adsabs/AstroCLIMB huggingface dataset:
Paper: Retrieved Atmospheres and Inferred Surface Properties for Terrestrial Exoplanets Using Transmission and Reflected-light Spectroscopy
Authors: Samantha Gilbert-Janizek, Victoria S. Meadows, Jacob Lustig-Yaeger
Figure caption: A comparison of O3 total column abundance distributions calculated for retrieval models with and without vertical resolution for both the clear-sky and cloudy direct-imaging cases. For both cases, we find that the total column abundance of O3 is well constrained using any of the vertically resolved models, while the evenly mixed model shows a small bias toward higher column abundances that worsens in the presence of clouds.
Paper: Retrieved Atmospheres and Inferred Surface Properties for Terrestrial Exoplanets Using Transmission and Reflected-light Spectroscopy
Authors: Samantha Gilbert-Janizek, Victoria S. Meadows, Jacob Lustig-Yaeger
Figure caption: A comparison of the vertically resolved O3 profiles retrieved by the ﹩{{ \mathcal M }}_{3P}﹩ and ﹩{{ \mathcal M }}_{3F}﹩ forward model for the clear-sky Earth. The Bayes factors weakly favor the three-fixed-points model (﹩{{ \mathcal M }}_{3P}﹩) over the evenly mixed case (﹩{{ \mathcal M }}_{\mathrm{iso}}﹩) and the three-free-points model (﹩{{ \mathcal M }}_{3F}﹩), which has more free parameters.
Paper: Accretion of Meteoric Organic Matter at the Surface of Mars and Potential Production of Methane by Ultraviolet Radiation
Authors: Juan Diego Carrillo-Sánchez, John M. C. Plane, Diego Janches, Gerónimo L. Villanueva
Figure caption: Seasonal and latitudinal variability for the diurnal average temperature at the Martian surface as provided by the MCD (left-hand panel of Figure 7(a)); the diurnal average UV radiation in the wavelength range between 200 and 400 nm, in W m−2, at the surface of Mars (left-hand panel of Figure 7(b)); and the atmospheric pressure at the surface level provided by the MCD (left-hand panel of Figure 7(c)). Right-hand panels show the annual average surface temperature (Figure 7(a)), the annual average UV flux (solid black line; Moores et al. 2017) compared to a previous estimate (dashed green line; Moores & Schuerger 2012), and the annual average surface pressure (Figure 7(c)), where the vertical dashed red line represents the corresponding average value of this profile.
Paper: Accretion of Meteoric Organic Matter at the Surface of Mars and Potential Production of Methane by Ultraviolet Radiation
Authors: Juan Diego Carrillo-Sánchez, John M. C. Plane, Diego Janches, Gerónimo L. Villanueva
Figure caption: Diagram illustrating the variability with the orbital position (L  S ) of the total mass flux of MMs, the total accreted mass of carbon, and the methane production rates by UV (200–400 nm) radiation at the Martian surface. The values in parentheses represent the fraction of total MMs with respect to the total initial mass input before atmospheric ablation. The fluxes of carbon and the methane production rates are first estimated assuming a CI-chondrite carbon content of 5 wt% for all meteoroid populations, while the values in italics represent the corresponding fluxes for a carbon content of 25.6 wt% for comets—JFCs and HTCs (see also Figure 4). The methane fluxes shown in this figure are calculated assuming a UV photolysis yield for methane production of 20%. As discussed in Section 2.3, the methane production rates are estimated considering the yearly average accretion rates of carbon and, therefore, assuming that the reservoir of carbon is not altered substantially by the orbital fluctuations of the accretion of MMs; therefore, the methane fluxes only depend on the latitudinal and orbital fluctuations of UV radiation at the Martian surface. The maximum accretion of MMs is located around the FCEP (L  S  = 325°), whereas the maximum methane rates occur between L  S  = 251° (perihelion) and L  S  = 270° (northern winter/southern summer). Note that the mass fluxes are expressed in kg sol−1 (1 solar day at Mars is equivalent to 1.0275 Earth days).
