AustralieFrV1, Main, Exploration, bibRecord, 006384

Molecular gas in intermediate‐redshift ultraluminous infrared galaxies

Identifieur interne : 006384 ( Main/Exploration ); précédent : 006383; suivant : 006385

Molecular gas in intermediate‐redshift ultraluminous infrared galaxies

Auteurs : R. Braun [Australie] ; A. Popping [Australie] ; K. Brooks [Australie] ; F. Combes [France]

Source :

Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011-10-01.

RBID : ISTEX:3804D5C1F252FBB6695F96282351A68E2A9E15CC

Descripteurs français

Pascal (Inist)
- Corrélation, Déplacement vers le rouge, Fonction masse, Formation stellaire, Galaxies infrarouges, Gaz moléculaire, Luminosité, Molécule d'hydrogène, Petit Nuage Magellan, Taux formation.

English descriptors

Abstract

We report on the results of observations in the CO(1–0) transition of a complete sample of Southern, intermediate‐redshift (z= 0.2–0.5) ultraluminous infrared galaxies (ULIRGs) using the Mopra 22‐m telescope. The 11 ULIRGs with LFIR > 1012.5 L⊙ south of δ=−12° were observed with integration times that varied between 5 and 24 h. Four marginal detections were obtained for individual targets in the sample. The ‘stacked’ spectrum of the entire sample yields a high significance, 10σ detection of the CO(1–0) transition at an average redshift of z= 0.38. The tightest correlation of LFIR and LCO for published low‐redshift ULIRG samples (z < 0.2) is obtained after normalization of both these measures to a fixed dust temperature. With this normalization the relationship is linear. The distribution of dust‐to‐molecular hydrogen gas mass displays a systematic increase in dust‐to‐gas mass with galaxy luminosity for low‐redshift samples, but this ratio declines dramatically for intermediate‐redshift ULIRGs down to values comparable to that of the Small Magellanic Cloud. The upper envelope to the distribution of ULIRG molecular mass as function of look‐back time demonstrates a dramatic rise by almost an order of magnitude from the current epoch out to 5 Gyr. This increase in maximum ULIRG gas mass with look‐back time is even more rapid than that of the star formation rate density.

Url:

https://api.istex.fr/document/3804D5C1F252FBB6695F96282351A68E2A9E15CC/fulltext/pdf

DOI: 10.1111/j.1365-2966.2011.19212.x

Affiliations:

