adsabs/AstroCLIMB huggingface dataset:
Paper: Accretion Burst Echoes as Probes of Protostellar Environments and Episodic Mass Assembly
Authors: Logan Francis, Doug Johnstone, Jeong-Eun Lee, Gregory J. Herczeg, Feng Long, Steve Mairs, Carlos Contreras Peña, Gerald Moriarty-Schieven
Figure caption: Comparison of our fiducial EC 53 model light curves and the observations from the SMA and JCMT (850 μm). The models and observations are shown over the 2020 decay and 2021 outburst (top), and zoom in on the 2021 outburst (bottom). The model light curves are normalized to the minimum flux, while the data are normalized as in the lower panel of Figure 5.
Paper: Accretion Burst Echoes as Probes of Protostellar Environments and Episodic Mass Assembly
Authors: Logan Francis, Doug Johnstone, Jeong-Eun Lee, Gregory J. Herczeg, Feng Long, Steve Mairs, Carlos Contreras Peña, Gerald Moriarty-Schieven
Figure caption: Light curves for EC 53 as observed during the 2021 outburst by the SMA (large orange circles) and JCMT (small blue circles). The left-hand scale shows the SMA flux with our relative flux calibration applied (see Section 3.1). The right-hand scale shows the SMA and JCMT fluxes, normalized to the minimum observed flux of EC 53 on 2021 April 2 for the SMA and 2021 April 8 for the JCMT.
Paper: Accretion Burst Echoes as Probes of Protostellar Environments and Episodic Mass Assembly
Authors: Logan Francis, Doug Johnstone, Jeong-Eun Lee, Gregory J. Herczeg, Feng Long, Steve Mairs, Carlos Contreras Peña, Gerald Moriarty-Schieven
Figure caption: Lookback time contours over the domain used for our toy model envelope. The dashed red circle denotes the outer envelope edge, while the solid blue and orange lines show the radii of our model beams for JCMT 850 μm (3270 au) and SMA (654 au).
Paper: Accretion Burst Echoes as Probes of Protostellar Environments and Episodic Mass Assembly
Authors: Logan Francis, Doug Johnstone, Jeong-Eun Lee, Gregory J. Herczeg, Feng Long, Steve Mairs, Carlos Contreras Peña, Gerald Moriarty-Schieven
Figure caption: Fiducial EC 53 model luminosity function (top), envelope dust temperature at 100 au (center), and normalized model SMA and JCMT 850 μm light curves (bottom). The parameters of the model are presented in Table 5.
Paper: Accretion Burst Echoes as Probes of Protostellar Environments and Episodic Mass Assembly
Authors: Logan Francis, Doug Johnstone, Jeong-Eun Lee, Gregory J. Herczeg, Feng Long, Steve Mairs, Carlos Contreras Peña, Gerald Moriarty-Schieven
Figure caption: A subsection of the Serpens Main star-forming region monitored by JCMT at 850 μm, annotated to show the positions of the four variable protostars and four stable calibrator sources. The map combines all 81 epochs observed through 2022 March 14. The FWHM of the beam is shown by the white circle.
Paper: Accretion Burst Echoes as Probes of Protostellar Environments and Episodic Mass Assembly
Authors: Logan Francis, Doug Johnstone, Jeong-Eun Lee, Gregory J. Herczeg, Feng Long, Steve Mairs, Carlos Contreras Peña, Gerald Moriarty-Schieven
Figure caption: SMA relative calibration. Rescaling factors vs. date for each of the three YSO calibrators (colored triangles) and the mean relative flux scaling factor (black triangles). Top: Rx230. Bottom: Rx240.
Paper: Accretion Burst Echoes as Probes of Protostellar Environments and Episodic Mass Assembly
Authors: Logan Francis, Doug Johnstone, Jeong-Eun Lee, Gregory J. Herczeg, Feng Long, Steve Mairs, Carlos Contreras Peña, Gerald Moriarty-Schieven
Figure caption: ACA relative calibration. Rescaling factors vs. date for each of the three YSO calibrators (colored circles) and the mean relative flux scaling factor (black circles).
