adsabs/AstroCLIMB huggingface dataset:
Paper: What Do Halo CMEs Tell Us about Solar Cycle 25?
Authors: Nat Gopalswamy, Grzegorz Michalek, Seiji Yashiro, Pertti Mäkelä, Sachiko Akiyama, Hong Xie
Figure caption: (a) The number of HCMEs summed over Carrington rotation (CR) periods plotted as a function of time since the beginning of 1996. The 13 month smoothed monthly SSN is shown in gray for reference. The rise phases of SCs 23, 24, and 25 are distinguished by the red, blue, and green segments of the plot. (b) Scatterplot between CME daily rate averaged over CR periods and the sunspot number (v2) for the rise phase of three SCs: 23 (red), 24 (blue), and 25 (green). (c) Scatterplot between the SSN and HCME occurrence rate (per CR). The number of data points in SC 23 is smaller because we dropped six CRs that had < 50% duty cycle due to SOHO data gap. All the correlation coefficients in the plots exceed the Pearson’s critical coefficients: for 35 and 41 samples are 0.53 and 0.50, respectively, with the chance-coincidence probability < 5 × 10−4.
Paper: What Do Halo CMEs Tell Us about Solar Cycle 25?
Authors: Nat Gopalswamy, Grzegorz Michalek, Seiji Yashiro, Pertti Mäkelä, Sachiko Akiyama, Hong Xie
Figure caption: The heights at which a limb CME becomes a halo (halo heights) during the rise phase of each cycle (a)–(c). The top panels show the halo heights measured using the natural cadence of LASCO observations. The bottom panels show halo heights obtained by reducing the cadence of LASCO observations in cycles 24 and 25 to match that in cycle 23. The number of limb halos is small, so the statistics are poor. The average speeds of limb halos in SCs 23, 24, and 25 are marked on the plots.
Paper: What Do Halo CMEs Tell Us about Solar Cycle 25?
Authors: Nat Gopalswamy, Grzegorz Michalek, Seiji Yashiro, Pertti Mäkelä, Sachiko Akiyama, Hong Xie
Figure caption: The solar source locations of HCMEs during the rise phase of the three solar cycles: heliographic coordinates (not corrected for B0 angle), latitude variation with time, source longitude, and source latitude for each cycle. The hemispheric mean and median values of the source longitudes and latitudes are shown on the plots. Backside HCMEs are excluded because their source locations are unknown in cycle 23.
Paper: What Do Halo CMEs Tell Us about Solar Cycle 25?
Authors: Nat Gopalswamy, Grzegorz Michalek, Seiji Yashiro, Pertti Mäkelä, Sachiko Akiyama, Hong Xie
Figure caption: Sky-plane (top panels) and space speed (bottom panels) of rise-phase HCMEs of SCs 23, 24, and 25. The space speeds are obtained by a simple cone-model correction. The number of HCMEs (n) in each plot and the average speeds (with standard deviations σ) are marked on the plots.
Paper: SN 2023ixf in Messier 101: A Variable Red Supergiant as the Progenitor Candidate to a Type II Supernova
Authors: Charles D. Kilpatrick, Ryan J. Foley, Wynn V. Jacobson-Galán, Anthony L. Piro, Stephen J. Smartt, Maria R. Drout, Alexander Gagliano, Christa Gall, Jens Hjorth, David O. Jones, Kaisey S. Mandel, Raffaella Margutti, Enrico Ramirez-Ruiz, Conor L. Ransome, V. Ashley Villar, David A. Coulter, Hua Gao, David Jacob Matthews, Kirsty Taggart, Yossef Zenati
Figure caption: Left: a 15.″4 × 13.″1 cutout of HST/ACS imaging toward M101 in F435W (blue), F555W (green), and F814W (red). We show the approximate explosion site of SN 2023ixf as a 1″ diameter white circle. Right panels: panels showing preexplosion F658N, F675W, F658N, Gemini/NIRI K band, and Spitzer Channel 1 (3.6 μm) and 2 (4.5 μm) imaging where we detect a counterpart at the site of SN 2023ixf. The HST and K-band images are on the same scale, while the Spitzer 3.6 and 4.5 μm images show a zoomed-out scale to highlight the location of the counterpart. We show red circles corresponding to the locations of Sources A and B, close to the site of SN 2023ixf as discussed in Section 2.1. We also note the position of the SN (with the approximate systematic uncertainty 0.″04) with a green circle in the F814W panel (see Section 3.1).
