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Title:
The Carnegie Supernova Project: First Near-Infrared Hubble Diagram to z ~ 0.7
Authors:
Freedman, Wendy L.; Burns, Christopher R.; Phillips, M. M.; Wyatt, Pamela; Persson, S. E.; Madore, Barry F.; Contreras, Carlos; Folatelli, Gaston; Gonzalez, E. Sergio; Hamuy, Mario; Hsiao, Eric; Kelson, Daniel D.; Morrell, Nidia; Murphy, D. C.; Roth, Miguel; Stritzinger, Maximilian; Sturch, Laura; Suntzeff, Nick B.; Astier, P.; Balland, C.; Bassett, Bruce; Boldt, Luis; Carlberg, R. G.; Conley, Alexander J.; Frieman, Joshua A.; Garnavich, Peter M.; Guy, J.; Hardin, D.; Howell, D. Andrew; Kessler, Richard; Lampeitl, Hubert; Marriner, John; Pain, R.; Perrett, Kathy; Regnault, N.; Riess, Adam G.; Sako, Masao; Schneider, Donald P.; Sullivan, Mark; Wood-Vasey, Michael
Affiliation:
AA(Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101, USA ), AB(Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101, USA ), AC(Carnegie Institution of Washington, Las Campanas Observatory, Colina El Pino, Casilla 601, Chile ), AD(Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101, USA ), AE(Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101, USA ), AF(Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101, USA ), AG(Carnegie Institution of Washington, Las Campanas Observatory, Colina El Pino, Casilla 601, Chile ), AH(Carnegie Institution of Washington, Las Campanas Observatory, Colina El Pino, Casilla 601, Chile ; Universidad de Chile, Departmento de Astronomia, Casilla 36-D, Santiago, Chile ), AI(Carnegie Institution of Washington, Las Campanas Observatory, Colina El Pino, Casilla 601, Chile ), AJ(Universidad de Chile, Departmento de Astronomia, Casilla 36-D, Santiago, Chile ), AK(Department of Physics and Astronomy, University of Victoria, P.O. Box 3055, Stn CSC, Victoria, BC V8W 3P6, Canada ), AL(Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101, USA ), AM(Carnegie Institution of Washington, Las Campanas Observatory, Colina El Pino, Casilla 601, Chile ), AN(Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101, USA ), AO(Carnegie Institution of Washington, Las Campanas Observatory, Colina El Pino, Casilla 601, Chile ), AP(Carnegie Institution of Washington, Las Campanas Observatory, Colina El Pino, Casilla 601, Chile ), AQ(Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101, USA ), AR(Physics Department, Texas A&M University, College Station, TX 77843, USA ), AS(LPNHE, CNRS-IN2P3 and Universités Paris VI & VII, 4 place Jussieu, 75252 Paris Cedex 05, France ), AT(LPNHE, CNRS-IN2P3 and Universités Paris VI & VII, 4 place Jussieu, 75252 Paris Cedex 05, France ; APC, Collège de France, 11 place Marcellin Berthelot, 75005 Paris, France ), AU(Department of Mathematics and Applied Mathematics, University of Cape Town, Rondebosch 7701, South Africa and South African Astronomical Observatory, P.O. Box 9, Observatory 7935, South Africa ), AV(Carnegie Institution of Washington, Las Campanas Observatory, Colina El Pino, Casilla 601, Chile ), AW(Department of Astronomy, University of Toronto, 60 St. George Street, Toronto, ON M5S 3H8, Canada ), AX(Department of Astronomy, University of Toronto, 60 St. George Street, Toronto, ON M5S 3H8, Canada ), AY(Center for Particle Astrophysics, Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USA ; Enrico Fermi Institute, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA ; Department of Astronomy and Astrophysics, The University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA ), AZ(University of Notre Dame, 225 Nieuwland Science, Notre Dame, IN 46556-5670, USA ), BA(LPNHE, CNRS-IN2P3 and Universités Paris VI & VII, 4 place Jussieu, 75252 Paris Cedex 05, France ), BB(LPNHE, CNRS-IN2P3 and Universités Paris VI & VII, 4 place Jussieu, 75252 Paris Cedex 05, France ), BC(Las Cumbres Observatory Global Telescope Network, 6740 Cortona Dr., Suite 102, Goleta, CA 93117, USA ; Department of Physics, University of California, Santa Barbara, Broida Hall, Mail Code 9530, Santa Barbara, CA 93106-9530, USA ), BD(Enrico Fermi Institute, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637, USA ; Kavli Institute for Cosmological Physics, The University of Chicago, 5640 South Ellis Avenue Chicago, IL 60637, USA ), BE(Institute of Cosmology and Gravitation, University of Portsmouth, Portsmouth, P01 3FX, UK ), BF(Center for Particle Astrophysics, Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USA ), BG(LPNHE, CNRS-IN2P3 and Universités Paris VI & VII, 4 place Jussieu, 75252 Paris Cedex 05, France ), BH(Department of Astronomy, University of Toronto, 60 St. George Street, Toronto, ON M5S 3H8, Canada ), BI(LPNHE, CNRS-IN2P3 and Universités Paris VI & VII, 4 place Jussieu, 75252 Paris Cedex 05, France ), BJ(Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA ; Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA ), BK(Department of Physics and Astronomy, University of Pennsylvania, 209 South 33rd Street, Philadelphia, PA 19104, USA ), BL(Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802, USA ), BM(Department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UK ), BN(Department of Physics and Astronomy, 3941 O'Hara Street, University of Pittsburgh, Pittsburgh, PA 15260, USA)
Publication:
The Astrophysical Journal, Volume 704, Issue 2, pp. 1036-1058 (2009). (ApJ Homepage)
Publication Date:
10/2009
Origin:
IOP
ApJ Keywords:
cosmology: observations, distance scale, supernovae: general
DOI:
10.1088/0004-637X/704/2/1036
Bibliographic Code:
2009ApJ...704.1036F

