# Instruments – IFS wiki

This pagina contains a list of current, upcoming, and ex-IFSs, together with a summary of their characteristics, their advantages and disadvantages. Wij also verbinding to the muziekinstrument huis pages and data-reduction resources where available. Note: not all the instruments listed here are open to use by the entire community. Also, please feel free to add yourself to this pagina.

### VIMOS (Visual and IR Multi-Object Spectrograph)

VIMOS is a muziekinstrument located on the VLT of ESO te Pimiento. It has various modes, an IFU being one of them. The IFU array is the largest (te terms of spatial coverage) presently available on an 8-m class telescope, and has good blue sensitivity down to

4000 A. The main drawbacks of VIMOS are (i) simultaneous sky observations are not possible, so for projects requiring a good sky subtraction a work-around has to be found, (ii) order-contamination from the 2nd, -1st, -2nd and 0th order persists ter the low resolution settings (LR[B,R]), and is particularly bad at either end of the spectral range.

It has Two dedicated pipelines which produce much the same results: the ESO CPL pipeline (which can be run through the gegevens organizer GUI gasgano or ESOrex on the instruction line), and VIPGI, which works well and permits for more user interaction, but takes longer to get used to.

Our instrument-specific/gegevens reduction help pagina is here.

### FLAMES + Giraffe

ARGUS is one of the modes available on the utterly multi-function muziekinstrument FLAMES. The spectrograph to which it is coupled is called GIRAFFE. Advantages include a good size FoV and access to a good spectrograph with high resolution gratings. Spil part of the FLAMES fibre positioner, 14 fibres are available for simultaneous sky observations. Each is individually positionable anywhere within the muziekinstrument FoV, thereby permitting for a very sturdy sky subtraction. The disadvantages are that the spaxel size is relatively large compared to the FoV (meaning that the PSF may not be well sampled), and the Phase II prep is long and complicated due to the accuracy with which the sky and guide fibres have to be placed. Presently there are Trio dead fibres ter the main array.

Help pagina for making the Phase II FLD opstopping.

There are Two dedicated pipelines which produce much the same results: the ESO CPL pipeline (which can be run through the gegevens organizer GUI gasgano or ESOrex on the directive line), and girBLDRS (GIRAFFE BaseLine Gegevens Reduction Software from the Geneva group). Our instrument-specific/gegevens reduction help pagina is here.

The IFU is deployable Integral Field Unit) of GIRAFFE. For each plate there are 15 IFU units dedicated to objects and another 15 dedicated to sky measurements. Ter the latter, only the central fibre is present.

Does anyone who has used the IFU mode have something they can add here? Tips and tricks on its use and its gegevens?

Our instrument-specific/gegevens reduction help pagina is here

### SINFONI

ESO provides a well working pipeline, which spil with the other pipelines for the instruments above uses the GUI Gasgano spil the vuurlijn end for the CPL libraries, or alternatively the scriptable ESOrex programme which does the same.

It is effortless to go after using the pipeline manual spil a commencing point, but you may want to read the further details, and set specific parameters when running the pipeline, to improve the sky subtraction, and avoid strong residuals for the sky lines. The ESO pipeline is built on the Spred reduction programme developed by the SINFONI team. This programme is presently not suggested directly to the public.

Our instrument-specific/gegevens reduction help pagina can be found here

## North and South

### GMOS (Gemini Multi-Object Spectrograph)

The IFU is only one part of the multi-function muziekinstrument GMOS. It is available on both Gemini-North te Hawaii and Gemini-South ter Pimiento, and the instruments are of an identical vormgeving (the only difference being that nod & shuffle is supported at Gemini-S). The advantages of the GMOS-IFU are that it covers its FoV (which is petite, but not little) with very good spatial sampling (good enough to conveniently over-sample the PSF), is fastened to a stable, medium resolution spectrograph, and permits for simultaneous sky observations (a yam-sized time-saver). Disadvantages are that high resolution gratings are not available, and that the lenslets are hexagonal meaning resampling the gegevens ter the x-y plane is unavoidable.

Reduction is carried out fully within the Gemini IRAF package. This works, is well developed, and fairly lithe.

Our instrument-specific/gegevens reduction help pagina is here.

## North only

### NIFS (Near-IR Integral Field Spectrograph)

NIFS is available on Gemini-North te Hawaii. The disadvantage of its petite field of view is offset by a good spatial resolution and capability to be coupled to the Altair AO system. Coronographic spectroscopy can also be performed through use of an occulting mask.

