adsabs/AstroCLIMB huggingface dataset:
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 and spiral galaxies. Top: log M • vs. log M *; bottom: log M * vs. log M •. Left: no additional scatter; center: additional ϵ  y ; right: ϵ  y  and ϵ  x . Dashed red lines: best fits for ellipticals; translucent pink lines: range of possible solutions for ellipticals. Solid black lines: best fits for spirals; translucent gray lines: range of possible solutions for spirals. Symbols as in Figure 15.
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 E+S galaxies. Top: log M • vs. log M *; bottom: log M * vs. log M •. Left: no additional scatter; center: additional ϵ  y ; right: ϵ  y  and ϵ  x . Lines and symbols as in Figure 15.
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 star formation main sequence (SFMS) of our sample. Gray dots represent individual galaxies, while black circles show median values in each stellar mass bin. By fitting in the range of ﹩9\lt \mathrm{log}(M/{M}_{\odot })\lt 11﹩, we obtain the best-fit SFMS shown by the black solid line. Green triangles are the typical values among many previous studies using observations at various wavelengths (Behroozi et al. 2013). The black dashed and dashed–dotted lines indicate the best-fit SFMSs of Speagle et al. (2014) and Whitaker et al. (2014), respectively. Red crosses represent the quiescent Hα emitters with well-constrained SEDs classified by the UVJ diagram. The dotted vertical line shows the stellar mass completeness limit of our sample, while the dotted horizontal line shows the SFR limit of our sample. This limit corresponds to the flux excess threshold to be selected as a Hα emitter.
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 equivalent widths as a function of stellar mass. The limiting equivalent widths of our sample are shown by the dashed black line as well. Since our selection is more sensitive to galaxies with strong continua, the limiting equivalent width depends on stellar mass. The gray and red circles represent individual galaxies and their medians in the mass bins, respectively. The best-fit relation obtained in the range of ﹩\mathrm{log}(M/{M}_{\odot })\gt 9﹩ is shown by the black line extrapolated toward the low-mass end. The blue line and intervals show the typical Hα equivalent width and its scatter reported by Reddy et al. (2018) for galaxies with ﹩\mathrm{log}(M/{M}_{\odot })\simeq 9.3﹩–10.7. Our method seems sensitive enough to detect most of the Hα emitters with ﹩\mathrm{log}(M/{M}_{\odot })\gt 9.0﹩, but only extreme ones can be detected below this 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: Correlation between Hα SFRs and the amount of dust attenuation estimated at the Hα emission line, A Hα . The red hexagonal tiles show the A Hα  distribution of our sample, where A Hα  values are derived by the IRX as described in 2.7. Median values of A Hα  in SFR bins derived from the IRX and the SED fitting by FAST are shown in the red circles and the blue squares, respectively.
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: Our cosmic star formation rate density measurement compared with previous studies. Red and magenta circles represent our measurement with an integration range of L Hα  = 0−1045 (erg s−1) and 1041.6−1045 (erg s−1), respectively. Blue squares and green triangles represent the results of Sobral et al. (2013), with the same integration range as ours. AGN contributions have been removed from both values. The gray circles and crosses show the results of previous studies summarized in Madau & Dickinson (2014) for a comparison, which are measured from UV and/or IR luminosities.
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: Relation between A  V  derived from the SED fitting by FAST and the IRX. Data are median values for each bin from all galaxies without a restriction on S/N. The orange curve shows the best-fit relation. The gray dashed line represents the one-to-one relation as a reference.
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: Locations of the Hα emitters on the rest-frame UVJ diagram (e.g., Wuyts et al. 2007). Symbol color reflects galaxy stellar mass. Red circles indicate objects identified as AGNs by either IR, radio, or X-ray in the catalog of Cowley et al. (2016). The black line represents the criterion of Spitler et al. (2014) separating the star-forming and quiescent galaxies. Identified AGNs by either IR, radio, or X-ray are indicated by the red open circles.
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: Cumulative fractions of Hα fluxes as a function of radius in our simulation. They are obtained assuming the Sérsic profiles with the structural parameters of Nelson et al. (2016) and the seeing of the HiZELS observation. The color coding reflects the stellar masses of the galaxies, while the gray vertical dashed line shows the physical scale corresponding to the 2″ aperture used in Sobral et al. (2013) at a distance of z = 2.23.
