adsabs/AstroCLIMB huggingface dataset:
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Broadband colors (logarithmic, adjacent bands) predicted by the new pop-cosmos generative model, compared to COSMOS2020 (J. R. Weaver et al. 2022) for Ch. 1 < 26.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Broadband magnitudes (logarithmic) predicted by the new pop-cosmos generative model, compared to COSMOS2020 (J. R. Weaver et al. 2022) for Ch. 1 < 26.
Paper: Very Bright, Very Blue, and Very Red: JWST CAPERS Analysis of Highly Luminous Galaxies with Extreme Ultraviolet Slopes at z = 10
Authors: Callum T. Donnan, Mark Dickinson, Anthony J. Taylor, Pablo Arrabal Haro, Steven L. Finkelstein, Thomas M. Stanton, Intae Jung, Casey Papovich, Hollis B. Akins, Anton M. Koekemoer, Derek J. McLeod, Lorenzo Napolitano, Ricardo O. Amorín, Ryan Begley, Denis Burgarella, Adam C. Carnall, Caitlin M. Casey, Antonello Calabrò, Fergus Cullen, James S. Dunlop, Richard S. Ellis, Vital Fernández, Mauro Giavalisco, Michaela Hirschmann, Weida Hu, Garth Illingworth, Jeyhan S. Kartaltepe, Dale D. Kocevski, Vasily Kokorev, Ho-Hin Leung, Ray A. Lucas, Alexa M. Morales, Ross McLure, Laura Pentericci, Pablo G. Pérez-González, Rachel S. Somerville, Struan Stevenson, Jonathan R. Trump, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: PYNEB models for pure hydrogen nebular continuum at a fixed electron density ne = 1000 cm−3 and varying temperature Te, normalized to match the spectrum of EGS-25297 at 2350 Å in the rest frame. All models predict large Balmer “jumps” at 3646 Å that are not observed for EGS-25297. Models with higher ne and large Te (not shown here) predict UV-continuum slopes that are too red compared to the observations. The two-photon continuum component of the high-temperature nebular models does not match the shape of the observed continuum at λ < 1400  Å.
Paper: Very Bright, Very Blue, and Very Red: JWST CAPERS Analysis of Highly Luminous Galaxies with Extreme Ultraviolet Slopes at z = 10
Authors: Callum T. Donnan, Mark Dickinson, Anthony J. Taylor, Pablo Arrabal Haro, Steven L. Finkelstein, Thomas M. Stanton, Intae Jung, Casey Papovich, Hollis B. Akins, Anton M. Koekemoer, Derek J. McLeod, Lorenzo Napolitano, Ricardo O. Amorín, Ryan Begley, Denis Burgarella, Adam C. Carnall, Caitlin M. Casey, Antonello Calabrò, Fergus Cullen, James S. Dunlop, Richard S. Ellis, Vital Fernández, Mauro Giavalisco, Michaela Hirschmann, Weida Hu, Garth Illingworth, Jeyhan S. Kartaltepe, Dale D. Kocevski, Vasily Kokorev, Ho-Hin Leung, Ray A. Lucas, Alexa M. Morales, Ross McLure, Laura Pentericci, Pablo G. Pérez-González, Rachel S. Somerville, Struan Stevenson, Jonathan R. Trump, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: A comparison of the AV derived from the Balmer line ratios of Hγ/Hδ, Hβ/Hγ, and Hβ/Hδ for EGS-25297 (assuming a J. A. Cardelli et al. 1989 attenuation curve), to the value derived from SED fitting with BAGPIPES.
