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\begin{document}
\setcounter{page}{44} 
\begin{deluxetable}{rlcccrccc}
\tablecaption{60 $\mu$m Sample Properties}
\small
\tablehead{\colhead{Num.}&\colhead{Name}&\colhead{Type}&\colhead{V$_{rad}$}&
\colhead{L$_{60~\mu m}$}&\colhead{F$_{3.6~cm}$}&\colhead{L$_{3.6~cm}$}&
\colhead{Radio Extent}&\colhead{Comments}\cr
& & &(km~s$^{-1}$)&(erg s$^{-1}$)&(mJy)&(W~Hz$^{-1}$)&at 3.6 cm (pc)&}
\startdata
16&MRK\,348          	&2&	4540&	43.52&  345.6& 23.18&	33&	\cr
24&TOL\,0109-38      	&2&	3496&	43.38&  13.1&  21.53&	\llap{3}30&	\cr	
26&MRK\,1  	   	&2&	4780&	43.81&  11.1&  21.73&	31&	u\cr
27&MRK\,359          	&1&	5012&	43.37&  0.5 &  20.43&	\llap{1}70&	\cr
33&MRK\,573          	&2&	5174&	43.56&  1.8 &  21.01&	\llap{10}03&	\cr	
37&IRAS\,01475-0740  	&2&	5306&	43.54&  135.4& 22.91&	34&	u\cr
41&ESO\,153-G20	   	&2&	5917&	43.52&  ---  & ---&	---&	\cr
47&MRK\,1040 	   	&1&	4927&	43.88&  1.1  & 20.76&	32&	u\cr
52&ESO\,355-G25 	&2&	5039&	43.59&  ---  & ---&	---&	\cr
53&UGC\,2024 	   	&2&	6714&	44.12&  0.7  & 20.83&	43&	u\cr
57&NGC\,1068         	&2&	1136&  	44.41&  762.4& 22.32&\llap{7}45&	\cr	
67&MCG\,-02-08-039   	&2&	8874&	43.69&  2.0  & 21.53&	57&	u\cr
68&UGC\,2514         	&1&	3957&	43.11&  0.6  & 20.30&	69&	\cr
75&IRAS\,03106-0254  	&2&	8154&	43.89&  10.8 & 22.18&	\llap{8}54&	\cr
78&IRAS\,03125+0119  	&2&	7200&	43.67&  8.8  & 21.99&	47&	u\cr
83&MRK\,607 	   	&2&	2716&	43.27&  1.3  & 20.31&	20&	u\cr
85&ESO\,116-G18 	&2&	5546&	43.64&  ---  & ---&	---&	\cr
141&IRAS\,04385-0828 	&2&	4527&	43.81&  7.5 &  21.52&	29&	u\cr
154&IRAS\,04502-0254 	&2&	4737&	43.34&  0.4 &  20.28&	\llap{1}07&	\cr
156&IRAS\,04507+0358 	&2&	8811&	43.74&  0.8 &  21.12&	\llap{2}05&	\cr
157&ESO\,33-G02      	&2&	5426&	43.34&  --- &  ---&	---&	\cr
174&MCG\,-05-13-017  	&1&	3790&	43.31&  2.5 &  20.88&	24&	u\cr
196&MRK\,3           	&2&	4050&	43.85&  79.0&  22.44&	\llap{3}75&	\cr
203&UGC\,3478        	&1&	3828&	43.38&  1.4 &  20.64&	25&	u\cr
209&MRK\,6           	&1&	5537&	43.63&  30.0&  22.29&	\llap{4}37&	\cr
213&FAIRALL\,265     	&1&	8844&	43.81&  --- &  ---&	---&	\cr
225&MRK\,79          	&1&	6652&	43.85&  2.9 &  21.44&	\llap{12}55&	\cr	
227&MRK\,10	   	&1&	8785&	43.85&  0.3 &  20.69&	57&	u\cr
233&UGC\,4155	   	&1&	7645&	43.83&  2.4 &  21.48&	49&	u\cr
236&MRK\,622         	&2&	6964&	43.85&  1.7 &  21.24&	\llap{1}10&	\cr	
