adsabs/AstroCLIMB huggingface dataset:
Paper: Disk Cooling and Wind Lines as Seen in the Spectral Line Evolution of V960 Mon
Authors: Adolfo Carvalho, Lynne Hillenbrand, Jerome Seebeck
Figure caption: The 8750 and 8862 Å HP lines in the HIRES spectra (left column) and the residual spectrum (right column). Notice the lines have been removed to within a few percent in every epoch, indicating the modeled T max change reproduces the evolution of the HP series accurately. The 8750 Å line is blended with the λ8751 Si I line and the 8862 Å line is blended with an Fe I line at 8866 Å but both are well modeled, do not show any evolution, and do not appear in the residuals. The emission residual in the lower right panel at −200 km s−1 is due to TiO absorption in the model that is not present in the data. We discuss this discrepancy in Appendix B.
Paper: Disk Cooling and Wind Lines as Seen in the Spectral Line Evolution of V960 Mon
Authors: Adolfo Carvalho, Lynne Hillenbrand, Jerome Seebeck
Figure caption: The EW ratio of the Si II λ6347 line to the Fe I λ6400 line for the HIRES spectra, showing that the ratio decreases in time and is consistent with a decreasing temperature. The color schemes in the left and right panels both show lighter red for larger EW ratios. Left: the time series of the EW ratios. Right: the EW ratios of the same lines as measured in the PHOENIX grid (blue contoured background) and in the HIRES spectra (red contours).
Paper: Disk Cooling and Wind Lines as Seen in the Spectral Line Evolution of V960 Mon
Authors: Adolfo Carvalho, Lynne Hillenbrand, Jerome Seebeck
Figure caption: The EW ratio of the O I λ8446 line to the Fe I λ8688 line for the HIRES spectra, showing that the ratio decreases in time and is consistent with a decreasing temperature. The color schemes in the left and right panels both show lighter red for larger EW ratios. Left: the time series of the EW ratios. Right: the EW ratios of the same lines as measured in the PHOENIX grid (blue contoured background) and in the HIRES spectra (red contours).
Paper: Disk Cooling and Wind Lines as Seen in the Spectral Line Evolution of V960 Mon
Authors: Adolfo Carvalho, Lynne Hillenbrand, Jerome Seebeck
Figure caption: Fe II lines in the HIRES spectra. Notice their behavior is similar to the high-EP lines shown in Figure 12, rapidly shrinking over time. This effect is strongest in the lines with higher EP, indicating sensitivity to the hot wind component. The Fe II lines here seem to trace the disk behavior at lower EPs and bluer wavelengths, and trace the wind at higher EPs and redder wavelengths.
Paper: Disk Cooling and Wind Lines as Seen in the Spectral Line Evolution of V960 Mon
Authors: Adolfo Carvalho, Lynne Hillenbrand, Jerome Seebeck
Figure caption: Left: the EW ratios of the Ca I λ6439 line and the Fe I λ6456 line as a function of time in the HIRES spectra. Right: the EW ratios of the same lines in the PHOENIX grid in the blue background and the ratios in the HIRES spectra shown in the red color map, with larger EW ratio values shown as darker shades.
Paper: Environmental Impacts on the Rest-frame UV Size and Morphology of Star-forming Galaxies at z ∼ 2
Authors: Abdurrahman Naufal, Yusei Koyama, Rhythm Shimakawa, Tadayuki Kodama
Figure caption: Similar to Figure 6, but for each cluster compared to the field sample in the gray histograms. We find some variations in the median offsets, but we cannot rule out that each distribution is drawn from the same parent distribution as the field sample.
Paper: Environmental Impacts on the Rest-frame UV Size and Morphology of Star-forming Galaxies at z ∼ 2
Authors: Abdurrahman Naufal, Yusei Koyama, Rhythm Shimakawa, Tadayuki Kodama
Figure caption: Gini-M 20 merger statistics divided into two SFMS offset bins: blue for those above the SFMS and orange for those below the SFMS. We find a higher fraction of disturbed galaxies in protoclusters. The fraction of disturbed galaxies is also correlated with the SFR in both protoclusters and in the field.
Paper: Solar Atmospheric Heating Due to Small-scale Events in an Emerging Flux Region
Authors: Rahul Yadav, Maria D. Kazachenko, Andrey N. Afanasyev, Jaime de la Cruz Rodríguez, Jorrit Leenaarts
Figure caption: Fitting of observed Stokes profiles and retrieved model atmosphere. Top panel: observed (dotted lines) and best-fit (solid colored lines) profiles of pixels located at different positions of slit L1, where the color corresponds to the colored cross symbols marked in Figure 8. Bottom panels: the retrieved stratification of physical parameters obtained after fitting observed Stokes profile.
