[6, 7] ( ) M V 19.3 mag [7] Ia Ia d d m λ M λ M λ = m λ lg d A λ, (1) A λ = 0 A λ ( λ mag) 0.1 mag 5% Ia [8] Ia SN 1994D A V = 0.18 mag [

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1 33 2 Vol. 33, No PROGRESS IN ASTRONOMY May, 2015 doi: /j.issn Ia ( ) Ia Ia Ia R V Ia 0.1 mag Ia Ia R V Ia Ia Ia P145.3 A 1 Ia [1] [2, H 0 Ω M Ω Λ 3] Saul Perlmutter Brian Schmidit Adam Riess Ia 2011 [4, 5] Ia ( ) ( ) 973 (2014CB845702) bjiang@bnu.edu.cn

2 [6, 7] ( ) M V 19.3 mag [7] Ia Ia d d m λ M λ M λ = m λ lg d A λ, (1) A λ = 0 A λ ( λ mag) 0.1 mag 5% Ia [8] Ia SN 1994D A V = 0.18 mag [9] SN 2003cg [10] A V = 2.3 mag SN 2002cv A V = 7.9 mag [11] Ia Ia 2 Ia 3 Ia 4 4 Ia Ia R V R V 2 Ia A λ ( A λ λ ) E(B V ) R V ( A V /E(B V )) Ia Ia [12 14] Ia [13, 15, 16] 2.1 Ia B Ia 20 d [17, 18] I B [17] U B V R 20 d R IJHK 30 d 50 d ( 1)

3 2 Ia SN 2014J R [19] [20, 21] Hamuy BV [20] Höflich [22] Pinto Eastman [23] (Fe II) Kasen Fe 56 Ni Ia Ca [24] 2.2 Parrent Ia [25] Ia Si II Ca II S II O I Mg II P Cygni Fe II P Cygni [26] Ia Ia [27] 1991T [28]

天文学进展 144 [29] 1991bg 33 卷 SN 1991bg 爆炸早期的光谱在波长 4200 A 附近表现出很宽的吸收特征被认为是由低激发的 Ti II 产生的在 SN 1991T 的光极大附近的光谱中高激发的 Fe III 占主导地位缺少 Si II 和 Ca II 的吸收线只有在光极大几周之后其谱线才与正常 Ia 型超新星一致图 2 给出了正常 Ia

4 天文学进展 144 [29] 1991bg 33 卷 SN 1991bg 爆炸早期的光谱在波长 4200 A 附近表现出很宽的吸收特征被认为是由低激发的 Ti II 产生的在 SN 1991T 的光极大附近的光谱中高激发的 Fe III 占主导地位缺少 Si II 和 Ca II 的吸收线只有在光极大几周之后其谱线才与正常 Ia 型超新星一致图 2 给出了正常 Ia 型超新星 SN 2014J 在 B 极大前后 10 d 内 µm 的光谱图图2 SN 2014J 在 B 极大前后 10 d 内 µm 的光谱图 [35] 光谱两侧的数字表示相对极大值时间的天数不同颜色代表来自不同观测设备的光谱光谱特征经常被用来表征 Ia 型超新星的物理性质根据谱线的多普勒速度和等值宽度 [30 32] 等可以将 Ia 型超新星进行分类不同的子类具有不一样的物理特征和消光性质 Wang 谱线计算的爆炸速度将 Ia 等人根据 158 个 Ia 型超新星在 B 极大附近的 Si II 6355 A 型超新星分为正常 (Normal) (hvi = ( ± 400) km s 1 ) 和高速 (High Velocity 简称

