adsabs/AstroCLIMB huggingface dataset:
Paper: Analysis of the Full Spitzer Microlensing Sample. I. Dark Remnant Candidates and Gaia Predictions
Authors: Krzysztof A. Rybicki, Yossi Shvartzvald, Jennifer C. Yee, Sebastiano Calchi Novati, Eran O. Ofek, Ian A. Bond, Charles Beichman, Geoff Bryden, Sean Carey, Calen Henderson, Wei Zhu, Michael M. Fausnaugh, Benjamin Wibking, Andrzej Udalski, Radek Poleski, Przemek Mróz, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Jan Skowron, Krzysztof Ulaczyk, Patryk Iwanek, Marcin Wrona, Yoon-Hyun Ryu, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clement Ranc, Nicholas J. Rattenbury, Yuki K. Satoh, Takahiro Sumi, Daisuke Suzuki, Paul. J. Tristram, Aikaterini Vandorou, Hibiki Yama, Łukasz Wyrzykowski, Kornel Howil, Katarzyna Kruszyńska
Figure caption: Visualization of all the known information about the Gaia measurements, under the assumption of the photometric microlensing model and θ E = 0.91 mas (see Table 4), for the case of OGLE-2016-BLG-0293. Top panel: photometric model with marked Gaia measurements. Middle panel: absolute astrometric shift calculated based on the photometric model (gray line). The black arrows indicate how much the astrometric signal is “reduced” owing to the projection on the ﹩\widehat{{AL}}﹩ direction. Bottom panel: circles represent scanning angles of Gaia mission for this field. Dark-colored dashed lines show the direction of the astrometric shift vector  δ  ±180°, while light-colored dashed lines mark perpendicular directions. Gaia only provides measurements along the instantaneous scanning direction ﹩\widehat{{AL}}﹩. As a result, whenever the astrometric shift vector  δ  and ﹩\widehat{{AL}}﹩ are aligned or counteraligned (﹩| \cos \angle ({\boldsymbol{\delta }},\widehat{{AL}})| \approx 1﹩), the signal measured by Gaia is larger. This occurs when the points in the bottom panel are darker and situated closer to one of the dark lines. Indeed, one can see that darker points in the bottom panel correspond to shorter arrows in the middle panel, meaning that more astrometric signal is “available” for Gaia.
Paper: Analysis of the Full Spitzer Microlensing Sample. I. Dark Remnant Candidates and Gaia Predictions
Authors: Krzysztof A. Rybicki, Yossi Shvartzvald, Jennifer C. Yee, Sebastiano Calchi Novati, Eran O. Ofek, Ian A. Bond, Charles Beichman, Geoff Bryden, Sean Carey, Calen Henderson, Wei Zhu, Michael M. Fausnaugh, Benjamin Wibking, Andrzej Udalski, Radek Poleski, Przemek Mróz, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Jan Skowron, Krzysztof Ulaczyk, Patryk Iwanek, Marcin Wrona, Yoon-Hyun Ryu, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clement Ranc, Nicholas J. Rattenbury, Yuki K. Satoh, Takahiro Sumi, Daisuke Suzuki, Paul. J. Tristram, Aikaterini Vandorou, Hibiki Yama, Łukasz Wyrzykowski, Kornel Howil, Katarzyna Kruszyńska
Figure caption: Detectability of the astrometric microlensing in Gaia data for the selected subsample of long-timescale Spitzer events, plotted as a function of Einstein radius θ E. The Δχ 2 parameter is the difference between the null model and the best-fit astrometric microlensing model (see details in the text). Points represent expected θ E values for each event that were calculated in Section 3.17 and listed in Table 4. Thickened lines mark 1σ errors on θ E. We also simulated Gaia astrometric data for a wider range of Einstein radii—the detectability for θ E in the range from 0.1 to 5 mas is plotted with dashed lines.
