adsabs/AstroCLIMB huggingface dataset:
Paper: A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715
Authors: Devarshi Choudhury, Tuomo Salmi, Serena Vinciguerra, Thomas E. Riley, Yves Kini, Anna L. Watts, Bas Dorsman, Slavko Bogdanov, Sebastien Guillot, Paul S. Ray, Daniel J. Reardon, Ronald A. Remillard, Anna V. Bilous, Daniela Huppenkothen, James M. Lattimer, Nathan Rutherford, Zaven Arzoumanian, Keith C. Gendreau, Sharon M. Morsink, Wynn C. G. Ho
Figure caption: Mass, radius, and compactness posteriors inferred by CST+PDT when the models are not informed by radio priors and do not involve any background constraints. In the absence of radio priors, the model prefers much smaller masses.
Paper: A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715
Authors: Devarshi Choudhury, Tuomo Salmi, Serena Vinciguerra, Thomas E. Riley, Yves Kini, Anna L. Watts, Bas Dorsman, Slavko Bogdanov, Sebastien Guillot, Paul S. Ray, Daniel J. Reardon, Ronald A. Remillard, Anna V. Bilous, Daniela Huppenkothen, James M. Lattimer, Nathan Rutherford, Zaven Arzoumanian, Keith C. Gendreau, Sharon M. Morsink, Wynn C. G. Ho
Figure caption: Posteriors obtained by ST-U as applied to the 3C50 data set, testing the implementation of different n  l  values when applying a lower 3C50 instrument-only background constraint.
Paper: A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715
Authors: Devarshi Choudhury, Tuomo Salmi, Serena Vinciguerra, Thomas E. Riley, Yves Kini, Anna L. Watts, Bas Dorsman, Slavko Bogdanov, Sebastien Guillot, Paul S. Ray, Daniel J. Reardon, Ronald A. Remillard, Anna V. Bilous, Daniela Huppenkothen, James M. Lattimer, Nathan Rutherford, Zaven Arzoumanian, Keith C. Gendreau, Sharon M. Morsink, Wynn C. G. Ho
Figure caption: Posteriors obtained by CST+PDT for NICER only (default-resolution run) involving both lower and upper background limits and for the joint NICER–XMM run.
Paper: Evidence for Nightside Water Emission Found in Transit of Ultra-hot Jupiter WASP-33 b
Authors: Yuanheng Yang, Guo Chen, Fei Yan, Xianyu Tan, Jianghui Ji
Figure caption: An example of phase-resolved general H2O transmission spectra simulation using a reference GCM with TiO and VO (i.e., nightside cooling is effective). Top panel: the normalized phase-resolved nightside thermal emission spectra from −17.5° to +17.5° with a step of 3.5° (color-coded from blue to red). Bottom panel: phase-resolved general transmission spectra with nightside thermal emission. The black line shows the classical transmission spectrum for H2O lines (i.e., without considering night emission).
Paper: Evidence for Nightside Water Emission Found in Transit of Ultra-hot Jupiter WASP-33 b
Authors: Yuanheng Yang, Guo Chen, Fei Yan, Xianyu Tan, Jianghui Ji
Figure caption: CCF and K p–Δv maps of H2O averaged over two nights of GIANO-B observations. First row: CCF map, where the two horizontal dashed lines indicate the start and end of the transit, and the tilted dashed line represents the expected planetary orbit. Second row: K p–Δv map with orthogonal black dashed lines for the expected K p and Δv, and a pentagram for the position of the S/N peak. Third row: the 1D CCF corresponding to the K p value at the S/N peak. The vertical gray dashed line indicates Δv = 0.
Paper: Evidence for Nightside Water Emission Found in Transit of Ultra-hot Jupiter WASP-33 b
Authors: Yuanheng Yang, Guo Chen, Fei Yan, Xianyu Tan, Jianghui Ji
Figure caption: The general transmission spectrum models with three types of nightside T-P profiles for WASP-33 b. The first three columns show the general transmission spectra of H2O, CO, and OH, respectively, while the fourth column shows the T-P profiles. Each inset shows a zoomed-in view of the spectrum. From top to bottom, correspond to the inverted, noninverted, and isothermal nightside T-P profiles.
