adsabs/AstroCLIMB huggingface dataset:
Paper: Rapid Localization of Gravitational Wave Sources from Compact Binary Coalescences Using Deep Learning
Authors: Chayan Chatterjee, Manoj Kovalam, Linqing Wen, Damon Beveridge, Foivos Diakogiannis, Kevin Vinsen
Figure caption: Architecture of our model,  GW-SkyLocator . The input data, consisting of the S/N time series, ﹩\rho ﹩(t), and intrinsic parameters, ﹩{\hat{\theta }}_{\mathrm{in}}﹩ are provided to the network through the ResNet34 channel (only one ResNet block is shown here) and the multilayered fully connected (dense) network channel respectively. The features extracted by ﹩\rho ﹩(t) and ﹩{\hat{\theta }}_{\mathrm{in}}﹩ are then combined and provided as conditional input to the MAF, denoted by f(z).
Paper: Blueshifted Fe II and Balmer Broad Emission lines in a Reddened Quasar
Authors: Yipeng Zhou, Peng Jiang, Xiheng Shi, Lei Hao
Figure caption: Decomposition of the emission-line spectrum of J1540+4923. In panel (A), the model Fe II emission-line spectrum (green) is the sum of that extracted from J2339−4923 (light magenta) and PHL 1092 (light blue; blueshifted by v ≈ 1500 km s−1). The residual spectrum after removal of the Fe II lines is shown in panel (B), with significantly detected emission lines other than Fe II labeled.
Paper: Blueshifted Fe II and Balmer Broad Emission lines in a Reddened Quasar
Authors: Yipeng Zhou, Peng Jiang, Xiheng Shi, Lei Hao
Figure caption: Hβ+[O III] + Fe II spectral regime of J1540+4923 (black), overlaid with a linear combination (green) of two properly scaled analogs, J2339−4923 (light magenta) and PHL 1092 (light blue; reddened and blueshifted by v ≈ 1560 km s−1 as labeled in the plot).
Paper: Blueshifted Fe II and Balmer Broad Emission lines in a Reddened Quasar
Authors: Yipeng Zhou, Peng Jiang, Xiheng Shi, Lei Hao
Figure caption: Continuum subtracted spectrum of Mg II regime overlaid with the best-fit UV Fe II model. The double-peaked profile of Mg II can be seen clearer in the insert panel.
Paper: Blueshifted Fe II and Balmer Broad Emission lines in a Reddened Quasar
Authors: Yipeng Zhou, Peng Jiang, Xiheng Shi, Lei Hao
Figure caption: Prominent emission lines plotted in their common velocity space, overlaid with the best-fit models (see the text in Section 2.2 for details).
Paper: A JWST/NIRSpec First Census of Broad-line AGNs at z = 4–7: Detection of 10 Faint AGNs with M BH ∼ 106–108 M ⊙ and Their Host Galaxy Properties
Authors: Yuichi Harikane, Yechi Zhang, Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yoshiaki Ono, Shun Hatano, Yi Xu, Hiroya Umeda
Figure caption: UV luminosity functions at z ∼ 4, 5, 6, and 7. The red diamonds show the number densities of our broad-line (BL) AGNs identified with NIRSpec (Table 4), and the red-dashed lines with the shaded regions denote the best-fit functions (Table 5). The cyan triangles and circles represent the X-ray-selected AGNs in Parsa et al. (2018) and Giallongo et al. (2019), respectively, and the blue squares show the number densities of quasars at z ∼ 4, 5, and 6 (Akiyama et al. 2018; Niida et al. 2020; Matsuoka et al. 2018). In the z ∼ 5 panel, the red open star and circles are number density estimates of z ∼ 5 faint BL AGNs detected with NIRSpec in Kocevski et al. (2023) and Maiolino et al. (2023), respectively, while the red crosses denote estimates for the BL AGNs found in the NIRCam Grism observations in Matthee et al. (2023). The orange open circles at z ∼ 4 and 6 denote the number densities of the red and compact AGN candidates in Labbe et al. (2023). The results in Matthee et al. (2023) and Labbe et al. (2023) are horizontally shifted by −0.1 dex for visualization purposes. The blue pentagon and circle at z ∼ 7 represent the lower limits for a red quasar (Fujimoto et al. 2022) and the radio-selected AGN (Endsley et al. 2023), respectively, whose number densities are estimated in Fujimoto et al. (2022). The gray symbols show the number densities of galaxies (diamond: Harikane et al. 2022, square: Bouwens et al. 2021, triangle: Bowler et al. 2015, 2017, circle: Finkelstein et al. 2015). The cyan solid and dashed lines represent the best-fit double power-law functions based on the X-ray-selected AGNs in Parsa et al. (2018) and Giallongo et al. (2019), respectively, and the blue lines represent the best-fit functions and their extrapolations based on the quasars (Akiyama et al. 2018; Niida et al. 2020; Matsuoka et al. 2018). The number densities of our AGNs newly identified in the NIRSpec spectra are higher than the extrapolations of the quasar luminosity function.
