<table><caption>**Table 48**
Derived Properties of Star Clusters in NGC 6786</caption><thead><tr><th>ID</th><th>Log(Age)</th><th>σ<sub>Age</sub></th><th>Log(M/M<sub>☉</sub>)</th><th>σ<sub>M</sub></th><th>A<sub>V</sub></th><th>σ<sub>A<sub>V</sub></sub></th></tr></thead><tbody><tr><td>1</td><td>6.78</td><td>0.49</td><td>5.48</td><td>0.39</td><td>0.90</td><td>0.35</td></tr><tr><td>2</td><td>6.74</td><td>0.56</td><td>5.97</td><td>0.43</td><td>0.80</td><td>0.40</td></tr><tr><td>3</td><td>6.22</td><td>0.67</td><td>5.41</td><td>0.50</td><td>1.70</td><td>0.48</td></tr><tr><td>4</td><td>6.74</td><td>0.55</td><td>4.84</td><td>0.38</td><td>0.90</td><td>0.33</td></tr><tr><td>5</td><td>8.41</td><td>0.07</td><td>6.64</td><td>0.23</td><td>0.01</td><td>0.13</td></tr><tr><td>6</td><td>6.66</td><td>0.01</td><td>6.45</td><td>0.17</td><td>1.10</td><td>0.46</td></tr><tr><td>7</td><td>6.66</td><td>0.34</td><td>6.97</td><td>0.17</td><td>0.50</td><td>0.01</td></tr><tr><td>8</td><td>6.66</td><td>0.01</td><td>7.10</td><td>0.17</td><td>1.00</td><td>0.11</td></tr><tr><td>9</td><td>6.44</td><td>0.06</td><td>6.57</td><td>0.21</td><td>1.10</td><td>0.11</td></tr><tr><td>10</td><td>7.00</td><td>0.17</td><td>5.91</td><td>0.26</td><td>1.70</td><td>0.16</td></tr><tr><td>11</td><td>6.66</td><td>0.01</td><td>5.03</td><td>0.20</td><td>0.80</td><td>0.07</td></tr><tr><td>12</td><td>8.01</td><td>0.08</td><td>6.99</td><td>0.22</td><td>0.40</td><td>0.13</td></tr><tr><td>13</td><td>6.66</td><td>0.04</td><td>6.50</td><td>0.18</td><td>0.50</td><td>0.05</td></tr><tr><td>14</td><td>8.41</td><td>0.04</td><td>7.00</td><td>0.20</td><td>0.01</td><td>0.07</td></tr><tr><td>15</td><td>6.66</td><td>0.04</td><td>5.05</td><td>0.23</td><td>0.60</td><td>0.13</td></tr><tr><td>16</td><td>8.51</td><td>0.05</td><td>7.44</td><td>0.23</td><td>0.50</td><td>0.15</td></tr><tr><td>17</td><td>6.66</td><td>0.57</td><td>5.86</td><td>0.43</td><td>1.20</td><td>0.40</td></tr><tr><td>18</td><td>6.66</td><td>0.03</td><td>5.02</td><td>0.21</td><td>0.70</td><td>0.10</td></tr><tr><td>19</td><td>7.72</td><td>0.44</td><td>6.47</td><td>0.35</td><td>0.30</td><td>0.30</td></tr><tr><td>20</td><td>7.86</td><td>0.55</td><td>6.55</td><td>0.40</td><td>0.01</td><td>0.36</td></tr><tr><td>21</td><td>6.48</td><td>0.04</td><td>6.43</td><td>0.22</td><td>1.10</td><td>0.12</td></tr><tr><td>22</td><td>5.10</td><td>0.04</td><td>5.55</td><td>0.19</td><td>1.50</td><td>0.07</td></tr><tr><td>23</td><td>7.63</td><td>0.24</td><td>6.37</td><td>0.25</td><td>0.50</td><td>0.16</td></tr><tr><td>24</td><td>6.72</td><td>0.05</td><td>5.84</td><td>0.18</td><td>1.30</td><td>0.06</td></tr><tr><td>25</td><td>6.84</td><td>0.35</td><td>4.91</td><td>0.27</td><td>0.40</td><td>0.19</td></tr><tr><td>26</td><td>6.66</td><td>0.05</td><td>5.67</td><td>0.18</td><td>1.30</td><td>0.02</td></tr><tr><td>27</td><td>6.66</td><td>0.35</td><td>5.97</td><td>0.18</td><td>0.70</td><td>0.03</td></tr><tr><td>28</td><td>6.74</td><td>0.57</td><td>5.27</td><td>0.43</td><td>0.80</td><td>0.40</td></tr><tr><td>29</td><td>6.66</td><td>0.29</td><td>6.41</td><td>0.17</td><td>0.80</td><td>0.04</td></tr><tr><td>30</td><td>6.72</td><td>0.05</td><td>4.70</td><td>0.20</td><td>0.50</td><td>0.09</td></tr><tr><td>31</td><td>6.66</td><td>0.58</td><td>5.61</td><td>0.18</td><td>0.80</td><td>0.04</td></tr><tr><td>32</td><td>6.40</td><td>0.05</td><td>5.67</td><td>0.20</td><td>1.50</td><td>0.08</td></tr></tbody></table>

