adsabs/AstroCLIMB huggingface dataset:
Paper: Climate of High-obliquity Exoterrestrial Planets with a Three-dimensional Cloud System Resolving Climate Model
Authors: Takanori Kodama, Daisuke Takasuka, Sam Sherriff-Tadano, Takeshi Kuroda, Tomoki Miyakawa, Ayako Abe-Ouchi, Masaki Satoh
Figure caption: Maps for cloud fraction of high clouds at low resolution with convective parameterization (left column) and at high resolution with explicit treatment of cloud microphysics (NSW6; right column). Right panels beside maps show zonally averaged cloud fraction.
Paper: Climate of High-obliquity Exoterrestrial Planets with a Three-dimensional Cloud System Resolving Climate Model
Authors: Takanori Kodama, Daisuke Takasuka, Sam Sherriff-Tadano, Takeshi Kuroda, Tomoki Miyakawa, Ayako Abe-Ouchi, Masaki Satoh
Figure caption: The same as Figure 2, except for high-resolution runs with explicit treatment of cloud microphysics.
Paper: Climate of High-obliquity Exoterrestrial Planets with a Three-dimensional Cloud System Resolving Climate Model
Authors: Takanori Kodama, Daisuke Takasuka, Sam Sherriff-Tadano, Takeshi Kuroda, Tomoki Miyakawa, Ayako Abe-Ouchi, Masaki Satoh
Figure caption: The same as Figure 1, except for high-resolution runs with explicit treatment of cloud microphysics.
Paper: Climate of High-obliquity Exoterrestrial Planets with a Three-dimensional Cloud System Resolving Climate Model
Authors: Takanori Kodama, Daisuke Takasuka, Sam Sherriff-Tadano, Takeshi Kuroda, Tomoki Miyakawa, Ayako Abe-Ouchi, Masaki Satoh
Figure caption: The same as Figure 3, except for high-resolution runs with explicit treatment of cloud microphysics.
Paper: Near-infrared Extragalactic Background Light Fluctuations on Nonlinear Scales
Authors: Yun-Ting Cheng, James J. Bock
Figure caption: Top: power spectra of the four cases described in Section 4.4 with four f IHL values. Black: fiducial case (case 1); blue: pixel masking-only case (case 2); orange: pixel masking and σ PSF = 7″ case (case 3); green: pixel masking and σ PSF = 70″ case (case 4). Error bars are the sample variance in a 200 deg2 survey. Bottom: fractional error with respect to the fiducial case.
Paper: Testing the Limits of AGN Feedback and the Onset of Thermal Instability in the Most Rapidly Star-forming Brightest Cluster Galaxies
Authors: Michael S. Calzadilla, Michael McDonald, Megan Donahue, Brian R. McNamara, Kevin Fogarty, Massimo Gaspari, Myriam Gitti, Helen R. Russell, Grant R. Tremblay, G. Mark Voit, Francesco Ubertosi
Figure caption: Continuum-subtracted [OII] maps of the BCGs in our sample, including Phoenix, H1821+643, IRAS 09104+4109, Abell 1835, RX J1532.9+3021, MACS 1931.8-2634, and RBS 797. In the left panel is a combination of broadband HST images using the filters listed in Table 1, as well as the continuum predicted by the procedure described in Section 2.2.1 and Figure 1. The middle panel is a zoom in of the central [OII] emitting nebulae with the continuum subtracted. Elliptical dashed regions denote the locations of known cavities from the literature that can also be identified from the Chandra X-ray images shown in the right panel, with overlaid [OII] contours in green. The region of H1821 within the red-dashed circle was masked to exclude possible contamination from the bright central quasar to the SFR measurement.
