adsabs/AstroCLIMB huggingface dataset:
Paper: A 38 Million Year Old Neptune-sized Planet in the Kepler Field
Authors: L. G. Bouma, J. L. Curtis, K. Masuda, L. A. Hillenbrand, G. Stefansson, H. Isaacson, N. Narita, A. Fukui, M. Ikoma, M. Tamura, A. L. Kraus, E. Furlan, C. L. Gnilka, K. V. Lester, S. B. Howell
Figure caption: Transit model residuals through time (binned by Kepler quarter). Left: phase-folded transit of Kepler 1627b, with stellar variability removed. Black points are binned to 20 minute intervals. The 2σ model uncertainties and the maximum a posteriori model are shown as the faint purple band, and the dark purple line. Right: as on the left, with the transit removed.
Paper: A 38 Million Year Old Neptune-sized Planet in the Kepler Field
Authors: L. G. Bouma, J. L. Curtis, K. Masuda, L. A. Hillenbrand, G. Stefansson, H. Isaacson, N. Narita, A. Fukui, M. Ikoma, M. Tamura, A. L. Kraus, E. Furlan, C. L. Gnilka, K. V. Lester, S. B. Howell
Figure caption: Spectroscopic activity indicators during the transit of 2021 Aug 7. The top panels show the median line profiles of Ca K, Ca H, and Hα from the HIRES spectra. The lower panels show the differences of each individual spectrum relative to the median spectrum. The bump in the red wing of Ca H is Hϵ. The spectra in the lower panels are smoothed for visualization purposes.
Paper: A 38 Million Year Old Neptune-sized Planet in the Kepler Field
Authors: L. G. Bouma, J. L. Curtis, K. Masuda, L. A. Hillenbrand, G. Stefansson, H. Isaacson, N. Narita, A. Fukui, M. Ikoma, M. Tamura, A. L. Kraus, E. Furlan, C. L. Gnilka, K. V. Lester, S. B. Howell
Figure caption: Transit model residuals through time (binned by year of observation). Left: phase-folded transit of Kepler 1627b, with stellar variability removed. Points and models are as in Figure 10. Right: as on the left, with the transit removed.
Paper: Difference of Photometric Properties between Regular and Nonregular Miras in the Magellanic Clouds
Authors: Jia-Yu Ou, Chow-Choong Ngeow
Figure caption: The VI-band light curves (top panels), the (V − I) color curves (middle panels), and the corresponding CMD (bottom panels) for a typical regular and nonregular Mira, presented on the left and right panels, respectively. The color of the data points in the bottom two panels corresponds to the time of observations.
Paper: Difference of Photometric Properties between Regular and Nonregular Miras in the Magellanic Clouds
Authors: Jia-Yu Ou, Chow-Choong Ngeow
Figure caption: Examples of SED fittings for regular Miras (left column) and nonregular Miras (right column). The data points in blue crosses are the available photometric data taken from the SIMBAD database. The red dashed and blue dotted curves are the best-fit blackbody radiation function for representing the star and the dust components, respectively. The sum of these two components is shown as the black solid curves. In the left column, the black dashed curves are the resulting SED fit using the DESK model (see text for details).
Paper: Difference of Photometric Properties between Regular and Nonregular Miras in the Magellanic Clouds
Authors: Jia-Yu Ou, Chow-Choong Ngeow
Figure caption: The VI-band CMD for the regular Miras (left panel) and nonregular Miras (right panels) in the LMC. Each data point represents the time-resolved I-band magnitude and the (V − I) color, based on the OGLE-III light curve, for every available LMC Miras in the OGLE database.
Paper: Difference of Photometric Properties between Regular and Nonregular Miras in the Magellanic Clouds
Authors: Jia-Yu Ou, Chow-Choong Ngeow
Figure caption: PR relation for nonregular Miras, separated for the stellar component with P  s  (left panel), the dust component with P  s  (middle panel), and the dust component with P  l  (right panel), based on the results of our SEDs fitting (see Table 5). The dashed line on the left panel is the “death line” adopted from Trabucchi et al. (2021).
