adsabs/AstroCLIMB huggingface dataset:
Paper: Planets Across Space and Time (PAST). III. Morphology of the Planetary Radius Valley as a Function of Stellar Age and Metallicity in the Galactic Context Revealed by the LAMOST-Gaia-Kepler Sample
Authors: Di-Chang Chen, Ji-Wei Xie, Ji-Lin. Zhou, Jia-Yi Yang, Subo Dong, Zi Zhu, Zheng Zheng, Chao Liu, Weikai Zong, Ali Luo
Figure caption: The period–radius diagram (top panel) and radius distribution (bottom panel) of planets with different kinematic ages t (Gyr) from our selected sample from the LAMOST-Gaia-Kepler catalog. The median values and 1σ uncertainties of kinematic age, [Fe/H], and [α/Fe] of each bin are printed at the top.
Paper: Planets Across Space and Time (PAST). III. Morphology of the Planetary Radius Valley as a Function of Stellar Age and Metallicity in the Galactic Context Revealed by the LAMOST-Gaia-Kepler Sample
Authors: Di-Chang Chen, Ji-Wei Xie, Ji-Lin. Zhou, Jia-Yi Yang, Subo Dong, Zi Zhu, Zheng Zheng, Chao Liu, Weikai Zong, Ali Luo
Figure caption: The five statistics to characterize the radius valley morphology (i.e., C valley, A valley, ﹩{R}_{\mathrm{valley}}^{+}﹩, ﹩{R}_{\mathrm{valley}}^{-}﹩, and f NP) as functions of [α/Fe]. In Section 4.1, we rescale the planet radii to eliminate the influence of stellar mass and planetary orbital period on the boundary of radius valley. The results with rescaling radii are plotted as open circles and shifted to the right to avoid overlapping.
Paper: Planets Across Space and Time (PAST). III. Morphology of the Planetary Radius Valley as a Function of Stellar Age and Metallicity in the Galactic Context Revealed by the LAMOST-Gaia-Kepler Sample
Authors: Di-Chang Chen, Ji-Wei Xie, Ji-Lin. Zhou, Jia-Yi Yang, Subo Dong, Zi Zhu, Zheng Zheng, Chao Liu, Weikai Zong, Ali Luo
Figure caption: The five statistics to characterize the radius valley morphology (i.e., C valley, A valley, ﹩{R}_{\mathrm{valley}}^{+}﹩, ﹩{R}_{\mathrm{valley}}^{-}﹩, and f NP) as functions of the relative probability between thick disk and thin disk (TD/D). In Section 4.1, we rescale the planet radii to eliminate the influence of stellar mass and planetary orbital period on the boundary of radius valley. The results with rescaling radii are plotted as open circles and shifted to the right to avoid overlapping.
Paper: Planets Across Space and Time (PAST). III. Morphology of the Planetary Radius Valley as a Function of Stellar Age and Metallicity in the Galactic Context Revealed by the LAMOST-Gaia-Kepler Sample
Authors: Di-Chang Chen, Ji-Wei Xie, Ji-Lin. Zhou, Jia-Yi Yang, Subo Dong, Zi Zhu, Zheng Zheng, Chao Liu, Weikai Zong, Ali Luo
Figure caption: The period–radius diagram (top panel) and radius distribution (bottom panel) of planets with different metallicity [Fe/H] from our selected sample from the LAMOST-Gaia-Kepler catalog. The median values and 1σ uncertainties of kinematic age, [Fe/H], and [α/Fe] of each bin are printed at the top.
