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Supernova host galaxies in the dark energy survey: I. Deep coadds, photometry, and stellar masses
ABSTRACT The 5-yr Dark Energy Survey Supernova Programme (DES-SN) is one of the largest and deepest transient surveys to date in terms of volume and number of supernovae. Identifying and characterizing the host galaxies of transients plays a key role in their classification, the study of their forma...
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| Published in: | Monthly notices of the Royal Astronomical Society 2020-05, Vol.495 (4), p.4040-4060 |
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| Main Authors: | , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , |
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| cites | cdi_FETCH-LOGICAL-c440t-c23be79c486897aa5fb8f4815d236b27694d8781f0a8300e3869388350b249693 |
| container_end_page | 4060 |
| container_issue | 4 |
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| container_title | Monthly notices of the Royal Astronomical Society |
| container_volume | 495 |
| creator | Wiseman, P Smith, M Childress, M Kelsey, L Möller, A Gupta, R R Swann, E Angus, C R Brout, D Davis, T M Foley, R J Frohmaier, C Galbany, L Gutiérrez, C P Inserra, C Kessler, R Lewis, G F Lidman, C Macaulay, E Nichol, R C Pursiainen, M Sako, M Scolnic, D Sommer, N E Sullivan, M Tucker, B E Abbott, T M C Aguena, M Allam, S Avila, S Bertin, E Brooks, D Buckley-Geer, E Burke, D L Carnero Rosell, A Carollo, D Carrasco Kind, M da Costa, L N De Vicente, J Desai, S Diehl, H T Doel, P Eifler, T F Everett, S Fosalba, P Frieman, J García-Bellido, J Gaztanaga, E Gerdes, D W Gill, M S S Glazebrook, K Gruendl, R A Gschwend, J Hartley, W G Hinton, S R Hollowood, D L Honscheid, K James, D J Kuehn, K Kuropatkin, N Lima, M Maia, M A G March, M Martini, P Melchior, P Menanteau, F Miquel, R Ogando, R L C Paz-Chinchón, F Plazas, A A Romer, A K Roodman, A Sanchez, E Scarpine, V Serrano, S Suchyta, E Swanson, M E C Tarle, G Thomas, D Tucker, D L Varga, T N Walker, A R Wilkinson, R D |
| description | ABSTRACT
The 5-yr Dark Energy Survey Supernova Programme (DES-SN) is one of the largest and deepest transient surveys to date in terms of volume and number of supernovae. Identifying and characterizing the host galaxies of transients plays a key role in their classification, the study of their formation mechanisms, and the cosmological analyses. To derive accurate host galaxy properties, we create depth-optimized coadds using single-epoch DES-SN images that are selected based on sky and atmospheric conditions. For each of the five DES-SN seasons, a separate coadd is made from the other four seasons such that each SN has a corresponding deep coadd with no contaminating SN emission. The coadds reach limiting magnitudes of order ∼27 in g band, and have a much smaller magnitude uncertainty than the previous DES-SN host templates, particularly for faint objects. We present the resulting multiband photometry of host galaxies for samples of spectroscopically confirmed type Ia (SNe Ia), core-collapse (CCSNe), and superluminous (SLSNe) as well as rapidly evolving transients (RETs) discovered by DES-SN. We derive host galaxy stellar masses and probabilistically compare stellar-mass distributions to samples from other surveys. We find that the DES spectroscopically confirmed sample of SNe Ia selects preferentially fewer high-mass hosts at high-redshift compared to other surveys, while at low redshift the distributions are consistent. DES CCSNe and SLSNe hosts are similar to other samples, while RET hosts are unlike the hosts of any other transients, although these differences have not been disentangled from selection effects. |
