New Perspectives on Type Ic Supernovae

Clocchiatti, A.; Wheeler, J. C.

doi:10.1007/978-94-011-5710-0_53

Cited by 11 publications

(4 citation statements)

References 40 publications

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“…These suggestions are not original to this paper, but they are strengthened by our finding that the H I and He I optical depths in SNe Ib are not very high. These suggestions also are not inconsistent with arguments, based on light curves, for the existence of different physical classes of hydrogen-poor events that cut across the conventional spectroscopic types (e.g., Clocchiatti & Wheeler 1997).…”

Section: Resultsmentioning

confidence: 49%

Direct Analysis of Spectra of Type Ib Supernovae

Branch

Benetti

Kasen

et al. 2002

ApJ

174

249

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Synthetic spectra generated with the parameterized supernova synthetic-spectrum code SYNOW are compared to photospheric-phase spectra of Type Ib supernovae (SNe Ib). Although the synthetic spectra are based on many simplifying approximations, including spherical symmetry, they account well for the observed spectra. Our sample of SNe Ib obeys a tight relation between the velocity at the photosphere, as determined from the Fe II features, and the time relative to that of maximum light. From this we infer that the masses and the kinetic energies of the events in this sample were similar. After maximum light the minimum velocity at which the He I features form usually is higher than the velocity at the photosphere, but the minimum velocity of the ejected helium is at least as low as 7000 kms. Previously unpublished spectra of SN 2000H reveal the presence of hydrogen absorption features, and we conclude that hydrogen lines also were present in SNe 1999di and 1954A. Hydrogen appears to be present in SNe Ib in general, although in most events it becomes too weak to identify soon after maximum light. The hydrogen-line optical depths that we use to fit the spectra of SNe 2000H, 1999di, and 1954A are not high, so only a mild reduction in the hydrogen optical depths would be required to make these events look like typical SNe Ib. Similarly, the He I line optical depths are not very high, so a moderate reduction would make SNe Ib look like SNe Ic.Comment: 21 pages and 24 figures, submitted to Ap

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Section: Resultsmentioning

confidence: 49%

Direct Analysis of Spectra of Type Ib Supernovae

Branch

Benetti

Kasen

et al. 2002

ApJ

174

249

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“…Although rarely seen in other SNe Ib, a similar feature was also present in the Type Ib SN 1996N (Sollerman et al 1998), and more notably in the well-studied transitional Type IIb supernova (SN IIb) 1993J (Clocchiatti & Wheeler 1994;Filippenko, Matheson, & Barth 1994;Patat et al 1995;Matheson et al 2000). A similar feature was also reported in nebular spectra of SN 2005bf (Soderberg et al 2005;Maeda et al 2007b).…”

Section: Early Phase Spectroscopic Evolutionmentioning

confidence: 58%

The He-Rich Core-Collapse Supernova 2007y: Observations From X-Ray to Radio Wavelengths

Stritzinger

Mazzali

Phillips

et al. 2009

ApJ

116

130

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A detailed study spanning approximately a year has been conducted on the Type Ib supernova 2007Y. Imaging was obtained from X-ray to radio wavelengths, and a comprehensive set of multiband (w2m2w1u ′ g ′ r ′ i ′ U BV Y JHK s ) light curves and optical spectroscopy is presented. A virtually complete bolometric light curve is derived, from which we infer a 56 Ni-mass of 0.06 M ⊙ . The early spectrum strongly resembles SN 2005bf and exhibits high-velocity features of Ca II and Hα; during late epochs the spectrum shows evidence of a ejecta-wind interaction. Nebular emission lines have similar widths and exhibit profiles that indicate a lack of major asymmetry in the ejecta. Late phase spectra are modeled with a non-LTE code, from which we find 56 Ni, O and total-ejecta masses (excluding He) to be 0.06, 0.2 and 0.42 M ⊙ , respectively, below 4,500 km s −1 . The 56 Ni mass confirms results obtained from the bolometric light curve. The oxygen abundance suggests the progenitor was most likely a ≈3.3 M ⊙ He core star that evolved from a zero-age-main-sequence mass of 10-13 M ⊙ . The explosion energy is determined to be ≈10 50 erg, and the mass-loss rate of the progenitor is constrained from X-ray and radio observations to be 10 −6 M ⊙ yr −1 . SN 2007Y is among the least energetic normal Type Ib supernovae ever studied. Subject headings: galaxies: individual (NGC 1187) -supernovae: general -supernovae: individual (SN 2007Y) 1 This paper includes data gathered with the 6.5 meter Magellan telescope at Las Campanas Observatory, Chile.2 Partly based on observations collected at the European Southern Observatory, La Silla and Paranal Observatories, Chile (ESO Programme 078.D-0048 and 380.D-0272.) 3

