adsabs/AstroCLIMB huggingface dataset:
Paper: BASS. XLII. The Relation between the Covering Factor of Dusty Gas and the Eddington Ratio in Nearby Active Galactic Nuclei
Authors: C. Ricci, K. Ichikawa, M. Stalevski, T. Kawamuro, S. Yamada, Y. Ueda, R. Mushotzky, G. C. Privon, M. J. Koss, B. Trakhtenbrot, A. C. Fabian, L. C. Ho, D. Asmus, F. E. Bauer, C. S. Chang, K. K. Gupta, K. Oh, M. Powell, R. W. Pfeifle, A. Rojas, F. Ricci, M. J. Temple, Y. Toba, A. Tortosa, E. Treister, F. Harrison, D. Stern, C. M. Urry
Figure caption: Schematic of radiation-regulated growth of SMBHs together with the median covering factors of dusty gas at different stages (see Section 3.3). The effective Eddington limit for dusty gas reported in Fabian et al. (2009) is shown with the black solid lines, while the blowout region is the green area. The plot also shows the effective Eddington limit when including IR radiation trapping (Ishibashi et al. 2018), adapted to the values of Fabian et al. (2009), similar to what was done by Lansbury et al. (2020; dashed–dotted lines). The effective Eddington limit for dusty gas reported by Ishibashi et al. (2018) is shown by the dashed line. The assumed maximum contribution to N H of gas from the host galaxy is illustrated by the horizontal line at ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})=22﹩. The number density contours in the ﹩-3\leqslant \mathrm{log}{\lambda }_{\mathrm{Edd}}\leqslant 1﹩ range are shown by the gray dashed (50%), dotted (68%), and dotted–dashed (90%) lines. The bolometric corrections of Vasudevan & Fabian (2007) were used for both CF and λ Edd.
Paper: BASS. XLII. The Relation between the Covering Factor of Dusty Gas and the Eddington Ratio in Nearby Active Galactic Nuclei
Authors: C. Ricci, K. Ichikawa, M. Stalevski, T. Kawamuro, S. Yamada, Y. Ueda, R. Mushotzky, G. C. Privon, M. J. Koss, B. Trakhtenbrot, A. C. Fabian, L. C. Ho, D. Asmus, F. E. Bauer, C. S. Chang, K. K. Gupta, K. Oh, M. Powell, R. W. Pfeifle, A. Rojas, F. Ricci, M. J. Temple, Y. Toba, A. Tortosa, E. Treister, F. Harrison, D. Stern, C. M. Urry
Figure caption: Dust covering factor (see Section 3 and Equations (2) and (3)) vs. Eddington ratio for the sources of our sample. The large points in the plots show the median values for the whole population (black circles; top panels) and for unobscured and obscured AGN (blue diamonds and red squares, respectively; bottom panels). The left panels show the case in which the bolometric luminosity is estimated by using a fixed 2–10 keV bolometric correction (κ 2−10 = 20), while in the right panels, the bolometric luminosity was estimated by using the Eddington ratio–dependent corrections of Vasudevan & Fabian (2007). The dust covering factors were calculated assuming an optical depth at 9.7 μm of τ 9.7 = 5 and Equations (2) and (3).
