adsabs/AstroCLIMB huggingface dataset:
Paper: LIGO–Virgo–KAGRA's Oldest Black Holes: Probing Star Formation at Cosmic Noon With GWTC-3
Authors: Maya Fishbach, Lieke van Son
Figure caption: Inferred formation rate assuming the default α  τ  = –1 delay time distribution (the green line shows the median a posteriori formation rate as a function of redshift, while the shaded bands enclose the 50% and 90% posterior probabilities). We adopt the formation rate parameterization from Katsianis et al. (2021) with two parameters controlling the shape and one parameter controlling the amplitude (see Equation (6)); the prior is shown in yellow (the dotted line shows median a priori formation rate, while the shaded band encloses the 90% prior probability). For comparison, we show the UV SFR (dashed light pink line) and UV+IR SFR (dotted–dashed dark pink line) from Katsianis et al. (2021) normalized by 10−6 M ⊙.
Paper: UNCOVER: Illuminating the Early Universe—JWST/NIRSpec Confirmation of z > 12 Galaxies
Authors: Bingjie Wang, 冰洁 王, Seiji Fujimoto, Ivo Labbé, Lukas J. Furtak, Tim B. Miller, David J. Setton, Adi Zitrin, Hakim Atek, Rachel Bezanson, Gabriel Brammer, Joel Leja, Pascal A. Oesch, Sedona H. Price, Iryna Chemerynska, Sam E. Cutler, Pratika Dayal, Pieter van Dokkum, Andy D. Goulding, Jenny E. Greene, Y. Fudamoto, Gourav Khullar, Vasily Kokorev, Danilo Marchesini, Richard Pan, John R. Weaver, Katherine E. Whitaker, Christina C. Williams
Figure caption: Mass–size relationship. UNCOVER-z12 and UNCOVER-z13 are shown as red diamonds. We take the average masses and uncertainties from the three SED fitting results. Also shown in unfilled red symbols are the UNCOVER-z12 sizes assuming two components. The triangle indicates an upper limit. We include five data sets from the literature as well: massive galaxies at z ∼ 8 (Baggen et al. 2023; Labbé et al. 2023), GN-z11 at z ∼ 11 (Tacchella et al. 2023), a plausible luminous galaxy at z ∼ 12 (Naidu et al. 2022b; Bakx et al. 2023), and z > 10 galaxies confirmed by JADES (Curtis-Lake et al. 2023; Robertson et al. 2023). The gray line is a fit of the mass–size relationship for satellites of Milky Way–like hosts (Carlsten et al. 2021); note that the local volume (LV) relation is measured at different rest-frame wavelengths than the high-redshift samples, and is included here only for reference. The galaxies of this Letter are among the largest known at z ≳ 10.
Paper: UNCOVER: Illuminating the Early Universe—JWST/NIRSpec Confirmation of z > 12 Galaxies
Authors: Bingjie Wang, 冰洁 王, Seiji Fujimoto, Ivo Labbé, Lukas J. Furtak, Tim B. Miller, David J. Setton, Adi Zitrin, Hakim Atek, Rachel Bezanson, Gabriel Brammer, Joel Leja, Pascal A. Oesch, Sedona H. Price, Iryna Chemerynska, Sam E. Cutler, Pratika Dayal, Pieter van Dokkum, Andy D. Goulding, Jenny E. Greene, Y. Fudamoto, Gourav Khullar, Vasily Kokorev, Danilo Marchesini, Richard Pan, John R. Weaver, Katherine E. Whitaker, Christina C. Williams
Figure caption: Stellar population modeling with Bagpipes. (a) The median model spectrum and photometry are shown in red, whereas the observations are shown in black. The model spectrum at the full resolution is additionally shown in gold, highlighting the predicted emission features that are washed out by the instrumental resolution. Both model spectra are scaled by a polynomial calibration vector to match the photometry. (b) The corner plot illustrates posterior distributions for a few key parameters; scale-dependent parameters are magnification-corrected. (c)–(d) Same as the above figure set, but for UNCOVER-z13. We note that the photometric data points at short wavelengths are consistent with zero flux at 1.5σ confidence.
