adsabs/AstroCLIMB huggingface dataset:
Paper: PhotoD with LSST: Stellar Photometric Distances Out to the Edge of the Galaxy
Authors: Lovro Palaversa, Željko Ivezić, Neven Caplar, Karlo Mrakovčić, Bob Abel, Oleksandra Razim, Filip Matković, Connor Yablonski, Toni Šarić, Tomislav Jurkić, Sandro Campos, Melissa DeLucchi, Derek Jones, Konstantin Malanchev, Alex I. Malz, Sean McGuire, Mario Jurić
Figure caption: Statistical performance analysis for the estimates of model parameter Mr (absolute magnitude), as a function of observed u-band magnitude and the g − i color, for the same simulated sample as shown in Figure 11. The left column shows the mean difference per pixel between the true and estimated values, the middle column shows scatter per pixel, and the right column shows the scatter normalized by the estimated uncertainties (χ2). Contours visualize the sample distribution in each diagram. Note that for main-sequence stars Mr > 4 and for most stars 4 < Mr < 10.
Paper: PhotoD with LSST: Stellar Photometric Distances Out to the Edge of the Galaxy
Authors: Lovro Palaversa, Željko Ivezić, Neven Caplar, Karlo Mrakovčić, Bob Abel, Oleksandra Razim, Filip Matković, Connor Yablonski, Toni Šarić, Tomislav Jurkić, Sandro Campos, Melissa DeLucchi, Derek Jones, Konstantin Malanchev, Alex I. Malz, Sean McGuire, Mario Jurić
Figure caption: Maps of the prior (left), likelihood (middle; computed using Equation (6)), and posterior (right; computed using Equation (3)) for a simulated main-sequence star with r = 21.2, (g − r) = 0.48, Mr = 4.58, [Fe/H] = −0.76, and Ar = 0.37. The prior in the Ar direction is uniform. The circles mark the values of the input Mr and [Fe/H]. The posterior marginal distributions for all three model parameters are shown in Figure 9.
Paper: PhotoD with LSST: Stellar Photometric Distances Out to the Edge of the Galaxy
Authors: Lovro Palaversa, Željko Ivezić, Neven Caplar, Karlo Mrakovčić, Bob Abel, Oleksandra Razim, Filip Matković, Connor Yablonski, Toni Šarić, Tomislav Jurkić, Sandro Campos, Melissa DeLucchi, Derek Jones, Konstantin Malanchev, Alex I. Malz, Sean McGuire, Mario Jurić
Figure caption: Examples of priors for model parameters, p(Mr, [Fe/H]), for main-sequence stars and red giants, for four sky positions (rows, for locations see the first column) and for several brightness levels in the LSST magnitude range (left to right: bright to faint). The integral of each map over Mr and [Fe/H] is unity. The dashed lines are the same in each panel and are added to guide the eye.
Paper: PhotoD with LSST: Stellar Photometric Distances Out to the Edge of the Galaxy
Authors: Lovro Palaversa, Željko Ivezić, Neven Caplar, Karlo Mrakovčić, Bob Abel, Oleksandra Razim, Filip Matković, Connor Yablonski, Toni Šarić, Tomislav Jurkić, Sandro Campos, Melissa DeLucchi, Derek Jones, Konstantin Malanchev, Alex I. Malz, Sean McGuire, Mario Jurić
Figure caption: Luminosity–color tracks, shown with gray symbols, for unresolved binaries composed of an M dwarf with [Fe/H] = −1.5 and an H WD. Analogous tracks for binaries composed of an M dwarf with [Fe/H] = 0 and either an H or He WD look very similar though not identical. Data, shown as colored symbols, are the same as in Figure 1 and in the middle panel in Figure 2.
