adsabs/AstroCLIMB huggingface dataset:
Paper: Outflow–Cloud Interaction as the Possible Origin of the Peculiar Radio Emission in the Tidal Disruption Event AT2018cqh
Authors: Lei Yang, Xinwen Shu, Guobin Mou, Yongquan Xue, Luming Sun, Fabao Zhang, Zhumao Zhang, Yibo Wang, Tao Wu, Ning Jiang, Hucheng Ding, Tinggui Wang
Figure caption: The evolution of the radius (left) and kinetic energy (right) as a function of time from our equipartition analysis, assuming a single outflow is launched into the CNM around the time of optical discovery. The blue and red filled circles indicate the parameters for a spherical homogeneous and a collimated conical outflow, respectively.
Paper: Outflow–Cloud Interaction as the Possible Origin of the Peculiar Radio Emission in the Tidal Disruption Event AT2018cqh
Authors: Lei Yang, Xinwen Shu, Guobin Mou, Yongquan Xue, Luming Sun, Fabao Zhang, Zhumao Zhang, Yibo Wang, Tao Wu, Ning Jiang, Hucheng Ding, Tinggui Wang
Figure caption: Natural-weighted images of VLBA observations of AT2018cqh at three frequencies. In each image, the bottom right ellipse is the shape of the restoring beam, with sizes of 14.51 × 5.29 mas for the L band, 3.20 × 1.30 mas for the C band, and 1.99 × 0.81 mas for the X band, respectively. The contour levels are 2.5σ × (−1, 1, 2, 4, 8) for the L band and 2.5σ × (−1, 1, 2, 4, 8, 16, 32, and 64) for the C band and X band.
Paper: Outflow–Cloud Interaction as the Possible Origin of the Peculiar Radio Emission in the Tidal Disruption Event AT2018cqh
Authors: Lei Yang, Xinwen Shu, Guobin Mou, Yongquan Xue, Luming Sun, Fabao Zhang, Zhumao Zhang, Yibo Wang, Tao Wu, Ning Jiang, Hucheng Ding, Tinggui Wang
Figure caption: Evolution for the outflow–cloud interaction. The panels from the left to the right show the density and CRe energy at three different epochs (observer’s frame): δt = 1246, 1730, and 2243 days.
Paper: Outflow–Cloud Interaction as the Possible Origin of the Peculiar Radio Emission in the Tidal Disruption Event AT2018cqh
Authors: Lei Yang, Xinwen Shu, Guobin Mou, Yongquan Xue, Luming Sun, Fabao Zhang, Zhumao Zhang, Yibo Wang, Tao Wu, Ning Jiang, Hucheng Ding, Tinggui Wang
Figure caption: Hydrodynamic modeling of the radio SEDs of  AT2018cqh. The cyan, orange, and red lines correspond to the model SEDs at δt = 1246, 1730, and 2243 days in the observer’s frame, respectively. The filled circles, stars, and diamonds represent the observed flux densities, as shown in Figure 3.
Paper: LAP1-B is the First Observed System Consistent with Theoretical Predictions for Population III Stars
Authors: Eli Visbal, Ryan Hazlett, Greg L. Bryan
Figure caption: Top panel: abundance of classical Pop III sources that have formed within the past 3 Myr. Middle panel: the mean Hα flux from these sources assuming a magnification of μ = 100. The horizontal dashed line corresponds to the 3σ uncertainty in K. Nakajima et al. (2025). Bottom panel: the predicted cumulative number of Pop III sources formed within 3 Myr at redshift from 5.9 to z within the area where galaxy cluster MACS J0416 has magnification μ > 30. The dashed vertical line corresponds to the redshift of z = 8 where the detection of the Hα line is at ∼3σ. The dotted vertical line indicates the redshift of LAP1-B, z = 6.6. The cumulative abundance at z = 6.6 is 0.88, consistent with the detection of LAP1-B.
