adsabs/AstroCLIMB huggingface dataset:
Paper: XRISM/Resolve Reveals the Complex Iron Structure of NGC 7213: Evidence for Radial Stratification between Inner Disk and Broad-line Region
Authors: E. Kammoun, T. Kawamuro, K. Murakami, S. Bianchi, F. Nicastro, A. Luminari, E. Aydi, M. Eracleous, O. K. Adegoke, E. Bertola, P. G. Boorman, V. Braito, G. Bruni, A. Comastri, P. Condò, M. Dadina, T. Enoto, J. A. García, V. E. Gianolli, F. A. Harrison, G. Lanzuisi, M. Laurenti, A. Marinucci, G. Mastroserio, H. Matsumoto, G. Matt, G. Matzeu, R. Middei, E. Nardini, H. Noda, H. Odaka, S. Ogawa, F. Panessa, E. Piconcelli, C. Pinto, J. M. Piotrowska, G. Ponti, C. Ricci, R. Ricci, R. Serafinelli, F. Shi, D. Stern, A. Tanimoto, Y. Terashima, R. Tomaru, F. Tombesi, A. Tortosa, Y. Ueda, F. Ursini, C. Vignali, S. Yamada, S. Yamada
Figure caption: Best fit of the low-ionization Fe Kα, assuming two lines (a broad base and a narrow core) with q = 3 (solid blue line) and a single line with q = 2.1 (red dashed line). We show the data after subtracting the power law.
Paper: XRISM/Resolve Reveals the Complex Iron Structure of NGC 7213: Evidence for Radial Stratification between Inner Disk and Broad-line Region
Authors: E. Kammoun, T. Kawamuro, K. Murakami, S. Bianchi, F. Nicastro, A. Luminari, E. Aydi, M. Eracleous, O. K. Adegoke, E. Bertola, P. G. Boorman, V. Braito, G. Bruni, A. Comastri, P. Condò, M. Dadina, T. Enoto, J. A. García, V. E. Gianolli, F. A. Harrison, G. Lanzuisi, M. Laurenti, A. Marinucci, G. Mastroserio, H. Matsumoto, G. Matt, G. Matzeu, R. Middei, E. Nardini, H. Noda, H. Odaka, S. Ogawa, F. Panessa, E. Piconcelli, C. Pinto, J. M. Piotrowska, G. Ponti, C. Ricci, R. Ricci, R. Serafinelli, F. Shi, D. Stern, A. Tanimoto, Y. Terashima, R. Tomaru, F. Tombesi, A. Tortosa, Y. Ueda, F. Ursini, C. Vignali, S. Yamada, S. Yamada
Figure caption: The posterior distribution of the Fe XXV forbidden-to-resonant line ratio. The red solid and dashed lines correspond to the median and 90% confidence region.
Paper: Exciting Stellar Eccentricity in Gaia BH3 via a Hidden Black Hole Binary
Authors: Qingru Hu, 清茹 胡, Bin Liu, 彬 刘, Wei Zhu, 伟 祝
Figure caption: Valid initial configurations and the eccentricity of the outer binary at 13 Gyr. The enclosed region by the three conditions—stability (solid curve), resonance (dashed curve), and merger time (dotted and dashed–dotted curves, for two chosen ages)—indicates the initial BHB configurations that could potentially undergo apsidal precession resonance. Colored circles and squares represent the initial configurations used in our numerical integrations, with face colors corresponding to the eccentricity of the outer binary at 13 Gyr. Circles denote systems that have not merged after 13 Gyr, whereas squares represent those that have merged. Initial parameters of inner BHBs consistent with the observations after 13 Gyr of evolution are highlighted with black open circles. The black plus symbol marks the example system whose time evolution is shown in Figure 2.
Paper: Exciting Stellar Eccentricity in Gaia BH3 via a Hidden Black Hole Binary
Authors: Qingru Hu, 清茹 胡, Bin Liu, 彬 刘, Wei Zhu, 伟 祝
Figure caption: The black open circles indicate the present orbital parameters ain and ein of inner BHBs that are able to reproduce the observed eccentricity of the stellar orbit in Gaia BH3 and remain stable at the end of the integration. The green-filled circle highlights the final state of the example system, whose time evolution is shown in Figure 2. The red contours show the semiamplitude of short-term RV oscillations (Equation (6)) due to the orbital motion of the inner BHB, and the blue contours show the expected apsidal precession rate of the stellar orbit (Equation (3)). The gray-shaded region indicates the unstable region of a coplanar triple with eout = 0.73 according to Equation (5).
