adsabs/AstroCLIMB huggingface dataset:
Paper: Large-scale Evolution of Seconds-long Relativistic Jets from Black Hole–Neutron Star Mergers
Authors: Ore Gottlieb, Danat Issa, Jonatan Jacquemin-Ide, Matthew Liska, Francois Foucart, Alexander Tchekhovskoy, Brian D. Metzger, Eliot Quataert, Rosalba Perna, Daniel Kasen, Matthew D. Duez, Lawrence E. Kidder, Harald P. Pfeiffer, Mark A. Scheel
Figure caption: Time evolution at r = 5r  g  for different models. Panel (a): mass accretion rate in all models with a magnetized disk features ﹩\dot{M}\propto {t}^{-2}﹩, whereas in the hydrodynamic model H 0, ﹩\dot{M}\propto {t}^{-1}﹩. Panel (b): dimensionless magnetic flux ﹩\phi ={\rm{\Phi }}/\sqrt{\dot{M}{{cr}}_{g}^{2}}﹩, where Φ is the magnetic flux. When the initial profile is a strong poloidal field, the flux reaches an MAD state within t ≲ 1 s. When the initial magnetic field is weaker or purely toroidal, the magnetic flux accumulates slower on the BH horizon, and the MAD onset is delayed. Ultimately, all models turn MAD when ϕ ≈ 50 (dashed line). In panel (c), the jet launching efficiency increases gradually as more flux is threading the BH, until it reaches the maximum launching efficiency η ≈ 0.9 in the MAD state (dashed line). In panel (d), the jet luminosity, ﹩{L}_{j}=\eta \dot{M}{c}^{2}﹩, is roughly constant once the jet launching has been established by virtue of decreasing accretion rate and increasing efficiency. Once the system reaches the MAD state, the jet efficiency saturates, and the jet luminosity falls off proportional to the mass accretion rate.
Paper: Large-scale Evolution of Seconds-long Relativistic Jets from Black Hole–Neutron Star Mergers
Authors: Ore Gottlieb, Danat Issa, Jonatan Jacquemin-Ide, Matthew Liska, Francois Foucart, Alexander Tchekhovskoy, Brian D. Metzger, Eliot Quataert, Rosalba Perna, Daniel Kasen, Matthew D. Duez, Lawrence E. Kidder, Harald P. Pfeiffer, Mark A. Scheel
Figure caption: Panel (a): time evolution of the energy contained in the material with asymptotic proper velocity u ∞ > 3 integrated on the horizon, r  s  = r H (solid lines), at r  s  = 1010 (dashed lines) and r  s  = 3 × 1010 (dashed–dotted lines) cm. The time axis is shifted by the time it takes ultrarelativistic fluid elements to reach r  s , i.e., t − r  s /c. Except for the initial launching, most jets retain their power profile throughout their propagation. In model T  s , the jets are subject to strong mixing; thus, their power drops with radius. Panel (b): isotropic equivalent energy of the homologously expanding gas at r ≳ 1010 cm for magnetized outflows and r > 109 cm for the pure hydrodynamic model H 0. In the absence of relativistic outflows in model H 0, the postmerger evolution results in quasi-isotropic winds. The initial toroidal field takes longer to launch a steady jet, which results in a wider outflow structure. The jet in model P  s  is too powerful to be collimated by the winds. Panel (c): cumulative energy in plasma at r > 1010 cm with magnetization larger than σ, normalized by the total energy. All jets contain at least a few percent of their total energy at high magnetization, σ ≫ 1, suggesting that magnetic processes may play a key role in the sGRB prompt emission.
