Data Analysis

Chapter 11 of 11 · 12 min read

Distances and the cosmic ladder

Parallax, standard candles, geometric methods and the Hubble law, with the IOAA problems that use each rung.

Geometry first

  • Parallax: d [pc]=1/π [′′]d\,[{\rm pc}] = 1/\pi\,[''], so 1 mas means 1 kpc. Errors: Δd/d=Δπ/π\Delta d/d = \Delta\pi/\pi. Beyond about 20% parallax error, 1/π1/\pi becomes biased, which is why HST and Gaia matter (2017 D1 used HST parallaxes of about 2–3 mas).
  • Angular size: D=2R/θD = 2R/\theta. If you know a physical size, an angle gives the distance. Examples: the Moon's radius from the eclipse geometry (2016 D2), eclipsing binaries with surface brightness (2023 DA1).
  • Triangulation in the Solar System: the Sun–Earth–Moon triangle at quarter phase (Aristarchus), Venus transits, radar.

Standard candles

A standard candle has a known MM, so m−Mm - M gives the distance.

  • Cepheids: the period–luminosity relation M=β′log⁡P+C′M = \beta'\log P + C', calibrated with parallaxes (2017 D1) and applied to the LMC or other galaxies (2015 P2: IC 342).
  • Type Ia supernovae: peak M≈−19.3M\approx-19.3, corrected for light curve width. Slower decliners are brighter (the Phillips relation; the stretch factor in 2016 D3).
  • Novae: the maximum-magnitude–rate-of-decline relation, M0M_0 from t2t_2 or t3t_3 (2019 Nova Del 2013).
  • Tip of the red giant branch and RR Lyrae: MI≈−4.0M_I\approx-4.0 and MV≈+0.6M_V\approx+0.6, respectively.

Each candle's calibration error is a systematic error for every distance it gives.

Physical methods

  • Baade–Wesselink: integrate a pulsating star's radial velocity to get ΔR\Delta R, combine with the flux and temperature at two phases to get RR and then dd (2015 P1).
  • Eclipsing binaries: radii in metres from the light and velocity curves, angular diameters from the surface-brightness–colour relation, so d=2R/θd = 2R/\theta (2023 DA1; the method behind the 1% LMC distance of 2019).
  • Microlensing parallax: θE\theta_E and πE\pi_E together give the lens mass and distance without any luminosity at all (2023 DA2).

The Hubble law

For z≪1z\ll1, v=cz=H0dv = cz = H_0d, so a distance to a galaxy with a known redshift gives H0H_0, and the Hubble time

TH=1H0=977.8H0 [km s−1 Mpc−1] GyrT_H = \frac{1}{H_0} = \frac{977.8}{H_0\,[{\rm km\,s^{-1}\,Mpc^{-1}}]}\ {\rm Gyr}

sets the age scale (2016 D3). Peculiar velocities of a few hundred km/s make nearby galaxies unreliable for this, so use galaxies beyond about 50 Mpc.

Key formulas

Parallax
d [pc]=1π [′′]d\,[{\rm pc}] = \frac{1}{\pi\,['']}
Size and distance
D=2RθD = \frac{2R}{\theta}
Hubble law
cz=H0d,TH=1H0cz = H_0 d, \qquad T_H = \frac{1}{H_0}
Einstein radius
θE=4GMc2 Ds−DℓDsDℓ\theta_E = \sqrt{\frac{4GM}{c^2}\,\frac{D_s - D_\ell}{D_s D_\ell}}

Common mistakes

  • Using 1/π for a parallax with a 30% error and quoting a symmetric error.
  • Forgetting extinction when using a standard candle in the Galactic plane.
  • Mixing up apparent and true distance moduli (with and without A).
  • Applying the Hubble law to the Local Group.

Practise this chapter

Past IOAA problems that use these skills.

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