adsabs/AstroCLIMB huggingface dataset:
Paper: Revisiting X-Ray-bright Optically Normal Galaxies with the Chandra Source Catalog
Authors: Dong-Woo Kim, Amanda Malnati, Alyssa Cassity, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan
Figure caption: Left: the HR(ms) distribution of the QSO sample in blue. The black points for the normal galaxy sample are the same as in Figure 5. Right: the QSO sample is divided into three L X bins. The vertical green dashed lines correspond to those in Figure 4. The number next to the object type in the legend box indicates the scaling factor of each distribution.
Paper: Revisiting X-Ray-bright Optically Normal Galaxies with the Chandra Source Catalog
Authors: Dong-Woo Kim, Amanda Malnati, Alyssa Cassity, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan
Figure caption: Predicted HR(ms) for a range of emission and absorption model parameters. Marked by the vertical green dashed lines are the HR(ms) of the typical unabsorbed AGN (power-law slope of 1.7 and N H = 3 × 1020 cm−2), absorbed AGN (power-law slope of 1.7 and N H = 1022 cm−2), and the emission of a hot-gas-rich galaxy (APEC with 1 keV gas and N H = 3 × 1020 cm−2).
Paper: Revisiting X-Ray-bright Optically Normal Galaxies with the Chandra Source Catalog
Authors: Dong-Woo Kim, Amanda Malnati, Alyssa Cassity, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan
Figure caption: The redshift distributions of the normal galaxy, XBONG, and QSO samples.
Paper: Revisiting X-Ray-bright Optically Normal Galaxies with the Chandra Source Catalog
Authors: Dong-Woo Kim, Amanda Malnati, Alyssa Cassity, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan
Figure caption: Same as Figure 1, but each subclass is separately plotted (left) for the Galaxy class and (right) for the QSO class. In each panel, we specify the subclass: N/A (not specified), SF (=star-forming), BROAD LINE (broad emission lines), and AGN (narrow nuclear emission lines including LINERs). The red diagonal line is the best-fit relation of galaxies as in Figure 1.
Paper: Revisiting X-Ray-bright Optically Normal Galaxies with the Chandra Source Catalog
Authors: Dong-Woo Kim, Amanda Malnati, Alyssa Cassity, Giuseppina Fabbiano, Juan Rafael Martinez Galarza, Ewan O'Sullivan
Figure caption: Same as the left panel of Figure 7 for QSOs and XBONGs, but with the hardness ratio derived from the hard and medium CSC2 photometric bands.
Paper: 3D MHD Time-dependent Charge State Ionization and Recombination Modeling of the Bastille Day Coronal Mass Ejection
Authors: Yeimy J. Rivera, John C. Raymond, Katharine K. Reeves, Susan T. Lepri, Roberto Lionello, Cooper Downs, Maurice L. Wilson, Nicolas Trueba
Figure caption: Stack plot showing the in situ observations for the Bastille Day CME, within the red vertical solid and dashed lines. Panels (a)–(c) show the relative charge state distributions for carbon, oxygen, and iron, with a red curve in panel (c) showing the 〈Q Fe〉. Panel (d) shows the O7+/O6+ and C6+/C5+ ion ratios; panel (e) shows the elemental composition of Mg/O, Fe/O, Si/O, S/O, C/O, N/O, and Ne/O compared to its photospheric ratio; and panels (f)–(h) show the proton temperature, speed, and density, respectively. Lastly, panel (i) shows the magnetic field components and magnitude.
Paper: 3D MHD Time-dependent Charge State Ionization and Recombination Modeling of the Bastille Day Coronal Mass Ejection
Authors: Yeimy J. Rivera, John C. Raymond, Katharine K. Reeves, Susan T. Lepri, Roberto Lionello, Cooper Downs, Maurice L. Wilson, Nicolas Trueba
Figure caption: Heated prominence material tracer evolution matched to the second part of the CME. Panels are the same as in Figure 3.
Paper: 3D MHD Time-dependent Charge State Ionization and Recombination Modeling of the Bastille Day Coronal Mass Ejection
Authors: Yeimy J. Rivera, John C. Raymond, Katharine K. Reeves, Susan T. Lepri, Roberto Lionello, Cooper Downs, Maurice L. Wilson, Nicolas Trueba
Figure caption: Three time stamps in the simulation showing (top row) two shock heating isosurfaces, along with Fe16+ and two temperature isosurfaces. The bottom row shows three 〈Q Fe〉 isosurfaces at the same time steps. The spheres show the location of the plasma tracked in the hot flux rope material (gray) and prominence structure (black) from Figures 3 and 4, respectively, along with the connected magnetic field line at the associated time step.
