adsabs/AstroCLIMB huggingface dataset:
Paper: Detection of Ubiquitous Weak and Impulsive Nonthermal Emissions from the Solar Corona
Authors: Rohit Sharma, Divya Oberoi, Marina Battaglia, Säm Krucker
Figure caption: Radio solar maps for the eight frequency bands. The color bar is saturated at 0.4 MK. The peak brightness temperatures from 108 to 240 MHz are 0.26, 0.30, 0.32, 0.34, 0.37, 0.40, 0.44, and 0.47 MK, respectively. The black circle in each panel marks the size of the visible Sun, i.e., 16′ radius. The maps were time-averaged over the entire 30 minutes ranging from 03:24 to 03:39 UT and 03:44 to 03:59 UT.
Paper: Detectability of Rotational Modulation in Kepler Sun-like Stars as a Function of Age
Authors: Kento Masuda
Figure caption: Test results for the old low-mass stars (Section 4.3.3). See the caption of Figure 7.
Paper: KIC 3440495: A Rapidly Rotating δ Scuti-γ Doradus Hybrid Pulsator in a Binary System
Authors: Shuguo Ma, Ali Esamdin, Antonio García Hernández, Simon J. Murphy, Chenglong Lv, Peng Wei, Michel Rieutord, Javier Pascual-Granado, Fei Dang, Hubiao Niu, TaoZhi Yang, Guojie Feng, Rivkat Karimov, Yusuf Tillayev
Figure caption: The phase evolution diagram over a time span of about four years for the residuals of the KLC data. Pixel shades, from dark to light, indicate the median flux in each (time, phase) bin from low to high. The pixels span 10 days in time and 0.05 in phase. The vertical white gap corresponds to a time span without Kepler data. The brightness can be seen to be uneven in one phase range from this diagram and to evolve gradually in time from left to right. The dark regions in the diagram can be seen as starspots on the surface of the star.
Paper: KIC 3440495: A Rapidly Rotating δ Scuti-γ Doradus Hybrid Pulsator in a Binary System
Authors: Shuguo Ma, Ali Esamdin, Antonio García Hernández, Simon J. Murphy, Chenglong Lv, Peng Wei, Michel Rieutord, Javier Pascual-Granado, Fei Dang, Hubiao Niu, TaoZhi Yang, Guojie Feng, Rivkat Karimov, Yusuf Tillayev
Figure caption: A prominent peak marked with a red line is displayed in the FT, AC, and HFD. The peak is around 2.33 day−1 (27 μHz) corresponding to the rotation. The other peaks at larger values do not coincide in the three methods. But there is a maximum value around 6.74 dat−1(78 μHz), which is 3 times the rotation frequency in the AC and HFD.
Paper: KIC 3440495: A Rapidly Rotating δ Scuti-γ Doradus Hybrid Pulsator in a Binary System
Authors: Shuguo Ma, Ali Esamdin, Antonio García Hernández, Simon J. Murphy, Chenglong Lv, Peng Wei, Michel Rieutord, Javier Pascual-Granado, Fei Dang, Hubiao Niu, TaoZhi Yang, Guojie Feng, Rivkat Karimov, Yusuf Tillayev
Figure caption: The échelle diagram with a frequency spacing of Δν = 54.5 μHz shows a clear ridge, which infers Δν is the possible large separation.
Paper: KIC 3440495: A Rapidly Rotating δ Scuti-γ Doradus Hybrid Pulsator in a Binary System
Authors: Shuguo Ma, Ali Esamdin, Antonio García Hernández, Simon J. Murphy, Chenglong Lv, Peng Wei, Michel Rieutord, Javier Pascual-Granado, Fei Dang, Hubiao Niu, TaoZhi Yang, Guojie Feng, Rivkat Karimov, Yusuf Tillayev
Figure caption: The time-delay measurements of the dominant high frequencies f  h1 by using multiple 10 day light-curve segments, and one of the best-fitting models for the time delay.
