The long-period Galactic Cepheid RS Puppis - I. A geometric distance from its light echoes

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Kervella"> <meta name="citation_author_institution" content="LESIA, Observatoire de Paris, CNRS UMR 8109, UPMC, Université Paris Diderot, 5 place Jules Janssen, 92195 Meudon, France e-mail: Pierre.Kervella@obspm.fr"> <meta name="citation_author" content="A. Mérand"> <meta name="citation_author_institution" content="Center for High Angular Resolution Astronomy, Georgia State University, PO Box 3965, Atlanta, Georgia 30302-3965, USA"> <meta name="citation_author" content="L. Szabados"> <meta name="citation_author_institution" content="Konkoly Observatory, 1525 Budapest XII, PO Box 67, Hungary"> <meta name="citation_author" content="P. Fouqué"> <meta name="citation_author_institution" content="Observatoire Midi-Pyrénées, Laboratoire d'Astrophysique, CNRS UMR 5572, Université Paul Sabatier – Toulouse 3, 14 avenue Édouard Belin, 31400 Toulouse, France"> <meta name="citation_author" content="D. Bersier"> <meta name="citation_author_institution" content="Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead, CH411LD, UK"> <meta name="citation_author" content="E. Pompei"> <meta name="citation_author_institution" content="European Southern Observatory, Alonso de Cordova 3107, Casilla 19001, Vitacura, Santiago 19, Chile"> <meta name="citation_author" content="G. Perrin"> <meta name="citation_author_institution" content="LESIA, Observatoire de Paris, CNRS UMR 8109, UPMC, Université Paris Diderot, 5 place Jules Janssen, 92195 Meudon, France e-mail: Pierre.Kervella@obspm.fr"> <meta name="citation_title" content="The long-period Galactic Cepheid RS Puppis - I. A geometric distance from its light echoes"> <meta name="citation_online_date" content="2008/01/09"> <meta name="citation_publication_date" content="2008/03/01"> <meta name="citation_volume" content="480"> <meta name="citation_issue" content="1"> <meta name="citation_firstpage" content="167"> <meta name="citation_lastpage" content="178"> <meta name="citation_doi" content="10.1051/0004-6361:20078961"> <meta name="citation_bibcode" content="2008A%26A...480..167K"> <meta name="citation_abstract_html_url" content="https://www.aanda.org/articles/aa/abs/2008/10/aa8961-07/aa8961-07.html"> <meta name="citation_pdf_url" content="https://www.aanda.org/articles/aa/pdf/2008/10/aa8961-07.pdf"> <meta name="citation_issn" content="0004-6361"> <meta name="citation_issn" content="1432-0746"> <meta name="citation_language" content="en"> <meta name="citation_keyword" content="stars: individual: RS Pup"> <meta name="citation_keyword" content="stars: circumstellar matter"> <meta name="citation_keyword" content="stars: distances"> <meta name="citation_keyword" content="stars: variables: Cepheids"> <meta name="citation_keyword" content="ISM: reflection nebulae"> <meta name="citation_keyword" content="ISM: dust, extinction"> <meta name="citation_article_type" content="Research Article"> <meta name="citation_abstract" lang="en" content="<i>Context.<i/>The bright southern Cepheid RS Pup is surrounded by a circumstellar nebula reflecting the light from the central star. The propagation of the light variations from the Cepheid inside the dusty nebula creates spectacular light echoes that can be observed up to large distances from the star itself. This phenomenon is currently unique in this class of stars.<i>Aims.<i/>For this relatively distant star, the trigonometric parallax available from Hipparcos has a low accuracy. A careful observation of the light echoes has the potential to provide a very accurate, geometric distance to RS Pup.<i>Methods.<i/>We obtained a series of CCD images of RS Pup with the NTT/EMMI instrument covering the variation period of the star ( d), allowing us to track the progression of the light wavefronts over the nebular features surrounding the star. We measured precisely the phase lag of the photometric variation in several regions of the circumstellar nebula.<i>Results.<i/>From our phase lag measurements, we derive a geometric distance of 1992 <i>±<i/> 28 pc to RS Pup. This distance is affected by a total uncertainty of 1.4%, and corresponds to a parallax of <i>π<i/> = 0.502 <i>±<i/> 0.007 mas and a distance modulus of <i>μ<i/> = 11.50 <i>±<i/> 0.03.<i>Conclusions.<i/>The geometric distance we derive is by far the most accurate to a Cepheid, and among the most accurate to any star. RS Pup appears both as somewhat neglected and particularly promising to investigate the mass-loss history of Cepheids. Thanks to its highly accurate distance, it is also bound to become an important luminosity fiducial for the long period part of the period-luminosity diagram."> <meta name="citation_reference" content="citation_author=T. G. Barnes;citation_author=J. Storm;citation_author=W. H. Jefferys;citation_author=W. P. Gieren;citation_author=P. Fouqué;citation_publication_date=2005;citation_journal_title=ApJ;citation_volume=631;citation_firstpage=572;"> <meta name="citation_reference" content="citation_author=H. C. Bhatt;citation_author=S. K. Jain;citation_author=R. 