<table><caption>**Table 49**
Observed Properties of Star Clusters in IRAS 20351+2521</caption><thead><tr><th>ID</th><th>R.A.</th><th>Decl.</th><th>M<sub>B</sub></th><th>σ<sub>B</sub></th><th>M<sub>I</sub></th><th>σ<sub>I</sub></th><th>M<sub>FUV</sub></th><th>σ<sub>FUV</sub></th></tr></thead><tbody><tr><td>1</td><td>309.3189111</td><td>25.52810092</td><td>-11.77</td><td>0.04</td><td>-11.99</td><td>0.06</td><td>-12.96</td><td>0.25</td></tr><tr><td>2</td><td>309.3201669</td><td>25.53148902</td><td>-12.10</td><td>0.03</td><td>-12.78</td><td>0.03</td><td>-13.40</td><td>0.14</td></tr><tr><td>3</td><td>309.3204655</td><td>25.53148786</td><td>-14.20</td><td>0.01</td><td>-14.34</td><td>0.02</td><td>-15.85</td><td>0.04</td></tr><tr><td>4</td><td>309.3207482</td><td>25.52879944</td><td>-11.57</td><td>0.05</td><td>-12.24</td><td>0.05</td><td>-12.86</td><td>0.05</td></tr><tr><td>5</td><td>309.3205846</td><td>25.52701311</td><td>-12.18</td><td>0.08</td><td>-11.64</td><td>0.16</td><td>-12.50</td><td>0.26</td></tr><tr><td>6</td><td>309.3209895</td><td>25.52805392</td><td>-12.80</td><td>0.04</td><td>-14.63</td><td>0.01</td><td>-12.35</td><td>0.24</td></tr><tr><td>7</td><td>309.3213802</td><td>25.52804452</td><td>-12.92</td><td>0.03</td><td>-13.44</td><td>0.03</td><td>-13.04</td><td>0.17</td></tr><tr><td>8</td><td>309.3212834</td><td>25.52633971</td><td>-11.39</td><td>0.06</td><td>-12.12</td><td>0.06</td><td>-12.77</td><td>0.22</td></tr><tr><td>9</td><td>309.3215513</td><td>25.53117662</td><td>-11.92</td><td>0.07</td><td>-11.68</td><td>0.12</td><td>-12.49</td><td>0.16</td></tr><tr><td>10</td><td>309.3227499</td><td>25.52581676</td><td>-12.05</td><td>0.06</td><td>-12.70</td><td>0.07</td><td>-12.76</td><td>0.16</td></tr><tr><td>11</td><td>309.3227896</td><td>25.52569385</td><td>-12.91</td><td>0.02</td><td>-12.96</td><td>0.05</td><td>-13.61</td><td>0.07</td></tr><tr><td>12</td><td>309.3232605</td><td>25.52520015</td><td>-12.72</td><td>0.05</td><td>-13.34</td><td>0.06</td><td>-13.80</td><td>0.12</td></tr><tr><td>13</td><td>309.3237357</td><td>25.52539922</td><td>-11.60</td><td>0.05</td><td>-12.42</td><td>0.03</td><td>-12.26</td><td>0.22</td></tr><tr><td>14</td><td>309.3236793</td><td>25.52933194</td><td>-11.99</td><td>0.06</td><td>-12.00</td><td>0.07</td><td>-13.48</td><td>0.12</td></tr><tr><td>15</td><td>309.3256351</td><td>25.52614986</td><td>-11.60</td><td>0.08</td><td>-12.04</td><td>0.10</td><td>-12.83</td><td>0.04</td></tr><tr><td>16</td><td>309.3255973</td><td>25.526354</td><td>-12.15</td><td>0.05</td><td>-12.24</td><td>0.08</td><td>-13.38</td><td>0.06</td></tr><tr><td>17</td><td>309.3256314</td><td>25.53101137</td><td>-11.60</td><td>0.05</td><td>-14.92</td><td>0.01</td><td>-12.71</td><td>0.01</td></tr><tr><td>18</td><td>309.3256579</td><td>25.53150391</td><td>-11.02</td><td>0.08</td><td>-11.77</td><td>0.06</td><td>-13.02</td><td>0.21</td></tr><tr><td>19</td><td>309.3259664</td><td>25.52654554</td><td>-11.17</td><td>0.15</td><td>-12.53</td><td>0.06</td><td>-12.95</td><td>0.27</td></tr><tr><td>20</td><td>309.3261938</td><td>25.52631453</td><td>-13.23</td><td>0.02</td><td>-13.84</td><td>0.02</td><td>-13.45</td><td>0.16</td></tr><tr><td>21</td><td>309.3262881</td><td>25.52747562</td><td>-13.98</td><td>0.02</td><td>-14.03</td><td>0.02</td><td>-16.15</td><td>0.01</td></tr><tr><td>22</td><td>309.3262506</td><td>25.53020748</td><td>-11.03</td><td>0.05</td><td>-11.65</td><td>0.05</td><td>-13.08</td><td>0.03</td></tr></tbody></table>
<table><caption>**Table 50**
Derived Properties of Star Clusters in IRAS 20351+2521</caption><thead><tr><th>ID</th><th>Log(Age)</th><th>σ<sub>Age</sub></th><th>Log(M/M<sub>☉</sub>)</th><th>σ<sub>M</sub></th><th>A<sub>V</sub></th><th>σ<sub>A<sub>V</sub></sub></th></tr></thead><tbody><tr><td>1</td><td>6.54</td><td>0.33</td><td>5.69</td><td>0.16</td><td>1.50</td><td>0.02</td></tr><tr><td>2</td><td>6.74</td><td>0.19</td><td>5.65</td><td>0.16</td><td>1.10</td><td>0.31</td></tr><tr><td>3</td><td>6.54</td><td>0.32</td><td>6.50</td><td>0.15</td><td>1.20</td><td>0.23</td></tr><tr><td>4</td><td>7.76</td><td>0.42</td><td>5.92</td><td>0.16</td><td>0.40</td><td>0.20</td></tr><tr><td>5</td><td>6.52</td><td>0.40</td><td>6.07</td><td>0.18</td><td>1.90</td><td>0.45</td></tr><tr><td>6</td><td>6.78</td><td>0.05</td><td>6.57</td><td>0.16</td><td>2.30</td><td>0.59</td></tr><tr><td>7</td><td>8.51</td><td>0.11</td><td>6.72</td><td>0.16</td><td>0.01</td><td>0.53</td></tr><tr><td>8</td><td>7.70</td><td>0.12</td><td>5.81</td><td>0.17</td><td>0.40</td><td>0.16</td></tr><tr><td>9</td><td>6.52</td><td>0.23</td><td>5.91</td><td>0.17</td><td>1.80</td><td>0.46</td></tr><tr><td>10</td><td>8.36</td><td>0.53</td><td>6.26</td><td>0.17</td><td>0.01</td><td>0.19</td></tr><tr><td>11</td><td>6.52</td><td>0.08</td><td>6.31</td><td>0.16</td><td>1.80</td><td>0.05</td></tr><tr><td>12</td><td>6.64</td><td>0.37</td><td>6.19</td><td>0.16</td><td>1.60</td><td>0.54</td></tr><tr><td>13</td><td>7.96</td><td>0.12</td><td>6.13</td><td>0.16</td><td>0.60</td><td>0.08</td></tr><tr><td>14</td><td>6.52</td><td>0.18</td><td>5.67</td><td>0.17</td><td>1.30</td><td>0.12</td></tr><tr><td>15</td><td>6.52</td><td>0.29</td><td>5.68</td><td>0.18</td><td>1.60</td><td>0.24</td></tr><tr><td>16</td><td>6.52</td><td>0.32</td><td>5.84</td><td>0.16</td><td>1.50</td><td>0.24</td></tr><tr><td>17</td><td>8.11</td><td>0.39</td><td>6.22</td><td>0.16</td><td>0.60</td><td>0.23</td></tr><tr><td>18</td><td>6.94</td><td>0.52</td><td>5.09</td><td>0.18</td><td>0.50</td><td>0.59</td></tr><tr><td>19</td><td>7.65</td><td>0.53</td><td>5.53</td><td>0.22</td><td>0.10</td><td>0.36</td></tr><tr><td>20</td><td>6.52</td><td>0.07</td><td>6.65</td><td>0.16</td><td>2.20</td><td>0.41</td></tr><tr><td>21</td><td>6.44</td><td>0.19</td><td>6.49</td><td>0.16</td><td>1.10</td><td>0.19</td></tr><tr><td>22</td><td>7.36</td><td>0.24</td><td>5.39</td><td>0.16</td><td>0.30</td><td>0.58</td></tr></tbody></table>

