Bringing SOUL on sky
Enrico Pinna, Fabio Rossi, Alfio Puglisi, Guido Agapito, Marco Bonaglia, Cedric Plantet, Tommaso Mazzoni, Runa Briguglio, Luca Carbonaro, Marco Xompero, Paolo Grani, Armando Riccardi, Simone Esposito, Phil Hinz, Amali Vaz, Steve Ertel, Oscar M. Montoya, Oliver Durney, Julian Christou, Doug L. Miller, Greg Taylor, Alessandro Cavallaro, Michael Lefebvre
BBringing SOUL on sky
Enrico Pinna a , Fabio Rossi a , Alfio Puglisi a , Guido Agapito a , Marco Bonaglia a , C´edric Plantet a ,Tommaso Mazzoni a , Runa Briguglio a , Luca Carbonaro a , Marco Xompero a , Paolo Grani a ,Armando Riccardi a , Simone Esposito a , Phil Hinz b , Amali Vaz b , Steve Ertel b , Oscar M.Montoya b , Oliver Durney b , Julian Christou c , Doug L. Miller c , Greg Taylor c , AlessandroCavallaro c , and Michael Lefebvre ca INAF - Osservatorio Astrofisico di Arcetri, Italy b Steward Observatory, University of Arizona, USA c Large Binocular Telescope Observatory, University of Arizona, USA
ABSTRACT
The SOUL project is upgrading the 4 SCAO systems of LBT, pushing the current guide star limits of about 2magnitudes fainter thanks to Electron Multiplied CCD detector. This improvement will open the NGS SCAOcorrection to a wider number of scientific cases from high contrast imaging in the visible to extra-galactic sourcein the NIR. The SOUL systems are today the unique case where pyramid WFS, adaptive secondary and EMCCDare used together. This makes SOUL a pathfinder for most of the ELT SCAO systems like the one of GMT,MICADO and HARMONI of E-ELT, where the same key technologies will be employed. Today we have 3 SOULsystems installed on the telescope in commissioning phase. The 4th system will be installed in a few months. Wewill present here the results achieved during daytime testing and commissioning nights up to the present date.
Keywords:
Pyramid, SCAO, LBT, high contrast, XAO, Adaptive Secondary
1. INTRODUCTION
The Large Binocular Telescope (LBT) is equipped with 4 Single Conjugated Adaptive Optics (SCAO) systems. All of them are composed by a pyramid WaveFront Sensor (WFS) working with Natural Guide Stars (NGS)and coupled with an Adaptive Secondary Mirror (ASM) as corrector. Two of these systems feed two NIRspector-imager (LUCI1 and LUCI2), while the remaining two feed the focal stations of LBTI. SOUL is aimedto upgrade all the 4 systems enabling the AO correction using stars 2 to 3 magnitude fainter. In fig.1 we reporta view of LBT with highlighted LBTI and the 2 LUCI together with the position of the 4 SOUL WFSs.In this work we will report about the current status of the SOUL commissioning (sect.2), the calibration ofthe SOUL-LUCI1 system (sect.3) and the main result obtained on-sky with LUCI1 and LBTI (sect.4).
2. THE UPGRADE
The SOUL upgrade has been described already in Pinna+2016, where the system details are reported togetherwith the performances estimated via numerical simulations. These have been performed analytically and withE2E tools. Here (fig.2), we report an update on the expected performance for SOUL in terms of SR valuesin R and Ks -band, compared with those estimated for FLAO under the same conditions. Considering thecurve of SR=20% in R -band, we expect that SOUL will deliver diffraction limited images on stars 3 magnitudefainter, moving the current limit from m R = 10 to 13 in good seeing conditions. This is a dramatic increasein the number of target available for SHARK-VIS. In the K s − band plot, we can take as reference the line ofSR=50%, showing a gain of about 2 magnitudes for good seeings and even larger in poor conditions ( > . >
50% with reference star m R = 15 and diffraction limited down to m R = 16, SOULis opening to extra-galactic targets, as bright AGN, diffraction limited images and long slit spectroscopy withLUCI2. This is a key feature at LBT, where LGS are available for GLAO correction only. Further author information:send correspondence to Enrico Pinna: [email protected] a r X i v : . [ a s t r o - ph . I M ] J a n igure 1. Top view of LBT with yellow lines marking the position of LUCI1 and LUCI2 and green for LBTI. The SOULlogos show the position of the 4 WFSs.Figure 2. Comparison of the FLAO and SOUL performance in R and K -band, as estimated via numerical simulations.The image report the SR value as color scale as function of guide star magnitude (x-axis) and seeing (y-axis). Wehighlighted in white the line of SR= 20% and 50% for R and K -band respectively.igure 3. The milestones of the SOUL project.Figure 4. Left: top view of the SOUL-LUCI1 WFS just before the telescope installation. In yellow the upgraded compo-nents. Center : WFS camera frame (averaged over 400 steps) showing the pupil images during on-sky operations. Themeasurement of the pupil positions confirmed that we achieved the desired magnification (40 ± SA on the diameter) andseparation (48 . ± . pix ). At 8 o’clock we can distinguish the beams of the LBT swing arms. Right
