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Paper: Radio Plateaus in Gamma-Ray Burst Afterglows and Their Application in Cosmology
Authors: Xiao Tian, Jia-Lun Li, Shuang-Xi Yi, Yu-Peng Yang, Jian-Ping Hu, Yan-Kun Qu, Fa-Yin Wang
Figure caption: Constraints on the cosmological parameters and calibrated GRB Hubble diagram for the L–T correlation. (a) Corner plots for the constraints for the joint radio GRB, SN Ia, and CMB samples. The confidence regions of the parameters Ωm and ΩΛ are 1σ and 2σ from inner to outer. (b) Blue points are SNe from the Pantheon sample. Black points are 27 GRBs with plateau phases. The red solid line is a flat ΛCDM model with Ωm = 0.3 and H 0 = 70.0 km s−1 Mpc−1. For the flat ΛCDM model, the black and green solid lines are the best fit of the calibrated GRB and SN+GRB samples, respectively. The best fit from the SN+GRB sample for the nonflat ΛCDM model is shown as the orange line.
Paper: Radio Plateaus in Gamma-Ray Burst Afterglows and Their Application in Cosmology
Authors: Xiao Tian, Jia-Lun Li, Shuang-Xi Yi, Yu-Peng Yang, Jian-Ping Hu, Yan-Kun Qu, Fa-Yin Wang
Figure caption: Best fit for two three-parameter correlations: L b,z–T b,z–E  γ,iso and L b,z–T b,z–E p,i. Here L b,z is the luminosity at the break time of the plateau, T b,z is the corresponding break time in the rest frame, and E  γ,iso and E p,i are the isotropic and peak gamma-ray energy of the prompt emission, respectively. The red shaded region is the 95% confidence level.
Paper: Radio Plateaus in Gamma-Ray Burst Afterglows and Their Application in Cosmology
Authors: Xiao Tian, Jia-Lun Li, Shuang-Xi Yi, Yu-Peng Yang, Jian-Ping Hu, Yan-Kun Qu, Fa-Yin Wang
Figure caption: Fitting results of radio light curves with plateau components. We have used a smooth broken power-law function to fit these curves. The black dots represent the radio data, and the solid red lines represent the best fit to the radio data.
Paper: Radio Plateaus in Gamma-Ray Burst Afterglows and Their Application in Cosmology
Authors: Xiao Tian, Jia-Lun Li, Shuang-Xi Yi, Yu-Peng Yang, Jian-Ping Hu, Yan-Kun Qu, Fa-Yin Wang
Figure caption: Logarithmic plots of two-parameter correlations, L b,z–T b,z. The red shaded region is the 95% confidence level.
Paper: Radio Plateaus in Gamma-Ray Burst Afterglows and Their Application in Cosmology
Authors: Xiao Tian, Jia-Lun Li, Shuang-Xi Yi, Yu-Peng Yang, Jian-Ping Hu, Yan-Kun Qu, Fa-Yin Wang
Figure caption: Constraints on the cosmological parameters and calibrated GRB Hubble diagram for the L–T–E  γ,iso correlation.
Paper: Radio Plateaus in Gamma-Ray Burst Afterglows and Their Application in Cosmology
Authors: Xiao Tian, Jia-Lun Li, Shuang-Xi Yi, Yu-Peng Yang, Jian-Ping Hu, Yan-Kun Qu, Fa-Yin Wang
Figure caption: Constraints on the cosmological parameters and calibrated GRB Hubble diagram for the L–T–E p,i correlation.