244&ESO\,18-G09	   	&2&	5341&	43.60&  --- &  ---&	---&	\cr
253&MCG\,-01-24-012  	&2&	5892&	43.41&  8.9 &  21.82&	\llap{1}33&	\cr
260&MRK\,1239 	   	&1&	5974&	43.73&  7.9 &  21.78&	53&	u\cr
272&NGC\,3393        	&2&	4107&	43.50&  10.7&  21.59&	\llap{6}83&	\cr
278&NGC\,3516        	&1&	2649&	43.15&  4.1 &  20.79&	18&	\cr
281&IRAS\,11215-2806 	&2&	4047&	43.01&  10.8&  21.58&	\llap{4}03&	\cr
282&MCG\,-05-27-013  	&2&	7162&	43.53&  4.7 &  21.71&	\llap{15}30&	\cr
283&MRK\,176         	&2&	8346&	43.69&  6.3 &  21.97&	\llap{1}35& interacting  \cr
286&NGC\,3783	   	&1&	2550&	43.42&  7.7 &  21.03&	17&	u\cr
292&MRK\,766         	&1&	3876&	43.79&  8.6 &  21.44&	67&	\cr
293&NGC\,4388        	&2&	2524&  	43.84&  9.4 &  21.11&	\llap{29}40&	\cr
299&NGC\,4507	   	&2&	3538&	43.73&  --- &  ---&	---&	\cr
301&NGC\,4593        	&1&	2698&	43.23&  2.1 &  20.51&	17&	u\cr
302&TOL\,1238-364    	&2&	3285&	43.87&  --- &  ---&	---&	\cr
306&NGC\,4704        	&2&	8134&	44.09&  0.8 &  21.05&	53&	u\cr
309&MCG\,-02-33-034  	&1&	4386&	43.35&  1.2 &  20.69& 	28&u interacting\cr
310&ESO\,323-G32     	&2&	4796&	43.34&  --- &  ---&	---&	\cr
313&MCG\,-04-31-030  	&2&	2957&	43.34&  6.5 &  21.08&	\llap{4}78&	\cr
314&IRAS\,13059-2407 	&2&	4175&	43.42&  10.4&  21.59&	27&	u\cr\tablebreak
317&MCG\,-03-34-064  	&2&	5152&	44.16&  54.1&  22.49&	\llap{2}78&	\cr
322&ESO\,383-G18     	&2&	3837&	43.01&  1.7 &  20.73&	\llap{1}07&	\cr
324&MCG\,-6-30-15    	&1&	2323&	42.77&  0.9 &  20.01&	\llap{1}10&	u\cr
329&NGC\,5347	   	&2&	2335&	42.96&  1.6 &  20.27&	15&	u\cr
340&IRAS\,14082+1347 	&2&	4836&	43.96&  3.2 &  21.2\phn&	53&	\cr
341&NGC\,5506        	&2&	1753&	43.47&  95.0&  21.79&	\llap{3}02&	\cr
344&NGC\,5548        	&1&	5149&	43.48&  3.1 &  21.24&	44&interacting\cr
349&IRAS\,14317-3237 	&2&	7615&	43.76&  1.9 &  21.37&	\llap{2}86&	\cr
354&IRAS\,14434+2714 	&2&	8814&	43.81&  8.8 &  22.16&	\llap{1}20&	u\cr
369&UGC\,9826 	   	&1&	8754&	43.59&  0.2 &  20.51&	57&	u\cr
377&UGC\,9944        	&2&	7354&	43.91&  5.9 &  21.83&	\llap{34}30&	\cr
383&IRAS\,15480-0344 	&2&	9084&	44.02&  11.2&  22.29&	59&	u\cr
409&IRAS\,16288+3929 	&2&	9091&	43.78&  4.8 &  21.93&	59&	u\cr
418&IRAS\,16382-0613 	&2&	8317&	43.81&  2.1 &  21.49&	54&	u\cr
445&UGC\,10889	   	&2&	8424&	43.72&  1.1 &  21.22&	54&	u\cr
447&MCG\,+03-45-003  	&2&	7292&	43.60&  0.3 &  20.53&	47&	u\cr
471&FAIRALL\,49	   	&2&	6065&	44.09&  --- &  ---&	---&	\cr
