adsabs/AstroCLIMB huggingface dataset:
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: Spectral comparison of the Chang’e-6 (CE6) landing region and returned soils. (a) Locations of small impact craters and flat mare regions surrounding the Chang’e-6 landing site analyzed in this study. The colors of the filled circles indicate the degrees of space weathering, represented by the maturity index Is/FeO. (b) Comparison of laboratory spectra of the Chang’e-6 soils with orbital spectra of impact craters and the Chang’e-6 landing site normalized at 750 nm. (c) Soil maturity parameters plot (Is/FeO vs. OMAT) of Chang’e-6 landing regions, Chang’e-6 soils, and Apollo soils.(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: Depth profiles for maturity index Is/FeO of Chang’e (X. Lu et al. 2023) and Apollo core samples (P. Lucey et al. 2006).(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 laboratory spectroscopic measurement of the Chang’e-6 soil samples. The observation geometry of the laboratory spectroscopic measurements is incidence angle (i) = 30°, emission angle (e) = 0°, and phase angle (g) = 30°.
Paper: A Possible Four Month Periodicity in the Activity of FRB 20240209A
Authors: Arpan Pal
Figure caption: Temporal and periodicity analysis of FRB 20240209A. Top panel: burst occurrence timeline showing the DM variations (blue squares), individual bursts (black ticks), and waiting times between consecutive bursts (red circles) as a function of Modified Julian Date (MJD). The mean waiting time of 5.886 days is indicated by the green dashed line. The filled blue regions show the error bars on the detected DM. The shaded green region shows the measured period visually, and each box has a width of the measured ACF periodicity. Middle panel: autocorrelation function (ACF) analysis revealing a significant peak at 123.615 days (red point with pink shaded uncertainty region). Bottom panel: Lomb–Scargle periodogram showing a strong peak at 126.6 days, with 1σ, 2σ, and 3σ significance levels indicated by horizontal dashed lines. The FWHM range of the peak (yellow shaded region) and the ACF-derived period (purple dashed line) demonstrate the consistency between different periodicity analysis methods.
Paper: Eclipse Mapping with MIRI: 2D Map of HD 189733b from 8 μm JWST MIRI LRS Observations
Authors: Maura Lally, Ryan C. Challener, Nikole K. Lewis, Julie Inglis, Tiffany Kataria, Heather A. Knutson, Brian M. Kilpatrick, Natasha E. Batalha, Paul Bonney, Ian J. M. Crossfield, Trevor Foote, Gregory W. Henry, David K. Sing, Kevin B. Stevenson, Hannah R. Wakeford, Robert T. Zellem
Figure caption: Dayside maps of HD 189733b fit to both MIRI eclipses, as well as seven Spitzer eclipses (E. Agol et al. 2010) and a Spitzer partial phase curve (H. A. Knutson et al. 2007). The top row shows a map fit to the Eureka! reduction, while the second row shows a map fit to the SPARTA reduction. Shown in each map is the resulting longitudinal hotspot offset; unlike previously discussed analysis tests, these fits are in agreement with each other, due to the extended baseline from the partial phase curve breaking the degeneracy between the instrumental ramp and the phase curve shape. These maps also cover some of the nightside due to the added visible longitudes from the inclusion of the partial phase curve, although our analysis only focuses on the dayside. The bottom two plots show 100 random draws from our posterior distribution at the equator vs. longitude, and the hotspot meridian vs. latitude. The meridional temperature plot shows our overall best-fitting model (lmax = 5, N = 2) against the best-fitting three-component fit (lmax = 5, N = 3, sensitive to latitudinal offsets). Based on the posterior distribution of our latitudinally sensitive fit, we can confidently exclude a strong hemisphere-scale latitudinal offset (>12∘, by 3σ).
Paper: A Possible Four Month Periodicity in the Activity of FRB 20240209A
Authors: Arpan Pal
Figure caption: Periodicity analysis of FRB 20240209A using the epoch folding method. Top panel: the χ2 statistic as a function of trial periods, showing a significant peak at 128.8  ±  15.4 days (marked by the green dashed line with green shaded region indicating the uncertainty). Middle panel: the total burst count distribution folded at the best-fit period of 128.8 days is shown in blue. The mean signal-to-noise ratio (SNR) across every phase interval is shown in a red line connecting the red dots. Bottom panel: evolution of the DM after folding with the period of 128.8 days is shown in violet circles, with the phase-averaged DM shown as an orange line. The average DM is shown in a dashed red line.
