adsabs/AstroCLIMB huggingface dataset:
Paper: Image Subtraction in Fourier Space
Authors: Lei Hu, Lifan Wang, Xingzhuo Chen, Jiawen Yang
Figure caption: Performance of the image subtraction of the TESS test. The figure, from left to right, shows the input reference image TESS-REF, science image TESS-SCI, and the resulting difference image by SFFT. The red dashed square at the center of the image indicates a known RRAB variable CV Scl (R.A. = 23:09:30.52 decl. = −35:47:16.9) from the VSX catalog (Watson et al. 2006).
Paper: Hubble Space Telescope Proper Motion (HSTPROMO) Catalogs of Galactic Globular Clusters. VII. Energy Equipartition
Authors: Laura L. Watkins, Roeland P. van der Marel, Mattia Libralato, Andrea Bellini, Jay Anderson, Mayte Alfaro-Cuello
Figure caption: Bianchini et al. (2016) fits to the velocity dispersion as a function of stellar mass for eight of the nine clusters in our sample (the fit for NGC 2808 was unsuccessful). The solid orange lines show the median of the fitted profiles. The darker shaded regions span the 15.9–84.1 percentiles of the fitted profiles (approximately analogous to the 1σ confidence interval). The lighter shaded regions span the 2.5–95.5 percentiles of the fitted profiles (approximately analogous to the 2σ confidence interval). The best-fitting value of the equipartition mass m eq is given in the top-right corner of each plot, and the cluster name in the bottom left. These fits were made to the discrete stars. For visualization purposes, we also show the binned velocity dispersion profiles estimated from the data as black points with error bars.
Paper: Hubble Space Telescope Proper Motion (HSTPROMO) Catalogs of Galactic Globular Clusters. VII. Energy Equipartition
Authors: Laura L. Watkins, Roeland P. van der Marel, Mattia Libralato, Andrea Bellini, Jay Anderson, Mayte Alfaro-Cuello
Figure caption: PM uncertainty quality statistics for NGC 6752 (top, our reference cluster in this work) and NGC 6397 (bottom, an example with two sequences). Left panels: PM uncertainty Δ μ  as a function of magnitude for F606W. Uncertainties in both x and y are shown in this panel. The equivalent plot for F814W is very similar and so is not shown. In the upper panel, there is only one sequence. In the lower panel, two sequences are clearly identified, isolated with a cut at baseline 7 yr for this cluster. The quality analysis was run separately for both sequences. Middle panels: CMD. Right panels: location of the stars in the plane of distance from the cluster center and stellar mass. In all three panels, the color of the points shows the percentile ξ Δ calculated as described in the text and shown in the color bar.
Paper: Hubble Space Telescope Proper Motion (HSTPROMO) Catalogs of Galactic Globular Clusters. VII. Energy Equipartition
Authors: Laura L. Watkins, Roeland P. van der Marel, Mattia Libralato, Andrea Bellini, Jay Anderson, Mayte Alfaro-Cuello
Figure caption: Power-law fits to the velocity dispersion as a function of stellar mass for the nine clusters in our sample. The solid yellow lines show the median of the fitted profiles. The darker shaded regions span the 15.9–84.1 percentiles of the fitted profiles (approximately analogous to the 1σ confidence interval). The lighter shaded regions span the 2.5–95.5 percentiles of the fitted profiles (approximately analogous to the 2σ confidence interval). The best-fitting value of the equipartition parameter η is given in the top-right corner of each plot, and the cluster name in the bottom left. These fits were made to the discrete stars. For visualization purposes, we also show the binned velocity dispersion profiles estimated from the data as black points with error bars.
Paper: Hubble Space Telescope Proper Motion (HSTPROMO) Catalogs of Galactic Globular Clusters. VII. Energy Equipartition
Authors: Laura L. Watkins, Roeland P. van der Marel, Mattia Libralato, Andrea Bellini, Jay Anderson, Mayte Alfaro-Cuello
Figure caption: The distribution of equipartition parameter η estimates from our power-law fits. Top panel: the median values estimated for each of our nine clusters. We see two distinct peaks. No clusters reach full equipartition at η = 0.5. Bottom panel: the distribution of final chain samples (2000 points for each cluster). We still see two peaks, but with considerably more scatter. It is still exceedingly rare for the estimates to reach η = 0.5, but not completely ruled out for some clusters.
