<figure><img src="image_28.png" /><figcaption>**Fig. 30.** Distribution on the sky of the clean sample of 270 905 DR3 RR Lyrae stars that were confirmed and characterised with the SOS Cep&RRL pipeline in galactic coordinates. The sample comprises 200,294 known RR Lyrae stars (Gold Sample) and 70,611 new discoveries by *Gaia*.</figcaption></figure>

<figure><img src="image_29.png" /><figcaption>**Fig. 31.** PA (270 905 sources; top panel), $\phi_{21}$ vs. *P* (251 423 sources; centre panel) and $\phi_{31}$ vs. *P* (136 015 sources; bottom panel) diagrams of the RR Lyrae stars in the DR3 clean sample. New discoveries by *Gaia* are marked with blue dots; 70 611 are shown in the top panel, 70 447 in the central panel, and 5317 in the bottom panel.</figcaption></figure>

parameter-richest catalogue of all-sky RR Lyrae stars published so far in the magnitude range from $\langle G \rangle = 7.64$ mag (the magnitude of RR Lyr itself; sourceid 2125982599343482624) and $\langle G \rangle = 21.14$ mag (the magnitude of star 658193189673442944, the faintest RR Lyrae in the catalogue). The DR3 RR Lyrae catalogue along with known RR Lyrae stars confirmed with the SOS pipeline, but for which the SOS periods differ from the literature periods (see Sect. 3.1), increases the census of RR Lyrae stars in our Galaxy and its close companions to about 370 000 within the limiting magnitude of *Gaia*.

*Gaia* Data Release 4 (DR4) will be based on 66 months of data. It will therefore allow the SOS Cep&RRL pipeline to better determine the pulsation period(s) and characterise RR Lyrae stars and Cepheids more effectively. The pipeline is currently being redesigned and simplified, and a number of changes will be implemented to improve the processing in view of *Gaia* DR4. Some of these changes are briefly outlined below.

1. Tests are in progress how the algorithm can be improved for the period determination (currently the Lomb-Scargle method, see Sect. 2) so that the number of spurious period detections is reduced, particularly when several peaks of similar power are present in the power spectrum of the sources.

2. The number of harmonics for modelling the light curves of RRc stars with a well-sampled light/RV curve will be increased to more than two to increase the number of RR Lyrae stars for which the $\phi_{31}$ Fourier parameter is available.

3. The skewness of the light curve and the time of rise to maximum light ($\phi$-rise time) will be adopted in addition to the position in the PA diagram to distinguish RRab from RRc stars, particularly in the short-period regime ($P < 0.4$ d).

4. Luminosity-metallicity (LZ) and PW and PW-metallicity (PWZ) relations in the *Gaia* bands, calibrated on *Gaia* parallaxes (e.g. those published by Garofalo et al. 2022) will be adopted in the pipeline to classify RR Lyrae stars with reliable parallax values.

5. CMDs in absolute magnitude, colour-colour diagrams, and the comparison with theoretical instability strips will be used to improve the source classification, the derivation of
<figure><img src="image_29.png" /><figcaption>**Fig. 30.** Distribution on the sky of the clean sample of 270 905 DR3 RR Lyrae stars that were confirmed and characterised with the SOS Cep&RRL pipeline in galactic coordinates. The sample comprises 200,294 known RR Lyrae stars (Gold Sample) and 70,611 new discoveries by *Gaia*.</figcaption></figure>

<figure><img src="image_30.png" /><figcaption>**Fig. 31.** PA (270 905 sources; top panel), $\phi_{21}$ vs. *P* (251 423 sources; centre panel) and $\phi_{31}$ vs. *P* (136 015 sources; bottom panel) diagrams of the RR Lyrae stars in the DR3 clean sample. New discoveries by *Gaia* are marked with blue dots; 70 611 are shown in the top panel, 70 447 in the central panel, and 5317 in the bottom panel.</figcaption></figure>

parameter-richest catalogue of all-sky RR Lyrae stars published so far in the magnitude range from $\langle G \rangle = 7.64$ mag (the magnitude of RR Lyr itself; sourceid 2125982599343482624) and $\langle G \rangle = 21.14$ mag (the magnitude of star 658193189673442944, the faintest RR Lyrae in the catalogue). The DR3 RR Lyrae catalogue along with known RR Lyrae stars confirmed with the SOS pipeline, but for which the SOS periods differ from the literature periods (see Sect. 3.1), increases the census of RR Lyrae stars in our Galaxy and its close companions to about 370 000 within the limiting magnitude of *Gaia*.

*Gaia* Data Release 4 (DR4) will be based on 66 months of data. It will therefore allow the SOS Cep&RRL pipeline to better determine the pulsation period(s) and characterise RR Lyrae stars and Cepheids more effectively. The pipeline is currently being redesigned and simplified, and a number of changes will be implemented to improve the processing in view of *Gaia* DR4. Some of these changes are briefly outlined below.

1. Tests are in progress how the algorithm can be improved for the period determination (currently the Lomb-Scargle method, see Sect. 2) so that the number of spurious period detections is reduced, particularly when several peaks of similar power are present in the power spectrum of the sources.

2. The number of harmonics for modelling the light curves of RRc stars with a well-sampled light/RV curve will be increased to more than two to increase the number of RR Lyrae stars for which the $\phi_{31}$ Fourier parameter is available.

3. The skewness of the light curve and the time of rise to maximum light ($\phi$-rise time) will be adopted in addition to the position in the PA diagram to distinguish RRab from RRc stars, particularly in the short-period regime ($P < 0.4$ d).

4. Luminosity-metallicity (LZ) and PW and PW-metallicity (PWZ) relations in the *Gaia* bands, calibrated on *Gaia* parallaxes (e.g. those published by Garofalo et al. 2022) will be adopted in the pipeline to classify RR Lyrae stars with reliable parallax values.

5. CMDs in absolute magnitude, colour-colour diagrams, and the comparison with theoretical instability strips will be used to improve the source classification, the derivation of
<figure><img src="image_30.png" /><figcaption>**Fig. 32.** Distribution on the sky of 70 611 DR3 RR Lyrae stars that are new discoveries by *Gaia* in galactic coordinates. The sources are colour-coded according to the number of epochs in the *G*-band light curves as encoded in the colour scale on the right.</figcaption></figure>

<figure><img src="image_31.png" /><figcaption>**Fig. 33.** Map in galactic coordinates of 133 559 RR Lyrae stars in the DR3 clean catalogue for which individual photometric metallicity estimates obtained with the SOS pipeline are published in the *Gaia* DR3 *variOOKlyrae* table. The sources are colour-coded according to their metallicity ([Fe/H]) as encoded in the colour scale on the right.</figcaption></figure>

<figure><img src="image_32.png" /><figcaption>**Fig. 34.** Same as in Fig. 33, but showing only 88 440 RR Lyrae stars with an error in metallicity $\sigma_{[Fe/H]} \le 0.46$ dex.</figcaption></figure>
<figure><img src="image_31.png" /><figcaption>**Fig. 32.** Distribution on the sky of 70 611 DR3 RR Lyrae stars that are new discoveries by *Gaia* in galactic coordinates. The sources are colour-coded according to the number of epochs in the *G*-band light curves as encoded in the colour scale on the right.</figcaption></figure>

<figure><img src="image_32.png" /><figcaption>**Fig. 33.** Map in galactic coordinates of 133 559 RR Lyrae stars in the DR3 clean catalogue for which individual photometric metallicity estimates obtained with the SOS pipeline are published in the *Gaia* DR3 *variOOKlyrae* table. The sources are colour-coded according to their metallicity ([Fe/H]) as encoded in the colour scale on the right.</figcaption></figure>

<figure><img src="image_33.png" /><figcaption>**Fig. 34.** Same as in Fig. 33, but showing only 88 440 RR Lyrae stars with an error in metallicity $\sigma_{[Fe/H]} \le 0.46$ dex.</figcaption></figure>
<figure><img src="image_33.png" /><figcaption>**Fig. 35.** PA diagram of the 133 559 RR Lyrae stars with a metallicity estimate. The sources are colour-coded according to their metal abundance ([Fe/H]) as encoded in the colour scale on the right.</figcaption></figure>

<figure><img src="image_34.png" /><figcaption>**Fig. 36.** Map in galactic coordinates of 142 660 RRab stars with individual G absorption values estimated with the SOS pipeline. The sources are colour-coded according to their A(G) values as encoded in the colour scale on the right.</figcaption></figure>

intrinsic parameters (e.g. effective temperatures), and the removal of contaminants.

6. We will test different calibrations of the relations that are used to estimate photometric metallicities from the $\phi_{31}$ Fourier parameter and the pulsation period of RR Lyrae stars, and we hope to derive new [Fe/H] – $\phi_{31}$ – *P* relations that are directly calibrated on the Gaia data using a sample of RR Lyrae stars with metallicity determinations from high-resolution spectra covering the whole parameter space spanned by these variable stars.

7. We will revise the computation of errors in metallicity because they may currently be overestimated.

8. Test will be made to derive astrophysical parameters (metallicities, gravities, and $T_{eff}$ values) to best select the template spectra for the cross-correlation to measure radial velocities of RR Lyrae stars. The time series of BP/RP spectra will also be used.

To conclude, the SOS Cep&RRL clean catalogue of 270 905 RR Lyrae stars published with Gaia DR3 already represents a significant step forward in the construction of a complete, homogeneous, and parameter-rich catalogue of all-sky RR Lyrae stars within the limiting magnitude of Gaia. This has been lacking so far. We anticipate that this RR Lyrae catalogue will be consolidated and further improved with Gaia DR4.

*Acknowledgements.* This work has made use of data from the ESA space mission Gaia, processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC has been provided by national institutions participating in the Gaia Multilateral Agreement. In particular, the Italian participation in DPAC has been supported by Istituto Nazionale di Astrofisica (INAF) and the Agenzia Spaziale Italiana (ASI) through grants I/037/08/0, I/058/10/0, 2014-025-R.0, 2014-025-R.1.2015 and 2018-24-HH.0 to INAF (PI M. G. Lattanzi), the Swiss participation by the Swiss State Secretariat for Education, Research and Innovation through the “Activités Nationales Complémentaires”. The work was supported in part by the French Centre National de la Recherche Scientifique (CNRS), the Centre National d'Etudes Spatiales (CNES), the Institut
<figure><img src="image_34.png" /><figcaption>**Fig. 35.** PA diagram of the 133 559 RR Lyrae stars with a metallicity estimate. The sources are colour-coded according to their metal abundance ([Fe/H]) as encoded in the colour scale on the right.</figcaption></figure>

<figure><img src="image_35.png" /><figcaption>**Fig. 36.** Map in galactic coordinates of 142 660 RRab stars with individual G absorption values estimated with the SOS pipeline. The sources are colour-coded according to their A(G) values as encoded in the colour scale on the right.</figcaption></figure>

intrinsic parameters (e.g. effective temperatures), and the removal of contaminants.

6. We will test different calibrations of the relations that are used to estimate photometric metallicities from the $\phi_{31}$ Fourier parameter and the pulsation period of RR Lyrae stars, and we hope to derive new [Fe/H] – $\phi_{31}$ – *P* relations that are directly calibrated on the Gaia data using a sample of RR Lyrae stars with metallicity determinations from high-resolution spectra covering the whole parameter space spanned by these variable stars.

