|
Size: 6013
Comment:
|
Size: 6290
Comment:
|
| Deletions are marked like this. | Additions are marked like this. |
| Line 3: | Line 3: |
| [[Anchor(beginOfPage)]] | <<Anchor(beginOfPage)>> Note that this page is no longer maintained. It has been replaced by a new page [[http://iram-institute.org/EN/content-page.php?ContentID=58&rub=7&srub=55&ssrub=58&sssrub=0&ssssrub=0|here]]. |
| Line 7: | Line 9: |
| This page summarizes the '''present instrumentation''' installed at the 30m observatory. [[BR]] The current system '''status''' is described [http://www.iram.es/IRAMES/mainWiki/TelescopeSystemStatus on a second page]. | '''This page summarizes the '''present instrumentation''' installed at the 30m observatory. <<BR>> The current system '''status''' is described [[http://www.iram.es/IRAMES/mainWiki/TelescopeSystemStatus|on a second page]] (ck, 7.7.09).''' |
| Line 9: | Line 11: |
| [[TableOfContents(4)]] | ------ ------ ------ <<TableOfContents(4)>> |
| Line 18: | Line 26: |
| * [http://www.iram.es/IRAMES/groups/receiver/receiver.html Web pages of the IRAM/Granada receiver group] | * [[http://www.iram.es/IRAMES/groups/receiver/receiver.html|Web pages of the IRAM/Granada receiver group]] |
| Line 22: | Line 30: |
| Two large field bolometer cameras are installed: '''MAMBO1''' with 37 pixels, and '''MAMBO2''' with 117 pixels ([http://www.mpifr-bonn.mpg.de/div/bolometer/#mamgo MAx-Planck Millimeter BOlometer Array]). Usually MAMBO2 is in use. Both cameras work at 1.2mm wavelength, the HPBW is 11", pixel spacing is 20", and the sensitivity is 1.5mJy. This is the rms after 10 minutes integration (normal bolometric conditions) with skynoise removal. See [http://www.iram.es/IRAMES/mainWiki/MamboWebPage the MAMBO page for details.] | Two large field bolometer cameras are installed: '''MAMBO1''' with 37 pixels, and '''MAMBO2''' with 117 pixels ([[http://www.mpifr-bonn.mpg.de/div/bolometer/#mamgo|MAx-Planck Millimeter BOlometer Array]]). Usually MAMBO2 is in use. Both cameras work at 1.2mm wavelength, the HPBW is 11", pixel spacing is 20", and the sensitivity is 1.5mJy. This is the rms after 10 minutes integration (normal bolometric conditions) with skynoise removal. See [[http://www.iram.es/IRAMES/mainWiki/MamboWebPage|the MAMBO page for details.]] |
| Line 24: | Line 32: |
| [#beginOfPage Back to top] | [[#beginOfPage|Back to top]] |
| Line 37: | Line 45: |
| [#beginOfPage Back to top] | [[#beginOfPage|Back to top]] |
| Line 43: | Line 51: |
| . [http://www.iram.es/IRAMES/ncs30m/ NCS documentation] [http://mrt-lx1/mainWiki/ Wiki with up-to-date Notes on NCS] | . [[http://www.iram.es/IRAMES/ncs30m/|NCS documentation]] [[http://mrt-lx1/mainWiki/|Wiki with up-to-date Notes on NCS]] |
| Line 50: | Line 58: |
| [#beginOfPage Back to top] | [[#beginOfPage|Back to top]] |
| Line 66: | Line 74: |
| * for more details on observing and switching modes, see the section "NCS explained" in the [http://www.iram.es/IRAMES/documents/ncs30mPako/Current/PDF/pako.pdf pako cookbook] | * for more details on observing and switching modes, see the section "NCS explained" in the [[http://www.iram.es/IRAMES/documents/ncs30mPako/Current/PDF/pako.pdf|pako cookbook]] |
| Line 74: | Line 82: |
| * '''Pointing''': Using nearby (within 10 degree) pointing sources, <1" accuracy can be obtained; with absolute ("blind") pointing, the accuracy is about 2" rms, the receivers are aligned within 1.7" (see the [http://www.iram.es/IRAMES/mainWiki/TelescopeSystemStatus Telescope Status page] for current values). Checking the pointing and alignment (using e.g. a planet) is the responsibility of the observer. * '''Focus''': residual errors of <1mm may need correction. There are systematic differences of upto 0.6mm in the focus of the different receivers (cf. [http://www.iram.es/IRAMES/mainWiki/TelescopeSystemStatus Telescope Status page]). The focus is subject to change especially during sunrise and sunset. |
* '''Pointing''': Using nearby (within 10 degree) pointing sources, <1" accuracy can be obtained; with absolute ("blind") pointing, the accuracy is about 2" rms, the receivers are aligned within 1.7" (see the [[http://www.iram.es/IRAMES/mainWiki/TelescopeSystemStatus|Telescope Status page]] for current values). Checking the pointing and alignment (using e.g. a planet) is the responsibility of the observer. * '''Focus''': residual errors of <1mm may need correction. There are systematic differences of upto 0.6mm in the focus of the different receivers (cf. [[http://www.iram.es/IRAMES/mainWiki/TelescopeSystemStatus|Telescope Status page]]). The focus is subject to change especially during sunrise and sunset. |
| Line 83: | Line 91: |
| [#beginOfPage Back to top] | [[#beginOfPage|Back to top]] |
| Line 87: | Line 95: |
| * [http://mrt-lx3.iram.es/tau/meteo-main.php Weather station] | * [[http://mrt-lx3.iram.es/tau/meteo-main.php|Weather station]] |
| Line 92: | Line 100: |
| * [http://mrt-lx3.iram.es/tau/taumeter-main-db.php Taumeter] does regular skydips to inform the observer about the sky transmission near '''225 GHz'''. The local oscillator works at 225GHz. The IF is 1.5GHz and the bandwidth is 0.5GHz. It is a double-sideband Schottky receiver. | * [[http://mrt-lx3.iram.es/tau/taumeter-main-db.php|Taumeter]] does regular skydips to inform the observer about the sky transmission near '''225 GHz'''. The local oscillator works at 225GHz. The IF is 1.5GHz and the bandwidth is 0.5GHz. It is a double-sideband Schottky receiver. |
| Line 94: | Line 102: |
| [#beginOfPage Back to top] | [[#beginOfPage|Back to top]] |
| Line 96: | Line 104: |
| Old [http://www.iram.es/IRAMES/telescope/telescopeSummary/telescope_summary.html Telescope System Summary page of September 07] | Old [[http://www.iram.es/IRAMES/telescope/telescopeSummary/telescope_summary.html|Telescope System Summary page of September 07]] |
Note that this page is no longer maintained. It has been replaced by a new page here.