Paper: Exciting Stellar Eccentricity in Gaia BH3 via a Hidden Black Hole Binary
Authors: Qingru Hu, 清茹 胡, Bin Liu, 彬 刘, Wei Zhu, 伟 祝
Figure caption: Time evolution of the semimajor axes a, eccentricities e and apsidal precession rates ﹩\dot{\varpi }﹩ of inner and outer binaries. This system is initialized with ain,0 = 1.25 au, ein,0 = 0.97, and ϖin = ϖout = 0°, as highlighted by the black plus symbol in Figure 1. The red (inner) and blue (outer) curves represent the numerical solutions of the double-averaged secular equations as detailed in B. Liu et al. (2015b).
Paper: Exciting Stellar Eccentricity in Gaia BH3 via a Hidden Black Hole Binary
Authors: Qingru Hu, 清茹 胡, Bin Liu, 彬 刘, Wei Zhu, 伟 祝
Figure caption: Time evolution of the outer eccentricity in misaligned triples with various mutual inclination angles (imut). The systems are initialized with ain,0 = 1.29 au, ein,0 = 0.97, Ωin = Ωout = 0°, ωin = 0°, and ωout = 180°, similar to that in Figure 2, except for the mutual inclination, which now varies from 0° to 60°. The black dashed line marks the observed value of the stellar eccentricity (eobs ≈ 0.73).
Paper: Exciting Stellar Eccentricity in Gaia BH3 via a Hidden Black Hole Binary
Authors: Qingru Hu, 清茹 胡, Bin Liu, 彬 刘, Wei Zhu, 伟 祝
Figure caption: Similar to Figure 1, but for three different BH systems (HD 130298, Gaia BH1, and Gaia BH2) based on relevant parameters as detailed in Section 4.2.
Paper: Exciting Stellar Eccentricity in Gaia BH3 via a Hidden Black Hole Binary
Authors: Qingru Hu, 清茹 胡, Bin Liu, 彬 刘, Wei Zhu, 伟 祝
Figure caption: Similar to Figure 1, but for three different mass ratios (q = 0.2, 0.4, and 0.6).
Paper: Strontium-84 Enrichments in Presolar Grains Provide First Evidence of p-process Nucleosynthesis in Core-collapse Supernovae
Authors: Ishita Pal, Manavi Jadhav, Danielle Z. Shulaker, Michael R. Savina, Marco Pignatari, Lorenzo Roberti, Heather Bouillion, Maria Lugaro, Christopher J. Dory, Frank Gyngard, Noriko Kita, Sachiko Amari
Figure caption: Comparison of subgrain data with results from the mixing model. Strontium isotopic ratios versus atomic masses of Sr isotopes for the five subgrains with 84Sr excesses (black) are shown in each subplot, along with the results from our two-layer mixing model. Uncertainties are 1σ. We show the best-fit mixing results from three different CCSNe models: RAU15, RIT15, and RIT20 (T. Rauscher et al. 2002; C. Ritter et al. 2018) plotted in red, blue, and orange, respectively. The proportions (in percentages) of the single layers within the specific zones (as defined in Figure 2) that were mixed together are specified for each mixing result. In all cases, the 84Sr anomalies can be reproduced by mixing small amounts of material from the O/Si zone to the C-rich material of the He/C zone of 15 M☉ CCSN models by T. Rauscher et al. (2002) and 15 M☉ and 20 M☉ models by C. Ritter et al. (2018) See Table A1 for the exact, model-specific, single-layer numbers used in these mixing calculations.
