adsabs/AstroCLIMB huggingface dataset:
Paper: The Anisotropic Circumgalactic Medium of Massive Early-type Galaxies
Authors: Huanian Zhang, 华年 张, Dennis Zaritsky
Figure caption: The BPT emission line ratios for two azimuthal and two radial bins. The inner bins, 0.05 < r  s  < 0.125, are represented in red, while the outer, 0.125 < r  s  < 0.25, are in blue. The symbols designate the azimuthal bins as given in the legend. The blue curve shows the boundary between the H II and AGN regions of the diagram and the light gray points represent individual SDSS galaxies.
Paper: Repeated Mergers of Black Hole Binaries: Implications for GW190521
Authors: Oliver Anagnostou, Michele Trenti, Andrew Melatos
Figure caption: Histogram of the various possible recoil velocities for each of the seven mergers in the Snowball merger chain. For each merger we calculate 10,000 different recoils, randomly assigning the spin directions isotropically, but keeping all other properties such as mass, initial separation, and spin magnitudes fixed. Mergers are labeled 1–7 in the order in which they occur, along with the corresponding BHB mass ratio.
Paper: Repeated Mergers of Black Hole Binaries: Implications for GW190521
Authors: Oliver Anagnostou, Michele Trenti, Andrew Melatos
Figure caption: The BH merger tree of Snowball (seven total BHB mergers). Black hole masses are shown on the vertical axis, and the time of mergers is shown on the horizontal axis.
Paper: Spitzer/IRS Full Spectral Modeling to Characterize Mineralogical Properties of Silicate Dust in Heavily Obscured AGNs
Authors: T. Tsuchikawa, H. Kaneda, S. Oyabu, T. Kokusho, H. Kobayashi, Y. Toba
Figure caption: Mass absorption and scattering coefficients of amorphous olivine (top), amorphous pyroxene (upper middle), crystalline olivine (lower middle), and amorphous carbon (bottom). In the panels of amorphous olivine and pyroxene, the mass absorption and scattering coefficients calculated with different ﹩{f}_{\max }﹩ and ﹩{a}_{\max }﹩ are shown with different line styles. The cyan and orange lines show the mass scattering coefficients, and the other colors show the mass absorption coefficients. The mass scattering coefficients of amorphous olivine and pyroxene calculated with ﹩{a}_{\max }=0.25\,\mu {\rm{m}}﹩, crystalline olivine and amorphous carbon are much smaller than their mass absorption coefficients and therefore are not visible in the figure.
Paper: Spitzer/IRS Full Spectral Modeling to Characterize Mineralogical Properties of Silicate Dust in Heavily Obscured AGNs
Authors: T. Tsuchikawa, H. Kaneda, S. Oyabu, T. Kokusho, H. Kobayashi, Y. Toba
Figure caption: Examples of mid-IR spectral fits with models 1 (left), 2 (middle left), 3 (middle right), and 4 (right) to example spectra of IRAS 12127-1412, IRAS 08572+3915, and IRAS15250+3609. The best-fit spectrum by each model is shown with the red solid line. The blue dashed and solid lines represent the AGN-heated dust emission components without ice absorption, ﹩{F}_{{\rm{d}}}^{\mathrm{agn}}﹩, and with ice absorption, ﹩{F}_{{\rm{d}}}^{\mathrm{agn}}\exp (-{\tau }_{\mathrm{ice}})﹩, respectively, while the yellow lines represent the SF-heated dust and PAH emission, F sf, and the line emission components. We show the reduced χ 2 values in the upper left corner in each panel.
Paper: Spitzer/IRS Full Spectral Modeling to Characterize Mineralogical Properties of Silicate Dust in Heavily Obscured AGNs
Authors: T. Tsuchikawa, H. Kaneda, S. Oyabu, T. Kokusho, H. Kobayashi, Y. Toba
Figure caption: An example result of the mid-IR 5–30 μm spectral modeling of heavily obscured AGNs. The black points and the red solid line show the observed spectrum and the best-fit model of IRAS 15250+3609. The blue solid line represents the AGN-heated dust emission components with ice absorption, ﹩{F}_{{\rm{d}}}^{\mathrm{agn}}\exp (-{\tau }_{\mathrm{ice}})﹩, while the yellow lines represent the SF-heated dust and PAH emission, F sf, and the line emission components. We show the reduced χ 2 value in the upper left corner. The residual spectrum normalized by the errors is depicted in the bottom panel.
