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A. Pastorello S. Mattila L. Zampieri M. Della Valle S. J. Smartt S. Valenti I. Agnoletto S. Benetti C. R. Benn D. Branch E. Cappellaro M. Dennefeld J. J. Eldridge A. Gal-Yam A. Harutyunyan I. Hunter H. Kjeldsen Y. Lipkin P. A. Mazzali P. Milne H. Navasardyan E. O. Ofek E. Pian O. Shemmer S. Spiro R. A. Stathakis S. Taubenberger M. Turatto H. Yamaoka 《Monthly notices of the Royal Astronomical Society》2008,389(1):113-130
We present new spectroscopic and photometric data of the Type Ibn supernovae 2006jc, 2000er and 2002ao. We discuss the general properties of this recently proposed supernova family, which also includes SN 1999cq. The early-time monitoring of SN 2000er traces the evolution of this class of objects during the first few days after the shock breakout. An overall similarity in the photometric and spectroscopic evolution is found among the members of this group, which would be unexpected if the energy in these core-collapse events was dominated by the interaction between supernova ejecta and circumstellar medium. Type Ibn supernovae appear to be rather normal Type Ib/c supernova explosions which occur within a He-rich circumstellar environment. SNe Ibn are therefore likely produced by the explosion of Wolf–Rayet progenitors still embedded in the He-rich material lost by the star in recent mass-loss episodes, which resemble known luminous blue variable eruptions. The evolved Wolf–Rayet star could either result from the evolution of a very massive star or be the more evolved member of a massive binary system. We also suggest that there are a number of arguments in favour of a Type Ibn classification for the historical SN 1885A (S-Andromedae), previously considered as an anomalous Type Ia event with some resemblance to SN 1991bg. 相似文献
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A. Pastorello E. Baron D. Branch L. Zampieri M. Turatto M. Ramina S. Benetti E. Cappellaro M. Salvo F. Patat A. Piemonte J. Sollerman B. Leibundgut G. Altavilla 《Monthly notices of the Royal Astronomical Society》2005,360(3):950-962
We present spectroscopic and photometric observations of the peculiar Type II supernova (SN) 1998A. The light curves and spectra closely resemble those of SN 1987A, suggesting that the SN 1998A progenitor exploded when it was a compact blue supergiant. However, the comparison with SN 1987A also highlights some important differences: SN 1998A is more luminous and the spectra show bluer continua and larger expansion velocities at all epochs. These observational properties indicate that the explosion of SN 1998A is more energetic than SN 1987A and more typical of Type II supernovae. Comparing the observational data with simulations, we deduce that the progenitor of SN 1998A was a massive star (∼25 M⊙ ) with a small pre-supernova radius (≲6 × 1012 cm) . The Ba ii lines, unusually strong in SN 1987A and some faint II-P events, are almost normal in the case of SN 1998A, indicating that the temperature plays a key role in determining their strength. 相似文献
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A. Pastorello D. Sauer S. Taubenberger P. A. Mazzali K. Nomoto K. S. Kawabata S. Benetti N. Elias-Rosa A. Harutyunyan H. Navasardyan L. Zampieri T. Iijima M. T. Botticella G. Di Rico M. Del Principe M. Dolci S. Gagliardi M. Ragni G. Valentini 《Monthly notices of the Royal Astronomical Society》2006,370(4):1752-1762
Early-time optical observations of supernova (SN) 2005cs in the Whirlpool Galaxy (M51) are reported. Photometric data suggest that SN 2005cs is a moderately underluminous Type II plateau SN (SN IIP). The SN was unusually blue at early epochs ( U − B ≈−0.9 about three days after explosion) which indicates very high continuum temperatures. The spectra show relatively narrow P Cygni features, suggesting ejecta velocities lower than observed in more typical SNe IIP. The earliest spectra show weak absorption features in the blue wing of the He i 5876-Å absorption component and, less clearly, of Hβ and Hα. Based on spectral modelling, two different interpretations can be proposed: these features may either be due to high-velocity H and He i components, or (more likely) be produced by different ions (N ii , Si ii ). Analogies with the low-luminosity, 56 Ni-poor, low-velocity SNe IIP are also discussed. While a more extended spectral coverage is necessary in order to determine accurately the properties of the progenitor star, published estimates of the progenitor mass seem not to be consistent with stellar evolution models. 相似文献
