adsabs/AstroCLIMB huggingface dataset:
Paper: Determinations of Asteroid Masses Using Mutual Encounters Observed in the Legacy Survey of Space and Time
Authors: Gary M. Bernstein, Negin Najafi, Daniel C. H. Gomes
Figure caption: Each plot gives information about the uncertainty σI on the applied impulse that is forecasted for observations of each individual tracer MBA of a mutual encounter. The columns assume progressively more information available from pre-LSST data about the tracers’ initial state vectors and Yarkovsky accelerations when going from left to right, as denoted in the text atop each column. The top row of plots is a scatter diagram (red dots) of σI vs. the apparent magnitude of the tracer; the black dots trace the mean vs. apparent magnitude. The middle panels give the distribution of the apparent magnitudes of those tracers that determine their deflectors’ masses with S/N > 3, i.e., the distribution of apparent magnitudes of the useful tracers. The bottom panels plot the distributions of σI for tracers of various magnitudes.
Paper: Determinations of Asteroid Masses Using Mutual Encounters Observed in the Legacy Survey of Space and Time
Authors: Gary M. Bernstein, Negin Najafi, Daniel C. H. Gomes
Figure caption: Histogram of the number of MBAs that are forecasted to attain S/N > 10 or S/N > 5 measurements of their masses by the use of LSST astrometry on tracer asteroids. The filled histograms assume that pre-LSST data establish the initial state vectors of the tracer MBAs. The open histograms show the conservative limit when only LSST observations are used. The left and right panels show results from assuming low-M/L and high-M/L asteroids, respectively. In each case, the mass census is nearly complete to some H value, and we forecast S/N > 5 mass measures for individual MBAs up to ≈4 mag fainter than the completion point enabled by unusually fortunate close encounters with known MBAs.
Paper: Determinations of Asteroid Masses Using Mutual Encounters Observed in the Legacy Survey of Space and Time
Authors: Gary M. Bernstein, Negin Najafi, Daniel C. H. Gomes
Figure caption: The distribution of forecasted σM, the uncertainty on the mass of the deflector, is plotted for all of the 725 MBA deflectors with H < 10. The dashed–dotted black histogram is the “LSST-only” case, the solid red histogram assumes that pre-LSST data strongly constrain the initial state vector of the tracer, and the dashed blue histogram shows what happens if the Yarkovsky coefficient A2 is also known precisely. Along the top are marked the ranges of σM needed to obtain a 5σ detection of the masses of MBAs at different H values, assuming our low-to-high range of possible masses at a given H.
Paper: Formation of Ammonium Nitrate Particles in CO2-rich Atmospheres
Authors: Antonio Jiménez-Escobar, Angela Ciaravella, Alfonso Mangione, Cesare Cecchi-Pestellini, Francesco Piazzese, Roberto Candia, Gaspare Di Cicca, Salvatore Varisco
Figure caption: Chemical evolution of pure carbon dioxide gas during electric discharge. Left: vacuum ultraviolet spectra at different times, with the effective elapsed discharge time indicated for each spectrum. For comparison, the top section shows the carbon dioxide absorption spectrum at 1 mbar (black), the spectrum after 10.5 minutes of discharge processing (yellow), and for comparison, the UV spectrum of CO (green). Right: mass spectra of carbon dioxide (m/z = 44) and discharge products (m/z = 12, 16, 28, 32 amu) as a function of processing time. All masses are normalized to the initial value of m/z = 44. The vertical orange stripes indicate the discharge steps.
Paper: Formation of Ammonium Nitrate Particles in CO2-rich Atmospheres
Authors: Antonio Jiménez-Escobar, Angela Ciaravella, Alfonso Mangione, Cesare Cecchi-Pestellini, Francesco Piazzese, Roberto Candia, Gaspare Di Cicca, Salvatore Varisco
Figure caption: Chemical evolution of pure ammonia gas during electric discharge. Left: vacuum ultraviolet spectra at different times, with the effective elapsed discharge time indicated for each spectrum. For comparison, the top section shows the ammonia absorption spectrum at 1 mbar (black) and the spectrum after 10.5 minutes of discharge processing (yellow). Right: mass spectra of ammonia (m/z = 17) and discharge products (m/z = 1, 2, 14, 28, 29 amu) as a function of processing time. All masses are normalized to the initial value of m/z = 17. The vertical orange stripes indicate the discharge steps.
