# Appendix A: Calibration of XLSSC 072 data

<figure><img src="image_10.png" /><figcaption>**Fig. A.1.** Surface brightness profile of XLSSC 072, after point source subtraction, for the different datasets and their combination.</figcaption></figure>

About a quarter of the data obtained toward XLSSC 072 (October 2018) were calibrated using a bright radio source in the cluster field, instead of the standard method, because of a failure in the calibration system. In Figure A.1, we present the cluster surface brightness profile for the different dataset. We check that the SZ profiles are in agreement within the statistical uncertainties and the 30% calibration uncertainty expected for the October 2018 data.

# Appendix B: Radio and submillimeter point source identification and modeling

## B.1. Source detection in NIKA2 data

NIKA2 sources are detected iteratively, at the positions of S/N peaks with a threshold of $4\sigma$, using the following procedure (see Ricci 2018 for further details). 1) The maps are filtered as $S = (G_{\theta_1} * M - G_{\theta_2} * M)/N$, where $G_{\theta}$ is a Gaussian filter with FWHM $\theta$ and $M$ is the NIKA2 150 or 260 GHz map. We use the respective beam FWHM for $\theta_1$ and $\theta_2$ is set to 75 arcsec. This allows us to amplify the signal from point sources by removing the noise below the telescope resolution, and large scale atmospheric residual noise fluctuations. The signal is normalized by the standard deviation map $N$ so that it is expressed in units of S/N. 2) A source is fitted on the map $M$ using a Gaussian function corresponding to the NIKA2 beam plus a local background, at the location of the highest signal to noise ratio, but the precise location is allowed to vary within one beam FWHM. 3) The best-fit source model is subtracted from the NIKA2 map $M$. 4) We repeat steps 1, 2, and 3 until no source is detected above the chosen signal to noise ratio threshold on the map $S$.

In the end, we obtain a point source catalog with fluxes and coordinates, as well as a point source model map. We note that the fluxes are corrected from transfer function filtering effects, which are estimated by injecting and recovering point sources in processed data (filtering factor of about 15%). The correlated noise is accounted for in the uncertainties using MC noise simulations. The catalog purity is estimated by applying the same procedure in half-difference maps. Given the S/N threshold and the detection parameters, it is estimated to be 0.88 at 150 GHz and 0.93 at 260 GHz. Once the source catalogs are made in each band independently, we measure the flux of the counterpart band by fitting a source at the location of the detection. We match the catalogs with other bands to associate the detected sources

using an aperture of one beam FWHM. We also list the possible matches within the same band of two nearby sources if they fall within a single beam.

The list of NIKA2 identified sources in both bands, within 5 arcmin of the cluster centers, are reported in Table B.1 for all clusters. In Figure B.1, the source positions are reported on the images.

## B.2. Submillimeter contamination

We compute the mean 150 GHz to 260 GHz flux ratio for all the sources detected at 150 GHz, excluding radio sources, $F_{150}/F_{260} = 0.221 \pm 0.014$. Using this reference value, we find that the expected S/N is nearly the same at 150 and 260 GHz, implying that any source that could significantly bias the SZ signal should be detected at 260 GHz. If instead we use the mean ratio for the sources detected at 260 GHz, $F_{150}/F_{260} = 0.123 \pm 0.008$, the S/N should be two times larger at 260 GHz, and the potential bias would be reduced. Accordingly, and given the fact that no hint of a 260 GHz source is visible in the SZ region for the three clusters, we do not expect that any significant submillimeter source that is blended in the SZ signal could be missed and significantly bias the clusters analysis.

The field of XLSSC 072 was observed with Herschel/SPIRE (Griffin et al. 2010) at 500, 350, and 250µm (obsID 1342189031 and 1342190313), and we compare the SPIRE maps to NIKA2 images in Figure B.2. Although the image depth is relatively shallow, the brightest regions match the NIKA2 sources well. This confirms that no bright submillimeter source is missed by NIKA2 and that the SZ signal from XLSSC 072 is not contaminated.

## B.3. Radio GMRT counterparts

While NIKA2 260 GHz data can be used to assess the contamination from submillimeter sources, radio data are necessary to address the contamination from radio galaxies. We use XXL/GMRT images and catalogs from Smolčić et al. (2018), hereafter XXL Paper XXIX, to do so. In Table B.2, we list all the GMRT sources identified in the 10 arcmin × 10 arcmin region around the three clusters. The GMRT positions uncertainties are at most 0.5 arcsec, which is negligible for our purpose. In addition, we provide estimates of the fluxes expected at 150 GHz assuming a power-law spectrum: $F_{\nu} = F_{0}(\nu/\nu_{0})^{\alpha}$. This is done by using a spectral index equal to the mean value of the sample selected in Paper XXIX, between 610 and 1400 MHz (or its mean value plus one standard deviation). This provides an upper limit of the expected flux since a steepening of the radio spectrum is common at higher frequencies. Some of the GMRT sources are also detected in the NVSS surveys, in which case a spectral index estimate is available for individual sources, which we use to compute a more reliable flux estimate at 150 GHz. Given these estimates, only XXL-GMRT J021511.4-034309 in the field of XLSSC 072 was expected to be detected and is indeed detected (NIKA2-150 J021511.5-034308, NIKA2-260 J021511.6-034309). Figure B.1 shows the GMRT maps and how they compare to the NIKA2 data. We also use the FIRST catalog, which we compare to the GMRT images. We note that it is very unlikely that radio sources that are not detected in the NVSS or FIRST significantly affect NIKA2 data given the survey sensitivity (down to 0.45 and 0.15 mJy/beam). No radio source is expected to significantly contaminate the SZ signal, at least in the region where the two could be blended.
# Appendix A: Calibration of XLSSC 072 data

<figure><img src="image_11.png" /><figcaption>**Fig. A.1.** Surface brightness profile of XLSSC 072, after point source subtraction, for the different datasets and their combination.</figcaption></figure>

About a quarter of the data obtained toward XLSSC 072 (October 2018) were calibrated using a bright radio source in the cluster field, instead of the standard method, because of a failure in the calibration system. In Figure A.1, we present the cluster surface brightness profile for the different dataset. We check that the SZ profiles are in agreement within the statistical uncertainties and the 30% calibration uncertainty expected for the October 2018 data.

# Appendix B: Radio and submillimeter point source identification and modeling

## B.1. Source detection in NIKA2 data

NIKA2 sources are detected iteratively, at the positions of S/N peaks with a threshold of $4\sigma$, using the following procedure (see Ricci 2018 for further details). 1) The maps are filtered as $S = (G_{\theta_1} * M - G_{\theta_2} * M)/N$, where $G_{\theta}$ is a Gaussian filter with FWHM $\theta$ and $M$ is the NIKA2 150 or 260 GHz map. We use the respective beam FWHM for $\theta_1$ and $\theta_2$ is set to 75 arcsec. This allows us to amplify the signal from point sources by removing the noise below the telescope resolution, and large scale atmospheric residual noise fluctuations. The signal is normalized by the standard deviation map $N$ so that it is expressed in units of S/N. 2) A source is fitted on the map $M$ using a Gaussian function corresponding to the NIKA2 beam plus a local background, at the location of the highest signal to noise ratio, but the precise location is allowed to vary within one beam FWHM. 3) The best-fit source model is subtracted from the NIKA2 map $M$. 4) We repeat steps 1, 2, and 3 until no source is detected above the chosen signal to noise ratio threshold on the map $S$.

In the end, we obtain a point source catalog with fluxes and coordinates, as well as a point source model map. We note that the fluxes are corrected from transfer function filtering effects, which are estimated by injecting and recovering point sources in processed data (filtering factor of about 15%). The correlated noise is accounted for in the uncertainties using MC noise simulations. The catalog purity is estimated by applying the same procedure in half-difference maps. Given the S/N threshold and the detection parameters, it is estimated to be 0.88 at 150 GHz and 0.93 at 260 GHz. Once the source catalogs are made in each band independently, we measure the flux of the counterpart band by fitting a source at the location of the detection. We match the catalogs with other bands to associate the detected sources

using an aperture of one beam FWHM. We also list the possible matches within the same band of two nearby sources if they fall within a single beam.

The list of NIKA2 identified sources in both bands, within 5 arcmin of the cluster centers, are reported in Table B.1 for all clusters. In Figure B.1, the source positions are reported on the images.

## B.2. Submillimeter contamination

We compute the mean 150 GHz to 260 GHz flux ratio for all the sources detected at 150 GHz, excluding radio sources, $F_{150}/F_{260} = 0.221 \pm 0.014$. Using this reference value, we find that the expected S/N is nearly the same at 150 and 260 GHz, implying that any source that could significantly bias the SZ signal should be detected at 260 GHz. If instead we use the mean ratio for the sources detected at 260 GHz, $F_{150}/F_{260} = 0.123 \pm 0.008$, the S/N should be two times larger at 260 GHz, and the potential bias would be reduced. Accordingly, and given the fact that no hint of a 260 GHz source is visible in the SZ region for the three clusters, we do not expect that any significant submillimeter source that is blended in the SZ signal could be missed and significantly bias the clusters analysis.

The field of XLSSC 072 was observed with Herschel/SPIRE (Griffin et al. 2010) at 500, 350, and 250µm (obsID 1342189031 and 1342190313), and we compare the SPIRE maps to NIKA2 images in Figure B.2. Although the image depth is relatively shallow, the brightest regions match the NIKA2 sources well. This confirms that no bright submillimeter source is missed by NIKA2 and that the SZ signal from XLSSC 072 is not contaminated.

