adsabs/AstroCLIMB huggingface dataset:
Paper: Constraining Cosmological Parameters Using the Cluster Mass–Richness Relation
Authors: Mohamed H. Abdullah, Gillian Wilson, Anatoly Klypin, Tomoaki Ishiyama
Figure caption: Systematical effects of cluster mass, lower and upper redshifts, and richness thresholds on our constraints on the cosmological parameters for the analysis on the fiducial samples of ﹩{ \mathcal S }{\mathrm{all}}_{17}﹩ for all members within R 200 (left) and ﹩{ \mathcal S }{\mathrm{red}}_{13}﹩ for red members within R 200 (right; see Section 4.3 for details). The 68% CLs for our fiducial sample, varying mass threshold logM 200 between 13.8 and 14.0 [h −1 M ⊙], fixing the upper redshift threshold to 0.125 and varying the lower redshift threshold from 0.01 to 0.07, fixing the lower redshift threshold to 0.045 and varying the upper redshift threshold from 0.11 to 0.15, varying N th from 15 to 19 for ﹩{ \mathcal S }{\mathrm{all}}_{17}﹩, and varying N th from 13 to 17 for ﹩{ \mathcal S }{\mathrm{red}}_{13}﹩.
Paper: Constraining Cosmological Parameters Using the Cluster Mass–Richness Relation
Authors: Mohamed H. Abdullah, Gillian Wilson, Anatoly Klypin, Tomoaki Ishiyama
Figure caption: Comparison of the best-fit red MRR, MRRred, derived in this work from ﹩{ \mathcal S }{\mathrm{red}}_{13}﹩ (dark green line with shading indicating 1σ uncertainty) with results reported in the literature (see legend and Table 2).
Paper: Constraining Cosmological Parameters Using the Cluster Mass–Richness Relation
Authors: Mohamed H. Abdullah, Gillian Wilson, Anatoly Klypin, Tomoaki Ishiyama
Figure caption: Schematic diagram showing the effect on the cluster abundance by varying either Ωm (upper) or σ 8 (lower) while holding the other parameter fixed. Each circle represents a cluster with its size (large to small) and color (yellow to magenta) indicating high to low mass. Increasing Ωm results in an approximately proportionally higher number of clusters of every mass. Increasing σ 8 also results in a higher number of clusters of every mass but also changes the ratio of high-to-low-mass clusters, so results in a larger number of high-mass clusters relative to low-mass clusters. Note that the clusters are distributed randomly in each box.
Paper: Detection of the Extended γ-Ray Emission around Supernova Remnant DA 530 with Fermi-LAT
Authors: Yuliang Xin, Xiaolei Guo
Figure caption: Left: 3.°0 × 3.°0 TS map in the energy range of 1 GeV–1 TeV. The red cross shows the position of 4FGL J2051.1+5539 in 4FGL-DR3 catalog. And the green solid circle marks the best-fit 68% containment radius of the uniform disk for the spatial template of SrcT. The radio image of SNR DA 530 at 1.4 GHz is shown as the cyan contours. Right: SED of SrcT in the energy range of 100 MeV–1 TeV with the gray histogram shown as the TS value for each energy bin. The red error bars show the statistical errors and the sums of the statistical and systematic errors calculated by σ = ﹩\sqrt{{\sigma }_{\mathrm{stat}}^{2}+{\sigma }_{\mathrm{syst}}^{2}}﹩ are marked by the blue error bars. The arrows indicate the 95% upper limits for the energy bin with TS value of SrcT smaller than 5.0. The black solid and dashed lines show the global best-fit power-law spectrum and its 1σ statistic error in the energy range of 100 MeV–1 TeV.