Paper: Corrected SFD: A More Accurate Galactic Dust Map with Minimal Extragalactic Contamination
Authors: Yi-Kuan Chiang
Figure caption: Pixel value correlations between our reconstructed LSS/CIB map ﹩{\rm{\Delta }}{I}_{\mathrm{LSS}}^{{\rm{rec}}}﹩ on the x-axis vs. the IRAS 100 μm channel map (ΔI IRAS 100 μm;  left panel), and the Galactic H I map (ΔN H I;  right panel) on the y-axis over the 5% of the sky with the lowest foreground. All maps are beam-matched and high-pass filtered over 1°. Data points show the binned averages and 68th percentile ranges. The ﹩{\rm{\Delta }}{I}_{\mathrm{LSS}}^{{\rm{rec}}}﹩ correlates with ΔI IRAS 100 μm (left) with a best-fit linear relation (dashed line) close to an unbiased, one-to-one relation. The scatter in ﹩{\rm{\Delta }}{I}_{\mathrm{LSS}}^{{\rm{rec}}}﹩ (x-axis) is much smaller, as, unlike the IRAS channel map, our LSS map is foreground-free, which can be verified by the lack of correlation seen with the purely Galactic H I in the right panel.
Paper: Corrected SFD: A More Accurate Galactic Dust Map with Minimal Extragalactic Contamination
Authors: Yi-Kuan Chiang
Figure caption: Same as Figure 7 but now centered on four samples of DESI targets, BGS, LRG, ELG, and QSO, from left to right columns, respectively. Similar to that in Figure 7, the CSFD dust map has a much lower residual CIB contamination than SFD. In addition, the CSFD stacks (lower row) reveal that LRG, ELG, and QSO are preferentially selected against high extinction patches of the sky as they push the faint magnitude limits of the DESI Legacy imaging surveys. Such a selection systematic can be removed by re-thresholding the DESI samples using CSFD.
Paper: Corrected SFD: A More Accurate Galactic Dust Map with Minimal Extragalactic Contamination
Authors: Yi-Kuan Chiang
Figure caption: Redshift tomography for the 30 LSS base templates T LSS(ϕ) constructed using the 18 CatWISE samples (middle) and the 12 WISE×SuperCOSMOS ones (bottom); that for the additional AKARI point-source template is shown in the top panel. The estimator extracts the excess dimensionless map values within 10′ around the SDSS references, the same as that applied to SFD/CSFD in Figure 1, with an additional 1 + z factor to better visualize the high-redshift part. The CatWISE templates are essential in covering the distant Universe, and the SuperCOSMOS ones offer finer sampling in the more local Universe, providing the basis we need to reconstruct the CIB in SFD. The AKARI point sources are restricted to mostly z < 0.1.
Paper: Corrected SFD: A More Accurate Galactic Dust Map with Minimal Extragalactic Contamination
Authors: Yi-Kuan Chiang
Figure caption: Stacked images of the E(B − V) in SFD in the upper row and CSFD in the lower row. From left to right, the stacks are centered on Gaia stars, SDSS MAIN sample galaxies, 2MASS galaxies, and Gaia variability selected AGNs, respectively. Except for the stars, the E(B − V) in SFD around all of these galaxy samples are biased high due to the LSS contamination. Such bias is significantly reduced in CSFD.
Paper: Corrected SFD: A More Accurate Galactic Dust Map with Minimal Extragalactic Contamination
Authors: Yi-Kuan Chiang
Figure caption: Two-dimensional angular and redshift tomography for the 30 base LSS templates T LSS(ϕ) with the ID labeled in the upper right. Each pixel in this plot is a 2D cross-correlation with the SDSS references using the compensated filter, the same as in the lower (B) and (C) panels in Figure 1 for SFD/CSFD. This plot shows that the templates contain clustered LSS over a wide range of redshifts and angular scales needed for the reconstruction. For a clear visualization, the color is normalized separately in each panel over the minimum and maximum cross-amplitudes ΔT LSS,C(z, θ C).
Paper: Corrected SFD: A More Accurate Galactic Dust Map with Minimal Extragalactic Contamination
Authors: Yi-Kuan Chiang
Figure caption: Stacked SFD E(B − V) profiles (left) and peak values (right) at the locations of secured AKARI galaxies in our cosmology area binned in 90 μm flux. The profiles are consistent with an 8′ Gaussian, slightly more extended than the SFD beam, and the peak excess E(B − V) scales linearly with 90 μm flux. This forms the basis for constructing our zeroth LSS template.
