adsabs/AstroCLIMB huggingface dataset:
Paper: The Nature of Spectral Variability of the Accreting Pulsar Centaurus X-3 Unveiled by NuSTAR Observation Covering Two Orbital Cycles
Authors: Tsubasa Tamba, Hirokazu Odaka, Atsushi Tanimoto, Hiromasa Suzuki, Satoshi Takashima, Aya Bamba
Figure caption: Left: orbital-phase variability of the best-fit spectral parameters derived from 4–78 keV spectroscopy. Right: correlation between NH and flux (top), Γ and flux (bottom). Different colors represent different types of orbital phases. Error bars represent 90% confidence levels.
Paper: The Nature of Spectral Variability of the Accreting Pulsar Centaurus X-3 Unveiled by NuSTAR Observation Covering Two Orbital Cycles
Authors: Tsubasa Tamba, Hirokazu Odaka, Atsushi Tanimoto, Hiromasa Suzuki, Satoshi Takashima, Aya Bamba
Figure caption: Light curves for various energy bands (left) and hardness ratios among the energy bands (right). The blue dotted lines indicate the start and end points of the eclipses. The red dotted lines represent the beginning of ingresses and the end of egresses.
Paper: The Nature of Spectral Variability of the Accreting Pulsar Centaurus X-3 Unveiled by NuSTAR Observation Covering Two Orbital Cycles
Authors: Tsubasa Tamba, Hirokazu Odaka, Atsushi Tanimoto, Hiromasa Suzuki, Satoshi Takashima, Aya Bamba
Figure caption: Orbital-phase variabilities of 4–78 keV flux and photon index plotted for various spin phases. Different colors correspond to distinct spin-phase intervals, labeled from A to H (see the main text). Error bars represent 90% confidence levels.
Paper: The Nature of Spectral Variability of the Accreting Pulsar Centaurus X-3 Unveiled by NuSTAR Observation Covering Two Orbital Cycles
Authors: Tsubasa Tamba, Hirokazu Odaka, Atsushi Tanimoto, Hiromasa Suzuki, Satoshi Takashima, Aya Bamba
Figure caption: 3–5 keV pulse fraction plotted as a function of (a) 4–5 keV absorbed flux and (b) photon index. Different colors represent different types of orbital phases.
Paper: The Nature of Spectral Variability of the Accreting Pulsar Centaurus X-3 Unveiled by NuSTAR Observation Covering Two Orbital Cycles
Authors: Tsubasa Tamba, Hirokazu Odaka, Atsushi Tanimoto, Hiromasa Suzuki, Satoshi Takashima, Aya Bamba
Figure caption: Variations of pulse profile parameters along the orbital phase calculated for multiple energy bands. Eclipse phases were excluded because of no pulsed emission.
Paper: The Nature of Spectral Variability of the Accreting Pulsar Centaurus X-3 Unveiled by NuSTAR Observation Covering Two Orbital Cycles
Authors: Tsubasa Tamba, Hirokazu Odaka, Atsushi Tanimoto, Hiromasa Suzuki, Satoshi Takashima, Aya Bamba
Figure caption: 3–78 keV pulse profile with spin-phase intervals definition.
