2014 Call for Proposals for Instrument Upgrades
and New Instruments
Summary of the Proposals
and New Instruments
Summary of the Proposals
iFUN@LBT (Integral Field Unit with NICS at LBT) - a short track, inexpensive, near-IR IFU to be coupled with FLAO
The full scientific exploitation of the extraordinary performances of FLAO at LBT can only be achieved with a diffraction limited near-IR Integral Field Unit. The importance of IFUs in tackling the hottest topics has been demonstrated in recent years, especially when they are coupled with AO systems. Currently, no existing instrument provides the high Strehl Ratio (SR), spatial resolution and sky coverage of the FLAO system. Therefore the combination of FLAO with a near-IR IFU would be greatly beneficial to many science cases, including galaxy evolution (dynamics, resolved physical properties), disks and jets from stars, circumnuclear regions of local galaxies and AGNs.
NICS, the near-IR camera and spectrograph of the Italian national telescope TNG, will be decommissioned in the near future. However, the instrument is still performing well and could be easily re-used.
We therefore propose to build a fast track, inexpensive, near-IR IFU by placing a bundle of fibers in one of the LBT foci and by sending them to the focal plane of NICS. The spectroscopic characteristics of NICS would not change(R=1000-2500, with possible extension up to 10000). We can place up to ~250 fibers onto the 1K detector, producing a ~16x16 IFU. The spatial scale can be between 50x50 mas (for detailed studies of stellar jets and AGNs) and 150x150mas (for galaxy evolution studies where the low surface brightness requires larger spaxels), with wavelength coverage between 1-2.5 μm. The only real competitors with such good AO correction will be the new ESO instrument ERIS and NIRSPEC on board of JWST, both available only in ~2019. Therefore having such an instrument in a short time and with a limited money investment ensures several years of frontline science at LBT.
The people involved at the moment are: G. Cresci, E. Oliva, F. Mannucci, A. Tozzi, D. Ferruzzi, J. Antichi, F. Bacciotti, C. Baffa, A. Gallazzi, E. Giani, L.K. Hunt, L. Magrini, F. Massi, L. Podio, E. Sani, S. di Serego Alighieri, P. Tozzi, S. Zibetti (INAF-Arcetri), P. Hinz, R. Thompson (Arizona), F. Ghinassi, E. Molinari (TNG), S. Antoniucci, A. Fontana, D. Lorenzetti, B. Nisini, F. Vitali (INAF-OAR), A. Marconi (UniFi), V. Foglietti (CNR-ISM).
We welcome people from all the partners interested in the project, both for the developing and for its scientific use. Interested people can contact us:
Giovanni Cresci <[email protected]>
Ernesto Oliva <[email protected]>
Filippo Mannucci <[email protected]>
The full scientific exploitation of the extraordinary performances of FLAO at LBT can only be achieved with a diffraction limited near-IR Integral Field Unit. The importance of IFUs in tackling the hottest topics has been demonstrated in recent years, especially when they are coupled with AO systems. Currently, no existing instrument provides the high Strehl Ratio (SR), spatial resolution and sky coverage of the FLAO system. Therefore the combination of FLAO with a near-IR IFU would be greatly beneficial to many science cases, including galaxy evolution (dynamics, resolved physical properties), disks and jets from stars, circumnuclear regions of local galaxies and AGNs.
NICS, the near-IR camera and spectrograph of the Italian national telescope TNG, will be decommissioned in the near future. However, the instrument is still performing well and could be easily re-used.
We therefore propose to build a fast track, inexpensive, near-IR IFU by placing a bundle of fibers in one of the LBT foci and by sending them to the focal plane of NICS. The spectroscopic characteristics of NICS would not change(R=1000-2500, with possible extension up to 10000). We can place up to ~250 fibers onto the 1K detector, producing a ~16x16 IFU. The spatial scale can be between 50x50 mas (for detailed studies of stellar jets and AGNs) and 150x150mas (for galaxy evolution studies where the low surface brightness requires larger spaxels), with wavelength coverage between 1-2.5 μm. The only real competitors with such good AO correction will be the new ESO instrument ERIS and NIRSPEC on board of JWST, both available only in ~2019. Therefore having such an instrument in a short time and with a limited money investment ensures several years of frontline science at LBT.
The people involved at the moment are: G. Cresci, E. Oliva, F. Mannucci, A. Tozzi, D. Ferruzzi, J. Antichi, F. Bacciotti, C. Baffa, A. Gallazzi, E. Giani, L.K. Hunt, L. Magrini, F. Massi, L. Podio, E. Sani, S. di Serego Alighieri, P. Tozzi, S. Zibetti (INAF-Arcetri), P. Hinz, R. Thompson (Arizona), F. Ghinassi, E. Molinari (TNG), S. Antoniucci, A. Fontana, D. Lorenzetti, B. Nisini, F. Vitali (INAF-OAR), A. Marconi (UniFi), V. Foglietti (CNR-ISM).
We welcome people from all the partners interested in the project, both for the developing and for its scientific use. Interested people can contact us:
Giovanni Cresci <[email protected]>
Ernesto Oliva <[email protected]>
Filippo Mannucci <[email protected]>
SHARK (System for coronagraphy with High order Adaptive optics from R to K band)
SHARK is intended to be an instrument taking advantage of the existing AO modules which are obtaining excellent performance in terms of extreme AO correction. Two channels are foreseen: a near infrared channel (0.9-2.5 mm) and a visible one (0.6 – 0.9 mm), both providing imaging and coronagraphic modes. Each channel may be installed in one arm of the telescope, at the LBTI focii, providing in this way possible contemporary observations from R to K bands.
