adsabs/AstroCLIMB huggingface dataset:
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: The log of the spiral arm strength vs. log sSFR for field galaxies in four concentration bins: C < 3.5 (top panel), 3.5 ≤ C < 4 (second panel), 4 ≤ C < 4.5 (third panel), and C ≥ 4.5 (bottom panel). The sSFRs in these plots come from the GSWLC-2. The black line in all plots is the best fit for that concentration range for log sSFR ≥ −12 and 10 ≤ log M* < 11. The slope (m), y-intercept (b), and rms of the best-fit lines are printed on the corresponding plot, along with the Spearman (ρ) and Pearson (r) correlation coefficients.
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: The pitch angle vs. log sSFR for field galaxies in four concentration bins: C < 3.5 (top panel), 3.5 ≤ C < 4 (second panel), 4 ≤ C < 4.5 (third panel), and C ≥ 4.5 (bottom panel). The sSFRs in these plots come from the GSWLC-2. The black line in each plot is the best fit for log sSFR ≥ −12 and 10 ≤ log M* < 11. The slope (m), y-intercept (b), and rms of the best-fit lines are printed on the corresponding plot, along with the Spearman (ρ) and Pearson (r) correlation coefficients.
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: Pitch angle ϕ vs. log sSFR for field galaxies (top panel) and galaxies in massive clusters (bottom panel). The sSFRs in these plots come from the GSWLC-2. The green and red lines in both plots are the best fits for field and cluster galaxies, respectively, with log sSFR ≥ −12 and 10 ≤ log M* < 11. The slope (m), y-intercept (b), and rms of the best-fit lines are printed on the corresponding plot, along with the Spearman (ρ) and Pearson (r) correlation coefficients. The data points are color coded based on concentration (red: C ≥ 4.5; yellow: 4.0 ≤ C < 4.5; green: 3.5 ≤ C < 4.0; blue: C < 3.5).
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: The f3 parameter vs. log sSFR for field galaxies in four concentration bins: C < 3.5 (top panel), 3.5 ≤ C < 4 (second panel), 4 ≤ C < 4.5 (third panel), and C ≥ 4.5 (bottom panel). The sSFRs in these plots come from the GSWLC-2. The Spearman (ρ) and Pearson (r) correlation coefficients for log sSFR ≥ −12 and 10 ≤ log M* < 11 are provided on the corresponding plot.
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: Concentration vs. log sSFR for field galaxies (top panel) and galaxies in massive clusters (bottom panel). The sSFRs in these plots come from the GSWLC-2. The green and red lines in these plots are the best fits for field and cluster galaxies, respectively, for log sSFR ≥ −12 and 10 ≤ log M* < 11. The slope (m), y-intercept (b), and rms of the best-fit lines are printed on the corresponding plot, along with the Spearman (ρ) and Pearson (r) correlation coefficients.
Paper: Destruction of Long-period Comets
Authors: David Jewitt
Figure caption: Nongravitational acceleration, α NG, as a function of the mass-loss rate, ﹩\dot{M}﹩, both referred to r H = 1 au, computed from the data in Table 2. Yellow and red filled circles denote nuclei that survived and that were destroyed by the perihelion passage, respectively. The solid black line has power-law slope B = 0.5. The red dashed line shows the least-squares fit and its index.
Paper: Destruction of Long-period Comets
Authors: David Jewitt
Figure caption: Sublimation timescale, τ  s  (Equation (9)), as a function of the time spent with r H <3 au. Yellow and red filled circles denote nuclei that survived and that were destroyed by the perihelion passage, respectively. The solid black line marks τ  s  = Δt.
Paper: Destruction of Long-period Comets
Authors: David Jewitt
Figure caption: Mass-loss rate vs. nucleus radius. The solid black line shows ﹩\dot{M}(1)=1850{\overline{{r}_{n}}}^{2}﹩.
