adsabs/AstroCLIMB huggingface dataset:
Paper: Atmospheric Effects on Neutron Star Parameter Constraints with NICER
Authors: Tuomo Salmi, Serena Vinciguerra, Devarshi Choudhury, Anna L. Watts, Wynn C. G. Ho, Sebastien Guillot, Yves Kini, Bas Dorsman, Sharon M. Morsink, Slavko Bogdanov
Figure caption: Effect of the atmosphere model on the posterior distributions of radius, compactness, mass, and temperatures for both primary and secondary hot regions, using the PSR J0030+0451 NICER data set conditional on the ST-U model. Five types of posterior distribution are shown with different atmosphere tables used in the analysis (see Table 1 for definitions). The 1D credible intervals and the KL-divergence estimates are reported for the fully ionized hydrogen NSX case: ST-U-nsxH (see Table 3 for mass and radius values in other cases). See the caption of Figure 3 for additional details about the figure elements. Posterior distributions for the other parameters are shown in Figure 9 of the Appendix.
Paper: Two Massive, Compact, and Dust-obscured Candidate z ≃ 8 Galaxies Discovered by JWST
Authors: Hollis B. Akins, Caitlin M. Casey, Natalie Allen, Micaela B. Bagley, Mark Dickinson, Steven L. Finkelstein, Maximilien Franco, Santosh Harish, Pablo Arrabal Haro, Olivier Ilbert, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Daizhong Liu, Arianna S. Long, Henry Joy McCracken, Louise Paquereau, Casey Papovich, Nor Pirzkal, Jason Rhodes, Brant E. Robertson, Marko Shuntov, Sune Toft, Guang Yang, Guillermo Barro, Laura Bisigello, Véronique Buat, Jaclyn B. Champagne, Olivia Cooper, Luca Costantin, Alexander de la Vega, Nicole E. Drakos, Andreas Faisst, Adriano Fontana, Seiji Fujimoto, Steven Gillman, Carlos Gómez-Guijarro, Ghassem Gozaliasl, Nimish P. Hathi, Christopher C. Hayward, Michaela Hirschmann, Benne W. Holwerda, Shuowen Jin, Dale D. Kocevski, Vasily Kokorev, Erini Lambrides, Ray A. Lucas, Georgios E. Magdis, Benjamin Magnelli, Jed McKinney, Bahram Mobasher, Pablo G. Pérez-González, R. Michael Rich, Lise-Marie Seillé, Margherita Talia, C. Megan Urry, Francesco Valentino, Katherine E. Whitaker, L. Y. Aaron Yung, Jorge Zavala
Figure caption: Cumulative stellar mass density ρ ⋆ vs. M ⋆. The red points indicate the cumulative stellar mass density inferred from the detection of COS-z8M1 and CEERS-z7M1. We additionally plot the result for z ∼ 8 from Labbé et al. (2023a) and integrated Schechter function fits to UV-luminous LBGs from Stefanon et al. (2021). In tabulating these results, we adopt the same redshift bin, z ∼ 7–9 (see main text), and remove the z = 5.6 AGN from the Labbé et al. (2023a) sample. The light blue points show the Labbé et al. (2023a) sample with the most massive candidate removed. The candidates presented in this work are consistent with the Stefanon et al. (2021) z ∼ 7–9 stellar mass function, though the uncertainties are large given the identification of just two sources.