7. We will revise the computation of errors in metallicity because they may currently be overestimated.

8. Test will be made to derive astrophysical parameters (metallicities, gravities, and $T_{eff}$ values) to best select the template spectra for the cross-correlation to measure radial velocities of RR Lyrae stars. The time series of BP/RP spectra will also be used.

To conclude, the SOS Cep&RRL clean catalogue of 270 905 RR Lyrae stars published with Gaia DR3 already represents a significant step forward in the construction of a complete, homogeneous, and parameter-rich catalogue of all-sky RR Lyrae stars within the limiting magnitude of Gaia. This has been lacking so far. We anticipate that this RR Lyrae catalogue will be consolidated and further improved with Gaia DR4.

*Acknowledgements.* This work has made use of data from the ESA space mission Gaia, processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC has been provided by national institutions participating in the Gaia Multilateral Agreement. In particular, the Italian participation in DPAC has been supported by Istituto Nazionale di Astrofisica (INAF) and the Agenzia Spaziale Italiana (ASI) through grants I/037/08/0, I/058/10/0, 2014-025-R.0, 2014-025-R.1.2015 and 2018-24-HH.0 to INAF (PI M. G. Lattanzi), the Swiss participation by the Swiss State Secretariat for Education, Research and Innovation through the “Activités Nationales Complémentaires”. The work was supported in part by the French Centre National de la Recherche Scientifique (CNRS), the Centre National d'Etudes Spatiales (CNES), the Institut
des Sciences de l'Univers (INSU) through the Service National d'Observation (SNO) Gaia. UK community participation in this work has been supported by funding from the UK Space Agency, and from the UK Science and Technology Research Council. RA has been funded by the DLR (German space agency) via grants 50QG0602, 50QG1001, 50QG1403, and 50QG201. The Gaia mission website is: http://www.cosmos.esa.int/gaia. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. We warmly thank O. Creevey, A. Recio-Blanco and M. Fouesneau for advises on the use of products from the GSP_Spec and GSP_Phot modules of the Apis pipeline, D. Harrison for running the SEAPipe pipeline on the catalogue of RR Lyrae stars produced by the SOS Cep&RRL pipeline and P. Montegriffo for the development and maintenance of the GRATIS software. In this study we have largely made use of TOPCAT (Taylor 2005).

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## References

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# Appendix A: RVS radial velocities

## A.1. Tables with the source-level parameters of 51 Cepheids and 45 RR Lyrae stars for which this information is lacking in the *gaia_source* table of the Gaia DR3 archive.

<table><caption>**Table A.1.** Source-level information for 51 Cepheids for which the all-epoch-combined RV was deemed of insufficient quality.</caption><thead><tr><th>Gaia sourceid</th><th>rv_template_teff</th><th>rv_template_logg</th><th>rv_template_feh</th><th>rv_atm_param_origin</th><th>grvs_mag</th><th>grvs_mag_error</th><th>radvelinvalidreason</th></tr></thead><tbody><tr><td>5351161399793209984</td><td>5 000</td><td>1.5</td><td>0.25</td><td>222</td><td>6.281</td><td>0.043</td><td>D</td></tr><tr><td>5329352998951582976</td><td>6 000</td><td>1</td><td>-0.25</td><td>222</td><td>6.492</td><td>0.056</td><td>D</td></tr><tr><td>5355057622307185280</td><td>5 500</td><td>3.5</td><td>0</td><td>333</td><td>6.607</td><td>0.038</td><td>D</td></tr><tr><td>5338036117182452096</td><td>6 250</td><td>2</td><td>0.25</td><td>222</td><td>6.815</td><td>0.070</td><td>D</td></tr><tr><td>473043922712140928</td><td>5 500</td><td>4.5</td><td>0</td><td>333</td><td>6.834</td><td>0.047</td><td>D</td></tr></tbody></table>

**Notes.** radVelInvalidReason provides the reason why the source-level parameters are excluded from publication. D: Double-lined detected in more than 10% of the epochs; P: variations in the spectral-sample flux from epoch to epoch; H: hot star; CF: poor cross-correlation-function; T: potential template mismatch; E=the error of the all-epochs combined radial velocity is larger than 40 km s⁻¹ (see Sartoretti et al. 2022, Chap. 6, for details). This table is available in its entirety at the CDS.

<table><caption>**Table A.2.** Same as in table A.1, but for 45 RR Lyrae stars.</caption><thead><tr><th>Gaia sourceid</th><th>rv_template_teff</th><th>rv_template_logg</th><th>rv_template_feh</th><th>rv_atm_param_origin</th><th>grvs_mag</th><th>grvs_mag_error</th><th>radvelinvalidreason</th></tr></thead><tbody><tr><td>2857456211775108480</td><td>6 500</td><td>3</td><td>0</td><td>222</td><td>9.076</td><td>0.127</td><td>D</td></tr><tr><td>2142052889490819328</td><td>6 250</td><td>3</td><td>-0.5</td><td>444</td><td>9.324</td><td>0.083</td><td>T</td></tr><tr><td>234108363683247616</td><td>6 500</td><td>3</td><td>-0.25</td><td>555</td><td>9.411</td><td>0.091</td><td>D</td></tr><tr><td>6686289122295812736</td><td>6 250</td><td>3.5</td><td>-0.5</td><td>444</td><td>9.534</td><td>0.051</td><td>D</td></tr><tr><td>1858568795812429056</td><td>6 000</td><td>3</td><td>-0.5</td><td>444</td><td>10.242</td><td>0.059</td><td>D</td></tr></tbody></table>

**Notes.** This table is available in its entirety at the CDS.
# Appendix A: RVS radial velocities

## A.1. Tables with the source-level parameters of 51 Cepheids and 45 RR Lyrae stars for which this information is lacking in the *gaia_source* table of the Gaia DR3 archive.

<table><caption>**Table A.1.** Source-level information for 51 Cepheids for which the all-epoch-combined RV was deemed of insufficient quality.</caption><thead><tr><th>Gaia sourceid</th><th>rv_template_teff</th><th>rv_template_logg</th><th>rv_template_feh</th><th>rv_atm_param_origin</th><th>grvs_mag</th><th>grvs_mag_error</th><th>radvelinvalidreason</th></tr></thead><tbody><tr><td>5351161399793209984</td><td>5 000</td><td>1.5</td><td>0.25</td><td>222</td><td>6.281</td><td>0.043</td><td>D</td></tr><tr><td>5329352998951582976</td><td>6 000</td><td>1</td><td>-0.25</td><td>222</td><td>6.492</td><td>0.056</td><td>D</td></tr><tr><td>5355057622307185280</td><td>5 500</td><td>3.5</td><td>0</td><td>333</td><td>6.607</td><td>0.038</td><td>D</td></tr><tr><td>5338036117182452096</td><td>6 250</td><td>2</td><td>0.25</td><td>222</td><td>6.815</td><td>0.070</td><td>D</td></tr><tr><td>473043922712140928</td><td>5 500</td><td>4.5</td><td>0</td><td>333</td><td>6.834</td><td>0.047</td><td>D</td></tr></tbody></table>

**Notes.** radVelInvalidReason provides the reason why the source-level parameters are excluded from publication. D: Double-lined detected in more than 10% of the epochs; P: variations in the spectral-sample flux from epoch to epoch; H: hot star; CF: poor cross-correlation-function; T: potential template mismatch; E=the error of the all-epochs combined radial velocity is larger than 40 km s⁻¹ (see Sartoretti et al. 2022, Chap. 6, for details). This table is available in its entirety at the CDS.

<table><caption>**Table A.2.** Same as in table A.1, but for 45 RR Lyrae stars.</caption><thead><tr><th>Gaia sourceid</th><th>rv_template_teff</th><th>rv_template_logg</th><th>rv_template_feh</th><th>rv_atm_param_origin</th><th>grvs_mag</th><th>grvs_mag_error</th><th>radvelinvalidreason</th></tr></thead><tbody><tr><td>2857456211775108480</td><td>6 500</td><td>3</td><td>0</td><td>222</td><td>9.076</td><td>0.127</td><td>D</td></tr><tr><td>2142052889490819328</td><td>6 250</td><td>3</td><td>-0.5</td><td>444</td><td>9.324</td><td>0.083</td><td>T</td></tr><tr><td>234108363683247616</td><td>6 500</td><td>3</td><td>-0.25</td><td>555</td><td>9.411</td><td>0.091</td><td>D</td></tr><tr><td>6686289122295812736</td><td>6 250</td><td>3.5</td><td>-0.5</td><td>444</td><td>9.534</td><td>0.051</td><td>D</td></tr><tr><td>1858568795812429056</td><td>6 000</td><td>3</td><td>-0.5</td><td>444</td><td>10.242</td><td>0.059</td><td>D</td></tr></tbody></table>

