adsabs/AstroCLIMB huggingface dataset:
Paper: Apophis Planetary Defense Campaign
Authors: Vishnu Reddy, Michael S. Kelley, Jessie Dotson, Davide Farnocchia, Nicolas Erasmus, David Polishook, Joseph Masiero, Lance A. M. Benner, James Bauer, Miguel R. Alarcon, David Balam, Daniel Bamberger, David Bell, Fabrizio Barnardi, Terry H. Bressi, Marina Brozovic, Melissa J. Brucker, Luca Buzzi, Juan Cano, David Cantillo, Ramona Cennamo, Serge Chastel, Omarov Chingis, Young-Jun Choi, Eric Christensen, Larry Denneau, Marek Dróżdż, Leonid Elenin, Orhan Erece, Laura Faggioli, Carmelo Falco, Dmitry Glamazda, Filippo Graziani, Aren N. Heinze, Matthew J. Holman, Alexander Ivanov, Cristovao Jacques, Petro Janse van Rensburg, Galina Kaiser, Krzysztof Kamiński, Monika K. Kamińska, Murat Kaplan, Dong-Heun Kim, Myung-Jin Kim, Csaba Kiss, Tatiana Kokina, Eduard Kuznetsov, Jeffrey A. Larsen, Hee-Jae Lee, Robert C. Lees, Julia de León, Javier Licandro, Amy Mainzer, Anna Marciniak, Michael Marsset, Ron A. Mastaler, Donovan L. Mathias, Robert S. McMillan, Hissa Medeiros, Marco Micheli, Artem Mokhnatkin, Hong-Kyu Moon, David Morate, Shantanu P. Naidu, Alessandro Nastasi, Artem Novichonok, Waldemar Ogłoza, András Pál, Fabricio Pérez-Toledo, Alexander Perminov, Elisabeta Petrescu, Marcel Popescu, Mike T. Read, Daniel E. Reichart, Inna Reva, Dong-Goo Roh, Clemens Rumpf, Akash Satpathy, Sergei Schmalz, James V. Scotti, Aleksander Serebryanskiy, Miquel Serra-Ricart, Eda Sonbas, Robert Szakáts, Patrick A. Taylor, John L. Tonry, Andrew F. Tubbiolo, Peter Veres, Richard Wainscoat, Elizabeth Warner, Henry J. Weiland, Guy Wells, Robert Weryk, Lorien F. Wheeler, Yulia Wiebe, Hong-Suh Yim, Michał Żejmo, Anastasiya Zhornichenko, Stanisław Zoła, Patrick Michel
Figure caption: The probability histogram (top) shows how the probability of the impact affecting different orders of magnitude of population evolves over the different epochs. For example, in epoch 3, there is a ∼50% chance of affecting between 106 and 107 people. The complementary cumulative distribution plot (bottom) shows how the probability that a certain population level or more will be affected in each epoch. For example, in epoch 3, there is a 5% chance that 107 or more people will be affected.