Paper: Two Massive, Compact, and Dust-obscured Candidate z ≃ 8 Galaxies Discovered by JWST
Authors: Hollis B. Akins, Caitlin M. Casey, Natalie Allen, Micaela B. Bagley, Mark Dickinson, Steven L. Finkelstein, Maximilien Franco, Santosh Harish, Pablo Arrabal Haro, Olivier Ilbert, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Daizhong Liu, Arianna S. Long, Henry Joy McCracken, Louise Paquereau, Casey Papovich, Nor Pirzkal, Jason Rhodes, Brant E. Robertson, Marko Shuntov, Sune Toft, Guang Yang, Guillermo Barro, Laura Bisigello, Véronique Buat, Jaclyn B. Champagne, Olivia Cooper, Luca Costantin, Alexander de la Vega, Nicole E. Drakos, Andreas Faisst, Adriano Fontana, Seiji Fujimoto, Steven Gillman, Carlos Gómez-Guijarro, Ghassem Gozaliasl, Nimish P. Hathi, Christopher C. Hayward, Michaela Hirschmann, Benne W. Holwerda, Shuowen Jin, Dale D. Kocevski, Vasily Kokorev, Erini Lambrides, Ray A. Lucas, Georgios E. Magdis, Benjamin Magnelli, Jed McKinney, Bahram Mobasher, Pablo G. Pérez-González, R. Michael Rich, Lise-Marie Seillé, Margherita Talia, C. Megan Urry, Francesco Valentino, Katherine E. Whitaker, L. Y. Aaron Yung, Jorge Zavala
Figure caption: Optical-MIR SEDs of COS-939 and COS-3627, the two candidates that fall into our color selection criteria but are fainter and thus have poorly constrained redshifts. As in Figures 2 and 3, we show cutouts in the ACS, NIRCam, and MIRI bands and the measured photometry in red. We show the best-fit EAzY SED in black and a forced z < 6 model in gray.
Paper: Atmospheric Effects on Neutron Star Parameter Constraints with NICER
Authors: Tuomo Salmi, Serena Vinciguerra, Devarshi Choudhury, Anna L. Watts, Wynn C. G. Ho, Sebastien Guillot, Yves Kini, Bas Dorsman, Sharon M. Morsink, Slavko Bogdanov
Figure caption: Effect of the atmosphere model on the posterior distributions of radius and the other parameters not including those shown in Figure 3 (except the beaming parameters a and b) using the PSR J0740+6620 NICER data set conditional on the ST-U model. The additional parameters are cosine Earth inclination to spin axis (﹩\cos i﹩), primary region initial phase (ϕ  p ), primary region center colatitude (Θ p ), primary region angular radius (ζ  p ), secondary region initial phase (ϕ  s ), secondary region center colatitude (Θ s ), secondary region angular radius (ζ  s ), distance (D), effective area scaling factor of NICER (α NICER), and interstellar neutral hydrogen column density (N H). See the caption of Figure 3 for more details.
Paper: Atmospheric Effects on Neutron Star Parameter Constraints with NICER
Authors: Tuomo Salmi, Serena Vinciguerra, Devarshi Choudhury, Anna L. Watts, Wynn C. G. Ho, Sebastien Guillot, Yves Kini, Bas Dorsman, Sharon M. Morsink, Slavko Bogdanov
Figure caption: Effect of the atmosphere model on the posterior distributions of radius, mass, and beaming parameters a, b, c, and d, using the PSR J0030+0451 NICER data set conditional on the ST-U model and energy-dependent beaming parameterization. Priors (dashed–dotted curves) and posteriors for the four beaming parameters are shown only for the models where those parameters were kept free. The same two hydrogen and helium posteriors without beaming modifications are also shown, as in Figure 4 (ST-U-nsxH and ST-U-nsxHe), in the radius and mass panels. The posteriors for ST-U-nsxH and ST-U-nsxH-E-beam5 models are almost exactly overlapping. The credible intervals and KL-divergence estimates are reported for the latter (see Table 3 for mass and radius values in other cases). See the caption of Figure 3 for additional details about the figure elements. Posterior distributions for the other parameters are shown in Figure 10 of the Appendix.
