HAT-P-27 b / WASP-40 b


HAT-P-27 b (discovered by Béky et al. 2011), also known as WASP-40 b (individually discovered by Anderson et al. (2011)). Looking at the RV-meassurements of both groups, one can see an almost perfect fit of the Béky et al. data, but strong deviations in the Anderson et al. data. Interestingly both groups come to equal results leading to a 0.62 jupiter mass planet with a radius of 1.05 jupiter radii. While Anderson et al. have adopted an eccentricity of 0, Béky et al. found a nonzero eccentricity of e=0.078+/-0.047 as a best fit, thus matching our requirements of interesting TTV-targets to be observed.

Figure caption: The combined RV data from Béky et al. (red) and Anderson et al. (green).


The number of observed transits for HAT-P-27b lead to a redetermination of the orbital period by about 0.3s. Not TTV analysis possible yet.


The campaign started in 2011 and is continuing in 2013. If you can contribute a light curve, please let me know.


(update: 2013-03-18)


No. Date Epoch Instrument Comment
1 2011 Apr 05 97 Lulin 0.4m
2 2011 Apr 08 98 Lulin 0.4m
3 2011 May 05 107 Trebur 1.2m
4 2012 Apr 01 216 Tenagra II 0.8m
5 2012 Apr 25 224 Xinglong 0.6m

Epochs given according to Anderson et al. 2011


No. Date Telescope Comment
1 2011 May 21 Tenagra II target star saturated
2 2012 Mar 07 Stara Lesna bad conditions for observations
3 2012 Mar 29 Tenagra II 1.5m partly saturated
4 2012 Apr 01 Tenagra II 1.5m partly saturated
5 2012 Apr 04 Tenagra II 1.5m partly saturated
6 2012 May 16 Trebur 1.2m only egress phase observed
7 2013 Jun 06 Calar Alto 1.23m clouds occured, only normal light phase observed


PI: Martin Seeliger martin.seeliger@uni-jena.de

hat27.txt · Last modified: 2017/02/21 10:23 (external edit)
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