Instrumentation at the Magellan Telescopes 2008

Instrumentation at the Magellan Telescopes 2008

David J. Osip*, David Floyd, Ricardo Covarrubias

Carnegie Observatories, Las Campanas Observatory, Colina El Pino, Casilla 601, La Serena, Chile

ABSTRACT

The Carnegie Institution operates the twin 6.5m Magellan Telescopes on behalf of the Magellan consortium (Carnegie Institution of Washington, Harvard University, the University of Arizona, Massachusetts Institute of Technology, and the University of Michigan). The two telescopes have been in routine operations at the Las Campanas Observatory since 2001 and 2002 respectively. We currently operate with a suite of instruments available at 6 active ports during regular night-time science operations. Here, we briefly describe the capabilities, operation, and performance of the suite of commissioned instruments including MagIC, PANIC, MIKE, MIKE-Fibers, LDSS3, IMACS, and MagE. Beyond the instruments that are presently installed on site, we will also introduce the large number of instruments that are in advanced stages of construction by teams throughout our consortium (FIRE, Four-Star, MegaCam, MMIRS, PFS, PISCO, MIRAC4).

Keywords: instrument, telescope, Magellan

MAGELLAN TELESCOPES

The Carnegie Institution of Washington owns and operates the twin 6.5m Magellan Telescopes for the benefit of the remaining Magellan consortium members (Harvard University, Massachusetts Institute of Technology, and the Universities of Arizona and Michigan). Both telescopes are of alt-azimuth design with f/11 principal foci, in a Gregorian configuration and are described in detail in papers by de Jonge1, Johns2,3, and Shectman4,5. The rotatable tertiary mirrors feed the f/11 beam to two Nasmyth foci and three additional folded foci around the mirror cell center section. The Walter Baade telescope began science operations in early 2001 and currently maintains three active instrument ports. The Landon Clay telescope initiated science operations in late 2002 and currently also maintains three active instrument ports for f/11 instruments and is undergoing initial testing of the Cassegrain focus to be fed by a new f/5 secondary mirror later this year. The unvignetted field of view at the f/11 foci is 24 arc minutes, however, the nominal corrected field of view is only about 6 arc minutes. On Baade a deployable ADC/corrector in front of the tertiary mirror provides a fully corrected beam across the entire unvignetted f/11 field.

The telescope interface for most instruments at Magellan consists of an instrument (de)rotator mated to a standardized Magellan guider assembly. These guider mechanical/optical assemblies are in turn instrumented with a pair of custom designed and built Magellan Guide Cameras6. Indeed, the first Magellan instrument brought into operation was actually one of these cameras. Used for the first light observations on the Baade Telescope on 15 September 2000, these cameras are found as critical components in all instrumentation deployed at Magellan.

* Magellan Instrumentation Scientist, [email protected]; phone 56-51-207301; fax 56-51-207308

Ground-based and Airborne Instrumentation for Astronomy II, edited by Ian S. McLean, Mark M. Casali,Proc. of SPIE Vol. 7014, 70140A, (2008) · 0277-786X/08/$18 · doi: 10.1117/12.790011

Proc. of SPIE Vol. 7014 70140A-12008 SPIE Digital Library -- Subscriber Archive Copy

Four of the six current operating instruments are cooled via closed cycle coolers (CryoTigers), with the compressors mounted below the azimuth disk of each telescope where they can safely vent heat external to the dome environment. Up to 100’ of flexible cryolines are routed through the altitude disk cable wrap and distributed to the required instrument port. The CryoTiger cooled systems are generally maintained at operational temperatures at all times and dewar hold times between scheduled vacuum pumping and getter cleaning can be in excess of several months. The remaining two instruments are cooled via LN2, with portable 50 liter nitrogen dewars maintained in each telescope dome for routine dewar fillings twice per day.

