adsabs/AstroCLIMB huggingface dataset:
Paper: Implication of the Velocity Dispersion Scalings on High-mass Star Formation in Molecular Clouds
Authors: An-Xu Luo, Hong-Li Liu, Sheng-Li Qin, Dong-ting Yang, Sirong Pan
Figure caption: Velocity-dispersion–radius relation for different density structures from GMCs to dense cores. The sources with α vir  >  2 are circled in black, while those with α vir  <  2 are not. The black solid line is the linear regression fit to the data points with α vir  >  2, for a best fit slope of 0.26 ± 0.04 and a Pearsons coefficient of ρ = 0.75. The black dashed line is the same but for the data points with α vir  <  2, for a best fit slope of 0.30 ± 0.03 and a Pearsons coefficient of ρ = 0.78. For comparison, the universal Larsons’s relation is represented by the dashed–dotted line.
Paper: Implication of the Velocity Dispersion Scalings on High-mass Star Formation in Molecular Clouds
Authors: An-Xu Luo, Hong-Li Liu, Sheng-Li Qin, Dong-ting Yang, Sirong Pan
Figure caption:                       ﹩{ \mathcal L }﹩– Σ relation for different density structures from GMCs to dense cores, where ﹩{ \mathcal L }﹩ is the σ/R0.5 ratio. The black dashed lines correspond to different predicted ﹩{ \mathcal L }﹩– Σ relation at the virial parameters of 0.5, 1, and 2. The dashed–dotted line indicates the predicted, magnetic version of the ﹩{ \mathcal L }﹩– Σ relation, ﹩{{ \mathcal L }}_{m}=1.08\ {{\rm{\Sigma }}}^{0.5}﹩, which corresponds to a simple model of magnetically supported clouds in an equilibrium state.
Paper: Implication of the Velocity Dispersion Scalings on High-mass Star Formation in Molecular Clouds
Authors: An-Xu Luo, Hong-Li Liu, Sheng-Li Qin, Dong-ting Yang, Sirong Pan
Figure caption: Violin plot of the α vir distribution for different density structures. The shape of each distribution shows the probability density of the α vir. The black horizontal bars from the top to bottom in violin plot represent the maximum, median, and minimum values, respectively. For different density structures, the median values of the α vir are 2.69, 0.90, and 0.74, respectively. The data for GMCs are sourced from Heyer et al. (2009). The data for clumps are from Ohashi et al. (2016), Traficante et al. (2018), and this work. The data for cores are from Peretto et al. (2006), Ohashi et al. (2016), Lu et al. (2018), and Li et al. (2023).
Paper: Implication of the Velocity Dispersion Scalings on High-mass Star Formation in Molecular Clouds
Authors: An-Xu Luo, Hong-Li Liu, Sheng-Li Qin, Dong-ting Yang, Sirong Pan
Figure caption: Violin plot of the α vir, velocity dispersion, and size distribution for the GMCs in two subsamples with different mass-surface density. The shape of each distribution shows the probability density of the α vir, velocity dispersion, and size, respectively. The black horizontal bars from the top to bottom in violin plot represent the maximum, median, and minimum values, respectively. The Σ1 on the horizontal axis represents the median of subsamples with low-mass-surface density, while Σ2 represents the median of subsamples with high-mass-surface density, which are 0.03 g cm−2 and 0.16 g cm−2, respectively.
Paper: Implication of the Velocity Dispersion Scalings on High-mass Star Formation in Molecular Clouds
Authors: An-Xu Luo, Hong-Li Liu, Sheng-Li Qin, Dong-ting Yang, Sirong Pan
Figure caption: An example of clump classification inferred from Spitzer images overlaid with 870 μm dust continuum emission. In each row from left to right, the images are ATLASGAL 870 μm dust continuum emission in gray-scale, Spitzer three-color image of 3.6, 4.5 and 8.0 μm, and Spitzer three-color image of 3.6, 8.0 and 24 μm. the yellow contours indicate the 870 μm dust continuum emission, starting from 0.3 Jy beam−1 with a step of 0.5 Jy beam−1. Rows (a)–(d) correspond to the examples of classified phases of clumps from the quiescent, protostellar, H II region, and PDR phase, respectively. In all images, the clump name is indicated at the top of each panel. The red star symbol identifies peak emission at 870 μm of the clump.
