adsabs/AstroCLIMB huggingface dataset:
Paper: High-resolution Search for Kuiper Belt Object Binaries from New Horizons
Authors: H.A. Weaver, S.B. Porter, and J.R. Spencer
Figure caption: Composite images of JY31 from two different epochs (2018 September 5 above the red line and 2018 September 11 below the red line) are displayed. The layout is exactly as previously described for HK103. In the first epoch of images coaligned on the KBO’s ephemeris, JY31 is clearly elongated in a diagonal direction relative to the stellar images. In the second epoch of images coaligned on the KBO’s ephemeris, JY31 appears to be broader horizontally relative to the stellar images. Thus, there is evidence for binarity for both epochs. All images are displayed using a linear stretch ranging from −1 to 2.5 DN, except that 64 × 64 126pp and 64 × 64 126qqrr (stars) are displayed on a linear scale from −1 to 3 DN to avoid saturating on the brightest pixel and 64 × 64 126oopp (stars) is displayed on a linear scale from −1 to 2 DN to bring out the fainter stars. Celestial north points down and east points to the right in all images.
Paper: High-resolution Search for Kuiper Belt Object Binaries from New Horizons
Authors: H.A. Weaver, S.B. Porter, and J.R. Spencer
Figure caption: Single- and double-PSF fits to the double-sampled LORRI images of CC JY31. The pair of panels on the left-hand side shows the two observations from the first epoch (REQIDs 126oo and 126pp), and the pair of panels on the right-hand side shows the two observations from the second epoch (REQIDs 126qq and 126pp). See Figure 4 for detailed descriptions of each panel. Here, the double-PSF solution is clearly much better than the single-PSF solution, and the location of the two PSFs is consistent between the two observations in each epoch. The “high-low-high” residuals in the single-PSF fits are typical of two barely resolved PSFs. We thus conclude that JY31 is almost certainly a binary.
Paper: High-resolution Search for Kuiper Belt Object Binaries from New Horizons
Authors: H.A. Weaver, S.B. Porter, and J.R. Spencer
Figure caption: Composite images of HZ102 from two different epochs (2018 November 30 above the red line and 2018 December 4 below the red line) are displayed. The layout is exactly as previously described for HK103. In all the composite images, HZ102 has a similar appearance to the PSF (i.e., to the stars), which shows there is no evidence for binarity in either epoch. All images are displayed using a linear stretch ranging from −1 to 1 DN, except 64 × 64 129qq and 64 × 64 129qqrr which are displayed on a linear scale from −1 to 1.5 DN to avoid saturating on the brightest pixel. Celestial north points down and east points to the right in all images.
Paper: High-resolution Search for Kuiper Belt Object Binaries from New Horizons
Authors: H.A. Weaver, S.B. Porter, and J.R. Spencer
Figure caption: Single- and double-PSF fits to the double-sampled LORRI images of HZ102. The pair of panels on the left-hand side shows the two observations from the first epoch (REQIDs 129qq and 129rr), and the pair of panels on the right-hand side shows the two observations from the second epoch (REQIDs 129ss and 129tt). See Figure 4 for detailed descriptions of each panel. Much like HK103, HZ102 is well fit with a single PSF. While there is a consistency in the angle of the two PSFs in the first epoch, the dimmer second PSF flips sides relative to the primary PSF, and so is likely not real.
Paper: High-resolution Search for Kuiper Belt Object Binaries from New Horizons
Authors: H.A. Weaver, S.B. Porter, and J.R. Spencer
Figure caption: Composite images of OS393 from two different epochs (2019 January 5 above the red line and 2019 January 6 below the red line) are displayed. The layout is exactly as previously described for HK103. OS393 appears to be elongated relative to the expected PSF in the first epoch, suggesting it is a binary object. Unfortunately, OS393 could not be detected in the second epoch when it was near the minimum in its lightcurve brightness. All images are displayed using a linear stretch ranging from −1 to 1 DN. Celestial north points down and east points to the right in all images.