Paper: Tidal Wave Breaking in the Eccentric Lead-in to Mass Transfer and Common Envelope Phases
Authors: Morgan MacLeod, Michelle Vick, Abraham Loeb
Figure caption: Contours indicating the stellar surface (left panels) and mass distributions with respect to Lagrangian displacement ξ  r  (right panels). Through more distorted surface contours and larger ξ  r , we observe that closer tidal passages lead to larger amplitude tidal waves near the star’s surface. In the r  p  = 1.1 R 1 through r  p  = 1.7 cases, this wave breaks, and we see abrupt distortions of the wavelike profile of the surface contours. The weakest, r  p  = 1.9 R 1 case features a sufficiently small wave amplitude that it does not break, and the object’s surface retains its oscillatory motion. From the mass distributions, we see that the condition ∣k  r  ξ  r ∣ > 1 distinguishes the wave breaking cases from those that remain linear.
Paper: Tidal Wave Breaking in the Eccentric Lead-in to Mass Transfer and Common Envelope Phases
Authors: Morgan MacLeod, Michelle Vick, Abraham Loeb
Figure caption: The transformation of the spherical harmonic mode spectrum during the periapse passage due to wave breaking, in the r  p  = 1.3 R 1 case. The upper panel compares the mode spectrum to that predicted by linear theory. In the lead-in to periapse, the simulated mode spectrum mirrors the linear prediction. In the immediate aftermath the mode spectrum is transformed to a power law, similar to l −5/3, by wave breaking. In the lower panel, we see how, as the power in low-degree modes grows, wave breaking transforms the radial velocity field at r = R 1, extracting power from the coherent, wavelike motion and depositing it in higher-degree modes and turbulence.
Paper: Tidal Wave Breaking in the Eccentric Lead-in to Mass Transfer and Common Envelope Phases
Authors: Morgan MacLeod, Michelle Vick, Abraham Loeb
Figure caption: Wave breaking during a close periapse passage. These panels show slices through the equatorial plane. Top panels show gas density, center panels show velocity divergence, and lower panels show specific entropy. Contours in each panel are at ρ = 10−5, 10−4, and ﹩{10}^{-3}\,{M}_{1}/{R}_{1}^{3}﹩. The dashed line and cross marker indicate the orbital path and position of the perturbing object, respectively. In this case, the perturber passes at a periapse distance of 1.3 R 1, giving rise to a large amplitude tidal wave, which collapses on itself and breaks, forming shocks. These shocks are traced by purple regions of strong velocity convergence. Shocks increase the entropy of some of the initially isentropic stellar material.
Paper: Tidal Wave Breaking in the Eccentric Lead-in to Mass Transfer and Common Envelope Phases
Authors: Morgan MacLeod, Michelle Vick, Abraham Loeb
Figure caption: Structure of two model polytropic stars used in our simulations. The upper panel shows density, the middle shows the central enclosed mass, and the lower shows the radial wavenumber k  r  ≈ ω  α /c  s , adopting the frequency of the l = 2 fundamental mode. Both objects have a core mass of 0.1 M 1 enclosed within 0.1 R 1, surrounded by polytropic envelopes with structural indices of Γs = 1.35 and 5/3. The Γs = 1.35 case is more centrally concentrated, with less mass in its outer envelope while the Γs = 5/3 case is more homogeneous.
Paper: Tidal Wave Breaking in the Eccentric Lead-in to Mass Transfer and Common Envelope Phases
Authors: Morgan MacLeod, Michelle Vick, Abraham Loeb
Figure caption: Damping of oscillatory motions by dissipation into the turbulent atmosphere. While wave breaking during the periapse passage initially increases the specific entropy of the surface layer, the subsequent interaction of the primary l = 2 oscillatory mode in the interior with this overlying atmosphere drives the damping of the oscillation, and the development of a coherently rotating surface layer subject to spiral shock waves that propagates azimuthally with the l = 2 mode pattern speed.
