adsabs/AstroCLIMB huggingface dataset:
Paper: A Candidate High-velocity Exoplanet System in the Galactic Bulge
Authors: Sean K. Terry, Jean-Philippe Beaulieu, David P. Bennett, Aparna Bhattacharya, Jon Hulberg, Macy J. Huston, Naoki Koshimoto, Joshua W. Blackman, Ian A. Bond, Andrew A. Cole, Jessica R. Lu, Clément Ranc, Natalia E. Rektsini, Aikaterini Vandorou
Figure caption: Posterior probability distributions for the planetary companion mass, host mass, projected separation, and the distance to the lens system are shown with only light-curve constraints in blue (e.g., the D. P. Bennett et al. 2014 results) and with the additional constraints from our Keck follow-up observations in red. The central 68.3% of the distributions is shaded in darker colors (dark red and dark blue) and the remaining central 95.4% of the distributions is shaded in lighter colors. The vertical black lines mark the median of the probability distribution for the respective parameters.
Paper: A Candidate High-velocity Exoplanet System in the Galactic Bulge
Authors: Sean K. Terry, Jean-Philippe Beaulieu, David P. Bennett, Aparna Bhattacharya, Jon Hulberg, Macy J. Huston, Naoki Koshimoto, Joshua W. Blackman, Ian A. Bond, Andrew A. Cole, Jessica R. Lu, Clément Ranc, Natalia E. Rektsini, Aikaterini Vandorou
Figure caption: The mass–distance relation for MB11262L with constraints from the lens flux measurement in Keck K band (red). Dashed lines show the 1σ error bars derived from the flux measurement uncertainty and intrinsic error in the empirical mass–luminosity relation of X. Delfosse et al. (2000). The solid teal region shows the mass–distance relation from the angular Einstein radius measurement (θE), where the uncertainty in the source distance (Table 4) is the largest contributor to the uncertainty in the lens distance.
Paper: A Candidate High-velocity Exoplanet System in the Galactic Bulge
Authors: Sean K. Terry, Jean-Philippe Beaulieu, David P. Bennett, Aparna Bhattacharya, Jon Hulberg, Macy J. Huston, Naoki Koshimoto, Joshua W. Blackman, Ian A. Bond, Andrew A. Cole, Jessica R. Lu, Clément Ranc, Natalia E. Rektsini, Aikaterini Vandorou
Figure caption: Proper motions of all stars detected in both Keck epochs (gray points), given in Galactic coordinates. The yellow star indicates the position of the MB11262 source and the blue star indicates the position of the MB11262 high-velocity lens. The orange points show the crossmatched Gaia–Keck reference stars used for the transformation described in Section 4.1. The majority of the Gaia objects are likely foreground disk stars, owing to their larger μl values compared to the mean motion of galactic bulge stars centered around μl ~ 0 mas yr–1.
Paper: A Candidate High-velocity Exoplanet System in the Galactic Bulge
Authors: Sean K. Terry, Jean-Philippe Beaulieu, David P. Bennett, Aparna Bhattacharya, Jon Hulberg, Macy J. Huston, Naoki Koshimoto, Joshua W. Blackman, Ian A. Bond, Andrew A. Cole, Jessica R. Lu, Clément Ranc, Natalia E. Rektsini, Aikaterini Vandorou
Figure caption: Best-fit planetary light-curve model (solid black curve) for MB11262 with constraints from the high-resolution follow-up data as described in Section 3. This 2L1S model is given by the best-fit values listed in column 2 of Table 3. A 1L1S model is shown as a dashed gray curve.
Paper: A Tentative Detection of a Point Source in the Disk Gap of HD 100546 with VLT/SPHERE-IRDIS Sparse Aperture Masking Interferometry 
Authors: Dori Blakely, Doug Johnstone, Tomas Stolker, Myriam Benisty, Jens Kammerer, Brodie J. Norfolk, William Thompson, Jean-Philippe Berger
Figure caption: Reduced chi-squared (﹩{\chi }_{r}^{2}﹩) maps, calculated by fitting a point-source (binary) model to the residuals of the PG model fit, at each location (with a step size of 1 mas) within a radius of 125 mas. The significance of the 2018 detection is a >8σ result and the 2021 detection is a 5σ result, using the method by A. Gallenne et al. (2015). The 3σ credible interval contours on the location of the point source at each epoch are denoted by the teal (2018; left) and maroon (2021; right) contours. The 90% and 50% contours of the disk from the single PG fit are denoted by the black lines.
