The ALPINE-ALMA [CII] Survey: Investigation of 10 Galaxies at $z\sim4.5$ with [OII] and [CII] Line Emission $-$ ISM Properties and [OII]$-$SFR Relation
We present $10$ main-sequence ALPINE galaxies (log($M/M_{\odot}$) = 9.2-11.1 and ${\rm SFR}=23-190\,{\rm M_{\odot}\,yr^{-1}}$) at $z\sim4.5$ with optical [OII] measurements from Keck/MOSFIRE spectroscopy and Subaru/MOIRCS narrow-band imaging. This is the largest such multi-wavelength sample at these...
Gespeichert in:
Hauptverfasser: | , , , , , , , , , , , , , , , , , , , , , , , , , |
---|---|
Format: | Artikel |
Sprache: | eng |
Schlagworte: | |
Online-Zugang: | Volltext bestellen |
Tags: |
Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
|
container_end_page | |
---|---|
container_issue | |
container_start_page | |
container_title | |
container_volume | |
creator | Vanderhoof, Brittany N Faisst, A. L Shen, L Lemaux, B. C Béthermin, M Capak, P. L Cassata, P Fèvre, O. Le Schaerer, D Silverman, J Yan, L Boquien, M Gal, R Kartaltepe, J Lubin, L. M Dessauges-Zavadsky, M Fudamoto, Y Ginolfi, M Hathi, N. P Jones, G. C Koekemoer, A. M Narayanan, D Romano, M Talia, M Vergani, D Zamorani, G |
description | We present $10$ main-sequence ALPINE galaxies (log($M/M_{\odot}$) = 9.2-11.1
and ${\rm SFR}=23-190\,{\rm M_{\odot}\,yr^{-1}}$) at $z\sim4.5$ with optical
[OII] measurements from Keck/MOSFIRE spectroscopy and Subaru/MOIRCS narrow-band
imaging. This is the largest such multi-wavelength sample at these redshifts,
combining various measurements in the ultra-violet, optical, and far-infrared
including [CII]$_{158{\rm \mu m}}$ line emission and dust continuum from ALMA
and H$\alpha$ emission from Spitzer photometry. For the first time, this unique
sample allows us to analyze the relation between [OII] and total star-formation
rate (SFR) and the interstellar medium (ISM) properties via [OII]/[CII] and
[OII]/\halpha luminosity ratios at $z\sim4.5$. The [OII]$-$SFR relation at
$z\sim4.5$ cannot be described using standard local descriptions, but is
consistent with a metal-dependent relation assuming metallicities around $50\%$
solar. To explain the measured dust-corrected luminosity ratios of
$L[OII]/L[CII] \sim 0.98^{+0.21}_{-0.22}$ and $L[OII]/LHa \sim
-0.22^{+0.13}_{-0.15}$ for our sample, ionization parameters $\log(U)< -2$ and
electron densities $\log(\rm n_e / {\rm [cm^{-3}]}) \sim 2.5-3$ are required.
The former is consistent with galaxies at $z\sim2-3$, however lower than at
$z>6$. The latter may be slightly higher than expected given the galaxies'
specific SFR. The analysis of this pilot sample suggests that typical log($
M/M_{\odot})$ > 9 galaxies at $z\sim4.5$ to have broadly similar ISM properties
as their descendants at $z\sim2$ and suggest a strong evolution of ISM
properties since the Epoch of Reionization at $z>6$. |
doi_str_mv | 10.48550/arxiv.2201.03587 |