Paper: Spitzer/IRS Full Spectral Modeling to Characterize Mineralogical Properties of Silicate Dust in Heavily Obscured AGNs
Authors: T. Tsuchikawa, H. Kaneda, S. Oyabu, T. Kokusho, H. Kobayashi, Y. Toba
Figure caption: Properties of silicate dust as a function of the total infrared luminosity, L IR, shown together with the Pearson’s correlation coefficient and the p-value in the top left corner.
Paper: Spitzer/IRS Full Spectral Modeling to Characterize Mineralogical Properties of Silicate Dust in Heavily Obscured AGNs
Authors: T. Tsuchikawa, H. Kaneda, S. Oyabu, T. Kokusho, H. Kobayashi, Y. Toba
Figure caption: Comparison between the results of the four models. The panels at the diagonal positions show the histograms of reduced χ 2 of each model. Black and white bars represent the objects, the fits of which are accepted and rejected, respectively, with a significance level of 5%. The scatter plots at lower diagonal positions are the relationship between the reduced χ 2 values of different two models. Red dashed lines show the thresholds at which the χ 2 between two models are significantly different, with a significance level of 5% on the basis of F-test.
Paper: Spitzer/IRS Full Spectral Modeling to Characterize Mineralogical Properties of Silicate Dust in Heavily Obscured AGNs
Authors: T. Tsuchikawa, H. Kaneda, S. Oyabu, T. Kokusho, H. Kobayashi, Y. Toba
Figure caption: Correlation plots of the pyroxene mass fraction, r pyr, and the crystallinity, r cry, between the results of the previous studies and ours. Note that Tsuchikawa et al. (2021) defined the pyroxene mass fraction with the total mass of amorphous and crystalline silicate, while the present study defines r pyr with the total mass of amorphous silicate. Therefore, we converted the pyroxene mass fraction obtained in Tsuchikawa et al. (2021) to the present definition in this figure.
Paper: Spitzer/IRS Full Spectral Modeling to Characterize Mineralogical Properties of Silicate Dust in Heavily Obscured AGNs
Authors: T. Tsuchikawa, H. Kaneda, S. Oyabu, T. Kokusho, H. Kobayashi, Y. Toba
Figure caption: Histograms of the pyroxene mass fraction, r pyr, and the crystallinity, r cry. Red dashed lines correspond to typical dust properties of the diffuse ISM observed in our Galaxy (Do-Duy et al. 2020).
Paper:  HYPHY: Deep Generative Conditional Posterior Mapping of Hydrodynamical Physics
Authors: Benjamin Horowitz, Max Dornfest, Zarija Lukić, Peter Harrington
Figure caption: Distributions of the χ value for each of our three reconstructions in relation to a single sample. Also plotted is a unit normal Gaussian distribution, showing close agreement. Excess values along the tails indicate model failure, either to estimate proper variance or strong residual biases, or potentially the importance of off-diagonal covariance terms not captured in this analysis. We find these value points constitute a very small volume fraction (≲0.1%). The field with the most variance that is not captured by our model is the temperature field, which is also the most numerically complex to calculate in the original hydrodynamical simulation due to shock physics.
Paper:  HYPHY: Deep Generative Conditional Posterior Mapping of Hydrodynamical Physics
Authors: Benjamin Horowitz, Max Dornfest, Zarija Lukić, Peter Harrington
Figure caption: Two-dimensional histogram of temperature and hydrogen density relation in truth compared to the reconstruction. The orange line indicates a best-fit power-law solution, ﹩T={T}_{0}{n}_{{\rm{H}}}^{\gamma }﹩, across the range of 10−4 < n H < 10−6. Red dashed lines indicate the classification of the gas content of the universe into wCGM, WHIM, diffuse gas, and halo gas. We find excellent agreement in terms of the mean relation, as well as the WHIM component. However, the cool highest-density regions, corresponding to centers of cluster regions (i.e., CGM regions), are not well reconstructed.