Paper: Atmospheric Effects on Neutron Star Parameter Constraints with NICER
Authors: Tuomo Salmi, Serena Vinciguerra, Devarshi Choudhury, Anna L. Watts, Wynn C. G. Ho, Sebastien Guillot, Yves Kini, Bas Dorsman, Sharon M. Morsink, Slavko Bogdanov
Figure caption: Effect of the atmosphere model on the posterior distributions of radius, compactness, mass, radius, and temperatures for both primary and secondary hot regions, using the PSR J0030+0451 NICER data set conditional on the ST+PST model. Posterior distributions are shown for fully ionized hydrogen and helium, and for partially ionized hydrogen NSX models. The credible intervals and KL-divergence estimates are reported for the ST+PST-nsxH model (see Table 3 for mass and radius values of the other models). See the caption of Figure 3 for additional details about the figure elements. Posterior distributions for the other parameters are shown in Figure 11 of the Appendix.
Paper: Atmospheric Effects on Neutron Star Parameter Constraints with NICER
Authors: Tuomo Salmi, Serena Vinciguerra, Devarshi Choudhury, Anna L. Watts, Wynn C. G. Ho, Sebastien Guillot, Yves Kini, Bas Dorsman, Sharon M. Morsink, Slavko Bogdanov
Figure caption: Effect of the atmosphere model on the posterior distributions of radius and the other parameters not including those shown in Figure 6 using the PSR J0030+0451 NICER data set conditional on the ST+PST model. In addition to the parameters defined in Figures 8 and 9, we show the posteriors for azimuth offset between the emitting and the masking spherical caps of the secondary hot spot (χ  s ), colatitude of the masking region of the secondary hot spot (Θ o,s ), and radius of the masking region of the secondary hot spot (ζ  o,s ). See the caption of Figure 6 for additional details.
Paper: Atmospheric Effects on Neutron Star Parameter Constraints with NICER
Authors: Tuomo Salmi, Serena Vinciguerra, Devarshi Choudhury, Anna L. Watts, Wynn C. G. Ho, Sebastien Guillot, Yves Kini, Bas Dorsman, Sharon M. Morsink, Slavko Bogdanov
Figure caption: Effect of the atmosphere model on the posterior distributions of radius, compactness, mass, and temperatures for both primary and secondary hot regions, using the PSR J0030+0451 joint NICER and XMM-Newton (NxX) data sets conditional on the ST-U model. Posterior distributions are shown for fully ionized hydrogen and helium, and partially ionized hydrogen NSX models. The credible intervals and KL-divergence estimates are reported for the ST-U-NxX-nsxH model (see Table 3 for mass and radius values the other models). See the caption of Figure 3 for additional details about the figure elements. Posterior distributions for the other parameters are shown in Figure 12 of the Appendix.
Paper: Atmospheric Effects on Neutron Star Parameter Constraints with NICER
Authors: Tuomo Salmi, Serena Vinciguerra, Devarshi Choudhury, Anna L. Watts, Wynn C. G. Ho, Sebastien Guillot, Yves Kini, Bas Dorsman, Sharon M. Morsink, Slavko Bogdanov
Figure caption: Effect of the atmosphere model on the posterior distributions of radius and the other parameters not including those shown in Figure 4 using the PSR J0030+0451 NICER data set conditional on the ST-U model. The parameters are the same as described in the caption of Figure 8, except that D and α NICER are replaced with β = α NICER D −2. See the caption of Figure 4 for additional details.
Paper: Atmospheric Effects on Neutron Star Parameter Constraints with NICER
Authors: Tuomo Salmi, Serena Vinciguerra, Devarshi Choudhury, Anna L. Watts, Wynn C. G. Ho, Sebastien Guillot, Yves Kini, Bas Dorsman, Sharon M. Morsink, Slavko Bogdanov
Figure caption: Effect of the atmosphere model on the posterior distributions of radius and the other parameters not including those shown in Figure 7 using the PSR J0030+0451 joint NICER and XMM-Newton (NxX) data sets conditional on the ST-U model. In addition to the parameters defined in Figure 8, we show the posteriors for the effective area scaling factor of XMM-Newton (α XMM). See the caption of Figure 7 for additional details.
