NIRPS is a fiber-fed AO nIR spectrograph working simultaneously with HARPS at the La Silla-ESO 3.6m telescope. The cryogenic spectrograph operating at 75K employs a cross-dispersed echelle grating (R4), covering a wavelength range of 0.98-1.80 microns in a single image using a Teledyne Hawaii-4RG infrared detector. In early 2022, the NIRPS spectrograph was transported to Chile by plane with all the optical elements mechanically attached to the optical bench inside the vaccum vessel. To ensure the safety of the spectrograph, dedicated work was performed on the shipping crate design, which could survive up to 7g shocks. In La Silla, the vacuum vessel was re-integrated on its support structure and the spectrograph alignment was verified with the H4RG and the injection module. Given the optical design, the alignment phase was performed using a metrology arm and a few optical tests, which minimize the time required for this critical phase. From the validation/technical phase results, two major modifications were required. Firstly, the original grating element was replaced by a new etched crystalline silicon component made by the Fraunhofer Institute for Applied Optics and Precision Engineering. A novel technique was developed to verify the alignment at a warm temperature with the H4RG detector. Secondly, a thermal enclosure was added around the vacuum vessel to optimize thermal stability. Since then, the long-term thermal stability has been better than 0.2mK over 20 days. In this paper, we will review the final spectrograph performances, prior to shipping, and describe the novel techniques developed to minimize shipping costs, AITV phase duration, and grating replacement at the observatory. Additionally, we will discuss the thermal enclosure design to achieve the sub-mK thermal stability.
The Near-InfraRed Planet Searcher or NIRPS is a precision radial velocity spectrograph developed through collaborative efforts among laboratories in Switzerland, Canada, Brazil, France, Portugal and Spain. NIRPS extends to the 0.98-1.8 μm domain of the pioneering HARPS instrument at the La Silla 3.6-m telescope in Chile and it has achieved unparalleled precision, measuring stellar radial velocities in the infrared with accuracy better than 1 m/s. NIRPS can be used either standalone, or simultaneously with HARPS. Commissioned in late 2022 and early 2023, NIRPS embarked on a 5-year Guaranteed Time Observation (GTO) program in April 2023, spanning 720 observing nights. This program focuses on planetary systems around M dwarfs, encompassing both the immediate solar vicinity and transit follow-ups, alongside transit and emission spectroscopy observations. We highlight NIRPS’s current performances and the insights gained during its deployment at the telescope. The lessons learned and successes achieved contribute to the ongoing advancement of precision radial velocity measurements and high spectral fidelity, further solidifying NIRPS’ role in the forefront of the field of exoplanets.
HISPEC is a new, high-resolution near-infrared spectrograph being designed for the W.M. Keck II telescope. By offering single-shot, R 100,000 spectroscopy between 0.98 – 2.5 μm, HISPEC will enable spectroscopy of transiting and non-transiting exoplanets in close orbits, direct high-contrast detection and spectroscopy of spatially separated substellar companions, and exoplanet dynamical mass and orbit measurements using precision radial velocity monitoring calibrated with a suite of state-of-the-art absolute and relative wavelength references. MODHIS is the counterpart to HISPEC for the Thirty Meter Telescope and is being developed in parallel with similar scientific goals. In this proceeding, we provide a brief overview of the current design of both instruments, and the requirements for the two spectrographs as guided by the scientific goals for each. We then outline the current science case for HISPEC and MODHIS, with focuses on the science enabled for exoplanet discovery and characterization. We also provide updated sensitivity curves for both instruments, in terms of both signal-to-noise ratio and predicted radial velocity precision.
In less than a year, the James Webb Space Telescope (JWST) will inherit the mantle of being the world’s pre- eminent infrared observatory. JWST will carry with it an Aperture Masking Interferometer (AMI) as one of the supported operational modes of the Near-InfraRed Imager and Slitless Spectrograph (NIRISS) instrument. Aboard such a powerful platform, the AMI mode will deliver the most advanced and scientifically capable interferometer ever launched into space, exceeding anything that has gone before it by orders of magnitude in sensitivity. Here we present key aspects of the design and commissioning of this facility: data simulations (ami_sim), the extraction of interferometeric observables using two different approaches (IMPLANEIA and AMICAL), an updated view of AMI’s expected performance, and our reference star vetting programs.
