adsabs/AstroCLIMB huggingface dataset:
Paper: Repeated Partial Disruptions in a White Dwarf–Neutron Star or White Dwarf–Black Hole Merger Modulate the Prompt Emission of Long-duration Merger-type GRBs
Authors: Junping Chen, Rong-Feng Shen, Wen-Jun Tan, Chen-Wei Wang, Shao-Lin Xiong, Run-Chao Chen, Bin-Bin Zhang
Figure caption: The WWZ power plot of the light curve (0–50 s) of GRB 230307A in the 500–2000 keV band.
Paper: Repeated Partial Disruptions in a White Dwarf–Neutron Star or White Dwarf–Black Hole Merger Modulate the Prompt Emission of Long-duration Merger-type GRBs
Authors: Junping Chen, Rong-Feng Shen, Wen-Jun Tan, Chen-Wei Wang, Shao-Lin Xiong, Run-Chao Chen, Bin-Bin Zhang
Figure caption: Same as in Figure A2 but for GRB 230307A (300–500 keV).
Paper: Repeated Partial Disruptions in a White Dwarf–Neutron Star or White Dwarf–Black Hole Merger Modulate the Prompt Emission of Long-duration Merger-type GRBs
Authors: Junping Chen, Rong-Feng Shen, Wen-Jun Tan, Chen-Wei Wang, Shao-Lin Xiong, Run-Chao Chen, Bin-Bin Zhang
Figure caption: Same as in Figure A2 but for GRB 211211A (15–5000 keV).
Paper: Metis Observation of the Onset of Fully Developed Turbulence in the Solar Corona
Authors: Daniele Telloni, Luca Sorriso-Valvo, Gary P. Zank, Marco Velli, Vincenzo Andretta, Denise Perrone, Raffaele Marino, Francesco Carbone, Antonio Vecchio, Laxman Adhikari, Lingling Zhao, Sabrina Guastavino, Fabiana Camattari, Chen Shi, Nikos Sioulas, Zesen Huang, Marco Romoli, Ester Antonucci, Vania Da Deppo, Silvano Fineschi, Catia Grimani, Petr Heinzel, John D. Moses, Giampiero Naletto, Gianalfredo Nicolini, Daniele Spadaro, Marco Stangalini, Luca Teriaca, Michela Uslenghi, Lucia Abbo, Frédéric Auchère, Regina Aznar Cuadrado, Arkadiusz Berlicki, Roberto Bruno, Aleksandr Burtovoi, Gerardo Capobianco, Chiara Casini, Marta Casti, Paolo Chioetto, Alain J. Corso, Raffaella D'Amicis, Yara De Leo, Michele Fabi, Federica Frassati, Fabio Frassetto, Silvio Giordano, Salvo L. Guglielmino, Giovanna Jerse, Federico Landini, Alessandro Liberatore, Enrico Magli, Giuseppe Massone, Giuseppe Nisticò, Maurizio Pancrazzi, Maria G. Pelizzo, Hardi Peter, Christina Plainaki, Luca Poletto, Fabio Reale, Paolo Romano, Giuliana Russano, Clementina Sasso, Udo Schühle, Sami K. Solanki, Leonard Strachan, Thomas Straus, Roberto Susino, Rita Ventura, Cosimo A. Volpicelli, Joachim Woch, Luca Zangrilli, Gaetano Zimbardo, Paola Zuppella
Figure caption: (a) Map of the spectral index α = − (ζ 2 + 1) derived from the second-order structure functions S 2 in the scale range from Δt = 1 to Δt = 10 hr. (b) Distributions of the ensembles of α values extracted from the polar profiles at 1.8, 2.2, 2.6, and 3.0 R ⊙, indicated with color-coded, dashed circles in (a); the mean and standard deviation of each distribution are also reported. (c) Averages of the second-order structure functions S 2 obtained along the same circular profiles and displayed in the same color scheme (the curves are downscaled, according to the indicated values, to retain the same value at the largest timescale of 10 hr for easy comparison of the corresponding scaling laws); the exponents ﹩-\overline{{\zeta }_{2}}﹩ computed from power-law fitting in the 1 hr ≤Δt ≤ 10 hr range (along with the corresponding uncertainties) are also shown.
