Measuring the Hubble Constant through Cepheid Distances“Final Results from the Hubble Space Telescope Key Project to Measure the Hubble Constant” Freedman, Madore, Gibson, et al., Astrophysical Journal 553, pp. 47.Brian GleimAST 591 - Rolf JansenIntroduction• In standard Big Bang cosmology, universe expands uniformly according to:–v = H0d, Hubble law•Finding accurate value of H0 is challenging– primary difficulty is establishing accurate distances at cosmological scalesUses of Hubble Constant•H0-1 sets the age of Universe: t0•Size of observable Universe: Robs=c t0•H02 relates total energy density to geometry•Critical density of Universe: crit=3H2/8G•Many physical properties of galaxies and quasars, and abundances of primordial light elements all require knowledge of H0H0 Key Project•Goal: to measure H0 based on Cepheid calibration of independent, secondary distance methods• Avoids relying on a single methodH0 Key Project• Uses HST Cepheid distances to provide an absolute distance scale for:–Type Ia and II SNe–Tully-Fisher Relation–Fundamental Plane for Ellipticals–Surface Brightness FluctuationsCosmic Distance ScaleCepheid Variables• Lie on instability strip of HR diagram• Instability leads to pulsations and variability• Strong correlation between period of pulsation and luminosty of CepheidCepheid Variables• Lie on instability strip of HR diagram• Instability leads to pulsations and variability• Strong correlation between period of pulsation and luminosty of CepheidCepheid Variables• Lie on instability strip of HR diagram• Instability leads to pulsations and variability• Strong correlation between period of pulsation and luminosty of CepheidAdvantages of Cepheids• Among brightest stellar indicators• Abundant in spiral galaxies• Long lifetimes• Small scatter in PL relation• Studied and modeled extensivelyDisadvantages of Cepheids• Young stars, founds in dusty regions• Dependence of PL relation on metallicity• Resolving individual Cepheids becomes difficult at greater distances–Limited to < 30 MpcSearching for Cepheids• Search target spiral galaxies in regions of active star-formation, but low in dust-extinction•Observe with WFPC2 in V and I bands to correct for dust• Targeted 31 galaxies to find distance, calibrate secondary methods, and test effects of metallicity on PL relationMeasuring Cepheid Distances• Large Magellanic Cloud PL relation used as a fiducial– Distance modulus: 0 = 18.50 mag–Distance of 50 kpc–Mean reddening E(V-I) = 0.13" i- 0 = 5 log(di/d0)Effect of Metallicity• Longstanding uncertainty in Cepheid distance•Calibrating metallicity effects from theoretical models was still unfeasible• Empirical values from Cepheids in M31 and M101 suggest 0<VI<-0.4–Adopted VI = -0.2 ±0.2 mag/dexAdopting PL Relations• Udalski et al. (1999) studied more LMC Cepheids, improved calibration•With improved Udalski data, adopted period-luminosity relations become:• And the true distance modulus for galaxies:•whereEffects of Udalski PL Slopes• V-band PL Slope remained -2.76•I-band PL Slope changed from -3.06 to -2.96•New Calibration predicts higher reddening– therefore, smaller distances• Systematically higher reddening for longer period Cepheids– difference is largest at greater distancesLocal Flow Field•H0 requires knowing distance and velocity• Peculiar velocities of nearby galaxies complicate measuring Hubble velocity•=> H0 measurements more accurate at higher distancesCepheid Hubble Diagram• 23 galaxies with Cepheid distances• Slope of 75 km s-1 Mpc-1, excluding systematic errors• Scatter is larger than in secondary methods (local flow), but in good agreementSecondary Distance MethodsCumulative H0 ValuesCumulative Hubble DiagramOverall Systematic Error• Uncertainty in the zero point of PL relation•Effect of reddening and metallicity on observed PL relations•Effects of incompleteness bias and crowding on Cepheid distances• Velocity perturbation about the Hubble flow•Overall Systematic uncertainty: ±10%Implications for Cosmology•Knowing H0, the average density of matter , and , the Friedmann equation•yields a measure of the expansion age of Universe•For, H0 = 72 km s-1 Mpc-1, m=0.3, =0.7, the expansion age is 13 ±1 Gyr•Consistent with globular cluster agesReferences• “Final Results from the Hubble Space Telescope Key Project to Measure the Hubble Constant” Freedman, Madore, Gibson, et al., Astrophysical Journal 553, pp. 47.• Images from:– hubblesite.org/gallery/spacecraft/03/– http://ircamera.as.arizona.edu/NatSci102/images/distladder.jpg– http://odin.physastro.mnsu.edu/~eskridge/astr101/kauf21_12.JPG– http://will114.asu.edu/varstar.pdf– http://www.astronomy.com/asy/objects/images/cepheid_p-l_600.jpg– http://seds.lpl.arizona.edu/messier/Pics/More/m81cep_hs.jpg– http://heritage.stsci.edu/2006/07/images/i0607aw.jpgThank You• Any