Paper: Strontium-84 Enrichments in Presolar Grains Provide First Evidence of p-process Nucleosynthesis in Core-collapse Supernovae
Authors: Ishita Pal, Manavi Jadhav, Danielle Z. Shulaker, Michael R. Savina, Marco Pignatari, Lorenzo Roberti, Heather Bouillion, Maria Lugaro, Christopher J. Dory, Frank Gyngard, Noriko Kita, Sachiko Amari
Figure caption: Isotopic abundance profiles in CCSNe. Isotopic abundance profiles of 15 M☉ models from RAU15 (top; T. Rauscher et al. 2002) and RIT15 (bottom; C. Ritter et al. 2018). The isotopic abundances of 4He, 12C, 14N, 16O, 20Ne, and 28Si are used to assign model layers into zones and are shown in solid thin lines with colors as indicated in the legend. Vertical dashed lines demarcate the stellar zones based on the two most abundant elements in each zone (B. S. Meyer et al. 1995). Isotopic abundances of 84,86,87,88Sr are plotted with thick purple lines. The two shaded regions in the He/C zones and O/Si zones highlight the regions that can mix to reproduce the observed 84Sr anomalies, according to our mixing calculations. To reproduce the isotopic patterns of the grains with 84Sr excesses, we have mixed single layers from the two shaded areas highlighted in the He/C and O/Si zones of the stellar models. Figure 3 shows best-case mixing proportions of these layers for each anomalous subgrain.
Paper: Strontium-84 Enrichments in Presolar Grains Provide First Evidence of p-process Nucleosynthesis in Core-collapse Supernovae
Authors: Ishita Pal, Manavi Jadhav, Danielle Z. Shulaker, Michael R. Savina, Marco Pignatari, Lorenzo Roberti, Heather Bouillion, Maria Lugaro, Christopher J. Dory, Frank Gyngard, Noriko Kita, Sachiko Amari
Figure caption: Comparison of grain data with stellar models. Three-isotope Sr plots of presolar HD graphites from KFB1 Murchison analyzed in this work. The five subgrains with positive δ84Sr86 values are indicated with black filled circles; all the others are indicated with gray filled circles. All the shown uncertainties represent 1σ variation. (a) Mainstream SiC grains from the Presolar Grain Database (T. Stephan et al. 2024) are plotted as empty circles. Isotopic ratios of the envelopes in low-metallicity AGB stars (M. Lugaro et al. 2018; D. Vescovi et al. 2020) are shown as blue and green lines as indicated in the legend. Markers along the prediction lines indicate isotopic ratios when the stellar envelope is C rich. (b) Sr isotopic abundance predictions from all interior layers of CCSN models with initial masses of 15, 20, and 25 M☉ (T. Rauscher et al. 2002; C. Ritter et al. 2018) are plotted in blue, orange, and pink, respectively. See the Appendix for details on AGB and CCSNe models.
Paper: Strontium-84 Enrichments in Presolar Grains Provide First Evidence of p-process Nucleosynthesis in Core-collapse Supernovae
Authors: Ishita Pal, Manavi Jadhav, Danielle Z. Shulaker, Michael R. Savina, Marco Pignatari, Lorenzo Roberti, Heather Bouillion, Maria Lugaro, Christopher J. Dory, Frank Gyngard, Noriko Kita, Sachiko Amari
Figure caption: An alternative explanation for 84Sr enrichments in our graphite grains. The figure shows six δ88Sr86 versus δ84Sr86 subplots with measured data on 49 HD graphite grains from the KFB1 fraction of Murchison. The five subgrains with positive δ84Sr86 values are indicated in black. The subplots are overlaid with the resultant isotopic values from varying initial Sr compositions and dilution of the He shell by the envelopes of the model stars. Each subplot shows the calculated results from a different stellar model: RIT15, RIT20, RIT25, RAU25, RAU20, and RAU15, respectively (moving clockwise from the upper left corner). The colored lines in each subplot represent different initial Sr compositions of the respective model star (see legend). In each colored line, different marker symbols represent different percentages of contribution of the envelope relative to the He shell: the “x” sign (0%), the plus sign (25%), upright triangle (50%), inverted triangle (75%), and square box (95%). Only the combinations with C/O > 0.99 are plotted. All uncertainties shown are 1σ.
Paper: Strontium-84 Enrichments in Presolar Grains Provide First Evidence of p-process Nucleosynthesis in Core-collapse Supernovae
Authors: Ishita Pal, Manavi Jadhav, Danielle Z. Shulaker, Michael R. Savina, Marco Pignatari, Lorenzo Roberti, Heather Bouillion, Maria Lugaro, Christopher J. Dory, Frank Gyngard, Noriko Kita, Sachiko Amari
Figure caption: Three-isotope Sr plots of presolar HD graphites from KFB1 Murchison analyzed in this work. The five subgrains with positive δ84Sr86 values are indicated by solid black circles. All the uncertainties represent 1σ variation. Isotopic ratios of the envelopes in low-metallicity AGB stars (A. I. Karakas et al. 2018; M. Lugaro et al. 2018) with 1X and 2X initial abundances of 84Sr are shown as green and yellow colored lines, respectively. Markers along the prediction lines indicate isotopic ratios when the stellar envelope is C rich. These yellow and green markers have almost identical isotopic ratios, indicating that there is essentially no difference in the abundance of 84Sr for the 1X and 2X cases in C-rich envelopes of low-metallicity AGB stars.
