adsabs/AstroCLIMB huggingface dataset:
Paper: Nuclear Activity in the Low-metallicity Dwarf Galaxy SDSS J0944-0038 : A Glimpse into the Primordial Universe
Authors: Michael Reefe, Shobita Satyapal, Remington O. Sexton, Nathan J. Secrest, William Matzko, Emma Schwartzman, Kristina Nyland, Gabriela Canalizo, Barry Rothberg, Ryan W. Pfeifle, Jenna M. Cann, Archana Aravindan, Camilo Vazquez, Tracy Clarke
Figure caption: Top: 1D extraction of the MUSE spectrum from a 1″ diameter circular aperture centered on Nucleus 1 (corresponding to the positions of the northern white circle in Figure 3) showing the [Fe X] λ6374 and Hα region of the spectrum. The spectrum of Nucleus 1 was decomposed into broad and narrow components. A broad line was detected at the >99.92% confidence level in Nucleus 1 with an FWHM of 446 ± 17 km s−1. Center: 1D MUSE spectrum from a 1″ circular aperture centered on Nucleus 2 (southern white circle in Figure 3). Bottom: 1D SDSS spectrum from the 3″ fiber. No significant broad lines could be fit from with MUSE Nucleus 2 or SDSS spectrum.
Paper: Nuclear Activity in the Low-metallicity Dwarf Galaxy SDSS J0944-0038 : A Glimpse into the Primordial Universe
Authors: Michael Reefe, Shobita Satyapal, Remington O. Sexton, Nathan J. Secrest, William Matzko, Emma Schwartzman, Kristina Nyland, Gabriela Canalizo, Barry Rothberg, Ryan W. Pfeifle, Jenna M. Cann, Archana Aravindan, Camilo Vazquez, Tracy Clarke
Figure caption:  M BH–M bulge relation for classical bulges and elliptical morphological types from Kormendy & Ho (2013) extrapolated to the estimated stellar mass of 6.76 × 106 M ⊙ and virial BH mass estimate of M BH ∼ 3150 M ⊙. The shaded region represents the 95% confidence interval for the fit to the M BH–M bulge relation, which has an intrinsic scatter of 0.29 dex.
Paper: Nuclear Activity in the Low-metallicity Dwarf Galaxy SDSS J0944-0038 : A Glimpse into the Primordial Universe
Authors: Michael Reefe, Shobita Satyapal, Remington O. Sexton, Nathan J. Secrest, William Matzko, Emma Schwartzman, Kristina Nyland, Gabriela Canalizo, Barry Rothberg, Ryan W. Pfeifle, Jenna M. Cann, Archana Aravindan, Camilo Vazquez, Tracy Clarke
Figure caption: VLA X-band contours of the radio emission coincident with the [Fe X] source, overlaid on a 2″×2″ cutout ofthe HST image from Figure 1. The contours start at the 3σ level (23.5 µJy beam−1) and increase by integer multiples of the √2. The VLA image has an angular resolution of 0.2.
Paper: The Radio to GeV Afterglow of GRB 221009A
Authors: Tanmoy Laskar, Kate D. Alexander, Raffaella Margutti, Tarraneh Eftekhari, Ryan Chornock, Edo Berger, Yvette Cendes, Anne Duerr, Daniel A. Perley, Maria Edvige Ravasio, Ryo Yamazaki, Eliot H. Ayache, Thomas Barclay, Rodolfo Barniol Duran, Shivani Bhandari, Daniel Brethauer, Collin T. Christy, Deanne L. Coppejans, Paul Duffell, Wen-fai Fong, Andreja Gomboc, Cristiano Guidorzi, Jamie A. Kennea, Shiho Kobayashi, Andrew Levan, Andrei P. Lobanov, Brian D. Metzger, Eduardo Ros, Genevieve Schroeder, P. K. G. Williams
Figure caption: Light curves of GRB 221009A from 1 GeV to 400 MHz together with the broken power-law model fits used to interpolate data to a common time and to inform the multiwavelength modeling (Sections 3.1 and 3.2). The light curves have been multiplied by the factors listed in the legends to offset them in the plot for clarity. The three panels with radio data are on the same temporal scale to facilitate comparison.