Paper: Distinct Solar Energetic Particle Shock Intensity–Diffusion Coefficient Relationships in the Inner Heliosphere
Authors: M. E. Cuesta, F. Fraschetti, G. Livadiotis, H. A. Farooki, M. M. Shen, L. Y. Khoo, J. R. Szalay, J. S. Rankin, D. J. McComas, D. G. Mitchell, E. R. Christian, J. G. Mitchell, G. D. Berland, C. M. S. Cohen, R. A. Leske, Z. Xu, G. D. Muro, F. Pecora, D. Ruffolo, W. H. Matthaeus, J. Giacalone, N. A. Schwadron, M. I. Desai, M. A. Dayeh, S. D. Bale, M. L. Stevens, R. Livi
Figure caption: Radial profile of ﹩{\kappa }_{\parallel }{\cos }^{2}{\theta }_{{\rm{BN}}}﹩, κfit, jshock, αfit, and α∥ in descending order. The first three quantities are referenced for energetic protons at ∼80 keV.
Paper: LAP1-B is the First Observed System Consistent with Theoretical Predictions for Population III Stars
Authors: Eli Visbal, Ryan Hazlett, Greg L. Bryan
Figure caption: The total stellar mass of Pop III stars required to generate the Hα emission observed in LAP1-B as a function of the mass of each individual star (computed from Equation (1) assuming all stars are of the same mass). This value is calculated assuming fractional numbers of stars are allowed, which is unphysical, but shows that the ionizing efficiency saturates at stellar masses of ∼200 M⊙. Diagonal dashed lines indicate constant numbers of stars.
Paper: On the Formation of GW231123 in Population III Star Clusters
Authors: Shuai Liu, 帅 刘, Long Wang, 龙 王, Ataru Tanikawa, Weiwei Wu,  维 为 吴, Michiko S. Fujii
Figure caption: Distributions of the primary mass m1 and mass ratio q = m2/m1 for candidate progenitors of GW231123. The upper and lower panels show results from models of Pop III clusters with PBF = 0 and 1, respectively. Symbols indicate the formation channels of candidate progenitors. Circles and squares correspond to cases where both of m1 and m2 originate from stellar mergers (the massive components are PIBHs evolved from massive stars that underwent stellar mergers, thereby avoiding PI supernovae) and BBH mergers, respectively. Triangles represent mixed mergers, i.e., m1 and m2 are from stellar mergers and BBH mergers, respectively. Symbols filled with tan color denote candidate progenitors whose components are ejected from their host clusters due to kick velocities exceeding the clusters’ escape velocities. Colors indicate the total number of mergers contributing to the formation of candidate progenitors, defined as the sum of the mergers producing m1 and those producing m2 (n1 + n2), with red, blue, and green denoting 1, 2 and 3, respectively. Note that most m2 originate from the evolution of ordinary single stars in stellar merger and mixed merger channels, i.e., n2 = 0. The gray dot marks the median value of GW231123, with the error bar indicating the 90% probability intervals inferred from GW observations.
Paper: On the Formation of GW231123 in Population III Star Clusters
Authors: Shuai Liu, 帅 刘, Long Wang, 龙 王, Ataru Tanikawa, Weiwei Wu,  维 为 吴, Michiko S. Fujii
Figure caption: Peak frequency fpeak and the corresponding characteristic strain ﹩{h}_{{{\rm{cn}}}_{{\rm{peak}}}}﹩ of GWs emitted by candidate progenitors of GW231123 in all the models. The copper and winter color bars represent redshift z and eccentricities at peak fpeak = 0.01 Hz, respectively. Sensitivity curves of GW detectors LISA, Taiji, TianQin, DECIGO, CE, ET, LIGO, and KAGRA are represented by different colors and line styles.
Paper: On the Formation of GW231123 in Population III Star Clusters
Authors: Shuai Liu, 帅 刘, Long Wang, 龙 王, Ataru Tanikawa, Weiwei Wu,  维 为 吴, Michiko S. Fujii
Figure caption: Merger remnant mass mf and merger time tmerger of candidate progenitors of GW231123. The merger time tmerger refers to the moment during the evolution of Pop III star clusters, at which the mergers occur. Red and green circles represent the results from different models with PBF = 0 and 1, respectively.
Paper: On the Formation of GW231123 in Population III Star Clusters
Authors: Shuai Liu, 帅 刘, Long Wang, 龙 王, Ataru Tanikawa, Weiwei Wu,  维 为 吴, Michiko S. Fujii
Figure caption: The orbital element (eccentricity e and semimajor axis a) distributions of candidate progenitors of GW231123 at their formation time, defined as the moment BBHs emerge during binary star evolution. The red and green dots represent the results from different models with PBF = 0 and 1, respectively.
