The 4th Workshop on
Extra-Solar Planet Search withAccurate Radial Velocity
Measurements

7-9 October 2009

Jozankei View Hotel
Hokkaido
Japan

SOC:
Yuqin Chen
Inwoo Han
Hideyuki Izumiura

LOC：
Hiroyasu Ando
Masayuki Fujimoto
Hideyuki Izumiura
Asako Sato
Kiyomi Hatou

Exoplanet Transit Observations at Weihai Observatory of Shandong University
Progress of LiJET and Transit Search with Lijiang 2.4m Telescope

Session 3. Host Stars and Their Evolution I…… Chair:Characteristics of Oscillations in G-type Giants
Spectrophotometric Properties of the Nearest Pre-Main Sequence Stars

8 Thu 10 09:00-09:30 30
11 09:30-10:00 30
12 10:00-10:30 30

Okayama and Subaru Planet Search Programs
Current Status of BOAO Planet Search Program
Current Status and Future Prospect of Exoplanet Searching in Xinglong

Session 4. Doppler Search for Planets among EAPS-NET…… Chair:

18:00-20:00 120 <DINNER>

16:30-17:00 30
17:00-17:30 30

89Orbital Evolution of Planets around Evolving Low- and Intermediate-Mass Stars<BREAK>

15:20-15:50 30

15:50-16:30 40

Planet Formation Theory around Low-Mass or Intermediate-Mass Stars
Planet Formation with Diffrent Disk-Depletion Time Scale: Comparing with Observations

14:00-14:40 40
14:40-15:20 40

Session 2. Theory of Planet Formation and Planetary Systems…… Chair:

12:00-14:00 120 <LUNCH>

11:00-11:30 30
11:30-12:00 30

7

5
6

3
4

<BREAK>

10:30-11:00 30

Session 1. Detection and Characteriztion of Exo Planets…… Chair:Protoplanetary Disks around Intermediate-Mass Stars
Planet Characterization by Transit Observations

09:10-09:50 40
09:50-10:30 40

Welcome Speech

Title

1
2

⊿T

Session 0. Arrival and Registration<Registration><Dinner>

09:00-09:10 10

Time

17:00 ~
18:00-20:00

Time

7 Wed 0Date Day #6 Tue

Date Day #Workshop Program

NAOJ

InstituteSato, B.
Han, I.
Wang L.

Ando, H.
Lyo, A-R.

Ikoma, M.

Tanaka, H.
Liu H.G.

Cao C.
Bai J. M.

TITech
KASI
NAOC

NAOJ
KASI

TITechHokkaido U.
NJU

SDU
YNO

Fukagawa, M. Osaka U.
Narita, N.
NAOJ

Ando, H.

Speaker

9 Fri

Planet search with HDS at Subaru
Current status of Korean-Japanese Planet Search Program
Planet Detection and Abundance Analysis on Late G giants --- Status of Xinglong Planet Search Program<BREAK>, Workshop Photo

Session 5. Instrumentation among EAPS-NET…… Chair:

The Prototype Design and Feasible Experience for Multi-Object Exoplanet-Survey System Based on LAMOST
Optical Frequency Combs for Astronomical Observations
Discussion: Astronomical Application of Optical Frequency Combs<BREAK>

Progress in Developing the Fiber-Link of 188-cm Telescope and HIDESThe High Resolution Spectrograph for Chinese Weihai 1m Telescope
High-Contrast Coronagraph Development in China for Direct Imaging of Extra-solar Planets

Solar Twins: Are They the Best Candidates for Finding Earth-Like Planets?
Discussion: Verification Methods of Exoplanet Candidates<BREAk>Abundances of Refractory Elements for Planet-Host Stars
Stellar Abundance for Galactic Archeology (SAGA) Database and its Extension for Planet-Hosting Stars

Session 6. Host Stars and Their Evolution II …… Chair:

Astronomy in China Today - Large Astronomical Facilities in China

27 14:00-15:00 60

Concluding Discussion

12:00-14:00 120 <LUNCH>

25 11:00-11:30 30
26 11:30-12:00 30

10:30-11:00 30

23 09:30-10:00 30
24 10:00-10:30 20

22 09:00-09:30 30

18:00-20:00 120 <WORKSHOP DINNER>

19 16:00-16:30 30
20 16:30-17:10 40
21 17:10-17:40 30

15:30-16:00 30

16 14:00-14:30 30
17 14:30-15:00 30
18 15:00-15:30 30

12:00-14:00 120 <LUNCH>

13 11:00-11:20 20
14 11:20-11:40 20
15 11:40-12:00 20

10:30-11:00 30

All

Chen, Y. Q.
All

Kang, W.-S.
Katsuta, Y.

Zhao G.

