adsabs/AstroCLIMB huggingface dataset:
Paper: Hidden Little Monsters: Spectroscopic Identification of Low-mass, Broad-line AGNs at z > 5 with CEERS
Authors: Dale D. Kocevski, Masafusa Onoue, Kohei Inayoshi, Jonathan R. Trump, Pablo Arrabal Haro, Andrea Grazian, Mark Dickinson, Steven L. Finkelstein, Jeyhan S. Kartaltepe, Michaela Hirschmann, James Aird, Benne W. Holwerda, Seiji Fujimoto, Stéphanie Juneau, Ricardo O. Amorín, Bren E. Backhaus, Micaela B. Bagley, Guillermo Barro, Eric F. Bell, Laura Bisigello, Antonello Calabrò, Nikko J. Cleri, M. C. Cooper, Xuheng Ding, Norman A. Grogin, Luis C. Ho, Taylor A. Hutchison, Akio K. Inoue, Linhua Jiang, Brenda Jones, Anton M. Koekemoer, Wenxiu Li, Zhengrong Li, Elizabeth J. McGrath, Juan Molina, Casey Papovich, Pablo G. Pérez-González, Nor Pirzkal, Stephen M. Wilkins, Guang Yang, L. Y. Aaron Yung
Figure caption: NIRSpec spectra of sources CEERS 2782 and CEERS 746 taken in the G235M grating with R ∼ 1000. The 2D spectra are shown above, with extraction windows highlighted in red. Gray regions in both the 1D and 2D spectra indicate regions masked owing to artifacts identified via visual inspection and the detector chip gap. The expected locations of notable emission lines, both detected and not detected, are noted.
Paper: Hidden Little Monsters: Spectroscopic Identification of Low-mass, Broad-line AGNs at z > 5 with CEERS
Authors: Dale D. Kocevski, Masafusa Onoue, Kohei Inayoshi, Jonathan R. Trump, Pablo Arrabal Haro, Andrea Grazian, Mark Dickinson, Steven L. Finkelstein, Jeyhan S. Kartaltepe, Michaela Hirschmann, James Aird, Benne W. Holwerda, Seiji Fujimoto, Stéphanie Juneau, Ricardo O. Amorín, Bren E. Backhaus, Micaela B. Bagley, Guillermo Barro, Eric F. Bell, Laura Bisigello, Antonello Calabrò, Nikko J. Cleri, M. C. Cooper, Xuheng Ding, Norman A. Grogin, Luis C. Ho, Taylor A. Hutchison, Akio K. Inoue, Linhua Jiang, Brenda Jones, Anton M. Koekemoer, Wenxiu Li, Zhengrong Li, Elizabeth J. McGrath, Juan Molina, Casey Papovich, Pablo G. Pérez-González, Nor Pirzkal, Stephen M. Wilkins, Guang Yang, L. Y. Aaron Yung
Figure caption: Multicomponent SED fit for CEERS 2782 using a linear combination of galaxy and AGN templates. The galaxy and AGN contributions are shown in green and red, respectively, while their sum is shown in blue. The host mass implied by this fit is M * = 108 M ⊙.
Paper: TOI-4600 b and c: Two Long-period Giant Planets Orbiting an Early K Dwarf
Authors: Ismael Mireles, Diana Dragomir, Hugh P. Osborn, Katharine Hesse, Karen A. Collins, Steven Villanueva, Allyson Bieryla, David R. Ciardi, Keivan G. Stassun, Mallory Harris, Jack J. Lissauer, Richard P. Schwarz, Gregor Srdoc, Khalid Barkaoui, Arno Riffeser, Kim K. McLeod, Joshua Pepper, Nolan Grieves, Vera Maria Passegger, Solène Ulmer-Moll, Joseph E. Rodriguez, Dax L. Feliz, Samuel Quinn, Andrew W. Boyle, Michael Fausnaugh, Michelle Kunimoto, Pamela Rowden, Andrew Vanderburg, Bill Wohler, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua N. Winn
Figure caption: Top: full TESS PDCSAP light curve of TOI-4600 showing four clear transits of TOI-4600 b and two transits of TOI-4600 c. An additional transit of TOI-4600 b is obscured by a sudden systematic increase in flux due to scattered light near TBJD 1850 while another transit at TBJD 2750 is obscured by a transit of TOI-4600 c that occurs 1.5 days later. Another transit of TOI-4600 b near TBJD 2419 occurred during a downlink gap and thus was not observed by TESS. The apparent difference in the transit depths is due to the different time resolutions, with the left portion showing 30 minute data and the middle and right portions showing 2 minute data. Bottom left: phase-folded detrended 2 (gray) and 30 minute (black) TESS data and best-fit model for TOI-4600 b. Bottom right: same as the bottom left but for TOI-4600 c.