Paper: Relation of Observable Stellar Parameters to Mass-loss Rate of AGB Stars in the LMC
Authors: Henry A. Prager, Lee Anne Willson, Massimo Marengo, Michelle J. Creech-Eakman
Figure caption: The split of carbon-rich, fundamental-mode pulsator (C0) AGB stars into “normal” and “extreme” populations is depicted here, using the method found in Blum et al. (2006), Srinivasan et al. (2009), and Boyer et al. (2011), where xAGB stars are those brighter than the 3.6 μm TRGB and with J − [3.6] > 3.1 mag (a), or if there is no near-IR detection, [3.6] − [8.0] > 0.8 (b). Stars in blue are “normal” C stars, and stars in orange are “extreme” AGB stars. All stars could be sorted through the primary method, so the scattered blue stars in panel (b) may be ignored.
Paper: Relation of Observable Stellar Parameters to Mass-loss Rate of AGB Stars in the LMC
Authors: Henry A. Prager, Lee Anne Willson, Massimo Marengo, Michelle J. Creech-Eakman
Figure caption: Plot of [3.6] vs. ﹩\mathrm{log}P﹩ for the stars in the Riebel et al. (2012) data set. M-type stars are in black and C-type stars in blue. M stars brighter than [3.6] = 10.3 are assumed to be red supergiant stars, and are excluded from the analysis. Following the naming convention established in Riebel et al. (2010), sequence 1 defines AGB stars pulsating in the fundamental mode, and sequence 2 defines AGB stars pulsating in the first overtone mode. Definitions of the sequence bounds can be found in Equations (4)–(7).
Paper:  HYPHY: Deep Generative Conditional Posterior Mapping of Hydrodynamical Physics
Authors: Benjamin Horowitz, Max Dornfest, Zarija Lukić, Peter Harrington
Figure caption: Postage stamp posterior samples of the temperature field from Figure 4. There is high variation in the shocked region, showing the hydrodynamical uncertainty the model has learned, while the areas outside the shocked region are stationary (with some occasional edge effects).
Paper:  HYPHY: Deep Generative Conditional Posterior Mapping of Hydrodynamical Physics
Authors: Benjamin Horowitz, Max Dornfest, Zarija Lukić, Peter Harrington
Figure caption: Performance of HYPHY in terms of the Lyα forest flux in redshift space using Equation (7) as implemented in GIMLET. We show the resulting probability density function of Lyα flux, showing substantial biases in the reconstructed flux at F ∼ 0.25, but good agreement at the extremes.
Paper:  HYPHY: Deep Generative Conditional Posterior Mapping of Hydrodynamical Physics
Authors: Benjamin Horowitz, Max Dornfest, Zarija Lukić, Peter Harrington
Figure caption: Performance of HYPHY in terms of the Lyα forest power spectrum in redshift space using Equation (7) as implemented in GIMLET. We show the resulting power spectra of Lyα flux, finding good agreement across a range of scales up to k ∼ 14 h −1 Mpc.
Paper:  HYPHY: Deep Generative Conditional Posterior Mapping of Hydrodynamical Physics
Authors: Benjamin Horowitz, Max Dornfest, Zarija Lukić, Peter Harrington
Figure caption: Figure demonstrating the generation of a light cone using HYPHY. In the top two panels, we show the HYPHY-generated temperature corresponding to the same dark matter distribution as though it was at z = 2.4 and z = 4.0. In the bottom panel we show the same distribution but with a varying redshift across the box, going from z = 4.0 (left) to z = 2.4 (right).
