adsabs/AstroCLIMB huggingface dataset:
Paper: High-resolution Transmission Spectroscopy of Warm Jupiters: An ESPRESSO Sample with Predictions for ANDES
Authors: Bibiana Prinoth, Elyar Sedaghati, Julia V. Seidel, H. Jens Hoeijmakers, Rafael Brahm, Brian Thorsbro, Andrés Jordán
Figure caption: Change of planetary radial velocity for different orbital configurations per 1 minute exposure (panels (a)–(c)), and from ingress to egress for varying eccentricities ϵ and argument of periastron ω (panel (d)). The planetary and stellar parameters are those of the TOI-3362 system, Table 2, but with varying eccentricity and omega as indicated. Panel (a): circular orbit (ω = 90 deg), resulting in a small radial velocity change during transit. Panel (b): eccentric orbit with ω = 60 deg, leading to a large change in radial velocity during transit. Panel (c): eccentric orbit with ω = 240 deg, resulting in a small change of radial velocity during transit. For the successful application of the cross-correlation technique, a large radial velocity change is desired to avoid overlap with the star’s systemic velocity. Panel (d): change in radial velocity during transit for the same system, with varying eccentricity ϵ and ω. The radial velocity change is larger for highly eccentric orbits when the transit happens close or during periastron (e.g., panel (b)). The smallest change occurs when ω = 270 deg, with the transit center coinciding with apoastron. Below a certain eccentricity, it is preferable that the periastron passage does not coincide with the transit center to distinguish components as the radial velocity goes through 0.
Paper: High-resolution Transmission Spectroscopy of Warm Jupiters: An ESPRESSO Sample with Predictions for ANDES
Authors: Bibiana Prinoth, Elyar Sedaghati, Julia V. Seidel, H. Jens Hoeijmakers, Rafael Brahm, Brian Thorsbro, Andrés Jordán
Figure caption:                         Transmission spectra models for TOI-3362 b (top) and TOI-677 b (bottom). The spectra in black include absorption of H2O, CH4 and CO, as well as continuum absorption. The models assume an isothermal atmosphere at the calculated equilibrium temperature of the corresponding planet T                      eq,A=0 = 1100 K (TOI-3362 b, top) and T                      eq = 1252 K (TOI-677 b, bottom; Jordán et al. 2020). The corresponding abundance profiles were computed with FastChem Cond (Stock et al. 2018; Stock et al. 2022; Kitzmann et al. 2023; see Figure 4), and then translated into mass fractions to produce the transmission models using petitRADTRANS (Mollière et al. 2019). The H2O mass fractions were scaled with factors of 1 (nominal), 10, 100, and 1000 for model injection, and are shown in different shades of gray. The cross-correlation templates of H2O, CH4 and CO, assuming the same planetary and stellar parameters as the models, are plotted in shades of pink to identify the features. The wavelength coverage of ESPRESSO, ANDES (baseline) and ANDES (goal) are shown in blue, orange and green, respectively.
Paper: High-resolution Transmission Spectroscopy of Warm Jupiters: An ESPRESSO Sample with Predictions for ANDES
Authors: Bibiana Prinoth, Elyar Sedaghati, Julia V. Seidel, H. Jens Hoeijmakers, Rafael Brahm, Brian Thorsbro, Andrés Jordán
Figure caption: Water cross-correlation results for K2-139 b, K2-329 b, TOI-3362 b, WASP-130 b, WASP-106 b, and TOI-677 b (from left to right). Top panels: two-dimensional cross-correlation function in the stellar rest frame as a function of radial velocity vs. normalized exposure number. We normalized the exposure number for plotting purposes, but indicated the number of exposures in the panel. The radial velocities of the telluric residuals v tel (dotted, white), the planet v planet (solid, black), the star v star (solid, white), and the RM effect v RM,RV (dashed, black) are shown. The contact times of the transit, ingress and egress are indicated with white horizontal dashed lines. Note that we masked out the first exposure of the transit of WASP-130 b due to telluric contamination. Middle panels: same as top panels but in the rest frame of the planet. Bottom panels: one-dimensional cross-correlation function, given as the time-average (vertical averaging) of the middle panels.