Paper: High-resolution Search for Kuiper Belt Object Binaries from New Horizons
Authors: H.A. Weaver, S.B. Porter, and J.R. Spencer
Figure caption: OS393 lightcurve data from Porter et al. (2022) are plotted showing the strong variation of signal over time. The observation time for REQIDs 131ss and 131tt (green vertical line) occurred near the time of maximum brightness, whereas REQIDs 131qq and 131rr (red vertical line) were conducted near the time of minimum brightness.
Paper: High-resolution Search for Kuiper Belt Object Binaries from New Horizons
Authors: H.A. Weaver, S.B. Porter, and J.R. Spencer
Figure caption: Single- and double-PSF fits to the double-sampled LORRI images of OS393. The pair of panels on the left-hand side shows the two observations from the first epoch (REQIDs 131ss and 131tt), and the pair of panels on the right-hand side shows the two observations from the second epoch (REQIDs 131qq and 131rr). See Figure 4 for detailed descriptions of each panel. The images of OS393 in the first epoch appear to be elongated. Moreover, the locations of the PSFs in the double-PSF solutions are roughly consistent in the two separate image sets taken in the first epoch. However, OS393 is not visible at all in the second epoch. This is consistent with its lightcurve (see Figure 10), which predicts that the KBO should be about one magnitude dimmer in the second epoch than the first.
Paper: High-resolution Search for Kuiper Belt Object Binaries from New Horizons
Authors: H.A. Weaver, S.B. Porter, and J.R. Spencer
Figure caption: Composite images of PN70 from two different epochs (2019 March 9 above the red line and 2019 March 11 below the red line) are displayed. The layout is exactly as previously described for HK103. PN70 is detected in all these images but with low S/N. All images are displayed using a linear stretch ranging from −1 to 1 DN. Celestial north points down and east points to the right in all images.
Paper: High-resolution Search for Kuiper Belt Object Binaries from New Horizons
Authors: H.A. Weaver, S.B. Porter, and J.R. Spencer
Figure caption: LORRI 1×1 observations for PN70. The pair of panels on the left-hand side shows the two observations from the first epoch (REQIDs 132v and 132w), and the pair of panels on the right-hand side shows the two observations from the second epoch (REQIDs 132x and 132u). See Figure 4 for detailed description. While PN70 was detected in all four observations, it had a low S/N in both epochs. In none of the observations was the two-PSF solution significantly better than the single-PSF solution, which suggests there is no evidence that PN70 is binary.
Paper: High-resolution Search for Kuiper Belt Object Binaries from New Horizons
Authors: H.A. Weaver, S.B. Porter, and J.R. Spencer
Figure caption: The probability distribution function of the mutual orbit solution for JY31’s binary orbit using relative astrometry from the LORRI 1 × 1 images (see Figure 6). The orbit is assumed to be circular, and the fit parameters are period, orbital radius, inclination, longitude of the ascending node, and mean anomaly at the epoch. For this solution, the period is unconstrained, which results in a wide spread in the fit parameters.
Paper: High-resolution Search for Kuiper Belt Object Binaries from New Horizons
Authors: H.A. Weaver, S.B. Porter, and J.R. Spencer
Figure caption: The same as for Figure 14, except for this solution the period is constrained by the lightcurve results from the 4 × 4 data (Porter et al. 2022), which results in much tighter distributions of the fit parameters.
Paper: A Snowball in Hell: The Potential Steam Atmosphere of TOI-1266c
Authors: C. E. Harman, Ravi Kumar Kopparapu, Guðmundur Stefánsson, Andrea S.J. Lin, Suvrath Mahadevan, Christina Hedges, and Natasha E. Batalha
Figure caption: A mass–radius diagram for currently known exoplanets (small circles), the solar system planets (diamonds with letter designations), and TOI-1266c (square). Error bars for the mass and radius of TOI-1266c are also shown. The symbols are colored by instellation normalized to what Earth receives (∼1367 W m−2). The gray shaded region denotes the commonly accepted mass–radius regime for super-Earths. Two compositional trends are identified in the plot: the mass–radius relationship for a pure water ice planet (“H2O ice”; Seager et al. 2007) and for a planet with the same core mass fraction as Earth (“CMF⊕”; Unterborn et al. 2016).
