adsabs/AstroCLIMB huggingface dataset:
Paper: In the Trenches of the Solar–Stellar Connection. VI. Total EclipSS
Authors: Thomas Ayres, Derek Buzasi
Figure caption: Merged, coadded COS G130M+G160M spectrum of HD 24636. The y-axis is the bolometrically normalized flux density. Tracing for λ < 1430 Å is from Paper III. Local fluxes at the airglow lines (yellow shading) were based on G130M splits displaying minimal contamination. The current program added a G160M-1533 spectrum, overlapping the original G130M between 1340–1430 Å. Individual CENWAVEs are depicted in blue (1222), red (1291), and green (1533). The combined spectrum is the dark curve, slightly smoothed to reveal the underlying spectral contributions more clearly. The thin dotted–dashed line below the spectrum is the 1 σ  λ  photometric error, heavily smoothed for display purposes.
Paper: In the Trenches of the Solar–Stellar Connection. VI. Total EclipSS
Authors: Thomas Ayres, Derek Buzasi
Figure caption: Merged, coadded COS G130M-1222 + G160M-1533 spectrum of ξ Boo A. CENWAVE 1222 is in blue, and CENWAVE 1533 is in red. The dark curve is the slightly smoothed merged spectrum. The thin dotted–dashed trace is the heavily filtered 1σ photometric error.
Paper: In the Trenches of the Solar–Stellar Connection. VI. Total EclipSS
Authors: Thomas Ayres, Derek Buzasi
Figure caption: Rogues gallery of the Chandra HRC-I pointings on the EclipSS subsample (upper two rows), and several of the reference stars (bottom row). Individual maps are 20″ on a side, and the X-ray events were binned into 0.″25 pixels. The reverse gray scale saturates at 5 count px−1. Exposures were 5–10 ks. The r = 1.″5 detect cells (95% encircled energy) are marked in red.
Paper: A Catalog of Quasar Properties from Sloan Digital Sky Survey Data Release 16
Authors: Qiaoya Wu, Yue Shen
Figure caption: Distribution of DR16Q quasars in the C IV equivalent width vs. C IV blueshift (with respect to systemic) plane.
Paper: In the Trenches of the Solar–Stellar Connection. VI. Total EclipSS
Authors: Thomas Ayres, Derek Buzasi
Figure caption: Additional examples of spectral fits for STIS and COS pointings on reference stars from specific epochs (rather than epoch-average spectra illustrated routinely in previous papers of this series). See Figure 10 caption for details. For the STIS spectra, highlighted points (dark dots) represent only every third native wavelength bin. (a) α Cen A (STIS: 2011 May); (b) α Cen B (STIS: 2011 May); (c) Procyon (STIS: 2011 April); (d) ϵ Eri (STIS: 2000 March; compare with COS spectrum, Figure 10(c), in the main text); (e) ξ Boo B (COS: 2020 February); and (f) 70 Oph B (COS: 2020 July).
Paper: In the Trenches of the Solar–Stellar Connection. VI. Total EclipSS
Authors: Thomas Ayres, Derek Buzasi
Figure caption: Similar to Figure 15, but now including empirical turnover times derived from Figure 16. The color coding and symbols are the same as in previous figures.
Paper: Detection of δ Scuti Pulsators in the Eclipsing Binaries Observed by TESS
Authors: Xinghao Chen, Xu Ding, Liantao Cheng, Xiaobin Zhang, Yan Li, Kaifan Ji, Jianping Xiong, Xuzhi Li, Changqing Luo
Figure caption: The distribution of the targets in the Hertzsprung–Russell diagram. Newly discovered and old targets are marked with red and blue circles, respectively. The zero-age main sequence line and the evolutionary tracks of eight different initial stellar masses with Z = 0.015 are computed with the one-dimensional stellar evolution code Modules for Experiments in Stellar Astrophysics (MESA; Paxton et al. 2011, 2013, 2015, 2018) using the same input physics as Chen et al. (2021). The green lines represent the instability strip derived by Xiong et al. (2016) and the purple line is the theoretical blue edge of the δ Scuti instability strip derived by Li & Stix (1994). Luminosities L are taken from Gaia DR3, while the values of T eff of the stars are taken from the TIC.