| doi_str_mv | 10.1093/mnras/staa1302 |
| format | article |
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The 5-yr Dark Energy Survey Supernova Programme (DES-SN) is one of the largest and deepest transient surveys to date in terms of volume and number of supernovae. Identifying and characterizing the host galaxies of transients plays a key role in their classification, the study of their formation mechanisms, and the cosmological analyses. To derive accurate host galaxy properties, we create depth-optimized coadds using single-epoch DES-SN images that are selected based on sky and atmospheric conditions. For each of the five DES-SN seasons, a separate coadd is made from the other four seasons such that each SN has a corresponding deep coadd with no contaminating SN emission. The coadds reach limiting magnitudes of order ∼27 in g band, and have a much smaller magnitude uncertainty than the previous DES-SN host templates, particularly for faint objects. We present the resulting multiband photometry of host galaxies for samples of spectroscopically confirmed type Ia (SNe Ia), core-collapse (CCSNe), and superluminous (SLSNe) as well as rapidly evolving transients (RETs) discovered by DES-SN. We derive host galaxy stellar masses and probabilistically compare stellar-mass distributions to samples from other surveys. We find that the DES spectroscopically confirmed sample of SNe Ia selects preferentially fewer high-mass hosts at high-redshift compared to other surveys, while at low redshift the distributions are consistent. DES CCSNe and SLSNe hosts are similar to other samples, while RET hosts are unlike the hosts of any other transients, although these differences have not been disentangled from selection effects.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1093/mnras/staa1302</identifier><language>eng</language><publisher>United Kingdom: Oxford University Press</publisher><subject>ASTRONOMY AND ASTROPHYSICS ; catalogues ; image processing techniques ; supernovae</subject><ispartof>Monthly notices of the Royal Astronomical Society, 2020-05, Vol.495 (4), p.4040-4060</ispartof><rights>2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society 2020</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c440t-c23be79c486897aa5fb8f4815d236b27694d8781f0a8300e3869388350b249693</citedby><cites>FETCH-LOGICAL-c440t-c23be79c486897aa5fb8f4815d236b27694d8781f0a8300e3869388350b249693</cites><orcidid>0000-0003-0313-0487 ; 0000-0002-3073-1512 ; 0000-0001-9809-9958 ; 0000-0002-4934-5849 ; 0000-0002-4213-8783 ; 0000-0002-4269-7999 ; 0000000230731512 ; 0000000303130487 ; 0000000249345849 ; 0000000242138783 ; 0000000242697999 ; 0000000198099958</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,315,786,790,891,1591,27957,27958</link.rule.ids><backlink>$$Uhttps://www.osti.gov/biblio/1632730$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Wiseman, P</creatorcontrib><creatorcontrib>Smith, M</creatorcontrib><creatorcontrib>Childress, M</creatorcontrib><creatorcontrib>Kelsey, L</creatorcontrib><creatorcontrib>Möller, A</creatorcontrib><creatorcontrib>Gupta, R R</creatorcontrib><creatorcontrib>Swann, E</creatorcontrib><creatorcontrib>Angus, C R</creatorcontrib><creatorcontrib>Brout, D</creatorcontrib><creatorcontrib>Davis, T M</creatorcontrib><creatorcontrib>Foley, R J</creatorcontrib><creatorcontrib>Frohmaier, C</creatorcontrib><creatorcontrib>Galbany, L</creatorcontrib><creatorcontrib>Gutiérrez, C