Paper: Implication of the Velocity Dispersion Scalings on High-mass Star Formation in Molecular Clouds
Authors: An-Xu Luo, Hong-Li Liu, Sheng-Li Qin, Dong-ting Yang, Sirong Pan
Figure caption: Velocity-dispersion distribution for different evolutionary phases of clumps, including the quiescent, protostellar, H II region, and PDR phases. The black vertical dashed line indicates the median ratio for each phase. The median value for each phase is 0.8 km s−1, 1.1 km s−1, 1.4 km s−1, 1.3 km s−1, respectively. The velocity dispersion increases from the quiescent to H II region phase, but then decreases toward the PDR phase.
Paper: Implication of the Velocity Dispersion Scalings on High-mass Star Formation in Molecular Clouds
Authors: An-Xu Luo, Hong-Li Liu, Sheng-Li Qin, Dong-ting Yang, Sirong Pan
Figure caption: Velocity-dispersion–radius relation for 221 massive clumps.
Paper: Dynamical Structures under Nonrestricted Hierarchical Planetary Systems with Different Mass Ratios
Authors: Xiumin Huang, Hanlun Lei
Figure caption: The FLI maps under different mass ratios with the initial angles at g 1 = 0 and g 2 = π. The chaotic orbits are marked by yellow dots, and the regular orbits are marked by blue dots. The white area stands for the forbidden region.
Paper: Dynamical Structures under Nonrestricted Hierarchical Planetary Systems with Different Mass Ratios
Authors: Xiumin Huang, Hanlun Lei
Figure caption: The FLI maps under different mass ratios with the initial angles at g 1 = 0 and g 2 = 0. The chaotic orbits are marked by yellow dots, and the regular orbits are marked by blue dots. The white area stands for the forbidden region.
Paper: Ground- and Space-based Dust Observations of VV 191 Overlapping Galaxy Pair
Authors: Clayton Robertson, Benne W. Holwerda, Jason Young, William C. Keel, Jessica M. Berkheimer, Kyle Cook, Christopher J. Conselice, Brenda L. Frye, Norman A. Grogin, Anton M. Koekemoer, Camella-Rosa Nasr, Divya Patel, Wade Roemer, Dominic Smith, Rogier A. Windhorst
Figure caption: Top left: A  V,stars, computed from Keel et al. (2023), plotted against A  V,H II , calculated from Equation (7) using the common Milky Way reddening slope R  V  = 3.1 (Cardelli et al. 1989). The plot is fitted to a linear regression shown by the blue line. The dotted black line represents a 1:1 ratio of attenuations, i.e., A  V,stars = A  V,H II . Top right: Linear regression fits for individual A  V,stars vs. A  V,H II  for each R  V  value given in Figures 11 and 12. Bottom left: Both attenuations, A  V,stars and A  V,H II  plotted analogous to Kreckel et al. (2013) Figure 4. We find that the physical scales from Kreckel et al. (2013) are closest to our own, giving us a direct comparison of our data to other works. Like Kreckel et al. (2013), we use R  V  = 3.1. Bottom right: The same data as in the bottom left figure, but plotted against the radius from the center, normalized by the Petrosian radius.
Paper: Ground- and Space-based Dust Observations of VV 191 Overlapping Galaxy Pair
Authors: Clayton Robertson, Benne W. Holwerda, Jason Young, William C. Keel, Jessica M. Berkheimer, Kyle Cook, Christopher J. Conselice, Brenda L. Frye, Norman A. Grogin, Anton M. Koekemoer, Camella-Rosa Nasr, Divya Patel, Wade Roemer, Dominic Smith, Rogier A. Windhorst
Figure caption: Attenuation, ﹩{A}_{V}=-1.086\times \mathrm{ln}(\mathrm{Transmission})﹩ derived from the HST F606W dust map plotted against the Balmer decrement values from GCMS IFU observations. Attenuation relations are plotted using the R  V  values derived from Keel et al. (2023). Due to matching the number of pixels, and therefore arrays in configuring the data, the “pixelated” version of the transmission map is needed. Zones 1, 2, and 3 are arm regions with organized dust lanes, while zones 4 and 5 are interarm regions with minimal coverage by distinct lanes. Detailed images of the different zones are shown in great detail in Keel et al. (2013), their Figure 8.
