adsabs/AstroCLIMB huggingface dataset:
Paper: Catalog of Wide Binary, Trinary and Quaternary Candidates from the Gaia Data Release 2 (Region ∣b∣ > 25°)
Authors: Petr Zavada, Karel Píška
Figure caption: Distributions of true binaries P bin (red and blue,which is wider, due to measurement errors) and background P  bg  (green). Parameter η represent some selection parameter (d ij, α ij, …). The numbers of the true binaries n 2 are given by the area under red and blue curves. Corresponding numbers of background pairs b 2 are given by the yellow area and the whole area under the green curve.
Paper: Catalog of Wide Binary, Trinary and Quaternary Candidates from the Gaia Data Release 2 (Region ∣b∣ > 25°)
Authors: Petr Zavada, Karel Píška
Figure caption: Correlation of angular separation d ij[as] and projected distance Δij[pc] for α ≤ α  c . Left and right panel–linear and logarithmic scales. Binning: 1.44 as × 0.004 pc, 0.36 as × 0.001 pc.
Paper: Catalog of Wide Binary, Trinary and Quaternary Candidates from the Gaia Data Release 2 (Region ∣b∣ > 25°)
Authors: Petr Zavada, Karel Píška
Figure caption: Projected distance Δij of pairs in domains A  of regions  R  1 and  R  2    defined in Figure 8. ( a): all events; (b): enriched exposition; (c): only stars of magnitude G ≤ 15. Binning: 0.0004 pc.
Paper: Catalog of Wide Binary, Trinary and Quaternary Candidates from the Gaia Data Release 2 (Region ∣b∣ > 25°)
Authors: Petr Zavada, Karel Píška
Figure caption: (a): correlation of the transverse separation Δij with the transverse velocity v ij of orbital motion in region  R . (b) and (c): distributions of Δij and v ij in domain (37). Units: Δij[pc], v ij[kms−1]. Binning: 0.001 pc × 0.1 km s−1, 0.001 pc, 0.1 km s−1.
Paper: Catalog of Wide Binary, Trinary and Quaternary Candidates from the Gaia Data Release 2 (Region ∣b∣ > 25°)
Authors: Petr Zavada, Karel Píška
Figure caption: Distributions of angular separations x ijk, y ijk and d ijk in trinary candidates. Upper panels show results from the region  R  (enriched exposition). The lower panels represent background. Unit: x ijk, y ijk, d ijk[as]. Binning: 2.88 as × 2.88 as, 0.288 as.
Paper: Catalog of Wide Binary, Trinary and Quaternary Candidates from the Gaia Data Release 2 (Region ∣b∣ > 25°)
Authors: Petr Zavada, Karel Píška
Figure caption: Distributions of angular separations d ij. Left: random sources with the admixture of close pairs. Right: real event data from region  R  (enriched exposition). Unit: d ij[as]. Binning: 0.288 as.
Paper: Catalog of Wide Binary, Trinary and Quaternary Candidates from the Gaia Data Release 2 (Region ∣b∣ > 25°)
Authors: Petr Zavada, Karel Píška
Figure caption: Distributions of angular triangle separations x ijk, y ijk and d  ijk  for the same set of simulated events used in the previous figure. Unit: x ijk, y ijk, d ijk[as]. Binning: 2.88 as × 2.88 as, 0.288 as.
Paper: Catalog of Wide Binary, Trinary and Quaternary Candidates from the Gaia Data Release 2 (Region ∣b∣ > 25°)
Authors: Petr Zavada, Karel Píška
Figure caption: Examples of patterns relevant to the selection (rejection) of candidates for multiple stars.
Paper: Catalog of Wide Binary, Trinary and Quaternary Candidates from the Gaia Data Release 2 (Region ∣b∣ > 25°)
Authors: Petr Zavada, Karel Píška
Figure caption: Distances of all candidate sources. Binning: 30 pc.
Paper: Catalog of Wide Binary, Trinary and Quaternary Candidates from the Gaia Data Release 2 (Region ∣b∣ > 25°)
Authors: Petr Zavada, Karel Píška
Figure caption: Correlation of radial velocities for 6469 pairs. Unit: [km s−1].
Paper: Catalog of Wide Binary, Trinary and Quaternary Candidates from the Gaia Data Release 2 (Region ∣b∣ > 25°)
Authors: Petr Zavada, Karel Píška
Figure caption: Distribution of velocities v ij for all pairs (left) and for pairs in the peak (15) (right) in the region  R  1 (enriched exposition). Unit: v ij[km s−1]. Binning: 0.1 km s−1.
Paper: Difference of Photometric Properties between Regular and Nonregular Miras in the Magellanic Clouds
Authors: Jia-Yu Ou, Chow-Choong Ngeow
Figure caption: Left Panel: histogram of P  l /P  s  ratio for nonregular Miras in the sample. Right Panel: P  l /P  s  ratios as a function of P  s .
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 light curves for nonregular Miras. The black curves are the best-fit light curves based on the determined short- and long-term periods, as described in the text. The dashed curves are the long-term variation L  l (t) given by Equation (3).