Paper: PhotoD with LSST: Stellar Photometric Distances Out to the Edge of the Galaxy
Authors: Lovro Palaversa, Željko Ivezić, Neven Caplar, Karlo Mrakovčić, Bob Abel, Oleksandra Razim, Filip Matković, Connor Yablonski, Toni Šarić, Tomislav Jurkić, Sandro Campos, Melissa DeLucchi, Derek Jones, Konstantin Malanchev, Alex I. Malz, Sean McGuire, Mario Jurić
Figure caption: Luminosity–color tracks for H and He WDs based on models from P. Bergeron et al. (1995), with colors slightly shifted to bring them in agreement with the SDSS photometry. Data, shown as symbols, are the same as in Figure 1 and in the middle panel in Figure 2. Note the crucial role of the u − g color for distinguishing H and He tracks.
Paper: PhotoD with LSST: Stellar Photometric Distances Out to the Edge of the Galaxy
Authors: Lovro Palaversa, Željko Ivezić, Neven Caplar, Karlo Mrakovčić, Bob Abel, Oleksandra Razim, Filip Matković, Connor Yablonski, Toni Šarić, Tomislav Jurkić, Sandro Campos, Melissa DeLucchi, Derek Jones, Konstantin Malanchev, Alex I. Malz, Sean McGuire, Mario Jurić
Figure caption: An illustration of the improvement in the “knowledge” of model parameters between the prior and posterior, brought by measurements via the likelihood map. The lines show marginal distributions produced with the prior (blue), likelihood (green), and posterior (red) maps from Figure 8. The dashed line shows the expectation value for the marginalized posterior and the vertical solid line marks the true input value.
Paper: PhotoD with LSST: Stellar Photometric Distances Out to the Edge of the Galaxy
Authors: Lovro Palaversa, Željko Ivezić, Neven Caplar, Karlo Mrakovčić, Bob Abel, Oleksandra Razim, Filip Matković, Connor Yablonski, Toni Šarić, Tomislav Jurkić, Sandro Campos, Melissa DeLucchi, Derek Jones, Konstantin Malanchev, Alex I. Malz, Sean McGuire, Mario Jurić
Figure caption: Analogous to Figure 12, except for estimates of [Fe/H] (metallicity) instead of Mr.
Paper: PhotoD with LSST: Stellar Photometric Distances Out to the Edge of the Galaxy
Authors: Lovro Palaversa, Željko Ivezić, Neven Caplar, Karlo Mrakovčić, Bob Abel, Oleksandra Razim, Filip Matković, Connor Yablonski, Toni Šarić, Tomislav Jurkić, Sandro Campos, Melissa DeLucchi, Derek Jones, Konstantin Malanchev, Alex I. Malz, Sean McGuire, Mario Jurić
Figure caption: Two-parameter covariances and marginal distributions for the posterior map from Figure 8. The symbols and dashed lines show the true input values.
Paper: Peering into the Black Box: Forward Modeling of the Uncertainty Budget of High-resolution Spectroscopy of Exoplanet Atmospheres
Authors: Arjun B. Savel, Megan Bedell, Eliza M.-R. Kempton, Peter C. B. Smith, Jacob L. Bean, Lily L. Zhao, Kaze W. K. Wong, Jorge A. Sanchez, Michael R. Line
Figure caption: The spectral components learned by four PCA components from a simulated HRCCS data set that only includes the planetary signal and instrumental blaze function. The PCA algorithm is able to approximate the diagonal trace of the planetary atmosphere with a superposition of a few strong stationary components. When other spectral components are present (including photon noise), PCA is not able to approximate the planetary signal, as it is most sensitive to the time-invariant signals with greater variance across wavelengths.
