adsabs/AstroCLIMB huggingface dataset:
Paper: A High-resolution Far-infrared Survey to Probe Black Hole–Galaxy Co-evolution
Authors: Matteo Bonato, David Leisawitz, Gianfranco De Zotti, Laura Sommovigo, Irene Shivaei, C. Megan Urry, Duncan Farrah, Locke Spencer, Berke V. Ricketti, Hannah Rana, Susanne Aalto, David B. Sanders, Lee G. Mundy
Figure caption: Evolution of the cosmic star formation history from UV data (uncorrected for dust extinction) and from FIR data (blue circles and red triangles, respectively; data taken from the P. Madau & M. Dickinson 2014 compilation). Because of dust obscuration, UV surveys miss a large fraction of the cosmic star formation, recovered by FIR data. The latter, however, is largely missing at z ≳ 3, due to the strong confusion limits affecting the Herschel SPIRE surveys. As a consequence, our understanding of the cosmic star formation history is incomplete. The reference survey described in this paper would extend measurements up to the EoR. As further examples of more recent measurements, we also plot data points from: C. M. Casey et al. (2021; gray hexagons), derived from the ALMA “MORA” survey on a sample of 2 mm selected dusty SFGs; from F. Loiacono et al. (2021; the “field” case—brown star), derived from the ALMA “ALPINE” survey on a sample of serendipitous [C II] emitters; from H. S. B. Algera et al. (2023; results based on their Monte Carlo approach—green square); and from L. Barrufet et al. (2023; magenta diamond) derived from the ALMA “REBELS” survey on a UV-selected galaxy sample.
Paper: A High-resolution Far-infrared Survey to Probe Black Hole–Galaxy Co-evolution
Authors: Matteo Bonato, David Leisawitz, Gianfranco De Zotti, Laura Sommovigo, Irene Shivaei, C. Megan Urry, Duncan Farrah, Locke Spencer, Berke V. Ricketti, Hannah Rana, Susanne Aalto, David B. Sanders, Lee G. Mundy
Figure caption: 25, 100, and 300 μm wavelength slices from the simulated hyperspectral data cube (left, with insets that reveal the richness of the model data set) and convolved to the resolution of a 2 m telescope (right). The beam size of a 2 m telescope at each wavelength is shown with a circle, indicating that light from most or all the galaxies in the inset area would blend at 100 μm and longer wavelengths. The white arrow in the 100 μm convolved image points to the location of the aperture analyzed in the spectral domain.
Paper: Multizone Modeling of Black Hole Accretion and Feedback in 3D GRMHD: Bridging Vast Spatial and Temporal Scales
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Kung-Yi Su, Ramesh Narayan, Priyamvada Natarajan
Figure caption: Comparison between multizone simulations with varying runtime per zone (colored dashed lines) and a fiducial one-zone simulation (black solid line). The numbers in the legend indicate the fraction of the capped characteristic timescale t char,i , where the fiducial choice is 0.02 in Equation (6). When adopting a short runtime per zone with a factor of 0.01, the insufficient diffusion of the boundary effect leads to a spurious increase in feedback η. As long as the runtimes are chosen to be close to the suitable factor of 0.04, the multizone is insensitive to the choice of runtime per zone.
Paper: Multizone Modeling of Black Hole Accretion and Feedback in 3D GRMHD: Bridging Vast Spatial and Temporal Scales
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Kung-Yi Su, Ramesh Narayan, Priyamvada Natarajan
Figure caption: Comparison between multizone simulations with varying choices of base b (colored dashed lines) and a fiducial one-zone simulation (black solid line). Note that the multizone method is not sensitive to the choice of the base except for the efficiency η where using a small base (b = 6) can lead to an artificial increase in feedback.
Paper: A High-resolution Far-infrared Survey to Probe Black Hole–Galaxy Co-evolution
Authors: Matteo Bonato, David Leisawitz, Gianfranco De Zotti, Laura Sommovigo, Irene Shivaei, C. Megan Urry, Duncan Farrah, Locke Spencer, Berke V. Ricketti, Hannah Rana, Susanne Aalto, David B. Sanders, Lee G. Mundy
Figure caption: The same rest-frame spectra are adopted for all galaxies and AGNs. The solid curve is the spectrum of a star-forming disk galaxy. The dotted curve is the adopted SED of a Type 2 AGN, and the dashed curve is the SED of a Type 1 AGN. The spectral templates are normalized such that the 8–1000  μm IR luminosity is 1 erg s−1. Each galaxy's spectrum is scaled to its actual luminosity. These SEDs are taken from Z.-Y. Cai et al. (2013).
