WIRO-Prime: 2048x2048 Prime Focus CCD Camera (manual (pdf) (web))
WIRO Prime is the first of a new generation of facility instruments for the Wyoming Infrared Observatory (WIRO).  Although the 2048x2048 detector is an optical CCD this instrument it will be ideal for several wide-field imaging surveys planned at WIRO.  The camera mounts to a mechanical stage which allows focusing of the CCD camera.  The mechanical design is based upon an earlier instrument built by Ed Loh of Michigan State University.  The University of Wyoming obtained a new, larger CCD and the process of modernizing the MSU instrument was undertaken by Michael Pierce, Philip Haynes and Andy Monson. Steve Hodder was the primary machinist for the project and James Weger developed the electronic design. The upgrades include larger stepper motors controlled with a Compumotor 6k4 controller, improved filter wheels with Hall-effect positioning sensors and the instrument uses a new optical prime focus corrector designed by Chip Kobulnicky, that replaced a smaller original 4-element Wynne corrector designed by Loh, which provides a well-corrected field at f/2.1.


Optical Design




The above figure shows the optical design of the 4-element Wynne corrector.  The cross section on the left shows the light from the primary mirror coming from the left and entering the corrector with the filter, dewar window, and detector to the right, respectively.  The right figure shows a "spot diagram" calculated through focus on-axis and at four off-axis field angles.  The square boxes (2.1 arcsec) show a 4x4 pixel region with the Marconni/EEV CCD.

Mechanical Design
The figure below shows the re-designed Michigan State prime-focus assembly mounted at the WIRO prime focus.  The gold dewar is visible right of center with the filter wheel extending below the dewar.  The assembly features a motorized stage that supports the dewar and is used for focusing.  A lower stage supports the prime focus corrector and allows it to be positioned relative to the primary mirror in order to be placed at the "sweet spot" of the design.  The motorized stage also holds the filter wheel and a 60-mm Prontar leaf shutter.  Linearity tests with this shutter indicate that the exposure time is reliable down to about 0.1 seconds.




Detector
The primary CCD camera used at the WIRO 2.3 meter telescope features a 2048x2048 detector manufactured by
Marconi/EEV.  The detector has 13.5 um pixels and has excellent cosmetics(see images below).  When used for imaging at prime focus this results in a field of view of 17.8 arcmin on a side with 0.5224 arcsec/pixel.  This detector has a remarkably high quantum efficiency (QE) over a broad range in wavelength (see left hand figure below).  Our detector has the "midband" anti-reflection coating plotted in green below.  This results in good QE over a broad range in wavelengths.  In the red the QE peaks at over 90% and is about 70% in the blue, but it drops rapidly at shorter wavelengths.




The detector was integrated into an  Infrared Laboratories   LN2 dewar with control electronics from Astronomical Cameras by Bob Leach. The control electronics allow for a "region of interest" as well as on-chip binning.  Dual read-out amplifiers allows the entire detector to be read out in only 12 seconds, including the time to write the data to disk.  Single amplifier readout takes about 20 seconds but has the advantage of simpler data display and analysis.










Below are some images taken from WIRO by observers during less than science quality night


M16, The Eagle Nebula
OII,OIII,H-alpha
Andy Monson & Bob Berrington



IC434, The Horsehead Nebula
B,V,R
Chris Rodgers & Dave Allen



M17, The Omega Nebula, The Swan Nebula
OII,OIII,H-alpha
Andy Monson & Bob Berrington



NGC891
B,V,R
Chris Rodgers & Andy Monson




Abell 39
B(600s),V(300s),R(300s)
Andy Monson & Stevi Fawcett



M27, The Dumbell Nebula
B(15x10s),V(15x10s),R(15x10s)
Andy Monson & Stevi Fawcett



NGC7293, The Helix Nebula
B(9x30s),V(15x10s),R(15x10s)
Andy Monson & Stevi Fawcett



NGC7331
B(15x20s),V(15x10s),R(15x10s)
Andy Monson & Stevi Fawcett




Bubble nebula
OIII(3x180s),H-alpha(3x300s)
Andy Monson & Stevi Fawcett



M27, The Dumbell Nebula
OII(3x180s),OIII(3x90s),H-alpha(3x90s)
Andy Monson & Stevi Fawcett



