adsabs/AstroCLIMB huggingface dataset:
Paper: The Active Chromospheres of Lithium-rich Red Giant Stars 
Authors: Christopher Sneden, Melike Afşar, Zeynep Bozkurt, Monika Adamów, Anohita Mallick, Bacham E. Reddy, Steven Janowiecki, Suvrath Mahadevan, Brendan P. Bowler, Keith Hawkins, Karin Lind, Andrea K. Dupree, Joe P. Ninan, Neel Nagarajan, Gamze Böcek Topcu, Cynthia S. Froning, Chad F. Bender, Ryan Terrien, Lawrence W. Ramsey, Gregory N. Mace
Figure caption: log(RWHe) values vs. lithium abundances log ϵ(Li). The horizontal shaded region serves to roughly divide Li-rich from Li-poor stars, and the vertical shaded region separates the weak and strong λ10830 absorption strengths. The location of these lines is discussed in the text. As in Figures 6 and 7, black × symbols represent stars with Gaussian measured line profiles, blue open circles are stars with rotational line profiles, and a blue filled circle denotes TYC 3797-01268-1 (see Section 5.3).
Paper: The Active Chromospheres of Lithium-rich Red Giant Stars 
Authors: Christopher Sneden, Melike Afşar, Zeynep Bozkurt, Monika Adamów, Anohita Mallick, Bacham E. Reddy, Steven Janowiecki, Suvrath Mahadevan, Brendan P. Bowler, Keith Hawkins, Karin Lind, Andrea K. Dupree, Joe P. Ninan, Neel Nagarajan, Gamze Böcek Topcu, Cynthia S. Froning, Chad F. Bender, Ryan Terrien, Lawrence W. Ramsey, Gregory N. Mace
Figure caption: Top panel: color–magnitude diagram (CMD) for the targets. The plot boundaries have been set to show only the CMD area containing the first-ascent red giants, the RC, and the RHB. The main sequence, most of the subgiant branch, and the luminous giants and supergiants are outside of this CM area. Different colors and symbols denote Li-rich and Li-poor stars, and a freehand shaded region represents the He-fusing RC/RHB domain. Bottom panel: HR diagram based on Gaia photometric quantities. The colors and symbols are the same as in the top panel.
Paper: The Active Chromospheres of Lithium-rich Red Giant Stars 
Authors: Christopher Sneden, Melike Afşar, Zeynep Bozkurt, Monika Adamów, Anohita Mallick, Bacham E. Reddy, Steven Janowiecki, Suvrath Mahadevan, Brendan P. Bowler, Keith Hawkins, Karin Lind, Andrea K. Dupree, Joe P. Ninan, Neel Nagarajan, Gamze Böcek Topcu, Cynthia S. Froning, Chad F. Bender, Ryan Terrien, Lawrence W. Ramsey, Gregory N. Mace
Figure caption: Empirical broadening estimates compared to He I λ10830 reduced widths for stars that have relatively narrow line profiles. Point, line, and color types are identified in the figure. The ordinate of the plot is restricted to 0−12 km s−1 in order to see individual points clearly. This means that stars with Vsin(i) ≳ 12 km s−1 are not shown here. The point with error bars in the lower right-hand corner represents the typical uncertainties of the measurements, as explained in the text. The FWHM values were estimated to the nearest 0.01 Å (≃0.3 km s−1), as can be seen in their “quantized” values.
Paper: The Active Chromospheres of Lithium-rich Red Giant Stars 
Authors: Christopher Sneden, Melike Afşar, Zeynep Bozkurt, Monika Adamów, Anohita Mallick, Bacham E. Reddy, Steven Janowiecki, Suvrath Mahadevan, Brendan P. Bowler, Keith Hawkins, Karin Lind, Andrea K. Dupree, Joe P. Ninan, Neel Nagarajan, Gamze Böcek Topcu, Cynthia S. Froning, Chad F. Bender, Ryan Terrien, Lawrence W. Ramsey, Gregory N. Mace
Figure caption: Small section of spectra showing details of the He line profiles. The solid black line represents the mean line profile of the strongest He I λ10830 transitions for program stars without significant rotational broadening. The λ10830 line is a triplet, whose components are marked with vertical red lines. The feature at 10827 Å is a residual of imperfect cancellation of the very strong photospheric Si I line and should be ignored. The dotted blue line shows our single observation of TYC 3797-01288-1. In the figure legend we quote our derived Vsin(i) value. See the text for discussion of this unusual star.
