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1 Understanding Black Hole Formation and Natal Kicks: The Case of Cygnus X-1 TsingWai Wong Francesca Valsecchi, Tassos Fragos, Bart Willems, Vicky Kalogera
2 Background & Purpose Find the mass relationship between stellar mass black holes (BH) and their immediate progenitors Determine the natal kicks magnitude imparted to the black hole Shed light on the core collapse mechanism 2
3 16 fairly well constrained BH X-ray binaries in Milky way: (from Charles Bailyn) 3
4 16 fairly well constrained BH X-ray binaries in Milky way: I. wind-fed, high mass (from Charles Bailyn) 3
5 16 fairly well constrained BH X-ray binaries in Milky way: I. wind-fed, high mass II. late-type, P < 1 day (from Charles Bailyn) 3
6 16 fairly well constrained BH X-ray binaries in Milky way: I. wind-fed, high mass II. late-type, P < 1 day III. early-type, P > 1 day (from Charles Bailyn) 3
7 16 fairly well constrained BH X-ray binaries in Milky way: I. wind-fed, high mass II. late-type, P < 1 day III. early-type, P > 1 day IV. giants, P > 1 day (from Charles Bailyn) 3
8 16 fairly well constrained BH X-ray binaries in Milky way: I. wind-fed, high mass II. late-type, P < 1 day III. early-type, P > 1 day IV. giants, P > 1 day In other galaxies: M33 X-7, IC 10 X-1, NGC 300 X-1 (from Charles Bailyn) 3
9 16 fairly well constrained BH X-ray binaries in Milky way: I. wind-fed, high mass II. late-type, P < 1 day III. early-type, P > 1 day IV. giants, P > 1 day In other galaxies: M33 X-7, IC 10 X-1, NGC 300 X-1 (from Charles Bailyn) 3
10 16 fairly well constrained BH X-ray binaries in Milky way: I. wind-fed, high mass II. late-type, P < 1 day III. early-type, P > 1 day IV. giants, P > 1 day In other galaxies: M33 X-7, IC 10 X-1, NGC 300 X-1 (from Charles Bailyn) 3
11 Black Hole High mass X-ray Binary (Wind-fed) Low mass X-ray Binary (Roche lobe overflow) Step 1: Model current observed properties Step 2: Find the peculiar velocity post BH formation Step 3: Compute the dynamics involved in core collapse Step 4: Match the observed orbital period and eccentricity Derive limits on immediate progenitor mass and natal kicks magnitude 4
12 Black Hole Cygnus X-1 High mass X-ray Binary (Wind-fed) Step 1: Model current observed properties Step 2: Find the peculiar velocity post BH formation Step 3: Compute the dynamics involved in core collapse Step 4: Match the observed orbital period and eccentricity Derive limits on immediate progenitor mass and natal kicks magnitude 4
13 Black Hole Cygnus X-1 High mass X-ray Binary (Wind-fed) Step 1 Step 1: Model current observed properties Step 2: Find the peculiar velocity post BH formation Step 3: Compute the dynamics involved in core collapse Step 4: Match the observed orbital period and eccentricity Derive limits on immediate progenitor mass and natal kicks magnitude 4
14 Black Hole Cygnus X-1 High mass X-ray Binary (Wind-fed) Step 2 Step 1: Model current observed properties Step 2: Find the peculiar velocity post BH formation Step 3: Compute the dynamics involved in core collapse Step 4: Match the observed orbital period and eccentricity Derive limits on immediate progenitor mass and natal kicks magnitude 4
15 Black Hole Cygnus X-1 High mass X-ray Binary (Wind-fed) Step 3 Step 1: Model current observed properties Step 2: Find the peculiar velocity post BH formation Step 3: Compute the dynamics involved in core collapse Step 4: Match the observed orbital period and eccentricity Derive limits on immediate progenitor mass and natal kicks magnitude 4
