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Globular Cluster X-ray Sources David Pooley University of Wisconsin Chandra’s First Decade of Discovery 2009 Sep 24 September 24, 1759 with thanks to friends, colleagues, and collaborators: Walter Lewin Josh Grindlay Didier Barret Frank Verbunt Craig Heinke Bruce Gendre Cees Bassa Peter Edmonds Natalie Webb Lee Homer Steve Murray Mathieu Servillat Scott Anderson Haldan Cohn Bruce Margon Phyllis Luger Vicky Kaspi Adrienne Cool Piet Hut Brian Gaensler Daryl Haggard Simon Portegies Zwart Derek Fox John Fregeau Rudy Wijnands Albert Kong Natalia Ivanova Ed Cackett Ting-Ni Lu Jeroen Homan Shih Hao Lan Harvey Tananbaum and the entire CXC staff X-ray astronomy & globular clusters 36 1 Luminous X-ray sources (LX > 10 erg s ) Discovered by Uhuru and OSO-7; argued to be formed via cluster dynamics Gursky 1973, Clark 1975, Katz 1975 Stimulated flurry of theoretical work Fabian, Pringle, & Rees 1975, Sutantyo 1975, Hills 1975, 1976, Heggie 1975, Verbunt & Hut 1983 12 globular clusters thought to contain one each All but one show Type-I X-ray bursts NS-LMXBs e.g., Kuulkers et al. 1996 Bright X-ray Sources: New Chandra discoveries M15 NGC 6440 Heinke et al. 2009 DP et al. 2002 White & Angelini 2001 in’t Zand et al. 2001 X-ray astronomy & globular clusters 36 1 Luminous X-ray sources (LX > 10 erg s ) Discovered by Uhuru and OSO-7; argued to be formed via cluster dynamics Gursky 1973, Clark 1975, Katz 1975 Stimulated flurry of theoretical work Fabian, Pringle, & Rees 1975, Sutantyo 1975, Hills 1975, 1976, Heggie 1975, Verbunt & Hut 1983 12 globular clusters thought to contain one each All but one show Type-I X-ray bursts NS-LMXBs e.g., Kuulkers et al. 1996 34 1 Low Luminosity X-ray sources (LX < 10 erg s ) Discovered by Einstein Hertz & Grindlay 1983 More found with ROSAT e.g., Verbunt 2001 No secure identifications Suggested to be CVs (Hertz & Grindlay 1983), qLMXBs (Hertz & Grindlay 1983, Verbunt et al. 1984), radio MSPs (Saito 1997), magnetically active binaries (Bailyn et al. 1990) Extragalactic globular cluster X-ray sources (T. Maccarone) Detailed MSP studies (S. Bogdanov) Intermediate Mass Black Holes Globular Cluster NGC 2808 15Rcore = 0.74 parsecNGC 2808 = 2.4 lightyears 18 20 = 2.3corr10 cm CGB1 ADH-6829 4 3 coreA-11944 = 410 star pc 25 UP-6817 SB-1721 Illi. scan 3 usIlli. = ann. 1 star pc Cheb. poly. 30 0123 log (r/arcsec) credit: S. Juchnowski Trager, King, & Djorgovski 1995 adapted from Servillat et al. (2008) see poster by M. Servillat Surface Brightness Profiles “core collapsed” 20% of globular clusters 15 NGC 2808 “normal” 20 corr 80% of CGB1 ADH-6829 A-11944 25 UP-6817 globular SB-1721 Illi. scan Illi. ann. clusters Cheb. poly. 30 0123 Trager, King, & log (r/arcsec) Djorgovski 1995 Simulating Globular Clusters Fregeau et al. 2003 Globular Cluster Life Stages 80% Binary burning Core contraction 20% Core collapse Deep core collapse Binary burning Gravothermal oscillations Fregeau et al. 2003 X-ray Sources in Globular Clusters Chandra image of 47 Tuc Low-mass X-ray Binaries Millisecond pulsars Cataclysmic Variables Active main-sequence binaries adapted from Grindlay et al. 2001 NGC 6397 M4 47 Tuc 47 Tuc in X-rays Einstein (8 ksec) ROSAT (77 ksec) Chandra (240 ksec) Identifying the X-ray Sources 47 Tuc NGC 6752 CX1CX1 CX2CX2 CX3CX3 N E CX4CX4 CX5CX5 CX6CX6 CX7CX7 CX10CX10 CX11CX11 Edmonds et al. (2003) DP et al. (2002) Identifying the X-ray Sources NGC 6397 NGC 6752 Grindlay et al. (2001) DP et al. (2002) Source Identification