Paper: Large-scale Evolution of Seconds-long Relativistic Jets from Black Hole–Neutron Star Mergers
Authors: Ore Gottlieb, Danat Issa, Jonatan Jacquemin-Ide, Matthew Liska, Francois Foucart, Alexander Tchekhovskoy, Brian D. Metzger, Eliot Quataert, Rosalba Perna, Daniel Kasen, Matthew D. Duez, Lawrence E. Kidder, Harald P. Pfeiffer, Mark A. Scheel
Figure caption: Panel (a): time evolution of the bound (solid lines) and unbound (dashed lines) ejecta in the different models. When the disk is magnetized, MRI-driven winds and the extended relativistic outflow structure unbind a fraction of the merger debris. Stronger fields lead to earlier and stronger outflows. Panel (b): 3D rendering of the system at 33 ms postmerger in simulation P  c , with colors reflecting the mass density for nonrelativistic gas and proper velocity for relativistic gas (the spin axis direction is up, and the jet–cocoon outflow extends to r ≈ 2000 km). The jets (white) are launched from the BH into the expanding disk winds (red), generating a cocoon (light blue). The bound tidal tail becomes part of the accretion disk, whereas the unbound tail, shown as the extended yellow component on the right, expands along the equatorial plane.
Paper: Large-scale Evolution of Seconds-long Relativistic Jets from Black Hole–Neutron Star Mergers
Authors: Ore Gottlieb, Danat Issa, Jonatan Jacquemin-Ide, Matthew Liska, Francois Foucart, Alexander Tchekhovskoy, Brian D. Metzger, Eliot Quataert, Rosalba Perna, Daniel Kasen, Matthew D. Duez, Lawrence E. Kidder, Harald P. Pfeiffer, Mark A. Scheel
Figure caption: Volume rendering of the final snapshot of each simulation (see Table 1). The outflows in the poloidal field configurations reach r ≈ ct, whereas in model T  s , the outflow front is at r ≈ 6.4 × 1010 cm. The BH spin axis direction is up, and different colors show different quantities. The asymptotic proper velocity is depicted in blue, revealing the presence of a sub- and mildly relativistic cocoon (dark) surrounding relativistic jets (light). Red and yellow components represent the mass density, showing the merger ejecta and the accretion disk components, respectively. See full movies of models T  s  and P  c  at http://www.oregottlieb.com/bhns.html.
Paper: Large-scale Evolution of Seconds-long Relativistic Jets from Black Hole–Neutron Star Mergers
Authors: Ore Gottlieb, Danat Issa, Jonatan Jacquemin-Ide, Matthew Liska, Francois Foucart, Alexander Tchekhovskoy, Brian D. Metzger, Eliot Quataert, Rosalba Perna, Daniel Kasen, Matthew D. Duez, Lawrence E. Kidder, Harald P. Pfeiffer, Mark A. Scheel
Figure caption: Panel (a): radial profile of the density-averaged angular momentum, l, normalized to the nonrelativistic expression of the Keplerian angular momentum at r  g  at different times. The Keplerian angular momentum profile, l  k (r) ∝ r 1/2 (dotted black line), illustrates that the angular momentum profile is always sub-Keplerian. Panel (b): radial profile of the density-averaged physical radial velocity, ﹩{u}_{\hat{r}}=\sqrt{{g}_{{rr}}}{u}^{r}﹩, normalized to the local Keplerian velocity, V  K (r) ∝ r −1/2, at different times. The radial flux of angular momentum drives accretion in the inner regions and radial outflow in the outer regions.
Paper: Large-scale Evolution of Seconds-long Relativistic Jets from Black Hole–Neutron Star Mergers
Authors: Ore Gottlieb, Danat Issa, Jonatan Jacquemin-Ide, Matthew Liska, Francois Foucart, Alexander Tchekhovskoy, Brian D. Metzger, Eliot Quataert, Rosalba Perna, Daniel Kasen, Matthew D. Duez, Lawrence E. Kidder, Harald P. Pfeiffer, Mark A. Scheel
Figure caption: Same as Figure 1 but for model configuration P  c  with different resolutions, original (P  c ) and high-resolution (P  c,HR), where the resolution in the disk is doubled in all three dimensions. Negligible differences are seen at all times in all quantities, indicating that the simulations are converged.