Paper: Metis Observation of the Onset of Fully Developed Turbulence in the Solar Corona
Authors: Daniele Telloni, Luca Sorriso-Valvo, Gary P. Zank, Marco Velli, Vincenzo Andretta, Denise Perrone, Raffaele Marino, Francesco Carbone, Antonio Vecchio, Laxman Adhikari, Lingling Zhao, Sabrina Guastavino, Fabiana Camattari, Chen Shi, Nikos Sioulas, Zesen Huang, Marco Romoli, Ester Antonucci, Vania Da Deppo, Silvano Fineschi, Catia Grimani, Petr Heinzel, John D. Moses, Giampiero Naletto, Gianalfredo Nicolini, Daniele Spadaro, Marco Stangalini, Luca Teriaca, Michela Uslenghi, Lucia Abbo, Frédéric Auchère, Regina Aznar Cuadrado, Arkadiusz Berlicki, Roberto Bruno, Aleksandr Burtovoi, Gerardo Capobianco, Chiara Casini, Marta Casti, Paolo Chioetto, Alain J. Corso, Raffaella D'Amicis, Yara De Leo, Michele Fabi, Federica Frassati, Fabio Frassetto, Silvio Giordano, Salvo L. Guglielmino, Giovanna Jerse, Federico Landini, Alessandro Liberatore, Enrico Magli, Giuseppe Massone, Giuseppe Nisticò, Maurizio Pancrazzi, Maria G. Pelizzo, Hardi Peter, Christina Plainaki, Luca Poletto, Fabio Reale, Paolo Romano, Giuliana Russano, Clementina Sasso, Udo Schühle, Sami K. Solanki, Leonard Strachan, Thomas Straus, Roberto Susino, Rita Ventura, Cosimo A. Volpicelli, Joachim Woch, Luca Zangrilli, Gaetano Zimbardo, Paola Zuppella
Figure caption: (a) Average of the 298 coronal brightness images acquired by Metis between 10:15 and 20:16 UT on 2022 October 12. (b) Same as (a), but with the DoG filter applied to sharpen the boundaries between different coronal magnetic structures.
Paper: Metis Observation of the Onset of Fully Developed Turbulence in the Solar Corona
Authors: Daniele Telloni, Luca Sorriso-Valvo, Gary P. Zank, Marco Velli, Vincenzo Andretta, Denise Perrone, Raffaele Marino, Francesco Carbone, Antonio Vecchio, Laxman Adhikari, Lingling Zhao, Sabrina Guastavino, Fabiana Camattari, Chen Shi, Nikos Sioulas, Zesen Huang, Marco Romoli, Ester Antonucci, Vania Da Deppo, Silvano Fineschi, Catia Grimani, Petr Heinzel, John D. Moses, Giampiero Naletto, Gianalfredo Nicolini, Daniele Spadaro, Marco Stangalini, Luca Teriaca, Michela Uslenghi, Lucia Abbo, Frédéric Auchère, Regina Aznar Cuadrado, Arkadiusz Berlicki, Roberto Bruno, Aleksandr Burtovoi, Gerardo Capobianco, Chiara Casini, Marta Casti, Paolo Chioetto, Alain J. Corso, Raffaella D'Amicis, Yara De Leo, Michele Fabi, Federica Frassati, Fabio Frassetto, Silvio Giordano, Salvo L. Guglielmino, Giovanna Jerse, Federico Landini, Alessandro Liberatore, Enrico Magli, Giuseppe Massone, Giuseppe Nisticò, Maurizio Pancrazzi, Maria G. Pelizzo, Hardi Peter, Christina Plainaki, Luca Poletto, Fabio Reale, Paolo Romano, Giuliana Russano, Clementina Sasso, Udo Schühle, Sami K. Solanki, Leonard Strachan, Thomas Straus, Roberto Susino, Rita Ventura, Cosimo A. Volpicelli, Joachim Woch, Luca Zangrilli, Gaetano Zimbardo, Paola Zuppella
Figure caption: Second-order structure functions S 2 at the lag Δt of 1 hr (a), 2 hr (b), 4 hr (c), and 8 hr (d), computed from the series of Metis VL images in the whole FOV of the detector.
