adsabs/AstroCLIMB huggingface dataset:
Paper: A Diverse, Overlooked Population of Type Ia Supernovae Exhibiting Mid-infrared Signatures of Delayed Circumstellar Interaction
Authors: Geoffrey Mo, Kishalay De, Eli Wiston, Nayana A. J., Raffaella Margutti, Danielle Frostig, Jesper Sollerman, Yashvi Sharma, Takashi J. Moriya, Kevin B. Burdge, Jacob Jencson, Viraj R. Karambelkar, Nathan P. Lourie
Figure caption: Optical and MIR light curves of PTF11kx and SN 2015cp. We present NEOWISE photometry extracted using our difference imaging pipeline. We also show optical data from the Palomar Transient Factory (PTF; B. Dilday et al. 2012) and MIR data from Spitzer for PTF11kx (M. L. Graham et al. 2017). The NEOWISE and Spitzer photometry are marginally offset, which can be attributed to differences in filters between each instrument (T. H. Jarrett et al. 2011). For SN 2015cp, we show optical data from the intermediate PTF (iPTF; M. L. Graham et al. 2019).
Paper: Evidence for a Volcanic Atmosphere on the Sub-Earth L 98-59 b
Authors: Aaron Bello-Arufe, Mario Damiano, Katherine A. Bennett, Renyu Hu, Luis Welbanks, Ryan J. MacDonald, Darryl Z. Seligman, David K. Sing, Armen Tokadjian, Apurva V. Oza, Jeehyun Yang
Figure caption: Self-consistent models of an SO2-dominated atmosphere on L 98-59 b. The figure shows the mixing ratio of key molecules (left) and the temperature (right) as a function of pressure, and the solid and dashed lines correspond to internal heat fluxes of 1× and 10× the insolation, respectively, corresponding to tidal Q values of 30 and 3. The atmosphere should build up abundant SO3 and gas-phase elemental sulfur (S8) produced from the photolysis of SO2.
Paper: A Diverse, Overlooked Population of Type Ia Supernovae Exhibiting Mid-infrared Signatures of Delayed Circumstellar Interaction
Authors: Geoffrey Mo, Kishalay De, Eli Wiston, Nayana A. J., Raffaella Margutti, Danielle Frostig, Jesper Sollerman, Yashvi Sharma, Takashi J. Moriya, Kevin B. Burdge, Jacob Jencson, Viraj R. Karambelkar, Nathan P. Lourie
Figure caption: NEOWISE W2 reference, stacked science, and subtraction cutouts of our sources at their brightest epoch. Each cutout has a width and height of 3﹩{}^{{\prime} }﹩ centered at the location of the transient, aligned north up and east left.
Paper: Evidence for a Volcanic Atmosphere on the Sub-Earth L 98-59 b
Authors: Aaron Bello-Arufe, Mario Damiano, Katherine A. Bennett, Renyu Hu, Luis Welbanks, Ryan J. MacDonald, Darryl Z. Seligman, David K. Sing, Armen Tokadjian, Apurva V. Oza, Jeehyun Yang
Figure caption: ExoTR retrieval results for L 98-59 b. Top: retrieved mean spectrum (mean model and 2σ confidence interval) from scenario 8 in Table C2. Bottom: Posterior distribution functions for selected gases. The posterior distribution functions suggest a heavy atmosphere rich in SO2.
Paper: Evidence for a Volcanic Atmosphere on the Sub-Earth L 98-59 b
Authors: Aaron Bello-Arufe, Mario Damiano, Katherine A. Bennett, Renyu Hu, Luis Welbanks, Ryan J. MacDonald, Darryl Z. Seligman, David K. Sing, Armen Tokadjian, Apurva V. Oza, Jeehyun Yang
Figure caption: The transmission spectra of L 98-59 b using independent pipelines (left), and in the case of Eureka!, different lightcurve fitting strategies (right). Brown is our standard Eureka! reduction obtained when we binned the lightcurves to Δλ = 0.04 μm, and yellow is the FIREFLy  reduction with the same binning (the retrievals on the FIREFLy data used the equal-counts-per-bin reduction, not shown here). Blue is the same reduction as brown, but allowing for the quadratic term of the polynomial (c2, only used in NRS1) to be freely fit in each channel instead of fixing it to the value derived from the white lightcurve. Green is the same reduction as brown, but allowing for limb darkening (LD) to be freely fit in each channel.
