adsabs/AstroCLIMB huggingface dataset:
Paper: Detecting Biosignatures in Nearby Rocky Exoplanets Using High-contrast Imaging and Medium-resolution Spectroscopy with the Extremely Large Telescope
Authors: Huihao Zhang, Ji Wang, 吉 王, Michael K. Plummer
Figure caption: Flowchart outlining the simulation of ELT direct imaging applied to exoplanets. Photons from the star and planet pass through Earth’s atmosphere and are processed by the coronagraph and captured by the detector. After obtaining the data, the effects of the atmosphere and star are removed through observations of the host star and the positions where no planet signals are received.
Paper: High-resolution, Mid-infrared Color Temperature Mapping of the Central 10″ of the Galaxy
Authors: Cuc K. Dinh, Anna Ciurlo, Mark R. Morris, Rainer Schödel, Andrea Ghez, Tuan Do
Figure caption: The western edge of the mini-cavity as observed in the 3.6 μm band (upper left), 8.6 μm band (upper right), color temperature map (lower left), and optical depth map at 3.8 μm (lower right). The western mini-cavity appears to be colder than its surrounding constituents, possibly because of dust shielding of incoming radiation.
Paper: Atmospheric Metallicity and C/O of HD 189733 b from High-resolution Spectroscopy
Authors: Luke Finnerty, Jerry W. Xuan, Yinzi Xin, Joshua Liberman, Tobias Schofield, Michael P. Fitzgerald, Shubh Agrawal, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Chih-Chun Hsu, Nemanja Jovanovic, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Jean-Baptiste Ruffio, Ben Sappey, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Jason J. Wang, 劲飞 王, Ji Wang, 王 吉
Figure caption:  v sys−K p diagrams for H2O, CO, CH4, and 13CO. Dashed red lines indicate the nominal values of the planetary velocity parameters, and the red dot indicates the maximum-likelihood values for the full model. These maps were made by subtracting a map omitting each species from a map made using the maximum-likelihood model, in order to better account for the impact of other atmospheric species on the continuum. Significance was estimated by dividing each map by the standard deviation of the K p < 0 region. Continuum impacts are still significant, leading to weaker-than-expected detections of H2O and CO and biasing the CO velocity. These effects are less important for lower-abundance species. As expected based on the retrieved posteriors, we do not detect CH4, and 13CO shows a weak (∼3σ) feature near the expected planet velocity. This 13CO feature does not constitute an independent detection, but the inclusion of 13CO is favored over a 12CO-only model at ∼3σ, consistent with other results for 13CO in hot Jupiter atmospheres (Line et al. 2021; Finnerty et al. 2023b).
Paper: Insight into the Formation of β Pic b through the Composition of Its Parent Protoplanetary Disk as Revealed by the β Pic Moving Group Member HD 181327
Authors: Henrique Reggiani, Jhon Yana Galarza, Kevin C. Schlaufman, David K. Sing, Brian F. Healy, Andrew McWilliam, Joshua D. Lothringer, Laurent Pueyo
Figure caption: On the left we present the planetary-to-stellar (protoplanetary disk proxy) C/O ratios of β Pic b as a function of planetary-to-stellar carbon abundances, and on the right we present the planetary-to-stellar C/O ratios as a function of planetary-to-stellar oxygen abundance. In dark and light green we present the planetary results of the GRAVITY Collaboration et al. (2020) study, scaled to solar and stellar (HD 181327) abundances, respectively. In dark and light blue we present the same, but for the carbon and oxygen abundances retrieved for β Pic b from our study. We see that regardless of the retrieval there is a difference in using solar and stellar abundances, portraying the importance of a dedicated stellar analysis. It is also clear that our retrieval has considerably changed the results. While there are visible differences, for β Pic b our different analyses corroborate previous conclusions about the planetary formation. It formed beyond the H2O ice line, accreting large amounts of icy planetesimals after envelope accretion.