Paper: The Radio to GeV Afterglow of GRB 221009A
Authors: Tanmoy Laskar, Kate D. Alexander, Raffaella Margutti, Tarraneh Eftekhari, Ryan Chornock, Edo Berger, Yvette Cendes, Anne Duerr, Daniel A. Perley, Maria Edvige Ravasio, Ryo Yamazaki, Eliot H. Ayache, Thomas Barclay, Rodolfo Barniol Duran, Shivani Bhandari, Daniel Brethauer, Collin T. Christy, Deanne L. Coppejans, Paul Duffell, Wen-fai Fong, Andreja Gomboc, Cristiano Guidorzi, Jamie A. Kennea, Shiho Kobayashi, Andrew Levan, Andrei P. Lobanov, Brian D. Metzger, Eduardo Ros, Genevieve Schroeder, P. K. G. Williams
Figure caption: SEDs (left) and a sampling of available light curves (right) at X-ray, UV, optical, and NIR wavelengths of GRB 221009A (data points), together with the highest-likelihood FS wind model (lines) that explains most of these observations (Section 3.1). Thin lines indicate the underlying synchrotron spectrum. The break at ≈2 × 1014 Hz in the first epoch is ν m. The X-ray SEDs shown here are the result of joint spectral fits of Swift and NuSTAR observations at the corresponding times (Section 2.4.2). Optical points have been interpolated using the best-fit broken power-law light curves (Figure 1). The model cannot explain the UV/optical light curves at ≲1 day; these points (open symbols) were excluded from the fit. These caveats are discussed further in Section 4.3.
Paper: The Radio to GeV Afterglow of GRB 221009A
Authors: Tanmoy Laskar, Kate D. Alexander, Raffaella Margutti, Tarraneh Eftekhari, Ryan Chornock, Edo Berger, Yvette Cendes, Anne Duerr, Daniel A. Perley, Maria Edvige Ravasio, Ryo Yamazaki, Eliot H. Ayache, Thomas Barclay, Rodolfo Barniol Duran, Shivani Bhandari, Daniel Brethauer, Collin T. Christy, Deanne L. Coppejans, Paul Duffell, Wen-fai Fong, Andreja Gomboc, Cristiano Guidorzi, Jamie A. Kennea, Shiho Kobayashi, Andrew Levan, Andrei P. Lobanov, Brian D. Metzger, Eduardo Ros, Genevieve Schroeder, P. K. G. Williams
Figure caption: Correlations and marginalized posterior density from multiwavelength modeling of GRB 221009A with E K,iso and E K in erg. We compute the opening angle (θ jet) in degrees from E K,iso, A *, and t jet. The contours enclose 39.3%, 86.4%, and 98.9% of the probability mass in each correlation plot (corresponding to 1σ, 2σ, and 3σ regions for two-dimensional Gaussian distributions), while the dashed lines in the histograms indicate the 15.9%, 50% (median), and 84.1% quantiles (corresponding to ±1σ for one-dimensional Gaussian distributions). The distribution for ϵ B cuts off at high values due to the prior bound of ϵ e + ϵ B < 1. Strong correlations are evident between most parameters as ν a is unconstrained in this model. See Table 6 for a summary.