Paper: Accretion of Meteoric Organic Matter at the Surface of Mars and Potential Production of Methane by Ultraviolet Radiation
Authors: Juan Diego Carrillo-Sánchez, John M. C. Plane, Diego Janches, Gerónimo L. Villanueva
Figure caption: Seasonal and latitudinal variability of the average diameter distributions, in microns, of the accreted MMs at the Martian surface determined by the CABMOD-MIF model as a function of the Martian latitude and the solar longitude for the JFCs (a), the ASTs (b), and the HTCs (c). Note that the color scales are different for each meteoroid population.
Paper: Accretion of Meteoric Organic Matter at the Surface of Mars and Potential Production of Methane by Ultraviolet Radiation
Authors: Juan Diego Carrillo-Sánchez, John M. C. Plane, Diego Janches, Gerónimo L. Villanueva
Figure caption: Elemental abundance of carbon relative to Si and to the CI-chondrite composition for the solar photosphere (brown star; Lodders & Fegley 2011) compared to the JFC 67P/Churyumov–Gerasimenko (blue triangle; Bardyn et al. 2017); the preliminary measurements of asteroid Bennu by the OSIRIS-REx mission (dark cyan triangle; Witze 2023); the HTC 1P/Halley (orange triangles; Bergin et al. 2015); five OCCs, C/2013 US10 Catalina, C/2012 K1 Pan-STARRS, C/2013 X1 Pan-STARRS, C/2018 W2 Africano, and C/1995 O1 Hale–Bopp (magenta triangles; Woodward et al. 2021); and the average for bulk chondritic porous IDPs (gray square; Thomas et al. 1994). On average, cometary particles exhibit an enrichment in the elemental ratio of carbon relative to Si and to the CI-chondrite composition of ﹩{7.1}_{-1.4}^{+2.4}﹩ (light blue circle).
Paper: Accretion of Meteoric Organic Matter at the Surface of Mars and Potential Production of Methane by Ultraviolet Radiation
Authors: Juan Diego Carrillo-Sánchez, John M. C. Plane, Diego Janches, Gerónimo L. Villanueva
Figure caption: Panel (a): total accretion rates of carbon at the surface of Mars, in kg m−2 s−1, as a function of the Martian latitude and the solar longitude. Panel (b): annual average of the total accretion rates of carbon assuming an average carbon content of 5 wt% for all meteoroid populations, typical for CI chondrites (solid black line). The shaded blue region represents the accretion rates between a chondritic composition and those with a carbon content of 25.6 wt% for particles with a cometary origin (dashed black line). The contribution of each meteoroid population to the total accretion rates of carbon is also displayed in panel (b): the JFCs (solid blue line), the ASTs (solid green line), and the HTCs (solid orange line). Panel (b) also illustrates the fluxes of organic carbon inferred by Flynn (1996; dashed–dotted black line) and Frantseva et al. (2018; dashed–dotted red line) and weighted assuming the surface area of each latitudinal band has a resolution of 5°.
Paper: Accretion of Meteoric Organic Matter at the Surface of Mars and Potential Production of Methane by Ultraviolet Radiation
Authors: Juan Diego Carrillo-Sánchez, John M. C. Plane, Diego Janches, Gerónimo L. Villanueva
Figure caption: Annual average mass input as a function of the impact velocity for the JFCs (solid blue line), ASTs (solid green line), HTCs (solid orange line), and total mass flux (solid black line). The shaded regions represent the corresponding mass influxes between aphelion (L  S  = 71°; dashed–dotted lines) and perihelion (L  S  = 251°; dashed lines). This figure also shows the annual average input velocities for each meteoroid population along with the corresponding average values at aphelion and perihelion. The lower and upper limits of the top bars illustrate the average velocity at aphelion and perihelion for each meteoroid population and the total mass influx, respectively. The vertical lines in these bars show the corresponding annual average input velocity.