Paper: Difference of Photometric Properties between Regular and Nonregular Miras in the Magellanic Clouds
Authors: Jia-Yu Ou, Chow-Choong Ngeow
Figure caption: PL relations for nonregular Miras in the LMC, using either the P  s  (left panel), the P  l  (middle panel), or the P  l /P  s  ratios (right panel) as independent variables.
Paper: Difference of Photometric Properties between Regular and Nonregular Miras in the Magellanic Clouds
Authors: Jia-Yu Ou, Chow-Choong Ngeow
Figure caption: PL relations at maximum light (left panel) and at mean light (right panel) for nonregular Miras after removing the long-term variations. The curves are the fitted quadratic models as given in Table 2 and not the fittings to the O-rich nonregular Miras.
Paper: Difference of Photometric Properties between Regular and Nonregular Miras in the Magellanic Clouds
Authors: Jia-Yu Ou, Chow-Choong Ngeow
Figure caption: PL relations for regular Miras in the LMC. The green dashed lines and the blue solid lines are the fitted PL relations using the two-slope model at maximum (black circles) and mean (red triangles) light, respectively.
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 light curves for nonregular Miras after removing the long-term variation L  l (t).
Paper: Difference of Photometric Properties between Regular and Nonregular Miras in the Magellanic Clouds
Authors: Jia-Yu Ou, Chow-Choong Ngeow
Figure caption: PL relations for regular Miras in the LMC. The green dashed lines and the blue solid lines are the fitted PL relations using the quadratic model at maximum (black circles) and mean (red triangles) light, respectively.
Paper: Difference of Photometric Properties between Regular and Nonregular Miras in the Magellanic Clouds
Authors: Jia-Yu Ou, Chow-Choong Ngeow
Figure caption: Same as in Figure 9, but for the combined samples of regular Miras in the LMC and SMC.
Paper: Difference of Photometric Properties between Regular and Nonregular Miras in the Magellanic Clouds
Authors: Jia-Yu Ou, Chow-Choong Ngeow
Figure caption: Same as in Figure 8, but for the combined samples of regular Miras in the LMC and SMC.
Paper: Revisiting WASP-47 with ESPRESSO and TESS
Authors: Edward M. Bryant, Daniel Bayliss
Figure caption: Generalized Lomb–Scargle periodograms for ESPRESSO radial-velocity residuals to the initial model from Section 3.2 (top), the ESPRESSO CCF FWHM measurements (middle), measurements of ﹩\mathrm{log}{R}_{\mathrm{HK}}^{{\prime} }﹩ from the ESPRESSO spectra (bottom). The solid vertical blue line denotes the rotation period of P Rot = 32.5 days derived from the K2 photometry, with the vertical dashed blue lines marking P Rot/2 and P Rot/3 harmonics. The shaded area highlights stellar rotation periods that are excluded by the calculated minimum rotation period of 28.762 days. The horizontal lines indicate the 1% (dashed) and 10% (solid) false-alarm probabilities, respectively.
Paper: Revisiting WASP-47 with ESPRESSO and TESS
Authors: Edward M. Bryant, Daniel Bayliss
Figure caption: Top: K2 photometry from campaign 3 for WASP-47 used for the rotation analysis in this work. The gray points show the detrended data (see Section 3.3.1) and the blue points give the data binned to a timescale of 1 day. The orange line shows the most significant Lomb–Scargle period of 16.26 days with an amplitude of 0.1 mmag. Bottom: Lomb–Scargle periodogram for the K2 photometry. As with Figure 6 the shaded area highlights the rotation periods excluded by the minimum P Rot = ﹩{P}_{\mathrm{Rot};\min }﹩. The significant peak at 16.26  days likely corresponds to half the true rotation period. The horizontal lines give the 0.1% (solid) and 0.01% (dashed) false-alarm probabilities, respectively.
Paper: Revisiting WASP-47 with ESPRESSO and TESS
Authors: Edward M. Bryant, Daniel Bayliss
Figure caption: Phase-folded Transiting Exoplanet Survey Satellite photometry of WASP-47 zoomed around the transit events for WASP-47 b (top), WASP-47 d (middle), and WASP-47 e (bottom). For all panels the photometry (blue circles) has had the transit models from the other two planets subtracted and is binned in phase on a timescale of 20 minutes for WASP-47 b and WASP-47 e and 60 minutes for WASP-47 d. The orange lines show the best-fit transit models from the modeling in Section 3.1.
Paper: Revisiting WASP-47 with ESPRESSO and TESS
Authors: Edward M. Bryant, Daniel Bayliss
Figure caption: Measured transit times for WASP-47 b transit events in the Transiting Exoplanet Survey Satellite (TESS) data (black circles) compared with the literature ephemeris (blue square and green shaded regions) from Becker et al. (2015). The uncertainties on the TESS transit times have had an additional 1 minute added in quadrature to account for the transit timing variations of WASP-47 b. The shaded green regions give the 1, 2, and 3σ uncertainties of the predicted ephemeris from Becker et al. (2015). The red dashed line represents the updated ephemeris determined in this work.