Paper: 3D MHD Time-dependent Charge State Ionization and Recombination Modeling of the Bastille Day Coronal Mass Ejection
Authors: Yeimy J. Rivera, John C. Raymond, Katharine K. Reeves, Susan T. Lepri, Roberto Lionello, Cooper Downs, Maurice L. Wilson, Nicolas Trueba
Figure caption: Hot flux rope material tracer evolution matched to the first part of the CME. Top to bottom: C, O, and Fe fractional charge state distributions; proton and electron temperature and density; and bulk speed. The bottom row shows the final, freeze-in, simulated charge state distributions at 20 R ⊙ of C, O, and Fe (blue bars), along with the observed ions from ACE/SWICS (black curve).
Paper: 3D MHD Time-dependent Charge State Ionization and Recombination Modeling of the Bastille Day Coronal Mass Ejection
Authors: Yeimy J. Rivera, John C. Raymond, Katharine K. Reeves, Susan T. Lepri, Roberto Lionello, Cooper Downs, Maurice L. Wilson, Nicolas Trueba
Figure caption: Three time stamps in the simulation showing the two plasma tracks in the hot flux rope material (gray) and prominence structure (black) from Figures 3 and 4, respectively. We include two additional field lines different from Figure 5, in light blue, that capture the main flux rope structure. The panels include the distribution of the 〈Q Fe〉 across a plane intercepting the polarity inversion line at the active region. The wedge illustrates regions of 〈Q Fe〉 between 6 and 16+ across the flux rope evolution.
Paper: 3D MHD Time-dependent Charge State Ionization and Recombination Modeling of the Bastille Day Coronal Mass Ejection
Authors: Yeimy J. Rivera, John C. Raymond, Katharine K. Reeves, Susan T. Lepri, Roberto Lionello, Cooper Downs, Maurice L. Wilson, Nicolas Trueba
Figure caption: Mean charge state distributions of C, O, and Fe from ACE/SWICS for DOY 197.8–198.2 (top row) and DOY 198.8–199.2 (bottom row).
Paper: 3D MHD Time-dependent Charge State Ionization and Recombination Modeling of the Bastille Day Coronal Mass Ejection
Authors: Yeimy J. Rivera, John C. Raymond, Katharine K. Reeves, Susan T. Lepri, Roberto Lionello, Cooper Downs, Maurice L. Wilson, Nicolas Trueba
Figure caption: Heating terms along the two tracer particle trajectories, where the black curve represents the prominence material and the gray curve represents the hot flux rope material in connection with the tracks in Figure 5.
Paper: KIC 9845907: A δ Scuti Star with the First Overtone as the Dominant Frequency and with Many Equidistant Structures in Its Spectrum
Authors: Xiao-Ya Sun, Zhao-Yu Zuo, Tao-Zhi Yang, Antonio García Hernández
Figure caption: In the left panel, the black, gray, and blue lines represent the Fourier transform (FT), the histogram of frequency differences (HFD), and the autocorrelation function (AC), respectively, using the methodology of García Hernández et al. (2013) and Ramón-Ballesta et al. (2021). The red dotted–dashed line indicates the possible value of Δν = 5.25 day−1. The right panel shows the echelle diagram of the frequencies. The value of 60.8 μHz is used for the plot.
Paper: KIC 9845907: A δ Scuti Star with the First Overtone as the Dominant Frequency and with Many Equidistant Structures in Its Spectrum
Authors: Xiao-Ya Sun, Zhao-Yu Zuo, Tao-Zhi Yang, Antonio García Hernández
Figure caption: Two pairs of quintuplet structures in SC spectrum of KIC 9845907. The vertical blue dotted lines indicate the locations of frequencies. We marked the two pairs as Q1 (upper panel) and Q2 (lower panel), sorted according to the increasing value of the central frequency, respectively. The intervals from the side peaks to the center are marked with f  m1 = 0.065 day−1 and f  m2 = 1.693 day−1, respectively. In the upper and lower panels, the zoomed-in view of the central triplets can be seen in Figure 4 (i.e., T7 and T10) for clarity.