Paper: Difference of Photometric Properties between Regular and Nonregular Miras in the Magellanic Clouds
Authors: Jia-Yu Ou, Chow-Choong Ngeow
Figure caption: Composite of the fitted SED between the I-band and 10 micron. The left for the regular Miras and the right for nonregular Miras. It is clear that the peaks of the SED for regular Miras are around ∼1.26 micron (or ﹩\mathrm{log}\lambda \sim 0.1﹩), but for nonregular Miras the peaks are around ∼1.6 to ∼6.3 micron (or ﹩\mathrm{log}\lambda \sim 0.2﹩ to ∼0.8).
Paper: Difference of Photometric Properties between Regular and Nonregular Miras in the Magellanic Clouds
Authors: Jia-Yu Ou, Chow-Choong Ngeow
Figure caption:  JHK-band color–color diagram for various samples of Miras. The blue and green points are the dust-poor and dust-rich Miras presented in Whitelock et al. (2000) and Whitelock & Feast (2000), respectively. The red and black crosses are the regular and nonregular Miras in the LMC, respectively, based on the single-epoch 2MASS data. Similarly, the red and black triangles are the regular and nonregular Miras in the LMC, respectively, based on the multiepoch LMCNISS data.
Paper: Difference of Photometric Properties between Regular and Nonregular Miras in the Magellanic Clouds
Authors: Jia-Yu Ou, Chow-Choong Ngeow
Figure caption: PR relation for regular Miras, separated for the stellar component (left panel) and the dust component (right panel), based on the results of our SEDs fitting (see Table 5). The dashed line on the left panel is the “death line” adopted from Trabucchi et al. (2021).
Paper: Revisiting WASP-47 with ESPRESSO and TESS
Authors: Edward M. Bryant, Daniel Bayliss
Figure caption: Mass–radius diagram for low-mass exoplanets. The measurements and uncertainties are taken from the NASA Exoplanet Archive (accessed 2021 May 12). The black points show exoplanets with masses and radii measured to better than 10% precision. WASP-47 e is shown with the magenta star, and 55-Cancri e is plotted with the blue triangle. These two planets now have the most precise density measurements for any known super-Earths. The solid lines give various composition models from Zeng et al. (2016, 2019).
Paper: Revisiting WASP-47 with ESPRESSO and TESS
Authors: Edward M. Bryant, Daniel Bayliss
Figure caption: Comparison of transmission spectroscopy metric vs. orbital period for various known exoplanets. We plot the sample of planets from the NASA Exoplanet Archive with a radius measured to better than 10% precision and a mass measured to better than 50% precision (gray points), the JWST community targets (green squares; Stevenson et al. 2016) and the sample of planets from Figure 11 (black points). WASP-47 b and WASP-47 e are depicted by the magenta stars and 55-Cancri e by the blue triangle.
Paper: Revisiting WASP-47 with ESPRESSO and TESS
Authors: Edward M. Bryant, Daniel Bayliss
Figure caption: The variation of bulk planetary density with stellar irradiation for the sample of planets plotted in Figure 11. WASP-47 e is depicted by the magenta star and 55-Cancri e by the blue triangle.
Paper: Revisiting WASP-47 with ESPRESSO and TESS
Authors: Edward M. Bryant, Daniel Bayliss
Figure caption: Planet bulk density plotted against stellar metallicity for WASP-47 e, 55-Cancri e, and the sample of super-Earths from Figure 11.
Paper: Plaskett 1.8 m Observations of Starlink Satellites
Authors: Aaron C. Boley, Ewan Wright, Samantha Lawler, Paul Hickson, Dave Balam
Figure caption: Magnitude distributions for the Starlink satellites observed in this study. Each satellite was observed once only. Left: apparent m  g  magnitudes, with blue showing the contribution to each bin from Starlinks and red the Starlink-Vs. Right: similar to the left panel, but for the range corrected magnitude, as defined by seeing the satellite at a range of 550 km. No STO correction is applied. Because some values fall on bin edges, we use the interval [a, b) for edges a and b when assigning a magnitude to a bin.
