AustralieFrV1, PascalFrancis, Corpus, bibRecord, 000F12

OBSERVATIONAL LIMITS ON THE GAS MASS OF A z = 4.9 GALAXY

Identifieur interne : 000F12 ( PascalFrancis/Corpus ); précédent : 000F11; suivant : 000F13

OBSERVATIONAL LIMITS ON THE GAS MASS OF A z = 4.9 GALAXY

Auteurs : R. C. Livermore ; A. M. Swinbank ; Ian Smail ; R. G. Bower ; K. E. K. Coppin ; R. A. Crain ; A. C. Edge ; J. E. Geach ; J. Richard

Source :

The Astrophysical journal [ 0004-637X ] ; 2012.

RBID : Pascal:12-0421291

Descripteurs français

Pascal (Inist)
- Galaxies, Gaz moléculaire, Mirage gravitationnel, Position, Déplacement vers le rouge, Observatoire spatial, Spectrométrie, Luminosité, Formation galaxies, Formation stellaire.

English descriptors

KwdEn :
- Galaxies, Galaxy formation, Gravitational lensing, Luminosity, Molecular gas, Positions, Red shift, Spatial observatory, Spectroscopy, Star formation.

Abstract

We present the results of a search for molecular gas emission from a star-forming galaxy at z = 4.9. The galaxy benefits from magnification of 22 ± 5x due to strong gravitational lensing by the foreground cluster MS 1358+62. We target the CO(5-4) emission at a known position and redshift from existing Hubble Space Telescope/Advanced Camera for Surveys imaging and Gemini/NIFS [O II]3727 imaging spectroscopy, and obtain a tentative detection at the 4.3σ level with a flux of 0. 104 ± 0.024 Jy km s^-1. From the CO line luminosity and assuming a CO-to-H₂ conversion factor α = 2, we derive a gas mass M_gas∼ 1⁺¹_-0.6 × 10⁹ M_◦.. Combined with the existing data, we derive a gas fraction M_gas/(M_gas + M_*) = 0.59^+0.11_-0.06. The faint line flux of this galaxy highlights the difficulty of observing molecular gas in representative galaxies at this epoch, and suggests that routine detections of similar galaxies in the absence of gravitational lensing will remain challenging even with ALMA in full science operations.

Notice en format standard (ISO 2709)

Pour connaître la documentation sur le format Inist Standard.

