adsabs/AstroCLIMB huggingface dataset:
Paper: Stellar Characterization, Magnesium Abundances, and Chromospheric Activity Analysis of Stars with Confirmed Exoplanets from the K2 Mission
Authors: V. Loaiza-Tacuri, Diogo Souto, F. Quispe-Huaynasi, Katia Cunha, S. Daflon, Ellen Costa-Almeida, V. V. Smith, Luan Ghezzi
Figure caption: The left panel shows the distribution of ﹩\mathrm{log}{R}{{\prime} }_{{\rm{HK}}}﹩ for the FGK main-sequence stars in our sample. In contrast, the right panel presents the ﹩\mathrm{log}{R}{{\prime} }_{{\rm{HK}}}﹩ distribution estimated using KDE, which is independent of binning. The gray dashed lines in both panels indicate different activity levels (as identified by T. J. Henry et al. 1996).
Paper: Stellar Characterization, Magnesium Abundances, and Chromospheric Activity Analysis of Stars with Confirmed Exoplanets from the K2 Mission
Authors: V. Loaiza-Tacuri, Diogo Souto, F. Quispe-Huaynasi, Katia Cunha, S. Daflon, Ellen Costa-Almeida, V. V. Smith, Luan Ghezzi
Figure caption: Stellar activity indices (﹩\mathrm{log}{R}_{\mathrm{HK}}^{{\prime} }﹩ and ﹩\mathrm{log}{I}_{{\rm{H}}\alpha }﹩) vs. the ratios of NUV and FUV to bolometric luminosities for the stars with UV magnitude in GALEX. Red points represent the FUV luminosity fraction, while blue points correspond to the NUV luminosity fraction. FUV emission decreases with lower activity, while NUV remains nearly constant.
Paper: Linear Mode Conversion Theory of Radio Emission from Turbulent Solar Wind Plasmas
Authors: C. Krafft, A. S. Volokitin
Figure caption: Variations of the electromagnetic radiation rate ﹩\dot{\eta }﹩ as a function of 1/cL (in logarithmic scales), for ﹩{ \mathcal O }﹩-mode (left) and ﹩{ \mathcal Z }﹩-mode (right) waves, at plasma conditions of Figure 8. The radiation rates calculated by the model equations are represented by black diamonds; linear interpolations are shown by red dashed lines, indicating that σ = 1.53 (left) and σ = 2.3 (right). The black lines show the scaling with the index p = 2. All variables are normalized. Scales are logarithmic.
Paper: Linear Mode Conversion Theory of Radio Emission from Turbulent Solar Wind Plasmas
Authors: C. Krafft, A. S. Volokitin
Figure caption: Variations with the average level of density fluctuations ΔN of the radiation rates ﹩\dot{\eta }{({c}_{L}/30)}^{2}﹩ of ﹩{ \mathcal O }﹩-mode (left) and ﹩{ \mathcal Z }﹩-mode (right) waves, for ωc/ωp = 0.05 (upper row) and ωc/ωp = 0.15 (bottom row), for different cL (see the legend in the upper-left panel). All variables are normalized.
Paper: Linear Mode Conversion Theory of Radio Emission from Turbulent Solar Wind Plasmas
Authors: C. Krafft, A. S. Volokitin
Figure caption: Dispersion of electromagnetic modes near the frequency ωp, for ωc/ωp = 0.1 and θ = 10°: variation of ﹩{c}^{2}{k}^{2}/{\omega }_{p}^{2}﹩ as a function of ω/ωp. Green (blue) lines represent the ﹩{ \mathcal Z }﹩-mode waves and the curve ω = ωp (the ﹩{ \mathcal O }﹩-mode waves), calculated using Equation (B6). The black dashed (at ω ≃ ωp) and solid (at 1.015ωp ≲ ω ≲ 1.04ωp) lines represent the approximated dispersion curves, Equations (B7) and (B8), near the plasma frequency, respectively.
Paper: Linear Mode Conversion Theory of Radio Emission from Turbulent Solar Wind Plasmas
Authors: C. Krafft, A. S. Volokitin
Figure caption: Variations with ωc/ωp of the radiation rate ﹩\dot{\eta }{({c}_{L}/30)}^{2}﹩ of ﹩{ \mathcal O }﹩-mode (left) and ﹩{ \mathcal Z }﹩-mode (right) waves, for ΔN = 0.05 and different cL (see the legend in the left panel). All variables are normalized.
