SN 2009E: a faint clone of SN 1987A

Pastorello, A.; Pumo, M. L.; Navasardyan, H.; Zampieri, L.; Turatto, M.; Sollerman, J.; Taddia, F.; Kankare, E.; Mattila, S.; Nicolas, J.; Prosperi, E.; Delgado, Adolfo; Taubenberger, S.; Boles, T.; Bachini, Mauro; Benetti, S.; Bufano, F.; Cappellaro, E.; Cason, A. D.; Cetrulo, G.; Ergon, M.; Harutyunyan, A.; Howerton, S.; Hurst, G. M.; Patat, F.; Stritzinger, M. D.; Strolger, Louis-Gregory; Wells, William D.

doi:10.1051/0004-6361/201118112

Cited by 86 publications

(165 citation statements)

References 73 publications

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“…Figure 4 shows the maximum likelihood fit of this revised SN 1987A model to the observed SN Refsdal data in all bands (including the optical bands from ACS/WFC). From this fit we find that the color-temperature of SNRefsdal around maximum light is T≈5300 K. This is consistent with the range of temperatures (∼4000-9000 K) seen for other SNe1987A-like events at the same epoch (Pastorello et al 2005(Pastorello et al , 2012Taddia et al 2012). As discussed in Kelly et al (2015a), the SNRefsdal rest-frame optical colors (with B − V ≈ 0.5 mag) are slightly bluer than most SN1987A-like objects.…”

Section: Maximally Constrained Model Fitsupporting

confidence: 88%

“…In this case we assume that all bands (F160W, F125W, and F105W) have the same intrinsic light curve shape, meaning that they would reach peak brightness at the same epoch. This is not a good assumption for SN 1987A-like explosions, which tend to reach peak brightness much earlier in bluer bands (e.g., Pastorello et al 2012;Taddia et al 2012). Using both the net posterior probability and the Bayesian Information Criterion (Schwarz 1978) as metrics to evaluate the fitness of these simpler models, we found that we consistently get a better fit when using the more complex alternative.…”

Section: Flexible Curve Fitting Resultsmentioning

confidence: 99%

“…We constructed templates based on the prototype SN 1987A itself (Hamuy & Suntzeff 1990), and also using the 87A-like events SN 1998A (Woodings et al 1998;Pastorello et al 2005), SN 2000cb (Hamuy et al 2001;Kleiser et al 2011), SN 2006V, and SN 2006au (Taddia et al 2012, and SN 2009E (Pastorello et al 2012). All of these template SNe have well-sampled light curve coverage in the B, V, and R bands extending over at least 80 days in the rest-frame.…”

Section: Template Fitting Methodsmentioning

confidence: 99%

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Sn Refsdal: Photometry and Time Delay Measurements of the First Einstein Cross Supernova

Rodney

Strolger

Kelly

et al. 2016

ApJ

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102

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We present the first year of Hubble Space Telescope imaging of the unique supernova (SN) "Refsdal," a gravitationally lensed SN at z=1.488±0.001 with multiple images behind the galaxy cluster MACS J1149.6 +2223. The first four observed images of SN Refsdal (images S1-S4) exhibited a slow rise (over ∼150 days) to reach a broad peak brightness around 2015 April 20. Using a set of light curve templates constructed from SN 1987A-like peculiar Type II SNe, we measure time delays for the four images relative to S1 of 4±4 (for S2), 2±5 (S3), and 24±7 days (S4). The measured magnification ratios relative to S1 are 1.15±0.05 (S2), 1.01±0.04 (S3), and 0.34±0.02 (S4). None of the template light curves fully captures the photometric behavior of SN Refsdal, so we also derive complementary measurements for these parameters using polynomials to represent the intrinsic light curve shape. These more flexible fits deliver fully consistent time delays of 7±2 (S2), 0.6±3 (S3), and 27±8 days (S4). The lensing magnification ratios are similarly consistent, measured as 1.17±0.02 (S2), 1.00±0.01 (S3), and 0.38±0.02 (S4). We compare these measurements against published predictions from lens models, and find that the majority of model predictions are in very good agreement with our measurements. Finally, we discuss avenues for future improvement of time delay measurements-both for SN Refsdal and for other strongly lensed SNe yet to come.