KEYWORDS: Spectrographs, Telescopes, Lanthanum, Planets, Spectroscopes, Exoplanets, Aerospace engineering, Space operations, James Webb Space Telescope
NIRPS is a near-infrared (YJH bands), fiber-fed, high-resolution precision radial velocity (pRV) spectrograph currently under construction for deployment at the ESO 3.6-m telescope in La Silla, Chile. Through the use of a dichroic, NIRPS will be operated simultaneously with the optical HARPS pRV spectrograph and will be used to conduct ambitious planet-search and characterization surveys through a 720-night of guaranteed time allocation. NIRPS aims at detecting and characterizing Earth-like planets in the habitable zone of low-mass dwarfs and obtain high-accuracy transit spectroscopy of exoplanets. Here we present a summary of the full performances obtained in laboratory tests conducted at Université Laval (Canada), and the first results of the on-going on-sky commissioning of the front-end. Science operations of NIRPS is expected to start in late-2020, enabling significant synergies with major space and ground instruments such as the JWST, TESS, ALMA, PLATO and the ELT.
The HiCIBaS (High-Contrast Imaging Balloon System) project aims at launching a balloon borne telescope up to 36km to test high contrast imaging equipment and algorithms. The payload consists of a off the shelf 14-inch telescope with a custom-built Alt-Az mount. This telescope provides lights to two sensors, a pyramidal low order wave front sensor, and a coronagraphic wavefront sensor. Since the payload will reach its cruise altitude at about midnight mission, two target stars have been designated for observations, Capella as the night target, and Polaris as the early morning target. Data will be collected mainly on the magnitude of atmospheric and gondola’s turbulences, the luminosity of the background. The whole system is already built and ready to ship to Timmins for the launch in mid-August 2018.
WFIRST-AFTA is the NASA’s highest ranked astrophysics mission for the next decade that was identified in the New
World, New Horizon survey. The mission scientific drivers correspond to some of the deep questions identified in the
Canadian LRP2010, and are also of great interest for the Canadian scientists. Given that there is also a great interest in
having an international collaboration in this mission, the Canadian Space Agency awarded two contracts to study a
Canadian participation in the mission, one related to each instrument. This paper presents a summary of the technical
contributions that were considered for a Canadian contribution to the coronagraph and wide field instruments.
JWST’s Near-Infrared Imager and Slitless Spectrograph (NIRISS) includes an Aperture Masking Interferometry (AMI) mode designed to be used between 2.7μm and 4.8μm. At these wavelengths, it will have the highest angular resolution of any mode on JWST, and, for faint targets, of any existing or planned infrastructure. NIRISS AMI is uniquely suited to detect thermal emission of young massive planets and will permit the characterization of the mid-IR flux of exoplanets discovered by the GPI and SPHERE adaptive optics surveys. It will also directly detect massive planets found by GAIA through astrometric accelerations, providing the first opportunity ever to get both a mass and a flux measurement for non-transiting giant planets. NIRISS AMI will also enable the study of the nuclear environment of AGNs.
The Gemini Planet Imager (GPI) has as its science instrument an infrared integral field spectrograph/polarimeter (IFS). Integral field spectrographs are scientificially powerful but require sophisticated data reduction systems. For GPI to achieve its scientific goals of exoplanet and disk characterization, IFS data must be reconstructed into high quality astrometrically and photometrically accurate datacubes in both spectral and polarization modes, via flexible software that is usable by the broad Gemini community. The data reduction pipeline developed by the GPI instrument team to meet these needs is now publicly available following GPI’s commissioning.
This paper, the first of a series, provides a broad overview of GPI data reduction, summarizes key steps, and presents the overall software framework and implementation. Subsequent papers describe in more detail the algorithms necessary for calibrating GPI data. The GPI data reduction pipeline is open source, available from planetimager.org, and will continue to be enhanced throughout the life of the instrument. It implements an extensive suite of task primitives that can be assembled into reduction recipes to produce calibrated datasets ready for scientific analysis. Angular, spectral, and polarimetric differential imaging are supported. Graphical tools automate the production and editing of recipes, an integrated calibration database manages reference files, and an interactive data viewer customized for high contrast imaging allows for exploration and manipulation of data.
