A JVLA 10~degree^2 deep survey
(Abridged)One of the fundamental challenges for astrophysics in the 21st century is finding a way to untangle the physical processes that govern galaxy formation and evolution. Given the importance and scope of this problem, the multi-wavelength astronomical community has used the past decade to bui...
| Main Authors: | , , , , , , , , , , , , |
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| Format: | Internet publication |
| Language: | English |
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2014
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| _version_ | 1811141278154358784 |
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| author | Jarvis, M Bhatnagar, S Brüggen, M Ferrari, C Heywood, I Hardcastle, M Murphy, E Taylor, R Smirnov, O Simpson, C Smolcic, V Stil, J van der Heyden, K |
| author_facet | Jarvis, M Bhatnagar, S Brüggen, M Ferrari, C Heywood, I Hardcastle, M Murphy, E Taylor, R Smirnov, O Simpson, C Smolcic, V Stil, J van der Heyden, K |
| author_sort | Jarvis, M |
| collection | OXFORD |
| description | (Abridged)One of the fundamental challenges for astrophysics in the 21st century is finding a way to untangle the physical processes that govern galaxy formation and evolution. Given the importance and scope of this problem, the multi-wavelength astronomical community has used the past decade to build up a wealth of information over specific extragalactic deep fields to address key questions in galaxy formation and evolution. These fields generally cover at least 10square degrees to facilitate the investigation of the rarest, typically most massive, galaxies and AGN. Furthermore, such areal coverage allows the environments to be fully accounted for, thereby linking the single halo to the two-halo terms in the halo occupation distribution. Surveys at radio wavelengths have begun to lag behind those at other wavelengths, especially in this medium-deep survey tier. However, the survey speed offered by the JVLA means that we can now reach a point where we can begin to obtain commensurate data at radio wavelengths to those which already exists from the X-ray through to the far-infrared over ~10 square degrees. We therefore present the case for a 10 square degree survey to 1.5uJy at L-band in A or B Array, requiring ~4000 hours to provide census of star-formation and AGN-accretion activity in the Universe. For example, the observations will allow galaxies forming stars at 10Msolar/yr to be detected out to z~1 and luminous infrared galaxies (1000Msolar/yr to be found out to z~6. Furthermore, the survey area ensures that we will have enough cosmic volume to find these rare sources at all epochs. The bandwidth will allow us to determine the polarisation properties galaxies in the high-redshift Universe as a function of stellar mass, morphology and redshift. |
| first_indexed | 2024-03-07T01:50:50Z |
| format | Internet publication |
| id | oxford-uuid:9a08b9bd-3732-4be0-8e56-781b0ca83a70 |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-09-25T04:35:20Z |
| publishDate | 2014 |
| record_format | dspace |
| spelling | oxford-uuid:9a08b9bd-3732-4be0-8e56-781b0ca83a702024-09-17T13:09:18ZA JVLA 10~degree^2 deep surveyInternet publicationhttp://purl.org/coar/resource_type/c_7ad9uuid:9a08b9bd-3732-4be0-8e56-781b0ca83a70EnglishSymplectic Elements at Oxford2014Jarvis, MBhatnagar, SBrüggen, MFerrari, CHeywood, IHardcastle, MMurphy, ETaylor, RSmirnov, OSimpson, CSmolcic, VStil, Jvan der Heyden, K(Abridged)One of the fundamental challenges for astrophysics in the 21st century is finding a way to untangle the physical processes that govern galaxy formation and evolution. Given the importance and scope of this problem, the multi-wavelength astronomical community has used the past decade to build up a wealth of information over specific extragalactic deep fields to address key questions in galaxy formation and evolution. These fields generally cover at least 10square degrees to facilitate the investigation of the rarest, typically most massive, galaxies and AGN. Furthermore, such areal coverage allows the environments to be fully accounted for, thereby linking the single halo to the two-halo terms in the halo occupation distribution. Surveys at radio wavelengths have begun to lag behind those at other wavelengths, especially in this medium-deep survey tier. However, the survey speed offered by the JVLA means that we can now reach a point where we can begin to obtain commensurate data at radio wavelengths to those which already exists from the X-ray through to the far-infrared over ~10 square degrees. We therefore present the case for a 10 square degree survey to 1.5uJy at L-band in A or B Array, requiring ~4000 hours to provide census of star-formation and AGN-accretion activity in the Universe. For example, the observations will allow galaxies forming stars at 10Msolar/yr to be detected out to z~1 and luminous infrared galaxies (1000Msolar/yr to be found out to z~6. Furthermore, the survey area ensures that we will have enough cosmic volume to find these rare sources at all epochs. The bandwidth will allow us to determine the polarisation properties galaxies in the high-redshift Universe as a function of stellar mass, morphology and redshift. |
| spellingShingle | Jarvis, M Bhatnagar, S Brüggen, M Ferrari, C Heywood, I Hardcastle, M Murphy, E Taylor, R Smirnov, O Simpson, C Smolcic, V Stil, J van der Heyden, K A JVLA 10~degree^2 deep survey |
| title | A JVLA 10~degree^2 deep survey |
| title_full | A JVLA 10~degree^2 deep survey |
| title_fullStr | A JVLA 10~degree^2 deep survey |
| title_full_unstemmed | A JVLA 10~degree^2 deep survey |
| title_short | A JVLA 10~degree^2 deep survey |
| title_sort | jvla 10 degree 2 deep survey |
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