Paper: Formation of Ammonium Nitrate Particles in CO2-rich Atmospheres
Authors: Antonio Jiménez-Escobar, Angela Ciaravella, Alfonso Mangione, Cesare Cecchi-Pestellini, Francesco Piazzese, Roberto Candia, Gaspare Di Cicca, Salvatore Varisco
Figure caption: The left panel presents a true-color image of a ZnSe window, while the central panel shows the solid substance deposited onto the cooled ZnSe window. The right panel displays the infrared absorbance of this material (black line) as a function of both wavenumber (cm−1 and wavelength (μm)). For comparison, the red line represents the infrared spectrum of ammonium nitrate (NH4NO3, phase IV, stable between 213 and 323 K) from A. Théorêt & C. Sandorfy (1964) over the same spectral range. Labels indicate the wavenumbers and their corresponding spectroscopic assignments.
Paper: Formation of Ammonium Nitrate Particles in CO2-rich Atmospheres
Authors: Antonio Jiménez-Escobar, Angela Ciaravella, Alfonso Mangione, Cesare Cecchi-Pestellini, Francesco Piazzese, Roberto Candia, Gaspare Di Cicca, Salvatore Varisco
Figure caption: Chemical evolution of 20 mbar binary-gas mixture containing a (10:1) ratio of CO2 and NH3 during the electric discharge. Left: vacuum ultraviolet spectra at different times, with the effective elapsed discharge time indicated for each spectrum. For comparison, the top section shows the ammonia, the CO2, and the CO2:NH3 mixture after 10.5 minutes of discharge processing. Right: mass spectra of the mixture in which all the masses are normalized to the initial value of m/z = 44. The vertical orange stripes indicate the discharge steps.
Paper: Formation of Ammonium Nitrate Particles in CO2-rich Atmospheres
Authors: Antonio Jiménez-Escobar, Angela Ciaravella, Alfonso Mangione, Cesare Cecchi-Pestellini, Francesco Piazzese, Roberto Candia, Gaspare Di Cicca, Salvatore Varisco
Figure caption: Mass spectra of the solid residue deposited onto the ZnSe window (black bars). The green bars represent the results of the blank experiment.
Paper: Formation of Ammonium Nitrate Particles in CO2-rich Atmospheres
Authors: Antonio Jiménez-Escobar, Angela Ciaravella, Alfonso Mangione, Cesare Cecchi-Pestellini, Francesco Piazzese, Roberto Candia, Gaspare Di Cicca, Salvatore Varisco
Figure caption: Ultraviolet emission spectrum of CO2:NH3 gas mixture in the 250−380 nm range.
Paper: Unoccupied Aircraft Systems Sampling for Earth and Mars
Authors: Colin Chen, Christopher W. Hamilton, Christian Sipe, Kathryn Bywaters, Justin Lawrence, Paul Creekmore, Nicklaus Traeden, Kris Zacny
Figure caption: Scoop sampler tests around the Poleta Folds, including ((a) and (b)) fine-grained sampling and ((c) and (d)) cobble sampling.
Paper: DART-scale Impacts into a Complex Low-strength Target: Insights into Asteroid Dimorphos’s Interior from Simulations
Authors: Cem Berk Senel, Robert Luther, Özgür Karatekin, Gareth S. Collins, Steven Goderis, Philippe Claeys
Figure caption: Sensitivity analysis of the fast-time integration to the hand-off time, th. The time evolution of (a–c) the momentum enhancement factor (β) and (d–f) the crater diameter are presented for th = 0.05, 0.1, and 0.5 s. Vertical dashed lines show the corresponding hand-off times. Purple dashed and light-blue dotted lines represent simulations with and without fast-time integration, respectively.
Paper: DART-scale Impacts into a Complex Low-strength Target: Insights into Asteroid Dimorphos’s Interior from Simulations
Authors: Cem Berk Senel, Robert Luther, Özgür Karatekin, Gareth S. Collins, Steven Goderis, Philippe Claeys
Figure caption: The time evolution of the simulated (a) momentum enhancement factor, β, and (b) crater diameter from DART-scale impacts on a curved asteroid featuring a homogeneous interior (case 02: Y0 = 1 Pa, f = 0.50, ϕ = 30%) with (purple solid line) or without (light-blue solid line) a fast-time integration approach.