Paper: First Results from the JWST Early Release Science Program Q3D: Ionization Cone, Clumpy Star Formation, and Shocks in a z = 3 Extremely Red Quasar Host
Authors: Andrey Vayner, Nadia L. Zakamska, Yuzo Ishikawa, Swetha Sankar, Dominika Wylezalek, David S. N. Rupke, Sylvain Veilleux, Caroline Bertemes, Jorge K. Barrera-Ballesteros, Hsiao-Wen Chen, Nadiia Diachenko, Andy D. Goulding, Jenny E. Greene, Kevin N. Hainline, Fred Hamann, Timothy Heckman, Sean D. Johnson, Hui Xian Grace Lim, Weizhe Liu, Dieter Lutz, Nora Lützgendorf, Vincenzo Mainieri, Ryan McCrory, Grey Murphree, Nicole P. H. Nesvadba, Patrick Ogle, Eckhard Sturm, Lillian Whitesell
Figure caption: Spatially resolved emission-line diagnostic diagrams for J1652. The top row shows the line ratios for the kinematically integrated line ratios. The bottom three rows are for the three distinct kinematic components. The star represents the average emission-line flux ratio for the individual kinematic component. The circle point to the lower left shows the median error on the emission-line ratios. The points are color coded to match the maps presented in Figure 5. The dashed orange line shows the location of the star formation abundance sequence at z = 0 from Kauffmann et al. (2003) on the log([O  III]/Hβ) vs. log([N II]/Hα) line-ratio diagram and the separation between Seyferts and LINERs on the log([O  III]/Hβ) vs. log([S  II]/Hα) and log([O I]/Hα) diagrams, and the solid orange line shows the delineation between star formation and AGN photoionization based on the theoretical models by Kewley et al. (2001) for low redshift, while the solid red line shows the upper bound on the theoretical abundance sequence with evolving gas conditions as a function of redshift at z = 3 (Kewley et al. 2013).
Paper: First Results from the JWST Early Release Science Program Q3D: Ionization Cone, Clumpy Star Formation, and Shocks in a z = 3 Extremely Red Quasar Host
Authors: Andrey Vayner, Nadia L. Zakamska, Yuzo Ishikawa, Swetha Sankar, Dominika Wylezalek, David S. N. Rupke, Sylvain Veilleux, Caroline Bertemes, Jorge K. Barrera-Ballesteros, Hsiao-Wen Chen, Nadiia Diachenko, Andy D. Goulding, Jenny E. Greene, Kevin N. Hainline, Fred Hamann, Timothy Heckman, Sean D. Johnson, Hui Xian Grace Lim, Weizhe Liu, Dieter Lutz, Nora Lützgendorf, Vincenzo Mainieri, Ryan McCrory, Grey Murphree, Nicole P. H. Nesvadba, Patrick Ogle, Eckhard Sturm, Lillian Whitesell
Figure caption: Examples of kinematic decomposition of the quasar host galaxy, outflow, and the nearby companions. We present multicomponent Gaussian model fits to the Hβ, [O III], [O I], Hα, [N II], and [S II] emission lines in a single spaxel of a region at the systemic velocity in the quasar host galaxy, the outflow, a second region at the systemic velocity orthogonal to the outflow, and a companion galaxy toward the northeast. The top panel for each spectrum shows a multicomponent Gaussian fit (dashed lines) to the extended emission lines, while the black curve shows the total best fit. The red curve shows the spatially unresolved emission fit to that spaxel part of the quasar PSF-subtraction procedure in q3dfit. The bottom panel shows the residuals after subtracting out the spatially unresolved emission, showcasing only the extended emission. The dashed curves show the individual multicomponent Gaussian fit to the extended emission while.
Paper: First Results from the JWST Early Release Science Program Q3D: Ionization Cone, Clumpy Star Formation, and Shocks in a z = 3 Extremely Red Quasar Host
Authors: Andrey Vayner, Nadia L. Zakamska, Yuzo Ishikawa, Swetha Sankar, Dominika Wylezalek, David S. N. Rupke, Sylvain Veilleux, Caroline Bertemes, Jorge K. Barrera-Ballesteros, Hsiao-Wen Chen, Nadiia Diachenko, Andy D. Goulding, Jenny E. Greene, Kevin N. Hainline, Fred Hamann, Timothy Heckman, Sean D. Johnson, Hui Xian Grace Lim, Weizhe Liu, Dieter Lutz, Nora Lützgendorf, Vincenzo Mainieri, Ryan McCrory, Grey Murphree, Nicole P. H. Nesvadba, Patrick Ogle, Eckhard Sturm, Lillian Whitesell
Figure caption: On the left, we present line-integrated [O III] 5007 Å flux in units of ×10−17 erg s−1 cm−2 Å−1 arcsec−2, in the middle, we present the radial velocity centroid (v 50) map in units of km s−1, and on the right the velocity dispersion maps for each detected kinematic components in J1652. In each map, “c” stands for the Gaussian component number, where component 1 is associated with the systemic gas in the quasar host galaxy, component 2 with the outflow, and component 3 with the tidal tail feature and the neighboring galaxies. North is up, and east is to the left. The ellipse in the lower left corner shows the size of the NIRSpec-IFU PSF.