Paper: Multizone Modeling of Black Hole Accretion and Feedback in 3D GRMHD: Bridging Vast Spatial and Temporal Scales
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Kung-Yi Su, Ramesh Narayan, Priyamvada Natarajan
Figure caption: Time evolution of the density profiles for simulations with different initial densities. The black dotted lines show the initial density profiles for each simulation with (a) piecewise constant initial density and (b) Bondi initial density.
Paper: Multizone Modeling of Black Hole Accretion and Feedback in 3D GRMHD: Bridging Vast Spatial and Temporal Scales
Authors: Hyerin Cho, 혜린 조, Ben S. Prather, Kung-Yi Su, Ramesh Narayan, Priyamvada Natarajan
Figure caption: The time evolution of (a) the density ρ and (b) the feedback efficiency η profiles for the MHD run in Section 5.4. The profiles are averaged over the time range indicated in the legend where it is in units of the total runtime of the simulation. The time increases from yellow to purple.
Paper: A High-resolution Far-infrared Survey to Probe Black Hole–Galaxy Co-evolution
Authors: Matteo Bonato, David Leisawitz, Gianfranco De Zotti, Laura Sommovigo, Irene Shivaei, C. Megan Urry, Duncan Farrah, Locke Spencer, Berke V. Ricketti, Hannah Rana, Susanne Aalto, David B. Sanders, Lee G. Mundy
Figure caption: Total IR luminosities (sum of star-forming disk and AGN components) and redshifts of 6275 galaxies in the simulated COSMOS field area. The lower envelope corresponds to the fact that source counts were modeled to a 1 μJy lower bound in flux density.
Paper: Dust-obscured Galaxies in the XMM-SERVS Fields: Selection, Multiwavelength Characterization, and Physical Nature
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Ziyuan Zhu, Franz E. Bauer, Nathan Cristello, Bin Luo, Qingling Ni, Fabio Vito, Yongquan Xue
Figure caption: HR vs. redshift in W-CDF-S (left-hand panel), ELAIS-S1 (middle panel), and XMM-LSS (right-hand panel) for the core sample. The colored points are our X-ray detected DOGs, and the legend in the middle panel indicates their detection status in the SB and HB. Green points with error bars represent the median HR values with 1σ uncertainties for sources detected in both bands. The blue downward triangles, which are detected in the SB but not the HB, represent 1σ HR upper limits. The red upward triangles, which are detected in the HB but not the SB, are 1σ HR lower limits. The black squares represent stacked X-ray undetected DOGs that are classified as reliable SED AGNs in the core sample (see Section 3.3), with the error bar in the x-axis direction showing the 25–75% redshift quantile range. The solid lines are the expected relations for redshifted absorbed power laws, whose intrinsic photon index Γ = 1.8, with several different N H values, as labeled in the legend.
Paper: Dust-obscured Galaxies in the XMM-SERVS Fields: Selection, Multiwavelength Characterization, and Physical Nature
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Ziyuan Zhu, Franz E. Bauer, Nathan Cristello, Bin Luo, Qingling Ni, Fabio Vito, Yongquan Xue
Figure caption: Top panel: The rest-frame 2–10 keV L X,obs vs. L 6μm,AGN for the core sample. Bottom Panel: The rest-frame 2–10 keV absorption-corrected L X vs. L 6μm,AGN for the core sample. The blue points represent X-ray detected DOGs, and the associated error bars represent 1σ uncertainties. The black square represents the stacked average L X,obs vs. the median L 6μm,AGN for X-ray undetected reliable SED AGNs. The solid line shows the absorption-corrected L X–L 6μm,AGN relation in D. Stern (2015); the dashed and dotted lines are the 1σ and 3σ dispersions of their sample, respectively. The results for our full sample are similar.
