| Original Articles |
|
|
|
|
Comparison of Supernovae Datasets Constraints on Dark Energy |
| ZHANG Cheng-Wu;XU Li-Xin;CHANG Bao-Rong;LIU Hong-Ya |
| School of Physics and Optoelectronic Technology, Dalian University of Technology, Dalian 116024 |
|
| Cite this article: |
|
ZHANG Cheng-Wu, XU Li-Xin, CHANG Bao-Rong et al 2007 Chin. Phys. Lett. 24 1425-1428 |
|
|
|
|
Abstract Cosmological measurements suggest that our universe contains a dark energy component. In order to study the dark energy evolution, we constrain a parameterized dark energy equation of state w(z)=w0 + w1 z/1+z using the recent observational datasets: 157 Gold type Ia supernovae and the newly released 182 Gold type Ia supernovae by the maximum likelihood method. It is found that the best fit w(z) crosses -1 in the past and the present best fit value of w(0)<-1 obtained from 157 Gold-type Ia supernovae. The crossing of -1 is not realized and w0=-1 is not ruled out in 1σ confidence level for the 182 Gold-type Ia supernovae. It is also found that the range of parameter w0 is wide even in 1σ confidence level and the best fit w(z) is sensitive to the prior of Ωm.
|
| Keywords:
98.80.Es
98.80.-k
95.36.+x
|
|
|
Received: 13 January 2007
Published: 23 April 2007
|
|
| PACS: |
98.80.Es
|
(Observational cosmology (including Hubble constant, distance scale, cosmological constant, early Universe, etc))
|
| |
98.80.-k
|
(Cosmology)
|
| |
95.36.+x
|
(Dark energy)
|
|
|
|
|
|
[1] Riess A G et al 1998 Astron. J. 116 1009 astro-ph/9805201
[2] Perlmutter S et al 1999 Astrophys. J. 517 565astro-ph/9812133
[3]Spergel D N et al 2003 Astrophy. J. Suppl. 148175 astro-ph/0302209
[4] Spergel D N et al 2006 arXiv astro-ph/0603449
[5] Peebles P J E and Ratra B 2003 Rev. Mod. Phys. 75559 (astro-ph/0207347)
[6] Zlatev I, Wang L M and Steinhardt P J 1999 Phys. Rev.Lett. 82 896
[7] Caldwell R R, Kamionkowski M and Weinberg N N 2003 Phys.Rev. Lett. 91 071301
[8] Feng B, Wang X L and Zhang X M 2005 Phys. Lett. B 607 35
[9] Armendariz-Picon C, Damour T and Mukhanov V 1999 Phys.Lett. B 458 209
[10] Padmanabhan T 2002 Phys. Rev. D 66 021301
[11] Riess A G et al 2004 Astrophys. J. 607 665astro-ph/0402512
[12] Riess A G et al 2006 arXiv astro-ph/0611572
[13] Chevallier M and Polarski D 2001 Int. J. Mod. Phys. D 10 213 (gr-qc/0009008)
[14] Linder E V 2003 Phys. Rev. Lett. 90 091301astro-ph/0208512
[15] Choudhury T R and Padmanabhan T 2005 Astron.Astrophys. 429 807 (astro-ph/0311622)
[16] Nesseris S and Perivolaropoulos L 2005 Phys. Rev. D 72123519 (astro-ph/0511040)
[17] Lewis A and Bridle S 2002 Phys. Rev. D 66 103511
[18] Alam U et al 2004 ArXiv astro-ph/0406672
[19] Eisenstein D J et al 2005 Astrophys. J. 633 560
[20] Allen S W et al 2004 Mon. Not. R. Astron. Soc. 353 457astro-ph/0405340
[21] Verde L et al 2002 Mon. Not. R. Astron. Soc. 335 432astro-ph/0112161
[22] Http://camb.info
[23] Http://cosmologist.info/cosmomc
[24] Http://cosmocoffee.info |
|
Viewed |
|
|
|
Full text
|
|
|
|
|
Abstract
|
|
|
|
|