Paper: Corrected SFD: A More Accurate Galactic Dust Map with Minimal Extragalactic Contamination
Authors: Yi-Kuan Chiang
Figure caption: Same as Figure 13 but now for the augmented LSS templates with six angular beam sizes for three selected base sets (base ID 23, 12, and 18 for the top, middle, and bottom panels, respectively). This plot shows how the beam augmentation shifts angular clustering toward progressively larger scales for larger beams, as expected.
Paper: Corrected SFD: A More Accurate Galactic Dust Map with Minimal Extragalactic Contamination
Authors: Yi-Kuan Chiang
Figure caption: Galaxy number density in the W1 vs. W1–W2 color–magnitude space of the full-sky CatWISE2020 catalog (Marocco et al. 2021) in our LSS reconstruction footprint. Dashed lines define the 18 cells we use to build our first part of the base LSS templates.
Paper: Corrected SFD: A More Accurate Galactic Dust Map with Minimal Extragalactic Contamination
Authors: Yi-Kuan Chiang
Figure caption: Redshift distributions for the cross-correlation reference sample and subsamples from spectroscopic galaxies and quasars in SDSS.
Paper: Kinetic-scale Topological Structures Associated with Energy Dissipation in the Turbulent Reconnection Outflow
Authors: S. Y. Huang, J. Zhang, Q. Y. Xiong, Z. G. Yuan, K. Jiang, S. B. Xu, Y. Y. Wei, R. T. Lin, L. Yu, Z. Wang
Figure caption: The joint pdf of (a) P(nR  X , nQ  X ), (b) P(nQ  J , − nQ  K ), (c) ﹩P({{nQ}}_{{\rm{\Omega }}}^{e},-{{nQ}}_{D}^{e})﹩, (d) ﹩P({{nQ}}_{{\rm{\Omega }}}^{i},-{{nQ}}_{D}^{i})﹩. The magenta line refers to the discriminant line D  X  = 0.
Paper: HST FUV Spectroscopy of Super Star Cluster A in the Green Pea Analog Mrk 71: Revealing the Presence of Very Massive Stars
Authors: Linda J. Smith, M. S. Oey, Svea Hernandez, Jenna Ryon, Claus Leitherer, Stephane Charlot, Gustavo Bruzual, Daniela Calzetti, You-Hua Chu, Matthew J. Hayes, Bethan L. James, Anne E. Jaskot, Göran Östlin
Figure caption: Top panel: Comparison of the Mrk 71-A STIS spectrum with the best-fitting C&B models (upper mass limits M  U  = 300, 600 M ⊙, Z = 0.002, age =1 Myr). The main stellar features (above the spectrum) and interstellar lines (below the spectrum) are identified. Bottom panel: Comparison for a C&B model with M  U  = 300 M ⊙, Z = 0.004, age =1 Myr. The flux is in units of 10−15 erg cm−2 s−1 Å−1.
Paper: HST FUV Spectroscopy of Super Star Cluster A in the Green Pea Analog Mrk 71: Revealing the Presence of Very Massive Stars
Authors: Linda J. Smith, M. S. Oey, Svea Hernandez, Jenna Ryon, Claus Leitherer, Stephane Charlot, Gustavo Bruzual, Daniela Calzetti, You-Hua Chu, Matthew J. Hayes, Bethan L. James, Anne E. Jaskot, Göran Östlin
Figure caption: Normalized STIS spectra of SSCs A and B in Mrk 71 in the region of the Lyα absorption feature and interstellar absorption lines of Si II λ1260, O I λ1302, Si II λ1304, and C II λ λ 1334,1335. For SSC A, the observed spectrum (black) and the Lyα corrected spectrum (blue) are shown. The observed spectrum of SSC A (black) should be compared with the spectrum of SSC B (red) to gauge the different strengths of the Lyα absorption. The spectrum for SSC A (blue) should be compared with the spectrum of SSC B (red) to gauge the similar strengths of the interstellar absorption lines.
