1 hour before sunset:  Old Console Room ( C Floor )

1. Check Weather Conditions [1]
2. Orient the shutter eastward to make sure no direct sunlight will enter the dome.
3. Open the dome (before opening mirror cover!)
4. Open the mirror cover
5. Turning OFF mirror cooler executed automatically ( BECS [2] )
6. Turning ON sucker & extractors executed automatically ( BECS [2] )
7. Turn OFF dome floor stirring fan
8. Turn OFF both AHU's units
9. Open the lateral sliding doors

             Note: if wind is greater than 15 mph on average wind buffet on the telescope may produce elengated images in which case the sliding doors should be closed.Under any circumstances,the lateral doors must be closed if the wind speed is greater than 25 mph.

      10. Make sure all passageway doors are closed, especially the glass door in front of the lift at GR floor, the cryocooler compressor and pump rooms.

** In the Console Room : G Floor

- Using the TCS GUI :

      11. Turn on 4MAP Optical Corrections for M1 : (See why [3])

                   ** If working at f/8: COSMOS - ARCOIRIS :

                            - Choose 4MAP table for F8

                            - Turn ON M2 Corrections ON ALWAYS!!!

                            - Check collimation [4]

                    **  If working at Prime: DECAM

                             - Choose 4MAP table for PF

                             - Activate TWK ON  ( ONLY FOR PF )

At Sunset :

1. OPEN AtmCam
2. OPEN Rasicam

Blanco 4-m Daily Procedures - During the Night

• Watch the weather, make sure the bad weather rules [5] are followed.
• A 1° temperature difference between the mirror surface and the ambient air will create additional mirror-seeing (typically up to 0.5" extra for 1° difference). Thus our goal is to maintain the mirror temperature within 1° of the predicted temperature of the following night.
• If wind speed is greater than 15 mph on average wind buffet on the telescope may produce elongated images in which case the sliding doors should be closed if need be,raise windscreen.
• Occasionally look at BCS telemetry [6] and check that:
  • All for mirror sensors are within 0.5-1°C of each other
  • Mirror temperature, dome temperature and outside temperature are within 1°C of each other
  • R.A. bearing hydraulic oil cooling is working (if not, the oil temperature will rise quickly to around 30°)
• Do DECAM CheckList around 3 A.M.
• Report any problems.

Blanco 4-m Daily Procedures - End of the Night

1. Turning OFF the mirror sucker executed automatically ( BECS )
2. Turning  ON the mirror cooler executed automatically (BECS )
3. Turn ON dome floor stirring fan
4. Turn ON both AHU's units.
5. If working at Cass, turn off the chimney fans ( not in use...TBD )
6. Close the mirror cover (before closing dome!)
7. Close the dome
8. Close the lateral sliding doors
9. Make sure an End-of-night report has been filled.
10. If this is the last night of a run, remind the observer to complete an End-of-run report.
11. Close the ATMCAM
12. Rasicam status
13. Windscreen status
14. Make sure an Telescope Operator Report has been filled

 

 

Revised 18 Feb 2010 by A. R. Walker

		Contents:
	1.	Weather and thermal issues
		1.1	General closure conditions
		1.2	Dome opening
		1.3	Lateral sliding doors opening
		1.4	Primary mirror cooling
		1.5	Floor cooling ans stirring fan on main floor (M)
		1.6	Oil cooler
		1.7	Chimney fans
		1.8	Air conditioning
		1.9	Temo4m and weat
	2.	Brief reminder of known optical problems
		2.1	Astigmatism
		2.2	Coma
		2.3	Defocus
	3.	Prime Focus nights
	4.	F/8 nights

ACTR#002/00

DT: 18th October 1999
TO: Telops, Scistaff, ETS leaders
FM: ACTR and Maxime Boccas
RE: Revised operation instructions at the 4m-telescope for image quality program

 

Since the end of 1993, many improvements have been carried out at the 4m telescope to improve its image quality. The principal changes are: an active primary mirror support with lookup tables, a repolished f/8 secondary mirror, an image analyzer for the Cassegrain foci, removal of most heat sources inside the dome, active control of the primary temperature during the day, active ventilation of the primary cell at night, dome ventilation doors and active control of oil temperature.

 

 

 

1. Weather and thermal issues

The night assistant must check that all the environmental control functions explained below are working properly during the night.