Paper: Revisiting WASP-47 with ESPRESSO and TESS
Authors: Edward M. Bryant, Daniel Bayliss
Figure caption: ESPRESSO time-series data for WASP-47. Top: ESPRESSO radial-velocity measurements with the systemic velocity γ ESP subtracted. The blue line gives the full Keplerian model for all four planets and the Gaussian process (GP). Second: ESPRESSO radial-velocity measurements with γ ESP, the Keplerian models for WASP-47 b and c, and the GP model subtracted. The blue line gives the two-planet Keplerian model for WASP-47 d and e. Third: ESPRESSO radial-velocity residuals to the four-planet Keplerian model. The red line gives the GP model and the shaded area provides the 1σ confidence interval of the GP. Bottom: FWHM measurements of the ESPRESSO CCFs. The orange line gives the GP model and the shaded area provides the 1σ confidence interval of the GP.
Paper: Revisiting WASP-47 with ESPRESSO and TESS
Authors: Edward M. Bryant, Daniel Bayliss
Figure caption: Transiting Exoplanet Survey Satellite 20 s PDCSAP_FLUX photometry for WASP-47. The colored bars at the bottom show the positions of the transits of WASP-47 b (blue), WASP-47 d (green), and WASP-47 e (orange), with the dashed bars showing the positions of transits which fall in the large data gap caused by Earth and Moon crossing events.
Paper: Revisiting WASP-47 with ESPRESSO and TESS
Authors: Edward M. Bryant, Daniel Bayliss
Figure caption: The contrast and FWHM values for the ESPRESSO cross-correlation functions for our observations of WASP-47. We see a strong anticorrelation, indicative of spot-induced stellar activity (Boisse et al. 2011).
Paper: Revisiting WASP-47 with ESPRESSO and TESS
Authors: Edward M. Bryant, Daniel Bayliss
Figure caption: Phase-folded radial velocities with all Gaussian processes (GPs) and systemic velocities removed for WASP-47 b (top), WASP-47 c (second), WASP-47 d (third), and WASP-47 e (bottom). The colors of the data from the various instruments are as follows: ESPRESSO (red), HARPS-N (blue), HIRES (green), and CORALIE (magenta). Note we do not plot the CORALIE data for planets d and e as the rms of the CORALIE data is larger than the semiamplitudes of these two planets.
Paper: Revisiting WASP-47 with ESPRESSO and TESS
Authors: Edward M. Bryant, Daniel Bayliss
Figure caption: Observed transit timing variations (TTVs) for WASP-47 b for the transits in the (left) K2 photometry and (right) TESS photometry. The orange line gives the TTV model from Becker et al. (2015).
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: Images from the Pan-STARRS survey (Chambers et al. 2016) of selected binary systems from our sample of transiting exoplanet hosts. In each image, the exoplanet host and its binary companion are labeled (with the planet host labeled as a TOI); red arrows show their relative proper motion after subtracting the velocity of the system’s center of mass. The blue bar at the top of each image shows the scale. The two images are labeled with the binary inclination from our LOFTI fits. The image on the left is misaligned with the orbit of the transiting planet, while the image on the right shows an aligned orbit. In general, only orbits with i = 90 will have proper motion vectors that are parallel to the projected semimajor axis. All other angles between proper motion vectors and projected semimajor axes a priori allow all inclination values, although given a uniform prior on eccentricity, higher inclination values will be favored for nearly parallel semimajor axis and proper motion vectors.
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: Histogram of ∣90 − i∣ (a) and ﹩\sin (| 90-i| )﹩ (b). We see an overabundance of systems with i ≈ 90° in our exoplanet sample compared to our control sample, indicating that there is some preferential alignment between the orbital planes of close-in exoplanets and visual binaries. We also find that the inclinations of binaries in our control sample are significantly different from the expected purely random ﹩\sin (i)﹩ distribution (the dashed line in (b)), likely due to either selection effects (El-Badry & Rix 2018) or biases from inferring orbits from short arcs (Ferrer-Chávez et al. 2021).
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 diagram of the orbital configurations relevant to this paper. The diagram is centered on the primary star. Apparent relative alignment is calculated as ∣90° − i∣, where i is the inclination of the binary system (the transiting exoplanets will always have approximately 90° inclination). In the diagram, the green wedge is the inclination of the binary system. The primary star is the star that hosts the exoplanet, while the binary companion is the companion star without detected exoplanets. The angular momentum of the star is the axis that the star rotates on. The exoplanet (orange) orbits at 90° to the line of sight.
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: Histograms of properties of the binary systems. From left to right: parallax in milliarcseconds, projected separation in arcminutes, apparent G magnitude, BP − RP color, G  p  − G  s , where p is the primary star (defined as the brighter star) and s is the secondary star, ﹩{\mathrm{log}}_{10}(a)﹩ where a is the projected semimajor axis, and mass ratio of the primary and secondary star.