16 Black Hole Cygnus X-1 High mass X-ray Binary (Wind-fed) Step 4 Step 1: Model current observed properties Step 2: Find the peculiar velocity post BH formation Step 3: Compute the dynamics involved in core collapse Step 4: Match the observed orbital period and eccentricity Derive limits on immediate progenitor mass and natal kicks magnitude 4
17 Step 1: Model current observed properties evolve the companion as an isolated star BH Cyg X-1 Step 1 modified version of stellar evolution code EZ (originally developed by Paxton 2004) 5
18 Step 1: Model current observed properties evolve the companion as an isolated star BH Cyg X-1 Step 1 modified version of stellar evolution code EZ (originally developed by Paxton 2004) Parameter Value Reference Inclination angle (deg) ± 0.76 Orosz et al. (2011) Black hole mass (M ) ± 0.98 Orosz et al. (2011) Black hole spin > 0.95 Gou et al. (2011) Companion mass (M ) ± 1.90 Orosz et al. (2011) Companion radius (R ) ± 0.84 Orosz et al. (2011) Companion luminosity (10 5 L ) 2.33 ± 0.42 Orosz et al. (2011) Companion Teff (K) ± 1000 K ± Orosz et al. (2011) X-ray luminosity (10 37 erg/s) ( )( d 1.86 kpc )2 Frontera et al. (2001), McConnell et al. (2002), Cadolle Bel et al. (2006) 5
19 Step 1: Model current observed properties evolve the companion as an isolated star BH Cyg X-1 Step 1 modified version of stellar evolution code EZ (originally developed by Paxton 2004) Parameter Value Reference Inclination angle (deg) ± 0.76 Orosz et al. (2011) Black hole mass (M ) ± 0.98 Orosz et al. (2011) Black hole spin > 0.95 Gou et al. (2011) Companion mass (M ) ± 1.90 Orosz et al. (2011) Companion radius (R ) ± 0.84 Orosz et al. (2011) Companion luminosity (10 5 L ) 2.33 ± 0.42 Orosz et al. (2011) Companion Teff (K) ± 1000 K ± Orosz et al. (2011) X-ray luminosity (10 37 erg/s) ( )( d 1.86 kpc )2 Frontera et al. (2001), McConnell et al. (2002), Cadolle Bel et al. (2006) 5
20 14.81 ± 0.98 M Black Hole MBH = ± 0.98 M Mc = ± 1.90 M Cygnus X-1 6
21 14.81 ± 0.98 M Black Hole MBH = ± 0.98 M Mc = ± 1.90 M Cygnus X M M M 6
22 14.81 ± 0.98 M Black Hole Myr MBH = ± 0.98 M Mc = ± 1.90 M Cygnus X M M M 6
23 Step 2: Find the peculiar velocity post BH formation BH Step 2 Cyg X-1 Parameter Value Reference Distance (kpc) 1.86 ± 0.12 Reid et al. (2009) Galactic longitude (deg) 71.3 Lestrade et al. (1999) Galactic latitude (deg) +3.1 Lestrade et al. (1999) Proper motion in R.A. (mas/yr) 3.78 ± 0.06 Reid et al. (2009) Proper motion in decl. (mas/yr) 6.40 ± 0.12 Reid et al. (2009) track the system s motion in a Galactic potential backwards in time find the peculiar velocity of the system right after the BH formation 7
24 V pec right after the BH formation = 27 ± 5 km/s resulted from the collapse core event 8
25 Step 3: Compute the dynamics involved in core collapse Step 3 BH Cyg X-1 perform Monte Carlo simulation for the - (pre-sn) binary configuration: 1) M 2) A presn 3) e presn 4) orbital phase 5) natal kick (magnitude + direction) 9
26 Step 3: Compute the dynamics involved in core collapse Step 3 BH Cyg X-1 perform Monte Carlo simulation for the - (pre-sn) binary configuration: 1) M 2) A presn 3) e presn 4) orbital phase 5) natal kick (magnitude + direction) constraints: a) survival of the binary b) conservation of orbital energy and angular momentum c) peculiar velocity of the post-sn binary (from step 2: V pec = 27 ± 5 km/s) 9
27 Step 4: Match the observed orbital period and eccentricity observed period = (16) days (Brocksopp et al. 1999) observed eccentricity = 0.018(3) (Orosz et al. 2011) orbital evolution accounts for: 1) mass transfer (wind-fed) 2) tides 3) gravitation radiation 4) wind mass loss BH Step 4 Cyg X-1 10