Paper: KIC 3440495: A Rapidly Rotating δ Scuti-γ Doradus Hybrid Pulsator in a Binary System
Authors: Shuguo Ma, Ali Esamdin, Antonio García Hernández, Simon J. Murphy, Chenglong Lv, Peng Wei, Michel Rieutord, Javier Pascual-Granado, Fei Dang, Hubiao Niu, TaoZhi Yang, Guojie Feng, Rivkat Karimov, Yusuf Tillayev
Figure caption: The amplitude spectrum of the residuals after filtering out all the significant pulsating frequencies (S/N ≥ 5) independent of rotation in the KLC data, but leaving the rotation frequency and its harmonics.
Paper: KIC 3440495: A Rapidly Rotating δ Scuti-γ Doradus Hybrid Pulsator in a Binary System
Authors: Shuguo Ma, Ali Esamdin, Antonio García Hernández, Simon J. Murphy, Chenglong Lv, Peng Wei, Michel Rieutord, Javier Pascual-Granado, Fei Dang, Hubiao Niu, TaoZhi Yang, Guojie Feng, Rivkat Karimov, Yusuf Tillayev
Figure caption: The amplitude spectra of KIC 3440495 from Kepler data and Altair from MOST data from 2012. KSC and KLC are the abbreviations for Kepler short and long cadence, respectively.
Paper: KIC 3440495: A Rapidly Rotating δ Scuti-γ Doradus Hybrid Pulsator in a Binary System
Authors: Shuguo Ma, Ali Esamdin, Antonio García Hernández, Simon J. Murphy, Chenglong Lv, Peng Wei, Michel Rieutord, Javier Pascual-Granado, Fei Dang, Hubiao Niu, TaoZhi Yang, Guojie Feng, Rivkat Karimov, Yusuf Tillayev
Figure caption: The amplitude spectra and phase folded light curves of each segment. The phases are binned every 0.002 phase.
Paper: KIC 3440495: A Rapidly Rotating δ Scuti-γ Doradus Hybrid Pulsator in a Binary System
Authors: Shuguo Ma, Ali Esamdin, Antonio García Hernández, Simon J. Murphy, Chenglong Lv, Peng Wei, Michel Rieutord, Javier Pascual-Granado, Fei Dang, Hubiao Niu, TaoZhi Yang, Guojie Feng, Rivkat Karimov, Yusuf Tillayev
Figure caption: The time-delay measurements of the four high frequencies, using 10 day light-curve segments.
Paper: KIC 3440495: A Rapidly Rotating δ Scuti-γ Doradus Hybrid Pulsator in a Binary System
Authors: Shuguo Ma, Ali Esamdin, Antonio García Hernández, Simon J. Murphy, Chenglong Lv, Peng Wei, Michel Rieutord, Javier Pascual-Granado, Fei Dang, Hubiao Niu, TaoZhi Yang, Guojie Feng, Rivkat Karimov, Yusuf Tillayev
Figure caption: The phase folded light curve of KIC 3440495 with a period of 0.430495(1) days in the KSC data. The phase is binned every 0.002 phase.
Paper: Mapping the Thermal Condensation of Diffuse H I in the North Celestial Pole Loop
Authors: Mukesh Taank, Antoine Marchal, Peter G. Martin, Luka Vujeva
Figure caption: Mosaic of N H I maps of the individual Gaussian components. The maps are sorted by mean velocity. The labels in the bottom left corner represent the sorting of that particular Gaussian component. The number beside this label is the mean velocity dispersion (σ) in units of km s−1. Note the different ranges of the color bars.
Paper: Mapping the Thermal Condensation of Diffuse H I in the North Celestial Pole Loop
Authors: Mukesh Taank, Antoine Marchal, Peter G. Martin, Luka Vujeva
Figure caption: Gaussian decomposition by ROHSA at the absorption position of DF from our final LVC model cube. The original signal is shown in gray and the total brightness temperature encoded by ROHSA is shown in black. Colored lines represent each of the four components, as seen in Figure 8. Red represents CNM, green represents LNM, blue represents WNMA, and cyan represents WNMD.
