The 1990 Calan/Tololo Supernova Search

Hamuy, M.; Maza, J.; Phillips, M. M.; Suntzeff, Nicholas B.; Wischnjewsky, M.; Smith, R. C.; Antezana, R.; Wells, Lisa A.; González, L.; Gigoux, Pedro; Navarrete, Mauricio; Barrientos, L. Felipe; Lamontagne, R.; Valle, M. Della; Elias, J.; Phillips, Andrew C.; Odewahn, S. C.; Baldwin, J. A.; Walker, A. R.; Williams, T. B.; Sturch, C. R.; Baganoff, F. K.; Chaboyer, Brian; Schommer, R. A.; Tirado, H.; Hernández, M. S.; Ugarte, P.; Guhathakurta, P.; Howell, Steve B.; Szkody, Paula; Schmidtke, P. C.; Roth, Joshua

doi:10.1086/116811

Cited by 115 publications

(80 citation statements)

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“…Standouts include SNe 1994ae, 1995D, 1995al, 1995bd, 1995ac, and 1996X, each with 80 to 100 observations beginning before maximum and extending 60 to 100 days after maximum. Figure 8 shows BV RI composite light curves formed by normalizing the data in time and brightness at the Ðt to the initial peak, including a correction for 1 ] z time dilation and a K-correction (Hamuy et al 1993). By affixing the light curves at maximum, their inhomogeneity is readily apparent.…”

Section: Discussionmentioning

confidence: 99%

“…Regrettably, light curves have been collected, reduced, and published for fewer than 50 of these objects (Cadonau & Leibundgut 1990 ;Hamuy et al 1993Hamuy et al , 1994Hamuy et al , 1996aSadakane et al 1996 ;Phillips 1993 and references therein). Of these, less than one-half include I and R light curves that, combined with shorter wavelength light curves, can be used to determine the reddening due to dust (Ford et al 1993 ;Hamuy et al 1996a).…”

Section: Introductionmentioning

confidence: 99%

“…The largest contribution to date has been made by the Supernova Survey, a program begun in 1990 Cala n/Tololo by astronomers at Cerro Tololo Inter-American Observatory (CTIO) and the Cerro Observatory of the UniCala n versity of Chile (Hamuy et al 1993). This photographic search with follow-up BV I CCD photometry netted 27 SNe Ia with 0.01 \ z \ 0.1.…”

Section: Introductionmentioning

confidence: 99%

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[ITAL]BVRI[/ITAL] Light Curves for 22 Type I[CLC]a[/CLC] Supernovae

Riess¹,

Kirshner²,

Schmidt³

et al. 1999

The Astronomical Journal

656

320

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We present 1210 Johnson/Cousins B, V , R, and I photometric observations of 22 recent Type Ia supernovae (SNe Ia) : SNe 1993ac, 1993ae, 1994M, 1994S, 1994T, 1994Q, 1994ae, 1995D, 1995E, 1995al, 1995ac, 1995ak, 1995bd, 1996C, 1996X, 1996Z, 1996ab, 1996ai, 1996bk, 1996bl, 1996bo, and 1996bv. Most of the photometry was obtained at the Fred Lawrence Whipple Observatory of the HarvardSmithsonian Center for Astrophysics in a cooperative observing plan aimed at improving the database for SNe Ia. The redshifts of the sample range from cz \ 1200 to 37,000 km s~1 with a mean of cz \ 7000 km s~1.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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[ITAL]BVRI[/ITAL] Light Curves for 22 Type I[CLC]a[/CLC] Supernovae

Riess¹,

Kirshner²,

Schmidt³

et al. 1999

The Astronomical Journal

656

320

View full text Add to dashboard Cite

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“…The remaining SNe were observed using a variety of telescopes equipped with CCD detectors and UBV RI z KC ( ) filters, as indicated in Table 3. The observational techniques employed by the C&T project are presented by Hamuy et al (1993), and the photometric reductions are in Hamuy et al (1996). The observations and data reductions during the SOIRS project are explained in , whereas the techniques employed during the CATS project can be found in Hamuy et al (2009).…”