Paper: High-resolution Transmission Spectroscopy of Warm Jupiters: An ESPRESSO Sample with Predictions for ANDES
Authors: Bibiana Prinoth, Elyar Sedaghati, Julia V. Seidel, H. Jens Hoeijmakers, Rafael Brahm, Brian Thorsbro, Andrés Jordán
Figure caption: Top: predicted volume mixing ratios for TOI-3362 b at the expected minimum temperature at apoastron T apo = 800 K (solid), the equilibrium temperature calculated assuming an albedo of 0 T eq = 1100 K (dotted), and the expected maximum temperature at periastron T per = 2500 K (dashed; see Espinoza-Retamal et al. 2023 for temperature range). Bottom: predicted volume mixing ratios for TOI-677 b at the calculated minimum temperature at apoastron T apo = 930 K (solid), the equilibrium temperature T eq = 1252 K (dotted; Jordán et al. 2020), and the calculated maximum temperature at periastron T per = 2500 K (dashed). Note that at several locations the solid lines overlap with the dashed lines.
Paper: High-resolution Transmission Spectroscopy of Warm Jupiters: An ESPRESSO Sample with Predictions for ANDES
Authors: Bibiana Prinoth, Elyar Sedaghati, Julia V. Seidel, H. Jens Hoeijmakers, Rafael Brahm, Brian Thorsbro, Andrés Jordán
Figure caption: Cross-correlation results for model injection in the wavelength range of ESPRESSO of TOI-677 b using 1× (nominal), 10×, 100× and 1000× the predicted H2O abundance, see Figure 3 for the model spectra. Panels as in Figure 5.
Paper: High-resolution Transmission Spectroscopy of Warm Jupiters: An ESPRESSO Sample with Predictions for ANDES
Authors: Bibiana Prinoth, Elyar Sedaghati, Julia V. Seidel, H. Jens Hoeijmakers, Rafael Brahm, Brian Thorsbro, Andrés Jordán
Figure caption: Planetary radius as a function of semimajor axis. The scatter points show the population of exoplanets discovered using transits for comparison, extracted from the NASA Exoplanet Archive on 2024 February 19. The yellow scatter points are considered hot and ultra-hot Jupiters (M p ≥ 0.36 M Jup, P ≤ 10 days, R  p  ≥ 0.4 R Jup, Winn 2010; Fortney et al. 2021). The radii of Jupiter and Earth are given as a reference.
Paper: The ∼50 Myr Old TOI-942c is Likely on an Aligned, Coplanar Orbit and Losing Mass
Authors: Huan-Yu Teng, 环宇 滕, Fei Dai, 飞 戴, Andrew W. Howard, Howard Isaacson, Ryan A. Rubenzahl, Isabel Angelo, Alex S. Polanski
Figure caption: The absolute values of projected stellar obliquity ﹩\left|\lambda \right|﹩ against host star age. Planets in single-planet systems are marked in black while those in multiplanet systems are marked in red. Host stars having effective temperature lower and higher than 6100 K (Kraft break; R. P. Kraft 1967) are, respectively, marked by circles and squares. More specifically, TOI-942c is highlight1ed by red edge. Different obliquity-exciting mechanisms on different timescales are marked by dashed lines in different colors, e.g., Kozai–Lidov mechanism, with a timescale shorter than a hundred Myr, and secular interaction, with a timescale in the magnitude of hundred Myr. Tidal realignment, which operates after a few hundred Myr, is shaded green with darker color indicating a stronger effect.
Paper: The ∼50 Myr Old TOI-942c is Likely on an Aligned, Coplanar Orbit and Losing Mass
Authors: Huan-Yu Teng, 环宇 滕, Fei Dai, 飞 戴, Andrew W. Howard, Howard Isaacson, Ryan A. Rubenzahl, Isabel Angelo, Alex S. Polanski
Figure caption: Top: normalized spectra of Hα line Å during transit event of planet c with their color indicating their observation number (epoch). The dashed line marks the line center at 6564.7 Å, and the dotted lines indicate 1 Å from the line center. Left: excess absorption of Hα variation by time, with the absorption referenced by an average postegress spectrum, and calculated in a bandpass of 2 Å centered at 6564.7 Å. The color scale is the same for the top subplot. The dashed line and dotted line indicate midtransit and egress, respectively. Notably, ingress is not included. Main (bottom right): the measured Hα line profile residuals as a function of time and wavelength. The dashed line and vertical dotted line correspond to the top subplot the top subplot, while the horizontal dotted line indicates the egress as in the left subplot. The predicted planetary velocity is marked by green solid line. An excess absorption and blueshift can be seen in dark blue.
