A distance to the Large Magellanic Cloud that is precise to one per cent
In the era of precision cosmology, it is essential to determine the Hubble constant empirically with an accuracy of one per cent or better 1 . At present, the uncertainty on this constant is dominated by the uncertainty in the calibration of the Cepheid period–luminosity relationship 2 , 3 (also kno...
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| Veröffentlicht in: | Nature (London) 2019-03, Vol.567 (7747), p.200-203 |
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| creator | Pietrzyński, G. Graczyk, D. Gallenne, A. Gieren, W. Thompson, I. B. Pilecki, B. Karczmarek, P. Górski, M. Suchomska, K. Taormina, M. Zgirski, B. Wielgórski, P. Kołaczkowski, Z. Konorski, P. Villanova, S. Nardetto, N. Kervella, P. Bresolin, F. Kudritzki, R. P. Storm, J. Smolec, R. Narloch, W. |
| description | In the era of precision cosmology, it is essential to determine the Hubble constant empirically with an accuracy of one per cent or better
1
. At present, the uncertainty on this constant is dominated by the uncertainty in the calibration of the Cepheid period–luminosity relationship
2
,
3
(also known as the Leavitt law). The Large Magellanic Cloud has traditionally served as the best galaxy with which to calibrate Cepheid period–luminosity relations, and as a result has become the best anchor point for the cosmic distance scale
4
,
5
. Eclipsing binary systems composed of late-type stars offer the most precise and accurate way to measure the distance to the Large Magellanic Cloud. Currently the limit of the precision attainable with this technique is about two per cent, and is set by the precision of the existing calibrations of the surface brightness–colour relation
5
,
6
. Here we report a calibration of the surface brightness–colour relation with a precision of 0.8 per cent. We use this calibration to determine a geometrical distance to the Large Magellanic Cloud that is precise to 1 per cent based on 20 eclipsing binary systems. The final distance is 49.59 ± 0.09 (statistical) ± 0.54 (systematic) kiloparsecs.
A new calibration of the surface brightness–colour relation of eclipsing binary stars gives a distance to the Large Magellanic Cloud that is precise to one per cent. |
| doi_str_mv | 10.1038/s41586-019-0999-4 |
| format | Article |
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1
. At present, the uncertainty on this constant is dominated by the uncertainty in the calibration of the Cepheid period–luminosity relationship
2
,
3
(also known as the Leavitt law). The Large Magellanic Cloud has traditionally served as the best galaxy with which to calibrate Cepheid period–luminosity relations, and as a result has become the best anchor point for the cosmic distance scale
4
,
5
. Eclipsing binary systems composed of late-type stars offer the most precise and accurate way to measure the distance to the Large Magellanic Cloud. Currently the limit of the precision attainable with this technique is about two per cent, and is set by the precision of the existing calibrations of the surface brightness–colour relation
5
,
6
. Here we report a calibration of the surface brightness–colour relation with a precision of 0.8 per cent. We use this calibration to determine a geometrical distance to the Large Magellanic Cloud that is precise to 1 per cent based on 20 eclipsing binary systems. The final distance is 49.59 ± 0.09 (statistical) ± 0.54 (systematic) kiloparsecs.
