# Benchmarking the fundamental parameters of Ap stars with optical long-baseline interferometric measurements
(Corrigendum)

K. Perraut, M. Cunha, A. Romanovskaya, D. Shulyak, T. Ryabchikova, V.

Hocdé, N. Nardetto, D. Mourard, A. Meilland, F. Morand, et al.

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► To cite this version:

K. Perraut, M. Cunha, A. Romanovskaya, D. Shulyak, T. Ryabchikova, et al. Benchmarking the fundamental parameters of Ap stars with optical long-baseline interferometric measurements (Corrigendum). Astronomy & Astrophysics - A&A, 2023, 675, pp.C3. 10.1051/0004-6361/202038753e. hal-04310134

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# Benchmarking the fundamental parameters of Ap stars with optical long-baseline interferometric measurements* (Corrigendum)

K. Perraut¹, M. Cunha²,³, A. Romanovskaya⁴, D. Shulyak⁵, T. Ryabchikova⁴, V. Hocdé⁶, N. Nardetto⁶, D. Mourard⁶, A. Meilland⁶, F. Morand⁶, I. Tallon-Bosc⁷, C. Farrington⁸, and C. Lanthermann⁹

¹ Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France
e-mail: karine.perraut@univ-grenoble-alpes.fr

² Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal

³ School of Physics and Astronomy, University of Birmingham, Birmingham, B15 2TT, UK

⁴ Institute of Astronomy, Russian Academy of Sciences, Pyatnitskaya 48, 119017 Moscow, Russia

⁵ Max-Planck Institute fur Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, Germany

⁶ Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, France

⁷ Univ. Lyon, Univ. Lyon1, Ens de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574, 69230 Saint-Genis-Laval, France

⁸ CHARA Array, Mount Wilson Observatory, 91023 Mount Wilson CA, USA

⁹ Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, 3001 Leuven, Belgium

A&A, 642, A101 (2020), https://doi.org/10.1051/0004-6361/202038753

**Key words.** methods: observational – techniques: high angular resolution – techniques: interferometric – stars: fundamental parameters – errata, addenda

This corrigendum corrects Table 1 in which the columns gathering the *B* and *V* magnitudes were inverted, and the erroneous value of the effective temperature of HD 201601 that was derived from interferometric observations in Table 4. The corrected Table 1 is given below.

An effective temperature of 7364 ± 235 K was derived for HD 201601, as reported previously in Perraut et al. (2011). Figure 5 and Table 4 have been updated accordingly. These corrections affect neither the results nor the conclusions of the original paper.

Acknowledgements. We thank Victor Maraud for pointing out these imprecisions in our original manuscript.

## References

Bruntt, H., North, J. R., Cunha, M., et al. 2008, MNRAS, 386, 2039

Bruntt, H., Kervella, P., Mérand, A., et al. 2010, A&A, 512, A55

Glagolevskij, Y. V. 2019, Astrophys. Bull., 74, 66

Kochukhov, O. 2017, A&A, 597, A58

Kochukhov, O., & Bagnulo, S. 2006, A&A, 450, 763

Kochukhov, O., Shulyak, D., & Ryabchikova, T. 2009, A&A, 499, 851

Nesvacil, N., Shulyak, D., Ryabchikova, T. A., et al. 2013, A&A, 552, A28

Perraut, K., Brandão, I., Mourard, D., et al. 2011, A&A, 526, A89

Perraut, K., Borgniet, S., Cunha, M., et al. 2013, A&A, 559, A21

Perraut, K., Cunha, M., Brandão, I., et al. 2015, A&A, 579, A85

Perraut, K., Brandão, I., Cunha, M., et al. 2016, A&A, 590, A117

Romanovskaya, A., Ryabchikova, T., & Shulyak, D. 2019a, ASP Conf. Ser., 518, 173

Romanovskaya, A., Ryabchikova, T., Shulyak, D., et al. 2019b, MNRAS, 488, 2343

Romanovskaya, A. M., Ryabchikova, T. A., & Shulyak, D. V. 2020a, Astron. Lett., 46, 331

Romanovskaya, A. M., Ryabchikova, T. A., & Shulyak, D. V. 2020b, INASAN Sci. Rep., 5, 219

