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The Irénée du Pont Telescope

Instrument

Description

Specs

Website

Notes

CCD Direct CCD Camera yellow page page.gif A
WFCCD Wide Field Reimaging CCD Camera yellow page page.gif B
Boller & Chivens Spectrograph Slit Spectrograph yellow page page.gif C
Echelle Echelle Spectrograph   page.gif D
CAPSCam Astrometric Planet Search Camera yellow page page.gif E
RetroCam HgCdTe IR Camera
yellow page page F

 

The Telescope Operator can enter target coordinates by hand. However, it is often useful to have coordinates in a file that can be automatically read by the TCS. A target list can be prepared prior to the observing run and uploaded to clarity or caballo. A suitable target list will consist of a text file containing the following columns separated by a pipe: Object designation, RA, DEC, EQUINOX, comment (optional). The file can have any name but it needs to have an ".objects" extension. An example follows:

	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

Once the target list is uploaded to clarity or caballo, you need to open the 'TeleGUI' (from telescope icon in the bottom task bar), click on 'File' (top bar, left, next to TeleGUI, and select 'Open ObjectList'. This will bring up a browser where you can select the desired file. The list will show up in a separate window which provides buttons for editing, adding, removing, and 'send to TCS'. To save changes just click again on 'File' and 'Open ObjectList', and the option of 'saving changes' will be offered.

 


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 1024x1024 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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