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For refcode 1998ApJ...499..577L:
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1998ApJ...499..577L The Far-Field Hubble Constant TOD R. LAUER Kitt Peak National Observatory, National Optical Astronomy Observatories, 2 P. O. Box 26732, Tucson, AZ 85726; lauer@noao.edu JOHN L. TONRY Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822; jt@avidya.ifa.hawaii.edu MARC POSTMAN Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218; postman@stsci.edu EDWARD A. AJHAR Kitt Peak National Observatory, National Optical Astronomy Observatories, 2 P. O. Box 26732, Tucson, AZ 85726; ajhar@noao.edu AND JON A. HOLTZMAN New Mexico State University, Box 30001, Department 4500, Las Cruces, NM 88003; holtz@nmsu.edu Received 1997 August 26; accepted 1998 January 13 ABSTRACT We used the Hubble Space Telescope to obtain surface brightness fluctuation (SBF) observations of four nearby brightest cluster galaxies (BCGs) to calibrate the BCG Hubble diagram of Lauer & Postman. This BCG Hubble diagram contains 114 galaxies covering the full celestial sphere and is volume-limited to 15,000 km s-1, providing excellent sampling of the far-field Hubble flow. The SBF zero point is based on the Cepheid calibration of the ground IKC method as extended to the WFPC2 F814W filter by Ajhar and coworkers. The BCG globular cluster luminosity functions give distances essentially identical to the SBF results. Using the velocities and SBF distances of the four BCGs alone gives H_0_ = 82 +/- 8 km s^-1^ Mpc^-1^ in the CMB frame, valid on ~4500 km s^-1^ scales; the error includes both systematic and random contributions. Use of BCGs as photometric redshift estimators allows the BCG Hubble diagram to be calibrated independently of recession velocities of the four nearby BCGs, yielding a far-field H_0_ = 89 +/- 10 km s^-1^ Mpc^-1^ with an effective depth of ~11,000 km s^-1^. The larger error in this case is due to the photometric cosmic scatter in using BCGs as redshift estimators; this H_0_ is not significantly different from the more local value. The concordance of the present results with other recent H_0_ determinations and a review of theoretical treatments on perturbations in the near-field Hubble flow argue that going to the far field removes an important source of uncertainty, but that there is not a large systematic error to be corrected for to begin with. Further improvements in H_0_ depend more on understanding nearby calibrators than on improved sampling of the distant flow. Subject headings: distance scale-galaxies: clusters: general -galaxies: distances and redshifts-galaxies: photometry
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