adsabs/AstroCLIMB huggingface dataset:
Paper: The Convergence of Heavy and Light Seeds to Overmassive Black Holes at Cosmic Dawn
Authors: Haojie Hu, Kohei Inayoshi, Zoltán Haiman, Luis C. Ho, Ken Ohsuga
Figure caption: Left: the mass evolution for DM mergers and seed BHs. The gray curves are evolutionary tracks of main progenitors of 100 (out of 104) DM halos ended up as massive halos with Mh = 1012 M⊙ at z = 6. Three typical merger histories are shown in black solid curves. The growth rate (kh) for different merger trees at z ∼ 6 varies from ∼0.25 to ∼1.15. The blue and red curves are evolutionary tracks for light (10 M⊙ BH at z = 30) and heavy seed (105 M⊙ at z = 15) BHs based on the three merger trees, adopting a fiducial model with p = 0.5. The blue and red shaded regions are parameters for possible SMBHs from our models. The high-redshift SMBHs are overlaid with crosses, with the most massive SMBH from X.-B. Wu et al. (2015). SMBHs from the pre-JWST era are overlaid with gray crosses (D. J. Mortlock et al. 2011; E. Bañados et al. 2018; T. Izumi et al. 2019), while SMBHs from the JWST era are shown with black crosses (data collected from X. Ding et al. 2023; Y. Harikane et al. 2023; D. D. Kocevski et al. 2023, 2024; V. Kokorev et al. 2023, 2024; R. L. Larson et al. 2023; R. Maiolino et al. 2024a, 2024b; M. Yue et al. 2023; Á. Bogdán et al. 2024; J. E. Greene et al. 2024; I. Juodžbalis et al. 2024; L. Napolitano et al. 2024; M. A. Stone et al. 2024). Right: the evolution of the MBH/M⋆ ratio for light seed BHs (blue curves) and heavy seed BHs (red curves). The JWST samples are overlaid for reference. The solid horizontal line indicates the maximum value of MBH/M⋆ ∼ ϵnuc/ϵ⋆ = 0.2. The dashed, dashed–dotted, and dotted horizontal lines are MBH/M⋆ ratios for late-type, early-type, and all galaxies at M⋆ = 3 × 1010 M⊙, respectively (J. E. Greene et al. 2020).
Paper: The Convergence of Heavy and Light Seeds to Overmassive Black Holes at Cosmic Dawn
Authors: Haojie Hu, Kohei Inayoshi, Zoltán Haiman, Luis C. Ho, Ken Ohsuga
Figure caption: The evolutionary trend for two different seed BHs at four epochs (z = 25, 15, 10, and 8). The blue (gray) arrows indicate positive (negative) second-order derivatives ﹩{\mathscr{S}}﹩, while lengths of arrows are calculated assuming a 10 Myr growth for the BH and host galaxy at the current epoch and renormalized to [0.2, 1.2] times the length of a unit vector. The two evolutionary tracks represent that for a light seed with an initial mass of MBH = 10 M⊙ at z = 30 (red) and a heavy seed with MBH = 105 M⊙ at z = 15 (green). The solid curve illustrates the evolution from the seeding time to the redshift of each panel (marked with filled circles), while the dashed curves show the continuation of the track toward lower redshifts. In this figure, we adopt a constant value p = 0.5 and halo growth rates kh = 0.7 at z ≤ 15 and kh = 0.35 at z > 15 to be consistent with the evolutionary tracks shown in Figure 1. The open circle in each model indicates the transition from super-Eddington to sub-Eddington accretion, after which p = 0 is assumed. The diagonal orange line in the top right panel represents the boundary with ﹩{\mathscr{S}}=0﹩ for p = 0.5.
Paper: The Convergence of Heavy and Light Seeds to Overmassive Black Holes at Cosmic Dawn
Authors: Haojie Hu, Kohei Inayoshi, Zoltán Haiman, Luis C. Ho, Ken Ohsuga
Figure caption: The evolutionary tracks for two classes of seed BHs harbored in galaxies on different mass scales: the blue region for heavy seed BHs and the red region for light seed BHs. The flow patterns are calculated at each redshift adopting the SP1 feedback model. The seed BHs are chosen so that they are located above and below the local relation when they were seeded at z = 15. The BH–galaxy systems evolve to z = 4 with JWST SMBHs overlaid with stars in each redshift bin. For our fiducial parameters, we adopt kh = 0.7 and ϵnuc = 0.02. The two colored contours are the probability distributions of the evolutionary tracks for the two seed BH models when normal distributions for kh and ϵnuc are adopted, with 〈kh〉 = 0.70, ﹩{\sigma }_{k}^{2}=0.06﹩, and ﹩\langle {\mathrm{log}}\,{\epsilon }_{{\rm{nuc}}}\rangle =-1.7﹩, ﹩{\sigma }_{{\rm{nuc}}}^{2}=0.25﹩. The contour lines represent coverages of 16% and 84%, respectively.