Paper: A JWST/NIRSpec First Census of Broad-line AGNs at z = 4–7: Detection of 10 Faint AGNs with M BH ∼ 106–108 M ⊙ and Their Host Galaxy Properties
Authors: Yuichi Harikane, Yechi Zhang, Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yoshiaki Ono, Shun Hatano, Yi Xu, Hiroya Umeda
Figure caption: Relation between the bolometric luminosity (L bol) and black hole mass (M BH). The blue symbols show previous measurements for quasars at z > 4 (square: Onoue et al. 2019 and Matsuoka et al. 2019, circle: Shen et al. 2019, triangle: Willott et al. 2010a, cross: Trakhtenbrot et al. 2011). Our AGNs at z = 4–7 identified with JWST/NIRSpec (the red and magenta diamonds) occupy a unique parameter space with lower L bol and M BH, distinct from the quasars previously identified with ground-based telescopes. The red open symbols show faint AGNs identified with JWST/NIRSpec observations (star: Übler et al. 2023, square: Larson et al. 2023, circle: Maiolino et al. 2023, cross: Kokorev et al. 2023). The green and gray contours show the low-redshift AGNs at z = 1–2 (Shen et al. 2019) and z < 0.35 (Liu et al. 2019). The dashed lines show the bolometric luminosities with the Eddington ratios of λ Edd = L bol/L Edd = 1.0, 0.1, and 0.01.
Paper: A JWST/NIRSpec First Census of Broad-line AGNs at z = 4–7: Detection of 10 Faint AGNs with M BH ∼ 106–108 M ⊙ and Their Host Galaxy Properties
Authors: Yuichi Harikane, Yechi Zhang, Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yoshiaki Ono, Shun Hatano, Yi Xu, Hiroya Umeda
Figure caption: Relation between the black hole mass (M BH) and the host’s stellar mass (M *). The red and magenta diamonds show our AGNs at z = 4–7. The red open symbols show faint AGNs identified with JWST/NIRSpec observations (star: Übler et al. 2023, square: Larson et al. 2023, circle: Maiolino et al. 2023, cross: Kokorev et al. 2023). The blue circles show the z > 6 quasar samples compiled in Izumi et al. (2021; see also Izumi et al. 2018, 2019). The gray crosses and circles denote the z ∼ 0 AGNs in Kormendy & Ho (2013) and Reines & Volonteri (2015), respectively. The black solid line with the shaded region denotes the relation at z ∼ 0 in Reines & Volonteri (2015), and the dashed lines correspond to M BH/M * = 0.1, 0.01, and 0.001. Our z = 4–7 AGNs show systematically higher M BH (lower M *) compared to z ∼ 0 galaxies.
Paper: A JWST/NIRSpec First Census of Broad-line AGNs at z = 4–7: Detection of 10 Faint AGNs with M BH ∼ 106–108 M ⊙ and Their Host Galaxy Properties
Authors: Yuichi Harikane, Yechi Zhang, Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yoshiaki Ono, Shun Hatano, Yi Xu, Hiroya Umeda
Figure caption: (Top) Rest-frame UV spectrum of CEERS_00397 at z = 6.000 around wavelengths of C IV λ λ 1548,1551 (left), He II λ1640 (middle), and C III]λ λ 1907,1909 (right). The spectrum shows the broad (FWHM ∼ 1000 km s−1) and redshifted (+800 km s−1) C IV, tentative He II, and clear C III] emission lines. (Bottom) The rest-UV line diagnostics to separate AGNs and star-forming galaxies. The dashed lines are criteria to distinguish the AGNs, composites, and star-forming galaxies proposed in Hirschmann et al. (2019, 2023), while the dotted line is used to separate AGNs from the star-forming galaxies proposed in Nakajima et al. (2018). Our faint AGN, CEERS_00397, is located in the composite region in Hirschmann et al. (2019, 2023) and around the boundary in Nakajima et al. (2018), indicating that these rest-UV lines in CEERS_00397 are partly dominated by its AGN.
