adsabs/AstroCLIMB huggingface dataset:
Paper: Direct Exoplanet Detection using Convolutional Image Reconstruction (ConStruct): A New Algorithm for Post-processing High-contrast Images
Authors: Trevor N. Wolf, Brandon A. Jones, Brendan P. Bowler
Figure caption: Marginalized representations for our parametric parameter search for the 2011 July 21 epoch of HR 8799. Each contour plot shows the S/N values projected onto two of the variables. The projection operation takes the maximum S/N along the axis of the marginalized variable. The violin plots show the spread in the S/N in each variable bin. Panels (a), (b), (c), and (d) correspond to HR 8799 b, c, d, and e, respectively.
Paper: Direct Exoplanet Detection using Convolutional Image Reconstruction (ConStruct): A New Algorithm for Post-processing High-contrast Images
Authors: Trevor N. Wolf, Brandon A. Jones, Brendan P. Bowler
Figure caption: Full-frame reductions with ConStruct and PCA of HD 114174 (Crepp et al. 2013a) for Sequence 5 in Table 1. The top two panels correspond to (left) the flux map and (right) the S/N map produced by ConStruct. The bottom panels are that produced with PCA.
Paper: Direct Exoplanet Detection using Convolutional Image Reconstruction (ConStruct): A New Algorithm for Post-processing High-contrast Images
Authors: Trevor N. Wolf, Brandon A. Jones, Brendan P. Bowler
Figure caption: 5σ contrast curves with associated 1σ confidence bounds for (left) Sequence 11 and (right) Sequence 12 in Table 1. The blue and orange contrast curves correspond to ConStruct and annular PCA, respectively. For Sequence 11, ConStruct shows an improvement over PCA for most separations. Sequence 12, however, presents nearly identical 5σ contrasts for both algorithms.
Paper: Direct Exoplanet Detection using Convolutional Image Reconstruction (ConStruct): A New Algorithm for Post-processing High-contrast Images
Authors: Trevor N. Wolf, Brandon A. Jones, Brendan P. Bowler
Figure caption: Marginalized representations for our parametric parameter search for the 2012 October 26 epoch of HR 8799. Each contour plot shows the S/N values projected onto two of the variables. The projection operation takes the maximum S/N along the axis of the marginalized variable. The violin plots show the spread in the S/N in each variable bin. Panels (a), (b), (c), and (d) correspond to HR 8799 b, c, d, and e, respectively.
Paper: Direct Exoplanet Detection using Convolutional Image Reconstruction (ConStruct): A New Algorithm for Post-processing High-contrast Images
Authors: Trevor N. Wolf, Brandon A. Jones, Brendan P. Bowler
Figure caption: Marginalized representations for our parametric parameter search for the 2010 July 13 epoch of HR 8799. Each contour plot shows the S/N values projected onto two of the variables. The projection operation takes the maximum S/N along the axis of the marginalized variable. The violin plots show the spread in the S/N in each variable bin. Panels (a), (b), (c), and (d) correspond to HR 8799 b, c, d, and e, respectively.
Paper: The Hidden Clumps in VY CMa Uncovered by the Atacama Large Millimeter/submillimeter Array
Authors: Roberta M. Humphreys, A. M. S. Richards, Kris Davidson, A. P. Singh, L. Decin, L. M. Ziurys
Figure caption: Position–velocity map of the continuum-subtracted 12CO emission at position angle 120°; see Figure 4. The vertical coordinate is the Dopper velocity, while the horizontal scale is the spatial position along a line oriented at position angle 120° (roughly ESE). The location of the star is marked “+,” and the approximate position of Clump C by a small circle. To some extent the Doppler velocities are correlated with location along our line of sight, with the “near side” at the top of the figure. However, at least two sets of ejecta with different ages and size scales are superimposed, e.g., at velocities +30 to +50 km−1. See also Figure 8.
Paper: The Hidden Clumps in VY CMa Uncovered by the Atacama Large Millimeter/submillimeter Array
Authors: Roberta M. Humphreys, A. M. S. Richards, Kris Davidson, A. P. Singh, L. Decin, L. M. Ziurys
Figure caption: The continuum image at 249 GHz. The contours showing the structure and outlines of the clumps are in multiples of (1, 4, 16, 64) × I 1, where I 1 ≈ 0.6 mJy beam−1 ≈8 mJy arcsec−2. The brightness temperature at the outer contour is about 0.2 K. The synthesized beam (FWHM) is shown as an ellipse in the lower-left corner.
