adsabs/AstroCLIMB huggingface dataset:
Paper: TOI-4010: A System of Three Large Short-period Planets with a Massive Long-period Companion
Authors: Michelle Kunimoto, Andrew Vanderburg, Chelsea X. Huang, M. Ryleigh Davis, Laura Affer, Andrew Collier Cameron, David Charbonneau, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martnez Fiorenzano, Adriano Ghedina, R. D. Haywood, Florian Lienhard, Mercedes López-Morales, Michel Mayor, Francesco Pepe, Matteo Pinamonti, Ennio Poretti, Jesús Maldonado, Ken Rice, Alessandro Sozzetti, Thomas G. Wilson, Stéphane Udry, Jay Baptista, Khalid Barkaoui, Juliette Becker, Paul Benni, Allyson Bieryla, Pau Bosch-Cabot, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Elise Evans, Trent J. Dupuy, Maria V. Goliguzova, Pere Guerra, Adam Kraus, Jack J. Lissauer, Daniel Huber, Felipe Murgas, Enric Palle, Samuel N. Quinn, Boris S. Safonov, Richard P. Schwarz, Avi Shporer, Keivan G. Stassun, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua Winn, Zahra Essack, Hannah M. Lewis, Mark E. Rose
Figure caption: Top: HARPS-N RV time series, which has a long-term trend best explained by an outer giant planet. The four-planet model is overplotted in red, and the residuals after subtracting the model are in the lower panel. Bottom: RV phase diagram for the long-period giant planet TOI-4010 e with the signals of the other three planets removed, in the same format as in Figure 10. The Keplerian model is plotted in purple. The gap in the phase diagram reflects the fact that the RV observing baseline is shorter than the estimated orbital period of the planet.
Paper: TOI-4010: A System of Three Large Short-period Planets with a Massive Long-period Companion
Authors: Michelle Kunimoto, Andrew Vanderburg, Chelsea X. Huang, M. Ryleigh Davis, Laura Affer, Andrew Collier Cameron, David Charbonneau, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martnez Fiorenzano, Adriano Ghedina, R. D. Haywood, Florian Lienhard, Mercedes López-Morales, Michel Mayor, Francesco Pepe, Matteo Pinamonti, Ennio Poretti, Jesús Maldonado, Ken Rice, Alessandro Sozzetti, Thomas G. Wilson, Stéphane Udry, Jay Baptista, Khalid Barkaoui, Juliette Becker, Paul Benni, Allyson Bieryla, Pau Bosch-Cabot, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Elise Evans, Trent J. Dupuy, Maria V. Goliguzova, Pere Guerra, Adam Kraus, Jack J. Lissauer, Daniel Huber, Felipe Murgas, Enric Palle, Samuel N. Quinn, Boris S. Safonov, Richard P. Schwarz, Avi Shporer, Keivan G. Stassun, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua Winn, Zahra Essack, Hannah M. Lewis, Mark E. Rose
Figure caption: Spectral energy distribution of TOI-4010. Red symbols represent the observed photometric measurements, where the horizontal bars represent the effective width of the passband. Blue symbols are the model fluxes from the best-fit Kurucz atmosphere model (black).
Paper: TOI-4010: A System of Three Large Short-period Planets with a Massive Long-period Companion
Authors: Michelle Kunimoto, Andrew Vanderburg, Chelsea X. Huang, M. Ryleigh Davis, Laura Affer, Andrew Collier Cameron, David Charbonneau, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martnez Fiorenzano, Adriano Ghedina, R. D. Haywood, Florian Lienhard, Mercedes López-Morales, Michel Mayor, Francesco Pepe, Matteo Pinamonti, Ennio Poretti, Jesús Maldonado, Ken Rice, Alessandro Sozzetti, Thomas G. Wilson, Stéphane Udry, Jay Baptista, Khalid Barkaoui, Juliette Becker, Paul Benni, Allyson Bieryla, Pau Bosch-Cabot, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Elise Evans, Trent J. Dupuy, Maria V. Goliguzova, Pere Guerra, Adam Kraus, Jack J. Lissauer, Daniel Huber, Felipe Murgas, Enric Palle, Samuel N. Quinn, Boris S. Safonov, Richard P. Schwarz, Avi Shporer, Keivan G. Stassun, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua Winn, Zahra Essack, Hannah M. Lewis, Mark E. Rose
Figure caption: Left: Time series of activity indicators from HARPS-N spectra. Right: GLS periodograms of activity indicators. The horizontal lines mark 1% (dotted line) and 0.1% (dashed–dotted line) false-alarm probability levels, while vertical lines mark the orbital periods of the three planets. The line at P = 762 days marks the possible orbital period of the fourth planet that was uncovered in our later RV analysis (see Section 4.2).
