Giovanna Giardino, Nora Luetzgendorf, Pierre Ferruit, Bernhard Dorner, Catarina Alves de Oliveira, Stephan Birkmann, Torsten Boeker, Tim Rawle, Marco Sirianni
The NIRSpec instrument of JWST can be operated in multi-object (MOS), long-slit, and integral field mode with spectral resolutions from 100 to 2700. Its MOS mode uses about a quarter of a million individually addressable mini-slits for object selection, covering a field of view of 9 square-arcminute. We have developed a procedure to optimize a parametric model of the instrument that provides the basis for the extraction of wavelength calibrated spectra from NIRSpec data, from any of the apertures and for all the modes. Here, we summarize the steps undertaken to optimize the instrument model parameters using the data acquired during the latest cryo-vacuum campaign of the JWST Integrated Science Instrument Module, recently carried out at NASA Goddard Space Flight Center. The calibrated parametric model is able to reproduce the spatial and spectral position of the input spectra with an intrinsic accuracy (1-sigma, RMS) ~ 1/10 of a pixel in spatial and spectral direction for all the modes. The overall wavelength calibration accuracy (RMS) of the model as measured on the extracted spectra is better than 1/20 of a resolution element for all of the grating-based spectral modes and at the level of 1/14 of a resolution element for the prism. These results are well within the allocations for the model in the overall spatial and spectral calibration budget of NIRSpec.
KEYWORDS: Space telescopes, James Webb Space Telescope, Aerospace engineering, Camera shutters, Sensors, Staring arrays, Electroluminescent displays, Acoustics, Instrument modeling, Spectroscopy
The Near-Infrared Spectrograph (NIRSpec) is one of the four instruments on the James Webb Space Telescope (JWST) which is scheduled for launch in 2018. NIRSpec is developed by the European Space Agency (ESA) with Airbus Defense and Space Germany as prime contractor. The instrument offers seven dispersers covering the wavelength range from 0.6 to 5.3 micron with resolutions from R ∼ 100 to R ∼ 2700. NIRSpec will be capable of obtaining spectra for more than 100 objects simultaneously using an array of micro-shutters. It also features an integral field unit with 3” x 3” field of view and a range of slits for high contrast spectroscopy of individual objects and time series observations of e.g. transiting exoplanets. NIRSpec is in its final flight configuration and underwent cryogenic performance testing at the Goddard Space Flight Center in Winter 2015/16 as part of the Integrated Science Instrument Module (ISIM). We present the current status of the instrument and also provide an update on NIRSpec performances based on results from the ISIM level test campaign.
Stephan Birkmann, Pierre Ferruit, Catarina Alves de Oliveira, Torsten Böker, Guido De Marchi, Giovanna Giardino, Marco Sirianni, Martin Stuhlinger, Peter Jensen, Peter Rumler, Massimo Falcolini, Maurice B. te Plate, Giovanni Cresci, Bernhard Dorner, Ralf Ehrenwinkler, Xavier Gnata, Thomas Wettemann
KEYWORDS: James Webb Space Telescope, Calibration, Mirrors, Sensors, Staring arrays, Aerospace engineering, Space telescopes, Camera shutters, Near infrared, Computer aided design
The Near-Infrared Spectrograph (NIRSpec) is one of the four instruments on the James Webb Space Telescope (JWST), scheduled for launch in 2018. NIRSpec has been designed and built by the European Space Agency (ESA) with Airbus Defense and Space Germany as prime contractor. The instrument covers the wavelength range from 0.6 to 5.3 micron and will be able to obtain spectra of more than 100 astronomical objects simultaneously by means of a configurable array of micro-shutters. It also features an integral field unit and a suite of slits for high contrast spectroscopy of individual objects. The extensive ground calibration campaign of NIRSpec was completed in Summer 2013, after which it was delivered to NASA for integration into the Integrated Science Instrument Module (ISIM). We highlight the major results from the instrument level calibration campaign which demonstrated full compliance with all opto-mechanical performance requirements. In addition, we present the current status of the instrument, describe the ongoing preparations for the Integrated Science Instrument Module (ISIM) test campaign to begin in June 2014, and briefly discuss plans for the pending exchange of the detector and micro-shutter assemblies following the first ISIM test cycle.
