Light curves of SN 1993J from the Keck Northeast Astronomy Consortium

Benson, P. J.; Herbst, W.; Salzer, John J.; Vinton, G.; Hanson, G. J.; Ratcliff, S. J.; Winkler, P. F.; Elmegreen, D. M.; Chromey, F. R.; Strom, C.; Balonek, T. J.; Elmegreen, Bruce G.

doi:10.1086/116958

Cited by 28 publications

(26 citation statements)

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“…light curves have been further contributed by the Padova group (see, e.g., [9,97,116,117] and the results of the Harvard-Smithsonian Center for Astrophysics (CfA) team [50,92]). There are additional contributions on SN1993J [8,11,27,64,74,90,120] and more recently SN1998S [32] and SN1999em [45,63]. Many amateur groups are also collecting supernova light curves.…”

Section: Observationsmentioning

confidence: 99%

Optical Light Curves of Supernovae

Leibundgut

Suntzeff

2003

Supernovae and Gamma-Ray Bursters

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Abstract. Photometry is the most easily acquired information about supernovae. The light curves constructed from regular imaging provide signatures not only for the energy input, the radiation escape, the local environment and the progenitor stars, but also for the intervening dust. They are the main tool for the use of supernovae as distance indicators through the determination of the luminosity.The light curve of SN1987A still is the richest and longest observed example for a core-collapse supernova. Despite the peculiar nature of this object, as explosion of a blue supergiant, it displayed all the characteristics of type II supernovae. The light curves of type Ib/c supernovae are more homogeneous, but still display the signatures of explosions in massive stars, among them early interaction with their circumstellar material.Wrinkles in the near-uniform appearance of thermonuclear (type Ia) supernovae have emerged during the past decade. Subtle differences have been observed especially at near infrared (NIR) wavelengths. Interestingly, the light curve shapes appear to correlate with a variety of other characteristics of these supernovae.The construction of bolometric light curves provides the most direct link to theoretical predictions and can yield sorely needed constraints for the models. First steps in this direction have been already made.

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Section: Observationsmentioning

confidence: 99%

Optical Light Curves of Supernovae

Leibundgut

Suntzeff

2003

Supernovae and Gamma-Ray Bursters

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“…This led to another rapid decrease in brightness for D3 weeks, followed by an approximately exponential decline. For a complete discussion of the photometry of SN 1993J, see Okyudo et al (1993), Schmidt et al (1993), van Driel et al (1993), Wheeler et al (1993), Benson et al (1994), Lewis et al (1994), Richmond et al (1994Richmond et al ( , 1996, Barbon et al (1995), Doroshenko, EÐmov, & Shakhovskoi (1995), and Prabhu et al (1995).…”

Section: Previous Studies Of Supernova 1993jmentioning

confidence: 99%

Optical Spectroscopy of Supernova 1993J During Its First 2500 Days

Matheson

Filippenko

Barth

et al. 2000

The Astronomical Journal

124

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We present 42 low-resolution spectra of supernova (SN) 1993J, our complete collection from the Lick and Keck observatories, from day 3 after explosion to day 2454, as well as one Keck high-dispersion spectrum from day 383. SN 1993J began as an apparent SN II, albeit an unusual one. After a few weeks, a dramatic transition took place, as prominent helium lines emerged in the spectrum. SN 1993J had metamorphosed from a SN II to a SN IIb. Nebular spectra of SN 1993J closely resemble those of SNe Ib and Ic, but with a persistent Ha line. At very late times, the Ha emission line dominated the spectrum, but with an unusual, boxlike proÐle. This is interpreted as an indication of circumstellar interaction.

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“…The dotted lines represent the linear extrapolations of the K-and L 0 -band data of day 39 and day 97. The visual data are compiled from Benson et al (1994) and Richmond et al (1996); the non-Caltech near-infrared data around the peak of the emission curves are taken from Wada & Ueno (1997) and the IAU Circulars of Lawrence et al (1993), Romanishin (1993), and Smith (1993). of the K and L 0 magnitudes on these days is due to thermal emission by the dust. In Figure 6 we show the excesses in the emission above exponentially decreasing emission at a level smoothly extrapolated from days 36 and 97.…”

Section: Resultsmentioning

confidence: 99%

“…The photometry of SN 1993J was established relative to the photometric standards set up by Elias et al (1982), one of which was generally measured just prior to the observation of SN 1993J and one afterward. On five marginally photometric occasions, especially near the outburst, the neighboring star '' C '' (see, e.g., Benson et al 1994) was used to obtain relative photometry at J, H, and K; star C was in turn calibrated against the Elias et al standards. It has a visual magnitude V = 14.50 mag and visual and nearinfrared colors which are typical of a G-type main-sequence star (Koornneef 1983); its near-infrared magnitudes are included in Table 1.…”

Section: Photometrymentioning

confidence: 99%

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Early Near-Infrared Observations of SN 1993J

Matthews¹,

Neugebauer²,

Armus³

et al. 2002

The Astronomical Journal

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Photometric observations in the near-infrared atmospheric windows from 1.25 to 3.7 lm and spectrographic observations from 1.2 to 2.4 lm are presented of supernova SN 1993J for 250 days after the outburst. After an initial rise to a secondary maximum the infrared observations show an exponential drop much like the visual observations. At day 130 after the outburst, however, the 3.7 lm data show an excess, which we take as a signature of dust emission. Broadband spectral energy distributions (SEDs) were derived combining published visual photometry and the infrared photometry. The early SEDs during the supernova rise to its secondary maximum could be fitted with blackbodies, but during the exponential decrease the SEDs were too narrow to be fitted by a blackbody energy distribution. The low-resolution spectra were initially featureless, but beyond about day 30 after the outburst, when SN 1993J was in exponential decline, the spectra were dominated by line emission, probably by hydrogen, helium, and iron lines.

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Light curves of SN 1993J from the Keck Northeast Astronomy Consortium

Cited by 28 publications

References 0 publications

Optical Light Curves of Supernovae

Optical Light Curves of Supernovae

Optical Spectroscopy of Supernova 1993J During Its First 2500 Days

Early Near-Infrared Observations of SN 1993J

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