Paper: Tidal Wave Breaking in the Eccentric Lead-in to Mass Transfer and Common Envelope Phases
Authors: Morgan MacLeod, Michelle Vick, Abraham Loeb
Figure caption: Exchange of angular momentum and energy in the encounter between the Γs = 1.35 star and a perturber at r  p  = 1.9 R 1—the weakest tidal encounter of our simulated cases. Our fiducial resolution and model parameters allow the exchange of energy and angular momentum to be accurately captured for dimensionless amplitudes ≳10−6.
Paper: A Clear View of a Cloudy Brown Dwarf Companion from High-resolution Spectroscopy
Authors: Jerry W. Xuan, Jason Wang, Jean-Baptiste Ruffio, Heather Knutson, Dimitri Mawet, Paul Mollière, Jared Kolecki, Arthur Vigan, Sagnick Mukherjee, Nicole Wallack, Ji Wang, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Marta Bryan, Benjamin Calvin, Sylvain Cetre, Mark Chun, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Katelyn Horstman, Julie Inglis, Nemanja Jovanovic, Ronald López, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Sam Ragland, Bin Ren, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Peter Wizinowich
Figure caption: Posterior distributions for five key parameters from HRS retrievals of HD 4747 B, using the EddySed cloud model (MgSiO3, “am” and “cd” in blue and red, respectively), and the clear model in purple. The titles on each histogram show the median and 68% credible interval for the baseline retrieval (MgSiO3, am). Regardless of the cloud model used, the results agree well between different fits for the RV, ﹩v\sin i﹩, C/O, [C/H] (discussed in Section 5.1), and quench pressure (discussed in Section 5.3).
Paper: A Clear View of a Cloudy Brown Dwarf Companion from High-resolution Spectroscopy
Authors: Jerry W. Xuan, Jason Wang, Jean-Baptiste Ruffio, Heather Knutson, Dimitri Mawet, Paul Mollière, Jared Kolecki, Arthur Vigan, Sagnick Mukherjee, Nicole Wallack, Ji Wang, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Marta Bryan, Benjamin Calvin, Sylvain Cetre, Mark Chun, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Katelyn Horstman, Julie Inglis, Nemanja Jovanovic, Ronald López, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Sam Ragland, Bin Ren, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Peter Wizinowich
Figure caption: The KPIC HRS used in this study are plotted in black, with error bars inflated to the best-fit value in gray. A sample full model is shown in teal (dashed), and consists of the companion model in orange (which has been RV shifted and broadened), and the stellar model in blue to model the speckle contribution. The companion model shown does not include tellurics to focus on molecular features, but tellurics are included in our fits. The residuals are shown as gray points.
Paper: A Clear View of a Cloudy Brown Dwarf Companion from High-resolution Spectroscopy
Authors: Jerry W. Xuan, Jason Wang, Jean-Baptiste Ruffio, Heather Knutson, Dimitri Mawet, Paul Mollière, Jared Kolecki, Arthur Vigan, Sagnick Mukherjee, Nicole Wallack, Ji Wang, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Marta Bryan, Benjamin Calvin, Sylvain Cetre, Mark Chun, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Katelyn Horstman, Julie Inglis, Nemanja Jovanovic, Ronald López, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Sam Ragland, Bin Ren, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Peter Wizinowich
Figure caption: Our extracted LRS of HD 4747 B from GPI and SPHERE are plotted in black circles and squares, respectively, and the published spectra for GPI is shown in gray dots from Crepp et al. (2018). Overplotted in color are spectra of a L9.5 dwarf and T0 dwarf from SPEX (Burgasser 2014), which show good agreement with our extracted spectra, demonstrating that HD 4747 B is consistent with a spectral type near the L/T transition.