Instrument and/or detector control computers are maintained either at the instrument platform or in an auxiliary equipment room below the main telescope observing floor. Ethernet and fiber optic communication lines are routed through the main telescope azimuth cable guide and distributed through the altitude disk cable guides and the telescope support structure to the appropriate Nasmyth platform or specified auxiliary folded port. Each instrument port is also provided with local power, glycol cooling lines, and a regulated supply of clean, dry, compressed air. The maintenance of instrument and detector control computers external to the telescope control room allows for optimal use of limited space and presents the observers with a quasi-standard interface to all instruments via a pair of dedicated observer workstations. Mac Mini OSX workstations containing 2GB memory and in excess of 500GB external disk storage are mated to 24” high resolution LCD monitors for efficient instrument control and real time data analysis. Since multiple instruments are often used within a given observing program, observers can choose to operate individual instruments from each workstation; or to run the instrument(s) interface(s) at one workstation while carrying out more intensive analysis tasks at the other via cross-mounted data disks. All instrument GUI interfaces that are not run locally on the observer workstations are via either secure remote X windows display or a secure Virtual Network Client (VNC) connection to the instrument computers with data then piped directly to the observer workstation, all over a high-speed local network. No long term data archive is maintained at the observatory, although data are kept spinning on disk for at least one month and individual consortium members maintain various levels of off-site archives.

The following six sections will each present one of the existing Magellan instruments, including a brief instrument description, an explanation of current supported operating modes, and an up-to-date analysis of the instrument performance characteristics.

IMACS

The Inamori-Magellan Areal Camera and Spectrograph (IMACS) is the most versatile and perhaps not surprisingly the most requested and used instrument at Magellan. IMACS is permanently installed at the Baade NASW platform where it has been in routine science operation since shortly after first light on 19 August 2003. The instrument has been described in detail by Dressler7 and references therein.

IMACS has two independent cameras with a single 6-inch beam refractive collimator going straight through a double-asphere refractive f/2.3 camera or being reflected to feed an f/4 all spherical refractive camera. The f/2 camera re-images a 27.4 arcmin diameter field onto the new Mosaic_2 array of 8 (2kx4k) e2v CCDs sampled at 0.20 arcseconds per pixel. The f/4 camera fully illuminates a 15.5 x 15.5 arcmin field on the Mosaic_1 array of 8 (2kx4k) SITe CCDs at 0.11 arcseconds per pixel. Spectroscopy at f/2 covers a wavelength range of 3900 < < 10500 utilizing three 150 mm grisms producing spectral resolutions of 5-11 FWHM with a slit-width of 0.8 arcseconds along with a low dispersion prism offering a resolving power of 10-30. At the f/4 camera, spectroscopy with wavelength coverage of 3650 < < 10000 is by means of five standard 150 mm x 200 mm reflection gratings – typical spectral resolutions are 1-2 FWHM for a slit-width of 0.7 arcseconds. Multi-slit masks are laser-cut on site to provide a general multiplex of up to 200 slits with the f/4 gratings, up to 600 slits with the f/2 grisms, and the greatest possible multiplexing is achieved with the low dispersion prism at f/2 with over 4000 slits per mask possible.

Imaging and multi-slit spectroscopy using the standard grating or grisms are the principal operating modes of IMACS.In the following figures and tables, the spetcrophotometric throughput and photometric zeropoints are provided for both cameras. Recent cleaning and refilling of all the oil multiplets has improved throughput in both cameras. Most notable, however, is the far superior quantum efficiency provided by the e2v CCDs in the new Mosaic_2 dewar installed in March 2008 at the f/2 camera.

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4000 6000 8000

A (angstroms)

IMACSI/4 Mosaici February 2008

GRAT 1200—I +17.5 (19.0GRAT 1200—I +267 (27.1

GRAT 600—I +13.0 (14.0)GRAT 300—I +4.3 (6.0)

4000 6000

A (angstroms)8000

Figure 1. IMACS spectrophotometric throughput measurements for the f/2 camera with the Mosaic_2 CCD array and the f/4 camera with the Mosaic_1 CCD array. All measurements are total throughput including telescope.