Paper: TOI-4600 b and c: Two Long-period Giant Planets Orbiting an Early K Dwarf
Authors: Ismael Mireles, Diana Dragomir, Hugh P. Osborn, Katharine Hesse, Karen A. Collins, Steven Villanueva, Allyson Bieryla, David R. Ciardi, Keivan G. Stassun, Mallory Harris, Jack J. Lissauer, Richard P. Schwarz, Gregor Srdoc, Khalid Barkaoui, Arno Riffeser, Kim K. McLeod, Joshua Pepper, Nolan Grieves, Vera Maria Passegger, Solène Ulmer-Moll, Joseph E. Rodriguez, Dax L. Feliz, Samuel Quinn, Andrew W. Boyle, Michael Fausnaugh, Michelle Kunimoto, Pamela Rowden, Andrew Vanderburg, Bill Wohler, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua N. Winn
Figure caption: Top left: ground-based photometry from LCO, Wendelstein Observatory, Kotizarovci Observatory, and Whitin Observatory showing a transit from TOI-4600 b with the best-fit model overlaid. Top right: Palomar NIR AO imaging and sensitivity curves for TOI-4600 taken in the Brγ filter. The images were taken in good seeing conditions, and we reach a contrast of ∼7 mag fainter than the host star within 0.″5. Inset: image of the central portion of the data, centered on the star. Bottom: RVs extracted from the TRES reconnaissance spectra taken over the span of over a year and best-fit radvel model.
Paper: TOI-4600 b and c: Two Long-period Giant Planets Orbiting an Early K Dwarf
Authors: Ismael Mireles, Diana Dragomir, Hugh P. Osborn, Katharine Hesse, Karen A. Collins, Steven Villanueva, Allyson Bieryla, David R. Ciardi, Keivan G. Stassun, Mallory Harris, Jack J. Lissauer, Richard P. Schwarz, Gregor Srdoc, Khalid Barkaoui, Arno Riffeser, Kim K. McLeod, Joshua Pepper, Nolan Grieves, Vera Maria Passegger, Solène Ulmer-Moll, Joseph E. Rodriguez, Dax L. Feliz, Samuel Quinn, Andrew W. Boyle, Michael Fausnaugh, Michelle Kunimoto, Pamela Rowden, Andrew Vanderburg, Bill Wohler, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua N. Winn
Figure caption: Top left: period–radius diagram of verified transiting planets orbiting stars with V < 13 (black) and V > 13 (gray), as of 2022 November (NASA Exoplanet Archive). Bottom left: equilibrium temperature diagram (assuming albedo a = 0) for the same sample. Right: the TOI-4600 system and other warm gas giant systems with multiple transiting planets. TOI-4600 c is the coldest and has the longest orbital period of any transiting planet in these systems.
Paper: TOI-4600 b and c: Two Long-period Giant Planets Orbiting an Early K Dwarf
Authors: Ismael Mireles, Diana Dragomir, Hugh P. Osborn, Katharine Hesse, Karen A. Collins, Steven Villanueva, Allyson Bieryla, David R. Ciardi, Keivan G. Stassun, Mallory Harris, Jack J. Lissauer, Richard P. Schwarz, Gregor Srdoc, Khalid Barkaoui, Arno Riffeser, Kim K. McLeod, Joshua Pepper, Nolan Grieves, Vera Maria Passegger, Solène Ulmer-Moll, Joseph E. Rodriguez, Dax L. Feliz, Samuel Quinn, Andrew W. Boyle, Michael Fausnaugh, Michelle Kunimoto, Pamela Rowden, Andrew Vanderburg, Bill Wohler, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua N. Winn
Figure caption: SED of TOI-4600. Red symbols represent the observed photometric measurements, where the horizontal bars represent the effective width of the passband. Blue symbols are the model fluxes from the best-fit Kurucz atmosphere model (black).
