adsabs/AstroCLIMB huggingface dataset:
Paper: A CEERS Discovery of an Accreting Supermassive Black Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars
Authors: Rebecca L. Larson, Steven L. Finkelstein, Dale D. Kocevski, Taylor A. Hutchison, Jonathan R. Trump, Pablo Arrabal Haro, Volker Bromm, Nikko J. Cleri, Mark Dickinson, Seiji Fujimoto, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Casey Papovich, Nor Pirzkal, Sandro Tacchella, Jorge A. Zavala, Micaela Bagley, Peter Behroozi, Jaclyn B. Champagne, Justin W. Cole, Intae Jung, Alexa M. Morales, Guang Yang, Haowen Zhang, Adi Zitrin, Ricardo O. Amorín, Denis Burgarella, Caitlin M. Casey, Óscar A. Chávez Ortiz, Isabella G. Cox, Katherine Chworowsky, Adriano Fontana, Eric Gawiser, Andrea Grazian, Norman A. Grogin, Santosh Harish, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Stéphanie Juneau, Gene C. K. Leung, Ray A. Lucas, Elizabeth J. McGrath, Pablo G. Pérez-González, Jane R. Rigby, Lise-Marie Seillé, Raymond C. Simons, Alexander de la Vega, Benjamin J. Weiner, Stephen M. Wilkins, L. Y. Aaron Yung
Figure caption: The “OHNO” diagram, the line ratio diagnostic using [O III]5008/Hβ vs.  [Ne III]3870/[O II]3727+3729, with the black curve showing the boundary between star-forming and AGN regions at z ∼ 1 (as defined in Backhaus et al. 2022, with the shaded region showing the star-forming area). The orange stars are from this work, representing the narrow component fit (big star) and the single-Gaussian fit (to the full profile; small star) of the Hβ emission line in our galaxy. The black polygons represent other high-redshift (z > 5) galaxies with JWST/NIRSpec observations (Trump et al. 2023; Kocevski et al. 2023; Tang et al. 2023). Underplotted on both panels are photoionization models, with the left panel showing star-forming (blue) and AGN models (red) using the CLOUDY v17 code (Ferland et al. 2017) and the right panel showing star-forming models (green) from Kewley et al. (2019a) using the MAPPINGS V code (Sutherland et al. 2018). Each line of points represents a specific set of ionization parameters of log10 U = [−2.5, −2.1, −1.5] for the CLOUDY models and log10 U = [−2.5, −1.5] for the MAPPINGS models, with increasing ionization toward darker colors (or toward the top right of each panel). For the MAPPINGS models, the lines are further separated by isobaric pressure (denoted by line type). The sizes of the points represent the metallicities of the models.
Paper: A CEERS Discovery of an Accreting Supermassive Black Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars
Authors: Rebecca L. Larson, Steven L. Finkelstein, Dale D. Kocevski, Taylor A. Hutchison, Jonathan R. Trump, Pablo Arrabal Haro, Volker Bromm, Nikko J. Cleri, Mark Dickinson, Seiji Fujimoto, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Casey Papovich, Nor Pirzkal, Sandro Tacchella, Jorge A. Zavala, Micaela Bagley, Peter Behroozi, Jaclyn B. Champagne, Justin W. Cole, Intae Jung, Alexa M. Morales, Guang Yang, Haowen Zhang, Adi Zitrin, Ricardo O. Amorín, Denis Burgarella, Caitlin M. Casey, Óscar A. Chávez Ortiz, Isabella G. Cox, Katherine Chworowsky, Adriano Fontana, Eric Gawiser, Andrea Grazian, Norman A. Grogin, Santosh Harish, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Stéphanie Juneau, Gene C. K. Leung, Ray A. Lucas, Elizabeth J. McGrath, Pablo G. Pérez-González, Jane R. Rigby, Lise-Marie Seillé, Raymond C. Simons, Alexander de la Vega, Benjamin J. Weiner, Stephen M. Wilkins, L. Y. Aaron Yung
