TEPCat: Rossiter-McLaughlin effect observations of transiting planets

This table catalogues the Rossiter-McLaughlin effects measured for known (published) transiting extrasolar planets. This effect is normally observed spectroscopically (usually via radial velocity measurements) but can be obtained photometrically, by analysis of starspot crossing events during transits.

All known Rossiter-McLaughlin measurements are included. Many systems have multiple measurements, often resulting from the same data. In these cases the most recent is normally the most reliable but it is worthwhile checking the literature to be sure.

The Rossiter-McLaughlin effect was originally predicted by Holt (1893) and observed (but not definitively) in the eclipsing binary star systems δ Librae (Schlesinger 1910) and λ Tauri (Schlesinger 1916). It was subsequently described and clearly demonstrated by Rossiter (1924) for β Lyrae and McLaughlin (1924) for β Persei. The designation "Rossiter-McLaughlin effect" arose from the latter two papers.

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System	λ (degrees)	Reference
CoRoT-1	77 ± 11	Pont et al. (2010)
CoRoT-2	7.2 ± 4.5 4.0 + 6.1 - 5.9	Bouchy et al. (2008) Gillon et al. (2010)
CoRoT-3	37.6 + 10.0 - 22.3	Triaud et al. (2009)
CoRoT-11	prograde	Gandolfi et al. (2010)
CoRoT-18	−10 ± 20	Hébrard et al. (2011)
CoRoT-19	−52 + 27 - 22	Guenther et al. (2011)
HAT-P-1	3.7 ± 2.1	Johnson et al. (2008)
HAT-P-2	1.2 ± 13.4 0.2 + 12.2 - 12.5	Winn et al. (2007) Loeillet et al. (2008)
HAT-P-4	−4.9 ± 11.9	Winn et al. (2011)
HAT-P-6	166 ± 10	Hébrard et al. (2011)
HAT-P-7	182.5 ± 9.4 −132.6 + 10.5 - 16.3	Winn et al. (2009) Narita et al. (2009)
HAT-P-8	−9.7 + 9.0 - 7.7 −17 + 9.2 - 11.5	Simpson et al. (2011) Moutou et al. (2011)
HAT-P-9	−16 ± 8	Moutou et al. (2011)
HAT-P-11	103 + 26 - 10 103 + 22 - 18 90 ± 28 83 + 77 - 76 almost polar orbit	Winn et al. (2010) Hirano et al. (2010) Sanchis-Ojeda et al. (2011) solution 1 Sanchis-Ojeda et al. (2011) solution 2 Deming et al. (2011)
HAT-P-13	1.9 ± 8.6	Winn et al. (2010)
HAT-P-14	189.1 ± 5.1	Winn et al. (2011)
HAT-P-16	−10 ± 16	Moutou et al. (2011)
HAT-P-23	15 ± 22	Moutou et al. (2011)
HAT-P-30	73.5 ± 9.0	Johnson et al. (2011)
HD 17156	62 ± 25 9.4 ± 9.3 −4.8 ± 5.3 10.0 ± 5.1	Narita et al. (2008) Cochran et al. (2008) Barbieri et al. (2009) Narita et al. (2009)
HD 80606	50 + 61 - 36 53 + 34 - 21 42 ± 8	Pont et al. (2009) Winn et al. (2009) Hébrard et al. (2010)
HD 149026	−12 ± 15	Wolf et al. (2007)
HD 189733	−1.4 ± 1.1 0.85 + 0.28 - 0.32 −0.50 ± 0.30	Winn et al. (2006) Triaud et al. (2009) Collier Cameron et al. (2010)
HD 209458	3.9 + 18 - 21 −4.4 ± 1.4	Queloz et al. (2000) Winn et al. (2005)
Kepler-8	−26.4 ± 10.1	Jenkins et al. (2011)
Kepler-17	less than 15	Désert et al. (2011)
TrES-1	30 ± 21	Narita et al. (2007)
TrES-2	−9 ± 12	Winn et al. (2008)
TrES-4	6.3 ± 4.7	Narita et al. (2010)
WASP-1	−79.0 + 4.5 - 4.3 −59 + 99 - 26	Simpson et al. (2011) Albrecht et al. (2011)
WASP-2	−153 + 15 - 11 indeterminate	Triaud et al. (2010) Albrecht et al. (2011)
WASP-3	15 + 10 - 9 3.3 + 2.5 - 4.4 5 + 6 - 5	Simpson et al. (2010) Tripathi et al. (2010) Miller et al. (2010)
WASP-4	4 + 34 - 43 −1 + 14 - 12	Triaud et al. (2010) Sanchis-Ojeda et al. (2011)
WASP-5	12.1 + 8.0 - 10.0 7.2 ± 9.5	Triaud et al. (2010) Fukui et al. (2010)
WASP-6	11 + 14 - 18	Gillon et al. (2009)
WASP-7	86 ± 6	Albrecht et al. (2011)
WASP-8	−123.3 + 3.4 - 4.4	Queloz et al. (2010)
WASP-14	−14 + 21 - 13 −33.1 ± 7.4	Joshi et al. (2009) Johnson et al. (2009)
WASP-15	−139.6 + 4.3 - 5.2	Triaud et al. (2010)
WASP-16	−4.2 + 11.0 - 13.9	Brown et al. (2012)
WASP-17	−147 + 49 - 11 −167.4 ± 11.2 −148.5 + 4.2 - 5.4 −148.7 + 7.7 - 6.7	Anderson et al. (2010) Bayliss et al. (2010) Triaud et al. (2010) Anderson et al. (2011)
WASP-18	4.0 ± 5.0	Triaud et al. (2010)
WASP-19	4.6 ± 5.2	Hellier et al. (2011)
WASP-22	22 ± 16	Anderson et al. (2011)
WASP-23	prograde	Triaud et al. (2011)
WASP-24	−4.7 ± 4.0	Simpson et al. (2011)
WASP-25	14.6 ± 6.7	Brown et al. (2012)
WASP-26	indeterminate	Anderson et al. (2011)
WASP-31	2.8 ± 3.1	Brown et al. (2012)
WASP-33	252 ± 2	Collier Cameron et al. (2011)
WASP-38	15 + 33 - 43	Simpson et al. (2011)
XO-2	10 ± 72	Narita et al. (2011)
XO-3	70 ± 15 37.3 ± 3.7 37.4 ± 2.2	Hébrard et al. (2008) Winn et al. (2009) Hirano et al. (2011)
XO-4	−46.7 + 8.1 - 6.1	Narita et al. (2010)

Last modified: 2012/05/16 John Southworth (Keele University, UK)