adsabs/AstroCLIMB huggingface dataset:
Paper: Detection of a Deeply Embedded Protocluster Candidate in NGC 602 with JWST
Authors: Beena Meena, Peter Zeidler, Elena Sabbi, Antonella Nota, Camilla Pacifici, Olivia C. Jones
Figure caption: Each panel presents a 12″ × 12″ cutout of the region surrounding the Sk183, spanning from wideband NIRCam filters to MIRI filters. This progression highlights the gradual emergence of the extended emission as we move to longer wavelengths. In the NIRCam images, it remains undetected, while in the mid-IR, particularly in MIRI F1000W and longer-wavelength filters, the emission from MZS-1 becomes increasingly prominent. This trend suggests that this object is deeply embedded and heavily obscured at shorter wavelengths, with its emission peaking in the mid-IR. The apparent fainter nature of the F1130W filter is due to its relatively narrow bandwidth, which is less than half the width of other MIRI wideband filters. This reduced bandwidth results in lower integrated flux compared to adjacent filters.
Paper: Detection of a Deeply Embedded Protocluster Candidate in NGC 602 with JWST
Authors: Beena Meena, Peter Zeidler, Elena Sabbi, Antonella Nota, Camilla Pacifici, Olivia C. Jones
Figure caption: F1130W image of MZS-1. The fainter emission in this band compared to the other MIRI filters allows for a clearer view of the morphology. Flux contours are overlaid at levels exceeding 10σ above the background flux, following a Gaussian scaling over the image smoothed using a 2 × 2 box kernel. The several flux peaks (named MZS-1-“a,” “b,” “c,” “d,” “e,” “f”) are potentially associated with six distinct protostellar sources in MZS-1.
Paper: Detection of a Deeply Embedded Protocluster Candidate in NGC 602 with JWST
Authors: Beena Meena, Peter Zeidler, Elena Sabbi, Antonella Nota, Camilla Pacifici, Olivia C. Jones
Figure caption: A color-composite NIRCam image of the central region of NGC 602, adopted from P. Zeidler et al. (2024). The image combines the following filters: F115W+F140M+F150W (blue), F210M (cyan), F277W (green), F335M (yellow), F356W (orange), and F480M (red). The strong mid-IR emission from MZS-1 (discussed in Section 3.1) is not detected in this NIR image. The bright O3 star Sk183 is indicated for reference. The inset at the bottom right shows an RGB image constructed from MIRI F1000W, F1130W, and F1550W data, highlighting a 25″ × 25″ region centered on the mid-IR emission, which appears as diffuse pink emission. In this view, Sk183 appears fainter and is marked with a green cross. North is up, and East is to the left. Note that this image does not cover the full NIRCam field of view. Credits: ESA/Webb, NASA & CSA, P. Zeidler, E. Sabbi, A. Nota, M. Zamani (ESA/Webb).
Paper: Detection of a Deeply Embedded Protocluster Candidate in NGC 602 with JWST
Authors: Beena Meena, Peter Zeidler, Elena Sabbi, Antonella Nota, Camilla Pacifici, Olivia C. Jones
Figure caption: YSO fits for MZS-1a using the T. P. Robitaille (2017) model grid “spubhmi.” A cartoon representation of the YSO model configuration is shown in the inset. The observed MIRI fluxes are plotted as black circles, while the upper limits for the NIRCam filters (obtained using the background region) are indicated by downward triangles. The error bars on MIRI data-points represent the uncertainties in flux calculated from PSF fitting. The best-fit model is shown as the solid black line, and the corresponding output parameters are listed at the top left. Here the mass of the central star is derived using L = M3.5L⊙. The SED fitting for rest of the candidate protostellar cores are given in the Appendix.
Paper: Detection of a Deeply Embedded Protocluster Candidate in NGC 602 with JWST
Authors: Beena Meena, Peter Zeidler, Elena Sabbi, Antonella Nota, Camilla Pacifici, Olivia C. Jones
Figure caption: SEDs generated for each core identified in Figure 3, derived using PSF photometry. Measured fluxes for each core are shown using distinct marker styles and colors, as indicated in the legend (bottom right). The gray line shows the total flux measured in a 8″ × 4″ elliptical aperture around MZS-1. All fluxes are normalized to flux in F1500W. While individual cores vary in brightness, their overall SED shapes are comparable. Overlaid are blackbody curves for three temperatures: 100 K (red), 120 K (green), and 140 K (blue). The error bars correspond to flux uncertainties derived from the PSF-fitting procedure.
