adsabs/AstroCLIMB huggingface dataset:
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 distributions of velocity and distance parameters, inferred using three different priors. The orange line is a KDE that represents the distribution of parameters inferred with a Gaussian prior, estimated from the bright half of the RV sample (G < 13). The blue dashed line shows the results from a prior estimated from the faint half of the RV sample (G > 13)). The black line shows the results from a prior calculated from all stars with RV measurements and is the prior we adopt in our final analysis. This figure shows that all parameters except v  y  are relatively insensitive to the three priors that were tested.
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 posterior PDF over parameters v  x , v  y , v   z   and ln(distance) for a Kepler target chosen at random: KIC 12218729. Blue lines show the location of the star’s “true” parameters, based on a calculation that includes the RV measurement. This figure shows that the velocity parameters are correlated and the star’s posterior is elongated in v  y .
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: A magnitude–temperature diagram of stars in the Kepler field with (left) and without (right) RVs provided by Gaia, LAMOST, and APOGEE. The stars with RVs are generally hotter and more luminous than those without RVs, and include a large number of red clump stars and red-giant-branch stars. Stars without RVs are mostly concentrated on the main sequence.
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 velocity and distance distributions for stars with RV measurements, used to construct a multivariate Gaussian prior over velocity and distance parameters for stars without RVs. The 1 and 2D distributions of the data are shown in black and the prior is indicated in red.
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 apparent Gaia magnitudes for stars in our sample with and without RV measurements from Gaia, LAMOST, and APOGEE.
Paper: USNO Bright Star Catalog, Version 1
Authors: Norbert Zacharias, Valeri V. Makarov, Charles T. Finch, Hugh C. Harris, Jeffrey A. Munn, John P. Subasavage
Figure caption: Median coordinate differences URAT − Hipparcos for 1211 bright stars.
Paper: wdwarfdate: A Python Package to Derive Bayesian Ages of White Dwarfs
Authors: Rocio Kiman, Siyi Xu, 偲艺 许, Jacqueline K. Faherty, Jonathan Gagné, Ruth Angus, Timothy D. Brandt, Sarah L. Casewell, Kelle L. Cruz
Figure caption: Comparison of the fast-test and Bayesian methods included in wdwarfdate for the cooling age and final mass (left and right panels, respectively). We included the one-to-one relation in a black solid line. We run a grid of white dwarfs with T eff = 1500−100,000 K and log g = 7−9.3 and uncertainties of 10% and 1%, respectively. This comparison shows that the estimation of the final mass and cooling age using both methods is similar. The purple points in both panels represent calculations of cooling age that differ more than 1σ between the two methods. The small panel of T eff and log g shows that these points are situated in a dense area of isochrones (Figure 2), which makes the likelihood less constrained. As a consequence, the prior has more influence and makes the Bayesian cooling ages larger.
Paper: wdwarfdate: A Python Package to Derive Bayesian Ages of White Dwarfs
Authors: Rocio Kiman, Siyi Xu, 偲艺 许, Jacqueline K. Faherty, Jonathan Gagné, Ruth Angus, Timothy D. Brandt, Sarah L. Casewell, Kelle L. Cruz
Figure caption: Probabilistic graphical model for the Bayesian method of wdwarfdate. In short, T eff and log g are calculated from the parameters being sampled (m i, t cool and Δm), and these values are compared to the input parameters. In the figure, ﹩\hat{{m}_{{\rm{f}}}}﹩ is the scattered final mass (mass of the white dwarf) calculated from the initial mass using an IFMR, and Δm is an extra parameter to take into account the scatter in this relation. Therefore, m f is the true final mass, calculated by adding Δm to ﹩\hat{{m}_{{\rm{f}}}}﹩.