Paper: Planets Across Space and Time (PAST). III. Morphology of the Planetary Radius Valley as a Function of Stellar Age and Metallicity in the Galactic Context Revealed by the LAMOST-Gaia-Kepler Sample
Authors: Di-Chang Chen, Ji-Wei Xie, Ji-Lin. Zhou, Jia-Yi Yang, Subo Dong, Zi Zhu, Zheng Zheng, Chao Liu, Weikai Zong, Ali Luo
Figure caption: The period–radius diagram (top panel) and radius distribution (bottom panel) of planets in different TD/D bins from our sample based on the LAMOST-Gaia-Kepler catalog. Different colors represent planets of different radius: green for super-Earths (1–1.7 R ⊕), gray for valley planets (1.7–2.1 R ⊕), yellow for sub-Neptunes (2.1–3.5 R ⊕), and purple for Neptune-size planets (3.5–6 R ⊕). The median values and 1σ uncertainties of kinematic age, [Fe/H], and [α/Fe] of each bin are printed at the top.
Paper: Planets Across Space and Time (PAST). III. Morphology of the Planetary Radius Valley as a Function of Stellar Age and Metallicity in the Galactic Context Revealed by the LAMOST-Gaia-Kepler Sample
Authors: Di-Chang Chen, Ji-Wei Xie, Ji-Lin. Zhou, Jia-Yi Yang, Subo Dong, Zi Zhu, Zheng Zheng, Chao Liu, Weikai Zong, Ali Luo
Figure caption: The cumulative distributions of stellar mass M *, radius R *, CDPP 4.5 hr, [Fe/H], and [α/Fe] for the four bins with different relative probabilities between thick disk and thin disk TD/D (Section 3.1) before parameter controlling. Here we directly divide our sample into four samples with approximately equal size (∼111) according to TD/D. In each panel, p denotes the p-value of the two-sample K-S test for the distributions of neighboring stars belonging to the last three bins compared to the first bins.
Paper: Planets Across Space and Time (PAST). III. Morphology of the Planetary Radius Valley as a Function of Stellar Age and Metallicity in the Galactic Context Revealed by the LAMOST-Gaia-Kepler Sample
Authors: Di-Chang Chen, Ji-Wei Xie, Ji-Lin. Zhou, Jia-Yi Yang, Subo Dong, Zi Zhu, Zheng Zheng, Chao Liu, Weikai Zong, Ali Luo
Figure caption: The period–radius diagram (top panel) and radius distribution (bottom panel) of planets with different [α/Fe] from our selected sample from the LAMOST-Gaia-Kepler catalog. The median values and 1σ uncertainties of kinematic age, [Fe/H], and [α/Fe] of each bin are printed at the top.
Paper: Size Distribution of Small Jupiter Trojans in the L5 Swarm 
Authors: Kotomi Uehata, Tsuyoshi Terai, Keiji Ohtsuki, Fumi Yoshida
Figure caption: Locations of the nine observed fields of our survey. The size of each circle corresponds to the field of view of Hyper Suprime-Cam. Lines of ecliptic latitude (β) are also shown, with the ecliptic plane shown with the thick line. The background image is taken from Pan-STARRS1 (Chambers et al. 2016).
Paper: Reassessing the Evidence for Time Variability in the Atmosphere of the Exoplanet HAT-P-7 b
Authors: Maura Lally, Andrew Vanderburg
Figure caption: Comparison of measured distributions and simulated distributions. The red histograms in each panel show the distribution of our phase-offset and amplitude variability detected in HAT-P-7 b resulting from our original analysis (shown as a time series in Figure 7). The blue histograms show the results of the test described in Section 5.5, wherein a simulated light curve imitating the background noise from the Kepler light curve of HAT-P-7 b near the period of the planet was created, and phase-offset and amplitude variations were extracted using a linear-fitting scheme imitating our initial analysis. The histogram on the left compares our real results to our simulated results for phase-offset variations, and the histogram on the right does the same for amplitude variations. These histograms show that the variability we detected from our original analysis can be explained by nonplanetary sources of background noise present in the Kepler light curve of HAT-P-7 b, and thus cannot be definitively said to indicate atmospheric variability of the atmosphere of HAT-P-7 b.