A new polarimeter has been built for the “Observatoire du Mont-Mégantic” (POMM) and is now in commissioning
phase. It will allow polarization measurements with a precision of 10-6, an improvement by a factor of 100 over the
previous observatory polarimeter. The characteristics of the instrument that allow this goal are briefly discussed and the
planned science observations are presented. They include exoplanets near their host star (hot Jupiters), transiting
exoplanets, stars with debris disks, young stars with proto-planetary disks, brown dwarfs, massive Wolf-Rayet stars and
comets. The details of the optical and mechanical designs are presented in two other papers.
SPIRou is a near-infrared, echelle spectropolarimeter/velocimeter under design for the 3.6m Canada-France-
Hawaii Telescope (CFHT) on Mauna Kea, Hawaii. The unique scientific capabilities and technical design features
are described in the accompanying papers at this conference. In this paper we focus on the data reduction software
(DRS) and the data simulation tool. The SPIRou DRS builds upon the experience of the existing SOPHIE,
HARPS and ESPADONS spectrographs; class-leaders instruments for high-precision RV measurements and
spectropolarimetry. While SPIRou shares many characteristics with these instruments, moving to the near-
infrared domain brings specific data-processing challenges: the presence of a large number of telluric absorption
lines, strong emission sky lines, thermal background, science arrays with poorer cosmetics, etc. In order for the
DRS to be fully functional for SPIRou's first light in 2015, we developed a data simulation tool that incorporates
numerous instrumental and observational e_ects. We present an overview of the DRS and the simulation tool
architectures.
The Aperture Masked Interferometry (AMI) mode on JWST-NIRISS is implemented as a 7-hole, 15% throughput, non-redundant mask (NRM) that operates with 5-8% bandwidth filters at 3.8, 4.3, and 4.8 microns. We present refined estimates of AMI's expected point-source contrast, using realizations of noise matched to JWST pointing requirements, NIRISS detector noise, and Rev-V JWST wavefront error models for the telescope and instrument. We describe our point-source binary data reduction algorithm, which we use as a standardized method to compare different observational strategies. For a 7.5 magnitude star we report a 10-a detection at between
8.7 and 9.2 magnitudes of contrast between 100 mas to 400 mas respectively, using closure phases and squared visibilities in the absence of bad pixels, but with various other noise sources. With 3% of the pixels unusable, the expected contrast drops by about 0.5 magnitudes. AMI should be able to reach targets as bright as M=5. There will be significant overlap between Gemini-GPI and ESO-SPHERE targets and AMI's search space, and a complementarity with NIRCam's coronagraph. We also illustrate synthesis imaging with AMI, demonstrating an imaging dynamic range of 25 at 100 mas scales. We tailor existing radio interferometric methods to retrieve a faint bar across a bright nucleus, and explain the similarities to synthesis imaging at radio wavelengths. Modest contrast observations of dusty accretion flows around AGNs will be feasible for NIRISS AMI. We show our early results of image-plane deconvolution as well. Finally, we report progress on an NRM-inspired approach to mitigate mission-level risk associated with JWST's specialized wavefront sensing hardware. By combining narrow band and medium band Nyquist-sampled images taken with a science camera we can sense JWST primary mirror segment tip-tilt to lOmas, and piston to a few nm. We can sense inter-segment piston errors of up to 5 coherence lengths of the broadest bandpass filter used ( 250-500 0m depending on the filters). Our approach scales well with an increasing number of segments, which makes it relevant for future segmented-primary space missions.