format | Article |
fullrecord | <record><control><sourceid>arxiv_GOX</sourceid><recordid>TN_cdi_arxiv_primary_2201_03587</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>2201_03587</sourcerecordid><originalsourceid>FETCH-arxiv_primary_2201_035873</originalsourceid><addsrcrecordid>eNqFj7sKwkAQRbexEPUDrJwibeJGExS7IFEX4gNjFyUsuOpAHrK7xseP-Lu6wd5qinvPHQ4hXZc63tj3aZ_LB1bOYEBdhw798ahJ3ruLgCDasFVoB9EygGTK2AHim6zEcwKsqITSeOYaywLKE7gU5jzjDxQKuAbrtVeYe45vwR31BZK1oXlx_O1EWAgIc1TK8JZtAYuXsJHlVUhdb5iqgb5ZPNvCVmT1rzZpnHimROd3W6Q3C3fThV0rpFeJOZfP1Kiktcrwf-MD3j9Pqg</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype></control><display><type>article</type><title>The ALPINE-ALMA [CII] Survey: Investigation of 10 Galaxies at $z\sim4.5$ with [OII] and [CII] Line Emission $-$ ISM Properties and [OII]$-$SFR Relation</title><source>arXiv.org</source><creator>Vanderhoof, Brittany N ; Faisst, A. L ; Shen, L ; Lemaux, B. C ; Béthermin, M ; Capak, P. L ; Cassata, P ; Fèvre, O. Le ; Schaerer, D ; Silverman, J ; Yan, L ; Boquien, M ; Gal, R ; Kartaltepe, J ; Lubin, L. M ; Dessauges-Zavadsky, M ; Fudamoto, Y ; Ginolfi, M ; Hathi, N. P ; Jones, G. C ; Koekemoer, A. M ; Narayanan, D ; Romano, M ; Talia, M ; Vergani, D ; Zamorani, G</creator><creatorcontrib>Vanderhoof, Brittany N ; Faisst, A. L ; Shen, L ; Lemaux, B. C ; Béthermin, M ; Capak, P. L ; Cassata, P ; Fèvre, O. Le ; Schaerer, D ; Silverman, J ; Yan, L ; Boquien, M ; Gal, R ; Kartaltepe, J ; Lubin, L. M ; Dessauges-Zavadsky, M ; Fudamoto, Y ; Ginolfi, M ; Hathi, N. P ; Jones, G. C ; Koekemoer, A. M ; Narayanan, D ; Romano, M ; Talia, M ; Vergani, D ; Zamorani, G</creatorcontrib><description>We present $10$ main-sequence ALPINE galaxies (log($M/M_{\odot}$) = 9.2-11.1
and ${\rm SFR}=23-190\,{\rm M_{\odot}\,yr^{-1}}$) at $z\sim4.5$ with optical
[OII] measurements from Keck/MOSFIRE spectroscopy and Subaru/MOIRCS narrow-band
imaging. This is the largest such multi-wavelength sample at these redshifts,
combining various measurements in the ultra-violet, optical, and far-infrared
including [CII]$_{158{\rm \mu m}}$ line emission and dust continuum from ALMA
and H$\alpha$ emission from Spitzer photometry. For the first time, this unique
sample allows us to analyze the relation between [OII] and total star-formation
rate (SFR) and the interstellar medium (ISM) properties via [OII]/[CII] and
[OII]/\halpha luminosity ratios at $z\sim4.5$. The [OII]$-$SFR relation at
$z\sim4.5$ cannot be described using standard local descriptions, but is
consistent with a metal-dependent relation assuming metallicities around $50\%$
solar. To explain the measured dust-corrected luminosity ratios of
$L[OII]/L[CII] \sim 0.98^{+0.21}_{-0.22}$ and $L[OII]/LHa \sim
-0.22^{+0.13}_{-0.15}$ for our sample, ionization parameters $\log(U)< -2$ and
electron densities $\log(\rm n_e / {\rm [cm^{-3}]}) \sim 2.5-3$ are required.
