adsabs/AstroCLIMB huggingface dataset:
Paper: Characterizing the Broadband Reflection Spectrum of MAXI J1803-298 during Its 2021 Outburst with NuSTAR and NICER
Authors: Oluwashina K. Adegoke, Javier A. García, Riley M. T. Connors, Yuanze Ding, Guglielmo Mastroserio, James F. Steiner, Adam Ingram, Fiona A. Harrison, John A. Tomsick, Erin Kara, Missagh Mehdipour, Keigo Fukumura, Daniel Stern, Santiago Ubach, Matteo Lucchini
Figure caption: Left: best-fit model to the NICER+NuSTAR spectra of Epoch 4, where relativistic reflection is modeled with relxillCp. The subplots (a) and (b) show residuals without and with the Gauss model included, respectively, for the absorption feature at ∼6.7 keV. Right: best-fit model to the NICER+NuSTAR spectra of Epoch 4, where relativistic reflection is modeled with relxillNS. The subplots (c) and (d) show residuals without and with the Gauss model included, respectively, for the absorption feature at ∼6.7 keV. For both plots, the model components are shown as indicated by the plot labels.
Paper: Characterizing the Broadband Reflection Spectrum of MAXI J1803-298 during Its 2021 Outburst with NuSTAR and NICER
Authors: Oluwashina K. Adegoke, Javier A. García, Riley M. T. Connors, Yuanze Ding, Guglielmo Mastroserio, James F. Steiner, Adam Ingram, Fiona A. Harrison, John A. Tomsick, Erin Kara, Missagh Mehdipour, Keigo Fukumura, Daniel Stern, Santiago Ubach, Matteo Lucchini
Figure caption: Residuals for all four epochs based on an absorbed diskbb+cutoffpl fit to the NuSTAR data in the energy range 3–4.5 keV, 8.5–15 keV, and 40–79 keV (40–70 keV for Epoch 2), extrapolated over the complete energy band (the complete energy band for Epoch 4 is 3–25 keV). The spectra have been rebinned for plotting purposes.
Paper: Characterizing the Broadband Reflection Spectrum of MAXI J1803-298 during Its 2021 Outburst with NuSTAR and NICER
Authors: Oluwashina K. Adegoke, Javier A. García, Riley M. T. Connors, Yuanze Ding, Guglielmo Mastroserio, James F. Steiner, Adam Ingram, Fiona A. Harrison, John A. Tomsick, Erin Kara, Missagh Mehdipour, Keigo Fukumura, Daniel Stern, Santiago Ubach, Matteo Lucchini
Figure caption: HID from FPMA for all four NuSTAR epochs. While HR is the ratio of count rates in the hard band (8.5–15 keV) to those in the soft band (3–4.5 keV), intensity is the sum of count rates in both bands. For Epoch 1, the dashed (orange) horizontal line separates data from the nondip vs. the dip intervals.
Paper: Characterizing the Broadband Reflection Spectrum of MAXI J1803-298 during Its 2021 Outburst with NuSTAR and NICER
Authors: Oluwashina K. Adegoke, Javier A. García, Riley M. T. Connors, Yuanze Ding, Guglielmo Mastroserio, James F. Steiner, Adam Ingram, Fiona A. Harrison, John A. Tomsick, Erin Kara, Missagh Mehdipour, Keigo Fukumura, Daniel Stern, Santiago Ubach, Matteo Lucchini
Figure caption: Left: residuals for Epoch 1 persistent and dip FPMA spectra based on an absorbed diskbb+cutoffpl fit to the NuSTAR data in the energy range 3–4.5 keV, 8.5–15 keV, and 40–79 keV, extrapolated over the complete energy band. The black arrow indicates a prominent absorption dip superimposed on the broad Fe Kα line of the dip spectra. The spectra have been rebinned for plotting purposes. Right: NuSTAR FPMA light curves in the 3–5.5 keV, 5.5–8.5 keV, 8.5–15 keV, 15–40 keV, and 40–79 keV bands, from top to bottom panels respectively.