## B.3. Radio GMRT counterparts

While NIKA2 260 GHz data can be used to assess the contamination from submillimeter sources, radio data are necessary to address the contamination from radio galaxies. We use XXL/GMRT images and catalogs from Smolčić et al. (2018), hereafter XXL Paper XXIX, to do so. In Table B.2, we list all the GMRT sources identified in the 10 arcmin × 10 arcmin region around the three clusters. The GMRT positions uncertainties are at most 0.5 arcsec, which is negligible for our purpose. In addition, we provide estimates of the fluxes expected at 150 GHz assuming a power-law spectrum: $F_{\nu} = F_{0}(\nu/\nu_{0})^{\alpha}$. This is done by using a spectral index equal to the mean value of the sample selected in Paper XXIX, between 610 and 1400 MHz (or its mean value plus one standard deviation). This provides an upper limit of the expected flux since a steepening of the radio spectrum is common at higher frequencies. Some of the GMRT sources are also detected in the NVSS surveys, in which case a spectral index estimate is available for individual sources, which we use to compute a more reliable flux estimate at 150 GHz. Given these estimates, only XXL-GMRT J021511.4-034309 in the field of XLSSC 072 was expected to be detected and is indeed detected (NIKA2-150 J021511.5-034308, NIKA2-260 J021511.6-034309). Figure B.1 shows the GMRT maps and how they compare to the NIKA2 data. We also use the FIRST catalog, which we compare to the GMRT images. We note that it is very unlikely that radio sources that are not detected in the NVSS or FIRST significantly affect NIKA2 data given the survey sensitivity (down to 0.45 and 0.15 mJy/beam). No radio source is expected to significantly contaminate the SZ signal, at least in the region where the two could be blended.
<figure><img src="image_11.png" /><figcaption>**Fig. B.1.** Submillimeter and radio sources' identification in the fields of XLSSC 072 (left), XLSSC 100 (center), and XLSSC 102 (right). **Top:** NIKA2 260 GHz images with detected sources indicated as red crosses. **Middle:** NIKA2 150 GHz images with detected sources indicated as blue crosses. **Bottom:** GMRT images at 610 MHz, with detected sources indicated as orange circles. Sources with NVSS counterparts are indicated as solid lines, and dashed otherwise. FIRST sources are indicated as magenta circles. The 150 GHz S/N contours at -9, -7, -5, and -3 σ are reported in all maps. All identified radio and submillimeter sources are reported in the 150 GHz maps.</figcaption></figure>

### B.4. Point source model and impact on the SZ signal

No radio or submillimeter source is expected to bias significantly the SZ signal observed with NIKA2 in XLSSC 072, XLSSC 100, or XLSSC 102, as no source is expected to be blended in the SZ signal. Nonetheless, several sources are detected within the cluster region, where the SZ signal, although fainter, extends. We built a point source model according to the 150 GHz cata-

log and use it to account for the point source in the SZ analysis. Since the sources are fitted using a local background, this assumes that the SZ signal is smooth at the location of the point sources. In Figure B.3, we show the surface brightness profiles when accounting (or not) for the detected point sources. This is done either by masking the point sources or correcting for them. The point sources have a mild contribution, so uncertainties in the model should be negligible.
<figure><img src="image_12.png" /><figcaption>**Fig. B.1.** Submillimeter and radio sources' identification in the fields of XLSSC 072 (left), XLSSC 100 (center), and XLSSC 102 (right). **Top:** NIKA2 260 GHz images with detected sources indicated as red crosses. **Middle:** NIKA2 150 GHz images with detected sources indicated as blue crosses. **Bottom:** GMRT images at 610 MHz, with detected sources indicated as orange circles. Sources with NVSS counterparts are indicated as solid lines, and dashed otherwise. FIRST sources are indicated as magenta circles. The 150 GHz S/N contours at -9, -7, -5, and -3 σ are reported in all maps. All identified radio and submillimeter sources are reported in the 150 GHz maps.</figcaption></figure>

### B.4. Point source model and impact on the SZ signal

No radio or submillimeter source is expected to bias significantly the SZ signal observed with NIKA2 in XLSSC 072, XLSSC 100, or XLSSC 102, as no source is expected to be blended in the SZ signal. Nonetheless, several sources are detected within the cluster region, where the SZ signal, although fainter, extends. We built a point source model according to the 150 GHz cata-