Paper: A Snowball in Hell: The Potential Steam Atmosphere of TOI-1266c
Authors: C. E. Harman, Ravi Kumar Kopparapu, Guðmundur Stefánsson, Andrea S.J. Lin, Suvrath Mahadevan, Christina Hedges, and Natasha E. Batalha
Figure caption: Top panel: the notional luminosity evolution of TOI-1266 (black curve). The two red dashed curves denote the 0.4 and 0.45 M⊙ stellar evolution tracks of Hidalgo et al. (2018), which have been interpolated and normalized to match the observed luminosity at the current age estimate (denoted with the gray cross and labeled “Today”) for TOI-1266. The XUV saturation time is denoted as τsat, and the start of the main sequence with “MS.” Bottom panel: the X-ray (red), EUV (blue), and total XUV (black dashed) reflect the combination of both the evolving luminosity (top panel) and the saturation parameterizations from Peacock et al. (2020). For reference, the XUV flux is shown on the right-hand axis as normalized to what Earth receives (∼4.5 erg cm−2 s−1).
Paper: A Snowball in Hell: The Potential Steam Atmosphere of TOI-1266c
Authors: C. E. Harman, Ravi Kumar Kopparapu, Guðmundur Stefánsson, Andrea S.J. Lin, Suvrath Mahadevan, Christina Hedges, and Natasha E. Batalha
Figure caption: An example of one planetary evolution simulation, starting at ∼2 M⊕ and ∼1.7 R⊕, which ultimately evolves to match TOI-1266c’s observed mass and radius at TOI-1266's estimated age (vertical dashed line). Top panel: 10% H2O by mass; bottom panel: 9.6% H2O and 0.4% H2 by mass. Note that the vertical axis is logarithmic above the tilde and linear below it.
Paper: A Snowball in Hell: The Potential Steam Atmosphere of TOI-1266c
Authors: C. E. Harman, Ravi Kumar Kopparapu, Guðmundur Stefánsson, Andrea S.J. Lin, Suvrath Mahadevan, Christina Hedges, and Natasha E. Batalha
Figure caption: Water loss ensemble results calculated based on the range of planet parameter uncertainties from Table 2, plotted as a function of the current planet mass and the current envelope mass fraction of free oxygen. Symbols are colored by the initial envelope mass fraction of H2O, and the size is scaled based on the fraction of the planet initially designated as envelope (taken to be the maximum water abundance permitted by the mass–radius relationship of Noack et al. 2016). A red edge color for a given symbol denotes a scenario with less than 1 Earth ocean at present day, which would likely be short-lived (Kasting & Pollack 1983).
Paper: A Snowball in Hell: The Potential Steam Atmosphere of TOI-1266c
Authors: C. E. Harman, Ravi Kumar Kopparapu, Guðmundur Stefánsson, Andrea S.J. Lin, Suvrath Mahadevan, Christina Hedges, and Natasha E. Batalha
Figure caption: Temperature (left) and water vapor volume mixing ratio (vmr; right) profiles for the cases outlined in the text. The onset of water vapor condensation (vertical range in the left panel) occurs just above the “knee” in the water profiles, consistently around ∼1–10 mbar.
Paper: A Snowball in Hell: The Potential Steam Atmosphere of TOI-1266c
Authors: C. E. Harman, Ravi Kumar Kopparapu, Guðmundur Stefánsson, Andrea S.J. Lin, Suvrath Mahadevan, Christina Hedges, and Natasha E. Batalha
Figure caption: Left panel: CO mixing ratio profiles for the three atmospheres that contain CO2 in significant abundance. Right panel: O3 mixing ratio profiles for the nine principle scenarios included in this study.
Paper: A Snowball in Hell: The Potential Steam Atmosphere of TOI-1266c
Authors: C. E. Harman, Ravi Kumar Kopparapu, Guðmundur Stefánsson, Andrea S.J. Lin, Suvrath Mahadevan, Christina Hedges, and Natasha E. Batalha
Figure caption: Signal-to-noise ratio for observations with JWST at 0.7–5 μm. The composition is dominated by H2O and has secondary constituents denoted by the label.
