Wide-Field Science Capabilities at the AAO Stuart Ryder Australian Gemini Office Australian Astronomical Observatory.

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Presentation transcript:

Wide-Field Science Capabilities at the AAO Stuart Ryder Australian Gemini Office Australian Astronomical Observatory

OutlineOutline Radio – Optical synergiesRadio – Optical synergies ATAC “open skies” access toATAC “open skies” access to –(UKST) –AAT –Gemini –Magellan –Time exchange Complementing ASKAP SurveysComplementing ASKAP Surveys

UKSTUKST United Kingdom Schmidt TelescopeUnited Kingdom Schmidt Telescope 1.2m aperture, >6° FoV.1.2m aperture, >6° FoV – 2005: photographic surveys1973 – 2005: photographic surveys 2001 – 2012: 6dF multi-object spectroscopy (6dFGS, RAVE)2001 – 2012: 6dF multi-object spectroscopy (6dFGS, RAVE) “User pays” operation“User pays” operation TAIPAN: spectroscopic survey of ~500,000 galaxies to r <17.5 (cf. SDSS) via refurbished/replacement positioner & spectrograph.TAIPAN: spectroscopic survey of ~500,000 galaxies to r <17.5 (cf. SDSS) via refurbished/replacement positioner & spectrograph. Excellent complement to WALLABY and EMU.Excellent complement to WALLABY and EMU. Collaborators/benefactors welcome! Contact Andrew Hopkins welcome! Contact Andrew Hopkins

Anglo-Australian Telescope 3.9m aperture, commissioned m aperture, commissioned UCLES/UHRF R>40,000 optical spectrographs.UCLES/UHRF R>40,000 optical spectrographs. IRIS2 1–2.5  m imager, R~2400 long-slit & multi-object spectrograph, 7'.7 FoV.IRIS2 1–2.5  m imager, R~2400 long-slit & multi-object spectrograph, 7'.7 FoV. GNOSIS OH-suppression fibre-feed for IRIS2.GNOSIS OH-suppression fibre-feed for IRIS2.

AAOmegaAAOmega Dual-beam spectrograph, R=1300–8000, VPH gratings.Dual-beam spectrograph, R=1300–8000, VPH gratings. 2dF robotic fibre positioner places 392 2" fibres within a 2° FoV (2dFGRS, 2QZ, WiggleZ, GAMA).2dF robotic fibre positioner places 392 2" fibres within a 2° FoV (2dFGRS, 2QZ, WiggleZ, GAMA). SPIRAL Integral Field Unit lenslet array covers FoV 22.4"  11.2" at 0.7" per lenslet.SPIRAL Integral Field Unit lenslet array covers FoV 22.4"  11.2" at 0.7" per lenslet. KOALA (2012/13) will double the SPIRAL FoV.KOALA (2012/13) will double the SPIRAL FoV.

SAMISAMI Sydney-AAO Multi-object IFSSydney-AAO Multi-object IFS 13 “hexabundles” of 61 lightly-fused fibres covering 14" at 1.6" per fibre, manually plugged into pre-drilled plates covering 1° FoV.13 “hexabundles” of 61 lightly-fused fibres covering 14" at 1.6" per fibre, manually plugged into pre-drilled plates covering 1° FoV.

HERMESHERMES R=28,000 in 4 channels centered on 478, 577, 661, and 774 nm; fed by 2dF.R=28,000 in 4 channels centered on 478, 577, 661, and 774 nm; fed by 2dF. S/N = 100 in 1 hr for V=14.S/N = 100 in 1 hr for V=14. “Galactic Archaeology”: chemical tagging to reconstruct assembly history of Milky Way.“Galactic Archaeology”: chemical tagging to reconstruct assembly history of Milky Way. Optics fabricated by KiwiStar Optics.Optics fabricated by KiwiStar Optics. Commissioning early-2013.Commissioning early-2013.

