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Paper: Spectropolarimetry of SN 2023ixf Reveals Both Circumstellar Material and an Aspherical Helium Core
Authors: Manisha Shrestha, Sabrina DeSoto, David J. Sand, G. Grant Williams, Jennifer L. Hoffman, Paul S. Smith, Callum McCall, Justyn R. Maund, Iain A. Steele, Klaas Wiersema, Jennifer E. Andrews, Nathan Smith, Christopher Bilinski, Peter Milne, Ramya M. Anche, K. Azalee Bostroem, Griffin Hosseinzadeh, Jeniveve Pearson, Douglas C. Leonard, Brian Hsu, Yize Dong, 一泽 董, Emily Hoang, Daryl Janzen, Jacob E. Jencson, Saurabh W. Jha, M. J. Lundquist, Darshana Mehta, Nicolás Meza Retamal, Stefano Valenti, Joseph Farah, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran
Figure caption: Relative flux (black) and polarization (red, binned to 20 Å) of SN 2023ixf in the region near Hα from our SPOL observation +14.50 days post-explosion. The comparison contrasts the P Cygni profile in the flux spectrum with the inverse P Cygni profile in polarization.
Paper: Spectropolarimetry of SN 2023ixf Reveals Both Circumstellar Material and an Aspherical Helium Core
Authors: Manisha Shrestha, Sabrina DeSoto, David J. Sand, G. Grant Williams, Jennifer L. Hoffman, Paul S. Smith, Callum McCall, Justyn R. Maund, Iain A. Steele, Klaas Wiersema, Jennifer E. Andrews, Nathan Smith, Christopher Bilinski, Peter Milne, Ramya M. Anche, K. Azalee Bostroem, Griffin Hosseinzadeh, Jeniveve Pearson, Douglas C. Leonard, Brian Hsu, Yize Dong, 一泽 董, Emily Hoang, Daryl Janzen, Jacob E. Jencson, Saurabh W. Jha, M. J. Lundquist, Darshana Mehta, Nicolás Meza Retamal, Stefano Valenti, Joseph Farah, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran
Figure caption: Evolution of the polarization level for various Type II SNe as a function of phase with respect to the fall from plateau (+81.50 days). For SN 2023ixf, different symbols signify data from different instruments: MOPTOP (circle), SPOL (square), and Kast (star; S. S. Vasylyev et al. 2023). Red, blue, and yellow points refer to SN 2004dj, SN 2012aw, and SN 2013ej from D. C. Leonard et al. (2006), L. Dessart et al. (2021), and T. Nagao et al. (2021), respectively.
Paper: A JWST Panchromatic Thermal Emission Spectrum of the Warm Neptune Archetype GJ 436b
Authors: Sagnick Mukherjee, Everett Schlawin, Taylor J. Bell, Jonathan J. Fortney, Thomas G. Beatty, Thomas P. Greene, Kazumasa Ohno, Matthew M. Murphy, Vivien Parmentier, Michael R. Line, Luis Welbanks, Lindsey S. Wiser, Marcia J. Rieke
Figure caption: Top: example broadband NIRCam light curves for observation 1185-14 (F322W2; top left) and Observation 1185-15 (F444W; top right) before and after detrending, as well as the residuals. In each time panel section, the data are plotted as blue points with error, and the model curve is plotted as an orange line for the raw light curve (top) and the detrended light curve (middle). The bottom panel section shows the residuals and a set of 60 equally spaced time bins (4.8 minutes apart). Bottom: broadband MIRI LRS light curve for Observation 1177-5.
Paper: A JWST Panchromatic Thermal Emission Spectrum of the Warm Neptune Archetype GJ 436b
Authors: Sagnick Mukherjee, Everett Schlawin, Taylor J. Bell, Jonathan J. Fortney, Thomas G. Beatty, Thomas P. Greene, Kazumasa Ohno, Matthew M. Murphy, Vivien Parmentier, Michael R. Line, Luis Welbanks, Lindsey S. Wiser, Marcia J. Rieke
Figure caption: The leftmost panel shows the T(P) profile obtained from the clear free chemistry retrieval with the solid blue line along with the 1σ and 2σ envelopes on the T(P) profile. The T(P) profile of the best-fit model from the clear equilibrium chemistry grid is shown with the green solid line. The T(P) profiles from the cloudy equilibrium chemistry grid and clear disequilibrium chemistry grid are shown with black solid and red dotted–dashed lines, respectively. The thermal contribution functions from each of these models at 4 μm are also shown on the left side of the panel. The second column shows the cloud optical depth per atmospheric layer as a function of pressure at 4 μm for the best-fit cloudy equilibrium chemistry model. The third column shows the cloud mass mixing ratio as a function of pressure for the KCl and Na2S cloud included in the cloudy best-fit model. The fourth column shows the mean cloud particle sizes in the best-fit model as a function of pressure for KCl and Na2S.
