We present an analysis of six independent on-sky datasets taken with the Keck-II/NIRC2 instrument. Using the off-axis point spread function (PSF) reconstruction software AIROPA, we extract stellar astrometry, photometry, and other fitting metrics to characterize the performance of this package. We test the effectiveness of AIROPA to reconstruct the PSF across the field of view in varying atmospheric conditions, number and location of PSF reference stars, stellar crowding, and telescope position angle (PA). We compare the astrometric precision and fitting residuals between a static PSF model and a spatially varying PSF model that incorporates instrumental aberrations and atmospheric turbulence during exposures. Most of the fitting residuals we measure show little to no improvement in the variable-PSF mode over the single-PSF mode. For one of the data sets, we find photometric performance is significantly improved (by ∼10 × ) by measuring the trend seen in photometry as a function of off-axis location. For nearly all other metrics we find comparable astrometric and photometric precision across both PSF modes, with a ∼13 % smaller astrometric uncertainty in variable-PSF mode in the best case. We largely confirm that the spatially variable PSF does not significantly improve the astrometric and other PSF fitting residuals over the static PSF for on-sky observations. We attribute this to unaccounted instrumental aberrations that are not characterized through afternoon adaptive optics (AO) bench calibrations.
Images obtained with single-conjugate adaptive optics (AO) show spatial variation of the point spread function (PSF) due to both atmospheric anisoplanatism and instrumental aberrations. The poor knowledge of the PSF across the field of view strongly impacts the ability to take full advantage of AO capabilities. The AIROPA project aims to model these PSF variations for the NIRC2 imager at the Keck Observatory. Here, we present the characterization of the instrumental phase aberrations over the entire NIRC2 field of view and we present a metric for quantifying the quality of the calibration, the fraction of variance unexplained (FVU). We used phase diversity measurements obtained on an artificial light source to characterize the variation of the aberrations across the field of view and their evolution with time. We find that there is a daily variation of the wavefront error (RMS of the residuals is 94 nm) common to the whole detector, but the differential aberrations across the field of view are very stable (RMS of the residuals between different epochs is 59 nm). This means that instrumental calibrations need to be monitored often only at the center of the detector, and the much more time-consuming variations across the field of view can be characterized less frequently (most likely when hardware upgrades happen). Furthermore, we tested AIROPA’s instrumental model through real data of the fiber images on the detector. We find that modeling the PSF variations across the field of view improves the FVU metric by 60% and reduces the detection of fake sources by 70%.
Adaptive optics (AO) images from the W. M. Keck Observatory have delivered numerous influential scientific results, including detection of multi-system asteroids, the supermassive black hole at the center of the Milky Way, and directly imaged exoplanets. Specifically, the precise and accurate astrometry these images yield was used to measure the mass of the supermassive black hole using orbits of the surrounding star cluster. Despite these successes, one of the major obstacles to improved astrometric measurements is the spatial and temporal variability of the point-spread function delivered by the instruments. Anisoplanatic and Instrumental Reconstruction of Off-axis PSFs for AO (AIROPA) is a software package for the astrometric and photometric analysis of AO images using point-spread function fitting together with the technique of point-spread function reconstruction. In AO point-spread function reconstruction, the knowledge of the instrument performance and of the atmospheric turbulence is used to predict the long-exposure point-spread function of an observation. We present the results of our tests using AIROPA on both simulated and on-sky images of the Galactic Center. We find that our method is very reliable in accounting for the static aberrations internal to the instrument, but it does not improve significantly the accuracy on sky, possibly due to uncalibrated telescope aberrations.
PSF knowledge is central to extract science from observations with adaptive optics.
However, it is often challenging to have a good PSF estimate. For instance, this is a problem for the integral field unit (IFU) OSIRIS at Keck Observatory. OSIRIS has a field of only few arcseconds, and it is often impossible to obtain a good empirical PSF. OSIRIS is equipped with an imager designed to track changes in the PSF on a reference star. However, the imager is 20 arcseconds away, which prevents to apply the observed PSF directly to spectroscopic data.
We developed a new software package to predict PSF variability for Keck AO images (AIROPA, see Paolo Turri’s contribution, this conference). To properly use the parallel imager to predict a PSF on the IFU, we adapted the code to the OSIRIS case (AIROPA-IFU).