Le document en format XML

<record><TEI wicri:istexFullTextTei="biblStruct"><teiHeader><fileDesc><titleStmt><title xml:lang="en">Molecular gas in intermediate‐redshift ultraluminous infrared galaxies</title>
<author><name sortKey="Braun, R" sort="Braun, R" uniqKey="Braun R" first="R." last="Braun">R. Braun</name>
</author>
<author><name sortKey="Popping, A" sort="Popping, A" uniqKey="Popping A" first="A." last="Popping">A. Popping</name>
</author>
<author><name sortKey="Brooks, K" sort="Brooks, K" uniqKey="Brooks K" first="K." last="Brooks">K. Brooks</name>
</author>
<author><name sortKey="Combes, F" sort="Combes, F" uniqKey="Combes F" first="F." last="Combes">F. Combes</name>
</author>
</titleStmt>
<publicationStmt><idno type="wicri:source">ISTEX</idno>
<idno type="RBID">ISTEX:3804D5C1F252FBB6695F96282351A68E2A9E15CC</idno>
<date when="2011" year="2011">2011</date>
<idno type="doi">10.1111/j.1365-2966.2011.19212.x</idno>
<idno type="url">https://api.istex.fr/document/3804D5C1F252FBB6695F96282351A68E2A9E15CC/fulltext/pdf</idno>
<idno type="wicri:Area/Istex/Corpus">000A37</idno>
<idno type="wicri:explorRef" wicri:stream="Istex" wicri:step="Corpus" wicri:corpus="ISTEX">000A37</idno>
<idno type="wicri:Area/Istex/Curation">000A37</idno>
<idno type="wicri:Area/Istex/Checkpoint">000803</idno>
<idno type="wicri:explorRef" wicri:stream="Istex" wicri:step="Checkpoint">000803</idno>
<idno type="wicri:doubleKey">0035-8711:2011:Braun R:molecular:gas:in</idno>
<idno type="wicri:Area/Main/Merge">006760</idno>
<idno type="wicri:source">INIST</idno>
<idno type="RBID">Pascal:11-0424834</idno>
<idno type="wicri:Area/PascalFrancis/Corpus">001936</idno>
<idno type="wicri:Area/PascalFrancis/Curation">004620</idno>
<idno type="wicri:Area/PascalFrancis/Checkpoint">001888</idno>
<idno type="wicri:explorRef" wicri:stream="PascalFrancis" wicri:step="Checkpoint">001888</idno>
<idno type="wicri:doubleKey">0035-8711:2011:Braun R:molecular:gas:in</idno>
<idno type="wicri:Area/Main/Merge">006D39</idno>
<idno type="wicri:Area/Main/Curation">006384</idno>
<idno type="wicri:Area/Main/Exploration">006384</idno>
</publicationStmt>
<sourceDesc><biblStruct><analytic><title level="a" type="main">Molecular gas in intermediate‐redshift ultraluminous infrared galaxies</title>
<author><name sortKey="Braun, R" sort="Braun, R" uniqKey="Braun R" first="R." last="Braun">R. Braun</name>
<affiliation wicri:level="1"><country xml:lang="fr">Australie</country>
<wicri:regionArea>CSIRO Astronomy and Space Science, PO Box 76, Epping, NSW 1710</wicri:regionArea>
<wicri:noRegion>NSW 1710</wicri:noRegion>
</affiliation>
<affiliation wicri:level="1"><country wicri:rule="url">Australie</country>
</affiliation>
</author>
<author><name sortKey="Popping, A" sort="Popping, A" uniqKey="Popping A" first="A." last="Popping">A. Popping</name>
<affiliation wicri:level="1"><country xml:lang="fr">Australie</country>
<wicri:regionArea>CSIRO Astronomy and Space Science, PO Box 76, Epping, NSW 1710</wicri:regionArea>
<wicri:noRegion>NSW 1710</wicri:noRegion>
</affiliation>
<affiliation wicri:level="1"><country xml:lang="fr">Australie</country>
<wicri:regionArea>ICRAR, The University of Western Australia, Crawley, WA 6009</wicri:regionArea>
<wicri:noRegion>WA 6009</wicri:noRegion>
</affiliation>
</author>
<author><name sortKey="Brooks, K" sort="Brooks, K" uniqKey="Brooks K" first="K." last="Brooks">K. Brooks</name>
<affiliation wicri:level="1"><country xml:lang="fr">Australie</country>
<wicri:regionArea>CSIRO Astronomy and Space Science, PO Box 76, Epping, NSW 1710</wicri:regionArea>
<wicri:noRegion>NSW 1710</wicri:noRegion>
</affiliation>
</author>
<author><name sortKey="Combes, F" sort="Combes, F" uniqKey="Combes F" first="F." last="Combes">F. Combes</name>
<affiliation wicri:level="3"><country xml:lang="fr">France</country>
<wicri:regionArea>Observatoire de Paris, 61 Av. de l’Observatoire, 75014 Paris</wicri:regionArea>
<placeName><region type="region" nuts="2">Île-de-France</region>
<settlement type="city">Paris</settlement>
</placeName>
</affiliation>
</author>
</analytic>
<monogr></monogr>
<series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title>
<title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title>
<idno type="ISSN">0035-8711</idno>
<idno type="eISSN">1365-2966</idno>
<imprint><biblScope unit="vol">416</biblScope>
<biblScope unit="issue">4</biblScope>
<biblScope unit="page" from="2600">2600</biblScope>
<biblScope unit="page" to="2606">2606</biblScope>
<biblScope unit="page-count">7</biblScope>
<publisher>Blackwell Publishing Ltd</publisher>
<pubPlace>Oxford, UK</pubPlace>
<date type="published" when="2011-10-01">2011-10-01</date>
</imprint>
<idno type="ISSN">0035-8711</idno>
</series>
</biblStruct>
</sourceDesc>
<seriesStmt><idno type="ISSN">0035-8711</idno>
</seriesStmt>
</fileDesc>
<profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Antenna temperature</term>
<term>Australia telescope</term>
<term>Average redshift</term>
<term>Centre frequencies</term>
<term>Combes</term>
<term>Correlations</term>
<term>Csiro</term>
<term>Deep integrations</term>
<term>Dust mass</term>
<term>Dust temperature</term>
<term>Emission lines</term>
<term>Entire spectrum</term>
<term>Final spectra</term>
<term>Formation rate</term>
<term>Fourier spectrum</term>
<term>Galaxy</term>
<term>Gure</term>
<term>Hopkins beacom</term>
<term>Hydrogen mass</term>
<term>Hydrogen molecules</term>
<term>Individual targets</term>
<term>Infrared galaxies</term>
<term>Ira</term>
<term>Least squares</term>
<term>Lfir</term>
<term>Line luminosity</term>
<term>Line strength</term>
<term>Luminosity</term>
<term>Luminosity distance</term>
