adsabs/AstroCLIMB huggingface dataset:
Paper: Polycyclic Aromatic Hydrocarbon Emission in the Central Regions of Three Seyferts and the Implication for Underlying Feedback Mechanisms
Authors: Lulu Zhang, Ismael García-Bernete, Chris Packham, Fergus R. Donnan, Dimitra Rigopoulou, Erin K. S. Hicks, Ric I. Davies, Taro T. Shimizu, Almudena Alonso-Herrero, Cristina Ramos Almeida, Miguel Pereira-Santaella, Claudio Ricci, Andrew J. Bunker, Mason T. Leist, David J. Rosario, Santiago García-Burillo, Laura Hermosa Muñoz, Francoise Combes, Masatoshi Imanishi, Alvaro Labiano, Donaji Esparza-Arredondo, Enrica Bellocchi, Anelise Audibert, Lindsay Fuller, Omaira González-Martín, Sebastian Hönig, Takuma Izumi, Nancy A. Levenson, Enrique López-Rodríguez, Daniel Rouan, Marko Stalevski, Martin J. Ward
Figure caption: The same as Figure 2 but for all apertures studied here.
Paper: The Large-scale Anisotropy and Flux (de)magnification of Ultrahigh-energy Cosmic Rays in the Galactic Magnetic Field
Authors: Teresa Bister, Glennys R. Farrar, Michael Unger
Figure caption: Predicted and measured dipole directions in Galactic coordinates: colored markers indicate the dipole directions for different coherent GMF models and two realizations of the random field with l  c  = 60 pc (duplicate heavy symbols) and one with l  c  = 30 pc (light symbols). The blue region shows the 1σ uncertainty due to cosmic variance in the source positions, for the base model with l  c  = 60 pc and n  s  = 10−3 Mpc−3. The black contours represent the 1σ and 2σ uncertainty domains of the measured dipole (G. Golup 2023).
Paper: The Large-scale Anisotropy and Flux (de)magnification of Ultrahigh-energy Cosmic Rays in the Galactic Magnetic Field
Authors: Teresa Bister, Glennys R. Farrar, Michael Unger
Figure caption: Number of random realizations of source locations, out of 10,000 total for each n  s , for which the predicted dipole direction (left) or the dipole direction, dipole amplitude, and quadrupole amplitude all simultaneously (right) lie within the measured 2σ uncertainty in all of the the mutually exclusive energy bins (E = (8−16)EeV, E = (16−32)EeV, and E > 32 EeV). Different GMF models are shown with different markers; their thickness indicates the random field coherence length, as in Figure 1. Duplicate markers denote two realizations of the turbulent field for the same coherent field. The markers for each value of n  s /Mpc−3 = 10−6, 10−5,...,10−2 are offset on the x-axis for better visibility. The gray region (left) marks the range of n  s  satisfying the dipole and quadrupole amplitudes discussed in the main text. For comparison, the arrows indicate estimates for the source number densities of different steady source candidate classes: Milky Way–like galaxies (C. J. Conselice et al. 2016), low-luminosity AGNs (L. C. Ho 2008), star-forming galaxies (C. Gruppioni et al. 2013), starburst galaxies (C. Gruppioni et al. 2013; K. Murase & M. Fukugita 2019), and high-luminosity AGNs (P. N. Best & T. M. Heckman 2012; C. Gruppioni et al. 2013).
Paper: The Large-scale Anisotropy and Flux (de)magnification of Ultrahigh-energy Cosmic Rays in the Galactic Magnetic Field
Authors: Teresa Bister, Glennys R. Farrar, Michael Unger
Figure caption: The markers show the dipole and quadrupole moments, d and Q, in the limit of continuous source density (n  s  = ∞ ) for the various GMF models and energy >8 EeV, as in Figure 1. The dashed curves show, for the base GMF model and different values of n  s , the 1σ domain from cosmic variance. The gray regions mark the data 1σ uncertainty for the dipole (G. Golup 2023) and the quadrupole (L. Caccianiga et al. 2023). Note that the measured quadrupole amplitude is not significant as it is compatible with isotropy within 2σ.
