hsc with tao nirobservationssumire.ipmu.jp/wp-content/uploads/2012/09/hscws_20120927...2012/09/27...
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HSC with TAO NIR ObservationsTo Probe Galaxy Evolution
Kentaro Motohara (IoA, University of Tokyo),TAO Project Team, and
TAO Project Science Collaborators
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TAO : The University of Tokyo Atacama Observatory
A 6.5m IR/Optical telescope
At the highest site on the world (18500ft)⇒ High atmospheric transmittance
50% open use observation / 50% project observation
TAO Project
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One of the peaks at the Chajnantor plateau At northern edge of ALMA concession Altitude of 5640m (18500ft) 20deg‐S/30deg‐W
Co. Chajnantor
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A pathfinder telescope RC Cassegrain telescope Focal ratio F/12.0 FOV φ10 arcmin Two facility instruments
near‐infrared camera ANIR mid‐infrared camera MAX38
Installed at the summit in 2009
Existing Facility : miniTAO 1.0m
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Now Seen in Google Earth,
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in Wikipedia,http://en.wikipedia.org/wiki/List_of_highest_astronomical_observatories
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… and Certified as Guinness World Record
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Very low water vapor (PWV~0.5mm@25%tile) High transmittance in the infrared
TAO site
continuous windows in the NIR New windows at 30 um
ATRAN simulation
PWV=5mm
PWV=1mm
PWV=0.5mm
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Ver 2.0 :http://www.ioa.s.u‐tokyo.ac.jp/TAO/pjbook/pjbook.html
宇宙論 Ia型超新星サーベイ
銀河形成 Z=1‐3銀河の分光サーベイ 近傍銀河のPaα撮像・分光サーベイ
AGN ダストに埋もれたAGNサーベイ 変光モニタによるダストトーラスの構造
星 小中大質量星、分子雲でのダスト形成プロセス AGB星の中間赤外変光モニタ 晩期型星の分子光球
惑星系形成 Transition ダスト円盤サーベイ
TAO Science
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Instrumentation for TAO 6.5m
Two Instruments NIR MOS spectrograph/Imager (SWIMS) MIR Imager/Spectrograph (MIMIZUKU)
Development started from 2009, funded by economy stimulus budget
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NIR Camera : SWIMS
Simultaneous‐band Wide field Infrared MOS Spectrograph 9.6’ Φ with 4kx4k pixels Simultaneous 2‐band Imaging
blue channel : 0.9‐1.4um red channel : 1.5‐2.5um
0.9‐2.5m MOS spectroscopy with cooled multi‐slit masks max. 30 objects R~1000(0.6”slit)
IFU module under feasibility study
2.0m
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Filter WheelsFor BBFs & DIspersers
Filter WheelsFor NBFs
NBFs are placed in Converging light
Dichroic Mirror
Blue Channel( = 0.9‐1.4 m)
Red Channel(= 1.4‐2.5 m)
SWIMS Optics
2channels split by DM at 1.4um Spectroscopy from 0.9‐2.5um
=> accurate line ratios Dual‐band wide‐field imaging
Each focal plane is covered by 2 H2RGs (extendable to4x4)
9.6’
Future
8.1 x 4.0’
1600mm
230mm
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2m
SWIMS Manufacturing Underway
MOS Exchanger (Sentencia)
Main Dewar /Cooler(SHI)
HAWAII‐2RGs (Teledyne)
Grism (Optcraft / Richardson)
Aspherical ZnSe Lenses(Optcraft / II‐IV)
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Assembly Test at Mitaka New Building (2011/6)
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Large Imaging / Spectroscopic Survey using Large amount of Observing Time
Wide Field Deep NIR Survey
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0.9‐2.5m corresponds to rest optical wavelength of z=1‐3 galaxies
⇒ precise continuum / line ratio measurement RedshiftBalmer decrementSFR measurementMetallicity measurementAGN diagnosis
Rest Optical Sectroscopy
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Ideal for Redshift Survey at z=1‐3 Multi‐Line Observation for wider redshift range
Continuous NIR Window
Little transmittance at TAO site Little transmittance at ~2600m
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Advantage of TAO 6.5m/SWIMS Wide FoV High spatial resolution (0.12”/pix, ~0.5”seeing) Complete coverage of redshift Large amount of observing time⇒
NIR Follow‐up Imaging of HSC Deep Imaging Field NIR Follow‐up Spectroscopy of HSC/PFS Redshift Survey
Collaboration with HSC Survey
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Mass Assembly Activity Peaks at z=1‐3 More than 50% of present stellar mass was formed
Mass Assembly History in the Universe
Hopkins & Beacom 2006
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High Redshift Galaxies seem to be assembled not by intense merging⇒ Cold Accretion Model?: Cold gas (<10000K) accretes on a galaxy through filamentary structure
Cold Accretion
Dekel+09
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Steidel et al. 2010 NIR spectroscopy of 89
BX/BMs Redshift of a Galaxy ( ) :
Emission lines from HII regions in rest‐Optical
Redshift of Cold Gas ( ) :Absorption lines in rest‐UV
‐ So far, no detection
Cold Accretion Model
Steidel+10
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Covering fraction is ~1%‐⇒ Larger sample (>few x 1000) is necessary to confirm and study the detail of cold accretion
Difficulties in Observing Cold Accretion
Faucher‐Giguere+11
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HSC/PFS surveys will provide numbers of z~2 galaxies (~10000)
PFS provides UV absorption lines⇒
NIR follow‐up observation by TAO/SWIMS⇒
Targeting H 6563 @ 1.5<z<2.6 ~30/FoV 2hr / pointings ~300 pointings=> 600hr = 100 nights
Testing Cold Accretion Model
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Metallicity Evolution : Yes/No?
Erb+06 Hayashi, KM+09
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M‐Z relation becomes univeral when normalization by SFR?
Universal Funamental Plane?
Mannucci+10
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HSC + NIR imaging surveys Broad‐band SED => Mass, Age, …
SWIMS spectroscopy obtain all the major rest‐optical emission lines [OII] 3727 : 1.4<z<5.4 H 4861 : 0.9<z<3.9 [OIII] 5007 : z<3.8 H 6563 : z<2.6⇒ Dust extinction, Metallicity, SFR, …
HSC Imaging andSWIMS Spectroscopy
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Environmental Effect on Galaxy Evolution
Z=1.5 cluster : Hayashi+11A851 @ Z=0.41 : Koyama+11
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Kodama et al: Kakenhi‐Kiban‐B (2012‐2015) 8 MBF : Precise (z~0.02) photo‐z 4 (?) NBFs : Targeted dual emission‐line
MBF/NBF Imaging Survey of Distant Clusters
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Exisiting High‐z Cluster Survey Newly discovered high‐z cluster by HSC Survey (~1000)
⇒MBF Imaging Survey : ⇒ NBF Imaging Survey (~50 clusters)⇒ Spectroscopic follow‐up
Large sample with various environment
Cluster/Group Environment Effect at z>1
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Target : 2014~???? Will be opened as a PI instrument 2x faster survey speed than MOIRCS Same FoV (7.2’ x 3.6’) Simultaneous 2‐band Imaging (e.g., J and Ks)
SWIMS on Subaru
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TAO 6.5m telescope at 5640m Good weather/seeing condition Wide wavelength coverage Capable of large survey
SWIMS : NIR spectrograph under development 9.6’ FoV Planning to go to Subaru First (7.2’x3.6’ FoV on Subaru)
Synergy with HSC/PSF Provides NIR follow‐up capablility 2nd Gen TAO NIR WFC?
Summary