Paper: A JWST Panchromatic Thermal Emission Spectrum of the Warm Neptune Archetype GJ 436b
Authors: Sagnick Mukherjee, Everett Schlawin, Taylor J. Bell, Jonathan J. Fortney, Thomas G. Beatty, Thomas P. Greene, Kazumasa Ohno, Matthew M. Murphy, Vivien Parmentier, Michael R. Line, Luis Welbanks, Lindsey S. Wiser, Marcia J. Rieke
Figure caption: The top panel shows the comparison of the best-fit clear equilibrium chemistry grid model (green line), clear disequilibrium chemistry grid model (red line), and cloudy equilibrium chemistry grid model (black line) with the JWST spectrum of GJ 436b. The middle panel shows the residuals of the model fits divided by the errors in the data. Similar to Figure 2, the bottom left and bottom right panels show a zoomed-in version of the top panel with comparison of the best-fit grid models with parts of the spectrum observed with NIRCam and MIRI, respectively. The clear and cloudy equilibrium chemistry models are consistent with very elevated metallicities (≥500× solar and ≥300× solar at 1σ, respectively), whereas the disequilibrium chemistry models are consistent with metallicities higher than 80× solar.
Paper: A JWST Panchromatic Thermal Emission Spectrum of the Warm Neptune Archetype GJ 436b
Authors: Sagnick Mukherjee, Everett Schlawin, Taylor J. Bell, Jonathan J. Fortney, Thomas G. Beatty, Thomas P. Greene, Kazumasa Ohno, Matthew M. Murphy, Vivien Parmentier, Michael R. Line, Luis Welbanks, Lindsey S. Wiser, Marcia J. Rieke
Figure caption: The ratio of planets’ derived dayside effective/average brightness temperatures and equilibrium temperatures from their JWST emission spectroscopy or phase-curve measurements as a function of their equilibrium temperatures is shown. GJ 436b and GJ 1214b are the only two nonterrestrial planets where this ratio is less than or similar to 1. The gray points show the ratio for the sample of planets presented in D. Deming et al. (2023). These ratios are computed using the brightness temperature derived from their Spitzer 3.6 μm flux in D. Deming et al. (2023).
Paper: A JWST Panchromatic Thermal Emission Spectrum of the Warm Neptune Archetype GJ 436b
Authors: Sagnick Mukherjee, Everett Schlawin, Taylor J. Bell, Jonathan J. Fortney, Thomas G. Beatty, Thomas P. Greene, Kazumasa Ohno, Matthew M. Murphy, Vivien Parmentier, Michael R. Line, Luis Welbanks, Lindsey S. Wiser, Marcia J. Rieke
Figure caption: Allan variance plots of the broadband light curves of the eight observations analyzed by the tshirt pipeline (top left: F322W2; top right: F444W; bottom: LRS). Significant levels of noise enter at the 100 ppm level, requiring a GP to mitigate systematics and ensure consistency across independent eclipse observations. The dotted lines (“White Noise Scaling”) show the expectation for uncorrelated white noise, which follows 1/﹩\sqrt{N}﹩ statistics for N data points. The dashed line shows the light-curve residuals with the GP component removed (“Before de-trending”). The solid lines show the light-curve residuals with the GP applied (“GP de-trended”).
Paper: A JWST Panchromatic Thermal Emission Spectrum of the Warm Neptune Archetype GJ 436b
Authors: Sagnick Mukherjee, Everett Schlawin, Taylor J. Bell, Jonathan J. Fortney, Thomas G. Beatty, Thomas P. Greene, Kazumasa Ohno, Matthew M. Murphy, Vivien Parmentier, Michael R. Line, Luis Welbanks, Lindsey S. Wiser, Marcia J. Rieke
Figure caption: Lomb–Scargle periodograms of the broadband light curves of the eight observations analyzed by the tshirt pipeline (top left: F322W2; top right: F444W; bottom: LRS). There can sometimes be broad periodicities near 80 and 130 minutes, which are mitigated by the GP. The solid lines show the periodogram of residuals with the GP applied (“GP de-trended”). The solid lines show the periodogram of residuals without removing the GP correlated noise (“Before de-trending”).