Paper: The Active Chromospheres of Lithium-rich Red Giant Stars 
Authors: Christopher Sneden, Melike Afşar, Zeynep Bozkurt, Monika Adamów, Anohita Mallick, Bacham E. Reddy, Steven Janowiecki, Suvrath Mahadevan, Brendan P. Bowler, Keith Hawkins, Karin Lind, Andrea K. Dupree, Joe P. Ninan, Neel Nagarajan, Gamze Böcek Topcu, Cynthia S. Froning, Chad F. Bender, Ryan Terrien, Lawrence W. Ramsey, Gregory N. Mace
Figure caption: Empirical broadening estimates compared to He I λ10830 reduced widths for the whole sample. Point types and colors are as in Figure 6, except that a filled circle is used to call attention of TYC 3797-01268-1, a program star with large infrared color excesses. This object will be discussed in Section 5.3.
Paper: The Active Chromospheres of Lithium-rich Red Giant Stars 
Authors: Christopher Sneden, Melike Afşar, Zeynep Bozkurt, Monika Adamów, Anohita Mallick, Bacham E. Reddy, Steven Janowiecki, Suvrath Mahadevan, Brendan P. Bowler, Keith Hawkins, Karin Lind, Andrea K. Dupree, Joe P. Ninan, Neel Nagarajan, Gamze Böcek Topcu, Cynthia S. Froning, Chad F. Bender, Ryan Terrien, Lawrence W. Ramsey, Gregory N. Mace
Figure caption: Examples of photospheric spectrum cancellation. For each star the top panel shows an observed spectrum (black points) and the best-fit model photospheric spectrum (line), and the bottom panel shows the result of the observed/computed division.
Paper: The Active Chromospheres of Lithium-rich Red Giant Stars 
Authors: Christopher Sneden, Melike Afşar, Zeynep Bozkurt, Monika Adamów, Anohita Mallick, Bacham E. Reddy, Steven Janowiecki, Suvrath Mahadevan, Brendan P. Bowler, Keith Hawkins, Karin Lind, Andrea K. Dupree, Joe P. Ninan, Neel Nagarajan, Gamze Böcek Topcu, Cynthia S. Froning, Chad F. Bender, Ryan Terrien, Lawrence W. Ramsey, Gregory N. Mace
Figure caption: Histograms representing the distribution of log(RWHe) values for Li-poor (upper panel) and Li-rich (lower panel) stars. The vertical shaded region, drawn at log(RWHe) = −4.85 as in Figure 9, separates the weak and strong λ10830 absorption strengths.
Paper: The Active Chromospheres of Lithium-rich Red Giant Stars 
Authors: Christopher Sneden, Melike Afşar, Zeynep Bozkurt, Monika Adamów, Anohita Mallick, Bacham E. Reddy, Steven Janowiecki, Suvrath Mahadevan, Brendan P. Bowler, Keith Hawkins, Karin Lind, Andrea K. Dupree, Joe P. Ninan, Neel Nagarajan, Gamze Böcek Topcu, Cynthia S. Froning, Chad F. Bender, Ryan Terrien, Lawrence W. Ramsey, Gregory N. Mace
Figure caption: Comparison of Vsin(i) estimates in this work vs. values published in various literature sources. The red dashed line indicates agreement between the two data sets. The thick blue × symbol marks TYC-3797-01268-1, noted earlier in Figure 7.
Paper: The Active Chromospheres of Lithium-rich Red Giant Stars 
Authors: Christopher Sneden, Melike Afşar, Zeynep Bozkurt, Monika Adamów, Anohita Mallick, Bacham E. Reddy, Steven Janowiecki, Suvrath Mahadevan, Brendan P. Bowler, Keith Hawkins, Karin Lind, Andrea K. Dupree, Joe P. Ninan, Neel Nagarajan, Gamze Böcek Topcu, Cynthia S. Froning, Chad F. Bender, Ryan Terrien, Lawrence W. Ramsey, Gregory N. Mace
Figure caption: Another CMD for the targets. This plot contains the same data that are displayed in the top panel of Figure 4, but here the stars are divided into He-weak and He-strong groups, as indicated in the figure legend.