Paper: A JWST/NIRSpec First Census of Broad-line AGNs at z = 4–7: Detection of 10 Faint AGNs with M BH ∼ 106–108 M ⊙ and Their Host Galaxy Properties
Authors: Yuichi Harikane, Yechi Zhang, Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yoshiaki Ono, Shun Hatano, Yi Xu, Hiroya Umeda
Figure caption: Broad-line AGN fraction and 3σ  sensitivity for an Hα broad emission line in each study. The sensitivity is for a broad-line width of an FWHM = 2000 km s−1. The purple, blue, and green shaded regions indicate AGN fractions and the 16th−84th percentiles of the broad-line sensitivities for the AGNs reported in JADES (Maiolino et al. 2023), CEERS+GLASS (this study), and EIGER+FRESCO (Matthee et al. 2023), respectively. The low AGN fraction from NIRCam Grism observations in Matthee et al. (2023) is due to the shallower depth compared to NIRSpec observations in this study and in Maiolino et al. (2023).
Paper: A JWST/NIRSpec First Census of Broad-line AGNs at z = 4–7: Detection of 10 Faint AGNs with M BH ∼ 106–108 M ⊙ and Their Host Galaxy Properties
Authors: Yuichi Harikane, Yechi Zhang, Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yoshiaki Ono, Shun Hatano, Yi Xu, Hiroya Umeda
Figure caption: BPT diagram. The red symbols show the narrow emission-line ratios of our galaxies having AGNs at z = 4–7, and the cyan symbols show other galaxies at z ≳ 4 in Nakajima et al. (2023). The black contours show SDSS galaxies at z ∼ 0 (Abazajian et al. 2009). The black solid and dashed curves denote the boundaries between AGNs and star-forming galaxies obtained in Kewley et al. (2001) and Kauffmann et al. (2003), respectively. Our galaxies having AGNs cannot be distinguished from normal star-forming galaxies at z > 4 in the BPT diagram.
Paper: A JWST/NIRSpec First Census of Broad-line AGNs at z = 4–7: Detection of 10 Faint AGNs with M BH ∼ 106–108 M ⊙ and Their Host Galaxy Properties
Authors: Yuichi Harikane, Yechi Zhang, Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yoshiaki Ono, Shun Hatano, Yi Xu, Hiroya Umeda
Figure caption: SEDs of two red AGNs, CEERS_00746 (left) and CEERS_00672 (right). CEERS_00746 is also reported in Kocevski et al. (2023). The red circles and arrows show the measured magnitudes and 2σ upper limits, respectively. The blue curve represents the best-fit SEDs if we use galaxy templates. The inset panel shows the false color image in Figure 6.
Paper: A JWST/NIRSpec First Census of Broad-line AGNs at z = 4–7: Detection of 10 Faint AGNs with M BH ∼ 106–108 M ⊙ and Their Host Galaxy Properties
Authors: Yuichi Harikane, Yechi Zhang, Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yoshiaki Ono, Shun Hatano, Yi Xu, Hiroya Umeda
Figure caption: Dust attenuation estimated from the Balmer decrement as a function of spectroscopic redshift (left) and UV magnitude (right). The magenta diamonds denote red AGNs (E(B − V) > 0.5) and the red diamonds denote the other AGNs identified in this study. The gray circles show the star-forming galaxies in Nakajima et al. (2023).
Paper: A JWST/NIRSpec First Census of Broad-line AGNs at z = 4–7: Detection of 10 Faint AGNs with M BH ∼ 106–108 M ⊙ and Their Host Galaxy Properties
Authors: Yuichi Harikane, Yechi Zhang, Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yoshiaki Ono, Shun Hatano, Yi Xu, Hiroya Umeda
Figure caption: Examples of the AGN-host decomposition analysis. The top and bottom panels show the images of CEERS_01665 and CEERS_01236 in the F606W and F150W bands, respectively. The left, middle, and right panels show the observed images, models, and residuals, respectively. CEERS_01665 (CEERS_01236) is well fitted by a model with one PSF and the Sérsic profile (2 × PSF and the Sérsic profile).
