adsabs/AstroCLIMB huggingface dataset:
Paper: Validating AU Microscopii d with Transit Timing Variations
Authors: Justin M. Wittrock, Peter P. Plavchan, Bryson L. Cale, Thomas Barclay, Mathis R. Ludwig, Richard P. Schwarz, Djamel Mékarnia, Amaury H. M. J. Triaud, Lyu Abe, Olga Suarez, Tristan Guillot, Dennis M. Conti, Karen A. Collins, Ian A. Waite, John F. Kielkopf, Kevin I. Collins, Stefan Dreizler, Mohammed El Mufti, Dax L. Feliz, Eric Gaidos, Claire S. Geneser, Keith D. Horne, Stephen R. Kane, Patrick J. Lowrance, Eder Martioli, Don J. Radford, Michael A. Reefe, Veronica Roccatagliata, Avi Shporer, Keivan G. Stassun, Christopher Stockdale, Thiam-Guan Tan, Angelle M. Tanner, Laura D. Vega
Figure caption: Histograms of the semimajor axis of AU Mic d with SPOCK (top left), MEGNO (top right), and Nbody (bottom), each marked with the corresponding orbital periods of AU Mic d. SPOCK and Nbody estimates the stability probability after 109 and 2 × 105 orbits, respectively, of the innermost planet, while MEGNO is a fast indicator for chaotic orbits. For each parameter set, 20,000 random configurations of masses and orbital parameters were generated following the respective Gaussian distributions of planetary parameters from Exo-Striker; each of these random configurations was given its own stability probability by SPOCK, and the semimajor axis of AU Mic d is then plotted in the histogram for each of these configurations. Since the same number of random configurations was generated for each parameter set, the result is a mixture distribution in which the respective underlying distributions have the same weighting. The values were then weighted with the stability probability in the histogram, resulting in the overlapping histogram for SPOCK, MEGNO, and Nbody. Thus, each histogram contains 200,000 values. Nbody uses the same aforementioned simulation object generated by rebound to perform Nbody simulations and outputs either 0 (unstable) or 1 (stable); these outputs are then used for weighting. Nbody is more accurate than SPOCK but is much more computationally intensive over a large simulation time, so both the 200,000-orbit integrations were performed and the pretrained classifier was used. The MEGNO value threshold is set to 2.1, so any configurations that lead to their MEGNO value exceeding this threshold are considered unstable and given a weight of 0 while all other configurations that are considered stable are given a weight of 1. By weighting with the SPOCK or MEGNO outputs, the 5.64 days case appears to be favored over other inner d cases, and both 12.6 and 12.7 days appear to be preferred among the middle d cases.
Paper: Validating AU Microscopii d with Transit Timing Variations
Authors: Justin M. Wittrock, Peter P. Plavchan, Bryson L. Cale, Thomas Barclay, Mathis R. Ludwig, Richard P. Schwarz, Djamel Mékarnia, Amaury H. M. J. Triaud, Lyu Abe, Olga Suarez, Tristan Guillot, Dennis M. Conti, Karen A. Collins, Ian A. Waite, John F. Kielkopf, Kevin I. Collins, Stefan Dreizler, Mohammed El Mufti, Dax L. Feliz, Eric Gaidos, Claire S. Geneser, Keith D. Horne, Stephen R. Kane, Patrick J. Lowrance, Eder Martioli, Don J. Radford, Michael A. Reefe, Veronica Roccatagliata, Avi Shporer, Keivan G. Stassun, Christopher Stockdale, Thiam-Guan Tan, Angelle M. Tanner, Laura D. Vega
Figure caption:  rebound models of the stability of the AU Mic system on a timescale of 20 Myr for a two-planet high-eccentricity configuration with original K’s from Table 12 (left) and with K’s from Cale et al. (2021) RV models (right), due to the original K’s being very small (<0.07 m s−1). While the original K’s case appears to be stable, both planets’ orbits become increasingly eccentric over time, and both planets would quickly become nontransiting due to their increasing orbital misalignment. The RV K’s case exhibits signs of chaos in the AU Mic system, with the planets undergoing orbital migrations but no orbital crossing, their eccentricities being extremely erratic throughout, rapidly oscillating between 0 and 1, and their highly fluctuating inclinations frequently placing both transiting planets in nontransiting configurations.
