Mathematics – Logic
Scientific paper
Dec 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...197.7503o&link_type=abstract
American Astronomical Society, 197th AAS Meeting, #75.03; Bulletin of the American Astronomical Society, Vol. 32, p.1521
Mathematics
Logic
Scientific paper
Probably, the most intriguing case of closely associated objects having discordand redshifts is represented by the galaxy NGC 4319 (z=0.006) and a peculiar object Mrk 205 (z=0.07) just 40'' away [1]. The luminous connection extending from Mrk 205 into the galaxian nucleus as well as a corresponding feature on the opposite side of the disk linking the nucleus with a bright UV knot may indicate an explosive ejection of both the objects from the nucleus [2]. Below, I propose to explain the essentially discordant redshifts of Mrk 205 and the UV knot by ejecting them with a relativistic velocity, similar to the two redshifted peculiar objects aligned across NGC 4258 [3]. In my interpretation, the redshift of Mrk 205 includes (i) a receding component, zr=0.065, due to the transverse Doppler effect and (ii) a cosmological component, zc=0.006. The velocity of ejection and the angle between the direction of ejection and the line of sight are found to be vej/c=(zr+z_a) )1/2≈ 0.261 and \vartheta= arccos (zr-z_a) (z_r+z_a) -1/2≈ 76o.3, correspondingly, assuming the UV knot to approach with redshift za≈ 0.003 [2]. The proposed interpretation has a number of testable consequences, including the decisive test: Mrk 205 is expected to have an annual proper motion of >= 0.8 (D/20 Mpc) )-1 milliarcsec, which could be measured at radio wavelengths for the unresolved radio counterpart [4] to Mrk 205. If confirmed, this model would indicate that some pairs of quasar-like sources aligned with galaxies represent relativistic ejecta from the galactic nuclei, and the redshifts of those sources include a substantial component produced by the transverse Doppler effect.
References:
[1] Arp, H. 1995, IAU Symp. 168, p. 369 and refs. therein
[2] Sulentic, J.W. & Arp, H. 1987, ApJ 319, 687 and 693
[3] Ozernoy, L.M. 1996, Bull. Amer. Astr. Soc. 28, 846
[4] Sulentic, J.W. 1986, ApJ 304, 617
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