adsabs/AstroCLIMB huggingface dataset:
Paper: Dependence of Molecular Cloud Samples on Angular Resolution, Sensitivity, and Algorithms
Authors: Qing-Zeng Yan, Ji Yang, Yang Su, Yan Sun, Xin Zhou, Ye Xu, Hongchi Wang, Shaobo Zhang, Zhiwei Chen
Figure caption: Molecular clouds of the MWISP survey against the velocity resolution. The number of molecular clouds only takes into account of those that have parts in the PPV range of 130° ≤ l ≤ 135°, −2° ≤ b ≤ −1°, and −20 ≤ V LSR ≤ −10 km s−1. In the displayed three cases, the velocity resolutions are 0.33, 0.84, or 1.34 km s−1, and 99, 84, and 69 molecular clouds are identified, respectively.
Paper: Dependence of Molecular Cloud Samples on Angular Resolution, Sensitivity, and Algorithms
Authors: Qing-Zeng Yan, Ji Yang, Yang Su, Yan Sun, Xin Zhou, Ye Xu, Hongchi Wang, Shaobo Zhang, Zhiwei Chen
Figure caption: Molecular clouds against spatial smoothing of the MWISP survey. The number of molecular clouds only takes into account those that have parts in the PPV range of 130° ≤ l ≤ 135°, −2° ≤ b ≤ −1°, and −20 ≤ V LSR ≤ −10 km s−1. In the displayed three cases, from top to bottom, 31, 5, and 2 molecular clouds are identified, respectively.
Paper: Dependence of Molecular Cloud Samples on Angular Resolution, Sensitivity, and Algorithms
Authors: Qing-Zeng Yan, Ji Yang, Yang Su, Yan Sun, Xin Zhou, Ye Xu, Hongchi Wang, Shaobo Zhang, Zhiwei Chen
Figure caption: Molecular clouds under different cutoffs of the MWISP survey. The number of molecular clouds only takes into account those that have parts in the PPV range of 130° ≤ l ≤ 135°, −2° ≤ b ≤ −1°, and −20 ≤ V LSR ≤ −10 km s−1. In the displayed three cases, from top to bottom, 118, 88, and 49 molecular clouds are identified, respectively.
Paper: Speckle Interferometry at SOAR in 2021
Authors: Andrei Tokovinin, Brian D. Mason, Rene A. Mendez, Edgardo Costa
Figure caption: Updated orbits of two calibrators, STF 1196 AB (top) and STF 2262 AB (bottom). Accurate speckle measurements are plotted as squares (red color marks the 2021 observations published here), the less accurate micrometric observations as crosses. Dotted lines connect the positions to the locations on the orbit (ellipse). The scale is in arcseconds, and the main component is at coordinate origin.
Paper: Speckle Interferometry at SOAR in 2021
Authors: Andrei Tokovinin, Brian D. Mason, Rene A. Mendez, Edgardo Costa
Figure caption: Fragments of speckle ACFs of some newly resolved triple stars. The intensity and spatial scales are chosen for best representation of each system. North is up, and east is left. Blue letters mark the ACF peaks corresponding to the component’s location (as opposed to other symmetric peaks); O marks the ACF center. The outer and inner separations are indicated.
Paper: Speckle Interferometry at SOAR in 2021
Authors: Andrei Tokovinin, Brian D. Mason, Rene A. Mendez, Edgardo Costa
Figure caption: Four orbits computed here for the first time but, nevertheless, are relatively well constrained. See the caption to Figure 4.
Paper: Rotation of Low-mass Stars in Upper Centaurus–Lupus and Lower Centaurus–Crux with TESS
Authors: L. M. Rebull, J. R. Stauffer, L. A. Hillenbrand, A. M. Cody, Ethan Kruse, Brian P. Powell
Figure caption: The log of the mean flux from the PCA eleanor LCs plotted against Gaia G (left), and the log of the mean flux from the CDIPS LCs plotted against Gaia G (right). The discarded targets are red; gold, silver, and bronze members are colored correspondingly. The black line on the left is given by log(mean PCA flux)=−0358 × G + 8.45. The black line divides the stars whose G is much different than the mean PCA LC flux from those whose G seems appropriate given their mean PCA flux; stars above this line are likely to be contaminated by neighbors. Gold members (by definition) have a mean PCA flux consistent with their G. Not every one of our targets has an eleanor LC, so the right plot repeats the analysis using CDIPS; the black line is the same on the right, just shifted down by 0.3 dex. The scatter is worse for the eleanor LCs (left plot) than for the CDIPS LCs (right plot), because there are many more outliers in the eleanor LCs.