Paper: DART-scale Impacts into a Complex Low-strength Target: Insights into Asteroid Dimorphos’s Interior from Simulations
Authors: Cem Berk Senel, Robert Luther, Özgür Karatekin, Gareth S. Collins, Steven Goderis, Philippe Claeys
Figure caption: The bulk modulus, A, reduction in steps at specified times after transition timescale, i.e., t = 0.5, 1.0, 2.0, 30, 35 s post-impact. The light-blue dashed and dark-blue solid lines depict the simulation results for no fast-time integration vs. fast-time integration activated, respectively.
Paper: Determinations of Asteroid Masses Using Mutual Encounters Observed in the Legacy Survey of Space and Time
Authors: Gary M. Bernstein, Negin Najafi, Daniel C. H. Gomes
Figure caption: The mass-to-light ratio M10 defined in Equation (2) is plotted vs. absolute magnitude H for all MBAs in the SSODNET database (J. Berthier et al. 2023) with mass measurements accurate to 20% or better. For our forecasts, we will consider the two values of M10 marked by the horizontal lines labeled “low M/L” and “high M/L.”
Paper: Architecture and Field Operation of a Portable Digital Holographic Microscope for In Situ Measurements of Bacterial Motility
Authors: J. Kent Wallace, Manuel Bedrossian, Stephanie Rider, Dylan McKeithen, Felipe Fregoso, Frank Loya, Scott M. Perl
Figure caption: The microfluidic sample chamber is a composition of a few key simple elements. It comprises the following (left): 1: bottom substrate, 18 mm × 40 mm × 1 mm float glass; 2: acetate layer with the microfluidic channels; 3: upper window, 18 mm wide × 22 mm long × 1 mm thick float glass; 4: interface plate with through holes for the microfluidic channels; 5: barbs for interface to microfluidic sources. On the right is shown the science and reference beam fields of view overlaid onto the sample chamber channels. The light gray boxes indicate the alignment tolerances for the sample chamber in the instrument, which is approximately 2.5 mm × 5.0 mm.
Paper: Architecture and Field Operation of a Portable Digital Holographic Microscope for In Situ Measurements of Bacterial Motility
Authors: J. Kent Wallace, Manuel Bedrossian, Stephanie Rider, Dylan McKeithen, Felipe Fregoso, Frank Loya, Scott M. Perl
Figure caption: The key functions of the electronics are illustrated above in the functional block diagram. The custom electronics card serves as the interface between the instrument control buttons and status LEDs (located on the outside of the enclosure) and the internal lithium-ion battery. Power is distributed to the laser diode driver electronics and the UDOO computer. The UDOO interfaces to the imaging array via a power-over-USB3 cable. An external Ethernet port allows for direct communication to the computer via a cabled connection.
Paper: Architecture and Field Operation of a Portable Digital Holographic Microscope for In Situ Measurements of Bacterial Motility
Authors: J. Kent Wallace, Manuel Bedrossian, Stephanie Rider, Dylan McKeithen, Felipe Fregoso, Frank Loya, Scott M. Perl
Figure caption: The instrument is rendered above. The optical side is on the left, the electrical side is on the right.
Paper: Architecture and Field Operation of a Portable Digital Holographic Microscope for In Situ Measurements of Bacterial Motility
Authors: J. Kent Wallace, Manuel Bedrossian, Stephanie Rider, Dylan McKeithen, Felipe Fregoso, Frank Loya, Scott M. Perl
Figure caption: Optical layout of the holographic microscope. Equipment details: 1: input single-mode fiber; 2: source collimating lens; 3: glass sample chamber; 4: objective lens pair; 5: fold mirrors; 6: tube lens; 7: array detector.
Paper: Architecture and Field Operation of a Portable Digital Holographic Microscope for In Situ Measurements of Bacterial Motility
Authors: J. Kent Wallace, Manuel Bedrossian, Stephanie Rider, Dylan McKeithen, Felipe Fregoso, Frank Loya, Scott M. Perl
Figure caption: The instrument is photographed from its two sides above. The optical side is on the left, and the electrical side is on the right.