Figure caption: Mass of BHs vs. redshift. The gold star represents the result of this work. The green points denote published z = 6–7.64 quasars, taken from the compilation of Inayoshi et al. (2020) and augmented by more recent z > 7 quasars from Fan et al. (2022). The different lines show potential tracks of BH growth. The purple lines show a 100 M⊙ Population III stellar remnant seed forming at z ∼ 30, with growth beginning after a 100 Myr delay due to progenitor gas heating. The dashed purple line shows constant Eddington growth, which is both likely unphysical and cannot reproduce our observed object mass. The solid line shows one example of how periods of super-Eddington growth (10 times Eddington for 10 Myr) separated by periods of sub-Eddington growth (0.1 times Eddington for 50 Myr) could plausibly create the observed source. The red lines show potential formation mechanisms from a small (3×104 M ⊙) DCBH forming at z = 15 (dotted) and a large (106 M ⊙) DCBH forming at z = 10.5 (dashed), each growing at the Eddington rate. Either of the mechanisms that could explain our observed BH source, DCBH+Eddington or stellar+super-Eddington, are somewhat exotic scenarios, pushing standard assumptions. Probing SMBHs out to higher redshifts and lower masses will clarify the formation mechanisms of these objects.
Paper: A CEERS Discovery of an Accreting Supermassive Black Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars
Authors: Rebecca L. Larson, Steven L. Finkelstein, Dale D. Kocevski, Taylor A. Hutchison, Jonathan R. Trump, Pablo Arrabal Haro, Volker Bromm, Nikko J. Cleri, Mark Dickinson, Seiji Fujimoto, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Casey Papovich, Nor Pirzkal, Sandro Tacchella, Jorge A. Zavala, Micaela Bagley, Peter Behroozi, Jaclyn B. Champagne, Justin W. Cole, Intae Jung, Alexa M. Morales, Guang Yang, Haowen Zhang, Adi Zitrin, Ricardo O. Amorín, Denis Burgarella, Caitlin M. Casey, Óscar A. Chávez Ortiz, Isabella G. Cox, Katherine Chworowsky, Adriano Fontana, Eric Gawiser, Andrea Grazian, Norman A. Grogin, Santosh Harish, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Stéphanie Juneau, Gene C. K. Leung, Ray A. Lucas, Elizabeth J. McGrath, Pablo G. Pérez-González, Jane R. Rigby, Lise-Marie Seillé, Raymond C. Simons, Alexander de la Vega, Benjamin J. Weiner, Stephen M. Wilkins, L. Y. Aaron Yung
Figure caption: The images show ﹩{5}^{{\prime} ^{\prime} }﹩×﹩{5}^{{\prime} ^{\prime} }﹩ cutouts around this source in the CANDELS HST/ACS optical bands, CEERS NIRCam near-infrared bands, and CEERS MIRI bands. The source is a clear dropout in the optical and is well detected at 1–8 μm. The large inset plot shows the photometric SED from HST and JWST. We also show Spitzer/IRAC measurements from Finkelstein et al. (2022a) with both TPHOT (light gray) and Galfit (dark gray); this source was highly blended in IRAC, and the Galfit measurements appear closer to the NIRCam measurements. The lines are best-fit models from Prospector (gray) and BAGPIPES (purple). The SED is dominated by stellar emission (Section 5), and these stellar models infer a massive (log M/M⊙ ∼ 9.5) and highly star-forming (log sSFR ∼ − 7.9 Gyr−1) stellar population. The small inset panel shows constraints on the photometric redshift before (green) and after (red and yellow) the inclusion of JWST data. All three are consistent with the spectroscopic redshift, with those including JWST data placing much tighter constraints.
