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Procedures for requesting telescope time on the Thai Southern Hemisphere Telescope (TST)

Procedures for requesting telescope time on the Thai Southern Hemisphere Telescope (TST)

  1. Complete the TST Time Request Form
  2. The TAC (Time Allocation Committee)could take up to 6 weeks to process your request. So it's recommended that you give your application an ample amount of time before the planned observation.
  3. Once your request has been processed, you will receive an email back with your form, along with the decision from the TAC.
  4. If your request is approved, you will also be given an account with password,and priority that best suited to the nature of your project. You will also be given your project "Request Number" Please include this code in the prefix of the name of your observation. This will help the TACto monitor the usage.
  5. The user is REQUIRED to regularly monitor your observation. This include, but not limited to, checking if your target can still be observed in the images, notice if there is any problem with the telescope, adjust and modify your observation accordingly should any unexpected change arise, do some preliminary data analysis to make sure that the data obtained are usable to achieve your science goals.
  6. Observations are subjected to cancellation by the TAC without prior notice if it is in according with the following violations:
    • not adhere to the procedures mentioned in #1-7

    • overuse

    • observing targets outside approved proposal

    • risk of camera damage, e.g., running into the moon

    • gross deviation from PROMPT policy

    • any other circumstances as approved by TAC

  7. If you encounter any problem during your project, please contact theTAC.
  8. Once your observations have been completed, please submit the "End of Run Report" (download <here>) to <This email address is being protected from spambots. You need JavaScript enabled to view it.>. Future request could be put on hold until the End of Run Report for previous projects have been received.
  9. This account cannot be used outside the requested project time.
  10. For publications using observations from the Thai Southern Hemisphere Telescope, please observe the Skynet Authorship Policy (https://skynet.unc.edu/skynet/help/authorship_policy)

Telescope

Planewave, CDK24

Aperture

24 inch   (610 mm)

Focal Length

3962 mm   (155.98 inch)

Focal Ratio

f/6.5

Central Obstruction

47% of the Primary Mirror Diameter (11.38")

Back Focus from Mounting Surface

14.1 inch   (358 mm)

Back Focus from Racked in Hedrick Focuser (including front spacer)

5.81 inch   (148 mm)

Back Focus from Racked in IRF90 Rotating Focuser (including front spacer)

5.30 inch   (135 mm)

Weight

240 lbs   (108.9 kg)

OTA Length

56 inch   (1,422 mm)

OTA Width

31 inch   (787 mm)

OTA Height

35 inch   (889 mm)

Upper Cage

Carbon Fiber Truss

Lower Cage

Carbon Fiber Truss with Aluminum Light Shroud

Optimal Field of View

70 mm (58 arcminute)


PRIMARY MIRROR

Diameter

24.5 inch   (622 mm)

Aperture

24 inch   (610 mm)

Focal Ratio          

f/3.2

Mounting

Laser Collimated and Permanently Fixed

Material

Precision Annealed Borosilicate

Shape

Prolate Ellipsoid

Coating

Enhanced Aluminum - 96%


SECONDARY MIRROR

Diameter          

9.45 inch   (240 mm)

Material

Precision Annealed Borosilicate

Shape

Spherical

Coating

Enhanced Aluminum - 96%


LENS GROUP

Diameter

135 mm   (5.31 inch)

Number of lenses          

2

Coating

Broadband AR Coatings (less than .5% reflected from 400 to 700nm)


STANDARD FEATURES

Carbon Fiber Truss Design

Minimizes thermal expansion which causes focus shift with changes in temperature

Lower Light Shroud

Protects the primary mirror from damage and stray light

Dovetail expansion joint

Allows for the difference in thermal expansion between carbon fiber and aluminum.

The expansion joint allows the aluminum dovetail expand and contract without

stressing the carbon fiber lower truss

3.5 inch Hedrick Focuser

Heavy duty no-slip focuser. The focus tube runs on 5 bearings and is driven by a

leadscrew so there is no chance of slipping. Focus may be automated through a

computer using PlaneWave's EFA Kit add-on. The draw tube travel is 1.3 inch.

Cooling Fans

The CDK24 has two different cooling schemes. First, there are three fans behind

the primary mirror that blow air out of the optical tube pulling air though the telescope

and by the primary mirror. This helps the telescope to equilibrate quickly. Second,

there are 4 fans placed around the face of the primary mirror to equilibrate the

face of the mirror and to keep a laminar air flow above the telescope's light path.