Paper: Strontium-84 Enrichments in Presolar Grains Provide First Evidence of p-process Nucleosynthesis in Core-collapse Supernovae
Authors: Ishita Pal, Manavi Jadhav, Danielle Z. Shulaker, Michael R. Savina, Marco Pignatari, Lorenzo Roberti, Heather Bouillion, Maria Lugaro, Christopher J. Dory, Frank Gyngard, Noriko Kita, Sachiko Amari
Figure caption: Time evolution of the RIMS signal for grain KFB1h-412. (a) The variation in Sr and Mo elemental counts in 30 s time bins, corresponding to 30,000 laser shots each. (b) The δ(84Sr/86Sr) and δ(92Mo/96Mo) values for each bin. Large error bars correspond to very few counts of 84Sr.
Paper: Strontium-84 Enrichments in Presolar Grains Provide First Evidence of p-process Nucleosynthesis in Core-collapse Supernovae
Authors: Ishita Pal, Manavi Jadhav, Danielle Z. Shulaker, Michael R. Savina, Marco Pignatari, Lorenzo Roberti, Heather Bouillion, Maria Lugaro, Christopher J. Dory, Frank Gyngard, Noriko Kita, Sachiko Amari
Figure caption: Images of grain KFB1h-011 before any SIMS analysis (left) and after SIMS analysis (middle and right). The example images provide ample evidence of there being enough grain material left over for RIMS analysis after SIMS analysis
Paper: Magnetic Reconnection in the Heliospheric Current Sheet Embedded in an Interplanetary Coronal Mass Ejection Sheath
Authors: Matti Ala-Lahti, Tuija I. Pulkkinen, Jonas Suni, Heli Hietala, Simon W. Good, Mojtaba Akhavan-Tafti, Minna Palmroth, Emilia K. J. Kilpua
Figure caption: Approximated preshock solar wind conditions, magnetic shear versus Δβ across the HCS crossings, and a sketch of the HCS reconnection exhausts downstream of an interplanetary shock in the ICME sheath. Panel (a) shows the approximated preshock solar wind conditions based on the magnetohydrodynamic Rankine–Hugoniot relations (yellow), with the compression ratio r given by the ratio of proton density in the sheath and upstream of the shock. The dashed horizontal lines represent the reference values measured upstream of the shock. Panel (b) shows magnetic shear and Δβ across the HCS crossings, with open circles denoting the magnetic shear in the approximated preshocked solar wind. The theoretical curves are shown for pressure gradient layer widths of L = 0.5 di and L = 1.0 di. Panel (c) illustrates the exhaust directions, widths, X-point locations and exhaust distances from the shock at 1 au as well as the exhaust geometries. The “Jet ﹩| | \pm \bar{{L}}﹩” labels refer to an exhaust jet in the ±L direction. Panel (d) shows the BL profiles across the exhausts as observed by the L1 fleet. The ACE and DSCOVR data are time shifted to align with the Wind data. Panel (e) shows the spacecraft positions in GSE coordinates and the X-point locations from single spacecraft measurements based on a fast reconnection rate of 0.1.
Paper: Magnetic Reconnection in the Heliospheric Current Sheet Embedded in an Interplanetary Coronal Mass Ejection Sheath
Authors: Matti Ala-Lahti, Tuija I. Pulkkinen, Jonas Suni, Heli Hietala, Simon W. Good, Mojtaba Akhavan-Tafti, Minna Palmroth, Emilia K. J. Kilpua
Figure caption: Wind magnetic field, plasma, and electron number flux observations across the four HCS crossings. First HCS crossing: panel (a) shows the magnetic field magnitude and the field components in LMN coordinates; panel (b) shows the proton velocity in the LMN coordinates with the mean velocity being subtracted; panel (c) shows the proton number density and temperature; and panel (d) shows the electron number flux at 165 eV energies for different pitch angles (PAs). Panels (e)–(p) show the corresponding parameters for the other three crossings. The L and N vectors of the local LMN coordinate system, average VLMN, and the current sheet widths (δCS) computed from VN and expressed in units of ion inertial length scale (di) are given. The cyan and white shading show the current sheet intervals. The gray shading shows the predicted VL based on the Walén relation.