Paper: Large-scale Evolution of Seconds-long Relativistic Jets from Black Hole–Neutron Star Mergers
Authors: Ore Gottlieb, Danat Issa, Jonatan Jacquemin-Ide, Matthew Liska, Francois Foucart, Alexander Tchekhovskoy, Brian D. Metzger, Eliot Quataert, Rosalba Perna, Daniel Kasen, Matthew D. Duez, Lawrence E. Kidder, Harald P. Pfeiffer, Mark A. Scheel
Figure caption: Relative deviations from the azimuthally averaged surface density profile, ﹩{\rm{\Sigma }}/\overline{{\rm{\Sigma }}}-1﹩, taken 0.5 s after the merger. Here Σ(r, φ) is the surface density, and ﹩\overline{{\rm{\Sigma }}}(r)﹩ is the azimuthally averaged surface density.
Paper: Large-scale Evolution of Seconds-long Relativistic Jets from Black Hole–Neutron Star Mergers
Authors: Ore Gottlieb, Danat Issa, Jonatan Jacquemin-Ide, Matthew Liska, Francois Foucart, Alexander Tchekhovskoy, Brian D. Metzger, Eliot Quataert, Rosalba Perna, Daniel Kasen, Matthew D. Duez, Lawrence E. Kidder, Harald P. Pfeiffer, Mark A. Scheel
Figure caption: Azimuthal angle (φ) averaged β  p  on the equator at the start of the simulation for each of the models, weighted by density.
Paper: Large-scale Evolution of Seconds-long Relativistic Jets from Black Hole–Neutron Star Mergers
Authors: Ore Gottlieb, Danat Issa, Jonatan Jacquemin-Ide, Matthew Liska, Francois Foucart, Alexander Tchekhovskoy, Brian D. Metzger, Eliot Quataert, Rosalba Perna, Daniel Kasen, Matthew D. Duez, Lawrence E. Kidder, Harald P. Pfeiffer, Mark A. Scheel
Figure caption: Relative difference in the φ-averaged specific internal energy (left) and specific angular momentum (right) before and after the remapping procedure. The largest differences, which do not exceed ∼10%, are seen in the region surrounding the BH, where the SpEC metric differs the most from the time-independent Kerr metric, and the difference is even smaller at larger radii.
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: The SEDs of the two low-luminosity AGNs (CEERS 2782 and CEERS 746) obtained with the JSWT NIRSpec and NIRCam. (a) The continuum spectral shape is explained by the composite quasar spectrum of VB01 scaled to match the photometry of CEERS 2782 (blue) and is fitted well with a single power law with an index of α  λ  = − 1.14 (dashed). The galaxy SED model with M ⋆ ≃ 2.5 × 109 M ⊙ is overlaid (red), where the stellar continuum in the F356W filter becomes comparable to the observed F356W flux density. This gives a robust upper bound of the underlying stellar population. (b) The source has a blue continuum spectrum with a UV slope of α  λ  < − 3.0 at λ obs ≃ 1–2 μm and a very steep continuum spectrum (α  λ  ≃ 2.0). The redder part can be explained by either a heavily obscured quasar (cyan) or a dusty starburst galaxy (red). As a possible explanation of the blue excess in the spectrum, the unobscured broad-line AGN contribution is added to the dusty starburst galaxy (blue). In the dusty galaxy model, the stellar mass is found to be M ⋆ ≃ 5.5 × 1010 M ⊙ (see the text in Section 6.3).