Paper: The Large-scale Anisotropy and Flux (de)magnification of Ultrahigh-energy Cosmic Rays in the Galactic Magnetic Field
Authors: Teresa Bister, Glennys R. Farrar, Michael Unger
Figure caption: (a) and (b) Magnification maps for rigidity ﹩{ \mathcal R }=5\,\mathrm{EV}﹩ (see the text for an explanation). Gray pixels are source directions contributing no events at Earth. Contours indicating the extragalactic directions with large flux (panel (c)) are shown in red. (c) The E > 8 EeV illumination map calculated from the LSS model (T. Bister & G. R. Farrar 2024), showing the flux at the edge of the Galaxy.
Paper: Hints of a Sulfur-rich Atmosphere around the 1.6 R ⊕ Super-Earth L98-59 d from JWST NIRspec G395H Transmission Spectroscopy
Authors: Amélie Gressier, Néstor Espinoza, Natalie H. Allen, David K. Sing, Agnibha Banerjee, Joanna K. Barstow, Jeff A. Valenti, Nikole K. Lewis, Stephan M. Birkmann, Ryan C. Challener, Elena Manjavacas, Catarina Alves de Oliveira, Nicolas Crouzet, Tracy. L Beck
Figure caption: Top left: transmission spectrum of L98-59 d obtained using  transitspectroscopy (pink data points) and  FIREFLy (blue data points) and binned to R ∼ 100 compared to an atmospheric retrieval model with 1σ uncertainty. An offset is fitted between NRS1 and NRS2. Top right: posterior distributions from the atmospheric retrieval analyses. We do not represent all parameters for clarity. The values are printed for the  FIREFLy atmospheric fit. Bottom left: transmission spectrum of L98-59 d obtained using  FIREFLy (blue data points) binned to R ∼ 60 compared to the atmospheric retrieval model with 1σ uncertainty. An offset is fitted between NRS1 and NRS2. Bottom right: posterior distributions from the atmospheric retrieval analysis.
Paper: The Large-scale Anisotropy and Flux (de)magnification of Ultrahigh-energy Cosmic Rays in the Galactic Magnetic Field
Authors: Teresa Bister, Glennys R. Farrar, Michael Unger
Figure caption: Combined magnification maps for different rigidities of all  UF23 models with Planck random field, including both l  c  = 30 pc and l  c  = 60 pc, the latter with two variations. The color bar displays the magnification range in directions where all models agree; for the white area there is no consensus among the models. The directions of source candidates are indicated by stars, and the marker size is proportional to 1/distance.
Paper: Hints of a Sulfur-rich Atmosphere around the 1.6 R ⊕ Super-Earth L98-59 d from JWST NIRspec G395H Transmission Spectroscopy
Authors: Amélie Gressier, Néstor Espinoza, Natalie H. Allen, David K. Sing, Agnibha Banerjee, Joanna K. Barstow, Jeff A. Valenti, Nikole K. Lewis, Stephan M. Birkmann, Ryan C. Challener, Elena Manjavacas, Catarina Alves de Oliveira, Nicolas Crouzet, Tracy. L Beck
Figure caption: Posterior distributions from the stellar retrieval analysis.
Paper: Hints of a Sulfur-rich Atmosphere around the 1.6 R ⊕ Super-Earth L98-59 d from JWST NIRspec G395H Transmission Spectroscopy
Authors: Amélie Gressier, Néstor Espinoza, Natalie H. Allen, David K. Sing, Agnibha Banerjee, Joanna K. Barstow, Jeff A. Valenti, Nikole K. Lewis, Stephan M. Birkmann, Ryan C. Challener, Elena Manjavacas, Catarina Alves de Oliveira, Nicolas Crouzet, Tracy. L Beck
Figure caption: Posterior distributions from the equilibrium chemistry retrieval analysis. Not all parameters in the fit are plotted for clarity.
Paper: Swiftly Chasing Gravitational Waves across the Sky in Real Time
Authors: Aaron Tohuvavohu, Jamie A. Kennea, Christopher J. Roberts, James DeLaunay, Samuele Ronchini, S. Bradley Cenko, Becca Ewing, Ryan Magee, Cody Messick, Surabhi Sachdev, Leo P. Singer
Figure caption: The reverse cumulative distribution of the BAT normalized sensitivity to the true BNS location using 29 Hz sky maps at various response latencies. We mark the saturation condition for 29 Hz at 50% of the mergers and the “edge” of the BAT FOV at 0.1. One can easily read off that an early-warning time of −60 s (pink) doubles the fraction of mergers inside the FOV. Note that the relative gain increases with coding, meaning that early-warning response not only maximizes the fraction of mergers in the FOV but also independently increases the average sensitivity to those already in the FOV. On the right, we present the fraction of mergers inside the BAT FOV as a function of warning time for sky maps derived at different truncation frequencies. We can easily see that, despite the improved localization precision at higher frequencies, acting on the earliest sky map is always better than waiting given Swift’s finite slew speed. We also show capabilities assuming an early-warning time of >70 s, achievable only by upgraded GW detectors. For these cases, we assume the same sky maps as produced at 29 Hz by Advanced LIGO/Virgo.
