The clustering and evolution of Hα emitters at z ∼ 1 from HiZELS
The clustering properties of a well-defined sample of 734 Hα emitters at z= 0.845 ± 0.015, obtained as part of the Hi-z Emission Line Survey, are investigated. The spatial correlation function of these Hα emitters is very well described by the power-law ξ = (r/r0)-1.8, with a real-space correlation,...
| Main Authors: | , , , , , , , |
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| Format: | Journal article |
| Language: | English |
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2010
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| _version_ | 1797062087491452928 |
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| author | Sobral, D Best, P Geach, J Smail, I Cirasuolo, M Garn, T Dalton, G Kurk, J |
| author_facet | Sobral, D Best, P Geach, J Smail, I Cirasuolo, M Garn, T Dalton, G Kurk, J |
| author_sort | Sobral, D |
| collection | OXFORD |
| description | The clustering properties of a well-defined sample of 734 Hα emitters at z= 0.845 ± 0.015, obtained as part of the Hi-z Emission Line Survey, are investigated. The spatial correlation function of these Hα emitters is very well described by the power-law ξ = (r/r0)-1.8, with a real-space correlation, r0, of 2.7 ± 0.3 h-1 Mpc. The correlation length r0 increases strongly with Hα luminosity (LHα), from r0 ∼ 2 h-1 Mpc for the most quiescent galaxies [star formation rates (SFRs) of ∼4 M⊙ yr-1] up to r0 > 5 h-1 Mpc for the brightest galaxies in Hα. The correlation length also increases with increasing rest-frame K-band (MK) luminosity, but the r0-LHα correlation maintains its full statistical significance at fixed MK. At z = 0.84, star-forming galaxies classified as irregulars or mergers are much more clustered than discs and non-mergers, respectively; however, once the samples are matched in LHα and MK, the differences vanish, implying that the clustering is independent of morphological type at z ∼ 1 just as in the local Universe. The typical Hα emitters found at z = 0.84 reside in dark matter haloes of ≈1012 M⊙, but those with the highest SFRs reside in more massive haloes of ≈1013 M⊙. The results are compared with those of Hα surveys at different redshifts: although the break of the Hα luminosity function L*Hα evolves by a factor of ∼30 from z= 0.24 to 2.23, if the Hα luminosities at each redshift are scaled by L*Hα(z) then the correlation lengths indicate that, independently of cosmic time, galaxies with the same (LHα)/L*Hα(z) are found in dark matter haloes of similar masses. This not only confirms that the star formation efficiency in high redshift haloes is higher than locally but also suggests a fundamental connection between the strong negative evolution of L*Hα since z = 2.23 and the quenching of star formation in galaxies residing within dark matter haloes significantly more massive than 1012 M⊙ at any given epoch. © 2010 The Authors. Journal compilation © 2010 RAS. |
| first_indexed | 2024-03-06T20:40:32Z |
| format | Journal article |
| id | oxford-uuid:34208bc7-dbec-4407-a2e4-d5ad55290a7a |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-06T20:40:32Z |
| publishDate | 2010 |
| record_format | dspace |
| spelling | oxford-uuid:34208bc7-dbec-4407-a2e4-d5ad55290a7a2022-03-26T13:24:09ZThe clustering and evolution of Hα emitters at z ∼ 1 from HiZELSJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:34208bc7-dbec-4407-a2e4-d5ad55290a7aEnglishSymplectic Elements at Oxford2010Sobral, DBest, PGeach, JSmail, ICirasuolo, MGarn, TDalton, GKurk, JThe clustering properties of a well-defined sample of 734 Hα emitters at z= 0.845 ± 0.015, obtained as part of the Hi-z Emission Line Survey, are investigated. The spatial correlation function of these Hα emitters is very well described by the power-law ξ = (r/r0)-1.8, with a real-space correlation, r0, of 2.7 ± 0.3 h-1 Mpc. The correlation length r0 increases strongly with Hα luminosity (LHα), from r0 ∼ 2 h-1 Mpc for the most quiescent galaxies [star formation rates (SFRs) of ∼4 M⊙ yr-1] up to r0 > 5 h-1 Mpc for the brightest galaxies in Hα. The correlation length also increases with increasing rest-frame K-band (MK) luminosity, but the r0-LHα correlation maintains its full statistical significance at fixed MK. At z = 0.84, star-forming galaxies classified as irregulars or mergers are much more clustered than discs and non-mergers, respectively; however, once the samples are matched in LHα and MK, the differences vanish, implying that the clustering is independent of morphological type at z ∼ 1 just as in the local Universe. The typical Hα emitters found at z = 0.84 reside in dark matter haloes of ≈1012 M⊙, but those with the highest SFRs reside in more massive haloes of ≈1013 M⊙. The results are compared with those of Hα surveys at different redshifts: although the break of the Hα luminosity function L*Hα evolves by a factor of ∼30 from z= 0.24 to 2.23, if the Hα luminosities at each redshift are scaled by L*Hα(z) then the correlation lengths indicate that, independently of cosmic time, galaxies with the same (LHα)/L*Hα(z) are found in dark matter haloes of similar masses. This not only confirms that the star formation efficiency in high redshift haloes is higher than locally but also suggests a fundamental connection between the strong negative evolution of L*Hα since z = 2.23 and the quenching of star formation in galaxies residing within dark matter haloes significantly more massive than 1012 M⊙ at any given epoch. © 2010 The Authors. Journal compilation © 2010 RAS. |
| spellingShingle | Sobral, D Best, P Geach, J Smail, I Cirasuolo, M Garn, T Dalton, G Kurk, J The clustering and evolution of Hα emitters at z ∼ 1 from HiZELS |
| title | The clustering and evolution of Hα emitters at z ∼ 1 from HiZELS |
| title_full | The clustering and evolution of Hα emitters at z ∼ 1 from HiZELS |
| title_fullStr | The clustering and evolution of Hα emitters at z ∼ 1 from HiZELS |
| title_full_unstemmed | The clustering and evolution of Hα emitters at z ∼ 1 from HiZELS |
| title_short | The clustering and evolution of Hα emitters at z ∼ 1 from HiZELS |
| title_sort | clustering and evolution of hα emitters at z ∼ 1 from hizels |
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