Paper: Analysis of the Full Spitzer Microlensing Sample. I. Dark Remnant Candidates and Gaia Predictions
Authors: Krzysztof A. Rybicki, Yossi Shvartzvald, Jennifer C. Yee, Sebastiano Calchi Novati, Eran O. Ofek, Ian A. Bond, Charles Beichman, Geoff Bryden, Sean Carey, Calen Henderson, Wei Zhu, Michael M. Fausnaugh, Benjamin Wibking, Andrzej Udalski, Radek Poleski, Przemek Mróz, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Jan Skowron, Krzysztof Ulaczyk, Patryk Iwanek, Marcin Wrona, Yoon-Hyun Ryu, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clement Ranc, Nicholas J. Rattenbury, Yuki K. Satoh, Takahiro Sumi, Daisuke Suzuki, Paul. J. Tristram, Aikaterini Vandorou, Hibiki Yama, Łukasz Wyrzykowski, Kornel Howil, Katarzyna Kruszyńska
Figure caption: The cumulative plot of Δχ 2 of the astrometric 1D fit for the event OGLE-2016-BLG-0293 for an example realization of the Gaia data and θ E = 0.91 mas (see Table 4). Top panel: mock Gaia astrometry (gray points) of the centroid displacement during microlensing (proper motion and parallax not included here). The model used to generate the data is marked by the dashed line. Middle panel: residuals of the data and the model shown in the top panel. Bottom panel: cumulative Δχ 2, which is the difference between the null model and the astrometric microlensing model (see details in the text).
Paper: Tidal Spin-up of Subdwarf B Stars
Authors: Linhao Ma, 林昊 马, Jim Fuller
Figure caption: Left: the tidal torque calculated for a 0.47 M ⊙ sdB model with a companion of 0.4 M ⊙, when the central helium fraction is 60%, assuming the sdB is nonrotating. The thick lines show the total torque calculated by summing over contributions from individual tidally excited g-modes (thin lines). We also show the torque calculated from Zahn’s formalism for comparison. At short periods, the total tidal torque is dominated by resonance peaks from individual weakly damped g-modes, different from the power-law dependence on forcing period of Zahn’s formalism. However, on-resonance torques at short periods (thick dashed gray lines) may trigger nonlinear dissipation, and the real torques may not be as large as seen in the plot. At longer periods, g-modes are more efficiently damped, and the torque agrees better with Zahn’s model. Right: the mode eigenfunctions for an example weakly damped standing mode (blue line) and an example strongly damped mode (red line) in the left panel. The weakly damped mode has nodes in its eigenfunction, while the strongly damped mode efficiently damps near the surface.
Paper: Tidal Spin-up of Subdwarf B Stars
Authors: Linhao Ma, 林昊 马, Jim Fuller
Figure caption: The observed trend of tidal synchronization (defined by 0.8 ≤ Ωspin/Ωorb ≤ 1; shaded gray region) for short-period sdB binaries (crosses) vs. the calculation results from binary spin–orbit evolution (dots). The red, purple, and green crosses indicate rotational measurements from spectral line broadening, p-mode frequency splitting, and g-mode frequency splitting. The red and blue dots indicate the modeled sdB binaries with the 0.47 M ⊙ and the 0.37 M ⊙ sdB primary, respectively. All modeled binaries have a 0.4 M ⊙ companion and initial orbital periods ranging from 1 to 18 hr. For 0.47 M ⊙ sdB binaries, we see that all systems with orbital periods less than ∼0.2 day reach tidal synchronization, while for 0.37 M ⊙ sdB binaries, this synchronization period becomes ∼0.15 day due to weaker torques on these smaller sdBs. These results match the observed trends of sdB tidal synchronization. In addition, most systems with 0.3 day ≲ P orb ≲ 0.6 day are spun up to rotational periods of a few days, which also agrees with the observed period range of partially synchronized binaries.