Paper: Accretion of Meteoric Organic Matter at the Surface of Mars and Potential Production of Methane by Ultraviolet Radiation
Authors: Juan Diego Carrillo-Sánchez, John M. C. Plane, Diego Janches, Gerónimo L. Villanueva
Figure caption: Seasonal variability of the mass fluxes, in kg sol−1, with the orbital position. Panel (a): mass fluxes of meteoroids before atmospheric entry for the JFCs (blue line), ASTs (green line), HTCs (orange line), and total mass input (black line). Panel (b): mass fluxes of total MMs (gray line), uMMs (dashed light green line), CSs (dashed red line), and total ablated (solid dark red line). Panel (c): mass fluxes of accreted sulfur (solid dark green line), total carbon (solid dark blue line), soluble and insoluble phases of carbon (dashed green and brown lines), carbon accreted from particles that do not reach the pyrolysis temperature (∼900 K) during their atmospheric entry (dashed gray line), and methane production rates (solid dark yellow line) assuming a UV photolysis yield of 20%. The fluxes of carbon and methane are estimated assuming a chondritic carbon content of 5 wt% for all meteoroid populations.
Paper: Accretion of Meteoric Organic Matter at the Surface of Mars and Potential Production of Methane by Ultraviolet Radiation
Authors: Juan Diego Carrillo-Sánchez, John M. C. Plane, Diego Janches, Gerónimo L. Villanueva
Figure caption: Seasonal and latitudinal variability of the overall mass influxes, in kg sol−1, of meteoroids before atmospheric entry (panel (a)) and total accreted MMs at the Martian surface—uMMs and CSs (panel (b))—as a function of the Martian latitude and the solar longitude.
Paper: Accretion of Meteoric Organic Matter at the Surface of Mars and Potential Production of Methane by Ultraviolet Radiation
Authors: Juan Diego Carrillo-Sánchez, John M. C. Plane, Diego Janches, Gerónimo L. Villanueva
Figure caption: Average lifetimes of organics within the accreted particles in Log10(Earth years) as a function of the Martian latitude and the particle diameter in microns. Note that the particle diameters considered in this study range from 10 to 1500 μm. The average lifetimes predicted by the CABMOD-MIF model for the three meteoroid populations—the JFCs (b), the ASTs (c), and the HTCs (d)—are compared with the estimates provided by Moores et al. (2017) (panel (a)). Values of lifetimes range from 61.7 Earth yr (32.8 Martian yr) to 3.16 × 105 Earth yr (1.68 × 105 Martian yr). The vertical dashed lines represent the range of the average typical diameters of accreted particles for each meteoroid population estimated by the CABMOD-MIF model (see also Figure 5). According to Moores et al. (2017), the fraction of MMs that survive pyrolysis during atmospheric entry decreases drastically for diameters larger than 580 μm, tending to zero for diameters >1240 μm. In contrast, the CABMOD-MIF model estimates that there is a fraction of large MMs that do not pyrolyze in the upper atmosphere. Likewise, the differences between the calculated lifetimes in the three meteoroid sources ultimately depend on the fraction of MMs in each population that do not pyrolyze during their atmospheric entry.
Paper: Accretion of Meteoric Organic Matter at the Surface of Mars and Potential Production of Methane by Ultraviolet Radiation
Authors: Juan Diego Carrillo-Sánchez, John M. C. Plane, Diego Janches, Gerónimo L. Villanueva
Figure caption: Annual average of the total surface load of carbon assuming mixing with the near-surface regolith until saturation (black lines). The solid black line represents the saturation limit assuming an average carbon content of 5 wt% for all meteoroid populations—typical for CI chondrites—and, consequently, mixing occurs below this limit. The horizontal red lines indicate the individual measurements of surface carbon for MSL (Freissinet et al. 2015) and for the Viking 1 and 2 landers (Navarro-González et al. 2010). Note that the results of MSL can be explained assuming an enrichment in carbon for cometary particles by a factor of 5.5 (blue shaded region). The gray circles represent the linear extrapolation of these mixing ratios estimated by the Viking landers for an average perchlorate content of 0.5 wt%. The contribution of each meteoroid population to the total surface load of carbon is also displayed: the JFCs (solid blue line), the ASTs (solid green line), and the HTCs (solid orange line). Note that the ASTs are the main supplier of larger particles with comparatively longer lifetimes at northern/southern high latitudes.