Paper: A Clear View of a Cloudy Brown Dwarf Companion from High-resolution Spectroscopy
Authors: Jerry W. Xuan, Jason Wang, Jean-Baptiste Ruffio, Heather Knutson, Dimitri Mawet, Paul Mollière, Jared Kolecki, Arthur Vigan, Sagnick Mukherjee, Nicole Wallack, Ji Wang, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Marta Bryan, Benjamin Calvin, Sylvain Cetre, Mark Chun, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Katelyn Horstman, Julie Inglis, Nemanja Jovanovic, Ronald López, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Sam Ragland, Bin Ren, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Peter Wizinowich
Figure caption: Cross-correlation functions (CCFs) in blue show detections of CO and H2O using three spectral orders of the KPIC HRS. Gray lines represent CCFs of the background flux (from the slit) and speckle flux, whose standard deviations are used as estimates of the CCF noise. The vertical dashed lines at 15 km s−1 show the expected RV of the companion from its known orbit. The strong structure in the blue CCFs outside the peaks arise because we only fit single molecules here.
Paper: A Clear View of a Cloudy Brown Dwarf Companion from High-resolution Spectroscopy
Authors: Jerry W. Xuan, Jason Wang, Jean-Baptiste Ruffio, Heather Knutson, Dimitri Mawet, Paul Mollière, Jared Kolecki, Arthur Vigan, Sagnick Mukherjee, Nicole Wallack, Ji Wang, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Marta Bryan, Benjamin Calvin, Sylvain Cetre, Mark Chun, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Katelyn Horstman, Julie Inglis, Nemanja Jovanovic, Ronald López, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Sam Ragland, Bin Ren, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Peter Wizinowich
Figure caption: Retrieved C and O abundances (relative to solar) and C/O for HD 4747 B in blue. The titles on each histogram showing the median and 68% credible interval. The red points show the stellar values from Section 2.1. The [C/H] agrees well, [O/H] is consistent within 1σ between the companion and star, and C/O is consistent at the 2σ level.
Paper: Contribution of Spicules to Solar Coronal Emission
Authors: Shanwlee Sow Mondal, James A. Klimchuk, Aveek Sarkar
Figure caption: Radiative loss function and excess heating implemented to prevent cooling of plasma below T min. When the temperature of the loop is above T ch, the radiative loss is given by the CHIANTI radiative loss function Λ(T) (Equation (A1)). The only heating applied to the loop at these temperatures is the uniform background heating Q bg. The radiative cooling smoothly goes to zero as the temperature approaches T min from above. In the temperature range T min to T ch, depending on the plasma density and temperature, an additional heating is provided to the loop to balance the lost energy through radiative cooling. Below the temperature T min, an additional heating Q ch, proportional to nch 2, is applied to bring the plasma back T ch.
Paper: Contribution of Spicules to Solar Coronal Emission
Authors: Shanwlee Sow Mondal, James A. Klimchuk, Aveek Sarkar
Figure caption: Variation in the shock speeds as a function of the loop coordinates for an injection speed of 150 km s−1 and tip temperatures of 2, 1, and 0.02 MK.
Paper: Galactic Cosmic-Ray Propagation in the Inner Heliosphere: Improved Force-field Model
Authors: Jung-Tsung Li, 融宗 李, John F. Beacom, Annika H. G. Peter
Figure caption: Parallel diffusion coefficient of protons (left) and electrons (right) as a function of kinetic energy T for heliocentric distances between 0.1 and 1 au, spaced in intervals of 0.1 au. The open circles and upward-pointing triangles are derived from the actual and lower-limit values of the measurements of λ ∥ at the heliocentric distance of 1 au, respectively.
Paper: Galactic Cosmic-Ray Propagation in the Inner Heliosphere: Improved Force-field Model
Authors: Jung-Tsung Li, 融宗 李, John F. Beacom, Annika H. G. Peter
Figure caption: Parallel diffusion coefficient (left), κ ∥, and parallel mean free path (right), λ ∥, as a function of heliocentric distance r for various particle kinetic energies, T. The blue line in the right plot is where λ ∥ = r; above this line (approximately for T ≳ 33 GeV), the diffusion description of the cosmic-ray transport in the inner heliosphere is not strictly valid.
