adsabs/AstroCLIMB huggingface dataset:
Paper: Induction Heating in Super-Earths: A Thermochemical Perspective
Authors: Yihang Peng, Kristina Kislyakova, Donghao Zheng, Zhongtian Zhang, Jie Deng
Figure caption: The electrical conductivity (a), the modulus of the time-varying magnetic field (b), and the energy release per unit mass due to induction heating (c) as a function of depth inside GJ 486b with or without post-perovskite (pPv) phase in the conductivity profile.
Paper: Induction Heating in Super-Earths: A Thermochemical Perspective
Authors: Yihang Peng, Kristina Kislyakova, Donghao Zheng, Zhongtian Zhang, Jie Deng
Figure caption: The modulus of the θ and ϕ components of the time-varying magnetic field as a function of depth inside GJ 486b with a potential temperature of 1600 K and a mantle iron content of 11 mol%.
Paper: First Temperature Profile of a Stellar Flare Using Differential Chromatic Refraction
Authors: Riley W. Clarke, Federica Bianco, James R. A. Davenport, Jeffery Cooke, Sara Webb, Igor Andreoni, Tyler Pritchard, Aaron Roodman
Figure caption: Panel (A): lightcurve of the DWF 030225.574–545707.45 flare expressed as g magnitudes in excess of the quiescent stellar brightness. Open points indicate preflare epochs, and filled points indicate flaring epochs. We define the start of the flare as the first measurement to exceed the quiescent magnitude by 3σ, where the quiescent magnitude is taken to be the mean magnitude of the first 1000 s of observation, and σ is the standard deviation of all points within the first 1000 s. As noted in S. Webb et al. (2021), the lightcurve does not return to preflare brightness before the end of the observing period. Panel (B): raw d∥ measured on the images, relative to source position at t0. The weighted average d∥ of 91 reference stars, weighted by the stars’ astrometric standard deviation across the entire time series, is shown as a gray line, and the standard deviation of their relative position itself is shown as a filled region. Panel (C): detrended d∥ of the flare star generated by subtracting the weighted average d∥ of the reference stars shown in panel (B). A nine-point rolling median is shown by the dashed black line. Panel (D): rolling median over a nine-point window of the detrended data shown in panel (C) and the time series used for subsequent analysis in this work.
Paper: First Temperature Profile of a Stellar Flare Using Differential Chromatic Refraction
Authors: Riley W. Clarke, Federica Bianco, James R. A. Davenport, Jeffery Cooke, Sara Webb, Igor Andreoni, Tyler Pritchard, Aaron Roodman
Figure caption: The effect of emission lines on the effective wavelength λeff in a stellar flare. In red, the quiescent spectrum of an active dM7 star (see Section 5.1). The quiescent spectrum has been magnified by a factor of 60 for visibility. In green, the blackbody-only flaring spectrum with TBB = 14,000 K and XBB = 0.25%. In blue, the flaring spectrum with TBB = 14,000 K and XBB = 0.25%, as well as enhanced Ca H and K, Hβ, Hγ, and Hδ lines. The transmission function of the DES g filter is shown in gray. The vertical dashed lines correspond to the effective wavelength in g for each model: λeff,quiescent = 5035 Å, ﹩{\lambda }_{\mathrm{eff},\mathrm{flare}}=4721\,\,\unicode{x0212B}\,﹩, ﹩{\lambda }_{\mathrm{eff},\mathrm{flare}+\mathrm{lines}}=4677\,\,\unicode{x0212B}\,﹩. While this is a simplistic model for the inclusion of emission lines, it illustrates the effect the lines have on λeff: for the same blackbody temperature, the effective wavelength decreases. Conversely, a lower temperature is needed to explain the DCR if emission features are enhanced during the flare.
Paper: First Temperature Profile of a Stellar Flare Using Differential Chromatic Refraction
Authors: Riley W. Clarke, Federica Bianco, James R. A. Davenport, Jeffery Cooke, Sara Webb, Igor Andreoni, Tyler Pritchard, Aaron Roodman
Figure caption: The derived evolution of TBB and XBB under models with and without the inclusion of emission lines (colored and grey points, respectively) and that implement different postpeak constraints on XBB. In scenario 1 (top), XBB is allowed to vary freely throughout. In scenario 2 (middle), the value of XBB is held constant after peak. In scenario 3 (bottom), the postpeak evolution of XBB is constrained such that it cannot change by more than 0.107% of its peak value per second.