Paper: Reassessing the Evidence for Time Variability in the Atmosphere of the Exoplanet HAT-P-7 b
Authors: Maura Lally, Andrew Vanderburg
Figure caption: Lomb–Scargle periodogram of the Kepler short-cadence light curve of HAT-P-7, with the planetary signal removed. Each line represents one of 60 segments of the light curve. The period of HAT-P-7 b is denoted by the vertical black line. The vertical black dotted lines represent the largest range in which we could reasonably expect periodogram features to correspond to variability from the planet itself, based on the fastest phase-offset variability we identified in our HAT-P-7 b results. There is fairly consistent noise over all periods, but there is not a significant spike near the period of the planet. The implications of this are further discussed in Section 5.4.
Paper: Planets Across Space and Time (PAST). III. Morphology of the Planetary Radius Valley as a Function of Stellar Age and Metallicity in the Galactic Context Revealed by the LAMOST-Gaia-Kepler Sample
Authors: Di-Chang Chen, Ji-Wei Xie, Ji-Lin. Zhou, Jia-Yi Yang, Subo Dong, Zi Zhu, Zheng Zheng, Chao Liu, Weikai Zong, Ali Luo
Figure caption: The cumulative distributions of stellar mass M *, radius R *, CDPP 4.5 hr, [Fe/H], and [α/Fe] for the four bins with different relative probabilities between thick disk and thin disk TD/D (Section 3.1). In each panel, p denotes the p-value of the two-sample K-S test for the distributions of neighboring stars belonging to the last three bins compared to the first bins. Note that only stellar mass M *, radius R *, CDPP, and Kepler magnitude have been controlled here. We did not control [Fe/H] and [α/Fe] when exploring the dependence on TD/D here because the differences in stellar metallicity between thin- and thick-disk stars are essential and inevitable.
Paper: Planets Across Space and Time (PAST). III. Morphology of the Planetary Radius Valley as a Function of Stellar Age and Metallicity in the Galactic Context Revealed by the LAMOST-Gaia-Kepler Sample
Authors: Di-Chang Chen, Ji-Wei Xie, Ji-Lin. Zhou, Jia-Yi Yang, Subo Dong, Zi Zhu, Zheng Zheng, Chao Liu, Weikai Zong, Ali Luo
Figure caption: Similar to Figure A2, but here showing the cumulative distributions of stellar mass M *, radius R *, CDPP 4.5 hr, [Fe/H], and [α/Fe] for the four bins with different kinematic ages (Section 3.2). Note that here stellar mass M *, radius R *, CDPP, [Fe/H], [α/Fe], and Kepler magnitude have all been controlled in order to isolate the effect of age.
Paper: Planets Across Space and Time (PAST). III. Morphology of the Planetary Radius Valley as a Function of Stellar Age and Metallicity in the Galactic Context Revealed by the LAMOST-Gaia-Kepler Sample
Authors: Di-Chang Chen, Ji-Wei Xie, Ji-Lin. Zhou, Jia-Yi Yang, Subo Dong, Zi Zhu, Zheng Zheng, Chao Liu, Weikai Zong, Ali Luo
Figure caption: Similar to Figure A2, but here showing the cumulative distributions of stellar mass M *, radius R *, CDPP 4.5 hr, TD/D, and [Fe/H] for the four bins with different [α/Fe] (Section 3.4). Note that here stellar mass M *, radius R *, CDPP, TD/D, and [Fe/H] have all been controlled in order to isolate the effect of [α/Fe].
Paper: Planets Across Space and Time (PAST). III. Morphology of the Planetary Radius Valley as a Function of Stellar Age and Metallicity in the Galactic Context Revealed by the LAMOST-Gaia-Kepler Sample
Authors: Di-Chang Chen, Ji-Wei Xie, Ji-Lin. Zhou, Jia-Yi Yang, Subo Dong, Zi Zhu, Zheng Zheng, Chao Liu, Weikai Zong, Ali Luo
Figure caption: Similar to Figure A2, but here showing the cumulative distributions of stellar mass M *, radius R *, CDPP 4.5 hr, TD/D, and [α/Fe] for the four bins with different [Fe/H] (Section 3.3). Note that here stellar mass M *, radius R *, CDPP, TD/D, [α/Fe], and Kepler magnitude have all been controlled in order to isolate the effect of [Fe/H].
