Okayama Planet Search Program
This article may meet Wikipedia's criteria for speedy deletion because: I assume because the copyvio version was deleted, and this wasn't moved to the article site, this didn't qualify?. For valid criteria, see CSD.
If this article does not meet the criteria for speedy deletion, or you intend to fix it, please remove this notice, but do not remove this notice from pages that you have created yourself. If you created this page and you disagree with the given reason for deletion, you can click the button below and leave a message explaining why you believe it should not be deleted. You can also visit the talk page to check if you have received a response to your message. Note that this article may be deleted at any time if it unquestionably meets the speedy deletion criteria, or if an explanation posted to the talk page is found to be insufficient.
Note to administrators: this article has content on its talk page which should be checked before deletion. Administrators: check links, talk, history (last), and logs before deletion. Consider checking Google.This page was last edited by 70.55.86.100 (contribs | logs) at 12:23, 31 October 2008 (UTC) (16 years ago) |
 | This article may require copy editing for grammar, style, cohesion, tone, or spelling. |
Okayama Planet Search Program was started in 2001, spectroscopically searching for planetary systems around stars, reporting on the detection of 3 new extrasolar planets (18 Delphini b, Xi Aquilae|Xi Aql b, HD 81688b) around intermediate-mass G and K giants (18 Delphini, Xi Aql, HD 81688). Also, it updated the orbital parameters of HD 104985 b, the first planet discovered around G giants from our survey, by using the data collected during the past six years. Since 2001, it has been conducting a precise Doppler survey of about 300 G and K giants using a 1.88m telescope, the HIgh Dispersion Echelle Spectrograph (HIDES), and an iodine absorption cell (I2 cell - the internal statistical error can be very small.) at Okayama Astrophysical Observatory (OAO), for precise radial velocity measurements. Use of numerical calculations suggest that Jupiter-mass planets within about (distance range) +0.5
−0.25 AU in fuction of the metallicity and adopted models).
Observatory
Reference
- "Okayama Astrophysical Observatory Homepage". http://www.oao.nao.ac.jp. Retrieved 2008-10-11.
{{cite web}}: External link in|work= - "Planetary Companions around Three Intermediate-Mass G and K Giants: 18 Delphini, Xi Aquilae, and HD81688" (PDF). http://www.oao.nao.ac.jp. Retrieved 2008-10-11.
{{cite web}}: External link in|work= - "telescope". http://www.oao.nao.ac.jp. Retrieved 2008-10-11.
{{cite web}}: External link in|work=
 | This article has not been added to any content categories. Please help out by adding categories to it so that it can be listed with similar articles, in addition to a stub category. |
 | This astronomy-related article is a stub. You can help Wikipedia by expanding it. |