Paper: Kinetic-scale Topological Structures Associated with Energy Dissipation in the Turbulent Reconnection Outflow
Authors: S. Y. Huang, J. Zhang, Q. Y. Xiong, Z. G. Yuan, K. Jiang, S. B. Xu, Y. Y. Wei, R. T. Lin, L. Yu, Z. Wang
Figure caption: Time series of (a) nR  X , (b) nQ  X , (c) ﹩{\boldsymbol{j}}\cdot {{\boldsymbol{E}}}^{{\prime} }﹩, (d) nQ  J , (e) −nQ  K , (f) ﹩{{nQ}}_{{\rm{\Omega }}}^{e}﹩, (g) ﹩-{{nQ}}_{D}^{e}﹩, (h) ﹩{{nQ}}_{{\rm{\Omega }}}^{i}﹩, and (i) ﹩-{{nQ}}_{D}^{i}﹩. The detailed definitions and normalizations can be found in the main text.
Paper: HST FUV Spectroscopy of Super Star Cluster A in the Green Pea Analog Mrk 71: Revealing the Presence of Very Massive Stars
Authors: Linda J. Smith, M. S. Oey, Svea Hernandez, Jenna Ryon, Claus Leitherer, Stephane Charlot, Gustavo Bruzual, Daniela Calzetti, You-Hua Chu, Matthew J. Hayes, Bethan L. James, Anne E. Jaskot, Göran Östlin
Figure caption: Comparison of normalized FUV spectra of SSCs containing VMS. The spectra are ordered in increasing age and Z from top to bottom. All the spectra, except for the Sunburst Cluster, were obtained with the STIS G140L grating. The vertical dashed line represents the maximum wind velocity of −3300 km s−1 measured for the C IV P Cygni absorption in Mrk 71-A.
Paper: HST FUV Spectroscopy of Super Star Cluster A in the Green Pea Analog Mrk 71: Revealing the Presence of Very Massive Stars
Authors: Linda J. Smith, M. S. Oey, Svea Hernandez, Jenna Ryon, Claus Leitherer, Stephane Charlot, Gustavo Bruzual, Daniela Calzetti, You-Hua Chu, Matthew J. Hayes, Bethan L. James, Anne E. Jaskot, Göran Östlin
Figure caption: Top panel: STIS G140L spectrum of Mrk 71-A, with the error array plotted along the bottom. The main stellar features and interstellar lines are identified. The damped Lyα fit is shown in red, and the Lyα-corrected N V emission line profile is in blue. Bottom panel: FOS G130H and G190H spectra of Mrk 71-A. The main stellar features, as well as interstellar and nebular lines, are identified. The flux is in units of 10−15 erg cm−2 s−1 Å−1.
Paper: HST FUV Spectroscopy of Super Star Cluster A in the Green Pea Analog Mrk 71: Revealing the Presence of Very Massive Stars
Authors: Linda J. Smith, M. S. Oey, Svea Hernandez, Jenna Ryon, Claus Leitherer, Stephane Charlot, Gustavo Bruzual, Daniela Calzetti, You-Hua Chu, Matthew J. Hayes, Bethan L. James, Anne E. Jaskot, Göran Östlin
Figure caption: WFC3/UVIS F438W (blue), F502N (green), F814W (red) image of Mrk 71-A showing the positions of the long STIS slit and the FOS apertures (square represents G190H, and circle represents G130H observations).
