adsabs/AstroCLIMB huggingface dataset:
Paper: JWST Imaging of Edge-on Protoplanetary Disks. III. Drastic Morphological Transformation Across the Mid-infrared in Oph163131
Authors: Marion Villenave, Karl R. Stapelfeldt, Gaspard Duchêne, François Ménard, Marshall D. Perrin, Christophe Pinte, Schuyler G. Wolff, Ryo Tazaki, Deborah L. Padgett
Figure caption: Toy model including a very massive and vertically thick inner region, allowing to reproduce a sharp transition in the source appearance beyond 4.4 μm. The fields of view of the panels showing the observations at 7.7, 12.8, and 21 μm are twice as small as those in Figure 2. The compact source appearing at 7.7 μm and longer wavelengths is not centered on the position of the star in the model, but offset by 20 mas or more toward the upper nebulae.
Paper: JWST Imaging of Edge-on Protoplanetary Disks. III. Drastic Morphological Transformation Across the Mid-infrared in Oph163131
Authors: Marion Villenave, Karl R. Stapelfeldt, Gaspard Duchêne, François Ménard, Marshall D. Perrin, Christophe Pinte, Schuyler G. Wolff, Ryo Tazaki, Deborah L. Padgett
Figure caption: JWST three-color composite image of Oph163131; the full field of view spans 10″ × 6″. The 2.0, 4.44, and 7.7 μm images are rendered (using a logarithmic stretch) in the blue, green, and red channels, respectively.
Paper: JWST Imaging of Edge-on Protoplanetary Disks. III. Drastic Morphological Transformation Across the Mid-infrared in Oph163131
Authors: Marion Villenave, Karl R. Stapelfeldt, Gaspard Duchêne, François Ménard, Marshall D. Perrin, Christophe Pinte, Schuyler G. Wolff, Ryo Tazaki, Deborah L. Padgett
Figure caption: Comparison of data and radiative transfer models of the dark lane thickness as a function of wavelength. The models with grains of 1 μm or more present in the upper layers do not show sufficient variation with wavelength to reproduce the observations.
Paper: JWST Imaging of Edge-on Protoplanetary Disks. III. Drastic Morphological Transformation Across the Mid-infrared in Oph163131
Authors: Marion Villenave, Karl R. Stapelfeldt, Gaspard Duchêne, François Ménard, Marshall D. Perrin, Christophe Pinte, Schuyler G. Wolff, Ryo Tazaki, Deborah L. Padgett
Figure caption: Model A from S. G. Wolff et al. (2021), including only one smooth disk region, computed at JWST wavelengths. Contrary to the data, this model does not become dominated by a central source starting at 7.7 μm and does not include extended emission at 7.7 and 12.8 μm. The fields of view of the panels showing the observations at 7.7, 12.8, and 21 μm are twice as small as those in Figure 2.
Paper: Discovery of a Dense Association of Stars in the Vicinity of the Supermassive Black Hole Sgr A*
Authors: S. Elaheh Hosseini, Andreas Eckart, Michal Zajaček, Silke Britzen, Harshitha K. Bhat, Vladimír Karas
Figure caption: Distribution of flying angles of N sources. The zero angle stands for a northward flying angle. The negative angles indicate the NW-ward flying angles up to −35°, whereas the positive angles represent the NE-ward flying angles up to about 40°. There is an indication that the NW-ward sources are members of a denser association of stars, while the rest of the sources might be the foreground/background sources that are still part of the nuclear star cluster.
Paper: Discovery of a Dense Association of Stars in the Vicinity of the Supermassive Black Hole Sgr A*
Authors: S. Elaheh Hosseini, Andreas Eckart, Michal Zajaček, Silke Britzen, Harshitha K. Bhat, Vladimír Karas
Figure caption: The K s-band image from 2005.366 epoch with superimposed proper motions for each N source. Four arrows are shown for each source. The white arrows demonstrate the velocity vectors of each source, including the uncertainty of the velocity angle, whereas the red arrows indicate the uncertainty in the velocity magnitude. The size of the arrows is proportional to the velocity magnitude. The proper-motion vectors are based on Table 3 and the arrows are 1 order of magnitude smaller than proper motions. In total, 42 sources move northward (N sources).