Paper: wdwarfdate: A Python Package to Derive Bayesian Ages of White Dwarfs
Authors: Rocio Kiman, Siyi Xu, 偲艺 许, Jacqueline K. Faherty, Jonathan Gagné, Ruth Angus, Timothy D. Brandt, Sarah L. Casewell, Kelle L. Cruz
Figure caption: Color–magnitude diagram for the 30 white dwarfs that are candidate wide comovers with M dwarfs (Kiman et al. 2021). We show as red empty circles the white dwarfs that were discarded because they are outside the ranges, which are likely to have followed single-star evolution: 0.5 M ⊙ < m f < 1.1 M ⊙, and also white dwarfs with G BP−GRP < 0.9 to avoid contamination from nonsingle white dwarfs. The only object within these limits that is also discarded did not have an estimation of T eff and log g in Gentile Fusillo et al. (2021). We also show the models of constant mass 0.5 M ⊙, 0.7 M ⊙, 0.9 M ⊙, and 1 M ⊙ for DA white dwarfs (Bergeron et al. 1995; Fontaine et al. 2001; Holberg & Bergeron 2006; Kowalski & Saumon 2006; Bergeron et al. 2011; Tremblay et al. 2011; Blouin et al. 2018).
Paper: wdwarfdate: A Python Package to Derive Bayesian Ages of White Dwarfs
Authors: Rocio Kiman, Siyi Xu, 偲艺 许, Jacqueline K. Faherty, Jonathan Gagné, Ruth Angus, Timothy D. Brandt, Sarah L. Casewell, Kelle L. Cruz
Figure caption: Comparison of the performance of wdwarfdate at lower masses, with the results from Canton et al. (2021). These white dwarfs belong to the M67 cluster (3.5 Gyr). For the final mass, cooling age, and initial mass we show the one-to-one line in black, and for the total age we show the age distributions with the age of the cluster in a black line. For the total age and initial mass we only show the vetted white dwarfs from Canton et al. (2021). We found good agreement between our results and their study. The uncertainties in the initial mass calculated by Canton et al. (2021) are smaller than the point in some cases because they used a well-constrained total age to estimate these masses.
Paper: wdwarfdate: A Python Package to Derive Bayesian Ages of White Dwarfs
Authors: Rocio Kiman, Siyi Xu, 偲艺 许, Jacqueline K. Faherty, Jonathan Gagné, Ruth Angus, Timothy D. Brandt, Sarah L. Casewell, Kelle L. Cruz
Figure caption: We run the white dwarfs in Cummings et al. (2018) using wdwarfdate to compare the results. Most of the parameters are within 1σ, and we color-coded the rest. Both the green and purple points are outliers in the IFMR. In addition, the three purple white dwarfs with higher cooling age have high effective temperatures, which are better modeled with the new cooling tracks implemented in our code (Bédard et al. 2020). The black dot is the massive white dwarf GD 50.
Paper: wdwarfdate: A Python Package to Derive Bayesian Ages of White Dwarfs
Authors: Rocio Kiman, Siyi Xu, 偲艺 许, Jacqueline K. Faherty, Jonathan Gagné, Ruth Angus, Timothy D. Brandt, Sarah L. Casewell, Kelle L. Cruz
Figure caption: Limits of T eff and log g for wdwarfdate: In brown are the values for which the code does not estimate any parameters because they are outside of the allowed range by the cooling tracks. The green-blue five-point stars are the values for which only a final mass and cooling age are estimated using the fast-test method, but not the rest of the parameters because of the limits where the MIST-based Cummings et al. (2018) IFMR (the chosen relation for this example) is calibrated. We color-coded by final mass the values for which wdwarfdate estimates all the parameters using the Bayesian method: final mass, cooling age, initial mass, main-sequence age, and total age.
Paper: wdwarfdate: A Python Package to Derive Bayesian Ages of White Dwarfs
Authors: Rocio Kiman, Siyi Xu, 偲艺 许, Jacqueline K. Faherty, Jonathan Gagné, Ruth Angus, Timothy D. Brandt, Sarah L. Casewell, Kelle L. Cruz
Figure caption: Median relative uncertainty in the total age calculated using the Bayesian method in wdwarfdate. The median is calculated over all T eff and log g results with the same input uncertainties, and the uncertainty in the median is calculated as the standard deviation. In the left panel, the relative uncertainty in T eff is fixed at 1% and 10%. In the right panel, the relative uncertainty in log g is fixed at 1% and 5%.
