mapping star formation at the peak epoch of galaxy formation and evolution “mahalo-subaru”...
TRANSCRIPT
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Mapping star formation at the peak epoch of galaxy formation and evolution
“MAHALO-Subaru”
MApping HAlpha and Lines of Oxygen with Subaru
Taddy Kodama (Subaru Telescope),
Yusei Koyama (Univ of Tokyo),Masao Hayashi (NAOJ),Kenichi Tadaki (NAOJ/UTokyo),Ichi Tanaka (Subaru Telescope), et al.
Hα survey in CL0939 (z=0.41) (P19)
[OII] survey in CL0218 (z=1.62) (P21)
[OII] survey in CL0332 (z=1.61) (P20)
A Subaru Intensive Program for S10B-S11A, started in last Sep.
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z = 3
Nature? (intrinsic)
earlier galaxy formation and evolution in high density regions
Nurture? (external)
galaxy-galaxy interaction/mergers, gas-stripping
SpiralsLenticulars
Ellipticals
Star-forming(young)
No/little SF(old)
morphology‐density relation(Dressler 1980)
z~0
log surface density (Mpc-2)
Nature? (intrinsic)
Need to go higher redshifts when it becomes more evident.
Nurture? (external)
Need to go outer infall regions to see directly what’s happening there.
What’s the origin of the environmental dependence
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ACS(3.5’)
XMM1.14
PPanoramic anoramic IImaging and maging and SSpectroscopy ofpectroscopy of CCluster luster
EEvolution with volution with SSubaruubaru
XMMJ2215.9-1738 22 15 58.5 -17 38 02.5 1.45 4.4 VRi’z’,NBCIGJ0218.3-0510 02 18 21.3 -05 10 27 1.62 BVRi’z’,NB
z~1.5XMMXMM
~10 X-ray clusters (0.4 < z < 1.6) are completed
Kodama et al. (2005) +update
,NB
( )
( )
( )
( )
( )
( )
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75%
50%
25%
Cluster outskirts is the key environment for environmental effects
Sharp color transition in the “medium-density” regions
( i.e. cluster outskirts / groups / filaments )
Kodama et al. (2001), see also Tanaka+05 and Koyama+08
ClusterGroup
Field
Log Σ (galaxy number density)
(SFRHα > 0.3M☉/yr)
Hα (6563A)@z=0.4
NB921
z’
“Octopus cluster “ (CL0939 cluster at z=0.4)
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BB selection (passive) + NB emitters (active)
Hα emitters
All true members
phot-z member
spec-z member
Phot-z distribution of true members
Kodama et al. (2004)
CL0024 cluster (z=0.4)
NB912 + Suprime-Cam
Advantages of NB survey:(1)Good indicators of SFR, especially Hα (low reddening, well calibrated)(2)“Unbiased” sample (no pre-selection of targets is required).(3)“Complete” census of star forming galaxies to a certain limit in SFR.(4)Membership can be confirmed by the presence of emitters in NB +colours.(5)On top of the phot-z selected members (e.g. “passive” galaxies), we can pick out “active” galaxies which tend to be missed by phot-z selection.
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Koyama et al. (2011),
□: Hα emitters
□: red Hα emitters
□: weak Hα emitters (SFR<0.75M☉/yr)
(B-I>2)
“Octopus cluster”(CL0939@z=0.41)
see P19
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Red Hα emitters in groups !
A significant fraction of red galaxies in groups show SF activities (dusty galaxies!)
Koyama et al. (2011),
N (all Hα emitters)
N (red Hα emitters)
see P19
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JNB119
H (6563A) @ z=0.81±2000km/s
NB91
2
XCS J2215.9-1738 (z=1.46)RX J1716.6+6708 (z=0.81)MOIRCS + NB119 (Hα) Suprime-Cam + NB912 ([OII])
[OII] (3727A) of spec-z members
Two examples of NB survey at z<1.5
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Comparison of spatial distribution of star forming galaxies in cluster cores.
Star forming activity in the core is much higher in the higher redshift cluster!
Hα emitters at z=0.81 (RXJ1716) [OII] emitters at z=1.46 (XCS2215)
Koyama, et al. (2010) Hayashi, et al. (2010)
□ □
● phot-z members
Lx=2.7×1044 erg/s Lx=4.4×1044 erg/s
0.5 x R200 0.5 x R200
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z=0
z~0.8
z~1.5
: passive red galaxy: normal SF galaxy: dusty starburst
?
Inside-Out Propagation of Star Formation Activity and its Truncation?
Illustrated by Yusei Koyama
Do we eventually see the reversal of the SFR-density relation at z>1.5 as a result of galaxy formation bias?
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Narrow-band emitters (Hα, [OII]) surveys at 0.4<z<2.5 (primarily z>1.5)
“MAHALO-Subaru” MApping HAlpha and Lines of Oxygen with Subaru
c
lust
ers
field
s
Subaru Intensive Program for S10B-S11A10 nights allocation (6 nights completed under clear skies, 4 nights to come)
(However, one of the MOIRCS chips was broken and FoV was halved in S10B…)
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ClG J0218.3-0510 (z=1.62) in SXDF CL0332-2742 (z=1.61) in GOODS-S
Two recently found, confirmed clusters at z~1.6
Kurk et al. (2009)(Papovich et al. 2010; Tanaka et al. 2010)X-ray detection (4.5σ)
9 spec-z members, σ=540km/s42 spec-z members, σ=500km/s
[OII] fromz=1.61-1.62
Suprime-Cam
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ClG J0218.3-0510 (z=1.62) in SXDF
● [OII] emitters (star-forming, AGN)● Red sequence galaxies (~passive)
Tadaki et al. in prep.
see P21
a bright star
cluster core
●
●
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Star forming galaxies
Red sequence galaxies
ClG J0218.3-0510 (z=1.62) in SXDF
Fraction of star formingGalaxies is higher
in the cluster core !?