Zhang K.
Inaba, H.
All

Kambe, E.
Wang L.
Dou J. P.

…

NAOC
…

SNU
Hokkaido U.

NAOC

NIAOT
AIST
…

NAOJ
NIAOT
NIAOT

Harakawa, H. TITech
Omiya, M.
Tokai U.
Liu Y.J.
NAOC

Abstract

This page is intentionally left blankProtoplanetary Disks around Intermediate-Mass Stars
Misato Fukagawa (Osaka University)

Circumstellar disks are commonly observed around young A-type stars with infraredexcesses. Observational study of protoplanetary disks gives insight into the initialcondition of planet formation, while that of debris (second-generation) disks may hint
the dynamical history of planetary systems. Therefore properties of disks aroundintermediate-mass stars can be related to statistics of mature planets around G giants.
I first review the observational results for protoplanetary disks around Herbig Ae stars,
comparing with those for lower/higher-mass counter parts, and focusing on their spatial
structure revealed in thermal and dust-scattered emission. High resolution, direct
imaging by Subaru and HST in particular suggests significant variety in the outer diskmorphology, which could be caused by evolution, multiplicity, or local star-forming
environments. In addition to “diversity”, “variability” of disk structure is the other key
to understand how disks evolve during the era of the planet formation. I mention recent
multi-epoch infrared studies using various observing techniques for two
intermediate-mass stars. The variability may be interpreted as temporal change of theinner wall of the dusty disk for one star, and production of debris is implied for anotherone.

Planet Characterization by Transit Observations
Norio Narita (NAOJ)

Transiting extrasolar planets provide us useful information to understand theircharacteristics such as orbits, size, density, etc, through photometric and spectroscopic
observations of planetary transits. I will review several studies on transiting planets
conducted so far, including determination of the planetary size, secondary eclipse
observations, transit timing variations, transmission spectroscopy, and the
Rossiter-McLaughlin effect.

Exoplanet Transit Observations at Weihai Observatory of
Shandong University
Chen Cao (Shandong University at Weihai, China)caochen@sdu.edu.cn

In this talk, I will first give a brief introduction to Weihai Observatory of Shandong
University, mainly focus on its one meter telescope and related instruments. Weihai
Observatory of Shandong University was joint constructed and managed by Shandong
University, National Astronomical Observatories of China (NAOC) and Weihai city.
The one meter German-made reflecting telescope is one of the largest optical telescopes
among all the universities in China for advanced scientific researches.
About one year ago, we began to observe exoplanet transits using this telescope.
Our purpose of research is: 1. Observe short-period exoplanet transits to obtain moredata and try to make new discoveries by transit timing; 2. Try to detect transits ofexoplanets which were discovered by the RV method but still without transit
observations; 3. Prepare to make follow-up photometric observations of exoplanetcandidates discovered by the new high-res spectrographs of NAOC and our university.
In the past year from Oct. 2008 to Sep. 2009, using about 30 nights, we haveobserved 63 predicted transit events and successfully detected 12 of them. The
exoplanets which we detect transits are: TrES-1b, TrES-3b (*4), WASP-1b, WASP-2b,
WASP-3b, XO-2b (*3), HAT-P-7b. I will show these transits’ light curves and somederived results, then make prospects on our further studies.

Progress of LiJET and transit search with Lijiang 2.4m telescope
Jinming Bai (Yunnan Observatory)In this talk, I will briefly introduce the progress of Lijiang Exoplanet Tracker (LiJET)
which will be installed in October 2009, at the 2.4m telescope in Lijiang station of
Yunnan Observatory. Then I will talk about the transit events follow up project with thistelescope. The project is aimed to confirm planet detection and discover new planets,
and emphases will be give to the detection of low mass (a few Earth masses) exoplanets
around nearby bright solar-type stars. Planet candidates are mainly from the
MARVELS (The SDSS-III Multi-object Apo Radial-velocity Exoplanet Large-area
Survey) and SuperWASP (Super Wide Angle Search for Planets). We will also search
for transits in some open clusters with the YFOSC (Yunnan Faint Object Spectrographand Camera) which has a 9’X9’ field of view, and will be installed at the Lijiang 2.4m
telescope by the end of this year.

Planet formation theory around low-mass or intermediate-mass stars
Hidekazu Tanaka (Hokkaido University)

In my talk, I will review the theory of planet formation around various stars. Dependingon the luminosity of the central star and the disk model, the locations of the habitablezone and the snow line would change. This causes a diversity of planet systems formed
around low-mass or intermediate-mass stars. In the present theory of planet formation,
rocky planets (and cores of giant planets) are expected to be formed throughaccumulation of planetesimals but the process of planetesimal formation still has a large
uncertainty. Recent studies of planetesimal formation suggest that planetesimalformation might occur only in a limited region of protoplanetary disks. This limitation
is more strict for intermediate-mass stars than low-mass ones. The limitation onplanetesimal formation would strongly affect the final configuration of planet systems
around intermediate-mass stars.