Paper: A Multiwavelength Light-curve Analysis of the Classical Nova V392 Per: Optical Contribution from an Irradiated Accretion Disk during the Nova Wind Phase
Authors: Izumi Hachisu, Mariko Kato
Figure caption: (a) The time-stretched (B − V)0–﹩({M}_{V}-2.5\mathrm{log}{f}_{{\rm{s}}})﹩ color–magnitude diagram for V392 Per (filled magenta circles) and KT Eri (open cyan circles). The data of V392 Per are taken from U. Munari et al. (2020) (large filled magenta circles), AAVSO (small magenta circles), and VSOLJ (small magenta circles). The data of KT Eri are taken from K. Imamura & K. Tanabe (2012) and SMARTS (F. M. Walter et al. 2012). Each start of the nebular, first plateau, and second plateau phases of KT Eri is indicated by an arrow, which is shown in Figure 9(b), taken from I. Hachisu et al. (2025). The vertical solid red line of (B − V)0 = −0.03 is the intrinsic color of optically thick free–free emission (I. Hachisu & M. Kato 2014). The solid green and orange lines denote the template tracks of V1500 Cyg and LV Vul, respectively. The track of LV Vul splits into two branches in the later phase. See I. Hachisu & M. Kato (2016b) and I. Hachisu & M. Kato (2019a) for details of these template tracks. (b) The time-stretched (V − I)0–﹩({M}_{I}-2.5\mathrm{log}{f}_{{\rm{s}}})﹩ color–magnitude diagram for V392 Per and KT Eri. The data of V392 Per and KT Eri are taken from the same sources in panel (a). The thick solid lines of orange correspond to the outburst tracks of LV Vul, which are taken from I. Hachisu & M. Kato (2021). The vertical solid red line of (V − I)0 = +0.22 is the intrinsic color of optically thick free–free emission (I. Hachisu & M. Kato 2021). See Figure 12 of I. Hachisu et al. (2025) for more details on the KT Eri track.
Paper: A Multiwavelength Light-curve Analysis of the Classical Nova V392 Per: Optical Contribution from an Irradiated Accretion Disk during the Nova Wind Phase
Authors: Izumi Hachisu, Mariko Kato
Figure caption: Our FF+BB optical V light curves for the distance modulus in the V band of (m − M)V = 14.6, and our X-ray (0.3–10.0 keV) light curves, for different sets of WD mass and chemical composition. We add the same V and X-ray count rate data as those in Figure 2. The mass accretion rate onto the WDs is fixed to ﹩{\dot{M}}_{{\rm{acc}}}=1\times 1{0}^{-9}{M}_{\odot }﹩ yr−1 for all models. (a) The chemical composition of the envelope is CO nova 2: 1.2 M⊙ (gray lines), 1.25 M⊙ (yellow+green), 1.3 M⊙ (red), 1.33 M⊙ (magenta), 1.35 M⊙ (blue), and 1.37 M⊙ (green) WDs. (b) CO nova 3: 1.2 M⊙ (gray), 1.25 M⊙ (yellow+green), 1.3 M⊙ (red), 1.33 M⊙ (magenta), 1.35 M⊙ (blue), and 1.37 M⊙ (green) WDs. (c) Neon nova 2: 1.3 M⊙ (red), 1.33 M⊙ (magenta), 1.35 M⊙ (blue), and 1.37 M⊙ (green) WDs. (d) Ne3: 1.3 M⊙ (red), 1.33 M⊙ (magenta), 1.35 M⊙ (blue), and 1.37 M⊙ (green) WDs.
Paper: A Multiwavelength Light-curve Analysis of the Classical Nova V392 Per: Optical Contribution from an Irradiated Accretion Disk during the Nova Wind Phase
Authors: Izumi Hachisu, Mariko Kato
Figure caption: (a) Two V light curves of V392 Per and LV Vul are overlapped along Equation (B1). The text “LV Vul V+0.75, 0.158 t,” for example, means fs = 0.158 and ΔV = +0.75 for the template nova LV Vul against the V light curve of the target nova V392 Per (“V392 Per V, 1.0 t”). We also add M. Kato et al. (2022a)’s fully self-consistent nova model (thin black line). The V peak (green plus symbol labeled “0”) of V392 Per is overlapped with the peak of this self-consistent nova model. (b) Same as panel (a), but for the template nova KT Eri. (c) Same as panel (a), but for the template nova V339 Del. The data of LV Vul, KT Eri, and V339 Del are the same as those in I. Hachisu & M. Kato (2023), I. Hachisu et al. (2025), and I. Hachisu et al. (2024), respectively.
