adsabs/AstroCLIMB huggingface dataset:
Paper: VaTEST. II. Statistical Validation of 11 TESS-detected Exoplanets Orbiting K-type Stars
Authors: Priyashkumar Mistry, Kamlesh Pathak, Aniket Prasad, Georgios Lekkas, Surendra Bhattarai, Sarvesh Gharat, Mousam Maity, Dhruv Kumar, Karen A. Collins, Richard P. Schwarz, Christopher R. Mann, Elise Furlan, Steve B. Howell, David Ciardi, Allyson Bieryla, Elisabeth C. Matthews, Erica Gonzales, Carl Ziegler, Ian Crossfield, Steven Giacalone, Thiam-Guan Tan, Phil Evans, Krzysztof G. Hełminiak, Kevin I. Collins, Norio Narita, Akihiko Fukui, Francisco J. Pozuelos, Courtney Dressing, Abderahmane Soubkiou, Zouhair Benkhaldoun, Joshua E. Schlieder, Olga Suarez, Khalid Barkaoui, Enric Palle, Felipe Murgas, Gregor Srdoc, Maria V. Goliguzova, Ivan A. Strakhov, Crystal Gnilka, Kathryn Lester, Colin Littlefield, Nic Scott, Rachel Matson, Michaël Gillon, Emmanuel Jehin, Mathilde Timmermans, Mourad Ghachoui, Lyu Abe, Philippe Bendjoya, Tristan Guillot, Amaury H. M. J. Triaud
Figure caption: Phase-folded light curves of newly validated planetary systems. The black line shows the best-fit model, blue dots are binned observations.
Paper: VaTEST. II. Statistical Validation of 11 TESS-detected Exoplanets Orbiting K-type Stars
Authors: Priyashkumar Mistry, Kamlesh Pathak, Aniket Prasad, Georgios Lekkas, Surendra Bhattarai, Sarvesh Gharat, Mousam Maity, Dhruv Kumar, Karen A. Collins, Richard P. Schwarz, Christopher R. Mann, Elise Furlan, Steve B. Howell, David Ciardi, Allyson Bieryla, Elisabeth C. Matthews, Erica Gonzales, Carl Ziegler, Ian Crossfield, Steven Giacalone, Thiam-Guan Tan, Phil Evans, Krzysztof G. Hełminiak, Kevin I. Collins, Norio Narita, Akihiko Fukui, Francisco J. Pozuelos, Courtney Dressing, Abderahmane Soubkiou, Zouhair Benkhaldoun, Joshua E. Schlieder, Olga Suarez, Khalid Barkaoui, Enric Palle, Felipe Murgas, Gregor Srdoc, Maria V. Goliguzova, Ivan A. Strakhov, Crystal Gnilka, Kathryn Lester, Colin Littlefield, Nic Scott, Rachel Matson, Michaël Gillon, Emmanuel Jehin, Mathilde Timmermans, Mourad Ghachoui, Lyu Abe, Philippe Bendjoya, Tristan Guillot, Amaury H. M. J. Triaud
Figure caption: TOI-672 Sector-09 background flux at the time of first two transits. No spikes are observed at the time of transit.
Paper: VaTEST. II. Statistical Validation of 11 TESS-detected Exoplanets Orbiting K-type Stars
Authors: Priyashkumar Mistry, Kamlesh Pathak, Aniket Prasad, Georgios Lekkas, Surendra Bhattarai, Sarvesh Gharat, Mousam Maity, Dhruv Kumar, Karen A. Collins, Richard P. Schwarz, Christopher R. Mann, Elise Furlan, Steve B. Howell, David Ciardi, Allyson Bieryla, Elisabeth C. Matthews, Erica Gonzales, Carl Ziegler, Ian Crossfield, Steven Giacalone, Thiam-Guan Tan, Phil Evans, Krzysztof G. Hełminiak, Kevin I. Collins, Norio Narita, Akihiko Fukui, Francisco J. Pozuelos, Courtney Dressing, Abderahmane Soubkiou, Zouhair Benkhaldoun, Joshua E. Schlieder, Olga Suarez, Khalid Barkaoui, Enric Palle, Felipe Murgas, Gregor Srdoc, Maria V. Goliguzova, Ivan A. Strakhov, Crystal Gnilka, Kathryn Lester, Colin Littlefield, Nic Scott, Rachel Matson, Michaël Gillon, Emmanuel Jehin, Mathilde Timmermans, Mourad Ghachoui, Lyu Abe, Philippe Bendjoya, Tristan Guillot, Amaury H. M. J. Triaud
Figure caption: Centroid raw and column position at transit events.