Paper: Detection of a Deeply Embedded Protocluster Candidate in NGC 602 with JWST
Authors: Beena Meena, Peter Zeidler, Elena Sabbi, Antonella Nota, Camilla Pacifici, Olivia C. Jones
Figure caption: Same as Figure 5, but for the remaining candidate YSOs in MZS-1. Each panel shows SED fits using models from T. P. Robitaille (2017), based on the simplest and most likely model set as indicated in the insets. The black curve represents the best-fit model determined by χ2 minimization, with the corresponding parameters listed in the top-left corner. The gray curves show the other models within the same grid, which are used to estimate the parameter ranges reported in Table A1.
Paper: Extreme Starlight Polarization Efficiency toward ζ Ophiuchi: A Case for Line-of-sight Foreground Subtraction
Authors: Jordan A. Bartlett, Henry A. Kobulnicky
Figure caption: The target stars plotted in the Stokes q–u plane. The shapes of the markers represent the three distance groupings: Near Group as circles, ζ Oph Group as triangles, and Far Group as squares. The gray line segments (alternating light and dark for visibility) connect the targets in order of increasing distance, beginning with Target 34 and ending with Target 49. For clarity, Target 24 has been offset by −1σ in q and Target 6 has been offset by −0.5σ in q and +0.5σ in u.
Paper: Extreme Starlight Polarization Efficiency toward ζ Ophiuchi: A Case for Line-of-sight Foreground Subtraction
Authors: Jordan A. Bartlett, Henry A. Kobulnicky
Figure caption: Schematic representation of dust and magnetic structure along the ζ Oph line of sight.
Paper: Extreme Starlight Polarization Efficiency toward ζ Ophiuchi: A Case for Line-of-sight Foreground Subtraction
Authors: Jordan A. Bartlett, Henry A. Kobulnicky
Figure caption: The target stars’ E(B − V) vs. distance. The error bars represent the 1σ uncertainties. The dashed lines and gray labels demarcate the three distance groups. The red ×’s indicate the weighted averages of each group.
Paper: Extreme Starlight Polarization Efficiency toward ζ Ophiuchi: A Case for Line-of-sight Foreground Subtraction
Authors: Jordan A. Bartlett, Henry A. Kobulnicky
Figure caption: The structure function of ﹩\Vert {\rm{\Delta }}{{\boldsymbol{P}}}_{{\rm{V}}}\Vert ﹩ for line of sight Δd and angular separation Δθ. The data are binned into 22 bins for clarity, with the black data points representing the mean value of each bin. The error bars represent the 1σ uncertainties. These data are limited to Δd < 300 pc and Δθ < 1° due to lack of target pairs beyond these separations. The unbinned data are presented as semitransparent points.
Paper: High-pass Filtering and Gaussian Process Regularization: Stellar Activity Characterization Techniques Applied to the 55 Cancri Planetary System
Authors: Justin Harrell, Sarah E Dodson-Robinson
Figure caption: Left: long-term trend (dashed black line) computed using a Gaussian filter (GF) via Equation (2) superposed onto the 55 Cnc RV time series. The GF used here has a width of σ = 500 days. The gray shaded region is composed of 30 GF trends for a reasonable range of σ ∈ [400, 1000] days (sampled uniformly). We include a GF trend with a poorly chosen width of σ = 200 days (cyan dashed–dotted line) for comparison. The GF long-term trend represents the weighted moving average of RVs across this high-pass filter. Right: the detrended RV time series after the long-term trend is subtracted out.
Paper: Optimized Asteroid Rotation and Shape Modeling through an Integrated Shape-from-silhouette and Optical Flow Approach
Authors: Yi Liu, Bo Wu, Hongliang Li
Figure caption: Estimated surface displacement results on Bennu. (a) Frame 1, (b) Frame 2, (c) Reference optical flow. Estimated surface displacement of (d) proposed approach at ﹩(\lambda ,\beta ,\mathrm{Thres})=\left(-87.^\circ 87,43.^\circ 23,12\right)﹩, (e) SFS method at ﹩(\lambda ,\beta ,\mathrm{Thres})=\left(-93^\circ ,42^\circ ,10\right)﹩, (f) SFS method at ﹩(\lambda ,\beta ,\mathrm{Thres})=\left(-40^\circ ,39^\circ ,10\right)﹩, (9) SFS method at ﹩(\lambda ,\beta ,\mathrm{Thres})=\left(143^\circ ,-36^\circ ,10\right)﹩, and (f) SFS method at ﹩(\lambda ,\beta ,\mathrm{Thres})=\left(80^\circ ,-43^\circ ,10\right)﹩. The color is used for flow visualization, with saturation showing length and hue showing direction. The arrows are for flow direction visualization.