Planet Formation with diffrent disk-depltion time scale:comparing with observations
Huigen Liu, Zhou Jilin & Wang Su (Nanjing University)

Abstract
There are abundant fruits about the formations of various planets, while theobservational data become more and more abundant. Some theories reproduce the
distribution of a-M (the semi-major axis and the mass of planets) well comparing toobservations. But few people consider the N-body interactions which play a key role
during the evolution of planetary system and excite their eccentricities. This is mainly
because of the exorbitant time-costing of simulations and the uncertainty of initialconditions.
In this series of papers, we focus on the influences of N-body interaction. As weknow N-body interaction may excite the eccentricity by scattering and resonance. This
interaction might still halt the migration of planets by resonance so that the distributionof semi-major axis changes possibly. We survey the distributions of planets especiallythe eccentricity of multi-planetary systems and try to reproduce them by Monte Carloapproach and comparing with observations. In this paper we mainly considerate theinfluence of the gas disk depleted time scale $¥tau_{disk}$, which will influence theevolutions of semi-major axis, planetary mass and eccentricity directly. We set a groupof initial conditions with different $¥tau_{disk}$, and find some correlations. These
correlations would be tested by further observations and will be useful for detecting
other exoplanets.

Orbital Evolution of Planets around Evolving Low- and Intermediate-Mass Stars
Masahiro IKOMA
Department of Earth and Planetary Sciences, Tokyo Institute of Technology, 2-12-1 I2-26 Ookayama, Meguro-ku,
Tokyo 152-8551, Japan; mikoma@geo.titech.ac.jp

About twenty planets orbiting evolved low- and intermediate-mass stars have been detected so far.
Unlike around low-mass main-sequence stars, no planet has been found inside about 0.7AU aroundthose stars. That deficit may be due to the evolution of their parent stars, which I have explored inthis study. A star expands after leaving the main-sequence track and its radius reaches approximately
0.1AU; planets orbiting at < 0.1AU are thus engulfed by the star. In addition, the tidal action of thestar removes the angular momentum from orbiting planets; thereby the planets migrate inward andmay eventually spiral into the parent star. In contrast, loss of the mass of the parent star during its
RGB phase pushes planets outward. In this study, I have simulated changes in semi-major axes ofplanets orbiting low- and intermediate mass stars evolving in the RGB phase, taking into account theeffects of the tidal action and mass loss of the stars. I have not simulated the stellar evolution directly,
but used data available on the Web. Our preliminary results show that the tidal effect dominates the
mass-loss effect, resulting in orbital decay of the planets. The idea examined is consistent with theplanetary deficit in the region interior to 0.7 AU around the intermediate-mass giants. Concerning
low-mass giants, more detailed investigation is found to be necessary, because some of them arehighly eccentric. I will discuss current uncertainties that have to be removed to specify the cause of
the orbital properties of the planets around the evolved stars.

Characteristics of oscillations in G-type giants
Hiroyasu ANDO (NAOJ), Yusuke TSUBOI (Tokyo Univ.),
Eiji KAMBE(NAOJ), and Bun’ei SATO (TITech)

We have performed observation of four G-type giants (ζHya, ηHer, εTau, 11Com) with
precise radial velocity measurement to detect solar-like oscillations. We found tiny
amplitude oscillations in these giants, whose periods range from 4 hours to 10 hours andtheir amplitudes are 1-6m/s. We have conducted period analysis for these stars andconfirmed a significant power excess centered at 30-80 μHz (νmax). In these
period-grams, we can also see some equidistant power peak distribution like solar 5 min.
oscillation, which is called large separation (Δν). These two oscillation characteristics
are confirmed to follow the well-known scaling law. We also investigated damping
time of these oscillations, whose times are about two days. These values are
confirmed to exist in the extension of those for dwarfs like the sun. From these results,
it is concluded that tiny oscillations in G-type giants are solar-like oscillation excited byturbulent convective motions.
In this program, stars with extra-solar planet, say, εTau, 11Com are included to see ifcharacteristics of oscillations may be related with existence of exo-planet. But it isconfirmed that there is no correlation between the two.

Spectrophotometric properties of the nearest pre-main sequence stars
A-Ran Lyo (Korea Astronomy and Space Science Institute)

We present a study of flux-calibrated low-resolution optical spectroscopy of the nearest
pre-main sequence (PMS) associations; Eta Chamaeleontis, Epsilon Chamaeleontis, TW
hydrae, Beta Pictoris, Lower Centaurus Crux. Using synthetic broad-band colors andnarrow-band continuum, temperature- and gravity-sensitive spectral line, we can study
the physical properties of PMS stars. Especially, we found that the gravity-sensitive
indices are the very useful tools to address the age rank of these young stellar groups
compared to the HR diagram.