Paper: Testing the Limits of AGN Feedback and the Onset of Thermal Instability in the Most Rapidly Star-forming Brightest Cluster Galaxies
Authors: Michael S. Calzadilla, Michael McDonald, Megan Donahue, Brian R. McNamara, Kevin Fogarty, Massimo Gaspari, Myriam Gitti, Helen R. Russell, Grant R. Tremblay, G. Mark Voit, Francesco Ubertosi
Figure caption:                         Illustration of the pixel-by-pixel spectral energy distribution (SED) fitting procedure we use to produce emission-line only maps (see Figure 2). For each object, we use narrowband observations tuned to the redshifted wavelength of [OII]λ                         λ3726, 3729, bracketed by images of broadband filters chosen to be free from strong emission lines usually associated with star formation or AGN emission (e.g., Hα and [OIII]). The flux in a single pixel from the bracketing broadband images is then used to construct an SED and is fit by a linear combination of a 10 Myr starburst and 6 Gyr passive elliptical galaxy template, allowing their normalizations to vary (see top-right and bottom-right panels, highlighting two distinct pixel fits). The combined, predicted template flux at the wavelength of the narrowband filter is then subtracted from the narrowband image at that pixel, resulting in a continuum-subtracted image after the procedure is run for every common pixel in the aligned images.
Paper: Deep Learning–based Fast Spectral Inversion of Hα and Ca II 8542 Line Spectra
Authors: Kyoung-Sun Lee, Jongchul Chae, Eunsu Park, Yong-Jae Moon, Hannah Kwak, Kyuhyoun Cho
Figure caption: Example pairs—the input object and the desired output value—for supervised learning. The left panels display the inputs for the observed line profiles of Hα and Ca II 8542 Å (in black) and their shapes after the standardization processes described in Section 2.2 (in red). Details of the preprocessing are provided in the text. The right panels show the physical parameters calculated from the MLSI model using the input spectra.
Paper: Deep Learning–based Fast Spectral Inversion of Hα and Ca II 8542 Line Spectra
Authors: Kyoung-Sun Lee, Jongchul Chae, Eunsu Park, Yong-Jae Moon, Hannah Kwak, Kyuhyoun Cho
Figure caption: Physical parameter maps of the Ca II 8542 Å line using MLSI (upper three rows) and the DNN (lower three rows) for the QR. The cross and square symbols mark the locations of a network feature and a region with a large standard error, respectively.
Paper: Deep Learning–based Fast Spectral Inversion of Hα and Ca II 8542 Line Spectra
Authors: Kyoung-Sun Lee, Jongchul Chae, Eunsu Park, Yong-Jae Moon, Hannah Kwak, Kyuhyoun Cho
Figure caption: Monochromatic images constructed at the wavelengths of the Hα and the Ca II 8542 Å lines, obtained from FISS. The upper (first and second rows) and lower (third and fourth rows) panels show sample images of a QR and an AR, respectively. The cross symbols in the QR and AR images mark the positions of a network feature and a superpenumbral fibril that we selected to compare the observed line profiles with the modeled spectra, using the physical parameters inferred from the DNN in Figures 10 and 11. The white vertical slits in the scanned raster images of the AR indicate that data are missing.
Paper: Identifying the 3FHL Catalog. VI. Swift Observations of 3FHL Unassociated Objects with Source Classification via Machine Learning
Authors: S. Joffre, R. Silver, M. Rajagopal, M. Ajello, N. Torres-Albà, A. Pizzetti, S. Marchesi, A. Kaur
Figure caption: ROC curve resulting in an accuracy of 0.93. This curve comes from the SVM model used on our 21 blazar counterpart candidates. The effectiveness of the classifier is measured by the area under the curve, with 1 being the ideal value i.e., all true positives and no false positives.
Paper: Identifying the 3FHL Catalog. VI. Swift Observations of 3FHL Unassociated Objects with Source Classification via Machine Learning
Authors: S. Joffre, R. Silver, M. Rajagopal, M. Ajello, N. Torres-Albà, A. Pizzetti, S. Marchesi, A. Kaur
Figure caption: ROC curve from the random forest method on the validation sample. The area under the curve yielded 0.95. The diagonal line represents the nondiscriminatory curve. Hence, any point below this line would not be classified by the model.
Paper: Identifying the 3FHL Catalog. VI. Swift Observations of 3FHL Unassociated Objects with Source Classification via Machine Learning
Authors: S. Joffre, R. Silver, M. Rajagopal, M. Ajello, N. Torres-Albà, A. Pizzetti, S. Marchesi, A. Kaur
Figure caption: Random forest feature importance for class identification. The addition of the W3–W4 feature was included because it is more significant than two other features used in previous campaigns of this kind (see Kaur et al. 2019; Silver et al. 2020).