Paper: Evidence for a Volcanic Atmosphere on the Sub-Earth L 98-59 b
Authors: Aaron Bello-Arufe, Mario Damiano, Katherine A. Bennett, Renyu Hu, Luis Welbanks, Ryan J. MacDonald, Darryl Z. Seligman, David K. Sing, Armen Tokadjian, Apurva V. Oza, Jeehyun Yang
Figure caption: Different choices of limb-darkening coefficients. The Eureka! reduction fixed the quadratic limb-darkening coefficients u1 and u2 to those calculated with ExoTiC-LD (in the plot, we show ﹩{q}_{1}={({u}_{1}+{u}_{2})}^{2}﹩ and ﹩{q}_{2}=0.5{u}_{1}{({u}_{1}+{u}_{2})}^{-2}﹩ instead; D. M. Kipping 2013), while FIREFLy  opted for fixing q1 = 0.1 and q2 = 0. We also present the values from an alternative Eureka! reduction in which q1 and q2 were freely fitted in each spectroscopic lightcurve. The uncertainties correspond to the 16th and 84th percentiles in all samples in each channel.
Paper: Evidence for a Volcanic Atmosphere on the Sub-Earth L 98-59 b
Authors: Aaron Bello-Arufe, Mario Damiano, Katherine A. Bennett, Renyu Hu, Luis Welbanks, Ryan J. MacDonald, Darryl Z. Seligman, David K. Sing, Armen Tokadjian, Apurva V. Oza, Jeehyun Yang
Figure caption: The existence of widespread volcanism on L 98-59 b—if caused by the runaway melting mechanism—provides constraints on the tidal quality factor and size of the subsurface magma ocean. Left: Tidal quality factor versus radius for solar system planets and satellites along with the constraint for L 98-59 b given by Equation (E3) (i.e., Q < 1400QIo; see Appendix E) and by assuming that volcanic outgassing must balance atmospheric escape (Q < 700QIo; see Section 5.2). Right: Volume-integrated tidal heating for a composite body consisting of a liquid interior surrounded by a solid mantle as a function of subsurface magma ocean radius, normalized to the case of no magma ocean. The location where the derivative of this function with respect to the melt radius is zero indicates the approximate equilibrium value for the runaway melting process.
Paper: Evidence for a Volcanic Atmosphere on the Sub-Earth L 98-59 b
Authors: Aaron Bello-Arufe, Mario Damiano, Katherine A. Bennett, Renyu Hu, Luis Welbanks, Ryan J. MacDonald, Darryl Z. Seligman, David K. Sing, Armen Tokadjian, Apurva V. Oza, Jeehyun Yang
Figure caption: POSEIDON retrieval results for L 98-59 b. Top: retrieved transmission spectra (median model and 1σ confidence interval) for three models: a flat line (gray), stellar contamination (blue), and an SO2-rich planetary atmosphere (orange). The retrieval models shown correspond to fits on the highest-resolution (Δλ = 0.01 μm) Eureka! data (transparent error bars), with the lower-resolution Δλ = 0.04 μm data overplotted for clarity (nontransparent error bars). Bottom: posterior histograms corresponding to the atmosphere and stellar contamination models. The mean molecular weight (μ)—a derived property from the atmospheric mixing ratio parameters—rules out light atmospheres dominated by H2 and He (μ ≈ 2.3 amu). The statistically favored solution is a high mean molecular weight atmosphere dominated by SO2 (μ = 64 amu).
Paper: Evidence for a Volcanic Atmosphere on the Sub-Earth L 98-59 b
Authors: Aaron Bello-Arufe, Mario Damiano, Katherine A. Bennett, Renyu Hu, Luis Welbanks, Ryan J. MacDonald, Darryl Z. Seligman, David K. Sing, Armen Tokadjian, Apurva V. Oza, Jeehyun Yang
Figure caption: The model preference for a planet with an atmosphere over a flat line is consistent with regions of dominant SO2 absorption. The data are color coded by the pointwise difference in the expected log pointwise predictive density (elpd) between the simple atmospheric model and the bare-rock (that is, flat-line) model. The retrieved median and 2σ confidence interval from the simple atmospheric model are shown in gray. Redder data points, that is those with larger positive Δelpd, are better explained by the atmospheric model with SO2 absorption.
