Spectra of Supernovae

Minkowski, R.

doi:10.1086/125315

Cited by 226 publications

(159 citation statements)

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“…The most prominent object is of course the Crab Nebular (Messier 1), the leftover from the supernova in 1054 (Baade 1942, Mayall & Oort 1942. With extensive observations of bright supernovae Minkowski (1941) introduced two subclasses. Zwicky (1965) refined the classification scheme for supernovae further.…”

Section: Some Early Historymentioning

confidence: 99%

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Supernovae and cosmology

Leibundgut

2007

Gen Relativ Gravit

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The extreme luminosity and their fairly unique temporal behaviour have made supernovae a superb tool to measure distances in the universe. As complex astrophysical events they provide interesting insights into explosion physics, explosive nucleosynthesis, hydrodynamics of the explosion and radiation transport. They are an end product of stellar evolution and provide clues to the stellar composition. Since they can be observed at large distances they have become critical probes to further explore astrophysical effects, like dust properties in external galaxies and the star formation history of galaxies. Some of the astrophysics interferes with the cosmological applications of supernovae. The local velocity field, distorted by the gravitational attraction of the local large scale structure, and the reddening law appear at the moment the major limitations in the accuracy with which cosmological parameters can be determined. These absorption effects can introduce a secondary bias into the observations of the distant supernovae, which needs to be carefully evaluated. Supernovae have been used for the measurement of the Hubble constant, i.e. the current expansion rate of the universe, and the accelerated cosmic expansion directly inferred from the apparent faintness of the distant supernovae.

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Section: Some Early Historymentioning

confidence: 99%

“…In fact, a clear definition of a supernova does not exist. There is a classification scheme, which dates back to Walter Baade, Fritz Zwicky and Robert Minkowski (Baade & Zwicky 1934, Minkowski 1941, 1964. For a modern version with detailed definitions see Filippenko (1997).…”

Section: Introductionmentioning

confidence: 99%

Supernovae and cosmology

Leibundgut

2007

Gen Relativ Gravit

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“…It is customary to divide the SN population into two main subgroups: Type II SNe, which show prominent hydrogen lines in their spectra, and Type I SNe, which do not (Minkowski 1941). Type I SNe are further divided into Type Ia, whose spectra are characterized by a deep absorption trough around 6150 Å , attributed to blueshifted Si ii ll6347, 6371 lines; Type Ib, which show prominent He i lines; and Type Ic, which lack both Si ii and He i (e.g., Matheson et al 2001 and references therein).…”

Section: Supernova Subtypesmentioning

confidence: 99%

Not Color‐Blind: Using Multiband Photometry to Classify Supernovae

Poznanski

Gal‐Yam

Maoz

et al. 2002

PUBL ASTRON SOC PAC

133

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ABSTRACT. Large numbers of supernovae (SNe) have been discovered in recent years, and many more will be found in the near future. Once discovered, further study of a SN and its possible use as an astronomical tool (e.g., as a distance estimator) require knowledge of the SN type. Current classification methods rely almost solely on the analysis of SN spectra to determine their type. However, spectroscopy may not be possible or practical when SNe are faint, numerous, or discovered in archival studies. We present a classification method for SNe based on the comparison of their observed colors with synthetic ones, calculated from a large database of multiepoch optical spectra of nearby events. We discuss the capabilities and limitations of this method. For example, Type Ia SNe at redshifts can be distinguished from most other SN types during the first few z ! 0.1 weeks of their evolution, based on VϪR versus RϪI colors. Type II-P SNe have distinct (very red) colors at late ( days) stages. Broadband photometry through standard Johnson-Cousins UBVRI filters can be useful to t 1 100 classify SNe out to . The use of Sloan Digital Sky Survey (SDSS) ugriz filters allows the extension of z ≈ 0.6 our classification method to even higher redshifts ( ), and the use of infrared bands, to . We z p 0.75 z p 2.5 demonstrate the application of this method to a recently discovered SN from the SDSS. Finally, we outline the observational data required to further improve the sensitivity of the method and discuss prospects for its use on future SN samples. Community access to the tools developed is provided by a dedicated Web site. 5

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“…Among these SNe, many show evidence for hydrogen (H) in their spectra, being historically classified as Type II (Minkowski 1941). For this spectral type, Barbon et al (1979) proposed a subclassification based on the shape of the light curve during the photospheric phase, i.e., the stage between maximum light and the transition to the radioactive tail: Type II "plateau" (II-P) for those SNe that display a nearly constant optical luminosity during ∼100 days and Type II "linear" (II-L) for those that show a linearly declining luminosity.…”

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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Spectra of Supernovae

Cited by 226 publications

References 0 publications

Supernovae and cosmology

Supernovae and cosmology

Not Color‐Blind: Using Multiband Photometry to Classify Supernovae

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

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