Paper: Validating AU Microscopii d with Transit Timing Variations
Authors: Justin M. Wittrock, Peter P. Plavchan, Bryson L. Cale, Thomas Barclay, Mathis R. Ludwig, Richard P. Schwarz, Djamel Mékarnia, Amaury H. M. J. Triaud, Lyu Abe, Olga Suarez, Tristan Guillot, Dennis M. Conti, Karen A. Collins, Ian A. Waite, John F. Kielkopf, Kevin I. Collins, Stefan Dreizler, Mohammed El Mufti, Dax L. Feliz, Eric Gaidos, Claire S. Geneser, Keith D. Horne, Stephen R. Kane, Patrick J. Lowrance, Eder Martioli, Don J. Radford, Michael A. Reefe, Veronica Roccatagliata, Avi Shporer, Keivan G. Stassun, Christopher Stockdale, Thiam-Guan Tan, Angelle M. Tanner, Laura D. Vega
Figure caption: TTV log-likelihood periodograms of AU Mic d’s orbital period using the parameters from Table 14 as the starting point and initial inclinations i d = 85° (top) and 90° (bottom). We obtained the six most favored inner d periods based on their log-likelihood: 5.08 days (﹩\mathrm{ln}{ \mathcal L }﹩ = 208.22 and 208.84), 5.39 days (﹩\mathrm{ln}{ \mathcal L }﹩ = 209.99 and 209.80), 5.64 days (﹩\mathrm{ln}{ \mathcal L }﹩ = 209.65 and 209.62), 5.86 days (﹩\mathrm{ln}{ \mathcal L }﹩ = 214.36 and 214.33), 6.20 days (﹩\mathrm{ln}{ \mathcal L }﹩ = 209.95 and 208.43), and 6.47 days (﹩\mathrm{ln}{ \mathcal L }﹩ = 207.76 and 211.40) from both respective inclination cases. The red lines denote those periods corresponding to best-fitting peaks in the periodograms.
Paper: Validating AU Microscopii d with Transit Timing Variations
Authors: Justin M. Wittrock, Peter P. Plavchan, Bryson L. Cale, Thomas Barclay, Mathis R. Ludwig, Richard P. Schwarz, Djamel Mékarnia, Amaury H. M. J. Triaud, Lyu Abe, Olga Suarez, Tristan Guillot, Dennis M. Conti, Karen A. Collins, Ian A. Waite, John F. Kielkopf, Kevin I. Collins, Stefan Dreizler, Mohammed El Mufti, Dax L. Feliz, Eric Gaidos, Claire S. Geneser, Keith D. Horne, Stephen R. Kane, Patrick J. Lowrance, Eder Martioli, Don J. Radford, Michael A. Reefe, Veronica Roccatagliata, Avi Shporer, Keivan G. Stassun, Christopher Stockdale, Thiam-Guan Tan, Angelle M. Tanner, Laura D. Vega
Figure caption: TTV periodograms of AU Mic d’s orbital period using the parameters from Table 15 as the starting point and initial inclinations i d = 80° (top) and 90° (bottom). We obtained the four most favored periods based on their log-likelihood: 11.9 days (﹩\mathrm{ln}{ \mathcal L }﹩ = 208.16) and 14.1 days (﹩\mathrm{ln}{ \mathcal L }﹩ = 201.45) from the initial i d = 80° case, and 12.6 days (﹩\mathrm{ln}{ \mathcal L }﹩ = 209.21 and 205.70) and 12.7 days (﹩\mathrm{ln}{ \mathcal L }﹩ = 211.25 and 209.79) from both respective inclination cases. The red lines denote those days corresponding to best-fitting peaks in the periodograms.
Paper: Validating AU Microscopii d with Transit Timing Variations
Authors: Justin M. Wittrock, Peter P. Plavchan, Bryson L. Cale, Thomas Barclay, Mathis R. Ludwig, Richard P. Schwarz, Djamel Mékarnia, Amaury H. M. J. Triaud, Lyu Abe, Olga Suarez, Tristan Guillot, Dennis M. Conti, Karen A. Collins, Ian A. Waite, John F. Kielkopf, Kevin I. Collins, Stefan Dreizler, Mohammed El Mufti, Dax L. Feliz, Eric Gaidos, Claire S. Geneser, Keith D. Horne, Stephen R. Kane, Patrick J. Lowrance, Eder Martioli, Don J. Radford, Michael A. Reefe, Veronica Roccatagliata, Avi Shporer, Keivan G. Stassun, Christopher Stockdale, Thiam-Guan Tan, Angelle M. Tanner, Laura D. Vega
Figure caption:  O−C diagrams of AU Mic b (left) and AU Mic c (right), with comparison between TTVs (green) and Exo-Striker-generated MCMC models (black) for a two-planet low-eccentricity configuration.
