adsabs/AstroCLIMB huggingface dataset:
Paper: The RS Oph Outburst of 2021 Monitored in X-Rays with NICER
Authors: Marina Orio, Keith Gendreau, Morgan Giese, Gerardo Juan M. Luna, Jozef Magdolen, Tod E. Strohmayer, Andy E. Zhang, Diego Altamirano, Andrej Dobrotka, Teruaki Enoto, Elizabeth C. Ferrara, Richard Ignace, Sebastian Heinz, Craig Markwardt, Joy S. Nichols, Michael L. Parker, Dheeraj R. Pasham, Songpeng Pei, Pragati Pradhan, Ron Remillard, James F. Steiner, Francesco Tombesi
Figure caption: The spectrum of RS Oph observed with NICER in the first ≃1000 s long GTI of day 57 (2021 October 5), fitted with a blackbody at a temperature of 37 eV, absorbing column density N(H) = 4.3 1021 cm−2 with nonsolar abundances of C and O (C/C⊙ = 4.9, N/N⊙ = 2.5), two components of BVAPEC thermal plasma at 81 and 462 eV. The flux is 1.74 × 10−9 erg s−1, of which the BVAPEC thermal plasma contributes only less than 2%. The total unabsorbed luminosity would be about 2 × 1040 erg s−1 (a blackbody overestimates the luminosity; see text for the discussion).
Paper: The RS Oph Outburst of 2021 Monitored in X-Rays with NICER
Authors: Marina Orio, Keith Gendreau, Morgan Giese, Gerardo Juan M. Luna, Jozef Magdolen, Tod E. Strohmayer, Andy E. Zhang, Diego Altamirano, Andrej Dobrotka, Teruaki Enoto, Elizabeth C. Ferrara, Richard Ignace, Sebastian Heinz, Craig Markwardt, Joy S. Nichols, Michael L. Parker, Dheeraj R. Pasham, Songpeng Pei, Pragati Pradhan, Ron Remillard, James F. Steiner, Francesco Tombesi
Figure caption: Folded QPO pulse profile for the 17th GTI of Table 5 fitted with a model that includes a sine function at the fundamental and the first overtone with relative amplitude of 7.3. The full model (red), fundamental (blue), and first overtone components (magenta) are also shown.
Paper: The RS Oph Outburst of 2021 Monitored in X-Rays with NICER
Authors: Marina Orio, Keith Gendreau, Morgan Giese, Gerardo Juan M. Luna, Jozef Magdolen, Tod E. Strohmayer, Andy E. Zhang, Diego Altamirano, Andrej Dobrotka, Teruaki Enoto, Elizabeth C. Ferrara, Richard Ignace, Sebastian Heinz, Craig Markwardt, Joy S. Nichols, Michael L. Parker, Dheeraj R. Pasham, Songpeng Pei, Pragati Pradhan, Ron Remillard, James F. Steiner, Francesco Tombesi
Figure caption: Two examples illustrating how the modulation with the ≃35 s period is evident even visually. On the left, a portion of the RS Oph NICER light curve on 2021 September 18 (day 40); and on the right, a portion of the NICER light curve on 2021 September 19 (day 41); both measured in the 0.2–0.6 keV range with 1 s bins.
Paper: The RS Oph Outburst of 2021 Monitored in X-Rays with NICER
Authors: Marina Orio, Keith Gendreau, Morgan Giese, Gerardo Juan M. Luna, Jozef Magdolen, Tod E. Strohmayer, Andy E. Zhang, Diego Altamirano, Andrej Dobrotka, Teruaki Enoto, Elizabeth C. Ferrara, Richard Ignace, Sebastian Heinz, Craig Markwardt, Joy S. Nichols, Michael L. Parker, Dheeraj R. Pasham, Songpeng Pei, Pragati Pradhan, Ron Remillard, James F. Steiner, Francesco Tombesi
Figure caption: Lomb–Scargle periodogram of the light curve of the seventh GTI of observation 4202300113, 2021 August 22 (day 13). The dashed line shows the 99.99% confidence level.
