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Paper: The JWST Early Release Observations
Authors: Klaus M. Pontoppidan, Jaclyn Barrientes, Claire Blome, Hannah Braun, Matthew Brown, Margaret Carruthers, Dan Coe, Joseph DePasquale, Néstor Espinoza, Macarena Garcia Marin, Karl D. Gordon, Alaina Henry, Leah Hustak, Andi James, Ann Jenkins, Anton M. Koekemoer, Stephanie LaMassa, David Law, Alexandra Lockwood, Amaya Moro-Martin, Susan E. Mullally, Alyssa Pagan, Dani Player, Charles Proffitt, Christine Pulliam, Leah Ramsay, Swara Ravindranath, Neill Reid, Massimo Robberto, Elena Sabbi, Leonardo Ubeda, Michael Balogh, Kathryn Flanagan, Jonathan Gardner, Hashima Hasan, Bonnie Meinke, Antonella Nota
Figure caption: The NIRSpec MOS spectrum of a galaxy at z = 8.49 shows robust detections of Hβ and the [O III] λλ4960, 5008 doublet. The SNR on the lines ranges from 13 to 44.
Paper: Testing Galaxy Feedback Models with Resolved X-Ray Profiles of the Hot Circumgalactic Medium
Authors: Urmila Chadayammuri, Ákos Bogdán, Benjamin D. Oppenheimer, Ralph P. Kraft, William R. Forman, Christine Jones
Figure caption: Surface brightness profiles of the low-mass (left) and high-mass (right) stacks, split into star-forming (top) and quiescent (bottom) thirds. The green bands show the predictions for the TNG simulations, while the orange bands show EAGLE (Oppenheimer et al. 2020). The solid horizontal line shows the mean background for the stack, and the dotted line is 5% of this background. Black crosses show the background-corrected profile. Purple crosses remove the expected PSF-scattered contribution from LMXBs (shown as the solid curve), while blue additionally removes that from HMXBs and hot ISM (dotted curve). In the quiescent galaxies, by definition, the HMXB contribution is zero, so we correct only for the LMXB. Where the Poisson error is greater than the mean, we show only the upper error bar and mark the mean with a downward-pointing triangle.
Paper: Testing Galaxy Feedback Models with Resolved X-Ray Profiles of the Hot Circumgalactic Medium
Authors: Urmila Chadayammuri, Ákos Bogdán, Benjamin D. Oppenheimer, Ralph P. Kraft, William R. Forman, Christine Jones
Figure caption: Comparison of the mean observed and simulated luminosity from 10 to 100 kpc as a function of stellar mass, for star-forming (blue) and quiescent (red) galaxies, with the expected contribution from all XRBs removed. The observations are shown as crosses with 1σ Poisson error, as well as systematic errors from changing the background level by 5%. TNG is shown as crosses and EAGLE as hexagons.
Paper: Testing Galaxy Feedback Models with Resolved X-Ray Profiles of the Hot Circumgalactic Medium
Authors: Urmila Chadayammuri, Ákos Bogdán, Benjamin D. Oppenheimer, Ralph P. Kraft, William R. Forman, Christine Jones
Figure caption: Background-corrected surface brightness maps of the star-forming (top) and quiescent (bottom) low-mass (﹩10.2\lt \mathrm{log}({M}_{* }/{M}_{\odot })\lt 10.7﹩, left) and high-mass (﹩10.7\lt \mathrm{log}({M}_{* }/{M}_{\odot })\lt 11.2﹩, right) stacks in the 0.5–2.0 keV band. The annulus shows the region used to compute the background. Note that the emission from XRBs, scattered by the PSF, is not subtracted from these images. Emission is seen in all four stacks but is more extended in the high-mass galaxies and brighter in the center of star-forming galaxies. The scale bar corresponds to 50 kpc in each panel.