Paper: Magnetic Reconnection in the Heliospheric Current Sheet Embedded in an Interplanetary Coronal Mass Ejection Sheath
Authors: Matti Ala-Lahti, Tuija I. Pulkkinen, Jonas Suni, Heli Hietala, Simon W. Good, Mojtaba Akhavan-Tafti, Minna Palmroth, Emilia K. J. Kilpua
Figure caption: Wind spacecraft observations of an ICME ejecta and a preceding shock and sheath region at 1 au on 2020 April 20. Panel (a) shows the magnetic field (B) magnitude and Geocentric Solar Ecliptic (GSE) components of the field; panel (b) shows the magnetic field azimuthal (ϕB) component, and panel (c) shows the magnetic field latitudinal (θB) component with respect to the ecliptic plane; panel (d) shows the proton speed (∣V∣); panel (e) shows the proton density (np); and panel (f) shows the electron number flux at 165 eV energies for different pitch angles (PAs). The vertical lines indicate the shock (magenta), the ICME ejecta leading edge (blue), and the four HCS crossings (cyan).
Paper: Magnetic Reconnection in the Heliospheric Current Sheet Embedded in an Interplanetary Coronal Mass Ejection Sheath
Authors: Matti Ala-Lahti, Tuija I. Pulkkinen, Jonas Suni, Heli Hietala, Simon W. Good, Mojtaba Akhavan-Tafti, Minna Palmroth, Emilia K. J. Kilpua
Figure caption: Multispacecraft observations across the reconnecting HCS crossings embedded in the ICME sheath (the second and third HCS crossings). Panel (a) shows the Wind magnetic field measurements across the crossings in GSE coordinates, and panels (b)–(c) show the electron number flux at different energies for different pitch angles (PAs). Panel (d) illustrates electron signatures observed within reconnection exhausts that are magnetically disconnected from Sun and magnetically connected to Sun. Panels (e)–(p) show magnetic field and plasma observations across the second and third HCS crossings from ARTEMIS-P2 and Cluster in a similar format to Figure 2.
Paper: Magnetic Reconnection in the Heliospheric Current Sheet Embedded in an Interplanetary Coronal Mass Ejection Sheath
Authors: Matti Ala-Lahti, Tuija I. Pulkkinen, Jonas Suni, Heli Hietala, Simon W. Good, Mojtaba Akhavan-Tafti, Minna Palmroth, Emilia K. J. Kilpua
Figure caption: 3D sketch of the observed HCS reconnection exhausts at Earth’s orbit, including an illustration of the current sheet folding in interplanetary space. The exhaust separatrices in gray and the spacecraft path through the folded HCS are adjusted to the current sheet NGSE and MGSE directions. The planar exhaust regions in yellow are aligned with the LGSE direction. The “Jet ﹩| | \pm \bar{{L}}﹩” labels refer to exhaust jets in the ±L direction.
Paper: The Inner Kernel of the Classical Kuiper Belt
Authors: Amir Siraj, Christopher F. Chyba, Scott Tremaine
Figure caption: Normalized histograms of the abary, efree, and Ifree distributions shown in Figure 1. Dotted lines show best-fit Gaussian distribution for abary and Rayleigh distributions for efree and Ifree. These kernel-like and newly identified clusters have distributions of abary described by Gaussians with means of 44.00 and 42.98 au and standard deviations of 0.25 and 0.24 au, respectively. Rayleigh distributions with modes of 0.026 and 0.046 describe their respective distributions of efree, and dispersions of 1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩4 and 1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩​​​​​​3 describe their respective distributions of Ifree. The fit of the efree distributions to the Rayleigh form is not good; fitting these distributions instead with Gaussians would yield means of 0.063 and 0.036, and standard deviations of 0.017 and 0.011, respectively. Nonclustered classicals in gray.