Paper: A CEERS Discovery of an Accreting Supermassive Black Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars
Authors: Rebecca L. Larson, Steven L. Finkelstein, Dale D. Kocevski, Taylor A. Hutchison, Jonathan R. Trump, Pablo Arrabal Haro, Volker Bromm, Nikko J. Cleri, Mark Dickinson, Seiji Fujimoto, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Casey Papovich, Nor Pirzkal, Sandro Tacchella, Jorge A. Zavala, Micaela Bagley, Peter Behroozi, Jaclyn B. Champagne, Justin W. Cole, Intae Jung, Alexa M. Morales, Guang Yang, Haowen Zhang, Adi Zitrin, Ricardo O. Amorín, Denis Burgarella, Caitlin M. Casey, Óscar A. Chávez Ortiz, Isabella G. Cox, Katherine Chworowsky, Adriano Fontana, Eric Gawiser, Andrea Grazian, Norman A. Grogin, Santosh Harish, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Stéphanie Juneau, Gene C. K. Leung, Ray A. Lucas, Elizabeth J. McGrath, Pablo G. Pérez-González, Jane R. Rigby, Lise-Marie Seillé, Raymond C. Simons, Alexander de la Vega, Benjamin J. Weiner, Stephen M. Wilkins, L. Y. Aaron Yung
Figure caption: The predicted z = 8.7 median M • − M * relation for quasars with different bolometric luminosity thresholds from the TRINITY model (solid curves; Zhang et al. 2023a, 2023b). The pink shaded region is the 1 − σ spread around the median scaling relation for quasars (∼0.55 dex), which includes the random scatter in observed M • when using virial estimates. This (log-)normal scatter is nearly luminosity-independent, so we only show it for the brightest quasars for clarity. The black solid line is the predicted M • − M * relation for all SMBHs at z = 8.7, and the black shaded region is the intrinsic+observed scatter around the intrinsic M • − M * relation. The green solid line is the M • − M * relation for AGNs brighter than ﹩\mathrm{log}{L}_{\mathrm{bol}}[\mathrm{erg}/{\rm{s}}]\geqslant 45.1﹩, corresponding to the bolometric luminosity of the AGN in this work (gold star). For comparison, we also show the z = 0 relation from Greene et al. (2016) with the black dashed line and the z = 0 AGN sample from Reines & Volonteri (2015) with the black crosses. The following data are shown in symbols color-coded by bolometric AGN luminosities: (1) z ∼ 6 quasars compiled by Izumi et al. (2021) and Übler et al. (2023; filled circles); and (2) the two z > 5 AGNs from Kocevski et al. (2023; pentagons).
Paper: A CEERS Discovery of an Accreting Supermassive Black Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars
Authors: Rebecca L. Larson, Steven L. Finkelstein, Dale D. Kocevski, Taylor A. Hutchison, Jonathan R. Trump, Pablo Arrabal Haro, Volker Bromm, Nikko J. Cleri, Mark Dickinson, Seiji Fujimoto, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Casey Papovich, Nor Pirzkal, Sandro Tacchella, Jorge A. Zavala, Micaela Bagley, Peter Behroozi, Jaclyn B. Champagne, Justin W. Cole, Intae Jung, Alexa M. Morales, Guang Yang, Haowen Zhang, Adi Zitrin, Ricardo O. Amorín, Denis Burgarella, Caitlin M. Casey, Óscar A. Chávez Ortiz, Isabella G. Cox, Katherine Chworowsky, Adriano Fontana, Eric Gawiser, Andrea Grazian, Norman A. Grogin, Santosh Harish, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Stéphanie Juneau, Gene C. K. Leung, Ray A. Lucas, Elizabeth J. McGrath, Pablo G. Pérez-González, Jane R. Rigby, Lise-Marie Seillé, Raymond C. Simons, Alexander de la Vega, Benjamin J. Weiner, Stephen M. Wilkins, L. Y. Aaron Yung
Figure caption: Left: dual-component Gaussian fit to the Hβ emission line (green), yielding FWHMbroad = 1196.3 ± 349.1 km s−1 and FWHMnar = 354.8 ±  19.6 km s−1. Alternative single-Gaussian line profile fits are shown where the FWHM is restricted to FWHM [O III]  ±  30 km s−1 (blue) or left unrestricted (purple). In both cases, the fit to the Hβ emission line is worse than the dual-component fits, as indicated by the higher Bayesian Information Criterion (BIC) measurement (Section 4.2). Right: scaled-down fits of the same dual-component fit from Hβ to the peak of the Hδ (top) and Hγ (bottom) emission lines. In both cases, the broad component is not distinguishable from the noise, indicating that a broad component could be present in these lines below our noise threshold.