Paper: Testing Galaxy Feedback Models with Resolved X-Ray Profiles of the Hot Circumgalactic Medium
Authors: Urmila Chadayammuri, Ákos Bogdán, Benjamin D. Oppenheimer, Ralph P. Kraft, William R. Forman, Christine Jones
Figure caption: Comparison of stellar mass (top) and sSFR (bottom) distributions in our observed sample (blue), EAGLE (orange), and TNG (green). The stellar mass distributions are additionally shown for the star-forming and quiescent bins, and the sSFRs for the low- and high-mass bins. The vertical lines indicate the cutoffs for the star-forming (SF) and quiescent (Q) substacks for the sample of the corresponding color.
Paper: The JWST Early Release Observations
Authors: Klaus M. Pontoppidan, Jaclyn Barrientes, Claire Blome, Hannah Braun, Matthew Brown, Margaret Carruthers, Dan Coe, Joseph DePasquale, Néstor Espinoza, Macarena Garcia Marin, Karl D. Gordon, Alaina Henry, Leah Hustak, Andi James, Ann Jenkins, Anton M. Koekemoer, Stephanie LaMassa, David Law, Alexandra Lockwood, Amaya Moro-Martin, Susan E. Mullally, Alyssa Pagan, Dani Player, Charles Proffitt, Christine Pulliam, Leah Ramsay, Swara Ravindranath, Neill Reid, Massimo Robberto, Elena Sabbi, Leonardo Ubeda, Michael Balogh, Kathryn Flanagan, Jonathan Gardner, Hashima Hasan, Bonnie Meinke, Antonella Nota
Figure caption: Field of view of NGC 3132 covered by NIRCam and MIRI. The framing was selected using archival images from Spitzer, as shown.
Paper: The JWST Early Release Observations
Authors: Klaus M. Pontoppidan, Jaclyn Barrientes, Claire Blome, Hannah Braun, Matthew Brown, Margaret Carruthers, Dan Coe, Joseph DePasquale, Néstor Espinoza, Macarena Garcia Marin, Karl D. Gordon, Alaina Henry, Leah Hustak, Andi James, Ann Jenkins, Anton M. Koekemoer, Stephanie LaMassa, David Law, Alexandra Lockwood, Amaya Moro-Martin, Susan E. Mullally, Alyssa Pagan, Dani Player, Charles Proffitt, Christine Pulliam, Leah Ramsay, Swara Ravindranath, Neill Reid, Massimo Robberto, Elena Sabbi, Leonardo Ubeda, Michael Balogh, Kathryn Flanagan, Jonathan Gardner, Hashima Hasan, Bonnie Meinke, Antonella Nota
Figure caption: Field of view in SMACS J0723.3-7327 covered by NIRCam and MIRI.
Paper: The JWST Early Release Observations
Authors: Klaus M. Pontoppidan, Jaclyn Barrientes, Claire Blome, Hannah Braun, Matthew Brown, Margaret Carruthers, Dan Coe, Joseph DePasquale, Néstor Espinoza, Macarena Garcia Marin, Karl D. Gordon, Alaina Henry, Leah Hustak, Andi James, Ann Jenkins, Anton M. Koekemoer, Stephanie LaMassa, David Law, Alexandra Lockwood, Amaya Moro-Martin, Susan E. Mullally, Alyssa Pagan, Dani Player, Charles Proffitt, Christine Pulliam, Leah Ramsay, Swara Ravindranath, Neill Reid, Massimo Robberto, Elena Sabbi, Leonardo Ubeda, Michael Balogh, Kathryn Flanagan, Jonathan Gardner, Hashima Hasan, Bonnie Meinke, Antonella Nota
Figure caption: Field of view in NGC 3324 covered by NIRCam and MIRI. The framing was selected using archival images from Spitzer, as shown.