Paper: Identifying the 3FHL Catalog. VI. Swift Observations of 3FHL Unassociated Objects with Source Classification via Machine Learning
Authors: S. Joffre, R. Silver, M. Rajagopal, M. Ajello, N. Torres-Albà, A. Pizzetti, S. Marchesi, A. Kaur
Figure caption: The probability mass function plotted for the likelihood to detect a double X-ray detection in a given number of fields out of the 21 fields observed. The probability of detecting five fields with a double X-ray detection is 14%.
Paper: Deep Learning–based Fast Spectral Inversion of Hα and Ca II 8542 Line Spectra
Authors: Kyoung-Sun Lee, Jongchul Chae, Eunsu Park, Yong-Jae Moon, Hannah Kwak, Kyuhyoun Cho
Figure caption: Flowchart of our DNN with skip connection and branching architecture. The red numbers for each of the layers indicate the numbers of nodes. The black number above the ellipsis denotes the number of layers that have the same number of nodes as the previous layer.
Paper: An Atmospheric Retrieval of the Brown Dwarf Gliese 229B
Authors: Emily Calamari, Jacqueline K. Faherty, Ben Burningham, Eileen Gonzales, Daniella Bardalez-Gagliuffi, Johanna M. Vos, Marina Gemma, Niall Whiteford, Josefine Gaarn
Figure caption: In the figure on the left, we show retrieved C/O values for objects with a main sequence companion with known C/O. Substellar objects are marked by a circle or square while their stellar primaries are marked by a triangle. On the right, we show a sample of brown dwarfs with retrieved C/O taken from Line et al. (2015), Line et al. (2017), Gonzales et al. (2020), Zalesky et al. (2019, 2022), Kitzmann et al. (2020) and Howe et al. (2022). Points in dark blue are isolated objects, while points shown in green are companions. Gl 229B results from this work are marked by a yellow star, whereas Gl 229B results from Howe et al. (2022) are marked by a gray star. Across both plots, objects marked by a circle denote the reported bulk C/O ratio, while squares denote the C/O reported as CH4/H2O. The dashed line in both plots shows the Solar C/O ratio of 0.55 taken from Asplund et al. (2009).
Paper: An Atmospheric Retrieval of the Brown Dwarf Gliese 229B
Authors: Emily Calamari, Jacqueline K. Faherty, Ben Burningham, Eileen Gonzales, Daniella Bardalez-Gagliuffi, Johanna M. Vos, Marina Gemma, Niall Whiteford, Josefine Gaarn
Figure caption: This figure shows the results of a cloudless model with Burrows alkalies where the spectral fit to the K-I doublet in the J spectral band (around 1.25 μm) is severely overestimated. Observed data is shown in black, whereas the maximum likelihood retrieved spectrum is in blue. This model used a wavelength coverage of 1.0–5.0 μm, however, we shorten the wavelength coverage in this figure to give a clearer view of this alkali feature. This serves as a comparison to our best fit model which uses Allard alkalies and shows an objectively good fit in this region.
Paper: Modeling Gamma-Ray Burst Afterglow Observations with an Off-axis Jet Emission
Authors: N. Fraija, A. Galvan-Gamez, B. Betancourt Kamenetskaia, M. G. Dainotti, S. Dichiara, P. Veres, R. L. Becerra, A. C. Caligula do E. S. Pedreira
Figure caption: Promising GW events in O3 that could generate electromagnetic emission with the synchrotron light curves evolving in a constant-density medium with n = 1 cm−3 (left panels) and n = 10−2 cm−3 (right panels), which are decelerating in a constant-density medium. The synchrotron light curves are shown in the X-ray (1 keV; green), optical (R band; brown), and radio (3 GHz; red) bands. The parameter values used are E = 5 × 1050 erg, θ j = 3°, θ obs = 6°, Γ = 100, ε e = 0.1, p = 2.5, ζ  e  = 1.0, and ε B = 10−2. Upper limits are taken from Bochenek (2019); Breeveld et al. (2019); Corsi et al. (2019); Mooley et al. (2019); Palmer et al. (2019); Rhodes et al. (2019); Ridnaia et al. (2020a, 2020b); Sakamoto & Swift Team (2020); Thakur et al. (2020); Tohuvavohu et al. (2019a, 2019b).