Paper: Very Bright, Very Blue, and Very Red: JWST CAPERS Analysis of Highly Luminous Galaxies with Extreme Ultraviolet Slopes at z = 10
Authors: Callum T. Donnan, Mark Dickinson, Anthony J. Taylor, Pablo Arrabal Haro, Steven L. Finkelstein, Thomas M. Stanton, Intae Jung, Casey Papovich, Hollis B. Akins, Anton M. Koekemoer, Derek J. McLeod, Lorenzo Napolitano, Ricardo O. Amorín, Ryan Begley, Denis Burgarella, Adam C. Carnall, Caitlin M. Casey, Antonello Calabrò, Fergus Cullen, James S. Dunlop, Richard S. Ellis, Vital Fernández, Mauro Giavalisco, Michaela Hirschmann, Weida Hu, Garth Illingworth, Jeyhan S. Kartaltepe, Dale D. Kocevski, Vasily Kokorev, Ho-Hin Leung, Ray A. Lucas, Alexa M. Morales, Ross McLure, Laura Pentericci, Pablo G. Pérez-González, Rachel S. Somerville, Struan Stevenson, Jonathan R. Trump, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: The 1D spectra of EGS-25297 from the CAPERS reduction (black) and from the DJA (red), which extends the spectrum out to λobserved = 5.5 μm. The inset panel shows the best-fitting Gaussian models (blue) to the emission lines at λ > 5.3 μm.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Stellar mass vs. redshift for Ch. 1 < 26. Cells are shaded by (left) model galaxy count and (right) median AGN bolometric luminosity fraction, fAGN. Cells are shaded only if they contain >10 model galaxies from the total sample of two million. The black and gray dashed lines show, respectively, the mass completeness limit and upper mass limit (see Figures 8 and 27, and Appendix E). Solid, dashed, and dashed–dotted yellow lines show, respectively, the 50th, 84th, and 97.5th percentiles of ﹩{\mathrm{log}}_{10}(M/{M}_{\odot })﹩ given z (same as Figure 8).
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Star-forming main sequence predicted by pop-cosmos. The solid red line shows the rolling median SFR (units of M⊙ yr−1) conditional on stellar mass. Red shaded regions show the rolling 68% and 95% credible intervals. Rolling quantities are computed in a stellar mass window of width ﹩\delta {\mathrm{log}}_{10}(M/{M}_{\odot })=0.4﹩ dex. The mass limits from Figure 11 are applied and indicated with vertical dashed lines. The overlaid cyan lines show the median and 68% interval for the subset of star-forming model galaxies with ﹩{\mathrm{log}}_{10}(\rm{sSFR}\,/{\,\rm{yr}}^{-1})\gt -11﹩. The overlaid green line shows the double power law from J. Leja et al. (2022).
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Stellar mass–metallicity relation (red) predicted by pop-cosmos in the redshift bins from Figure 12, for galaxies with Ch. 1 < 26. The gas-phase metallicity vs. stellar mass relation is overlaid in cyan. Overlaid in green in the first panel, we show the A. Gallazzi et al. (2005, hereafter G05) stellar metallicity vs. mass relation (median and 68% interval) based on Sloan Digital Sky Survey (SDSS) spectra. In the second panel, the green shows the z ∼ 0.7 results from A. Gallazzi et al. (2014, hereafter G14).
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Observer-frame color vs. redshift relations, for (left) g − r and (right) r − i, predicted by pop-cosmos for Ch. 1 < 26. The cell in each panel is shaded only if it contains >100 model galaxies (0.005% of the full mock catalog), and galaxies are only included above the mass completeness limit. Panels are shaded by (row 1) model galaxy count; (row 2) median ﹩{\mathrm{log}}_{10}({\rm{SFR}}\,/{M}_{\odot }{\,\rm{yr}}^{-1})﹩; (row 3) median ﹩{\mathrm{log}}_{10}(M/{M}_{\odot })﹩; (row 4) diffuse dust optical depth at 5500 Å, τ2; and (row 5) median AGN bolometric luminosity fraction, fAGN.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Median star-forming sequence predictions from Figure 12 for (left) all galaxies and (right) galaxies with ﹩{\mathrm{log}}_{10}(\,\rm{sSFR}\,)\gt -11﹩. The black dashed lines show constant sSFR; top to bottom these correspond to ﹩{\mathrm{log}}_{10}(\rm{sSFR}\,/{\,\rm{yr}}^{-1})=[-8,-9,-10,-11]﹩.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: FMR for Ch. 1 galaxies at 0.0 < z < 3.2, visualized in the style of M. Curti et al. (2020). Mock galaxies drawn from the generative model are binned by stellar mass and SFR, with the cells shaded by the median gas-phase metallicity. Cells are shaded only if they contain >100 model galaxies.