adsabs/AstroCLIMB huggingface dataset:
Paper: CMB/kSZ and Compton-y Maps from 2500 deg2 of SPT-SZ and Planck Survey Data
Authors: L. E. Bleem, T. M. Crawford, B. Ansarinejad, B. A. Benson, S. Bocquet, J. E. Carlstrom, C. L. Chang, R. Chown, A. T. Crites, T. de Haan, M. A. Dobbs, W. B. Everett, E. M. George, R. Gualtieri, N. W. Halverson, G. P. Holder, W. L. Holzapfel, J. D. Hrubes, L. Knox, A. T. Lee, D. Luong-Van, D. P. Marrone, J. J. McMahon, S. S. Meyer, M. Millea, L. M. Mocanu, J. J. Mohr, T. Natoli, Y. Omori, S. Padin, C. Pryke, S. Raghunathan, C. L. Reichardt, J. E. Ruhl, K. K. Schaffer, E. Shirokoff, Z. Staniszewski, A. A. Stark, J. D. Vieira, and R. Williamson
Figure caption: Left panel: minimum-variance Compton-y map for the SPT-SZ ra5h30dec-55 field constructed without correcting for large-scale dust emission. Right panel: the same field after correcting for this emission as discussed in Section 3.3. The maps are smoothed with a beam of FWHM = 5′ for display purposes.
Paper: CMB/kSZ and Compton-y Maps from 2500 deg2 of SPT-SZ and Planck Survey Data
Authors: L. E. Bleem, T. M. Crawford, B. Ansarinejad, B. A. Benson, S. Bocquet, J. E. Carlstrom, C. L. Chang, R. Chown, A. T. Crites, T. de Haan, M. A. Dobbs, W. B. Everett, E. M. George, R. Gualtieri, N. W. Halverson, G. P. Holder, W. L. Holzapfel, J. D. Hrubes, L. Knox, A. T. Lee, D. Luong-Van, D. P. Marrone, J. J. McMahon, S. S. Meyer, M. Millea, L. M. Mocanu, J. J. Mohr, T. Natoli, Y. Omori, S. Padin, C. Pryke, S. Raghunathan, C. L. Reichardt, J. E. Ruhl, K. K. Schaffer, E. Shirokoff, Z. Staniszewski, A. A. Stark, J. D. Vieira, and R. Williamson
Figure caption: Left panel: y-CIB cross-spectrum for different CIB covariance multiplier values (see text for details) relative to the y-CIB cross-spectrum for a y map made just from dividing a 150 GHz map by the tSZ factor for that frequency. Solid lines show results using band weights created assuming normal-depth SPT-SZ field noise; dashed lines show results using band weights created assuming “double-depth” SPT-SZ field noise. Right panel: y-CIB cross-spectrum ratio at ℓ = 1000 and ℓ = 4000 divided by the MDPL prediction for that ratio (see text for details) and total y-map rms as a function of CIB multiplier. As in the left panel, normal-depth and double-depth results are indicated with solid and dashed lines, respectively. (The single- and double-depth results for ℓ = 1000 are indistinguishable because that multipole range is dominated by Planck data.) From this plot it is clear that a significant reduction in spurious y-CIB correlation (caused by residual CIB in the synthesized y map) can be achieved with a small noise penalty.
Paper: CMB/kSZ and Compton-y Maps from 2500 deg2 of SPT-SZ and Planck Survey Data
Authors: L. E. Bleem, T. M. Crawford, B. Ansarinejad, B. A. Benson, S. Bocquet, J. E. Carlstrom, C. L. Chang, R. Chown, A. T. Crites, T. de Haan, M. A. Dobbs, W. B. Everett, E. M. George, R. Gualtieri, N. W. Halverson, G. P. Holder, W. L. Holzapfel, J. D. Hrubes, L. Knox, A. T. Lee, D. Luong-Van, D. P. Marrone, J. J. McMahon, S. S. Meyer, M. Millea, L. M. Mocanu, J. J. Mohr, T. Natoli, Y. Omori, S. Padin, C. Pryke, S. Raghunathan, C. L. Reichardt, J. E. Ruhl, K. K. Schaffer, E. Shirokoff, Z. Staniszewski, A. A. Stark, J. D. Vieira, and R. Williamson
Figure caption: Two examples of component maps provided in association with this work. (Top) tSZ-nulled CMB/kSZ map constructed using observations from the SPT-SZ survey and Planck HFI. (Bottom) Minimum-variance Compton-y map from the same. Both of these maps are smoothed here for display purposes; we provide minimum-variance map products at ﹩1\buildrel{\,\prime}\over{.} 25﹩ resolution and map products with other signals nulled at ﹩1\buildrel{\,\prime}\over{.} 75﹩ resolution in the data release.