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: Far-IR color–color plot from WISE. The long rectangular box defines the limits of these colors for red giant stars without IR excesses, as computed by Mallick et al. (2022). Special attention is called TYC 3797-01268-1 with a dark green × symbol. See Section 5.4 for discussion of this 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: Correlations of log(RWHe) with the Gaia RUWE (top panel) and HGCA (bottom panel). The symbols are the same as in Figure 9 and noted in the figure legend. The red line in each panel indicates the minimum value of each of these excess astrometric motion indicators that might suggest the presence of binary motion. See the text for more details.
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: U − V velocity plane for Li-rich stars (orange ‘x's) and Li-poor stars (gray ‘x's). Bottom Panel: Toomre diagram for Li-rich stars and Li-poor stars. In the Toomre diagram panel, we subtract 239 km s−1 to place the velocities in the local standard of rest. For reference, the dashed lines represent a constant total velocity of 70 and 180 km s−1, respectively. No significant kinematic difference is detected between the Li-rich and Li-poor populations.
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: Constraints on the frequency of binary companions for stars in our sample with Gaia RUWE measurements (top) and those with HGCA accelerations (bottom). In both cases, stars with strong helium absorption have a higher companion occurrence rate at the 2.3σ level for the RUWE subsample and at the 2.0σ level for the HGCA subsample.
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: CDFs of log(M */M ⊙) (left) and sSFR (right) for short GRB hosts (purple), Type Ia SNe hosts (green), Type II SNe hosts (orange), Ca-rich transients hosts (red), SLSNe hosts (pink), and long GRB hosts (blue). For the short GRB host CDFs, we draw 5000 random samples from the respective Prospector posterior distribution, and plot the medians of the resulting CDFs as well as the 68% credible region to represent uncertainty (in light purple). We perform AD tests between all 5000 short GRB host distributions and the other transient hosts’ distributions and show the percentage of tests that reject the null hypothesis that they are derived from the same underlying distribution in the legend. We find Type Ia, Ca-rich transient, and short GRB hosts’ sSFRs to be less than those of other transients and find their stellar masses to be higher.
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: Here, we present the Prospector-produced model spectra (purple lines), photometry (purple squares), and observed photometry (green circles) for the 20 short GRBs with no spectroscopic redshift. Upper limits are denoted with green triangles. We find excellent agreement among the model and observed SED, suggesting that photometric redshifts are in agreement with the true redshifts of the hosts.
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 optical afterglow luminosities of short GRBs at a common rest-frame time of 5 hr in the host frame. While the optical afterglows appear to be fainter in quiescent and transitioning hosts (blue), we find no statistically significant difference when compared to those in star-forming (blue) hosts, implying that luminosity and detectability are not strongly dependent on global host properties.
Paper: Constraining the Nature of the 18 min Periodic Radio Transient GLEAM-X J162759.5-523504.3 via Multiwavelength Observations and Magneto-thermal Simulations
Authors: N. Rea, F. Coti Zelati, C. Dehman, N. Hurley-Walker, D. de Martino, A. Bahramian, D. A. H. Buckley, J. Brink, A. Kawka, J. A. Pons, D. Viganò, V. Graber, M. Ronchi, C. Pardo Araujo, A. Borghese, E. Parent, T. J. Galvin
Figure caption: Left panel: color–magnitude diagram of the five Gaia stars adopting a distance range between 0.8 kpc (filled circles) and 1.8 kpc (empty circles), and extinctions A  V  = 1.0 (magenta) and A  V  = 4.1 (black). The small dots represent the stars in the color–magnitude diagram retrieved from the Gaia DR3 archive within 100 pc and negligible extinction (A  G  < 0.04). Those flagged as non-single stars are shown in blue. The white dwarfs within 100 pc from the Gaia DR2 catalog of Torres et al. (2019) are reported as black dots, and the white dwarfs within 100 pc from the Gaia EDR3 catalog with a probability >90% of being a white dwarf (Gentile Fusillo et al. 2021) are reported as red dots. An extinction vector A  V  = 2 is also reported. Right panel: mass and temperature for known magnetic isolated white dwarfs from Ferrario et al. (2020) compared to the upper limit of r > 22.9 at 5σ obtained by DECam (blue dotted line).