Paper: wdwarfdate: A Python Package to Derive Bayesian Ages of White Dwarfs
Authors: Rocio Kiman, Siyi Xu, 偲艺 许, Jacqueline K. Faherty, Jonathan Gagné, Ruth Angus, Timothy D. Brandt, Sarah L. Casewell, Kelle L. Cruz
Figure caption: We compare the total age posterior PDF obtained with wdwarfdate for the white dwarfs in Cummings et al. (2018), with the age of the cluster they belong to. Also, we divided the white dwarfs according to their membership and added in a black vertical line the age of the group. We found good agreement between the age of the cluster and the age derived with wdwarfdate.
Paper: wdwarfdate: A Python Package to Derive Bayesian Ages of White Dwarfs
Authors: Rocio Kiman, Siyi Xu, 偲艺 许, Jacqueline K. Faherty, Jonathan Gagné, Ruth Angus, Timothy D. Brandt, Sarah L. Casewell, Kelle L. Cruz
Figure caption: Relative uncertainty in the Bayesian total age estimated using wdwarfdate. We include four cases of different input uncertainties to show the variation as a function of T eff and log g.
Paper: Structural and Dynamical Analysis of the Quiescent Molecular Ridge in the Large Magellanic Cloud
Authors: Molly K. Finn, Remy Indebetouw, Kelsey E. Johnson, Allison H. Costa, C.-H. Rosie Chen, Akiko Kawamura, Toshikazu Onishi, Jürgen Ott, Marta Sewiło, Kazuki Tokuda, Tony Wong, Sarolta Zahorecz
Figure caption: Line widths plotted against sizes of structures in the four different regions: the Ridge (black circles), 30 Dor (blue squares), N159 (orange upward-facing triangles), and N113 (red downward-facing triangles). A power law with a fixed slope of a 1 = 0.5 has been fit to the structures in each region, the error on each fit is shown as shading colored according to the region, and the value of the fitted power-law intercept, a 0, is written in the legend for each region. The relation fit by Solomon et al. (1987) for Milky Way clouds is shown as a solid line, where a 0 = 0.72. The Ridge has a significantly lower fitted intercept than the other three regions, indicating that it has much less kinetic energy for a given size scale.
Paper: Structural and Dynamical Analysis of the Quiescent Molecular Ridge in the Large Magellanic Cloud
Authors: Molly K. Finn, Remy Indebetouw, Kelsey E. Johnson, Allison H. Costa, C.-H. Rosie Chen, Akiko Kawamura, Toshikazu Onishi, Jürgen Ott, Marta Sewiło, Kazuki Tokuda, Tony Wong, Sarolta Zahorecz
Figure caption: Line widths plotted against sizes of structures in the four different regions: the Ridge (black circles), 30 Dor (blue squares), N159 (orange upward-facing triangles), and N113 (red downward-facing triangles). A power law has been fit to the structures in the Ridge (dashed line) and 30 Dor (dotted line), with the error in the fit shown as shaded regions, and the value of the fitted power-law slope, a 1, is written in the legend for each region. We do not fit power laws for N159 and N113 since their small numbers of data points cannot constrain the parameters well. The relation fit by Solomon et al. (1987) for Milky Way clouds is shown as a solid line, where a 0 = 0.72 and a 1 = 0.5. This indicates that 30 Dor follows a steeper power law than the Ridge, so it may have more kinetic energy at larger size scales than the Ridge, although the two values of a 1 are within 3σ of both each other and the fit by Solomon et al. (1987).