A01	`01`	`1`		`@0 0004-637X`
A02	`01`			`@0 ASJOAB`
A03		`1`		`@0 Astrophys. j.`
A05				`@2 758`
A06				`@2 2 @3 p. 2`
A08	`01`	`1`	`ENG`	`@1 OBSERVATIONAL LIMITS ON THE GAS MASS OF A z = 4.9 GALAXY`
A11	`01`	`1`		`@1 LIVERMORE (R. C.)`
A11	`02`	`1`		`@1 SWINBANK (A. M.)`
A11	`03`	`1`		`@1 SMAIL (Ian)`
A11	`04`	`1`		`@1 BOWER (R. G.)`
A11	`05`	`1`		`@1 COPPIN (K. E. K.)`
A11	`06`	`1`		`@1 CRAIN (R. A.)`
A11	`07`	`1`		`@1 EDGE (A. C.)`
A11	`08`	`1`		`@1 GEACH (J. E.)`
A11	`09`	`1`		`@1 RICHARD (J.)`
A14	`01`			`@1 Institute for Computational Cosmology, Durham University, South Road @2 Durham DH1 3LE @3 GBR @Z 1 aut. @Z 2 aut. @Z 3 aut. @Z 4 aut. @Z 5 aut. @Z 7 aut. @Z 8 aut. @Z 9 aut.`
A14	`02`			`@1 Department of Physics, McGill University, 3600 me University @2 Montréal, QC H3A 2T8 @3 CAN @Z 5 aut. @Z 8 aut.`
A14	`03`			`@1 Centre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218 @2 Hawthorn, Victoria 3122 @3 AUS @Z 6 aut.`
A14	`04`			`@1 Leiden Observatory, Leiden University, PO Box 9513 @2 2300 RA Leiden @3 NLD @Z 6 aut.`
A14	`05`			`@1 CRAL, Observatoire de Lyon, 9 Avenue Charles André @2 69561 Saint-Genis-Laval @3 FRA @Z 9 aut.`
A20				`@2 L35.1-L35.5`
A21				`@1 2012`
A23	`01`			`@0 ENG`
A43	`01`			`@1 INIST @2 512 @5 354000505368390110`
A44				`@0 0000 @1 © 2012 INIST-CNRS. All rights reserved.`
A45				`@0 1/4 p.`
A47	`01`	`1`		`@0 12-0421291`
A60				`@1 P`
A61				`@0 A`
A64	`01`	`1`		`@0 The Astrophysical journal`
A66	`01`			`@0 GBR`
C01	`01`		`ENG`	@0 We present the results of a search for molecular gas emission from a star-forming galaxy at z = 4.9. The galaxy benefits from magnification of 22 ± 5x due to strong gravitational lensing by the foreground cluster MS 1358+62. We target the CO(5-4) emission at a known position and redshift from existing Hubble Space Telescope/Advanced Camera for Surveys imaging and Gemini/NIFS [O II]3727 imaging spectroscopy, and obtain a tentative detection at the 4.3σ level with a flux of 0. 104 ± 0.024 Jy km s^-1. From the CO line luminosity and assuming a CO-to-H₂ conversion factor α = 2, we derive a gas mass M_gas∼ 1⁺¹_-0.6 × 10⁹ M_◦.. Combined with the existing data, we derive a gas fraction M_gas/(M_gas + M_*) = 0.59^+0.11_-0.06. The faint line flux of this galaxy highlights the difficulty of observing molecular gas in representative galaxies at this epoch, and suggests that routine detections of similar galaxies in the absence of gravitational lensing will remain challenging even with ALMA in full science operations.
C02	`01`	`3`		`@0 001E03`
C03	`01`	`3`	`FRE`	`@0 Galaxies @5 26`
C03	`01`	`3`	`ENG`	`@0 Galaxies @5 26`
C03	`02`	`X`	`FRE`	`@0 Gaz moléculaire @5 27`
C03	`02`	`X`	`ENG`	`@0 Molecular gas @5 27`
C03	`02`	`X`	`SPA`	`@0 Gas molecular @5 27`
C03	`03`	`X`	`FRE`	`@0 Mirage gravitationnel @5 28`
C03	`03`	`X`	`ENG`	`@0 Gravitational lensing @5 28`
C03	`03`	`X`	`SPA`	`@0 Espejismo gravitacional @5 28`
C03	`04`	`3`	`FRE`	`@0 Position @5 29`
C03	`04`	`3`	`ENG`	`@0 Positions @5 29`
C03	`05`	`3`	`FRE`	`@0 Déplacement vers le rouge @5 30`
C03	`05`	`3`	`ENG`	`@0 Red shift @5 30`
C03	`06`	`X`	`FRE`	`@0 Observatoire spatial @5 31`
C03	`06`	`X`	`ENG`	`@0 Spatial observatory @5 31`
C03	`06`	`X`	`SPA`	`@0 Observatorio espacial @5 31`
C03	`07`	`3`	`FRE`	`@0 Spectrométrie @5 32`
C03	`07`	`3`	`ENG`	`@0 Spectroscopy @5 32`
C03	`08`	`3`	`FRE`	`@0 Luminosité @5 33`
C03	`08`	`3`	`ENG`	`@0 Luminosity @5 33`
C03	`09`	`3`	`FRE`	`@0 Formation galaxies @5 34`
C03	`09`	`3`	`ENG`	`@0 Galaxy formation @5 34`
C03	`10`	`3`	`FRE`	`@0 Formation stellaire @5 35`
C03	`10`	`3`	`ENG`	`@0 Star formation @5 35`
N21				`@1 331`
N44	`01`			`@1 OTO`
N82				`@1 OTO`

Format Inist (serveur)