Paper: Rotation of Low-mass Stars in Upper Centaurus–Lupus and Lower Centaurus–Crux with TESS
Authors: L. M. Rebull, J. R. Stauffer, L. A. Hillenbrand, A. M. Cody, Ethan Kruse, Brian P. Powell
Figure caption:  P (in days) vs. ﹩{(V-{K}_{{\rm{s}}})}_{0}﹩, with disks removed: density maps, where the darker shades indicate more sources in those cells. Each cluster is self-normalized, such that the darkest shade is the best populated within that cluster, which is a different absolute number (and sample fraction) in each cluster. At the high-mass end, the distribution is well defined in Pleiades and Praesepe, but much less so in USco or UCL/LCC (which is just the gold member sample). The low-mass end is well defined in all four clusters. See the text for more discussion.
Paper: Rotation of Low-mass Stars in Upper Centaurus–Lupus and Lower Centaurus–Crux with TESS
Authors: L. M. Rebull, J. R. Stauffer, L. A. Hillenbrand, A. M. Cody, Ethan Kruse, Brian P. Powell
Figure caption: Comparisons of the periods derived here with those found in the literature. Upper left: Kiraga (2012) periods; upper right: Mellon et al. (2017) periods; center left: Gaia DR2 periods; center right: ASAS-SN periods; lower left: all other literature (see the text and Table 4). Periods >20 days are not shown. In all panels, the gold, silver, and bronze members are indicated, along with the discarded sources (red); note that some of the discarded sources are rejected because the period in the LC cannot be securely tied to an individual source. Most periods agree well; the percentages quoted in the figure indicate the periods matching within 20% overall and just for those periods reported in the literature to be <20 days. Note that most points in these plots fall on the 1:1 line.
Paper: Rotation of Low-mass Stars in Upper Centaurus–Lupus and Lower Centaurus–Crux with TESS
Authors: L. M. Rebull, J. R. Stauffer, L. A. Hillenbrand, A. M. Cody, Ethan Kruse, Brian P. Powell
Figure caption: Absolute Gaia color–magnitude diagram, using distances from Bailer-Jones et al. (2018), for the gold, silver, and bronze members, and the rejected targets (see Section 2.3). The stars that appear to be giants (or are even just significantly above the ZAMS defined by the rest of the sample) are immediately apparent. The gold member sample, by definition, has no objects with Bailer-Jones distances >300 pc.
Paper: Rotation of Low-mass Stars in Upper Centaurus–Lupus and Lower Centaurus–Crux with TESS
Authors: L. M. Rebull, J. R. Stauffer, L. A. Hillenbrand, A. M. Cody, Ethan Kruse, Brian P. Powell
Figure caption: [W1] vs. [W1]−[W3] for the gold, silver, bronze, and rejected targets (see Section 2.3). High-confidence disks have an additional star and lower-confidence disks have an additional square. The black line marks the expected disk-free colors from Pecaut & Mamajek (2013). The points that are not identified as disks, but still appear in this plot to have significant [W1]−[W3], are stars for which the only indication of an excess is a marginal [W3] detection with a larger than typical error bar—that is, they do not have a significant excess. Conversely, stars with [W1]−[W3] near 0 that are selected as disks are those that have an IR excess at wavelengths >12 μm. Most of the stars with disks are in the gold sample. Disked stars are not preferentially dropped from the member sample.