Paper: UNCOVER: Illuminating the Early Universe—JWST/NIRSpec Confirmation of z > 12 Galaxies
Authors: Bingjie Wang, 冰洁 王, Seiji Fujimoto, Ivo Labbé, Lukas J. Furtak, Tim B. Miller, David J. Setton, Adi Zitrin, Hakim Atek, Rachel Bezanson, Gabriel Brammer, Joel Leja, Pascal A. Oesch, Sedona H. Price, Iryna Chemerynska, Sam E. Cutler, Pratika Dayal, Pieter van Dokkum, Andy D. Goulding, Jenny E. Greene, Y. Fudamoto, Gourav Khullar, Vasily Kokorev, Danilo Marchesini, Richard Pan, John R. Weaver, Katherine E. Whitaker, Christina C. Williams
Figure caption: Morphological modeling. (a) UNCOVER-z12 is first modeled as a single source. The upper left panel shows its image in F277W, tracing recent unobscured star formation, whereas the lower left panel shows the single-component model fit. The model residual, scaled by the rms, is shown in the middle. A corner plot illustrating the posterior distributions is also included. (b) UNCOVER-z12 is also modeled as two components, and the results are presented in a similar manner. (c) Same as the first figure set, but for UNCOVER-z13.
Paper: UNCOVER: Illuminating the Early Universe—JWST/NIRSpec Confirmation of z > 12 Galaxies
Authors: Bingjie Wang, 冰洁 王, Seiji Fujimoto, Ivo Labbé, Lukas J. Furtak, Tim B. Miller, David J. Setton, Adi Zitrin, Hakim Atek, Rachel Bezanson, Gabriel Brammer, Joel Leja, Pascal A. Oesch, Sedona H. Price, Iryna Chemerynska, Sam E. Cutler, Pratika Dayal, Pieter van Dokkum, Andy D. Goulding, Jenny E. Greene, Y. Fudamoto, Gourav Khullar, Vasily Kokorev, Danilo Marchesini, Richard Pan, John R. Weaver, Katherine E. Whitaker, Christina C. Williams
Figure caption: Forced fits at low redshift. (a) The left panel displays the 1D spectrum for UNCOVER-z12 in f  λ  as a function of the observed wavelength. Data are plotted in gray, whereas the best-fit EAzY model at z ∼ 3 is plotted in red. Also plotted are the uncertainties in blue. The cyan horizontal line is at y = 0 to guide the eye. The right panel shows the probability density over the redshift range of the search for a minimum χ 2. (b) Same as the above figure, but for UNCOVER-z13. The high-redshift solutions are favored for both sources.
Paper: UNCOVER: Illuminating the Early Universe—JWST/NIRSpec Confirmation of z > 12 Galaxies
Authors: Bingjie Wang, 冰洁 王, Seiji Fujimoto, Ivo Labbé, Lukas J. Furtak, Tim B. Miller, David J. Setton, Adi Zitrin, Hakim Atek, Rachel Bezanson, Gabriel Brammer, Joel Leja, Pascal A. Oesch, Sedona H. Price, Iryna Chemerynska, Sam E. Cutler, Pratika Dayal, Pieter van Dokkum, Andy D. Goulding, Jenny E. Greene, Y. Fudamoto, Gourav Khullar, Vasily Kokorev, Danilo Marchesini, Richard Pan, John R. Weaver, Katherine E. Whitaker, Christina C. Williams
Figure caption: Low-redshift interlopers or unconfirmed sources. For each figure, the left panel displays the 1D spectrum in f λ as a function of the observed wavelength. Data, the best-fit EAzY model, and uncertainties are plotted in gray, red, and blue, respectively. A convolved observed spectrum is additionally shown as a dashed black line for visualization purposes. The cyan horizontal line is at y = 0 to guide the eye. The right panel shows the probability density over the redshift range of the search for a minimum  χ 2.
Paper: Decomposing the Origin of TeV–PeV Emission from the Galactic Plane: Implications of Multimessenger Observations
Authors: Ke Fang, Kohta Murase
Figure caption: Comparison of intensities of γ-rays from resolved sources (cool colors) and GDE (warm colors) in three sky regions including (1) Tibet Regions A, (2) Tibet Region B, and (3) LHAASO Outer Galaxy region. The source emissivity is evaluated based on (a) 3HWC catalog (Albert et al. 2020), which includes 38, 32, and 10 sources, (b) 4FGL catalog (Abdollahi et al. 2022), which includes 81, 73, and 25 sources, (c) 1LHAASO catalog (Cao et al. 2023b), which includes 37, 34, and 9 sources detected by WCDA, and 40, 37, and 10 sources detected by KM2A in the three sky regions, respectively. The total source flux is averaged over the solid angle of the corresponding sky regions. For the GDE, the error bars of Tibet ASγ observations correspond to 1σ statistical errors and those of the LHAASO flux points correspond to the quadratic sum of the statistical and systematic errors. In the last energy bin of the Tibet ASγ GDE flux, the fainter data points indicate the residual intensity after removing the events relevant to Cygnus Cocoon (40%). In the Tibet Region A plot, the LHAASO flux points correspond to a similar but larger sky region, the LHAASO inner Galaxy region defined as 15° < l < 125° and ∣b∣ < 5°. The Fermi-LAT data points (De La Torre Luque et al. 2023) correspond to the total flux of the two Tibet regions.