Paper: The Radio to GeV Afterglow of GRB 221009A
Authors: Tanmoy Laskar, Kate D. Alexander, Raffaella Margutti, Tarraneh Eftekhari, Ryan Chornock, Edo Berger, Yvette Cendes, Anne Duerr, Daniel A. Perley, Maria Edvige Ravasio, Ryo Yamazaki, Eliot H. Ayache, Thomas Barclay, Rodolfo Barniol Duran, Shivani Bhandari, Daniel Brethauer, Collin T. Christy, Deanne L. Coppejans, Paul Duffell, Wen-fai Fong, Andreja Gomboc, Cristiano Guidorzi, Jamie A. Kennea, Shiho Kobayashi, Andrew Levan, Andrei P. Lobanov, Brian D. Metzger, Eduardo Ros, Genevieve Schroeder, P. K. G. Williams
Figure caption: Left: radio to X-ray SEDs (same as Figure 4), together with a fiducial, single-component, broken power-law SED model (lines) where the three break frequencies evolve with time as ν peak ∝ t −0.49, ﹩{\nu }_{{{\rm{b}}}_{1}}\propto {t}^{-1.32}﹩, and ﹩{\nu }_{{{\rm{b}}}_{2}}\propto {t}^{0}﹩, while the peak flux evolves as F  ν,peak ∝ t −0.7 (motivated by the observed radio evolution; see Figure 5). The underlying model without the ≈4.3 mag of total extinction is shown as thin lines. Right: the corresponding light curves from the GeV to the millimeter band. The model underpredicts the optical observations at ≲3 days, the entire 1.3 mm light curve, and does not match any of the temporal breaks seen in the 3 mm light curve.
Paper: The Power of the Rings: The GRB 221009A Soft X-Ray Emission from Its Dust-scattering Halo
Authors: Andrea Tiengo, Fabio Pintore, Beatrice Vaia, Simone Filippi, Andrea Sacchi, Paolo Esposito, Michela Rigoselli, Sandro Mereghetti, Ruben Salvaterra, Barbara Šiljeg, Andrea Bracco, Željka Bošnjak, Vibor Jelić, Sergio Campana
Figure caption: Left panel: differential extinction in the direction of GRB 221009A from Lallement et al. (2022), sampled every 5 pc and obtained using the G-Tomo app on the EXPLORE website (https://explore-platform.eu). Vertical red lines and light blue shaded areas indicate the distances and widths of dust layers producing rings 0–6 (Table 1). Right panel: cumulative extinction from Green et al. (2019) in eight equally spaced directions along the average position of ring 6 during Obs2 (∼11.5﹩{}^{{\prime} }﹩ from GRB 221009A), extracted using the dustmaps software (Green 2018).
Paper: The Radio to GeV Afterglow of GRB 221009A
Authors: Tanmoy Laskar, Kate D. Alexander, Raffaella Margutti, Tarraneh Eftekhari, Ryan Chornock, Edo Berger, Yvette Cendes, Anne Duerr, Daniel A. Perley, Maria Edvige Ravasio, Ryo Yamazaki, Eliot H. Ayache, Thomas Barclay, Rodolfo Barniol Duran, Shivani Bhandari, Daniel Brethauer, Collin T. Christy, Deanne L. Coppejans, Paul Duffell, Wen-fai Fong, Andreja Gomboc, Cristiano Guidorzi, Jamie A. Kennea, Shiho Kobayashi, Andrew Levan, Andrei P. Lobanov, Brian D. Metzger, Eduardo Ros, Genevieve Schroeder, P. K. G. Williams
Figure caption: Left: radio SEDs from our uGMRT, VLA, ALMA, NOEMA, and SMA observations reveal a self-absorbed spectrum with a peak at ≈2 GHz. The spectral index above the peak is shallow (β ≈ −0.2) with a flattening in the millimeter band (≳100 GHz), as confirmed by extrapolations (open circles) of broken power-law model fits (lines) to the observations at ≲50 GHz. Right: evolution of peak flux and peak frequency from broken power-law fits to the radio SED at ≲50 GHz (Table 7).