Paper: Birth of Rapidly Spinning, Overmassive Black Holes in the Early Universe
Authors: Kohei Inayoshi, Kohei Ichikawa
Figure caption: Left: Cosmic evolution of the BH mass density in a comoving volume. At z ∼ 5, the BH mass density is derived from the integration of the BHMF for LRDs (red symbols). From this point, the mass density grows toward lower redshifts following the BHAD deduced from known AGN populations with a 10% radiative efficiency (solid curve; Y. Ueda et al. 2014) and reaches the density of relic BHs in the nearby universe (F. Shankar et al. 2009). At z > 5, the cumulative mass accreted to BHs during the LRD phase, Δρ • ≡ BHAD × Δt inferred from their bolometric luminosity function over a time span Δt for given redshift range based on the COSMOS-Web (magenta) and the other surveys (blue), assuming a 10% radiative efficiency, substantially exceed the observed mass density at z ≃ 5 as well as the predictions from a BH growth model calibrated with UV and X-ray selected AGN luminosity function (dotted curve; W. Li et al. 2024a). Data for LRDs are derived from luminosity functions and BH mass estimates provided in the literature (open symbols, H. B. Akins et al. 2024; J. E. Greene et al. 2024; J. Matthee et al. 2024; V. Kokorev et al. 2024) and the mean values for each group (filled symbols). Right: Summary of the BH mass density and the cumulative mass density during the LRD phase assuming a 10% radiative efficiency. Shaded areas indicate the BH mass density ρ • at z ≃ 5 (red) and the cumulative mass density accrued during the LRD stage calculated from the COSMOS-Web (magenta) and the other surveys (blue). The total sum of Δρ • over the entire redshift range in each data group is shown with a star symbol.
Paper: Birth of Rapidly Spinning, Overmassive Black Holes in the Early Universe
Authors: Kohei Inayoshi, Kohei Ichikawa
Figure caption: The critical X-ray luminosities for LRDs at z ∼ 5, determined by the requirement for LRDs not to be classified as X-ray AGNs nor contributing to the abundance of X-ray AGNs (red horizontal lines with arrows). For comparison, several models for bolometric correction to X-rays are shown (Y. Ueda et al. 2003; R. Nanni et al. 2017; F. Duras et al. 2020), as well as the cases with constant optical-to-X-ray spectral indices of α OX = −1.5 (dashed) and −1.8 (solid). The L bol − L X values of the two LRDs detected in X-rays are shown with orange symbols; JADES 21925 (square) and PRIMER-COS 3982 (diamond; D. D. Kocevski et al. 2024). The shaded area denotes X-ray luminosities below the detection threshold of current Chandra observations for JWST fields.
Paper: Birth of Rapidly Spinning, Overmassive Black Holes in the Early Universe
Authors: Kohei Inayoshi, Kohei Ichikawa
Figure caption: The cosmic BHAD as a function of redshift. Each data point and curve represents BHADs estimated under the assumption of a 10% radiative efficiency (ϵ rad = 0.1) for the three different populations, including LRDs (H. B. Akins et al. 2024; J. E. Greene et al. 2024; J. Matthee et al. 2024; V. Kokorev et al. 2024), X-ray-selected AGNs including Compton-thick populations (J. Aird et al. 2015; T. T. Ananna et al. 2019; E. Pouliasis et al. 2024), and mid-infrared-selected AGNs (I. Delvecchio et al. 2014). For comparison, the cosmic SFRD scaled by a factor of 3000 is overlaid (Y. Harikane et al. 2022). The BHAD attributed to LRDs remains significantly dominant at z > 6.