Paper: A CEERS Discovery of an Accreting Supermassive Black Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars
Authors: Rebecca L. Larson, Steven L. Finkelstein, Dale D. Kocevski, Taylor A. Hutchison, Jonathan R. Trump, Pablo Arrabal Haro, Volker Bromm, Nikko J. Cleri, Mark Dickinson, Seiji Fujimoto, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Casey Papovich, Nor Pirzkal, Sandro Tacchella, Jorge A. Zavala, Micaela Bagley, Peter Behroozi, Jaclyn B. Champagne, Justin W. Cole, Intae Jung, Alexa M. Morales, Guang Yang, Haowen Zhang, Adi Zitrin, Ricardo O. Amorín, Denis Burgarella, Caitlin M. Casey, Óscar A. Chávez Ortiz, Isabella G. Cox, Katherine Chworowsky, Adriano Fontana, Eric Gawiser, Andrea Grazian, Norman A. Grogin, Santosh Harish, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Stéphanie Juneau, Gene C. K. Leung, Ray A. Lucas, Elizabeth J. McGrath, Pablo G. Pérez-González, Jane R. Rigby, Lise-Marie Seillé, Raymond C. Simons, Alexander de la Vega, Benjamin J. Weiner, Stephen M. Wilkins, L. Y. Aaron Yung
Figure caption: Combined JWST/NIRSpec spectrum from G140M+G235M+G395M of CEERS_1019, plotted in F λ  [10−19 erg s−1 cm−2 Å−1] vs. observed wavelength [ μm]. Plotted in green is the fit to the continuum in the spectrum (see Section 3.1) plus the detected emission lines, as discussed in Section 4. We require an S/N >2.3 (with our simulation-estimated noise as described in Section 3.2) for a line to be considered detected.
Paper: A CEERS Discovery of an Accreting Supermassive Black Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars
Authors: Rebecca L. Larson, Steven L. Finkelstein, Dale D. Kocevski, Taylor A. Hutchison, Jonathan R. Trump, Pablo Arrabal Haro, Volker Bromm, Nikko J. Cleri, Mark Dickinson, Seiji Fujimoto, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Casey Papovich, Nor Pirzkal, Sandro Tacchella, Jorge A. Zavala, Micaela Bagley, Peter Behroozi, Jaclyn B. Champagne, Justin W. Cole, Intae Jung, Alexa M. Morales, Guang Yang, Haowen Zhang, Adi Zitrin, Ricardo O. Amorín, Denis Burgarella, Caitlin M. Casey, Óscar A. Chávez Ortiz, Isabella G. Cox, Katherine Chworowsky, Adriano Fontana, Eric Gawiser, Andrea Grazian, Norman A. Grogin, Santosh Harish, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Stéphanie Juneau, Gene C. K. Leung, Ray A. Lucas, Elizabeth J. McGrath, Pablo G. Pérez-González, Jane R. Rigby, Lise-Marie Seillé, Raymond C. Simons, Alexander de la Vega, Benjamin J. Weiner, Stephen M. Wilkins, L. Y. Aaron Yung
Figure caption: Fits to the emission lines identified in the JWST/NIRSpec spectrum of CEERS_1019. Each panel shows an individual emission-line fit, with the type of line profile as described in Section 3. The panels are plotted in F  λ  (10−19 erg s−1 cm−2 Å−1) vs. observed wavelength (μm), are presented in order of increasing wavelength, and are scaled vertically to show the extent of the highlighted emission line. Emission-line values are tabulated in Table 3 and discussions of specific lines are given in Section 4.