Paper: A Snowball in Hell: The Potential Steam Atmosphere of TOI-1266c
Authors: C. E. Harman, Ravi Kumar Kopparapu, Guðmundur Stefánsson, Andrea S.J. Lin, Suvrath Mahadevan, Christina Hedges, and Natasha E. Batalha
Figure caption: Synthetic spectra (R = 500) of the nine cases highlighted previously. The panels are divided into families based on the gas mixture of interest: H2+H2O (top panel), CO2+H2+H2O (middle panel), and O2+H2O (bottom panel). A zoomed-in view of the 4.3 μm CO2 feature can be found in Figure 9, while Figure 10 focuses on key O2 and O3 features. For each 1% mixture, we overplot two other spectra. The orange error bars are for a simulated observation using JWST’s NIRSpec-Prism totaling 50 hr of in-transit time (R = 25). We also overplot a cloudy scenario, assuming that 14 μm liquid water droplets with a volume mixing ratio of 0.1 ppm (Kopparapu et al. 2021) are distributed throughout the pressure range identified in Figure 5.
Paper: A Snowball in Hell: The Potential Steam Atmosphere of TOI-1266c
Authors: C. E. Harman, Ravi Kumar Kopparapu, Guðmundur Stefánsson, Andrea S.J. Lin, Suvrath Mahadevan, Christina Hedges, and Natasha E. Batalha
Figure caption: Synthetic spectra (R = 500) for just the 1% CO2+H2+H2O and 1% O2+H2O mixtures from Figure 8, focusing on the 4.3 μm CO2 absorption feature. The corresponding error bars are for simulated observations using JWST’s NIRSpec-Prism for 50 hr of in-transit time (R = 100) and indicate that these two cases would be distinct from one another with JWST.
Paper: A Snowball in Hell: The Potential Steam Atmosphere of TOI-1266c
Authors: C. E. Harman, Ravi Kumar Kopparapu, Guðmundur Stefánsson, Andrea S.J. Lin, Suvrath Mahadevan, Christina Hedges, and Natasha E. Batalha
Figure caption: Synthetic spectra (R = 500) for just the O2+H2O mixtures from Figure 8, compared with the 10% CO2 mixture. Note that the O2 A-band feature at 0.76 μm increases to ∼10 ppm at 10% O2. However, the 0.2–0.3 μm and 9.6 μm ozone features are absent owing to the lack of a substantial O3 column abundance (the 0.2–0.3 μm region has O2 features from the Herzberg continuum but no contributions from O3). Variations between the spectra in this region are due to the increasing atmospheric mean molecular weight at higher O2 abundances. The orange error bars are for a simulated observation using JWST’s NIRSpec-Prism for 50 hr of in-transit time (R = 100). We also overplot a cloudy scenario, assuming that 14 μm liquid water droplets with a volume mixing ratio of 0.1 ppm (Kopparapu et al. 2021) are distributed throughout the pressure range identified in Figure 5.
Paper: A Snowball in Hell: The Potential Steam Atmosphere of TOI-1266c
Authors: C. E. Harman, Ravi Kumar Kopparapu, Guðmundur Stefánsson, Andrea S.J. Lin, Suvrath Mahadevan, Christina Hedges, and Natasha E. Batalha
Figure caption: The water inventory for planets in our Monte Carlo atmospheric escape ensemble as a function of the assumed H2 escape efficiency. The circle size indicates the initial envelope mass as a fraction of the total planet mass. A red edge color for a given symbol denotes a scenario with less than 1 Earth ocean at present day, which would likely be short-lived (Kasting & Pollack 1983).
Paper: A Snowball in Hell: The Potential Steam Atmosphere of TOI-1266c
Authors: C. E. Harman, Ravi Kumar Kopparapu, Guðmundur Stefánsson, Andrea S.J. Lin, Suvrath Mahadevan, Christina Hedges, and Natasha E. Batalha
Figure caption: Molecular oxygen response to changing eddy diffusion profile strengths (values indicated in the key, with units of cm2 s−1) for the 10% H2 scenario. Smaller values of Kzz prevent photochemically produced O2 from being mixed down into the middle atmosphere, resulting in larger upper atmospheric concentrations at the expense of lower atmospheric concentrations.