NO :	PASCAL 12-0421291 INIST
ET :	OBSERVATIONAL LIMITS ON THE GAS MASS OF A z = 4.9 GALAXY
AU :	LIVERMORE (R. C.); SWINBANK (A. M.); SMAIL (Ian); BOWER (R. G.); COPPIN (K. E. K.); CRAIN (R. A.); EDGE (A. C.); GEACH (J. E.); RICHARD (J.)
AF :	Institute for Computational Cosmology, Durham University, South Road/Durham DH1 3LE/Royaume-Uni (1 aut., 2 aut., 3 aut., 4 aut., 5 aut., 7 aut., 8 aut., 9 aut.); Department of Physics, McGill University, 3600 me University/Montréal, QC H3A 2T8/Canada (5 aut., 8 aut.); Centre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218/Hawthorn, Victoria 3122/Australie (6 aut.); Leiden Observatory, Leiden University, PO Box 9513/2300 RA Leiden/Pays-Bas (6 aut.); CRAL, Observatoire de Lyon, 9 Avenue Charles André/69561 Saint-Genis-Laval/France (9 aut.)
DT :	Publication en série; Niveau analytique
SO :	The Astrophysical journal; ISSN 0004-637X; Coden ASJOAB; Royaume-Uni; Da. 2012; Vol. 758; No. 2 p. 2; L35.1-L35.5; Bibl. 1/4 p.
LA :	Anglais
EA :	We present the results of a search for molecular gas emission from a star-forming galaxy at z = 4.9. The galaxy benefits from magnification of 22 ± 5x due to strong gravitational lensing by the foreground cluster MS 1358+62. We target the CO(5-4) emission at a known position and redshift from existing Hubble Space Telescope/Advanced Camera for Surveys imaging and Gemini/NIFS [O II]3727 imaging spectroscopy, and obtain a tentative detection at the 4.3σ level with a flux of 0. 104 ± 0.024 Jy km s^-1. From the CO line luminosity and assuming a CO-to-H₂ conversion factor α = 2, we derive a gas mass M_gas∼ 1⁺¹_-0.6 × 10⁹ M_◦.. Combined with the existing data, we derive a gas fraction M_gas/(M_gas + M_*) = 0.59^+0.11_-0.06. The faint line flux of this galaxy highlights the difficulty of observing molecular gas in representative galaxies at this epoch, and suggests that routine detections of similar galaxies in the absence of gravitational lensing will remain challenging even with ALMA in full science operations.
CC :	001E03
FD :	Galaxies; Gaz moléculaire; Mirage gravitationnel; Position; Déplacement vers le rouge; Observatoire spatial; Spectrométrie; Luminosité; Formation galaxies; Formation stellaire
ED :	Galaxies; Molecular gas; Gravitational lensing; Positions; Red shift; Spatial observatory; Spectroscopy; Luminosity; Galaxy formation; Star formation
SD :	Gas molecular; Espejismo gravitacional; Observatorio espacial
LO :	INIST-512.354000505368390110
ID :	12-0421291

