adsabs/AstroCLIMB huggingface dataset:
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Posteriors and best-fit spectrum for amplitude fitting of WASP-107 b.
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Same as Figure 33 but for FeH.
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Same as Figure 33 but for e−.
Paper: Clump-scale Gas Infall in High-mass Star Formation: A Multitransition View with James Clerk Maxwell Telescope HCN (4–3) Mapping
Authors: Fengwei Xu, Ke Wang, Yuxin He, Jingwen Wu, Lei Zhu, Diego Mardones
Figure caption: Simulated grids of predicted optical depth (τ pred) based on the kinetic temperature (T kin) and the column density of HCN (﹩{N}_{\mathrm{HCN}}﹩), with three different volume densities of collisional partner H2 (﹩{n}_{{{\rm{H}}}_{2}}﹩). The white lines outline the contour levels of τ = 1 and 10. The 38 clumps are shown as filled circles, with blue, red, and gray colors representing blue profiles, red profiles, and nonasymmetric profiles, respecitvely. The five clumps with the highest τ pred are labeled. The color bars are shown in the lower right.
Paper: Clump-scale Gas Infall in High-mass Star Formation: A Multitransition View with James Clerk Maxwell Telescope HCN (4–3) Mapping
Authors: Fengwei Xu, Ke Wang, Yuxin He, Jingwen Wu, Lei Zhu, Diego Mardones
Figure caption: For the 11 infall candidates, the line grids are overlaid on M0 color maps. Green ellipses mark the footprints of HCN cores. The lines shown are averaged from the 2 × 2 pix2 box and smoothed to 0.4 km s−1. For the three core-rotation candidates, black dashed lines show the rotation axes, which are overlaid on M1 color maps. The JCMT beam and the scale bar of 0.2 pc are shown in the bottom left and right, respectively.
Paper: Clump-scale Gas Infall in High-mass Star Formation: A Multitransition View with James Clerk Maxwell Telescope HCN (4–3) Mapping
Authors: Fengwei Xu, Ke Wang, Yuxin He, Jingwen Wu, Lei Zhu, Diego Mardones
Figure caption: The averaged HCN (4–3) lines are indicated by the black solid line, while the best-fit Hill5 model are indicated by the red solid line, with five parameters shown in the upper-left corner. We highlight the velocity range used for Hill5 model fitting in orange color at the bottom. The red band indicates the systematic velocity v LSR. The blue band indicates the velocity span of the infall motion, that is, from v LSR − v infall to v LSR + v infall.
Paper: Clump-scale Gas Infall in High-mass Star Formation: A Multitransition View with James Clerk Maxwell Telescope HCN (4–3) Mapping
Authors: Fengwei Xu, Ke Wang, Yuxin He, Jingwen Wu, Lei Zhu, Diego Mardones
Figure caption: The low detection rate of blue profiles (BPs) in star-forming clumps guided by ATLASGAL and BGPS. In this, 3246 ATLASGAL clumps with 870 μm flux larger than 0.25 Jy are observed in HCO+/N2H+ (1–0) at a spectral resolution of 0.11 km s−1 by the Mopra MALT90 line survey; 732 clumps have a solid detection of S/N > 3, among which 231 clumps have BPs by the canonical criterion of δ V < −0.25. The detection rate of BPs is then 31.6% (He et al. 2015, 2016). Further, 6194 BGPS clumps without flux threshold are observed in HCO+/N2H+(3-2) at a spectral resolution of 1.1 km s−1 by the SMT line survey (Schlingman et al. 2011; Shirley et al. 2013); 1795 clumps have a solid detection of S/N > 3, among which 48 have BPs, giving a detection rate of 2.8% (Shirley et al. 2013).
Paper: Clump-scale Gas Infall in High-mass Star Formation: A Multitransition View with James Clerk Maxwell Telescope HCN (4–3) Mapping
Authors: Fengwei Xu, Ke Wang, Yuxin He, Jingwen Wu, Lei Zhu, Diego Mardones
Figure caption: The M0 maps of HCN (4–3) in 38 fields. The names are labeled in the top left of each panel. The green solid ellipses mark the HCN cores by SExtractor, while the green dashed circles outline the regions where the spectra are extracted in the nondetection fields. The JCMT beam and its physical scale in each map are shown in the bottom left.
Paper: Clump-scale Gas Infall in High-mass Star Formation: A Multitransition View with James Clerk Maxwell Telescope HCN (4–3) Mapping
Authors: Fengwei Xu, Ke Wang, Yuxin He, Jingwen Wu, Lei Zhu, Diego Mardones
Figure caption: The number distribution (histogram) and the fraction (line-connected scatter plot) of different line profiles change with peak column density bins ﹩\mathrm{log}N({{\rm{H}}}_{2})({\mathrm{cm}}^{-2})﹩ in a beam of 21″. The blue, red, and gray colors stand for blue profiles, red profiles, and nonasymmetric profiles (including single peaked and nondetection), respectively.