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: The Hα luminosity function of our sample with the result of Sobral et al. (2013) for a comparison, which is shown by red circles and blue squares, respectively. Green triangles illustrate how our result changes after removing AGNs as cataloged by Cowley et al. (2016). Each curve shows the best-fit Schechter function with the parameters summarized in Table 1, where 1σ fitting uncertainties of our result are shown by red dashed curves.
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 luminosity function derived from the ZFOURGE data without the aperture corrections assuming A Hα  = 1 (orange triangles). The difference between this work (gray circles) and Sobral et al. (2013; blue squares) is almost completely gone.
Paper: “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap
Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar
Figure caption: Detection horizons for the gravitational waves from our fiducial model shown in Figure 2, with p = 4.5, f K = 0.3, and r b = 1.5 × 109 cm, for aLIGO at design sensitivity (top) and BBO (bottom), assuming optimal matched filtering and an S/N of 8. While the detection horizon for aLIGO is typically limited to ≲100 Mpc, BBO will typically be able to detect such sources from up to several hundred Mpc to several Gpc, with particular sensitivity to progenitors with low–angular momentum “cores” (medium to large values of r b). The contours delineate the final BH masses, as in previous figures.
Paper: “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap
Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar
Figure caption: Scan of the parameter space for model 250.25. The GRB timescale t GRB (top), the total accreted mass [M ⊙] (center top), the accreted mass M GRB during the GRB phase [M ⊙] (center bottom), and the final dimensionless BH spin a BH,fin (bottom) are shown. The red contours indicate the inferred primary mass of GW190521 [M ⊙], together with its 90% confidence limits. The cyan contours delineate the final BH masses of 60 M ⊙ and 130 M ⊙, which approximately correspond to the lower and upper end of the PI mass gap.
Paper: “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap
Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar
Figure caption: Mininum (top) and maximum (bottom) frequencies of the predicted l = m = 2 gravitational-wave emission during the gravitationally unstable phase of collapsar accretion, for the same model shown in Figure 9. The final BH mass contours are drawn as in previous figures.
Paper: “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap
Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar
Figure caption: Scan of the parameter space for model E20 of Heger et al. (2000). The GRB timescale t GRB (top), the total accreted mass [M ⊙] (top center), the accreted mass M GRB during the GRB phase [M ⊙] (bottom center), and the final dimensionless BH spin a BH,fin (bottom) are shown.
Paper: “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap
Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar
Figure caption: The maximum strain amplitude of the characteristic strain h  c  of the gravitational waves from nonaxisymmetric instabilities in self-gravitating collapsar disks across the parameter space of {r b, f K} for our fiducial model shown in Figure 2, with p = 4.5, f K = 0.3, and r b = 1.5 × 109 cm. The characteristic strains range from ∼ 10−24 to 10−22, depending on the rotation profile of the progenitor. The final BH mass contours are drawn as in previous figures.
Paper: “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap
Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar
Figure caption: Scan of the parameter space for model E20 of Heger et al. (2000). The final BH mass (top) and the total ejected mass [M ⊙] in heavy (A > 136) r-process elements (center top), in light (A < 136) r-process elements (center bottom), and in 56Ni (bottom) are shown.
Paper: Follow-up of Young Stars Identified with BANYAN Σ: New Low-mass Members of Nearby Moving Groups
Authors: Asa G. Stahl, Christopher M. Johns-Krull, L. Flagg
Figure caption:  V magnitudes of our observed targets.
Paper: LYRA. III. The Smallest Reionization Survivors
Authors: Thales A. Gutcke, Christoph Pfrommer, Greg L. Bryan, Rüdiger Pakmor, Volker Springel, Thorsten Naab
Figure caption: The peak of the stellar rotation curve, v rot, the 1D velocity dispersion within the half-mass radius, σ ⋆, and their ratio as a function of total stellar mass. Gray data points with error bars show the LG dwarf observations (compiled by Wheeler et al. 2017). Halo A and Halo D are partially rotationally supported.