Paper: Birth of Rapidly Spinning, Overmassive Black Holes in the Early Universe
Authors: Kohei Inayoshi, Kohei Ichikawa
Figure caption: Bolometric AGN luminosity functions at 4.5 < z < 6 (left) and 6.5 < z < 8.5 (right). The luminosity function data obtained from different surveys are shown: the rest-UV-selected quasars (M. Niida et al. 2020; Y. Matsuoka et al. 2023), the X-ray-selected AGNs (Y. Ueda et al. 2014), and dust-reddened AGNs reported as “LRDs” identified with JWST photometry and slitless spectroscopy (H. B. Akins et al. 2024; J. E. Greene et al. 2024; J. Matthee et al. 2024; V. Kokorev et al. 2024). The bright-end slope of the LRD luminosity function is consistent with ﹩{\rm{\Phi }}\propto {L}_{\mathrm{bol}}^{-1}﹩ at both redshifts.
Paper: Birth of Rapidly Spinning, Overmassive Black Holes in the Early Universe
Authors: Kohei Inayoshi, Kohei Ichikawa
Figure caption:  M • − M ⋆ distribution for high-redshift AGNs, including LRDs, JWST-detected unobscured ANGs at z = 4–8 (purple, R. Maiolino et al. 2023; green, Y. Harikane et al. 2023; cyan, M. A. Stone et al. 2024; and blue, X. Ding et al. 2023), and quasars identified in ground-based surveys (T. Izumi et al. 2021). For the LRDs at 4.5 < z < 6.5 (red) and 6.5 < z < 8.5 (orange), we derive the upper bound of the stellar mass based on the dust-corrected continuum flux measured by J. E. Greene et al. (2024) using Equations (1) and (2). Additionally, a z = 8.5 LRD with broad Hβ emission, for which the stellar mass is constrained by ALMA nondetections, is overlaid (blue; V. Kokorev et al. 2023). Two different mass correlations are overlaid: the local relationship (solid; J. Kormendy & L. C. Ho 2013) and the JWST-detected AGNs (dashed; F. Pacucci et al. 2023).
Paper: Birth of Rapidly Spinning, Overmassive Black Holes in the Early Universe
Authors: Kohei Inayoshi, Kohei Ichikawa
Figure caption: Stellar mass density in galaxies hosting LRDs at various redshifts, calculated using Equation (1) and assuming ﹩{\mathscr{F}}(\equiv {f}_{\mathrm{IMF}}{f}_{L})=1.0﹩ (open symbols) at two redshift ranges of 4.5 < z < 6.5 and 6.5 < z < 8.5. For comparison, the stellar mass function derived from the DM halo mass function at 5 ≤ z ≤ 8 is shown with a 100% star formation efficiency. An upper bound of the stellar mass constrains ﹩{\mathscr{F}}\lt 0.3{f}_{\star }﹩ for 4.5 < z < 6.5 and ﹩{\mathscr{F}}\lt 0.04{f}_{\star }﹩ for 6.5 < z < 8.5 (filled symbols).
Paper: Insight-HXMT, NICER, and NuSTAR Views to the Newly Discovered Black Hole X-Ray Binary Swift J151857.0–572147
Authors: Jing-Qiang Peng, Shu Zhang, Qing-Cang Shui, Yu-Peng Chen, Shuang-Nan Zhang, Ling-Da Kong, A. Santangelo, Zhuo-Li Yu, Long Ji, Peng-Ju Wang, Zhi Chang, Jian Li, Zhao-sheng Li
Figure caption: The light curves of Swift J151857.0–572147 observed by Insight-HXMT and NICER during the 2024 outburst. The red dots represent Insight-HXMT observations and the black dots represent NICER observations. Top panel: the light curve of Insight-HXMT LE and NICER in 2–12 keV. Middle panel: the light curves are normalized to the Crab. Bottom panel: the light curve of Insight- HXMT after subtracting off the Cir X–1 (a gray area) and the light curve of NICER. The red dotted lines correspond to about 90%, 50%, and 10% of the peak flux, respectively.
Paper: Insight-HXMT, NICER, and NuSTAR Views to the Newly Discovered Black Hole X-Ray Binary Swift J151857.0–572147
Authors: Jing-Qiang Peng, Shu Zhang, Qing-Cang Shui, Yu-Peng Chen, Shuang-Nan Zhang, Ling-Da Kong, A. Santangelo, Zhuo-Li Yu, Long Ji, Peng-Ju Wang, Zhi Chang, Jian Li, Zhao-sheng Li
Figure caption: The simultaneous broadband spectrum with the model (constant∗tbabs∗(diskbb+cutoffpl)) of Swift J151857.0–572147 is observed from NuSTAR/FPMA (black), NuSTAR/FPMB (red), Insight-HXMT ME (green), and Insight-HXMT HE (blue).