The first light onSOUL-LUCI1 in November 2018 with a SR(K)=87% on a reference star m R = 9 . . . kHz with no NCPA compensation. The project is now in advanced state, as shown in the timeline of fig.3. After a forced stop in order to allowthe completion of the HOST survey, we upgraded the first WFS (LBTI-SX) on March 2018 and the secondone (LUCI1) few months later (fig.4-left). Then, we had the first light for LBTI-SX on September 2018 and forLUCI1 in November of the same year (fig.4-center), delivering the first SOUL image in NIR (fig.4-right). Aboutthe WFS upgrade, details are available in the proceedings of this conference, as for tip-tilt mirror calibration, the optical alignment and software. After the successful first light for the first 2 systems, we upgraded the LBTI-DX system in the winter 2018-2019having its first light in February. Then the LUCI2 upgraded has been set in stand-by waiting for SOUL-LUCI1to be operational and offered for routine science observations. The two LUCI are both facility instrumentsfor LBT and the continuity in science operation is a requirement for the telescope. When we upgraded the FLAOon LUCI1, FLAO-LUCI2 was operative and available for science observations. Then, the first goal has been toprovide, on LUCI1, FLAO-like performances with high reliability, releasing it for science observations in SCAOmode and as NGS for ARGOS. This is foreseen to happen in Nov 2019 when LUCI2 FLAO system will thenavailable for the WFS upgrade. The first light on SOUL-LUCI2 in scheduled in February 2020. In the summer igure 5. Long exposure SR measured on LUCI1 during daytime testing with the calibration source. No NCPA correctionwas applied and the SR values are saturated around 75%. Different symbols represent different WFS camera binnings,while colors different seeing values. SHARK-VIS ans iLocater ), all fed by SOUL systems,will start to populate the LBT focal stations.
3. SYSTEM CALIBRATION
The calibration of the AO system has been performed at the telescope in daytime using the FLAO source andthe retro-reflector at the near focus of the ASM, following the same procedure as for the FLAO systems. Ascalibration we refer to: 1) the Interaction Matrix (IM) measurement; 2) tuning of the AO parameters as functionof the reference star brightness.The IM measurement has been performed with fast modal push and pull as described in Eposito+2010. We measured IMs for the WFS configurations of binning 1x1, 2x2 and 4x4 corresponding to 40, 20 and 10SAon the pupil diameter respectively. The calibration of binning 3x3 has been postponed to the next phase of theproject, where we will focus on the ultimate system performances.The parameter tuning has been done on the SOUL-LUCI1 system, because this instrument can provide H -band focal plane images, used here as merit function. On the SOUL-LBTI systems, we ported the same tuningobtained on SOUL-LUCI1. As light source for phase 2), we used the ARGOS calibration unit providing aneasier handling with respect to the FLAO one. We applied commands to the ASM mimicking the atmosphericturbulence equivalent to 0 .
6” and 1 .
0” of seeing. We explored binning (1x1, 2x2 and 4x4) and loop framerates as function of the simulated star brightness. As for the FLAO system, the AO loop gain are optimizedautomatically at the beginning of each closed loop, scanning the values (on 3 group of modes) and minimizingthe WF residuals. So, the gains are not included in the parameter to be tuned. This is the operation baseline,but an on-line optimization of the loop gain mode-by-mode is in progress and we plan to be the final operationalmode for SOUL. The on-line optimization of the gains is based on the Genndron-Lena technique applied to thepyramid WFS thanks to the measurement on the WS optical gain as described in Esposito+2015. The numerical simulations indicated that the tip-tilt modulation of 3 λ/D radius is suitable for the full rangeof magnitude. During this first tuning, we adopted this modulation value as fix, while in the future we plan tooptimize it for magnitude and seeing conditions. At this stage, we had no NCPA correction, so the maximum SRin H -band was saturated at about 80%. The result of these tests is reported in fig.5. Table 1 report the tuningobtained considering the performances measured in fig.5. This table is used for the automatic configurationof the system for on-sky operations. The EM gain of the WFS camera is set to 600 for m R > .
5, the valuerecommended by First Light, and decreased for brighter magnitudes in order to reduce the excess noise or avoidsaturation. able 1. AO parameters tuned on SOUL-LUCI1, as function of the reference star magnitude. These values are used forthe automatic configuration of the system for science operations. m R Binning framerate EM gain < . > . This control demonstrated to relax significantly theforces on the ASM, when high orders are controlled, producing a remarkable improvement of the loop robustness.In this phase of the project, we were limited to a maximum of 500 controlled modes due to the current opticalcalibration of the ASM. The SX-ASM calibration is 4 years old and does not match anymore the response ofthe optical surface at the higher spatial frequencies. In order to achieve the ultimate performance of SOUL, anew calibration of the ASM with the interferometer is planned in the next months. As you can notice in table5, the maximum frame rate is set to 1 . kHz , while the goal for SOUL is 2 . kHz . This is due to a limitation inthe fast diagnostic and could be solved in the next future. However, at this stage, the frame rate of 1 . kHz isnot the limiting factor for the SOUL performances.As future work in the daytime calibrations, we have: calibration of WFS binning 3x3 (improving in theregime around m r = 14 . m R >
4. ON-SKY RESULTS
In this section, we report the results obtained on the system up to June 2019. On-sky commissioning is ongoingand just a fraction of the planned nights (5 of 15) has been executed, mainly due to the weather conditions reallypoor in winter 2018-2019.