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Diffuse dust attenuation τ2 vs. (left) stellar mass and (right) SFR, as predicted by pop-cosmos for galaxies with Ch. 1 < 26.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Median mass–metallicity relations predicted by pop-cosmos in the redshift bins from Figure 14. We show the predictions for (left) the r < 25 selection, (right) the Ch. 1 < 26 selection, (top) the stellar metallicity, and (bottom) the gas-phase metallicity.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Redshift evolution of the observer-frame (left) g − r and (right) r − i color distributions predicted by pop-cosmos. Histograms are plotted for the Ch. 1 < 26 mock catalog, with the r < 25 portion of this catalog shaded in yellow.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Marginals of the pop-cosmos population distribution over SPS parameters for (top triangle, yellow) r < 25, and (bottom triangle, red) Ch. 1 < 26. Contours enclose the 68% and 95% highest probability density regions.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Flux uncertainty (microjanskys, logarithmic axes) vs. magnitude (logarithmic) for the COSMOS broad bands, compared to the flux errors reported in COSMOS2020 for r < 25. Contours enclose the 68% and 95% highest-density regions.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Broadband colors (logarithmic, A24 band combinations) predicted by the new pop-cosmos generative model, compared to COSMOS2020 (J. R. Weaver et al. 2022) for r < 25. Contours enclose the 68% and 95% highest-density regions.
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Narrow- and intermediate-band colors from pop-cosmos compared to COSMOS2020 (J. R. Weaver et al. 2022).
Paper: pop-cosmos: Insights from Generative Modeling of a Deep, Infrared-selected Galaxy Population
Authors: Stephen Thorp, Hiranya V. Peiris, Gurjeet Jagwani, Sinan Deger, Justin Alsing, Boris Leistedt, Daniel J. Mortlock, Anik Halder, Joel Leja
Figure caption: Narrow- and intermediate-band magnitudes from pop-cosmos vs. COSMOS2020 (J. R. Weaver et al. 2022).
Paper: The Accretion Disk Size Problem in AGN Disk Reverberation Mapping Is an Obscuration Effect: A Uniform AGN Sample Study with Swift
Authors: Collin Lewin, Erin Kara, Christos Panagiotou, Edward M. Cackett, Jonathan Gelbord, Juan V. Hernández Santisteban, Keith Horne, Gerard A. Kriss
Figure caption: Best-fit lag normalizations (τ0), corresponding to the dashed black curves in Figure 3, plotted against ﹩{M}^{2}\dot{m}﹩. The orange dashed line shows the predicted scaling ﹩{\tau }_{0}\propto {({M}^{2}\dot{m})}^{1/3}﹩, computed from a modified version of Equation (12) in M. M. Fausnaugh et al. (2016), assuming standard disk parameters stated in the text. Most sources lie above the theoretical prediction, highlighting a systematic excess in lag normalizations relative to expectations. However, while the obscured sources are well described by the best-fit relation, the unobscured sources tend to lie closer to the predicted scaling, suggesting that the excess lag normalizations are most significantly driven by the obscured population.
Paper: The Accretion Disk Size Problem in AGN Disk Reverberation Mapping Is an Obscuration Effect: A Uniform AGN Sample Study with Swift
Authors: Collin Lewin, Erin Kara, Christos Panagiotou, Edward M. Cackett, Jonathan Gelbord, Juan V. Hernández Santisteban, Keith Horne, Gerard A. Kriss
Figure caption: Normalization excesses—defined as the ratio of the measured lag normalization to the predicted value—for each AGN in the sample. Dotted lines indicate the sample means for each unobscured and obscured subgroup, with shaded bands denoting the standard error of the mean. The full sample has a mean excess of 3.45  ±  0.27, with the obscured subgroup showing a larger average excess (5.21  ±  0.47) than the unobscured group (1.00  ±  0.31). A similar trend is observed in the U-band lag excesses on their own. Hypothesis testing confirms that the excesses in the full and obscured samples are significantly greater than 1 (p = 0.011 and p = 0.008, respectively), while the unobscured group (as expected) shows no significant deviation from theoretical expectations (p = 0.50). The one super-Eddington source (Mrk 142) occupies a distinct region of the parameter space.