Paper: KIC 9845907: A δ Scuti Star with the First Overtone as the Dominant Frequency and with Many Equidistant Structures in Its Spectrum
Authors: Xiao-Ya Sun, Zhao-Yu Zuo, Tao-Zhi Yang, Antonio García Hernández
Figure caption: Twelve pairs of equidistant frequency-triplet structures in the SC spectrum of KIC 9845907. The vertical blue dotted lines indicate the locations of the detected frequencies, where f  m1 = 0.065 day−1 represents the spacing. We marked the triplets with f  m1 as T1 to T12 sorted according to the increasing value of the central frequency.
Paper: KIC 9845907: A δ Scuti Star with the First Overtone as the Dominant Frequency and with Many Equidistant Structures in Its Spectrum
Authors: Xiao-Ya Sun, Zhao-Yu Zuo, Tao-Zhi Yang, Antonio García Hernández
Figure caption: Two pairs of equidistant frequency-triplet structures in SC spectrum of KIC 9845907. The vertical blue dotted lines indicate the locations of frequencies, where f  m2 = 1.693 day−1 represents the equally spaced frequency. We marked the triplets with f  m2 as T13 and T14 according to Table 2.
Paper: KIC 9845907: A δ Scuti Star with the First Overtone as the Dominant Frequency and with Many Equidistant Structures in Its Spectrum
Authors: Xiao-Ya Sun, Zhao-Yu Zuo, Tao-Zhi Yang, Antonio García Hernández
Figure caption: Evolutionary tracks from the zero-age MS to the post-MS for the four candidate models, as listed in Table 4. The black rectangle marks the 1σ error box of the effective temperature T eff and the luminosity L, while the diamonds mark the minimum χ 2 for each specific model by fitting the observed f 1 = 17.597 day−1 and f 3 = 31.428 day−1 with the theoretical values.
Paper: KIC 9845907: A δ Scuti Star with the First Overtone as the Dominant Frequency and with Many Equidistant Structures in Its Spectrum
Authors: Xiao-Ya Sun, Zhao-Yu Zuo, Tao-Zhi Yang, Antonio García Hernández
Figure caption: Amplitude variations of the components of Triplet 4 (T4) and Triplet 2 (T2). Two dominant frequencies, f  m1 and f 1, are also shown for comparison.
Paper: KIC 9845907: A δ Scuti Star with the First Overtone as the Dominant Frequency and with Many Equidistant Structures in Its Spectrum
Authors: Xiao-Ya Sun, Zhao-Yu Zuo, Tao-Zhi Yang, Antonio García Hernández
Figure caption: The same as in Figure 7 but for phase variations of the modes.
Paper: Three-dimensional Simulation of Thermodynamics on Confined Turbulence in a Large-scale CME-flare Current Sheet
Authors: Jing Ye, John C. Raymond, Zhixing Mei, Qiangwei Cai, Yuhao Chen, Yan Li, Jun Lin
Figure caption: Log of density (first column), temperature (second column), adiabatic term (third column), ohmic heating (fourth column), and thermal conduction (fifth column) for the x-z plane at the center (y  =  0) at different times. Note that the contribution from adiabatic, ohmic heating, and thermal conduction is shown in cgs units for better understanding of the plasma heating process in the CS.
Paper: Three-dimensional Simulation of Thermodynamics on Confined Turbulence in a Large-scale CME-flare Current Sheet
Authors: Jing Ye, John C. Raymond, Zhixing Mei, Qiangwei Cai, Yuhao Chen, Yan Li, Jun Lin
Figure caption: Plots of quantities along the central line (x = 0) in Figure 6 at the same times as in this figure: density and temperature (first row), heating terms and change in the temperature (dT/dt), and heat transport terms. The vertical dashed lines mark the CS ends.
Paper: Three-dimensional Simulation of Thermodynamics on Confined Turbulence in a Large-scale CME-flare Current Sheet
Authors: Jing Ye, John C. Raymond, Zhixing Mei, Qiangwei Cai, Yuhao Chen, Yan Li, Jun Lin
Figure caption: Face-on view of the CME-flare CS at given times t = 0.52, 0.96, and 1.42. From left to right for each row, there are the current density ∣J∣, velocities V  y , V  z  in the y- and z-directions, and the synthetic EUV image for AIA 131 Å. The black solid lines in the first column are the PX lines. Note that ∣J∣, V  y , V  z  are averaged over the LOS for x ∈  [−0.1, 0.1].
Paper: Three-dimensional Simulation of Thermodynamics on Confined Turbulence in a Large-scale CME-flare Current Sheet
Authors: Jing Ye, John C. Raymond, Zhixing Mei, Qiangwei Cai, Yuhao Chen, Yan Li, Jun Lin
Figure caption: Distributions of the turbulent kinetic and magnetic energy density at different evolution times t = 0.96, 1.42, and 1.64.