Paper: TOI-4010: A System of Three Large Short-period Planets with a Massive Long-period Companion
Authors: Michelle Kunimoto, Andrew Vanderburg, Chelsea X. Huang, M. Ryleigh Davis, Laura Affer, Andrew Collier Cameron, David Charbonneau, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martnez Fiorenzano, Adriano Ghedina, R. D. Haywood, Florian Lienhard, Mercedes López-Morales, Michel Mayor, Francesco Pepe, Matteo Pinamonti, Ennio Poretti, Jesús Maldonado, Ken Rice, Alessandro Sozzetti, Thomas G. Wilson, Stéphane Udry, Jay Baptista, Khalid Barkaoui, Juliette Becker, Paul Benni, Allyson Bieryla, Pau Bosch-Cabot, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Elise Evans, Trent J. Dupuy, Maria V. Goliguzova, Pere Guerra, Adam Kraus, Jack J. Lissauer, Daniel Huber, Felipe Murgas, Enric Palle, Samuel N. Quinn, Boris S. Safonov, Richard P. Schwarz, Avi Shporer, Keivan G. Stassun, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua Winn, Zahra Essack, Hannah M. Lewis, Mark E. Rose
Figure caption: Photometric observations from TESS, LCO, and OAA, folded on the transit-only model fit periods of TOI-4010.01 (orange), 4010.02 (green), and 4010.03 (blue). The gray points reflect the photometric observations while colored circles are data averaged in 30 minute bins. The solid lines show the median transit model. The phase diagrams are offset by an arbitrary flux amount to improve visibility.
Paper: TOI-4010: A System of Three Large Short-period Planets with a Massive Long-period Companion
Authors: Michelle Kunimoto, Andrew Vanderburg, Chelsea X. Huang, M. Ryleigh Davis, Laura Affer, Andrew Collier Cameron, David Charbonneau, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martnez Fiorenzano, Adriano Ghedina, R. D. Haywood, Florian Lienhard, Mercedes López-Morales, Michel Mayor, Francesco Pepe, Matteo Pinamonti, Ennio Poretti, Jesús Maldonado, Ken Rice, Alessandro Sozzetti, Thomas G. Wilson, Stéphane Udry, Jay Baptista, Khalid Barkaoui, Juliette Becker, Paul Benni, Allyson Bieryla, Pau Bosch-Cabot, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Elise Evans, Trent J. Dupuy, Maria V. Goliguzova, Pere Guerra, Adam Kraus, Jack J. Lissauer, Daniel Huber, Felipe Murgas, Enric Palle, Samuel N. Quinn, Boris S. Safonov, Richard P. Schwarz, Avi Shporer, Keivan G. Stassun, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua Winn, Zahra Essack, Hannah M. Lewis, Mark E. Rose
Figure caption: Top: 112 HARPS-N RV observations of TOI-4010. Bottom: GLS periodogram of the RVs using the same format as Figure 5. There is a long-period signal with a semi-amplitude of ∼50 m s−1 that dominates, indicating a fourth planet.
Paper: TOI-4010: A System of Three Large Short-period Planets with a Massive Long-period Companion
Authors: Michelle Kunimoto, Andrew Vanderburg, Chelsea X. Huang, M. Ryleigh Davis, Laura Affer, Andrew Collier Cameron, David Charbonneau, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martnez Fiorenzano, Adriano Ghedina, R. D. Haywood, Florian Lienhard, Mercedes López-Morales, Michel Mayor, Francesco Pepe, Matteo Pinamonti, Ennio Poretti, Jesús Maldonado, Ken Rice, Alessandro Sozzetti, Thomas G. Wilson, Stéphane Udry, Jay Baptista, Khalid Barkaoui, Juliette Becker, Paul Benni, Allyson Bieryla, Pau Bosch-Cabot, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Elise Evans, Trent J. Dupuy, Maria V. Goliguzova, Pere Guerra, Adam Kraus, Jack J. Lissauer, Daniel Huber, Felipe Murgas, Enric Palle, Samuel N. Quinn, Boris S. Safonov, Richard P. Schwarz, Avi Shporer, Keivan G. Stassun, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua Winn, Zahra Essack, Hannah M. Lewis, Mark E. Rose
Figure caption: GLS periodograms of the HARPS-N RVs. The top panel shows periodograms of the original RVs, while subsequent panels show periodograms of the RVs after subtracting our median model fits for TOI-4010 e, d, c, and b, respectively. In each panel, the horizontal lines mark 1% (dotted line) and 0.1% (dashed–dotted line) false-alarm probability levels, while vertical lines mark the orbital periods of the four planets.