Paper: The Accretion Disk Size Problem in AGN Disk Reverberation Mapping Is an Obscuration Effect: A Uniform AGN Sample Study with Swift
Authors: Collin Lewin, Erin Kara, Christos Panagiotou, Edward M. Cackett, Jonathan Gelbord, Juan V. Hernández Santisteban, Keith Horne, Gerard A. Kriss
Figure caption: Spearman’s rank correlation matrix among key parameters in the sample, including black hole mass, accretion rate, normalization excess, X-ray-to-UV lag, column density (NH), fractional UVW2 rms variability, optical-to–X-ray spectral slope (αox), and maximum correlation coefficients (﹩{R}_{{\rm{\max }}}﹩). In order to assess which correlations reflect real associations rather than occurring by chance, we computed p-values using a permutation test: one variable in each pair was randomly shuffled many times to build the distribution of correlations expected under the null hypothesis of no relationship. Black dashed outlines highlight boxes for correlations that are statistically significant at the α = 0.05 level, corresponding to ∣ρ∣ ≥ 0.61.
Paper: The Accretion Disk Size Problem in AGN Disk Reverberation Mapping Is an Obscuration Effect: A Uniform AGN Sample Study with Swift
Authors: Collin Lewin, Erin Kara, Christos Panagiotou, Edward M. Cackett, Jonathan Gelbord, Juan V. Hernández Santisteban, Keith Horne, Gerard A. Kriss
Figure caption: Relationships between X-ray/UV timing properties and physical parameters. Left: X-ray-to-UV (UVW2, 1928 Å) lag amplitude vs. column density (NH). The obscured subgroup exhibits notably larger scatter in lag amplitude compared to unobscured sources. Middle: maximum linear correlation between the X-ray and UVW2 light curves (﹩{R}_{{\rm{\max }}}^{{\rm{X}}-{\rm{ray}}}﹩) vs. column density. Right: ﹩{R}_{{\rm{\max }}}^{{\rm{X}}-{\rm{ray}}}﹩ vs. the optical-to–X-ray spectral slope (αox). These plots explore whether the coherence between the X-ray and UV emission—and the lag between them—depends on absorption or accretion properties.
Paper: The Accretion Disk Size Problem in AGN Disk Reverberation Mapping Is an Obscuration Effect: A Uniform AGN Sample Study with Swift
Authors: Collin Lewin, Erin Kara, Christos Panagiotou, Edward M. Cackett, Jonathan Gelbord, Juan V. Hernández Santisteban, Keith Horne, Gerard A. Kriss
Figure caption: Measured interband lags as a function of wavelength using the ICCF approach. The dashed black line shows the best-fit power-law relation, τ ∝ λ4/3, with the normalization treated as a free parameter. The orange dotted line shows the same relation, but with the normalization instead predicted from a standard accretion disk given the black hole mass and accretion rate of each source. As such, the differences between these measured and predicted curves reflect departures from theoretical expectations (the “normalization excess”).
Paper: The Accretion Disk Size Problem in AGN Disk Reverberation Mapping Is an Obscuration Effect: A Uniform AGN Sample Study with Swift
Authors: Collin Lewin, Erin Kara, Christos Panagiotou, Edward M. Cackett, Jonathan Gelbord, Juan V. Hernández Santisteban, Keith Horne, Gerard A. Kriss
Figure caption: Per-source Swift X-ray spectra (0.3–10 keV), with unobscured spectra in pink and obscured spectra in green. For Mrk 817 and Fairall 9, two epochs are overplotted. Pink spectra exhibit smooth, power-law-like continua, whereas green spectra show pronounced curvature (particularly ∼1–4 keV) characteristic of absorption along the line of sight.
