot-Neptune Desert: Transit Observations of LTT 9779 b with the Hubble Space Telescope/WFC3
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Andrew Allan, Patrick Behr, Simone R. Hagey, Michael D. Himes, Sushuang Ma, Keivan G. Stassun, Luis Thomas, Alexandra Thompson, Aaron Boley, Luke Booth, Jeroen Bouwman, Kevin France, Nataliea Lowson, Annabella Meech, Caprice L. Phillips, Aline A. Vidotto, Kai Hou Yip, Michelle Bieger, Amélie Gressier, Estelle Janin, Ing-Guey Jiang, Pietro Leonardi, Subhajit Sarkar, Nour Skaf, Jake Taylor, Ming Yang, Derek Ward-Thompson
Figure caption: LTT 9779 b in context with the known population of transiting planets. In the period–mass and period–radius spaces, LTT 9779 b occupies a region which is sparsely populated. The majority of other planets on such a short orbital period are either stripped rocky cores or Jupiter-sized worlds.
Paper: Characterizing a World Within the Hot-Neptune Desert: Transit Observations of LTT 9779 b with the Hubble Space Telescope/WFC3
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Andrew Allan, Patrick Behr, Simone R. Hagey, Michael D. Himes, Sushuang Ma, Keivan G. Stassun, Luis Thomas, Alexandra Thompson, Aaron Boley, Luke Booth, Jeroen Bouwman, Kevin France, Nataliea Lowson, Annabella Meech, Caprice L. Phillips, Aline A. Vidotto, Kai Hou Yip, Michelle Bieger, Amélie Gressier, Estelle Janin, Ing-Guey Jiang, Pietro Leonardi, Subhajit Sarkar, Nour Skaf, Jake Taylor, Ming Yang, Derek Ward-Thompson
Figure caption: Raw images from the G102 (top) and G141 (bottom) observation sequences. In each case, the image illustrates the second forward scan of the second orbit, which is the first data set used in this analysis. For each panel, the left image shows the final read while the middle image displays a nondestructive read. The right image shows the flux levels once the nondestructive read is subtracted. The regions of negative flux highlight the persistence effect for these data sets. The color scale for the right images differ from the others in this figure to highlight this negative region.
Paper: Characterizing a World Within the Hot-Neptune Desert: Transit Observations of LTT 9779 b with the Hubble Space Telescope/WFC3
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Andrew Allan, Patrick Behr, Simone R. Hagey, Michael D. Himes, Sushuang Ma, Keivan G. Stassun, Luis Thomas, Alexandra Thompson, Aaron Boley, Luke Booth, Jeroen Bouwman, Kevin France, Nataliea Lowson, Annabella Meech, Caprice L. Phillips, Aline A. Vidotto, Kai Hou Yip, Michelle Bieger, Amélie Gressier, Estelle Janin, Ing-Guey Jiang, Pietro Leonardi, Subhajit Sarkar, Nour Skaf, Jake Taylor, Ming Yang, Derek Ward-Thompson
Figure caption: Retrieved molecular abundances from free chemistry (orange) and chemical equilibrium (purple) retrievals. Our free chemistry retrievals suggest the presence of H2O, CO2, and FeH. They also place upper limits on the abundances of TiO and VO but could not constrain CO or e-. The preferred abundance of CO2 is very different between the models, as is the H2O abundance in the lower atmosphere. The retrieved temperature profiles also slightly differ, but are generally within 1σ.
Paper: Characterizing a World Within the Hot-Neptune Desert: Transit Observations of LTT 9779 b with the Hubble Space Telescope/WFC3
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Andrew Allan, Patrick Behr, Simone R. Hagey, Michael D. Himes, Sushuang Ma, Keivan G. Stassun, Luis Thomas, Alexandra Thompson, Aaron Boley, Luke Booth, Jeroen Bouwman, Kevin France, Nataliea Lowson, Annabella Meech, Caprice L. Phillips, Aline A. Vidotto, Kai Hou Yip, Michelle Bieger, Amélie Gressier, Estelle Janin, Ing-Guey Jiang, Pietro Leonardi, Subhajit Sarkar, Nour Skaf, Jake Taylor, Ming Yang, Derek Ward-Thompson
Figure caption: Shifts in the position of the spectrum on the detector in the spectral (x) and spatial (y) directions for the G102 (top) and G141 (bottom) visits. In both cases, the pointing across the visit was excellent.