Paper: A JWST Panchromatic Thermal Emission Spectrum of the Warm Neptune Archetype GJ 436b
Authors: Sagnick Mukherjee, Everett Schlawin, Taylor J. Bell, Jonathan J. Fortney, Thomas G. Beatty, Thomas P. Greene, Kazumasa Ohno, Matthew M. Murphy, Vivien Parmentier, Michael R. Line, Luis Welbanks, Lindsey S. Wiser, Marcia J. Rieke
Figure caption: The left panel shows the corner plot obtained by fitting the Spitzer photometry of GJ 436b from C. V. Morley et al. (2017) and A. A. Lanotte et al. (2014) with our clear disequilibrium chemistry model grid in blue. The corner plot obtained by fitting the JWST data with the same grid has been overplotted in red. The top right panel compares the Spitzer photometry with the best-fit disequilibrium chemistry model in blue and the best-fit model to the JWST data in red. The model photometry derived from each model has been shown with blue and red dashes as well. Note that the C/O plotted here is relative to the solar value, where the assumed solar value is 0.458.
Paper: A JWST Panchromatic Thermal Emission Spectrum of the Warm Neptune Archetype GJ 436b
Authors: Sagnick Mukherjee, Everett Schlawin, Taylor J. Bell, Jonathan J. Fortney, Thomas G. Beatty, Thomas P. Greene, Kazumasa Ohno, Matthew M. Murphy, Vivien Parmentier, Michael R. Line, Luis Welbanks, Lindsey S. Wiser, Marcia J. Rieke
Figure caption: Comparison of the transmission spectrum computed from the various best-fit self-consistent models from this work with the HST/WFC3 transmission spectrum observations of GJ 436b. Green and black lines show the clear and cloudy equilibrium chemistry models, respectively. The red line shows the best-fit clear disequilibrium chemistry model.
Paper: A JWST Panchromatic Thermal Emission Spectrum of the Warm Neptune Archetype GJ 436b
Authors: Sagnick Mukherjee, Everett Schlawin, Taylor J. Bell, Jonathan J. Fortney, Thomas G. Beatty, Thomas P. Greene, Kazumasa Ohno, Matthew M. Murphy, Vivien Parmentier, Michael R. Line, Luis Welbanks, Lindsey S. Wiser, Marcia J. Rieke
Figure caption: Individual eclipse observations with NIRCam as reduced by tshirt. The errors, inflated by the GP fit, give largely consistent spectra.
Paper: Black Hole Pulsars and Monster Shocks as Outcomes of Black Hole–Neutron Star Mergers
Authors: Yoonsoo Kim, Elias R. Most, Andrei M. Beloborodov, Bart Ripperda
Figure caption: Post-merger magnetosphere of the remnant BH, having settled down to a rotating split monopole. The physical quantities are shown in the xz plane. Left: fluid Lorentz factor γ. Right: ratio of the thermal pressure Pth to the rest-energy density ρc2. The black solid lines show the in-plane magnetic field lines. An equatorial current sheet is formed, at which the magnetic field lines in the upper and lower hemispheres reconnect, dissipating magnetic energy and causing a flux decay (balding) of the BH. The inner magnetosphere is driven to corotate with the BH due to frame dragging. As a result, the post-merger magnetosphere of an inclined model (e.g., θB = 30°; bottom panels) exhibits features similar to those of tilted pulsars (see also Figure 10). The spin axis of the BH is along ﹩\hat{z}﹩ in all models.
Paper: Black Hole Pulsars and Monster Shocks as Outcomes of Black Hole–Neutron Star Mergers
Authors: Yoonsoo Kim, Elias R. Most, Andrei M. Beloborodov, Bart Ripperda
Figure caption: A spacetime diagram of the approximate electric current ﹩\left|{j}^{\phi }\right|﹩ on a meridional arc ϕ = 0 at r = 2.4rg in three simulations with different initial inclinations of the NS magnetic dipole moment (θB = 0°, 30°, 60°), displaying the latitude of the post-merger magnetospheric BH current sheet. For the inclined models (θB = 30°, 60°), the periodic oscillation in the latitude represents the rotation of the inclined current sheet. The orbital current sheet of the NS in the inspiral phase is also visible for t − tmerger ≲ −2 ms, where tmerger indicates the merger time.