Paper: The Convergence of Heavy and Light Seeds to Overmassive Black Holes at Cosmic Dawn
Authors: Haojie Hu, Kohei Inayoshi, Zoltán Haiman, Luis C. Ho, Ken Ohsuga
Figure caption: The evolutionary trend for different feedback models at z = 15 (from left to right: SP1, SP2, and SP3). The blue arrows indicate the positive signs of second-order derivatives, while the orange arrows are for negative ones. The lengths of arrows are same as in Figure 2. The inserts in each panel show the corresponding feedback models.
Paper: Observational Constraints of Radial Migration in the Galactic Disk Driven by the Slowing Bar
Authors: HanYuan Zhang, Vasily Belokurov, N. Wyn Evans, Jason L. Sanders, Yuxi(Lucy) Lu, Chengye Cao, GyuChul Myeong, Adam M. Dillamore, Sarah G. Kane, Zhao-Yu Li
Figure caption: Left panel (a): the age–metallicity plane of the test particle simulation with a slowing-down bar. The blue line shows the metallicity evolution for stars that formed at the corotation radius of their corresponding age, [Fe/H](τ, RCR(τ)), where the blue dots and annotation denote RCR(t) at the respective times in units of kiloparsecs; the orange line shows the metallicity evolution of stars that formed around the solar circle, [Fe/H](τ, R⊙). The red line indicates the moment of bar formation, tbf. Middle panel (b): the same as panel (a), except that the Galactic bar is rotating with a constant pattern speed at all times. Right panel (c): the column-normalized age–metallicity distribution of the subgiant-star sample we constructed based on M. Xiang & H.-W. Rix (2022), where the red circle indicates the Sun in this plane. The blue and orange dashed lines denote the upper and lower age–metallicity sequences, and the red dashed–dotted line marks the turning point of the upper sequence.
Paper: Observational Constraints of Radial Migration in the Galactic Disk Driven by the Slowing Bar
Authors: HanYuan Zhang, Vasily Belokurov, N. Wyn Evans, Jason L. Sanders, Yuxi(Lucy) Lu, Chengye Cao, GyuChul Myeong, Adam M. Dillamore, Sarah G. Kane, Zhao-Yu Li
Figure caption: Left: the fraction of outward-migrated stars as a function of azimuthal angle in different guiding radius bins. The vertical solid and dashed lines denote the bar major and minor axes. Middle: the observed fraction of high-α stars as a function of azimuthal angle. Right: the radial surface density profile of old stars/high-[Fe/H] stars in the test particle simulation with a decelerating bar (solid lines) and with a constant pattern speed bar (dashed lines). The vertical dashed line represents the current corotation radius.
Paper: Observational Constraints of Radial Migration in the Galactic Disk Driven by the Slowing Bar
Authors: HanYuan Zhang, Vasily Belokurov, N. Wyn Evans, Jason L. Sanders, Yuxi(Lucy) Lu, Chengye Cao, GyuChul Myeong, Adam M. Dillamore, Sarah G. Kane, Zhao-Yu Li
Figure caption: Left panel: the background is the column-normalized distribution of the test particles in the simulation in the age–birth radius (Rb) plane, and the contour shows the same distribution of the selected particles that are corotating with the bar. The blue line indicates the temporal evolution of the corotation radius in the test particle simulation, in which the dashed part is for the time before the bar formation, and the solid line is after the bar formation. Right panel: the same as the left panel but for the observed stars with the birth radii inferred in Y. L. Lu et al. (2024), and the contours are for the selected corotation stars. The blue line is fitted for the sequences of the corotation stars, from which we inferred the slowing-down history of the Galactic bar.