Here, we present results of the application of this post-processing tools to Galactic Center observation. We also discuss the challenges encountered and the lessons learned when doing PSF
The progress achieved in implementing Point Spread Function reconstruction (PSF-R) capability at W. M. Keck Observatory (WMKO) is discussed. Observations of low-mass binary systems have been used to evaluate the improvements in astrometry and photometry using reconstructed PSFs. The on-sky performance of PSF-R is discussed by comparing the binary-fitting analysis using the reconstructed PSFs with the standard methods. We show that the PSFR in the NGS provides comparable performance to having a close reference star in the imaging science instrument. The on-sky troubleshooting efforts and the recent PSF-R technical developments are also presented. We find that the PSF-R reconstruction is more of a systems science problem that a post-processing problem. We close by discussing the lessons learned in the context of existing and future extremely large telescopes.
The integral field spectrograph OSIRIS at Keck I has been used to measure the motion of the stars around the supermassive black hole at the Center of the Galaxy. The small field of view provided and the crowding of the region prevent any good PSF estimate. A parallel imager can be used simultaneously to the IFU. However, its distance of 19 arcseconds prevents the observed PSF to be directly applied to the IFU because of anisoplanatism and instrumental aberrations. The Galactic Center Group at UCLA has developed an algorithms to predict PSF variability for Keck AO images (Off-axis PSF reconstruction, AIROPA software package). AIROPA allows us to use the parallel imager to correctly predict the IFU’s PSF. We modified this package to adapt it to the case of OSIRIS imager and IFU (AIROPA-IFU) and characterized the instrumental aberrations of both detectors. Here, we present preliminary results of the application of this post-processing tool to OSIRIS datasets of the Galactic Center.
KEYWORDS: Point spread functions, Imaging systems, Stars, Spectrographs, Signal to noise ratio, Adaptive optics, Atmospheric modeling, Data modeling, Astronomy
Knowledge of the point spread function (PSF) is critical to many astronomical science cases. However, the PSF can be very difficult to estimate for cases where there are many crowded point sources or for observations of extended objects. Additionally, for adaptive optics observations, the PSF can be very complex with both spatial and temporal variability in the PSF. Integral-field spectroscopy behind adaptive optics is especially challenging because the fields of view are typically too small to sample the halo for even a single PSF. Here, we present a method for semi-empirical PSF reconstruction for integral field spectrographs using a combination of point source observations on a parallel imager, instrumental aberration measurements, and atmospheric turbulence profiles. This work builds upon the PSF reconstruction project AIROPA designed for imaging and extending it to IFU work (AIROPA-IFU). By using empirical calibrators from the parallel imager, which has a much larger field of view, and accounting for anisoplantic effects and instrumental aberrations, we can predict the PSF on the spectrograph. An important aspect is being able to predict the PSF at many different wavelengths based on observations from broad-band imaging. Here, we discuss how science cases such as observations of stars at the Galactic center can benefit from this method. We also establish metrics to quantitatively assess the performance of PSF reconstruction. We show that for bright stars, AIROPA-IFU can produce spectra with signal to noise ratio 50% higher than with simple aperture extraction of a data cube.
KEYWORDS: Point spread functions, Adaptive optics, Photometry, General relativity, Sensors, Data modeling, Stars, Optical transfer functions, Atmospheric modeling, Instrument modeling
General relativity can be tested in the strong gravity regime by monitoring stars orbiting the supermassive black hole at the Galactic Center with adaptive optics. However, the limiting source of uncertainty is the spatial PSF variability due to atmospheric anisoplanatism and instrumental aberrations. The Galactic Center Group at UCLA has completed a project developing algorithms to predict PSF variability for Keck AO images. We have created a new software package (AIROPA), based on modified versions of StarFinder and Arroyo, that takes atmospheric turbulence profiles, instrumental aberration maps, and images as inputs and delivers improved photometry and astrometry on crowded fields. This software package will be made publicly available soon.
One of the primary scientific limitations of adaptive optics (AO) has been the incomplete knowledge of the point spread function (PSF), which has made it difficult to use AO for accurate photometry and astrometry in both crowded and sparse fields, for extracting intrinsic morphologies and spatially resolved kinematics, and for detecting faint sources in the presence of brighter sources. To address this limitation, we initiated a program to determine and demonstrate PSF reconstruction for science observations obtained with Keck AO. This paper aims to give a broad view of the progress achieved in implementing a PSF reconstruction capability for Keck AO science observations.
This paper describes the implementation of the algorithms, and the design and development of the prototype operational tools for automated PSF reconstruction. On-sky performance is discussed by comparing the reconstructed PSFs to the measured PSF’s on the NIRC2 science camera. The importance of knowing the control loop performance, accurate mapping of the telescope pupil to the deformable mirror and the science instrument pupil, and the telescope segment piston error are highlighted. We close by discussing lessons learned and near-term future plans.