Paper: The Hidden Clumps in VY CMa Uncovered by the Atacama Large Millimeter/submillimeter Array
Authors: Roberta M. Humphreys, A. M. S. Richards, Kris Davidson, A. P. Singh, L. Decin, L. M. Ziurys
Figure caption:  12CO images of a 6″ × 6″ region centered on VY CMa. The tick marks are 1″. Clumps C and D are redshifted relative to VY CMa and observed over the same range of Doppler velocities, while Clump A is blueshifted. Clump B is not resolved from the bright CO emission from VY CMa’s circumstellar ejecta. (a) 12CO emission at V LSR 43 km s−1 toward Clumps C and D, and new outflow ﹩{{\rm{B}}}^{{\prime} }﹩. The position of Clump B is marked. (b) Toward Clump A at V LSR +6 km s−1. The position of VY CMa is shown as a + in each panel; its Doppler velocity is +22 km s−1 relative to the LSR. The brightness scales differ between panels. The images are continuum subtracted.
Paper: The Hidden Clumps in VY CMa Uncovered by the Atacama Large Millimeter/submillimeter Array
Authors: Roberta M. Humphreys, A. M. S. Richards, Kris Davidson, A. P. Singh, L. Decin, L. M. Ziurys
Figure caption: The observed line-of-sight velocity of the 12CO emission relative to VY CMa toward Clump D vs. the corresponding projected distance from the star in milliarcseconds and au for 15 channels representing the diffuse arc in Figure 5. The open circles show the more diffuse fainter 12CO emission at the end of the arc in Figure 5. Each measurement used a sampling parameter of 5 pixels (0.″2). The error bar represents the typical uncertainty in the centroid position. The main trend agrees with the diffuse arc in Figure 5.
Paper: The Hidden Clumps in VY CMa Uncovered by the Atacama Large Millimeter/submillimeter Array
Authors: Roberta M. Humphreys, A. M. S. Richards, Kris Davidson, A. P. Singh, L. Decin, L. M. Ziurys
Figure caption: Sketch illustrating how Figure 5 was produced. The upper panel is a sum of the 12CO images at Doppler velocities from +15 to +49 km s−1 relative to the LSR, and shows a virtual sampling slit oriented at position angle 120° to include Clumps C and D (Figure 2). The lower panel shows its spatial parameters. The intensity along that virtual slit was measured for each frequency channel, and the resulting one-dimensional data sets were stacked to produce the two-dimensional Figure 5.
Paper: The Hidden Clumps in VY CMa Uncovered by the Atacama Large Millimeter/submillimeter Array
Authors: Roberta M. Humphreys, A. M. S. Richards, Kris Davidson, A. P. Singh, L. Decin, L. M. Ziurys
Figure caption: Map of the proper motions showing the direction of motion for the clumps relative to their positions in 2015. The 2015 positions are marked by solid circles and the 2021 positions by hollow squares. The vectors and error bars have been multiplied by 3 to make them more visible.
Paper: A Combined Ground-based and JWST Atmospheric Retrieval Analysis: Both IGRINS and NIRSpec Agree that the Atmosphere of WASP-77A b Is Metal-poor
Authors: Peter C. B. Smith, Michael R. Line, Jacob L. Bean, Matteo Brogi, Prune August, Luis Welbanks, Jean-Michel Desert, Jonathan Lunine, Jorge Sanchez, Megan Mansfield, Lorenzo Pino, Emily Rauscher, Eliza Kempton, Joseph Zalesky, Martin Fowler
Figure caption: Top: best-fit model spectrum from the combined IGRINS+NIRSpec retrieval at R = 500,000 (gray), converted to brightness temperature and smoothed to R = 1000 (black) for visual clarity. The shaded regions illustrate contributions and light absorbed from H2O, CO, and CO2 individually. The NIRSpec data are shown as gold diamonds and have been further binned down to R ∼ 85 for visual clarity. While the planet spectrum is not visible in the actual IGRINS data, to give a sense of its wavelength coverage and spectral resolution, the best fit has been further convolved to the IGRINS resolution (R = 45,000) and interpolated onto the instrument’s wavelength grid, alternating colors with echelle order. Goodness of fit with both data sets is discussed in detail in Section 6.3. Also shown for comparison are the previously published HST/WFC3 eclipse measurements presented in Mansfield et al. (2022) but not considered in this study (circles). Bottom left: cross-correlation residuals with the IGRINS data after the best-fit spectrum has been divided out. A 2D detection map was calculated as in Section 3, and shown here is a horizontal slice at the planet’s K  P . The lack of a signal at rest velocity indicates that the best-fit spectrum is an adequate fit to the true planet signal. This process is described more in Section 6.3. Bottom right: residuals from subtracting the binned NIRSpec data from the best fit binned onto the same wavelength grid.