SHARK will provide extreme Strehl Ratios, reaching top performance >90% in H and K bands with a typical resolution of 50 mas at 2 micron, and SR values >45% in the visible with a resolution ~20 mas at 650 nm. The diffraction limited FoV (increasing with the wavelength) is limited to a distance of few arcsec from the reference star where the AO correction is more effective. Partial AO correction can be obtained at larger radii (<30 arcsec in K Band). An IFU facility is planned in the visible, in a 2 arcsec region, with spaxel in the range 40-80 mas and spectral resolution in the range 100-5000.
SHARK requirement specifications will be driven by its science core: direct imaging of giant exoplanets at very close separation from the reference star. As an optical-IR imager making use of extreme AO correction, SHARK will deliver unprecedented results also in solar system science (e.g., asteroids and planetary satellites), stellar science (e.g., SFRs, disks, and Jets; very low-mass objects and BDs; the inner part of nearby GCs), and in the extragalactic field (e.g., nearby bright AGNs).
Jacopo Farinato: <[email protected]>
Fernando Pedichini: <[email protected]>
Enrico Pinna: <[email protected]>
SHARK is intended to be an instrument taking advantage of the existing AO modules which are obtaining excellent performance in terms of extreme AO correction. Two channels are foreseen: a near infrared channel (0.9-2.5 mm) and a visible one (0.6 – 0.9 mm), both providing imaging and coronagraphic modes. Each channel may be installed in one arm of the telescope, at the LBTI focii, providing in this way possible contemporary observations from R to K bands.
SHARK will provide extreme Strehl Ratios, reaching top performance >90% in H and K bands with a typical resolution of 50 mas at 2 micron, and SR values >45% in the visible with a resolution ~20 mas at 650 nm. The diffraction limited FoV (increasing with the wavelength) is limited to a distance of few arcsec from the reference star where the AO correction is more effective. Partial AO correction can be obtained at larger radii (<30 arcsec in K Band). An IFU facility is planned in the visible, in a 2 arcsec region, with spaxel in the range 40-80 mas and spectral resolution in the range 100-5000.
SHARK requirement specifications will be driven by its science core: direct imaging of giant exoplanets at very close separation from the reference star. As an optical-IR imager making use of extreme AO correction, SHARK will deliver unprecedented results also in solar system science (e.g., asteroids and planetary satellites), stellar science (e.g., SFRs, disks, and Jets; very low-mass objects and BDs; the inner part of nearby GCs), and in the extragalactic field (e.g., nearby bright AGNs).
Jacopo Farinato: <[email protected]>
Fernando Pedichini: <[email protected]>
Enrico Pinna: <[email protected]>
LBC-2 (LBC upgrade)
With the purpose of maintaing LBC competitive during the coming decade among the instruments working at 8m class telescopes, we propose some technical improvement functional to a better performance.
Before describing these upgrades, we mention that - in close collaboration with LBTO - we are starting a dedicated work to improve the performances and stability of the active optics control. We will test better algorithms of image analysis and try to implement faster corrections. We therefore do not include any modification of the optical and electronic system of the cameras at this stage, pending the conclusion of these tests.
In making our analysis we have taken into account new projects and instruments ready to be in operation or in a developing status. For instance, Hyper-Suprimecam, the new camera at the primary focus of Subaru , with its 90 arcmin FoV offers a solution that cannot be reached at the primary focus of LBT, given the constraints posed by the available volumes. As a consequence, our efforts are on ameliorate the LBC performance via an increase of the quantum efficiency and/or a larger spectral coverage.
In other words, LBC-2 will be a camera for deep multi-band observations in a medium FoV.
The main characteristics of LBC optics is the high efficiency in the UV of the blue channel. In this window, LBC-2 will continue to be unique (for instance, Hyper-Suprimecam is blind at wavelengths shorter than the B band) in its being the only one instrument capable in delivering UV images till m=27 in a few hours of exposure. This uniqueness can be largely improved. At moment, the 4 chip mosaic of the blue channel has an efficiency of about 50% at 350 nm. We are evaluating with E2V the possibility they deliver a 6000x6000 monolithic detector with a FoV equivalent to the mosaic we have now, but with an efficiency >70% (goal 80%) at 350 nm that would imply a gain of more than 0.7 mag with the same exposure time.
As for the red channel, we are considering a similar upgrade with a 6000x6000 monolithic detecor, having >100 micron thickness, reaching a significant efficiency till 1 micron (40%). In such a way, performances similar to those given by the primary focus at Subaru can be obtained, even tough on a significantly smaller FoV (~25x25 arcmin). An high efficiency at 1 micron is relevant, for instance, to the study of primordial galaxies.
The typical cost of the upgrade for each channel is expected in the range 200-300KEuro.
We have also explored the possibility of replacing the silicon-based detectors with near-IR detectors, in order to make it efficient over the whole range 600 nm to 1.8 microns, which would allow imaging from visible until the H band. This camera should adopt a next-generation 4000x4000 detector with a cut-off at 1.8um and would have a field ~ 17x17 arcmin, i.e., > 4 times the field of Hawk-I at the VLT.
With this option LBC-2, in terms of quantum efficiency is therefore complementary to Hyper-Suprimecam, adding information UV and YJH. It is important to note that the new NIR detectors, if treated properly, are able to provide high quantum efficiency starting from about 500 nm. In this way it is possible to maintain a continuity between the two spectral channels of LBC-2. With the blue channel it would obtain images in the UV-BV and with the NIR channel images in RIZYJH.
This option is of course more challenging (considering the so far not optimal performances of IR detectors with a 1.8um cutoff) and more expensive (exceeding 1ME), and is therefore considered of lower priority.