Paper: Hubble Space Telescope Proper Motion (HSTPROMO) Catalogs of Galactic Globular Clusters. VII. Energy Equipartition
Authors: Laura L. Watkins, Roeland P. van der Marel, Mattia Libralato, Andrea Bellini, Jay Anderson, Mayte Alfaro-Cuello
Figure caption: Local dispersion cleaning for NGC 6752. Left panel: location of the final sample in the plane of distance from the cluster center and stellar mass, colored by the local dispersion estimated from the fit as indicated by the color bar above. Middle panel: fitted velocity dispersion as a function of distance from the cluster center for the final sample, colored by the stellar mass as indicated by the color bar above. Right panel: fitted velocity dispersion as a function of stellar mass for the final sample, colored by the distance from the cluster center as indicated by the color bar above.
Paper: Hubble Space Telescope Proper Motion (HSTPROMO) Catalogs of Galactic Globular Clusters. VII. Energy Equipartition
Authors: Laura L. Watkins, Roeland P. van der Marel, Mattia Libralato, Andrea Bellini, Jay Anderson, Mayte Alfaro-Cuello
Figure caption: MCMC chain results for the 1D classic power-law fit to NGC 6752. Top panels: progression of the two free parameters σ 1 (left) and η (right) for the whole run. Both panels are flat showing that the chain has converged well. Bottom panels: distribution of walkers at the end of the run. The histograms show the distribution of the individual σ 1 and η parameters and are approximately Gaussian; the scatter plot shows their correlation in phase space.
Paper: Hubble Space Telescope Proper Motion (HSTPROMO) Catalogs of Galactic Globular Clusters. VII. Energy Equipartition
Authors: Laura L. Watkins, Roeland P. van der Marel, Mattia Libralato, Andrea Bellini, Jay Anderson, Mayte Alfaro-Cuello
Figure caption: MCMC chain results for the 1D Bianchini et al. (2016) fit to NGC 6752. Top panels: progression of the two free parameters ﹩{\mathrm{log}}_{10}{m}_{\mathrm{eq}}﹩(left) and σ s(right) for the whole run. Both panels are flat showing that the chain has converged well. Bottom panels: distribution of walkers at the end of the run. The histograms show the distribution of the individual ﹩{\mathrm{log}}_{10}{m}_{\mathrm{eq}}﹩ and σ s parameters and are approximately Gaussian; the scatter plot shows their correlation in phase space.
Paper: Hubble Space Telescope Proper Motion (HSTPROMO) Catalogs of Galactic Globular Clusters. VII. Energy Equipartition
Authors: Laura L. Watkins, Roeland P. van der Marel, Mattia Libralato, Andrea Bellini, Jay Anderson, Mayte Alfaro-Cuello
Figure caption: PSF fit quality statistics for NGC 6752. Left panel: QFIT as a function of magnitude for F606W. The equivalent plot for F814W is very similar and so is not shown. Middle panel: CMD. Right panel: location of the stars in the plane of distance from the cluster center and stellar mass. In all three panels, the color of the points shows the QFIT percentile calculated as described in the text and shown in the color bar.
Paper: Hubble Space Telescope Proper Motion (HSTPROMO) Catalogs of Galactic Globular Clusters. VII. Energy Equipartition
Authors: Laura L. Watkins, Roeland P. van der Marel, Mattia Libralato, Andrea Bellini, Jay Anderson, Mayte Alfaro-Cuello
Figure caption: Surface density profiles of cataloged stars for NGC 6752 (top) and NGC 6441 (bottom). The color of the pixels shows the surface density of stars in the pixel; the color scale is the same in plots so they may be directly compared. The solid, dashed, dotted–dashed, and dotted circles mark 20″, 40″, 60″, and 80″ from the center.
Paper: Hubble Space Telescope Proper Motion (HSTPROMO) Catalogs of Galactic Globular Clusters. VII. Energy Equipartition
Authors: Laura L. Watkins, Roeland P. van der Marel, Mattia Libralato, Andrea Bellini, Jay Anderson, Mayte Alfaro-Cuello
Figure caption: The same as the bottom panels of Figure 9 for NGC 2808. This fit was unsuccessful as it hit the prior boundary at ﹩{\mathrm{log}}_{10}{m}_{\mathrm{eq}}=1﹩.