Paper: Atmospheric Effects on Neutron Star Parameter Constraints with NICER
Authors: Tuomo Salmi, Serena Vinciguerra, Devarshi Choudhury, Anna L. Watts, Wynn C. G. Ho, Sebastien Guillot, Yves Kini, Bas Dorsman, Sharon M. Morsink, Slavko Bogdanov
Figure caption: Effect of the atmosphere model on the posterior distributions of radius and the other parameters not including those shown in Figure 5 using the PSR J0030+0451 NICER data set conditional on the ST-U model and energy-dependent beaming parameterization. The shown parameters are the same as in Figure 9. See the caption of Figure 5 for additional details.
Paper: Two Massive, Compact, and Dust-obscured Candidate z ≃ 8 Galaxies Discovered by JWST
Authors: Hollis B. Akins, Caitlin M. Casey, Natalie Allen, Micaela B. Bagley, Mark Dickinson, Steven L. Finkelstein, Maximilien Franco, Santosh Harish, Pablo Arrabal Haro, Olivier Ilbert, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Daizhong Liu, Arianna S. Long, Henry Joy McCracken, Louise Paquereau, Casey Papovich, Nor Pirzkal, Jason Rhodes, Brant E. Robertson, Marko Shuntov, Sune Toft, Guang Yang, Guillermo Barro, Laura Bisigello, Véronique Buat, Jaclyn B. Champagne, Olivia Cooper, Luca Costantin, Alexander de la Vega, Nicole E. Drakos, Andreas Faisst, Adriano Fontana, Seiji Fujimoto, Steven Gillman, Carlos Gómez-Guijarro, Ghassem Gozaliasl, Nimish P. Hathi, Christopher C. Hayward, Michaela Hirschmann, Benne W. Holwerda, Shuowen Jin, Dale D. Kocevski, Vasily Kokorev, Erini Lambrides, Ray A. Lucas, Georgios E. Magdis, Benjamin Magnelli, Jed McKinney, Bahram Mobasher, Pablo G. Pérez-González, R. Michael Rich, Lise-Marie Seillé, Margherita Talia, C. Megan Urry, Francesco Valentino, Katherine E. Whitaker, L. Y. Aaron Yung, Jorge Zavala
Figure caption: The m 277–m 444 vs. m 444–m 770 color–color diagram indicating selection of z ≳ 7 dusty galaxies. Points indicate objects detected at 5σ significance in F444W and F770W and at least 2σ significance in F277W. The points are colored by their best-fit photometric redshift from first-pass EAzY runs, and contours indicate the point density. The dashed lines indicate our proposed color selection criterion, which captures 4 objects, all with photometric redshifts ≳7. We show in gray two model tracks generated from BAGPIPES for young (10 Myr) stellar populations with A  V  = 2.5 and 3.5 from z ∼ 1 to 9. We additionally show in red a QSO model with A  V  = 4, which, at z > 3, is redder in m 444–m 770 than the galaxy models. The color–color selection shown here is optimized for selecting z ≳ 6–7 obscured galaxies with young ages and bright emission lines but rejecting objects with steeply rising MIR SEDs (e.g., obscured AGN).