Links to Exploration step

Pascal:12-0421291

Le document en format XML

<record><TEI><teiHeader><fileDesc><titleStmt><title xml:lang="en" level="a">OBSERVATIONAL LIMITS ON THE GAS MASS OF A z = 4.9 GALAXY</title>
<author><name sortKey="Livermore, R C" sort="Livermore, R C" uniqKey="Livermore R" first="R. C." last="Livermore">R. C. Livermore</name>
<affiliation><inist:fA14 i1="01"><s1>Institute for Computational Cosmology, Durham University, South Road</s1>
<s2>Durham DH1 3LE</s2>
<s3>GBR</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>7 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>9 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Swinbank, A M" sort="Swinbank, A M" uniqKey="Swinbank A" first="A. M." last="Swinbank">A. M. Swinbank</name>
<affiliation><inist:fA14 i1="01"><s1>Institute for Computational Cosmology, Durham University, South Road</s1>
<s2>Durham DH1 3LE</s2>
<s3>GBR</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>7 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>9 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Smail, Ian" sort="Smail, Ian" uniqKey="Smail I" first="Ian" last="Smail">Ian Smail</name>
<affiliation><inist:fA14 i1="01"><s1>Institute for Computational Cosmology, Durham University, South Road</s1>
<s2>Durham DH1 3LE</s2>
<s3>GBR</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>7 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>9 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Bower, R G" sort="Bower, R G" uniqKey="Bower R" first="R. G." last="Bower">R. G. Bower</name>
<affiliation><inist:fA14 i1="01"><s1>Institute for Computational Cosmology, Durham University, South Road</s1>
<s2>Durham DH1 3LE</s2>
<s3>GBR</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>7 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>9 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Coppin, K E K" sort="Coppin, K E K" uniqKey="Coppin K" first="K. E. K." last="Coppin">K. E. K. Coppin</name>
<affiliation><inist:fA14 i1="01"><s1>Institute for Computational Cosmology, Durham University, South Road</s1>
<s2>Durham DH1 3LE</s2>
<s3>GBR</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>7 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>9 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="02"><s1>Department of Physics, McGill University, 3600 me University</s1>
<s2>Montréal, QC H3A 2T8</s2>
<s3>CAN</s3>
<sZ>5 aut.</sZ>
<sZ>8 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Crain, R A" sort="Crain, R A" uniqKey="Crain R" first="R. A." last="Crain">R. A. Crain</name>
<affiliation><inist:fA14 i1="03"><s1>Centre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218</s1>
<s2>Hawthorn, Victoria 3122</s2>
<s3>AUS</s3>
<sZ>6 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="04"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1>
<s2>2300 RA Leiden</s2>
<s3>NLD</s3>
<sZ>6 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Edge, A C" sort="Edge, A C" uniqKey="Edge A" first="A. C." last="Edge">A. C. Edge</name>
<affiliation><inist:fA14 i1="01"><s1>Institute for Computational Cosmology, Durham University, South Road</s1>
<s2>Durham DH1 3LE</s2>
<s3>GBR</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>7 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>9 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Geach, J E" sort="Geach, J E" uniqKey="Geach J" first="J. E." last="Geach">J. E. Geach</name>
<affiliation><inist:fA14 i1="01"><s1>Institute for Computational Cosmology, Durham University, South Road</s1>
<s2>Durham DH1 3LE</s2>
<s3>GBR</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>7 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>9 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="02"><s1>Department of Physics, McGill University, 3600 me University</s1>
<s2>Montréal, QC H3A 2T8</s2>
<s3>CAN</s3>
<sZ>5 aut.</sZ>
<sZ>8 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Richard, J" sort="Richard, J" uniqKey="Richard J" first="J." last="Richard">J. Richard</name>
<affiliation><inist:fA14 i1="01"><s1>Institute for Computational Cosmology, Durham University, South Road</s1>
<s2>Durham DH1 3LE</s2>
<s3>GBR</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>7 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>9 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="05"><s1>CRAL, Observatoire de Lyon, 9 Avenue Charles André</s1>
<s2>69561 Saint-Genis-Laval</s2>
<s3>FRA</s3>
<sZ>9 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
</titleStmt>
<publicationStmt><idno type="wicri:source">INIST</idno>
<idno type="inist">12-0421291</idno>
<date when="2012">2012</date>
<idno type="stanalyst">PASCAL 12-0421291 INIST</idno>
<idno type="RBID">Pascal:12-0421291</idno>
<idno type="wicri:Area/PascalFrancis/Corpus">000F12</idno>
</publicationStmt>
<sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">OBSERVATIONAL LIMITS ON THE GAS MASS OF A z = 4.9 GALAXY</title>