Paper: Hubble Space Telescope Proper Motion (HSTPROMO) Catalogs of Galactic Globular Clusters. VII. Energy Equipartition
Authors: Laura L. Watkins, Roeland P. van der Marel, Mattia Libralato, Andrea Bellini, Jay Anderson, Mayte Alfaro-Cuello
Figure caption: Correlations between equipartition parameter η (top row) and equipartition mass m eq (bottom row) with number of core relaxation times ﹩{N}_{\mathrm{core}}﹩ (left column), number of median relaxation times N half (middle column), and metallicity [Fe/H] (right column). The yellow (η) and orange (m eq) points show the results for clusters not believed to be core collapsed. Green points highlight the two clusters believed to be core collapsed (NGC 6397 and NGC 6752). The strongest correlations are observed with ﹩{N}_{\mathrm{core}}﹩, weaker correlations are also seen with N half. No correlation is observed with [Fe/H]. In the bottom-left panel, the solid line shows the trend line observed in simulated clusters by Bianchini et al. (2016) in non-core-collapsed (orange) clusters. Our clusters agree with this trend line. The shaded region in the top-left panel shows this trend line for a range of different stellar masses. This panel also provides some insight into how equipartition changes with time and the behavior is consistent with that observed in simulated clusters by Trenti & van der Marel (2013).
Paper: Extremely Slow (V sw < 300 km s−1) Solar Winds (ESSWs) at 1 au: Causes of Extreme Geomagnetic Quiet at Earth
Authors: Bruce T. Tsurutani, Rajkumar Hajra
Figure caption: The ranges of solar wind parameters and geomagnetic activity indices from 1963–2021. From top to bottom are the temporal variations of the ranges of (a) the solar wind velocity (V sw), (b) the proton density (N sw), (c) the proton temperature (T sw), (d) the IMF magnitude (B 0), (e) the z component of the IMF (B z), (f) the Dst index, and (g) the AE index. Panel (h) gives the number of ESSW events (black histograms, scale on the left) and the F10.7 solar flux (blue, scale on the right). For panels (a)–(g), all of the solar wind and geomagnetic activity data with V sw < 300 km s−1 are shown in red and V sw ≥ 300 km s−1 are shown in black.
Paper: Extremely Slow (V sw < 300 km s−1) Solar Winds (ESSWs) at 1 au: Causes of Extreme Geomagnetic Quiet at Earth
Authors: Bruce T. Tsurutani, Rajkumar Hajra
Figure caption: The solar wind velocities at high solar latitudes obtained by Ulysses at ∼2 au from the Sun. On the top (a), the solar wind velocities are given by the radial extent of the plot from the center of the figure (a dial plot). The polar coronal hole area is indicated in the figure of the Sun. Two dashed lines indicate the radial extent of the northern polar coronal hole. On the bottom are histograms of (b) the velocities and (c) densities for the interval over the solar north pole between the two radial dashed lines. Panel (a) is adapted from McComas et al. (2000).
Paper: Hubble Space Telescope Proper Motion (HSTPROMO) Catalogs of Galactic Globular Clusters. VII. Energy Equipartition
Authors: Laura L. Watkins, Roeland P. van der Marel, Mattia Libralato, Andrea Bellini, Jay Anderson, Mayte Alfaro-Cuello
Figure caption: Equipartition radial profiles. Left panels: velocity dispersion of a 1 M ⊙ star σ 1 as a function of distance from the cluster center (shown in blue). Right panels: equipartition parameter η as a function of distance from the cluster center (shown in green). In both panels, the solid line shows the median of the fit in each radial bin, the darker shaded region spans the 15.9–84.1 percentile interval (approximately analogous to the 1σ confidence region), and the lighter shaded region spans the 2.5–95.5 percentile interval (approximately analogous to the 2σ confidence region). The dots mark the bin centers. Horizontal dotted lines mark η = 0 (no equipartition) and η = 0.5 (full equipartition). Where they fall within the fields of view, vertical dotted lines mark the half-light radii R half. In general, the velocity dispersion profiles are highest at the center and fall off with radius, as expected. The equipartition profiles are broadly flat with radius.