Paper: Discovery of a Dense Association of Stars in the Vicinity of the Supermassive Black Hole Sgr A*
Authors: S. Elaheh Hosseini, Andreas Eckart, Michal Zajaček, Silke Britzen, Harshitha K. Bhat, Vladimír Karas
Figure caption: Distribution of N sources as a function of the projected distance with respect to the geometrical center of the association. The y-axis denotes the number of sources and the x-axis shows the radial distance (in arcseconds) from the geometrical center of N sources. The width of the bins in the histogram is defined by concentric apertures centered at the geometrical center of N sources. In addition, each annulus has an equal area to the central disk, with a radius of 0.″6 for the central disk, and a radial extent of 0.″6–0.″8 for the first annulus, 0.″8–1.″0 for the second annulus, 1.″0–1.″2 for the third annulus, and 1.″2–1.″3 for the fourth annulus.
Paper: Discovery of a Dense Association of Stars in the Vicinity of the Supermassive Black Hole Sgr A*
Authors: S. Elaheh Hosseini, Andreas Eckart, Michal Zajaček, Silke Britzen, Harshitha K. Bhat, Vladimír Karas
Figure caption: The image obtained in the K  s  band from the 2005.366 epoch. Symbol “x” denotes the position of Sgr A*. The encircled N sources at the projected distance of ∼6.″05 with respect to Sgr A* stands for the region of our study.
Paper: Discovery of a Dense Association of Stars in the Vicinity of the Supermassive Black Hole Sgr A*
Authors: S. Elaheh Hosseini, Andreas Eckart, Michal Zajaček, Silke Britzen, Harshitha K. Bhat, Vladimír Karas
Figure caption: The spatial distribution of the NW-ward flying sources. The zero-point of the x-axis is at the geometrical center of the N sources. The spatial distribution is Gaussian-like.
Paper: Discovery of a Dense Association of Stars in the Vicinity of the Supermassive Black Hole Sgr A*
Authors: S. Elaheh Hosseini, Andreas Eckart, Michal Zajaček, Silke Britzen, Harshitha K. Bhat, Vladimír Karas
Figure caption:  HKL two-color diagram. The solid blue line denotes the colors of a one-component blackbody at different temperatures. The red cross represents the uncertainty of the values. The red cross denotes the mean photometric uncertainties.
Paper: Discovery of a Dense Association of Stars in the Vicinity of the Supermassive Black Hole Sgr A*
Authors: S. Elaheh Hosseini, Andreas Eckart, Michal Zajaček, Silke Britzen, Harshitha K. Bhat, Vladimír Karas
Figure caption: The spatial distribution of the NE-ward flying sources. The zero-point of the x-axis is at the geometrical center of the N sources. The spatial distribution is flat within the uncertainties.
Paper: Discovery of a Dense Association of Stars in the Vicinity of the Supermassive Black Hole Sgr A*
Authors: S. Elaheh Hosseini, Andreas Eckart, Michal Zajaček, Silke Britzen, Harshitha K. Bhat, Vladimír Karas
Figure caption: The K  s -band image from the 2005.366 epoch. The sources are labeled from N1/IRS 1W to N42. The figure is a zoom-in of the encircled N sources’ region in Figure 1, which is located ∼6.″05 NE of Sgr A*.
Paper: Discovery of a Dense Association of Stars in the Vicinity of the Supermassive Black Hole Sgr A*
Authors: S. Elaheh Hosseini, Andreas Eckart, Michal Zajaček, Silke Britzen, Harshitha K. Bhat, Vladimír Karas
Figure caption: In this vector-point diagram we denote the spatial distribution of velocities. The position of N1/IRS 1W is depicted with a black arrow.
Paper: Discovering Subsolar Metallicity Brown Dwarf Candidates in the Small Magellanic Cloud
Authors: Peter Zeidler, Elena Sabbi, Antonella Nota, Elena Manjavacas, Olivia C. Jones, Camilla Pacifici
Figure caption: The F150W−F335M vs. F150W CMD of the cluster region (left) and CF (right). The red arrow indicates the reddening vector for A V = 0.25 mag, while the orange arrow indicates an assumed A V = 1.0 mag. The ZAMS is represented as a green line, and we show the 2 Myr MESA isochrones in blue using an LMC metallicity with a low-mass limit of 0.01 M ⊙. The dashed blue line shows the BT-Settl BD isochrone, which includes the BD regime. The yellow lines represent the limits used to identify the lower-mass PMS population (shaded in red), the cYSO region (shaded in green), and the region mostly affected by background galaxies (shaded in blue). The red diamonds are those objects in the CF that are classified as PMS after applying all selection criteria.