Paper: The ∼50 Myr Old TOI-942c is Likely on an Aligned, Coplanar Orbit and Losing Mass
Authors: Huan-Yu Teng, 环宇 滕, Fei Dai, 飞 戴, Andrew W. Howard, Howard Isaacson, Ryan A. Rubenzahl, Isabel Angelo, Alex S. Polanski
Figure caption: The radial velocities (RVs) during the transit event of TOI-942c on 2021 November 25th (UTC), measured by Keck/HIRES spectra. In the upper subplot, the solid red line is the best-fit model (﹩\left|\lambda \right|={24}_{-14}^{+14\circ }﹩), incorporating the Rossiter–McLaughlin effect and RV long-term trend. The solid gray lines are the solutions randomly selected from the Markov chain Monte Carlo sampling. In the lower panel, the residuals are given by subtracting the best-fit model.
Paper: The ∼50 Myr Old TOI-942c is Likely on an Aligned, Coplanar Orbit and Losing Mass
Authors: Huan-Yu Teng, 环宇 滕, Fei Dai, 飞 戴, Andrew W. Howard, Howard Isaacson, Ryan A. Rubenzahl, Isabel Angelo, Alex S. Polanski
Figure caption: The posterior distribution obtained from the MCMC chain of Model 3 in Table 2 (i.e., the best model).
Paper: SPRITEly: Time-domain Millimeter Interferometry at the Owens Valley Radio Observatory
Authors: Nitika Yadlapalli Yurk, Vikram Ravi, Mark W. Hodges, James W. Lamb, Richard Hobbs, David P. Woody, Anthony C. S. Readhead
Figure caption: Example of data collected on 23 stars for calculation of the optical pointing model coefficients. Top: the smaller, darker markers shown are the true locations and offsets of the stars measured with each antenna. The larger, lighter markers show the results from applying pointing coefficients that best reproduce the observed offsets. Offsets are shown in the antenna-specific X and Y coordinates for each SPRITEly antenna. Bottom: residuals for the fit shown in the top panel, showing that there is no directional dependence to the fidelity of the model fitting.
Paper: SPRITEly: Time-domain Millimeter Interferometry at the Owens Valley Radio Observatory
Authors: Nitika Yadlapalli Yurk, Vikram Ravi, Mark W. Hodges, James W. Lamb, Richard Hobbs, David P. Woody, Anthony C. S. Readhead
Figure caption: The two 10.4 m Leighton antennas, located at OVRO, that are used for the initial SPRITEly deployment. The receivers are housed within the sidecabs at the Nasmyth focus of each antenna, located nearer to the viewer. The smaller dishes are part of the 110-antenna Deep Synoptic Array. In the background is the Mayer control building, which houses the final steps of the signal processing chain and the data processing computers for the telescopes.
Paper: SPRITEly: Time-domain Millimeter Interferometry at the Owens Valley Radio Observatory
Authors: Nitika Yadlapalli Yurk, Vikram Ravi, Mark W. Hodges, James W. Lamb, Richard Hobbs, David P. Woody, Anthony C. S. Readhead
Figure caption: Diagram showing how the LO signal for the SIS mixer is generated. The components within the dotted box are located in the basement of the Mayer control building and are one set of components shared between both antennas. Signals leaving the Mayer control building are sent out over optical fiber and converted back to RF within each of the antennas. The components within the dashed line represent the system in the sidecab of SPRITEly Antenna 2 only. In Antenna 1, the dashed box is replaced by a single synthesizer that generates a 50 MHz signal.
Paper: SPRITEly: Time-domain Millimeter Interferometry at the Owens Valley Radio Observatory
Authors: Nitika Yadlapalli Yurk, Vikram Ravi, Mark W. Hodges, James W. Lamb, Richard Hobbs, David P. Woody, Anthony C. S. Readhead
Figure caption: Locations of all sources allowed for use as gain calibrators for SPRITEly science observations overlaid on a Mollweide projection of a 100 GHz all-sky map (with the cosmic microwave background subtracted) created with observations from the Planck High Frequency Instrument (Planck Collaboration et al. 2020). The gray points represent sources taken from the ALMA calibrator list, while pink points represent sources used as calibrators for CARMA. The red points represent a few science targets of interest located at a variety of coordinates to demonstrate the broad availability of calibrator sources.