Enrico.Cappellaro: [email protected]
With the purpose of maintaing LBC competitive during the coming decade among the instruments working at 8m class telescopes, we propose some technical improvement functional to a better performance.
Before describing these upgrades, we mention that - in close collaboration with LBTO - we are starting a dedicated work to improve the performances and stability of the active optics control. We will test better algorithms of image analysis and try to implement faster corrections. We therefore do not include any modification of the optical and electronic system of the cameras at this stage, pending the conclusion of these tests.
In making our analysis we have taken into account new projects and instruments ready to be in operation or in a developing status. For instance, Hyper-Suprimecam, the new camera at the primary focus of Subaru , with its 90 arcmin FoV offers a solution that cannot be reached at the primary focus of LBT, given the constraints posed by the available volumes. As a consequence, our efforts are on ameliorate the LBC performance via an increase of the quantum efficiency and/or a larger spectral coverage.
In other words, LBC-2 will be a camera for deep multi-band observations in a medium FoV.
The main characteristics of LBC optics is the high efficiency in the UV of the blue channel. In this window, LBC-2 will continue to be unique (for instance, Hyper-Suprimecam is blind at wavelengths shorter than the B band) in its being the only one instrument capable in delivering UV images till m=27 in a few hours of exposure. This uniqueness can be largely improved. At moment, the 4 chip mosaic of the blue channel has an efficiency of about 50% at 350 nm. We are evaluating with E2V the possibility they deliver a 6000x6000 monolithic detector with a FoV equivalent to the mosaic we have now, but with an efficiency >70% (goal 80%) at 350 nm that would imply a gain of more than 0.7 mag with the same exposure time.
As for the red channel, we are considering a similar upgrade with a 6000x6000 monolithic detecor, having >100 micron thickness, reaching a significant efficiency till 1 micron (40%). In such a way, performances similar to those given by the primary focus at Subaru can be obtained, even tough on a significantly smaller FoV (~25x25 arcmin). An high efficiency at 1 micron is relevant, for instance, to the study of primordial galaxies.
The typical cost of the upgrade for each channel is expected in the range 200-300KEuro.
We have also explored the possibility of replacing the silicon-based detectors with near-IR detectors, in order to make it efficient over the whole range 600 nm to 1.8 microns, which would allow imaging from visible until the H band. This camera should adopt a next-generation 4000x4000 detector with a cut-off at 1.8um and would have a field ~ 17x17 arcmin, i.e., > 4 times the field of Hawk-I at the VLT.
With this option LBC-2, in terms of quantum efficiency is therefore complementary to Hyper-Suprimecam, adding information UV and YJH. It is important to note that the new NIR detectors, if treated properly, are able to provide high quantum efficiency starting from about 500 nm. In this way it is possible to maintain a continuity between the two spectral channels of LBC-2. With the blue channel it would obtain images in the UV-BV and with the NIR channel images in RIZYJH.
This option is of course more challenging (considering the so far not optimal performances of IR detectors with a 1.8um cutoff) and more expensive (exceeding 1ME), and is therefore considered of lower priority.
Enrico.Cappellaro: [email protected]
iLocater - The World's First Diffraction-Limited Doppler Spectrometer
We propose to design and build a new high-resolution spectrometer that will identify and characterize Earth-like planets orbiting the nearest stars. The instrument concept, named “iLocater,” will be the world's first diffraction-limited Doppler spectrometer. By operating in a new wavelength range, the near-infrared, and simultaneously correcting for image-blurring effects introduced by Earth’s turbulent atmosphere, iLocater will generate ultra-precise radial velocity (RV) measurements that address outstanding questions in exoplanetary science.
iLocater will receive a well-corrected beam of starlight from LBTI. With input images that achieve 30 times higher spatial resolution than “seeing-limited” designs (i.e., all radial velocity predecessors), iLocater will simultaneously enable high spectral resolution (R=110,000), high throughput, and a compact optical design at low cost. Compared to present-day Doppler instruments, a diffraction-limited spectrometer will: (1) be significantly easier to stabilize (temperature, pressure), thus leading to higher radial velocity precision; (2) receive three orders of magnitude less background contamination from sky-emission and the moon; (3) employ a single-mode optical fiber to eliminate modal noise, which is known to induce spurious Doppler shifts; and (4) reduce astrophysical jitter arising from spots that rotate with the surface of stars. Further, iLocater will have the unique ability to monitor and ameliorate internal systematic errors by using two separate telescope dishes simultaneously, enabling the first RV measurement precisions below 1 m/s at near-infrared wavelengths.
Taking advantage of the LBT’s dual aperture configuration, diffraction-limited capabilities, and optimized infrared performance, the proposed instrument represents an advance in technology that would rank first internationally in terms of sensitivity, precision, and ability to conduct leading-edge science. iLocater will: (1) identify Earth-like planets orbiting in the habitable-zone around the nearest stars; (2) perform the first systematic study of planet occurrence around binary stars as a function of their orbital separation and mass ratio, placing new constraints on planet formation models; (3) obtain the first spin-orbit measurements of transiting terrestrial planets; (4) study the youngest exoplanets to inform our understanding of planet formation and migration; (5) acquire essential follow-up observations for NASA's planned Transiting Exoplanet Survey Satellite (TESS) mission; and (6) assess the composition of transiting “mini-Neptunes” and “super-Earths.”
iLocater is a low-risk, high-reward instrument with low power consumption that takes up very little real-estate, complements the suite of current LBTO instruments, and may be easily integrated within the observatory. Hardware deliverables include an acquisition camera mounted to LBTI and stabilized spectrometer fed by long optical fibers; both will be developed on a 3 year timescale. iLocater will become a facility-class instrument available to all LBT consortium users through the standard competitive observing proposal process. An international team of senior scientists representing all LBT partners has been assembled to help design, build, and commission the instrument and contribute observing time to address the aforementioned science cases.