Paper: Validating AU Microscopii d with Transit Timing Variations
Authors: Justin M. Wittrock, Peter P. Plavchan, Bryson L. Cale, Thomas Barclay, Mathis R. Ludwig, Richard P. Schwarz, Djamel Mékarnia, Amaury H. M. J. Triaud, Lyu Abe, Olga Suarez, Tristan Guillot, Dennis M. Conti, Karen A. Collins, Ian A. Waite, John F. Kielkopf, Kevin I. Collins, Stefan Dreizler, Mohammed El Mufti, Dax L. Feliz, Eric Gaidos, Claire S. Geneser, Keith D. Horne, Stephen R. Kane, Patrick J. Lowrance, Eder Martioli, Don J. Radford, Michael A. Reefe, Veronica Roccatagliata, Avi Shporer, Keivan G. Stassun, Christopher Stockdale, Thiam-Guan Tan, Angelle M. Tanner, Laura D. Vega
Figure caption:  O−C diagrams of AU Mic b (left) and AU Mic c (right), with comparison between TTVs (green) and Exo-Striker-generated MCMC models (black) for P d = 12.7 days.
Paper: Validating AU Microscopii d with Transit Timing Variations
Authors: Justin M. Wittrock, Peter P. Plavchan, Bryson L. Cale, Thomas Barclay, Mathis R. Ludwig, Richard P. Schwarz, Djamel Mékarnia, Amaury H. M. J. Triaud, Lyu Abe, Olga Suarez, Tristan Guillot, Dennis M. Conti, Karen A. Collins, Ian A. Waite, John F. Kielkopf, Kevin I. Collins, Stefan Dreizler, Mohammed El Mufti, Dax L. Feliz, Eric Gaidos, Claire S. Geneser, Keith D. Horne, Stephen R. Kane, Patrick J. Lowrance, Eder Martioli, Don J. Radford, Michael A. Reefe, Veronica Roccatagliata, Avi Shporer, Keivan G. Stassun, Christopher Stockdale, Thiam-Guan Tan, Angelle M. Tanner, Laura D. Vega
Figure caption: Corner plot of AU Mic b and c’s orbital parameters from Exo-Striker MCMC analysis for a two-planet low-eccentricity configuration.
Paper: Validating AU Microscopii d with Transit Timing Variations
Authors: Justin M. Wittrock, Peter P. Plavchan, Bryson L. Cale, Thomas Barclay, Mathis R. Ludwig, Richard P. Schwarz, Djamel Mékarnia, Amaury H. M. J. Triaud, Lyu Abe, Olga Suarez, Tristan Guillot, Dennis M. Conti, Karen A. Collins, Ian A. Waite, John F. Kielkopf, Kevin I. Collins, Stefan Dreizler, Mohammed El Mufti, Dax L. Feliz, Eric Gaidos, Claire S. Geneser, Keith D. Horne, Stephen R. Kane, Patrick J. Lowrance, Eder Martioli, Don J. Radford, Michael A. Reefe, Veronica Roccatagliata, Avi Shporer, Keivan G. Stassun, Christopher Stockdale, Thiam-Guan Tan, Angelle M. Tanner, Laura D. Vega
Figure caption: Initial three-planet (with d between b and c) best-fit O − C diagrams of AU Mic b (top) and AU Mic c (bottom), with comparison between TTVs (green) and Exo-Striker-generated MCMC models (black).