Paper: Linear Mode Conversion Theory of Radio Emission from Turbulent Solar Wind Plasmas
Authors: C. Krafft, A. S. Volokitin
Figure caption: Variations with ωc/ωp of the radiation rate ﹩\dot{\eta }{({c}_{L}/30)}^{2}﹩ of ﹩{ \mathcal O }﹩-mode (left) and ﹩{ \mathcal Z }﹩-mode (right) waves, for ΔN = 0.02 and different cL (see the legend in the left panel). All variables are normalized.
Paper: Linear Mode Conversion Theory of Radio Emission from Turbulent Solar Wind Plasmas
Authors: C. Krafft, A. S. Volokitin
Figure caption: Electromagnetic ﹩{ \mathcal O }﹩-mode waves: dispersion curves in the map (ck∥/ωp, ck⊥/ωp), for ωc/ωp = 0.2 and the frequencies ω/ωp = 1.005, 1.0125, and 1.025 (see the legend), obtained by solving the exact Equation (B6).
Paper: Linear Mode Conversion Theory of Radio Emission from Turbulent Solar Wind Plasmas
Authors: C. Krafft, A. S. Volokitin
Figure caption: Variations with ωc/ωp of the radiation rate ﹩\dot{\eta }{({c}_{L}/30)}^{2}﹩ of ﹩{ \mathcal O }﹩-mode (left) and ﹩{ \mathcal Z }﹩-mode (right) waves, for ΔN = 0.06 and different cL (see the legend in the left panel). All variables are normalized.
Paper: Detection of Kink Oscillations in Solar Coronal Loops by a Convolutional Neural Network–Long Short-term Memory Neural Network
Authors: Sergey A. Belov, Yu Zhong, Dmitrii Y. Kolotkov, Valery M. Nakariakov
Figure caption: The t-SNE visualization of LSTM feature embeddings for 200 randomly selected positive and 200 negative synthetic samples combined with all real samples. Diamonds and circles denote samples with and without oscillations, respectively. Left panel: relationship between real data samples without oscillations and the clustered synthetic data. Right panel: relationship between real data samples with oscillations and the clustered synthetic data. Large markers indicate the centers of mass of the data clouds. Color coding for synthetic samples was adjusted to emphasize negatives in the left panel and positives in the right.
Paper: Detection of Kink Oscillations in Solar Coronal Loops by a Convolutional Neural Network–Long Short-term Memory Neural Network
Authors: Sergey A. Belov, Yu Zhong, Dmitrii Y. Kolotkov, Valery M. Nakariakov
Figure caption: The user interface of the browser application for the CNN-LSTM based kink-oscillation detection in solar coronal-imaging data.
Paper: A Large Sample of JWST/NIRSpec Brown Dwarfs: New Distant Discoveries
Authors: Zhijun Tu, Shu Wang, Xiaodian Chen, Jifeng Liu
Figure caption: Distance estimates using evolutionary tracks for the two most distant brown dwarfs, JWST J001418.22−302223.2 (left) and JWST J033240.07−274907.8 (right). For each object we fixed Teff to 2200 and 2300 K, respectively, and interpolated the evolutionary models over the radius range consistent with Teff ± 50 K. Distances D were derived from the measured ﹩{\mathrm{log}}({R}^{2}/{D}^{2})﹩ values and the corresponding radii R, with vertical error bars reflecting the ±0.05 dex uncertainty in ﹩{\mathrm{log}}({R}^{2}/{D}^{2})﹩. The color coding represents the ﹩{\mathrm{log}}\,g﹩ predicted by the evolutionary models at each radius.
Paper: A Large Sample of JWST/NIRSpec Brown Dwarfs: New Distant Discoveries
Authors: Zhijun Tu, Shu Wang, Xiaodian Chen, Jifeng Liu
Figure caption: The panels show the relationship between metallicity and vertical height ∣Z∣, with sources colored by age. The title of each panel specifies the model from which the parameters are derived, while the legend reports the coefficients of the linear fit according to ﹩[{\rm{M}}/{\rm{H}}]=a+b\,{\mathrm{log}}| Z| ﹩.