Paper: The Accretion Disk Size Problem in AGN Disk Reverberation Mapping Is an Obscuration Effect: A Uniform AGN Sample Study with Swift
Authors: Collin Lewin, Erin Kara, Christos Panagiotou, Edward M. Cackett, Jonathan Gelbord, Juan V. Hernández Santisteban, Keith Horne, Gerard A. Kriss
Figure caption: U-band excess as a function of X-ray column density. Dotted lines indicate the sample means for each unobscured and obscured subgroup, with shaded bands denoting the standard error of the mean. The mean excess is 5.30  ±  0.49 across the full sample, 7.70  ±  0.96 in the obscured subgroup, and 1.63  ±  0.76 in the unobscured subgroup. Like the full normalization excess, only the unobscured subgroup reveals no significant deviation from theoretical expectations (p = 0.012 for the obscured group vs. p = 0.36 for the unobscured group).
Paper: Simulating Propagation of a Coronal Mass Ejection from Solar Corona to 1 au with the Alfvén Wave Solar Atmosphere Model and Fitting of Gibson–Low
Authors: Xinghua Dai
Figure caption: Grid refinement in the steady sate of SC and IH components on the xy and xz planes, along with the field of velocity. The direction and location of STA are marked by an arrow and a sphere in the SC and IH, respectively. Magnetic lines are also shown in the xy plane, which is also the solar equatorial plane.
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: Comparisons of the Hα and Hβ spectra between the observation (black solid lines, the quiescent phase component subtracted spectra at time [4] of Flare 23 taken from Figures 15 and 16) and modeling results (colored). The observed spectra correspond to the peaks of line broadenings during Flare 23 (see Figure 14), and the normalizations of the line center intensities are done with the Gaussian fitting around the line center components (for the range of ±150 km s−1 for Hα and ±200 km s−1 for Hβ, respectively). The modeling results, which are normalized where the line emission is largest considering the existence of the central reversal components, correspond to the time-averaged spectra from the M dwarf RHD calculation results provided in A. F. Kowalski et al. (2024a) (see the main text of Section 5.5 for more details). The error bars and shaded ranges correspond to the 1σ error of the above Gaussian fittings to the observed line peak intensities around the line centers. The modeling cases of 5F12-37-3 are plotted twice in (a)–(d), so that the comparisons of different model cases become easier.
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: (a) Line profiles of the Hα emission line during Flare 65 on 2018 October 24 from the CHIRON spectra. The horizontal and vertical axes represent the wavelength and flux normalized by the continuum. The gray vertical dashed lines with velocity values represent the Doppler velocities from the Hα line center. The red solid and blue dashed lines indicate the line profiles at the time [1] and time [2], respectively, which are indicated in Figure 22(a) and (b) (lightcurve and intensity map) and are during Flare 65. The black dotted line indicates the line profiles in quiescent phase, which is the average profile during −0.10 to +0.37 hr on this date (see Figure 22(a)). (e) and (i) Same as panel (a), but the line profiles at time [3]–time [6] during Flare 65. (b), (f), and (j) Same as panels (a), (e), and (i), respectively, but the line profile differences from the quiescent phase. (c), (d), (g), (h), (k), and (l) Same as panels (a), (b), (e), (f), (i), and (j), respectively, but for the Hβ line.
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: Same as Figure 15, the He I D3 5876 Å and Na D1 and D2 lines.
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: Same as Figure 15, the Ca II 8542 Å line.
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: The PN and MOS1 spectra and best-fit model result for rise and decay phase data of Flares 35 and 36 (see Figure 18), which are plotted in the same way as in Figure 11.
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: The PN and MOS1 spectra and best-fit model result for the Phases No. 1–No. 4 (see Figure 17) of Flare 11. The data and fit results are plotted in the same way as in Figures 11 and 34.
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: Same as Figure 34, but the Phases No. 5–No. 8 (see Figure 13).
Paper: A Seven-day Multiwavelength Flare Campaign on AU Mic. III. Quiescent and Flaring Properties of the X-Ray Spectra and Chromospheric Lines
Authors: Yuta Notsu, Isaiah I. Tristan, Rachel A. Osten, Alexander Brown, Adam F. Kowalski, Carol A. Grady
Figure caption: Same as Figure 34, but the Phases No. 9–No. 12 (see Figure 13).