adsabs/AstroCLIMB huggingface dataset:
Paper: Verification of Gaia Data Release 3 Single-lined Spectroscopic Binary Solutions With Three Transiting Low-mass Secondaries
Authors: Stephen P. Schmidt, Kevin C. Schlaufman, Keyi Ding, 可怿 丁, Samuel K. Grunblatt, Theron Carmichael, Allyson Bieryla, Joseph E. Rodriguez, Jack Schulte, Noah Vowell, George Zhou, Samuel N. Quinn, Samuel W. Yee, Joshua N. Winn, Joel D. Hartman, David W. Latham, Douglas A. Caldwell, M. M. Fausnaugh, Christina Hedges, Jon M. Jenkins, Hugh P. Osborn, S. Seager
Figure caption: TESS FFI approximately 2048 × 2048 pixel postage stamps for TOI-1712, TOI-2533, and TOI-5427. TESS collected the FFI for TOI-1712 during Sector 20, the FFI for TOI-2533 during Sector 23, and the FFI for TOI-5427 during Sector 6. We center each postage stamp on the target and mark each G < 15 Gaia DR3 source with a white circle of radius inversely proportional to the Gaia G magnitude. These FFIs show that blending is not a concern for the light curves of the objects.
Paper: Verification of Gaia Data Release 3 Single-lined Spectroscopic Binary Solutions With Three Transiting Low-mass Secondaries
Authors: Stephen P. Schmidt, Kevin C. Schlaufman, Keyi Ding, 可怿 丁, Samuel K. Grunblatt, Theron Carmichael, Allyson Bieryla, Joseph E. Rodriguez, Jack Schulte, Noah Vowell, George Zhou, Samuel N. Quinn, Samuel W. Yee, Joshua N. Winn, Joel D. Hartman, David W. Latham, Douglas A. Caldwell, M. M. Fausnaugh, Christina Hedges, Jon M. Jenkins, Hugh P. Osborn, S. Seager
Figure caption: Detrended light curves for TOI-1712, TOI-2533, and TOI-5427. In addition to the 30 minute cadence data for each of the objects, we include two-minute cadence data for TOI-1712 from TESS Sector 47 and ten-minute cadence data for TOI-5427 from Sectors 43, 44, and 45. We overlay the data with red lines representing our juliet-derived transit fits. These fits demonstrate that the periods and transit shape parameters reported in the TOI catalog accurately reflect the data and are sufficient for comparison to external catalogs.
Paper: Verification of Gaia Data Release 3 Single-lined Spectroscopic Binary Solutions With Three Transiting Low-mass Secondaries
Authors: Stephen P. Schmidt, Kevin C. Schlaufman, Keyi Ding, 可怿 丁, Samuel K. Grunblatt, Theron Carmichael, Allyson Bieryla, Joseph E. Rodriguez, Jack Schulte, Noah Vowell, George Zhou, Samuel N. Quinn, Samuel W. Yee, Joshua N. Winn, Joel D. Hartman, David W. Latham, Douglas A. Caldwell, M. M. Fausnaugh, Christina Hedges, Jon M. Jenkins, Hugh P. Osborn, S. Seager
Figure caption: TESS Science Processing Operations Center (SPOC)-reduced light curves for TOI-1712, TOI-2533, and TOI-5427. In addition to the 30 minute cadence data for each of the objects, we include two-minute cadence data for TOI-1712 from TESS Sector 47 and ten-minute cadence data for TOI-5427 from Sectors 43, 44, and 45. We plot in red on top of the data the juliet-derived Gaussian process fits the light curves. We next use these fits to detrend the light curves before subsequently fitting the transits.
Paper: Astrophysical Distance Scale. VII. A Self-consistent, Multiwavelength Calibration of the Slopes and Relative Zero Points for the Run of Luminosity with the Color of Stars Defining the Tip of the Red Giant Branch
Authors: Barry F. Madore, Wendy L. Freedman, Kayla Owens
Figure caption: Near-infrared (JHK) Basti models of red-giant branch isochrones for a variety of metallicities (in each panel) and for a solar mixture in the three (JHK; top to bottom) panels in left column, and an ɑ-enhanced mixture in the three (JHK) panels in the right column. The dashed black line is a fit to the TRGB as defined by the five highest metallicity isochrones. Those slopes are individually given in the lower right portion of each of the color–magnitude diagrams.