Paper: Characterizing the Near-infrared Spectra of Flares from TRAPPIST-1 during JWST Transit Spectroscopy Observations
Authors: Ward S. Howard, Adam F. Kowalski, Laura Flagg, Meredith A. MacGregor, Olivia Lim, Michael Radica, Caroline Piaulet, Pierre-Alexis Roy, David Lafrenière, Björn Benneke, Alexander Brown, Néstor Espinoza, René Doyon, Louis-Philippe Coulombe, Doug Johnstone, Nicolas B. Cowan, Ray Jayawardhana, Jake D. Turner, Lisa Dang
Figure caption: Continuum is observed in each event. The continuum of the NIRSpec flares (top) is readily discernible without binning due to the low wavelength resolution. The wavelength points of the NIRISS flares (bottom) are binned to more clearly illustrate the flare spectrum, with the native resolution data shown in light gray and the binned spectrum in dark gray. The best-fit Planck function and uncertainties are displayed in red. The higher temperatures of the NIRSpec flares are a result of the higher cadence. Binning the NIRSpec flares to 105 s cadence produces nearly identical spectra to the NIRISS flares. For comparison, the effective temperature of the star is 2628 K. All spectra are plotted to the wavelength range of NIRISS to facilitate comparison.
Paper: Characterizing the Near-infrared Spectra of Flares from TRAPPIST-1 during JWST Transit Spectroscopy Observations
Authors: Ward S. Howard, Adam F. Kowalski, Laura Flagg, Meredith A. MacGregor, Olivia Lim, Michael Radica, Caroline Piaulet, Pierre-Alexis Roy, David Lafrenière, Björn Benneke, Alexander Brown, Néstor Espinoza, René Doyon, Louis-Philippe Coulombe, Doug Johnstone, Nicolas B. Cowan, Ray Jayawardhana, Jake D. Turner, Lisa Dang
Figure caption: Left: the relative impulsiveness of the flare light curve for each hydrogen line in our F3 event (red) and the largest EV Lac flare from Schmidt et al. (2012). More impulsive flares have light curves that are spiky, while less impulsive flares have light curves that are gradual. To facilitate comparisons with different flare light curves of different amplitudes and FWHM times, we normalize amplitudes to one and FWHM times by the FWHM of the Pβ line of each flare prior to computing the impulsiveness index ﹩{{ \mathcal I }}_{\mathrm{line},\mathrm{norm}}={A}_{\mathrm{fl},\mathrm{line}}/{\mathrm{FWHM}}_{\mathrm{line}}﹩. The impulsiveness of both flares reaches a maximum at Pγ, suggesting that its excitation period is brief and intense relative to the lower- and higher-order transitions. Right: light curves of the F3 lines are peak-normalized to show changes in the light curve shape across the Paschen series, described by the line-normalized impulse ﹩{{ \mathcal I }}_{\mathrm{line},\mathrm{norm}}﹩. Pα and Hα are shown with solid lines to emphasize their similar shapes, while the other lines are shown with dashed lines.
Paper: Characterizing the Near-infrared Spectra of Flares from TRAPPIST-1 during JWST Transit Spectroscopy Observations
Authors: Ward S. Howard, Adam F. Kowalski, Laura Flagg, Meredith A. MacGregor, Olivia Lim, Michael Radica, Caroline Piaulet, Pierre-Alexis Roy, David Lafrenière, Björn Benneke, Alexander Brown, Néstor Espinoza, René Doyon, Louis-Philippe Coulombe, Doug Johnstone, Nicolas B. Cowan, Ray Jayawardhana, Jake D. Turner, Lisa Dang
Figure caption: Left: effective temperature of the flares during the peak phase T eff as a function of TESS-band energy E TESS. The T eff values are lower than the peak temperatures often observed in earlier M-dwarf flares (Kowalski et al. 2013), as well as those reported in a sample of TRAPPIST-1 flares by Maas et al. (2022). For reference, we display the distribution of peak flare temperatures as a function of TESS energy for early- and mid-M dwarfs observed by Evryscope and TESS (Howard et al. 2020). The E TESS–T eff scaling relationship from Howard et al. (2020) is also shown in black and qualitatively agrees with the lower temperatures of the TRAPPIST-1 flares. Right: scaling relations from the TESS band to the 2MASS broadband luminosities during the flare peaks. Model predictions from Davenport et al. (2012) are shown for reference.