Paper: Constraining the Nature of the 18 min Periodic Radio Transient GLEAM-X J162759.5-523504.3 via Multiwavelength Observations and Magneto-thermal Simulations
Authors: N. Rea, F. Coti Zelati, C. Dehman, N. Hurley-Walker, D. de Martino, A. Bahramian, D. A. H. Buckley, J. Brink, A. Kawka, J. A. Pons, D. Viganò, V. Graber, M. Ronchi, C. Pardo Araujo, A. Borghese, E. Parent, T. J. Galvin
Figure caption: Evolutionary tracks for crust-dominated (top panel) and core-dominated (bottom panel) B-field configurations superimposed on the X-ray luminosity of different pulsar classes, in particular radio-loud magnetars (labeled using a gray circle), XDINSs (in light blue), and low-field magnetars (labeled using gray names). The shaded region corresponds to the limits on the X-ray luminosity and the characteristic age derived for GLEAM-X J1627.
Paper: Constraining the Nature of the 18 min Periodic Radio Transient GLEAM-X J162759.5-523504.3 via Multiwavelength Observations and Magneto-thermal Simulations
Authors: N. Rea, F. Coti Zelati, C. Dehman, N. Hurley-Walker, D. de Martino, A. Bahramian, D. A. H. Buckley, J. Brink, A. Kawka, J. A. Pons, D. Viganò, V. Graber, M. Ronchi, C. Pardo Araujo, A. Borghese, E. Parent, T. J. Galvin
Figure caption: Radio-transient plane including all transient sources with a particular focus on radio magnetars’ bright single pulses (different green tones), GLEAM-X J1627 (violet), and white dwarf systems (different red tones). Data collected from Camilo et al. (2006, 2007), Weltevrede et al. (2011), Deller et al. (2012), Lynch et al. (2015), Majid et al. (2017), Pearlman et al. (2018), Lower et al. (2020), Esposito et al. (2021), Pietka et al. (2015), Marsh et al. (2016), Keane (2018), and Nimmo et al. (2022).
Paper: Recipe for Inferring Subsurface Solar Magnetism via Local Mode Coupling Using Slepian Basis Functions
Authors: Srijan Bharati Das
Figure caption: Sunspot from NOAA 11084/HARP 71 at 00:00:00 of 2010 July 2. Panels (A)–(F) show the six independent components of Lorentz stress computed using HMI vector magnetograms. Panels (G)–(L) show the corresponding reconstructed maps using 38 Slepian functions. Panel (AmG), following the nomenclature A minus G, represents the difference between panel (A) and panel (G). Similarly, (BmH), (CmI), and so on, represent corresponding differences according to this nomenclature. The two lower panels show the first 16 basis functions and the concentration of energy in the spectral domain given by ﹩{\sum }_{\alpha =1}^{38}{\lambda }_{\alpha }\,{G}_{\alpha }^{2}({\boldsymbol{q}})﹩, in logarithmic scale. These basis functions’ subplots share the same x-, y-axes in units of Mm as those in panels (A)–(F). The black dashed circle represents the contour ﹩{ \mathcal R }﹩ in the physical space and the spectral space contour ﹩{ \mathcal Q }﹩ is denoted by the red circle.
Paper: Recipe for Inferring Subsurface Solar Magnetism via Local Mode Coupling Using Slepian Basis Functions
Authors: Srijan Bharati Das
Figure caption: Active region from NOAA 12757/HARP 7405 averaged over two 720 s HMI measurements from 15:00:00–15:24:00 of 2020 January 26. Panels (A)–(F) show the six independent components of Lorentz stress computed using HMI vector magnetograms. Panels (G)–(L) show the corresponding reconstructed maps using 119 Slepian functions. As per the nomenclature adopted in Figure 2, the panels showing the differences between HMI and reconstructed maps are named as (AmG), (BmH), (CmI), and so on. The two lower panels show the first 16 basis functions and the concentration of energy in the spectral domain given by ﹩{\sum }_{\alpha =1}^{119}{\lambda }_{\alpha }\,{G}_{\alpha }^{2}({\boldsymbol{q}})﹩, in logarithmic scale. These basis functions’ subplots share the same x-, y-axes in units of Mm as those in panels (A)–(F). The physical space contour ﹩{ \mathcal R }﹩ is denoted by the closed black dashed curve around the active region, and the spectral space contour ﹩{ \mathcal Q }﹩ is denoted by the red circle.