adsabs/AstroCLIMB huggingface dataset:
Paper: CEERS Key Paper. III. The Diversity of Galaxy Structure and Morphology at z = 3–9 with JWST
Authors: Jeyhan S. Kartaltepe, Caitlin Rose, Brittany N. Vanderhoof, Elizabeth J. McGrath, Luca Costantin, Isabella G. Cox, L. Y. Aaron Yung, Dale D. Kocevski, Stijn Wuyts, Henry C. Ferguson, Micaela B. Bagley, Steven L. Finkelstein, Ricardo O. Amorín, Brett H. Andrews, Pablo Arrabal Haro, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Antonello Calabrò, Caitlin M. Casey, Rosemary T. Coogan, M. C. Cooper, Darren Croton, Alexander de la Vega, Mark Dickinson, Adriano Fontana, Maximilien Franco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Benne W. Holwerda, Marc Huertas-Company, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Lisa J. Kewley, Allison Kirkpatrick, Anton M. Koekemoer, James Liu, Jennifer M. Lotz, Ray A. Lucas, Jeffrey A. Newman, Camilla Pacifici, Viraj Pandya, Casey Papovich, Laura Pentericci, Pablo G. Pérez-González, Jayse Petersen, Nor Pirzkal, Marc Rafelski, Swara Ravindranath, Raymond C. Simons, Gregory F. Snyder, Rachel S. Somerville, Elizabeth R. Stanway, Amber N. Straughn, Sandro Tacchella, Jonathan R. Trump, Jesús Vega-Ferrero, Stephen M. Wilkins, Guang Yang, Jorge A. Zavala
Figure caption: NIRCam F150W+F277W+F356W postage stamp cutouts of a selection of example galaxies in each of the seven morphological groups described in Section 4.1 at three different redshift bins. Each cutout is 2″ on a side.
Paper: CEERS Key Paper. III. The Diversity of Galaxy Structure and Morphology at z = 3–9 with JWST
Authors: Jeyhan S. Kartaltepe, Caitlin Rose, Brittany N. Vanderhoof, Elizabeth J. McGrath, Luca Costantin, Isabella G. Cox, L. Y. Aaron Yung, Dale D. Kocevski, Stijn Wuyts, Henry C. Ferguson, Micaela B. Bagley, Steven L. Finkelstein, Ricardo O. Amorín, Brett H. Andrews, Pablo Arrabal Haro, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Antonello Calabrò, Caitlin M. Casey, Rosemary T. Coogan, M. C. Cooper, Darren Croton, Alexander de la Vega, Mark Dickinson, Adriano Fontana, Maximilien Franco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Benne W. Holwerda, Marc Huertas-Company, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Lisa J. Kewley, Allison Kirkpatrick, Anton M. Koekemoer, James Liu, Jennifer M. Lotz, Ray A. Lucas, Jeffrey A. Newman, Camilla Pacifici, Viraj Pandya, Casey Papovich, Laura Pentericci, Pablo G. Pérez-González, Jayse Petersen, Nor Pirzkal, Marc Rafelski, Swara Ravindranath, Raymond C. Simons, Gregory F. Snyder, Rachel S. Somerville, Elizabeth R. Stanway, Amber N. Straughn, Sandro Tacchella, Jonathan R. Trump, Jesús Vega-Ferrero, Stephen M. Wilkins, Guang Yang, Jorge A. Zavala
Figure caption: Fraction of z > 3 galaxies detected by both JWST and HST with M ⋆ > 109 M ⊙ as a function of redshift for each morphology class. The top row from left to right shows galaxies with disks, galaxies with spheroids, galaxies with irregular features, and point sources and unclassifiable galaxies. The bottom row shows all of the same morphological groups but divided in different ways for easy comparison. From left to right, the combination of all disks, spheroids, and irregulars; the combination of disk-, spheroid-, and irregular-only groups; and the remaining mixed groups. Error bars represent the 1σ binomial confidence limits given the number of objects in each category, following the method of Cameron (2011).
