Reionization and the ISM/Stellar Origins with JWST and ALMA (RIOJA): The Core of the Highest-redshift Galaxy Overdensity at z = 7.88 Confirmed by NIRSpec/JWST
The protoclusters in the epoch of reionization, traced by galaxy overdensity regions, are ideal laboratories for studying the process of stellar assembly and cosmic reionization. We present the spectroscopic confirmation of the core of the most distant protocluster at z = 7.88, A2744-z7p9OD, with th...
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| Veröffentlicht in: | Astrophysical journal. Letters 2023-09, Vol.955 (1), p.L2 |
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| creator | Hashimoto, T. Álvarez-Márquez, J. Fudamoto, Y. Colina, L. Inoue, A. K. Nakazato, Y. Ceverino, D. Yoshida, N. Costantin, L. Sugahara, Y. Gómez, A. Crespo Blanco-Prieto, C. Mawatari, K. Arribas, S. Marques-Chaves, R. Pereira-Santaella, M. Bakx, T. J. L. C. Hagimoto, M. Hashigaya, T. Matsuo, H. Tamura, Y. Usui, M. Ren, Y. W. |
| description | The protoclusters in the epoch of reionization, traced by galaxy overdensity regions, are ideal laboratories for studying the process of stellar assembly and cosmic reionization. We present the spectroscopic confirmation of the core of the most distant protocluster at
z
= 7.88, A2744-z7p9OD, with the James Webb Space Telescope NIRSpec integral field unit spectroscopy. The core region includes as many as four galaxies detected in [O
iii
] 4960 and 5008 Å in a small area of ∼3″ × 3″, corresponding to ∼11 × 11 kpc, after the lensing magnification correction. Three member galaxies are also tentatively detected in dust continuum in Atacama Large Millimeter/submillimeter Array Band 6, which is consistent with their red ultraviolet continuum slopes,
β
∼ −1.3. The member galaxies have stellar masses in the range of log(
M
*
/
M
⊙
) ∼7.6–9.2 and star formation rates of ∼3–50
M
⊙
yr
−1
, showing a diversity in their properties. FirstLight cosmological simulations reproduce the physical properties of the member galaxies including the stellar mass, [O
iii
] luminosity, and dust-to-stellar mass ratio, and predict that the member galaxies are on the verge of merging in a few to several tens of Myr to become a large galaxy with
M
*
∼ 6 × 10
9
M
⊙
. The presence of a multiple merger and evolved galaxies in the core region of A2744-z7p9OD indicates that environmental effects are already at work 650 Myr after the Big Bang. |
| doi_str_mv | 10.3847/2041-8213/acf57c |
| format | Article |
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z
= 7.88, A2744-z7p9OD, with the James Webb Space Telescope NIRSpec integral field unit spectroscopy. The core region includes as many as four galaxies detected in [O
iii
] 4960 and 5008 Å in a small area of ∼3″ × 3″, corresponding to ∼11 × 11 kpc, after the lensing magnification correction. Three member galaxies are also tentatively detected in dust continuum in Atacama Large Millimeter/submillimeter Array Band 6, which is consistent with their red ultraviolet continuum slopes,
β
∼ −1.3. The member galaxies have stellar masses in the range of log(
M
*
/
M
⊙
) ∼7.6–9.2 and star formation rates of ∼3–50
M
⊙
yr
−1
, showing a diversity in their properties. FirstLight cosmological simulations reproduce the physical properties of the member galaxies including the stellar mass, [O
iii
] luminosity, and dust-to-stellar mass ratio, and predict that the member galaxies are on the verge of merging in a few to several tens of Myr to become a large galaxy with
M
*
∼ 6 × 10
9
M
⊙
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z
= 7.88, A2744-z7p9OD, with the James Webb Space Telescope NIRSpec integral field unit spectroscopy. The core region includes as many as four galaxies detected in [O