P</creatorcontrib><creatorcontrib>Inserra, C</creatorcontrib><creatorcontrib>Kessler, R</creatorcontrib><creatorcontrib>Lewis, G F</creatorcontrib><creatorcontrib>Lidman, C</creatorcontrib><creatorcontrib>Macaulay, E</creatorcontrib><creatorcontrib>Nichol, R C</creatorcontrib><creatorcontrib>Pursiainen, M</creatorcontrib><creatorcontrib>Sako, M</creatorcontrib><creatorcontrib>Scolnic, D</creatorcontrib><creatorcontrib>Sommer, N E</creatorcontrib><creatorcontrib>Sullivan, M</creatorcontrib><creatorcontrib>Tucker, B E</creatorcontrib><creatorcontrib>Abbott, T M C</creatorcontrib><creatorcontrib>Aguena, M</creatorcontrib><creatorcontrib>Allam, S</creatorcontrib><creatorcontrib>Avila, S</creatorcontrib><creatorcontrib>Bertin, E</creatorcontrib><creatorcontrib>Brooks, D</creatorcontrib><creatorcontrib>Buckley-Geer, E</creatorcontrib><creatorcontrib>Burke, D L</creatorcontrib><creatorcontrib>Carnero Rosell, A</creatorcontrib><creatorcontrib>Carollo, D</creatorcontrib><creatorcontrib>Carrasco Kind, M</creatorcontrib><creatorcontrib>da Costa, L N</creatorcontrib><creatorcontrib>De Vicente, J</creatorcontrib><creatorcontrib>Desai, S</creatorcontrib><creatorcontrib>Diehl, H T</creatorcontrib><creatorcontrib>Doel, P</creatorcontrib><creatorcontrib>Eifler, T F</creatorcontrib><creatorcontrib>Everett, S</creatorcontrib><creatorcontrib>Fosalba, P</creatorcontrib><creatorcontrib>Frieman, J</creatorcontrib><creatorcontrib>García-Bellido, J</creatorcontrib><creatorcontrib>Gaztanaga, E</creatorcontrib><creatorcontrib>Gerdes, D W</creatorcontrib><creatorcontrib>Gill, M S S</creatorcontrib><creatorcontrib>Glazebrook, K</creatorcontrib><creatorcontrib>Gruendl, R A</creatorcontrib><creatorcontrib>Gschwend, J</creatorcontrib><creatorcontrib>Hartley, W G</creatorcontrib><creatorcontrib>Hinton, S R</creatorcontrib><creatorcontrib>Hollowood, D L</creatorcontrib><creatorcontrib>Honscheid, K</creatorcontrib><creatorcontrib>James, D J</creatorcontrib><creatorcontrib>Kuehn, K</creatorcontrib><creatorcontrib>Kuropatkin, N</creatorcontrib><creatorcontrib>Lima, M</creatorcontrib><creatorcontrib>Maia, M A G</creatorcontrib><creatorcontrib>March, M</creatorcontrib><creatorcontrib>Martini, P</creatorcontrib><creatorcontrib>Melchior, P</creatorcontrib><creatorcontrib>Menanteau, F</creatorcontrib><creatorcontrib>Miquel, R</creatorcontrib><creatorcontrib>Ogando, R L C</creatorcontrib><creatorcontrib>Paz-Chinchón, F</creatorcontrib><creatorcontrib>Plazas, A A</creatorcontrib><creatorcontrib>Romer, A K</creatorcontrib><creatorcontrib>Roodman, A</creatorcontrib><creatorcontrib>Sanchez, E</creatorcontrib><creatorcontrib>Scarpine, V</creatorcontrib><creatorcontrib>Serrano, S</creatorcontrib><creatorcontrib>Suchyta, E</creatorcontrib><creatorcontrib>Swanson, M E C</creatorcontrib><creatorcontrib>Tarle, G</creatorcontrib><creatorcontrib>Thomas, D</creatorcontrib><creatorcontrib>Tucker, D L</creatorcontrib><creatorcontrib>Varga, T N</creatorcontrib><creatorcontrib>Walker, A R</creatorcontrib><creatorcontrib>Wilkinson, R D</creatorcontrib><creatorcontrib>DES Collaboration</creatorcontrib><creatorcontrib>SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States)</creatorcontrib><creatorcontrib>Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States)</creatorcontrib><creatorcontrib>Univ. of Chicago, IL (United States)</creatorcontrib><creatorcontrib>Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States)</creatorcontrib><creatorcontrib>Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)</creatorcontrib><title>Supernova host galaxies in the dark energy survey: I. Deep coadds, photometry, and stellar masses</title><title>Monthly notices of the Royal Astronomical Society</title><description>ABSTRACT
