adsabs/AstroCLIMB huggingface dataset:
Paper: Detection of Near-infrared Water Ice at the Surface of the (Pre)Transitional Disk of AB Aur: Informing Icy Grain Abundance, Composition, and Size
Authors: S. K. Betti, K. Follette, S. Jorquera, G. Duchêne, J. Mazoyer, M. Bonnefoy, G. Chauvin, L. M. Pérez, A. Boccaletti, C. Pinte, A. J. Weinberger, C. Grady, L. M. Close, D. Defrère, E. C. Downey, P. M. Hinz, F. Ménard, G. Schneider, A. J. Skemer, and A. Vaz
Figure caption: Surface brightness spectra along with the NE (right), SW (center), and SE (left) directions of the disk of AB Aur. Each spectrum is extracted within a 0.″132 × 0.″0.066 wide rectangle. The spectra are centered at 0.″528, 0.″660, and 0.″792 along each axis. The inset 3.08 μm Ice-band deprojected images show the location of each box along each direction. In all cases, a dip at 3.08 μm is seen.
Paper: Detection of Near-infrared Water Ice at the Surface of the (Pre)Transitional Disk of AB Aur: Informing Icy Grain Abundance, Composition, and Size
Authors: S. K. Betti, K. Follette, S. Jorquera, G. Duchêne, J. Mazoyer, M. Bonnefoy, G. Chauvin, L. M. Pérez, A. Boccaletti, C. Pinte, A. J. Weinberger, C. Grady, L. M. Close, D. Defrère, E. C. Downey, P. M. Hinz, F. Ménard, G. Schneider, A. J. Skemer, and A. Vaz
Figure caption: Color–color difference diagram of the MCFOST scattered light spectra from Figure 7. The black lines are models for maximum grain sizes of 1.0, 3.0, and 10.0 μm (left to right), while the dashed lines show the ice mass fraction (circle: 0%; diamond: 5%; square: 15%; and triangle: 68%.) The individual colored markers show the color difference for each extracted spectrum (SE: orange diamond; NE: olive circle; and SW: blue square) from Figure 7, with the size further increasing with the distance from the star. The black square indicates the average of all of the spectra. The black arrow is the interstellar reddening vector.
Paper: Detection of Near-infrared Water Ice at the Surface of the (Pre)Transitional Disk of AB Aur: Informing Icy Grain Abundance, Composition, and Size
Authors: S. K. Betti, K. Follette, S. Jorquera, G. Duchêne, J. Mazoyer, M. Bonnefoy, G. Chauvin, L. M. Pérez, A. Boccaletti, C. Pinte, A. J. Weinberger, C. Grady, L. M. Close, D. Defrère, E. C. Downey, P. M. Hinz, F. Ménard, G. Schneider, A. J. Skemer, and A. Vaz
Figure caption: Scattered light spectra at a radius of 0.″792 normalized to Ks band (the left-hand column) or ﹩L^{\prime} ﹩ band (the right-hand column), overlain with the modeled spectra for various ice abundances. The points indicate the relative photometry in the SE (diamond), NE (circle), and SW (square) directions. Models with maximum grain sizes of 10 (green), 3.0 (gold), and 1.0 μm (purple) are overplotted for a range of power-law grain size distribution indices, namely: −2.0 (dotted), −2.5 (solid), −3.0 (dashed–dotted), and −3.5 (dashed). Vertically, the panels range from high to low ice mass composition fractions, with values of 68%, 15%, 5%, and 0% ice. Grains that are 0% or 5% ice best match the Ks–﹩L^{\prime} ﹩ slope (the lower left-hand panels), while the 3.08 μm–﹩L^{\prime} ﹩ slope is best matched by grains with very high ice fractions (∼68%, the upper right-hand panel).