Paper: Evidence for Nightside Water Emission Found in Transit of Ultra-hot Jupiter WASP-33 b
Authors: Yuanheng Yang, Guo Chen, Fei Yan, Xianyu Tan, Jianghui Ji
Figure caption: Comparison of K p–Δv maps for the injection-recovery tests of WASP-33 b. The injected general transmission model has included the nightside thermal emission. The cyan dashed lines indicate the expected values of the injected signal. The left and right panels show the results from the correct general transmission spectrum template and the pure transmission spectrum template, respectively. The first and second rows present the results for H2O and CO, respectively. The strength of the injected CO signal has been enhanced by 5 times.
Paper: Evidence for Nightside Water Emission Found in Transit of Ultra-hot Jupiter WASP-33 b
Authors: Yuanheng Yang, Guo Chen, Fei Yan, Xianyu Tan, Jianghui Ji
Figure caption: Masking of the CARMENES and GIANO-B spectral orders. The vertical red and gray shaded areas indicate the masked orders for CARMENES and GIANO-B, respectively. The green line indicates the H2O thermal emission spectrum. The purple line indicates the Earth’s telluric spectrum.
Paper: Evidence for Nightside Water Emission Found in Transit of Ultra-hot Jupiter WASP-33 b
Authors: Yuanheng Yang, Guo Chen, Fei Yan, Xianyu Tan, Jianghui Ji
Figure caption:  K p–Δv maps of H2O for GIANO-B data (≲1.75 μm) with two nights combined. The crossed white dashed lines indicate the S/N peak. The crossed black dashed lines indicate the expected K p and Δv.
Paper: Evidence for Nightside Water Emission Found in Transit of Ultra-hot Jupiter WASP-33 b
Authors: Yuanheng Yang, Guo Chen, Fei Yan, Xianyu Tan, Jianghui Ji
Figure caption:  K p–Δv maps of H2O from individual nights of GIANO-B observations. The crossed white dashed lines indicate the S/N peak.
Paper: The Unluckiest Star: A Spectroscopically Confirmed Repeated Partial Tidal Disruption Event AT 2022dbl
Authors: Zheyu Lin, Ning Jiang, Tinggui Wang, Xu Kong, Dongyue Li, Han He, Yibo Wang, Jiazheng Zhu, Wentao Li, Ji-an Jiang, Avinash Singh, Rishabh Singh Teja, D. K. Sahu, Chichuan Jin, Keiichi Maeda, Shifeng Huang
Figure caption: Comparison of optical repeated pTDEs AT 2020vdq (Somalwar et al. 2023b; Yao et al. 2023) and AT 2022dbl (this work), as well as optical TDEs listed in Yao et al. (2023). BH mass vs. (a) peak blackbody luminosity, (b) peak blackbody radius, and (c) rest-frame rise time from half-peak luminosity to peak luminosity vs. decline time from peak luminosity to half-peak luminosity. In plot (b), both AT 2020vdq and AT 2022dbl show similar blackbody radii in their two flares. The parameters of AT 2020vdq are mostly adopted or derived from Somalwar et al. (2023b). However, in plot (c), the derived rise and decline timescales of the first flare of AT 2020vdq in Somalwar et al. (2023b) and Yao et al. (2023) are greatly different and hence plotted in green and light green, respectively.