Paper: Observational Constraints of Radial Migration in the Galactic Disk Driven by the Slowing Bar
Authors: HanYuan Zhang, Vasily Belokurov, N. Wyn Evans, Jason L. Sanders, Yuxi(Lucy) Lu, Chengye Cao, GyuChul Myeong, Adam M. Dillamore, Sarah G. Kane, Zhao-Yu Li
Figure caption: Top panels: the observed age–metallicity (column-normalized) distribution of the subgiant stars in various guiding radius bins. The blue and orange dashed lines in the middle panel denote the migrated and local age–metallicity sequence, which we will use in Figure 3. Bottom panels: the age–metallicity (column-normalized) distribution of the test particle simulation with a slowing-down bar in different guiding radius bins.
Paper: Observational Constraints of Radial Migration in the Galactic Disk Driven by the Slowing Bar
Authors: HanYuan Zhang, Vasily Belokurov, N. Wyn Evans, Jason L. Sanders, Yuxi(Lucy) Lu, Chengye Cao, GyuChul Myeong, Adam M. Dillamore, Sarah G. Kane, Zhao-Yu Li
Figure caption: The model used for the metallicity assignment. Lines with different colors correspond to the metallicity evolution at different radii. The background shows the results of the test particle simulation with the decelerating bar. The dots denote the trend of [Fe/H](age, RCR).
Paper: Observational Constraints of Radial Migration in the Galactic Disk Driven by the Slowing Bar
Authors: HanYuan Zhang, Vasily Belokurov, N. Wyn Evans, Jason L. Sanders, Yuxi(Lucy) Lu, Chengye Cao, GyuChul Myeong, Adam M. Dillamore, Sarah G. Kane, Zhao-Yu Li
Figure caption: The (non-column-normalized) [α/Fe]–[Fe/H] distribution of the observed stars in three guiding radius bins. In the middle panel, the blue (orange) contours show the column-normalized distribution of stars in the upper (lower) age–metallicity sequence, which we selected in the top middle panel in Figure 2.
Paper: Observational Constraints of Radial Migration in the Galactic Disk Driven by the Slowing Bar
Authors: HanYuan Zhang, Vasily Belokurov, N. Wyn Evans, Jason L. Sanders, Yuxi(Lucy) Lu, Chengye Cao, GyuChul Myeong, Adam M. Dillamore, Sarah G. Kane, Zhao-Yu Li
Figure caption: The age–metallicity distribution of the observed subgiant stars (M. Xiang & H.-W. Rix 2022) in different guiding radius bins, each with width of 0.5 kpc. The orange dashed lines denote the separation between the upper and lower sequences.
Paper: Evidence for Environmental Effects in the z = 4.3 Protocluster Core SPT2349–56
Authors: Chayce Hughes, Ryley Hill, Scott C. Chapman, Manuel Aravena, Melanie Archipley, Veronica J. Dike, Anthony Gonzalez, Thomas R. Greve, Gayathri Gururajan, Chris Hayward, Kedar Phadke, Cassie Reuter, Justin Spilker, Nikolaus Sulzenauer, Joaquin D. Vieira, David Vizgan, George Wang, Axel Weiss, Dazhi Zhou
Figure caption: Comparison of [C I] and CO line luminosities and line ratios in SPT2349–56 and the literature field sample. Top: the L[CI](2−1) / L[CI](1−0) ratio as a function of S850 for protocluster galaxies (blue) and field galaxies (red), with the ﹩{L}^{{\prime} }﹩ units shown on the right axis. The horizontal dashed line at ﹩{L}_{[\,\rm{C}\,{\rm\small{I}}](2-1)}^{{\prime} }\,/\,{L}_{[\,\rm{C}\,{\rm\small{I}}](1-0)}^{{\prime} }=2.11﹩ indicates where the line ratio becomes unphysical (see Equation (2)). Sources with  >3.5σ measurements in both lines are shown as detections, otherwise we show upper/lower limits. The mean and scatter of the samples are shown as the solid lines and shaded regions, respectively. Bottom left: L[CI](1−0) vs. S850 for protocluster galaxies vs. field galaxies. Upper limits are shown for measurements below 3.5σ. The best-fit power-law models for both the SPT2349–56 (blue) and G. Gururajan et al. (2023; red) samples are shown as the solid lines, with the fit parameters and covariances listed. The shaded regions correspond to 95% confidence intervals, assuming that the fit parameters α and γ follow a multivariate normal distribution. Bottom right: the same as the bottom left but for L[CI](2−1).
