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Photometric Variability of Be/X‐Ray Pulsar Binaries in the Small Magellanic Cloud

  • Authors: P. C. Schmidtke and A. P. Cowley

Schmidtke & Cowley 2006 The Astronomical Journal 132 919.

  • Provider: AAS Journals

Caption: Fig. 7.

Top panel: Long‐term R (upper) and I (lower) light curves of RX J0105.1−7211 (SXP3.34). Second panel: Periodogram of ﹩R^{*}﹩ data showing the exceptionally strong peak at ﹩P=1.099﹩ days. Third panel: Folded and binned light curves in ﹩V^{*}﹩, ﹩R^{*}﹩, and ﹩I^{*}﹩ at ﹩P=1.099﹩ days. The amplitude is largest in ﹩I^{*}﹩. Fourth panel: Periodogram of ﹩R^{*}﹩ data after the 1.099 day variation has been subtracted. The strongest remaining power is at ﹩P=0.980﹩ days. Bottom panel: ﹩V^{*}﹩, ﹩R^{*}﹩, and ﹩I^{*}﹩ light curves, folded on ﹩P=0.980﹩ days, after removal of the 1.099 day signal. See text for further discussion of this source.

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