The 5-yr Dark Energy Survey Supernova Programme (DES-SN) is one of the largest and deepest transient surveys to date in terms of volume and number of supernovae. Identifying and characterizing the host galaxies of transients plays a key role in their classification, the study of their formation mechanisms, and the cosmological analyses. To derive accurate host galaxy properties, we create depth-optimized coadds using single-epoch DES-SN images that are selected based on sky and atmospheric conditions. For each of the five DES-SN seasons, a separate coadd is made from the other four seasons such that each SN has a corresponding deep coadd with no contaminating SN emission. The coadds reach limiting magnitudes of order ∼27 in g band, and have a much smaller magnitude uncertainty than the previous DES-SN host templates, particularly for faint objects. We present the resulting multiband photometry of host galaxies for samples of spectroscopically confirmed type Ia (SNe Ia), core-collapse (CCSNe), and superluminous (SLSNe) as well as rapidly evolving transients (RETs) discovered by DES-SN. We derive host galaxy stellar masses and probabilistically compare stellar-mass distributions to samples from other surveys. We find that the DES spectroscopically confirmed sample of SNe Ia selects preferentially fewer high-mass hosts at high-redshift compared to other surveys, while at low redshift the distributions are consistent. DES CCSNe and SLSNe hosts are similar to other samples, while RET hosts are unlike the hosts of any other transients, although these differences have not been disentangled from selection effects.</description><subject>ASTRONOMY AND ASTROPHYSICS</subject><subject>catalogues</subject><subject>image processing techniques</subject><subject>supernovae</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2020</creationdate><recordtype>article</recordtype><recordid>eNqFkL9PwzAQhS0EEqWwMltsSE1rx4njsCF-VqrEAMzRxbk0gTSJfG5F_nsCLTPTu-G7J72PsUsp5lKkarFpHdCCPIBUIjxiE6l0HISp1sdsIoSKA5NIecrOiD6EEJEK9YTB67ZH13Y74FVHnq-hga8aidct9xXyAtwnxxbdeuC0dTscbvhyzu8Re247KAqa8b7qfLdB74YZh7bg5LFpwPENECGds5MSGsKLQ07Z--PD291zsHp5Wt7drgIbRcIHNlQ5JqmNjDZpAhCXuSkjI-MiVDoPE51GhUmMLAUYJQQqo1NljIpFHkbpeE_Z1b53nFFnZGuPtrJd26L1mdQqTJQYofkesq4jclhmvas34IZMiuzHYvZrMfuzOD5cH1q3_X_sN6HHdLg</recordid><startdate>20200519</startdate><enddate>20200519</enddate><creator>Wiseman, P</creator><creator>Smith, M</creator><creator>Childress, M</creator><creator>Kelsey, L</creator><creator>Möller, A</creator><creator>Gupta, R R</creator><creator>Swann, E</creator><creator>Angus, C R</creator><creator>Brout, D</creator><creator>Davis, T M</creator><creator>Foley, R J</creator><creator>Frohmaier, C</creator><creator>Galbany, L</creator><creator>Gutiérrez, C P</creator><creator>Inserra, C</creator><creator>Kessler, R</creator><creator>Lewis, G F</creator><creator>Lidman, C</creator><creator>Macaulay, E</creator><creator>Nichol, R C</creator><creator>Pursiainen, M</creator><creator>Sako, M</creator><creator>Scolnic, D</creator><creator>Sommer, N E</creator><creator>Sullivan, M</creator><creator>Tucker, B E</creator><creator>Abbott, T M C</creator><creator>Aguena, M</creator><creator>Allam, S</creator><creator>Avila, S</creator><creator>Bertin, E</creator><creator>Brooks, D</creator><creator>Buckley-Geer, E</creator><creator>Burke, D