**Notes.** This table is available in its entirety at the CDS.
<table><caption>**Table A.3.** Information for 19 RR Lyrae stars with high accuracy RV curves available in the literature.</caption><thead><tr><th>Source_id<br>(1)</th><th>Name<br>(2)</th><th>Mode<br>(3)</th><th>Period<br>days<br>(4)</th><th>⟨G⟩<br>mag<br>(5)</th><th>N<sub>RVS</sub><br>(6)</th><th>Amp(RV)<br>km s<sup>-1</sup><br>(7)</th><th>γ<sub>(RVS+L<sub>IT</sub>)</sub><br>km s<sup>-1</sup><br>(8)</th><th>γ<sub>L<sub>IT</sub></sub><br>km s<sup>-1</sup><br>(9)</th><th>[Fe/H]<sub>L<sub>IT</sub></sub><br>dex<br>(10)</th><th>⟨T<sub>eff</sub>⟩<sub>L<sub>IT</sub></sub><br>K<br>(11)</th><th>⟨logg⟩<sub>L<sub>IT</sub></sub><br>km s<sup>-1</sup><br>(12)</th><th>Ref1<br>(13)</th><th>Ref2<br>(14)</th><th>Notes<br>(15)</th><th>Ins.<br>(16)</th></tr></thead><tbody><tr><td>1286188056265485952</td><td>RS Boo</td><td>RRab</td><td>0.3773523</td><td>10.34</td><td>28</td><td>67.38</td><td>-3.96 (2.57)</td><td>-3.7</td><td>-0.50</td><td>6.795</td><td>3.261<sup>(a,b)</sup></td><td>8</td><td>8</td><td>Blaz.</td><td>b</td></tr><tr><td>1492230556717187456</td><td>TV Boo</td><td>RRc</td><td>0.312551</td><td>10.91</td><td>34</td><td>27.07</td><td>-102.44 (5.00)</td><td>-104.0</td><td>-2.20±0.15</td><td>7.057</td><td>2.90</td><td>1</td><td>1</td><td>-</td><td>b</td></tr><tr><td>6884361748289023488</td><td>YZ Cap</td><td>RRc</td><td>0.2734508</td><td>11.22</td><td>27</td><td>26.19</td><td>-106.91 (2.29)</td><td>-106.5 ± 1.6</td><td>-1.25</td><td>7.280±100</td><td>3.00±0.10</td><td>2</td><td>10</td><td>-</td><td>a</td></tr><tr><td>2558296724402139392</td><td>RR Cet</td><td>RRab</td><td>0.5530296</td><td>9.61</td><td>30</td><td>62.79</td><td>-74.42 (2.50)</td><td>-74.6/-75.1</td><td>-1.25±0.10</td><td>6.434</td><td>2.71</td><td>1.6</td><td>1</td><td>-</td><td>b</td></tr><tr><td>2414817603803476864</td><td>UU Cet</td><td>RRab</td><td>0.6060755</td><td>11.94</td><td>21</td><td>55.71</td><td>-113.88 (3.10)</td><td>-114.4</td><td>-0.87</td><td>6.290</td><td>2.75<sup>(c,b)</sup></td><td>3</td><td>13</td><td>-</td><td>a</td></tr><tr><td>3546458301374134528</td><td>W Crt</td><td>RRab</td><td>0.4120288</td><td>11.45</td><td>31</td><td>75.76</td><td>59.87 (3.64)</td><td>58.8</td><td>-0.70</td><td>6.715</td><td>2.70<sup>(c)</sup></td><td>4</td><td>4</td><td>-</td><td>c</td></tr><tr><td>1760981190300823808</td><td>DX Del</td><td>RRab</td><td>0.4726188</td><td>9.81</td><td>26</td><td>55.48</td><td>-55.15 (2.80)</td><td>-55.1</td><td>-0.25</td><td>6.512</td><td>2.7±0.2<sup>(d,b)</sup></td><td>5.6</td><td>12</td><td>-</td><td>d,a</td></tr><tr><td>1058066262817534336</td><td>SU Dra</td><td>RRab</td><td>0.6604232</td><td>9.68</td><td>13</td><td>60.63</td><td>-167.08 (1.87)</td><td>-166.9</td><td>-1.60±0.20</td><td>6.433</td><td>2.72</td><td>1</td><td>1</td><td>-</td><td>b</td></tr><tr><td>1683444631038133248</td><td>SW Dra</td><td>RRab</td><td>0.5696720</td><td>10.38</td><td>20</td><td>62.04</td><td>-29.13 (2.57)</td><td>-29.8</td><td>-0.80/-1.40</td><td>6.380±50<sup>c</sup></td><td>2.78±0.10</td><td>2.7</td><td>11.8</td><td>-</td><td>a,b</td></tr><tr><td>2981136563934324224</td><td>RX Eri</td><td>RRab</td><td>0.5872470</td><td>9.56</td><td>26</td><td>67.15</td><td>67.72 (3.89)</td><td>66.4</td><td>-1.40±0.20</td><td>6.326</td><td>2.67</td><td>1</td><td>1</td><td>-</td><td>b</td></tr><tr><td>5117708899055276416</td><td>SS For</td><td>RRab</td><td>0.49544999</td><td>10.10</td><td>28</td><td>62.81</td><td>-109.93 (4.92)</td><td>-111.7</td><td>-1.50</td><td>6.710±50</td><td>2.85±0.10</td><td>2</td><td>11</td><td>Blaz.</td><td>a</td></tr><tr><td>4596935593202765184</td><td>TW Her</td><td>RRab</td><td>0.3996157</td><td>11.22</td><td>27</td><td>72.90</td><td>-3.31 (2.66)</td><td>-4.5</td><td>-0.50</td><td>6.770</td><td>3.424<sup>(a,b)</sup></td><td>8</td><td>8</td><td>-</td><td>b</td></tr><tr><td>648368033223588896</td><td>V Ind</td><td>RRab</td><td>0.4796017</td><td>9.86</td><td>12</td><td>52.83</td><td>202.71 (1.74)</td><td>202.5</td><td>-1.51</td><td>-</td><td>-</td><td>3</td><td>-</td><td>-</td><td>a</td></tr><tr><td>1793460115244988800</td><td>AV Peg</td><td>RRab</td><td>0.3903809</td><td>10.39</td><td>16</td><td>65.68</td><td>-58.22 (1.70)</td><td>-58.7</td><td>0.00±0.10</td><td>6.603</td><td>2.99</td><td>1</td><td>1</td><td>-</td><td>b</td></tr><tr><td>6526559499016401408</td><td>RV Phe</td><td>RRab</td><td>0.5963778</td><td>11.81</td><td>37</td><td>59.72</td><td>99.72 (6.65)</td><td>99.1</td><td>-1.50</td><td>6.370±50/6.290</td><td>2.76±0.10</td><td>2</td><td>10.13</td><td>Blaz.</td><td>a</td></tr><tr><td>6771307454464848768</td><td>V440 Sgr<sup>(f)</sup></td><td>RRab</td><td>0.4774854</td><td>10.23</td><td>10</td><td>76.61</td><td>-60.92 (2.95)</td><td>-61.6</td><td>-1.40</td><td>6.810±50</td><td>2.87±0.10</td><td>2</td><td>10</td><td>-</td><td>a</td></tr><tr><td>4709830423483623808</td><td>W Tuc</td><td>RRab</td><td>0.6422386</td><td>11.34</td><td>18</td><td>69.22</td><td>64.69 (1.90)</td><td>64.60</td><td>-1.35</td><td>6.440</td><td>2.75<sup>(c,b)</sup></td><td>3</td><td>13</td><td>-</td><td>a</td></tr><tr><td>3698725337376560512</td><td>UU Vir</td><td>RRab</td><td>0.4756085</td><td>10.52</td><td>14</td><td>72.32</td><td>-7.80 (2.07)</td><td>-8.2/-7.1</td><td>-0.40±0.10/-0.7</td><td>6.520/6.570</td><td>2.84/3.279<sup>(a,b)</sup></td><td>1.5,8</td><td>1.8</td><td>Bin.</td><td>b</td></tr><tr><td>6045485228725626752</td><td>M4-V32<sup>(g)</sup></td><td>RRab</td><td>0.5791070</td><td>12.90</td><td>34</td><td>63.50</td><td>67.93 (5.31)</td><td>66.4</td><td>-1.3 ± 0.2</td><td>6.324</td><td>2.67</td><td>9</td><td>9</td><td>-</td><td>b</td></tr></tbody></table>