A new calibration of the surface brightness–colour relation of eclipsing binary stars gives a distance to the Large Magellanic Cloud that is precise to one per cent.</description><identifier>ISSN: 0028-0836</identifier><identifier>EISSN: 1476-4687</identifier><identifier>DOI: 10.1038/s41586-019-0999-4</identifier><identifier>PMID: 30867610</identifier><language>eng</language><publisher>London: Nature Publishing Group UK</publisher><subject>639/33/34/4126 ; 639/33/34/867 ; Astrophysics ; Binary stars ; Calibration ; Clouds ; Cosmology ; Eclipsing binary stars ; Galaxies ; Hubble constant ; Humanities and Social Sciences ; Letter ; Luminosity ; Magellanic Clouds ; multidisciplinary ; Natural history ; Observations ; Physics ; Science ; Science (multidisciplinary) ; Stars & galaxies ; Surface brightness ; Uncertainty</subject><ispartof>Nature (London), 2019-03, Vol.567 (7747), p.200-203</ispartof><rights>The Author(s), under exclusive licence to Springer Nature Limited 2019</rights><rights>COPYRIGHT 2019 Nature Publishing Group</rights><rights>Copyright Nature Publishing Group Mar 14, 2019</rights><rights>Distributed under a Creative Commons Attribution 4.0 International License</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c608t-97b5c6abf9d117a15b9fbec1097c66e5bdb716a837cd1b0ad32c0d57ae226fbf3</citedby><cites>FETCH-LOGICAL-c608t-97b5c6abf9d117a15b9fbec1097c66e5bdb716a837cd1b0ad32c0d57ae226fbf3</cites><orcidid>0000-0002-7399-0231 ; 0000-0003-0626-1749 ; 0000-0002-9443-4138 ; 0000-0001-7853-4094 ; 0000-0002-8627-6096 ; 0000-0003-3861-8124 ; 0000-0001-7217-4884</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://link.springer.com/content/pdf/10.1038/s41586-019-0999-4$$EPDF$$P50$$Gspringer$$H</linktopdf><linktohtml>$$Uhttps://link.springer.com/10.1038/s41586-019-0999-4$$EHTML$$P50$$Gspringer$$H</linktohtml><link.rule.ids>230,314,776,780,881,27901,27902,41464,42533,51294</link.rule.ids><backlink>$$Uhttps://www.ncbi.nlm.nih.gov/pubmed/30867610$$D View this record in MEDLINE/PubMed$$Hfree_for_read</backlink><backlink>$$Uhttps://hal.science/hal-02307840$$DView record in HAL$$Hfree_for_read</backlink></links><search><creatorcontrib>Pietrzyński, G.</creatorcontrib><creatorcontrib>Graczyk, D.</creatorcontrib><creatorcontrib>Gallenne, A.</creatorcontrib><creatorcontrib>Gieren, W.</creatorcontrib><creatorcontrib>Thompson, I. B.</creatorcontrib><creatorcontrib>Pilecki, B.</creatorcontrib><creatorcontrib>Karczmarek, P.</creatorcontrib><creatorcontrib>Górski, M.</creatorcontrib><creatorcontrib>Suchomska, K.</creatorcontrib><creatorcontrib>Taormina, M.</creatorcontrib><creatorcontrib>Zgirski, B.</creatorcontrib><creatorcontrib>Wielgórski, P.</creatorcontrib><creatorcontrib>Kołaczkowski, Z.</creatorcontrib><creatorcontrib>Konorski, P.</creatorcontrib><creatorcontrib>Villanova, S.</creatorcontrib><creatorcontrib>Nardetto, N.</creatorcontrib><creatorcontrib>Kervella, P.</creatorcontrib><creatorcontrib>Bresolin, F.</creatorcontrib><creatorcontrib>Kudritzki, R. P.</creatorcontrib><creatorcontrib>Storm, J.</creatorcontrib><creatorcontrib>Smolec, R.</creatorcontrib><creatorcontrib>Narloch, W.</creatorcontrib><title>A distance to the Large Magellanic Cloud that is precise to one per cent</title><title>Nature (London)</title><addtitle>Nature</addtitle><addtitle>Nature</addtitle><description>In the era of precision cosmology, it is essential to determine the Hubble constant empirically with an accuracy of one per cent or better
1
. At present, the uncertainty on this constant is dominated by the uncertainty in the calibration of the Cepheid period–luminosity relationship
2
,
3
(also known as the Leavitt law). The Large Magellanic Cloud has traditionally served as the best galaxy with which to calibrate Cepheid period–luminosity relations, and as a result has become the best anchor point for the cosmic distance scale
4
,
5
. Eclipsing binary systems composed of late-type stars offer the most precise and accurate way to measure the distance to the Large Magellanic Cloud. Currently the limit of the precision attainable with this technique is about two per cent, and is set by the precision of the existing calibrations of the surface brightness–colour relation
5
,
6
. Here we report a calibration of the surface brightness–colour relation with a precision of 0.8 per cent. We use this calibration to determine a geometrical distance to the Large Magellanic Cloud that is precise to 1 per cent based on 20 eclipsing binary systems. The final distance is 49.59 ± 0.09 (statistical) ± 0.54 (systematic) kiloparsecs.