Paper: TOI-4010: A System of Three Large Short-period Planets with a Massive Long-period Companion
Authors: Michelle Kunimoto, Andrew Vanderburg, Chelsea X. Huang, M. Ryleigh Davis, Laura Affer, Andrew Collier Cameron, David Charbonneau, Rosario Cosentino, Mario Damasso, Xavier Dumusque, A. F. Martnez Fiorenzano, Adriano Ghedina, R. D. Haywood, Florian Lienhard, Mercedes López-Morales, Michel Mayor, Francesco Pepe, Matteo Pinamonti, Ennio Poretti, Jesús Maldonado, Ken Rice, Alessandro Sozzetti, Thomas G. Wilson, Stéphane Udry, Jay Baptista, Khalid Barkaoui, Juliette Becker, Paul Benni, Allyson Bieryla, Pau Bosch-Cabot, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Elise Evans, Trent J. Dupuy, Maria V. Goliguzova, Pere Guerra, Adam Kraus, Jack J. Lissauer, Daniel Huber, Felipe Murgas, Enric Palle, Samuel N. Quinn, Boris S. Safonov, Richard P. Schwarz, Avi Shporer, Keivan G. Stassun, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua Winn, Zahra Essack, Hannah M. Lewis, Mark E. Rose
Figure caption: TESS light curve for TOI-4010 before removal of stellar variability. The transits of TOI-4010.01, .02, and .03 are indicated by blue, green, and orange dots, respectively, based on the transit ephemerides found in Section 4.3.
Paper: The Spitzer Coverage of HSC-Deep with IRAC for Z studies (SHIRAZ). I. IRAC Mosaics
Authors: Marianna Annunziatella, Anna Sajina, Mauro Stefanon, Danilo Marchesini, Mark Lacy, Ivo Labbé, Lilianna Houston, Rachel Bezanson, Eiichi Egami, Xiaohui Fan, Duncan Farrah, Jenny Greene, Andy Goulding, Yen-Ting Lin, Xin Liu, Thibaud Moutard, Yoshiaki Ono, Masami Ouchi, Marcin Sawicki, Jason Surace, Katherine Whitaker
Figure caption: Top row: growth curves for a sample of ≥ 100 bright unsaturated stars for all three fields at 3.6 μm normalized to the flux of the star in an aperture of 6″ diameter. The black curve in each panel represents the median of the distribution. The last panel shows the median growth curve of each field at 3.6 μm. Middle row: same as top row but at 4.5 μm. Bottom row: CH2/CH1 growth curves in the three fields.
Paper: The Spitzer Coverage of HSC-Deep with IRAC for Z studies (SHIRAZ). I. IRAC Mosaics
Authors: Marianna Annunziatella, Anna Sajina, Mauro Stefanon, Danilo Marchesini, Mark Lacy, Ivo Labbé, Lilianna Houston, Rachel Bezanson, Eiichi Egami, Xiaohui Fan, Duncan Farrah, Jenny Greene, Andy Goulding, Yen-Ting Lin, Xin Liu, Thibaud Moutard, Yoshiaki Ono, Masami Ouchi, Marcin Sawicki, Jason Surace, Katherine Whitaker
Figure caption: Depth vs. area for extragalactic surveys at 3.6 μm. Stars indicate surveys taken during the postcryogenic phase of Spitzer as Exploration Science or Frontier Legacy surveys. The circles show surveys taken during the cryogenic mission of Spitzer as cyan circles. Our program SHIRAZ is marked as a magenta diamond. References: SpIES (Timlin et al. 2016), SWIRE (Lonsdale et al. 2003), SERVS-DeepDrill (Lacy et al. 2021), SERVS (Mauduit et al. 2012), SPLASH (Steinhardt et al. 2014), S-COSMOS (Sanders et al. 2007), COMPLETE (Labbé et al. 2015), SpUDS (Kim et al. 2011), SEDS (Ashby et al. 2013), SMUVS (Ashby et al. 2018), S-CANDELS (Ashby et al. 2015), SIMPLE (Damen et al. 2011), and GOODS (Dickinson et al. 2003).