**Notes.** Meaning of the different columns is as follows: (1) Gaia DR3 source id; (2) Literature Name; (3) Pulsation mode (RRab=Fundamental; RRc= First Overtone); (4) Pulsation period (P), as re-evaluated in the present analysis; (5) Intensity-averaged G-band mean magnitude, as derived from the SOS Cep&RRL pipeline; (6) number of valid RVS RV measurements; (7) Peak-to-peak amplitude of the combined RVS and literature RV data. The RVS measurements of TV Boo and M4-V32 were shifted by +5km s⁻¹, those of TW Her and UU Vir by −4 km/s, and those of AV Peg by −3 km/s to better match the corresponding literature data; (8) Centre of mass RV (γ) of the curve obtained by combining RVS and literature RV data, with in parentheses the rms scatter of the modelled RV curve; (9) Literature values for γ; (10) Iron abundance; (11) Mean effective temperature; (12) Mean gravity; (13) References for the literature RV; (14) References for the stellar parameters; (15) Notes: Binary (Bin) and/or Blazhko (Blaz.).; (16) Instrument type: a=CORAVEL; b=spectra; c=image-tube spectrograph; d=photoelectric RV meter. The meaning of the numbers in columns (13) and (14) is as follows: 1=Liu & Janes (1989); 2=Cacciari et al. (1987); 3=Clementini et al. (1990); 4=Skillen et al. (1993); 5=Barnes et al. (1988); 6=Meylan et al. (1986); 7=Jones et al. (1987); 8=Jones et al. (1988); 9=Liu & Janes (1990); 10=Cacciari et al. (1989a); 11=Cacciari et al. (1989b); 12=Skillen et al. (1989); 13=Cacciari et al. (1992); The binarity information is taken from Kervella et al. (2019).<sup>a</sup>Gravity value at φ=0.0.<sup>b</sup>Cacciari et al. (1992) derived a mean gravity of 2.83±0.11 dex by averaging the gravity values inferred from the radii and masses published by Jones et al. (1992), which were derived from the B-W analysis of 18 RRab and 2 RRc stars. This mean gravity value can be used in place of <sup>(a)</sup>, <sup>(c)</sup> and <sup>(d)</sup> or when a <sup>(logg)</sup> value is missing.<sup>c</sup>Constant gravity value adopted in Cacciari et al. (1992) B-W analysis of UU Cet, RV Phe and W Tuc, and in Skillen et al. (1993) analysis of W Crt. <sup>d</sup>2.7±0.2 is the ‘static’ gravity, that is the gravity of an RR Lyrae star were it not pulsating (Fernley et al. 1989). <sup>e</sup>⟨T<sub>eff</sub>⟩=6460 K estimated from the V − K colour by (Jones et al. 1988).<sup>f</sup>The period derived by the SOS pipeline for this star (P<sub>SOS</sub>=0.428933547 d) is incorrect, we provide in the table the correct period (P=0.4774854 d). The ⟨G⟩, Amp(RV) and γ<sub>RVS</sub> values of V440 Sgr listed in the table were computed using the correct period. <sup>g</sup>Two RV measurements from Gaia RVS around the curve maximum are outliers with large errors. They were discarded when computing the Amp(RV) and γ values in columns (7) and (8).
<table><caption>**Table A.3.** Information for 19 RR Lyrae stars with high accuracy RV curves available in the literature.</caption><thead><tr><th>Source_id<br>(1)</th><th>Name<br>(2)</th><th>Mode<br>(3)</th><th>Period<br>days<br>(4)</th><th>⟨G⟩<br>mag<br>(5)</th><th>N<sub>RVS</sub><br>(6)</th><th>Amp(RV)<br>km s<sup>-1</sup><br>(7)</th><th>γ<sub>(RVS+L<sub>IT</sub>)</sub><br>km s<sup>-1</sup><br>(8)</th><th>γ<sub>L<sub>IT</sub></sub><br>km s<sup>-1</sup><br>(9)</th><th>[Fe/H]<sub>L<sub>IT</sub></sub><br>dex<br>(10)</th><th>⟨T<sub>eff</sub>⟩<sub>L<sub>IT</sub></sub><br>K<br>(11)</th><th>⟨logg⟩<sub>L<sub>IT</sub></sub><br>km s<sup>-1</sup><br>(12)</th><th>Ref1<br>(13)</th><th>Ref2<br>(14)</th><th>Notes<br>(15)</th><th>Ins.<br>(16)</th></tr></thead><tbody><tr><td>1286188056265485952</td><td>RS Boo</td><td>RRab</td><td>0.3773523</td><td>10.34</td><td>28</td><td>67.38</td><td>-3.96 (2.57)</td><td>-3.7</td><td>-0.50</td><td>6.795</td><td>3.261<sup>(a,b)</sup></td><td>8</td><td>8</td><td>Blaz.</td><td>b</td></tr><tr><td>1492230556717187456</td><td>TV Boo</td><td>RRc</td><td>0.312551</td><td>10.91</td><td>34</td><td>27.07</td><td>-102.44 (5.00)</td><td>-104.0</td><td>-2.20±0.15</td><td>7.057</td><td>2.90</td><td>1</td><td>1</td><td>-</td><td>b</td></tr><tr><td>6884361748289023488</td><td>YZ Cap</td><td>RRc</td><td>0.2734508</td><td>11.22</td><td>27</td><td>26.19</td><td>-106.91 (2.29)</td><td>-106.5 ± 1.6</td><td>-1.25</td><td>7.280±100</td><td>3.00±0.10</td><td>2</td><td>10</td><td>-</td><td>a</td></tr><tr><td>2558296724402139392</td><td>RR Cet</td><td>RRab</td><td>0.5530296</td><td>9.61</td><td>30</td><td>62.79</td><td>-74.42 (2.50)</td><td>-74.6/-75.1</td><td>-1.25±0.10</td><td>6.434</td><td>2.71</td><td>1.6</td><td>1</td><td>-</td><td>b</td></tr><tr><td>2414817603803476864</td><td>UU Cet</td><td>RRab</td><td>0.6060755</td><td>11.94</td><td>21</td><td>55.71</td><td>-113.88 (3.10)</td><td>-114.4</td><td>-0.87</td><td>6.290</td><td>2.75<sup>(c,b)</sup></td><td>3</td><td>13</td><td>-</td><td>a</td></tr><tr><td>3546458301374134528</td><td>W Crt</td><td>RRab</td><td>0.4120288</td><td>11.45</td><td>31</td><td>75.76</td><td>59.87 (3.64)</td><td>58.8</td><td>-0.70</td><td>6.715</td><td>2.70<sup>(c)</sup></td><td>4</td><td>4</td><td>-</td><td>c</td></tr><tr><td>1760981190300823808</td><td>DX Del</td><td>RRab</td><td>0.4726188</td><td>9.81</td><td>26</td><td>55.48</td><td>-55.15 (2.80)</td><td>-55.1</td><td>-0.25</td><td>6.512</td><td>2.7±0.2<sup>(d,b)</sup></td><td>5.6</td><td>12</td><td>-</td><td>d,a</td></tr><tr><td>1058066262817534336</td><td>SU Dra</td><td>RRab</td><td>0.6604232</td><td>9.68</td><td>13</td><td>60.63</td><td>-167.08 (1.87)</td><td>-166.9</td><td>-1.60±0.20</td><td>6.433</td><td>2.72</td><td>1</td><td>1</td><td>-</td><td>b</td></tr><tr><td>1683444631038133248</td><td>SW Dra</td><td>RRab</td><td>0.5696720</td><td>10.38</td><td>20</td><td>62.04</td><td>-29.13 (2.57)</td><td>-29.8</td><td>-0.80/-1.40</td><td>6.380±50<sup>c</sup></td><td>2.78±0.10</td><td>2.7</td><td>11.8</td><td>-</td><td>a,b</td></tr><tr><td>2981136563934324224</td><td>RX Eri</td><td>RRab</td><td>0.5872470</td><td>9.56</td><td>26</td><td>67.15</td><td>67.72 (3.89)</td><td>66.4</td><td>-1.40±0.20</td><td>6.326</td><td>2.67</td><td>1</td><td>1</td><td>-</td><td>b</td></tr><tr><td>5117708899055276416</td><td>SS For</td><td>RRab</td><td>0.49544999</td><td>10.10</td><td>28</td><td>62.81</td><td>-109.93 (4.92)</td><td>-111.7</td><td>-1.50</td><td>6.710±50</td><td>2.85±0.10</td><td>2</td><td>11</td><td>Blaz.</td><td>a</td></tr><tr><td>4596935593202765184</td><td>TW Her</td><td>RRab</td><td>0.3996157</td><td>11.22</td><td>27</td><td>72.90</td><td>-3.31 (2.66)</td><td>-4.5</td><td>-0.50</td><td>6.770</td><td>3.424<sup>(a,b)</sup></td><td>8</td><td>8</td><td>-</td><td>b</td></tr><tr><td>648368033223588896</td><td>V Ind</td><td>RRab</td><td>0.4796017</td><td>9.86</td><td>12</td><td>52.83</td><td>202.71 (1.74)</td><td>202.5</td><td>-1.51</td><td>-</td><td>-</td><td>3</td><td>-</td><td>-</td><td>a</td></tr><tr><td>1793460115244988800</td><td>AV Peg</td><td>RRab</td><td>0.3903809</td><td>10.39</td><td>16</td><td>65.68</td><td>-58.22 (1.70)</td><td>-58.7</td><td>0.00±0.10</td><td>6.603</td><td>2.99</td><td>1</td><td>1</td><td>-</td><td>b</td></tr><tr><td>6526559499016401408</td><td>RV Phe</td><td>RRab</td><td>0.5963778</td><td>11.81</td><td>37</td><td>59.72</td><td>99.72 (6.65)</td><td>99.1</td><td>-1.50</td><td>6.370±50/6.290</td><td>2.76±0.10</td><td>2</td><td>10.13</td><td>Blaz.?</td><td>a</td></tr><tr><td>6771307454464848768</td><td>V440 Sgr<sup>(f)</sup></td><td>RRab</td><td>0.4774854</td><td>10.23</td><td>10</td><td>76.61</td><td>-60.92 (2.95)</td><td>-61.6</td><td>-1.40</td><td>6.810±50</td><td>2.87±0.10</td><td>2</td><td>10</td><td>-</td><td>a</td></tr><tr><td>4709830423483623808</td><td>W Tuc</td><td>RRab</td><td>0.6422386</td><td>11.34</td><td>18</td><td>69.22</td><td>64.69 (1.90)</td><td>64.60</td><td>-1.35</td><td>6.440</td><td>2.75<sup>(c,b)</sup></td><td>3</td><td>13</td><td>-</td><td>a</td></tr><tr><td>3698725337376560512</td><td>UU Vir</td><td>RRab</td><td>0.4756085</td><td>10.52</td><td>14</td><td>72.32</td><td>-7.80 (2.07)</td><td>-8.2/-7.1</td><td>-0.40±0.10/-0.7</td><td>6.520/6.570</td><td>2.84/3.279<sup>(a,b)</sup></td><td>1.5,8</td><td>1.8</td><td>Bin.?</td><td>b</td></tr><tr><td>6045485228725626752</td><td>M4-V32<sup>(g)</sup></td><td>RRab</td><td>0.5791070</td><td>12.90</td><td>34</td><td>63.50</td><td>67.93 (5.31)</td><td>66.4</td><td>-1.3 ± 0.2</td><td>6.324</td><td>2.67</td><td>9</td><td>9</td><td>-</td><td>b</td></tr></tbody></table>

**Notes.** Meaning of the different columns is as follows: (1) Gaia DR3 source id; (2) Literature Name; (3) Pulsation mode (RRab=Fundamental; RRc= First Overtone); (4) Pulsation period (P), as re-evaluated in the present analysis; (5) Intensity-averaged G-band mean magnitude, as derived from the SOS Cep&RRL pipeline; (6) number of valid RVS RV measurements; (7) Peak-to-peak amplitude of the combined RVS and literature RV data. The RVS measurements of TV Boo and M4-V32 were shifted by +5km s⁻¹, those of TW Her and UU Vir by -4 km/s, and those of AV Peg by -3 km/s to better match the corresponding literature data; (8) Centre of mass RV (γ) of the curve obtained by combining RVS and literature RV data, with in parentheses the rms scatter of the modelled RV curve; (9) Literature values for γ; (10) Iron abundance; (11) Mean effective temperature; (12) Mean gravity; (13) References for the literature RV; (14) References for the stellar parameters; (15) Notes: Binary (Bin) and/or Blazhko (Blaz.); (16) Instrument type: a=CORAVEL; b=spectra; c=image-tube spectrograph; d=photoelectric RV meter. The meaning of the numbers in columns (13) and (14) is as follows: 1=Liu & Janes (1989); 2=Cacciari et al. (1987); 3=Clementini et al. (1990); 4=Skillen et al. (1993); 5=Barnes et al. (1988); 6=Meylan et al. (1986); 7=Jones et al. (1987); 8=Jones et al. (1988); 9=Liu & Janes (1990); 10=Cacciari et al. (1989a); 11=Cacciari et al. (1989b); 12=Skillen et al. (1989); 13=Cacciari et al. (1992); The binarity information is taken from Kervella et al. (2019). aGravity value at φ=0.0. bCacciari et al. (1992) derived a mean gravity of 2.83±0.11 dex by averaging the gravity values inferred from the radii and masses published by Jones et al. (1992), which were derived from the B-W analysis of 18 RRab and 2 RRc stars. This mean gravity value can be used in place of (a), (c) and (d) or when a ⟨logg⟩ value is missing. cConstant gravity value adopted in Cacciari et al. (1992) B-W analysis of UU Cet, RV Phe and W Tuc, and in Skillen et al. (1993) analysis of W Crt. d2.7±0.2 is the 'static' gravity, that is the gravity of an RR Lyrae star were it not pulsating (Fernley et al. 1989). e⟨T<sub>eff</sub>⟩=6460 K estimated from the V - K colour by (Jones et al. 1988). fThe period derived by the SOS pipeline for this star (P<sub>SOS</sub>=0.428933547 d) is incorrect, we provide in the table the correct period (P=0.4774854 d). The ⟨G⟩, Amp(RV) and γ<sub>RVS</sub> values of V440 Sgr listed in the table were computed using the correct period. gTwo RV measurements from Gaia RVS around the curve maximum are outliers with large errors. They were discarded when computing the Amp(RV) and γ values in columns (7) and (8).
## A.2. Comparison of literature and Gaia RV curves for 13 of the 19 RR Lyrae stars for which high-accuracy RVs are available (see Sect. 4.3).

<figure><img src="image_35.png" /><figcaption>**Fig. A.1.** Same as in Fig. 18 for the remaining 13 RR Lyrae stars in the sample of 19 sources discussed in Sect. 4.3. The Gaia RV curves of TW Her and UU Vir were shifted by -4 km/s, the curve of TV Boo was shifted by +5 km/s, and the curve of AV Peg was shifted by -3 km/s to better match the literature RV curves.</figcaption></figure>
A.2. Comparison of literature and Gaia RV curves for 13 of the 19 RR Lyrae stars for which high-accuracy RVs are available (see Sect. 4.3).

<figure><img src="image_36.png" /><figcaption>**Fig. A.1.** Same as in Fig. 18 for the remaining 13 RR Lyrae stars in the sample of 19 sources discussed in Sect. 4.3. The Gaia RV curves of TW Her and UU Vir were shifted by -4 km/s, the curve of TV Boo was shifted by +5 km/s, and the curve of AV Peg was shifted by -3 km/s to better match the literature RV curves.</figcaption></figure>
### A.3. Atlas of the light curves and RV curves for the RR Lyrae stars with RVS time-series data published in DR3.

We show $G$, $G_{BP}$, and $G_{RP}$ light curves and RV curves for a total sample of 1100 sources for which RVS time-series RVs are released in DR3. The sample includes 1096

bona fide RR Lyrae stars and four sources that were reclassified as different variable types during validation. Specifically, source 53376268583351180 was reclassified as DCEP_10 (see Sect. 6.5), and the sources 4130380472726484608, 3062985235999231104, and 573418300979785817 were reclassified as ECLs (see Sect 6.9).