Paper: Not All Sub-Neptune Exoplanets Have Magma Oceans
Authors: Bodie Breza, Matthew C. Nixon, Eliza M.-R. Kempton
Figure caption: Mass–radius curves for a selection of model planets within the model grid. Each panel shows the effect of varying a given parameter on the mass–radius relationship and the presence (or absence) of a magma ocean. The purple line represents the minimum value of each parameter, and the yellow line represents the maximum. Intermediate colors represent evenly spaced values between the minimum and maximum, using either linear or log spacing according to Table 1. Other parameters are held constant at fixed fiducial values, denoted in the legend. Red triangles indicate model planets with magma oceans, while blue circles indicate a solid silicate layer at the boundary.
Paper: Not All Sub-Neptune Exoplanets Have Magma Oceans
Authors: Bodie Breza, Matthew C. Nixon, Eliza M.-R. Kempton
Figure caption: Pressure–temperature profiles of GJ 1214 b with different compositions (300× and 500× solar metallicity) and haze properties (maximally reflective hazes and tholin hazes), from M. C. Nixon et al. (2024). The profiles are overlaid on the phase diagram of MgSiO3, showing the solid–liquid and bridgmanite–postperovskite (Brg–PPv) boundaries. Circles indicate the pressure and temperature at the envelope–mantle boundary for each model. In all cases, the boundary occurs in the solid phase. The dotted orange line shows the best-fit isothermal-adiabatic profile (i.e., the parameterization used in this work) to the 300× solar, maximally reflective haze model.
Paper: The First Proper Motion Measurement of the Acceleration Regions in the Large-scale Jets of SS 433 Powering the W50 Nebula
Authors: Naomi Tsuji, Yoshiyuki Inoue, Dmitry Khangulyan, Kaya Mori, Samar Safi-Harb, Takaaki Tanaka, Laura Olivera-Nieto, Brydyn Mac Intyre, Kazuho Kayama, Takeshi Go Tsuru, Hiroyuki Uchida, Tatsuki Fujiwara, Felix Aharonian
Figure caption: Top: the new 0.5–7 keV Chandra image taken in 2023–2024 (e3 in 2019), with a spatial bin size of 2″. The white contours indicate the radio continuum radiation at 1.4 GHz (G. M. Dubner et al. 1998). Bottom: zoomed-in images of the X-ray knots and comparison of the archival and new data. The cyan dashed box indicates the region used to produce projection profiles in Figure 2, while the solid box shows the background region. The energy band is 0.5–7 keV, except 0.5–1.2 keV for the e3 knot. The pixel sizes of the Chandra and XMM-Newton images are 2″ and 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩5, respectively. The maps are shown in units of counts s−1 arcsec−2.
Paper: The First Proper Motion Measurement of the Acceleration Regions in the Large-scale Jets of SS 433 Powering the W50 Nebula
Authors: Naomi Tsuji, Yoshiyuki Inoue, Dmitry Khangulyan, Kaya Mori, Samar Safi-Harb, Takaaki Tanaka, Laura Olivera-Nieto, Brydyn Mac Intyre, Kazuho Kayama, Takeshi Go Tsuru, Hiroyuki Uchida, Tatsuki Fujiwara, Felix Aharonian
Figure caption: The relation between the shock velocity (﹩{v}_{{\rm{u}}}^{{\prime} }﹩) and the electron cutoff energy (E0) in Equation (4) with different values of the magnetic field. The colored diagonal lines indicate the Bohm-limit cases with B of 5, 12, 20, and 40 μG, and the arrows show the allowed parameter space with ηB > 1. The vertical lines denote the constrained values of ﹩{v}_{{\rm{u}}}^{{\prime} }﹩ for the e0 knot, assuming the constant-speed and expanding jet model (vd = 0.045c), the constant-speed and nonexpanding jet (vd = 0.061c), and the lower limit of vd = 0.021c (HESS Collaboration et al. 2024).
Paper: The First Proper Motion Measurement of the Acceleration Regions in the Large-scale Jets of SS 433 Powering the W50 Nebula
Authors: Naomi Tsuji, Yoshiyuki Inoue, Dmitry Khangulyan, Kaya Mori, Samar Safi-Harb, Takaaki Tanaka, Laura Olivera-Nieto, Brydyn Mac Intyre, Kazuho Kayama, Takeshi Go Tsuru, Hiroyuki Uchida, Tatsuki Fujiwara, Felix Aharonian
Figure caption: Left: the projection profiles, extracted from the regions shown in Figure 1. Right: the χ2 profiles, where the positive shift indicates a direction to the west.
