[19] Ia Ia [20] Ia Phillips [21] [22] 0.15 mag [23 25] Ia Ia Ia [26, 27] Ia [26, 28, 29] Ia [29, 30] Ia 2σ Ia [31 33] Ia [34] Ia [35] Ia [36] I

31 4 Vol. 31, No. 4 2013 11 PROGRESS IN ASTRONOMY Nov., 2013 doi: 10.3969/j.issn.1000-8349.2013.04.02 Ia 1,2,3 1,2 ( 1. / 650011 2. 650011 3. 100049 ) Ia Ia 56 Ni 56 Ni Ia Ia Ia Ia 56 Ni Ia P145.3 A 1 Perlmutter Riess Ia [1, 2] [3 6] [7 12] Ia Ia C+O [13 17] [18] (Ia ) 2013-03-13 2013-06-13 973 (2009CB824800) (11133006,11163006,11173054) (KJCX2- YW-T24)

412 31 [19] Ia Ia [20] Ia Phillips [21] [22] 0.15 mag [23 25] Ia Ia Ia [26, 27] Ia [26, 28, 29] Ia [29, 30] Ia 2σ Ia [31 33] Ia [34] Ia [35] Ia [36] Ia 3σ Ia [35 37] Ia 2 Ia 3 Ia Ia 2 Ia Ia [17] (t < 420 Ma) ( t > 2.4 Ga) ( ) Ia Ia ( ) Ia Ia

4 Ia 413 2.1 2005 Mannucci [26] 2MASS 0.99 Ia E/S0 20 B K < 2.6 mag B K > 4.1 mag 30 Ia / Ia E/S0 2006 Sullivan [28] 0.2 < z < 0.75 SNLS Ia (, specific star formation rates, ssfr) S NR(t) = AM(t) + bṁ(t) A = (5.3 ± 1.1) 10 14 (H/70) 2 SNeM 1 a 1 B = (3.9 ± 0.7) 10 4 (H/70) 2 SNe(M 1 a 1 ) 1 a 1 M(t) t Ṁ 0.5 Ga ss FR 2011 Smith [29] SDSS 0.05 < z < 0.25 342 Ia ( passive galaxy ) Ia S NR M 0.67 Ia S NR M 0.94 Ia Ia 1 Smith 1 Ia [29] Smith [29] SDSS Sullivan [28] SNLS Mannucci [26] 2011 Li [38] LOSS rate-size Ia 2012 Graur [39] SDSS 7 70 000

414 31 90 z 0.1 Ia Li rate-size Ia ( ) ( ) Ia [40, 41] Ia Mannucci [26, 42] t 1 Ia Li [38] 2011 rate-size t 1 Ia Ia 2.2 Ia 2007 Sharon [43] 100 Abell 6 Ia Ia Ia 2008 Mannucci [44] 0.98 Ia 3 2008 Garlberg [45] SNLS Ia Ia Ia 2010 Han [46] Abell Ia Ia Garlberg Han Mannucci Dilday [47] Dilday [47] 0.5 z 0.9 SDSSII ( ) 2010 Sharon [48] 0.5 < z < 0.9 Ia [49, 50]

4 Ia 415 3 Ia 3.1 Ia Ia 0.3 mag [51] (1) Phillips [21, 52, 53] m 15 m 15 15 d (2) [22, 54, 55] E(B V) 0.15 mag Ia Ia Ia (Hubble residuals) HR = µ B µ Z, (1) µ B µ Z z 3.2 ( E/S0 ) ( Sa Sd/Irr ) Ia [56, 57] 50 Ia [58] Ia 2009 Hicken [33] 3 E/S0 Sa Sc Scd/Sd/Irr Ia Scd/Sd/Irr E/S0 (2σ ) 2012 Galbany [59] SDSS E/S0 Ia E/S0

416 31 2012 Meyers [60] Ia z > 0.9 Ia χ 2 Ia 3.3 Ia ( ) Ia spectral energy distribution (SED) SED Ia 2009 Neil [61] 168 Ia Ia 2010 Lampeitl [35] SDSSII 361 Ia Ia ( ) Ia (2σ ) 2010 Lampeitl [35] 2σ Ia 0.1 mag 2010 Sullivan [36] SNLS 2.6σ 2011 Andrea [62] SDSSII 3σ Ia 0.1 mag 2 3.4 Ia 2005 Gallagher [57] Ia Ia [45, 57] Ia 2009 Neil [61] 168 UV Gallagher 22

