Clustering of supernova ia host galaxies
For the first time the cross-correlation between Type Ia supernova host galaxies and surrounding field galaxies is measured using the Supernova Legacy Survey sample. Over the z p 0.2-0.9 redshift range we find that supernova hosts are correlated an average of 60% more strongly than similarly selecte...
| Main Authors: | , , , , , , , , , , , , , , , , , , |
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| Format: | Journal article |
| Language: | English |
| Published: |
Institute of Physics Publishing
2008
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| _version_ | 1797062018767781888 |
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| author | Carlberg, R Sullivan, M Le Borgne, D Conley, A Howell, D Perrett, K Astier, P Balam, D Balland, C Basa, S Hardin, D Fouchez, D Guy, J Hook, I Pain, R Pritchet, C Regnault, N Rich, J Perlmutter, S |
| author_facet | Carlberg, R Sullivan, M Le Borgne, D Conley, A Howell, D Perrett, K Astier, P Balam, D Balland, C Basa, S Hardin, D Fouchez, D Guy, J Hook, I Pain, R Pritchet, C Regnault, N Rich, J Perlmutter, S |
| author_sort | Carlberg, R |
| collection | OXFORD |
| description | For the first time the cross-correlation between Type Ia supernova host galaxies and surrounding field galaxies is measured using the Supernova Legacy Survey sample. Over the z p 0.2-0.9 redshift range we find that supernova hosts are correlated an average of 60% more strongly than similarly selected field galaxies over the 3″-100″ range and about a factor of 3 more strongly below 10″. The correlation errors are empirically established with a jackknife analysis of the four SNLS fields. The hosts are more correlated than the field at a significance of 99% in the fitted amplitude and slope, with the point-by-point difference of the two correlation functions having a reduced x2 for 8 degrees of freedom of 4.3, which has a probability of random occurrence of less than 3 × 10-5. The correlation angle is 1.5″ ± 0.5″, which deprojects to a fixed comoving correlation length of approximately 6.5 ± 2 h-1 Mpc. Weighting the field galaxies with the mass and star formation rate supernova frequencies of the simple A + B model produces good agreement with the observed clustering. We conclude that these supernova clustering differences are primarily the expected outcome of the dependence of supernova rates on galaxy masses and stellar populations with their clustering environment. © 2008. The American Astronomical Society. |
| first_indexed | 2024-03-06T20:39:32Z |
| format | Journal article |
| id | oxford-uuid:33cc6902-57bd-4ed0-936d-8917dbc667fa |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-06T20:39:32Z |
| publishDate | 2008 |
| publisher | Institute of Physics Publishing |
| record_format | dspace |
| spelling | oxford-uuid:33cc6902-57bd-4ed0-936d-8917dbc667fa2022-03-26T13:22:20ZClustering of supernova ia host galaxiesJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:33cc6902-57bd-4ed0-936d-8917dbc667faEnglishSymplectic Elements at OxfordInstitute of Physics Publishing2008Carlberg, RSullivan, MLe Borgne, DConley, AHowell, DPerrett, KAstier, PBalam, DBalland, CBasa, SHardin, DFouchez, DGuy, JHook, IPain, RPritchet, CRegnault, NRich, JPerlmutter, SFor the first time the cross-correlation between Type Ia supernova host galaxies and surrounding field galaxies is measured using the Supernova Legacy Survey sample. Over the z p 0.2-0.9 redshift range we find that supernova hosts are correlated an average of 60% more strongly than similarly selected field galaxies over the 3″-100″ range and about a factor of 3 more strongly below 10″. The correlation errors are empirically established with a jackknife analysis of the four SNLS fields. The hosts are more correlated than the field at a significance of 99% in the fitted amplitude and slope, with the point-by-point difference of the two correlation functions having a reduced x2 for 8 degrees of freedom of 4.3, which has a probability of random occurrence of less than 3 × 10-5. The correlation angle is 1.5″ ± 0.5″, which deprojects to a fixed comoving correlation length of approximately 6.5 ± 2 h-1 Mpc. Weighting the field galaxies with the mass and star formation rate supernova frequencies of the simple A + B model produces good agreement with the observed clustering. We conclude that these supernova clustering differences are primarily the expected outcome of the dependence of supernova rates on galaxy masses and stellar populations with their clustering environment. © 2008. The American Astronomical Society. |
| spellingShingle | Carlberg, R Sullivan, M Le Borgne, D Conley, A Howell, D Perrett, K Astier, P Balam, D Balland, C Basa, S Hardin, D Fouchez, D Guy, J Hook, I Pain, R Pritchet, C Regnault, N Rich, J Perlmutter, S Clustering of supernova ia host galaxies |
| title | Clustering of supernova ia host galaxies |
| title_full | Clustering of supernova ia host galaxies |
| title_fullStr | Clustering of supernova ia host galaxies |
| title_full_unstemmed | Clustering of supernova ia host galaxies |
| title_short | Clustering of supernova ia host galaxies |
| title_sort | clustering of supernova ia host galaxies |
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