Paper: CEERS Key Paper. III. The Diversity of Galaxy Structure and Morphology at z = 3–9 with JWST
Authors: Jeyhan S. Kartaltepe, Caitlin Rose, Brittany N. Vanderhoof, Elizabeth J. McGrath, Luca Costantin, Isabella G. Cox, L. Y. Aaron Yung, Dale D. Kocevski, Stijn Wuyts, Henry C. Ferguson, Micaela B. Bagley, Steven L. Finkelstein, Ricardo O. Amorín, Brett H. Andrews, Pablo Arrabal Haro, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Antonello Calabrò, Caitlin M. Casey, Rosemary T. Coogan, M. C. Cooper, Darren Croton, Alexander de la Vega, Mark Dickinson, Adriano Fontana, Maximilien Franco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Benne W. Holwerda, Marc Huertas-Company, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Lisa J. Kewley, Allison Kirkpatrick, Anton M. Koekemoer, James Liu, Jennifer M. Lotz, Ray A. Lucas, Jeffrey A. Newman, Camilla Pacifici, Viraj Pandya, Casey Papovich, Laura Pentericci, Pablo G. Pérez-González, Jayse Petersen, Nor Pirzkal, Marc Rafelski, Swara Ravindranath, Raymond C. Simons, Gregory F. Snyder, Rachel S. Somerville, Elizabeth R. Stanway, Amber N. Straughn, Sandro Tacchella, Jonathan R. Trump, Jesús Vega-Ferrero, Stephen M. Wilkins, Guang Yang, Jorge A. Zavala
Figure caption: Stellar mass vs. redshift for the z > 3 sample used in this paper. Above and to the right are the distributions of redshift and stellar mass, respectively. The horizontal dashed line at ﹩\mathrm{log}({M}_{\star }/{M}_{\odot }﹩) = 9 corresponds to the mass cut used for the subsample of objects in Section 4.1.
Paper: CEERS Key Paper. III. The Diversity of Galaxy Structure and Morphology at z = 3–9 with JWST
Authors: Jeyhan S. Kartaltepe, Caitlin Rose, Brittany N. Vanderhoof, Elizabeth J. McGrath, Luca Costantin, Isabella G. Cox, L. Y. Aaron Yung, Dale D. Kocevski, Stijn Wuyts, Henry C. Ferguson, Micaela B. Bagley, Steven L. Finkelstein, Ricardo O. Amorín, Brett H. Andrews, Pablo Arrabal Haro, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Antonello Calabrò, Caitlin M. Casey, Rosemary T. Coogan, M. C. Cooper, Darren Croton, Alexander de la Vega, Mark Dickinson, Adriano Fontana, Maximilien Franco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Benne W. Holwerda, Marc Huertas-Company, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Lisa J. Kewley, Allison Kirkpatrick, Anton M. Koekemoer, James Liu, Jennifer M. Lotz, Ray A. Lucas, Jeffrey A. Newman, Camilla Pacifici, Viraj Pandya, Casey Papovich, Laura Pentericci, Pablo G. Pérez-González, Jayse Petersen, Nor Pirzkal, Marc Rafelski, Swara Ravindranath, Raymond C. Simons, Gregory F. Snyder, Rachel S. Somerville, Elizabeth R. Stanway, Amber N. Straughn, Sandro Tacchella, Jonathan R. Trump, Jesús Vega-Ferrero, Stephen M. Wilkins, Guang Yang, Jorge A. Zavala
Figure caption: Top: rest-frame optical asymmetry value as a function of concentration for all galaxies at z > 3 split by all disk galaxies (left), spheroids (middle), and irregulars (right). The dashed–dotted lines show the boundaries between disk, elliptical, and intermediate galaxies from Bershady et al. (2000), and the dashed line is the dividing line above which nearby galaxies are expected to be major mergers (A = 0.35; Conselice 2003). Bottom: rest-frame optical Gini value as a function of M 20 for all galaxies at z > 3 split by all disk galaxies (left), spheroids (middle), and irregulars (right). The lines show the boundaries between disk and elliptical galaxies (dashed–dotted) and mergers (dashed) from Lotz et al. (2008a). The colors indicate the different combinations of the main morphological class chosen by two out of three people during the visual classifications, as described in Section 4.1 and Figure 2.