Paper: BASS. XLII. The Relation between the Covering Factor of Dusty Gas and the Eddington Ratio in Nearby Active Galactic Nuclei
Authors: C. Ricci, K. Ichikawa, M. Stalevski, T. Kawamuro, S. Yamada, Y. Ueda, R. Mushotzky, G. C. Privon, M. J. Koss, B. Trakhtenbrot, A. C. Fabian, L. C. Ho, D. Asmus, F. E. Bauer, C. S. Chang, K. K. Gupta, K. Oh, M. Powell, R. W. Pfeifle, A. Rojas, F. Ricci, M. J. Temple, Y. Toba, A. Tortosa, E. Treister, F. Harrison, D. Stern, C. M. Urry
Figure caption: Cumulative Eddington ratio distribution of sources showing polar mid-IR emission. Cumulative distribution of λ Edd for sources showing elongated mid-IR emission from interferometric (Leftley et al. 2019; dotted blue line) and high-resolution noninterferometric (Asmus 2019; dashed orange line) observations. The solid line shows the total cumulative distribution. The dashed vertical lines represent the effective Eddington limit for dusty gas with N H = 1020 cm−2                      ﹩[{\lambda }_{\mathrm{Edd}}^{\,\mathrm{eff}}(20)﹩], N H = 1022 cm−2                      ﹩[{\lambda }_{\mathrm{Edd}}^{\,\mathrm{eff}}(22)﹩], N H = 1023 cm−2                      ﹩[{\lambda }_{\mathrm{Edd}}^{\,\mathrm{eff}}(23)]﹩, and N H = 1024 cm−2                      ﹩[{\lambda }_{\mathrm{Edd}}^{\,\mathrm{eff}}(24)]﹩ for dust grain abundance consistent with the ISM.
Paper: BASS. XLII. The Relation between the Covering Factor of Dusty Gas and the Eddington Ratio in Nearby Active Galactic Nuclei
Authors: C. Ricci, K. Ichikawa, M. Stalevski, T. Kawamuro, S. Yamada, Y. Ueda, R. Mushotzky, G. C. Privon, M. J. Koss, B. Trakhtenbrot, A. C. Fabian, L. C. Ho, D. Asmus, F. E. Bauer, C. S. Chang, K. K. Gupta, K. Oh, M. Powell, R. W. Pfeifle, A. Rojas, F. Ricci, M. J. Temple, Y. Toba, A. Tortosa, E. Treister, F. Harrison, D. Stern, C. M. Urry
Figure caption: Covering factor of dust vs. Eddington ratio for the sources of our samples considering the Eddington ratio–dependent corrections of Vasudevan & Fabian (2007; black circles) and fixed 2–10 keV bolometric corrections (κ 2−10 = 20; green diamonds). The solid blue line shows the covering factor of gas inferred from the fraction of obscured sources (Ricci et al. 2022a, assuming κ 2−10 = 20; see Ricci et al. 2017a for a discussion on how bolometric corrections affect the f obs − λ Edd trend), while the hatched area represents the 1σ uncertainty. The dust covering factors were calculated assuming an optical depth at 9.7 μm of τ 9.7 = 5 and Equations (2) and (3).
Paper: BASS. XLII. The Relation between the Covering Factor of Dusty Gas and the Eddington Ratio in Nearby Active Galactic Nuclei
Authors: C. Ricci, K. Ichikawa, M. Stalevski, T. Kawamuro, S. Yamada, Y. Ueda, R. Mushotzky, G. C. Privon, M. J. Koss, B. Trakhtenbrot, A. C. Fabian, L. C. Ho, D. Asmus, F. E. Bauer, C. S. Chang, K. K. Gupta, K. Oh, M. Powell, R. W. Pfeifle, A. Rojas, F. Ricci, M. J. Temple, Y. Toba, A. Tortosa, E. Treister, F. Harrison, D. Stern, C. M. Urry
Figure caption: Median dust covering factor (see Section 3 and Equations (2) and (3)) vs. column density for the sources of our sample. The bolometric luminosity was estimated by using fixed 2–10 keV bolometric corrections (κ 2−10 = 20; blue circles) or the Eddington ratio–dependent corrections of Vasudevan & Fabian (2007; red diamonds). The dust covering factors were calculated assuming an optical depth at 9.7 μm of τ 9.7 = 5 and Equations (2) and (3).
Paper: Blueshifted Fe II and Balmer Broad Emission lines in a Reddened Quasar
Authors: Yipeng Zhou, Peng Jiang, Xiheng Shi, Lei Hao
Figure caption: Direct comparison of the optical and NIR spectra between J1540+4923 and the red NLS1 galaxy, J2339−0912 (scaled by a factor of 0.4), in their rest frame determined by [O II] emission lines. Prominent emission lines are labeled in the plots. Note the different peak velocities of Balmer and individual Fe II lines between these two quasars.