Paper: Rotation of Low-mass Stars in Upper Centaurus–Lupus and Lower Centaurus–Crux with TESS
Authors: L. M. Rebull, J. R. Stauffer, L. A. Hillenbrand, A. M. Cody, Ethan Kruse, Brian P. Powell
Figure caption: Histogram of the distances from Bailer-Jones et al. (2018) for the entire sample (black); the discarded targets (red); and the bronze, silver, and gold members (see Section 2.3). There are additional targets with a Bailer-Jones+ distance >300, and those are indicated by the correspondingly colored numbers on the far right-hand side. Most of the sample (and all of the gold sample) straddles the range of the expected distances for UCL/LCC, ∼100–200 pc.
Paper: Rotation of Low-mass Stars in Upper Centaurus–Lupus and Lower Centaurus–Crux with TESS
Authors: L. M. Rebull, J. R. Stauffer, L. A. Hillenbrand, A. M. Cody, Ethan Kruse, Brian P. Powell
Figure caption: Dereddened K s vs. ﹩{(V-{K}_{{\rm{s}}})}_{0}﹩ for the gold, silver, and bronze members, and the rejected targets. The gold sample is the most well-populated across the full color range. There is more scatter here in all the member subsamples than in Figure 9, in part because the stellar distances vary significantly over the cluster. The discarded sample has the most scatter, which makes sense, given that source confusion is important for many of the rejected stars.
Paper: Rotation of Low-mass Stars in Upper Centaurus–Lupus and Lower Centaurus–Crux with TESS
Authors: L. M. Rebull, J. R. Stauffer, L. A. Hillenbrand, A. M. Cody, Ethan Kruse, Brian P. Powell
Figure caption: The log of the contamination ratio from the TIC (Stassun et al. 2018, 2019) plotted against K s. The discarded targets are red; gold, silver, and bronze members are colored correspondingly. The horizontal line is at a contamination ratio of 1.6, a number that we arrived at by inspection (of this and other similar plots) as a reasonable cutoff between the LC being “likely contaminated” and “likely not or at least less likely to be contaminated.” Gold members (by definition) have a contamination ratio <1.6.
Paper: Rotation of Low-mass Stars in Upper Centaurus–Lupus and Lower Centaurus–Crux with TESS
Authors: L. M. Rebull, J. R. Stauffer, L. A. Hillenbrand, A. M. Cody, Ethan Kruse, Brian P. Powell
Figure caption:  P (in days) vs. ﹩{(V-{K}_{{\rm{s}}})}_{0}﹩ for the gold, silver, and bronze members, and the rejected targets. Note that there are two stars from the discarded sample with ﹩{(V-{K}_{{\rm{s}}})}_{0}﹩>8, beyond the plot limits. The gold sample is the best populated and, in this distribution, it is easiest to see structure in. The structure is similar to that found in other clusters; see the text and Figure 12.
Paper: Line-by-line Velocity Measurements: an Outlier-resistant Method for Precision Velocimetry
Authors: Étienne Artigau, Charles Cadieux, Neil J. Cook, René Doyon, Thomas Vandal, Jean-François Donati, Claire Moutou, Xavier Delfosse, Pascal Fouqué, Eder Martioli, François Bouchy, Jasmine Parsons, Andres Carmona, Xavier Dumusque, Nicola Astudillo-Defru, Xavier Bonfils, Lucille Mignon
Figure caption: Sample spectrum of Barnard’s star over a short-domain wavelength within the H band. The telluric-corrected observation is overplotted with the template registered to that star’s line-of-sight velocity accounting for the barycentric radial velocity at the time of observation.
Paper: Transit Hunt for Young and Maturing Exoplanets (THYME). VIII. A Pleiades-age Association Harboring Two Transiting Planetary Systems from Kepler
Authors: Madyson G. Barber, Andrew W. Mann, Jonathan L. Bush, Benjamin M. Tofflemire, Adam L. Kraus, Daniel M. Krolikowski, Andrew Vanderburg, Matthew J. Fields, Elisabeth R. Newton, Dylan A. Owens, Pa Chia Thao
Figure caption: Three-dimensional distance from KOI-3876 as a function of the difference between the observed and predicted radial velocity of candidate members of MELANGE-3, color-coded by the tangential velocity offset from KOI-3876. Errors are shown, although many stars have distance and velocity errors comparable to or smaller than the point size. The top panel shows a histogram of the radial velocity difference. The predicted velocities were calculated assuming each candidate has an identical UVW to KOI-3876. We do not expect all true members to be exactly consistent with zero velocity difference: KOI-3876 is not necessarily at the kinematic center of the group, the group has some intrinsic velocity spread, and some stars may be tight binaries. The overdensity of points near zero velocity difference is strong evidence that the association is real and extends to at least to 50 pc from KOI-3876.