473&FAIRALL\,51	   	&1&	4255&	43.56&  --- &  ---&	---&	\cr
497&ESO\,143-G09	&1&	4462&	43.33&  --- &  ---&	---&	\cr
501&FAIRALL\,341	&2&	4887&	43.32&  --- &  ---&	---&	\cr
510&UGC\,11630	   	&2&	3657&	43.25&  0.4 &  20.06&	24&	u\cr
512&PKS\,2048-57     	&2&	3402&	43.84&  229.1& 22.75&	\llap{9}24&	\cr
530&NGC\,7213	   	&1&	1792&	42.93&  187.9& 22.11&	12&	u\cr
537&MRK\,915	   	&1&	7230&	43.48&  14.7 & 22.21&	47&	u\cr
538&UGC\,12138	   	&1&	7375&	43.72&  1.9  & 21.34&	81&	u\cr
540&AKN\,564         	&1&	7195&	43.67&  7.0  & 21.89&	\llap{3}16&	\cr
549&UGC\,12348	   	&2&	7585&	43.97&  1.1  & 21.13&	\llap{1}18&	u\cr
555&NGC\,7674        	&2&	8713&	44.64&  39.8 & 22.81&	\llap{4}22&	\cr
590&MRK\,590	   	&1&	7910&	43.49&  3.2  & 21.63&	51&	u\cr
594&MRK\,1058	   	&2&	5138&	43.19&  0.2  & 20.05&	33&	u\cr
602&NGC\,1386        	&2&	868&	42.61&  10.8 & 20.24&	20&	\cr
615&MCG\,+8-11-11    	&1&	6141&	44.06&  24.4 & 22.29&	\llap{12}30&	\cr
627&MRK\,705	   	&1&	8658&	43.65&  2.0  & 21.50&	56&	u\cr
634&NGC\,3281	   	&2&	3200&	43.85&  17.0 & 21.57&	60&	\cr
638&UGC\,6100	   	&2&	8778&	43.65&  0.8  & 21.12&	57&	u\cr
665&NGC\,4941        	&2&	1108&	42.26&  4.0  & 20.02&	15&	\cr
703&UGC\,10683B      	&1&	9234&	43.61&  0.6  & 21.04& 	60&u interacting\cr
708&ESO\,103-G35	&2&	3983&	43.57&  ---  & ---&	---&	\cr
721&NGC\,7212        	&2&	7984&	44.27&  18.1 & 22.39& 	\llap{3}61&interacting\cr
\tablenotetext{}{In the cases where the radio emission was not extended
we assumed an upper limit of 0.1$^{\prime\prime}$. These cases are indicated by
a letter ``u'' in the last column.}
\enddata
\normalsize
\end{deluxetable}
 


\begin{deluxetable}{lcrrrcccc}
\tablewidth{0pc}
\tablecaption{Measurements for Galaxies with Extended Radio Emission
in the 60 $\mu$m sample}
\tablehead{\colhead{Name}&\colhead{Type}&\colhead{PA$_{MA}$}&
\colhead{i}&\colhead{PA$_{RAD}$}&\colhead{closer}&
\colhead{source}&\colhead{Radio}&\colhead{references/}\cr
&&&&&side&side&Morphology&comments}
\startdata
MRK\,348        &2 & 170 &  16 &  $-15$ &   e  &  rot   & L &1, 9  \cr
TOL\,0109-38    &2 &  61 &  64 &  96  &   s  &  dust  & S &2, 5  \cr
MRK\,359        &1 &   8 &  34 &  75  &   --  &    ---   & S &2, 5 \cr
MRK\,573        &2 &   5 &  30 &  125 &   n  &  rot   & L &3, 5   \cr
NGC\,1068       &2 & 115 &  28 &  0   &   s  &  rot   & L &4, 10  \cr 
UGC\,2514       &1 & $-40$ &  55 &  56  &   sw &  dust  & L &5, 5   \cr