Paper: The Power of the Rings: The GRB 221009A Soft X-Ray Emission from Its Dust-scattering Halo
Authors: Andrea Tiengo, Fabio Pintore, Beatrice Vaia, Simone Filippi, Andrea Sacchi, Paolo Esposito, Michela Rigoselli, Sandro Mereghetti, Ruben Salvaterra, Barbara Šiljeg, Andrea Bracco, Željka Bošnjak, Vibor Jelić, Sergio Campana
Figure caption: EPIC exposure-corrected 0.7–4 keV images, in units of counts s−1 arcmin−2, of the expanding rings from Obs1 (top panels: MOS2 data in three consecutive time intervals with ∼16 ks of exposure time each) and Obs2 (bottom panels, from left to right: MOS1, MOS2, and PN data for the full 33 ks time interval of quiescent background). All the images have been smoothed with a Gaussian kernel of σ = 2.″5. Two red circles of radii ﹩{8}^{{\prime} }﹩ and ﹩{11}^{{\prime} }﹩ are shown as a reference for ring expansion.
Paper: The Radio to GeV Afterglow of GRB 221009A
Authors: Tanmoy Laskar, Kate D. Alexander, Raffaella Margutti, Tarraneh Eftekhari, Ryan Chornock, Edo Berger, Yvette Cendes, Anne Duerr, Daniel A. Perley, Maria Edvige Ravasio, Ryo Yamazaki, Eliot H. Ayache, Thomas Barclay, Rodolfo Barniol Duran, Shivani Bhandari, Daniel Brethauer, Collin T. Christy, Deanne L. Coppejans, Paul Duffell, Wen-fai Fong, Andreja Gomboc, Cristiano Guidorzi, Jamie A. Kennea, Shiho Kobayashi, Andrew Levan, Andrei P. Lobanov, Brian D. Metzger, Eduardo Ros, Genevieve Schroeder, P. K. G. Williams
Figure caption: Multiepoch SEDs from our uGMRT, VLA, ALMA, NOEMA, and SMA programs, compared with optical observations and Swift/XRT SEDs at similar times, together with a wind FS model (lines). The FS cannot explain the observed radio flux and slowly evolving radio peak.
Paper: The Power of the Rings: The GRB 221009A Soft X-Ray Emission from Its Dust-scattering Halo
Authors: Andrea Tiengo, Fabio Pintore, Beatrice Vaia, Simone Filippi, Andrea Sacchi, Paolo Esposito, Michela Rigoselli, Sandro Mereghetti, Ruben Salvaterra, Barbara Šiljeg, Andrea Bracco, Željka Bošnjak, Vibor Jelić, Sergio Campana
Figure caption: Azimuthal distribution of the MOS2 exposure-corrected surface brightness in the 0.7–4 keV band detected between ﹩4\buildrel{\,\prime}\over{.} 8﹩ and ﹩5\buildrel{\,\prime}\over{.} 8﹩ (thick solid blue line) and between ﹩11\buildrel{\,\prime}\over{.} 1﹩ and ﹩12\buildrel{\,\prime}\over{.} 1﹩ (thin solid red line) from the GRB position in Obs2. Each annulus contains two rings: 13 and 14, produced by dust at ∼3.5 kpc, and rings 5 and 6, produced by dust at ∼0.7 kpc. Both annuli are compared to the same background signal (black dashed line), extracted from an ﹩{8}^{{\prime} }﹩–﹩10\buildrel{\,\prime}\over{.} 5﹩ annulus, where only two very faint rings (7 and 8) have been detected. All point sources have been excluded.
Paper: The Power of the Rings: The GRB 221009A Soft X-Ray Emission from Its Dust-scattering Halo
Authors: Andrea Tiengo, Fabio Pintore, Beatrice Vaia, Simone Filippi, Andrea Sacchi, Paolo Esposito, Michela Rigoselli, Sandro Mereghetti, Ruben Salvaterra, Barbara Šiljeg, Andrea Bracco, Željka Bošnjak, Vibor Jelić, Sergio Campana
Figure caption: Fit of the ring spectra with the BARE-GR-B model (best-fit parameters in Table 2). Top panel: PN (black) and MOS2 (red) spectra of ring 6 in Obs2. Middle panel: MOS2 spectra of rings 1–6 in Obs1. Bottom panel: MOS2 spectra of rings 1–6 in Obs1 and PN spectra of rings 7–19 in Obs2.