Paper: Characterizing a World Within the Hot-Neptune Desert: Transit Observations of LTT 9779 b with the Hubble Space Telescope/WFC3
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Andrew Allan, Patrick Behr, Simone R. Hagey, Michael D. Himes, Sushuang Ma, Keivan G. Stassun, Luis Thomas, Alexandra Thompson, Aaron Boley, Luke Booth, Jeroen Bouwman, Kevin France, Nataliea Lowson, Annabella Meech, Caprice L. Phillips, Aline A. Vidotto, Kai Hou Yip, Michelle Bieger, Amélie Gressier, Estelle Janin, Ing-Guey Jiang, Pietro Leonardi, Subhajit Sarkar, Nour Skaf, Jake Taylor, Ming Yang, Derek Ward-Thompson
Figure caption: Probability distributions for the C/O (top) and atmospheric metallicity (log10(Z), bottom) from the different chemical equilibrium retrievals conducted here. The constraints placed on these properties are poor in each case, but all three prefer solutions with very low atmospheric metallicities.
Paper: Characterizing a World Within the Hot-Neptune Desert: Transit Observations of LTT 9779 b with the Hubble Space Telescope/WFC3
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Andrew Allan, Patrick Behr, Simone R. Hagey, Michael D. Himes, Sushuang Ma, Keivan G. Stassun, Luis Thomas, Alexandra Thompson, Aaron Boley, Luke Booth, Jeroen Bouwman, Kevin France, Nataliea Lowson, Annabella Meech, Caprice L. Phillips, Aline A. Vidotto, Kai Hou Yip, Michelle Bieger, Amélie Gressier, Estelle Janin, Ing-Guey Jiang, Pietro Leonardi, Subhajit Sarkar, Nour Skaf, Jake Taylor, Ming Yang, Derek Ward-Thompson
Figure caption: The obtained spectrum from HST WFC3 G102 and G141. Overplotted are the preferred free chemistry (orange) and chemical equilibrium (purple) models. Based on the Bayesian evidence, the free chemistry model is preferred by 2.4σ.
Paper: Characterizing a World Within the Hot-Neptune Desert: Transit Observations of LTT 9779 b with the Hubble Space Telescope/WFC3
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Andrew Allan, Patrick Behr, Simone R. Hagey, Michael D. Himes, Sushuang Ma, Keivan G. Stassun, Luis Thomas, Alexandra Thompson, Aaron Boley, Luke Booth, Jeroen Bouwman, Kevin France, Nataliea Lowson, Annabella Meech, Caprice L. Phillips, Aline A. Vidotto, Kai Hou Yip, Michelle Bieger, Amélie Gressier, Estelle Janin, Ing-Guey Jiang, Pietro Leonardi, Subhajit Sarkar, Nour Skaf, Jake Taylor, Ming Yang, Derek Ward-Thompson
Figure caption: Spectrum from the chemical equilibrium retrieval which included an offset for the HST WFC3 G141 data. The retrieval preferred to reduce the depth of the G141 data by 60 ppm but the solution is not preferred over a retrieval without an offset.
Paper: Clustering Properties of Intermediate and High-mass Young Stellar Objects 
Authors: Miguel Vioque, Manuel Cavieres, Michelangelo Pantaleoni González, Álvaro Ribas, René D. Oudmaijer, Ignacio Mendigutía, Lena Kilian, Héctor Cánovas, Michael A. Kuhn
Figure caption: Proportion of clustered intermediate- and high-mass YSOs as a function of stellar mass. Top plots show the proportion of clustered stars in 3D and 5D HDBSCAN executions, left plot with 2 M ⊙ bins and right plot with 3 M ⊙ bins. Bottom plots show the proportion of clustered stars in either “3D or 5D” and both “3D and 5D.” Shown in black are the “3D or 5D” results when only considering those sources for which HDBSCAN reports more than a 95% clustering probability. Unless otherwise specified, in this work we define as “clustered” the “3D or 5D” combination (Section 4). Complete error is ﹩1/\sqrt{n}﹩, with n being the number of sources per bin.