Paper: Transit Hunt for Young and Maturing Exoplanets (THYME). VIII. A Pleiades-age Association Harboring Two Transiting Planetary Systems from Kepler
Authors: Madyson G. Barber, Andrew W. Mann, Jonathan L. Bush, Benjamin M. Tofflemire, Adam L. Kraus, Daniel M. Krolikowski, Andrew Vanderburg, Matthew J. Fields, Elisabeth R. Newton, Dylan A. Owens, Pa Chia Thao
Figure caption: Gaia color–magnitude diagram of all stars within 5  km s−1 in tangential velocity and 50 pc of KOI-3876, excluding those with highly contaminated photometry (Riello et al. 2021). Points are color-coded by the difference between their expected and observed tangential velocity, assuming a perfect UVW match to KOI-3876 and assigned transparency based on their three-dimensional distance from KOI-3876. Stars with radial velocities consistent with KOI-3876 are marked with blue circles, and those with discrepant velocities are changed to plus signs (and excluded from the color-coding). Approximate main and Pleiades single-star sequences are shown as colored lines (Pecaut & Mamajek 2013; Lodieu et al. 2019).
Paper: Transit Hunt for Young and Maturing Exoplanets (THYME). VIII. A Pleiades-age Association Harboring Two Transiting Planetary Systems from Kepler
Authors: Madyson G. Barber, Andrew W. Mann, Jonathan L. Bush, Benjamin M. Tofflemire, Adam L. Kraus, Daniel M. Krolikowski, Andrew Vanderburg, Matthew J. Fields, Elisabeth R. Newton, Dylan A. Owens, Pa Chia Thao
Figure caption: Lithium equivalent width as a function of Gaia B  P  − R  P  color for candidate friends of KOI-3876 (MELANGE-3; orange), KOI-3876 (red), and members of the 125 Myr Pleiades from Bouvier et al. (2018) and ≃700 Myr Hyades (Cummings et al. 2017). Triangles indicate upper limits. We have excluded MELANGE-3 candidates with velocities inconsistent with membership (as defined in Section 4.7). The MELANGE-3 sequence is consistent with that from Pleiades members; only one star has an anomalously low Li (Gaia EDR3 2044150037698600448) compared to the Pleiades sequence. The high levels of lithium seen in the mid-G dwarfs alone demonstrate that MELANGE-3 is much younger than Hyades. Kepler-970 has weak lithium (Eq W < 40 m Å), but at B  P  − R  P  = 1.5, we expect it to be depleted at this age; we left it off the edge of the figure.
Paper: The COS CGM Compendium. IV. Effects of Varying Ionization Backgrounds on Metallicity Determinations in the z < 1 Circumgalactic Medium
Authors: Justus L. Gibson, Nicolas Lehner, Benjamin D. Oppenheimer, J. Christopher Howk, Kathy L. Cooksey, Andrew J. Fox
Figure caption: Frequency of the metallicity uncertainties for our three different models expressed as number of systems per 1σ uncertainty given by the 84th percentile minus the 16th percentile divided by 2. To summarize the eight different metallicity estimates from the runs with fixed α EUVB, we averaged the uncertainties of each of these runs (gray histogram). The flat prior on α EUVB (red histogram) and Gaussian prior on α EUVB (blue histogram) give almost identical results. The average uncertainty for each model run is shown below the figure legend. Uncertainties are smaller on average when using a single EUVB slope value, but marginalizing over uncertainties in α EUVB generally does not increase the metallicity uncertainties by a large amount.
