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I-band Cepheid Distance to WLM

Published online by Cambridge University Press:  15 February 2018

Myung Gyoon Lee ,
Wendy L. Freedman  and
Barry F. Madore
Myung Gyoon Lee
Affiliation:
Carnegie Observatories, Pasadena, USA
Wendy L. Freedman
Affiliation:
Carnegie Observatories, Pasadena, USA
Barry F. Madore
Affiliation:
IPAC/JPL/Caltech, Pasadena, USA

Extract

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WLM (DD0221) is a highly resolved dwarf irregular galaxy in the Local Group. Fifteen Cepheids in this galaxy have been studied by Sandage & Carlson (1985, AJ, 90, 1464) using photographic photometry. We have obtained BVRI CCD photometry of stars in the central area (2.2' x 3.5') of WLM. Figure 1 shows an I–(V – I) diagram of ∼ 2,600 measured stars including five known Cepheids. The distance to WLM has been estimated using the random-phase I band photometr y of five Cepheids (V7(I=20.52), V29(I=20.77), V48(I=20.43), V66(I=21.19), V67(I=21.14)) combined with their periods given by Sandage & Carlson. We have obtained Δ(m - M)II(WLM – LMC) = 6.25 ± 0.11 and (m - M)0 = 24.92 ± 0.21, adopting (m - M)o(LMC) = 18.5 and AI(WLM) = 0.04.

Type
Variable Stars as Distance Indicators
Information
International Astronomical Union Colloquium , Volume 139: New Perspectives on Stellar Pulsation and Pulsating Variable Stars , 1993 , pp. 92
Copyright
Copyright © Cambridge University Press 1993