Paper: Black Hole Pulsars and Monster Shocks as Outcomes of Black Hole–Neutron Star Mergers
Authors: Yoonsoo Kim, Elias R. Most, Andrei M. Beloborodov, Bart Ripperda
Figure caption: Monster shocks launched from BH–NS mergers. Shown here are the Lorentz factor (left panels) and the radial spatial velocity (right panels) on the meridional (xz) plane. The dashed orange circles are light spheres with radius r = c(t − tmerger). Top: simulation snapshot from the aligned model (θB = 0°). A monster shock can be found near x ≃ 250 km, with its characteristic feature of a plasma moving radially inward (vr < 0) preceding the shockfront. Bottom: inclined model θB = 60°. A similar feature can be seen near x ≃ −400 km.
Paper: Black Hole Pulsars and Monster Shocks as Outcomes of Black Hole–Neutron Star Mergers
Authors: Yoonsoo Kim, Elias R. Most, Andrei M. Beloborodov, Bart Ripperda
Figure caption: Poloidal structure (cut in the yz plane) of the perturbed magnetosphere of the BH–NS binary 0.9 ms before the merger for the aligned (θB = 0°) model. Fast magnetosonic waves have toroidal electric fields Eϕ (left), and Alfvén waves have toroidal magnetic perturbations δBϕ (right). The streamlines show fluid velocity in the left panel and magnetic field lines in the right panel. The BH and NS are shown with black and blue circles, respectively.
Paper: Black Hole Pulsars and Monster Shocks as Outcomes of Black Hole–Neutron Star Mergers
Authors: Yoonsoo Kim, Elias R. Most, Andrei M. Beloborodov, Bart Ripperda
Figure caption: Angular velocity of magnetic field lines threading the apparent BH horizon for the θB = 0° simulation. Shown are the distributions of ΩF for each latitude and the stationary axisymmetric force-free solution ΩF ≃ ΩH/2 (red dashed line).
Paper: Black Hole Pulsars and Monster Shocks as Outcomes of Black Hole–Neutron Star Mergers
Authors: Yoonsoo Kim, Elias R. Most, Andrei M. Beloborodov, Bart Ripperda
Figure caption: Merger of the BH–NS binary in our simulations, where the NS is swallowed whole. The entire process shown in this figure happens in less than 1 ms.
Paper: Black Hole Pulsars and Monster Shocks as Outcomes of Black Hole–Neutron Star Mergers
Authors: Yoonsoo Kim, Elias R. Most, Andrei M. Beloborodov, Bart Ripperda
Figure caption: Time evolution of the current-sheet inclination angle χ for the θB = 30°, 60° models.
Paper: 3D MC. I. X-Ray Tomography Begins to Unravel the 3D Structure of a Molecular Cloud in our Galaxy’s Center
Authors: Samantha W. Brunker, Cara Battersby, Danya Alboslani, Maïca Clavel, Daniel L. Walker, Dani Lipman, H Perry Hatchfield, Régis Terrier
Figure caption: A comparison between each year of X-ray observations (colored contours) and consecutive H2CO integrated velocity slices (grayscale background) suggests a good match in the overall morphological structures. Each panel shown has the average velocity indicated at the bottom of the image. The contours for each year of X-ray observations were matched with an integrated H2CO image sequentially. By eye, we see relatively good agreement between the X-ray and molecular gas features, especially in the bottom three panels. Unsurprisingly, the sequential comparison between X-ray echoes and velocity slices is not perfect though we do see some strikingly good correlation for the small-scale structure in years 2013, 2015, and 2016 especially.
Paper: 3D MC. I. X-Ray Tomography Begins to Unravel the 3D Structure of a Molecular Cloud in our Galaxy’s Center
Authors: Samantha W. Brunker, Cara Battersby, Danya Alboslani, Maïca Clavel, Daniel L. Walker, Dani Lipman, H Perry Hatchfield, Régis Terrier
Figure caption: The column density calculated for each year of X-ray observations of the Sticks cloud. The contours shown for each year are the same ones plotted in the previous figures. We see a variety of dense cores throughout the cloud in the X-ray observations.
