Dimitra Rigopoulou(Oxford Univ. & RAL-Space, STFC)

Oxford, March 19 & 20th 2013

Science with ALMA Band 11

ALMA Band 11 : Why a THz Band Originally ALMA to

reach up to 950 GHz But results from ISO,

APEX, Herschel & SOFIA highlight the tremendous scientific potential of observing in the THz bands

Is it feasible? Yes,

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Is it scientifically important?

Band 11: Sensitivities & Resolution

Based on work carried out byS. Graves and J. Richer

redshift

High J CO transitions, H2 rotational transitions and fine structure lines

H2 is the most abundant molecule in the Universe

• Its whereabouts:found in regions where shielding from UV photons (responsible for its dissociation) is sufficiently large Av >=0.5-1mag

Key role:• H2 formation on grains initiates chemistry of ISM• Major contributor to the cooling of astrophysical media

Band 11 Science DriversVery high redshift Universe: probe pristine gas in protogalaxies through detection of the pure rotational H2 lines 28 and 17 μm lines

Devriendt & Slyz, using GALACTICA

Band 11 Science Drivers

External Galaxies : Probe the properties of intermediate redshift 0.3<z<1 Universe

Magnelli et al. (2011))

[CII] @158 m (1.899 THz) in the redshift range 0.2-0.8

[NII] @ 205 m (1.950 THz) in the redshift range ~0.8

[OI] @ 63 m (4.758 THz) @ z~0.3

Arp220Rangwala et al. 2011

Band 11 Science Drivers

ELAIS-S1z=0.27

Bootes1z=0.35

FLS01z=0.46

A survey of [CII], [NII] and [OI] in intermediate redshift ULIRGs

Band 11 Science DriversInterstellar Medium of the Milky Way

Probe PDRs via spatially resolved studies of [NII] and high-J CO

High/low Excitation Lines of Fundamental MoleculesHCN, HNC, HCO+Higher J transitions of CO : e.g. CO(10-9), CO(11-10), CO(12-11) Hydrogen Fluorine @1232 GHz – tracer of H2, potential for detecting small H2 clouds

Sonnentrucker, Neufeld et al AA, 521

Deduce HF/H2, calculate N(HF)

Infer N(H2)

Band 11 Science DriversHigh Mass Star Formation : SFR in galaxies traced via massive stars. Also responsible for the buildup of chemical elements, origins of planets and Life

• high-J transitions of CO HCN, HNC and HCO+

Low mass star Formation: fundamental rotational transitions of NH+: N2H+, NH3Para-NH3 (2-1) multiplet 1214.85 and 1215.24 GHz, chemistry of N

H2D+ : ortho H2D+ @373 GHz BUT para H2D+ @ 1370 GHzdominant form of H2D+, probe mid-plane of protostellar disks

Para-D2H+

Ortho-D2H+

Vastel et al, from the CHESS program

Search for o-D2H+In 16293E

Upper limit foro=-D2H+

Band 11 Science DriversContinuum imaging

Band 11 Science Drivers

Studies of the continuum at 200-300 microns @ z 3-5(essesntial for constraining AGN)

Band 11 Science Drivers: Synergies & complementarities

from E. Bergin

B11

B11

140011

From ALMA-NRAO

Para-D2H+

Ortho-D2H+

Band 11 Science Drivers:Spectral LinesUnique Lines: fundamental rotational transitions of NH+: N2H+, NH3Para-NH3 (2-1) multiplet 1214.85 and 1215.24 GHz, chemistry of N

H2D+ : ortho H2D+ @373 GHz BUT para H2D+ @ 1370 GHzdominant form of H2D+, probe mid-plane of protostellar disks

High Excitation Lines of Fundamental MoleculesHCN, HNC, HCO+Higher J transitions of CO : e.g. CO(10-9), CO(11-10), CO(12-11) etc

Band 11 Science Drivers:Spectral LinesUnique Lines: fundamental rotational transitions of NH+: N2H+, NH3Para-NH3 (2-1) multiplet 1214.85 and 1215.24 GHz, chemistry of N

H2D+ : ortho H2D+ @373 GHz BUT para H2D+ @ 1370 GHzdominant form of H2D+, probe mid-plane of protostellar disks

High Excitation Lines of Fundamental MoleculesHCN, HNC, HCO+Higher J transitions of CO : e.g. CO(10-9), CO(11-10), CO(12-11) etc

Band 11 Science Drivers:Spectral LinesUnique Lines: fundamental rotational transitions of NH+: N2H+, NH3Para-NH3 (2-1) multiplet 1214.85 and 1215.24 GHz, chemistry of N

H2D+ : ortho H2D+ @373 GHz BUT para H2D+ @ 1370 GHzdominant form of H2D+, probe mid-plane of protostellar disks

High Excitation Lines of Fundamental MoleculesHCN, HNC, HCO+Higher J transitions of CO : e.g. CO(10-9), CO(11-10), CO(12-11) etc

Band 11 Science Drivers:Spectral LinesUnique Lines: fundamental rotational transitions of NH+: N2H+, NH3Para-NH3 (2-1) multiplet 1214.85 and 1215.24 GHz, chemistry of N

H2D+ : ortho H2D+ @373 GHz BUT para H2D+ @ 1370 GHzdominant form of H2D+, probe mid-plane of protostellar disks

D2H+High Excitation Lines of Fundamental MoleculesHCN, HNC, HCO+Higher J transitions of CO : e.g. CO(10-9), CO(11-10), CO(12-11) etc