Paper: Ground- and Space-based Dust Observations of VV 191 Overlapping Galaxy Pair
Authors: Clayton Robertson, Benne W. Holwerda, Jason Young, William C. Keel, Jessica M. Berkheimer, Kyle Cook, Christopher J. Conselice, Brenda L. Frye, Norman A. Grogin, Anton M. Koekemoer, Camella-Rosa Nasr, Divya Patel, Wade Roemer, Dominic Smith, Rogier A. Windhorst
Figure caption: The attenuation (Equation (3)), derived from the HST F606W dust map, plotted against the Balmer decrement values from GCMS. The different reddening slopes, R  V , are from the literature. For each slope defined besides Charlot & Fall (2000; relation defined in Equation (11)), the attenuation curves are calculated using Equations (7) and (8).
Paper: Ground- and Space-based Dust Observations of VV 191 Overlapping Galaxy Pair
Authors: Clayton Robertson, Benne W. Holwerda, Jason Young, William C. Keel, Jessica M. Berkheimer, Kyle Cook, Christopher J. Conselice, Brenda L. Frye, Norman A. Grogin, Anton M. Koekemoer, Camella-Rosa Nasr, Divya Patel, Wade Roemer, Dominic Smith, Rogier A. Windhorst
Figure caption: Data gathered from the hand-picked region shown in Figure 7. The Balmer line fluxes (top) and the Balmer decrement values (bottom) are plotted against the radius from the center spaxel of VV 191b divided by the Petrosian radius (R P = 12 kpc).
Paper: Ground- and Space-based Dust Observations of VV 191 Overlapping Galaxy Pair
Authors: Clayton Robertson, Benne W. Holwerda, Jason Young, William C. Keel, Jessica M. Berkheimer, Kyle Cook, Christopher J. Conselice, Brenda L. Frye, Norman A. Grogin, Anton M. Koekemoer, Camella-Rosa Nasr, Divya Patel, Wade Roemer, Dominic Smith, Rogier A. Windhorst
Figure caption: Linear fits (red lines) for determining the dust scale length. See Section 6.3. Values for h labeled on each plot are determined from Equation (10).
Paper: TRANSLIENT: Detecting Transients Resulting from Point-source Motion or Astrometric Errors
Authors: Ofer Springer, Eran O. Ofek, Barak Zackay, Ruslan Konno, Amir Sharon, Guy Nir, Adam Rubin, Asaf Haddad, Jonathan Friedman, Leora Schein-Lubomirsky, Iakov Aizenberg, Alexander Krassilchtchikov, Avishay Gal-Yam
Figure caption: Resulting translient statistic (Z 2;  left panel) and proper statistic (S 2;  right panel) images computed for the image pair shown in Figure 2. The red crosses mark the location of  x   c  ≡ ( p  +  q )/2, the center between the positions of the point sources in the reference and new images. In the squared translient statistic image one can see a single peak approximately centered at  x   c , whereas in the squared proper statistic image two peaks on opposite sides of  x   c  (diagonally) can be observed. This is the typical qualitative appearance of the two detector images when the data are generated by a point source undergoing pure translation (without any flux change). S 2 has units of ﹩{\left({\rm{S}}/{\rm{N}}\right)}^{2}﹩, and since σ  n  = σ  r , then the S/N in the N and R images is about ﹩\sqrt{2}﹩ times higher compared to the value in the S image.
Paper: TRANSLIENT: Detecting Transients Resulting from Point-source Motion or Astrometric Errors
Authors: Ofer Springer, Eran O. Ofek, Barak Zackay, Ruslan Konno, Amir Sharon, Guy Nir, Adam Rubin, Asaf Haddad, Jonathan Friedman, Leora Schein-Lubomirsky, Iakov Aizenberg, Alexander Krassilchtchikov, Avishay Gal-Yam
Figure caption: Example of a pair of reference and new images generated in simulation 1 (see Table 2). The red and black crosses mark the positions of the original point sources in the reference and new images, respectively. It can be seen that the translation is a 1 pixel translation (diagonally), which is considerably smaller than the width of the PSFs and that the Gaussian PSF profile of the new image differs from that of the reference image by a 90◦ rotation.