Additional team members are encouraged to contact PI Justin Crepp for more information [[email protected]].
We propose to design and build a new high-resolution spectrometer that will identify and characterize Earth-like planets orbiting the nearest stars. The instrument concept, named “iLocater,” will be the world's first diffraction-limited Doppler spectrometer. By operating in a new wavelength range, the near-infrared, and simultaneously correcting for image-blurring effects introduced by Earth’s turbulent atmosphere, iLocater will generate ultra-precise radial velocity (RV) measurements that address outstanding questions in exoplanetary science.
iLocater will receive a well-corrected beam of starlight from LBTI. With input images that achieve 30 times higher spatial resolution than “seeing-limited” designs (i.e., all radial velocity predecessors), iLocater will simultaneously enable high spectral resolution (R=110,000), high throughput, and a compact optical design at low cost. Compared to present-day Doppler instruments, a diffraction-limited spectrometer will: (1) be significantly easier to stabilize (temperature, pressure), thus leading to higher radial velocity precision; (2) receive three orders of magnitude less background contamination from sky-emission and the moon; (3) employ a single-mode optical fiber to eliminate modal noise, which is known to induce spurious Doppler shifts; and (4) reduce astrophysical jitter arising from spots that rotate with the surface of stars. Further, iLocater will have the unique ability to monitor and ameliorate internal systematic errors by using two separate telescope dishes simultaneously, enabling the first RV measurement precisions below 1 m/s at near-infrared wavelengths.
Taking advantage of the LBT’s dual aperture configuration, diffraction-limited capabilities, and optimized infrared performance, the proposed instrument represents an advance in technology that would rank first internationally in terms of sensitivity, precision, and ability to conduct leading-edge science. iLocater will: (1) identify Earth-like planets orbiting in the habitable-zone around the nearest stars; (2) perform the first systematic study of planet occurrence around binary stars as a function of their orbital separation and mass ratio, placing new constraints on planet formation models; (3) obtain the first spin-orbit measurements of transiting terrestrial planets; (4) study the youngest exoplanets to inform our understanding of planet formation and migration; (5) acquire essential follow-up observations for NASA's planned Transiting Exoplanet Survey Satellite (TESS) mission; and (6) assess the composition of transiting “mini-Neptunes” and “super-Earths.”
iLocater is a low-risk, high-reward instrument with low power consumption that takes up very little real-estate, complements the suite of current LBTO instruments, and may be easily integrated within the observatory. Hardware deliverables include an acquisition camera mounted to LBTI and stabilized spectrometer fed by long optical fibers; both will be developed on a 3 year timescale. iLocater will become a facility-class instrument available to all LBT consortium users through the standard competitive observing proposal process. An international team of senior scientists representing all LBT partners has been assembled to help design, build, and commission the instrument and contribute observing time to address the aforementioned science cases.
Additional team members are encouraged to contact PI Justin Crepp for more information [[email protected]].
LIVE - The LBT Interferometer Visible Extension
The Large Binocular Telescope with its integrated adaptive optics systems and the LBTI beamcombiner provides a good platform for carrying out coherent imaging across its 22.6 m baseline. The first cameras used with LBTI have focused on infrared wavelengths.
We describe a concept, called the LBT Interferometer Visible Extension (LIVE) to carry out coherent imaging with the LBT at wavelengths shorter than 1 µm.
LIVE will be able to create images of some of the stars with the largest angular diameters, map the surface of solar system moons, and provide detailed imaging of the inner scattered light regions of protoplanetary and transition disks.
An initial approach can use the beamcombiner with its existing infrared phase sensor to carry out coherent imaging using frame selection to improve the image quality. Refined and more versatile phase sensing and correction can be implemented in a second stage to enable observations of a wider range of targets.
Phil Hinz - [email protected]
Simone Esposito - [email protected]
The Large Binocular Telescope with its integrated adaptive optics systems and the LBTI beamcombiner provides a good platform for carrying out coherent imaging across its 22.6 m baseline. The first cameras used with LBTI have focused on infrared wavelengths.
We describe a concept, called the LBT Interferometer Visible Extension (LIVE) to carry out coherent imaging with the LBT at wavelengths shorter than 1 µm.
LIVE will be able to create images of some of the stars with the largest angular diameters, map the surface of solar system moons, and provide detailed imaging of the inner scattered light regions of protoplanetary and transition disks.
An initial approach can use the beamcombiner with its existing infrared phase sensor to carry out coherent imaging using frame selection to improve the image quality. Refined and more versatile phase sensing and correction can be implemented in a second stage to enable observations of a wider range of targets.
Phil Hinz - [email protected]
Simone Esposito - [email protected]
Upgrading LMIRcam
A proposal is pending at the NSF Advanced Technologies and Instrumentation program to execute three upgrades to the existing LMIRcam mid-infrared imager that operates at the combined LBT focus provided by the LBTI. The primary aspects of this upgrade are
1) Replacement of the readout electronics for the HAWAII-2RG array with a Teledyne SIDECAR configuration. The current electronics can only address a 1024x1024 (10” x 10”) region of the 2048 x 2048 array whereas the existing optics deliver the full unvignetted 20” x 20” field-of-view with image quality capable of supporting interferometry.
