SHOCK BREAKOUT IN TYPE II PLATEAU SUPERNOVAE: PROSPECTS FOR HIGH-REDSHIFT SUPERNOVA SURVEYS

Journal Article · Tue Mar 15 00:00:00 EDT 2011 · Astrophysical Journal, Supplement Series

DOI:https://doi.org/10.1088/0067-0049/193/1/20· OSTI ID:21557049

Tominaga, N ^[1]; Morokuma, T ^[2]; Blinnikov, S I; Nomoto, K ^[3]; Baklanov, P ^[4]

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1. Department of Physics, Faculty of Science and Engineering, Konan University, 8-9-1 Okamoto, Kobe, Hyogo 658-8501 (Japan)
2. Institute of Astronomy, University of Tokyo, Mitaka, Tokyo 181-0015 (Japan)
3. Institute for the Physics and Mathematics of the Universe, University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583 (Japan)
4. Institute for Theoretical and Experimental Physics (ITEP), Moscow 117218 (Russian Federation)

Shock breakout is the brightest radiative phenomenon in a supernova (SN) but is difficult to be observed owing to the short duration and X-ray/ultraviolet (UV)-peaked spectra. After the first observation from the rising phase reported in 2008, its observability at high redshift is attracting enormous attention. We perform multigroup radiation hydrodynamics calculations of explosions for evolutionary presupernova models with various main-sequence masses M {sub MS}, metallicities Z, and explosion energies E. We present multicolor light curves of shock breakouts in Type II plateau SNe, being the most frequent core-collapse SNe, and predict apparent multicolor light curves of shock breakout at various redshifts z. We derive the observable SN rate and reachable redshift as functions of filter x and limiting magnitude m {sub x,lim} by taking into account an initial mass function, cosmic star formation history, intergalactic absorption, and host galaxy extinction. We propose a realistic survey strategy optimized for shock breakout. For example, the g'-band observable SN rate for m {sub g',lim} = 27.5 mag is 3.3 SNe deg{sup -2} day{sup -1} and half of them are located at z {>=} 1.2. It is clear that the shock breakout is a beneficial clue for probing high-z core-collapse SNe. We also establish ways to identify shock breakout and constrain SN properties from the observations of shock breakout, brightness, timescale, and color. We emphasize that the multicolor observations in blue optical bands with {approx}hour intervals, preferably over {>=}2 continuous nights, are essential to efficiently detect, identify, and interpret shock breakout.

• OSTI ID: 21557049
• Journal Information: Astrophysical Journal, Supplement Series, Vol. 193, Issue 1; Other Information: DOI: 10.1088/0067-0049/193/1/20; ISSN 0067-0049
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
BRIGHTNESS
COLOR
HYDRODYNAMICS
RADIANT HEAT TRANSFER
RED SHIFT
SHOCK WAVES
STAR EVOLUTION
SUPERNOVAE
BINARY STARS
ENERGY TRANSFER
ERUPTIVE VARIABLE STARS
EVOLUTION
FLUID MECHANICS
HEAT TRANSFER
MECHANICS
OPTICAL PROPERTIES
ORGANOLEPTIC PROPERTIES
PHYSICAL PROPERTIES
STARS
VARIABLE STARS