Paper: A Combined Ground-based and JWST Atmospheric Retrieval Analysis: Both IGRINS and NIRSpec Agree that the Atmosphere of WASP-77A b Is Metal-poor
Authors: Peter C. B. Smith, Michael R. Line, Jacob L. Bean, Matteo Brogi, Prune August, Luis Welbanks, Jean-Michel Desert, Jonathan Lunine, Jorge Sanchez, Megan Mansfield, Lorenzo Pino, Emily Rauscher, Eliza Kempton, Joseph Zalesky, Martin Fowler
Figure caption: Cross-correlation maps for the pre- and post-eclipse sequences, as well as from all three nights of IGRINS data combined. Each column is the resultant map from cross-correlating using a different atmospheric template. Below each map is a cross section of both the CCF S/N (red) and Δlog ﹩{ \mathcal L }﹩ (divided by its standard deviation; blue) at the highest-likelihood K  P .
Paper: A Combined Ground-based and JWST Atmospheric Retrieval Analysis: Both IGRINS and NIRSpec Agree that the Atmosphere of WASP-77A b Is Metal-poor
Authors: Peter C. B. Smith, Michael R. Line, Jacob L. Bean, Matteo Brogi, Prune August, Luis Welbanks, Jean-Michel Desert, Jonathan Lunine, Jorge Sanchez, Megan Mansfield, Lorenzo Pino, Emily Rauscher, Eliza Kempton, Joseph Zalesky, Martin Fowler
Figure caption: Similar to Figure 7, marginalized posterior distributions of relevant gas abundances, as well as the P-T profile from the pre-eclipse IGRINS data alone (red), NIRSpec alone (blue), and both combined (purple). From the confidence intervals of these parameters, it is evident that in the combined retrieval, the composition inferences are driven by the high-resolution data, while the P-T inferences are driven by the low-resolution data.
Paper: A Combined Ground-based and JWST Atmospheric Retrieval Analysis: Both IGRINS and NIRSpec Agree that the Atmosphere of WASP-77A b Is Metal-poor
Authors: Peter C. B. Smith, Michael R. Line, Jacob L. Bean, Matteo Brogi, Prune August, Luis Welbanks, Jean-Michel Desert, Jonathan Lunine, Jorge Sanchez, Megan Mansfield, Lorenzo Pino, Emily Rauscher, Eliza Kempton, Joseph Zalesky, Martin Fowler
Figure caption: Marginalized posterior distributions of relevant gas abundances, as well as the P-T profile from the three different subsets of IGRINS data: pre-eclipse (red), post-eclipse (blue), and all three nights (purple). The vertical P-T panel shows the median posterior profile (solid lines), and the shaded regions are the 1σ confidence intervals. Also plotted is the τ = 1 spectrum assuming the best-fit parameters from the pre+post retrieval.
Paper: A Combined Ground-based and JWST Atmospheric Retrieval Analysis: Both IGRINS and NIRSpec Agree that the Atmosphere of WASP-77A b Is Metal-poor
Authors: Peter C. B. Smith, Michael R. Line, Jacob L. Bean, Matteo Brogi, Prune August, Luis Welbanks, Jean-Michel Desert, Jonathan Lunine, Jorge Sanchez, Megan Mansfield, Lorenzo Pino, Emily Rauscher, Eliza Kempton, Joseph Zalesky, Martin Fowler
Figure caption: Measured velocity from the CCF signal in the planet literature rest frame (diamonds) and best fits from various assumptions about WASP-77A b’s orbit. The purple lines are the estimated velocity trail using both IGRINS sequences, and the red and blue lines are estimates from each sequence alone. Pre-eclipse is red, and post-eclipse is blue. The reduced χ 2 from each best fit is also listed in its corresponding color. Only a combined pre+post fit appears for the jet model because after that initial analysis it was clear the jet was not a viable path of inquiry. Note that some of the data points appear to be at the same phase because the CCF frames were binned in BJD time and have been phase-folded for visualization.