GeminiGemini 2  8.1 m diameter infrared-optimised telescopes on Cerro Pachon (Chile) and Mauna Kea (Hawaii).2  8.1 m diameter infrared-optimised telescopes on Cerro Pachon (Chile) and Mauna Kea (Hawaii). Cassegrain foci only.Cassegrain foci only. ~90% queue-scheduled observing, ~25% ToO.~90% queue-scheduled observing, ~25% ToO. Australia has 6.2% share in partnership with USA, UK (till end 2012), Canada, Argentina, Brazil, and Chile.Australia has 6.2% share in partnership with USA, UK (till end 2012), Canada, Argentina, Brazil, and Chile.

Gemini North Reaches Dec  37°.Reaches Dec  37°. GMOS: 0.36–0.94  m 5'.5 FoV imager, long-slit, multi- object, and IFU (5"  7") spectrograph.GMOS: 0.36–0.94  m 5'.5 FoV imager, long-slit, multi- object, and IFU (5"  7") spectrograph.

Gemini North Reaches Dec  37°.Reaches Dec  37°. GMOS: 0.36–0.94  m 5'.5 FoV imager, long-slit, multi- object, and IFU (5"  7") spectrograph.GMOS: 0.36–0.94  m 5'.5 FoV imager, long-slit, multi- object, and IFU (5"  7") spectrograph. Michelle: 10–20  m imager/spectrograph.Michelle: 10–20  m imager/spectrograph. GNIRS: 1–5  m long-slit and 0.9–2.5  m cross- dispersed spectrograph.GNIRS: 1–5  m long-slit and 0.9–2.5  m cross- dispersed spectrograph. NIRI: 1–5  m imager with 22", 51", or 120" FoV.NIRI: 1–5  m imager with 22", 51", or 120" FoV. NIFS: R=5000 1–2.4  m integral field spectrograph with 3" FoV.NIFS: R=5000 1–2.4  m integral field spectrograph with 3" FoV.

Gemini North Reaches Dec  37°.Reaches Dec  37°. GMOS: 0.36–0.94  m 5'.5 FoV imager, long-slit, multi- object, and IFU (5"  7") spectrograph.GMOS: 0.36–0.94  m 5'.5 FoV imager, long-slit, multi- object, and IFU (5"  7") spectrograph. Michelle: 10–20  m imager/spectrograph.Michelle: 10–20  m imager/spectrograph. GNIRS: 1–5  m long-slit and 0.9–2.5  m cross- dispersed spectrograph.GNIRS: 1–5  m long-slit and 0.9–2.5  m cross- dispersed spectrograph. NIRI: 1–5  m imager with 22", 51", or 120" FoV.NIRI: 1–5  m imager with 22", 51", or 120" FoV. NIFS: R=5000 1–2.4  m integral field spectrograph with 3" FoV.NIFS: R=5000 1–2.4  m integral field spectrograph with 3" FoV. ALTAIR: Natural or Laser guide star adaptive optics system, delivering FWHM <0".1 at 2  m.ALTAIR: Natural or Laser guide star adaptive optics system, delivering FWHM <0".1 at 2  m.

Gemini South GMOS: 0.36–0.94  m 5'.5 FoV imager, long-slit, multi- object, and IFU (5"  7") spectrograph.GMOS: 0.36–0.94  m 5'.5 FoV imager, long-slit, multi- object, and IFU (5"  7") spectrograph. T-ReCS: 8–26  m imager and spectrograph.T-ReCS: 8–26  m imager and spectrograph. NICI: 1–5  m coronagraphic dual-channel adaptive optics imager, 18" FoV.NICI: 1–5  m coronagraphic dual-channel adaptive optics imager, 18" FoV. FLAMINGOS-2: 0.95–2.4  m imager, long-slit, and multi-object R=1200–3000 spectrograph, 6'.1 FoV.FLAMINGOS-2: 0.95–2.4  m imager, long-slit, and multi-object R=1200–3000 spectrograph, 6'.1 FoV. GSAOI: 0.9–2.4  m imager, 85" FoV.GSAOI: 0.9–2.4  m imager, 85" FoV.