Paper: LYRA. III. The Smallest Reionization Survivors
Authors: Thales A. Gutcke, Christoph Pfrommer, Greg L. Bryan, Rüdiger Pakmor, Volker Springel, Thorsten Naab
Figure caption:  V-band magnitude as a function of stellar half-mass (light) radius, R 1/2. Gray data points show LG dwarf observations from McConnachie (2012). Filled diamonds show half-mass radii. Small back diamonds also show the Milky Way GCs from Harris (1996). The gray shaded area represents sizes below the dark matter softening length of our simulations. The diagonal light-blue lines are lines of constant surface brightness.
Paper: LYRA. III. The Smallest Reionization Survivors
Authors: Thales A. Gutcke, Christoph Pfrommer, Greg L. Bryan, Rüdiger Pakmor, Volker Springel, Thorsten Naab
Figure caption: Baryon fraction normalized to the cosmic baryon fraction, Ω b /Ω m , as a function of redshift for each simulation. The vertical gray band indicates the time of hydrogen reionization.
Paper: LYRA. III. The Smallest Reionization Survivors
Authors: Thales A. Gutcke, Christoph Pfrommer, Greg L. Bryan, Rüdiger Pakmor, Volker Springel, Thorsten Naab
Figure caption: Line-of-sight (z-axis) stellar velocity (left), velocity dispersion (middle), and skewness (right) of the central ﹩5{R}_{1/2}^{\star }﹩ for Halo A. The halo was rotated such that the angular momentum vector of the stars points in the y-direction; thus, we see a rotating disk edge-on. Some stellar substructure is visible.
Paper: LYRA. III. The Smallest Reionization Survivors
Authors: Thales A. Gutcke, Christoph Pfrommer, Greg L. Bryan, Rüdiger Pakmor, Volker Springel, Thorsten Naab
Figure caption: Cumulative radial distribution of stars within R = 1 kpc for Halo A. The red line shows the distribution for stars formed before reionization, while the blue line is all stars formed afterward. Clearly, the younger stars are more centrally concentrated.
Paper: LYRA. III. The Smallest Reionization Survivors
Authors: Thales A. Gutcke, Christoph Pfrommer, Greg L. Bryan, Rüdiger Pakmor, Volker Springel, Thorsten Naab
Figure caption: Age–metallicity relation for Halo A. The color bar shows the logarithm of the mean SFR in each bin of age and metallicity. Age bins are 500 Myr wide, while metallicity bins are 0.25 dex. Compare this figure to Figure 8(a) of Savino et al. (2019) showing the age–metallicity relation of Tucana dSph.
Paper: LYRA. III. The Smallest Reionization Survivors
Authors: Thales A. Gutcke, Christoph Pfrommer, Greg L. Bryan, Rüdiger Pakmor, Volker Springel, Thorsten Naab
Figure caption: Mass loading factor as a function of time, using the mean SFR until z = 4 as opposed to the instantaneous SFR.
Paper: LYRA. III. The Smallest Reionization Survivors
Authors: Thales A. Gutcke, Christoph Pfrommer, Greg L. Bryan, Rüdiger Pakmor, Volker Springel, Thorsten Naab
Figure caption: Metallicity as a function of V-band magnitude. Gray data points show LG dwarf observations from McConnachie (2012).
Paper: A Low-mass Pre-main-sequence Eclipsing Binary in Lower Centaurus Crux Discovered with TESS
Authors: Keivan G. Stassun, Guillermo Torres, Marina Kounkel, Dax L. Feliz, Luke G. Bouma, Steve B. Howell, Crystal L. Gnilka, E. Furlan
Figure caption: Multicomponent fit to the combined-light SED of 2M1222−57 with NextGen stellar atmosphere models. Observed fluxes are represented as red symbols (horizontal error bars represent filter widths); blue symbols are the corresponding model fluxes. The black curve is a single-source fit using T eff = 3660 K, [Fe/H] = 0, and A  V  = 0, based on the spectroscopic observations of Bowler et al. (2019). Final multicomponent fit includes contributions from the primary eclipsing star (cyan curve), the secondary eclipsing star (red curve), the tertiary companion (magenta curve), and the circumbinary disk (green curve). The disk component is represented both without any material within the central cavity (dotted curve) and with 8 × 10−10 M ⊙ (i.e., 3 × 10−4 M ⊕) of optically thin dust within the cavity (solid curve). The dark blue curve represents the sum total of all components (dotted and solid for the disk model without and with material in the cavity, respectively). Residuals at bottom are in σ units, in the sense of (O − C)/σ  o  for both the bare stellar model (black) and the full multicomponent model (blue).
