Multiwavelength Study of Distant Galaxies Toru Yamada (Subaru Telescope, NAOJ)
Studying Galaxy Formation with ALMA 1. Studying Galaxy Forming Region with ALMA 2. Multi-wavelength Study of Galaxy Formation/Evolution 3. ALMA Deep Survey Studying Galaxy Formation with Dust-selected objects
Detecting Dust Thermal Continuum with ALMA 450um 850um Smail et al. 2001 40-80K sources with L=3x1012 Lsun (SFR= a few x100m/yr) 1-0.1 mjy ALMA @ 850um 0.1mJy (5σ, 3h) 1 (~50 FoV Nq.) ~50hours!
Distribution of Distant Red Galaxies (J-K>2.3) near HDF 7 arcmin Subru MOIRCS Kajisawa et al. 2006
1. Studying Galaxy Forming Region with ALMA
Giant Lyα Blob at z=3.1 (Steidel et al. 2000; Matsuda, TY, et al. 2004) Subaru 7h image of LAB1 25 = 190 kpc VLA / CO source Lyα image (after continuum subtraction) Cont. subtracted image z=3.1 LBG (before subtraction) B, V, NB. Lyα= green
Giant Lyα Blob at z=3.1 (Steidel et al. 2000; Matsuda, TY, et al. 2004) Subaru 7h image of LAB1 25 = 190 kpc VLA / CO source z=3.1 LBG SCUBA 850um ~ 17mJy (Chapman et al. 2003) Lyα image One of the brightest high-z Sub-mm Galaxy (before subtraction) (after continuum subtraction) Cont. subtracted image B, V, NB. Lyα= green
Giant Lyα Blob at z=3.1 (Steidel et al. 2000; Matsuda, TY, et al. 2004) Subaru 7h image of LAB1 25 = 190 kpc VLA / CO source z=3.1 LBG SCUBA 850um VLA 20cm 44.4 ujy ~ 17mJy (Chapman et al. 2003) Chapman et al. (2003) Lyα image One of the brightest high-z Sub-mm Galaxy (before subtraction) (after continuum subtraction) Cont. subtracted image B, V, NB. Lyα= green
Giant Lyα Blob at z=3.1 (Steidel et al. 2000; Matsuda, TY, et al. 2004) Subaru 7h image of LAB1 25 = 190 kpc VLA / CO source z=3.1 LBG OVRO Marginal Detection SCUBA 850um ~ 17mJy VLA 20cm 44.4 ujy CO (4-3) (Chapman et al. 2003) Chapman et al. (2003) (Chapman et al. (2003) Lyα image One of the brightest high-z Sub-mm Galaxy (before subtraction) (after continuum subtraction) Cont. subtracted image B, V, NB. Lyα= green
Giant Lyα Blob at z=3.1 (Steidel et al. 2000; Matsuda, TY, et al. 2004) 7h image of LAB1 SCUBA Detection one of Subaru the brightest high-z SMG 25 = 190 kpc Chapman et al. (2003) Simple Questions Is this an assembling giant galaxy? Where did intense SF sub-mm / CO occur? source Where is intense SF on-going? z=3.1 LBG SCUBA 17mJy source: how many / how extended? ALMA can answer(before subtraction) Lyα image (after continuum subtraction) Cont. subtracted image B, V, NB. Lyα= green
Matsuda et al. 2004 Mori & Umemura cf. Ohyama et al. 2003 See Poster by M. Mori Box size: or 190 kpc athydrodynaminc z = 3.1 Ultra25 high-resolution simulation
SCUBA11mJy! 25 or 190 kpc at z = 3.1 Matsuda et al. 2004 Simulation by Mori: Time Sequence
Geach et al. (2005) 5/25(observed) detected above 4.5mJy (>3.5σ) with SCUBA Statistical detection for the combined sample ~3mJy ~1000 Msun/yr SCUBA11mJy! 25 or 190 kpc at z = 3.1 Matsuda et al. 2004 Simulation by Mori: Time Sequence
Geach et al. (2005) 5/25(observed) detected above 4.5mJy (>3.5σ) with SCUBA Statistical detection for the combined sample ~3mJy ~1000 Msun/yr SCUBA11mJy! 25 or 190 kpc at z = 3.1 Matsuda et al. 2004 Simulation by Mori: Time Sequence
Lyα Blobs Lyα Emitters Isophotal detection aperture detection The largest Blob L!B1 and LAB2
Redshift Distribution of LAEs Obs: Subaru FOCAS 56 objects LAEs Redshift Matsuda, TY, et al. (2005) LAB1, LAB2
Distribution of ~2000 SSA22 z=3.1 Lyα emitters (Yamada et al., in prep) NB ~60 Mpc depth (comoving)
Distribution of ~2000 SSA22 z=3.1 Lyα emitters (Yamada et al., in prep) Galaxy Forming Region To study formation of massive and less-massive galaxies NB ~60 Mpc depth (comoving)
EW distribution of z=3.1 Lyα Emitters Needs Top Heavy IMF & Very Young Age (<107yr) (e.g., Charlot and Fall 1993) Nakamura, TY, et al.