Paper: Clustering Properties of Intermediate and High-mass Young Stellar Objects 
Authors: Miguel Vioque, Manuel Cavieres, Michelangelo Pantaleoni González, Álvaro Ribas, René D. Oudmaijer, Ignacio Mendigutía, Lena Kilian, Héctor Cánovas, Michael A. Kuhn
Figure caption: Left: histogram of cluster radii identified in 3D and 5D spaces. Cluster radius is defined as that containing 80% of the cluster’s stars from the cluster geometrical center. Center: histogram of the number of sources in each cluster. Right: cluster radii vs. number of sources per cluster identified in 3D (blue) and 5D (red) spaces.
Paper: Clustering Properties of Intermediate and High-mass Young Stellar Objects 
Authors: Miguel Vioque, Manuel Cavieres, Michelangelo Pantaleoni González, Álvaro Ribas, René D. Oudmaijer, Ignacio Mendigutía, Lena Kilian, Héctor Cánovas, Michael A. Kuhn
Figure caption: Left: Hertzsprung–Russell (HR) diagram of the considered sample of 337 intermediate- and high-mas YSOs. PARSEC 1.2S PMS tracks and isochrones corresponding to 1.5, 2, 3, 4, 6, 8, 10, 15, and 20 M ⊙ and 1, 3, and 10 Myr are presented (Bressan et al. 2012 and Marigo et al. 2017). Right: histogram of the number of YSOs considered in this work as a function of stellar mass. The lines indicate a Salpeter (1955) initial mass function (IMF) adjusted to the 2–3 M ⊙ bin.
Paper: Clustering Properties of Intermediate and High-mass Young Stellar Objects 
Authors: Miguel Vioque, Manuel Cavieres, Michelangelo Pantaleoni González, Álvaro Ribas, René D. Oudmaijer, Ignacio Mendigutía, Lena Kilian, Héctor Cánovas, Michael A. Kuhn
Figure caption: Histogram of the 337 YSOs considered in this work as a function of distance (light blue contour). Black contours are isolated stars. Blue and red bars indicate stars clustered in 3D or 5D space, respectively (we note 49 sources appear clustered in both). The green area shows the region within which the clustering algorithm HDBSCAN is most sensitive, and where we limit our analysis. Distances are Bailer-Jones et al. (2021) geometric distances.
Paper: Physical Properties of the Young Asteroid Pair 2010 UM26 and 2010 RN221
Authors: David Jewitt, Yoonyoung Kim, Jing Li, Max Mutchler
Figure caption: Angular frequency of the primary as a function of the component mass ratio. Data from asteroid pairs tabulated by Pravec et al. (2019) are shown as gray filled circles. The UM26 binary is plotted as a large yellow circle. Lines are rotational instability models described in the text which, in the homogeneous sphere approximation, correspond to bulk densities ρ = 500, 1000 and 2000 kg m−3, as marked.
Paper: Developing a Drift Rate Distribution for Technosignature Searches of Exoplanets
Authors: Megan G. Li, Sofia Z. Sheikh, Christian Gilbertson, Matthias Y. He, Howard Isaacson, Steve Croft, Evan L. Sneed
Figure caption: A histogram of all of the calculated drift rate magnitudes for the 5286 planet sample from the NASA Exoplanet Archive, with drift rates calculated for each planet at 200 evenly spaced times in the orbit. This histogram therefore contains 1,057,200 drift rates (200 for each of the 5286 exoplanets). The dotted line at 53 nHz designates the 99% boundary: 99% of calculated drift rates fall between 0 and this absolute value. The solid line demonstrates the suggested drift rate upper limits from Sheikh et al. (2019). Note that for 99% of the known exoplanet sample, the Sheikh et al. drift rate is at least four times larger than necessary.
Paper: Developing a Drift Rate Distribution for Technosignature Searches of Exoplanets
Authors: Megan G. Li, Sofia Z. Sheikh, Christian Gilbertson, Matthias Y. He, Howard Isaacson, Steve Croft, Evan L. Sneed
Figure caption: This figure shows an example orbit of an exoplanet. The reference direction, γ, is pointed toward Earth. Periapsis refers to the point of the orbit in which the orbiting body is closest to the body it orbits. For our purposes, this is always the periastron, as our exoplanets are orbiting stars. Figure by Lasunncty at the English Wikipedia from Wikimedia Commons (https://commons.wikimedia.org/wiki/File:Orbit1.svg).