Okayama and Subaru Planet Search Programs
Bun’ei Sato (Tokyo Institute of Technology)

We have been conducting a Doppler planet search program targetingintermediate-mass (1.5-5Msun) GK giants using the High Dispersion Echelle
Spectrograph (HIDES) and 1.88m telescope at Okayama Astrophysical Observatory(OAO). Since 2001, we have been continuously monitoring about 300 GK giants andfound 9 planets and 1 brown dwarf candidate around them so far. Although the number
is still small, the planets show different properties from those around solar-type stars:
high frequency of super-massive planets, lack of inner planets with semimajor axis of a
<0.7AU, and lack of a metal-rich tendency in the planet host stars. We have also
identified candidates of multi-planet systems and long-period planets residing ina>4AU.
We also started a large scale survey of GK giants using the High Dispersion
Spectrograph (HDS) of Subaru 8.2m telescope in 2006. The main purpose of the Subaru
program is to find planet-host candidates showing large radial velocity variations
efficiently from hundreds of targets thanks to the large aperture of Subaru. We havescreened about 200 stars in the last three years and found about 40 stars showing radial
velocity variations with 30—200 m/s. These stars are now under follow-up observations
mainly at OAO.
We here report the current status of these programs and discuss future prospects.

Current Status of BOAO Planet Search Program
Inwoo Han (KASI, e-mail: iwhan@kasi.re.kr),
B.-C. Lee, (KASI), and K.M. Kim, (KASI)

We have conducted exoplanet survey around about 50 K giant stars since 2003. Our
sample includes some M giant and Ap stars. In this presentation we report the result of
our survey - exoplanet candidates and their statistical characteristics. We will alsopresent the detailed results of some exoplanet stars.

Current Status and Future Prospect of Exoplanet Searching in
Xinglong
Liang Wang (National Astronomical Observatories of China)

As a part of East Asia Planets Search Network (EAPSNet), precise Doppler survey byiodine cell on 2.16m telescope in Xinglong has been undertaken since 2004. About
1,500 exposure of more than 100 G,K giants have been taken in the past 5 years. One
brown dwarf candidate and one planet have been discovered. The 1k x 1k CCD of theCoude Echelle Spectrograph had been replaced by a 2k x 2k one on April, 2009. This
talk will focus on current status, instrumental upgrading and some new ideas on data
reduction pipeline and precision limitation. Furthermore, a laser frequecy comb forwavelength calibration on fiber-feed echelle spectrograph is under development in
NIAOT and Institute of Physics, Chinese Academy of Sciences. An estimation of radial
velocity precision of this new reference system is also given.

Planet search with HDS at Subaru
Hiroki Harakawa, Bun’ei Sato, Shigeru Ida, Yasunori Hori (TITech),
Masashi Omiya (Tokay University), Debra A. Fischer (San Francisco State
University)

Since 1995, precise radial velocity (RV) observations have unveiled more than 350
extrasolar planets from thousands of nearby (<100pc) stars. They show a great diversity
in their mass and orbital parameters, and some theoretical approaches to understand theorigin of the properties have been proposed during the past decade. And new planetswith remarkable properties have been being discovered even now. Thus it is importantto find further planets in various parameter spaces of planets and host stars and toestablish their properties. We have identified tens of planet-host candidates with HDS at
Subaru from a survey carried out in the framework of N2K consortium which is acollaborative planet searching project between US and Japanese teams.
It is important to increase the number of target stars to enlarge the detection ofplanetary candidates. Also, improving the RV precision is important to avoid
observational biases against low-mass planets and enhance the detection rate. We
applied the methods of Sato et al. (2002) to the RV analysis for HDS and attained atypical short-term precision of 5-6 m/s and long-term one of 10 m/s. However, in thecase of Okayama/HIDES with revised RV methods described in Kambe et al. (2008),
the precision of RV observations could reach below 3 m/s which is equivalent to avelocity semi-amplitude of the Sun imparted by a Saturn mass planet in semimajor axisof 5 AU. Furthermore, Keck telescope/HIRES have reached almost 1 m/s. The RV
methods with Subaru/HDS should be improved to catch up with them.