5 2 Ia 145 HV) (v km s 1 ) R V 2 R V (Normal) = 2.36 ± 0.09 R V (HV) = 1.58 ± 0.08 [32] Wang 2013 Ia Ia [33] 2.3 Ia Lira Ia B V V d [34] Phillips SN 1992A, 1992bc, 1992bo 1994D 4 Ia V d [13] (B V ) 0 = (t V 60), (2) t V V ( d ) Lira Lira [34] Folatelli (CSP) Ia [21] Lira (B V ) 0 = 0.732(0.006) (0.0005)(t V 55) Phillips 3 Ia d (B V ) 0 E(B V ) Förster [36] B V 89 Ia 3 10 Ia B V Lira 30 d t V 80 d B V [21]

6 Ia Krisciunas 8 Ia V K V H B B 4 V J V K V H 8 Ia V K V H V J mag, mag, mag [8] B V ( 0.1 mag) 30 d ( 1.1 mag) (V R R I) B V [37] Meikle 1986G J H 0.2 mag 1.3 mag H K 0.2 mag 0.2 mag [38] Ia B (B V ) 0 = ( 0.07 ± 0.03) mag, (V I) 0 = ( 0.32 ± 0.04) mag [13] 3 Ia Ia 4 (1) (2) (Inter-Galactic Medium IGM) (3) Ia (Circumstellar Medium CSM) (4) Ia (Interstellar Medium ISM) 3.1 Ia 1998 Schlegel IRAS (Infrared Astronomical Satellite) COBE (Cosmic Background Explorer) [39] (CCM ) [40] 2011 Schlafly SDSS (Sloan Digital Sky Survey) Schlegel [41] A V = R V E(B V ) R V [42] Ia R V Ia R V R V 3.1 R V 3.2 (IGM) (CMB) (CIB) IGM [43] IGM Aguirre IGM

7 2 Ia 147 R V Ia [44, 45] Ménard SDSS R V 4.9 IGM z <0.5 A V 0.03 mag [46] IGM Ia IGM [43] 3.3 [47] 2011 Sternberg Ia Na I D ( ) [48] Na I D CSM [49, 50] Patat SN 2006X Na I D 1 D 2 CSM Ia CSM Johansson Herschel SN 2011by, 2011fe 2012cg Ia 70 µm 160 µm T dust 500 K a = 0.1 µm SN 2011fe M dust M SN 2011by 2012cg M dust 0.1 M [51] Phillips 32 Ia Na I 5780 Å DIB (Diffuse Interstellar Band) DIB CSM Ia Na I [52] SN 2003gd NGC 628 II 250 d 0.02 M [53] SN 1987A 1999em 10 4 M [54, 55] SN 1987A 1 mag 2014 Indebetouw ALMA (Atacama Large Millimeter/sub-millimeter Array) SN 1987A 0.2 M 2 3 [56] Gall IIn 2010jl R V 6.4 ( 6.0) [57] R V 3.0 R V = 6.4 II Ia Ia Ia ( )

8 Ia R V [42] Ia R V [58] Ia (edge-on) (face-on) Ia [59] K Ia z K Oke Sandage [60] Humanson [61] K K (Spectral Energy Distribution SED) F (λ) S i (λ) λ i K K i (z) = 2.5 lg(1 + z) lg { } F (λ)si (λ)dλ F [λ/(1 + z)]si (λ)dλ, (3) λ F (λ) 1/(1 + z) z [62] 1993 Hamuy 3 Ia z = B V K [62] Kim 1996 R K K Ia [63] Ia 2002 Nugent Ia SED R V =3.1 SED [64] Ia SED SED SED [65] (1) (

