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| = Telescope System Status = | |
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| ''(Date 2004-12-01)'' |
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| NORMAL OPERATION | The 30-m telescope is now operating using the New Control System (NCS) (2005-11-30 HU) [http://www.iram.es/IRAMES/ncs30m/ NCS documentation] [http://mrt-lx1/mainWiki/ Wiki with up-to-date Notes on NCS] NCS supports only source coordinates in Equatorial J2000.0 system. (More systems will be made available as soon as possible) Observations near and towards the Sun are not yet supported. NCS supports observing modes and source offsets in: * Projection "Radio" (same offsets as in old CS) in Equatorial J2000.0 * "true angle" horizontal * Nasmyth (receiver offsets) All 4 Switching Modes are supported by the NCS (total power, beam switching, wobbler switching, frequency switching.) * (./) Observations with "rotated" wobbler and the bolometer are now possible within the pool; contact the pool manager, Stephane Leon, on how to prepare such observations. After finishing with rotated Wobbler, make sure that the operator puts the rotation back to '''exactly 0 degrees'''. Observing modes supported by the NCS: * Calibrate (for heterodyne) * Pointing * Focus * Tip * Track * Frequency Switching * ON-OFF * Position Switching * Wobbler Switching * On-The-Fly Map * Heterodyne * Total Power (like Position Switching) * Frequency Switching * Bolometer * Wobbler Switching * VLBI (./) Automatic calibration and processing of heterodyne data using the MIRA software is in operation for all observing modes. MIRA can also be used manually and offline. /!\ Online data processing, in some circumstances, still may have problems with scans extending over midnight. Please check data and report problems to Albrecht Sievers. It may be safer to avoid long scans extending over midnight. |
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| OK | (./) OK /!\ On 30.10.2007 the GISMO bolometer has been installed. It is in the beam of single pixel or HERA observation for all declinations smaller than 25 degrees. There is no alarm, so astronomers should be aware of this (RM 30.10.2007) |
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| Avoid wobbler throw of 120"; with a throw of 120" the specification of a phase time may not work properly. With a throw of 119 or 121 is should be OK. (2003-07-09) Results from first pointing after unlocking the wobbler can be wrong! Usually it's sufficient to ignore the first pointing and repeat the pointing (2003-07-09) Wobbler rotation implemented. Current range: +/- 60deg (2004-12-01 AW) [#beginOfPage Back to top] == Pointing Model == heterodyn: OK (last model update: 2004-11-17 ). bolometer: OK (last model update: 2004-11-02 ). Operator/AOD: Check regularly that automatic P4 P5 is working (2002-12-13). Narrowband continuum pointing (for SiO masers) is out of service! (2003-07-09, 2003-07-30) |
Available under NCS. [#beginOfPage Back to top] == Pointing Model and Focus == The Pointing Model is maintained with respect to the receiver B100. The misalignment and focus error (D-focus) of the other receivers with respect to B100 is the following: {{{ Rx misal.(") date D_focus(mm) date A100 0.16 ±0.06 27-Feb-07, +0.09 ±0.03 13-Mar-07 A230 1.34 ±0.18 27-Feb-07, +0.43 ±0.02 13-Mar-07 B100 0.00 0.00 B230 1.74 ±0.16 27-Feb-07, +0.40 ±0.10 17-Apr-07 C150 1.26 ±0.24 5-Feb-07, +0.64 ±0.13 17-Apr-07 C270 0.78 ±0.18 5-Feb-07, +0.36 ±0.15 17-Apr-07 D150 1.03 ±0.13 12-Mar-07, +0.26 ±0.02 12-Mar-07 D270 1.40 ±0.19 12-Mar-07, +0.18 ±0.05 12-Mar-07 }}} heterodyne: last model update: 2007-10-23, 40 points, previous rms = 3.44", new rms = 1.69" bolometer: last model update: 2007-11-16, 36 points, new rms < 1.5" /!\ Pointing on spectral line sources like SiO masers is not yet supported by the data processing. |
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| A, B, C and D receivers are aligned within 3", checked (2003-09-24) Calibration Tcold temperatures have been checked by receiver group. New scaling factor of 1.0 has been implemented into obs. Obs Tcold should be ok (2004-01-17) |