Paper: The Formation of Star-forming Disks in the TNG50 Simulation
Authors: Enci Wang, Simon J. Lilly
Figure caption: Left panel: The stellar mass–SFR relation for the galaxies in the TNG50 simulation at redshift of z = 0. We perform a linear fitting to the star formation main sequence for the TNG50 galaxies iteratively, which is shown as a green solid line. The green dashed line is the defined demarcation line of star-forming galaxies and quenched galaxies, and is 1 dex below the green solid line. For comparison, we show the SFMS of SDSS galaxies as a cyan solid line (Bluck et al. 2016). The selected subsample investigated in the present work is shown using red triangles. Right panel: The stellar mass–size relation for the TNG50 galaxies. The selected subsample is shown using red triangles. For comparison, we show the mass–size relation of SDSS late-type galaxies as a cyan line (Shen et al. 2003), multiplied by 1.4 to account for the use of circularized radii (Furlong et al. 2017).
Paper: The Formation of Star-forming Disks in the TNG50 Simulation
Authors: Enci Wang, Simon J. Lilly
Figure caption: Left panel: An example to illustrate the definitions of ﹩{r}_{\max }﹩, SFR(﹩\lt {r}_{\max }﹩), ΔSFR, and SFRtot. The black solid line shows the cumulative SFR as a function of radius for an individual MaNGA galaxy (8326–12701), and the red solid line shows the fit of the cumulative SFR with an exponential ΣSFR profile. Therefore, the ΔSFR is defined as the maximum (absolute) deviation of the black line to the red fitted line, shown as a green line segment. The ﹩{r}_{\max }﹩ shows the maximum radius of the coverage in MaNGA observation, and the SFR(﹩\lt {r}_{\max }﹩) is the SFR within the radius of ﹩{r}_{\max }﹩. The SFRtot is the fitted total SFR, i.e., SFR(< + ∞ ). Right panel: The distribution of the ratio of SFR(﹩\lt {r}_{\max }﹩) to SFRtot for MaNGA galaxies. This distribution is peaked at SFR(﹩\lt {r}_{\max }﹩)/SFRtot ∼  0.8. We therefore perform a similar analysis for TNG50 galaxies, defining the ﹩{r}_{\max }﹩ as the radius within which 80% of the star formation is enclosed.
Paper: The Formation of Star-forming Disks in the TNG50 Simulation
Authors: Enci Wang, Simon J. Lilly
Figure caption: The same as Figure 2, but showing the profiles as a function of the normalized radius r/R 1/2 (or the effective radius for MaNGA galaxies). We also plot a normalized SFR surface density, which is computed as the SFR in an area that itself scales as ﹩{R}_{1/2}^{2}﹩. This ensures that the visual integration of a profile on the ΣSFR-radius diagram reflects the actual integrated quantity in physical terms (see also Wang et al. 2019). In each panel, the blue and red diamonds show the median ΣSFR of that stellar mass bin for the MaNGA and TNG50 galaxies, respectively. The median ΣSFR profiles of MaNGA galaxies are close to exponential functions, and we therefore fit an exponential function to the MaNGA median ΣSFR profile shown in the blue solid line of each panel.
Paper: The Formation of Star-forming Disks in the TNG50 Simulation
Authors: Enci Wang, Simon J. Lilly
Figure caption: The mean SFR surface density profiles of TNG50 galaxies (red lines) and MaNGA galaxies (blue lines). The galaxies are separated into four stellar mass bins, as denoted in each panels.
Paper: The Formation of Star-forming Disks in the TNG50 Simulation
Authors: Enci Wang, Simon J. Lilly
Figure caption: The distribution of ΔSFR/SFR(﹩\lt {r}_{\max }﹩) for TNG50 (red histograms) and MaNGA (blue histograms) galaxies. In each panel, the red and blue vertical dashed lines indicate the median values of ΔSFR/SFR(﹩\lt {r}_{\max }﹩) for TNG50 and MaNGA, respectively. As above, galaxies are separated into the four stellar mass bins.