Paper: Validating AU Microscopii d with Transit Timing Variations
Authors: Justin M. Wittrock, Peter P. Plavchan, Bryson L. Cale, Thomas Barclay, Mathis R. Ludwig, Richard P. Schwarz, Djamel Mékarnia, Amaury H. M. J. Triaud, Lyu Abe, Olga Suarez, Tristan Guillot, Dennis M. Conti, Karen A. Collins, Ian A. Waite, John F. Kielkopf, Kevin I. Collins, Stefan Dreizler, Mohammed El Mufti, Dax L. Feliz, Eric Gaidos, Claire S. Geneser, Keith D. Horne, Stephen R. Kane, Patrick J. Lowrance, Eder Martioli, Don J. Radford, Michael A. Reefe, Veronica Roccatagliata, Avi Shporer, Keivan G. Stassun, Christopher Stockdale, Thiam-Guan Tan, Angelle M. Tanner, Laura D. Vega
Figure caption: Initial three-planet (with d interior to b) best-fit O−C diagrams of AU Mic b (top) and AU Mic c (bottom), with comparison between TTVs (green) and Exo-Striker-generated MCMC models (black).
Paper: Validating AU Microscopii d with Transit Timing Variations
Authors: Justin M. Wittrock, Peter P. Plavchan, Bryson L. Cale, Thomas Barclay, Mathis R. Ludwig, Richard P. Schwarz, Djamel Mékarnia, Amaury H. M. J. Triaud, Lyu Abe, Olga Suarez, Tristan Guillot, Dennis M. Conti, Karen A. Collins, Ian A. Waite, John F. Kielkopf, Kevin I. Collins, Stefan Dreizler, Mohammed El Mufti, Dax L. Feliz, Eric Gaidos, Claire S. Geneser, Keith D. Horne, Stephen R. Kane, Patrick J. Lowrance, Eder Martioli, Don J. Radford, Michael A. Reefe, Veronica Roccatagliata, Avi Shporer, Keivan G. Stassun, Christopher Stockdale, Thiam-Guan Tan, Angelle M. Tanner, Laura D. Vega
Figure caption:                    ﹩\mathrm{ln}{ \mathcal L }﹩ brute-force periodogram of AU Mic’s RVs, including models for both AU Mic b and c. AU Mic d’s T  C  was allowed to vary. The dotted vertical lines, from right to left, are P b, 2*P rot, P d = 12.74 days, P d = 13.31 days, 3*P rot, P c, P candidate = 65.22 days. There appears to be no obvious peaks consistent with d’s periods derived from the TTVs, but there is additional power in the periodogram, particularly near 12.75 and 13.3 days. Also note that the 22 days peak would not be dynamically stable, and that there is the possibility of a 65 days planetary candidate in the RVs.
Paper: Validating AU Microscopii d with Transit Timing Variations
Authors: Justin M. Wittrock, Peter P. Plavchan, Bryson L. Cale, Thomas Barclay, Mathis R. Ludwig, Richard P. Schwarz, Djamel Mékarnia, Amaury H. M. J. Triaud, Lyu Abe, Olga Suarez, Tristan Guillot, Dennis M. Conti, Karen A. Collins, Ian A. Waite, John F. Kielkopf, Kevin I. Collins, Stefan Dreizler, Mohammed El Mufti, Dax L. Feliz, Eric Gaidos, Claire S. Geneser, Keith D. Horne, Stephen R. Kane, Patrick J. Lowrance, Eder Martioli, Don J. Radford, Michael A. Reefe, Veronica Roccatagliata, Avi Shporer, Keivan G. Stassun, Christopher Stockdale, Thiam-Guan Tan, Angelle M. Tanner, Laura D. Vega
Figure caption: GLS periodograms of the AU Mic system. Top four panels: GLS generated without HARPS data. Bottom four panels: GLS generated with HARPS data. From top to bottom: zero-point corrected, activity corrected, planet b corrected, planet c corrected. The dotted vertical lines, from right to left, are P b, 2*P rot, P d = 12.74 days, P d = 13.31 days, 3*P rot, P c, P candidate = 65.22 days. AU Mic d’s signal vanishes when HARPS data are added to the GLS periodogram. Also, the 16 days peak in the bottom row of the periodogram is not credible in term of orbital dynamics stability.