Paper: Peering into the Black Box: Forward Modeling of the Uncertainty Budget of High-resolution Spectroscopy of Exoplanet Atmospheres
Authors: Arjun B. Savel, Megan Bedell, Eliza M.-R. Kempton, Peter C. B. Smith, Jacob L. Bean, Lily L. Zhao, Kaze W. K. Wong, Jorge A. Sanchez, Michael R. Line
Figure caption: The effect of removing different numbers of PCA components from HRCCS data on the CCF detection significance in our baseline results. This is calculated in noiseless simulations (top left), SNR = 250 simulations (top right), and SNR = 60 simulations (bottom left) with 10 different noise realizations. Including more spectral components (e.g., the stellar spectrum) severely decreases the planet's detection significance, but a small number of PCA components can recover the planet detection about the detection threshold. These significance values are compared to a commonly accepted HRCCS detection threshold (SNR = 4.5; e.g., S. H. Cabot et al. 2019).
Paper: Peering into the Black Box: Forward Modeling of the Uncertainty Budget of High-resolution Spectroscopy of Exoplanet Atmospheres
Authors: Arjun B. Savel, Megan Bedell, Eliza M.-R. Kempton, Peter C. B. Smith, Jacob L. Bean, Lily L. Zhao, Kaze W. K. Wong, Jorge A. Sanchez, Michael R. Line
Figure caption: The learned normalizing flow topology as compared with PyMultiNest equally weighted samples from a baseline retrieval. The normalizing flow is able to learn the topology of the posterior distribution. Note that this exercise does not constitute actual parameter inference—rather, we are demonstrating the flexibility of the global sampling scheme to approximate the final global posterior distribution.
Paper: Peering into the Black Box: Forward Modeling of the Uncertainty Budget of High-resolution Spectroscopy of Exoplanet Atmospheres
Authors: Arjun B. Savel, Megan Bedell, Eliza M.-R. Kempton, Peter C. B. Smith, Jacob L. Bean, Lily L. Zhao, Kaze W. K. Wong, Jorge A. Sanchez, Michael R. Line
Figure caption: A set of spurious HCN signals in our baseline simulations. The maxima of these KP–Vsys maps are denoted with a white cross. While HCN is not included in this set of models, its signal can be found in cross-correlation when using ATRAN tellurics (top left), when using data-driven tellurics (top right), with low photon noise (top row), with high photon noise (bottom row), and in different noise realizations (bottom left).
Paper: Peering into the Black Box: Forward Modeling of the Uncertainty Budget of High-resolution Spectroscopy of Exoplanet Atmospheres
Authors: Arjun B. Savel, Megan Bedell, Eliza M.-R. Kempton, Peter C. B. Smith, Jacob L. Bean, Lily L. Zhao, Kaze W. K. Wong, Jorge A. Sanchez, Michael R. Line
Figure caption: Results of an MCMC fit to the velocity parameters (in km s−1) and scale factor for simulated HRCCS data at two photon noise levels. This model used four PCA components to remove the stellar, telluric, and instrumental features in the simulated data. Using PCA in this experiment did not bias the scale factor toward smaller values, indicating that using PCA alone does not scale the planetary signal in HRCCS data.
Paper: Peering into the Black Box: Forward Modeling of the Uncertainty Budget of High-resolution Spectroscopy of Exoplanet Atmospheres
Authors: Arjun B. Savel, Megan Bedell, Eliza M.-R. Kempton, Peter C. B. Smith, Jacob L. Bean, Lily L. Zhao, Kaze W. K. Wong, Jorge A. Sanchez, Michael R. Line
Figure caption: Gas constraints from our baseline retrieval on simulated data of WASP-77Ab. We are able to recover gas constraints about as well as M. R. Line et al. (2021), with bounded constraints on H2O, CO, and the CO isotope ratio in the lower-noise case (SNR = 250). The higher-noise case (SNR = 60) substantially changes the likelihood surface for the gas constraints shown, with less of an impact on velocity and temperature–pressure parameters.
Paper: Peering into the Black Box: Forward Modeling of the Uncertainty Budget of High-resolution Spectroscopy of Exoplanet Atmospheres
Authors: Arjun B. Savel, Megan Bedell, Eliza M.-R. Kempton, Peter C. B. Smith, Jacob L. Bean, Lily L. Zhao, Kaze W. K. Wong, Jorge A. Sanchez, Michael R. Line
Figure caption: Gas and velocity constraints from our PyMultiNest high-resolution atmospheric retrieval. Including strongly time-dependent tellurics (maroon) yields distinct posteriors from our time-dependent telluric (teal) model.