Filter Magnitude f/2

Mosaic_2

Magnitude f/4

Mosaic_1

Extinction

Coefficient

B 26.69 26.69 0.19

V 27.11 27.00 0.14

R 27.49 27.27 0.08

I 26.98 26.50 0.04

u’ 23.07 24.32 0.48

g’ 27.35 27.35 0.18

r’ 27.69 27.51 0.10

i’ 27.47 27.06 0.04

z’ 26.90 26.14 0.02

Table 1. IMACS Zero-point magnitudes (1e-/s at 1 airmass).

IMACS has been built primarily for wide-field multi-object spectroscopy using laser-cut curved mutli-slit masks. However, from the first it was intended to be very versatile in order to support a wide range of astronomical observations. True to this intention, IMACS has now acquired more modes and capabilities than any spectrograph on an 8 m class telescope. The wide array of operating options for IMACS are outlined in the following diagram.

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fieldlens

collimator

f/4 camera1/4º field

f/2.5 camera1/2º field

With f/4 camera: -- reflecting gratings

Magellan telescope

Mosaic_1

8k x8 k CCD

With f/2 camera: -- Refracting grisms

f/11 Baade focus:-- Multislit, longslit masks -- TV slit viewing

GISMO

MOE

IFU

MMTF LDP

Mosaic_2

8k x8 k CCD

IMACS optical layout & modes

Figure 2: Schematic diagram of IMACS operating modes and optional “accessories”.

Beyond the standard imaging, multi-slit, long-slit, and slit-viewer operating modes, IMACS offers diverse capabilities via the optional addition of a choice of several “accessories”.

The Durham-IMACS Integral Field Unit (IFU) provides a mode for two-dimensional spectroscopy with either the f/2 or f/4 camera. Using ~1000 fibers with a spatial scale of 0.2 arcsec, the IFU samples two 5x7 arcsec areas when deployed with the f/2 camera and two 4x6 arcsec areas with the f/4 camera. This “accessory” is added into the Slit-Mask server occupying the space of 3 out of 6 normal masks. This observing mode has been operational since early 2004.

The Multi-Object Echelle (MOE) mode of IMACS (P.I. Andrew McWilliam) permits crossed-dispersed echelle spectra to be obtained over the 15x15 arc minute field of the f/4 camera, accomplished by the use of a grating and cross-dispersing prism mounted on the IMACS disperser server wheel. For a 0.6 arcsecond slit-width MOE provides a 2.5 pixel resolving power of R=21000 in the center of the field. Using one of six positions in the instrument disperser server, this “accessory” essentially transforms IMACS into a spectrograph with properties similar to ESI on Keck, however with a significant multiplexing capability. With each echelle spectrum composed of 9 orders, from roughly 3400 Å to 9500 Å, MOE delivers full wavelength coverage for ~10-15 objects, or as many as ~100 objects in a single order with appropriate blocking filter. Throughput measurements indicate for a V=17.5 RGB star a S/N ~ 50 per extracted pixel can be obtained in approximately 3 hours under average seeing. MOE was installed and commissioned in the instrument during several campaigns during 2006. The high resolution observing mode is generally available.

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The Maryland-Magellan Tunable Filter (MMTF) mode of IMACS (P.I. Sylvain Veilleux), uses a 150 mm diamter Fabry-Perot Etalon operating with the full f/2 camera field of view to provide a tunable bandpass of 10-30 Å FWHM over the wavelength range 5000-9200 Å. The etalon provides a monochromatic spot diameter of 7-11 arcminutes. The measured 6 sensitivity to a emission line point source at 6600 angstroms is 3 x 10-17 ergs/s/cm2 for a 1 hour exposure with a 25-angstrom bandpass. This sensitivity can be improved by frequency switching the etalon in synchronization with charge shuffling in the CCDs of the Mosaic_2 array. This observing mode averages over temporal variations of the atmosphere and the instrument. This “accessory” can be installed in one of the six disperser server positions and can be used following a brief calibration procedure of the etalon controller unit. The MMTF had first light in 2006 and initiated commissioning in February of 2007 with follow-up campaign observations in November 2007. This observing mode is currently scheduled in campaign observing mode.