iii
] 4960 and 5008 Å in a small area of ∼3″ × 3″, corresponding to ∼11 × 11 kpc, after the lensing magnification correction. Three member galaxies are also tentatively detected in dust continuum in Atacama Large Millimeter/submillimeter Array Band 6, which is consistent with their red ultraviolet continuum slopes,
β
∼ −1.3. The member galaxies have stellar masses in the range of log(
M
*
/
M
⊙
) ∼7.6–9.2 and star formation rates of ∼3–50
M
⊙
yr
−1
, showing a diversity in their properties. FirstLight cosmological simulations reproduce the physical properties of the member galaxies including the stellar mass, [O
iii
] luminosity, and dust-to-stellar mass ratio, and predict that the member galaxies are on the verge of merging in a few to several tens of Myr to become a large galaxy with
M
*
∼ 6 × 10
9
M
⊙
. The presence of a multiple merger and evolved galaxies in the core region of A2744-z7p9OD indicates that environmental effects are already at work 650 Myr after the Big Bang.</description><subject>Big bang cosmology</subject><subject>Cosmic dust</subject><subject>Dust</subject><subject>Environmental effects</subject><subject>Galactic evolution</subject><subject>Galaxies</subject><subject>Ionization</subject><subject>James Webb Space Telescope</subject><subject>Luminosity</subject><subject>Physical properties</subject><subject>Primordial galaxies</subject><subject>Protoclusters</subject><subject>Radio telescopes</subject><subject>Red shift</subject><subject>Space telescopes</subject><subject>Spectroscopy</subject><subject>Star & galaxy formation</subject><subject>Star formation</subject><subject>Stars & galaxies</subject><subject>Stellar mass</subject><issn>2041-8205</issn><issn>2041-8213</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2023</creationdate><recordtype>article</recordtype><sourceid>O3W</sourceid><sourceid>DOA</sourceid><recordid>eNp9kV-LEzEUxQdRcF199zEggoKzTTJ_kgg-lKK7s3QttBUfQya5aVNmJ2Mm6273w_hZnXakvohP93I5v3Mv9yTJa4IvMp6zCcU5STkl2URpWzD9JDk7jZ6eelw8T170_Q5jikvCz5JfS3C-dY8qDgWp1qC4BVStbiarCE2jAloEt3Ftj-5d3KLr76v1UTWd30zRu2W1uJ6-_4jWAzPzAZC3R_7KbbbQxzSA6bfORnSpGvWwR4ufEAy0vYt7pCJ6RJ8Qu-B8YFvrwi0YVO_R12q56kBPDrteJs-sanp49aeeJ9--fF7PrtL54rKaTeepzgWOKbCcEGCUCVrWJWegC2KyUltKjdWsqAnhNeUahIECtKI5z62whmVAqKA0O0-q0dd4tZNdcLcq7KVXTh4HPmykCtHpBiQVTJCS1XWBVQ4F5oQakme1tdgyi9Xg9Wb06oL_cTe8Qe78XWiH8yXlZS4EpjkZVHhU6eD7PoA9bSVYHhKVh8jkIT45JjogH0bE-e6v53_kb_8hV92ukaIoJJFzKjtjs9_ZTawe</recordid><startdate>20230901</startdate><enddate>20230901</enddate><creator>Hashimoto, T.</creator><creator>Álvarez-Márquez, J.</creator><creator>Fudamoto, Y.</creator><creator>Colina, L.</creator><creator>Inoue, A. K.</creator><creator>Nakazato, Y.</creator><creator>Ceverino, D.</creator><creator>Yoshida, N.</creator><creator>Costantin, L.</creator><creator>Sugahara, Y.</creator><creator>Gómez, A. Crespo</creator><creator>Blanco-Prieto, C.</creator><creator>Mawatari, K.</creator><creator>Arribas, S.</creator><creator>Marques-Chaves, R.</creator><creator>Pereira-Santaella, M.</creator><creator>Bakx, T. J. L. C.</creator><creator>Hagimoto, M.</creator><creator>Hashigaya, T.</creator><creator>Matsuo, H.</creator><creator>Tamura, Y.</creator><creator>Usui, M.</creator><creator>Ren, Y. W.