観測的宇宙論ゼミ 4/21 田中 ( 賢 ) 担当分 のおもしろかった話をかいつまみます。

Highlights from VVDS O. Le Fevre

LSS out to z>1! Garilli et al. in prep. The most massive gals already in place by z= Low-mass gals strongly evolve. Pozetti et al. in prep.

Magnitude selected high-z galaxies A significant fraction of high-z gals cannot be selected via the Lyman-break technique.

Luminosity function of 3<z<4 gals M* brighter than 0.7mag at least. LD(VVDS)/LD(LBG)=2.8 (alpha=-1.4, M(1700)<-21) Paltani et al. in prep.

N. Drory Optical-nearIR photo-z sigma(z/1+z)=0.028 alpha=-1.6 is unlikely Steidel et al FORS Deep Field

“zOSMOS”, S. Lilly 600 hours on VLT! Obs in progress.

“Deep2 survey”, A. Coil 3 sq. degrees of sky 4 fields (0.5 o x <2 o ) - lower cosmic variance errors primary z~ (pre-selected using BRI photometry) >40,000 redshifts comoving volume: ~5·10 6 h -3 Mpc slitmasks over 80 Keck nights One-hour exposures R AB =24.1 limiting magnitude 1200 l/mm: ~ Å 1.0” slit: FWHM  68 km/s - high-resolution

BO effect in DEEP2 Gals in groups stop forming stars at z~1.5? Gerken et al in prep.

SWIRE, A. Franceschini The Spitzer Wide-area Infrared Extragalactic Survey: is the largest Spitzer Legacy Program (851 hours) is an areal survey of 50 square degrees, split into 6 sky areas is specifically located in the lowest-background regions of the IR sky. Most optical survey regions have very high infrared backgrounds covers the wavelengths: 3.6, 4.5, 5.8, and 8μm with the Infrared Array Camera, and 24, 70, 160 μm with MIPS also includes UgriZ imaging over most of the survey area is publicly available makes available advanced data products including images and catalogs can detect an L* galaxy to z=2 is equivalent to the Sloan Digital Sky Survey at higher redshift, encompassing the same volume at z=1 as the SDSS

SWIRE, A. Franceschini Red: SWIRE data (Shupe et al.) Black: Papovich et al (2004), Chary et al (2004) Ngal of 24um sources peaks at 0.3uJy......tricky interpretation.

“Morphology-Density Rel. in COSMOS”, P. Capak Morphology : Asymmetry + Gini (on ACS images) Photo-z selected? Accelerated evol. in high-density env.

“evolution of early-type gals ”, E. Bell emergence of red-sequence Red/Blue stellar mass func. Weak evolution in blue gals, and strong evolution in red gals.

IR LF very strongly evolves. Almost all SF is in the blue guys. IR LF evolution --> SMF evolution From SF history to SMF evolution

Merger rate : ~1/3 per L* gal. Mergers are not the only way to make blue gals red.

“massive gals at high-z”, A. Fontana GOODS+MUSIC catalog --> photo-z Stellar Mass U-V 2<z<3.5 Bimodal color distrib. up to z~3, inconsistent with Bell et al.? Massive gals at 2<z<3.5 are intrinsically red.

“SF gals at z~2”, E. Erb Near-IR spec. obs. of z~2 gals. Mass-metallicity relation at z~2: offset at all masses compared to local relation. They dicsuss the origin of this relation.

“LFs and SFRs at z=6-10”, R. Bowens z~6 z~3 M* =  =  * = I'-dropouts : LF at z~6. Lumonisity evolution gives a good fit.

■ 大規模可視分光サーベイはすごい 。 ■ Spitzer はすごい。 ■ SDF/SXDS という言葉を耳にしなかった … 。