Current status of Korean-Japanese Planet Search Program
Masashi Omiya (Tokai University)

Korean-Japanese Planet Search Program has been carried out since 2005 to search forplanets around intermediate-mass giant stars (1.5-5.0 solar masses) by an international
collaboration between Korean and Japanese researchers. In this planet search program,
we have been carrying out a precise Doppler survey of 188 GK-type giants (6.2<V<6.5)
using 1.8m telescope at Bohyunsan Optical Astronomy Observatory (BOAO, Korea)
and 1.88m telescope at Okayama Astrophysical Observatory (OAO, Japan).
So far, we observed in total 178 stars more than three times and detected about 45
candidate stars in our sample stars. Among the candidate stars, we discovered a browndwarf-mass companion with a semimajor axis of 1.71 AU and a minimum mass of 37.6
Jupiter masses orbiting an intermediate-mass giant star HD 119445 (G6III) with a massof 3.9 solar masses. This companion is the most massive one discovered within 3 AU ofa central intermediate-mass star. The host star also ranks among the most massive stars
with substellar companions detected by the Doppler surveys. This result supports thecurrent view of substellar systems that more massive substellar companions tend toexist around more massive stars.
We also detected a probable planet candidate star. Adopting the host star mass of 2.7
solar masses, the planet has a semi-major axis of 0.8 AU and a minimum mass of 1.8
Jupiter masses. Moreover, we found 7 candidate stars with a periodic radial velocity
variation, which may indicate the existence of a planet or a brown dwarf-masscompanion.
We report the recent results and current status of Korean-Japanese Planet Search
Program.

Planet Detection and Abundance Analysis on Late G giants---Status of Xinglong Planet Search Program
Yujuan Liu (NAOJ/NAOC)

We report the detection of a brown dwarf orbiting the intermediate-mass giant star 11
Comae (G8 III) and a planet candidate around HD173416 from our Japan-China Planet
Search Program. Due to precise Doppler measurements of the stars from Xinglong
station and Okayama Astrophysical Observatory (OAO), the minimum masses of thetwo companions are 19.4±1.5 MJ and 2.7±0.3 MJ, respectively. We make abundance
analysis for a part of Xinglong Planet Search Program sample--58 late G-type giants
taken with OAO, and establish the atmospheric parameters, as well as determine surface
chemical compositions, especially for C and Na.

Progress in developing the fiber-link of 188-cm telescope and HIDES
E. Kambe, M. Yoshida, H. Izumiura, H. Koyano, S. Nagayama, Y. Shimizu,
K. Okita, A. Sakamoto (NAOJ/OAO), B. Sato (Tokyo Inst. Tech.),T. Yamamuro (Optcraft)

We have been developing the fiber-link from the Cassegrain focus of our 188-cm
reflector to its Coude focus where the entrance slit of the HIDES spectrograph locates.
The primary purpose of this project is to increase the through-put of our observing
system by one magnitude, by skipping some mirrors/windows between two foci and by
introducing the image slicer at the fiber output. If it is successful, we will be able tomonitor four times as many targets as we have now for such observations where
exposure times are limited. Thus, exoplanet hunting and asteroseismology are greatly
benefited from this project.
Throughout this project, we also envisage development of a state-of-the-art
fiber-fed high-resolution spectrograph in near future and plan to examine very carefully
how the fiber modal noise affects the signal-to-noise ratio of the spectra and radial
velocity measurement. For this purpose, we have made a low cost, narrow
wavelength-coveraged high-resolution spectrograph on a optical bench at ourlaboratory.
We have almost completed optical components and mechanical parts of thefiber-link and are now making final assembly. We expect to have its first-light verysoon.Okayama and Subaru Planet Search Programs

The high resolution spectrograph for Chinese Weihai 1m telescope
Lei Wang1,2, Yongtian Zhu1,2, Zhongwen Hu1,2
1. National Astronomical Observatories/Nanjing Institute of Astronomical Optics& Technology, Chinese Academy of Sciences, Nanjing 210042,China
2. Key Laboratory of Astronomical Optics & Technology, Nanjing Institute of
Astronomical Optics & Technology, Chinese Academy of Sciences, Nanjing
210042,China

Abstract
Whrs, a high-resolution fiber-fed echelle spectrograph is currently under development
for Chinese Weihai 1m telescope at Weihai observatory of Shandong University. The
flexible scheduling character of Chinese Weihai 1m telescope allows for long-termmonitoring programs with a focus on stellar astrophysics. The Whrs spectrograph will
significantly enlarge the scientific potentiality of 1m telescope with the possibility toobtain high quality spectrum. The optical design is based on a middle R2.9 echelle,
operating in quasi-Littrow and white-pupil configuration, and a double-prismcross-disperser. This instrument records the spectrum from 370 to 940 nm in one
single exposure on a 2k×2k CCD. With a large fiber aperture of 2.5 arcsec, theresolving power is 38000, a value that can be increased to 55000 with an adjustable
slit at the fiber exit. The ThAr lamp or I2 cell wavelength calibration methods isavailable. High instrument stability is achieved by installing the whole instrument in a
precisely temperature controlled chamber. This work presents the spectrographdesign.