Paper: The Spitzer Coverage of HSC-Deep with IRAC for Z studies (SHIRAZ). I. IRAC Mosaics
Authors: Marianna Annunziatella, Anna Sajina, Mauro Stefanon, Danilo Marchesini, Mark Lacy, Ivo Labbé, Lilianna Houston, Rachel Bezanson, Eiichi Egami, Xiaohui Fan, Duncan Farrah, Jenny Greene, Andy Goulding, Yen-Ting Lin, Xin Liu, Thibaud Moutard, Yoshiaki Ono, Masami Ouchi, Marcin Sawicki, Jason Surace, Katherine Whitaker
Figure caption: We compare the total magnitudes for objects detected in our new mosaic of EN1 and those from the SERVS catalog (Mauduit et al. 2012) in the same area in both channels. Since the SERVS catalog excludes stars Mauduit et al. (2012), in this cross-match stars are also excluded. Contours, from the inner to the outer, contain 10%, 30%, 50%, 70%, 90%, 95%, and 99% of the galaxies. Overplotted in gray are the running medians and the correspondent 1σ confidence interval. We see pretty good agreement with only small median offsets. For channel 1, this is largely explained by the recalibration of the first year of Spitzer warm mission data that was not known at the time of the original SERVS catalog construction.
Paper: The Spitzer Coverage of HSC-Deep with IRAC for Z studies (SHIRAZ). I. IRAC Mosaics
Authors: Marianna Annunziatella, Anna Sajina, Mauro Stefanon, Danilo Marchesini, Mark Lacy, Ivo Labbé, Lilianna Houston, Rachel Bezanson, Eiichi Egami, Xiaohui Fan, Duncan Farrah, Jenny Greene, Andy Goulding, Yen-Ting Lin, Xin Liu, Thibaud Moutard, Yoshiaki Ono, Masami Ouchi, Marcin Sawicki, Jason Surace, Katherine Whitaker
Figure caption: The coverage maps for E-COSMOS (top) and EN1 (bottom). Here we have incorporated both our new as well as archival IRAC data leading to a inhomogeneous depth. For example, the shallower area on the outside of the EN1 mosaic comes from the SWIRE survey, but the irregular shaped deeper patches are all within the HSC-Deep footprint (see Figure 1). These E-COSMOS coverage maps include all available IRAC data, although to avoid the large contrasts in depths in this field, we did our image quality assessments on the new data plus S-COSMOS alone (which is what is shown in Figure 1 for E-COSMOS).
Paper: The Spitzer Coverage of HSC-Deep with IRAC for Z studies (SHIRAZ). I. IRAC Mosaics
Authors: Marianna Annunziatella, Anna Sajina, Mauro Stefanon, Danilo Marchesini, Mark Lacy, Ivo Labbé, Lilianna Houston, Rachel Bezanson, Eiichi Egami, Xiaohui Fan, Duncan Farrah, Jenny Greene, Andy Goulding, Yen-Ting Lin, Xin Liu, Thibaud Moutard, Yoshiaki Ono, Masami Ouchi, Marcin Sawicki, Jason Surace, Katherine Whitaker
Figure caption: The left-hand side shows the reference z-band mosaic for the DEEP2-F3 field overlaid with the 3.6 and 4.5μm mosaic contours. This shows the good degree of overlap between the mosaics of both channels thanks to the two observing epochs. The right-hand side shows the coverage maps for the DEEP2-F3 field for both channels. These only include our new Spitzer observations and therefore help illustrate our observing strategy. These clearly show the tiling of the individual AORs each of which consists of 3 × 3 IRAC pointings.
Paper: The Spitzer Coverage of HSC-Deep with IRAC for Z studies (SHIRAZ). I. IRAC Mosaics
Authors: Marianna Annunziatella, Anna Sajina, Mauro Stefanon, Danilo Marchesini, Mark Lacy, Ivo Labbé, Lilianna Houston, Rachel Bezanson, Eiichi Egami, Xiaohui Fan, Duncan Farrah, Jenny Greene, Andy Goulding, Yen-Ting Lin, Xin Liu, Thibaud Moutard, Yoshiaki Ono, Masami Ouchi, Marcin Sawicki, Jason Surace, Katherine Whitaker
Figure caption: The key ancillary data for the four HSC-Deep fields. Greyscale background shows the IRAC exposure maps, with overlaid the footprints of CLAUDS U-band (blue outline), HSC-Deep grizy (pink), and several near-IR surveys (hashed cyan). The total area of overlap of CLAUDS+HSC-Deep+near-IR+IRAC is ≈18 deg2.