via X-rays Cen qLMXB Cen CV kT = 67 ± 2 eV kT = 23 +39/-10 keV R = 12.6 ± 3 km Webb & Barret 2004 (from Gendre et al. 2003) A Link to Stellar Dynamics DP et al. 2003 Heinke et al. 2003 Gendre et al. 2003 X-ray CMD 1034 To Date: 77 GCs 1032 114 ACIS Obs. (erg/s) 30 3 Msec 10 0.5-8 keV L >1500 sources 1028 ~250 background -2 -1 0 1 2 3 log10 (C0.5-2 keV / C2-8 keV) adapted from DP & Hut 2006 X-ray CMD 1034 )))) ) ) Uniform: -1-1-1-1 NS Atmosphere 31 -1 -1 Lx > 410 erg s 1033 (erg s 22 GCs + 20% PL ~200 sources + 50% PL 0.5-6 keV [0.5-6 keV] (erg s [0.5-6 keV] (erg s [0.5-6 keV] (erg s [0.5-6 keV] (erg s ~15 background XXXX L 32 LLLL 10 qLMXB Pulsar Active Binary CV Field Burster -2 -1 0 1 2 log (Flux [0.5-2 keV] / Flux [2-6 keV]) Field Pulsar 10log 10 (F 0.5-2 keV /F 2-6 keV ) Cluster LMXBs 100 Can rule out constant n at 4 10 LMXBLMXB n = as + c nn s = 1.8 ± 0.4 1 c = 0.4 ± 0.5 1 10 100 1000 DP & Hut 2006 Specific units: n = N/M = /M 6 M in units of 10 M building on Gendre et al. 2003, Heinke et al. 2003, DP et al 2003 Are Globular Cluster CVs overabundant? They should be: Hut & Verbunt 1983 Di Stefano & Rappaport 1994 Are Globular Cluster CVs overabundant? They’re not: Shara 1996 , 6 elliptical galaxies. Likewise, we predict that there should be 60–180 CVs for every 10 L , K in an old stellar population. The population of X-ray–identified CVs in the globular cluster 47 Tuc is similar to this number, showing no overabundance relative to the field. The observed CN Porb distribution also contains evidence for a CV population Townsley & Bildsten 2005 With our simulations, we predict that the formation rates of CVs Maybe a little? and AM CVn systems in GCs are not very different from those in the field population. The numbers of CVs and AM CVn systems per mass unit are comparable to numbers in the field if the whole cluster population is considered, and they are only two to three times larger in the core than in the field. Dynamical formation is responsible only for 60–70 per cent of CVs in the core. This fraction decreases Ivanova et al. 2006 X-ray CMD 1034 ) ) ) Uniform: -1 NS Atmosphere 31 -1 -1 Lx > 410 erg s 1033 (erg s 22 GCs + 20% PL ~200 sources + 50% PL 0.5-6 keV [0.5-6 keV] (erg s ~15 background X 32 L L 10 qLMXB Pulsar Active Binary CV Field Burster -2 -1 0 1 2 log10 (Flux [0.5-2 keV] / Flux [2-6 keV]) Field Pulsar log 10 (F 0.5-2 keV /F 2-6 keV ) Bright, hard sources 100 (mostly CVs) 10 Can rule out CVCV nn constant n at 6 1 n = as + c s = 0.8 ± 0.2 1 10 100 1000 ± c = 0.3 1.4 DP & Hut 2006 Specific units: n = N/M = /M 6 M in units of 10 M Dynamical 200 Formation “Core collapsed” 150 All sources with 30 -1 Lx > 410 erg s xxx 100 nnn s n = a + c 47 Tuc 50 s = 0.45 ± 0.17 Cen c = 5.3 ± 7.7 0 1 10 100 1000 DP & Hut 2006 Specific units: nx = Nx/M = /M 6 M in units of 10 M Globular Cluster Life Stages Revisited Fregeau (2008) pointed out: 80% Binary burning Better simulations reveal rc was over- Core contraction 20% Core collapse estimated by 10 in binary-burning phase Deep core collapse Binary burning Production of X-ray sources in binary burning phase is 2–20 higher than in core Gravothermal oscillations contraction phase Chandra reveals that “core collapsed” Fregeau et al. 2003 clusters have many more binaries than the N- relation predicts Paradigm shift? 