L</creator><creator>Carnero Rosell, A</creator><creator>Carollo, D</creator><creator>Carrasco Kind, M</creator><creator>da Costa, L N</creator><creator>De Vicente, J</creator><creator>Desai, S</creator><creator>Diehl, H T</creator><creator>Doel, P</creator><creator>Eifler, T F</creator><creator>Everett, S</creator><creator>Fosalba, P</creator><creator>Frieman, J</creator><creator>García-Bellido, J</creator><creator>Gaztanaga, E</creator><creator>Gerdes, D W</creator><creator>Gill, M S S</creator><creator>Glazebrook, K</creator><creator>Gruendl, R A</creator><creator>Gschwend, J</creator><creator>Hartley, W G</creator><creator>Hinton, S R</creator><creator>Hollowood, D L</creator><creator>Honscheid, K</creator><creator>James, D J</creator><creator>Kuehn, K</creator><creator>Kuropatkin, N</creator><creator>Lima, M</creator><creator>Maia, M A G</creator><creator>March, M</creator><creator>Martini, P</creator><creator>Melchior, P</creator><creator>Menanteau, F</creator><creator>Miquel, R</creator><creator>Ogando, R L C</creator><creator>Paz-Chinchón, F</creator><creator>Plazas, A A</creator><creator>Romer, A K</creator><creator>Roodman, A</creator><creator>Sanchez, E</creator><creator>Scarpine, V</creator><creator>Serrano, S</creator><creator>Suchyta, E</creator><creator>Swanson, M E C</creator><creator>Tarle, G</creator><creator>Thomas, D</creator><creator>Tucker, D L</creator><creator>Varga, T N</creator><creator>Walker, A R</creator><creator>Wilkinson, R D</creator><general>Oxford University Press</general><general>Royal Astronomical Society</general><scope>AAYXX</scope><scope>CITATION</scope><scope>OTOTI</scope><orcidid>https://orcid.org/0000-0003-0313-0487</orcidid><orcidid>https://orcid.org/0000-0002-3073-1512</orcidid><orcidid>https://orcid.org/0000-0001-9809-9958</orcidid><orcidid>https://orcid.org/0000-0002-4934-5849</orcidid><orcidid>https://orcid.org/0000-0002-4213-8783</orcidid><orcidid>https://orcid.org/0000-0002-4269-7999</orcidid><orcidid>https://orcid.org/0000000230731512</orcidid><orcidid>https://orcid.org/0000000303130487</orcidid><orcidid>https://orcid.org/0000000249345849</orcidid><orcidid>https://orcid.org/0000000242138783</orcidid><orcidid>https://orcid.org/0000000242697999</orcidid><orcidid>https://orcid.org/0000000198099958</orcidid></search><sort><creationdate>20200519</creationdate><title>Supernova host galaxies in the dark energy survey: I. Deep coadds, photometry, and stellar masses</title><author>Wiseman, P ; Smith, M ; Childress, M ; Kelsey, L ; Möller, A ; Gupta, R R ; Swann, E ; Angus, C R ; Brout, D ; Davis, T M ; Foley, R J ; Frohmaier, C ; Galbany, L ; Gutiérrez, C P ; Inserra, C ; Kessler, R ; Lewis, G F ; Lidman, C ; Macaulay, E ; Nichol, R C ; Pursiainen, M ; Sako, M ; Scolnic, D ; Sommer, N E ; Sullivan, M ; Tucker, B E ; Abbott, T M C ; Aguena, M ; Allam, S ; Avila, S ; Bertin, E ; Brooks, D ; Buckley-Geer, E ; Burke, D L ; Carnero Rosell, A ; Carollo, D ; Carrasco Kind, M ; da Costa, L N ; De Vicente, J ; Desai, S ; Diehl, H T ; Doel, P ; Eifler, T F ; Everett, S ; Fosalba, P ; Frieman, J ; García-Bellido, J ; Gaztanaga, E ; Gerdes, D W ; Gill, M S S ; Glazebrook, K ; Gruendl, R A ; Gschwend, J ; Hartley, W G ; Hinton, S R ; Hollowood, D L ; Honscheid, K ; James, D J ; Kuehn, K ; Kuropatkin, N ; Lima, M ; Maia, M A G ; March, M ; Martini, P ; Melchior, P ; Menanteau, F ; Miquel, R ; Ogando, R L C ; Paz-Chinchón, F ; Plazas, A A ; Romer, A K ; Roodman, A ; Sanchez, E ; Scarpine, V ; Serrano, S ; Suchyta, E ; Swanson, M E C ; Tarle, G ; Thomas, D ; Tucker, D L ; Varga, T N ; Walker, A R ; Wilkinson, R D</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c440t-c23be79c486897aa5fb8f4815d236b27694d8781f0a8300e3869388350b249693</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2020</creationdate><topic>ASTRONOMY AND ASTROPHYSICS</topic><topic>catalogues</topic><topic>image processing techniques</topic><topic>supernovae</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Wiseman, P</creatorcontrib><creatorcontrib>Smith, M</creatorcontrib><creatorcontrib>Childress, M</creatorcontrib><creatorcontrib>Kelsey, L</creatorcontrib><creatorcontrib>Möller, A</creatorcontrib><creatorcontrib>Gupta, R R</creatorcontrib><creatorcontrib>Swann, E</creatorcontrib><creatorcontrib>Angus, C R</creatorcontrib><creatorcontrib>Brout, D</creatorcontrib><creatorcontrib>Davis, T M</creatorcontrib><creatorcontrib>Foley, R J</creatorcontrib><creatorcontrib>Frohmaier, C</creatorcontrib><creatorcontrib>Galbany, L</creatorcontrib><creatorcontrib>Gutiérrez, C P</creatorcontrib><creatorcontrib>Inserra, C</creatorcontrib><creatorcontrib>Kessler, R</creatorcontrib><creatorcontrib>Lewis, G F</creatorcontrib><creatorcontrib>Lidman, C</creatorcontrib><creatorcontrib>Macaulay, E</creatorcontrib><creatorcontrib>Nichol, R C</creatorcontrib><creatorcontrib>Pursiainen, M</creatorcontrib><creatorcontrib>Sako, M</creatorcontrib><creatorcontrib>Scolnic, D</creatorcontrib><creatorcontrib>Sommer, N E</creatorcontrib><creatorcontrib>Sullivan, M</creatorcontrib><creatorcontrib>Tucker, B E</creatorcontrib><creatorcontrib>Abbott, T M C</creatorcontrib><creatorcontrib>Aguena, M</creatorcontrib><creatorcontrib>Allam, S</creatorcontrib><creatorcontrib>Avila, S</creatorcontrib><creatorcontrib>Bertin, E</creatorcontrib><creatorcontrib>Brooks, D</creatorcontrib><creatorcontrib>Buckley-Geer, E</creatorcontrib><creatorcontrib>Burke, D L</creatorcontrib><creatorcontrib>Carnero Rosell, A</creatorcontrib><creatorcontrib>Carollo, D</creatorcontrib><creatorcontrib>Carrasco Kind, M</creatorcontrib><creatorcontrib>da Costa, L N</creatorcontrib><creatorcontrib>De Vicente, J</creatorcontrib><creatorcontrib>Desai, S</creatorcontrib><creatorcontrib>Diehl, H T</creatorcontrib><creatorcontrib>Doel, P</creatorcontrib><creatorcontrib>Eifler, T F</creatorcontrib><creatorcontrib>Everett, S</creatorcontrib><creatorcontrib>Fosalba, P</creatorcontrib><creatorcontrib>Frieman, J</creatorcontrib><creatorcontrib>García-Bellido, J</creatorcontrib><creatorcontrib>Gaztanaga, E</creatorcontrib><creatorcontrib>Gerdes, D W</creatorcontrib><creatorcontrib>Gill, M S S</creatorcontrib><creatorcontrib>Glazebrook, K</creatorcontrib><creatorcontrib>Gruendl, R A</creatorcontrib><creatorcontrib>Gschwend, J</creatorcontrib><creatorcontrib>Hartley, W G</creatorcontrib><creatorcontrib>Hinton, S R</creatorcontrib><creatorcontrib>Hollowood, D L</creatorcontrib><creatorcontrib>Honscheid, K</creatorcontrib><creatorcontrib>James, D J</creatorcontrib><creatorcontrib>Kuehn, K</creatorcontrib><creatorcontrib>Kuropatkin, N</creatorcontrib><creatorcontrib>Lima, M</creatorcontrib><creatorcontrib>Maia, M A G</creatorcontrib><creatorcontrib>March, M</creatorcontrib><creatorcontrib>Martini, P</creatorcontrib><creatorcontrib>Melchior, P</creatorcontrib><creatorcontrib>Menanteau, F</creatorcontrib><creatorcontrib>Miquel, R</creatorcontrib><creatorcontrib>Ogando, R L C</creatorcontrib><creatorcontrib>Paz-Chinchón, F</creatorcontrib><creatorcontrib>Plazas, A A</creatorcontrib><creatorcontrib>Romer, A