HerMES: Lyman break galaxies individually detected at 0.7 ≤ z ≤ 2.0 in GOODS-N with Herschel/SPIRE
As part of the Herschel Multi-tiered Extragalactic Survey we have investigated the rest-frame far-infrared (FIR) properties of a sample of more than 4800 Lyman Break Galaxies (LBGs) in the Great Observatories Origins Deep Survey North field. Most LBGs are not detected individually, but we do detect...
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| Format: | Journal article |
| Language: | English |
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2010
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| _version_ | 1797055743331926016 |
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| author | Burgarella, D Buat, V Magdis, G |
| author_facet | Burgarella, D Buat, V Magdis, G |
| author_sort | Burgarella, D |
| collection | OXFORD |
| description | As part of the Herschel Multi-tiered Extragalactic Survey we have investigated the rest-frame far-infrared (FIR) properties of a sample of more than 4800 Lyman Break Galaxies (LBGs) in the Great Observatories Origins Deep Survey North field. Most LBGs are not detected individually, but we do detect a sub-sample of 12 objects at 0.7 < z < 1.6 and one object at z = 2.0. The LBGs have been selected using color-color diagrams; the ones detected by Herschel SPIRE have redder colors than the others, while the undetected ones have colors consistent with average LBGs at z > 2.5. The spectral energy distributions of the objects detected in the rest-frame FIR are investigated using the code cigale to estimate physical parameters. We include far-UV (FUV) data from GALEX. We find that LBGs detected by SPIRE are high mass, luminous infrared galaxies. It appears that LBGs are located in a triangle-shaped region in the AFUV vs. Log LFUV = 0 diagram limited by A FUV = 0 at the bottom and by a diagonal following the temporal evolution of the most massive galaxies from the bottom-right to the top-left of the diagram. This upper envelop can be used as upper limits for the UV dust attenuation as a function of LFUV. The limits of this region are well explained using a closed-box model, where the chemical evolution of galaxies produces metals, which in turn lead to higher dust attenuation when the galaxies age. © Copyright International Astronomical Union 2011. |
| first_indexed | 2024-03-06T19:14:09Z |
| format | Journal article |
| id | oxford-uuid:17c5a315-cf5a-4ff5-938b-3f91c666c872 |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-06T19:14:09Z |
| publishDate | 2010 |
| record_format | dspace |
| spelling | oxford-uuid:17c5a315-cf5a-4ff5-938b-3f91c666c8722022-03-26T10:39:25ZHerMES: Lyman break galaxies individually detected at 0.7 ≤ z ≤ 2.0 in GOODS-N with Herschel/SPIREJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:17c5a315-cf5a-4ff5-938b-3f91c666c872EnglishSymplectic Elements at Oxford2010Burgarella, DBuat, VMagdis, GAs part of the Herschel Multi-tiered Extragalactic Survey we have investigated the rest-frame far-infrared (FIR) properties of a sample of more than 4800 Lyman Break Galaxies (LBGs) in the Great Observatories Origins Deep Survey North field. Most LBGs are not detected individually, but we do detect a sub-sample of 12 objects at 0.7 < z < 1.6 and one object at z = 2.0. The LBGs have been selected using color-color diagrams; the ones detected by Herschel SPIRE have redder colors than the others, while the undetected ones have colors consistent with average LBGs at z > 2.5. The spectral energy distributions of the objects detected in the rest-frame FIR are investigated using the code cigale to estimate physical parameters. We include far-UV (FUV) data from GALEX. We find that LBGs detected by SPIRE are high mass, luminous infrared galaxies. It appears that LBGs are located in a triangle-shaped region in the AFUV vs. Log LFUV = 0 diagram limited by A FUV = 0 at the bottom and by a diagonal following the temporal evolution of the most massive galaxies from the bottom-right to the top-left of the diagram. This upper envelop can be used as upper limits for the UV dust attenuation as a function of LFUV. The limits of this region are well explained using a closed-box model, where the chemical evolution of galaxies produces metals, which in turn lead to higher dust attenuation when the galaxies age. © Copyright International Astronomical Union 2011. |
| spellingShingle | Burgarella, D Buat, V Magdis, G HerMES: Lyman break galaxies individually detected at 0.7 ≤ z ≤ 2.0 in GOODS-N with Herschel/SPIRE |
| title | HerMES: Lyman break galaxies individually detected at 0.7 ≤ z ≤ 2.0 in GOODS-N with Herschel/SPIRE |
| title_full | HerMES: Lyman break galaxies individually detected at 0.7 ≤ z ≤ 2.0 in GOODS-N with Herschel/SPIRE |
| title_fullStr | HerMES: Lyman break galaxies individually detected at 0.7 ≤ z ≤ 2.0 in GOODS-N with Herschel/SPIRE |
| title_full_unstemmed | HerMES: Lyman break galaxies individually detected at 0.7 ≤ z ≤ 2.0 in GOODS-N with Herschel/SPIRE |
| title_short | HerMES: Lyman break galaxies individually detected at 0.7 ≤ z ≤ 2.0 in GOODS-N with Herschel/SPIRE |
| title_sort | hermes lyman break galaxies individually detected at 0 7 ≤ z ≤ 2 0 in goods n with herschel spire |
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