Presentation on theme: "Yusei Koyama (NAOJ) From MAHALO-Subaru to ALOHA-TMT: unveiling internal physics of distant galaxies across environment T. Kodama (NAOJ), K.I. Tadaki (NAOJ),"— Presentation transcript:
Yusei Koyama (NAOJ) From MAHALO-Subaru to ALOHA-TMT: unveiling internal physics of distant galaxies across environment T. Kodama (NAOJ), K.I. Tadaki (NAOJ), M. Hayashi (Tokyo), I. Tanaka (Subaru), R. Shimakawa (Sokendai), and MAHALO-Subaru collaboration TMT science Asahi-seimei building, 16/10/2013
Outline - MAHALO-Subaru quick overview - Prospects for TMT era (ALOHA-TMT) - Summary & Conclusions Thank you ! Hello !
Galaxy properties vs. Environment E S0 Spiral High-density Morphology–Density Relation red, old, low SF activity blue, young, high SF activity Low-density (Dressler 1980)
MAHALO-Subaru project Narrow-band H /[OII] emission-line survey for 0.4
z = 30z = 5 z = 2 z = 3 z = 0z = 1 Subaru: big advantage with wide FoV Yahagi et al. (2005) M=6×10^14 Msun, 20Mpc×20Mpc (co-moving) MOIRCS (4 x 7) MOIRCS Suprime-Cam (34 x 27)
High-z structures revealed by MAHALO (Koyama+11) (Koyama+10) (Hayashi+10, 11) (Tadaki+12) (Koyama+13) (Hayashi+12) z=0.4 z=0.8 z=1.5 z=1.6 z=2.2 z=2.5 Many strong emitters in z>1.5 cluster cores Many strong emitters in z>1.5 cluster cores
SF main sequence is independent of environment out to z~2 (as far as we rely on H -based SFR). (Koyama et al. 2013b, MNRAS, 434, 423) From rest-frame R-band photometry + M/L correction From L(H ) + M -dependent dust correction
Beyond the SF Main Sequence (two important caveats)
Dust extinction depends on environment Cluster SF galaxies tend to be dustier – different SF mode? z=0.4 HAE sample A(H ) from SFR(IR)/SFR(H ) A(H ) from A(H )-M* relation (calibrated at z=0) (Koyama et al. 2013b, MNRAS, 434, 423)
Mass segregation in z>2 proto-cluster (Koyama et al. 2013a, MNRAS, 428, 1551) SF galaxies in z>2 proto-cluster show redder colours and higher M* (>10 11 M ) compared to general field galaxies. : 24um-source red HAE (dusty SF) (J-K AB >1.4, DRG) green HAE (0.8
Towards the TMT era ALOHA-TMT A natomy with L ines of O xygen and H ydrogen with A O on TMT
cluster phenomena ! HST/i-band snapshots (4x4=30 kpc for each) z=2.2 HAEs in PKS1138 M: 24um source X: X-ray source (Koyama et al. 2013a) HST morphologies of H emitters at z=2 z~2 proto-cluster galaxies (rest-UV)
rest-UV H H (seeing) H emitters at z=2.5 in SXDF/CANDELS from Tadaki et al. (2013) red clump rest-UV HST image (ACS+WFC3) HST image (ACS+WFC3) Deep TMT+IFU observation will allow us to map H /H ratio (i.e. extinction map) over the galaxies. ALOHA : (Dust-corrected) mapping H -strong (but UV-faint) dusty red clumps. Responsible for major SF activity in these galaxies?
ALOHA : Spatially-resolved line ratios Pixel-by-pixel BPT diagram from SINFONI+AO observation (Newman et al. 2013) Mapping multiple emission-lines over the galaxies allow us to unveil central AGN, metallicity gradient, excitation state… etc. AGN in the central regionPurely star-forming Redder symbols show galaxy central pixels
Recent discovery: high-z clumpy (field) galaxies are disk-rotating. ALOHA  : Galaxy dynamics with IFU Shapiro et al. (2008) Disk/merger classification with kinemetry merger disk Genzel et al. (2006) Forster-Schreiber et al. (2011)
Is it really true for high-z cluster galaxies as well? Proto-cluster (z=2) General Field (z=2) rest-UV (ACS) Tadaki et al. (2013) Koyama et al. (2013) ALOHA-TMT will give us a direct answer !! ALOHA  : Galaxy dynamics with IFU (and for more normal, low-mass galaxies?)
Summary (2) Using MAHALO sample, we find that SF main sequence is independent of environment at any time in the history of the universe since z~2 (as far as we rely on the H -based SFRs). (4) SF galaxies in z~2 proto-cluster environments tend to be more massive (and have higher SFR) than the field counterparts. (5) High-z galaxies are clumpy (both in clusters and fields). ALOHA-TMT will reveal the environmental impacts on the internal physics of high-z galaxies with deep IFU observation. (1) MAHALO-Subaru unveiled large-scale structures at z>>1 with wide-field emission-line galaxy survey with Subaru. (3) SF galaxies in cluster environments may be more highly obscured by dust – implying a different mode of SF activity from general field galaxies.