Paper: Characterizing the Broadband Reflection Spectrum of MAXI J1803-298 during Its 2021 Outburst with NuSTAR and NICER
Authors: Oluwashina K. Adegoke, Javier A. García, Riley M. T. Connors, Yuanze Ding, Guglielmo Mastroserio, James F. Steiner, Adam Ingram, Fiona A. Harrison, John A. Tomsick, Erin Kara, Missagh Mehdipour, Keigo Fukumura, Daniel Stern, Santiago Ubach, Matteo Lucchini
Figure caption: Left: best-fit model to the NuSTAR FPMA/B spectra of Epoch 2 with the model components shown as described in the plot label. Right: best-fit model to the NICER+NuSTAR FPMA/B spectra of Epoch 3. The model components are shown as described in the plot label, where, for each of the components, one curve fits for the low-flux spectra (green), and one for the high-flux spectra (brown).
Paper: Characterizing the Broadband Reflection Spectrum of MAXI J1803-298 during Its 2021 Outburst with NuSTAR and NICER
Authors: Oluwashina K. Adegoke, Javier A. García, Riley M. T. Connors, Yuanze Ding, Guglielmo Mastroserio, James F. Steiner, Adam Ingram, Fiona A. Harrison, John A. Tomsick, Erin Kara, Missagh Mehdipour, Keigo Fukumura, Daniel Stern, Santiago Ubach, Matteo Lucchini
Figure caption: Left: best-fit residuals from model fits to the NuSTAR FPMA/B persistent spectra. Right: best-fit residuals from model fits to the NuSTAR FPMA/B dip spectra.
Paper: Multiwavelength Emission from Jets and Magnetically Arrested Disks in Nearby Radio Galaxies: Application to M87
Authors: Riku Kuze, Shigeo S. Kimura, Kenji Toma
Figure caption: Photon spectrum for M87. The thick and thin lines are the photon spectra after and before internal attenuation by the Breit–Wheeler process, respectively. Gray points are the multiwavelength simultaneous data taken from EHT MWL Science Working Group et al. (2021) and MAGIC Collaboration et al. (2020). Blue and orange shaded regions are power-law and log-parabola fitting spectra taken from the Fermi-4FGL-DR3 catalog (https://fermi.gsfc.nasa.gov/ssc/data/access/lat/12yr_catalog/).
Paper: Multiwavelength Emission from Jets and Magnetically Arrested Disks in Nearby Radio Galaxies: Application to M87
Authors: Riku Kuze, Shigeo S. Kimura, Kenji Toma
Figure caption: Same as Figure 2, but timescales in the jet as a function of the electron energy. Here t SSC (dotted) and t ad (dotted–dashed) are the synchrotron self-Compton and adiabatic cooling timescales, respectively. The vertical dashed gray line represents E  e,cut = γ cut m  e  c 2.
Paper: Multiwavelength Emission from Jets and Magnetically Arrested Disks in Nearby Radio Galaxies: Application to M87
Authors: Riku Kuze, Shigeo S. Kimura, Kenji Toma
Figure caption: Cooling (blue), escape (green), loss (black), and acceleration (red) timescales in the MAD as a function of the proton energy. Here t syn, t BH, t  pp , and t  p γ  are the synchrotron, Bethe–Heitler, pp inelastic collision, and photomeson production cooling timescales, respectively. Due to the hard-sphere-like diffusion coefficient, the acceleration and the diffusion timescales (green dashed line) do not depend on the proton energy.
Paper: Multiwavelength Emission from Jets and Magnetically Arrested Disks in Nearby Radio Galaxies: Application to M87
Authors: Riku Kuze, Shigeo S. Kimura, Kenji Toma
Figure caption: Same as Figure 3, but for the weak plasma entrainment. Total and jet synchrotron photon spectra with δ B/B = 0.033 (thick lines) and δ B/B = 0.02 (thin lines). We set δ B/B = 0.02 to emit the optical photons and δ B/B = 0.033 to emit the X-ray photons. Both photon spectra cannot reproduce the multiwavelength data simultaneously. Due to high σ dis, the photon flux of the synchrotron self-Compton scattering is low.