Paper: Validating AU Microscopii d with Transit Timing Variations
Authors: Justin M. Wittrock, Peter P. Plavchan, Bryson L. Cale, Thomas Barclay, Mathis R. Ludwig, Richard P. Schwarz, Djamel Mékarnia, Amaury H. M. J. Triaud, Lyu Abe, Olga Suarez, Tristan Guillot, Dennis M. Conti, Karen A. Collins, Ian A. Waite, John F. Kielkopf, Kevin I. Collins, Stefan Dreizler, Mohammed El Mufti, Dax L. Feliz, Eric Gaidos, Claire S. Geneser, Keith D. Horne, Stephen R. Kane, Patrick J. Lowrance, Eder Martioli, Don J. Radford, Michael A. Reefe, Veronica Roccatagliata, Avi Shporer, Keivan G. Stassun, Christopher Stockdale, Thiam-Guan Tan, Angelle M. Tanner, Laura D. Vega
Figure caption: Raw TESS photometry of AU Mic overlaid with observed transits of AU Mic b (red) and c (blue) and range of predicted transit midpoint times for AU Mic d (green). This case is for P d = 12.7 days. Left panel is from Cycle 1, and right panel is from Cycle 3. Owing to AU Mic d’s estimated 160 ppm depth and AU Mic’s intense stellar activity, the potential transit signatures from AU Mic d are not readily apparent by eye, nor detectable at high statistical significance in the TESS light curve given the stellar activity and photon noise.
Paper: Validating AU Microscopii d with Transit Timing Variations
Authors: Justin M. Wittrock, Peter P. Plavchan, Bryson L. Cale, Thomas Barclay, Mathis R. Ludwig, Richard P. Schwarz, Djamel Mékarnia, Amaury H. M. J. Triaud, Lyu Abe, Olga Suarez, Tristan Guillot, Dennis M. Conti, Karen A. Collins, Ian A. Waite, John F. Kielkopf, Kevin I. Collins, Stefan Dreizler, Mohammed El Mufti, Dax L. Feliz, Eric Gaidos, Claire S. Geneser, Keith D. Horne, Stephen R. Kane, Patrick J. Lowrance, Eder Martioli, Don J. Radford, Michael A. Reefe, Veronica Roccatagliata, Avi Shporer, Keivan G. Stassun, Christopher Stockdale, Thiam-Guan Tan, Angelle M. Tanner, Laura D. Vega
Figure caption:  O−C diagrams of AU Mic b (left) and AU Mic c (right), with comparison between TTVs (green) and Exo-Striker-generated MCMC models (black) for P d = 5.08 days (top row), 5.39 days (middle row), and 5.64 days (bottom row).
Paper: Validating AU Microscopii d with Transit Timing Variations
Authors: Justin M. Wittrock, Peter P. Plavchan, Bryson L. Cale, Thomas Barclay, Mathis R. Ludwig, Richard P. Schwarz, Djamel Mékarnia, Amaury H. M. J. Triaud, Lyu Abe, Olga Suarez, Tristan Guillot, Dennis M. Conti, Karen A. Collins, Ian A. Waite, John F. Kielkopf, Kevin I. Collins, Stefan Dreizler, Mohammed El Mufti, Dax L. Feliz, Eric Gaidos, Claire S. Geneser, Keith D. Horne, Stephen R. Kane, Patrick J. Lowrance, Eder Martioli, Don J. Radford, Michael A. Reefe, Veronica Roccatagliata, Avi Shporer, Keivan G. Stassun, Christopher Stockdale, Thiam-Guan Tan, Angelle M. Tanner, Laura D. Vega
Figure caption:  O−C diagrams of AU Mic b (left) and AU Mic c (right), with comparison between TTVs (green) and Exo-Striker-generated MCMC models (black) for 11.9 days (top row), 12.6 days (middle row), and 14.1 days (bottom row).
Paper: Validating AU Microscopii d with Transit Timing Variations
Authors: Justin M. Wittrock, Peter P. Plavchan, Bryson L. Cale, Thomas Barclay, Mathis R. Ludwig, Richard P. Schwarz, Djamel Mékarnia, Amaury H. M. J. Triaud, Lyu Abe, Olga Suarez, Tristan Guillot, Dennis M. Conti, Karen A. Collins, Ian A. Waite, John F. Kielkopf, Kevin I. Collins, Stefan Dreizler, Mohammed El Mufti, Dax L. Feliz, Eric Gaidos, Claire S. Geneser, Keith D. Horne, Stephen R. Kane, Patrick J. Lowrance, Eder Martioli, Don J. Radford, Michael A. Reefe, Veronica Roccatagliata, Avi Shporer, Keivan G. Stassun, Christopher Stockdale, Thiam-Guan Tan, Angelle M. Tanner, Laura D. Vega
Figure caption:  Exo-Striker-generated TTV models of AU Mic b (left) and c (right) projected over 10 yr since last observed transit of the AU Mic system for P d = 12.7 days. The observed TTVs (green) are included with the model (black).
