Hostname: page-component-586b7cd67f-vdxz6 Total loading time: 0 Render date: 2024-11-29T17:45:37.270Z Has data issue: false hasContentIssue false
  • English
  • Français

An Hα Image of Nova V1500 Cygni Twelve Years After Outburst

Published online by Cambridge University Press:  12 April 2016

Richard A. Wade ,
R. Ciardullo ,
J.B. DeVeny ,
G.H. Jacoby  and
W.E. Schoening
Richard A. Wade
Affiliation:
Steward Observatory, University of Arizona, Tucson, Arizona 85721
R. Ciardullo
Affiliation:
National Optical Astronomy Observatories, Tucson, Arizona 85726
J.B. DeVeny
Affiliation:
National Optical Astronomy Observatories, Tucson, Arizona 85726
G.H. Jacoby
Affiliation:
National Optical Astronomy Observatories, Tucson, Arizona 85726
W.E. Schoening
Affiliation:
National Optical Astronomy Observatories, Tucson, Arizona 85726

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.

We obtained a narrow band Hα image of V1500 Cyg during an engineering run at the R-C focus of the KPNO 4 m telescope on UT 1987 July 19. Our detector was an 800 × 800 format TI CCD, which yielded a plate scale of 0.1013 arcsec/pixel. The exposure was 2000 sec and was made through a 75 Å wide filter centered at 6563 Å. The seeing was ~ 1.2 arcsec.

Our reductions were accomplished with the DAOPHOT photometry package (Stetson 1987) and IRAF data reduction facility. After performing standard bias level subtraction and flat field division, we used DAOPHOT to find the frame’s normalized point spread function (PSF) by summing the images of several field stars. We then scaled the PSF to calculate the instrumental magnitudes of the stars and of V1500 Cyg. This procedure overestimates the brightness of the nova, since the nebula contributes extra light to the central object and modifies the expected intensity distribution. (This is especially true in the narrow Hα bandpass.) Hence, in a frame where the PSF has been used to remove the fitted images, all the stars have satisfactorily small residuals around the mean sky level, except the nova itself. The image of V1500 Cyg shows sky level at the center, but a halo that rises from the center and then falls away.

Type
1c. Nebular Ejecta
Information
International Astronomical Union Colloquium , Volume 122: Physics of Classical Novae , 1990 , pp. 195 - 196
Copyright
Copyright © Springer-Verlag 1990

References

Becker, HJ., and Duerbeck, H.W. 1980, Pub. A.S.P., 92, 792.Google Scholar
Boyarchuk, A.A., and Gershberg, R.E. 1977, Astron. Zh., 54, 488.Google Scholar
Cohen, J.G. 1985, Ap. J., 292, 90.Google Scholar
Hutchings, J.B., and McCall, M.L. 1977, Ap. J., 217, 775.Google Scholar
Hutchings, J.B., Bernard, J.E., and Margetish, L. 1978, Ap. J., 224, 889.CrossRefGoogle Scholar
Lance, C.M., McCall, M.L., and Uomoto, A.K. 1988, Ap. J. Suppl, 66, 151.Google Scholar
Stetson, P.B. 1987, Pub. A.S.P., 99, 191.Google Scholar