Paper: Apophis Planetary Defense Campaign
Authors: Vishnu Reddy, Michael S. Kelley, Jessie Dotson, Davide Farnocchia, Nicolas Erasmus, David Polishook, Joseph Masiero, Lance A. M. Benner, James Bauer, Miguel R. Alarcon, David Balam, Daniel Bamberger, David Bell, Fabrizio Barnardi, Terry H. Bressi, Marina Brozovic, Melissa J. Brucker, Luca Buzzi, Juan Cano, David Cantillo, Ramona Cennamo, Serge Chastel, Omarov Chingis, Young-Jun Choi, Eric Christensen, Larry Denneau, Marek Dróżdż, Leonid Elenin, Orhan Erece, Laura Faggioli, Carmelo Falco, Dmitry Glamazda, Filippo Graziani, Aren N. Heinze, Matthew J. Holman, Alexander Ivanov, Cristovao Jacques, Petro Janse van Rensburg, Galina Kaiser, Krzysztof Kamiński, Monika K. Kamińska, Murat Kaplan, Dong-Heun Kim, Myung-Jin Kim, Csaba Kiss, Tatiana Kokina, Eduard Kuznetsov, Jeffrey A. Larsen, Hee-Jae Lee, Robert C. Lees, Julia de León, Javier Licandro, Amy Mainzer, Anna Marciniak, Michael Marsset, Ron A. Mastaler, Donovan L. Mathias, Robert S. McMillan, Hissa Medeiros, Marco Micheli, Artem Mokhnatkin, Hong-Kyu Moon, David Morate, Shantanu P. Naidu, Alessandro Nastasi, Artem Novichonok, Waldemar Ogłoza, András Pál, Fabricio Pérez-Toledo, Alexander Perminov, Elisabeta Petrescu, Marcel Popescu, Mike T. Read, Daniel E. Reichart, Inna Reva, Dong-Goo Roh, Clemens Rumpf, Akash Satpathy, Sergei Schmalz, James V. Scotti, Aleksander Serebryanskiy, Miquel Serra-Ricart, Eda Sonbas, Robert Szakáts, Patrick A. Taylor, John L. Tonry, Andrew F. Tubbiolo, Peter Veres, Richard Wainscoat, Elizabeth Warner, Henry J. Weiland, Guy Wells, Robert Weryk, Lorien F. Wheeler, Yulia Wiebe, Hong-Suh Yim, Michał Żejmo, Anastasiya Zhornichenko, Stanisław Zoła, Patrick Michel
Figure caption: (A) The visible and near-IR reflectance spectrum of Apophis compared to spectra of average S-, C-, X-complex asteroids. Apophis’ spectrum resembles S types rather than C or X types. (B) Comparison of Apophis’ spectrum to S-complex taxonomic classes. The Apophis spectrum is similar to Sq types, indicating an affinity to LL-chondrite meteorites.
Paper: Apophis Planetary Defense Campaign
Authors: Vishnu Reddy, Michael S. Kelley, Jessie Dotson, Davide Farnocchia, Nicolas Erasmus, David Polishook, Joseph Masiero, Lance A. M. Benner, James Bauer, Miguel R. Alarcon, David Balam, Daniel Bamberger, David Bell, Fabrizio Barnardi, Terry H. Bressi, Marina Brozovic, Melissa J. Brucker, Luca Buzzi, Juan Cano, David Cantillo, Ramona Cennamo, Serge Chastel, Omarov Chingis, Young-Jun Choi, Eric Christensen, Larry Denneau, Marek Dróżdż, Leonid Elenin, Orhan Erece, Laura Faggioli, Carmelo Falco, Dmitry Glamazda, Filippo Graziani, Aren N. Heinze, Matthew J. Holman, Alexander Ivanov, Cristovao Jacques, Petro Janse van Rensburg, Galina Kaiser, Krzysztof Kamiński, Monika K. Kamińska, Murat Kaplan, Dong-Heun Kim, Myung-Jin Kim, Csaba Kiss, Tatiana Kokina, Eduard Kuznetsov, Jeffrey A. Larsen, Hee-Jae Lee, Robert C. Lees, Julia de León, Javier Licandro, Amy Mainzer, Anna Marciniak, Michael Marsset, Ron A. Mastaler, Donovan L. Mathias, Robert S. McMillan, Hissa Medeiros, Marco Micheli, Artem Mokhnatkin, Hong-Kyu Moon, David Morate, Shantanu P. Naidu, Alessandro Nastasi, Artem Novichonok, Waldemar Ogłoza, András Pál, Fabricio Pérez-Toledo, Alexander Perminov, Elisabeta Petrescu, Marcel Popescu, Mike T. Read, Daniel E. Reichart, Inna Reva, Dong-Goo Roh, Clemens Rumpf, Akash Satpathy, Sergei Schmalz, James V. Scotti, Aleksander Serebryanskiy, Miquel Serra-Ricart, Eda Sonbas, Robert Szakáts, Patrick A. Taylor, John L. Tonry, Andrew F. Tubbiolo, Peter Veres, Richard Wainscoat, Elizabeth Warner, Henry J. Weiland, Guy Wells, Robert Weryk, Lorien F. Wheeler, Yulia Wiebe, Hong-Suh Yim, Michał Żejmo, Anastasiya Zhornichenko, Stanisław Zoła, Patrick Michel
Figure caption: Opposite-circular echo power spectra from Apophis obtained on six days between March 3–10 using Goldstone to transmit and the Green Bank Telescope to receive. In each figure, echo power in standard deviations of the off-echo noise is plotted as a function of Doppler frequency. The resolution is 0.1 Hz, and each figure is shown at the same scale. Dates are indicated in each panel.