<term>Luminous galaxies</term>
<term>Luminous sources</term>
<term>Magellanic cloud</term>
<term>Magnitude decline</term>
<term>Marginal detections</term>
<term>Mass function</term>
<term>Mass ratio</term>
<term>Maximum ulirg</term>
<term>Mnras</term>
<term>Molecular gas</term>
<term>Molecular hydrogen mass</term>
<term>Molecular mass function</term>
<term>Monthly notices</term>
<term>Mopra radio telescope</term>
<term>Mopra telescope</term>
<term>National facility</term>
<term>Northern sample</term>
<term>Planck function</term>
<term>Red shift</term>
<term>Redshift</term>
<term>Reference spectra</term>
<term>Reference temperature</term>
<term>Sanders mirabel</term>
<term>Small Magellanic Cloud</term>
<term>Solomon</term>
<term>Spectral resolution</term>
<term>Star formation</term>
<term>Star formation rate density</term>
<term>Subsequent publication</term>
<term>Systemic velocity</term>
<term>Target galaxies</term>
<term>Target galaxy</term>
<term>Time evolution</term>
<term>Uctuation level</term>
<term>Ulirg</term>
<term>Ulirgs</term>
<term>Upper envelope</term>
<term>Upper limits</term>
</keywords>
<keywords scheme="Pascal" xml:lang="fr"><term>Corrélation</term>
<term>Déplacement vers le rouge</term>
<term>Fonction masse</term>
<term>Formation stellaire</term>
<term>Galaxies infrarouges</term>
<term>Gaz moléculaire</term>
<term>Luminosité</term>
<term>Molécule d'hydrogène</term>
<term>Petit Nuage Magellan</term>
<term>Taux formation</term>
</keywords>
<keywords scheme="Teeft" xml:lang="en"><term>Antenna temperature</term>
<term>Australia telescope</term>
<term>Average redshift</term>
<term>Centre frequencies</term>
<term>Combes</term>
<term>Csiro</term>
<term>Deep integrations</term>
<term>Dust mass</term>
<term>Dust temperature</term>
<term>Emission lines</term>
<term>Entire spectrum</term>
<term>Final spectra</term>
<term>Fourier spectrum</term>
<term>Galaxy</term>
<term>Gure</term>
<term>Hopkins beacom</term>
<term>Hydrogen mass</term>
<term>Individual targets</term>
<term>Ira</term>
<term>Least squares</term>
<term>Lfir</term>
<term>Line luminosity</term>
<term>Line strength</term>
<term>Luminosity</term>
<term>Luminosity distance</term>
<term>Luminous galaxies</term>
<term>Luminous sources</term>
<term>Magellanic cloud</term>
<term>Magnitude decline</term>
<term>Marginal detections</term>
<term>Mass ratio</term>
<term>Maximum ulirg</term>
<term>Mnras</term>
<term>Molecular hydrogen mass</term>
<term>Molecular mass function</term>
<term>Monthly notices</term>
<term>Mopra radio telescope</term>
<term>Mopra telescope</term>
<term>National facility</term>
<term>Northern sample</term>
<term>Planck function</term>
<term>Redshift</term>
<term>Reference spectra</term>
<term>Reference temperature</term>
<term>Sanders mirabel</term>
<term>Solomon</term>
<term>Spectral resolution</term>
<term>Star formation</term>
<term>Star formation rate density</term>
<term>Subsequent publication</term>
<term>Systemic velocity</term>
<term>Target galaxies</term>
<term>Target galaxy</term>
<term>Time evolution</term>
<term>Uctuation level</term>
<term>Ulirg</term>
<term>Ulirgs</term>
<term>Upper envelope</term>
<term>Upper limits</term>
</keywords>
</textClass>
</profileDesc>
</teiHeader>
<front><div type="abstract" xml:lang="en">We report on the results of observations in the CO(1–0) transition of a complete sample of Southern, intermediate‐redshift (z= 0.2–0.5) ultraluminous infrared galaxies (ULIRGs) using the Mopra 22‐m telescope. The 11 ULIRGs with LFIR > 1012.5 L⊙ south of δ=−12° were observed with integration times that varied between 5 and 24 h. Four marginal detections were obtained for individual targets in the sample. The ‘stacked’ spectrum of the entire sample yields a high significance, 10σ detection of the CO(1–0) transition at an average redshift of z= 0.38. The tightest correlation of LFIR and LCO for published low‐redshift ULIRG samples (z < 0.2) is obtained after normalization of both these measures to a fixed dust temperature. With this normalization the relationship is linear. The distribution of dust‐to‐molecular hydrogen gas mass displays a systematic increase in dust‐to‐gas mass with galaxy luminosity for low‐redshift samples, but this ratio declines dramatically for intermediate‐redshift ULIRGs down to values comparable to that of the Small Magellanic Cloud. The upper envelope to the distribution of ULIRG molecular mass as function of look‐back time demonstrates a dramatic rise by almost an order of magnitude from the current epoch out to 5 Gyr. This increase in maximum ULIRG gas mass with look‐back time is even more rapid than that of the star formation rate density.</div>
</front>
</TEI>
<affiliations><list><country><li>Australie</li>
<li>France</li>
</country>
<region><li>Île-de-France</li>
</region>
<settlement><li>Paris</li>
</settlement>
</list>
<tree><country name="Australie"><noRegion><name sortKey="Braun, R" sort="Braun, R" uniqKey="Braun R" first="R." last="Braun">R. Braun</name>
</noRegion>
<name sortKey="Braun, R" sort="Braun, R" uniqKey="Braun R" first="R." last="Braun">R. Braun</name>
<name sortKey="Brooks, K" sort="Brooks, K" uniqKey="Brooks K" first="K." last="Brooks">K. Brooks</name>
<name sortKey="Popping, A" sort="Popping, A" uniqKey="Popping A" first="A." last="Popping">A. Popping</name>
<name sortKey="Popping, A" sort="Popping, A" uniqKey="Popping A" first="A." last="Popping">A. Popping</name>
</country>
<country name="France"><region name="Île-de-France"><name sortKey="Combes, F" sort="Combes, F" uniqKey="Combes F" first="F." last="Combes">F. Combes</name>
</region>
</country>
</tree>
</affiliations>
</record>

