Data Analysis

Chapter 10 of 11 · 11 min read

Spectra and velocities

Doppler shifts, rotation curves and dynamical masses, binary orbits and the mass function, and expanding shells.

Doppler shifts

For v≪cv\ll c,

z=λobs−λemitλemit,vr=cz.z = \frac{\lambda_{\rm obs} - \lambda_{\rm emit}}{\lambda_{\rm emit}}, \qquad v_r = cz.

Positive means receding (redshift). For larger speeds, 1+z=(1+β)/(1−β)1+z = \sqrt{(1+\beta)/(1-\beta)}. Use the air wavelength when the data are in air (Hα at 6562.82 Å in air, 656.281 nm in the 2017 problem; follow the value the problem gives).

The 2017 galaxy spectra show shifts of only 0.1–0.2 nm on 656 nm, so keep all the decimals: a 0.001 nm reading error is 0.5 km/s.

Rotation curves and dark matter

For circular orbits in a spherical mass distribution,

v2r=GM(r)r2  ⇒  M(r)=rv2G.\frac{v^2}{r} = \frac{GM(r)}{r^2} \;\Rightarrow\; M(r) = \frac{rv^2}{G}.

Independent components add in quadrature: vobs2=vgas2+v∗2+vDM2v_{\rm obs}^2 = v_{\rm gas}^2 + v_*^2 + v_{\rm DM}^2. A flat rotation curve (vv constant) means M∝rM\propto r, so ρ∝r−2\rho\propto r^{-2} at large radius. Visible matter alone would give v∝r−1/2v\propto r^{-1/2} (Keplerian) outside the light. The difference is the evidence for dark matter.

Binary stars and the mass function

For a star in a circular orbit with period PP and RV semi-amplitude KK:

a1sin⁡i=PK2π,f(M)=(M2sin⁡i)3(M1+M2)2=PK32πG.a_1\sin i = \frac{PK}{2\pi}, \qquad f(M) = \frac{(M_2\sin i)^3}{(M_1+M_2)^2} = \frac{PK^3}{2\pi G}.

The mass function is a lower limit on M2M_2 (it equals M2M_2 only if sin⁡i=1\sin i = 1 and M1=0M_1 = 0). To get M2M_2 you need M1M_1 and ii from elsewhere: log⁡g\log g and a radius give M1=gR2/GM_1 = gR^2/G; a rotation period and vsin⁡iv\sin i give sin⁡i=Pvsin⁡i/(2πR)\sin i = Pv\sin i/(2\pi R) if the rotation is synchronised.

If M2M_2 exceeds about 2.5 M⊙M_\odot and the companion emits nothing, it is a black hole candidate (2018 D2).

Pulsars and accelerations

An orbiting pulsar's apparent spin period is Doppler shifted, P=P0(1+vr/c)P = P_0(1 + v_r/c), and the line-of-sight acceleration a=v˙ra = \dot v_r is measured from the drift of PP. For a circular orbit the pair (P,a)(P, a) traces an ellipse with semi-axes Pt=P0v/cP_t = P_0v/c and at=v2/ra_t = v^2/r, which is the basis of 2016 D1.

Expanding shells and P Cygni profiles

An expanding shell produces emission at the line's rest wavelength and blueshifted absorption from gas between us and the star: a P Cygni profile. The absorption minimum gives the expansion velocity. Integrating the velocity over time gives the shell's radius:

R(t)=∫0tv dt,R(t) = \int_0^t v\,dt,

and with a distance, an angular size θ=2R/d\theta = 2R/d. The 2019 nova problem used this. A pulsating star works the same way, with ΔR=−p∫(vr−γ) dt\Delta R = -p\int(v_r - \gamma)\,dt (the projection factor p≈1.3p\approx1.3; the sign because a positive radial velocity means the surface is moving away from us, i.e. contracting).

Key formulas

Doppler shift
vr=c λobs−λemitλemitv_r = c\,\frac{\lambda_{\rm obs} - \lambda_{\rm emit}}{\lambda_{\rm emit}}
Enclosed mass
M(r)=r v2GM(r) = \frac{r\,v^2}{G}
Mass function
f(M)=(M2sin⁡i)3(M1+M2)2=PK32πGf(M) = \frac{(M_2\sin i)^3}{(M_1+M_2)^2} = \frac{P K^3}{2\pi G}
Projected orbit
a1sin⁡i=PK2πa_1\sin i = \frac{PK}{2\pi}

Common mistakes

  • Forgetting to subtract the systemic velocity γ before integrating a velocity curve.
  • Treating the mass function as the companion's mass.
  • Mixing vacuum and air wavelengths.
  • Adding velocity components linearly instead of in quadrature.

Practise this chapter

Past IOAA problems that use these skills.

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