Paper: Evidence for a Volcanic Atmosphere on the Sub-Earth L 98-59 b
Authors: Aaron Bello-Arufe, Mario Damiano, Katherine A. Bennett, Renyu Hu, Luis Welbanks, Ryan J. MacDonald, Darryl Z. Seligman, David K. Sing, Armen Tokadjian, Apurva V. Oza, Jeehyun Yang
Figure caption: Allan deviation plots. Left: Allan deviation plots for the Eureka! white lightcurves of both detectors. Right: Allan deviation plots for the Eureka! spectroscopic lightcurves. We present the reduction with the Δλ = 0.04 μm binning.
Paper: Evidence for a Volcanic Atmosphere on the Sub-Earth L 98-59 b
Authors: Aaron Bello-Arufe, Mario Damiano, Katherine A. Bennett, Renyu Hu, Luis Welbanks, Ryan J. MacDonald, Darryl Z. Seligman, David K. Sing, Armen Tokadjian, Apurva V. Oza, Jeehyun Yang
Figure caption: Retrieved SO2 abundances for models using radiative-convective equilibrium vertical temperature structures. The 1× and 10×  insolation models infer SO2 abundances over 90% within their 68% confidence interval, favoring an SO2-rich atmosphere and disfavoring large CO2 abundances.
Paper: Evidence for a Volcanic Atmosphere on the Sub-Earth L 98-59 b
Authors: Aaron Bello-Arufe, Mario Damiano, Katherine A. Bennett, Renyu Hu, Luis Welbanks, Ryan J. MacDonald, Darryl Z. Seligman, David K. Sing, Armen Tokadjian, Apurva V. Oza, Jeehyun Yang
Figure caption: SO2/CO2 abundance ratio retrieved with Aurora.
Paper: Maximal Jet Energy of Gamma-Ray Bursts through the Blandford–Znajek Mechanism
Authors: Zhao-Feng Wu, Michail Damoulakis, Paz Beniamini, Dimitrios Giannios
Figure caption: (a) The observed cumulative energy of the jet normalized by the total accretion energy, Ejet/(Maccc2), as a function of the transition function at spin equilibrium ﹩{{\rm{\Delta }}}_{{\rm{eq}}}={\left({{\rm{\Phi }}}_{{\rm{BH}}}/{{\rm{\Phi }}}_{{\rm{MAD}}}\right)}_{{\rm{eq}}}﹩. The solid blue line shows the full numerical calculations for ﹩\dot{m}=0.1\,{M}_{\odot }\,{{\rm{s}}}^{-1},{t}_{{\rm{e}}}=40\,{\rm{s}},{a}_{0}=0.01,{M}_{\mathrm{BH},{\rm{0}}}=3\,{M}_{\odot },{M}_{* }\,=15\,{M}_{\odot }﹩, while the red dashed–dotted line represents the fit from Equation (19). The black dotted lines mark the maximum observed cumulative jet energy, ﹩{E}_{{\rm{jet}},{\rm{\max }}}﹩, which is 1.44% of the accretion energy, about 12 times higher than that for the MAD state. (b) The blue solid curve is the same as (a), while the orange dashed and green dotted lines show results for different initial spins, a0 = 0.1 and a0 = 0.25, respectively. The red dashed–dotted line shows results for ﹩\dot{m}=0.05\,{M}_{\odot }\,{{\rm{s}}}^{-1}﹩ and te = 80 s, keeping the total accreted mass Macc constant. For a0 ≲ 0.25, the normalized jet energy is largely insensitive to system parameters.
Paper: Maximal Jet Energy of Gamma-Ray Bursts through the Blandford–Znajek Mechanism
Authors: Zhao-Feng Wu, Michail Damoulakis, Paz Beniamini, Dimitrios Giannios
Figure caption: Evolution of jet power and black hole spin for initial magnetic fluxes ΦBH,0 = 1026.5−28.65 G cm2, initial BH spin a0 = 0.01 (top), and a0 = 0.25 (bottom). The black hole initial mass, accretion rate, and progenitor mass are fixed at MBH,0 = 3 M⊙, ﹩\dot{m}=0.1{M}_{\odot }\,{{\rm{s}}}^{-1}﹩, and M* = 15 M⊙, respectively. Colored dots mark the breakout time tb of the jet from the stellar envelope and colored triangles mark the spin equilibrium timescale teq given in Equation (14). In both cases, jet power and spin approach equilibrium after t ∼ 10 s. As the magnetic flux approaches the MAD limit, the equilibrium spin decreases, reaching aeq ≈ 0.06 in the fully MAD state. The equilibrium timescale teq is similar to tb for a0 = 0.01, but it is significantly longer than tb for a0 = 0.25, especially when the magnetic flux is high. The relatively constant observed jet luminosity suggests a small initial black hole spin in collapsar models.