Paper: CEERS Key Paper. III. The Diversity of Galaxy Structure and Morphology at z = 3–9 with JWST
Authors: Jeyhan S. Kartaltepe, Caitlin Rose, Brittany N. Vanderhoof, Elizabeth J. McGrath, Luca Costantin, Isabella G. Cox, L. Y. Aaron Yung, Dale D. Kocevski, Stijn Wuyts, Henry C. Ferguson, Micaela B. Bagley, Steven L. Finkelstein, Ricardo O. Amorín, Brett H. Andrews, Pablo Arrabal Haro, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Antonello Calabrò, Caitlin M. Casey, Rosemary T. Coogan, M. C. Cooper, Darren Croton, Alexander de la Vega, Mark Dickinson, Adriano Fontana, Maximilien Franco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Benne W. Holwerda, Marc Huertas-Company, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Lisa J. Kewley, Allison Kirkpatrick, Anton M. Koekemoer, James Liu, Jennifer M. Lotz, Ray A. Lucas, Jeffrey A. Newman, Camilla Pacifici, Viraj Pandya, Casey Papovich, Laura Pentericci, Pablo G. Pérez-González, Jayse Petersen, Nor Pirzkal, Marc Rafelski, Swara Ravindranath, Raymond C. Simons, Gregory F. Snyder, Rachel S. Somerville, Elizabeth R. Stanway, Amber N. Straughn, Sandro Tacchella, Jonathan R. Trump, Jesús Vega-Ferrero, Stephen M. Wilkins, Guang Yang, Jorge A. Zavala
Figure caption: Rest-frame optical Sérsic index (n) plotted as a function of the effective radius (R  e ) in kiloparsecs (top left) and the axis ratio (b/a) (top right) for the z > 3 galaxy sample. The axis ratio plotted as a function of the effective radius is shown in the bottom left. The colors of each point indicate the different combinations of the main morphological class chosen by two out of three people during the visual classifications, as described in Section 4.1 and Figure 2. The median values for each group are shown as stars, with the error bars representing the 16th–84th percentile range of the distribution.
Paper: CEERS Key Paper. III. The Diversity of Galaxy Structure and Morphology at z = 3–9 with JWST
Authors: Jeyhan S. Kartaltepe, Caitlin Rose, Brittany N. Vanderhoof, Elizabeth J. McGrath, Luca Costantin, Isabella G. Cox, L. Y. Aaron Yung, Dale D. Kocevski, Stijn Wuyts, Henry C. Ferguson, Micaela B. Bagley, Steven L. Finkelstein, Ricardo O. Amorín, Brett H. Andrews, Pablo Arrabal Haro, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Antonello Calabrò, Caitlin M. Casey, Rosemary T. Coogan, M. C. Cooper, Darren Croton, Alexander de la Vega, Mark Dickinson, Adriano Fontana, Maximilien Franco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Benne W. Holwerda, Marc Huertas-Company, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Lisa J. Kewley, Allison Kirkpatrick, Anton M. Koekemoer, James Liu, Jennifer M. Lotz, Ray A. Lucas, Jeffrey A. Newman, Camilla Pacifici, Viraj Pandya, Casey Papovich, Laura Pentericci, Pablo G. Pérez-González, Jayse Petersen, Nor Pirzkal, Marc Rafelski, Swara Ravindranath, Raymond C. Simons, Gregory F. Snyder, Rachel S. Somerville, Elizabeth R. Stanway, Amber N. Straughn, Sandro Tacchella, Jonathan R. Trump, Jesús Vega-Ferrero, Stephen M. Wilkins, Guang Yang, Jorge A. Zavala
Figure caption: Fraction of z > 3 galaxies detected by HST with M ⋆ > 109 M ⊙ as a function of redshift for each morphology class based on the CANDELS HST visual classifications of Kartaltepe et al. (2015). The top row from left to right shows galaxies with disks, galaxies with spheroids, galaxies with irregular features, and point sources and unclassifiable galaxies. The bottom row shows all of the same morphological groups but divided in different ways for easy comparison. From left to right is the combination of all disks, spheroids, and irregulars; the combination of disk-, spheroid-, and irregular-only groups; and the remaining mixed groups. Error bars represent the 1σ binomial confidence limits given the number of objects in each category, following the method of Cameron (2011).
