JWST's PEARLS: resolved study of the stellar and dust components in starburst galaxies at cosmic noon

Dusty star-forming galaxies (DSFGs) contribute significantly to the stellar buildup at cosmic noon. Major mergers and gas accretion are often invoked to explain DSFGs' prodigious star-formation rates (SFRs) and large stellar masses. We conducted a spatially-resolved morphological analysis of th...

Full description

Saved in:
Bibliographic Details
Published in:arXiv.org 2024-08
Main Authors: Polletta, M, Frye, B L, Garuda, N, Willner, S P, Berta, S, Kneissl, R, Dole, H, Jansen, R A, Lehnert, M D, Cohen, S H, Summers, J, Windhorst, R A, D'Silva, J C J, Koekemoer, A M, Coe, D, Conselice, C J, Driver, S P, Grogin, N A, Marshall, M A, Nonino, M, Ortiz, R, Pirzkal, N, Robotham, A, Ryan, R E, Jr, Willmer, C N A, Yan, H, Arumugam, V, Cheng, C, Gim, H B, Hathi, N P, Holwerda, B, Kamieneski, P, Keel, W C, J Li, Pascale, M, Rottgering, H, Smith, B M, Yun, M S
Format: Article
Language:English
Subjects:
Clumps
Cosmic dust
Dust
Emitters
Galaxy distribution
James Webb Space Telescope
Morphology
Skewed distributions
Star & galaxy formation
Star formation
Starburst galaxies
Starbursts
Stellar mass
Online Access:Get full text
Tags: Add Tag
No Tags, Be the first to tag this record!
cited_by
cites
container_end_page
container_issue
container_start_page
container_title arXiv.org
container_volume
creator Polletta, M
Frye, B L
Garuda, N
Willner, S P
Berta, S
Kneissl, R
Dole, H
Jansen, R A
Lehnert, M D
Cohen, S H
Summers, J
Windhorst, R A
D'Silva, J C J
Koekemoer, A M
Coe, D
Conselice, C J
Driver, S P
Grogin, N A
Marshall, M A
Nonino, M
Ortiz, R
Pirzkal, N
Robotham, A
Ryan, R E
Jr
Willmer, C N A
Yan, H
Arumugam, V
Cheng, C
Gim, H B
Hathi, N P
Holwerda, B
Kamieneski, P
Keel, W C
J Li
Pascale, M
Rottgering, H
Smith, B M
Yun, M S
description Dusty star-forming galaxies (DSFGs) contribute significantly to the stellar buildup at cosmic noon. Major mergers and gas accretion are often invoked to explain DSFGs' prodigious star-formation rates (SFRs) and large stellar masses. We conducted a spatially-resolved morphological analysis of the rest-frame UV/NIR emission in three DSFGs at z~2.5. Initially discovered as CO emitters by NOEMA observations of a bright Herschel source, we observed them with the JWST/NIRCam as part of the PEARLS program. The NIRCam data reveal the galaxies' stellar populations and dust distributions on scales of 250 pc. Spatial variations in stellar mass, SFR, and dust extinction are determined in resolved maps obtained through pixel-based SED fitting. The CO emitters are massive, dusty starburst galaxies with SFRs=340-2500 Msun/yr, positioning them among the most active SFGs at 2
doi_str_mv 10.48550/arxiv.2405.07986
format article
fullrecord <record><control><sourceid>proquest</sourceid><recordid>TN_cdi_proquest_journals_3054665506</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>3054665506</sourcerecordid><originalsourceid>FETCH-LOGICAL-a526-d6c97ce66418d089ce3f8ce70b257c6053d4e6e623890e0f54862d52619b600d3</originalsourceid><addsrcrecordid>eNotUMtKw0AUHQTBUvsB7gZcuEq9mcfNxF0p9UVBsQWXZTpzoylpps4kpf69EV0dzuPeA4exqxymymgNtzae6uNUKNBTKEqDZ2wkpMwzo4S4YJOUdgAgsBBayxGj5_fV-ibx18Xsbbm645FSaI7keep6_81DxbtPGgg1jY3ctp77PnXchf0htNR2idftYNu47eOgf9jGnmpK3P5m0r52vA2hvWTnlW0STf5xzNb3i_X8MVu-PDzNZ8vMaoGZR1cWjhBVbjyY0pGsjKMCtkIXDkFLrwgJhTQlEFRaGRR-uMzLLQJ4OWbXf28PMXz1lLrNLvSxHRo3ErRCHPZB-QMyJ1bg</addsrcrecordid><sourcetype>Aggregation