Paper: The Hazardous km-sized NEOs of the Next Thousands of Years
Authors: Oscar Fuentes-Muñoz, Daniel J. Scheeres, Davide Farnocchia, Ryan S. Park
Figure caption: Numerical propagation of the orbit of 2015 FP332, a km-sized NEO. The trajectories are shown using the Keplerian elements semimajor axis, eccentricity, inclination, longitude of the ascending node, argument of perihelion and mean anomaly with respect to the nominal propagation. Individual Monte Carlo runs (N = 21) are shown in colors, the nominal trajectory is shown in a black line. The bottom rows show the propagation of Earth and Venus MOID.
Paper: The Hazardous km-sized NEOs of the Next Thousands of Years
Authors: Oscar Fuentes-Muñoz, Daniel J. Scheeres, Davide Farnocchia, Ryan S. Park
Figure caption: Propagation of the Earth MOID of km-sized NEOs with a nonzero probability of having an encounter closer than 1 LD by year 3000. Individual Monte Carlo runs are shown in colors, where the black continuous line shows the nominal trajectory. The dashed red line indicates the first date in which the standard deviation in mean anomaly was found greater than 10°. Close encounters are indicated with circles in colors and close encounters of the nominal trajectory are shown as vertical black nodes. Encounters of closest approach distance <1LD (0.0026 au) are highlighted with a larger red circle.
Paper: The Hazardous km-sized NEOs of the Next Thousands of Years
Authors: Oscar Fuentes-Muñoz, Daniel J. Scheeres, Davide Farnocchia, Ryan S. Park
Figure caption: Propagation of the Earth MOID of a few selected examples of km-sized near-Earth objects. For each asteroid we show the 21 Monte Carlo simulations (colors) and the nominal orbit propagation (black, continuous). The orbit elements in the figure indicate the initial conditions of the propagation.
Paper: The Hazardous km-sized NEOs of the Next Thousands of Years
Authors: Oscar Fuentes-Muñoz, Daniel J. Scheeres, Davide Farnocchia, Ryan S. Park
Figure caption: Propagation of the Earth MOID of km-sized NEOs with a low-MOID for a large fraction of the next 1000 yr, as shown in Table 1. Individual Monte Carlo runs are shown in colors, black continuous line shows the nominal trajectory. The dashed red line indicates the first date in which the standard deviation in mean anomaly was found greater than 10°, which does not happen for 68950 (2002 QF15).
Paper: The Hazardous km-sized NEOs of the Next Thousands of Years
Authors: Oscar Fuentes-Muñoz, Daniel J. Scheeres, Davide Farnocchia, Ryan S. Park
Figure caption: Km-sized NEOs that meet the MOID < 0.01 au condition in the next 1000 yr. Color code indicates the number of Monte Carlo samples that show a MOID < 0.01 au at the given date. Black means an agreement between all Monte Carlo runs to show a low-MOID. The NEOs are sorted by the first date in which they meet the MOID < 0.01 au condition.
Paper: The Hazardous km-sized NEOs of the Next Thousands of Years
Authors: Oscar Fuentes-Muñoz, Daniel J. Scheeres, Davide Farnocchia, Ryan S. Park
Figure caption: Km-sized NEOs with nonzero estimated probability of encounters closer than 1 LD. Color code indicates the standard deviation in mean anomaly, S(MA), in log10. S(MA) is shown only in dates in which the MOID is lower than 0.01 au.
Paper: The Hazardous km-sized NEOs of the Next Thousands of Years
Authors: Oscar Fuentes-Muñoz, Daniel J. Scheeres, Davide Farnocchia, Ryan S. Park
Figure caption: Number of km-sized NEOs that present a low-MOID throughout the next 1000 yr. defined as an Earth MOID <0.01 au. Minimum number of NEOs is estimated by NEOs in which there was an agreement between all Monte Carlo runs. Maximum number of NEOs is estimated by at least one Monte Carlo run fulfilling the low-MOID condition.