Paper: Tidal Spin-up of Subdwarf B Stars
Authors: Linhao Ma, 林昊 马, Jim Fuller
Figure caption: Left: the magnitude of γ  α  J  α  C  α  (defined in the main text) for different sdB models. This quantity determines the tidal torque of each mode per unit tidal forcing strength, and we see that they are of similar orders of magnitude without clear dependence on the different stellar models. Hence, the physical torque should be roughly proportional to the tidal forcing strength, which scales as R 6. Note that sdB models with hydrogen masses greater than 10−3 M ⊙ have some unstable modes, and their tidal excitation cannot be treated with our current method. Right: stellar radii as a function of age for different sdB models. More massive systems with more hydrogen left in the envelope have larger radii, and the tidal torques are expected to be stronger based on the R 6 scaling.
Paper: Tidal Spin-up of Subdwarf B Stars
Authors: Linhao Ma, 林昊 马, Jim Fuller
Figure caption: The ratio between the tidal synchronization timescale ﹩{\bar{T}}_{\mathrm{sync}}﹩ and the sdB lifetime T EHB interpolated between different choices of companion masses and initial orbital periods. The blue regions show the parameter space where ﹩{\bar{T}}_{\mathrm{sync}}\lt {T}_{\mathrm{EHB}}﹩. The brackets on the y-axis indicate the typical companion masses for sdB+WD or sdB+dM systems (V. Schaffenroth et al. 2022). Left: the results for the 0.47 M ⊙ sdB model, with T EHB = 164 Myr. We see that for systems in orbits less than ∼0.15–0.22 day, the synchronization timescale is less than the stellar lifetime, meaning these systems are likely to be observed as tidally synchronized. The results have a weak dependence on companion masses. Right: the results for the 0.37 M ⊙ sdB model. The critical orbital period below which systems become synchronized now becomes ∼0.10–0.17 day.
Paper: Tidal Spin-up of Subdwarf B Stars
Authors: Linhao Ma, 林昊 马, Jim Fuller
Figure caption: Upper: the ratios between the lhs and rhs of Equations (A1), (A2), and (A4) for an example MESA snapshot, which should all be unity. We see that in the original stellar profile calculated from MESA, Equation (A4) is sometimes not satisfied, with the largest discrepancy happening at the convective core boundary with a density discontinuity. We fix the P, M  r , and ρ profiles by the method described in the Appendix, and the fixed profiles satisfy Equation (A4) better. Lower: the original and fixed P, M  r , ρ, and Γ1 profiles of the example MESA snapshot. The pressure, density, and enclosed mass are almost identical to original MESA profiles, so the change of stellar structure after the fixing process is negligible. Γ1 is different by a small amount in some regions of the star, which means that the energy processes in the fixed stellar model are in general not consistent.
Paper: Tidal Spin-up of Subdwarf B Stars
Authors: Linhao Ma, 林昊 马, Jim Fuller
Figure caption: A sketch of the physics of sdB tidal spin-up. Gravity waves, propagating in the radiative envelope, can be tidally excited by the gravity from the orbiting companion. In the hydrogen-rich outer envelope, the waves damp (either partially or fully) and deposit their angular momentum into the star, transferring angular momentum from the orbit to the stellar spin. The color scale shows the hydrogen fraction in the radiative envelope.
