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##language:en
#pragma section-numbers off
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= Telescope System Status =
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''(Date 2004-12-01)''  This page provides information on the __status__ of the 30m telescope for the __visiting astronomers__. The IRAM staff tries to keep this page up to date as much as possible. It may however happen that some information is outdated. Please contact the __Astronomer of Duty or the Operator__ in case of doubt. Note that the present instrumentation and software at the telescope is summarized here: [http://www.iram.es/IRAMES/telescope/telescopeSummary/telescope_summary.html Telescope Summary]
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The 30-m telescope runs under the New Control System (NCS), see:
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NORMAL OPERATION  . [http://www.iram.es/IRAMES/ncs30m/ NCS documentation] [http://mrt-lx1/mainWiki/ Wiki with up-to-date Notes on NCS]
The 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.

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:

 * total power
 * beam switching
 * wobbler switching
 * frequency switching
Observations with "rotated" wobbler and the bolometer are 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:

 * 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.
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OK		 (./) OK
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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)		 (./) OK
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== Pointing Model == == Heterodyne Pointing Model and Focus ==
The Pointing Model is maintained with respect to the 3mm receiver B100. The misalignment and focus error (D-focus) of the other receivers with respect to B100 is the following:
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heterodyn: OK (last model update: 2004-11-17 ).
bolometer: OK (last model update: 2004-11-02 ).		 {{{
  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: 2008-06-25, 29 points, previous rms = 2.58", new rms = 1.97"
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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)

[#beginOfPage Back to top]
 
== SIS Receivers ==

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)		 /!\ Pointing on spectral line sources like SiO masers is not yet supported by the data processing.
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== Pointing and Flux monitoring with SIS receivers: == == Bolometer Pointing Model ==
bolometer: last model update: 2007-12-19, 46 points, previous rms = 2.33", new rms = 1.75"
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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:		 [#beginOfPage Back to top]
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    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)		 == SIS Receivers A, B, C, D ==
Image/Signal gain-ratio calibration is supported by NCS, processing in MIRA. It is highly recommended to use this feature!

A standard table of T_cold calibration temperatures for A, B, C, D receivers is implemented in the NCS. This built-in table covers most frequencies. /!\ Outside this range, T_cold has to be set manually, ask the RX engineers or operators! Tables and plots:

 . 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)
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Second polarization installed. One blind pixel.
No SSB tuning tables except for few standard frequencies.
Sideband rejections not determined (2004-12-01 AW)		 HERA is a HEterodyne REceiver Array, a 3x3 dual polarisation array in the 1.2mm band
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 * SSB (Single side band) tuning tables for standard frequencies.
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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.		  * Sideband rejections not determined (2004-12-01 AW). Use standard value of 0.1!

 * /!\ For HERA calibration, measured values of the load temperatures are automatically used!

 * /!\ 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".

 * /!\ 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)

 * /!\ The control software does not yet support connecting HERA2 to the 4MHz backend (2008-08-29 wb). Note that paKo does not issue any warning. (ck)
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== Pointing with SIS receivers A, B, C, D and HERA ==
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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Mambo1 is OFFLINE
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Mambo II is installed and ready for operation (AW 2004-12-01) Mambo2 was re-installed and commissioned the week 13.11.2007/20.11.2007 (AS)
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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)
  * Continuum Backends
 * 4 MHz Filterbanks, note: cannot yet be used with HERA2
 * 1 MHz Filterbank in parts of 256, 512, 768, or 1024 channels
 * WILMA for observations with HERA
  . /!\ Out of operation for 2 o 3 weeks. Hardware upgrade to new broadband receivers (JLS, GP, 05.06.2008)
 * VESPA
 * ABBA for MAMBO bolometer
 * /!\ the 100 kHz Filterbank is decommissioned. (RM, HU, 19.9.2007)
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/!\ The NCS supports most essential features, but still has some limitations; see the documentation for details. (see links above)
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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) /!\ Online data processing, in a few 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.

/!\ Pako does not run under the default gildas version on mrt-lx3, mrt-lx2. Use '''gag_aug06''' before starting '''pako''' (2008-01-15 AS). [[BR]] ''Note: the instructions to start pako explicitly say to run it on mrt-lx1. The trick suggested by AS for mrt-lx2, mrt-lx3 may work, but it is not guaranteed.''

