adsabs/AstroCLIMB huggingface dataset:
Paper: AGN Selection and Demographics in GOODS-S/HUDF from X-Ray to Radio
Authors: Jianwei Lyu, 建伟 吕, Stacey Alberts, George H. Rieke, Wiphu Rujopakarn
Figure caption: The distribution of AGN luminosity and BH mass for AGNs identified in this work.
Paper: The Impact of Beam Variations on Power Spectrum Estimation for 21 cm Cosmology. I. Simulations of Foreground Contamination for HERA
Authors: Honggeun Kim, Bang D. Nhan, Jacqueline N. Hewitt, Nicholas S. Kern, Joshua S. Dillon, Eloy de Lera Acedo, Scott B. C. Dynes, Nivedita Mahesh, Nicolas Fagnoni, David R. DeBoer
Figure caption: Spherically averaged 1D foreground power spectrum estimates for the vertical (left), horizontal (middle), and tilting (right) feed motions. The power spectra are constructed from the 2D power spectra (Figure 15), with k modes satisfying k ∥ ≥ k ∥,hor + 0.4 h Mpc−1, to minimize the intrinsic foreground spillovers due to the spectral structure in the primary beam together with the pitchfork effect. The solid black curve is the power spectrum estimate of the fiducial model and the colored dashed curves are for the perturbed beams labeled in the legend. The dotted gray curve denotes the EoR power spectrum with the same cut applied.
Paper: The Impact of Beam Variations on Power Spectrum Estimation for 21 cm Cosmology. I. Simulations of Foreground Contamination for HERA
Authors: Honggeun Kim, Bang D. Nhan, Jacqueline N. Hewitt, Nicholas S. Kern, Joshua S. Dillon, Eloy de Lera Acedo, Scott B. C. Dynes, Nivedita Mahesh, Nicolas Fagnoni, David R. DeBoer
Figure caption: Comparison of CST simulated beams and interpolated ones at off-grid feed positions or tilts, labeled in the title of each panel, at 165 MHz. The title indicates the (x, y, z) feed positions for the vertical and horizontal feed offsets, and (ϕ, θ) for the tilts. Each pair consists of the line profiles of the power beams, with the zenith angle in the EW direction (top) and their fractional difference (bottom). The top three are for the vertical feed offset, the middle three are for the horizontal displacement, and the bottom three for the tilting motion.
Paper: The Impact of Beam Variations on Power Spectrum Estimation for 21 cm Cosmology. I. Simulations of Foreground Contamination for HERA
Authors: Honggeun Kim, Bang D. Nhan, Jacqueline N. Hewitt, Nicholas S. Kern, Joshua S. Dillon, Eloy de Lera Acedo, Scott B. C. Dynes, Nivedita Mahesh, Nicolas Fagnoni, David R. DeBoer
Figure caption: Comparison of the CST simulated beams and interpolated ones at off-grid feed positions along the frequency. The zenith point is chosen for validation. From top to bottom, each pair plot represents the feed offset in the z-axis, in the xy plane, and in the tilt. Overall, the two power beams in each panel agree better than ∼1%, and the Fourier transform of the interpolated beam does not show extra high-frequency structure compared to that of the CST simulated one.
Paper: The Orbits and Dynamical Masses of the Castor System
Authors: Guillermo Torres, Gail H. Schaefer, John D. Monnier, Narsireddy Anugu, Claire L. Davies, Jacob Ennis, Christopher D. Farrington, Tyler Gardner, Robert Klement, Stefan Kraus, Aaron Labdon, Cyprien Lanthermann, Jean-Baptiste Le Bouquin, Benjamin R. Setterholm, Theo ten Brummelaar
Figure caption: Radial velocities in the Castor AB orbit along with our model (solid blue line for the primary). Motion in the inner orbits has been subtracted. For TRES we represent the individual observations, whereas the DS measurements are shown by green squares at their median value and median time of observation. The corresponding velocity uncertainties are calculated from the median absolute deviations and are approximately the same size as the symbols. The horizontal error bars for the DS represent the total time span of those observations. A dotted line marks the center-of-mass velocity of the quadruple system. As a check, we display also the historical velocities of both Castor A and B from the sources described in the Appendix. In each case we subtract off the motion in the inner orbits, and plot the median value with its associated uncertainty, at the median epoch. The horizontal error bars represent the time span.