Paper: Insight-HXMT, NICER, and NuSTAR Views to the Newly Discovered Black Hole X-Ray Binary Swift J151857.0–572147
Authors: Jing-Qiang Peng, Shu Zhang, Qing-Cang Shui, Yu-Peng Chen, Shuang-Nan Zhang, Ling-Da Kong, A. Santangelo, Zhuo-Li Yu, Long Ji, Peng-Ju Wang, Zhi Chang, Jian Li, Zhao-sheng Li
Figure caption: The simultaneous broadband spectrum with the model M1 of Swift J151857.0–572147 is observed from NuSTAR/FPMA (black), NuSTAR/FPMB (red), Insight-HXMT ME (green), and Insight-HXMT HE (blue).
Paper: Insight-HXMT, NICER, and NuSTAR Views to the Newly Discovered Black Hole X-Ray Binary Swift J151857.0–572147
Authors: Jing-Qiang Peng, Shu Zhang, Qing-Cang Shui, Yu-Peng Chen, Shuang-Nan Zhang, Ling-Da Kong, A. Santangelo, Zhuo-Li Yu, Long Ji, Peng-Ju Wang, Zhi Chang, Jian Li, Zhao-sheng Li
Figure caption: Evolution of the spectral parameters of Swift J151857.0–572147 in 2024 from model M2: N H is the column density, Γ the low-energy power-law photon index, T in the temperature of the inner disk, Cov_frac the coverage factor, and r in the inner radius of the disk. F disk and F non−thermal are disk flux and nonthermal flux, respectively.
Paper: Insight-HXMT, NICER, and NuSTAR Views to the Newly Discovered Black Hole X-Ray Binary Swift J151857.0–572147
Authors: Jing-Qiang Peng, Shu Zhang, Qing-Cang Shui, Yu-Peng Chen, Shuang-Nan Zhang, Ling-Da Kong, A. Santangelo, Zhuo-Li Yu, Long Ji, Peng-Ju Wang, Zhi Chang, Jian Li, Zhao-sheng Li
Figure caption: The disk unabsorbed flux (0.01–100 keV) versus the disk inner temperature (T in). Flux is found to vary with temperature in form ﹩{T}_{\mathrm{in}}^{3.83\pm 0.17}﹩.
Paper: Insight-HXMT, NICER, and NuSTAR Views to the Newly Discovered Black Hole X-Ray Binary Swift J151857.0–572147
Authors: Jing-Qiang Peng, Shu Zhang, Qing-Cang Shui, Yu-Peng Chen, Shuang-Nan Zhang, Ling-Da Kong, A. Santangelo, Zhuo-Li Yu, Long Ji, Peng-Ju Wang, Zhi Chang, Jian Li, Zhao-sheng Li
Figure caption: The NICER HID of Swift J151857.0–572147, where the hardness is defined as the ratio of 4–10 to 1–4 keV count rate. The subplot shows the distribution of the outburst trajectory of Swift J151857.0–572147 after scaling the count rate relative to the trajectory of the 2021 outburst of GX 339–4.
Paper: Insight-HXMT, NICER, and NuSTAR Views to the Newly Discovered Black Hole X-Ray Binary Swift J151857.0–572147
Authors: Jing-Qiang Peng, Shu Zhang, Qing-Cang Shui, Yu-Peng Chen, Shuang-Nan Zhang, Ling-Da Kong, A. Santangelo, Zhuo-Li Yu, Long Ji, Peng-Ju Wang, Zhi Chang, Jian Li, Zhao-sheng Li
Figure caption: The spectral fittings for the data born out of NICER observations of Swift J151857.0–572147.