Paper: Multiwavelength Emission from Jets and Magnetically Arrested Disks in Nearby Radio Galaxies: Application to M87
Authors: Riku Kuze, Shigeo S. Kimura, Kenji Toma
Figure caption: Magnetization parameters for M87 with p = 1.0,  p tail = 2.5. The red line is σ ±, and the blue dashed line is ﹩{B}_{\mathrm{rec}}^{2}/(4\pi {n}_{\pm ,\mathrm{tot}}{m}_{e}{c}^{2})﹩. The vertical gray dotted–dashed line and dashed line are magnetization parameters of E  γ,σ  = (2m  e  c 2)/E  γ,rad and E  γ,σ  = E thr, respectively.
Paper: Multiwavelength Emission from Jets and Magnetically Arrested Disks in Nearby Radio Galaxies: Application to M87
Authors: Riku Kuze, Shigeo S. Kimura, Kenji Toma
Figure caption: Magnetization parameters for BH mass of 109  M ⊙ as a function of ﹩\dot{m}﹩, calculated in the methods of A. Y. Chen et al. (2023, red solid line) and S. S. Kimura et al. (2022, blue dashed line) and estimated by Equation (B3) (green dashed–dotted line).
Paper: Multiwavelength Emission from Jets and Magnetically Arrested Disks in Nearby Radio Galaxies: Application to M87
Authors: Riku Kuze, Shigeo S. Kimura, Kenji Toma
Figure caption: Estimated magnetization parameter for the power-law tail distribution as a function of the tail index (red solid line) and the magnetization parameter estimated in the way of A. Y. Chen et al. (2023, gray dashed line).
Paper: Multiwavelength Emission from Jets and Magnetically Arrested Disks in Nearby Radio Galaxies: Application to M87
Authors: Riku Kuze, Shigeo S. Kimura, Kenji Toma
Figure caption: Same as Figure 4, but for the acceleration by the Alfvén wave dissipation.
Paper: Multiwavelength Emission from Jets and Magnetically Arrested Disks in Nearby Radio Galaxies: Application to M87
Authors: Riku Kuze, Shigeo S. Kimura, Kenji Toma
Figure caption: Same as Figure 3, but for the acceleration by the Alfvén wave dissipation. We set the power-law index as 1.3 to achieve the high synchrotron photon flux.
Paper: Identifying New High-confidence Polluted White Dwarf Candidates Using Gaia XP Spectra and Self-organizing Maps
Authors: Xabier Pérez-Couto, Lara Pallas-Quintela, Minia Manteiga, Eva Villaver, Carlos Dafonte
Figure caption: SOM with our sample of 66,337 clean sources. WDs with known spectral types in the MWDD catalog appear in different colors, and candidates are invisible to enhance visualization.
Paper: Identifying New High-confidence Polluted White Dwarf Candidates Using Gaia XP Spectra and Self-organizing Maps
Authors: Xabier Pérez-Couto, Lara Pallas-Quintela, Minia Manteiga, Eva Villaver, Carlos Dafonte
Figure caption: SOM of the Gaia–SDSS spectroscopic sample after 5 × 104 iterations. SDSS-confirmed WDs are shown in blue and SDSS and synthetic contaminants in red. The sidebar shows the IND or how similar are the objects within the same neuron.
Paper: Identifying New High-confidence Polluted White Dwarf Candidates Using Gaia XP Spectra and Self-organizing Maps
Authors: Xabier Pérez-Couto, Lara Pallas-Quintela, Minia Manteiga, Eva Villaver, Carlos Dafonte
Figure caption: Normalized median spectra for the neurons with identified polluted WDs.
Paper: Identifying New High-confidence Polluted White Dwarf Candidates Using Gaia XP Spectra and Self-organizing Maps
Authors: Xabier Pérez-Couto, Lara Pallas-Quintela, Minia Manteiga, Eva Villaver, Carlos Dafonte
Figure caption: Confusion matrix of the SOM classification for WD primary spectral types with respect to MWDD classification.