Paper: A Possible Alignment Between the Orbits of Planetary Systems and their Visual Binary Companions
Authors: Sam Christian, Andrew Vanderburg, Juliette Becker, Daniel A. Yahalomi, Logan Pearce, George Zhou, Karen A. Collins, Adam L. Kraus, Keivan G. Stassun, Zoe de Beurs, George R. Ricker, Roland K. Vanderspek, David W. Latham, Joshua N. Winn, S. Seager, Jon M. Jenkins, Lyu Abe, Karim Agabi, Pedro J. Amado, David Baker, Khalid Barkaoui, Zouhair Benkhaldoun, Paul Benni, John Berberian, Perry Berlind, Allyson Bieryla, Emma Esparza-Borges, Michael Bowen, Peyton Brown, Lars A. Buchhave, Christopher J. Burke, Marco Buttu, Charles Cadieux, Douglas A. Caldwell, David Charbonneau, Nikita Chazov, Sudhish Chimaladinne, Kevin I. Collins, Deven Combs, Dennis M. Conti, Nicolas Crouzet, Jerome P. de Leon, Shila Deljookorani, Brendan Diamond, René Doyon, Diana Dragomir, Georgina Dransfield, Zahra Essack, Phil Evans, Akihiko Fukui, Tianjun Gan, Gilbert A. Esquerdo, Michaël Gillon, Eric Girardin, Pere Guerra, Tristan Guillot, Eleanor Kate K. Habich, Andreea Henriksen, Nora Hoch, Keisuke I Isogai, Emmanuël Jehin, Eric L. N. Jensen, Marshall C. Johnson, John H. Livingston, John F. Kielkopf, Kingsley Kim, Kiyoe Kawauchi, Vadim Krushinsky, Veronica Kunzle, Didier Laloum, Dominic Leger, Pablo Lewin, Franco Mallia, Bob Massey, Mayuko Mori, Kim K. McLeod, Djamel Mékarnia, Ismael Mireles, Nikolay Mishevskiy, Motohide Tamura, Felipe Murgas, Norio Narita, Ramon Naves, Peter Nelson, Hugh P. Osborn, Enric Palle, Hannu Parviainen, Peter Plavchan, Francisco J. Pozuelos, Markus Rabus, Howard M. Relles, Cristina Rodríguez López, Samuel N. Quinn, Francois-Xavier Schmider, Joshua E. Schlieder, Richard P. Schwarz, Avi Shporer, Laurie Sibbald, Gregor Srdoc, Caitlin Stibbards, Hannah Stickler, Olga Suarez, Chris Stockdale, Thiam-Guan Tan, Yuka Terada, Amaury Triaud, Rene Tronsgaard, William C. Waalkes, Gavin Wang, Noriharu Watanabe, Marie-Sainte Wenceslas, Geof Wingham, Justin Wittrock, Carl Ziegler
Figure caption: Lidov–Kozai timescale for binary systems with exoplanets plotted against the semimajor axis of the binary companion. The color bar represents ∣90° − i∣ for each system. The dashed line represents the approximate ages of the stars (∼1 Gyr). The wide binaries with semimajor axes less than about 700 au are close enough that the Kozai–Lidov effect could operate on similar timescales, but other factors make this explanation for the alignment less likely.
Paper: A Possible Alignment Between the Orbits of Planetary Systems and their Visual Binary Companions
Authors: Sam Christian, Andrew Vanderburg, Juliette Becker, Daniel A. Yahalomi, Logan Pearce, George Zhou, Karen A. Collins, Adam L. Kraus, Keivan G. Stassun, Zoe de Beurs, George R. Ricker, Roland K. Vanderspek, David W. Latham, Joshua N. Winn, S. Seager, Jon M. Jenkins, Lyu Abe, Karim Agabi, Pedro J. Amado, David Baker, Khalid Barkaoui, Zouhair Benkhaldoun, Paul Benni, John Berberian, Perry Berlind, Allyson Bieryla, Emma Esparza-Borges, Michael Bowen, Peyton Brown, Lars A. Buchhave, Christopher J. Burke, Marco Buttu, Charles Cadieux, Douglas A. Caldwell, David Charbonneau, Nikita Chazov, Sudhish Chimaladinne, Kevin I. Collins, Deven Combs, Dennis M. Conti, Nicolas Crouzet, Jerome P. de Leon, Shila Deljookorani, Brendan Diamond, René Doyon, Diana Dragomir, Georgina Dransfield, Zahra Essack, Phil Evans, Akihiko Fukui, Tianjun Gan, Gilbert A. Esquerdo, Michaël Gillon, Eric Girardin, Pere Guerra, Tristan Guillot, Eleanor Kate K. Habich, Andreea Henriksen, Nora Hoch, Keisuke I Isogai, Emmanuël Jehin, Eric L. N. Jensen, Marshall C. Johnson, John