Paper: Decomposing the Origin of TeV–PeV Emission from the Galactic Plane: Implications of Multimessenger Observations
Authors: Ke Fang, Kohta Murase
Figure caption: All-flavor flux of neutrinos expected from resolved Galactic sources (cool colors, unhatched) and GDE (warm colors, hatched) averaged over the full sky. The source emission is an upper limit based on the assumption that all γ-ray sources not associated with pulsars are hadronic emitters. The source flux is calculated using the measurements of 227 sources from 4FGL (Abdollahi et al. 2022), 65 sources from HGPS (Abdalla et al. 2018), 51 sources from 3HWC (Albert et al. 2020), 36 WCDA sources, and 43 KM2A sources from 1LHAASO (Cao et al. 2023b). The GDE intensity is converted from Fermi-LAT’s Galactic interstellar emission model (Abdollahi et al. 2022), LHAASO (Cao et al. 2023a; Li 2023) and Tibet ASγ's GDE observations (Amenomori et al. 2021; Fang & Murase 2021). The hatched gray band is the IceCube measurement of the GP using the π 0 template (Abbasi et al. 2023).
Paper: Decomposing the Origin of TeV–PeV Emission from the Galactic Plane: Implications of Multimessenger Observations
Authors: Ke Fang, Kohta Murase
Figure caption: Summary of the sky regions observed by various γ-ray experiments, including H.E.S.S. Telescope for the GP survey (red rectangle; Abdalla et al. 2018), Tibet ASγ Observatory for the GDE observation (yellow rectangle for region A and dashed cyan rectangle for region B; Amenomori et al. 2021), LHAASO Observatory for the GDE measurement (purple rectangle for outer Galaxy; Cao et al. 2023a), HAWC Observatory for the Third HAWC Catalog of Very-high-energy Gamma-ray Sources (3HWC; sky blue curves Albert et al. 2020) and LHAASO for the First LHAASO Catalog of Gamma-Ray Sources (1LHAASO; pink curves; Cao et al. 2021). Fermi-LAT and IceCube observe the full sky and are not shown in this plot. Details of the observations are summarized in Tables 1 and 2 . For reference, the neutral hydrogen (21 cm) emission from HI 4-PI Survey (HI4PI Collaboration et al. 2016) is shown with the column density indicated by the color bar. Plot is in Galactic coordinates.
Paper: Decomposing the Origin of TeV–PeV Emission from the Galactic Plane: Implications of Multimessenger Observations
Authors: Ke Fang, Kohta Murase
Figure caption: All-flavor, 4π-averaged flux of neutrinos observed by IceCube with π 0 (black) and KRA templates (gray and silver) comparing to that derived from the Tibet ASγ's GDE observations (orange; Amenomori et al. 2021; Fang & Murase 2021) and LHAASO’s GP observations (orange red; Cao et al. 2023a, 2023b; Li 2023). The orange red band sums the flux of the nonpulsar sources and diffuse emission derived from WCDA and KM2A observations in 1–10 TeV and 10–100 TeV, respectively.
Paper: Open Magnetic Fields in the Martian Magnetosphere Revealing Dipole-like Intrinsic Magnetic Fields at Mars
Authors: Shaosui Xu, Janet G. Luhmann, David L. Mitchell, Tristan Weber, David A. Brain, Yingjuan Ma, Shannon M. Curry, Gina A. DiBraccio, Jasper Halekas, Suranga Ruhunusiri, Christian Mazelle, Robert J. Lillis, Benoit Langlais
Figure caption: (A1)–(A2) Schematics show closed field lines from a southward-oriented dipole field (A1), which interacts with the IMF producing open field lines (A2). (B1)–(B4) Schematics show the tail field polarities (red for sunward and blue for tailward) from an intrinsic dipole-like field (B1) and the induced magnetotail comprised of draped IMFs (B2). (B3) Eastward IMF (dashed gray line) magnetically reconnects with open field lines (red and blue dashed lines) from quadrants 1 and 3, producing new open field lines (red and blue solid lines), overlaid over tail field polarities from the dipole-like field. (B4) The tail field polarities observed by MAVEN at X MSO = [−2, −1] R  M  for open fields under the east IMF condition.