Paper: The Orbits and Dynamical Masses of the Castor System
Authors: Guillermo Torres, Gail H. Schaefer, John D. Monnier, Narsireddy Anugu, Claire L. Davies, Jacob Ennis, Christopher D. Farrington, Tyler Gardner, Robert Klement, Stefan Kraus, Aaron Labdon, Cyprien Lanthermann, Jean-Baptiste Le Bouquin, Benjamin R. Setterholm, Theo ten Brummelaar
Figure caption: CHARA observations of Castor A along with our best-fit model described in Section 3. Except for one observation from 2007 in the first quadrant, error ellipses and short line segments connecting each measurement to the predicted position on the orbit are generally too small to be seen. Orange circles are drawn at the location of each measurement for better visibility. An enlargement of a small section of the orbit is shown in the inset to illustrate the error ellipses. The cross at the origin marks the position of Castor Aa, and the dotted line represents the line of nodes (the ascending node is marked with the Ω symbol). Periastron is indicated with a red square labeled “P.”
Paper: The Orbits and Dynamical Masses of the Castor System
Authors: Guillermo Torres, Gail H. Schaefer, John D. Monnier, Narsireddy Anugu, Claire L. Davies, Jacob Ennis, Christopher D. Farrington, Tyler Gardner, Robert Klement, Stefan Kraus, Aaron Labdon, Cyprien Lanthermann, Jean-Baptiste Le Bouquin, Benjamin R. Setterholm, Theo ten Brummelaar
Figure caption: Top: measurements of the relative position of Castor AB from the Washington Double Star catalog (Worley & Douglass 1997; Mason et al. 2001) along with our best-fit model described in Section 3. Thin line segments connect the measured position to the expected location from our model. The dotted line represents the line of nodes (the Ω symbol indicates the ascending node), and periastron is marked with a cyan square (“P”). Only measurements that have both a position angle and a separation are shown. Others are shown below. Bottom panels: all position angle and separation measurements as a function of time. Incomplete observations missing either the position angle or the separation are distinguished with red squares. The arrow marks the time of periastron passage.
Paper: The Orbits and Dynamical Masses of the Castor System
Authors: Guillermo Torres, Gail H. Schaefer, John D. Monnier, Narsireddy Anugu, Claire L. Davies, Jacob Ennis, Christopher D. Farrington, Tyler Gardner, Robert Klement, Stefan Kraus, Aaron Labdon, Cyprien Lanthermann, Jean-Baptiste Le Bouquin, Benjamin R. Setterholm, Theo ten Brummelaar
Figure caption: Similar to Figure 1 for Castor B. The error ellipses are now visible because of the smaller scale of the orbit.
Paper: The Orbits and Dynamical Masses of the Castor System
Authors: Guillermo Torres, Gail H. Schaefer, John D. Monnier, Narsireddy Anugu, Claire L. Davies, Jacob Ennis, Christopher D. Farrington, Tyler Gardner, Robert Klement, Stefan Kraus, Aaron Labdon, Cyprien Lanthermann, Jean-Baptiste Le Bouquin, Benjamin R. Setterholm, Theo ten Brummelaar
Figure caption: Measured masses and radii of Castor Aa and Ba shown against solar-metallicity model isochrones from the PARSEC series of Chen et al. (2014). Ages every 20 Myr are as labeled. The isochrone that best fits the measurements for Castor Aa, shown with a solid line, has an age of 290 Myr.
Paper: The Orbits and Dynamical Masses of the Castor System
Authors: Guillermo Torres, Gail H. Schaefer, John D. Monnier, Narsireddy Anugu, Claire L. Davies, Jacob Ennis, Christopher D. Farrington, Tyler Gardner, Robert Klement, Stefan Kraus, Aaron Labdon, Cyprien Lanthermann, Jean-Baptiste Le Bouquin, Benjamin R. Setterholm, Theo ten Brummelaar
Figure caption: Radial velocity measurements for Castor Aa from the DS and TRES instruments. The solid curve is our model from Section 3, and motion in the outer orbit has been subtracted from the measurements for display purposes. The dashed line marks the center-of-mass velocity of the quadruple system. Error bars are not shown in the top panel for clarity. The lower panels display the residuals separately for the two instruments (note the different scales).