H. Livingston, John F. Kielkopf, Kingsley Kim, Kiyoe Kawauchi, Vadim Krushinsky, Veronica Kunzle, Didier Laloum, Dominic Leger, Pablo Lewin, Franco Mallia, Bob Massey, Mayuko Mori, Kim K. McLeod, Djamel Mékarnia, Ismael Mireles, Nikolay Mishevskiy, Motohide Tamura, Felipe Murgas, Norio Narita, Ramon Naves, Peter Nelson, Hugh P. Osborn, Enric Palle, Hannu Parviainen, Peter Plavchan, Francisco J. Pozuelos, Markus Rabus, Howard M. Relles, Cristina Rodríguez López, Samuel N. Quinn, Francois-Xavier Schmider, Joshua E. Schlieder, Richard P. Schwarz, Avi Shporer, Laurie Sibbald, Gregor Srdoc, Caitlin Stibbards, Hannah Stickler, Olga Suarez, Chris Stockdale, Thiam-Guan Tan, Yuka Terada, Amaury Triaud, Rene Tronsgaard, William C. Waalkes, Gavin Wang, Noriharu Watanabe, Marie-Sainte Wenceslas, Geof Wingham, Justin Wittrock, Carl Ziegler
Figure caption: A histogram (a) and scatterplot (b) showing the error in inclination’s distribution and dependence on 90 − i, respectively. The noticeable difference in the errors of (a) is likely caused by more-aligned systems, which are more prevalent in the sample with exoplanets, tending to have tighter constraints on inclination.
Paper: A Possible Alignment Between the Orbits of Planetary Systems and their Visual Binary Companions
Authors: Sam Christian, Andrew Vanderburg, Juliette Becker, Daniel A. Yahalomi, Logan Pearce, George Zhou, Karen A. Collins, Adam L. Kraus, Keivan G. Stassun, Zoe de Beurs, George R. Ricker, Roland K. Vanderspek, David W. Latham, Joshua N. Winn, S. Seager, Jon M. Jenkins, Lyu Abe, Karim Agabi, Pedro J. Amado, David Baker, Khalid Barkaoui, Zouhair Benkhaldoun, Paul Benni, John Berberian, Perry Berlind, Allyson Bieryla, Emma Esparza-Borges, Michael Bowen, Peyton Brown, Lars A. Buchhave, Christopher J. Burke, Marco Buttu, Charles Cadieux, Douglas A. Caldwell, David Charbonneau, Nikita Chazov, Sudhish Chimaladinne, Kevin I. Collins, Deven Combs, Dennis M. Conti, Nicolas Crouzet, Jerome P. de Leon, Shila Deljookorani, Brendan Diamond, René Doyon, Diana Dragomir, Georgina Dransfield, Zahra Essack, Phil Evans, Akihiko Fukui, Tianjun Gan, Gilbert A. Esquerdo, Michaël Gillon, Eric Girardin, Pere Guerra, Tristan Guillot, Eleanor Kate K. Habich, Andreea Henriksen, Nora Hoch, Keisuke I Isogai, Emmanuël Jehin, Eric L. N. Jensen, Marshall C. Johnson, John H. Livingston, John F. Kielkopf, Kingsley Kim, Kiyoe Kawauchi, Vadim Krushinsky, Veronica Kunzle, Didier Laloum, Dominic Leger, Pablo Lewin, Franco Mallia, Bob Massey, Mayuko Mori, Kim K. McLeod, Djamel Mékarnia, Ismael Mireles, Nikolay Mishevskiy, Motohide Tamura, Felipe Murgas, Norio Narita, Ramon Naves, Peter Nelson, Hugh P. Osborn, Enric Palle, Hannu Parviainen, Peter Plavchan, Francisco J. Pozuelos, Markus Rabus, Howard M. Relles, Cristina Rodríguez López, Samuel N. Quinn, Francois-Xavier Schmider, Joshua E. Schlieder, Richard P. Schwarz, Avi Shporer, Laurie Sibbald, Gregor Srdoc, Caitlin Stibbards, Hannah Stickler, Olga Suarez, Chris Stockdale, Thiam-Guan Tan, Yuka Terada, Amaury Triaud, Rene Tronsgaard, William C. Waalkes, Gavin Wang, Noriharu Watanabe, Marie-Sainte Wenceslas, Geof Wingham, Justin Wittrock, Carl Ziegler
Figure caption: A comparison of binaries with exoplanets with and without spectroscopic metallicity measurements from TFOP (a) and the binaries in the control sample with and without archival spectroscopy (which metallicity is derived from). Neither comparison shows a statistically significant difference, so differences in metallicity measurements are unlikely to explain the difference in the inclination distributions between the exoplanet and control sample.