Paper: Detection of the Extended γ-Ray Emission around Supernova Remnant DA 530 with Fermi-LAT
Authors: Yuliang Xin, Xiaolei Guo
Figure caption: Modeling of the γ-ray spectra with the hadronic escaping models. The red solid, green, and blue dashed lines indicate the scenarios with the different values for χ, δ, and η and the cutoff energy of E p,cut = 3 PeV. And the red dotted line shows the scenario with E p,cut = 10 TeV, as shown in the legend. The cyan dotted–dashed line shows the differential sensitivity of CTA-North (50 hr; Cherenkov Telescope Array Consortium et al. 2019).
Paper: Detection of the Extended γ-Ray Emission around Supernova Remnant DA 530 with Fermi-LAT
Authors: Yuliang Xin, Xiaolei Guo
Figure caption: Integrated CO emission intensity (K km s−1) around DA 530 in the velocity range of −6 ∼ +5 km s−1. The 68% containment radius of the extended γ-ray emission of SrcT is marked by the yellow solid circle. The green and cyan contours show the γ-ray morphology of SrcT and the radio image of SNR DA 530 at 1.4 GHz, as shown in the left panel of Figure 1.
Paper: First Results from the JWST Early Release Science Program Q3D: Ionization Cone, Clumpy Star Formation, and Shocks in a z = 3 Extremely Red Quasar Host
Authors: Andrey Vayner, Nadia L. Zakamska, Yuzo Ishikawa, Swetha Sankar, Dominika Wylezalek, David S. N. Rupke, Sylvain Veilleux, Caroline Bertemes, Jorge K. Barrera-Ballesteros, Hsiao-Wen Chen, Nadiia Diachenko, Andy D. Goulding, Jenny E. Greene, Kevin N. Hainline, Fred Hamann, Timothy Heckman, Sean D. Johnson, Hui Xian Grace Lim, Weizhe Liu, Dieter Lutz, Nora Lützgendorf, Vincenzo Mainieri, Ryan McCrory, Grey Murphree, Nicole P. H. Nesvadba, Patrick Ogle, Eckhard Sturm, Lillian Whitesell
Figure caption: A color composite of ionized gas emission in the J1652 quasar host galaxy and the immediate environment. [O III] is assigned to blue, Hα is assigned to green, [N II] is assigned to red, and [S II] is assigned to orange. Bar on the left represents 1″, and the quasar is located behind the white ellipse near the center. The ellipse to the lower left represents the FWHM of the PSF. Regions for which spectra are extracted in Figure 3 are labeled a–d. North is up, and east is to the left.
Paper: A Reanalysis of the Isolated Black Hole Candidate OGLE-2011-BLG-0462/MOA-2011-BLG-191
Authors: Casey Y. Lam, Jessica R. Lu
Figure caption: Five reference stars nearest to OB110462. The title indicates the separation of the reference star from OB110462 in R.A., decl., and total distance, and the magnitude of the star in F814W and F606W. In the individual panels, data in the F606W (F814W) filters are shown in blue (red). First column: trajectory on sky. Note the scales across different rows vary. The positions are relative to the ΔR.A., and Δdecl. offsets, which are relative to OB110462. The best-fit linear trajectory is shown in gray. Note these velocities are in a reference frame where the mean velocity of the reference stars is 0, and not the Gaia reference frame. Second column: residuals to the best-fit linear trajectory in R.A. The dashed lines are the 1σ  uncertainties to the best-fit line. Third column: same as the second column, but for decl. instead of R.A. Fourth column: histograms of the position residuals to the best-fit linear trajectory, in units of σ. The solid gray is for R.A.; the outlined black is for decl. Fifth column: residuals to the best-fit constant magnitude. F814W and F606W are fit to the respective magnitudes in the title; the dashed lines show the 1σ  uncertainties to the best-fit magnitude. Sixth column: residuals to the best-fit constant magnitude, in units of σ. The solid blue is for F606W; the outlined red is for F814W.