Paper: Verification of Gaia Data Release 3 Single-lined Spectroscopic Binary Solutions With Three Transiting Low-mass Secondaries
Authors: Stephen P. Schmidt, Kevin C. Schlaufman, Keyi Ding, 可怿 丁, Samuel K. Grunblatt, Theron Carmichael, Allyson Bieryla, Joseph E. Rodriguez, Jack Schulte, Noah Vowell, George Zhou, Samuel N. Quinn, Samuel W. Yee, Joshua N. Winn, Joel D. Hartman, David W. Latham, Douglas A. Caldwell, M. M. Fausnaugh, Christina Hedges, Jon M. Jenkins, Hugh P. Osborn, S. Seager
Figure caption: Phased light curves for the 30 minute cadence data of TOI-1712, TOI-2533, and TOI-5427. We overlay the data with red lines representing the juliet-derived transit fits. The relative flux axes are consistent across the three objects to illustrate their differing transit depths.
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 diagram of AU Mic b with the super-period model overlaid (black). The super-period model was generated using the coefficients from Table 9 and Equation (1), and the O−C diagram was generated using the EXOFASTv2-generated measured midpoint times (Table 11) and the calculated expected midpoint times for all transit data sets from Table 1. The planet’s period and T C from EXOFASTv2 posteriors were used for the calculation of expected midpoint times. The time is with respect to the first transit of b.
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: Comparison between ground-based + Spitzer + TESS transits (multicolors) and EXOFASTv2’s best-fit model (black) for AU Mic b (first three columns in the top row) and c (last column in the bottom row). Each transit is labeled with the name of telescope, the date of observation in UT, and the epoch, which refers to the number of transits since the first transit of b and c, respectively.
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 high-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 (top) and AU Mic c (bottom), using the EXOFASTv2-generated measured midpoint times (Table 11) and the calculated expected midpoint times for all transit data sets from Table 1. The planets’ period and T  C  from EXOFASTv2 posteriors were used for the calculation of expected midpoint times. The epoch refers to the number of transits since the first transit of b and c, respectively.
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 high-eccentricity configuration.
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: Planetary RV predictions from the accepted fit (purple histogram), together with the planetary RV measurement from Petrus et al. (2021; dashed black line, with 1σ range in shaded gray). Takeaways: The planetary RV measurement does not constrain the orbital parameters, beyond breaking the 180° degeneracy for Ω and ω. A planetary RV of −3 km s−1 is allowed, given the astrometry alone, but is disfavored (relative to a planetary RV of 3 km s−1) because of the relative RV measurement.
Paper: The Advantages of Global Photometric Models in Fitting Transit Variations
Authors: Yair Judkovsky, Aviv Ofir, Oded Aharonson
Figure caption: The distribution of the deviation of the parameters estimates from the true values in terms of error estimates, calculated among a set of 15,505 experiments with different noise realizations, shown for two methods: the global fit method and the transit-by-transit method. Top row: the high-S/N case. In this case, the global fit method generates parameter estimates that nicely fit a Gaussian, while the transit-by-transit method generates a broader distribution. The black dashed line indicates a normal distribution with unity standard deviation. Bottom row: the low-S/N case. In this case, both distributions deviate from a Gaussian; the transit-by-transit method generates a much broader distribution, for which the peak is almost erased, while the global fit remains well-centered.
Paper: The Advantages of Global Photometric Models in Fitting Transit Variations
Authors: Yair Judkovsky, Aviv Ofir, Oded Aharonson
Figure caption: The χ 2 surface in the timing method and the flux method for the high-S/N case (left-hand side) and for the low-S/N case (right-hand side). The Δχ 2 surface (relative to the minimum) in the method using individual mid-transit times fitting is shown in blue; the Δχ 2 surface for the global flux method is shown in orange. A dashed black line indicates the true TTV frequency. In the high-S/N case, both methods generate a clear global deep minimum around the true TTV frequency. In the low-S/N case, additional, deeper minima are found around other frequencies in the timing method. Local minima exist in the flux-fitting method, but the global minimum remains around the true TTV frequency.