Paper: Maximal Jet Energy of Gamma-Ray Bursts through the Blandford–Znajek Mechanism
Authors: Zhao-Feng Wu, Michail Damoulakis, Paz Beniamini, Dimitrios Giannios
Figure caption: (a) Distribution of accreted mass, Macc, assuming all lGRBs are produced in the MAD limit (blue solid line). The red solid line represents the mass distribution of Galactic WC and WO stars (A. A. C. Sander et al. 2019), with the red dashed line indicating the peak. If the MAD assumption holds, the Macc distribution should peak around 10% of the M* peak. However, for subluminous lGRBs, Macc may be as low as ∼0.1 M⊙, i.e., potentially too small relative to the progenitor mass. Additionally, the broad distribution of accreted masses does not align with the narrow range of progenitor masses. (b) Accreted mass, Macc, distribution for sGRBs under the MAD limit (blue solid line). The red dashed line indicates the typical mass of the remnant disk (∼0.1 M⊙). The Macc distribution peaks at around 0.1% of the disk mass, suggesting that the accreted mass is too small for typical remnant disks. The tensions in (a) and (b) can be alleviated if lGRBs and standard sGRBs are produced by systems far from the MAD state.
Paper: Maximal Jet Energy of Gamma-Ray Bursts through the Blandford–Znajek Mechanism
Authors: Zhao-Feng Wu, Michail Damoulakis, Paz Beniamini, Dimitrios Giannios
Figure caption: Top panel: Equilibrium spin aeq as a function of the transition parameter at spin equilibrium, ﹩{{\rm{\Delta }}}_{{\rm{eq}}}={\left({{\rm{\Phi }}}_{{\rm{BH}}}/{{\rm{\Phi }}}_{{\rm{MAD}}}\right)}_{{\rm{eq}}}﹩. The dashed red line marks the equilibrium spin at the MAD limit. Bottom panel: Normalized spin-equilibrium jet power, ﹩{L}_{{\rm{jet}},{\rm{eq}}}/(\dot{m}{c}^{2})﹩, as a function of Δeq. The solid blue lines represent the full numerical calculations, while the red dashed–dotted line shows the fitted results using Equation (17). The black dotted lines indicate the maximum jet power at spin equilibrium, which is 2.2% of the accretion power ﹩\dot{m}{c}^{2}﹩, corresponding to ﹩{{\rm{\Delta }}}_{{\rm{eq}},{\rm{\max }}}=0.365﹩ and ﹩{a}_{{\rm{eq}},{\rm{\max }}}=0.5﹩. The maximum spin-equilibrium jet power is approximately 15 times greater than that at the MAD limit, which is 0.16% of the accretion power.
Paper: Maximal Jet Energy of Gamma-Ray Bursts through the Blandford–Znajek Mechanism
Authors: Zhao-Feng Wu, Michail Damoulakis, Paz Beniamini, Dimitrios Giannios
Figure caption: Probability distributions for flux ratio, Δeq = (ΦBH/ΦMAD)eq (left), and magnetic flux, ΦBH,eq (right), at spin equilibrium for lGRBs. The blue dashed, orange solid, and red dashed–dotted lines correspond to Macc = 0.2, 1, and 5 M⊙, respectively. As Macc increases, systems move further from the MAD state. Even at Macc = 0.2 M⊙, the peak of Δeq remains below ﹩{{\rm{\Delta }}}_{{\rm{eq}},{\rm{\max }}}﹩, consistent with the assumption that ﹩{{\rm{\Delta }}}_{{\rm{eq}}}\lt {{\rm{\Delta }}}_{{\rm{eq}},{\rm{\max }}}﹩ for all systems. The distributions of ΦBH,eq remain similar across Macc values since aeq ∼ 1 in systems far from MAD, and the magnetic flux just follows the observed luminosity distribution.
Paper: Maximal Jet Energy of Gamma-Ray Bursts through the Blandford–Znajek Mechanism
Authors: Zhao-Feng Wu, Michail Damoulakis, Paz Beniamini, Dimitrios Giannios
Figure caption: Mean collimation-corrected jet energy inferred from observations (X.-G. Wang et al. 2018) (black solid line). Dark cyan dashed and magenta dotted lines show the 1σ and 2σ confidence intervals, respectively. The blue solid line indicates the energy of the BOAT. If the BOAT were produced by a system in the MAD state, the required accreted mass would reach Macc ∼ 50 M⊙. In contrast, with the optimal flux ratio (﹩{{\rm{\Delta }}}_{{\rm{eq}}}={{\rm{\Delta }}}_{{\rm{eq}},{\rm{\max }}}﹩), Macc is reduced to ∼4 M⊙.
