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Dimitra Rigopoulou (Oxford Univ. & RAL-Space, STFC) Oxford, March 19 & 20 th 2013 Science with ALMA Band 11.

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Presentation on theme: "Dimitra Rigopoulou (Oxford Univ. & RAL-Space, STFC) Oxford, March 19 & 20 th 2013 Science with ALMA Band 11."— Presentation transcript:

1 Dimitra Rigopoulou (Oxford Univ. & RAL-Space, STFC) Oxford, March 19 & 20 th 2013 Science with ALMA Band 11

2 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, above 30% transmission Is it scientifically important?

3 Band 11: Sensitivities & Resolution Based on work carried out by S. Graves and J. Richer

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

5 H 2 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: H 2 formation on grains initiates chemistry of ISM Major contributor to the cooling of astrophysical media Band 11 Science Drivers Very high redshift Universe: probe pristine gas in protogalaxies through detection of the pure rotational H 2 lines 28 and 17 μm lines Devriendt & Slyz, using GALACTICA

6 Band 11 Science Drivers External Galaxies : Probe the properties of intermediate redshift 0.3 { "@context": "http://schema.org", "@type": "ImageObject", "contentUrl": "http://images.slideplayer.com/5/1517797/slides/slide_6.jpg", "name": "Band 11 Science Drivers External Galaxies : Probe the properties of intermediate redshift 0.3

7 Arp220 Rangwala et al. 2011 Band 11 Science Drivers ELAIS-S1 z=0.27 Bootes1 z=0.35 FLS01 z=0.46 A survey of [CII], [NII] and [OI] in intermediate redshift ULIRGs

8 Band 11 Science Drivers Interstellar Medium of the Milky Way Probe PDRs via spatially resolved studies of [NII] and high-J CO High/low Excitation Lines of Fundamental Molecules HCN, 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) Deduce HF/H2, calculate N(HF) Infer N(H2)

9 Band 11 Science Drivers High 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+, NH3 Para-NH3 (2-1) multiplet 1214.85 and 1215.24 GHz, chemistry of N H2D+ : ortho H2D+ @373 GHz BUT para H2D+ @ 1370 GHz dominant 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 for o=-D2H+ Search for o-D2H+ In 16293E Upper limit for o=-D2H+

10 Band 11 Science Drivers Continuum imaging

11 Band 11 Science Drivers Studies of the continuum at 200-300 microns @ z 3-5 (essesntial for constraining AGN)

12 Band 11 Science Drivers: Synergies & complementarities from E. Bergin B11 1400 11 From ALMA-NRAO

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16 Para-D2H+ Ortho-D2H+

17 Band 11 Science Drivers: Spectral Lines Unique Lines: fundamental rotational transitions of NH+: N2H+, NH3 Para-NH3 (2-1) multiplet 1214.85 and 1215.24 GHz, chemistry of N H2D+ : ortho H2D+ @373 GHz BUT para H2D+ @ 1370 GHz dominant form of H2D+, probe mid-plane of protostellar disks High Excitation Lines of Fundamental Molecules HCN, HNC, HCO+ Higher J transitions of CO : e.g. CO(10-9), CO(11-10), CO(12-11) etc

18 Band 11 Science Drivers: Spectral Lines Unique Lines: fundamental rotational transitions of NH+: N2H+, NH3 Para-NH3 (2-1) multiplet 1214.85 and 1215.24 GHz, chemistry of N H2D+ : ortho H2D+ @373 GHz BUT para H2D+ @ 1370 GHz dominant form of H2D+, probe mid-plane of protostellar disks High Excitation Lines of Fundamental Molecules HCN, HNC, HCO+ Higher J transitions of CO : e.g. CO(10-9), CO(11-10), CO(12-11) etc

19 Band 11 Science Drivers: Spectral Lines Unique Lines: fundamental rotational transitions of NH+: N2H+, NH3 Para-NH3 (2-1) multiplet 1214.85 and 1215.24 GHz, chemistry of N H2D+ : ortho H2D+ @373 GHz BUT para H2D+ @ 1370 GHz dominant form of H2D+, probe mid-plane of protostellar disks High Excitation Lines of Fundamental Molecules HCN, HNC, HCO+ Higher J transitions of CO : e.g. CO(10-9), CO(11-10), CO(12-11) etc

20 Band 11 Science Drivers: Spectral Lines Unique Lines: fundamental rotational transitions of NH+: N2H+, NH3 Para-NH3 (2-1) multiplet 1214.85 and 1215.24 GHz, chemistry of N H2D+ : ortho H2D+ @373 GHz BUT para H2D+ @ 1370 GHz dominant form of H2D+, probe mid-plane of protostellar disks D2H+ High Excitation Lines of Fundamental Molecules HCN, HNC, HCO+ Higher J transitions of CO : e.g. CO(10-9), CO(11-10), CO(12-11) etc


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