High-contrast Coronagraph Development in China for Direct
Imaging of Extra-solar Planets
Jiangpei Dou1, 2, Deqing Ren1, 2, 3, Yongtian Zhu1, 2, Xi Zhang1, 2, 4
1. National Astronomical Observatories/Nanjing Institute of Astronomical Optics& Technology, Chinese Academy of Sciences, Nanjing 210042,China
2. Key Laboratory of Astronomical Optics & Technology, Nanjing Institute of
Astronomical Optics & Technology, Chinese Academy of Sciences, Nanjing
210042,China
3. Physics & Astronomy Department, California State University Northridge,
18111 Nordhoff Street, Northridge, California 91330-8268
4. Graduate University of Chinese Academy of Sciences, Beijing 100049, China
Abstract
A high-contrast coronagraph is proposed for direct imaging of extra-solar planets orbiting nearby
bright stars. We have developed a coronagraph based on the step-transmission filter in which theintensity is apodized with a finite number of steps of identical transmission in each step. At
present, the step-transmission filter based coronagraph has reached a high contrast of 10-6 at anangular distance of 4λ/D. At first, the coronagraph should be installed on a large ground based
telescope equipped with state-of-the-art adaptive optics systems. In that case, contrast ratios
around 10-5 should be accessible within 0.1 arc seconds of the central star, which is promising todirect image the young extra-solar plants. In recent progress, a upgraded coronagraph with circularapodizing filter has been developed to direct image extra-solar planets, which is specificallysuitable for ground observation. For a long-term run, we will improve the contrast of thecoronagraph to 10-9~10-10 through inducing other techniques such as speckle removing anddifferential imaging techniques. Such a coronagraph should be installed on a space telescope andis promising to direct image earth-like planets finally.
Keywords: Extra-solar planet, earth-like planet, high-contrast imaging, stellar coronagraph,apodizing filter.

The prototype design and feasible experience for multi-object
exoplanet-survey system based on LAMOSTKai Zhang1,2,3, Yongtian Zhu1,2

1. National Astronomical Observatories/Nanjing Institute of Astronomical Optics& Technology, Chinese Academy of Sciences, Nanjing 210042,China
2. Key Laboratory of Astronomical Optics & Technology, Nanjing Institute of
Astronomical Optics & Technology, Chinese Academy of Sciences, Nanjing
210042,China
3. Graduate University of Chinese Academy of Sciences, Beijing 100049, China

Abstract
A new technique called External Dispersed Interferometer (EDI) is recently used toenhance the measurement accuracy of medial resolution spectrometer. Now, a related
multi-object system with this advanced technique based on LAMOST is being
developed by NIAOT and NAOC, and supported by National Natural Sciences
Foundation of China (NSFC). This system is composed of a multi-object fixed delay
interferometer and a multi-object medial resolution spectrometer. In the meeting, theprototype design for multi-object exoplanet-survey system based on LAMOST, andsome results of feasible experience inner door are given.
Keywords: External Dispersed Interferometer; multi-object exoplanet-probing system;
multi-object medial resolution spectrometer; multi-object fixed delay interferometer

Optical frequency combs for astronomical observations

Hajime Inaba, Kaoru Minoshima, Atsushi Onae, and Feng-Lei Hong
National Metrology Institute of Japan (NMIJ), National Institute of Advanced Industrial Science and Technology(AIST),
1-1-1 Umezono, Tsukuba, 305-8563 Ibaraki, Japanh.inaba@aist.go.jp
k.minoshima@aist.go.jp
a-onae@aist.go.jp
f.hong@aist.go.jp

Optical frequency combs provide an absolute, repeatable wavelength scale defined by aseries of laser modes equally spaced across the spectrum, which is suitable forastronomical observations [1]. The train of femtosecond pulses from a mode-locked
laser generates a frequency comb equally spaced by the pulse repetition rate, frep.
Therefore, in the frequency domain, the frequency of the pulses can be written as f(n) =fceo + n × frep. Here, fceo is the offset frequency from the multiple of frep, so called“carrier envelope offset frequency”. fceo is originated from a difference between thegroup and phase velocities of the pulses. The detection of fceo is a key technique tocount optical frequency based on microwave reference frequency. n is a large integer,
typically between 30 000 and 10 000 000. Optical frequencies f(n) are at hundreds of
THz whereas both frep and fceo are radio frequencies and can be handled with present
electronics and stabilized by an atomic clock. The preciseness in each mode’s absolute
frequency is basically dominated by the reference clock.
We have developed mode-locked, erbium-doped fiber-laser-based frequency combs(fiber combs) because of their robustness, compactness, and cost effectiveness in recent
years. In this presentation, basics and a proposal of the comb used for the
astronomical observations are described.
[1] T. Steinmetz, et al., Science 321, 1335 (2008).