Paper: Peering into the Black Box: Forward Modeling of the Uncertainty Budget of High-resolution Spectroscopy of Exoplanet Atmospheres
Authors: Arjun B. Savel, Megan Bedell, Eliza M.-R. Kempton, Peter C. B. Smith, Jacob L. Bean, Lily L. Zhao, Kaze W. K. Wong, Jorge A. Sanchez, Michael R. Line
Figure caption: A comparison of our data-driven telluric reconstruction against ATRAN (S. D. Lord 1992) radiative transfer simulations over one IGRINS order.
Paper: Hα Variability of AB Aur b with the Hubble Space Telescope: Probing the Nature of a Protoplanet Candidate with Accretion Light Echoes
Authors: Brendan P. Bowler, Yifan Zhou, Lauren I. Biddle, Lillian Yushu Jiang, Jaehan Bae, Laird M. Close, Katherine B. Follette, Kyle Franson, Adam L. Kraus, Aniket Sanghi, Quang Tran, Kimberly Ward-Duong, Ya-Lin Wu, Zhaohuan Zhu
Figure caption: Examples of the impact of orbital geometry on light echo time delays. Stochastic changes in the brightness of a host star (from episodic accretion, for instance) will be seen as delayed variability from a compact disk feature at an orbital distance r. This time delay will range from 0 at inferior conjunction (ω + ν(t) = π/2; left panel) to r/c in the sky plane (middle panel) to 2r/c at superior conjunction (ω + ν(t) = 3π/2; right panel).
Paper: The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets
Authors: Judah Van Zandt, Erik A. Petigura, Jack Lubin, Lauren M. Weiss, Emma V. Turtelboom, Tara Fetherolf, Joseph M. Akana Murphy, Ian J. M. Crossfield, Gregory J. Gilbert, Teo Močnik, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Isabel Angelo, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Steve B. Howell, Andrew W. Mayo, Daria Pidhorodetska, Alex S. Polanski, James Rogers, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Dakotah Tyler, Samuel W. Yee, Jon Zink
Figure caption: The same as Figure A1 but for HD 12572. We measured the mass of the 20 days sub-Neptune in this system and also found a strong linear trend with no significant curvature. We also measured a marginal astrometric acceleration, which imposed added constraints (blue contours). Note that the gray line denotes orbital models that are ruled out by direct imaging under the assumption of a circular, face-on orbit. Companions with nonzero inclinations and eccentricities may lie beyond the line without being ruled out.
Paper: The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets
Authors: Judah Van Zandt, Erik A. Petigura, Jack Lubin, Lauren M. Weiss, Emma V. Turtelboom, Tara Fetherolf, Joseph M. Akana Murphy, Ian J. M. Crossfield, Gregory J. Gilbert, Teo Močnik, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Isabel Angelo, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Steve B. Howell, Andrew W. Mayo, Daria Pidhorodetska, Alex S. Polanski, James Rogers, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Dakotah Tyler, Samuel W. Yee, Jon Zink
Figure caption: The same as Figure A1 but for TIC 142381532. The inner transiting planet in this system in a sub-Saturn, which we characterized at high significance. Although this planet passed Rp < 10 R⊕, it is likely a gas giant, so we exclude this system from our occurrence calculations. Our trend measurement is marginal and evinces planetary and brown dwarf models with roughly equal probability.