Paper: TOI-4600 b and c: Two Long-period Giant Planets Orbiting an Early K Dwarf
Authors: Ismael Mireles, Diana Dragomir, Hugh P. Osborn, Katharine Hesse, Karen A. Collins, Steven Villanueva, Allyson Bieryla, David R. Ciardi, Keivan G. Stassun, Mallory Harris, Jack J. Lissauer, Richard P. Schwarz, Gregor Srdoc, Khalid Barkaoui, Arno Riffeser, Kim K. McLeod, Joshua Pepper, Nolan Grieves, Vera Maria Passegger, Solène Ulmer-Moll, Joseph E. Rodriguez, Dax L. Feliz, Samuel Quinn, Andrew W. Boyle, Michael Fausnaugh, Michelle Kunimoto, Pamela Rowden, Andrew Vanderburg, Bill Wohler, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua N. Winn
Figure caption: TESS target pixel file image of TOI-4600 for Sector 53 made using tpfplotter (Aller et al. 2020).
Paper: TOI-4600 b and c: Two Long-period Giant Planets Orbiting an Early K Dwarf
Authors: Ismael Mireles, Diana Dragomir, Hugh P. Osborn, Katharine Hesse, Karen A. Collins, Steven Villanueva, Allyson Bieryla, David R. Ciardi, Keivan G. Stassun, Mallory Harris, Jack J. Lissauer, Richard P. Schwarz, Gregor Srdoc, Khalid Barkaoui, Arno Riffeser, Kim K. McLeod, Joshua Pepper, Nolan Grieves, Vera Maria Passegger, Solène Ulmer-Moll, Joseph E. Rodriguez, Dax L. Feliz, Samuel Quinn, Andrew W. Boyle, Michael Fausnaugh, Michelle Kunimoto, Pamela Rowden, Andrew Vanderburg, Bill Wohler, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua N. Winn
Figure caption: Corner plot of the derived parameters obtained from allesfitter.
Paper: TOI-4600 b and c: Two Long-period Giant Planets Orbiting an Early K Dwarf
Authors: Ismael Mireles, Diana Dragomir, Hugh P. Osborn, Katharine Hesse, Karen A. Collins, Steven Villanueva, Allyson Bieryla, David R. Ciardi, Keivan G. Stassun, Mallory Harris, Jack J. Lissauer, Richard P. Schwarz, Gregor Srdoc, Khalid Barkaoui, Arno Riffeser, Kim K. McLeod, Joshua Pepper, Nolan Grieves, Vera Maria Passegger, Solène Ulmer-Moll, Joseph E. Rodriguez, Dax L. Feliz, Samuel Quinn, Andrew W. Boyle, Michael Fausnaugh, Michelle Kunimoto, Pamela Rowden, Andrew Vanderburg, Bill Wohler, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua N. Winn
Figure caption: Corner plot of the fitted parameters obtained from allesfitter.