Paper: Identifying the Physical Origin of Gamma-Ray Bursts with Supervised Machine Learning
Authors: Jia-Wei Luo, Fei-Fei Wang, Jia-Ming Zhu-Ge, Ye Li, Yuan-Chuan Zou, Bing Zhang
Figure caption: SHAP values of individual feature values of GRB 200826A, GRB 211211A, and GRB 230307A. The features marked with red push the prediction results toward Type I, while the features marked with blue push the prediction results toward Type II. Upper: GRB 200826A. Middle: GRB 211211A. Lower: GRB 230307A.
Paper: Identifying the Physical Origin of Gamma-Ray Bursts with Supervised Machine Learning
Authors: Jia-Wei Luo, Fei-Fei Wang, Jia-Ming Zhu-Ge, Ye Li, Yuan-Chuan Zou, Bing Zhang
Figure caption: Distributions of T90 and HR of the unclassified GRBs. The points are marked with their predicted classes.
Paper: Identifying the Physical Origin of Gamma-Ray Bursts with Supervised Machine Learning
Authors: Jia-Wei Luo, Fei-Fei Wang, Jia-Ming Zhu-Ge, Ye Li, Yuan-Chuan Zou, Bing Zhang
Figure caption: Probability distribution of the unclassified GRBs being Type II. The probability for Type I is 1 − the shown value.
Paper: Identifying the Physical Origin of Gamma-Ray Bursts with Supervised Machine Learning
Authors: Jia-Wei Luo, Fei-Fei Wang, Jia-Ming Zhu-Ge, Ye Li, Yuan-Chuan Zou, Bing Zhang
Figure caption: Examples of confusion matrices and SHAP feature importance values of the host galaxy subgroup without offset.
Paper: Identifying the Physical Origin of Gamma-Ray Bursts with Supervised Machine Learning
Authors: Jia-Wei Luo, Fei-Fei Wang, Jia-Ming Zhu-Ge, Ye Li, Yuan-Chuan Zou, Bing Zhang
Figure caption: Examples of confusion matrices of the T 90–HR decision tree.
Paper: Identifying the Physical Origin of Gamma-Ray Bursts with Supervised Machine Learning
Authors: Jia-Wei Luo, Fei-Fei Wang, Jia-Ming Zhu-Ge, Ye Li, Yuan-Chuan Zou, Bing Zhang
Figure caption: Examples of confusion matrices and SHAP feature importance values of the host galaxy subgroup.
Paper: Identifying the Physical Origin of Gamma-Ray Bursts with Supervised Machine Learning
Authors: Jia-Wei Luo, Fei-Fei Wang, Jia-Ming Zhu-Ge, Ye Li, Yuan-Chuan Zou, Bing Zhang
Figure caption: Examples of confusion matrices and SHAP feature importance values of the all features subgroup.
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: Sky maps of real GW events detected during O2 and O3 generated by GW-SkyLocator. The upper panel shows sky maps for the BBH and BNS events GW200224_22234 and GW170817, respectively. The bottom panel shows the sky map for the NSBH event GW200115_042309. The heat maps show the probability density obtained from GW-SkyLocator with the 90% and 50% credible intervals shown in blue and green, respectively. The yellow contour shows published sky localization results obtained from full parameter estimation software and the white contour shows the sky location estimates obtained from BAYESTAR. The areas of the 90% and 50% credible regions from GW-SkyLocator are shown in the inset.