Paper: SPRITEly: Time-domain Millimeter Interferometry at the Owens Valley Radio Observatory
Authors: Nitika Yadlapalli Yurk, Vikram Ravi, Mark W. Hodges, James W. Lamb, Richard Hobbs, David P. Woody, Anthony C. S. Readhead
Figure caption: Diagram of the SPRITEly second-stage downconversion system showing how IF signals from both antennas are split into high- and low-band components to be fed to their respective ROACH2 boards for correlation. The thick arrows represent input signals to the downconverter and output signals to the ROACH2. The thick dotted lines indicate clocking signals. One of our ROACH2 boards contains two inputs for two clock signals, whereas the other ROACH2 board contains only one clock signal input and splits the signal internally.
Paper: SPRITEly: Time-domain Millimeter Interferometry at the Owens Valley Radio Observatory
Authors: Nitika Yadlapalli Yurk, Vikram Ravi, Mark W. Hodges, James W. Lamb, Richard Hobbs, David P. Woody, Anthony C. S. Readhead
Figure caption: Example of data collected on Jupiter for single-dish radio pointing measurements. Light curves are shown for both SPRITEly antennas from scans in both the elevation and cross-elevation directions across the disk of the planet, which are represented by the first and second portions of the light curves, respectively. This scan measured total powers at offsets of up to ±90″ at 10″ increments.
Paper: SPRITEly: Time-domain Millimeter Interferometry at the Owens Valley Radio Observatory
Authors: Nitika Yadlapalli Yurk, Vikram Ravi, Mark W. Hodges, James W. Lamb, Richard Hobbs, David P. Woody, Anthony C. S. Readhead
Figure caption: Behavior of phase as a function of time and frequency as seen on a 2 hr observation of bandpass calibrator source 3C 84 after refinements to the baseline solution. In the bottom panel, red indicates negative phase, blue indicates positive phase, and white indicates zero phase. The top panel of this figure shows the small amount of delay variations over the whole observation. The middle panel shows a band-averaged measurement of phase as a function of time.
Paper: SPRITEly: Time-domain Millimeter Interferometry at the Owens Valley Radio Observatory
Authors: Nitika Yadlapalli Yurk, Vikram Ravi, Mark W. Hodges, James W. Lamb, Richard Hobbs, David P. Woody, Anthony C. S. Readhead
Figure caption: SPRITEly measurements of the flux density of ALMA calibrator source J1342+2709 (red points). An ALMA measurement obtained 36 days earlier is indicated as a black line (1σ uncertainty shown as a blue shaded region).
Paper: SPRITEly: Time-domain Millimeter Interferometry at the Owens Valley Radio Observatory
Authors: Nitika Yadlapalli Yurk, Vikram Ravi, Mark W. Hodges, James W. Lamb, Richard Hobbs, David P. Woody, Anthony C. S. Readhead
Figure caption: Time-averaged spectrum of SiO maser emission in R Leo, zoomed in to corresponding frequencies in both the USB (right) and LSB (left), after sideband separation, shown with and without cross-talk mitigation using 180° phase switching.
Paper: SPRITEly: Time-domain Millimeter Interferometry at the Owens Valley Radio Observatory
Authors: Nitika Yadlapalli Yurk, Vikram Ravi, Mark W. Hodges, James W. Lamb, Richard Hobbs, David P. Woody, Anthony C. S. Readhead
Figure caption: Measurements of elevation-dependent double-sideband system temperature of the SPRITEly baseline in reasonable weather conditions. Each measurement contains the T sys of both the high band and low band, shown as circles connected by a line.
Paper: SPRITEly: Time-domain Millimeter Interferometry at the Owens Valley Radio Observatory
Authors: Nitika Yadlapalli Yurk, Vikram Ravi, Mark W. Hodges, James W. Lamb, Richard Hobbs, David P. Woody, Anthony C. S. Readhead
Figure caption: SPRITEly measurements of the flux density of the flaring BL Lac object S2 0109+22 (top) and the binary classical T Tauri system DQ Tau (bottom). The blue shaded region in the bottom panel indicates an approximate quiescent level for the 90 GHz emission from DQ Tau (see text for details).