Paper: Evidence for Environmental Effects in the z = 4.3 Protocluster Core SPT2349–56
Authors: Chayce Hughes, Ryley Hill, Scott C. Chapman, Manuel Aravena, Melanie Archipley, Veronica J. Dike, Anthony Gonzalez, Thomas R. Greve, Gayathri Gururajan, Chris Hayward, Kedar Phadke, Cassie Reuter, Justin Spilker, Nikolaus Sulzenauer, Joaquin D. Vieira, David Vizgan, George Wang, Axel Weiss, Dazhi Zhou
Figure caption: Continuum-subtracted Band 3 and 4 spectra for all sources with a  >2σ peak-pixel [C I](1–0) or aperture [C I](2–1) measurement. The average per-channel noise in millijanskys over the displayed channels is listed at the top right of each panel, and the name of each galaxy in R. Hill et al. (2020) is listed at the top left. All spectra are unbinned. The fits to the Band 3 and 4 spectra are shown in green and red, respectively. The scaled [C II] line profiles are overlaid on top of the Band 3 spectra. The shaded regions represent the integration ranges, although we note that we subtract the blended Band 4 lines before performing the integration. The sources are ordered by the [C I](1–0) signal-to-noise ratio.
Paper: Evidence for Environmental Effects in the z = 4.3 Protocluster Core SPT2349–56
Authors: Chayce Hughes, Ryley Hill, Scott C. Chapman, Manuel Aravena, Melanie Archipley, Veronica J. Dike, Anthony Gonzalez, Thomas R. Greve, Gayathri Gururajan, Chris Hayward, Kedar Phadke, Cassie Reuter, Justin Spilker, Nikolaus Sulzenauer, Joaquin D. Vieira, David Vizgan, George Wang, Axel Weiss, Dazhi Zhou
Figure caption: Gas-mass estimates from CO(4–3) measurements compared to gas-mass estimates from [C I]. R. Hill et al. (2020) assumed r4,1 = 0.60 ± 0.05 to convert CO(4–3) to CO(1–0) line luminosities (in units of K km s−1 pc2) and αCO = 1.0 M⊙ (K km s−1 pc2)−1. We have used Equation (4) with XCI × αCO = (6.31 ± 0.67) × 10−5 (G. Gururajan et al. 2023), along with the same αCO value.
Paper: Evidence for Environmental Effects in the z = 4.3 Protocluster Core SPT2349–56
Authors: Chayce Hughes, Ryley Hill, Scott C. Chapman, Manuel Aravena, Melanie Archipley, Veronica J. Dike, Anthony Gonzalez, Thomas R. Greve, Gayathri Gururajan, Chris Hayward, Kedar Phadke, Cassie Reuter, Justin Spilker, Nikolaus Sulzenauer, Joaquin D. Vieira, David Vizgan, George Wang, Axel Weiss, Dazhi Zhou
Figure caption: [C II] cutouts from R. Hill et al. (2020) are shown in the background, with blue contours overlaid in steps of 2nσ (where n = 0, 1, 2, 3. . . ). [C I](1–0) (red) and [C I](2–1) (yellow) contours are overlaid following the same σ levels, for comparison. The peak pixels in the [C II] cutouts are indicated by circles. In all cases, the line integration ranges are 2σ around the centers of the lines. The [C I](2–1) maps have been lightly smoothed by a Gaussian with a standard deviation of 1 pixel for presentation purposes.
Paper: Kiloparsec-scale Alignment of a Radio Jet with Cool Gas and Dust in a z ∼ 6 Quasar
Authors: Fabian Walter, Eduardo Bañados, Chris Carilli, Marcel Neeleman, Thomas Connor, Roberto Decarli, Emanuele Paulo Farina, Yana Khusanova, Chiara Mazzucchelli, Romain Meyer, Emmanuel Momjian, Hans–Walter Rix, Sofía Rojas-Ruiz, Bram Venemans
Figure caption: Position–velocity diagram (top left) of the [C II] emission oriented along the direction of the jet as shown by the dashed line (PA = 303∘) in the velocity field of the [C II] emission line (top right). In both panels, positive spatial offsets correspond to offsets toward the east. The cross indicates the position of the brightest peak in the VLBA observations (E. Momjian et al. 2018). Contours are plotted in powers of ﹩\sqrt{2}﹩, starting at ±2σ (negative contours are dashed). To increase the S/N of the extended emission, we smoothed the data to a resolution of ∼0﹩\mathop{.}\limits^{^{\prime\prime} }﹩1, as shown by the updated beam in the bottom-right inset of the right panel (the contours in the right panel are the integrated [C II] flux density map using the original resolution shown in Figures 1 and 2). A smooth, linear increase velocity gradient is apparent, reaching maximum velocities of approximately +(−) 200 km s−1 along the eastern (western) jet. The bottom panels are single-beam spectra extracted from different positions along the jet (labeled (A), (B), and (C) in top-right panel) spaced 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩25 apart. The velocity dispersion determined from a Gaussian fit to the data (red line) is given in the two bottom-left panels. No successful fit was obtained for the spectrum at position (C).