Paper: Structural and Dynamical Analysis of the Quiescent Molecular Ridge in the Large Magellanic Cloud
Authors: Molly K. Finn, Remy Indebetouw, Kelsey E. Johnson, Allison H. Costa, C.-H. Rosie Chen, Akiko Kawamura, Toshikazu Onishi, Jürgen Ott, Marta Sewiło, Kazuki Tokuda, Tony Wong, Sarolta Zahorecz
Figure caption: Surface density plotted against the velocity metric, ﹩{\sigma }_{v}^{2}/R﹩, for the Ridge, 30 Dor, N159, and N113. The black line shows virial equilibrium, the blue line shows how equilibrium shifts when clouds are in freefall, and the dashed lines show those same quantities but when an external pressure is applied (Field et al. 2011). The large, semitransparent symbols corresponding to each region indicate the average surface density and velocity metric for each region. The systematic uncertainties for all data points are shown in the legend. The structures in the massive-star-forming regions appear to fall below the line of virial equilibrium more than the structures in the Ridge.
Paper: Structural and Dynamical Analysis of the Quiescent Molecular Ridge in the Large Magellanic Cloud
Authors: Molly K. Finn, Remy Indebetouw, Kelsey E. Johnson, Allison H. Costa, C.-H. Rosie Chen, Akiko Kawamura, Toshikazu Onishi, Jürgen Ott, Marta Sewiło, Kazuki Tokuda, Tony Wong, Sarolta Zahorecz
Figure caption: Perimeter plotted against area of the full contours for dendrogram structures identified in the Ridge, 30 Dor, and N113. We fit power laws to each region to measure the fractal dimension, D 2, with the area−perimeter relation, ﹩P\propto {A}^{{D}_{2}/2}﹩. We fit only structures that are larger than the area of the beam, 45 pc, represented by the vertical line. All of the data sets are consistent with one another, suggesting that they have a similar hierarchical morphology.
Paper: Structural and Dynamical Analysis of the Quiescent Molecular Ridge in the Large Magellanic Cloud
Authors: Molly K. Finn, Remy Indebetouw, Kelsey E. Johnson, Allison H. Costa, C.-H. Rosie Chen, Akiko Kawamura, Toshikazu Onishi, Jürgen Ott, Marta Sewiło, Kazuki Tokuda, Tony Wong, Sarolta Zahorecz
Figure caption: Distribution of α vir values in the Ridge and 30 Dor, showing that the Ridge tends toward higher values of α vir than 30 Dor. A K-S test indicates that the two data sets are not drawn from the same distribution with a p-value of ≪ 0.01.
Paper: Structural and Dynamical Analysis of the Quiescent Molecular Ridge in the Large Magellanic Cloud
Authors: Molly K. Finn, Remy Indebetouw, Kelsey E. Johnson, Allison H. Costa, C.-H. Rosie Chen, Akiko Kawamura, Toshikazu Onishi, Jürgen Ott, Marta Sewiło, Kazuki Tokuda, Tony Wong, Sarolta Zahorecz
Figure caption: Line widths plotted against the sizes of structures in the Ridge identified by 13CO (1–0) (black) and CS (2–1) (blue). We fit a power law with a fixed slope of a 1 = 0.5 to each, which shows that the CS (2–1) structures have a significantly higher fitted intercept than the 13CO (1–0) structures. This indicates that the dense gas traced by CS (2–1) has higher kinetic energy at a given size scale.
Paper: Structural and Dynamical Analysis of the Quiescent Molecular Ridge in the Large Magellanic Cloud
Authors: Molly K. Finn, Remy Indebetouw, Kelsey E. Johnson, Allison H. Costa, C.-H. Rosie Chen, Akiko Kawamura, Toshikazu Onishi, Jürgen Ott, Marta Sewiło, Kazuki Tokuda, Tony Wong, Sarolta Zahorecz
Figure caption: Dendrogram for the Ridge created by astrodendro. Each structure is represented by a vertical line, where the green lines are leaves, black lines are branches, and red lines are trunks. The y-axis indicates the peak of each structure and the intensity at which the structures merge with one another. This plot shows that the Ridge is composed of a few large trunks with a lot of substructure, but also several smaller and more isolated structures.