Paper: A Low-mass Pre-main-sequence Eclipsing Binary in Lower Centaurus Crux Discovered with TESS
Authors: Keivan G. Stassun, Guillermo Torres, Marina Kounkel, Dax L. Feliz, Luke G. Bouma, Steve B. Howell, Crystal L. Gnilka, E. Furlan
Figure caption: Mass, radius, and effective temperature determinations for the eclipsing binary components of 2M1222−57 compared against standard stellar evolution models by Baraffe et al. (2015) and the Dartmouth series (Dotter et al. 2008; Feiden 2016). Isochrone ages are labeled. The best match to the radii (shown in red) is obtained at about 12 Myr for both models, but theoretical predictions appear too hot at this age.
Paper: A Low-mass Pre-main-sequence Eclipsing Binary in Lower Centaurus Crux Discovered with TESS
Authors: Keivan G. Stassun, Guillermo Torres, Marina Kounkel, Dax L. Feliz, Luke G. Bouma, Steve B. Howell, Crystal L. Gnilka, E. Furlan
Figure caption: Out-of-eclipse variations in the TESS light curve of 2M1222−57 for Sectors 10–11 (top) and Sectors 37–38 (bottom). While there is some change in overall morphology of the variations, at both epochs the variations can be characterized with two dominant periodic components: a “double-humped” component at the orbital period that we attribute to rotationally modulated spot variations on one or both of the eclipsing stars (blue dashed curve) and a somewhat more complex, sawtooth-like component with a period of 2.1 days that we attribute to rotationally modulated spot variations on the tertiary companion (red dashed curve). Both periodic components added together are shown in green overlaid on the TESS light-curve data (gray symbols). The residuals (black, bottom) reveal additional, quasi-stochastic variations at the level of ∼2% peak-to-peak that may be attributable to accretion in the system from the circumbinary disk (see Section 5).
Paper: A Low-mass Pre-main-sequence Eclipsing Binary in Lower Centaurus Crux Discovered with TESS
Authors: Keivan G. Stassun, Guillermo Torres, Marina Kounkel, Dax L. Feliz, Luke G. Bouma, Steve B. Howell, Crystal L. Gnilka, E. Furlan
Figure caption: Same as Figure 13 (and on the same scale), now comparing the measured properties of 2M1222−57 against a version of the Dartmouth models that incorporates the effects of magnetic fields (Feiden 2016). Both the radii and temperatures of the two components are well matched by theory at an age of 17 Myr.
Paper: A Low-mass Pre-main-sequence Eclipsing Binary in Lower Centaurus Crux Discovered with TESS
Authors: Keivan G. Stassun, Guillermo Torres, Marina Kounkel, Dax L. Feliz, Luke G. Bouma, Steve B. Howell, Crystal L. Gnilka, E. Furlan
Figure caption: Radial-velocity measurements of 2M1222−57 with our adopted model. Primary and secondary observations are represented with filled and open circles, respectively, the dotted line marks the center-of-mass velocity of the system. Error bars are smaller than the symbol sizes. Residuals are shown at bottom.
Paper: A Low-mass Pre-main-sequence Eclipsing Binary in Lower Centaurus Crux Discovered with TESS
Authors: Keivan G. Stassun, Guillermo Torres, Marina Kounkel, Dax L. Feliz, Luke G. Bouma, Steve B. Howell, Crystal L. Gnilka, E. Furlan
Figure caption: Detrended TESS observations of 2M1222−57 (2 min and 30 min cadence) at primary and secondary eclipse. The 30 min data are displaced vertically for clarity, the solid curve is our binary model. Residuals for both data sets are shown at bottom.
