adsabs/AstroCLIMB huggingface dataset:
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: Relative constraining power of the astrometric data for semimajor axis (top), eccentricity (middle), and inclination (bottom). The results of the following fits are shown and compared: (1) only literature astrometry (i.e., no GRAVITY data; gray), (2) literature astrometry and the first epoch of GRAVITY data (dark pink outline), (3) literature astrometry and the second epoch of GRAVITY data (light pink outline), (4) only GRAVITY astrometry (i.e., no literature data), and (5) all astrometric data (i.e., the accepted fit; purple outline). Takeaways: Most of the constraining power of the fit comes from the GRAVITY data, evident by the similarity between the GRAVITY-only fit and the accepted fit. In addition, neither GRAVITY point alone drives the fit, as evidenced by the similarity between fits (2) and (3). In other words, the posterior preference for moderate eccentricities is robust to the possibility that one of the two GRAVITY epochs is an outlier.
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:  BT-SETTL CIFIST models representing the two posterior peaks shown in Figure 11, together with the SPHERE IFS data. Top: both models, resampled onto the SPHERE IFS wavelength grid using spectres (Carnall 2017), and multiplied by a scalar chosen to minimize the sum of the squared residuals for the SPHERE IFS data alone. The SPHERE IFS data are shown as blue points, with error bars representing their reported statistical uncertainties. Middle: the low-T eff model (dashed purple line), SPHERE IFS data, and GP 1σ uncertainties (solid purple band; computed using the MAP GP parameters). Bottom: same as middle, but the high-T eff model is shown as a solid pink line, and GP uncertainties as a pink band. Takeaway: there are correlated residuals in the SPHERE passband for both of the T eff modes recovered from comparisons to the BT-Settl CIFIST grid, which we model with a squared-exponential GP.
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: Sky-projected visualization of the posterior of the orbit fit 4 described in the text. Left: 100 orbit tracks projected onto the plane of the sky, colored by elapsed time. The astrometric data are visible as pink points in the bottom left corner of the panel. Middle column: the same 100 posterior orbits (gray) in separation (top) and position angle (bottom) vs. time, together with the astrometric data used for orbit-fitting. Right column: the same 100 posterior orbits (gray), together with earlier (bottom) and later (top) astrometric measurements taken with VLTI/GRAVITY. 1σ and 2σ error ellipses are shaded in dark and light pink, respectively. Takeaway: the VLTI/GRAVITY epochs are ∼50× more precise than existing astrometric measurements of HIP 65426, and reduce the posterior uncertainty.
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:  Exo-REM posterior fits to all data, showing 2D covariances and 1D marginalized posteriors over the fitted model parameters and derived parameters (radius, luminosity, and mass). Also see Figure 14. Note: parallax is denoted as ϖ here, and π elsewhere in the text. Takeaways: The Exo-REM derived atmosphere parameters are about 150 K lower than the low-T eff BT-SETTL CIFIST parameters (Figure 11). The surface gravity hits the edge of the available grid. A slightly supersolar-metallicity atmosphere with a C/O ratio of 0.6 is favored, although there are likely systematic errors unaccounted for in this fit.
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: Maximum log(likelihood) as a function of eccentricity. Although the MAP eccentricity is moderate (∼0.5), the maximum likelihood at low and moderate eccentricities is comparable. This allows us to understand the shape of the eccentricity posterior (Figure 8): the likelihood is high at lower eccentricities, but the prior volume here is lower. The posterior “drop-off” at higher eccentricities is caused by a real decrease in likelihood. More eccentric orbits are less consistent with the data.
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: 1D marginalized eccentricity posteriors for fits with uniform (purple) and linearly decreasing (pink) priors on the eccentricity. The priors themselves are also plotted as lines of the same colors. Takeaways: The eccentricity posterior depends on the choice of prior. However, both the linearly decreasing prior and the uniform prior result in posterior peaks at moderate eccentricity values.
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: GRAVITY and SINFONI K-band spectra comparison. Top: GRAVITY (gray) and SINFONI (purple) 1σ flux confidence intervals are shown as filled bands. The SINFONI spectrum was resampled onto the GRAVITY wavelength grid using spectres (Carnall 2017). Bottom: the residuals, with propagated uncertainties, are shown relative to the flux = 0 line. Takeaway: the agreement between these two independent data sets is excellent. The GRAVITY fluxes, uncertainties, and interchannel flux covariances are provided in the FITS format as data behind the figure.(The data used to create this figure are available.)
Paper: The Wagging Plasma Tail of Comet C/2020 S3 (Erasmus)
Authors: Jing Li, Yoonyoung Kim, David Jewitt
Figure caption: An example image taken with the HI-1 wide-field camera. Top: the median image from UT 2020 December 05. The anti-Sun (−S) and antiorbital (−V) directions are indicated by solid and dashed arrows, respectively. The bright long tail is the plasma tail. The faint tail above the plasma tail is the dust tail. The middle and bottom panels are the modeled synchrones and syndynes overlapping the image. Synchrones were computed for ejection times of 20, 40, 60, 80, and 100 days prior to the date of observation (curves from bottom to top, in the figure). Syndynes were computed for β = 1, 0.3, 0.1, 0.03, and 0.01 (curves from bottom to top), corresponding to nominal particle radii of 1, 3, 10, 30, and 100 μm, respectively. Celestial north is up, east is to the left. The region shown is 3.°2 × 1.°2 (160 × 60 pixels).