log and use it to account for the point source in the SZ analysis. Since the sources are fitted using a local background, this assumes that the SZ signal is smooth at the location of the point sources. In Figure B.3, we show the surface brightness profiles when accounting (or not) for the detected point sources. This is done either by masking the point sources or correcting for them. The point sources have a mild contribution, so uncertainties in the model should be negligible.
<table><caption>Table B.1. Point sources detected with NIKA2 in the fields of XLSSC 072, XLSSC 100, and XLSSC 102.</caption><thead><tr><th>Name</th><th>Label</th><th>S/N</th><th>R.A.<br>[deg]</th><th>Dec.<br>[deg]</th><th>Distance<sup>†</sup><br>[arcsec]</th><th>F<sub>detection</sub><br>[mJy]</th><th>ΔF<sub>detection</sub><br>[mJy]</th><th>F<sub>counterpart</sub><br>[mJy]</th><th>ΔF<sub>counterpart</sub><br>[mJy]</th><th>Match</th></tr></thead><tbody><tr><td colspan="11"><strong>Field of XLSSC 072</strong></td></tr><tr><td colspan="11">Detection at 260 GHz, counterparts at 150 GHz</td></tr><tr><td>NIKA2-260 J021511.6-034309</td><td>N260-1</td><td>25.5</td><td>33.7982</td><td>-3.7192</td><td>187.8</td><td>20.48</td><td>0.79</td><td>30.15</td><td>0.15</td><td>N260-10, N150-1, RS-1</td></tr><tr><td>NIKA2-260 J021533.8-034025</td><td>N260-2</td><td>14.9</td><td>33.8909</td><td>-3.6738</td><td>238.5</td><td>12.50</td><td>0.82</td><td>2.86</td><td>0.18</td><td>N150-2, RS-14</td></tr><tr><td>NIKA2-260 J021527.0-034203</td><td>N260-3</td><td>9.9</td><td>33.8623</td><td>-3.7009</td><td>100.5</td><td>5.75</td><td>0.56</td><td>0.95</td><td>0.12</td><td>N260-6, N260-15, N150-3</td></tr><tr><td>NIKA2-260 J021516.4-034300</td><td>N260-4</td><td>8.1</td><td>33.8182</td><td>-3.7167</td><td>118.9</td><td>5.27</td><td>0.62</td><td>0.40</td><td>0.13</td><td></td></tr><tr><td>NIKA2-260 J021537.0-034354</td><td>N260-5</td><td>6.5</td><td>33.9040</td><td>-3.7318</td><td>195.0</td><td>4.43</td><td>0.68</td><td>0.15</td><td>0.15</td><td></td></tr><tr><td>NIKA2-260 J021526.4-034159</td><td>N260-6</td><td>5.9</td><td>33.8600</td><td>-3.6998</td><td>100.9</td><td>4.91</td><td>0.56</td><td>0.72</td><td>0.12</td><td>N260-3</td></tr><tr><td>NIKA2-260 J021535.3-034024</td><td>N260-7</td><td>5.8</td><td>33.8969</td><td>-3.6735</td><td>253.3</td><td>4.88</td><td>0.87</td><td>0.63</td><td>0.19</td><td></td></tr><tr><td>NIKA2-260 J021527.4-034129</td><td>N260-8</td><td>5.6</td><td>33.8641</td><td>-3.6914</td><td>134.4</td><td>3.12</td><td>0.60</td><td>0.12</td><td>0.13</td><td></td></tr><tr><td>NIKA2-260 J021531.6-034041</td><td>N260-9</td><td>5.3</td><td>33.8818</td><td>-3.6781</td><td>207.0</td><td>3.57</td><td>0.73</td><td>0.20</td><td>0.16</td><td></td></tr><tr><td>NIKA2-260 J021512.2-034309</td><td>N260-10</td><td>5.0</td><td>33.8010</td><td>-3.7192</td><td>177.7</td><td>9.42</td><td>0.76</td><td>16.06</td><td>0.15</td><td>N260-1, N150-1 RS-1</td></tr><tr><td>NIKA2-260 J021528.6-034511</td><td>N260-11</td><td>4.9</td><td>33.8690</td><td>-3.7531</td><td>119.1</td><td>2.93</td><td>0.57</td><td>0.41</td><td>0.13</td><td></td></tr><tr><td>NIKA2-260 J021536.5-034526</td><td>N260-12</td><td>4.5</td><td>33.9022</td><td>-3.7573</td><td>218.9</td><td>3.46</td><td>0.74</td><td>0.35</td><td>0.17</td><td></td></tr><tr><td>NIKA2-260 J021528.5-034250</td><td>N260-13</td><td>4.4</td><td>33.8688</td><td>-3.7139</td><td>80.5</td><td>2.28</td><td>0.53</td><td>0.66</td><td>0.11</td><td>N150-4, N150-6</td></tr><tr><td>NIKA2-260 J021533.8-034247</td><td>N260-14</td><td>4.3</td><td>33.8906</td><td>-3.7131</td><td>153.2</td><td>2.70</td><td>0.61</td><td>0.39</td><td>0.13</td><td></td></tr><tr><td>NIKA2-260 J021527.1-034211</td><td>N260-15</td><td>4.3</td><td>33.8628</td><td>-3.7032</td><td>94.0</td><td>4.00</td><td>0.55</td><td>0.93</td><td>0.12</td><td>N260-3, N150-3</td></tr><tr><td>NIKA2-260 J021531.8-034425</td><td>N260-16</td><td>4.2</td><td>33.8826</td><td>-3.7404</td><td>128.2</td><td>2.45</td><td>0.57</td><td>0.46</td><td>0.13</td><td></td></tr><tr><td>NIKA2-260 J021533.5-034320</td><td>N260-17</td><td>4.2</td><td>33.8894</td><td>-3.7225</td><td>142.3</td><td>2.51</td><td>0.59</td><td>0.38</td><td>0.13</td><td></td></tr><tr><td>NIKA2-260 J021531.8-034509</td><td>N260-18</td><td>4.2</td><td>33.8824</td><td>-3.7527</td><td>151.2</td><td>2.33</td><td>0.61</td><td>0.09</td><td>0.14</td><td></td></tr><tr><td>NIKA2-260 J021539.3-034205</td><td>N260-19</td><td>4.1</td><td>33.9136</td><td>-3.7015</td><td>244.9</td><td>3.53</td><td>0.82</td><td>1.16</td><td>0.18</td><td>N150-5</td></tr><tr><td>NIKA2-260 J021505.7-034157</td><td>N260-20</td><td>4.1</td><td>33.7739</td><td>-3.6992</td><td>290.1</td><td>5.72</td><td>1.36</td><td>0.03</td><td>0.25</td><td></td></tr><tr><td>NIKA2-260 J021523.1-034613</td><td>N260-21</td><td>4.0</td><td>33.8462</td><td>-3.7703</td><td>160.2</td><td>2.80</td><td>0.65</td><td>-0.15</td><td>0.14</td><td></td></tr><tr><td>NIKA2-260 J021529.6-034300</td><td>N260-22</td><td>4.0</td><td>33.8732</td><td>-3.7168</td><td>89.8</td><td>2.09</td><td>0.53</td><td>0.50</td><td>0.12</td><td></td></tr><tr><td>NIKA2-260 J021513.9-034417</td><td>N260-23</td><td>4.0</td><td>33.8077</td><td>-3.7382</td><td>158.1</td><td>2.75</td><td>0.70</td><td>0.53</td><td>0.14</td><td></td></tr><tr><td colspan="11">Detection at 150 GHz, counterparts at 260 GHz</td></tr><tr><td>NIKA2-150 J021511.5-034308</td><td>N150-1</td><td>199.0</td><td>33.7979</td><td>-3.7190</td><td>188.8</td><td>30.30</td><td>0.15</td><td>19.71</td><td>0.81</td><td>N260-1, N260-10, RS-1</td></tr><tr><td>NIKA2-150 J021533.8-034025</td><td>N150-2</td><td>16.6</td><td>33.8910</td><td>-3.6739</td><td>238.5</td><td>2.84</td><td>0.17</td><td>12.47</td><td>0.84</td><td>N260-2, RS-14</td></tr><tr><td>NIKA2-150 J021527.0-034207</td><td>N150-3</td><td>8.6</td><td>33.8626</td><td>-3.7021</td><td>97.1</td><td>1.12</td><td>0.11</td><td>4.97</td><td>0.57</td><td>N260-3, N260-6, N260-15</td></tr><tr><td>NIKA2-150 J021528.3-034248</td><td>N150-4</td><td>6.5</td><td>33.8681</td><td>-3.7133</td><td>79.5</td><td>0.81</td><td>0.11</td><td>2.06</td><td>0.54</td><td>N150-6, N260-13</td></tr><tr><td>NIKA2-150 J021539.2-034205</td><td>N150-5</td><td>6.2</td><td>33.9134</td><td>-3.7016</td><td>244.1</td><td>1.01</td><td>0.18</td><td>3.43</td><td>0.84</td><td>N260-19</td></tr><tr><td>NIKA2-150 J021528.5-034300</td><td>N150-6</td><td>4.5</td><td>33.8686</td><td>-3.7168</td><td>74.7</td><td>0.74</td><td>0.11</td><td>1.40</td><td>0.54</td><td>N150-4, N260-13, N260-22</td></tr><tr><td>NIKA2-150 J021522.7-034241</td><td>N150-7</td><td>4.2</td><td>33.8446</td><td>-3.7115</td><td>55.6</td><td>0.43</td><td>0.11</td><td>0.18</td><td>0.55</td><td></td></tr><tr><td colspan="11"><strong>Field of XLSSC 100</strong></td></tr><tr><td colspan="11">Detection at 260 GHz, counterparts at 150 GHz</td></tr><tr><td>NIKA2-260 J020618.6-061123</td><td>N260-1</td><td>7.5</td><td>31.5774</td><td>-6.1898</td><td>102.5</td><td>4.46</td><td>0.57</td><td>0.60</td><td>0.13</td><td>N150-5</td></tr><tr><td>NIKA2-260 J020612.4-061038</td><td>N260-2</td><td>6.4</td><td>31.5515</td><td>-6.1774</td><td>56.7</td><td>3.62</td><td>0.55</td><td>0.97</td><td>0.12</td><td>N150-1</td></tr><tr><td>NIKA2-260 J020606.8-061357</td><td>N260-3</td><td>5.6</td><td>31.5284</td><td>-6.2327</td><td>160.6</td><td>4.09</td><td>0.71</td><td>0.84</td><td>0.16</td><td>N150-2</td></tr><tr><td>NIKA2-260 J020622.2-060801</td><td>N260-4</td><td>5.3</td><td>31.5925</td><td>-6.1337</td><td>264.1</td><td>5.12</td><td>0.97</td><td>0.74</td><td>0.22</td><td>N150-6</td></tr><tr><td>NIKA2-260 J020616.1-061012</td><td>N260-5</td><td>4.7</td><td>31.5669</td><td>-6.1701</td><td>104.4</td><td>2.74</td><td>0.58</td><td>0.41</td><td>0.13</td><td></td></tr><tr><td>NIKA2-260 J020618.4-061217</td><td>N260-6</td><td>4.6</td><td>31.5766</td><td>-6.2049</td><td>107.8</td><td>2.69</td><td>0.58</td><td>0.22</td><td>0.13</td><td></td></tr><tr><td>NIKA2-260 J020613.8-061313</td><td>N260-7</td><td>4.6</td><td>31.5574</td><td>-6.2204</td><td>103.3</td><td>2.78</td><td>0.59</td><td>0.23</td><td>0.13</td><td></td></tr><tr><td>NIKA2-260 J020627.6-061008</td><td>N260-8</td><td>4.3</td><td>31.6150</td><td>-6.1691</td><td>251.4</td><td>3.82</td><td>0.89</td><td>0.89</td><td>0.21</td><td>N150-3</td></tr><tr><td>NIKA2-260 J020628.0-061344</td><td>N260-9</td><td>4.2</td><td>31.6165</td><td>-6.2290</td><td>274.3</td><td>4.36</td><td>1.00</td><td>0.25</td><td>0.24</td><td></td></tr><tr><td>NIKA2-260 J020609.4-061306</td><td>N260-10</td><td>4.1</td><td>31.5392</td><td>-6.2184</td><td>97.8</td><td>2.65</td><td>0.60</td><td>-0.05</td><td>0.13</td><td></td></tr><tr><td>NIKA2-260 J020602.6-061204</td><td>N260-11</td><td>4.1</td><td>31.5109</td><td>-6.2013</td><td>139.5</td><td>2.93</td><td>0.70</td><td>-0.02</td><td>0.15</td><td></td></tr><tr><td colspan="11">Detection at 150 GHz, counterparts at 260 GHz</td></tr><tr><td>NIKA2-150 J020612.4-061040</td><td>N150-1</td><td>7.8</td><td>31.5516</td><td>-6.1778</td><td>55.6</td><td>0.93</td><td>0.12</td><td>3.64</td><td>0.57</td><td>N260-2</td></tr><tr><td>NIKA2-150 J020606.7-061357</td><td>N150-2</td><td>5.3</td><td>31.5281</td><td>-6.2327</td><td>161.4</td><td>0.88</td><td>0.15</td><td>4.06</td><td>0.73</td><td>N260-3</td></tr><tr><td>NIKA2-150 J020627.4-061011</td><td>N150-3</td><td>4.8</td><td>31.6140</td><td>-6.1697</td><td>247.3</td><td>1.04</td><td>0.20</td><td>3.23</td><td>0.90</td><td>N260-8</td></tr><tr><td>NIKA2-150 J020624.9-061056</td><td>N150-4</td><td>4.8</td><td>31.6039</td><td>-6.1824</td><td>200.3</td><td>0.83</td><td>0.17</td><td>2.11</td><td>0.75</td><td></td></tr><tr><td>NIKA2-150 J020618.6-061123</td><td>N150-5</td><td>4.4</td><td>31.5775</td><td>-6.1898</td><td>102.6</td><td>0.56</td><td>0.13</td><td>4.41</td><td>0.59</td><td>N260-1</td></tr><tr><td>NIKA2-150 J020622.5-060800</td><td>N150-6</td><td>4.0</td><td>31.5937</td><td>-6.1334</td><td>267.7</td><td>0.91</td><td>0.22</td><td>4.55</td><td>1.02</td><td>N260-4</td></tr><tr><td colspan="11"><strong>Field of XLSSC 102</strong></td></tr><tr><td colspan="11">Detection at 260 GHz, counterparts at 150 GHz</td></tr><tr><td>NIKA2-260 J020517.7-044037</td><td>N260-1</td><td>5.6</td><td>31.3239</td><td>-4.6770</td><td>90.3</td><td>3.40</td><td>0.61</td><td>0.38</td><td>0.15</td><td>N150-4</td></tr><tr><td>NIKA2-260 J020459.7-043852</td><td>N260-2</td><td>4.9</td><td>31.2486</td><td>-4.6478</td><td>263.7</td><td>6.07</td><td>1.15</td><td>0.92</td><td>0.27</td><td></td></tr><tr><td>NIKA2-260 J020522.4-043903</td><td>N260-3</td><td>4.7</td><td>31.3434</td><td>-4.6509</td><td>76.9</td><td>2.84</td><td>0.59</td><td>0.61</td><td>0.14</td><td>N150-2</td></tr><tr><td>NIKA2-260 J020502.6-043824</td><td>N260-4</td><td>4.4</td><td>31.2607</td><td>-4.6401</td><td>224.2</td><td>4.31</td><td>0.93</td><td>0.41</td><td>0.22</td><td></td></tr><tr><td>NIKA2-260 J020509.2-044100</td><td>N260-5</td><td>4.3</td><td>31.2881</td><td>-4.6834</td><td>165.9</td><td>3.32</td><td>0.75</td><td>0.30</td><td>0.18</td><td></td></tr><tr><td>NIKA2-260 J020520.6-043843</td><td>N260-6</td><td>4.2</td><td>31.3357</td><td>-4.6454</td><td>54.5</td><td>2.50</td><td>0.57</td><td>0.34</td><td>0.14</td><td>RS-4</td></tr><tr><td colspan="11">Detection at 150 GHz, counterparts at 260 GHz</td></tr><tr><td>NIKA2-150 J020511.8-044305</td><td>N150-1</td><td>4.7</td><td>31.2991</td><td>-4.7182</td><td>252.2</td><td>1.20</td><td>0.25</td><td>2.95</td><td>1.05</td><td></td></tr><tr><td>NIKA2-150 J020522.3-043905</td><td>N150-2</td><td>4.6</td><td>31.3429</td><td>-4.6516</td><td>75.2</td><td>0.63</td><td>0.14</td><td>2.67</td><td>0.59</td><td>N260-3</td></tr><tr><td>NIKA2-150 J020536.1-043748</td><td>N150-3</td><td>4.4</td><td>31.4006</td><td>-4.6301</td><td>292.9</td><td>1.46</td><td>0.30</td><td>5.05</td><td>1.30</td><td></td></tr><tr><td>NIKA2-150 J020517.6-044047</td><td>N150-4</td><td>4.2</td><td>31.3235</td><td>-4.6798</td><td>100.3</td><td>0.56</td><td>0.15</td><td>2.36</td><td>0.62</td><td>N260-1</td></tr></tbody></table>