Paper: The First Proper Motion Measurement of the Acceleration Regions in the Large-scale Jets of SS 433 Powering the W50 Nebula
Authors: Naomi Tsuji, Yoshiyuki Inoue, Dmitry Khangulyan, Kaya Mori, Samar Safi-Harb, Takaaki Tanaka, Laura Olivera-Nieto, Brydyn Mac Intyre, Kazuho Kayama, Takeshi Go Tsuru, Hiroyuki Uchida, Tatsuki Fujiwara, Felix Aharonian
Figure caption: The velocity profile in the SS 433/W50 system, assuming d = 5.5 kpc. The blue and light-blue error bars show the 90% and 3σ uncertainties, respectively. The positive velocity is defined as the direction toward the outer lobe away from SS 433 (i.e., the positive values of the eastern knots mean motions to the east, while the positive values of the western knots mean motions to the west). The velocities of the knots (e0–e3 and w1–w2) were measured by proper motion studies (this work, and H. Sakemi et al. 2021 for e3), while that of SS 433 was derived by the shift of line emission in the arcsec-scale X-ray jets (H. L. Marshall et al. 2002).
Paper: The First Proper Motion Measurement of the Acceleration Regions in the Large-scale Jets of SS 433 Powering the W50 Nebula
Authors: Naomi Tsuji, Yoshiyuki Inoue, Dmitry Khangulyan, Kaya Mori, Samar Safi-Harb, Takaaki Tanaka, Laura Olivera-Nieto, Brydyn Mac Intyre, Kazuho Kayama, Takeshi Go Tsuru, Hiroyuki Uchida, Tatsuki Fujiwara, Felix Aharonian
Figure caption: The constraints on the upstream velocity at the observer frame vu (left) and at the shock rest frame ﹩{v}_{{\rm{u}}}^{{\prime} }﹩ (right) as functions of vsh and vd (top: e0 and bottom: w1). The vertical solid and dashed lines show the 90% and 3σ uncertainties of vsh, respectively. The horizontal lines show the constraints on the downstream velocity, assuming decreasing speed profile and expanding jet (vd = 0.083c), constant speed and nonexpanding jet (0.061c), and constant speed and expanding jet (0.045c), and the lower and upper limits including the systematic uncertainties (0.021c and 0.12c) in HESS Collaboration et al. (2024). The region enclosed by the thick black line indicates the allowed parameter space.
Paper: H I Properties of Field Galaxies at z ≈ 0.2–0.6: Insights into Declining Cosmic Star Formation
Authors: David DePalma, Neeraj Gupta, Hsiao-Wen Chen, Robert A. Simcoe, Sergei Balashev, Erin Boettcher, Sebastiano Cantalupo, Mandy C. Chen, Françoise Combes, Claude-André Faucher-Giguère, Sean D. Johnson, Hans-Rainer Klöckner, Jens-Kristian Krogager, Jennifer I-Hsiu Li, Sebastián López, Pasquier Noterdaeme, Patrick Petitjean, Zhijie Qu, Gwen C. Rudie, Joop Schaye, Fakhri Zahedy
Figure caption: Summary of galaxy properties in the CUBS-MALS galaxy sample. The data points are color coded according to redshift, with galaxies at z < 0.44 shown in blue and higher-redshift galaxies in red. The redshift distribution of stellar mass is presented in the left panels. In the bottom panel, the blue and red lines indicate the corresponding redshift coverage of the L and UHF bands, respectively. Hatched regions demarcate bands of RFI. Except where truncated by RFI or the samples’ boundary, the bins in the histogram of redshifts in the top panel bridge multiples of Δz = 1/30. The dashed orange and solid green stairs represent the moving weighted median and weighted mean, respectively (see Section 3 for details), within each bin of redshift. The stellar mass vs. the observed g − r color is displayed in the middle panels with the g − r = 1.1 color threshold marked by a dashed line. In the histogram of stellar mass in the right panel, the bins span multiples of 0.2 dex. The CUBS-MALS galaxy sample spans a broad range in stellar mass, from ﹩\mathrm{log}\,{M}_{\mathrm{star}}/{M}_{\odot }\approx 8﹩ to ﹩\mathrm{log}\,{M}_{\mathrm{star}}/{M}_{\odot }\approx 11﹩, with a median of ﹩{\langle \mathrm{log}\,{M}_{\mathrm{star}}/{M}_{\odot }\rangle }_{\mathrm{med}}\approx 10﹩ and a wide range in redshift from z ≈ 0.24 to z ≈ 0.63 with a median of 〈 z〉med = 0.44. The observed g − r color correlates well with Mstar, but with a large scatter.
