adsabs/AstroCLIMB huggingface dataset:
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 between the masses derived using isochrone fitting in this paper versus the TIC-derived masses for the control sample. The plotted error bars are one standard deviation. An orange line denotes where a 1:1 correspondence of masses would lie. We see good correspondence between our mass estimates and those in the TIC.
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 hierarchy of the cuts performed on the sample of visual binaries with transiting exoplanet candidates. The same cuts were performed on the control sample. The specific cuts performed are described in detail in Section 2.
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: Most of the planets in our sample are small (1–5 R ⊕), and thus have relatively low false-positive probabilities (e.g., Morton & Johnson 2011; Guerrero et al. 2021) compared to giant planet candidates (Santerne et al. 2012).
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: 100 orbits from the posterior of a sample LOFTI fit.
Paper: Atmospheric and Fundamental Parameters of Eight Nearby Multiple Stars
Authors: Abdallah M. Hussein, Mashhoor A. Al-Wardat, Ahmad Abushattal, Hatem S. Widyan, Enas M. Abu-Alrob, Oleg Malkov, Martin A. Barstow
Figure caption: The position of components of the HIP 46199 on the HR diagram, the isochrones (left), and the evolutionary tracks (right) for solar metallicity. The evolutionary tracks and isochrones are taken from (Girardi et al. 2000b), where (H) is Hipparcos parallax, (G2) is Gaia DR2 parallax, and (G3) is Gaia EDR3 parallax.
Paper: Atmospheric and Fundamental Parameters of Eight Nearby Multiple Stars
Authors: Abdallah M. Hussein, Mashhoor A. Al-Wardat, Ahmad Abushattal, Hatem S. Widyan, Enas M. Abu-Alrob, Oleg Malkov, Martin A. Barstow
Figure caption: The position of components of the HIP 14524 on the HR diagram, the isochrones (left), and the evolutionary tracks (right) for solar metallicity. The evolutionary tracks and isochrones are taken from (Girardi et al. 2000b), where (Ph) is the photometric parallax and (H) is Hipparcos parallax.
Paper: Atmospheric and Fundamental Parameters of Eight Nearby Multiple Stars
Authors: Abdallah M. Hussein, Mashhoor A. Al-Wardat, Ahmad Abushattal, Hatem S. Widyan, Enas M. Abu-Alrob, Oleg Malkov, Martin A. Barstow
Figure caption: The dynamical mass calculated in this work vs. Al-Wardat’s estimated mass sum. The line represents y = x. Based on Hipparcos 2 parallax (Red), Gaia DR2 parallax (Blue), Gaia EDR3 (Green), and photometric parallax (Black).
Paper: Atmospheric and Fundamental Parameters of Eight Nearby Multiple Stars
Authors: Abdallah M. Hussein, Mashhoor A. Al-Wardat, Ahmad Abushattal, Hatem S. Widyan, Enas M. Abu-Alrob, Oleg Malkov, Martin A. Barstow
Figure caption: The position of components of the HIP 28671 on the HR diagram, the isochrones (left), and the evolutionary tracks (right) for low-metalicity stars Z = 0.001 metallicity. The evolutionary tracks and isochrones are taken from (Girardi et al. 2000b).
Paper: Atmospheric and Fundamental Parameters of Eight Nearby Multiple Stars
Authors: Abdallah M. Hussein, Mashhoor A. Al-Wardat, Ahmad Abushattal, Hatem S. Widyan, Enas M. Abu-Alrob, Oleg Malkov, Martin A. Barstow
Figure caption: The position of components of the HIP 60444 on the HR diagram, the isochrones (left), and the evolutionary tracks (right) for solar metallicity. The evolutionary tracks and isochrones are taken from (Girardi et al. 2000b), where (G3) is Gaia EDR3 parallax, and (H) is Hipparcos parallax.
Paper: Atmospheric and Fundamental Parameters of Eight Nearby Multiple Stars
Authors: Abdallah M. Hussein, Mashhoor A. Al-Wardat, Ahmad Abushattal, Hatem S. Widyan, Enas M. Abu-Alrob, Oleg Malkov, Martin A. Barstow
Figure caption: The position of components of the HIP 16025 on the HR diagram with evolutionary tracks and ages line. The evolutionary tracks and age line which taken from Girardi et al. (2000b), where (G2) is Gaia DR2 parallax, (G3) is Gaia EDR3 parallax, and (H) is Hipparcos parallax.
