A Type II Supernova Hubble Diagram from the CSP-I, SDSS-II, and SNLS Surveys

Article, Preprint English OPEN
de Jaeger, T. ; González-Gaitán, S. ; Hamuy, M. ; Galbany, L. ; Anderson, J. P. ; Phillips, M. M. ; Stritzinger, M. D. ; Carlberg, R. G. ; Sullivan, M. ; Gutiérrez, C. P. ; Hook, I. M. ; Howell, D. Andrew ; Hsiao, E. Y. ; Kuncarayakti, H. ; Ruhlmann-Kleider, V. ; Folatelli, G. ; Pritchet, C. ; Basa, S. (2017)
  • Publisher: IOP Publishing
  • Related identifiers: doi: 10.3847/1538-4357/835/2/166, doi: 10.3847/1538-4357/835/2/166/meta
  • Subject: general [supernovae] | Galaxies | Redshifts | Ciencias Físicas | distances and redshifts [galaxies] | Supernovae | Distances (galaxias) | distance scale | Astronomía | Astrophysics - Cosmology and Nongalactic Astrophysics | CIENCIAS NATURALES Y EXACTAS

The coming era of large photometric wide-field surveys will increase the detection rate of supernovae by orders of magnitude. Such numbers will restrict spectroscopic follow-up in the vast majority of cases, and hence new methods based solely on photometric data must be developed. Here, we construct a complete Hubble diagram of Type II supernovae (SNe II) combining data from three different samples: the Carnegie Supernova Project-I, the Sloan Digital Sky Survey II SN, and the Supernova Legacy Survey. Applying the Photometric Color Method (PCM) to 73 SNe II with a redshift range of 0.01-0.5 and with no spectral information, we derive an intrinsic dispersion of 0.35 mag. A comparison with the Standard Candle Method (SCM) using 61 SNe II is also performed and an intrinsic dispersion in the Hubble diagram of 0.27 mag, i.e., 13% in distance uncertainties, is derived. Due to the lack of good statistics at higher redshifts for both methods, only weak constraints on the cosmological parameters are obtained. However, assuming a flat universe and using the PCM, we derive the universes matter density: m= 0.32 m+0.30 - 0.21 providing a new independent evidence for dark energy at the level of two sigma. Fil: Jaeger, T. De. Millennium Institute Of Astrophysics; Chile. University of California at Berkeley; Estados Unidos. Universidad de Chile; Chile Fil: González Gaitán, S.. Millennium Institute Of Astrophysics; Chile. Universidad de Chile; Chile Fil: Hamuy, M.. Universidad de Chile; Chile. Millennium Institute Of Astrophysics; Chile Fil: Galbany, L.. University of Pittsburgh at Johnstown; Estados Unidos. University of Pittsburgh; Estados Unidos Fil: Anderson, J. P.. European Southern Observatory Santiago; Chile Fil: Phillips, M. M.. Las Campanas Observatory; Chile Fil: Stritzinger, M. D.. University Aarhus; Dinamarca Fil: Carlberg, R. G.. University of Toronto; Canadá Fil: Sullivan, M.. University of Southampton; Reino Unido Fil: Gutiérrez, C. P.. European Southern Observatory Santiago; Chile. Millennium Institute Of Astrophysics; Chile. Universidad de Chile; Chile Fil: Hook, I. M.. Lancaster University; Reino Unido Fil: Howell, D. Andrew. Las Cumbres Observatory Global Telescope Network; Estados Unidos. University Of California, Santa Barbara; Estados Unidos Fil: Hsiao, E. Y.. Las Campanas Observatory; Chile. University Aarhus; Dinamarca. Florida State University; Estados Unidos Fil: Kuncarayakti, H.. Universidad de Chile; Chile. Millennium Institute Of Astrophysics; Chile Fil: Ruhlmann Kleider, V.. Cea Saclay; Francia Fil: Folatelli, Gaston. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata. Instituto de Astrofísica La Plata. Universidad Nacional de La Plata. Facultad de Ciencias Astronómicas y Geofísicas. Instituto de Astrofísica La Plata; Argentina Fil: Pritchet, C.. University Of Victoria; Canadá Fil: Basa, S.. Laboratoire D'astrophysique de Marseille; Francia
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