Narrow-band emission-line and continuum images obtained in subarcsecond seeing conditions are presented for the Seyfert 2 galaxy, Markarian 573. Images in the emission-lines of O I], O II], O III], S II], and H + N II] are used to measure the structure and excitation in the extended emission regions surrounding the active nucleus. The biconical region contains a variety of complex features, including two arc-like structures within 2 00 of the active nucleus that appear to be associated with the extended radio continuum emission in the sense that the radio lobes lie just inside the centroids of the emission-line arcs. These arcs probably arise from an interaction between the ISM and the radio plasma from the active nucleus. Two other emission-line features lie 3 4 00 on either side of the nucleus, and appear to be elongated nearly perpendicular to the symmetry axis of the inner radio and optical structures. The existence of multiple emission-line components could be evidence for episodic ejection of radio plasma from the active nucleus.
We have obtained low-and high-resolution spectra of the core of the highly reddened elliptical galaxy Maffei 1. From these data, we have obtained the first measurement of the Mg 2 index and have measured the velocity dispersion and radial velocity with improved accuracy. To evaluate the extinction, a correlation between the Mg 2 index and effective VÀI color has been established for elliptical galaxies. Using a new method for correcting for effective wavelength shifts, the VÀI color excess reveals that the optical depth of Galactic dust at 1 lm is 1:69 AE 0:07. Thus, A V ¼ 4:67 AE 0:19 mag, which is lower by 0.4 mag than previously thought. To establish the distance, the fundamental plane for elliptical galaxies has been constructed in I. The velocity dispersion of Maffei 1, measured to be 186:8 AE 7:4 km s À1 , in combination with modern widefield photometry in I, leads to a distance of 2:92 AE 0:37 Mpc. The D n -relation, which is independently calibrated, gives 3:08 AE 0:85 and 3:23 AE 0:67 Mpc from photometry in B and K 0 , respectively. The weighted mean of the three estimates is 3:01 AE 0:30 Mpc, which is lower than distances judged with reference to M32 and the bulge of M31 from the brightest stars seen at K 0 . Since the luminosity of asymptotic giant branch stars at K 0 is strongly dependent on age, the lower distance suggests that the last epoch of star formation in Maffei 1 occurred farther in the past than in these other systems. The distance and luminosity make Maffei 1 the nearest giant elliptical galaxy. In the absence of extinction, the galaxy would be among the brightest in the sky and would have an apparent size 2 3 that of the full Moon. The radial velocity of Maffei 1 is +66:4 AE 5:0 km s À1 , significantly higher than the accepted value of À10 km s À1 . The Hubble distance corresponding to the mean velocity of Maffei 1, Maffei 2, and IC 342 is 3.5 Mpc. Thus, it is unlikely that Maffei 1 has had any influence on Local Group dynamics.
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