Paper: The Unluckiest Star: A Spectroscopically Confirmed Repeated Partial Tidal Disruption Event AT 2022dbl
Authors: Zheyu Lin, Ning Jiang, Tinggui Wang, Xu Kong, Dongyue Li, Han He, Yibo Wang, Jiazheng Zhu, Wentao Li, Ji-an Jiang, Avinash Singh, Rishabh Singh Teja, D. K. Sahu, Chichuan Jin, Keiichi Maeda, Shifeng Huang
Figure caption: The evolution of the FWHM, velocity shift, and luminosity of the N III λ4100 (blue squares) and Hα (red dots) emission lines as well as their ratios (black diamonds) and the power-law indexes of the continua. In the last panel, measurements from the LCO spectra taken during the first flare and P200 spectra taken during the second flare are marked in dots and asterisks, respectively.
Paper: The Unluckiest Star: A Spectroscopically Confirmed Repeated Partial Tidal Disruption Event AT 2022dbl
Authors: Zheyu Lin, Ning Jiang, Tinggui Wang, Xu Kong, Dongyue Li, Han He, Yibo Wang, Jiazheng Zhu, Wentao Li, Ji-an Jiang, Avinash Singh, Rishabh Singh Teja, D. K. Sahu, Chichuan Jin, Keiichi Maeda, Shifeng Huang
Figure caption: The fitting plots for optical spectra of AT 2022dbl.
Paper: The Unluckiest Star: A Spectroscopically Confirmed Repeated Partial Tidal Disruption Event AT 2022dbl
Authors: Zheyu Lin, Ning Jiang, Tinggui Wang, Xu Kong, Dongyue Li, Han He, Yibo Wang, Jiazheng Zhu, Wentao Li, Ji-an Jiang, Avinash Singh, Rishabh Singh Teja, D. K. Sahu, Chichuan Jin, Keiichi Maeda, Shifeng Huang
Figure caption: The SED fitting result of the prospector package, in units of AB magnitudes. The best-fit SED and photometry are plotted in green and red, respectively. The blue circles represent the synthetic magnitudes of the UVOT UVW2, UVM2, UVW1, U, B, and V bands.
Paper: The Unluckiest Star: A Spectroscopically Confirmed Repeated Partial Tidal Disruption Event AT 2022dbl
Authors: Zheyu Lin, Ning Jiang, Tinggui Wang, Xu Kong, Dongyue Li, Han He, Yibo Wang, Jiazheng Zhu, Wentao Li, Ji-an Jiang, Avinash Singh, Rishabh Singh Teja, D. K. Sahu, Chichuan Jin, Keiichi Maeda, Shifeng Huang
Figure caption: The optical spectra of AT 2022dbl. Black dotted lines limit the range of the spectral fitting.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The Unluckiest Star: A Spectroscopically Confirmed Repeated Partial Tidal Disruption Event AT 2022dbl
Authors: Zheyu Lin, Ning Jiang, Tinggui Wang, Xu Kong, Dongyue Li, Han He, Yibo Wang, Jiazheng Zhu, Wentao Li, Ji-an Jiang, Avinash Singh, Rishabh Singh Teja, D. K. Sahu, Chichuan Jin, Keiichi Maeda, Shifeng Huang
Figure caption: Spectra after subtracting the host-galaxy contribution and the continuum. Spectra of both flares show similar emission lines.
Paper: Evidence for Nightside Water Emission Found in Transit of Ultra-hot Jupiter WASP-33 b
Authors: Yuanheng Yang, Guo Chen, Fei Yan, Xianyu Tan, Jianghui Ji
Figure caption: The H2O transmission spectrum model for WASP-33 b. The upper-left panel shows the model spectra of H2O, with our general transmission spectrum (with nightside emission) in orange and the classical transmission spectrum (without nightside emission) in black. The lower-left panel shows the normalized continuum-free model spectrum. The middle panel shows the T-P profiles for the limb and nightside atmospheres. The gray shaded area shows the contribution function of the nightside thermal emission, integrated over the wavelength space. The dashed–dotted lines show the condensation profiles of condensates commonly expected on high-temperature giants (Visscher et al. 2010; Wakeford et al. 2017). The peak of the contribution function here is above the intersection of the condensation profile with the nightside T-P, indicating that the thermal emission is not obscured by clouds. The right panel shows the H2O mass fraction calculated from the chemical equilibrium given by the T-P in the middle panel, compared to that of the nightside condensates.
