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2 iS 73 3.

SPECTROPHOTOMETRY OF SEYFERT 1 GALAXIES

4000WAVELENGTH (,1)

:s werePDP-8on and 2ampler .rbrock,'pectralthe top.-1. Note

star orxendenten varyhe fluxi:e theseih, the

neasurety of atraight-permitbe, the

ged, theI with aI in theDbinson'amplerare dueines are: 106 in

rases toen line.Sof the

derlyinggions ispower-

>rogrammits anhe scane scaledh otherbserved7 were8, 6583

bidden-.1 ratios,hat theh. Thisi] A4363ad often

cents is

provided by the Fe ii emission lines which are presentin nearly every Seyfert 1 galaxy (Osterbrock 1975;Boksenberg et al. 1975). These permitted lines, firstidentified in the quasar 3C 273 by Wampler and Oke(1967) and confirmed in the Seyfert galaxy I Zw I bySargent (1968), occur in several closely spaced multi-

plets and are blended to greater or lesser degrees in allSeyfert I galaxies, depending upon the widths of theFe 1i lines. In the present survey the blend of Fe ii linesbetween Hy and Hf, due to multiplets (37) and (38),was measured as one feature, called A4570 in thefigures and tables. The group of Fe nii lines just to the

No. 3, 1977

10

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ol. 215

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nits of-n are

re thus

he linemps toof thewith aiations

5000 6000

WAVELENGTH (A)

FIG. 1.-Spectral scans of Seyfert I galaxy Markarian 106, in relative energy units (ergs cm-2 s-1 A 1) versus wavelengthunits (A). Upper scan shows "blue" spectral region, lower shows "red" region; wavelengths are indicated in the rest system ofMrk 106.

D~f o, 197, _;Lu~~vraR~jrs G Ji iL _

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FIG. i. Spectra of four Seyfert galaxies, from Mk 509, typical Seyfert x, with brn

Balmer emission lines, to Mk 176, typical Seyfert 2, with narrow Balmer lines. NGC 4

and Mk 6 have Balmer-line profiles with both narrow and broad components andintermediate between these two classes.

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FIG. 1.--VLA maps of the central region of NGC 1068. The main map is at 4.9 GHz with resolution 0:4 x 0'4, and the optical nucleuscoincides with its brightest part. Contours are plotted at -0.1% (dotted), 0.1%, 0.20, 0.3%o%, 0.4°,, 0.6 0., 1%, 1.50, 20, 3%, 50, 7'o, 1000,15%, 20%, 30%, 50%, 70 oi, and 900 of the peak brightness of 0.273 Jy (beam area)-'. Insets (a), (b), and (d) show details of the brighterregions at 15.0 GHz with resolution 0"15 x 0'15, while inset (c) shows 4.9 GHz contours of the region immediately to the SW of the nucleuswith slightly better resolution than the main map. We give contour levels for the insets as percentages .of the peak brightness in theentire map. Contours for inset (a), the NE lobe at 15.0 GHz, are plotted at - 1.50 % (dotted), 1.5"0, 3",, and 4.5 ", of 56.8 mJy (beam area)-'Contours for inset (b), the central component at 15.0 GHz, are plotted at 2%, 4,, 60%, 80%, 100o, 150o, 20%, 300, 50

" , 700%, and 900,of the peak brightness of 56.8 mJy (beam area)- . Contours for inset (c), the SW "jet" at 4.9 GHz, are plotted at 0.20 , 0.4-o, 0.6",. 0.8",and 1% of 0.276 Jy (beam area)-'. Contours for inset (d), the "hot spot" to the SW of the nucleus at 15.0 GHz, are plotted at -1.500(dotted), 1.5%, 3%, 4.5%, 6%, 7.5 %,9%, 10.5 %, 12 %, and 13.5% of 56.8 mJy (beam area)-'

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