Paper: Solar Atmospheric Heating Due to Small-scale Events in an Emerging Flux Region
Authors: Rahul Yadav, Maria D. Kazachenko, Andrey N. Afanasyev, Jaime de la Cruz Rodríguez, Jorrit Leenaarts
Figure caption: Temporal evolution of physical quantities for a bipolar region shown in Figure 5. Left panel: the unsigned magnetic flux in the photosphere and chromosphere is represented by solid blue and orange lines, respectively. Middle panel: the temporal evolution of interaction distance (d 0), the separation between two opposite polarities (d), and the height of the magnetic reconnection separator (Z  s ). Right panel: the total rate of release of magnetic field energy as heat, dW/dt.
Paper: Solar Atmospheric Heating Due to Small-scale Events in an Emerging Flux Region
Authors: Rahul Yadav, Maria D. Kazachenko, Andrey N. Afanasyev, Jaime de la Cruz Rodríguez, Jorrit Leenaarts
Figure caption: Temporal evolution and stratification of physical parameters obtained from non-LTE inversion for the slit L2 highlighted in Figure 3. The fitting of observed Stokes profiles and retrieved parameters at the location of colored cross symbols is shown in the bottom panels.
Paper: Solar Atmospheric Heating Due to Small-scale Events in an Emerging Flux Region
Authors: Rahul Yadav, Maria D. Kazachenko, Andrey N. Afanasyev, Jaime de la Cruz Rodríguez, Jorrit Leenaarts
Figure caption: Same as Figure 13, but for slit L4.
Paper: Solar Atmospheric Heating Due to Small-scale Events in an Emerging Flux Region
Authors: Rahul Yadav, Maria D. Kazachenko, Andrey N. Afanasyev, Jaime de la Cruz Rodríguez, Jorrit Leenaarts
Figure caption: The vertical Poynting flux (S  z ) in the photosphere (left panel) and the evolution of average S  z  (right panel) in the black box shown in the left panel.
Paper: Solar Atmospheric Heating Due to Small-scale Events in an Emerging Flux Region
Authors: Rahul Yadav, Maria D. Kazachenko, Andrey N. Afanasyev, Jaime de la Cruz Rodríguez, Jorrit Leenaarts
Figure caption: Same as Figure 13, but for slit L3.
Paper: Secondary Outflow Driven by the Protostar Ser-emb 15 in Serpens
Authors: Asako Sato, Kazuki Tokuda, Masahiro N. Machida, Kengo Tachihara, Naoto Harada, Hayao Yamasaki, Shingo Hirano, Toshikazu Onishi, Yuko Matsushita
Figure caption: SiO(J = 5–4) channel map in the LSR velocity range from 7 to 10 and from 38 to 45 km s−1. The color scale and black contours represent the SiO emission with a velocity resolution of 1.0 km s−1. The magenta cross is the peak flux position for Source A in the 1.3 mm continuum emission. The black contour levels are [3, 4, 5, 6]× 1σ at the channels from 7 to 10 km s−1 and [2, 3, 4, 5, 6]× 1σ at the channels from 38 to 45 km s−1 (1σ = 7.0 mJy beam−1). The dashed orange circle in the panel in the bottom right corner is the area in which the line spectrum was measured (see Figure 10). The radius of the blue circle centered on the magenta cross is 6.″9 (∼3000au). The synthesized beam for the SiO emission is denoted by the magenta ellipse in the panel in the bottom left corner. The color bar on the right side is the same as in Figure 8.
Paper: Secondary Outflow Driven by the Protostar Ser-emb 15 in Serpens
Authors: Asako Sato, Kazuki Tokuda, Masahiro N. Machida, Kengo Tachihara, Naoto Harada, Hayao Yamasaki, Shingo Hirano, Toshikazu Onishi, Yuko Matsushita
Figure caption: SiO(J = 5–4) line spectrum obtained from the integrated emission over the circular area denoted by the dashed blue line in the 45 km s−1 channel of Figure 9. The solid gray line represents the line spectrum from the SiO data with a velocity resolution of 1.0 km s−1. The solid orange line is the result of a Gaussian fitting with multiple components. The dotted green line corresponds to the systemic velocity of 10.5 km s−1. These SiO data contain the frequency channels with an LSR velocity from −36 to 45 km s−1.