Paper: Open Magnetic Fields in the Martian Magnetosphere Revealing Dipole-like Intrinsic Magnetic Fields at Mars
Authors: Shaosui Xu, Janet G. Luhmann, David L. Mitchell, Tristan Weber, David A. Brain, Yingjuan Ma, Shannon M. Curry, Gina A. DiBraccio, Jasper Halekas, Suranga Ruhunusiri, Christian Mazelle, Robert J. Lillis, Benoit Langlais
Figure caption: The averaged B  x /∣B∣ for open fields (a)–(c) and draped fields (d)–(f) in the MSO Y–Z plane for different X MSO ranges, (a), (d) [0, 1] R  M , (b), (d) [−1, 0] R  M , and (c), (f) [−2, −1] R  M , combining all IMF directions.
Paper: Open Magnetic Fields in the Martian Magnetosphere Revealing Dipole-like Intrinsic Magnetic Fields at Mars
Authors: Shaosui Xu, Janet G. Luhmann, David L. Mitchell, Tristan Weber, David A. Brain, Yingjuan Ma, Shannon M. Curry, Gina A. DiBraccio, Jasper Halekas, Suranga Ruhunusiri, Christian Mazelle, Robert J. Lillis, Benoit Langlais
Figure caption: The averaged B  x /∣B∣ for all topologies (top row), open fields (middle row), and draped fields (bottom row) in the MSO Y–Z plane for X MSO = [−2, −1] R  M  under the east IMF (A1)–(A3), the west IMF (B1)–(B3), and the whole IMF (C1)–(C3).
Paper: Constraining the Jet Composition of GRB 221009A with the Prompt TeV Emission Limit
Authors: Cui-Yuan Dai, Xiang-Yu Wang, Ruo-Yu Liu, Bing Zhang
Figure caption: Modeling GRB 221009A in the internal shock scenario through numerical simulation. We use four colors to represent different cases and variability timescales: blue (Case I, Δt c = 82 ms), gray (Case I, Δt c = 200 ms), black (Case II, Δt c = 82 ms) and red (Case II, Δt c = 200 ms). (a) Initial distribution of mass m for the injected shells, with T inj representing the time elapsed after the first shell is injected in the source frame. (b) The initial distribution of Lorentz factors Γ for the injected shells. (c) The collision radius R c for the N cth observed pulse. (d) The distribution of collision radii R c, where P is the probability density. (e) The time-average spectra in the observer frame during three time intervals: T 0 + 220 − T 0 + 223 s (the dashed-dot line), T 0 + 223 − T 0 + 226 s (the dashed line), and T 0 + 226 − T 0 + 230 s (the solid line). (f) The synthetic light curve in the 20–200 keV range, integrated on equal arrival time surfaces (EATS) with a time bin of 1 s in the observer frame. The magenta light curve represents the observed one (An et al. 2023). Light curves with smaller time bins are provided in Figure 5 in the Appendix. Here, T obs represents the time elapsed after T 0 + 220 s in the observer frame.
Paper: Constraining the Jet Composition of GRB 221009A with the Prompt TeV Emission Limit
Authors: Cui-Yuan Dai, Xiang-Yu Wang, Ruo-Yu Liu, Bing Zhang
Figure caption: Absorption ratio f  γ γ  in the single-pulse (the solid line) case and two-pulse case (the dashed lines).
Paper: MOSEL Survey: JWST Reveals Major Mergers/strong Interactions Drive the Extreme Emission Lines in the Early Universe
Authors: Anshu Gupta, Ravi Jaiswar, Vicente Rodriguez-Gomez, Ben Forrest, Kim-Vy Tran, Themiya Nanayakkara, Anishya Harshan, Elisabete da Cunha, Glenn G. Kacprzak, Michaela Hirschmann
Figure caption: Bootstrapped distribution of the median number of companions (left), the stellar mass ratio of the brightest companion (middle), and the total stellar mass ratio of all companions (right) for EELGs (top row), full control sample (second row), stellar mass–matched sample (third row), and stellar mass plus sSFR–matched sample (fourth row). EELGs have roughly similar stellar mass companion galaxies, whereas the stellar mass ratio of companions for all control samples is 3–10 times smaller.