Our instrument-specific/gegevens reduction help pagina is here.

### GNIRS (Gemini Near-Infrared Spectrograph)

The IFU mode for this muziekinstrument has bot discontinued. Here is an explanation of what it wasgoed:

The IFU wasgoed an extra optical system, provided for GNIRS by the University of Durham (UK). The IFU takes a cuadrilongo input field, of approximate dimensions Trio.Trio x Four.8 arcsec, and divides it into 22 slices 0.15 arcsec ter width. The IFU optics schrijfmap the slices of the cuadrilongo field onto the input plane of the spectrograph, aligning the slices more or less along the regular input slit position (the slices are offset from each other by toughly Two pixels/slice). The optics also switch the input scale to 0.12 arcsec/pixel along the slit, and 0.075 arcsec/pixel te the dispersion direction. The IFU wasgoed intended to feed the brief cameras, and therefore can be operated at a maximum resolution of

### OSIRIS

OSIRIS huis pagina at Keck. See also the OSIRIS pagina at UCLA, from which you can obtain the muziekinstrument manual and the gegevens reduction pipeline.

Does anyone have something to add here: tips and tricks on using this muziekinstrument, writing proposals/phaseIIs, or reducing the gegevens. Information that is not te manuals? Postbode here and wij will organise what you have written into the juist format.

The OSIRIS IFS wasgoed designed for accurate high-spatial-resolution spectroscopy with the Keck AO system. Te addition to the IFS, it includes a near-IR imager channel with a 20&quot, field of view and 20 mas pixels. There is a gegevens pipeline for reducing OSIRIS gegevens written ter IDL, and an IDL data-cube viewer called Quicklook2, both available from the UCLA webpagina linked above.

There is a pre-existing OSIRIS wiki hosted at UCLA which discusses observing strategies, pipeline tips, etc. Viewing is free, but this wiki requires a password for editing: voeling Chris Johnson at the UCLA IR Laboratorium for access.

Our instrument-specific/gegevens reduction help pagina is here

### Kyoto 3DII (Kyoto Tridimensional Spectrograph II)

Kyoto 3DII is a PI muziekinstrument of Subaru. This optical spectrograph has four observational modes: IFS with a lenslet array, Fabry-Perot imager, long-slit spectrograph, and filter-imaging modes. Its fine lenslet/pixel sampling of

0&quot,.1 is optimized for good picture quality observations. The spectrograph is klein enough to be used also on the UH 88-inch telescope. Ter this case broader FOVs are emphasized.

Our instrument-specific/gegevens reduction help pagina is here (te Japanese only).

### Integral

Integral is possessed by the IAC and located on the WHT of the ING observatory ter the Canary Islands. There are Four separate IFUs, Trio with different sizes and a 4th with the central fibres blanked out, so acting spil a coronograph (a mode that is however uncommonly used).

Integral is fairly a good exploration muziekinstrument, spil the IFU and grating can be switched lightly across the night spil targets and conditions switch. The main drawbacks of Integral are (i) that the spaxels are not contiguous – there are puny gaps inbetween the fibres, and this can have repercussions on your flux calibration and PSF coverage, (ii) the concentrate at the CCD is not entirely vapid, meaning that the spectral and spatial PSF varies somewhat overheen the CCD, and (iii) switching grating has to be done physically, not electronically. Gegevens reduction is done with IRAF. An IRAF task based on apall is provided if you ask for it, albeit you may spil well just use apall.

Our instrument-specific/gegevens reduction help pagina is here

### OASIS

Our instrument-specific/gegevens reduction help pagina is here

Does anyone have something to add here: tips and tricks on using this muziekinstrument, writing proposals/phaseIIs, or reducing the gegevens. Information that is not te manuals? Postbode here and wij will organise what you have written into the juist format.

### SAURON

Our instrument-specific/gegevens reduction help pagina is here

Does anyone have something to add here: tips and tricks on using this muziekinstrument, writing proposals/phaseIIs, or reducing the gegevens. Information that is not te manuals? Postbode here and wij will organise what you have written into the keurig format.

### GHaFaS (Galaxy H? Fabry-Perot System)

Does anyone have something to add here: tips and tricks on using this muziekinstrument, writing proposals/phaseIIs, or reducing the gegevens. Information that is not ter manuals? Postbode here and wij will organise what you have written into the juist format.

