Spectrophotometric time series of SN 2011fe from the Nearby Supernova Factory
R. PereiraUniversité de Lyon 1, France, CNRS/IN2P3, Institut de Physique Nucléaire de Lyon, 69622 Villeurbanne Cedex, FranceR. C. ThomasComputational Cosmology Center, Computational Research Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road MS 50B-4206, Berkeley, CA, 94611, USAG. AlderingPhysics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USAP. AntilogusLaboratoire de Physique Nucléaire et des Hautes Énergies, Université Pierre et Marie Curie Paris 6, Université Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu, 75252 Paris Cedex 05, FranceC. BaltayDepartment of Physics, Yale University, New Haven, CT 06520-8121, USAS. Benitez-HerreraMax-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching bei München, GermanyS. BongardLaboratoire de Physique Nucléaire et de Hautes ÉnergiesC. ButonPhysikalisches Institut, Universität Bonn, Nußallee 12, 53115 Bonn, GermanyA. CantoLaboratoire de Physique Nucléaire et des Hautes Énergies, Université Pierre et Marie Curie Paris 6, Université Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu, 75252 Paris Cedex 05, FranceF. Cellier-HolzemLaboratoire de Physique Nucléaire et des Hautes Énergies, Université Pierre et Marie Curie Paris 6, Université Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu, 75252 Paris Cedex 05, FranceJ. ChenTsinghua Center for Astrophysics, Tsinghua University, Beijing 100084, PR ChinaM. ChildressDepartment of Physics, University of California Berkeley, 366 LeConte Hall MC 7300, Berkeley, CA, 94720-7300, USAN. ChotardNational Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, PR ChinaY. CopinUniversité de Lyon 1, France, CNRS/IN2P3, Institut de Physique Nucléaire de Lyon, 69622 Villeurbanne Cedex, FranceH. FakhouriDepartment of Physics, University of California Berkeley, 366 LeConte Hall MC 7300, Berkeley, CA, 94720-7300, USAM. FinkMax-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching bei München, GermanyD. FouchezCentre de Physique des Particules de Marseille, Aix-Marseille Université, CNRS/IN2P3, 163, avenue de Luminy, Case 902, 13288 Marseille Cedex 09, FranceÉ. GanglerUniversité de Lyon 1, France, CNRS/IN2P3, Institut de Physique Nucléaire de Lyon, 69622 Villeurbanne Cedex, FranceJ. GuyLaboratoire de Physique Nucléaire et des Hautes Énergies, Université Pierre et Marie Curie Paris 6, Université Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu, 75252 Paris Cedex 05, FranceW. HillebrandtMax-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching bei München, GermanyE. Y. HsiaoPhysics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USAM. KerschhagglPhysikalisches Institut, Universität Bonn, Nußallee 12, 53115 Bonn, GermanyM. KowalskiPhysikalisches Institut, Universität Bonn, Nußallee 12, 53115 Bonn, GermanyMarkus KromerMax-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching bei München, GermanyJ. NordinPhysics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USAP. NugentComputational Cosmology Center, Computational Research Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road MS 50B-4206, Berkeley, CA, 94611, USAK. PaechPhysikalisches Institut, Universität Bonn, Nußallee 12, 53115 Bonn, GermanyR. PainLaboratoire de Physique Nucléaire et des Hautes Énergies, Université Pierre et Marie Curie Paris 6, Université Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu, 75252 Paris Cedex 05, FranceÉ. PécontalCentre de Recherche Astronomique de Lyon, Université Lyon 1, 9 avenue Charles André, 69561 Saint Genis Laval Cedex, FranceS. PerlmutterDepartment of Physics, University of California Berkeley, 366 LeConte Hall MC 7300, Berkeley, CA, 94720-7300, USAD. RabinowitzDepartment of Physics, Yale University, New Haven, CT 06520-8121, USAM. RigaultUniversité de Lyon 1, France, CNRS/IN2P3, Institut de Physique Nucléaire de Lyon, 69622 Villeurbanne Cedex, FranceK. RungePhysics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USAC. SaundersPhysics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USAG. SmadjaUniversité de Lyon 1, France, CNRS/IN2P3, Institut de Physique Nucléaire de Lyon, 69622 Villeurbanne Cedex, FranceC. TaoCentre de Physique des Particules de Marseille, Aix-Marseille Université, CNRS/IN2P3, 163, avenue de Luminy, Case 902, 13288 Marseille Cedex 09, FranceS. TaubenbergerMax-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85741 Garching bei München, GermanyA. TilquinCentre de Physique des Particules de Marseille, Aix-Marseille Université, CNRS/IN2P3, 163, avenue de Luminy, Case 902, 13288 Marseille Cedex 09, FranceChengyuan WuLaboratoire de Physique Nucléaire et des Hautes Énergies, Université Pierre et Marie Curie Paris 6, Université Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu, 75252 Paris Cedex 05, France
2013en
ABI
Аннотация
We present 32 epochs of optical (3300−9700 Å) spectrophotometric observations of the nearby quintessential “normal” type Ia supernova (SN Ia) SN 2011fe in the galaxy M101, extending from −15 to +97 d with respect to B-band maximum, obtained by the Nearby Supernova Factory collaboration. SN 2011fe is the closest (μ = 29.04) and brightest (Bmax = 9.94 mag) SN Ia observed since the advent of modern large scale programs for the intensive periodic followup of supernovae. Both synthetic light curve measurements and spectral feature analysis attest to the normality of SN 2011fe. There is very little evidence for reddening in its host galaxy. The homogeneous calibration, intensive time sampling, and high signal-to-noise ratio of the data set make it unique. Thus it is ideal for studying the physics of SN Ia explosions in detail, and for furthering the use of SNe Ia as standardizable candles for cosmology. Several such applications are shown, from the creation of a bolometric light curve and measurement of the 56Ni mass, to the simulation ofdetection thresholds for unburned carbon, direct comparisons with other SNe Ia, and existing spectral templates.
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