Database</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>3054665506</pqid></control><display><type>article</type><title>JWST's PEARLS: resolved study of the stellar and dust components in starburst galaxies at cosmic noon</title><source>Publicly Available Content (ProQuest)</source><creator>Polletta, M ; Frye, B L ; Garuda, N ; Willner, S P ; Berta, S ; Kneissl, R ; Dole, H ; Jansen, R A ; Lehnert, M D ; Cohen, S H ; Summers, J ; Windhorst, R A ; D'Silva, J C J ; Koekemoer, A M ; Coe, D ; Conselice, C J ; Driver, S P ; Grogin, N A ; Marshall, M A ; Nonino, M ; Ortiz, R ; Pirzkal, N ; Robotham, A ; Ryan, R E ; Jr ; Willmer, C N A ; Yan, H ; Arumugam, V ; Cheng, C ; Gim, H B ; Hathi, N P ; Holwerda, B ; Kamieneski, P ; Keel, W C ; J Li ; Pascale, M ; Rottgering, H ; Smith, B M ; Yun, M S</creator><creatorcontrib>Polletta, M ; Frye, B L ; Garuda, N ; Willner, S P ; Berta, S ; Kneissl, R ; Dole, H ; Jansen, R A ; Lehnert, M D ; Cohen, S H ; Summers, J ; Windhorst, R A ; D'Silva, J C J ; Koekemoer, A M ; Coe, D ; Conselice, C J ; Driver, S P ; Grogin, N A ; Marshall, M A ; Nonino, M ; Ortiz, R ; Pirzkal, N ; Robotham, A ; Ryan, R E ; Jr ; Willmer, C N A ; Yan, H ; Arumugam, V ; Cheng, C ; Gim, H B ; Hathi, N P ; Holwerda, B ; Kamieneski, P ; Keel, W C ; J Li ; Pascale, M ; Rottgering, H ; Smith, B M ; Yun, M S</creatorcontrib><description>Dusty star-forming galaxies (DSFGs) contribute significantly to the stellar buildup at cosmic noon. Major mergers and gas accretion are often invoked to explain DSFGs' prodigious star-formation rates (SFRs) and large stellar masses. We conducted a spatially-resolved morphological analysis of the rest-frame UV/NIR emission in three DSFGs at z~2.5. Initially discovered as CO emitters by NOEMA observations of a bright Herschel source, we observed them with the JWST/NIRCam as part of the PEARLS program. The NIRCam data reveal the galaxies' stellar populations and dust distributions on scales of 250 pc. Spatial variations in stellar mass, SFR, and dust extinction are determined in resolved maps obtained through pixel-based SED fitting. The CO emitters are massive, dusty starburst galaxies with SFRs=340-2500 Msun/yr, positioning them among the most active SFGs at 2&lt;z&lt;3. They belong to the ~1.5% of the entire JWST population with extremely red colors. Their morphologies are disk like, with radii of 2.0-4.4 kpc, and exhibit substructures such as clumps and spiral arms. The galaxies have dust extinctions up to Av=5-7 mag extending over several kpc with asymmetric distributions that include off-center regions resembling bent spiral arms and clumps. Their NIR dust-attenuation curve deviates from standard laws, possibly implying different dust-star geometries or dust grain properties than commonly assumed in starburst galaxies. The proximity of galaxies with consistent redshifts, strong color gradients, an overall disturbed appearance, asymmetric dust obscuration, and widespread star formation collectively favor interactions (minor mergers and flybys) as the mechanism driving the CO galaxies' exceptional SFRs. The galaxies' large masses and rich environment hint at membership in two proto-structures, as initially inferred from their association with a Planck-selected high-z source.