1.1 General closure conditions:

ABSOLUTE closure when:

• wind > 45 mph on average over the last 20 minutes (the telescope might still not shake badly but the air is dusty and will bring too much dirt inside the domes)
• If wind > 25 mph absolute closure of the lateral sliding doors
• humidity > 85 %, as indicated by the met tower 
• Tmirror - Tdew < 2°C. The values of Tdew and Tmirror-Tdew are shown in Blanco ECS:Sensors Diagram [7], which is actualized every 5 minutes.
• See calculating risk of condensation [8] for more information about dew point.

Dome re-opening:

• if wind <= 45mph on average over the last 20 minutes
• if RH < 85% for 30 consecutive minutes (in all cases, check outside that no water is dripping from the buildings).
• if Tmirror - Tdew >= 2°C for 30 consecutive minutes

GUIDELINE :

1.  If  wind > 25 mph, avoid observing into the wind direction as it could jitter the telescope and will bring dirt inside the dome.
2.  If wind > 15 mph   evaluate image quality ,close doors if need be, raise wind blind ( A.K.A.: windscreen ) 

BEWARE PLEASE: Don't permit observing beyond these limits! If you have trouble to be heard by the astronomer, please REPORT it (so we can politely explain the rules).

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1.2. Dome opening:

The dome AND the mirror cover have to be opened 1 hour before sunset, orienting the shutter eastward to make sure no direct sunlight will enter the dome. Dome and mirror cover have to be closed at the end of the night.

 

1.3. Lateral sliding doors opening:

These doors have to be opened just after sunset and left opened all night.

• If the wind > 15 mph on average, evaluate the image quality to decide whether to close them or not (elongated images mean you have to close the doors).
• If wind > 25 mph on average, ABSOLUTE closure (because of wind-shake on the telescope and deposit of dust).

 

1.4. Primary mirror cooling:  

• The Primary mirror cooling system is now running automatically        
• Let's recall that a 1° temperature difference between the mirror surface and the ambient air will create additional mirror-seeing (typically up to 0.5" extra for 1° difference). Thus our goal is to maintain the mirror temperature within 1° of the predicted temperature of the following night.

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During the night, you are invited to check  Blanco ECS Telemetry [6] and check that:

• the 4 sensors of the mirror are within a 0.5-1° range
• the mirror temperature, dome temperature and outside temperature are within a 1° range
• Any problems detected should be reported by email.
• The mirror cooling should NOT be turned off for instrument change unless you are really freezing to death. If ever you do turn it off, DON'T FORGET to turn it back on!
• The Blanco ECS [2] automatically controls the mirror temperature according to the following logic: where Tgoal is the lower of Tlow_dome and Toutside

1/ Tmirror < Tgoal - 2.5° : glycol valve closed (but ambient air is still blown onto the mirror)

2/ Tgoal + 1.7° < Tmirror < Tgoal -2.5°: glycol valve partially opened

3/ Tmirror > Tgoal + 1.7 ° : glycol valve fully opened

4/ If Tmirror < Tdew_point + 7 ° : the glycol valve will close (safe limit to prevent condensation)

 

1.5. Floor cooling and stirring fan on main floor (M):

The cooling of the C floor and M floor in the dome is always ON. It is currently regulated automatically

The large stirring fan on the M floor (inside the dome) should always be ON when the dome is closed and OFF when the dome is opened. This fan improves greatly the air circulation inside the dome. It can be turned off during instrument change or any other works around the telescope if the noise bothers you. But turn it back on when you are done!

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1.6. Oil cooler:

The cooling of the oil circulating under the R.A. rear and front pads is activated automatically when the pumps are turned ON by Observer support at sunset. The oil glycol valve is controlled (range is 1-2.25 V) by an equation involving the low dome and oil glycol temperature sensors. It is important that the oil cooling be working: if it is not, you can diagnostic it in ECS Telemetry [6] (the "before pad" and "glycol" entries on the OIL line will quickly indicate around 30°).

 

1.7. Chimney fans:   Not in use..TBD!!!

These fans are located inside the chimney at the level of the primary mirror and suck ambient air into the mirror cell so as to form a laminar downward flow in the chimney. This is to prevent Cass cage heat sources from creating convection in the light path in the chimney.

At Cassegrain foci (f/8), Observer Support has to turn ON the chimney fans before sunset. The switch is on the power supply on the old console room desk. The night assistant must turn it OFF at the end of the night.

1.8. Dome Cooling : The AHU blowers.

These units are located inside de dome.The East unit  is on the roof ( elevator )  and the West unit close to stairs to M floor.
Both units must be turned ON at opening time and turned off at the end of the night.