Paper: The Active Galactic Nuclei in the Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX). III. A Red Quasar with Extremely High Equivalent Widths Showing Powerful Outflows
Authors: Chenxu Liu, Karl Gebhardt, Wolfram Kollatschny, Robin Ciardullo, Erin Mentuch Cooper, Dustin Davis, Daniel J. Farrow, Steven L. Finkelstein, Eric Gawiser, Caryl Gronwall, Gary J. Hill, Lindsay House, Donald P. Schneider, Tanya Urrutia, Gregory R. Zeimann
Figure caption: Top panels: the r-band image and the expanded version from HSC-DEX. The pointing of the IR detection in the WISE survey is marked with an orange square. The green diamond marks another HSC-DEX r-band detection (22.5 mag) that is covered by the HETDEX fibers in this field. Middle panel: the narrowband image of the Lyα emission line derived from the HETDEX data. The small blue plus signs mark the positions of all HETDEX fibers in this field. The cyan circle marks the density peak of the Lyα line, which is also the recorded HETDEX coordinate in Table 1. The magenta triangle is a random position chosen to demonstrate the spatial changes of the Lyα line profiles in Figure 4. Bottom panels: the narrowband images of the C IV λ1549 (left) and He II λ1640 (right) emission lines. The seeing of the HETDEX observation is 1.″6 (FWHM). All images are centered at the coordinate of WISE (continuum center) in Table 1.
Paper: The Active Galactic Nuclei in the Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX). III. A Red Quasar with Extremely High Equivalent Widths Showing Powerful Outflows
Authors: Chenxu Liu, Karl Gebhardt, Wolfram Kollatschny, Robin Ciardullo, Erin Mentuch Cooper, Dustin Davis, Daniel J. Farrow, Steven L. Finkelstein, Eric Gawiser, Caryl Gronwall, Gary J. Hill, Lindsay House, Donald P. Schneider, Tanya Urrutia, Gregory R. Zeimann
Figure caption: Upper two rows: the spectra of Lyα at the four positions marked by the cyan circle (Lyα density peak), the orange square (the WISE pointing), the magenta triangle (a random position), and the green diamond (another r-band detection) in the narrowband image of the Lyα emission line in Figure 3. Black data points with error bars are the observed spectra. Our best-fit double-Gaussian model is shown by the green curve. The blue and red solid curves are the best-fit blue component and red component. The blue and red vertical lines mark the best-fit central wavelengths of the two peaks. Bottom panels: the surface density map of the spectral decomposed blue peak and red peak of Lyα. The orange square again marks the position of the WISE detection. The blue and the red crosses show the positions where the blue peak and the red peak have the highest line flux respectively.
Paper: The Active Galactic Nuclei in the Hobby–Eberly Telescope Dark Energy Experiment Survey (HETDEX). III. A Red Quasar with Extremely High Equivalent Widths Showing Powerful Outflows
Authors: Chenxu Liu, Karl Gebhardt, Wolfram Kollatschny, Robin Ciardullo, Erin Mentuch Cooper, Dustin Davis, Daniel J. Farrow, Steven L. Finkelstein, Eric Gawiser, Caryl Gronwall, Gary J. Hill, Lindsay House, Donald P. Schneider, Tanya Urrutia, Gregory R. Zeimann
Figure caption: Left: the line flux ratio map of the C IV λ1549 emission over the Lyα emission. Only spatial pixels with both emission lines detected at >1σ level are used in the map. Labels are the same with the ones in the narrowband images in Figure 3. Right: similar plot with the left panel, but for the line ratio of the He II λ1640 emission over the Lyα emission.
Paper: Oblique Electromagnetic Instabilities Driven by Pickup Ion Ring-beam Distributions in the Outer Heliosheath. I. Linear Instability Analysis
Authors: Ameneh Mousavi, Kaijun Liu, Sina Sadeghzadeh
Figure caption: The growth rates and real frequencies of the mirror waves (left column), parallel/quasi-parallel left-helicity waves (middle column) and oblique left- and right-helicity waves (right column) for α = 30°, 45°, 73°, and 85°. The growth rates are indicated by the color scale and the solid contours correspond to the real frequencies, both are normalized to the proton cyclotron frequency Ω p .