Paper: A Tentative Detection of a Point Source in the Disk Gap of HD 100546 with VLT/SPHERE-IRDIS Sparse Aperture Masking Interferometry 
Authors: Dori Blakely, Doug Johnstone, Tomas Stolker, Myriam Benisty, Jens Kammerer, Brodie J. Norfolk, William Thompson, Jean-Philippe Berger
Figure caption: The white contours show the median model disk component of the PG+PS model plotted on top of a Ks-band total intensity image of HD 100546 from B. B. Ren et al. (2023; left) and ALMA band 6 data of HD 100546 from B. J. Norfolk et al. (2022; right). The images are shown on a linear scale. In both panels, the location of the central star is denoted by the white star and the 3 σ credible interval on the point-source positions from the joint fit to all datasets with the PG+PS model are shown by the teal (2018) and maroon (2021) contours. The beam size of the ALMA image is shown in the bottom left corner of the right panel. 1000 randomly drawn orbits from the orbital fit posteriors are plotted on top of both images. Note that in the right panel the inner disk in the ALMA image is almost entirely occulted by the plotted orbits.
Paper: A Tentative Detection of a Point Source in the Disk Gap of HD 100546 with VLT/SPHERE-IRDIS Sparse Aperture Masking Interferometry 
Authors: Dori Blakely, Doug Johnstone, Tomas Stolker, Myriam Benisty, Jens Kammerer, Brodie J. Norfolk, William Thompson, Jean-Philippe Berger
Figure caption: Median geometrical models from the PG (left), PG+PS (middle), and 2PG (right) joint fits to the closure phase data, calculated using the median parameters displayed in Table 2. The top row shows the 2018 results and the bottom row shows the 2021 results. For the PG+PS model, the 1 and 3σ credible intervals on the companion position are shown by the teal (2018) and maroon (2021) contours. The semitransparent contours denote the credible intervals of the other epoch, to illustrate the significance of the motion between the two epochs. The Bayesian evidence (Log﹩{ \mathcal Z }﹩), calculated with nested sampling, are shown for each model at the top of each row. With a Log﹩{ \mathcal Z }﹩ = −2592.9, 378.4 greater than the PG model, and 285.9 greater than the 2PG model, the PG+PS is resoundingly the best representation of the data of the explored models, supporting the interpretation that there is asymmetric emission originating in the disk gap.
Paper: A Tentative Detection of a Point Source in the Disk Gap of HD 100546 with VLT/SPHERE-IRDIS Sparse Aperture Masking Interferometry 
Authors: Dori Blakely, Doug Johnstone, Tomas Stolker, Myriam Benisty, Jens Kammerer, Brodie J. Norfolk, William Thompson, Jean-Philippe Berger
Figure caption: Closure phase data (using the same colors as in Figure 1) and model (black), for the PG (left), PG+PS (middle), and 2PG (right) models. The bottom panels in each plot show the noise normalized residuals, with the binned residuals shown on the right and the red curve denoting a unit normal distribution.
Paper: A Tentative Detection of a Point Source in the Disk Gap of HD 100546 with VLT/SPHERE-IRDIS Sparse Aperture Masking Interferometry 
Authors: Dori Blakely, Doug Johnstone, Tomas Stolker, Myriam Benisty, Jens Kammerer, Brodie J. Norfolk, William Thompson, Jean-Philippe Berger
Figure caption: Calibrated closure phases for HD 100546, extracted from the 2018 2.1 μm (teal), 2.3 μm data (blue), 2021 1.6 μm (maroon), and 1.7 μm data (purple).
Paper: The Effects of the Carbon-to-oxygen Ratio on the Condensate Compositions around Solar-like Stars
Authors: Cody J. Shakespeare, Min Li, Shichun Huang, Zhaohuan Zhu, Jason H. Steffen
Figure caption: The solid surface density profiles of five select elements in three different simulations: (left) solar, (middle) C/O = 0.8, and (right) C/O = 1. The solar C/O is 0.501, and the solar N/O is 0.138. The surface density profile does not change significantly between the C/O = 1 simulation, the C/O = 1 w/Oc simulation, and the N/O = 1.5 simulation, which has an indirect C/O of 1.10. See Figure 15 for the same graphic but with different methods of varying the initial C/O.