Paper: The Spitzer Coverage of HSC-Deep with IRAC for Z studies (SHIRAZ). I. IRAC Mosaics
Authors: Marianna Annunziatella, Anna Sajina, Mauro Stefanon, Danilo Marchesini, Mark Lacy, Ivo Labbé, Lilianna Houston, Rachel Bezanson, Eiichi Egami, Xiaohui Fan, Duncan Farrah, Jenny Greene, Andy Goulding, Yen-Ting Lin, Xin Liu, Thibaud Moutard, Yoshiaki Ono, Masami Ouchi, Marcin Sawicki, Jason Surace, Katherine Whitaker
Figure caption: Differential source counts in the E-COSMOS, DEEP2-F3, and EN1 fields measured in the 3.6 μm mosaic (left panel) and in the 4.5 μm mosaic (right panel). The vertical lines are the 50th percentile of the 5σ depths. For comparison, we overplot the counts from the S-CANDELS (Ashby et al. 2015), and from the Deep Drill (Lacy et al. 2021) surveys.
Paper: The Spitzer Coverage of HSC-Deep with IRAC for Z studies (SHIRAZ). I. IRAC Mosaics
Authors: Marianna Annunziatella, Anna Sajina, Mauro Stefanon, Danilo Marchesini, Mark Lacy, Ivo Labbé, Lilianna Houston, Rachel Bezanson, Eiichi Egami, Xiaohui Fan, Duncan Farrah, Jenny Greene, Andy Goulding, Yen-Ting Lin, Xin Liu, Thibaud Moutard, Yoshiaki Ono, Masami Ouchi, Marcin Sawicki, Jason Surace, Katherine Whitaker
Figure caption: 3σ magnitude depths of the 3.6  μm (left) and 4.5  μm (right) mosaics. These are computed from Equation (1) based on the width of the distribution of fluxes measured in ∼4000 empty apertures from the noise-normalized images (see text for details). We see that in the areas of interest (overlapping with the HSC-Deep layer) our mosaics have a 3σ depth of ∼24 [AB] or better.
Paper: Visual Orbits and Alignments of Planet-hosting Binary Systems
Authors: Kathryn V. Lester, Steve B. Howell, Rachel A. Matson, Elise Furlan, Crystal L. Gnilka, Colin Littlefield, David R. Ciardi, Mark E. Everett, Sergio B. Fajardo-Acosta, Catherine A. Clark
Figure caption: Left: visual orbit solutions for EPIC 220555384. The primary star is positioned at the origin (black cross), and the relative positions of the secondary component are marked with colored points. A random subset of the accepted orbital solutions from orbitize! are shown in gray. The green arrow shows the Gaia proper motion of the primary star (in a single year), which is inconsistent with the observed motion of the secondary. Right: the observed changes in position angle and relative separation over time, plotted against the possible orbital solutions.
Paper: Visual Orbits and Alignments of Planet-hosting Binary Systems
Authors: Kathryn V. Lester, Steve B. Howell, Rachel A. Matson, Elise Furlan, Crystal L. Gnilka, Colin Littlefield, David R. Ciardi, Mark E. Everett, Sergio B. Fajardo-Acosta, Catherine A. Clark
Figure caption: Left: visual orbit solutions for EPIC 212303338. The primary star is positioned at the origin (black cross), and the relative positions of the secondary component are marked with colored points. A random subset of the accepted orbital solutions from orbitize! are shown in gray. The green arrow shows the Gaia proper motion of the primary star (in a single year), which is inconsistent with the observed motion of the secondary. Right: the observed changes in position angle and relative separation over time, plotted against the possible orbital solutions.