The fans can be controlled with a manual switch on the optical tube or by a computer

if the optional Electronic Focus Accessory (EFA Kit) is purchased.

cdk24 a200 wide

Planewave, CDK24


Mount

Astro-Physics, 3600GTO

Mechanical Specification

Construction

All CNC machined aluminum bar stock, stainless steel, brass; stainless steel fasteners

Finishing and Assembly

Every part is hand-finished and inspected. All assembly is done by hand, by highly

skilled mount assembly staff.

Worm wheel - R.A./Dec.

13.0" (330 mm), 256 tooth aluminum

Worm gear - R.A./Dec.

Brass, 1.41" (35.8 mm) diameter

Axis shaft - R.A./Dec.

4.72" (120 mm) diameter with 4.02" (102 mm) clear inside diameter

Shaft axis bearings - R.A./Dec.

7.09" (180 mm) diameter deep groove ball bearings

Worm gear bearings

1.57" (40 mm) angular contact ball bearings

Latitude range

15-70 degrees

Azimuth adjustment

Approximately 14 degrees (+/- 7 degrees from center)

Counterweight shaft

2.5" (64 mm) diameter x 31.5" (800 mm) long [30" (760 mm) useable length], incl.

large machined safety stop knob. Will fit 12 optional 30 lb. (13.6 kg) counterweights.

Optional 10" (254 mm) shaft extension available.

Weight of mount

Total: 247 lb. (112.3 kg); R.A. axis/polar fork: 121 lb.lpadding="0" cellspacing="1"

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Electronic components

Rated for industrial and automotive applications

Motors

High-torque, zero-cogging Swiss DC servo motors, enclosed in machined aluminum housing

Motor encoder

2000 tic quadrature yielding an effective resolution of 0.044 arcseconds per tic

Motor reduction gear train

57.6:1 gear reduction through a custom built set of large diameter, fine-toothed, precision,

spur gears for vastly superior performance

Servo Motor Control Box

GTOCP3 Control Box, removeable

Hand-held computer

GTO Keypad to control all mount functions. Includes extensive databases and tour features

in a simple, intuitive interface. Firmware updates via the internet

Power consumption

~ 0.4 to 0.8 amps at 15 volts - tracking
~ 1.5 to 3.0 amps at 15 volts - both motors slewing at top speed of 600x

Power requirements

Nominal 15 volt DC supply at 10 amps recommended

Periodic error

5 arc seconds peak-to-peak (+/- 2.5 arc seconds) or less in one worm cycle (5.6 minutes);

native, prior to any error correction

Maximum slew speed

2.5 degrees / second


apshowroomje2

Astro-Physics, 3600GTO

Location

Location    Cerro Tololo Inter-American Observatory (CTIO) , Coquimbo Region, Chile

Coordinates 30?10?10.78?S   70?48?23.49?W

Altitude 2,207 meter

tnst03 1

Cerro Tololo Inter-American Observatory (CTIO)

TST (Thai Southern Hemisphere Telescope)

11 tnst03


     NARIT is developing the Thai Southern Hemisphere Telescope (TST), at the Cerro Tololo Inter-American Observatory (CTIO).   The TST will be a 0.6-meter telescope, operated in collaboration with the University of North Carolina at Chapel Hill.   The telescope is a Cassegrain reflector, made by Planewave.   It is expected to begin operation in late 2013.

     The location, in the Coquimbo region of the Republic of Chile, provides some of the world's best conditions for astronomical observation.   The region's high desert climate provides stable, dry air that results in consistently excellent seeing and visibility.   The observatory is located far from any towns or cities, so that it has negligible light pollution.   The observatory will primarily be operated remotely, so that researchers can plan and execute observations from anywhere in the world, using UNC's Skynet software.

12 13


     The telescope will be a part of the UNC-led PROMPT project, and will also be known as "PROMPT-8".   The PROMPT project will observe the afterglows of gamma ray bursts (GRBs), using a network of ground-based telescopes (at CTIO and elsewhere).   Initial detection of GRBs will be done by space-based telescopes (such as NASA's SWIFT gamma-ray observatory), which will then send information used to direct the ground-based telescopes; the ground-based PROMPT network telescopes will then observe the quickly evolving GRB afterglow.   This will provide data to allow researchers to study the evolution, spectra, and magnetic fields of these highly dynamic phenomena.

     When not engaged in the primary mission of GRB study, the telescopes will be available to member institutions for other research - so that NARIT researchers will be able to schedule observations for other research, using multiple telescopes as necessary.   The telescopes will also be available for education; yet another benefit of the network's widespread geographical reach is that teachers in Thailand can observe with their students even in the daytime.

TST 02

TST 03

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