Paper: Detection of Near-infrared Water Ice at the Surface of the (Pre)Transitional Disk of AB Aur: Informing Icy Grain Abundance, Composition, and Size
Authors: S. K. Betti, K. Follette, S. Jorquera, G. Duchêne, J. Mazoyer, M. Bonnefoy, G. Chauvin, L. M. Pérez, A. Boccaletti, C. Pinte, A. J. Weinberger, C. Grady, L. M. Close, D. Defrère, E. C. Downey, P. M. Hinz, F. Ménard, G. Schneider, A. J. Skemer, and A. Vaz
Figure caption: Δ(Ks − H2O) color (top) and ﹩{\rm{\Delta }}({{\rm{H}}}_{2}{\rm{O}}-L^{\prime} )﹩ color (bottom) of scattered light spectra as a function of grain size. The dashed lines show the ice mass fractions for MCFOST models with grain size distribution power-law index q = −3.5. The solid horizontal lines are the colors of the AB Aur disk with LMIRCam (SE: orange; NE: olive; and SW: blue) in Figure 9. The best-fitting ice mass fraction differs substantially between the two colors, from 0%–15% in Δ(Ks − H2O) to ∼68% in ﹩{\rm{\Delta }}({{\rm{H}}}_{2}{\rm{O}}-L^{\prime} )﹩.
Paper: Detection of Near-infrared Water Ice at the Surface of the (Pre)Transitional Disk of AB Aur: Informing Icy Grain Abundance, Composition, and Size
Authors: S. K. Betti, K. Follette, S. Jorquera, G. Duchêne, J. Mazoyer, M. Bonnefoy, G. Chauvin, L. M. Pérez, A. Boccaletti, C. Pinte, A. J. Weinberger, C. Grady, L. M. Close, D. Defrère, E. C. Downey, P. M. Hinz, F. Ménard, G. Schneider, A. J. Skemer, and A. Vaz
Figure caption: The effect of dereddening on the AB Aur spectra in order to match the modeled scattered light spectra. The darker colors indicate a larger dereddening correction (AV). The models are as in Figure 9 for an ice mass composition fraction of 5% ice. ﹩L^{\prime} ﹩ must have an extra ∼45–50 mag of extinction to get its observed spectral slope.
Paper: Detection of Near-infrared Water Ice at the Surface of the (Pre)Transitional Disk of AB Aur: Informing Icy Grain Abundance, Composition, and Size
Authors: S. K. Betti, K. Follette, S. Jorquera, G. Duchêne, J. Mazoyer, M. Bonnefoy, G. Chauvin, L. M. Pérez, A. Boccaletti, C. Pinte, A. J. Weinberger, C. Grady, L. M. Close, D. Defrère, E. C. Downey, P. M. Hinz, F. Ménard, G. Schneider, A. J. Skemer, and A. Vaz
Figure caption: DE optimization of the best-fit model for the Ks-band KLIP–RDI reduction of AB Aur. The off-diagonal plots show solutions for two parameters binned 6 × 6. The color of each bin represents the ﹩{\chi }_{r}^{2}﹩ of the best-fitting model within that bin. Lighter colors indicate smaller values of ﹩{\chi }_{r}^{2}﹩. The diagonal plots show a one-dimensional view of each parameter of the minimum ﹩{\chi }_{r}^{2}﹩ as a function of the parameter range, and colored by ﹩{\chi }_{r}^{2}﹩. The best-fit solutions are shown by the red square/line, while the solutions within the “acceptable range” (﹩{\chi }_{r}^{2}\leqslant {\chi }_{r,\min }^{2}+\sqrt{2/\nu }﹩) are those whose ﹩{\chi }_{r}^{2}﹩ falls below the dashed black line in the diagonal plots.
Paper: Detection of Near-infrared Water Ice at the Surface of the (Pre)Transitional Disk of AB Aur: Informing Icy Grain Abundance, Composition, and Size
Authors: S. K. Betti, K. Follette, S. Jorquera, G. Duchêne, J. Mazoyer, M. Bonnefoy, G. Chauvin, L. M. Pérez, A. Boccaletti, C. Pinte, A. J. Weinberger, C. Grady, L. M. Close, D. Defrère, E. C. Downey, P. M. Hinz, F. Ménard, G. Schneider, A. J. Skemer, and A. Vaz
Figure caption: The same as Figure 12, but for 3.08 μm Ice-band DE optimization.