K</creatorcontrib><creatorcontrib>Roodman, A</creatorcontrib><creatorcontrib>Sanchez, E</creatorcontrib><creatorcontrib>Scarpine, V</creatorcontrib><creatorcontrib>Serrano, S</creatorcontrib><creatorcontrib>Suchyta, E</creatorcontrib><creatorcontrib>Swanson, M E C</creatorcontrib><creatorcontrib>Tarle, G</creatorcontrib><creatorcontrib>Thomas, D</creatorcontrib><creatorcontrib>Tucker, D L</creatorcontrib><creatorcontrib>Varga, T N</creatorcontrib><creatorcontrib>Walker, A R</creatorcontrib><creatorcontrib>Wilkinson, R D</creatorcontrib><creatorcontrib>DES Collaboration</creatorcontrib><creatorcontrib>SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States)</creatorcontrib><creatorcontrib>Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States)</creatorcontrib><creatorcontrib>Univ. of Chicago, IL (United States)</creatorcontrib><creatorcontrib>Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States)</creatorcontrib><creatorcontrib>Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)</creatorcontrib><collection>CrossRef</collection><collection>OSTI.GOV</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Wiseman, P</au><au>Smith, M</au><au>Childress, M</au><au>Kelsey, L</au><au>Möller, A</au><au>Gupta, R R</au><au>Swann, E</au><au>Angus, C R</au><au>Brout, D</au><au>Davis, T M</au><au>Foley, R J</au><au>Frohmaier, C</au><au>Galbany, L</au><au>Gutiérrez, C P</au><au>Inserra, C</au><au>Kessler, R</au><au>Lewis, G F</au><au>Lidman, C</au><au>Macaulay, E</au><au>Nichol, R C</au><au>Pursiainen, M</au><au>Sako, M</au><au>Scolnic, D</au><au>Sommer, N E</au><au>Sullivan, M</au><au>Tucker, B E</au><au>Abbott, T M C</au><au>Aguena, M</au><au>Allam, S</au><au>Avila, S</au><au>Bertin, E</au><au>Brooks, D</au><au>Buckley-Geer, E</au><au>Burke, D L</au><au>Carnero Rosell, A</au><au>Carollo, D</au><au>Carrasco Kind, M</au><au>da Costa, L N</au><au>De Vicente, J</au><au>Desai, S</au><au>Diehl, H T</au><au>Doel, P</au><au>Eifler, T F</au><au>Everett, S</au><au>Fosalba, P</au><au>Frieman, J</au><au>García-Bellido, J</au><au>Gaztanaga, E</au><au>Gerdes, D W</au><au>Gill, M S S</au><au>Glazebrook, K</au><au>Gruendl, R A</au><au>Gschwend, J</au><au>Hartley, W G</au><au>Hinton, S R</au><au>Hollowood, D L</au><au>Honscheid, K</au><au>James, D J</au><au>Kuehn, K</au><au>Kuropatkin, N</au><au>Lima, M</au><au>Maia, M A G</au><au>March, M</au><au>Martini, P</au><au>Melchior, P</au><au>Menanteau, F</au><au>Miquel, R</au><au>Ogando, R L C</au><au>Paz-Chinchón, F</au><au>Plazas, A A</au><au>Romer, A K</au><au>Roodman, A</au><au>Sanchez, E</au><au>Scarpine, V</au><au>Serrano, S</au><au>Suchyta, E</au><au>Swanson, M E C</au><au>Tarle, G</au><au>Thomas, D</au><au>Tucker, D L</au><au>Varga, T N</au><au>Walker, A R</au><au>Wilkinson, R D</au><aucorp>DES Collaboration</aucorp><aucorp>SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States)</aucorp><aucorp>Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States)</aucorp><aucorp>Univ. of Chicago, IL (United States)</aucorp><aucorp>Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States)</aucorp><aucorp>Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)</aucorp><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Supernova host galaxies in the dark energy survey: I. Deep coadds, photometry, and stellar masses</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><date>2020-05-19</date><risdate>2020</risdate><volume>495</volume><issue>4</issue><spage>4040</spage><epage>4060</epage><pages>4040-4060</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><notes>AC02-07CH11359; AC02-76SF00515; SC0009924; 465376/2014-2; ST/R000506/1; ST/P006760/1; SEV-2016-0588; SEV-2016-0597; MDM-2015-0509; FPA2015-68048; ESP2015-66861; AYA2015-71825; 