Optical System for Imaging and low Resolution Integrated ... · Optical System for Imaging and low...

Jordi Cepa 3D-NTT Scientific Committee, April 2nd 2008 1

OSIRISOSIRISOOptical ptical SSystem for ystem for IImaging and low maging and low RResolution esolution IIntegrated ntegrated SSpectroscopypectroscopy

Large Format ProjectsLarge Format Projects


OutlineOutline

• Telescope status

• OSIRIS status including upgrades

• Large format projects


TheThe TelescopeTelescope

GTCGTC


Current GTC status in a Current GTC status in a nutshellnutshell

• All civil work (building, dome, air conditioning, etc) finished

• Telescope mechanics, hydraulics & optics (M1,M2,M3) ready

• 24 segments mounted (out of 36 + 4 as aluminizing backup)

• The remaining 12 already aluminized and ready to install

• Pointing and tracking tests successfully started 20 days ago

− Pointing: 2.5 arcsec r.m.s. over +5º < δ < +85º

− Tracking: working although not yet characterized

• Other works in progress:

− TCS

− DPK (Data Processing Kit)

− OPMS (Observation Proposal Management System≡phase II)


Current GTC status in a Current GTC status in a nutshell: next tasksnutshell: next tasks

• Finishing pointing and tracking tests• Alignment of the 24 segments already installed

• Installing and alignment of the remaining 12 segments

• A&G tests (acquiring, guiding, lamps…) by July

• OSIRIS Commissioning by October

• CanaryCam Commissioning by December

• Day One: March 2009


GTCGTC


GTCGTC


GTCGTC


TheThe InstrumentInstrument

OSIRISOSIRIS


OSIRIS statusOSIRIS status


OSIRIS StatusOSIRIS Status

• All subsystems ready, tested and fulfilling specs

• Mechanical assembly, optical alignment & characterization finished

• Mechanisms functional tests on rotator with final harness & electronics finished

• CCD performance tests finished (almost nominal RON: 3.6e- @ 50 kHz)

• Most subsystems already operational under GTC control system

• Characterisation of filters and grisms at the instrument finished

• TF status:

− Red TF characterized and its OS ready

− Blue TF characterization in progress

− Blue OS to be purchased

• Flexures characterization & flexure correction system about to start

• OSIRIS Factory acceptance: May-June 2008

• OSIRIS on site: October 2008 for commissioning


OSIRIS ModesOSIRIS Modes

• Broad band Imaging• Narrow band imaging using TF

− Standard

− Shuffle modes (ON-OFF, ON-OFF1-ON-OFF2, ON1-ON2,…)

• Long slit spectroscopy• Multiple Object Spectroscopy

− Standard

− Nod & Shuffle, µShuffle, λ-sorting

• Fast photometry− Shuffle (same band or different bands using TF)

− Defining windows in the CCDs

• Fast spectroscopy− Shuffle

− Frame-transfer


OSIRIS UpgradesOSIRIS Upgrades

• Higher resolution etalon (M. Rosado, IA-UNAM)

− R = 10000

− Coatings from 650 through 900 nm

− ET100, controller CS100 (as TFs)

− Order sorters pending

− Lower R (5000) under study

• Integral Field Units− Work will start by October (once OSIRIS is finished)

− Available by end 2009

− 100 µm φ OH doped fibres

− Microlenses 0.6 arcsec φ

− Two IFUs:

⋅ Compact array: 12 × 12 arcsec2

⋅ Sparse array: 40 × 40 arcsec2


OSIRIS basic OSIRIS basic characteristicscharacteristics

0.125 arcsec/pixel (imaging and spectroscopy)Plate scale

2 MAT 4k ×××× 2k (8 arcsec gap) from same Si waferDetector

∼∼∼∼40 targets per mask (classical slits of 15” length) orSeveral hundred (Nod&Shuffle, µµµµShuffle or λλλλ-sorting)

MOS (masks)

300, 500, 1.000, 2.000, 2.500 and 5.000λλλλ/∆λ∆λ∆λ∆λ for 0.6” slit widthR=300 & 500 limited by order, higher R by detector

Spectral resolutions

Central λλλλ tunable from 365 through 1000 nmFWHM tunable from ∼∼∼∼6 through ∼∼∼∼30 Å, dep. on λλλλLower FWHM limited by OS, and higher by etalon gapTuning time ~1-100 msTuning accuracy in λλλλ and FWHM ~0.1 Å

Narrow band (2 TF: blue & red)

ugriz filters & TF order sorters (OS)Broad band

8.53 ×××× 8.67 arcminutesFOV (imaging)


OSIRIS OSIRIS basicbasiccharacteristicscharacteristics

• Very high efficiency, red optimized & UV sensitive• Distortion: < 2%

• Image quality: Measured resolution 0.16”