Gladders Image-Slicing Multislit Option for IMACS – GISMO – is a system for reformatting the inner field of IMACS designed by Mike Gladders. Through a series of mirrors at the focal surface, and lenses above, the inner 4x4 arcminutes of the IMACS field are broken up into 16 individual areas that are re-imaged at the proper focal ratio back to the focal surface, but now spread over the full f/4 camera field. This means that the spectra of objects whose spectra would normally overlap are clearly separated, utilizing the entire IMACS 8k x 8k Mosaic_1 detector array. In densely packed target-rich regions, GISMO offers a typical multiplex of 5-8 times the number of objects that can be independently sampled compared to the standard IMACS multi-slit density. This “accessory” is installed in the IMACS mask server and takes the place of all 6 normally available mask positions. GISMO uses its own slit-masks (laser-cut steel sheets prepared analogously to the normal multi-slit masks) to provide up to 5 slit fields and one open imaging position on each setup. This observing mode was originally tested in the instrument in 2007 and following subsequent corrections to the re-imaging optics, the final commissioning is now being completed on the updated system to make it available for general use during the 2008B observing semester.

With a choice of two cameras with different spatial scales and spectral resolutions, and these various “accessories”, IMACS is easily the world’s most versatile astronomical spectrograph. Observers can configure IMACS to utilize any combination of these capabilities for any given night’s observing. In addition, IMACS is also “at the ready” for short-term use when the principal observations are being made with other instruments (currently, either PANIC or MagIC ) on alternate ports.

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MAGIC

The Raymond and Beverly Sackler Magellan Instant Camera (MagIC) is an efficient direct visible imager incorporating a choice of two CCDs; a SITe 424a 2048x2048 array with a pixel scale of 0.069 arcsec/pixel - or - an e2v 1024x1024 frame transfer array with a pixel scale of 0.038 arcsec/pixel. The dewar is mounted to an 18 position dual filter wheel with a standard filter complement consisting of Harris B,V,R,I and Sloan u',g',r',i',z' filters as well as a custom VR filter. Zero-point magnitudes (1e-/s at 1 airmass) for the two CCDs are tabulated below.

Filter SITe e2v Extinction Coefficient

B 27.52 27.46 0.21

V 27.56 27.74 0.12

R 27.75 27.84 0.10

I 27.14 27.09 0.04

u’ 25.87 24.94 0.49

g’ 27.82 27.87 0.16

r’ 27.90 28.00 0.09

i’ 27.53 27.48 0.04

z’ 26.53 26.31 0.04

Supported operating modes for MagIC SITe include: un-binned quad-amp readout (23s), un-binned single-amp readout (84s), and single-amp subframe readout. For the e2v, supported modes include: un-binned dual-amp readout in ~5s and binned dual amp readout (2x2 or 4x4 read in a fraction of a second with total overhead of 2 seconds). Array gain and read noise are ~2e-/ADU and 6-8 e- for SITe; ~0.5e-/ADU and 5e- for e2v. MagIC was first installed in March 2001 and was upgraded to include the second CCD array in August 2007. The instrument is currently installed at the AUX2 port on the Baade Telescope and maintained cold and always at the ready for full and partial night scheduled observations.