Paper: Secondary Outflow Driven by the Protostar Ser-emb 15 in Serpens
Authors: Asako Sato, Kazuki Tokuda, Masahiro N. Machida, Kengo Tachihara, Naoto Harada, Hayao Yamasaki, Shingo Hirano, Toshikazu Onishi, Yuko Matsushita
Figure caption: SiO(J = 5–4) channel map in the LSR velocity range from −31 to −20 km s−1. The color scale and black contours represent the SiO emission with a velocity resolution of 1.0 km s−1. The magenta cross is the peak flux position for Source A in the 1.3 mm continuum emission. The black contour levels are [3, 4, 5, 6, 7] × 1σ (1σ = 7.0 mJy beam−1). The synthesized beam for the SiO emission is denoted by the magenta ellipse in the panel in the bottom left corner.
Paper: Secondary Outflow Driven by the Protostar Ser-emb 15 in Serpens
Authors: Asako Sato, Kazuki Tokuda, Masahiro N. Machida, Kengo Tachihara, Naoto Harada, Hayao Yamasaki, Shingo Hirano, Toshikazu Onishi, Yuko Matsushita
Figure caption:  12CO(J = 2–1) channel map in the LSR velocity range from 20 to 60 km s−1. The color scale and black contours represent the CO emission. Each panel is obtained by combining the frequency channels to be in a velocity range of 5.0 km s−1 using the CASA task imrebin. The white cross is the peak flux position for Source A in the 1.3 mm continuum emission. The white contour levels are [3, 5, 7, 10, 12, 15, 17]× 1σ (1σ = 3.0 mJy beam−1). The synthesized beam for the CO emission is denoted by the white ellipse in the panel in the bottom left corner. The color bar on the right side is the same as that in Figure 6.
Paper: Unraveling the Complex Structure of AGN-driven Outflows. VI. Strong Ionized Outflows in Type 1 AGNs and the Outflow Size–Luminosity Relation
Authors: Changseok Kim, Jong-Hak Woo, Rongxin Luo, Aeree Chung, Junhyun Baek, Huynh Anh N. Le, Donghoon Son
Figure caption: BPT maps of all GMOS-IFU targets. The first and second rows are 15 type 2 AGNs from Karouzos et al. (2016a, 2016b), Kang & Woo (2018), and Luo et al. (2019), while the third and fourth rows are type 1 and type 2 AGNs in this study. The color bar demonstrates the ionization source corresponding to each color. The Hα detected region (light blue) is where Hα is detected, but one or more of the other BPT lines are not detected, which is a proxy of the entire emission-line region, while the gray area shows where Hα is also not detected. The kinematic outflow size and its uncertainty are shown as black solid and gray dashed circles, respectively. Note that the last six AGNs in the second row are from Luo et al. (2019) sample, which has no measured outflow sizes due to no or weak outflow components.
Paper: Unraveling the Complex Structure of AGN-driven Outflows. VI. Strong Ionized Outflows in Type 1 AGNs and the Outflow Size–Luminosity Relation
Authors: Changseok Kim, Jong-Hak Woo, Rongxin Luo, Aeree Chung, Junhyun Baek, Huynh Anh N. Le, Donghoon Son
Figure caption: Radial profiles of the ratio between [O III] and stellar velocity dispersion. Light blue points show individual spaxels, while large blue points are error-weighted means of each radial bin. The green horizontal line and shaded region show where the velocity dispersion ratio becomes unity and 1σ error. Kinematic outflow size and its error are plotted as a red vertical line and shaded region. Black vertical lines represent the HWHM of the seeing size. We obtained kinematic outflow sizes of 15 among 16 targets except [6]J074645, which lacks [O III] detected spaxels.
Paper: Unraveling the Complex Structure of AGN-driven Outflows. VI. Strong Ionized Outflows in Type 1 AGNs and the Outflow Size–Luminosity Relation
Authors: Changseok Kim, Jong-Hak Woo, Rongxin Luo, Aeree Chung, Junhyun Baek, Huynh Anh N. Le, Donghoon Son
Figure caption: Mass outflow rate (﹩{\dot{M}}_{\mathrm{out}}﹩) as a function of AGN bolometric luminosity (left) and dust-luminosity-based SFR from CIGALE (right). The dashed lines in each figure indicate where the mass outflow rate becomes a factor of 100, 10, 1, 0.1, and 0.01 of the mass accretion rate (radiative efficiency η is assumed to be 0.1) and 1, 0.1, 0.01, and 0.001 of the SFR.