Paper: Identifying New High-confidence Polluted White Dwarf Candidates Using Gaia XP Spectra and Self-organizing Maps
Authors: Xabier Pérez-Couto, Lara Pallas-Quintela, Minia Manteiga, Eva Villaver, Carlos Dafonte
Figure caption: Normalized median spectra of WDs with confirmed spectral classification in the MWDD and identified candidates for several neurons.
Paper: Identifying New High-confidence Polluted White Dwarf Candidates Using Gaia XP Spectra and Self-organizing Maps
Authors: Xabier Pérez-Couto, Lara Pallas-Quintela, Minia Manteiga, Eva Villaver, Carlos Dafonte
Figure caption: Density histograms of G-band magnitude for WDs with confirmed spectral classification and WD candidates. No differences between spectral classes were observed.
Paper: Identifying New High-confidence Polluted White Dwarf Candidates Using Gaia XP Spectra and Self-organizing Maps
Authors: Xabier Pérez-Couto, Lara Pallas-Quintela, Minia Manteiga, Eva Villaver, Carlos Dafonte
Figure caption: Parallax relative error distribution (density in log scale) of the 66,337 WD candidates and of the 38,507 sources classified as possible contaminants.
Paper: Identifying New High-confidence Polluted White Dwarf Candidates Using Gaia XP Spectra and Self-organizing Maps
Authors: Xabier Pérez-Couto, Lara Pallas-Quintela, Minia Manteiga, Eva Villaver, Carlos Dafonte
Figure caption: CMD of Gaia–SDSS spectroscopically confirmed WDs (blue) and contaminants (red).
Paper: Identifying New High-confidence Polluted White Dwarf Candidates Using Gaia XP Spectra and Self-organizing Maps
Authors: Xabier Pérez-Couto, Lara Pallas-Quintela, Minia Manteiga, Eva Villaver, Carlos Dafonte
Figure caption: UMAP of M. L. Kao et al. (2024) with all of their WD candidates in blue and our DZ and DZA candidates in red and orange, respectively. The black dotted lines served us to discriminate the polluted WD candidates identified in their work from those identified here.
Paper: Identifying New High-confidence Polluted White Dwarf Candidates Using Gaia XP Spectra and Self-organizing Maps
Authors: Xabier Pérez-Couto, Lara Pallas-Quintela, Minia Manteiga, Eva Villaver, Carlos Dafonte
Figure caption: Intraneuron distance distribution for the SOM used for filtering out contaminants from reliable WDs (see Figure 2). Neuron 0 is z 0,0, 1 is z 0,1, 5 is z 1,0, and so on.
Paper: Identifying New High-confidence Polluted White Dwarf Candidates Using Gaia XP Spectra and Self-organizing Maps
Authors: Xabier Pérez-Couto, Lara Pallas-Quintela, Minia Manteiga, Eva Villaver, Carlos Dafonte
Figure caption: Intraneuron distance distribution for the SOM used for spectral classification (see Figure 3). Neuron 0 is z 0,0, 1 is z 0,1, 8 is z 1,0, and so on.
Paper: Identifying New High-confidence Polluted White Dwarf Candidates Using Gaia XP Spectra and Self-organizing Maps
Authors: Xabier Pérez-Couto, Lara Pallas-Quintela, Minia Manteiga, Eva Villaver, Carlos Dafonte
Figure caption: Confusion matrices of our work (the predicted labels) with E. M. García-Zamora et al. (2023) (a) and O. Vincent et al. (2024) (b) (the true labels). The numbers in each cell have the same meaning as those in Figure 5.
Paper: Identifying New High-confidence Polluted White Dwarf Candidates Using Gaia XP Spectra and Self-organizing Maps
Authors: Xabier Pérez-Couto, Lara Pallas-Quintela, Minia Manteiga, Eva Villaver, Carlos Dafonte
Figure caption: Density histograms of T eff assuming mixed H and He atmospheres from N. P. Gentile Fusillo et al. (2021) for DZA and DZ neurons in bins of 100 K.