Paper: CMB/kSZ and Compton-y Maps from 2500 deg2 of SPT-SZ and Planck Survey Data
Authors: L. E. Bleem, T. M. Crawford, B. Ansarinejad, B. A. Benson, S. Bocquet, J. E. Carlstrom, C. L. Chang, R. Chown, A. T. Crites, T. de Haan, M. A. Dobbs, W. B. Everett, E. M. George, R. Gualtieri, N. W. Halverson, G. P. Holder, W. L. Holzapfel, J. D. Hrubes, L. Knox, A. T. Lee, D. Luong-Van, D. P. Marrone, J. J. McMahon, S. S. Meyer, M. Millea, L. M. Mocanu, J. J. Mohr, T. Natoli, Y. Omori, S. Padin, C. Pryke, S. Raghunathan, C. L. Reichardt, J. E. Ruhl, K. K. Schaffer, E. Shirokoff, Z. Staniszewski, A. A. Stark, J. D. Vieira, and R. Williamson
Figure caption: Top panel: azimuthally averaged Compton-y profiles for ACO 3667 at z = 0.0556. Bottom panels: on the left is a cutout from the Planck Compton-y map (Planck Collaboration et al. 2016d) centered on the cluster. We make a similar cutout on the right from the minimum-variance Compton-y map presented in this work. The arcminute-scale circular decrements in this image are located at the locations of bright radio sources readily detected in SPT data, enabling us to mask these regions when measuring the cluster’s pressure profile.
Paper: CMB/kSZ and Compton-y Maps from 2500 deg2 of SPT-SZ and Planck Survey Data
Authors: L. E. Bleem, T. M. Crawford, B. Ansarinejad, B. A. Benson, S. Bocquet, J. E. Carlstrom, C. L. Chang, R. Chown, A. T. Crites, T. de Haan, M. A. Dobbs, W. B. Everett, E. M. George, R. Gualtieri, N. W. Halverson, G. P. Holder, W. L. Holzapfel, J. D. Hrubes, L. Knox, A. T. Lee, D. Luong-Van, D. P. Marrone, J. J. McMahon, S. S. Meyer, M. Millea, L. M. Mocanu, J. J. Mohr, T. Natoli, Y. Omori, S. Padin, C. Pryke, S. Raghunathan, C. L. Reichardt, J. E. Ruhl, K. K. Schaffer, E. Shirokoff, Z. Staniszewski, A. A. Stark, J. D. Vieira, and R. Williamson
Figure caption: Angular power spectra of selected output maps, with results from ACT+Planck (Madhavacheril et al. 2020) shown for comparison. The agreement between the three curves in the signal-dominated multipole region (ℓ ≲ 2200 for SPT and ACT D56, ℓ ≲ 1500 for ACT BN) provides a rough validation of both sets of data products. The differences in the noise-dominated multipole region are discussed in the text. Top left: power spectra of the minimum-variance y maps from this work and from the two different sky regions used in Madhavacheril et al. (2020). Top right: similar for the CMB-nulled y map. Bottom left: similar for the y-nulled CMB/kSZ map. Bottom right: predicted power spectra for the y-nulled CMB/kSZ map from SPT and the ACT D56 region, using noise levels reported in this work and Table 1 of Madhavacheril et al. (2020). To demonstrate the importance of high-frequency data and angular resolution in the component-separation process, curves for the ACT D56 noise levels are shown in the hypothetical scenario in which 220 GHz data (at the rough noise levels of the SPT data) are added and in which the resolution of the ACT data is improved (see text for details).