Paper: Validating AU Microscopii d with Transit Timing Variations
Authors: Justin M. Wittrock, Peter P. Plavchan, Bryson L. Cale, Thomas Barclay, Mathis R. Ludwig, Richard P. Schwarz, Djamel Mékarnia, Amaury H. M. J. Triaud, Lyu Abe, Olga Suarez, Tristan Guillot, Dennis M. Conti, Karen A. Collins, Ian A. Waite, John F. Kielkopf, Kevin I. Collins, Stefan Dreizler, Mohammed El Mufti, Dax L. Feliz, Eric Gaidos, Claire S. Geneser, Keith D. Horne, Stephen R. Kane, Patrick J. Lowrance, Eder Martioli, Don J. Radford, Michael A. Reefe, Veronica Roccatagliata, Avi Shporer, Keivan G. Stassun, Christopher Stockdale, Thiam-Guan Tan, Angelle M. Tanner, Laura D. Vega
Figure caption: Corner plot of AU Mic b and c’s orbital parameters from Exo-Striker MCMC analysis for P d = 12.7 days.
Paper: Validating AU Microscopii d with Transit Timing Variations
Authors: Justin M. Wittrock, Peter P. Plavchan, Bryson L. Cale, Thomas Barclay, Mathis R. Ludwig, Richard P. Schwarz, Djamel Mékarnia, Amaury H. M. J. Triaud, Lyu Abe, Olga Suarez, Tristan Guillot, Dennis M. Conti, Karen A. Collins, Ian A. Waite, John F. Kielkopf, Kevin I. Collins, Stefan Dreizler, Mohammed El Mufti, Dax L. Feliz, Eric Gaidos, Claire S. Geneser, Keith D. Horne, Stephen R. Kane, Patrick J. Lowrance, Eder Martioli, Don J. Radford, Michael A. Reefe, Veronica Roccatagliata, Avi Shporer, Keivan G. Stassun, Christopher Stockdale, Thiam-Guan Tan, Angelle M. Tanner, Laura D. Vega
Figure caption:  O−C diagrams of AU Mic b (left) and AU Mic c (right), with comparison between TTVs (green) and Exo-Striker-generated MCMC models (black) for P d = 5.86 days (top row), 6.20 days (middle row), and 6.47 days (bottom row).
Paper: Validating AU Microscopii d with Transit Timing Variations
Authors: Justin M. Wittrock, Peter P. Plavchan, Bryson L. Cale, Thomas Barclay, Mathis R. Ludwig, Richard P. Schwarz, Djamel Mékarnia, Amaury H. M. J. Triaud, Lyu Abe, Olga Suarez, Tristan Guillot, Dennis M. Conti, Karen A. Collins, Ian A. Waite, John F. Kielkopf, Kevin I. Collins, Stefan Dreizler, Mohammed El Mufti, Dax L. Feliz, Eric Gaidos, Claire S. Geneser, Keith D. Horne, Stephen R. Kane, Patrick J. Lowrance, Eder Martioli, Don J. Radford, Michael A. Reefe, Veronica Roccatagliata, Avi Shporer, Keivan G. Stassun, Christopher Stockdale, Thiam-Guan Tan, Angelle M. Tanner, Laura D. Vega
Figure caption:  rebound model of the stability of the AU Mic system on a timescale of 2 Myr for P d = 12.7 days.
