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| Fältnamn | Indikatorer | Metadata |
|---|---|---|
| 000 | 04435naa a2200841 4500 | |
| 001 | oai:DiVA.org:su-76353 | |
| 003 | SwePub | |
| 008 | 120510s2012 | |||||||||||000 ||eng| | |
| 024 | 7 | a https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-763532 URI |
| 024 | 7 | a https://doi.org/10.1088/0004-637X/745/1/322 DOI |
| 040 | a (SwePub)su | |
| 041 | a engb eng | |
| 042 | 9 SwePub | |
| 072 | 7 | a ref2 swepub-contenttype |
| 072 | 7 | a art2 swepub-publicationtype |
| 100 | 1 | a Barbary, K.4 aut |
| 245 | 1 0 | a THE HUBBLE SPACE TELESCOPE CLUSTER SUPERNOVA SURVEY. II. THE TYPE Ia SUPERNOVA RATE IN HIGH-REDSHIFT GALAXY CLUSTERS |
| 264 | 1 | c 2012 |
| 338 | a print2 rdacarrier | |
| 500 | a 43 | |
| 520 | a We report a measurement of the Type Ia supernova (SN Ia) rate in galaxy clusters at 0.9 < z < 1.46 from the Hubble Space Telescope Cluster Supernova Survey. This is the first cluster SN Ia rate measurement with detected z > 0.9 SNe. Finding 8 +/- 1 cluster SNe Ia, we determine an SN Ia rate of 0.50(-0.19)(+0.23) (stat) (+0.10)(-0.09) (sys) h(70)(2) SNuB (SNuB equivalent to 10(-12) SNe (L-1)circle dot(,B) yr(-1)). In units of stellar mass, this translates to 0.36(-0.13)(+0.16) (stat) (+0.07)(-0.06) (sys) h(70)(2) SNuM (SNuM = 10(-12) SNe M-1 circle dot yr(-1)). This represents a factor of approximate to 5 +/- 2 increase over measurements of the cluster rate at z < 0.2. We parameterize the late-time SN Ia delay time distribution (DTD) with a power law: Psi(t) t(s). Under the approximation of a single-burst cluster formation redshift of z(f) = 3, our rate measurement in combination with lower-redshift cluster SN Ia rates constrains s = -1.41(-0.40)(+0.47), consistent with measurements of the DTD in the field. This measurement is generally consistent with expectations for the double degenerate scenario and inconsistent with some models for the single degenerate scenario predicting a steeper DTD at large delay times. We check for environmental dependence and the influence of younger stellar populations by calculating the rate specifically in cluster red-sequence galaxies and in morphologically early-type galaxies, finding results similar to the full cluster rate. Finally, the upper limit of one hostless cluster SN Ia detected in the survey implies that the fraction of stars in the intra-cluster medium is less than 0.47 (95% confidence), consistent with measurements at lower redshifts. | |
| 650 | 7 | a NATURVETENSKAPx Fysik0 (SwePub)1032 hsv//swe |
| 650 | 7 | a NATURAL SCIENCESx Physical Sciences0 (SwePub)1032 hsv//eng |
| 653 | a cosmology: observations | |
| 653 | a supernovae: general | |
| 653 | a white dwarfs | |
| 700 | 1 | a Aldering, G.4 aut |
| 700 | 1 | a Amanullah, R.4 aut |
| 700 | 1 | a Brodwin, M.4 aut |
| 700 | 1 | a Connolly, N.4 aut |
| 700 | 1 | a Dawson, K. S.4 aut |
| 700 | 1 | a Doi, M.4 aut |
| 700 | 1 | a Eisenhardt, P.4 aut |
| 700 | 1 | a Faccioli, L.4 aut |
| 700 | 1 | a Fadeyev, V.4 aut |
| 700 | 1 | a Fakhouri, H. K.4 aut |
| 700 | 1 | a Fruchter, A. S.4 aut |
| 700 | 1 | a Gilbank, D. G.4 aut |
| 700 | 1 | a Gladders, M. D.4 aut |
| 700 | 1 | a Goldhaber, G.4 aut |
| 700 | 1 | a Goobar, Arielu Stockholms universitet,Fysikum4 aut0 (Swepub:su)ariel |
| 700 | 1 | a Hattori, T.4 aut |
| 700 | 1 | a Hsiao, E.4 aut |
| 700 | 1 | a Huang, X.4 aut |
| 700 | 1 | a Ihara, Y.4 aut |
| 700 | 1 | a Kashikawa, N.4 aut |
| 700 | 1 | a Koester, B.4 aut |
| 700 | 1 | a Konishi, K.4 aut |
| 700 | 1 | a Kowalski, M.4 aut |
| 700 | 1 | a Lidman, C.4 aut |
| 700 | 1 | a Lubin, L.4 aut |
| 700 | 1 | a Meyers, J.4 aut |
| 700 | 1 | a Morokuma, T.4 aut |
| 700 | 1 | a Oda, T.4 aut |
| 700 | 1 | a Panagia, N.4 aut |
| 700 | 1 | a Perlmutter, S.4 aut |
| 700 | 1 | a Postman, M.4 aut |
| 700 | 1 | a Ripoche, P.4 aut |
| 700 | 1 | a Rosati, P.4 aut |
| 700 | 1 | a Rubin, D.4 aut |
| 700 | 1 | a Schlegel, D. J.4 aut |
| 700 | 1 | a Spadafora, A. L.4 aut |
| 700 | 1 | a Stanford, S. A.4 aut |
| 700 | 1 | a Strovink, M.4 aut |
| 700 | 1 | a Suzuki, N.4 aut |
| 700 | 1 | a Takanashi, N.4 aut |
| 700 | 1 | a Tokita, K.4 aut |
| 700 | 1 | a Yasuda, N.4 aut |
| 710 | 2 | a Stockholms universitetb Fysikum4 org |
| 773 | 0 | t Astrophysical Journalg 745:1, s. 32-q 745:1<32-x 0004-637Xx 1538-4357 |
| 856 | 4 | u https://arxiv.org/abs/1010.5786y arXiv:1010.5786 |
| 856 | 4 8 | u https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-76353 |
| 856 | 4 8 | u https://doi.org/10.1088/0004-637X/745/1/32 |
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- Doi, M.
- Eisenhardt, P.
- Faccioli, L.
- Fadeyev, V.
- Fakhouri, H. K.
- Fruchter, A. S.
- Gilbank, D. G.
- Gladders, M. D.
- Goldhaber, G.
- Goobar, Ariel
- Hattori, T.
- Hsiao, E.
- Huang, X.
- Ihara, Y.
- Kashikawa, N.
- Koester, B.
- Konishi, K.
- Kowalski, M.
- Lidman, C.
- Lubin, L.
- Meyers, J.
- Morokuma, T.
- Oda, T.
- Panagia, N.
- Perlmutter, S.
- Postman, M.
- Ripoche, P.
- Rosati, P.
- Rubin, D.
- Schlegel, D. J.
- Spadafora, A. L.
- Stanford, S. A.
- Strovink, M.
- Suzuki, N.
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- Tokita, K.
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