Paper: Hubble Space Telescope Proper Motion (HSTPROMO) Catalogs of Galactic Globular Clusters. VII. Energy Equipartition
Authors: Laura L. Watkins, Roeland P. van der Marel, Mattia Libralato, Andrea Bellini, Jay Anderson, Mayte Alfaro-Cuello
Figure caption: Estimates of equipartition η vs. estimates of equipartition mass m eq for the two global fits. Black points with error bars show the estimates. The lines show how η and m eq are related for different stellar masses from Equation (3), colored by mass according to the legend. Proximity to a given line roughly indicates the median mass of the sample.
Paper: Hubble Space Telescope Proper Motion (HSTPROMO) Catalogs of Galactic Globular Clusters. VII. Energy Equipartition
Authors: Laura L. Watkins, Roeland P. van der Marel, Mattia Libralato, Andrea Bellini, Jay Anderson, Mayte Alfaro-Cuello
Figure caption: Comparison of equipartition η as a function of stellar mass for the eight clusters for which both fits could be performed. The yellow lines and shaded regions show the median η from the power-law fits and the 15.9–84.1 percentile interval. These lines are constant by definition. The orange lines and shaded regions shows the median η from the Bianchini et al. (2016) fits and the 15.9–84.1 percentile interval. These are straight lines with slope ﹩\tfrac{1}{2{m}_{\mathrm{eq}}}﹩ for m eq the Bianchini et al. (2016) equipartition parameter.
Paper: Hubble Space Telescope Proper Motion (HSTPROMO) Catalogs of Galactic Globular Clusters. VII. Energy Equipartition
Authors: Laura L. Watkins, Roeland P. van der Marel, Mattia Libralato, Andrea Bellini, Jay Anderson, Mayte Alfaro-Cuello
Figure caption: The distribution of equipartition parameter m eq estimates from our Bianchini et al. (2016) fits. Top panel: the median values estimated for each of the eight clusters. We see two distinct peaks, as we did for the η distribution. Bottom panel: the distribution of final chain samples (2000 points for each cluster). Again, there are hints of two peaks here.
Paper: Disconnecting the Dots: Re-examining the Nature of Stellar “Strings” in the Milky Way
Authors: Catherine Zucker, J. E. G. Peek, Sarah Loebman
Figure caption: Center: a top-down view of stellar strings, colored by age, based on KC19 (see their Figure 13). In the zoom-in boxes, we show the actual distribution of stellar members around the string “spine” in Gaia DR2 for a subsample of four strings spanning a range of ages. The typical distance error to stars is very small with N average parallax signal-to-noise ratio > 44 in Gaia DR2. Because the strings’ “spines” are derived using Gaia DR2 data, these DR2 stellar distributions are the actual data used to derive the string properties in KC19. We find that these four strings are representative of the morphology seen across the full sample: The dispersion along the line of sight is significantly larger than the typical error on the parallax measurements (e.g., Theia 1532, Theia 1104), and many strings are composed of isolated groups with no evidence of a connection between them (e.g., Theia 74, Theia 435). See Figure Set A1 in the Appendix or faun.rc.fas.harvard.edu/czucker/Paper_Figures/String_Gallery_Interactive.html for similar panels for the remaining strings in the KC19 sample, as well as additional comparisons to the Gaia DR3 stellar distributions.
Paper: Disconnecting the Dots: Re-examining the Nature of Stellar “Strings” in the Milky Way
Authors: Catherine Zucker, J. E. G. Peek, Sarah Loebman
Figure caption: The virial state of strings versus the discrepancy between the strings’ reported and predicted lifetimes. The vertical axis shows the ratio of the predicted virial masses of the strings (based on their observed radial velocity dispersions) over their observed masses. Every string in the sample is gravitationally unbound, requiring on average 2 × 104 times larger mass than observed to be in virial equilibrium. Given their unbound state, the dispersal time of the strings should be roughly the crossing time. As shown on the horizontal axis, we find that the reported ages of the strings are orders of magnitude larger than the dispersal time, meaning that strings should have dispersed in a small fraction of their reported lifetimes and are thus inconsistent with being physical structures.