Paper: Swiftly Chasing Gravitational Waves across the Sky in Real Time
Authors: Aaron Tohuvavohu, Jamie A. Kennea, Christopher J. Roberts, James DeLaunay, Samuele Ronchini, S. Bradley Cenko, Becca Ewing, Ryan Magee, Cody Messick, Surabhi Sachdev, Leo P. Singer
Figure caption: A GW early-warning alert at 29 Hz. Plotted are the GW sky map 50% and 90% containment contours and BAT FOV (heat map) at the exact truncation frequency time relative to merger T0. Left shows the orientation at the time the alert is produced, with little coverage of the GW sky map. Center and right show the optimal trajectory found by the sampler (after 200 and 100 trials, respectively) and the BAT FOV at merger time if that trajectory is executed. The portion of the sky occulted by the Earth at the time is in white, and the Sun and Moon boresight constraints are marked. The bull's-eye marks the true location of the merger, not known to the trajectory optimizer. The black cross is the commanded target of the slew, and the green reticle is the Swift boresight.
Paper: Swiftly Chasing Gravitational Waves across the Sky in Real Time
Authors: Aaron Tohuvavohu, Jamie A. Kennea, Christopher J. Roberts, James DeLaunay, Samuele Ronchini, S. Bradley Cenko, Becca Ewing, Ryan Magee, Cody Messick, Surabhi Sachdev, Leo P. Singer
Figure caption: A sample of GW early-warning sky maps at a truncation frequency of 29 Hz (∼−60 s before merger). The left column shows BAT coverage at the alert time, and the right panel shows the optimal trajectory found and BAT coverage at merger time if the trajectory is executed. Note a tragic (rare) occurrence in the third row of slewing away from the correct position, not yet known. But note also marked successes in the second and fourth panels.
Paper: Swiftly Chasing Gravitational Waves across the Sky in Real Time
Authors: Aaron Tohuvavohu, Jamie A. Kennea, Christopher J. Roberts, James DeLaunay, Samuele Ronchini, S. Bradley Cenko, Becca Ewing, Ryan Magee, Cody Messick, Surabhi Sachdev, Leo P. Singer
Figure caption: Comparison of best objective values achieved by the TPE, random, and CMA-ES samplers as a function of trials. The shaded areas represent the standard deviation across >1000 runs on different sky maps and starting conditions. TPE shows slightly superior overall performance and consistency, achieving the best results on average, although all samplers show significant performance variability across trajectory conditions.
Paper: Swiftly Chasing Gravitational Waves across the Sky in Real Time
Authors: Aaron Tohuvavohu, Jamie A. Kennea, Christopher J. Roberts, James DeLaunay, Samuele Ronchini, S. Bradley Cenko, Becca Ewing, Ryan Magee, Cody Messick, Surabhi Sachdev, Leo P. Singer
Figure caption: Same as Figure 6 but for a truncation frequency of 38 Hz. Note the successes in the first and fourth panels.
Paper: Swiftly Chasing Gravitational Waves across the Sky in Real Time
Authors: Aaron Tohuvavohu, Jamie A. Kennea, Christopher J. Roberts, James DeLaunay, Samuele Ronchini, S. Bradley Cenko, Becca Ewing, Ryan Magee, Cody Messick, Surabhi Sachdev, Leo P. Singer
Figure caption: The latency of GW alerts during O4, measured as the difference between alert receipt and merger time. The red line denotes the median latency across all alerts in O4. Note that these latencies must be added on top of early-warning negative latencies, leading most “early-warning” alerts to be distributed after merger.
Paper: Swiftly Chasing Gravitational Waves across the Sky in Real Time
Authors: Aaron Tohuvavohu, Jamie A. Kennea, Christopher J. Roberts, James DeLaunay, Samuele Ronchini, S. Bradley Cenko, Becca Ewing, Ryan Magee, Cody Messick, Surabhi Sachdev, Leo P. Singer
Figure caption: Left: minimum slew time required to put any location on the sky inside the BAT FOV; white sky areas are occulted by the Earth. Right: the cumulative fraction of sky accessible to the BAT FOV as a function of slew time. If given a target, Swift can put almost any position on the unocculted sky into the BAT FOV in <175 s.