Paper: JWST Thermal Emission of the Terrestrial Exoplanet GJ 1132b
Authors: Qiao Xue, Jacob L. Bean, Michael Zhang, Alexandra Mahajan, Jegug Ih, Jason D. Eastman, Jonathan Lunine, Megan Weiner Mansfield, Brandon Park Coy, Eliza M.-R. Kempton, Daniel Koll, Edwin Kite
Figure caption: Light curves produced by our nominal SPARTA reduction. (a) Raw 2D light curves in the wavelength–integration plane. Anomalies such as the odd–even effect and exponential downward ramps at the beginning ∼400 integrations of the observation (∼30 minutes) are found. The red arrow indicates the very bright strip (3× baseline flux) that we eventually removed from our nominal reduction. The start, middle, and end of the eclipse are shown with dashed dark-red lines. (b) The systematics-corrected white-light curve is shown in the top panel overplotted with the best batman eclipse model (blue line) and binned systematics-corrected fluxes (orange circles). The bottom panel shows the residuals between the best-fit total model (F sys and F batman) and binned fluxes. We excluded the first 400 integrations (30 minutes) owing to the strong exponential ramp. The middle two panels show the drifts of the trace positions in the spatial and dispersion directions, which are decorrelated from the data with linear models.
Paper: JWST Thermal Emission of the Terrestrial Exoplanet GJ 1132b
Authors: Qiao Xue, Jacob L. Bean, Michael Zhang, Alexandra Mahajan, Jegug Ih, Jason D. Eastman, Jonathan Lunine, Megan Weiner Mansfield, Brandon Park Coy, Eliza M.-R. Kempton, Daniel Koll, Edwin Kite
Figure caption: Emission spectra (main panel) and white-light eclipse depths (inset) from the different reductions. The results from Eureka! are shown in dark blue, and the results from SPARTA with different up-the-ramp fitting strategies are presented in pink (using all groups), green (with the first five groups removed), and yellow (with the first 11 groups removed). The wavelengths are shifted for visualization purposes. The gray dashed line in the inset shows eclipse depth corresponding to the maximum dayside temperature of the planet, with the shaded area indicating ±1σ. The white-light bandpass is shown with the gray triangle in the main plot. We plot the eclipse depth measured by the global model described in Section 4 with the red square.
Paper: JWST Thermal Emission of the Terrestrial Exoplanet GJ 1132b
Authors: Qiao Xue, Jacob L. Bean, Michael Zhang, Alexandra Mahajan, Jegug Ih, Jason D. Eastman, Jonathan Lunine, Megan Weiner Mansfield, Brandon Park Coy, Eliza M.-R. Kempton, Daniel Koll, Edwin Kite
Figure caption: Goodness of fit (χ 2) of the eclipse depths of the suite of atmospheric models, plotted as functions of the modeled surface pressure. The best-fit blackbody (691 K) to the emission spectrum is shown with the black dashed line. The bare surface models are shown in the leftmost column with diamonds. The median and 1σ and 2σ equivalent quantiles of the χ 2 distribution (k = 14, where k is the degree of freedom) are shown as the solid black line, the dark-gray band, and the light-gray band, respectively. The atmosphere models with compositions of CO2 filled with O2 are shown with squares, and those of H2O filled with O2 are shown with circles, where colors indicate the percentage of trace gases. The atmosphere models generally move, from the thinnest (10−4 bars) to the thickest (102 bars) surface pressures, from the χ 2 for the maximally hot temperature (blue dashed line) to the χ 2 for the equilibrium temperature (red dashed line), with deviating inflection points arising owing to spectral features in the LRS bandpass and changes in the temperature–pressure profile. Atmospheric models that produce χ 2 values comparable to the best-fit blackbody are plotted in Figure 6.