Paper: Detection of δ Scuti Pulsators in the Eclipsing Binaries Observed by TESS
Authors: Xinghao Chen, Xu Ding, Liantao Cheng, Xiaobin Zhang, Yan Li, Kaifan Ji, Jianping Xiong, Xuzhi Li, Changqing Luo
Figure caption: Distribution of the pulsating stars in eclipsing binaries in the P dom–P orb diagram. Newly discovered and old targets are marked with red and blue circles, respectively. The solid line in black is the theoretical relation from Zhang et al. (2013), and the two dashed lines correspond to its 3σ uncertainties. The purple line denotes the upper limit of the P dom/P orb ratio derived by Zhang et al. (2013) for the δ Scuti stars in eclipsing binaries. The systems marked with green and black cross symbols correspond to targets in Figures 6 and 7, respectively.
Paper: Detection of δ Scuti Pulsators in the Eclipsing Binaries Observed by TESS
Authors: Xinghao Chen, Xu Ding, Liantao Cheng, Xiaobin Zhang, Yan Li, Kaifan Ji, Jianping Xiong, Xuzhi Li, Changqing Luo
Figure caption: Light curve, O − C residuals, and amplitude spectrum of TIC 125498216. The light curve is displayed with black circles in the top panel, the O − C residuals are presented in the middle panel, and the amplitude spectra is depicted in the bottom panel. The red line in the top panel denotes the synthesis mean curve. The peaks marked in gray are possible orbital harmonics. The dashed line marks the positions of S/N = 5.
Paper: Detection of δ Scuti Pulsators in the Eclipsing Binaries Observed by TESS
Authors: Xinghao Chen, Xu Ding, Liantao Cheng, Xiaobin Zhang, Yan Li, Kaifan Ji, Jianping Xiong, Xuzhi Li, Changqing Luo
Figure caption: Fourier amplitude spectra of objects TIC 19193162, TIC 141622065, TIC 262958558, TIC 304030311, TIC 431555426, and TIC 449486448, respectively. The dashed lines mark the positions of S/N = 5.
Paper: Detection of δ Scuti Pulsators in the Eclipsing Binaries Observed by TESS
Authors: Xinghao Chen, Xu Ding, Liantao Cheng, Xiaobin Zhang, Yan Li, Kaifan Ji, Jianping Xiong, Xuzhi Li, Changqing Luo
Figure caption: Fourier amplitude spectra for the pulsating components in eclipsing binaries with P orb < 0.65 day. The dashed lines mark the positions of S/N = 5.
Paper: Detection of δ Scuti Pulsators in the Eclipsing Binaries Observed by TESS
Authors: Xinghao Chen, Xu Ding, Liantao Cheng, Xiaobin Zhang, Yan Li, Kaifan Ji, Jianping Xiong, Xuzhi Li, Changqing Luo
Figure caption: The same as in Figure 3, but the values of effective temperature T eff of the stars are taken from the Gaia DR3.
Paper: Detection of δ Scuti Pulsators in the Eclipsing Binaries Observed by TESS
Authors: Xinghao Chen, Xu Ding, Liantao Cheng, Xiaobin Zhang, Yan Li, Kaifan Ji, Jianping Xiong, Xuzhi Li, Changqing Luo
Figure caption: Distribution of the δ Scuti–type pulsating stars in eclipsing binaries within the T eff–ν dom relation. Newly discovered and old targets are marked with red and blue circles, respectively. The black solid line marks the theoretical relation derived by Barceló Forteza et al. (2020), and the dashed lines denote the limits of their predicted dispersion due to the gravity-darkening effect.
Paper: Detection of δ Scuti Pulsators in the Eclipsing Binaries Observed by TESS
Authors: Xinghao Chen, Xu Ding, Liantao Cheng, Xiaobin Zhang, Yan Li, Kaifan Ji, Jianping Xiong, Xuzhi Li, Changqing Luo
Figure caption: Distribution of the dominant pulsation frequencies of δ Scuti pulsators in eclipsing binaries.
