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Keywords:

  • errata, addenda;
  • stars: emission-line, Be;
  • stars: individual: MWC 656;
  • stars: individual: MWC 148;
  • gamma-rays: stars;
  • X-rays: stars

The paper ‘On the binary nature of the γ-ray sources AGL J2241+4454 (=MWC 656) and HESS J0632+057 (=MWC 148)’ was published in Mon. Not. R. Astron. Soc. 421, 1103–1112 (2012). We have recently discovered a small typo in the value of the zero phase used to produce the right-hand panel of Fig. 4. As a result, the orbital phase plotted is offset by approximately 0.5 with respect to the correct phase. The error affects only the phasing of the Hα emission-line parameters of MWC 148. The remainder of the paper, including Table 3 and Figs 6 and 7, is not affected. In this Erratum we provide a corrected version of Fig. 4. Note that now, with the correct phasing, the maximum in the equivalent width (EW) of the Hα line occurs ∼0.5 orbital phases past periastron.

image

Figure 4. Left: time evolution of the Hα line parameters in MWC 148. Different symbols indicate different data sets as follows: asterisk (WHT), open triangles (MT), open circles (ST) and filled circles (LT). Note the sinusoidal modulation in the LT data with a time-scale of ≈300 d. Error bars are not plotted because they are always smaller than the symbol size. Right: same as in the left-hand panel but folded on the 321-d X-ray period of Bongiorno et al. (2011). Phase 0 has been set to HJD 245 4857.5. Periastron is marked by a vertical dotted line.

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ACKNOWLEDGMENTS

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  2. ACKNOWLEDGMENTS
  3. REFERENCES

We thank Diego F. Torres, Nanda Rea and Alessandro Papitto for pointing out the presence of a phase error in the published version of the right-hand panel in Fig. 4.

REFERENCES

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  2. ACKNOWLEDGMENTS
  3. REFERENCES