Tadaki et al. in prep.
Environmental variation
see P21
“preliminary result”
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[OII] emitters Ellipticals w/ GMASS spec-zSpirals w/ GMASS spec-zIrregulars w/ GMASS spec-z
MUSIC obj. w/ 1.43<phot-z<1.77
GO
OD
S-S
outh
CL0332-2742(z=1.61) in GOODS-S
Hayashi et al., in prep. see P20
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Our unique NB-filter system onSubaru MOIRCS (+Suprime-Cam)
specifically designed for this purpose!
Brank field, multi-line NB survey at z=2.2
Secure redshifts of emittersHβ/Hα (dust extinction)Lyα/Hα (escape fraction)
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Tadaki et al., in preperation
Hα emitters at z=2.2 traced by MOIRCS/NB209
Tadaki et al. (2011), in press
GOODS-N SXDS
5 MOIRCS pointings
8 MOIRCS pointings
NB209: ~2.5hrsKs: UDS
~2-3×10-17 erg/s/cm2 ⇔ ~10-15 M☉/yr (3σ)
“preliminary result”
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“Mahalo-plot” (in analogy to “Madau-plot”)
Emitters Only
Tadaki et al. (2011), in press
〈 SSFR 〉 vs. z and environment for emitters
Highly uncertain yet !
incompletenesscosmic variance
…
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Mapping gas and dust at the peak epoch of galaxy formation and evolution
“MAHALO-ALMA”
Molecular Associations with HAlpha and Lines of Oxygen probed with ALMA
at ~100GHz (Band-3), highest sensitivity & largest FoV (1’)
CO(21) for z=21, CO(32) for z=32High density gas:
Dust cotinuum: 850 μm – 1.1 mm, SFR~10M☉/yr at z>1.5
SFR~20M☉/yr (4hrs, 5σ) with CO(2-1)@z=1.5 and CO(3-2)@z=2.5
Internal kinematical structure: 0.01-0.1”(<1kpc) : gas in-/outflow, rotation
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Mapping star formation at the peak epoch of galaxy formation and evolution
“MAHALO-Subaru”
MApping HAlpha and Lines of Oxygen with Subaru
Taddy Kodama (Subaru Telescope),
Yusei Koyama (Univ of Tokyo),Masao Hayashi (NAOJ),Kenichi Tadaki (NAOJ/UTokyo),Ichi Tanaka (Subaru Telescope), et al.
Hα survey in CL0939 (z=0.41) (P19)
[OII] survey in CL0218 (z=1.62) (P21)
[OII] survey in CL0332 (z=1.61) (P20)
A Subaru Intensive Program for S10B-S11A, started in last Sep.
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Backup Slides
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NB921/S-Cam[OII] @z=1.46
NB973/S-Cam[OII] @z=1.62
NB1657/MOIRCSHα @z=1.52
1.46<z<1.65 is the golden redshift range for FMOS follow-up!
[OII] + Hβ + [OIII] + Hα + [NII]
Made by K. Tadaki
Dust extinction (Hα/Hβ), Metallicity (R23, N2), AGN ([OIII], [NII])
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ClG J0218.3-0510 (z=1.62) in SXDF
Tadaki et al., in prep.
[OII]
Hβ,[OIII]Hα
NB973: ~10 hrs (Ota et al.)zR: 5.5hrs
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Close-pair galaxies tend to have enhanced SF activities.
Environmental dependence Stellar-mass dependence
close-pair galaxies
SFR
SSFR
SFR
SSFR
Hayashi et al., in prep.
CL0332-2742 (z=1.61) in GOODS-S
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Hα emitters survey in a proto-cluster
4C23.56 at z=2.483 with MOIRCS/NB2288
Tanaka, I., et al. (2011), in press
Very strong star forming activitiesin the high-z proto-cluster!
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Number density of QSOsStar formation density
Bouwens et al. (2005)
Galaxy/AGN evolution peaks at z~2(Tuniv= 3.5 Gyrs)
Fan et al. (2006)
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Koyama et al. (2011)
□: Hα emitters
□: red Hα emitters
□: weak Hα emitters (SFR<0.75M☉/yr)
(B-I>2)
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NB973 emitters [OII] emitters at z=1.6
(Flux > 2.5 x 10-17 erg/s/cm2)>3 σ
Hayashi et al., in prep.
CL0332-2742 (z=1.61)in GOODS-S
NB973: 7hrszR: 3hrs
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Tadaki et al. (2011), in press
Hα emitters at z=2.2in GOODS-N
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Hα emitters at z=2.2in SXDF
16 arcmin x 6 arcmnin
Tadaki et al . In prep.
NB209: ~2.5hrsKs: UDS
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Eastern Clump
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A part of the FMOS-SSP-- to cover the highest-density regions --
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Advantages of narrow-band surveys (Hα, [OII])
CL0939 cluster (z=0.4)
(1) Good indicators of SFR, especially Hα (low reddening, well calibrated)(2) “Unbiased” sample (no pre-selection of targets is required).(3) Membership can be confirmed by the presence of emitters in NB +colours.(4) On top of the phot-z selected members (e.g. “passive” galaxies), we can
pick out “active” galaxies which tend to be missed by phot-z selection.
Blue galaxies tend to be missed by phot-z selection.
Low-z tail isdominatedby SF galaxies.
Koyama+ (2011)
□ Hα emitters