Paper: SN 2023ixf in Messier 101: A Variable Red Supergiant as the Progenitor Candidate to a Type II Supernova
Authors: Charles D. Kilpatrick, Ryan J. Foley, Wynn V. Jacobson-Galán, Anthony L. Piro, Stephen J. Smartt, Maria R. Drout, Alexander Gagliano, Christa Gall, Jens Hjorth, David O. Jones, Kaisey S. Mandel, Raffaella Margutti, Enrico Ramirez-Ruiz, Conor L. Ransome, V. Ashley Villar, David A. Coulter, Hua Gao, David Jacob Matthews, Kirsty Taggart, Yossef Zenati
Figure caption: A part of HST/ACS F814W imaging (top) of M101 from 2002 November 16 compared with a gri image from Gemini-North/GMOS (bottom) of the same field from 2023 June showing the location of SN 2023ixf. We identify a single counterpart at the position of SN 2023ixf in the ACS image, discussed in detail in Section 3.1.
Paper: SN 2023ixf in Messier 101: A Variable Red Supergiant as the Progenitor Candidate to a Type II Supernova
Authors: Charles D. Kilpatrick, Ryan J. Foley, Wynn V. Jacobson-Galán, Anthony L. Piro, Stephen J. Smartt, Maria R. Drout, Alexander Gagliano, Christa Gall, Jens Hjorth, David O. Jones, Kaisey S. Mandel, Raffaella Margutti, Enrico Ramirez-Ruiz, Conor L. Ransome, V. Ashley Villar, David A. Coulter, Hua Gao, David Jacob Matthews, Kirsty Taggart, Yossef Zenati
Figure caption: Light curve of the preexplosion counterpart to SN 2023ixf from Spitzer/IRAC Channel 1 and 2 observations from ∼11.3–3.6 yr prior to discovery of the SN. We note that both channels exhibit ∼16 μJy peak-to-peak variability during this time frame, with a significant peaks spaced ∼2.8 yr apart. The flux-weighted average in Channels 1 and 2 are shown as blue and red dashed lines, respectively, with their values given in Table 2. For comparison, we show the 3.9 μm light curve of Betelgeuse binned every 2 weeks from Taniguchi et al. (2022), scaled to the average flux of the SN 2023ixf counterpart at ∼23 μJy and shifted in time by 4 yr to overlap with our light curve.
Paper: SN 2023ixf in Messier 101: A Variable Red Supergiant as the Progenitor Candidate to a Type II Supernova
Authors: Charles D. Kilpatrick, Ryan J. Foley, Wynn V. Jacobson-Galán, Anthony L. Piro, Stephen J. Smartt, Maria R. Drout, Alexander Gagliano, Christa Gall, Jens Hjorth, David O. Jones, Kaisey S. Mandel, Raffaella Margutti, Enrico Ramirez-Ruiz, Conor L. Ransome, V. Ashley Villar, David A. Coulter, Hua Gao, David Jacob Matthews, Kirsty Taggart, Yossef Zenati
Figure caption: SED of the preexplosion counterpart to SN 2023ixf, with red circles denoting detections and pink circles denoting upper limits (described in Section 3.2). We fit the HST, Spitzer, and ground-based photometry with a 1640 K blackbody (green), which describes the data but is much cooler than typical effective temperatures for the RSG progenitor stars of SNe II (e.g., Smartt 2015). We also show an RSG SED for a reddened RSG supergiant with a T eff = 3920 K photosphere inside of a 880 K dust shell exhibiting mid-IR excess (orange; from Kilpatrick & Foley 2018) as well as the intrinsic stellar SED without reddening. The individual components of the overall reddened RSG SED (reddened star, dust shell, and unreddened star) are shown in blue, red, and purple, respectively. The SED of the preexplosion counterpart to SN 2023ixf is available as data behind the figure.(The data used to create this figure are available.)