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.2405.07986</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Clumps ; Cosmic dust ; Dust ; Emitters ; Galaxy distribution ; James Webb Space Telescope ; Morphology ; Skewed distributions ; Star &amp; galaxy formation ; Star formation ; Starburst galaxies ; Starbursts ; Stellar mass</subject><ispartof>arXiv.org, 2024-08</ispartof><rights>2024. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktohtml>$$Uhttps://www.proquest.com/docview/3054665506?pq-origsite=primo$$EHTML$$P50$$Gproquest$$Hfree_for_read</linktohtml><link.rule.ids>780,784,25753,27925,37012,44590</link.rule.ids></links><search><creatorcontrib>Polletta, M</creatorcontrib><creatorcontrib>Frye, B L</creatorcontrib><creatorcontrib>Garuda, N</creatorcontrib><creatorcontrib>Willner, S P</creatorcontrib><creatorcontrib>Berta, S</creatorcontrib><creatorcontrib>Kneissl, R</creatorcontrib><creatorcontrib>Dole, H</creatorcontrib><creatorcontrib>Jansen, R A</creatorcontrib><creatorcontrib>Lehnert, M D</creatorcontrib><creatorcontrib>Cohen, S H</creatorcontrib><creatorcontrib>Summers, J</creatorcontrib><creatorcontrib>Windhorst, R A</creatorcontrib><creatorcontrib>D'Silva, J C J</creatorcontrib><creatorcontrib>Koekemoer, A M</creatorcontrib><creatorcontrib>Coe, D</creatorcontrib><creatorcontrib>Conselice, C J</creatorcontrib><creatorcontrib>Driver, S P</creatorcontrib><creatorcontrib>Grogin, N A</creatorcontrib><creatorcontrib>Marshall, M A</creatorcontrib><creatorcontrib>Nonino, M</creatorcontrib><creatorcontrib>Ortiz, R</creatorcontrib><creatorcontrib>Pirzkal, N</creatorcontrib><creatorcontrib>Robotham, A</creatorcontrib><creatorcontrib>Ryan, R E</creatorcontrib><creatorcontrib>Jr</creatorcontrib><creatorcontrib>Willmer, C N A</creatorcontrib><creatorcontrib>Yan, H</creatorcontrib><creatorcontrib>Arumugam, V</creatorcontrib><creatorcontrib>Cheng, C</creatorcontrib><creatorcontrib>Gim, H B</creatorcontrib><creatorcontrib>Hathi, N P</creatorcontrib><creatorcontrib>Holwerda, B</creatorcontrib><creatorcontrib>Kamieneski, P</creatorcontrib><creatorcontrib>Keel, W C</creatorcontrib><creatorcontrib>J Li</creatorcontrib><creatorcontrib>Pascale, M</creatorcontrib><creatorcontrib>Rottgering, H</creatorcontrib><creatorcontrib>Smith, B M</creatorcontrib><creatorcontrib>Yun, M S</creatorcontrib><title>JWST's PEARLS: resolved study of the stellar and dust components in starburst galaxies at cosmic noon</title><title>arXiv.org</title><description>Dusty star-forming galaxies (DSFGs) contribute significantly to the stellar buildup at cosmic noon. Major mergers and gas accretion are often invoked to explain DSFGs' prodigious star-formation rates (SFRs) and large stellar masses. We conducted a spatially-resolved morphological analysis of the rest-frame UV/NIR emission in three DSFGs at z~2.5. Initially discovered as CO emitters by NOEMA observations of a bright Herschel source, we observed them with the JWST/NIRCam as part of the PEARLS program. The NIRCam data reveal the galaxies' stellar populations and dust distributions on scales of 250 pc. Spatial variations in stellar mass, SFR, and dust extinction are determined in resolved maps obtained through pixel-based SED fitting. The CO emitters are massive, dusty starburst galaxies with SFRs=340-2500 Msun/yr, positioning them among the most active SFGs at 2&lt;z&lt;3. They belong to the ~1.5% of the entire JWST population with extremely red colors. Their morphologies are disk like, with radii of 2.0-4.4 kpc, and exhibit substructures such as clumps and spiral arms. The galaxies have dust extinctions up to Av=5-7 mag extending over several kpc with asymmetric