The former is consistent with galaxies at $z\sim2-3$, however lower than at
$z>6$. The latter may be slightly higher than expected given the galaxies'
specific SFR. The analysis of this pilot sample suggests that typical log($
M/M_{\odot})$ > 9 galaxies at $z\sim4.5$ to have broadly similar ISM properties
as their descendants at $z\sim2$ and suggest a strong evolution of ISM
properties since the Epoch of Reionization at $z>6$.</description><identifier>DOI: 10.48550/arxiv.2201.03587</identifier><language>eng</language><subject>Physics - Astrophysics of Galaxies</subject><creationdate>2022-01</creationdate><rights>http://creativecommons.org/licenses/by/4.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,780,885</link.rule.ids><linktorsrc>$$Uhttps://arxiv.org/abs/2201.03587$$EView_record_in_Cornell_University$$FView_record_in_$$GCornell_University$$Hfree_for_read</linktorsrc><backlink>$$Uhttps://doi.org/10.48550/arXiv.2201.03587$$DView paper in arXiv$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.1093/mnras/stac071$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink></links><search><creatorcontrib>Vanderhoof, Brittany N</creatorcontrib><creatorcontrib>Faisst, A. L</creatorcontrib><creatorcontrib>Shen, L</creatorcontrib><creatorcontrib>Lemaux, B. C</creatorcontrib><creatorcontrib>Béthermin, M</creatorcontrib><creatorcontrib>Capak, P. L</creatorcontrib><creatorcontrib>Cassata, P</creatorcontrib><creatorcontrib>Fèvre, O. Le</creatorcontrib><creatorcontrib>Schaerer, D</creatorcontrib><creatorcontrib>Silverman, J</creatorcontrib><creatorcontrib>Yan, L</creatorcontrib><creatorcontrib>Boquien, M</creatorcontrib><creatorcontrib>Gal, R</creatorcontrib><creatorcontrib>Kartaltepe, J</creatorcontrib><creatorcontrib>Lubin, L. M</creatorcontrib><creatorcontrib>Dessauges-Zavadsky, M</creatorcontrib><creatorcontrib>Fudamoto, Y</creatorcontrib><creatorcontrib>Ginolfi, M</creatorcontrib><creatorcontrib>Hathi, N. P</creatorcontrib><creatorcontrib>Jones, G. C</creatorcontrib><creatorcontrib>Koekemoer, A. M</creatorcontrib><creatorcontrib>Narayanan, D</creatorcontrib><creatorcontrib>Romano, M</creatorcontrib><creatorcontrib>Talia, M</creatorcontrib><creatorcontrib>Vergani, D</creatorcontrib><creatorcontrib>Zamorani, G</creatorcontrib><title>The ALPINE-ALMA [CII] Survey: Investigation of 10 Galaxies at $z\sim4.5$ with [OII] and [CII] Line Emission $-$ ISM Properties and [OII]$-$SFR Relation</title><description>We present $10$ main-sequence ALPINE galaxies (log($M/M_{\odot}$) = 9.2-11.1
and ${\rm SFR}=23-190\,{\rm M_{\odot}\,yr^{-1}}$) at $z\sim4.5$ with optical
[OII] measurements from Keck/MOSFIRE spectroscopy and Subaru/MOIRCS narrow-band
imaging. This is the largest such multi-wavelength sample at these redshifts,
combining various measurements in the ultra-violet, optical, and far-infrared
including [CII]$_{158{\rm \mu m}}$ line emission and dust continuum from ALMA
and H$\alpha$ emission from Spitzer photometry. For the first time, this unique
sample allows us to analyze the relation between [OII] and total star-formation
rate (SFR) and the interstellar medium (ISM) properties via [OII]/[CII] and
[OII]/\halpha luminosity ratios at $z\sim4.5$. The [OII]$-$SFR relation at
$z\sim4.5$ cannot be described using standard local descriptions, but is
consistent with a metal-dependent relation assuming metallicities around $50\%$
solar. To explain the measured dust-corrected luminosity ratios of
$L[OII]/L[CII] \sim 0.98^{+0.21}_{-0.22}$ and $L[OII]/LHa \sim
-0.22^{+0.13}_{-0.15}$ for our sample, ionization parameters $\log(U)< -2$ and
electron densities $\log(\rm n_e / {\rm [cm^{-3}]}) \sim 2.5-3$ are required.