2) Installation of an R~3000 ruled germanium grism and an R~50 direct-vision prism to complement the existing R~300 grism capability.
3) Development and installation of a 150x150 element pupil-plane lenslet IFU that disperses 20,000 points in a 3” x 3” field.
Expanding the field-of-view by four times enables a variety of mid-infrared "wide-field" studies. For example this field size is well matched to active star forming regions in nearby luminous infrared galaxies and LMIRcam L-band spatial resolution is well matched to HST resolution in the UV/Visible. The larger field of view also accommodates the 20,000 IFU spectra from a 3"x3" field, a spatial scale well matched to direct-imaging exoplanet searches where the spectral behavior of quasi-static speckles is well-distinguished from planetary spectra. These upgrades will be made available to the consortium as part of the evolving availability of LMIRcam/LBTI.
Michael Skrutskie - [email protected]
Phil Hinz - [email protected]
A proposal is pending at the NSF Advanced Technologies and Instrumentation program to execute three upgrades to the existing LMIRcam mid-infrared imager that operates at the combined LBT focus provided by the LBTI. The primary aspects of this upgrade are
1) Replacement of the readout electronics for the HAWAII-2RG array with a Teledyne SIDECAR configuration. The current electronics can only address a 1024x1024 (10” x 10”) region of the 2048 x 2048 array whereas the existing optics deliver the full unvignetted 20” x 20” field-of-view with image quality capable of supporting interferometry.
2) Installation of an R~3000 ruled germanium grism and an R~50 direct-vision prism to complement the existing R~300 grism capability.
3) Development and installation of a 150x150 element pupil-plane lenslet IFU that disperses 20,000 points in a 3” x 3” field.
Expanding the field-of-view by four times enables a variety of mid-infrared "wide-field" studies. For example this field size is well matched to active star forming regions in nearby luminous infrared galaxies and LMIRcam L-band spatial resolution is well matched to HST resolution in the UV/Visible. The larger field of view also accommodates the 20,000 IFU spectra from a 3"x3" field, a spatial scale well matched to direct-imaging exoplanet searches where the spectral behavior of quasi-static speckles is well-distinguished from planetary spectra. These upgrades will be made available to the consortium as part of the evolving availability of LMIRcam/LBTI.
Michael Skrutskie - [email protected]
Phil Hinz - [email protected]
Technology Development for Flexible LBT Multi-object Multi-instrument Spectroscopy
In the era of massive imaging surveys like DECam, PanSTARS, and soon LSST, rapidly-reconfigurable moderate-multiplex spectroscopy for efficient spectral follow-up will be an essential capability for any 8– 10 meter class telescope.
A robotic fiber positioner system at the Gregorian Foci of the LBT 8.4-m telescopes will leverage existing and future LBT investments in optical and near-infrared spectrographs. This facility positioner would rapidly reconfigure hundreds of fibers (and lenslets as necessary) in real-time between observations.
The output end of the fibers would be bundled together in multi-fiber connectors mounted in a ‘gang-connector’ to allow efficient simultaneous connection of all fibers to the fiber input of an instrument. Doing so permits connection to various, and even simultaneously to multiple, instruments on the observing floor. We are proposing to lead the conceptual development of and ultimately construct a prototype of such a universal fiber positioning system. We are seeking seed money to survey available positioner technologies and fund lab prototype evaluations.
This investment would lead to a future NSF proposal at the few $100K level for a phase1 20-fiber telescope demonstrator to fiber feed an existing MODS spectrograph. That demonstrator would be the gateway for an MSIP proposal for full binocular deployment and possibly additional instruments that could receive the ganged fibers.
Rick Pogge - [email protected]
Michael Strutskie - [email protected]
In the era of massive imaging surveys like DECam, PanSTARS, and soon LSST, rapidly-reconfigurable moderate-multiplex spectroscopy for efficient spectral follow-up will be an essential capability for any 8– 10 meter class telescope.
A robotic fiber positioner system at the Gregorian Foci of the LBT 8.4-m telescopes will leverage existing and future LBT investments in optical and near-infrared spectrographs. This facility positioner would rapidly reconfigure hundreds of fibers (and lenslets as necessary) in real-time between observations.
The output end of the fibers would be bundled together in multi-fiber connectors mounted in a ‘gang-connector’ to allow efficient simultaneous connection of all fibers to the fiber input of an instrument. Doing so permits connection to various, and even simultaneously to multiple, instruments on the observing floor. We are proposing to lead the conceptual development of and ultimately construct a prototype of such a universal fiber positioning system. We are seeking seed money to survey available positioner technologies and fund lab prototype evaluations.
This investment would lead to a future NSF proposal at the few $100K level for a phase1 20-fiber telescope demonstrator to fiber feed an existing MODS spectrograph. That demonstrator would be the gateway for an MSIP proposal for full binocular deployment and possibly additional instruments that could receive the ganged fibers.
Rick Pogge - [email protected]
Michael Strutskie - [email protected]
LBT-IFTS A deployable wide-field Imaging Fourier Transform Spectrograph for LBT
We envisages a unique spectroscopic capability for LBT using deployable wide-field Imaging Fourier Transform Spectrograph (IFTS) in the optical that offers high multiplex spectroscopy over the full Gregorian F/15 field of view (FoV).
LBT-IFTS is capable of obtaining spectra in selected bandpasses in the visible (from 350 to 850 nm) of every light source in a 12' x 12' FoV with a spatial sampling of 0.32". Its spectral resolution is variable, depending on the requirement of the observer, from R = 1 (broad-band image) to R in excess of ~1E4 . The spatial resolution is limited by the seeing at Mt. Graham, about 0.8" in R-band.
