1. Jounal Club 04/04, Sunmyon Chon [1a]Gravitational Waves from the Remnants of the First Stars, T. Hartwig et al. [arXiv:1603.05655 ]arXiv:1603.05655 and [1b]Strong gravitational wave background from Population III binary black holes consistent with cosmic reionization, K.Inayoshi et al. [arXiv:1603.06921]arXiv:1603.06921 [2] Faint COSMOS AGN at z 〜 3.3 - I. Black Hole Properties and Constraints on Early Black Hole Growth, B. Trakhtenbrot et al.[arXiv:1512.04551]arXiv:1512.04551 [3] Shock Breakout and Early Light Curves of Type II-P Supernovae Observed with Kepler, P. M. Garnavich et al., 2016ApJ...820...23G2016ApJ...820...23G

2. [1a]Gravitational Waves from the Remnants of the First Stars GW150914 observed by aLIGO => Binary Black Hole (BBH) with M 1 〜 36 M  and M 2 〜 36 M  => local merger density : 2 – 400/yr/Gpc 3 ・ Previous study (Kinugawa et al., 2014) predicts the typical chirp mass around M = 30 M . ・ This paper estimate the merger rate density of PopIII remnant BH and its detectability based on, -SFR consistent with Planck result, τ = 0.066 -Initial condition motivated by numerical simulation -different stellar evolution model

3. [1a]Gravitational Waves from the Remnants of the First Stars ・ Give star formation history of PopIII stars by Semi-analytical model based on Monte-Carlo merger tree ・ log flat IMF ・ Pop I/II star formation histories are given analytically. Initial condition for the PopIII binary ・ binary fraction = 36 % ・ distributions of eccentricity (e) and semi-major axis (a) p(e)de ∝ e de where 0.1 < e < 1.0 p(x)dx ∝ x -1/2 dx where x = log(a/R  ) and 50 R  < a < 2×10 6 R  Binary evolution model ・ tabulated model by de Mink & Belczynski (2015) ( stellar evolution model with Z=0.002, etc)

4. [1a]Gravitational Waves from the Remnants of the First Stars Give initial condition (M 1, M 2, a, e) from presentation slide by Kinugawa at Rironkon2015

5. [1a]Gravitational Waves from the Remnants of the First Stars This paper Kinugawa+14 => Pop III SFR density is lower than the previous study Fig. 1 Fig. 3

6. [1b] Strong gravitational wave background from Population III binary black holes consistent with cosmic reionization In this paper, authors focus on the GW background. f esc f binary mass ratiostellar evolution model Harwig et al.0.538%semi-analyticde Mink & Belczynski (2015), Z=0.002 Inayoshi et al.0.170% Φ(q)dq ∝ q dq Kinugawa et al. (2014), Z=0 Fig. 3 Fig. 4 = 30 M  = 50 M 

7. [2] Faint COSMOS AGN at z 〜 3.3 - I. Black Hole Properties and Constraints on Early Black Hole Growth ・ This paper investigates the early growth of AGN and SMBH. => focus on 14 faint AGNs in COSMOS Field. => estimate M BH, f Edd = L/L edd, η ・ Conclusion Significant number of z 〜 6 AGNs should be detected by CDF-S 4Ms, but not. Why? Hβ: 4861 Å Fig. 1 Fig. 2

8. M BH : estimated by virial theorem by line width: σ Hβ, σ Hα [2] Faint COSMOS AGN at z 〜 3.3 - I. Black Hole Properties and Constraints on Early Black Hole Growth this study  ・ small M BH 〜 8×10 8 M  ・ 0.1 < f Edd < 1 (consistent with SSDS quasars at 0.5 < z < 1) ・ f Edd < 0.1 only for 1 sample (SMBH at the final stage?)

9. [2] Faint COSMOS AGN at z 〜 3.3 - I. Black Hole Properties and Constraints on Early Black Hole Growth solid : f Edd = const dashed : f Edd ∝ (1+z) 2 significant population of faint AGNs at z 〜 6 is expected but not observed so far.

10. [2] Faint COSMOS AGN at z 〜 3.3 - I. Black Hole Properties and Constraints on Early Black Hole Growth Why faint z 〜 6 AGNs are not observed? (i) obscured fraction is higher at the high-z (“receding torus” model, but have little observational evidence) (ii) radiative efficiency η is lower at high-z (iii) AGN duty cycle is smaller at the initial stage => not enough time for the SMBH growth Combination of (i) and (ii)?

11. [3] Shock Breakout and Early Light Curves of Type II-P Supernovae Observed with Kepler Roger Chevalier, 2008 The first optical detection of a shock breakout from a type II-P supernova by Kepler. (UV detection; Schawinski+,2008; Gezari+,2015) The radiation from the shock wave “breaks out” of the stellar surface. Typical duration ： sec 〜 day Stellar structure before the explosion can be studied. Kepler: monitored about 500 galaxies at 30-min cadence

12. [3] Shock Breakout and Early Light Curves of Type II-P Supernovae Observed with Kepler zoom in Fig. 2 Fig. 4 Fig. 1