Paper: A Combined Ground-based and JWST Atmospheric Retrieval Analysis: Both IGRINS and NIRSpec Agree that the Atmosphere of WASP-77A b Is Metal-poor
Authors: Peter C. B. Smith, Michael R. Line, Jacob L. Bean, Matteo Brogi, Prune August, Luis Welbanks, Jean-Michel Desert, Jonathan Lunine, Jorge Sanchez, Megan Mansfield, Lorenzo Pino, Emily Rauscher, Eliza Kempton, Joseph Zalesky, Martin Fowler
Figure caption: WASP-77A b in context of other hot and ultrahot Jupiters with both measured [O/H] and [C/H] values. These include HD 209458 b (Gandhi et al. 2019; VLT/CRIRES and HST/WFC3), τ Bootis b (Pelletier et al. 2021; CFHT/SPIRou), KELT-20 b (Kasper et al. 2023; GN/MAROON-X and HST/WFC3), HD 149026 b (Bean et al. 2023; JWST/NIRCam), and WASP-96 b (Taylor et al. 2023; JWST/NIRISS). Note the first two studies also combined high- and low-resolution data to obtain these measurements. The values and uncertainties here for WASP-77A b are from the combined IGRINS+NIRSpec retrieval (turquoise diamond), which were mostly driven by the IGRINS data, but the NIRSpec-only constraints are also shown for comparison (denoted with a hexagon). Also included is Jupiter (Atreya et al. 2018) to illustrate the high precision achieved on WASP-77A b’s composition with the combined IGRINS and NIRSpec analysis, as well as regions in this parameter space associated with several broad predicted formation pathways as summarized in Reggiani et al. (2022).
Paper: A Combined Ground-based and JWST Atmospheric Retrieval Analysis: Both IGRINS and NIRSpec Agree that the Atmosphere of WASP-77A b Is Metal-poor
Authors: Peter C. B. Smith, Michael R. Line, Jacob L. Bean, Matteo Brogi, Prune August, Luis Welbanks, Jean-Michel Desert, Jonathan Lunine, Jorge Sanchez, Megan Mansfield, Lorenzo Pino, Emily Rauscher, Eliza Kempton, Joseph Zalesky, Martin Fowler
Figure caption: Posterior distributions for the radial velocity semiamplitude, K  P , and systemic offset velocity, V sys, with different assumptions about WASP-77A b’s orbit as described in Section 4. Each label states the period reference and eccentricity. T16 stands for Turner et al. (2016), and CZ20 stands for Cortés-Zuleta et al. (2020).
Paper: A Combined Ground-based and JWST Atmospheric Retrieval Analysis: Both IGRINS and NIRSpec Agree that the Atmosphere of WASP-77A b Is Metal-poor
Authors: Peter C. B. Smith, Michael R. Line, Jacob L. Bean, Matteo Brogi, Prune August, Luis Welbanks, Jean-Michel Desert, Jonathan Lunine, Jorge Sanchez, Megan Mansfield, Lorenzo Pino, Emily Rauscher, Eliza Kempton, Joseph Zalesky, Martin Fowler
Figure caption: Cross-correlation trails tracking the planet signal throughout the phases captured in this program. The same 1D equilibrium model used to create the 2D CCF maps in Figure 3 was cross-correlated with each individual frame at a range of line-of-sight velocities (horizontal axis). For visual clarity, the two post-eclipse sequences have been combined and pairs of frames have been binned together to boost the visible CCF. The dashed lines are the expected planet radial velocity per the best-fit values of K  P  and V sys from Section 4, offset by 35 km s−1 on either side of the actual CCF trail for clarity. The horizontal dashed lines indicate secondary eclipse, when the planet is occulted by the star. The white space indicates phases at which no data were taken.