Paper: Apophis Planetary Defense Campaign
Authors: Vishnu Reddy, Michael S. Kelley, Jessie Dotson, Davide Farnocchia, Nicolas Erasmus, David Polishook, Joseph Masiero, Lance A. M. Benner, James Bauer, Miguel R. Alarcon, David Balam, Daniel Bamberger, David Bell, Fabrizio Barnardi, Terry H. Bressi, Marina Brozovic, Melissa J. Brucker, Luca Buzzi, Juan Cano, David Cantillo, Ramona Cennamo, Serge Chastel, Omarov Chingis, Young-Jun Choi, Eric Christensen, Larry Denneau, Marek Dróżdż, Leonid Elenin, Orhan Erece, Laura Faggioli, Carmelo Falco, Dmitry Glamazda, Filippo Graziani, Aren N. Heinze, Matthew J. Holman, Alexander Ivanov, Cristovao Jacques, Petro Janse van Rensburg, Galina Kaiser, Krzysztof Kamiński, Monika K. Kamińska, Murat Kaplan, Dong-Heun Kim, Myung-Jin Kim, Csaba Kiss, Tatiana Kokina, Eduard Kuznetsov, Jeffrey A. Larsen, Hee-Jae Lee, Robert C. Lees, Julia de León, Javier Licandro, Amy Mainzer, Anna Marciniak, Michael Marsset, Ron A. Mastaler, Donovan L. Mathias, Robert S. McMillan, Hissa Medeiros, Marco Micheli, Artem Mokhnatkin, Hong-Kyu Moon, David Morate, Shantanu P. Naidu, Alessandro Nastasi, Artem Novichonok, Waldemar Ogłoza, András Pál, Fabricio Pérez-Toledo, Alexander Perminov, Elisabeta Petrescu, Marcel Popescu, Mike T. Read, Daniel E. Reichart, Inna Reva, Dong-Goo Roh, Clemens Rumpf, Akash Satpathy, Sergei Schmalz, James V. Scotti, Aleksander Serebryanskiy, Miquel Serra-Ricart, Eda Sonbas, Robert Szakáts, Patrick A. Taylor, John L. Tonry, Andrew F. Tubbiolo, Peter Veres, Richard Wainscoat, Elizabeth Warner, Henry J. Weiland, Guy Wells, Robert Weryk, Lorien F. Wheeler, Yulia Wiebe, Hong-Suh Yim, Michał Żejmo, Anastasiya Zhornichenko, Stanisław Zoła, Patrick Michel
Figure caption: Collage of selected delay-Doppler images obtained on March 8, 9, and 10 using Goldstone to transmit and Green Bank to receive. In each image, time delay (range) increases downward and Doppler frequency increases to the right, so rotation is counterclockwise. Each row corresponds to 37.5 m (0.25 μs). The resolution in Doppler frequency is 0.1 Hz. Each image is an integration spanning about 1 hr and corresponds to about 12 degrees of rotation. The images are shown with the same dimensions in time delay and Doppler frequency.
