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Assessment of SDSS-derived Galaxy Morphologies Using HST Imaging
The Sloan Digital Sky Survey (SDSS) was foundational to the study of galaxy evolution, having revealed the bimodality of galaxies and the relationship between their structure and star-forming activity. However, ground-based optical surveys like SDSS are limited in resolution and depth, which may lea...
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Published in: | The Astrophysical journal 2024-04, Vol.965 (2), p.161 |
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description | The Sloan Digital Sky Survey (SDSS) was foundational to the study of galaxy evolution, having revealed the bimodality of galaxies and the relationship between their structure and star-forming activity. However, ground-based optical surveys like SDSS are limited in resolution and depth, which may lead to biases or poor quality in the derived morphological properties, potentially impacting our understanding of how and why galaxies cease their star formation (quench). We use archival Hubble Space Telescope (HST) imaging of ∼2000 SDSS objects to assess the reliability of SDSS-derived morphologies, taking advantage of both SDSS statistical samples and HST’s superior resolution and sensitivity. Single Sérsic fitting and bulge-disk decomposition is performed on HST images for direct comparison with SDSS results. Of the three catalogs of SDSS-derived morphologies considered, none is significantly more accurate or precise than the others. For disk-dominated galaxies (
n
< 2.5), global Sérsic indices (
n
) from Meert et al. (hereafter, M15) are preferred. For bulge-dominated galaxies (
n
> 2.5), Simard et al. (hereafter, S11) and M15 overestimate
n
by ∼20%, and derived global
n
from Blanton et al. are preferred. We provide an empirical relation to correct S11 global Sérsic indices. Global
R
eff
from S11 overestimates
R
eff
for the largest galaxies by 0.1 dex. Despite these moderate biases, SDSS-derived single-component parameters are generally significantly more robust than SDSS-derived two-component parameters. The bulge Sérsic index (
n
bulge
) cannot be reliably constrained from SDSS imaging at all, whereas the bulge-to-total (
B
/
T
) ratio can be inferred from SDSS (provided that
n
bulge
= 4 is enforced) but has a large random error of ∼0.2. |
doi_str_mv | 10.3847/1538-4357/ad320f |
format | article |
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n
< 2.5), global Sérsic indices (
n
) from Meert et al. (hereafter, M15) are preferred. For bulge-dominated galaxies (
n
> 2.5), Simard et al. (hereafter, S11) and M15 overestimate
n
by ∼20%, and derived global
n
from Blanton et al. are preferred. We provide an empirical relation to correct S11 global Sérsic indices. Global
R
eff
from S11 overestimates
R
eff
for the largest galaxies by 0.1 dex. Despite these moderate biases, SDSS-derived single-component parameters are generally significantly more robust than SDSS-derived two-component parameters. The bulge Sérsic index (
n
bulge
) cannot be reliably constrained from SDSS imaging at all, whereas the bulge-to-total (
B
/
T
) ratio can be inferred from SDSS (provided that
n
bulge
= 4 is enforced) but has a large random error of ∼0.2.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.3847/1538-4357/ad320f</identifier><language>eng</language><publisher>Philadelphia: The American Astronomical Society</publisher><subject>Bias ; Digital imaging ; Disk galaxies ; Early-type galaxies ; Galactic and extragalactic astronomy ; Galactic evolution ; Galaxies ; Galaxy bulges ; Galaxy classification systems ; Galaxy evolution ; Galaxy quenching ; Galaxy structure ; Hubble Space Telescope ; Imaging techniques ; Late-type galaxies ; Morphology ; Parameters ; Quenched galaxies ; Random errors ; Random sampling ; Reliability analysis ; Sky surveys (astronomy) ; Space telescopes ; Star & galaxy formation ; Star formation ; Stars & galaxies ; Statistical analysis ; Statistical sampling</subject><ispartof>The Astrophysical journal, 2024-04, Vol.965 (2), p.161</ispartof><rights>2024. The Author(s). Published by the American Astronomical Society.</rights><rights>2024. The Author(s). Published by the American Astronomical Society. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><cites>FETCH-LOGICAL-c399t-80276106f3d44f87c415ec1fd69d536968690378e224fc360f1a174a948fe68e3</cites><orcidid>0000-0003-2342-7501</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,776,780,27901,27902</link.rule.ids></links><search><creatorcontrib>Osborne, Chandler</creatorcontrib><creatorcontrib>Salim, Samir</creatorcontrib><title>Assessment of SDSS-derived Galaxy Morphologies Using HST Imaging</title><title>The Astrophysical journal</title><addtitle>APJ</addtitle><addtitle>Astrophys. J</addtitle><description>The Sloan Digital Sky Survey (SDSS) was foundational to the study of galaxy evolution, having revealed the bimodality of galaxies and the relationship between their structure and star-forming activity. However, ground-based optical surveys like SDSS are limited in resolution and depth, which may lead to biases or poor quality in the derived morphological properties, potentially impacting our understanding of how and why galaxies cease their star formation (quench). We use archival Hubble Space Telescope (HST) imaging of ∼2000 SDSS objects to assess the reliability of SDSS-derived morphologies, taking advantage of both SDSS statistical samples and HST’s superior resolution and sensitivity. Single Sérsic fitting and bulge-disk decomposition is performed on HST images for direct comparison with SDSS results. Of the three catalogs of SDSS-derived morphologies considered, none is significantly more accurate or precise than the others. For disk-dominated galaxies (
n
< 2.5), global Sérsic indices (
n
) from Meert et al. (hereafter, M15) are preferred. For bulge-dominated galaxies (
n
> 2.5), Simard et al. (hereafter, S11) and M15 overestimate
n
by ∼20%, and derived global
n
from Blanton et al. are preferred. We provide an empirical relation to correct S11 global Sérsic indices. Global
R
eff
from S11 overestimates
R
eff
for the largest galaxies by 0.1 dex. Despite these moderate biases, SDSS-derived single-component parameters are generally significantly more robust than SDSS-derived two-component parameters. The bulge Sérsic index (
n
bulge
) cannot be reliably constrained from SDSS imaging at all, whereas the bulge-to-total (
B
/
T
) ratio can be inferred from SDSS (provided that
n
bulge
= 4 is enforced) but has a large random error of ∼0.2.</description><subject>Bias</subject><subject>Digital imaging</subject><subject>Disk galaxies</subject><subject>Early-type galaxies</subject><subject>Galactic and extragalactic astronomy</subject><subject>Galactic evolution</subject><subject>Galaxies</subject><subject>Galaxy bulges</subject><subject>Galaxy classification systems</subject><subject>Galaxy evolution</subject><subject>Galaxy quenching</subject><subject>Galaxy structure</subject><subject>Hubble Space Telescope</subject><subject>Imaging techniques</subject><subject>Late-type galaxies</subject><subject>Morphology</subject><subject>Parameters</subject><subject>Quenched galaxies</subject><subject>Random errors</subject><subject>Random sampling</subject><subject>Reliability analysis</subject><subject>Sky surveys (astronomy)</subject><subject>Space telescopes</subject><subject>Star & galaxy formation</subject><subject>Star formation</subject><subject>Stars & galaxies</subject><subject>Statistical analysis</subject><subject>Statistical sampling</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2024</creationdate><recordtype>article</recordtype><sourceid>DOA</sourceid><recordid>eNp9kM1PAjEQxRujiYjePW5ivLnS7vTzJkEFEo0HIPHWNNsWlwBdWzDy37u4Bi_G08y8vHkz-SF0SfAtSCp6hIHMKTDRMxYK7I9Q5yAdow7GmOYcxOspOktpsR8LpTrorp-SS2nl1pss-GxyP5nk1sXqw9lsaJbmc5c9h1i_hWWYVy5ls1St59loMs3GKzNv-nN04s0yuYuf2kWzx4fpYJQ_vQzHg_5TXoJSm1ziQnCCuQdLqZeipIS5knjLlWXAFZdcYRDSFQX1JXDsiSGCGkWld1w66KJxm2uDWeg6VisTdzqYSn8LIc61iZuqXDrNi0KAp4oRTCihpQFSKmEoA6YsZ7LJumqz6hjety5t9CJs47p5XwOmmClGBTQu3LrKGFKKzh-uEqz3zPUesN4D1i3zZuWmXalC_Zv5j_36D7upF1pxpgtNONG19fAFNsyLMw</recordid><startdate>20240401</startdate><enddate>20240401</enddate><creator>Osborne, Chandler</creator><creator>Salim, Samir</creator><general>The American Astronomical Society</general><general>IOP Publishing</general><scope>O3W</scope><scope>TSCCA</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope><scope>DOA</scope><orcidid>https://orcid.org/0000-0003-2342-7501</orcidid></search><sort><creationdate>20240401</creationdate><title>Assessment of SDSS-derived Galaxy Morphologies Using HST Imaging</title><author>Osborne, Chandler ; Salim, Samir</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c399t-80276106f3d44f87c415ec1fd69d536968690378e224fc360f1a174a948fe68e3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2024</creationdate><topic>Bias</topic><topic>Digital