Paper: Atmospheric and Fundamental Parameters of Eight Nearby Multiple Stars
Authors: Abdallah M. Hussein, Mashhoor A. Al-Wardat, Ahmad Abushattal, Hatem S. Widyan, Enas M. Abu-Alrob, Oleg Malkov, Martin A. Barstow
Figure caption: The position of components of the HIP 47791 on the HR diagram with evolutionary tracks and ages line. The evolutionary tracks and age line taken from Girardi et al. (2000b)
Paper: Atmospheric and Fundamental Parameters of Eight Nearby Multiple Stars
Authors: Abdallah M. Hussein, Mashhoor A. Al-Wardat, Ahmad Abushattal, Hatem S. Widyan, Enas M. Abu-Alrob, Oleg Malkov, Martin A. Barstow
Figure caption: Structure of HIP 28671.
Paper: Atmospheric and Fundamental Parameters of Eight Nearby Multiple Stars
Authors: Abdallah M. Hussein, Mashhoor A. Al-Wardat, Ahmad Abushattal, Hatem S. Widyan, Enas M. Abu-Alrob, Oleg Malkov, Martin A. Barstow
Figure caption: The synthetic SEDs of entire and individual components for the eight system.
Paper: Atmospheric and Fundamental Parameters of Eight Nearby Multiple Stars
Authors: Abdallah M. Hussein, Mashhoor A. Al-Wardat, Ahmad Abushattal, Hatem S. Widyan, Enas M. Abu-Alrob, Oleg Malkov, Martin A. Barstow
Figure caption: The position of components of the HIP 73085 on the HR diagram, the isochrones (left), and the evolutionary tracks (right) for solar metallicity. The evolutionary tracks and isochrones are taken from (Girardi et al. 2000b), where (G2) is Gaia DR2 parallax and (G3) is Gaia EDR2 parallax.
Paper: Atmospheric and Fundamental Parameters of Eight Nearby Multiple Stars
Authors: Abdallah M. Hussein, Mashhoor A. Al-Wardat, Ahmad Abushattal, Hatem S. Widyan, Enas M. Abu-Alrob, Oleg Malkov, Martin A. Barstow
Figure caption: The position of components of the HIP 61100 on the HR diagram, the isochrones (left), and the evolutionary tracks (right) for solar metallicity. The evolutionary tracks and isochrones are taken from Girardi et al. (2000b).
Paper: Bayesian Inference in Single-line Spectroscopic Binaries with a Visual Orbit
Authors: Miguel Videla, Rene A. Mendez, Rubén M. Clavería, Jorge F. Silva, Marcos E. Orchard
Figure caption: Estimated orbit and RV curves for the HIP 3504 binary system. First column: MAP point estimate projection of the posterior distribution for the SB1, SB1 + p(ϖ), SB1 + p(m 1∣θ), and SB1 + p(ϖ) + p(m 1∣θ) cases. Second to fifth columns: projected posterior distribution of the SB1 SB1 + p(ϖ), SB1 + p(m 1∣θ), and SB1 + p(ϖ) + p(m 1∣θ) cases.
Paper: Bayesian Inference in Single-line Spectroscopic Binaries with a Visual Orbit
Authors: Miguel Videla, Rene A. Mendez, Rubén M. Clavería, Jorge F. Silva, Marcos E. Orchard
Figure caption: Same as Figure 14 but for the HIP 109951 binary system.
Paper: Bayesian Inference in Single-line Spectroscopic Binaries with a Visual Orbit
Authors: Miguel Videla, Rene A. Mendez, Rubén M. Clavería, Jorge F. Silva, Marcos E. Orchard
Figure caption: Same as Figure 13 but for the HIP 99675 binary system.
Paper: Bayesian Inference in Single-line Spectroscopic Binaries with a Visual Orbit
Authors: Miguel Videla, Rene A. Mendez, Rubén M. Clavería, Jorge F. Silva, Marcos E. Orchard
Figure caption: Same as Figure 14 but for the HIP 99675 binary system.
Paper: Bayesian Inference in Single-line Spectroscopic Binaries with a Visual Orbit
Authors: Miguel Videla, Rene A. Mendez, Rubén M. Clavería, Jorge F. Silva, Marcos E. Orchard
Figure caption: Same as Figure 13 but for the HIP 109951 binary system.