Paper: A Large Sample of JWST/NIRSpec Brown Dwarfs: New Distant Discoveries
Authors: Zhijun Tu, Shu Wang, Xiaodian Chen, Jifeng Liu
Figure caption: Flux calibration check for the two most distant brown dwarf candidates. Red points represent the NIRCam photometric measurements, while blue points show the synthetic photometry obtained by convolving the observed spectra with the corresponding NIRCam filter transmission curves.
Paper: A Large Sample of JWST/NIRSpec Brown Dwarfs: New Distant Discoveries
Authors: Zhijun Tu, Shu Wang, Xiaodian Chen, Jifeng Liu
Figure caption: JWST/NIRSpec PRISM/CLEAR spectra of the brown dwarf candidates, shown as deep blue lines with light blue shaded regions indicating the uncertainties. The best-fit model spectra are overplotted in red. We show the object names and corresponding best-fit model parameters in the legend.
Paper: A Large Sample of JWST/NIRSpec Brown Dwarfs: New Distant Discoveries
Authors: Zhijun Tu, Shu Wang, Xiaodian Chen, Jifeng Liu
Figure caption: Comparison of the observed spectra of 2MASS J00470038+6803543 (dashed blue) with the best-fit parameters of cloud-free Sonora Elf Owl model (gray) and the cloudy SAND model (red).
Paper: A Large Sample of JWST/NIRSpec Brown Dwarfs: New Distant Discoveries
Authors: Zhijun Tu, Shu Wang, Xiaodian Chen, Jifeng Liu
Figure caption: The blue histogram shows the distance distribution of all brown dwarfs in our sample, while the red histogram highlights the distribution of 12 new brown dwarf candidates.
Paper: Super-size Me: The Big Multi-AGN Catalog (The Big MAC) Data Release 1: The Source Catalog
Authors: Ryan W. Pfeifle, Kimberly A. Weaver, Nathan J. Secrest, Barry Rothberg, David R. Patton
Figure caption: AGN fueling across the merger sequence and across individual host orbits. Here we provide a cartoon illustration of the first and second pericenter passages of a pair of interacting galaxies and the possible AGN activity levels of the SMBHs. Left: the two galaxies experience a close passage at ∼10 kpc; torques induced during the interaction excite gas inflow mechanisms (e.g., bars, shocks, clump inflows; K. A. Blumenthal & J. E. Barnes 2018). Middle: gas is delivered into the nuclei on varying timescales with varying efficiencies (P. R. Capelo & M. Dotti 2017; K. A. Blumenthal & J. E. Barnes 2018), SMBH fueling begins. AGNs will flicker on and off across the merger sequence due to changes in the nuclear gas reservoirs. AGNs are shown as red diamonds, and the size and opacity of the diamonds indicate the activity level of the AGNs (larger and more opaque diamonds are more luminous AGNs). The numbers indicate “snapshots” as in a cosmological simulation; AGN activity levels vary between snapshots. Right: as the merger progresses to the second (and later) pericenter passage, the orbits decay, bringing the galaxies and AGNs closer together. Gas inflows are expected to continue, either triggered from the prior passage or the new pericenter passage, and AGN activity is expected to continue, with different activity levels caught in different snapshots. The exact timescales for the orbital evolution of pericentercurrent → apocenter → pericenternext once the galaxies have passed within 10 kpc is unique to a given merging pair of galaxies, but these timescales can range from as short as a few tens of Myr to hundreds of Myr. Note in these panels: dual AGNs are only visible during certain snapshots, to reflect realistic expectations for AGN duty cycles.
Paper: Super-size Me: The Big Multi-AGN Catalog (The Big MAC) Data Release 1: The Source Catalog
Authors: Ryan W. Pfeifle, Kimberly A. Weaver, Nathan J. Secrest, Barry Rothberg, David R. Patton
Figure caption: The transition from dual AGNs to binary AGNs. The logarithm of the total enclosed mass of an SMBH pair is shown on the x-axis, and the physical separation (in parsecs) is given on the y-axis. The dashed, black line corresponds to the radius, rb, at which the two SMBHs in a pair become dominated by their mutual gravity, and hence a dual AGN/SMBH transitions to a binary AGN. Labels for “Dual AGNs” and “Binary AGNs” are used to indicate that dual AGNs are found above this transition line, and binaries are found below it. We plot several subkiloparsec dual AGNs/SMBHs (blue: UGC 4211; M. J. Koss et al. 2023; green: NGC 7727; K. T. Voggel et al. 2022) and the single known binary AGN, CSO 0402+379 (H. L. Maness et al. 2004; C. Rodriguez et al. 2006), where the separations are the projected separations, and the enclosed masses were either inferred from the stellar velocity dispersion (for CSO 0402+379) or direct dynamical or spectroscopic measurements (K. T. Voggel et al. 2022; M. J. Koss et al. 2023).