Paper: SN 2023ixf in Messier 101: Photo-ionization of Dense, Close-in Circumstellar Material in a Nearby Type II Supernova
Authors: W. V. Jacobson-Galán, L. Dessart, R. Margutti, R. Chornock, R. J. Foley, C. D. Kilpatrick, D. O. Jones, K. Taggart, C. R. Angus, S. Bhattacharjee, L. A. Braff, D. Brethauer, A. J. Burgasser, F. Cao, C. M. Carlile, K. C. Chambers, D. A. Coulter, E. Dominguez-Ruiz, C. B. Dickinson, T. de Boer, A. Gagliano, C. Gall, H. Gao, E. L. Gates, S. Gomez, M. Guolo, M. R. J. Halford, J. Hjorth, M. E. Huber, M. N. Johnson, P. R. Karpoor, T. Laskar, N LeBaron, Z. Li, Y. Lin, S. D. Loch, P. D. Lynam, E. A. Magnier, P. Maloney, D. J. Matthews, M. McDonald, H.-Y. Miao, D. Milisavljevic, Y.-C. Pan, S. Pradyumna, C. L. Ransome, J. M. Rees, A. Rest, C. Rojas-Bravo, N. R. Sandford, L. Sandoval Ascencio, S. Sanjaripour, A. Savino, H. Sears, N. Sharei, S. J. Smartt, E. R. Softich, C. A. Theissen, S. Tinyanont, H. Tohfa, V. A. Villar, Q. Wang, R. J. Wainscoat, A. L. Westerling, E. Wiston, M. A. Wozniak, S. K. Yadavalli, Y. Zenati
Figure caption: Peak (a) U-band, (b) B-band, and (c) V-band absolute magnitudes vs. duration of IIn-like line profiles (t IIn) for SN 2023ixf (black star) with respect to CSM-interacting SNe II presented in W. V. Jacobson-Galán et al. (2023, in preparation) shown as circles (color delineation discussed in Section 3.2). SN 2020jfo (Teja et al. 2022) shown as reference canonical SN II without significant CSM interaction (gray square). CMFGEN models plotted as colored octagons, polygons, diamonds, and plus signs. SN 2023ixf has an observed t IIn and peak absolute magnitude that is consistent with the other gold sample SNe II displaying the strongest signs of CSM interaction, e.g., SNe 1998S, 2017ahn, 2020pni, 2020tlf (Leonard et al. 2000; Fassia et al. 2001; Shivvers et al. 2015; Tartaglia et al. 2021; Terreran et al. 2022;W. V. Jacobson-Galán et al. 2023, in preparation).
Paper: SN 2023ixf in Messier 101: Photo-ionization of Dense, Close-in Circumstellar Material in a Nearby Type II Supernova
Authors: W. V. Jacobson-Galán, L. Dessart, R. Margutti, R. Chornock, R. J. Foley, C. D. Kilpatrick, D. O. Jones, K. Taggart, C. R. Angus, S. Bhattacharjee, L. A. Braff, D. Brethauer, A. J. Burgasser, F. Cao, C. M. Carlile, K. C. Chambers, D. A. Coulter, E. Dominguez-Ruiz, C. B. Dickinson, T. de Boer, A. Gagliano, C. Gall, H. Gao, E. L. Gates, S. Gomez, M. Guolo, M. R. J. Halford, J. Hjorth, M. E. Huber, M. N. Johnson, P. R. Karpoor, T. Laskar, N LeBaron, Z. Li, Y. Lin, S. D. Loch, P. D. Lynam, E. A. Magnier, P. Maloney, D. J. Matthews, M. McDonald, H.-Y. Miao, D. Milisavljevic, Y.-C. Pan, S. Pradyumna, C. L. Ransome, J. M. Rees, A. Rest, C. Rojas-Bravo, N. R. Sandford, L. Sandoval Ascencio, S. Sanjaripour, A. Savino, H. Sears, N. Sharei, S. J. Smartt, E. R. Softich, C. A. Theissen, S. Tinyanont, H. Tohfa, V. A. Villar, Q. Wang, R. J. Wainscoat, A. L. Westerling, E. Wiston, M. A. Wozniak, S. K. Yadavalli, Y. Zenati
Figure caption: Early time spectra of SNe II with varying degrees of CSM interaction, selected from W. V. Jacobson-Galán et al. (2023, in preparation). Colors delineate differences between duration of IIn-like signatures as well as the presence of different high-ionization species at phases of t ≈ 2 days (e.g., spectra in blue show N III while others do not). Overplotted in gray are best fitting CMFGEN models for high (10−1 M ⊙ yr−1; top) to low (10−5 M ⊙ yr−1; bottom) mass-loss rates. SN 2023ixf lies within the continuum of CSM-interacting SNe II, and the evolution of its prominent spectral signatures of photoionized CSM is consistent with a progenitor mass-loss rate of ﹩\dot{M}={10}^{-2}\,{M}_{\odot }﹩ yr−1.