Paper: SN 2023ixf in Messier 101: A Variable Red Supergiant as the Progenitor Candidate to a Type II Supernova
Authors: Charles D. Kilpatrick, Ryan J. Foley, Wynn V. Jacobson-Galán, Anthony L. Piro, Stephen J. Smartt, Maria R. Drout, Alexander Gagliano, Christa Gall, Jens Hjorth, David O. Jones, Kaisey S. Mandel, Raffaella Margutti, Enrico Ramirez-Ruiz, Conor L. Ransome, V. Ashley Villar, David A. Coulter, Hua Gao, David Jacob Matthews, Kirsty Taggart, Yossef Zenati
Figure caption: A Hertzsprung–Russell diagram zoomed in on the RSG branch. The location of the SN 2023ixf progenitor candidate inferred from our RSG spectral model (Section 3.2) is shown as a red star. For context, we show the locations of other SN II progenitor stars from Smartt (2015) as red squares, the progenitor stars of the SNe IIb 1993J (Aldering et al. 1994), 2011dh (Maund et al. 2011), and 2013df (Van Dyk et al. 2014) as green circles, and the progenitor candidate of the SN Ib 2019yvr (Kilpatrick et al. 2021) as a blue diamond. The black lines are single-star evolutionary tracks from MIST (Choi et al. 2016) as described in Section 3.2.
Paper: A Large Population of Faint 8 < z < 16 Galaxies Found in the First JWST NIRCam Observations of the NGDEEP Survey
Authors: Duncan Austin, Nathan Adams, Christopher J. Conselice, Thomas Harvey, Katherine Ormerod, James Trussler, Qiong Li, Leonardo Ferreira, Pratika Dayal, Ignas Juodžbalis
Figure caption: Corrected LePhare stellar masses as a function of redshift (“Z_BEST”) for our NGDEEP candidates at z > 8.5. We find an abundance of low-mass galaxies, with ∼50% of our sample having LePhare masses M * < 108 M ⊙. Our NGD-z9a is seen with M ⋆ ≃ 1010  M ⊙ and is comparable to the large masses found by Labbé et al. (2023) and Tacchella et al. (2022). LePhare does not perform Bayesian SED fitting; therefore, we do not include stellar mass errors here, although we note the typical 0.2−0.3 dex mass errors from our Bagpipes fits. Previous results from JWST are shown as stars (Curtis-Lake et al. 2023; Arrabal Haro et al. 2023; Fujimoto et al. 2023; Nakajima et al. 2023; Tang et al. 2023, spectroscopy) and diamonds (Naidu et al. 2022b; Bouwens et al. 2022; Labbé et al. 2023; Leethochawalit et al. 2022; Atek et al. 2023, photometry). We also show pre-JWST data from the HST CANDELS fields by Tacchella et al. (2022) and the stacked sample of Stefanon et al. (2023) from GOODS with mass calculated assuming a nonparametric SFH. The singular HST-selected source at z > 8.5 (NGD-z9d) is shown as a beige diamond.
Paper: A Large Population of Faint 8 < z < 16 Galaxies Found in the First JWST NIRCam Observations of the NGDEEP Survey
Authors: Duncan Austin, Nathan Adams, Christopher J. Conselice, Thomas Harvey, Katherine Ormerod, James Trussler, Qiong Li, Leonardo Ferreira, Pratika Dayal, Ignas Juodžbalis
Figure caption: Ultraviolet continuum spectral slope (β) as a function of absolute UV magnitude (M UV) at z > 8.5 only. JWST galaxies are plotted as stars (spectroscopically confirmed; Curtis-Lake et al. 2023) and diamonds (photometric candidates; Naidu et al. 2022b; Castellano et al. 2022; Atek et al. 2023; Cullen et al. 2023; Whitler et al. 2023). We also show the bright HST CANDELS and stacked GOODS galaxies by Stefanon et al. (2023) and Tacchella et al. (2022) as brown and pink circles, respectively. We note here that the faint Cullen et al. (2023) sources have larger σ  β , as they take into account redshift uncertainties that increase the errors by a factor 1.13. There is good agreement between the majority of our results and the previous literature, except for the extremely blue NGD-z11c and NGD-z9a, which are our intrinsically brightest and reddest candidates. The singular HST-selected source at z > 8.5 (NGD-z9d) is shown as a beige diamond.
Paper: A Large Population of Faint 8 < z < 16 Galaxies Found in the First JWST NIRCam Observations of the NGDEEP Survey
Authors: Duncan Austin, Nathan Adams, Christopher J. Conselice, Thomas Harvey, Katherine Ormerod, James Trussler, Qiong Li, Leonardo Ferreira, Pratika Dayal, Ignas Juodžbalis
Figure caption: Absolute UV luminosity plotted against LePhare redshift (“Z_BEST”) for z > 8.5. JWST galaxies are plotted as stars (spectroscopically confirmed; Curtis-Lake et al. 2023; Cameron et al. 2023; Fujimoto et al. 2023; Nakajima et al. 2023; Tang et al. 2023) and diamonds (photometric candidates; Finkelstein et al. 2023; Naidu et al. 2022b; Castellano et al. 2022; Donnan et al. 2023; Harikane et al. 2022; Atek et al. 2023; Leethochawalit et al. 2023; Whitler et al. 2023). HST CANDELS sources and stacked GOODS results by Tacchella et al. (2022) and Stefanon et al. (2023), respectively, are shown as circles. The singular HST-matched source at z > 8.5 (NGD-z9d) is shown as a beige diamond. Our NGD-z15a is unique in that it is the faintest and least massive object at z > 13.5 seen in JWST data.