<figure><img src="image_36.png" /><figcaption>**Fig. A.2.** $G_{BP}$, $G$, and $G_{RP}$ light curves and RV curves for RR Lyrae stars with RVS time-series data published in DR3. The atlas is published in its entirety only at the CDS.</figcaption></figure>
### A.3. Atlas of the light curves and RV curves for the RR Lyrae stars with RVS time-series data published in DR3.

We show $G$, $G_{BP}$, and $G_{RP}$ light curves and RV curves for a total sample of 1100 sources for which RVS time-series RVs are released in DR3. The sample includes 1096

bona fide RR Lyrae stars and four sources that were reclassified as different variable types during validation. Specifically, source 53376268583351180 was reclassified as DCEP_10 (see Sect. 6.5), and the sources 4130380472726484608, 3062985235999231104, and 573418300979785817 were reclassified as ECLs (see Sect 6.9).

<figure><img src="image_37.png" /><figcaption>**Fig. A.2.** $G_{BP}$, $G$, and $G_{RP}$ light curves and RV curves for RR Lyrae stars with RVS time-series data published in DR3. The atlas is published in its entirety only at the CDS.</figcaption></figure>
# Appendix B: Tests of the astrophysical parameters for RR Lyrae stars

## B.1. Metallicities

In this section we present comparisons of the SOS Cep&RRL photometric metallicities with metal abundances from high-resolution spectra of RR Lyrae stars in Clementini et al. (1995), Lambert et al. (1996), Pancino et al. (2015), and with the metal abundances reported in column 10 of Table A.3 for the 19 RR Lyrae stars used to validate the RV curves from the RVS.

## B.2. Absorption and metallicity values from the GSP_Phot module of Apsis

RR Lyrae stars have unusually large flux errors in their time-averaged *BP/RP* spectra compared to non-variable sources. The

reason is that when the mean *BP/RP* spectra are computed, the amplitude of the light variation, which can range in the *G* band from ~0.2 mag for RRC to more than one magnitude for RRab stars, enters the computed time-averaged *BP/RP* spectra as an additional flux error. This is clearly shown by the comparison of the S/Ns (median of each sample in each pixel) of the continuous *BP/RP* spectra of a sample of 1000 RR Lyrae stars with 14 < ⟨*G*⟩ < 16 extracted from the *vari Rae* table and the continuous *BP/RP* spectra of a comparison sample composed of 1000 random sources again within 14 < *G* < 16 presented in Fig. B.3.

The larger *BP/RP* flux uncertainties cause larger uncertainties in the temperatures derived for RR Lyrae stars, thus opening space for temperature-extinction degeneracies in the GSP_Phot absorption estimates for RR Lyrae stars and causing large uncertainties and systematic offsets in the GSP_Phot metallicities for these variable stars.

<figure><img src="image_37.png" /><figcaption>**Fig. B.1.** Comparison of the photometric metallicities derived by the SOS Cep&RRL pipeline and the metal abundances from high-resolution spectra of 8 RR Lyrae stars in Clementini et al. (1995) (left panel) and metal abundances from high-resolution spectra of 15 RR Lyrae stars in Lambert et al. (1996) (right panel).</figcaption></figure>

<figure><img src="image_38.png" /><figcaption>**Fig. B.2.** Comparison of the photometric metallicities derived by the SOS Cep&RRL pipeline and the metal abundances from high-resolution spectra of 16 RR Lyrae stars in Pancino et al. (2015) (left panel) and the metal abundances listed in Column 10 of Table A.3 of 19 RR Lyrae stars used to validate the RV curves from the RVS (right panel).</figcaption></figure>
# Appendix B: Tests of the astrophysical parameters for RR Lyrae stars

## B.1. Metallicities

In this section we present comparisons of the SOS Cep&RRL photometric metallicities with metal abundances from high-resolution spectra of RR Lyrae stars in Clementini et al. (1995), Lambert et al. (1996), Pancino et al. (2015), and with the metal abundances reported in column 10 of Table A.3 for the 19 RR Lyrae stars used to validate the RV curves from the RVS.

## B.2. Absorption and metallicity values from the GSP_Phot module of Apsis

RR Lyrae stars have unusually large flux errors in their time-averaged *BP/RP* spectra compared to non-variable sources. The

reason is that when the mean *BP/RP* spectra are computed, the amplitude of the light variation, which can range in the *G* band from ~0.2 mag for RRC to more than one magnitude for RRab stars, enters the computed time-averaged *BP/RP* spectra as an additional flux error. This is clearly shown by the comparison of the S/Ns (median of each sample in each pixel) of the continuous *BP/RP* spectra of a sample of 1000 RR Lyrae stars with 14 < ⟨*G*⟩ < 16 extracted from the *vari raisiae* table and the continuous *BP/RP* spectra of a comparison sample composed of 1000 random sources again within 14 < *G* < 16 presented in Fig. B.3.

The larger *BP/RP* flux uncertainties cause larger uncertainties in the temperatures derived for RR Lyrae stars, thus opening space for temperature-extinction degeneracies in the GSP_Phot absorption estimates for RR Lyrae stars and causing large uncertainties and systematic offsets in the GSP_Phot metallicities for these variable stars.

<figure><img src="image_38.png" /><figcaption>**Fig. B.1.** Comparison of the photometric metallicities derived by the SOS Cep&RRL pipeline and the metal abundances from high-resolution spectra of 8 RR Lyrae stars in Clementini et al. (1995) (left panel) and metal abundances from high-resolution spectra of 15 RR Lyrae stars in Lambert et al. (1996) (right panel).</figcaption></figure>

<figure><img src="image_39.png" /><figcaption>**Fig. B.2.** Comparison of the photometric metallicities derived by the SOS Cep&RRL pipeline and the metal abundances from high-resolution spectra of 16 RR Lyrae stars in Pancino et al. (2015) (left panel) and the metal abundances listed in Column 10 of Table A.3 of 19 RR Lyrae stars used to validate the RV curves from the RVS (right panel).</figcaption></figure>
<figure><img src="image_39.png" /><figcaption>**Fig. B.3.** Comparison of the S/Ns (median of each sample in each pixel) of the continuous BP/RP spectra of a sample of 1000 RR Lyrae stars with $14 < G < 16$ mag extracted from the *vari Rae* table (red line) and the continuous BP/RP spectra of a control sample composed by 1000 random non-variable sources with $14 < G < 16$ mag. The random sources (black line) have a much higher pixel-wise S/N than the RR Lyrae stars (red line), even though both samples are drawn from the same apparent G range.</figcaption></figure>

<figure><img src="image_40.png" /><figcaption>**Fig. B.4.** Same as in Fig. 25, but now the sources are colour-coded according to the GSP_Phot best library [Panel (a)]. The numbers next to each library name indicate how often each library is “best”. The outlier group above the one-to-one relation consists of OB stars and some A stars (although other A stars fall nicely onto the 1-1 relation). Panels (b) to (d) show the results from each library individually (not best) as taken from the *astrophysical_parameters_supp* table in the *Gaia* archive. Panels (b) and (c) show that the MARCS and PHOENIX libraries do not have the outlier group above the identity relation, but for high SOS Cep&RRL A(G) values, the GSP_Phot absorption appears to be lower. The median absolute differences (AD) are also plotted in panels (b) to (d). They are 0.212 mag for MARCS and 0.208 mag for PHOENIX.</figcaption></figure>
<figure><img src="image_40.png" /><figcaption>**Fig. B.3.** Comparison of the S/Ns (median of each sample in each pixel) of the continuous BP/RP spectra of a sample of 1000 RR Lyrae stars with $14 < G < 16$ mag extracted from the *vari Rae* table (red line) and the continuous BP/RP spectra of a control sample composed by 1000 random non-variable sources with $14 < G < 16$ mag. The random sources (black line) have a much higher pixel-wise S/N than the RR Lyrae stars (red line), even though both samples are drawn from the same apparent G range.</figcaption></figure>

<figure><img src="image_41.png" /><figcaption>**Fig. B.4.** Same as in Fig. 25, but now the sources are colour-coded according to the GSP_Phot best library [Panel (a)]. The numbers next to each library name indicate how often each library is “best”. The outlier group above the one-to-one relation consists of OB stars and some A stars (although other A stars fall nicely onto the 1-1 relation). Panels (b) to (d) show the results from each library individually (not best) as taken from the *astrophysical_parameters_supp* table in the *Gaia* archive. Panels (b) and (c) show that the MARCS and PHOENIX libraries do not have the outlier group above the identity relation, but for high SOS Cep&RRL A(G) values, the GSP_Phot absorption appears to be lower. The median absolute differences (AD) are also plotted in panels (b) to (d). They are 0.212 mag for MARCS and 0.208 mag for PHOENIX.</figcaption></figure>
<figure><img src="image_41.png" /></figure>

**Fig. B.5.** Run of the GSP_Phot $T_{\text{eff}}$, pulsation period ($Pf$), and peak-to-peak amplitude in the G band [Amp(G)] of RR Lyrae stars for which both the GSP_Phot and the SOS Cep&RRL G absorption [A(G)] values are available as a function of the difference between the two absorption estimates, using for GSP_Phot only the MARCS library results in the astrophysical_parameters_supp table of the DR3 archive. The absorption differences are clearly unrelated to the pulsation period or the G peak-to-peak amplitude. The top panel clearly shows that large absorption differences are caused by an incorrect temperature in GSP_Phot MARCS. The absorption estimates agree for $6300 \le T_{\text{eff}} \le 6800$ K, which is the typical mean temperature range of RRab stars (see also Column 11 in Table A.3). The variability (0.2-1.0 mag peak-to-peak amplitude in the G band) of the RR Lyrae stars is absorbed as increased flux uncertainties in the time-averaged BP/RP spectra. Through the unusually large BP/RP flux uncertainties, the $\chi^2$ is flattened, and thus space for degeneracies is opened. In particular, a temperature-extinction degeneracy takes place that would explain the difference between the SOS Cep&RRL and the GSP_Phot absorption estimates for RR Lyrae stars.
<figure><img src="image_42.png" /></figure>

**Fig. B.5.** Run of the GSP_Phot $T_{\text{eff}}$, pulsation period ($Pf$), and peak-to-peak amplitude in the G band [Amp(G)] of RR Lyrae stars for which both the GSP_Phot and the SOS Cep&RRL G absorption [A(G)] values are available as a function of the difference between the two absorption estimates, using for GSP_Phot only the MARCS library results in the astrophysical_parameters_supp table of the DR3 archive. The absorption differences are clearly unrelated to the pulsation period or the G peak-to-peak amplitude. The top panel clearly shows that large absorption differences are caused by an incorrect temperature in GSP_Phot MARCS. The absorption estimates agree for $6300 \le T_{\text{eff}} \le 6800$ K, which is the typical mean temperature range of RRab stars (see also Column 11 in Table A.3). The variability (0.2-1.0 mag peak-to-peak amplitude in the G band) of the RR Lyrae stars is absorbed as increased flux uncertainties in the time-averaged BP/RP spectra. Through the unusually large BP/RP flux uncertainties, the $\chi^2$ is flattened, and thus space for degeneracies is opened. In particular, a temperature-extinction degeneracy takes place that would explain the difference between the SOS Cep&RRL and the GSP_Phot absorption estimates for RR Lyrae stars.
## Appendix C: Parameters for 14 RR Lyrae that are missing in the variature table.

not published in the DR3 variature table in Table C.1 (see Sect. 6.6).

