The Irénée du Pont Telescope

The Irénée du Pont Telescope

InstrumentDescription (Specs link)Notes
CCDDirect CCD CameraA
WFCCDWide Field Reimaging CCD CameraB
Boller & Chivens SpectrographSlit SpectrographC
EchelleEchelle SpectrographD
CAPSCamAstrometric Planet Search CameraE
RetroCamHgCdTe IR CameraF
file name: echelle.objects
	HD5980       |  00:59:26.6 | -72:09:53.9 | 2000.000 | 
	Sk80         |  00:59:32.0 | -72:10:46.3 | 2000.000 | 
	HR718        |  02:28:09.5 | +08:27:36.0 | 2000.000 | flux standard
	R71          |  05:02:07.4 | -71:20:13.1 | 2000.000 | 
	HDE269582    |  05:27:52.7 | -68:59:08.6 | 2000.000 | 
	R127         |  05:36:43.7 | -69:29:47.5 | 2000.000 | 
	Feige110     |  23:19:58.4 | -05:09:56.2 | 2000.000 | flux standard


NOTES

A. The SITe2K CCD is available for direct imaging on the du Pont 2.5-meter telescope, and gives a scale of 0.259″ per pixel over a field of 8.85 arcmin square.

B. The wide field reimaging CCD (WFCCD) camera reimages a 25 arc-minute diameter field onto the WF4K CCD camera, with a scale of 0.484 arcsec/pixel. It produces images of approximately two pixels over the full field, and has good transmission from 3800 Å to 9000 Å. Metal slit masks are used to provide a multi-object spectroscopy capability. Observers should consult J. Mulchaey (mulchaey@obs.carnegiesciene.edu) or I. Thompson (ian@obs.carnegiesciene.edu) about mask making procedures and should allow three months for the production of the masks.

C.  The B & C spectrograph uses a Marconi CCD mated to a Bowen Schmidt camera as the detector. When used with the 600 line/mm grating the dispersion is 1.5 Å/pixel with a wavelength coverage of 3100 Å. The spatial scale on the du Pont Telescope is 0.70 arcsec/pixel, and the maximum slit length 271 arcsec.

D. The Echelle Spectrograph provides simultaneous wavelength coverage from ~3700-7000 Å at a typical resolution of ~40,000.

E. CAPSCam is a specialized astrometric camera designed for an astrometric search for Jupiter-like planets.  The camera employs a Rockwell Hawaii-2RG HyViSI array, and the design is optimized for high accuracy astrometry of red dwarf stars.  Observers interested in using this instrument should contact Alan Boss (Carnegie-DTM) or Ian Thompson (OCIW).

F. RetroCam is a near-IR imager built especially for the Carnegie Supernova Program, but which is generally available to users.  RetroCam employs a Rockwell Hawaii-1 HgCdTe 1024×1024 array. The focal plane scale is 0.201 arcsec/pixel, with a total field size of  3.4arcmin square. A single filter wheel containing Y, J, and H filters is available.

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