Paper: A Combined Ground-based and JWST Atmospheric Retrieval Analysis: Both IGRINS and NIRSpec Agree that the Atmosphere of WASP-77A b Is Metal-poor
Authors: Peter C. B. Smith, Michael R. Line, Jacob L. Bean, Matteo Brogi, Prune August, Luis Welbanks, Jean-Michel Desert, Jonathan Lunine, Jorge Sanchez, Megan Mansfield, Lorenzo Pino, Emily Rauscher, Eliza Kempton, Joseph Zalesky, Martin Fowler
Figure caption: Residual Δlog-likelihood maps from cross-correlating the solar composition 1D-RCTE template with the IGRINS data after the best-fit model spectra from each of the three main retrievals were divided out. The maps have been median subtracted, and in contrast to the CCF maps in Figure 3, there are no peaks near the expected planet velocity, indicating that the best-fit spectra matched the true underlying planet signal within the precision of the IGRINS data.
Paper: The Orbital Geometries and Stellar Obliquities of Exoplanet-hosting Multistar Systems
Authors: Malena Rice, Konstantin Gerbig, Andrew Vanderburg
Figure caption: Stellar binary inclination (i) vs. sky-projected spin–orbit angle (λ) for exoplanets in binary star systems. Edge-on binary orbits correspond to i = 90°, and all companion planets in the sample have near–edge-on orbits such that they transit the host star. Triple-star systems have been excluded from this figure. Systems with σ  i  > 25° or σ  λ  > 25° are shown at low opacity. Histograms of the 2D distributions of each parameter are provided in the top and right panels. Both the scatter plot and the histograms are colored by the host star’s effective temperature, as in Figure 3.
Paper: The Orbital Geometries and Stellar Obliquities of Exoplanet-hosting Multistar Systems
Authors: Malena Rice, Konstantin Gerbig, Andrew Vanderburg
Figure caption: The nine identified “fully aligned” systems, ordered by the sky-projected separation between the exoplanet host star and its aligned companion star. The same color scheme from Figure 1 is used here, with stellar relative velocity vectors shown in blue for all systems with γ measured within this work. All primary, exoplanet-hosting stars are placed at the 1 au mark, with the sky-projected stellar spin axis (as approximated by λ) shown for each host star. Temperatures were drawn from the NASA Exoplanet Archive for exoplanet host stars, and they were drawn either from Gaia DR3 or from previously published works (Ngo et al. 2015; Mugrauer 2019) where available for the secondary stars. No previous measurement of T eff was found for TrES-4 B, so the value was estimated from our isochrone fit as ﹩{T}_{\mathrm{eff}}={4349}_{-386}^{+521}﹩ K.
Paper: The Orbital Geometries and Stellar Obliquities of Exoplanet-hosting Multistar Systems
Authors: Malena Rice, Konstantin Gerbig, Andrew Vanderburg
Figure caption: Sky-projected orbit–orbit angle (γ) vs. sky-projected spin–orbit angle (λ) for exoplanets in multistar systems. For triple-star systems, γ is measured between the primary and the nearest resolved stellar companion. Systems with σ  γ  > 25° and σ  λ  > 25° are shown at low opacity. Systems are colored by the host star’s effective temperature, where the division between “hot” (red) and “cool” (blue) stars is set roughly at the location of the Kraft break.
Paper: The Inner Disk Rim of HD 163296: Linking Radiative Hydrostatic Models with Infrared Interferometry
Authors: Ondřej Chrenko, Mario Flock, Takahiro Ueda, Antoine Mérand, Myriam Benisty, Raúl O. Chametla
Figure caption: Left: Temperature map of model M1 with neglected viscous heating. There is a shadowed region outwards from the rim and an apparent cold spot. Right: Evolution of surfaces of full dust evaporation (solid curve) and IR emission (dashed curve) during the full iteration cycle of model M2.
Paper: The Inner Disk Rim of HD 163296: Linking Radiative Hydrostatic Models with Infrared Interferometry
Authors: Ondřej Chrenko, Mario Flock, Takahiro Ueda, Antoine Mérand, Myriam Benisty, Raúl O. Chametla
Figure caption: Radial profiles of the midplane temperature based on the model S100 of Flock et al. (2016). The individual panels demonstrate the influence of the boundary conditions for the radiation energy density (Section 2.2)—the warm boundary is used in the top panel while the cold boundary is used in the bottom panel. Individual curves are labeled in the plot legend and described in detail in Appendix A. To guide the eye, we advise the reader to mainly follow the changes of the blue and green curves (black and gray curves remain fixed, while the red curve changes only slightly).