Paper: The Inner Kernel of the Classical Kuiper Belt
Authors: Amir Siraj, Christopher F. Chyba, Scott Tremaine
Figure caption: Normalized histograms of the abary, efree, and Ifree distributions shown in Figure 3. Dotted lines show best-fit bimodal Gaussian distribution for abary and Rayleigh distributions for efree and Ifree. The distribution of abary is described by two Gaussian distributions with means of 44.01 and 43.00 au, standard deviations of 0.26 and 0.29 au, and relative weights of 0.62 and 0.38, respectively. Rayleigh distributions with modes of 0.040 and ﹩1\mathop{.}\limits^{^\circ }5﹩ describe the distributions of efree and Ifree, respectively. Fitting efree instead with two Gaussians would yield means of 0.037 and 0.072, standard deviations of 0.013 for each, and relative weights of 0.59 and 0.41, respectively. Nonclustered classicals in gray.
Paper: The Inner Kernel of the Classical Kuiper Belt
Authors: Amir Siraj, Christopher F. Chyba, Scott Tremaine
Figure caption: DBSCAN results for Nmin = 50 and ϵ = 0.16, illustrating (relative to Figure 1) that a slightly higher value of ϵ can lead to a combined kernel plus inner kernel cluster (shown here in purple). As in Figure 1, the nonclustered classicals are shown in gray.
Paper: The Inner Kernel of the Classical Kuiper Belt
Authors: Amir Siraj, Christopher F. Chyba, Scott Tremaine
Figure caption: DBSCAN results for Nmin = 50 and ϵ = 0.15. Kernel-like cluster in red, new cluster in blue, nonclustered classicals in gray.
Paper: Evidence of Titanate Clouds in the Dayside Atmosphere of the Ultrahot Jupiter WASP-121b
Authors: Suman Saha, James S. Jenkins
Figure caption: (Upper) The observed panchromatic planet-to-star flux ratio of WASP-121b, spanning a wavelength range of ∼0.6–5.1 μm, extracted using the Eureka! pipeline from JWST NIRISS and NIRSpec/G395H observations, followed by spectral lightcurve fitting with ExoELF. Contributions from individual datasets across the wavelength range are shown in different colors. (Lower) The panchromatic emission spectral energy distribution (SED) of WASP-121b, derived from the planet-to-star flux ratio and a PHEONIX stellar model. Overplotted blackbody curves corresponding to different brightness temperatures illustrate spectral features in the planet’s spectrum. The significant deviation of the observed spectra from blackbody expectations at shorter wavelengths indicates the increasing dominance of starlight reflected by the planet in this regime.
Paper: Evidence of Titanate Clouds in the Dayside Atmosphere of the Ultrahot Jupiter WASP-121b
Authors: Suman Saha, James S. Jenkins
Figure caption: Known and well-constrained C/O ratios for a sample of exoplanets spanning a wide range of equilibrium temperatures are shown, alongside the precise C/O ratio of WASP-121b derived in this work (highlighted as a magenta bowtie). Values based on JWST observations are marked as circles, while those from other facilities are shown as squares. The plot reveals a clear trend of super-solar C/O ratios among the UHJ population. To investigate potential correlations between C/O ratios and equilibrium temperatures, model fits using a quadratic polynomial (applied to the full dataset and a JWST-only subset), and a smooth step function are shown, each with shaded 1σ confidence intervals.
Paper: Evidence of Titanate Clouds in the Dayside Atmosphere of the Ultrahot Jupiter WASP-121b
Authors: Suman Saha, James S. Jenkins
Figure caption: Pressure-dependent median abundances (in log-MMRs) from the best-fit equilibrium chemistry retrieval of the observed emission spectrum of WASP-121b (from Eureka!), along with the median abundance profiles of the condensate species CaTiO3. Overplotted are the pressure–temperature (PT) profiles from the best-fit retrievals using both free and equilibrium chemistry models, highlighting their close agreement. The condensation curves for CaTiO3 from both retrieval approaches are also shown, along with the Fe condensation curve from the equilibrium chemistry retrieval.
Paper: Evidence of Titanate Clouds in the Dayside Atmosphere of the Ultrahot Jupiter WASP-121b
Authors: Suman Saha, James S. Jenkins
Figure caption: The observed panchromatic emission spectrum of WASP-121b (from the Eureka! reduction), shown in terms of brightness temperature, overplotted with the best fit free-chemistry model from the retrieval analyses, along with the corresponding residuals. Additional retrieved models, each generated by excluding specific species, are also overplotted; these were used to assess the detection significance of those species.