adsabs/AstroCLIMB huggingface dataset:
Paper: Col-OSSOS: The Two Types of Kuiper Belt Surfaces
Authors: Wesley C. Fraser, Rosemary E. Pike, Michaël Marsset, Megan E. Schwamb, Michele T. Bannister, Laura Buchanan, J. J. Kavelaars, Susan D. Benecchi, Nicole J. Tan, Nuno Peixinho, Stephen D. J. Gwyn, Mike Alexandersen, Ying-Tung Chen, Brett Gladman, Kathryn Volk
Figure caption: Free inclination, inclination, and eccentricity vs. semimajor axes of the objects from Col-OSSOS and H/WTSOSS. Those two surveys are the only two from which reliable classification into BrightIR and FaintIR can be made. The left column shows the cold classical region, while the right column shows the broader extended Kuiper Belt.
Paper: Col-OSSOS: The Two Types of Kuiper Belt Surfaces
Authors: Wesley C. Fraser, Rosemary E. Pike, Michaël Marsset, Megan E. Schwamb, Michele T. Bannister, Laura Buchanan, J. J. Kavelaars, Susan D. Benecchi, Nicole J. Tan, Nuno Peixinho, Stephen D. J. Gwyn, Mike Alexandersen, Ying-Tung Chen, Brett Gladman, Kathryn Volk
Figure caption: Cutouts around a typical NIRI calibration star. Left: original image. Middle: subtraction of an average Moffat profile. Right: subtraction of the azimuthally variable Moffat profile. The residual flux in the wings is improved through use of the azimuthally variable profile.
Paper: Col-OSSOS: The Two Types of Kuiper Belt Surfaces
Authors: Wesley C. Fraser, Rosemary E. Pike, Michaël Marsset, Megan E. Schwamb, Michele T. Bannister, Laura Buchanan, J. J. Kavelaars, Susan D. Benecchi, Nicole J. Tan, Nuno Peixinho, Stephen D. J. Gwyn, Mike Alexandersen, Ying-Tung Chen, Brett Gladman, Kathryn Volk
Figure caption: GMOS instrumental magnitudes vs. (g − r) colors of stars in the Pan-STAARS v1 data set. Red lines show the linear color terms derived from those measurements.
Paper: There’s More to Life than O2: Simulating the Detectability of a Range of Molecules for Ground-based, High-resolution Spectroscopy of Transiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows, Kaitlin C. Rasmussen
Figure caption: Upper panel: spectral energy distributions of the M-dwarf host stars in this study incident at the top of the planets’ atmospheres. Lower panel: the stellar fluxes as seen by an observer 12 pc away. The spectral resolution is binned down to R = 50 for clarity. The colored horizontal lines are the selected molecular absorption bands we investigate in our planetary atmospheres.
Paper: There’s More to Life than O2: Simulating the Detectability of a Range of Molecules for Ground-based, High-resolution Spectroscopy of Transiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows, Kaitlin C. Rasmussen
Figure caption: Mixing ratios for the major species in the preindustrial Earth-like (PIE) atmospheres and temperature profiles. Each line represents a self-consistent Earth-like atmosphere orbiting a stellar host. Earlier-type M-dwarf hosts are lighter and later-type M-dwarf hosts are darker. The dashed blue line represents profiles for the Earth orbiting the Sun for comparison.
Paper: There’s More to Life than O2: Simulating the Detectability of a Range of Molecules for Ground-based, High-resolution Spectroscopy of Transiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows, Kaitlin C. Rasmussen
Figure caption: Mixing ratios for the major species in the Archean Earth–like (ARE) atmospheres and temperature profiles. Each line represents a self-consistent Earth-like atmosphere orbiting a stellar host. Earlier-type M-dwarf hosts are lighter and later-type M-dwarf hosts are darker. The dashed blue line represents profiles for the Earth orbiting the Sun for comparison.