Paper: Disconnecting the Dots: Re-examining the Nature of Stellar “Strings” in the Milky Way
Authors: Catherine Zucker, J. E. G. Peek, Sarah Loebman
Figure caption: Change in the 3D spatial dispersion of stars around their string’s spine from Gaia DR2 to Gaia DR3. Each gray dot represents one of the 328 individual strings. The dots show the average percentage change in the 3D spatial offset from the spine as a function of the average increase in the signal-to-noise ratio of the parallax measurements for the stars. A positive percentage (blue region) indicates the stars move closer to their spine with improved parallax measurements, while a negative percentage (orange region) indicates they move farther away. The black line shows the rolling median and indicates that despite a significant improvement in the signal-to-noise ratio of the parallax measurements, the dispersion around the spine does not improve on average as expected of genuine spatial structures. The diagonal line in the top left shows the predicted trend for genuine space structures.
Paper: Disconnecting the Dots: Re-examining the Nature of Stellar “Strings” in the Milky Way
Authors: Catherine Zucker, J. E. G. Peek, Sarah Loebman
Figure caption: Error-weighted radial velocity dispersions of the strings as a function of their reported ages in KC19. Alongside the strings, we show comparable measurements for the extended stellar coronae (Meingast et al. 2021) around nearby open clusters (including, e.g., the Pleaides and α Per) and the stellar streams (Meingast-1/Pisces–Eridanus; see Meingast et al. 2019; Hawkins et al. 2020) summarized in Table 1.
Paper: The Molecular Composition of Shadowed Proto-solar Disk Midplanes Beyond the Water Snowline
Authors: Shota Notsu, Kazumasa Ohno, Takahiro Ueda, Catherine Walsh, Christian Eistrup, Hideko Nomura
Figure caption: Pie charts of the percentage contributions of the dominant carbon-bearing molecules to the total elemental carbon abundance (=1.4 × 10−4, top panels), the dominant oxygen-bearing molecules to the total elemental oxygen abundance (=3.2 × 10−4, middle panels), and the dominant nitrogen-bearing molecules to the total eelemental nitrogen abundancelemental nitrogen abundance (=7.5 × 10−5, bottom panels), at r = 5.3 au (around the current orbit of Jupiter) and t = 106 yr. The left panels show the contributions for the disk midplane with the monotonically decreasing density and temperature profile (f = 1.0), whereas the right panel shows the contributions for the shadowed disk midplane (f = 0.03). These panels show the results for molecular initial abundances (the “inheritance” scenario) and ξ CR(r) = 1.0 × 10−17 [s−1]. The filled and hatched slices are, respectively, the contributions of gaseous and icy molecules. (Top panels): the dark blue, red, black, purple, green, orange, yellow, and light blue slices are, respectively, the contributions of CO2 ice, CO ice, CO gas, H2CO ice, CH4 ice, HCN ice, C2H6 ice, and other molecules (such as NH2CHO ice and CH3OH ice for f = 0.03, and CH3CCH ice, CH2CCH2 ice, and CH3CHCH2 ice for f = 1.0). (Middle panels): the dark blue, red, black, purple, green, and light blue slices are, respectively, the contributions of CO2 ice, CO ice, CO gas, H2CO ice, H2O ice, and other molecules (such as NH2CHO ice and CH3OH ice). (Bottom panels): the dark blue, red, black, purple, green, orange, and light blue slices are, respectively, the contributions of N2 gas, N2 ice, NH3 ice, NH2CHO ice, NH2OH ice, HCN ice, and other molecules (such as HC3N ice).
Paper: The Molecular Composition of Shadowed Proto-solar Disk Midplanes Beyond the Water Snowline
Authors: Shota Notsu, Kazumasa Ohno, Takahiro Ueda, Catherine Walsh, Christian Eistrup, Hideko Nomura
Figure caption: The radial profiles of fractional abundances with respect to total hydrogen nuclei densities at t = 106 yr for H2O (﹩{n}_{{{\rm{H}}}_{2}{\rm{O}}}﹩/n H, top-left panel), CO (n CO/n H, top-right panel), CO2 (﹩{n}_{{\mathrm{CO}}_{2}}﹩/n H, bottom-left panel), and O2 (﹩{n}_{{{\rm{O}}}_{2}}﹩/n H, bottom-right panel). These panels show the results for the radially constant cosmic-ray ionization rate ξ CR(r) = 1.0 × 10−17 [s−1] and molecular initial abundances (the “inheritance” scenario). The dashed and solid lines show the profiles for gaseous and icy molecules, respectively. The black, red, blue, and green lines show the profiles for different values of the parameter f (=1.0, 0.3, 0.03, and 0.003), respectively.
