adsabs/AstroCLIMB huggingface dataset:
Paper: Comparison of Exact and Approximate MHD Slow Body Mode Solutions in Photospheric Waveguides
Authors: Anwar A. Aldhafeeri, Gary Verth, Viktor Fedun, Matthew Lennard, I. Ballai
Figure caption: Polar representation of kink modes in a cylindrical waveguide. The top row shows different branches of the kink modes obtained by assuming v  z  = 0 on the boundary of the cylindrical waveguide. The bottom row shows the same branches of the kink modes obtained by solving the whole dispersion relation. The labels (m = (x, y)) represent the type of mode and branch; e.g., x = 1 refers to the kink mode, and y = 2 refers to the second branch.
Paper: Comparison of Exact and Approximate MHD Slow Body Mode Solutions in Photospheric Waveguides
Authors: Anwar A. Aldhafeeri, Gary Verth, Viktor Fedun, Matthew Lennard, I. Ballai
Figure caption: Same as Figure 4 but for sausage modes.
Paper: Comparison of Exact and Approximate MHD Slow Body Mode Solutions in Photospheric Waveguides
Authors: Anwar A. Aldhafeeri, Gary Verth, Viktor Fedun, Matthew Lennard, I. Ballai
Figure caption: Same as Figure 2, but here we plot the amplitude of the z-component of the velocity for slow body kink modes under photospheric conditions.
Paper: Characterizing Extreme Emission Line Galaxies. II. A Self-consistent Model of Their Ionizing Spectrum 
Authors: Grace M. Olivier, Danielle A. Berg, John Chisholm, Dawn K. Erb, Richard W. Pogge, Evan D. Skillman
Figure caption: The same as Figure 5 but showing the line ratio diagrams for the other five emission lines spanning the different ionization zones with the observed line ratio plotted as the point for J104457 and J141851. The “Stars Only” column shows the CLOUDY photoionization models where we used the ionizing continuum from the stellar population we fit to these galaxies in Section 3.2 as the input ionizing spectrum. Each line is a different metallicity from low metallicity at 1% Z ⊙ in yellow to 11% Z ⊙ in purple for J104457, and for J141851 the range starts with 3% Z ⊙ in yellow and goes to 13% Z ⊙ in purple. The black dashed line shows the results of a model run with the observed gas-phase metallicity of each galaxy, 5.8% Z ⊙ for J104457 and 8.7% Z ⊙ for J141851. In the “Stars + BB” column, the models are plotted in bands with the same metallicity color-coding system, but the bands now include the effects of the blackbodies we modeled. The band is bordered by a dotted line showing the 0% L tot (no BB) model and a dashed–dotted line showing the 75% L tot from a 100 kK blackbody. The black hatched region shows the models run with the observed gas-phase metallicity of the galaxy.
Paper: Characterizing Extreme Emission Line Galaxies. II. A Self-consistent Model of Their Ionizing Spectrum 
Authors: Grace M. Olivier, Danielle A. Berg, John Chisholm, Dawn K. Erb, Richard W. Pogge, Evan D. Skillman
Figure caption: The ionizing continuum from the stellar continuum fits for the BPASS models for J104457 is shown in the top panel and for J141851 in the bottom panel. It includes a blackbody with a luminosity 45% of L tot for J104457 and 55% of L tot for J141851, a temperature of 80 kK, and the stellar continuum fit plus the plotted blackbody. The circles show the intersection of each model with the wavelength required to produce He II and C IV.
Paper: Characterizing Extreme Emission Line Galaxies. II. A Self-consistent Model of Their Ionizing Spectrum 
Authors: Grace M. Olivier, Danielle A. Berg, John Chisholm, Dawn K. Erb, Richard W. Pogge, Evan D. Skillman
Figure caption: Similar to Figure 5 but this demonstrates the [Fe V] λ4227 emission line ratios and the models we used in Appendix B. The models without an additional source do not reproduce the observed emission lines, but an added BB source does enable the models to reach the observations. These models greatly overpredict the emission line ratios we observe from [Fe V], so we show a cropped version of the plot in the bottom row to show observations more clearly.