distributions that include off-center regions resembling bent spiral arms and clumps. Their NIR dust-attenuation curve deviates from standard laws, possibly implying different dust-star geometries or dust grain properties than commonly assumed in starburst galaxies. The proximity of galaxies with consistent redshifts, strong color gradients, an overall disturbed appearance, asymmetric dust obscuration, and widespread star formation collectively favor interactions (minor mergers and flybys) as the mechanism driving the CO galaxies' exceptional SFRs. The galaxies' large masses and rich environment hint at membership in two proto-structures, as initially inferred from their association with a Planck-selected high-z source.</description><subject>Clumps</subject><subject>Cosmic dust</subject><subject>Dust</subject><subject>Emitters</subject><subject>Galaxy distribution</subject><subject>James Webb Space Telescope</subject><subject>Morphology</subject><subject>Skewed distributions</subject><subject>Star &amp; galaxy formation</subject><subject>Star formation</subject><subject>Starburst galaxies</subject><subject>Starbursts</subject><subject>Stellar mass</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2024</creationdate><recordtype>article</recordtype><sourceid>PIMPY</sourceid><recordid>eNotUMtKw0AUHQTBUvsB7gZcuEq9mcfNxF0p9UVBsQWXZTpzoylpps4kpf69EV0dzuPeA4exqxymymgNtzae6uNUKNBTKEqDZ2wkpMwzo4S4YJOUdgAgsBBayxGj5_fV-ibx18Xsbbm645FSaI7keep6_81DxbtPGgg1jY3ctp77PnXchf0htNR2idftYNu47eOgf9jGnmpK3P5m0r52vA2hvWTnlW0STf5xzNb3i_X8MVu-PDzNZ8vMaoGZR1cWjhBVbjyY0pGsjKMCtkIXDkFLrwgJhTQlEFRaGRR-uMzLLQJ4OWbXf28PMXz1lLrNLvSxHRo3ErRCHPZB-QMyJ1bg</recordid><startdate>20240830</startdate><enddate>20240830</enddate><creator>Polletta, M</creator><creator>Frye, B L</creator><creator>Garuda, N</creator><creator>Willner, S P</creator><creator>Berta, S</creator><creator>Kneissl, R</creator><creator>Dole, H</creator><creator>Jansen, R A</creator><creator>Lehnert, M D</creator><creator>Cohen, S H</creator><creator>Summers, J</creator><creator>Windhorst, R A</creator><creator>D'Silva, J C J</creator><creator>Koekemoer, A M</creator><creator>Coe, D</creator><creator>Conselice, C J</creator><creator>Driver, S P</creator><creator>Grogin, N A</creator><creator>Marshall, M A</creator><creator>Nonino, M</creator><creator>Ortiz, R</creator><creator>Pirzkal, N</creator><creator>Robotham, A</creator><creator>Ryan, R E</creator><creator>Jr</creator><creator>Willmer, C N A</creator><creator>Yan, H</creator><creator>Arumugam, V</creator><creator>Cheng, C</creator><creator>Gim, H B</creator><creator>Hathi, N P</creator><creator>Holwerda, B</creator><creator>Kamieneski, P</creator><creator>Keel, W C</creator><creator>J Li</creator><creator>Pascale, M</creator><creator>Rottgering, H</creator><creator>Smith, B M</creator><creator>Yun, M S</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope></search><sort><creationdate>20240830</creationdate><title>JWST's PEARLS: resolved study of the stellar and dust components in starburst galaxies at cosmic noon</title><author>Polletta, M ; Frye, B L ; Garuda, N ; Willner, S P ; Berta, S ; Kneissl, R ; Dole, H ; Jansen, R A ; Lehnert, M D ; Cohen, S H ; Summers, J ; Windhorst, R A ; D'Silva, J C J ; Koekemoer, A M ; Coe, D ; Conselice, C J ; Driver, S P ; Grogin, N A ; Marshall, M A ; Nonino, M ; Ortiz, R ; Pirzkal, N ; Robotham, A ; Ryan, R E ; Jr ; Willmer, C N A ; Yan, H ; Arumugam, V ; Cheng, C ; Gim, H B ; Hathi, N