BINARIES - Key to Comprehension of the Universe, Brno, Czech Republic, June 8-12, 2009

Selim O. SELAMMesut YILMAZ

Ankara University Observatory

Hideyuki IZUMIURAOkayama Astrophysical Observatory-

NAOJ

Ilfan BIKMAEVKazan State University

Bun’ei SATOTokyo Institute of Technology

Eiji KAMBEOkayama Astrophysical Observatory-

NAOJ

Varol KESKİNEge University Observatory

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HD 114762 (F9 V)Latham et al., 1989,

Nature, 339, 38

M sini = 11 Mjup

Porb = 84 days

i = ? a Brown Dwarf ?

Confirmed byMarcy in 1996

M sini = 11.02 Mjup

Porb = 84.03 daysa = 0.35 AU

Cephei (K1 IVe + M4V)

Campbell, Walker & Yang, 1988 ApJ, 331, 902

K = 25 m/s

Porb = 2.7 years

M sini = 1.7 Mjup

?

Orbital Phase

Vr

(km

/s)

Confirmed byHatzes et al., 2003,

ApJ, 599, 1383

M sini = 1.7 Mjup

Porb = 2.48 yearsa = 2.13 AU

Rad

ial v

elo

city

(m

/s)

Years

PSR 1257 + 12 Wolszczan & Frail, 1992, Nature, 355, 145

M sini : 3.4 M & 2.8 M

Porb : 66.6 days & 98.2 days

a : 0.36 AU & 0.47 AU

3th planet ?!

51 Peg bMayor & Queloz 1995

Nature, 378, 355

M sini = 0.47 Mjup

Porb = 4.231 days

a = 0.05 AU

G1 V

14.1 pc

70 Vir bMarcy & Butler 1996

ApJ, 464, L147

M sini = 6.6 Mjup

Porb = 116.6 days

a = 0.43 AU

G2.5 V

17.8 pc

47 UMa bButler & Marcy 1996

ApJ, 464, L153

M sini = 2.39 Mjup

Prot = 2.98 years

a = 2.1 AU

G0 V

5.1 pc

• Doppler Technique

• Astrometry

• Planetary Transits

• Microlensing

• Direct Imaging

• Timing

• Polarimetry

322 (>90% DT)

8

11

7

by 1st June 2009

59

0

348

Data from: Schneider J., 2009, http://exoplanet.eu

Data From: Schneider J., 2009, http://exoplanet.eu

0.1

1

10

100

1000

10000

1988 1990 1992 1994 1996 1998 2000 2002 2004 2006 2008 2010 2012

Doppler - As trom etry

Trans its

Microlens ing

Direct Im aging

Tim ing

M s

in i

(M

Ea

rth

)

Time of Discovery (years)

EARTH

NEPTUN

SATURN

JUPITER

621 3 1 1 6 1 7 11 19 12 34 25 28 32 28 62 = 34815

DOPPLER TECHNIQUE

Jupiter 12.4 m/sec

Saturn 2.7 m/sec

Earth 0.1 m/sec

Mercury 0.01 m/sec

rV

Limitations in precision of measured radial velocities arise

from spatial and temporal differences in the way of

obtaining the stellar and reference spectra

a) taken at different times

b) taken over different optical paths

c) flexture and thermal changes

in the spectrometer

1 km/s

Griffin & Griffin, 1973 (MNRAS, 162, 243 and MNRAS, 162, 255)

Telluric Lines ( 6800-7400 Å)

40 - 50 m/sn

FT

t

PAo

MonochromaticLight wave

1/P

Ao

Delta Function

1/P

AoPerfect

Spectrograph1/P

AoReal

Spectrograph

1/P

Ao

1/PInstrumental Profile

The instrumental profile produces a 2-4 pixel wide “BLURING” effect and can be represented with Gaussian profiles.