Paper: Insight into the Formation of β Pic b through the Composition of Its Parent Protoplanetary Disk as Revealed by the β Pic Moving Group Member HD 181327
Authors: Henrique Reggiani, Jhon Yana Galarza, Kevin C. Schlaufman, David K. Sing, Brian F. Healy, Andrew McWilliam, Joshua D. Lothringer, Laurent Pueyo
Figure caption: We show the 4500–4540 Å region of our spectra along with HARPS archival data of β Pic from observing program ID 0104.C-0418(C). The high rotational velocities of HD 191089 (≈40 km s−1, Zúñiga-Fernández et al. 2021) and β Pic are visible, and individual important atomic features are not possible to distinguish.
Paper: Insight into the Formation of β Pic b through the Composition of Its Parent Protoplanetary Disk as Revealed by the β Pic Moving Group Member HD 181327
Authors: Henrique Reggiani, Jhon Yana Galarza, Kevin C. Schlaufman, David K. Sing, Brian F. Healy, Andrew McWilliam, Joshua D. Lothringer, Laurent Pueyo
Figure caption: We present, as blue points, the distribution of carbon and oxygen abundances (in different scales) as a function of metallicity from the GALAH DR3 survey. In white we show the abundance of HD 181327, as a proxy for β Pic’s molecular cloud. One can see that its abundance is outside of the most populated region in all abundance spaces. This shows the importance of individually determining the stellar abundances for the interpretation of planetary retrievals.
Paper: Insight into the Formation of β Pic b through the Composition of Its Parent Protoplanetary Disk as Revealed by the β Pic Moving Group Member HD 181327
Authors: Henrique Reggiani, Jhon Yana Galarza, Kevin C. Schlaufman, David K. Sing, Brian F. Healy, Andrew McWilliam, Joshua D. Lothringer, Laurent Pueyo
Figure caption: We show the abundance differences between HD 181327 and β Pic. The abundances from β Pic are from Saffe et al. (2021).
Paper: Insight into the Formation of β Pic b through the Composition of Its Parent Protoplanetary Disk as Revealed by the β Pic Moving Group Member HD 181327
Authors: Henrique Reggiani, Jhon Yana Galarza, Kevin C. Schlaufman, David K. Sing, Brian F. Healy, Andrew McWilliam, Joshua D. Lothringer, Laurent Pueyo
Figure caption:  β Pic b GPI and Gravity spectrum (black data points) along with the posterior distribution of the spectral retrieval model.
Paper: Insight into the Formation of β Pic b through the Composition of Its Parent Protoplanetary Disk as Revealed by the β Pic Moving Group Member HD 181327
Authors: Henrique Reggiani, Jhon Yana Galarza, Kevin C. Schlaufman, David K. Sing, Brian F. Healy, Andrew McWilliam, Joshua D. Lothringer, Laurent Pueyo
Figure caption: Posterior distribution for the ATMO atmospheric retrieval model fit to the β Pic b spectrum.
Paper: Robust Detrending of Spatially Correlated Systematics in Kepler Light Curves Using Low-rank Methods
Authors: Jamila S. Taaki, Athol J. Kemball, Farzad Kamalabadi
Figure caption: Three sample light curves across injected signal type  a  [m] m ∈ {s, t, f} (sine, transit, and flare) from run #0, a representative run of Experiment A. The figure shows the preprocessed light curve before detrending  y  (upper row), the detrended light curve using PCA ﹩{{\boldsymbol{y}}}_{\mathrm{PCA}}^{{\prime} }﹩ (middle row), and the detrended light curve using the spatial systematics algorithm ﹩{\boldsymbol{y}}^{\prime} ﹩ (lower row). Simulated injected signals are overlaid in black. The x-axis is Kepler's long-cadence time sample index. This sample shows an instance where PCA detrending removed the injected astrophysical sine and flare signals, while spatial detrending preserved those signals.