Paper: Unraveling the Complex Structure of AGN-driven Outflows. VI. Strong Ionized Outflows in Type 1 AGNs and the Outflow Size–Luminosity Relation
Authors: Changseok Kim, Jong-Hak Woo, Rongxin Luo, Aeree Chung, Junhyun Baek, Huynh Anh N. Le, Donghoon Son
Figure caption: Outflow size–[O III] luminosity relation (R out—L [O III] relation) plot of the total sample. Blue and red markers indicate GMOS-IFU type 1 and type 2 samples, and star markers are the targets from this study. Magenta squares are SNIFS type 2 AGN samples from Luo et al. (2021). The dashed line is the best-fit relation from the total sample (75 AGNs, slope ∼0.22), and the solid line is the best-fit using only GMOS-IFU targets (38 AGNs, slope ∼0.29).
Paper: Unraveling the Complex Structure of AGN-driven Outflows. VI. Strong Ionized Outflows in Type 1 AGNs and the Outflow Size–Luminosity Relation
Authors: Changseok Kim, Jong-Hak Woo, Rongxin Luo, Aeree Chung, Junhyun Baek, Huynh Anh N. Le, Donghoon Son
Figure caption: Left: R out–R NLR comparison plot. The black dashed line shows the one-to-one relation. Right: the photoionization size–[O III] luminosity plot for the GMOS-IFU targets. The black solid line shows the best-fit relation (slope ∼0.33).
Paper: Unraveling the Complex Structure of AGN-driven Outflows. VI. Strong Ionized Outflows in Type 1 AGNs and the Outflow Size–Luminosity Relation
Authors: Changseok Kim, Jong-Hak Woo, Rongxin Luo, Aeree Chung, Junhyun Baek, Huynh Anh N. Le, Donghoon Son
Figure caption: Bolometric luminosity dependency of ﹩{\dot{P}}_{\mathrm{out}}﹩ (left) and ﹩{\dot{E}}_{\mathrm{out}}﹩ (right). Dashed lines show the comparisons with bolometric luminosity.
Paper: Unraveling the Complex Structure of AGN-driven Outflows. VI. Strong Ionized Outflows in Type 1 AGNs and the Outflow Size–Luminosity Relation
Authors: Changseok Kim, Jong-Hak Woo, Rongxin Luo, Aeree Chung, Junhyun Baek, Huynh Anh N. Le, Donghoon Son
Figure caption: Stellar mass–SFR relation. Solid and dashed lines represent the SFMS line and its 1σ distribution from Noeske et al. (2007). Strong outflow AGNs in this study and Kang & Woo (2018) are located on or above the SFMS line, which implies no evidence of instantaneous quenching.
Paper: Unraveling the Complex Structure of AGN-driven Outflows. VI. Strong Ionized Outflows in Type 1 AGNs and the Outflow Size–Luminosity Relation
Authors: Changseok Kim, Jong-Hak Woo, Rongxin Luo, Aeree Chung, Junhyun Baek, Huynh Anh N. Le, Donghoon Son
Figure caption: Velocity maps of the [O III] core (top) and wing (bottom) components.
Paper: Unraveling the Complex Structure of AGN-driven Outflows. VI. Strong Ionized Outflows in Type 1 AGNs and the Outflow Size–Luminosity Relation
Authors: Changseok Kim, Jong-Hak Woo, Rongxin Luo, Aeree Chung, Junhyun Baek, Huynh Anh N. Le, Donghoon Son
Figure caption: Velocity maps of the Hα core (top) and wing (bottom) components.
Paper: Disk Cooling and Wind Lines as Seen in the Spectral Line Evolution of V960 Mon
Authors: Adolfo Carvalho, Lynne Hillenbrand, Jerome Seebeck
Figure caption: The HIRES spectra shown in a time series, with bluer to redder spectra indicating earlier to later epochs. The lower set of curves in each panel are the residuals after subtracting the disk model appropriate to each epoch. See Figures 2–4 of Paper I for a direct comparison between the outburst epoch spectrum (bluest line here) and the disk model. Strong excess absorption in certain lines (marked) is attributed to wind contributions in the spectra; see Section 5. Outside of these lines, the typical rms value of the residuals is <3%. The remaining 28 orders are shown in Appendix C.