Paper: Evidence for Nightside Water Emission Found in Transit of Ultra-hot Jupiter WASP-33 b
Authors: Yuanheng Yang, Guo Chen, Fei Yan, Xianyu Tan, Jianghui Ji
Figure caption: Top panel: comparison between time-averaged nightside emission flux ﹩{\overline{{ \mathcal F }}}_{\lambda ,{\rm{p}}(\mathrm{night}),\mathrm{out}}(t)﹩ and nightside emission flux at the moment of mid-transit ﹩{{ \mathcal F }}_{\lambda ,{\rm{p}}(\mathrm{night}),\mathrm{in}}(t=0)﹩. Bottom panel: comparison between classical and general transmission spectra. The gray dashed line shows the classical transmission spectrum. The solid lines show our proposed general transmission spectra, which incorporate the nightside emission. The purple and cyan colors indicate that the nightside temperature structure is inverted and noninverted, respectively. All models include rotational broadening.
Paper: Big Galaxies and Big Black Holes: The Massive Ends of the Local Stellar and Black Hole Mass Functions and the Implications for Nanohertz Gravitational Waves
Authors: Emily R. Liepold, Chung-Pei Ma
Figure caption: (Top) The z = 0 BHMF inferred from our GSMF and the M BH−M * scaling relation (violet band; 90% confidence interval). The dashed curves represent the BHMFs computed from the other GSMFs in Figure 3. The two cyan curves compare the BHMFs inferred from the galaxy VDF instead of the GSMF using the standard M BH–σ relation (dotted–dashed) vs. the ad hoc M BH–σ relation (dotted) from Sato-Polito et al. (2023). (Bottom) The SMBH number counts (above mass M BH) within the MASSIVE survey volume predicted by each BHMF in the top panel. The gray histograms compare the counts of dynamically detected SMBHs within 108 Mpc (top for the entire sphere; bottom for the northern portion surveyed by MASSIVE).
Paper: Big Galaxies and Big Black Holes: The Massive Ends of the Local Stellar and Black Hole Mass Functions and the Implications for Nanohertz Gravitational Waves
Authors: Emily R. Liepold, Chung-Pei Ma
Figure caption: Stellar mass M * vs. absolute K-band magnitude M  K  of MASSIVE galaxies with M * measurements from dynamical modeling (left and middle) or SPS modeling (right). For dynamical M *, two sets of M  K  are shown: 2MASS (left) and CFHT (middle). The solid line in each panel represents the respective best-fitting relation (from left to right): ﹩{\mathrm{log}}_{10}({M}_{* }/{M}_{\odot })=11.92-0.49({M}_{K}^{2\mathrm{MASS}}+26)﹩, ﹩{\mathrm{log}}_{10}({M}_{* }/{M}_{\odot })=11.85-0.43({M}_{K}^{\mathrm{CFHT}}+26)﹩, and ﹩{\mathrm{log}}_{10}({M}_{* }/{M}_{\odot })=11.81-0.41({M}_{K}^{\mathrm{CFHT}}+26);﹩ each shaded band indicates the intrinsic scatter. Filled symbols indicate the measurements used in each fit. Open circles in the left panel mark either multiple M * measurements of the same galaxy from other methods not used in the fit or systems excluded from the fit (see Section 2.1 and Table A1). For ease of comparison, the best-fit blue line in the middle panel is shown as a dashed blue line in the right panel, and similarly for the red lines, illustrating that SPS M * is on average ∼7% lower than dynamical M *.