Paper: Hints of a Sulfur-rich Atmosphere around the 1.6 R ⊕ Super-Earth L98-59 d from JWST NIRspec G395H Transmission Spectroscopy
Authors: Amélie Gressier, Néstor Espinoza, Natalie H. Allen, David K. Sing, Agnibha Banerjee, Joanna K. Barstow, Jeff A. Valenti, Nikole K. Lewis, Stephan M. Birkmann, Ryan C. Challener, Elena Manjavacas, Catarina Alves de Oliveira, Nicolas Crouzet, Tracy. L Beck
Figure caption: Top panel: transmission spectrum of L98-59 d obtained using  transitspectroscopy and binned to R ∼ 100 (black points) compared to a free chemistry retrieval model from  TauREx (purple) and NEMESISPY (dashed blue) from Paper II Middle: opacity contributions from the best-fit model. The model suggests a contribution from H2S (purple) and SO2 (green) opacities. Bottom: transmission spectrum compared to stellar (yellow) and atmospheric (purple) retrieval models.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Hints of a Sulfur-rich Atmosphere around the 1.6 R ⊕ Super-Earth L98-59 d from JWST NIRspec G395H Transmission Spectroscopy
Authors: Amélie Gressier, Néstor Espinoza, Natalie H. Allen, David K. Sing, Agnibha Banerjee, Joanna K. Barstow, Jeff A. Valenti, Nikole K. Lewis, Stephan M. Birkmann, Ryan C. Challener, Elena Manjavacas, Catarina Alves de Oliveira, Nicolas Crouzet, Tracy. L Beck
Figure caption: Transmission spectra of L98-59 d obtained using  transitspectroscopy (pink) and  FIREFLy (blue) pipelines. The spectral light curves from the two independent reductions were fitted independently.  transitspectroscopy are fitted at pixel-level resolution using Gaussian processes to model the noise and then binned to the native resolution of the  FIREFLy's reduction to approximately an R ∼ 60.  FIREFLy light curves are binned to R ∼ 60 and then fitted using a linear detrending model. For both fittings, the coefficients of the limb-darkening coefficients are fixed to q 1 = 0.13 and q 2 = 0.0.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Hints of a Sulfur-rich Atmosphere around the 1.6 R ⊕ Super-Earth L98-59 d from JWST NIRspec G395H Transmission Spectroscopy
Authors: Amélie Gressier, Néstor Espinoza, Natalie H. Allen, David K. Sing, Agnibha Banerjee, Joanna K. Barstow, Jeff A. Valenti, Nikole K. Lewis, Stephan M. Birkmann, Ryan C. Challener, Elena Manjavacas, Catarina Alves de Oliveira, Nicolas Crouzet, Tracy. L Beck
Figure caption: Top panel: transmission spectrum of L98-59 d obtained using  transitspectroscopy and binned to R ∼ 100 (black points) compared to an equilibrium chemistry retrieval model from  TauREx (light green). Bottom: opacity contributions from the best-fit model. The model suggests a contribution from H2S (purple) and CO2 (red) opacities.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Hints of a Sulfur-rich Atmosphere around the 1.6 R ⊕ Super-Earth L98-59 d from JWST NIRspec G395H Transmission Spectroscopy
Authors: Amélie Gressier, Néstor Espinoza, Natalie H. Allen, David K. Sing, Agnibha Banerjee, Joanna K. Barstow, Jeff A. Valenti, Nikole K. Lewis, Stephan M. Birkmann, Ryan C. Challener, Elena Manjavacas, Catarina Alves de Oliveira, Nicolas Crouzet, Tracy. L Beck
Figure caption: Top: raw white light curves for NRS1 (left) and NRS2 (right) from  transitspectroscopy and spectral light-curves map. Middle: corrected white light curves (colored data points) overplotted with the best-fit transit model (black line) from  juliet. Bottom: residuals between raw light curves and transit model.(The data used to create this figure  are available in the online article.)