1.9. Air conditioning:

The current thermal plan in the building is not changed. Always leave the air conditioning at full power. Do not use heat sources at level M, MZ and C. Always maintain the doors closed in the passageways (especially the glass door in front of the lift at GR floor, the cryocooler compressor and pump rooms). In general, respect the signs in the building.

 

 Temperatures and Weather Conditions 

Use ECS Telemetry [6] for temperatures and Environmental Web Page [1] for weather conditions . We are working on a web page for thermal related issues. [9]

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2. Brief reminder of known optical problems

The image quality of the telescope can suffer deterioration mainly from 3 optical problems:

 

2.1. Astigmatism

 This is due to tiny slippage of M1 and/or deformation under its own gravity. Astigmatism will show up as elongated images, perpendicular on each side of the focus, especially for large H.A. (typically more than 2 hours). We compensate that with a lookup table, which controls the pressure in the air bags under M1. Thus the TCP toggle "CORR" should always be ON, at all foci. Note that if the F/8 secondary mirror lose its vacuum, strong astigmatism will immediately show up (typically 2-4 microns as measured by iman).

 

2.2. Coma

This aberration shows up in 2 cases: at Prime Focus if the primary mirror axis is not aligned with the PFADC and in the 2-mirror configuration (f/8) when there is a misalignment between them. Coma produces images with a flare (a tail like a comet) which is identical (same amplitude and direction) on each side of the focus.

At Prime Focus, we don't have a "quick-fix" tool to correct coma so any problem need to be reported (it hasn't happened, though).

Coma usually increases the further you go from the optical axis -this is called "field coma" and is normal (it is always supposed to be 0 on axis)- and also shows up when the optical axis of M1 and M2 are not coaligned -this is called "decentering coma" and is abnormal-. Our f/8 is a Ritchey-Chretien (RC) type, which means it is optically designed to correct the field coma. If the telescope is properly aligned there should not be any visible coma at f/8. If coma shows up anywhere in the field (it would usually be constant all over the field), there is a mirror misalignment and this can be corrected by using IMAN.

IMAN detailed instructions are on the web at Instructions for normal use and in the written manual next to the TCP ("User documentation: active optics system").

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2.3. Defocus

Thermal expansion that can occur at night will cause the telescope to defocus. The prime focus changes at a rate of -110 microns/°C, the f/8 focus at -780microns/°C. The actual movement of He f/8 mirror is a factor 10 less (i.e. -78 microns/°C)

Use Blanco ECS Sensors Diagram [7] to check the Serrurier truss temperature and adjust the focus accordingly.

 

 

 

3. Prime Focus nights:

* CORR ON all the time.

* Temperature drift compensation:

Focus number increases when focal plane moves away from M1

Focus number is in microns neglecting the effect of the PFADC [10] (the PFADC has a power of 1.076, i.e. multiply the focus change by 1.076 to get the real motion in microns in the focal plane).

Decrease focus setting by 110 units per 1° increase in temperature

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4. f/8 nights:

* CORR ON all the time.

* M2 Corrections ON all the time 

* Note from Manuel Martinez : Before turning M2 Corrections OFF move telescope at zenith with Corrections ON when telescope gets there turning corrections OFF.To keep the nominal values at zenith.

 

* Temperature drift compensation:

Focus number increases when focal plane (and M2) moves up

The focus number represents microns of motion of the focal plane (not of M2)

Decrease focus setting 780 units per 1° increase in temperature

 

*Collimation:this has to be checked according to the following procedure:

• On the first night of a f/8 run, check in the TCS the tilt value (amplitude and azimuth) written on the white board and in the logbook. If this is not the case, choose /Absolute_Tilt and enter the right values. Next, run IMAN according to the instructions in the IMAN instruction book (a version is also available on the web). Write the new tilt values on the white board and in the logbook.
• At the beginning of each following night of the f/8 run, check tilt value as described above and correct with /Absolute_Tilt if necessary.

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The images are automatically stored in the appropriate archive.

One image should be taken at the beginning of the night, after doing the telescope zpoint and focussing the instrument. ). The spectro mode of Osiris needs to be focused in the imaging mode (both modes are parfocal), thus it is easy to take that first seeing sequence.

A second image should be taken by the time it is 1 hour before morning twilight, preferably after the focus has been rechecked. If Osiris is used in spectro mode, you obviously need to change back to imaging mode to take this second seeing frame.

In case some problems forced you to start late (i.e. after 11PM), only a single measurement will be required.

For the time being, no seeing measurement is required with IRS. In the near future, we hope to do the seeing measurement with the Tip-Tilt camera for all IR instruments.