Paper: First Temperature Profile of a Stellar Flare Using Differential Chromatic Refraction
Authors: Riley W. Clarke, Federica Bianco, James R. A. Davenport, Jeffery Cooke, Sara Webb, Igor Andreoni, Tyler Pritchard, Aaron Roodman
Figure caption: Number of reference stars detected in each frame. Empty circles are preflare, filled circle are after the start of the flare (see Section 4). Between 72 and 94 stars are detected and used as reference in each frame.
Paper: First Temperature Profile of a Stellar Flare Using Differential Chromatic Refraction
Authors: Riley W. Clarke, Federica Bianco, James R. A. Davenport, Jeffery Cooke, Sara Webb, Igor Andreoni, Tyler Pritchard, Aaron Roodman
Figure caption: Top left: flare lightcurve as shown in the top panel of Figure 2. Top right: d∥ as shown in the bottom panel of Figure 2. Bottom: the evolution of temperature (TBB; left) and filling factor (right) from our most simplistic model described in Section 5.4: a blackbody flare on top of a dM SED and no constraints on the filling factor evolution. The peak of the flare is marked in each panel with a vertical line. The uncertainties are derived by bootstrapping over the observable uncertainties 1000 times.
Paper: First Temperature Profile of a Stellar Flare Using Differential Chromatic Refraction
Authors: Riley W. Clarke, Federica Bianco, James R. A. Davenport, Jeffery Cooke, Sara Webb, Igor Andreoni, Tyler Pritchard, Aaron Roodman
Figure caption: Left: change in g magnitude relative to the quiescent stellar magnitude as a function of flare temperature and filling factor. Right: effective wavelength of the model flare spectrum in the g band as a function of flare temperature and filling factor. Each grid consists of 400 x 400 cells, giving a resolution of 170 K in temperature and 0.005% in filling factor.
Paper: First Temperature Profile of a Stellar Flare Using Differential Chromatic Refraction
Authors: Riley W. Clarke, Federica Bianco, James R. A. Davenport, Jeffery Cooke, Sara Webb, Igor Andreoni, Tyler Pritchard, Aaron Roodman
Figure caption: PSF photometry and effective wavelengths measured on the images (gray) compared to the forward-model solutions for each of the three models described in Section 5.6, as well as for both SED models described in Section 5.5.
Paper: Masses, Star Formation Efficiencies, and Dynamical Evolution of 18,000 H II Regions
Authors: Debosmita Pathak, Adam K. Leroy, Ashley. T. Barnes, Todd A. Thompson, Laura A. Lopez, Karin M. Sandstrom, Jiayi Sun, Simon C. O. Glover, Ralf S. Klessen, Eric W. Koch, Kirsten L. Larson, Janice Lee, Sharon Meidt, Patricia Sanchez-Blazquez, Eva Schinnerer, Zein Bazzi, Francesco Belfiore, Médéric Boquien, Ryan Chown, Dario Colombo, Enrico Congiu, Oleg V. Egorov, Cosima Eibensteiner, Sushma Kurapati, Miguel Querejeta, Daniel A. Dale, Timo Kravtsov, Mansi Padave, D. J. Pisano, Erik Rosolowsky, Sumit K. Sarbadhicary, Thomas G. Williams, Remy Indebetouw, Hsi-An Pan, Leonardo Úbeda, Amirnezam Amiri, Frank Bigiel, Guillermo A. Blanc, Kathryn Grasha
Figure caption: Top: summarizing H II region-scale SFEs. Data density contours for the 5th/16th/25th/50th/75th/84th/95th percentile SFE using MIon,S II (dark green), ﹩{M}_{{\rm{Ion}}},{\rm{Str}}\ddot{{\rm{o}}}{\rm{mgren}}﹩ (light green), and ﹩{M}_{{\rm{Mol}}}^{{\rm{init}}}﹩ (purple). The full histogram and medians as before (dashed line) for ﹩{M}_{{\rm{Ion}}},{\rm{Str}}\ddot{{\rm{o}}}{\rm{mgren}}﹩ and ﹩{M}_{{\rm{Mol}}}^{{\rm{init}}}﹩ are included. We also include the medians using ﹩{M}_{{\rm{Mol}}}^{{\rm{init}}}﹩ at 90–60 pc resolution. Middle: from left to right, the fraction of current gas and stars in young stars, the moderate correlation (Spearman ρ = 0.42) and large scatter between MNew and ﹩{\langle {{\rm{\Sigma }}}_{{\rm{Mol}}}\rangle }_{150\,{\rm{pc}}}﹩, and three estimates of MNew/MCloud vs. ﹩{\langle {{\rm{\Sigma }}}_{{\rm{Mol}}}\rangle }_{150\,{\rm{pc}}}﹩. Bottom: from left to right, the fraction of initial gas seen in stars and ionized gas, the fraction of depleted initial molecular gas in stars and ionized gas, the statistical local depletion in molecular gas toward H II regions at our fiducial 150 pc resolution, and finally, the depletion for smaller samples (where available) at 90 pc (purple) and 60 pc (gray) resolution, relative to the dashed black 1:1 line.