Paper: Hidden Giants in JWST's PEARLS: An Ultramassive z = 4.26 Submillimeter Galaxy that Is Invisible to HST
Authors: Ian Smail, Ugnė Dudzevičiūtė, Mark Gurwell, Giovanni G. Fazio, S. P. Willner, A. M. Swinbank, Vinodiran Arumugam, Jake Summers, Seth H. Cohen, Rolf A. Jansen, Rogier A. Windhorst, Ashish Meena, Adi Zitrin, William C. Keel, Cheng Cheng, Dan Coe, Christopher J. Conselice, Jordan C. J. D'Silva, Simon P. Driver, Brenda Frye, Norman A. Grogin, Anton M. Koekemoer, Madeline A. Marshall, Mario Nonino, Nor Pirzkal, Aaron Robotham, Michael J. Rutkowski, Russell E. Ryan Jr., Scott Tompkins, Christopher N. A. Willmer, Haojing Yan, Thomas J. Broadhurst, José M. Diego, Patrick Kamieneski, Min Yun
Figure caption: The stellar and interstellar medium (ISM) properties of 850.1 and 850.2. For comparison, several panels show samples of 870 μm selected ALMA-identified galaxies from the AS2UDS (Stach et al. 2019; Dudzevičiūtė et al. 2020) and AS2COSMOS (Simpson et al. 2019; S. Ikarashi et al. 2023, in preparation) surveys and the CO properties of a sample of submillimeter-continuum selected galaxies from Birkin et al. (2021). (a) The trend of specific SFR with stellar mass (SFR/M *–M *) where the dotted line shows the starburst boundary at z = 4 from Speagle et al. (2014). (b) A  V  vs. M *, where the dashed and dotted lines show the best-fit relation and 1σ scatter for a K-selected z > 4 galaxies sample with M * > 1010 M ⊙ drawn from the UKIDSS UDS survey (Lawrence et al. 2007) analyzed by Dudzevičiūtė et al. (2020). (c) The dust temperature vs. far-infrared luminosity (L IR–T  d ) relation. (d) CO-derived gas fraction, M g/(M g + M *), as a function of redshift, including low-redshift SMG-analogs from Oteo et al. (2017). (e) The ratio of the [C I]/CO(4–3) line luminosities vs. the [C I] to far-infrared luminosity ratio, which also include sources and photodissociation region (PDR) model tracks from Alaghband-Zadeh et al. (2013) and Valentino et al. (2020). The literature sources are flagged if they are estimated to have ≥20% contributions from an AGN to their far-infrared luminosities (Valentino et al. 2020). (f) Dust-to-stellar mass ratio, M d/M *, as a function of gas consumption timescale, M g/SFR, including two model tracks from Calura et al. (2017) for halos with baryonic masses of 1011 M ⊙ and 1012 M ⊙ roughly matching 850.2 and 850.1, respectively. The tracks were rescaled from their assumed Larson IMF with m c = 1.2 for comparison to the MAGPHYS derived values.
Paper: Hidden Giants in JWST's PEARLS: An Ultramassive z = 4.26 Submillimeter Galaxy that Is Invisible to HST
Authors: Ian Smail, Ugnė Dudzevičiūtė, Mark Gurwell, Giovanni G. Fazio, S. P. Willner, A. M. Swinbank, Vinodiran Arumugam, Jake Summers, Seth H. Cohen, Rolf A. Jansen, Rogier A. Windhorst, Ashish Meena, Adi Zitrin, William C. Keel, Cheng Cheng, Dan Coe, Christopher J. Conselice, Jordan C. J. D'Silva, Simon P. Driver, Brenda Frye, Norman A. Grogin, Anton M. Koekemoer, Madeline A. Marshall, Mario Nonino, Nor Pirzkal, Aaron Robotham, Michael J. Rutkowski, Russell E. Ryan Jr., Scott Tompkins, Christopher N. A. Willmer, Haojing Yan, Thomas J. Broadhurst, José M. Diego, Patrick Kamieneski, Min Yun