Paper: Apophis Planetary Defense Campaign
Authors: Vishnu Reddy, Michael S. Kelley, Jessie Dotson, Davide Farnocchia, Nicolas Erasmus, David Polishook, Joseph Masiero, Lance A. M. Benner, James Bauer, Miguel R. Alarcon, David Balam, Daniel Bamberger, David Bell, Fabrizio Barnardi, Terry H. Bressi, Marina Brozovic, Melissa J. Brucker, Luca Buzzi, Juan Cano, David Cantillo, Ramona Cennamo, Serge Chastel, Omarov Chingis, Young-Jun Choi, Eric Christensen, Larry Denneau, Marek Dróżdż, Leonid Elenin, Orhan Erece, Laura Faggioli, Carmelo Falco, Dmitry Glamazda, Filippo Graziani, Aren N. Heinze, Matthew J. Holman, Alexander Ivanov, Cristovao Jacques, Petro Janse van Rensburg, Galina Kaiser, Krzysztof Kamiński, Monika K. Kamińska, Murat Kaplan, Dong-Heun Kim, Myung-Jin Kim, Csaba Kiss, Tatiana Kokina, Eduard Kuznetsov, Jeffrey A. Larsen, Hee-Jae Lee, Robert C. Lees, Julia de León, Javier Licandro, Amy Mainzer, Anna Marciniak, Michael Marsset, Ron A. Mastaler, Donovan L. Mathias, Robert S. McMillan, Hissa Medeiros, Marco Micheli, Artem Mokhnatkin, Hong-Kyu Moon, David Morate, Shantanu P. Naidu, Alessandro Nastasi, Artem Novichonok, Waldemar Ogłoza, András Pál, Fabricio Pérez-Toledo, Alexander Perminov, Elisabeta Petrescu, Marcel Popescu, Mike T. Read, Daniel E. Reichart, Inna Reva, Dong-Goo Roh, Clemens Rumpf, Akash Satpathy, Sergei Schmalz, James V. Scotti, Aleksander Serebryanskiy, Miquel Serra-Ricart, Eda Sonbas, Robert Szakáts, Patrick A. Taylor, John L. Tonry, Andrew F. Tubbiolo, Peter Veres, Richard Wainscoat, Elizabeth Warner, Henry J. Weiland, Guy Wells, Robert Weryk, Lorien F. Wheeler, Yulia Wiebe, Hong-Suh Yim, Michał Żejmo, Anastasiya Zhornichenko, Stanisław Zoła, Patrick Michel
Figure caption: Hypothetical impact swaths for epochs 0/1, 2, and 3. The impact swaths represent all possible considered impact positions and asteroid properties. A hypothetical impact would only occur at one position along the swath, but all possible positions are shown. The rings show the extent of different levels of damage for specific impact locations along the swath.
Paper: Apophis Planetary Defense Campaign
Authors: Vishnu Reddy, Michael S. Kelley, Jessie Dotson, Davide Farnocchia, Nicolas Erasmus, David Polishook, Joseph Masiero, Lance A. M. Benner, James Bauer, Miguel R. Alarcon, David Balam, Daniel Bamberger, David Bell, Fabrizio Barnardi, Terry H. Bressi, Marina Brozovic, Melissa J. Brucker, Luca Buzzi, Juan Cano, David Cantillo, Ramona Cennamo, Serge Chastel, Omarov Chingis, Young-Jun Choi, Eric Christensen, Larry Denneau, Marek Dróżdż, Leonid Elenin, Orhan Erece, Laura Faggioli, Carmelo Falco, Dmitry Glamazda, Filippo Graziani, Aren N. Heinze, Matthew J. Holman, Alexander Ivanov, Cristovao Jacques, Petro Janse van Rensburg, Galina Kaiser, Krzysztof Kamiński, Monika K. Kamińska, Murat Kaplan, Dong-Heun Kim, Myung-Jin Kim, Csaba Kiss, Tatiana Kokina, Eduard Kuznetsov, Jeffrey A. Larsen, Hee-Jae Lee, Robert C. Lees, Julia de León, Javier Licandro, Amy Mainzer, Anna Marciniak, Michael Marsset, Ron A. Mastaler, Donovan L. Mathias, Robert S. McMillan, Hissa Medeiros, Marco Micheli, Artem Mokhnatkin, Hong-Kyu Moon, David Morate, Shantanu P. Naidu, Alessandro Nastasi, Artem Novichonok, Waldemar Ogłoza, András Pál, Fabricio Pérez-Toledo, Alexander Perminov, Elisabeta Petrescu, Marcel Popescu, Mike T. Read, Daniel E. Reichart, Inna Reva, Dong-Goo Roh, Clemens Rumpf, Akash Satpathy, Sergei Schmalz, James V. Scotti, Aleksander Serebryanskiy, Miquel Serra-Ricart, Eda Sonbas, Robert Szakáts, Patrick A. Taylor, John L. Tonry, Andrew F. Tubbiolo, Peter Veres, Richard Wainscoat, Elizabeth Warner, Henry J. Weiland, Guy Wells, Robert Weryk, Lorien F. Wheeler, Yulia Wiebe, Hong-Suh Yim, Michał Żejmo, Anastasiya Zhornichenko, Stanisław Zoła, Patrick Michel
Figure caption: Daily number of observations from surveys and follow-up observers. The follow-up data on 2020 December 22 were collected by the NEO community at large when Apophis was on the NEOCP as N00hp15. For later dates, the count of follow-up data only refers to observations collected as part of the campaign.