Paper: Masses, Star Formation Efficiencies, and Dynamical Evolution of 18,000 H II Regions
Authors: Debosmita Pathak, Adam K. Leroy, Ashley. T. Barnes, Todd A. Thompson, Laura A. Lopez, Karin M. Sandstrom, Jiayi Sun, Simon C. O. Glover, Ralf S. Klessen, Eric W. Koch, Kirsten L. Larson, Janice Lee, Sharon Meidt, Patricia Sanchez-Blazquez, Eva Schinnerer, Zein Bazzi, Francesco Belfiore, Médéric Boquien, Ryan Chown, Dario Colombo, Enrico Congiu, Oleg V. Egorov, Cosima Eibensteiner, Sushma Kurapati, Miguel Querejeta, Daniel A. Dale, Timo Kravtsov, Mansi Padave, D. J. Pisano, Erik Rosolowsky, Sumit K. Sarbadhicary, Thomas G. Williams, Remy Indebetouw, Hsi-An Pan, Leonardo Úbeda, Amirnezam Amiri, Frank Bigiel, Guillermo A. Blanc, Kathryn Grasha
Figure caption: Variation in the different mass components relative to the young cluster mass MNew for the full sample of H II regions, binned in LHαcorr (top left) and Rcirc (top right) and summarized as histograms (bottom left). MIon, S II/MNew (dark green), ﹩{M}_{{\rm{Ion}}},{\rm{Str}}\ddot{{\rm{o}}}{\rm{mgren}}/{M}_{{\rm{New}}}﹩ (light green), MOld/MNew (red), ﹩{M}_{{\rm{Mol}}}^{{\rm{init}}}/{M}_{{\rm{New}}}﹩ (dashed pink), and ﹩{M}_{{\rm{Atom}}}^{{\rm{init}}}/{M}_{{\rm{New}}}﹩ (dashed gray) are included for comparison. The dashed line indicates where a mass component is equal to MNew. The bottom right panel includes the distribution of the measured Rcirc (black), the estimated radius at which ﹩{M}_{{\rm{New}}}={M}_{{\rm{Mol}}}^{{\rm{init}}}﹩ (dashed pink), and the radius where MNew = MOld (red).