Paper: TRANSLIENT: Detecting Transients Resulting from Point-source Motion or Astrometric Errors
Authors: Ofer Springer, Eran O. Ofek, Barak Zackay, Ruslan Konno, Amir Sharon, Guy Nir, Adam Rubin, Asaf Haddad, Jonathan Friedman, Leora Schein-Lubomirsky, Iakov Aizenberg, Alexander Krassilchtchikov, Avishay Gal-Yam
Figure caption: Resulting translient statistic (Z 2;  left panel) and proper statistic (S 2;  right panel) images computed for zero-mean noise-only images (no moving point source). These patterns (arising from the action of the translient statistic and proper statistic on the observational noise) are responsible for false-positive detection events (at a certain detection threshold), i.e., cases of an event being classified as a detection of a translating point source when there was none. The highest peak, on the left panel, (Z 2 ≅ 11) corresponds to a false-alarm probability of 0.004 pixel–1 (i.e., a χ 2 distribution with 2 degrees of freedom) and close to unity for 642 trials.
Paper: TRANSLIENT: Detecting Transients Resulting from Point-source Motion or Astrometric Errors
Authors: Ofer Springer, Eran O. Ofek, Barak Zackay, Ruslan Konno, Amir Sharon, Guy Nir, Adam Rubin, Asaf Haddad, Jonathan Friedman, Leora Schein-Lubomirsky, Iakov Aizenberg, Alexander Krassilchtchikov, Avishay Gal-Yam
Figure caption: The ratio of the variance added due to an astrometric error Δx to that of the background, V ast/V(B), as a function of the source flux F and Δx. The upper x-axis shows the corresponding S/N for detection of the source (Ofek & Ben-Ami 2020), while the vertical dashed line shows the position where the variance of the source flux in the central pixel is equal to the variance of the background (i.e., to the left of this line we are in the background-noise-dominated regime).
Paper: The Strength and Variability of the Helium 10830 Å Triplet in Young Stars, with Implications for Exosphere Detection
Authors: Daniel M. Krolikowski, Adam L. Kraus, Benjamin M. Tofflemire, Caroline V. Morley, Andrew W. Mann, Andrew Vanderburg
Figure caption: EW[He] (top panel) and the Ca I 10842 Å line (bottom panel) as a function of effective temperature. Our sample is plotted as large colored circles and squares, and values are taken as the median of the time-series measurements. The uncertainties are often smaller than the points. In the top panel, the black x and red + symbols show literature He-10830 triplet EWs for field inactive (Zarro & Zirin 1986) and active (Sanz-Forcada & Dupree 2008) dwarfs, respectively. Our young stars have EW[He] greater than that of the inactive dwarfs, confirming that active stars feature enhanced He-10830 triplet absorption. The dashed line and gray shaded region show a linear fit and 3σ range for the EW–T eff relation. The EW[He] outliers (V1298 Tau and HD 283869) are excluded from the helium-T eff fit. The chromospheric He-10830 triplet has no T eff dependence, unlike the photospheric Ca I 10842 Å line, highlighting the difference in line formation. The different combinations of marker shape and color for our sample correspond to particular stars as designated in Table 1. This plotting scheme is also used in Figures 7, 8, 9, and 11.
Paper: The Strength and Variability of the Helium 10830 Å Triplet in Young Stars, with Implications for Exosphere Detection
Authors: Daniel M. Krolikowski, Adam L. Kraus, Benjamin M. Tofflemire, Caroline V. Morley, Andrew W. Mann, Andrew Vanderburg
Figure caption: The spectral region around the He-10830 triplet for the A2 star HR 5162. We show an A-star to highlight the emission line oversubtraction, as it is devoid of stellar absorption lines. The cyan spectrum is the science fiber flux prior to sky subtraction, which shows the sky emission lines, and the pink spectrum is the sky-subtracted spectrum following naive subtraction. For the strongest sky line, the oversubtraction is roughly 10% of the nearby continuum, which is significantly larger than the measurement error. The red spectrum shows the sky-subtracted spectrum using the scale factor β determined from the sky emission line at 10289.5 Å. The scaling removes the oversubtraction, and the resultant spectrum agrees with the nearby continuum within errors. Both subtraction methods are adequate and agree for the nearby weak emission doublet.