Paper: On the Origin of Quenched but Gas-rich Regions at Kiloparsec Scales in Nearby Galaxies
Authors: Tao Jing, Cheng Li
Figure caption: Left panel: the ﹩\mathrm{log}﹩ EW(Hα) vs. D  n (4000) diagram of our sample. Contour lines represent data percentages (10%, 40%, 70%, 90%, and 99%), while black dots indicate data outside the 99% contour line. GRQRs and GPQRs are denoted by green and red dots, respectively (same for the other two panels). The horizontal and vertical dashed lines represent EW(Hα) = 2 Å and D  n (4000) = 1.6 separately. Center panel: The EW(Hα) vs. absorption EW(Hδ  A ) diagram of our sample. The right-bottom corner is the poststarburst region, according to Y.-M. Chen et al. (2019). Right panel: The ﹩\mathrm{log}{{\rm{\Sigma }}}_{\mathrm{gas}}﹩ vs. D  n (4000) - ﹩\mathrm{log}﹩ EW(Hα) diagram of our sample. The horizontal dashed line represents the boundary between gas-rich and gas-poor regions at ﹩\mathrm{log}{{\rm{\Sigma }}}_{\mathrm{gas}}({M}_{\odot }{\mathrm{kpc}}^{-2})=7.3﹩. Spaxels on the right side of the vertical dashed line (D  n (4000) - ﹩\mathrm{log}﹩ EW(Hα) ﹩\gt 1.6-\mathrm{log}2\approx 1.3﹩) are considered as quenched spaxels, which would be found in the lower right side of the blue solid line in the left panel.
Paper: On the Origin of Quenched but Gas-rich Regions at Kiloparsec Scales in Nearby Galaxies
Authors: Tao Jing, Cheng Li
Figure caption: The Gini feature importance for selecting quenched regions (gray), GPQRs (red), and GRQRs (green) of each input property. The error bar shows 1σ uncertainty of importance, estimated by reselecting the sub-sample of nonquenched spaxels and resplitting the train/test set.
Paper: On the Origin of Quenched but Gas-rich Regions at Kiloparsec Scales in Nearby Galaxies
Authors: Tao Jing, Cheng Li
Figure caption: The correlation between D  n (4000)-﹩\mathrm{log}﹩ EW(Hα) and the properties with the top six highest Gini importance. The dashed horizontal line shows the criterion we used to select the quenched region in Figure 1. The meanings of contours and black dots are the same as in Figure 1. The gray contours in the top center panel show the joint distribution of mass-weighted age and D  n (4000)-﹩\mathrm{log}﹩ EW(Hα).
Paper: On the Origin of Quenched but Gas-rich Regions at Kiloparsec Scales in Nearby Galaxies
Authors: Tao Jing, Cheng Li
Figure caption: The figure displays the standard deviation of the residuals for the best combination with a given number of features (N comp.) in blue, while the standard deviation of residuals for other combinations is depicted as light-blue dots. The red line demonstrates the best, balanced accuracy of classifying the quenching state with a given N comp. The label 〈1〉 denotes Σ*, Σgas, E(B − V), and ﹩{\rm{R}}/\mathrm{Re};﹩ 〈2〉 represents Σ*, Σgas, ﹩\mathrm{log}{M}_{* }﹩, Σ1kpc, σ c; and 〈3〉 corresponds to Σ*, Σgas, N2Hα, ﹩\mathrm{log}{M}_{* }﹩, Σ1kpc, σ c.
Paper: On the Origin of Quenched but Gas-rich Regions at Kiloparsec Scales in Nearby Galaxies
Authors: Tao Jing, Cheng Li
Figure caption: Comparison of global properties among all MaNGA galaxies (background contour, the contour lines include 10%, 40%, 70%, and 90% data separately), galaxies in our sample (blue dots), the host galaxies of GRQRs (green ring) and the host galaxies of GPQRs (red dots). The distribution of MaNGA galaxies is corrected by galaxy weight. Each panel is a y-axis parameter vs. galaxy mass diagram. The y-axis parameters of these nine panels are color (NUV − r), logarithmic SFR, galaxy size, Sérsic index, Concentration (r 90/r 50), stellar mass surface density in central 1 kpc, T-type, B/T, and axial ratio (b/a), from left to right, and top to bottom. The subpanel on the right side of each panel is the probability density profile of the y-axis parameter. Note that for the host galaxies of GPQRs, the red dots cover the blue dots, which leads to these dots showing as red.
