Galaxy Distances Astronomy 274
Why measure distances?
Distance Ladder
Galaxies are not distributed randomly (why we cannot use redshifts to estimate distances)
Local Group of Galaxies
Local Supercluster
Slide 7
Redshift Survey
Cepheid Variable Stars One of the most accurate distance estimators
Slide 10
Observing Cepheid Variable Stars with HST
Slide 12
Sources of Error
Slide 14
Tully-Fisher Relation
Slide 16
The Physical Basis of the Tully-Fisher Relation
The Physical Basis of the Tully-Fisher Relation (con’d)
Tully-Fisher Relation (con’d)
Calibration of the Tully-Fisher Relations and Hubble Constant Sakai et al. 2000 ApJ in close collaboration with Jeremy Mould (MSSSO, NOAO), Shaun Hughes (Cambridge), John Huchra (Harvard), Lucas Macri (Harvard) and Robert Kennicutt (Arizona)
Tully-Fisher Relation Data
NGC 4535
Extinction Spiral galaxies have lots of dust in them!
Internal Extinction in Spiral Galaxies
Interstellar Dust Reddening
Redshift (k) correction
Tully-Fisher Relation for (late-type) Spiral Galaxies
Tully-Fisher: mostly uses Late-Type spiral galaxies
Calibration of the Multi-lTF Relations
Slide 30
Tully-Fisher Relations and H0
Uncertainties in H0 : RANDOM ERRORS
Uncertainties in H0: SYSTEMATIC ERRORS
Cluster Population Incompleteness (Malmquist) Bias
Malmquist Bias
Slide 36
Type Ia Supernovae
Slide 38
SNIa Distances
TheTip of the Red Giant Branch as a Distance Indicator
Red Giant Branches of Globular Clusters
Surface Brightness Fluctuations (SBF)
Slide 43
Other indicators:
Author: matt a malkan
E-mail: malkan@astro.ucla.edu
Homepage: www.astro.ucla.edu/~malkan
Further information: Shoko Sakai's lectures for Astronomy 274 class on Galaxy Distances: What Works