Paper: JWST Thermal Emission of the Terrestrial Exoplanet GJ 1132b
Authors: Qiao Xue, Jacob L. Bean, Michael Zhang, Alexandra Mahajan, Jegug Ih, Jason D. Eastman, Jonathan Lunine, Megan Weiner Mansfield, Brandon Park Coy, Eliza M.-R. Kempton, Daniel Koll, Edwin Kite
Figure caption: Planetary dayside temperature as a function of Bond albedo A B and heat recirculation efficiency ε. The median and ±1σ contours show the 709 ± 31 K dayside temperature derived from the white-light curve. The yellow arrow indicates the maximum dayside temperature (746﹩{}_{-11}^{+14}﹩ K) assuming no reflection and no heat recirculation. We adopt A B = 0.119, 0.75, 0.306, 0.250, and 0.11 for Mercury, Venus, Earth, Mars, and the Moon, respectively. Since the solar system terrestrial planets are not tidally locked, we calculated their heat redistribution efficiency using their polar and equatorial temperatures. Following Equations (4) and (5) in N. B. Cowan & E. Agol (2011), we derived ﹩\epsilon =\tfrac{8/3}{({({T}_{\mathrm{equator}}/{T}_{\mathrm{pole}})}^{4}+5/3)}﹩.
Paper: JWST Thermal Emission of the Terrestrial Exoplanet GJ 1132b
Authors: Qiao Xue, Jacob L. Bean, Michael Zhang, Alexandra Mahajan, Jegug Ih, Jason D. Eastman, Jonathan Lunine, Megan Weiner Mansfield, Brandon Park Coy, Eliza M.-R. Kempton, Daniel Koll, Edwin Kite
Figure caption: Median data number counts summed over the data images as a function of group number after linearity correction of the first data segment. Nonlinear behavior is seen in the first ∼11 groups, and a downward offset in the last group (#28) is seen. Although each pixel behaves differently, this nonlinearity is found in all integrations. Two red dashed lines indicate groups #5 and #11. The nonlinearity could be caused by the reset-switch charge decay (RSCD; J. E. Morrison et al. 2023; A. Dyrek et al. 2024), which causes a greater increase in the ramp at the start of an integration. Besides our standard Eureka! reduction shown in Section 3, we also implemented RscdStep (https://jwst-pipeline.readthedocs.io/en/latest/api/jwst.rscd.RscdStep.html) from the standard jwst pipeline in Eureka!. Similar to what our preferred SPARTA reduction did (i.e., excluding the first five groups), RscdStep excluded the first four groups from the up-the-ramp fitting for this data set. The resulting best-fit white-light eclipse depth is 147 ± 17 ppm, compared to ﹩{143}_{-19}^{+17}﹩ ppm from our Eureka! standard reduction, 145 ± 20 ppm from our preferred SPARTA gr5 reduction, and 141 ± 17 ppm from the global fitting.
Paper: JWST Thermal Emission of the Terrestrial Exoplanet GJ 1132b
Authors: Qiao Xue, Jacob L. Bean, Michael Zhang, Alexandra Mahajan, Jegug Ih, Jason D. Eastman, Jonathan Lunine, Megan Weiner Mansfield, Brandon Park Coy, Eliza M.-R. Kempton, Daniel Koll, Edwin Kite
Figure caption: Observed brightness temperature spectrum from SPARTA (cyan) and Eureka! (black) plotted against models for bare surfaces (top panel) and atmospheres (bottom) that fit the data. The expected brightness temperatures and their uncertainties propagated from the system parameters are plotted as horizontal lines for varying Bond albedos and redistribution factors. The bandpass functions for the LRS and the 12.8 and 15 μm MIRI photometry filters are also shown for illustration. As can be seen from 1 and 10 ppm CO2 models, the presence of CO2 can be further constrained using 15 μm MIRI photometry.
Paper: JWST Thermal Emission of the Terrestrial Exoplanet GJ 1132b
Authors: Qiao Xue, Jacob L. Bean, Michael Zhang, Alexandra Mahajan, Jegug Ih, Jason D. Eastman, Jonathan Lunine, Megan Weiner Mansfield, Brandon Park Coy, Eliza M.-R. Kempton, Daniel Koll, Edwin Kite
Figure caption: GJ 1132b in the context of the cosmic shoreline (K. J. Zahnle & D. C. Catling 2017). In the solar system, the dashed blue line separates bodies that have atmospheres from those that do not. Blue shading illustrates uncertainty on the y-axis. For exoplanets, only rocky planets around M dwarfs with thermal emission measurements are shown.