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: (a) The BPT emission-line diagnostic diagram. The gray contours denote the distribution of local star-forming galaxies and AGNs as measured by the SDSS (York et al. 2000). Black diamonds denote stacked line ratios of CEERS galaxies at z ∼ 5.6, z ∼ 4.5, and z ∼ 3.3 (Sanders et al. 2023). The black- long and short-dashed lines denote the z = 0 and z = 2.3 boundary between the star-forming and AGN regions of the diagram defined by Kauffmann et al. (2003) and Kewley et al. (2013b), respectively. (b) The OHNO diagnostic diagram. Black squares denote line ratios of SMACS ERO galaxies at 5.3 < z < 8.5 (Trump et al. 2023), and gray contours denote the distribution of z ∼ 0 SDSS galaxies. The dashed line denotes the boundary between star-forming and AGN regions as defined in Backhaus et al. (2022). Colored curves in both panels show MAPPINGS V photoionization models (Kewley et al. 2019). The three color-coded sets of curves and points along those curves correspond to different ionization parameters and metallicities, as indicated by the legends, with three curves for each color corresponding to different gas pressures as described in the text. Both of our z ∼ 5 AGNs have narrow-line ratios that are consistent with low metallicity and high ionization, with little difference from the emission-line ratios observed for other populations of high-redshift galaxies.
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 G395M 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 locations of several prominent emission lines 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: JWST NIRCam images of our broad-line AGN sample at z > 5 taken in the short-wavelength (F150W and F200W) and long-wavelength (F277W, F356W, and F444W) filters. The RGB images are composed of images in the F150W, F277W, and F444W filters. All images are 2″ ×  2″ in size. The alignment of the NIRSpec microshutter aperture relative to each source is shown in red overlaying the F444W image.
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: The rest-frame spectra (black histograms) and associated uncertainty (gray error bars) of both sources in regions with emission-line features. Red lines show the best-fit Gaussians for narrow emission lines, and the blue line shows the best-fit broad component for Hα, which have an FWHM of 2060 ± 286 km s−1 and 1802 ± 204 km s−1 for CEERS 2782 and CEERS 746, respectively.
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 fits for CEERS 746. Top panel: best-fit 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 * = 5.5 × 1010 M ⊙. Bottom panel: an alternative SED fit assuming that nuclear light dominates the emission at all wavelengths and that the observed blue excess is due to scattered light from a patchy obscuring medium. The best-fit SED (green) is the linear combination of a heavily obscured quasar with A  V  = 4.0 (red) and an unobscured quasar (blue). See Section 6.3 for details.
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: The BH mass vs. stellar mass relation of CEERS 2782 (red) and CEERS 746 (orange; A  V  = 4). Circles show the z > 6 quasar samples compiled by Izumi et al. (2021): brighter ones with M 1450 < − 25 mag (blue), and fainter ones with M 1450 > − 25 mag (cyan). The gray and green crosses are the observational samples in the local Universe provided by Kormendy & Ho (2013) and Reines & Volonteri (2015), respectively. The diagonal dashed lines represent M BH/M ⋆ = 0.1, 0.01, and 10−3.
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: The BH mass–bolometric luminosity plane. Quasar samples at z ≥ 5 are shown as blue and green symbols and contours, while low-redshift AGNs are shown in black. CEERS 2782 and CEERS 746 have BH masses 1–2 dex below those of known high-redshift quasars and more comparable to those of typical nearby AGNs. Two z > 5 AGNs recently discovered by JWST are also shown for comparison (light blue; Larson et al. 2023; Übler et al. 2023). See Section 6.1 for details on the uncertainties of these measurements.
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: The AGN luminosity function at z ∼ 5 based on CEERS 2782 (red) with the Poisson error from one object. The binned luminosity functions from the literature are shown for AGNs (McGreer et al. 2018; Giallongo et al. 2019; Grazian et al. 2020; Niida et al. 2020) and Lyman break galaxies (Bouwens et al. 2021; Harikane et al. 2022). The short-dashed line represents the parametric luminosity function of Niida et al. (2020), and the long-dashed line is from Finkelstein & Bagley (2022b) without a correction term from a double power-law function (i.e., δ = 0 in their Equation (1)).
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 G140M 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.