Cecilia Fariña - ING Support Astronomer

Introduction: WHT William Herschel Telescope 2

Introduction: WHT WHT located in La Palma, Canary Islands, Spain William Herschel Telescope l 2 3

Introduction: WHT 2400m above sea level. William Herschel Telescope Located at La Palma, Canary Islands 2400m altitude above sea level 706 km² (~15x45 km) ~86000 inhabitants 4

Introduction: WHT 5

Introduction: WHT 6

Introduction: WHT 7

Introduction: WHT 8

Introduction: WHT 9

Introduction: WHT Instruments: - ACAM - ISIS - LIRIS - AF2 - PFIP - NAOMI / INGRID: ZJHKK_s and 10 narrow-band - NAOMI/OASIS: Integral-field spectrograph, with/without adaptive-optics. - OSCA + visitor instruments: GhaFaS, INTEGRAL, PN.S, Ultracam 10

Introduction: WEAVE New wide-field multi-fibre spectroscopy facility (survey) for the prime focus of WHT (4.2-m). Dual-beam spectrograph (blue and red arm) Spectral resolution: R ~ 5000 (mid) and R ~20000 (high) 2 deg FoV (diameter) 1000 fibres Large IFU Set of smaller IFUs Project started in 2010. Preliminary design review 2013. Expected to be on-sky (for commissioning) by 2017. 11

Scientific Motivation Science drivers (3 main lines which lead the instrument specifications): I. Galactic science (Gaia mission): Dynamics of the MW. Structure and history of the disks and halo. II. Galaxy evolution science (Apertif and LOFAR): Connect galaxy evolution to internal and external effects: Couple internal motions and stellar content to neutral gas and large scale environment. III.Cosmological Science (linked to LOFAR and EUCLID): What is the dark energy how does it evolve. Other community science projects. 12

Scientific Motivation A number of other science cases have been proposed for WEAVE Galactic Plane spectroscopic surveys, to trace rare and short-lived phases of stellar evolution Chemical abundances of pulsating variable stars, to calibrate the cosmic distance scale Extragalactic star clusters, to constrain the evolution of star formation and chemical evolution of nearby galaxies Stellar populations and kinematics of galaxies at intermediate redshifts, to understand the evolution of stellar mass in galaxies Integral-field observations of strong lenses to understand the distribution of dark matter and the stellar initial mass function in massive early-type galaxies These surveys will be used to fill in target lists in the main surveys to maximally utilize fibres in any given field. 13

Scientific Motivation: I) Galactic Science WEAVE + Gaia Gaia (ESA) launched Dec. 2013. Compile a 3D space catalogue of 109 stars Radial velocities for the brightest 15% of the 109 stars it will survey Chemical compositions for the brightest 0.1% the 109 stars it will survey 14

Scientific Motivation: I) Galactic Science WEAVE + Gaia Gaia (ESA) launhed Dec. 2013. Compile a 3D space catalogue of 109 stars Radial velocities for the brightest 15% of the 109 stars it will survey Chemical compositions for the brightest 0.1% the 109 stars it will survey WEAVE will complement Gaia with radial velocities at V>17 and abundances at V>12. 15

Scientific Motivation: I) Galactic Science WEAVE has access to the MW outer disk and halo WEAVE outer DISK outer DISK HALO HALO BULGE inner DISK 16

Scientific Motivation: I) Galactic Science WEAVE at R~20000 Chemical tagging of stars δvr < 1kms 1 Abundances to ~ 0.1 dex accuracy 50,000 halo giants 2500 deg2 17

Scientific Motivation: I) Galactic Science WEAVE at R~5000 370 1000nm δvr < 5kms 1 Abundances ~0.2 dex accuracy >106 stars 10000 deg2 18

Scientific Motivation: II) Galaxy Evolution WEAVE + Apertif Apertif is a set of phased array detectors at the Westerbork Synthesis Radio Telescope (x25 FoV). Surveys to study the evolution of the HI content of galaxies, pulsars, transients, continuum surveys, etc. 19

Scientific Motivation: II) Galaxy Evolution WEAVE + Apertif Apertif Medium-Deep Survey Apertif Shallow all-sky Survey HI data for tens of thousands (104) at of gas-rich galaxies in the local Universe (0.1<z<0.4). WEAVE will provide their resolved Optical spectroscopic Information. 20

Scientific Motivation: II) Galaxy Evolution + III) Cosmology WEAVE + LOFAR LOFAR: Low Frequency Array. Largest radio telescope at low Frequencies:10-90 MHz (LBA) + 110-250 MHz (HBA). Interferometric array antenna stations distributed throughout the Netherlands and in several countries in Europe. Research the origin of the first galaxies, black holes and gas clouds at the 'birth' of the Universe. 21