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Blanco 4-m Daily Procedures - Environmental Control

• The mirror cooling should NOT be turned off for instrument change except for safety reasons. That is, if the noise or temperature is such that you are likely to make a mistake. If ever you do turn it off, DON'T FORGET to turn it back on!
   
• The temperature control system automatically controls mirror temperature according to the following logic:
  1. T_mirror < T_goal - 2.5°: glycol valve closed (but ambient air is still blown onto the mirror)
  2. T_goal + 1.7° < T_mirror < T_goal -2.5°: glycol valve partially opened
  3. T_mirror > T_goal + 1.7°: glycol valve fully opened
  4. If T_mirror < T_{dew_point} + 7°: the glycol valve will close (safe limit to prevent condensation)
   
• The cooling of the C floor and M floor in the dome is always ON. It is currently regulated automatically
   
• The large stirring fan on the M floor (inside the dome) should always be ON when the dome is closed and OFF when the dome is opened. This fan improves greatly the air circulation inside the dome. It can be turned off during instrument change or any other works around the telescope if the noise bothers you. But turn it back on when you are done!
   
• Oil Cooling: The cooling of the oil circulating under the R.A. rear and front pads is activated automatically when the pumps are turned ON by Observer support at sunset. The oil glycol valve is controlled (range is 1-2.25 V) by an equation involving the low dome and oil glycol temperature sensors. It is important that the oil cooling be working: if it is not, you can diagnostic it in Blanco ECS [6] and OIL COOLING SCHEMA [11] (the "before pad" and "glycol" entries on the OIL line will quickly indicate around 30°).
   
• The Chimney Fans are located inside the chimney at the level of the primary mirror and suck ambient air into the mirror cell so as to form a laminar downward flow in the chimney. This is to prevent Cass cage heat sources from creating convection in the light path in the chimney. At all Cassegrain foci (f/8), Observer Support is to turn ON the chimney fans before sunset. The switch is on the power supply on the old console room desk. The night assistant must turn it OFF at the end of the night.Not in use at the moment..TBD
   
• Air conditioning - Always leave on. Do not use heat sources at level M, MZ and C. Always keep passageway doors closed, especially the glass oor in front of the lift at GR floor, the cryocooler compressor and pump rooms). In general, respect the signs in the building.

Calculating the risk of condensation

Each material has its own radiation cooling property (which is not easy to calculate by the way). Just know that if there is no wind, the radiation cooling is low and surfaces will not equilibrate thermally with the ambient temperature very quick. Also, a surface, even with moderate ability to radiate, looking into a "cold" sky can cool down several degrees below ambient temperature. Fortunately, a mirror radiates very little. Nevertheless, when cooling the mirror during the day, the mirror temperature is usually several degrees below ambient temperature and there are risk of condensation. The control loop will turn off the cooling when the difference between the mirror temperature and the dew point shrinks to only 2 degrees.

Knowing the Relative Humidity (RH in %) and the ambient temperature (T_a) of the air, one can calculate the dew point temperature (T_d) and determine whether a surface at temperature T_s can become wet or not :

• if T_s<T_d: surface becomes wet
• if T_s>T_d: surface keeps dry

I think "dew point" refers only to the case where RH=100%; when RH<100% we might have to talk about condensation point. We won't do that distinction anymore in the text.

How to use the table?

From your ambient temperature on the X-axis, go up to intersect the curve corresponding to the RH, then move horizontally onto the left to read the dew point on the Y-axis. You can then check if your surface is hotter or colder than this dew point value.

Example: Ta is 10°C, RH is 80%, Td is 6.5°C. So a 5°C mirror would be wet!

[12]

 

Calculation of dew point:

• The dew point is the temperature at which the partial pressure of ambient air (PA) is equal to the partial pressure of saturated water vapour (PS).
• The pressure of saturated water vapour is tabulated versus temperature at sea level in thermodynamic books. Numbers from -10 to +35°C are used to determine empirically the relation PS = f(T) and adjust it for Tololo's elevation.

PS = (5.10^-7.T³ + 10^-5.T² + 5.10^-4.T + 0.0061) / 1.294

•  PV = RH * PS where RH is between 0 and 1
• We can then empirically determine T_d = g(PV) for different values of RH with the following equation:

T_d = 6.10⁸.PV⁵ - 10⁸.PV⁴ + 6.10⁶.PV³ - 193789.PV² + 3957.9.PV -14.911

•   The fit is quite good, yielding accuracy for Td of less then 0.3°between 0 and 20°C.