Paper: The Power of the Rings: The GRB 221009A Soft X-Ray Emission from Its Dust-scattering Halo
Authors: Andrea Tiengo, Fabio Pintore, Beatrice Vaia, Simone Filippi, Andrea Sacchi, Paolo Esposito, Michela Rigoselli, Sandro Mereghetti, Ruben Salvaterra, Barbara Šiljeg, Andrea Bracco, Željka Bošnjak, Vibor Jelić, Sergio Campana
Figure caption: Pseudodistance distributions in the 0.7–4 keV energy band for the two XMM-Newton observations (Obs1: top; Obs2: bottom). Arrows indicate the number of the rings as reported in Table 1. MOS2 data are in red and PN in blue. The green line of the top panel indicates the best-fit model with a power law plus 9 Lorentzian functions.
Paper: The Power of the Rings: The GRB 221009A Soft X-Ray Emission from Its Dust-scattering Halo
Authors: Andrea Tiengo, Fabio Pintore, Beatrice Vaia, Simone Filippi, Andrea Sacchi, Paolo Esposito, Michela Rigoselli, Sandro Mereghetti, Ruben Salvaterra, Barbara Šiljeg, Andrea Bracco, Željka Bošnjak, Vibor Jelić, Sergio Campana
Figure caption: Map of the total hydrogen column density in the sky area around GRB 221009A (Planck Collaboration 2014; see Appendix C for details. The white circles (radii of 2′ and 12′) indicate the region covered by the X-ray rings during XMM-Newton observations.
Paper: The Power of the Rings: The GRB 221009A Soft X-Ray Emission from Its Dust-scattering Halo
Authors: Andrea Tiengo, Fabio Pintore, Beatrice Vaia, Simone Filippi, Andrea Sacchi, Paolo Esposito, Michela Rigoselli, Sandro Mereghetti, Ruben Salvaterra, Barbara Šiljeg, Andrea Bracco, Željka Bošnjak, Vibor Jelić, Sergio Campana
Figure caption: EPIC-MOS2 exposure-corrected 0.7–4 keV images, in units of counts s−1 arcmin−2, of the expanding rings from Obs1 (left panel) and Obs2 (right panel). All the images have been smoothed with a Gaussian kernel of σ = 3.″5.
Paper: The Radio to GeV Afterglow of GRB 221009A
Authors: Tanmoy Laskar, Kate D. Alexander, Raffaella Margutti, Tarraneh Eftekhari, Ryan Chornock, Edo Berger, Yvette Cendes, Anne Duerr, Daniel A. Perley, Maria Edvige Ravasio, Ryo Yamazaki, Eliot H. Ayache, Thomas Barclay, Rodolfo Barniol Duran, Shivani Bhandari, Daniel Brethauer, Collin T. Christy, Deanne L. Coppejans, Paul Duffell, Wen-fai Fong, Andreja Gomboc, Cristiano Guidorzi, Jamie A. Kennea, Shiho Kobayashi, Andrew Levan, Andrei P. Lobanov, Brian D. Metzger, Eduardo Ros, Genevieve Schroeder, P. K. G. Williams
Figure caption: Left: radio spectral luminosity at 8 GHz (rest frame) as a function of rest-frame time for GRBs (deep blue), subenergetic GRBs (light blue), SNe with evidence for relativistic ejecta (dark gray), and hydrogen-poor SNe (light gray). The radio afterglow of GRB 221009A is more luminous than any known radio SN and comparable in luminosity to the afterglows of typical long GRBs. Right: the same plot showing X-ray luminosity in the 0.3–10 keV band. In contrast to the radio, GRB 221009A is one of the most X-ray-luminous GRBs for much of its evolution. Adapted from Margutti et al. (2014).
