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LBT “baseline” offered modes

NIR Imaging NIR Low Res Spec OPT Imaging (wide) OPT Imaging (narrow) OPT Low Res Spect. Nulling TIR Interf. Fizeau TIR Interf. Fizeau OPT Interf. ICE spectrograph for PEPSI at the LBT. Bertinoro (Forlì), 7-9 October 2002. LBT “baseline” offered modes. NIRVANA- …. AMBER-MIDI-PRIMA.

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LBT “baseline” offered modes

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  1. NIR Imaging NIR Low Res Spec OPT Imaging (wide) OPT Imaging (narrow) OPT Low Res Spect Nulling TIR Interf. Fizeau TIR Interf. Fizeau OPT Interf. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 LBT “baseline” offered modes NIRVANA- …. AMBER-MIDI-PRIMA MODS-LBC-LUCIFER ???- …. FORS-(VIMOS)-ISAAC UVES - … Why not High Resolution Spectroscopy ?

  2. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 Existing instruments (*) now modified in a bench-mounted fiber-feed high-resolution spectrograph

  3. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 Scientific drivers for any HR spectrograph • Galactic: • stellar structure and evolution, chemical abundances, internal mixing, line profiles, radial velocities, winds and mass losses • magnetic fields, magnetic surface structures, Doppler imaging • formation and evolution of the galactic disk, bulge and halo • ISM kinematics and chemical composition • stellar pulsations and oscillations • extrasolar planets • Extragalactic: • emission and absorption lines in QSOs and distant galaxies • physics of intergalactic medium, observational cosmology, high-z universe • structure and dynamics of central regions of AGNs

  4. High Resolution Spectroscopy Twin Mirrors deserve more Spectropolarimetry • Two mirrors – 2 Stokes • Gregorian Foci Ultra High Res. Spectroscopy • High thrughput • AO – narrow slit

  5. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 Unique science drivers for the LBTprimary scientific drivers for ICE/PEPSI • Spectropolarimetry : • structure and dynamics of surface magnetic fields in: • normal stars (late-type stars, young stellar objects) • accretion sources in close binaries • central black holes in AGNs • UHR spectroscopy : • line profiles, asymmetries, bisectors • stars (convection, rotation, velocity fields, isotopic ratios) • interstellar medium (velocity components, 6Li/7Li) • astroseismology, extrasolar planets

  6. ICE and PEPSI @ the LBT R. Pallavicini & F.M. Zerbi on behalf of the PEPSI with ICE Consortium Istituto Nazionale di Astrofisica Astrophysikalisches Institut Potsdam

  7. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 ICE and PEPSI @ the LBT two useful acronyms: PEPSIPotsdam Echelle Polarimetric & SpectroscopicInstrument proposed for LBT by K.G.Strassmeier ICEItalian Consortium Echelle Spectrograph for PEPSI proposed by R.Pallavicini & F.M.Zerbi as Italian contribution to PEPSI

  8. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 PEPSI with ICE Italian Consortium Institutes INAF/Osservatorio Astronomico Palermo INAF/Osservatorio Astronomico Brera INAF/Osservatorio Astrofisico Catania INAF/Osservatorio Astronomico Trieste (science only) Associate Scientists R.Gratton (OAPd), M.Rodonò (Univ. Catania), S.Randich (Arcetri), A.Bragaglia (OABo), E.Covino (OAC), G.Mulas (OACa),… others welcome !

  9. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 Instrument requirements • R ~ 80,000 with 1” slit in HR polarimetric mode • Max R ~ 200,000 - 400,000 with AO in UHR mode • wavelength range: ~ 500-1000 nm in 3-4 exposures • slit sampling of 2.5 pixels • four spectra per echelle order • different fiber sizes for different resolutions • total throughput ~20% at 650 nm (telescope+spectr.+CCD butno slit losses and fiber losses) • limiting magnitude V~19 at R=80,000, S/N=10 per resolution element in 1 hr • CCD: 4Kx4K (HR mode) or 8Kx4K (UHR mode) maximum • fiber fed, bench mounted, thermally controlled, high mechanical stability