Paper: A CEERS Discovery of an Accreting Supermassive Black Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars
Authors: Rebecca L. Larson, Steven L. Finkelstein, Dale D. Kocevski, Taylor A. Hutchison, Jonathan R. Trump, Pablo Arrabal Haro, Volker Bromm, Nikko J. Cleri, Mark Dickinson, Seiji Fujimoto, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Casey Papovich, Nor Pirzkal, Sandro Tacchella, Jorge A. Zavala, Micaela Bagley, Peter Behroozi, Jaclyn B. Champagne, Justin W. Cole, Intae Jung, Alexa M. Morales, Guang Yang, Haowen Zhang, Adi Zitrin, Ricardo O. Amorín, Denis Burgarella, Caitlin M. Casey, Óscar A. Chávez Ortiz, Isabella G. Cox, Katherine Chworowsky, Adriano Fontana, Eric Gawiser, Andrea Grazian, Norman A. Grogin, Santosh Harish, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Stéphanie Juneau, Gene C. K. Leung, Ray A. Lucas, Elizabeth J. McGrath, Pablo G. Pérez-González, Jane R. Rigby, Lise-Marie Seillé, Raymond C. Simons, Alexander de la Vega, Benjamin J. Weiner, Stephen M. Wilkins, L. Y. Aaron Yung
Figure caption: From left to right: JWST/NIRCam F277W; Spitzer/MIPS 24  μm; Herschel/PACS 100  μm; and VLA 3 GHz (north is up, east is to the left). All the 20″ × 20″ cutouts are centered on the coordinates of the 6σ SCUBA-2/850  μm detection (yellow contours) found around the location of CEERS_1019 (red circle). The blue cross marks the position of a z ∼ 3 galaxy detected at 24 μm and 3 GHz, which is likely the correct counterpart and the main contributor to the SCUBA-2 detection.
Paper: A CEERS Discovery of an Accreting Supermassive Black Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars
Authors: Rebecca L. Larson, Steven L. Finkelstein, Dale D. Kocevski, Taylor A. Hutchison, Jonathan R. Trump, Pablo Arrabal Haro, Volker Bromm, Nikko J. Cleri, Mark Dickinson, Seiji Fujimoto, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Casey Papovich, Nor Pirzkal, Sandro Tacchella, Jorge A. Zavala, Micaela Bagley, Peter Behroozi, Jaclyn B. Champagne, Justin W. Cole, Intae Jung, Alexa M. Morales, Guang Yang, Haowen Zhang, Adi Zitrin, Ricardo O. Amorín, Denis Burgarella, Caitlin M. Casey, Óscar A. Chávez Ortiz, Isabella G. Cox, Katherine Chworowsky, Adriano Fontana, Eric Gawiser, Andrea Grazian, Norman A. Grogin, Santosh Harish, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Stéphanie Juneau, Gene C. K. Leung, Ray A. Lucas, Elizabeth J. McGrath, Pablo G. Pérez-González, Jane R. Rigby, Lise-Marie Seillé, Raymond C. Simons, Alexander de la Vega, Benjamin J. Weiner, Stephen M. Wilkins, L. Y. Aaron Yung
Figure caption: JWST NIRCam 1.5″ × 1.5″ cutouts of CEERS_1019 in four different filters (F200W, F277W, F356W, and F444W) and an RGB color composite (with blue = F115W + F150W + F200W, green = F277W + F356W + F410M, and red = F444W) with each filter at its native resolution, highlighting the substructure visible at shorter wavelengths. The positions of the NIRSpec MOS shutters are overlaid. This source has a bright central component centered in the shutter and two extended components as discussed in Section 5.2.