Paper: Mapping the Thermal Condensation of Diffuse H I in the North Celestial Pole Loop
Authors: Mukesh Taank, Antoine Marchal, Peter G. Martin, Luka Vujeva
Figure caption: Centroid velocity map of WNMA+WNMD from our best model inferred with ROHSA. (The geometric/nonphysical structure in regions of low intensity arises from imperfect stray radiation correction in blocks of the survey observed at different times.) Contours and annotation are the same as in Figure 8.
Paper: Mapping the Thermal Condensation of Diffuse H I in the North Celestial Pole Loop
Authors: Mukesh Taank, Antoine Marchal, Peter G. Martin, Luka Vujeva
Figure caption: Polygons (white regions in left panel) were developed to isolate contaminating extra-Galactic emission. This contamination can be seen in the map of the total column density (right) and is removed channel by channel by in-painting, with the final result seen in Figure 2. The large white box outlines the subregion of the data that we chose to focus on for the analysis.
Paper: Mapping the Thermal Condensation of Diffuse H I in the North Celestial Pole Loop
Authors: Mukesh Taank, Antoine Marchal, Peter G. Martin, Luka Vujeva
Figure caption: Mosaic like Figure B1, but of maps of the velocity dispersion, σ, of the individual Gaussian components.
Paper: Mapping the Thermal Condensation of Diffuse H I in the North Celestial Pole Loop
Authors: Mukesh Taank, Antoine Marchal, Peter G. Martin, Luka Vujeva
Figure caption: Mosaic like Figure B1, but of maps of the mean velocity, μ, of the individual Gaussian components.
Paper: A Millimeter-multiwavelength Continuum Study of VLA 1623 West
Authors: Arnaud Michel, Sarah I. Sadavoy, Patrick D. Sheehan, Leslie W. Looney, Erin G. Cox
Figure caption: Top: simulated observations at 0.87 mm of the flared, edge-on disk toy model image using the same observational conditions as VLA 1623W. The parameters used are h off = 4 au, h 0 = 0.1, β = 5, and R 0 = 30 au. The black dotted lines represent the contours of the 0.87 mm model disk emission at 20, 50, and 100 σ 7. Bottom: imaged residuals after the subtraction of the Fourier transform of the best-fit FTG model from the simulated observations of the toy model (top panel). These imaged residuals correspond to the central panel in Figure 10 as it is the qualitatively most similar to the observation’s residuals. The black contours represent ±3, 5, 10, and 20 σ 7 residuals.
Paper: A Millimeter-multiwavelength Continuum Study of VLA 1623 West
Authors: Arnaud Michel, Sarah I. Sadavoy, Patrick D. Sheehan, Leslie W. Looney, Erin G. Cox
Figure caption: The variety of morphologies from the best-fit geometric models for the 0.87 mm data are shown here. Top: the intensities as a function of radial distance are shown. The solid black curve represents the normalized 0.87 mm circularized Gaussian beam, thus illustrating the approximate image resolution. Bottom: the corresponding uv profiles of the best-fit geometric models at 0.87 mm with the observations plotted in black. These are the same profiles shown as red lines in the right-most panels of Figure 2.
Paper: A Millimeter-multiwavelength Continuum Study of VLA 1623 West
Authors: Arnaud Michel, Sarah I. Sadavoy, Patrick D. Sheehan, Leslie W. Looney, Erin G. Cox
Figure caption: Testing the effect of changing R 0 on the residual morphologies. For both grids we use h off = 4 au, and the black contours represent ±3, 5, 10, 15, and 20 σ 7 residuals. Top grid: we use R 0 = 10 au with varying h 0 and β. Bottom grid: we use R 0 = 50 au with varying h 0 and β, which are different from R 0 = 10 and 30 au.