(./) A, B, C, D receivers are supported by NCS for observations. (./) Image/Signal gain-ratio calibration is supported by NCS. (./) A standard table of T_cold calibration temperatures for A, B, C, D receivers is implemented in NCS. This built-in table covers most frequencies. /!\ Outside this range, T_cold has to be set manually. /!\ Note that the tables and plots at [http://gra-lx1.iram.es/mainWiki/ReceiverGroupColdloadPlots] appear to be out of date! /!\ Tables and plots are now at [http://gra-lx1/mainWiki/ReceiverGroupColdLoadPlotsCurrent] 2007-10-11 dj /!\ Receiver C150 shows low continuum signal at the higher frequencies (>168 GHz). It has to be fully checked. Use D150 instead. (2005-11-16) '''Note: the last 2 points need to be checked and maybe corrected by the RX group!''' [#beginOfPage Back to top] == HERA == (./) HERA is supported by the NCS. (2006-02 HU) Second polarization installed. [[BR]] (./) One previously blind pixel is now fixed (2006-04). [[BR]] SSB tuning tables for standard frequencies. [[BR]] Sideband rejections not determined (2004-12-01 AW). Use standard value of 0.1! [[BR]] (./) For HERA calibration, measured values of the load temperatures are automatically used! /!\ Watch the computer control of the derotator closely (2002-12-22). [[BR]] /!\ Make sure the derotator tracking is stopped after observations, i.e., set to zero degrees in "frame". [[BR]] /!\ The automatic tuning of both HERA1 and 2 can be improved by manually changing the mixer current according to DJ; HERA Pool managers should be aware of this, and operators will receive training (2007-09-19 RM) HERA 2 is more noisy than HERA 1, limiting HERA2's useful frequency range to below about 242 GHz (2006-09-27 HU according to info from SN)[[BR]] '''Note: these comments on HERA need to be checked and, if necessary, corrected by the RX group!''' |
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| Continuum instability ("ripple") can occur with all receivers, making pointing and focussing difficult. In general some receivers are better then others in this respect as summarized here: A100 generally OK for pointing. (2003-11-12) B100 OK, will be replaced (2003-11-12) C150 often bad for pointing, ripple. (2002-07-16) D150 generally good performance for pointing.(2002-07-16) A230 often unstable, bad for pointing and flux monitoring. (2003-11-12) B230 OK, will be replaced (2003-11-12) C270 very bad for pointing at 265 Ghz. (2002-07-16) D270 can be unstable and difficult for pointing. (2002-07-16) HERA pointing difficulties using beam switch mode - total power mode gave better results (2004-01-17) [#beginOfPage Back to top] == HERA == Second polarization installed. One blind pixel. No SSB tuning tables except for few standard frequencies. Sideband rejections not determined (2004-12-01 AW) Watch the computer control of the derotator closely (2002-12-22). Make sure the derotator tracking is stopped after observations, i.e, set to zero degrees in "frame". With VESPA, only two spectra per pixel can be used. [#beginOfPage Back to top] |
Continuum instability ("ripple") can occur with all receivers, making pointing and focusing difficult. In general some receivers are better than others in this respect as summarized here: A100 generally OK for pointing. (2003-11-12) [[BR]] B100 OK, is best for pointing. B100 is the standard reference for the heterodyne pointing model[[BR]] /!\ C150 often bad for pointing, ripple. (2002-07-16) [[BR]] D150 generally good performance for pointing.(2002-07-16) [[BR]] /!\ A230 often unstable, bad for pointing and flux monitoring. (2003-11-12) [[BR]] B230 OK [[BR]] /!\ C270 can be unstable and difficult for pointing. (2007-04-30) [[BR]] /!\ D270 can be unstable and difficult for pointing. (2002-07-16) [[BR]] With HERA pointing may be difficult using beam switch mode - total power mode may give better results but requires excellent weather [[BR]] [#beginOfPage Back to top] |
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| Mambo II is installed and ready for operation (AW 2004-12-01) | (./) Bolometer Observations are supported by the NCS. Mambo1: OFFLINE /!\ Mambo2: has been removed to install Gismo (RM 30.10.2007) Mambo2 was re-installed and commissioned the week 13.11.2007/20.11.2007 |
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| 256 MHz shift in 100kHz FB header (AW 2004-12-01) Software and/or hardware problem in the 1MHz FB - problem is currently investigated (AW 2004-12-01) Spikes in VESPA at intersection of different units (AW 2004-12-01) |
Support by NCS: * (./) Continuum Backends for heterodyne receivers * (./) 4 MHz Filterbanks * (./) 1 MHz Filterbank in parts of 256, 512, 768, or 1024 channels * (./) WILMA for observations with HERA * (./) VESPA * (./) ABBA for MAMBO bolometer * /!\ the 100 kHz Filterbank is decommissioned. (RM, HU, 19.9.2007) |