We present a model of field-dependent aberrations arising in the NIRC2 instrument on the W. M. Keck II telescope. We use high signal-to-noise phase diversity data employing a source in the Nasmyth focal plane to construct a model of the optical path difference as a function of field position and wavelength. With a differential wavefront error of up to 190 nm, this effect is one of the main sources of astrometric and photometric measurement uncertainties. Our tests of temporal stability show sufficient reliability for our measurements over a 20-month period at the field extrema. Additionally, while chromaticity exists, applying a correction for field-dependent aberrations provides overall improvement compared to the existing aberrations present across the field of view.
Anisoplanatism is a primary source of photometric and astrometric error in single-conjugate adaptive optics. We present initial results of a project to model the off-axis optical transfer function in the adaptive optics system at the Keck II telescope. The model currently accounts for the effects of atmospheric anisoplanatism in natural guide star observations. The model for the atmospheric contribution to the anisoplanatic transfer function uses contemporaneous MASS/ DIMM measurements. Here we present the results of a validation campaign using observations of naturally guided visual binary stars under varying conditions, parameterized by the r0 and θ0 parameters of the C2n atmospheric turbulence profile. We are working to construct a model of the instrumental field-dependent aberrations in the NIRC2 camera using an artificial source in the Nasmyth focal plane. We also discuss our plans to extend the work to laser guide star operation.
The super-massive 4 million solar mass black hole (SMBH) SgrA* shows variable emission from the millimeter to the X-ray domain. A detailed analysis of the infrared light curves allows us to address the accretion phenomenon in a statistical way. The analysis shows that the near-infrared flux density excursions are dominated by a single state power law, with the low states of SgrA* are limited by confusion through the unresolved stellar background. We show that for 8-10m class telescopes blending effects along the line of sight will result in artificial compact star-like objects of 0.5-1 mJy that last for about 3-4 years. We discuss how the imaging capabilities of GRAVITY at the VLTI, LINC-NIRVANA at the LBT and METIS at the E-ELT will contribute to the investigation of the low variability states of SgrA*.
The dynamics of stars and gas undoubtedly shows the existence of a 4 million solar mass black hole at the
center of the Milky Way: Sagittarius A* (SgrA*). Violent flare emission allows us to probe the immediate
environment of the central mass. Near-infrared polarimetry now shows signatures of strong gravity that are
statistically significant against randomly polarized red noise. Using these signatures we can derive spin and
inclination information of SgrA*. A combined synchrotron self Compton (SSC) and adiabatic expansion model
with source components peaking in the sub-mm domain can fully account for the observed flare flux densities
and the time delays towards the (sub-)mm flares that have been reported in some cases. We discuss the expected
centroid paths of the NIR images and summarize how the geometrical structure of the emitting region (i.e.
spot shape, presence of a torus or spiral-arm pattern etc.) affects this centroid tracks. While most of the
mentioned geometries are able to fit the observed fluxes, future NIR interferometry with GRAVITY at the
VLT will break some of the degeneracies between different emission models. In this contribution we summarize
several GRAVITY science cases for SgrA*. Our simulations propose that focusing GRAVITY observations on
the polarimetry mode could reveal a clear centroid track of the spot(s). A non-detection of centroid shifts cannot
rule out the multi-component model or spiral arms scenarios. However, a clear wander between alternating
centroid positions during the flares will prove the idea of bright long-lived spots occasionally orbiting the central
black hole.
LINC-NIRVANA is the NIR homothetic imaging camera for the Large Binocular Telescope (LBT). Its Fringe
and Flexure Tracking System (FFTS) is mandatory for an efficient interferometric operation of LINC-NIRVANA:
the task of this cophasing system is to assure a time-stable interference pattern in the focal plane of the camera.
Differential piston effects will be detected and corrected in a real-time closed loop by analyzing the PSF of
a guide star at a frequency of 100Hz-200Hz. A dedicated piston mirror will then be moved in a corresponding
manner by a piezo actuator. The long-term flexure tip/tilt variations will be compensated by the AO deformable
mirrors.
A testbed interferometer has been designed to simulate the control process of the movement of a scaled
piston mirror under disturbances. Telescope vibration and atmospheric variations with arbitrary power spectra
are induced into the optical path by a dedicated piezo actuator. Limiting factors of the control bandwith are
the sampling frequency and delay of the detector and the resonance frequency of the piston mirror. In our setup
we can test the control performance under realistic conditions by considering the real piston mirrors dynamics
with an appropriate software filter and inducing a artificial delay of the PSF detector signal. Together with
the expected atmospheric OPD variations and a realistic vibration spectrum we are able to quantify the piston
control performance for typical observation conditions. A robust control approach is presented as result from
in-system control design as provided by the testbed interferometer with simulated dynamics.