Paper: The Effects of the Carbon-to-oxygen Ratio on the Condensate Compositions around Solar-like Stars
Authors: Cody J. Shakespeare, Min Li, Shichun Huang, Zhaohuan Zhu, Jason H. Steffen
Figure caption: The final C/O, denoted by color, at different distances from the central star and initial C/Os. The y-axis is a linear scale of the radii in astronomical units. The z-axis, or colored contours, is a log scale of the final local C/O for the given simulation’s initial conditions and at the indicated distance from the central star. Black lines help emphasize each change of 106, and the contour line for C/O = 1 is represented with a dotted line. The black dot located at C/O = 0.501 and R = 1 au represents the location and initial C/O of Earth’s position in the solar protoplanetary disk. Note that the resolution of these two contour plots is not uniform between the x- and y-axis. The resolution is the poorest at the far left, far right, and top. Lastly, note that the resolution of the x-axis is not uniform; see Table 1 for the exact initial C/Os we explore. (Left) The x-axis is a log scale of the initial C/O spanning all ratios examined. (Right) The x-axis is a linear scale and spans C/Os of 0–2.1. The z-axis here is limited from 10−3 to 103 to better display small changes in the final C/O. The dashed–dotted lines in the right plot represent the 10−3 and 103 cutoffs in the z-axis. See Figure 14 for the same graphic but with the C/O varied while oxygen is held constant (i.e. w/Oc).
Paper: The Effects of the Carbon-to-oxygen Ratio on the Condensate Compositions around Solar-like Stars
Authors: Cody J. Shakespeare, Min Li, Shichun Huang, Zhaohuan Zhu, Jason H. Steffen
Figure caption: The total carbon (green) and oxygen (red) fractions summed over all radii for simulations with a given initial C/O. The vertical solid line indicates the solar C/O simulation. Purely dotted lines correspond to ﹩\frac{f\rm{C}\,}{f\,\rm{O}}=0.01﹩ and 100. Dashed and dotted lines correspond to ﹩\frac{f\rm{C}\,}{f\,\rm{O}}=0.1﹩ and 10. The purely dashed line corresponds to ﹩\frac{f\rm{C}\,}{f\,\rm{O}}=1﹩. (Left) In order from left to right: ﹩\frac{f\rm{C}\,}{f\,\rm{O}}=0.01﹩, ﹩\frac{f\rm{C}\,}{f\,\rm{O}}=0.1﹩, ﹩\frac{f\rm{C}\,}{f\,\rm{O}}=1﹩, ﹩\frac{f\rm{C}\,}{f\,\rm{O}}=10﹩, ﹩\frac{f\rm{C}\,}{f\,\rm{O}}=100﹩ are located at C/O values of 0.762, 0.828, 1.005, 2.457, and 37.633, respectively. (Right) Here the amount of oxygen is held constant at the solar value while the C/O varies (i.e., C/O w/Oc). In order from left to right: ﹩\frac{f\rm{C}\,}{f\,\rm{O}}=0.01﹩, ﹩\frac{f\rm{C}\,}{f\,\rm{O}}=0.1﹩, ﹩\frac{f\rm{C}\,}{f\,\rm{O}}=1﹩, ﹩\frac{f\rm{C}\,}{f\,\rm{O}}=10﹩, ﹩\frac{f\rm{C}\,}{f\,\rm{O}}=100﹩ are located at C/O values of 0.798, 0.859, 1.005, 1.684, and 6.964, respectively. Note that recent studies show C/Os above 1 occur in <0.1% of stars (J. M. Brewer & D. A. Fischer 2016).
Paper: The Effects of the Carbon-to-oxygen Ratio on the Condensate Compositions around Solar-like Stars
Authors: Cody J. Shakespeare, Min Li, Shichun Huang, Zhaohuan Zhu, Jason H. Steffen
Figure caption: The same figure type as M. Li et al.'s (2020) Figure 9 with four different C/Os. Carbon, nitrogen, and oxygen are appended to the right with red letters to denote the elements being artificially altered. The top-left graph is the same simulation as M. Li et al.'s (2020) M2G1 model in Figure 9 and has a solar C/O, which is 0.501. The top-right, bottom-left, and bottom-right plots correspond to the initial C/Os of 0.8, 1, and 2, respectively. Those three simulations are the closest to the ﹩\frac{f\rm{C}\,}{f\,\rm{O}}﹩ = 0.1, ﹩\frac{f\rm{C}\,}{f\,\rm{O}}﹩ = 1, and ﹩\frac{f\rm{C}\,}{f\,\rm{O}}﹩ = 10 lines in Figure 2, in the same order.