Figure caption: (a) The spectral energy distributions (SEDs) for 850.1 (including B2) and (b) 850.2, showing the measured photometry (Tables 1 & 4) and the best-fit MAGPHYS model at the redshifts determined from the NOEMA CO observations, z = 4.26. The lower two panels, (c) and (d), show an expanded view of the rest-frame UV–near-infrared region of the SEDs. Two SEDs are shown for each source, one derived from summing the resolved-pixel-level SED fits (Σpix, including B2) and one from fitting to the integrated source photometry. For the latter in 850.1, the individual fits to B2 and 850.1 were summed, although the emission longward of ∼3 μm is dominated by 850.1. Wave bands used in the resolved-pixel fits are shown as solid points. For the source-integrated fits, these bands were used as well as the unresolved photometry in the wave bands marked with open symbols. Also shown for comparison are the composite SED from the MAGPHYS analysis of z   ≥ 3 SMGs from the AS2UDS survey by Dudzevičiūtė et al. (2020) and the SED of Arp 220, both normalized to the SMA 880 μm flux density. These illustrate that the combined SED of 850.1+B2 is similar to the AS2UDS composite between rest-frame B band (observed ∼2μm) and the near-infrared, but due to the contribution from B2 it becomes much bluer into the rest-frame UV, better matching Arp 220. 850.1 alone is redder than the AS2UDS composite shortward of 2 μm. While 850.2 has an SED comparable to Arp 220 longward of ∼3 μm (rest frame ∼6000 Å) but bluer shortward of this and considerably bluer than the AS2UDS composite. In panel (c) the results of fitting to the photometry and limits for just 850.1 are shown (gray open squares), as well as a single MAGPHYS fit to the combined (“unresolved”) photometry from 850.1 and B2, illustrating that this provides a poorer description of the observations, especially longward of 3 μm. In all panels, the resolved-pixel modeling, Σpix, had only a single constraint beyond 4.4 μm from the SMA at 880 μm, yet it does at least as well out to 8 μm as the fits to the integrated source photometry (that included the IRAC 5.8 and 8.0 μm fluxes in the fit), although the absence of spatially resolved constraints at 450 μm resulted in poorer agreement in the rest-frame far-infrared region.
Paper: Hidden Giants in JWST's PEARLS: An Ultramassive z = 4.26 Submillimeter Galaxy that Is Invisible to HST
Authors: Ian Smail, Ugnė Dudzevičiūtė, Mark Gurwell, Giovanni G. Fazio, S. P. Willner, A. M. Swinbank, Vinodiran Arumugam, Jake Summers, Seth H. Cohen, Rolf A. Jansen, Rogier A. Windhorst, Ashish Meena, Adi Zitrin, William C. Keel, Cheng Cheng, Dan Coe, Christopher J. Conselice, Jordan C. J. D'Silva, Simon P. Driver, Brenda Frye, Norman A. Grogin, Anton M. Koekemoer, Madeline A. Marshall, Mario Nonino, Nor Pirzkal, Aaron Robotham, Michael J. Rutkowski, Russell E. Ryan Jr., Scott Tompkins, Christopher N. A. Willmer, Haojing Yan, Thomas J. Broadhurst, José M. Diego, Patrick Kamieneski, Min Yun
Figure caption: 6″ × 6″ thumbnails of 850.1 and 850.2. From left to right, the panels show the HST ACS F435W, F606W, and F814W imaging and JWST NIRCam F090W, F150W, F200W, F277W, F356W, and F444W images. The striking red colors of 850.1 are clear as the bulk of the emission from the galaxy, apart from the knots B1 and B2 (we suggest that the former is likely to be foreground), is undetectable shortward of 2 μm (the F200W band). In contrast, the high surface brightness regions of 850.2 are detected down to F606W (corresponding to ∼1100 Å in the rest frame at z = 4.26), but are undetected in F435W (rest frame ∼830 Å) showing the presence of a strong Lyman break. Fitted ellipses at three isophote levels are overlaid on the F356W image of 850.1, illustrating the “bar”-like feature seen in the central regions of the galaxy. At z = 4.26, the 912-Å Lyman break falls at the extreme red end of the F435W filter transmission, while the Lyα emission line falls in F606W, Hα in F356W (strong emission from which likely explains the pointlike feature C1 in 850.2, which probably corresponds to a giant [HII] region with an intrinsic size of ∼50–100 pc), and the nebular emission lines [OIII] 4959/5007 are in F277W and [OII] 3727 lies in F200W. The various sources and features discussed in the text are identified on the F090W thumbnails.