Paper: Robust Detrending of Spatially Correlated Systematics in Kepler Light Curves Using Low-rank Methods
Authors: Jamila S. Taaki, Athol J. Kemball, Farzad Kamalabadi
Figure caption: Estimated basis vectors  v   k , k ∈ {1, 20}(K = 20) obtained for run #0, a single representative run of Experiment A, shown here for the spatial systematics algorithm (blue) and the reference PCA method (red). The spatial basis vectors and PCA basis vectors closely overlap for the first two terms.
Paper: Robust Detrending of Spatially Correlated Systematics in Kepler Light Curves Using Low-rank Methods
Authors: Jamila S. Taaki, Athol J. Kemball, Farzad Kamalabadi
Figure caption: Leading PCA basis vector  v  1 for quarters Q6, Q10, and Q14 (top) and an associated color map of the leading PCA coefficient ﹩{c}_{i\leftarrow (x,y)}^{1}﹩ at each spatial cell position (bottom). The spatial structure of the leading coefficient term is persistent between quarters.
Paper: Robust Detrending of Spatially Correlated Systematics in Kepler Light Curves Using Low-rank Methods
Authors: Jamila S. Taaki, Athol J. Kemball, Farzad Kamalabadi
Figure caption: Basis vectors  V  (upper) and coefficients  C  (lower) used for the full simulation of light curves in experiment B using a rank K = 4 model. The basis vectors were selected at approximately equal spacing as index sets (1, 5, 11, 16) from the 16 Kepler CBV published for Q10 and channel 30 (Stumpe et al. 2012). The coefficient spatial dependence was simulated as a mixture of random smooth features and sharp discontinuities. Both components are arbitrarily chosen and the discontinuities are not constrained to match the Kepler module gridding.
Paper: Robust Detrending of Spatially Correlated Systematics in Kepler Light Curves Using Low-rank Methods
Authors: Jamila S. Taaki, Athol J. Kemball, Farzad Kamalabadi
Figure caption: Scaled mean correlation of injected signals and associated detrended light curves ﹩\bar{\rho }({{\boldsymbol{a}}}_{[m]},{{\boldsymbol{y}}}_{[m]}^{{\prime} })﹩ for Experiment A for sine, flare, and transit signal types m ∈ {s, t, f} (across columns) for each of five separate simulation runs (across rows). This mean correlation, defined in the main text, is plotted for the spatial systematics algorithm (blue) and the PCA decomposition method (red). The mean correlation is scaled by the maximum value achieved by either method; this maximum is shown in the legend of each subplot. The PCA algorithm is noniterative and is depicted as a straight line accordingly. The x-axis label is the iteration number of the spatial systematics algorithm. The spatial systematics algorithm is generally convergent and typically has comparable or improved performance relative to PCA but this is not universal for all runs.
Paper: Robust Detrending of Spatially Correlated Systematics in Kepler Light Curves Using Low-rank Methods
Authors: Jamila S. Taaki, Athol J. Kemball, Farzad Kamalabadi
Figure caption: Estimated (left) and known simulated (right) basis vectors  v   k , k ∈ {1,..,8} for Experiment B. The estimated basis vectors (left) are shown for the spatial systematics algorithm (blue) and the reference PCA method (red). The x-axis is in units of Kepler long-cadence time sample. The estimated spatial and PCA basis vectors (left) for the first four terms overlap one another in these plots.
Paper: Robust Detrending of Spatially Correlated Systematics in Kepler Light Curves Using Low-rank Methods
Authors: Jamila S. Taaki, Athol J. Kemball, Farzad Kamalabadi
Figure caption: Example simulated sine  a   s , transit  a   t , and flare  a   f  signals as defined in Section 2.5.3. The inset panel (blue outline) shows the tapered transit profile at higher temporal resolution.