<author><name sortKey="Livermore, R C" sort="Livermore, R C" uniqKey="Livermore R" first="R. C." last="Livermore">R. C. Livermore</name>
<affiliation><inist:fA14 i1="01"><s1>Institute for Computational Cosmology, Durham University, South Road</s1>
<s2>Durham DH1 3LE</s2>
<s3>GBR</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>7 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>9 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Swinbank, A M" sort="Swinbank, A M" uniqKey="Swinbank A" first="A. M." last="Swinbank">A. M. Swinbank</name>
<affiliation><inist:fA14 i1="01"><s1>Institute for Computational Cosmology, Durham University, South Road</s1>
<s2>Durham DH1 3LE</s2>
<s3>GBR</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>7 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>9 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Smail, Ian" sort="Smail, Ian" uniqKey="Smail I" first="Ian" last="Smail">Ian Smail</name>
<affiliation><inist:fA14 i1="01"><s1>Institute for Computational Cosmology, Durham University, South Road</s1>
<s2>Durham DH1 3LE</s2>
<s3>GBR</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>7 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>9 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Bower, R G" sort="Bower, R G" uniqKey="Bower R" first="R. G." last="Bower">R. G. Bower</name>
<affiliation><inist:fA14 i1="01"><s1>Institute for Computational Cosmology, Durham University, South Road</s1>
<s2>Durham DH1 3LE</s2>
<s3>GBR</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>7 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>9 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Coppin, K E K" sort="Coppin, K E K" uniqKey="Coppin K" first="K. E. K." last="Coppin">K. E. K. Coppin</name>
<affiliation><inist:fA14 i1="01"><s1>Institute for Computational Cosmology, Durham University, South Road</s1>
<s2>Durham DH1 3LE</s2>
<s3>GBR</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>7 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>9 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="02"><s1>Department of Physics, McGill University, 3600 me University</s1>
<s2>Montréal, QC H3A 2T8</s2>
<s3>CAN</s3>
<sZ>5 aut.</sZ>
<sZ>8 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Crain, R A" sort="Crain, R A" uniqKey="Crain R" first="R. A." last="Crain">R. A. Crain</name>
<affiliation><inist:fA14 i1="03"><s1>Centre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218</s1>
<s2>Hawthorn, Victoria 3122</s2>
<s3>AUS</s3>
<sZ>6 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="04"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1>
<s2>2300 RA Leiden</s2>
<s3>NLD</s3>
<sZ>6 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Edge, A C" sort="Edge, A C" uniqKey="Edge A" first="A. C." last="Edge">A. C. Edge</name>
<affiliation><inist:fA14 i1="01"><s1>Institute for Computational Cosmology, Durham University, South Road</s1>
<s2>Durham DH1 3LE</s2>
<s3>GBR</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>7 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>9 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Geach, J E" sort="Geach, J E" uniqKey="Geach J" first="J. E." last="Geach">J. E. Geach</name>
<affiliation><inist:fA14 i1="01"><s1>Institute for Computational Cosmology, Durham University, South Road</s1>
<s2>Durham DH1 3LE</s2>
<s3>GBR</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>7 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>9 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="02"><s1>Department of Physics, McGill University, 3600 me University</s1>
<s2>Montréal, QC H3A 2T8</s2>
<s3>CAN</s3>
<sZ>5 aut.</sZ>
<sZ>8 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Richard, J" sort="Richard, J" uniqKey="Richard J" first="J." last="Richard">J. Richard</name>
<affiliation><inist:fA14 i1="01"><s1>Institute for Computational Cosmology, Durham University, South Road</s1>
<s2>Durham DH1 3LE</s2>
<s3>GBR</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>7 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>9 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="05"><s1>CRAL, Observatoire de Lyon, 9 Avenue Charles André</s1>
<s2>69561 Saint-Genis-Laval</s2>
<s3>FRA</s3>
<sZ>9 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
</analytic>
<series><title level="j" type="main">The Astrophysical journal</title>
<title level="j" type="abbreviated">Astrophys. j.</title>
<idno type="ISSN">0004-637X</idno>
<imprint><date when="2012">2012</date>
</imprint>
</series>
</biblStruct>
</sourceDesc>
<seriesStmt><title level="j" type="main">The Astrophysical journal</title>
<title level="j" type="abbreviated">Astrophys. j.</title>
<idno type="ISSN">0004-637X</idno>
</seriesStmt>
</fileDesc>
<profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Galaxies</term>