Paper: MOSEL Survey: JWST Reveals Major Mergers/strong Interactions Drive the Extreme Emission Lines in the Early Universe
Authors: Anshu Gupta, Ravi Jaiswar, Vicente Rodriguez-Gomez, Ben Forrest, Kim-Vy Tran, Themiya Nanayakkara, Anishya Harshan, Elisabete da Cunha, Glenn G. Kacprzak, Michaela Hirschmann
Figure caption: The ratio of stellar mass of the brightest companion (top) and total stellar mass of all companions (bottom) to the target galaxy as a function of stellar mass of primary targets. Color scheme is the same as Figure 1. The larger symbols represent the median of the respective samples. The blue shaded region represents the stellar mass limit (﹩\mathrm{log}({M}_{* }/{M}_{\odot })﹩ = 7) of our companion population. A higher stellar mass ratio of companions around EELGs suggests EELGs might be undergoing strong interaction/major mergers.
Paper: MOSEL Survey: JWST Reveals Major Mergers/strong Interactions Drive the Extreme Emission Lines in the Early Universe
Authors: Anshu Gupta, Ravi Jaiswar, Vicente Rodriguez-Gomez, Ben Forrest, Kim-Vy Tran, Themiya Nanayakkara, Anishya Harshan, Elisabete da Cunha, Glenn G. Kacprzak, Michaela Hirschmann
Figure caption: Stellar mass and specific SFR distribution of EELGs (golden stars) and full control sample (gray circles). The SFR are derived from the MAGPHYS SED fitting code. The dashed line corresponds to the star-forming main sequence at z = 3 by Popesso et al. (2022). At a fixed stellar mass EELGs have 0.3  dex higher sSFR compared to the control galaxies.
Paper: MOSEL Survey: JWST Reveals Major Mergers/strong Interactions Drive the Extreme Emission Lines in the Early Universe
Authors: Anshu Gupta, Ravi Jaiswar, Vicente Rodriguez-Gomez, Ben Forrest, Kim-Vy Tran, Themiya Nanayakkara, Anishya Harshan, Elisabete da Cunha, Glenn G. Kacprzak, Michaela Hirschmann
Figure caption: Example JWST/NIRCam F444W images from the JADES survey (Rieke & the JADES Collaboration 2023) for four EELGs (black circles and their companions (pink circles) showing the variety of companions around the target galaxy.
Paper: MOSEL Survey: JWST Reveals Major Mergers/strong Interactions Drive the Extreme Emission Lines in the Early Universe
Authors: Anshu Gupta, Ravi Jaiswar, Vicente Rodriguez-Gomez, Ben Forrest, Kim-Vy Tran, Themiya Nanayakkara, Anishya Harshan, Elisabete da Cunha, Glenn G. Kacprzak, Michaela Hirschmann
Figure caption: Distribution of the number of companions around EELGs (solid gold) and the control sample (black). The dashed lines indicate the medians of the respective samples. EELGs on average have two companions, whereas galaxies in the control sample only have one companion.
Paper: Constraining the Jet Composition of GRB 221009A with the Prompt TeV Emission Limit
Authors: Cui-Yuan Dai, Xiang-Yu Wang, Ruo-Yu Liu, Bing Zhang
Figure caption: Left panel: the spectra of five pulses in the simulation for both Case I and Case II (refer to Section 2.1), using Δt c = 82 ms. In Case I, we choose the first five observed pulses; in Case II, we choose five pulses with intervals of 17 pulses to see the evolution of cutoff energies from different pulses. Right panel: the time-integrated absorption ratio f  γ γ  for the simulated GRB, which reproduces the key characteristics of GRB 221009A.
Paper: Constraining the Jet Composition of GRB 221009A with the Prompt TeV Emission Limit
Authors: Cui-Yuan Dai, Xiang-Yu Wang, Ruo-Yu Liu, Bing Zhang
Figure caption: The simulated light curve in 20–200 keV of GRB 221009A, assuming a time resolution ≪82 ms.
Paper: Constraining the Jet Composition of GRB 221009A with the Prompt TeV Emission Limit
Authors: Cui-Yuan Dai, Xiang-Yu Wang, Ruo-Yu Liu, Bing Zhang
Figure caption: The γγ absorption optical depth τ at 1 TeV of the pulses generated from internal shock simulations as a function of the emission radius of pulses in Case I (see Section 2.1) with Δt c = 82 ms.