Paper: The Hazardous km-sized NEOs of the Next Thousands of Years
Authors: Oscar Fuentes-Muñoz, Daniel J. Scheeres, Davide Farnocchia, Ryan S. Park
Figure caption: Numerical propagation of the orbit of 66391 Moshup (1999 KW4), a km-sized NEO. The trajectories are shown using the Keplerian elements semimajor axis, eccentricity, inclination, longitude of the ascending node, argument of perihelion, and mean anomaly with respect to the nominal propagation. Individual Monte Carlo runs (N = 21) are shown in colors, the nominal trajectory is shown in a continuous black line.
Paper: The Hazardous km-sized NEOs of the Next Thousands of Years
Authors: Oscar Fuentes-Muñoz, Daniel J. Scheeres, Davide Farnocchia, Ryan S. Park
Figure caption: Earth close encounters of 66391 Moshup (1999 KW4), bounded by the osculating Earth MOID and as obtained through numerical Monte Carlo analysis. Close encounters are highlighted with vertical lines and points, and the Earth MOID is shown in continuous lines. Individual Monte Carlo runs are shown in colors, black continuous line shows the nominal trajectory. Encounters of closest approach distance <1LD (0.0026 au) are highlighted with a larger red circle.
Paper: The Hazardous km-sized NEOs of the Next Thousands of Years
Authors: Oscar Fuentes-Muñoz, Daniel J. Scheeres, Davide Farnocchia, Ryan S. Park
Figure caption: Earth close encounters of 7482 (1994 PC1), bounded by the osculating Earth MOID and as obtained through numerical Monte Carlo analysis. Close encounters are highlighted with vertical lines and points, and the Earth MOID is shown in continuous lines. Individual Monte Carlo runs are shown in colors, black continuous line shows the nominal trajectory. Encounters of closest approach distance <1LD (0.0026 au) are highlighted with a larger red circle.
Paper: The Hazardous km-sized NEOs of the Next Thousands of Years
Authors: Oscar Fuentes-Muñoz, Daniel J. Scheeres, Davide Farnocchia, Ryan S. Park
Figure caption: Numerical propagation of the orbit of 143651 (2003 QO104), a km-sized NEO. The trajectories are shown using the Keplerian elements semimajor axis, eccentricity, inclination, longitude of the ascending node, argument of perihelion, and mean anomaly with respect to the nominal propagation. Individual Monte Carlo runs (N = 21) are shown in colors, the nominal trajectory is shown in a continuous black line.
Paper: The Hazardous km-sized NEOs of the Next Thousands of Years
Authors: Oscar Fuentes-Muñoz, Daniel J. Scheeres, Davide Farnocchia, Ryan S. Park
Figure caption: Numerical propagation of the orbit of 7482 (1994 PC1), a km-sized NEO. The trajectories are shown using the Keplerian elements semimajor axis, eccentricity, inclination, longitude of the ascending node, argument of perihelion, and mean anomaly with respect to the nominal propagation. Individual Monte Carlo runs (N = 21) are shown in colors, the nominal trajectory is shown in a continuous black line.
Paper: The Hazardous km-sized NEOs of the Next Thousands of Years
Authors: Oscar Fuentes-Muñoz, Daniel J. Scheeres, Davide Farnocchia, Ryan S. Park
Figure caption: Numerical propagation of the orbit of 29075 (1950 AD), a km-sized NEO. The trajectories are shown using the Keplerian elements semimajor axis, eccentricity, inclination, longitude of the ascending node, argument of perihelion, and mean anomaly with respect to the nominal propagation. Individual Monte Carlo runs (N = 21) are shown in colors, the nominal trajectory is shown in a continuous black line.
Paper: The Hazardous km-sized NEOs of the Next Thousands of Years
Authors: Oscar Fuentes-Muñoz, Daniel J. Scheeres, Davide Farnocchia, Ryan S. Park
Figure caption: Earth close encounters of 29075 (1950 AD), bounded by the osculating Earth MOID and as obtained through numerical Monte Carlo analysis. Close encounters are highlighted with vertical lines and points, and the Earth MOID is shown in continuous lines. Individual Monte Carlo runs are shown in colors, black continuous line shows the nominal trajectory.