839090; 615929; AST-1536171; AST-1138766; 291329; 240672; 306478</notes><notes>USDOE Office of Science (SC), High Energy Physics (HEP)</notes><notes>USDOE Office of Science (SC), Basic Energy Sciences (BES)</notes><notes>Ministry of Economic Affairs and Digital Transformation of Spain (MINECO)</notes><notes>STFC</notes><notes>Horizon 2020</notes><notes>National Science Foundation (NSF)</notes><notes>FERMILAB-PUB-20-002-AE; DES-2019-0511; arXiv:2001.02640</notes><abstract>ABSTRACT
The 5-yr Dark Energy Survey Supernova Programme (DES-SN) is one of the largest and deepest transient surveys to date in terms of volume and number of supernovae. Identifying and characterizing the host galaxies of transients plays a key role in their classification, the study of their formation mechanisms, and the cosmological analyses. To derive accurate host galaxy properties, we create depth-optimized coadds using single-epoch DES-SN images that are selected based on sky and atmospheric conditions. For each of the five DES-SN seasons, a separate coadd is made from the other four seasons such that each SN has a corresponding deep coadd with no contaminating SN emission. The coadds reach limiting magnitudes of order ∼27 in g band, and have a much smaller magnitude uncertainty than the previous DES-SN host templates, particularly for faint objects. We present the resulting multiband photometry of host galaxies for samples of spectroscopically confirmed type Ia (SNe Ia), core-collapse (CCSNe), and superluminous (SLSNe) as well as rapidly evolving transients (RETs) discovered by DES-SN. We derive host galaxy stellar masses and probabilistically compare stellar-mass distributions to samples from other surveys. We find that the DES spectroscopically confirmed sample of SNe Ia selects preferentially fewer high-mass hosts at high-redshift compared to other surveys, while at low redshift the distributions are consistent. DES CCSNe and SLSNe hosts are similar to other samples, while RET hosts are unlike the hosts of any other transients, although these differences have not been disentangled from selection effects.</abstract><cop>United Kingdom</cop><pub>Oxford University Press</pub><doi>10.1093/mnras/staa1302</doi><tpages>21</tpages><orcidid>https://orcid.org/0000-0003-0313-0487</orcidid><orcidid>https://orcid.org/0000-0002-3073-1512</orcidid><orcidid>https://orcid.org/0000-0001-9809-9958</orcidid><orcidid>https://orcid.org/0000-0002-4934-5849</orcidid><orcidid>https://orcid.org/0000-0002-4213-8783</orcidid><orcidid>https://orcid.org/0000-0002-4269-7999</orcidid><orcidid>https://orcid.org/0000000230731512</orcidid><orcidid>https://orcid.org/0000000303130487</orcidid><orcidid>https://orcid.org/0000000249345849</orcidid><orcidid>https://orcid.org/0000000242138783</orcidid><orcidid>https://orcid.org/0000000242697999</orcidid><orcidid>https://orcid.org/0000000198099958</orcidid><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0035-8711 |
| ispartof | Monthly notices of the Royal Astronomical Society, 2020-05, Vol.495 (4), p.4040-4060 |
| issn | 0035-8711 1365-2966 |
| language | eng |
| recordid | cdi_osti_scitechconnect_1632730 |
| source | Oxford University Press Journals All Titles (1996-Current); EZB Electronic Journals Library |
| subjects | ASTRONOMY AND ASTROPHYSICS catalogues image processing techniques supernovae |
| title | Supernova host galaxies in the dark energy survey: I. Deep coadds, photometry, and stellar masses |
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