Paper: Three-dimensional Simulation of Thermodynamics on Confined Turbulence in a Large-scale CME-flare Current Sheet
Authors: Jing Ye, John C. Raymond, Zhixing Mei, Qiangwei Cai, Yuhao Chen, Yan Li, Jun Lin
Figure caption: Fourier power spectra of the velocity in the x-, y-, and z-directions for different parts of the CS as a function of the wavenumber k. The red and black dotted lines in each panel denote the spectral slopes in the x- and z-directions, respectively, for different regions.
Paper: Three-dimensional Simulation of Thermodynamics on Confined Turbulence in a Large-scale CME-flare Current Sheet
Authors: Jing Ye, John C. Raymond, Zhixing Mei, Qiangwei Cai, Yuhao Chen, Yan Li, Jun Lin
Figure caption: Detailed evolution of the downward blobs from t = 1.38 to t = 1.44. (a–d) Structures of the blobs shown by the current isosurface with value ∣J∣ = 50 colored by the velocity along the z-direction V  z  at the successive times. (e–h) 3D magnetic structures of the blob. Note that the colors for the magnetic field lines are used to better display the different lines.
Paper: Three-dimensional Simulation of Thermodynamics on Confined Turbulence in a Large-scale CME-flare Current Sheet
Authors: Jing Ye, John C. Raymond, Zhixing Mei, Qiangwei Cai, Yuhao Chen, Yan Li, Jun Lin
Figure caption: Detailed evolution of an antisunward blob from t = 1.56 to 1.64. The physical terms are the same as in Figure 11.
Paper: Three-dimensional Simulation of Thermodynamics on Confined Turbulence in a Large-scale CME-flare Current Sheet
Authors: Jing Ye, John C. Raymond, Zhixing Mei, Qiangwei Cai, Yuhao Chen, Yan Li, Jun Lin
Figure caption: Log of density (first column), temperature (second column), and current normal to plane for the x-z plane at the center (y  =  0) at t = 1.58. (a) Run A; (b) Run B.
Paper: CMR Exploration. II. Filament Identification with Machine Learning
Authors: Duo Xu, Shuo Kong, Avichal Kaul, Héctor G. Arce, Volker Ossenkopf-Okada
Figure caption: Detection of CMR filament candidates in the Taurus B213 region using CASI-2D and the diffusion model. Note that the dust image displayed in this figure has been rotated by a certain degree to minimize the presence of blank regions in the four corners. Consequently, the coordinates in the image no longer align with the x- or y-axes, but instead follow the trajectory indicated by the white dashed line in the figure. A similar rotation has been applied to Figures 8 and 9.
Paper: CMR Exploration. II. Filament Identification with Machine Learning
Authors: Duo Xu, Shuo Kong, Avichal Kaul, Héctor G. Arce, Volker Ossenkopf-Okada
Figure caption: Detection of CMR filament candidates in the Orion A north region using CASI-2D and the diffusion model. Note that the stick-like filament in this region has previously been identified as a high-confidence CMR candidate in K21.
Paper: CMR Exploration. II. Filament Identification with Machine Learning
Authors: Duo Xu, Shuo Kong, Avichal Kaul, Héctor G. Arce, Volker Ossenkopf-Okada
Figure caption: Detection of CMR filament candidates in the Auriga–California Cloud region using CASI-2D and the diffusion model.
Paper: CMR Exploration. II. Filament Identification with Machine Learning
Authors: Duo Xu, Shuo Kong, Avichal Kaul, Héctor G. Arce, Volker Ossenkopf-Okada
Figure caption: Performance of CASI-2D and the diffusion model in identifying CMR filaments on cropped synthetic images that do not contain CMR filaments.
Paper: CMR Exploration. II. Filament Identification with Machine Learning
Authors: Duo Xu, Shuo Kong, Avichal Kaul, Héctor G. Arce, Volker Ossenkopf-Okada
Figure caption: Performance of machine-learning approaches in identifying CMR filaments on synthetic images containing bright blobs.
Paper: CMR Exploration. II. Filament Identification with Machine Learning
Authors: Duo Xu, Shuo Kong, Avichal Kaul, Héctor G. Arce, Volker Ossenkopf-Okada
Figure caption: Similar to Figure 2, but including supplementary panels showcasing the filaments detected by FilFinder. Long filaments are represented by red lines, while short filaments are represented by white lines.