Paper: On the Origin of Quenched but Gas-rich Regions at Kiloparsec Scales in Nearby Galaxies
Authors: Tao Jing, Cheng Li
Figure caption: Each panel is a y-axis vs. ﹩\mathrm{log}{{\rm{\Sigma }}}_{* }﹩ diagram. The colors blue, green, yellow, and red correspond to the f  Q  intervals of 0.0–0.1, 0.1–0.5, 0.5–0.9, and 0.9–1.0 separately. The y-axes in the first row represent local parameters N2Hα, ﹩\mathrm{log}{{\rm{\Sigma }}}_{{gas}}﹩, E(B − V), and Z *, while the y-axes in the second row denote global parameters B/T, ﹩\mathrm{log}{{\rm{\Sigma }}}_{1\mathrm{kpc}}﹩, ﹩\mathrm{log}{\sigma }_{c}﹩, and ﹩\mathrm{log}{M}_{* }﹩. The meanings of black contours and dots are the same as in Figure 1. The mean value and 1σ scatter of GRQRs and GPQRs are shown as red and green circles with an error bar, separately. In the second panel of the first row, the contours of f gas are shown as black dashed lines.
Paper: On the Origin of Quenched but Gas-rich Regions at Kiloparsec Scales in Nearby Galaxies
Authors: Tao Jing, Cheng Li
Figure caption: The star formation scaling laws in our sample. From left to right, the three panels show rSK law and extend rSK law and rSFMS, separately. The meanings of green dots and red dots are the same as in Figure 1. The blue and black contours display the distribution of SF regions and all regions in our sample, with each line indicating specific data percentages (10%, 40%, 70%, 90%, and 99%). Additionally, blue and black dots mark data points outside the corresponding 99% contour line. The blue solid lines represent the best-fitted scaling law on the SF regions in our sample, while colorful dashed lines are scaling laws reported in the literature. Each relation has been converted to the G. Chabrier (2003) initial mass function case.
Paper: On the Origin of Quenched but Gas-rich Regions at Kiloparsec Scales in Nearby Galaxies
Authors: Tao Jing, Cheng Li
Figure caption: BPT diagnostics of our sample. We use the line ratios of central spaxels to trace the existence of AGN for MaNGA galaxies (background contour, the contour lines include 10%, 40%, 70%, and 90% data separately), galaxies in our sample (blue dots), the host galaxies of GRQRs (green ring) and the host galaxies of GPQRs (red dots). The distribution of MaNGA galaxies has been corrected by the galaxy weight. The center and right panels are the same as the left panels but for retired galaxies (central EW(Hα) < 3 Å) and SF galaxies (central EW(Hα) > 3 Å), separately.
Paper: On the Origin of Quenched but Gas-rich Regions at Kiloparsec Scales in Nearby Galaxies
Authors: Tao Jing, Cheng Li
Figure caption: The distance to scaling law vs. D  n (4000) - ﹩\mathrm{log}﹩ EW(Hα) diagram for all spaxels in our sample. From left to right, the three panels show the distance to rSK law and extend rSK law and rSFMS, separately. The meanings of contours and dots are the same as in Figure 2.
Paper: Up, Up, and Away: Winds and Dynamical Structure as a Function of Altitude in the Ultrahot Jupiter WASP-76b
Authors: Aurora Y. Kesseli, Hayley Beltz, Emily Rauscher, I. A. G. Snellen
Figure caption: Binary-mask CCF grids for the three different opacity bins from the combined two ESPRESSO data sets. The horizontal lines show the point of first contact/last during transit (opaque navy) and the point of full transit (transparent navy). White residuals indicate excess absorption at the line positions included in each separate binary mask. The grids have been shifted into the planet’s rest frame using the well-constrained planet velocity, and so without any atmospheric dynamics we would expect the signal from the planet to lie along the orange line at 0 km s−1. We have masked out a region around the host star’s rest velocity (diagonal gray stripe) that shows contamination from the Rossiter–McLaughlin effect. In each case we detect a clear signal from the planet with SNRs of 8.73, 7.04, and 5.64 for the strong, middle, and weak bins, respectively.