  10. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 Requirements for polarimetry • 10-3...-4 precision in Stokes parameter IQUV for V=5 • 10-2 precision for AGNs with V=17 • time resolution for the sum of IQUV of »10 minutes for target brighter than 10th magnitude • 2 polarization components from each mirror • 2 exposures required to recover all Stokes parameters

  11. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 Science with PEPSI • The science case of “PEPSI with ICE” has been preliminary discussed by K.G. Strassmeier, J.B. Rice, R. Pallavicini, F.M. Zerbi and S.Catalano: “The Science case for the PEPSI with ICE high-resolution echelle spectropolarimeter for the LBT” to be published in Astronomical Notes 324 (2003) • Further inputs from the Italian community have been solicited and are expected from a number of associated scientists: P.Molaro, P.Bonifacio, S.Cristiani, G.Vladilo (OATs), M.Rodonò (Univ. CT), R.Gratton and E.Carretta (OAPd), S.Randich (Arcetri), A.Bragaglia (OABo), E.Covino (OAC), G.Mulas (OACa) + other scientists interested in the scientific use of the instrument.

  12. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 Scientific drivers in polarimetric mode • Magnetic fields in active late-type stars: Zeeman-Doppler imaging of active cool stars will allow understanding their magnetic activity and dynamo • Magnetic fields in chemically peculiar A and B stars: will allow mapping the structure of large-scale magnetic fields and to understand their effects on chemical inhomogeneities • Magnetic fields in T-Tauri stars and circumstellar disks: will allow studying magnetically-controlled accretion and to infer magnetic field geometries and spatial structure of scattering envelopes • Geometry of the central regions of AGNs and of jets: will allow inferring the geometry of the inner regions of AGNs from the polarization produced by asymmetric configurations

  13. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 Scientific drivers in non-polarimetric mode • Asteroseismology of hot and cool stars: radial and non-radial pulsations in a variety of stars (l Bootis, d Scuti, Herbig Ae/Be, solar-type stars) will provide information on stellar interiors and evolutionary state • Atmospheric dynamics: accurate radial velocity measurements and line profiles will allow understanding the velocity fields in the atmospheres of dwarfs and giants • Doppler imaging of rapidly rotating stars: surface inhomogeneities in active stars will be mapped from Doppler signatures in line profiles • Search for extrasolar planets: planets orbiting nearby stars will be detected, and their properties determined, from radial velocity measurements

  14. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 Scientific drivers in non-polarimetric mode II • Chemical abundance determinations: accurate chemical abundances for individual elements and their ratios will provide information on stellar nucleosynthesis, internal mixing processes, and galactic chemical evolution • Circumstellar disks and protoplanetary systems: will allow resolving absorption and/or emission components and to study the kinematics of gaseous circumstellar shells (e.g. b Pic systems and shells around AGB stars) • QSO absoption lines : will allow investigating the chemical evolution of galaxies over cosmological timescales, the dynamics of the central regions of early galaxies and the distribution and kinematics of the intergalactic medium at high redshift

  15. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 Scientific drivers in the UHR (AO) mode • Stellar granulation and line bisectors: will allow investigating the properties of convection in late-type stars through their effects on line profiles • Li6/Li 7 isotopic ratio in metal poor stars: will allow setting the issue of the Li primordial abundance and understand Li enrichment during galactic evolution • Physical, chemical and dynamical studies of the diffuseinterstellar medium: will allow the separation of different velocity components and the determination of thermal and turbulent line broadenings • Stellar oscillations, asteroseismology, extrasolar planetsearches and QSO absorption line studies: will all benefit from the increased spectral resolution

  16. Cosmological Suggestions by F. Mannucci • Determination of the cosmological evolution of : measuring metallic absorption lines of Quasars at 100 m/s velocity resolution. • Direct measure of the Cosmological constants: measuring the time variation of the redshift in absorption lines of quasars or gravitational lensed galaxies ( 1 mt/s)

  17. Integral Integral Flip mirror Flip mirror light light Polarimeter Polarimeter Thick fiber bundles Thin fiber bundles Exchange mechanism Slit ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 PEPSI schematic layout

  18. Flip mirror Thin fiber bundles (UHR) l /2 frenel rhomb Thick fiber bundles (HR) l /4 K prism Flip mirror st 1 mirror: Star + Th-Ar beam splitter nd 2 mirror: Star + Sky Circular or Linear polarization Thick fiber bundles (HR) ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 Integral light Polarimeter

  19. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 How to build the Spectrograph ? • Span from R=30,000 (with polarimeters) to R=300,000 in • Integral light (still with some light). • Large Spectral coverage in limited amount of shots. • Within the limits of “reasonable” R4 mosaic fabrication. • Process multiple traces per order (ord/extraord- ThAr –Sky…) • Good image quality in the whole format • Don’t spend a fortune in detectors. • …..