Paper: The Effects of the Carbon-to-oxygen Ratio on the Condensate Compositions around Solar-like Stars
Authors: Cody J. Shakespeare, Min Li, Shichun Huang, Zhaohuan Zhu, Jason H. Steffen
Figure caption: The nitrogen species that comprise the increased nitrogen in three simulations. Note the y-axis of the percent condensed mass plot is limited to 10% here. (Left) The N/O = 1.5 simulation. Note that N/O = 1.5 is positioned on the left to avoid being misidentified as C/O = 0.8 or C/O = 1, which hold the middle and right positions, and because the solar plot is not shown here. (Middle) The C/O = 0.8 simulation (the middle panel of Figure 4). (Right) The C/O = 1 simulation, shown here, is the C/O simulation that has the closest C/O to the indirect C/O of N/O = 1.5. Additionally, N/O = 1.5 has an indirect C/O of 1.10. Note that these species are not permanent and will change with later heating and aqueous alteration.
Paper: The Effects of the Carbon-to-oxygen Ratio on the Condensate Compositions around Solar-like Stars
Authors: Cody J. Shakespeare, Min Li, Shichun Huang, Zhaohuan Zhu, Jason H. Steffen
Figure caption: The solid surface density of carbon and the most significant species that comprise the total carbon in the three simulations shown in Figure 4; (left) solar, (middle) C/O = 0.8, and (right) C/O = 1. Note that these species are not permanent and will change with later heating and aqueous alteration.
Paper: The Effects of the Carbon-to-oxygen Ratio on the Condensate Compositions around Solar-like Stars
Authors: Cody J. Shakespeare, Min Li, Shichun Huang, Zhaohuan Zhu, Jason H. Steffen
Figure caption: The solid surface density profiles of five select elements in three different simulations: (left) C/O = 1.1, (middle) C/O = 1.3, and (right) C/O = 1.5. Note that the y-axis for the molar plot has changed compared to Figure 4. The surface density profile of Si, O, Fe, and N does not change significantly between the C/O = 1 simulation (see Figure 4) and the simulations shown here. Recent studies show C/Os above 1 occur in <0.1% of stars (J. M. Brewer & D. A. Fischer 2016). We include these simulation results for comparison with past studies like J. C. Bond et al. (2010b).
Paper: The Effects of the Carbon-to-oxygen Ratio on the Condensate Compositions around Solar-like Stars
Authors: Cody J. Shakespeare, Min Li, Shichun Huang, Zhaohuan Zhu, Jason H. Steffen
Figure caption: The same as Figure 6 but examining N/Os. The top-left, top-right, bottom-left, and bottom-right plots correspond to the initial N/Os of 0.1, 0.5, 0.75, and 1.5, respectively. Note that the solar N/O is 0.138, and the solar results are shown in the top-left plot of Figure 6.
Paper: The Effects of the Carbon-to-oxygen Ratio on the Condensate Compositions around Solar-like Stars
Authors: Cody J. Shakespeare, Min Li, Shichun Huang, Zhaohuan Zhu, Jason H. Steffen
Figure caption: The evolution of the gaseous disk parameters from the beginning (0.0 te) to the end (5.0 te) of our simulations. (Top) Midplane temperature; (Bottom) midplane pressure.
Paper: AstroSat/UVIT Far- and Near-UV Deep Field Around IC 4329A
Authors: Piyali Ganguly, Priyanka Rani, Gulab C. Dewangan
Figure caption: AstroSat/UVIT images of NGC 5298. Left panel: Two-color image constructed from NUV band (red) and FUV band (blue) images. A ring-like structure possibly connected with spiral arms and point-like sources inside the ring is clearly seen. Right panel: NUV band image of the same source showing extended diffuse emission. The two XMM-Newton sources found inside the galaxy are shown in red circles with labels “A” and “B.” The radius of each circle corresponds to 3σ, where σ represents the astrometric error on the X-ray source position. Additional diffuse emission including a patchy region in the upper-right side of the galaxy is clearly seen.
Paper: AstroSat/UVIT Far- and Near-UV Deep Field Around IC 4329A
Authors: Piyali Ganguly, Priyanka Rani, Gulab C. Dewangan
Figure caption: Two-color image of NGC 5302 constructed by showing the NUV band image in red and the FUV band image in blue. The galaxy is seen with a UV bright central core along with prominent spiral arms that are bright in both the FUV and NUV. A clear bifurcation can also be seen in one of the spiral arms (the arm in the lower-left region of the image).