28 Step 4: Match the observed orbital period and eccentricity observed period = (16) days (Brocksopp et al. 1999) observed eccentricity = 0.018(3) (Orosz et al. 2011) orbital evolution accounts for: 1) mass transfer (wind-fed) 2) tides 3) gravitation radiation 4) wind mass loss BH Step 4 Cyg X M BH 21.7 M 5 Myr Cyg X-1 10
29 Result ± 0.98 M Black Hole MBH = ± 0.98 M Mc = ± 1.90 M Cygnus X-1 11
30 Result ± 0.98 M Black Hole Myr MBH = ± 0.98 M Mc = ± 1.90 M Cygnus X M M 11
31 Result ± 0.98 M Black Hole Vpec = 27 ± 5 km/s Myr MBH = ± 0.98 M Mc = ± 1.90 M Cygnus X M M 11
32 Result M ± 0.98 M Vkick 77 km/s Black Hole Vpec = 27 ± 5 km/s Myr MBH = ± 0.98 M Mc = ± 1.90 M Cygnus X M M 11
33 Result M ± 0.98 M Vkick 77 km/s Black Hole Vpec = 27 ± 5 km/s Myr MBH = ± 0.98 M Mc = ± 1.90 M Cygnus X M M 95% 90% 60% 11
34 Results System Observed Current BH mass (M ) Post-SN BH mass (M ) Immediate Progenitor mass (M ) Natal Kick (km/s) GRO J (early-type, P>1d) 6.3 ± 0.5 (Greene et al. 2001) 5.4 ± 0.3 (Beer & Podsiadlowski 2002) (Willems et al. 2005) (Willems et al. 2005) (Willems et al. 2005) (Willems et al. 2005) (Willems et al. 2005) 210 (Willems et al. 2005) XTE J (late-type, P<1d) 8.0 ± 2.0 (McClintock et al. 2001, Wagner et al. 2001, Gelino et al. 2006) (Fragos et al. 2009) (Fragos et al. 2009) (Fragos et al. 2009) Cygnus X-1 (wind-fed, high mass) ± 0.98 (Orosz et al. 2011) (Wong et al. 2012) (Wong et al. 2012) 77 (Wong et al. 2012) M33 X-7 (wind-fed, high mass) (Orosz et al. 2007, Valsecchi et al.2010) (Valsecchi et al.2010) (Valsecchi et al.2010) (Valsecchi et al.2010) 12
35 Results System Observed Current BH mass (M ) Post-SN BH mass (M ) Immediate Progenitor mass (M ) Natal Kick (km/s) GRO J (early-type, P>1d) 6.3 ± 0.5 (Greene et al. 2001) 5.4 ± 0.3 (Beer & Podsiadlowski 2002) (Willems et al. 2005) (Willems et al. 2005) M33 X (Willems et al. 2005) (Willems et al. 2005) (Willems et al. 2005) 210 (Willems et al. 2005) XTE J (late-type, P<1d) 8.0 ± 2.0 (McClintock et al. 2001, Wagner et al. 2001, Gelino et al. 2006) (Fragos et al. 2009) (Fragos et al. 2009) (Fragos et al. 2009) Cygnus X-1 (wind-fed, high mass) ± 0.98 (Orosz et al. 2011) (Wong et al. 2012) (Wong et al. 2012) 77 (Wong et al. 2012) M33 X-7 (wind-fed, high mass) (Orosz et al. 2007, Valsecchi et al.2010) (Valsecchi et al.2010) (Valsecchi et al.2010) (Valsecchi et al.2010) 12 (from Charles Bailyn)
36 Results System Observed Current BH mass (M ) Post-SN BH mass (M ) Immediate Progenitor mass (M ) Natal Kick (km/s) GRO J (early-type, P>1d) 6.3 ± 0.5 (Greene et al. 2001) 5.4 ± 0.3 (Beer & Podsiadlowski 2002) (Willems et al. 2005) (Willems et al. 2005) (Willems et al. 2005) (Willems et al. 2005) (Willems et al. 2005) 210 (Willems et al. 2005) XTE J (late-type, P<1d) 8.0 ± 2.0 (McClintock et al. 2001, Wagner et al. 2001, Gelino et al. 2006) (Fragos et al. 2009) (Fragos et al. 2009) (Fragos et al. 2009) Cygnus X-1 (wind-fed, high mass) ± 0.98 (Orosz et al. 2011) (Wong et al. 2012) (Wong et al. 2012) 77 (Wong et al. 2012) M33 X-7 (wind-fed, high mass) (Orosz et al. 2007, Valsecchi et al.2010) (Valsecchi et al.2010) (Valsecchi et al.2010) (Valsecchi et al.2010) 12
37 Conclusion M ± 0.98 M Vkick 77 km/s Black Hole Vpec = 27 ± 5 km/s Myr MBH = ± 0.98 M Mc = ± 1.90 M Cygnus X M M Cygnus X-1: M = M ; V kick 77 km/s (95% CL) together with previous studies on GRO J , XTE J , M33 X-7, it seems that: massive black holes smaller natal kicks low mass black holes larger natal kicks working on supernova hydrodynamics simulations: can the asymmetries produce the derived mass loss and natal kicks? 13
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