Paper: The JWST Early Release Observations
Authors: Klaus M. Pontoppidan, Jaclyn Barrientes, Claire Blome, Hannah Braun, Matthew Brown, Margaret Carruthers, Dan Coe, Joseph DePasquale, Néstor Espinoza, Macarena Garcia Marin, Karl D. Gordon, Alaina Henry, Leah Hustak, Andi James, Ann Jenkins, Anton M. Koekemoer, Stephanie LaMassa, David Law, Alexandra Lockwood, Amaya Moro-Martin, Susan E. Mullally, Alyssa Pagan, Dani Player, Charles Proffitt, Christine Pulliam, Leah Ramsay, Swara Ravindranath, Neill Reid, Massimo Robberto, Elena Sabbi, Leonardo Ubeda, Michael Balogh, Kathryn Flanagan, Jonathan Gardner, Hashima Hasan, Bonnie Meinke, Antonella Nota
Figure caption: Field of view in Stephan’s Quintet covered by NIRCam and MIRI.
Paper: Testing Galaxy Feedback Models with Resolved X-Ray Profiles of the Hot Circumgalactic Medium
Authors: Urmila Chadayammuri, Ákos Bogdán, Benjamin D. Oppenheimer, Ralph P. Kraft, William R. Forman, Christine Jones
Figure caption: Distribution of the properties of the galaxies used in this study. We set a floor of 10−13 yr−1 to the sSFR, since SFRs lower than 10−3 M ⊙ yr−1 would produce very weak signals. For each mass bin, the top third of galaxies by sSFR make up the star-forming galaxy stack, while the bottom third are marked quiescent. This split is shown for the entire sample in the left panel. The dotted line in the second panel shows the division between the low-mass and high-mass samples. The blue and red histograms in the middle and right panels show the star-forming and quiescent galaxies, respectively.
Paper: Testing Galaxy Feedback Models with Resolved X-Ray Profiles of the Hot Circumgalactic Medium
Authors: Urmila Chadayammuri, Ákos Bogdán, Benjamin D. Oppenheimer, Ralph P. Kraft, William R. Forman, Christine Jones
Figure caption: X-ray luminosity in the 0.5–2.0 keV band, from 10 to 100 kpc around each galaxy, for the simulated galaxies. EAGLE stacks are shown in orange, and TNG stacks are shown in green. The solid line shows the mean at the given stellar mass, the dotted line shows the median, and the shaded regions show the 16th−84th percentiles. The mean is 3–6 times higher than the median at the low-mass end and two times higher at the high-mass end and lies close to the 84th percentile.
Paper: The Prolific Thermonuclear X-Ray Bursts from the Outburst of the Newly Discovered Millisecond Pulsar MAXI J1816–195 Observed by Insight-HXMT and NICER
Authors: Yu-Peng Chen, Shu Zhang, Long Ji, Shuang-Nan Zhang, Peng-Ju Wang, Ling-Da Kong, Zhi Chang, Jing-Qiang Peng, Qing-Cang Shui, Jian Li, Lian Tao, Ming-Yu Ge, Jin-Lu Qu
Figure caption: Left panel: simultaneous broadband energy spectrum of MAXI J1816–195 as observed from NICER (black), Insight-HXMT/LE (red), Insight-HXMT/ME (green), and Insight-HXMT/HE (blue); the best-fitting model consists of an absorbed convolution thermal Comptonization model (with an input seed photon spectrum diskbb) and an absorbed Gaussian emission line fixed at 6.4 keV. Right panel: the spectral fitting results by NICER (black), Insight-HXMT/LE (red), and Insight-HXMT/ME (green) when the burst reached its peak flux with the f  a  model (top). The blackbody model and the enhancement of the persistent emission are labeled. The two panels below: residuals of spectral fitting results by the f  a  model (middle) and an absorbed blackbody (bottom).
Paper: The Prolific Thermonuclear X-Ray Bursts from the Outburst of the Newly Discovered Millisecond Pulsar MAXI J1816–195 Observed by Insight-HXMT and NICER
Authors: Yu-Peng Chen, Shu Zhang, Long Ji, Shuang-Nan Zhang, Peng-Ju Wang, Ling-Da Kong, Zhi Chang, Jing-Qiang Peng, Qing-Cang Shui, Jian Li, Lian Tao, Ming-Yu Ge, Jin-Lu Qu
Figure caption: The stacked light curves of LE (top), ME (middle), and HE (bottom) of the burst in 1–10 keV, 8–30 keV, and 30–100 keV, respectively. The time bin for LE and ME is 0.25 s; for the HE it is 2 s. The red line in the bottom panel indicates the preburst emission (persistent emission and background) in the HE detectors. There is 1 s data gap around T = 35 in the LE light curve of burst nine, which causes a dip around T = 35. For other bursts, for LE, ME, and HE, there is no such gap observed.