Paper: In the Trenches of the Solar–Stellar Connection. VI. Total EclipSS
Authors: Thomas Ayres, Derek Buzasi
Figure caption: Flux–flux diagrams for the Total EclipSS stars. See the text for descriptions of the symbols. Color coding by spectral type is the same as in Figure 1. The fan of dashed lines emanating from the α Cen A points depicts simple power laws with slopes of 0.5, 1, 2, and 3. Square brackets are shorthand for ﹩\mathrm{log}{f}_{{\rm{L}}}/{f}_{\mathrm{BOL}}﹩ for the indicated transitions. In these diagrams, low-activity τ Cet always is the orange symbol at lower left (although absent in the upper-left panel of Figure 13(d)), while hyperactive EK Dra always is the yellow circle at the upper right. (a) Various species vs. chromospheric O I 1306 Å. (b) Various species vs. upper chromosphere C II 1335 Å. (c) High-temperature species vs. low-TZ Si III 1206 Å. (d) High-temperature species vs. mid-TZ C IV 1550 Å. (e) Mixed-temperature species vs. the hybrid XUV flux.
Paper: In the Trenches of the Solar–Stellar Connection. VI. Total EclipSS
Authors: Thomas Ayres, Derek Buzasi
Figure caption: Comparison of various proposed convective turnover times vs. stellar effective temperature. Abbreviated citations in the legend are spelled out in the text. C21 and W11 points are semiempirical; A19 and L10 are based on stellar structure models. The vertical dashed line marks the solar T eff. The dashed boundary curve for A19 refers to metal-rich models ([Fe/H] = +0.3); the dotted–dashed line is for metal-poor models ([Fe/H] = −0.5); and the solid curve in the middle is for solar composition. Small dots of various colors trace how the turnover time evolves during the MS lifetime for different masses and metallicities. Small x’s are equivalent evolution-resolved points for the L10 model grid ([Fe/H] = 0).
Paper: In the Trenches of the Solar–Stellar Connection. VI. Total EclipSS
Authors: Thomas Ayres, Derek Buzasi
Figure caption: Schematic depiction of emission-line profile modeling process. All examples are from COS. The observed spectrum (thin dark curve) in each panel is normalized to a local intensity maximum. The original spectrum was resampled into uniform 0.05 Å bins (∼0.7 resolution element (resel)). The vertical dotted–dashed lines represent laboratory wavelengths in the stellar (photospheric) reference frame. Green dotted curves are smoothed 5σ photometric errors. Orange dashed lines under the emission features represent an adopted background level, based on a long-range continuum model. The background is tilted for O V 1218 Å and Fe XII 1241 Å, to account for wings of nearby stronger emissions. Dark dots highlight specific points included in the pseudo-Gaussian modeling. The fitted profile is illustrated by a red curve. If the model curve is absent, the highlighted intensities above the background level were numerically integrated. (a) HD 24636 (F3); (b) HD 150706 (G0); (c) ϵ Eri (K2: 2017 August); (d) ξ Boo A (G7: 2020 February); and (e) 70 Oph A (K0: 2020 September).
Paper: In the Trenches of the Solar–Stellar Connection. VI. Total EclipSS
Authors: Thomas Ayres, Derek Buzasi
Figure caption: The left and right panels display, respectively, the variation of normalized X-ray fluxes, and hybrid XUV index, vs. stellar rotation period, P ROT. Color coding (here, and in subsequent figures) by spectral type is the same as in Figure 1. Unadorned circles are for the EclipSS subsample and related objects (together, “EclipSS+”). Adorned dots are for the reference stars, according to the legend: “AB P ϵ” refers to α Cen, Procyon, and ϵ Eri. An open circle plus an asterisk for 70 Oph B indicates an uncertain rotation rate. Additional annotations in gray (here, and in subsequent figures) are for low-activity τ Cet (“τ”), medium-activity HD 150706 (“150”), and hyperactive EK Dra (“EK”). Error flags (±1σ), where visible, were based on standard deviations of logarithmic flux ratios over multiepoch time series, if applicable (which, for the X-rays, might involve instrumental intercalibration uncertainties), or simple measurement errors otherwise. The thick dashed curves are schematic expectations for rotation-activity connections.