Paper: A JWST Panchromatic Thermal Emission Spectrum of the Warm Neptune Archetype GJ 436b
Authors: Sagnick Mukherjee, Everett Schlawin, Taylor J. Bell, Jonathan J. Fortney, Thomas G. Beatty, Thomas P. Greene, Kazumasa Ohno, Matthew M. Murphy, Vivien Parmentier, Michael R. Line, Luis Welbanks, Lindsey S. Wiser, Marcia J. Rieke
Figure caption: The top panel shows the panchromatic emission spectrum of GJ 436b observed with JWST using three instrument modes—NIRCam F322W2 (yellow points), NIRCam F444W (red points), and MIRI LRS (blue points). The NIRCam data shown here are from the tshirt reduction pipeline, and the MIRI LRS data are from the Eureka! pipeline. The panchromatic spectrum is obtained from the weighted average of individual visits for each instrument mode. The pink diamonds, black diamonds, and green crosses also show photometry of the planet observed with Spitzer and analyzed by K. B. Stevenson et al. (2010), C. V. Morley et al. (2017), and A. A. Lanotte et al. (2014), respectively. The bottom panel compares the Fp/Fs spectra derived from the JWST observations with two different data reduction pipelines—tshirt and Eureka!.
Paper: A JWST Panchromatic Thermal Emission Spectrum of the Warm Neptune Archetype GJ 436b
Authors: Sagnick Mukherjee, Everett Schlawin, Taylor J. Bell, Jonathan J. Fortney, Thomas G. Beatty, Thomas P. Greene, Kazumasa Ohno, Matthew M. Murphy, Vivien Parmentier, Michael R. Line, Luis Welbanks, Lindsey S. Wiser, Marcia J. Rieke
Figure caption: The top panel shows the median spectrum obtained from the isothermal retrieval with the red solid line compared with the JWST spectrum of the planet. The 1σ and 2σ envelopes on the model spectra are shown with dark-red and light-red shaded regions, respectively. The middle panel shows the residuals of the model fit divided by the errors in the data. The bottom panel shows the corner plot between Bond albedo (AB) and heat recirculation parameter (ϵ) obtained by fitting the dayside blackbody temperature constrained from the isothermal retrieval with the methodology described in N. B. Cowan & E. Agol (2011). The dashed lines show the median and 3σ constraints on each parameter.
Paper: A JWST Panchromatic Thermal Emission Spectrum of the Warm Neptune Archetype GJ 436b
Authors: Sagnick Mukherjee, Everett Schlawin, Taylor J. Bell, Jonathan J. Fortney, Thomas G. Beatty, Thomas P. Greene, Kazumasa Ohno, Matthew M. Murphy, Vivien Parmentier, Michael R. Line, Luis Welbanks, Lindsey S. Wiser, Marcia J. Rieke
Figure caption: The top panel shows the median spectral model obtained from the free chemistry retrieval with the solid blue line compared with the JWST observations. The 1σ and 2σ envelopes on the model spectra are shown with dark-blue and light-blue shaded regions, respectively. The middle panel shows the residuals of the model fit divided by the errors in the data. The bottom left and bottom right panels show a zoomed-in version of the top panel with comparison of the retrieved models with parts of the spectrum observed with NIRCam and MIRI, respectively.
Paper: Black Hole Pulsars and Monster Shocks as Outcomes of Black Hole–Neutron Star Mergers
Authors: Yoonsoo Kim, Elias R. Most, Andrei M. Beloborodov, Bart Ripperda
Figure caption: Top: total magnetic flux extracted on a spherical surface r = 2.4rg near the apparent horizon. The results from θB = 30° (cyan solid line) and θB = 60° (orange solid line) are lying almost on top of each other. Middle: the imaginary part of the (l, m) = (1, 1) mode of the Maxwell NP scalar ϕ2 extracted at r = 4.3rg. Bottom: the imaginary part of the (l, m) = (2, 2) mode of the NP scalar ψ4 extracted at r = 4.3rg. We only show the result from θB = 0°, since the result is almost identical for all simulations. Exponential decays with timescales 31rg c−1, 23rg c−1, and 13rg c−1 are indicated by the black dashed, blue dotted, and red dashed lines.
