Type Ia and II supernovae contributions to the metal enrichment in the intra-cluster medium observed with Suzaku ApJ Letter, vol. 667, L41, 2007 PASJ, vol. 59, 299, 2007 PASJ, in press, astro-ph/070.4342, Kosuke Sato1, K. Tokoi2, K. Matsusihta1, Y. Ishisaki2, N. Y. Yamasaki3, M. Ishida3, and T. Ohashi2 1 Tokyo Univ. of Science, 2 Tokyo Metropolitan Univ., 3 ISAS/JAXA

Introduction – past X-ray observations – “ ASCA ” ⇒ Dupke & White (2000), Baumgartner et al. (2005) “ XMM ” ⇒ de Plaa et al. (2006,2007), Werner et al. (2006) XMM 22 clusters O in the only central region Mg with large uncertainties de Plaa et al. (2007) SNe II/Ia ratio ~3.5 Poor information from SNe II products Suzaku Low & stable background level Higher sensitivity below ~1 keV Determination of various elements from O to Fe

Merits of Suzaku XIS A1060 Suzaku Oxygen XMM XMM Suzaku BI FI Superior O Line sensitivity Suzaku BI FI XMM Tsunemi et al. (2006) A1060 Oxygen Suzaku XMM Low intrinsic non X-ray Background (NXB) & Good reproducibility (～5%） due to low orbit satellite & short focal length High line sensitivity below ～1 keV Suitable for extended objects, like clusters & groups

Selected clusters and groups Nearby and Bright objects in early Suzaku observations Moderate low temperature (kT<4 keV) for O measurement Obs. redshift r180（Mpc） date A1060 AWM7 HCG62 NGC507 0.0114 0.0172 0.0145 0.0165 1.53 1.65 1.08 22/Nov./2005 5/Aug./2006 23/Jan./2006 28/Jul./2006 Sampling ranging: Groups (~1.5 keV) ~ Clusters (~4 keV) Not including in de Plaa et al. (2007) Measurements of the metal abundance and distributions to ~0.3 r180 Analysis methods : See in Sato et al. (2007a, 2007b) & Tokoi et al. (2007)

X-ray Images with Suzaku Smoothed with σ = 16″gaussian, Exposure time corrected Cosmic X-ray Background, Non X-ray Background subtracted A1060 AWM7 0.5-7.0 keV 10′ (140 kpc） (210 kpc) 0.1 r180 HCG62 0.5-4.0 keV (178 kpc) 0.1 r180 NGC507 0.5-4.0 keV (200 kpc) 0.1 r180 10′ 10′

O & Mg measurements with Suzaku OVII OVIII O Mg

Metal distributions 1 From O to Fe radial profiles AWM7 A1060 HCG62 NGC507 1 From O to Fe radial profiles （solar: Anders & Grevesse 1989） Comparison the metals to Fe ratio Si, S / Fe : fairly flat ~1 – 2 O, Mg / Fe : increase with radius? ⇒ Difference from SNe Ia or II ? 1 （solar） 0.1 Radial profiles of Fe r / r180 O/Fe 1 1 1 Mg/Fe Si/Fe r / r180 r / r180 r / r180

Numbers of Type Ia and II supernovae How each metal is synthesized with SN Ia & II ? ⇒ Estimation of the numbers of SN Ia & II （NIa, NII） Fit the amount of metals with nucleosynthesis model SNe nucleosynthesis model SNe Ia ： W7 model （Nomoto et al. 1984） WDD1 or 2 model（Iwamoto et al. 1999） SNe II : 10 – 50 M (Salpeter Initial Mass Function) Progenitor Metallicity Z = 0.02（Nomoto et al. 2006） ψ（M） ∝ M -2.35

Results : 1 Metal mass （M） AWM7 HCG62 （Ne） NGC507 A1060 O Mg Si S Fe W7, W7,< 0.1 r180 WDD1, WDD2 AWM7 O （Ne） Mg Si S Fe HCG62 NGC507