Notes. † distance from the cluster reference center.
<table><caption>Table B.1. Point sources detected with NIKA2 in the fields of XLSSC 072, XLSSC 100, and XLSSC 102.</caption><thead><tr><th>Name</th><th>Label</th><th>S/N</th><th>R.A.<br>[deg]</th><th>Dec.<br>[deg]</th><th>Distance<sup>†</sup><br>[arcsec]</th><th>F<sub>detection</sub><br>[mJy]</th><th>ΔF<sub>detection</sub><br>[mJy]</th><th>F<sub>counterpart</sub><br>[mJy]</th><th>ΔF<sub>counterpart</sub><br>[mJy]</th><th>Match</th></tr></thead><tbody><tr><td colspan="12"><strong>Field of XLSSC 072</strong></td></tr><tr><td colspan="12">Detection at 260 GHz, counterparts at 150 GHz</td></tr><tr><td>NIKA2-260 J021511.6-034309</td><td>N260-1</td><td>25.5</td><td>33.7982</td><td>-3.7192</td><td>187.8</td><td>20.48</td><td>0.79</td><td>30.15</td><td>0.15</td><td>N260-10, N150-1, RS-1</td></tr><tr><td>NIKA2-260 J021533.8-034025</td><td>N260-2</td><td>14.9</td><td>33.8909</td><td>-3.6738</td><td>238.5</td><td>12.50</td><td>0.82</td><td>2.86</td><td>0.18</td><td>N150-2, RS-14</td></tr><tr><td>NIKA2-260 J021527.0-034203</td><td>N260-3</td><td>9.9</td><td>33.8623</td><td>-3.7009</td><td>100.5</td><td>5.75</td><td>0.56</td><td>0.95</td><td>0.12</td><td>N260-6, N260-15, N150-3</td></tr><tr><td>NIKA2-260 J021516.4-034300</td><td>N260-4</td><td>8.1</td><td>33.8182</td><td>-3.7167</td><td>118.9</td><td>5.27</td><td>0.62</td><td>0.40</td><td>0.13</td><td></td></tr><tr><td>NIKA2-260 J021537.0-034354</td><td>N260-5</td><td>6.5</td><td>33.9040</td><td>-3.7318</td><td>195.0</td><td>4.43</td><td>0.68</td><td>0.15</td><td>0.15</td><td></td></tr><tr><td>NIKA2-260 J021526.4-034159</td><td>N260-6</td><td>5.9</td><td>33.8600</td><td>-3.6998</td><td>100.9</td><td>4.91</td><td>0.56</td><td>0.72</td><td>0.12</td><td>N260-3</td></tr><tr><td>NIKA2-260 J021535.3-034024</td><td>N260-7</td><td>5.8</td><td>33.8969</td><td>-3.6735</td><td>253.3</td><td>4.88</td><td>0.87</td><td>0.63</td><td>0.19</td><td></td></tr><tr><td>NIKA2-260 J021527.4-034129</td><td>N260-8</td><td>5.6</td><td>33.8641</td><td>-3.6914</td><td>134.4</td><td>3.12</td><td>0.60</td><td>0.12</td><td>0.13</td><td></td></tr><tr><td>NIKA2-260 J021531.6-034041</td><td>N260-9</td><td>5.3</td><td>33.8818</td><td>-3.6781</td><td>207.0</td><td>3.57</td><td>0.73</td><td>0.20</td><td>0.16</td><td></td></tr><tr><td>NIKA2-260 J021512.2-034309</td><td>N260-10</td><td>5.0</td><td>33.8010</td><td>-3.7192</td><td>177.7</td><td>9.42</td><td>0.76</td><td>16.06</td><td>0.15</td><td>N260-1, N150-1 RS-1</td></tr><tr><td>NIKA2-260 J021528.6-034511</td><td>N260-11</td><td>4.9</td><td>33.8690</td><td>-3.7531</td><td>119.1</td><td>2.93</td><td>0.57</td><td>0.41</td><td>0.13</td><td></td></tr><tr><td>NIKA2-260 J021536.5-034526</td><td>N260-12</td><td>4.5</td><td>33.9022</td><td>-3.7573</td><td>218.9</td><td>3.46</td><td>0.74</td><td>0.35</td><td>0.17</td><td></td></tr><tr><td>NIKA2-260 J021528.5-034250</td><td>N260-13</td><td>4.4</td><td>33.8688</td><td>-3.7139</td><td>80.5</td><td>2.28</td><td>0.53</td><td>0.66</td><td>0.11</td><td>N150-4, N150-6</td></tr><tr><td>NIKA2-260 J021533.8-034247</td><td>N260-14</td><td>4.3</td><td>33.8906</td><td>-3.7131</td><td>153.2</td><td>2.70</td><td>0.61</td><td>0.39</td><td>0.13</td><td></td></tr><tr><td>NIKA2-260 J021527.1-034211</td><td>N260-15</td><td>4.3</td><td>33.8628</td><td>-3.7032</td><td>94.0</td><td>4.00</td><td>0.55</td><td>0.93</td><td>0.12</td><td>N260-3, N150-3</td></tr><tr><td>NIKA2-260 J021531.8-034425</td><td>N260-16</td><td>4.2</td><td>33.8826</td><td>-3.7404</td><td>128.2</td><td>2.45</td><td>0.57</td><td>0.46</td><td>0.13</td><td></td></tr><tr><td>NIKA2-260 J021533.5-034320</td><td>N260-17</td><td>4.2</td><td>33.8894</td><td>-3.7225</td><td>142.3</td><td>2.51</td><td>0.59</td><td>0.38</td><td>0.13</td><td></td></tr><tr><td>NIKA2-260 J021531.8-034509</td><td>N260-18</td><td>4.2</td><td>33.8824</td><td>-3.7527</td><td>151.2</td><td>2.33</td><td>0.61</td><td>0.09</td><td>0.14</td><td></td></tr><tr><td>NIKA2-260 J021539.3-034205</td><td>N260-19</td><td>4.1</td><td>33.9136</td><td>-3.7015</td><td>244.9</td><td>3.53</td><td>0.82</td><td>1.16</td><td>0.18</td><td>N150-5</td></tr><tr><td>NIKA2-260 J021505.7-034157</td><td>N260-20</td><td>4.1</td><td>33.7739</td><td>-3.6992</td><td>290.1</td><td>5.72</td><td>1.36</td><td>0.03</td><td>0.25</td><td></td></tr><tr><td>NIKA2-260 J021523.1-034613</td><td>N260-21</td><td>4.0</td><td>33.8462</td><td>-3.7703</td><td>160.2</td><td>2.80</td><td>0.65</td><td>-0.15</td><td>0.14</td><td></td></tr><tr><td>NIKA2-260 J021529.6-034300</td><td>N260-22</td><td>4.0</td><td>33.8732</td><td>-3.7168</td><td>89.8</td><td>2.09</td><td>0.53</td><td>0.50</td><td>0.12</td><td></td></tr><tr><td>NIKA2-260 J021513.9-034417</td><td>N260-23</td><td>4.0</td><td>33.8077</td><td>-3.7382</td><td>158.1</td><td>2.75</td><td>0.70</td><td>0.53</td><td>0.14</td><td></td></tr><tr><td colspan="12">Detection at 150 GHz, counterparts at 260 GHz</td></tr><tr><td>NIKA2-150 J021511.5-034308</td><td>N150-1</td><td>199.0</td><td>33.7979</td><td>-3.7190</td><td>188.8</td><td>30.30</td><td>0.15</td><td>19.71</td><td>0.81</td><td>N260-1, N260-10, RS-1</td></tr><tr><td>NIKA2-150 J021533.8-034025</td><td>N150-2</td><td>16.6</td><td>33.8910</td><td>-3.6739</td><td>238.5</td><td>2.84</td><td>0.17</td><td>12.47</td><td>0.84</td><td>N260-2, RS-14</td></tr><tr><td>NIKA2-150 J021527.0-034207</td><td>N150-3</td><td>8.6</td><td>33.8626</td><td>-3.7021</td><td>97.1</td><td>1.12</td><td>0.11</td><td>4.97</td><td>0.57</td><td>N260-3, N260-6, N260-15</td></tr><tr><td>NIKA2-150 J021528.3-034248</td><td>N150-4</td><td>6.5</td><td>33.8681</td><td>-3.7133</td><td>79.5</td><td>0.81</td><td>0.11</td><td>2.06</td><td>0.54</td><td>N150-6, N260-13</td></tr><tr><td>NIKA2-150 J021539.2-034205</td><td>N150-5</td><td>6.2</td><td>33.9134</td><td>-3.7016</td><td>244.1</td><td>1.01</td><td>0.18</td><td>3.43</td><td>0.84</td><td>N260-19</td></tr><tr><td>NIKA2-150 J021528.5-034300</td><td>N150-6</td><td>4.5</td><td>33.8686</td><td>-3.7168</td><td>74.7</td><td>0.74</td><td>0.11</td><td>1.40</td><td>0.54</td><td>N150-4, N260-13, N260-22</td></tr><tr><td>NIKA2-150 J021522.7-034241</td><td>N150-7</td><td>4.2</td><td>33.8446</td><td>-3.7115</td><td>55.6</td><td>0.43</td><td>0.11</td><td>0.18</td><td>0.55</td><td></td></tr><tr><td colspan="12"><strong>Field of XLSSC 100</strong></td></tr><tr><td colspan="12">Detection at 260 GHz, counterparts at 150 GHz</td></tr><tr><td>NIKA2-260 J020618.6-061123</td><td>N260-1</td><td>7.5</td><td>31.5774</td><td>-6.1898</td><td>102.5</td><td>4.46</td><td>0.57</td><td>0.60</td><td>0.13</td><td>N150-5</td></tr><tr><td>NIKA2-260 J020612.4-061038</td><td>N260-2</td><td>6.4</td><td>31.5515</td><td>-6.1774</td><td>56.7</td><td>3.62</td><td>0.55</td><td>0.97</td><td>0.12</td><td>N150-1</td></tr><tr><td>NIKA2-260 J020606.8-061357</td><td>N260-3</td><td>5.6</td><td>31.5284</td><td>-6.2327</td><td>160.6</td><td>4.09</td><td>0.71</td><td>0.84</td><td>0.16</td><td>N150-2</td></tr><tr><td>NIKA2-260 J020622.2-060801</td><td>N260-4</td><td>5.3</td><td>31.5925</td><td>-6.1337</td><td>264.1</td><td>5.12</td><td>0.97</td><td>0.74</td><td>0.22</td><td>N150-6</td></tr><tr><td>NIKA2-260 J020616.1-061012</td><td>N260-5</td><td>4.7</td><td>31.5669</td><td>-6.1701</td><td>104.4</td><td>2.74</td><td>0.58</td><td>0.41</td><td>0.13</td><td></td></tr><tr><td>NIKA2-260 J020618.4-061217</td><td>N260-6</td><td>4.6</td><td>31.5766</td><td>-6.2049</td><td>107.8</td><td>2.69</td><td>0.58</td><td>0.22</td><td>0.13</td><td></td></tr><tr><td>NIKA2-260 J020613.8-061313</td><td>N260-7</td><td>4.6</td><td>31.5574</td><td>-6.2204</td><td>103.3</td><td>2.78</td><td>0.59</td><td>0.23</td><td>0.13</td><td></td></tr><tr><td>NIKA2-260 J020627.6-061008</td><td>N260-8</td><td>4.3</td><td>31.6150</td><td>-6.1691</td><td>251.4</td><td>3.82</td><td>0.89</td><td>0.89</td><td>0.21</td><td>N150-3</td></tr><tr><td>NIKA2-260 J020628.0-061344</td><td>N260-9</td><td>4.2</td><td>31.6165</td><td>-6.2290</td><td>274.3</td><td>4.36</td><td>1.00</td><td>0.25</td><td>0.24</td><td></td></tr><tr><td>NIKA2-260 J020609.4-061306</td><td>N260-10</td><td>4.1</td><td>31.5392</td><td>-6.2184</td><td>97.8</td><td>2.65</td><td>0.60</td><td>-0.05</td><td>0.13</td><td></td></tr><tr><td>NIKA2-260 J020602.6-061204</td><td>N260-11</td><td>4.1</td><td>31.5109</td><td>-6.2013</td><td>139.5</td><td>2.93</td><td>0.70</td><td>-0.02</td><td>0.15</td><td></td></tr><tr><td colspan="12">Detection at 150 GHz, counterparts at 260 GHz</td></tr><tr><td>NIKA2-150 J020612.4-061040</td><td>N150-1</td><td>7.8</td><td>31.5516</td><td>-6.1778</td><td>55.6</td><td>0.93</td><td>0.12</td><td>3.64</td><td>0.57</td><td>N260-2</td></tr><tr><td>NIKA2-150 J020606.7-061357</td><td>N150-2</td><td>5.3</td><td>31.5281</td><td>-6.2327</td><td>161.4</td><td>0.88</td><td>0.15</td><td>4.06</td><td>0.73</td><td>N260-3</td></tr><tr><td>NIKA2-150 J020627.4-061011</td><td>N150-3</td><td>4.8</td><td>31.6140</td><td>-6.1697</td><td>247.3</td><td>1.04</td><td>0.20</td><td>3.23</td><td>0.90</td><td>N260-8</td></tr><tr><td>NIKA2-150 J020624.9-061056</td><td>N150-4</td><td>4.8</td><td>31.6039</td><td>-6.1824</td><td>200.3</td><td>0.83</td><td>0.17</td><td>2.11</td><td>0.75</td><td></td></tr><tr><td>NIKA2-150 J020618.6-061123</td><td>N150-5</td><td>4.4</td><td>31.5775</td><td>-6.1898</td><td>102.6</td><td>0.56</td><td>0.13</td><td>4.41</td><td>0.59</td><td>N260-1</td></tr><tr><td>NIKA2-150 J020622.5-060800</td><td>N150-6</td><td>4.0</td><td>31.5937</td><td>-6.1334</td><td>267.7</td><td>0.91</td><td>0.22</td><td>4.55</td><td>1.02</td><td>N260-4</td></tr><tr><td colspan="12"><strong>Field of XLSSC 102</strong></td></tr><tr><td colspan="12">Detection at 260 GHz, counterparts at 150 GHz</td></tr><tr><td>NIKA2-260 J020517.7-044037</td><td>N260-1</td><td>5.6</td><td>31.3239</td><td>-4.6770</td><td>90.3</td><td>3.40</td><td>0.61</td><td>0.38</td><td>0.15</td><td>N150-4</td></tr><tr><td>NIKA2-260 J020459.7-043852</td><td>N260-2</td><td>4.9</td><td>31.2486</td><td>-4.6478</td><td>263.7</td><td>6.07</td><td>1.15</td><td>0.92</td><td>0.27</td><td></td></tr><tr><td>NIKA2-260 J020522.4-043903</td><td>N260-3</td><td>4.7</td><td>31.3434</td><td>-4.6509</td><td>76.9</td><td>2.84</td><td>0.59</td><td>0.61</td><td>0.14</td><td>N150-2</td></tr><tr><td>NIKA2-260 J020502.6-043824</td><td>N260-4</td><td>4.4</td><td>31.2607</td><td>-4.6401</td><td>224.2</td><td>4.31</td><td>0.93</td><td>0.41</td><td>0.22</td><td></td></tr><tr><td>NIKA2-260 J020509.2-044100</td><td>N260-5</td><td>4.3</td><td>31.2881</td><td>-4.6834</td><td>165.9</td><td>3.32</td><td>0.75</td><td>0.30</td><td>0.18</td><td></td></tr><tr><td>NIKA2-260 J020520.6-043843</td><td>N260-6</td><td>4.2</td><td>31.3357</td><td>-4.6454</td><td>54.5</td><td>2.50</td><td>0.57</td><td>0.34</td><td>0.14</td><td>RS-4</td></tr><tr><td colspan="12">Detection at 150 GHz, counterparts at 260 GHz</td></tr><tr><td>NIKA2-150 J020511.8-044305</td><td>N150-1</td><td>4.7</td><td>31.2991</td><td>-4.7182</td><td>252.2</td><td>1.20</td><td>0.25</td><td>2.95</td><td>1.05</td><td></td></tr><tr><td>NIKA2-150 J020522.3-043905</td><td>N150-2</td><td>4.6</td><td>31.3429</td><td>-4.6516</td><td>75.2</td><td>0.63</td><td>0.14</td><td>2.67</td><td>0.59</td><td>N260-3</td></tr><tr><td>NIKA2-150 J020536.1-043748</td><td>N150-3</td><td>4.4</td><td>31.4006</td><td>-4.6301</td><td>292.9</td><td>1.46</td><td>0.30</td><td>5.05</td><td>1.30</td><td></td></tr><tr><td>NIKA2-150 J020517.6-044047</td><td>N150-4</td><td>4.2</td><td>31.3235</td><td>-4.6798</td><td>100.3</td><td>0.56</td><td>0.15</td><td>2.36</td><td>0.62</td><td>N260-1</td></tr></tbody></table>