Paper: Classifying Be Star Variability With TESS. I. The Southern Ecliptic
Authors: Jonathan Labadie-Bartz, Alex C. Carciofi, Tajan Henrique de Amorim, Amanda Rubio, André Luiz Figueiredo, Pedro Ticiani dos Santos, Keegan Thomson-Paressant
Figure caption: A selection of frequency spectra showing various permutations of group configurations and morphology. Solid colored vertical lines are the signals recovered with iterative pre-whitening, and the solid black line is the modified Fourier periodogram without any pre-whitening. The inverted solid lines show the same frequencies multiplied by two, and below that, the dashed lines show the frequencies multiplied by three to aid in visualizing the locations of the first and second harmonics of the recovered signals. The center of the two main frequency groups (g1 and g2) are marked in each plot with the symbol size indicating which is the stronger of the two (or with equal symbol sizes when both groups are similar in strength). Panel (1): closely spaced, narrow groups monotonically decreasing in strength. Panel (2): g1 and g2 have similar strengths, without further harmonics. Panel (3): wider groups, with signals corresponding to the second harmonic of g1, but without significant signals corresponding to the first harmonic of g2 (or the third harmonic of g1). Panel (4): g1 and g2 are wide, and the region beyond g2 is populated with signals that form a “continuum” corresponding to harmonics of signals in g1 and g2. Panel (5): g1 is narrow and dominated by a single signal, and g2 is relatively wide and centered at a frequency less than 2 × g1. Panel (6): g2 is centered at greater than 2 × g1, and there are also signals located in the region occupied by the second harmonic of g1. Panel (7): g1 and g2 are narrow and mirror each other in structure, but there are only signals that correspond to 2 × g2 and not 3 × g1. Panel (8): two fairly typical groups, g1 and g2, being centered near 2.5 and 5 day−1, plus a strong apparently isolated signal at 1.30 day−1 and its weaker subharmonic at 0.65 day−1. Panel (9): widely separated groups, where g2 is stronger than g1, and with power located in the region corresponding to 2 × g2 and not 3 × g1. Panel (10): only one frequency group exists, along with weak low-frequency signals.
Paper: Classifying Be Star Variability With TESS. I. The Southern Ecliptic
Authors: Jonathan Labadie-Bartz, Alex C. Carciofi, Tajan Henrique de Amorim, Amanda Rubio, André Luiz Figueiredo, Pedro Ticiani dos Santos, Keegan Thomson-Paressant
Figure caption: TESS light curves (left) and frequency spectra (right) for a representative selection of Be stars that show certain characteristic features, as described in Section 4. For panel (B), the periodogram is re-calculated after removing the low-frequency (<0.5 day−1) signals (which are shown in a lighter gray color). Panel (F) uses 2 minutes cadence data, which better emphasizes the highest-frequency signals. All other panels use 30 minutes cadence data. The frequency axis of the periodogram in panel (F) is extended to include the high frequencies. Signals at frequencies higher than 10 day−1 are absent in all other stars shown here. The TIC ID, common ID, spectral type, and TESS sectors are printed in the periodogram plots.
Paper: Classifying Be Star Variability With TESS. I. The Southern Ecliptic
Authors: Jonathan Labadie-Bartz, Alex C. Carciofi, Tajan Henrique de Amorim, Amanda Rubio, André Luiz Figueiredo, Pedro Ticiani dos Santos, Keegan Thomson-Paressant
Figure caption: Analysis of an artificial light curve with known signals injected. The locations of injected signals are shown with red dotted vertical lines, with amplitudes of constant signals marked by a red x, and the maximum amplitude of signals that vary in strength with time is marked by a green circle. The frequency spectrum of the artificial light curve is shown in light blue, and the signals found through iterative pre-whitening of the artificial light curve are vertical black lines, where their height reflects the amplitude of the recovered signal. The window function (with arbitrary vertical scale), centered at 3.1 day−1, is shown in panel (B). Note that each sector will have a slightly different window function, and for systems viewed in multiple sectors the window function becomes more narrow. Panel (A): a frequency group where all injected signals have a constant amplitude. Panel (B): a single frequency with a linearly decreasing amplitude is injected. Panel (C): the same as panel (A), but the strongest signal at 3.5 day−1 has a linearly decreasing amplitude. Panel (D): the same as the panel (A), but the middle signal at 3.32 day−1 has a linearly decreasing amplitude. Panel (E): the same as the panel (B), but the amplitude is modulated by a sinusoid. Panel (F): the same as panel (A), but all amplitudes are smaller by a factor of ten.