Paper: A Reanalysis of the Isolated Black Hole Candidate OGLE-2011-BLG-0462/MOA-2011-BLG-191
Authors: Casey Y. Lam, Jessica R. Lu
Figure caption: Measurement bias of a source in F814W (left) and F606W (right) due to proximity to a bright star. The bias correction is defined as the recovered minus injected value. The amount of positional bias is shown decomposed into radial r (top row) and azimuthal θ (middle row) components. The radial direction is defined by the OB110462-neighbor star separation vector, and the azimuthal direction is measured counterclockwise from the separation vector. The amount of magnitude bias is shown in the bottom row. The colored points show the mean and standard deviation of the measurement bias for the four different neighbor-like stars; the colors correspond to those in Figures 2 and 3. The black points are the mean and standard deviation of the mean measurement bias of the four neighbor-like stars. The positional and magnitude bias in F606W is smaller than that in F814W by about a factor of two; this is not surprising since at shorter wavelengths the angular resolution is higher.
Paper: A Reanalysis of the Isolated Black Hole Candidate OGLE-2011-BLG-0462/MOA-2011-BLG-191
Authors: Casey Y. Lam, Jessica R. Lu
Figure caption: OB110462 astrometry. Left column, top to bottom: R.A. vs. time with MLE unlensed source motion model subtracted; residuals to the MLE model for R.A. vs. time fit. HST F814W astrometric data are shown in red; HST F606W astrometric data are shown in blue. The MLE model is shown in black. Fifty random draws from the posterior distribution are shown in light gray. Middle column, top to bottom: same as the left column, except for decl. instead of R.A. Right panel: astrometry as seen on sky, in the barycentric frame.
Paper: A Reanalysis of the Isolated Black Hole Candidate OGLE-2011-BLG-0462/MOA-2011-BLG-191
Authors: Casey Y. Lam, Jessica R. Lu
Figure caption: Top panel: HST F814W (red triangles), HST F606W (black squares), and detrended OGLE light curves (blue), with the corresponding maximum likelihood estimator (MLE; described in Section 5) plotted over the data. Second from top panel: residuals to the MLE model. The Gaussian process (GP) model is plotted on top of the OGLE residuals. Second from bottom panel: same as the top panel, but zoomed into the three most magnified years (2010–2012). Bottom panel: same as the second from top panel, but zoomed into the three most magnified years (2010–2012).
Paper: A Reanalysis of the Isolated Black Hole Candidate OGLE-2011-BLG-0462/MOA-2011-BLG-191
Authors: Casey Y. Lam, Jessica R. Lu
Figure caption: Top: histograms of χ 2 residual values to linear proper motion fits (no parallax) of the reference stars. Bottom: histograms of χ 2 residual values to constant magnitude vs. time fits of the reference stars. The left column shows the reference stars for F606W; the right column shows the reference stars for F814W. N denotes the number of reference stars.
Paper: A Reanalysis of the Isolated Black Hole Candidate OGLE-2011-BLG-0462/MOA-2011-BLG-191
Authors: Casey Y. Lam, Jessica R. Lu
Figure caption: Location of neighbor-like stars on an HST CMD. The black circle marks OB110462's bright neighbor. The four other colored circles mark the neighbor-like stars (colors correspond to those in Figure 2). The black star marks OB110462 at baseline (i.e., unmagnified).
Paper: A Reanalysis of the Isolated Black Hole Candidate OGLE-2011-BLG-0462/MOA-2011-BLG-191
Authors: Casey Y. Lam, Jessica R. Lu
Figure caption: Spatial distribution of neighbor-like stars. The image shows a 36″ × 36″  area centered on OB110462. The black circle in the center shows the location of OB110462's bright neighbor. The four other colored circles show the location of the neighbor-like stars.
Paper: A Reanalysis of the Isolated Black Hole Candidate OGLE-2011-BLG-0462/MOA-2011-BLG-191
Authors: Casey Y. Lam, Jessica R. Lu
Figure caption: Same as Figure 6, but for the next five reference stars nearest to OB110462.
Paper: A Reanalysis of the Isolated Black Hole Candidate OGLE-2011-BLG-0462/MOA-2011-BLG-191
Authors: Casey Y. Lam, Jessica R. Lu
Figure caption: Difference between the OGLE photometry used in Mróz et al. (2022) to that used in Lam et al. (2022a, 2022b) and Sahu et al. (2022). Left: full light curve. Right: light curve zoomed into the first three years (photometric peak year ±1 yr).