Paper: Optimized Asteroid Rotation and Shape Modeling through an Integrated Shape-from-silhouette and Optical Flow Approach
Authors: Yi Liu, Bo Wu, Hongliang Li
Figure caption: Estimated surface displacement results on Itokawa. (a) Frame 1, (b) Frame 2, (c) Reference optical flow. Estimated surface displacement of (d) proposed approach at ﹩(\lambda ,\beta ,\mathrm{Thres})=\left(88.^\circ 59,-67.^\circ 98,8\right)﹩, (e) SFS method at ﹩(\lambda ,\beta ,\mathrm{Thres})=\left(93^\circ ,-69^\circ ,10\right)﹩, and (f) SFS method at ﹩(\lambda ,\beta ,\mathrm{Thres})=\left(89^\circ ,67^\circ ,10\right)﹩. The color is used for flow visualization, with saturation showing length and hue showing direction. The arrows are for flow direction visualization.
Paper: Optimized Asteroid Rotation and Shape Modeling through an Integrated Shape-from-silhouette and Optical Flow Approach
Authors: Yi Liu, Bo Wu, Hongliang Li
Figure caption: Three-sided views of the ground-truth shape model of Itokawa. Views from the positive directions of the (a) x-, (b) y-, and (c) z-axes.
Paper: Optimized Asteroid Rotation and Shape Modeling through an Integrated Shape-from-silhouette and Optical Flow Approach
Authors: Yi Liu, Bo Wu, Hongliang Li
Figure caption: Representative experimental images of Bennu. (a) Initial status, (b) rotation by 90°, (c) rotation by 180°.
Paper: Optimized Asteroid Rotation and Shape Modeling through an Integrated Shape-from-silhouette and Optical Flow Approach
Authors: Yi Liu, Bo Wu, Hongliang Li
Figure caption: GWO performance on Bennu. (a) Search history, (b) convergence curve, (c) trajectory of λ of the first wolf, and (d) trajectory of β of the first wolf of the best result.
Paper: Optimized Asteroid Rotation and Shape Modeling through an Integrated Shape-from-silhouette and Optical Flow Approach
Authors: Yi Liu, Bo Wu, Hongliang Li
Figure caption: GWO performance on Itokawa. (a) Search history, (b) convergence curve, (c) trajectory of λ of the first wolf, and (d) trajectory of β of the first wolf of the best result.
Paper: Optimized Asteroid Rotation and Shape Modeling through an Integrated Shape-from-silhouette and Optical Flow Approach
Authors: Yi Liu, Bo Wu, Hongliang Li
Figure caption: Some simulation images of Itokawa under different illumination conditions.
Paper: Optimized Asteroid Rotation and Shape Modeling through an Integrated Shape-from-silhouette and Optical Flow Approach
Authors: Yi Liu, Bo Wu, Hongliang Li
Figure caption: Schematic of the silhouette-based method.
Paper: Optimized Asteroid Rotation and Shape Modeling through an Integrated Shape-from-silhouette and Optical Flow Approach
Authors: Yi Liu, Bo Wu, Hongliang Li
Figure caption: Visible regions at different times.
Paper: FAST Search for Circumstellar Atomic Hydrogen. IV. Bubbles Associated with Planetary Nebulae
Authors: Jun-Yang Liu, Yong Zhang, Xu-Jia Ouyang
Figure caption: Comparison between our measured distances with others. The straight line denotes x = y. The inset is a zoom-in view. The strength of correlations with our distances, ranked in descending order, is: FW16 (r = 0.56, p = 0.44; 4 PNe); CGDR2 (r = 0.37, p = 0.19; 14 PNe); CGDR3 (r = 0.32, p = 0.27; 14 PNe); A15 (r = 0.20, p = 0.58; 10 PNe); A22 (r = 0.17, p = 0.63; 10 PNe); Vdsz95 (r = 0.09, p = 0.88; 5 PNe); CKS92 (r = −0.10, p = 0.81; 8 PNe); Z95 (Mion – r)(r = −0.12, p = 0.78; 8 PNe); and Z95 (Tb – r) (r = −0.14, p = 0.74; 8 PNe).