Paper: Dust-obscured Galaxies in the XMM-SERVS Fields: Selection, Multiwavelength Characterization, and Physical Nature
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Ziyuan Zhu, Franz E. Bauer, Nathan Cristello, Bin Luo, Qingling Ni, Fabio Vito, Yongquan Xue
Figure caption: Example distributions of M ⋆ (left-hand column), SFRnorm (middle column), and N H (right-hand column) for our X-ray detected DOGs in the core sample (blue) compared with those for non-DOG X-ray AGNs (red). We control for z and L X,obs in the top row, and we control for z, L X,obs, and M ⋆ in the bottom row. When we only control for z and L X,obs, M ⋆ and N H both show distinct differences between X-ray detected DOGs and X-ray AGNs, while the difference in SFRnorm is not significant. After we further control for M ⋆, the difference in SFRnorm remains insignificant and the difference in N H remains significant. Note that further controlling for M ⋆ makes building consistent comparison samples more difficult, which results in fewer sources in the bottom panels.
Paper: Dust-obscured Galaxies in the XMM-SERVS Fields: Selection, Multiwavelength Characterization, and Physical Nature
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Ziyuan Zhu, Franz E. Bauer, Nathan Cristello, Bin Luo, Qingling Ni, Fabio Vito, Yongquan Xue
Figure caption: Comparison between our samples and previous studies in the N H–L X plane. The N H values of our DOGs are converted from their HRs. The blue points are our X-ray DOGs detected in both SB and HB with 1σ confidence error bars; the blue leftward and rightward triangles represent X-ray DOGs detected only in HB or SB (1σ lower/upper limits for N H), respectively. Our full and core samples are indicated by empty and filled symbols, respectively. The gray, green, yellow, and red points are reddened type 1 quasars, SMGs, DOGs, and Hot DOGs from previous studies, respectively (see the text for sample references). Our X-ray detected DOGs are luminous with a wide range of obscuration.
Paper: Dust-obscured Galaxies in the XMM-SERVS Fields: Selection, Multiwavelength Characterization, and Physical Nature
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Ziyuan Zhu, Franz E. Bauer, Nathan Cristello, Bin Luo, Qingling Ni, Fabio Vito, Yongquan Xue
Figure caption:  L 1.4 GHz vs. L IR for our core sample. The left-hand panel shows sources in XMM-LSS, and the right-hand panel shows sources in W-CDF-S and ELAIS-S1. XMM-LSS has much higher radio sensitivity, and thus has more radio-detected DOGs. X-ray detected and X-ray undetected DOGs are shown in blue and orange, respectively. The empty circles represent radio AGNs selected via q IR in B. Zhang et al. (2024). The plus signs represent radio AGNs selected via q 24 in S. Zhu et al. (2023). The “X”s represent radio AGNs selected via morphology or spectral index in S. Zhu et al. (2023). The dashed lines represent the IRRC of I. Delvecchio et al. (2021) at z = 1.8 and ﹩\mathrm{log}{M}_{\star }/{M}_{\odot }=11﹩ with an additional 0.3 dex offset.
Paper: Dust-obscured Galaxies in the XMM-SERVS Fields: Selection, Multiwavelength Characterization, and Physical Nature
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Ziyuan Zhu, Franz E. Bauer, Nathan Cristello, Bin Luo, Qingling Ni, Fabio Vito, Yongquan Xue
Figure caption: Comparison between our HR-derived N H values and those derived from X-ray spectral fitting. The gray squares represent the results from A. Kayal & V. Singh (2024). The brown circles represent the results from N. Cristello et al. (2024b). The error bars represent 1σ uncertainties.
Paper: Dust-obscured Galaxies in the XMM-SERVS Fields: Selection, Multiwavelength Characterization, and Physical Nature
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Ziyuan Zhu, Franz E. Bauer, Nathan Cristello, Bin Luo, Qingling Ni, Fabio Vito, Yongquan Xue
Figure caption: SFR/SFRMS distribution for the core sample. Blue and orange histograms represent X-ray detected DOGs and X-ray undetected DOGs, respectively. Solid histograms represent the safe sources where the corresponding star-forming MS can be reliably obtained. Dashed histograms represent all the sources in our sample. Note that the number of X-ray detected DOGs in each bin is multiplied by a factor of 20 for easier visibility. X-ray detected DOGs have a higher fraction of sources below the MS. The distributions for our full sample are similar.