Paper: Detection of Near-infrared Water Ice at the Surface of the (Pre)Transitional Disk of AB Aur: Informing Icy Grain Abundance, Composition, and Size
Authors: S. K. Betti, K. Follette, S. Jorquera, G. Duchêne, J. Mazoyer, M. Bonnefoy, G. Chauvin, L. M. Pérez, A. Boccaletti, C. Pinte, A. J. Weinberger, C. Grady, L. M. Close, D. Defrère, E. C. Downey, P. M. Hinz, F. Ménard, G. Schneider, A. J. Skemer, and A. Vaz
Figure caption: The same as Figure 12, but for ﹩L^{\prime} ﹩-band DE optimization.
Paper: Detection of Near-infrared Water Ice at the Surface of the (Pre)Transitional Disk of AB Aur: Informing Icy Grain Abundance, Composition, and Size
Authors: S. K. Betti, K. Follette, S. Jorquera, G. Duchêne, J. Mazoyer, M. Bonnefoy, G. Chauvin, L. M. Pérez, A. Boccaletti, C. Pinte, A. J. Weinberger, C. Grady, L. M. Close, D. Defrère, E. C. Downey, P. M. Hinz, F. Ménard, G. Schneider, A. J. Skemer, and A. Vaz
Figure caption: The best-fit model and residuals from the DE optimization for Ks. Top left: the best-fit model image. Top center: the best-fit convolved and forward modeled image. Top right: residuals between the model-convolved + FM model and the KLIP-reduced data for just the area of interest (i.e., the disk of AB Aur). Bottom left: the best-fit model image after being convolved with an observed LMIRCam PSF (shown in the offset at the bottom left of the image). Bottom center: the observed Ks-band image of AB Aur after pyKLIP RDI reduction. Bottom right: χ2 residuals between the model-convolved + FM model and the KLIP-reduced data for the area of interest.
Paper: Detection of Near-infrared Water Ice at the Surface of the (Pre)Transitional Disk of AB Aur: Informing Icy Grain Abundance, Composition, and Size
Authors: S. K. Betti, K. Follette, S. Jorquera, G. Duchêne, J. Mazoyer, M. Bonnefoy, G. Chauvin, L. M. Pérez, A. Boccaletti, C. Pinte, A. J. Weinberger, C. Grady, L. M. Close, D. Defrère, E. C. Downey, P. M. Hinz, F. Ménard, G. Schneider, A. J. Skemer, and A. Vaz
Figure caption: The same as Figure 15, but for the 3.08 μm Ice-band best-fit model and residuals.
Paper: Detection of Near-infrared Water Ice at the Surface of the (Pre)Transitional Disk of AB Aur: Informing Icy Grain Abundance, Composition, and Size
Authors: S. K. Betti, K. Follette, S. Jorquera, G. Duchêne, J. Mazoyer, M. Bonnefoy, G. Chauvin, L. M. Pérez, A. Boccaletti, C. Pinte, A. J. Weinberger, C. Grady, L. M. Close, D. Defrère, E. C. Downey, P. M. Hinz, F. Ménard, G. Schneider, A. J. Skemer, and A. Vaz
Figure caption: The same as Figure 15, but for the ﹩L^{\prime} ﹩-band best-fit model and residuals.
Paper: Detection of Near-infrared Water Ice at the Surface of the (Pre)Transitional Disk of AB Aur: Informing Icy Grain Abundance, Composition, and Size
Authors: S. K. Betti, K. Follette, S. Jorquera, G. Duchêne, J. Mazoyer, M. Bonnefoy, G. Chauvin, L. M. Pérez, A. Boccaletti, C. Pinte, A. J. Weinberger, C. Grady, L. M. Close, D. Defrère, E. C. Downey, P. M. Hinz, F. Ménard, G. Schneider, A. J. Skemer, and A. Vaz
Figure caption: Azimuthally averaged TP radial profiles for varying amplitude and inclination. All other parameters are the fixed and best-fit solutions in Tables 4 and 5. The black curve is the best-fit profile.