Paper: A Quest for Sulfur-bearing Refractory Species: Identification of CaS in the Interstellar Medium
Authors: A. Tasa-Chaveli, Á. Sánchez-Monge, A. Fuente, A. Ginsburg, H. S. P. Müller, T. Möller, P. Rivière-Marichalar, D. Navarro-Almaida, G. Esplugues, P. Schilke, M. Rodríguez-Baras, S. Thorwirth, L. Beitia-Antero
Figure caption: ALMA 1.5 mm continuum emission toward the G351.77−0.54 star-forming region. Crosses mark the positions of the millimeter continuum sources identified by H. Beuther et al. (2019). The synthesized beam of the image (beam ﹩\,=\,0\mathop{.}\limits{^{\prime\prime} }21\times 0\mathop{.}\limits{^{\prime\prime} }15﹩, PA  = ​​​​​​−86°; with an rms ≃ 0.32 mJy beam−1) is shown in the bottom-left corner. The spectra shown in Figures 2 and A1 have been extracted toward the peak position of G351.77-mm1, located at α(J2000)  =  17h26m42﹩\mathop{.}\limits^{{\rm{s}}}﹩533 and ﹩\delta ({\rm{J2000}})\,=\,-3{6}^{\circ }9^{\prime} 17.37^{\prime\prime} ﹩.
Paper: H I Properties of Field Galaxies at z ≈ 0.2–0.6: Insights into Declining Cosmic Star Formation
Authors: David DePalma, Neeraj Gupta, Hsiao-Wen Chen, Robert A. Simcoe, Sergei Balashev, Erin Boettcher, Sebastiano Cantalupo, Mandy C. Chen, Françoise Combes, Claude-André Faucher-Giguère, Sean D. Johnson, Hans-Rainer Klöckner, Jens-Kristian Krogager, Jennifer I-Hsiu Li, Sebastián López, Pasquier Noterdaeme, Patrick Petitjean, Zhijie Qu, Gwen C. Rudie, Joop Schaye, Fakhri Zahedy
Figure caption: Variation of mean H I mass with redshift (panel (a)) and galaxy stellar mass (panel (b)). Data points and vertical error bars mark the weighted mean H I mass measurements and the associated uncertainties, color coded according to redshift, following what is presented in Figure 1. The horizontal bars indicate the dispersion of each subsample. For comparison, the solid green curve in panel (a) shows the anticipated redshift evolution of neutral gas content inferred from the cosmic star formation rate density (P. Madau & M. Dickinson 2014, Equation (15)), assuming a Kennicutt–Schmidt relation (R. C. Kennicutt 1998, see Section 4.2 for details). The solid green line and the associated shaded band in panel (b) show the scaling relation and uncertainties from the combined MIGHTEE-H I+CHILES study by A. Bianchetti et al. (2025). The gray dashed lines mark fixed MH I/Mstar ratios to facilitate visual calibrations.
Paper: H I Properties of Field Galaxies at z ≈ 0.2–0.6: Insights into Declining Cosmic Star Formation
Authors: David DePalma, Neeraj Gupta, Hsiao-Wen Chen, Robert A. Simcoe, Sergei Balashev, Erin Boettcher, Sebastiano Cantalupo, Mandy C. Chen, Françoise Combes, Claude-André Faucher-Giguère, Sean D. Johnson, Hans-Rainer Klöckner, Jens-Kristian Krogager, Jennifer I-Hsiu Li, Sebastián López, Pasquier Noterdaeme, Patrick Petitjean, Zhijie Qu, Gwen C. Rudie, Joop Schaye, Fakhri Zahedy
Figure caption: Weighted mean (left) and weighted median (right) spectra of the H I 21 cm emission line extracted using a physical aperture of 300 kpc in diameter around CUBS-MALS galaxies at 0.24 < z < 0.63. The stacked spectra of CUBS galaxies are shown in thick green, while the reference spectra are shown in thin orange (see Section 3 for details). The gray band marks the rms fluctuations in the error spectrum. The signal associated with the full sample is presented in the top panel, where the signals extracted for individual subsamples are presented in the bottom four rows. The dotted vertical lines mark the velocity window for extracting the total H I mass for each sample. The 21 cm line is confidently detected in all samples with high-z galaxies displaying the strongest signal strength in both low- and high-mass galaxies (bottom two panels). The mean stacks for 150 and 450 kpc diameter apertures are shown in the Appendix.