Paper: Physical Properties of the Young Asteroid Pair 2010 UM26 and 2010 RN221
Authors: David Jewitt, Yoonyoung Kim, Jing Li, Max Mutchler
Figure caption: Apparent V-band photometry of UM26 (red circles) compared with a model (solid black line) for the brightness variation of an inert (constant cross section) asteroid, taking into account variations in the Sun-Asteroid-Earth viewing geometry.
Paper: Physical Properties of the Young Asteroid Pair 2010 UM26 and 2010 RN221
Authors: David Jewitt, Yoonyoung Kim, Jing Li, Max Mutchler
Figure caption: Surface brightness profile plotted perpendicular to the line connecting UM26 and RM221, as described in the text. The red dashed line marks the mean and the short black, horizontal line marks the 3σ upper limit to the possible surface brightness of any diffuse material.
Paper: Physical Properties of the Young Asteroid Pair 2010 UM26 and 2010 RN221
Authors: David Jewitt, Yoonyoung Kim, Jing Li, Max Mutchler
Figure caption: Surface brightness profiles of UM26 (solid red line), RN221 (dashed blue line), and the WFC3 point-spread function (solid black line) showing the absence of evidence for resolved material near each asteroid.
Paper: Physical Properties of the Young Asteroid Pair 2010 UM26 and 2010 RN221
Authors: David Jewitt, Yoonyoung Kim, Jing Li, Max Mutchler
Figure caption: Lightcurves of 2010 UM26 (yellow circles) and 2010 RN221 (green circles) measured on UT 2023 January 4. Note that the upper and lower portions of the figure have different vertical scales and that the y-axis is broken in the range 22.05 ≤ V ≤ 23.10, for clarity of presentation.
Paper: Physical Properties of the Young Asteroid Pair 2010 UM26 and 2010 RN221
Authors: David Jewitt, Yoonyoung Kim, Jing Li, Max Mutchler
Figure caption: Images of (top) UM26/RN221 and (bottom) 331P at the same scale. White, vertical bars mark the major components in each object. The image of 331P was taken on UT 2015 December 25 (Jewitt et al. 2021).
Paper: ELemental abundances of Planets and brown dwarfs Imaged around Stars (ELPIS). I. Potential Metal Enrichment of the Exoplanet AF Lep b and a Novel Retrieval Approach for Cloudy Self-luminous Atmospheres
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Keith Hawkins, Catherine Manea, Jonathan J. Fortney, Caroline V. Morley, Andrew Skemer, Mark S. Marley, Brendan P. Bowler, Aarynn L. Carter, Kyle Franson, Zachary G. Maas, Christopher Sneden
Figure caption: Top left: The retrieved T–P profiles (orange) with the atmospheric thermal structure modeled via the temperature gradient. The input data include the ﹩K1/K2/L^{\prime} ﹩ photometry and both spectra of AF Lep b, with constrained M and R priors; thus, the retrieved T–P profiles shown here are exactly the same as the middle left panel of Figure 9. The 1σ/2σ/3σ confidence intervals are shown as orange shades. Overlaid is an RCE T–P profile (black) created at the median values of all parameters, which is consistent with the retrieved T–P profiles. Bottom left: Contribution function of the best-fit model for the retrieval shown in the top left panel. The 1–4 μm photosphere is located above 1 bar due to the cloud effect; the retrieved silicate cloud has a base pressure near 3 bar with a relatively small f sed and large mass fraction. Top and bottom right: Retrieved T–P profiles and contribution function of the best-fit model (purple), with the atmospheric thermal structure modeled in terms of the temperature. In comparison, modeling the thermal structure via the temperature gradient offers the flexibility to incorporate an RCE prior and thereby better constraints on cloud properties.