Paper: Black Hole Pulsars and Monster Shocks as Outcomes of Black Hole–Neutron Star Mergers
Authors: Yoonsoo Kim, Elias R. Most, Andrei M. Beloborodov, Bart Ripperda
Figure caption: Pulsar-like striped wind from the remnant BH at t − tmerger = 7.0 ms from the θB = 30° simulation. We show the toroidal magnetic field Bϕ with the magnetic field lines on the equatorial (xy) plane in both panels. The remnant BH is shown with a black circle and is spinning counterclockwise in this figure. In the right panel, we show the stagnation surface (ur = 0) with a black dashed line.
Paper: Black Hole Pulsars and Monster Shocks as Outcomes of Black Hole–Neutron Star Mergers
Authors: Yoonsoo Kim, Elias R. Most, Andrei M. Beloborodov, Bart Ripperda
Figure caption: The dissipation luminosity from a BH pulsar LD(t) computed with an analytic model developed in Section 4.5, normalized with LD,43 ≡ LD/(1043 erg s−1) and B*,13 ≡ B*/(1013 G). Due to the high (unphysical) numerical resistivity in our simulation, we construct the light curves using τΦ = 100rg c−1 (blue solid line) and τΦ = 500rg c−1 (orange solid line), consistent with the bounds from the high-resolution kinetic simulations of A. Bransgrove et al. (2021).
Paper: Black Hole Pulsars and Monster Shocks as Outcomes of Black Hole–Neutron Star Mergers
Authors: Yoonsoo Kim, Elias R. Most, Andrei M. Beloborodov, Bart Ripperda
Figure caption: The imaginary part of the Maxwell NP scalar ﹩{\phi }_{2}^{(l=1,m=1)}﹩, corresponding approximately to outgoing fast magnetosonic waves, on the vertical (xz) plane, normalized with the magnitude of the magnetic field for the aligned case θB = 0° at t − tmerger = 1.05 ms.
Paper: Black Hole Pulsars and Monster Shocks as Outcomes of Black Hole–Neutron Star Mergers
Authors: Yoonsoo Kim, Elias R. Most, Andrei M. Beloborodov, Bart Ripperda
Figure caption: Toroidal magnetic field of the striped wind ∣Bϕ(r)∣ on the equatorial plane along the ﹩\hat{x}﹩ axis. The alternating signs (polarities) of Bϕ with each stripe are denoted with different colors. The dashed line shows the fit with Equation (11).
Paper: Examining the Potential for Methyl Halide Accumulation and Detectability in Possible Hycean-type Atmospheres
Authors: Michaela Leung, Shang-Min Tsai, Edward W. Schwieterman, Daniel Angerhausen, Janina Hansen
Figure caption: Top: methyl halide opacities used in spectral simulations. Data sourced from the HITRAN database (I. E. Gordon et al. 2022). Middle: comparison of haze precursor molecules in Hycean atmospheres for a variety of methyl halide flux levels. These gases are investigated here because S.-M. Tsai et al. (2024) showed that that CO and C2H6 are highly responsive to DMS levels, with CO showing a large drop-off and C2H6 a large increase as the organosulfur gas level increases. However, this trend does not hold here due to the rates of methyl halide reformation consuming the methyl radical and preventing further downstream chemical impacts. This is especially apparent in the large drop in C2H6 levels between the “no methyl halide flux” case and the “Earth-like flux.” Bottom: comparison of average volume mixing ratios of methyl halide gases in Hycean-type atmospheres for the Sun and GJ 436, used here as a well-characterized test case for a relatively inactive M2 star like K2-18. The triangles show the GJ 436 stellar environment and circle markers the solar environment. The difference in accumulation level for CH3Cl is smaller in comparison to the other methyl halides because CH3Cl has less opacity in the near-UV and is less affected by the increased brightness of the Sun at these shorter wavelengths (see Figure 1). One part-per-million is shown with the black horizontal line as an approximate threshold for spectral relevance. Dashed yellow horizontal lines indicate mixing ratios reported for the most productive biological production flux scenario (1000x globally averaged) under modern Earth-like (O2-rich) bulk conditions in M. Leung et al. (2022) for CH3Cl and CH3Br. The same indicator for CH3I is from preliminary Earth-like photochemical simulations, provided here only as an estimate.