1 -> 0.5 -> -> BC384-322) ( )

 1  ->  0.5  ->     ->      BC384-322)   (  )

1 -> 0.5 ->

->

BC384-322)

( )

Takeshi Chiba Cosmology with x-matter Takeshi Chiba, Naoshi Sugiyama, Takashi Nakamura, Monthly Notices of the Royal Astronomical Society, 289,

L5-L9 (1997). 1996 COE

XCDM paper by Turner and White(1997) : p=w x componentx component

Only 7 SNIa and decelerating universe XCDM paper by Turner and White(1997) : p=w x componentx component

cs2=w<0 w0 cs2 X-matter: p=w00+ccs2 (-0) w c 2 X-matter

0 s ( ) X-matter Turner-White Caldwell-DaveSteinhardt(quintessence)

(Nomura-Watari-Yanagida) Only 7 SNIa and decelerating universe

Union 2.1: 580 SNIa 1105.3470 review by Copeland-Sami-Tsujikawa(2006) Turner White: 388 Chiba Sugiyama Nakamura: 116 Caldwell Dave Steinhardt:

1735 (1998) CMB A B B A

(AIC) : Likelihood =chi^2 +c 2 x (# of parameters) likelihood AIC

: a paper should be concise as much as possible should include x componentanything new even if it sounds uninteresting then

Kinetically Driven Quintessence Takeshi Chiba, Takahiro Okabe, and Masahide Yamaguchi, Physical Review D62, 023511 (2000). PD 2 p

Armendariz-Picon, Damour, Mukhanov paper (k-inflation) May(1999): p(X); X=(d/dt)dt)2 p=p(X), =2Xp,X-p

- d/dtdt k-inflation ( D1)

6 power-law model (dark energy with constant equation of state) Phantom menace paper by Caldwell: possibility of w<-1

PRD 1999 11 kinetically driven quintessence

10 (Tracking k-essence)

K-essence 4 Armendariz-Picon,Mukhanov,Steinhardt: k-essence 2000 4

2 1/dt)R Gravity and Scalar-Tensor Gravity Takeshi Chiba,

Physics Letters B, 575, 1-3 (2003). Carroll-Duvvuri-Trodden-Turner s influential paper appeared on arxiv June, 2003: R-M4/dt)R

: R, etc Strings 2003 (Kyoto) coffee break

(R ) =0! 3

Carroll (Cline, Kaloper, Flanagan, Kamionkowski )

Mark Kamionkowski (Tristan Smith and Adrienne Erickcek): f(R) Hello Dr. Chiba, We would like to call your attention to our preprint astroph/dt)0610483 where we address issues related to calculating the Solar System spacetime in F(R) = R-\mu4/dt)R gravity theory. We thought, given your work in astro-ph/dt)0307338,

you would find this article interesting. You might be aware of a recent controversy surrounding the use of scalar/dt)tensor theories to study F(R) modifications to GR. In particular, there are several articles which cast doubt on the statement that \gamma = 1/dt)2 for F(R) = R-\mu4/dt)R gravity theory. We thought you might be interested in a calculation that reproduces your result of \gamma = 1/dt)2 without appealing to scalar/dt)tensor theory. We would appreciate any comments that you might have.

Thank you very much. Sincerely, Tristan Smith and Adrienne Erickcek 3 e-mail

Thanksgiving Day 3 JGRG arXiv PPN

Brans-Dicke PPN parameter (primordial/dt)secondary) nonGaussianity : (Chiba-Takahashi, Chiba-Nakamura,07): compare H(z) or m

Tycho Brahe : 2 f m/dt)r2 f(r)

f=GMm/dt)r2 It is just the research field very few people (in Japan) did at that time: I might be able to be the first person! Nowadays, everyone talks about dark

energy Takashi Nakamura, Naoshi Sugiyama, Masahide Yamaguchi, Takahiro Okabe, Ryuichi Takahashi, Ryo Nagata, Tristan L. Smith, Adrienne L. Erickcek., Sourish Dutta, Robert J. Scherrer, and others for fruitful collaboration!

JSPS, Kyoto University and Nihon University for financial support

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