Paper: A Snowball in Hell: The Potential Steam Atmosphere of TOI-1266c
Authors: C. E. Harman, Ravi Kumar Kopparapu, Guðmundur Stefánsson, Andrea S.J. Lin, Suvrath Mahadevan, Christina Hedges, and Natasha E. Batalha
Figure caption: The water vapor profiles for the scenarios outlined in the main text from the photochemical model (thick lines) compared with the water profiles produced by the radiative−convective model (thin lines). Differences between the two profiles are confined to the upper atmosphere (above ∼10 mbar) and do not produce more than a ∼5 ppm change in the resulting transmission spectra.
Paper: A Snowball in Hell: The Potential Steam Atmosphere of TOI-1266c
Authors: C. E. Harman, Ravi Kumar Kopparapu, Guðmundur Stefánsson, Andrea S.J. Lin, Suvrath Mahadevan, Christina Hedges, and Natasha E. Batalha
Figure caption: OH profiles for the cases seen in Figure 5, and sharing the same color palette.
Paper: Toward Detecting Polycyclic Aromatic Hydrocarbons on Planetary Objects with ORIGIN
Authors: K. A. Kipfer, N. F. W. Ligterink, J. Bouwman, L. Schwander, V. Grimaudo, C. P. de Koning, N. J. Boeren, P. Keresztes Schmidt, R. Lukmanov, M. Tulej, P. Wurz, and A. Riedo
Figure caption: Schematic drawing of the sample holder with its five cavities (left). A zoom of a single cavity (right) shows the analyte inhomogeneities in the sample (gray areas), which have been exaggerated to exemplify the purpose of averaging over the 40 positions. The blue points signify the laser pulses. Note that not all of the 40 positions are shown. The x and y directions for the orientation of the sample stage are indicated. In this sketch, the z direction points out of the plane of the paper.
Paper: Toward Detecting Polycyclic Aromatic Hydrocarbons on Planetary Objects with ORIGIN
Authors: K. A. Kipfer, N. F. W. Ligterink, J. Bouwman, L. Schwander, V. Grimaudo, C. P. de Koning, N. J. Boeren, P. Keresztes Schmidt, R. Lukmanov, M. Tulej, P. Wurz, and A. Riedo
Figure caption: Mass spectra of the four PAH species investigated in this campaign measured at a laser pulse energy of 4 μJ. From bottom to top, the PAHs displayed are coronene (C24H12, spectra shown in blue), perylene (C20H12, spectra shown in green), pyrene (C16H10, spectra shown in orange), and anthracene (C14H10, spectra shown in red). A concentration of 100 μM was used for all PAHs in this measurement. Prominent peaks are indicated in the plot. The spectra are normalized to the highest peak for the respective PAH and offset from each other. The structure of the PAHs is shown on the right side.
Paper: Toward Detecting Polycyclic Aromatic Hydrocarbons on Planetary Objects with ORIGIN
Authors: K. A. Kipfer, N. F. W. Ligterink, J. Bouwman, L. Schwander, V. Grimaudo, C. P. de Koning, N. J. Boeren, P. Keresztes Schmidt, R. Lukmanov, M. Tulej, P. Wurz, and A. Riedo
Figure caption: Mass spectra of pyrene, measured at a laser pulse energy of, from bottom to top, 1 (blue), 2 (green), 3 (orange), and 4 (red) μJ and with an average surface concentration of 14 pmol mm−2. A zoom on the area shaded in gray is provided in the right panel. The most abundant peak is indicated with its mass, and the spectra are offset from each other.
Paper: Toward Detecting Polycyclic Aromatic Hydrocarbons on Planetary Objects with ORIGIN
Authors: K. A. Kipfer, N. F. W. Ligterink, J. Bouwman, L. Schwander, V. Grimaudo, C. P. de Koning, N. J. Boeren, P. Keresztes Schmidt, R. Lukmanov, M. Tulej, P. Wurz, and A. Riedo
Figure caption: Normalized peak area of the parent peak for the four PAHs as a function of applied laser pulse energy. Displayed are perylene (black triangle), pyrene (red square), anthracene (blue circle), and coronene (green diamond). The standard error of 20% as explained in Section 2.4 has been added to the perylene measurement to indicate the magnitude and omitted from the other measurements for easier readability of the plot. Note that there has been no detection of a peak for anthracene at 1 μJ.