Paper: Keck/NIRSPEC Studies of He I in the Atmospheres of Two Inflated Hot Gas Giants Orbiting K Dwarfs: WASP-52b and WASP-177b
Authors: James Kirk, Leonardo A. Dos Santos, Mercedes López-Morales, Munazza K. Alam, Antonija Oklopčić, Morgan MacLeod, Li Zeng, George Zhou
Figure caption: Example stellar spectrum of WASP-52 (top panel) and WASP-177 (bottom panel) before and after the telluric correction using molecfit (Kausch et al. 2015; Smette et al. 2015). The black spectra are the pre-corrected data, with the post-corrected data in red. The telluric models are shown in green with the shaded blue region indicating the wavelengths of strong OH emission lines that are removed by our differenced AB nod pairs. The helium triplet is denoted by the vertical dashed gray lines.
Paper: Keck/NIRSPEC Studies of He I in the Atmospheres of Two Inflated Hot Gas Giants Orbiting K Dwarfs: WASP-52b and WASP-177b
Authors: James Kirk, Leonardo A. Dos Santos, Mercedes López-Morales, Munazza K. Alam, Antonija Oklopčić, Morgan MacLeod, Li Zeng, George Zhou
Figure caption: WASP-52's spectra centered on the helium triplet (shown by the vertical dashed lines). Top panel: individual stellar spectra, showing the out-of-transit spectra (black) and the in-transit spectra (red). Middle panel: combined “master” out-of-transit and in-transit spectra. Bottom panel: residual (excess) absorption centered on the helium triplet.
Paper: Keck/NIRSPEC Studies of He I in the Atmospheres of Two Inflated Hot Gas Giants Orbiting K Dwarfs: WASP-52b and WASP-177b
Authors: James Kirk, Leonardo A. Dos Santos, Mercedes López-Morales, Munazza K. Alam, Antonija Oklopčić, Morgan MacLeod, Li Zeng, George Zhou
Figure caption: Same as Figure 2 but for WASP-177.
Paper: The 3D Galactocentric Velocities of Kepler Stars: Marginalizing Over Missing Radial Velocities
Authors: Ruth Angus, Adrian M. Price-Whelan, Joel C. Zinn, Megan Bedell, Yuxi (Lucy) Lu, Daniel Foreman-Mackey
Figure caption: The distribution of inferred stellar velocities and distances. Figure 8 shows the inferred velocities of 5000 randomly selected Kepler stars. The 2D distributions of inferred stellar velocities are plotted in the lower-left panels, with black contours indicating the stellar number density. The red contours in the lower-left panels show the marginal projections of the Gaussian prior distribution in 2D. The upper-right panels in the figure, lying on the plot’s diagonal, show the 1D distributions (histograms) of stellar velocities. The black histogram shows the distribution of inferred velocities, the blue histogram shows the distribution of velocities for stars with RVs, and the red lines show the 1D marginal Gaussian prior distributions. This figure shows that the distributions of inferred velocities are broadly similar to the distributions of velocities directly calculated using RVs, and the prior constructed from them.
Paper: The 3D Galactocentric Velocities of Kepler Stars: Marginalizing Over Missing Radial Velocities
Authors: Ruth Angus, Adrian M. Price-Whelan, Joel C. Zinn, Megan Bedell, Yuxi (Lucy) Lu, Daniel Foreman-Mackey
Figure caption:  x, y, and  z  positions of stars observed by Kepler, showing the orientation of the Kepler field. The Sun’s position is indicated with a Solar symbol. The direction of the field is almost aligned with the  y -axis and almost perpendicular to the x- and  z -axes, which is why v  x  and v   z   can be tightly constrained for Kepler stars without RVs, but v  y  cannot.
Paper: The 3D Galactocentric Velocities of Kepler Stars: Marginalizing Over Missing Radial Velocities
Authors: Ruth Angus, Adrian M. Price-Whelan, Joel C. Zinn, Megan Bedell, Yuxi (Lucy) Lu, Daniel Foreman-Mackey
Figure caption: Velocity and distance distributions of faint (blue) and bright (orange) stars with RVs, shown as KDEs. Gaussian fits to these distributions are shown as dashed lines in corresponding colors. The solid black line shows the Gaussian fit to all data (bright and faint combined) and is the prior we ended up using in our model. This figure highlights the differences between the velocities and distances of bright and faint stars (with RVs) in our sample.