Paper: Discovering Subsolar Metallicity Brown Dwarf Candidates in the Small Magellanic Cloud
Authors: Peter Zeidler, Elena Sabbi, Antonella Nota, Elena Manjavacas, Olivia C. Jones, Camilla Pacifici
Figure caption: NGC 602 observed with NIRCam. This image highlights the cluster stars, the young YSOs embedded in the surrounding gas and dust ridges, as well as the gas and dust itself, while also showing the significant contamination by background galaxies and SMC field stars. This image is a composite of the F115W+F140M+F150W (blue), F210M (cyan), F277W (green), F335M (yellow), F356W (orange), and F480M+MIRI-F1000W (red) filters. While the wideband filters show the stellar and galaxy continua, the F335M highlights the 3.3 μm PAH emission. This image is zoomed in on the star cluster. The full data (see Figure 5) cover an area of 3 × 5.8 arcmin2, of which ∼2/3 is occupied by NGC 602 and its surrounding H II region. North is up and east to the left.
Paper: Discovering Subsolar Metallicity Brown Dwarf Candidates in the Small Magellanic Cloud
Authors: Peter Zeidler, Elena Sabbi, Antonella Nota, Elena Manjavacas, Olivia C. Jones, Camilla Pacifici
Figure caption: The F115W−F335M vs. F115W (top) and F277W–F356W vs. F277W (bottom), similar to Figure 2, showing the additional limits utilized to obtain a cleaner sample of PMS and BD candidates.
Paper: Fully Kinetic Simulations of Proton-beam-driven Instabilities from Parker Solar Probe Observations
Authors: L. Pezzini, A. N. Zhukov, F. Bacchini, G. Arrò, R. A. López, A. Micera, M. E. Innocenti, G. Lapenta
Figure caption: Evolution of different types of energy and proton temperature anisotropy. Panels (a)–(c) illustrate the time evolution of different energy components. In panels (d)–(f), the temporal evolution of the temperature anisotropy for the proton core, the proton beam, and the total proton population (encompassing both core and beam) is displayed. The three distinct phases of the instability, labeled I, II, and III, corresponding to the stationary, linear, and nonlinear phases, are also depicted. The gray region identifies Phase II, with the dashed–dotted line indicating the inflection point of the curves, where the conversion of kinetic energy into magnetic energy peaks at ﹩{t}_{\mathrm{peak}}/{{\rm{\Omega }}}_{{\rm{p}}}^{-1}\approx 170﹩. Panel (a) displays the changes in magnetic and total kinetic energy of electrons and protons, normalized by the initial total energy of the system. Panel (b) presents the thermal energies (parallel and perpendicular with respect to the guide field direction) of both the core and beam populations, along with the core and beam drift (i.e., bulk) energy. In panel (c), the thermal and bulk energies of the electron population are shown. The formal definition of these quantities is provided in the text.
Paper: Fully Kinetic Simulations of Proton-beam-driven Instabilities from Parker Solar Probe Observations
Authors: L. Pezzini, A. N. Zhukov, F. Bacchini, G. Arrò, R. A. López, A. Micera, M. E. Innocenti, G. Lapenta
Figure caption: Results from linear Vlasov theory corresponding to our initial setup, in the left column, compared with the simulation results in the right column. The left panels show the following: the real frequency ω r/ω p (a); the imaginary frequency γ (c); and the polarization of the wave (e). The right column shows the following: In panel (b), the power spectrum measured for a cut at y = L  y /2 is plotted against the frequency at different positions along the x-axis; the black and red dashed lines represent the frequencies obtained from the linear theory and the numerical simulation, respectively. Panel (d) shows the power spectrum at ﹩t/{{\rm{\Omega }}}_{{\rm{p}}}^{-1}\approx 218﹩, with some of the instability growth rate contours of panel (c) overlaid, and the black dot denoting the fastest-growing mode. Panel (f) is the hodogram at ﹩t/{{\rm{\Omega }}}_{{\rm{p}}}^{-1}\approx 218﹩, where the red triangle shows the value of the magnetic fluctuation corresponding to the point x = L  x  (see text for details on how this is computed).