<term>Galaxy formation</term>
<term>Gravitational lensing</term>
<term>Luminosity</term>
<term>Molecular gas</term>
<term>Positions</term>
<term>Red shift</term>
<term>Spatial observatory</term>
<term>Spectroscopy</term>
<term>Star formation</term>
</keywords>
<keywords scheme="Pascal" xml:lang="fr"><term>Galaxies</term>
<term>Gaz moléculaire</term>
<term>Mirage gravitationnel</term>
<term>Position</term>
<term>Déplacement vers le rouge</term>
<term>Observatoire spatial</term>
<term>Spectrométrie</term>
<term>Luminosité</term>
<term>Formation galaxies</term>
<term>Formation stellaire</term>
</keywords>
</textClass>
</profileDesc>
</teiHeader>
<front><div type="abstract" xml:lang="en">We present the results of a search for molecular gas emission from a star-forming galaxy at z = 4.9. The galaxy benefits from magnification of 22 ± 5x due to strong gravitational lensing by the foreground cluster MS 1358+62. We target the CO(5-4) emission at a known position and redshift from existing Hubble Space Telescope/Advanced Camera for Surveys imaging and Gemini/NIFS [O II]3727 imaging spectroscopy, and obtain a tentative detection at the 4.3σ level with a flux of 0. 104 ± 0.024 Jy km s<sup>-1</sup>
. From the CO line luminosity and assuming a CO-to-H<sub>2</sub>
 conversion factor α = 2, we derive a gas mass M<sub>gas </sub>
∼ 1<sup>+1</sup>
<sub>-0.6</sub>
 × 10<sup>9</sup>
 M<sub>◦.</sub>
. Combined with the existing data, we derive a gas fraction M<sub>gas</sub>
/(M<sub>gas</sub>
 + M<sub>*</sub>
) = 0.59<sup>+0.11</sup>
<sub>-0.06</sub>
. The faint line flux of this galaxy highlights the difficulty of observing molecular gas in representative galaxies at this epoch, and suggests that routine detections of similar galaxies in the absence of gravitational lensing will remain challenging even with ALMA in full science operations.</div>
</front>
</TEI>
<inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0004-637X</s0>
</fA01>
<fA02 i1="01"><s0>ASJOAB</s0>
</fA02>
<fA03 i2="1"><s0>Astrophys. j.</s0>
</fA03>
<fA05><s2>758</s2>
</fA05>
<fA06><s2>2</s2>
<s3>p. 2</s3>
</fA06>
<fA08 i1="01" i2="1" l="ENG"><s1>OBSERVATIONAL LIMITS ON THE GAS MASS OF A z = 4.9 GALAXY</s1>
</fA08>
<fA11 i1="01" i2="1"><s1>LIVERMORE (R. C.)</s1>
</fA11>
<fA11 i1="02" i2="1"><s1>SWINBANK (A. M.)</s1>
</fA11>
<fA11 i1="03" i2="1"><s1>SMAIL (Ian)</s1>
</fA11>
<fA11 i1="04" i2="1"><s1>BOWER (R. G.)</s1>
</fA11>
<fA11 i1="05" i2="1"><s1>COPPIN (K. E. K.)</s1>
</fA11>
<fA11 i1="06" i2="1"><s1>CRAIN (R. A.)</s1>
</fA11>
<fA11 i1="07" i2="1"><s1>EDGE (A. C.)</s1>
</fA11>
<fA11 i1="08" i2="1"><s1>GEACH (J. E.)</s1>
</fA11>
<fA11 i1="09" i2="1"><s1>RICHARD (J.)</s1>
</fA11>
<fA14 i1="01"><s1>Institute for Computational Cosmology, Durham University, South Road</s1>
<s2>Durham DH1 3LE</s2>
<s3>GBR</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>7 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>9 aut.</sZ>
</fA14>
<fA14 i1="02"><s1>Department of Physics, McGill University, 3600 me University</s1>
<s2>Montréal, QC H3A 2T8</s2>
<s3>CAN</s3>
<sZ>5 aut.</sZ>
<sZ>8 aut.</sZ>
</fA14>
<fA14 i1="03"><s1>Centre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218</s1>
<s2>Hawthorn, Victoria 3122</s2>
<s3>AUS</s3>
<sZ>6 aut.</sZ>
</fA14>
<fA14 i1="04"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1>
<s2>2300 RA Leiden</s2>
<s3>NLD</s3>
<sZ>6 aut.</sZ>
</fA14>
<fA14 i1="05"><s1>CRAL, Observatoire de Lyon, 9 Avenue Charles André</s1>
<s2>69561 Saint-Genis-Laval</s2>
<s3>FRA</s3>
<sZ>9 aut.</sZ>
</fA14>
<fA20><s2>L35.1-L35.5</s2>
</fA20>
<fA21><s1>2012</s1>
</fA21>
<fA23 i1="01"><s0>ENG</s0>
</fA23>
<fA43 i1="01"><s1>INIST</s1>
<s2>512</s2>
<s5>354000505368390110</s5>
</fA43>
<fA44><s0>0000</s0>
<s1>© 2012 INIST-CNRS. All rights reserved.</s1>
</fA44>
<fA45><s0>1/4 p.</s0>
</fA45>
<fA47 i1="01" i2="1"><s0>12-0421291</s0>
</fA47>
<fA60><s1>P</s1>
</fA60>
<fA61><s0>A</s0>
</fA61>
<fA64 i1="01" i2="1"><s0>The Astrophysical journal</s0>
</fA64>
<fA66 i1="01"><s0>GBR</s0>
</fA66>
<fC01 i1="01" l="ENG"><s0>We present the results of a search for molecular gas emission from a star-forming galaxy at z = 4.9. The galaxy benefits from magnification of 22 ± 5x due to strong gravitational lensing by the foreground cluster MS 1358+62. We target the CO(5-4) emission at a known position and redshift from existing Hubble Space Telescope/Advanced Camera for Surveys imaging and Gemini/NIFS [O II]3727 imaging spectroscopy, and obtain a tentative detection at the 4.3σ level with a flux of 0. 104 ± 0.024 Jy km s<sup>-1</sup>
. From the CO line luminosity and assuming a CO-to-H<sub>2</sub>
 conversion factor α = 2, we derive a gas mass M<sub>gas </sub>
∼ 1<sup>+1</sup>
<sub>-0.6</sub>
 × 10<sup>9</sup>
 M<sub>◦.</sub>
. Combined with the existing data, we derive a gas fraction M<sub>gas</sub>
/(M<sub>gas</sub>
 + M<sub>*</sub>
) = 0.59<sup>+0.11</sup>
<sub>-0.06</sub>