The former is consistent with galaxies at $z\sim2-3$, however lower than at
$z>6$. The latter may be slightly higher than expected given the galaxies'
specific SFR. The analysis of this pilot sample suggests that typical log($
M/M_{\odot})$ > 9 galaxies at $z\sim4.5$ to have broadly similar ISM properties
as their descendants at $z\sim2$ and suggest a strong evolution of ISM
properties since the Epoch of Reionization at $z>6$.</description><subject>Physics - Astrophysics of Galaxies</subject><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2022</creationdate><recordtype>article</recordtype><sourceid>GOX</sourceid><recordid>eNqFj7sKwkAQRbexEPUDrJwibeJGExS7IFEX4gNjFyUsuOpAHrK7xseP-Lu6wd5qinvPHQ4hXZc63tj3aZ_LB1bOYEBdhw798ahJ3ruLgCDasFVoB9EygGTK2AHim6zEcwKsqITSeOYaywLKE7gU5jzjDxQKuAbrtVeYe45vwR31BZK1oXlx_O1EWAgIc1TK8JZtAYuXsJHlVUhdb5iqgb5ZPNvCVmT1rzZpnHimROd3W6Q3C3fThV0rpFeJOZfP1Kiktcrwf-MD3j9Pqg</recordid><startdate>20220110</startdate><enddate>20220110</enddate><creator>Vanderhoof, Brittany N</creator><creator>Faisst, A. L</creator><creator>Shen, L</creator><creator>Lemaux, B. C</creator><creator>Béthermin, M</creator><creator>Capak, P. L</creator><creator>Cassata, P</creator><creator>Fèvre, O. Le</creator><creator>Schaerer, D</creator><creator>Silverman, J</creator><creator>Yan, L</creator><creator>Boquien, M</creator><creator>Gal, R</creator><creator>Kartaltepe, J</creator><creator>Lubin, L. M</creator><creator>Dessauges-Zavadsky, M</creator><creator>Fudamoto, Y</creator><creator>Ginolfi, M</creator><creator>Hathi, N. P</creator><creator>Jones, G. C</creator><creator>Koekemoer, A. M</creator><creator>Narayanan, D</creator><creator>Romano, M</creator><creator>Talia, M</creator><creator>Vergani, D</creator><creator>Zamorani, G</creator><scope>GOX</scope></search><sort><creationdate>20220110</creationdate><title>The ALPINE-ALMA [CII] Survey: Investigation of 10 Galaxies at $z\sim4.5$ with [OII] and [CII] Line Emission $-$ ISM Properties and [OII]$-$SFR Relation</title><author>Vanderhoof, Brittany N ; Faisst, A. L ; Shen, L ; Lemaux, B. C ; Béthermin, M ; Capak, P. L ; Cassata, P ; Fèvre, O. Le ; Schaerer, D ; Silverman, J ; Yan, L ; Boquien, M ; Gal, R ; Kartaltepe, J ; Lubin, L. M ; Dessauges-Zavadsky, M ; Fudamoto, Y ; Ginolfi, M ; Hathi, N. P ; Jones, G. C ; Koekemoer, A. M ; Narayanan, D ; Romano, M ; Talia, M ; Vergani, D ; Zamorani, G</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-arxiv_primary_2201_035873</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2022</creationdate><topic>Physics - Astrophysics of Galaxies</topic><toplevel>online_resources</toplevel><creatorcontrib>Vanderhoof, Brittany N</creatorcontrib><creatorcontrib>Faisst, A. L</creatorcontrib><creatorcontrib>Shen, L</creatorcontrib><creatorcontrib>Lemaux, B. C</creatorcontrib><creatorcontrib>Béthermin, M</creatorcontrib><creatorcontrib>Capak, P. L</creatorcontrib><creatorcontrib>Cassata, P</creatorcontrib><creatorcontrib>Fèvre, O. Le</creatorcontrib><creatorcontrib>Schaerer, D</creatorcontrib><creatorcontrib>Silverman, J</creatorcontrib><creatorcontrib>Yan, L</creatorcontrib><creatorcontrib>Boquien, M</creatorcontrib><creatorcontrib>Gal, R</creatorcontrib><creatorcontrib>Kartaltepe, J</creatorcontrib><creatorcontrib>Lubin, L. M</creatorcontrib><creatorcontrib>Dessauges-Zavadsky, M</creatorcontrib><creatorcontrib>Fudamoto, Y</creatorcontrib><creatorcontrib>Ginolfi, M</creatorcontrib><creatorcontrib>Hathi, N. P</creatorcontrib><creatorcontrib>Jones, G. C</creatorcontrib><creatorcontrib>Koekemoer, A. M</creatorcontrib><creatorcontrib>Narayanan, D</creatorcontrib><creatorcontrib>Romano, M</creatorcontrib><creatorcontrib>Talia, M</creatorcontrib><creatorcontrib>Vergani, D</creatorcontrib><creatorcontrib>Zamorani, G</creatorcontrib><collection>arXiv.org</collection></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Vanderhoof, Brittany