Paper: CEERS Key Paper. III. The Diversity of Galaxy Structure and Morphology at z = 3–9 with JWST
Authors: Jeyhan S. Kartaltepe, Caitlin Rose, Brittany N. Vanderhoof, Elizabeth J. McGrath, Luca Costantin, Isabella G. Cox, L. Y. Aaron Yung, Dale D. Kocevski, Stijn Wuyts, Henry C. Ferguson, Micaela B. Bagley, Steven L. Finkelstein, Ricardo O. Amorín, Brett H. Andrews, Pablo Arrabal Haro, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Antonello Calabrò, Caitlin M. Casey, Rosemary T. Coogan, M. C. Cooper, Darren Croton, Alexander de la Vega, Mark Dickinson, Adriano Fontana, Maximilien Franco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Benne W. Holwerda, Marc Huertas-Company, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Lisa J. Kewley, Allison Kirkpatrick, Anton M. Koekemoer, James Liu, Jennifer M. Lotz, Ray A. Lucas, Jeffrey A. Newman, Camilla Pacifici, Viraj Pandya, Casey Papovich, Laura Pentericci, Pablo G. Pérez-González, Jayse Petersen, Nor Pirzkal, Marc Rafelski, Swara Ravindranath, Raymond C. Simons, Gregory F. Snyder, Rachel S. Somerville, Elizabeth R. Stanway, Amber N. Straughn, Sandro Tacchella, Jonathan R. Trump, Jesús Vega-Ferrero, Stephen M. Wilkins, Guang Yang, Jorge A. Zavala
Figure caption: Fraction of z > 3 galaxies detected by HST with M ⋆ > 109 M ⊙ as a function of redshift for each morphology class based on the CEERS JWST visual classifications (as in Figure 3) compared to the CANDELS HST visual classifications of Kartaltepe et al. (2015; as in Figure 9) for the 59 objects from EGS that were bright enough to be classified. From left to right is the combination of all disks, spheroids, and irregulars; the combination of disk-, spheroid-, and irregular-only groups; and objects that were unclassifiable or point sources. Error bars represent the 1σ binomial confidence limits given the number of objects in each category, following the method of Cameron (2011).
Paper: CEERS Key Paper. III. The Diversity of Galaxy Structure and Morphology at z = 3–9 with JWST
Authors: Jeyhan S. Kartaltepe, Caitlin Rose, Brittany N. Vanderhoof, Elizabeth J. McGrath, Luca Costantin, Isabella G. Cox, L. Y. Aaron Yung, Dale D. Kocevski, Stijn Wuyts, Henry C. Ferguson, Micaela B. Bagley, Steven L. Finkelstein, Ricardo O. Amorín, Brett H. Andrews, Pablo Arrabal Haro, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Antonello Calabrò, Caitlin M. Casey, Rosemary T. Coogan, M. C. Cooper, Darren Croton, Alexander de la Vega, Mark Dickinson, Adriano Fontana, Maximilien Franco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Benne W. Holwerda, Marc Huertas-Company, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Lisa J. Kewley, Allison Kirkpatrick, Anton M. Koekemoer, James Liu, Jennifer M. Lotz, Ray A. Lucas, Jeffrey A. Newman, Camilla Pacifici, Viraj Pandya, Casey Papovich, Laura Pentericci, Pablo G. Pérez-González, Jayse Petersen, Nor Pirzkal, Marc Rafelski, Swara Ravindranath, Raymond C. Simons, Gregory F. Snyder, Rachel S. Somerville, Elizabeth R. Stanway, Amber N. Straughn, Sandro Tacchella, Jonathan R. Trump, Jesús Vega-Ferrero, Stephen M. Wilkins, Guang Yang, Jorge A. Zavala
Figure caption: Rest-frame optical axis ratio (b/a) plotted as a function of the effective radius (R  e ) in kiloparsecs in six different redshift bins. The colors indicate the different combinations of the main morphological class chosen by two out of three people during the visual classifications, as described in Section 4.1 and Figure 2. The individual sources are shown as transparent points, and the median for each group is shown as a star with the 16th–84th percentile range of the distribution shown as error bars.
Paper: CEERS Key Paper. III. The Diversity of Galaxy Structure and Morphology at z = 3–9 with JWST
Authors: Jeyhan S. Kartaltepe, Caitlin Rose, Brittany N. Vanderhoof, Elizabeth J. McGrath, Luca Costantin, Isabella G. Cox, L. Y. Aaron Yung, Dale D. Kocevski, Stijn Wuyts, Henry C. Ferguson, Micaela B. Bagley, Steven L. Finkelstein, Ricardo O. Amorín, Brett H. Andrews, Pablo Arrabal Haro, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Antonello Calabrò, Caitlin M. Casey, Rosemary T. Coogan, M. C. Cooper, Darren Croton, Alexander de la Vega, Mark Dickinson, Adriano Fontana, Maximilien Franco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Benne W. Holwerda, Marc Huertas-Company, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Lisa J. Kewley, Allison Kirkpatrick, Anton M. Koekemoer, James Liu, Jennifer M. Lotz, Ray A. Lucas, Jeffrey A. Newman, Camilla Pacifici, Viraj Pandya, Casey Papovich, Laura Pentericci, Pablo G. Pérez-González, Jayse Petersen, Nor Pirzkal, Marc Rafelski, Swara Ravindranath, Raymond C. Simons, Gregory F. Snyder, Rachel S. Somerville, Elizabeth R. Stanway, Amber N. Straughn, Sandro Tacchella, Jonathan R. Trump, Jesús Vega-Ferrero, Stephen M. Wilkins, Guang Yang, Jorge A. Zavala
Figure caption: Rest-frame optical asymmetry value as a function of concentration (left) and Gini value as a function of M 20 (right) for all galaxies at z > 3, color coded by the median Sérsic index in each bin. The dividing lines are the same as described in Figure 7.