Paper: Lunar Degree-2 Tidal Love Number Determination Based on Combination of Four-way Radiometric Tracking and LLR Data
Authors: Chongyang Wang, Jianguo Yan, Shangbiao Sun, Denggao Qiu, Jean-Pierre Barriot
Figure caption: Sensitivity of two-way and four-way observations with respect to ﹩{h}_{2}﹩ (left) and ﹩{l}_{2}﹩ (right). The sensitivity of the 2W laser ranging for Apollo mirrors is plotted as a green “x,” that of the 2W laser ranging in SPA is plotted as a blue “+,” that of the 4W range rate in SPA is plotted as a red “*,” and that of the 4W ranging in SPA is plotted as orange dots.
Paper: Lunar Degree-2 Tidal Love Number Determination Based on Combination of Four-way Radiometric Tracking and LLR Data
Authors: Chongyang Wang, Jianguo Yan, Shangbiao Sun, Denggao Qiu, Jean-Pierre Barriot
Figure caption: The formal uncertainty (left) and relative true error (right) of tidal Love numbers ﹩{h}_{2}﹩ and ﹩{l}_{2}﹩.
Paper: Lunar Degree-2 Tidal Love Number Determination Based on Combination of Four-way Radiometric Tracking and LLR Data
Authors: Chongyang Wang, Jianguo Yan, Shangbiao Sun, Denggao Qiu, Jean-Pierre Barriot
Figure caption: Sensitivity of two-way and four-way observations with respect to ﹩{k}_{2}﹩. The sensitivity of the 2W range rate is plotted as a blue “+,” that of the 2W range is plotted as green dots, that of the 4W range rate is plotted as an orange “x,” and that of the 4W range is plotted in red “*.”
Paper: Lunar Degree-2 Tidal Love Number Determination Based on Combination of Four-way Radiometric Tracking and LLR Data
Authors: Chongyang Wang, Jianguo Yan, Shangbiao Sun, Denggao Qiu, Jean-Pierre Barriot
Figure caption: Schematic of the two-way laser ranging and four-way radiometric tracking.
Paper: Orbital and Atmospheric Modeling of H II 1348B: An Eccentric Young Substellar Companion in the Pleiades
Authors: Gabriel Weible, Kevin Wagner, Jordan Stone, Steve Ertel, Dániel Apai, Kaitlin Kratter, Jarron Leisenring
Figure caption: Four ADI-KLIP-subtracted reduced images of the H II 1348 system, one from each telescope aperture of the LBT at each of two nod positions. The images have been cropped to the inner ﹩3\mathop{.}\limits^{^{\prime\prime} }1944\times 3\mathop{.}\limits^{^{\prime\prime} }1944﹩ and are shown with an ﹩{\rm{a}}\rm{sin}{\rm{h}}﹩ stretch in arbitrary units with SAOImageDS 9  (W. A. Joye & E. Mandel 2003). In the lower-right panel, the companion is labeled “B” and the binary host star residuals are masked and labeled “A.” Orientation on the celestial sphere and a scale is shown.
Paper: Multibeam SETI Observations Toward Nearby M Dwarfs with FAST
Authors: Xiao-Hang Luan, Bo-Lun Huang, Zhen-Zhao Tao, Yan Cui, Tong-Jie Zhang, Pei Wang
Figure caption: Waterfall plots around 1312.50 MHz of the observations toward other three sources. The left panels show XX, and the right panels show YY. They are only present in Beam 2 and appear obviously stronger in XX than YY, consistent with NBS 230624.
Paper: Multibeam SETI Observations Toward Nearby M Dwarfs with FAST
Authors: Xiao-Hang Luan, Bo-Lun Huang, Zhen-Zhao Tao, Yan Cui, Tong-Jie Zhang, Pei Wang
Figure caption: The power variation of NBS 230624 over time and the Lomb–Scargle periodogram. The left panels show the power variation of the signal bins of NBS 230624 over time for XX and YY polarizations. The right panels are the Lomb–Scargle periodograms accordingly. The solid line in the upper left panel denote a first-order Fourier function fitting, while the dotted black lines in the right panels are the FAP level at 0.001. See the main text for details.
Paper: Multibeam SETI Observations Toward Nearby M Dwarfs with FAST
Authors: Xiao-Hang Luan, Bo-Lun Huang, Zhen-Zhao Tao, Yan Cui, Tong-Jie Zhang, Pei Wang
Figure caption: A flow chart of the search pipeline and results. The pipeline consists of five steps. All hits in the 19 beams are obtained in the first step. All events are obtained using the MBCM blind search mode in the second step. The last three steps use RFI removal methods to filter the events. The numbers in each step are shown in the boxes, where the first row is for XX and the second row is for YY. Finally, NBS 230624 is found in both XX and YY polarizations.