Paper: An ALMA Glimpse of Dense Molecular Filaments Associated with High-mass Protostellar Systems in the Large Magellanic Cloud
Authors: Kazuki Tokuda, Naoto Harada, Kei E. I. Tanaka, Tsuyoshi Inoue, Takashi Shimonishi, Yichen Zhang, Marta Sewiło, Yuri Kunitoshi, Ayu Konishi, Yasuo Fukui, Akiko Kawamura, Toshikazu Onishi, Masahiro N. Machida
Figure caption: The 0.87 mm continuum distributions toward high-mass YSOs in the LMC. The angular resolution, ∼0.″46 × 0.″39, is indicated with the white ellipse in the lower left corner of the bottom left panel. Plus signs represent the position of the YSOs (Seale et al. 2009). Lines show the identified spines of the filament that we used to derive the physical properties (see the text in Section 3.2).
Paper: An ALMA Glimpse of Dense Molecular Filaments Associated with High-mass Protostellar Systems in the Large Magellanic Cloud
Authors: Kazuki Tokuda, Naoto Harada, Kei E. I. Tanaka, Tsuyoshi Inoue, Takashi Shimonishi, Yichen Zhang, Marta Sewiło, Yuri Kunitoshi, Ayu Konishi, Yasuo Fukui, Akiko Kawamura, Toshikazu Onishi, Masahiro N. Machida
Figure caption: Enlarged views of the 0.87 mm and HCO+ (4–3) emission toward three example targets. The color-scale images show the distribution of the 0.87 mm continuum emission (left panel), the HCO+ peak brightness temperature (middle panel), and the velocity-integrated intensity (right panel). The plus signs indicate the positions of massive protostars identified by Spitzer (Seale et al. 2009). The velocity range used to derive the peak brightness temperature and moment 0 maps are indicated on the upper part of each right image. The synthesized beam size is indicated in white in the lower left corner of each image.
Paper: An ALMA Glimpse of Dense Molecular Filaments Associated with High-mass Protostellar Systems in the Large Magellanic Cloud
Authors: Kazuki Tokuda, Naoto Harada, Kei E. I. Tanaka, Tsuyoshi Inoue, Takashi Shimonishi, Yichen Zhang, Marta Sewiło, Yuri Kunitoshi, Ayu Konishi, Yasuo Fukui, Akiko Kawamura, Toshikazu Onishi, Masahiro N. Machida
Figure caption: Moment 0 maps of HCO+ (4–3) toward high-mass YSOs in the LMC. The integrated velocity ranges are V sys ± Δv FWHM for each source (see Table 3). In the case of Δv FWHM not listed objects, namely those for which the filament spine could not be identified, a uniform integration range of V sys ± 2.5 km s−1 was adopted. Cyan lines show the identified spines of the filament that we used to derive the physical properties (see the text in Section 3.2).
Paper: An ALMA Glimpse of Dense Molecular Filaments Associated with High-mass Protostellar Systems in the Large Magellanic Cloud
Authors: Kazuki Tokuda, Naoto Harada, Kei E. I. Tanaka, Tsuyoshi Inoue, Takashi Shimonishi, Yichen Zhang, Marta Sewiło, Yuri Kunitoshi, Ayu Konishi, Yasuo Fukui, Akiko Kawamura, Toshikazu Onishi, Masahiro N. Machida
Figure caption: The distribution of the HCO+ (4–3) peak brightness temperature toward high-mass YSOs in the LMC. Symbols and lines are the same as in Figure 2.