9 2 Ia 149 Ia ) Ia Ia Ia Tammann Leibundgut 1990 B σ B 0.53 mag [66] Ia ( ) σ B = 0.43 mag σ V = 0.08 mag [67] Virgo 6 Ia Branch Tammann σ B = 0.36 mag σ V = 0.29 mag 0.38 mag σ B σ V = mag [67] m 15 (B) ➀ 1993 Phillips Ia BVI m 15 (B) Phillips [12] V M max (V ) = m 15 (B), (4) m 15 (B) Ia Hamuy 29 ( 3 ) Ia BVI 0.17 mag 0.14 mag 0.13 mag [14] Tripp m 15 (B V ) ➁ max 7 Ia Hamuy 29 Ia χ 2 B 0.14 mag [15] m 15 (B) Riess (MLCS) 20 Ia 0.12 mag [68] Perlmutter s ➂ B 0.19 mag [4, 69] s m 15 (B) [69] m 15 (B) = (1.96 ± 0.17)(s 1 1) , (5) m 15 (B) Wang B ➀ B 15 d B Ia SED m 15 (B) 0.1E(B V ) [13] 0.065E(B V ) [21] ➁ B V 1 ➂ Ia Ia s [69]

10 (CMAGIC) m 15 (B) (B V ) max 0.05 mag Ia 0.11 mag [70] Wang C 12 B 12 d B V M B = ( ± 0.06) mag M V = ( ± 0.05) mag [71] Ia m 15 m 15 (B) m 15 (B) [21, 72 76] Phillips 1993 I [12] Elias Ia mag [77] Krisciunas JHK mag [72] B V Ia [78] Ia 4.3 Ia E(B V ) B V (B V ) 0 Ia E(B V ) Gal E(B V ) Host (B V ) 0 max Ia [21, 79, 80] Ia (B V ) 0 max m 15 Ia [81] Ia Ia 3 (1) Na I Ca II (2) E S0 (3) 3 Ia 1 m 15 (B) 4 (B V ) 0 max = a + b[ m 15 (B) 1.1] 1.1 m 15 (B) a B V m 15 Ia ( m 15 (B) > 1.7 mag) m 15 (B) > 1.7 mag m 15 Foley B V Si II Ca II H&K (B V ) 0 max =

11 2 Ia a b rms N ( ) (0.012) (0.037) [13] 0.08 (0.03) 0.09 (0.08) 5 [81] (0.010) (0.044) [82] (0.014) 0.12 (0.05) [21] ( 0.20 ± 0.06) (0.013 ± 0.004) (vca 0 II H&K /1000 km s 1 ) / ( km s 1 ) ( ± 0.008)/(0.013 ± 0.009) mag [83] Burns S BV ( s B V ) Ia [84] Phillips 19 E S0 Ia E(B V ) Avg = (0.02 ± 0.03) mag [13] 0 E S0 Ia 4.4 A V E(B V ) R V Ia m 15 (B) E(B V ) Ia (1) Tully-Fisher Ia Ia V R V Ia R V (1) R V Ia ( 4) Folatelli CSP Ia R V R V 1.7 R V [21] (2) Ia Tripp Tripp Branch [15, 16] CSP Folatelli R V 1.5 [21] Ia ( ) R V [82] 2 Ia R V

12 SN 2005 SN 2006X X λ =u,g,r,i,b,y,j,h,k E(V X λ ) CCM+O CCM+O R V = 3.1 Goobar(2008) [98] [21] R V 3.0 Ia R V 2.0 [85] Ia R V < 2 E(B V ) < 0.3 Ia R V 3.0 [21, 78] R V 3.0 HD R V 2.0 [86] Szomoru Guhathakurata 4 R V 2 [87] R V < 3.0 Brown Ia 2014J R V 1.4 [88] HD R V R V R V 0.7 R V [89] Ia R V Phillips Ia R V Ia R V 3.1 [52] R V R V R V R V Ia Ia 30 Dor R V Å M Å

