The small Blue Straggler star population in the dense Galactic Globular Cluster NGC 6752 E.Sabbi E.Sabbi Dipartimento di Astronomia,Università di Bologna,via Ranzani 1,I Bologna,Italy F.R.Ferraro F.R.Ferraro A.Sills A.Sills Department of Physics and Astronomy,McMaster University,1280 Main Street West, Department of Physics and Astronomy,McMaster University,1280 Main Street West, Hamilton,ON L8S 4M1,Canada Hamilton,ON L8S 4M1,Canada and and R.T.Rood R.T.Rood Astronomy Dept.,University of Virginia Charlottesville VA ,USA Astronomy Dept.,University of Virginia Charlottesville VA ,USA

IntroductionIntroduction Observations and data analysisObservations and data analysis The CMD and the BSS candidatesThe CMD and the BSS candidates  The HST data  The WFI data BSS radial distributionBSS radial distribution Comparison with other GCsComparison with other GCs Collisional ModelsCollisional Models Summary and DiscussionSummary and Discussion

Introduction Two mechanisms of making BSSTwo mechanisms of making BSS  Mass transfer between or the merger of two stars in a primordial binary  Collisions in regions of very high stellar density Direct collisions Direct collisions Created as collisions harden primordial binaries until they merge Created as collisions harden primordial binaries until they merge Resulting when binaries are produced in a collision and merge later Resulting when binaries are produced in a collision and merge later

Introduction Provide new insights not only dynamical interaction and evolution of individual stars,but also of the cluster as a wholeProvide new insights not only dynamical interaction and evolution of individual stars,but also of the cluster as a whole  Segregation toward the center of the more massive stars (or binaries)  Binaries are thought to play a fundamental role in the core collapse — delay the collapse of the core

Introduction GGC NGC 6752GGC NGC 6752  Host many faint X-ray sources in the core  At least five millisecond pulsars (MSPs) Two of which are in the outer part—most radially distant MSPs gravitationally bound to a GC Two of which are in the outer part—most radially distant MSPs gravitationally bound to a GC Two of the three central MSPs display an anomalous acceleration Two of the three central MSPs display an anomalous acceleration  The existence of a binary black hole of intermediate mass could be a viable possibility

Observations and data analysis Observations and data analysis Two data setsTwo data sets  High resolution set-a series of high-resolution WFPC2-HST image,using the F555W(V),F336W(U)and F255W(mid-UV) filters Planetary camera(PC)(0’’.046/pixel) centered on the cluster center Planetary camera(PC)(0’’.046/pixel) centered on the cluster center Wide Field (WF) cameras(0’’1/pixel) sampled the surrounding outer regions Wide Field (WF) cameras(0’’1/pixel) sampled the surrounding outer regions  Wide Field set-Wide Field Imager (WFI) (B,V,I) 8 CCD chips (each with a field of view of 8’ ×16’)giving a global field of view of 33’ ×34’ 8 CCD chips (each with a field of view of 8’ ×16’)giving a global field of view of 33’ ×34’

The CMD and the BSS candidates The CMD and the BSS candidates The HST dataThe HST data  The main contributors to the UV emission of GCs are the hot stars which populate the horizontal branch (HB) and the BSS The ( ) plane is an ideal tool for selecting BSS The ( ) plane is an ideal tool for selecting BSS Select 28 ‘safe’ BSS in the HST-WFPC2 FoV Select 28 ‘safe’ BSS in the HST-WFPC2 FoV  Brighter than ~18(0.3 mag brighter than the cluster TO)  Bluer than ~0.76

The CMD and the BSS candidates The CMD and the BSS candidates The WFI dataThe WFI data  Consider the stars contained within the tidal r ~16’.67( ~1000”)  Select 15 BSS candidates from the (V,B-V) CMD Brighter than V ~16.9 Brighter than V ~16.9 Bluer than (B-V) ~0.44 Bluer than (B-V) ~0.44