Paper: The Hazardous km-sized NEOs of the Next Thousands of Years
Authors: Oscar Fuentes-Muñoz, Daniel J. Scheeres, Davide Farnocchia, Ryan S. Park
Figure caption: Earth close encounters of 143651 (2003 QO104), bounded by the osculating Earth MOID and as obtained through numerical Monte Carlo analysis. Close encounters are highlighted with vertical lines and points, and the Earth MOID is shown in continuous lines. Individual Monte Carlo runs are shown in colors, black continuous line shows the nominal trajectory.
Paper: The Hazardous km-sized NEOs of the Next Thousands of Years
Authors: Oscar Fuentes-Muñoz, Daniel J. Scheeres, Davide Farnocchia, Ryan S. Park
Figure caption: Earth close encounters of 2022 AP7, bounded by the osculating Earth MOID and as obtained through numerical Monte Carlo analysis. Close encounters are highlighted with vertical lines and points, and the Earth MOID is shown in continuous lines. Individual Monte Carlo runs are shown in colors, black continuous line shows the nominal trajectory.
Paper: The Hazardous km-sized NEOs of the Next Thousands of Years
Authors: Oscar Fuentes-Muñoz, Daniel J. Scheeres, Davide Farnocchia, Ryan S. Park
Figure caption: Numerical propagation of the orbit of 2022 AP7, a km-sized NEO. The trajectories are shown using the Keplerian elements semimajor axis, eccentricity, inclination, longitude of the ascending node, argument of perihelion, and mean anomaly with respect to the nominal propagation. Individual Monte Carlo runs (N = 21) are shown in colors, the nominal trajectory is shown in a continuous black line.
Paper: Keck Planet Imager and Characterizer Emission Spectroscopy of WASP-33b
Authors: Luke Finnerty, Tobias Schofield, Ben Sappey, Jerry W. Xuan, Jean-Baptiste Ruffio, Jason J. Wang, Jacques-Robert Delorme, Geoffrey A. Blake, Cam Buzard, Michael P. Fitzgerald, Ashley Baker, Randall Bartos, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Greg Doppmann, Daniel Echeverri, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Caprice L. Phillips, Sam Ragland, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Ji Wang, 吉 王, Peter Wizinowich
Figure caption: Retrieved PT profile (top left), K-band emission contribution (top right), and spectrum (bottom) for the best-fit atmospheric parameters. The weighted mean of all PT profiles is plotted as a solid green line, with the 1σ range shaded. The PT profile from the maximum-likelihood parameters is plotted as a dashed blue line and generally agrees well, though with a somewhat shallower and higher inversion. The condensation curves for solid iron and liquid iron from Ackerman & Marley (2001) are overplotted, though we do not expect dayside clouds. In the right panel, the contribution of each pressure layer to the overall planet emission with the best-fit abundances and median PT profile is indicated by the shading, with the observed NIRSPEC orders overplotted in gray. The observed emission emerges primarily from the 1-0.1 bar range. The CO line cores beyond ∼2.3 μm include significant contributions from the upper atmosphere. The bottom panel shows the spectrum obtained from the median parameters convolved to the approximate resolution of NIRSPEC, again with the NIRSPEC orders overplotted in gray.
Paper: Keck Planet Imager and Characterizer Emission Spectroscopy of WASP-33b
Authors: Luke Finnerty, Tobias Schofield, Ben Sappey, Jerry W. Xuan, Jean-Baptiste Ruffio, Jason J. Wang, Jacques-Robert Delorme, Geoffrey A. Blake, Cam Buzard, Michael P. Fitzgerald, Ashley Baker, Randall Bartos, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Greg Doppmann, Daniel Echeverri, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Caprice L. Phillips, Sam Ragland, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Ji Wang, 吉 王, Peter Wizinowich
Figure caption: Comparisons between retrieved CO and H2O abundances and abundances interpolated from the poor_mans_nonequ_chem functionality of petitRADTRANS (Mollière et al. 2017, 2019) using the median retrieved PT profile. The shaded pressure layers indicate the region to which our observations are most sensitive based on the emission contribution function in Figure 7. We compare the retrieved OH abundance to the equilibrium prediction for H2O. These comparisons show the CO abundance is largely insensitive to the C/O ratio, while the H2O abundance is set by both the metallicity and C/O ratio. Our results are most consistent with C/O = 0.8 ± 0.1 and [Fe/H] = 1.2 ± 1, with significant uncertainty in metallicity due to the lack of continuum information. These models predict large SiO abundances, which may be detectable in L-band observations.