Paper: Robust Detrending of Spatially Correlated Systematics in Kepler Light Curves Using Low-rank Methods
Authors: Jamila S. Taaki, Athol J. Kemball, Farzad Kamalabadi
Figure caption: Spatial correlation structure within modules for Q6, Q10, and Q14 across the (30 × 50) gridded region of the Kepler sensor. The module number is shown in the top left corner of each module. The mean pairwise correlation ﹩{\bar{\rho }}_{M}﹩ within each module is tabulated in black. The difference ﹩{\bar{\rho }}_{{M}_{\mathrm{XY}}}-{\bar{\rho }}_{M}﹩ is tabulated in red, where ﹩{\bar{\rho }}_{{M}_{\mathrm{XY}}}﹩ is the mean pairwise correlation of neighboring light curves within each module. The shaded color intensity is proportional to ﹩{\bar{\rho }}_{{M}_{\mathrm{XY}}}﹩. In most modules, the correlation between neighboring light curves is greater than the mean pairwise correlation between all pairs of light curves on the module.
Paper: Robust Detrending of Spatially Correlated Systematics in Kepler Light Curves Using Low-rank Methods
Authors: Jamila S. Taaki, Athol J. Kemball, Farzad Kamalabadi
Figure caption: Basis vector coefficients ﹩{c}_{i}^{k},k\in \{1,..,5\}(K=20)﹩ for light curve i → (x, y) ∈ (X, Y) obtained using the spatial systematics (top row) and PCA algorithms (bottom row) for run #0, a representative run of Experiment A. The coefficient index k is shown in the top left of each subfigure. The x- and y-axes are in units of gridded spatial cells.
Paper: VLTI/GRAVITY Provides Evidence the Young, Substellar Companion HD 136164 Ab Formed Like a “Failed Star”
Authors: William O. Balmer, L. Pueyo, S. Lacour, J. J. Wang, T. Stolker, J. Kammerer, N. Pourré, M. Nowak, E. Rickman, S. Blunt, A. Sivaramakrishnan, D. Sing, K. Wagner, G.-D. Marleau, A.-M. Lagrange, R. Abuter, A. Amorim, R. Asensio-Torres, J.-P. Berger, H. Beust, A. Boccaletti, A. Bohn, M. Bonnefoy, H. Bonnet, M. S. Bordoni, G. Bourdarot, W. Brandner, F. Cantalloube, P. Caselli, B. Charnay, G. Chauvin, A. Chavez, E. Choquet, V. Christiaens, Y. Clénet, V. Coudé du Foresto, A. Cridland, R. Davies, R. Dembet, A. Drescher, G. Duvert, A. Eckart, F. Eisenhauer, N. M. Förster Schreiber, P. Garcia, R. Garcia Lopez, E. Gendron, R. Genzel, S. Gillessen, J. H. Girard, S. Grant, X. Haubois, G. Heißel, Th. Henning, S. Hinkley, S. Hippler, M. Houllé, Z. Hubert, L. Jocou, M. Keppler, P. Kervella, L. Kreidberg, N. T. Kurtovic, V. Lapeyrère, J.-B. Le Bouquin, P. Léna, D. Lutz, A.-L. Maire, F. Mang, A. Mérand, P. Mollière, C. Mordasini, D. Mouillet, E. Nasedkin, T. Ott, G. P. P. L. Otten, C. Paladini, T. Paumard, K. Perraut, G. Perrin, O. Pfuhl, D. C. Ribeiro, L. Rodet, Z. Rustamkulov, J. Shangguan, T. Shimizu, C. Straubmeier, E. Sturm, L. J. Tacconi, A. Vigan, F. Vincent, K. Ward-Duong, F. Widmann, T. Winterhalder, J. Woillez, S. Yazici
Figure caption: The spectrum of HD 136164 Ab (black data points) fit to the cloudless ATMO equilibrium chemistry self-consistent model, with and without a prior on the dynamical mass of the companion (median samples are plotted as blue and red curves, respectively). 30 random samples from each posterior distribution are plotted as semitransparent curves. In each fit, the SPHERE YJH1 data are allowed to scale by a factor, so for the fit with a dynamical mass prior, the scaled SPHERE data are shown as black circles, and without a dynamical mass prior, they are shifted to the right for visualization as gray squares. The SPHERE and GRAVITY spectra are available as the data behind the figure. (The data used to create this figure are available.)