Paper: Maximal Jet Energy of Gamma-Ray Bursts through the Blandford–Znajek Mechanism
Authors: Zhao-Feng Wu, Michail Damoulakis, Paz Beniamini, Dimitrios Giannios
Figure caption: Probability distributions of magnetic flux threading the black hole, ΦBH, for sGRBs. The blue dashed, orange solid, and red dashed–dotted lines correspond to distributions of ﹩{\mathrm{log}}_{10}({E}_{{\rm{jet}}})﹩ following ﹩{ \mathcal N }(50,0.5)﹩, ﹩{ \mathcal N }(50,0.75)﹩, and ﹩{ \mathcal N }(49,0.5)﹩, respectively. The ΦBH distributions for sGRBs resemble those of lGRBs and remain largely insensitive to reasonable variations in the Ejet distribution, owing to their similar luminosity distributions and high black hole spin values during the bursts.
Paper: The Influence of Stellar Chromospheres and Coronae on Exoplanet Transmission Spectroscopy
Authors: Volker Perdelwitz, Adam Chaikin-Lifshitz, Aviv Ofir, Oded Aharonson
Figure caption: The geometry of the observation. Left: in perspective view, the chromospheric/coronal intensity falls off exponentially with radial distance r from the surface of the star. We integrate this quantity along chords parallel to the line of sight (for example, inside and outside the photospheric limb as dashed blue lines). Right: in the x − y plane perpendicular to the observer’s line of sight, the chromosphere is discretized, and the symmetry about the z-axis is used for efficient computation of the apparent intensity on the sky plane Ic(d), where d is the projected distance between the planet and star centers in this plane.
Paper: The Influence of Stellar Chromospheres and Coronae on Exoplanet Transmission Spectroscopy
Authors: Volker Perdelwitz, Adam Chaikin-Lifshitz, Aviv Ofir, Oded Aharonson
Figure caption: Depiction of the effect of chromospheres/coronae on transit shapes. We computed three scenarios of a stellar disk with a photosphere and an optically thin outer layer, with increasing brightness ratio Br (i.e., the ratio between the brightness of the chromosphere/corona and that of the photosphere) from 0 to 0.2 and unity. The lower panel shows the light curve of a planet transiting a star with the three brightness profiles displayed above, all assuming the planetary parameters of HAT-P-18 b. The solid section of each curve highlights the corresponding profile in the panel above.
Paper: The Influence of Stellar Chromospheres and Coronae on Exoplanet Transmission Spectroscopy
Authors: Volker Perdelwitz, Adam Chaikin-Lifshitz, Aviv Ofir, Oded Aharonson
Figure caption: Transmission spectra of HAT-P-18 b and POSEIDON fits, binned to a resolution of 100. The POSEIDON models (one active region) are plotted as solid lines, and 1σ errors are marked by the shaded regions. The lower panel shows the relative point-by-point difference between the transit depths of TACHELES and the photosphere (black dots) as well as that of the two POSEIDON fits (solid line).
Paper: The Influence of Stellar Chromospheres and Coronae on Exoplanet Transmission Spectroscopy
Authors: Volker Perdelwitz, Adam Chaikin-Lifshitz, Aviv Ofir, Oded Aharonson
Figure caption: Relative difference in transit depth derived for the TACHELES model radius (rp,TACH) and the photospheric model radius (rp,phot) as a function of the TACHELES brightness ratio. The color-coding denotes the Bayes factor.
Paper: The Influence of Stellar Chromospheres and Coronae on Exoplanet Transmission Spectroscopy
Authors: Volker Perdelwitz, Adam Chaikin-Lifshitz, Aviv Ofir, Oded Aharonson
Figure caption: Example of a wavelength bin exhibiting significant chromospheric/coronal emission (left column) and an adjacent nearly unaffected wavelength bin (right column). Top row: illustration of the best-fit TACHELES models. Second row: the observed light curve along with the resulting model fits. Third row: residuals from the traditional MA photospheric model fit, highlighting the difference between MA and TACHELES models. Bottom row: residuals from the TACHELES model.
