ALMA! Fabian Walter MPIA
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- Ophelia Marsh
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1 ALMA! Fabian Walter MPIA
2 early science
![[Co- PIs: Smail, Walter, Weiss], 10 papers out.](/docs-images/76/73776176/images/3-1.jpg "ECDFS at 870 µm ALMA primary beam at 870 µm: ~20 (i.e. APEX beam size) need >10.")
3 What ALMA will not be: A Survey Machine e.g., LABOCA Survey of the Extended Chandra Deep Field South (LESS) ESO Large Program [Co- PIs: Smail, Walter, Weiss], 10 papers out. ECDFS at 870 µm ALMA primary beam at 870 µm: ~20 (i.e. APEX beam size) need > poinings for ECDFS...close to poinings for COSMOS Weiss et al. 2009
4 What ALMA will enable: Detailed studies of Dust and Mol. Gas band 10 band 9 band 8 band 7 band 6 band 5 band 4 band 3 early ALMA science - detecion - resolved imaging - excitaion - high- density tracer - atomic lines
5 What ALMA will enable: Detailed studies of Dust and Mol. Gas band 10 band 9 band 8 band 7 band 6 band 5 band 4 band 3 early ALMA science - detecion - resolved imaging - excitaion - high- density tracer - atomic lines
6 What ALMA will enable: Detailed studies of Dust and Mol. Gas band 10 band 9 band 8 band 7 band 6 band 5 band 4 band 3 early ALMA science - detecion - resolved imaging - excitaion - high- density tracer - atomic lines
7 What ALMA will enable: Detailed studies of Dust and Mol. Gas band 10 band 9 band 8 band 7 band 6 band 5 band 4 band 3 early ALMA capabiliies - detecion - resolved imaging - excitaion - high- density tracer - atomic lines
8 What ALMA will enable: Detailed studies of Dust and Mol. Gas band 10 band 9 band 8 band 7 band 6 band 5 band 4 band 3 early ALMA science - detecion - resolved imaging - excitaion - high- density tracer - atomic lines
9 What ALMA will enable: Detailed studies of Dust and Mol. Gas band 10 band 9 band 8 band 7 band 6 band 5 band 4 band 3 early ALMA science - detecion - resolved imaging - excitaion - high- density tracer - atomic lines Flux at 230/345 GHz ~ constant as f(z)
10 What ALMA will enable: Detailed studies of Dust and Mol. Gas band 10 band 9 band 8 band 7 band 6 band 5 band 4 band 3 early ALMA science - detecion - resolved imaging - excitaion - high- density tracer - atomic lines Flux at 230/345 GHz ~ constant as f(z)
11 What ALMA will enable: Detailed studies of Dust and Mol. Gas band 10 band 9 band 8 band 7 band 6 band 5 band 4 band 3 early ALMA science - detecion - resolved imaging - excitaion - high- density tracer - atomic lines Flux at 230/345 GHz ~ constant as f(z)
12 What ALMA will enable: Detailed studies of Dust and Mol. Gas band 10 band 9 band 8 band 7 band 6 band 5 band 4 band 3 early ALMA science - detecion - resolved imaging - excitaion - high- density tracer - atomic lines Flux at 230/345 GHz ~ constant as f(z)
13 What ALMA will enable: Detailed studies of Dust and Mol. Gas band 10 band 9 band 8 band 7 band 6 band 5 band 4 band 3 early ALMA science - detecion - resolved imaging - excitaion - high- density tracer - atomic lines Flux at 230/345 GHz ~ constant as f(z)
14 OpIcal Deep Field z<1.5 z>1.5
15 (HypotheIcal) Submillimeter Deep Field z<1.5 z>1.5
16 Massive Galaxies at z= Daddi et al Tacconi et al. 2010