Pour manipuler ce document sous Unix (Dilib)

EXPLOR_STEP=$WICRI_ROOT/Wicri/Asie/explor/AustralieFrV1/Data/Main/Exploration

HfdSelect -h $EXPLOR_STEP/biblio.hfd -nk 006384 | SxmlIndent | more

HfdSelect -h $EXPLOR_AREA/Data/Main/Exploration/biblio.hfd -nk 006384 | SxmlIndent | more

Pour mettre un lien sur cette page dans le réseau Wicri

{{Explor lien
   |wiki=    Wicri/Asie
   |area=    AustralieFrV1
   |flux=    Main
   |étape=   Exploration
   |type=    RBID
   |clé=     ISTEX:3804D5C1F252FBB6695F96282351A68E2A9E15CC
   |texte=   Molecular gas in intermediate‐redshift ultraluminous infrared galaxies
}}

This area was generated with Dilib version V0.6.33.
Data generation: Tue Dec 5 10:43:12 2017. Site generation: Tue Mar 5 14:07:20 2024

Serveur d'exploration sur les relations entre la France et l'Australie

Molecular gas in intermediate‐redshift ultraluminous infrared galaxies

Molecular gas in intermediate‐redshift ultraluminous infrared galaxies

Source :

Descripteurs français

English descriptors

Abstract

Links toward previous steps (curation, corpus...)

Le document en format XML

Pour manipuler ce document sous Unix (Dilib)

Pour mettre un lien sur cette page dans le réseau Wicri

	Serveur d'exploration sur les relations entre la France et l'Australie
	Attention, ce site est en cours de développement ! Attention, site généré par des moyens informatiques à partir de corpus bruts. Les informations ne sont donc pas validées.