The Fine Guidance Sensor (FGS) is one of the four science instruments on board the James Webb Space Telescope (JWST). FGS features two modules: an infrared camera dedicated to fine guiding of the observatory and a science camera module, the Near-Infrared Imager and Slitless Spectrograph (NIRISS) covering the wavelength range between 0.7 and 5.0 μm with a field of view of 2.2' X 2.2'. NIRISS has four observing modes: 1) broadband imaging featuring seven of the eight NIRCam broadband filters, 2) wide-field slitless spectroscopy at a resolving power of rv150 between 1 and 2.5 μm, 3) single-object cross-dispersed slitless spectroscopy enabling simultaneous wavelength coverage between 0. 7 and 2.5 μm at Rrv660, a mode optimized for transit spectroscopy of relatively
bright (J > 7) stars and, 4) sparse aperture interferometric imaging between 3.8 and 4.8 μm enabling high
contrast ("' 10-4) imaging of M < 8 point sources at angular separations between 70 and 500 milliarcsec. This
paper presents an overview of the FGS/NIRISS design with a focus on the scientific capabilities and performance offered by NIRISS.
Direct imaging and spectroscopy can advance our understanding of planet formation and migration through
the detection and characterization of extrasolar planets on wide orbits. Accurate photometry and astrometry of
detected companions are of crucial importance to derive the planet physical properties.We present an extension of
the Locally optimized combination of images (LOCI) method to measure the highest-fidelity photometry as well
as accurate astrometry of detected companions. This algorithm is also generalized to Integral-Field Spectrograph
(IFS) data processing, giving advantages of a simultaneous angular and spectral differential imaging reduction,
retrieving high-fidelity spectra from PSF-subtracted cubes.
KEYWORDS: James Webb Space Telescope, Stars, Space telescopes, Visibility, Sensors, Planets, Telescopes, Calibration, Point spread functions, Wavefronts
Non-redundant masking (NRM) is a high contrast high resolution technique that is relevant for future space
missions dedicated to either general astrophysics or extrasolar planetary astronomy. On the ground NRM
has opened a rich target space between 0.5 to 4 resolution elements from bright stars. It enabled moderate
contrast very high angular resolution observations that have provided dynamical masses for targets beyond the
resolution of the Hubble Space Telescope. Such observations challenge the best models of ultra-cool dwarf stars'
atmospheres and interiors. The technique succeeds because it sidesteps the effects of speckle noise that plagues
direct imaging at moderate Strehl ratios. On a space telescope NRM mitigates instrument-induced speckle
noise, thus enabling high contrast even when images are barely diffraction-limited. The non-redundant mask in
the Fine Guidance Sensor Tunable Filter Imager (FGS-TFI) on the James Webb Space Telescope (JWST) will
open up a search space between 50 and 400 mas at wavelengths longer than 3.8μm. We present simulations that
estimate achievable contrast on JWST, and report preliminary results of a testbed experiment using a mask with
the same geometry as JWST's. We expect contrast of the order of 104 will be achievable in a 10 ks exposure
of an M = 7 star, with observing, target acquisition, and data calibration methods common to the three other
imaging instruments on board JWST. As an example of the potential science possible with NRM, we show that
if a planet were responsible for clearing the inner 5 AU of the disk around HR8799, it would likely be detectable
using JWST FGS-TFI's NRM at 4.6 microns. Stars as bright as M = 3 will also be observable with JWST's
NRM, meshing well with next-generation ground-based extreme adaptive optics coronagraphs. JWST NRM's
parameter space is inaccessible to both JWST coronagraphs and future 30-m class ground-based telescopes,
especially in the mid-IR.
The Fine Guidance Sensor (FGS) of the James Webb Space Telescope (JWST) features a tunable filter imager (TFI)
module covering the wavelength range from 1.5 to 5.0 μm at a resolving power of ~100 over a field of view of
2.2'×2.2'. TFI also features a set of occulting spots and a non-redundant mask for high-contrast imaging. This paper
presents the current status of the TFI development. The instrument is currently under its final integration and test phase.
We present the results of the design studies of the science calibration system for the adaptive optics and infrared
instruments of the Thirty Meter Telescope. The two major requirements of the science calibration system are to provide
pupil-simulated telescope beams to the adaptive optics system for calibration of the telescope pupil and to provide flatfielding
and wavelength-calibration illuminations to client instruments of the adaptive optics system. Our current system
is composed an integrating sphere with calibration light sources, a retractable pupil-mask system, a lens assembly
consisting of a pair of achromatic triplets, and fold mirrors. This system appears to be capable of producing highlyuniform
of f/15 beams at the telescope focal plane and pupil simulation at a pupil location within the adaptive optics
system. We describe the present design and development of the calibration system along with relevant analyses.