Paper: Decomposing the Spectrum of Ultraluminous X-Ray Pulsar NGC 300 ULX-1
Authors: Shogo B. Kobayashi, Hirofumi Noda, Teruaki Enoto, Tomohisa Kawashima, Akihiro Inoue, Ken Ohsuga
Figure caption: Top panel: spectra and the best-fit model unfolded with the instrumental response. The faint phase, stable-component, and variable-component spectra are shown in black, red, and blue, respectively. Panels (a), (b), and (c): residuals from diskbb  st  + cutoffpl  v , diskbb  st  + Gauss  st  + diskbb  v  + power  v , and diskbb  st  + Gauss  st  + simpl  v  ∗ nthcomp  v , respectively.
Paper: Decomposing the Spectrum of Ultraluminous X-Ray Pulsar NGC 300 ULX-1
Authors: Shogo B. Kobayashi, Hirofumi Noda, Teruaki Enoto, Tomohisa Kawashima, Akihiro Inoue, Ken Ohsuga
Figure caption: Phase-resolved (black) and decomposed stable (red)/variable (blue) component spectra. They are shown in ratios over a power-law model for the same reason as in Figure 7. The difference between spectra in left-hand and right-hand panels is whether assuming zero (left) or certain count rates (right) as the intensity floor (see the text for detail). Filled and open markers represent the data from XMM-Newton and NuSTAR, respectively. Data from NuSTAR FPM-A are shown with circle markers and those from FPM-B are shown with square markers.
Paper: Decomposing the Spectrum of Ultraluminous X-Ray Pulsar NGC 300 ULX-1
Authors: Shogo B. Kobayashi, Hirofumi Noda, Teruaki Enoto, Tomohisa Kawashima, Akihiro Inoue, Ken Ohsuga
Figure caption: A CCP obtained from the 0.3–7  keV band of the XMM-Newton PN data (top) and its residuals from the respective model function (bottom). The red and blue solid lines are the best-fit breaking-linear function and exponential function, respectively. The colors of the residual data points are in correspondence with those of the function curves above. The data points with the highest and lowest count rate correspond to the peak and bottom of the pulse, respectively.
Paper: Decomposing the Spectrum of Ultraluminous X-Ray Pulsar NGC 300 ULX-1
Authors: Shogo B. Kobayashi, Hirofumi Noda, Teruaki Enoto, Tomohisa Kawashima, Akihiro Inoue, Ken Ohsuga
Figure caption: Upper panel: phase-resolved spectra (on phase: black, off phase: red). The instrumental response is tentatively removed by taking ratios over a power-law model with a photon index of 2. Bottom panel: spectral ratio between two phases.
Paper: Decomposing the Spectrum of Ultraluminous X-Ray Pulsar NGC 300 ULX-1
Authors: Shogo B. Kobayashi, Hirofumi Noda, Teruaki Enoto, Tomohisa Kawashima, Akihiro Inoue, Ken Ohsuga
Figure caption: Top panel: spectra and the best-fit model unfolded with the instrumental response. The bright phase, stable-component, and variable-component spectra are shown in black, red, and blue, respectively. Panels (a), (b), and (c): residuals from the best-fit faint phase model+, cutoffpl  v , simpl  v  ∗ cutoffpl  v , and simpl  v  ∗ nthcomp  v , respectively.
Paper: Decomposing the Spectrum of Ultraluminous X-Ray Pulsar NGC 300 ULX-1
Authors: Shogo B. Kobayashi, Hirofumi Noda, Teruaki Enoto, Tomohisa Kawashima, Akihiro Inoue, Ken Ohsuga
Figure caption: XMM-Newton pn phase-resolved count–count plot of ULX-1. The red and blue solid lines represent the best-fit polynomial functions. The data points with the highest and lowest count rate correspond to the peak and bottom of the pulse, respectively.
Paper: Decomposing the Spectrum of Ultraluminous X-Ray Pulsar NGC 300 ULX-1
Authors: Shogo B. Kobayashi, Hirofumi Noda, Teruaki Enoto, Tomohisa Kawashima, Akihiro Inoue, Ken Ohsuga
Figure caption: Significance contours of the electron temperature vs. photon index of nthcomp  v . The confidence levels from the faint phase are shown in blue, while those from the bright phase are in red. Inner, middle, and outer solid lines represent 68%, 90%, and 99.7% confidence level, respectively. The crosses indicate the best-fit values.