Paper: SN 2023ixf in Messier 101: Photo-ionization of Dense, Close-in Circumstellar Material in a Nearby Type II Supernova
Authors: W. V. Jacobson-Galán, L. Dessart, R. Margutti, R. Chornock, R. J. Foley, C. D. Kilpatrick, D. O. Jones, K. Taggart, C. R. Angus, S. Bhattacharjee, L. A. Braff, D. Brethauer, A. J. Burgasser, F. Cao, C. M. Carlile, K. C. Chambers, D. A. Coulter, E. Dominguez-Ruiz, C. B. Dickinson, T. de Boer, A. Gagliano, C. Gall, H. Gao, E. L. Gates, S. Gomez, M. Guolo, M. R. J. Halford, J. Hjorth, M. E. Huber, M. N. Johnson, P. R. Karpoor, T. Laskar, N LeBaron, Z. Li, Y. Lin, S. D. Loch, P. D. Lynam, E. A. Magnier, P. Maloney, D. J. Matthews, M. McDonald, H.-Y. Miao, D. Milisavljevic, Y.-C. Pan, S. Pradyumna, C. L. Ransome, J. M. Rees, A. Rest, C. Rojas-Bravo, N. R. Sandford, L. Sandoval Ascencio, S. Sanjaripour, A. Savino, H. Sears, N. Sharei, S. J. Smartt, E. R. Softich, C. A. Theissen, S. Tinyanont, H. Tohfa, V. A. Villar, Q. Wang, R. J. Wainscoat, A. L. Westerling, E. Wiston, M. A. Wozniak, S. K. Yadavalli, Y. Zenati
Figure caption: (a) Hα velocity evolution in SN 2023ixf from δt = 2.4 to 14.4 days with respect to r1w6b model spectra (red), which has been scaled to the emission line peaks of SN 2023ixf and smoothed with a Gaussian filter to better compare with the data. Early time spectral profiles are shaped by electron-scattering in the dense CSM. The transition shown from black to blue lines (t IIn ≈ 8 days) marks the emergence of broad absorption features derived from the fastest moving SN ejecta. (b) Hβ velocity evolution, also showing that the electron-scattering line profiles subside after ∼8 days. (c) He II λ4686 velocity evolution reveals that the electron-scattering profile fades by ∼8 days, suggesting a significant decrease in CSM density.
Paper: SN 2023ixf in Messier 101: Photo-ionization of Dense, Close-in Circumstellar Material in a Nearby Type II Supernova
Authors: W. V. Jacobson-Galán, L. Dessart, R. Margutti, R. Chornock, R. J. Foley, C. D. Kilpatrick, D. O. Jones, K. Taggart, C. R. Angus, S. Bhattacharjee, L. A. Braff, D. Brethauer, A. J. Burgasser, F. Cao, C. M. Carlile, K. C. Chambers, D. A. Coulter, E. Dominguez-Ruiz, C. B. Dickinson, T. de Boer, A. Gagliano, C. Gall, H. Gao, E. L. Gates, S. Gomez, M. Guolo, M. R. J. Halford, J. Hjorth, M. E. Huber, M. N. Johnson, P. R. Karpoor, T. Laskar, N LeBaron, Z. Li, Y. Lin, S. D. Loch, P. D. Lynam, E. A. Magnier, P. Maloney, D. J. Matthews, M. McDonald, H.-Y. Miao, D. Milisavljevic, Y.-C. Pan, S. Pradyumna, C. L. Ransome, J. M. Rees, A. Rest, C. Rojas-Bravo, N. R. Sandford, L. Sandoval Ascencio, S. Sanjaripour, A. Savino, H. Sears, N. Sharei, S. J. Smartt, E. R. Softich, C. A. Theissen, S. Tinyanont, H. Tohfa, V. A. Villar, Q. Wang, R. J. Wainscoat, A. L. Westerling, E. Wiston, M. A. Wozniak, S. K. Yadavalli, Y. Zenati
Figure caption: Hα velocity of SN 2023ixf at δ t = 2.4 days (black) with respect to CMFGEN model spectra at +2 days post-explosion. Best-fit models (e.g., Section 3.3) shown as solid lines; additional, inconsistent models plotted as dotted lines. For proper comparison, models are scaled to the continuum of SN 2023ixf and the peak of the presented emission line profile. These models have varying mass-loss rates that are contained within CSM radii of (a) R CSM = (4–6) × 1014 cm, (b) R CSM = (0.8–1) × 1015 cm, and (c) R CSM = 1016 cm. (d), (e), (f) Same as above, but for He II velocities.