This project exploits the LBT's large light collecting power with a commercially available `turn-key ready' optical IFTS. Based on SITELLE (FoV 11' x 11'), soon to be deployed at CFHT in late 2014, the LBT-IFTS would use the wide FoV at the F/15 station to provide a large FoV with 100% field coverage and a very large number of fields sampling points to exceed 4 million. The concept uses ready available technology and experience from ABB, which controls costs due to industrial replication, reduces R&D efforts, aids maintenance, and minimizes risks.
Such an instrument would complete well against the current generation of narrow FoV integral field units (IFU) and also with the next generation of sparse sampling IFUs such as VIRUS (22' FoV; 1/7 or 52 sq. arcmin; 350-550nm) and would greatly expand on Principle Investigator (PI) driven science goals that require a contiguous, wide FoV.
IFTS on LBT would cover 144 sq. arcmin per pointing, providing integral field spectroscopy from 300nm out to 1um. Based on the proven design by ABB, LBT-IFTS offers a science field of 12' yielding a multiplex advantage of large sky coverage+100% filling factor compared to current generation of integral field spectrograph which have FoV up to 1' x 1' for MUSE on VLT. Co-added LBT spectral cubes would have 4-5x the sensitivity of the SITELLE+CFHT pairing offering a SNR=5 in a 4hr data cube of emission lines with flux levels of ~1E-17 erg/s/cm^2. The IFTS provides wide & contiguous spectroscopic fields of view that are well suited for any multiple, extended objects with low surface brightness or complex structures, such as nebulae, galaxies, mergers, clusters and gravitational lensed objects. In addition to emission line work, ABB IFTS, SpIOMM, has demonstrated its ability to observe absorption line object as well, possibly opening up such fields as stellar archaeology for the first time to an IFTS.
Glenn Morrison - [email protected]
Frederic Grandmont - [email protected]
We envisages a unique spectroscopic capability for LBT using deployable wide-field Imaging Fourier Transform Spectrograph (IFTS) in the optical that offers high multiplex spectroscopy over the full Gregorian F/15 field of view (FoV).
LBT-IFTS is capable of obtaining spectra in selected bandpasses in the visible (from 350 to 850 nm) of every light source in a 12' x 12' FoV with a spatial sampling of 0.32". Its spectral resolution is variable, depending on the requirement of the observer, from R = 1 (broad-band image) to R in excess of ~1E4 . The spatial resolution is limited by the seeing at Mt. Graham, about 0.8" in R-band.
This project exploits the LBT's large light collecting power with a commercially available `turn-key ready' optical IFTS. Based on SITELLE (FoV 11' x 11'), soon to be deployed at CFHT in late 2014, the LBT-IFTS would use the wide FoV at the F/15 station to provide a large FoV with 100% field coverage and a very large number of fields sampling points to exceed 4 million. The concept uses ready available technology and experience from ABB, which controls costs due to industrial replication, reduces R&D efforts, aids maintenance, and minimizes risks.
Such an instrument would complete well against the current generation of narrow FoV integral field units (IFU) and also with the next generation of sparse sampling IFUs such as VIRUS (22' FoV; 1/7 or 52 sq. arcmin; 350-550nm) and would greatly expand on Principle Investigator (PI) driven science goals that require a contiguous, wide FoV.
IFTS on LBT would cover 144 sq. arcmin per pointing, providing integral field spectroscopy from 300nm out to 1um. Based on the proven design by ABB, LBT-IFTS offers a science field of 12' yielding a multiplex advantage of large sky coverage+100% filling factor compared to current generation of integral field spectrograph which have FoV up to 1' x 1' for MUSE on VLT. Co-added LBT spectral cubes would have 4-5x the sensitivity of the SITELLE+CFHT pairing offering a SNR=5 in a 4hr data cube of emission lines with flux levels of ~1E-17 erg/s/cm^2. The IFTS provides wide & contiguous spectroscopic fields of view that are well suited for any multiple, extended objects with low surface brightness or complex structures, such as nebulae, galaxies, mergers, clusters and gravitational lensed objects. In addition to emission line work, ABB IFTS, SpIOMM, has demonstrated its ability to observe absorption line object as well, possibly opening up such fields as stellar archaeology for the first time to an IFTS.
Glenn Morrison - [email protected]
Frederic Grandmont - [email protected]
LUCIPOL - Diffraction limited polarimetry and spectropolarimetry with LUCI@LBT
Polarimetry is a powerful diagnostic tool to study astrophysical sources. Radiation mechanisms that produce similar radiation output can be disentangled by means of their polarisation signatures. Also, polarisation provides unique insights into the geometry of unresolved sources, even at cosmological distances.
We propose to equip the two LUCIs with dual-beam polarimetric units able to measure the four STOKES parameters both in imaging and spectroscopic mode. The polarimeters will be located within the AGWs, before the LUCI entrance windows, without any interference with the normal LUCI operative mode. Simply, at request, it will be possible to insert a polarimeter in the telescope beam.
Taking advantage of the best Adaptive Optics System with the smallest instrumental polarisation, LBT will be able to perform the largest field of view diffraction limited polarimetry and the highest resolution spectropolarimetry in the near infrared worldwide.
The uniqueness of LBT will be the possibility of continuous spectropolarimetric observations, LUCI + PEPSI, from 0.35 to 2.5 μm in one shot.
Francesco Leone - [email protected]
Polarimetry is a powerful diagnostic tool to study astrophysical sources. Radiation mechanisms that produce similar radiation output can be disentangled by means of their polarisation signatures. Also, polarisation provides unique insights into the geometry of unresolved sources, even at cosmological distances.
