SMTO Receiver Information

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SMT RECEIVERS

Bolometers

The 19 Element Bolometer Array
In March 2000, the MPIfR 19-channel 870 micron bolometer array arrived. It was installed and quickly has become a favorite with both Steward and MPIfR observers. Currently, the standard observing modes include both CONOFF (a simple continuum on-off scan) and CMAP (On-the-fly mapping) modes. Data reduction can be done with either MOPSI or NIC. While we are still learning about the instrument and data reduction, it has already proved to be a great success.
Note that the array will allow observers, with proper data reduction techniques, to use weather that is too unstable for single channel bolometer work. Thus, we anticipate that this instrument will be used a great deal in the future.
More details about this instrument can be found on an extra page
The Four Color Bolometer
This MPIfR bolometer has 4 channels (1300, 870, 450, and 350 microns). The bolometer can only observe one channel at a time, but changes between the 4 colors takes less than 10 minutes. The bolometer will be the bolometer of choice for continuum observations. The SMTO staff will characterize the 4 channels on the sky at the beginning of the 1997/1998 season. Observations of standards last spring found the 1300 micron NEFD(Jy/Hz^(1/2)) = 0.6-0.8 Jy/sec^(1/2). This number is preliminary.
(See the SMTO Electronic Newsletter - Volume 1, Number 2 for details).
It was successfully used to study Hale Bopp as well as determining flux densities of several YSO's (Guertler, Jena).
BOL-1300:
The MPIfR 1300 micron bolometer has been extensively used during previous seasons. With the arrival of the 4-color system, the 1300 micron has been decommissioned but remains available on-site as a back-up instrument.
BOL-870:
The MPIfR 1300 micron bolometer has been extensively used during previous seasons. With the arrival of the 4-color system, the 870 micron has been decommissioned but remains available on-site as a back-up instrument.

Heterodyne Receivers

SIS-230:
The SORAL 230 GHz Receiver achieved double side-band temperatures of 100 K across the 210-275 GHz tuning range in good observing setups. Main beam efficiency on Jupiter has been measured at 76%. Currently the receiver has received provisional acceptance as a facility instrument pending the delivery of full documentation.
(See the SMTO Electronic Newsletter - Volume 1, Number 2 for details).
SIS-345:
The MPIfR 345 GHz dual-channel receiver has double sideband temperatures of less than 125 K across a range of 320 to 375 GHz frequency range at the telescope. Typically, the SIS-345 has been used in single channel mode to achieve the highest sensitivity in that channel. Currently, it is provisionally accepted as a facility instrument.
(See the SMTO Electronic Newsletter - Volume 1, Number 2 for details).
SIS-490:
The SORAL 490 GHz single-channel receiver has T(DSB) < 150 K across the range of 430 to 480 GHz. An unfortunate resonance at the upper edge of the tuning range degrades its performance to about T(DSB) of 225 K at 490 GHz The main beam efficiency was measured to be 47% on Saturn and 45% on Mars. Currently, it is provisionally accepted as a facility instrument. The current 490 GHz setup can be difficult to tune, but improvements are planned over the summer shutdown period.
(See the SMTO Electronic Newsletter - Volume 1, Number 2 for details).
Hot-electron Bolometer:
Built by the CFA Submillimeter Receiver Lab, the Hot-electron Bolometer receiver was tested in Febuary 1998 at the SMTO. It was used quite successfully by a variety of programs during the 1998-1999 season. The HEB receiver will be available in winter 1999 for use by CFA/Steward observers. (See the SMTO Electronic Newsletter - Volume 1, Number 2 for details).
Note that only observers checked out on the HEB are allowed to touch the instrument. The observations are usually done in a priority observing mode by the FOT on duty.

Contact Harold M. Butner (hbutner@as.arizona.edu) or Michael Dumke (mdumke@as.arizona.edu).
Last modified: 1 May 2002