imaging</topic><topic>Disk galaxies</topic><topic>Early-type galaxies</topic><topic>Galactic and extragalactic astronomy</topic><topic>Galactic evolution</topic><topic>Galaxies</topic><topic>Galaxy bulges</topic><topic>Galaxy classification systems</topic><topic>Galaxy evolution</topic><topic>Galaxy quenching</topic><topic>Galaxy structure</topic><topic>Hubble Space Telescope</topic><topic>Imaging techniques</topic><topic>Late-type galaxies</topic><topic>Morphology</topic><topic>Parameters</topic><topic>Quenched galaxies</topic><topic>Random errors</topic><topic>Random sampling</topic><topic>Reliability analysis</topic><topic>Sky surveys (astronomy)</topic><topic>Space telescopes</topic><topic>Star & galaxy formation</topic><topic>Star formation</topic><topic>Stars & galaxies</topic><topic>Statistical analysis</topic><topic>Statistical sampling</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Osborne, Chandler</creatorcontrib><creatorcontrib>Salim, Samir</creatorcontrib><collection>Institute of Physics Open Access Journal Titles</collection><collection>IOPscience (Open Access)</collection><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Open Access: DOAJ - Directory of Open Access Journals</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Osborne, Chandler</au><au>Salim, Samir</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Assessment of SDSS-derived Galaxy Morphologies Using HST Imaging</atitle><jtitle>The Astrophysical journal</jtitle><stitle>APJ</stitle><addtitle>Astrophys. J</addtitle><date>2024-04-01</date><risdate>2024</risdate><volume>965</volume><issue>2</issue><spage>161</spage><pages>161-</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><abstract>The Sloan Digital Sky Survey (SDSS) was foundational to the study of galaxy evolution, having revealed the bimodality of galaxies and the relationship between their structure and star-forming activity. However, ground-based optical surveys like SDSS are limited in resolution and depth, which may lead to biases or poor quality in the derived morphological properties, potentially impacting our understanding of how and why galaxies cease their star formation (quench). We use archival Hubble Space Telescope (HST) imaging of ∼2000 SDSS objects to assess the reliability of SDSS-derived morphologies, taking advantage of both SDSS statistical samples and HST’s superior resolution and sensitivity. Single Sérsic fitting and bulge-disk decomposition is performed on HST images for direct comparison with SDSS results. Of the three catalogs of SDSS-derived morphologies considered, none is significantly more accurate or precise than the others. For disk-dominated galaxies (
n
< 2.5), global Sérsic indices (
n
) from Meert et al. (hereafter, M15) are preferred. For bulge-dominated galaxies (
n
> 2.5), Simard et al. (hereafter, S11) and M15 overestimate
n
by ∼20%, and derived global
n
from Blanton et al. are preferred. We provide an empirical relation to correct S11 global Sérsic indices. Global
R
eff
from S11 overestimates
R
eff
for the largest galaxies by 0.1 dex. Despite these moderate biases, SDSS-derived single-component parameters are generally significantly more robust than SDSS-derived two-component parameters. The bulge Sérsic index (
n
bulge
) cannot be reliably constrained from SDSS imaging at all, whereas the bulge-to-total (
B
/
T
) ratio can be inferred from SDSS (provided that
n
bulge
= 4 is enforced) but has a large random error of ∼0.2.</abstract><cop>Philadelphia</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-4357/ad320f</doi><tpages>12</tpages><orcidid>https://orcid.org/0000-0003-2342-7501</orcidid><oa>free_for_read</oa></addata></record> |
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subjects | Bias Digital imaging Disk galaxies Early-type galaxies Galactic and extragalactic astronomy Galactic evolution Galaxies Galaxy bulges Galaxy classification systems Galaxy evolution Galaxy quenching Galaxy structure Hubble Space Telescope Imaging techniques Late-type galaxies Morphology Parameters Quenched galaxies Random errors Random sampling Reliability analysis Sky surveys (astronomy) Space telescopes Star & galaxy formation Star formation Stars & galaxies Statistical analysis Statistical sampling |
title | Assessment of SDSS-derived Galaxy Morphologies Using HST Imaging |
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