Paper: The Radio to GeV Afterglow of GRB 221009A
Authors: Tanmoy Laskar, Kate D. Alexander, Raffaella Margutti, Tarraneh Eftekhari, Ryan Chornock, Edo Berger, Yvette Cendes, Anne Duerr, Daniel A. Perley, Maria Edvige Ravasio, Ryo Yamazaki, Eliot H. Ayache, Thomas Barclay, Rodolfo Barniol Duran, Shivani Bhandari, Daniel Brethauer, Collin T. Christy, Deanne L. Coppejans, Paul Duffell, Wen-fai Fong, Andreja Gomboc, Cristiano Guidorzi, Jamie A. Kennea, Shiho Kobayashi, Andrew Levan, Andrei P. Lobanov, Brian D. Metzger, Eduardo Ros, Genevieve Schroeder, P. K. G. Williams
Figure caption: Radio SEDs (left) and light curves (right) for a low-p ISM model with parameters p = 1.5, ϵ e = 0.07, ϵ B = 0.03, n 0 = 10 cm−3, E K,iso = 1.5 × 1052 erg, and A V,host = 0.3 mag. This model requires a jet break at t jet = 0.55 days (implying θ jet = 9° and E K = 2 × 1050 erg) in order to match the X-ray and optical light curves; however, the model significantly overpredicts the millimeter-band observations at ≲28 days, overpredicts the Fermi/LAT observations by two orders of magnitude, and does not match the centimeter-band SED at all, and is therefore ruled out.
Paper: The Radio to GeV Afterglow of GRB 221009A
Authors: Tanmoy Laskar, Kate D. Alexander, Raffaella Margutti, Tarraneh Eftekhari, Ryan Chornock, Edo Berger, Yvette Cendes, Anne Duerr, Daniel A. Perley, Maria Edvige Ravasio, Ryo Yamazaki, Eliot H. Ayache, Thomas Barclay, Rodolfo Barniol Duran, Shivani Bhandari, Daniel Brethauer, Collin T. Christy, Deanne L. Coppejans, Paul Duffell, Wen-fai Fong, Andreja Gomboc, Cristiano Guidorzi, Jamie A. Kennea, Shiho Kobayashi, Andrew Levan, Andrei P. Lobanov, Brian D. Metzger, Eduardo Ros, Genevieve Schroeder, P. K. G. Williams
Figure caption: Beaming-corrected kinetic energies of GRBs with multiwavelength data sets and known jet opening angles, as a function of redshift, together with the value of E K for GRB 221009A derived from our best-fit FS model. The extraordinary brightness of GRB 221009A at high energies may arise from a combination of its proximity and a narrow beaming angle, rather than a high intrinsic E K.
Paper: The Radio to GeV Afterglow of GRB 221009A
Authors: Tanmoy Laskar, Kate D. Alexander, Raffaella Margutti, Tarraneh Eftekhari, Ryan Chornock, Edo Berger, Yvette Cendes, Anne Duerr, Daniel A. Perley, Maria Edvige Ravasio, Ryo Yamazaki, Eliot H. Ayache, Thomas Barclay, Rodolfo Barniol Duran, Shivani Bhandari, Daniel Brethauer, Collin T. Christy, Deanne L. Coppejans, Paul Duffell, Wen-fai Fong, Andreja Gomboc, Cristiano Guidorzi, Jamie A. Kennea, Shiho Kobayashi, Andrew Levan, Andrei P. Lobanov, Brian D. Metzger, Eduardo Ros, Genevieve Schroeder, P. K. G. Williams
Figure caption: Spectral luminosity of GRB 221009A as a function of rest-frame time in the 3 mm band (red stars), compared to a population of long-duration GRBs (deep blue), SNe (gray), tidal disruption events (light green), and fast blue optical transients (light blue). No K-corrections for variations in intrinsic spectral shape have been applied. The millimeter-band emission from GRB 221009A is a factor of ≈5–10 less luminous than GRB 030329 (orange), but of comparable luminosity to that of other GRB afterglows. Adapted from Eftekhari et al. (2022).