Paper: FAST Search for Circumstellar Atomic Hydrogen. IV. Bubbles Associated with Planetary Nebulae
Authors: Jun-Yang Liu, Yong Zhang, Xu-Jia Ouyang
Figure caption: Vlsr of bubbles against their distances derived from CGDR3, with data shown for different directions. The curves illustrate the relational trends predicted by different GRMs, while the square symbols represent the observed values.
Paper: FAST Search for Circumstellar Atomic Hydrogen. IV. Bubbles Associated with Planetary Nebulae
Authors: Jun-Yang Liu, Yong Zhang, Xu-Jia Ouyang
Figure caption: Same as Figure 2 but for A21. The black dotted circle marks the optical angular extent of A21, reported by FW16. The white dashed grid displays the Galactic coordinate system.
Paper: FAST Search for Circumstellar Atomic Hydrogen. IV. Bubbles Associated with Planetary Nebulae
Authors: Jun-Yang Liu, Yong Zhang, Xu-Jia Ouyang
Figure caption: Rotational velocity Θ(R) vs. Galactocentric radius R across different GRMs. The squares denote the observed values obtained based on the calibrated parallax distances from CGDR3 and the bubbles’ Vlsr under different GRMs.
Paper: FAST Search for Circumstellar Atomic Hydrogen. IV. Bubbles Associated with Planetary Nebulae
Authors: Jun-Yang Liu, Yong Zhang, Xu-Jia Ouyang
Figure caption: Same as Figure 1 but for Sh 2-71.
Paper: FAST Search for Circumstellar Atomic Hydrogen. IV. Bubbles Associated with Planetary Nebulae
Authors: Jun-Yang Liu, Yong Zhang, Xu-Jia Ouyang
Figure caption: Same as Figure 1 but for Sh 2-68.
Paper: FAST Search for Circumstellar Atomic Hydrogen. IV. Bubbles Associated with Planetary Nebulae
Authors: Jun-Yang Liu, Yong Zhang, Xu-Jia Ouyang
Figure caption: Same as Figure 2 but for Sh 2-68.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: Phase-folded Kepler data for KIC08285349 with the joint fit LC solution (magenta curve), as in Figure 2.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: BFs for the contact system KIC04999357, as in Figure 3. The extracted tertiary is shown as the pale blue spike.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: BFs for the detached system KIC04850874, as in Figure 3.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: Phase-folded Kepler data for the detached binary KIC04850874 with the joint fit LC solution (magenta curve) and residuals, as in Figure 2.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: Phase-folded Kepler data for KIC05977736 with the joint fit LC solution (magenta curve), as in Figure 2.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: Phase-folded Kepler data for KIC04999357 with the joint fit LC solution (magenta curve), as in Figure 2.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: BFs for the detached system KIC05977736, as in Figure 3.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: Posterior probability distributions of the system parameters for KIC03443519 from the MCMC Bayesian analysis.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: BFs for the detached system KIC08285349, as in Figure 3.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: Phase-folded TESS data (Sector 60) for IP Lyn with the LC solution (magenta curve), as in Figure 2.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: BFs for the contact system FP Boo, as in Figure 3.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: BF for the contact system KIC11097678, as in Figure 14.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: Phase-folded TESS data for KIC08539720 with the LC solution (magenta curve).
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: Phase-folded TESS data (Sectors 23, 24, 50, and 51) for FP Boo with the joint fit LC solution (magenta curve), as in Figure 2.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: BF for the CB KIC08539720 (black curve) with the PHOEBE model (magenta curve) evincing an RV profile generated using the results of the LC fitting. The given primary mass is merely the mass used to generate the PHOEBE model. It is not a result.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: Phase-folded Kepler data for KIC11097678 with the LC solution (magenta curve).
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: Phase-folded Kepler data for KIC12066630 with the joint fit LC solution (magenta curve), as in Figure 2.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: BFs for the detached system KIC12066630, as in Figure 3.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: BFs for the contact system V857 Her, as in Figure 3.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: Phase-folded TESS data (Sectors 42 and 43) for EM Psc with the LC solution (magenta curve), as in Figure 2.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: Phase-folded TESS data (Sector 51) for V1187 Her with the joint fit LC solution (magenta curve), as in Figure 2.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: Phase-folded TESS data for V857 Her (Sectors 24, 25, 78, and 79) with the joint fit LC solution (magenta curve), as in Figure 2.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: BFs for the contact system NSVS 2569022, as in Figure 3. The considerable l3 (light blue) spike near 50 km s−1 is cut off for better viewing of the RV profile of the binary (dark blue).