4 Ia 417 2 [62] Ia 2.1σ Ia 2011 Gupta [34] SDSSII 206 Ia (0.01 < z < 0.42) SED 1.9 σ Ia 3 3.5 Ia SED Ia [35, 37] Ia (3 σ ) 2010 Kelly [37] 70 (0.015 < z < 0.08) Ia 2.5 σ 10% 2010 Lampeitl [35] SDSSII 361 (z < 0.21) Ia Kelly 4σ 4 2011 Gupta [34] 206 SDSSII Ia Sullivan [36]

418 31 3 [34] SNLS3 195 110 Ia 4σ Ia 0.08 mag 4 [35] ( )

4 Ia 419 3.6 Ia 56 Ni 56 Ni Ia Ia [45, 61] 2010 Sullivan [36] SNLS3 Howll 2009 O/H 3σ Ia 5 [30, 62] 2011 Konishi [30] SDSSII 118 Ia R = [N II ]λ6585/[o II ]λ3727 O/H 1.8σ (lg(o/h)+12 > 9) Ia 0.13 mag 2011 Andrea [62] SDSSII R = [N II ]λ6585/[o II ]λ3727 40 3σ Ia 5 [36] Ia Ia S C S S C 3.7 Ia

420 31 Ia 56 Ni 56 Ni 56 Ni ( 56 Ni ) Timmes [63] 2003 56 Ni Howell [64] 2009 Howell (0.2 < z < 0.75) 100 Ia SED ( [65] ) O/H Ia 56 Ni 56 Ni 56 Ni Ia ( ) 6 56 Ni 2009 Neil [61] Ia O/H Howll Timmes 6 56 Ni [61] 7 Kasen [66] 3 0.3 7 3 Phillips 0.3

4 Ia 421 Phillips m 15 < 1.5 m 15 ( Phillips m 15 ) Ia 56 Ni Ia ( ) Kasen 7 Ia Phillips [66] B m 15 B 4 Ia Ia Ia Ia Ia Ia Ia Ia Ia Cooper [67] Ia Ia Ia 56 Ni

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424 31 [69] Wang B, Chen X, Meng X, et al. ApJ, 2009, 701: 1540 [70] Wang B, Han Z. A&A, 2010, 515: A88 [71] Wang X, Wang L, Filippenko A V, et al. Science, 2013, 340: 170 Dependence of SNe Ia Rates and Luminosities on Host Galaxies LIANG Wen-ke 1,2,3, WANG Jian-cheng 1,2 (1. National Astronomical Observatories, Yunnan Observatory, Chinese Academy of Sciences, Kunming 650011, China; 2. Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650011, China; 3. University of Chinese Academy of Sciences, Beijing, China) Abstract: We mainly present the dependence of SNe Ia rate and luminosity on their host galaxies. Firstly, we show that the host galaxy mass is lower or host star-formation rate is higher, SNe Ia rate will be larger. Secondly, we show that before light-curve correction, dimmer SNe Ia fluently occur in higher mass, higher star-formation rate, higher metal abundance, or older stellar galaxy system. However, after light-curve correction, brighter SNe Ia fluently occur in higher mass, higher star-formation rate, higher metal abundance, or older stellar galaxy system. Higher-metallicity progenitors are more neutron rich, producing more stable burning products relative to radioactive 56 Ni. Since SNe Ia explosions are powered by the radioactive decay 56 Ni, it is widely accepted that the intrinsic variation in SNe Ia brightness and decline rate is primarily driven by the amount of 56 Ni present in SNe explosion, where more luminous and much slowly declining explosions are powered by more 56 Ni, hence, under higher-metallicity circumstances, SNe Ia are dimmer. Whereas, after light-curve correction, SNe Ia in higher-metallicity progenitors are brighter. Therefore, the metallicity diversity is responsible for the dependence of SNe Ia luminosties on host galaxies. Key words: supernova; rate; luminosity; host galaxy