The Rise Time of Nearby Type I[CLC]a[/CLC] Supernovae

Riess, Adam G.; Filippenko, A. V.; Li, Weidong; Treffers, R. R.; Schmidt, B. P.; Qiu, Y.; Hu, Jingyao; Armstrong, Mark; Faranda, Chuck; Thouvenot, Éric; Buil, C.

doi:10.1086/301143

Cited by 238 publications

(236 citation statements)

References 39 publications

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“…The rise in brightness is due to the increase in size of the ejecta and lasts for almost three weeks [1,23,42,93] with the color and temperature rather constant. The earliest observed supernovae are SN1990N and SN1998bu, which were observed about 17 days before maximum [58,93]. The light curves are shaped by the progressing diffusion of photons out of the ejecta (see, e.g., [85]).…”

Section: Thermonuclear Supernovaementioning

confidence: 99%

“…They are the rise time to maximum [93], color near maximum light [88], line strengths of the primary Ca and Si absorption lines [79], the velocities as measured in Fe lines at late phases [70], the host galaxy morphology [101], and host galaxy colors [16,43]. There may be indications that the secondary peak in the I light curves and the shoulder in the bolometric light curves correlate with the absolute luminosity [24,44,91].…”

Section: Thermonuclear Supernovaementioning

confidence: 99%

“…It is, at the moment, not clear what fraction of SNIa show a similar behavior as the rise phase is often not observed and the correlations have been based on the decline rate. Nevertheless, the fact that for some SNIa the rise and decline rates do correlate [24,93] hints at intrinsic differences within this class.…”

Section: Thermonuclear Supernovaementioning

confidence: 99%

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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: Thermonuclear Supernovaementioning

confidence: 99%

Section: Thermonuclear Supernovaementioning

confidence: 99%

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Optical Light Curves of Supernovae

Leibundgut

Suntzeff

2003

Supernovae and Gamma-Ray Bursters

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“…Most of the observations were performed without filter (white light, hereinafter W h) in order to get the best photon statistics for the study of faint Cepheid light curves. The properties of this photometric band are discussed in Paper I (Antonello et al 1999a) and Paper III of this series; other information can be obtained from the paper by Riess et al (1999). Moreover, two images were taken in Johnson V and R filter to obtain information on star colors.…”

Section: Observations Of Ngc 6822mentioning

confidence: 99%

Variable stars in nearby galaxies

Antonello

Fugazza

Mantegazza

et al. 2002

A&A

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Abstract.The results of a CCD survey for variability of stars in the nearby galaxy NGC 6822 are presented. The goal of the survey was to obtain good light curves of Cepheids for Fourier decomposition and to detect shorter period Cepheids. Since the program was carried out with a relatively small telescope, the Dutch 0.9 m at ESO-La Silla, the observations were unfiltered (white light, or W h-band). The analysis revealed the presence of more than 130 variable stars. 21 population I Cepheids are detected; 6 of them were already known from previous works (Kayser 1967). For at least three Cepheids, however, the previous identification or period was wrong. Some probable population II (W Vir) stars are also identified. The dispersion of the fundamental mode Cepheid P L relation appears to be small.

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“…Examples of our light curves of SNe are presented in Figure 1. Journal papers that summarize part of the LOSS data include the study of SN 1997br (la; Li et al 1999Van Dyk et al 2000), SN 1998bu (la; Jha et al 1999Modjaz et al 2001Matheson et al 2000), the rise time of SNe la (Riess et al 1999a(Riess et al , 1999b, the peculiarity rate of SNe la (Li et al 2001), and observations of SNe Ib/Ic (Matheson et al 2001). Several more papers are now in preparation.…”

mentioning

confidence: 99%

The Lick Observatory Supernova Search with the Katzman Automatic Imaging Telescope

Filippenko

Treffers

et al. 2001

International Astronomical Union Colloquium

Self Cite

184

144

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Abstract. The Katzman Automatic Imaging Telescope (KAIT) at LickObservatory is a fully robotic 0.76-m reflector equipped with a CCD imaging camera. Its telescope control system checks the weather, opens the dome, points to the desired objects, finds and acquires guide stars, exposes, stores the data, and manipulates the data without human intervention. There is a 20-slot filter wheel, including UBVRI. Five-minute guided exposures yield detections of stars at R « 20 mag when the seeing is good (< 2").One of our main goals is to discover nearby supernovae (SNe; redshifts generally less than 5000 km s _ 1 ), to be used for a variety of studies. Special emphasis is placed on finding them well before maximum brightness. A limit of ~ 19 mag is reached in the 25-sec unfiltered, unguided exposures of our Lick Observatory Supernova Search (LOSS). We can observe over 1200 galaxies in a long night, and we try to cycle back to the same galaxies after 3 to 4 nights. Our software automatically subtracts template images from new observations and identifies supernova candidates that are subsequently examined by student research assistants. LOSS found 20 SNe in 1998SNe in , 40 in 1999SNe in , and 36 in 2000 KAIT the world's most successful search engine for nearby SNe. We also find novae in the Local Group, comets, asteroids, and cataclysmic variables. Multifilter follow-up photometry is conducted of the most important SNe, and all objects are monitored in unfiltered mode. A Web page describing LOSS is at http://astro.berkeley.edu/~bait/kait.html .

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The Rise Time of Nearby Type I[CLC]a[/CLC] Supernovae

Cited by 238 publications

References 39 publications

Optical Light Curves of Supernovae

Optical Light Curves of Supernovae

Variable stars in nearby galaxies

The Lick Observatory Supernova Search with the Katzman Automatic Imaging Telescope

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