Paper: An ALMA Glimpse of Dense Molecular Filaments Associated with High-mass Protostellar Systems in the Large Magellanic Cloud
Authors: Kazuki Tokuda, Naoto Harada, Kei E. I. Tanaka, Tsuyoshi Inoue, Takashi Shimonishi, Yichen Zhang, Marta Sewiło, Yuri Kunitoshi, Ayu Konishi, Yasuo Fukui, Akiko Kawamura, Toshikazu Onishi, Masahiro N. Machida
Figure caption: (a) The relation between the bolometric luminosity (L bol) of the protostar and the average column density (﹩{N}_{{{\rm{H}}}_{2}}﹩) along the filament spine. Crosses and filled circles represent the presence and absence of hub filaments, respectively. (b) The relation between the column density of the filament and the velocity dispersion derived from HCO+.
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 same as the bottom right panel of Figure 15. The best-fit L X–L  r  relation of QSOs is overplotted (green dashed line). The red horizontal line indicates L X = 3 ×  1043 erg s−1. Most XBONGs under this line are below the QSO best-fit line. Right: also marked a gap between XBONGs and normal galaxies (see the text).
Paper: An ALMA Glimpse of Dense Molecular Filaments Associated with High-mass Protostellar Systems in the Large Magellanic Cloud
Authors: Kazuki Tokuda, Naoto Harada, Kei E. I. Tanaka, Tsuyoshi Inoue, Takashi Shimonishi, Yichen Zhang, Marta Sewiło, Yuri Kunitoshi, Ayu Konishi, Yasuo Fukui, Akiko Kawamura, Toshikazu Onishi, Masahiro N. Machida
Figure caption: Average spectra of HCO+ (4–3) along each filament spine are shown in blue solid profile. Orange dashed lines show the Gaussian fitting results. For the targets with an asterisk just after the name label, we illustrated the HCO+ spectra toward the nearest neighbor of the 0.87 mm peak from the YSO.
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: X-ray luminosity functions of galaxies, clusters, and AGNs taken from the literature: K06 (Kim et al. 2006), N04 (Norman et al. 2004), G05 (Georgantopoulos et al. 2005), B02 (Böhringer et al. 2002), F20 (Finoguenov et al. 2020), A19 (Annana et al. 2019).
Paper: Cosmic-Ray Drag and Damping of Compressive Turbulence
Authors: Chad Bustard, S. Peng Oh
Figure caption: Partitioning of input turbulent energy rate ﹩\tilde{\epsilon }﹩ into three different channels: CR reacceleration f CR, dissipation via CR collisionless heating f CR,heating (i.e., streaming energy loss), and grid-scale heating f th − f CR,heating. Without CRs, this choice of ﹩\tilde{\epsilon }﹩ produces ﹩{{ \mathcal M }}_{{\rm{s}}}\sim 0.15﹩ turbulence. Each simulation here starts with P CR ∼ P  g  but with varying CR transport treatments, either with diffusion only (all with κ ∼ 0.15v ph L 0) or diffusion plus additional streaming. For each β, the first three simulations use an isothermal equation of state, so there is no gas heating. The last two, denoted by “Adiab.,” use an adiabatic equation of state, in which case the total thermal gas heating rate is the sum of CR heating and grid-scale heating. With diffusion only, reacceleration is very efficient: most turbulent energy is soaked up by CRs. With streaming, both gas heating and CR energization are relatively inefficient in the low-β regime, but for β ∼ 10, 100, CR heating is the dominant energy channel. Instead of turbulent energy cascading to small scales and eventually dissipating into thermal energy at the grid scale, CRs intercept this energy transfer at large scales; astoundingly, even in these subsonic flows, very high fractions of turbulent energy are channeled through CRs when P CR ≳ P  g .