Paper: A Possible Alignment Between the Orbits of Planetary Systems and their Visual Binary Companions
Authors: Sam Christian, Andrew Vanderburg, Juliette Becker, Daniel A. Yahalomi, Logan Pearce, George Zhou, Karen A. Collins, Adam L. Kraus, Keivan G. Stassun, Zoe de Beurs, George R. Ricker, Roland K. Vanderspek, David W. Latham, Joshua N. Winn, S. Seager, Jon M. Jenkins, Lyu Abe, Karim Agabi, Pedro J. Amado, David Baker, Khalid Barkaoui, Zouhair Benkhaldoun, Paul Benni, John Berberian, Perry Berlind, Allyson Bieryla, Emma Esparza-Borges, Michael Bowen, Peyton Brown, Lars A. Buchhave, Christopher J. Burke, Marco Buttu, Charles Cadieux, Douglas A. Caldwell, David Charbonneau, Nikita Chazov, Sudhish Chimaladinne, Kevin I. Collins, Deven Combs, Dennis M. Conti, Nicolas Crouzet, Jerome P. de Leon, Shila Deljookorani, Brendan Diamond, René Doyon, Diana Dragomir, Georgina Dransfield, Zahra Essack, Phil Evans, Akihiko Fukui, Tianjun Gan, Gilbert A. Esquerdo, Michaël Gillon, Eric Girardin, Pere Guerra, Tristan Guillot, Eleanor Kate K. Habich, Andreea Henriksen, Nora Hoch, Keisuke I Isogai, Emmanuël Jehin, Eric L. N. Jensen, Marshall C. Johnson, John H. Livingston, John F. Kielkopf, Kingsley Kim, Kiyoe Kawauchi, Vadim Krushinsky, Veronica Kunzle, Didier Laloum, Dominic Leger, Pablo Lewin, Franco Mallia, Bob Massey, Mayuko Mori, Kim K. McLeod, Djamel Mékarnia, Ismael Mireles, Nikolay Mishevskiy, Motohide Tamura, Felipe Murgas, Norio Narita, Ramon Naves, Peter Nelson, Hugh P. Osborn, Enric Palle, Hannu Parviainen, Peter Plavchan, Francisco J. Pozuelos, Markus Rabus, Howard M. Relles, Cristina Rodríguez López, Samuel N. Quinn, Francois-Xavier Schmider, Joshua E. Schlieder, Richard P. Schwarz, Avi Shporer, Laurie Sibbald, Gregor Srdoc, Caitlin Stibbards, Hannah Stickler, Olga Suarez, Chris Stockdale, Thiam-Guan Tan, Yuka Terada, Amaury Triaud, Rene Tronsgaard, William C. Waalkes, Gavin Wang, Noriharu Watanabe, Marie-Sainte Wenceslas, Geof Wingham, Justin Wittrock, Carl Ziegler
Figure caption: The two empirical cumulative distributions used in the Kolmogorov–Smirnov (K-S) test. The black line shows the maximum distance between the two distributions which corresponds to a K-S value of 0.223 and a p-value of 0.0037.