Paper: A Millimeter-multiwavelength Continuum Study of VLA 1623 West
Authors: Arnaud Michel, Sarah I. Sadavoy, Patrick D. Sheehan, Leslie W. Looney, Erin G. Cox
Figure caption: Left: map of spectral index for the region where the intensity is greater than 10 σ both in Bands 6 and 7. The dotted lines represent the contours of 0.87 mm disk emission of VLA 1623W at 20, 50, 100, and 200 σ 7 smoothed to the same resolution as the spectral index map. Right: spectral index along the disk’s major axis. The x-axis is the offset from the disk center, and from the FTG fits, we find σ  D  ∼ 0.″45–0.″46. The shaded light blue is the spectral index evaluated assuming a 10% flux uncertainty from the calibration for both 1.3 and 0.87 mm data.
Paper: A Millimeter-multiwavelength Continuum Study of VLA 1623 West
Authors: Arnaud Michel, Sarah I. Sadavoy, Patrick D. Sheehan, Leslie W. Looney, Erin G. Cox
Figure caption: The parameters used to generate the flared disk models for this grid are h off = 3 au and R 0 = 30 au, where we explore the effect of changing h 0 and β. The black contours represent ±3, 5, 10, 15, and 20 σ 7 residuals.
Paper: A Millimeter-multiwavelength Continuum Study of VLA 1623 West
Authors: Arnaud Michel, Sarah I. Sadavoy, Patrick D. Sheehan, Leslie W. Looney, Erin G. Cox
Figure caption: Intensity profiles along the disk major axis of the best-fit disk model images presented in Figure 7. The best-fit disk profiles prior to the uv plane sampling, Fourier transformation, and beam convolution are shown in Figure 4. Left: at 1.3 mm and Right: at 0.87 mm.
Paper: A Millimeter-multiwavelength Continuum Study of VLA 1623 West
Authors: Arnaud Michel, Sarah I. Sadavoy, Patrick D. Sheehan, Leslie W. Looney, Erin G. Cox
Figure caption: Images of the best-fit disk models compared to the observations (leftmost panel). The model images were obtained by taking the Fourier transform of the best-fit disk model image and sampling the uv plane of the observations using GALARIO. Top: at 1.3 mm and Bottom: at 0.87 mm.
Paper: A Millimeter-multiwavelength Continuum Study of VLA 1623 West
Authors: Arnaud Michel, Sarah I. Sadavoy, Patrick D. Sheehan, Leslie W. Looney, Erin G. Cox
Figure caption: Same as Figure 9 but for this grid we use h off = 4 au.
Paper: A Millimeter-multiwavelength Continuum Study of VLA 1623 West
Authors: Arnaud Michel, Sarah I. Sadavoy, Patrick D. Sheehan, Leslie W. Looney, Erin G. Cox
Figure caption: Same as Figure 9 but for this grid we use h off = 5 au.
Paper: Three-dimensional Global Hybrid Simulations of Flux Transfer Event Showers at Mercury
Authors: Quanming Lu, Jin Guo, San Lu, Xueyi Wang, James A. Slavin, Weijie Sun, Rongsheng Wang, Yu Lin, Jun Zhong
Figure caption: 3D view of Mercury’s magnetosphere obtained from our hybrid simulation at t = 127.89s in Case 2. (a) The ion number density N  i  in the noon–midnight meridian and equatorial planes. The magnetic structure of six FTEs is represented by 3D magnetic field lines with different colors (red, green, and violet). (b) The enlarged view of the denoted region in (a), and F1–3 represent three FTEs. (c) Three components of the magnetic field (B  x , B  y , and B  z ) and the ion number density N  i  along the dashed line in (b).