Paper: Oblique Electromagnetic Instabilities Driven by Pickup Ion Ring-beam Distributions in the Outer Heliosheath. I. Linear Instability Analysis
Authors: Ameneh Mousavi, Kaijun Liu, Sina Sadeghzadeh
Figure caption: Classification of electromagnetic waves based on their polarization, helicity, and propagation direction. ω, k ∥, and ﹩{ \mathcal P }﹩ are the real frequency, parallel wavenumber, and the polarization parameter, respectively.
Paper: Short GRB Host Galaxies. II. A Legacy Sample of Redshifts, Stellar Population Properties, and Implications for Their Neutron Star Merger Origins
Authors: Anya E. Nugent, Wen-Fai Fong, Yuxin Dong, 雨欣 董, Joel Leja, Edo Berger, Michael Zevin, Ryan Chornock, Bethany E. Cobb, Luke Zoltan Kelley, Charles D. Kilpatrick, Andrew Levan, Raffaella Margutti, Kerry Paterson, Daniel Perley, Alicia Rouco Escorial, Nathan Smith, Nial Tanvir
Figure caption: Left: the cumulative distribution function (CDF) in redshift for the Gold, Silver, and Bronze samples, as well as 5000 realizations of the CDF based on random draws from the individual posterior distributions. The thicker lines represent the median CDF while the thin lines show the individual realizations to demonstrate the sample spread. We find that there is an increasing redshift median from the Gold to Bronze Samples, as indicated by the arrows. Middle: the CDF and 5000 realizations in redshift of all short GRB hosts in our sample (purple), along with the photometric redshift (blue) and spectroscopic redshift sample (green). Right: redshift histograms of all hosts (purple), spectroscopic redshift hosts (green), and photometric redshift hosts (blue). The “All” hosts and photometric redshift distributions are built from the individual posterior distributions as described in Section 4.1. The photometric sample hosts most notably fill in the “redshift desert” (z > 1.0), and the photometric redshift sample has a median ∼0.5 greater than the spectroscopic redshift sample.
Paper: Short GRB Host Galaxies. II. A Legacy Sample of Redshifts, Stellar Population Properties, and Implications for Their Neutron Star Merger Origins
Authors: Anya E. Nugent, Wen-Fai Fong, Yuxin Dong, 雨欣 董, Joel Leja, Edo Berger, Michael Zevin, Ryan Chornock, Bethany E. Cobb, Luke Zoltan Kelley, Charles D. Kilpatrick, Andrew Levan, Raffaella Margutti, Kerry Paterson, Daniel Perley, Alicia Rouco Escorial, Nathan Smith, Nial Tanvir
Figure caption: Representative fits from two of the 69 short GRBs in our sample. Prospector produced model spectra (purple lines) and photometry (purple squares) compared to the observed spectra (green line) and error (gray line) and photometry (green circles) for the joint spectroscopy and photometry fit of GRB 150728A (left panel) and the redshift-free, photometry-only fit of GRB 160411A (right panel). We highlight these fits to show the accuracy in measurement of the spectral continuum and line locations (GRB 150728A) and the photometric colors for redshift determination (GRB 160411A). In total, we have performed 40 joint spectroscopic and photometric fits and 29 photometry-only fits. These modeling products are all available on the BRIGHT website.
Paper: Short GRB Host Galaxies. II. A Legacy Sample of Redshifts, Stellar Population Properties, and Implications for Their Neutron Star Merger Origins
Authors: Anya E. Nugent, Wen-Fai Fong, Yuxin Dong, 雨欣 董, Joel Leja, Edo Berger, Michael Zevin, Ryan Chornock, Bethany E. Cobb, Luke Zoltan Kelley, Charles D. Kilpatrick, Andrew Levan, Raffaella Margutti, Kerry Paterson, Daniel Perley, Alicia Rouco Escorial, Nathan Smith, Nial Tanvir
Figure caption: The fractions of star-forming (SF; blue), transitioning (T; yellow), and quiescent (Q; red) short GRB host galaxies based on the results in Table 2 for several subgroups of the sample. We see that in the full sample, a majority (∼84%) of short GRBs occur in star-forming galaxies, and ∼16% occur in transitioning or quiescent galaxies. These fractions also stay fairly consistent for the Gold, Silver, and Bronze samples. We find a lower star-forming fraction for the spectroscopic redshift sample than the photometric redshift sample, likely because the photometric redshift sample reaches higher redshifts, where star-forming galaxies are much more prevalent.