Paper: Complex Modulation of Rapidly Rotating Young M Dwarfs: Adding Pieces to the Puzzle
Authors: Maximilian N. Günther, David A. Berardo, Elsa Ducrot, Catriona A. Murray, Keivan G. Stassun, Katalin Olah, L. G. Bouma, Saul Rappaport, Joshua N. Winn, Adina D. Feinstein, Elisabeth C. Matthews, Daniel Sebastian, Benjamin V. Rackham, Bálint Seli, Amaury H. M. J. Triaud, Edward Gillen, Alan M. Levine, Brice-Olivier Demory, Michaël Gillon, Didier Queloz, George R. Ricker, Roland K. Vanderspek, Sara Seager, David W. Latham, Jon M. Jenkins, C. E. Brasseur, Knicole D. Colón, Tansu Daylan, Laetitia Delrez, Michael Fausnaugh, Lionel J. Garcia, Rahul Jayaraman, Emmanuel Jehin, Martti H. Kristiansen, J. M. Diederik Kruijssen, Peter Pihlmann Pedersen, Francisco J. Pozuelos, Joseph E. Rodriguez, Bill Wohler, and Zhuchang Zhan
Figure caption: A collage of different morphology classes of young M dwarfs with complex photometric variability. First row: a typical complex rotator (TIC 206544316) with a period of 0.32 days. Its phase-folded light curve highlights the complex modulation, and its frequency spectrum shows dozens of harmonics down to timescales of minutes. Second row: a typical scallop shell (EPIC 204897050) with a period of 0.26 days. It is apparent that these targets share the same morphology class as the complex rotators, even though the data are constrained by the Nyquist limit for K2 (30 minutes cadence). Third row: a typical spotted M dwarf with a period of 0.58 days (GJ 1243; see, e.g., Davenport et al. 2015; Günther & Daylan 2021; Davenport et al. 2020), showing a simple modulation and only two peaks in the frequency spectrum (two peaks rather than one due to differential rotation). Fourth row: a typical dipper star observed with TESS (RY Lup; Bredall et al. 2020), usually showing no strict periodicity, no presence of multiple clear harmonics, and a wider range of periods (multiple days to weeks). Not shown are the more standard variability classes, such as single-spot modulation and binary stars.
Paper: Complex Modulation of Rapidly Rotating Young M Dwarfs: Adding Pieces to the Puzzle
Authors: Maximilian N. Günther, David A. Berardo, Elsa Ducrot, Catriona A. Murray, Keivan G. Stassun, Katalin Olah, L. G. Bouma, Saul Rappaport, Joshua N. Winn, Adina D. Feinstein, Elisabeth C. Matthews, Daniel Sebastian, Benjamin V. Rackham, Bálint Seli, Amaury H. M. J. Triaud, Edward Gillen, Alan M. Levine, Brice-Olivier Demory, Michaël Gillon, Didier Queloz, George R. Ricker, Roland K. Vanderspek, Sara Seager, David W. Latham, Jon M. Jenkins, C. E. Brasseur, Knicole D. Colón, Tansu Daylan, Laetitia Delrez, Michael Fausnaugh, Lionel J. Garcia, Rahul Jayaraman, Emmanuel Jehin, Martti H. Kristiansen, J. M. Diederik Kruijssen, Peter Pihlmann Pedersen, Francisco J. Pozuelos, Joseph E. Rodriguez, Bill Wohler, and Zhuchang Zhan
Figure caption: Three hypotheses to explain complex morphologies of young M dwarfs. First panel: accreting dust disk hypothesis (Bodman et al. 2016), where an accreting dust disk seen from different observing angles could explain dipper and burster stars. Second panel: corotating clouds hypothesis (Stauffer et al. 2017, 2018), where a patchy torus of gas clouds at the Keplerian corotation orbit periodically blocks out stellar light and might cause scallop shell modulation. Third panel: spots and misaligned disk hypothesis (Zhan et al. 2019), where spot occultations might explain the complex rotator’s modulation.