</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/0000-0002-7779-8677</orcidid><orcidid>https://orcid.org/0000-0001-6820-0015</orcidid><orcidid>https://orcid.org/0000-0003-2119-277X</orcidid><orcidid>https://orcid.org/0000-0003-3278-2484</orcidid><orcidid>https://orcid.org/0000-0001-7440-8832</orcidid><orcidid>https://orcid.org/0000-0002-8680-248X</orcidid><orcidid>https://orcid.org/0000-0002-7093-1877</orcidid><orcidid>https://orcid.org/0000-0002-5268-2221</orcidid><orcidid>https://orcid.org/0000-0001-6958-7856</orcidid><orcidid>https://orcid.org/0000-0002-9090-4227</orcidid><orcidid>https://orcid.org/0000-0001-7925-238X</orcidid><orcidid>https://orcid.org/0009-0005-5448-5239</orcidid><orcidid>https://orcid.org/0000-0002-4005-9619</orcidid><orcidid>https://orcid.org/0000-0001-8083-5814</orcidid><orcidid>https://orcid.org/0000-0001-8442-1846</orcidid><orcidid>https://orcid.org/0000-0002-0984-7713</orcidid><orcidid>https://orcid.org/0000-0003-4985-0201</orcidid><orcidid>https://orcid.org/0000-0001-7997-1640</orcidid><orcidid>https://orcid.org/0000-0002-0898-4038</orcidid><orcidid>https://orcid.org/0000-0003-4807-8117</orcidid></search><sort><creationdate>20230901</creationdate><title>Reionization and the ISM/Stellar Origins with JWST and ALMA (RIOJA): The Core of the Highest-redshift Galaxy Overdensity at z = 7.88 Confirmed by NIRSpec/JWST</title><author>Hashimoto, T. ; Álvarez-Márquez, J. ; Fudamoto, Y. ; Colina, L. ; Inoue, A. K. ; Nakazato, Y. ; Ceverino, D. ; Yoshida, N. ; Costantin, L. ; Sugahara, Y. ; Gómez, A. Crespo ; Blanco-Prieto, C. ; Mawatari, K. ; Arribas, S. ; Marques-Chaves, R. ; Pereira-Santaella, M. ; Bakx, T. J. L. C. ; Hagimoto, M. ; Hashigaya, T. ; Matsuo, H. ; Tamura, Y. ; Usui, M. ; Ren, Y. W.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c490t-e7411e727926b687ec51d36cf22dfc75b118b28ce9de5eca2484f9fd73e129223</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2023</creationdate><topic>Big bang cosmology</topic><topic>Cosmic dust</topic><topic>Dust</topic><topic>Environmental effects</topic><topic>Galactic evolution</topic><topic>Galaxies</topic><topic>Ionization</topic><topic>James Webb Space Telescope</topic><topic>Luminosity</topic><topic>Physical properties</topic><topic>Primordial galaxies</topic><topic>Protoclusters</topic><topic>Radio telescopes</topic><topic>Red shift</topic><topic>Space telescopes</topic><topic>Spectroscopy</topic><topic>Star & galaxy formation</topic><topic>Star formation</topic><topic>Stars & galaxies</topic><topic>Stellar mass</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Hashimoto, T.</creatorcontrib><creatorcontrib>Álvarez-Márquez, J.</creatorcontrib><creatorcontrib>Fudamoto, Y.</creatorcontrib><creatorcontrib>Colina, L.</creatorcontrib><creatorcontrib>Inoue, A. 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W.</creatorcontrib><collection>Open Access: IOP Publishing Free Content</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>Directory of Open Access Journals</collection><jtitle>Astrophysical journal. Letters</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Hashimoto, T.</au><au>Álvarez-Márquez, J.</au><au>Fudamoto, Y.</au><au>Colina, L.</au><au>Inoue, A. K.</au><au>Nakazato, Y.</au><au>Ceverino, D.</au><au>Yoshida, N.</au><au>Costantin, L.</au><au>Sugahara, Y.</au><au>Gómez, A. Crespo</au><au>Blanco-Prieto, C.</au><au>Mawatari, K.</au><au>Arribas, S.</au><au>Marques-Chaves, R.</au><au>Pereira-Santaella, M.</au><au>Bakx, T. J. L. C.</au><au>Hagimoto, M.</au><au>Hashigaya, T.</au><au>Matsuo, H.</au><au>Tamura, Y.</au><au>Usui, M.</au><au>Ren, Y. W.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Reionization and the ISM/Stellar Origins with JWST and ALMA (RIOJA): The Core of the Highest-redshift Galaxy Overdensity at z = 7.88 Confirmed by NIRSpec/JWST</atitle><jtitle>Astrophysical journal. Letters</jtitle><stitle>APJL</stitle><addtitle>Astrophys. J. Lett</addtitle><date>2023-09-01</date><risdate>2023</risdate><volume>955</volume><issue>1</issue><spage>L2</spage><pages>L2-</pages><issn>2041-8205</issn><eissn>2041-8213</eissn><abstract>The protoclusters in the epoch of reionization, traced by galaxy overdensity regions, are ideal laboratories for studying the process of stellar assembly and cosmic reionization. We present the spectroscopic confirmation of the core of the most distant protocluster at