PANICPANIC (Persson's Auxiliary Nasmyth Infrared Camera) is a 1-2.5 micron imager built at the Carnegie Observatories and described in detail in Martini8. The instrument was installed and commissioned in April 2003 and is regularly mounted at the east Nasmyth port of the Baade Telescope. The instrument is an all-refractive, six element design that re-images the Magellan f/11 input beam to f/4.5 to create a 0.125''/pixel scale at the 1024x1024 HgCdTe Hawaii array, corresponding to a 2x2 arcminute field of view. PANIC includes two filter wheels with a current filter complement including four broadband filters: Y, J, H, Ks and two narrowband filters: H2 and Br . Zero-point magnitudes (1e-/s at 1 airmass) for the broadband filters are provided in the following table.

Filter Magnitude Extinction Coefficient

Y 27.3 0.10

Jc 27.4 0.12

Hc 27.1 0.04

Ks 26.6 0.08

Dark current has been measured in PANIC to less than 0.03e-/s and the detector gain and read noise are 2.4e-/ADU and about 25 e- respectively. The detector saturation limit is 45,000 ADU with nonlinearity of 5% at 30,000 ADU and down to 1% at 15,000 ADU. PANIC is maintained cold (via LN2) at all times and is the primary bright-time instrument on the Baade Telescope.

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MIKE & MIKE-FIBERS

The Magellan Inamori Kyocera Echelle (MIKE) is a high-throughput, double-beam, double-pass, echelle spectrograph (see Bernstein9 for complete description and detailed optical design). The spectrograph red side covers a wavelength range from 4400-10000 Å, while the blue side covers 3200-4800 Å. Each side mates to a dewar with a single 2048x4096 CCD (0.14”/pix red, 0.13”/pix blue) with custom readout electronics (developed by Thompson and Burley at the Carnegie Observatories) and individual shutters providing for independent exposure capability. The diameter of the image produced by both cameras is less than a pixel, so the resolving power improves linearly with decreasing slit width. The full resolving power is roughly 55,000 (red) and 65,000 (blue) with a 0.35 arcsec slit, or 19,000 (red) and 25,000 (blue) for a 1.0 arcsec slit.

MIKE was installed and commissioned in late 2002 and has been in routine operation since. The CCD for the blue-side of MIKE was upgraded in 2004 with a lower noise and far more sensitive thinned, back-illuminated MIT/LL 2048x4096 detector. Detector gain and read noise were measured at 0.47e-/ADU and 1.8e-. Recently, in June of 2008, the CCD for the red-side of MIKE has been upgraded (final throughput tests are not yet available). Detector gain and read noise for the new red CCD have been measured at 1.02e-/ADU and 2.9e- with linear response over the full well.

The Michigan/MIKE Fiber System (MMFS, P.I. M. Mateo) is a front end fiber-feed addition to MIKE that turns the single object instrument into a wide-field multi-object echelle spectrograph. The system includes 128 fibers feeding each CCD camera of the spectrograph with each fiber encircling a 1.4 arcsecond aperture. Fiber positioning is achieved via manually assigned pre-drilled ‘plugplates’. Fibers have a minimum separation of 14.5 arcseconds and can be placed out to a field diameter of 23 arcminutes.The effective resolution with the fibers is approximately 70% that of MIKE direct with a 1 arcsecond slit, or about 15,000 in the Red and 19,000 in the Blue. The 175 micron diameter fibers project to 6-8 pixels on the Red and Blue CCDs, therefore, it is advisable to bin the CCDs 2x2 or even 3x3 in normal use.

System throughput is strongly filter/order dependent, but observations so far indicate that the system delivers 1 photon/sec/Angstrom at V=17.2 in the Red fibers, and 1 photon/sec/Angstrom at V=17.7 with the Blue fibers at about 5180 Å. Throughput is highly seeing-dependent; the values above refer to about 0.8 arcsec seeing. Considerably better seeing gains about a factor of 1.5-2.0 over the realistic range of good seeing at Clay. Available interference filters to isolate specific orders on both the red and blue sides include Mg (around 5180 Å, one tuned for the red side and one tuned for the blue side), H-alpha, red order 56 (about 6140 Å), and the Ca IR triplet. The current filters isolate single orders, but multi-order operation is possible.

