AAS Meeting #194 - Chicago, Illinois, May/June 1999
Session 73. AGN: Radio Galaxies, QSO's and Blazars
Display, Wednesday, June 2, 1999, 10:00am-6:30pm, Southeast Exhibit Hall

[73.16] Proper Motion of the quasar Ton 202

J. Talbot, Y. P. Varshni (Univ. of Ottawa)

One of us has proposed a theory of quasars based on sound physical principles which does not require the assumption of redshifts (Varshni, 1975, ApSS 37, L1; 1977, ApSS 46,443; 1979 Phys.Canada 35,11). According to this theory quasars are stars, the strength of the emission lines arises due to laser action. A search of Luyten's measurements (Luyten, 1969, A Search for Faint Blue Stars, Paper 50) has shown that the quasar Ton 202 (apparent z=0.366) has a substantial proper motion. From the data given by Luyten, the absolute proper motion for Ton 202 turns out to be 52.6 ms/year with a mean error of 16 ms/year. If we calculate the transverse velocity corresponding to the smallest value of the proper motion within the uncertainty range, assuming H = 50 km/sec  per Mpc and q0= 0, it turns out to be 1100c. The evidence clearly indicates that Ton 202 is a star. More accurate measurements of the proper motion of Ton 202 are highly desirable. We identify the observed emission lines (wavelengths in Å): 1640 (He II 1640), 2110 (Ca II 2103,2113), 2600 (O III 2598, 2605 and C III 2610,2614,2617), 3810 (O VI 3811,3834). We note here that while most members of the same spectral class (e.g., PKS 2059+034, 4C 27.38, 4C 09.31, 3C 48, 4C 37.43 etc) show the He II 4686 emission line, Ton 202 does not. This further supports the interpretation that the strength of the emission lines is due to laser action.

If the author provided an email address or URL for general inquiries, it is a s follows:


An numbered index of references or a sequential list of abstracts is also available.