Paper: The Orbital Geometries and Stellar Obliquities of Exoplanet-hosting Multistar Systems
Authors: Malena Rice, Konstantin Gerbig, Andrew Vanderburg
Figure caption: Binary inclination i (top panel) and sky-projected spin–orbit angle ∣λ∣ (bottom panel) as a function of sky-projected binary separation. The gray lines indicate i = 90° and ∣λ∣ = 90° for reference. As in Figure 4, systems with σ  i  > 25° or σ  λ  > 25° are shown at low opacity. Both the scatter plots and the histogram are colored by the host star’s effective temperature, as in Figures 3 and 4.
Paper: The Orbital Geometries and Stellar Obliquities of Exoplanet-hosting Multistar Systems
Authors: Malena Rice, Konstantin Gerbig, Andrew Vanderburg
Figure caption: A selection of potential spin–orbit and orbit–orbit configurations for binary star systems with a circumprimary, transiting exoplanet. The transiting planet’s orbit is shown in these example systems, while only the relative positional displacement and velocity vector are displayed for the stellar binary orbit.
Paper: The Orbital Geometries and Stellar Obliquities of Exoplanet-hosting Multistar Systems
Authors: Malena Rice, Konstantin Gerbig, Andrew Vanderburg
Figure caption: Two well-defined cases for γ: edge-on orbits (γ ∼ 0° or γ ∼ 180°) and circular, face-on orbits (γ ∼ 90°). Here, the stellar binary orbit is shown for reference. Edge-on orbits always remain close to γ ∼ 0° or γ ∼ 180°, whereas face-on orbits span a wide range of γ values for nonzero eccentricities. The stellar relative velocity vector and positional displacement are colored here as in Figure 1.
Paper: Large Interferometer For Exoplanets (LIFE). XII. The Detectability of Capstone Biosignatures in the Mid-infrared—Sniffing Exoplanetary Laughing Gas and Methylated Halogens
Authors: Daniel Angerhausen, Daria Pidhorodetska, Michaela Leung, Janina Hansen, Eleonora Alei, Felix Dannert, Jens Kammerer, Sascha P. Quanz, Edward W. Schwieterman
Figure caption: Same as Figure 2 for 100 days of observation time.
Paper: Large Interferometer For Exoplanets (LIFE). XII. The Detectability of Capstone Biosignatures in the Mid-infrared—Sniffing Exoplanetary Laughing Gas and Methylated Halogens
Authors: Daniel Angerhausen, Daria Pidhorodetska, Michaela Leung, Janina Hansen, Eleonora Alei, Felix Dannert, Jens Kammerer, Sascha P. Quanz, Edward W. Schwieterman
Figure caption: Same as Figure 2 for 10 days of observation time.
Paper: Large Interferometer For Exoplanets (LIFE). XII. The Detectability of Capstone Biosignatures in the Mid-infrared—Sniffing Exoplanetary Laughing Gas and Methylated Halogens
Authors: Daniel Angerhausen, Daria Pidhorodetska, Michaela Leung, Janina Hansen, Eleonora Alei, Felix Dannert, Jens Kammerer, Sascha P. Quanz, Edward W. Schwieterman
Figure caption: Retrieval results for 100 Tmol yr−1N2O case.
Paper: Large Interferometer For Exoplanets (LIFE). XII. The Detectability of Capstone Biosignatures in the Mid-infrared—Sniffing Exoplanetary Laughing Gas and Methylated Halogens
Authors: Daniel Angerhausen, Daria Pidhorodetska, Michaela Leung, Janina Hansen, Eleonora Alei, Felix Dannert, Jens Kammerer, Sascha P. Quanz, Edward W. Schwieterman
Figure caption: Results for AD Leonis–type star in 100 days.
Paper: Large Interferometer For Exoplanets (LIFE). XII. The Detectability of Capstone Biosignatures in the Mid-infrared—Sniffing Exoplanetary Laughing Gas and Methylated Halogens
Authors: Daniel Angerhausen, Daria Pidhorodetska, Michaela Leung, Janina Hansen, Eleonora Alei, Felix Dannert, Jens Kammerer, Sascha P. Quanz, Edward W. Schwieterman
Figure caption: Results for AD Leonis–type star in 10 days.