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A geometric distance from its light echoes</h3> <div class="article-authors"><p class="bold"><span id="aa8961-07-author-1" data-url="/component/author/?dkey=10.1051/0004-6361:20078961&n=1" class="author">P. Kervella</span><sup>1</sup>, <span id="aa8961-07-author-2" data-url="/component/author/?dkey=10.1051/0004-6361:20078961&n=2" class="author">A. Mérand</span><sup>2</sup>, <span id="aa8961-07-author-3" data-url="/component/author/?dkey=10.1051/0004-6361:20078961&n=3" class="author">L. Szabados</span><sup>3</sup>, <span id="aa8961-07-author-4" data-url="/component/author/?dkey=10.1051/0004-6361:20078961&n=4" class="author">P. Fouqué</span><sup>4</sup>, <span id="aa8961-07-author-5" data-url="/component/author/?dkey=10.1051/0004-6361:20078961&n=5" class="author">D. Bersier</span><sup>5</sup>, <span id="aa8961-07-author-6" data-url="/component/author/?dkey=10.1051/0004-6361:20078961&n=6" class="author">E. Pompei</span><sup>6</sup> and <span id="aa8961-07-author-7" data-url="/component/author/?dkey=10.1051/0004-6361:20078961&n=7" class="author">G. Perrin</span><sup>1</sup></p></div> <p class="aff"> <sup>1</sup> LESIA, Observatoire de Paris, CNRS UMR 8109, UPMC, Université Paris Diderot, 5 place Jules Janssen, 92195 Meudon, France e-mail: Pierre.Kervella@obspm.fr <br> <sup>2</sup> Center for High Angular Resolution Astronomy, Georgia State University, PO Box 3965, Atlanta, Georgia 30302-3965, USA <br> <sup>3</sup> Konkoly Observatory, 1525 Budapest XII, PO Box 67, Hungary <br> <sup>4</sup> Observatoire Midi-Pyrénées, Laboratoire d'Astrophysique, CNRS UMR 5572, Université Paul Sabatier – Toulouse 3, 14 avenue Édouard Belin, 31400 Toulouse, France <br> <sup>5</sup> Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead, CH411LD, UK <br> <sup>6</sup> European Southern Observatory, Alonso de Cordova 3107, Casilla 19001, Vitacura, Santiago 19, Chile <br></p> <p class="history"><span class="bold">Received: </span> 30 October 2007 <br><span class="bold">Accepted: </span> 20 December 2007 </p> <p class="bold"><a name="abs"></a>Abstract</p> <p><i>Context.</i>The bright southern Cepheid RS Pup is surrounded by a circumstellar nebula reflecting the light from the central star. The propagation of the light variations from the Cepheid inside the dusty nebula creates spectacular light echoes that can be observed up to large distances from the star itself. This phenomenon is currently unique in this class of stars.</p> <p><i>Aims.</i>For this relatively distant star, the trigonometric parallax available from Hipparcos has a low accuracy. A careful observation of the light echoes has the potential to provide a very accurate, geometric distance to RS Pup.</p> <p><i>Methods.</i>We obtained a series of CCD images of RS Pup with the NTT/EMMI instrument covering the variation period of the star (<span class="img-inline ressouce-equation ressouce-equation-inline" data-latex="$P = 41.4$"><span class="ressouce-equation-container"><span class="img img-block"><img src="/articles/aa/abs/2008/10/aa8961-07/aa8961-07_tex_eq1.png" id="img_eq1" alt="$P = 41.4$"></span></span></span> d), allowing us to track the progression of the light wavefronts over the nebular features surrounding the star. We measured precisely the phase lag of the photometric variation in several regions of the circumstellar nebula.</p> <p><i>Results.</i>From our phase lag measurements, we derive a geometric distance of 1992 <i>±</i> 28 pc to RS Pup. This distance is affected by a total uncertainty of 1.4%, and corresponds to a parallax of <i>π</i> = 0.502 <i>±</i> 0.007 mas and a distance modulus of <i>μ</i> = 11.50 <i>±</i> 0.03.</p> <p><i>Conclusions.</i>The geometric distance we derive is by far the most accurate to a Cepheid, and among the most accurate to any star. RS Pup appears both as somewhat neglected and particularly promising to investigate the mass-loss history of Cepheids. Thanks to its highly accurate distance, it is also bound to become an important luminosity fiducial for the long period part of the period-luminosity diagram.</p> <div class="kword"><p><span class="bold">Key words: </span>stars: individual: RS Pup / stars: circumstellar matter / stars: distances / stars: variables: Cepheids / ISM: reflection nebulae / ISM: dust, extinction</p></div> </div> <p><i>© ESO, 2008</i></p> </div> </div> <div id="metrics-tabs" data-doi="10.1051/0004-6361:20078961" data-edps_ref="aa8961-07"> <nav class="toolbar"> <button class="toolbar-item" id="metrics-siq">Current usage metrics</button> <button class="toolbar-item" id="info">About article metrics</button> <button class="toolbar-item" id="return">Return to article</button> </nav> <div class="panel" data-for="metrics-siq"> </div> <div class="panel" data-for="metrics-alm"></div> <div class="panel" data-for="info"> <p>Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.</p> <p>Data correspond to usage on the plateform after 2015. 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