Paper: Characterizing Extreme Emission Line Galaxies. II. A Self-consistent Model of Their Ionizing Spectrum 
Authors: Grace M. Olivier, Danielle A. Berg, John Chisholm, Dawn K. Erb, Richard W. Pogge, Evan D. Skillman
Figure caption: Similar to Figure 5 but showing the [Ne V] λ3426 emission line and the models we tested in Appendix B, which include the [Ne V]/Hβ line ratio to constrain the very-high-energy photons with energies > ∼ 100 eV. The models with the added BB component sharply increase at high ﹩\mathrm{log}U﹩ values and are able to reach the observed emission line ratio for both galaxies.
Paper: Shocks in the Outflow of the RS Oph 2021 Eruption Observed with X-Ray Gratings
Authors: Marina Orio, E. Behar, G. J. M. Luna, J. J. Drake, J. Gallagher, J. S. Nichols, J. U. Ness, A. Dobrotka, J. Mikolajewska, M. Della Valle, R. Ignace, R. Rahin
Figure caption: The observed profile, in the count rate spectrum, of the Si XIII (right) and S XV (left) He-like triplets observed with the HEG. The clear line on the left with the highest count rate is the resonance (r), the clear line on the right is the forbidden (f), while in the middle an intercombination (i) line is barely resolved, The i line is composed of two lines very close in wavelength, hardly resolvable. The red lines show the fits with three Gaussians with the same width, and a locally evaluated underlying continuum, convolved with the instrumental response.
Paper: Shocks in the Outflow of the RS Oph 2021 Eruption Observed with X-Ray Gratings
Authors: Marina Orio, E. Behar, G. J. M. Luna, J. J. Drake, J. Gallagher, J. S. Nichols, J. U. Ness, A. Dobrotka, J. Mikolajewska, M. Della Valle, R. Ignace, R. Rahin
Figure caption: A close-up showing the model with two thermal components in Table 1 (middle column) and in Figure 1, resulting from fitting the binned spectrum with signal-to-noise ratio of 10 and convolving it with the instrument response for the Si XIV H-like, S XIII He-like, Mg XII H-like, and Mg XI He-like lines. The hotter component is shown in red, the less hot with the black dotted line, and the sum of the two with the black solid line. As shown also by Figure 2, the intercombination lines are predicted to be unresolvable, so we see only two clear lines (r and f) in the model.
Paper: Shocks in the Outflow of the RS Oph 2021 Eruption Observed with X-Ray Gratings
Authors: Marina Orio, E. Behar, G. J. M. Luna, J. J. Drake, J. Gallagher, J. S. Nichols, J. U. Ness, A. Dobrotka, J. Mikolajewska, M. Della Valle, R. Ignace, R. Rahin
Figure caption: The spectrum observed with the Chandra MEG grating (left) and with the Chandra HEG grating (right) on 2021 August 27, day 18 after optical maximum, and a fit with the two APEC components described in the text, whose parameters are given in the second column of Table 1.
Paper: Shocks in the Outflow of the RS Oph 2021 Eruption Observed with X-Ray Gratings
Authors: Marina Orio, E. Behar, G. J. M. Luna, J. J. Drake, J. Gallagher, J. S. Nichols, J. U. Ness, A. Dobrotka, J. Mikolajewska, M. Della Valle, R. Ignace, R. Rahin
Figure caption: HEG line profiles of the the H-like lines of Si XIV and Mg XII and fit with a Gaussian, in velocity space. The profile is clearly asymmetric; we interpret this as the effect of differential photoelectric absorption by the outflowing material of the nova, which erodes the red wing much more than the blue one.
Paper: Shocks in the Outflow of the RS Oph 2021 Eruption Observed with X-Ray Gratings
Authors: Marina Orio, E. Behar, G. J. M. Luna, J. J. Drake, J. Gallagher, J. S. Nichols, J. U. Ness, A. Dobrotka, J. Mikolajewska, M. Della Valle, R. Ignace, R. Rahin
Figure caption: Comparison of the Chandra MEG spectrum (in black) observed on 2021 August 27 and the XMM-Newton RGS spectrum (in red) observed on 2021 August 30–31 in the 5–14 Å wavelength range.