Paper: Solar Flare Forecast Using 3D Convolutional Neural Networks
Authors: Pengchao Sun, Wei Dai, Weiqi Ding, Song Feng, Yanmei Cui, Bo Liang, Zeyin Dong, Yunfei Yang
Figure caption: (a) The original SHARP magnetogram from AR 12673. (b) The downsampling magnetogram with 128 × 128 pixels. Panels (c) and (e) are the vertical and horizontal gradient maps of the panel (a). Panels (d) and (f) are similar to panels (c) and (e), but they are the gradient maps of panel (b).
Paper: The Orbits and Dynamical Masses of the Castor System
Authors: Guillermo Torres, Gail H. Schaefer, John D. Monnier, Narsireddy Anugu, Claire L. Davies, Jacob Ennis, Christopher D. Farrington, Tyler Gardner, Robert Klement, Stefan Kraus, Aaron Labdon, Cyprien Lanthermann, Jean-Baptiste Le Bouquin, Benjamin R. Setterholm, Theo ten Brummelaar
Figure caption: Same as Figure 3 for Castor Ba.
Paper: A Scintillation Arc Survey of 22 Pulsars with Low to Moderate Dispersion Measures
Authors: Dan R. Stinebring, Barney J. Rickett, Anthony H. Minter, Alex S. Hill, Adam P. Jussila, Lele Mathis, Maura A. McLaughlin, Stella Koch Ocker, Scott M. Ransom
Figure caption:  Left: curvature η  p  vs. single screen theory η 0.5; points without error bars represent estimates with zero credibility index. Points connected by a blue line are from the same pulsar at 2 or 3 frequencies. Two pulsars with discrepant frequency scaling between 1400 and 825 MHz are highlighted. Right: single screen hypothesis is distance to the screen (﹩{D}_{\mathrm{psr}}(1-{s}_{\max })﹩) vs. distance to each pulsar, assuming isotropic scattering. If the scattering were anisotropic, this becomes a minimum screen distance. Observations of the same pulsar are joined by a blue line, and marked by a black circle for 1400 MHz observations in 2020. The small symbols mark curvature estimates classified as low credibility. Narrow arcs are defined by ﹩{\rm{\Delta }}\mathrm{log}\eta \lt 0.2﹩ as estimated from the parabola-summation plots.
Paper: A Scintillation Arc Survey of 22 Pulsars with Low to Moderate Dispersion Measures
Authors: Dan R. Stinebring, Barney J. Rickett, Anthony H. Minter, Alex S. Hill, Adam P. Jussila, Lele Mathis, Maura A. McLaughlin, Stella Koch Ocker, Scott M. Ransom
Figure caption: Theoretical secondary spectra for strong scattering in a screen with a Kolmogorov phase spectrum. Format as for the observations. Left: isotropic (axial ratio = 1). Center: anisotropy axial ratio = 1.5, velocity along major spatial axis (ψ = 0). Right: axial ratio = 1.5, velocity perpendicular to major spatial axis (ψ = 90). The lower left panel is the autocorrelation function R(ν, t) vs. normalized frequency lag (vertical) and normalized spatial lag (horizontal); the lower right panel is an estimation of parabolic curvature from the secondary spectrum.
Paper: A Scintillation Arc Survey of 22 Pulsars with Low to Moderate Dispersion Measures
Authors: Dan R. Stinebring, Barney J. Rickett, Anthony H. Minter, Alex S. Hill, Adam P. Jussila, Lele Mathis, Maura A. McLaughlin, Stella Koch Ocker, Scott M. Ransom
Figure caption: Curvature. Left: comparison of the two methods (maxima in cross cuts and parabolic summation) for estimating curvature described in the text, averaged from positive and negative Doppler frequencies. As discussed in Section 3.2.2, we have created a subjective credibility index (0, 1, 2) for the η  p  estimate and plot green error bars to indicate low credibility index. Right: the pseudo-curvature η iss, which is defined below in Equation (7), plotted vs. the observed η  p  for data with credibility index greater than zero and valid results for the corrected Δν iss and Δt iss.