Paper: SN 2023zaw: The Low-energy Explosion of an Ultrastripped Star
Authors: T. Moore, J. H. Gillanders, M. Nicholl, M. E. Huber, S. J. Smartt, S. Srivastav, H. F. Stevance, T.-W. Chen, K. C. Chambers, J. P. Anderson, M. D. Fulton, S. R. Oates, C. Angus, G. Pignata, N. Erasmus, H. Gao, J. Herman, C.-C. Lin, T. Lowe, E. A. Magnier, P. Minguez, C.-C. Ngeow, X. Sheng, S. A. Sim, K. W. Smith, R. Wainscoat, S. Yang, D. R. Young, K.-J. Zeng
Figure caption: Top: multicolor light curves with corrections for Milky Way foreground extinction and time dilation (for z = 0.010150) applied. Each telescope is shown with a different marker, and open markers indicate upper limits. We exclude Swift/UVOT nondetections for visual clarity. Additionally, we show the expected decline rate of a 56Co tail (0.98 mag/100 days; S. E. Woosley et al. 1989). This photometry is available as the data behind the figure. Bottom: a pseudobolometric (gcroizy-band) light curve of SN 2023zaw  compared to the model light curves from Section 3.3 integrated between the gcroizy-band observations. Model light curves are corrected for foreground extinction and the modeling-derived estimate of the host extinction.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: SN 2023zaw: The Low-energy Explosion of an Ultrastripped Star
Authors: T. Moore, J. H. Gillanders, M. Nicholl, M. E. Huber, S. J. Smartt, S. Srivastav, H. F. Stevance, T.-W. Chen, K. C. Chambers, J. P. Anderson, M. D. Fulton, S. R. Oates, C. Angus, G. Pignata, N. Erasmus, H. Gao, J. Herman, C.-C. Lin, T. Lowe, E. A. Magnier, P. Minguez, C.-C. Ngeow, X. Sheng, S. A. Sim, K. W. Smith, R. Wainscoat, S. Yang, D. R. Young, K.-J. Zeng
Figure caption: Results of the MOSFiT (J. Guillochon et al. 2018) model analysis for each physical model compared to the complete light curves, where downward-pointing arrows are upper limits, realizations are repented as solid lines, and band colors match those in Figure 1. Panel (a) shows nickel-only model realizations. Panels (c), (d), and (e) show the nickel + exp model (J. Guillochon et al. 2018), magnetar + nickel model (M. Nicholl et al. 2017), and circumstellar material interaction + nickel (V. A. Villar et al. 2017) model, respectively. Panel (b) shows a fit to only the late-time light curve to estimate a synthesized nickel mass, and panel (f) shows shock cooling emission + nickel, where the shock cooling treatment follows (A. L. Piro et al. 2021). The Bayesian evidence for each model is calculated for model comparison. When quoting the evidence for each model, the name of each model in the MOSFiT code is used to ensure the reproducibility of these results. Model evidence is not included in panel (b), as the model is only evaluated against the light-curve tail.
Paper: The Influence of Stellar Chromospheres and Coronae on Exoplanet Transmission Spectroscopy
Authors: Volker Perdelwitz, Adam Chaikin-Lifshitz, Aviv Ofir, Oded Aharonson
Figure caption: Results of the retrieval tests. (a) Accuracy of the brightness ratio as a function of SNR. Points with error bars denote the retrieved values and uncertainties for different actual values shown in colors. For each value of Br and SNR, multiple scale heights were tested, shown with small horizontal offsets. (b) Same as a but for the dependence of scale height retrievals on SNR, for different brightness ratios. (c) Scaling of parameter errors with SNR for example choices of Br = 0.32, H = 0.1, and rp = 0.135. The predicted convergence lines of α, rp, Br, and H are marked as dashed lines and annotated with simple expressions that predict well the relative errors in the parameters. We ran tests for SNR = 10{2,2.2,2.4,…,5}, Br = 10{−2,−1.5,−1,−0.5,0}, and H = 10{−2, −1.75, −1.5,…,0}.
Paper: The Influence of Stellar Chromospheres and Coronae on Exoplanet Transmission Spectroscopy
Authors: Volker Perdelwitz, Adam Chaikin-Lifshitz, Aviv Ofir, Oded Aharonson
Figure caption: Chromospheric/coronal emission spectrum of HAT-P-18 derived by multiplication of the TACHELES model brightness ratios with a PHOENIX photospheric spectrum. The solid blue line shows the spectrum smoothed to the instrumental resolution, along with the 1σ error region in light blue. Preliminary line identifications are written in black, and marginal/nondetection identifications of notable species are written in red.