Paper: Fully Kinetic Simulations of Proton-beam-driven Instabilities from Parker Solar Probe Observations
Authors: L. Pezzini, A. N. Zhukov, F. Bacchini, G. Arrò, R. A. López, A. Micera, M. E. Innocenti, G. Lapenta
Figure caption: Evolution of the proton VDF f p(v  x , v  y , t) (left column) and its parallel cut f p(v  x , v  y  = 0, t) (right column). Panels (a) and (b) represent the quasi-stationary phase of the proton beam instability. Panel (a) shows the initial distribution of protons f p(v  x , v  y , t), whereas panel (b) shows the horizontal cut f p(v  x , v  y  = 0, t) (with the core and beam subpopulations indicated by different lines), at ﹩t/{{\rm{\Omega }}}_{{\rm{p}}}^{-1}=0﹩. Panels (c) and (d) represent the phase space of protons during the quasi-linear phase at ﹩t/{{\rm{\Omega }}}_{{\rm{p}}}^{-1}\approx 218﹩. The proton VDF during the nonlinear phase at ﹩t/{{\rm{\Omega }}}_{{\rm{p}}}^{-1}\approx 436﹩ is shown in panels (e) and (f). The resonant velocity of the system, ﹩{v}_{\mathrm{res}}=({\omega }_{{\rm{r}}}+{{\rm{\Omega }}}_{{\rm{p}}})/{k}_{\parallel }﹩, is shown by the blue line in panel (f).
Paper: Fully Kinetic Simulations of Proton-beam-driven Instabilities from Parker Solar Probe Observations
Authors: L. Pezzini, A. N. Zhukov, F. Bacchini, G. Arrò, R. A. López, A. Micera, M. E. Innocenti, G. Lapenta
Figure caption: Magnetic field fluctuations resulting from the PIC simulation. Panel (a) displays the spectral power of magnetic fluctuations for different wavenumbers (i.e., different modes), corresponding to those within the region delimited by the innermost contour in Figure 1(d) with ﹩{k}_{\parallel }/{d}_{{\rm{p}}}^{-1}\in [0.3,0.6]﹩. The calculated fastest-growing mode, represented by the violet line and highlighted with its corresponding wavenumber, is compared with the expected maximum growth rate from linear theory, indicated by the dashed black line. In panel (b), a spatiotemporal analysis is presented, focusing on the cut along y = L  y /2 of the magnetic fluctuation stacked in time. The black line in panel (b) has a slope equal to the phase velocity of the wave calculated from linear theory.
Paper: Fully Kinetic Simulations of Proton-beam-driven Instabilities from Parker Solar Probe Observations
Authors: L. Pezzini, A. N. Zhukov, F. Bacchini, G. Arrò, R. A. López, A. Micera, M. E. Innocenti, G. Lapenta
Figure caption: Proton VDF f p(v  x , v  y , t) at time ﹩t/{{\rm{\Omega }}}_{{\rm{p}}}^{-1}\approx 436﹩ normalized by its value at the initial time. The blue line shows the parallel resonant velocity v r. The black dashed circle centered at (v  x , v  y ) = (v ph, 0), with v ph = ω r/k ∥ the parallel phase velocity of the waves, is the diffusion path due to the resonant interaction.
Paper: Fully Kinetic Simulations of Proton-beam-driven Instabilities from Parker Solar Probe Observations
Authors: L. Pezzini, A. N. Zhukov, F. Bacchini, G. Arrò, R. A. López, A. Micera, M. E. Innocenti, G. Lapenta
Figure caption: Fluctuations in the proton density ρ p (a), with δ ρ p = ρ p(t) − ρ 0, and fluctuations in the magnetic field components B  x , B  y , B  z  (b)–(d), at the moment of instability saturation ﹩t/{{\rm{\Omega }}}_{{\rm{p}}}^{-1}\approx 218﹩. The amplitudes of ρ p and B  x  fluctuations have been multiplied by a factor of 10 for visualization purposes.