Paper: The Radio to GeV Afterglow of GRB 221009A
Authors: Tanmoy Laskar, Kate D. Alexander, Raffaella Margutti, Tarraneh Eftekhari, Ryan Chornock, Edo Berger, Yvette Cendes, Anne Duerr, Daniel A. Perley, Maria Edvige Ravasio, Ryo Yamazaki, Eliot H. Ayache, Thomas Barclay, Rodolfo Barniol Duran, Shivani Bhandari, Daniel Brethauer, Collin T. Christy, Deanne L. Coppejans, Paul Duffell, Wen-fai Fong, Andreja Gomboc, Cristiano Guidorzi, Jamie A. Kennea, Shiho Kobayashi, Andrew Levan, Andrei P. Lobanov, Brian D. Metzger, Eduardo Ros, Genevieve Schroeder, P. K. G. Williams
Figure caption: Radio SEDs (left) and light curves (right) for a joint wind model (solid lines) combining a reverse shock (dotted) with the forward-shock model (dashed) described in Section 3.1. This Newtonian RS model with g ≈ 5 is tailored to roughly match the centimeter-band SED at ≈17.48 days. Even with an extreme value of g, the RS model cannot match the rest of the radio data and the early (≲1 day) UV/optical light curves, and is therefore disfavored.
Paper: CEERS Key Paper. IV. A Triality in the Nature of HST-dark Galaxies
Authors: Pablo G. Pérez-González, Guillermo Barro, Marianna Annunziatella, Luca Costantin, Ángela García-Argumánez, Elizabeth J. McGrath, Rosa M. Mérida, Jorge A. Zavala, Pablo Arrabal Haro, Micaela B. Bagley, Bren E. Backhaus, Peter Behroozi, Eric F. Bell, Laura Bisigello, Véronique Buat, Antonello Calabrò, Caitlin M. Casey, Nikko J. Cleri, Rosemary T. Coogan, M. C. Cooper, Asantha R. Cooray, Avishai Dekel, Mark Dickinson, David Elbaz, Henry C. Ferguson, Steven L. Finkelstein, Adriano Fontana, Maximilien Franco, Jonathan P. Gardner, Mauro Giavalisco, Carlos Gómez-Guijarro, Andrea Grazian, Norman A. Grogin, Yuchen Guo, Marc Huertas-Company, Shardha Jogee, Jeyhan S. Kartaltepe, Lisa J. Kewley, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Arianna S. Long, Jennifer M. Lotz, Ray A. Lucas, Casey Papovich, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Sandro Tacchella, Jonathan R. Trump, Weichen Wang, Stephen M. Wilkins, Stijn Wuyts, Guang Yang, L. Y. Aaron Yung
Figure caption: Morphological properties of our sample of near-IR-faint, mid-IR-bright galaxies. On the left panel, we show the mass–size plot for HST-dark galaxies (hexagons) and HST-faint sources (circles), compared to the CEERS sample (gray-shaded density map). Sizes are represented by the effective radius of the Sérsic profile fit performed with the GALFIT software (Peng et al. 2002) on F356W images. MIPS24 emitters are marked with a cyan circle, submillimeter and radio galaxies with a blue star, quiescent galaxies by sSFR with a red square, and XELG-z6 with green triangles. We depict the scaling relationships for star-forming and quiescent galaxies at z = 2.75 (blue and red, respectively) from van der Wel et al. (2014). In the middle panels, histograms for the Sérsic index (top) and effective radius (bottom) are provided. We show estimations based on F356W images (light) as explained before, and on mass maps analyzed with the statmorph software (Rodriguez-Gomez et al. 2019). The middle-bottom panel also shows the distributions of Petrosian (1976) radii in mass maps. On the right panel, the mass–size relationship is again shown, this time based on mass map analyses performed with statmorph. Orange points show Petrosian radii. The blue and red lines show the (r  e,mass-based) mass–size relations for SFGs and quiescent galaxies from Suess et al. (2019). The cutouts on the bottom show the 5″ × 5″ images of XELG-z6 galaxies and other similar objects (not identified explicitly as such) at redshifts ranging from 5 < z < 7, also providing IDs and redshifts. From bottom to top, the images are color composites of three HST bands and three JWST bands, short and long wavelengths, respectively.