Paper: A Low-mass Pre-main-sequence Eclipsing Binary in Lower Centaurus Crux Discovered with TESS
Authors: Keivan G. Stassun, Guillermo Torres, Marina Kounkel, Dax L. Feliz, Luke G. Bouma, Steve B. Howell, Crystal L. Gnilka, E. Furlan
Figure caption: Cutouts of Full Frame Images from TESS Sectors 10–11, and of 2 minute observations from TESS Sectors 37–38, centered on 2M1222−57. Other stars from the TIC within (cyan) and outside of (green) the pixel mask are shown along with their apparent TESS magnitudes.
Paper: A Low-mass Pre-main-sequence Eclipsing Binary in Lower Centaurus Crux Discovered with TESS
Authors: Keivan G. Stassun, Guillermo Torres, Marina Kounkel, Dax L. Feliz, Luke G. Bouma, Steve B. Howell, Crystal L. Gnilka, E. Furlan
Figure caption: Representative double-lined spectrum of 2M1222−57 for the region around the Li λ6708 line (top) and the Hα λ6563 line (bottom).
Paper: A Low-mass Pre-main-sequence Eclipsing Binary in Lower Centaurus Crux Discovered with TESS
Authors: Keivan G. Stassun, Guillermo Torres, Marina Kounkel, Dax L. Feliz, Luke G. Bouma, Steve B. Howell, Crystal L. Gnilka, E. Furlan
Figure caption: Speckle imaging at 832 nm of 2M1222−57 showing the presence of a faint tertiary companion with Δm = 3.3 ± 0.3 at a separation of 0.″89 (i.e., ∼100 au physical separation).
Paper: Thermal Energy Budget of Electrons in the Inner Heliosphere: Parker Solar Probe Observations
Authors: Joel B. Abraham, Daniel Verscharen, Robert T. Wicks, Jeffersson A. Agudelo Rueda, Christopher J. Owen, Georgios Nicolaou, Seong-Yeop Jeong
Figure caption: Thermal energy budget of solar wind electrons as a function of radial distance. The color scheme is the same as in Figure 1. The black line represents Ξ with cumulative error bars. We use solid lines when a quantity is positive and dashed lines when a quantity is negative.
Paper: Thermal Energy Budget of Electrons in the Inner Heliosphere: Parker Solar Probe Observations
Authors: Joel B. Abraham, Daniel Verscharen, Robert T. Wicks, Jeffersson A. Agudelo Rueda, Christopher J. Owen, Georgios Nicolaou, Seong-Yeop Jeong
Figure caption: Thermal energy budget of solar wind electrons as a function of radial distance. The blue line represents the advection of the thermal energy by the bulk flow. The red line represents the divergence of the heat flux. The yellow line represents the pressure strain term. The purple line represents the expansion term.
Paper: Black Hole Images as Tests of General Relativity: Effects of Plasma Physics
Authors: Feryal Özel, Dimitrios Psaltis, Ziri Younsi
Figure caption: Intensity across a horizontal cross section of a black hole image for different analytic emissivity profiles in optically thin accretion flows. (a) Three radial emissivity profiles for a spherical geometry (h/r → ∞). (b) Same as (a) but for a disk scale height h/r = 0.25. (c) Same as (b) but varying the disk scale height. (d) Same as (b) but varying the observer’s inclination.
Paper: Deblending Galaxies with Generative Adversarial Networks
Authors: Shoubaneh Hemmati, Eric Huff, Hooshang Nayyeri, Agnès Ferté, Peter Melchior, Bahram Mobasher, Jason Rhodes, Abtin Shahidi, Harry Teplitz
Figure caption: GAN trained on multiwavelength HST cutouts. From left to right, columns correspond to F435W, F606W, F750W, F814W, F850lp, F120W, and F160W. Rows show the HST, Subaru, and GAN-recovered resolutions from top to bottom. Peak detection using the PSFs is shown by red crosses on the i-band cutouts in each of the resolutions.
Paper: Deblending Galaxies with Generative Adversarial Networks
Authors: Shoubaneh Hemmati, Eric Huff, Hooshang Nayyeri, Agnès Ferté, Peter Melchior, Bahram Mobasher, Jason Rhodes, Abtin Shahidi, Harry Teplitz
Figure caption: Same as the left panel of Figure 5. Dashed–dotted lines show the improved fractions measured using the multiwavelength GAN. The fall in the last bin is insignificant and due to both poor statistics and proximity to edges of the cutouts.