Spectropolarimetric observations of supernovae

Filippenko, A. V.; Leonard, Douglas C.

doi:10.1017/cbo9780511536236.003

Cited by 9 publications

(3 citation statements)

References 52 publications

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“…This group of supernovae includes also SN 1991T, SN 1997br (Li et al 1999), and SN 2000cx (Li et al 2001, not in our sample but well observed. However, it should be noted that the spectroscopically SN 1991T-like event -SN 1995ac (Filippenko & Leonard 1995) does not show the bump that defines this group.…”

Section: The Shapes Of the Color-magnitude Diagrams Of Type Ia Supern...mentioning

confidence: 84%

Multicolor Light Curves of Type Ia Supernovae on the Color‐Magnitude Diagram: A Novel Step toward More Precise Distance and Extinction Estimates

Wang

Goldhaber

Aldering

et al. 2003

ApJ

116

139

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We show empirically that fits to the color-magnitude relation of Type Ia supernovae after optical maximum can provide accurate relative extragalactic distances. We report the discovery of an empirical color relation for Type Ia light curves: During much of the first month past maximum, the magnitudes of Type Ia supernovae defined at a given value of color index have a very small magnitude dispersion; moreover, during this period the relation between B magnitude and B−V color (or B−R or B−I color) is strikingly linear, to the accuracy of existing well-measured data. These linear relations can provide robust distance estimates, in particular, by using the magnitudes when the supernova reaches a given color. After correction for light curve strech factor or decline rate, the dispersion of the magnitudes taken at the intercept of the linear color-magnitude relation are found to be around 0 m .08 for the sub-sample of supernovae with (B max − V max ) ≤ 0 m .05, and around 0 m .11 for the sub-sample with (B max −V max ) ≤ 0 m .2. This small dispersion is consistent with being mostly due to observational errors. The method presented here and the conventional light curve fitting methods can be combined to further improve statistical dispersions of distance estimates. It can be combined with the magnitude at maximum to deduce dust extinction. The slopes of the color-magnitude relation may also be used to identify intrinsically different SN Ia systems. The method provides a tool that is fundamental to using SN Ia to estimate cosmological parameters such as the Hubble constant and the mass and dark energy content of the universe.

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Section: The Shapes Of the Color-magnitude Diagrams Of Type Ia Supern...mentioning

confidence: 84%

Multicolor Light Curves of Type Ia Supernovae on the Color‐Magnitude Diagram: A Novel Step toward More Precise Distance and Extinction Estimates

Wang

Goldhaber

Aldering

et al. 2003

ApJ

116

139

View full text Add to dashboard Cite

show abstract

“…Type Ic supernovae (SNe) are H-/He-poor core-collapse supernovae Clocchiatti & Wheeler (1997); Filippenko (1997); Matheson et al (2001); Modjaz et al (2016). Significant diversity can be found among the He-poor SNe whose data have been published (Bianco et al 2014;Taddia et al 2015;Lyman et al 2016;Prentice et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Modelling the Type Ic SN 2004aw: a moderately energetic explosion of a massive C+O star without a GRB

Mazzali

Sauer

Pian

et al. 2017

Monthly Notices of the Royal Astronomical Society

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An analysis of the Type Ic supernova (SN) 2004aw is performed by means of models of the photospheric and nebular spectra and of the bolometric light curve. SN 2004aw is shown not to be "broad-lined", contrary to previous claims, but rather a "fast-lined" SN Ic. The spectral resemblance to the narrow-lined Type Ic SN 1994I, combined with the strong nebular [O i] emission and the broad light curve, point to a moderately energetic explosion of a massive C+O star. The ejected 56 Ni mass is ≈ 0.20 M ⊙ . The ejecta mass as constrained by the models is ∼ 3 − 5 M ⊙ , while the kinetic energy is estimated as E K ∼ 3 − 6 × 10 51 ergs. The ratio E K /M ej , the specific energy which influences the shape of the spectrum, is therefore ≈ 1. The corresponding zero-age main-sequence mass of the progenitor star may have been ∼ 23 − 28 M ⊙ . Tests show that a flatter outer density structure may have caused a broad-lined spectrum at epochs before those observed without affecting the later epochs when data are available, implying that our estimate of E K is a lower limit. SN 2004aw may have been powered by either a collapsar or a magnetar, both of which have been proposed for gamma-ray burst-supernovae. Evidence for this is seen in the innermost layers, which appear to be highly aspherical as suggested by the nebular line profiles. However, any engine was not extremely powerful, as the outer ejecta are more consistent with a spherical explosion and no gamma-ray burst was detected in coincidence with SN 2004aw.

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“…In addition to continuum polarization, which points to global asymmetries, line polarization features can provide specific clues to the nature of SN ejecta and their surrounding circumstellar material (CSM; Leonard et al 2000aKawabata et al 2002;Kasen et al 2003;Wang et al 2003aWang et al , 2003bWang et al ,. 2004Filippenko & Leonard 2004;Chornock et al 2006;.…”

Section: Introductionmentioning

confidence: 99%

The Dual‐Axis Circumstellar Environment of the Type IIn Supernova 1997eg

Hoffman

Leonard

Chornock

et al. 2008

Astrophysical Journal

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We present multi-epoch spectral and spectropolarimetric observations of the Type IIn supernova (SN ) 1997eg that indicate the presence of a flattened disklike concentration of circumstellar material surrounding aspherical ejecta, with which the disk is misaligned. The polarization across the broad H , H , and He i k5876 lines of SN 1997eg forms closed loops when viewed in the Stokes q-u plane. Such loops occur when the geometrical symmetry of one or both of the Stokes parameters across spectral lines is broken, in this case most likely by occultation of the ejecta by the equatorial circumstellar matter concentration. The polarization of the narrow Balmer lines possesses an intrinsic axis that differs by 12 from that of the elongated ejecta and probably indicates the orientation of the disklike circumstellar material. The existence of two different axes of symmetry in SN 1997eg suggests that neither rotation of the progenitor nor the influence of a companion star can be the sole mechanism creating a preferred axis within the supernova system. Our model supports the emerging hypothesis that the progenitors of some Type IIn supernovae are luminous blue variable stars, whose presupernova mass eruptions form the circumstellar shells that physically characterize the SN IIn subclass. These conclusions, which are independent of interstellar polarization effects, would have been unobservable with only a single epoch of spectropolarimetry.

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Spectropolarimetric observations of supernovae

Abstract: Abstract.We

Cited by 9 publications

References 52 publications

Multicolor Light Curves of Type Ia Supernovae on the Color‐Magnitude Diagram: A Novel Step toward More Precise Distance and Extinction Estimates

Multicolor Light Curves of Type Ia Supernovae on the Color‐Magnitude Diagram: A Novel Step toward More Precise Distance and Extinction Estimates

Modelling the Type Ic SN 2004aw: a moderately energetic explosion of a massive C+O star without a GRB

The Dual‐Axis Circumstellar Environment of the Type IIn Supernova 1997eg

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