80% Binary burning 80% Core contraction + 20% Core collapsed + 20% Binary burning Dynamical 15 "core-collapsed" GCs Formation 48 "normal" GCs All sources with 100 31 -1 Lx > 410 erg s 6 PRELIMINARY / M X N 10 1 10 100 1000 / M6 DP et al. in prep. Future Work Individual identifications Subpopulation dynamics Investigate importance of other parameters (e.g., metallicity) Fast (~3 day) transients Heinke et al. Low density clusters (primordial binaries) Kong, Lu, Lan et al. Deep exposures of M4 (DP et al.) and NGC 6397 (Grindlay et al.) Extending into rich open clusters: see poster by N. Gosnell Fermi survey to determine overall MSP population Summary It’s Guinness’s 250th birthday! X-ray sources are dynamically formed Great tracers for large scale simulations (especially LMXBs) CVs are finally being found in large numbers in globular clusters and are overabundant Chandra is the most efficient and effective means of finding the important close binaries in a globular cluster Possible revolution in our understanding of the current dynamically states of globular clusters Understanding Globular Clusters (is tough) No Thermodynamic Limit 3 2 5/3 M R Ekin M but Epot M /R M ⇒ “Infrared Divergence” Negative Heat Capacity Mass segregation stratified system dense core Encounters extract energy from core, increasing temperature Nearly Unlimited Reservoir of Binary Binding Energy 3-body encounters tap into binary energy ⇒ “Ultraviolet Divergence” Feedback between Stellar Dynamics and Stellar Evolution No Easy Way to Compare Theory to Observation Input theory to simulations Compare simulations to observations Bright X-ray Sources: Ultrashort Period X=0 Normal Period X=0.73 Neutron Star LMXBs Unknown Period Discovered by Uhuru and OSO-7; argued to be formed via cluster dynamics Gursky 1973, Clark 1975, Katz 1975 Stimulated flurry of theoretical work Fabian, Pringle, & Rees 1975 Sutantyo, 1975 Hills, 1975, 1976 Heggie 1975 Kuulkers et al. 2003 Verbunt & Hut 1983 12 globular clusters thought to contain one each All but one show Type-I X-ray bursts NS-LMXBs e.g., Kuulkers et al.
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    rs uvvwxyuzyws { yz|z|} rsz}~suzywsu}u~w vz~wsw 456789@A C 99D 7EFGH67A7I P @AQ R8@S9 RST9AS9 UVWUX `abcdUVVe fATg96GTHP7Eh96HE76QGiT69pf q rAS76876@HTAs tFR u Fv wxxy @AQ 4FR 4u Fv wxxy UVVe abbc d dbdc e f gc hi` ij ad bch dgcadabdddc c d ac k lgbc bcgb dmg agd g` kg bdcd dW dd k bg c ngddbaadgc gabmob nb boglWad g kdcoddog kedgcW pd gc bcogbpd kb obpcggc dd kfq` UVVe c iba ! " #$%& $' ())01023 Book of Abstracts – Table of Contents Welcome to the European Week of Astronomy & Space Science ...................................................... iii How space, and a few stars, came to Hatfield ............................................................................... v Plenary I: UK Solar Physics (UKSP) and Magnetosphere, Ionosphere and Solar Terrestrial (MIST) ....... 1 Plenary II: European Organisation for Astronomical Research in the Southern Hemisphere (ESO) ....... 2 Plenary III: European Space Agency (ESA) .................................................................................. 3 Plenary IV: Square Kilometre Array (SKA), High-Energy Astrophysics, Asteroseismology ................... 4 Symposia (1) The next era in radio astronomy: the pathway to SKA .............................................................. 5 (2) The standard cosmological models - successes and challenges .................................................. 17 (3) Understanding substellar populations and atmospheres: from brown dwarfs to exo-planets .......... 28 (4) The life cycle of dust ...........................................................................................................