Download - Planet search with HDS at Subaru
Planet search with HDS at Subaru1Tokyo Institute of TechnologyHiroki Harakawa,
Bunei Sato, Shigeru Ida, Yasunori HoriTITech,Masashi OmiyaTokai Univ., Eri ToyotaKobe Science Museum, Debra A. Fischer (Yale Univ.)#13Todays MENUN2K consortium ~a planet searching project~StrategyCurrent StatusImproving the precision of RV analysis for Subaru/HDS
Summary22consortiumA collaborative planet searching project between US and Japanese teamAiming to detect Transit PlanetsRadial Velocity observations with I2 cellHigh Dispersion Spectrograph (Subaru/HDS)The RV precision: 45m/sSurveying for Hot Jupiters around ,, dwarfs & subgiantsSubaru holds 630 targets3
KeckMagellanSubaru3StrategyNext 2,000 (N2K) starsV < 10.5, d < 110 pc, FGK V, IVHigh priority to metal-rich stars
3+1 nights observation3 observations in 3 nights in a row1 scatter > 20 m/s follow up1 scatter < 20 m/s dropVerify candidates to reject binary system in 1 month later4Current Status of Subaru N2KOrbital determination to 4 candidatesShort period (P < 25 d) and transiting!!HD149026b(Sato et al. 2005, ApJ)HD17156b(Fischer et al. 2007, ApJ)Long period (P > 400 d) and low eccentricity (e < 0.1)HD16760b(Sato et al. 2009, ApJ)HD38801b(Harakawa et al. submitted to ApJ)Above 40 planetary system candidates
Overall status of N2K consortiumDiscovered 23 exo-planetsDetection rate of Subaru 10MJUP, P > 100 d, e < 0.1
A small improvement of the RV analysis methodModified how to select data for stellar templateImprovement of long term precision of RV10 m/s to 5 m/sFurther improvement should be made< 3 m/s1818The shape of IP is affected by the optical condition(ex: temperature, humidity) changes every moment in HDS, HIDES is also determined by seeing size
19
1920
The shape of IP is affected by the optical condition(ex: temperature, humidity) changes every moment in HDS, HIDES is also determined by seeing size
20Stellar templateS(+) Sato et al. (2002)
Iobs
5S/N2110
Result of incorrect IP modeling
22IP (Instrumental Profile)PSF (Point Spread Function)IP(convolution)23pixelI (photon count)pixelI (photon count)*IP23HD16760bHD16760(G5V, V=8.7)M1=0.78M, R1=0.81R,[Fe/H] = 0.067
Period:466.5 dSemi-amplitude:407.7 m/sMin. mass:13.1MJUPSemi-major axis:1.1AUEccentricity:0.084
Low-eccentricity brown dwarf24
NEWSato et al. 2009, ApJ32003600400044004800JD(-2450000)HD38801bHD38801(K0IV, V=8.26)M1=1.36M, R1=2.53R,[Fe/H] = 0.26
Period:696.0 dSemi-amplitude:200.0 m/sMin. mass:10.7MJUPSemi-major axis:1.7AUEccentricity:0.03
Super massive planet with almost circular orbit25
NEWHarakawa et al. submitted2001000-100-200Radial velocity [m/s]38004000420044004600JD(-2450000)
HD38801bHD16760bM sin i [MJUP] or 26 2627
0.5Strategy14000V 26 -> 236 Cet, Procyon37
HIDES 2006/20075.6 m/s (Sato et al. 2002) 2.9 m/s < 3 m/s Cet Cet, Procyon38
HIDESLick200210m/sRVLickProcyonKambe et al. 2008Sato et al. (2002)IP-Cet 2.9m/s Procyon 10 m/s 39CCDpixelDoppler-shift40()
40S/N(Butler et al. 1996)
41HDS
S/N or
i: i
iiwave length (pixel)I (photon count)i41S/N=150, R=60,000, Na-D line (=5890)
42HDS2.0[m/s]42HDS HD940734 [m/s] 10 [m/s] 143HDS
433444 (Lick Observatory)pixelwavelengthpixelwavelength343 ()4rINT4.45 (m/s)4.38 (m/s)rBIN5.49 (m/s)4.64 (m/s)44
4545
46m*mp sini(sini)
Doppler shift
47
(z)target star
47
.48m*mp sini(sini)
Doppler Shift 49
target star(z)(RV)
Keplers 3rd Law
m2p m1*
m*mp sini(sini)
50.Mayor
Th-Ar
51
52a:e:i :::T:
(z)target star
ESO 3.6-m Telescope
HIDES(High Dispersion Echelle Spectrograph)photo : B Sato