Paper: Two Massive, Compact, and Dust-obscured Candidate z ≃ 8 Galaxies Discovered by JWST
Authors: Hollis B. Akins, Caitlin M. Casey, Natalie Allen, Micaela B. Bagley, Mark Dickinson, Steven L. Finkelstein, Maximilien Franco, Santosh Harish, Pablo Arrabal Haro, Olivier Ilbert, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Daizhong Liu, Arianna S. Long, Henry Joy McCracken, Louise Paquereau, Casey Papovich, Nor Pirzkal, Jason Rhodes, Brant E. Robertson, Marko Shuntov, Sune Toft, Guang Yang, Guillermo Barro, Laura Bisigello, Véronique Buat, Jaclyn B. Champagne, Olivia Cooper, Luca Costantin, Alexander de la Vega, Nicole E. Drakos, Andreas Faisst, Adriano Fontana, Seiji Fujimoto, Steven Gillman, Carlos Gómez-Guijarro, Ghassem Gozaliasl, Nimish P. Hathi, Christopher C. Hayward, Michaela Hirschmann, Benne W. Holwerda, Shuowen Jin, Dale D. Kocevski, Vasily Kokorev, Erini Lambrides, Ray A. Lucas, Georgios E. Magdis, Benjamin Magnelli, Jed McKinney, Bahram Mobasher, Pablo G. Pérez-González, R. Michael Rich, Lise-Marie Seillé, Margherita Talia, C. Megan Urry, Francesco Valentino, Katherine E. Whitaker, L. Y. Aaron Yung, Jorge Zavala
Figure caption: Illustration of the various galaxy+AGN possibilities associated with the composite SED shape of CEERS-z7M1, with a blue UV slope but red optical colors. Left: galaxy-only composite model with a massive (﹩\mathrm{log}{M}_{\star }/{M}_{\odot }=10﹩) obscured (A  V  = 4) galaxy combined with a low-mass (﹩\mathrm{log}{M}_{\star }/{M}_{\odot }=7﹩) unobscured galaxy. Physically, this corresponds to a patchy distribution of dust with “holes” allowing some UV light to escape unattenuated. Middle: galaxy+quasar model with a massive obscured galaxy combined with a faint unobscured type I quasar. We adopt the SDSS QSO composite spectrum (Vanden Berk et al. 2001; Glikman et al. 2006). Right: galaxy+quasar model with a low-mass unobscured galaxy combined with a bright but heavily dust-reddened type I quasar.
Paper: Two Massive, Compact, and Dust-obscured Candidate z ≃ 8 Galaxies Discovered by JWST
Authors: Hollis B. Akins, Caitlin M. Casey, Natalie Allen, Micaela B. Bagley, Mark Dickinson, Steven L. Finkelstein, Maximilien Franco, Santosh Harish, Pablo Arrabal Haro, Olivier Ilbert, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Daizhong Liu, Arianna S. Long, Henry Joy McCracken, Louise Paquereau, Casey Papovich, Nor Pirzkal, Jason Rhodes, Brant E. Robertson, Marko Shuntov, Sune Toft, Guang Yang, Guillermo Barro, Laura Bisigello, Véronique Buat, Jaclyn B. Champagne, Olivia Cooper, Luca Costantin, Alexander de la Vega, Nicole E. Drakos, Andreas Faisst, Adriano Fontana, Seiji Fujimoto, Steven Gillman, Carlos Gómez-Guijarro, Ghassem Gozaliasl, Nimish P. Hathi, Christopher C. Hayward, Michaela Hirschmann, Benne W. Holwerda, Shuowen Jin, Dale D. Kocevski, Vasily Kokorev, Erini Lambrides, Ray A. Lucas, Georgios E. Magdis, Benjamin Magnelli, Jed McKinney, Bahram Mobasher, Pablo G. Pérez-González, R. Michael Rich, Lise-Marie Seillé, Margherita Talia, C. Megan Urry, Francesco Valentino, Katherine E. Whitaker, L. Y. Aaron Yung, Jorge Zavala
Figure caption: Optical through MIR SED of COS-z8M1. The top panels show 1.5 arcsec2 cutouts in the available HST/JWST bands plus stacked ground-based imaging from Subaru/HSC and UltraVISTA. The bottom panel shows the measured photometry (or 2σ upper limits) from all available JWST bands (shown in dark red), as well as HST/ACS, Spitzer/IRAC, and ground-based bands (light red). We additionally show maximum a posteriori model SEDs from CIGALE, BEAGLE, BAGPIPES, and PROSPECTOR (for clarity, we do not show the EAzY SED). The inset shows the full redshift probability distributions P(z) from each photo-z code. Robust detection in NIRCam/F444W and MIRI/F770W with a sharp break between F444W and F277W mandates a massive, dusty, z > 7 solution.