Paper: Kiloparsec-scale Alignment of a Radio Jet with Cool Gas and Dust in a z ∼ 6 Quasar
Authors: Fabian Walter, Eduardo Bañados, Chris Carilli, Marcel Neeleman, Thomas Connor, Roberto Decarli, Emanuele Paulo Farina, Yana Khusanova, Chiara Mazzucchelli, Romain Meyer, Emmanuel Momjian, Hans–Walter Rix, Sofía Rojas-Ruiz, Bram Venemans
Figure caption: ALMA 400 pc resolution imaging of the dust continuum emission at 285 GHz (left) and the [C II] emission averaged over the central 600 km s−1 (right). Contours start at ±2σ and increase/decrease in powers of ﹩\sqrt{2}﹩. For the continuum, 1 σ corresponds to 4.1 μJy beam−1, and for the [C II] line, 1σ = 11.8 mJy km s−1 beam−1. Coordinates are given relative to the brightest source seen in the VLBA observations discussed in Section 3.3 at R.A.(International Celestial Reference System, ICRS) = ﹩2{3}^{{\rm{h}}}2{9}^{{\rm{m}}}36\mathop{.}\limits^{s}8316﹩, decl.(ICRS)﹩=\,-1{5}^{\circ }2{0}^{{\prime} }14\mathop{.}\limits^{^{\prime\prime} }498﹩ (E. Momjian et al. 2018). The beam size is indicated in the lower-left corner of both panels, and a 1 kpc scale is shown in the bottom right of the [C II] map.
Paper: Kiloparsec-scale Alignment of a Radio Jet with Cool Gas and Dust in a z ∼ 6 Quasar
Authors: Fabian Walter, Eduardo Bañados, Chris Carilli, Marcel Neeleman, Thomas Connor, Roberto Decarli, Emanuele Paulo Farina, Yana Khusanova, Chiara Mazzucchelli, Romain Meyer, Emmanuel Momjian, Hans–Walter Rix, Sofía Rojas-Ruiz, Bram Venemans
Figure caption: Superposition of the ALMA dust continuum (blue contours), ALMA [C II] emission (orange contours), and the VLBA 1.54 GHz radio continuum image (black contours). The dust continuum emission at 285 GHz and [C II] emission have the same contour levels, as shown in Figure 1. The VLBA image presented in E. Momjian et al. (2018) is shown in black contours starting at ±3σ (1σ = 67 μJy beam−1) and increase/decrease by powers of ﹩\sqrt{2}﹩. The ALMA (VLBA) beam size is indicated in the lower-left (right) corner. The origin in this figure and the kiloparsec-scale bar are as in Figure 1. As discussed in Section 3.3, we have shifted the ALMA data slightly (<25 mas) in order to center the ALMA dust continuum peak on the peak of the VLBA image.
Paper: Observational Constraints of Radial Migration in the Galactic Disk Driven by the Slowing Bar
Authors: HanYuan Zhang, Vasily Belokurov, N. Wyn Evans, Jason L. Sanders, Yuxi(Lucy) Lu, Chengye Cao, GyuChul Myeong, Adam M. Dillamore, Sarah G. Kane, Zhao-Yu Li
Figure caption: The age–metallicity distribution of the test particles (with a slowing-down bar) in different guiding radius bins. The orange dashed lines denote the sequence of particles that migrated with the expansion of the corotation radius. We draw attention to the similarity between the observation and simulation around and outside the corotation.
Paper: Primordial Origin of Methane on Eris and Makemake Supported by D/H Ratios
Authors: Olivier Mousis, Aaron Werlen, Tom Benest Couzinou, Antoine Schneeberger
Figure caption: Deuterium enrichment profile f calculated along the trajectory of the methane ice line in the PSN, assuming a condensation temperature of 28 K. The thick horizontal lines indicate the nominal enrichment values observed for Makemake (gray), Eris (green), and Titan (red). The dashed lines in matching colors represent the 1σ uncertainties associated with these measurements. From left to right, the initial enrichment values were set at 0.5, one, and two times the central value of 115 measured in Comet 67P/C-G. The epochs where f intersects the central values observed for the three bodies are highlighted, corresponding to a very narrow variation in the location of the methane ice line within the PSN.