Paper: Effects of the 2018 Martian Global Dust Storm on Boundary Positions in the Induced Magnetosphere
Authors: Catherine E. Regan, Andrew J. Coates, Mark Lester, Anne Wellbrock, Geraint H. Jones, Beatriz Sánchez-Cano, Philippe Garnier, Louisa J. Preston, František Němec, Václav Linzmayer, Rudy A. Frahm, Mats Holmström
Figure caption: Results for the bow shock (a)–(c) and induced magnetospheric boundary (d)–(f) across the Martian surface for all dayside crossings of MAVEN and Mars Express from 2018 April 1 to November 30, in 10°×10° bins. (a), (d) Mean fitted terminator distance from Equation (1); (b), (e) normalized (to r2.02) mean fitted terminator distance, considering the changing Mars–Sun distance and dynamic pressure; (c), (f) number of boundary crossings within each bin. Base map of the Martian topography for reference to surface features. Topography obtained by the Mars Global Surveyor’s Mars Orbiter Laser Altimeter digital elevation model (USGS 2023).
Paper: Effects of the 2018 Martian Global Dust Storm on Boundary Positions in the Induced Magnetosphere
Authors: Catherine E. Regan, Andrew J. Coates, Mark Lester, Anne Wellbrock, Geraint H. Jones, Beatriz Sánchez-Cano, Philippe Garnier, Louisa J. Preston, František Němec, Václav Linzmayer, Rudy A. Frahm, Mats Holmström
Figure caption: Mean corrected terminator distance of the IMB, calculated for each 20° longitude interval with a latitude limited to −80° to −30°, split into three stages of dust development as outlined in Table 3, with error bars as standard deviation plotted over the radial component of the magnetic field at 400 km altitude for this latitude range from the Gao model (J. W. Gao et al. 2021).
Paper: Effects of the 2018 Martian Global Dust Storm on Boundary Positions in the Induced Magnetosphere
Authors: Catherine E. Regan, Andrew J. Coates, Mark Lester, Anne Wellbrock, Geraint H. Jones, Beatriz Sánchez-Cano, Philippe Garnier, Louisa J. Preston, František Němec, Václav Linzmayer, Rudy A. Frahm, Mats Holmström
Figure caption: Positions of boundary crossings of MAVEN and MEx from 2018 April 1 to November 30 for the (a) bow shock and (b) induced magnetospheric boundary. Plotted over the radial crustal magnetic field strength at 400 km altitude, given by the Gao model (J. W. Gao et al. 2021).
Paper: Effects of the 2018 Martian Global Dust Storm on Boundary Positions in the Induced Magnetosphere
Authors: Catherine E. Regan, Andrew J. Coates, Mark Lester, Anne Wellbrock, Geraint H. Jones, Beatriz Sánchez-Cano, Philippe Garnier, Louisa J. Preston, František Němec, Václav Linzmayer, Rudy A. Frahm, Mats Holmström
Figure caption: Mean corrected terminator distance of the bow shock, calculated for each 20° longitude interval with latitude limited to −80° to −60°, and error bars of standard deviation plotted over the radial component of the magnetic field at 400 km altitude for this latitude range from the Gao model (J. W. Gao et al. 2021).
Paper: Effects of the 2018 Martian Global Dust Storm on Boundary Positions in the Induced Magnetosphere
Authors: Catherine E. Regan, Andrew J. Coates, Mark Lester, Anne Wellbrock, Geraint H. Jones, Beatriz Sánchez-Cano, Philippe Garnier, Louisa J. Preston, František Němec, Václav Linzmayer, Rudy A. Frahm, Mats Holmström
Figure caption: Possible cause of the depression in the induced magnetospheric boundary over crustal fields seen during global dust storms.
Paper: Effects of the 2018 Martian Global Dust Storm on Boundary Positions in the Induced Magnetosphere
Authors: Catherine E. Regan, Andrew J. Coates, Mark Lester, Anne Wellbrock, Geraint H. Jones, Beatriz Sánchez-Cano, Philippe Garnier, Louisa J. Preston, František Němec, Václav Linzmayer, Rudy A. Frahm, Mats Holmström
Figure caption: Rolling mean of the fitted and corrected terminator distance, RTD, for the bow shock. Mean calculated every 50 days in 25 day steps from 2018 April 1 to November 30, with error bars of the standard deviation.
Paper: Effects of the 2018 Martian Global Dust Storm on Boundary Positions in the Induced Magnetosphere
Authors: Catherine E. Regan, Andrew J. Coates, Mark Lester, Anne Wellbrock, Geraint H. Jones, Beatriz Sánchez-Cano, Philippe Garnier, Louisa J. Preston, František Němec, Václav Linzmayer, Rudy A. Frahm, Mats Holmström
Figure caption: Rolling mean of the fitted and normalized terminator distance, RTD, for the IMB. Mean calculated every 50 days in 25 day steps from 2018 April 1 to November 30, with error bars showing the standard deviation.
Paper: JWST Reveals Spectral Tracers of Recent Surface Modification on Europa
Authors: Richard J. Cartwright, Charles A. Hibbitts, Bryan J. Holler, Ujjwal Raut, Tom A. Nordheim, Marc Neveu, Silvia Protopapa, Christopher R. Glein, Erin J. Leonard, Lorenz Roth, Chloe B. Beddingfield, Geronimo L. Villanueva
Figure caption: Left: band depth measurements for the 4.38 μm band (>3σ detection, also shown in Figure 5). White polygons show the locations of JWST/NIRSpec spaxels incorporated into the regional spectra shown on the right: (1) Tara Regio (red), (2) Powys Regio (purple), (3) northern low latitudes (blue), and their 1σ uncertainties (gray error bars). These data are normalized to 1 at 4.0 μm and offset vertically for clarity. The central wavelengths (μm) for detected solid-state CO2 features are listed vertically along each dotted line.
Paper: JWST Reveals Spectral Tracers of Recent Surface Modification on Europa
Authors: Richard J. Cartwright, Charles A. Hibbitts, Bryan J. Holler, Ujjwal Raut, Tom A. Nordheim, Marc Neveu, Silvia Protopapa, Christopher R. Glein, Erin J. Leonard, Lorenz Roth, Chloe B. Beddingfield, Geronimo L. Villanueva
Figure caption: Spaxel maps displaying the ratios between Europa’s 3.1 μm Fresnel region and its 1.65 μm band (3.1 μm region/1.65 μm band), generated with the spectral contrast and area measurements shown in Figures 3 and 4. These ratio maps highlight the dissimilar trends in the distribution of crystalline H2O ice on Europa, with the 1.65 μm band stronger at northern latitudes and the 3.1 μm Fresnel region stronger at southern latitudes, particularly in Tara and Powys Regiones. This dissimilarity points to vertical stratification of H2O ice in Europa’s regolith, with more exposed crystalline H2O ice at southern latitudes. The spatial extents of large-scale geologic units on Europa’s leading and anti-Jovian sides, including Tara (10°S, 75°W) and Powys (0°, 145°W) Regiones, are indicated and described in the included legend (see E. J. Leonard et al. 2024).
Paper: Multiwavelength JWST Observations of (3200) Phaethon Show a Dehydrated Object with an Aqueously Altered Origin
Authors: Cristina A. Thomas, Andrew S. Rivkin, Ian Wong, Matthew M. Knight, Sean E. Marshall, Christopher W. Haberle, Aidan Madden-Watson, Joshua P. Emery, Annika Gustafsson, Stefanie N. Milam, Heidi B. Hammel, Ellen S. Howell, Ronald J. Vervack
Figure caption: Simulated views of Phaethon as seen from Spitzer and JWST during the mid-infrared spectral observations . The plane-of-sky orientations and the shape model are the same as in Figure 1. The three MIRI views are at the start of the MIRI observation, mid-observation, and at the end of the observation sequence.
Paper: Multiwavelength JWST Observations of (3200) Phaethon Show a Dehydrated Object with an Aqueously Altered Origin
Authors: Cristina A. Thomas, Andrew S. Rivkin, Ian Wong, Matthew M. Knight, Sean E. Marshall, Christopher W. Haberle, Aidan Madden-Watson, Joshua P. Emery, Annika Gustafsson, Stefanie N. Milam, Heidi B. Hammel, Ellen S. Howell, Ronald J. Vervack
Figure caption: Simulated views of Phaethon as seen from JWST during the NIRSpec and NIRCam observations (S. E. Marshall et al. 2025, in preparation). In these plane-of-sky views, north is up and east is to the left. The magenta arrow is the spin axis (as defined by the right-hand rule; shortest principal axis) with the arrow pointing to the north pole, and the red and green shafts are the long and intermediate principal axes, respectively.