Paper: T-matrix and Hapke Modeling of the Thermal Infrared Spectra of Trojan Asteroids and (944) Hidalgo: Implications for Their Regolith Particle Size and Porosity
Authors: Vanessa C. Lowry, Kerri L. Donaldson Hanna, Gen Ito, Michael S. P. Kelley, Humberto Campins, Sean Lindsay
Figure caption: The best-fit NEATM SED is shown in panels (a), (c), and (e) for the Trojan asteroids, and (944) Hidalgo is shown in panel (g). Panels (b), (d), (f), and (h) show the ∼7.5–13.5 μm portion of the emissivity spectrum used in the MSTM and Hapke modeling.
Paper: T-matrix and Hapke Modeling of the Thermal Infrared Spectra of Trojan Asteroids and (944) Hidalgo: Implications for Their Regolith Particle Size and Porosity
Authors: Vanessa C. Lowry, Kerri L. Donaldson Hanna, Gen Ito, Michael S. P. Kelley, Humberto Campins, Sean Lindsay
Figure caption: Forsterite complex indices of refraction n and k are shown in the top and middle panels. The Oxford laboratory forsterite spectrum is plotted in the bottom panel (Donaldson Hanna & Bowles 2020; solid curve). The modeled spectrum is plotted with weight contributions of (41.6%, 32.6%, 25.8%) for (A, B, C), respectively (bottom panel, dashed curve).
Paper: T-matrix and Hapke Modeling of the Thermal Infrared Spectra of Trojan Asteroids and (944) Hidalgo: Implications for Their Regolith Particle Size and Porosity
Authors: Vanessa C. Lowry, Kerri L. Donaldson Hanna, Gen Ito, Michael S. P. Kelley, Humberto Campins, Sean Lindsay
Figure caption: Fayalite complex indices of refraction n and k are shown in the top and middle panels. The ASU laboratory fayalite spectrum is shown in the bottom panel (Christensen et al. 2000; solid curve). The modeled spectrum (bottom panel, dashed curve) is plotted with weight contributions of (39.5%, 31.0%, 29.4%) for (A, B, C), respectively.
Paper: T-matrix and Hapke Modeling of the Thermal Infrared Spectra of Trojan Asteroids and (944) Hidalgo: Implications for Their Regolith Particle Size and Porosity
Authors: Vanessa C. Lowry, Kerri L. Donaldson Hanna, Gen Ito, Michael S. P. Kelley, Humberto Campins, Sean Lindsay
Figure caption: Emissivity spectra of Trojan asteroids (911) Agamemnon, (1172) Aneas, and (624) Hektor from Emery et al. (2006) and primitive asteroid (944) Hidalgo from Campins (2006) over the ∼7.5–37.5 μm region showcasing the prominent 10 μm plateau (emphasized in yellow) in each of the spectra.