EW distribution of z=3.1 Lyα Emitters Needs Top Heavy IMF & Very Young Age (<107yr) (e.g., Charlot and Fall 1993) Nakamura, TY, et al.
EW distribution of z=3.1 Lyα Emitters Top Heavy IMF Star Formation Strong Dust / Molecular Gas Emission Unexpected? (low metallicity, high dust T) SFR(Lyα ~ 10 Msun/yr ~ 0.01mJy (80K, 850um) Molecular Gas? Any Dust Emission? ALMA can put the strongest limit High Gas/Dust T? Needs rest-fir SED Needs Top Heavy IMF & Very Young Age (<107yr) (e.g., Charlot and Fall 1993) Nakamura, TY, et al.
2. Multi-wavelength Study of Galaxy Formation/Evolution and ALMA
Subaru/XMM Deep Survey Field (SXDS, 02h18m -05d) Subaru Deep Field ~27 1.2 deg
Z<1 SF history by Spitzer/GALEX LIRG ULIRG GALEX Le Floc h et al. 2005
SDF: Lyman Break Galaxies at z=3-6 SFR(UV, dust uncorrected)~50-100 Msun/yr Yoshida et al. 2006 (see also Iwata et al. 2005)
Subaru XMM Deep Survey (SXDS) Field 1.2 deg2 Optical (Subaru) X-ray (XMM-Newton) NIR (UKIDSS UDS), MIR-FIR (SWIRE), radio (VLA), sub-mm (SHADES), etc.
Subaru XMM Deep Survey (SXDS) Field 1.2 deg2 Optical (Subaru) X-ray (XMM-Newton) UKIDSS Deep Extragalactic Survey 50ks UKIDSS Ultra Deep Survey K<23 J < 25 Almaini, et al. XMM 100ks VLA Simpson et al. 2006 NIR (UKIDSS UDS), MIR-FIR (SWIRE), radio (VLA), sub-mm (SHADES), etc.
Subaru XMM Deep Survey (SXDS) Field 1.2 deg2 Optical (Subaru) X-ray (XMM-Newton) SHADES Coppin et al. 2006 NIR (UKIDSS UDS), MIR-FIR (SWIRE), radio (VLA), sub-mm (SHADES), etc.
B-Drop Lyman Break Galaxies ~6000 B-drop LBGs i < 24 24 < i < 25 25 < i < 26
B-Drop Lyman Break Galaxies B-drop LBGs (i<27) r La -s e g ing r te s u MDH~1012 cl le Mo ca mass Small scale clustering Ouchi et al. in prep
Luminous Large LBG @ z~4 20 False color
z~1 Old Passively-Evolving Galaxies 4400 OPEGs selected Ri z colors to z =25
Emergence of optically-faint X-ray Sources Akiyama et al. Typical BL QSO Large number of optically-faint X-ray sources appear in the deep X-ray surveys.
100 Mpc In comoving Z=4.9 Subaru Deep Field Shimasaku et al. 2003 Z=5.7 Subaru/XMM Deep Survey (SXDS) Field Ouchi et al.(ty) 2005, ApJ, 620, L1
What Are the Reddest Galaxies? S3.6um/S0.8um) S3.6/S0.8 IRAC 3.6um selected red sources with model tracks Kodama+Arimoto 97: E(Coma): zf=10, 4.6 GRASIL(Silva +98): E, Sa, Sb, Sc S3.6(uJy) S3.6 (ujy) (Y.Sato, SCDXT team)
S(3.6)/S(0.8) Magenta: 24 um sources S(3.6 um) [ ujy]
SDF: z=6.95 Lyα emitter (Iye et al. 2006)
ALMA Adds Dust/Gas Views to these panoramic study of the history of galaxies
3. a consideration for ALMA Deep Survey Studying Galaxy Formation with Dust-selected objects for JSAC (now EA-SAC) Extragalaxy WG
Characteristic of ALMA Deep Surveys High resolution: free from source confusion High sensitivity: ~ 0.1 mjy (5σ) in 3h @ 850μm Sensitive for thermal dust continuum - negative K-correction Simultaneous spectroscopy - Serendipitous line emitter survey (very) narrow field of view ~ 0.1 arcmin^2 @ 850μm Needs 5640 FoV with Nqst. to cover 100 arcmin2
Unbiased Survey of Distant Galaxies The deepest dust thermal view of the universe Search for the most distant dusty objects Feed Targets for ALMA Spectroscopy
Unbiased Survey of Distant Galaxies Formation and evolution of galaxies FIR Luminosity function (LF) Dust distribution in galaxies Dust / stellar mass Galaxy merging and dust emission BH/Galaxies co-evolution Cosmic star formation history Un-obscured cosmic star formation Exploration of new population of galaxies
Survey strategy
single band vs multi-bands? Choice 1: multi-band images with the same area, similar depth Effective for selection of distant objects; peak of dust SED e.g., band-9 drop galaxies Rough estimate of redshift not the deepest image (compared with choice 2) Choice 2: the deepest image at a selected band + targeted obs. at other bands The deepest image is obtained (band 6 or 7 for z=2-10) Can we select important/interesting sources from a single-band source catalogue? e.g.are there any sources undetected at band 6/7 but detectable at other band!?