Paper: Eclipse Mapping with MIRI: 2D Map of HD 189733b from 8 μm JWST MIRI LRS Observations
Authors: Maura Lally, Ryan C. Challener, Nikole K. Lewis, Julie Inglis, Tiffany Kataria, Heather A. Knutson, Brian M. Kilpatrick, Natasha E. Batalha, Paul Bonney, Ian J. M. Crossfield, Trevor Foote, Gregory W. Henry, David K. Sing, Kevin B. Stevenson, Hannah R. Wakeford, Robert T. Zellem
Figure caption: Throughputs of MIRI LRS and Spitzer IRAC 8 μm. Our observations were taken over the full MIRI bandpass, and then weighted by the Spitzer IRAC 8 μm bandpass to create an 8 μm eclipse map for comparison to previously published Spitzer results (C. Majeau et al. 2012; J. de Wit et al. 2012).
Paper: Eclipse Mapping with MIRI: 2D Map of HD 189733b from 8 μm JWST MIRI LRS Observations
Authors: Maura Lally, Ryan C. Challener, Nikole K. Lewis, Julie Inglis, Tiffany Kataria, Heather A. Knutson, Brian M. Kilpatrick, Natasha E. Batalha, Paul Bonney, Ian J. M. Crossfield, Trevor Foote, Gregory W. Henry, David K. Sing, Kevin B. Stevenson, Hannah R. Wakeford, Robert T. Zellem
Figure caption: Lightcurves of the two MIRI LRS eclipses analyzed in this work. The red best-fit model shown over both eclipses is the result of a simultaneous ThERESA fit of both MIRI LRS eclipses and, although not shown on the plot, the seven Spitzer IRAC 8 μm eclipses of E. Agol et al. (2010) and the partial phase curve of H. A. Knutson et al. (2007). The MIRI LRS data are shown unbinned, as well as binned to 130 points (about 2 minutes) for visual clarity. The joint fit of the eight eclipses and partial phase curve achieves an SDNR of 334 ppm, which is 1.8×  the photon noise floor of 181 ppm.
Paper: Eclipse Mapping with MIRI: 2D Map of HD 189733b from 8 μm JWST MIRI LRS Observations
Authors: Maura Lally, Ryan C. Challener, Nikole K. Lewis, Julie Inglis, Tiffany Kataria, Heather A. Knutson, Brian M. Kilpatrick, Natasha E. Batalha, Paul Bonney, Ian J. M. Crossfield, Trevor Foote, Gregory W. Henry, David K. Sing, Kevin B. Stevenson, Hannah R. Wakeford, Robert T. Zellem
Figure caption: Dayside maps of HD 189733b fit to both MIRI eclipses. The top row shows a map fit to the Eureka! reduction, while the bottom row shows a map fit to the SPARTA reduction. Shown in each map is the resulting longitudinal hotspot offset; although we achieve high-precision maps, they are still inconsistent across different data reduction methods. The reasons for the disagreement are further discussed in Section 3.2.
Paper: Eclipse Mapping with MIRI: 2D Map of HD 189733b from 8 μm JWST MIRI LRS Observations
Authors: Maura Lally, Ryan C. Challener, Nikole K. Lewis, Julie Inglis, Tiffany Kataria, Heather A. Knutson, Brian M. Kilpatrick, Natasha E. Batalha, Paul Bonney, Ian J. M. Crossfield, Trevor Foote, Gregory W. Henry, David K. Sing, Kevin B. Stevenson, Hannah R. Wakeford, Robert T. Zellem
Figure caption: Dayside maps of HD 189733b fit to single individual eclipses. The top row shows maps fit to the Eureka! reduction, while the bottom row shows maps fit to the SPARTA reduction. Shown in each map is the resulting longitudinal hotspot offset; although we achieve high-precision maps, when we fit them individually, they are not necessarily consistent across different eclipses nor across different data reduction methods.
Paper: A Possible Four Month Periodicity in the Activity of FRB 20240209A
Authors: Arpan Pal
Figure caption: Comparison of Lomb–Scargle periodogram analysis between unbinned (black), 1 day and (red) 8 day (blue) binning.