Results : 2 AWM7（3.5 keV） χ2 / d.o.f. = 15.9 / 3 A1060（3 keV） W7, W7,< 0.1 r180 WDD1, WDD2 AWM7（3.5 keV） χ2 / d.o.f. = 15.9 / 3 A1060（3 keV） χ2 / d.o.f. = 8.5 / 3 Ratio HCG62（1.5 keV） χ2 / d.o.f. = 3.0 / 3 NGC507（1.5 keV） χ2 / d.o.f. = 11.7 / 3 O Mg S Fe （Ne） Si Fits are not acceptable….

Results : 3 AWM7（3.5 keV） A1060（3 keV） Fractions from SNe Ia 0.8 0.6 0.4 AWM7（3.5 keV） W7, W7,< 0.1 r180 WDD1, WDD2 A1060（3 keV） 0.8 0.6 0.4 Fractions from SNe Ia HCG62（1.5 keV） 0.8 0.6 0.4 0.8 0.6 0.4 NGC507（1.5 keV） O Mg Si S Fe ~3/4 of Fe from SNe Ia

Numbers and Ratio of SNe Ia & II SNe II SNe Ia（W7） ＋ 3.5 SNe II/Ia ratio Numbers of SNe Ia & II A1060 AWM7 HCG62 NGC507 A1060 AWM7 HCG62 NGC507 Gas mass（M） Gas mass（M） Numbers of SNe Ia & II are propose to the gas mass SNe II/Ia Ratio: ~3.5 cf. Clusters (XMM ; de Plaa et al. 2007): ~3.5 Our Galaxy (Tsujimoto et al. 1995): ~6.7 LMC & SMC (Tsujimoto et al. 1995): 3.3 – 5

Comparison of Numbers of SNe II Number of SNe II expected from Star Formation Rate of Hubble Deep Field (Madau et al. 1998) Numbers of SNe II expected from the metal mass observed with Suzaku Normalized by K-band（2MASS） luminosities Now, only the metals in the ICM, not including in the stars (galaxies) AWM7 HDF NII / LK （LK-1） A1060 Considering in the stars, the results with X-ray increase by factor ~2 Numbers of SNe II（Mpc-3）

Mass-to-Light Ratio: MLR Metals are synthesized in stars (galaxies): Compare Mmetal, < R ( in units of M ) With B-band luminosity LB, < R ( in units of L ) Also use K-band luminosity because of the comparison of galaxy type Fe mass / B-band Luminosity Mmetal, < R LB or K, < R MLR = M L Makishima et al. (2001) Temperature (keV) ∝ size of system Oxygen Mass-to-Light Ratio: OMLR Magnesium Mass-to-Light Ratio: MMLR Iron Mass-to-Light Ratio: IMLR First time

With K-band, close to the MLR between clusters and groups MLR（B-band vs. K-band）Sato et al. in preparation AWM7 A1060 HCG62 NGC507 AWM7 A1060 HCG62 NGC507 MMLR AWM7 A1060 HCG62 NGC507 IMLR MLR OMLR r / r180 r / r180 r / r180 With K-band, close to the MLR between clusters and groups B-band K-band AWM7 A1060 HCG62 NGC507 AWM7 A1060 HCG62 NGC507 AWM7 A1060 HCG62 NGC507 MLR OMLR IMLR MMLR r / r180 r / r180 r / r180

Summary Conducted spatially resolved spectral analysis of clusters & groups with Suzaku Measurements of the metals (O to Fe) to ~0.3 r180 Assuming nucleosynthesis models, we determined the numbers of SNe II in the past using the metal masses of O, Mg, Si, S, and Fe SNe II / Ia number ratio ~3.5 The Numbers from X-ray observations are consistent with the number from SFR in HDF Measurements of OMLR & MMLR for the first time MLRs with K-band are close between clusters & groups