Paper: CMB/kSZ and Compton-y Maps from 2500 deg2 of SPT-SZ and Planck Survey Data
Authors: L. E. Bleem, T. M. Crawford, B. Ansarinejad, B. A. Benson, S. Bocquet, J. E. Carlstrom, C. L. Chang, R. Chown, A. T. Crites, T. de Haan, M. A. Dobbs, W. B. Everett, E. M. George, R. Gualtieri, N. W. Halverson, G. P. Holder, W. L. Holzapfel, J. D. Hrubes, L. Knox, A. T. Lee, D. Luong-Van, D. P. Marrone, J. J. McMahon, S. S. Meyer, M. Millea, L. M. Mocanu, J. J. Mohr, T. Natoli, Y. Omori, S. Padin, C. Pryke, S. Raghunathan, C. L. Reichardt, J. E. Ruhl, K. K. Schaffer, E. Shirokoff, Z. Staniszewski, A. A. Stark, J. D. Vieira, and R. Williamson
Figure caption: Power spectrum of the CMB-CIB-nulled y map. The data points show the measured power spectrum of the y map from the three-component analysis in this work. The power spectrum is estimated using independent halves of the data to avoid noise bias. Error bars are estimated using resampling of the values from the individual SPT-SZ fields. Lines show the expectation for power from various components in the y map, given the signal models used in the linear combination algorithm. These are calculated by multiplying the model power spectra at each band by the band weights for the CMB-CIB-nulled y map and summing. The blue and gray shaded areas indicate the possible effect of dust cleaning on the CIB (see text for details). The by-eye agreement between the solid black line (sum of all model components) and the data points indicates that the signal variance models are roughly representative of the true signals in the data.
Paper: The Preprocessing of Galaxies in the Early Stages of Cluster Formation in Abell 1882 at z = 0.139
Authors: Aparajita Sengupta, William C. Keel, Glenn Morrison, Rogier A. Windhorst, Neal Miller, and Brent Smith
Figure caption: The schematic diagram shows galaxy evolution in a Cluster vs. a SuperGroup environment. A SuperGroup has a shallower but wider effective dark matter potential (bottom) compared to that of a Cluster (top). The blue and red circles represent star-forming and non-star-forming galaxies, respectively. The green circles represent the transition state (“Green Valley”) galaxies between the two.
Paper: The Preprocessing of Galaxies in the Early Stages of Cluster Formation in Abell 1882 at z = 0.139
Authors: Aparajita Sengupta, William C. Keel, Glenn Morrison, Rogier A. Windhorst, Neal Miller, and Brent Smith
Figure caption: (a) Redshift histogram of SuperGroup A1882. (b) Line-of-sight velocity profiles of the A1882 galaxies. The red, blue, and green circles represent the line-of-sight velocities for the galaxies in Group 1, Group 2, and Group 3, from their respective centers. The orange crosses represent the line-of-sight velocities for the “swept-up” region. The brown open circles are the velocities of the filaments of galaxies. The blue dashed line shows a linear model fit with 95% CI. (c) Spectroscopic completeness for A1882 as a function of r-magnitude and the cluster-centric radius in megaparsecs.
Paper: The Preprocessing of Galaxies in the Early Stages of Cluster Formation in Abell 1882 at z = 0.139
Authors: Aparajita Sengupta, William C. Keel, Glenn Morrison, Rogier A. Windhorst, Neal Miller, and Brent Smith
Figure caption: (a) Correlation plot of the projected radial distance ﹩{ \mathcal R }﹩ from the adopted center of A1882, and the local galaxy density Σ of the galaxies. The yellow line represents the running mean of Σ. (b) Average densities of galaxies in the three groups, the “swept-up” region, the feeding filaments, and the “others” (see Section 3.1 and Table 4), respectively, with standard error (1σ) bars. The average densities of the galaxies within the three individual filaments are shown in gray.
Paper: The Preprocessing of Galaxies in the Early Stages of Cluster Formation in Abell 1882 at z = 0.139
Authors: Aparajita Sengupta, William C. Keel, Glenn Morrison, Rogier A. Windhorst, Neal Miller, and Brent Smith
Figure caption: The three major filaments detected by the Friends-Of-Friends algorithm are shown in red dots, aquamarine triangles, and yellow squares, and also indicated by the blue arrows. The green dots encircled in red represent the galaxy group members. The blue dots represent the “swept-up” region. The gray dots represent all of the galaxies categorized as “others.” The contours show a galaxy number density map. The dotted circles represent the areas covered by the various surveys used in the current work.
Paper: The Preprocessing of Galaxies in the Early Stages of Cluster Formation in Abell 1882 at z = 0.139
Authors: Aparajita Sengupta, William C. Keel, Glenn Morrison, Rogier A. Windhorst, Neal Miller, and Brent Smith
Figure caption: The optical galaxies overlaid with the galaxies detected in the NUV (blue dots) and the galaxies with Hα data (red crosses). The contours show a galaxy number density map.