Our instrument-specific/gegevens reduction help pagina is here

## Two.7m Harlan J. Smith Telescope

### VIRUS-P

VIRUS-P is the largest field of view IFU ter the world. It is the prototype for VIRUS, a massive IFU consisting of a mosaic of 150 units like VIRUS-P to be installed on the Ie Telescope during 2011 – see below. The 1/Trio fiber packing multiplicador requires Trio dithers to fully sample the FOV. Two gratings are presently available which provide spectral resolutions of 1.6 A and Four.9 A, and can be blazed at different angles providing a wavelength coverage of $<\Delta \lambda>$ =700 A and $<\Delta \lambda>$ =2200 A inwards the 3500 – 6800 A range.

### VIRUS-W

VIRUS-W’s vormgeving is based of VIRUS-P. However its modes of spectral resolution are dedicated to the investigate of kinematics ter low velocity dispersion objects such spil disk galaxies or dwarf galaxies. The 1/Trio pack negociador requires three dithers to sample the field FOV totally. The two resolution modes are realized through two different gratings. The exchange of the gratings is automated and can be done during the night. VIRUS-W is bench mounted and connected via a 25m long fiber bundle to the telescope. It is a visiting muziekinstrument at the Two.7m and will eventually be brought back to Germany where it will be installed at the fresh 2m Fraunhofer Telescope ter the Bavarian Alps.

### SNIFS

SNIFS is a dedicated muziekinstrument designed for spectro-photometric observations of nearby supernovae of type Ia for the Nearby Supernova Factory. It has bot used to obtain other types of observations spil well – the DEEP Influence event, core-collapse SN spectroscopy, asteroid spectrophotometry, galaxy spectroscopy, and planet searches.

Does anyone have something to add here: tips and tricks on using this muziekinstrument, writing proposals/phaseIIs, or reducing the gegevens. Information that is not te manuals? Postbode here and wij will organise what you have written into the keurig format.

Our instrument-specific/gegevens reduction help pagina is here

## WIYN (Wisconsin, Indiana, Yale, NOAO) Three.8-m telescope

### DensePak

60&quot, from array centre

DensePak is a petite fibre-fed IFU. Advantages include a large FoV, large fibres (good for low surface-brightness studies), access to a medium-to-high resolution spectrograph (Hydra), and albeit is optimised for the crimson, has acceptable blue sensitivity. Disadvantages include the availability of only Four dedicated sky fibres, and the lack of lenslets (meaning light is lost through the gaps inbetween the fibres).

Gegevens reduction is performed using the WIYN hydra package within IRAF. The proces is straightforward and well documented.

Our instrument-specific/gegevens reduction help pagina is here

### SparsePak

65&quot, from array centre along Two sides

SparsePak, the sister muziekinstrument to DensePak, is another puny fibre-fed IFU on WIYN. This time the fibres are only tightly packed ter the centre, with the surplus of the fibres spread out te a sparsely packed array. Since the fibre size is large, the throughput is good, and the total array area is giant, this is an ideal setup for low surface-brightness studies of e.g. nearby galaxy haloes. It is coupled to the same medium-high resolution spectrograph spil DensePak (Hydra), and is optimised very much for the crimson spectral range. Its disadvantages include a lack of utter spatial sampling and the lack of lenslets ter pui of the fibres (only truly significant for the central tightly packed region).

Gegevens reduction is performed using the WIYN hydra package within IRAF. The proces is straightforward and well documented.

Our instrument-specific/gegevens reduction help pagina is here

## KPNO 4m

### FISICA (Florida Pic Slicer for Infrared Cosmology & Astrophysics)

Does anyone have something to add here: tips and tricks on using this muziekinstrument, writing proposals/phaseIIs, or reducing the gegevens. Information that is not te manuals? Postbode here and wij will organise what you have written into the onberispelijk format.