Up to 8 stars can be used in each field as "acquisition targets", allowing one to quickly set up on target fields (typical time is ‹ 5 minutes). Guiding is carried out with two coherent fiber bundles that are positioned at the locations of two suitable guide stars. MMFS also includes an integral Shack-Hartmann mask (on axis) that allows normal active corrections to be calculated and sent to the primary mirror provided a bright star is positioned at the field center. With no bright star on axis for a given field, it is still possible to periodically offset the telescope and apply mirror corrections in an efficient manner.

This modified operating mode for MIKE is available for general use by the Magellan community in campaign mode with support provided by personnel at the University of Michigan. Otherwise, MIKE is maintained cold (via LN2) at all times on the East Nasmyth port of Clay.

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LDSS3

LDSS-3 is the upgraded version of the LDSS-2 spectrograph that was in operation on Magellan from 2001-2004. The upgrade includes a new collimator, camera, CCD, filters and grisms. LDSS-3 was designed to be very red sensitive - allowing efficient multi-object spectroscopy out to 1 micron.

Installed at the West Nasmyth port of the Clay Telescope, LDSS-3 re-images an ~8.3 arc-minute diameter field onto the CCD camera (STA0500A 4064x4064 array from Mike Lesser), with a scale of 0.189 arcsec/pixel. The array operates in a dual amp readout mode with an un-binned readout time of ~72 seconds. The spectrograph currently operates with three VPH-grisms installed for general use. These new grisms were designed by Mike Gladders and assembled by Ivan Baldry, Karl Glazebrook and the JHU Instrument Design Group. These grisms offer R=850-1900 and significantly higher throughput and resolution than the old LDSS grisms and are the currently supported options. The throughputs and wavelength ranges of the VPH-ALL, VPH-RED and VPH-BLUE grisms are shown for a central slit position in the following figure. A feature of these grisms is that the wavelength coverage and blaze varies substantially over the detector (additional throughput plots at varied field positions are available at http://www.lco.cl/telescopes-information/magellan/instruments/ldss-3/).

Available observing modes for LDSS-3 include: broadband imaging, long-slit spectroscopy, and multi-slit spectroscopy with a multiplex for several 10s of objects. The instrument is permanently mounted at the West Nasmyth port of the Clay Telescope and maintained cold (via CryoTiger) and operational at all times.

LDSS3 Throughput

Filter Mag

g’ 27.71

r’ 27.70

i’ 27.32

z’ 26.37

Figure 3. Throughput measurements for LDSS-3. All three VPH-grisms are measured for a central slit and tabulated values include telescope. Zero-point magnitudes (1e-/s at 1 airmass) are also tabulated for the installed Sloan filters.

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MAGE

The Magellan Echellette (MagE) developed by P.I. Scott Burles is the most recent addition to the Magellan instrument suite. The instrument saw first light in November of 2007 and was commissioned and introduced into routine science operations before the end of the year. A detailed description of MagE is already provided by Marshall10 in these conference proceedings. In brief, MagE is an optical echellette with R~4500 covering a wavelength range of 0.3-1.0 micron. It is primarily a single object spectrograph with slit length up to 10 arcseconds and is optimized for high throughput in the blue. The measured throughput for the combined telescope and instrument is included in the following table.

Order Lambda Dlambda Zeropoint Extra Extinction Efficiency Efficiency

(Å) (Å) (1 ct/s/Å) Flux (Instrument)20 3125 0.231 17.504 0.191 1.523 0.091 0.14919 3260 0.244 18.434 0.046 0.952 0.116 0.18918 3440 0.258 18.791 0.036 0.587 0.120 0.19617 3650 0.274 19.042 0.042 0.464 0.144 0.23516 3860 0.292 19.212 0.025 0.370 0.161 0.26315 4130 0.311 19.438 0.026 0.291 0.198 0.32214 4400 0.335 19.461 0.024 0.215 0.200 0.32613 4750 0.360 19.491 0.007 0.176 0.211 0.34412 5140 0.390 19.503 0.000 0.114 0.217 0.35311 5590 0.426 19.415 0.000 0.117 0.218 0.35510 6130 0.469 19.316 0.000 0.085 0.212 0.3459 6800 0.521 19.125 0.000 0.028 0.187 0.3058 7520 0.590 18.682 0.000 0.004 0.135 0.2197 8610 0.674 18.057 0.000 0.149 0.099 0.1616 9700 0.788 16.300 0.000 0.027 0.020 0.032