17 Massive Galaxies at z= ALMA simulaions input: BzK galaxy at z~1.5 with CO(2-1) peak: 1mJy [typical values in Daddi, Tacconi for BzK galaxy with SFR~100M sun yr - 1 ] CO(2-1) CO(2-1)
18 Massive Galaxies at z= ALMA simulaions input: BzK galaxy at z~1.5 with CO(2-1) peak: 1mJy [typical values in Daddi, Tacconi for BzK galaxy with SFR~100M sun yr - 1 ] CO(2-1) CO(2-1)
19 Massive Galaxies at z= ALMA simulaions input: BzK galaxy at z~1.5 with CO(2-1) peak: 1mJy [typical values in Daddi, Tacconi for BzK galaxy with SFR~100M sun yr - 1 ] CO(2-1) CO(2-1)
20 Massive Galaxies at z= ALMA simulaions input: BzK galaxy at z~1.5 with CO(2-1) peak: 1mJy [typical values in Daddi, Tacconi for BzK galaxy with SFR~100M sun yr - 1, M H2 ~ few M sun ] HC3N(25-24) CO(2-1) CS(5-4) SiO(5-4) HC3N(24-23) 13 CO(2-1) CO(2-1) need high S/N for imaging
21 Less massive Galaxies at z= ALMA simulaion so far, only the brightest BzKs have been looked at: input: same as before, but SFR~20 M sun yr - 1, M H2 =few x 10 9 M sun Daddi et al CO(2-1)
22 Massive Galaxies at z= Resolving the Gas science drivers: resolved dynamical analysis resolved star formaion law - - evidence for interacion Daddi et al Tacconi et al Sources are extended on ~1 scales. 1kpc resoluion (0.15 ) ~50 independent beams previous example: S/N=25 in 50 km/s channel for the full source.
23 Massive Galaxies at any redshij- - - Resolving the FIR Emission flux density inverse- K correcion 230/345 GHz fluxes ~constant z>1 map star formaion - - also a way to separate AGN contribuion redshij early science (µjy) 1h integraion (230 GHz; 345 GHz) h integraion (230 GHz; 345 GHz) SFR = 100 M sun yr - 1 : S 230GHz = 100 µjy; S 345GHz = 250 µjy full array (µjy) 1km array (early science): 0.2 resoluion (~1kpc) 10km array (full ALMA): 0.02 resoluion (~100pc)
24 QSOs/SMGs at z>2: Major Molecular Gas Reservoirs Wang et al Frayer et al. 1998
25 QSOs at z=6 w/ ALMA state of the art: Wang et al CO(6-5)
26 QSOs at z=6 w/ ALMA state of the art: Wang et al CO(6-5)
27 QSOs at z=6 w/ ALMA state of the art: Wang et al CO(6-5)
28 QSOs at z=6 w/ ALMA state of the art: Wang et al CS(14-13) HCN(8-7) HCO + (8-7) HNC(8-7) CS(15-14) CO(6-5)
29 CO Line redshij coverage for ALMA and EVLA
30 ExcitaIon is important thermalized QSOs SMGs MW BzK excitaion (Daddi s talk)
31 CO Line redshij coverage for ALMA and EVLA
32 CO Line redshij coverage for ALMA and EVLA gas not excited
33 CO Line redshij coverage for ALMA and EVLA atomic lines: [CII], [NII] [OIII], [OI] gas not excited
![[CII] to the rescue at z>6 1!](/docs-images/76/73776176/images/34-0.jpg "Maiolino ea 2005, Walter ea.")
![2009 [CII] size ~ 1.](/docs-images/76/73776176/images/34-2.jpg "5 kpc => SFR/area ~ 1000 M o")
34 [CII] to the rescue at z>6 1! Maiolino ea 2005, Walter ea [CII] size ~ 1.5 kpc => SFR/area ~ 1000 M o yr - 1 kpc - 2 Maximal starburst: (Thompson, Quataert, Murray 2005) Self- gravitaing gas disk, VerIcal support: radiaion pressure Eddington limited SFR/area ~ 1000 M o yr - 1 kpc - 2
35 Take- home messages Early Science with 16 antennas staring next year ALMA will not be a wide- field survey machine Full ALMA: <100pc resoluion at any redshij, both in FIR and line Gas masses down to ~10 9 M sun Choose your transiion/lines wisely At highest (z>6) redshijs: need to resort to atomic fine structure lines
36 THE END
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