The Extreme Hosts of Extreme Supernovae
We use GALEX ultraviolet (UV) and optical integrated photometry of the hosts of seventeen luminous supernovae (LSNe, having peak M_V < -21) and compare them to a sample of 26,000 galaxies from a cross-match between the SDSS DR4 spectral catalog and GALEX interim release 1.1. We place the LSNe...
| Main Authors: | , , , , , , , , , , , , , , , , , , , , , , , , |
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| Format: | Journal article |
| Language: | English |
| Published: |
Institute of Physics Publishing
2010
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| _version_ | 1797071971009167360 |
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| author | Neill, J Sullivan, M Gal-Yam, A Quimby, R Ofek, E Wyder, T Howell, D Nugent, P Seibert, M Martin, D Overzier, R Barlow, T Foster, K Friedman, P Morrissey, P Neff, S Schiminovich, D Bianchi, L Donas, J Heckman, T Lee, Y Madore, B Milliard, B Rich, R Szalay, A |
| author_facet | Neill, J Sullivan, M Gal-Yam, A Quimby, R Ofek, E Wyder, T Howell, D Nugent, P Seibert, M Martin, D Overzier, R Barlow, T Foster, K Friedman, P Morrissey, P Neff, S Schiminovich, D Bianchi, L Donas, J Heckman, T Lee, Y Madore, B Milliard, B Rich, R Szalay, A |
| author_sort | Neill, J |
| collection | OXFORD |
| description | We use GALEX ultraviolet (UV) and optical integrated photometry of the hosts of seventeen luminous supernovae (LSNe, having peak M_V < -21) and compare them to a sample of 26,000 galaxies from a cross-match between the SDSS DR4 spectral catalog and GALEX interim release 1.1. We place the LSNe hosts on the galaxy NUV-r versus M_r color magnitude diagram (CMD) with the larger sample to illustrate how extreme they are. The LSN hosts appear to favor low-density regions of the galaxy CMD falling on the blue edge of the blue cloud toward the low luminosity end. From the UV-optical photometry, we estimate the star formation history of the LSN hosts. The hosts have moderately low star formation rates (SFRs) and low stellar masses (M_*) resulting in high specific star formation rates (sSFR). Compared with the larger sample, the LSN hosts occupy low-density regions of a diagram plotting sSFR versus M_* in the area having higher sSFR and lower M_*. This preference for low M_*, high sSFR hosts implies the LSNe are produced by an effect having to do with their local environment. The correlation of mass with metallicity suggests that perhaps wind-driven mass loss is the factor that prevents LSNe from arising in higher-mass, higher-metallicity hosts. The massive progenitors of the LSNe (>100 M_sun), by appearing in low-SFR hosts, are potential tests for theories of the initial mass function that limit the maximum mass of a star based on the SFR. |
| first_indexed | 2024-03-06T23:00:52Z |
| format | Journal article |
| id | oxford-uuid:620e3f1a-0061-4f16-881a-b28d5c4acb6c |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-06T23:00:52Z |
| publishDate | 2010 |
| publisher | Institute of Physics Publishing |
| record_format | dspace |
| spelling | oxford-uuid:620e3f1a-0061-4f16-881a-b28d5c4acb6c2022-03-26T18:03:57ZThe Extreme Hosts of Extreme SupernovaeJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:620e3f1a-0061-4f16-881a-b28d5c4acb6cEnglishSymplectic Elements at OxfordInstitute of Physics Publishing2010Neill, JSullivan, MGal-Yam, AQuimby, ROfek, EWyder, THowell, DNugent, PSeibert, MMartin, DOverzier, RBarlow, TFoster, KFriedman, PMorrissey, PNeff, SSchiminovich, DBianchi, LDonas, JHeckman, TLee, YMadore, BMilliard, BRich, RSzalay, AWe use GALEX ultraviolet (UV) and optical integrated photometry of the hosts of seventeen luminous supernovae (LSNe, having peak M_V < -21) and compare them to a sample of 26,000 galaxies from a cross-match between the SDSS DR4 spectral catalog and GALEX interim release 1.1. We place the LSNe hosts on the galaxy NUV-r versus M_r color magnitude diagram (CMD) with the larger sample to illustrate how extreme they are. The LSN hosts appear to favor low-density regions of the galaxy CMD falling on the blue edge of the blue cloud toward the low luminosity end. From the UV-optical photometry, we estimate the star formation history of the LSN hosts. The hosts have moderately low star formation rates (SFRs) and low stellar masses (M_*) resulting in high specific star formation rates (sSFR). Compared with the larger sample, the LSN hosts occupy low-density regions of a diagram plotting sSFR versus M_* in the area having higher sSFR and lower M_*. This preference for low M_*, high sSFR hosts implies the LSNe are produced by an effect having to do with their local environment. The correlation of mass with metallicity suggests that perhaps wind-driven mass loss is the factor that prevents LSNe from arising in higher-mass, higher-metallicity hosts. The massive progenitors of the LSNe (>100 M_sun), by appearing in low-SFR hosts, are potential tests for theories of the initial mass function that limit the maximum mass of a star based on the SFR. |
| spellingShingle | Neill, J Sullivan, M Gal-Yam, A Quimby, R Ofek, E Wyder, T Howell, D Nugent, P Seibert, M Martin, D Overzier, R Barlow, T Foster, K Friedman, P Morrissey, P Neff, S Schiminovich, D Bianchi, L Donas, J Heckman, T Lee, Y Madore, B Milliard, B Rich, R Szalay, A The Extreme Hosts of Extreme Supernovae |
| title | The Extreme Hosts of Extreme Supernovae |
| title_full | The Extreme Hosts of Extreme Supernovae |
| title_fullStr | The Extreme Hosts of Extreme Supernovae |
| title_full_unstemmed | The Extreme Hosts of Extreme Supernovae |
| title_short | The Extreme Hosts of Extreme Supernovae |
| title_sort | extreme hosts of extreme supernovae |
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