  20. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 ICE - double echelle (Zerbi, Spanò, Conconi, Molinari, Mazzoleni, Pallavicini, Strassmeier: 2002, AN 324)

  21. M3 M1 M2 Slit Echelle 1 Echelle 2 4Kx4K CCD Short Camera VPH Cross-disperser 8Kx4K CCD Long Camera M4 ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 ICE - double echelle

  22. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 ICE - double echelle Main characteristics • 2 R4 12.9 gr/mm echelles • Wavelength range: 500-1000 nmin 150 orders • Beam size: 16 cm • 4 VPHG cross-dispersers • F/3.0 short camera (SC) • F/4.9 long camera (LC) • 4Kx4K CCD (SC) • 8Kx4K CCD (LC) • 200 micron fibers (SC) • 50 micron fibers (LC)

  23. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 ICE – double echelle Image quality Troughput l (nm) 550 700 900 Optics 0.79 0.79 0.79 2 echelles 0.30 0.30 0.30 Cross disp. 0.92 0.91 0.92 CCD QE 0.92 0.87 0.51 Telescope 0.75 0.75 0.75 Fibers 0.80 0.80 0.80 Total 0.12 0.11 0.07 Spot diagrams for the short camera. Boxes are 4 pixels wide (60 mm). Rows show spots for three different orders; columns show the borders and the center of the related free spectral range.

  24. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 ICE – double echelle Limits of this configuration • low efficiency • customized R4 echelle (12.9 gr/mm) • mechanical complexity and cost • limited image quality (10-15 mm typical RMS spot radii) Better go back to “classical” single Echelle Solution

  25. SHORT CAMERA – NO AO Fiber input 0”.13 = fiber core 0”.4 = bundle size 0”.33 = fiber core 1” = bundle size input output LONG CAMERA WITH AO 1” ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 ICE – single echelle Fiber slicing The optical layout has a resolution-slit product of ~40,000 arcsec. In order to obtain an effective resolution of ~100,000 a circular slit of 1” can be divided in seven 0.33” slices through a microlens array, as shown here. At the output, a second linear microlens array simulates a narrow slit 0.40x3.50 arcsec2. Alternative solution based on single fiber and image slicer under study.

  26. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 ICE – single echelle Short camera short camera VPH cross-disperser folding mirror slit R4 echelle (R. Pallavicini, F.M. Zerbi, P. Spanò, P. Conconi, R. Mazzoleni, E. Molinari, K.G. Strassmeier: 2002, SPIE 4841)

  27. VPH cross-disperser long camera folding mirror slit R4 echelle ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 ICE – single echelle Long camera

  28. Short camera M2 Output microlens M1 Focal reducer Echelle ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 ICE – single echelle

  29. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 ICE – single echelle Main characteristics • 1 R4 31.6 gr/mm echelle • Wavelength range: 450-1100 nmin 81 orders • Beam size: 20 cm • 4 VPHG cross-dispersers • F/2.27 short camera (SC) • F/3.64 long camera (LC) • 4.6Kx4K CCD (SC) • 9.2Kx2K CCD (LC) • 100 micron fiber bundles (SC) • 50 micron fiber bundles (LC)

  30. 3 4 9.2K ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 ICE – single echelle Spectral format • SHORT CAMERA (f=500 mm): • full spectral coverage until 910 nm • 4.6K x 4K CCD mosaic • 25-27 orders per exposure • minimum interorder separation: 12” • 2.5 pixel sampling for 0”.33 projected slit width LONG CAMERA (f=1200 mm): • full spectral coverage until 770 nm • 9.2K x 2K CCD mosaic • fewer orders per exposure (<7) • minimum interorder separation: 12” • 2.2 pixel sampling for 0”.13 projected slit width 2 1