N</au><au>Faisst, A. L</au><au>Shen, L</au><au>Lemaux, B. C</au><au>Béthermin, M</au><au>Capak, P. L</au><au>Cassata, P</au><au>Fèvre, O. Le</au><au>Schaerer, D</au><au>Silverman, J</au><au>Yan, L</au><au>Boquien, M</au><au>Gal, R</au><au>Kartaltepe, J</au><au>Lubin, L. M</au><au>Dessauges-Zavadsky, M</au><au>Fudamoto, Y</au><au>Ginolfi, M</au><au>Hathi, N. P</au><au>Jones, G. C</au><au>Koekemoer, A. M</au><au>Narayanan, D</au><au>Romano, M</au><au>Talia, M</au><au>Vergani, D</au><au>Zamorani, G</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>The ALPINE-ALMA [CII] Survey: Investigation of 10 Galaxies at $z\sim4.5$ with [OII] and [CII] Line Emission $-$ ISM Properties and [OII]$-$SFR Relation</atitle><date>2022-01-10</date><risdate>2022</risdate><abstract>We present $10$ main-sequence ALPINE galaxies (log($M/M_{\odot}$) = 9.2-11.1
and ${\rm SFR}=23-190\,{\rm M_{\odot}\,yr^{-1}}$) at $z\sim4.5$ with optical
[OII] measurements from Keck/MOSFIRE spectroscopy and Subaru/MOIRCS narrow-band
imaging. This is the largest such multi-wavelength sample at these redshifts,
combining various measurements in the ultra-violet, optical, and far-infrared
including [CII]$_{158{\rm \mu m}}$ line emission and dust continuum from ALMA
and H$\alpha$ emission from Spitzer photometry. For the first time, this unique
sample allows us to analyze the relation between [OII] and total star-formation
rate (SFR) and the interstellar medium (ISM) properties via [OII]/[CII] and
[OII]/\halpha luminosity ratios at $z\sim4.5$. The [OII]$-$SFR relation at
$z\sim4.5$ cannot be described using standard local descriptions, but is
consistent with a metal-dependent relation assuming metallicities around $50\%$
solar. To explain the measured dust-corrected luminosity ratios of
$L[OII]/L[CII] \sim 0.98^{+0.21}_{-0.22}$ and $L[OII]/LHa \sim
-0.22^{+0.13}_{-0.15}$ for our sample, ionization parameters $\log(U)< -2$ and
electron densities $\log(\rm n_e / {\rm [cm^{-3}]}) \sim 2.5-3$ are required.
The former is consistent with galaxies at $z\sim2-3$, however lower than at
$z>6$. The latter may be slightly higher than expected given the galaxies'
specific SFR. The analysis of this pilot sample suggests that typical log($
M/M_{\odot})$ > 9 galaxies at $z\sim4.5$ to have broadly similar ISM properties
as their descendants at $z\sim2$ and suggest a strong evolution of ISM
properties since the Epoch of Reionization at $z>6$.</abstract><doi>10.48550/arxiv.2201.03587</doi><oa>free_for_read</oa></addata></record> |
fulltext | fulltext_linktorsrc |
identifier | DOI: 10.48550/arxiv.2201.03587 |
ispartof | |
issn | |
language | eng |
recordid | cdi_arxiv_primary_2201_03587 |
source | arXiv.org |
subjects | Physics - Astrophysics of Galaxies |
title | The ALPINE-ALMA [CII] Survey: Investigation of 10 Galaxies at $z\sim4.5$ with [OII] and [CII] Line Emission $-$ ISM Properties and [OII]$-$SFR Relation |
url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2024-12-23T03%3A53%3A14IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-arxiv_GOX&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=The%20ALPINE-ALMA%20%5BCII%5D%20Survey:%20Investigation%20of%2010%20Galaxies%20at%20$z%5Csim4.5$%20with%20%5BOII%5D%20and%20%5BCII%5D%20Line%20Emission%20$-$%20ISM%20Properties%20and%20%5BOII%5D$-$SFR%20Relation&rft.au=Vanderhoof,%20Brittany%20N&rft.date=2022-01-10&rft_id=info:doi/10.48550/arxiv.2201.03587&rft_dat=%3Carxiv_GOX%3E2201_03587%3C/arxiv_GOX%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_id=info:pmid/&rfr_iscdi=true |