Paper: Three-dimensional Global Hybrid Simulations of Flux Transfer Event Showers at Mercury
Authors: Quanming Lu, Jin Guo, San Lu, Xueyi Wang, James A. Slavin, Weijie Sun, Rongsheng Wang, Yu Lin, Jun Zhong
Figure caption: 3D view of Mercury’s magnetosphere obtained from our hybrid simulation at t = 120.10 s in Case 1. (a) The ion number density N  i  in the noon–midnight meridian and equatorial planes. The magnetic structure of flux ropes is represented by 3D magnetic field lines with different colors (red, blue, and green). (b) The enlarged view of the denoted region in (a), and F1–2 represent two FTEs. (c) Three components of the magnetic field (B  x , B  y , and B  z ) and the ion number density N  i  along the dashed line in (b).
Paper: Three-dimensional Global Hybrid Simulations of Flux Transfer Event Showers at Mercury
Authors: Quanming Lu, Jin Guo, San Lu, Xueyi Wang, James A. Slavin, Weijie Sun, Rongsheng Wang, Yu Lin, Jun Zhong
Figure caption: The comparison of magnetic field obtained from our gcPIC-hybrid simulation in Case 1 with that in time following the MESSENGER orbit related to the observation on 2013 June 18. (a) The amplitude of magnetic field in the noon–midnight meridian and equatorial planes obtained from the simulation at t = 104.04 s,and the MESSENGER’s trajectory on 2013 June 18 is plotted in red. (b) The magnetic field from the MESSENGER observation on 2013 June 18. The magnetic field from the simulation at t = 104.04 s, which is obtained along the satellite trajectory denoted by the red line in (b), is also exhibited for reference. The vertical shaded region with the yellow color and vertical green dashed line denote respectively the intervals in the observation and simulation, where FTEs are formed.
Paper: A Mid-infrared Flare in the Seyfert Galaxy NGC 3786: A Changing-look Event Triggered by an Obscured Tidal Disruption Event?
Authors: Suyeon Son, Minjin Kim, Luis C. Ho, Dohyeong Kim, Taehyun Kim
Figure caption: Spectra obtained with the Perkins 1.8 m telescope before the flare (left) and with Gemini-North after the flare (right), for the Hβ and [O III] region (top) and Hα and [N II] region (bottom). In all panels, the histogram and the green line represent the original spectra and the best-fit model, respectively, whereas the blue and the magenta dashed lines denote the best-fit models for the narrow and the broad emission lines, respectively.
Paper: A Mid-infrared Flare in the Seyfert Galaxy NGC 3786: A Changing-look Event Triggered by an Obscured Tidal Disruption Event?
Authors: Suyeon Son, Minjin Kim, Luis C. Ho, Dohyeong Kim, Taehyun Kim
Figure caption: Fitting results for NIR spectra obtained before and after the IR flare. Spectra obtained with IRTF before the flare (left) and with Gemini-North after the flare (right), for Paβ (top) and Paα (bottom). Note that Paα data from IRTF are heavily compromised due to the imperfect telluric correction. Therefore, the emission-like feature around 18750 Å in the IRTF spectrum is an artifact caused by incomplete removal of the telluric features rather than Paα emission.
Paper: Three-dimensional Global Hybrid Simulations of Flux Transfer Event Showers at Mercury
Authors: Quanming Lu, Jin Guo, San Lu, Xueyi Wang, James A. Slavin, Weijie Sun, Rongsheng Wang, Yu Lin, Jun Zhong
Figure caption: The magnetic field lines and ion number density N  i  in the northern hemisphere of the high-latitude nightside magnetosphere (in the noon–midnight meridian plane) at t = (a) 127.89, (b) 135.72, (c) 143.55, and (d) 160.78 s. The results are obtained in Case 2 and represented in the noon–midnight meridian plane, and F1–7 denote the positions of seven FTEs.