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A. Pastorello S. Valenti L. Zampieri H. Navasardyan S. Taubenberger S. J. Smartt A. A. Arkharov O. Bärnbantner H. Barwig S. Benetti P. Birtwhistle M. T. Botticella E. Cappellaro M. Del Principe F. Di Mille G. Di Rico M. Dolci N. Elias-Rosa N. V. Efimova M. Fiedler A. Harutyunyan P. A. Höflich W. Kloehr V. M. Larionov V. Lorenzi J. R. Maund N. Napoleone M. Ragni M. Richmond C. Ries S. Spiro S. Temporin M. Turatto J. C. Wheeler 《Monthly notices of the Royal Astronomical Society》2009,394(4):2266-2282
We present the results of the one-year long observational campaign of the type II plateau SN 2005cs, which exploded in the nearby spiral galaxy M51 (the Whirlpool galaxy). This extensive data set makes SN 2005cs the best observed low-luminosity, 56 Ni-poor type II plateau event so far and one of the best core-collapse supernovae ever. The optical and near-infrared spectra show narrow P-Cygni lines characteristic of this SN family, which are indicative of a very low expansion velocity (about 1000 km s−1 ) of the ejected material. The optical light curves cover both the plateau phase and the late-time radioactive tail, until about 380 d after core-collapse. Numerous unfiltered observations obtained by amateur astronomers give us the rare opportunity to monitor the fast rise to maximum light, lasting about 2 d. In addition to optical observations, we also present near-infrared light curves that (together with already published ultraviolet observations) allow us to construct for the first time a reliable bolometric light curve for an object of this class. Finally, comparing the observed data with those derived from a semi-analytic model, we infer for SN 2005cs a 56 Ni mass of about 3 × 10−3 M⊙ , a total ejected mass of 8–13 M⊙ and an explosion energy of about 3 × 1050 erg . 相似文献
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A. Pastorello R. M. Quimby † S. J. Smartt S. Mattila H. Navasardyan R. M. Crockett N. Elias-Rosa P. Mondol J. C. Wheeler D. R. Young 《Monthly notices of the Royal Astronomical Society》2008,389(1):131-140
We present photometric and spectroscopic data of the peculiar SN 2005la, an object which shows an optical light curve with some luminosity fluctuations and spectra with comparably strong narrow hydrogen and helium lines, probably of circumstellar nature. The increasing full width at half-maximum velocity of these lines is indicative of an acceleration of the circumstellar material. SN 2005la exhibits hybrid properties, sharing some similarities with both Type IIn supernovae and 2006jc-like (Type Ibn) events. We propose that the progenitor of SN 2005la was a very young Wolf–Rayet (WN-type) star which experienced mass ejection episodes shortly before core collapse. 相似文献
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Ferdinando Patat Stefano Benetti Enrico Cappellaro Massimo Turatto 《Monthly notices of the Royal Astronomical Society》2006,369(4):1949-1960
In this paper, we present and discuss the effects of scattered light echoes (LEs) on the luminosity and spectral appearance of Type Ia supernovae (SNe). After introducing the basic concept of LE spectral synthesis by means of LE models and real observations, we investigate the deviations from pure SN spectra, light and colour curves, the signatures that witness the presence of an LE and the possible inferences on the extinction law. The effects on the photometric parameters and spectral features are also discussed. In particular, for the case of circumstellar dust, LEs are found to introduce an apparent relation between the post-maximum decline rate and the absolute luminosity, which is most likely going to affect the well-known Pskowski–Phillips relation. 相似文献