z
= 7.88, A2744-z7p9OD, with the James Webb Space Telescope NIRSpec integral field unit spectroscopy. The core region includes as many as four galaxies detected in [O
iii
] 4960 and 5008 Å in a small area of ∼3″ × 3″, corresponding to ∼11 × 11 kpc, after the lensing magnification correction. Three member galaxies are also tentatively detected in dust continuum in Atacama Large Millimeter/submillimeter Array Band 6, which is consistent with their red ultraviolet continuum slopes,
β
∼ −1.3. The member galaxies have stellar masses in the range of log(
M
*
/
M
⊙
) ∼7.6–9.2 and star formation rates of ∼3–50
M
⊙
yr
−1
, showing a diversity in their properties. FirstLight cosmological simulations reproduce the physical properties of the member galaxies including the stellar mass, [O
iii
] luminosity, and dust-to-stellar mass ratio, and predict that the member galaxies are on the verge of merging in a few to several tens of Myr to become a large galaxy with
M
*
∼ 6 × 10
9
M
⊙
. The presence of a multiple merger and evolved galaxies in the core region of A2744-z7p9OD indicates that environmental effects are already at work 650 Myr after the Big Bang.</abstract><cop>Austin</cop><pub>The American Astronomical Society</pub><doi>10.3847/2041-8213/acf57c</doi><tpages>8</tpages><orcidid>https://orcid.org/0000-0002-7779-8677</orcidid><orcidid>https://orcid.org/0000-0001-6820-0015</orcidid><orcidid>https://orcid.org/0000-0003-2119-277X</orcidid><orcidid>https://orcid.org/0000-0003-3278-2484</orcidid><orcidid>https://orcid.org/0000-0001-7440-8832</orcidid><orcidid>https://orcid.org/0000-0002-8680-248X</orcidid><orcidid>https://orcid.org/0000-0002-7093-1877</orcidid><orcidid>https://orcid.org/0000-0002-5268-2221</orcidid><orcidid>https://orcid.org/0000-0001-6958-7856</orcidid><orcidid>https://orcid.org/0000-0002-9090-4227</orcidid><orcidid>https://orcid.org/0000-0001-7925-238X</orcidid><orcidid>https://orcid.org/0009-0005-5448-5239</orcidid><orcidid>https://orcid.org/0000-0002-4005-9619</orcidid><orcidid>https://orcid.org/0000-0001-8083-5814</orcidid><orcidid>https://orcid.org/0000-0001-8442-1846</orcidid><orcidid>https://orcid.org/0000-0002-0984-7713</orcidid><orcidid>https://orcid.org/0000-0003-4985-0201</orcidid><orcidid>https://orcid.org/0000-0001-7997-1640</orcidid><orcidid>https://orcid.org/0000-0002-0898-4038</orcidid><orcidid>https://orcid.org/0000-0003-4807-8117</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 2041-8205 |
| ispartof | Astrophysical journal. Letters, 2023-09, Vol.955 (1), p.L2 |
| issn | 2041-8205 2041-8213 |
| language | eng |
| recordid | cdi_proquest_journals_2864990241 |
| source | Open Access: IOP Publishing Free Content; IOPscience journals; Directory of Open Access Journals; Alma/SFX Local Collection; EZB Electronic Journals Library |
| subjects | Big bang cosmology Cosmic dust Dust Environmental effects Galactic evolution Galaxies Ionization James Webb Space Telescope Luminosity Physical properties Primordial galaxies Protoclusters Radio telescopes Red shift Space telescopes Spectroscopy Star & galaxy formation Star formation Stars & galaxies Stellar mass |
| title | Reionization and the ISM/Stellar Origins with JWST and ALMA (RIOJA): The Core of the Highest-redshift Galaxy Overdensity at z = 7.88 Confirmed by NIRSpec/JWST |
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