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| Mirroring between IRAM Grenoble ( http://www.iram.fr ) and Granada( http://www.iram.es/ ) websites sometimes takes several days to update. (2003-07-01) | /!\ The 30-m telescope is now operating using the New Control System (NCS) (2005-11-30 HU). Note that the NCS supports most essential features, but still has some limitations! See the NCS documentation for details, in particular links from the Wiki [https://mrt-lx1.iram.es/mainWiki/OperationNotesObservers NCS Operation Notes for Observers] /!\ Online data processing, in some circumstances, still may have problems with scans extending over midnight. Please check data and report problems to Albrecht Sievers. It may be safer to avoid long scans extending over midnight. |
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| OK | * (./) Remote observing via ''VNC'' is available from Granada, Grenoble, and Bonn. Coordinate with Walter Brunswig. |
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| ''(in reverse order by date!)'' 2004-12-01 AW [[BR]] 2004-07-24 RM [[BR]] 2004-03-24, 25 HU [[BR]] 2004-01-17 AW [[BR]] 2003-11-12 HU [[BR]] 2003-09-25 MR [[BR]] 2003-09-08 HU [[BR]] 2003-08-20 HU [[BR]] 2003-08-05 AS [[BR]] 2003-07-09 RM [[BR]] 2003-07-01,04/5, 7 HU [[BR]] 2003-06-08, 09 HU [[BR]] 2003-04-22, 26 HU [[BR]] 2003-04-06 AS [[BR]] 2003-03-31 HU [[BR]] 2003-03-20 RM [[BR]] 2003-02-11 AW [[BR]] 2003-01-10, 2003-01-17, 2003-02-05 RM [[BR]] 2003-01-14 TG [[BR]] 2003-01-03, 06 HU [[BR]] 2002-12-31 HU [[BR]] 2002-12-21, 22 HU [[BR]] 2002-12-19 RM [[BR]] 2002-12-13, 14, 15, 16 HU [[BR]] 2002-12-11 RM [[BR]] 2002-12-05 TG [[BR]] 2002-11-27 RM [[BR]] 2002-11-05 AW [[BR]] 2002-10-18 DJ [[BR]] 2002-10-15 DJ [[BR]] 2002-10-09, 12, 14 HU [[BR]] 2002-10-08 AW [[BR]] 2002-09-27 TG [[BR]] 2002-09-26 DJ [[BR]] 2002-09-23 AW [[BR]] 2002-09-11/12, 17 HU [[BR]] ... (?) [[BR]] 2002-08-07,10 HU [[BR]] 2002-07-22 DJ [[BR]] ... (?) [[BR]] 2002-07-16 HU [[BR]] ... (?) [[BR]][[BR]] [#beginOfPage Back to top] '''Created by R. Mauersberger, June 18th, 2002''' |
To see the changes between the actual and the last version, please see '''''Show Changes''''' in the Wiki Interface. If you want to see the Revision History of this page, please see '''''Get Info''''' in the Wiki Interface. [#beginOfPage Back to top] == Legend == (./) : OK[[BR]] /!\ : Warning[[BR]] {X} : Error[[BR]] The wiki markup of these icons is: {{{(./) : OK /!\ : Warning {X} : Error }}} [#beginOfPage Back to top] |
System - General
The 30-m telescope is now operating using the New Control System (NCS) (2005-11-30 HU)
[http://www.iram.es/IRAMES/ncs30m/ NCS documentation]
[http://mrt-lx1/mainWiki/ Wiki with up-to-date Notes on NCS]
NCS supports only source coordinates in Equatorial J2000.0 system. (More systems will be made available as soon as possible)
Observations near and towards the Sun are not yet supported.
NCS supports observing modes and source offsets in:
- Projection "Radio" (same offsets as in old CS) in Equatorial J2000.0
- "true angle" horizontal
- Nasmyth (receiver offsets)
All 4 Switching Modes are supported by the NCS (total power, beam switching, wobbler switching, frequency switching.)
Observations with "rotated" wobbler and the bolometer are now possible within the pool; contact the pool manager, Stephane Leon, on how to prepare such observations. After finishing with rotated Wobbler, make sure that the operator puts the rotation back to exactly 0 degrees.
Observing modes supported by the NCS:
- Calibrate (for heterodyne)
- Pointing
- Focus
- Tip
- Track
- Frequency Switching
- ON-OFF
- Position Switching
- Wobbler Switching
- On-The-Fly Map
- Heterodyne
- Total Power (like Position Switching)
- Frequency Switching
- Bolometer
- Wobbler Switching
- Heterodyne
- VLBI
Automatic calibration and processing of heterodyne data using the MIRA software is in operation for all observing modes. MIRA can also be used manually and offline.
 date D_focus(mm) date
A100 0.16 ±0.06 27-Feb-07, +0.09 ±0.03 13-Mar-07
A230 1.34 ±0.18 27-Feb-07, +0.43 ±0.02 13-Mar-07
B100 0.00 0.00
B230 1.74 ±0.16 27-Feb-07, +0.40 ±0.10 17-Apr-07
C150 1.26 ±0.24 5-Feb-07, +0.64 ±0.13 17-Apr-07
C270 0.78 ±0.18 5-Feb-07, +0.36 ±0.15 17-Apr-07
D150 1.03 ±0.13 12-Mar-07, +0.26 ±0.02 12-Mar-07
D270 1.40 ±0.19 12-Mar-07, +0.18 ±0.05 12-Mar-07heterodyne: last model update: 2007-10-23, 40 points, previous rms = 3.44", new rms = 1.69"
bolometer: last model update: 2007-11-16, 36 points, new rms < 1.5"
Pointing on spectral line sources like SiO masers is not yet supported by the data processing.