Notes. † distance from the cluster reference center.
<table><caption>Table B.2. Radio sources identified around the three clusters with GMRT.</caption><thead><tr><th>Name</th><th>Label</th><th>S/N</th><th>R.A.<br>[deg]</th><th>Dec.<br>[deg]</th><th>Distance<br>[arcsec]</th><th>F<sub>610 MHz</sub><br>[mJy]</th><th>ΔF<sub>610 MHz</sub><br>[mJy]</th><th>α<sub>610-1400 MHz</sub></th><th>F<sub>150 GHz</sub>(α<sub>mean</sub>)<br>[mJy]</th><th>F<sub>150 GHz</sub>(α<sub>mean</sub> + σ<sub>σ</sub>)<br>[mJy]</th><th>F<sub>150 GHz</sub>(α<sub>610-1400 MHz</sub>)<br>[mJy]</th></tr></thead><tbody><tr><td colspan="13"><strong>Field of XLSSC 072</strong></td></tr><tr><td>XXL-GMRT J021511.4-034309</td><td>RS-1</td><td>2628.3</td><td>33.7979</td><td>-3.7192</td><td>188.8</td><td>313.29</td><td>0.23</td><td>0.60</td><td>5.05</td><td>32.79</td><td>11.52</td></tr><tr><td>XXL-GMRT J021536.1-034423</td><td>RS-2</td><td>357.6</td><td>33.9008</td><td>-3.7399</td><td>189.2</td><td>28.52</td><td>0.12</td><td>0.96</td><td>0.46</td><td>2.99</td><td>0.14</td></tr><tr><td>XXL-GMRT J021522.5-034441</td><td>RS-3</td><td>145.9</td><td>33.8440</td><td>-3.7447</td><td>70.7</td><td>11.74</td><td>0.08</td><td>0.98</td><td>0.19</td><td>1.23</td><td>0.05</td></tr><tr><td>XXL-GMRT J021516.7-034555</td><td>RS-4</td><td>37.0</td><td>33.8197</td><td>-3.7654</td><td>178.8</td><td>2.94</td><td>0.08</td><td></td><td>0.05</td><td>0.31</td><td></td></tr><tr><td>XXL-GMRT J021519.5-034756</td><td>RS-5</td><td>31.2</td><td>33.8313</td><td>-3.7991</td><td>271.6</td><td>2.39</td><td>0.08</td><td></td><td>0.04</td><td>0.25</td><td></td></tr><tr><td>XXL-GMRT J021534.2-034002</td><td>RS-6</td><td>28.0</td><td>33.8925</td><td>-3.6673</td><td>260.7</td><td>3.87</td><td>0.13</td><td></td><td>0.06</td><td>0.40</td><td></td></tr><tr><td>XXL-GMRT J021509.3-034357</td><td>RS-7</td><td>27.3</td><td>33.7890</td><td>-3.7326</td><td>220.4</td><td>2.31</td><td>0.08</td><td></td><td>0.04</td><td>0.24</td><td></td></tr><tr><td>XXL-GMRT J021530.4-034041</td><td>RS-8</td><td>26.2</td><td>33.8768</td><td>-3.6781</td><td>197.5</td><td>2.23</td><td>0.08</td><td></td><td>0.04</td><td>0.23</td><td></td></tr><tr><td>XXL-GMRT J021541.7-033931</td><td>RS-9</td><td>18.0</td><td>33.9239</td><td>-3.6587</td><td>359.4</td><td>1.64</td><td>0.09</td><td></td><td>0.03</td><td>0.17</td><td></td></tr><tr><td>XXL-GMRT J021506.8-034205</td><td>RS-10</td><td>9.9</td><td>33.7786</td><td>-3.7014</td><td>271.4</td><td>0.86</td><td>0.09</td><td></td><td>0.01</td><td>0.09</td><td></td></tr><tr><td>XXL-GMRT J021529.2-034713</td><td>RS-11</td><td>9.5</td><td>33.8720</td><td>-3.7872</td><td>234.1</td><td>1.00</td><td>0.07</td><td></td><td>0.01</td><td>0.07</td><td></td></tr><tr><td>XXL-GMRT J021540.8-034418</td><td>RS-12</td><td>9.4</td><td>33.9202</td><td>-3.7383</td><td>256.0</td><td>0.75</td><td>0.08</td><td></td><td>0.01</td><td>0.08</td><td></td></tr><tr><td>XXL-GMRT J021531.9-033839</td><td>RS-13</td><td>9.0</td><td>33.8830</td><td>-3.6442</td><td>317.4</td><td>0.78</td><td>0.09</td><td></td><td>0.01</td><td>0.08</td><td></td></tr><tr><td>XXL-GMRT J021533.7-034025</td><td>RS-14</td><td>8.9</td><td>33.8906</td><td>-3.6737</td><td>238.2</td><td>0.71</td><td>0.08</td><td></td><td>0.01</td><td>0.07</td><td></td></tr><tr><td>XXL-GMRT J021530.2-034341</td><td>RS-15</td><td>8.5</td><td>33.8759</td><td>-3.7282</td><td>93.4</td><td>0.55</td><td>0.06</td><td></td><td>0.01</td><td>0.06</td><td></td></tr><tr><td colspan="13"><strong>Field of XLSSC 100</strong></td></tr><tr><td>XXL-GMRT J020619.5-061147</td><td>RS-1</td><td>115.7</td><td>31.5816</td><td>-6.1966</td><td>117.4</td><td>8.14</td><td>0.07</td><td>0.83</td><td>0.13</td><td>0.85</td><td>0.08</td></tr><tr><td>XXL-GMRT J020611.3-061616</td><td>RS-2</td><td>51.3</td><td>31.5474</td><td>-6.2712</td><td>281.6</td><td>3.36</td><td>0.07</td><td></td><td>0.05</td><td>0.35</td><td></td></tr><tr><td>XXL-GMRT J020611.1-061102</td><td>RS-3</td><td>22.5</td><td>31.5465</td><td>-6.1840</td><td>33.6</td><td>1.71</td><td>0.08</td><td></td><td>0.03</td><td>0.18</td><td></td></tr><tr><td>XXL-GMRT J020555.8-060920</td><td>RS-4</td><td>14.6</td><td>31.4828</td><td>-6.1558</td><td>272.2</td><td>1.00</td><td>0.07</td><td></td><td>0.02</td><td>0.10</td><td></td></tr><tr><td>XXL-GMRT J020620.7-061629</td><td>RS-5</td><td>13.2</td><td>31.5866</td><td>-6.2749</td><td>324.1</td><td>0.77</td><td>0.06</td><td></td><td>0.01</td><td>0.08</td><td></td></tr><tr><td>XXL-GMRT J020613.9-061001</td><td>RS-6</td><td>11.9</td><td>31.5580</td><td>-6.1671</td><td>98.6</td><td>0.90</td><td>0.08</td><td></td><td>0.01</td><td>0.09</td><td></td></tr><tr><td>XXL-GMRT J020618.3-060742</td><td>RS-7</td><td>10.4</td><td>31.5766</td><td>-6.1285</td><td>252.3</td><td>0.83</td><td>0.08</td><td></td><td>0.01</td><td>0.09</td><td></td></tr><tr><td>XXL-GMRT J020615.6-060940</td><td>RS-8</td><td>8.3</td><td>31.5653</td><td>-6.1612</td><td>128.5</td><td>0.56</td><td>0.07</td><td></td><td>0.01</td><td>0.06</td><td></td></tr><tr><td>XXL-GMRT J020606.6-061303</td><td>RS-9</td><td>8.3</td><td>31.5278</td><td>-6.2178</td><td>117.2</td><td>0.48</td><td>0.06</td><td></td><td>0.01</td><td>0.05</td><td></td></tr><tr><td>XXL-GMRT J020614.8-061556</td><td>RS-10</td><td>8.1</td><td>31.5620</td><td>-6.2658</td><td>266.2</td><td>0.48</td><td>0.06</td><td></td><td>0.01</td><td>0.05</td><td></td></tr><tr><td>XXL-GMRT J020602.0-061139</td><td>RS-11</td><td>7.5</td><td>31.5084</td><td>-6.1942</td><td>145.4</td><td>0.45</td><td>0.06</td><td></td><td>0.01</td><td>0.05</td><td></td></tr><tr><td colspan="13"><strong>Field of XLSSC 102</strong></td></tr><tr><td>XXL-GMRT J020537.2-043904</td><td>RS-1</td><td>228.3</td><td>31.4054</td><td>-4.6511</td><td>299.3</td><td>12.86</td><td>0.09</td><td>0.8</td><td>0.21</td><td>1.35</td><td>0.16</td></tr><tr><td>XXL-GMRT J020523.5-043441</td><td>RS-2</td><td>71.9</td><td>31.3480</td><td>-4.5781</td><td>281.9</td><td>3.34</td><td>0.05</td><td></td><td>0.05</td><td>0.35</td><td></td></tr><tr><td>XXL-GMRT J020528.7-044132</td><td>RS-3</td><td>30.3</td><td>31.3696</td><td>-4.6924</td><td>224.3</td><td>1.60</td><td>0.05</td><td></td><td>0.03</td><td>0.17</td><td></td></tr><tr><td>XXL-GMRT J020520.6-043843</td><td>RS-4</td><td>24.2</td><td>31.3360</td><td>-4.6454</td><td>55.6</td><td>1.24</td><td>0.05</td><td></td><td>0.02</td><td>0.13</td><td></td></tr><tr><td>XXL-GMRT J020457.2-044308</td><td>RS-5</td><td>13.3</td><td>31.2386</td><td>-4.7191</td><td>384.6</td><td>0.68</td><td>0.05</td><td></td><td>0.01</td><td>0.07</td><td></td></tr><tr><td>XXL-GMRT J020520.6-044118</td><td>RS-6</td><td>8.8</td><td>31.3361</td><td>-4.6886</td><td>141.1</td><td>0.47</td><td>0.05</td><td></td><td>0.01</td><td>0.05</td><td></td></tr><tr><td>XXL-GMRT J020523.6-044028</td><td>RS-7</td><td>7.8</td><td>31.3485</td><td>-4.6746</td><td>125.1</td><td>0.42</td><td>0.05</td><td></td><td>0.01</td><td>0.04</td><td></td></tr><tr><td>XXL-GMRT J020520.5-044031</td><td>RS-8</td><td>7.6</td><td>31.3356</td><td>-4.6755</td><td>97.7</td><td>2.18</td><td>0.05</td><td></td><td>0.04</td><td>0.23</td><td></td></tr><tr><td>XXL-GMRT J020519.8-044006</td><td>RS-9</td><td>7.3</td><td>31.3327</td><td>-4.6683</td><td>70.1</td><td>2.15</td><td>0.05</td><td></td><td>0.03</td><td>0.22</td><td></td></tr></tbody></table>