Paper: A Large Population of Faint 8 < z < 16 Galaxies Found in the First JWST NIRCam Observations of the NGDEEP Survey
Authors: Duncan Austin, Nathan Adams, Christopher J. Conselice, Thomas Harvey, Katherine Ormerod, James Trussler, Qiong Li, Leonardo Ferreira, Pratika Dayal, Ignas Juodžbalis
Figure caption: A comparison of our z > 8.5 NGDEEP completeness-corrected cumulative number counts against those predicted by simulations covering the same sky area to limiting magnitude m = 29.5. We find an underabundance of 8.5 < z < 10.5 galaxies owing to our requirement of an F115W nondetection, which would be remedied by including bluer HST data. Our z = 15.6 galaxy stands out in the z > 10.5 regime, although the large ∼50% cosmic variance (Driver & Robotham 2010) could help explain this discrepancy.
Paper: A Large Population of Faint 8 < z < 16 Galaxies Found in the First JWST NIRCam Observations of the NGDEEP Survey
Authors: Duncan Austin, Nathan Adams, Christopher J. Conselice, Thomas Harvey, Katherine Ormerod, James Trussler, Qiong Li, Leonardo Ferreira, Pratika Dayal, Ignas Juodžbalis
Figure caption: Source counts within the NGDEEP F277W filter in comparison to a selection of other public imaging reduced following the same pipeline. These include SMACS 0723, GLASS, and the deepest pointing (P9) of CEERS. We observe the expected result that NGDEEP is around 0.5 mag deeper than GLASS, which has 5σ depth of 29.15 in F277W. See Adams et al. (2023b) and C. Conselice et al. (2023, in preparation) for a full discussion of the depths of various public NIRCam data sets, including SMACS 0723, GLASS, and CEERS. Displayed errors are purely Poissonian, and we do not consider the contribution of cosmic variance here.
Paper: A Large Population of Faint 8 < z < 16 Galaxies Found in the First JWST NIRCam Observations of the NGDEEP Survey
Authors: Duncan Austin, Nathan Adams, Christopher J. Conselice, Thomas Harvey, Katherine Ormerod, James Trussler, Qiong Li, Leonardo Ferreira, Pratika Dayal, Ignas Juodžbalis
Figure caption: Comparison of our non-aperture-corrected F277W SExtractor magnitudes (in 0.″32-diameter apertures) against LePhare redshift (“Z_BEST”) showing the large number of faintly observed candidates we obtain. Literature results from CEERS (Finkelstein et al. 2023; Donnan et al. 2023; Arrabal Haro et al. 2023; Fujimoto et al. 2023), GLASS (Naidu et al. 2022b), and the semi-overlapping MIRI-DS (Pérez-González et al. 2023) are shown, where spectroscopic results are shown as stars and photometric results are shown as diamonds. The singular HST-selected source at z > 8.5 (NGD-z9d) is shown as a beige diamond.
Paper: A Large Population of Faint 8 < z < 16 Galaxies Found in the First JWST NIRCam Observations of the NGDEEP Survey
Authors: Duncan Austin, Nathan Adams, Christopher J. Conselice, Thomas Harvey, Katherine Ormerod, James Trussler, Qiong Li, Leonardo Ferreira, Pratika Dayal, Ignas Juodžbalis
Figure caption: Sérsic profile fit for NGD-z10c. The left panel shows the source, the middle panel shows the two-dimensional Sérsic model, and the right panel shows the residual image.