Paper: Accretion Disk Wind of Hercules X-1 during the Short High State
Authors: P. Kosec, E. Kara, A. C. Fabian, C. Pinto, I. Psaradaki, D. Rogantini, R. Staubert, D. J. Walton
Figure caption: A schematic of the Her X-1 system, adapted from Figure 1 in Kosec et al. (2023). In this simplified scenario, the warped precessing disk is fixed, and instead the observer line of sight is moving throughout the various states of the 35-day precession cycle. The disk precession allows our line of sight to pass through different parts of the accretion disk wind, at different heights above the disk. While Kosec et al. (2023) focused on the Main High state, this work focuses on the fainter, Short High state.
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: Left to right: P–P plots for the BBH, BNS, and NSBH test samples, respectively. The dotted diagonal line shows the expected cumulative distribution of events within different credible intervals. The gray bands in the P–P plots show the 95% error margins arising due to statistical fluctuations. The p-values for the K-S tests of α and δ for each injection are shown in the legend.
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: Upper panels (a)–(c) show sky maps of a simulated BBH event obtained using BAYESTAR, GW-SkyLocator with fixed bandwidth Gaussian KDE and GW-SkyLocator with ligo.skymap's KDE, respectively. Middle panels (d)–(f) and bottom panels (g)–(i) show similar sky maps for simulated BNS and NSBH events obtained using the same methods as (a)–(c).
Paper: Accretion Disk Wind of Hercules X-1 during the Short High State
Authors: P. Kosec, E. Kara, A. C. Fabian, C. Pinto, I. Psaradaki, D. Rogantini, R. Staubert, D. J. Walton
Figure caption: Her X-1 spectrum from the Short High state Chandra observation, focusing only on the narrow energy bands of interest around the strongest elemental transitions. The absorption lines near these transitions imply the presence of an ionized disk wind. MEG data are in blue, HEG data are in black, and the best-fitting spectral model (including the ionized absorption component) is in red.
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: Box and whisker plots showing areas of the 90% credible intervals for a set of 200 BBH, BNS, and NSBH injections each, obtained using BAYESTAR, GW-SkyLocator with fixed bandwidth Gaussian KDE, and GW-SkyLocator with  ligo.skymap ’s KDE.
Paper: Accretion Disk Wind of Hercules X-1 during the Short High State
Authors: P. Kosec, E. Kara, A. C. Fabian, C. Pinto, I. Psaradaki, D. Rogantini, R. Staubert, D. J. Walton
Figure caption: The 0.6–9 keV Short High state Chandra HETG spectrum of Her X-1 (heavily overbinned), showing the broadband continuum fit with the full spectral model. MEG data are shown in blue, HEG data are in black, and the best-fitting model is in red.
Paper: Accretion Disk Wind of Hercules X-1 during the Short High State
Authors: P. Kosec, E. Kara, A. C. Fabian, C. Pinto, I. Psaradaki, D. Rogantini, R. Staubert, D. J. Walton
Figure caption: RXTE/ASM lightcurve (2–10 keV) of Her X-1 superorbital cycle number 323, during which the archival Chandra observation of the Short High state occurred. The cycle counting is according to Staubert et al. (1983), following Davison & Fabian (1977). The midpoint of the Chandra exposure is at MJD = 52581.4 and is shown with the vertical blue dashed line.
Paper: The Triggering Process of an X-class Solar Flare on a Small Quadrupolar Active Region
Authors: Qiao Song, Jing-Song Wang, Xiaoxin Zhang, Hechao Chen, Shuhong Yang, Zhenyong Hou, Yijun Hou, Qian Ye, Peng Zhang, Xiuqing Hu, Jinping Dun, Weiguo Zong, Xianyong Bai, Bo Chen, Lingping He, Kefei Song
Figure caption: Magnetic configuration and analysis of two interacting magnetic flux ropes (MFRs) in the extrapolated coronal magnetic fields of AR 12887 at 14:48 UT on 2021 October 28. Panel (a) displays the large-scale arcades and 3D quadrupolar fields above the two MFRs, and the colored lines represent extrapolated coronal magnetic field lines, with different colors used to distinguish magnetic field lines at different locations of the quadrupole field and large-scale arcades overlying filament. Panels (b) and (d) show MFR1 and MFR2 from different viewing angles. For comparison with the extrapolated fields in panel (b), panel (c) shows the distribution of two filaments (F1 and F2) in a simultaneously AIA 304 Å image, and the white arrows indicate two important footpoints of the filaments. Green and blue contours indicate positive and negative magnetic fields, respectively. Panels (e)–(f) display vertical cross sections of Q and T  w  along a slice of the red dashed line shown in panel (b), respectively.