Paper: The COS CGM Compendium. IV. Effects of Varying Ionization Backgrounds on Metallicity Determinations in the z < 1 Circumgalactic Medium
Authors: Justus L. Gibson, Nicolas Lehner, Benjamin D. Oppenheimer, J. Christopher Howk, Kathy L. Cooksey, Andrew J. Fox
Figure caption: The relationship between [X/H] and α EUVB for the 34 absorbers in our sample. This illustrates the results of our single EUVB slope runs where we calculate the metallicity for α EUVB values of −2.0, −1.8, −1.6, and −1.4. We show results for models with [C/α] fixed to solar (red) and models where we placed a flat prior on [C/α] (blue). Not all absorbers show flat prior results owing to a lack of detected carbon and/or α-elements. There is a clear trend of metallicity increasing as α EUVB increases, and the two sets of models are statistically consistent in the majority of systems. For absorbers 21 and 28, the MCMC modeling is pushing the inferred N H I inference away from the observed value for low and high values of α EUVB, respectively, leading to unreliable results.
Paper: The COS CGM Compendium. IV. Effects of Varying Ionization Backgrounds on Metallicity Determinations in the z < 1 Circumgalactic Medium
Authors: Justus L. Gibson, Nicolas Lehner, Benjamin D. Oppenheimer, J. Christopher Howk, Kathy L. Cooksey, Andrew J. Fox
Figure caption: Individual α EUVB posterior probability distributions for the 34 absorption systems in our sample. Red histograms show the results when assuming a flat prior on α EUVB, and the blue histograms show the results for a Gaussian prior. There are three noticeable “types” of α EUVB posteriors ranging from broad/flat, broad/skewed, and skewed toward either bound of the α EUVB range. Switching to a Gaussian prior generally lowers the probability at the edges of flat distributions but does little for the posteriors that were strongly skewed with a flat prior. Note that out of all of the absorbers, absorber 28 is the only one with a quasi-Gaussian shape fairly well centered on α EUVB = −1.8.
Paper: The COS CGM Compendium. IV. Effects of Varying Ionization Backgrounds on Metallicity Determinations in the z < 1 Circumgalactic Medium
Authors: Justus L. Gibson, Nicolas Lehner, Benjamin D. Oppenheimer, J. Christopher Howk, Kathy L. Cooksey, Andrew J. Fox
Figure caption: The relationship between [X/H] and α EUVB for the 34 absorption systems in our sample when α EUVB is included in our model described with a flat prior. The error bars represent the 16th and 84th percentiles of their respective posterior probability distribution functions. The absorbers are colored by observed N H I to assess any trends with H I column density. Although there is a clear clustering for values of α EUVB around −1.7 to 1.8, the uncertainties here are large and are likely an artifact of being in the center of the α EUVB distribution. The six absorbers at the edge of the α EUVB range have probability distributions strongly skewed toward one bound and will be discussed in more detail in Section 5.
Paper: The COS CGM Compendium. IV. Effects of Varying Ionization Backgrounds on Metallicity Determinations in the z < 1 Circumgalactic Medium
Authors: Justus L. Gibson, Nicolas Lehner, Benjamin D. Oppenheimer, J. Christopher Howk, Kathy L. Cooksey, Andrew J. Fox
Figure caption: Comparison of metallicities from our adopted model with the metallicities derived in CCCII and CCCII, which used the same model with the exception of the choice of EUVB. The dashed black line shows the one-to-one correspondence indicating that the metallicities derived in this work are larger than those derived with the HM05 background. The dotted line shows the median of the differences between the two metallicity estimates. The metallicities derived here are larger by about 0.3 dex on average compared to those derived with the HM05 background.
Paper: The COS CGM Compendium. IV. Effects of Varying Ionization Backgrounds on Metallicity Determinations in the z < 1 Circumgalactic Medium
Authors: Justus L. Gibson, Nicolas Lehner, Benjamin D. Oppenheimer, J. Christopher Howk, Kathy L. Cooksey, Andrew J. Fox
Figure caption: The results of running ﹩{\mathtt{PosteriorStacker}}﹩ (described in the text) on the α EUVB posteriors from our run where we assumed a Gaussian prior on α EUVB. ﹩{\mathtt{PosteriorStacker}}﹩ performs two MCMC runs using UltraNest (Buchner 2021) to infer the properties of the parent α EUVB distribution: one where the parent distribution is assumed to be a Gaussian (red), and one with a less informative Dirichlet assumption (black symbols). The gray symbols show the distribution of mean α EUVB values for our sample.