Paper: Dust-obscured Galaxies in the XMM-SERVS Fields: Selection, Multiwavelength Characterization, and Physical Nature
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Ziyuan Zhu, Franz E. Bauer, Nathan Cristello, Bin Luo, Qingling Ni, Fabio Vito, Yongquan Xue
Figure caption: Results from our Monte Carlo X-ray stacking for the core sample. For each plot, we perform 100,000 stacking trials at random positions around the undetected sources. The vertical dashed lines represent the stacked count rates at the positions of the undetected sources. In all three bands, we have significant detections. The results for our full sample are similar.
Paper: Dust-obscured Galaxies in the XMM-SERVS Fields: Selection, Multiwavelength Characterization, and Physical Nature
Authors: Zhibo Yu, 知博 喻, W. N. Brandt, Fan Zou, Ziyuan Zhu, Franz E. Bauer, Nathan Cristello, Bin Luo, Qingling Ni, Fabio Vito, Yongquan Xue
Figure caption: Smoothed stacked X-ray images combining all three EPIC cameras for our core-sample DOGs that are away from known X-ray sources (647 in total) in the FB, SB, and HB. Each image has a size of 60″ × 60″. The numbers on the color bars are in units of count s−1.
Paper: UNCOVER: A NIRSpec Census of Lensed Galaxies at z = 8.50–13.08 Probing a High-AGN Fraction and Ionized Bubbles in the Shadow
Authors: Seiji Fujimoto, Bingjie Wang, John R. Weaver, Vasily Kokorev, Hakim Atek, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Jenny E. Greene, Iryna Chemerynska, Pratika Dayal, Anna de Graaff, Lukas J. Furtak, Pascal A. Oesch, David J. Setton, Sedona H. Price, Tim B. Miller, Christina C. Williams, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Joel Leja, Richard Pan, Dan Coe, Pieter van Dokkum, Robert Feldmann, Yoshinobu Fudamoto, Andy D. Goulding, Gourav Khullar, Danilo Marchesini, Michael Maseda, Themiya Nanayakkara, Erica J. Nelson, Renske Smit, Mauro Stefanon, Andrea Weibel
Figure caption: Constraints on the UV LF at z ∼ 9, z ∼ 10, and z ∼ 12. The magenta pentagons represent the AGN sources from BL (ID20466) and X-ray (ID26185) detections, and the red circles present the other eight sources in our spec-z-confirmed sample in UNCOVER. The red squares denote the spec-z-confirmed nonobvious AGN sources from UNCOVER, CEERS, and JADES GOODS-S, where we do not include several sources in the z = 8.7 overdensity reported in the CEERS field (see text). The gray shaded region and gray squares show the previous photometric measurements, and the black solid curve denotes the best-fit Schechter function estimated in P. G. Pérez-González et al. (2023). The orange squares show the recent spectroscopic measurements (Y. Harikane et al. 2023b). The green squares denote the recent JWST-observed bright objects of GNz11 (R. Maiolino et al. 2024b) and CEERS1019 (R. L. Larson et al. 2023) reported as AGNs. The magenta dashed curve presents the best-fit double power-law function for z ∼ 6 AGNs (E. Giallongo et al. 2019). The open magenta pentagon remarks the two possible AGN sources at different redshifts that show uniquely high-ionization emission lines such as N IV] λ1749, C IV λ1549, and He II λ1640 (ID10646 at z = 8.51) and high [O III] λ5008/Hβ ratio of >10 (ID3686 at z = 9.33), where the excess is not caused by an overdensity but by their uniquely UV-bright properties.
Paper: UNCOVER: A NIRSpec Census of Lensed Galaxies at z = 8.50–13.08 Probing a High-AGN Fraction and Ionized Bubbles in the Shadow
Authors: Seiji Fujimoto, Bingjie Wang, John R. Weaver, Vasily Kokorev, Hakim Atek, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Jenny E. Greene, Iryna Chemerynska, Pratika Dayal, Anna de Graaff, Lukas J. Furtak, Pascal A. Oesch, David J. Setton, Sedona H. Price, Tim B. Miller, Christina C. Williams, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Joel Leja, Richard Pan, Dan Coe, Pieter van Dokkum, Robert Feldmann, Yoshinobu Fudamoto, Andy D. Goulding, Gourav Khullar, Danilo Marchesini, Michael Maseda, Themiya Nanayakkara, Erica J. Nelson, Renske Smit, Mauro Stefanon, Andrea Weibel
Figure caption: 2D and 1D prism spectra for the 10 sources whose spec-z are successfully confirmed at z ≥ 8.5 in this study. The red horizontal lines indicate the 2σ range of the Gaussian, which is used for extracting the 1D spectrum shown in the bottom panel. The orange and green vertical lines denote wavelengths of the Lyα break and the faint emission lines detected at SNR ≥ 2.5, respectively. The right panel shows the likelihood of the source redshift P(z) estimated from the eazy template fitting to the prism spectrum, and the best-fit SED (forced at z < 6) is presented with the red (blue) curve overlaid on the 1D spectrum.