Paper: BASS XXXVII: The Role of Radiative Feedback in the Growth and Obscuration Properties of Nearby Supermassive Black Holes
Authors: C. Ricci, T. T. Ananna, M. J. Temple, C. M. Urry, M. J. Koss, B. Trakhtenbrot, Y. Ueda, D. Stern, F. E. Bauer, E. Treister, G. C. Privon, K. Oh, S. Paltani, M. Stalevski, L. C. Ho, A. C. Fabian, R. Mushotzky, C. S. Chang, F. Ricci, D. Kakkad, L. Sartori, R. Baer, T. Caglar, M. Powell, F. Harrison
Figure caption: Top panel: BASS AGNs (red diamonds) in the N H–λ Edd plane. The dashed, dotted, and dotted–dashed black lines represent the 50%, 68%, and 90% number density contours in the 10−3 ≤ λ Edd ≤ 1 range. The black continuous line represents the effective Eddington limit for dusty gas reported in Fabian et al. (2009). The horizontal line at ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})=22﹩ represents the assumed maximum contribution to N H of gas from the host galaxy. The colored surface represents the blowout region. The dashed–dotted line shows the effective Eddington limit when including infrared radiation trapping (Ishibashi et al. 2018), adapted to the values of Fabian et al. (2009), similarly to what was done by Lansbury et al. (2020). The dashed line represents the effective Eddington limit for dusty gas reported by Ishibashi et al. (2018; see also Venanzi et al. 2020). The typical uncertainties are reported in the top-left corner for Compton-thin and CT AGNs. Sources for which N H was too low to be constrained were assigned ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})=20﹩. The low number of low λ Edd points is due to relatively low sensitivity of Swift/BAT, which does not allow it to detect low-luminosity AGNs. Bottom panel: a schematic of the radiation-regulated growth model outlined here: an accretion event (1) leads to an increase of the Eddington ratio and typical column density of an AGN (2), which would be preferentially observed as an obscured or type 2 source, due to the large covering factor of the obscuring material. As the Eddington ratio increases above the effective Eddington limit for dusty gas, the AGN spends a short time in the blowout region (3), before its covering factor decreases, and it is mostly observed as an unobscured or type 1 source (4). Once most of the material has been accreted, or blown away by infrared radiation trapping, the source moves back to having low values of N H and λ Edd. The lines are the same as in the top panel.
Paper: BASS XXXVII: The Role of Radiative Feedback in the Growth and Obscuration Properties of Nearby Supermassive Black Holes
Authors: C. Ricci, T. T. Ananna, M. J. Temple, C. M. Urry, M. J. Koss, B. Trakhtenbrot, Y. Ueda, D. Stern, F. E. Bauer, E. Treister, G. C. Privon, K. Oh, S. Paltani, M. Stalevski, L. C. Ho, A. C. Fabian, R. Mushotzky, C. S. Chang, F. Ricci, D. Kakkad, L. Sartori, R. Baer, T. Caglar, M. Powell, F. Harrison
Figure caption: Fraction of obscured Compton-thin ﹩[22\leqslant \mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\lt 24]﹩ sources vs. Eddington ratio for AGNs from our hard X-ray selected sample with ﹩-4.8\leqslant \mathrm{log}{\lambda }_{\mathrm{Edd}}\lt 0﹩. For each λ Edd bin, the fractions were normalized to unity in the ﹩20\leqslant \mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\lt 24﹩ interval. The red lines show the expected Eddington limit for dusty gas with ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\simeq 22﹩ from Fabian et al. (2006                       2008                       2009; dashed line) and Ishibashi et al. (2018; dotted line). The fractions are calculated following Cameron (2011), and the uncertainties quoted represent the 16th and 84th quantiles of a binomial distribution.