Paper: The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the M •–M * Correlation
Authors: Rosa A. González-Lópezlira, Luis Lomelí-Núñez, Yasna Ordenes-Briceño, Laurent Loinard, Stephen Gwyn, Karla Alamo-Martínez, Gustavo Bruzual, Ariane Lançon, Thomas H. Puzia
Figure caption: BCES fits to elliptical galaxies. Top: log M • vs. log N GC; bottom: log N GC vs. log M •. Left: no additional scatter; center: additional ϵ  y ; right: ϵ  y  and ϵ  x . Solid black lines: best fits; translucent gray lines: range of possible solutions. Solid (red) and open (green) circles represent, respectively, elliptical and lenticular galaxies in the sample of Harris et al. (2014), reclassified as per Sahu et al. (2019b); the blue crosses are the spiral galaxies M 31, M 81, and M 104. Solid blue star: Milky Way. Solid light olive star: NGC 256, with correct number of GCs. Solid purple star: NGC 4258 (González-Lópezlira et al. 2017, 2019); Solid violet, light brown, dark brown, and light blue stars: NGC 3368, NGC 4395, NGC 4736, and NGC 4826, respectively (this work). For NGC 3368, NGC 4395, NGC 4258, NGC 4736, and NGC 4826, random errors of N GC are shown by small bars, while systematic errors, added in quadrature, are illustrated by the large bars. Errors for the MW are smaller than the blue star.
Paper: The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the M •–M * Correlation
Authors: Rosa A. González-Lópezlira, Luis Lomelí-Núñez, Yasna Ordenes-Briceño, Laurent Loinard, Stephen Gwyn, Karla Alamo-Martínez, Gustavo Bruzual, Ariane Lançon, Thomas H. Puzia
Figure caption: MW GC system, at the distance and orientation of studied galaxies, projected coordinates +X proj, +Y proj. Top: NGC 3368; bottom: NGC 4395. Left: 3D rotation about the Galactic ﹩X^{\prime} ﹩-axis before projection on the plane of the sky. Right: 3D rotation about Galactic Y-axis. Solid black line: mask; red crosses: sources visible in the WIRCam FOV; yellow crosses: recovered in the simulation, but outside of the WIRCam FOV; black crosses: masked-out GCs.
Paper: The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the M •–M * Correlation
Authors: Rosa A. González-Lópezlira, Luis Lomelí-Núñez, Yasna Ordenes-Briceño, Laurent Loinard, Stephen Gwyn, Karla Alamo-Martínez, Gustavo Bruzual, Ariane Lançon, Thomas H. Puzia
Figure caption:  K  s -band luminosity functions of the GCCs. Top left: NGC 3368; top right: NGC 4395; bottom left: NGC 4736; bottom right: NGC 4826. Histograms: number of detected objects; solid red lines: expected Gaussian GCLFs (see Table 4 and Section 7).
Paper: The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the M •–M * Correlation
Authors: Rosa A. González-Lópezlira, Luis Lomelí-Núñez, Yasna Ordenes-Briceño, Laurent Loinard, Stephen Gwyn, Karla Alamo-Martínez, Gustavo Bruzual, Ariane Lançon, Thomas H. Puzia
Figure caption: (u* – ﹩i^{\prime} ﹩) vs. (﹩i^{\prime} ﹩ – K  s ) colors and structural parameters of sources in and closely around the selection region of NGC 4826. Top: FWHM; bottom: 100 × SPREAD_MODEL. Left column: all sources; right column: final sample. Symbols as in Figure 5.
Paper: The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the M •–M * Correlation
Authors: Rosa A. González-Lópezlira, Luis Lomelí-Núñez, Yasna Ordenes-Briceño, Laurent Loinard, Stephen Gwyn, Karla Alamo-Martínez, Gustavo Bruzual, Ariane Lançon, Thomas H. Puzia
Figure caption: MW GC system, at the distance and orientation of studied galaxies, projected coordinates + X proj,   + Y proj. Top: NGC 4736; bottom: NGC 4826. Symbols as in Figure 13.
Paper: The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the M •–M * Correlation
Authors: Rosa A. González-Lópezlira, Luis Lomelí-Núñez, Yasna Ordenes-Briceño, Laurent Loinard, Stephen Gwyn, Karla Alamo-Martínez, Gustavo Bruzual, Ariane Lançon, Thomas H. Puzia
Figure caption: Spatial distributions of the GCC samples. Top left: NGC 3368; top right: NGC 4395; bottom left: NGC 4736; bottom right: NGC 4826. The GCCs are shown as green-filled circles. Dark blue ellipse: boundary of areas where source confusion is highest (see text); solid cyan line: R 25.