IRAS\,03106-0254&2 & $-14$ &  71 &  37  &   --  &    ---   & L &5, 5   \cr    
IRAS\,04502-0317&2 &  15 &  59 &  22  &   e  &  dust  & L &5, 5   \cr 
IRAS\,04507+0358&2 &  46 &  36 &  153 &   --  &    ---   & S &5, 5 \cr
MRK\,3          &2 &  28 &  33 &  86  &   --  &    ---   & L &3, 5 \cr
MRK\,6          &1 & $-46$ &  54 &  $-3$  &   ne &  dust  & L &5, 5   \cr
MRK\,79         &1 & $-47$ &  36 &  11  &   e  &  rot   & L &5, 5  \cr
MRK\,622        &2 & $-35$ &  26 &  0   &   --  &   ---   & S &2, 5 \cr
MGC\,-01-24-012 &2 &  42 &  54 &  89  &   nw &  rot   & L &5, 5  \cr
NGC\,3393       &2 &  41 &  30 &  56  &   nw &  rot   & L &5, 5 \cr
NGC\,3516       &1 &  56 &  36 &  10  &   n  &  dust  & L &2, 5  \cr
IRAS\,11215-2806&2 & $-34$ &  70 &  75  &   --  &   ---   & L &5, 5 \cr
MGC\,-05-27-013 &2 & $-82$ &  69 &  2   &   s  &  dust  & L &5, 5 \cr
MRK\,766        &1 &  67 &  31 &  32  &   --  &    ---   & S &2, 5\cr
NGC\,4388       &2 & $-89$ &  70 &  21  &   n  &  dust  & L &2, 5 \cr
MGC\,-04-31-030 &2 &  58 &  62 &  84  &   n  &  dust  & L &5, 5  \cr
MGC\,-03-34-064 &2 &  48 &  46 &  39  &   --  &    ---   & L &5, 5 \cr
ESO\,383-g18    &2 &  88 &  63 &  178 &   --  &    ---   & S &5, 5\cr
IRAS\,14082+1347&2 & $-85$ &  47 &  99  &   n  &  dust  & S &5, 5 \cr
NGC\,5506       &2 & $-89$ &  76 &  70  &   s  &  dust  & L &5, 5 \cr
IRAS\,14317-3237&2 &   3 &  41 &  169 &   --  &    ---   & L &5, 5\cr
UGC\,9944       &2 &  $-7$ &  71 &  67  &   w  &  rot   & L &5, 5 \cr
PKS\,2048-57    &2 & $-60$ &  32 &  $-65$ &   sw &  dust  & L &6, 5 \cr
AKN\,564        &1 & $-73$ &  37 &  6   &   --  &    ---   & L &5, 5 \cr
NGC\,7674       &2 & $-26$ &  43 &  117 &   sw &  rot   & L &7, 5 \cr
NGC\,1386       &2 &  25 &  68 &  170 &   nw &  dust  & S &2, 5 \cr
MGC\,+8-11-11   &1 &  33 &  16 &  128 &   --  &    ---   & L &5, 11  \cr
NGC\,4941       &2 &  17 &  61 &  $-25$ &   e  &  rot   & L &5, 5\cr
MRK\,176        &2 &  59 &  70 &  92  &   --  &    ---   & S &5, 5  interact\cr
NGC\,5548       &1 & $-80$ &  33 &  168 &   --  &    ---   & L &2, 5  interact\cr
NGC\,7212       &2 &  -- &  -- &  $-7$  &  --  &   ---   & L &8, -  interact\cr
\tablenotetext{}{Column 7 indicates the kind of measurement used to
determine the closer side of the galaxy: dust lane (dust) or rotation
curve (rot). Column~8 shows the morphology of the extended radio emission,
L~(linear), S~(slightly resolved), D~(difuse).