As a near-infrared (NIR) wide field interferometric imager offering an angular resolution of about 10 milliarcseconds
LINC-NIRVANA at the Large Binocular Telescope will be an ideal instrument for imaging the center of the
Milky Way especially in conjunction with mm/sub-mm interferometers like CARMA, ATCA or, in the near
future, ALMA. Sagittarius A* (Sgr A*) is the electromagnetc manifestation of the ~4×106M super-massive
black hole (SMBH) at the Galactic Center. First results from a mult-wavelength campaign focused on Sgr A*,
based on the VLT
and on CARMA, ATCA, and the IRAM 30m-telescope, in May 2007 show that the NIR
data are consistent with partially depolarized non-thermal emission from confined hot spots in relativistic orbits
around SgrA*. A 3mm flare following a May 2007 NIR flare is consistent with SSC emission from adiabatically
expanding plasma in a wind or jet. With the LBT and ALMA we will be able to study the spectral evolution
of NIR/sub-mm/mm flare emission in order to constrain the emission mechanism, the jet/wind physics, and
possibly determine the angular momentum of the SMBH. LINC/NIRVANA will also serve to investigate the
stellar population and dynamics in the cluster surrounding Sgr A*. A particular emphasis will lie on examining
dust embedded and young stars and to unravel the star formation history in the cluster.
For the 0.3 parsec core radius central star cluster the investigation of will be investigated.
LINC-NIRVANA is the near-infrared homothetic imaging camera for the Large Binocular Telescope. Once
operational, it will provide an unprecedented combination of angular resolution, sensitivity and field of view. Its
Fringe and Flexure Tracking System (FFTS) is mandatory for an efficient interferometric operation of LINC-NIRVANA.
It is tailored to compensate low-order phase perturbations in real-time to allow for a time-stable
interference pattern in the focal plane of the science camera during the integration. Two independent control
loops are realized within FFTS: A cophasing loop continuously monitors and corrects for atmospheric and
instrumental differential piston between the two arms of the interferometer. A second loop controls common
and differential image motion resulting from changing orientations of the two optical axes of the interferometer.
Such changes are caused by flexure but also by atmospheric dispersion.
Both loops obtain their input signals from different quadrants of a NIR focal plane array. A piezo-driven
piston mirror in front of the beam combining optics serves as actuator in the cophasing loop. Differential piston
is determined by fitting a parameterized analytical model to the observed point spread function of a reference
target. Tip-tilt corrections in the flexure loop are applied via the secondary mirrors. Image motion is sensed for
each optical axis individually in out-of-focus images of the same reference target.
In this contribution we present the principles of operation, the latest changes in the opto-mechanical design,
the current status of the hardware development.
LINC-NIRVANA is the NIR homothetic imaging camera for the Large Binocular Telescope (LBT). Its Fringe
and Flexure Tracking System (FFTS) is mandatory for an effcient interferometric operation of LINC-NIRVANA:
the task of this cophasing system is to assure a time-stable interference pattern in the focal plane of the camera.
A testbed interferometer, set up as laboratory experiment, is used to develop the FFTS control loop and
to test the robustness of the fringe tracking concept. The geometry of the resulting interferometric intensity
distribution in the focal plane of the implemented CCD corresponds to that of the LBT PSF. The setup allows to
produce monochromatic (He-Ne laser) and polychromatic (halogen lamp) PSFs and allows to actively introduce
well defined low-order phase perturbations, namely OPD and differential tip/tilt. Furthermore, all components
that are required in a fringe tracking servo loop are included: a sensor for fringe acquisition and an actuator
to counteract measured OPD. With this setup it is intended to determine the performance with which a fringe
tracking control loop is able to compensate defined OPD sequences, to test different control algorithms, and to
optimize the control parameters of an existing servo system.
In this contribution we present the design and the realization of the testbed interferometer. Key parameters
describing the white light testbed interferometer, such as fringe contrast and thermal sensitivity are discussed.
The effects of all controllable phase perturbations are demonstrated.
Access to the requested content is limited to institutions that have purchased or subscribe to SPIE eBooks.
You are receiving this notice because your organization may not have SPIE eBooks access.*
*Shibboleth/Open Athens users─please
sign in
to access your institution's subscriptions.
To obtain this item, you may purchase the complete book in print or electronic format on
SPIE.org.
INSTITUTIONAL Select your institution to access the SPIE Digital Library.
PERSONAL Sign in with your SPIE account to access your personal subscriptions or to use specific features such as save to my library, sign up for alerts, save searches, etc.