Paper: There’s More to Life than O2: Simulating the Detectability of a Range of Molecules for Ground-based, High-resolution Spectroscopy of Transiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows, Kaitlin C. Rasmussen
Figure caption: Overview of methods pipeline. The red round boxes represent the start and end points of the pipeline. The solid green boxes represent models or software pipelines, the white parallelograms represent input or output data products, and the rhombuses represent user-specified metadata or parameters. Cartoon examples of the data products are shown next to each data product node.
Paper: There’s More to Life than O2: Simulating the Detectability of a Range of Molecules for Ground-based, High-resolution Spectroscopy of Transiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows, Kaitlin C. Rasmussen
Figure caption: Mixing ratios for the major species in the abiotic O2 buildup from CO2 photolysis atmospheres and temperature profiles. The solid and dotted red lines represent profiles for a CO2 photolysis atmosphere with lightning turned on and off, respectively, orbiting an M4V-type stellar host. The dashed blue line represents profiles for the Earth orbiting the Sun for comparison.
Paper: There’s More to Life than O2: Simulating the Detectability of a Range of Molecules for Ground-based, High-resolution Spectroscopy of Transiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows, Kaitlin C. Rasmussen
Figure caption: Detection significance as a function of total integration time for the most detectable molecular bands in photochemically self-consistent preindustrial Earth-like (PIE) atmospheres, Archean Earth–like (ARE) atmospheres, CO2 photolysis atmospheres (lightning on/off), and 10 bar O2 worlds (ocean loss/outgassing) (columns left to right) at distances of 5 pc from Earth observed with a TMT-sized telescope. The shaded regions are the 1﹩{\sigma }_{\det }﹩ uncertainties on detection significance. The dark and light gray dotted lines mark the 3 and 5﹩{\sigma }_{\det }﹩ thresholds, respectively.
Paper: There’s More to Life than O2: Simulating the Detectability of a Range of Molecules for Ground-based, High-resolution Spectroscopy of Transiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows, Kaitlin C. Rasmussen
Figure caption: Detection significance as a function of total integration time for the most detectable molecular bands in photochemically self-consistent preindustrial Earth-like (PIE) atmospheres, Archean Earth–like (ARE) atmospheres, CO2 photolysis atmospheres (lightning on/off), and 10 bar O2 worlds (ocean loss/outgassing) (columns left to right) at distances of 12 pc from Earth observed with an E-ELT-sized telescope. The shaded regions are the 1﹩{\sigma }_{\det }﹩ uncertainties on detection significance. The dark and light gray dotted lines mark the 3 and 5﹩{\sigma }_{\det }﹩ thresholds, respectively.
Paper: There’s More to Life than O2: Simulating the Detectability of a Range of Molecules for Ground-based, High-resolution Spectroscopy of Transiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows, Kaitlin C. Rasmussen
Figure caption: Detection significance as a function of number of observed transits for four molecular bands in our simulated TRAPPIST-1 e atmospheres observed with the E-ELT. The shaded regions are the 1﹩{\sigma }_{\det }﹩ uncertainties on detection significance. The horizontal dark and light gray dotted lines mark the 3 and 5﹩{\sigma }_{\det }﹩ thresholds, respectively. The vertical dotted dark and light gray lines, and corresponding labels to their right, denote the precise integration time required for 3 and 5﹩{\sigma }_{\det }﹩ detections. Note that the transit duration is 0.99 hr, so the integration time required is nearly the same as the number of observed transits required.
Paper: There’s More to Life than O2: Simulating the Detectability of a Range of Molecules for Ground-based, High-resolution Spectroscopy of Transiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows, Kaitlin C. Rasmussen
Figure caption: Noise sources per resolution element considered in this work for a band in the visible (top panel) and a band in the NIR (bottom panel) for a 2 hr exposure at R = 100,000. The background shot noise is comprised of zodiacal light, telluric emission, airglow, and telescope/instrument thermal emission, and the airglow continuum dominates the background continuum. The shot noise is plotted for all stars at 12 pc, and includes attenuation from the Earth’s telluric transmission. Photon (shot) noise from the M2V and M8V stars exceeds the combined readout and dark noise by a factor of 25 and 8, respectively, for the visible, and 12 and 15, respectively, for the NIR.