Paper: Super-size Me: The Big Multi-AGN Catalog (The Big MAC) Data Release 1: The Source Catalog
Authors: Ryan W. Pfeifle, Kimberly A. Weaver, Nathan J. Secrest, Barry Rothberg, David R. Patton
Figure caption: The distribution of 2D projected separations and line-of-sight velocity differences of interacting galaxy pairs with reconstructed orbits in Illustris-TNG100 (D. R. Patton et al. 2024) after a recent (<1 Gyr) close passage <10 kpc. The shaded region indicates our expectation for the parameter space of galaxy mergers likely to host dual AGNs (see Section 2.3); the shaded box outlined by the dashed black line encloses 95% of the sample of interacting galaxy pairs (rp ≤ 110 kpc and ∣Δv∣ ≤ 600 km s−1).
Paper: Super-size Me: The Big Multi-AGN Catalog (The Big MAC) Data Release 1: The Source Catalog
Authors: Ryan W. Pfeifle, Kimberly A. Weaver, Nathan J. Secrest, Barry Rothberg, David R. Patton
Figure caption: Shown is a breakdown of the selection methods used to identify dual AGNs and candidates in the literature (spanning confidence ranks 1 to –1). This chart shows the aggregate percent usage of all dual AGN candidate selection techniques (normalized by the total number of dual AGN candidates—ranks 1 to –1—in the catalog) and corresponds to Section 4.1.1. Note, these selection methods are not all necessarily mutually exclusive (for example, selection based on double-peak optical spectroscopic emission lines necessarily requires the use of optical spectroscopy, and often specifically involves the use of optical fiber spectroscopy).
Paper: Super-size Me: The Big Multi-AGN Catalog (The Big MAC) Data Release 1: The Source Catalog
Authors: Ryan W. Pfeifle, Kimberly A. Weaver, Nathan J. Secrest, Barry Rothberg, David R. Patton
Figure caption: A flowchart illustrating our systematic method of identifying papers in ADS related to observational searches and analyses of multi-AGN systems. Each panel of this flowchart represents a relatively distinct “phase” of our systematic assembly of the literature library and catalog, and each panel is meant to be read from left to right starting with the first box in each panel.
Paper: Super-size Me: The Big Multi-AGN Catalog (The Big MAC) Data Release 1: The Source Catalog
Authors: Ryan W. Pfeifle, Kimberly A. Weaver, Nathan J. Secrest, Barry Rothberg, David R. Patton
Figure caption: Representative examples of confidence rank assignment. These three flowcharts illustrate our basic (subjective) process of confidence rank assignment. For each of these three cases (and throughout the catalog), the initial selection methodology sets the initial confidence ranking, and the confidence rank then evolves as additional evidence is obtained (either within the original article or through follow-up studies); these cases differ from those described in Section 3.4 and serve as additional examples. Red text is used to denote pieces of evidence that explain (if needed) the final ranking (and/or the demotion in rank). For example, the red text in the bottom flowchart illustrates why the confidence rank of the dual AGN candidate in NGC 3393 was demoted first to “–0.5,” and then finally to “–1.” As another example, the red text in the top panel explains why the confidence rank of the dual AGN candidate DESJ0122+0358 remained at “+0.5” and was not elevated to “1.”
Paper: Super-size Me: The Big Multi-AGN Catalog (The Big MAC) Data Release 1: The Source Catalog
Authors: Ryan W. Pfeifle, Kimberly A. Weaver, Nathan J. Secrest, Barry Rothberg, David R. Patton
Figure caption: Dual AGN candidates (ranks 1 to –1) that required optical spectroscopy for selection (see Section 4.1.2). Shown is a breakdown of dual AGN selection strategies used in concert with (left) or independently (right) of optical spectroscopy, where the bars of the histograms are normalized to the total number of candidates that required optical spectroscopy as a part of their selection function.