Paper: Hints of a Sulfur-rich Atmosphere around the 1.6 R ⊕ Super-Earth L98-59 d from JWST NIRspec G395H Transmission Spectroscopy
Authors: Amélie Gressier, Néstor Espinoza, Natalie H. Allen, David K. Sing, Agnibha Banerjee, Joanna K. Barstow, Jeff A. Valenti, Nikole K. Lewis, Stephan M. Birkmann, Ryan C. Challener, Elena Manjavacas, Catarina Alves de Oliveira, Nicolas Crouzet, Tracy. L Beck
Figure caption: Transmission spectra of L98-59 d obtained using  transitspectroscopy (pink) and  FIREFLy (blue) pipelines. The spectral light curves from the two independent reductions were fitted using  juliet with a similar parameterization at pixel resolution and then binned to R ∼ 100. The residuals between the two reductions show a global offset between the two reductions for the NRS2 detector.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Hints of a Sulfur-rich Atmosphere around the 1.6 R ⊕ Super-Earth L98-59 d from JWST NIRspec G395H Transmission Spectroscopy
Authors: Amélie Gressier, Néstor Espinoza, Natalie H. Allen, David K. Sing, Agnibha Banerjee, Joanna K. Barstow, Jeff A. Valenti, Nikole K. Lewis, Stephan M. Birkmann, Ryan C. Challener, Elena Manjavacas, Catarina Alves de Oliveira, Nicolas Crouzet, Tracy. L Beck
Figure caption: Top: transmission spectra of L98-59 d obtained using the reductions from  transitspectroscopy and binned to a resolution of R ∼ 60. The two spectra are derived by fitting the limb-darkening coefficients uniformly between 0 and 1 using a quadratic law (orange) and employing a square-root law (blue). The light orange points are obtained by applying an offset corresponding to the median differences between the two spectra. Bottom: residuals between the two transmission spectra after subtraction of the median transit depth. Each detector is treated independently. The shape of the two spectra is similar, but there is a 400 ppm offset between the two reductions.
Paper: Hints of a Sulfur-rich Atmosphere around the 1.6 R ⊕ Super-Earth L98-59 d from JWST NIRspec G395H Transmission Spectroscopy
Authors: Amélie Gressier, Néstor Espinoza, Natalie H. Allen, David K. Sing, Agnibha Banerjee, Joanna K. Barstow, Jeff A. Valenti, Nikole K. Lewis, Stephan M. Birkmann, Ryan C. Challener, Elena Manjavacas, Catarina Alves de Oliveira, Nicolas Crouzet, Tracy. L Beck
Figure caption: Transmission spectrum of L98-59 d obtained using  transitspectroscopy and binned to R ∼ 100 (black points) compared to forward models from  Exo-REM (colored dashed and filled lines). The pure H2S model provides the best fit according to χ 2 statistics. No offset is added between NRS1 and NRS2.
Paper: Hints of a Sulfur-rich Atmosphere around the 1.6 R ⊕ Super-Earth L98-59 d from JWST NIRspec G395H Transmission Spectroscopy
Authors: Amélie Gressier, Néstor Espinoza, Natalie H. Allen, David K. Sing, Agnibha Banerjee, Joanna K. Barstow, Jeff A. Valenti, Nikole K. Lewis, Stephan M. Birkmann, Ryan C. Challener, Elena Manjavacas, Catarina Alves de Oliveira, Nicolas Crouzet, Tracy. L Beck
Figure caption: Posterior distributions from the free retrieval analysis. Not all parameters in the fit are plotted for clarity.
Paper: Lava Worlds Surface Measurements at High Temperatures
Authors: Marc-Antoine Fortin, Esteban Gazel, Daniel B. Williams, James O. Thompson, Lisa Kaltenegger, Michael S. Ramsey
Figure caption: Selected potential exoplanet surface compositions classification according to their total alkali vs. silica (TAS). Modified from M.-A. Fortin et al. (2022).
Paper: Lava Worlds Surface Measurements at High Temperatures
Authors: Marc-Antoine Fortin, Esteban Gazel, Daniel B. Williams, James O. Thompson, Lisa Kaltenegger, Michael S. Ramsey
Figure caption: Emissivity spectra of investigated compositions from 800° C to 1350° C. The full data set is available as data behind the figure.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Lava Worlds Surface Measurements at High Temperatures
Authors: Marc-Antoine Fortin, Esteban Gazel, Daniel B. Williams, James O. Thompson, Lisa Kaltenegger, Michael S. Ramsey
Figure caption: Linear fit for all data across all temperatures from Equation (1), with 95% confidence level interval shown by the dotted lines.