Paper: The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the M •–M * Correlation
Authors: Rosa A. González-Lópezlira, Luis Lomelí-Núñez, Yasna Ordenes-Briceño, Laurent Loinard, Stephen Gwyn, Karla Alamo-Martínez, Gustavo Bruzual, Ariane Lançon, Thomas H. Puzia
Figure caption: Color distributions of GC systems. Top: NGC 3368 GCCs; second row: NGC 4395; third row: NGC 4736; bottom: NGC 4826. From left to right: (﹩u* -g^{\prime} ﹩), (﹩u* -i^{\prime} ﹩), (g′ − r′), (g′ − i′), (g′ − K  s ), (r′ − i′).
Paper: The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the M •–M * Correlation
Authors: Rosa A. González-Lópezlira, Luis Lomelí-Núñez, Yasna Ordenes-Briceño, Laurent Loinard, Stephen Gwyn, Karla Alamo-Martínez, Gustavo Bruzual, Ariane Lançon, Thomas H. Puzia
Figure caption: Grayscale images of GC candidates, from HST exposures. Top, left to right: J104635+114912 and J104651+114819, in NGC 3368. Bottom: J125039+410913, J125045+410950, and J125131+410849, in NGC 4736.
Paper: The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the M •–M * Correlation
Authors: Rosa A. González-Lópezlira, Luis Lomelí-Núñez, Yasna Ordenes-Briceño, Laurent Loinard, Stephen Gwyn, Karla Alamo-Martínez, Gustavo Bruzual, Ariane Lançon, Thomas H. Puzia
Figure caption: (u* – ﹩i^{\prime} ﹩) vs. (﹩i^{\prime} ﹩ – K  s ) colors and structural parameters of sources in and closely around the selection region of NGC 4736. Top: FWHM; bottom: 100 × SPREAD_MODEL. Left column: all sources; right column: final sample. Symbols as in Figure 5.
Paper: A Selection of Hα Emitters at z = 2.1–2.5 Using the K  s -band Photometry of ZFOURGE
Authors: Yasunori Terao, Lee R. Spitler, Kentaro Motohara, Nuo Chen
Figure caption: Examples of the best-fit SEDs with (blue) and without (orange) the emission-line templates, where IDs are from the ZFOURGE catalog. The Spitzer/IRAC photometry at 3.6 and 4.5 μm bands, which sample rest frame ∼2 μm, cannot be fitted well unless the effects of the emission lines are taken into account. The estimated stellar masses can differ at most ∼0.8 dex. The residuals shown just below the best-fit SEDs are the differences between the observations and the best-fit templates, including emission lines (purple crosses). On the other hand, the flux excesses shown in the bottom panels show the differences between the observations and the continuum fluxes estimated from the best-fit SEDs. Red circles represent the photometry of the K s band, in which Hα emission-line falls. Green circles represent the H medium-band filters of ZFOURGE, in which Hβ and/or O[III] emission lines fall.
Paper: STITCH: A Subgrid-scale Model for Energy Buildup in the Solar Corona
Authors: J. T. Dahlin, C. R. DeVore, S. K. Antiochos
Figure caption: Initial configuration (panels (a) and (c)) of a more complex flux distribution with a corrugated PIL and later snapshots during (b) formation and (d) eruption of its filament channel. Magnetic field lines are color-coded and radial velocity is color shaded as in Figure 3.
Paper: A Selection of Hα Emitters at z = 2.1–2.5 Using the K  s -band Photometry of ZFOURGE
Authors: Yasunori Terao, Lee R. Spitler, Kentaro Motohara, Nuo Chen
Figure caption: Comparison between the Hα fluxes derived from the NB209 color excesses and the flux excesses in the K s band. Both fluxes are in the units of erg s−1 cm−2. The gray line shows the one-to-one relation, while the regions shaded in gray and light gray indicate factor 2 and 5 intervals, respectively. The color coding of individual galaxies corresponds to their stellar masses.