Paper: Disk Cooling and Wind Lines as Seen in the Spectral Line Evolution of V960 Mon
Authors: Adolfo Carvalho, Lynne Hillenbrand, Jerome Seebeck
Figure caption: The effect of varying ﹩\dot{M}﹩ and R inner on the width and depth of absorption lines with different EPs. Left: models of the Ca I λ6439 (upper panel) and Si II λ6347 (lower panel) lines for different values of ﹩\dot{M}﹩. Notice the Ca I λ6439 line broadens as ﹩\dot{M}﹩ decreases, whereas the Si II λ6347 line only changes in depth. Right: models of the same two lines for different values of R inner. Notice here that the T max-dependent broadening still dominates in the Ca I line as R inner decreases, making the line counterintuitively broader. However, in Si II, the broadening decreases with increasing R inner, as expected due to the decrease in the maximum Keplerian velocity.
Paper: Disk Cooling and Wind Lines as Seen in the Spectral Line Evolution of V960 Mon
Authors: Adolfo Carvalho, Lynne Hillenbrand, Jerome Seebeck
Figure caption: The EW evolution (black squares) of two higher-EP and two lower-EP lines in the spectrum of V960 Mon. The AAVSO V-band lightcurve is plotted (green points) for reference, showing the evolution of the continuum brightness over the spectral epochs. Left column: the evolution of the λ5316 Fe II line and λ8862 HP EWs, which both closely follow the lightcurve of the target in their decreasing strength. The EW measurement for the λ8862 HP line is blended with the Fe I λ8866 line, but the Fe I line does not vary in time. Right column: the evolution of the λ5328 Fe I line and λ6439 Ca I line, where both follow an inverse trend to the lightcurve in their growth, similarly strengthening as the target fades and plateaus at later times.
Paper: Disk Cooling and Wind Lines as Seen in the Spectral Line Evolution of V960 Mon
Authors: Adolfo Carvalho, Lynne Hillenbrand, Jerome Seebeck
Figure caption: The Ca I λ6439 (upper profiles) and Si II λ6347 (lower profiles) absorption lines shown for the different epochs of the HIRES spectra. Notice the Si II line becomes narrower, in addition to weaker, consistent with an increase in R inner, while the broadening of the Ca I line remains relatively unchanged.
Paper: Disk Cooling and Wind Lines as Seen in the Spectral Line Evolution of V960 Mon
Authors: Adolfo Carvalho, Lynne Hillenbrand, Jerome Seebeck
Figure caption: The HWHD measurements of several isolated absorption lines in the HIRES outburst (2014 December 9) spectrum (black) and the spectral model (red). Empty symbols show lines that are isolated and easily measured in the data but appear severely blended in the models. Although there are some line-by-line inconsistencies (largely due to imperfections in the PHOENIX models), neither set of measurements is significantly correlated with wavelength. The data and the disk model also have similar standard deviations and the scatter in the HWHD measurements does not vary with wavelength. The error bars shown reflect the uncertainty in the width parameter fit used to compute the HWHD measurements.
Paper: Disk Cooling and Wind Lines as Seen in the Spectral Line Evolution of V960 Mon
Authors: Adolfo Carvalho, Lynne Hillenbrand, Jerome Seebeck
Figure caption: The epochs of our HIRES spectra are shown (vertical solid lines) relative to the AAVSO B (black circles) and Gaia BP (gray connected points) lightcurves of V960 Mon. The lightcurve illustrates the rapid postoutburst fading and eventual plateauing in later epochs. The quiescent B magnitude reported in Kóspál (2015) is shown as the black horizontal line for reference. The 2014 December 10 HIRES epoch is marked with a dotted–dashed line due to overlap with the 2014 December 9 epoch.
Paper: Unraveling the Complex Structure of AGN-driven Outflows. VI. Strong Ionized Outflows in Type 1 AGNs and the Outflow Size–Luminosity Relation
Authors: Changseok Kim, Jong-Hak Woo, Rongxin Luo, Aeree Chung, Junhyun Baek, Huynh Anh N. Le, Donghoon Son
Figure caption: Velocity dispersion maps of [O III] core (top) and wing (bottom) components.
Paper: Unraveling the Complex Structure of AGN-driven Outflows. VI. Strong Ionized Outflows in Type 1 AGNs and the Outflow Size–Luminosity Relation
Authors: Changseok Kim, Jong-Hak Woo, Rongxin Luo, Aeree Chung, Junhyun Baek, Huynh Anh N. Le, Donghoon Son
Figure caption: Velocity dispersion maps of Hα core (top) and wing (bottom) components.