Paper: The Advantages of Global Photometric Models in Fitting Transit Variations
Authors: Yair Judkovsky, Aviv Ofir, Oded Aharonson
Figure caption: The best-fitting TTV solutions for two numerical experiments, each with a different single-transit S/N value. The blue error bars are the TTV estimates from fitting individual transit times, and the solid orange curve is the best-fitting TTV model, obtained from an LM search beginning at the correct ω value. The yellow curve on the right-hand-side plot is the best-fitting TTV model in the Lomb–Scargle peak frequency. In the high-S/N case (left-hand side), the true TTV frequency is apparent in the estimated TTV obtained from a transit-by-transit analysis, leading to a correct estimation of the TTV frequency ω up to the estimated error. In the low-S/N case (right-hand side), the noise has erased the transit events, thus leading to wrong or highly uncertain estimates of the individual mid-transit times. The estimated TTV frequency, in this case, is far from the true value.
Paper: The Advantages of Global Photometric Models in Fitting Transit Variations
Authors: Yair Judkovsky, Aviv Ofir, Oded Aharonson
Figure caption: The mean deviation of the parameter estimates from the true value and the normalized deviation in error estimate as a function of transit S/N. Top row: the dots indicate the mean parameter estimate, and the error bars indicate the spread of the parameter estimates. The black dashed line indicates the true parameter value. Bottom row: the square root of the mean square of the deviation-to-error-estimate ratio. Color legend: blue = transit-by-transit, yellow = global flux fit, purple = transit-by-transit with a fixed ω value, green = global flux fit with a fixed ω value. See the text for further explanations.
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: Best-fit spectral energy distribution (SED) model of HIP 65426 A used to convert our transmission functions of photometric bands (in the top panel, where each is plotted as a data point with errors immediately beneath). Middle: MAP BT-NextGen model and photometric data from TYCHO, 2MASS, and WISE. Bottom: MAP model residuals.
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: Detections of HIP 65426 b with VLTI/GRAVITY in epochs 1 and 2. Both periodogram power maps visualize the χ 2 fit to the interferometric observables assuming a point source, after removing the contribution of the star using a fourth-order polynomial. The outer dashed gray circle indicates the effective fiber field of view (60 mas in diameter), and the red circles indicate the most probable planet position at each epoch. The planet is detected at high confidence in both epochs (periodogram power >500).
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: Detection of HIP 65426 b with VLTI/GRAVITY in epoch 3. See Figure 1.
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: Full best-fit model SED from comparison with the Exo-REM grid, together with all fitted spectral data. Top: transmission functions of the photometric bands. Middle: MAP model spectrum, along with 100 random draws from the posterior (in gray; barely distinguishable from the MAP spectrum). The spectral data are plotted as points with error bars. The horizontal bars of the photometry points indicate their spectral bandpasses. The corresponding band-integrated model predictions are overplotted as empty symbols. Bottom: MAP model residuals. Takeaways: Overall, the model spectrum fits well. Correlated noise is visible in the residuals of the SPHERE data set. The NACO and JWST/NIRCAM points beyond 3 μm are underestimated by the model.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: The results of applying the SYSREM algorithm to five orders of the data at the blue end of the spectrum. Top: the raw data after being extracted from the telescope and normalized. Middle: the results of applying seven iterations of the SYSREM algorithm to the data. Bottom: the standard deviation of the SYSREM-reduced data along each wavelength channel. As described in Section 5.1, all of these orders were excluded from our analysis.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: The model injection/recovery process for Zr I. The plots are as described in the captions of Figures 12 and 13.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: The model injection/recovery process for Sc II. The plots are as described in the captions of Figures 12 and 13.
Paper: ExoGemS High-resolution Transmission Spectroscopy of WASP-76b with GRACES
Authors: Emily K. Deibert, Ernst J. W. de Mooij, Ray Jayawardhana, Jake D. Turner, Andrew Ridden-Harper, Callie E. Hood, Jonathan J. Fortney, Laura Flagg, Luca Fossati, Romain Allart, Matteo Brogi, Ryan J. MacDonald
Figure caption: The model injection/recovery process for Sc I. The plots are as described in the captions of Figures 12 and 13.