Paper: Masses, Star Formation Efficiencies, and Dynamical Evolution of 18,000 H II Regions
Authors: Debosmita Pathak, Adam K. Leroy, Ashley. T. Barnes, Todd A. Thompson, Laura A. Lopez, Karin M. Sandstrom, Jiayi Sun, Simon C. O. Glover, Ralf S. Klessen, Eric W. Koch, Kirsten L. Larson, Janice Lee, Sharon Meidt, Patricia Sanchez-Blazquez, Eva Schinnerer, Zein Bazzi, Francesco Belfiore, Médéric Boquien, Ryan Chown, Dario Colombo, Enrico Congiu, Oleg V. Egorov, Cosima Eibensteiner, Sushma Kurapati, Miguel Querejeta, Daniel A. Dale, Timo Kravtsov, Mansi Padave, D. J. Pisano, Erik Rosolowsky, Sumit K. Sarbadhicary, Thomas G. Williams, Remy Indebetouw, Hsi-An Pan, Leonardo Úbeda, Amirnezam Amiri, Frank Bigiel, Guillermo A. Blanc, Kathryn Grasha
Figure caption: The distribution of masses associated with our sample of ∼18,000 H II regions (solid violins) and the subsample of ∼4000 regions where we can calculate [S II] densities (dashed violins), including contributions from young clusters (MNew, in blue; see Section 2.1.1), ionized gas mass (MIon, Strömgren in light green and [S II]-emitting clump in dark green; see Section 2.1.2), old stellar mass (MOld, in red; see Section 2.1.3), initial molecular gas mass (﹩{M}_{{\rm{Mol}}}^{{\rm{init}}}﹩, in pink; Section 2.2.1), and initial atomic gas mass (﹩{M}_{{\rm{Atom}}}^{{\rm{init}}}﹩, in gray; Section 2.2.2) as violin plots with the median and 16th–84th range included. Below we show how MNew, MIon, MOld, and ﹩{M}_{{\rm{Mol}}}^{{\rm{init}}}﹩ scale with physical size (Rcirc). Contours show the 16th/25th/50th/75th/84th percentiles, and we include ﹩\mathrm{log}\unicode{8210}\mathrm{log}﹩ fits (bold lines, repeated as dashed lines in each panel) to the binned medians (hexagons) and the 16th–84th percentile scatter in each bin (error bars on hexagons). Attached to each scatter plot are stacked histograms of region masses for galaxy centers (orange) and disks (blue) (following M. Querejeta et al. 2021), the sample median (dashed line), and the 16th–84th percentile range (hatches).
Paper: Radiation Forces and Trajectory of Hayabusa2♯ Target 1998 KY26
Authors: Davide Farnocchia, David Vokrouhlický, Toni Santana-Ros, Przemysław Bartczak, Marco Micheli, Steven R. Chesley
Figure caption: Ephemeris uncertainty on 2031 July 15 projected along the ICRF X, Y, and Z components and the orbital radial (R), transverse (T), and normal (N) components. The error ellipses correspond to the 3σ level for five different solutions: “Fixed Pole” solution as in Table 2 (blue), “Estimated Pole” solution as in Table 2 (red), a solution with gravity and Yarkovsky perturbations based on data since 2002 (green), and a solution with gravity and nongravitational accelerations modeled using A1, A2, and A3 also based on data since 2002 (yellow). The magenta ellipse is derived from 1000 statistically drawn Monte Carlo (MC) samples (black dots) based on the posterior distribution obtained in Section 4. The origin corresponds to the “Fixed Pole” solution. Axes use different scales.
Paper: Radiation Forces and Trajectory of Hayabusa2♯ Target 1998 KY26
Authors: Davide Farnocchia, David Vokrouhlický, Toni Santana-Ros, Przemysław Bartczak, Marco Micheli, Steven R. Chesley
Figure caption: Left panel: distribution of 1998 KY26’s bulk density ρ (in g cm−3, abscissa) and surface thermal inertia Γ (in SI units, ordinate) from the orbit determination. The horizontal and vertical dashed gray lines are median values of the respective parameter. Middle and right panels: cumulative distribution of ρ and Γ, with the dashed horizontal line helping to identify the median value. The gray rectangles in the middle panel shows bulk densities inferred for Xe-type asteroids (light gray) and enstatite chondrites (dark gray); dashed vertical lines indicate the mean value (data from B. Carry 2012; see also M. Fenucci et al. 2024). The light gray region in the right panel corresponds to the thermal inertia determined from the smallest E-type asteroid (33342) 1998 WT24 (see M. Delbo et al. 2015).
Paper: Radiation Forces and Trajectory of Hayabusa2♯ Target 1998 KY26
Authors: Davide Farnocchia, David Vokrouhlický, Toni Santana-Ros, Przemysław Bartczak, Marco Micheli, Steven R. Chesley
Figure caption: Raster scan for the 1998 KY26 pole orientation. For each grid point, we computed the best-fit orbital solution by assuming the nominal albedo, absorptivity, and axis ratio from T. Santana-Ros et al. (2025). The orbital parameters, area-to-mass ratio A/M, and λ0 were estimated from the fit. The contour curves correspond to the 1σ and 3σ levels around the minimum, which is achieved for (R.A., decl.) = (56, −39) deg with a weighted rms of 0.43. The black dots correspond to nonphysical solutions with a negative area-to-mass ratio, a negative λ0, or λ0 > 100. The crosses indicate the four pole solutions from T. Santana-Ros et al. (2025).
