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Cepheids in IC 4182, Calibration of SNIa 1937C and the Hubble constant

Published online by Cambridge University Press:  15 February 2018

A. Saha ,
A. Sandage ,
N. Panagia ,
G. A. Tammann ,
L. Labhardt ,
H. Schwengeler  and
F. D. Macchetto
A. Saha
Affiliation:
Space Telescope Science Institute, Baltimore, MD, USA
A. Sandage
Affiliation:
Observatories of the Carnegie Institution of Washington, Pasadena, CA, USA
N. Panagia
Affiliation:
Space Telescope Science Institute, Baltimore, MD, USA
G. A. Tammann
Affiliation:
Universitat Basel, Basel, Switzerland
L. Labhardt
Affiliation:
Universitat Basel, Basel, Switzerland
H. Schwengeler
Affiliation:
Universitat Basel, Basel, Switzerland
F. D. Macchetto
Affiliation:
Space Telescope Science Institute, Baltimore, MD, USA

Abstract

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Observations with the Wide Field Camera on HST were examined, and 27 Cepheids were discovered. Photometry and period analysis have produced unambiguous light curves free of alias. The observed P-L relation has a slope consistent with seminal calibration studies of Galactic and LMC Cepheids. An apparent distance modulus (in V) of 28.47 ± 0.10 to IC 4182 is derived. This implies that Mv(max) for SNIa 1937C is -19.92 ± 0.2 mag, independent of everything except differential absorption between the Cepheids and the supernova. Using this to calibrate Hubble diagrams for SNIa by several authors, and allowing for a 1-σ uncertainty in the absolute magnitude from the calibration of only one SNIa, we obtain H0 = 45 ± 14kms-1Mpc-1.

Type
Variable Stars as Distance Indicators
Information
International Astronomical Union Colloquium , Volume 139: New Perspectives on Stellar Pulsation and Pulsating Variable Stars , 1993 , pp. 53 - 60
Copyright
Copyright © Cambridge University Press 1993

References

Baade, W., Zwicky, F., 1938, Astrophys. J., 88, 418.Google Scholar
Beyer, M. 1939, Astron. Nachr., 268, 341.CrossRefGoogle Scholar
Delia Valle, M., Panagia, N. 1992, Astron. J. 104, 696.CrossRefGoogle Scholar
Faber, S. et al. 1992, Wide Field/Planetary Camera Final Orbital Science Verification Report, STScI.Google Scholar
Feast, M., Walker, A. R., 1987, ARA&A, 25, 345.Google Scholar
Harris, H. C., Baum, W. A., Hunter, D. A., Kreidl, T. J. 1991, Astron. J. 101, 677.CrossRefGoogle Scholar
Lafler, J., Kinman, T. D., 1965, Astrophys. J. Supp., 11, 216.CrossRefGoogle Scholar
Leibundgut, B., Tammann, G. A., Cadonau, R., Cerrito, D., 1989, Astron. & Astrophys. 89, 537.Google Scholar
Madore, B., Freedman, W. L., Pub. Astron. Soc. Pac., 1991, 103, 933.CrossRefGoogle Scholar
Mateo, M., Schechter, P. 1989, in The First ESO/ST-ECF Workshop on Data Analysis, ed. Grosbol, P. J., Murtagh, F., and Warmels, R.H. (ESO, Munich), p. 69.Google Scholar
Saha, A., Hoessel, J. G., 1990, Astron. J., 99, 97.CrossRefGoogle Scholar
Sandage, A., Tammann, G. A., 1968, Astrophys. J., 151, 531.CrossRefGoogle Scholar
Sandage, A., Tammann, G. A., 1982, Astrophys. J., 256, 339.CrossRefGoogle Scholar
Tammann, G. A., Leibundgut, B., 1990, Astron. & Astroph., 236, 9.Google Scholar