Gemini South GMOS: 0.36–0.94  m 5'.5 FoV imager, long-slit, multi- object, and IFU (5"  7") spectrograph.GMOS: 0.36–0.94  m 5'.5 FoV imager, long-slit, multi- object, and IFU (5"  7") spectrograph. T-ReCS: 8–26  m imager and spectrograph.T-ReCS: 8–26  m imager and spectrograph. NICI: 1–5  m coronagraphic dual-channel adaptive optics imager, 18" FoV.NICI: 1–5  m coronagraphic dual-channel adaptive optics imager, 18" FoV. FLAMINGOS-2: 0.95–2.4  m imager, long-slit, and multi-object R=1200–3000 spectrograph, 6'.1 FoV.FLAMINGOS-2: 0.95–2.4  m imager, long-slit, and multi-object R=1200–3000 spectrograph, 6'.1 FoV. GSAOI: 0.9–2.4  m imager, 85" FoV.GSAOI: 0.9–2.4  m imager, 85" FoV. GeMS: Multi-Conjugate Adaptive Optics, 5  10 W laser guide star constellation.GeMS: Multi-Conjugate Adaptive Optics, 5  10 W laser guide star constellation.

GeMS in action

MagellanMagellan 2  6.5m telescopes at Las Campanas Observatory, Chile.2  6.5m telescopes at Las Campanas Observatory, Chile. Australia purchases 15 nights per year from Carnegie Institution for Science.Australia purchases 15 nights per year from Carnegie Institution for Science. MIKE: 0.34–0.95 mm R>20,000 spectrograph.MIKE: 0.34–0.95 mm R>20,000 spectrograph. IMACS: optical imager, long-slit, MOS, IFU, and tunable filter spectrograph, FoV up to 27'.IMACS: optical imager, long-slit, MOS, IFU, and tunable filter spectrograph, FoV up to 27'. FourStar: 0.9–2.4  m imager, 11' FoV.FourStar: 0.9–2.4  m imager, 11' FoV. Megacam: optical CCD mosaic 25' FoV.Megacam: optical CCD mosaic 25' FoV. MMIRS: 1–2.4 mm imager, long-slit, and multi-object R=1500/2800 spectrograph, 6'.9 FoV.MMIRS: 1–2.4 mm imager, long-slit, and multi-object R=1500/2800 spectrograph, 6'.9 FoV. MagE, FIRE, PFS.MagE, FIRE, PFS.

Time exchange Gemini time exchange with Keck (5n/semester, HIRES 0.3–1.0  m R>25,000 spectrograph only) and Subaru (up to 10n/semester) on any of:Gemini time exchange with Keck (5n/semester, HIRES 0.3–1.0  m R>25,000 spectrograph only) and Subaru (up to 10n/semester) on any of: –FMOS: 0.9–1.8  m spectrograph, 400 fibre positioner, 30' FoV. –Suprime-Cam: optical CCD mosaic, 34'  27 ' FoV. –MOIRCS: 0.9 – 2.5 mm imager, long-slit, and multi- object R=500–3000 spectrograph, 4'  7' FoV. –COMICS, HDS, IRCS

Time exchange AAO and CTIO have agreed to swap 20 nights/year each on the AAT and Blanco 4 m telescopes from 2012B.AAO and CTIO have agreed to swap 20 nights/year each on the AAT and Blanco 4 m telescopes from 2012B. –ISPI: 1–2.4  m imager, 10' FoV. –Hydra: 0.32–0.9  m R<50,  2" multi-object fibre spectrograph, 40' FoV. –DECam: 62 CCD (570 Mpixel) mosaic, FoV 2.2° (!)

Meeting the Need EMU WALLABY FLASH VAST GASKAPPOSSUM CRAFT DINGO VLBI COAST 2dF / Hydra / TAIPAN KOALA / SAMI HERMES GMOS / IMACS IRIS2 / F2 / 4Star / MMIRS / MOIRCS / ISPI GeMS Suprime-Cam / DECam / Megacam