Paper: Galactic Cosmic-Ray Propagation in the Inner Heliosphere: Improved Force-field Model
Authors: Jung-Tsung Li, 融宗 李, John F. Beacom, Annika H. G. Peter
Figure caption: Predicted spectra of GCR protons (left) and electrons (right) at r = 0.1 au. The blue solid lines indicate our results. The red dashed lines indicate the rigidity-independent Φ model. The gray circles are the PAMELA proton and electron observations with the error bars denoting the combined statistical and systematic errors, and the black dashed–dotted lines showing their model spectra (Adriani et al. 2013, 2015). Inset: the percentage change of GCR intensity from 1–0.1 au.
Paper: Galactic Cosmic-Ray Propagation in the Inner Heliosphere: Improved Force-field Model
Authors: Jung-Tsung Li, 融宗 李, John F. Beacom, Annika H. G. Peter
Figure caption: Calculated growth of the rigidity-dependent Φ (solid lines) from 1 au to radii r between 0.1 and 0.9 au in steps of 0.1 au. As a comparison, we show the growth of the rigidity-independent Φ for r = 0.1 au (top dashed line) and r = 0.9 au (bottom dashed line).
Paper: Galactic Cosmic-Ray Propagation in the Inner Heliosphere: Improved Force-field Model
Authors: Jung-Tsung Li, 融宗 李, John F. Beacom, Annika H. G. Peter
Figure caption: Calculated differential radial gradients G  r,diff of GCR protons and electrons for T = [0.25, 0.7] GeV. Blue solid lines indicate our results for the standard QLT treatment. Red dashed lines indicate the rigidity-independent Φ model. The green datum is the measured G  r  of GCR protons of 2% ± 2.5% au−1 between 0.3 au and 1 au obtained from the Helios Experiment-6 (Marquardt & Heber 2019).
Paper: Galactic Cosmic-Ray Propagation in the Inner Heliosphere: Improved Force-field Model
Authors: Jung-Tsung Li, 融宗 李, John F. Beacom, Annika H. G. Peter
Figure caption: Predicted spectrum of GCR helium nuclei at 3 au. The blue solid line indicates our result. The red dashed line indicates the rigidity-independent Φ model. The gray circles are the PAMELA helium nuclei observations with the error bars denoting the combined statistical and systematic errors; the black dashed–dotted line is their model spectrum (Marcelli et al. 2020). Inset: the percentage change of the intensity of GCR helium nuclei from 1–3 au.
Paper: Galactic Cosmic-Ray Propagation in the Inner Heliosphere: Improved Force-field Model
Authors: Jung-Tsung Li, 融宗 李, John F. Beacom, Annika H. G. Peter
Figure caption: Calculated change in rigidity-dependent Φ per helium nucleon from 1 au to radii r between 1.5 and 5 au every 0.5 au. As a comparison, we show the decrease of rigidity-independent Φ for r = 1.5 au (top dotted line) and r = 5 au (bottom dotted line).
Paper: Galactic Cosmic-Ray Propagation in the Inner Heliosphere: Improved Force-field Model
Authors: Jung-Tsung Li, 融宗 李, John F. Beacom, Annika H. G. Peter
Figure caption: Parallel diffusion coefficient of GCR helium nuclei for heliocentric distances between 1 and 5 au in steps of 0.5 au.
Paper: Accretion Burst Echoes as Probes of Protostellar Environments and Episodic Mass Assembly
Authors: Logan Francis, Doug Johnstone, Jeong-Eun Lee, Gregory J. Herczeg, Feng Long, Steve Mairs, Carlos Contreras Peña, Gerald Moriarty-Schieven
Figure caption: Gallery of submillimeter continuum images for the ALMA ACA observations, produced by concatenating data from all epochs, with the relative calibration in Section 3.1 applied. The beam size is denoted by the black ellipse in the lower left corner.