Notes. The parameters $\alpha_{\text{mean}} = -0.75$ and $\sigma_{\alpha} = 0.34$ are the mean and standard deviation of the spectral indices measured by matching GMRT 610 MHz data and NVSS 1400 MHz data in the XXL survey (Paper XXIX). The parameter $\alpha_{610-1400\text{MHz}}$ is the measured spectral index for the given source when detected in the NVSS (Condon et al. 1998).
<table><caption>Table B.2. Radio sources identified around the three clusters with GMRT.</caption><thead><tr><th>Name</th><th>Label</th><th>S/N</th><th>R.A.<br>[deg]</th><th>Dec.<br>[deg]</th><th>Distance<br>[arcsec]</th><th>F<sub>610 MHz</sub><br>[mJy]</th><th>ΔF<sub>610 MHz</sub><br>[mJy]</th><th>α<sub>610-1400 MHz</sub></th><th>F<sub>150 GHz</sub>(α<sub>mean</sub>)<br>[mJy]</th><th>F<sub>150 GHz</sub>(α<sub>mean</sub> + σ<sub>σ</sub>)<br>[mJy]</th><th>F<sub>150 GHz</sub>(α<sub>610-1400 MHz</sub>)<br>[mJy]</th></tr></thead><tbody><tr><td colspan="13"><strong>Field of XLSSC 072</strong></td></tr><tr><td>XXL-GMRT J021511.4-034309</td><td>RS-1</td><td>2628.3</td><td>33.7979</td><td>-3.7192</td><td>188.8</td><td>313.29</td><td>0.23</td><td>0.60</td><td>5.05</td><td>32.79</td><td>11.52</td></tr><tr><td>XXL-GMRT J021536.1-034423</td><td>RS-2</td><td>357.6</td><td>33.9008</td><td>-3.7399</td><td>189.2</td><td>28.52</td><td>0.12</td><td>0.96</td><td>0.46</td><td>2.99</td><td>0.14</td></tr><tr><td>XXL-GMRT J021522.5-034441</td><td>RS-3</td><td>145.9</td><td>33.8440</td><td>-3.7447</td><td>70.7</td><td>11.74</td><td>0.08</td><td>0.98</td><td>0.19</td><td>1.23</td><td>0.05</td></tr><tr><td>XXL-GMRT J021516.7-034555</td><td>RS-4</td><td>37.0</td><td>33.8197</td><td>-3.7654</td><td>178.8</td><td>2.94</td><td>0.08</td><td></td><td>0.05</td><td>0.31</td><td></td></tr><tr><td>XXL-GMRT J021519.5-034756</td><td>RS-5</td><td>31.2</td><td>33.8313</td><td>-3.7991</td><td>271.6</td><td>2.39</td><td>0.08</td><td></td><td>0.04</td><td>0.25</td><td></td></tr><tr><td>XXL-GMRT J021534.2-034002</td><td>RS-6</td><td>28.0</td><td>33.8925</td><td>-3.6673</td><td>260.7</td><td>3.87</td><td>0.13</td><td></td><td>0.06</td><td>0.40</td><td></td></tr><tr><td>XXL-GMRT J021509.3-034357</td><td>RS-7</td><td>27.3</td><td>33.7890</td><td>-3.7326</td><td>220.4</td><td>2.31</td><td>0.08</td><td></td><td>0.04</td><td>0.24</td><td></td></tr><tr><td>XXL-GMRT J021530.4-034041</td><td>RS-8</td><td>26.2</td><td>33.8768</td><td>-3.6781</td><td>197.5</td><td>2.23</td><td>0.08</td><td></td><td>0.04</td><td>0.23</td><td></td></tr><tr><td>XXL-GMRT J021541.7-033931</td><td>RS-9</td><td>18.0</td><td>33.9239</td><td>-3.6587</td><td>359.4</td><td>1.64</td><td>0.09</td><td></td><td>0.03</td><td>0.17</td><td></td></tr><tr><td>XXL-GMRT J021506.8-034205</td><td>RS-10</td><td>9.9</td><td>33.7786</td><td>-3.7014</td><td>271.4</td><td>0.86</td><td>0.09</td><td></td><td>0.01</td><td>0.09</td><td></td></tr><tr><td>XXL-GMRT J021529.2-034713</td><td>RS-11</td><td>9.5</td><td>33.8720</td><td>-3.7872</td><td>234.1</td><td>1.00</td><td>0.07</td><td></td><td>0.01</td><td>0.07</td><td></td></tr><tr><td>XXL-GMRT J021540.8-034418</td><td>RS-12</td><td>9.4</td><td>33.9202</td><td>-3.7383</td><td>256.0</td><td>0.75</td><td>0.08</td><td></td><td>0.01</td><td>0.08</td><td></td></tr><tr><td>XXL-GMRT J021531.9-033839</td><td>RS-13</td><td>9.0</td><td>33.8830</td><td>-3.6442</td><td>317.4</td><td>0.78</td><td>0.09</td><td></td><td>0.01</td><td>0.08</td><td></td></tr><tr><td>XXL-GMRT J021533.7-034025</td><td>RS-14</td><td>8.9</td><td>33.8906</td><td>-3.6737</td><td>238.2</td><td>0.71</td><td>0.08</td><td></td><td>0.01</td><td>0.07</td><td></td></tr><tr><td>XXL-GMRT J021530.2-034341</td><td>RS-15</td><td>8.5</td><td>33.8759</td><td>-3.7282</td><td>93.4</td><td>0.55</td><td>0.06</td><td></td><td>0.01</td><td>0.06</td><td></td></tr><tr><td colspan="13"><strong>Field of XLSSC 100</strong></td></tr><tr><td>XXL-GMRT J020619.5-061147</td><td>RS-1</td><td>115.7</td><td>31.5816</td><td>-6.1966</td><td>117.4</td><td>8.14</td><td>0.07</td><td>0.83</td><td>0.13</td><td>0.85</td><td>0.08</td></tr><tr><td>XXL-GMRT J020611.3-061616</td><td>RS-2</td><td>51.3</td><td>31.5474</td><td>-6.2712</td><td>281.6</td><td>3.36</td><td>0.07</td><td></td><td>0.05</td><td>0.35</td><td></td></tr><tr><td>XXL-GMRT J020611.1-061102</td><td>RS-3</td><td>22.5</td><td>31.5465</td><td>-6.1840</td><td>33.6</td><td>1.71</td><td>0.08</td><td></td><td>0.03</td><td>0.18</td><td></td></tr><tr><td>XXL-GMRT J020555.8-060920</td><td>RS-4</td><td>14.6</td><td>31.4828</td><td>-6.1558</td><td>272.2</td><td>1.00</td><td>0.07</td><td></td><td>0.02</td><td>0.10</td><td></td></tr><tr><td>XXL-GMRT J020620.7-061629</td><td>RS-5</td><td>13.2</td><td>31.5866</td><td>-6.2749</td><td>324.1</td><td>0.77</td><td>0.06</td><td></td><td>0.01</td><td>0.08</td><td></td></tr><tr><td>XXL-GMRT J020613.9-061001</td><td>RS-6</td><td>11.9</td><td>31.5580</td><td>-6.1671</td><td>98.6</td><td>0.90</td><td>0.08</td><td></td><td>0.01</td><td>0.09</td><td></td></tr><tr><td>XXL-GMRT J020618.3-060742</td><td>RS-7</td><td>10.4</td><td>31.5766</td><td>-6.1285</td><td>252.3</td><td>0.83</td><td>0.08</td><td></td><td>0.01</td><td>0.09</td><td></td></tr><tr><td>XXL-GMRT J020615.6-060940</td><td>RS-8</td><td>8.3</td><td>31.5653</td><td>-6.1612</td><td>128.5</td><td>0.56</td><td>0.07</td><td></td><td>0.01</td><td>0.06</td><td></td></tr><tr><td>XXL-GMRT J020606.6-061303</td><td>RS-9</td><td>8.3</td><td>31.5278</td><td>-6.2178</td><td>117.2</td><td>0.48</td><td>0.06</td><td></td><td>0.01</td><td>0.05</td><td></td></tr><tr><td>XXL-GMRT J020614.8-061556</td><td>RS-10</td><td>8.1</td><td>31.5620</td><td>-6.2658</td><td>266.2</td><td>0.48</td><td>0.06</td><td></td><td>0.01</td><td>0.05</td><td></td></tr><tr><td>XXL-GMRT J020602.0-061139</td><td>RS-11</td><td>7.5</td><td>31.5084</td><td>-6.1942</td><td>145.4</td><td>0.45</td><td>0.06</td><td></td><td>0.01</td><td>0.05</td><td></td></tr><tr><td colspan="13"><strong>Field of XLSSC 102</strong></td></tr><tr><td>XXL-GMRT J020537.2-043904</td><td>RS-1</td><td>228.3</td><td>31.4054</td><td>-4.6511</td><td>299.3</td><td>12.86</td><td>0.09</td><td>0.8</td><td>0.21</td><td>1.35</td><td>0.16</td></tr><tr><td>XXL-GMRT J020523.5-043441</td><td>RS-2</td><td>71.9</td><td>31.3480</td><td>-4.5781</td><td>281.9</td><td>3.34</td><td>0.05</td><td></td><td>0.05</td><td>0.35</td><td></td></tr><tr><td>XXL-GMRT J020528.7-044132</td><td>RS-3</td><td>30.3</td><td>31.3696</td><td>-4.6924</td><td>224.3</td><td>1.60</td><td>0.05</td><td></td><td>0.03</td><td>0.17</td><td></td></tr><tr><td>XXL-GMRT J020520.6-043843</td><td>RS-4</td><td>24.2</td><td>31.3360</td><td>-4.6454</td><td>55.6</td><td>1.24</td><td>0.05</td><td></td><td>0.02</td><td>0.13</td><td></td></tr><tr><td>XXL-GMRT J020457.2-044308</td><td>RS-5</td><td>13.3</td><td>31.2386</td><td>-4.7191</td><td>384.6</td><td>0.68</td><td>0.05</td><td></td><td>0.01</td><td>0.07</td><td></td></tr><tr><td>XXL-GMRT J020520.6-044118</td><td>RS-6</td><td>8.8</td><td>31.3361</td><td>-4.6886</td><td>141.1</td><td>0.47</td><td>0.05</td><td></td><td>0.01</td><td>0.05</td><td></td></tr><tr><td>XXL-GMRT J020523.6-044028</td><td>RS-7</td><td>7.8</td><td>31.3485</td><td>-4.6746</td><td>125.1</td><td>0.42</td><td>0.05</td><td></td><td>0.01</td><td>0.04</td><td></td></tr><tr><td>XXL-GMRT J020520.5-044031</td><td>RS-8</td><td>7.6</td><td>31.3356</td><td>-4.6755</td><td>97.7</td><td>2.18</td><td>0.05</td><td></td><td>0.04</td><td>0.23</td><td></td></tr><tr><td>XXL-GMRT J020519.8-044006</td><td>RS-9</td><td>7.3</td><td>31.3327</td><td>-4.6683</td><td>70.1</td><td>2.15</td><td>0.05</td><td></td><td>0.03</td><td>0.22</td><td></td></tr></tbody></table>