Paper: The Preprocessing of Galaxies in the Early Stages of Cluster Formation in Abell 1882 at z = 0.139
Authors: Aparajita Sengupta, William C. Keel, Glenn Morrison, Rogier A. Windhorst, Neal Miller, and Brent Smith
Figure caption: A redshift-decl. slice of SuperGroup A1882 with redshift. The dimmer red circles represent galaxies that are further away from that vantage point (i.e., the fainter the dots, the larger the value of their R.A.).
Paper: The Preprocessing of Galaxies in the Early Stages of Cluster Formation in Abell 1882 at z = 0.139
Authors: Aparajita Sengupta, William C. Keel, Glenn Morrison, Rogier A. Windhorst, Neal Miller, and Brent Smith
Figure caption: (a) Correlation plot of the regions (defined in Section 4.1 and Table 5) and Σ in A1882.
Paper: The Preprocessing of Galaxies in the Early Stages of Cluster Formation in Abell 1882 at z = 0.139
Authors: Aparajita Sengupta, William C. Keel, Glenn Morrison, Rogier A. Windhorst, Neal Miller, and Brent Smith
Figure caption: (a) The u–r color–magnitude relation and (b) the NUV–r color–magnitude relation in A1882. The black dashed lines represent the 95% prediction interval (PI) for all of the galaxies in the sample set. The red and blue lines represent the best fits for the RS and the BC. The gray dots represent the galaxies in A1882 in the color–color diagram. The black circles are the Hα emitters. The gray dashed line in panel (b) shows the NUV magnitude limit (= −15.9) for A1882.
Paper: The Preprocessing of Galaxies in the Early Stages of Cluster Formation in Abell 1882 at z = 0.139
Authors: Aparajita Sengupta, William C. Keel, Glenn Morrison, Rogier A. Windhorst, Neal Miller, and Brent Smith
Figure caption: Histograms for the red, blue, and green galaxies, shown in red, blue, and green colors, respectively, in (a) u–r and (b) NUV–r colors. The RS, BC, and GV galaxies are represented by red, blue, and green colors, respectively, using the new classification based on the optical and UV colors, as well as Hα emissions.
Paper: The Preprocessing of Galaxies in the Early Stages of Cluster Formation in Abell 1882 at z = 0.139
Authors: Aparajita Sengupta, William C. Keel, Glenn Morrison, Rogier A. Windhorst, Neal Miller, and Brent Smith
Figure caption: (a) u–r color–mass relation and (b) NUV–r color–mass relation in A1882. The red, blue, and green dots represent the RS, BC, and GV galaxies, respectively. The black open circles represent the Hα emitters, all of which have been reclassified as blue galaxies. The black dashed lines represent the 95% PI for all of the galaxies in the sample. (c) The fraction of optical galaxies and (d) the fraction of UV galaxies for different mass ranges. The galaxy mass bins are defined in Section 3.3. The RS, BC, and GV galaxies are represented by red, blue, and green colors, respectively, using the new classification based on the optical and UV colors, as well as Hα emissions.
Paper: The Preprocessing of Galaxies in the Early Stages of Cluster Formation in Abell 1882 at z = 0.139
Authors: Aparajita Sengupta, William C. Keel, Glenn Morrison, Rogier A. Windhorst, Neal Miller, and Brent Smith
Figure caption: Fractional numbers of red, blue, and green galaxies in optical and UV colors as functions of their underlying structure, as described in Section 4.1 and Table 4 (top panels), and as functions of the regions described in Table 5 (bottom panels) in A1882. The fractional numbers of the optical and the NUV colors are shown in the left column and the right column, respectively. The RS, BC, and GV galaxies are represented by red, blue, and green colors, respectively, using the new classification based on the optical and UV colors, as well as Hα emissions.
Paper: The Preprocessing of Galaxies in the Early Stages of Cluster Formation in Abell 1882 at z = 0.139
Authors: Aparajita Sengupta, William C. Keel, Glenn Morrison, Rogier A. Windhorst, Neal Miller, and Brent Smith
Figure caption: Local galaxy density map of A1882 overlaid with the GV galaxies in the NUV (in green), with red highlighting the densest regions. The green galaxies with blue and orange dots indicate the galaxies that are optically blue and red, respectively. The plus signs in black indicate Hα-emitting galaxies. The gray dots indicate all of the galaxies in A1882. The gray circles indicate the galaxies within the filaments.