Paper: Visual Orbits and Alignments of Planet-hosting Binary Systems
Authors: Kathryn V. Lester, Steve B. Howell, Rachel A. Matson, Elise Furlan, Crystal L. Gnilka, Colin Littlefield, David R. Ciardi, Mark E. Everett, Sergio B. Fajardo-Acosta, Catherine A. Clark
Figure caption: Left: visual orbit solutions for KOI 3456. The primary star is positioned at the origin (black cross), and the relative positions of the secondary component are marked with colored points. A random subset of the accepted orbital solutions from orbitize! are shown in gray. The green arrow shows the Gaia proper motion of the primary star (in a single year), which is inconsistent with the observed motion of the secondary. Right: the observed changes in position angle and relative separation over time, plotted against the possible orbital solutions.
Paper: Visual Orbits and Alignments of Planet-hosting Binary Systems
Authors: Kathryn V. Lester, Steve B. Howell, Rachel A. Matson, Elise Furlan, Crystal L. Gnilka, Colin Littlefield, David R. Ciardi, Mark E. Everett, Sergio B. Fajardo-Acosta, Catherine A. Clark
Figure caption: Left: visual orbit solutions for KOI 5971. The primary star is positioned at the origin (black cross), and the relative positions of the secondary component are marked with colored points. A random subset of the accepted orbital solutions from orbitize! are shown in gray. The green arrow shows the Gaia proper motion of the primary star (in a single year), which is inconsistent with the observed motion of the secondary. Right: the observed changes in position angle and relative separation over time, plotted against the possible orbital solutions.
Paper: Visual Orbits and Alignments of Planet-hosting Binary Systems
Authors: Kathryn V. Lester, Steve B. Howell, Rachel A. Matson, Elise Furlan, Crystal L. Gnilka, Colin Littlefield, David R. Ciardi, Mark E. Everett, Sergio B. Fajardo-Acosta, Catherine A. Clark
Figure caption: Left: visual orbit solutions for KOI 3234. The primary star is positioned at the origin (black cross), and the relative positions of the secondary component are marked with colored points. A random subset of the accepted orbital solutions from orbitize! are shown in gray. The green arrow shows the Gaia proper motion of the primary star (in a single year), which is inconsistent with the observed motion of the secondary. Right: the observed changes in position angle and relative separation over time, plotted against the possible orbital solutions.
Paper: Visual Orbits and Alignments of Planet-hosting Binary Systems
Authors: Kathryn V. Lester, Steve B. Howell, Rachel A. Matson, Elise Furlan, Crystal L. Gnilka, Colin Littlefield, David R. Ciardi, Mark E. Everett, Sergio B. Fajardo-Acosta, Catherine A. Clark
Figure caption: Left: visual orbit solutions for TOI 1287. The primary star is positioned at the origin (black cross), and the relative positions of the secondary component are marked with colored points. A random subset of the accepted orbital solutions from orbitize! are shown in gray. The green arrow shows the Gaia proper motion of the primary star (in a single year), which is inconsistent with the observed motion of the secondary. Right: the observed changes in position angle and relative separation over time, plotted against the possible orbital solutions.
Paper: Visual Orbits and Alignments of Planet-hosting Binary Systems
Authors: Kathryn V. Lester, Steve B. Howell, Rachel A. Matson, Elise Furlan, Crystal L. Gnilka, Colin Littlefield, David R. Ciardi, Mark E. Everett, Sergio B. Fajardo-Acosta, Catherine A. Clark
Figure caption: Left: visual orbit solutions for KOI 4252. The primary star is positioned at the origin (black cross), and the relative positions of the secondary component are marked with colored points. A random subset of the accepted orbital solutions from orbitize! are shown in gray. The green arrow shows the Gaia proper motion of the primary star (in a single year), which is inconsistent with the observed motion of the secondary. Right: the observed changes in position angle and relative separation over time, plotted against the possible orbital solutions.
Paper: Visual Orbits and Alignments of Planet-hosting Binary Systems
Authors: Kathryn V. Lester, Steve B. Howell, Rachel A. Matson, Elise Furlan, Crystal L. Gnilka, Colin Littlefield, David R. Ciardi, Mark E. Everett, Sergio B. Fajardo-Acosta, Catherine A. Clark
Figure caption: Left: visual orbit solutions for TOI 271. The primary star is positioned at the origin (black cross), and the relative positions of the secondary component are marked with colored points. A random subset of the accepted orbital solutions from orbitize! are shown in gray. The green arrow shows the Gaia proper motion of the primary star (in a single year), which is inconsistent with the observed motion of the secondary. Right: the observed changes in position angle and relative separation over time, plotted against the possible orbital solutions.