. The faint line flux of this galaxy highlights the difficulty of observing molecular gas in representative galaxies at this epoch, and suggests that routine detections of similar galaxies in the absence of gravitational lensing will remain challenging even with ALMA in full science operations.</s0>
</fC01>
<fC02 i1="01" i2="3"><s0>001E03</s0>
</fC02>
<fC03 i1="01" i2="3" l="FRE"><s0>Galaxies</s0>
<s5>26</s5>
</fC03>
<fC03 i1="01" i2="3" l="ENG"><s0>Galaxies</s0>
<s5>26</s5>
</fC03>
<fC03 i1="02" i2="X" l="FRE"><s0>Gaz moléculaire</s0>
<s5>27</s5>
</fC03>
<fC03 i1="02" i2="X" l="ENG"><s0>Molecular gas</s0>
<s5>27</s5>
</fC03>
<fC03 i1="02" i2="X" l="SPA"><s0>Gas molecular</s0>
<s5>27</s5>
</fC03>
<fC03 i1="03" i2="X" l="FRE"><s0>Mirage gravitationnel</s0>
<s5>28</s5>
</fC03>
<fC03 i1="03" i2="X" l="ENG"><s0>Gravitational lensing</s0>
<s5>28</s5>
</fC03>
<fC03 i1="03" i2="X" l="SPA"><s0>Espejismo gravitacional</s0>
<s5>28</s5>
</fC03>
<fC03 i1="04" i2="3" l="FRE"><s0>Position</s0>
<s5>29</s5>
</fC03>
<fC03 i1="04" i2="3" l="ENG"><s0>Positions</s0>
<s5>29</s5>
</fC03>
<fC03 i1="05" i2="3" l="FRE"><s0>Déplacement vers le rouge</s0>
<s5>30</s5>
</fC03>
<fC03 i1="05" i2="3" l="ENG"><s0>Red shift</s0>
<s5>30</s5>
</fC03>
<fC03 i1="06" i2="X" l="FRE"><s0>Observatoire spatial</s0>
<s5>31</s5>
</fC03>
<fC03 i1="06" i2="X" l="ENG"><s0>Spatial observatory</s0>
<s5>31</s5>
</fC03>
<fC03 i1="06" i2="X" l="SPA"><s0>Observatorio espacial</s0>
<s5>31</s5>
</fC03>
<fC03 i1="07" i2="3" l="FRE"><s0>Spectrométrie</s0>
<s5>32</s5>
</fC03>
<fC03 i1="07" i2="3" l="ENG"><s0>Spectroscopy</s0>
<s5>32</s5>
</fC03>
<fC03 i1="08" i2="3" l="FRE"><s0>Luminosité</s0>
<s5>33</s5>
</fC03>
<fC03 i1="08" i2="3" l="ENG"><s0>Luminosity</s0>
<s5>33</s5>
</fC03>
<fC03 i1="09" i2="3" l="FRE"><s0>Formation galaxies</s0>
<s5>34</s5>
</fC03>
<fC03 i1="09" i2="3" l="ENG"><s0>Galaxy formation</s0>
<s5>34</s5>
</fC03>
<fC03 i1="10" i2="3" l="FRE"><s0>Formation stellaire</s0>
<s5>35</s5>
</fC03>
<fC03 i1="10" i2="3" l="ENG"><s0>Star formation</s0>
<s5>35</s5>
</fC03>
<fN21><s1>331</s1>
</fN21>
<fN44 i1="01"><s1>OTO</s1>
</fN44>
<fN82><s1>OTO</s1>
</fN82>
</pA>
</standard>
<server><NO>PASCAL 12-0421291 INIST</NO>
<ET>OBSERVATIONAL LIMITS ON THE GAS MASS OF A z = 4.9 GALAXY</ET>
<AU>LIVERMORE (R. C.); SWINBANK (A. M.); SMAIL (Ian); BOWER (R. G.); COPPIN (K. E. K.); CRAIN (R. A.); EDGE (A. C.); GEACH (J. E.); RICHARD (J.)</AU>
<AF>Institute for Computational Cosmology, Durham University, South Road/Durham DH1 3LE/Royaume-Uni (1 aut., 2 aut., 3 aut., 4 aut., 5 aut., 7 aut., 8 aut., 9 aut.); Department of Physics, McGill University, 3600 me University/Montréal, QC H3A 2T8/Canada (5 aut., 8 aut.); Centre for Astrophysics and Supercomputing, Swinburne University of Technology, P.O. Box 218/Hawthorn, Victoria 3122/Australie (6 aut.); Leiden Observatory, Leiden University, PO Box 9513/2300 RA Leiden/Pays-Bas (6 aut.); CRAL, Observatoire de Lyon, 9 Avenue Charles André/69561 Saint-Genis-Laval/France (9 aut.)</AF>
<DT>Publication en série; Niveau analytique</DT>
<SO>The Astrophysical journal; ISSN 0004-637X; Coden ASJOAB; Royaume-Uni; Da. 2012; Vol. 758; No. 2 p. 2; L35.1-L35.5; Bibl. 1/4 p.</SO>
<LA>Anglais</LA>
<EA>We present the results of a search for molecular gas emission from a star-forming galaxy at z = 4.9. The galaxy benefits from magnification of 22 ± 5x due to strong gravitational lensing by the foreground cluster MS 1358+62. We target the CO(5-4) emission at a known position and redshift from existing Hubble Space Telescope/Advanced Camera for Surveys imaging and Gemini/NIFS [O II]3727 imaging spectroscopy, and obtain a tentative detection at the 4.3σ level with a flux of 0. 104 ± 0.024 Jy km s<sup>-1</sup>
. From the CO line luminosity and assuming a CO-to-H<sub>2</sub>
 conversion factor α = 2, we derive a gas mass M<sub>gas </sub>
∼ 1<sup>+1</sup>
<sub>-0.6</sub>
 × 10<sup>9</sup>
 M<sub>◦.</sub>
. Combined with the existing data, we derive a gas fraction M<sub>gas</sub>
/(M<sub>gas</sub>
 + M<sub>*</sub>
) = 0.59<sup>+0.11</sup>
<sub>-0.06</sub>
. The faint line flux of this galaxy highlights the difficulty of observing molecular gas in representative galaxies at this epoch, and suggests that routine detections of similar galaxies in the absence of gravitational lensing will remain challenging even with ALMA in full science operations.</EA>
<CC>001E03</CC>
<FD>Galaxies; Gaz moléculaire; Mirage gravitationnel; Position; Déplacement vers le rouge; Observatoire spatial; Spectrométrie; Luminosité; Formation galaxies; Formation stellaire</FD>
<ED>Galaxies; Molecular gas; Gravitational lensing; Positions; Red shift; Spatial observatory; Spectroscopy; Luminosity; Galaxy formation; Star formation</ED>
<SD>Gas molecular; Espejismo gravitacional; Observatorio espacial</SD>
<LO>INIST-512.354000505368390110</LO>
<ID>12-0421291</ID>
</server>
</inist>
</record>