Notes. The parameters $\alpha_{\text{mean}} = -0.75$ and $\sigma_{\sigma} = 0.34$ are the mean and standard deviation of the spectral indices measured by matching GMRT 610 MHz data and NVSS 1400 MHz data in the XXL survey (Paper XXIX). The parameter $\alpha_{610-1400\text{MHz}}$ is the measured spectral index for the given source when detected in the NVSS (Condon et al. 1998).
<figure><img src="image_12.png" /><figcaption>**Fig. B.2.** Herschel/PACS images of XLSSC 072 at 500, 350, and 250 µm (from top to bottom). Black contours give the S/N in units of 1σ, starting at 3σ. The gray circles in the bottom left corner show the PACS beam FWHM in each band. White dashed contours show the NIKA2 150 GHz contours at -3, -5, -7, and -9 σ. Magenta and cyan contours show the 3, 4, and 5σ NIKA2 S/N at 150 and 260 GHz, respectively. The blue and red crosses indicate the point sources identified at 150 and 260 GHz in the NIKA2 data.</figcaption></figure>
<figure><img src="image_13.png" /><figcaption>**Fig. B.2.** Herschel/PACS images of XLSSC 072 at 500, 350, and 250 µm (from top to bottom). Black contours give the S/N in units of 1σ, starting at 3σ. The gray circles in the bottom left corner show the PACS beam FWHM in each band. White dashed contours show the NIKA2 150 GHz contours at -3, -5, -7, and -9 σ. Magenta and cyan contours show the 3, 4, and 5σ NIKA2 S/N at 150 and 260 GHz, respectively. The blue and red crosses indicate the point sources identified at 150 and 260 GHz in the NIKA2 data.</figcaption></figure>
<figure><img src="image_13.png" /><figcaption>Fig. B.3. Comparison of 150 GHz surface brightness profiles when accounting (or not) for the point sources.</figcaption></figure>

## Appendix C: Thermal electron density profiles

The electron density profiles of the three clusters derived from XMM-Newton data are reported in Figure C.1.

<figure><img src="image_14.png" /><figcaption>Fig. C.1. Thermal electron density profile, from left to right, of XLSSC 072, XLSSC 100, and XLSSC 102. The solid lines provide the best profiles and the 68% confidence interval. The 1000 MC realizations are also provided via transparent markings to show the dispersion.</figcaption></figure>

## Appendix D: Thermodynamic profile diagnosis

This appendix presents the temperature, entropy, and gas fraction profiles of our target clusters, which we use as a thermodynamic diagnosis of the dynamical state and to address systematic effects in the mass measurement. They are computed within the framework of the MINOT software (Adam et al. 2020) given the pressure and the density inferred from the SZ and X-ray data. As a reference, we use the pressure profile inferred from the gNFW model fit to the data. We note that detailed discussions regarding the recovered temperature, entropy and gas fraction were presented in Paper XLIV for XLSSC 102. The thermodynamic profiles reported here are in agreement with our previous analysis, but they differ slightly due to the updated density profile.

The entropy and temperature are given by

$$K_e(r) = \frac{P_e(r)}{n_e(r)^{5/3}} \qquad (D.1)$$

and

$$k_B T(r) = \frac{P_e(r)}{n_e(r)}, \qquad (D.2)$$

respectively. The gas fraction is computed as

$$f_{\text{gas}}(r) = \frac{M_{\text{gas}}(r)}{M_{\text{tot}}(r)}, \qquad (D.3)$$

where the gas mass is obtained by integrating the electron density profile as

$$M_{\text{gas}}(r) = 4\pi \int_{0}^{r} \mu_{e} m_{p} n_{e}(r') r'^{2} dr', \qquad (D.4)$$

with the mean molecular weight $\mu_e \approx 1.15$ and $m_p$ is the proton mass. The total mass is related to the hydrostatic mass via

$$M_{\text{tot}}(r) = \frac{M_{\text{HSE}}(r)}{(1 - b_{\text{HSE}})}, \qquad (D.5)$$

where $b_{\text{HSE}}$ is the hydrostatic mass bias. The entropy, temperature and gas fraction profiles are shown in Figure D.1 for the three clusters.

The three entropy profiles are compared to the self-similar baseline, in the case where only gravitational effect are present
<figure><img src="image_14.png" /><figcaption>Fig. B.3. Comparison of 150 GHz surface brightness profiles when accounting (or not) for the point sources.</figcaption></figure>

## Appendix C: Thermal electron density profiles

The electron density profiles of the three clusters derived from XMM-Newton data are reported in Figure C.1.

<figure><img src="image_15.png" /><figcaption>Fig. C.1. Thermal electron density profile, from left to right, of XLSSC 072, XLSSC 100, and XLSSC 102. The solid lines provide the best profiles and the 68% confidence interval. The 1000 MC realizations are also provided via transparent markings to show the dispersion.</figcaption></figure>

## Appendix D: Thermodynamic profile diagnosis

This appendix presents the temperature, entropy, and gas fraction profiles of our target clusters, which we use as a thermodynamic diagnosis of the dynamical state and to address systematic effects in the mass measurement. They are computed within the framework of the MINOT software (Adam et al. 2020) given the pressure and the density inferred from the SZ and X-ray data. As a reference, we use the pressure profile inferred from the gNFW model fit to the data. We note that detailed discussions regarding the recovered temperature, entropy and gas fraction were presented in Paper XLIV for XLSSC 102. The thermodynamic profiles reported here are in agreement with our previous analysis, but they differ slightly due to the updated density profile.