Paper: Kinetic Features of Alpha Particles in a Pestchek-like Magnetic Reconnection Event in the Solar Wind Observed by Solar Orbiter
Authors: Die Duan, Jiansen He, Xingyu Zhu, Rui Zhuo, Ziqi Wu, Georgios Nicolaou, Jia Huang, Daniel Verscharen, Liu Yang, Christopher J. Owen, Andrey Fedorov, Philippe Louarn, Timothy S. Horbury
Figure caption: Overview of the reconnection event. (a) Magnetic field and solar wind speed. (b)–(c) Magnetic field and proton bulk velocity in RTN coordinates. (d)–(e) Magnetic field and proton bulk velocity in LMN coordinates. (f) Proton density, parallel and perpendicular temperature. (g) Differential energy flux of protons and alpha particles. The white line marks the energy with maximum proton flux, and the black line marks the energy with maximum alpha particle flux; the red line marks the energy per charge E  m  with minimum flux between the distributions of protons and alpha particles. (h) Pitch-angle distribution of suprathermal electrons (70–163 eV). The green dashed lines mark the two rotational discontinuities, the purple dashed lines mark the two slow shocks, and red dashed lines mark the separatrices of the reconnection exhaust region.
Paper: Kinetic Features of Alpha Particles in a Pestchek-like Magnetic Reconnection Event in the Solar Wind Observed by Solar Orbiter
Authors: Die Duan, Jiansen He, Xingyu Zhu, Rui Zhuo, Ziqi Wu, Georgios Nicolaou, Jia Huang, Daniel Verscharen, Liu Yang, Christopher J. Owen, Andrey Fedorov, Philippe Louarn, Timothy S. Horbury
Figure caption: (a) Magnetic field (blue) and solar wind speed (red). The vertical dashed lines are the same as in Figure 2. (b)–(g) 2D cuts of the ion VDF in the R–T plane at the time stamps as indicated in panel (a). The black lines indicate the magnetic field direction. The length of the black line is the local Alfvén speed in the R–T plane. The starting points of the black lines represent the maximum values of the VDF for both protons and alpha particles. (h) Illustration of this reconnection event in the L–N plane. Black arrows show the direction of the magnetic field. The red arrows represent the direction of the plasma bulk velocity. The purple dashed lines show the position of the SSs, and the green dashed lines represent the RDs. The blue dashed arrow represents the trajectory of Solar Orbiter.
Paper: Kinetic Features of Alpha Particles in a Pestchek-like Magnetic Reconnection Event in the Solar Wind Observed by Solar Orbiter
Authors: Die Duan, Jiansen He, Xingyu Zhu, Rui Zhuo, Ziqi Wu, Georgios Nicolaou, Jia Huang, Daniel Verscharen, Liu Yang, Christopher J. Owen, Andrey Fedorov, Philippe Louarn, Timothy S. Horbury
Figure caption: Parameters of protons and alpha particles during the reconnection event. (a) Magnetic field and solar wind speed. (b) Number densities of protons n  p  (blue) and alpha particles n  α  × 100 (red). (c) Bulk velocity components of protons (blue) and alpha particles (red) along the L direction in LMN coordinates. (d) Parallel (blue) and perpendicular (red) temperatures of the protons. (e) Same as (d) but for the alpha particles. (f) Modified Alfvén wave speed ﹩{v}_{{\rm{A}}}^{{\prime} }﹩ (blue) and slow wave speed ﹩{c}_{\mathrm{sl}}^{{\prime} }﹩ (red) calculated with the temperature anisotropy for θ = 65°. The vertical dashed lines are the same as in Figure 2.
Paper: Kinetic Features of Alpha Particles in a Pestchek-like Magnetic Reconnection Event in the Solar Wind Observed by Solar Orbiter
Authors: Die Duan, Jiansen He, Xingyu Zhu, Rui Zhuo, Ziqi Wu, Georgios Nicolaou, Jia Huang, Daniel Verscharen, Liu Yang, Christopher J. Owen, Andrey Fedorov, Philippe Louarn, Timothy S. Horbury
Figure caption: Time series plots of a crossing of a small transient event on 2020 October 14. (a) Magnetic field and solar wind speed. (b) Proton density and temperature. (c) Differential energy flux of protons and alpha particles. (d) Pitch-angle distribution of superthermal electrons (70–163 eV). (e) The azimuth ϕ  B  and elevation angle θ  B  of the magnetic field. (f)–(g) Magnetic field components and solar wind velocity in RTN coordinates. The yellow-shaded region is the magnetic reconnection event, which is detailed in Figure 2.
Paper: Kinetic Features of Alpha Particles in a Pestchek-like Magnetic Reconnection Event in the Solar Wind Observed by Solar Orbiter
Authors: Die Duan, Jiansen He, Xingyu Zhu, Rui Zhuo, Ziqi Wu, Georgios Nicolaou, Jia Huang, Daniel Verscharen, Liu Yang, Christopher J. Owen, Andrey Fedorov, Philippe Louarn, Timothy S. Horbury
Figure caption: (a) Magnetic field (blue) and ion number density (red) across SS1. The pink square marks the shock, and the gray and orange squares mark the upstream and downstream regions of the shock used in the shock fitting. (b) Same as (a) but for SS2. (c) Walén test result for RD1. V HT is the moving velocity component of the de Hoffman–Teller reference frame in the spacecraft reference frame. (d) Walén test result of RD2.