P ; Holwerda, B ; Kamieneski, P ; Keel, W C ; J Li ; Pascale, M ; Rottgering, H ; Smith, B M ; Yun, M S</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a526-d6c97ce66418d089ce3f8ce70b257c6053d4e6e623890e0f54862d52619b600d3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2024</creationdate><topic>Clumps</topic><topic>Cosmic dust</topic><topic>Dust</topic><topic>Emitters</topic><topic>Galaxy distribution</topic><topic>James Webb Space Telescope</topic><topic>Morphology</topic><topic>Skewed distributions</topic><topic>Star &amp; galaxy formation</topic><topic>Star formation</topic><topic>Starburst galaxies</topic><topic>Starbursts</topic><topic>Stellar mass</topic><toplevel>online_resources</toplevel><creatorcontrib>Polletta, M</creatorcontrib><creatorcontrib>Frye, B L</creatorcontrib><creatorcontrib>Garuda, N</creatorcontrib><creatorcontrib>Willner, S P</creatorcontrib><creatorcontrib>Berta, S</creatorcontrib><creatorcontrib>Kneissl, R</creatorcontrib><creatorcontrib>Dole, H</creatorcontrib><creatorcontrib>Jansen, R A</creatorcontrib><creatorcontrib>Lehnert, M D</creatorcontrib><creatorcontrib>Cohen, S H</creatorcontrib><creatorcontrib>Summers, J</creatorcontrib><creatorcontrib>Windhorst, R A</creatorcontrib><creatorcontrib>D'Silva, J C J</creatorcontrib><creatorcontrib>Koekemoer, A M</creatorcontrib><creatorcontrib>Coe, D</creatorcontrib><creatorcontrib>Conselice, C J</creatorcontrib><creatorcontrib>Driver, S P</creatorcontrib><creatorcontrib>Grogin, N A</creatorcontrib><creatorcontrib>Marshall, M A</creatorcontrib><creatorcontrib>Nonino, M</creatorcontrib><creatorcontrib>Ortiz, R</creatorcontrib><creatorcontrib>Pirzkal, N</creatorcontrib><creatorcontrib>Robotham, A</creatorcontrib><creatorcontrib>Ryan, R E</creatorcontrib><creatorcontrib>Jr</creatorcontrib><creatorcontrib>Willmer, C N A</creatorcontrib><creatorcontrib>Yan, H</creatorcontrib><creatorcontrib>Arumugam, V</creatorcontrib><creatorcontrib>Cheng, C</creatorcontrib><creatorcontrib>Gim, H B</creatorcontrib><creatorcontrib>Hathi, N P</creatorcontrib><creatorcontrib>Holwerda, B</creatorcontrib><creatorcontrib>Kamieneski, P</creatorcontrib><creatorcontrib>Keel, W C</creatorcontrib><creatorcontrib>J Li</creatorcontrib><creatorcontrib>Pascale, M</creatorcontrib><creatorcontrib>Rottgering, H</creatorcontrib><creatorcontrib>Smith, B M</creatorcontrib><creatorcontrib>Yun, M S</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science &amp; Engineering Collection</collection><collection>ProQuest Central (Alumni)</collection><collection>ProQuest Central</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Publicly Available Content (ProQuest)</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Polletta, M</au><au>Frye, B L</au><au>Garuda, N</au><au>Willner, S P</au><au>Berta, S</au><au>Kneissl, R</au><au>Dole, H</au><au>Jansen, R A</au><au>Lehnert, M D</au><au>Cohen, S H</au><au>Summers, J</au><au>Windhorst, R A</au><au>D'Silva, J C J</au><au>Koekemoer, A M</au><au>Coe, D</au><au>Conselice, C J</au><au>Driver, S P</au><au>Grogin, N A</au><au>Marshall, M A</au><au>Nonino, M</au><au>Ortiz, R</au><au>Pirzkal, N</au><au>Robotham, A</au><au>Ryan, R E</au><au>Jr</au><au>Willmer, C N A</au><au>Yan, H</au><au>Arumugam, V</au><au>Cheng, C</au><au>Gim, H B</au><au>Hathi, N P</au><au>Holwerda, B</au><au>Kamieneski, P</au><au>Keel, W C</au><au>J Li</au><au>Pascale, M</au><au>Rottgering, H</au><au>Smith, B M</au><au>Yun, M