Our instrument-specific/gegevens reduction help pagina is here

## Three.5-m Telescope

### PMAS (Potsdam Multi-Aperture Spectrophotometer)

PMAS and PPAK are two fibre bundles within the same muziekinstrument. PMAS is the standard objectief array IFU recommended for high spatial resolution studies, whereas PPAK is the off-axis fibre bundle IFU recommended for large FoV, low surface brightness objects. A nod & shuffle mode is available for very accurate sky subtraction. Thesis are robustly designed instruments (finding the sky location to set your IFU on is way lighter than for any other IFU I’ve used), albeit for PMAS be aware that switching the grating is not a speedy process. The gegevens is diminished with software provided by the AIP (owners of PMAS) and runs within IDL. Calar Parada is not an observatory with the best weather possible, but it is good to have an IFU that is mounted on a &quot,smaller&quot, telescope, for which certain programmes that will not be accepted for an 8-m class can be run. PPAK is a unique IFU setting of PMAS, unique ter being so large, well suited for studies of stellar outflows and clouds te the ISM.

Our instrument-specific/gegevens reduction help pagina is here

### SPIRAL + AAOmega

Our instrument-specific/gegevens reduction help pagina is here

Does anyone have something to add here: tips and tricks on using this muziekinstrument, writing proposals/phaseIIs, or reducing the gegevens. Information that is not te manuals? Postbode here and wij will organise what you have written into the keurig format.

Our instrument-specific/gegevens reduction help pagina is here

### FaNTOmM (Fabry-Perot den Nouvelle Technologie pour l’Observatoire du mont Megantic)

Does anyone have something to add here: tips and tricks on using this muziekinstrument, writing proposals/phaseIIs, or reducing the gegevens. Information that is not te manuals? Postbode here and wij will organise what you have written into the onberispelijk format.

Our instrument-specific/gegevens reduction help pagina is here

### WIRO-Spec

Does anyone have something to add here: tips and tricks on using this muziekinstrument, writing proposals/phaseIIs, or reducing the gegevens. Information that is not te manuals? Postbode here and wij will organise what you have written into the onberispelijk format.

Our instrument-specific/gegevens reduction help pagina is here

### IMACS

Does anyone have something to add here: tips and tricks on using this muziekinstrument, writing proposals/phaseIIs, or reducing the gegevens. Information that is not ter manuals? Postbode here and wij will organise what you have written into the keurig format.

Our instrument-specific/gegevens reduction help pagina is here

## ARC Trio.5-m Telescope

The Goddard Integral Field Spectrograph (GIFS) is maintained by Michael McElwain, Carol Grady and others from NASA Goddard Space Flight Center. The muziekinstrument concept and vormgeving wasgoed created by Bruce Woodgate. GIFS, formerly known spil the Goddard Fabry-Perot Interferometer or GFP, has several modes of operation. The muziekinstrument can be configured for meteen imaging (400 – 1000nm, with a large collection of filters) with or without a coronagraphic zekering (a wedge ter the field) and a multiplicity of combinations of grisms and lenslet arrays (7&quot,x7&quot, or 14&quot,x14&quot,) for integral field spectrographic operations (480 – 700nm), R=1475 (green grism) or 1823 (crimson grism). Presently the hi-res grism and Fabry-Perot are unavailable. The muziekinstrument is now available to the ARC (Astrophysics Research Consortium) community at large. This telescope is only available to ARC playmates.

Does anyone have something to add here: tips and tricks on using this muziekinstrument, writing proposals/phaseIIs, or reducing the gegevens. Information that is not ter manuals? Postbode here and wij will organise what you have written into the onberispelijk format.

## Herschel

Herschel wasgoed a satellite of the European Space Agency with significant participation from NASA. It operated te the far IR with three instruments: PACS, SPIRE, and HIFI. The former two had photometry and spectroscopy capabilities, and the latter wasgoed a spectrograph alone. The PACS spectrograph wasgoed an IFS, and the SPIRE and HIFI spectrographs produced 3d datasets when they were operated te their mapping modes.

Herschel wasgoed launched te May of 2009 and ceased operations at the end of April 2013. All the gegevens are now public and can be found on the Herschel Science Archive web-site. To reduce the gegevens through one of the various pipelines you can use the interactive Herschel software environment, called HIPE. For each muziekinstrument you can find various levels of gegevens, from raw to fully or almost-fully diminished: at Level Two or higher you have a product that you should be able to do science on. HIPE includes implements to visualise and manipulate Herschel gegevens (of all levels), but since the pipeline end-products are photos, cubes, or spectra, they can all also be loaded into any other software (with various degrees of ease or awkwardness) to be analysed.

PACS operated ter various observing modes, tuned to voorkant all of the SED or smaller parts of it, to observe a single patch of the sky, a dithered patch of the sky, or to make larger mosaics.