Paper: There’s More to Life than O2: Simulating the Detectability of a Range of Molecules for Ground-based, High-resolution Spectroscopy of Transiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows, Kaitlin C. Rasmussen
Figure caption: Total observed transits required for a 3﹩{\sigma }_{\det }﹩ significance detection using an E-ELT-sized telescope for selected bands in all atmosphere classes orbiting a range of host stars at a distance of 12 pc from the observer. A marker is missing either where the atmosphere does not contain a molecule or >300 observed transits are required to detect the molecular band.
Paper: There’s More to Life than O2: Simulating the Detectability of a Range of Molecules for Ground-based, High-resolution Spectroscopy of Transiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows, Kaitlin C. Rasmussen
Figure caption: Selected molecular bands in this work. Each molecular band is plotted at R = 100,000 and is continuum subtracted using a high-pass filter (see Section 2). Note the scale in each row: planets transiting later-type M-dwarf hosts typically have larger relative transit depths than planets transiting early-type hosts.
Paper: There’s More to Life than O2: Simulating the Detectability of a Range of Molecules for Ground-based, High-resolution Spectroscopy of Transiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows, Kaitlin C. Rasmussen
Figure caption: Ratios of the number of transits required to detect the most sensitive molecular bands in our study for cloudy to clear-sky preindustrial Earth-like (PIE) atmospheres. Missing markers signify that cloudy spectra require >300 transits to detect the molecular feature.
Paper: There’s More to Life than O2: Simulating the Detectability of a Range of Molecules for Ground-based, High-resolution Spectroscopy of Transiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows, Kaitlin C. Rasmussen
Figure caption: Number of transits required to detect the O2 1.27 μm band as a function of spectral resolution for PIE atmospheres transiting M-dwarf stars 5 pc away from Earth. The benefits of increasing the spectral resolution are marginal for resolutions greater than R ∼ 150,000.
Paper: There’s More to Life than O2: Simulating the Detectability of a Range of Molecules for Ground-based, High-resolution Spectroscopy of Transiting Terrestrial Exoplanets
Authors: Miles H. Currie, Victoria S. Meadows, Kaitlin C. Rasmussen
Figure caption: Mixing ratios for the major species in the 10 bar O2 ocean-outgassing (dashed) and ocean-loss (solid) atmospheres and temperature profiles. The dashed blue line represents profiles for the Earth orbiting the Sun for comparison. There is no H2O in the ocean-loss atmosphere.
Paper: Thermal Creep on Mars: Visualizing a Soil Layer under Tension
Authors: Tetyana Bila, Jonathan Kollmer, Jens Teiser, Gerhard Wurm
Figure caption: The basic principle of thermal creep and Knudsen compressor. (a) Gas flow in an open tube of the large cross section with a temperature gradient between the tube ends. In a tube with a large cross section, there are two opposing gas flows: a gas flow from the colder end to the warmer end in a thin layer on the order of the mean free path of molecules λ  g , called thermal creep, and a backflow from the warmer to the colder end. (b) In a tube with a cross section on the order of λ  g , the thermal creep gas flow dominates. (c)–(d) A tube with a cross section on the order of λ  g  with a temperature gradient between its ends. On the warmer side the tube is followed by a smaller tube of the same cross section having a constant temperature. The thermal creep gas flow cannot proceed into the smaller tube and the pressure increases at the junction. This leads to a pressure-driven gas flow through the smaller tube. The pressure adjusts itself until the incoming temperature gradient-driven gas flow equals the pressure-driven gas flow. (e) In-depth basic pressure distribution in a dust bed heated from above. y 0 denotes the surface of a particle bed. In the near-surface layer from y 0 to y 1 the temperature is constant. Below y 1 down to y 2 the temperature gradient is present.