Paper: Complex Modulation of Rapidly Rotating Young M Dwarfs: Adding Pieces to the Puzzle
Authors: Maximilian N. Günther, David A. Berardo, Elsa Ducrot, Catriona A. Murray, Keivan G. Stassun, Katalin Olah, L. G. Bouma, Saul Rappaport, Joshua N. Winn, Adina D. Feinstein, Elisabeth C. Matthews, Daniel Sebastian, Benjamin V. Rackham, Bálint Seli, Amaury H. M. J. Triaud, Edward Gillen, Alan M. Levine, Brice-Olivier Demory, Michaël Gillon, Didier Queloz, George R. Ricker, Roland K. Vanderspek, Sara Seager, David W. Latham, Jon M. Jenkins, C. E. Brasseur, Knicole D. Colón, Tansu Daylan, Laetitia Delrez, Michael Fausnaugh, Lionel J. Garcia, Rahul Jayaraman, Emmanuel Jehin, Martti H. Kristiansen, J. M. Diederik Kruijssen, Peter Pihlmann Pedersen, Francisco J. Pozuelos, Joseph E. Rodriguez, Bill Wohler, and Zhuchang Zhan
Figure caption: Revised stellar parameters of the 10 complex rotators after correcting for activity-induced radius inflation and temperature suppression. Solid curves are isochrones from the Baraffe et al. (2015) models for ages of 20, 50, and 150 Myr, with gray circles marking masses at 0.1 M⊙ increments. Error bars show apparent effective temperatures (Teff) and radii measured from SED analyses. Arrows show where the stars would fall if they were inactive, i.e., after they are corrected for activity. Filled blue circles mark the four targets with Hα measurements from ANU (Section 2.3), whereas empty blue circles mark the remaining six targets for which we provide estimates only. The “corrected” values place most of the stars near isochrones consistent with the respective ages estimated from their young association memberships, suggesting inferred masses of 0.1–0.3 M⊙ (Table 1).
Paper: Complex Modulation of Rapidly Rotating Young M Dwarfs: Adding Pieces to the Puzzle
Authors: Maximilian N. Günther, David A. Berardo, Elsa Ducrot, Catriona A. Murray, Keivan G. Stassun, Katalin Olah, L. G. Bouma, Saul Rappaport, Joshua N. Winn, Adina D. Feinstein, Elisabeth C. Matthews, Daniel Sebastian, Benjamin V. Rackham, Bálint Seli, Amaury H. M. J. Triaud, Edward Gillen, Alan M. Levine, Brice-Olivier Demory, Michaël Gillon, Didier Queloz, George R. Ricker, Roland K. Vanderspek, Sara Seager, David W. Latham, Jon M. Jenkins, C. E. Brasseur, Knicole D. Colón, Tansu Daylan, Laetitia Delrez, Michael Fausnaugh, Lionel J. Garcia, Rahul Jayaraman, Emmanuel Jehin, Martti H. Kristiansen, J. M. Diederik Kruijssen, Peter Pihlmann Pedersen, Francisco J. Pozuelos, Joseph E. Rodriguez, Bill Wohler, and Zhuchang Zhan
Figure caption: Flares on complex rotators appear randomly uniform distributed in phase, exemplified by 1 yr of TESS data on TIC 177309964. The top panel shows the phase-folded light curve with all flares. The middle panel shows the locations of all flare peaks, illustrating the randomly uniform distribution. The bottom panel illustrates that there is no clear correlation between flare amplitude and phase.