Paper: VLTI/GRAVITY Provides Evidence the Young, Substellar Companion HD 136164 Ab Formed Like a “Failed Star”
Authors: William O. Balmer, L. Pueyo, S. Lacour, J. J. Wang, T. Stolker, J. Kammerer, N. Pourré, M. Nowak, E. Rickman, S. Blunt, A. Sivaramakrishnan, D. Sing, K. Wagner, G.-D. Marleau, A.-M. Lagrange, R. Abuter, A. Amorim, R. Asensio-Torres, J.-P. Berger, H. Beust, A. Boccaletti, A. Bohn, M. Bonnefoy, H. Bonnet, M. S. Bordoni, G. Bourdarot, W. Brandner, F. Cantalloube, P. Caselli, B. Charnay, G. Chauvin, A. Chavez, E. Choquet, V. Christiaens, Y. Clénet, V. Coudé du Foresto, A. Cridland, R. Davies, R. Dembet, A. Drescher, G. Duvert, A. Eckart, F. Eisenhauer, N. M. Förster Schreiber, P. Garcia, R. Garcia Lopez, E. Gendron, R. Genzel, S. Gillessen, J. H. Girard, S. Grant, X. Haubois, G. Heißel, Th. Henning, S. Hinkley, S. Hippler, M. Houllé, Z. Hubert, L. Jocou, M. Keppler, P. Kervella, L. Kreidberg, N. T. Kurtovic, V. Lapeyrère, J.-B. Le Bouquin, P. Léna, D. Lutz, A.-L. Maire, F. Mang, A. Mérand, P. Mollière, C. Mordasini, D. Mouillet, E. Nasedkin, T. Ott, G. P. P. L. Otten, C. Paladini, T. Paumard, K. Perraut, G. Perrin, O. Pfuhl, D. C. Ribeiro, L. Rodet, Z. Rustamkulov, J. Shangguan, T. Shimizu, C. Straubmeier, E. Sturm, L. J. Tacconi, A. Vigan, F. Vincent, K. Ward-Duong, F. Widmann, T. Winterhalder, J. Woillez, S. Yazici
Figure caption: HD 136164 orbital analysis. Top left: the visual orbit of HD 136164 Ab around HD 136164 A (black star). 1000 randomly chosen orbits from our fit using the MCMC are shown in color, with the color corresponding to the eccentricity of a given orbit. Top middle and right: the proper motion of the host star HD 136164 A over time in R.A. and decl. (middle and right, respectively). The proper motion of the host as predicted by the orbit fit is shown in curves colored corresponding to the mass of the companion. Observations from Hipparcos and Gaia are shown with error bars as recorded in the HGCA. Note that the orbitize! proper-motion log-likelihood function evaluates the time-averaged proper motions, and not the instantaneous proper motions that are overplotted here (see Hinkley et al. 2023); the instantaneous measurements are shown here for visualization purposes only. Bottom: VLTI/GRAVITY measurements of the position of HD 136164 Ab across four epochs (see Table 2), plotted against the same sample of MCMC orbits as in the top left panel. The 1, 2, and 3σ confidence contours on each measurement are shown with decreasing transparency; the covariance of the measurement is related to the u–v plane coverage of the observation.