Paper: Keck Planet Imager and Characterizer Emission Spectroscopy of WASP-33b
Authors: Luke Finnerty, Tobias Schofield, Ben Sappey, Jerry W. Xuan, Jean-Baptiste Ruffio, Jason J. Wang, Jacques-Robert Delorme, Geoffrey A. Blake, Cam Buzard, Michael P. Fitzgerald, Ashley Baker, Randall Bartos, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Greg Doppmann, Daniel Echeverri, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Caprice L. Phillips, Sam Ragland, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Ji Wang, 吉 王, Peter Wizinowich
Figure caption: Retrieved C/O, C/H, and O/H number ratio posteriors. The C/O ratio is better constrained than the individual C/H and O/H ratios, consistent with our expectation that high-resolution spectroscopy over a narrow band is more sensitive to abundance ratios than absolute abundances due to the loss of continuum information during the data processing. The prior that the total mass fraction of all species be <1 can be seen in the absence of points to the upper left of the 2D plots, where low C/O ratio and high C abundances would require more than the entire remaining atmospheric mass in the form of H2O.
Paper: Keck Planet Imager and Characterizer Emission Spectroscopy of WASP-33b
Authors: Luke Finnerty, Tobias Schofield, Ben Sappey, Jerry W. Xuan, Jean-Baptiste Ruffio, Jason J. Wang, Jacques-Robert Delorme, Geoffrey A. Blake, Cam Buzard, Michael P. Fitzgerald, Ashley Baker, Randall Bartos, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Greg Doppmann, Daniel Echeverri, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Caprice L. Phillips, Sam Ragland, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Ji Wang, 吉 王, Peter Wizinowich
Figure caption: Full corner plot for the test retrieval with no planet. Columns from left to right are the parameters as listed in Table 3. Red solid lines indicate the dynesty median, and red dashed lines indicate the bounds of the marginalized 68% confidence interval. Despite using the same stopping criteria as the other retrievals, none of the posteriors show strong preferences, and the fitter converged in far fewer iterations than when the planet is present in the simulation. The scale parameter shows a weak preference toward smaller values, consistent with the known absence of a planet in the simulated data. The impact of the T < 6000 K at all pressure levels requirement can be seen in the behavior of the pressure–temperature profile parameters in the first six columns.
Paper: Keck Planet Imager and Characterizer Emission Spectroscopy of WASP-33b
Authors: Luke Finnerty, Tobias Schofield, Ben Sappey, Jerry W. Xuan, Jean-Baptiste Ruffio, Jason J. Wang, Jacques-Robert Delorme, Geoffrey A. Blake, Cam Buzard, Michael P. Fitzgerald, Ashley Baker, Randall Bartos, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Greg Doppmann, Daniel Echeverri, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Caprice L. Phillips, Sam Ragland, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Ji Wang, 吉 王, Peter Wizinowich
Figure caption: Full corner plot for the test retrieval based on the parameters in Table 4. Columns from left to right are the parameters as listed in Table 3. Red solid lines indicate the dynesty median, and red dashed lines indicate the bounds of the marginalized 68% confidence interval. True values for the simulated data are shown as the solid blue line. The true values are generally retrieved to within 1σ.
Paper: Keck Planet Imager and Characterizer Emission Spectroscopy of WASP-33b
Authors: Luke Finnerty, Tobias Schofield, Ben Sappey, Jerry W. Xuan, Jean-Baptiste Ruffio, Jason J. Wang, Jacques-Robert Delorme, Geoffrey A. Blake, Cam Buzard, Michael P. Fitzgerald, Ashley Baker, Randall Bartos, Charlotte Z. Bond, Benjamin Calvin, Sylvain Cetre, Greg Doppmann, Daniel Echeverri, Nemanja Jovanovic, Joshua Liberman, Ronald A. López, Emily C. Martin, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Caprice L. Phillips, Sam Ragland, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Nicole L. Wallack, Ji Wang, 吉 王, Peter Wizinowich
Figure caption: Full corner plot for the WASP-33b retrieval. Columns from left to right are the parameters as listed in Table 3. Red solid lines indicate the dynesty median, and red dashed lines indicate the bounds of the marginalized 68% confidence interval. We discuss these results in Section 4.