Paper: Three-dimensional Global Hybrid Simulations of Flux Transfer Event Showers at Mercury
Authors: Quanming Lu, Jin Guo, San Lu, Xueyi Wang, James A. Slavin, Weijie Sun, Rongsheng Wang, Yu Lin, Jun Zhong
Figure caption: Stack plot of B  x  along the magnetopause (denoted by the dashed line in Figure 2(b)) in the northern hemisphere at different times. The boundaries between the magnetopause and cusp are denoted by the gray dashed lines. (b) The evolution of B  x  at z = 0.7 R  M  (green dashed line in (a)). The results are obtained in Case 1.
Paper: A Mid-infrared Flare in the Seyfert Galaxy NGC 3786: A Changing-look Event Triggered by an Obscured Tidal Disruption Event?
Authors: Suyeon Son, Minjin Kim, Luis C. Ho, Dohyeong Kim, Taehyun Kim
Figure caption: Results of 2D imaging decomposition of MIR imaging data obtained with Spitzer IRAC1 (3.6 μm). (a) Top panel shows surface brightness profiles of original data (open circles), nucleus (dotted line), bulge (solid red line), oval (dotted–dashed green line), and disk (dashed blue line) component. The residuals are displayed in the bottom panel. (b) Original image. (c) Best-fit model for only the host components. (d) Residuals.
Paper: Contribution of Spicules to Solar Coronal Emission
Authors: Shanwlee Sow Mondal, James A. Klimchuk, Aveek Sarkar
Figure caption: Loop-integrated intensity in Fe XII and Fe XIV as a function of time for Run1. The red dashed curve is the contribution only from the injected spicule material, while the green dashed curve is the contribution of the loop material excluding the injected spicule. The black curve is the sum of both the spicule and nonspicule intensities. Time-integrated intensities over the 190 s required for the shock to reach the right foot point are indicated. Even though the emission from the injected spicule material decreases rapidly, it is so much brighter than the shock-heated preexisting material that it contributes more to the time integration.
Paper: Contribution of Spicules to Solar Coronal Emission
Authors: Shanwlee Sow Mondal, James A. Klimchuk, Aveek Sarkar
Figure caption: Spatially and temporally averaged synthetic spectral line profiles of Fe XII and Fe XIV for Run1. The line profiles are averaged over the full length of the loop and over the 190 s needed for the shock to reach the other end of the loop. Spectral line profiles are highly blueshifted, and the shapes do not agree with the observed asymmetric line profiles.
Paper: Contribution of Spicules to Solar Coronal Emission
Authors: Shanwlee Sow Mondal, James A. Klimchuk, Aveek Sarkar
Figure caption: Plasma variables along the loop at t = 70 s in Run1. The colored dashed line marks the location of the shock front. The observed density and velocity jumps match well with γ = 1.015 indicating that the shock is locally isothermal, consistent with the temperature profile.
Paper: Contribution of Spicules to Solar Coronal Emission
Authors: Shanwlee Sow Mondal, James A. Klimchuk, Aveek Sarkar
Figure caption: Injection velocity, density, and temperature profiles as a function of time at the bottom boundary from Run1.
Paper: Contribution of Spicules to Solar Coronal Emission
Authors: Shanwlee Sow Mondal, James A. Klimchuk, Aveek Sarkar
Figure caption: Required number of spicules at any given time on the Sun as a function of the spicule cross-sectional area, estimated from the spicule occurrence rate (derived using Run1). Spicules with widths of 200–400 km are fairly common. The required number of spicules having widths in this range is marked by the shaded region in both plots.
Paper: Contribution of Spicules to Solar Coronal Emission
Authors: Shanwlee Sow Mondal, James A. Klimchuk, Aveek Sarkar
Figure caption: Logarithm of Fe XII and Fe XIV intensity (yellow and green, respectively) and temperature (dark orange) as a function of the position along the loop at t = 10 and 70 s in Run1. Units are given in the legend. The blue curve is the logarithm of the density with the scale on the right. The marked light orange region indicates the hot tip of the spicule, while the red region indicates the compressed post-shock plasma. The dotted–dashed line (ahead of the red region) marks the location of the shock front.