Paper: Searching for Radio Late-type Dwarf Stars in the GLEAM-X DR1 Catalog
Authors: Qichen Huang, 启宸 黄, Biwei Jiang, 碧沩 姜, Zehao Zhang, 泽浩 张, Albert Zijlstra
Figure caption: The near-infrared (J − H)0/(H − W1)0 diagram. The red dots represent the 988 sources selected by the quality screening of 2MASS and WISE observations, and the green dots represent the 541 dwarf stars selected by the Gaia CMD obtained in Section 3.1 with infrared data. The blue crosses represent the 536 galaxies from the SIMBAD database with infrared data. The solid-blue line represents the intrinsic color indices of F0-M5 spectral type dwarfs by M. J. Pecaut & E. E. Mamajek (2013), where positions further to the right correspond to later spectral type stars, and the dashed lines above and below represent a 0.1 mag offset. The black-dashed line represents the border for dwarf classification we set, i.e., (J − H)0 = (H − W1)0 + 1.3.
Paper: Searching for Radio Late-type Dwarf Stars in the GLEAM-X DR1 Catalog
Authors: Qichen Huang, 启宸 黄, Biwei Jiang, 碧沩 姜, Zehao Zhang, 泽浩 张, Albert Zijlstra
Figure caption: The ﹩{({\rm{NUV}}-{G}_{\mathrm{BP}})}_{0}﹩ vs. ﹩{({G}_{\mathrm{BP}}-{G}_{\mathrm{RP}})}_{0}﹩ diagram for the 89 sources cross-matched with the GALEX/DR6 + 7 catalog. The color bar encodes the effective temperature. The black-dashed line distinguishes five sources with ultraviolet excess on the right side.
Paper: Searching for Radio Late-type Dwarf Stars in the GLEAM-X DR1 Catalog
Authors: Qichen Huang, 启宸 黄, Biwei Jiang, 碧沩 姜, Zehao Zhang, 泽浩 张, Albert Zijlstra
Figure caption: The result of the cross-match between Gleam-X and Gaia/DR3 within a 5″ radius. The initial data are shown in purple, which contains 15,365 sources, and the selected data in green, reduced to 7654 sources after filtering with the Angular distance ﹩\lt \sqrt{{\left({E}_{{\rm{R}}.{\rm{A}}.}\times \cos \delta \right)}^{2}+{E}_{\mathrm{decl}.}^{2})}﹩.
Paper: Searching for Radio Late-type Dwarf Stars in the GLEAM-X DR1 Catalog
Authors: Qichen Huang, 启宸 黄, Biwei Jiang, 碧沩 姜, Zehao Zhang, 泽浩 张, Albert Zijlstra
Figure caption: The relationship between Rossby number and rotation period for the 13 periodic variable late-type dwarf stars. The blue-dashed line represents the boundary at Ro = 0.13, where stars to the left side of the dashed line can be identified as sources with stronger chromospheric activity. The colors indicate the effective temperature of the stars, with all temperatures being above 3500 K, allowing for activity assessment based on the Rossby number.
Paper: Searching for Radio Late-type Dwarf Stars in the GLEAM-X DR1 Catalog
Authors: Qichen Huang, 启宸 黄, Biwei Jiang, 碧沩 姜, Zehao Zhang, 泽浩 张, Albert Zijlstra
Figure caption: The Gaia color–magnitude diagram of the sample. The x-axis is ﹩{({G}_{\mathrm{BP}}-{G}_{\mathrm{RP}})}_{0}﹩ color index after subtracting the interstellar extinction effects and the y-axis is the absolute magnitude in the Gaia G-band. The color bar decodes the extinction in the G-band. The red and green dots are the sources that we identified as radio late-type dwarfs by UV excess and TESS rotation period, respectively.