Paper: Planets Across Space and Time (PAST). III. Morphology of the Planetary Radius Valley as a Function of Stellar Age and Metallicity in the Galactic Context Revealed by the LAMOST-Gaia-Kepler Sample
Authors: Di-Chang Chen, Ji-Wei Xie, Ji-Lin. Zhou, Jia-Yi Yang, Subo Dong, Zi Zhu, Zheng Zheng, Chao Liu, Weikai Zong, Ali Luo
Figure caption: The cumulative distributions of Kepler magnitudes and effective temperature for the planet host stars in the entire Kepler sample (blue) and LAMOST-Gaia-Kepler sample (red).
Paper: Planets Across Space and Time (PAST). III. Morphology of the Planetary Radius Valley as a Function of Stellar Age and Metallicity in the Galactic Context Revealed by the LAMOST-Gaia-Kepler Sample
Authors: Di-Chang Chen, Ji-Wei Xie, Ji-Lin. Zhou, Jia-Yi Yang, Subo Dong, Zi Zhu, Zheng Zheng, Chao Liu, Weikai Zong, Ali Luo
Figure caption: Orbital periods vs. radii for the planets in the four bins of different TD/D after parameter controlling. In each panel, we plot their average detection efficiencies (10%, 50%, and 90%) for stars in each bin (red lines). For ease of comparison, we also plot the same mean detection efficiencies for all stars in the whole sample (black lines).
Paper: Planets Across Space and Time (PAST). III. Morphology of the Planetary Radius Valley as a Function of Stellar Age and Metallicity in the Galactic Context Revealed by the LAMOST-Gaia-Kepler Sample
Authors: Di-Chang Chen, Ji-Wei Xie, Ji-Lin. Zhou, Jia-Yi Yang, Subo Dong, Zi Zhu, Zheng Zheng, Chao Liu, Weikai Zong, Ali Luo
Figure caption: Similar to Figure B1, but for the four bins of different [α/Fe].
Paper: Planets Across Space and Time (PAST). III. Morphology of the Planetary Radius Valley as a Function of Stellar Age and Metallicity in the Galactic Context Revealed by the LAMOST-Gaia-Kepler Sample
Authors: Di-Chang Chen, Ji-Wei Xie, Ji-Lin. Zhou, Jia-Yi Yang, Subo Dong, Zi Zhu, Zheng Zheng, Chao Liu, Weikai Zong, Ali Luo
Figure caption: Similar to Figure B1, but the four bins of different [Fe/H].
Paper: Planets Across Space and Time (PAST). III. Morphology of the Planetary Radius Valley as a Function of Stellar Age and Metallicity in the Galactic Context Revealed by the LAMOST-Gaia-Kepler Sample
Authors: Di-Chang Chen, Ji-Wei Xie, Ji-Lin. Zhou, Jia-Yi Yang, Subo Dong, Zi Zhu, Zheng Zheng, Chao Liu, Weikai Zong, Ali Luo
Figure caption: Similar to Figure B1, but the four bins of different age.
Paper: Planets Across Space and Time (PAST). III. Morphology of the Planetary Radius Valley as a Function of Stellar Age and Metallicity in the Galactic Context Revealed by the LAMOST-Gaia-Kepler Sample
Authors: Di-Chang Chen, Ji-Wei Xie, Ji-Lin. Zhou, Jia-Yi Yang, Subo Dong, Zi Zhu, Zheng Zheng, Chao Liu, Weikai Zong, Ali Luo
Figure caption: The cumulative distributions of stellar mass M *, radius R *, age, and CDPP 4.5 hr for the four bins with different metallicity [Fe/H] of CKS VII after parameter control. In each panel, p denotes the p-value of the two-sample K-S test for the distributions of neighboring stars belonging to the last three bins compared to the first bins.