Paper: A Multiwavelength Light-curve Analysis of the Classical Nova V392 Per: Optical Contribution from an Irradiated Accretion Disk during the Nova Wind Phase
Authors: Izumi Hachisu, Mariko Kato
Figure caption: Geometric configuration models of our disk and companion star in Figures 2(b) and 3. The masses of the WD and Roche lobe–filling companion star are 1.37 M⊙ and 1.0 M⊙, respectively. The orbital period is Porb = 3.23 days. The inclination angle of the binary is i = 20°. The separation is a = 12.26 R⊙ while their effective Roche lobe radii are RRL,1 = 4.98 R⊙ and RRL,2 = 4.31 R⊙. The disk size is Rdisk = 4.23 R⊙ (= 0.85RRL,1). We assume, in panel (a), the height of the disk edge to be 0.05 times the disk size during the nova wind phase but, in panel (b), the edge height is 0.3 times the disk size after the winds stop. The photospheric surfaces of the disk and companion star are irradiated by the central hot WD. Such irradiation effects are all included in the calculation of the V light-curve reproduction (see I. Hachisu & M. Kato 2001 for the partition of each surface and the calculation method of irradiation). In panel (b), an L1 stream from the companion impacts the disk edge and makes a spray, which elevates the disk edge (S. Schandl et al. 1997). We also include the effect of viscous heating in the accretion disk for a given mass accretion rate (I. Hachisu & M. Kato 2001).
Paper: A Multiwavelength Light-curve Analysis of the Classical Nova V392 Per: Optical Contribution from an Irradiated Accretion Disk during the Nova Wind Phase
Authors: Izumi Hachisu, Mariko Kato
Figure caption: The distance–reddening relations toward V392 Per, whose Galactic coordinates are ﹩(\ell ,b)=(157\mathop{.}\limits^{^\circ }99,+0\mathop{.}\limits^{^\circ }90)﹩. The blue line denotes the relation of Equation (1) together with (m − M)V = 14.6 for V392 Per. The thin magenta lines are the sample distance–reddening relations given by G. M. Green et al. (2019) while the thick magenta line is the best-fit line for them. Here, we use the relation of E(B − V) = 0.884 × (Bayestar19) (G. M. Green et al. 2019). The two relations (blue and magenta) cross at the distance of d ≈ 3.5 kpc and E(B − V) ≈ 0.62.
Paper: A Multiwavelength Light-curve Analysis of the Classical Nova V392 Per: Optical Contribution from an Irradiated Accretion Disk during the Nova Wind Phase
Authors: Izumi Hachisu, Mariko Kato
Figure caption: Schematic illustration of a nova ejecta configuration of V392 Per in the (a) postmaximum phase and (b) SSS phase. A shock wave arose just after the optical maximum and has already moved far outside the WD photosphere (and the binary). The shocked shell emits Balmer lines such as Hα. This figure is taken from Figures 2(c) and (d) of I. Hachisu & M. Kato (2023) with a modification. We assume that ejecta are spherically symmetric.
Paper: A Multiwavelength Light-curve Analysis of the Classical Nova V392 Per: Optical Contribution from an Irradiated Accretion Disk during the Nova Wind Phase
Authors: Izumi Hachisu, Mariko Kato
Figure caption: Same as Figure 8, but each FF+BB V and model X-ray light curve is time-stretched with the stretching factor ﹩\mathrm{log}{f}_{{\rm{s}}}﹩ in (a) Table 2, (b) Table 3, (c) Table 4, and (d) Table 5. We add a 0.98 M⊙ (CO3) WD model to each panel, depicted by the solid black line.
Paper: The Nature of Spectral Variability of the Accreting Pulsar Centaurus X-3 Unveiled by NuSTAR Observation Covering Two Orbital Cycles
Authors: Tsubasa Tamba, Hirokazu Odaka, Atsushi Tanimoto, Hiromasa Suzuki, Satoshi Takashima, Aya Bamba
Figure caption: Left: fitting results of orbital-phase-resolved spectra with the physically motivated spectral model given by Equation (6). kT and Lbb are plotted only for the orbital-phase intervals where the blackbody component is significantly detected. Eclipse phases are indicated by blue dotted lines, and ingress and egress phases are marked with red dotted lines. Right: correlation between ﹩{N}_{{\rm{H}}}^{{\rm{PE}}}﹩ and ﹩{N}_{{\rm{H}}}^{{\rm{CS}}}﹩ (top), and Lbb and flux (bottom). Different colors represent different types of orbital phases. Error bars represent 90% confidence levels.