Paper: Two Massive, Compact, and Dust-obscured Candidate z ≃ 8 Galaxies Discovered by JWST
Authors: Hollis B. Akins, Caitlin M. Casey, Natalie Allen, Micaela B. Bagley, Mark Dickinson, Steven L. Finkelstein, Maximilien Franco, Santosh Harish, Pablo Arrabal Haro, Olivier Ilbert, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Daizhong Liu, Arianna S. Long, Henry Joy McCracken, Louise Paquereau, Casey Papovich, Nor Pirzkal, Jason Rhodes, Brant E. Robertson, Marko Shuntov, Sune Toft, Guang Yang, Guillermo Barro, Laura Bisigello, Véronique Buat, Jaclyn B. Champagne, Olivia Cooper, Luca Costantin, Alexander de la Vega, Nicole E. Drakos, Andreas Faisst, Adriano Fontana, Seiji Fujimoto, Steven Gillman, Carlos Gómez-Guijarro, Ghassem Gozaliasl, Nimish P. Hathi, Christopher C. Hayward, Michaela Hirschmann, Benne W. Holwerda, Shuowen Jin, Dale D. Kocevski, Vasily Kokorev, Erini Lambrides, Ray A. Lucas, Georgios E. Magdis, Benjamin Magnelli, Jed McKinney, Bahram Mobasher, Pablo G. Pérez-González, R. Michael Rich, Lise-Marie Seillé, Margherita Talia, C. Megan Urry, Francesco Valentino, Katherine E. Whitaker, L. Y. Aaron Yung, Jorge Zavala
Figure caption: Inferred stellar mass vs. redshift for COS-z8M1 (red) and CEERS-z7M1 (green), adopting the results from PROSPECTOR. We additionally show measurements for spectroscopically confirmed, dust continuum–detected star-forming galaxies from the literature (Marrone et al. 2018; Tamura et al. 2019; Endsley et al. 2022b; Ferrara et al. 2022b), as well as recent UV-bright galaxies confirmed with JWST/NIRSpec (Fujimoto et al. 2023a). The orange stripe shows the range of stellar masses expected for halos with a constant number density, computed from an evolving halo mass function assuming a baryon conversion efficiency ϵ ∼ 20%–30%. Both COS-z8M1 and CEERS-z7M1 appear to be among the most massive dust-obscured galaxies at this epoch.
Paper: Two Massive, Compact, and Dust-obscured Candidate z ≃ 8 Galaxies Discovered by JWST
Authors: Hollis B. Akins, Caitlin M. Casey, Natalie Allen, Micaela B. Bagley, Mark Dickinson, Steven L. Finkelstein, Maximilien Franco, Santosh Harish, Pablo Arrabal Haro, Olivier Ilbert, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Daizhong Liu, Arianna S. Long, Henry Joy McCracken, Louise Paquereau, Casey Papovich, Nor Pirzkal, Jason Rhodes, Brant E. Robertson, Marko Shuntov, Sune Toft, Guang Yang, Guillermo Barro, Laura Bisigello, Véronique Buat, Jaclyn B. Champagne, Olivia Cooper, Luca Costantin, Alexander de la Vega, Nicole E. Drakos, Andreas Faisst, Adriano Fontana, Seiji Fujimoto, Steven Gillman, Carlos Gómez-Guijarro, Ghassem Gozaliasl, Nimish P. Hathi, Christopher C. Hayward, Michaela Hirschmann, Benne W. Holwerda, Shuowen Jin, Dale D. Kocevski, Vasily Kokorev, Erini Lambrides, Ray A. Lucas, Georgios E. Magdis, Benjamin Magnelli, Jed McKinney, Bahram Mobasher, Pablo G. Pérez-González, R. Michael Rich, Lise-Marie Seillé, Margherita Talia, C. Megan Urry, Francesco Valentino, Katherine E. Whitaker, L. Y. Aaron Yung, Jorge Zavala
Figure caption: Contours of the marginal 2 mm emission from Ex-MORA overlaid on the JWST/F444W image. The location of the 2.9σ peak is marked with a cross, offset ∼0.″5 from the NIRCam source but consistent within the positional uncertainty given the large beam size. No other ±2σ signal falls within 2″ of the source. The Ex-MORA flux, if real, suggests a high IR luminosity of ﹩\mathrm{log}{L}_{\mathrm{IR}}/{L}_{\odot }\sim {11.9}_{-0.3}^{+0.4}﹩, comparable to local ULIRGs.