Paper: Planets Across Space and Time (PAST). III. Morphology of the Planetary Radius Valley as a Function of Stellar Age and Metallicity in the Galactic Context Revealed by the LAMOST-Gaia-Kepler Sample
Authors: Di-Chang Chen, Ji-Wei Xie, Ji-Lin. Zhou, Jia-Yi Yang, Subo Dong, Zi Zhu, Zheng Zheng, Chao Liu, Weikai Zong, Ali Luo
Figure caption: Similar to Figure C1, but after controlling parameters (i.e., stellar mass, radius, age, and CDPP) to let them have similar distributions to those shown in Figure C2.
Paper: Planets Across Space and Time (PAST). III. Morphology of the Planetary Radius Valley as a Function of Stellar Age and Metallicity in the Galactic Context Revealed by the LAMOST-Gaia-Kepler Sample
Authors: Di-Chang Chen, Ji-Wei Xie, Ji-Lin. Zhou, Jia-Yi Yang, Subo Dong, Zi Zhu, Zheng Zheng, Chao Liu, Weikai Zong, Ali Luo
Figure caption: Correlations between planetary and stellar properties for the CKS VII sample before parameter control. In each panel, ρ and p denote the Pearson correlation coefficient and p-value for each pair of variables, respectively.
Paper: Planets Across Space and Time (PAST). III. Morphology of the Planetary Radius Valley as a Function of Stellar Age and Metallicity in the Galactic Context Revealed by the LAMOST-Gaia-Kepler Sample
Authors: Di-Chang Chen, Ji-Wei Xie, Ji-Lin. Zhou, Jia-Yi Yang, Subo Dong, Zi Zhu, Zheng Zheng, Chao Liu, Weikai Zong, Ali Luo
Figure caption: The period–radius diagram for the planetary sample (Section 2.1). Areas of different colors represent planets of different radius: green for super-Earths (1–1.7 R ⊕), gray for valley planets (1.7–2.1 R ⊕), yellow for sub-Neptunes (2.1–3.5 R ⊕), and purple for Neptunes (3.5–6 R ⊕). Histograms of planetary radius (R  p ) and orbital period (P) are shown in the right panel and the top panel, respectively.
Paper: Planets Across Space and Time (PAST). III. Morphology of the Planetary Radius Valley as a Function of Stellar Age and Metallicity in the Galactic Context Revealed by the LAMOST-Gaia-Kepler Sample
Authors: Di-Chang Chen, Ji-Wei Xie, Ji-Lin. Zhou, Jia-Yi Yang, Subo Dong, Zi Zhu, Zheng Zheng, Chao Liu, Weikai Zong, Ali Luo
Figure caption: The [Fe/H]–[α/Fe] diagram color-coded by the relative probability between thick disk and thin disk TD/D for the stellar sample (Section 2.1).
Paper: Comparison of Composite and Star-forming Early-type Galaxies
Authors: Yu-Zhong Wu
Figure caption: Comparison of stellar-mass (left-hand panel) and sSFR (right-band panel) distributions for star-forming ETGs and composite ETGs. The blue dotted and red dashed lines show the distributions of star-forming and composite ETGS, respectively. The green solid and magenta dotted–dashed lines present the distributions of star-forming and composite ETGs with p > 0.8, respectively.
Paper: Comparison of Composite and Star-forming Early-type Galaxies
Authors: Yu-Zhong Wu
Figure caption: BPT diagnostic diagram. The black dashed curve shows the semi-empirical lower boundary for SFGs from Kauffmann et al. (2003a); the green solid curves represent the Kewley et al. (2001) theoretical upper limit for SFGs. The blue and red dots display star-forming ETGs and composite ETGs, respectively.