The Gemini Planet Imager (GPI) high-contrast adaptive optics system, which is currently under construction
for Gemini South, has an IFS as its science instrument. This paper describes the data reduction pipeline of the
GPI science instrument. Written in IDL, with a modular architecture, this pipeline reduces an ensemble of highcontrast
spectroscopic or polarimetric raw science images and calibration data into a final dataset ready for
scientific analysis. It includes speckle suppression techniques such as angular and spectral differential imaging
that are necessary to achieve extreme contrast performances for which the instrument is designed. This paper
presents also raw GPI IFS simulated data developed to test the pipeline.
KEYWORDS: Point spread functions, Coronagraphy, Halftones, Imaging systems, Prototyping, Signal attenuation, James Webb Space Telescope, Sensors, Mirrors, Solids
The JWST Fine Guidance Sensor (FGS) Tunable Filter Imager (TFI) will feature a coronagraph for high contrast
imaging applications. TFI will provide unique narrow-band imaging and coronagraphic capabilities impacting the
detection of "First Light", i.e. stellar systems formed just after the Big Bang, and the detection and characterization of
exoplanets. The TFI coronagraph is made of a set of four occulting spots and four Lyot stops. The TFI focal-plane masks
under consideration are apodized (Gaussian profile) or hard masks. The masks are operating in reflection and
implemented as small cones directly engraved on the pick-off mirror located at the telescope focus. This paper presents
laboratory performance of two prototype masks. The hard mask results are in good agreement with the expected
performance of a standard Lyot coronagraph. On the other hand, the halftone mask shows significant departure from
theoretical expectation; these results could be due to diffraction effects within the halftone mask.
Direct exoplanet detections are limited by the speckle noise of the point spread function (PSF). This noise can
be reduced by subtracting PSF images obtained simultaneously in adjacent narrow spectral bands using a multichannel
camera (MCC). Experiments have shown that speckle attenuation performances are severely degraded
by differential optical aberrations between channels that decorrelate the PSFs of the different spectral bands.
We present a new technique which can greatly alleviate this problem: the introduction of a holographic diffuser
at the focal plane of the MCC. The holographic diffuser converts the PSF image into an incoherent illumination
scene that is then re-imaged with the MCC. This imaging process is equivalent to a convolution of the scene
with the PSF of each channel of the MCC. The optical aberrations in the MCC then affect only the convolution
kernel of each channel and not the PSF globally, resulting in more correlated images. We report laboratory
measurements with a dual channel prototype (1.575 μm and 1.625 μm) to validate this approach. We achieved
a speckle noise suppression factor of 12-14, which is ~4-6 times better than what has been achieved by existing
MCCs.
Quasi-static speckles are the main source of noise preventing the direct detection of exoplanets around bright stars. We
are investigating the use of an infrared (1.5-2.4 μm) integral field spectrograph (IFS) specialised for speckle suppression
and the detection of self-luminous giant planets. This paper presents the optical design and laboratory results obtained
with a TIGER-type IFS prototype based on a microlens array. A similar IFS will be used for the Gemini Planet Imager
(GPI). Preliminary speckle-suppression performances of the IFS along with simulations are presented.
We present an overview of the OSIRIS integral field spectrograph which was recently commissioned on the Keck II Telescope. OSIRIS works with the Keck Adaptive Optics system and utilizes an infrared transmissive lenslet array to sample a rectangular field of view at close to the Keck diffraction limit. By packing the spectra close together (2 pixel rows per spectrum) and using the Rockwell Hawaii-2 detector (wavelengths between 1 and 2.5 microns), we achieve a relatively large field of view (up to 6."4) while maintaining full broad-band spectral coverage at a resolution of 3800. Among the challenges of the instrument are: a fully cryogenic design (approximately 250 kg are brought down to 55K); four spatial scales from 0."02 to 0."10; extremely low wavefront error (approximately 25 nm of non-common path error); large all aluminum optics for the spectrograph; extremely repeatable spectral formats; and a sophisticated data reduction pipeline. OSIRIS also serves as a starting point for our design of IRIS which is a planned integral field spectrograph for the Thirty Meter Telescope.