Paper: Clump-scale Gas Infall in High-mass Star Formation: A Multitransition View with James Clerk Maxwell Telescope HCN (4–3) Mapping
Authors: Fengwei Xu, Ke Wang, Yuxin He, Jingwen Wu, Lei Zhu, Diego Mardones
Figure caption: Grids (2 × 2 pix2) of HCN (4–3) line profiles overlaid on a continuum map (either ATLASGAL or SCUBA-2) for BG012.889, BG081.721, BG133.748, and BG133.949, respectively. The beam size of the HARP receiver at 350 GHz is shown in the bottom left. The scale bar of 0.2 pc is shown in the bottom right.
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Retrieved abundances of H2O, CH4, HCN, NH3, TiO, VO, FeH, and e− against planet equilibrium temperature. In some cases, only an upper bound on the presence of the molecule could be placed and, for these, the error bar extends to log10(VMR) = −12, the lower bound of our priors. The upper bound is shown by the dashed line. The filled regions bounded by dashed–dotted gray lines indicate the predicted abundances from GGchem chemical equilibrium models (assuming C/O = 0.54 and solar metallicity) across 1 × 102 to 1 × 105 Pa (1 × 10–3 to 1 bar). For the lower four plots, black data points indicate planets for which the retrieval model with these optical absorbers are preferred while gray points represent those for which the fit is preferable without them. In all cases, abundances are only plotted if the associated models provided a >3σ detection compared to a flat model. The thick colored line on each plot indicates the linear trend from the BHM while the thinner colors lines represent the traces from the fit that were within the 1σ errors of the best-fit model. Only the fit to the abundance of e− gave a Bayesian evidence which was greater than the null hypothesis.
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Top: the signal-to-noise ratio (S/N) on the expected spectral modulation due to 1 scale height of a H/He-dominated atmosphere against the significance of the atmospheric detection from this work. While there is a positive correlation, in some cases no atmosphere is detected despite very precise observations. Middle: scatter plot of planet radius against planet temperature, where the color of the points indicates the significance of the atmosphere detection and the size shows the S/N on 1 scale height of atmosphere. Nondetections when detections might be expected happen more often for cooler, smaller planets while large, hot planets generally have a better chance of an atmospheric detection, even at low S/Ns. Bottom: scatter plot of planet surface gravity against planet temperature where the color and size again represent the detection significance and S/N, respectively. No clear trend can be distinguished given the variance in the precision of the data will affect the significance of the detection.
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Comparison of the retrieved abundances of H2O and e−. Black data points indicate planets for which the retrieval model with these optical absorbers were preferred to >3σ compared to the retrieval without optical absorbers. Gray points represent those which are still best fit with optical absorbers present, but at a lower significance compared to the models without them. In all cases, abundances are only plotted if the associated models provided a >3σ detection compared to a flat model. The blue, red, and green filled regions indicate the abundances derived from GGchem at different metallicities at pressure of 1 × 102 to 1 × 105 Pa. The dotted lines indicate the upper bound used as a prior for each molecule. The lower bound in each case was log10(VMR) = −12.
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: HST/WFC3/G141 data sets utilized in this study. For each planet, the preferred model is denoted by the solid line while the dotted lines show other models which provide a poorer fit. Models including optical absorbers (red) are only shown if they provide a preferable fit to the data than those without (blue). In each case, the gray line denotes the flat model. The error bar in the top-right corner of each plot highlights the transit depth variation due to 1 scale height of atmosphere. Planets have been ordered in terms of their equilibrium temperature, from coolest (top left) to hottest (bottom right).
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: The retrieved carbon-to-oxygen ratio for planets within our sample against the retrieved metallicity (top) and planet’s semimajor axis (bottom). We note that the C/O ratio is poorly constrained in most cases due to the narrow wavelength coverage offered by HST WFC3 G141. In both plots, the dotted line highlights the prior range assuming a solar metallicity. The dashed line indicates the upper bound on the metallicity used for the planet around the star with the highest metallicity. The dashed–dotted line is the lower bound for the planet around the lowest-metallicity star.
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: Retrieved metallicity from our GGChem runs with the model from Thorngren et al. (2016) also shown. Top: BHM results when only using retrievals which give a >3σ atmospheric detection. Bottom: BHM results when using retrievals which give a >2σ atmospheric detection. In both cases, the BHM found a best-fit trend line which had a negative slope. However, in both cases, the null hypothesis (metallicity is not dependent upon mass) was preferred.
Paper: Exploring the Ability of Hubble Space Telescope WFC3 G141 to Uncover Trends in Populations of Exoplanet Atmospheres through a Homogeneous Transmission Survey of 70 Gaseous Planets
Authors: Billy Edwards, Quentin Changeat, Angelos Tsiaras, Kai Hou Yip, Ahmed F. Al-Refaie, Lara Anisman, Michelle F. Bieger, Amélie Gressier, Sho Shibata, Nour Skaf, Jeroen Bouwman, James Y-K. Cho, Masahiro Ikoma, Olivia Venot, Ingo Waldmann, Pierre-Olivier Lagage, Giovanna Tinetti
Figure caption: For the planets studied here, the distribution of their semimajor axis and mass (gold). The entire currently known transiting population with mass measurements is shown in gray.