Paper: Comparison of Composite and Star-forming Early-type Galaxies
Authors: Yu-Zhong Wu
Figure caption: The diagram of stellar mass and corrected u − r color. The two green lines represent the position of the green valley, defined as the region between the blue cloud and the red sequence. The blue and red contours show the distributions of star-forming and composite ETGs, respectively.
Paper: Comparison of Composite and Star-forming Early-type Galaxies
Authors: Yu-Zhong Wu
Figure caption: The distributions of [N II]/Hα and EWHα  for star-forming and composite ETGs. The blue dotted and red dashed lines are the same as in Figure 2.
Paper: Comparison of Composite and Star-forming Early-type Galaxies
Authors: Yu-Zhong Wu
Figure caption: The distributions of W2 − W3 for star-forming ETGs and composite ETGs. The blue dotted and red dashed lines show their distributions for the two types of ETGs.
Paper: Thermal Phase Curves of XO-3b: An Eccentric Hot Jupiter at the Deuterium Burning Limit
Authors: Lisa Dang, Taylor J. Bell, Nicolas B. Cowan, Daniel Thorngren, Tiffany Kataria, Heather A. Knutson, Nikole K. Lewis, Keivan G. Stassun, Jonathan J. Fortney, Eric Agol, Gregory P. Laughlin, Adam Burrows, Karen A. Collins, Drake Deming, Diana Jovmir, Jonathan Langton, Sara Rastegar, Adam P. Showman
Figure caption: Raw photometry at 3.6 μm (left) and 4.5 μm (right). The top panel shows photometry using the preferred extraction scheme. The second and third panels show the x and y centroid coordinates, respectively. The fourth and fifth panels show the PSF width along the x and y axes, respectively. The colored data points represent those used in the analysis while the gray points are discarded from the analysis. The vertical dark colored line represents the time of periastron passage. The vertical dashed lines represent the AOR breaks when the pointing of the spacecraft is readjusted. Note that the data were binned by 64-frame data cube for better visualization.
Paper: Ages and Masses of Star Clusters in M33: a Multiwavelength Study
Authors: Caitlin Moeller, Daniela Calzetti
Figure caption: The B–V flux ratio vs. age using our measurements, without any extinction correction. Correcting the flux ratio for the effect of the Milky Way foreground extinction would make it bluer (move downward) by 0.036 dex, which is significantly smaller than the scatter in the data.
Paper: Ages and Masses of Star Clusters in M33: a Multiwavelength Study
Authors: Caitlin Moeller, Daniela Calzetti
Figure caption: NUV-I prior to extinction corrections plotted against our calculated ages. For the FUV–I color axis, blue is down and red is up. Correction for the Milky Way foreground extinction makes the color bluer by less than 0.1 dex.
Paper: Thermal Phase Curves of XO-3b: An Eccentric Hot Jupiter at the Deuterium Burning Limit
Authors: Lisa Dang, Taylor J. Bell, Nicolas B. Cowan, Daniel Thorngren, Tiffany Kataria, Heather A. Knutson, Nikole K. Lewis, Keivan G. Stassun, Jonathan J. Fortney, Eric Agol, Gregory P. Laughlin, Adam Burrows, Karen A. Collins, Drake Deming, Diana Jovmir, Jonathan Langton, Sara Rastegar, Adam P. Showman
Figure caption: PSF metrics for the 3.6 μm (left) and the 4.5 μm (right) observations. Each point represent the median of a data cube. The gray dots in the 3.6 μm plot represent data that were discarded from our analysis due to deviant PSF centroids or widths. The darker points represent the in-eclipse and in-transit points data.