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A few Type Ia supernovae (SNe Ia) have been suggested to be an explosion of a super-Chandrasekhar-mass white dwarf (WD) in order to account for their large luminosities, requiring a large amount of 56 Ni. However, the candidate overluminous SNe Ia 2003fg, 2006gz and (moderately overluminous) SN 1991T have very different observational features: the characteristic time-scale and velocity are very different. We examine if and how the diversity can be explained, by one-dimensional spherical radiation transport calculations covering a wide range of model parameters (e.g. WD mass). The observations of SN 2006gz are naturally explained by the super-Chandrasekhar-mass model. SN 1991T represents a marginal case, which may either be a Chandrasekhar or a super-Chandrasekhar-mass WD explosion. In contrast, the low velocity and short time-scale seen in SN 2003fg indicate that the ejecta mass is smaller than the Chandrasekhar mass, which is in apparent contradiction to the large luminosity. We suggest that the problem is solved if the progenitor WD, and thus the SN explosion, is aspherical. This may reflect a rapid rotation of the progenitor star, likely a consequence of the super-Chandrasekhar-mass WD progenitor. The observed differences between SNe 2003fg and 2006gz may be attributed to different viewing orientations. 相似文献
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A. Pastorello P. A. Mazzali G. Pignata S. Benetti E. Cappellaro A. V. Filippenko W. Li W. P. S. Meikle A. A. Arkharov G. Blanc F. Bufano A. Derekas M. Dolci N. Elias-Rosa R. J. Foley M. Ganeshalingam A. Harutyunyan L. L. Kiss R. Kotak V. M. Larionov J. R. Lucey N. Napoleone H. Navasardyan F. Patat J. Rich S. D. Ryder M. Salvo B. P. Schmidt V. Stanishev P. Székely S. Taubenberger S. Temporin M. Turatto W. Hillebrandt 《Monthly notices of the Royal Astronomical Society》2007,377(4):1531-1552
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Recent evidence of a young progenitor population for many Type Ia supernovae (SNe Ia) raises the possibility that evolved intermediate-mass progenitor stars may be detected in pre-explosion images. NGC 1316, a radio galaxy in the Fornax cluster, is a prolific producer of SNe Ia, with four detected since 1980. We analyse Hubble Space Telescope ( HST ) pre-explosion images of the sites of two of the SNe Ia that exploded in this galaxy, SN2006dd (a normal Type Ia) and SN2006mr (likely a subluminous, 1991bg-like, SN Ia). Astrometric positions are obtained from optical and near-infrared ground-based images of the events. We find no candidate point sources at either location, and set upper limits on the flux in B, V and I from any such progenitors. We also estimate the amount of extinction that could be present, based on analysis of the surface-brightness inhomogeneities in the HST images themselves. At the distance of NGC 1316, the limits correspond to absolute magnitudes of ∼−5.5, −5.4 and −6.0 mag in M B , M V and M I , respectively. Comparison to stellar evolution models argues against the presence at the supernova sites, 3 yr prior to the explosion, of normal stars with initial masses ≳6 M⊙ at the tip of their asymptotic-giant branch (AGB) evolution, young post-AGB stars that had initial masses ≳4 M⊙ and post-red giant stars of initial masses ≳9 M⊙ . 相似文献
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M. Hernandez W. P. S. Meikle A. Aparicio C. R. Benn M. R. Burleigh A. C. Chrysostomou A. J. L. Fernandes T. R. Geballe P. L. Hammersley J. Iglesias-Paramo D. J. James P. A. James S. N. Kemp T. A. Lister D. Martinez-Delgado A. Oscoz D. L. Pollacco M. Rozas S. J. Smartt P. Sorensen R. A. Swaters J. H. Telting W. D. Vacca N. A. Walton M. R. Zapatero-Osorio 《Monthly notices of the Royal Astronomical Society》2000,319(1):223-234