Paper: CMR Exploration. II. Filament Identification with Machine Learning
Authors: Duo Xu, Shuo Kong, Avichal Kaul, Héctor G. Arce, Volker Ossenkopf-Okada
Figure caption: Performance of CASI-2D and the diffusion model in identifying CMR filaments on combined synthetic images that do not contain CMR filaments.
Paper: A Titov–Démoulin Type Eruptive Event Generator for β > 0 Plasmas
Authors: Igor V. Sokolov, Tamas I Gombosi
Figure caption: Left panel: same as in Figure 4, with superposed uniform strapping field, B (s)= −L 0 B  c /(2π μ 0 R ∞), where the inductance for n = 0 harmonics is given by Equation (108) below. White lines: field lines of the poloidal field (B  z , B  r ). Color: toroidal magnetic field, B  φ , perpendicular to the image plane, the outgoing field being positive, and the incoming one being negative. The figure corresponds to positive helicity; otherwise, the blue and red circles would swap. Right panel: close-up image of the cross section of the plasma filament. Coincidence of the filament boundary (yellow color) with the magnetic surface (white line) demonstrates that the equilibrium condition is satisfied.
Paper: A Titov–Démoulin Type Eruptive Event Generator for β > 0 Plasmas
Authors: Igor V. Sokolov, Tamas I Gombosi
Figure caption: Left panel: solution of the reduced GS equation, in the meridional cross section (z, r plane), for ﹩{R}_{\infty }=1,{\kappa }_{0}^{{\prime} }=0.1,{B}_{c}=1﹩ and positive helicity. White lines: field lines of the poloidal field (B  z , B  r ). Color: toroidal magnetic field, B  φ , perpendicular to the image plane, outgoing field being positive, incoming one being negative. The figure corresponds to positive helicity; otherwise, the blue and red circles would swap. Right panel: close-up image of the cross section of the plasma filament.
Paper: A Titov–Démoulin Type Eruptive Event Generator for β > 0 Plasmas
Authors: Igor V. Sokolov, Tamas I Gombosi
Figure caption: Left panel: amplitudes of poloidal (blue line) and axial (black line) magnetic field components for the current concentrated at the filament boundary. Middle panel: normalized current distributions for uniform (black solid line), parabolic (blue line), and linear surface decrease current (black dashed line) for ε = 0.1. Right panel: amplitudes of poloidal (blue line) and axial magnetic field (black line) components for uniform current (solid lines) and for linear surface decrease current (dashed lines). For ﹩{\kappa }_{0}^{{\prime} }=0.1﹩ (a/R 0 ≈ 0.2) the argument, ﹩{\kappa }^{{\prime} }={R}_{-}/{R}_{+}﹩, ranges from ﹩{\kappa }^{{\prime} }=0﹩ (at the toroidal magnetic axis) to ﹩{\kappa }^{{\prime} }=0.1﹩ at the filament boundary; while ﹩{\kappa }^{{\prime} }\gt 0.1﹩ values correspond to the loop exterior.
Paper: A Titov–Démoulin Type Eruptive Event Generator for β > 0 Plasmas
Authors: Igor V. Sokolov, Tamas I Gombosi
Figure caption: Toroidal coordinate surfaces for R ∞ = 1: ﹩\sinh u=5﹩ (﹩{\kappa }^{{\prime} }\approx 0.1﹩)—orange torus; v = 0—gray part of plane z = 0; v = π/2—blue hemisphere; v = π–invisible part of plane z = 0; v = 3π/2—red hemisphere. Coordinate u decreases outward from the torus and increases inward, turning to infinity at the (invisible) circumference, x 2 + y 2 = 1, z = 0.
Paper: A Titov–Démoulin Type Eruptive Event Generator for β > 0 Plasmas
Authors: Igor V. Sokolov, Tamas I Gombosi
Figure caption: Amplitudes of the toroidal field component for uniform current (solid line) and for linear surface decrease current (dashed line), for the same filament and in the same coordinate as used in Figure 2.