Paper: The Triggering Process of an X-class Solar Flare on a Small Quadrupolar Active Region
Authors: Qiao Song, Jing-Song Wang, Xiaoxin Zhang, Hechao Chen, Shuhong Yang, Zhenyong Hou, Yijun Hou, Qian Ye, Peng Zhang, Xiuqing Hu, Jinping Dun, Weiguo Zong, Xianyong Bai, Bo Chen, Lingping He, Kefei Song
Figure caption: Evolution of sunspots and magnetic fields in AR 12887. Panels (a1)–(a3) display SDO/HMI intensitygrams with the contours of the photospheric magnetic field representing the positive (red) and negative (blue) polarities at 800 and −800 G, respectively. Panel (a4) specifically gives the magnetic field in the AR on the day of the X1.0 flare eruption, where the meaning of the contours is the same as (a1). Panels (b1)–(b2) show that the AR on 2021 October 28 was located near the center of the solar disk in FY-3E/X-EUVI EUV 195 Å image, and the green box in (b2) gives the FOV of Figure 2, while blue and pink boxes show the FOVs of Figures 5(a1)–(a2) and Figure 6, respectively.
Paper: The Triggering Process of an X-class Solar Flare on a Small Quadrupolar Active Region
Authors: Qiao Song, Jing-Song Wang, Xiaoxin Zhang, Hechao Chen, Shuhong Yang, Zhenyong Hou, Yijun Hou, Qian Ye, Peng Zhang, Xiuqing Hu, Jinping Dun, Weiguo Zong, Xianyong Bai, Bo Chen, Lingping He, Kefei Song
Figure caption: Observations of flare triggering and erupting process with multipassband images of SDO/AIA. Panels (a1)–(a2) show the evolution of the two filaments (F1 and F2) before the X-class flare, and the dashed line in panel (a2) indicates the location of the slice shown in the time–distance diagram of (b). Panels (c1)–(c4) display multiple brightening around Nc in AIA 131, 171, 1600, and 304 Å channels, respectively. The red (30 and 800 G) and blue (−30 and −800 G) contours represent the longitudinal magnetic fields of HMI. Panel (d) shows repeated brightening along Slice C–D in (c2). The colored lines in panel (e) give the normalized light curves of EUV/UV multipassband brightness of the dashed box area in panel (c4).
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: (Left) Cosmic ionizing emissivity density, ϵ 912, contributed by AGNs as a function of redshift. The red diamonds show estimates for our AGNs identified with the NIRSpec spectra assuming an escape fraction of 50%. The cyan circles and blue squares are measurements from X-ray AGNs (Giallongo et al. 2019) and quasars (Palanque-Delabrouille et al. 2013), respectively. The gray squares represent the measurements in Becker & Bolton (2013), and the black curve shows the model in Madau & Haardt (2015). (Right) Cosmic photoionization rate, Γ, a function of redshift. The red diamonds show estimates for our AGNs, and the cyan circles are the measurements in Giallongo et al. (2019). The gray open symbols show measurements from the Lyα forest analysis in quasar spectra (circle: Bosman et al. 2022, diamond: Davies et al. 2018, square: Becker & Bolton 2013, pentagon: Wyithe & Bolton 2011, triangle: Faucher-Giguère et al. 2008).