Paper: In the Trenches of the Solar–Stellar Connection. VI. Total EclipSS
Authors: Thomas Ayres, Derek Buzasi
Figure caption: Comparison of key emission lines of the FUV region. The x-axis scale is relative velocity: each column is ±200 km s−1. The y-axis is the bolometrically normalized flux density. Stars are ordered by spectral type. Major divisions, by which the individual spectra were shifted, are indicated at the lower left. (a) EclipSS subsample (all COS). Red curves and squares highlight the fastest rotators, green curves and diamonds are moderate rotators, and dark or open points are slow rotators. Identifications at the right are by spectral type and the first three digits of the HD number. (b) Related objects (all STIS). Abbreviated star names are noted at the right. The red curve and squares are for fast-rotator EK Dra. The blue curve and diamonds are for low-activity τ Cet (multiplied by 10 to be visible on this scale). (c) Reference stars. Here, color coding highlights STIS objects: α Cen AB (“α A:” blue squares; “α B:” orange diamonds) and Procyon (“Proc:” green diamonds). All of the stars are slow or moderate rotators. Dark and open symbols refer to ϵ Eri and Cycles binaries ξ Boo (“ξ”) and 70 Oph (“70”), all observed by COS.
Paper: In the Trenches of the Solar–Stellar Connection. VI. Total EclipSS
Authors: Thomas Ayres, Derek Buzasi
Figure caption: Blue diamonds trace the X-ray flux ratio (“flux multiplier”), r X ≡ f (0.05−12)/f (0.1−2.4), as a function of X-ray surface flux, ﹩\mathrm{log}{F}_{{\rm{X}}}﹩, calculated from a theoretical temperature-dependent relation folded through the various EMD models (which are designated according to the associated ﹩\mathrm{log}{F}_{{\rm{X}}}﹩). The smooth, red dotted–dashed curve is a parabolic fit to the discrete values. Filled circles refer to the Total EclipSS sample, for which the X-ray flux multiplier was calculated from the smooth fit. Color coding of the spectral types is the same as in Figure 1. Small open circles depict empirical values of solar r X over the years 2000–2020, averaged into 81 day (three rotations) bins. The connected filled boxes refer to stellar (and solar) ratios of the λ > 250 Å “E/FUV” flux contribution relative to the reference 0.1–2.4 keV X-ray intensity. The F stars and G/K dwarfs are separately connected by solid lines owing to their apparently divergent behavior.
Paper: In the Trenches of the Solar–Stellar Connection. VI. Total EclipSS
Authors: Thomas Ayres, Derek Buzasi
Figure caption: Results of modeling TESS light curves of representative members of EclipSS subsample. The image in the upper panel schematically depicts the wavelet analysis. The second panel down is the TESS light curve normalized to its median value (sector by sector). The “time” axis for these two panels is JD–2457000. The third panel down is the wavelet period–amplitude distribution. The lowest panel is the DFT analysis. (a) HD 39755; (b) HD 41004; (c) HD 62850; (d) HD 150706; and (e) HD 180712.
Paper: In the Trenches of the Solar–Stellar Connection. VI. Total EclipSS
Authors: Thomas Ayres, Derek Buzasi
Figure caption: Results of applying the A19                       τ c vs. T eff relation for solar composition to the Total EclipSS sample, then displaying the stellar X-ray (left panel) and XUV (right panel) fluxes against the corresponding Rossby numbers. Symbol marking and color coding are the same as in Figure 14. The thick dashed power law in the left-hand panel, fitted to a subset of the Sunlike stars, has a slope of −2.2.
Paper: In the Trenches of the Solar–Stellar Connection. VI. Total EclipSS
Authors: Thomas Ayres, Derek Buzasi
Figure caption: Merged, coadded COS spectrum of ϵ Eri from a COS-Team wavelength calibration exercise in 2017 August. Individual settings are represented by different colors. The combined spectrum is the darker curve. The thin dark dotted–dashed trace below the spectrum is the smoothed 1σ photometric noise. The deeply exposed, spliced spectrum demonstrates exceptional S/N and dynamic range.
Paper: Multigroup Radiation Magnetohydrodynamics Based on Discrete Ordinates including Compton Scattering
Authors: Yan-Fei Jiang, 燕飞 姜
Figure caption: Spatial and frequency distribution of the monochromatic radiation energy density variations ﹩\delta {E}_{r}(x,\tilde{\nu })﹩ (Equation (47)) at time t = 2 for the bulk Compton test with a convergent–divergent flow described in Section 4.4.3. The variation ﹩\delta {E}_{r}(x,\tilde{\nu })﹩ represents relative fluctuations of ﹩{E}_{r}(x,\tilde{\nu })﹩ scaled by the spatially averaged values for each frequency ﹩\tilde{\nu }﹩. The colormap is symmetric logarithmic, which means positive and negative values of ﹩\delta {E}_{r}(x,\tilde{\nu })﹩ are shown separately in the logarithmic scale of ﹩| \delta {E}_{r}(x,\tilde{\nu })| ﹩.