<table><caption>**Table 51**
Observed Properties of Star Clusters in II Zw 096</caption><thead><tr><th>ID</th><th>R.A.</th><th>Decl.</th><th>M<sub>B</sub></th><th>σ<sub>B</sub></th><th>M<sub>I</sub></th><th>σ<sub>I</sub></th><th>M<sub>FUV</sub></th><th>σ<sub>FUV</sub></th></tr></thead><tbody><tr><td>1</td><td>314.347937</td><td>17.13209914</td><td>-14.40</td><td>0.02</td><td>-14.52</td><td>0.01</td><td>-16.48</td><td>0.01</td></tr><tr><td>2</td><td>314.3488605</td><td>17.12855532</td><td>-13.82</td><td>0.03</td><td>-14.60</td><td>0.03</td><td>-15.53</td><td>0.05</td></tr><tr><td>3</td><td>314.3490196</td><td>17.12831079</td><td>-13.91</td><td>0.02</td><td>-14.50</td><td>0.05</td><td>-15.42</td><td>0.02</td></tr><tr><td>4</td><td>314.3489006</td><td>17.12844657</td><td>-14.02</td><td>0.05</td><td>-14.14</td><td>0.07</td><td>-14.94</td><td>0.12</td></tr><tr><td>5</td><td>314.3487591</td><td>17.13097999</td><td>-13.81</td><td>0.02</td><td>-13.94</td><td>0.02</td><td>-15.86</td><td>0.01</td></tr><tr><td>6</td><td>314.3491325</td><td>17.12863715</td><td>-13.77</td><td>0.02</td><td>-14.84</td><td>0.01</td><td>-14.42</td><td>0.03</td></tr><tr><td>7</td><td>314.349413</td><td>17.12830611</td><td>-13.18</td><td>0.02</td><td>-14.06</td><td>0.02</td><td>-14.27</td><td>0.04</td></tr><tr><td>8</td><td>314.3494999</td><td>17.12879568</td><td>-14.29</td><td>0.01</td><td>-14.38</td><td>0.02</td><td>-16.21</td><td>0.01</td></tr><tr><td>9</td><td>314.3497151</td><td>17.12841414</td><td>-16.14</td><td>0.01</td><td>-16.84</td><td>0.01</td><td>-17.62</td><td>0.01</td></tr><tr><td>10</td><td>314.3501466</td><td>17.12654531</td><td>-17.92</td><td>0.01</td><td>-18.33</td><td>0.01</td><td>-19.48</td><td>0.01</td></tr><tr><td>11</td><td>314.3501115</td><td>17.12664894</td><td>-15.51</td><td>0.05</td><td>-16.26</td><td>0.05</td><td>-16.12</td><td>0.03</td></tr><tr><td>12</td><td>314.3500502</td><td>17.12680274</td><td>-13.52</td><td>0.11</td><td>-13.88</td><td>0.19</td><td>-14.82</td><td>0.07</td></tr><tr><td>13</td><td>314.3501617</td><td>17.12810109</td><td>-14.29</td><td>0.02</td><td>-14.84</td><td>0.02</td><td>-15.64</td><td>0.02</td></tr><tr><td>14</td><td>314.3504248</td><td>17.12671799</td><td>-14.41</td><td>0.10</td><td>-14.91</td><td>0.09</td><td>-15.82</td><td>0.05</td></tr><tr><td>15</td><td>314.3504765</td><td>17.12652561</td><td>-16.42</td><td>0.01</td><td>-16.64</td><td>0.02</td><td>-17.80</td><td>0.02</td></tr><tr><td>16</td><td>314.350505</td><td>17.12642631</td><td>-16.31</td><td>0.01</td><td>-16.51</td><td>0.02</td><td>-17.94</td><td>0.01</td></tr><tr><td>17</td><td>314.352852</td><td>17.12679784</td><td>-14.29</td><td>0.01</td><td>-14.06</td><td>0.03</td><td>-16.45</td><td>0.01</td></tr><tr><td>18</td><td>314.353755</td><td>17.1273767</td><td>-13.74</td><td>0.01</td><td>-13.88</td><td>0.02</td><td>-15.87</td><td>0.01</td></tr><tr><td>19</td><td>314.3538332</td><td>17.12884574</td><td>-13.71</td><td>0.01</td><td>-14.39</td><td>0.01</td><td>-15.76</td><td>0.01</td></tr><tr><td>20</td><td>314.3539789</td><td>17.12839369</td><td>-12.26</td><td>0.02</td><td>-12.92</td><td>0.02</td><td>-14.44</td><td>0.03</td></tr></tbody></table>

western component is a roughly face-on spiral galaxy with star clusters along the spiral arms. The southeast end of the spiral, approximately 11"6 (8.4 kpc) from the nucleus, contains a distinct cluster-rich region (Figure 53). The maximum $A_V$