Paper: Improving Photometric Redshifts of Epoch of Reionization Galaxies: A New Empirical Transmission Curve with Neutral Hydrogen Damping Wing Lyα Absorption
Authors: Yoshihisa Asada, Guillaume Desprez, Chris J. Willott, Marcin Sawicki, Maruša Bradač, Gabriel Brammer, Florian Dubath, Kartheik G. Iyer, Nicholas S. Martis, Adam Muzzin, Gaël Noirot, Stéphane Paltani, Ghassan T. E. Sarrouh, Anishya Harshan, Vladan Markov
Figure caption: NH I, CGM vs. redshift relation. Black symbols denote the NH I, CGM measurements in this work from the CANUCS zspec > 6 sample. Black open upward/downward triangles represent lower/upper limits. The median value in each redshift bin is shown by red open diamonds. Blue symbols are NH I, CGM measurements from the literature (H. Umeda et al. 2024; S. Carniani et al. 2024; F. D’Eugenio et al. 2024; K. N. Hainline et al. 2024b; K. E. Heintz et al. 2024), and the cyan open square is the median value of the literature galaxies at zspec > 9. Some of the literature data points at z > 12 are not displayed in this figure. The red solid curve shows the best-fitting sigmoid parameterization of the NH I, CGM–z relation.
Paper: Improving Photometric Redshifts of Epoch of Reionization Galaxies: A New Empirical Transmission Curve with Neutral Hydrogen Damping Wing Lyα Absorption
Authors: Yoshihisa Asada, Guillaume Desprez, Chris J. Willott, Marcin Sawicki, Maruša Bradač, Gabriel Brammer, Florian Dubath, Kartheik G. Iyer, Nicholas S. Martis, Adam Muzzin, Gaël Noirot, Stéphane Paltani, Ghassan T. E. Sarrouh, Anishya Harshan, Vladan Markov
Figure caption: Photo-z improvements with the new IGM+CGM model. (a) zphot − zspec plot with the A. K. Inoue et al. (2014) IGM model. zphot are systematically overestimated when the standard IGM transmission is assumed at zspec > 7.5, and the median offset (δz = zphot − zspec) is 0.21 at the redshift range (orange dashed lines). (b) Same as panel (a) but with the new IGM+CGM transmission. The new transmission significantly improves zphot estimations, and zphot and zspec agree well at all z > 6. (c) The effect of the new IGM+CGM transmission on a catalog of all F277W S/N > 5 photometric sources. The new transmission has almost no effect on low-z photo-z estimations but corrects the bias by δz ∼ 0.2 at z ≳ 7.5.
Paper: Improving Photometric Redshifts of Epoch of Reionization Galaxies: A New Empirical Transmission Curve with Neutral Hydrogen Damping Wing Lyα Absorption
Authors: Yoshihisa Asada, Guillaume Desprez, Chris J. Willott, Marcin Sawicki, Maruša Bradač, Gabriel Brammer, Florian Dubath, Kartheik G. Iyer, Nicholas S. Martis, Adam Muzzin, Gaël Noirot, Stéphane Paltani, Ghassan T. E. Sarrouh, Anishya Harshan, Vladan Markov
Figure caption: Verification of the new IGM+CGM transmission with different setups. The top row are zphot − zspec plots with the standard A. K. Inoue et al. (2014) IGM model (similar to Figure 4(a)), and the bottom row are those with the new IGM+CGM transmission (Figure 4(b)). From left to right, comparisons with a different template set (left), a different photometric catalog by JADES (middle), and a different photo-z code (right) are shown. The new transmission remarkably improves photo-z estimations in all cases.
Paper: Improving Photometric Redshifts of Epoch of Reionization Galaxies: A New Empirical Transmission Curve with Neutral Hydrogen Damping Wing Lyα Absorption
Authors: Yoshihisa Asada, Guillaume Desprez, Chris J. Willott, Marcin Sawicki, Maruša Bradač, Gabriel Brammer, Florian Dubath, Kartheik G. Iyer, Nicholas S. Martis, Adam Muzzin, Gaël Noirot, Stéphane Paltani, Ghassan T. E. Sarrouh, Anishya Harshan, Vladan Markov
Figure caption: New IGM+CGM transmission curves at z = 6, 7, 8, 9, and 10. The dashed curves show the original IGM model by A. K. Inoue et al. (2014), and the solid curves show the new transmission with damping absorption.
