Physical Characteristics of V 1016 Cygni

Ciatti, F.; Mammano, A.; Rosino, L.

doi:10.1017/s0074180900010536

Cited by 7 publications

(10 citation statements)

References 2 publications

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“…At this peak, it was brighter than the maximum of the Type IIP SN 1969L (e.g. Ciatti et al 1971) and comparable to the peak of the Type Ic SN 2007gr (Valenti et al 2008), the two other SN in NGC 1058. It then dropped in brightness, going through a series of extended plateaus, including a 4 year period from 1963 to 1967 where it was only moderately fainter than the progenitor, with m pg ≃ 19.…”

Section: Introductionmentioning

confidence: 63%

THE SUPERNOVA IMPOSTOR IMPOSTOR SN 1961V:SPITZERSHOWS THAT ZWICKY WAS RIGHT (AGAIN)

Kochanek

Szczygiel

Stanek

2011

ApJ

100

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SN 1961V, one of Zwicky's defining Type V supernovae (SN), was a peculiar transient in NGC 1058 that has variously been categorized as either a true core collapse SN leaving a black hole (BH) or neutron star (NS) remnant, or an eruption of a luminous blue variable (LBV) star. The former case is suggested by its association with a decaying non-thermal radio source, while the latter is suggested by its peculiar transient light curve and its low initial expansion velocities. The crucial difference is that the star survives a transient eruption but not an SN. All stars identified as possible survivors are significantly fainter, L opt ∼ 10 5 L ⊙ , than the L opt ≃ 3×10 6 L ⊙ progenitor star at optical wavelengths. While this can be explained by dust absorption in a shell of material ejected during the transient, the survivor must then be present as a L IR ≃ 3 × 10 6 L ⊙ mid-infrared source. Using archival Spitzer observations of the region, we show that such a luminous mid-IR source is not present. The brightest source of dust emission is only L IR ≃ 10 5 L ⊙ and does not correspond to the previously identified candidates for the surviving star. The dust cannot be made sufficiently distant and cold to avoid detection unless the ejection energy, mass and velocity scales are those of a SN or greater. We conclude that SN 1961V was a peculiar, but real, supernova. Its peculiarities are probably due to enhanced mass loss just prior to the SN, followed by the interactions of the SN blast wave with this ejecta. This adds to the evidence that there is a population of SN progenitors that have major mass loss episodes shortly before core collapse. The progenitor is a low metallicity, ∼ 1/3 solar, high mass, M ZAMS > ∼ 80M ⊙ , star, which means either that BH formation can be accompanied by an SN or that surprisingly high mass stars can form a NS. We also report on the mid-IR properties of the two other SN in NGC 1058, SN 1969L and SN 2007gr.

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Section: Introductionmentioning

confidence: 63%

THE SUPERNOVA IMPOSTOR IMPOSTOR SN 1961V:SPITZERSHOWS THAT ZWICKY WAS RIGHT (AGAIN)

Kochanek

Szczygiel

Stanek

2011

ApJ

100

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“…Excellent examples of SNe II-P are SN 1969L (Ciatti et al 1971), SN 1986I (Pennypacker et al 1989), SN 1988A (Turatto et al 1993a, SN 1990E (Schmidt et al 1993, and SN 1991G (Blanton et al 1995). At very early times, the spectrum is nearly featureless and quite blue, indicating a high color temperature ( 10,000 K).…”

Section: Type Ii-p Supernovaementioning

confidence: 99%

Optical Spectra of Supernovae

Filippenko

1997

Annu. Rev. Astron. Astrophys.

1,673

1,405

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The temporal evolution of the optical spectra of various types of supernovae (SNe) is illustrated, in part to aid observers classifying supernova candidates. Type II SNe are defined by the presence of hydrogen, and they exhibit a very wide variety of photometric and spectroscopic properties. Among hydrogen-deficient SNe (Type I), three subclasses are now known: those whose early-time spectra show strong Si II (Ia), prominent He I (Ib), or neither Si II nor He I (Ic). The late-time spectra of SNe Ia consist of a multitude of blended emission lines of iron-group elements; in sharp contrast, those of SNe Ib and SNe Ic (which are similar to each other) are dominated by several relatively unblended lines of intermediatemass elements. Although SNe Ia, which result from the thermonuclear runaway of white dwarfs, constitute a rather homogeneous subclass, important variations in their photometric and spectroscopic properties are undeniably present. SNe Ib/Ic probably result from core collapse in massive stars largely stripped of their hydrogen (Ib) and helium (Ic) envelopes, and hence they are physically related to SNe II. Indeed, the progenitors of some SNe II seem to have only a low-mass skin of hydrogen; their spectra gradually evolve to resemble those of SNe Ib. In addition to the two well-known photometric subclasses (linear and plateau) of SNe II, which may exhibit minor spectroscopic differences, there is a new subclass (SNe IIn) distinguished by relatively narrow emission lines with little or no P Cygni absorption component and slowly declining light curves. These objects probably have unusually dense circumstellar gas with which the ejecta interact.

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“…The light curve of N Vul-2, on the contrary, has been smooth, with a regular decline (d=0.1 mag/day). It looks somewhat alike, among many others, to the light curve of Nova V1229 Aql 1970 (Ciatti and Rosino, 1974). If the statistical relation between velocity of decline and absolute magnitude at maximum of the novae (Payne-Gaposchkin, 1957) can be applied, we obtain Mpg = -8.5 for N Vul-1, which may be rather uncertain because of the irregularity of its light curve, and Mpg = -7.4for N Vul-2.…”

Section: Discussionmentioning

confidence: 67%

Spectroscopic Evolution of Nova Vul 1984 No. 1 (PW Vul) and No. 2

Rosino¹,

Iijima²

1987

International Astronomical Union Colloquium

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ABSTRACT. Spectroscopic observations of two novae (Nova Vul 1984 No. 1 and No. 2) have been carried out at the Asiago Observatory from the moment of their discovery up to now. A short preliminary description of the spectral characteristics and evolution of these two novae is reported together with a brief comparison of their properties. The purpose of this paper is that of giving a preliminary description of the characteristics and spectral evolution of the two novae. Detailed data on the available material and final results will be presented in successive papers.

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Physical Characteristics of V 1016 Cygni

Cited by 7 publications

References 2 publications

THE SUPERNOVA IMPOSTOR IMPOSTOR SN 1961V:SPITZERSHOWS THAT ZWICKY WAS RIGHT (AGAIN)

THE SUPERNOVA IMPOSTOR IMPOSTOR SN 1961V:SPITZERSHOWS THAT ZWICKY WAS RIGHT (AGAIN)

Optical Spectra of Supernovae

Spectroscopic Evolution of Nova Vul 1984 No. 1 (PW Vul) and No. 2

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