• Shutter: accuracy better than 1ms and minimum exposure time of 0.1s

• Number of elements simultaneously loaded:− 13 focal plane masks in the mask loader

− 24 filters 19 cm φ in three filter wheels in collimated beam

− 2 TF and 6 prisms/grisms/VPHs in pupil wheel

• Masks available:− Long slit widths: 0.4, 0.6, 0.8, 1.0, 1.2, 1.5, 1.8, 2.0, 2.5, 3.0, 3.5, 5.0

− User customized masks for MOS (goal: drilling in 24h)

− 1/3 FOV for shuffle tunable imaging

− Half-field mask for frame transfer

− Decentered slit for fast photometry

• High performance in configuration changes (< than detector readout)


The ScienceThe Science

Large ProjectsLarge Projects


Large format projectsLarge format projects

• The ones that I know

• That are relatively developed

• Not at the same level of detail (some of them still developing)

• Requiring at least 100 GTC hours (some require 300 or more)

• Using mainly OSIRIS (although NIR follow-ups in some cases)

• Using the TF

• Most of them based on TF tomography


z2

z1

λλλλ1

λλλλ2

TF TomographyTF Tomography

OSIRIS TF FOV

Angle: OSIRIS FOV

Heigh: ∆λ∆λ∆λ∆λ scanned = λλλλ2-λλλλ1

Limiting magnitude: exposure time

LimitedLimited flux flux surveysurvey ofof a a perfectlyperfectly defineddefined

volumevolume ofof Universe Universe

(same emission line)



OTELOOTELOOOSIRIS SIRIS TTunable unable EEmission mission LLine ine OObject surveybject survey


OTELO snapshotOTELO snapshot

• The project of the instrument builders• Appointed as “Strategic Project” by the IAC• Ultra-deep emission line survey at red λλλλ windows using TF• Searching for emission line galaxies from z=0.24 to z=7.0• Deblending Hαααα from [NII] for nearby galaxies• Some scientific objectives:

− Lymanα Emitters (LAEs) LF evolution

− AGN fraction and LF evolution

− QSO LF evolution, especially at high reshift (z>5)

− SFR vs. z

− Evolution of emission line galaxies

− Metallicity evolution

• Some expected follow-ups: Hαααα in NIR for Oxygen emitters


OTELO TeamOTELO Team

J. Cepa (PI, IAC-ULL) I. González-Serrano (IFCA-UNICAN)

J. Acosta-Pulido (IAC) J. González (IA-UNAM)

E. Alfaro (IAA) M.A. Lara (IAC)

A. Bongiovanni (IAC) A.M. Pérez-García (IAC)

H. Castañeda (IAC) M. Povic (IAC)

C. Esteban (IAC) J.M. Rodríguez-Espinosa (IAC)

M. Fernández (IAC) M. Sánchez-Portal (INSA-ESAC)

J. Gallego (UCM)


OTELO wavelength OTELO wavelength windowswindows

Stockton 1999


OTELO Survey OTELO Survey CharacteristicsCharacteristics

YesNoDeblend Hαααα −−−− [NII]

Different fieldsOnly 1 fieldCosmic statistics

10–3 −−−− 10–410–1 −−−− 10–2Redshift accuracy

0.10 sq. deg.0.25 sq. deg.Area

2 Å15 ÅMinimum EW

10–18 erg cm–2 s–16 · 10–18 erg cm–2 s–1Flux limit at 5σσσσ

OTELOSUBARU CHARACTERISTICS

SUBARU data from Ly et al. 2007


OTELO LyOTELO Lyαααααααα emittersemitters

OTELO luminosity

Limit (z=5.6 & 6.7)2.000 LAEs expected

Dijkstra et al. 2007


Spiral galaxies in OTELOSpiral galaxies in OTELO

OTELO EW limit at10–18 erg cm–2 s–1

(z up to 1.5)

SUBARU EW limit

Hameed & Devereux 2005


Elliptical/S0 galaxies in Elliptical/S0 galaxies in OTELOOTELO

For the typicalemission line

luminosity of anelliptical galaxy

OTELO can detect EW~0.2

(z up to 0.9)

Fukugita et al. 2004


OTELO Chemical OTELO Chemical EvolutionEvolution

Metallicity vs. [NII]λλλλ658.3nm/Hαααα for KISS emission line galaxies (Melbourne & Salzer

2002)

Using [NII]λλλλ658.3nm/Hααααas metallicity indicator.

Up to z=0.40 with OSIRIS, up to z=1.5 via NIR spectroscopy of

OTELO Hββββ, [OIII], [OII] emitters.