Paper: BASS XXXVII: The Role of Radiative Feedback in the Growth and Obscuration Properties of Nearby Supermassive Black Holes
Authors: C. Ricci, T. T. Ananna, M. J. Temple, C. M. Urry, M. J. Koss, B. Trakhtenbrot, Y. Ueda, D. Stern, F. E. Bauer, E. Treister, G. C. Privon, K. Oh, S. Paltani, M. Stalevski, L. C. Ho, A. C. Fabian, R. Mushotzky, C. S. Chang, F. Ricci, D. Kakkad, L. Sartori, R. Baer, T. Caglar, M. Powell, F. Harrison
Figure caption: Top panel: covering factor of obscuring material vs. Eddington ratio for the objects in our hard X-ray selected sample with ﹩-4\leqslant \mathrm{log}{\lambda }_{\mathrm{Edd}}\lt 0﹩. The covering factor was obtained by considering the fraction of obscured sources, as in Figure 1, including the Compton-thick fraction from Ricci et al. (2017a), and normalizing to unity in the ﹩20\leqslant \mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\lt 25﹩ interval. The red vertical line shows the break in the ERDF (﹩{\lambda }_{\mathrm{Edd}}^{* }﹩), while the hatched vertical area shows the uncertainty on ﹩{\lambda }_{\mathrm{Edd}}^{* }﹩ (Ananna et al. 2022b). The blue hatched horizontal area represents the observed interval of the covering factor overlapping with ﹩{\lambda }_{\mathrm{Edd}}^{* }﹩. The blue dashed line corresponds to f obs = 50%. The value of ﹩{\lambda }_{\mathrm{Edd}}^{* }﹩ corresponds to the Eddington ratio where the transition between most of the sources being obscured (f obs > 50%) to most of the sources being unobscured (f obs < 50%) is observed. Bottom panel: same as the top panel for the 14–150 keV luminosity. The red vertical line shows the break in the LF (﹩{L}_{14\mbox{--}150}^{* }﹩), while the hatched vertical area shows its uncertainty (Ananna et al. 2022b).
Paper: BASS XXXVII: The Role of Radiative Feedback in the Growth and Obscuration Properties of Nearby Supermassive Black Holes
Authors: C. Ricci, T. T. Ananna, M. J. Temple, C. M. Urry, M. J. Koss, B. Trakhtenbrot, Y. Ueda, D. Stern, F. E. Bauer, E. Treister, G. C. Privon, K. Oh, S. Paltani, M. Stalevski, L. C. Ho, A. C. Fabian, R. Mushotzky, C. S. Chang, F. Ricci, D. Kakkad, L. Sartori, R. Baer, T. Caglar, M. Powell, F. Harrison
Figure caption: Fraction of sources with N H in a given range vs. Eddington ratio for the objects in our hard X-ray selected sample with ﹩-4.5\leqslant \mathrm{log}{\lambda }_{\mathrm{Edd}}\lt 0﹩. For each λ Edd bin, the fractions were normalized to unity in the ﹩20\leqslant \mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\lt 24﹩ interval. The red lines show the expected Eddington limit for dusty gas with ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\simeq 22﹩ (bottom-left panel; dashed line from Fabian et al. 2006, 2008, 2009; dotted line from Ishibashi et al. 2018) and ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\simeq 23﹩ (bottom-right panel; Ishibashi et al. 2018; Venanzi et al. 2020). The latter value of the effective Eddington limit includes the contribution from IR radiation trapping. The fractions are calculated following Cameron (2011), and the uncertainties quoted represent the 16th and 84th quantiles of a binomial distribution.
Paper: BASS XXXVII: The Role of Radiative Feedback in the Growth and Obscuration Properties of Nearby Supermassive Black Holes
Authors: C. Ricci, T. T. Ananna, M. J. Temple, C. M. Urry, M. J. Koss, B. Trakhtenbrot, Y. Ueda, D. Stern, F. E. Bauer, E. Treister, G. C. Privon, K. Oh, S. Paltani, M. Stalevski, L. C. Ho, A. C. Fabian, R. Mushotzky, C. S. Chang, F. Ricci, D. Kakkad, L. Sartori, R. Baer, T. Caglar, M. Powell, F. Harrison
Figure caption: Top panel: ERDFs of type 1 and type 2 BASS AGNs from Ananna et al. (2022b). The vertical red lines show the expected Eddington limit for dusty gas with ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\simeq 22﹩ (dashed line from Fabian et al. 2006, 2008, 2009; dotted line from Ishibashi et al. 2018) and ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\simeq 23﹩ (dotted–dashed line from Ishibashi et al. 2018; see also Venanzi et al. 2020). Bottom panel: ratio between the Eddington ratio distribution function of type 2 AGNs and that of the whole AGN population, which is a proxy of the fraction of obscured sources and of the covering factor of the obscuring material.