Paper: BASS. XXXIII. Swift-BAT Blazars and Their Jets through Cosmic Time
Authors: L. Marcotulli, M. Ajello, C. M. Urry, V. S. Paliya, M. Koss, K. Oh, G. Madejski, Y. Ueda, M. Baloković, B. Trakhtenbrot, F. Ricci, C. Ricci, D. Stern, F. Harrison, M. C. Powell
Figure caption: Average high-energy SED of the FSRQs in our sample derived by fitting: (i) only sources that are BAT and LAT detected (46 sources, left panel) and (ii) the whole sample (88 sources, right panel). The details of the fits can be found in Section 5. The different lines represent the mean of the distribution at different luminosity bins (as labeled). The errors (shown as colored shaded regions) are derived employing a Jackknife technique. The high-energy SED spectral form does not show strong dependence of the chosen luminosity bin. In the right panel, it can be noticed that the lowest-luminosity sources have, on average, an SED peaking at lower energies (∼3 MeV vs. ∼17 MeV for the highest-luminosity sources). This relation between the energy break position and the source luminosity has been calibrated (see Section 5.2 and Figure 8, right panel) in order to properly take into account the contribution to the MeV background. The shaded hatched pink and light-blue regions represent the BAT and LAT energy bands, respectively, shifted for sources at z = 0 (forward slash) and z = 4 (backward slash). As can be seen, the MeV peak of the sources falls exactly in the region that still remains uncovered by both instruments and is critical to determine the entire SED.
Paper: BASS. XXXIII. Swift-BAT Blazars and Their Jets through Cosmic Time
Authors: L. Marcotulli, M. Ajello, C. M. Urry, V. S. Paliya, M. Koss, K. Oh, G. Madejski, Y. Ueda, M. Baloković, B. Trakhtenbrot, F. Ricci, C. Ricci, D. Stern, F. Harrison, M. C. Powell
Figure caption: Total blazar (left) and FSRQs (right) XLF, ϕ(L, z) (where L ≡ L X). The top panels show them as a function of redshift in various luminosity bins; the bottom panels show them as a function of luminosity at different redshift bins. The data points are those deconvolved via the N obs/N mdl method described in Section 4.1. The solid lines instead show our best-fit mPLE model. In the bottom panels, to highlight the evolution at different luminosities, the XLF from the previous redshift bin is overplotted with the dashed lines.
Paper: BASS. XXXIII. Swift-BAT Blazars and Their Jets through Cosmic Time
Authors: L. Marcotulli, M. Ajello, C. M. Urry, V. S. Paliya, M. Koss, K. Oh, G. Madejski, Y. Ueda, M. Baloković, B. Trakhtenbrot, F. Ricci, C. Ricci, D. Stern, F. Harrison, M. C. Powell
Figure caption: Intensity spectrum of the CXB and derived contribution of the FSRQs using the best-fit mPLE model (pink dashed–dotted line and gray shaded region) and the mPDE one (light-blue dashed–dotted line and cyan shaded region). The data points represent the different measurements of the cosmic diffuse background, and have been extracted from the works indicated in the label (Fukada et al. 1975; Gendreau et al. 1995; Watanabe et al. 1997; Weidenspointner et al. 2000; Revnivtsev et al. 2003; Ajello et al. 2008; Cappelluti et al. 2017). The dashed black line is the model prediction of the total contribution of AGNs to the CXB as derived by Ananna et al. (2019). The solid black and gray lines represent the sum of the total contribution from AGNs and FSRQs using the mPLE and mPDE models, respectively. The spectrum of FSRQs has been taken from the best-fit SED derived in Section 5. The shaded areas are derived from Monte Carlo simulations employing the best-fit parameter ranges.