adopted for this galaxy is 3.0 mag of visual extinction (see Figure 54; Inami et al. 2010). The observed and derived properties for the star clusters identified in this galaxy are given in Tables 51 and 52, respectively.
<table><caption>**Table 52**
Derived Properties of Star Clusters in II Zw 096</caption><thead><tr><th>ID</th><th>Log(Age)</th><th>σ<sub>Age</sub></th><th>Log(M/M<sub>☉</sub>)</th><th>σ<sub>M</sub></th><th>A<sub>V</sub></th><th>σ<sub>A<sub>V</sub></sub></th></tr></thead><tbody><tr><td>1</td><td>6.40</td><td>0.08</td><td>6.76</td><td>0.22</td><td>1.20</td><td>0.12</td></tr><tr><td>2</td><td>7.40</td><td>0.25</td><td>6.64</td><td>0.24</td><td>0.50</td><td>0.16</td></tr><tr><td>3</td><td>6.74</td><td>0.45</td><td>6.32</td><td>0.39</td><td>1.00</td><td>0.35</td></tr><tr><td>4</td><td>6.52</td><td>0.53</td><td>6.70</td><td>0.52</td><td>1.70</td><td>0.50</td></tr><tr><td>5</td><td>6.42</td><td>0.12</td><td>6.52</td><td>0.24</td><td>1.20</td><td>0.16</td></tr><tr><td>6</td><td>7.63</td><td>0.27</td><td>7.04</td><td>0.26</td><td>1.00</td><td>0.19</td></tr><tr><td>7</td><td>7.63</td><td>0.26</td><td>6.64</td><td>0.26</td><td>0.70</td><td>0.18</td></tr><tr><td>8</td><td>6.52</td><td>0.02</td><td>6.49</td><td>0.18</td><td>1.10</td><td>0.06</td></tr><tr><td>9</td><td>7.65</td><td>0.01</td><td>7.68</td><td>0.17</td><td>0.40</td><td>0.13</td></tr><tr><td>10</td><td>5.70</td><td>0.62</td><td>8.60</td><td>0.44</td><td>1.60</td><td>0.41</td></tr><tr><td>11</td><td>6.54</td><td>0.85</td><td>7.45</td><td>0.81</td><td>2.00</td><td>0.93</td></tr><tr><td>12</td><td>6.54</td><td>0.55</td><td>6.39</td><td>0.53</td><td>1.50</td><td>0.52</td></tr><tr><td>13</td><td>6.72</td><td>0.61</td><td>6.60</td><td>0.54</td><td>1.20</td><td>0.54</td></tr><tr><td>14</td><td>6.58</td><td>0.62</td><td>6.73</td><td>0.55</td><td>1.40</td><td>0.55</td></tr><tr><td>15</td><td>6.54</td><td>0.01</td><td>7.50</td><td>0.17</td><td>1.40</td><td>0.03</td></tr><tr><td>16</td><td>6.52</td><td>0.01</td><td>7.40</td><td>0.18</td><td>1.30</td><td>0.04</td></tr><tr><td>17</td><td>6.54</td><td>0.01</td><td>6.33</td><td>0.18</td><td>0.80</td><td>0.05</td></tr><tr><td>18</td><td>5.70</td><td>0.41</td><td>6.71</td><td>0.27</td><td>1.20</td><td>0.20</td></tr><tr><td>19</td><td>6.78</td><td>0.07</td><td>5.98</td><td>0.17</td><td>0.50</td><td>0.02</td></tr><tr><td>20</td><td>6.96</td><td>0.15</td><td>5.57</td><td>0.18</td><td>0.40</td><td>0.06</td></tr></tbody></table>

<table><caption>**Table 53**
Observed Properties of Star Clusters in ESO 148-IG002</caption><thead><tr><th>ID</th><th>R.A.</th><th>Decl.</th><th>M<sub>B</sub></th><th>σ<sub>B</sub></th><th>M<sub>I</sub></th><th>σ<sub>I</sub></th><th>M<sub>FUV</sub></th><th>σ<sub>FUV</sub></th></tr></thead><tbody><tr><td>1</td><td>348.9465405</td><td>-59.05411541</td><td>-14.15</td><td>0.01</td><td>-14.90</td><td>0.01</td><td>-14.43</td><td>0.03</td></tr><tr><td>2</td><td>348.9468576</td><td>-59.0539657</td><td>-13.60</td><td>0.02</td><td>-14.73</td><td>0.02</td><td>-13.26</td><td>0.10</td></tr><tr><td>3</td><td>348.9462256</td><td>-59.05361789</td><td>-12.73</td><td>0.03</td><td>-13.39</td><td>0.04</td><td>-12.63</td><td>0.18</td></tr><tr><td>4</td><td>348.9469037</td><td>-59.05365887</td><td>-11.95</td><td>0.09</td><td>-13.24</td><td>0.08</td><td>-12.87</td><td>0.14</td></tr><tr><td>5</td><td>348.9454074</td><td>-59.05331294</td><td>-13.54</td><td>0.15</td><td>-14.19</td><td>0.09</td><td>-14.48</td><td>0.06</td></tr><tr><td>6</td><td>348.9468404</td><td>-59.05307144</td><td>-14.27</td><td>0.02</td><td>-15.05</td><td>0.01</td><td>-14.84</td><td>0.02</td></tr><tr><td>7</td><td>348.9456965</td><td>-59.05497655</td><td>-14.45</td><td>0.04</td><td>-15.22</td><td>0.03</td><td>-14.50</td><td>0.06</td></tr></tbody></table>

<table><caption>**Table 54**
Derived Properties of Star Clusters in ESO 148-IG002</caption><thead><tr><th>ID</th><th>Log(Age)</th><th>σ<sub>Age</sub></th><th>Log(M/M<sub>☉</sub>)</th><th>σ<sub>M</sub></th><th>A<sub>V</sub></th><th>σ<sub>A<sub>V</sub></sub></th></tr></thead><tbody><tr><td>1</td><td>8.46</td><td>0.03</td><td>7.17</td><td>0.16</td><td>0.01</td><td>0.78</td></tr><tr><td>2</td><td>8.41</td><td>0.40</td><td>7.23</td><td>0.45</td><td>0.60</td><td>0.43</td></tr><tr><td>3</td><td>8.61</td><td>0.06</td><td>6.73</td><td>0.17</td><td>0.01</td><td>0.02</td></tr><tr><td>4</td><td>7.65</td><td>0.25</td><td>6.21</td><td>0.24</td><td>0.80</td><td>0.14</td></tr><tr><td>5</td><td>8.26</td><td>0.79</td><td>6.80</td><td>0.69</td><td>0.01</td><td>0.73</td></tr><tr><td>6</td><td>6.48</td><td>0.90</td><td>7.13</td><td>0.84</td><td>2.20</td><td>0.97</td></tr><tr><td>7</td><td>8.56</td><td>0.04</td><td>7.38</td><td>0.17</td><td>0.01</td><td>0.04</td></tr></tbody></table>

### ESO 148-IG002

ESO 148-IG002 is a late-stage merger with a projected nuclear separation of ~4.7" (4.2 kpc). The galaxy has a series of bright clusters which lie along a north-south ridge to the east of the bulge (Figure 55). The maximum $A_V$ adopted for this galaxy is 2.5 mag of visual extinction (see Figure 56; Johansson & Bergvall 1988). The observed and derived properties for the star clusters identified in this galaxy are given in Tables 53 and 54, respectively.