Paper: The COS CGM Compendium. IV. Effects of Varying Ionization Backgrounds on Metallicity Determinations in the z < 1 Circumgalactic Medium
Authors: Justus L. Gibson, Nicolas Lehner, Benjamin D. Oppenheimer, J. Christopher Howk, Kathy L. Cooksey, Andrew J. Fox
Figure caption: Normalized metallicity distribution for the 34 absorbers in our sample showing that our sample of absorbers tend to have high metallicities.
Paper: An Integrative Analysis of the Rich Planetary System of the Nearby Star e Eridani: Ideal Targets for Exoplanet Imaging and Biosignature Searches
Authors: Ritvik Basant, Jeremy Dietrich, Dániel Apai
Figure caption: The upper left plot shows the DYNAMITE analysis without planet candidates g, c, and f. The upper right plot shows DYNAMITE analysis without planet candidates c and f. The lower left plot shows DYNAMITE analysis without planet candidate c while the lower right plot shows the DYNAMITE analysis with all the planets and planet candidates.
Paper: An Integrative Analysis of the Rich Planetary System of the Nearby Star e Eridani: Ideal Targets for Exoplanet Imaging and Biosignature Searches
Authors: Ritvik Basant, Jeremy Dietrich, Dániel Apai
Figure caption: The number of stable vs. unstable iterations in the four dynamic stability simulations—for the three- and six-planet systems assuming normal and lognormal eccentricity distributions.
Paper: An Integrative Analysis of the Rich Planetary System of the Nearby Star e Eridani: Ideal Targets for Exoplanet Imaging and Biosignature Searches
Authors: Ritvik Basant, Jeremy Dietrich, Dániel Apai
Figure caption: The upper plot shows DYNAMITE analysis on inner solar system when Mars was excluded from the system. The lower plot shows surface temperature distribution for inner solar system based on DYNAMITE analysis.
Paper: An Integrative Analysis of the Rich Planetary System of the Nearby Star e Eridani: Ideal Targets for Exoplanet Imaging and Biosignature Searches
Authors: Ritvik Basant, Jeremy Dietrich, Dániel Apai
Figure caption: The upper left plot shows the DYNAMITE analysis without planet candidates g, c, and f. The upper right plot shows DYNAMITE analysis without planet candidates c and f. The lower left plot shows DYNAMITE analysis without planet candidate f while the lower right plot shows the DYNAMITE analysis with all the planets and planet candidates.
Paper: Atmospheric Characterization of Hot Jupiter CoRoT-1 b Using the Wide Field Camera 3 on the Hubble Space Telescope
Authors: Kayli Glidic, Everett Schlawin, Lindsey Wiser, Yifan Zhou, Drake Deming, Michael Line
Figure caption: Sc-CHIMERA modeled thermal emission spectra for CoRoT-1 b. The median fit closely corresponds to a retrieved maximum value of the heat redistribution parameter (f ), i.e., no redistribution, [M/H] = −0.8, log(C/O) = −1.2, and a = 0.87. However, constraints on [M/H] and log(C/O) are not significant. The scaling factor, a, scales the resulting emission spectrum to account for a hot spot dominating the spectrum (Taylor et al. 2020). Overlaid are four additional spectra with noted values for f, [M/H], log(C/O), and a. A heat redistribution parameter of 1.0 represents full redistribution, 2.0 represents dayside redistribution only, and 2.66 represents no heat redistribution with a concentrated hot spot at the substellar point. Finally, the points shown are the resulting average emission spectrum at HST wavelengths and corresponding Spitzer points at 3.6 and 4.5 μm. We updated Spitzer eclipse depths from Deming et al. (2011) as mentioned in Section 3.6. In the bottom panel, the median fit has been multiplied by the stellar flux to isolate the planet flux and to highlight that the HST data probes the peak of the planet’s flux.