KEYWORDS: Stars, Spectral resolution, Sensors, Signal to noise ratio, Spectroscopy, Exoplanets, Interference (communication), James Webb Space Telescope, Spectroscopes, Electrons
Recent publications resulting from observations conducted with the Hubble Space Telescope (HST) have highlighted the diagnostic power of near-infrared spectroscopy for the study of the atmospheric properties of transiting exoplanets. In this context, the James Webb Space Telescope (JWST) and it suite of instruments will have an unprecedented combination of sensitivity and spectral coverage. In this article, we focus on one of these instruments, the near-infrared spectrograph NIRSpec. NIRSpec will offer an aperture spectroscopy mode dedicated to the characterization of transiting exoplanets. It will cover the 0.6-5.3 μm spectral domain with 3 ranges of spectral resolution (R 100, 1000 and 2700). The predicted noise floor (photon noise and detector noise only, no systematics included) is lower than 100 ppm for a single 1-hour in-transit observation of an 7th magnitude star, indicating that transit spectroscopy programs with NIRSpec will routinely have photon-noise limited noise floors of a few tens of ppm. In terms of brightness limits, at high spectral resolution, NIRSpec will be able to observe planets transiting stars with J-band magnitudes up to 6.5 in the worst case and 4.5 in the best case.
PANIC is the new PAnoramic Near-Infrared camera for Calar Alto, a joint project by the MPIA in Heidelberg, Germany,
and the IAA in Granada, Spain. It can be operated at the 2.2m or 3.5m CAHA telescopes to observe a field of view of
30'x30' or 15'x15' respectively, with a sampling of 4096x4096 pixels. It is designed for the spectral bands from Z to K,
and can be equipped with additional narrow-band filters.
The instrument is close to completion and will be delivered to the observatory in Spain in fall 2014. It is currently in the
last stage of assembly, where the optical elements are being aligned, which will be followed by final laboratory tests of
the instrument. This paper contains an update of the recent progress and shows results from the optical alignment and
detector performance tests.
Stephan Birkmann, Pierre Ferruit, Torsten Böker, Guido De Marchi, Giovanna Giardino, Marco Sirianni, Martin Stuhlinger, Peter Jensen, Maurice B. J. te Plate, Peter Rumler, Bernhard Dorner, Xavier Gnata, Thomas Wettemann
KEYWORDS: Calibration, James Webb Space Telescope, Spectrographs, Spectral calibration, Camera shutters, Near infrared, Electroluminescent displays, Spectroscopes, Cryogenics, Mirrors
The Near Infrared Spectrograph (NIRSpec) is one of four science instruments aboard the James Webb Space
Telescope (JWST) scheduled for launch in 2018. NIRSpec is sensitive in the wavelength range from ~0.6 to 5.0
micron and will be capable of obtaining spectra from more than a 100 objects simultaneously by means of a
programmable micro shutter array. It will also provide an integral eld unit for 3D spectroscopy and xed slits
for high contrast spectroscopy of individual sources and planet transit observations. We present results obtained
during the rst cryogenic instrument testing in early 2011, demonstrating the excellent optical performance of
the instrument. We also describe the planning of NIRSpecs forthcoming second calibration campaign scheduled
for early 2013.
Pierre Ferruit, Giorgio Bagnasco, Reiner Barho, Stephan Birkmann, Torsten Böker, Guido De Marchi, Bernhard Dorner, Ralf Ehrenwinkler, Massimo Falcolini, Giovanna Giardino, Xavier Gnata, Karl Honnen, Peter Jakobsen, Peter Jensen, Manfred Kolm, Hans-Ulrich Maier, Ralf Maurer, Markus Melf, Peter Mosner, Peter Rumler, Jean-Christophe Salvignol, Marco Sirianni, Paolo Strada, Maurice te Plate, Thomas Wettemann
The Near-Infrared Spectrograph NIRSpec is one of the four instruments of the James Webb Space Telescope (JWST).
NIRSpec will cover the 0.6-5.0 micron range and will be capable of obtaining spectra of more than 100 objects
simultaneously in its multi-object spectroscopy (MOS) mode. It also features a set of slits and an aperture for high
contrast spectroscopy of individual sources, as well as an integral-field unit (IFU) for 3D spectroscopy. We will first
show how these capabilities are linked to the four main JWST scientific themes. We will then give an overview of the
NIRpec modes and spectral configurations with an emphasis on the layout of the field of view and of the spectra. Last,
we will provide an update on the status of the instrument.