Paper: The Directly Imaged Exoplanet Host Star 51 Eridani is a Gamma Doradus Pulsator
Authors: Aldo G. Sepulveda, Daniel Huber, Zhoujian Zhang, Gang Li, Michael C. Liu, Timothy R. Bedding
Figure caption: (a) TESS Sector 5 light curve of 51 Eri. Error bars are smaller than the symbol sizes. (b) Same as (a) but for Sector 32. (c) Corresponding amplitude spectra of each light curve in log–log space. (d) Corresponding amplitude spectra of each light curve in linear–linear space and zoomed in on the location of the γ Dor pulsations. Downward triangles denote the significant pulsation frequencies that we extracted from the concatenated time series as described in Section 2.1.
Paper: The Directly Imaged Exoplanet Host Star 51 Eridani is a Gamma Doradus Pulsator
Authors: Aldo G. Sepulveda, Daniel Huber, Zhoujian Zhang, Gang Li, Michael C. Liu, Timothy R. Bedding
Figure caption: Kepler γ Dor stars from Li et al. (2020) that pulsate in ℓ = 1 gravity modes and that also have a core rotation measurement. The black dots denote their mean ℓ = 1 gravity mode frequency compared to their core rotation period. The vertical blue lines denote the boundaries of our estimate for the mean ℓ = 1 gravity mode frequency of 51 Eri (1.57 ± 0.09 cycle day−1) which is used to collect a subpopulation of core rotation periods. The inset histogram corresponds to this subpopulation that lies within our boundary for 51 Eri and its median and 16th/84th percentiles correspond to ﹩{0.9}_{-0.1}^{+0.3}﹩ days. We show the y-axis at a limit of ∼5 days for aesthetic purposes but a few long-period outliers reside above this limit.
Paper: The Directly Imaged Exoplanet Host Star 51 Eridani is a Gamma Doradus Pulsator
Authors: Aldo G. Sepulveda, Daniel Huber, Zhoujian Zhang, Gang Li, Michael C. Liu, Timothy R. Bedding
Figure caption: Gaia-based color–magnitude diagram for a sample of Kepler stars as described in Section 3.1. The orange diamonds are the δ Scuti stars and the blue squares are the γ Dor stars overplotted. 51 Eri is overplotted as a large magenta star. The small, gray, semitransparent dots represent the general population of Kepler stars.
Paper: The Directly Imaged Exoplanet Host Star 51 Eridani is a Gamma Doradus Pulsator
Authors: Aldo G. Sepulveda, Daniel Huber, Zhoujian Zhang, Gang Li, Michael C. Liu, Timothy R. Bedding
Figure caption: Residual TESS light curve of 51 Eri after removing high-frequency signal as described in Section 2.2. No significant nonstellar variability is detected.
Paper: Alternative Methylated Biosignatures. I. Methyl Bromide, a Capstone Biosignature
Authors: Michaela Leung, Edward W. Schwieterman, Mary N. Parenteau, Thomas J. Fauchez
Figure caption: Comparison of mixing ratios from Segura et al. (2005) and this work for the Sun and AD Leo. Our work also shows the photochemical buildup around TRAPPIST-1, which is the latest-type M dwarf typically evaluated for exoplanet studies. We construct a CH3Cl profile with surface mixing ratio of 0.5 ppb based on best available data for the Earth (Seinfeld & Pandis 2016), which is slightly higher than the profile used by Segura et al. (2005). We also generate a mixing ratio profile for AD Leo that is lower than than the previous results by more than an order of magnitude. These changes can be attributed to significant overhauls of the atmos model in the intervening years (e.g., Arney et al. 2016; Lincowski et al. 2018).
Paper: Alternative Methylated Biosignatures. I. Methyl Bromide, a Capstone Biosignature
Authors: Michaela Leung, Edward W. Schwieterman, Mary N. Parenteau, Thomas J. Fauchez
Figure caption: Buildup of CH3Cl in planetary atmospheres around different stellar types. The white circle shows the Earth’s flux levels, the thick bar shows an order of magnitude above and below, and the thinner line represents a 1000× enhancement or depletion of the flux vs. Earth’s global average. The green line shows the Earth’s global average mixing ratio, and the blue line indicates 1 ppm.
Paper: Alternative Methylated Biosignatures. I. Methyl Bromide, a Capstone Biosignature
Authors: Michaela Leung, Edward W. Schwieterman, Mary N. Parenteau, Thomas J. Fauchez
Figure caption: Concept figure showing the production, reaction, and absorption by CH3Br in a theoretical exoplanet. Methylated chalcogens such as ﹩{({\mathrm{CH}}_{3})}_{2}\mathrm{Se}﹩ are shown in orange and yellow.
