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

[Previous] | [Session 73] | [Next]

[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 A): 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 inter- pretation that the strength of the emission ines is due to laser action.

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


[Previous] | [Session 73] | [Next]