Paper: CEERS Key Paper. III. The Diversity of Galaxy Structure and Morphology at z = 3–9 with JWST
Authors: Jeyhan S. Kartaltepe, Caitlin Rose, Brittany N. Vanderhoof, Elizabeth J. McGrath, Luca Costantin, Isabella G. Cox, L. Y. Aaron Yung, Dale D. Kocevski, Stijn Wuyts, Henry C. Ferguson, Micaela B. Bagley, Steven L. Finkelstein, Ricardo O. Amorín, Brett H. Andrews, Pablo Arrabal Haro, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Antonello Calabrò, Caitlin M. Casey, Rosemary T. Coogan, M. C. Cooper, Darren Croton, Alexander de la Vega, Mark Dickinson, Adriano Fontana, Maximilien Franco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Benne W. Holwerda, Marc Huertas-Company, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Lisa J. Kewley, Allison Kirkpatrick, Anton M. Koekemoer, James Liu, Jennifer M. Lotz, Ray A. Lucas, Jeffrey A. Newman, Camilla Pacifici, Viraj Pandya, Casey Papovich, Laura Pentericci, Pablo G. Pérez-González, Jayse Petersen, Nor Pirzkal, Marc Rafelski, Swara Ravindranath, Raymond C. Simons, Gregory F. Snyder, Rachel S. Somerville, Elizabeth R. Stanway, Amber N. Straughn, Sandro Tacchella, Jonathan R. Trump, Jesús Vega-Ferrero, Stephen M. Wilkins, Guang Yang, Jorge A. Zavala
Figure caption: Distribution of Sérsic index, size, axis ratio, and asymmetry of the z > 3 CEERS galaxy in three different redshift bins compared to the distribution from the CEERS mock catalog derived from the Santa Cruz SAM (blue dotted line; Somerville et al. 2015, 2021; Yung et al. 2019, 2022), measurements from mock images based on IllustrisTNG50 (red dashed line; Costantin et al. 2022b), and measurements from mock images based on IllustrisTNG100 (orange dashed–dotted line; Rose et al. 2022).
Paper: CEERS Key Paper. III. The Diversity of Galaxy Structure and Morphology at z = 3–9 with JWST
Authors: Jeyhan S. Kartaltepe, Caitlin Rose, Brittany N. Vanderhoof, Elizabeth J. McGrath, Luca Costantin, Isabella G. Cox, L. Y. Aaron Yung, Dale D. Kocevski, Stijn Wuyts, Henry C. Ferguson, Micaela B. Bagley, Steven L. Finkelstein, Ricardo O. Amorín, Brett H. Andrews, Pablo Arrabal Haro, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Antonello Calabrò, Caitlin M. Casey, Rosemary T. Coogan, M. C. Cooper, Darren Croton, Alexander de la Vega, Mark Dickinson, Adriano Fontana, Maximilien Franco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Benne W. Holwerda, Marc Huertas-Company, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Lisa J. Kewley, Allison Kirkpatrick, Anton M. Koekemoer, James Liu, Jennifer M. Lotz, Ray A. Lucas, Jeffrey A. Newman, Camilla Pacifici, Viraj Pandya, Casey Papovich, Laura Pentericci, Pablo G. Pérez-González, Jayse Petersen, Nor Pirzkal, Marc Rafelski, Swara Ravindranath, Raymond C. Simons, Gregory F. Snyder, Rachel S. Somerville, Elizabeth R. Stanway, Amber N. Straughn, Sandro Tacchella, Jonathan R. Trump, Jesús Vega-Ferrero, Stephen M. Wilkins, Guang Yang, Jorge A. Zavala
Figure caption: HST and JWST postage stamps for five example galaxies with different morphologies in HST F160W images compared to JWST images or differences across the JWST filters. The F150W, F277W, and F356W filters are shown along with an RGB combination of these three filters. Each stamp is 2″ on a side.
