adsabs/AstroCLIMB huggingface dataset:
Paper: Ultra-diffuse Galaxies as Extreme Star-forming Environments. I. Mapping Star Formation in H I-rich UDGs
Authors: Erin Kado-Fong, Jenny E. Greene, Song Huang, Andy Goulding
Figure caption: An example of the fitting process for one of the NSA galaxies (NSA ID 5449). Top row: from left, the HSC gri-composite image, the SED cluster map (analogous to panel (f) of Figure 5), and the joint UV-optical SED fit. The joint model SED is the result of fitting the spatially resolved (cluster) optical photometry and global UV photometry. The black curves show the model spectra, while the orange points show the model photometry for each filter. The red points show the global UV-optical photometry. The model fitting and figure fluxes are computed as HSC counts. Middle row: optical-only results for the individual cluster SEDs. The color of the title text corresponds to the color of the region in the top middle panel; the format is equivalent to the joint SED fit (top right), with the addition of the SEDs measured in individual spatial regions (i.e., regional SEDs) as blue points. Here, the red points show the cluster SEDs (i.e., the sum of the regional SEDs) rather than the global photometry. Bottom row: the resultant stellar mass (left) and SFR (right) maps.
Paper: Ultra-diffuse Galaxies as Extreme Star-forming Environments. I. Mapping Star Formation in H I-rich UDGs
Authors: Erin Kado-Fong, Jenny E. Greene, Song Huang, Andy Goulding
Figure caption: A comparison between radial profiles in stellar mass surface density (left) and SFR surface density (right) from our SED fitting method (solid curves) as compared to direct measurements from Leroy et al. (2008, dashed curves). The color of the curves shows the integrated stellar mass of the galaxy in all cases. We find that there is good agreement between our radial profiles and the directly measured profiles in both amplitude and extent.
Paper: Ultra-diffuse Galaxies as Extreme Star-forming Environments. I. Mapping Star Formation in H I-rich UDGs
Authors: Erin Kado-Fong, Jenny E. Greene, Song Huang, Andy Goulding
Figure caption: Optical color vs. stellar mass-to-light ratios in the HSC-g band computed for our UDG (red) and NSA (purple) samples. We find no significant difference in the color–mass relation between the two samples, and additionally find the samples to be reasonably well described by color–mass relations from the literature (Into & Portinari 2013 as the dashed line, Bell et al. 2003 as the dotted line).
Paper: Ultra-diffuse Galaxies as Extreme Star-forming Environments. I. Mapping Star Formation in H I-rich UDGs
Authors: Erin Kado-Fong, Jenny E. Greene, Song Huang, Andy Goulding
Figure caption: Top: a comparison between the best-fit stellar masses of the NSA (purple) and UDG (red) samples using the difference between results derived from the spatially resolved and global photometry (y-axis) and the global optical photometry (x-axis). Bottom: the same as above, but for SFR.
Paper: Ultra-diffuse Galaxies as Extreme Star-forming Environments. I. Mapping Star Formation in H I-rich UDGs
Authors: Erin Kado-Fong, Jenny E. Greene, Song Huang, Andy Goulding
Figure caption: A sample of three example galaxies from the NSA sample, as labeled. From the left, we show the HSC-SSP gri-composite RGB image, the median SFR surface density map, and the median stellar mass surface density map. These galaxies are chosen to span the range of morphologies present in the sample.
Paper: A Stochastic Theory of the Hierarchical Clustering. III. The Nonuniversality and Nonstationarity of the Halo Mass Function
Authors: Andrea Lapi, Tommaso Ronconi, Luigi Danese
Figure caption: Halo mass function at redshifts z = 0 (solid), 1 (dotted–dashed), 3 (dashed), 6 (dotted), 10 (loosely dashed), and 15 (loosely dotted). The best-fit rendition from the time-dependent (green lines) and stationary (blue lines) solutions of the Fokker–Planck equation, and from the excursion set framework (red lines, very close to the blue ones), are compared with the outcomes from the N-body simulations by Shirasaki et al. (2021; gray circles) at z ≲ 6. For higher redshift z ≳ 10 we also report (sampled in 0.5 dex mass logarithmic bins) the inference by Behroozi et al. (2013, 2020; gray crosses), which is an educated recalibration and extrapolation of the Tinker et al. (2008) simulations.
Paper: Conditional H I Mass Functions and the H I-to-halo Mass Relation in the Local Universe
Authors: Xiao Li, Cheng Li, H. J. Mo, Ting Xiao, Jing Wang
Figure caption: The left panel shows the average H I mass of dark matter halos, and the right panel shows the average H I mass of central galaxies. In both panels, the black open circles are the result of Guo et al. (2020) in N  g  ≥ 1 case. For central galaxies, they have been corrected for the confusion effect using our estimator. The black solid line is our result derived from group catalog. The brown, orange, and green solid lines represent the result of L-GALAXIES semianalytical model, Illustris simulation, and IllustrisTNG simulation, respectively. The black upward and downward triangles represent the Milky Way and M31, respectively. In the left panel, the pink dashed line is the result of our CHIMF, and the pink upward arrow with error bars represents Virgo cluster. In the right panel, the black dashed line is the average central H I mass derived from our CHIMFs, and the gray-shaded region represents the 16%–84% percentile of the central CHIMFs in each halo mass bin. The red and blue dashed lines are the mean H I mass of red and blue central galaxies from our CHIMFs. The magenta downward arrows represent the upper limit of H I masses of central galaxies in xGASS sample.