Paper: Structural and Dynamical Analysis of the Quiescent Molecular Ridge in the Large Magellanic Cloud
Authors: Molly K. Finn, Remy Indebetouw, Kelsey E. Johnson, Allison H. Costa, C.-H. Rosie Chen, Akiko Kawamura, Toshikazu Onishi, Jürgen Ott, Marta Sewiło, Kazuki Tokuda, Tony Wong, Sarolta Zahorecz
Figure caption: Integrated intensity map of N113 in 13CO (1–0). Contours show 1, 5, 9, and 13 K km s−1. The beam is shown in the lower left corner.
Paper: Structural and Dynamical Analysis of the Quiescent Molecular Ridge in the Large Magellanic Cloud
Authors: Molly K. Finn, Remy Indebetouw, Kelsey E. Johnson, Allison H. Costa, C.-H. Rosie Chen, Akiko Kawamura, Toshikazu Onishi, Jürgen Ott, Marta Sewiło, Kazuki Tokuda, Tony Wong, Sarolta Zahorecz
Figure caption: Integrated intensity map of N159 in 13CO (1–0). Contours show 1, 5, 9, and 13 K km s−1. The beam is shown in the lower left corner.
Paper: Unusual Gas Structure in an Otherwise Normal Spiral Galaxy Hosting GRB 171205A/SN 2017iuk
Authors: M. Arabsalmani, S. Roychowdhury, F. Renaud, A. Burkert, E. Emsellem, E. Le Floc'h, E. Pian
Figure caption: Left panel: contours of H I 21 cm emission line overlaid on the R-band Pan-STARRS image of GRB 171205A host galaxy. The outermost contour marks the 3σ level of emission in a single channel (with a velocity width of 34 km s−1). This is equivalent to a H I column density of 5 × 1020 cm−2. Each subsequent contour is in multiples of ﹩\sqrt{2}﹩. The green circle marks the position of GRB 171205A. Middle panel: total intensity map of H I 21 cm emission line in color, overlaid with contours of the velocity map of H I 21 cm emission line for GRB host. The velocity contours in the left butterfly wing mark the velocities of +115, +95, and +75 km s−1 from left to bottom right. In the right butterfly wing, the contours mark the velocities of −25, −45, −65, −85, −105, and −125 km s−1 from bottom left to top. Right panel: the intensity-weighted velocity map of H I 21 cm emission line in color, overlaid with velocity contours as in the middle panel. The size of the images in all panels are 50″ × 50″. The synthesized beam of JVLA observations is shown in the bottom-left corners of the maps.
Paper: Unusual Gas Structure in an Otherwise Normal Spiral Galaxy Hosting GRB 171205A/SN 2017iuk
Authors: M. Arabsalmani, S. Roychowdhury, F. Renaud, A. Burkert, E. Emsellem, E. Le Floc'h, E. Pian
Figure caption: The intensity map of the H I 21 cm emission in 12 successive channels. Each map has a size of 1′ × 1′ and a velocity width of 34 km s−1. The contours of the H I 21 cm intensity are overlaid in white with the dashed contours at −2σ level. The first solid contours are at 2σ level, with each subsequent contours increasing by 1σ. The black contour marks the total H I 21 cm emission (moment-0) from the host galaxy at 3σ significance. The synthesized beam of JVLA observations is shown in the bottom-left corner of each map. The number in the top-left corner of each map is the central velocity of the channel corresponding to the map, relative to the redshift of the galaxy obtained from H I.