Paper: The Molecular Composition of Shadowed Proto-solar Disk Midplanes Beyond the Water Snowline
Authors: Shota Notsu, Kazumasa Ohno, Takahiro Ueda, Catherine Walsh, Christian Eistrup, Hideko Nomura
Figure caption: The radial profiles of C/O ratios (left panels) and N/O ratios (right panels) at t =106 yr and for molecular initial abundances (the “inheritance” scenario). The dashed and solid lines show the profiles for gaseous and icy molecules, respectively. The black, red, blue, and green lines show the profiles for different values of the parameter f (=1.0, 0.3, 0.03, and 0.003), respectively. The top panels show the results for ξ CR(r) =1.0 × 10−17 [s−1], whereas the bottom panels show the results for ξ CR(r) =1.0 × 10−18 [s−1]. The horizontal dotted lines show the values of the initial elemental abundance ratios (C/O ratio =0.44, N/O ratio =0.23).
Paper: The Molecular Composition of Shadowed Proto-solar Disk Midplanes Beyond the Water Snowline
Authors: Shota Notsu, Kazumasa Ohno, Takahiro Ueda, Catherine Walsh, Christian Eistrup, Hideko Nomura
Figure caption: Same as Figure 3, but for C2H2 (﹩{n}_{{{\rm{C}}}_{2}{{\rm{H}}}_{2}}﹩/n H, top-left panel), C2H4 (﹩{n}_{{{\rm{C}}}_{2}{{\rm{H}}}_{4}}﹩/n H, top-right panel), C3H2 (﹩{n}_{{{\rm{C}}}_{3}{{\rm{H}}}_{2}}﹩/n H, middle-left panel), CH3CCH (﹩{n}_{{\mathrm{CH}}_{3}\mathrm{CCH}}﹩/n H, middle-right panel), CH2CCH2 (﹩{n}_{{\mathrm{CH}}_{2}{\mathrm{CCH}}_{2}}﹩/n H, bottom-left panel), and CH3CHCH2 (﹩{n}_{{\mathrm{CH}}_{3}{\mathrm{CHCH}}_{2}}﹩/n H, bottom-right panel).
Paper: The Molecular Composition of Shadowed Proto-solar Disk Midplanes Beyond the Water Snowline
Authors: Shota Notsu, Kazumasa Ohno, Takahiro Ueda, Catherine Walsh, Christian Eistrup, Hideko Nomura
Figure caption: Same as Figure 3, but for CH3CHO (﹩{n}_{{\mathrm{CH}}_{3}\mathrm{CHO}}﹩/n H, top-left panel), CH3OCH3 (﹩{n}_{{\mathrm{CH}}_{3}{\mathrm{OCH}}_{3}}﹩/n H, top-right panel), HCOOH (n HCOOH/n H, middle-left panel), HCOOCH3 (﹩{n}_{{\mathrm{HCOOCH}}_{3}}﹩/n H, middle-right panel), CH3COOH (﹩{n}_{{\mathrm{CH}}_{3}\mathrm{COOH}}﹩/n H, bottom-left panel), and C2H5OH (﹩{n}_{{{\rm{C}}}_{2}{{\rm{H}}}_{5}{OH}}﹩/n H, bottom-right panel).
Paper: The Molecular Composition of Shadowed Proto-solar Disk Midplanes Beyond the Water Snowline
Authors: Shota Notsu, Kazumasa Ohno, Takahiro Ueda, Catherine Walsh, Christian Eistrup, Hideko Nomura
Figure caption: Same as Figure 3, but for N2 (﹩{n}_{{{\rm{N}}}_{2}}﹩/n H, top-left panel), NH3 (﹩{n}_{{\mathrm{NH}}_{3}}﹩/n H, top-right panel), HCN (﹩{n}_{\mathrm{HCN}}﹩/n H, bottom-left panel), and NH2CHO (﹩{n}_{{\mathrm{NH}}_{2}\mathrm{CHO}}﹩/n H, bottom-right panel).