Paper: The Strength and Variability of the Helium 10830 Å Triplet in Young Stars, with Implications for Exosphere Detection
Authors: Daniel M. Krolikowski, Adam L. Kraus, Benjamin M. Tofflemire, Caroline V. Morley, Andrew W. Mann, Andrew Vanderburg
Figure caption: An example result for the spectral fitting of the He-10830 triplet region on an observation of K2-136. The brown spectrum is the telluric-corrected data, the red line is the best-fit spectral model, and the teal line is the continuum polynomial. The telluric absorption model has been removed from the data and spectral model to highlight the stellar lines. The bottom panel shows the residuals from subtracting the model from the data. The standard deviation of the residuals is 0.8 e−/s, which corresponds to a percent error on the flux of 1.4%. This is slightly larger than the typical measurement error of 0.5 e−/s (0.9%). The continuum level and stellar line profiles are well-matched by the model.
Paper: The Strength and Variability of the Helium 10830 Å Triplet in Young Stars, with Implications for Exosphere Detection
Authors: Daniel M. Krolikowski, Adam L. Kraus, Benjamin M. Tofflemire, Caroline V. Morley, Andrew W. Mann, Andrew Vanderburg
Figure caption: Telluric absorption model fitting for the A-star HR 3711. The black spectrum shows the sky-subtracted, continuum-normalized data. The red spectrum is the best-fit telluric model, and the pink spectrum is the telluric-corrected spectrum. Left Panel:  The region in spectral order 20 used to find the best-fit model. There are slight residuals, likely due to continuum division or theoretical model imperfections. Right panel:  The He-10830 triplet spectral region. The two strong water lines are well corrected. The resulting residuals across the range shown is 0.4%, which is very close to the typical measurement uncertainty of 0.3%.
Paper: The Strength and Variability of the Helium 10830 Å Triplet in Young Stars, with Implications for Exosphere Detection
Authors: Daniel M. Krolikowski, Adam L. Kraus, Benjamin M. Tofflemire, Caroline V. Morley, Andrew W. Mann, Andrew Vanderburg
Figure caption: Comparison of the amplitudes for the strong sky emission line near the He-10830 triplet (λ = 10834.3 Å) and the calibration sky emission line (λ = 10289.5 Å) used to determine the sky subtraction scale factor β. The amplitudes of the emission lines are well correlated, and their relationship is linear over an order of magnitude in amplitude.
Paper: The Strength and Variability of the Helium 10830 Å Triplet in Young Stars, with Implications for Exosphere Detection
Authors: Daniel M. Krolikowski, Adam L. Kraus, Benjamin M. Tofflemire, Caroline V. Morley, Andrew W. Mann, Andrew Vanderburg
Figure caption: The measurement error of each spectral line for all targets as a function of the median spectrum signal-to-noise ratio in the He-10830 triplet order. The three-pronged smaller markers are measurements for K2-100 and V1298 Tau, which feature larger error than the rest, due to their rapid rotation. The inverse relationship expected is shown, and the uncertainty plateaus at ≲5 mÅ for the He-10830 triplet above S/N ∼ 300.
Paper: Dynamical Architectures of S-type Transiting Planets in Binaries. I. Target Selection Using Hipparcos and Gaia Proper Motion Anomalies 
Authors: Jingwen Zhang, 婧雯 张, Lauren M. Weiss, Daniel Huber, Eric L. N. Jensen, Timothy D. Brandt, Karen Collins, Dennis M. Conti, Howard Isaacson, Pablo Lewin, Giuseppe Marino, Bob Massey, Felipe Murgas, Enric Palle, Don J. Radford, Howard M. Relles, Gregor Srdoc, Chris Stockdale, Thiam-Guan Tan, Gavin Wang
Figure caption: Panel (a): planet orbital period versus stellar companion separations of TOIs (green, Ziegler et al. 2020; Howell et al. 2021; Lester et al. 2021; Ziegler et al. 2021) and KOIs (purple, Kraus et al. 2016) in binary systems. We only include CPs or KPs. Panel (b): marginalized distribution of planet orbital periods of TOIs in binaries (green) and singles (gray). Panel (c): same as panel (b) but for KOIs in binary (purple) and single (gray) systems. Panel (d): marginalized distribution of stellar companion separations of TOIs (green) and KOIs (purple) in binaries.