Paper: Dimming of Continuum Captured in Mrk 841: New Clues on the Nature of the Soft X-Ray Excess
Authors: Missagh Mehdipour, Gerard A. Kriss, Jelle S. Kaastra, Elisa Costantini, Junjie Mao
Figure caption: IR, optical, UV, and X-ray spectra of Mrk 841 from the 2001/historical and 2022 epochs. The data are shown as observed, including all foreground effects. Major changes in shape and flux of the observed SED in 2022 are evident. The underlying intrinsic SEDs are derived and shown in Figure 2.
Paper: Dimming of Continuum Captured in Mrk 841: New Clues on the Nature of the Soft X-Ray Excess
Authors: Missagh Mehdipour, Gerard A. Kriss, Jelle S. Kaastra, Elisa Costantini, Junjie Mao
Figure caption: Top panel: derived intrinsic SED continuum model for the 2001/historical and the 2022 epochs of Mrk 841. Bottom panel: individual components of the SED. The significant changes in the dbb (solid line) and comt (dashed line) components are apparent. The parameters of the continuum components are given in Table 1.
Paper: Early Hard X-Rays from the Nearby Core-collapse Supernova SN 2023ixf
Authors: Brian W. Grefenstette, Murray Brightman, Hannah P. Earnshaw, Fiona A. Harrison, R. Margutti
Figure caption: Left: Digitized Sky Survey image of M101, with the NuSTAR field of view indicated with a black dashed line, the NuSTAR contours indicated in magenta, and the optical measured position of SN 2023ixf indicated with a blue cross. Right: the NuSTAR image, with the source extraction region marked with a solid purple circle, and the nearby background region marked with a dotted–dashed circle.
Paper: Early Hard X-Rays from the Nearby Core-collapse Supernova SN 2023ixf
Authors: Brian W. Grefenstette, Murray Brightman, Hannah P. Earnshaw, Fiona A. Harrison, R. Margutti
Figure caption: (Top) The background-subtracted spectrum for Epoch I (δt ≈  4 days, black) and Epoch II (δt ≈  11 days, red) showing the best-fit model (solid lines) and the Gaussian component (dotted lines) demonstrating the spectral evolution of the source. (Bottom) Residuals to the best-fit model.
Paper: The Role of High-frequency Transverse Oscillations in Coronal Heating
Authors: Daye Lim, Tom Van Doorsselaere, David Berghmans, Richard J. Morton, Vaibhav Pant, Sudip Mandal
Figure caption: Top: the top panels show the distribution of oscillation number per energy flux, n(F), and its power-law fitting (dashed lines). The fitting was only considered for bins with a nonzero amount of cases. A bin size of ﹩\overline{F}=0.1﹩ for the energy flux distribution has been considered. Blue, red, and black colors represent observations from AIA, EUI, and both of them, respectively. The power-law slopes are ﹩{\alpha }_{F,\mathrm{AIA}}={0.94}_{-0.11}^{+0.12}﹩, ﹩{\alpha }_{F,\mathrm{EUI}}={1.00}_{-0.07}^{+0.06}﹩, and ﹩{\alpha }_{F,\mathrm{ALL}}={1.00}_{-0.05}^{+0.05}﹩. The middle and bottom panels show the number of oscillations and mean oscillation frequencies for each energy flux bin. The vertical bars show uncertainties ﹩{\sigma }_{n(F)}=\sqrt{{n}_{{F}_{j}}}﹩. Bottom: the same as in the top panel, but for energies, n(E), with uncertainties ﹩{\sigma }_{n(E)}=\sqrt{{n}_{{E}_{l}}}﹩. A bin size of ﹩\overline{E}=0.1﹩ for the energy distribution has been considered. The power-law slopes are ﹩{\alpha }_{E,\mathrm{AIA}}={0.84}_{-0.10}^{+0.09}﹩, ﹩{\alpha }_{E,\mathrm{EUI}}={0.88}_{-0.10}^{+0.11}﹩, and ﹩{\alpha }_{E,\mathrm{ALL}}={0.93}_{-0.09}^{+0.08}﹩.