Paper: Classifying Be Star Variability With TESS. I. The Southern Ecliptic
Authors: Jonathan Labadie-Bartz, Alex C. Carciofi, Tajan Henrique de Amorim, Amanda Rubio, André Luiz Figueiredo, Pedro Ticiani dos Santos, Keegan Thomson-Paressant
Figure caption: Examples of systems with flickers. Below each light curve is the wavelet plot showing the evolution of the frequency spectrum over time after subtracting the low-frequency signals (the red curve), mainly demonstrating how one or both of the frequency groups typically reach higher amplitudes during flickers.
Paper: Classifying Be Star Variability With TESS. I. The Southern Ecliptic
Authors: Jonathan Labadie-Bartz, Alex C. Carciofi, Tajan Henrique de Amorim, Amanda Rubio, André Luiz Figueiredo, Pedro Ticiani dos Santos, Keegan Thomson-Paressant
Figure caption: A system where flickers correspond to the enhancement of the two main frequency groups. First: 2 minutes cadence LC (black), with the low-frequency signals in red. Second: the LC after removing low-frequency signals. Third: wavelet analysis (after removing the low frequencies). Fourth: frequency spectrum (after removing the low frequencies). The top three panels share the same x-axis (TJD).
Paper: Classifying Be Star Variability With TESS. I. The Southern Ecliptic
Authors: Jonathan Labadie-Bartz, Alex C. Carciofi, Tajan Henrique de Amorim, Amanda Rubio, André Luiz Figueiredo, Pedro Ticiani dos Santos, Keegan Thomson-Paressant
Figure caption: The center of the two main frequency groups is shown for each system with a typical frequency group configuration. The stars are ordered according to the location of f  g1, increasing upwards. Black (red) dots mark f  g1 (f  g2), and green triangles mark f  g2 − f  g1. The gray lines are centered at 2 × (f  g1 ± 5%). In the main panel, marker size is proportional to the relative group strength.
Paper: Classifying Be Star Variability With TESS. I. The Southern Ecliptic
Authors: Jonathan Labadie-Bartz, Alex C. Carciofi, Tajan Henrique de Amorim, Amanda Rubio, André Luiz Figueiredo, Pedro Ticiani dos Santos, Keegan Thomson-Paressant
Figure caption: Top: histogram of the ratio of the weighted central frequency of g2 and g1 (f  g2/f  g1). Bottom: comparison of the relative strength of g1 and g2, with the fraction of each spectral subtype bin falling into the three categories printed above its respective bar in the plot. A comparison of the relative strengths of g1 and g2 is also made for all systems with flickers (the majority being early-type).
Paper: Classifying Be Star Variability With TESS. I. The Southern Ecliptic
Authors: Jonathan Labadie-Bartz, Alex C. Carciofi, Tajan Henrique de Amorim, Amanda Rubio, André Luiz Figueiredo, Pedro Ticiani dos Santos, Keegan Thomson-Paressant
Figure caption: Artificial light curve (top), modified Fourier periodogram (left), and wavelet plot (middle) for the first trial discussed in Section 3.4 with two frequency groups, with each signal having a constant amplitude. The wavelet plot shows both groups having apparently variable power, which is solely a consequence of the beating phenomenon. In the wavelet plot, horizontal dashed lines mark the injected frequencies, and regions occupied by hash marks denote gaps in data and regions where wavelet signals are otherwise unreliable due to edge effects.
Paper: Around the Spindle Galaxy: The Dark Halo Mass of NGC 3115
Authors: I. D. Karachentsev, L. N. Makarova, G. S. Anand, R. B. Tully
Figure caption: The distribution of companions around the Spindle galaxy (NGC 3115) in equatorial coordinates. The early-type galaxies and late-type galaxies are indicated by red and blue symbols, respectively. The green ring corresponds to the virial radius of 365 kpc around the NGC 3115. The rectangular perimeter delineates our viewing area on the DESI Lagacy Imaging Surveys. The arrow marks the direction toward the neighboring group around NGC 3521.