Paper: The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets
Authors: Judah Van Zandt, Erik A. Petigura, Jack Lubin, Lauren M. Weiss, Emma V. Turtelboom, Tara Fetherolf, Joseph M. Akana Murphy, Ian J. M. Crossfield, Gregory J. Gilbert, Teo Močnik, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Isabel Angelo, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Steve B. Howell, Andrew W. Mayo, Daria Pidhorodetska, Alex S. Polanski, James Rogers, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Dakotah Tyler, Samuel W. Yee, Jon Zink
Figure caption: Our second analysis of the trend in the HD 93963 system. We expanded the semimajor-axis range over which we tested companion models and therefore did not use the informative mass–separation prior described in Section 5.2, which is defined for separations ≤64 au. We indicate the position of the stellar companion, HD 93963 B, with a yellow star. Our analysis suggests that an M5 dwarf at a separation of 484 au is too small/too distant to have caused the observed trend.
Paper: The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets
Authors: Judah Van Zandt, Erik A. Petigura, Jack Lubin, Lauren M. Weiss, Emma V. Turtelboom, Tara Fetherolf, Joseph M. Akana Murphy, Ian J. M. Crossfield, Gregory J. Gilbert, Teo Močnik, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Isabel Angelo, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Steve B. Howell, Andrew W. Mayo, Daria Pidhorodetska, Alex S. Polanski, James Rogers, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Dakotah Tyler, Samuel W. Yee, Jon Zink
Figure caption: The same as Figure A1 but for HD 75732. We detected only one of the four nontransiting planets in this system using our blind search algorithm. The residual trend, together with a low-significance astrometric acceleration, constrain the mass–separation posterior primarily to the planetary regime.
Paper: The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets
Authors: Judah Van Zandt, Erik A. Petigura, Jack Lubin, Lauren M. Weiss, Emma V. Turtelboom, Tara Fetherolf, Joseph M. Akana Murphy, Ian J. M. Crossfield, Gregory J. Gilbert, Teo Močnik, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Isabel Angelo, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Steve B. Howell, Andrew W. Mayo, Daria Pidhorodetska, Alex S. Polanski, James Rogers, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Dakotah Tyler, Samuel W. Yee, Jon Zink
Figure caption: The same as Figure A1 but for HD 93963. We did not recover either of this system’s two transiting planets at high significance. We measured a significant trend and marginal curvature in this system. Our analysis showed that the source of this RV variability is most likely a planet.
Paper: The TESS–Keck Survey. XXIV. Outer Giants May Be More Prevalent in the Presence of Inner Small Planets
Authors: Judah Van Zandt, Erik A. Petigura, Jack Lubin, Lauren M. Weiss, Emma V. Turtelboom, Tara Fetherolf, Joseph M. Akana Murphy, Ian J. M. Crossfield, Gregory J. Gilbert, Teo Močnik, Natalie M. Batalha, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Paul Robertson, Arpita Roy, Isabel Angelo, Aida Behmard, Corey Beard, Ashley Chontos, Fei Dai, Steven Giacalone, Michelle L. Hill, Rae Holcomb, Steve B. Howell, Andrew W. Mayo, Daria Pidhorodetska, Alex S. Polanski, James Rogers, Lee J. Rosenthal, Ryan A. Rubenzahl, Nicholas Scarsdale, Dakotah Tyler, Samuel W. Yee, Jon Zink
Figure caption: The same as Figure A1 but for HD 156141. We obtained a marginally significant measurement of the inner transiting planet’s mass and high-significance trend and curvature measurements. The long-term signals in this system are consistent with planets and brown dwarfs, whereas stellar models are nearly ruled out with the aid of direct imaging.
Paper: Four Planets Found through Microlensing Events Involving Faint Source Stars
Authors: Cheongho Han, Michael D. Albrow, Chung-Uk Lee, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, In-Gu Shin, Jennifer C. Yee, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Doeon Kim, Dong-Jin Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge
Figure caption: Lensing light curve of KMT-2023-BLG-2209.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Four Planets Found through Microlensing Events Involving Faint Source Stars
Authors: Cheongho Han, Michael D. Albrow, Chung-Uk Lee, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, In-Gu Shin, Jennifer C. Yee, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Doeon Kim, Dong-Jin Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge
Figure caption: Bayesian posteriors of the host masses of the planetary systems. In each panel, the distributions shown in blue and red curves represent the contributions from disk and bulge lens populations, respectively, while the black curve denotes the combined contribution from both populations. The solid vertical line marks the median of the distribution, and the dotted vertical lines represent the 1σ uncertainty range.