Paper: Decomposing the Spectrum of Ultraluminous X-Ray Pulsar NGC 300 ULX-1
Authors: Shogo B. Kobayashi, Hirofumi Noda, Teruaki Enoto, Tomohisa Kawashima, Akihiro Inoue, Ken Ohsuga
Figure caption: Same as Figure 5, but the vertical axis represents the count rate of NuSTAR FPM-A.
Paper: Decomposing the Spectrum of Ultraluminous X-Ray Pulsar NGC 300 ULX-1
Authors: Shogo B. Kobayashi, Hirofumi Noda, Teruaki Enoto, Tomohisa Kawashima, Akihiro Inoue, Ken Ohsuga
Figure caption: The Δχ 2 distribution obtained from adding a Gaussian line to the 5000 simulated spectral fits. The gray-hatched histogram represents the distribution of the total simulations, and the filled-black one is for those given values consistent with the observational results within the statistical errors.
Paper: Rapidly Evolving Transients in Archival ZTF Public Alerts
Authors: Wenxiong Li, 文雄 李, Iair Arcavi, Ehud Nakar, Alexei V. Filippenko, Thomas G. Brink, WeiKang Zheng, Yi Yang, 轶 杨, Marco C. Lam, Ido Keinan, Seán J. Brennan, Noi Shitrit
Figure caption: Comparison of the light curves of our RET candidates to the SN Ibc r-band template (gray solid line) from Drout et al. (2011), the SN Ibn r-band template (blue solid line) from Hosseinzadeh et al. (2017), and r-band light curves of a few representative RETs: AT 2018cow (red solid line; Perley et al. 2019), and AT 2017gfo (the KN; black solid line; Andreoni et al. 2017; Arcavi et al. 2017; Coulter et al. 2017; Cowperthwaite et al. 2017; Díaz et al. 2017; Drout et al. 2017; Kasliwal et al. 2017; Pian et al. 2017; Shappee et al. 2017; Smartt et al. 2017; Tanvir et al. 2017; Utsumi et al. 2017; Valenti et al. 2017). In all cases we shift the comparison light curves to match the peak apparent magnitude of the RET candidates, except AT 2020ohw, for which we have a spectroscopic redshift and can thus display the light curves in absolute magnitude. For that event we also plot the r-band light curve of Type Ib SN iPTF13bvn (red dashed line; Fremling et al. 2016) and the R-band light curve of Type Ic SN 1994I (red dashed–dotted line; Richmond et al. 1996). In all light curves, triangles denote 3σ nondetection limits. A high-cadence oscillating portion of the light curve is seen in the inset of AT 2019wjk.(The data used to create this figure are available.)
Paper: Rapidly Evolving Transients in Archival ZTF Public Alerts
Authors: Wenxiong Li, 文雄 李, Iair Arcavi, Ehud Nakar, Alexei V. Filippenko, Thomas G. Brink, WeiKang Zheng, Yi Yang, 轶 杨, Marco C. Lam, Ido Keinan, Seán J. Brennan, Noi Shitrit
Figure caption: The observed (light gray) and binned (black) spectrum taken at the position of AT 2019wjk in 2022. The double-peaked z ≈ 0 Hα and Hβ emission lines (black dashed lines) are consistent with an accreting Galactic source, making the 2019 outburst a possible nova. The continuum-normalized spectra of Hα and Hβ in velocity space are displayed in the inset.
Paper: Rapidly Evolving Transients in Archival ZTF Public Alerts
Authors: Wenxiong Li, 文雄 李, Iair Arcavi, Ehud Nakar, Alexei V. Filippenko, Thomas G. Brink, WeiKang Zheng, Yi Yang, 轶 杨, Marco C. Lam, Ido Keinan, Seán J. Brennan, Noi Shitrit
Figure caption: The observed (light gray) and binned (black) spectrum taken at the position of ZTF21abcyioo in 2022. The z = 0 Na I D absorption doublet is labeled (dashed line), and the continuum-normalized spectrum of it is displayed in the inset.
Paper: Evolution of Elemental Abundances in Hot Active Region Cores from Chandrayaan-2 XSM Observations
Authors: Biswajit Mondal, Santosh V. Vadawale, Giulio Del Zanna, N. P. S. Mithun, Aveek Sarkar, Helen E. Mason, P. Janardhan, Anil Bhardwaj
Figure caption: Simulated spectra from CHIANTI v 10 in the energy range of the Mg/Al line complex of the XSM observed spectrum. The red curve shows the multithermal spectrum, and the blue curve shows the isothermal spectrum.