Paper: Accretion of Meteoric Organic Matter at the Surface of Mars and Potential Production of Methane by Ultraviolet Radiation
Authors: Juan Diego Carrillo-Sánchez, John M. C. Plane, Diego Janches, Gerónimo L. Villanueva
Figure caption: Panels (a), (b), and (c): seasonal variability of the equivalent column concentration of the methane rates generated by UV-radiated surface carbon, in ppbv sol−1, assuming a UV photolysis yield of 20% and for the JFCs (a); the ASTs (b); and the total, JFCs + ASTs + HTCs (c), in terms of the Martian latitude and solar longitude. Note that seasonal variations of the methane rates of the HTCs are not displayed in this figure given its negligible contribution to the total flux. The methane rates are calculated assuming a chondritic carbon content of 5 wt%. Panel (d): annual average of the equivalent column concentration of methane assuming an average carbon content of 5 wt% for all meteoroid populations (solid black line). The blue shaded region in panel (d) represents the average methane production rate between a chondritic composition and a carbon content of 25.6 wt% for particles with a cometary origin (dashed black line). The contribution of each meteoroid population to the total accretion rates of carbon is also displayed in panel (d): the JFCs (solid blue line), the ASTs (solid green line), and the HTCs (solid orange line).
Paper: Accretion of Meteoric Organic Matter at the Surface of Mars and Potential Production of Methane by Ultraviolet Radiation
Authors: Juan Diego Carrillo-Sánchez, John M. C. Plane, Diego Janches, Gerónimo L. Villanueva
Figure caption: Panel (a): mass histograms of the accretion rate of carbon (dark blue) and sulfur (dark green), along with the methane production rates generated by surface carbon assuming a UV photolysis yield of 20% (light green) at L  s  = 251° (perihelion) for average carbon and sulfur contents of 5 wt% and 7 wt%, respectively. Panel (b): mass histograms of the mixing ratios of carbon in the top 200 μm assuming an average carbon content of 5 wt% (dark red) and 25.6 wt% (light blue) for cometary particles.
Paper: Accretion of Meteoric Organic Matter at the Surface of Mars and Potential Production of Methane by Ultraviolet Radiation
Authors: Juan Diego Carrillo-Sánchez, John M. C. Plane, Diego Janches, Gerónimo L. Villanueva
Figure caption: Seasonal variability of the equivalent column concentration of methane, in ppbv sol−1, generated by UV-radiated surface carbon assuming a UV photolysis yield of 20% and averaged over different latitudinal bands for the northern hemisphere (panel (a)) and the southern hemisphere (panel (b)). Note that the methane rates are calculated assuming a chondritic carbon content of 5 wt% for all meteoroid populations.
Paper: Lethal Surface Ozone Concentrations Are Possible on Habitable Zone Exoplanets
Authors: G. J. Cooke, D. R. Marsh, C. Walsh, F. Sainsbury-Martinez
Figure caption: The three stellar input spectra used for the WACCM6 simulations are the PC MUSCLES spectrum for Proxima Centauri at b (magenta) and the P19 (orange) and W21 (blue) spectra for TRAPPIST-1 at e. The top-of-atmosphere irradiance per unit wavelength is shown against the wavelength in nm. In the simulations, TRAPPIST-1 e receives 900 W m−2 of irradiation (0.66 S ⊕, where S ⊕ is the total insolation received by Earth), and Proxima Centauri b receives 884 W m−2 (0.65 S ⊕). The UV range is highlighted in gray between 100 and 400 nm, and the Lyα line is labeled. The average difference between the TRAPPIST-1 spectra in the UV range is a factor of 500, with a difference of up to 5000 in some wavelength bins.
Paper: Lethal Surface Ozone Concentrations Are Possible on Habitable Zone Exoplanets
Authors: G. J. Cooke, D. R. Marsh, C. Walsh, F. Sainsbury-Martinez
Figure caption: The surface mixing ratio of O3, in ppbv, is displayed for the simulations in this work that have time-averaged surface O3 mixing ratios exceeding 40 ppbv. This includes all TP-1 e P19 cases, the TP-1 e W21 1% PAL and 0.1% PAL simulations, and only a single Proxima Cenaturi b case (0.1% PAL). The PI cases start with an initial PI atmospheric composition. The PI case has the substellar point placed over the Pacific Ocean, the SPL case has it placed over Africa, and the noTL case is not tidally locked, so that the substellar point moves with time. PAL is the PAL of O2, which is a mixing ratio of 21% by volume. The TP-1 e P19 simulations have stronger incident ultraviolet radiation than the TP-1 e W21 simulations. See Table 1 for a more detailed description of the simulations. Gray indicates where the O3 mixing ratio is below 40 ppbv and thus at “safe” levels, while the different shades of yellow/orange/purple indicate places that exceed 40 ppbv, i.e., these concentrations are known to be harmful to life on Earth. The color map has a log scale that extends from 40 to 2120 ppbv.
Paper: Lethal Surface Ozone Concentrations Are Possible on Habitable Zone Exoplanets
Authors: G. J. Cooke, D. R. Marsh, C. Walsh, F. Sainsbury-Martinez
Figure caption: (a) Surface O3 mixing ratios are presented for the tidally locked P19 (orange) and W21 (blue) TP-1 e simulations, and the PCb simulations (magenta). All of these simulations have the substellar point placed over ocean. The circles show the mean mixing ratio, while the top bar shows the maximum and the bottom bar shows the minimum surface O3 mixing ratios. Also shown in black are the time-averaged O3 mixing ratios of data taken from Cooke et al. (2022). The horizontal axis indicates the simulations with a fixed O2 mixing ratio at the lower boundary, such that the horizontal ticks are categories rather than absolute values (the values are offset from each other for clarity). The gray dotted line indicates the 40 ppbv “harmful threshold,” above which O3 surface mixing ratios are considered dangerous to some forms of life on Earth. (b) The PI scenarios are compared in the TP-1 e simulations. These include the substellar point over ocean (PI), over land (PI SPL), and the nontidally locked cases (PI noTL).
Paper: Lethal Surface Ozone Concentrations Are Possible on Habitable Zone Exoplanets
Authors: G. J. Cooke, D. R. Marsh, C. Walsh, F. Sainsbury-Martinez
Figure caption: The tropospheric HOx/NOx column ratio is shown against the maximum and mean surface O3 mixing ratio in each tidally locked simulation in panels (a) and (b), respectively. The tropospheric NOx and HOx columns are shown against the mean O3 surface mixing ratio in panels (c) and (d), respectively. The gray vertical dotted lines show the 40 ppbv cutoff for harmful O3 levels. The tropospheric column is calculated as the column abundance of molecules between 120 hPa and the surface. Its units are molecules m−2. The circles indicate simulations where the substellar point is placed over ocean, and the crosses indicate simulations where it is placed over land.
Paper: Lethal Surface Ozone Concentrations Are Possible on Habitable Zone Exoplanets
Authors: G. J. Cooke, D. R. Marsh, C. Walsh, F. Sainsbury-Martinez
Figure caption: The dry deposition flux of O3, given in terms of kg m−2 s−1, is plotted for six simulations: the Earth PI simulation; the TRAPPIST-1 e P19 PI, SPL, and noTL simulations; and the W21 PI and 0.1% PAL simulations. Yellow indicates relatively large amounts of dry deposition, while red indicates relatively low amounts. The white areas indicate regions where the dry deposition flux of O3 is below 10−13 kg m−2 s−1.
Paper: Lethal Surface Ozone Concentrations Are Possible on Habitable Zone Exoplanets
Authors: G. J. Cooke, D. R. Marsh, C. Walsh, F. Sainsbury-Martinez
Figure caption: The surface temperature is displayed for the 12 TP-1 e simulations used in this work. The left column shows the P19 simulations, and the right column shows the W21 simulations. From top to bottom: PI, PI SPL, PI noTL, and the 0.1% PAL simulations are displayed. White arrows indicate the magnitude and direction of the surface winds. The magenta contours show surface temperatures of 273 K. The 10% PAL and 1% PAL simulations are not shown for brevity, but their surface temperatures are very similar to the PI and 0.1% PAL cases. For scale, a 10 m s−1 arrow is shown in the middle of the figure.