Paper: Up, Up, and Away: Winds and Dynamical Structure as a Function of Altitude in the Ultrahot Jupiter WASP-76b
Authors: Aurora Y. Kesseli, Hayley Beltz, Emily Rauscher, I. A. G. Snellen
Figure caption: LOS velocities including the effects of both winds and rotation during ingress, midtransit, and egress for the east and west limbs from the three different GCM models analyzed in this work. Contours of constant pressure (shown in black) correspond to the pressure levels for the medium and weak lines. The inner boundary corresponds to 1 bar and the inner black circle is not to scale. In this projection, the left half of each plot corresponds to the eastern terminator at each phase while the right half corresponds to the western terminator. The limbs are plotted in altitude space and are to scale, with the difference in atmospheric extent between the limbs due to changing scale heights resulting from different temperature structures. However, we note that these models did not include hydrogen dissociation, which can also alter predicted scale heights (X. Tan & T. D. Komacek 2019). The 3G model has the largest day–night temperature contrast and therefore shows the starkest limb extent contrast. The two classes of lines are probing different LOS velocities, which are dependent on the choice of magnetic prescription.
Paper: Up, Up, and Away: Winds and Dynamical Structure as a Function of Altitude in the Ultrahot Jupiter WASP-76b
Authors: Aurora Y. Kesseli, Hayley Beltz, Emily Rauscher, I. A. G. Snellen
Figure caption: The same binary-mask CCFs for the three different opacity bins (strong, middle, and weak Fe I lines) shown in Figure 3, now coadded across the full transit. We show our Gaussian fits to the CCFs with dotted lines and the central radial velocity of the Gaussian for each bin with dashed lines. We find that at each altitude the Fe I signal is blueshifted with respect to the planet’s rest frame and also see a significant trend where at higher altitudes (stronger lines) the Fe I signal is less blueshifted.
Paper: Up, Up, and Away: Winds and Dynamical Structure as a Function of Altitude in the Ultrahot Jupiter WASP-76b
Authors: Aurora Y. Kesseli, Hayley Beltz, Emily Rauscher, I. A. G. Snellen
Figure caption: Same plot as Figure 4, but now we have split each 1D CCF into two temporal bins, phases −0.04 to −0.02 (pink) and +0.02 to +0.04 (black), in order to assess the Fe I asymmetry at different altitudes. The dotted lines of the same color show the Gaussians that were fit to each CCF. The vertical dashed lines show the measured peak radial velocities of the Gaussians, and the shaded regions correspond to the 2σ uncertainties in the position of the peak. The radial velocities and uncertainties that are plotted here are all displayed in Table 1.
Paper: Up, Up, and Away: Winds and Dynamical Structure as a Function of Altitude in the Ultrahot Jupiter WASP-76b
Authors: Aurora Y. Kesseli, Hayley Beltz, Emily Rauscher, I. A. G. Snellen
Figure caption: Top: transmission contribution function, showing the altitude where different Fe lines primarily absorb in the atmosphere of WASP-76 b. Darker colors indicate higher importance of the specific wavelength and altitude in creating the final transmission spectrum, and demonstrates that the Fe line cores primarily absorb at pressures between 10−4 and 10−9 bars. The contribution function is calculated using the retrieved exoplanet parameters from S. Gandhi et al. (2023) and the atmospheric modeling code petitRADTRANS (see P. Mollière et al. 2019 for details). Bottom: Kurucz line list, showing the opacity of Fe I as a function of wavelength, at a pressure of 1 mbar and assuming a temperature of 2500 K. By comparing the two plots, one can see that the most opaque lines absorb high in the atmosphere, while the less opaque lines absorb lower in the atmosphere as photons will not reach the τ = 1 surface until lower depths. The bottom panel also marks which Fe lines are included in each opacity bin. The bin with the most opaque (strong) Fe lines are shown as blue crosses, the middle Fe lines are marked with purple crosses, and the Fe lines that are part of the weak altitude bin are marked with orange crosses.