Astronomy in China Today- Large Astronomical Facilities in China
Gang Zhao (NAOC)

During the last decade, astronomy in China has experienced enormous advances, among
which the most significant progress is reflected by the construction and development oflarge astronomical facilities. This talk will give a brief introduction of some facilities
and missions representing current status of astronomy in China as well as future projects
in designing and planning. Many ground-based facilities have been or are planned to bebuilt, including the Large sky Area Multi-Object fiber Spectroscopic Telescope(LAMOST), which is unique in combining a large aperture with wide field of view and
worldly renowned for its unprecedented 4000 fibers for spectroscopy; theFive-hundred-meter Aperture Spherical Radio Telescope (FAST), and taking advantageof the unique Karst depression of the site; the 21 CentiMeter Antenna (21CMA), whichaims to carry out a survey to detect the first light after Big Bang, and a number offacilities for solar physics. On the other hand, progresses in space missions are also
remarkable. With the successful launch of the first dedicated Chinese space astronomy
satellite Chang’E, several more missions with strong international collaborations areplanned for launch in between 2010 through 2015, which includes the Hard X-ray
Modulation Telescope (HXMT), a multi-wavelength GRB project - SVOM, the WorldSpace Observatory (WSO/UV), space lab for GRB polarization - POLAR, and also aseries of space telescopes for solar physics like Space Solar Telescope (SST), and SMall
Explorer for Solar Eruptions (SMESE). The development of large facilities vividly
witnesses and strongly reflects the impressing progress taking place in the astronomy ofChina, and also promises a more prosperous future for Chinese astronomy.

Abundances of Refractory Elements for Planet-Host Stars
Won-Seok Kang1, Sang-Gak Lee1, Kang-Min Kim2
1

Department of Physics and Astronomy, Seoul National University,
2
Korea Astronomy and Space Science Institute

We obtained the spectra of Planet-Host Stars(PHSs) and normal field stars of the same
spectral type with BOES. We measured the equivalent width of Fe and some refractoryelement lines using the automatic EW measurement program, TAME(Tools for
Automatic Measurement of Equivalent-widths). Since the absence of planets in thenormal field stars cannot be "completely" proved, this work focused on the PHSs whichhave the massive planets close to the parent star relatively, called as "Hot Jupiter". We
carried out an investigation for the difference of abundances between stars with "HotJupiter" and normal field stars with no known planets. We examined the chemicalcomposition of the host stars with planets, especially "Hot Jupiter", to find somecharacteristic feature.

Stellar Abundance for Galactic Archeology (SAGA) Database andits Extension for Planet-Hosting Stars
Yutaka Katsuta (Hokkaido University)

One of the major characteristics of the planet-hosting stars(PHS) is that they have highsurface metal abundances. These overabundances are well studied on iron, and PHSs
have on average about 0.2 dex overabundance in [Fe/H] compared to average stars. In
recent years, many researches are presented on PHSs' chemical abundances other thaniron, and the differences in the chemical abundance between PHS and non-PHSs are
discussed. In this talk we introduce the metal-poor star database system (SAGA;
http://saga.sci.hokudai.ac.jp/) which is open to the public since 2008, and the metal-richstar and PHS database system under development. The SAGA is designed as a
web-based application, so that users can search objects and plot data such as chemical
abundances, stellar parameters and so on with a web-browser. These data and functionsof the database with extension to metal-rich stars and PHSs enable us to use theenormous data statistically, and it is expected that the databases helps us to clarify the
Galactic chemical evolution from extremely metal-poor stars to the super-metal-richstars and reveal the nature of the PHSs.

Solar Twins: Are They the Best Candidates for
Finding Earth-like Planets?
Yuqin Chen (NAOC)

The search and the study of stars identical to the Sun (solar twins) are interesting in thesense that they may be the best targets for future space missions that will probe
Earth-like planets. In this respect, we have carried out the search for solar twins among
photometrically-selected solar analogues in the solar neighborhood and made thedifferential abundance analysis between solar analogues and the Sun.
In this talk, I will involve with three subjects. Firstly, present status of finding solar
twins in the literature is briefly introduced and the colors of the Sun are derived fromsolar twins by product. Then the detection of one new solar twin among 27 solar
analogues in our project and its main characteristics are presented. Finally, we attempt
to summarize the observation views on the physical link between solar twins withearth-like planet search in the future.