Paper: Cosmic-Ray Drag and Damping of Compressive Turbulence
Authors: Chad Bustard, S. Peng Oh
Figure caption: Modified kinetic energy spectra for a Kolmogorov (left), Kraichnan (middle), and Burgers (right) cascade with varying levels of CR damping, all with v ph = 2v 0. E(k) is in units of the outer-scale, undamped kinetic energy, where k denotes the wavenumber. Different line colors denote different ratios of the cascade time to the damping time, showing that if damping becomes competitive, the outer-scale velocity decreases, and the slope of the spectrum steepens. Dashed lines show E(k) = k −2 and E(k) = k −3 for comparison. For t cascade/t damp ⪆ 1.5, 1 for Kolmogorov and Kraichnan, respectively, the cascade sharply cuts off at progressively smaller k. For smaller t cascade/t damp, CRs damp fluctuations, but the cascade returns to its normal scaling at large k. For Burgers turbulence, which is not a genuine cascade, there can be an appreciable decrease in power at small k, but at high k, the spectrum recovers a k −2 slope.
Paper: Cosmic-Ray Drag and Damping of Compressive Turbulence
Authors: Chad Bustard, S. Peng Oh
Figure caption: Kinetic energy spectra of 5123 simulations when P CR ∼ P  g  but varying the diffusion coefficient from κ ∣∣ ∼ 0 (where the only diffusivity is numerical) to the most efficient reacceleration regime (κ ∣∣ ∼ 0.15v ph L 0 and κ ∣∣ ∼ 1.5v ph L 0) to the fast diffusion regime (κ ∣∣ ∼ 15v ph L 0). Note how the power spectrum is somewhat different for the two-fluid system even in the absence of CR transport, presumably because of changes to the phase velocity and other adiabatic properties, but deviations from the MHD spectrum are mild compared to simulations with added diffusion. Left: k 2 E(k)dk normalized by the k = 3 MHD value. Right: ratio of each spectrum to the MHD spectrum. Note how diffusion introduces a characteristic scale l CR where the kinetic energy is reduced: in the fast diffusion limit, l CR > L 0, and the outer-scale kinetic energy drops significantly while the rest of the spectrum retains the same shape as the MHD case. Going to smaller κ ∣∣, overall changes are more drastic because reacceleration is more efficient but also the scale where the spectrum cuts off most dramatically shifts to l CR < L 0.
Paper: Cosmic-Ray Drag and Damping of Compressive Turbulence
Authors: Chad Bustard, S. Peng Oh
Figure caption: The average CR energy gain rate and thermal energy gain rate relative to the turbulent driving rate (﹩{f}_{\mathrm{CR}}={\dot{E}}_{\mathrm{CR}}/\tilde{\epsilon }﹩ and ﹩{f}_{g}={\dot{E}}_{g}/\tilde{\epsilon }﹩, respectively) for simulations without streaming, as a function of P CR/P g. These all are adiabatic, ﹩{{ \mathcal M }}_{s}\sim 0.5﹩ simulations on a 1283 grid, with β ∼ 1. Top: κ ∣∣ ∼ 0.15L 0 v ph, where CR energy gain is maximized. The dashed black curve is the analytic expectation from Equation (6), showing good agreement when P CR/P  g  < 1, and the dashed–dotted curve shows Equation (7), which accounts for CR back-reaction on the flow and subsequent saturation of f CR. Bottom: κ ∣∣ ∼ 0. For P CR ≫ P  g , even κ ∼ 0 leads to significant fractions of turbulent energy converted to CR energy, but this CR reacceleration is due to numerical diffusion caused by finite resolution.
Paper: Cosmic-Ray Drag and Damping of Compressive Turbulence
Authors: Chad Bustard, S. Peng Oh
Figure caption: The turbulent kinetic energy spectrum, multiplied by k 2 for a set of ﹩{{ \mathcal M }}_{s}\sim 0.5﹩ and ﹩{{ \mathcal M }}_{s}\sim 0.15﹩ diffusion-only simulations, keeping κ = 0.15L 0 v ph and β ∼ 1, as we vary P CR/P  g . Spectra are normalized to the k = 3 mode for the ﹩{{ \mathcal M }}_{s}\sim 0.5﹩ MHD run. Ratios of the outer-scale nonlinear time to damping time, calculated with ﹩{t}_{\mathrm{damp}}=\langle \rho {v}^{2}/{\dot{P}}_{\mathrm{CR}}\rangle ﹩ and t NL = L 0/v, are also denoted. Points show the energy in each k-bin averaged over 10 outputs at late times, when turbulence is fully developed, while shaded regions show the minima and maxima during those time periods. Each simulation was run on a 5123 grid. While MHD runs produce overall spectra shallower than k −2, CRs damp fluctuations, slightly decreasing the power in low k modes while steepening the spectra at high k.