MagE is currently mounted and maintained cold (via CryoTiger) at the AUX2 port of the Clay Telescope. Due to the combined accessibility of MIKE and MagE, many observers are utilizing both instruments during scheduled observing campaigns with a brief (10-12 minute) tertiary rotation required to change ports.

OTHER INSTRUMENTS

Apart from the current supported suite of 6 Facility class instruments, Magellan has hosted several temporary instruments (B&C Spectrograph, Classic_Cam, and LDSS-2) as well as several visiting instruments (MIRAC/BLINC, CorMass, and POETS). In addition, the partners of the Magellan Consortium are currently developing a host of new instrumentation along with two new secondary mirror systems (f/5 and a fully adaptive f/16). Current instruments under development include:

FIRE: A compact folded-port f/11 infrared echellette providing R~6,000 cross-dispersed spectra covering the entire near-IR, and a low resolution (R~1200) mode. (PI. Rob Simcoe). A detailed description is available in Simcoe11 in these proceedings.FourStar: a wide-field 11’x11’ near-IR imager using 4 Rockwell Hawaii IIRG arrays (P.I. E. Persson). A detailed description is available in Persson12 in these proceedings. MMIRS: a medium-resolution R~3000 multi-object near-IR spectrograph being built for the f/5 Cassegrain focus on Clay and to be shared with the MMT. (P.I. B. McLeod). A detailed description is available in McLeod13 in these proceedings.Megacam: a wide-field 24’x24’ 36 CCD mosaic camera being built for the f/5 Cassegrain focus on Clay and to be shared with the MMT. (P.I. B. McLeod). PFS: Carnegie Planet Finder Spectrograph (PI instrument): high stability optical echelle spectrograph optimized for single object planet hunting to ~1m/s (P.I. S. Shectman, P. Butler, J. Crane). A detailed description is available in Crane14 in these proceedings.

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PISCO: Multi-channel simultaneous visible imager (PI instrument) (P.I. C. Stubbs)MIRAC4: thermal infrared imaging spectrograph (f/16 AO fed) (P.I. Phil Hinz). Described in detail along with the f/16 adaptive secondary in Close15 in these proceedings.

ACKNOWLEDGEMENTS

We acknowledge the dedicated efforts of the large number of personnel at OCIW and the various Magellan consortium partners that have had a role in bringing the first generation Magellan instruments to fruition. In particular we acknowledge the instrument P.I.s ; Alan Dressler, Eric Persson, Steve Shectman, Rebecca Bernstein, Jim Elliot, Scott Burles, and Mike Gladders. It is also a great pleasure to acknowledge the superb team of astronomers, instrument specialists, technical staff, and telescope operators at the Las Campanas Observatory, Magellan Telescopes that prepare, operate, troubleshoot, and maintain this instrument suite. The superb observational results and the almost non-existent down time of these instruments serve as testament to the extraordinary efforts of all involved.

REFERENCES1. M. J. de Jonge, “Status of the Magellan Project”, Advanced Technology Optical Telescopes V, ed. L. M. Stepp,

Proc. SPIE 2199, pp. 22-30, 1994. 2. M. W. Johns, “Magellan 6.5-m Telescopes Project: Status Report”, Optical Telescopes of Today and Tomorrow, ed.