Paper: BASS. XXXIII. Swift-BAT Blazars and Their Jets through Cosmic Time
Authors: L. Marcotulli, M. Ajello, C. M. Urry, V. S. Paliya, M. Koss, K. Oh, G. Madejski, Y. Ueda, M. Baloković, B. Trakhtenbrot, F. Ricci, C. Ricci, D. Stern, F. Harrison, M. C. Powell
Figure caption: Number density plot of BAT FSRQs as a function of redshift and luminosity bins. The data points are those deconvolved via the N obs/N mdl method, and the solid lines show the best-fit mPLE model. For comparison, number densities model prediction from A09 in the highest-luminosity bin are shown (﹩\mathrm{log}L=47.1\mbox{--}48.4\,[\mathrm{erg}\,{{\rm{s}}}^{-1}]﹩, black dotted line). It can be seen how our best-fit XLF predicts a different XLF shape implying fewer sources at the highest redshifts, z = [3–5].
Paper: BASS. XXXIII. Swift-BAT Blazars and Their Jets through Cosmic Time
Authors: L. Marcotulli, M. Ajello, C. M. Urry, V. S. Paliya, M. Koss, K. Oh, G. Madejski, Y. Ueda, M. Baloković, B. Trakhtenbrot, F. Ricci, C. Ricci, D. Stern, F. Harrison, M. C. Powell
Figure caption: Left: BAT (14–195 keV) photon index vs. redshift of all BAT FSRQs in our sample. Red data points represent LAT-detected sources, while blue data points are the LAT-undetected ones. The yellow line is the best-fit linear relationship calculated for these data. The slope is very flat (m BAT = 0.01 ± 0.01), indicating that there is no evolution in redshift of the BAT photon index, and the intercept values give us the average value of c BAT = 1.71 ± 0.01. Right: LAT (0.1–300 GeV) photon index vs. redshift of all LAT-detected BAT FSRQs in our sample (red data points). The best-fit line is shown in yellow. Similarly to the BAT regime, the slope is very flat (m LAT = 0.09 ± 0.03), and the intercept returns an average photon index c LAT = 2.48 ± 0.05. These empirical relations confirm that there is no dependence on redshift of the high-energy SED spectral slopes of BAT FSRQs.
Paper: BASS. XXXIII. Swift-BAT Blazars and Their Jets through Cosmic Time
Authors: L. Marcotulli, M. Ajello, C. M. Urry, V. S. Paliya, M. Koss, K. Oh, G. Madejski, Y. Ueda, M. Baloković, B. Trakhtenbrot, F. Ricci, C. Ricci, D. Stern, F. Harrison, M. C. Powell
Figure caption: Results of the beaming fit to the BAT FSRQ population for p = 5 (left) and p = 7 (right). The red data points are the de-evolved luminosity function, ϕ(L, 0), the blue dotted line is the fit derived for the FSRQ population, and the green line shows the distribution of the parent population (labeled here as RGs). As can be noted, different values of p predict different number densities of the parent population at different luminosity bins. For p = 5, RGs would show a break in the distribution at L ∼ 1041 erg s−1, the luminosity at which they would be found with number densities of 104 Gpc−3. For p = 7, instead this break would appear at even lower luminosities, and their number densities at L ∼ 1041 erg s−1 would be 2 orders of magnitude lower with respect to p = 5.
Paper: BASS. XXXIII. Swift-BAT Blazars and Their Jets through Cosmic Time
Authors: L. Marcotulli, M. Ajello, C. M. Urry, V. S. Paliya, M. Koss, K. Oh, G. Madejski, Y. Ueda, M. Baloković, B. Trakhtenbrot, F. Ricci, C. Ricci, D. Stern, F. Harrison, M. C. Powell
Figure caption: Cumulative BAT-blazars logN-logS, i.e., total number of sources above a certain flux corrected for the survey sky coverage ω(S), N( > S), as a function flux (Equations (14) and (15)). The observed logN-logS is represented by the red data points, while the blue solid and green dashed lines show the prediction from the best-fit mPLE and mPDE models, respectively. We note that in this representation, the data points are not independent from one another. As can be seen, both models explain reasonably well the observed distribution in the region 8 × 10−12 erg cm−2 s−1 to 10−10 erg cm−2 s−1, where most source counts lie. As detailed in the Appendix, the slight discrepancy between the data and the model predictions below 8 × 10−12 erg cm−2 s−1 does not influence the validity of our results. The derived spectral slope for the logN-logS is 1.62 ± 0.05, indicative of a positive evolution of this source class (see Section 3.2).