Paper: The Preprocessing of Galaxies in the Early Stages of Cluster Formation in Abell 1882 at z = 0.139
Authors: Aparajita Sengupta, William C. Keel, Glenn Morrison, Rogier A. Windhorst, Neal Miller, and Brent Smith
Figure caption: Smoothed histograms of the Dn4000 index for the red (shown in red), blue (shown in blue), and green galaxies (shown in green), in (a) optical colors and (b) NUV colors. The black dashed and dotted lines represent the modes of the entire population for each category. The black dotted line represents the Dn4000 index ∼1.5, which corresponds to a stellar population of 1 Gyr. The RS, BC, and GV galaxies are represented by the red, blue, and green colors, respectively, using the new classification based on the optical and UV colors, as well as Hα emissions.
Paper: The Preprocessing of Galaxies in the Early Stages of Cluster Formation in Abell 1882 at z = 0.139
Authors: Aparajita Sengupta, William C. Keel, Glenn Morrison, Rogier A. Windhorst, Neal Miller, and Brent Smith
Figure caption: Smoothed histograms of the Dn4000 index for different mass bins. The black histogram represents all of the galaxies. The black dashed and dotted lines represent the modes of the entire population in each category. The black dotted line represents the Dn4000 index ∼1.5, which corresponds to a stellar population of 1 Gyr. The galaxy mass bins are defined in Section 3.3.
Paper: The Preprocessing of Galaxies in the Early Stages of Cluster Formation in Abell 1882 at z = 0.139
Authors: Aparajita Sengupta, William C. Keel, Glenn Morrison, Rogier A. Windhorst, Neal Miller, and Brent Smith
Figure caption: Fractions of Hα-emitting (in blue) and non-Hα-emitting galaxies (in blue) for different mass ranges. The galaxy mass bins are defined in Section 3.3.
Paper: The Preprocessing of Galaxies in the Early Stages of Cluster Formation in Abell 1882 at z = 0.139
Authors: Aparajita Sengupta, William C. Keel, Glenn Morrison, Rogier A. Windhorst, Neal Miller, and Brent Smith
Figure caption: Top panels: the mean u–r color and NUV–r color, respectively, with standard error bars, for galaxies of all masses (in black), the high-mass galaxies (the large brown solid circles), the intermediate-mass galaxies (the smaller solid magenta circles), and the dwarf galaxies (the smallest solid blue circles) within the various underlying large-scale structures of A1882. The galaxy mass ranges are as defined in Section 3.3. Middle panels: the evolutions of the mean u–r color and NUV–r color with radial distance from the assumed core of A1882. Bottom panels: smoothed histograms of the color distributions in dwarf galaxies (cyan), intermediate-mass galaxies (magenta), and massive galaxies (brown). The dotted lines represent smoothed histograms of all of the galaxies for u–r color and NUV–r color, respectively. The RS, BC, and GV galaxies are represented by the red, blue, and green colors, respectively, using the new classification based on the optical and UV colors, as well as Hα emissions.
Paper: Autodifferentiable Spectrum Model for High-dispersion Characterization of Exoplanets and Brown Dwarfs
Authors: Hajime Kawahara, Yui Kawashima, Kento Masuda, Ian J. M. Crossfield, Erwan Pannier, and Dirk van den Bekerom
Figure caption: Spectrum fitting procedure using ExoJAX. The blue boxes are autodifferentiable modules using JAX. The yellow boxes indicate the model parameters of the atmosphere. In addition, the parameters from observations and instruments are also shown in the yellow boxes. The green boxes are the statistical quantities used in HMC–NUTS by NumPyro. The data required as external inputs are observational data and molecular databases (red boxes). The blue arrows indicate the direction of the forward modeling of the spectrum. HMC–NUTS uses the derivatives of the posterior (∝ prior × likelihood) by fitting parameters. The green arrows shows the propagation of the autogradient (Appendix D).
Paper: Autodifferentiable Spectrum Model for High-dispersion Characterization of Exoplanets and Brown Dwarfs
Authors: Hajime Kawahara, Yui Kawashima, Kento Masuda, Ian J. M. Crossfield, Erwan Pannier, and Dirk van den Bekerom
Figure caption: Examples of H(x, a) and its automatic differentiations computed by hjert in ExoJAX.