Paper: The Triggering Process of an X-class Solar Flare on a Small Quadrupolar Active Region
Authors: Qiao Song, Jing-Song Wang, Xiaoxin Zhang, Hechao Chen, Shuhong Yang, Zhenyong Hou, Yijun Hou, Qian Ye, Peng Zhang, Xiuqing Hu, Jinping Dun, Weiguo Zong, Xianyong Bai, Bo Chen, Lingping He, Kefei Song
Figure caption: Schematic illustrations of the magnetic field evolution and the trigger process for the X1.0 flare in AR 12887. The green and light blue lines represent two distinct MFRs (MFR1 and MFR2) before the merging process, respectively, and the red line represents the newly formed MFR (MFR3) during the eruption. Other lines display the magnetic fields of the AR. Panels (c) and (d) show that the magnetic reconnections (MRs) occur first around the collisional polarities (Nc and Pc) where two MFRs meet and then at the null point in higher corona during the flare.
Paper: The Triggering Process of an X-class Solar Flare on a Small Quadrupolar Active Region
Authors: Qiao Song, Jing-Song Wang, Xiaoxin Zhang, Hechao Chen, Shuhong Yang, Zhenyong Hou, Yijun Hou, Qian Ye, Peng Zhang, Xiuqing Hu, Jinping Dun, Weiguo Zong, Xianyong Bai, Bo Chen, Lingping He, Kefei Song
Figure caption: Motion of Nc and four larger flares in AR 12887. The locations of flare ribbons are displayed by enhancing brightness on the SDO/AIA 1600 Å images. The contours have the same meaning as those in Figure 1. Green dashed lines show the trajectory of Nc. The black dashed box in (d) represents the FOV of Figure 3.
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: Broadband light curves of the flare-affected transits of TRAPPIST-1b and f. The transit models are shown in orange, and the exponential fit to the integrations in both the transit and flare is shown in blue. The exponential fit is necessary to determine the shape of the transit light curve. As shown in the O − C diagrams at the bottom, we use an initial guess of c 1 and c 2 to fit the exponential, then subtract the exponential to obtain final values of c 1 and c 2. We note c 1 and c 2 represent the coefficients of the quadratic limb-darkening equation. The first and third O − C diagrams are directly comparable and show the light curve with the final transit model removed. The middle O − C diagram shows an intermediate step in the determination of the TRAPPIST-1f transit model fit in which the initial guess on the transit model is subtracted prior to fitting and subtracting the exponential. The residuals of the middle panel therefore show the quality of the exponential fit.
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: Comparison of flare photometry from our implementation of the supreme-SPOON and transitspectroscopy pipelines for lines from the F3 flare at representative wavelengths. Both reductions produce qualitatively similar flare light curves. However, we find the supreme-SPOON reduction is more optimized for flare photometry as the point-to-point variability during the peak phase is reduced by >20%. This effect is particularly noticeable in the second peak in the Hα light curves and the Pβ peak.
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 stellar activity in the Hα line during transit spectroscopy observations of TRAPPIST-1 used in this work. During the JWST observations, the Hα line shows considerable variability, including flares as described in Sections 3.5 and 4.2. Flares with high enough signal for multiwavelength characterization (approximately E Hα  = 1029 erg in the Hα line) are numbered by TESS band energy. Energies in these bands are given in Tables 2 and 3. The x-axis timescales of the top and bottom panels are fixed within each panel to better observe changes in activity between observations. The final transit of TRAPPIST-1g is 44.4 days after the previous observation, so a break in the x-axis (but still at the same timescale) is used to include this data in the figure. NIRSpec observations are binned to the same cadence as NIRISS and have a lower photometric uncertainty.
Paper: Erratum: “UVIT Observations of the Small Magellanic Cloud: Point-source Catalog” (2023, ApJ, 946, 65)
Authors: A. Devaraj, P. Joseph, C. S. Stalin, S. N. Tandon, S. K. Ghosh
Figure caption: Error-magnitude plots for the detected sources in different filters. The three distinct bands in each filter correspond to sources common to all three pointings (red), common in two pointings (green), and present in each individual pointing (blue). The splitting seen in blue and green is due to the difference in exposure time between the three different pointings.