Paper: The Power of High-precision Broadband Photometry: Tracing the Milky Way Density Profile with Blue Horizontal Branch Stars in the Dark Energy Survey
Authors: Fengqing Yu, 枫青 余, Ting S. Li, Joshua S. Speagle, 佳士 沈, Gustavo E. Medina, Sergey E. Koposov, Joss Bland-Hawthorn, Lara R. Cullinane, Gwendolyn M. Eadie, Denis Erkal, Geraint F. Lewis, Guilherme Limberg, Daniel B. Zucker
Figure caption: Left: BHB candidate count given different probability thresholds. Right: best-fit power-law index α for BHB samples corresponding to the differing probability thresholds p. The error bar shows the 95% (2σ) credible interval. The normalization coefficient A is completely degenerate with α and is thus omitted. The criterion we used for the previous section, p BHB ≥ 0.5, is highlighted. As the selection becomes stricter, BHB count decreases and we observe a steeper descent. We note that the trends in both panels are not smooth, with small bumps discernible, which is explained in Figure 11. The orange star shows the best-fit α where we weigh the log-likelihood of each star by its BHB probability, instead of using the unweighted log-likelihood of BHB candidates selected from hard thresholding (see text for details).
Paper: The Power of High-precision Broadband Photometry: Tracing the Milky Way Density Profile with Blue Horizontal Branch Stars in the Dark Energy Survey
Authors: Fengqing Yu, 枫青 余, Ting S. Li, Joshua S. Speagle, 佳士 沈, Gustavo E. Medina, Sergey E. Koposov, Joss Bland-Hawthorn, Lara R. Cullinane, Gwendolyn M. Eadie, Denis Erkal, Geraint F. Lewis, Guilherme Limberg, Daniel B. Zucker
Figure caption: Averaged BHB probability with respect to g 0-band photometry and Galactocentric distance. Stars are selected with p BHB ≥ 0.3 (same as the first threshold in Figure 10). Then, the selected candidates are separated into different 2D bins based on g 0 and Galactocentric distance R. Within each bin, the average BHB probability is computed over the stars inside that bin, shown by color. We observe that BHB probability generally decreases as distance increases, or when the magnitude becomes larger. However, it is worth noting that the trend is not smooth with respect to magnitude and distance. Some bins appear to have higher BHB probabilities than their neighbors. A hard probability threshold cutoff may accidentally remove a group of stars in those bins, resulting in the bumps we see in Figure 10.
Paper: The Power of High-precision Broadband Photometry: Tracing the Milky Way Density Profile with Blue Horizontal Branch Stars in the Dark Energy Survey
Authors: Fengqing Yu, 枫青 余, Ting S. Li, Joshua S. Speagle, 佳士 沈, Gustavo E. Medina, Sergey E. Koposov, Joss Bland-Hawthorn, Lara R. Cullinane, Gwendolyn M. Eadie, Denis Erkal, Geraint F. Lewis, Guilherme Limberg, Daniel B. Zucker
Figure caption: Left: we split DES coverage into three patches, shown by the dashed lines. Iso-latitude lines at b = −80°, −60°, −40° are shown in gray. Right: best-fit parameter α with 95% (2σ) credible interval of the BHB density profile within each patch. The dashed line and shaded region show the best-fit parameter for the entire DES footprint. We see that α varies considerably among different sky patches, which reflects the spatial inhomogeneity of the Milky Way halo and illustrates the importance of considering the location and coverage of a survey when fitting a density profile.
Paper: The Power of High-precision Broadband Photometry: Tracing the Milky Way Density Profile with Blue Horizontal Branch Stars in the Dark Energy Survey
Authors: Fengqing Yu, 枫青 余, Ting S. Li, Joshua S. Speagle, 佳士 沈, Gustavo E. Medina, Sergey E. Koposov, Joss Bland-Hawthorn, Lara R. Cullinane, Gwendolyn M. Eadie, Denis Erkal, Geraint F. Lewis, Guilherme Limberg, Daniel B. Zucker
Figure caption: Same as Figure 4, but with a more complex parametric form of the BHB ratio. Bottom left: a corner plot depicting the 2D and 1D marginal posterior probability distributions of the 17 parameters of our photometric mixture model estimated with dynesty. All values are multiplied by a factor of 100 for visualization purposes. The parameters d  i  are defined according to Appendix A. Top right: the predicted class probabilities for the stars used to derive the model in color–color space. BHB (blue) and BS (purple) sequences are shown as a solid line, with the best-fit scatter as a light shaded region and dashed lines defining its boundary. Stars classifited as BHBs, BSs, and outliers based on their posterior-marginalized class probabilities are shown with blue circles, purple squares, and red stars, respectively. The parameters are well constrained, accurately trace the photometric distribution of stars, and successfully identify photometric outliers.