Paper: Thermal Creep on Mars: Visualizing a Soil Layer under Tension
Authors: Tetyana Bila, Jonathan Kollmer, Jens Teiser, Gerhard Wurm
Figure caption: Motion depth profiles at the latest time (395 s); top: high-pressure data with clear split in two parts, a downward decreasing and then nearly constant part; middle: overplotted example of low-pressure data with an additional increase at larger depths. The orange dashed line is a fit with ﹩{r}_{\mathrm{high}}=\mathrm{const}.﹩ on the flat parts of all three of the higher-pressure depth profiles. r low is the value of the depth profile of lowest pressure at y = 5 mm. Δr is the difference between r low and r high; bottom: all low-pressure data.
Paper: Thermal Creep on Mars: Visualizing a Soil Layer under Tension
Authors: Tetyana Bila, Jonathan Kollmer, Jens Teiser, Gerhard Wurm
Figure caption: Strength of the motion of grains with depth y over time at 5.2 mbar ambient pressure. Dark color marks little motion (reversed color from correlation plot Figure 5).
Paper: Thermal Creep on Mars: Visualizing a Soil Layer under Tension
Authors: Tetyana Bila, Jonathan Kollmer, Jens Teiser, Gerhard Wurm
Figure caption: Top: the experimental setup used. (1) Vacuum chamber, (2) polarizing filter, (3) camera lens, (4) camera, (5) red filter, (6) lens with f = 300 mm, (7) lens with f = 10.8 mm, (8) polarizing filter, (9) laser, (10) optical fiber, (11) digital thermometer, (12) analog-to-digital converter, (13) pressure display unit and (14) vacuum gauge. Middle and bottom figures show the sketch of the setup in top view and side view respectively. A granular soil simulant sample within a vessel is placed in a vacuum chamber. Heating from the top (IR radiation) simulates insolation. The speckle pattern of a laser backscattered from the sample from the side is imaged by a camera.
Paper: Thermal Creep on Mars: Visualizing a Soil Layer under Tension
Authors: Tetyana Bila, Jonathan Kollmer, Jens Teiser, Gerhard Wurm
Figure caption: Top: pressure dependence of Δr; center: dependence of Δr on Knudsen number; bottom: temperature difference at the end of the measurement over the ambient pressure at the beginning of the measurement.
Paper: Thermal Creep on Mars: Visualizing a Soil Layer under Tension
Authors: Tetyana Bila, Jonathan Kollmer, Jens Teiser, Gerhard Wurm
Figure caption: Example of a time evolution of the correlation for the measurement at 5.2 mbar; times after the heater is switched on are imprinted in each image. The dashed green line indicates the position of the sample surface. y denotes downward direction and x is the horizontal. The size of one metapixel is 20 pixels.
Paper: Thermal Creep on Mars: Visualizing a Soil Layer under Tension
Authors: Tetyana Bila, Jonathan Kollmer, Jens Teiser, Gerhard Wurm
Figure caption: Model of a granular medium as a collection of pore-size tubes (from Steinpilz et al. 2017).
Paper: Thermal Creep on Mars: Visualizing a Soil Layer under Tension
Authors: Tetyana Bila, Jonathan Kollmer, Jens Teiser, Gerhard Wurm
Figure caption: Volume size distribution of the basalt sample used. From this distribution the mean particle diameter is calculated to 51 ± 28 μm.
Paper: Thermal Creep on Mars: Visualizing a Soil Layer under Tension
Authors: Tetyana Bila, Jonathan Kollmer, Jens Teiser, Gerhard Wurm
Figure caption: Same as Figure 5 but without heating at ∼1190 mbar ambient pressure.