Paper: A CEERS Discovery of an Accreting Supermassive Black Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars
Authors: Rebecca L. Larson, Steven L. Finkelstein, Dale D. Kocevski, Taylor A. Hutchison, Jonathan R. Trump, Pablo Arrabal Haro, Volker Bromm, Nikko J. Cleri, Mark Dickinson, Seiji Fujimoto, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Casey Papovich, Nor Pirzkal, Sandro Tacchella, Jorge A. Zavala, Micaela Bagley, Peter Behroozi, Jaclyn B. Champagne, Justin W. Cole, Intae Jung, Alexa M. Morales, Guang Yang, Haowen Zhang, Adi Zitrin, Ricardo O. Amorín, Denis Burgarella, Caitlin M. Casey, Óscar A. Chávez Ortiz, Isabella G. Cox, Katherine Chworowsky, Adriano Fontana, Eric Gawiser, Andrea Grazian, Norman A. Grogin, Santosh Harish, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Stéphanie Juneau, Gene C. K. Leung, Ray A. Lucas, Elizabeth J. McGrath, Pablo G. Pérez-González, Jane R. Rigby, Lise-Marie Seillé, Raymond C. Simons, Alexander de la Vega, Benjamin J. Weiner, Stephen M. Wilkins, L. Y. Aaron Yung
Figure caption: 2D and 1D spectra of the NIRSpec/PRISM spectrum of CEERS_1019, taken in 2022 December, which encountered a short contaminating a majority of the data. We show the spectra here for completeness and also to illustrate that many of the emission lines are visible, including N IV], C III], Hβ, and [O III], even though the data are contaminated.
Paper: A CEERS Discovery of an Accreting Supermassive Black Hole 570 Myr after the Big Bang: Identifying a Progenitor of Massive z > 6 Quasars
Authors: Rebecca L. Larson, Steven L. Finkelstein, Dale D. Kocevski, Taylor A. Hutchison, Jonathan R. Trump, Pablo Arrabal Haro, Volker Bromm, Nikko J. Cleri, Mark Dickinson, Seiji Fujimoto, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Casey Papovich, Nor Pirzkal, Sandro Tacchella, Jorge A. Zavala, Micaela Bagley, Peter Behroozi, Jaclyn B. Champagne, Justin W. Cole, Intae Jung, Alexa M. Morales, Guang Yang, Haowen Zhang, Adi Zitrin, Ricardo O. Amorín, Denis Burgarella, Caitlin M. Casey, Óscar A. Chávez Ortiz, Isabella G. Cox, Katherine Chworowsky, Adriano Fontana, Eric Gawiser, Andrea Grazian, Norman A. Grogin, Santosh Harish, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Stéphanie Juneau, Gene C. K. Leung, Ray A. Lucas, Elizabeth J. McGrath, Pablo G. Pérez-González, Jane R. Rigby, Lise-Marie Seillé, Raymond C. Simons, Alexander de la Vega, Benjamin J. Weiner, Stephen M. Wilkins, L. Y. Aaron Yung
Figure caption: Full-band (0.5–7 keV) X-ray images from Nandra et al. (2015). The format is similar to Figure 12. The left panel shows the original image, where each white pixel indicates one (or multiple) X-ray photon(s). The right panel is a smoothed version of the left. Noise dominates in the region around the source.
Paper: The Interaction between AGN and Starburst Activity in the Circumnuclear Region of NGC 7469 as Viewed with JWST
Authors: Lulu Zhang, Luis C. Ho
Figure caption: The FWHM as a function of wavelength of the PSF models for each slice within the first three channels of the MIRI/MRS data cubes. The PSF models of the stars HD 159222 (gray dots) and HD 163466 (brown dots) are measured from MIRI/MRS observations (ID 1050; PI: B. Vandenbussche) by fitting each slice of the data cubes with a 2D Gaussian function. The black dots in the bottom show the difference between the FWHMs of the two sets of PSF models. The green curves represent the analytical fit of the FWHM as a function of wavelength based on the average FWHMs of the two sets of PSF models (Table 4). The blue line depicts the FWHM of the theoretical MIRI PSF model from WebbPSF, FWHM (″) = 0.31 × λ (μm)/8, which applies to MIRI imaging observations.