Paper: The Nature of Spectral Variability of the Accreting Pulsar Centaurus X-3 Unveiled by NuSTAR Observation Covering Two Orbital Cycles
Authors: Tsubasa Tamba, Hirokazu Odaka, Atsushi Tanimoto, Hiromasa Suzuki, Satoshi Takashima, Aya Bamba
Figure caption: Example of spectral fitting based on physically motivated models for the orbital-phase-resolved spectrum of Φ = 0.195–0.120. (a) Only the attenuation due to the photoelectric absorption and Compton scattering is considered. Fitting was applied to the 6–78 keV spectrum. (b) Additional blackbody component with kT = 0.47 keV was included in the fitting. Fitting was applied to the 3–78 keV spectrum.
Paper: A Systematic Search for Rapid Transients in the Subaru HSC-SSP Transient Survey
Authors: Seiji Toshikage, Masaomi Tanaka, Naoki Yasuda, Takashi J. Moriya, Ichiro Takahashi, Ji-an Jiang, Mitsuru Kokubo, Naoki Matsumoto, Keiichi Maeda, Tomoki Morokuma, Nao Suzuki, Nozomu Tominaga
Figure caption: Three-color images of the rapid transients (green) and their putative host galaxies (magenta). The left panels show the reference images and the right panels show the images after the SN discovery at around the peak brightness. Each image has a size of 10″ × 10″ centered at the SN location. North is up and east is left. We also marked the other marginal candidates of host galaxies (white) for HSC17btum, HSC17cgdi, and HSC17dadp.
Paper: A Systematic Search for Rapid Transients in the Subaru HSC-SSP Transient Survey
Authors: Seiji Toshikage, Masaomi Tanaka, Naoki Yasuda, Takashi J. Moriya, Ichiro Takahashi, Ji-an Jiang, Mitsuru Kokubo, Naoki Matsumoto, Keiichi Maeda, Tomoki Morokuma, Nao Suzuki, Nozomu Tominaga
Figure caption: Phase diagram of optical transients (M. R. Drout et al. 2014; M. Pursiainen et al. 2018; D. A. Perley et al. 2020) with our simulated rapid transient samples shown as orange shaded region (the density plot of the color represents relative numbers of simulated samples).
Paper: A Systematic Search for Rapid Transients in the Subaru HSC-SSP Transient Survey
Authors: Seiji Toshikage, Masaomi Tanaka, Naoki Yasuda, Takashi J. Moriya, Ichiro Takahashi, Ji-an Jiang, Mitsuru Kokubo, Naoki Matsumoto, Keiichi Maeda, Tomoki Morokuma, Nao Suzuki, Nozomu Tominaga
Figure caption: Light curves of HSC rapid transient samples. To define the light-curve peak, we use a band corresponding to the rest-frame g band (z < 0.2: HSC-G, 0.2 < z < 0.5: HSC-R2, 0.5 < z < 0.8: HSC-I2, 0.8 < z: HSC-Z) and set the peak date in the band as t = 0. The gray-shaded region shows the light-curve template of Type Ibc SNe in the g band from F. Taddia et al. (2015) while the blue-shaded region shows the light-curve template of Type Ibn SNe with the error in the R band from G. Hosseinzadeh et al. (2017). The black dashed line is the light curve of AT2018cow in the g band as the representative of the LFBOTs.
Paper: A Systematic Search for Rapid Transients in the Subaru HSC-SSP Transient Survey
Authors: Seiji Toshikage, Masaomi Tanaka, Naoki Yasuda, Takashi J. Moriya, Ichiro Takahashi, Ji-an Jiang, Mitsuru Kokubo, Naoki Matsumoto, Keiichi Maeda, Tomoki Morokuma, Nao Suzuki, Nozomu Tominaga
Figure caption: Distribution of redshifts for our SN samples in the SXDS field (red lines) and the COSMOS field (black lines). Dashed lines represent the distribution of SN samples with spectroscopically measured redshifts in each field.