13 2 Ia Ia R V Ia E(B V ) host R V 1999cl 1.24 (0.07) 1.55 (0.08) [90] 2001el 0.21 (0.05) 2.15 (0.23) [91] 2002cv 5.45 (0.28) 1.59 (0.07) [92] 2003cg 1.33 (0.11) 1.80 (0.19) [10] 2005A 1.11 (0.07) 1.68 (0.10) [21] 2006X 1.34 (0.07) 1.55 (0.07) [21] 2006X 1.42 (0.04) 1.48 (0.06) [93] 2014J 1.23 (0.01) 1.46 [35] 0.5 [67] (0.30) [96] (0.11) [97] 80 E(B V ) host < (0.27) 69 E(B V ) host < (0.25) [94] 42 HV 1.58 (0.07) 83 Normal 2.36 (0.07) [32] 34 CSP 1.7 (0.1) 32 SN 2005A SN 2006X 3.2 (0.4) [21] A V A V 1.0 < 2 [95] NGC 2207 R V = 5.0 AM R V = 3.4 ± 0.2 AM R V 2.5 ± 0.4 Sc NGC 3314A R V = 3.5 ± 0.2 R V Draine 2003 [42] Ia R V Branch (1) (2) Ia Ia Ia (3) R V R V (4) Ia B V [67] Ia Ia R V [95] R V 0.5 R V 0.7 Riess MLCS 20 Ia Ia R V = 2.6 ± 0.3 Ia ISM CSM

14 [96] Ia ISM R V Ia Mandel MCMC 127 Ia (A V 0.4) Ia R V R V (A V 1.0) R V < 2.0 [95] R V Reindl R V Ia Ia [82] Wang Ia R V [97] Goobar Ia R V [98] Amanullah Goobar Ia r = cm m 15 σ BV = mag [99] Phillips Ia 5780 Å DIB Ia DIB ISM Ia ISM ISM R V ISM [52] Johansson Ia 2014J 10 5 M [100] R V Ia 4 SN 2005A SN 2006X Ia [21] (CCM+O CCM89 O Donnell [101] ) R V u Goobar Ia Amanullah SN 2014J 2750 Å K Fitzpatrick [102] R V 1.4 [103] Ia R V 2.0 [85, 104] Ia 2.0 R V (E(B V ) < 0.3 mag) (A V < 0.4 mag) Ia R V 3.0 [21, 78] R V Ia

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18 [102] Fitzpatrick E L. PASP, 1999, 111: 63 [103] Amanullah R, Goobar A, Johansson J, et al. ApJ, 2014, 788: L21 [104] Conley A, Carlberg R G, Guy J, et al. ApJ, 2007, 664: L13 [105] Gao J, Jiang B, Li A, et al. to appear in ApJ, 2015 Extinction Correction for Type Ia Supernovae LI Jun, JIANG Bi-wei (Department of Astronomy, Beijing Normal University, Beijing , China) Abstract: Type Ia supernovae (SNe Ia) are widely used as a standard candle in cosmology. They have very high (as bright as an entire galaxy) and almost constant luminosity. Their absolute magnitude in visual bands presents very small dispersion of around 0.1 mag after modified according to their declining rate and correction for the extinction. Their intrinsic color index shows very homogeneous law of variation in a period after the maximum light. Understanding the extinction of SNe Ia is a key to its application in cosmology. In principle, there are four sources of extinction to SNe Ia in extra-galaxies: (1) the Galactic foreground interstellar extinction, (2) the intergalactic extinction, (3) the circumstellar extinction, and (4) the interstellar extinction of the host galaxy, with the later two contributors being significant and unclear. The extinction is calculated by comparing the observed colors and the intrinsic colors derived from their light-variation properties or from the dispersion in the Hubble diagram. The selective extinction ratio R V is found generally smaller than the typical Galactic value 3.1, although different methods and samples yield a range of values with some of them being consistent with the Galactic case. The extinction curve from ultra-violet to near-infrared is obtained for several SNe Ia with abundant observations, which can either be fit by the Galactic extinction law but with low R V value or by a power law. This fact may imply that the dust in the SNe Ia host galaxies tends to have smaller average size than the Galactic one. Meanwhile, a multiple-scattering model in the circumstellar envelope can also explain the difference in R V. Key words: supernovae; type Ia supernovae; extinction; dust

[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

[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