Stephan Birkmann, Torsten Böker, Pierre Ferruit, Giovanna Giardino, Peter Jakobsen, Guido de Marchi, Marco Sirianni, Maurice te Plate, Jean-Christophe Savignol, Xavier Gnata, Thomas Wettemann, Bernhard Dorner, Giovanni Cresci, Fabiàn Rosales-Ortega, Martin Stuhlinger, Richard Cole, Jason Tandy, Chris Brockley-Blatt
KEYWORDS: Calibration, Argon, James Webb Space Telescope, Lamps, Instrument modeling, Spectrographs, Data modeling, Space telescopes, Optical filters, Cryogenics
The Near Infrared Spectrograph (NIRSpec) is one of four science instruments aboard the James Webb Space
Telescope (JWST) that is to be launched later this decade. NIRSpec is sensitive in the wavelength range from 0.6
to 5.0 μm and operates at temperatures ≤ 40 K. It offers multi-object, fixed slit, and integral field spectroscopy
with seven selectable dispersers. The on-ground spectrophotometric calibration of the instrument is performed
by means of continuum and line emission lamps. NIRSpec also contains an internal calibration assembly (CAA)
that will provide the wavelength and radiometric calibration in orbit. Due to thermal constraints, the CAA
features low power tungsten filament lamps in combination with long-pass and Fabry-Perot-like interference
filters, which need to be calibrated at instrument level. We will report on the wavelength calibration of the
NIRSpec flight model and the CAA, carried out during the first cryogenic performance testing.
Guido De Marchi, Maurice B. te Plate, Stephan Birkmann, Torsten Böker, Pierre Ferruit, Giovanna Giardino, Peter Jakobsen, Marco Sirianni, Jean-Christophe Savignol, Xavier Gnata, Reiner Barho, Michel Kosse, Peter Mosner, Bernhard Dorner, Giovanni Cresci, Fabian Rosales-Ortega, Martin Stuhlinger, Torsten Gross, Thomas Leikert
The Near Infrared Spectrograph (NIRSpec) is one of four science instruments on board the James Webb Space
Telescope (JWST). NIRSpec offers multi-object, fixed slit, and integral field spectroscopy. There are eight optical
elements mounted on the grating wheel assembly (GWA), six gratings, a double-pass prism, and a mirror. The precise
knowledge of the position and tilt of these elements is critical for target acquisition and an accurate extraction and
calibration of science data. We present the concept of calibrating the position/tilt sensors during the NIRSpec flight
model ground calibration campaign, the performance of the sensors and first results concerning the GWA repeatability.
KEYWORDS: Phase retrieval, Wavefronts, Sensors, James Webb Space Telescope, Wavefront sensors, Cryogenics, Monochromatic aberrations, Monte Carlo methods, Data modeling, Error analysis
Phase retrieval results are presented for the James Webb Space Telescope (JWST) Near InfraRed Spectrograph
(NIRSpec) demonstration model (DM). NIRSpec is one of five science instruments (SIs) comprising the Integrated
Science Instrument Module (ISIM); the NIRSpec is being built for the European Space Agency by a consortium led
by EADS Astrium GmbH. During this initial DM test campaign, focal-sweep images were collected over the
science field of view (FOV) for determining best focus at both ambient and cryogenic (cryo) temperature
environments, and these images were then used as input to the Hybrid Diversity Algorithm (HDA) for phase
retrieval, using Variable Sampling Mapping (VSM). Wavefront estimates from phase retrieval, an error budget, and
diagnostics used to assess phase retrieval stability and convergence are discussed. The ambient phase retrieval
results were compared against wavefront measurements taken with a Shack-Hartmann wavefront sensor.
The Near Infrared Spectrograph (NIRSpec) is one of the four science instruments aboard the James Webb Space
Telescope (JWST) scheduled for launch in 2014. NIRSpec is sensitive in the wavelength range from ~ 0.6 to
5.0 μm and will be capable of obtaining spectra of more than a 100 objects simultaneously, as well as fixed slit
high contrast spectroscopy of individual sources. It also features an integral field unit for 3D spectroscopy. The
key scientific objectives of the instrument include studies of star formation and chemical abundances of young
distant galaxies and tracing the creation of the chemical elements back in time. In this paper, we present the
status of the NIRSpec instrument as it is currently being prepared for its extensive ground calibration campaign
later in 2010.