Paper: A Selection of Hα Emitters at z = 2.1–2.5 Using the K  s -band Photometry of ZFOURGE
Authors: Yasunori Terao, Lee R. Spitler, Kentaro Motohara, Nuo Chen
Figure caption: (Left) Changes of the estimated continuum fluxes of our sample when assuming a doubled production rate of the Lyman continuum photons in the SED fitting. (Right) The distribution of the continuum offsets the two models.
Paper: A Selection of Hα Emitters at z = 2.1–2.5 Using the K  s -band Photometry of ZFOURGE
Authors: Yasunori Terao, Lee R. Spitler, Kentaro Motohara, Nuo Chen
Figure caption: Combinations of the emission lines and the filters at each redshift. At z > 1, Hα, Hβ, and [O III] emission lines are observed in the near-infrared regime. Especially, at 2.1 < z < 2.5, Hα falls into the K s broadband filter of the ZFOURGE, while Hβ and [O III] are simultaneously observed in the H medium-band filters.
Paper: STITCH: A Subgrid-scale Model for Energy Buildup in the Solar Corona
Authors: J. T. Dahlin, C. R. DeVore, S. K. Antiochos
Figure caption: Tangential magnetic field injection for a more complex surface flux distribution with a corrugated PIL. Black contours show values of B  r  = [−30, −20, −10, 0, +10, +20] G.
Paper: A Selection of Hα Emitters at z = 2.1–2.5 Using the K  s -band Photometry of ZFOURGE
Authors: Yasunori Terao, Lee R. Spitler, Kentaro Motohara, Nuo Chen
Figure caption: Same as Figure 4, but for the ZFIRE and our method, where the K s-band excesses are derived using the 1.″2 aperture photometry.
Paper: A Selection of Hα Emitters at z = 2.1–2.5 Using the K  s -band Photometry of ZFOURGE
Authors: Yasunori Terao, Lee R. Spitler, Kentaro Motohara, Nuo Chen
Figure caption: Same as Figure 4, but for the KMOS3D and our method.
Paper: A Selection of Hα Emitters at z = 2.1–2.5 Using the K  s -band Photometry of ZFOURGE
Authors: Yasunori Terao, Lee R. Spitler, Kentaro Motohara, Nuo Chen
Figure caption: SFMS plot same as Figure 15 but individual observed galaxies are colored according to luminosity ratios between Hα and UV (see Section 3.8). Simulated observations are shown as gray dots, with the scatter in certain stellar mass bins shown as orange bars. The difference between the simulations and observations at ﹩\mathrm{log}(M/{M}_{\odot })\lt 9﹩ suggest that high photometric scatter is not likely causing the high SFRs at low masses.
Paper: A Selection of Hα Emitters at z = 2.1–2.5 Using the K  s -band Photometry of ZFOURGE
Authors: Yasunori Terao, Lee R. Spitler, Kentaro Motohara, Nuo Chen
Figure caption: Same as Figure 17, but only the starburst galaxies are plotted separately according to their stellar masses. Dashed black horizontal lines represent thresholds of the Hα SFR to be classified as the starburst galaxies in our definition, while the dashed–dotted horizontal lines are our Hα emitter selection. As the luminosity criteria used for starburst selection are always higher than the limiting luminosity for HAE selection, we conclude the ratios in Figure 18 are not likely due to a selection bias.
Paper: A Selection of Hα Emitters at z = 2.1–2.5 Using the K  s -band Photometry of ZFOURGE
Authors: Yasunori Terao, Lee R. Spitler, Kentaro Motohara, Nuo Chen
Figure caption: Hα/UV ratios of the starburst galaxies as a function of stellar mass. The blue circles represent median values in each stellar mass bin. The gray horizontal line shows the value expected from a constant SFH, while the dashed vertical line indicates the stellar mass completeness limit.
Paper: A Selection of Hα Emitters at z = 2.1–2.5 Using the K  s -band Photometry of ZFOURGE
Authors: Yasunori Terao, Lee R. Spitler, Kentaro Motohara, Nuo Chen
Figure caption: Comparison between the Hα and UV luminosities, which are both corrected for dust attenuation. The color coding reflects the stellar masses of the galaxies. The gray line shows the expected relation from a constant SFH without starbursts within 100 Myr (Faisst et al. 2019). The shaded region indicates a ±0.3 dex region about the relation.