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B. ; Pilecki, B. ; Karczmarek, P. ; Górski, M. ; Suchomska, K. ; Taormina, M. ; Zgirski, B. ; Wielgórski, P. ; Kołaczkowski, Z. ; Konorski, P. ; Villanova, S. ; Nardetto, N. ; Kervella, P. ; Bresolin, F. ; Kudritzki, R. 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Academic</collection><collection>Hyper Article en Ligne (HAL)</collection><jtitle>Nature (London)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Pietrzyński, G.</au><au>Graczyk, D.</au><au>Gallenne, A.</au><au>Gieren, W.</au><au>Thompson, I. B.</au><au>Pilecki, B.</au><au>Karczmarek, P.</au><au>Górski, M.</au><au>Suchomska, K.</au><au>Taormina, M.</au><au>Zgirski, B.</au><au>Wielgórski, P.</au><au>Kołaczkowski, Z.</au><au>Konorski, P.</au><au>Villanova, S.</au><au>Nardetto, N.</au><au>Kervella, P.</au><au>Bresolin, F.</au><au>Kudritzki, R. P.</au><au>Storm, J.</au><au>Smolec, R.</au><au>Narloch, W.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>A distance to the Large Magellanic Cloud that is precise to one per cent</atitle><jtitle>Nature (London)</jtitle><stitle>Nature</stitle><addtitle>Nature</addtitle><date>2019-03</date><risdate>2019</risdate><volume>567</volume><issue>7747</issue><spage>200</spage><epage>203</epage><pages>200-203</pages><issn>0028-0836</issn><eissn>1476-4687</eissn><abstract>In the era of precision cosmology, it is essential to determine the Hubble constant empirically with an accuracy of one per cent or better
1
. At present, the uncertainty on this constant is dominated by the uncertainty in the calibration of the Cepheid period–luminosity relationship
2
,
3
(also known as the Leavitt law). The Large Magellanic Cloud has traditionally served as the best galaxy with which to calibrate Cepheid period–luminosity relations, and as a result has become the best anchor point for the cosmic distance scale
4
,
5
. Eclipsing binary systems composed of late-type stars offer the most precise and accurate way to measure the distance to the Large Magellanic Cloud. Currently the limit of the precision attainable with this technique is about two per cent, and is set by the precision of the existing calibrations of the surface brightness–colour relation
5
,
6
. Here we report a calibration of the surface brightness–colour relation with a precision of 0.8 per cent. We use this calibration to determine a geometrical distance to the Large Magellanic Cloud that is precise to 1 per cent based on 20 eclipsing binary systems. The final distance is 49.59 ± 0.09 (statistical) ± 0.54 (systematic) kiloparsecs.
A new calibration of the surface brightness–colour relation of eclipsing binary stars gives a distance to the Large Magellanic Cloud that is precise to one per cent.</abstract><cop>London</cop><pub>Nature Publishing Group UK</pub><pmid>30867610</pmid><doi>10.1038/s41586-019-0999-4</doi><tpages>4</tpages><orcidid>https://orcid.org/0000-0002-7399-0231</orcidid><orcidid>https://orcid.org/0000-0003-0626-1749</orcidid><orcidid>https://orcid.org/0000-0002-9443-4138</orcidid><orcidid>https://orcid.org/0000-0001-7853-4094</orcidid><orcidid>https://orcid.org/0000-0002-8627-6096</orcidid><orcidid>https://orcid.org/0000-0003-3861-8124</orcidid><orcidid>https://orcid.org/0000-0001-7217-4884</orcidid></addata></record> |
| fulltext | fulltext |
| identifier | ISSN: 0028-0836 |
| ispartof | Nature (London), 2019-03, Vol.567 (7747), p.200-203 |
| issn | 0028-0836 1476-4687 |
| language | eng |
| recordid | cdi_hal_primary_oai_HAL_hal_02307840v1 |
| source | Springer Journals; Nature |
| subjects | 639/33/34/4126 639/33/34/867 Astrophysics Binary stars Calibration Clouds Cosmology Eclipsing binary stars Galaxies Hubble constant Humanities and Social Sciences Letter Luminosity Magellanic Clouds multidisciplinary Natural history Observations Physics Science Science (multidisciplinary) Stars & galaxies Surface brightness Uncertainty |
| title | A distance to the Large Magellanic Cloud that is precise to one per cent |
| url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-02-04T18%3A03%3A21IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-gale_hal_p&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=A%20distance%20to%20the%20Large%20Magellanic%20Cloud%20that%20is%20precise%20to%20one%20per%20cent&rft.jtitle=Nature%20(London)&rft.au=Pietrzy%C5%84ski,%20G.&rft.date=2019-03&rft.volume=567&rft.issue=7747&rft.spage=200&rft.epage=203&rft.pages=200-203&rft.issn=0028-0836&rft.eissn=1476-4687&rft_id=info:doi/10.1038/s41586-019-0999-4&rft_dat=%3Cgale_hal_p%3EA578318033%3C/gale_hal_p%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_pqid=2194525771&rft_id=info:pmid/30867610&rft_galeid=A578318033&rfr_iscdi=true |