### NGC 7674

NGC 7674 is an early-stage merger with a face-on spiral galaxy and companions to the northeast and southeast. Star clusters are visible along the prominent spiral arms throughout the galaxy (Figure 57). The maximum $A_V$ adopted for this galaxy is 2.0 mag of visual extinction (see Figure 58; Momjian et al. 2003). The observed and derived properties for the star clusters identified in this galaxy are given in Tables 55 and 56, respectively.
<table><caption>**Table 55**
Observed Properties of Star Clusters in NGC 7674</caption><thead><tr><th>ID</th><th>R.A.</th><th>Decl.</th><th>M<sub>B</sub></th><th>σ<sub>B</sub></th><th>M<sub>I</sub></th><th>σ<sub>I</sub></th><th>M<sub>FUV</sub></th><th>σ<sub>FUV</sub></th></tr></thead><tbody><tr><td>1</td><td>351.9831239</td><td>8.778349264</td><td>-12.20</td><td>0.02</td><td>-12.57</td><td>0.03</td><td>-14.06</td><td>0.02</td></tr><tr><td>2</td><td>351.9849596</td><td>8.772096618</td><td>-11.55</td><td>0.02</td><td>-11.73</td><td>0.04</td><td>-13.17</td><td>0.05</td></tr><tr><td>3</td><td>351.9850026</td><td>8.772116709</td><td>-11.44</td><td>0.02</td><td>-11.76</td><td>0.03</td><td>-12.79</td><td>0.08</td></tr><tr><td>4</td><td>351.9832985</td><td>8.779441129</td><td>-10.77</td><td>0.11</td><td>-11.11</td><td>0.13</td><td>-13.04</td><td>0.06</td></tr><tr><td>5</td><td>351.9830552</td><td>8.780545473</td><td>-10.91</td><td>0.03</td><td>-11.08</td><td>0.05</td><td>-12.85</td><td>0.04</td></tr><tr><td>6</td><td>351.9840117</td><td>8.778513551</td><td>-12.29</td><td>0.04</td><td>-12.74</td><td>0.03</td><td>-13.63</td><td>0.04</td></tr><tr><td>7</td><td>351.9849762</td><td>8.780046055</td><td>-12.87</td><td>0.02</td><td>-12.92</td><td>0.03</td><td>-15.07</td><td>0.02</td></tr><tr><td>8</td><td>351.9855017</td><td>8.779670342</td><td>-12.42</td><td>0.04</td><td>-12.61</td><td>0.09</td><td>-13.89</td><td>0.06</td></tr><tr><td>9</td><td>351.9862949</td><td>8.779049017</td><td>-17.60</td><td>0.01</td><td>-18.76</td><td>0.01</td><td>-19.06</td><td>0.01</td></tr><tr><td>10</td><td>351.9882912</td><td>8.773938539</td><td>-12.62</td><td>0.01</td><td>-13.32</td><td>0.01</td><td>-14.50</td><td>0.02</td></tr><tr><td>11</td><td>351.9885463</td><td>8.773640234</td><td>-11.47</td><td>0.03</td><td>-12.12</td><td>0.05</td><td>-13.84</td><td>0.03</td></tr><tr><td>12</td><td>351.9857724</td><td>8.780029971</td><td>-11.03</td><td>0.05</td><td>-10.37</td><td>0.20</td><td>-12.96</td><td>0.07</td></tr><tr><td>13</td><td>351.9869669</td><td>8.777906039</td><td>-11.45</td><td>0.04</td><td>-11.50</td><td>0.06</td><td>-12.83</td><td>0.05</td></tr><tr><td>14</td><td>351.9868119</td><td>8.778402264</td><td>-13.02</td><td>0.01</td><td>-13.05</td><td>0.03</td><td>-14.91</td><td>0.01</td></tr><tr><td>15</td><td>351.9875291</td><td>8.777102907</td><td>-13.70</td><td>0.03</td><td>-13.66</td><td>0.03</td><td>-15.37</td><td>0.02</td></tr><tr><td>16</td><td>351.9886887</td><td>8.774122684</td><td>-11.76</td><td>0.03</td><td>-11.76</td><td>0.06</td><td>-14.04</td><td>0.05</td></tr><tr><td>17</td><td>351.9874886</td><td>8.7769875</td><td>-11.39</td><td>0.19</td><td>-12.26</td><td>0.16</td><td>-14.14</td><td>0.04</td></tr><tr><td>18</td><td>351.9864376</td><td>8.77992672</td><td>-11.09</td><td>0.04</td><td>-11.46</td><td>0.07</td><td>-13.01</td><td>0.06</td></tr><tr><td>19</td><td>351.9873013</td><td>8.778022066</td><td>-10.96</td><td>0.06</td><td>-11.33</td><td>0.13</td><td>-12.90</td><td>0.07</td></tr><tr><td>20</td><td>351.9867238</td><td>8.779687958</td><td>-12.50</td><td>0.03</td><td>-12.67</td><td>0.04</td><td>-14.62</td><td>0.01</td></tr><tr><td>21</td><td>351.9877438</td><td>8.778029429</td><td>-12.90</td><td>0.02</td><td>-13.24</td><td>0.04</td><td>-14.16</td><td>0.02</td></tr><tr><td>22</td><td>351.988047</td><td>8.779603842</td><td>-10.36</td><td>0.13</td><td>-11.65</td><td>0.09</td><td>-13.07</td><td>0.03</td></tr><tr><td>23</td><td>351.9895457</td><td>8.777038636</td><td>-10.67</td><td>0.05</td><td>-10.77</td><td>0.09</td><td>-12.88</td><td>0.07</td></tr><tr><td>24</td><td>351.9886045</td><td>8.779833873</td><td>-12.05</td><td>0.03</td><td>-12.33</td><td>0.05</td><td>-13.70</td><td>0.03</td></tr><tr><td>25</td><td>351.9823723</td><td>8.778916581</td><td>-11.27</td><td>0.03</td><td>-11.67</td><td>0.04</td><td>-12.86</td><td>0.07</td></tr></tbody></table>