Paper: A Possible Alignment Between the Orbits of Planetary Systems and their Visual Binary Companions
Authors: Sam Christian, Andrew Vanderburg, Juliette Becker, Daniel A. Yahalomi, Logan Pearce, George Zhou, Karen A. Collins, Adam L. Kraus, Keivan G. Stassun, Zoe de Beurs, George R. Ricker, Roland K. Vanderspek, David W. Latham, Joshua N. Winn, S. Seager, Jon M. Jenkins, Lyu Abe, Karim Agabi, Pedro J. Amado, David Baker, Khalid Barkaoui, Zouhair Benkhaldoun, Paul Benni, John Berberian, Perry Berlind, Allyson Bieryla, Emma Esparza-Borges, Michael Bowen, Peyton Brown, Lars A. Buchhave, Christopher J. Burke, Marco Buttu, Charles Cadieux, Douglas A. Caldwell, David Charbonneau, Nikita Chazov, Sudhish Chimaladinne, Kevin I. Collins, Deven Combs, Dennis M. Conti, Nicolas Crouzet, Jerome P. de Leon, Shila Deljookorani, Brendan Diamond, René Doyon, Diana Dragomir, Georgina Dransfield, Zahra Essack, Phil Evans, Akihiko Fukui, Tianjun Gan, Gilbert A. Esquerdo, Michaël Gillon, Eric Girardin, Pere Guerra, Tristan Guillot, Eleanor Kate K. Habich, Andreea Henriksen, Nora Hoch, Keisuke I Isogai, Emmanuël Jehin, Eric L. N. Jensen, Marshall C. Johnson, John H. Livingston, John F. Kielkopf, Kingsley Kim, Kiyoe Kawauchi, Vadim Krushinsky, Veronica Kunzle, Didier Laloum, Dominic Leger, Pablo Lewin, Franco Mallia, Bob Massey, Mayuko Mori, Kim K. McLeod, Djamel Mékarnia, Ismael Mireles, Nikolay Mishevskiy, Motohide Tamura, Felipe Murgas, Norio Narita, Ramon Naves, Peter Nelson, Hugh P. Osborn, Enric Palle, Hannu Parviainen, Peter Plavchan, Francisco J. Pozuelos, Markus Rabus, Howard M. Relles, Cristina Rodríguez López, Samuel N. Quinn, Francois-Xavier Schmider, Joshua E. Schlieder, Richard P. Schwarz, Avi Shporer, Laurie Sibbald, Gregor Srdoc, Caitlin Stibbards, Hannah Stickler, Olga Suarez, Chris Stockdale, Thiam-Guan Tan, Yuka Terada, Amaury Triaud, Rene Tronsgaard, William C. Waalkes, Gavin Wang, Noriharu Watanabe, Marie-Sainte Wenceslas, Geof Wingham, Justin Wittrock, Carl Ziegler
Figure caption: Distribution of ∣90 − i∣ (with median i) for binaries with exoplanets with semimajor axes (a) below and above 700 au. The binaries with semimajor axes less than 700 au are clustered within 20° of edge-on orbits, while the binaries with semimajor axes greater than 700 show a more uniform distribution of inclinations.
Paper: A Possible Alignment Between the Orbits of Planetary Systems and their Visual Binary Companions
Authors: Sam Christian, Andrew Vanderburg, Juliette Becker, Daniel A. Yahalomi, Logan Pearce, George Zhou, Karen A. Collins, Adam L. Kraus, Keivan G. Stassun, Zoe de Beurs, George R. Ricker, Roland K. Vanderspek, David W. Latham, Joshua N. Winn, S. Seager, Jon M. Jenkins, Lyu Abe, Karim Agabi, Pedro J. Amado, David Baker, Khalid Barkaoui, Zouhair Benkhaldoun, Paul Benni, John Berberian, Perry Berlind, Allyson Bieryla, Emma Esparza-Borges, Michael Bowen, Peyton Brown, Lars A. Buchhave, Christopher J. Burke, Marco Buttu, Charles Cadieux, Douglas A. Caldwell, David Charbonneau, Nikita Chazov, Sudhish Chimaladinne, Kevin I. Collins, Deven Combs, Dennis M. Conti, Nicolas Crouzet, Jerome P. de Leon, Shila Deljookorani, Brendan Diamond, René Doyon, Diana Dragomir, Georgina Dransfield, Zahra Essack, Phil Evans, Akihiko Fukui, Tianjun Gan, Gilbert A. Esquerdo, Michaël Gillon, Eric Girardin, Pere Guerra, Tristan Guillot, Eleanor Kate K. Habich, Andreea Henriksen, Nora Hoch, Keisuke I Isogai, Emmanuël Jehin, Eric L. N. Jensen, Marshall C. Johnson, John H. Livingston, John F. Kielkopf, Kingsley Kim, Kiyoe Kawauchi, Vadim Krushinsky, Veronica Kunzle, Didier Laloum, Dominic Leger, Pablo Lewin, Franco Mallia, Bob Massey, Mayuko Mori, Kim K. McLeod, Djamel Mékarnia, Ismael Mireles, Nikolay Mishevskiy, Motohide Tamura, Felipe Murgas, Norio Narita, Ramon Naves, Peter Nelson, Hugh P. Osborn, Enric Palle, Hannu Parviainen, Peter Plavchan, Francisco J. Pozuelos, Markus Rabus, Howard M. Relles, Cristina Rodríguez López, Samuel N. Quinn, Francois-Xavier Schmider, Joshua E. Schlieder, Richard P. Schwarz, Avi Shporer, Laurie Sibbald, Gregor Srdoc, Caitlin Stibbards, Hannah Stickler, Olga Suarez, Chris Stockdale, Thiam-Guan Tan, Yuka Terada, Amaury Triaud, Rene Tronsgaard, William C. Waalkes, Gavin Wang, Noriharu Watanabe, Marie-Sainte Wenceslas, Geof Wingham, Justin Wittrock, Carl Ziegler
Figure caption: A comparison in the distribution of inclinations in binary systems in the control sample with 2 minute cadence and those without. The two distributions are essentially indistinguishable, so selection biases from the TESS 2 minute target selection are unlikely to affect our results.