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Section: Maximally Constrained Model Fitsupporting

confidence: 88%

Section: Flexible Curve Fitting Resultsmentioning

confidence: 99%

Section: Template Fitting Methodsmentioning

confidence: 99%

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Sn Refsdal: Photometry and Time Delay Measurements of the First Einstein Cross Supernova

Rodney

Strolger

Kelly

et al. 2016

ApJ

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102

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“…Also the code computes the fallback of material on the central compact object and consequently determines the amount of 56 Ni in the ejected envelope at late times. The code has been widely used to model the observations of core-collapse SNe (e.g., Pastorello et al 2012;Dall'Ora et al 2014;Spiro et al 2014;Takáts et al 2014), having also the capability of simulating the bolometric lightcurve and the time evolution of the photospheric velocity and temperature.…”

Section: Modeling the Post-explosion Evolution Of The Snmentioning

confidence: 99%

Modeling SNR Cassiopeia a From the Supernova Explosion to Its Current Age: The Role of Post-Explosion Anisotropies of Ejecta

Orlando

Miceli

Pumo

et al. 2016

ApJ

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113

138

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The remnants of core-collapse supernovae (SNe) have complex morphologies that may reflect asymmetries and structures developed during the progenitor SN explosion. Here we investigate how the morphology of the supernova remnant Cassiopeia A (Cas A) reflects the characteristics of the progenitor SN with the aim of deriving the energies and masses of the post-explosion anisotropies responsible for the observed spatial distribution of Fe and Si/S. We model the evolution of Cas A from the immediate aftermath of the progenitor SN to the three-dimensional interaction of the remnant with the surrounding medium. The post-explosion structure of the ejecta is described by small-scale clumping of material and larger-scale anisotropies. The hydrodynamic multi-species simulations consider an appropriate post-explosion isotopic composition of the ejecta. The observed average expansion rate and shock velocities can be well reproduced by models with ejecta mass M ej ≈4M e and explosion energy E SN ≈2.3×10 51 erg. The post-explosion anisotropies (pistons) reproduce the observed distributions of Fe and Si/ S if they had a total mass of ≈0.25 M e and a total kinetic energy of ≈1.5×10 50 erg. The pistons produce a spatial inversion of ejecta layers at the epoch of Cas A, leading to the Si/S-rich ejecta physically interior to the Fe-rich ejecta. The pistons are also responsible for the development of the bright rings of Si/S-rich material which form at the intersection between the reverse shock and the material accumulated around the pistons during their propagation. Our result supports the idea that the bulk of asymmetries observed in Cas A are intrinsic to the explosion.

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“…Two other subclasses have been introduced based on spectral characteristics: IIn for SNe that show narrow H emission lines (Schlegel 1990), and IIb for those that show H in early spectra that soon disappear (Woosley et al 1987). Finally, a few SNe do not fit into the aforementioned subclasses, but show characteristics similar to SN 1987A (e.g., Kleiser et al 2011;Taddia et al 2012;Pastorello et al 2012). More recently, Anderson et al (2014) performed a photometric analysis of a sample of 116 SNe II.…”

Section: Introductionmentioning

confidence: 99%

Photospheric Magnitude Diagrams for Type Ii Supernovae: A Promising Tool to Compute Distances

Rodríguez

Clocchiatti

Hamuy

2014

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We develop an empirical color-based standardization for Type II supernovae (SNe II), equivalent to the classical surface brightness method given in Wesselink. We calibrate this standardization using SNe II with host galaxy distances measured using Cepheids, and a well-constrained shock breakout epoch and extinction due to the host galaxy. We estimate the reddening with an analysis of the B −V versus V −I color-color curves, similar to that of Natali et al. With four SNe II meeting the above requirements, we build a photospheric magnitude versus color diagram (similar to an H-R diagram) with a dispersion of 0.29 mag. We also show that when using time since shock breakout instead of color as the independent variable, the same standardization gives a dispersion of 0.09 mag. Moreover, we show that the above time-based standardization corresponds to the generalization of the standardized candle method of Hamuy & Pinto for various epochs throughout the photospheric phase. To test the new tool, we construct Hubble diagrams for different subsamples of 50 low-redshift (cz < 10 4 km s −1 ) SNe II. For 13 SNe within the Hubble flow (cz CMB > 3000 km s −1 ) and with a well-constrained shock breakout epoch we obtain values of 68-69 km s −1 Mpc −1 for the Hubble constant and a mean intrinsic scatter of 0.12 mag or 6% in relative distances.

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SN 2009E: a faint clone of SN 1987A

Cited by 86 publications

References 73 publications

Sn Refsdal: Photometry and Time Delay Measurements of the First Einstein Cross Supernova

Sn Refsdal: Photometry and Time Delay Measurements of the First Einstein Cross Supernova

Modeling SNR Cassiopeia a From the Supernova Explosion to Its Current Age: The Role of Post-Explosion Anisotropies of Ejecta

Photospheric Magnitude Diagrams for Type Ii Supernovae: A Promising Tool to Compute Distances

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