Paper: The AllWISE Catalog as an Infrared Celestial Reference Frame in the Gaia Era
Authors: J.-C. Liu, N. Liu, Z. Zhu, J. Yao, I. Nurul Huda, Z.-W. Wang
Figure caption: Distribution of normalized parameters between the Gaia DR3 and AllWISE for common sources and QSO-like sources. The upper panels show the distributions of normalized difference in each coordinate (X Δα  and X Δδ ) and proper motions components (﹩{X}_{{\rm{\Delta }}{\mu }_{\alpha * }}﹩ and ﹩{X}_{{\rm{\Delta }}{\mu }_{\delta }}﹩). Below are the distributions of normalized angular separation (X Δρ ) and general proper motion differences (X Δμ ). The black curves are the expected Rayleigh distribution.
Paper: The AllWISE Catalog as an Infrared Celestial Reference Frame in the Gaia Era
Authors: J.-C. Liu, N. Liu, Z. Zhu, J. Yao, I. Nurul Huda, Z.-W. Wang
Figure caption: Mean positions and proper motions difference in the sense of [Gaia DR3−AllWISE] as a function of W1−W2 magnitude. Each point represents the mean value of the corresponding parameter for 20,000 common sources. The thick points are the moving average of the scatter points.
Paper: The AllWISE Catalog as an Infrared Celestial Reference Frame in the Gaia Era
Authors: J.-C. Liu, N. Liu, Z. Zhu, J. Yao, I. Nurul Huda, Z.-W. Wang
Figure caption: Mean positions and proper motions difference in the sense of [Gaia DR3−AllWISE] as a function of W1 magnitude. Each point represents a value of the corresponding parameter for 20,000 common sources. The thick points are the moving average of the scatter points.
Paper: The AllWISE Catalog as an Infrared Celestial Reference Frame in the Gaia Era
Authors: J.-C. Liu, N. Liu, Z. Zhu, J. Yao, I. Nurul Huda, Z.-W. Wang
Figure caption: Upper panels: histograms of uncertainties in positions (α* and δ) and proper motion components of all sources and QSO-like sources in the AllWISE catalog. Lower panels: scatter plot of total positional and proper motion uncertainties vs. the AllWISE W1 magnitude.
Paper: The AllWISE Catalog as an Infrared Celestial Reference Frame in the Gaia Era
Authors: J.-C. Liu, N. Liu, Z. Zhu, J. Yao, I. Nurul Huda, Z.-W. Wang
Figure caption: Density distribution of common sources in Gaia DR3 and AllWISE surveys. The color bars to the right side of the figures give the number of sources counted in each 2° × 2° area.
Paper: The AllWISE Catalog as an Infrared Celestial Reference Frame in the Gaia Era
Authors: J.-C. Liu, N. Liu, Z. Zhu, J. Yao, I. Nurul Huda, Z.-W. Wang
Figure caption: Top: scatter plot of the coordinate difference for 273 million common sources (gray dots) and 0.57 million QSO-like sources (blue dots). Bottom: scatter plot of the differences in proper motion components for 273 million common sources.
Paper: The AllWISE Catalog as an Infrared Celestial Reference Frame in the Gaia Era
Authors: J.-C. Liu, N. Liu, Z. Zhu, J. Yao, I. Nurul Huda, Z.-W. Wang
Figure caption: Regional differences of source positions (top) and proper motions (bottom) between Gaia DR3 and AllWISE in the equatorial coordinate system. The vectors are the mean difference calculated within equal-area cells of about 100 sq. deg. The solid line is the location of the Galactic plane. The positions for the Galactic Center (GC) and the North Galactic Pole (NGP) are marked in blue.
Paper: The AllWISE Catalog as an Infrared Celestial Reference Frame in the Gaia Era
Authors: J.-C. Liu, N. Liu, Z. Zhu, J. Yao, I. Nurul Huda, Z.-W. Wang
Figure caption: Regional differences of QSO-like source positions between Gaia DR3 and AllWISE in the equatorial coordinate system. The vectors are the mean difference calculated within equal-area cells of about 100 sq. deg. The solid line is the location of the Galactic plane. The positions for the Galactic Center (GC) and the North Galactic Pole (NGP) are marked in blue.
Paper: Analysis of KIC 7023917: Spotted Low-mass Ratio Eclipsing Binary with δ Scuti Pulsations
Authors: Pavol Gajdoš, Štefan Parimucha, Marek Skarka, Matúš Kamenec, Jozef Lipták, Raine Karjalainen
Figure caption:  O − C diagrams based on data from Kepler (top panel) and TESS missions (bottom panel).