Paper: The Open Cluster Chemical Abundances and Mapping Survey. VI. Galactic Chemical Gradient Analysis from APOGEE DR17
Authors: Natalie Myers, John Donor, Taylor Spoo, Peter M. Frinchaboy, Katia Cunha, Adrian M. Price-Whelan, Steven R. Majewski, Rachael L. Beaton, Gail Zasowski, Julia O'Connell, Amy E. Ray, Dmitry Bizyaev, Cristina Chiappini, D. A. García-Hernández, Doug Geisler, Henrik Jönsson, Richard R. Lane, Penélope Longa-Peña, Ivan Minchev, Dante Minniti, Christian Nitschelm, A. Roman-Lopes
Figure caption: Metallicity ([Fe/H]) gradients from the full high-quality sample mapped as a function of guiding radius (R guide; top panel) and current radius (R GC; bottom panel), along with a bilinear fit as in Donor et al. (2020). Clusters flagged as potentially unreliable are shown as light blue circles. The color bar indicates the number of OCCAM member stars per cluster, saturating at five.
Paper: The Open Cluster Chemical Abundances and Mapping Survey. VI. Galactic Chemical Gradient Analysis from APOGEE DR17
Authors: Natalie Myers, John Donor, Taylor Spoo, Peter M. Frinchaboy, Katia Cunha, Adrian M. Price-Whelan, Steven R. Majewski, Rachael L. Beaton, Gail Zasowski, Julia O'Connell, Amy E. Ray, Dmitry Bizyaev, Cristina Chiappini, D. A. García-Hernández, Doug Geisler, Henrik Jönsson, Richard R. Lane, Penélope Longa-Peña, Ivan Minchev, Dante Minniti, Christian Nitschelm, A. Roman-Lopes
Figure caption: Five example color–magnitude diagrams of open clusters analyzed in this study (Table 1). Stars from Gaia EDR3 within twice the cluster radius, as defined in Cantat-Gaudin et al. (2020), are included; stars identified as PM members and inside the cluster radius are blue. Nonmember stars are shown as a Hess diagram in gray. The OCCAM pipeline-identified APOGEE members from DR16 (Donor et al. 2020) are shown in purple. New DR17 OCCAM pipeline-identified APOGEE member stars are shown as orange stars.
Paper: The Open Cluster Chemical Abundances and Mapping Survey. VI. Galactic Chemical Gradient Analysis from APOGEE DR17
Authors: Natalie Myers, John Donor, Taylor Spoo, Peter M. Frinchaboy, Katia Cunha, Adrian M. Price-Whelan, Steven R. Majewski, Rachael L. Beaton, Gail Zasowski, Julia O'Connell, Amy E. Ray, Dmitry Bizyaev, Cristina Chiappini, D. A. García-Hernández, Doug Geisler, Henrik Jönsson, Richard R. Lane, Penélope Longa-Peña, Ivan Minchev, Dante Minniti, Christian Nitschelm, A. Roman-Lopes
Figure caption: We present the measured standard deviations of three key cluster properties (radial velocity, transverse velocity, and parallax) using three different membership subsamples: (1) includes member stars common to both our OCCAM analysis and Cantat-Gaudin et al. (2018), (2) OCCAM members that are not Cantat-Gaudin et al. (2018) members (OCCAM only), and (3) Cantat-Gaudin et al. (2018) only member stars (CG only). Note that the histogram are artificially cut off at 30 to show relevant detail.
Paper: The Open Cluster Chemical Abundances and Mapping Survey. VI. Galactic Chemical Gradient Analysis from APOGEE DR17
Authors: Natalie Myers, John Donor, Taylor Spoo, Peter M. Frinchaboy, Katia Cunha, Adrian M. Price-Whelan, Steven R. Majewski, Rachael L. Beaton, Gail Zasowski, Julia O'Connell, Amy E. Ray, Dmitry Bizyaev, Cristina Chiappini, D. A. García-Hernández, Doug Geisler, Henrik Jönsson, Richard R. Lane, Penélope Longa-Peña, Ivan Minchev, Dante Minniti, Christian Nitschelm, A. Roman-Lopes
Figure caption: The OCCAM DR17 sample in common with Cantat-Gaudin et al. (2020) plotted in the Galactic plane, color-coded by [Fe/H]. Square points are “high-quality” clusters, triangles are the lower quality clusters, and crosses denote clusters which were in the “high-quality” sample of OCCAM-IV but are now in the “low-quality” sample.