BSS radial distribution BSS radial distribution Combine the two samples (HST+WFI)Combine the two samples (HST+WFI)  Require the same limiting magnitude Use F555W (HST) and V (WFI) Use F555W (HST) and V (WFI) Select 19 BSS sample from the BBS-HST brighter than V ~16.9 Select 19 BSS sample from the BBS-HST brighter than V ~16.9 Use HB and RGB as reference to study the BSS radial distributionUse HB and RGB as reference to study the BSS radial distribution  The two samples are well matched  87 HB and 255 RGB in HST and 264 HB and 1984 RGB in WFI

BSS radial distribution BSS radial distribution The inner sample (HST)The inner sample (HST)  The exact value of the limiting magnitude chosen does not affect our results  More concentrated than the RGB and the HB stars selected in the same area The outer sample (WFI)The outer sample (WFI)  Not statistically different (less than 1σ)  Could be due to the fact that the number of BSS is too small to draw a definite conclusion

BSS radial distribution BSS radial distribution Comparison with M3 and 47TucComparison with M3 and 47Tuc  In M3 and 47Tuc The BSS are more concentrated than the reference population in the central regions. In the outer regions with the BSS being less concentrated than the reference population  Less well defined in NGC 6752 Could not show up in a sample of this size Could not show up in a sample of this size

BSS radial distribution Computed the radial behavior of the BSS relative frequencyComputed the radial behavior of the BSS relative frequency  Reach the maximum in the innermost annulus F ~0.42  Decrease to less then 0.04 as r increase  In the most external annuli the distribution shows a small upturn reaching ~0.2

BSS radial distribution Normalized the BSS number to the RGB populationNormalized the BSS number to the RGB population Follows the bimodality observed in M3,M55 and recently in 47TucFollows the bimodality observed in M3,M55 and recently in 47Tuc Extensive surveys in the outer region of other cluster are needed before we can conclude that this is the “natural” radial distribution of BSS in globularsExtensive surveys in the outer region of other cluster are needed before we can conclude that this is the “natural” radial distribution of BSS in globulars

Comparison with other GCs Comparison with other GCs Apply the same criteria adopted by Ferraro et al.Apply the same criteria adopted by Ferraro et al.  Shift in magnitude and color to match the MS of M3  Bright BSS with magnitude brighter than 19.0 are considered One single mass King model and two single mass King modelsOne single mass King model and two single mass King models

Collisional Models Collisional Models The models are described in detail in Sills & Bailyn (1999)The models are described in detail in Sills & Bailyn (1999)  Assume that all the BSS were formed via direct stellar collisions between two stars during an encounter between a single star and a binary system.  The out put of these simulations is the probability that a collision between stars of specific masses will occur

Collisional Models We must question our assumptions about the formation mechanism for the most luminous BSSWe must question our assumptions about the formation mechanism for the most luminous BSS  Maybe the product of three stars coming together (mass greater than twice the TO mass)  Some mixing mechanism, such as rotation, the stars can be significantly bluer, brighter, and have longer MS lifetimes  Not formed through collisions at all,but rather through the merger of the two components of a primordial binary system

Summary and Discussion A bimodal radial distribution(M3&47Tuc), more BSS surveys, covering the full spatial extent of the host cluster, are necessary to determine just how common bimodality isA bimodal radial distribution(M3&47Tuc), more BSS surveys, covering the full spatial extent of the host cluster, are necessary to determine just how common bimodality is A large binary population and high stellar density should lead to efficient production of BSS, yet we observe the reverse.A large binary population and high stellar density should lead to efficient production of BSS, yet we observe the reverse.

Summary and Discussion Cluster’s dynamic stateCluster’s dynamic state  M80 has very large BSS population and maybe at the onset of core contraction but models suggest that BSS formation ended a few Gyr ago.  NGC 6752 is undergoing a post-collapse bounce, a more advanced dynamical state than M80 Large number of luminous and hot BSS in the cluster core casts some doubt on our model formation mechanismLarge number of luminous and hot BSS in the cluster core casts some doubt on our model formation mechanism