We provide the parameters that were computed with the SOS Cep&RRL pipeline for 14 bona fide RR Lyrae stars that were

<table><caption>**Table C.1.** Main parameters computed by the SOS Cep&RRL pipeline for 14 RR Lyrae stars that do not appear in the DR3 variature table (see Sect. 6.6).</caption><caption>Main parameters computed by the SOS Cep&RRL pipeline</caption><thead><tr><th>Source ID</th><th>Type</th><th>Pf<br>σ(Pf)</th><th>P1O<br>σ(P1O)</th><th>E<sup>(a)</sup>(G)</th><th>(G)/(G<sub>BP</sub>)/(G<sub>RP</sub>)</th><th>Amp(G)/G<sub>BP</sub>/(G<sub>RP</sub>)<br>σAmp(G/G<sub>BP</sub>/G<sub>RP</sub>)</th><th>φ<sub>21</sub>(G)<br>σ[φ<sub>21</sub>(G)]</th><th>R<sub>21</sub>(G)<br>σ[R<sub>21</sub>(G)]</th><th>φ<sub>31</sub>(G)<br>σ[φ<sub>31</sub>(G)]</th><th>R<sub>31</sub><br>σ[R<sub>31</sub>(G)]</th><th>[Fe/H]<sup>(b)</sup><br>σ[Fe/H]</th><th>A(G)<sup>(c)</sup><br>σA(G)</th><th>N<sub>G</sub>/G<sub>BP</sub>/G<sub>RP</sub></th></tr></thead><tbody><tr><td>4092009204924599040</td><td>RRc</td><td>-</td><td>0.2581538<br>±5x10<sup>-7</sup></td><td>1716.555440</td><td>15.4824/15.9069/14.866<br>±9.7x10<sup>-4</sup>/±0.0023/±0.0033</td><td>0.126/0.156/0.085<br>±0.002/±0.007/±0.006</td><td>4.806<br>±0.232</td><td>0.070<br>±0.012</td><td>-</td><td>-</td><td>-</td><td>-</td><td>24/22/23</td></tr><tr><td>4120414435009794048</td><td>RRc</td><td>-</td><td>0.256715<br>±1x10<sup>-6</sup></td><td>1748.953931</td><td>17.317/18.136/16.401<br>±0.006/±0.018/0.012</td><td>0.380/0.385/0.303<br>±0.019/±0.040/±0.019</td><td>4.687<br>±0.174</td><td>0.174<br>±0.042</td><td>-</td><td>-</td><td>-</td><td>-</td><td>24/12/13</td></tr><tr><td>4144246349481643392</td><td>RRab</td><td>0.81001<br>±1x10<sup>-5</sup></td><td>-</td><td>1713.903329</td><td>17.216/18.149/16.119<br>±0.003/±0.026/±0.018</td><td>0.225/0.251/0.200<br>±0.013/±0.076/±0.064</td><td>4.859<br>±0.130</td><td>0.281<br>±0.045</td><td>-</td><td>-</td><td>-</td><td>2.827</td><td>25/24/23</td></tr><tr><td>5797652730842515968</td><td>RRc</td><td>-</td><td>0.2167765<br>±4x10<sup>-7</sup></td><td>1700.798893</td><td>16.3430/16.5870/15.8778<br>±7x10<sup>-4</sup>/±0.0056/±0.0030</td><td>0.158/0.197/0.107<br>±0.002/±0.017/±0.008</td><td>4.511<br>±0.182</td><td>0.067<br>±0.012</td><td>-</td><td>-</td><td>-</td><td>-</td><td>56/53/54</td></tr><tr><td>5797917193442176640</td><td>RRc</td><td>-</td><td>0.2637340<br>±4x10<sup>-7</sup></td><td>1701.161373</td><td>15.6366/15.8718/15.2366<br>±0.0005/±0.00196/±0.00245</td><td>0.147/0.170/0.101<br>±0.001/±0.009/±0.010</td><td>4.707<br>±0.130</td><td>0.083<br>±0.010</td><td>-</td><td>-</td><td>-</td><td>-</td><td>57/48/47</td></tr><tr><td>5846086424210395520</td><td>RRc</td><td>-</td><td>0.2933843<br>±5x10<sup>-7</sup></td><td>1700.684493</td><td>16.6451/16.8922/16.2396<br>±0.0008/±0.0036/±0.0035</td><td>0.156/0.186/0.118<br>±0.002/±0.011/±0.010</td><td>5.00<br>±0.178</td><td>0.080<br>±0.015</td><td>-</td><td>-</td><td>-</td><td>-</td><td>52/47/46</td></tr><tr><td>5917239841741208576</td><td>RRab</td><td>0.638600<br>±2x10<sup>-6</sup></td><td>-</td><td>1705.946735</td><td>16.3224/16.6628/15.8031<br>±0.0005/±0.0026/±0.0024</td><td>0.147/0.188/0.116<br>±0.001/±0.009/±0.006</td><td>4.422<br>±0.050</td><td>0.189<br>±0.007</td><td>2.937<br>±0.229</td><td>0.040<br>±0.011</td><td>-0.25<br>±0.344</td><td>0.415</td><td>81/80/76</td></tr><tr><td>5991733644318583424</td><td>RRc</td><td>-</td><td>0.258867<br>±1x10<sup>-6</sup></td><td>1707.080357</td><td>16.444/17.10244/15.636<br>±0.013/±0.004/±0.004</td><td>0.135/0.178/0.123<br>±0.003/±0.014/±0.012</td><td>4.378<br>±0.483</td><td>0.074<br>±0.015</td><td>-</td><td>-</td><td>-</td><td>-</td><td>53/53/50</td></tr><tr><td>6017924835910361344</td><td>RRc</td><td>-</td><td>0.268742<br>±2x10<sup>-6</sup></td><td>1708.808652</td><td>17.762/18.319/17.037<br>±0.002/±0.011/±0.006</td><td>0.214/0.294/0.183<br>±0.007/±0.023/±0.013</td><td>4.847<br>±0.184</td><td>0.178<br>±0.046</td><td>-</td><td>-</td><td>-</td><td>-</td><td>32/32/30</td></tr><tr><td>6069336998880602240</td><td>RRab</td><td>0.73337<br>±5x10<sup>-6</sup></td><td>-</td><td>1699.822497</td><td>16.3183/16.6855/15.7082<br>±0.0008/±0.0157/±0.0057</td><td>0.181/0.265/0.152<br>±0.004/±0.052/±0.019</td><td>4.516<br>±0.087</td><td>0.242<br>±0.020</td><td>-</td><td>-</td><td>-</td><td>0.712</td><td>37/35/36</td></tr><tr><td>6707009423228603904</td><td>RRc</td><td>-</td><td>0.306965<br>±1x10<sup>-6</sup></td><td>1709.373150</td><td>16.16385/16.3367/15.7239<br>±0.0009/±0.0155/±0.0261</td><td>0.154/0.138/0.245<br>±0.022/±0.043/±0.086</td><td>4.778<br>±0.320</td><td>0.048<br>±0.012</td><td>-</td><td>-</td><td>-</td><td>-</td><td>27/25/26</td></tr><tr><td>5935214760885709440</td><td>RRc</td><td>-</td><td>0.340823<br>±4x10<sup>-6</sup></td><td>1706.070130</td><td>19.0373/20.624/17.757<br>±0.004/±0.092/±0.011</td><td>0.158/0.819/0.113<br>±0.018/±0.301/±0.044</td><td>5.373<br>±0.495</td><td>0.193<br>±0.065</td><td>-</td><td>-</td><td>-</td><td>-</td><td>40/24/27</td></tr><tr><td>4362766825101261952</td><td>RRc</td><td>-</td><td>0.2631889<br>±5x10<sup>-7</sup></td><td>1716.317264</td><td>16.3937/16.9315/15.6715<br>±0.0008/±0.0071/±0.0036</td><td>0.140/0.153/0.115<br>±0.002/±0.027/±0.011</td><td>4.849<br>±0.380</td><td>0.0518<br>±0.019</td><td>-</td><td>-</td><td>-</td><td>-</td><td>43/40/41</td></tr><tr><td>5967334102579505664</td><td>RRab</td><td>0.62513<br>±2x10<sup>-5</sup></td><td>-</td><td>1707.700232</td><td>18.426/19.999/17.229<br>±0.005/±0.040/±0.012</td><td>0.130/0.372/0.124<br>±0.013/±0.310/±0.059</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>3.429</td><td>37/38/37</td></tr></tbody></table>

**Notes.** The G, G<sub>BP</sub>, G<sub>RP</sub> time series photometry of these sources can be retrieved from the gaiadr3.variClassifier_results table.

(a) The BJD of the epoch of maximum light is offset by JD 2455197.5 d (= J2010.0). (b) Photometric metal abundance derived from the φ<sub>31</sub> Fourier parameter of the light curve of RR Lyrae stars (see Sects. 5.1 and 7). (c) Absorption in the G band computed from a relation that links the star intrinsic colour to the period and the amplitude of the G-band light variation of RR Lyrae stars (see Sects. 5.3 and 7).
**Appendix C: Parameters for 14 RR Lyrae that are missing in the variature table.**

not published in the DR3 variature table in Table C.1 (see Sect. 6.6).