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“…If 56Co decay is powering the late light curve of SN 1998bw, there must be a fairly strong leakage in the c-ray deposition, as for SN 1996N (Sollerman et al 1998). Interestingly, fast and slow decliners seem to exist within the Type Ic class, as pointed out by Clocchiatti & Wheeler (1997). The range spanned by late-phase decline rates of SNe Ib/c is quite broad : ranges from 0.006 (SN c B 1990B ; Piemonte 2001) to 0.022 mag day~1 (SN 1990I ; ESO-KP database).…”

Section: Broadband and Bolometric Light Curvesmentioning

confidence: 87%

The Metamorphosis of SN 1998bw

Patat

Cappellaro

Danziger

et al. 2001

ApJ

399

529

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We present and discuss the photometric and spectroscopic evolution of the peculiar SN 1998bw, associated with GRB 980425, through an analysis of optical and near-IR data collected at ESOÈLa Silla. The spectroscopic data, spanning the period from day [9 to day ]376 (relative to B maximum), have shown that this supernova (SN) was unprecedented, although somewhat similar to SN 1997ef. Maximum expansion velocities as high as 3 ] 104 km s~1 to some extent mask its resemblance to other Type Ic SNe. At intermediate phases, between photospheric and fully nebular, the expansion velocities (D104 km s~1) remained exceptionally high compared to those of other recorded core-collapse SNe at a similar phase. The mild linear polarization detected at early epochs suggests the presence of asymmetry in the emitting material. The degree of asymmetry, however, cannot be decoded from these measurements alone. The He I 1.083 and 2.058 km lines are identiÐed, and He is suggested to lie in an outer region of the envelope. The temporal behavior of the Ñuxes and proÐles of emission lines of Mg I] j4571, [O I] jj6300, 6364, and a feature ascribed to Fe are traced to stimulate future modeling work. The uniqueness of SN 1998bw became less obvious once it entered the fully nebular phase (after 1 yr), when it was very similar to other Type Ib/cÈIIb objects, such as the Type Ib SN 1996N and the Type IIb SN 1993J, even though SN 1998bw was 1.4 mag brighter than SN 1993J and 3 mag brighter than SN 1996N at a comparable phase. The late-phase optical photometry, which extends up to 403 days after B maximum, shows that the SN luminosity declined exponentially but substantially faster than the decay rate of 56Co. The ultraviolet-optical-infrared bolometric light curve, constructed using all available optical data and the early JHK photometry presented in this work, shows a slight Ñattening starting on about day ]300. Since no clear evidence of ejecta-wind interaction was found in the late-time spectroscopy (see also the work of Sollerman and coworkers), this may be due to the contribution of the positrons since most c-rays escape thermalization at this phase. A contribution from the superposed H II region cannot, however, be excluded.

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New Perspectives on Type Ic Supernovae

Cited by 11 publications

References 40 publications

Direct Analysis of Spectra of Type Ib Supernovae

Direct Analysis of Spectra of Type Ib Supernovae

The He-Rich Core-Collapse Supernova 2007y: Observations From X-Ray to Radio Wavelengths

The Metamorphosis of SN 1998bw

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