Paper: Accretion Burst Echoes as Probes of Protostellar Environments and Episodic Mass Assembly
Authors: Logan Francis, Doug Johnstone, Jeong-Eun Lee, Gregory J. Herczeg, Feng Long, Steve Mairs, Carlos Contreras Peña, Gerald Moriarty-Schieven
Figure caption: Comparison of the responses of the fiducial EC 53 envelope model to Gaussian (left column), sigmoid (center column), and sine wave (right column) luminosity functions with various shapes. Top row: input luminosity function; middle row: normalized model SMA light curve; bottom row: normalized model JCMT light curve. For the Gaussian model, the maximum flux and the time during the decay when 20% of the maximum flux is reached are shown by the triangles and circles, respectively. For the sigmoid model, the circles mark the time when 80% of the maximum flux is reached, which is shown by the dotted line.
Paper: Accretion Burst Echoes as Probes of Protostellar Environments and Episodic Mass Assembly
Authors: Logan Francis, Doug Johnstone, Jeong-Eun Lee, Gregory J. Herczeg, Feng Long, Steve Mairs, Carlos Contreras Peña, Gerald Moriarty-Schieven
Figure caption: The same as Figure 13, but for the SMA observed targets.
Paper: Accretion Burst Echoes as Probes of Protostellar Environments and Episodic Mass Assembly
Authors: Logan Francis, Doug Johnstone, Jeong-Eun Lee, Gregory J. Herczeg, Feng Long, Steve Mairs, Carlos Contreras Peña, Gerald Moriarty-Schieven
Figure caption: The same as Figure 11, but for comparison of different observing properties with a Gaussian luminosity function. Top row: luminosity function profile; middle row: normalized light curve for a fixed wavelength and varying beam size θ; bottom row: normalized light curve for a fixed beam size and varying wavelength.
Paper: Accretion Burst Echoes as Probes of Protostellar Environments and Episodic Mass Assembly
Authors: Logan Francis, Doug Johnstone, Jeong-Eun Lee, Gregory J. Herczeg, Feng Long, Steve Mairs, Carlos Contreras Peña, Gerald Moriarty-Schieven
Figure caption: The same as Figure 9, but for a comparison of the luminosity function parameters; see Equation (8). Top row: maximum luminosity L max; bottom row: rise timescale τ rise.
Paper: A Clear View of a Cloudy Brown Dwarf Companion from High-resolution Spectroscopy
Authors: Jerry W. Xuan, Jason Wang, Jean-Baptiste Ruffio, Heather Knutson, Dimitri Mawet, Paul Mollière, Jared Kolecki, Arthur Vigan, Sagnick Mukherjee, Nicole Wallack, Ji Wang, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Charlotte Z. Bond, Marta Bryan, Benjamin Calvin, Sylvain Cetre, Mark Chun, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Katelyn Horstman, Julie Inglis, Nemanja Jovanovic, Ronald López, Emily C. Martin, Evan Morris, Jacklyn Pezzato, Sam Ragland, Bin Ren, Garreth Ruane, Ben Sappey, Tobias Schofield, Andrew Skemer, Taylor Venenciano, J. Kent Wallace, Peter Wizinowich
Figure caption: The P–T profiles from our HRS retrieval (left panel) and LRS retrieval (right panel) with the baseline cloud model (MgSiO3, am). In each panel, black lines show the best-fit profile and blue lines are 100 random draws from the posterior. We also show a cloudless Sonora P–T profile (Marley et al. 2021) with similar bulk properties as HD 4747 B in dotted gray. The condensation curves for MgSiO3 and Fe clouds are plotted as dashed lines. We also overplot the emission contribution function as contours, which show the fraction of flux (darker indicates higher fraction) a given pressure layer contributes to the total flux at a given wavelength (Mollière et al. 2019). Thus, these use the wavelength axes, and not the temperature axes. The HRS is sensitive to the continuum forming around a few bars and line cores, which form up to 10−2 bars. Over the same wavelength range of 2.29–2.49 μm, the LRS shows the continuum arises from ≈1–10 bars, consistent with the HRS.