Yusei Koyama (NAOJ) From MAHALO-Subaru to ALOHA-TMT: unveiling internal physics of distant galaxies...
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Transcript of Yusei Koyama (NAOJ) From MAHALO-Subaru to ALOHA-TMT: unveiling internal physics of distant galaxies...
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), andMAHALO-Subaru collaboration
TMT science workshop @ 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
ES0
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 Ha/[OII] emission-line survey for 0.4<z<2.5
MApping H-Alpha and Lines of Oxygen with Subaru
Collaborators: T.Kodama (PI), M.Hayashi, K.Tadaki, I.Tanaka, R.Shimakawa
Tadaki+’12Koyama+’13a
Hayashi+’12
z = 30 z = 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
SF main sequence is independent of environment out to z~2 (as far as we rely on Ha-based SFR).
(Koyama et al. 2013b, MNRAS, 434, 423)
From rest-frame R-band
photometry+ M/L correction
Fro
m L
(Ha)
+ M
★-
dep
en
den
t d
ust
co
rrect
ion
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 sampleA(Ha) from
SFR(IR)/SFR(Ha)
A(Ha) fromA(Ha)-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* (>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)
Towards the TMT era
ALOHA-TMTAnatomy with Lines of Oxygen
and Hydrogen with AO on TMT
cluster phenomena !
HST/i-band snapshots (4”x4”=30 kpc for each)
z=2.2 HAEs in PKS1138
M: 24um source X: X-ray source
(Koyama et al. 2013a)
HST morphologies of Ha emitters at z=2
z~2 proto-cluster galaxies (rest-UV)
rest-UVHa
Ha
(seeing)
(seeing)
Ha emitters at z=2.5 in SXDF/CANDELS from Tadaki et al. (2013)
red clum
p rest-UV
HST image(ACS+WFC
3)
HST image(ACS+WFC
3)
Deep TMT+IFU observation will allow us to map Ha/Hb ratio (i.e. extinction map)
over the galaxies.
ALOHA [1]: (Dust-corrected) Ha mapping
Ha-strong (but UV-faint)
dusty red clumps.
Responsible for major SF activity
in these galaxies?
ALOHA [2]: 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 [3] : 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) rest-UV (ACS)
Tadaki et al. (2013) Koyama et al. (2013)
ALOHA-TMT will give us a direct answer !!
ALOHA [3] : 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 Ha-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.