We present first-season infrared (IR) and optical photometry and spectroscopy of the Type Ia Supernova 1998bu in M96. We also report optical polarimetry of this event. SN 1998bu is one of the closest type Ia supernovae of modern times, and the distance of its host galaxy is well determined. We find that SN 1998bu is both photometrically and spectroscopically normal. However, the extinction to this event is unusually high, with We find that SN 1998bu peaked at an intrinsic Adopting a distance modulus of 30.25 (Tanvir et al.) and using Phillips et al.'s relations for the Hubble constant, we obtain Combination of our IR photometry with those of Jha et al. provides one of the most complete early-phase IR light curves for a SN Ia published so far. In particular, SN 1998bu is the first normal SN Ia for which good pre- t B max IR coverage has been obtained. It reveals that the J , H and K light curves peak about 5 days earlier than the flux in the B -band curve. 相似文献
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G. Pignata S. Benetti P. A. Mazzali R. Kotak F. Patat P. Meikle M. Stehle B. Leibundgut N. B. Suntzeff L. M. Buson E. Cappellaro A. Clocchiatti M. Hamuy J. Maza J. Mendez P. Ruiz-Lapuente M. Salvo B. P. Schmidt M. Turatto W. Hillebrandt 《Monthly notices of the Royal Astronomical Society》2008,388(3):971-990
As part of the European Supernova Collaboration, we obtained extensive photometry and spectroscopy of the Type Ia supernova (SN Ia) SN 2002dj covering epochs from 11 d before to nearly two years after maximum. Detailed optical and near-infrared observations show that this object belongs to the class of the high-velocity gradient events as indicated by Si, S and Ca lines. The light curve shape and velocity evolution of SN 2002dj appear to be nearly identical to SN 2002bo. The only significant difference is observed in the optical to near-infrared colours and a reduced spectral emission beyond 6500 Å. For high-velocity gradient SNe Ia, we tentatively identify a faster rise to maximum, a more pronounced inflection in the V and R light curves after maximum and a brighter, slower declining late-time B light curve as common photometric properties of this class of objects. They also seem to be characterized by a different colour and colour evolution with respect to 'normal' SNe Ia. The usual light curve shape parameters do not distinguish these events. Stronger, more blueshifted absorption features of intermediate-mass elements and lower temperatures are the most prominent spectroscopic features of SNe Ia displaying high-velocity gradients. It appears that these events burn more intermediate-mass elements in the outer layers. Possible connections to the metallicity of the progenitor star are explored. 相似文献
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S. Benetti M. Turatto S. Balberg L. Zampieri S. L. Shapiro E. Cappellaro K. Nomoto T. Nakamura P. A. Mazzali F. Patat 《Monthly notices of the Royal Astronomical Society》2001,322(2):361-368
We present a new set of spectroscopic and photometric data extending the observations of SN 1997D to over 400 d after the explosion. These observations confirm the peculiar properties of SN 1997D, such as the very low abundance of 56 Co (0.002 M⊙ ) and the low expansion velocity of the ejecta (∼1000 km s−1 ). We discuss the implications of these observations for the character of the progenitor and the nature of the remnant, showing that a Crab-like pulsar or an accreting neutron star formed in the explosion of a low-mass progenitor should already have produced a detectable luminosity at this epoch, in contrast with photometric data. On the other hand, the explosion of a high-mass progenitor with the formation of a black hole is consistent with the available observations. The consequences of this conclusion regarding the nature of the explosion and the prospects of directly identifying the black hole are also addressed. 相似文献
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A. Pastorello S. Taubenberger N. Elias-Rosa P. A. Mazzali G. Pignata E. Cappellaro G. Garavini S. Nobili G. C. Anupama D. D. R. Bayliss S. Benetti F. Bufano N. K. Chakradhari R. Kotak A. Goobar H. Navasardyan F. Patat D. K. Sahu M. Salvo B. P. Schmidt V. Stanishev M. Turatto W. Hillebrandt 《Monthly notices of the Royal Astronomical Society》2007,376(3):1301-1316