Paper: A Scintillation Arc Survey of 22 Pulsars with Low to Moderate Dispersion Measures
Authors: Dan R. Stinebring, Barney J. Rickett, Anthony H. Minter, Alex S. Hill, Adam P. Jussila, Lele Mathis, Maura A. McLaughlin, Stella Koch Ocker, Scott M. Ransom
Figure caption: The τ iss,1GHz values from the SAS are plotted against the DM values. The red line is a weighted least-squares fit. It has a logarithmic slope of 2.08, which is close to the τ ∝ DM2 behavior expected for scattering in a uniformly turbulent medium. However, it is clear that the line is a very poor fit to the data if the individual errors are to be believed, and they are well determined at the high DM part of the plot. See the text for further comments.
Paper: A Scintillation Arc Survey of 22 Pulsars with Low to Moderate Dispersion Measures
Authors: Dan R. Stinebring, Barney J. Rickett, Anthony H. Minter, Alex S. Hill, Adam P. Jussila, Lele Mathis, Maura A. McLaughlin, Stella Koch Ocker, Scott M. Ransom
Figure caption:  Left: arc width vs. DM, flagged by curvature credibility index. Right: the depth of the valley in the SS, as a ratio R v, defined by parabola summation at the estimated curvature divided by a summation of SS near the delay axis. In both left and right panels, points are flagged by the curvature credibility index.
Paper: Benchmark n ℓ-resolved Cross Sections of Single and Double Charge Exchange Processes in 1.67–20 keV u−1 C4+ Collisions with He
Authors: D. L. Guo, R. T. Zhang, X. L. Zhu, Y. Gao, K. Z. Lin, T. Cao, D. M. Zhao, X. B. Zhu, C. J. Zhang, S. F. Zhang, X. Ma
Figure caption: The absolute state-selective cross sections as a function of impact energy for SEC and DEC in collisions of C4+ with He. Experiments: present measurements (solid symbols); Guo et al. (2021) (opened symbols) and Dijkkamp et al. (1985) (crossed symbols); theories: Gao et al. (2017) (solid lines), Yan et al. (2013) (dashed lines), and Errea et al. (1995) (dotted–dashed lines).
Paper: Benchmark n ℓ-resolved Cross Sections of Single and Double Charge Exchange Processes in 1.67–20 keV u−1 C4+ Collisions with He
Authors: D. L. Guo, R. T. Zhang, X. L. Zhu, Y. Gao, K. Z. Lin, T. Cao, D. M. Zhao, X. B. Zhu, C. J. Zhang, S. F. Zhang, X. Ma
Figure caption: The fractions of 2ℓ population as a function of impact energy for SEC from He in collisions with C4+.
Paper: Benchmark n ℓ-resolved Cross Sections of Single and Double Charge Exchange Processes in 1.67–20 keV u−1 C4+ Collisions with He
Authors: D. L. Guo, R. T. Zhang, X. L. Zhu, Y. Gao, K. Z. Lin, T. Cao, D. M. Zhao, X. B. Zhu, C. J. Zhang, S. F. Zhang, X. Ma
Figure caption: Longitudinal recoil-ion momentum (p  rz ) distributions for single electron capture (SEC) and double electron capture (DEC) in C4++He collisions for various impact energies. The identified channels in the spectrum are indicated by n ℓ for SEC and n ℓ                      ﹩n^{\prime} {\ell }^{\prime} ﹩ for DEC.
Paper: Benchmark n ℓ-resolved Cross Sections of Single and Double Charge Exchange Processes in 1.67–20 keV u−1 C4+ Collisions with He
Authors: D. L. Guo, R. T. Zhang, X. L. Zhu, Y. Gao, K. Z. Lin, T. Cao, D. M. Zhao, X. B. Zhu, C. J. Zhang, S. F. Zhang, X. Ma
Figure caption: The fractions of ﹩2{\ell }2{\ell }^{\prime} ﹩ population as a function of impact energy for DEC from He in collisions with C4+.
Paper: LoTSS Jellyfish Galaxies. IV. Enhanced Star Formation on the Leading Half of Cluster Galaxies and Gas Compression in IC3949
Authors: Ian D. Roberts, Maojin Lang, 茂锦 郎, Daria Trotsenko, Ashley R. Bemis, Sara L. Ellison, Lihwai Lin, Hsi-An Pan, Alessandro Ignesti, Sarah Leslie, Reinout J. van Weeren
Figure caption: Maps of molecular gas and star formation properties in IC3949. From top to bottom: Hubble Space Telescope near-UV (F350LP), H2 surface density, H2 gas fraction (﹩{{\rm{\Sigma }}}_{{{\rm{H}}}_{2}}/{{\rm{\Sigma }}}_{\star }﹩), and H2 depletion time (﹩{{\rm{\Sigma }}}_{{{\rm{H}}}_{2}}/{{\rm{\Sigma }}}_{\mathrm{SFR}}﹩). The arrow in each panel shows the orientation of the observed RPS tail and the filled circle shows the FWHM resolution for the ALMA/MaNGA products. As a visual guide we also highlight the leading side region of enhanced star formation in each panel with the open circle. The HST data used in this figure can be found in MAST at: DOI: 10.17909/7ftv-0w17.