Paper: Big Galaxies and Big Black Holes: The Massive Ends of the Local Stellar and Black Hole Mass Functions and the Implications for Nanohertz Gravitational Waves
Authors: Emily R. Liepold, Chung-Pei Ma
Figure caption: Comparison of the characteristic amplitude of gravitational waves at f = 1 yr−1, h  c , reported by the PTA teams and predicted by BHMFs inferred from galaxy distribution functions. The right panel shows h  c , and the left panel shows the differential contribution to h 2  c , ﹩{{dh}}_{c}^{2}/d{\mathrm{log}}_{10}{M}_{\mathrm{BH}}﹩, as a function of M BH. The predicted amplitudes are computed from Equation (5) using the BHMFs in Figure 4. All error bars denote 90% confidence intervals. The published PPTA value quotes a 68% interval; we enlarge it by a factor of 1.64 to approximate the 90% interval. The individual value of h  c  (in units of 10−15) is (from left to right): ﹩({2.4}_{-0.6}^{+0.7}),({2.04}_{-0.36}^{+0.41}),(2.5\pm 0.7)﹩ from PTAs; ﹩({2.0}_{-0.5}^{+0.7}),({1.7}_{-0.4}^{+0.5}),({1.3}_{-0.3}^{+0.4}),({1.4}_{-0.4}^{+0.5})﹩ from the four M *-based GSMFs; and ﹩({1.1}_{-0.3}^{+0.4}),({2.5}_{-0.8}^{+1.5})﹩ from the σ-based GSMFs.
Paper: Big Galaxies and Big Black Holes: The Massive Ends of the Local Stellar and Black Hole Mass Functions and the Implications for Nanohertz Gravitational Waves
Authors: Emily R. Liepold, Chung-Pei Ma
Figure caption: (Top) The z = 0 GSMF from this Letter (violet band; 90% confidence interval). It is constructed to reproduce the z = 0 GSMF of Leja et al. (2020; green dashed curve) at M * ≲ 1011 M ⊙ and to match the stellar mass distribution of MASSIVE galaxies at M * ≳ 1011.5 M ⊙. The violet band represents the GSMF from averaging two separate posterior distributions for MASSIVE dynamically inferred M * (blue curve) and SPS inferred M * (red curve). Three GSMFs from prior studies of SDSS galaxies are shown for comparison: Bernardi et al. (2013; indigo), D’Souza et al. (2015; orange), and Moustakas et al. (2013; cyan). (Bottom) Cumulative galaxy counts in the MASSIVE survey volume estimated from each GSMF in the top panel. The orange, green, and cyan curves would yield fewer than 10 galaxies in the MASSIVE survey.
Paper: Big Galaxies and Big Black Holes: The Massive Ends of the Local Stellar and Black Hole Mass Functions and the Implications for Nanohertz Gravitational Waves
Authors: Emily R. Liepold, Chung-Pei Ma
Figure caption: Number of MASSIVE galaxies above stellar mass M *. Each histogram is for M * from the corresponding M *–M  K  relation in Figure 1; when available, the dynamical or SPS M * values are used instead of M * from the scaling relation. The blue and gray curves are very similar because both are calibrated to MASSIVE galaxies with reliable dynamical M *. The red curve has a lower amplitude because the SPS M * is on average ∼7% lower than the dynamical M *. Each shaded band represents the 90% confidence region.
Paper: Big Galaxies and Big Black Holes: The Massive Ends of the Local Stellar and Black Hole Mass Functions and the Implications for Nanohertz Gravitational Waves
Authors: Emily R. Liepold, Chung-Pei Ma
Figure caption: Comparison of the local black hole mass density, ρ BH, given by each BHMF in Figure 4 and inferred from the QLF. The right panel shows ρ BH, and the left panel shows the differential contribution to ρ BH, ﹩d{\rho }_{\mathrm{BH}}/d{\mathrm{log}}_{10}{M}_{\mathrm{BH}}﹩, as a function of M BH. All error bars denote 90% confidence intervals. Hopkins et al. (2007) quotes a 68% interval; we enlarge it by a factor of 1.64 to approximate the 90% interval.