Paper: A Systematic Search for Rapid Transients in the Subaru HSC-SSP Transient Survey
Authors: Seiji Toshikage, Masaomi Tanaka, Naoki Yasuda, Takashi J. Moriya, Ichiro Takahashi, Ji-an Jiang, Mitsuru Kokubo, Naoki Matsumoto, Keiichi Maeda, Tomoki Morokuma, Nao Suzuki, Nozomu Tominaga
Figure caption: Examples of simulated light curves. The observational epoch and depth follow the actual HSC-SSP observations. The circles show the significant detection with 5σ and the triangles represent the 3σ upper limit. Solid lines show the interpolated light curves by 2D GPR.
Paper: A Systematic Search for Rapid Transients in the Subaru HSC-SSP Transient Survey
Authors: Seiji Toshikage, Masaomi Tanaka, Naoki Yasuda, Takashi J. Moriya, Ichiro Takahashi, Ji-an Jiang, Mitsuru Kokubo, Naoki Matsumoto, Keiichi Maeda, Tomoki Morokuma, Nao Suzuki, Nozomu Tominaga
Figure caption: Normalized confusion matrix of the RF classifier with the simulation data set. The numbers in parentheses represent the raw numbers of the objects.
Paper: A Systematic Search for Rapid Transients in the Subaru HSC-SSP Transient Survey
Authors: Seiji Toshikage, Masaomi Tanaka, Naoki Yasuda, Takashi J. Moriya, Ichiro Takahashi, Ji-an Jiang, Mitsuru Kokubo, Naoki Matsumoto, Keiichi Maeda, Tomoki Morokuma, Nao Suzuki, Nozomu Tominaga
Figure caption: Flow chart of the rapid transient selection.
Paper: A Systematic Search for Rapid Transients in the Subaru HSC-SSP Transient Survey
Authors: Seiji Toshikage, Masaomi Tanaka, Naoki Yasuda, Takashi J. Moriya, Ichiro Takahashi, Ji-an Jiang, Mitsuru Kokubo, Naoki Matsumoto, Keiichi Maeda, Tomoki Morokuma, Nao Suzuki, Nozomu Tominaga
Figure caption: Phase diagram of our samples (red points) with literature SNe (M. R. Drout et al. 2014; M. Pursiainen et al. 2018; D. A. Perley et al. 2020). Time above half max time Δt 1/2 and the peak magnitude in the rest-frame g band are plotted. The red points are rapid transients from the Subaru HSC-SSP transient survey.
Paper: A Systematic Search for Rapid Transients in the Subaru HSC-SSP Transient Survey
Authors: Seiji Toshikage, Masaomi Tanaka, Naoki Yasuda, Takashi J. Moriya, Ichiro Takahashi, Ji-an Jiang, Mitsuru Kokubo, Naoki Matsumoto, Keiichi Maeda, Tomoki Morokuma, Nao Suzuki, Nozomu Tominaga
Figure caption: Temperture vs. photospheric radius estimated by blackbody fitting. We also plot the rapid transient samples from DES (M. Pursiainen et al. 2018) with black crosses, Type Ibn SNe (E. Karamehmetoglu et al. 2021; T. Ben-Ami et al. 2023) with blue circles, LFBOTs with orange stars (D. A. Perley et al. 2019, 2021; J.-a. Jiang et al. 2022), and rapidly evolving SLSNe with green circles (L. Whitesides et al. 2017; A. Y. Q. Ho et al. 2019). Green crosses represent the normal SLSN from W.-C. Zhao et al. (2020) for comparisons.
Paper: A Systematic Search for Rapid Transients in the Subaru HSC-SSP Transient Survey
Authors: Seiji Toshikage, Masaomi Tanaka, Naoki Yasuda, Takashi J. Moriya, Ichiro Takahashi, Ji-an Jiang, Mitsuru Kokubo, Naoki Matsumoto, Keiichi Maeda, Tomoki Morokuma, Nao Suzuki, Nozomu Tominaga
Figure caption:  g − r color evolution of our rapid transient samples. The upper panel shows our samples whose color evolves similarly to Type Ibn SNe, while the lower panel shows our samples whose color evolves similarly to normal SNe. We plotted the color evolution of Type Ibn SNe (blue-shaded region) and Type IIb SNe (red-shaded region) from ZTF (Lasair; K. W. Smith et al. 2019) for comparisons in each panel.