<table><caption>**Table 56**
Derived Properties of Star Clusters in NGC 7674</caption><thead><tr><th>ID</th><th>Log(Age)</th><th>σ<sub>Age</sub></th><th>Log(M/M<sub>☉</sub>)</th><th>σ<sub>M</sub></th><th>A<sub>V</sub></th><th>σ<sub>A<sub>V</sub></sub></th></tr></thead><tbody><tr><td>1</td><td>6.74</td><td>0.03</td><td>5.48</td><td>0.21</td><td>0.70</td><td>0.11</td></tr><tr><td>2</td><td>6.52</td><td>0.02</td><td>5.50</td><td>0.19</td><td>1.30</td><td>0.07</td></tr><tr><td>3</td><td>6.52</td><td>0.03</td><td>5.56</td><td>0.19</td><td>1.50</td><td>0.08</td></tr><tr><td>4</td><td>6.72</td><td>0.28</td><td>4.87</td><td>0.27</td><td>0.60</td><td>0.17</td></tr><tr><td>5</td><td>6.52</td><td>0.08</td><td>5.14</td><td>0.22</td><td>1.10</td><td>0.13</td></tr><tr><td>6</td><td>6.44</td><td>0.10</td><td>6.14</td><td>0.24</td><td>1.70</td><td>0.16</td></tr><tr><td>7</td><td>6.42</td><td>0.10</td><td>6.09</td><td>0.22</td><td>1.10</td><td>0.14</td></tr><tr><td>8</td><td>6.52</td><td>0.05</td><td>5.90</td><td>0.20</td><td>1.40</td><td>0.09</td></tr><tr><td>9</td><td>6.80</td><td>0.03</td><td>7.78</td><td>0.17</td><td>0.90</td><td>0.03</td></tr><tr><td>10</td><td>7.00</td><td>0.07</td><td>5.97</td><td>0.17</td><td>0.70</td><td>0.04</td></tr><tr><td>11</td><td>7.00</td><td>0.10</td><td>5.46</td><td>0.17</td><td>0.60</td><td>1.12</td></tr><tr><td>12</td><td>6.52</td><td>0.01</td><td>5.08</td><td>0.20</td><td>0.90</td><td>0.09</td></tr><tr><td>13</td><td>6.52</td><td>0.01</td><td>5.51</td><td>0.18</td><td>1.40</td><td>0.04</td></tr><tr><td>14</td><td>6.52</td><td>0.01</td><td>5.98</td><td>0.17</td><td>1.10</td><td>0.03</td></tr><tr><td>15</td><td>6.52</td><td>0.01</td><td>6.31</td><td>0.17</td><td>1.20</td><td>0.03</td></tr><tr><td>16</td><td>6.50</td><td>0.08</td><td>5.39</td><td>0.22</td><td>0.90</td><td>0.13</td></tr><tr><td>17</td><td>7.00</td><td>0.43</td><td>5.43</td><td>0.27</td><td>0.60</td><td>0.06</td></tr><tr><td>18</td><td>6.74</td><td>0.18</td><td>5.04</td><td>0.27</td><td>0.70</td><td>0.20</td></tr><tr><td>19</td><td>6.74</td><td>0.19</td><td>4.98</td><td>0.29</td><td>0.70</td><td>0.22</td></tr><tr><td>20</td><td>6.58</td><td>0.27</td><td>5.70</td><td>0.27</td><td>0.90</td><td>0.20</td></tr><tr><td>21</td><td>6.54</td><td>0.01</td><td>6.14</td><td>0.18</td><td>1.50</td><td>0.05</td></tr><tr><td>22</td><td>6.82</td><td>0.10</td><td>4.76</td><td>0.22</td><td>0.60</td><td>1.12</td></tr><tr><td>23</td><td>6.68</td><td>0.11</td><td>4.90</td><td>0.24</td><td>0.70</td><td>0.16</td></tr><tr><td>24</td><td>6.52</td><td>0.28</td><td>5.70</td><td>0.24</td><td>1.30</td><td>0.16</td></tr><tr><td>25</td><td>6.66</td><td>0.30</td><td>5.41</td><td>0.30</td><td>1.20</td><td>0.23</td></tr></tbody></table>
<figure><img src="image_9.png" /><figcaption>**Figure 7.** Inverted black and white *B*-*I* image of NGC 0017 taken with *HST* ACS/WFC F814W and F435W. The bright emission corresponds to redder (i.e., dustier) regions of the galaxy. The blue centroids correspond to clusters found in relatively “dust-free” regions of these galaxies, whereas the green centroids correspond to clusters found in relatively dustier regions of the galaxy.</figcaption></figure>

<figure><img src="image_10.png" /><figcaption>**Figure 9.** Inverted black and white *B*-*I* image of Arp 256S taken with *HST* ACS/WFC F814W and F435W. The bright emission corresponds to redder (i.e., dustier) regions of the galaxy. The blue centroids correspond to clusters found in relatively “dust-free” regions of these galaxies, whereas the green centroids correspond to clusters found in relatively dustier regions of the galaxy.</figcaption></figure>

<figure><img src="image_11.png" /><figcaption>**Figure 8.** Color-color plot of all star clusters identified in NGC 0017 in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 7.</figcaption></figure>

<figure><img src="image_12.png" /><figcaption>**Figure 10.** Color-color plot of all star clusters identified in Arp 256S in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 9.</figcaption></figure>
<figure><img src="image_13.png" /><figcaption>**Figure 11.** Inverted black and white *B*–*I* image of Arp 256N taken with HST ACS/WFC F814W and F435W. The bright emission corresponds to redder (i.e., dustier) regions of the galaxy. The blue centroids correspond to clusters found in relatively “dust-free” regions of these galaxies, whereas the green centroids correspond to clusters found in relatively dustier regions of the galaxy.</figcaption></figure>

<figure><img src="image_14.png" /><figcaption>**Figure 13.** Inverted black and white *B*–*I* image of NGC 0695 taken with HST ACS/WFC F814W and F435W. The bright emission corresponds to redder (i.e., dustier) regions of the galaxy. The blue centroids correspond to clusters found in relatively “dust-free” regions of these galaxies, whereas the green centroids correspond to clusters found in relatively dustier regions of the galaxy.</figcaption></figure>

<figure><img src="image_15.png" /><figcaption>**Figure 12.** Color–color plot of all star clusters identified in Arp 256N in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 11.</figcaption></figure>