Abstract

The Carnegie Supernova Project (CSP) is designed to measure the luminosity distance for Type Ia supernovae (SNe Ia) as a function of redshift, and to set observational constraints on the dark energy contribution to the total energy content of the universe. The CSP differs from other projects to date in its goal of providing an I-band rest-frame Hubble diagram. Here, we present the first results from near-infrared observations obtained using the Magellan Baade telescope for SNe Ia with 0.1 <z < 0.7. We combine these results with those from the low-redshift CSP at z < 0.1. In this paper, we describe the overall goals of this long-term program, the observing strategy, data reduction procedures, and treatment of systematic uncertainties. We present light curves and an I-band Hubble diagram for this first sample of 35 SNe Ia, and we compare these data to 21 new SNe Ia at low redshift. These data support the conclusion that the expansion of the universe is accelerating. When combined with independent results from baryon acoustic oscillations, these data yield Ω m = 0.27 ± 0.02(statistical) and ΩDE = 0.76 ± 0.13(statistical) ± 0.09(systematic), for the matter and dark energy densities, respectively. If we parameterize the data in terms of an equation of state, w (with no time dependence), assume a flat geometry, and combine with baryon acoustic oscillations, we find that w = -1.05 ± 0.13(statistical) ± 0.09(systematic). The largest source of systematic uncertainty on w arises from uncertainties in the photometric calibration, signaling the importance of securing more accurate photometric calibrations for future supernova cosmology programs. Finally, we conclude that either the dust affecting the luminosities of SNe Ia has a different extinction law (RV = 1.8) than that in the Milky Way (where RV = 3.1), or that there is an additional intrinsic color term with luminosity for SNe Ia, independent of the decline rate. Understanding and disentangling these effects is critical for minimizing the systematic uncertainties in future SN Ia cosmology studies.

This paper includes data gathered with the 6.5 meter Magellan Telescopes located at Las Campanas Observatory, Chile.


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