Paper: Magnetized Accretion Disks with Outflows for Changing-look AGNs
Authors: Wen-Biao Wu, Wei-Min Gu
Figure caption: The variations of the accretion timescale with mass under the λ = 1, l = 2, α = 0.01 ∼ 0.3, L bol/L Edd = 0.001 ∼ 0.1. The meaning of the colors and symbols is the same as in Figure 2. For the standard thin disks, the accretion timescale is much larger than the observed timescale. Magnetically dominated viscous disks only explain part of the CL-AGNs. However, our model (magnetically dominated viscous disks with outflows) can naturally explain all the observed sources.
Paper: A Spectroscopic Survey of Lyα Emitters and Lyα Luminosity Function at Redshifts 3.7 and 4.8
Authors: Weiyang Liu, Linhua Jiang
Figure caption: Same as Figure 4, but for all z ∼ 4.8 LAEs selected with narrow band NB704. Objects without B, V, and ﹩z^{\prime} ﹩ images are in the SDFn.
Paper: A Spectroscopic Survey of Lyα Emitters and Lyα Luminosity Function at Redshifts 3.7 and 4.8
Authors: Weiyang Liu, Linhua Jiang
Figure caption: Same as Figure 4, but for all z ∼ 4.8 LAEs selected with narrow band NB711. Objects without B, V, and ﹩z^{\prime} ﹩ images are in the SDFn.
Paper: A Spectroscopic Survey of Lyα Emitters and Lyα Luminosity Function at Redshifts 3.7 and 4.8
Authors: Weiyang Liu, Linhua Jiang
Figure caption: Same as Figure 3, but for all LAEs at z ∼ 3.7 with 270 lines mm−1 grating spectra.
Paper: Multiwavelength Observations of a B-class Flare Using XSM, AIA, and XRT
Authors: Yamini K. Rao, B. Mondal, Giulio Del Zanna, N. P. S. Mithun, S. V. Vadawale, K. K. Reeves, Helen E. Mason, Anil Bhardwaj
Figure caption: The temporal evolution of temperature using AIA (blue asterisk), XRT (green squares), and XSM (red and pink points). The red points represent the flaring plasma temperature obtained from a two-temperature fit of the XSM spectra, where the gray dashed line represents the temperature of the background AR. The pink triangular points represent the emission-measure-weighted temperature obtained from the cool and hot components of the flaring plasma while considering three-temperature components to the XSM spectra (see the text for details) The gray plot indicates the XSM light curve.
Paper: Multiwavelength Observations of a B-class Flare Using XSM, AIA, and XRT
Authors: Yamini K. Rao, B. Mondal, Giulio Del Zanna, N. P. S. Mithun, S. V. Vadawale, K. K. Reeves, Helen E. Mason, Anil Bhardwaj
Figure caption: Left panel: the variation of column EM with respect to temperature at the flare peak time from the full disk (excluding the limb) averaged over 3 minute intervals during the flare peak time (14:14–14:17 UT). Right panel: the variation of volume EM with respect to temperature at the flare peak time from the full disk (excluding the limb) averaged over 3 minute intervals during the flare peak time (14:14–14:17 UT). These values are used as an input to simulate the XSM spectra since the XSM provides full-disk emission signal. The size of temperature bins for both the plots is log T [K] = 0.1.
Paper: Multiwavelength Observations of a B-class Flare Using XSM, AIA, and XRT
Authors: Yamini K. Rao, B. Mondal, Giulio Del Zanna, N. P. S. Mithun, S. V. Vadawale, K. K. Reeves, Helen E. Mason, Anil Bhardwaj
Figure caption: Evolution of the loop structures observed in the 94 Å channel of SDO/AIA.
Paper: Multiwavelength Observations of a B-class Flare Using XSM, AIA, and XRT
Authors: Yamini K. Rao, B. Mondal, Giulio Del Zanna, N. P. S. Mithun, S. V. Vadawale, K. K. Reeves, Helen E. Mason, Anil Bhardwaj
Figure caption: Left panel: simulated spectra from CHIANTI corresponding to the Be-thin filter of XRT using photospheric abundances. Right panel: simulated spectra from CHIANTI corresponding to the Be-thin filter of XRT using coronal abundances.