Paper: Photometry and Polarimetry of 2010 XC15: Observational Confirmation of E-type Near-Earth Asteroid Pair
Authors: Jin Beniyama, Shigeyuki Sako, Katsuhito Ohtsuka, Tomohiko Sekiguchi, Masateru Ishiguro, Daisuke Kuroda, Seirato Urakawa, Fumi Yoshida, Asami Takumi, Natsuho Maeda, Jun Takahashi, Seiko Takagi, Hiroaki Saito, Tatsuya Nakaoka, Tomoki Saito, Tomohito Ohshima, Ryo Imazawa, Masato Kagitani, Satoshi Takita
Figure caption: Reflectance spectrum of 2010 XC15 (circles). Vertical bars indicate the 1σ uncertainties. Horizontal bars indicate the filter bandwidths. Visible spectra of other E-types are shown: 1998 WT24 (upper solid line on the right side; Lazzarin et al. 2004) and Nysa (lower solid line on the right side; Bus & Binzel 2002). Template spectra of S- (dashed line), Xe- (dotted line), and Xc-types (dotted–dashed line) are shown (Bus & Binzel 2002; DeMeo & Carry 2013). The reflectance spectra are normalized at 0.617 μm.
Paper: Photometry and Polarimetry of 2010 XC15: Observational Confirmation of E-type Near-Earth Asteroid Pair
Authors: Jin Beniyama, Shigeyuki Sako, Katsuhito Ohtsuka, Tomohiko Sekiguchi, Masateru Ishiguro, Daisuke Kuroda, Seirato Urakawa, Fumi Yoshida, Asami Takumi, Natsuho Maeda, Jun Takahashi, Seiko Takagi, Hiroaki Saito, Tatsuya Nakaoka, Tomoki Saito, Tomohito Ohshima, Ryo Imazawa, Masato Kagitani, Satoshi Takita
Figure caption: Phased lightcurves of 2010 XC15. From top to bottom, the g-, r-, i-, and z-band lightcurves are presented. The lightcurves are folded by the derived period of 2.673 hr. Phase zero is set to JD 2459936.125 (2022 December 22 15:00:00 UT). The lightcurves in each band are horizontally offset by 0.2 mag for the sake of clarity. Bars indicate the 1σ uncertainties.
Paper: Photometry and Polarimetry of 2010 XC15: Observational Confirmation of E-type Near-Earth Asteroid Pair
Authors: Jin Beniyama, Shigeyuki Sako, Katsuhito Ohtsuka, Tomohiko Sekiguchi, Masateru Ishiguro, Daisuke Kuroda, Seirato Urakawa, Fumi Yoshida, Asami Takumi, Natsuho Maeda, Jun Takahashi, Seiko Takagi, Hiroaki Saito, Tatsuya Nakaoka, Tomoki Saito, Tomohito Ohshima, Ryo Imazawa, Masato Kagitani, Satoshi Takita
Figure caption: Phase-corrected lightcurves of 2010 XC15. Phase-corrected lightcurves in the g (circles), r (triangles), i (squares), and z bands (diamonds) are presented. Time zero is set to JD 2459936.125 (2022 December 22 15:00:00 UT). Bars indicate the 1σ uncertainties.
Paper: Photometry and Polarimetry of 2010 XC15: Observational Confirmation of E-type Near-Earth Asteroid Pair
Authors: Jin Beniyama, Shigeyuki Sako, Katsuhito Ohtsuka, Tomohiko Sekiguchi, Masateru Ishiguro, Daisuke Kuroda, Seirato Urakawa, Fumi Yoshida, Asami Takumi, Natsuho Maeda, Jun Takahashi, Seiko Takagi, Hiroaki Saito, Tatsuya Nakaoka, Tomoki Saito, Tomohito Ohshima, Ryo Imazawa, Masato Kagitani, Satoshi Takita
Figure caption: Time variations of colors of 2010 XC15. The g − r (circles), r − i (triangles), and r − z (squares) colors are presented. Time zero is set to JD 2459936.125 (2022 December 22 15:00:00 UT). Bars indicate the 1σ uncertainties.
Paper: Photometry and Polarimetry of 2010 XC15: Observational Confirmation of E-type Near-Earth Asteroid Pair
Authors: Jin Beniyama, Shigeyuki Sako, Katsuhito Ohtsuka, Tomohiko Sekiguchi, Masateru Ishiguro, Daisuke Kuroda, Seirato Urakawa, Fumi Yoshida, Asami Takumi, Natsuho Maeda, Jun Takahashi, Seiko Takagi, Hiroaki Saito, Tatsuya Nakaoka, Tomoki Saito, Tomohito Ohshima, Ryo Imazawa, Masato Kagitani, Satoshi Takita
Figure caption: Lomb–Scargle periodogram of 2010 XC15. The number of harmonics of the model curve is 5.