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1 ALMA 2004 high-z galaxies Submm galaxies ~ before/after ALMA ~

2 Outline Introduction Submm galaxies: before ALMA number count optical/ir/redshift /radio/x-ray/co spectroscopy Submm galaxies: after ALMA Scuba/ interferometer survey plan

3 Submm galaxies ~ Introduction ~

4 Submm (z=2.5)

5 negative K-correction z>1 350GHz(850µm) rest frame flux density (mjy) oberved frequency

6 345 GHz(850µm) flux density (mjy) ALMA 345GHz 8h integ. redshift Blain et al. (2002)

7 850 m image of HDF HST SCUBA 850µm Hughes et al. (1998)

8 Ivison et al. 2000, MNRAS, 315, 209 Submm source w/o optical counterpart

9 Submm galaxies ~ before ALMA ~

10 Submm galaxies deep survey z=0.5~4 (z mean ~2.5) z Chapman et al. 2003; µm flux = a few ~ 10mJy L(IR)>10 11 ~10 12 L sun, SFR>10~1000M sun

11 Deep sub-mm surveys blank fields HDF-N (Hughes et al. 1997, Borys et al ) Lockman, SSA 13 (Barger et al. 1998) EliasN2 (Scott et al. 2002) CUDSS (Eales et al. 2000, Webb et al. 2003) behind lensed cluster Abell 370, CL , CL , CL , Abell1835, Abell2390 (Smail et al. 1997; 2002) Abell 370, Abell 851, Abell 2390 (Cowie et al. 2002) Cl , MS , Abell 520, Zwicky 3146, MS , MS , Abell 2163, Abell 2219, Abell 2261 (Chapman et al. 2002) Abell 478 (Knudsen et al. 2001)

12 Number count / for S(850µm)>8mJy 10-5 /Mpc 3 (comoving volume density) (L>3-4L*)! source confusion ( ) luminosity evolution? number evolution? ALMA

13 Number count vs model Number count (sr -1 ) ( ) ( ) Nuber count SED Luminosity function Evolution factor 850µm flux density (Jy) Takeuchi et al. (2000)

14 ! merger (60% or larger) (effective radius) nearby ULIRGs( ) nuclear separation ULIRGs

15 850µm on Optical 1.4GHz on NIR NIR (K-band) Optical (HST) 850µm on Optical 1.4GHz on NIR NIR (K-band) Optical (HST) SCUBA (15 )+ = Smail et al. (1999), Frayer et al. (2000)

16 HDF850.1 : JCMT + SCUBA 850 m HDF field Hughes, et al. 1998, Nature, 394, 241 PdB high resolution mm imaging: flux =1.2mm high resolution imaging ( arcsec) Downes et al. 1999, A&A, 347, 809

17 Subaru high quality deep imaging Dunlop et al. 2004, MNRAS, 350, 769

HDF850.1 counterpart Extremely faint K 23.5 mag Very red I- K>5.2, H-K>1.4 +/- 0.

18 HDF850.1 counterpart Extremely faint K 23.5 mag Very red I- K>5.2, H-K>1.4 +/ Estimated redshift: z = 4.1 +/- 0.5 (radiosubmm color method) Dunlop et al. 2004, MNRAS, 350, 769

19 Optical Images merger (60% or larger) field galaxies, LBGs (effective radius) surface brightness LBGs local ULIRGs nuclear separation ULIRGs

20 HST Images of Submm Gals asymmetry LBGs Submm STIS image concentration Chapman et al., Conselice et al. (2003)

21 Size of Submm galaxies Effective radius number blue: ULIRGs red: submm gals Total Mag :submm gals, : LBGs : field gals Separation (kpc) Chapman et al., Conselice et al. (2003)

22 Optical-NIR Magnitude & Colors 3 (Smail et al. 2002) type0: Opt,NIR faint type1: Opt-NIR red (EROs) type2: Opt-NIR blue Opt bright (LIRGs) type 0:1:2 = 60%:20%:20%( ) I-K K Smail et al. (2002)

23 Optical-NIR Colors flux S850um>5mJy:? S850um<5mJy: Opt/NIR faint K mag S(850) Smail et al. (2002)

24 Optical mag & color vs (z) K mag I-K color radio-to-submm index ~ redshift ( :S 850 >8mJy, : S 850 <8mJy) no systematic evolution on Opt/NIR mag & color Ivision et al. (2002)

25 Optical spectra (class I/II ) type-2 AGN and/or starburst type-1 AGN Chapman et al. (2004?) 68 Champan et al.(2003)

26 Optical spectra star-forming galaxy SMM J (Ivison et al. 2000) Type-1 AGN SMM J (Ledlow et al. 2002)

27 Optical spectra with Keck/LRIS (Chapman et al. 2003)

28 X Chandra source 17 1 Almaini et al. 2003, MNRAS, 338, ksec exposure X-ray source 10 7 Alexander et al. 2003, AJ, 125, Msec exposure non-stellar power source dust AGN Mid infra ISO/Spitzer submm galaxies AGN X-ray submm AGN Quasar Seyfert Alexander et al. 2003, AJ, 125, 383 ULIRGs remember NGC 6240

29 SCUBA sources vs Chandra source ELAIS N2 field SUCBA image =2.5 mjy 850 m 17 sources > 3.5 Chandra image 17 x 17 arcmin 2 75 ks exposure erg/sec/cm2 ( kev) 91 sources 55 SCUBA source Almaini et al. 2003, MNRAS, 338, 303