Paper: VLTI/GRAVITY Provides Evidence the Young, Substellar Companion HD 136164 Ab Formed Like a “Failed Star”
Authors: William O. Balmer, L. Pueyo, S. Lacour, J. J. Wang, T. Stolker, J. Kammerer, N. Pourré, M. Nowak, E. Rickman, S. Blunt, A. Sivaramakrishnan, D. Sing, K. Wagner, G.-D. Marleau, A.-M. Lagrange, R. Abuter, A. Amorim, R. Asensio-Torres, J.-P. Berger, H. Beust, A. Boccaletti, A. Bohn, M. Bonnefoy, H. Bonnet, M. S. Bordoni, G. Bourdarot, W. Brandner, F. Cantalloube, P. Caselli, B. Charnay, G. Chauvin, A. Chavez, E. Choquet, V. Christiaens, Y. Clénet, V. Coudé du Foresto, A. Cridland, R. Davies, R. Dembet, A. Drescher, G. Duvert, A. Eckart, F. Eisenhauer, N. M. Förster Schreiber, P. Garcia, R. Garcia Lopez, E. Gendron, R. Genzel, S. Gillessen, J. H. Girard, S. Grant, X. Haubois, G. Heißel, Th. Henning, S. Hinkley, S. Hippler, M. Houllé, Z. Hubert, L. Jocou, M. Keppler, P. Kervella, L. Kreidberg, N. T. Kurtovic, V. Lapeyrère, J.-B. Le Bouquin, P. Léna, D. Lutz, A.-L. Maire, F. Mang, A. Mérand, P. Mollière, C. Mordasini, D. Mouillet, E. Nasedkin, T. Ott, G. P. P. L. Otten, C. Paladini, T. Paumard, K. Perraut, G. Perrin, O. Pfuhl, D. C. Ribeiro, L. Rodet, Z. Rustamkulov, J. Shangguan, T. Shimizu, C. Straubmeier, E. Sturm, L. J. Tacconi, A. Vigan, F. Vincent, K. Ward-Duong, F. Widmann, T. Winterhalder, J. Woillez, S. Yazici
Figure caption: Detections of HD 136164 Ab with VLTI/GRAVITY. Each panel visualizes the χ 2 map calculated after subtracting the stellar contamination. Each epoch in Table 1 is presented chronologically, left to right. The dashed gray circle indicates the fiber’s field of view. The origin is the placement of the science fiber on sky for a given observation, a prediction based on the previous available orbit fit, and the units are in ΔR.A. and Δdecl., e.g., the displacement of the fiber with respect to the host star HD 136164 A. The strongest peak in the χ 2 map (indicated with a blue arrow) reveals the position of the companion, with characteristic interferometric side lobes whose shape and distribution depend on the u–v plane coverage.
Paper: VLTI/GRAVITY Provides Evidence the Young, Substellar Companion HD 136164 Ab Formed Like a “Failed Star”
Authors: William O. Balmer, L. Pueyo, S. Lacour, J. J. Wang, T. Stolker, J. Kammerer, N. Pourré, M. Nowak, E. Rickman, S. Blunt, A. Sivaramakrishnan, D. Sing, K. Wagner, G.-D. Marleau, A.-M. Lagrange, R. Abuter, A. Amorim, R. Asensio-Torres, J.-P. Berger, H. Beust, A. Boccaletti, A. Bohn, M. Bonnefoy, H. Bonnet, M. S. Bordoni, G. Bourdarot, W. Brandner, F. Cantalloube, P. Caselli, B. Charnay, G. Chauvin, A. Chavez, E. Choquet, V. Christiaens, Y. Clénet, V. Coudé du Foresto, A. Cridland, R. Davies, R. Dembet, A. Drescher, G. Duvert, A. Eckart, F. Eisenhauer, N. M. Förster Schreiber, P. Garcia, R. Garcia Lopez, E. Gendron, R. Genzel, S. Gillessen, J. H. Girard, S. Grant, X. Haubois, G. Heißel, Th. Henning, S. Hinkley, S. Hippler, M. Houllé, Z. Hubert, L. Jocou, M. Keppler, P. Kervella, L. Kreidberg, N. T. Kurtovic, V. Lapeyrère, J.-B. Le Bouquin, P. Léna, D. Lutz, A.-L. Maire, F. Mang, A. Mérand, P. Mollière, C. Mordasini, D. Mouillet, E. Nasedkin, T. Ott, G. P. P. L. Otten, C. Paladini, T. Paumard, K. Perraut, G. Perrin, O. Pfuhl, D. C. Ribeiro, L. Rodet, Z. Rustamkulov, J. Shangguan, T. Shimizu, C. Straubmeier, E. Sturm, L. J. Tacconi, A. Vigan, F. Vincent, K. Ward-Duong, F. Widmann, T. Winterhalder, J. Woillez, S. Yazici
