dc.contributor.author | Rest, Armin Wolfgang | |
dc.contributor.author | Scolnic, D. | |
dc.contributor.author | Foley, R. J. | |
dc.contributor.author | Huber, M. E. | |
dc.contributor.author | Chornock, R. | |
dc.contributor.author | Narayan, Gautham Siddharth | |
dc.contributor.author | Tonry, J. L. | |
dc.contributor.author | Berger, Edo | |
dc.contributor.author | Soderberg, Alicia M. | |
dc.contributor.author | Stubbs, Christopher William | |
dc.contributor.author | Riess, A. | |
dc.contributor.author | Kirshner, Robert P. | |
dc.contributor.author | Smartt, S. J. | |
dc.contributor.author | Schlafly, E. | |
dc.contributor.author | Rodney, S. | |
dc.contributor.author | Botticella, M. T. | |
dc.contributor.author | Brout, D. | |
dc.contributor.author | Challis, P. | |
dc.contributor.author | Czekala, Ian Philip | |
dc.contributor.author | Drout, Maria Rebecca | |
dc.contributor.author | Hudson, M. J. | |
dc.contributor.author | Kotak, R. | |
dc.contributor.author | Leibler, C. | |
dc.contributor.author | Lunnan, Ragnhild | |
dc.contributor.author | Marion, G. H. | |
dc.contributor.author | McCrum, M. | |
dc.contributor.author | Milisavljevic, D. | |
dc.contributor.author | Pastorello, A. | |
dc.contributor.author | Sanders, Nathan Edward | |
dc.contributor.author | Smith, K. | |
dc.contributor.author | Stafford, E. | |
dc.contributor.author | Thilker, D. | |
dc.contributor.author | Valenti, S. | |
dc.contributor.author | Wood-Vasey, W. M. | |
dc.contributor.author | Zheng, Z. | |
dc.contributor.author | Burgett, W. S. | |
dc.contributor.author | Chambers, K. C. | |
dc.contributor.author | Denneau, L. | |
dc.contributor.author | Draper, P. W. | |
dc.contributor.author | Flewelling, H. | |
dc.contributor.author | Hodapp, K. W. | |
dc.contributor.author | Kaiser, N. | |
dc.contributor.author | Kudritzki, R.-P. | |
dc.contributor.author | Magnier, E. A. | |
dc.contributor.author | Metcalfe, N. | |
dc.contributor.author | Price, P. A. | |
dc.contributor.author | Sweeney, W. | |
dc.contributor.author | Wainscoat, R. | |
dc.contributor.author | Waters, C. | |
dc.date.accessioned | 2015-07-02T19:20:07Z | |
dc.date.issued | 2014 | |
dc.identifier.citation | Rest, A., D. Scolnic, R. J. Foley, M. E. Huber, R. Chornock, G. Narayan, J. L. Tonry, et al. 2014. “Cosmological Constraints from Measurements of Type Ia Supernovae Discovered during the First 1.5 yr of the Pan-STARRS1 Survey.” The Astrophysical Journal 795, no. 1: 44. doi:10.1088/0004-637x/795/1/44 | en_US |
dc.identifier.issn | 1538-4357 | en_US |
dc.identifier.uri | http://nrs.harvard.edu/urn-3:HUL.InstRepos:16953381 | |
dc.description.abstract | We present griz P1 light curves of 146 spectroscopically confirmed Type Ia supernovae (SNe Ia; 0.03 < z < 0.65) discovered during the first 1.5 yr of the Pan-STARRS1 Medium Deep Survey. The Pan-STARRS1 natural photometric system is determined by a combination of on-site measurements of the instrument response function and observations of spectrophotometric standard stars. We find that the systematic uncertainties in the photometric system are currently 1.2% without accounting for the uncertainty in the Hubble Space Telescope Calspec definition of the AB system. A Hubble diagram is constructed with a subset of 113 out of 146 SNe Ia that pass our light curve quality cuts. The cosmological fit to 310 SNe Ia (113 PS1 SNe Ia + 222 light curves from 197 low-z SNe Ia), using only supernovae (SNe) and assuming a constant dark energy equation of state and flatness, yields $w=-1.120^{+0.360}_{-0.206}\hbox{(Stat)} ^{+0.269}_{-0.291}\hbox{(Sys)}$. When combined with BAO+CMB(Planck)+H 0, the analysis yields $\Omega _{\rm M}=0.280^{+0.013}_{-0.012}$ and $w=-1.166^{+0.072}_{-0.069}$ including all identified systematics. The value of w is inconsistent with the cosmological constant value of –1 at the 2.3σ level. Tension endures after removing either the baryon acoustic oscillation (BAO) or the H 0 constraint, though it is strongest when including the H 0 constraint. If we include WMAP9 cosmic microwave background (CMB) constraints instead of those from Planck, we find $w=-1.124^{+0.083}_{-0.065}$, which diminishes the discord to <2σ. We cannot conclude whether the tension with flat ΛCDM is a feature of dark energy, new physics, or a combination of chance and systematic errors. The full Pan-STARRS1 SN sample with ~three times as many SNe should provide more conclusive results. | en_US |
dc.description.sponsorship | Astronomy | en_US |
dc.language.iso | en_US | en_US |
dc.publisher | IOP Publishing | en_US |
dc.relation.isversionof | doi:10.1088/0004-637x/795/1/44 | en_US |
dc.relation.hasversion | http://arxiv.org/pdf/1310.3828v2.pdf | en_US |
dash.license | OAP | |
dc.subject | cosmological parameters | en_US |
dc.subject | cosmology: observations | en_US |
dc.subject | dark energy | en_US |
dc.subject | supernovae: general | en_US |
dc.title | Cosmological Constraints from Measurements of Type Ia Supernovae Discovered during the First 1.5 yr of the Pan-STARRS1 Survey | en_US |
dc.type | Journal Article | en_US |
dc.description.version | Accepted Manuscript | en_US |
dc.relation.journal | The Astrophysical Journal | en_US |
dash.depositing.author | Stubbs, Christopher William | |
dc.date.available | 2015-07-02T19:20:07Z | |
dc.identifier.doi | 10.1088/0004-637x/795/1/44 | * |
dash.authorsordered | false | |
dash.contributor.affiliated | Rest, Armin | |
dash.contributor.affiliated | Lunnan, R | |
dash.contributor.affiliated | Czekala, Ian | |
dash.contributor.affiliated | Narayan, Gautham | |
dash.contributor.affiliated | Stubbs, Christopher | |
dash.contributor.affiliated | Drout, Maria Rebecca | |
dash.contributor.affiliated | Kirshner, Robert | |
dash.contributor.affiliated | Soderberg, Alicia | |
dash.contributor.affiliated | Berger, Edo | |
dash.contributor.affiliated | Sanders, Nathan Edward | |