In fig.6 we report SR values (at 1650nm, measured at this wavelength or rescaled using Marechal’s approximation)obtained on LUCI1 during the commissioning at different star fluxes and seeing conditions. All these values arelong exposures (10 to 60s), obtained as direct sum of sub-frames with no shift and add. We mainly focused on igure 6. SR values at 1650 nm reported as function of the flux detected on the WFS and the Dimm seeing in the line ofsight (colors). Different symbols represent different WFS samplings (binnings). The dashed lines report the simulationsvalues expected with no and strong telescope vibrations for a seeing of 1 . the higher part of the flux range (binning 1x1 and binning 2x2), while the faint end is still to be explored. Weexperienced seeing usually higher than 0 .
9” on the line of sight. In the plot we report as comparison the valuesexpected from simulation with seeing of 1 .
0” for two cases, considering no and strong telescope vibrations. Thecorrection of NCPA was not calibrated at that time and so no correction was applied. With LUCI N30 cameraNCPA limits the maximum achievable SR around 80% in H -band.In this first phase of commissioning, we collected good performances showing already the gain of SOUL w.r.t.to FLAO. In fig.7, we report a sample of PSFs measured during the commissioning nights. In fig.7 top-leftwe show the long exposure PSF in bright regime ( m r = 9 .
5) under strong seeing conditions (fast variability1 . − . In fig.7 top-center we show the PSF of a guide star of m R = 12 . . SR ( H ) = 36% on a reference star of m R = 13 . . Both systems are operational and routinely used for science since their respective upgrades. The commissioning ofboth systems has been carried on to the point where system can be operated by the LBTI team, enabling scienceoperation both in imaging and interferometric modes. The automation of the AO operations is progressing inthe commissioning of SOUL-LUCI1 and all improvements are periodically ported to LBTI systems. This is nowallowed by the alignment of the control SW on all the 4 SOUL systems. The performance tuning and theirquantitative assessment is postponed to the availability of SHARK-NIR and SHARK-Vis that will provide PSFimages at shorter wavelength in daytime with the calibration source.Said that, the qualitative feedback of the LBTI observers states that SOUL shows better stability (higherefficiency in time) and increased limiting magnitude. In addition, the system can be operated and delivers good
Figure 7.
Top: a sample of PSF measured on LUCI1 during the SOUL commissioning. All are long exposures on the AOreference star.
Bottom: radial profile of the top-left PSF (solid line) compared with the theoretical PSF on the LUCI1focal plane (dotted). The plot shows a raw contrast of the order of 10 − at 400 − mas off the peak. correction under higher seeing ( > . m r = 8 . M (cid:48) and the deepest one in L (cid:48) (see fig.8).All the details and scientific results have been published in Wagner+2019. On the fainter end, we report theobservation of a quad lensed quasar of integrated magnitude over the 4 components of m R = 15 .
3. Again guidingon the target, well resolved images have been acquired in K s , L (cid:48) and M (cid:48) -bands (see fig.9 and Jones+2019 ).The upgrade AO has also been demonstrated to be usable for nulling interferometry, and a first data set tocharacterize the impact of the upgrade on the nulling data quality has been obtained (to be analyzed). Higherstability and wavefront correction have a positive impact on the efficiency of nulling observations, the range ofsuitable seeing conditions, and the ability to observe at low elevations. The actual nulling data quality is thoughtto be limited by other factors, so that only minor improvements from the SOUL upgrade are expected here.
5. CONCLUSIONS
The SOUL project is in progress and in advanced status, having upgraded 3 of 4 systems. The two serving LBTIare routinely used for science operations both in imaging and interferometric modes. The one serving LUCI1will be released for science on November 2019. The fourth system will be upgraded in the winter 2019-2020. igure 8. Example of observation with SOUL-LBTI on a bright source. Here a young star shows spiral arms in L (cid:48) and M (cid:48) -band in a dual-aperture observation just after the SOUL first light on LBTI-DX.Figure 9. Quad lensed quasar observed with SOUL-LBTI SX on this February. From left to right the images are in K s , L an M -bands. This images allowed to compare the flux ration of the central peaks with the model. Credit: T. J. Jones& L. L. R. Williams, University of Minnesota. he on-sky performances with LUCI1 still requires a full characterization under the full range of referencestar magnitudes and seeing conditions. However, the first results show that the system is able to reach theexpected performances in terms of SR in the range 9 < m R < . > . and HARMONI on the E-ELT and the NGAO ofGMT. Therefore, SOUL represents a unique pathfinder for such systems that will provide the first AO correctionon ELTs. ACKNOWLEDGMENTS
The SOUL team wants to acknowledge the valuable and constant support provided by the LBTO personnelduring the integration and commissioning activity both at the Steward Observatory labs. and on the mountain.
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