Paper: UNCOVER: A NIRSpec Census of Lensed Galaxies at z = 8.50–13.08 Probing a High-AGN Fraction and Ionized Bubbles in the Shadow
Authors: Seiji Fujimoto, Bingjie Wang, John R. Weaver, Vasily Kokorev, Hakim Atek, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Jenny E. Greene, Iryna Chemerynska, Pratika Dayal, Anna de Graaff, Lukas J. Furtak, Pascal A. Oesch, David J. Setton, Sedona H. Price, Tim B. Miller, Christina C. Williams, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Joel Leja, Richard Pan, Dan Coe, Pieter van Dokkum, Robert Feldmann, Yoshinobu Fudamoto, Andy D. Goulding, Gourav Khullar, Danilo Marchesini, Michael Maseda, Themiya Nanayakkara, Erica J. Nelson, Renske Smit, Mauro Stefanon, Andrea Weibel
Figure caption: Zoom-in 3.″6 × 3.″6 NIRCam RGB (R: F444W, G: F356W, and B: F277W) cutouts of the 10 sources whose spec-z are successfully confirmed. The rectangles show the shutter configurations, where the standard three-shutter slitlets and a three-point nodding were adopted, and thus the five shutter positions are presented. The white, magenta, yellow, orange, red, and cyan rectangles represent our MSA observations of MSA-2, 3, 4, 5, 6, and 7, respectively, where MSA-5, 6, and 7 overlap nearly entirely.
Paper: UNCOVER: A NIRSpec Census of Lensed Galaxies at z = 8.50–13.08 Probing a High-AGN Fraction and Ionized Bubbles in the Shadow
Authors: Seiji Fujimoto, Bingjie Wang, John R. Weaver, Vasily Kokorev, Hakim Atek, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Jenny E. Greene, Iryna Chemerynska, Pratika Dayal, Anna de Graaff, Lukas J. Furtak, Pascal A. Oesch, David J. Setton, Sedona H. Price, Tim B. Miller, Christina C. Williams, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Joel Leja, Richard Pan, Dan Coe, Pieter van Dokkum, Robert Feldmann, Yoshinobu Fudamoto, Andy D. Goulding, Gourav Khullar, Danilo Marchesini, Michael Maseda, Themiya Nanayakkara, Erica J. Nelson, Renske Smit, Mauro Stefanon, Andrea Weibel
Figure caption: Left: comparison between z phot and z spec for our spec-z-confirmed sources. The red filled and open circles represent the sources selected from A23 and other selections, respectively (see Section 3.1). The error bars show the 1σ error range for the A23 sample, while the other sources show the 2σ error range given the nonhomogeneous selection criteria adopted in the MSA target selection process (Section 2.2). Right: comparison between the redshift estimates based on lines (z line) and the Lyα break (z break) for six sources whose multiple emission lines are successfully detected in the prism spectrum. Two sources (ID20466 and ID10646) show z break − z line < −0.1, indicating the presence of the nonzero fluxes blueward of the Lyα emission in the prism spectra and the ionized bubbles around these two sources (Section 5).
Paper: UNCOVER: A NIRSpec Census of Lensed Galaxies at z = 8.50–13.08 Probing a High-AGN Fraction and Ionized Bubbles in the Shadow
Authors: Seiji Fujimoto, Bingjie Wang, John R. Weaver, Vasily Kokorev, Hakim Atek, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Jenny E. Greene, Iryna Chemerynska, Pratika Dayal, Anna de Graaff, Lukas J. Furtak, Pascal A. Oesch, David J. Setton, Sedona H. Price, Tim B. Miller, Christina C. Williams, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Joel Leja, Richard Pan, Dan Coe, Pieter van Dokkum, Robert Feldmann, Yoshinobu Fudamoto, Andy D. Goulding, Gourav Khullar, Danilo Marchesini, Michael Maseda, Themiya Nanayakkara, Erica J. Nelson, Renske Smit, Mauro Stefanon, Andrea Weibel
Figure caption: NIRCam RGB (R: F444W, G: F356W, and B: F277W) map of A2744 taken in UNCOVER (R. Bezanson et al. 2024). The white-shaded region indicates the highly magnified area with magnifications of ≥2 (L. J. Furtak et al. 2023b). The yellow squares show the positions of the 10 sources that are spectroscopically confirmed at z ≥ 8.5 in UNCOVER.