Paper: Shape Models of Lucy Targets (3548) Eurybates and (21900) Orus from Disk-integrated Photometry
Authors: Stefano Mottola, Stephan Hellmich, Marc W. Buie, Amanda M. Zangari, Robert D. Stephens, Mario Di Martino, Gerrit Proffe, Simone Marchi, Catherine B. Olkin, Harold F. Levison
Figure caption: Composite light curves of Eurybates for the period 2012–2018. The data points beyond rotational phase 1.0 are repeated for clarity. P syn is the exact value of the synodic period used for folding the light curves, and as such, it is quoted without error. The reference epoch T 0 is one-leg light-time corrected and expressed in the TDB uniform frame. The magnitudes are reduced to the distance of 1 au from the Sun and from the observer. A small correction is applied to the magnitudes to reduce them to the reference phase angle of each observation set, shown in the respective y-axis label. Each symbol corresponds to an individual night of observation, centered at the UT epoch listed in the label. Observations on different nights reported with the same color have been reduced with the same set of catalog stars and are therefore tied in an absolute way. Observations reported in different colors have been performed with different sets of catalog stars and have been arbitrarily shifted in magnitude to account for catalog uncertainties. The applied shifts are typically smaller than 0.01 mag. The solid gray curve is the synthetic light curve obtained for the respective T 0 epoch with the best-fit shape model and photometric parameters (see text).
Paper: Shape Models of Lucy Targets (3548) Eurybates and (21900) Orus from Disk-integrated Photometry
Authors: Stefano Mottola, Stephan Hellmich, Marc W. Buie, Amanda M. Zangari, Robert D. Stephens, Mario Di Martino, Gerrit Proffe, Simone Marchi, Catherine B. Olkin, Harold F. Levison
Figure caption: Time-resolved color observations of Eurybates during the 2020 apparition. The top panel shows the R-band light curve along with the corresponding Fourier fit. The second panel from the top shows the R-band residuals to the fit, while the third and fourth panel show the B − R and R − I time-resolved color indices, respectively. See text for details.
Paper: Shape Models of Lucy Targets (3548) Eurybates and (21900) Orus from Disk-integrated Photometry
Authors: Stefano Mottola, Stephan Hellmich, Marc W. Buie, Amanda M. Zangari, Robert D. Stephens, Mario Di Martino, Gerrit Proffe, Simone Marchi, Catherine B. Olkin, Harold F. Levison
Figure caption: Composite light curves of Eurybates for the period 2019–2020. Notation is the same as in Figure 1.
Paper: Shape Models of Lucy Targets (3548) Eurybates and (21900) Orus from Disk-integrated Photometry
Authors: Stefano Mottola, Stephan Hellmich, Marc W. Buie, Amanda M. Zangari, Robert D. Stephens, Mario Di Martino, Gerrit Proffe, Simone Marchi, Catherine B. Olkin, Harold F. Levison
Figure caption: Polar azimuthal equidistant projection of the χ 2 of the pole solutions for Eurybates. The coordinates are expressed in the J2000 ecliptic frame. The left panel is centered on the north ecliptic pole and the right one on the south ecliptic pole. The equatorial region (ecliptic latitudes −30° to +30°) is mapped in both panels. The loci of the two complementary best solutions are clearly visible as white regions. The red circle marks the correct solution identified through its match with the stellar occultation chords by Keeney et al. (2021).
Paper: Shape Models of Lucy Targets (3548) Eurybates and (21900) Orus from Disk-integrated Photometry
Authors: Stefano Mottola, Stephan Hellmich, Marc W. Buie, Amanda M. Zangari, Robert D. Stephens, Mario Di Martino, Gerrit Proffe, Simone Marchi, Catherine B. Olkin, Harold F. Levison
Figure caption: Time-resolved color observations of Orus during the 2020 apparition. The top panel shows the R-band light curve along with the corresponding Fourier fit. The second panel from the top shows the R-band residuals to the fit, while the third and fourth panels show the B − R and V − R time-resolved color indices, respectively. See text for details.
