1 Comparison of the 20cm map with an H{alpha} mage of the galaxy reveals no 
 1  source coincident with source {beta}.
 2 The position of each of these sources is within 1"-5" of a corresponding 
 2  source found by Turner & Ho (1994ApJ...421..122T).
 3 This emission region is associated with the central regions of NGC 3169. 
 4 This source is relatively far from the center of NGC 3627.
 5 This source is only visible at 3.6cm because of the reduced noise at that
 5  wavelength. It has a position within 4" of an H II region listed by Hodge 
 5  (1974ApJS...27..113H) (see Appendix). 
 6 This source is not visible at 20cm because of reduced noise level at 6 and
 6  3.6cm. The reduced flux at 3.6cm relative to 6cm is indicative of nonthermal
 6  emission, but this source is coincident with an H II region from Hodge 
 6  (1974ApJS...27..113H) (see Appendix). 
 7 The nonthermal spectral index for this source and the coincidence with the 
 7  central regions of NGC 3627 indicate this region may be associated with the 
 7  dynamic center for the galaxy. 
 8 The amorphous shape of this extended emission region and its positional 
 8  coincidence over several Hodge (1974ApJS...27..113H) H II regions indicate 
 8  that this source is probably one or more H II regions. 
 9 Source delta has a peak flux of only 4.5{sigma}.
10 Source eta eems to be a complex composed of several distinguishable smaller 
10  sources. The flux and position listed are for the strongest source. 
11 This source was not visible at 20cm because of increased noise at that 
11 wavelength. 
12 The spectral index for this source, +0.6, is very similar to those of 
12  background radio galaxies and/or quasars found in Donnelly, Partridge, & 
12  Windhorst (1987ApJ...321...94D). 
13 The spectral index for this source, +0.4, is also similar to background 
13  radio galaxies and/or quasars in Donnelly et al. (1987ApJ...321...94D).
14 This source is also extended and has an amorphous shape. Perhaps it is 
14  actually several sources. 
15 The source detected here is resolved at both wavelengths. The integrated 
15  fluxes are 6060 and 380mJy at 6 and 2cm, respectively. The resulting scaled 
15  array spectral index is -2.5. 
16 This source has a position that is within the uncertainties for an H II 
16  region found by Hodge et al., 1990, Cat. <J/ApJS/73/661>. We list our source
16  and the corresponding H II region identification in Hodge et al., 1990: 
16  psi, No. 141; rho, No. 217; tetha, no. 158; epsilon, No.365; delta, No.592.
17 These sources did not have a signal above 4{sigma} at 3.6cm. 
18 This source is coincident with the position of NGC 5455, an H II region. 
18  While alpha is 3.6" outside of the uncertainty (+/-10") of a source 
18  (No. 416) reported to be associated with NGC 5455 in Hodge et al., 1990,
18  Cat. <J/ApJS/73/661>, our source has an extended structure (see Fig. 8) 
18  that makes the identification likely. 
19 The flat spectral index ({alpha}^20^_3.6_=-0.052) indicates probable 
19  identification as an H II region. 
20 The flat spectral index for this source {alpha}^20^_3.6_=+0.026) indicates 
20  thermal emission characteristic of H II regions. 
21 These sources have positions within the uncertainties for H II regions found 
21  by Hodge et al., 1990, Cat. <J/ApJS/73/661>. 
22 Superposition of the radio map of NGC 5461 and 5462 with H{alpha} maps in 
22  Israel et al. (1975A&A....40..421I) has these sources lying over H{alpha} 
22  emission regions. 
23 This source was observed by the FIRST survey at the VLA at 21.4cm and is 
23  somewhat amorphous. The flux reported by FIRST is about 2.5 times larger 
23  than our peak flux. 
24 Also observed in the FIRST survey, this source is extended and has a jetlike 
24  shape that points toward/away from source alpha. The peak flux observed by 
24  us is very similar to that reported by FIRST. 
31 This upper limit provided by Crane et al., 1992ApJ...390L...9C.
32 Observation was made at 3.6 cm. 
33 Brown & Marscher (1978ApJ...220..467B) report radio observations of these 
33  SNe resulting in upper limits to detection.
34 The upper limits from observations of these SNe are quoted from Cowan & 
34  Branch (1982ApJ...258...31C) and Branch & Cowan (1985ApJ...297L..33B) since 
34  a map was unavailable for independent analysis. 
35 There is some discrepancy with the NED-reported position for SN 1921C and 
35  the astrometric position reported in Branch & Cowan (1985ApJ...297L..33B).
36 There is not much evidence that the explosion associated with SN 1954J was 
36  an actual SN. 
37 It is not certain that SN 1961V was actually an SN explosion 
37  (Filippenko et al., 1995AJ....110.2261F). 
38 The 20cm upper limit for SN 1969L is quoted from Branch & Cowan 
38  (1985ApJ...297L..33B) since a map was unavailable for independent analysis. 
39 NGC 4699 is also home to SN 1948A, but its position lies outside of the field
39  of view for our map. 
40 Observation was made at 2cm.