Paper: The Interaction between AGN and Starburst Activity in the Circumnuclear Region of NGC 7469 as Viewed with JWST
Authors: Lulu Zhang, Luis C. Ho
Figure caption: Distribution of the power-law index n for the central region of NGC 7469, where smaller n corresponds to higher hot gas fraction, with n derived from the H2 rotational lines assuming a power-law distribution of H2 excitation temperatures.
Paper: The Interaction between AGN and Starburst Activity in the Circumnuclear Region of NGC 7469 as Viewed with JWST
Authors: Lulu Zhang, Luis C. Ho
Figure caption: Distribution of line-of-sight velocity (top) and velocity dispersion (bottom) in the central region of NGC 7469 for the emission lines of (a) [Fe II] 5.340 μm, (b) [Ne II] 12.814 μm, and (c) the narrow and (d) broad components of [Ne III] 15.555 μm. The color bars span the same velocity range in panels (a)–(c).
Paper: The Interaction between AGN and Starburst Activity in the Circumnuclear Region of NGC 7469 as Viewed with JWST
Authors: Lulu Zhang, Luis C. Ho
Figure caption: (a) Diagnostic diagram of PAH band ratios 6.2 μm/7.7 μm vs. 11.3 μm/7.7 μm for spatially resolved bins of 2 × 2 pixels, color-coded according to their locations from the central SFR peak [(ΔX, ΔY) = (0, 0)]. The spatial distribution of (b) PAH 11.3 μm/7.7 μm and (c) PAH 6.2 μm/7.7 μm.
Paper: The Interaction between AGN and Starburst Activity in the Circumnuclear Region of NGC 7469 as Viewed with JWST
Authors: Lulu Zhang, Luis C. Ho
Figure caption: The spatial distribution of mid-IR line ratio diagnostics (a) [Ne III]/[Ne II] and (b) H2 S(0–3)/PAH 7.7 μm.
Paper: Deuterium Escape on Photoevaporating Sub-Neptunes
Authors: Pin-Gao Gu, Howard Chen
Figure caption: Fractionation evolution of the envelope for 5 and 10 M ⊕ at d = 0.2 au with various initial mass fractions of the envelope f evn. Left panels: mass-loss evolution of hydrogen (X H/X H,0 − 1; solid), deuterium (X D/X D,0 − 1; dashed), and helium (X He/X He,0 − 1; dotted). Middle panels: Y evolution. Right panels: D/H evolution. The fractionation between H, D, and He becomes more substantial at later times due to the decrease in the mass-loss rate, leading to the increases in Y and D/H with time. The trend is more prominent for the planet with a smaller initial mass fraction of the gas envelope f env due to the even lower mass-loss rate. Notably, the mass loss of He or D can almost stop at later times, as indicated by the flat curves in the left panels.
Paper: Deuterium Escape on Photoevaporating Sub-Neptunes
Authors: Pin-Gao Gu, Howard Chen
Figure caption: Coevolution of Y (top panels), D/H ratio (bottom panels), and R  p  (color coding) for a grid of planetary models: M  p  = 4, 5, 10, and 15 M ⊕ and f env = 0.001, 0.003, 0.005, 0.1, 0.03, 0.05, and 0.1 at each orbital distance given by d = 0.1, 0.15, 0.2, 0.25, 0.3, 0.35, and 0.4 au. Some data with an anomalous evolution of planet radius are removed (see text). Similar to the evolution of helium-enhanced planets (top panels), the D/H ratios increase with time due to atmospheric escape and have larger values for the photoevaporating sub-Neptunes along the upper edge of the radius valley (i.e., R  p  ≈ 1.8–2 R ⊕).