Paper: SN 2023ixf in Messier 101: Photo-ionization of Dense, Close-in Circumstellar Material in a Nearby Type II Supernova
Authors: W. V. Jacobson-Galán, L. Dessart, R. Margutti, R. Chornock, R. J. Foley, C. D. Kilpatrick, D. O. Jones, K. Taggart, C. R. Angus, S. Bhattacharjee, L. A. Braff, D. Brethauer, A. J. Burgasser, F. Cao, C. M. Carlile, K. C. Chambers, D. A. Coulter, E. Dominguez-Ruiz, C. B. Dickinson, T. de Boer, A. Gagliano, C. Gall, H. Gao, E. L. Gates, S. Gomez, M. Guolo, M. R. J. Halford, J. Hjorth, M. E. Huber, M. N. Johnson, P. R. Karpoor, T. Laskar, N LeBaron, Z. Li, Y. Lin, S. D. Loch, P. D. Lynam, E. A. Magnier, P. Maloney, D. J. Matthews, M. McDonald, H.-Y. Miao, D. Milisavljevic, Y.-C. Pan, S. Pradyumna, C. L. Ransome, J. M. Rees, A. Rest, C. Rojas-Bravo, N. R. Sandford, L. Sandoval Ascencio, S. Sanjaripour, A. Savino, H. Sears, N. Sharei, S. J. Smartt, E. R. Softich, C. A. Theissen, S. Tinyanont, H. Tohfa, V. A. Villar, Q. Wang, R. J. Wainscoat, A. L. Westerling, E. Wiston, M. A. Wozniak, S. K. Yadavalli, Y. Zenati
Figure caption: Swift UV grism spectra (gray) with respect to best fitting CMFGEN model (red); y-axis is in units of λ 2 F  λ . The Swift UV grism response function below ∼3200 Å is not reflective of the true slope of the SN spectral energy distribution. The r1w6b model shows that the near-UV and far-UV spectra of SN 2023ixf likely contain a plethora of narrow, high-ionization emission lines (e.g., He II, C IV, N IV/V, and O IV) derived from CSM interaction.
Paper: SN 2023ixf in Messier 101: Photo-ionization of Dense, Close-in Circumstellar Material in a Nearby Type II Supernova
Authors: W. V. Jacobson-Galán, L. Dessart, R. Margutti, R. Chornock, R. J. Foley, C. D. Kilpatrick, D. O. Jones, K. Taggart, C. R. Angus, S. Bhattacharjee, L. A. Braff, D. Brethauer, A. J. Burgasser, F. Cao, C. M. Carlile, K. C. Chambers, D. A. Coulter, E. Dominguez-Ruiz, C. B. Dickinson, T. de Boer, A. Gagliano, C. Gall, H. Gao, E. L. Gates, S. Gomez, M. Guolo, M. R. J. Halford, J. Hjorth, M. E. Huber, M. N. Johnson, P. R. Karpoor, T. Laskar, N LeBaron, Z. Li, Y. Lin, S. D. Loch, P. D. Lynam, E. A. Magnier, P. Maloney, D. J. Matthews, M. McDonald, H.-Y. Miao, D. Milisavljevic, Y.-C. Pan, S. Pradyumna, C. L. Ransome, J. M. Rees, A. Rest, C. Rojas-Bravo, N. R. Sandford, L. Sandoval Ascencio, S. Sanjaripour, A. Savino, H. Sears, N. Sharei, S. J. Smartt, E. R. Softich, C. A. Theissen, S. Tinyanont, H. Tohfa, V. A. Villar, Q. Wang, R. J. Wainscoat, A. L. Westerling, E. Wiston, M. A. Wozniak, S. K. Yadavalli, Y. Zenati
Figure caption: Time series of the (a) luminosity, (b) density, (c) temperature, and (d) velocity vs. radius for best fitting CMFGEN model r1w6b. Circles show the location of the photosphere, which resides in the slow moving CSM until ∼8 days and after which recedes into the fast-moving dense shell. The model phases begin at the onset of the radiation hydrodynamics simulation, which is ∼1 hr before the shock crosses the progenitor radius (as given in the progenitor stellar model, i.e., without CSM).