Paper: Multigroup Radiation Magnetohydrodynamics Based on Discrete Ordinates including Compton Scattering
Authors: Yan-Fei Jiang, 燕飞 姜
Figure caption: Top: absorption opacity coefficient used in the radiating sphere as described in Section 4.2. The frequency-dependent opacity is taken from the tabulated value given by Graziani (2008) for brominated plastic. The total optical depth across the simulation domain for each frequency ﹩\tilde{\nu }﹩ is simply ρ κ  a  times the radial box size 0.03. Bottom: numerical solution (red dots) of the monochromatic radiation energy density in each frequency bin at radius r = 0.04. This is the solution at time t = 5.21 × 10−5. The dashed black line is the analytical solution using the opacity shown in the top panel. Radiation energy density is scaled by ﹩{a}_{r}{T}_{0}^{4}﹩ in this plot.
Paper: Multigroup Radiation Magnetohydrodynamics Based on Discrete Ordinates including Compton Scattering
Authors: Yan-Fei Jiang, 燕飞 姜
Figure caption: Spectra of the radiation energy density E  r,f  scaled by the injected value E  r,0 after the photons pass through the gas with opacity shown in Figure 5 as described in Section 4.3. The black lines show the results when gas is static, while the blue lines in the top and bottom panels show the results when gas has velocity v = 0.05c and v = −0.05c respectively.
Paper: Multigroup Radiation Magnetohydrodynamics Based on Discrete Ordinates including Compton Scattering
Authors: Yan-Fei Jiang, 燕飞 姜
Figure caption: Spectrum of the spatially averaged monochromatic radiation energy density ﹩{E}_{r}(\tilde{\nu })﹩ for the same test as shown in Figure 10. The black and red lines are for the initial blackbody spectrum and spectrum at time t = 2 corresponding to the Compton y parameter 2.76. The dashed green line is a spectrum with Bose–Einstein distribution at the effective temperature ﹩T+{m}_{e}{v}_{m}^{2}/(3{k}_{B})=27.57T﹩, where v  m  = 300 is the amplitude of the sinusoidal velocity used in this test, and gas temperature T = 1 in our unit system. Chemical potential of the distribution is chosen so that total radiation energy density matches the numerical solution at this time.
Paper: Multigroup Radiation Magnetohydrodynamics Based on Discrete Ordinates including Compton Scattering
Authors: Yan-Fei Jiang, 燕飞 姜
Figure caption: Opacity κ  a  used in the test of absorption due to a moving gas described in Section 4.3. The top panel shows the spatial variation of κ  a  at ﹩\tilde{\nu }=0.9﹩ while the bottom panel shows the value of κ  a  in each frequency bin at the location x = 0.496.
Paper: Multigroup Radiation Magnetohydrodynamics Based on Discrete Ordinates including Compton Scattering
Authors: Yan-Fei Jiang, 燕飞 姜
Figure caption: Comparing photon spectra due to Compton scattering without stimulated emission at different times for an initial delta function spectrum at ﹩\tilde{\nu }=1﹩ (Section 4.4.1). The circles are our numerical solutions for different y values while the solid lines are the corresponding analytic solutions given by Becker (2003).
Paper: Multigroup Radiation Magnetohydrodynamics Based on Discrete Ordinates including Compton Scattering
Authors: Yan-Fei Jiang, 燕飞 姜
Figure caption: Thermalization of gas and radiation due to Compton scattering for the test described in Section 4.4.2. The top panel shows the history of gas temperature T and effective radiation temperature ﹩{\left({E}_{r}/{a}_{r}\right)}^{1/4}﹩. The bottom panel shows spectra of the monochromatic radiation energy density at y = 0 and y = 4.29. The dashed line is the analytic solution.