<table><caption>**Table 1.** Stellar properties for the complete Ap sample, with $T_{\text{eff}}$ and $L$ derived from Kochukhov & Bagnulo (2006).</caption><thead><tr><th>#</th><th>HD</th><th>B</th><th>V</th><th>Sp. type</th><th><i>T</i><sub>eff</sub> [K]</th><th><i>L</i> [$L_{\odot}$]</th></tr></thead><tbody><tr><td>1</td><td>4778</td><td>6.16</td><td>6.15</td><td>A3Vp</td><td>9980</td><td>32.4</td></tr><tr><td>2</td><td>24 712<sup>(a)</sup></td><td>6.32</td><td>6.00</td><td>A9p</td><td>7190</td><td>7.4</td></tr><tr><td>3</td><td>108 662</td><td>5.21</td><td>5.24</td><td>A0p</td><td>10 500</td><td>64.6</td></tr><tr><td>4</td><td>108 945</td><td>5.50</td><td>5.44</td><td>A2pv</td><td>8950</td><td>51.3</td></tr><tr><td>5</td><td>118 022<sup>(b)</sup></td><td>4.96</td><td>4.94</td><td>Ap</td><td>9060</td><td>28.8</td></tr><tr><td>6</td><td>120 198</td><td>5.63</td><td>5.68</td><td>B9pe</td><td>10 540</td><td>44.7</td></tr><tr><td>7</td><td>128 898<sup>(c)</sup></td><td>3.43</td><td>3.19</td><td>A7p</td><td>7670</td><td>11.0</td></tr><tr><td>8</td><td>137 909<sup>(d)</sup></td><td>3.97</td><td>3.68</td><td>F2p</td><td>7430</td><td>27.5</td></tr><tr><td>9</td><td>153 882</td><td>6.35</td><td>6.31</td><td>B9p</td><td>9730</td><td>100</td></tr><tr><td>10</td><td>176 232<sup>(e)</sup></td><td>6.14</td><td>5.89</td><td>A7p</td><td>7930</td><td>20.9</td></tr><tr><td>11</td><td>188 041<sup>(f)</sup></td><td>5.84</td><td>5.62</td><td>A5p</td><td>8430</td><td>35.5</td></tr><tr><td>12</td><td>201 601<sup>(g)</sup></td><td>4.94</td><td>4.68</td><td>A9p</td><td>7620</td><td>12.6</td></tr><tr><td>13</td><td>204 411<sup>(f)</sup></td><td>5.38</td><td>5.31</td><td>A4pv</td><td>8750</td><td>89.1</td></tr><tr><td>14</td><td>220 825</td><td>4.98</td><td>4.94</td><td>A2pv</td><td>9080</td><td>22.4</td></tr></tbody></table>

**Notes.** The objects previously observed are in italics and the corresponding references are given in the notes.

**References.** (a) Perraut et al. (2016); (b) Perraut et al. (2015); (c) Bruntt et al. (2008); (d) Bruntt et al. (2010); (e) Perraut et al. (2013); (f) Romanovskaya et al. (2019b); and (g) Perraut et al. (2011).

Ryabchikova, T., Leone, F., & Kochukhov, O. 2005, A&A, 438, 973

Ryabchikova, T., Sachkov, M., Weiss, W. W., et al. 2007, A&A, 462, 1103

Shulyak, D., Ryabchikova, T., Mashonkina, L., & Kochukhov, O. 2009, A&A, 499, 879