<figure><img src="image_16.png" /><figcaption>**Figure 14.** Color–color plot of all star clusters identified in NGC 0695 in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 13.</figcaption></figure>
<figure><img src="image_17.png" /><figcaption>**Figure 15.** Inverted black and white *B*-*I* image of UGC 02369 taken with HST ACS/WFC F814W and F435W. The bright emission corresponds to redder (i.e., dustier) regions of the galaxy. The blue centroids correspond to clusters found in relatively “dust-free” regions of these galaxies, whereas the green centroids correspond to clusters found in relatively dustier regions of the galaxy.</figcaption></figure>

<figure><img src="image_18.png" /><figcaption>**Figure 17.** Inverted black and white *B*-*I* image of NGC 1614 taken with HST ACS/WFC F814W and F435W. The bright emission corresponds to redder (i.e., dustier) regions of the galaxy. The blue centroids correspond to clusters found in relatively “dust-free” regions of these galaxies, whereas the green centroids correspond to clusters found in relatively dustier regions of the galaxy.</figcaption></figure>

<figure><img src="image_19.png" /><figcaption>**Figure 16.** Color-color plot of all star clusters identified in UGC 02369 in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 15.</figcaption></figure>

<figure><img src="image_20.png" /><figcaption>**Figure 18.** Color-color plot of all star clusters identified in NGC 1614 in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 17.</figcaption></figure>
<figure><img src="image_21.png" /><figcaption>**Figure 19.** Inverted black and white *B*-*I* image of 2MASX J06094582-2140234 taken with HST ACS/WFC F814W and F435W. The bright emission corresponds to redder (i.e., dustier) regions of the galaxy. The blue centroids correspond to clusters found in relatively “dust-free” regions of these galaxies, whereas the green centroids correspond to clusters found in relatively dustier regions of the galaxy.</figcaption></figure>

<figure><img src="image_22.png" /><figcaption>**Figure 21.** Inverted black and white *B*-*I* image of 2MASX J08370182-4954302 taken with HST ACS/WFC F814W and F435W. The bright emission corresponds to redder (i.e., dustier) regions of the galaxy. The blue centroids correspond to clusters found in relatively “dust-free” regions of these galaxies, whereas the green centroids correspond to clusters found in relatively dustier regions of the galaxy.</figcaption></figure>

<figure><img src="image_23.png" /><figcaption>**Figure 20.** Color-color plot of all star clusters identified in 2MASX J06094582-2140234 in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 19.</figcaption></figure>

<figure><img src="image_24.png" /><figcaption>**Figure 22.** Color-color plot of all star clusters identified in 2MASX J08370182-4954302 in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 21.</figcaption></figure>
<figure><img src="image_25.png" /></figure>

**Figure 23.** Inverted black and white *B*-*I* image taken of NGC 2623 with HST ACS/WFC F814W and F435W. The bright emission corresponds to redder (i.e., dustier) regions of the galaxy. The blue centroids correspond to clusters found in relatively “dust-free” regions of these galaxies, whereas the green centroids correspond to clusters found in relatively dustier regions of the galaxy.

<figure><img src="image_26.png" /></figure>

**Figure 25.** Inverted black and white *B*-*I* image of UGC 04881 taken with HST ACS/WFC F814W and F435W. The bright emission corresponds to redder (i.e., dustier) regions of the galaxy. The blue centroids correspond to clusters found in relatively “dust-free” regions of these galaxies, whereas the green centroids correspond to clusters found in relatively dustier regions of the galaxy.

<figure><img src="image_27.png" /></figure>

**Figure 24.** Color-color plot of all star clusters identified in NGC 2623 in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 23.

<figure><img src="image_28.png" /></figure>

**Figure 26.** Color-color plot of all star clusters identified in UGC 04881 in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 25.
<figure><img src="image_29.png" /></figure>

**Figure 27.** Inverted black and white *B*-*I* image of IC 2545 taken with HST ACS/WFC F814W and F435W. The bright emission corresponds to redder (i.e., dustier) regions of the galaxy. The blue centroids correspond to clusters found in relatively “dust-free” regions of these galaxies, whereas the green centroids correspond to clusters found in relatively dustier regions of the galaxy.

<figure><img src="image_30.png" /></figure>

**Figure 29.** Inverted black and white *B*-*I* image of NGC 3256 taken with HST ACS/WFC F814W and F435W. The bright emission corresponds to redder (i.e., dustier) regions of the galaxy. The blue centroids correspond to clusters found in relatively “dust-free” regions of these galaxies, whereas the green centroids correspond to clusters found in relatively dustier regions of the galaxy.

<figure><img src="image_31.png" /></figure>

**Figure 28.** Color-color plot of all star clusters identified in IC 2545 in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 27.

<figure><img src="image_32.png" /></figure>

**Figure 30.** Color-color plot of all star clusters identified in NGC 3256 in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 29.
<figure><img src="image_33.png" /><figcaption>**Figure 31.** Inverted black and white *B*-*I* image of Arp 148 taken with HST ACS/WFC F814W and F435W. The bright emission corresponds to redder (i.e., dustier) regions of the galaxy. The blue centroids correspond to clusters found in relatively “dust-free” regions of these galaxies, whereas the green centroids correspond to clusters found in relatively dustier regions of the galaxy.</figcaption></figure>

<figure><img src="image_34.png" /><figcaption>**Figure 33.** Inverted black and white *B*-*I* image of NGC 3690E/W taken with HST ACS/WFC F814W and F435W. The bright emission corresponds to redder (i.e., dustier) regions of the galaxy. The blue centroids correspond to clusters found in relatively “dust-free” regions of these galaxies, whereas the green centroids correspond to clusters found in relatively dustier regions of the galaxy.</figcaption></figure>

<figure><img src="image_35.png" /><figcaption>**Figure 32.** Color–color plot of all star clusters identified in Arp 148 in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 31.</figcaption></figure>

<figure><img src="image_36.png" /><figcaption>**Figure 34.** Color–color plot of all star clusters identified in NGC 3690E in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 33.</figcaption></figure>
NGC3690 Color-Color Plot

<figure><img src="image_37.png" /><figcaption>**Figure 35.** Color-color plot of all star clusters identified in NGC 3690W in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 33.</figcaption></figure>

NGC5257 Color-Color Plot

<figure><img src="image_38.png" /><figcaption>**Figure 37.** Color-color plot of all star clusters identified in NGC 5257E F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 36.</figcaption></figure>