Paper: The Wagging Plasma Tail of Comet C/2020 S3 (Erasmus)
Authors: Jing Li, Yoonyoung Kim, David Jewitt
Figure caption: Top: an example of a median image of LASCO/C3. -V (dotted arrow) and -S (solid arrow) represent the antimotion and anti-Sun directions, respectively, at the location of the comet. The plasma tail is indicated by an orange arrow. Middle and bottom panels: the computed synchrone and syndyne models superimposed on the comet image to simulate the dust tails. The solid white curves are the modeled synchrones and syndynes calculated with the same parameters as those in Figure 4. North is up, east is to the left, and the region shown is ∼1.°9 × 1.°6 (120 × 100 pixels).
Paper: The Wagging Plasma Tail of Comet C/2020 S3 (Erasmus)
Authors: Jing Li, Yoonyoung Kim, David Jewitt
Figure caption: Left column: examples of median COR2 images showing the rapidly changing position angle of the plasma tail (indicated by orange arrows). The anti-Sun (−S) and antiorbital velocity (−V) directions are indicated by solid and dotted arrows, respectively. Middle and right columns: the superimposed loci of synchrones and syndynes computed with same parameters as in Figure 4. Celestial north is up and east to the left. The region shown is ∼0.°6 × 0.°5 (150 × 120 pixels).
Paper: The Wagging Plasma Tail of Comet C/2020 S3 (Erasmus)
Authors: Jing Li, Yoonyoung Kim, David Jewitt
Figure caption: Observational geometry as a function of time. The S3 observations are made with the HI-1 wide-field camera (solid lines) and COR2 coronagraph (dotted lines) on STEREO-A. After DOY 350, S3 is detected by the LASCO/C3 coronagraph on SoHO (solid lines). Perihelion is at UT 2020 December 12.67, indicated by the gray vertical line. Heliocentric distance, phase angle, and elongation are represented by red, green, and purple, respectively. Calendar dates are indicated along the top axis.
Paper: The Wagging Plasma Tail of Comet C/2020 S3 (Erasmus)
Authors: Jing Li, Yoonyoung Kim, David Jewitt
Figure caption: Full coronal images from the wide-field camera HI-1 (top), the narrow-field camera COR2 (middle) both on STEREO-A, and the LASCO/C3 coronagraph (bottom) on SoHO. The projected comet paths are plotted with solid white curves. The comet positions at the times of images are circled on each image.
Paper: The Wagging Plasma Tail of Comet C/2020 S3 (Erasmus)
Authors: Jing Li, Yoonyoung Kim, David Jewitt
Figure caption: Plan view of the orbital paths of S3, the planets, STEREO-A, SoHO, and PSP in heliocentric Cartesian coordinates during the observing period, from 2020 mid-November to end-December. All objects orbit counterclockwise. The comet trajectories are plotted as blue, orange and purple arcs corresponding to observations made with the HI-1, COR2 and LASCO/C3 cameras, respectively. Tick marks “X” are plotted every 5 days on the S3 path starting with DOY 318. Three terrestrial planets are represented by brown. The spacecraft are plotted with dashed pink curves.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ’EM) Survey. III. Recovery and Confirmation of a Temperate, Mildly Eccentric, Single-transit Jupiter Orbiting TOI-2010
Authors: Christopher R. Mann, Paul A. Dalba, David Lafrenière, Benjamin J. Fulton, Guillaume Hébrard, Isabelle Boisse, Shweta Dalal, Magali Deleuil, Xavier Delfosse, Olivier Demangeon, Thierry Forveille, Neda Heidari, Flavien Kiefer, Eder Martioli, Claire Moutou, Michael Endl, William D. Cochran, Phillip MacQueen, Franck Marchis, Diana Dragomir, Arvind F. Gupta, Dax L. Feliz, Belinda A. Nicholson, Carl Ziegler, Steven Villanueva, Jason Rowe, Geert Jan Talens, Daniel Thorngren, Daryll LaCourse, Tom Jacobs, Andrew W. Howard, Allyson Bieryla, David W. Latham, Markus Rabus, Tara Fetherolf, Coel Hellier, Steve B. Howell, Peter Plavchan, Michael Reefe, Deven Combs, Michael Bowen, Justin Wittrock, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins, Thomas Barclay, David Watanabe, Karen A. Collins, Jason D. Eastman, Eric B. Ting