Paper: Toward Detecting Polycyclic Aromatic Hydrocarbons on Planetary Objects with ORIGIN
Authors: K. A. Kipfer, N. F. W. Ligterink, J. Bouwman, L. Schwander, V. Grimaudo, C. P. de Koning, N. J. Boeren, P. Keresztes Schmidt, R. Lukmanov, M. Tulej, P. Wurz, and A. Riedo
Figure caption: Mass spectra of pyrene for a series of concentrations measured at a fixed laser pulse energy of 3 μJ. From bottom to top, the concentrations are 1 (blue), 10 (green), 100 (orange), 1000 (red), and 5000 (purple) μM. A zoom on the area shaded in gray is provided in the right panel. A clear transition from the parent peak at m/z = 202 for low concentrations to m/z = 203 for high concentrations is visible. The structure is shown in the top right corner of the left panel, and the spectra are offset from each other.
Paper: Toward Detecting Polycyclic Aromatic Hydrocarbons on Planetary Objects with ORIGIN
Authors: K. A. Kipfer, N. F. W. Ligterink, J. Bouwman, L. Schwander, V. Grimaudo, C. P. de Koning, N. J. Boeren, P. Keresztes Schmidt, R. Lukmanov, M. Tulej, P. Wurz, and A. Riedo
Figure caption: Concentration scan measured for perylene at a laser pulse energy of 3 μJ. From bottom to top, the concentrations used are 5 (blue), 10 (green), 50 (orange), and 100 (red) μM. The areas shaded in gray in the left panel are shown in the right panels, providing a zoom on the parent peak of perylene at m/z = 252 and on the masses around m/z = 500. To see the structure of the masses around m/z = 500, the data for 5 and 10 μM are multiplied by a factor of 4 in the right panel. The structure of perylene is shown in the left panel, and the spectra are offset from each other.
Paper: Toward Detecting Polycyclic Aromatic Hydrocarbons on Planetary Objects with ORIGIN
Authors: K. A. Kipfer, N. F. W. Ligterink, J. Bouwman, L. Schwander, V. Grimaudo, C. P. de Koning, N. J. Boeren, P. Keresztes Schmidt, R. Lukmanov, M. Tulej, P. Wurz, and A. Riedo
Figure caption: Normalized peak area for the PAHs as a function of concentration. The PAHs shown are perylene (black triangle), anthracene (blue circle), and pyrene (red square). The error bar has been added for perylene to exemplify the magnitude of the error and has been omitted from the other PAHs for clarity.
Paper: Toward Detecting Polycyclic Aromatic Hydrocarbons on Planetary Objects with ORIGIN
Authors: K. A. Kipfer, N. F. W. Ligterink, J. Bouwman, L. Schwander, V. Grimaudo, C. P. de Koning, N. J. Boeren, P. Keresztes Schmidt, R. Lukmanov, M. Tulej, P. Wurz, and A. Riedo
Figure caption: The LOD for the different PAHs calculated as a function of concentration at a fixed applied pulse energy of 3 μJ (left) and of pulse energy using a fixed concentration of 100 μM (right). The PAHs shown are perylene (black triangle), pyrene (red square), anthracene (blue circle), and coronene (green star). The error bar has been added for one PAH in both plots to show the magnitude of the error and has been omitted from the other measurements for readability of the plot. It should be noted that for anthracene, no peak has been detected at m/z = 178 for a laser energy of 1 μJ.
Paper: Toward Detecting Polycyclic Aromatic Hydrocarbons on Planetary Objects with ORIGIN
Authors: K. A. Kipfer, N. F. W. Ligterink, J. Bouwman, L. Schwander, V. Grimaudo, C. P. de Koning, N. J. Boeren, P. Keresztes Schmidt, R. Lukmanov, M. Tulej, P. Wurz, and A. Riedo
Figure caption: Absorption spectra in the UV of anthracene (blue dotted), pyrene (green dashed), perylene (orange solid), and coronene (red dashed–dotted) recorded as a solution in cyclohexane. The wavelength of the laser (266 nm) used in this measurement campaign is indicated by a gray dashed line. The spectra of perylene, anthracene, and pyrene have been retrieved from the PhotochemCAD database and the data for the spectrum of coronene as a solution in cyclohexane from Ehrenfreund et al. (1992).