INSTRUMENTAL PROFILE (IP)

INSTRUMENTAL PROFILE (IP)

There is no problem with the IP if it not chance its character with time

stablesymmetic IP

stableasymmetic IP

IP with time dependentcharacter

V

V ~ 40-50 m/s

DOPPLER TECHNIQUE

A Thermally Stabilized Gas Absorption Cell

in the front of the entrance slit of a spectrograph

Iodine Cell (I2) gas filter

Butler et al., 1996, PASP, 108, 500

3 m/s ! (Lick 3m) 1 m/s ! (Keck 10m)

Overlays thousands of sharp I2 lines between 5000-6000 Å

onto stellar spectrum

THE MODEL

IPSAkI )()()(

I() : Observed “star+I2” composite spectrum

S() : Intrinsic stellar spectrum

: Stellar Doppler shift

A() : “Transmission function of the I2 Cell”- I2 template

IP : “Instrumental Profile” – produced by the 1D Point Spread Function of the detector

k : normalization factor

* : represents the convolution process made by FT

DOPPLER TECHNIQUE

(Butler et al., 1996, PASP, 108, 500 / Endl et al., 2000, A&Ap, 362, 585 / Takeda et al., 2002, PASJ, 54, 113 / Sato et al., 2002, PASJ, 54, 873)

The observed stellar spectrum through an I2-cell I() is expressed as the

product of intrinsic stellar spectrum S(), and the transmission function of

the I2-cell A() convolved with a modelled IP

THE MODEL

DOPPLER TECHNIQUE

The modeling process can be divided into the following three major steps (Endl et al., 2000):

Step 1: Reconstruction of instrumental effects and spectrograph instrumental profiles by modeling

pure iodine spectra using a high resolution Fourier Transform Spectrum (FTS) of the I2-cell.

Transmission function of the I2-cell, A() is also obtained at this step.

Step 2: Obtaining the “template” stellar spectra by deconvolving a pure star spectrum (taken without

the I2-cell) with the IPs reconstructed in step 1.

Step 3: Complete modeling of the star+I2 spectrum. Transmission function of the I2-cell from step 1

and the deconvolved “template” stellar spectrum from step 2 serve as model templates, A() and

S() to synthesize the observation. The Doppler shift between the iodine reference and the stellar

absorption lines is determined with high accuracy.

LICK GroupValenti et al., 1995, PASP, 107, 966Butler et al., 1996, PASP, 108, 500

ESO GroupEndl et al., 2000, A&Ap, 362, 585

OKAYAMA GroupTakeda et al., 2002, PASJ, 54, 113

Sato et al., 2002, PASJ, 54, 873

Turkish National Observatory (TUG)RTT150 Telescope - CES

Taurus Mountains-Bakirlitepe / Antalya, h=2500 m, 36º 49' 27“ N, 30º 20' 08“ Ehttp://www.tug.tubitak.gov.tr

RTT150 TelescopeØ = 1.5 meters

Coude f/48Cassegrain f/7.7

Coude Echelle Spectrograph (CES)R = / = 40 000

slit width = 1.5 arcsec (500 m) 3800 – 10000 Å (85 orders)

SAO-RAS 1Kx1K 16m pix LN cooled F.I. CCD

Registered wavelength interval on CCD 3900 – 8700 Å (68 orders)

To start exoplanet searches at Turkish National Observatory (TUG)we established an international collaboration

between Turkish-Russian-Japanese colleagues

An I2-Cell and its temperature controller was produced by our Japanese colleagues at Okayama Astrophysical Observatory (OAO)

and successfully integrated to RTT150-CES on OCTOBER 2007

(for technical details, see: Kambe et al., 2002, PASJ, 54, 865)

First Ligth with new I2-Cell26 October 2007

Test Observations

2007-II : TUG_RTT150.07.47 test

2008-I : TUG_RTT150.08.11 test

2008-II : TUG_RTT150.08.47 test + targets

2009-I : 09A_RTT150-439-2 test + targets

44 allocated nights distributed within 1.5 YEARS

Radial Velocity Standards

and

well known Planet-harboring Stars

whose RV behaviors are well established

within a few m/sn

Radial Velocity Standards Planet-harboring Stars

iot Per

tau Cet

ACHIEVED RV PRECISION

For V=3 mag stars under ~15 min. exposure time (S/N=200)

10-15 m/s

For V=6.5 mag stars under 30 min. exposure time (S/N=100)

~25 m/s

TARGET STARS OF OUR PROJECT50 G-type giants

showing RMS>25 m/s RV variation in previous RV surveys

• slow rotators, many sharp absorption lines

• relatively stable against pulsations

• relatively low surface activity