Paper: Shape Models of Lucy Targets (3548) Eurybates and (21900) Orus from Disk-integrated Photometry
Authors: Stefano Mottola, Stephan Hellmich, Marc W. Buie, Amanda M. Zangari, Robert D. Stephens, Mario Di Martino, Gerrit Proffe, Simone Marchi, Catherine B. Olkin, Harold F. Levison
Figure caption: Sphere-integrated phase curve for Eurybates. The blue squares represent the geometry-corrected individual data points for the subset of the observations for which a reliable transformation to the Johnson V band could be determined.
Paper: Shape Models of Lucy Targets (3548) Eurybates and (21900) Orus from Disk-integrated Photometry
Authors: Stefano Mottola, Stephan Hellmich, Marc W. Buie, Amanda M. Zangari, Robert D. Stephens, Mario Di Martino, Gerrit Proffe, Simone Marchi, Catherine B. Olkin, Harold F. Levison
Figure caption: Occulting silhouettes of the best-fit convex model of Eurybates (solid black line) along with the rejected complementary model (displayed in light gray) at the time of the 2021 October 20 occultation. The red, green, and blue arrows represent the X-, Y-, and Z-axes in the body-fixed reference frame, respectively.
Paper: Shape Models of Lucy Targets (3548) Eurybates and (21900) Orus from Disk-integrated Photometry
Authors: Stefano Mottola, Stephan Hellmich, Marc W. Buie, Amanda M. Zangari, Robert D. Stephens, Mario Di Martino, Gerrit Proffe, Simone Marchi, Catherine B. Olkin, Harold F. Levison
Figure caption: Sidereal period scan for Eurybates. Trial periods correspond to the start values for each individual optimization run, while fit periods are the resulting optimized values.
Paper: Shape Models of Lucy Targets (3548) Eurybates and (21900) Orus from Disk-integrated Photometry
Authors: Stefano Mottola, Stephan Hellmich, Marc W. Buie, Amanda M. Zangari, Robert D. Stephens, Mario Di Martino, Gerrit Proffe, Simone Marchi, Catherine B. Olkin, Harold F. Levison
Figure caption: Composite light curves of Orus for the period 2012–2017. Notation as in Figure 1.
Paper: Shape Models of Lucy Targets (3548) Eurybates and (21900) Orus from Disk-integrated Photometry
Authors: Stefano Mottola, Stephan Hellmich, Marc W. Buie, Amanda M. Zangari, Robert D. Stephens, Mario Di Martino, Gerrit Proffe, Simone Marchi, Catherine B. Olkin, Harold F. Levison
Figure caption: Composite light curves of Orus for the 2019 apparition. Notation as in Figure 1.
Paper: Shape Models of Lucy Targets (3548) Eurybates and (21900) Orus from Disk-integrated Photometry
Authors: Stefano Mottola, Stephan Hellmich, Marc W. Buie, Amanda M. Zangari, Robert D. Stephens, Mario Di Martino, Gerrit Proffe, Simone Marchi, Catherine B. Olkin, Harold F. Levison
Figure caption: Sidereal period scan for Orus.
Paper: Shape Models of Lucy Targets (3548) Eurybates and (21900) Orus from Disk-integrated Photometry
Authors: Stefano Mottola, Stephan Hellmich, Marc W. Buie, Amanda M. Zangari, Robert D. Stephens, Mario Di Martino, Gerrit Proffe, Simone Marchi, Catherine B. Olkin, Harold F. Levison
Figure caption: Three orthographic views of the Eurybates convex shape model.
Paper: Shape Models of Lucy Targets (3548) Eurybates and (21900) Orus from Disk-integrated Photometry
Authors: Stefano Mottola, Stephan Hellmich, Marc W. Buie, Amanda M. Zangari, Robert D. Stephens, Mario Di Martino, Gerrit Proffe, Simone Marchi, Catherine B. Olkin, Harold F. Levison
Figure caption: Occulting silhouettes of the best-fit convex model of Orus (solid black line) along with the rejected complementary model (displayed in light gray) at the time of the 2021 October 16 occultation. The blue line represents a negative detection. The red, green, and blue arrows represent the X-, Y-, and Z-axes in the body-fixed reference frame, respectively.