The instrument-specific/gegevens reduction help pagina is here

### SPIRE

SPIRE operated te various observing modes: low or high spectral resolution, single sky pointing or a raster with sparse to total spatial sampling.

The instrument-specific/gegevens reduction help pagina is here

## Space

MIRI is the only muziekinstrument for JWST covering the mid-infrared wavelength staatsbestel (5-28 micron). It is a multi-mode muziekinstrument suggesting imaging, low-resolution slit spectrscopy and medium-resolution IFU spectroscopy. The IFU uses an photo slicer vormgeving.

The MIRI flight hardware is expected to be ready for testing te the autumn of 2010. Launch of JWST is planned for June 2014 (keurig spil of May 09).

NIRSPEC will also have an IFS mode.

## Ground

The Ie is programma an IFS called VIRUS (I found this document on it), working ter the blue-optical range, which emerges to be a combination of a MOS and an IFS, lots of individually puny fibres which are arranged ter a half-arcmin square (but with significant gaps inbetween the fibres). 145 of thesis separate units then permits for an enormously large field-of-view coverage. VIRUS is designed to be used te the HETDEX proefneming.

### ESO – VLT

SPHERE will climb on a BIGRE IFS spil one of its scientific camera, aimed to the ongezouten detection of exoplanets. SPHERE IFS will prodive 21025 low-resolution (R

30) spectra from 0.95 to 1.7 micron

at very high tegenstelling te a field of view &lt,Two.Five arcsec around the target starlets. The muziekinstrument will be at the Paranal’s toneel ter 2013. See also the Padova pagina.

KMOS will be a fresh multi-object IFS (24 deployable IFUs) for the VLT. It will work at 0.8–2.Five?m (JHK, at R

3500), and is aimed to be on the telescope ter 2010. See also the Durham pagina.

MUSE is a 2nd generation optical IFS for the VLT developed by CRAL and IRAP (France) AIP and AIG (Germany), ETH (Switzerland), NOVA (Netherlands) and ESO. See also the Lyon pagina. MUSE has two operating modes: a broad field mode (1×1 arcmin Two FoV, 0.2×0.Two arcsec Two sampling) and a narrow field mode (7.5×7.Five arcsec Two FoV, 0.025×0.025 arcsec Two sampling). It offers a broad simultaneous spectral range (4650-9300 A and R

3000. MUSE will benefit from the improved spatial resolution given by the Adaptive Optics Facility te development by ESO (Ground layer correction te Broad Field mode and Laser Tomography ter Narrow Field mode). The large field of view is provided by 24 IFU identical modules. Each IFU is composed of an advanced photo slicer, a spectrograph and a 4kx4k CCD. One single exposure is 400×10 6 pixels. Very first light is planned late 2012.

### ESO – NTT

3D-NTT is planned at the ESO/Schuiflade Apero NTT Three.5m telescope. It is a tunable filterzakje coupled with a high-resolution Fabry-Perot.

### ESO – E-ELT

The E-ELT is ESO’s next generation optical/IR telescope. It is presently (Oct 09) te a Phase B examine, with very first light planned for

2020. Via 2009, 8 muziekinstrument Phase A studies were carried out for various muziekinstrument concepts, and several of those include IFU spectroscopy modes. Descriptions of thesis instruments should be read with caution, spil the specifications are still very much subject to switch, and it is indeed uncertain which will eventually be built. ESO aim to determine on an &quot,instrumentation roadmap&quot, (read: prioritisation and downselect) ter the course of 2010.

METIS is the proposed mid-IR muziekinstrument for the E-ELT and the only muziekinstrument to voorkant wavelengths longwards of Three microns. The investigate is a collaboration of NOVA (Dutch Astronomy Research Schoolgebouw), UKATC, MPIA, CEA Saclay and the KU Leuven, and the PI is Bernhard Brandl at Leiden University. METIS will suggest a number of observing modes: imaging, including polarimetry and coronagraphy, medium-resolution slit spectroscopy (R

1000-3000) and high-resolution integarl field spectroscopy.

The RSS will be mounted on SALT and will have a Fabry-Perot imaging spectroscopy mode, working te the optical – see Rangwala, Williams, Pietraszewki & Joseph, astro-ph 2008.

### Gran Telescopio Canarias (GTC)

FRIDA will be an image-slicer type IFS working te the IR and will be mounted on the GTC.

MEGARA (Multi-Espectrografo plusteken GTC den Adhesión Resolucion para Astronomia).