This page summarizes the present instrumentation installed at the 30m observatory.
The current system status is described on a second page (ck, 7.7.09).
Contents
Frontends
Heterodyne Receivers
EmirforAstronomers : new EMIR (Eight MIxer Receiver)
HeraforAstronomers : HERA 3x3 dual-polarisation 1mm receiver
AbcdforAstronomers : old ABCD receivers
Bolometers
Two large field bolometer cameras are installed: MAMBO1 with 37 pixels, and MAMBO2 with 117 pixels (MAx-Planck Millimeter BOlometer Array). Usually MAMBO2 is in use. Both cameras work at 1.2mm wavelength, the HPBW is 11", pixel spacing is 20", and the sensitivity is 1.5mJy. This is the rms after 10 minutes integration (normal bolometric conditions) with skynoise removal. See the MAMBO page for details.
Telescope efficiencies and beam widths
Backends
Backends for the new EMIR receiver, HERA, and MAMBO: BackendsForEmirHeraMambo
Backends for the old ABCD receivers (till mid March 2009): BackendsForAbcdReceivers
Control System
The 30-m telescope runs under the New Control System (NCS), see:
Observing modes and source offsets in:
- Projection "Radio" (same offsets as in old CS) in Equatorial J2000.0
- "true angle" horizontal
- Nasmyth (receiver offsets)
Observing Modes and Switching Modes
Observing mode |
swTotal |
swBeam |
swWobbler |
swFrequency |
Calibrate (Heterodyne) |
X |
|
|
|
Pointing |
X |
X |
X |
|
Focus |
X |
X |
X |
|
Tip (Skydip) |
X |
|
|
|
Track |
|
|
|
fsw |
ONOFF |
psw |
|
wsw |
|
OTFMAP (Heterodyne) |
otf/psw |
|
|
otf/fsw |
Raster |
|
|
|
|
OTFMAP (MAMBO Bolometer) |
|
|
X |
|
VLBI |
X |
|
|
|
for more details on observing and switching modes, see the section "NCS explained" in the pako cookbook
swTotal stands for total power observations without switching, while still using the internal synchronization signals.
swBeam beam switched observations using the chopper wheel on mirror M4.
swWobbler switching the wobbling secondary (M2). The maximum allowed throw is +/-2'.
swFrequency switching the local oscillator frequency
Pointing: Using nearby (within 10 degree) pointing sources, <1" accuracy can be obtained; with absolute ("blind") pointing, the accuracy is about 2" rms, the receivers are aligned within 1.7" (see the Telescope Status page for current values). Checking the pointing and alignment (using e.g. a planet) is the responsibility of the observer.
Focus: residual errors of <1mm may need correction. There are systematic differences of upto 0.6mm in the focus of the different receivers (cf. Telescope Status page). The focus is subject to change especially during sunrise and sunset.
Position switching (psw): the combination of ONOFF with swTotal is called "Position Switching". Only relative off-source reference positions are possible.
Wobbler switching (wsw): often called double beam switching mode: max. 240" throw at 0.25 Hz, standard phase duration 0.5 Hz.
Frequency switching (fsw): max. 45 km/s throw up to about 10 Hz.
On the fly mapping (Heterodyne): Works with all receivers and backends, typical dump rate 0.5 to 10 Hz. OTF can be observed without reference position, e.g. for galaxies, and MIRA is able to use emission-free OTF data as reference!
Raster mapping is at present not offered. The observer may want to use either psw or otf instead.
Polarimetry: using VESPA as an IF polarimeter
Weather station and Taumeter
- Wind velocity and direction measured on hill behind the telescope
- Outside temperature and relative humidity measured at base of telescope. In case the sensors are frozen, the operator will use a mobile weather station and enter values by hand into the drive program.
- Pressure measured at entrance to control building
Taumeter does regular skydips to inform the observer about the sky transmission near 225 GHz. The local oscillator works at 225GHz. The IF is 1.5GHz and the bandwidth is 0.5GHz. It is a double-sideband Schottky receiver.
Old Telescope System Summary page of September 07
This is page http://www.iram.es/IRAMES/mainWiki/TelescopeSystemSummary moderated by Carsten Kramer