M97, The Owl Nebula
OII(3x600s),OIII(3x300s),H-alpha(3x300s)
Andy Monson & Stevi Fawcett



M57, The Ring Nebula
OII(3x300s),OIII(3x180s),H-alpha(3x120s)
Andy Monson & Stevi Fawcett




M101, The Pinwheel Galaxy
B(9x100s),V(9x60s),R(9x60s)
Andy Monson & Stevi Fawcett



M51, The Whirlpool Galaxy
B(9x30s),V(9x20s),R(9x20s)
Andy Monson & Stevi Fawcett



M63, The Sunflower Galaxy
B(9x30s),V(9x20s),R(9x20s)
Andy Monson & Stevi Fawcett



M20, The Trifid Nebula
B(9x6s),V(9x4s),R(9x4s)
Andy Monson & Stevi Fawcett



Measured Performance of the EEV/Marconi CCD
The following figures show the linearity and read-noise floor for the dual-amplifiers of the Marconi/EEV CCD with the Leach controller.  Note that at a system gain of 2.5 e-/ADU the linearity extends to a level of approximately 60,000 ADU with a read-noise of 4.5 electrons.  The full-well is thought to occur slight above 64,000 ADU where the A/D saturates but this is presently uncertain.  These numbers will be updated once more detailed measurements are available.

The figure below shows the 5-sigma limiting magnitude as a function of time for the standard Johnson bandpasses.  These are theoretical curves based upon the QE of the CCD and the filter response curves assuming a seeing of 1 arcsec and no moon light.  The limited data obtained to date(~2002) suggest that these curves are accurate to about 0.1 - 0.2 mag.







Measured Performance
The following photometric zero-points were measured by M. Pierce and R. Berrington:

Bandpass

Zero-Point

Extinction

Color-Term

B

-25.082 ± 0.009

0.295 ± 0.004

-0.117 ± 0.005

V

-25.341 ± 0.009

0.193 ± 0.004

+0.091 ± 0.004

R

-25.373 ± 0.011

0.139 ± 0.004

+0.163 ± 0.005

I

-24.638 ± 0.027

0.061 ± 0.011

-0.037 ± 0.013


Dome Flats
The dome flat screen allows for taking flat frames if twilight frames are un-obtainable or unusable. The image below shows the ratio of a B-band Domeflat/Skyflat.(by Chip Kobulnicky based on 2010Oct13 data.)


User Interfaces

  1. WIRO-Prime Interface
    The WIRO-prime interface controls two stepper motors on the prime focus stage with a Visual-Basic application.  The motors allow for: 1) changing filters, and 2) focusing the CCD relative to the corrector.  The desired filter can be selected from a pull-down menu and the position will then be highlighted in the filter position text box.  Note: the user must hit the "go" button to complete the filter move command. To read the current position of the filter wheel, magnets have been placed around the filter wheel and are read by a hall-effect sensor. There are 12 filter position and each one is uniquely labeled by its order of magnets, as seen on the right. Once the filter wheel has stopped moving the sequence of magnets sensed by the hall effect reader is translated into a filter based on a file edited by the observer that translates which filter position corresponds to which filter.
    Focus is controlled by the Jog+/Jog- buttons. Jog+ moves the dewar assembly away from the primary and Jog- moves toward the primary. See Getting Good Focus.

  2. Voodoo Interface
    At the present time we use the user interface supplied by Astronomical Cameras known as Voodoo.  Voodoo is a Java based application which allows the user to select a region of interest, the on-chip binning (if any), as well as the exposure time.  It also features a simple interface for adding and editing FITS keywords into the image header.

FITS Header Editing
At the present time the CCD camera does not automatically communicate with the telescope control system (TCS).  However, Bob Berrington has written a program to communicate the telescope information to the Voodoo header.  Otherwise, the Voodoo interface allows the user to edit some the FITS header parameters.  Since Voodoo does not communicate with the instruments in use and not all of the appropriate KEYWORDS are automatically written into the header the user is advised to keep paper logs and/or fill out the header KEYWORDS themselves using the Voodoo editing tool.  Log sheets are available
here.



