Hostname: page-component-cd9895bd7-fscjk Total loading time: 0 Render date: 2024-12-25T15:38:56.476Z Has data issue: false hasContentIssue false

I-band Cepheid Distance to NGC 6822

Published online by Cambridge University Press:  15 February 2018

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

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.

NGC 6822 was the first galaxy outside the Galaxy where the Cepheid period-luminosity relation was applied as a distance indicator (Hubble 1925, ApJ, 62, 409). Later, thirteen Cepheids in this galaxy were studied by Kayser (1967, AJ, 72, 134) using BV photographic photometry. We have obtained BVRI CCD photometry of stars in two 2.2' X 3.5' fields of NGC 6822. Field 3) using Figure 1 shows an I – (V – I) diagram of ∼ 6,400 measured stars in NGC 6822 including seven known Cepheids. The reddening is estimated to E(B – V) = 0.28 ± 0.03 from the (B – V)-(V – I) diagram of the stars with V < 20 mag. The distance to NGC 6822 has been estimated using the random-phase I band photometry of seven Cepheids (V7(I=16.31), V5(I=18.97), V6(I=18.44), V3(I=17.88), V1(I=18.05), V28(I=17.61), and V2(I=17.29)) combined with their periods given by Kayser.

Type
Variable Stars as Distance Indicators
Copyright
Copyright © Cambridge University Press 1993