Paper: Prebiosignature Molecules Can Be Detected in Temperate Exoplanet Atmospheres with JWST
Authors: A. B. Claringbold, P. B. Rimmer, S. Rugheimer, O. Shorttle
Figure caption: Detection thresholds of prebiosignature molecules at different wavelengths for different model exoplanets. JWST noise is simulated using three transits per instrument of GJ 1132b at spectral resolution R = 100. Post-impact (1) refers to the 100 kyr post-impact case and post-impact (2) refers to the 10 Myr post-impact case.
Paper: Prebiosignature Molecules Can Be Detected in Temperate Exoplanet Atmospheres with JWST
Authors: A. B. Claringbold, P. B. Rimmer, S. Rugheimer, O. Shorttle
Figure caption: Full posterior distribution from the petitRADTRANS retrieval of a simulated NIRSpec G395M observation of a Hycean atmosphere with TriArc-calculated detection threshold abundances of three prebiosignatures (HCN, C2H2, and SO2) assuming realistic JWST noise from observing three transits of GJ 1132b. The prebiosignature mass fractions are identified within 2σ of their true values (HCN = −2.78, C2H2 = −3.92, SO2 = −4.1). Due to the overlapping strongest features of HCN, C2H2, and NH3, there is a tail in the posterior PDF of both HCN and C2H2 as the interpretation for the shared feature at 3 μm is somewhat degenerate.
Paper: Prebiosignature Molecules Can Be Detected in Temperate Exoplanet Atmospheres with JWST
Authors: A. B. Claringbold, P. B. Rimmer, S. Rugheimer, O. Shorttle
Figure caption: Full posterior distribution from the petitRADTRANS retrieval of a simulated NIRSpec G395M observation of a Hycean atmosphere with 5 times the TriArc-calculated detection threshold abundances of three prebiosignatures (HCN, C2H2, and SO2) assuming realistic JWST noise from observing three transits of GJ 1132b. The prebiosignature mass fractions are identified within 1–2σ of their true values (HCN = −2.28, C2H2 = −3.42, SO2 = −3.6). With the increased abundances all three prebiosignatures are robustly detected and distinguished, demonstrating the order-of-magnitude accuracy of the detection threshold method.
Paper: Prebiosignature Molecules Can Be Detected in Temperate Exoplanet Atmospheres with JWST
Authors: A. B. Claringbold, P. B. Rimmer, S. Rugheimer, O. Shorttle
Figure caption: Detection thresholds of HCN as a function of the number of transits for a selection of model stars, using simulated transmission spectra of a model Hycean exoplanet at spectral resolution R = 100.
Paper: Prebiosignature Molecules Can Be Detected in Temperate Exoplanet Atmospheres with JWST
Authors: A. B. Claringbold, P. B. Rimmer, S. Rugheimer, O. Shorttle
Figure caption: Detection thresholds of prebiosignature molecules as a function of the number of transits using simulated transmission spectra of TRAPPIST-1e with an early-Earth atmosphere at spectral resolution R = 100.
Paper: Prebiosignature Molecules Can Be Detected in Temperate Exoplanet Atmospheres with JWST
Authors: A. B. Claringbold, P. B. Rimmer, S. Rugheimer, O. Shorttle
Figure caption: Simulated transmission spectra of a Hycean planet with added abundances of SO2 above the detection threshold (3 ppm, top left) and below the detection threshold (0.5 ppm, top right), and the SO2 mass fraction posterior PDF from detection tests (bottom). The spectral feature at 4 μm is targeted by the detection test. The spectra are presented with and without simulated JWST noise, which is used for the detection test. The 1% input, above which the posterior PDF is integrated to calculate the significance of detection, is highlighted with a dotted line in the detection test.