Area & Depth Survey depth [mjy] 0.01 [ a case for 1.3 mm, 500 hrs integration ] Narrow & deep SFR ~ 10 Mo/yr L~10^10 Lo Medium area & depth 0.1 SFR ~ 100 Mo/yr L(FIR) ~ 10^11 Lo 1 Wide & shallow: SFR ~ 1000 Mo/yr L(FIR)~ 10^12 Lo 10 1 100 Limited to very luminous objects 10000 Survey area [arcmin2]
Case 1: Narrow & deep Survey depth [mjy] 0.01 Narrow & deep SFR ~ 10 Mo/yr Medium area & depth 0.1 SFR ~ 100 Mo/yr Wide & shallow: 1 SFR ~ 1000 Mo/yr 10 (a case for 1.3 mm, 500 hrs integration) 1 100 Limited to very luminous objects 10000 Survey area [arcmin^2]
Case 1: Narrow & deep 1 arcmin2, 500 hrs integration ~0.01 mjy @1.3mm, ~0.05mJy @850um SFR ~ 1-10 Msun/yr the longest integration Science goals The deepest dust thermal view of the universe (the most distant dusty objects?) dust properties of normal/less luminous objects Limitation -- Small volume to survey -- field-to-field variation -- poor statistics
Case 2: wide & shallow Survey depth [mjy] 0.01 SFR ~ 10 Mo/yr Narrow & deep: cosmic variance!!! Medium area & depth 0.1 SFR ~ 100 Mo/yr Wide & shallow: 1 SFR ~ 1000 Mo/yr 10 (a case for 1.3 mm, 500 hrs integration) 1 100 Limited to very luminous objects 10000 Survey area [arcmin^2]
Case 2: wide & shallow 10000 arcmin2, 500 hrs integ. ~ 1 mjy @ 1.3 mm or ~ 4 mjy@ 850um Science: a search for ultra-luminous objects (L > severalx1012 Lsun) Same as currently known SMGs from SCUBA ALMA: much less affected by confusion Positional accuracy Morphology Future single-dish (LMT,JCMT,,,,) surveys
Case 3: medium area & depth Survey depth [mjy] 0.01 SFR ~ 10 Mo/yr Narrow & deep Medium area & depth 0.1 SFR ~ 100 Mo/yr Wide & shallow: 1 SFR ~ 1000 Mo/yr 10 (a case for 1.3 mm, 500 hrs integration) 1 100 Limited to very luminous objects 10000 Survey area [arcmin^2]
A proposal: begin w/ medium survey ~100 arcmin2, 500 hrs integ. Limiting flux ~ 0.1 mjy@1.3mm SFR ~ 100 Mo/yr Luminous LBGs/DRGs/BzKs + new populations? ~ 300 sources expected. Then follow up of detected sources at short λ 300 sources @ 450μm, ~ 1 hrs/sources 300 hrs
Where to observe? 1. Currently Existing Fields Survey Area Best candidates Other possibility ~1 arcmin2 Hubble Ultra Deep Field HDF-S ~100 arcmin2 GOODS-South SEP ~1 deg2 SXDS, COSMOS SEP, SA22, GOODS-S 2. Future possibilities - HST WFC3 / JWST will develop other survey fields -Pre-study / Data accumulation before 2012 mm/sub-mm facilities + SST/Akari/HST/Subaru/VLT/Gemini -International collaboration across the regions
Studying Galaxy Formation with ALMA 1. Studying Galaxy Forming Region with ALMA 2. Multi-wavelength Study of Galaxy Formation/Evolution 3. ALMA Deep Survey Studying Galaxy Formation with Dust-selected objects