Paper: A Systematic Search for Rapid Transients in the Subaru HSC-SSP Transient Survey
Authors: Seiji Toshikage, Masaomi Tanaka, Naoki Yasuda, Takashi J. Moriya, Ichiro Takahashi, Ji-an Jiang, Mitsuru Kokubo, Naoki Matsumoto, Keiichi Maeda, Tomoki Morokuma, Nao Suzuki, Nozomu Tominaga
Figure caption: Redshift distribution of our samples. We also plot the rapid transient samples from ZTF (A. Y. Q. Ho et al. 2023), PS1 (M. R. Drout et al. 2014), and DES (M. Pursiainen et al. 2018). The dashed line represents detection limits for each limiting magnitude.
Paper: A Systematic Search for Rapid Transients in the Subaru HSC-SSP Transient Survey
Authors: Seiji Toshikage, Masaomi Tanaka, Naoki Yasuda, Takashi J. Moriya, Ichiro Takahashi, Ji-an Jiang, Mitsuru Kokubo, Naoki Matsumoto, Keiichi Maeda, Tomoki Morokuma, Nao Suzuki, Nozomu Tominaga
Figure caption: Relation between stellar mass and SFR of host galaxies. Red points represent the rapid transient in our samples. We also show the host galaxy properties of rapid transient from PS1 (M. R. Drout et al. 2014), DES (M. Pursiainen et al. 2018), and ZTF (A. Y. Q. Ho et al. 2023) with SDSS field galaxies (gray points, DR7; K. N. Abazajian et al. 2009).
Paper: A Systematic Search for Rapid Transients in the Subaru HSC-SSP Transient Survey
Authors: Seiji Toshikage, Masaomi Tanaka, Naoki Yasuda, Takashi J. Moriya, Ichiro Takahashi, Ji-an Jiang, Mitsuru Kokubo, Naoki Matsumoto, Keiichi Maeda, Tomoki Morokuma, Nao Suzuki, Nozomu Tominaga
Figure caption: Event rate as a function of the peak magnitude for the rapid transient from the Subaru HSC-SSP Transient Survey. We divided our samples into middle-redshift samples (z < 1.0, red) and high-redshift samples (z > 1.0, blue).
Paper: A Long-duration Superflare on the K Giant HD 251108
Authors: Hans Moritz Günther, Dheeraj Pasham, Alexander Binks, Stefan Czesla, Teruaki Enoto, Michael Fausnaugh, Franz-Josef Hambsch, Shun Inoue, Hiroyuki Maehara, Yuta Notsu, Jan Robrade, J. H. M. M. Schmitt, P. C. Schneider
Figure caption: TIGRE optical spectrum: the presence of the Li line and He I in emission (not shown) indicates that HD 251108 belongs to the subgroup of Li-rich, active giants.