Paper: Water Absorption in the Transmission Spectrum of the Water World Candidate GJ 9827 d
Authors: Pierre-Alexis Roy, Björn Benneke, Caroline Piaulet, Michael A. Gully-Santiago, Ian J. M. Crossfield, Caroline V. Morley, Laura Kreidberg, Thomas Mikal-Evans, Jonathan Brande, Simon Delisle, Thomas P. Greene, Kevin K. Hardegree-Ullman, Travis Barman, Jessie L. Christiansen, Diana Dragomir, Jonathan J. Fortney, Andrew W. Howard, Molly R. Kosiarek, Joshua D. Lothringer
Figure caption: Water detection in the transmission spectrum of GJ 9827 d. Left: transmission spectrum of GJ 9827 d (black points) shown with our model transmission spectrum constraints from the nested sampling atmosphere retrieval (blue) and the photometry-informed TLS retrieval (orange). The dark blue and light blue shaded regions show the 1σ and 2σ Bayesian credible intervals from the atmosphere retrieval, respectively. The atmospheric median transmission model is shown in blue, and the best-fitting model is shown in red. The best-fitting TLS model is shown in orange along with the 1σ and 2σ Bayesian credible intervals in light orange. Right: joint constraints on the cloud-top pressure vs. the water mixing ratio derived from our SCARLET well-mixed retrieval. The colored shading describes the normalized probability density as a function of the water mixing ratio (assuming uniform vertical profiles) of the atmosphere and cloud-top pressure. The black contours highlight the 1σ, 2σ, and 3σ Bayesian credible regions. The water abundance relative to a solar composition atmosphere is shown on the top axis. The posterior probability distribution allows for multiple atmospheric scenarios ranging from H2/He envelopes with small amounts of water to water-dominated envelopes. The blue points identify two representative samples of these two scenarios, which are displayed in Figure 6.
Paper: Water Absorption in the Transmission Spectrum of the Water World Candidate GJ 9827 d
Authors: Pierre-Alexis Roy, Björn Benneke, Caroline Piaulet, Michael A. Gully-Santiago, Ian J. M. Crossfield, Caroline V. Morley, Laura Kreidberg, Thomas Mikal-Evans, Jonathan Brande, Simon Delisle, Thomas P. Greene, Kevin K. Hardegree-Ullman, Travis Barman, Jessie L. Christiansen, Diana Dragomir, Jonathan J. Fortney, Andrew W. Howard, Molly R. Kosiarek, Joshua D. Lothringer
Figure caption: The HST/WFC3 transmission spectrum of GJ 9827 d (data points) along with SCARLET forward atmosphere models (colored lines). In the top panel, two samples from our well-mixed retrieval analysis (Figure 4) are shown, representing the mini-Neptune scenario with a cloudy H2/He atmosphere composed of ∼1% water (light blue) and a water world scenario with a water-rich atmosphere (dark blue). In the middle panel, a secondary atmosphere model for a pure methane envelope is also shown (magenta) in order to highlight the methane absorption features. Chemically consistent models (still assuming a uniform temperature profile) are shown for a cloud-free solar composition case (solar metallicity, solar C/O; orange) and a cloudy case with C/O = 0.1 and a 100× solar metallicity (green). The observed spectrum is inconsistent with cloud-free low-metallicity scenarios and prefers water absorption features to methane absorption features, mainly around 1.2 and 1.65 μm. The strength of the features in the spectrum is also displayed in units of H/He scale heights (right axis). In the bottom panel, the best-fit model from the retrieval analysis is shown (light blue) along with the transmission spectrum of the same model once the water opacity is turned off (gray). The contribution of water opacity to the spectral signatures is highlighted in blue. We also present a binned version of the transmission spectrum, where the points are binned together by pair with the exception of the blue-most channel.