Paper: The Power of High-precision Broadband Photometry: Tracing the Milky Way Density Profile with Blue Horizontal Branch Stars in the Dark Energy Survey
Authors: Fengqing Yu, 枫青 余, Ting S. Li, Joshua S. Speagle, 佳士 沈, Gustavo E. Medina, Sergey E. Koposov, Joss Bland-Hawthorn, Lara R. Cullinane, Gwendolyn M. Eadie, Denis Erkal, Geraint F. Lewis, Guilherme Limberg, Daniel B. Zucker
Figure caption: A comparison between our power-law index α (depicted in red, with 68% (1σ) credible interval highlighted in the red shaded region and systematic uncertainty indicated by a lighter-red shaded region), against values reported in existing literature (L. L. Watkins et al. 2009; A. J. Deason et al. 2011; X.-X. Xue et al. 2015; G. Iorio et al. 2018; G. E. Medina et al. 2018; G. F. Thomas et al. 2018; T. Fukushima et al. 2018; E. Starkenburg et al. 2019; A. Pieres et al. 2020; K. M. Stringer et al. 2021; J. J. Han et al. 2022; J. A. S. Amarante et al. 2024; G. E. Medina et al. 2024). The α values are plotted as a function of Galactocentric radius R, with shaded regions representing 68% (1σ) credible interval, taken from corresponding literature when applicable. The lines are categorized based on the types of stars being analyzed. Within the distance range covered by our sample, our best-fit α closely matches the findings of previous studies.
Paper: The Power of High-precision Broadband Photometry: Tracing the Milky Way Density Profile with Blue Horizontal Branch Stars in the Dark Energy Survey
Authors: Fengqing Yu, 枫青 余, Ting S. Li, Joshua S. Speagle, 佳士 沈, Gustavo E. Medina, Sergey E. Koposov, Joss Bland-Hawthorn, Lara R. Cullinane, Gwendolyn M. Eadie, Denis Erkal, Geraint F. Lewis, Guilherme Limberg, Daniel B. Zucker
Figure caption: Similar to Figure 7, but showing only BHB candidates within certain Galactocentric distances, as shown by the range of each color bar. Moving from the top left to the bottom right, we present examples of four streams, Turranburra, Willka Yaku, Chenab, and Elqui, which are shown in red. Our sample displays overdensities that align closely with these previously identified substructures. This alignment demonstrates the consistency of our catalog with prior discoveries and underscores its potential utility in future searches for additional substructures.
Paper: The Power of High-precision Broadband Photometry: Tracing the Milky Way Density Profile with Blue Horizontal Branch Stars in the Dark Energy Survey
Authors: Fengqing Yu, 枫青 余, Ting S. Li, Joshua S. Speagle, 佳士 沈, Gustavo E. Medina, Sergey E. Koposov, Joss Bland-Hawthorn, Lara R. Cullinane, Gwendolyn M. Eadie, Denis Erkal, Geraint F. Lewis, Guilherme Limberg, Daniel B. Zucker
Figure caption: Same as Figure 8, but with a more complex parametric form of the BHB ratio. Shown are histograms of final selected BHB candidates in DES DR2 vs. simulated samples from the best-fit density profile. Left: with heliocentric distance d; right: with Galactic radius R. The number of BHBs is 2111, which is very close to the value of 2103 in the previous fit.
Paper: The Power of High-precision Broadband Photometry: Tracing the Milky Way Density Profile with Blue Horizontal Branch Stars in the Dark Energy Survey
Authors: Fengqing Yu, 枫青 余, Ting S. Li, Joshua S. Speagle, 佳士 沈, Gustavo E. Medina, Sergey E. Koposov, Joss Bland-Hawthorn, Lara R. Cullinane, Gwendolyn M. Eadie, Denis Erkal, Geraint F. Lewis, Guilherme Limberg, Daniel B. Zucker
Figure caption: Same as Figure 9, but with a more complex parametric form of the BHB ratio. The corner plot shows the marginal posterior probability distributions of the two parameters of our density profile estimated with dynesty. We see that the power-law index ﹩\alpha ={4.27}_{-0.13}^{+0.13}﹩, very close to the previous fit ﹩\alpha ={4.34}_{-0.12}^{+0.13}﹩.