The Cosmic Origins Spectrograph (COS) was installed on the Hubble Space Telescope (HST) in 2009. The majority of science spectra are taken with the Far Ultraviolet (FUV) channel, which uses a cross delay line detector. This detector is subject to gain sag, which causes its sensitivity to decrease at locations where counts have fallen. Increasing the high voltage can be used to compensate for this effect, but when the voltage limit is reached, the spectra are moved to a different Lifetime Position (LP) by offsetting them in the cross-dispersion direction on the two-dimensional detector. However, since the optical design was optimized for the initial spectral position, other LPs show a change in the shape of the point spread function, with distortions that lead to a loss of resolution.
In anticipation of a move to a seventh lifetime position (LP7) in ~2025, we have conducted exploratory work to model the instrument performance over the full range of possible positions for the spectra on the detector. This effort includes (1) optical modeling of the spectrograph; (2) creating simulated science spectra and evaluating the resolving power and other spectral properties at a range of positions; (3) evaluating the detector properties at potential lifetime positions while considering mechanical limitations of the hardware; and (4) reserving sufficient space for later LPs. We have used this information to formulate preliminary plans for moving to the next position, which includes identifying which observing modes should be adjusted, and providing our initial thoughts on future Lifetime Positions.
Spectral Point Spread Function, or in other words Line Spread Function (LSF), quantifies a spectrograph’s response to a monochromatic light source. Accurate knowledge of the LSF is needed to measure the velocity dispersion of the stars or gas from the spectra of galaxies, when these quantities are comparable or smaller than the width of the LSF. The LSF information is also crucial to subtract background sky emission in near-infrared integral field spectroscopic (IFS) instruments from ground-based telescopes. Accurate models of LSF cannot be obtained from the spectrograph data itself due to their coarse sampling to provide a wide instantaneous wavelength coverage. In the case of IFS instruments, the LSF can assume complex shapes and these shapes can change dependent on the location on the IFS field-of-view. In this manuscript, we derive accurate LSF models in the H-band grating of the SINFONI spectrograph, a near-infrared IFS on board the Very Large Telescope in Chile, using a dedicated calibration programme. We model the LSF profiles using Gauss-Hermite polynomials and we use the parameters from these models to predict the shape of the LSF profile at any location on the detector. We also demonstrate that the LSF can be derived from the curvature in the arc-lamp frames. Finally, we derive the LSF of the upcoming ELT/HARMONI spectrograph using the slit-curvature method for different resolutions and grating set-ups
The Multi-Unit Spectroscopic Explorer instrument (MUSE), is an integral-field spectrograph at one of the Nasmyth foci of the 8m-class Yepun telescope at Paranal observatory. MUSE's most powerful modes use the Adaptive Optics Facility consisting of a Deformable Secondary Mirror with over 1000 actuators commanded by a real-time computer up to 1000 times per second. At the core of the system are 4 laser guide stars monitored by GALACSI, the wave-front sensor system. MUSE functions with two modes: Wide-Field Mode (1'x1' field), making use of Ground Layer Adaptive Optics and Narrow-Field Mode (7.5"x7.5" field) using full laser tomography. In this work, we will present the results of a campaign to monitor the AO performance as measured by MUSE during the first years of operations. We will evaluate the dependence of this performance, as characterized by the point-spread function, on easily monitored environmental parameters such as ground-layer fraction, coherence time, seeing, and airmass.
HARMONI is the first light visible and near-infrared (450 - 2450 nm,λ/Δλ = 3500 - 18000) integral field spectrograph (IFS) for the European Southern Observatory's Extremely Large Telescope (ELT). Spectroscopic observations from ground-based telescopes in these wavelengths are contaminated by emission from molecules in the Earth's atmosphere, called skylines. Conventional means of removing these skylines requires spending up to half of the telescope time on observing blank sky exposures. Observations with IFS can circumvent this inefficiency by making use of sky models from science exposure themselves to remove the background, called on- IFU sky-subtraction. However, this has not been achieved in practice as it requires an accurate knowledge on the Line Spread Function (LSF) of the spectrograph. The information on the LSF is also useful in telluric calibration of science observations, especially in case of telluric standards that underfill the slits. In this manuscript, we present a tunable Fabry-perot design which will be used to characterise the LSF of HARMONI. The Fabry- perot etalon will operate over HARMONI's entire wavelength range and spectral resolving powers. The design presented in this manuscript has the potential to be adapted for any spectroscopic instrument in the future, and fundamentally change the way we have been observing with IFS instruments.
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.