Paper: Thermal Phase Curves of XO-3b: An Eccentric Hot Jupiter at the Deuterium Burning Limit
Authors: Lisa Dang, Taylor J. Bell, Nicolas B. Cowan, Daniel Thorngren, Tiffany Kataria, Heather A. Knutson, Nikole K. Lewis, Keivan G. Stassun, Jonathan J. Fortney, Eric Agol, Gregory P. Laughlin, Adam Burrows, Karen A. Collins, Drake Deming, Diana Jovmir, Jonathan Langton, Sara Rastegar, Adam P. Showman
Figure caption: The top and bottom panels show the rms scatter for various photometry schemes performed on 3.6 and 4.5 μm data, respectively. The schemes resulting in the smallest rms scatter are hard-edge circular apertures with a radius of 3.0 pixels for the 3.6 μm observations and a soft-edge aperture of 2.4 pixels for the 4.5 μm observations; these are denoted by a gray circle in each panel.
Paper: Ages and Masses of Star Clusters in M33: a Multiwavelength Study
Authors: Caitlin Moeller, Daniela Calzetti
Figure caption: NUV-I without extinction corrections plotted against the measured E(B–V) values. The overplotted model is set at the median age of the data set, 200 Myr.
Paper: Thermal Phase Curves of XO-3b: An Eccentric Hot Jupiter at the Deuterium Burning Limit
Authors: Lisa Dang, Taylor J. Bell, Nicolas B. Cowan, Daniel Thorngren, Tiffany Kataria, Heather A. Knutson, Nikole K. Lewis, Keivan G. Stassun, Jonathan J. Fortney, Eric Agol, Gregory P. Laughlin, Adam Burrows, Karen A. Collins, Drake Deming, Diana Jovmir, Jonathan Langton, Sara Rastegar, Adam P. Showman
Figure caption: Top-view of XO-3b’s orbit with parameters from Wong et al. (2014). The gray dots represent the planet’s position at 1 hour intervals and the planet revolves counterclockwise. The shaded area represents our line of sight (the Earth is off the bottom of the plot).
Paper: The Chemical Composition of Extreme-velocity Stars 
Authors: Henrique Reggiani, Alexander P. Ji, Kevin C. Schlaufman, Anna Frebel, Lina Necib, Tyler Nelson, Keith Hawkins, Jhon Yana Galarza
Figure caption: Abundances of the α-elements magnesium, silicon, and calcium, as well as titanium. We plot our HVSs as dark blue stars. We plot in yellow the abundances of metal-poor stars in the Milky Way outer halo from Cayrel et al. (2004) and Jacobson et al. (2015); in red we show abundances of inner halo stars from H. Reggiani et al. (2022, in preparation), Reggiani et al. (2017), and Nissen & Schuster (2010); we display the Bensby et al. (2010) bulge stars in orange; in light-blue we include stars from the dwarf spheroidal galaxies Carina, Sculptor, Fornax, and Sagittarius from Shetrone et al. (2003), Geisler et al. (2005), Monaco et al. (2005), and Letarte et al. (2010).
Paper: The Chemical Composition of Extreme-velocity Stars 
Authors: Henrique Reggiani, Alexander P. Ji, Kevin C. Schlaufman, Anna Frebel, Lina Necib, Tyler Nelson, Keith Hawkins, Jhon Yana Galarza
Figure caption: Abundances of the neutron-capture elements strontium, yttrium, barium, and europium. We plot our HVSs as dark blue stars. We plot in yellow the abundances of metal-poor stars in the Milky Way outer halo from Cayrel et al. (2004) and Jacobson et al. (2015); in red we show abundances of inner halo stars from H. Reggiani et al. (2022, in preparation), Reggiani et al. (2017), and Nissen & Schuster (2010); we display the Bensby et al. (2010) bulge stars in orange; in light-blue we include stars from the dwarf spheroidal galaxies Carina, Sculptor, Fornax, and Sagittarius from Shetrone et al. (2003), Geisler et al. (2005), Monaco et al. (2005), and Letarte et al. (2010).