Paper: A Long-duration Superflare on the K Giant HD 251108
Authors: Hans Moritz Günther, Dheeraj Pasham, Alexander Binks, Stefan Czesla, Teruaki Enoto, Michael Fausnaugh, Franz-Josef Hambsch, Shun Inoue, Hiroyuki Maehara, Yuta Notsu, Jan Robrade, J. H. M. M. Schmitt, P. C. Schneider
Figure caption: Lightcurve for HD 251108. Where error bars are invisible, the statistical uncertainties are smaller than the plot symbols. Top: absorbed X-ray flux in the 0.5–4.0 keV range. The average flux in eRASS is marked by a purple line, and the observed variability (shaded) is also consistent with the XMM-Newton and ROSAT fluxes. The black line shows the best-fit exponential decay fitted to the early decay phase; see Section 3.2.1 for details. Second panel: ratio between X-ray flux and the simple exponential decay model. Third panel: g-band lightcurve from ASAS-SN. The survey uses different telescopes, and there are small systematic offsets between individual cameras that cause almost simultaneous measurements to differ slightly. Fourth panel: EW of the Hα emission line. Bottom: volume emission measure of the flare from a fit with four components at fixed temperature and abundance. See Section 3.2.3 for details. The hotter flare components decay faster, while the 0.2 keV component is mostly stable. Error bars are omitted for clarity. A full listing of all NICER observations and all the data in this figure (except for the two data points from LEIA; see Z. X. Ling et al. 2022) and Figure 9 are available as “data behind the figure.”(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: A Long-duration Superflare on the K Giant HD 251108
Authors: Hans Moritz Günther, Dheeraj Pasham, Alexander Binks, Stefan Czesla, Teruaki Enoto, Michael Fausnaugh, Franz-Josef Hambsch, Shun Inoue, Hiroyuki Maehara, Yuta Notsu, Jan Robrade, J. H. M. M. Schmitt, P. C. Schneider
Figure caption: The ﹩0.5\mathrm{log}\sqrt{\mathrm{VEM}}-\mathrm{log}T﹩ diagram for a single-temperature model. The thick, partially transparent blue line is the best fit to the data before MJD = 59901.5 and also describes the data after MJD 59903.3 reasonably well. The thick, partially transparent orange line is the best fit for the period in between. It is much steeper, consistent with little or no reheating. Data shown in this figure are included in the “data behind the figure” for Figure 7.
Paper: A Long-duration Superflare on the K Giant HD 251108
Authors: Hans Moritz Günther, Dheeraj Pasham, Alexander Binks, Stefan Czesla, Teruaki Enoto, Michael Fausnaugh, Franz-Josef Hambsch, Shun Inoue, Hiroyuki Maehara, Yuta Notsu, Jan Robrade, J. H. M. M. Schmitt, P. C. Schneider
Figure caption: Five sectors of TESS data for HD 251108. Sector 45 and to a lesser degree sector 44 are contaminated by noise due to an artifact in the image subtraction. Since we use difference imaging, the absolute magnitude might be wrong, but the relative changes within an observing sector are reliable.
Paper: A Long-duration Superflare on the K Giant HD 251108
Authors: Hans Moritz Günther, Dheeraj Pasham, Alexander Binks, Stefan Czesla, Teruaki Enoto, Michael Fausnaugh, Franz-Josef Hambsch, Shun Inoue, Hiroyuki Maehara, Yuta Notsu, Jan Robrade, J. H. M. M. Schmitt, P. C. Schneider
Figure caption: Examples of the Hα line profile observed with TIGRE.
Paper: A Long-duration Superflare on the K Giant HD 251108
Authors: Hans Moritz Günther, Dheeraj Pasham, Alexander Binks, Stefan Czesla, Teruaki Enoto, Michael Fausnaugh, Franz-Josef Hambsch, Shun Inoue, Hiroyuki Maehara, Yuta Notsu, Jan Robrade, J. H. M. M. Schmitt, P. C. Schneider
Figure caption: Visually selected flares in the TESS data.
Paper: A Long-duration Superflare on the K Giant HD 251108
Authors: Hans Moritz Günther, Dheeraj Pasham, Alexander Binks, Stefan Czesla, Teruaki Enoto, Michael Fausnaugh, Franz-Josef Hambsch, Shun Inoue, Hiroyuki Maehara, Yuta Notsu, Jan Robrade, J. H. M. M. Schmitt, P. C. Schneider
Figure caption: Evolution of NICER spectra during the flare; shown are four spectra from one orbit each. Spectra are binned to a minimum of 25 counts bin–1. Colors correspond to the time of the observation.
Paper: A Long-duration Superflare on the K Giant HD 251108
Authors: Hans Moritz Günther, Dheeraj Pasham, Alexander Binks, Stefan Czesla, Teruaki Enoto, Michael Fausnaugh, Franz-Josef Hambsch, Shun Inoue, Hiroyuki Maehara, Yuta Notsu, Jan Robrade, J. H. M. M. Schmitt, P. C. Schneider
Figure caption: Color evolution of HD 251108 over several of the 21.3 day cycles (big orange and green symbols) and over years (small blue symbols).