Hostname: page-component-76fb5796d-vfjqv Total loading time: 0 Render date: 2024-04-25T17:02:15.347Z Has data issue: false hasContentIssue false
  • English
  • Français

Cepheid distances from the Baade–Wesselink method

Published online by Cambridge University Press:  26 February 2013

Wolfgang Gieren ,
Jesper Storm ,
Nicolas Nardetto ,
Alexandre Gallenne ,
Grzegorz Pietrzyński ,
Pascal Fouqué ,
Thomas G. Barnes  and
Daniel Majaess
Wolfgang Gieren
Affiliation:
Universidad de Concepción, Departamento de Astronomía, Casilla 160-C, Concepción, Chile email: wgieren@astro-udec.cl
Jesper Storm
Affiliation:
Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany email: jstorm@aip.de
Nicolas Nardetto
Affiliation:
Laboratoire Lagrange, UMR7293, UNS/CNRS/OCA, 06300 Nice, France
Alexandre Gallenne
Affiliation:
Universidad de Concepción, Departamento de Astronomía, Casilla 160-C, Concepción, Chile email: wgieren@astro-udec.cl
Grzegorz Pietrzyński
Affiliation:
Universidad de Concepción, Departamento de Astronomía, Casilla 160-C, Concepción, Chile email: wgieren@astro-udec.cl
Pascal Fouqué
Affiliation:
IRAP, Université de Toulouse, CNRS, 14 Avenue E. Belin, 31400 Toulouse, France
Thomas G. Barnes
Affiliation:
University of Texas at Austin, McDonald Observatory, 82 Mt. Locke Road, TX 79734, USA
Daniel Majaess
Affiliation:
Department of Astronomy and Physics, Saint Mary's University, Halifax, NS B3H 3C3, Canada
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Recent progress on Baade–Wesselink (BW)-type techniques to determine the distances to classical Cepheids is reviewed. Particular emphasis is placed on the near-infrared surface-brightness (IRSB) version of the BW method. Its most recent calibration is described and shown to be capable of yielding individual Cepheid distances accurate to 6%, including systematic uncertainties. Cepheid distances from the IRSB method are compared to those determined from open cluster zero-age main-sequence fitting for Cepheids located in Galactic open clusters, yielding excellent agreement between the IRSB and cluster Cepheid distance scales. Results for the Cepheid period–luminosity (PL) relation in near-infrared and optical bands based on IRSB distances and the question of the universality of the Cepheid PL relation are discussed. Results from other implementations of the BW method are compared to the IRSB distance scale and possible reasons for discrepancies are identified.

Keywords

Cepheidsdistance scale
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S289: Advancing the Physics of Cosmic Distances , August 2012 , pp. 138 - 144
Copyright
Copyright © International Astronomical Union 2013

References

Baade, W. 1926, Astron. Nachr., 228, 359Google Scholar
Benedict, G. F., McArthur, B. E., Feast, M. W., et al. 2007, AJ, 133, 1810CrossRefGoogle Scholar
Fouqué, P., & Gieren, W. P. 1997, A&A, 320, 799Google Scholar
Gallenne, A., Kervella, P., & Mérand, A. 2011, A&A, 538, A24Google Scholar
Gallenne, A., Kervella, P., Mérand, A., et al. 2012, A&A, 541, A87Google Scholar
Gieren, W., Storm, J., Barnes, T. G. III, et al. 2005, ApJ, 627, 224Google Scholar
Gieren, W. P., Barnes, T. G. III, & Moffett, T. J. 1993, ApJ, 418, 135Google Scholar
Gieren, W. P., Fouque, P., & Gomez, M. 1998, ApJ, 496, 17Google Scholar
Gieren, W. P., Fouque, P., & Gomez, M. I. 1997, ApJ, 488, 74Google Scholar
Groenewegen, M. A. T. 2007, A&A, 474, 975Google Scholar
Groenewegen, M. A. T. 2013, A&A, in pressGoogle Scholar
Hindsley, R., & Bell, R. A. 1986, PASP, 98, 881Google Scholar
Joner, M. D. & Laney, C. D. 2012, in Am. Astron. Soc./Div. Dyn. Astron. Mtg 43 09.02Google Scholar
Kervella, P., Bersier, D., Mourard, D., et al. 2004a, A&A, 428, 587Google Scholar
Kervella, P., Fouqué, P., Storm, J., et al. 2004b, ApJ, 604, L113Google Scholar
Kervella, P., Mérand, A., Perrin, G. & Coudé Du Foresto, V. 2006, A&A, 448, 623Google Scholar
Luck, R. E., Moffett, T. J., Barnes, T. G. III, & Gieren, W. P. 1998, AJ, 115, 605Google Scholar
Majaess, D., Turner, D., & Gieren, W. 2012a, ApJ, 747, 145Google Scholar
Majaess, D., Turner, D., Gieren, W., Balam, D., & Lane, D. 2012b, ApJ, 748, L9Google Scholar
Majaess, D., Turner, D., Moni Bidin, C., et al. 2011, ApJ, 741, L27Google Scholar
Mérand, A., Aufdenberg, J. P., Kervella, P., et al. 2007, A&A, 664, 1093Google Scholar
Mérand, A., Kervella, P., Coudé Du Foresto, V., et al. 2006, A&A, 453, 155Google Scholar
Mérand, A., Kervella, P., Coudé Du Foresto, V., et al. 2005, A&A, 438, L9Google Scholar
Molinaro, R., Ripepi, V., Marconi, M., et al. 2011, MNRAS, 413, 942Google Scholar
Molinaro, R., Ripepi, V., Marconi, M., et al. 2012, ApJ, 748, 69Google Scholar
Nardetto, N., Fokin, A., Fouqué, P., et al. 2011, A&A, 534, L16Google Scholar
Nardetto, N., Gieren, W., Kervella, P., et al. 2009, A&A, 502, 951Google Scholar
Ngeow, C.-C., Neilson, H. R., Nardetto, N., & Marengo, M. 2012, A&A, 543, A55Google Scholar
Persson, S. E., Madore, B. F., Krzemiński, W., et al. 2004, AJ, 128, 2239CrossRefGoogle Scholar
Pietrzyński, G., Thompson, I. B., Gieren, W., et al. 2010, Nature 468 542Google Scholar
Pietrzyński, G., Thompson, I. B., Graczyk, D., et al. 2011, ApJ, 742, L20CrossRefGoogle Scholar
Pietrzyński, G., Thompson, I. B., Graczyk, D., et al. 2009, ApJ, 697, 862Google Scholar
Romaniello, M., Primas, F., Mottini, M., et al. 2008, A&A, 488, 731Google Scholar
Storm, J., Carney, B. W., Gieren, W. P., et al. 2004, A&A, 415, 531Google Scholar
Storm, J., Gieren, W., Fouqué, P., et al. 2011a, A&A, 534, A94Google Scholar
Storm, J., Gieren, W., Fouqué, P., et al. 2011b, A&A, 534, A95Google Scholar
Turner, D. G. 2010, Ap&SS 326 219Google Scholar
Turner, D. G., Majaess, D. J., Lane, D. J., et al. 2012, MNRAS, 422, 2501Google Scholar
van der Marel, R. P. & Cioni, M.-R. L. 2001, AJ, 122, 1807Google Scholar
Wesselink, A. J. 1946, Bull. Astron. Inst. Neth., 10, 91Google Scholar