Section: Photometrymentioning

confidence: 99%

UBVRIz LIGHT CURVES OF 51 TYPE II SUPERNOVAE

Galbany

Hamuy

Phillips

et al. 2016

Self Cite

102

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We present a compilation of UBVRIz light curves of 51 type II supernovae discovered during the course of four different surveys during 1986-2003: the Cerro Tololo Supernova Survey, the Calán/Tololo Supernova Program (C&T), the Supernova Optical and Infrared Survey (SOIRS), and the Carnegie Type II Supernova Survey (CATS). The photometry is based on template-subtracted images to eliminate any potential host galaxy light contamination, and calibrated from foreground stars. This work presents these photometric data, studies the color evolution using different bands, and explores the relation between the magnitude at maximum brightness and the brightness decline parameter (s) from maximum light through the end of the recombination phase. This parameter is found to be shallower for redder bands and appears to have the best correlation in the B band. In addition, it also correlates with the plateau duration, being shorter (longer) for larger (smaller) s values.

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“…The success of amateur and professional supernova surveys (e.g., Calán/Tololo, Hamuy et al 1993;LOSS, Li et al 2011;CHASE, Pignata et al 2009; PTF/iPTF, Rau et al 2009;Pan-Starrs, Kaiser et al 2002;ASAS-SN, Shappee et al 2014) has been paramount for follow-up studies that have uncovered the full range of observed and physical properties of normal SN II as well as significant correlations between some of their properties (e.g. Hamuy 2003;Arcavi et al 2012;Anderson et al 2014;Faran et al 2014;Gutiérrez et al 2014;Sanders et al 2015;Pejcha & Prieto 2015a,b;Holoien et al 2016;Valenti et al 2016;Rubin et al 2016).…”

Section: Introductionmentioning

confidence: 99%

The Nickel Mass Distribution of Normal Type II Supernovae

Müller

Prieto

Pejcha

et al. 2017

ApJ

112

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Core-collapse supernova explosions expose the structure and environment of massive stars at the moment of their death. We use the global fitting technique of Pejcha & Prieto (2015a,b) to estimate a set of physical parameters of 19 normal Type II SNe, such as their distance moduli, reddenings, 56 Ni masses M Ni , and explosion energies E exp from multicolor light curves and photospheric velocity curves. We confirm and characterize known correlations between M Ni and bolometric luminosity at 50 days after the explosion, and between M Ni and E exp . We pay special attention to the observed distribution of M Ni coming from a joint sample of 38 Type II SNe, which can be described as a skewed-Gaussian-like distribution between 0.005 M ⊙ and 0.280 M ⊙ , with a median of 0.031 M ⊙ , mean of 0.046 M ⊙ , standard deviation of 0.048 M ⊙ and skewness of 3.050. We use twosample Kolmogorov-Smirnov test and two-sample Anderson-Darling test to compare the observed distribution of M Ni to results from theoretical hydrodynamical codes of core-collapse explosions with the neutrino mechanism presented in the literature. Our results show that the theoretical distributions obtained from the codes tested in this work, KEPLER and Prometheus Hot Bubble, are compatible with the observations irrespective of different pre-supernova calibrations and different maximum mass of the progenitors.

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The 1990 Calan/Tololo Supernova Search

Cited by 115 publications

References 0 publications

[ITAL]BVRI[/ITAL] Light Curves for 22 Type I[CLC]a[/CLC] Supernovae

[ITAL]BVRI[/ITAL] Light Curves for 22 Type I[CLC]a[/CLC] Supernovae

UBVRIz LIGHT CURVES OF 51 TYPE II SUPERNOVAE

The Nickel Mass Distribution of Normal Type II Supernovae

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