Paper: Contribution of Spicules to Solar Coronal Emission
Authors: Shanwlee Sow Mondal, James A. Klimchuk, Aveek Sarkar
Figure caption: Spatially and temporally averaged synthetic spectral line profiles of Fe XII and Fe XIV for the case when a spicule (with tip temperature of 2 MK) is injected in a hot loop with an apex temperature of 2 MK. The line profiles are averaged over 180 s (the time taken by the shock to traverse the loop).
Paper: Contribution of Spicules to Solar Coronal Emission
Authors: Shanwlee Sow Mondal, James A. Klimchuk, Aveek Sarkar
Figure caption: Required occurrence rate of spicules to explain the typically observed Fe XII and Fe XIV intensities for active regions and the quiet Sun (curves are derived from Run1). The occurrence rate is plotted against the cross-sectional area of spicules.
Paper: Contribution of Spicules to Solar Coronal Emission
Authors: Shanwlee Sow Mondal, James A. Klimchuk, Aveek Sarkar
Figure caption: Density and temperature profiles of the initial static equilibrium loop.
Paper: The Tidal Disruption Event AT2021ehb: Evidence of Relativistic Disk Reflection, and Rapid Evolution of the Disk–Corona System
Authors: Yuhan Yao, Wenbin Lu, Muryel Guolo, Dheeraj R. Pasham, Suvi Gezari, Marat Gilfanov, Keith C. Gendreau, Fiona Harrison, S. Bradley Cenko, S. R. Kulkarni, Jon M. Miller, Dominic J. Walton, Javier A. García, Sjoert van Velzen, Kate D. Alexander, James C. A. Miller-Jones, Matt Nicholl, Erica Hammerstein, Pavel Medvedev, Daniel Stern, Vikram Ravi, R. Sunyaev, Joshua S. Bloom, Matthew J. Graham, Erik C. Kool, Ashish A. Mahabal, Frank J. Masci, Josiah Purdum, Ben Rusholme, Yashvi Sharma, Roger Smith, Jesper Sollerman
Figure caption: Upper: blackbody luminosity of the UV/optical emission (L bb;  Section 4.1) compared with the observed isotropic equivalent 0.3–10 keV X-ray luminosity (L X) from XRT (Section 4.4.5) and NICER (Section 4.4.6). Lower: the 2500 Å to X-ray spectral slope measured by Swift observations (Equation (3), (4)).
Paper: The Tidal Disruption Event AT2021ehb: Evidence of Relativistic Disk Reflection, and Rapid Evolution of the Disk–Corona System
Authors: Yuhan Yao, Wenbin Lu, Muryel Guolo, Dheeraj R. Pasham, Suvi Gezari, Marat Gilfanov, Keith C. Gendreau, Fiona Harrison, S. Bradley Cenko, S. R. Kulkarni, Jon M. Miller, Dominic J. Walton, Javier A. García, Sjoert van Velzen, Kate D. Alexander, James C. A. Miller-Jones, Matt Nicholl, Erica Hammerstein, Pavel Medvedev, Daniel Stern, Vikram Ravi, R. Sunyaev, Joshua S. Bloom, Matthew J. Graham, Erik C. Kool, Ashish A. Mahabal, Frank J. Masci, Josiah Purdum, Ben Rusholme, Yashvi Sharma, Roger Smith, Jesper Sollerman
Figure caption: The bolometric luminosity L bol as a function of α OX. L bol is converted to λ Edd assuming ﹩\mathrm{log}({M}_{\mathrm{BH}}/{M}_{\odot })=7.03﹩ (Section 3.1). Note that the uncertainty of λ Edd should be greater than the uncertainty of L bol by 0.44 dex (i.e., the uncertainty of M BH), which is not included in the figure.