Paper: A Possible Alignment Between the Orbits of Planetary Systems and their Visual Binary Companions
Authors: Sam Christian, Andrew Vanderburg, Juliette Becker, Daniel A. Yahalomi, Logan Pearce, George Zhou, Karen A. Collins, Adam L. Kraus, Keivan G. Stassun, Zoe de Beurs, George R. Ricker, Roland K. Vanderspek, David W. Latham, Joshua N. Winn, S. Seager, Jon M. Jenkins, Lyu Abe, Karim Agabi, Pedro J. Amado, David Baker, Khalid Barkaoui, Zouhair Benkhaldoun, Paul Benni, John Berberian, Perry Berlind, Allyson Bieryla, Emma Esparza-Borges, Michael Bowen, Peyton Brown, Lars A. Buchhave, Christopher J. Burke, Marco Buttu, Charles Cadieux, Douglas A. Caldwell, David Charbonneau, Nikita Chazov, Sudhish Chimaladinne, Kevin I. Collins, Deven Combs, Dennis M. Conti, Nicolas Crouzet, Jerome P. de Leon, Shila Deljookorani, Brendan Diamond, René Doyon, Diana Dragomir, Georgina Dransfield, Zahra Essack, Phil Evans, Akihiko Fukui, Tianjun Gan, Gilbert A. Esquerdo, Michaël Gillon, Eric Girardin, Pere Guerra, Tristan Guillot, Eleanor Kate K. Habich, Andreea Henriksen, Nora Hoch, Keisuke I Isogai, Emmanuël Jehin, Eric L. N. Jensen, Marshall C. Johnson, John H. Livingston, John F. Kielkopf, Kingsley Kim, Kiyoe Kawauchi, Vadim Krushinsky, Veronica Kunzle, Didier Laloum, Dominic Leger, Pablo Lewin, Franco Mallia, Bob Massey, Mayuko Mori, Kim K. McLeod, Djamel Mékarnia, Ismael Mireles, Nikolay Mishevskiy, Motohide Tamura, Felipe Murgas, Norio Narita, Ramon Naves, Peter Nelson, Hugh P. Osborn, Enric Palle, Hannu Parviainen, Peter Plavchan, Francisco J. Pozuelos, Markus Rabus, Howard M. Relles, Cristina Rodríguez López, Samuel N. Quinn, Francois-Xavier Schmider, Joshua E. Schlieder, Richard P. Schwarz, Avi Shporer, Laurie Sibbald, Gregor Srdoc, Caitlin Stibbards, Hannah Stickler, Olga Suarez, Chris Stockdale, Thiam-Guan Tan, Yuka Terada, Amaury Triaud, Rene Tronsgaard, William C. Waalkes, Gavin Wang, Noriharu Watanabe, Marie-Sainte Wenceslas, Geof Wingham, Justin Wittrock, Carl Ziegler
Figure caption: A clear alignment of binary and exoplanet below approximately 700 au is seen in (a), the sample with exoplanet candidates. No such alignment below 700 au is seen in (b), the control sample.