30 X-ray counterpart of submm galaxies (?) R-band image Chandra 10 arcsec Chandra source (1.4 GHz source identification SCUBA Detection rate only 5% Major episode of SF must be distinct from the observable quasar period. (?) Almaini et al. 2003, MNRAS, 338, 303

31 Deep (2 Ms) Chandra image 8.4 x X-ray source Compton-thin 4 thick 1 Rest, unobscured Lx erg/s Alexander et al. 2003, AJ, 125, 383

32 CO in submm galaxies Submm source redshift optical counter part redshift High IR luminosity SFR ~1000 Mo/yr gas 2004 Genzel et al astro-ph/ M gas = M sun ( ) M gas /M dyn = massive system( M sun ) M gas /M dust ULIRGs ( ) single dish

33 Powerful CO emission from Sub-mm galaxies at z= M gas = M sun, M gas /M dyn ~0.5 w/pdbi (Neri et al.2003)

34 SED of submm galaxies flux density flux density ULIRGs rest frequency(ghz) Smail et al. (2002) observed frequency(ghz) Ivison et al. (2002) ULIRGs

35 Dust Temperature 450µm, 850µm, 1350µm graybody, S ν B ν (T dust ) {1-exp[-(ν/ν 0 ) β ]} T dust 40K, β=1.5 T dust >>40K (AGN?) fitting ( ) Benford et al.(1999)

36 Redshift class 0 Photometric redshift at radio/submm wavelengths: 850 m/1.4 GHz flux ratio Carilli & Yun 1999, ApJ, 513, L13 HDF850.1 radio z>3 FIR/submm color-mag diagram photometric redshift Takeuchi et al. 2002, PASP, 113, 586 Dust-z

37 Submm/radio flux ratio as a redshift indicator 350GHz/850GHz index (Arp220) 350GHz/850GHz index redshift redshift Carilli & Yun (2000) Ivison et al. (2002) SED photometric redshift estimater spectroscopic redshift redshift

38 Dust-z Dust RJ redshift rough Takeuchi et al. 2001, PASP, 113, 586

39 Submm galaxies ~ after ALMA ~

40 ALMA submm galaxies 3 2 ALMA

41 ALMA submm galaxies ~1.5 mjy =3mm, NMA, Jy ALMA 1 mjy SCUBA, Jy ALMA, mm 1 =3mm, NMA 0.01 ALMA submm JCMT, ASTE, 15 =850 m, JCMT interferometer SCUBA

42 limiting flux = 40 Jy 5 onsource /sr or /

43 ALMA submm galaxies confusion ultra-deep integration SCUBA survey ISO FIR survey survey SCUBA 3 survey counterpart mm/submm range line z 850 m 20 FHWP

44 Confusion limit: SCUBA/ASTE vs ALMA Angular resolution: SCUBA/ASTE: 15 arcsec ALMA: arcsec ALMA confusion SCUBA confusion limited Hogg, D. W. 2000, AJ, 121, 1207 Eales et al. 2000, AJ, 120, 2244 ALMA Takeuchi, et al. 2001, PASP, 113, 586

45 Submm deep survey after ALMA Confusion limit SCUBA clustring factor factor

46 Deep survey of submm galaxies ( cosmic variance) 850 m 4 mjy 5 3sec /field FWHP 900 m through time

47 Deep survey of submm galaxies ( cosmic variance) 850 m 350 Jy /field FWHP 900 m hrs/yr 3!? 1000 order source High-z dusty galaxies

48 Deep survey of submm galaxies 850 m 5 Jy /field L(IR)~10 10 Lo, Td=40K z= source population

49 Determination of redshift from radio observations CO/CI/CII spectroscopy Separation of transitions: df = /(1+z) GHz for CO z = 9 12 GHz transition ALMA instantaneous band width 4 GHz or 8 GHz sensitivity velocity mosaic CI( 3 P 1-3 P 0 ) CO(J=4-3) df = /(1+z) GHz CI( 3 P 2-3 P 1 ) CO( =7-6) : df = /(1+z) GHz

50 Line [CII], the strongest! ISO ULIRGs [CII] deficient Vastel et al. 2002, ApJ, 581, 315 [CI] survey AGN CO(4-3) ASTE Israel & Baas 2002, A&A, 383, 82 AGN high-z gas CO [CI]

51 redshift PKS B, V, R, I, K SEST15m mosaic 14 GHz 40000km/s =3mm HCN, HCN, HCO+, H13CO+, N2H+ J=2-1 J=3-2 CS J= z = High-z CO interval = 115/(1+z) GHz z=5 19 GHz 1 Wiklind & Combes 1996, Nature, 379, 139

52 CO emission from a GRB host galaxy? GRB at z = NMA NMA: 8 days! integration ALMA: 10 min integration 5 ~ 3 mjy, dv ~ 10 km/s S(CO) = Jy km/s M(gas) = 2 x 10 9 Mo!? dv(co) 200 km/s Kohno et al. 2004, submitted to PASJ

53 Summary Submm galaxies: before ALMA redshift ULIRGs SED, irregular AGN source 350 GHz/1.4 GHz index method z After ALMA SCUBA mosaic CO/CI spectroscopy redshift mosaic / mosaic

Microsoft Word - 简历-施勇.docx

Microsoft Word - 简历-施勇.docx 施勇 1980 年 11 月出生南京大学天文与空间科学学院 email: yong@nju.edu.cn 教育经历 : 1999.9-2003.7 2003.8-2008.8 北京大学, 地球物理系, 天文专业, 学士学位亚利桑那大学 ( 美国 ), 天文学, 博士学位工作经历 : 2008.8-2009.8: