adsabs/AstroCLIMB huggingface dataset:
Paper: Estimate of Water and Hydroxyl Abundance on Asteroid (16) Psyche from JWST Data
Authors: Stephanie G. Jarmak, Tracy M. Becker, Charles E. Woodward, Casey I. Honniball, Andrew S. Rivkin, Margaret M. McAdam, Zoe A. Landsman, Saverio Cambioni, Thomas G. Müller, Driss Takir, Kurt D. Retherford, Anicia Arredondo, Linda T. Elkins-Tanton
Figure caption: Relative normalized reflectance spectrum of Psyche near 1.34 μm. Binned spectra are binned to 1 nm.
Paper: LunaIcy: Exploring Europa’s Icy Surface Microstructure through Multiphysics Simulations
Authors: Cyril Mergny, Frédéric Schmidt
Figure caption: Sintering efficiency heat map for the top layer as a function of porosity and albedo. Colors indicate the ratio of the top-layer bond radius after 1 million yr r b(t = t f) to the initial bond radius r b(t = 0). In the majority of scenarios, the bond radius more than doubles after 1 million yr, except for very high albedo.
Paper: LunaIcy: Exploring Europa’s Icy Surface Microstructure through Multiphysics Simulations
Authors: Cyril Mergny, Frédéric Schmidt
Figure caption: Top-layer grain and bond radius evolution over 1 million yr in a warm simulation scenario with a porosity of ϕ = 0.8 and an albedo of A = 0.4, resulting in a mean temperature of 114 K and a maximum daily temperature of 141 K. The bond radius has increased by 59 times its initial value, leading to significant changes in the thermal, mechanical, and optical properties of the ice.
Paper: LunaIcy: Exploring Europa’s Icy Surface Microstructure through Multiphysics Simulations
Authors: Cyril Mergny, Frédéric Schmidt
Figure caption: Evolution of the top-layer relative bond radius r b/r g for different initial grain radius r g(t = 0). Smaller grains show more efficient sintering due to their higher surface curvature. In situations of intense sintering, numerical instabilities start to appear after reaching a critical threshold r b > 0.6r g.
Paper: LunaIcy: Exploring Europa’s Icy Surface Microstructure through Multiphysics Simulations
Authors: Cyril Mergny, Frédéric Schmidt
Figure caption: Block diagram of the proposed multiphysics simulation model LunaIcy.
Paper: LunaIcy: Exploring Europa’s Icy Surface Microstructure through Multiphysics Simulations
Authors: Cyril Mergny, Frédéric Schmidt
Figure caption: Bond radius vs. depth after 1 million yr of sintering with an albedo of A = 0.4 and a porosity of ϕ = 0.8. The initial bond radius, r b(x, 0) ≈ 0.4 μm, is indicated by a blue dashed line for reference. Significant sintering is observed up to the diurnal thermal skin depth.
Paper: Evidence for Surprising Heavy Nitrogen Isotopic Enrichment in Comet 46P/Wirtanen’s Hydrogen Cyanide
Authors: M. A. Cordiner, K. Darnell, D. Bockelée-Morvan, N. X. Roth, N. Biver, S. N. Milam, S. B. Charnley, J. Boissier, B. P. Bonev, C. Qi, J. Crovisier, A. J. Remijan
Figure caption: Nitrogen isotope measurements in primitive solar system materials, expressed as 14N/15N (lower x-axis, with smaller values indicating greater 15N enrichment toward the right); the fractional isotopic enrichment δ 15N is shown on the upper x-axis. This figure was adapted from D. Bockelee-Morvan et al. (2015). The meteoritic bulk value is from CR chondrite insoluble organic matter (IOM) measurements (H. Nomura et al. 2023), while the 15N hot spots are regions that present strong isotopic enrichments relative to the surrounding meteoritic material. Gray ellipses represent the range of values from multiple laboratory sample analysis measurements. The CN, HCN, and NH2 measurements in cometary gases are the averages from D. Bockelée-Morvan et al. (2008), J. Manfroid et al. (2009), Y. Shinnaka et al. (2016), and N. Biver et al. (2016). 67P values are from K. Altwegg et al. (2019), and the 46P CN value is from Y. Moulane et al. (2023).
Paper: Evidence for Surprising Heavy Nitrogen Isotopic Enrichment in Comet 46P/Wirtanen’s Hydrogen Cyanide
Authors: M. A. Cordiner, K. Darnell, D. Bockelée-Morvan, N. X. Roth, N. Biver, S. N. Milam, S. B. Charnley, J. Boissier, B. P. Bonev, C. Qi, J. Crovisier, A. J. Remijan
Figure caption: ALMA ACA spectra of HCN, H13CN, and HC15N in comet 46P/Wirtanen, extracted from the central position(s) shown in Figure 1. Best-fitting SUBLIME radiative transfer models (including hyperfine structure) are overlaid in orange. The 3σ feature in the HC15N spectrum around −5 km s−1 is interpreted as an unusually strong (>3σ) noise spike.
Paper: Evidence for Surprising Heavy Nitrogen Isotopic Enrichment in Comet 46P/Wirtanen’s Hydrogen Cyanide
Authors: M. A. Cordiner, K. Darnell, D. Bockelée-Morvan, N. X. Roth, N. Biver, S. N. Milam, S. B. Charnley, J. Boissier, B. P. Bonev, C. Qi, J. Crovisier, A. J. Remijan
Figure caption: ALMA ACA maps of spectrally integrated HCN, H13CN, and HC15N emission from comet 46P/Wirtanen. Contour intervals are in units of 5σ for HCN and 1σ for H13CN and HC15N. Beam size (angular resolution) is shown in the lower left; sky-projected comet–Sun vectors are shown in the lower right. The HCN map is centered on the emission peak, whereas the H13CN and HC15N maps are centered on the stronger (simultaneously observed) CH3OH emission peak (not shown).
Paper: Evidence for Surprising Heavy Nitrogen Isotopic Enrichment in Comet 46P/Wirtanen’s Hydrogen Cyanide
Authors: M. A. Cordiner, K. Darnell, D. Bockelée-Morvan, N. X. Roth, N. Biver, S. N. Milam, S. B. Charnley, J. Boissier, B. P. Bonev, C. Qi, J. Crovisier, A. J. Remijan
Figure caption: ALMA ACA spectrum of CH3OH observed in comet 46P/Wirtanen (extracted from the CH3OH spectrally integrated brightness peak). Best-fitting SUBLIME radiative transfer model is overlaid in orange, demonstrating a gas kinetic temperature of T kin = 93 ± 3 K.
Paper: Simulated Solar-wind-induced Space Weathering of Olivine Powders: Spectral Alterations in the Ultraviolet, Visible, and Near-infrared
Authors: Camilo Jaramillo-Correa, Neil C. Pearson, Deborah Domingue, Daniel W. Savin, Roger N. Clark, Faith Vilas, Amanda R. Hendrix
Figure caption: Alteration of the Vis–NIR spectral properties of olivine powder (<25 μm) under 1.2 keV helium ion irradiation. The irradiation was carried out in sequential steps with a fluence of 5.8 × 1017 ions cm−2 each, for a total ion fluence of 5.80 × 1018 ions cm−2. (a) Vis–NIR reflectance spectra collected before and after each irradiation step. (b) Reflectance ratios calculated by dividing the reflectance corresponding to each step by the reflectance of the pristine olivine sample (step 00). (c) Optical depth derived from the measured reflectance R given in (a).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Simulated Solar-wind-induced Space Weathering of Olivine Powders: Spectral Alterations in the Ultraviolet, Visible, and Near-infrared
Authors: Camilo Jaramillo-Correa, Neil C. Pearson, Deborah Domingue, Daniel W. Savin, Roger N. Clark, Faith Vilas, Amanda R. Hendrix
Figure caption: Slope–slope plot of the Vis–NIR slope (550–1640 nm) vs. the UV–Vis slope (300–400 nm) displaying the corresponding slopes of different S-type asteroids and ordinary chondrites (LL, L, and H) as well as the evolution of the spectral slope of the ion-irradiated olivine powders in this work (error bars are within the data points). Asteroid (top-half-filled symbols) and meteorite (bottom-half-filled symbols) data are taken from A. R. Hendrix & F. Vilas (2006). The purple arrow indicates the direction of the spectral slope evolution with increasing ion irradiation fluence reported in this work. The black arrow indicates the general direction of the slope–slope relationship with increasing space weathering timescales proposed by A. R. Hendrix & F. Vilas (2006).
Paper: Simulated Solar-wind-induced Space Weathering of Olivine Powders: Spectral Alterations in the Ultraviolet, Visible, and Near-infrared
Authors: Camilo Jaramillo-Correa, Neil C. Pearson, Deborah Domingue, Daniel W. Savin, Roger N. Clark, Faith Vilas, Amanda R. Hendrix
Figure caption: Alteration of the UV–Vis spectral characteristics of olivine powder (<25 μm) by 1.2 keV helium ion irradiation. (a) Absolute reflectance of the mineral recorded at ion fluence intervals of 5.8 × 1017 ions cm−2. (b) Reflectance ratio calculated by dividing the reflectance spectrum of each step by the spectrum corresponding to irradiation step 01. The ratio data in the 500–650 nm range are omitted due to artifacts discussed in the text.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Simulated Solar-wind-induced Space Weathering of Olivine Powders: Spectral Alterations in the Ultraviolet, Visible, and Near-infrared
Authors: Camilo Jaramillo-Correa, Neil C. Pearson, Deborah Domingue, Daniel W. Savin, Roger N. Clark, Faith Vilas, Amanda R. Hendrix
Figure caption: NIR slope of the Vis–NIR reflectance spectra of ion-irradiated olivine powder. The slopes plotted correspond to the slope of a straight line between the reflectance values at 700 and 2000 nm. The purple squares correspond to <25 μm olivine powder irradiated with 1.2 keV helium ions (this work). The blue dots correspond to <45 μm olivine powder irradiated with 4 keV helium ions from M. J. Loeffler et al. (2009). The He ion energy and sample grain size are specified in the legend.
Paper: Simulated Solar-wind-induced Space Weathering of Olivine Powders: Spectral Alterations in the Ultraviolet, Visible, and Near-infrared
Authors: Camilo Jaramillo-Correa, Neil C. Pearson, Deborah Domingue, Daniel W. Savin, Roger N. Clark, Faith Vilas, Amanda R. Hendrix
Figure caption: Experimental setup used for the preparation and irradiation of olivine powder with in situ UV–Vis–NIR reflectance spectroscopy. (a) Vacuum suitcase used to transport the samples from the glovebox to the experimental facility. (b) The IGNIS facility, where the irradiation and spectra collection were carried out. (c) Schematic of the IGNIS main chamber showing the main components used for this work. Components of the Vis–NIR reflectance setup are shown in red, where the solid and dashed line represent the incident and reflected light, respectively. The components shown in blue correspond to the UV–Vis reflectance setup, where the solid and dashed line represent the incident and reflected light, respectively. The solid pink arrows represent the ion beam.
Paper: Simulated Solar-wind-induced Space Weathering of Olivine Powders: Spectral Alterations in the Ultraviolet, Visible, and Near-infrared
Authors: Camilo Jaramillo-Correa, Neil C. Pearson, Deborah Domingue, Daniel W. Savin, Roger N. Clark, Faith Vilas, Amanda R. Hendrix
Figure caption: Feature shifting of the olivine absorption band and band shoulder caused by the ion irradiation. (a) Absolute value of the band shoulder and band center shifts with respect to the position on the pristine olivine spectrum. (b) The shoulder shifting is coupled with a reduction of the albedo as the ion fluence increases. The black arrow indicates the direction of increasing fluence.
Paper: Simulated Solar-wind-induced Space Weathering of Olivine Powders: Spectral Alterations in the Ultraviolet, Visible, and Near-infrared
Authors: Camilo Jaramillo-Correa, Neil C. Pearson, Deborah Domingue, Daniel W. Savin, Roger N. Clark, Faith Vilas, Amanda R. Hendrix
Figure caption: UV slope of the UV–Vis reflectance spectra of ion-irradiated olivine powder. The values plotted correspond to the slope of a straight line between the reflectance at 300 and 400 nm.
Paper: Simulated Solar-wind-induced Space Weathering of Olivine Powders: Spectral Alterations in the Ultraviolet, Visible, and Near-infrared
Authors: Camilo Jaramillo-Correa, Neil C. Pearson, Deborah Domingue, Daniel W. Savin, Roger N. Clark, Faith Vilas, Amanda R. Hendrix
Figure caption: Evolution of the 1050 nm band area of the olivine reflectance spectra as a function of ion fluence.
Paper: Detectability Simulations of a Near-infrared Surface Biosignature on Proxima Centauri b with Future Space Observatories
Authors: Connor O. Metz, Nancy Y. Kiang, Geronimo L. Villanueva, M. N. Parenteau, Vincent Kofman
Figure caption: Integration times required to achieve an SNR of 5 with LUVOIR-A and B, plotted as a function of ﹩\overline{{A}_{{\rm{bac}}}}﹩ and ﹩{A}_{{\rm{\max }}}﹩. ﹩{A}_{max}﹩ shows the peak value for the BVLO area coverage fraction/spectral dilution factor possible in any grid cell, whereas ﹩\overline{{A}_{{\rm{bac}}}}﹩ shows the global average coverage fraction/spectral dilution factor. The gray dashed line shows the detectability threshold criterion of 1000 hr. At intermediate abundances for the less opaque atmospheric scenarios (Control and Archean Low), the BVLO Qy feature is detectable in some tens of hours.
Paper: Detectability Simulations of a Near-infrared Surface Biosignature on Proxima Centauri b with Future Space Observatories
Authors: Connor O. Metz, Nancy Y. Kiang, Geronimo L. Villanueva, M. N. Parenteau, Vincent Kofman
Figure caption: Measured reflectance spectrum of B. viridis (dashed black) and scaled-up version of this spectrum with the Qy biosignature feature having similar contrast to the VRE (solid black). The latter is the base-case spectrum used to represent a high-density surface biosignature in this work, which is then linearly diluted in concentration in detectability simulations. Overplotted (red) is the dayside average incident starlight spectrum available the surface of the Control Proxima b concept, as modeled with PSG. The Qy feature overlaps with a large peak in incident radiation at the surface, which would make this pigment well adapted for photosynthesis on such an M-star-hosted planet.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Detectability Simulations of a Near-infrared Surface Biosignature on Proxima Centauri b with Future Space Observatories
Authors: Connor O. Metz, Nancy Y. Kiang, Geronimo L. Villanueva, M. N. Parenteau, Vincent Kofman
Figure caption: Simulated planetary reflectance spectra from PSG for all DG19 states at a phase of 270°, observed with LUVOIR-B. Plotted are (purple) the planetary spectra with the BVLO and (black) the planetary spectrum with the modified BVLO spectrum without the Qy feature. Noise is shown by orange error bars. One can see that the Qy absorbance feature decreases the spectral albedo in the 0.9–1.1 μm range. Spectra with ﹩{A}_{\max }=1﹩ are shown so as to best illustrate the spectral effect of the Qy feature. The integration time used for these spectra is that which would bring the overall SNR to 5 (values given in Figure 7). Note that the increase in noise longward of 1 μm is due to a transition to a HgCdTe detector.
Paper: Detectability Simulations of a Near-infrared Surface Biosignature on Proxima Centauri b with Future Space Observatories
Authors: Connor O. Metz, Nancy Y. Kiang, Geronimo L. Villanueva, M. N. Parenteau, Vincent Kofman
Figure caption: Integration times for Control at various distances, placed in orbit around a Sun-like star at 1 au. The biosignature is completely undetectable at 15 pc when using LUVOIR-B but feasibly detectable otherwise. a = 1 au was chosen because at distances farther than 1.3 pc, larger angular separation was needed than Proxima b has in reality (so that the planet is not blocked by the coronagraph), and a Sun-like star was chosen to be roughly climatologically consistent with the DG19 states.
Paper: Detectability Simulations of a Near-infrared Surface Biosignature on Proxima Centauri b with Future Space Observatories
Authors: Connor O. Metz, Nancy Y. Kiang, Geronimo L. Villanueva, M. N. Parenteau, Vincent Kofman
Figure caption: Array components of Equation (1), the function that generates BVLO abundance maps, shown for the dayside of the planet only. The 2D arrays are multiplied together to yield the BVLO abundance array, shown in the right-hand column. The color bar scale is for an ﹩{A}_{{\rm{\max }}}﹩ of 1 (the global dilution factor).
Paper: Detectability Simulations of a Near-infrared Surface Biosignature on Proxima Centauri b with Future Space Observatories
Authors: Connor O. Metz, Nancy Y. Kiang, Geronimo L. Villanueva, M. N. Parenteau, Vincent Kofman
Figure caption: Spectral confusion of methane and the Qy feature, shown for the Archean Low scenario. Top panel: (purple) the planetary spectrum for Archean Low is shown with the Qy feature (with noise, integration time of 1 hr). Also shown are (black) Archean Low without the Qy feature and (blue) Archean Low without the Qy feature but with extra methane. Adding extra methane mimics the Qy absorption feature around 1 μm. Bottom panel: (blue) signal from/spectral difference between Archean Low with Qy and Archean Low without Qy, plus extra methane, plotted alongside (black) the noise from Archean Low with Qy. For most of the spectral range, the difference would be undetectable at this integration time (meaning that the signal is less than the noise). However, the signal is greater than the noise around 0.87 μm, so the degeneracy could be broken by observing at this wavelength.
Paper: Detectability Simulations of a Near-infrared Surface Biosignature on Proxima Centauri b with Future Space Observatories
Authors: Connor O. Metz, Nancy Y. Kiang, Geronimo L. Villanueva, M. N. Parenteau, Vincent Kofman
Figure caption:                       ﹩f(T)﹩ and ﹩\left.f({\rm{PAR}}\right)﹩ plotted over the range of values that occur in this work. These functions are used calculate the parameters in Equation (1) at every grid cell to yield ﹩{A}_{{\rm{b}}{\rm{a}}{\rm{c}}}﹩.
Paper: Detectability Simulations of a Near-infrared Surface Biosignature on Proxima Centauri b with Future Space Observatories
Authors: Connor O. Metz, Nancy Y. Kiang, Geronimo L. Villanueva, M. N. Parenteau, Vincent Kofman
Figure caption:  B.viridis-like organism (BVLO) abundance maps on the dayside of DG19 Proxima b states (﹩{A}_{{\rm{b}}{\rm{a}}{\rm{c}}}﹩ as a function of latitude and longitude), shown for ﹩{A}_{\max }=1﹩. Plotted above the maps is the surface area coverage fraction in each longitude band. The numbers at the bottom right of these top panel plots are multipliers indicating the total hemispherical east:west BVLO abundance ratio. When observing this planet at a phase of 270° (for an inclination of 90°), only the eastern half of the dayside is visible, and only the western is visible for a phase of 90°.
Paper: Near-infrared Spectral Homogeneity of the Didymos System Before and After the DART Impact 
Authors: Simone Ieva, E. Mazzotta Epifani, E. Dotto, V. Petropoulou, J. D. P. Deshapriya, P. H. Hasselmann, G. Poggiali, D. Perna, M. Dall'Ora, A. Lucchetti, M. Pajola, S. L. Ivanovski, A. Rossi, J. R. Brucato, P. Palumbo, V. Della Corte, A. Zinzi, C. A. Thomas, J. de León, T. Kareta, N. Moskovitz, N. L. Chabot, A. S. Rivkin, M. Amoroso, I. Bertini, A. Capannolo, S. Caporali, M. Ceresoli, G. Cremonese, I. Gai, L. Gomez-Casajus, E. Gramigna, G. Impresario, R. Lasagni Manghi, M. Lavagna, M. Lombardo, D. Modenini, S. Pirrotta, P. Tortora, F. Tusberti, M. Zannoni, G. Zanotti
Figure caption: Daily reflectance spectra of Didymos acquired during each of the six nights, together with spectrum from J. de León (2006). Spectra are all normalized at 1.6 μm.
Paper: Near-infrared Spectral Homogeneity of the Didymos System Before and After the DART Impact 
Authors: Simone Ieva, E. Mazzotta Epifani, E. Dotto, V. Petropoulou, J. D. P. Deshapriya, P. H. Hasselmann, G. Poggiali, D. Perna, M. Dall'Ora, A. Lucchetti, M. Pajola, S. L. Ivanovski, A. Rossi, J. R. Brucato, P. Palumbo, V. Della Corte, A. Zinzi, C. A. Thomas, J. de León, T. Kareta, N. Moskovitz, N. L. Chabot, A. S. Rivkin, M. Amoroso, I. Bertini, A. Capannolo, S. Caporali, M. Ceresoli, G. Cremonese, I. Gai, L. Gomez-Casajus, E. Gramigna, G. Impresario, R. Lasagni Manghi, M. Lavagna, M. Lombardo, D. Modenini, S. Pirrotta, P. Tortora, F. Tusberti, M. Zannoni, G. Zanotti
Figure caption: All the spectra taken at different rotational phases on the night of August 5 (a) and November 3 (b). Some wavelength regions were removed due to improper telluric correction.
Paper: Estimate of Water and Hydroxyl Abundance on Asteroid (16) Psyche from JWST Data
Authors: Stephanie G. Jarmak, Tracy M. Becker, Charles E. Woodward, Casey I. Honniball, Andrew S. Rivkin, Margaret M. McAdam, Zoe A. Landsman, Saverio Cambioni, Thomas G. Müller, Driss Takir, Kurt D. Retherford, Anicia Arredondo, Linda T. Elkins-Tanton
Figure caption: Psyche's reflectance spectra from JWST NIRSpec observations. The data in black correspond to observation 1, and the data in red correspond to observation 2. We omitted observation 1 G235H/F170LP mode data beyond 2.9 μm, due to likely instrumental contamination.
Paper: Estimate of Water and Hydroxyl Abundance on Asteroid (16) Psyche from JWST Data
Authors: Stephanie G. Jarmak, Tracy M. Becker, Charles E. Woodward, Casey I. Honniball, Andrew S. Rivkin, Margaret M. McAdam, Zoe A. Landsman, Saverio Cambioni, Thomas G. Müller, Driss Takir, Kurt D. Retherford, Anicia Arredondo, Linda T. Elkins-Tanton
Figure caption: Normalized reflectance spectrum of Psyche near 3 μm from observation 1 (black) and observation 2 (red), and normalized reflectance spectra for laboratory data from CM2- (magenta), CH/CBb- (blue), and CY-type (cyan) carbonaceous chondrites. The 3 μm feature on Psyche most closely resembles CBb-type chondrites.
Paper: Estimate of Water and Hydroxyl Abundance on Asteroid (16) Psyche from JWST Data
Authors: Stephanie G. Jarmak, Tracy M. Becker, Charles E. Woodward, Casey I. Honniball, Andrew S. Rivkin, Margaret M. McAdam, Zoe A. Landsman, Saverio Cambioni, Thomas G. Müller, Driss Takir, Kurt D. Retherford, Anicia Arredondo, Linda T. Elkins-Tanton
Figure caption: Normalized reflectance spectrum of Psyche near 3 μm from observation 1 (black), and normalized reflectance spectra for asteroid data from NIR observations of Themis (green), Pallas (cyan), Interamnia (blue), Europa (magenta), and Bamberga (red), with data points corresponding to a binned average using 25 bins and errors corresponding to the standard deviation across the bin.
Paper: Estimate of Water and Hydroxyl Abundance on Asteroid (16) Psyche from JWST Data
Authors: Stephanie G. Jarmak, Tracy M. Becker, Charles E. Woodward, Casey I. Honniball, Andrew S. Rivkin, Margaret M. McAdam, Zoe A. Landsman, Saverio Cambioni, Thomas G. Müller, Driss Takir, Kurt D. Retherford, Anicia Arredondo, Linda T. Elkins-Tanton
Figure caption: Psyche's reflectance spectra from JWST NIRSpec observations. The data in black correspond to observation 1, and the data in red correspond to observation 2. The darker points correspond to the binned data used to assess spectral feature properties. We omitted observation 1 G235H/F170LP mode data beyond 2.9 μm, due to likely instrumental contamination.
Paper: Estimate of Water and Hydroxyl Abundance on Asteroid (16) Psyche from JWST Data
Authors: Stephanie G. Jarmak, Tracy M. Becker, Charles E. Woodward, Casey I. Honniball, Andrew S. Rivkin, Margaret M. McAdam, Zoe A. Landsman, Saverio Cambioni, Thomas G. Müller, Driss Takir, Kurt D. Retherford, Anicia Arredondo, Linda T. Elkins-Tanton
Figure caption: Relative normalized emission spectrum of asteroid (16) Psyche produced by dividing the MIRI channel 1 flux by the TPM and then dividing by a linear fit for observation 1 (top) and observation 2 (bottom). The data are binned to a resolution of 20 nm. We do not detect any 6 μm emission feature in either observation.
Paper: Estimate of Water and Hydroxyl Abundance on Asteroid (16) Psyche from JWST Data
Authors: Stephanie G. Jarmak, Tracy M. Becker, Charles E. Woodward, Casey I. Honniball, Andrew S. Rivkin, Margaret M. McAdam, Zoe A. Landsman, Saverio Cambioni, Thomas G. Müller, Driss Takir, Kurt D. Retherford, Anicia Arredondo, Linda T. Elkins-Tanton
Figure caption: Relative normalized reflectance spectrum of Psyche near 1.25 μm. Binned spectra are binned to 1 nm.