Paper: Hidden Giants in JWST's PEARLS: An Ultramassive z = 4.26 Submillimeter Galaxy that Is Invisible to HST
Authors: Ian Smail, Ugnė Dudzevičiūtė, Mark Gurwell, Giovanni G. Fazio, S. P. Willner, A. M. Swinbank, Vinodiran Arumugam, Jake Summers, Seth H. Cohen, Rolf A. Jansen, Rogier A. Windhorst, Ashish Meena, Adi Zitrin, William C. Keel, Cheng Cheng, Dan Coe, Christopher J. Conselice, Jordan C. J. D'Silva, Simon P. Driver, Brenda Frye, Norman A. Grogin, Anton M. Koekemoer, Madeline A. Marshall, Mario Nonino, Nor Pirzkal, Aaron Robotham, Michael J. Rutkowski, Russell E. Ryan Jr., Scott Tompkins, Christopher N. A. Willmer, Haojing Yan, Thomas J. Broadhurst, José M. Diego, Patrick Kamieneski, Min Yun
Figure caption: 6″ × 6″ thumbnails of 850.1 and 850.2 showing the JWST F200W and F444W images along with the pixel-based MAGPHYS estimates of the log-scaled stellar mass and A  V . The stellar-mass surface density is per 0.″18× 0.″18 pixel, corresponding to ∼0.6 × 0.6 kpc in the source plane for 850.1 and ∼0.5 × 0.5 kpc for 850.2. B1 was excluded from the map for 850.1 due to the poor quality of the SED fits at z = 4.26, supporting its likely lower redshift. B2 has much lower A  V  and stellar-mass surface density compared to the bulk of the massive and dusty remainder of 850.1. These very distinct properties motivate the decision to fit B2 and the bulk of 850.1 separately and then sum the results. In contrast, 850.2 exhibits a smaller variation in A  V  and stellar-mass surface density across the source.
Paper: Hidden Giants in JWST's PEARLS: An Ultramassive z = 4.26 Submillimeter Galaxy that Is Invisible to HST
Authors: Ian Smail, Ugnė Dudzevičiūtė, Mark Gurwell, Giovanni G. Fazio, S. P. Willner, A. M. Swinbank, Vinodiran Arumugam, Jake Summers, Seth H. Cohen, Rolf A. Jansen, Rogier A. Windhorst, Ashish Meena, Adi Zitrin, William C. Keel, Cheng Cheng, Dan Coe, Christopher J. Conselice, Jordan C. J. D'Silva, Simon P. Driver, Brenda Frye, Norman A. Grogin, Anton M. Koekemoer, Madeline A. Marshall, Mario Nonino, Nor Pirzkal, Aaron Robotham, Michael J. Rutkowski, Russell E. Ryan Jr., Scott Tompkins, Christopher N. A. Willmer, Haojing Yan, Thomas J. Broadhurst, José M. Diego, Patrick Kamieneski, Min Yun
Figure caption: Comparisons between the (a) stellar-mass effective radii and (b) stellar-mass surface densities of 850.1 and 850.2 with z ∼ 0 quiescent early-type galaxies from the ATLAS-3D survey (Cappellari et al. 2011, 2013), color-coded by their formation redshift as determined from their SSP ages in McDermid et al. (2015). In addition, a sample of quiescent galaxies at z ∼ 1.5 with F160W-derived sizes and high stellar masses from Longhetti et al. (2007) are shown. Also plotted are the F444W-derived sizes and stellar densities for z ∼ 1–3 SMGs from Chen et al. (2022). The red arrow on both panels shows the effect of the expected (empirically and theoretically) size evolution from z = 4.26 to z ∼ 0, and the tick indicates the evolution to z = 1.5 for a massive galaxy such as 850.1 (Cimatti et al. 2012; Oser et al. 2012). This demonstrates that 850.1 will likely evolve to have a stellar size and surface mass density similar to those of massive, compact quiescent galaxies at z ∼ 1.5, and then go on to match the properties of the most massive, and oldest, early-type galaxies at the present day.