Paper: Characterizing the Near-infrared Spectra of Flares from TRAPPIST-1 during JWST Transit Spectroscopy Observations
Authors: Ward S. Howard, Adam F. Kowalski, Laura Flagg, Meredith A. MacGregor, Olivia Lim, Michael Radica, Caroline Piaulet, Pierre-Alexis Roy, David Lafrenière, Björn Benneke, Alexander Brown, Néstor Espinoza, René Doyon, Louis-Philippe Coulombe, Doug Johnstone, Nicolas B. Cowan, Ray Jayawardhana, Jake D. Turner, Lisa Dang
Figure caption: Overview of the continuum properties of the flares. The F1 and F2 NIRSpec events are shown together in the left column of panels, while the F3 and F4 NIRISS flares are displayed in the middle and right columns. For each flare, the best-fit effective temperature and filling factor are shown for the integrations, as well as the broadband light curves for the TESS and 2MASS filters. The temperature is hottest near the beginning of the flares for the F1–F3 events, and cools throughout each event. It is difficult to compare the times of maximum temperature and peak flux for the F4 event due to the binning of integrations to increase the S/N. The flare area expands as the plasma cools, leading to an increase in the filling factor. The TESS-band light curve evolves fastest, with the H- and Ks-band light curves evolving the slowest.
Paper: Characterizing the Near-infrared Spectra of Flares from TRAPPIST-1 during JWST Transit Spectroscopy Observations
Authors: Ward S. Howard, Adam F. Kowalski, Laura Flagg, Meredith A. MacGregor, Olivia Lim, Michael Radica, Caroline Piaulet, Pierre-Alexis Roy, David Lafrenière, Björn Benneke, Alexander Brown, Néstor Espinoza, René Doyon, Louis-Philippe Coulombe, Doug Johnstone, Nicolas B. Cowan, Ray Jayawardhana, Jake D. Turner, Lisa Dang
Figure caption: Left: luminosity emitted in each hydrogen line during the flare peak. Other flares with multiple NIR lines detected simultaneously are displayed for reference (Liebert et al. 1999; Schmidt et al. 2012; Kanodia et al. 2022). Both our flares and the strongest EV Lac flare indicate that higher Pγ luminosities might be a typical feature of NIR flares. Right: the same as the left panel, but for the helium and calcium lines.
Paper: Characterizing the Near-infrared Spectra of Flares from TRAPPIST-1 during JWST Transit Spectroscopy Observations
Authors: Ward S. Howard, Adam F. Kowalski, Laura Flagg, Meredith A. MacGregor, Olivia Lim, Michael Radica, Caroline Piaulet, Pierre-Alexis Roy, David Lafrenière, Björn Benneke, Alexander Brown, Néstor Espinoza, René Doyon, Louis-Philippe Coulombe, Doug Johnstone, Nicolas B. Cowan, Ray Jayawardhana, Jake D. Turner, Lisa Dang
Figure caption: Line emission is observed in the flare-only spectrum of the two NIRISS flares. Top: the F3 event is larger, with more candidate or confirmed lines during the flare peak. Bottom: the F4 event is the weakest flare for which lines beyond Hα could be detected.
Paper: Characterizing the Near-infrared Spectra of Flares from TRAPPIST-1 during JWST Transit Spectroscopy Observations
Authors: Ward S. Howard, Adam F. Kowalski, Laura Flagg, Meredith A. MacGregor, Olivia Lim, Michael Radica, Caroline Piaulet, Pierre-Alexis Roy, David Lafrenière, Björn Benneke, Alexander Brown, Néstor Espinoza, René Doyon, Louis-Philippe Coulombe, Doug Johnstone, Nicolas B. Cowan, Ray Jayawardhana, Jake D. Turner, Lisa Dang
Figure caption: Separation of Hα from the continuum contribution in the same NIRSpec wavelength point. On the left, the wavelength point containing Hα is highlighted in dark red, while two continuum reference wavelengths are highlighted in gray. In the second panel, the light curve at 0.6565 μm is displayed, presumably that of the Hα line. In the third panel, light curves are extracted for each wavelength point and compared (with an offset applied in the plot). The average of the two reference light curves is divided from the target light curve to remove behavior common to all three wavelengths. On the right, the resulting corrected Hα light curve is shown.
Paper: Characterizing the Near-infrared Spectra of Flares from TRAPPIST-1 during JWST Transit Spectroscopy Observations
Authors: Ward S. Howard, Adam F. Kowalski, Laura Flagg, Meredith A. MacGregor, Olivia Lim, Michael Radica, Caroline Piaulet, Pierre-Alexis Roy, David Lafrenière, Björn Benneke, Alexander Brown, Néstor Espinoza, René Doyon, Louis-Philippe Coulombe, Doug Johnstone, Nicolas B. Cowan, Ray Jayawardhana, Jake D. Turner, Lisa Dang
Figure caption: Left: relative timing of hydrogen line emission during the F3 flare. The faster rise of the higher-order Pβ–Pδ lines likely reflects a shorter period of excitation compared to the Hα and Pα lines. Note Hα has been scaled down by 100× to facilitate comparison with the weaker lines. Right: relative luminosity of the hydrogen lines during the F3 flare, normalized by the luminosity of Hα. Pβ and Pγ exhibit both the highest peak luminosity and fastest decay. The Hα light curve is shown for reference.