Paper: Cosmic-Ray Drag and Damping of Compressive Turbulence
Authors: Chad Bustard, S. Peng Oh
Figure caption: Projections perpendicular to the initial magnetic field direction of density (left column), kinetic energy (middle column), and magnetic energy (right column) after ∼10 eddy turnover times, normalized by their average values in the MHD-only case. Top: MHD-only simulations with β ∼ 10 and ﹩{{ \mathcal M }}_{{\rm{s}}}\sim 0.15﹩. Bottom: simulations with the same β and forcing rate, but with P CR ∼ P  g  and diffusive CR transport. Density, velocity, and magnetic fluctuations are all suppressed compared to the MHD case.
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: Freeze-in distances of C6+, O7+, and Fe16+ within the heated prominence tracks. The tracks flow within the simulation box and stop out at the point where each ion reaches its freeze-in value. The colors indicate the fractional abundance at each point. The gray curves are the tracks projected on the r-ϕ plane.
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: Total ionization and recombination rates with increasing electron temperature for Fe12+ to Fe19+ produced using the fiasco Python package (Barnes et al. 2023).
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: Time evolution of the variations in total magnetic, kinetic, and thermal energies in the corona (in dimensionless units). The red dashed–dotted line is the error on the total energy estimated by [ΔE  M (t) + ΔE  K (t) + ΔE  I (t)]/[E  M (0) + E  I (0)].
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: (a) Distributions of the current density ∣J∣, divergence ﹩{\rm{\nabla }}\cdot \vec{V}﹩, and velocity curl ﹩| {\rm{\nabla }}\times \vec{V}| ﹩ on the x-z plane at t = 1.42. (b) Current density on the x-y plane at different heights. The black solid lines in the current density distribution in panel (a) are the magnetic field, and the yellow cross therein shows the PX point on this slice.
Paper: Dynamics of Threads Wrapping a Filament's Leg Prior to the Eruption on 2021 October 28
Authors: Yue Fang, Jun Zhang, Yi Bi, Zhiping Song
Figure caption: A sequence of 304 Å images showing the variation of the connectivity between F1 and F2 before and after the bidirectional flows, as well as the eruption of the two filaments, which is associated with the X-class flare. The black arrows in (a1)–(a3) denote the variation of the connectivity.
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: (a) MR rates as a function of time; (b) local reconnection rates along the y-axis at times t = 0.52 and 1.42. Vertical dashed lines in panel (a) mark two selected moments for plots in panel (b).
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: Time evolution of the CS along the z-axis passing the origin. (a) Mass density in log-scale; (b) velocity in the z-direction; (c) velocity in the x-direction; (d) velocity in the y-direction. The solid black line in panel (a) stands for the PX line.
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 angle dependences of linear polarization degrees of 2010 XC15 and other E-type asteroids. The polarization degrees of 2010 XC15 are represented by circles (WFGS2), triangles (HONIR), and a square (MSI). The polarization degrees of other E-types are also shown: 1998 WT24 (diamonds; Kiselev et al. 2002), 2004 VD17 (inverted triangles; De Luise et al. 2007), and Nysa (hexagons; Zellner & Gradie 1976). Bars indicate the 1σ uncertainties. The polarization phase curve of 1998 WT24 and 2010 XC15 fitted with the empirical function (Lumme & Muinonen 1993; Penttilä et al. 2005) is indicated by a solid line. Uncertainty envelopes representing the 95% highest-density interval values are indicated by dashed lines.