Extinction correction & R23 comparison

Jordi Cepa 3D-NTT Scientific Committee, April 2nd 2008 28Díaz et al. 2006

OTELO lower metalicity limit

(z up to 0.4)

Dwarf galaxies in OTELO Dwarf galaxies in OTELO MetalicityMetalicity


OTELO ProductsOTELO Products

1037.0Lyαααα

1030.84BCD

7 · 1031.50Sy

3 · 104

1.50Sa-b-c-d-Im

0.84E/S0

Expected numberMaximum redshift Morphological Type

Assuming no evolution, H0=65 km/s/Mpc, ΩΩΩΩm0=0.3, ΩΩΩΩΛΛΛΛ0=0.7



HORUSHORUSHHydrogen and ydrogen and OOxygen xygen RRecombination ecombination UUltradeep ltradeep SSurveyurvey


HORUS snapshotHORUS snapshot

• Ultra-deep emission line survey at blue λλλλ windows using TF

• Searching for LAEs from z = 4 to z = 2

• Some scientific objectives:

− Physics of LAE

⋅ LF evolution

⋅ Properties of the ionized gas

− Physics of LABs : Lymanα “blobs” (Steidel et al. 2000)

⋅ Frequency of LABs

⋅ Start and end epochs

⋅ Ionization mechanism

⋅ Properties of the ionized gas


HORUS TeamHORUS Team

Jesús Gallego (PI, UCM)

Jordi Cepa (PI, ULL-IAC)

Angel Bongiovanni (IAC)

Héctor Castañeda (IAC)

Ignacio González (IFCA-UNICAN)

Rafael Guzmán (U.Fl-UCM)

Ana Pérez García (IAC)

José Miguel Rodríguez (IAC)

Miguel Sánchez-Portal (INSA-ESAC)

Jeremy Blaizot (U. Lyon)

Stéphane Charlot (IAP)

Jean-Gabriel Cuby (LAM)

Johan Fynbo (KU, Sweden)

Kim Nilsson (MPIA)

Ian Parry (IOA)

Roser Pelló (Toulouse)


LyLyαααααααα blobsblobs

35 robust candidates in Matsuda et al. 2004

SUBARU SuprimeCamArea: 0.20 sq deg

(31×23 arcmin)BB: BVR (4-10 ks each)NB: 4977/77 (26 ks)FWHM: 1.0 arcsecLAEs: 283 DLAs: 49LABs: 74

Hayashino et al. 2004


LyLyαααααααα blobs: general blobs: general characteristicscharacteristics

• Luminous and extended Lyαααα nebulae at high z

• LLyαααα >~ 1043 erg/s (~10−−−−18 erg/cm2/s/arcsec2 ~ 27 mag/arcsec2)

• EW >~ 100 Å

• φφφφ ~ 100 kpc (>~ 16 arcsec2 @ z = 3.1)

• ∆∆∆∆v = 150 – 1700 km/s (mean ~ 500 km/s)

• V ∼∼∼∼ 27, R ∼∼∼∼ 25, and K ∼∼∼∼ 21 mag (more compact than Lyαααα)

• LIR ~ 1013 LSun

• No rotation

• Not associated with strong radio sources or X-Ray

• Located in dense and massive SF environments


LyLyαααααααα blobs: doblobs: do’’s and s and don'tsdon'ts

• Some do not have any continuum at all

• Some have several components in the line

• Some can be associated with SCUBA sources

• The largest ones have bubble-like structures

• R counterpart might be shifted wrt K

• A wide variety of sizes exists (some are semi-compact)


LyLyαααααααα blobs: unknowns to blobs: unknowns to be answeredbe answered

• Ionization mechanism. Likely a mixed bag of:

– Photoionization due to SF regions (cannot explain 30%)

– Photoionization produced by AGN (seems not general)

– Photoionization by diffuse UV background (too weak)

– Shock heating due to starburst driven superwinds

– Cooling radiation from gas accreting over DM haloes

• When LABs began to form? When disappear? To form what?


HORUS outlineHORUS outline

• Scientific strategy: − Detecting LAEs/LABS using OSIRIS blue TF

− 3 × 10−18 erg/cm2/s/arcsec2 at S/N=3

− Observing “optical” emission lines in the NIR (EMIR MOS or CIRCE)

• Products (assuming same number at each z as of z = 3.1):− 45 LABs (the brightest 10% could be observed in GTC NIR spectroscopy)

− 436 LAEs

− 75 DLAs

• Then: ~529 objects (LABs, LAEs and DLAs) plus [OII] & [OIII] outliers

• Science:− LAEs LF vs z (exploring the “knee” between GALEX at 0.3 and 2.0)

− LABs at different z (looking for start and end of its formation)

− LAEs and LABs ionized gas properties via NIR spectroscopy

⋅ Ionization mechanism via Lyα/Hα

⋅ SFR

⋅ Metallicities via [NII]/Hα


LymanLymanαααααααα emitters in emitters in OSIRISOSIRIS

OTELO

OTELO

OTELO

HORUS

HORUS

HORUS

HORUS

Project

Brightest LABs?