S</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>JWST's PEARLS: resolved study of the stellar and dust components in starburst galaxies at cosmic noon</atitle><jtitle>arXiv.org</jtitle><date>2024-08-30</date><risdate>2024</risdate><eissn>2331-8422</eissn><abstract>Dusty star-forming galaxies (DSFGs) contribute significantly to the stellar buildup at cosmic noon. Major mergers and gas accretion are often invoked to explain DSFGs' prodigious star-formation rates (SFRs) and large stellar masses. We conducted a spatially-resolved morphological analysis of the rest-frame UV/NIR emission in three DSFGs at z~2.5. Initially discovered as CO emitters by NOEMA observations of a bright Herschel source, we observed them with the JWST/NIRCam as part of the PEARLS program. The NIRCam data reveal the galaxies' stellar populations and dust distributions on scales of 250 pc. Spatial variations in stellar mass, SFR, and dust extinction are determined in resolved maps obtained through pixel-based SED fitting. The CO emitters are massive, dusty starburst galaxies with SFRs=340-2500 Msun/yr, positioning them among the most active SFGs at 2&lt;z&lt;3. They belong to the ~1.5% of the entire JWST population with extremely red colors. Their morphologies are disk like, with radii of 2.0-4.4 kpc, and exhibit substructures such as clumps and spiral arms. The galaxies have dust extinctions up to Av=5-7 mag extending over several kpc with asymmetric distributions that include off-center regions resembling bent spiral arms and clumps. Their NIR dust-attenuation curve deviates from standard laws, possibly implying different dust-star geometries or dust grain properties than commonly assumed in starburst galaxies. The proximity of galaxies with consistent redshifts, strong color gradients, an overall disturbed appearance, asymmetric dust obscuration, and widespread star formation collectively favor interactions (minor mergers and flybys) as the mechanism driving the CO galaxies' exceptional SFRs. The galaxies' large masses and rich environment hint at membership in two proto-structures, as initially inferred from their association with a Planck-selected high-z source.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.2405.07986</doi><oa>free_for_read</oa></addata></record>
fulltext fulltext
identifier EISSN: 2331-8422
ispartof arXiv.org, 2024-08
issn 2331-8422
language eng
recordid cdi_proquest_journals_3054665506
source Publicly Available Content (ProQuest)
subjects Clumps
Cosmic dust
Dust
Emitters
Galaxy distribution
James Webb Space Telescope
Morphology
Skewed distributions
Star & galaxy formation
Star formation
Starburst galaxies
Starbursts
Stellar mass
title JWST's PEARLS: resolved study of the stellar and dust components in starburst galaxies at cosmic noon
url http://sfxeu10.hosted.exlibrisgroup.com/loughborough?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2024-12-18T18%3A36%3A04IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=JWST's%20PEARLS:%20resolved%20study%20of%20the%20stellar%20and%20dust%20components%20in%20starburst%20galaxies%20at%20cosmic%20noon&rft.jtitle=arXiv.org&rft.au=Polletta,%20M&rft.date=2024-08-30&rft.eissn=2331-8422&rft_id=info:doi/10.48550/arxiv.2405.07986&rft_dat=%3Cproquest%3E3054665506%3C/proquest%3E%3Cgrp_id%3Ecdi_FETCH-LOGICAL-a526-d6c97ce66418d089ce3f8ce70b257c6053d4e6e623890e0f54862d52619b600d3%3C/grp_id%3E%3Coa%3E%3C/oa%3E%3Curl%3E%3C/url%3E&rft_id=info:oai/&rft_pqid=3054665506&rft_id=info:pmid/&rfr_iscdi=true