Paper: Characterizing the Near-infrared Spectra of Flares from TRAPPIST-1 during JWST Transit Spectroscopy Observations
Authors: Ward S. Howard, Adam F. Kowalski, Laura Flagg, Meredith A. MacGregor, Olivia Lim, Michael Radica, Caroline Piaulet, Pierre-Alexis Roy, David Lafrenière, Björn Benneke, Alexander Brown, Néstor Espinoza, René Doyon, Louis-Philippe Coulombe, Doug Johnstone, Nicolas B. Cowan, Ray Jayawardhana, Jake D. Turner, Lisa Dang
Figure caption: Left: the light curves of the lines and candidate lines identified in the larger F3 flare. Pα and Brβ are the first detections of flare emission from a main-sequence star in these lines. Right: the light curves of the lines and candidate lines identified in the smaller F4 flare. ΔF/F is the fractional flux as defined in Section 6.2.
Paper: A Possible Mechanism for the “Late Phase” in Stellar White-light Flares
Authors: Kai E. Yang, 凯 杨, Xudong Sun, 旭东 孙, Graham S. Kerr, Hugh S. Hudson
Figure caption: Modeled flare atmosphere and synthesized TESS light curves. Cases 1–3 are shown in columns (a)–(c), respectively (fixed loop radius R L = 10 Mm, nominal footpoint heating timescale τ d,b = 29.5 minutes, and varying magnetic fields B = 400, 600, and 800 G). The top three rows show the evolution of electron number density n e, temperature T, and velocity v along the flare loop. The vertical axis is the loop coordinate l, and the horizontal axis is time t. The loop apex is located at the center l = 0; the footpoints are at the two ends. Positive (negative) velocities at positive (negative) loop coordinates indicate downflows, i.e., flows from the loop top to the footpoints, and are shown as red (blue). Time t = 0 marks the beginning of the heating input. The contours are for high-density region in the corona n e = 5 × 1012 cm−3. The dashed and dashed–dotted vertical lines in the second row indicate the end time of the loop-top and footpoint sources, respectively. The bottom row shows the synthesized TESS flare emission from the coronal plasma, normalized to the stellar disk emission. The total loop emission is shown in red, and the contributions from Thomson scattering, free–free emission, and free-bound emission are shown in blue, orange, and green, respectively.
Paper: A Possible Mechanism for the “Late Phase” in Stellar White-light Flares
Authors: Kai E. Yang, 凯 杨, Xudong Sun, 旭东 孙, Graham S. Kerr, Hugh S. Hudson
Figure caption: An example of a TESS flare light curve with a peak-bump morphology from the TESS Input Catalog (TIC) ID 272232401. The x-axis is a fraction of a day starting from Barycentric TESS Julian Date (BTJD) 2238. Black dots represent data outside the fitting range, red circles indicate data used for fitting, and gray circles denote excluded data around the time of 2238.23. These data are excluded due to a small local maximum that may come from another region of the star and is not well described by the peak-bump morphology. The light curve is fitted using an empirical double flare template f(t) from Pietras et al. (2022): ﹩f{\left(t)={\int }_{0}^{t}({A}_{1}\exp [-(x-{B}_{1}\right)}^{2}/{C}_{1}^{2}]\exp [-{D}_{1}(t-x)]﹩ + ﹩{A}_{2}\exp [-{(x-{B}_{2})}^{2}/{C}_{2}^{2}]\exp [-{D}_{2}(t-x)]){dx}﹩, where t represents time. The fitted impulsive phase (first portion of f(t)), late phase (second portion of f(t)), and total flare model are shown as gold dashed–dotted, cyan dashed, and green solid lines, respectively. The best-fit parameters are A 1 = 8.52 hr−1, B 1 = 1.07 hr, C 1 = 1.47 × 10−2 hr, D 1 = 2.11 × 101 hr−1, A 2 = 8.3 × 10−2 hr−1, B 2 = 1.6 hr, C 2 = 4.96 × 10−1 hr, and D 2 = 1.12 hr−1. The χ 2 of the fit is 2.72.