Paper: The Prolific Thermonuclear X-Ray Bursts from the Outburst of the Newly Discovered Millisecond Pulsar MAXI J1816–195 Observed by Insight-HXMT and NICER
Authors: Yu-Peng Chen, Shu Zhang, Long Ji, Shuang-Nan Zhang, Peng-Ju Wang, Ling-Da Kong, Zhi Chang, Jing-Qiang Peng, Qing-Cang Shui, Jian Li, Lian Tao, Ming-Yu Ge, Jin-Lu Qu
Figure caption: Spectral fitting result of burst nine with time bin 1 s with an absorbed blackbody (black), including the time evolution of the blackbody bolometric flux F bb, the temperature kT bb, the observed radius R of NS surface at 6.3 kpc, the goodness of fit ﹩{\chi }_{v}^{2}﹩. The bolometric flux of the blackbody model F bb is in units of 10−8 erg cm−2 s−1.
Paper: The Prolific Thermonuclear X-Ray Bursts from the Outburst of the Newly Discovered Millisecond Pulsar MAXI J1816–195 Observed by Insight-HXMT and NICER
Authors: Yu-Peng Chen, Shu Zhang, Long Ji, Shuang-Nan Zhang, Peng-Ju Wang, Ling-Da Kong, Zhi Chang, Jing-Qiang Peng, Qing-Cang Shui, Jian Li, Lian Tao, Ming-Yu Ge, Jin-Lu Qu
Figure caption: Top panel: the spectrum of the persistent emission by HE. Middle panel: the detected spectrum of the bursts. Bottom panel: deficit fraction VS energy during the bursts detected by HE.
Paper: The Prolific Thermonuclear X-Ray Bursts from the Outburst of the Newly Discovered Millisecond Pulsar MAXI J1816–195 Observed by Insight-HXMT and NICER
Authors: Yu-Peng Chen, Shu Zhang, Long Ji, Shuang-Nan Zhang, Peng-Ju Wang, Ling-Da Kong, Zhi Chang, Jing-Qiang Peng, Qing-Cang Shui, Jian Li, Lian Tao, Ming-Yu Ge, Jin-Lu Qu
Figure caption: Top panel: daily light curves of MAXI J1816–195 by MAXI (black) and Swift/BAT (red) during the outbursts in 2022, in 2–20 keV and 15–50 keV, respectively. The 73 bursts are indicated by vertical lines. Bottom panel: light curves of MAXI J1816–195 by LE (green), ME (blue), and HE (teal), which are rebinned by one ObsID (∼10,000 s).
Paper: Observation of a Magnetic Switchback in the Solar Corona
Authors: Daniele Telloni, Gary P. Zank, Marco Stangalini, Cooper Downs, Haoming Liang, Masaru Nakanotani, Vincenzo Andretta, Ester Antonucci, Luca Sorriso-Valvo, Laxman Adhikari, Lingling Zhao, Raffaele Marino, Roberto Susino, Catia Grimani, Michele Fabi, Raffaella D'Amicis, Denise Perrone, Roberto Bruno, Francesco Carbone, Salvatore Mancuso, Marco Romoli, Vania Da Deppo, Silvano Fineschi, Petr Heinzel, John D. Moses, Giampiero Naletto, Gianalfredo Nicolini, Daniele Spadaro, Luca Teriaca, Federica Frassati, Giovanna Jerse, Federico Landini, Maurizio Pancrazzi, Giuliana Russano, Clementina Sasso, Ruggero Biondo, Aleksandr Burtovoi, Giuseppe E. Capuano, Chiara Casini, Marta Casti, Paolo Chioetto, Yara De Leo, Marina Giarrusso, Alessandro Liberatore, David Berghmans, Frédéric Auchère, Regina Aznar Cuadrado, Lakshmi P. Chitta, Louise Harra, Emil Kraaikamp, David M. Long, Sudip Mandal, Susanna Parenti, Gabriel Pelouze, Hardi Peter, Luciano Rodriguez, Udo Schühle, Conrad Schwanitz, Phil J. Smith, Cis Verbeeck, Andrei N. Zhukov
Figure caption: MCMC-modeled switchback (white shape) before and after linear-theory-based propagation, compared with Metis observations at 800 and 2400 s after initiation.