Paper: UNCOVER: Illuminating the Early Universe—JWST/NIRSpec Confirmation of z > 12 Galaxies
Authors: Bingjie Wang, 冰洁 王, Seiji Fujimoto, Ivo Labbé, Lukas J. Furtak, Tim B. Miller, David J. Setton, Adi Zitrin, Hakim Atek, Rachel Bezanson, Gabriel Brammer, Joel Leja, Pascal A. Oesch, Sedona H. Price, Iryna Chemerynska, Sam E. Cutler, Pratika Dayal, Pieter van Dokkum, Andy D. Goulding, Jenny E. Greene, Y. Fudamoto, Gourav Khullar, Vasily Kokorev, Danilo Marchesini, Richard Pan, John R. Weaver, Katherine E. Whitaker, Christina C. Williams
Figure caption: NIRSpec/Prism observations of the two galaxies presented in this Letter. (a) The first row displays the 2D spectrum of UNCOVER-z12, with the rest-frame wavelength shown along the x-axis; the histogram indicates the extracted region. Second row, left panel, shows the 1D spectrum in f  ν  as a function of the observed wavelength. Data are plotted in gray, whereas the best-fit EAzY model is plotted in red. Also plotted are the uncertainties in blue. The cyan horizontal line is at y = 0 to guide the eye. Second row, right panel, includes the cutout in the F277W band, with the circle indicating the aperture size, 0.″32, in which photometry is extracted. Third row, left panel, shows the 1D spectrum again, but in f  λ  as a complementary visualization. Third row, right panel, plots the probability density over the redshift range of the search for a minimum χ 2. A strong Lyman break is clearly seen for UNCOVER-z12. (b) Same as the above figure set, but for UNCOVER-z13. We err on the conservative side and consider its redshift solution to be less well-determined due to the weaker break, even though p(z) sharply peaks at z > 12.
Paper: JWST Measurements of 13C, 18O, and 17O in the Atmosphere of Super-Jupiter VHS 1256 b
Authors: Siddharth Gandhi, Sam de Regt, Ignas Snellen, Yapeng Zhang, Benson Rugers, Niels van Leur, Quincy Bosschaart
Figure caption: Difference in the expected log posterior predictive density (ELPD) for each isotopologue against our fiducial model. A positive ΔELPD score indicates that the model with the isotopologue is preferred by that data point. The color bar indicates the Pareto k values for each of the data points, with points ≲0.7 indicating a good PSIS approximation (see Section 3.1.1). The vast majority of the data points fall into this category and hence our use of the leave-one-out cross-validation is robust for all three isotopologues. In gray we also show the molecular cross section for each of the isotopologues at 1 bar pressure and 1200 K temperature at the spectral resolution of the observations (R = 2700).
Paper: JWST Measurements of 13C, 18O, and 17O in the Atmosphere of Super-Jupiter VHS 1256 b
Authors: Siddharth Gandhi, Sam de Regt, Ignas Snellen, Yapeng Zhang, Benson Rugers, Niels van Leur, Quincy Bosschaart
Figure caption: Top panel: best-fitting model from the retrieval, along with the data points of the NIRSpec G395H/F290LP detector 2 (NRS2) observations of VHS 1256 b. We also show the 1σ range of the residuals of the data and model. Bottom panel: residuals of the best-fit model and the observations, with the 1σ, 2σ, and 3σ ranges shown in gray.
Paper: JWST Measurements of 13C, 18O, and 17O in the Atmosphere of Super-Jupiter VHS 1256 b
Authors: Siddharth Gandhi, Sam de Regt, Ignas Snellen, Yapeng Zhang, Benson Rugers, Niels van Leur, Quincy Bosschaart
Figure caption: Retrieved pressure–temperature profile form the retrieval of VHS 1256 b. The solid line shows the median values and the dark and light shaded regions indicate the 1σ and 2σ uncertainties respectively. The markers indicate the P–T knots used in the retrieval (see Section 2.2).
Paper: JWST Measurements of 13C, 18O, and 17O in the Atmosphere of Super-Jupiter VHS 1256 b
Authors: Siddharth Gandhi, Sam de Regt, Ignas Snellen, Yapeng Zhang, Benson Rugers, Niels van Leur, Quincy Bosschaart
Figure caption: Isotope ratios 12C/13C, 16O/18O, 16O/17O, and 18O/17O derived from the CO abundances of VHS 1256 b. The red dashed line and shaded area show the value measured for the local interstellar medium (ISM) and its 1σ uncertainty (Wilson 1999; Milam et al. 2005), and the dotted black line shows the value for the solar system.