  31. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 ICE – single echelle Image quality Spot diagrams for the short camera including fiber, microlenses and related optics. Boxes representes 1 pixel (13.5 mm). Rows show different orders; columns show the borders and the center of the related free spectral range. Spot diameters Camera Short Long RMS typical (mm)3-4 4-6 RMS maximum (mm)7 9 Geometric max (mm)17 18

  32. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 ICE – single echelle Throughput l (nm) 550 700 900 Optics 0.79 0.79 0.79 Echelle 0.71 0.69 0.68 Cross disp. 0.93 0.92 0.94 CCD QE 0.92 0.87 0.51 Telescope 0.75 0.75 0.75 Fibers 0.80 0.80 0.80 Total 0.28 0.26 0.15 A factor 2 higher than the 2-echelle configuration ! VPH efficiencies

  33. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 ICE – single echelle CCD QE

  34. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 ICE – single echelle Limiting magnitude • In HR mode (R~100,000) V=20.4 at S/N=10 per resolution element in 1 hour and 0.7” seeing. • Two magnitudes better than UVES at R=120,000 • In UHR (R ~ 300,000) V=17 at S/N=10 per resolution element in a few hours.

  35. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 What is actually PEPSI with ICE vs. LBT world • PEPSI with ICEis a first-light PI instrument (nationally funded) proposed by the Astrophysical Institute of Potsdam (PI: Klaus Strassmeier) • Implementation of PEPSI with ICE at the LBT has been recommended by the LBT ScienceAdvisory Committee (SAC) and accepted by the LBT Corporation • A Consortium of Italian Institutes will contribute to PEPSI with the design, construction and integration of the high-resolution ICE spectrograph (Co-PI: R. Pallavicini – Tech.Ref. F.M. Zerbi)

  36. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 PO PI: K.G.Strassmeier Manager: M.Andersen Work Packages AIP PI: Strassmeier Italian Consortium PI: Pallavicini Industry Polarimeter Spectrograph CCD camera Guiding unit Spectrograph Optics CCDs Optical assembly Fiberfeed Mosaic assembly LBT standard verification OABr (Zerbi) OAPa (Pallavicini) OACt (Catalano) Polarizers & Retarders Controller Mechanical structure Integration & tests Electronics assembly Manufacturing Optics Optics Control software Gratings Camera head Electronics hardware Data reduction Tests Mechanical structure Long camera (AO mode) Electronics Mirror & lenses Dewar Mode selector #1 & #2 Thermal enclosure Camera selector Calibration unit Fibers Control and Calibr. software Spectrograph pre-integration Science case Science case Telescope integration

  37. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 Italian Work Packages Spectrograph co-PI: R. Pallavicini OABr F.M.Zerbi OAPa R.Pallavicini OACt S.Catalano Associate Scientists R.Gratton (OAPd) P.Molaro (OATs) Optical Design Optical Design Electronics Optical Design (RG) Mechanical Structure AO Mode Control Software Science Case (RG, PM) Thermal Enclosure Camera selector Detector/Polarim.?? Other collaborators: contribution to science case Integration & Tests Science Case Science Case

  38. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 ICE Budget(preliminary) Total Budget 3.75 M€ - Germany 60% (fully allocated), Italy 40% Italian Cost Breakdown: Collimators 100 Echelle 400 Cross-dispersers 100 Camera (short) 200 Camera (long) 200 Mechanics 200 Electronics and SW 200 Managing 100 TOTAL 1,500 KEuro

  39. ICE spectrograph for PEPSI at the LBT Bertinoro (Forlì), 7-9 October 2002 Status of the project • Mid 2001: PEPSI with ICE approved and funded in Germany • Early 2001 to present: work in Italy carried out at OAPa, OABr, OACt for the ICE spectrograph • February 2002: project workpackage structure, responsabilities and schedule finalysed on the basis of a 60%(D) / 40%(I) share. Decision about funding in Italy still pending (end 2002 ?) • Expected time schedule • end 2002: Final optical design and preliminary mechanical design • early 2003 - mid 2005: construction phase and integration • end 2005: first light at LBT and commissioning (at least in the non-AO short-camera mode) …..with or without Italy

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