Observations of NGC 4151 During 1970 in the Optical and Infra-red

Creators: Penston, M. V.; Penston, Margaret J.; Neugebauer, G.; Tritton, K. P.; Becklin, E. E.; Visvanathan, N.

Abstract

Observations of NGC 4151 at seven wavelengths from 0.3 to 3.4 microns made during the 1970 season are presented. Variations are found at all observed wavelengths but the optical and infra-red light curves are different: an optical maximum was reached in April but the galaxy continued brightening at 2.2 μ . until the end of June. The energy distributions of the point source and the background galaxy have been separated and that of the point source Closely resembles that of the quasar 3C273. The general form of the light curves can possibly be attributed to a dust model for the infra-red emission but this would be ruled out if suspected rapid infra-red variations are confirmed.

Additional Information

© 1971 Royal Astronomical Society. Provided by the NASA Astrophysics Data System. Received 1971 March 11; Published: 01 August 1971. We are grateful to our night assistants Gene Hancock, Eugene Marosan, Pete Mastrosimone, Gary Tuton, and Tom Zinter and our colleagues John Danziger, Gordon Garmire, Frank Porter and Henry Tye for help in obtaining the infra-red observations. Mrs Rosemary Selmes measured most of the photographic material described here. We are also grateful to Dr T. D. Kinman for supplying us with a photoelectric sequence for NGC 4151 in advance of publication. One of us (M. V. P.) acknowledges the support of a Carnegie Fellowship, another of us (M. J.P.) wishes to thank the Carnegie Institution of Washington for providing hospitality and the status of Guest Investigator during the period of this work. Two of us (E. E. B. and N. V.) were Visiting Astronomers at the Kitt Peak National Observatory, which is operated by the Association of Universities for Research in Astronomy Inc., under contract with the National Science Foundation. This work was also supported in part by NASA Grant NGL 05-002-007. We are all grateful to the observatories at which we have worked for a generous allocation of observing time.

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