KEYWORDS: Photons, Sensors, Point spread functions, Diffraction, Device simulation, Calibration, Instrument modeling, Data modeling, Signal attenuation, James Webb Space Telescope
The James Webb Space Telescope (JWST) is the successor mission to the Hubble Space Telescope and will
operate in the near- and mid-infrared wavelength ranges. One of the four science instruments on board the
spacecraft is the multi-object spectrograph NIRSpec, currently developed by the European Space Agency (ESA)
with EADS Astrium Germany GmbH as the prime contractor. NIRSpec will be able to measure the spectra of
more than 100 objects simultaneously and will cover the near infrared wavelength range from 0.6 to 5.0 μm at
various spectral resolutions. To verify the performance of NIRSpec and simulate future on-ground and in-orbit
observations with this instrument, the Instrument Performance Simulator (IPS) software is developed at Centre
de Recherche Astrophysique de Lyon (CRAL) as subcontractor to Astrium.
In early and mid-2009, the NIRSpec Demonstration Model (DM), fully representative up to the slit plane,
underwent cryogenic tests and calibration runs. The detector was placed at the slit plane in case of the DM to
measure specific optical performance aspects. A simplified version of the IPS was prepared, matching the DM
configuration and also serving as a testbed for the final software for the flight model. In this paper, we first
present the simulation approach used in the IPS, followed by results of the DM calibration campaign. Then, for
the first time, simulation outputs are confronted with measured data to verify their validity.
NIRSpec is the near-infrared multi-object spectrograph for the future James Webb Space Telescope (JWST). It is
developed by EADS Astrium for the European Space Agency. The Centre de Recherche Astrophysique de Lyon (CRAL)
has developed the Instrument Performance Simulator (IPS) software that is being used for the modeling of NIRSpec's
performances and to simulate raw NIRSpec exposures. In this paper, we present the IPS software itself (main simulation
modules and user's interface) and discuss its intrinsic accuracy. We also show the results of simulations of calibration
exposures as they will be obtained during the NIRSpec on-ground calibration campaign.
The James Webb Space Telescope (JWST) mission is a collaborative project between the National Aeronautics and
Space Administration (NASA), the European Space Agency (ESA) and the Canadian Space Agency (CSA).
JWST is considered the successor to the Hubble Space Telescope (HST) and although its design and science objectives
are quite different, JWST is expected to yield equivalently astonishing breakthroughs in infrared space science.
Due to be launched in 2013 from the French Guiana, the JWST observatory will be placed in an orbit around the anti-
Sun Earth-Sun Lagrangian point, L2, by an Ariane 5 launcher provided by ESA.
The payload on board the JWST observatory consists of four main scientific instruments: a near-infrared camera
(NIRCam), a mid-infrared camera/spectrograph (MIRI), a near-infrared tunable filter (TFI) and a near-infrared
spectrograph (NIRSpec). The instrument suite is completed by a Fine Guidance Sensor (FGS).
NIRSpec is a multi-object spectrograph capable of measuring the spectra of about 100 objects simultaneously at low
(R~100), medium (R~1000) and high (R~2700) resolutions over the wavelength range between 0.6 micron and 5.0
micron. It features also a classical fix-slits spectroscopy mode as well as a 3D-spectrography mode with spectral
resolutions up to 2700.
The availability of extensive and accurate calibration data of the NIRSpec instrument is a key element to ensure that the
nominal performance of the instrument will be achieved and that high-quality processed data will be made available to
the users. In this context, an on-ground calibration is planned at instrument level that will supplement the later in-flight
calibration campaign.
In this article we describe the overall on-ground instrument calibration campaigns and we provide an overview of the
main features and performances of the individual elements of the sophisticated cryogenic optical ground support
equipment (OGSE) used to calibrate NIRSpec.
The James Webb Space Telescope (JWST) Observatory is the successor mission to the Hubble Space Telescope and will
lead to great scientific advancements in near- and mid-infrared astronomy. One of the four science instruments on board
the spacecraft is NIRSpec, which is being developed by the European Space Agency (ESA) with EADS Astrium
Germany GmbH as the prime contractor. This multi-object spectrograph will be able to measure the spectra of at least
100 objects simultaneously in the near infrared wavelength range from 0.6µm to 5.0µm and at various spectral
resolutions.
In order to assess the performance of the instrument, a simulator has been developed to calculate key characteristics of
the optical design and the final instrument output. It uses Fourier Optics with wavefront error maps to predict the point
spread function on the Micro Shutter Assembly (MSA) and the detector and can include real, as measured, spectral data
of filters and dispersive elements. With the implementation of parameterized image distortion and detector features, it is
possible to obtain full realistic detector frames for any optical input. Still the computation time is comparably short. The
program will be of great use to predict and verify response of NIRSpec during the test and calibration campaigns.
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