Paper: UNCOVER: A NIRSpec Census of Lensed Galaxies at z = 8.50–13.08 Probing a High-AGN Fraction and Ionized Bubbles in the Shadow
Authors: Seiji Fujimoto, Bingjie Wang, John R. Weaver, Vasily Kokorev, Hakim Atek, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Jenny E. Greene, Iryna Chemerynska, Pratika Dayal, Anna de Graaff, Lukas J. Furtak, Pascal A. Oesch, David J. Setton, Sedona H. Price, Tim B. Miller, Christina C. Williams, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Joel Leja, Richard Pan, Dan Coe, Pieter van Dokkum, Robert Feldmann, Yoshinobu Fudamoto, Andy D. Goulding, Gourav Khullar, Danilo Marchesini, Michael Maseda, Themiya Nanayakkara, Erica J. Nelson, Renske Smit, Mauro Stefanon, Andrea Weibel
Figure caption: Comparison of the LFs with the theoretical predictions in the literature at z ∼ 9, z ∼ 10, and z ∼ 12. The symbols are the same as Figure 6, The color dashed lines denote the theoretical predictions of SC-SAM (L. Y. A. Yung et al. 2019), FLARES (A. P. Vijayan et al. 2021; C. C. Lovell et al. 2023; S. M. Wilkins et al. 2023), DELPHI (P. Dayal et al. 2014; V. Mauerhofer & P. Dayal 2023), Thesan (R. Kannan et al. 2023), Bluetides (S. M. Wilkins et al. 2017), and Universe Machine (P. Behroozi et al. 2020). In each redshift range, our lower limit estimate in the brightest M UV challenges several theoretical predictions, confirming the earlier arguments of the high abundance of UV-bright (M UV ≲ −20) galaxies in previous photometric studies in a spectroscopic manner at z ∼ 9–12.
Paper: UNCOVER: A NIRSpec Census of Lensed Galaxies at z = 8.50–13.08 Probing a High-AGN Fraction and Ionized Bubbles in the Shadow
Authors: Seiji Fujimoto, Bingjie Wang, John R. Weaver, Vasily Kokorev, Hakim Atek, Rachel Bezanson, Ivo Labbe, Gabriel Brammer, Jenny E. Greene, Iryna Chemerynska, Pratika Dayal, Anna de Graaff, Lukas J. Furtak, Pascal A. Oesch, David J. Setton, Sedona H. Price, Tim B. Miller, Christina C. Williams, Katherine E. Whitaker, Adi Zitrin, Sam E. Cutler, Joel Leja, Richard Pan, Dan Coe, Pieter van Dokkum, Robert Feldmann, Yoshinobu Fudamoto, Andy D. Goulding, Gourav Khullar, Danilo Marchesini, Michael Maseda, Themiya Nanayakkara, Erica J. Nelson, Renske Smit, Mauro Stefanon, Andrea Weibel
Figure caption: AGN fraction at z ≥ 8.5. The blue and red histograms present the number of AGNs and the sources that are spectroscopically confirmed in our studies at each M UV bin. The histogram with a red outline represents the two possible AGN sources of ID10646 and ID3686 that fall in the brightest M UV bin. The red circles indicate the AGN fraction for the spec-z-confirmed UNCOVER sources at z ≥ 8.5, where we show the brightest M UV bin in the case that both AGN candidates are truly AGNs. The error bars represent the confidence intervals for the binomial proportion, derived using the Jeffreys interval at 1σ. The red hatched area shows the 1σ range for the AGN fraction over the entire M UV range (=2/10). This may be a lower limit, as more sources, including ID10646 and ID3686, might be confirmed to be AGNs in future observations. The black shaded area denotes the recent reports of ≃5%−10% BL AGN fractions from the BL AGN identifications in recent NIRSpec studies at z ≃ 4–7 (Y. Harikane et al. 2024; R. Maiolino et al. 2024a).