Paper: Four Planets Found through Microlensing Events Involving Faint Source Stars
Authors: Cheongho Han, Michael D. Albrow, Chung-Uk Lee, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, In-Gu Shin, Jennifer C. Yee, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Doeon Kim, Dong-Jin Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge
Figure caption: Positions of source stars with respect to the centroids of red giant clumps (RGC) in the color–magnitude diagrams constructed by combining the KMTC (gray dots) and HST (brown dots) observations.
Paper: Four Planets Found through Microlensing Events Involving Faint Source Stars
Authors: Cheongho Han, Michael D. Albrow, Chung-Uk Lee, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, In-Gu Shin, Jennifer C. Yee, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Doeon Kim, Dong-Jin Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge
Figure caption: Bayesian posteriors of the distances to the planetary systems. The notations are the same as those in Figure 10.
Paper: Four Planets Found through Microlensing Events Involving Faint Source Stars
Authors: Cheongho Han, Michael D. Albrow, Chung-Uk Lee, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, Yoon-Hyun Ryu, Yossi Shvartzvald, In-Gu Shin, Jennifer C. Yee, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Doeon Kim, Dong-Jin Kim, Seung-Lee Kim, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge
Figure caption: Lens-system configuration of KMT-2023-BLG-2209.
Paper: JWST/NIRCam Coronagraphic Search for Hidden Planets in the HD 163296 Protoplanetary Disk
Authors: Taichi Uyama, Luca Ricci, Marie Ygouf, Sean Andrews, Sara Gallagher, Jane Huang, Andrea Isella, Dimitri Mawet, Laura M. Pérez, Massimo Robberto, Garreth Ruane, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Left: Keck/NIRC2 Ms-band post-processed image after smoothing with a Gaussian with σ = 2 pixels to better highlight the extended features. Right: diagram showing the conversion between the NIRC2 Ms-band contrast limits and the mass from evolutionary models of planets with different properties (as in Figure 9; the colored shades indicate the contrast limits at the projected separations of the ALMA dust gaps (gray for D10 and sky blue for D45); the colored bars represent the hot- (red)/warm- (orange)/cold-start (blue) models (D. S. Spiegel & A. Burrows 2012) with cloud-free and hybrid cloud atmospheres at solar metallicity (A. Burrows et al. 2011) and ages between 1 and 5 Myr (the upper and lower limits of each model range correspond to 1 and 5 Myr, respectively), assuming the same extinction as the central star, i.e., AV = 0.
Paper: JWST/NIRCam Coronagraphic Search for Hidden Planets in the HD 163296 Protoplanetary Disk
Authors: Taichi Uyama, Luca Ricci, Marie Ygouf, Sean Andrews, Sara Gallagher, Jane Huang, Andrea Isella, Dimitri Mawet, Laura M. Pérez, Massimo Robberto, Garreth Ruane, Shangjia Zhang, Zhaohuan Zhu
Figure caption: Gallery of the forward-modeled disk (Figure 15) with different KL modes.
Paper: JWST/NIRCam Coronagraphic Search for Hidden Planets in the HD 163296 Protoplanetary Disk
Authors: Taichi Uyama, Luca Ricci, Marie Ygouf, Sean Andrews, Sara Gallagher, Jane Huang, Andrea Isella, Dimitri Mawet, Laura M. Pérez, Massimo Robberto, Garreth Ruane, Shangjia Zhang, Zhaohuan Zhu
Figure caption: F410M post-processed images with different KL modes after injecting a fake source with different contrast levels (ΔF410M = 14.6–15.6 mag) at the location of ALMA velocity kink #1. The injected source is indicated by a white arrow in each image.