Paper: Super-size Me: The Big Multi-AGN Catalog (The Big MAC) Data Release 1: The Source Catalog
Authors: Ryan W. Pfeifle, Kimberly A. Weaver, Nathan J. Secrest, Barry Rothberg, David R. Patton
Figure caption: Sky distribution of Big MAC DR1 systems (ranks 1 to −1). The top, middle, and bottom panels show the sky distribution of dual AGN/SMBH candidates, binary AGN/SMBH candidates, and recoiling AGN/SMBH candidates, respectively. The current populations of multi-AGN candidates are largely biased toward the Sloan Digital Sky Survey (SDSS) fields; SDSS coverage (drawn from the DR18 plate list, https://data.sdss.org/sas/dr18/spectro/sdss/redux/) is denoted by gray shaded regions 1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 in diameter.
Paper: Super-size Me: The Big Multi-AGN Catalog (The Big MAC) Data Release 1: The Source Catalog
Authors: Ryan W. Pfeifle, Kimberly A. Weaver, Nathan J. Secrest, Barry Rothberg, David R. Patton
Figure caption: The breakdown of single or cross-listed system types in Big MAC DR1. The majority of systems within DR1 have been assigned a single system class (89.7%); 10.15% systems fall into two system classes, and 0.3% systems fall into three system classes.
Paper: Super-size Me: The Big Multi-AGN Catalog (The Big MAC) Data Release 1: The Source Catalog
Authors: Ryan W. Pfeifle, Kimberly A. Weaver, Nathan J. Secrest, Barry Rothberg, David R. Patton
Figure caption: Dual AGN candidates (ranks 1 to −1) that required optical imaging for selection (see Section 4.1.3). Shown is a breakdown of dual AGN selection strategies used in concert with (left) or independently (right) of optical imaging, where the bars of the histograms are normalized to the total number of candidates that required optical imaging as a part of their selection function.
Paper: Super-size Me: The Big Multi-AGN Catalog (The Big MAC) Data Release 1: The Source Catalog
Authors: Ryan W. Pfeifle, Kimberly A. Weaver, Nathan J. Secrest, Barry Rothberg, David R. Patton
Figure caption: Dual AGN candidates (ranks 1 to −1) that required mid-IR imaging for selection (see Section 4.1.4). Shown is a breakdown of dual AGN selection strategies used in concert (left) or independently (right) of mid-IR imaging, where the bars of the histograms are normalized to the total number of candidates that required mid-IR imaging as a part of their selection function.
Paper: Super-size Me: The Big Multi-AGN Catalog (The Big MAC) Data Release 1: The Source Catalog
Authors: Ryan W. Pfeifle, Kimberly A. Weaver, Nathan J. Secrest, Barry Rothberg, David R. Patton
Figure caption: Selection method assignment in the Big MAC. These three examples illustrate the general way we add/assign selection methods to the “Selection Method” column for a given entry within the Big MAC. Each case begins with the “initial” selection strategy, and the arrows indicate the progression through additional, complementary methods used for the selection process. The final opaque box shows the “full” selection strategy for these examples included in the Big MAC.
Paper: Super-size Me: The Big Multi-AGN Catalog (The Big MAC) Data Release 1: The Source Catalog
Authors: Ryan W. Pfeifle, Kimberly A. Weaver, Nathan J. Secrest, Barry Rothberg, David R. Patton
Figure caption: Binary AGN/SMBH candidates (ranks 1 to −1) that required radio imaging for selection (see Section 4.2.4). Shown is a breakdown of binary AGN/SMBH selection strategies used in concert with (left) or independently of (right) radio imaging, where the bars of the histograms are normalized to the total number of candidates that required radio imaging as a part of their selection function.
