A multi-wavelength view of the star formation activity at z ∼ 3
We present a multi-wavelength, UV-to-radio analysis for a sample of massive (M * ∼ 1010 M ⊙) IRAC- and MIPS 24 μm detected Lyman break galaxies (LBGs) with spectroscopic redshifts z 3 in the GOODS-North field. For LBGs without individual 24 μm detections, we employ stacking techniques at 24 μm, 1.1m...
| Main Authors: | , , , , , , , |
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| Format: | Journal article |
| Language: | English |
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Institute of Physics Publishing
2010
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| _version_ | 1797058977498923008 |
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| author | Magdis, G Elbaz, D Daddi, E Morrison, G Dickinson, M Rigopoulou, D Gobat, R Hwang, H |
| author_facet | Magdis, G Elbaz, D Daddi, E Morrison, G Dickinson, M Rigopoulou, D Gobat, R Hwang, H |
| author_sort | Magdis, G |
| collection | OXFORD |
| description | We present a multi-wavelength, UV-to-radio analysis for a sample of massive (M * ∼ 1010 M ⊙) IRAC- and MIPS 24 μm detected Lyman break galaxies (LBGs) with spectroscopic redshifts z 3 in the GOODS-North field. For LBGs without individual 24 μm detections, we employ stacking techniques at 24 μm, 1.1mm, and 1.4GHz to construct the average UV-to-radio spectral energy distribution and find it to be consistent with that of a luminous infrared galaxy with L IR = 4.5 +1.1-2.3 × 1011 L ⊙ and a specific star formation rate of 4.3 Gyr-1 that corresponds to a mass doubling time 230 Myr. On the other hand, when considering the 24 μm detected LBGs we find among them galaxies with L IR>10 12 L ⊙, indicating that the space density of z 3 UV-selected ultra-luminous infrared galaxies (ULIRGs) is (1.5 0.5) × 10-5 Mpc-3. We compare measurements of star formation rates from data at different wavelengths and find that there is tight correlation (Kendall's τ>99.7%) and excellent agreement between the values derived from dust-corrected UV, mid-IR, millimeter, and radio data for the whole range of L IR up to L IR 1013 L ⊙. This range is greater than that for which the correlation is known to hold at z ∼ 2, possibly due to the lack of significant contribution from polycyclic aromatic hydrocarbons to the 24 μm flux at z ∼ 3. The fact that this agreement is observed for galaxies with L IR> 1012 L ⊙ suggests that star formation in UV-selected ULIRGs, as well as the bulk of star formation activity at this redshift, is not embedded in optically thick regions as seen in local ULIRGs and submillimeter-selected galaxies at z = 2. © 2010 The American Astronomical Society. All rights reserved. |
| first_indexed | 2024-03-06T19:57:42Z |
| format | Journal article |
| id | oxford-uuid:263585d7-70fa-4e0b-9830-6e08a74b1d5a |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-06T19:57:42Z |
| publishDate | 2010 |
| publisher | Institute of Physics Publishing |
| record_format | dspace |
| spelling | oxford-uuid:263585d7-70fa-4e0b-9830-6e08a74b1d5a2022-03-26T11:59:37ZA multi-wavelength view of the star formation activity at z ∼ 3Journal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:263585d7-70fa-4e0b-9830-6e08a74b1d5aEnglishSymplectic Elements at OxfordInstitute of Physics Publishing2010Magdis, GElbaz, DDaddi, EMorrison, GDickinson, MRigopoulou, DGobat, RHwang, HWe present a multi-wavelength, UV-to-radio analysis for a sample of massive (M * ∼ 1010 M ⊙) IRAC- and MIPS 24 μm detected Lyman break galaxies (LBGs) with spectroscopic redshifts z 3 in the GOODS-North field. For LBGs without individual 24 μm detections, we employ stacking techniques at 24 μm, 1.1mm, and 1.4GHz to construct the average UV-to-radio spectral energy distribution and find it to be consistent with that of a luminous infrared galaxy with L IR = 4.5 +1.1-2.3 × 1011 L ⊙ and a specific star formation rate of 4.3 Gyr-1 that corresponds to a mass doubling time 230 Myr. On the other hand, when considering the 24 μm detected LBGs we find among them galaxies with L IR>10 12 L ⊙, indicating that the space density of z 3 UV-selected ultra-luminous infrared galaxies (ULIRGs) is (1.5 0.5) × 10-5 Mpc-3. We compare measurements of star formation rates from data at different wavelengths and find that there is tight correlation (Kendall's τ>99.7%) and excellent agreement between the values derived from dust-corrected UV, mid-IR, millimeter, and radio data for the whole range of L IR up to L IR 1013 L ⊙. This range is greater than that for which the correlation is known to hold at z ∼ 2, possibly due to the lack of significant contribution from polycyclic aromatic hydrocarbons to the 24 μm flux at z ∼ 3. The fact that this agreement is observed for galaxies with L IR> 1012 L ⊙ suggests that star formation in UV-selected ULIRGs, as well as the bulk of star formation activity at this redshift, is not embedded in optically thick regions as seen in local ULIRGs and submillimeter-selected galaxies at z = 2. © 2010 The American Astronomical Society. All rights reserved. |
| spellingShingle | Magdis, G Elbaz, D Daddi, E Morrison, G Dickinson, M Rigopoulou, D Gobat, R Hwang, H A multi-wavelength view of the star formation activity at z ∼ 3 |
| title | A multi-wavelength view of the star formation activity at z ∼ 3 |
| title_full | A multi-wavelength view of the star formation activity at z ∼ 3 |
| title_fullStr | A multi-wavelength view of the star formation activity at z ∼ 3 |
| title_full_unstemmed | A multi-wavelength view of the star formation activity at z ∼ 3 |
| title_short | A multi-wavelength view of the star formation activity at z ∼ 3 |
| title_sort | multi wavelength view of the star formation activity at z ∼ 3 |
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