Abstract
Since Type Ia supernovae (SNe) explode in galaxies, they can, in principle, be used as the same tracer of the large-scale structure as their hosts to measure baryon acoustic oscillations (BAOs). To realize this, one must obtain a dense integrated sampling of SNe over a large fraction of the sky, which may only be achievable photometrically with future projects such as the Large Synoptic Survey Telescope. The advantage of SN BAOs is that SNe have more uniform luminosities and more accurate photometric redshifts than galaxies, but the disadvantage is that they are transitory and hard to obtain in large number at high redshift. We find that a half-sky photometric SN survey to redshift z = 0.8 is able to measure the baryon signature in the SN spatial power spectrum. Although dark energy constraints from SN BAOs are weak, they can significantly improve the results from SN luminosity distances of the same data, and the combination of the two is no longer sensitive to cosmic microwave background priors.
| Original language | English (US) |
|---|---|
| Journal | Astrophysical Journal |
| Volume | 675 |
| Issue number | 1 PART 2 |
| DOIs | |
| State | Published - 2008 |
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Keywords
- Cosmological parameters
- Distance scale
- Large-scale structure of universe
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science
Cite this
Measuring baryon acoustic oscillations with millions of supernovae. / Zhan, Hu; Wang, Lifan; Pinto, Philip A; Tyson, J. Anthony.
In: Astrophysical Journal, Vol. 675, No. 1 PART 2, 2008.Research output: Contribution to journal › Article
}
TY - JOUR
T1 - Measuring baryon acoustic oscillations with millions of supernovae
AU - Zhan, Hu
AU - Wang, Lifan
AU - Pinto, Philip A
AU - Tyson, J. Anthony
PY - 2008
Y1 - 2008
N2 - Since Type Ia supernovae (SNe) explode in galaxies, they can, in principle, be used as the same tracer of the large-scale structure as their hosts to measure baryon acoustic oscillations (BAOs). To realize this, one must obtain a dense integrated sampling of SNe over a large fraction of the sky, which may only be achievable photometrically with future projects such as the Large Synoptic Survey Telescope. The advantage of SN BAOs is that SNe have more uniform luminosities and more accurate photometric redshifts than galaxies, but the disadvantage is that they are transitory and hard to obtain in large number at high redshift. We find that a half-sky photometric SN survey to redshift z = 0.8 is able to measure the baryon signature in the SN spatial power spectrum. Although dark energy constraints from SN BAOs are weak, they can significantly improve the results from SN luminosity distances of the same data, and the combination of the two is no longer sensitive to cosmic microwave background priors.
AB - Since Type Ia supernovae (SNe) explode in galaxies, they can, in principle, be used as the same tracer of the large-scale structure as their hosts to measure baryon acoustic oscillations (BAOs). To realize this, one must obtain a dense integrated sampling of SNe over a large fraction of the sky, which may only be achievable photometrically with future projects such as the Large Synoptic Survey Telescope. The advantage of SN BAOs is that SNe have more uniform luminosities and more accurate photometric redshifts than galaxies, but the disadvantage is that they are transitory and hard to obtain in large number at high redshift. We find that a half-sky photometric SN survey to redshift z = 0.8 is able to measure the baryon signature in the SN spatial power spectrum. Although dark energy constraints from SN BAOs are weak, they can significantly improve the results from SN luminosity distances of the same data, and the combination of the two is no longer sensitive to cosmic microwave background priors.
KW - Cosmological parameters
KW - Distance scale
KW - Large-scale structure of universe
UR - http://www.scopus.com/inward/record.url?scp=62649088531&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=62649088531&partnerID=8YFLogxK
U2 - 10.1086/529546
DO - 10.1086/529546
M3 - Article
AN - SCOPUS:62649088531
VL - 675
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 1 PART 2
ER -