Figure caption: Left: mass vs. effective temperature for our atmospheric fits (contours) compared to the mass–radius relationship from the ATMO2020 evolutionary model (black curve). The uncertainty on the system’s age is represented by gray contours to the black curve, 16 ± 2 Myr. When the dynamical mass is included as a prior in the atmospheric model fit, the mass and effective temperature are consistent with the evolutionary model prediction to within 1σ. Right: mass vs. radius for our atmospheric fits compared to the mass–radius relationship from the evolutionary model. Without a dynamical mass prior, our spectral fits derive a ﹩\mathrm{log}(g)﹩ that results in a mass inconsistent with expectations from the evolutionary model. With a dynamical mass prior, the determined ﹩\mathrm{log}(g)﹩ is consistent with expectations to within 1σ.
Paper: VLTI/GRAVITY Provides Evidence the Young, Substellar Companion HD 136164 Ab Formed Like a “Failed Star”
Authors: William O. Balmer, L. Pueyo, S. Lacour, J. J. Wang, T. Stolker, J. Kammerer, N. Pourré, M. Nowak, E. Rickman, S. Blunt, A. Sivaramakrishnan, D. Sing, K. Wagner, G.-D. Marleau, A.-M. Lagrange, R. Abuter, A. Amorim, R. Asensio-Torres, J.-P. Berger, H. Beust, A. Boccaletti, A. Bohn, M. Bonnefoy, H. Bonnet, M. S. Bordoni, G. Bourdarot, W. Brandner, F. Cantalloube, P. Caselli, B. Charnay, G. Chauvin, A. Chavez, E. Choquet, V. Christiaens, Y. Clénet, V. Coudé du Foresto, A. Cridland, R. Davies, R. Dembet, A. Drescher, G. Duvert, A. Eckart, F. Eisenhauer, N. M. Förster Schreiber, P. Garcia, R. Garcia Lopez, E. Gendron, R. Genzel, S. Gillessen, J. H. Girard, S. Grant, X. Haubois, G. Heißel, Th. Henning, S. Hinkley, S. Hippler, M. Houllé, Z. Hubert, L. Jocou, M. Keppler, P. Kervella, L. Kreidberg, N. T. Kurtovic, V. Lapeyrère, J.-B. Le Bouquin, P. Léna, D. Lutz, A.-L. Maire, F. Mang, A. Mérand, P. Mollière, C. Mordasini, D. Mouillet, E. Nasedkin, T. Ott, G. P. P. L. Otten, C. Paladini, T. Paumard, K. Perraut, G. Perrin, O. Pfuhl, D. C. Ribeiro, L. Rodet, Z. Rustamkulov, J. Shangguan, T. Shimizu, C. Straubmeier, E. Sturm, L. J. Tacconi, A. Vigan, F. Vincent, K. Ward-Duong, F. Widmann, T. Winterhalder, J. Woillez, S. Yazici
Figure caption: The spectrum of HD 136164 Ab (black data points) fit to the cloudless SPHINX equilibrium chemistry self-consistent model, which varies abundance in addition to effective temperature and surface gravity, with and without a prior on the dynamical mass of the companion (median samples are plotted as blue and red curves, respectively). 30 random samples from each posterior distribution are plotted as semitransparent curves. In each fit, the SPHERE YJH1 data are allowed to scale by a factor, so for the fit with the dynamical mass prior, the scaled SPHERE data are shown as black circles, and without the dynamical mass prior, they are shifted to the right for visualization as gray squares.