Paper: Properties of Host Galaxies of Submillimeter Sources as Revealed by JWST Early Release Observations in SMACS J0723.3–7327
Authors: Cheng Cheng, Haojing Yan, Jia-Sheng Huang, Christopher N. A. Willmer, Zhiyuan Ma, Gustavo Orellana-González
Figure caption: SED fitting results given by MAGPHYS with the observed data (red), best-fitted model (black), and the stellar model (blue) before dust extinction, and the residual in each bottom panel.
Paper: Properties of Host Galaxies of Submillimeter Sources as Revealed by JWST Early Release Observations in SMACS J0723.3–7327
Authors: Cheng Cheng, Haojing Yan, Jia-Sheng Huang, Christopher N. A. Willmer, Zhiyuan Ma, Gustavo Orellana-González
Figure caption: The NIRCam F444W image (left panel), best fitted by a Sérsic model (central panel) and the fit residual (right panel) of ID2 and ID3.
Paper: Star Formation Suppression by Tidal Removal of Cold Molecular Gas from an Intermediate-redshift Massive Post-starburst Galaxy
Authors: Justin S. Spilker, Katherine A. Suess, David J. Setton, Rachel Bezanson, Robert Feldmann, Jenny E. Greene, Mariska Kriek, Sidney Lower, Desika Narayanan, Margaret Verrico
Figure caption: Near-IR and CO emission of SDSS J1448+1010. CO is detected within the prominent stellar tidal tails seen in the HST image, reaching projected distances up to 64 kpc from the central galaxy. The northern (southern) tidal features are blue- (red)shifted from the systemic velocity by ≈150  km s−1. The gas in the central galaxy is highly turbulent, while the dispersion is <50  km s−1 at all locations within the tidal features. Contours of the integrated CO emission begin at 3σ and increase in powers of 2 and are repeated in all panels. The ALMA synthesized beam is indicated at the lower left. The dotted circle in the second panel indicates the emission we consider to belong to the central galaxy; all else constitutes the tails.
Paper: Star Formation Suppression by Tidal Removal of Cold Molecular Gas from an Intermediate-redshift Massive Post-starburst Galaxy
Authors: Justin S. Spilker, Katherine A. Suess, David J. Setton, Rachel Bezanson, Robert Feldmann, Jenny E. Greene, Mariska Kriek, Sidney Lower, Desika Narayanan, Margaret Verrico
Figure caption: Left: HST WFC3/F110W image of SDSS J1448+1010, as in Figure 1, shown on log-stretch. Center: after subtraction of the best-fit single Sérsic profile, a second peak ≈0.″6 northwest of the main galaxy is more easily visible. Right: Gemini FLAMINGOS-2 H-band image with CO(2–1) contours. The white circle shows the photometric aperture used for all imaging data, matched to the SDSS catalog photometry. Note the object just off frame to the northwest is an unrelated foreground galaxy.