Paper: Super-size Me: The Big Multi-AGN Catalog (The Big MAC) Data Release 1: The Source Catalog
Authors: Ryan W. Pfeifle, Kimberly A. Weaver, Nathan J. Secrest, Barry Rothberg, David R. Patton
Figure caption: Shown is a breakdown of the selection methods used to identify binary AGNs/SMBHs candidates (confidence ranks 1 to −1) in the literature. This chart shows the aggregate percent usage of all binary AGN/SMBH selection techniques (normalized by the total number of binary candidates—ranks 1 to −1—in the catalog) and corresponds to Section 4.2.1. Note, these selection methods are not all necessarily mutually exclusive (for example, selection based on optical periodicity necessarily requires optical imaging in most cases).
Paper: Super-size Me: The Big Multi-AGN Catalog (The Big MAC) Data Release 1: The Source Catalog
Authors: Ryan W. Pfeifle, Kimberly A. Weaver, Nathan J. Secrest, Barry Rothberg, David R. Patton
Figure caption: Dual AGN candidates (ranks 1 to −1) that required radio imaging for selection (see Section 4.1.6). Shown is a breakdown of dual AGN selection strategies used in concert with (left) or independently of (right) radio imaging, where the bars of the histograms are normalized to the total number of candidates that required radio imaging as a part of their selection function.
Paper: Super-size Me: The Big Multi-AGN Catalog (The Big MAC) Data Release 1: The Source Catalog
Authors: Ryan W. Pfeifle, Kimberly A. Weaver, Nathan J. Secrest, Barry Rothberg, David R. Patton
Figure caption: Recoiling AGN candidates (ranks 1 to −1) that required radio imaging for selection (see Section 4.3.2). Shown is a breakdown of recoiling AGN/SMBH selection strategies used in conjunction with radio imaging, where the bars of the histogram are normalized to the total number of candidates that required radio imaging as a part of their selection function. None of these objects were selected independently of radio imaging using other techniques.
Paper: Super-size Me: The Big Multi-AGN Catalog (The Big MAC) Data Release 1: The Source Catalog
Authors: Ryan W. Pfeifle, Kimberly A. Weaver, Nathan J. Secrest, Barry Rothberg, David R. Patton
Figure caption: Binary AGN/SMBH candidates (ranks 1 to −1) that required optical spectroscopy for selection (see Section 4.2.2). Shown is a breakdown of binary AGN/SMBH selection strategies used in concert with (left) or independently of (right) optical spectroscopy, where the bars of the histograms are normalized to the total number of candidates that required optical spectroscopy as a part of their selection function.
Paper: Super-size Me: The Big Multi-AGN Catalog (The Big MAC) Data Release 1: The Source Catalog
Authors: Ryan W. Pfeifle, Kimberly A. Weaver, Nathan J. Secrest, Barry Rothberg, David R. Patton
Figure caption: Binary AGN/SMBH candidates (ranks 1 to −1) that required optical imaging for selection (see Section 4.2.3). Shown is a breakdown of binary AGN/SMBH selection strategies used in concert with (left) or independently of (right) optical imaging, where the bars of the histograms are normalized to the total number of candidates that required optical imaging as a part of their selection function.
Paper: Super-size Me: The Big Multi-AGN Catalog (The Big MAC) Data Release 1: The Source Catalog
Authors: Ryan W. Pfeifle, Kimberly A. Weaver, Nathan J. Secrest, Barry Rothberg, David R. Patton
Figure caption: Recoiling AGN/SMBH candidates (ranks 1 to −1) that required optical spectroscopy for selection (see Section 4.3.3). Shown is a breakdown of recoiling AGN/SMBH selection strategies used in concert with optical spectroscopy, where the bars of the histograms are normalized to the total number of candidates that required optical spectroscopy as a part of their selection function. None of these objects were selected independently of optical spectroscopy using other techniques.
Paper: Super-size Me: The Big Multi-AGN Catalog (The Big MAC) Data Release 1: The Source Catalog
Authors: Ryan W. Pfeifle, Kimberly A. Weaver, Nathan J. Secrest, Barry Rothberg, David R. Patton
Figure caption: Shown is a breakdown of the selection methods used to identify recoiling AGN/SMBH candidates in the literature (all confidence ranks). This chart shows the aggregate percent usage of all recoiling AGN/SMBH candidate selection techniques (normalized by the total number of recoil candidates in the catalog) and corresponds to Section 4.3.1. Note, these selection methods are not all necessarily mutually exclusive (for example, selection based on X-shaped radio sources necessarily requires radio imaging).