Paper: Can Solar Limb Flare Prediction Be Properly Made by Extreme-ultraviolet Intensities?
Authors: Jaewon Lee, Yong-Jae Moon, Hyun-Jin Jeong, Kangwoo Yi, Harim Lee
Figure caption: The distribution of summed intensities at 94 (y-axis) and 131 Å (x-axis). The data of each year are represented by a different color. Cross and circle symbols represent flaring and nonflaring samples, respectively. Panel (a) is the summation of pixels inside the solar disk. Panel (b) is the defined limb intensity and panel (c) is the cross-calibrated one by the 2011 nonflaring data set. All data are corrected by AIA response table version 10 and presented on a logarithmic scale.
Paper: Can Solar Limb Flare Prediction Be Properly Made by Extreme-ultraviolet Intensities?
Authors: Jaewon Lee, Yong-Jae Moon, Hyun-Jin Jeong, Kangwoo Yi, Harim Lee
Figure caption: Scatterplot of 22 events for the available models in NASA/CCMC flare scoreboard. The x-axis represents the average flare occurrence probability of the NASA/CCMC flare scoreboard, and the y-axis represents the flare occurrence probability predicted by our MLP model.
Paper: Can Solar Limb Flare Prediction Be Properly Made by Extreme-ultraviolet Intensities?
Authors: Jaewon Lee, Yong-Jae Moon, Hyun-Jin Jeong, Kangwoo Yi, Harim Lee
Figure caption: The flare occurrence rates of the test data set as a function of 94 Å limb intensity (a) and 131 Å total intensity (b). The ratios above each bin indicate the number of flaring events divided by that of the total ones.
Paper: Can Solar Limb Flare Prediction Be Properly Made by Extreme-ultraviolet Intensities?
Authors: Jaewon Lee, Yong-Jae Moon, Hyun-Jin Jeong, Kangwoo Yi, Harim Lee
Figure caption: ROC curves of our empirical and MLP models. Both the empirical and the MLP models show better performance than a random forecast, and the difference in performance between the two models is not significant.
Paper: A NICER View of the Nearest and Brightest Millisecond Pulsar: PSR J0437–4715
Authors: Devarshi Choudhury, Tuomo Salmi, Serena Vinciguerra, Thomas E. Riley, Yves Kini, Anna L. Watts, Bas Dorsman, Slavko Bogdanov, Sebastien Guillot, Paul S. Ray, Daniel J. Reardon, Ronald A. Remillard, Anna V. Bilous, Daniela Huppenkothen, James M. Lattimer, Nathan Rutherford, Zaven Arzoumanian, Keith C. Gendreau, Sharon M. Morsink, Wynn C. G. Ho
Figure caption: Posteriors obtained by CST+PDT (default-resolution run) as applied to the the 3C50 data set, testing the different implementations of the 3C50 background constraints.
Paper: The Unluckiest Star: A Spectroscopically Confirmed Repeated Partial Tidal Disruption Event AT 2022dbl
Authors: Zheyu Lin, Ning Jiang, Tinggui Wang, Xu Kong, Dongyue Li, Han He, Yibo Wang, Jiazheng Zhu, Wentao Li, Ji-an Jiang, Avinash Singh, Rishabh Singh Teja, D. K. Sahu, Chichuan Jin, Keiichi Maeda, Shifeng Huang
Figure caption: Top panel: the UV/optical light curves of AT 2022dbl during the first and second flares. 3σ upper limits are plotted in downward triangles. Bottom panel: the X-ray count rate of AT 2022dbl. The vertical dotted and dashed lines mark the approximate rise time of the first and second flares, respectively. 3σ upper limits are plotted in downward arrows.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The Unluckiest Star: A Spectroscopically Confirmed Repeated Partial Tidal Disruption Event AT 2022dbl
Authors: Zheyu Lin, Ning Jiang, Tinggui Wang, Xu Kong, Dongyue Li, Han He, Yibo Wang, Jiazheng Zhu, Wentao Li, Ji-an Jiang, Avinash Singh, Rishabh Singh Teja, D. K. Sahu, Chichuan Jin, Keiichi Maeda, Shifeng Huang
Figure caption: The historical light curves of the position of AT 2022dbl. Top panel: the non-host-subtracted light curves of three optical surveys, CRTS (V band), PTF (R band), and Gaia (G band), along with the MIR WISE survey (W1 and W2 bands). Bottom panel: the host-subtracted light curves of three optical surveys: ZTF (g and r bands), ATLAS (c and o bands), and ASAS-SN (g and V bands). To improve the SNR, we binned the data into 10 day bins for all optical bands except for Gaia G and approximately half-year bins for the W1 and W2 bands. Note that a potential early flare is displayed in the ASAS-SN V-band light curve; we discuss its reliability in Section 2.2.1.