Paper: Two Massive, Compact, and Dust-obscured Candidate z ≃ 8 Galaxies Discovered by JWST
Authors: Hollis B. Akins, Caitlin M. Casey, Natalie Allen, Micaela B. Bagley, Mark Dickinson, Steven L. Finkelstein, Maximilien Franco, Santosh Harish, Pablo Arrabal Haro, Olivier Ilbert, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Daizhong Liu, Arianna S. Long, Henry Joy McCracken, Louise Paquereau, Casey Papovich, Nor Pirzkal, Jason Rhodes, Brant E. Robertson, Marko Shuntov, Sune Toft, Guang Yang, Guillermo Barro, Laura Bisigello, Véronique Buat, Jaclyn B. Champagne, Olivia Cooper, Luca Costantin, Alexander de la Vega, Nicole E. Drakos, Andreas Faisst, Adriano Fontana, Seiji Fujimoto, Steven Gillman, Carlos Gómez-Guijarro, Ghassem Gozaliasl, Nimish P. Hathi, Christopher C. Hayward, Michaela Hirschmann, Benne W. Holwerda, Shuowen Jin, Dale D. Kocevski, Vasily Kokorev, Erini Lambrides, Ray A. Lucas, Georgios E. Magdis, Benjamin Magnelli, Jed McKinney, Bahram Mobasher, Pablo G. Pérez-González, R. Michael Rich, Lise-Marie Seillé, Margherita Talia, C. Megan Urry, Francesco Valentino, Katherine E. Whitaker, L. Y. Aaron Yung, Jorge Zavala
Figure caption: Same as Figure 2 but for CEERS-z7M1. The NIRCam short wavelength bands reveal a blue UV slope (β ∼ −2.5) at 1–2 μm despite the very red continuum at >2 μm. This could be from star formation in an unobscured line of sight or an unobscured AGN component. The additional filters constrain the redshift to precisely z = 7.6.
Paper: Two Massive, Compact, and Dust-obscured Candidate z ≃ 8 Galaxies Discovered by JWST
Authors: Hollis B. Akins, Caitlin M. Casey, Natalie Allen, Micaela B. Bagley, Mark Dickinson, Steven L. Finkelstein, Maximilien Franco, Santosh Harish, Pablo Arrabal Haro, Olivier Ilbert, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Daizhong Liu, Arianna S. Long, Henry Joy McCracken, Louise Paquereau, Casey Papovich, Nor Pirzkal, Jason Rhodes, Brant E. Robertson, Marko Shuntov, Sune Toft, Guang Yang, Guillermo Barro, Laura Bisigello, Véronique Buat, Jaclyn B. Champagne, Olivia Cooper, Luca Costantin, Alexander de la Vega, Nicole E. Drakos, Andreas Faisst, Adriano Fontana, Seiji Fujimoto, Steven Gillman, Carlos Gómez-Guijarro, Ghassem Gozaliasl, Nimish P. Hathi, Christopher C. Hayward, Michaela Hirschmann, Benne W. Holwerda, Shuowen Jin, Dale D. Kocevski, Vasily Kokorev, Erini Lambrides, Ray A. Lucas, Georgios E. Magdis, Benjamin Magnelli, Jed McKinney, Bahram Mobasher, Pablo G. Pérez-González, R. Michael Rich, Lise-Marie Seillé, Margherita Talia, C. Megan Urry, Francesco Valentino, Katherine E. Whitaker, L. Y. Aaron Yung, Jorge Zavala
Figure caption: Results of 2D point-source profile fitting to the NIRCam/F444W imaging for both sources. The columns show the data, best-fit model, and residuals for each source. Both sources are well characterized by a point-source model, suggesting extremely compact sizes. We derive an upper limit on the true sizes of R eff ≲ 200 pc, as discussed in the text.