Paper: Alternative Methylated Biosignatures. I. Methyl Bromide, a Capstone Biosignature
Authors: Michaela Leung, Edward W. Schwieterman, Mary N. Parenteau, Thomas J. Fauchez
Figure caption: Atmospheric buildup of CH3Cl. Crosshairs show the Earth flux and atmospheric abundance. The region highlighted in green is comparable to preindustrial methane concentrations on Earth.
Paper: Alternative Methylated Biosignatures. I. Methyl Bromide, a Capstone Biosignature
Authors: Michaela Leung, Edward W. Schwieterman, Mary N. Parenteau, Thomas J. Fauchez
Figure caption: Comparison of the number of transits needed to reach 3σ or 5σ detection for two different bands where both CH3Cl and CH3Br absorb for three scenarios: CH3Cl only, CH3Br only, and both gases together. We also consider both the 100× (prerunaway) and 1000× (runaway) flux conditions. All transits are calculated for TRAPPIST-1e, using planetary parameters from Agol et al. (2021) and the MISC-TRA instrument on the Origins Space Telescope concept, simulated using PSG.
Paper: Alternative Methylated Biosignatures. I. Methyl Bromide, a Capstone Biosignature
Authors: Michaela Leung, Edward W. Schwieterman, Mary N. Parenteau, Thomas J. Fauchez
Figure caption: Transmission spectra simulated by PSG for 100× Earth-averaged CH3Br, CH3Cl, and both gas fluxes for TRAPPIST-1e. The combined atmosphere typically has an absorption feature the size of or larger than the larger of the two individual gas features, with the major exceptions seen around 3.3 μm due to decreased CH4 and 9.65 μm from diminished O3. See Section 4.1 for more information.
Paper: Alternative Methylated Biosignatures. I. Methyl Bromide, a Capstone Biosignature
Authors: Michaela Leung, Edward W. Schwieterman, Mary N. Parenteau, Thomas J. Fauchez
Figure caption: Transmission spectra simulated by PSG for 100× Earth-averaged CH3Br and CH3Cl flux for TRAPPIST-1e. Assumes Origins space telescope in the MISC-T configuration observation of TRAPPIST-1e. Includes error bars for 27 transits, the minimum number to detect the broad coadded feature around 10 μm at this flux level.
Paper: Alternative Methylated Biosignatures. I. Methyl Bromide, a Capstone Biosignature
Authors: Michaela Leung, Edward W. Schwieterman, Mary N. Parenteau, Thomas J. Fauchez
Figure caption: Comparison of emission features for atmospheres with methylated biogenic gases around a K6V, M3.5Ve, and M5V star. From top to bottom: CH3Cl, CH3Br, and combination of CH3Cl and CH3Br for a range of fluxes ranging from globally averaged modern-Earth fluxes to most productive local terrestrial and marine environments. Spectra are shown for a 50% clear sky, 50% cloudy with equal parts cirrus and stratocumulus clouds.
Paper: Alternative Methylated Biosignatures. I. Methyl Bromide, a Capstone Biosignature
Authors: Michaela Leung, Edward W. Schwieterman, Mary N. Parenteau, Thomas J. Fauchez
Figure caption: Simulated high-resolution (R = 100,000) transmission spectroscopy of Proxima Centauri b. For maximally productive environments of CH3Cl (red) and CH3Br (blue), clearly distinct absorption lines are produced, which can be distinguished from each other, and from the base atmosphere, which is shown in gray. Also shown is an atmosphere with both CH3Cl and CH3Br, which shows both components (purple). The spectra are vertically offset to better show the line structure and are simulated for a clear sky atmosphere.
Paper: Alternative Methylated Biosignatures. I. Methyl Bromide, a Capstone Biosignature
Authors: Michaela Leung, Edward W. Schwieterman, Mary N. Parenteau, Thomas J. Fauchez
Figure caption: Atmospheric buildup of CH3Br in planetary atmospheres around different stellar types. The white circle shows the Earth’s flux levels, the thick bar shows an order of magnitude above and below, and the thinner line represents a 1000× extension of the flux. The green line shows the Earth’s mixing ratio, and the blue line indicates 1 ppm. Compare to Figure 3.