Paper: LoTSS Jellyfish Galaxies. IV. Enhanced Star Formation on the Leading Half of Cluster Galaxies and Gas Compression in IC3949
Authors: Ian D. Roberts, Maojin Lang, 茂锦 郎, Daria Trotsenko, Ashley R. Bemis, Sara L. Ellison, Lihwai Lin, Hsi-An Pan, Alessandro Ignesti, Sarah Leslie, Reinout J. van Weeren
Figure caption: Left, top: sSFR excess (see text for details) vs. galaxy stellar mass. Data points correspond to the jellyfish galaxy sample, error bars on ΔsSFR are calculated from bootstrap resampling, and error bars on stellar masses are taken from the Pipe3D catalog. The open markers correspond to the six jellyfish galaxies with marginally resolved ΣSFR maps (along the axis of the observed tail), since the sSFR/SFR excess measurements for these galaxies are less reliable than the rest of the sample. The dashed line shows the median ΔsSFR for the control sample and the shaded region encloses the interquartile range. Left, bottom: distributions of the sSFR excess for the jellyfish galaxy and control samples. Median (dashed) and mean (solid) are shown with the vertical lines. Right: same as left-hand panel but for the SFR excess (see text for details).
Paper: LoTSS Jellyfish Galaxies. IV. Enhanced Star Formation on the Leading Half of Cluster Galaxies and Gas Compression in IC3949
Authors: Ian D. Roberts, Maojin Lang, 茂锦 郎, Daria Trotsenko, Ashley R. Bemis, Sara L. Ellison, Lihwai Lin, Hsi-An Pan, Alessandro Ignesti, Sarah Leslie, Reinout J. van Weeren
Figure caption: sSFR/SFR excess vs. the offset between the axis which maximizes the star formation anisotropy and the LH–TH axis inferred from the observed tail direction. Star formation anisotropies measured with the sSFR excess are shown with magenta circles and star formation anisotropies measured with the SFR excess are shown with orange squares. Error bars on the sSFR/SFR excess are calculated from bootstrap resampling. The open markers correspond to the six jellyfish galaxies with marginally resolved ΣSFR maps (along the axis of the observed tail). In the upper panel we also show histograms of the distribution of Δθ sSFR and Δθ SFR.
Paper: LoTSS Jellyfish Galaxies. IV. Enhanced Star Formation on the Leading Half of Cluster Galaxies and Gas Compression in IC3949
Authors: Ian D. Roberts, Maojin Lang, 茂锦 郎, Daria Trotsenko, Ashley R. Bemis, Sara L. Ellison, Lihwai Lin, Hsi-An Pan, Alessandro Ignesti, Sarah Leslie, Reinout J. van Weeren
Figure caption: Position–velocity diagram (PVD) for IC3949 measured along the direction of the major axis (which roughly corresponds to the direction of the stripped tail). The width of the PVD box encompasses all of the CO emission shown in Figure 7. The gray contour corresponds to 3× rms of the CO cube.
Paper: LoTSS Jellyfish Galaxies. IV. Enhanced Star Formation on the Leading Half of Cluster Galaxies and Gas Compression in IC3949
Authors: Ian D. Roberts, Maojin Lang, 茂锦 郎, Daria Trotsenko, Ashley R. Bemis, Sara L. Ellison, Lihwai Lin, Hsi-An Pan, Alessandro Ignesti, Sarah Leslie, Reinout J. van Weeren
Figure caption: The location of the specific star formation rate peak for each jellyfish galaxy in polar coordinates. The azimuthal axis shows the orientation between the sSFR peak and the observed tail (see text for details) and the radial axis shows the radial offset of the sSFR peak from the galaxy center in units of the galaxy effective radius. The open markers correspond to the six jellyfish galaxies with marginally resolved ΣSFR maps (along the axis of the observed tail).