Paper: H I Properties of Field Galaxies at z ≈ 0.2–0.6: Insights into Declining Cosmic Star Formation
Authors: David DePalma, Neeraj Gupta, Hsiao-Wen Chen, Robert A. Simcoe, Sergei Balashev, Erin Boettcher, Sebastiano Cantalupo, Mandy C. Chen, Françoise Combes, Claude-André Faucher-Giguère, Sean D. Johnson, Hans-Rainer Klöckner, Jens-Kristian Krogager, Jennifer I-Hsiu Li, Sebastián López, Pasquier Noterdaeme, Patrick Petitjean, Zhijie Qu, Gwen C. Rudie, Joop Schaye, Fakhri Zahedy
Figure caption: Cumulative mean H I mass with increasing aperture diameter. Doubling the extraction aperture diameter, from 150 to 300 kpc, increases the extracted total H I 21 cm line flux by more than a factor of 2, indicating a significant amount of neutral gas located beyond 75 kpc from the central galaxies, while further increasing the aperture diameter to 450 kpc results in a substantial increase in noise without a corresponding gain in signal (see also Figure A1).
Paper: H I Properties of Field Galaxies at z ≈ 0.2–0.6: Insights into Declining Cosmic Star Formation
Authors: David DePalma, Neeraj Gupta, Hsiao-Wen Chen, Robert A. Simcoe, Sergei Balashev, Erin Boettcher, Sebastiano Cantalupo, Mandy C. Chen, Françoise Combes, Claude-André Faucher-Giguère, Sean D. Johnson, Hans-Rainer Klöckner, Jens-Kristian Krogager, Jennifer I-Hsiu Li, Sebastián López, Pasquier Noterdaeme, Patrick Petitjean, Zhijie Qu, Gwen C. Rudie, Joop Schaye, Fakhri Zahedy
Figure caption: Redshift evolution of measured mean H I mass for apertures with diameters of 150 kpc (left) and 450 kpc (right). The remaining details are the same as in Figure 4.
Paper: H I Properties of Field Galaxies at z ≈ 0.2–0.6: Insights into Declining Cosmic Star Formation
Authors: David DePalma, Neeraj Gupta, Hsiao-Wen Chen, Robert A. Simcoe, Sergei Balashev, Erin Boettcher, Sebastiano Cantalupo, Mandy C. Chen, Françoise Combes, Claude-André Faucher-Giguère, Sean D. Johnson, Hans-Rainer Klöckner, Jens-Kristian Krogager, Jennifer I-Hsiu Li, Sebastián López, Pasquier Noterdaeme, Patrick Petitjean, Zhijie Qu, Gwen C. Rudie, Joop Schaye, Fakhri Zahedy
Figure caption: Weighted mean spectral stacks for apertures with diameters of 150 kpc (left) and 450 kpc (right). The remaining details are the same as in Figure 2.
Paper: A Quest for Sulfur-bearing Refractory Species: Identification of CaS in the Interstellar Medium
Authors: A. Tasa-Chaveli, Á. Sánchez-Monge, A. Fuente, A. Ginsburg, H. S. P. Müller, T. Möller, P. Rivière-Marichalar, D. Navarro-Almaida, G. Esplugues, P. Schilke, M. Rodríguez-Baras, S. Thorwirth, L. Beitia-Antero
Figure caption: Spectra toward G351.77-mm1, with the intensity in brightness temperature. ALMA observational data are shown in black. The synthetic spectrum including all identified molecular species (see Section 3) is shown in red, and with the intensity multiplied by a factor of −1. Each major panel corresponds to a spectral window (see Table 1), with the minor panels showing the residual spectra (observed minus synthetic). Frequencies of CaS and KS transitions are marked with vertical lines. Blue and green colored areas mark the zoomed-in frequency ranges around these transitions shown in Figure 2.