Paper: Multibeam SETI Observations Toward Nearby M Dwarfs with FAST
Authors: Xiao-Hang Luan, Bo-Lun Huang, Zhen-Zhao Tao, Yan Cui, Tong-Jie Zhang, Pei Wang
Figure caption: An event detected at ∼1312.50 MHz toward AD Leo (NBS 230624). This figure shows XX polarization of all 19 beams.
Paper: Multibeam SETI Observations Toward Nearby M Dwarfs with FAST
Authors: Xiao-Hang Luan, Bo-Lun Huang, Zhen-Zhao Tao, Yan Cui, Tong-Jie Zhang, Pei Wang
Figure caption: Waterfall plots of AD Leo NBS 230624 in Beam 2. The left panels show XX, and the right panels show YY.
Paper: Giant Outer Transiting Exoplanet Mass (GOT ‘EM) Survey. V. Two Giant Planets in Kepler-511 but Only One Ran Away
Authors: Yayaati Chachan, Paul A. Dalba, Daniel P. Thorngren, Stephen R. Kane, Howard Isaacson, Eve J. Lee, Edward W. Schwieterman, Andrew W. Howard, Matthew J. Payne
Figure caption: Raw Kepler photometry showing the four transits of Kepler-511 b and three of the transits of Kepler-511 c. Each panel is centered on the mid-transit time of Kepler-511 b and includes 10 transit durations worth of data before and after. Some baseline data were lost in all quarters except for Quarter 7, and the Quarter 14 transit was lost altogether to a data gap. Even in the raw light curves, the transits of both planets are visible. The stellar variability, which was removed prior to fitting the transit, can be seen as a gentle, low-frequency variation in flux.
Paper: H2 Chemistry and Protonation in the Dayside Venusian Upper Atmosphere
Authors: Shiqi Wu, Xiaoshu Wu, Yanxing Liu, Jun Cui
Figure caption: A comparison of the total ion density profiles for protonated species (upper left) and nonprotonated species (upper right), among models assuming different imposed homospheric H2 mixing ratios: 5 ppb, 10 ppb, 50 ppb, 0.1 ppm, 0.2 ppm, 0.5 ppm, 1 ppm, 2 ppm, 4 ppm, 6 ppm, 8 ppm, and 10 ppm from light yellow to dark blue. Also presented are the profiles for the total ion (or electron) density (lower left) and the total density ratio of protonated to nonprotonated species (lower right) across the same range of homospheric H2 mixing ratios. Notice that in some panels, the displayed density profiles are nearly indistinguishable at sufficiently high H2 mixing ratios.
Paper: H2 Chemistry and Protonation in the Dayside Venusian Upper Atmosphere
Authors: Shiqi Wu, Xiaoshu Wu, Yanxing Liu, Jun Cui
Figure caption: The structure of the underlying Venusian upper atmosphere used in our model calculations, appropriate for the dayside averaged condition at moderate solar activity, including the density profiles of 10 background species: CO2, O(3P), CO, N2, N(4S), He, O2, H2, H, and Ar (left), along with the corresponding neutral, ion, and electron temperature profiles (right). The gray-shaded region encompasses the range of H2 distribution as model input, with a homospheric H2 mixing ratio from 5 ppb to 10 ppm.
Paper: H2 Chemistry and Protonation in the Dayside Venusian Upper Atmosphere
Authors: Shiqi Wu, Xiaoshu Wu, Yanxing Liu, Jun Cui
Figure caption: A comparison of the density profiles for several representative ion species, either protonated (HCO+ and OH+) or nonprotonated (O﹩{}_{2}^{+}﹩, O+(4S), and NO+), obtained with different choices of the homopsheric H2 mixing ratios: 10 ppb (upper left), 0.1 ppm (upper right), 1 ppm (lower left), and 10 ppm (lower right).
Paper: H2 Chemistry and Protonation in the Dayside Venusian Upper Atmosphere
Authors: Shiqi Wu, Xiaoshu Wu, Yanxing Liu, Jun Cui
Figure caption: A comparison of the variations of the topside densities for representative species, either protonated (left, HCO+ and OH+) or nonprotonated (right, O﹩{}_{2}^{+}﹩, O+(4S), and NO+), all as a function of the homospheric H2 mixing ratio.