Paper: Dynamical Architectures of S-type Transiting Planets in Binaries. I. Target Selection Using Hipparcos and Gaia Proper Motion Anomalies 
Authors: Jingwen Zhang, 婧雯 张, Lauren M. Weiss, Daniel Huber, Eric L. N. Jensen, Timothy D. Brandt, Karen Collins, Dennis M. Conti, Howard Isaacson, Pablo Lewin, Giuseppe Marino, Bob Massey, Felipe Murgas, Enric Palle, Don J. Radford, Howard M. Relles, Gregor Srdoc, Chris Stockdale, Thiam-Guan Tan, Gavin Wang
Figure caption: Panel (a): planet orbital period vs. differential velocities at Gaia epoch of TOIs with significant proper motion anomalies (color coded by their Gaia DR3 RUWE) and TOIs with marginal proper motion anomalies (gray). We exclude TOIs with FP/FA dispositions. High-S/N TOIs with RUWE ≥ 1.4 are in red, whereas those with RUWE < 1.4 are in blue. Panel (b): marginalized distribution of planet orbital periods of high (orange) and low (gray) S/N TOIs overlapped with the cumulative distribution function. We exclude TOIs with FP/FA dispositions.
Paper: Dynamical Architectures of S-type Transiting Planets in Binaries. I. Target Selection Using Hipparcos and Gaia Proper Motion Anomalies 
Authors: Jingwen Zhang, 婧雯 张, Lauren M. Weiss, Daniel Huber, Eric L. N. Jensen, Timothy D. Brandt, Karen Collins, Dennis M. Conti, Howard Isaacson, Pablo Lewin, Giuseppe Marino, Bob Massey, Felipe Murgas, Enric Palle, Don J. Radford, Howard M. Relles, Gregor Srdoc, Chris Stockdale, Thiam-Guan Tan, Gavin Wang
Figure caption: Orbit characterization of the LTT 1445 BC mass center around A using RVs, relative astrometry, and absolute astrometry from Hipparcos and Gaia. (a): relative astrometry orbits of LTT 1445 BC pair around A. The blue-filled circles are two observed relative astrometry used in our analysis. (c): Observed and fitted RVs of LTT 1445 from HARPS, HIRES, ESPRESSO, MAROON-X, and PFS. (d), (e): observed and fitted Hipparcos and Gaia proper motion of LTT 1445 A in R.A. and decl. In all of the above panels, the thicker black lines represent the best-fit orbit in the MCMC chain while the other 50 lines represent random draws from the chain; (b): relative astrometry orbits of LTT 1445 C around B from Winters et al. (2019).
Paper: Dynamical Architectures of S-type Transiting Planets in Binaries. I. Target Selection Using Hipparcos and Gaia Proper Motion Anomalies 
Authors: Jingwen Zhang, 婧雯 张, Lauren M. Weiss, Daniel Huber, Eric L. N. Jensen, Timothy D. Brandt, Karen Collins, Dennis M. Conti, Howard Isaacson, Pablo Lewin, Giuseppe Marino, Bob Massey, Felipe Murgas, Enric Palle, Don J. Radford, Howard M. Relles, Gregor Srdoc, Chris Stockdale, Thiam-Guan Tan, Gavin Wang
Figure caption: Right panel: the fraction of CPs, planet candidates, and several FPs of TOIs in our high-S/N sample. Left panel: the fraction of the same categories but for low-S/N TOIs. The two samples are both limited to 300 pc. We only present TOIs in this figure because the majority of KOI/K2 targets in our sample are EBs.
Paper: Dynamical Architectures of S-type Transiting Planets in Binaries. I. Target Selection Using Hipparcos and Gaia Proper Motion Anomalies 
Authors: Jingwen Zhang, 婧雯 张, Lauren M. Weiss, Daniel Huber, Eric L. N. Jensen, Timothy D. Brandt, Karen Collins, Dennis M. Conti, Howard Isaacson, Pablo Lewin, Giuseppe Marino, Bob Massey, Felipe Murgas, Enric Palle, Don J. Radford, Howard M. Relles, Gregor Srdoc, Chris Stockdale, Thiam-Guan Tan, Gavin Wang
Figure caption: Joint posterior distributions for selected orbital parameters of LTT 1445 BC. These are the host star’s mass (M pri), the companion mass (M sec), the semimajor axis a, the orbital eccentricity e, and the orbital inclination i. The values and histogram distributions of the posteriors of selected parameters are shown, along with 1σ uncertainties.