Paper: Searching for Radio Late-type Dwarf Stars in the GLEAM-X DR1 Catalog
Authors: Qichen Huang, 启宸 黄, Biwei Jiang, 碧沩 姜, Zehao Zhang, 泽浩 张, Albert Zijlstra
Figure caption: The J − H/H − W1 color–color diagram of 1989 sources displays the Pstar value for each source. The black-dashed line is consistent with the black-dashed line in Figure 3, which represents the border for dwarf classification we set, i.e., (J − H) = (H − W1) + 1.3.
Paper: Searching for Radio Late-type Dwarf Stars in the GLEAM-X DR1 Catalog
Authors: Qichen Huang, 启宸 黄, Biwei Jiang, 碧沩 姜, Zehao Zhang, 泽浩 张, Albert Zijlstra
Figure caption: The light curve of TIC 124984182 within about 12 days, which shows obvious periodic light variation and some prominent flares, with a rotation period of 1.475 days and an effective temperature of 5795 K corresponding to a G2-type star.
Paper: Searching for Radio Late-type Dwarf Stars in the GLEAM-X DR1 Catalog
Authors: Qichen Huang, 启宸 黄, Biwei Jiang, 碧沩 姜, Zehao Zhang, 泽浩 张, Albert Zijlstra
Figure caption: Comparison between model and observed NUV fractional flux densities.
Paper: Volatile Element Depletion of Carbonaceous Chondrites—Insights from Mass-dependent Zinc, Cadmium, and Tellurium Isotope Variations
Authors: Elin M. Morton, Harvey Pickard, Frank Wombacher, Yihang Huang, Emeliana Palk, Rayssa Martins, Sven Kuthning, Maria Schönbächler, Mark Rehkämper
Figure caption: Zn, Cd, and Te isotope compositions and concentrations of the carbonaceous chondrites. Data from this study are shown as outlined diamonds and can be found in Table 1. Literature data are shown as non-outlined diamonds and are compiled in Table A5. The Cd data of F. Wombacher et al. (2003, 2008) are not included, due to the large uncertainties of the results.
Paper: Volatile Element Depletion of Carbonaceous Chondrites—Insights from Mass-dependent Zinc, Cadmium, and Tellurium Isotope Variations
Authors: Elin M. Morton, Harvey Pickard, Frank Wombacher, Yihang Huang, Emeliana Palk, Rayssa Martins, Sven Kuthning, Maria Schönbächler, Mark Rehkämper
Figure caption: Column plot showing the maximum Zn-normalized within-group variations of the Zn, Cd, and Te isotope compositions for different CC groups. The plotted data are from this study (Table 1) and the literature (Table A2). The CM and CR data exclude samples that were affected by impact-induced heating after low-temperature aqueous alteration (see text for details). The ΔZZn max-min notation is defined in the main text.
Paper: Volatile Element Depletion of Carbonaceous Chondrites—Insights from Mass-dependent Zinc, Cadmium, and Tellurium Isotope Variations
Authors: Elin M. Morton, Harvey Pickard, Frank Wombacher, Yihang Huang, Emeliana Palk, Rayssa Martins, Sven Kuthning, Maria Schönbächler, Mark Rehkämper
Figure caption: Plots of Mg-normalized concentrations of (a) Zn and Cd, (b) Zn and Te, and (c) Cd and Te for the CCs analyzed in this study. The solid black lines represent the best-fit regressions for the samples of this study; the gray dashed lines are the CI reference lines. Zinc, Cd, and Te concentrations are from Table 1, and Mg concentrations from Table A1. The Mg concentrations of Ivuna, Murchison-3, and Allende-3 were not measured in this study, and are from N. Braukmüller et al. (2018). The Te data for CK chondrites are not plotted in (b) and (c), as the concentrations are strongly altered by parent-body processing. The legend in (a) applies to all panels. The CI reference lines were calculated based on data from this study (Table 1), J.-M. Luck et al. (2005), R. G. A. Baker et al. (2010), J. A. Barrat et al. (2012), N. Braukmüller et al. (2018), M. A. Fehr et al. (2018), and J. L. Hellmann et al. (2020).