We provide the parameters that were computed with the SOS Cep&RRL pipeline for 14 bona fide RR Lyrae stars that were

<table><caption>**Table C.1.** Main parameters computed by the SOS Cep&RRL pipeline for 14 RR Lyrae stars that do not appear in the DR3 variature table (see Sect. 6.6).</caption><thead><tr><th rowspan="2">Source ID</th><th rowspan="2">Type</th><th rowspan="2">Pf<br>σ(Pf)</th><th rowspan="2">P10<br>σ(P10)</th><th rowspan="2">E<sup>(a)</sup> (G)</th><th rowspan="2">(G)/(G<sub>BP</sub>)/(G<sub>RP</sub>)</th><th colspan="2">Main parameters computed by the SOS Cep&RRL pipeline</th><th rowspan="2">R<sub>21</sub>(G)<br>σ[φ<sub>21</sub>(G)]</th><th rowspan="2">R<sub>31</sub><br>σ[R<sub>31</sub>(G)]</th><th rowspan="2">[Fe/H]<sup>(b)</sup><br>σ[Fe/H]</th><th rowspan="2">A(G)<sup>(c)</sup><br>σA(G)</th><th rowspan="2">N<sub>G</sub>/G<sub>RP</sub>/G<sub>RP</sub></th></tr><tr><th>Amp(G)/G<sub>BP</sub>/(G<sub>RP</sub>)<br>σAmp(G/G<sub>BP</sub>/G<sub>RP</sub>)</th><th>φ<sub>21</sub>(G)<br>σ[φ<sub>21</sub>(G)]</th></tr></thead><tbody><tr><td>4092009204924599040</td><td>RRc</td><td>-</td><td>0.2581538<br>±5x10<sup>-7</sup></td><td>1716.555440</td><td>15.4824/15.9069/14.866<br>±9.7x10<sup>-4</sup>±0.0023/±0.0033</td><td>0.126/0.156/0.085<br>±0.002/±0.007/±0.006</td><td>4.806<br>±0.232</td><td>0.070<br>±0.012</td><td>-</td><td>-</td><td>-</td><td>24/22/23</td></tr><tr><td>4120414435009794048</td><td>RRc</td><td>-</td><td>0.256715<br>±1x10<sup>-6</sup></td><td>1748.953931</td><td>17.317/18.136/16.401<br>±0.006/±0.018/±0.012</td><td>0.380/0.385/0.303<br>±0.019/±0.040/±0.019</td><td>4.687<br>±0.174</td><td>0.174<br>±0.042</td><td>-</td><td>-</td><td>-</td><td>24/12/13</td></tr><tr><td>4144246349481643392</td><td>RRab</td><td>0.81001<br>±1x10<sup>-5</sup></td><td>-</td><td>1713.903329</td><td>17.216/18.149/16.119<br>±0.003/±0.026/±0.018</td><td>0.225/0.251/0.200<br>±0.013/±0.076/±0.064</td><td>4.859<br>±0.130</td><td>0.281<br>±0.045</td><td>-</td><td>-</td><td>2.827<br>±0.100</td><td>25/24/23</td></tr><tr><td>5797652730842515968</td><td>RRc</td><td>-</td><td>0.2167765<br>±4x10<sup>-7</sup></td><td>1700.798893</td><td>16.3430/16.5870/15.8778<br>±7x10<sup>-4</sup>±0.0056/±0.0030</td><td>0.158/0.197/0.107<br>±0.002/±0.017/±0.008</td><td>4.511<br>±0.182</td><td>0.067<br>±0.012</td><td>-</td><td>-</td><td>-</td><td>56/53/54</td></tr><tr><td>5797917193442176640</td><td>RRc</td><td>-</td><td>0.2637340<br>±4x10<sup>-7</sup></td><td>1701.161373</td><td>15.6366/15.8718/15.2366<br>±0.0005/±0.00196/±0.00245</td><td>0.147/0.170/0.101<br>±0.001/±0.009/±0.010</td><td>4.707<br>±0.130</td><td>0.083<br>±0.010</td><td>-</td><td>-</td><td>-</td><td>57/48/47</td></tr><tr><td>5846086424210395520</td><td>RRc</td><td>-</td><td>0.2933843<br>±5x10<sup>-7</sup></td><td>1700.684493</td><td>16.6451/16.8922/16.2396<br>±0.0008/±0.0036/±0.0035</td><td>0.156/0.186/0.118<br>±0.002/±0.011/±0.010</td><td>5.00<br>±0.178</td><td>0.080<br>±0.015</td><td>-</td><td>-</td><td>-</td><td>52/47/46</td></tr><tr><td>5917239841741208576</td><td>RRab</td><td>0.638600<br>±2x10<sup>-6</sup></td><td>-</td><td>1705.946735</td><td>16.3224/16.6628/15.8031<br>±0.0005/±0.0026/±0.0024</td><td>0.147/0.188/0.116<br>±0.001/±0.009/±0.006</td><td>4.422<br>±0.050</td><td>0.189<br>±0.007</td><td>2.937<br>±0.229</td><td>0.040<br>±0.011</td><td>-0.25<br>±0.344</td><td>0.415<br>±0.051</td></tr><tr><td>5991733644318583424</td><td>RRc</td><td>-</td><td>0.258867<br>±1x10<sup>-6</sup></td><td>1707.080357</td><td>16.444/17.10244/15.636<br>±0.013/±0.004/±0.004</td><td>0.135/0.178/0.123<br>±0.003/±0.014/±0.012</td><td>4.378<br>±0.483</td><td>0.074<br>±0.015</td><td>-</td><td>-</td><td>-</td><td>53/53/50</td></tr><tr><td>6017924835910361344</td><td>RRc</td><td>-</td><td>0.268742<br>±2x10<sup>-6</sup></td><td>1708.808652</td><td>17.762/18.319/17.037<br>±0.002/±0.011/±0.006</td><td>0.214/0.294/0.183<br>±0.007/±0.023/±0.013</td><td>4.847<br>±0.184</td><td>0.178<br>±0.046</td><td>-</td><td>-</td><td>-</td><td>32/32/30</td></tr><tr><td>6069336998880602240</td><td>RRab</td><td>0.73337<br>±5x10<sup>-6</sup></td><td>-</td><td>1699.822497</td><td>16.3183/16.6855/15.7082<br>±0.0008/±0.0157/±0.0057</td><td>0.181/0.265/0.152<br>±0.004/±0.052/±0.019</td><td>4.516<br>±0.087</td><td>0.242<br>±0.020</td><td>-</td><td>-</td><td>-</td><td>0.712<br>±0.051</td></tr><tr><td>6707009423228603904</td><td>RRc</td><td>-</td><td>0.306965<br>±1x10<sup>-6</sup></td><td>1709.373150</td><td>16.16385/16.3367/15.7239<br>±0.0009/±0.0155/±0.0261</td><td>0.154/0.138/0.245<br>±0.022/±0.043/±0.086</td><td>4.778<br>±0.320</td><td>0.048<br>±0.012</td><td>-</td><td>-</td><td>-</td><td>27/25/26</td></tr><tr><td>5935214760885709440</td><td>RRc</td><td>-</td><td>0.340823<br>±4x10<sup>-6</sup></td><td>1706.070130</td><td>19.0373/20.624/17.757<br>±0.004/±0.092/±0.011</td><td>0.158/0.819/0.113<br>±0.018/±0.301/±0.044</td><td>5.373<br>±0.495</td><td>0.193<br>±0.065</td><td>-</td><td>-</td><td>-</td><td>40/24/27</td></tr><tr><td>4362766825101261952</td><td>RRc</td><td>-</td><td>0.2631889<br>±5x10<sup>-7</sup></td><td>1716.317264</td><td>16.3937/16.9315/15.6715<br>±0.0008/±0.0071/±0.0036</td><td>0.140/0.153/0.115<br>±0.002/±0.027/±0.011</td><td>4.849<br>±0.380</td><td>0.0518<br>±0.019</td><td>-</td><td>-</td><td>-</td><td>43/40/41</td></tr><tr><td>5967334102579505664</td><td>RRab</td><td>0.62513<br>±2x10<sup>-5</sup></td><td>-</td><td>1707.700232</td><td>18.426/19.999/17.229<br>±0.005/±0.040/±0.012</td><td>0.130/0.372/0.124<br>±0.013/±0.310/±0.059</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>3.429<br>±0.090</td></tr></tbody></table>

**Notes.** The G, G<sub>BP</sub>, G<sub>RP</sub> time series photometry of these sources can be retrieved from the gaiadr3.variClassifier_results table.

(a) The BJD of the epoch of maximum light is offset by JD 2455197.5 d (= J2010.0). (b) Photometric metal abundance derived from the φ<sub>31</sub> Fourier parameter of the light curve of RR Lyrae stars (see Sects. 5.1 and 7). (c) Absorption in the G band computed from a relation that links the star intrinsic colour to the period and the amplitude of the G-band light variation of RR Lyrae stars (see Sects. 5.3 and 7).
**Appendix D: OGLE-IV, ASAS-SN, and CATALINA control samples**

Figures D.1, D.2, and D.3 show the footprints of RR Lyrae control samples drawn from the OGLE-IV, ASAS-SN, and

CATALINA catalogues, respectively, that were used to estimate the completeness (and contamination, only OGLE) of the final clean catalogue of 270 905 RR Lyrae stars that are released in DR3.

<figure><img src="image_42.png" /><figcaption>**Fig. D.1.** Regions (red areas) in the footprint of the OGLE-IV RR Lyrae stars (violet symbols) that we used to estimate the completeness, contamination, and percentage of new discoveries of the final clean catalogue of DR3 RR Lyrae stars (orange symbols) in the LMC, SMC, and in the Galactic bulge. For the LMC, we used a circular region with 8.3° in radius centred at (RA=81.5° Dec=-70.1°), for the SMC a region with 5.6° in radius centred at (RA=13.2°, Dec=-72.9°), and for the MW bulge, we used two regions with 3° degree in radius centred at (RA=274.7°, Dec=-31.8°; bulge-up) and (RA=261.2°, Dec=-24.9°; bulge-down).</figcaption></figure>

<figure><img src="image_43.png" /><figcaption>**Fig. D.2.** Footprint of the RR Lyrae stars in the ASAS-SN survey that we used to estimate the completeness of the Gaia DR3 RR Lyrae clean catalogue. In the region shown in the map lie 28 377 all-sky RR Lyrae stars observed by ASAS-SN with magnitudes in the range 10.4 < V < 17.4 mag. In the RR Lyrae clean catalogue, we recover 20 921 of them, using a cross-match radius of 2.5 arcsec.</figcaption></figure>
**Appendix D: OGLE-IV, ASAS-SN, and CATALINA control samples**

Figures D.1, D.2, and D.3 show the footprints of RR Lyrae control samples drawn from the OGLE-IV, ASAS-SN, and

CATALINA catalogues, respectively, that were used to estimate the completeness (and contamination, only OGLE) of the final clean catalogue of 270 905 RR Lyrae stars that are released in DR3.

<figure><img src="image_43.png" /><figcaption>**Fig. D.1.** Regions (red areas) in the footprint of the OGLE-IV RR Lyrae stars (violet symbols) that we used to estimate the completeness, contamination, and percentage of new discoveries of the final clean catalogue of DR3 RR Lyrae stars (orange symbols) in the LMC, SMC, and in the Galactic bulge. For the LMC, we used a circular region with 8.3° in radius centred at (RA=81.5° Dec=-70.1°), for the SMC a region with 5.6° in radius centred at (RA=13.2°, Dec=-72.9°), and for the MW bulge, we used two regions with 3° degree in radius centred at (RA=274.7°, Dec=-31.8°; bulge-up) and (RA=261.2°, Dec=-24.9°; bulge-down).</figcaption></figure>

<figure><img src="image_44.png" /><figcaption>**Fig. D.2.** Footprint of the RR Lyrae stars in the ASAS-SN survey that we used to estimate the completeness of the Gaia DR3 RR Lyrae clean catalogue. In the region shown in the map lie 28 377 all-sky RR Lyrae stars observed by ASAS-SN with magnitudes in the range 10.4 < V < 17.4 mag. In the RR Lyrae clean catalogue, we recover 20 921 of them, using a cross-match radius of 2.5 arcsec.</figcaption></figure>
<figure><img src="image_44.png" /><figcaption>**Fig. D.3.** Footprint of the RR Lyrae stars of the CATALINA survey that we used to estimate the completeness of the *Gaia* DR3 RR Lyrae clean catalogue. In the region shown in the map lie 42 775 RR Lyrae observed by CATALINA, with magnitudes in the range 11 < V < 21.1 mag. In the RR Lyrae clean catalogue, we recover 36 576 of them, using a cross-match radius of 2.5 arcsec.</figcaption></figure>
<figure><img src="image_45.png" /><figcaption>**Fig. D.3.** Footprint of the RR Lyrae stars of the CATALINA survey that we used to estimate the completeness of the *Gaia* DR3 RR Lyrae clean catalogue. In the region shown in the map lie 42 775 RR Lyrae observed by CATALINA, with magnitudes in the range 11 < V < 21.1 mag. In the RR Lyrae clean catalogue, we recover 36 576 of them, using a cross-match radius of 2.5 arcsec.</figcaption></figure>
**Appendix E: Examples of Gaia archive queries**

**Table E.1.** Queries to retrieve DR3 information on the RR Lyrae stars from the *Gaia* archive in the Astronomical Data Query Language (Osuna et al. 2008).