Figure caption: Constraints on a potential second bound body in the system creating the observed long-term RV acceleration, assuming the objects are at the same distance as TOI-2010. Small-orbit limits are provided by the long baseline over which the gradual acceleration occurs. Green contours show the 0.607, 0.135, and 0.011 relative probability levels, corresponding to the 1, 2, and 3σ probability density values of a normal distribution. White contours show the 25%, 50%, and 75% detection probability levels (from bottom to top) set by the Gemini-N/‘Alopeke contrast curve. Contours are smoothed by a Gaussian kernel with a standard deviation of one cell. Red and cyan points in the top right corner indicate the ‘Alopeke-discovered (1.″5) and Gaia (1.″9) close neighbor stars.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ’EM) Survey. III. Recovery and Confirmation of a Temperate, Mildly Eccentric, Single-transit Jupiter Orbiting TOI-2010
Authors: Christopher R. Mann, Paul A. Dalba, David Lafrenière, Benjamin J. Fulton, Guillaume Hébrard, Isabelle Boisse, Shweta Dalal, Magali Deleuil, Xavier Delfosse, Olivier Demangeon, Thierry Forveille, Neda Heidari, Flavien Kiefer, Eder Martioli, Claire Moutou, Michael Endl, William D. Cochran, Phillip MacQueen, Franck Marchis, Diana Dragomir, Arvind F. Gupta, Dax L. Feliz, Belinda A. Nicholson, Carl Ziegler, Steven Villanueva, Jason Rowe, Geert Jan Talens, Daniel Thorngren, Daryll LaCourse, Tom Jacobs, Andrew W. Howard, Allyson Bieryla, David W. Latham, Markus Rabus, Tara Fetherolf, Coel Hellier, Steve B. Howell, Peter Plavchan, Michael Reefe, Deven Combs, Michael Bowen, Justin Wittrock, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins, Thomas Barclay, David Watanabe, Karen A. Collins, Jason D. Eastman, Eric B. Ting
Figure caption: Contrast curves from Gemini-N/‘Alopeke speckle image. Curves show the 5σ contrast limit. The faint source in the lower left of the inset image is a previously unresolved neighbor star not present in the Gaia DR3 catalog.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ’EM) Survey. III. Recovery and Confirmation of a Temperate, Mildly Eccentric, Single-transit Jupiter Orbiting TOI-2010
Authors: Christopher R. Mann, Paul A. Dalba, David Lafrenière, Benjamin J. Fulton, Guillaume Hébrard, Isabelle Boisse, Shweta Dalal, Magali Deleuil, Xavier Delfosse, Olivier Demangeon, Thierry Forveille, Neda Heidari, Flavien Kiefer, Eder Martioli, Claire Moutou, Michael Endl, William D. Cochran, Phillip MacQueen, Franck Marchis, Diana Dragomir, Arvind F. Gupta, Dax L. Feliz, Belinda A. Nicholson, Carl Ziegler, Steven Villanueva, Jason Rowe, Geert Jan Talens, Daniel Thorngren, Daryll LaCourse, Tom Jacobs, Andrew W. Howard, Allyson Bieryla, David W. Latham, Markus Rabus, Tara Fetherolf, Coel Hellier, Steve B. Howell, Peter Plavchan, Michael Reefe, Deven Combs, Michael Bowen, Justin Wittrock, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins, Thomas Barclay, David Watanabe, Karen A. Collins, Jason D. Eastman, Eric B. Ting
Figure caption: A week-long observation by NEOSSat. Gaps in the light curve are due to Earth eclipse and other necessary telescope operations. The star was imaged with a cadence of 23 s while on target. Displayed bins are 60 minutes. Top: a KEPLERSPLINE fit to the out-of-transit region to model systematics (discussed in Section 3.3). Middle: the transit fitted to the corrected light curve. The dashed purple curve shows relative probability of the expected transit based on the RV-derived period constraints available at the time of observation. Bottom: residuals of the transit fit.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ’EM) Survey. III. Recovery and Confirmation of a Temperate, Mildly Eccentric, Single-transit Jupiter Orbiting TOI-2010
Authors: Christopher R. Mann, Paul A. Dalba, David Lafrenière, Benjamin J. Fulton, Guillaume Hébrard, Isabelle Boisse, Shweta Dalal, Magali Deleuil, Xavier Delfosse, Olivier Demangeon, Thierry Forveille, Neda Heidari, Flavien Kiefer, Eder Martioli, Claire Moutou, Michael Endl, William D. Cochran, Phillip MacQueen, Franck Marchis, Diana Dragomir, Arvind F. Gupta, Dax L. Feliz, Belinda A. Nicholson, Carl Ziegler, Steven Villanueva, Jason Rowe, Geert Jan Talens, Daniel Thorngren, Daryll LaCourse, Tom Jacobs, Andrew W. Howard, Allyson Bieryla, David W. Latham, Markus Rabus, Tara Fetherolf, Coel Hellier, Steve B. Howell, Peter Plavchan, Michael Reefe, Deven Combs, Michael Bowen, Justin Wittrock, George R. Ricker, S. Seager, Joshua N. Winn, Jon M. Jenkins, Thomas Barclay, David Watanabe, Karen A. Collins, Jason D. Eastman, Eric B. Ting
Figure caption: RV coverage of 110 measurements spanning ∼2.7 yr uniformly samples the full phase of the planet’s orbit. A small residual acceleration remains after the removal of the planet’s Keplerian signal.