Paper: The AllWISE Catalog as an Infrared Celestial Reference Frame in the Gaia Era
Authors: J.-C. Liu, N. Liu, Z. Zhu, J. Yao, I. Nurul Huda, Z.-W. Wang
Figure caption: Mean position difference for QSO-like source sample in the sense of [Gaia DR3−AllWISE] as a function of the AllWISE W1 magnitude and color index W1−W2. Each point represents a mean value of the corresponding parameter for 2000 common sources. The thick points are the moving average of the scatter points.
Paper: Analysis of KIC 7023917: Spotted Low-mass Ratio Eclipsing Binary with δ Scuti Pulsations
Authors: Pavol Gajdoš, Štefan Parimucha, Marek Skarka, Matúš Kamenec, Jozef Lipták, Raine Karjalainen
Figure caption: Amplitudes of maxima (top panel) and differences between heights of following maxima (bottom panel).
Paper: Analysis of KIC 7023917: Spotted Low-mass Ratio Eclipsing Binary with δ Scuti Pulsations
Authors: Pavol Gajdoš, Štefan Parimucha, Marek Skarka, Matúš Kamenec, Jozef Lipták, Raine Karjalainen
Figure caption: Example of the LC of KIC 7023917 obtained using TESS satellite. The solid line represents the LC model described in Section 5, which includes the stellar spot (Section 6).
Paper: Analysis of KIC 7023917: Spotted Low-mass Ratio Eclipsing Binary with δ Scuti Pulsations
Authors: Pavol Gajdoš, Štefan Parimucha, Marek Skarka, Matúš Kamenec, Jozef Lipták, Raine Karjalainen
Figure caption: Collected phase-folded LC in ﹩g^{\prime} ﹩ and ﹩r^{\prime} ﹩ filters by dates of observations (see details in Table 2). Solid-blue curves are synthetic models based on the parameters from Section 5.
Paper: Analysis of KIC 7023917: Spotted Low-mass Ratio Eclipsing Binary with δ Scuti Pulsations
Authors: Pavol Gajdoš, Štefan Parimucha, Marek Skarka, Matúš Kamenec, Jozef Lipták, Raine Karjalainen
Figure caption: RV measurements of the primary component of KIC 7023917 together with a synthetic model (solid line).
Paper: Analysis of KIC 7023917: Spotted Low-mass Ratio Eclipsing Binary with δ Scuti Pulsations
Authors: Pavol Gajdoš, Štefan Parimucha, Marek Skarka, Matúš Kamenec, Jozef Lipták, Raine Karjalainen
Figure caption: The mass–radius diagram for primary (red circle) and secondary component (red square) of KIC 7023917. White symbols show similar low-mass EBs from literature (both over-contact and detached systems; P.-E. Christopoulou et al. (2022), and references). The solid line represents the empirical relation for low-mass main sequence stars (Z. Eker et al. 2018).
Paper: Analysis of KIC 7023917: Spotted Low-mass Ratio Eclipsing Binary with δ Scuti Pulsations
Authors: Pavol Gajdoš, Štefan Parimucha, Marek Skarka, Matúš Kamenec, Jozef Lipták, Raine Karjalainen
Figure caption: A 3D model with the surface temperature distributions. The model is calculated for the parameters from Table 3 based on TESS observations (top panel). The model with predicted starspot (see Section 6) is shown in the bottom panel.
Paper: Analysis of KIC 7023917: Spotted Low-mass Ratio Eclipsing Binary with δ Scuti Pulsations
Authors: Pavol Gajdoš, Štefan Parimucha, Marek Skarka, Matúš Kamenec, Jozef Lipták, Raine Karjalainen
Figure caption: Pulsations on residual LC from TESS after removing the model LC (Section 5). The solid line shows the model from period analysis (70 strongest frequencies used).
Paper: Analysis of KIC 7023917: Spotted Low-mass Ratio Eclipsing Binary with δ Scuti Pulsations
Authors: Pavol Gajdoš, Štefan Parimucha, Marek Skarka, Matúš Kamenec, Jozef Lipták, Raine Karjalainen
Figure caption: Phase-folded LCs obtained by Kepler and TESS mission with model (solid line).