[#beginOfPage Back to top]
SIS Receivers
A, B, C, D receivers are supported by NCS for observations.
Image/Signal gain-ratio calibration is supported by NCS.
A standard table of T_cold calibration temperatures for A, B, C, D receivers is implemented in NCS. This built-in table covers most frequencies. Outside this range, T_cold has to be set manually.
Note that the tables and plots at [http://gra-lx1.iram.es/mainWiki/ReceiverGroupColdloadPlots] appear to be out of date!
Tables and plots are now at [http://gra-lx1/mainWiki/ReceiverGroupColdLoadPlotsCurrent] 2007-10-11 dj
Receiver C150 shows low continuum signal at the higher frequencies (>168 GHz). It has to be fully checked. Use D150 instead. (2005-11-16)
Note: the last 2 points need to be checked and maybe corrected by the RX group!
[#beginOfPage Back to top]
HERA
HERA is supported by the NCS. (2006-02 HU)
Second polarization installed. BR One previously blind pixel is now fixed (2006-04). BR SSB tuning tables for standard frequencies. BR Sideband rejections not determined (2004-12-01 AW). Use standard value of 0.1! BR
For HERA calibration, measured values of the load temperatures are automatically used!
Watch the computer control of the derotator closely (2002-12-22). BR Make sure the derotator tracking is stopped after observations, i.e., set to zero degrees in "frame". BR
The automatic tuning of both HERA1 and 2 can be improved by manually changing the mixer current according to DJ; HERA Pool managers should be aware of this, and operators will receive training (2007-09-19 RM)
HERA 2 is more noisy than HERA 1, limiting HERA2's useful frequency range to below about 242 GHz (2006-09-27 HU according to info from SN)BR
Note: these comments on HERA need to be checked and, if necessary, corrected by the RX group!
[#beginOfPage Back to top]
Pointing and Flux monitoring with SIS receivers:
Continuum instability ("ripple") can occur with all receivers, making pointing and focusing difficult.
In general some receivers are better than others in this respect as summarized here:
A100 generally OK for pointing. (2003-11-12) BR B100 OK, is best for pointing. B100 is the standard reference for the heterodyne pointing modelBR
C150 often bad for pointing, ripple. (2002-07-16) BR D150 generally good performance for pointing.(2002-07-16) BR A230 often unstable, bad for pointing and flux monitoring. (2003-11-12) BR B230 OK BR C270 can be unstable and difficult for pointing. (2007-04-30) BR D270 can be unstable and difficult for pointing. (2002-07-16) BR With HERA pointing may be difficult using beam switch mode - total power mode may give better results but requires excellent weather BR
[#beginOfPage Back to top]
Bolometers
Bolometer Observations are supported by the NCS.
Mambo1: OFFLINE
Mambo2: has been removed to install Gismo (RM 30.10.2007)
Mambo2 was re-installed and commissioned the week 13.11.2007/20.11.2007
[#beginOfPage Back to top]
Backends
Support by NCS:
- Continuum Backends for heterodyne receivers
- 4 MHz Filterbanks
- 1 MHz Filterbank in parts of 256, 512, 768, or 1024 channels
- WILMA for observations with HERA
- VESPA
- ABBA for MAMBO bolometer
- the 100 kHz Filterbank is decommissioned. (RM, HU, 19.9.2007)
[#beginOfPage Back to top]
Computer/Software
The 30-m telescope is now operating using the New Control System (NCS) (2005-11-30 HU). Note that the NCS supports most essential features, but still has some limitations! See the NCS documentation for details, in particular links from the Wiki [https://mrt-lx1.iram.es/mainWiki/OperationNotesObservers NCS Operation Notes for Observers]
Online data processing, in some circumstances, still may have problems with scans extending over midnight. Please check data and report problems to Albrecht Sievers. It may be safer to avoid long scans extending over midnight.
[#beginOfPage Back to top]
Other Items
- Remote observing via VNC is available from Granada, Grenoble, and Bonn. Coordinate with Walter Brunswig.
[#beginOfPage Back to top]
Updates/History
To see the changes between the actual and the last version, please see Show Changes in the Wiki Interface. If you want to see the Revision History of this page, please see Get Info in the Wiki Interface.
[#beginOfPage Back to top]
Legend
The wiki markup of these icons is:
{{{(./) : OK : Warning 
: Error }}}
[#beginOfPage Back to top]