Paper: Eclipse Mapping with MIRI: 2D Map of HD 189733b from 8 μm JWST MIRI LRS Observations
Authors: Maura Lally, Ryan C. Challener, Nikole K. Lewis, Julie Inglis, Tiffany Kataria, Heather A. Knutson, Brian M. Kilpatrick, Natasha E. Batalha, Paul Bonney, Ian J. M. Crossfield, Trevor Foote, Gregory W. Henry, David K. Sing, Kevin B. Stevenson, Hannah R. Wakeford, Robert T. Zellem
Figure caption: Top: distributions of best-fit hotspot offsets from the MIRI joint fit (purple), MIRI+Spitzer joint fit (blue), and the individual fits presented in this paper (purple dotted and dotted–dashed). Best-fit results are shown for the fits presented in this paper; the joint fit displays the distribution from an l = 5, N = 2 fit, the first individual eclipse fit shows the distribution from an l = 3, N = 2 fit, and the second eclipse from an l = 1, N = 3 fit (as displayed in the best-fit maps shown throughout the paper, as well as Table 2.). Also shown are the results of previous eclipse mapping studies C. Majeau et al. (2012; M2012) and J. de Wit et al. (2012; DW2012), as well as a test fit using only Spitzer eclipse and phase curve data (l = 5, N = 2; green). Single-model offsets presented in this paper are consistent with the offset presented from a fit to the Spitzer eclipses in M2012, but about 7σ larger than the Spitzer eclipse + phase curve result from M2012, and 5σ larger than the result presented in DW2012. The MIRI eclipses provide improved signal and constraints over what a Spitzer phase curve alone could provide. We note that the Spitzer-only and MIRI-only hotspot offsets have a 3σ separation. This is likely because the eigenmap calculation process is dependent on the time sampling of the lightcurves: while each of these shows the same l = 5, N = 2 model, there are differences in the two highest-variance eigenmaps used to form the model basis, contributing to differences in the resulting hotspot offsets. As discussed in Section 4, hotspot offset can vary with model assumptions; single-model fits, even if they are all l = 5, N = 2 models, have some discrepancies. The degeneracy present in the MIRI-only data set also has a significant impact on its longitudinal hotspot offset, complicating its use as a point of comparison. Bottom: All Eureka! models N = 1 to N = 3 are weighted by relative model probability (as described in Figure 7), and their posteriors are stacked to create the distribution shown. This process is done for fits to the MIRI data set, the Spitzer data set, and the combined MIRI+Spitzer data set. Credible regions for each fit are shown by the highlighted regions.
Paper: On the Million-degree Signature of Spicules
Authors: Souvik Bose, Jayant Joshi, Paola Testa, Bart De Pontieu
Figure caption: Propagation of spicules in the chromosphere, TR, and lower corona (∼1 MK) as observed from the raster in Figure 2. Panel (a): Mg II k2 peak separation. Panel (b): Si IV 1402.77 Å peak intensity. Panel (c): unsharp masked SDO/AIA 171 Å intensity; panel (d): unsharped masked EM computed using the method of sparsity; and panel (e): unsharped masked EM computed using Tikhonov regularization. The region bounded by two horizontal solid lines is analyzed further in Figure 12 in Appendix B.
Paper: Eclipse Mapping with MIRI: 2D Map of HD 189733b from 8 μm JWST MIRI LRS Observations
Authors: Maura Lally, Ryan C. Challener, Nikole K. Lewis, Julie Inglis, Tiffany Kataria, Heather A. Knutson, Brian M. Kilpatrick, Natasha E. Batalha, Paul Bonney, Ian J. M. Crossfield, Trevor Foote, Gregory W. Henry, David K. Sing, Kevin B. Stevenson, Hannah R. Wakeford, Robert T. Zellem
Figure caption: A visualization of our model selection process. Relative model probability (RMP) is related to the difference in BIC values between each possible fit (RMP = e(−ΔBIC/2)). Each square is a possible fit explored by ThERESA. Resulting longitudinal offsets are shown within each square for a selection of relatively probable models.
Paper: Eclipse Mapping with MIRI: 2D Map of HD 189733b from 8 μm JWST MIRI LRS Observations
Authors: Maura Lally, Ryan C. Challener, Nikole K. Lewis, Julie Inglis, Tiffany Kataria, Heather A. Knutson, Brian M. Kilpatrick, Natasha E. Batalha, Paul Bonney, Ian J. M. Crossfield, Trevor Foote, Gregory W. Henry, David K. Sing, Kevin B. Stevenson, Hannah R. Wakeford, Robert T. Zellem
Figure caption: The top row of this figure shows two GCM models at 8 μm; the left column shows a model assuming 1×  solar metallicity, and the right column assumes 5×  solar metallicity. The middle row shows our retrieved dayside joint fit map (the same map shown in the Eureka! row of Figure 4), overlaid with contour maps showing an eigenmap representation of the respective GCM maps shown in the top row. The bottom row shows residual differences between a uniform dayside model (horizontal dotted line) and our best-fit eclipse model, and each of the two GCMs. Data from both eclipses are binned down to a 2 minute cadence for visibility, and are consistent to a 1.3σ level.