Paper: JWST/NIRISS Reveals the Water-rich “Steam World” Atmosphere of GJ 9827 d
Authors: Caroline Piaulet-Ghorayeb, Björn Benneke, Michael Radica, Eshan Raul, Louis-Philippe Coulombe, Eva-Maria Ahrer, Daria Kubyshkina, Ward S. Howard, Joshua Krissansen-Totton, Ryan J. MacDonald, Pierre-Alexis Roy, Amy Louca, Duncan Christie, Marylou Fournier-Tondreau, Romain Allart, Yamila Miguel, Hilke E. Schlichting, Luis Welbanks, Charles Cadieux, Caroline Dorn, Thomas M. Evans-Soma, Jonathan J. Fortney, Raymond Pierrehumbert, David Lafrenière, Lorena Acuña, Thaddeus Komacek, Hamish Innes, Thomas G. Beatty, Ryan Cloutier, René Doyon, Anna Gagnebin, Cyril Gapp, Heather A. Knutson
Figure caption: Posterior distributions on the molecular abundances for all the fitted molecules in the SCARLET retrieval with H2/He used as a filler gas and without stellar contamination. The 1σ, 2σ, and 3σ lower (upper) limits for H2O (other molecules) are indicated by the color shadings.
Paper: JWST/NIRISS Reveals the Water-rich “Steam World” Atmosphere of GJ 9827 d
Authors: Caroline Piaulet-Ghorayeb, Björn Benneke, Michael Radica, Eshan Raul, Louis-Philippe Coulombe, Eva-Maria Ahrer, Daria Kubyshkina, Ward S. Howard, Joshua Krissansen-Totton, Ryan J. MacDonald, Pierre-Alexis Roy, Amy Louca, Duncan Christie, Marylou Fournier-Tondreau, Romain Allart, Yamila Miguel, Hilke E. Schlichting, Luis Welbanks, Charles Cadieux, Caroline Dorn, Thomas M. Evans-Soma, Jonathan J. Fortney, Raymond Pierrehumbert, David Lafrenière, Lorena Acuña, Thaddeus Komacek, Hamish Innes, Thomas G. Beatty, Ryan Cloutier, René Doyon, Anna Gagnebin, Cyril Gapp, Heather A. Knutson
Figure caption: Posterior distributions on the molecular abundances for all the fitted species in the POSEIDON retrieval with CLR priors and without stellar contamination. The 1σ, 2σ, and 3σ lower (upper) limits for H2O (other molecules) are indicated by the color shadings.
Paper: JWST/NIRISS Reveals the Water-rich “Steam World” Atmosphere of GJ 9827 d
Authors: Caroline Piaulet-Ghorayeb, Björn Benneke, Michael Radica, Eshan Raul, Louis-Philippe Coulombe, Eva-Maria Ahrer, Daria Kubyshkina, Ward S. Howard, Joshua Krissansen-Totton, Ryan J. MacDonald, Pierre-Alexis Roy, Amy Louca, Duncan Christie, Marylou Fournier-Tondreau, Romain Allart, Yamila Miguel, Hilke E. Schlichting, Luis Welbanks, Charles Cadieux, Caroline Dorn, Thomas M. Evans-Soma, Jonathan J. Fortney, Raymond Pierrehumbert, David Lafrenière, Lorena Acuña, Thaddeus Komacek, Hamish Innes, Thomas G. Beatty, Ryan Cloutier, René Doyon, Anna Gagnebin, Cyril Gapp, Heather A. Knutson
Figure caption: Composition of GJ 9827 d for a 100% water envelope. Joint and marginalized posterior distributions of the planet structure fit for GJ 9827 d assuming a vapor/supercritical hydrosphere on top of an interior composed of various mass fractions of rock and iron. The 1σ, 2σ, and 3σ probability contours are shown.
Paper: The AMS-02 Cosmic-Ray Deuteron Flux is Consistent with a Secondary Origin
Authors: Qiang Yuan, Yi-Zhong Fan
Figure caption: Production cross section of deuterons from the reaction p + C → D + X. The dashed line is the result of the parameterization given in B. Coste et al. (2012), and the solid line is the adjusted cross section of this work. The data of CNO fragmentation into D (R. Ramaty & R. E. Lingenfelter 1969; D. L. Olson et al. 1983), as compiled in B. Coste et al. (2012), are shown. Note that the lines should be compared with the blue points directly. For N and O, the normalizations (and energy-dependent shapes) differ slightly from those of C.