Paper: The Unluckiest Star: A Spectroscopically Confirmed Repeated Partial Tidal Disruption Event AT 2022dbl
Authors: Zheyu Lin, Ning Jiang, Tinggui Wang, Xu Kong, Dongyue Li, Han He, Yibo Wang, Jiazheng Zhu, Wentao Li, Ji-an Jiang, Avinash Singh, Rishabh Singh Teja, D. K. Sahu, Chichuan Jin, Keiichi Maeda, Shifeng Huang
Figure caption: The light-curve fitting results of AT 2022dbl. The luminosities of the o and g bands are normalized to the blackbody luminosities of the first and second flares, respectively. For comparison, the fitted decline curve for the second flare is extended to ∼+120 days in the dotted style.
Paper: The Unluckiest Star: A Spectroscopically Confirmed Repeated Partial Tidal Disruption Event AT 2022dbl
Authors: Zheyu Lin, Ning Jiang, Tinggui Wang, Xu Kong, Dongyue Li, Han He, Yibo Wang, Jiazheng Zhu, Wentao Li, Ji-an Jiang, Avinash Singh, Rishabh Singh Teja, D. K. Sahu, Chichuan Jin, Keiichi Maeda, Shifeng Huang
Figure caption: The pPXF fitting result of the SDSS host-galaxy spectrum. The residual shows no clear emission line, implying that the host galaxy should not be an AGN.
Paper: Transmission Spectroscopy of the Habitable Zone Exoplanet LHS 1140 b with JWST/NIRISS
Authors: Charles Cadieux, René Doyon, Ryan J. MacDonald, Martin Turbet, Étienne Artigau, Olivia Lim, Michael Radica, Thomas J. Fauchez, Salma Salhi, Lisa Dang, Loïc Albert, Louis-Philippe Coulombe, Nicolas B. Cowan, David Lafrenière, Alexandrine L'Heureux, Caroline Piaulet-Ghorayeb, Björn Benneke, Ryan Cloutier, Benjamin Charnay, Neil J. Cook, Marylou Fournier-Tondreau, Mykhaylo Plotnykov, Diana Valencia
Figure caption: Combined transmission spectrum of LHS 1140 b with NIRISS/SOSS from two transits and POSEIDON retrieval analysis results. The binned spectra at R ∼ 20 (white points) and at a higher R ∼ 100 (gray points) significantly improve on the HST/WFC3 data from Edwards et al. (2021; black diamonds). The median models with 1σ–2σ confidence envelopes are shown for a stellar contamination model (orange) and a joint stellar contamination and planetary atmosphere model (blue), with their respective posterior distributions shown in the bottom panels (same colors). Confidence intervals for each parameter are given in Table D1. The transmission spectrum of LHS 1140 b is mainly shaped by stellar contamination from unocculted faculae. A planetary atmosphere dominated by N2 or CO2 is compatible with the data, with the former pure composition being the maximum a posteriori model. A clear N2-rich atmosphere combined with unocculted faculae is preferred at 2.3σ over faculae alone (see Section 5.2 and Figure D1).