Reference z

Hα & Hβ or [OIII]

All optic lines

Comments

0.8---9807.0

0.9---9256.6

2.82.31.8 1.34262.5

1.1---8155.7

1.7

2.2

3.2

Age(Gyr)

-2.41.85843.8

-2.01.54993.1

2.11.61.23892.2

Hαααα(µµµµm)

Hββββ/[OIII] (µµµµm)

[OII] (µµµµm)

Lyαααα(nm)

z



GLACEGLACEGGaaLALAxy xy CClusters lusters EEvolutionvolution


GLACE snapshotGLACE snapshot

• Emission line survey of selected clusters using TF• Scanning several emission lines (2 Virial Radii, ±3000 km/s)

• At z ~ 0.24, 0.4, 0.6 and 0.8 (only [OII] at 0.6 and 0.8) TBC

• Some scientific objectives:− Study evolution of galaxies in clusters and of clusters of galaxies

− Star forming galaxies (position, suppressed, mergers, vs. MIR SFR)

− AGNs (concentration, fraction vs. redshift)

− Metallicities and ionized gas properties

− Comparison field vs cluster at similar redshifts (OTELO)

− Morphological segregation

− Cluster dynamical masses

− Optical cooling flows in cluster central galaxies

− Field LAEs and other emitters

• Some expected follow-ups: Hαααα in NIR for Oxygen emitters


GLACE TeamGLACE Team

Miguel Sánchez-Portal (PI, ESAC)

Jordi Cepa (PI, ULL-IAC)

Emilio Alfaro (IAA)

Bruno Altieri (ESAC)

Narciso Benítez (IEM-CSIC)

Francisco Castander (IEEC)

Héctor Castañeda (IAC)

Nieves Castro (IAC)

Daniella Coia (ESAC)

I. González-Serrano (IFCA-UNICAN)

Arturo Manchado (IAC)

Leo Metcalfe (ESAC)

Ismael Pérez-Fournón (IAC)

R. Pérez-Martínez (ESAC)

J.M. Rodríguez-Espinosa (IAC)

I. Valtchanov (ESAC)

Philippe Amram (OAMP)Alfonso Aragón-Salamanca (U.Nott)Chantal Balkowski (OPM)Michael Balogh (U. Waterloo)Andrea Biviano (INAF, Bologna)Malcolm Bremer (U. Bristol)Gianfranco Brunetti (INAF, Bologna)Pierre-Alain Duc (CEA)Dario Fadda (TBC, Caltech)Jean-Paul Kneib (OAMP)Karl-Heinz Mack (INAF, Bologna)Ben Maugham (U. Bristol)Brian mcBreen (U. Dublin)Bianca Poggianti (INAF, Padova)Mari Polleta (IAP)Piero Rosatti (TBC, ESO)Ian Smail (U. Durham)Letizia Stangellini (NOAO)Giovanna Temporin (CEA)Alessandra Zanichelli (INAF, Bologna)



OTHER:OTHER:Absorption lines and BCDs


Absorption lines Absorption lines program snapshotprogram snapshot

• Observing elliptical galaxies and globular clusters using TF

• Scanning absorption lines and nearby pseudo-continuum:

− Mg triplet at ~517.6 nm

− Hβ and Hγ

− Fe at ∼517.0 nm, ∼438.3 nm and ∼533.5 nm

− Ca ∼422.7 nm and CaT

• Using new “2D indices” designed for

− disentangling age-metallicity

− determining abundances

− estimating IMF

• These indices are stable vs. velocity dispersion and redshift

• Co-Pis: A. Vazdekis (IAC), M. Beasley (IAC), J. Cepa (ULL-IAC)


BCDsBCDs program program snapshotsnapshot

• Supported by instrument builders

• Observing 40 BCDs using OSIRIS TF

• From the sample of HERSCHEL OT KP program by S. Madden (FIR spectroscopy using PACS)

• Lines: Hββββ, Hαααα, [OII] 3727, [OIII] 4363 and 5007, [NII] 5755 and 6584, [SII] 6717 and 6731, [SIII] 9069, as well as the WR emission features at 4850-4686 and 5698-5808

• Products: maps of extinction, electron density, temperature, abundances, studies of SF regions, location of WR stars, number of ionizing stars, IMF estimates, faint emission line structures,…

• Team:H. Castañeda (PI, IAC)J. Cepa (ULL-IAC)

C. Esteban (ULL-IAC)

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