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: BFs for the contact system V1187 Her, as in Figure 3. The inset in the bottom panel shows a full BF with the l3 spike included.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: BFs for the contact system EM Psc, as in Figure 3.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: BFs for the contact system IP Lyn, as in Figure 3. We are unsure of the origin of the second spike in the BF shown in the top panel.
Paper: Observational Constraints on Close Binary Star Evolution. II. Extreme Mass Ratios
Authors: Evan M. Cook, Henry A. Kobulnicky
Figure caption: Phase-folded TESS data (Sectors 14, 20, 21, 40, 41, and 47) for NSVS 2569022 with the joint fit LC solution (magenta curve), as in Figure 2.
Paper: Characterizing Temperatures of Flares on the M Dwarf Wolf 359 from Simultaneous Multiband Optical Observations
Authors: Chia-Lung Lin, Li-Ching Huang, Wei-Jie Hou, Hsiang-Yao Hsiao, Wing-Huen Ip
Figure caption: Flares detected in Wolf 359 on 2023 February 17 in multiple photometric bands simultaneously. First row: light curves in the u, g, r, i, and z bands for each of the three detected flares. The purple solid curves represent synthetic flare profiles constructed to approximate the full flare variation in the u band based on the observed data points. These profiles were determined by using the flare profile model from M. Gryciuk et al. (2017), specifically their Equations (1) through (4). Second row: zoom-in profiles of the g-, r-, i-, and z-band light curves. Dashed horizontal lines indicate the quiescent flux levels in each band. The flares exhibit significant brightness enhancements in the u, g, and r bands, with much weaker or undetectable signals in the i and z bands. Third row: flares detected on 2023 February 18 and 20. Starting from February 18, observations were conducted only in the g, r, i, and z bands due to a malfunction of the u-band filter. Fourth and fifth rows: flares detected on 2023 February 21 and 22. In total, 12 flares were observed in Wolf 359 during our observation campaign.
Paper: Characterizing Temperatures of Flares on the M Dwarf Wolf 359 from Simultaneous Multiband Optical Observations
Authors: Chia-Lung Lin, Li-Ching Huang, Wei-Jie Hou, Hsiang-Yao Hsiao, Wing-Huen Ip
Figure caption: Peak flare-only SEDs and best-fit blackbody models for three flares detected in the g, r, and i bands: F5-0220 (Flare No. 1 on February 20), F10-0221 (Flare No. 4 on February 21), and F12-0222 (Flare No. 1 on February 22). Colored data points represent the flare-only flux densities derived for each band (g band in green, r band in red, and i band in brown), and the solid purple lines show the corresponding blackbody fits, with shaded regions indicating 1σ uncertainties. The derived peak flare temperatures are Tfl,SED = 5700 ± 600 K, 4500 ± 400 K, and 5500 ± 500 K, respectively.
Paper: Characterizing Temperatures of Flares on the M Dwarf Wolf 359 from Simultaneous Multiband Optical Observations
Authors: Chia-Lung Lin, Li-Ching Huang, Wei-Jie Hou, Hsiang-Yao Hsiao, Wing-Huen Ip
Figure caption: Top: u-band light curve of Wolf 359 obtained on 2021 April 20, showing relative flux variability throughout the observation. Vertical dashed lines mark the midpoint of each spectroscopic exposure taken by using the Shelyak LISA low-resolution spectrograph (R ∼ 1000) on the Lulin 1 m telescope. Spectra numbered 7 through 14 (blue lines) were identified as taken during a flare-free interval and were used to construct the quiescent spectrum. Bottom: the quiescent spectrum of Wolf 359 (blue), obtained by averaging spectra Nos. 7–14. The spectrum in gray represents the spectrum No. 19 observed during the flaring phase and is offset by 0.5 units for better visual comparison. The transmission curves of the g (green), r (red), and i (brown) filters used by TRIPOL are also shown. This quiescent spectrum was used to calculate the star’s quiescent luminosities in the g, r, and i bands.