The Fine Guider Sensor (FGS) of the James Webb Space Telescope (JWST) features two tunable filter (R~100) modules covering the 1.2-2.4 μm and 2.4-4.8 μm wavelength ranges, respectively. A set of occulting spots/bars mounted on a small slide located at the edge of the 2.3’x 2.3’ field of view (FOV) along with apodizing masks located in the filter wheel of each channel enable coronagraphic operation. Each coronagraphic field covers a square FOV of 20”x20”. The FGS-TF coronagraph complements the coronagraphic capabilities implemented in NIRCam and MIRI. This paper presents numerical simulations to predict the high-contrast imaging performance of the FGS-TF coronagraph. The combined coronagraphic and differential spectral imaging capabilities of the FGS-TF constitute a powerful tool for detecting and characterizing exoplanets with JWST.
Direct exoplanet detections are currently limited by speckle noise arising from residual atmospheric wavefront errors and optical aberrations. Simultaneous spectral differential imaging (SSDI) is a high contrast imaging technique that aims at reducing this noise by the subtraction of images obtained simultaneously in adjacent narrow spectral bands. SSDI performances are severely degraded by differential optical aberrations between channels. We discuss two novel approaches to implement SSDI in which there are no differential aberrations. The first uses a microlens array at the focal plane to sample the point spread function (PSF) and micro-filters on the backside of each microlens to separate colors. The micropupils are immediately imaged on the detector. The second preserves the microlens array at the focal plane but re-images the array of micropupils through a beam-splitter on the detector. In both concepts the PSF measurement is made at the microlens array, so all optics is common prior to the PSF measurement in all colors. A simple prototype was used to test the concepts; preliminary results yield noise attenuation of ~10-2.
OSIRIS is a near infrared diffraction limited imaging field spectrograph under development for the Keck observatory adaptive optics system and scheduled for commissioning in fall 2004. Based upon lenslet pupil imaging, diffraction grating, and a 2Kx2K Hawaii2 HgCdTe array, OSIRIS is a highly efficient instrument at the forefront of today's technology. OSIRIS will deliver per readout up to 4096 diffraction limited spectra in a complex interleaved format, requiring new challenges to be met regarding user interaction and data reduction. A data reduction software package is under development, aiming to provide the observer with a facility instrument allowing him to concentrate on science rather than dealing with instrumental as well as telescope and atmosphere related effects. Together with OSIRIS, a pipeline for basic data reduction will be provided for a new Keck instrument for the first time. A status report is presented here together with some aspects of the data reduction pipeline.
Detecting and characterizing exoplanets is one of the main science drives for extremely large telecopes. It requires a high-order (extreme) adaptive optics (ExAO) system combined with a coronagraph and a science camera optimized for efficient attenuation of point spread function (PSF) residuals induced by atmospheric speckles and high-frequency quasi-static aberrations. Spectral differential imaging is a very promising technique for attenuating PSF residuals. High-contrast imaging observations with the TRIDENT camera at the AO focus of the Canada-France-Hawaii Telescope (CFHT) have shown that companion detection using differential imaging is seriously compromised by very small amount of non-common path wave front errors between the different optical channels of the camera. Such problems can be eliminated with a new type of detector assembly: a multi-color detector assembly (MCDA). This paper describes the MCDA concept along with numerical simulations predicting the combined performance of an ExAO system with a Lyot coronagraph and an MCDA on a segmented 20m telescope.