Paper: Eclipse Mapping with MIRI: 2D Map of HD 189733b from 8 μm JWST MIRI LRS Observations
Authors: Maura Lally, Ryan C. Challener, Nikole K. Lewis, Julie Inglis, Tiffany Kataria, Heather A. Knutson, Brian M. Kilpatrick, Natasha E. Batalha, Paul Bonney, Ian J. M. Crossfield, Trevor Foote, Gregory W. Henry, David K. Sing, Kevin B. Stevenson, Hannah R. Wakeford, Robert T. Zellem
Figure caption: Schematic showing the weighted eigenmap components incorporated into our joint best-fit eclipse map shown in the Eureka! row of Figure 4. The top plot shows the two mapping components, the weights of which are described by C1 and C2 in Table 2. Our resulting map is a linear combination of these two components, in addition to a uniform brightness component. The rows beneath show their constituent harmonic components, with the strength of each component corresponding to its opacity. Some contributing higher-degree spherical harmonic modes (third, fourth, and fifth) are not shown in this plot, due to their contribution being minor compared to the modes shown.
Paper: Orthogonal Alignment of Galaxy Group Angular Momentum with Cosmic Filament Spines: An Observational Study
Authors: Yu Rong, Peng Wang, Xiao-xiao Tang
Figure caption: Panels (a), (b), and (c) illustrate the distributions of δ for galaxy groups categorized by member richness: groups with rich members (N > 10; red histogram), those of intermediate richness (3 < N ≤ 10; green histogram), and groups with poor members (2 ≤ N ≤ 3; blue histogram). The analyses detailed in these panels employ various weighting schemes: panel (a) incorporates both mass and radius weights of member galaxies, panel (b) utilizes only the mass weights, and panel (c) assigns equal weights to all members. Panel (d) assesses the alignment in the 2D plane, evaluating whether the angular momenta of groups exhibit perpendicular alignment with the filament spines in 3D space, as derived from the Millennium-II simulation. The K-S test p-values of comparing the distributions and a uniform distribution are presented, alongside the values of ﹩{ \mathcal I }(\delta )﹩, highlighting the significance of the observed alignment.
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: M3 spectral image of the Chang’e-6 landing region and selected spectra. (a) M3 reflectance image of 750 nm. The points and polygons represent the positions of the impact craters and flat mare areas selected for analysis. (b) The average spectra of craters, flat mare areas, and the Chang’e-6 landing region. The orange curves represent average spectra of the flat mare regions. The red curve represents average spectra of the Chang’e-6 landing site. (c) The comparison of modeled spectra (blue curves) using the Hapke model and measured spectra by M3 (gray dots).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Orthogonal Alignment of Galaxy Group Angular Momentum with Cosmic Filament Spines: An Observational Study
Authors: Yu Rong, Peng Wang, Xiao-xiao Tang
Figure caption: Schematic representation of a galaxy group and a segment of its associated large-scale filament. The galaxy group is depicted as a black ellipse, while a segment of the large-scale filament is illustrated as a black cylinder. Individual member galaxies within the group are represented by red and blue ellipses. The angular momentum of the group is indicated by dotted green arrows, and the mass flows relative to the galaxy group, signifying the infall of galaxies, are shown by dashed green arrows. The spin of the filament segment is denoted by a blue arrow.
Paper: Improving Photometric Redshifts of Epoch of Reionization Galaxies: A New Empirical Transmission Curve with Neutral Hydrogen Damping Wing Lyα Absorption
Authors: Yoshihisa Asada, Guillaume Desprez, Chris J. Willott, Marcin Sawicki, Maruša Bradač, Gabriel Brammer, Florian Dubath, Kartheik G. Iyer, Nicholas S. Martis, Adam Muzzin, Gaël Noirot, Stéphane Paltani, Ghassan T. E. Sarrouh, Anishya Harshan, Vladan Markov
Figure caption: Example SEDs of the NH I, CGM measurements in Section 3.2. Top: CANUCS–3117269 is at zspec = 8.3453, and the observed photometry (black squares) shows a flux deficit around the Lyman break as compared to the best-fitting template spectrum at zspec (black dashed line; black circles are the in-band fluxes of the best template). A damping absorption with ﹩\mathrm{log}({N}_{{\rm{HI}}}/{{\rm{cm}}}^{-2})=22.6﹩ is required to reproduce the observed SED. The red curve shows the best template spectrum after the additional damping wing absorption, whose in-band fluxes are shown by red circles. Bottom: CANUCS–2101494 is at zspec = 6.5676, and the observed photometry can be explained well without the additional damping wing absorption. The HST/WFC3 IR F110W photometry is not shown for clarity.
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 laboratory and orbital spectra of the Chang’e-6 soils. (a) Raw reflectance. (b) Reflectance after correction.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)