Paper: Multigroup Radiation Magnetohydrodynamics Based on Discrete Ordinates including Compton Scattering
Authors: Yan-Fei Jiang, 燕飞 姜
Figure caption: Spectra of comoving-frame, monochromatic specific intensities with flow velocity 0.134c and isotropic blackbody spectrum in the lab frame. Black and red lines are for intensities propagating along two different directions as indicated in the figure. The black and red squares are numerically estimated comoving-frame specific intensities at the center of each frequency bin based on the frequency-integrated intensities in each bin.
Paper: Multigroup Radiation Magnetohydrodynamics Based on Discrete Ordinates including Compton Scattering
Authors: Yan-Fei Jiang, 燕飞 姜
Figure caption: Gas and effective radiation temperatures in steady state as a function of number of frequency bins N  f  used in the Compton thermalization test described in Section 4.4.2. If we assume the radiation spectrum is blackbody without solving the Kompaneets equation, the gas and radiation temperatures will be the same in steady state, which is showed as the dashed black line T  bd .
Paper: Jupiter and Saturn as Spectral Analogs for Extrasolar Gas Giants and Brown Dwarfs
Authors: Daniel J. Coulter, Jason W. Barnes, Jonathan J. Fortney
Figure caption: Color images of all 12 cubes presented in this study with green mapped to 2.0 μm, red mapped to 5.0 μm, and blue mapped to 2.4 μm. In this color scheme, green represents reflected light, red represents thermal emission, and blue indicates the presence of water. The images of Saturn were created from the cubes before the ring-removal algorithm was implemented. Note the lack of blue in all images except for V1469259344_1, in which Saturn’s rings, primarily composed of water ice, are clearly visible in blue.
Paper: Jupiter and Saturn as Spectral Analogs for Extrasolar Gas Giants and Brown Dwarfs
Authors: Daniel J. Coulter, Jason W. Barnes, Jonathan J. Fortney
Figure caption: Visual representation of the four end members outlined in Section 2.4. Incident solar light (white) can either be reflected by dense clouds (green) or cloudless regions (orange). Thermal emission (red) are either directly emitted or scattered by cloud layers (blue).
Paper: Jupiter and Saturn as Spectral Analogs for Extrasolar Gas Giants and Brown Dwarfs
Authors: Daniel J. Coulter, Jason W. Barnes, Jonathan J. Fortney
Figure caption: Top: disk-integrated spectra of Jupiter in units of flux for six phase angles ranging from 1.°7 to 133.°5. Bottom: same as top, but in units of I/F. Prominent absorption bands are labeled. Absorption bands in the visual and infrared wavelengths are taken from Vdovichenko et al. (2021) and Baines et al. (2005), respectively.(The data used to create this figure are available.)
Paper: Jupiter and Saturn as Spectral Analogs for Extrasolar Gas Giants and Brown Dwarfs
Authors: Daniel J. Coulter, Jason W. Barnes, Jonathan J. Fortney
Figure caption: Top: disk-integrated spectra of Saturn in units of flux for four phase angles ranging from 39.°6 to 110.°2. Due to the nature of Cassini’s orbit around Saturn, full-disk, full-phase spectra were impossible to obtain. Bottom: same as top, but in units of I/F. Once again, prominent absorption bands, courtesy of Vdovichenko et al. (2021) and Baines et al. (2005), are labeled. The data used to generate this figure, as well as for two additional phase angles, can be found in machine-readable format in the online article.(The data used to create this figure are available.)
Paper: Jupiter and Saturn as Spectral Analogs for Extrasolar Gas Giants and Brown Dwarfs
Authors: Daniel J. Coulter, Jason W. Barnes, Jonathan J. Fortney
Figure caption: Top: Saturn end-member spectra obtained from cube V1469259344_1 (see Figure 1). Bottom: same as top but the y-axis has been adjusted to show detail. The features in the nightside spectra in the visible wavelengths are evidence of ring shine from Saturn’s rings.(The data used to create this figure are available.)
Paper: Jupiter and Saturn as Spectral Analogs for Extrasolar Gas Giants and Brown Dwarfs
Authors: Daniel J. Coulter, Jason W. Barnes, Jonathan J. Fortney
Figure caption: Jupiter end-member spectra obtained from cube V1357335218_1 (see Figure 1).(The data used to create this figure are available.)