Column~9 shows the references from which we obtained the
values of PA$_{RAD}$ and PA$_{MA}$, respectively. The galaxies
MRK\,176, NGC\,5548 and NGC\,7212 are show in this table because they
have extended radio emission, but they are not used in the analysis,
because they are interacting systems.  Sources of radio data (PA$_{RAD}$):
(1)~Ulvestad et~al.\ (1999);
(2)~Nagar et~al.\ (1999);
(3)~Ulvestad \& Wilson (1984)b;
(4)~Gallimore, Baum \& O'Dea (1996);
(5)~our measurements;
(6)~Morganti et~al.\ (1999);
(7)~Kukula et~al.\ (1995);
(8)~Falcke, Wilson \& Sipmson (1998);
Sources of optical data (PA$_{MA}$, i):
(9)~Simkin et~al.\ (1987);
(10)~Brinks \& Mundell (1996);
(11)~Canzian (1998).
}
\enddata
\end{deluxetable}

\clearpage
\newpage

\begin{deluxetable}{lcrrrcccc}
\tablewidth{0pc}
\tablecaption{Measurements for Galaxies in the Serendipitous Sample}
\tablehead{\colhead{Name}&\colhead{Type}&\colhead{PA$_{MA}$}&
\colhead{ellipticity}&\colhead{PA$_{RAD}$}&\colhead{closer}&
\colhead{source}&\colhead{Radio}&\colhead{references}\cr
&&&&&side&side&Morphology&}
\startdata
ngc513    & 2 &     69  & 55 &  167 &   --  &---   & S+D &1,13\cr
ngc591    & 2 &     5   & 33 & $-28$  &   --  & ---   & S   &2,13\cr
mrk1066   & 2 &     90  & 54 &  134 &   sw & dust& L   &2,15\cr
ngc1365   & 1 &     42  & 45 &  125 &   nw & rot & S   &3,16\cr
mrk618    & 1 &     80  & 39 &  146 &   s  & rot & S   &4,13\cr
eso362-g8 & 2 &    $-15$  & 63 &  165 &   --  & ---   & L   &1,14\cr
ngc2110   & 2 &    161  & 42 &  10  &   w  & rot & L   &1,17\cr
ngc2273   & 2 &     62  & 50 &  96  &   --  & ---   & L   &1,14\cr
eso428-g14& 2 &    $-44$  & 49 &  129 &   ne & rot & L   &2,14\cr
mrk78     & 2 &     84  & 56 &  90  &   --  & ---   & L   &5,14\cr
ngc2622   & 2 &     52  & 48 &  155 &   --  & ---   & S   &6,14\cr
ngc2639   & 2 &    $-43$  & 53 &  100 &   ne & dust& L   &7,14\cr
ngc3227   & 1 &     158 & 54 &  173 &   e  & rot & S   &8,18\cr
mrk34     & 2 &     65  & 30 &  158 &   --  & ---   & L   &5,14\cr
ngc4051   & 1 &     132 & 39 &  81  &   sw & rot & L+D &5,19\cr
ngc4117   & 2 &     18  & 60 &  177 &   e  & dust& L   &1,15\cr
ngc4151   & 1 &     26  & 21 &  77  &   e  & rot & L   &8,20\cr
eso323-g77& 1 &     155 & 60 &  35  &   ne & dust& L   &1,15\cr
ngc5135   & 2 &     15  & 34 &  25  &   w  & rot & A   &7,14\cr
ngc5252   & 2 &     15  & 59 & $-10$  &   --  & ---   & L   &8,14\cr
mrk268    & 2 &    $-67$  & 54 &  70  &   --  & ---   & S   &5,14\cr
mrk270    & 2 &    $-60$  & 30 &  48  &   s  & dust& L   &5,14\cr
ngc5273   & 1 &     11  & 32 &  5   &   w  & dust& S   &1,14\cr
ic4329a   & 1 &     44  & 58 &  97  &   se & dust& L   &1,14\cr
mrk279    & 1 &     33  & 57 &  90  &   --  & ---   & S   &4,14\cr
ngc5643   & 2 &     136 & 23 &  87  &   sw & rot & L   &9,9\cr
ngc5728   & 2 &     2   & 51 &  127 &   e  & rot & L   &10,10\cr
mrk509    & 1 &     75  & 35 &  110 &   --  & ---   & S   &4,13\cr