A. Ardeberg, Proc. SPIE 2871, pp. 49-56, 1996. 3. M. W. Johns, “Magellan 6.5-m Telescopes Project: Status Report”, Advanced Technology Optical/IR Telescopes VI,

ed. L. M. Stepp, Proc. SPIE 3352, pp. 102-110, 1998.4. S. A. Shectman, “The Magellan Project”, Telescope Structures, Enclosures, Controls, Assembly/Integration/

Validation and Commissioning, eds. T. A. Sebring and T. Andersen, Proc. SPIE 4004, pp. 47-56, 2000.5. S. A. Shectman, M. Johns, “Magellan Telescopes”, Large Ground-based Telescopes, eds. J. M. Oschmann, L. M.

Stepp, Proc. SPIE 4837, pp. 910-918, 2003.6. G. S. Burley, I. Thompson, C. Hull, "Compact CCD Guider Camera for Magellan", Scientific Detectors Workshop,

Hawaii, 2002.7. A. Dressler, T. Hare, B. Bigelow, D. Osip “IMACS: the wide-field imaging spectrograph on Magellan-Baade”,

Ground-based and Airborne Instrumentation for Astronomy. Edited by McLean, Ian S.; Iye, Masanori. Proceedings of the SPIE, Volume 6269, pp. 62690F, 2006.

8. P. Martini, S. E. Persson, D. C. Murphy, C. Birk, S. Shectman, S. Gunnels, E. Koch, “PANIC: a near-infrared camera for the Magellan telescopes”, Ground-based Instrumentation for Astronomy. Edited by Alan F. M. Moorwood and Iye Masanori. Proceedings of the SPIE, Volume 5492, pp. 1653-1660, 2004.

9. R. Bernstein, S. A. Shectman, S. M. Gunnels, S. Mochnaki, A. E. Athey, “MIKE: A Double Echelle Spectrograph for the Magellan Telescopes at Las Campanas Observatory”, Instrument Design and Performance for Optical/Infrared Ground-based Telescopes, eds. M. Iye, A. F. M. Moorwood, Proc. SPIE 4841, pp. 1694-1704, 2003.

10. J. L. Marshall, S. M. Burles, I. B. Thompson, S. A. Shectman, B. Bigelow, M. Smith, G.Burley, C. Birk, J. Estrada, P. Jones, V. Kowal, J. Castillo, R. Storts, "The MagE Spectrograph", Astronomical Telescopes 2008, Proc. SPIE (this conference) 2008.

11. R. A. Simcoe, A. J. Burgasser, R. A. Bernstein, B. Bigelow, J. Fishner, W. J. Forrest, C. W. McMurty, J. L. Pipher, P. Schechter, M. Smith, "FIRE: a near-infrared, cross-dispersed Echellette spectrometer for the Magella Telescopes", Astronomical Telescopes 2008, Proc. SPIE (this conference) 2008.

12. S. E. Persson, R. H. Barkhouser, R. P. Hammond, J. L. Marshall, D. C. Murphy, J. D. Orndoff, G. A. Scharfstein, S. A. Shectman, S. A. Smee, A. Uomoto, "The FourStar infrared camera", Astronomical Telescopes 2008, Proc. SPIE (this conference) 2008.

13. B. A. McLeod, G. U. Nystrom, H. W. Bergner, W. R. Brown, M. Burke, D. L. Curley, G. Furesz, J. C. Geary, K. McCracken, T. J. Norton, D. G. Fabricant, "MMT and Magellan infrared spectrofraph", Astronomical Telescopes 2008, Proc. SPIE (this conference) 2008.

14. J. D. Crane, S. A. Shectman, R. P. Butler, "The Carnegie Planet Finder Spectrograph: a status report.", Astronomical Telescopes 2008, Proc. SPIE (this conference) 2008.

15. L. M. Close, P. M. Hinz, D. A. Kopon, V. L. Gasho, "The Magellan adaptive secondary AO system", Astronomical Telescopes 2008, Proc. SPIE (this conference) 2008.

Proc. of SPIE Vol. 7014 70140A-10