Scientific Motivation: II) Galaxy Evolution + III) Cosmology WEAVE + LOFAR LOFAR s surveys will probe the low-frequency radio Universe: Tens of millions of star-forming and active galaxies. WEAVE WEAVE will perform spectroscopic follow-up of the LOFAR surveys: redshifts (distances) and optical properties. 22

Science Requirements The science cases provided a set of requirements for WEAVE: 23

Science Requirements The science cases provided a set of requirements for WEAVE: FoV: ~ 2 deg diameter 24

Science Requirements The science cases provided a set of requirements for WEAVE: FoV: ~ 2 deg diameter Multiplex: ~1000 fibres, final design: 960 fibres on plate A, 940 on plate B 25

Science Requirements The science cases provided a set of requirements for WEAVE: FoV: ~ 2 deg diameter Multiplex: ~1000 fibres, final design: 960 fibres on plate A, 940 on plate B. MOS aperture: 1.2-1.5, final design: 1.3 Spectral Resolution: - Low-res: R = 5000, blue arm 366-606 nm, red arm 579-959 nm - High-res: R = 20000, blue arm 404-465 nm or 473-545 nm, red arm 595-685 nm 27

WEAVE: Instrument Concept & Design A new mount to support the prime focus, replacing the existing flipring. A new prime focus corrector with ADC (Atmospheric Dispersion Corrector), instrument rotator and cable wrap. A focal plane exchanger (tumbler), with the two field plates with 1000 fibres each. 20 small IFU will replace some of the MOS fibres one of the plates. A large IFU. An image camera ahead of the field plate at the observing position to determine the telescope focus and overall calibrations of the instrument coordinate system. 31

WEAVE: Instrument Concept & Design 32

WEAVE: Instrument Concept & Design 33

WEAVE: Instrument Concept & Design 34

WEAVE: Instrument Concept & Design AF2-WYFFOS mounted at WHT prime 35

WEAVE: Instrument Concept & Design WEAVE Assembley WEAVE assembly to mount at prime focus (which includes the optics and mechanisms for atmospheric dispersion and field correction, a field rotator & cable wrap, fibre positioner). Total top end mass ~4500 kg 36

WEAVE: Instrument Concept & Design Prime focus corrector 2 deg PFC 2200 kg Diameter 1700 mm Length 2100 mm 37

WEAVE: Instrument Concept & Design 38

WEAVE: Instrument Concept & Design 39

WEAVE: Fibre Positioner 2dF-like (AAO) tumbler with 2 field plates 2 robots working in parallel low-risk, lowcost high flexibility 2dF (AAO) 40

WEAVE: Fibre Positioner 41

WEAVE: Fibre Positioner 97% of fibres allocated in test simulation (1.8x oversampled targets). ~8500 fibre crossings! c ~1800 moves within ~55 minutes with two robots. 42

WEAVE: Fibre Positioner Bull-ring triple-parking concept 43

WEAVE: Fibre Positioner Bull-ring triple-parking concept 44

WEAVE: The Spectrograph Dual-Beam Spectrograph Design Low-resolution (R~5000) 45

WEAVE: The Spectrograph Dual-Beam Spectrograph Design High-resolution (R~20000) By grating change and rotation). 46

WEAVE: The Spectrograph 47

WEAVE: The Spectrograph - mifus Number of mifus: 20 Structure of each mifu: 37 close-packed 1.3-arcsec fibres (same type as used for MOS-A, MOS-B) Field of view: 7x7 arcsec2 Minimum separation of mifus on the sky: 60 arcsec Location of mifus: MOS-B plate Area over which deployable: central 1.7-deg diameter. 48

WEAVE: The Spectrograph - LIFU Large single-field IFU located at 90 tumbler position Offset bundles for sky subtraction. 49

WEAVE: Throughput Overall throughput of WHT+WEAVE: Low-res mode, 450-850 nm: ~ 0.25 (taking into account all components along light path from bottom of atmosphere to detector. 50

WEAVE: Throughput Overall throughput of WHT+WEAVE : High-res mode, blue. 51

WEAVE: Throughput Overall throughput of WHT+WEAVE : High-res mode, red. 52

WEAVE: The Consortium 53

To summarize: WEAVE key parameters Telescope, diameter WHT, 4.2m Field of view 2deg (diameter) Number of fibres 960 fibres on plate A, 940 on plate B Fibre on-sky aperture 1.3 Number of small IFUs, size 20, 7 x7 (1.3 spaxels) LIFU size 78 x90 (2.6 spaxels) Low-resolution mode R ~ 5000 Low-resolution mode wavelength coverage blue arm 366-606 nm red arm 579-959 nm High-resolution mode resolution R ~ 20000 High-resolution mode wavelength coverage blue arm 404-465 nm or 473-545 nm red arm 595-685 nm 54

Conference La Palma 2015 http://www.ing.iac.es/conferences/mos/ 55

The End Thanks!!!! http://www.ing.iac.es/weave/index.html http://www.ing.iac.es/astronomy/telescopes/wht/weavepars.html 56