Paper: Surface Conditions and Resource Accessibility at Potential Artemis Landing Sites 007 and 011
Authors: Nandita Kumari, Jordan M. Bretzfelder, Indujaa Ganesh, Antonio Lang, David A. Kring
Figure caption: (a) Average solar illumination map with PSR overlay at Site 007 surrounded by 2 km and 10 km EZs (yellow dashed lines). The red star in the middle is the highest average solar illumination point. (b) Average solar illumination percentage within 2km EZ and outside it (excluding 2 km EZ) in Site 007. (c) Average solar illumination within 2 km EZ of sites 001, 004, 007, and 011. The beginning and end of the blue box represents the 25th and 75th percentiles of the values, and the pink line in the middle represents the 50th percentile (median). The green lines (or black dots) at the top and bottom are the maximum and minimum. The presence of black dots indicates that those values are outliers and more than 1.5 times of the 25th or 75th percentiles. (d) Average solar illumination map with PSR overlay at Site 011 surrounded by 2 km and 10 km EZs. (e) Average solar illumination percentage within 2 km EZ and outside it (excluding 2 km EZ) in Site 011. (f) Average solar illumination within 10 km EZ of sites 001, 004, 007, and 011.
Paper: Surface Conditions and Resource Accessibility at Potential Artemis Landing Sites 007 and 011
Authors: Nandita Kumari, Jordan M. Bretzfelder, Indujaa Ganesh, Antonio Lang, David A. Kring
Figure caption: (a) Temperature map (at 11 a.m. local time) of Site 007 surrounded by 2 km and 10 km EZs. The red star in the middle is the highest average solar illumination point. (b) Temperature variation within the PSR in an unnamed crater in Site 007 over a lunar day–night cycle. (c) Temperature variation within 2 km EZ in Site 007 over a lunar day–night cycle. (d) Temperature variation outside 2 km EZ (within 10 km) in Site 007 over a lunar day–night cycle. (e) Temperature map (at 11 a.m. local time) of Site 011 surrounded by 2 km and 10 km EZs. The red star in the middle is the highest average solar illumination point. (f) Temperature variation within the two large PSRs in Site 011 over a lunar day–night cycle. (g) Temperature variation within 2 km EZ in Site 011 over a lunar day–night cycle. (h) Temperature variation outside 2 km EZ (within 10 km) in Site 011 over a lunar day–night cycle.
Paper: Surface Conditions and Resource Accessibility at Potential Artemis Landing Sites 007 and 011
Authors: Nandita Kumari, Jordan M. Bretzfelder, Indujaa Ganesh, Antonio Lang, David A. Kring
Figure caption: (a) Boulder locations (yellow) overlaid on NAC mosaic within Site 007. (b) Boulder density distribution (500 × 500 m) of Site 007 overlaid on average solar illumination map. (c) Comparison of boulder lengths in Site 007 with the South Ray crater. (d) Boulder locations (yellow) overlaid on NAC mosaic within Site 011. (e) Boulder density distribution (500 × 500 m) of Site 011 overlaid on average solar illumination map. (f) Comparison of boulder lengths in Site 011 with the South Ray crater.
Paper: Surface Conditions and Resource Accessibility at Potential Artemis Landing Sites 007 and 011
Authors: Nandita Kumari, Jordan M. Bretzfelder, Indujaa Ganesh, Antonio Lang, David A. Kring
Figure caption: LOLA digital elevation model (20 m px−1) overlaid on a LRO-NAC mosaic with the south pole (yellow star) and proposed landing sites identified in a NASA (2020) report (red stars), which are coincident with the points of highest illumination from Mazarico et al. (2011) marked. The “S” indicates the Shackleton crater, “Sl” indicates the Slater crater, “dG” indicates the de Gerlache crater, “H” indicates the Henson crater, and “Sv” indicates the Sverdup crater.
Paper: Surface Conditions and Resource Accessibility at Potential Artemis Landing Sites 007 and 011
Authors: Nandita Kumari, Jordan M. Bretzfelder, Indujaa Ganesh, Antonio Lang, David A. Kring
Figure caption: (a) Geological units in the south pole region of the Moon mapped by USGS Astrogeology Science Center et al. (2013). (b) Close view of Site 007 with pre-Nectarian material. (c) Close view of Site 011 with Eratosthenian, Nectarian, and pre-Nectarian material. The arrows indicate potential Orientale secondary impacts.