Pour manipuler ce document sous Unix (Dilib)

EXPLOR_STEP=$WICRI_ROOT/Wicri/Asie/explor/AustralieFrV1/Data/PascalFrancis/Corpus

HfdSelect -h $EXPLOR_STEP/biblio.hfd -nk 000F12 | SxmlIndent | more

HfdSelect -h $EXPLOR_AREA/Data/PascalFrancis/Corpus/biblio.hfd -nk 000F12 | SxmlIndent | more

Pour mettre un lien sur cette page dans le réseau Wicri

{{Explor lien
   |wiki=    Wicri/Asie
   |area=    AustralieFrV1
   |flux=    PascalFrancis
   |étape=   Corpus
   |type=    RBID
   |clé=     Pascal:12-0421291
   |texte=   OBSERVATIONAL LIMITS ON THE GAS MASS OF A z = 4.9 GALAXY
}}

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
	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.

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

OBSERVATIONAL LIMITS ON THE GAS MASS OF A z = 4.9 GALAXY

OBSERVATIONAL LIMITS ON THE GAS MASS OF A z = 4.9 GALAXY

Source :

Descripteurs français

English descriptors

Abstract

Notice en format standard (ISO 2709)

Format Inist (serveur)

Links to Exploration step

Le document en format XML

Pour manipuler ce document sous Unix (Dilib)

Pour mettre un lien sur cette page dans le réseau Wicri