We propose to equip the two LUCIs with dual-beam polarimetric units able to measure the four STOKES parameters both in imaging and spectroscopic mode. The polarimeters will be located within the AGWs, before the LUCI entrance windows, without any interference with the normal LUCI operative mode. Simply, at request, it will be possible to insert a polarimeter in the telescope beam.
Taking advantage of the best Adaptive Optics System with the smallest instrumental polarisation, LBT will be able to perform the largest field of view diffraction limited polarimetry and the highest resolution spectropolarimetry in the near infrared worldwide.
The uniqueness of LBT will be the possibility of continuous spectropolarimetric observations, LUCI + PEPSI, from 0.35 to 2.5 μm in one shot.
Francesco Leone - [email protected]
SOUL - Single conjugated adaptive Optics Upgrade for LBT
Currently there are 4 SCAO systems operating at LBT, all composed by an Adaptive Secondary Mirror (672 actuators) and a Pyramid Wavefront Sensor (30x30 sub-apertures). Starting the on-sky operations in 2010, these systems provided the first high contrast images ever on 8m-class telescopes in the NIR. The use of state-of-the art devices is critical for the AO performances and, after about 10 years from the LBT SCAO design, the technological development made significant steps forward both in the visible detector and adaptive secondary fields. We propose here an upgrade of the two main AO system components: the wavefront sensor and the adaptive secondary.
Replacing the current wavefront sensor standard CCD with an Electron Multiplied CCD, we will provide: a faster read out (2kHz instead of 1kHz) at lower noise (< 1e- instead of ~10e-) and an higher spatial sampling (40 instead of 30 sub-apertures on the pupil diameter). Upgrading the adaptive secondary firmware, we will improve the mirror time response (from 1.0ms to 0.7 or 0.5ms as goal), being consistent with the new detector framerate, and the system robustness in strong seeing conditions. End-to-end simulations show that the higher spatial sampling and system frame rate allow correcting more modes with a larger control bandwidth, increasing so the Strehl Ratio (SR) in the case of bright guide stars and enabling operations at shorter wavelengths. The gain in magnitude (for a given SR) offered by SOUL is estimated to be around 1.5-2 magnitudes for all wavelengths in almost all the range of reference star brightness (7.5 < mR < 18). In terms of wavelengths, using a reference star mR = 12.5, the diffraction limit (SR~40%) will be achieved at 0.9 instead of 1.2 microns.
The gain in reference star magnitude implies a significant improvement of the sky-coverage that is currently the main limitations of the SCAO systems working with natural guide stars. SOUL will increase the sky coverage of the current systems up to a factor 10 at all wavelengths from R to KS. This allows to provide correction on extra-galactic objects, a category usually only available with LGS systems. As shown, providing a correction of SR = 25% at mR = 17.5 instead of mR = 16, it allows to close the loop on thousands of QSOs with z < 2.5 instead of a few tens. Moreover, all the scientific cases already exploited with the current SCAO systems, like imaging of disks and jets, study of stellar orbital motions, imaging of solar system objects and direct imaging of extrasolar planets will greatly benefit of the improved performances of SOUL.
Technical boundaries suggest the upgrade of the LBTI focal stations as first. This upgrade will boost the LBTI single dish and interferometric performances; moreover, it will be crucial for the newly proposed instrumentations, like SHARK, a NIR/VIS high contrast imager and coronagraph, and LIVE, the upgraded LBTI short wavelength interferometer, that will exploit the ultimate LBT potential with an angular resolution of 6mas.
SOUL is a fast track project that foresees the upgrade of the first two focal stations in about 1.5 years from the kick-off. It will allow the LBT SCAO systems to remain competitive and actually goes beyond the direct competitors currently in commissioning phase (SPHERE and GPI), or , with respect to ERIS, to take advantage of being ready for science about 2.5 years in advance.
Enrico Pinna <[email protected]>
Simone Esposito <[email protected]>
Armando Riccardi <[email protected]>
Currently there are 4 SCAO systems operating at LBT, all composed by an Adaptive Secondary Mirror (672 actuators) and a Pyramid Wavefront Sensor (30x30 sub-apertures). Starting the on-sky operations in 2010, these systems provided the first high contrast images ever on 8m-class telescopes in the NIR. The use of state-of-the art devices is critical for the AO performances and, after about 10 years from the LBT SCAO design, the technological development made significant steps forward both in the visible detector and adaptive secondary fields. We propose here an upgrade of the two main AO system components: the wavefront sensor and the adaptive secondary.
Replacing the current wavefront sensor standard CCD with an Electron Multiplied CCD, we will provide: a faster read out (2kHz instead of 1kHz) at lower noise (< 1e- instead of ~10e-) and an higher spatial sampling (40 instead of 30 sub-apertures on the pupil diameter). Upgrading the adaptive secondary firmware, we will improve the mirror time response (from 1.0ms to 0.7 or 0.5ms as goal), being consistent with the new detector framerate, and the system robustness in strong seeing conditions. End-to-end simulations show that the higher spatial sampling and system frame rate allow correcting more modes with a larger control bandwidth, increasing so the Strehl Ratio (SR) in the case of bright guide stars and enabling operations at shorter wavelengths. The gain in magnitude (for a given SR) offered by SOUL is estimated to be around 1.5-2 magnitudes for all wavelengths in almost all the range of reference star brightness (7.5 < mR < 18). In terms of wavelengths, using a reference star mR = 12.5, the diffraction limit (SR~40%) will be achieved at 0.9 instead of 1.2 microns.
