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Yusei Koyama (NAOJ)

TMT science workshop @ Asahi- seimei building , 16/ 10/2013. From MAHALO-Subaru to ALOHA-TMT: unveiling internal physics of distant galaxies across environment. Yusei Koyama (NAOJ).

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Yusei Koyama (NAOJ)

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  1. TMT science workshop @ Asahi-seimei building, 16/10/2013 From MAHALO-Subaru to ALOHA-TMT: unveiling internal physics of distant galaxies across environment Yusei Koyama (NAOJ) T. Kodama (NAOJ), K.I. Tadaki (NAOJ), M. Hayashi (Tokyo), I. Tanaka (Subaru), R. Shimakawa (Sokendai), and MAHALO-Subaru collaboration

  2. Outline Thank you ! - MAHALO-Subaru quick overview Hello ! - Prospects for TMT era (ALOHA-TMT) - Summary & Conclusions

  3. “Morphology–Density Relation” (Dressler 1980) red, old, low SF activity Spiral E S0 blue, young, high SF activity Galaxy propertiesvs. Environment Low-density High-density

  4. MAHALO-Subaru project Collaborators: T.Kodama (PI), M.Hayashi, K.Tadaki, I.Tanaka, R.Shimakawa MAppingH-Alpha and LinesofOxygenwith Subaru Narrow-band Ha/[OII] emission-line survey for 0.4<z<2.5 Tadaki+’12 Koyama+’13a Hayashi+’12

  5. Subaru: big advantage with wide FoV z = 30 z = 5 z = 3 MOIRCS z = 2 z = 1 z = 0 MOIRCS (4’ x 7’) Suprime-Cam (34’ x 27’) Yahagi et al. (2005) M=6×10^14 Msun, 20Mpc×20Mpc (co-moving)

  6. High-z structures revealed by MAHALO (Hayashi+10, 11) z=2.2 z=0.4 (Koyama+13) z=1.5 Many strong emitters in z>1.5 cluster cores (Koyama+11) (Tadaki+12) z=0.8 z=2.5 z=1.6 (Koyama+10) (Hayashi+12)

  7. SF main sequence is independent of environment out to z~2 (as far as we rely on Ha-based SFR). From L(Ha) + M★-dependent dust correction From rest-frame R-band photometry + M/L correction (Koyama et al. 2013b, MNRAS, 434, 423)

  8. Beyond the SF Main Sequence (two important caveats)

  9. Cluster SF galaxies tend to be dustier– different SF mode? A(Ha) from SFR(IR)/SFR(Ha) z=0.4 HAE sample Dust extinction depends on environment A(Ha) from A(Ha)-M* relation (calibrated at z=0) (Koyama et al. 2013b, MNRAS, 434, 423)

  10. “Mass segregation” in z>2 proto-cluster SF galaxies in z>2proto-cluster show redder colours and higher M* (>1011M) compared to general field galaxies. : 24um-source ■： red HAE (dusty SF) (J-KAB>1.4, DRG) ■： green HAE (0.8<J-KAB<1.4) ■： blue HAE (J-KAB<0.8) (Koyama et al. 2013a, MNRAS, 428, 1551)

  11. Towards the TMT era ALOHA-TMT Anatomy with Lines of Oxygen and Hydrogen with AO on TMT

  12. HST morphologies of Ha emitters at z=2 cluster phenomena ! z=2.2 HAEs in PKS1138 M: 24um source X: X-ray source HST/i-band snapshots (4”x4”=30 kpc for each) z~2 proto-cluster galaxies (rest-UV) (Koyama et al. 2013a)

  13. ALOHA[1]: (Dust-corrected) Ha mapping rest-UV Ha Ha-strong (but UV-faint) dusty red clumps. Responsible for major SF activity in these galaxies? (seeing) red clump HST image (ACS+WFC3) rest-UV Deep TMT+IFU observation will allow us to map Ha/Hb ratio (i.e. extinction map) over the galaxies. Ha HST image (ACS+WFC3) (seeing) Ha emitters at z=2.5 in SXDF/CANDELS from Tadaki et al. (2013)

  14. ALOHA[2]: Spatially-resolved line ratios Mapping multiple emission-lines over the galaxies allow us to unveil central AGN, metallicity gradient, excitation state… etc. AGN in the central region Purely star-forming Redder symbols show galaxy central pixels Pixel-by-pixel BPT diagram from SINFONI+AO observation (Newman et al. 2013)

  15. ALOHA [3] : Galaxy dynamics with IFU Recent discovery: high-z clumpy (field) galaxies are disk-rotating. Disk/merger classification with “kinemetry” merger disk Genzel et al. (2006) Shapiro et al. (2008) Forster-Schreiber et al. (2011)

  16. ALOHA [3] : Galaxy dynamics with IFU Is it really true for high-z “cluster” galaxies as well? (and for more normal, low-mass galaxies?) rest-UV (ACS) rest-UV (ACS) Proto-cluster (z=2) General Field (z=2) Koyama et al. (2013) Tadaki et al. (2013) ALOHA-TMT will give us a direct answer !!

  17. (1) MAHALO-Subaru unveiled large-scale structures at z>>1 with wide-field emission-linegalaxy survey with Subaru. (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 Ha-based SFRs). (3) SF galaxies in cluster environments may be more highly obscured by dust – implying a different mode of SF activity from general field galaxies. (4) SF galaxies in z~2 proto-cluster environments tend to be more massive (and have higher SFR) than the field counterparts. Summary (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.

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