Shulyak, D., Ryabchikova, T., & Kochukhov, O. 2013, A&A, 551, A14

<footnote>* CHARA/VEGA observations.</footnote>
<table><caption>**Table 4.** Limb-darkened angular diameters in the R band derived from interferometric measurements, Gaia DR2 parallaxes, radii, effective temperatures, and luminosities derived from interferometric measurements for the complete Ap sample.</caption><thead><tr><th rowspan="2">#</th><th rowspan="2">HD</th><th rowspan="2">θ<sub>LD</sub><br>[mas]</th><th rowspan="2">π<sub>P</sub><br>[mas]</th><th colspan="3">Interferometric observations</th><th colspan="3">Modelling</th></tr><tr><th>R<br>[R<sub>☉</sub>]</th><th>L<br>[L<sub>☉</sub>]</th><th>T<sub>eff</sub><br>[K]</th><th>R<br>[R<sub>☉</sub>]</th><th>T<sub>eff</sub><br>[K]</th><th>⟨B<sub>s</sub>⟩<br>[kG]</th></tr></thead><tbody><tr><td>1</td><td>4778</td><td>0.204 ± 0.008</td><td>9.32 ± 0.10</td><td>2.36 ± 0.12</td><td>34.9 ± 4.3</td><td>9135 ± 400</td><td></td><td></td><td>2.6<sup>(a)</sup></td></tr><tr><td>2</td><td>24712</td><td>0.335 ± 0.009</td><td>20.62 ± 0.09</td><td>1.75 ± 0.05</td><td>7.6 ± 1.2</td><td>7235 ± 280</td><td>1.75 ± 0.04</td><td>7250 ± 100<sup>(b)</sup></td><td>3.1<sup>(c)</sup></td></tr><tr><td>3</td><td>108662</td><td>0.328 ± 0.009</td><td>13.54 ± 0.24</td><td>2.59 ± 0.12</td><td>38.1 ± 4.9</td><td>8880 ± 330</td><td>2.09 ± 0.10</td><td>10225 ± 100<sup>(d)</sup></td><td>3.3<sup>(e)</sup></td></tr><tr><td>4</td><td>108945</td><td>0.315 ± 0.006</td><td>12.00 ± 0.15</td><td>2.82 ± 0.09</td><td>36.5 ± 4.2</td><td>8430 ± 270</td><td></td><td></td><td>0.1<sup>(a)</sup></td></tr><tr><td>5</td><td>118022</td><td>0.346 ± 0.006</td><td>17.16 ± 0.25</td><td>2.17 ± 0.06</td><td>28.9 ± 3.0</td><td>9100 ± 190</td><td>2.16 ± 0.02</td><td>9140 ± 30<sup>(f)</sup></td><td>3.0<sup>(f)</sup></td></tr><tr><td>6</td><td>120198</td><td>0.226 ± 0.008</td><td>10.62 ± 0.078</td><td>2.28 ± 0.10</td><td>44.9 ± 4.3</td><td>9865 ± 370</td><td></td><td></td><td>1.6<sup>(e)</sup></td></tr><tr><td>7</td><td>128898</td><td>1.105 ± 0.037</td><td>60.35 ± 0.14<sup>(*)</sup></td><td>1.967 ± 0.066</td><td>10.51 ± 0.60</td><td>7420 ± 170</td><td>1.94 ± 0.01</td><td>7500 ± 130<sup>(g)</sup></td><td>2.0<sup>(h)</sup></td></tr><tr><td>8</td><td>137909</td><td>0.699 ± 0.017</td><td>28.60 ± 0.69<sup>(*)</sup></td><td>2.63 ± 0.09</td><td>25.3 ± 2.9</td><td>7980 ± 180</td><td>2.47 ± 0.07</td><td>8100 ± 150<sup>(i)</sup></td><td>5.4<sup>(j)</sup></td></tr><tr><td>9</td><td>153882</td><td>0.193 ± 0.019</td><td>5.98 ± 0.053</td><td>3.46 ± 0.37</td><td>70.8 ± 6.5</td><td>8980 ± 600</td><td>3.35 ± 0.03</td><td>9150 ± 100<sup>(k)</sup></td><td>3.8<sup>(k)</sup></td></tr><tr><td>10</td><td>176232</td><td>0.275 ± 0.009</td><td>13.37 ± 0.08</td><td>2.21 ± 0.08</td><td>16.9 ± 1.4<sup>(+)</sup></td><td>7900 ± 190<sup>(+)</sup></td><td>2.35 ± 0.06</td><td>7550 ± 50<sup>(l)</sup></td><td>1.5<sup>(l)</sup></td></tr><tr><td>11</td><td>188041</td><td>0.247 ± 0.005</td><td>11.72 ± 0.11</td><td>2.26 ± 0.05</td><td>30.5 ± 4.2</td><td>9000 ± 360</td><td>2.39 ± 0.05</td><td>8770 ± 150<sup>(m)</sup></td><td>3.6<sup>(m)</sup></td></tr><tr><td>12</td><td>201601</td><td>0.564 ± 0.017</td><td>28.77 ± 0.25</td><td>2.11 ± 0.07</td><td>11.0 ± 0.93</td><td>7364 ± 235</td><td>1.98 ± 0.05</td><td>7550 ± 150<sup>(j)</sup></td><td>4.0<sup>(j)</sup></td></tr><tr><td>13</td><td>204411</td><td>0.328 ± 0.004</td><td>8.33 ± 0.12</td><td>4.23 ± 0.11</td><td>85.6 ± 9.2</td><td>8520 ± 220</td><td>4.42 ± 0.07</td><td>8300 ± 150<sup>(m)</sup></td><td>&lt;0.8<sup>(n)</sup></td></tr><tr><td>14</td><td>220825</td><td>0.339 ± 0.005</td><td>20.44 ± 0.23</td><td>1.78 ± 0.03</td><td>17.2 ± 1.7</td><td>8790 ± 230</td><td></td><td></td><td>2.0<sup>(e)</sup></td></tr></tbody></table>

**Notes.** The last three columns give the radii and the effective temperatures as derived from self-consistent modelling and when considering the Gaia DR2 parallaxes, and the magnetic field strengths. Four targets have not been modelled yet. (*)For these two targets, we have kept the parallaxes from HIPPARCOS because of the binarity and/or the brightness is too high. (+)We report the average values of the effective temperatures and luminosities provided in Perraut et al. (2013).

**References.** (a)Glagolevskij (2019); (b)Shulyak et al. (2009); (c)Ryabchikova et al. (2007); (d)Romanovskaya et al. (2020b); (e)Kochukhov (2017); (f)Romanovskaya et al. (2019a); (g)Bruntt et al. (2008); (h)Kochukhov et al. (2009); (i)Bruntt et al. (2010); (j)Shulyak et al. (2013); (k)Romanovskaya et al. (2020a); (l)Nesvacil et al. (2013); (m)Romanovskaya et al. (2019b); and (n)Ryabchikova et al. (2005).

<figure><img src="image_3.png" /><figcaption>**Fig. 5.** Comparison between the radii (left) and the effective temperatures (right) derived from interferometric measurements and those derived from the self-consistent spectroscopic modelling. The dash lines give the 1:1 relations. The numbers close to the symbols refer to Table 4.</figcaption></figure>