Paper: Lethal Surface Ozone Concentrations Are Possible on Habitable Zone Exoplanets
Authors: G. J. Cooke, D. R. Marsh, C. Walsh, F. Sainsbury-Martinez
Figure caption: The production of O from O2 photolysis (top row) and O3 photolysis (second row) is shown against pressure, with O3 production (third row) and O3 number density also shown (bottom row). All profiles are time-averaged global means. The TP-1 e PI, 10% PAL, 1% PAL, and 0.1% PAL simulations are shown for both the TP-1 e P19 (orange, brown, yellow, and red, respectively) and TP-1 e W21 (light blue, blue, lilac, and gray, respectively) stellar spectra in the left and middle columns, respectively. The right column show the PCb PI (indigo), 10% PAL (violet), 1% PAL (magenta), and 0.1% PAL (light pink) simulations.
Paper: Lethal Surface Ozone Concentrations Are Possible on Habitable Zone Exoplanets
Authors: G. J. Cooke, D. R. Marsh, C. Walsh, F. Sainsbury-Martinez
Figure caption: The surface temperature is displayed for the four PCb simulations used in this work: PCb PI (top left), PCb 10% PAL (top right), PCb 1% PAL (bottom left), and PCb 0.1% PAL (bottom right). White arrows indicate the magnitude and direction of the surface winds. The magenta contours show surface temperatures of 273 K. For scale, a 10 m s−1 arrow is shown in the middle of the figure.
Paper: Estimate of Water and Hydroxyl Abundance on Asteroid (16) Psyche from JWST Data
Authors: Stephanie G. Jarmak, Tracy M. Becker, Charles E. Woodward, Casey I. Honniball, Andrew S. Rivkin, Margaret M. McAdam, Zoe A. Landsman, Saverio Cambioni, Thomas G. Müller, Driss Takir, Kurt D. Retherford, Anicia Arredondo, Linda T. Elkins-Tanton
Figure caption: Relative normalized emission spectrum of asteroid (16) Psyche produced by dividing the MIRI channel 1 flux by a second-order polynomial masking the region 5.9–6.1 μm and beyond 6.33 μm for observation 1 (top) and observation 2 (bottom). The data are binned to a resolution of 20 nm.
Paper: Estimate of Water and Hydroxyl Abundance on Asteroid (16) Psyche from JWST Data
Authors: Stephanie G. Jarmak, Tracy M. Becker, Charles E. Woodward, Casey I. Honniball, Andrew S. Rivkin, Margaret M. McAdam, Zoe A. Landsman, Saverio Cambioni, Thomas G. Müller, Driss Takir, Kurt D. Retherford, Anicia Arredondo, Linda T. Elkins-Tanton
Figure caption: Relative normalized reflectance spectrum of Psyche near 4.8 μm. Top: observation 1. Bottom: observation 2. Binned spectra are binned to 20 nm.
Paper: Estimate of Water and Hydroxyl Abundance on Asteroid (16) Psyche from JWST Data
Authors: Stephanie G. Jarmak, Tracy M. Becker, Charles E. Woodward, Casey I. Honniball, Andrew S. Rivkin, Margaret M. McAdam, Zoe A. Landsman, Saverio Cambioni, Thomas G. Müller, Driss Takir, Kurt D. Retherford, Anicia Arredondo, Linda T. Elkins-Tanton
Figure caption: Relative normalized reflectance spectrum of Psyche near 2.67 μm. Top: observation 1. Bottom: observation 2. Binned spectra are binned to 1 nm.
Paper: Estimate of Water and Hydroxyl Abundance on Asteroid (16) Psyche from JWST Data
Authors: Stephanie G. Jarmak, Tracy M. Becker, Charles E. Woodward, Casey I. Honniball, Andrew S. Rivkin, Margaret M. McAdam, Zoe A. Landsman, Saverio Cambioni, Thomas G. Müller, Driss Takir, Kurt D. Retherford, Anicia Arredondo, Linda T. Elkins-Tanton
Figure caption: Relative normalized reflectance spectrum of Psyche near 1.59 μm. Binned spectra are binned to 10 nm.