/!\ Data processing on mrt-lx3 might affect the system performance and slow down the observing system. Observations have priority over any other activity and data processing on mrt-lx3 shall be stopped in this case. Users might try to do dataprocessing on mrt-lx2 in this case. If the observing system is still affected the data processing shall be stopped.(2008-08-29 wb)
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OK		 Remote observing via ''VNC'' is available from Granada, Grenoble, Madrid, and Bonn. See https://mrt-lx1.iram.es/mainWiki/RemoteObserving
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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]]		 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.
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'''Created by R. Mauersberger, June 18th, 2002''' == Legend ==
(./) : OK[[BR]] /!\ : Warning[[BR]] {X} : Error[[BR]]

The wiki markup of these icons is:

{{{
(./) : OK
/!\ : Warning
{X} : Error
}}}
[#beginOfPage Back to top]

Anchor(beginOfPage)

  • This page provides information on the status of the 30m telescope for the visiting astronomers. The IRAM staff tries to keep this page up to date as much as possible. It may however happen that some information is outdated. Please contact the Astronomer of Duty or the Operator in case of doubt. Note that the present instrumentation and software at the telescope is summarized here: [http://www.iram.es/IRAMES/telescope/telescopeSummary/telescope_summary.html Telescope Summary]

TableOfContents(3)

System - General

The 30-m telescope runs under the New Control System (NCS), see:

The 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.

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:

  • total power
  • beam switching
  • wobbler switching
  • frequency switching

Observations with "rotated" wobbler and the bolometer are 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:

  • 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.

[#beginOfPage Back to top]

Antenna

(./) OK

[#beginOfPage Back to top]

Wobbler

(./) OK

[#beginOfPage Back to top]

Heterodyne Pointing Model and Focus

The Pointing Model is maintained with respect to the 3mm 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: 2008-06-25, 29 points, previous rms = 2.58", new rms = 1.97"

/!\ Pointing on spectral line sources like SiO masers is not yet supported by the data processing.

[#beginOfPage Back to top]

Bolometer Pointing Model

bolometer: last model update: 2007-12-19, 46 points, previous rms = 2.33", new rms = 1.75"

[#beginOfPage Back to top]

SIS Receivers A, B, C, D

Image/Signal gain-ratio calibration is supported by NCS, processing in MIRA. It is highly recommended to use this feature!

A standard table of T_cold calibration temperatures for A, B, C, D receivers is implemented in the NCS. This built-in table covers most frequencies. /!\ Outside this range, T_cold has to be set manually, ask the RX engineers or operators! Tables and plots:

/!\ Receiver C150 shows low continuum signal at the higher frequencies (>168 GHz). It has to be fully checked. Use D150 instead. (2005-11-16)

[#beginOfPage Back to top]

HERA

HERA is a HEterodyne REceiver Array, a 3x3 dual polarisation array in the 1.2mm band

  • SSB (Single side band) tuning tables for standard frequencies.
  • Sideband rejections not determined (2004-12-01 AW). Use standard value of 0.1!

  • /!\ For HERA calibration, measured values of the load temperatures are automatically used!

  • /!\ 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".

  • /!\ 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)

  • /!\ The control software does not yet support connecting HERA2 to the 4MHz backend (2008-08-29 wb). Note that paKo does not issue any warning. (ck)

[#beginOfPage Back to top]

Pointing with SIS receivers A, B, C, D and HERA

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

Mambo1 is OFFLINE

Mambo2 was re-installed and commissioned the week 13.11.2007/20.11.2007 (AS)

[#beginOfPage Back to top]

Backends

  • Continuum Backends
  • 4 MHz Filterbanks, note: cannot yet be used with HERA2
  • 1 MHz Filterbank in parts of 256, 512, 768, or 1024 channels
  • WILMA for observations with HERA

    • /!\ Out of operation for 2 o 3 weeks. Hardware upgrade to new broadband receivers (JLS, GP, 05.06.2008)

  • VESPA
  • ABBA for MAMBO bolometer

  • /!\ the 100 kHz Filterbank is decommissioned. (RM, HU, 19.9.2007)

[#beginOfPage Back to top]

Computer/Software

/!\ The NCS supports most essential features, but still has some limitations; see the documentation for details. (see links above)

/!\ Online data processing, in a few 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.

/!\ Pako does not run under the default gildas version on mrt-lx3, mrt-lx2. Use gag_aug06 before starting pako (2008-01-15 AS). BR Note: the instructions to start pako explicitly say to run it on mrt-lx1. The trick suggested by AS for mrt-lx2, mrt-lx3 may work, but it is not guaranteed.

/!\ Data processing on mrt-lx3 might affect the system performance and slow down the observing system. Observations have priority over any other activity and data processing on mrt-lx3 shall be stopped in this case. Users might try to do dataprocessing on mrt-lx2 in this case. If the observing system is still affected the data processing shall be stopped.(2008-08-29 wb)

[#beginOfPage Back to top]

Other Items

Remote observing via VNC is available from Granada, Grenoble, Madrid, and Bonn. See https://mrt-lx1.iram.es/mainWiki/RemoteObserving

[#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

(./) : OKBR /!\ : WarningBR {X} : ErrorBR

The wiki markup of these icons is: 

(./) : OK
/!\ : Warning
{X} : Error

[#beginOfPage Back to top]

TelescopeSystemStatus (last edited 2025-01-25 17:12:49 by msanchez)