Galaxy Distances - Then and Now Brent Tully, University of Hawaii with the essential collaboration of Rick Fisher, Ed Shaya, and Helene Courtois I have now been able to reach a solution which I regard as definitive. The result is 865 km/s/Mpc. A.S. Eddington 1935, MNRAS, 95, 636 Are galaxies galaxies? E Hubble 1924, 33rd mtg AAS Cepheids in M31 and M33 d = 285 kpc Are galaxies galaxies? E Hubble 1924, 33rd mtg AAS Cepheids in M31 and M33 d = 285 kpc E Opik 1922, ApJ, 155, 406 Virial theorem: M~V 2 R d = 450 kpc Are galaxies galaxies? E Hubble 1924, 33rd mtg AAS Cepheids in M31 and M33 d = 285 kpc E Opik 1922, ApJ, 155, 406 Virial theorem: M~V 2 R d = 450 kpc Distances in the early 70s Desperation methods: - diameters of HII regions - brightest blue supergiants - brightest red supergiants - luminosity classifications - sosi Less desperate: - indicative total mass M T = 0.1 D V 2 / sin 2 i D = distance = size V = profile 1/2 width Roberts 1962, AJ, 67, 431 Balkowski et al. 1973, A&A, 23, 139 Opiks method Fisher and Tully Graduate: 1972 A Thought Experiment M31 M pg = W i = 258 km/s M33 M pg = W i = 109 km/s A Thought Experiment M31 M pg = W i = 258 km/s M33 M pg = W i = 109 km/s M pg = ?? M pg = ?? factor 2 distance changes Tully & Fisher 1977, A&A, 54, 661 Virgo Cluster: d = 13.2 Mpc H 0 ~ 80 km/s/Mpc my H 0 contributions TF: 1977, A&A, 54,661 PT: 1988, ApJ, 330, 579 TP: 2000, ApJ, 533, 744 CT: 2012, ApJ, 749, (Apr 10) H 0 = 85 PT: 2 clusters; 3 ZP I) H 0 = 77 TP: 12 clusters; 24 ZP H 0 = 75.9 CT: 13 clusters; 36 ZP; SNIa tie L band my H 0 contributions TF: 1977, A&A, 54,661 PT: 1988, ApJ, 330, 579 TP: 2000, ApJ, 533, 744 CT: 2012, ApJ, 749, (Apr 10) H 0 = 85 PT: 2 clusters; 3 ZP I) H 0 = 77 TP: 12 clusters; 24 ZP H 0 = 75.9 CT: 13 clusters; 36 ZP; SNIa tie L band We knew in 1988 that CDM with m =1 was wrong Calibration 2012 M i bik = (logW i mx ) Calibration 2012 M i bik = (logW i mx ) NGC 2403 (only ZP calibrator at I in 1988) M = 0.27 => 13% in distance H 0 : 75=>85 SNIa calibration: link to large scales Cepheid, TRGB, SBF, TF, FP Courtois & Tully 2012, ApJ, 748, #2 Mid Infrared Calibration 1. uniformity across sky 2. flux dominantly from old stars 3. minimal extinction corrections 4. deep `total photometry But: color is a 3rd parameter Sorce et al. 2012, in prep. S : Spitzer 3.5 m fluxes - color adjustment Deviations from Cosmic Expansion V obs = H 0 d + V pec H 0 = Aaronson, Huchra, Mould, Schechter, Tully 1982, ApJ, 258, 64 Virgocentric flows in Local Supercluster Ed Shayas thesis: Shaya 1984, ApJ, 280, 470 Anticipated Great Attractor influence Tully & Shaya 1984, ApJ, 281, 31 Virgo infall Shaya & Tully 1984, ApJ, 281, 56 Angular momentum in galaxies mass of Virgo Cluster well constrained by most extreme infalling galaxies many galaxies, mostly spirals, enter Virgo Cluster in next 3 Gyr Quiet Local Flow and Local Velocity Anomaly Sandage, Tammann, & Hardy 1972, ApJ, 172, 253 Tammann & Kraan 1978, IAU Symp 79, 71 Tully 1982, ApJ, 257, 389 Karachentsev, Kashibadze, Makarov, Tully 2009, 393, 1265 TRGB distances with HST los ~ 25 km/s Quiet Local Flow and Local Velocity Anomaly Faber & Burstein 1988, Vatican Study Week, p116 Tully 1988, Vatican Study Week, p169 Tully, Shaya, Karachentsev, Courtois, et al. 2008, ApJ, 676, 184 orange: V pec > 100 km/s green: |V pec | < 100 km/s purple: V pec < -100 km/s Local Superclusterzoom in Velocity discontinuity between Local Sheet and adjacent Leo Spur Quiet Local Flow and Local Velocity Anomaly Faber & Burstein 1988, Vatican Study Week, p116 Tully 1988, Vatican Study Week, p169 Tully, Shaya, Karachentsev, Courtois, et al. 2008, ApJ, 676, 184 orange: V pec > 100 km/s green: |V pec | < 100 km/s purple: V pec < -100 km/s Local Superclusterzoom in vectors orange: 323 km/s blue: 185 km/s toward Virgo red: 259 km/s away from Local Void Velocity discontinuity between Local Sheet and adjacent Leo Spur Numerical Action Models out of Local Void toward Virgo Peebles 1989, ApJ, 344, L53 Shaya, Peebles, Tully 1995, ApJ, 454, 15 Peebles, Phelps, Shaya, Tully 2001, ApJ, 554, 104 NAM: small scales Virgo from Void Model focusing on the interactions between the dominant galaxies in the Local and Maffei groups. NAM: intermediate scales Shaya, Peebles, & Tully 1995, ApJ, 454, 15 Distances to galaxies with V m = Gyr MAK Reconstruction (Monge-Ampere-Kantorovich) Lavaux, Tully, Mohayaee, Colombi 2010, ApJ, 709, 483 Action reconstruction with 10 5 galaxies Wiener Filter Cosmicflows-1 (distances) redshift survey local tidal Courtois, Hoffman, Tully, Gottloeber 2012, ApJ, 744, 43 Cosmicflows-2 Courtois, Tully, Fisher et al. 2009, AJ, 138, 1938 Courtois, Tully, Fisher et al. 2011, MNRAS, 414, 2005 Courtois, Tully, Heraudeau 2011 MNRAS, 415, 1935 As of 2012, April 1: 14,221 galaxies with HI profiles 11,353 galaxies good HI link Cepheid - TRGB - SBF link SFI++ - FPlink SNIa EDD: Extragalactic Distance DatabaseTully et al. 2009, AJ, 138, 323 Photometry Courtois et al. 2011, MNRAS, 415, 1935 Sorce et al. in preparation HST CMD Jacobs et al. 2009, AJ, 138, 332 HI profiles Courtois et al. 2009, AJ, 138, 1938 Courtois et al. 2011, MNRAS, 414, 2005 Redshift catalogs Group information Summary distances Curators: Luca Rizzi, Ed Shaya