Paper: Complex Modulation of Rapidly Rotating Young M Dwarfs: Adding Pieces to the Puzzle
Authors: Maximilian N. Günther, David A. Berardo, Elsa Ducrot, Catriona A. Murray, Keivan G. Stassun, Katalin Olah, L. G. Bouma, Saul Rappaport, Joshua N. Winn, Adina D. Feinstein, Elisabeth C. Matthews, Daniel Sebastian, Benjamin V. Rackham, Bálint Seli, Amaury H. M. J. Triaud, Edward Gillen, Alan M. Levine, Brice-Olivier Demory, Michaël Gillon, Didier Queloz, George R. Ricker, Roland K. Vanderspek, Sara Seager, David W. Latham, Jon M. Jenkins, C. E. Brasseur, Knicole D. Colón, Tansu Daylan, Laetitia Delrez, Michael Fausnaugh, Lionel J. Garcia, Rahul Jayaraman, Emmanuel Jehin, Martti H. Kristiansen, J. M. Diederik Kruijssen, Peter Pihlmann Pedersen, Francisco J. Pozuelos, Joseph E. Rodriguez, Bill Wohler, and Zhuchang Zhan
Figure caption: Different flare and brightening profiles of the complex rotators, exemplified by TIC 177309964. Each row shows a global (2 day) and local (5 hr) view of the light-curve brightening. Horizontal dashed lines show the typical nonflare maximum flux value. First row: normal flares are described by the same profiles as main-sequence M dwarfs, suggesting similar origins and processes driving them. Second row: complicated outbursts of flares also resemble those of main-sequence M dwarfs and can be explained as superpositions of sequential flare events (e.g., Günther et al. 2020). Third row: unusual brightenings in the complex rotators often, but not always, occur after large flares and show an amplified version of the usual morphology for a short time.
Paper: Complex Modulation of Rapidly Rotating Young M Dwarfs: Adding Pieces to the Puzzle
Authors: Maximilian N. Günther, David A. Berardo, Elsa Ducrot, Catriona A. Murray, Keivan G. Stassun, Katalin Olah, L. G. Bouma, Saul Rappaport, Joshua N. Winn, Adina D. Feinstein, Elisabeth C. Matthews, Daniel Sebastian, Benjamin V. Rackham, Bálint Seli, Amaury H. M. J. Triaud, Edward Gillen, Alan M. Levine, Brice-Olivier Demory, Michaël Gillon, Didier Queloz, George R. Ricker, Roland K. Vanderspek, Sara Seager, David W. Latham, Jon M. Jenkins, C. E. Brasseur, Knicole D. Colón, Tansu Daylan, Laetitia Delrez, Michael Fausnaugh, Lionel J. Garcia, Rahul Jayaraman, Emmanuel Jehin, Martti H. Kristiansen, J. M. Diederik Kruijssen, Peter Pihlmann Pedersen, Francisco J. Pozuelos, Joseph E. Rodriguez, Bill Wohler, and Zhuchang Zhan
Figure caption: Overlap and union of three young star catalogs cross-matched with the TESS short-cadence targets from Sectors 1 and 2. The three catalogs were assembled by Feinstein et al. (2020b), Bouma et al. (2019), and in this work using banyan sigma (Gagné et al. 2018).
Paper: Complex Modulation of Rapidly Rotating Young M Dwarfs: Adding Pieces to the Puzzle
Authors: Maximilian N. Günther, David A. Berardo, Elsa Ducrot, Catriona A. Murray, Keivan G. Stassun, Katalin Olah, L. G. Bouma, Saul Rappaport, Joshua N. Winn, Adina D. Feinstein, Elisabeth C. Matthews, Daniel Sebastian, Benjamin V. Rackham, Bálint Seli, Amaury H. M. J. Triaud, Edward Gillen, Alan M. Levine, Brice-Olivier Demory, Michaël Gillon, Didier Queloz, George R. Ricker, Roland K. Vanderspek, Sara Seager, David W. Latham, Jon M. Jenkins, C. E. Brasseur, Knicole D. Colón, Tansu Daylan, Laetitia Delrez, Michael Fausnaugh, Lionel J. Garcia, Rahul Jayaraman, Emmanuel Jehin, Martti H. Kristiansen, J. M. Diederik Kruijssen, Peter Pihlmann Pedersen, Francisco J. Pozuelos, Joseph E. Rodriguez, Bill Wohler, and Zhuchang Zhan
Figure caption: Effective temperatures and rotation periods of the 290 young M-dwarf stars in TESS short cadence from Sectors 1 and 2 (blue circles; NyM: number of young M dwarfs). Out of these, 175 targets show rotation periods shorter than 2 days (blue shaded area; NyMrr: number of young M dwarfs with rapid rotations), comparable to the 10 known complex rotators from this sample (red squares).