Paper: CEERS Key Paper. III. The Diversity of Galaxy Structure and Morphology at z = 3–9 with JWST
Authors: Jeyhan S. Kartaltepe, Caitlin Rose, Brittany N. Vanderhoof, Elizabeth J. McGrath, Luca Costantin, Isabella G. Cox, L. Y. Aaron Yung, Dale D. Kocevski, Stijn Wuyts, Henry C. Ferguson, Micaela B. Bagley, Steven L. Finkelstein, Ricardo O. Amorín, Brett H. Andrews, Pablo Arrabal Haro, Bren E. Backhaus, Peter Behroozi, Laura Bisigello, Antonello Calabrò, Caitlin M. Casey, Rosemary T. Coogan, M. C. Cooper, Darren Croton, Alexander de la Vega, Mark Dickinson, Adriano Fontana, Maximilien Franco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Benne W. Holwerda, Marc Huertas-Company, Kartheik G. Iyer, Shardha Jogee, Intae Jung, Lisa J. Kewley, Allison Kirkpatrick, Anton M. Koekemoer, James Liu, Jennifer M. Lotz, Ray A. Lucas, Jeffrey A. Newman, Camilla Pacifici, Viraj Pandya, Casey Papovich, Laura Pentericci, Pablo G. Pérez-González, Jayse Petersen, Nor Pirzkal, Marc Rafelski, Swara Ravindranath, Raymond C. Simons, Gregory F. Snyder, Rachel S. Somerville, Elizabeth R. Stanway, Amber N. Straughn, Sandro Tacchella, Jonathan R. Trump, Jesús Vega-Ferrero, Stephen M. Wilkins, Guang Yang, Jorge A. Zavala
Figure caption: Matrix highlighting the level of agreement between the three classifiers for all galaxies with a disk or spheroid or those with irregular features. Overall, classifiers regularly agree when a galaxy has a disk, agree less often about galaxies with a spheroid, and are more likely to disagree about irregular features.
Paper: CEERS Epoch 1 NIRCam Imaging: Reduction Methods and Simulations Enabling Early JWST Science Results
Authors: Micaela B. Bagley, Steven L. Finkelstein, Anton M. Koekemoer, Henry C. Ferguson, Pablo Arrabal Haro, Mark Dickinson, Jeyhan S. Kartaltepe, Casey Papovich, Pablo G. Pérez-González, Nor Pirzkal, Rachel S. Somerville, Christopher N. A. Willmer, Guang Yang, L. Y. Aaron Yung, Adriano Fontana, Andrea Grazian, Norman A. Grogin, Michaela Hirschmann, Lisa J. Kewley, Allison Kirkpatrick, Dale D. Kocevski, Jennifer M. Lotz, Aubrey Medrano, Alexa M. Morales, Laura Pentericci, Swara Ravindranath, Jonathan R. Trump, Stephen M. Wilkins, Antonello Calabrò, M. C. Cooper, Luca Costantin, Alexander de la Vega, Bryan Hilbert, Taylor A. Hutchison, Rebecca L. Larson, Ray A. Lucas, Elizabeth J. McGrath, Russell Ryan, Xin Wang, Stijn Wuyts
Figure caption: An example of the snowball correction. In the top row we show a portion of an F115W count-rate map that includes several snowballs. The left image shows the output of the default jwst, where there is a particularly large snowball present in the lower left corner of the image. The middle shows the mask generated by identifying and growing the snowball footprints, where the red contours identify the original footprints. The snowballs are color-coded by the group in which they were detected; brighter snowballs were detected in later groups. The right panel shows the count-rate map resulting from refitting the ramp with the updated snowball mask added to the GROUPDQ arrays. The dashed black circles show the new footprints of the snowballs and are there to guide the eye. In the bottom row we show the portion of the F115W mosaic that corresponds to this region. In the left panel, the mosaic has been created without correcting for the snowballs in the individual exposures, while the right panel shows a mosaic that included this correction. (Three input images contribute to this mosaic, and so there are some snowballs present in the bottom left panel that are not in the snowball mask in the top row because they come from one of the other two dithers.) The three CEERS dithers are not sufficient to compensate for the presence of snowballs. This additional correction is needed to remove them from the coadded mosaics. We note that the left panel also includes 1/f noise, which we discuss in Section 3.1.3.