Paper: Escape Fractions from Unattenuated Lyα Emitters around Luminous z > 6 Quasars
Authors: Minghao Yue, Anna-Christina Eilers, Jorryt Matthee, Rohan P. Naidu, Rongmon Bordoloi, Frederick B. Davies, Joseph F. Hennawi, Daichi Kashino, Ruari Mackenzie, Robert A. Simcoe
Figure caption: Top panels: redshift and Lyα luminosity distribution of galaxies in the J0100 field and the J1148 field, in the left and right panel, respectively. The red shaded region marks the quasar’s vicinity ∣Δv∣ < 2500 km s−1. Middle panels: similar to the top panel, but for the redshift and Lyα EW distribution. Bottom: the fraction of galaxies with ﹩{\rm{EW}\,}_{\rm{Ly}\alpha }^{\,\rm{rest}}﹩ > 10 Å. This fraction is estimated by fitting the galaxy ﹩{\rm{EW}\,}_{\rm{Ly}\alpha }^{\,\rm{rest}}﹩ with a lognormal distribution (see text for details). We also include the NIRSpec-observed galaxies at 6 < z < 7 from Y. Kageura et al. (2025) for comparison. In both quasar fields, galaxies in the quasar’s vicinity show higher LAE fractions than foreground and background galaxies and the general galaxy population. This comparison indicates that the IGM around luminous quasars has high transmission to Lyα photons.
Paper: Escape Fractions from Unattenuated Lyα Emitters around Luminous z > 6 Quasars
Authors: Minghao Yue, Anna-Christina Eilers, Jorryt Matthee, Rohan P. Naidu, Rongmon Bordoloi, Frederick B. Davies, Joseph F. Hennawi, Daichi Kashino, Ruari Mackenzie, Robert A. Simcoe
Figure caption: The stacked Lyα line profile for galaxies near quasars (left), foreground galaxies (middle), and background galaxies (right). The text in each panel marks the number of galaxies and the average redshift for the stacked spectra. The dashed lines mark the systemic Lyα wavelength and the level of zero flux. Galaxies near quasars show significant flux bluer than the systemic Lyα wavelength, indicating low IGM opacity around quasars. In contrast, the foreground and background galaxies do not have significant flux bluer than the Lyα wavelength.
Paper: Escape Fractions from Unattenuated Lyα Emitters around Luminous z > 6 Quasars
Authors: Minghao Yue, Anna-Christina Eilers, Jorryt Matthee, Rohan P. Naidu, Rongmon Bordoloi, Frederick B. Davies, Joseph F. Hennawi, Daichi Kashino, Ruari Mackenzie, Robert A. Simcoe
Figure caption: The two quasar fields targeted by this work, J0100+2802 (left) and J1148+5251 (right). We compose the red, green, and blue images using the NIRCam F115W, F200W, and F356W images from the EIGER project (e.g., D. Kashino et al. 2023). The quasars are at the field centers, marked by the squares. The circles mark the galaxy sample of this study, with the colors representing their systemic redshifts. There are 28 targets and 22 targets in the J0100+2802 and J1148+5251 fields, respectively.
Paper: Escape Fractions from Unattenuated Lyα Emitters around Luminous z > 6 Quasars
Authors: Minghao Yue, Anna-Christina Eilers, Jorryt Matthee, Rohan P. Naidu, Rongmon Bordoloi, Frederick B. Davies, Joseph F. Hennawi, Daichi Kashino, Ruari Mackenzie, Robert A. Simcoe
Figure caption: The stacked Lyα line for C IV emitters at the quasars’ foreground and background, showing significant flux bluer than the systemic Lyα wavelength. This result indicates that C IV emitters can produce their own ionized bubbles.
Paper: Black Hole Collisions with Thin Accretion Disks: OJ 287 and Small Mass Ratio Supermassive Black Hole Binary Candidates
Authors: Sean M. Ressler, Luciano Combi, Bart Ripperda, Xinyu Li
Figure caption: Comparison between our fiducial q = 0.1, H/r = 0.1 simulation (solid gold line) and our restarted, q = 0.1, H/r = 0.03 simulation (blue dashed line). Top: volume-integrated cooling rate, Lcool, vs. time. Bottom: comoving frame Maxwell stress, αM, vs. radius just before the secondary is introduced. Despite the thinner primary disk, the impacts from the secondary in the H/r = 0.03 simulation are relatively much less powerful than in the H/r = 0.1 simulation, where there is a clear peak in Lcool that stands out from quiescence. This is because of the much higher (by a factor of ≳100) αM in the H/r = 0.03 simulation caused by the rapid compression of the magnetic field and reduction in pressure. This makes the quiescent disk heating relatively stronger than in the H/r = 0.1 simulation. While this highlights the importance of the accretion state in modeling OJ 287–like systems, we caution in the main text that this state may be artificial.
