The Universe Is Expanding — Question 4

Section 44-10 · Physics pages 7478–7479

Question 4 The slope of a Hubble diagram can be estimated without fitting an intercept Assume negligible distance errors, equal velocity errors and the model vi = HDi through the origin. Three galaxies have distances 10,20,30 Mpc and velocities 720,1380,2130 km/s. D v Schematic; labels, not drawing lengths, specify the data. (a) Derive the least-squares slope and calculate H. (b) Find all residuals and their squared sum.
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Question 4 - Solution The slope of a Hubble diagram can be estimated without fitting an intercept D v (a) Method and calculation d dH ∑ (vi −HDi)2 = −2 ∑ Di(vi −HDi) = 0. H = ∑Divi ∑D2 i = 98700 1400 = 70.5 km s−1 Mpc−1 . (b) Interpretation and further calculation ri = (15, −30, 15) km/s . ∑ r2 i = 225 + 900 + 225 = 1350 (km/s)2 . Physical check An intercept, distance uncertainty, selection effects or correlated peculiar motions require a more complete fit.

Question 4

The slope of a Hubble diagram can be estimated without fitting an intercept

Assume negligible distance errors, equal velocity errors and the model vi=HDiv_i=HD_i through the origin. Three galaxies have distances 10,20,30 Mpc and velocities 720,1380,2130 km/s.

Diagram shown in the original SVG worksheet.

  1. Derive the least-squares slope and calculate H.

  2. Find all residuals and their squared sum.

Question 4 - Solution

The slope of a Hubble diagram can be estimated without fitting an intercept

Diagram shown in the original SVG worksheet.

(a) Method and calculation

ddH∑(vi−HDi)2=−2∑Di(vi−HDi)=0.\frac{d}{dH}\sum(v_i-HD_i)^2=-2\sum D_i(v_i-HD_i)=0.H=∑Divi∑Di2=987001400=70.5kms−1Mpc−1.\boxed{H=\frac{\sum D_iv_i}{\sum D_i^2}=\frac{98700}{1400}=70.5\ {\mathrm{km\,s^{-1}\,Mpc^{-1}}}}.

(b) Interpretation and further calculation

ri=(15,−30,15)km/s.\boxed{r_i=(15,-30,15)\ {\mathrm{km/s}}}.∑ri2=225+900+225=1350(km/s)2.\boxed{\sum r_i^2=225+900+225=1350\ ({\mathrm{km/s}})^2}.

Physical check

An intercept, distance uncertainty, selection effects or correlated peculiar motions require a more complete fit.