Paper: Volatile Element Depletion of Carbonaceous Chondrites—Insights from Mass-dependent Zinc, Cadmium, and Tellurium Isotope Variations
Authors: Elin M. Morton, Harvey Pickard, Frank Wombacher, Yihang Huang, Emeliana Palk, Rayssa Martins, Sven Kuthning, Maria Schönbächler, Mark Rehkämper
Figure caption: Plot of (a), (b) δ 66Zn vs. δ 114Cd, (c), (d) δ 114Cd vs. δ130Te, and (e), (f) δ 66Zn vs. δ 130Te for the CCs analyzed in this study. Isotope data are from Table 1.
Paper: Volatile Element Depletion of Carbonaceous Chondrites—Insights from Mass-dependent Zinc, Cadmium, and Tellurium Isotope Variations
Authors: Elin M. Morton, Harvey Pickard, Frank Wombacher, Yihang Huang, Emeliana Palk, Rayssa Martins, Sven Kuthning, Maria Schönbächler, Mark Rehkämper
Figure caption: Plot of δ 130Te vs. Te concentrations for CK chondrites. The plot also shows the modeled CK compositions resulting from progressive loss of Te from a CV3 starting composition (with δ 130Te = 0.53 ± 0.17‰ and 925 ± 17 ng g−1 Te) and associated open-system Rayleigh isotope fractionation. The curve is labeled with the value of the best-fit isotope fractionation factor that was employed in the modeling.
Paper: Volatile Element Depletion of Carbonaceous Chondrites—Insights from Mass-dependent Zinc, Cadmium, and Tellurium Isotope Variations
Authors: Elin M. Morton, Harvey Pickard, Frank Wombacher, Yihang Huang, Emeliana Palk, Rayssa Martins, Sven Kuthning, Maria Schönbächler, Mark Rehkämper
Figure caption: Concentrations of main component and volatile elements for carbonaceous chondrites, normalized to the CI chondrite and Fe concentration data of K. Lodders (2003). Elements are sorted along the x-axis by increasing volatility from left to right, based on the condensation temperatures of K. Lodders (2003).
Paper: Searching for Radio Late-type Dwarf Stars in the GLEAM-X DR1 Catalog
Authors: Qichen Huang, 启宸 黄, Biwei Jiang, 碧沩 姜, Zehao Zhang, 泽浩 张, Albert Zijlstra
Figure caption: The distribution of all 12 identified radio stars on color–magnitude diagram, with colors indicating the radio luminosity calculated through distance from PYSSED and peak flux from GLEAM-X.
Paper: Searching for Radio Late-type Dwarf Stars in the GLEAM-X DR1 Catalog
Authors: Qichen Huang, 启宸 黄, Biwei Jiang, 碧沩 姜, Zehao Zhang, 泽浩 张, Albert Zijlstra
Figure caption: The phase-folded light curves of the seven stars. Points deviating more than 3σ are removed to eliminate some unreasonable data caused by the section switching of TESS.
Paper: Volatile Element Depletion of Carbonaceous Chondrites—Insights from Mass-dependent Zinc, Cadmium, and Tellurium Isotope Variations
Authors: Elin M. Morton, Harvey Pickard, Frank Wombacher, Yihang Huang, Emeliana Palk, Rayssa Martins, Sven Kuthning, Maria Schönbächler, Mark Rehkämper
Figure caption: Plot of δ 66Zn, δ 114Cd, and δ 130Te vs. ε 54Cr (a)–(c); ε 96Zr (d)–(f); ε 50Ti (g)–(i); and ε 64Zn (j)–(l) for mean CC group compositions calculated using data from this and previous studies (Table A2). ε 50Ti, ε 54Cr, and ε 96Zr are the weighted mean values from M. Rufenacht et al. (2023). The ε 66Zn values are from R. Martins et al. (2023, 2024), P. S. Savage et al. (2022), T. Steller et al. (2022), and M. Paquet et al. (2023). Dotted lines denote mixing between CI and the NME-chondrule endmember; dashed lines represent mixing between CI and the NME-CAI endmember. The endmember compositions are defined in Tables 2 and 3.