Paper: Star Formation Suppression by Tidal Removal of Cold Molecular Gas from an Intermediate-redshift Massive Post-starburst Galaxy
Authors: Justin S. Spilker, Katherine A. Suess, David J. Setton, Rachel Bezanson, Robert Feldmann, Jenny E. Greene, Mariska Kriek, Sidney Lower, Desika Narayanan, Margaret Verrico
Figure caption: The available multiwavelength imaging and SDSS spectroscopic data (upper panels) allow detailed constraints on the star formation history of SDSS J1448+1010. The optical spectrum shows prominent Balmer absorption features, the hallmark of post-starburst galaxies. The reconstructed SFH (lower panels) indicates that the starburst event began ﹩{1.0}_{-0.4}^{+0.3}﹩ Gyr and ended ﹩{70}_{-30}^{+40}﹩ Myr ago, and formed ∼40% of the total stellar mass. The photometric data (black points) and best-fit model photometry (red points) are shown in the upper-left panel. The SDSS spectrum (unbinned: gray; binned: black) and best-fit model spectrum (red) are shown in the upper right. Vertical gray bands highlight wavelengths around [O II] 3727 Å and [O III] 4959,5007 Å, which are masked in our fitting. Red shaded regions in the lower panels indicate the 16th–84th percentile confidence interval on the reconstructed SFH, and the vertical blue shaded regions indicate the time period of the recent starburst.
Paper: Star Formation Suppression by Tidal Removal of Cold Molecular Gas from an Intermediate-redshift Massive Post-starburst Galaxy
Authors: Justin S. Spilker, Katherine A. Suess, David J. Setton, Rachel Bezanson, Robert Feldmann, Jenny E. Greene, Mariska Kriek, Sidney Lower, Desika Narayanan, Margaret Verrico
Figure caption: The molecular gas in the SDSS J1448+1010 tidal tails is extreme in both scale and magnitude in comparison to all known mergers at any redshift. The low-redshift merger comparison sample is coded by whether or not the molecular gas is thought to have been stripped from the host (solid) or recycled/formed in situ (empty). All objects use the same assumptions for CO excitation and α CO; this figure would appear identical using pure observable quantities.
Paper: Star Formation Suppression by Tidal Removal of Cold Molecular Gas from an Intermediate-redshift Massive Post-starburst Galaxy
Authors: Justin S. Spilker, Katherine A. Suess, David J. Setton, Rachel Bezanson, Robert Feldmann, Jenny E. Greene, Mariska Kriek, Sidney Lower, Desika Narayanan, Margaret Verrico
Figure caption: ALMA CO(2–1) spectra of SDSS J1448+1010 extracted from, in order, the central galaxy and the northern and southern tidal tails. Combined, the tidal tails contain 47% ± 5% of the total CO luminosity in the system.
Paper: The Unmixed Debris of Gaia-Sausage/Enceladus in the Form of a Pair of Halo Stellar Overdensities
Authors: Hélio D. Perottoni, Guilherme Limberg, João A. S. Amarante, Silvia Rossi, Anna B. A. Queiroz, Rafael M. Santucci, Angeles Pérez-Villegas, Cristina Chiappini
Figure caption: Orbital eccentricity distribution of SEGUE stars from HAC-S, HAC-N, VOD, and GSE in orange, pink, blue, and yellow, respectively. The histogram shows the fractions of stars in each bin, and the number of stars (N) in each panel is also provided. The first panel shows the eccentricity distribution of the full sample and each of the other panels corresponds to a slice in metallicity, with [Fe/H] increasing from left to right.
Paper: The Unmixed Debris of Gaia-Sausage/Enceladus in the Form of a Pair of Halo Stellar Overdensities
Authors: Hélio D. Perottoni, Guilherme Limberg, João A. S. Amarante, Silvia Rossi, Anna B. A. Queiroz, Rafael M. Santucci, Angeles Pérez-Villegas, Cristina Chiappini
Figure caption: Chemical abundances of HAC-S, HAC-N, and VOD stars in the [Mg/Fe]–[Fe/H] (top left), [Mg/Mn]–[Al/Fe] (top right), [Al/Fe]–[Fe/H] (bottom left), and [Ni/Fe]–[(C+N)/O] (bottom right). The empty symbols show stars from the stellar overdensities that either do not have the typical elemental abundances of ancient accreted populations (region in the top right panel delineated by red lines Hawkins et al. 2015; Das et al. 2020) or have low-eccentricity orbits (e < 0.7). The yellow contours indicate the chemical patterns of the GSE stars. The background 2D histogram shows the distribution of the APOGEE stars.