Paper: Autodifferentiable Spectrum Model for High-dispersion Characterization of Exoplanets and Brown Dwarfs
Authors: Hajime Kawahara, Yui Kawashima, Kento Masuda, Ian J. M. Crossfield, Erwan Pannier, and Dirk van den Bekerom
Figure caption: Comparison of the HITRAN CO cross section with Kawashima & Ikoma (2018) (Kawashima) and HELIOS-K 2.0. Here, Δν = 0.01 cm−1, T = 1000 K, and P = 10−3 bar. The bottom panel shows the fractional differences between ExoJAX and both Kawashima & Ikoma (2018) and HELIOS-K.
Paper: Autodifferentiable Spectrum Model for High-dispersion Characterization of Exoplanets and Brown Dwarfs
Authors: Hajime Kawahara, Yui Kawashima, Kento Masuda, Ian J. M. Crossfield, Erwan Pannier, and Dirk van den Bekerom
Figure caption: Computation time as a function of the number of the molecular lines. We used NVIDIA/DGX A100 for this benchmark test. The star and triangle symbols correspond to the direct LPF without data transfer to the GPU memory. Dashed lines with the same color indicate the cases with data transfer. The plus and cross are MODIT without data transfer.
Paper: Autodifferentiable Spectrum Model for High-dispersion Characterization of Exoplanets and Brown Dwarfs
Authors: Hajime Kawahara, Yui Kawashima, Kento Masuda, Ian J. M. Crossfield, Erwan Pannier, and Dirk van den Bekerom
Figure caption: Outward spectrum computed by ExoJAX (top panel) and its comparison with petitRADTRANS (bottom panel). The bottom panel shows the difference between ExoJAX and petitRADTRANS (i.e., ExoJAX − petitRADTRANS).
Paper: Autodifferentiable Spectrum Model for High-dispersion Characterization of Exoplanets and Brown Dwarfs
Authors: Hajime Kawahara, Yui Kawashima, Kento Masuda, Ian J. M. Crossfield, Erwan Pannier, and Dirk van den Bekerom
Figure caption: Spectrum of Luhman 16 A (detector 1) and the 90% credible interval by exojax (top). The blue and orange areas correspond to the case of the independent Gaussian noise (Case I) and that of the correlated noise using the Gaussian process (Case II). The bottom two panels show the residuals of the median of the predictions from the data for Cases I and II. The lines labeled A, B, and C are described in the text. A direct LPF was used to create this figure.
Paper: Autodifferentiable Spectrum Model for High-dispersion Characterization of Exoplanets and Brown Dwarfs
Authors: Hajime Kawahara, Yui Kawashima, Kento Masuda, Ian J. M. Crossfield, Erwan Pannier, and Dirk van den Bekerom
Figure caption: Corner plot of the posterior sampling. The posterior and marginal probability are shown by the colored contours and green lines (Direct LPF), or the thin black contours/lines (MODIT), respectively.
Paper: Autodifferentiable Spectrum Model for High-dispersion Characterization of Exoplanets and Brown Dwarfs
Authors: Hajime Kawahara, Yui Kawashima, Kento Masuda, Ian J. M. Crossfield, Erwan Pannier, and Dirk van den Bekerom
Figure caption: Line diagnostics using water (ExoMol POKAZATEL). Left: temperature dependence of line strength for three representative lines (A, B, and C). The shaded area corresponds to 1260–1340 K, which is approximately the range of the posterior of T0. Right: temperature equivalence of the lower state of water lines. The color indicates the logarithm of the line strength at 1300 K. The lines of A, B, and C are indicated by vertical lines.
Paper: Autodifferentiable Spectrum Model for High-dispersion Characterization of Exoplanets and Brown Dwarfs
Authors: Hajime Kawahara, Yui Kawashima, Kento Masuda, Ian J. M. Crossfield, Erwan Pannier, and Dirk van den Bekerom
Figure caption: Comparison of the CO cross section between HITEMP2019 and ExoMol/Li2015 (default: constant default values of αref = 0.07 and ﹩{n}_{\mathrm{texp}}=0.5﹩ in the definition file; .broad: broadening parameters in the “.broad” file). We assume T = 1300 K, P = 1 bar (Pair = 0.99 bar and Pself = 0.1 bar for HITEMP2019).