Paper: Multiwavelength JWST Observations of (3200) Phaethon Show a Dehydrated Object with an Aqueously Altered Origin
Authors: Cristina A. Thomas, Andrew S. Rivkin, Ian Wong, Matthew M. Knight, Sean E. Marshall, Christopher W. Haberle, Aidan Madden-Watson, Joshua P. Emery, Annika Gustafsson, Stefanie N. Milam, Heidi B. Hammel, Ellen S. Howell, Ronald J. Vervack
Figure caption: Final NIRSpec spectrum of Phaethon with the reflected and thermal flux (red triangles) and with the thermal flux removed (black crosses).
Paper: Multiwavelength JWST Observations of (3200) Phaethon Show a Dehydrated Object with an Aqueously Altered Origin
Authors: Cristina A. Thomas, Andrew S. Rivkin, Ian Wong, Matthew M. Knight, Sean E. Marshall, Christopher W. Haberle, Aidan Madden-Watson, Joshua P. Emery, Annika Gustafsson, Stefanie N. Milam, Heidi B. Hammel, Ellen S. Howell, Ronald J. Vervack
Figure caption: Final MIRI emissivity spectrum of Phaethon. We note the documented spectral leak at ∼12.2 μm as a gray line and the edges of sub-band 3B as gold bands. We use this artifact labeling methodology in subsequent figures.
Paper: Multiwavelength JWST Observations of (3200) Phaethon Show a Dehydrated Object with an Aqueously Altered Origin
Authors: Cristina A. Thomas, Andrew S. Rivkin, Ian Wong, Matthew M. Knight, Sean E. Marshall, Christopher W. Haberle, Aidan Madden-Watson, Joshua P. Emery, Annika Gustafsson, Stefanie N. Milam, Heidi B. Hammel, Ellen S. Howell, Ronald J. Vervack
Figure caption: Final NIRSpec reflectance spectrum of Phaethon. We compare the data to a ground-based near-infrared spectrum from the MITHNEOS survey (run “sp238”; R. Binzel et al. 2019). Both spectra are normalized to unity at 1.0 μm. The two spectra show similar slopes and spectral shape in their common wavelength regions.
Paper: Multiwavelength JWST Observations of (3200) Phaethon Show a Dehydrated Object with an Aqueously Altered Origin
Authors: Cristina A. Thomas, Andrew S. Rivkin, Ian Wong, Matthew M. Knight, Sean E. Marshall, Christopher W. Haberle, Aidan Madden-Watson, Joshua P. Emery, Annika Gustafsson, Stefanie N. Milam, Heidi B. Hammel, Ellen S. Howell, Ronald J. Vervack
Figure caption: We compare the 3 μm region of our NIRSpec data to Ryugu using in situ Hayabusa2 observations (M. Matsuoka et al. 2023) and laboratory data of the returned sample (T. Nakamura et al. 2022). Ryugu is clearly more hydrated than Phaethon.
Paper: Multiwavelength JWST Observations of (3200) Phaethon Show a Dehydrated Object with an Aqueously Altered Origin
Authors: Cristina A. Thomas, Andrew S. Rivkin, Ian Wong, Matthew M. Knight, Sean E. Marshall, Christopher W. Haberle, Aidan Madden-Watson, Joshua P. Emery, Annika Gustafsson, Stefanie N. Milam, Heidi B. Hammel, Ellen S. Howell, Ronald J. Vervack
Figure caption: We compare the 3 μm region of our NIRSpec data to a ground-based observation from D. Takir et al. (2020). We confirm the lack of absorption band in these wavelengths.
Paper: Multiwavelength JWST Observations of (3200) Phaethon Show a Dehydrated Object with an Aqueously Altered Origin
Authors: Cristina A. Thomas, Andrew S. Rivkin, Ian Wong, Matthew M. Knight, Sean E. Marshall, Christopher W. Haberle, Aidan Madden-Watson, Joshua P. Emery, Annika Gustafsson, Stefanie N. Milam, Heidi B. Hammel, Ellen S. Howell, Ronald J. Vervack
Figure caption: Our analysis shows that Phaethon is most similar to the CM Murchison sample heated to 1000°C. For clarity on the positions of the spectral features, the spectra for Phaethon and Y-86720 are scaled by a factor of 0.6, and all other spectra are scaled by a factor of 1.3 before being offset in emissivity.