<figure><img src="image_39.png" /><figcaption>**Figure 36.** Inverted black and white *B*-*I* image of NGC 5257E taken with *HST* ACS/WFC F814W and F435W. The bright emission corresponds to redder (i.e., dustier) regions of the galaxy. The blue centroids correspond to clusters found in relatively “dust-free” regions of these galaxies, whereas the green centroids correspond to clusters found in relatively dustier regions of the galaxy.</figcaption></figure>

<figure><img src="image_40.png" /><figcaption>**Figure 38.** Inverted black and white *B*-*I* image of NGC 5257W taken with *HST* ACS/WFC F814W and F435W. The bright emission corresponds to redder (i.e., dustier) regions of the galaxy. The blue centroids correspond to clusters found in relatively “dust-free” regions of these galaxies, whereas the green centroids correspond to clusters found in relatively dustier regions of the galaxy.</figcaption></figure>
<figure><img src="image_41.png" /><figcaption>**Figure 39.** Color-color plot of all star clusters identified in NGC 5257W in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 38.</figcaption></figure>

<figure><img src="image_42.png" /><figcaption>**Figure 40.** Inverted black and white B-I image of NGC 5331N/S taken with HST ACS/WFC F814W and F435W. The bright emission corresponds to redder (i.e., dustier) regions of the galaxy. The blue centroids correspond to clusters found in relatively “dust-free” regions of these galaxies, whereas the green centroids correspond to clusters found in relatively dustier regions of the galaxy.</figcaption></figure>

<figure><img src="image_43.png" /><figcaption>**Figure 41.** Color-color plot of all star clusters identified in NGC 5331S in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 40.</figcaption></figure>

<figure><img src="image_44.png" /><figcaption>**Figure 42.** Color-color plot of all star clusters identified in NGC 5331N in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 40.</figcaption></figure>
<figure><img src="image_45.png" /><figcaption>**Figure 43.** Inverted black and white *B*-*I* image of UGC 09618NED02 taken with HST ACS/WFC F814W and F435W. The bright emission corresponds to redder (i.e., dustier) regions of the galaxy. The blue centroids correspond to clusters found in relatively “dust-free” regions of these galaxies, whereas the green centroids correspond to clusters found in relatively dustier regions of the galaxy.</figcaption></figure>

<figure><img src="image_46.png" /><figcaption>**Figure 45.** Inverted black and white *B*-*I* image of IC 4687N taken with HST ACS/WFC F814W and F435W. The bright emission corresponds to redder (i.e., dustier) regions of the galaxy. The blue centroids correspond to clusters found in relatively “dust-free” regions of these galaxies, whereas the green centroids correspond to clusters found in relatively dustier regions of the galaxy.</figcaption></figure>

<figure><img src="image_47.png" /><figcaption>**Figure 44.** Color-color plot of all star clusters identified in UGC 09618NED02 in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 43.</figcaption></figure>

<figure><img src="image_48.png" /><figcaption>**Figure 46.** Color-color plot of all star clusters identified in IC 4687N in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 45.</figcaption></figure>
<figure><img src="image_49.png" /><figcaption>**Figure 47.** Inverted black and white *B*–*I* image of IC 4687S taken with HST ACS/WFC F814W and F435W. The bright emission corresponds to redder (i.e., dustier) regions of the galaxy. The blue centroids correspond to clusters found in relatively “dust-free” regions of these galaxies, whereas the green centroids correspond to clusters found in relatively dustier regions of the galaxy.</figcaption></figure>

<figure><img src="image_50.png" /><figcaption>**Figure 49.** Inverted black and white *B*–*I* image of NGC 6786 taken with HST ACS/WFC F814W and F435W. The bright emission corresponds to redder (i.e., dustier) regions of the galaxy. The blue centroids correspond to clusters found in relatively “dust-free” regions of these galaxies, whereas the green centroids correspond to clusters found in relatively dustier regions of the galaxy.</figcaption></figure>

<figure><img src="image_51.png" /><figcaption>**Figure 48.** Color–color plot of all star clusters identified in IC 4687S in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 47.</figcaption></figure>

<figure><img src="image_52.png" /><figcaption>**Figure 50.** Color–color plot of all star clusters identified in NGC 6786 in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 49.</figcaption></figure>
<figure><img src="image_53.png" /></figure>

**Figure 51.** Inverted black and white *B*-*I* image of IRAS 20351+2521 taken with HST ACS/WFC F814W and F435W. The bright emission corresponds to redder (i.e., dustier) regions of the galaxy. The blue centroids correspond to clusters found in relatively “dust-free” regions of these galaxies, whereas the green centroids correspond to clusters found in relatively dustier regions of the galaxy.

<figure><img src="image_54.png" /></figure>

**Figure 53.** Inverted black and white *B*-*I* image of II Zw 096 taken with HST ACS/WFC F814W and F435W. The bright emission corresponds to redder (i.e., dustier) regions of the galaxy. The blue centroids correspond to clusters found in relatively “dust-free” regions of these galaxies, whereas the green centroids correspond to clusters found in relatively dustier regions of the galaxy.

<figure><img src="image_55.png" /></figure>

**Figure 52.** Color-color plot of all star clusters identified in IRAS 20351+2521 in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 51.

<figure><img src="image_56.png" /></figure>

**Figure 54.** Color-color plot of all star clusters identified in II Zw 096 in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 53.
<figure><img src="image_57.png" /></figure>

**Figure 55.** Inverted black and white *B*-*I* image of ESO 148-IG002 taken with HST ACS/WFC F814W and F435W. The bright emission corresponds to redder (i.e., dustier) regions of the galaxy. The blue centroids correspond to clusters found in relatively “dust-free” regions of these galaxies, whereas the green centroids correspond to clusters found in relatively dustier regions of the galaxy.

<figure><img src="image_58.png" /></figure>

**Figure 56.** Color–color plot of all star clusters identified in ESO 148-IG002 in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 55.

<figure><img src="image_59.png" /></figure>

**Figure 57.** Inverted black and white *B*-*I* image of NGC 7674 taken with HST ACS/WFC F814W and F435W. The bright emission corresponds to redder (i.e., dustier) regions of the galaxy. The blue centroids correspond to clusters found in relatively “dust-free” regions of these galaxies, whereas the green centroids correspond to clusters found in relatively dustier regions of the galaxy.

<figure><img src="image_60.png" /></figure>

**Figure 58.** Color–color plot of all star clusters identified in NGC 7674 in F814W, F435W, and F140LP plotted against SSP models with various amounts of visual extinction. The green points correspond to the clusters found in dustier regions of the galaxy in Figure 57.
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