Paper: Black Hole Collisions with Thin Accretion Disks: OJ 287 and Small Mass Ratio Supermassive Black Hole Binary Candidates
Authors: Sean M. Ressler, Luciano Combi, Bart Ripperda, Xinyu Li
Figure caption: Top: volume-integrated cooling rate vs. time during the first impact of the secondary black hole with the primary accretion disk for different forms of the cooling function. Bottom: integrated cooling rate for a cooling function 10 times larger than our default cooling function for the three values of q used in the main text. These plots show that the default cooling function produces an Lcool that is close to the saturated value representing the “true” heating rate induced by the secondary impact and that the dependence of Lcool on q is not sensitive to the cooling function (compare with Figure 4).
Paper: Black Hole Collisions with Thin Accretion Disks: OJ 287 and Small Mass Ratio Supermassive Black Hole Binary Candidates
Authors: Sean M. Ressler, Luciano Combi, Bart Ripperda, Xinyu Li
Figure caption: Top: heating time (or disk crossing time), theat = H/vorbit (red circles), for each secondary impact and cooling-function-weighted volume average of the cooling time, tcool, vs. time (solid blue line). Bottom: volume-integrated cooling rate, Lcool, vs. time (solid purple), broken up into the contribution by the secondary cooling function (within qrorbit of the secondary; dotted blue line) and primary cooling function (everywhere else; dashed pink line). During impact events, the cooling function is typically dominated by the secondary contribution and the associated cooling time is always small compared with the heating/disk crossing time. This means that the integrated cooling rate can accurately measure the intrinsic heating rate induced by the secondary impacts.
Paper: A 50 minute Coronal Kink Oscillation and Its Possible Photospheric Counterpart
Authors: Sihui Zhong, Valery M. Nakariakov, Dmitrii Y. Kolotkov
Figure caption: Periodicity analysis of the oscillations in the loop of interest. From top to bottom, each row is for oscillations in S17, S26, and S33 (blue curves in Figures 2(b)–(d)) and the selected time interval [13:55 UT, 14:58 UT] in S33. First column: original signals (black) with their trend (blue) in the upper subpanel and detrended signals (red) in the bottom subpanel. The relative variation of the signals is linearly magnified by a factor of 8. From the second to the fourth column are the Fourier power spectrum with a 95% confidence level (red line), EMD energy spectrum with a 95% confidence interval (red lines), and Wavelet spectrum with a 95% confidence level (black contour), respectively. In panel (i), the vertical lines indicate the time interval selected for further detection of shorter periodicity (5 minutes) shown in panels (m)–(p). In panels (b)–(n), the blue lines are the best-fitting power-law functions. In panels (c)–(o), the vertical lines indicate the threshold of reliable period estimation, the blue lines are the mean energy, and gray horizontal lines indicate error bars. In panels (d)–(p), the color bars indicate the normalized spectral power, the blue curves in the right subpanels are the global normalized wavelet power as a function of period, and the red dotted curves indicate the 95% confidence levels. Here, “Mag.,” “E,” and “a.u.” stand for power magnitude, EMD modal energy, and arbitrary units, respectively.
Paper: A 50 minute Coronal Kink Oscillation and Its Possible Photospheric Counterpart
Authors: Sihui Zhong, Valery M. Nakariakov, Dmitrii Y. Kolotkov
Figure caption: Kink oscillations in the analyzed loop bundle. (a) AIA 171 Å image showing the loop ensemble marked by the dotted curve. White slits across the loop are used to make time–distance maps that reveal the oscillatory signals. The white box locates the possible negative footpoint of the oscillating loop. (b)–(d) Representative time–distance maps exhibiting the decayless kink oscillations. The data are magnified by a factor (magk) of 8. The blue curves are oscillation signals extracted by the Gaussian fitting of the transverse intensity profiles.