TY - JOUR
T1 - The first systematic study of type Ibc supernova multi-band light curves
AU - Drout, Maria R.
AU - Soderberg, Alicia M.
AU - Gal-Yam, Avishay
AU - Cenko, S. Bradley
AU - Fox, Derek B.
AU - Leonard, Douglas C.
AU - Sand, David J.
AU - Moon, Dae-Sik
AU - Arcavi, Iair
AU - Green, Yoav
N1 - National Science Foundation (NSF) [AST-1009571, AST-0401479]; Department of Defense [0754568]; Smithsonian Institution; Israeli Science Foundation (ISF); EU; Gruber AwardsM.R.D. and A.M.S. acknowledge support by the National Science Foundation Research Experiences for Undergraduates (REU) and Department of Defense Awards to Stimulate and Support Undergraduate Research Experiences (ASSURE) programs under grant 0754568 and by the Smithsonian Institution. The work of A.G. is supported by grants from the Israeli Science Foundation (ISF), an EU/FP7 Marie Curie IRG Fellowship and a research grant from the Gruber Awards. S.B.C acknowledges generous support from Gary and Cynthia Bengier and the Richard and Rhoda Goldman Foundation. The work of D.C.L. is supported by National Science Foundation (NSF) grant AST-1009571. D.C.L. is grateful for an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-0401479, during which part of this work was completed.
PY - 2011/11/10
Y1 - 2011/11/10
N2 - We present detailed optical photometry for 25 Type Ibc supernovae (SNe Ibc) within d ≈ 150 Mpc obtained with the robotic Palomar 60 inch telescope in 2004-2007. This study represents the first uniform, systematic, and statistical sample of multi-band SNe Ibc light curves available to date. We correct the light curves for host galaxy extinction using a new technique based on the photometric color evolution, namely, we show that the (V - R) color of extinction-corrected SNe Ibc at Δt ≈ 10 days after V-band maximum is tightly distributed, 〈(V - R)V10〉 = 0.26 ± 0.06mag. Using this technique, we find that SNe Ibc typically suffer from significant host galaxy extinction, 〈E(B - V)〉 ≈ 0.4mag. A comparison of the extinction-corrected light curves for helium-rich (Type Ib) and helium-poor (Type Ic) SNe reveals that they are statistically indistinguishable, both in luminosity and decline rate. We report peak absolute magnitudes of 〈M R 〉 = -17.9 ± 0.9mag and 〈MR 〉 = -18.3 ± 0.6mag for SNe Ib and Ic, respectively. Focusing on the broad-lined (BL) SNe Ic, we find that they are more luminous than the normal SNe Ibc sample, 〈MR 〉 = -19.0 ± 1.1mag, with a probability of only 1.6% that they are drawn from the same population of explosions. By comparing the peak absolute magnitudes of SNe Ic-BL with those inferred for local engine-driven explosions (GRB-SN1998bw, XRF-SN2006aj, and SN2009bb) we find a 25% probability that relativistic SNe are drawn from the overall SNe Ic-BL population. Finally, we fit analytic models to the light curves to derive typical 56Ni masses of M Ni ± 0.2 and 0.5 M ⊙ for SNe Ibc and SNe Ic-BL, respectively. With reasonable assumptions for the photospheric velocities, we further extract kinetic energy and ejecta mass values of M ej ≈ 2 M ⊙ and EK ≈ 1051erg for SNe Ibc, while for SNe Ic-BL we find higher values, M ej ≈ 5 M ⊙ and EK ≈ 1052erg. We discuss the implications for the progenitors of SNe Ibc and their relation to those of engine-driven explosions.
AB - We present detailed optical photometry for 25 Type Ibc supernovae (SNe Ibc) within d ≈ 150 Mpc obtained with the robotic Palomar 60 inch telescope in 2004-2007. This study represents the first uniform, systematic, and statistical sample of multi-band SNe Ibc light curves available to date. We correct the light curves for host galaxy extinction using a new technique based on the photometric color evolution, namely, we show that the (V - R) color of extinction-corrected SNe Ibc at Δt ≈ 10 days after V-band maximum is tightly distributed, 〈(V - R)V10〉 = 0.26 ± 0.06mag. Using this technique, we find that SNe Ibc typically suffer from significant host galaxy extinction, 〈E(B - V)〉 ≈ 0.4mag. A comparison of the extinction-corrected light curves for helium-rich (Type Ib) and helium-poor (Type Ic) SNe reveals that they are statistically indistinguishable, both in luminosity and decline rate. We report peak absolute magnitudes of 〈M R 〉 = -17.9 ± 0.9mag and 〈MR 〉 = -18.3 ± 0.6mag for SNe Ib and Ic, respectively. Focusing on the broad-lined (BL) SNe Ic, we find that they are more luminous than the normal SNe Ibc sample, 〈MR 〉 = -19.0 ± 1.1mag, with a probability of only 1.6% that they are drawn from the same population of explosions. By comparing the peak absolute magnitudes of SNe Ic-BL with those inferred for local engine-driven explosions (GRB-SN1998bw, XRF-SN2006aj, and SN2009bb) we find a 25% probability that relativistic SNe are drawn from the overall SNe Ic-BL population. Finally, we fit analytic models to the light curves to derive typical 56Ni masses of M Ni ± 0.2 and 0.5 M ⊙ for SNe Ibc and SNe Ic-BL, respectively. With reasonable assumptions for the photospheric velocities, we further extract kinetic energy and ejecta mass values of M ej ≈ 2 M ⊙ and EK ≈ 1051erg for SNe Ibc, while for SNe Ic-BL we find higher values, M ej ≈ 5 M ⊙ and EK ≈ 1052erg. We discuss the implications for the progenitors of SNe Ibc and their relation to those of engine-driven explosions.
KW - gamma-ray burst: general
KW - supernovae: general
UR - http://www.scopus.com/inward/record.url?scp=80155195174&partnerID=8YFLogxK
U2 - https://doi.org/10.1088/0004-637X/741/2/97
DO - https://doi.org/10.1088/0004-637X/741/2/97
M3 - مقالة
SN - 0004-637X
VL - 741
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - 97
ER -