Paper: Primordial Origin of Methane on Eris and Makemake Supported by D/H Ratios
Authors: Olivier Mousis, Aaron Werlen, Tom Benest Couzinou, Antoine Schneeberger
Figure caption: Temperature (T), pressure (P), and surface density (Σg) profiles of the gas in the PSN midplane, shown for various stages of its evolution.
Paper: Primordial Origin of Methane on Eris and Makemake Supported by D/H Ratios
Authors: Olivier Mousis, Aaron Werlen, Tom Benest Couzinou, Antoine Schneeberger
Figure caption: Similar to Figure 2 but showing the deuterium enrichment profile f calculated along the trajectory of the methane clathration in the PSN, with an assumed entrapment temperature of 55 K.
Paper: Space Weathering Properties of Chang’e-6 Soils and Implication for Regolith Evolution of Young Lunar Maria
Authors: Xuejin Lu, Jian Chen, Haijun Cao, Changqing Liu, Ziyi Jia, Chengxiang Yin, Tianwei Wang, Xiaohui Fu, Le Qiao, Xiaojia Zeng, Jiang Zhang, Zongcheng Ling
Figure caption: Comparison of VNIR spectral parameters and glassy agglutinate content of Chang’e-6 (CE6) and lunar nearside soils. The variation of NIR/VIS ratio with (a) reflectance at 750 nm and (b) band area at 1 μm of Chang’e (red stars) and Apollo soils (squares and diamonds). The variation of glassy agglutinates with (c) maturity and (d) basalt age. Chang’e-5 and Apollo soils were divided into four groups based on composition: TiO2-rich mare (TRM, TiO2 > 5 wt%, dark blue squares), TiO2-poor mare (TPM, TiO2 < 5 wt%, light green squares), moderate-FeO highland (MFH, FeO >  5 wt%, dark gray diamonds), and low-FeO highland (LFH, FeO < 5 wt%, light gray diamonds).
Paper: Space Weathering Properties of Chang’e-6 Soils and Implication for Regolith Evolution of Young Lunar Maria
Authors: Xuejin Lu, Jian Chen, Haijun Cao, Changqing Liu, Ziyi Jia, Chengxiang Yin, Tianwei Wang, Xiaohui Fu, Le Qiao, Xiaojia Zeng, Jiang Zhang, Zongcheng Ling
Figure caption: A cartoon illustration comparing the lunar regolith formation and evolution process at the younger (<3.0 Ga) and older maria (>3.0 Ga). Rocket exhaust destructs the optically mature veneer on the uppermost surface, exposing immature materials underneath on the young maria. Younger maria exhibit a thinner optically mature layer and less glassy agglutinate abundance. Older maria exhibit a thicker optically mature layer and higher glassy agglutinate abundance.
Paper: Space Weathering Properties of Chang’e-6 Soils and Implication for Regolith Evolution of Young Lunar Maria
Authors: Xuejin Lu, Jian Chen, Haijun Cao, Changqing Liu, Ziyi Jia, Chengxiang Yin, Tianwei Wang, Xiaohui Fu, Le Qiao, Xiaojia Zeng, Jiang Zhang, Zongcheng Ling
Figure caption: Comparison of modeled spectra and laboratory spectra. (a) The modeled spectra with various Fe0 contents. (b) The modeled spectra that best match the average laboratory spectra with an RMSE of 0.00137.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Space Weathering Properties of Chang’e-6 Soils and Implication for Regolith Evolution of Young Lunar Maria
Authors: Xuejin Lu, Jian Chen, Haijun Cao, Changqing Liu, Ziyi Jia, Chengxiang Yin, Tianwei Wang, Xiaohui Fu, Le Qiao, Xiaojia Zeng, Jiang Zhang, Zongcheng Ling
Figure caption: The lunar farside soils on the Moon and Earth. (a) Images of the Chang’e-6 lander, the sampling robotic arm, and the scooped area on the lunar surface (credit: CNSA). (b) Photograph, (c) reflectance spectra, and (d) continuum-removed spectra of Chang’e-6 soil samples in the laboratory.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)