Table A.1: The sample used in this paper.
galaxy $\mu_{{\rm HSTKP}}$ $m_{{\rm lim}}$ $\log P_{{\rm lim}}$ $V_{\rm c}$
IC 4182 28.26 25.0 1.60 303.
NGC 1326A 31.04 27.0 1.60 1370.
NGC 1365 31.27 27.0 1.65 1370.
NGC 1425 31.70 27.0 1.65 1370.
NGC 2090 30.35 26.0 1.65 807.
NGC 2541 30.25 26.0 1.65 802.
NGC 3031 27.80 24.0 1.60 254.
NGC 2403 27.54 21.8 1.90 254.
NGC 3198 30.70 26.0 1.70 857.
NGC 3319 30.62 26.0 1.65 929.
NGC 3351 30.00 26.0 1.65 588.
NGC 3368 30.11 26.0 1.60 588.
NGC 3621 29.11 25.0 1.65 493.
NGC 3627 30.01 26.0 1.65 504.
NGC 4258 29.51 26.0 1.50 512.
NGC 4321 30.91 26.0 1.70 1200.
NGC 4496A 30.86 26.0 1.70 1200.
NGC 4535 30.99 26.0 1.65 1200.
NGC 4536 30.87 26.0 1.65 1200.
NGC 4548 31.05 27.0 1.55 1200.
NGC 4639 31.71 27.0 1.70 1200.
NGC 4725 30.46 26.0 1.60 696.
NGC 5253 27.49 24.5 1.50 161.
NGC 5457 29.13 25.0 1.65 388.
NGC 7331 30.84 26.5 1.60 1099.
NGC 925 29.81 26.0 1.60 775.


Source LaTeX | All tables | In the text

Article Contents
1 Introduction
2 Evidence for the Cepheid bias
3 Derivation of the bias correction curve
4 Implications for the Local Hubble constant
5 Implications for the global Hubble constant
6 Concluding remarks
References
Online Material
Appendix A: Reality of the Cepheid bias from a simple simulation
List of tables
List of figures