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Mass Estimators in Astrophysics One of the most fundamental physical parameters of astrophysical systems is their mass. There are several techniques used.

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Presentation on theme: "Mass Estimators in Astrophysics One of the most fundamental physical parameters of astrophysical systems is their mass. There are several techniques used."— Presentation transcript:

1 Mass Estimators in Astrophysics One of the most fundamental physical parameters of astrophysical systems is their mass. There are several techniques used to estimate masses (absolute measures are only possible in a few very well defined cases) that rely on the general balance between gravity and motion in systems that are in equilibrium.

2 Mass Estimators: The simplest case = Bound Circular Orbit Consider a test particle in orbit, mass m, velocity v, radius R, around a body of mass M ½ mv 2 = GmM/R  M = ½ v 2 R /G This formula gets modified for elliptical orbits. What about complex systems of particles?

3 For Multi-Object Systems There are several estimators we use, the two most popular (and simplest) are the Virial Estimator, which is based on the Virial Theorem, and the Projected Mass Estimator. For these estimators, all you need are the positions and velocities of the test particles (e.g. the galaxies in the system). The velocities we measure are usually only the

4 Line-of-sight (l.o.s.) Velocities, so some correction must be made to account for velocities (and thus energy) perpendicular to the l.o.s. Ditto, the positions of objects we usually measure are just the positions on the plane of the sky, so some correction needs to be made for physical separations along the l.o.s. We usually simplify by assuming that our systems are spherical.

5 The Virial Theorem Consider a moment of inertia for a system of N particles and its derivatives: I = ½ Σ m i r i. r i (a moment of inertia) I = dI/dt = Σ m i r i. r i I = d 2 I/dt 2 = Σ m i (r i. r i + r i. r i ) i=1 N

6 Assume that the N particles have m i and r i and are self gravitating --- their mass forms the overall potential. We can use the equation of motion to elimiate r i. m i r i =  Σ ( r i - r j ) and note that Σ m i r i. r i = 2T (twice the Kinetic Energy).. |r i –r j | 3 j = i Gm i m j..

7 Then we can write (after substitution) I – 2T =  Σ Σ r i. (r i – r j ) =  Σ Σ r j. (r j – r i ) =  ½ Σ Σ (r i - r j ). (r i – r j ) =  ½ Σ Σ = U the potential energy.. i j=i Gm i m j |r i - r j | 3 Gm i m j j i=j |r j - r i | 3 reversing labels Gm i m j |r i - r j | 3 i j=i adding Gmi mj |r i - r j |

8 ∴ I = 2T + U If we have a relaxed (or statistically steady) system which is not changing shape or size, d 2 I/dt 2 = I = 0  2T + U = 0; U = -2T; E = T+U = ½ U conversely, for a slowly changing or periodic system 2 + = 0.. Virial Equilibrium

9 Virial Mass Estimator We use the Virial Theorem to estimate masses of astrophysical systems (e.g. Zwicky and Smith and the discovery of Dark Matter) Go back to: Σ m i = ΣΣ Gm i m j where denotes the time average, and we have N point masses of mass m i, position r i and velocity v i N i=1 N i=1 j

10 The observables are (1) the l.o.s. time average velocity: Ω = 1/3 v i 2 projected radial averaged over solid angle Ω i.e. we only see the radial component of motion & v i ~ √3 v r Ditto for position, we see projected radii, R = θ d, d = distance, θ = angular separation

11 So taking the average projection, Ω = Ω and Ω = = = π/2 1 |ri – rj| 1 1 sin θij 1 ∫ (sinθ) -1 dΩ dΩdΩ ∫0π dθ∫0π dθ ∫ 0 π sinθ dθ

12 Thus after taking into account all the projection effects, and if we assume masses are the same so that M sys = Σ m i = N m i we have M VT = N this is the Virial Theorem Mass Estimator Σ v i 2 = Velocity dispersion [ Σ (1/R ij )] -1 = Harmonic Radius 3π3π 2 G Σ (1/R ij ) i

13 This is a good estimator but it is unstable if there exist objects in the system with very small projected separations: x x x x x xx x x x x x x x x x all the potential energy is in this pair!

14 Projected Mass Estimator In the 1980’s, the search for a stable mass estimator led Bahcall & Tremaine and eventually Heisler, Bahcall & tremaine to posit a new estimator with the form ~ [dispersion x size ]

15 Derived PM Mass estimator checked against simulations: M P = Σ v i 2 R i,c where R i,c = Projected distance from the center v i = l.o.s. difference from the center f p = Projection factor which depends on (includes) orbital eccentricities fpfp GN

16 The projection factor depends fairly strongly on the average eccentricities of the orbits of the objects (galaxies, stars, clusters) in the system: f p = 32/π for primarily Radial Orbits = 16/π for primarily Isotropic Orbits = 8/π for primarily Circular Orbits Richstone and Tremaine plotted the effect of eccentricity vs radius on the velocity dispersion profile:

17 Richstone & Tremaine Expected projected l.o.s. sigmas

18 Applications: Coma Cluster σ ~ 1000 km/s M VT = 1.69 x M Sun M PM = 1.75 x M Sun M31 Globular Cluster System σ ~ 155 km/s M PM = 3.1  0.5 x M Sun

19 The Coma Cluster

20

21 Andromeda Galaxy = M31

22 M31 Globular Clusters

23

24 Velocity Histogram


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