Paper: Complex Modulation of Rapidly Rotating Young M Dwarfs: Adding Pieces to the Puzzle
Authors: Maximilian N. Günther, David A. Berardo, Elsa Ducrot, Catriona A. Murray, Keivan G. Stassun, Katalin Olah, L. G. Bouma, Saul Rappaport, Joshua N. Winn, Adina D. Feinstein, Elisabeth C. Matthews, Daniel Sebastian, Benjamin V. Rackham, Bálint Seli, Amaury H. M. J. Triaud, Edward Gillen, Alan M. Levine, Brice-Olivier Demory, Michaël Gillon, Didier Queloz, George R. Ricker, Roland K. Vanderspek, Sara Seager, David W. Latham, Jon M. Jenkins, C. E. Brasseur, Knicole D. Colón, Tansu Daylan, Laetitia Delrez, Michael Fausnaugh, Lionel J. Garcia, Rahul Jayaraman, Emmanuel Jehin, Martti H. Kristiansen, J. M. Diederik Kruijssen, Peter Pihlmann Pedersen, Francisco J. Pozuelos, Joseph E. Rodriguez, Bill Wohler, and Zhuchang Zhan
Figure caption: Example of TIC 177309964, illustrating the stability of major photometric features over year-long timescales (TESS orbits from Sectors 1–13, from 2018 July to 2019 July). Each orbit is phase-folded to show two periods of modulation and vertically offset for clarity. Flares have been clipped before plotting. The major features of the modulation remain stable over the full year, while minor features appear and disappear over a few weeks (dashed box).
Paper: Complex Modulation of Rapidly Rotating Young M Dwarfs: Adding Pieces to the Puzzle
Authors: Maximilian N. Günther, David A. Berardo, Elsa Ducrot, Catriona A. Murray, Keivan G. Stassun, Katalin Olah, L. G. Bouma, Saul Rappaport, Joshua N. Winn, Adina D. Feinstein, Elisabeth C. Matthews, Daniel Sebastian, Benjamin V. Rackham, Bálint Seli, Amaury H. M. J. Triaud, Edward Gillen, Alan M. Levine, Brice-Olivier Demory, Michaël Gillon, Didier Queloz, George R. Ricker, Roland K. Vanderspek, Sara Seager, David W. Latham, Jon M. Jenkins, C. E. Brasseur, Knicole D. Colón, Tansu Daylan, Laetitia Delrez, Michael Fausnaugh, Lionel J. Garcia, Rahul Jayaraman, Emmanuel Jehin, Martti H. Kristiansen, J. M. Diederik Kruijssen, Peter Pihlmann Pedersen, Francisco J. Pozuelos, Joseph E. Rodriguez, Bill Wohler, and Zhuchang Zhan
Figure caption: Comparison of multicolor light curves of 4 of the 10 complex rotators: TIC 201789285, TIC 206544316, TIC 332517282, and TIC 425933644. For each target, SSO observations were taken simultaneously in at least two of the g′, r′, i′, and z′ bandpasses (shown as green, orange, red and dark-red curves, respectively). For TESS observations, flares have been removed, and light curves are averaged over all available Sectors, binned in 5 minute intervals, and slightly shifted in phase to correct for imprecision in the period measurement (shown as dark-gray curves). The lower panel compares the normalized transmission functions of all respective bandpasses. There is a clear color dependency of the light-curve features visible in the simultaneous SSO observations, with features being much more prominent in bluer bandpasses. Additionally, the general shape and largest features in the SSO light curves are still comparable to the TESS light curve, even though the SSO data were taken about 1 yr later. This suggests that the overall mechanism causing these patterns also causes a color dependency (e.g., spots, nongray dust, or pulsations) and that it is stable over long times.