The new high resolution spectrograph for Chinese 2.16 metertelescope
Yongtian Zhu1,2, Zhongwen Hu1,2, Lei Wang1,2, Yi Chen1,2
1. National Astronomical Observatories/Nanjing Institute of Astronomical Optics &Technology, Chinese Academy of Sciences, Nanjing 210042,China
2. Key Laboratory of Astronomical Optics & Technology, Nanjing Institute of
Astronomical Optics & Technology, Chinese Academy of Sciences, Nanjing 210042,China

ABSTRACTThe new high-resolution echelle spectrograph that is currently underconstruction to be used for Chinese 2.16 meter telescope is presented. In orderto obtain a resolution-slit product of about 76800 as required by science case,the less expensive design used a 140 mm beam feeding a 420mm deep Echelle(R3) is good solution. The optical design of high resolution Echelle
spectrograph for Chinese 2.16 meter telescope is given. This spectrograph will
be more powerful tool for exoplanet research using high-resolution
spectroscopy in China. Some new technology and novel design concepts havebeen adopted in this spectrograph, such as white pupil collimator system andall-refracting camera without central obstruction and so on.
Keywords: Instrumentation; spectrograph; high resolution; Echelle grating.

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Professor
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PhD student
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Engineer
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PhD student
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Professor
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Professor
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Post Doctral Fellow
Post Doctral Fellow
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Researcher
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Associate Professor
Associate Professor(Family, Given)
China
Bai Jinming
Cao Chen
Chen Yuqin
Dou Jiangpei
Liu Huigen
Liu Yujuan
Wang Lei
Wang Liang
Zhang Kai
Zhao Gang
Zhu Yongtian

Korea
Han Inwoo
Kang Won-Seok
Lyo A-Ran

Japan
Ando Hiroyasu
Baba Naoshi
Fujimoto Masayuki
Fukagawa Misato
Harakawa Hiroki
Ikoma Masahiro
Inaba, Hajime
Izumiura Hideyuki
Kambe Eiji
Katsuta Yutaka
Narita Norio
Omiya Masashi
Onae Atsushi
Sato Bun'ei
Tanaka Hidekazu
Yoshida Michitoshi

National Astronomical Observatories of Japan
Hokkaido University
Hokkaido University
Osaka University
Tokyo Institute of Technology
Tokyo Institute of Technology
National Institute of Advanced Industrial Science and Technology
National Astronomical Observatories of Japan
National Astronomical Observatories of Japan
Hokkaido University
National Astronomical Observatories of Japan
Tokai University
National Institute of Advanced Industrial Science and Technology
Tokyo Institute of Technology
Hokkaido University
National Astronomical Observatories of Japan

Korea Astronomy and Space Science InstituteSeoul National University
Korea Astronomy and Space Science InstituteYunnan Astronomical Observatories, Chinese Academy of Sciences
Shandong University
National Astronomical Observatories, Chinese Academy of Sciences
Nanjing Institute of Astronomical Optics and Technology
Nanjing University
National Astronomical Observatories, Chinese Academy of Sciences
Nanjing Institute of Astronomical Optics and Technology
National Astronomical Observatories, Chinese Academy of Sciences
Nanjing Institute of Astronomical Optics and Technology
National Astronomical Observatories, Chinese Academy of Sciences
Nanjing Institute of Astronomical Optics and Technology

List of Participants

7-9 October 2009
Jozankei View Hotel Hokkaido JapanThe 4th Workshop on Extra-Solar Planet Searchwith Accurate Radial Velocity Measurements

ando.hys@nao.ac.jp
nbaba@eng.hokudai.ac.jp
fujimoto@astro1.sci.hokudai.ac.jp
misato@iral.ess.sci.osaka-u.ac.jp
harakawa@geo.titech.ac.jp
mikoma@geo.titech.ac.jp
h.inaba@aist.go.jp
izumiura@oao.nao.ac.jp
kambe@oao.nao.ac.jp
kat@astro1.sci.hokudai.ac.jp
norio.narita@nao.ac.jp
ohmiya@peacock.rh.u-tokai.ac.jp
a-onae@aist.go.jp
sato.b.aa@m.titech.ac.jp
hide@lowtem.hokudai.ac.jp
yoshida@oao.nao.ac.jp

iwhan@kasi.re.kr
wskang@astro.snu.ac.kr
arl@kasi.re.kr

baijinming@mail.ynao.ac.cn
caochen@sdu.edu.cn
cyq@bao.ac.cn
jpdou@niaot.ac.cn
huigen@nju.edu.cn
lyj@bao.ac.cn
leiwang@niaot.ac.cn
Wangliang@bao.ac.cn
kzhang@niaot.ac.cn
gzhao@bao.ac.cn
ytzhu@niaot.ac.cn