ngc7172   & 2 &     100 & 56 &  90  &   n  & dust& S   &11,15\cr
ic5169    & 2 &     24  & 72 &  16  &   --  & ---   & L   &1,13\cr
ngc7450   & 1 &     25  & 47 &  100 &   --  & ---   & L   &5,14\cr
ngc7465   & 2 &    $-19$  & 44 &  32  &   --  & ---   & S   &1,13\cr
mrk926    & 1 &    $-88$  & 38 &  90  &   --  & ---   & S   &4,13\cr
ngc7672   & 2 &     28  & 39 &  95  &   --  & ---   & L   &7,14\cr
ngc7743   & 2 &     86  & 38 &  21  &   --  & ---   & S   &1,13\cr
eso137-g34& 2 &    $-48$  & 40 & $-60$  &   --  & ---   & S   &12,13\cr
\tablenotetext{}{Column 7 indicates the kind of measurement used to
determine the closer side of the galaxy: dust lane (dust) or rotation
curve (rot). Column~8 shows the morphology of the
extended radio emission, L~(linear), S~(slightly resolved), D~(difuse)
and A~(amorphous). Column~9 gives the references
from which we obtained PA$_{RAD}$ and PA$_{MA}$, respectively.
Sources of PA$_{RAD}$:
(1)~Nagar et~al.\ 1999;
(2)~Bower et~al.\ 1995;
(3)~Sandqvist, Joersaeter \& Lindblad 1995;
(4)~Ulvestad \& Wilson 1984a;
(5)~Ulvestad \& Wilson 1984b;
(6)~Ulvestad 1986;
(7)~Ulvestad \& Wilson 1989;
(8)~Kukula et~al.\ 1995;
(9)~Morris et~al.\ 1985;
(10)~Schommer et~al.\ 1988;
(11)~Unger et~al.\ 1987;
(12)~Morganti et~al.\ 1999;
Sources of PA$_{MA}$:
(13)~Our measurements on DSS images;
(14)~Our measurements on our images;
(15)~RC3;
(16)~Ondrechen \& van der Hulst 1989;
(17)~Wilson \& Baldwin 1985;
(18)~Mundell et~al.\ 1995;
(19)~Lizst \& Dickey 1995;
(20)~Simkin 1975.}
\enddata
\end{deluxetable}

\clearpage
\newpage

\begin{deluxetable}{llc}
\tablewidth{0pc}
\tablecaption{Definition of the Angles Used in the Models}
\tablehead{\colhead{Angle}&\colhead{Definition}&\colhead{Allowed Range}}
\startdata
$\beta$&angle between the radio jet and the galaxy disk axis& \llap{0$^{\circ}$}--\rlap{$90^{\circ}$}\cr
$\phi$ &angle between the radio jet and line of sight&\llap{$-180^{\circ}$}--\rlap{$180^{\circ}$}\cr
$\delta$&difference between the PA of the radio jet and the PA of the galaxy major axis
&\llap{ 0$^{\circ}$}--\rlap{$90^{\circ}$}\cr
$i$    & inclination of the galaxy relative to the line of sight& \llap{0$^{\circ}$}--\rlap{$90^{\circ}$}\cr
$\theta$& azimuthal angle of the radio jet&\llap{0$^{\circ}$}--\rlap{$360^{\circ}$}\cr
$\beta_{min}$& minimum value $\beta$ can have, for a given pair ($i$,$\delta$)&---\cr
$\beta_1$& minimum value $\beta$ can have in the models &$<\beta_2$\cr
$\beta_2$& maximum value $\beta$ can have in the models &$>$sup$\beta_{min}$\tablenotemark{a}\cr
$\phi_c$ & maximum value of $\phi$ for a galaxy to be recognized as a Seyfert 1&---\cr
$i_c$    & maximum value of $i$ for a galaxy to be recognized as a Seyfert 1&---\cr
\tablenotetext{a}{sup$\beta_{min}$ is the largest value of $\beta_{min}$ among the galaxies
in the sample.}
\enddata
\end{deluxetable}


\end{document}
\end