TY - JOUR
T1 - Analysis of Spin-Orbit Alignment in the WASP-32, WASP-38, and HAT-P-27/WASP-40 Systems
AU - Brown, D.~J.~A.
AU - Collier Cameron, A.
AU - Díaz, R.~F.
AU - Doyle, A.~P.
AU - Gillon, M.
AU - Lendl, M.
AU - Smalley, B.
AU - Triaud, A.~H.~M.~J.
AU - Anderson, D.~R.
AU - Enoch, B.
AU - Hellier, C.
AU - Maxted, P.~F.~L.
AU - Miller, G.~R.~M.
AU - Pollacco, D.
AU - Queloz, D.
AU - Boisse, I.
AU - Hébrard, G.
PY - 2012/12/1
Y1 - 2012/12/1
N2 - We present measurements of the spin-orbit alignment angle, $, for the hot Jupiter systems WASP-32, WASP-38, and HAT-P-27/WASP-40, based on data obtained using the HARPS spectrograph. We analyze the Rossiter-McLaughlin effect for all three systems and also carry out Doppler tomography for WASP-32 and WASP-38. We find that WASP-32 (T $_eff$ = 6140$^+90$ $_- 100$ K) is aligned, with an alignment angle of $ = 10fdg5$^ + 6.4$ $_ - 6.5$ obtained through tomography, and that WASP-38 (T $_eff$ = 6180$^+40$ $_- 60$ K) is also aligned, with tomographic analysis yielding $ = 7fdg5$^ + 4.7$ $_ - 6.1$. The latter result provides an order-of-magnitude improvement in the uncertainty in $ compared to the previous analysis of Simpson et al. We are only able to loosely constrain the angle for HAT-P-27/WASP-40 (T $_eff$ = 5190$^+160$ $_- 170$ K) to $ = 24fdg2$^ + 76.0$ $_ - 44.5$, owing to the poor signal-to-noise ratio of our data. We consider this result a non-detection under a slightly updated version of the alignment test of Brown et al. We place our results in the context of the full sample of spin-orbit alignment measurements, finding that they provide further support for previously established trends. Based on observations (under proposal 087.C-0649) made using the HARPS High Resolution Échelle Spectrograph mounted on the ESO 3.6 m at the ESO La Silla observatory.
AB - We present measurements of the spin-orbit alignment angle, $, for the hot Jupiter systems WASP-32, WASP-38, and HAT-P-27/WASP-40, based on data obtained using the HARPS spectrograph. We analyze the Rossiter-McLaughlin effect for all three systems and also carry out Doppler tomography for WASP-32 and WASP-38. We find that WASP-32 (T $_eff$ = 6140$^+90$ $_- 100$ K) is aligned, with an alignment angle of $ = 10fdg5$^ + 6.4$ $_ - 6.5$ obtained through tomography, and that WASP-38 (T $_eff$ = 6180$^+40$ $_- 60$ K) is also aligned, with tomographic analysis yielding $ = 7fdg5$^ + 4.7$ $_ - 6.1$. The latter result provides an order-of-magnitude improvement in the uncertainty in $ compared to the previous analysis of Simpson et al. We are only able to loosely constrain the angle for HAT-P-27/WASP-40 (T $_eff$ = 5190$^+160$ $_- 170$ K) to $ = 24fdg2$^ + 76.0$ $_ - 44.5$, owing to the poor signal-to-noise ratio of our data. We consider this result a non-detection under a slightly updated version of the alignment test of Brown et al. We place our results in the context of the full sample of spin-orbit alignment measurements, finding that they provide further support for previously established trends. Based on observations (under proposal 087.C-0649) made using the HARPS High Resolution Échelle Spectrograph mounted on the ESO 3.6 m at the ESO La Silla observatory.
KW - planets and satellites: dynamical evolution and stability, stars: individual: WASP-32 WASP-38 WASP-40, techniques: radial velocities, techniques: spectroscopic
U2 - 10.1088/0004-637X/760/2/139
DO - 10.1088/0004-637X/760/2/139
M3 - Article
SN - 0004-637X
VL - 760
SP - 139
JO - The Astrophysical Journal
JF - The Astrophysical Journal
ER -