Paper: The Unmixed Debris of Gaia-Sausage/Enceladus in the Form of a Pair of Halo Stellar Overdensities
Authors: Hélio D. Perottoni, Guilherme Limberg, João A. S. Amarante, Silvia Rossi, Anna B. A. Queiroz, Rafael M. Santucci, Angeles Pérez-Villegas, Cristina Chiappini
Figure caption: MDFs of the SEGUE stars from HAC-S, HAC-N, VOD, and GSE. MDFs of the full sample (left); stars with eccentricity higher than 0.7 (middle) and lower than 0.7 (right) are presented with the same color scheme of Figure 2.
Paper: The Unmixed Debris of Gaia-Sausage/Enceladus in the Form of a Pair of Halo Stellar Overdensities
Authors: Hélio D. Perottoni, Guilherme Limberg, João A. S. Amarante, Silvia Rossi, Anna B. A. Queiroz, Rafael M. Santucci, Angeles Pérez-Villegas, Cristina Chiappini
Figure caption: Orbital parameters of HAC-S, HAC-N, and VOD stars in the E–L  z  (left) and e–L  z  (right) planes. The symbols are defined in Figure 4.
Paper: Properties of Host Galaxies of Submillimeter Sources as Revealed by JWST Early Release Observations in SMACS J0723.3–7327
Authors: Cheng Cheng, Haojing Yan, Jia-Sheng Huang, Christopher N. A. Willmer, Zhiyuan Ma, Gustavo Orellana-González
Figure caption: Upper panels: color composite images of the SMGs in this work combining the F150W (blue), F277W (green), and F444W (red) bands. The ALMA continuum is represented by contours in 2σ (cyan) and 3σ, 5σ (red) of the ALMA continuum map noise. The ALMA beams are shown as filled red ellipses of each panel. Bottom panels: best-fit SEDs of our sample. We show the photometry from the Hubble Space Telescope (HST; blue), JWST/NIRCam (green), and JWST/MIRI (red). Since the spec-z of the target ID2 is 2.464, we fit the SED with local galaxy templates (Brown et al. 2014), and find the best-fitted template is the one of NGC 5195. ID1 and ID3 have not been spectroscopically confirmed. Therefore, we estimate the photoz with EAZY, showing the templates with highest probability, and the p(z) vs. redshift in the subplot panel. The MIRI photometry matches well with the PAHs feature that is predicted by the best-fitted template. ID1 is the faintest target in our sample and the p(z) shows two peaks at z ∼ 0.9 and 2.9; we further discuss the ID1 photoz in Section 4.2.
Paper: Properties of Host Galaxies of Submillimeter Sources as Revealed by JWST Early Release Observations in SMACS J0723.3–7327
Authors: Cheng Cheng, Haojing Yan, Jia-Sheng Huang, Christopher N. A. Willmer, Zhiyuan Ma, Gustavo Orellana-González
Figure caption: The half-light radius from the NIRCam F444W image (red points) compared to the dust size from ALMA. We also show the F150W half-light radii (red circles), which are ∼1.5 times larger than the F444W radii, and the submillimeter galaxy (SMG) size measured from the JWST/NIRCam images (red diamond and star points; Chen et al. 2022; Wu et al. 2022), or the size measured from HST F140W or F160W images (black points, which is roughly considered as the stellar mass distribution radius; Rujopakarn et al. 2016; Tadaki et al. 2017, 2020; Cheng et al. 2020). The size difference between the F150W and F444W bands may be caused by the dust extinction, and implies that SMGs stellar distribution may be smaller than the size revealed by HST images. The blue circle is the F444W vs. F1500W size for ID3, which measures the extents of regions dominated by the stellar component and the PAH emission at z ∼ 1.