Available Filters
The WIRO prime focus camera features a 12 position filter wheel capable of accepting either 2" or 50 mm square filters up to 6 mm thick.  At the present time there are three filter wheels and the table below shows the currently available filters.  Note that thin inserts must be used with 50 mm filters if they are used in the 2" wheels. See Filter Wheel for information on how to change filter wheels at the telescope.


Filter Name

Central Wavelength

Bandwidth

Notes

Johnson  U

3640 A

700 A

Bessel: (wheel #1)

Johnson   B

4350 A

980 A

Bessel: (wheel #1)

Johnson   V

5380 A

980 A

Bessel: (wheel #1)

Kron-Cousins   R

6250 A

1180 A

Bessel: (wheel #1)

Kron-Cousins   I

7900 A

1400 A

Bessel: (wheel #1)

DDO  51

5130 A

154 A

Smith: (wheel #1)

Washington  C

3910 A

1100 A

Canterna: (wheel #3)

Washington  M

5085 A

1050 A

Canterna: (wheel #3)

Washington  T1

6300 A

800 A

Canterna: (wheel #3)

Washington  T2

8050 A

1500 A

Canterna: (wheel #3)

Halpha (Custom Scientific 656.3/3.0)  z = 0.000

6563 A

30 A

(wheel #1)

Halpha (Corion S10-656)  z = 0.000

6563 A

100 A

(wheel #1)

Halpha off (G572-6400)  ()

6400A

50 A

(wheel #1)

Halpha  z = 0.006 (1600 km/sec)

6600A

50 A

(wheel #1)

Halpha  z = 0.036 (11,000 km/sec; G572-6800)

6800A

100 A

(wheel #3)

Halpha  z = 0.066  (20,000 km/sec; unlabeled filter)

7000A

100 A

(wheel #3)

O[II] 

3727 A

?? A

(wheel #1)

O[III] 5007 

5007 A

?? A

(wheel #1)

Redshifted Halpha

7598 A

61 A

D. Dale 2inch filter

Redshifted Halpha

7661 A

61 A

D. Dale 2inch filter

Redshifted Halpha

8132 A

58 A

D. Dale 2inch filter

Redshifted Halpha

8199 A

57 A

D. Dale 2inch filter

Redshifted Halpha

8615 A

59 A

D. Dale 2inch filter

Redshifted Halpha

8685 A

64 A

D. Dale 2inch filter

Redshifted Halpha

9155 A

58 A

D. Dale 2inch filter

Redshifted Halpha

9233 A

59 A

D. Dale 2inch filter

WIRO Medium-01

5000 A

800 A

Loh & Spillar: Round 2-inch filters!? No filter wheel!

WIRO Medium-02

6000 A

1000 A

Loh & Spillar:

WIRO Medium-03

7000 A

1100 A

Loh & Spillar:

WIRO Medium-04

8100 A

1100 A

Loh & Spillar:

WIRO Medium-05

9000 A

800 A

Loh & Spillar:

WIRO Narrow-01

4250 A

800 A

Loh & Spillar:

WIRO Narrow-02

4900 A

800 A

Loh & Spillar:

WIRO Narrow-03

5350 A

500 A

Loh & Spillar:

WIRO Narrow-04

6450 A

500 A

Loh & Spillar:

WIRO Narrow-05

6800 A

500 A

Loh & Spillar:

WIRO Narrow-06

7150 A

500 A

Loh & Spillar:

WIRO Narrow-07

7450 A

500 A

Loh & Spillar:

Shutter Timing

Beware of using very short exposure times as the actual shutter open time is not linear with commanded exposure time. Also, owing to the finite shutter open-close time, different parts of the detector are illuminated for different durations. The image below shows the ratio of N-sec dome flats divided by a scaled 5-sec domeflat. Left: 0.1s ... Middle: 0.25s ... Right: 0.5s. (by Chip Kobulnicky based on 2010Oct13 data.) In a perfect system, the ratio would show 1.0 everywhere. Edges and corners have smaller effective exposure times than the middle of the detector.


Last Modified 05/04/06
Michael Pierce (mpierce@uwyo.edu), Andy Monson (amonson@uwyo.edu)