We present the design for a recently approved instrument for the Keck Telescope. Called OSIRIS, it was inspired by the optical spectrograph TIGER of R. Bacon et al. and will utilize an infrared transmissive lenslet array to sample a rectangular field of view at close to the Keck diffraction limit. By packing the spectra very closely together (2 pixel rows per spectrum) and using the Rockwell Hawaii-2 detector (wavelengths between 1 and 2.5 microns), we will achieve a relatively large field of view (up to 6."4) while maintaining full broad-band spectral coverage at a resolution of 3900. Due to the extremely low backgrounds between night sky lines and at AO spatial samplings, the instrument will reach point source sensitivities several times fainter than any existing infrared spectrograph. We are also coupling a separate infrared AO camera dubbed SHARC to work as an acquisition camera and to monitor the point spread function's behavior during long spectroscopic exposures. Among the challenges of the instrument are: a fully cryogenic design, four spatial resolutions from 0."02 to 0."10, large aluminum optics for the spectrography, extremely repeatable spectral formats and a sophisticated data reduction pipeline.
OSIRIS (OH-Suppressing InfraRed Integral-field Spectrograph) is a new facility instrument for the Keck Observatory. Starting in 2004, it will provide the capability of performing three-dimensional spectroscopy in the near-infrared z, J, H, and K bands at the resolution limit of the Keck II telescope, which is equipped with adaptive optics and a laser guide star. The innovative capabilities of OSIRIS will enable many new observing projects. Galaxies in the
early Universe will be among the most interesting targets for OSIRIS, which will perform detailed studies of their stellar content and dynamical properties. In more exotic objects, such as quasars, radio galaxies, and more nearby active galactic nuclei, OSIRIS can elucidate the relation of the central black hole to the properties of the host galaxy, and the mechanism by which gas
is fed into the central engine. In the center of our own Galaxy, it will be possible to search for signatures of interaction between the massive black hole and stars in its immediate vicinity. Closer to home, OSIRIS will perform spectroscopic observations of young stars and their environment, and of brown dwarfs. Imaging spectroscopy of the giant planets, their moons, and asteroids will shed new light on meteorology, mineralogy, and volcanism in the Solar System. OSIRIS observations of Kuiper Belt objects will provide sufficient sensitivity to establish their surface composition, which will contribute substantially to our understanding of the history of the Solar System.
OSIRIS is a near infrared diffraction limited imaging field spectrometer under development for the Keck observatory adaptive optics system. Based upon lenslet pupil imaging, diffraction grating, and a 2K×2K Hawaii2 HgCdTe array, OSIRIS is a highly efficient instrument at the forefront of today’s technology. OSIRIS will deliver per readout up to 4096 diffraction limited spectra in a complex interleaved format, requiring new challenges to be met regarding user interaction and data reduction. A data reduction software package is under development, aiming to provide the observer with a facility instrument allowing him to concentrate on science rather than dealing with instrumental as well as telescope and atmosphere related effects. Together with OSIRIS, a pipeline for basic data reduction will be provided for a new Keck instrument for the first time. Some aspects of the data reduction pipeline will be presented here. The OSIRIS instrument as such, the astronomical background as well as other software tools were presented elsewhere on this conference.
OSIRIS is an infrared integral-field spectrograph being built for the Keck AO system. OSIRIS presents novel data reduction and user-interaction challenges which are addressed by software being developed for OSIRIS. The complex raw data frames, containing up to 4096 interleaved spectra, are reduced in real-time and meaningfully displayed for quality-of-observation feedback to observers. Following an observing night, data are optimally reduced to science-quality data cubes in a semi-automated fashion. Further, the software must efficiently coordinate OSIRIS' spectroscopic observations with the SHARC off-axis imager and the AO system.
To meet these demands, OSIRIS software is comprehensive and integrates the planning, execution, and reduction of observations. Facilitating this architecture is the formulation of observations into 'datasets', rather than into individual frames. Datasets are functional groups of frames organized by the needs and capabilities of the data reduction software (DRS). A typical dataset consists of dithered OSIRIS observations, coupled with associated off-axis AO PSF imagery from SHARC. A Java-based planning tool enables 'sequences' of datasets to be planned and saved both prior to and during observing sessions. An execution client interprets these XML-based files, and configures the hardware servers for OSIRIS, SHARC, and AO before executing the observations. As observations are completed, extensive information
about the instrument and observatory are collated in an archival relational database. The DRS then uses information in the database, as well as archived calibration data and SHARC PSF data to produce a final science-quality data product, which may include differential refraction corrections, 3D PSF modeling/deconvolution, and OH-suppression.
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