Paper: First VLTI/GRAVITY Observations of HIP 65426 b: Evidence for a Low or Moderate Orbital Eccentricity
Authors: Sarah Blunt, W. O. Balmer, J. J. Wang, S. Lacour, S. Petrus, G. Bourdarot, J. Kammerer, N. Pourré, E. Rickman, J. Shangguan, T. Winterhalder, R. Abuter, A. Amorim, R. Asensio-Torres, M. Benisty, J.-P. Berger, H. Beust, A. Boccaletti, A. Bohn, M. Bonnefoy, H. Bonnet, 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. Dembet, A. Drescher, G. Duvert, A. Eckart, F. Eisenhauer, H. Feuchtgruber, P. Garcia, R. Garcia Lopez, E. Gendron, R. Genzel, S. Gillessen, J. H. Girard, X. Haubois, G. Heißel, Th. Henning, S. Hinkley, S. Hippler, M. Horrobin, M. Houllé, Z. Hubert, L. Jocou, M. Keppler, P. Kervella, L. Kreidberg, A.-M. Lagrange, V. Lapeyrère, J.-B. Le Bouquin, P. Léna, D. Lutz, A.-L. Maire, F. Mang, G.-D. Marleau, A. Mérand, P. Mollière, J. D. Monnier, C. Mordasini, D. Mouillet, E. Nasedkin, M. Nowak, T. Ott, G. P. P. L. Otten, C. Paladini, T. Paumard, K. Perraut, G. Perrin, O. Pfuhl, L. Pueyo, J. Rameau, L. Rodet, Z. Rustamkulov, T. Shimizu, D. Sing, T. Stolker, C. Straubmeier, E. Sturm, L. J. Tacconi, E. F. van Dishoeck, A. Vigan, F. Vincent, K. Ward-Duong, F. Widmann, E. Wieprecht, E. Wiezorrek, J. Woillez, S. Yazici, A. Young
Figure caption: Corner plot of the posterior of the accepted orbit fit, using all data and assuming a uniform eccentricity prior. Diagonal panels show marginalized 1D histograms of posterior elements, and off-diagonal panels show 2D covariances between posterior elements. 1σ, 2σ, and 3σ contours are outlined in the covariance panels, and individual posterior samples outside of the 3σ boundaries are plotted directly as black dots. Takeaways: The 1D marginalized posterior distributions of the semimajor axis and inclination are well constrained. Strong covariances are apparent, in particular between the eccentricity, inclination, and semimajor axis.
Paper: First VLTI/GRAVITY Observations of HIP 65426 b: Evidence for a Low or Moderate Orbital Eccentricity
Authors: Sarah Blunt, W. O. Balmer, J. J. Wang, S. Lacour, S. Petrus, G. Bourdarot, J. Kammerer, N. Pourré, E. Rickman, J. Shangguan, T. Winterhalder, R. Abuter, A. Amorim, R. Asensio-Torres, M. Benisty, J.-P. Berger, H. Beust, A. Boccaletti, A. Bohn, M. Bonnefoy, H. Bonnet, 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. Dembet, A. Drescher, G. Duvert, A. Eckart, F. Eisenhauer, H. Feuchtgruber, P. Garcia, R. Garcia Lopez, E. Gendron, R. Genzel, S. Gillessen, J. H. Girard, X. Haubois, G. Heißel, Th. Henning, S. Hinkley, S. Hippler, M. Horrobin, M. Houllé, Z. Hubert, L. Jocou, M. Keppler, P. Kervella, L. Kreidberg, A.-M. Lagrange, V. Lapeyrère, J.-B. Le Bouquin, P. Léna, D. Lutz, A.-L. Maire, F. Mang, G.-D. Marleau, A. Mérand, P. Mollière, J. D. Monnier, C. Mordasini, D. Mouillet, E. Nasedkin, M. Nowak, T. Ott, G. P. P. L. Otten, C. Paladini, T. Paumard, K. Perraut, G. Perrin, O. Pfuhl, L. Pueyo, J. Rameau, L. Rodet, Z. Rustamkulov, T. Shimizu, D. Sing, T. Stolker, C. Straubmeier, E. Sturm, L. J. Tacconi, E. F. van Dishoeck, A. Vigan, F. Vincent, K. Ward-Duong, F. Widmann, E. Wieprecht, E. Wiezorrek, J. Woillez, S. Yazici, A. Young
Figure caption: Results of forward modeling the photometric and spectral data of HIP 65426 b by comparing with the BT-SETTL CIFIST model grid. Posteriors over the free parameters in the fit, as well radius, a derived parameter, are shown. Fits performed using GRAVITY K-band spectra are shown in purple, and fits performed using SINFONI K-band spectra are shown in pink. The GP hyperparameters (defined as in Equation (4) in Wang et al. 2020) to the SPHERE IFS spectral data (length scale and amplitude) are shown as well. Takeaways: As expected, ﹩\mathrm{log}g﹩ correlates strongly with radius and T eff. Two families of solutions are apparent at high (1.3 R  J ) and low (0.9 R  J ) radii.