Paper: LoTSS Jellyfish Galaxies. IV. Enhanced Star Formation on the Leading Half of Cluster Galaxies and Gas Compression in IC3949
Authors: Ian D. Roberts, Maojin Lang, 茂锦 郎, Daria Trotsenko, Ashley R. Bemis, Sara L. Ellison, Lihwai Lin, Hsi-An Pan, Alessandro Ignesti, Sarah Leslie, Reinout J. van Weeren
Figure caption: Example schematics showing the observed tail direction (teal arrow) and the “tail direction” that is inferred by maximizing the SFR excess (gray arrow), overlaid on the SFR surface density maps. The solid lines show the corresponding divisions between the leading and trailing sides. We show three examples, one with Δθ SFR ∼ 0 (IC3913), one with an intermediate value of Δθ SFR (UGC10429), and one with Δθ SFR ∼ 180 (MRK0881).
Paper: LoTSS Jellyfish Galaxies. IV. Enhanced Star Formation on the Leading Half of Cluster Galaxies and Gas Compression in IC3949
Authors: Ian D. Roberts, Maojin Lang, 茂锦 郎, Daria Trotsenko, Ashley R. Bemis, Sara L. Ellison, Lihwai Lin, Hsi-An Pan, Alessandro Ignesti, Sarah Leslie, Reinout J. van Weeren
Figure caption: Redshift and integrated stellar mass distributions for jellyfish galaxies (magenta) and galaxies in the control sample (black).
Paper: The First Interferometric Measurements of NH2D/NH3 Ratio in Hot Corinos
Authors: Yoshihide Yamato, Kenji Furuya, Yuri Aikawa, Magnus V. Persson, John J. Tobin, Jes K. Jørgensen, Mihkel Kama
Figure caption: Same as Figure 3, but for 4A2.
Paper: The First Interferometric Measurements of NH2D/NH3 Ratio in Hot Corinos
Authors: Yoshihide Yamato, Kenji Furuya, Yuri Aikawa, Magnus V. Persson, John J. Tobin, Jes K. Jørgensen, Mihkel Kama
Figure caption: Comparison of model spectra of NH2D transitions predicted by the non-LTE simulation with central stellar masses of 1.0 M ⊙ (blue) and 0.08 M ⊙ (orange) and observed spectra toward 4A1 (top) and 4A2 (bottom). The zero intensity level is indicated by the gray dashed line.
Paper: The First Interferometric Measurements of NH2D/NH3 Ratio in Hot Corinos
Authors: Yoshihide Yamato, Kenji Furuya, Yuri Aikawa, Magnus V. Persson, John J. Tobin, Jes K. Jørgensen, Mihkel Kama
Figure caption: Dust temperature profile of the IRAS4A envelope presented in Persson et al. (2016).
Paper: The First Interferometric Measurements of NH2D/NH3 Ratio in Hot Corinos
Authors: Yoshihide Yamato, Kenji Furuya, Yuri Aikawa, Magnus V. Persson, John J. Tobin, Jes K. Jørgensen, Mihkel Kama
Figure caption: Gas density profile of the IRAS4A envelope presented in Persson et al. (2016).
Paper: Explaining the Moderate UV/X-Ray Correlation in AGN
Authors: Christos Panagiotou, Erin Kara, Michal Dovčiak
Figure caption: Example of the simulated X-ray (left), UVW2 (middle), and B (right panel) light curves. The vertical red lines in the left plot indicate the boundaries between time intervals with different heights. The colored region in the beginning of the X-ray light curve denotes the time when the UV/optical emission cannot yet be accurately estimated. The light curves have been arbitrarily scaled to allow comparison in a common plot.
Paper: Explaining the Moderate UV/X-Ray Correlation in AGN
Authors: Christos Panagiotou, Erin Kara, Michal Dovčiak
Figure caption: Normalized histogram of the maximum CCF between the X-ray and UVW2 light curve, R XW2, in the case of a variable height. The vertical red lines denote the values of the observed CCF for the sources listed in Table 1.
Paper: Explaining the Moderate UV/X-Ray Correlation in AGN
Authors: Christos Panagiotou, Erin Kara, Michal Dovčiak
Figure caption: Normalized histogram of the maximum CCF between the X-ray and UVW2 light curve, R XW2, in the case of a variable photon index.