Query to retrieve the sourceid of all RR Lyrae stars confirmed with the SOS Cep&RRL pipeline in the *Gaia* DR3.

select gaia.source_id from gaiadr3.gaia_source as gaia

inner join gaiadr3.variMETRICS as rrl on gaia.source_id=rrl.source_id

Query to retrieve the number of processed observations and SOS Cep&RRL-computed parameters of all RR Lyrae in the *Gaia* DR3.

select * from gaiadr3.variMETRICS, gaiadr3.galacticSkyPosition, gaiadr3.galacticSkyPosition_r, gaiadr3.galacticSkyPosition_v

from gaiadr3.variMETRICS rrl

inner join gaiadr3.vari_summary vs on rrl.source_id=vs.source_id
**Appendix E: Examples of Gaia archive queries**

**Table E.1.** Queries to retrieve DR3 information on the RR Lyrae stars from the *Gaia* archive in the Astronomical Data Query Language (Osuna et al. 2008).

Query to retrieve the sourceid of all RR Lyrae stars confirmed with the SOS Cep&RRL pipeline in the *Gaia* DR3.

select gaia.source_id from gaiadr3.gaia_source as gaia

inner join gaiadr3.variMETRICS as rrl on gaia.source_id=rrl.source_id

Query to retrieve the number of processed observations and SOS Cep&RRL-computed parameters of all RR Lyrae in the *Gaia* DR3.

select rrl.*, vs.num selected_g_fov, vs.num selected bp, vs.num selected rp

from gaiadr3.variMETRICS rrl

inner join gaiadr3.vari_summary vs on rrl.source_id=vs.source_id
Appendix F: Acronyms

<table><caption>**Table F.1.** List of acronyms used in this paper. Each acronym is also defined at its first occurrence in the paper.</caption><thead><tr><td>Acronym</td><td>Description</td></tr></thead><tbody><tr><td>ACEP</td><td>Anomalous Cepheid</td></tr><tr><td>A(G)</td><td>Absorption in the G band</td></tr><tr><td>AGN</td><td>Active Galactic Nuclei</td></tr><tr><td>All_Sky</td><td>The celestial region excluding the LMC, SMC, M31 and M33 regions</td></tr><tr><td>Amp(G)</td><td>Amplitude of the light variation in the G band</td></tr><tr><td>Amp(G<sub>BP</sub>)</td><td>Amplitude of the light variation in the G<sub>BP</sub> band</td></tr><tr><td>Amp(G<sub>RP</sub>)</td><td>Amplitude of the light variation in the G<sub>RP</sub> band</td></tr><tr><td>Amp(RV)</td><td>Amplitude of the RVS radial velocity variation</td></tr><tr><td>B-W</td><td>Baade-Wesselink</td></tr><tr><td>CMD</td><td>Colour Magnitude Diagram</td></tr><tr><td>DCEP</td><td>Classical Cepheid (Population I)</td></tr><tr><td>DPAC</td><td>Data Processing and Analysis Consortium</td></tr><tr><td>dSph</td><td>Dwarf spheroidal galaxy</td></tr><tr><td>DR</td><td>Data Release</td></tr><tr><td>EDR3</td><td>Early Data Release 3</td></tr><tr><td>ECL</td><td>Eclipsing binary</td></tr><tr><td>ELL</td><td>Ellipsoidal variable</td></tr><tr><td>F</td><td>Fundamental mode of pulsation</td></tr><tr><td>[Fe/H]</td><td>Iron abundance</td></tr><tr><td>FO or 1O</td><td>First overtone mode of pulsation</td></tr><tr><td>G</td><td>Gaia photometric G-band</td></tr><tr><td>G<sub>BP</sub></td><td>Gaia photometric G<sub>BP</sub> band</td></tr><tr><td>G<sub>RP</sub></td><td>Gaia photometric G<sub>RP</sub> band</td></tr><tr><td>G<sub>RVS</sub></td><td>Gaia photometric G<sub>RVS</sub> band</td></tr><tr><td>GC</td><td>Globular cluster</td></tr><tr><td>LMC</td><td>Large Magellanic Cloud</td></tr><tr><td>LZ</td><td>Luminosity-Metallicity</td></tr><tr><td>M31</td><td>Andromeda galaxy</td></tr><tr><td>M33</td><td>Triangulum galaxy</td></tr><tr><td>MAD</td><td>Median Absolute Deviation</td></tr><tr><td>M<sub>G0</sub></td><td>Absolute G magnitude</td></tr><tr><td>[M/H]</td><td>Total metal abundance</td></tr><tr><td>MORO</td><td>MultibandOutlierRemovalOperator</td></tr><tr><td>MW</td><td>Milky Way</td></tr><tr><td>PA</td><td>Period-Amplitude</td></tr><tr><td>Paper I</td><td>Clementini et al. (2016)</td></tr><tr><td>Paper II</td><td>Clementini et al. (2019)</td></tr><tr><td>PL</td><td>Period-Luminosity</td></tr><tr><td>PLZ</td><td>Period-Luminosity-Metallicity</td></tr><tr><td>PW</td><td>Period-Wesenheit</td></tr><tr><td>QSO</td><td>Quasi Stellar Object</td></tr><tr><td>ROFABO</td><td>RemoveOutliersFaintAndBrightOperator</td></tr><tr><td>RRab</td><td>RR Lyrae star of ab type</td></tr><tr><td>RRc</td><td>RR Lyrae star of c type</td></tr><tr><td>RRd</td><td>double-mode RR Lyrae star</td></tr><tr><td>RV</td><td>Radial Velocity</td></tr><tr><td>RVS</td><td>Radial Velocity Spectrometer</td></tr><tr><td>SEAPipe</td><td>Source Environment Analysis Pipeline</td></tr><tr><td>SMC</td><td>Small Magellanic Cloud</td></tr><tr><td>SOS</td><td>Specific Object Study</td></tr><tr><td>T2CEP</td><td>Type II Cepheid (Population II)</td></tr><tr><td>UFD</td><td>Ultra-faint dwarf galaxy</td></tr></tbody></table>
Appendix F: Acronyms

<table><caption>Table F.1. List of acronyms used in this paper. Each acronym is also defined at its first occurrence in the paper.</caption><thead><tr><td>Acronym</td><td>Description</td></tr></thead><tbody><tr><td>ACEP</td><td>Anomalous Cepheid</td></tr><tr><td>A(G)</td><td>Absorption in the G band</td></tr><tr><td>AGN</td><td>Active Galactic Nuclei</td></tr><tr><td>All_Sky</td><td>The celestial region excluding the LMC, SMC, M31 and M33 regions</td></tr><tr><td>Amp(G)</td><td>Amplitude of the light variation in the G band</td></tr><tr><td>Amp(G<sub>BP</sub>)</td><td>Amplitude of the light variation in the G<sub>BP</sub> band</td></tr><tr><td>Amp(G<sub>RP</sub>)</td><td>Amplitude of the light variation in the G<sub>RP</sub> band</td></tr><tr><td>Amp(RV)</td><td>Amplitude of the RVS radial velocity variation</td></tr><tr><td>B-W</td><td>Baade-Wesselink</td></tr><tr><td>CMD</td><td>Colour Magnitude Diagram</td></tr><tr><td>DCEP</td><td>Classical Cepheid (Population I)</td></tr><tr><td>DPAC</td><td>Data Processing and Analysis Consortium</td></tr><tr><td>dSph</td><td>Dwarf spheroidal galaxy</td></tr><tr><td>DR</td><td>Data Release</td></tr><tr><td>EDR3</td><td>Early Data Release 3</td></tr><tr><td>ECL</td><td>Eclipsing binary</td></tr><tr><td>ELL</td><td>Ellipsoidal variable</td></tr><tr><td>F</td><td>Fundamental mode of pulsation</td></tr><tr><td>[Fe/H]</td><td>Iron abundance</td></tr><tr><td>FO or 1O</td><td>First overtone mode of pulsation</td></tr><tr><td>G</td><td>Gaia photometric G-band</td></tr><tr><td>G<sub>BP</sub></td><td>Gaia photometric G<sub>BP</sub> band</td></tr><tr><td>G<sub>RP</sub></td><td>Gaia photometric G<sub>RP</sub> band</td></tr><tr><td>G<sub>RVS</sub></td><td>Gaia photometric G<sub>RVS</sub> band</td></tr><tr><td>GC</td><td>Globular cluster</td></tr><tr><td>LMC</td><td>Large Magellanic Cloud</td></tr><tr><td>LZ</td><td>Luminosity-Metallicity</td></tr><tr><td>M31</td><td>Andromeda galaxy</td></tr><tr><td>M33</td><td>Triangulum galaxy</td></tr><tr><td>MAD</td><td>Median Absolute Deviation</td></tr><tr><td>M<sub>G0</sub></td><td>Absolute G magnitude</td></tr><tr><td>[M/H]</td><td>Total metal abundance</td></tr><tr><td>MORO</td><td>MultibandOutlierRemovalOperator</td></tr><tr><td>MW</td><td>Milky Way</td></tr><tr><td>PA</td><td>Period-Amplitude</td></tr><tr><td>Paper I</td><td>Clementini et al. (2016)</td></tr><tr><td>Paper II</td><td>Clementini et al. (2019)</td></tr><tr><td>PL</td><td>Period-Luminosity</td></tr><tr><td>PLZ</td><td>Period-Luminosity-Metallicity</td></tr><tr><td>PW</td><td>Period-Wesenheit</td></tr><tr><td>QSO</td><td>Quasi Stellar Object</td></tr><tr><td>ROFABO</td><td>RemoveOutliersFaintAndBrightOperator</td></tr><tr><td>RRab</td><td>RR Lyrae star of ab type</td></tr><tr><td>RRc</td><td>RR Lyrae star of c type</td></tr><tr><td>RRd</td><td>double-mode RR Lyrae star</td></tr><tr><td>RV</td><td>Radial Velocity</td></tr><tr><td>RVS</td><td>Radial Velocity Spectrometer</td></tr><tr><td>SEAPipe</td><td>Source Environment Analysis Pipeline</td></tr><tr><td>SMC</td><td>Small Magellanic Cloud</td></tr><tr><td>SOS</td><td>Specific Object Study</td></tr><tr><td>T2CEP</td><td>Type II Cepheid (Population II)</td></tr><tr><td>UFD</td><td>Ultra-faint dwarf galaxy</td></tr></tbody></table>