Paper: ELemental abundances of Planets and brown dwarfs Imaged around Stars (ELPIS). I. Potential Metal Enrichment of the Exoplanet AF Lep b and a Novel Retrieval Approach for Cloudy Self-luminous Atmospheres
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Keith Hawkins, Catherine Manea, Jonathan J. Fortney, Caroline V. Morley, Andrew Skemer, Mark S. Marley, Brendan P. Bowler, Aarynn L. Carter, Kyle Franson, Zachary G. Maas, Christopher Sneden
Figure caption: Effective temperature (left) and bolometric luminosity (right) of AF Lep b (red star) compared to those of other directly imaged planets, free-floating planets, and brown dwarfs, which are color-coded by their surface gravities (orange and black for ﹩\mathrm{log}(g)﹩ below and above 4.5 dex, respectively); these ﹩\mathrm{log}(g)﹩ of the comparison sample are obtained from Filippazzo et al. (2015) and Zhang et al. (2020, 2021c, 2021d). The plotted properties of AF Lep b are inferred by our retrieval analysis performed for the full spectrophotometry with constrained priors for the planet’s mass and radius (i.e., the last column of Table 6). In both panels, we use black lines and gray shades to show the polynomials that convert spectral types to T eff (Table 13 of Kirkpatrick et al. 2021) and to L bol (footnote 16 of Zhang et al. 2020) in the high-gravity regime. AF Lep b is thus far the coldest exoplanet with suggested evidence of silicate clouds.
Paper: ELemental abundances of Planets and brown dwarfs Imaged around Stars (ELPIS). I. Potential Metal Enrichment of the Exoplanet AF Lep b and a Novel Retrieval Approach for Cloudy Self-luminous Atmospheres
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Keith Hawkins, Catherine Manea, Jonathan J. Fortney, Caroline V. Morley, Andrew Skemer, Mark S. Marley, Brendan P. Bowler, Aarynn L. Carter, Kyle Franson, Zachary G. Maas, Christopher Sneden
Figure caption: Our measured stellar parameters of AF Lep A (verticle red line with shadow) compared to those in the literature (black; sorted by M A, and then by [Fe/H]A if M A is not reported). References for labels shown on the y-axis are as follows. Tagl94: Tagliaferri et al. (1994); Alle99: Allende Prieto & Lambert (1999); Felt01: Feltzing et al. (2001); Vale05: Valenti & Fischer (2005); Ammo06: Ammons et al. (2006); Take07: Takeda et al. (2007); Casa11: Casagrande et al. (2011); Wrig11: Wright et al. (2011); Pale15: Paletou et al. (2015); Chan16: Chandler et al. (2016); Luck18: Luck (2018); Ande19: Anders et al. (2019); Kerv19: Kervella et al. (2019); Rice20: Rice & Brewer (2020); Mont21: Montalto et al. (2021); Ande22: Anders et al. (2022); Gaia22: Gaia Collaboration et al. (2023); Pear22: Pearce et al. (2022).
Paper: ELemental abundances of Planets and brown dwarfs Imaged around Stars (ELPIS). I. Potential Metal Enrichment of the Exoplanet AF Lep b and a Novel Retrieval Approach for Cloudy Self-luminous Atmospheres
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Keith Hawkins, Catherine Manea, Jonathan J. Fortney, Caroline V. Morley, Andrew Skemer, Mark S. Marley, Brendan P. Bowler, Aarynn L. Carter, Kyle Franson, Zachary G. Maas, Christopher Sneden
Figure caption: The abundance of several key species (solid) inferred from the retrieval performed on the ﹩K1/K2/L^{\prime} ﹩ photometry and the Mesa et al. (2023) spectrum, along with constrained priors on the planet’s mass and radius (Section 7.1). These profiles correspond to the median values of the parameters as summarized in Table 6, including a quenching pressure at 102.4 bar. Dashed lines present the abundances under chemical equilibrium. For H2O, CO, and CH4, our retrieved profiles suggest evidence of disequilibrium chemistry in the atmosphere of AF Lep b; for the other species (e.g., Na, K, and H2S), we assume their abundances follow the equilibrium chemistry in our retrievals (see Section 6.3).
Paper: ELemental abundances of Planets and brown dwarfs Imaged around Stars (ELPIS). I. Potential Metal Enrichment of the Exoplanet AF Lep b and a Novel Retrieval Approach for Cloudy Self-luminous Atmospheres
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Keith Hawkins, Catherine Manea, Jonathan J. Fortney, Caroline V. Morley, Andrew Skemer, Mark S. Marley, Brendan P. Bowler, Aarynn L. Carter, Kyle Franson, Zachary G. Maas, Christopher Sneden
Figure caption: Spectrophotometry of AF Lep b (black) compared to the top four best-matched ultracool dwarfs obtained from the template fitting that does not (left) and does (right) incorporate the reddening law of the interstellar medium, which we use to mimic the cloud effect for the purpose of spectral typing.