Paper: Surface Conditions and Resource Accessibility at Potential Artemis Landing Sites 007 and 011
Authors: Nandita Kumari, Jordan M. Bretzfelder, Indujaa Ganesh, Antonio Lang, David A. Kring
Figure caption: (a) LROC-NAC mosaic (∼1 m px−1) of Site 011. (b) LOLA DEM (∼20 m px−1) of Site 007 with contours of interval 500 m overlaid on it. (c) Slope map of Site 007 displaying nontraversable slopes in red color overlaid on average solar illumination map.
Paper: Surface Conditions and Resource Accessibility at Potential Artemis Landing Sites 007 and 011
Authors: Nandita Kumari, Jordan M. Bretzfelder, Indujaa Ganesh, Antonio Lang, David A. Kring
Figure caption: (a) Current ice terrain thickness in Site 007. (b) Ice favorability index of different locations within Site 007. (c) Current ice terrain thickness in Site 011. (d) Ice favorability index of different locations within Site 011 (Cannon & Britt 2020).
Paper: Surface Conditions and Resource Accessibility at Potential Artemis Landing Sites 007 and 011
Authors: Nandita Kumari, Jordan M. Bretzfelder, Indujaa Ganesh, Antonio Lang, David A. Kring
Figure caption: (a) LROC-NAC mosaic (∼1 m px−1) of Site 007 with unnamed crater. (b) LOLA DEM (∼20 m px−1) of Site 007 with contours of interval 500 m overlaid on it. (c) Slope map of Site 007 (displaying nontraversable slopes in red) overlaid on average solar illumination map.
Paper: Putative Methanogenic Biosphere in Enceladus's Deep Ocean: Biomass, Productivity, and Implications for Detection
Authors: Antonin Affholder, François Guyot, Boris Sauterey, Régis Ferrière, Stéphane Mazevet
Figure caption: (a) Posterior confidence in biotic glycine production as a function of the observed glycine concentration in the ocean plume and the prior confidence in the existence of methanogens. The map is drawn only for glycine concentration values that fall in the 95% confidence interval of the total model (abiotic or abiotic+biotic). The prior probability of methanogenesis is here bounded by the prior probability of habitability (Section 2.5.1), hence the plot stopping at ≈0.4. (b) Posterior (or methane-informed) confidence in biotic glycine production as a function of the observed glycine concentration and the prior confidence in the existence of methanogens using information from methane concentration in the plume. The black triangle denotes the average posterior probability of methanogenesis in Figure 3 of Affholder et al. (2021). This value highlights that a uniform prior distribution for P(B∣H) implies an average value of E(P(B)) ≈ 0.59. In Affholder et al. (2021), the posterior probability of methanogenesis can reach unity (if the conditional probability of life emergence is also unity); therefore, the methane-informed case considers probability of methanogenesis up to 1.
Paper: Putative Methanogenic Biosphere in Enceladus's Deep Ocean: Biomass, Productivity, and Implications for Detection
Authors: Antonin Affholder, François Guyot, Boris Sauterey, Régis Ferrière, Stéphane Mazevet
Figure caption: Required sample volume to capture at least one cell with 95% confidence as a function of the concentration factor. The concentration factor corresponds to a multiplicative term that either lowers (concentration factor <1) cell concentration in the space plume relative to the initial ocean plume (e.g., plume dilution, cell destruction) or concentrates (concentration factor >1) cells in the space plume relative to the initial ocean plume (e.g., bubble scrubbing). The dashed line corresponds to the required sample volume to get at least 1 cell with 95% probability assuming a cell density equal to the mean of the 10% simulations with the lower cell density. The solid (dotted) line represents this minimal sample volume assuming the prior (posterior) integrated probability density for the dead cell density in the plume. HF-to-seawater ratios lower than 1:10 are shaded gray, as they are deemed unlikely in Porco et al. (2017) and Steel et al. (2017). The horizontal red line denotes the sample volume collected from a 50 km altitude flight through the plume on a 0.04 m2 collector plate as estimated in Porco et al. (2017). The blue line represents the required sample size proposed for the Orbilander microscope (Exhibit B-6 in MacKenzie et al. 2021). The magenta line denotes the total sample volume for the Orbilander concept (MacKenzie et al. 2021).