The entropy and temperature are given by

$$K_e(r) = \frac{P_e(r)}{n_e(r)^{5/3}} \qquad (D.1)$$

and

$$k_B T(r) = \frac{P_e(r)}{n_e(r)}, \qquad (D.2)$$

respectively. The gas fraction is computed as

$$f_{\text{gas}}(r) = \frac{M_{\text{gas}}(r)}{M_{\text{tot}}(r)}, \qquad (D.3)$$

where the gas mass is obtained by integrating the electron density profile as

$$M_{\text{gas}}(r) = 4\pi \int_{0}^{r} \mu_{e} m_{p} n_{e}(r') r'^{2} dr', \qquad (D.4)$$

with the mean molecular weight $\mu_e \approx 1.15$ and $m_p$ is the proton mass. The total mass is related to the hydrostatic mass via

$$M_{\text{tot}}(r) = \frac{M_{\text{HSE}}(r)}{(1 - b_{\text{HSE}})}, \qquad (D.5)$$

where $b_{\text{HSE}}$ is the hydrostatic mass bias. The entropy, temperature and gas fraction profiles are shown in Figure D.1 for the three clusters.

The three entropy profiles are compared to the self-similar baseline, in the case where only gravitational effect are present
(Voit et al. 2005), given by $K(r) \propto (r/R_{500})^{1.1}$. The masses used for the comparison are obtained from the $Y_X$ proxy. We can observe that all clusters present a large excess entropy in the core, within $r \le 300$ kpc, of about 300 keV cm$^2$. Such a feature is typical for disturbed systems (Pratt et al. 2010). This indicates that all three systems are dynamically disturbed, most likely because of the presence of merging events, in agreement with our imaging analysis (see Section 3). We note that XLSSC 102 agrees with a flat entropy profile at all scales. Beyond $r \sim 300$ kpc, the profile is even lower than the self-similar baseline, although uncertainties are becoming very large. As the self-similar baseline corresponds to a minimal heat injection from gravitational collapse, such a feature is not expected. This could indicate an excess in the density profile caused by inhomogeneities in the gas, as observed for other nearby clusters with high-quality data (Tchernin et al. 2016), which would also bias low the HSE mass estimates. We note that this feature is reduced when using the direct HSE mass measurement since they are lower, but it does not entirely disappear.

The three temperature profiles agree with that of merging systems, with a profile decreasing from the core to the outskirt. We also report the projected temperature measured within 300 kpc from the core by Paper III and Paper XX. The same measurement from Paper XLVIII is also reported for XLSSC 072. Given the uncertainties and the fact that the two measurements are not strictly comparable, good qualitative agreement is observed for XLSSC 100 and XLSSC 102. On the other hand, our SZ plus X-ray-derived temperature for XLSSC 072 is in qualitative agreement with the one from Paper XLVIII, higher than but still comparable to the one from Paper III, but in significant disagreement with the one from Paper XX. As the $Y_X$-based masses are using Paper III temperatures, we conclude that while no significant issue is observed with XLSSC 102 and XLSSC 100, the

$Y_X$-derived mass for XLSSC 072 might be biased depending on the choice of the temperature measurement. For instance, using our SZ plus X-ray measurement would increase the mass within $\sim 2\sigma$.

The gas fraction profiles increase from the center to the outskirts, in agreement with the expected baryon depletion generally expected in the center. As we can see from Equation D.3 and D.5, the gas fraction depends on the hydrostatic mass bias, which is set to $b_{HSE} = 0$ here. On the other hand, the universal gas fraction at $R_{500}$ is given by

$$f_{\text{gas,univ}}(R_{500}) = \frac{\Omega_{\text{b}}}{\Omega_{\text{m}}} Y_{b,500} - f_{\star,500}, \qquad (\text{D.6})$$

with $Y_{b,500} \approx 0.85$ being the baryon depletion factor and where $f_{\star,500} \approx 0.015$ accounts for the baryons that have condensed into stars (see Eckert et al. 2019 for details). Assuming that the profiles should reach the universal gas fraction at $R_{500}$, it is possible to estimate the value of $b_{HSE}$. As we can see, the three profiles reach the cosmic baryon fraction at about $R_{500}$. While XLSSC 072 and XLSSC 100 are in rough agreement with the expected value, XLSSC 102 presents a gas fraction that is higher by about $2\sigma$. This might indicate that this system presents a high hydrostatic mass bias, in agreement with the fact that it is the most disturbed of our targets and already indicated thanks to the entropy profile. More quantitatively, a value of $1 - b_{HSE}$ of 0.85, 1.0, and 0.5 would bring XLSSC 072, XLSSC 100, and XLSSC 102 to the expected universal gas fraction value at $R_{500}$, respectively.

Given the entropy, temperature, and gas fraction profiles, we conclude that all three clusters are dynamically disturbed. Additionally, we find that the $Y_X$-derived masses may be biased low for XLSSC 072 (within $2\sigma$), and that direct HSE-derived masses may be biased low by up to a factor of two for XLSSC 102.

<figure><img src="image_15.png" /><figcaption>**Fig. D.1.** Thermodynamic profiles. **Left:** Entropy profiles derived by combining X-ray and SZ measurement. The self-similar baseline, accounting only for gravitational effects (Voit et al. 2005), is reported given the masses derived via the $Y_X - M$ relation (as well as $R_{500}$ shown by the vertical dashed lines). **Middle:** Temperature profiles derived by combining X-ray and SZ measurement. X-ray spectroscopic measurement from Paper III and Paper XX, obtained within 300 kpc, are reported. For XLSSC 072, we also report the result from Paper XLVIII, also obtained with 300 kpc from X-ray spectroscopy. **Right:** Gas fraction profiles derived by combining X-ray and SZ measurement, assuming $b_{HSE} = 0$. The mean cosmic value from Planck Collaboration XIII (2016) is reported for reference.</figcaption></figure>
(Voit et al. 2005), given by $K(r) \propto (r/R_{500})^{1.1}$. The masses used for the comparison are obtained from the $Y_X$ proxy. We can observe that all clusters present a large excess entropy in the core, within $r \le 300$ kpc, of about 300 keV cm$^2$. Such a feature is typical for disturbed systems (Pratt et al. 2010). This indicates that all three systems are dynamically disturbed, most likely because of the presence of merging events, in agreement with our imaging analysis (see Section 3). We note that XLSSC 102 agrees with a flat entropy profile at all scales. Beyond $r \sim 300$ kpc, the profile is even lower than the self-similar baseline, although uncertainties are becoming very large. As the self-similar baseline corresponds to a minimal heat injection from gravitational collapse, such a feature is not expected. This could indicate an excess in the density profile caused by inhomogeneities in the gas, as observed for other nearby clusters with high-quality data (Tchernin et al. 2016), which would also bias low the HSE mass estimates. We note that this feature is reduced when using the direct HSE mass measurement since they are lower, but it does not entirely disappear.

The three temperature profiles agree with that of merging systems, with a profile decreasing from the core to the outskirt. We also report the projected temperature measured within 300 kpc from the core by Paper III and Paper XX. The same measurement from Paper XLVIII is also reported for XLSSC 072. Given the uncertainties and the fact that the two measurements are not strictly comparable, good qualitative agreement is observed for XLSSC 100 and XLSSC 102. On the other hand, our SZ plus X-ray-derived temperature for XLSSC 072 is in qualitative agreement with the one from Paper XLVIII, higher than but still comparable to the one from Paper III, but in significant disagreement with the one from Paper XX. As the $Y_X$-based masses are using Paper III temperatures, we conclude that while no significant issue is observed with XLSSC 102 and XLSSC 100, the

$Y_X$-derived mass for XLSSC 072 might be biased depending on the choice of the temperature measurement. For instance, using our SZ plus X-ray measurement would increase the mass within $\sim 2\sigma$.

The gas fraction profiles increase from the center to the outskirts, in agreement with the expected baryon depletion generally expected in the center. As we can see from Equation D.3 and D.5, the gas fraction depends on the hydrostatic mass bias, which is set to $b_{HSE} = 0$ here. On the other hand, the universal gas fraction at $R_{500}$ is given by

$$f_{\text{gas,univ}}(R_{500}) = \frac{\Omega_{\text{b}}}{\Omega_{\text{m}}} Y_{b,500} - f_{\star,500}, \qquad (\text{D.6})$$

with $Y_{b,500} \approx 0.85$ being the baryon depletion factor and where $f_{\star,500} \approx 0.015$ accounts for the baryons that have condensed into stars (see Eckert et al. 2019 for details). Assuming that the profiles should reach the universal gas fraction at $R_{500}$, it is possible to estimate the value of $b_{HSE}$. As we can see, the three profiles reach the cosmic baryon fraction at about $R_{500}$. While XLSSC 072 and XLSSC 100 are in rough agreement with the expected value, XLSSC 102 presents a gas fraction that is higher by about $2\sigma$. This might indicate that this system presents a high hydrostatic mass bias, in agreement with the fact that it is the most disturbed of our targets and already indicated thanks to the entropy profile. More quantitatively, a value of $1 - b_{HSE}$ of 0.85, 1.0, and 0.5 would bring XLSSC 072, XLSSC 100, and XLSSC 102 to the expected universal gas fraction value at $R_{500}$, respectively.

Given the entropy, temperature, and gas fraction profiles, we conclude that all three clusters are dynamically disturbed. Additionally, we find that the $Y_X$-derived masses may be biased low for XLSSC 072 (within $2\sigma$), and that direct HSE-derived masses may be biased low by up to a factor of two for XLSSC 102.

<figure><img src="image_16.png" /><figcaption>**Fig. D.1.** Thermodynamic profiles. **Left:** Entropy profiles derived by combining X-ray and SZ measurement. The self-similar baseline, accounting only for gravitational effects (Voit et al. 2005), is reported given the masses derived via the $Y_X - M$ relation (as well as $R_{500}$ shown by the vertical dashed lines). **Middle:** Temperature profiles derived by combining X-ray and SZ measurement. X-ray spectroscopic measurement from Paper III and Paper XX, obtained within 300 kpc, are reported. For XLSSC 072, we also report the result from Paper XLVIII, also obtained with 300 kpc from X-ray spectroscopy. **Right:** Gas fraction profiles derived by combining X-ray and SZ measurement, assuming $b_{HSE} = 0$. The mean cosmic value from Planck Collaboration XIII (2016) is reported for reference.</figcaption></figure>
**Appendix E: SZ residuals**

The comparison between the SZ map and their best-fit gNFW
model is shown in Figure E.1. While some residual structures

can reach about 3σ due to deviation from spherical symmetry,
the best-fit model provides a fair description of the data in all
cases.

<figure><img src="image_16.png" /><figcaption>Fig. E.1. NIKA2 SZ maps (top), best-fit gNFW model (middle), and residual (bottom) maps for the three clusters. The contours are given in units of 2σ starting at ±2σ.</figcaption></figure>
**Appendix E: SZ residuals**

The comparison between the SZ map and their best-fit gNFW
model is shown in Figure E.1. While some residual structures

can reach about 3σ due to deviation from spherical symmetry,
the best-fit model provides a fair description of the data in all
cases.

<figure><img src="image_17.png" /><figcaption>Fig. E.1. NIKA2 SZ maps (top), best-fit gNFW model (middle), and residual (bottom) maps for the three clusters. The contours are given in units of 2σ starting at ±2σ.</figcaption></figure>