The gain in reference star magnitude implies a significant improvement of the sky-coverage that is currently the main limitations of the SCAO systems working with natural guide stars. SOUL will increase the sky coverage of the current systems up to a factor 10 at all wavelengths from R to KS. This allows to provide correction on extra-galactic objects, a category usually only available with LGS systems. As shown, providing a correction of SR = 25% at mR = 17.5 instead of mR = 16, it allows to close the loop on thousands of QSOs with z < 2.5 instead of a few tens. Moreover, all the scientific cases already exploited with the current SCAO systems, like imaging of disks and jets, study of stellar orbital motions, imaging of solar system objects and direct imaging of extrasolar planets will greatly benefit of the improved performances of SOUL.
Technical boundaries suggest the upgrade of the LBTI focal stations as first. This upgrade will boost the LBTI single dish and interferometric performances; moreover, it will be crucial for the newly proposed instrumentations, like SHARK, a NIR/VIS high contrast imager and coronagraph, and LIVE, the upgraded LBTI short wavelength interferometer, that will exploit the ultimate LBT potential with an angular resolution of 6mas.
SOUL is a fast track project that foresees the upgrade of the first two focal stations in about 1.5 years from the kick-off. It will allow the LBT SCAO systems to remain competitive and actually goes beyond the direct competitors currently in commissioning phase (SPHERE and GPI), or , with respect to ERIS, to take advantage of being ready for science about 2.5 years in advance.
Enrico Pinna <[email protected]>
Simone Esposito <[email protected]>
Armando Riccardi <[email protected]>
ARGOS Upgrade - the Path to all Sky Visible Wavelength Interferometry
With the start of the ARGOS GLAO system at LBT a major step forward for the scientific competitiveness of the LBT is under way. Moving consequently forward in laser guide star adaptive optics instrument development, can make LBT absolutely unique in the world in terms of spatial resolution and sensitivity.
We propose here a phased approach in enhancing the LBT performance by three steps, with each of the steps enhancing the spatial resolution of the LBT.
The implementation of the upgrade in multiple stages makes the project affordable, both in terms of required manpower but also in terms of costs. Along the way to a short wavelength imaging interferometer plenty of capabilities and knowledge will be developed and implemented. Controlling the wavefront down to the 50nm level, phasing the mirrors at highest precision, tomographic wavefront measurement and LGS hybrid guiding are all techniques that require some efforts to be developed. Going this way in a phased approach and learning to walk before learning to run ensures that success can be achieved in the end.
Other adaptive optics facilities that aim for extreme high order correction, e.g. for exoplanet detection, do rely on the use of very bright stars to guide the AO, allowing observations of only a very limited number of objects. In contrast we propose to make use of the combination of Rayleigh and Sodium laser guide stars- consequently extending extreme adaptive optics to all the sky. In the combination with a visible wavelength interferometer, making use of LBTs Fizeau capabilities, we could push the spatial resolution towards a ~5 mas level.
In short, we think, that following the outlined path consequently, LBT could develop absolutely unique capabilities in highest resolution astronomy.
Sebastian Rabiens <[email protected]>
Simone Esposito <[email protected]>
With the start of the ARGOS GLAO system at LBT a major step forward for the scientific competitiveness of the LBT is under way. Moving consequently forward in laser guide star adaptive optics instrument development, can make LBT absolutely unique in the world in terms of spatial resolution and sensitivity.
We propose here a phased approach in enhancing the LBT performance by three steps, with each of the steps enhancing the spatial resolution of the LBT.
- PHASE I: All Sky Diffraction Limit in the IR: Implementation of a single sodium guide star and hybrid guiding into ARGOS. This upgrade was already foreseen from the beginning and is technically straightforward. This step leads us to 8m diffraction limited operation in the IR -anywhere in the sky.
- Phase II: All SkyDiffraction Limit in the Visible: Extension of the Sodium guide star system towards a constellation tomographic reconstruction to remove the cone effect. With an upgrade of the ground layer detection to a higher number of sub-apertures we will be able to make full use of the LBT’s AO secondary capabilities. This phase will enhance the AO performance in shorter bands, allowing for diffraction limited operation even in V & I band. In conjunction with a matching camera & spectrometer this ARGOS upgrade could show the same resolution in the optical as the planned ELTs will have in the NIR, therefore ideally suited for optical counterpart observations.
- Phase III: All Sky Interferometry in the Visible: Once having achieved adaptive optics correction at visible wavelengths, a next logical step would be to use LBTs interferometric capabilities in this wavelength range. This would push the performance towards a level in spatial resolution that no other facility in the world will be able to achieve for a long time.
The implementation of the upgrade in multiple stages makes the project affordable, both in terms of required manpower but also in terms of costs. Along the way to a short wavelength imaging interferometer plenty of capabilities and knowledge will be developed and implemented. Controlling the wavefront down to the 50nm level, phasing the mirrors at highest precision, tomographic wavefront measurement and LGS hybrid guiding are all techniques that require some efforts to be developed. Going this way in a phased approach and learning to walk before learning to run ensures that success can be achieved in the end.
Other adaptive optics facilities that aim for extreme high order correction, e.g. for exoplanet detection, do rely on the use of very bright stars to guide the AO, allowing observations of only a very limited number of objects. In contrast we propose to make use of the combination of Rayleigh and Sodium laser guide stars- consequently extending extreme adaptive optics to all the sky. In the combination with a visible wavelength interferometer, making use of LBTs Fizeau capabilities, we could push the spatial resolution towards a ~5 mas level.
In short, we think, that following the outlined path consequently, LBT could develop absolutely unique capabilities in highest resolution astronomy.
Sebastian Rabiens <[email protected]>
Simone Esposito <[email protected]>