NARRABRI:
The Compact Array at Narrabri will be available for the entire term.

	• SERVICE OBSERVING ON THE COMPACT ARRAY
Because the basic time quantum for observations with the Compact Array is 13 hours (12 + setting up and calibration time), each term there are several unallocated periods of a few hours duration in the observing schedule.  Some of these periods are useful for maintenance and testing, but some could also be made available for general observing.  Therefore, beginning in the 1995 August observing term, it is proposed to implement a scheme of fill-in or service observations, under the following conditions:

(a)	Proposals will be required as for general observations, and will be reviewed by the Time Assignment Committee.  They will be added to a pool of projects and in general will be treated on a first-come-first-served basis,  within the limits imposed by TAC ratings, LST range, array configuration etc
(b)	The available time per session will be typically 4 - 8 hours
(c)	The Operations Group will slot the observing programs into the CA schedule as time becomes available during normal Observatory working hours.   There will be no guarantee given as to when a particular program will be  carried out - maintenance and array tests will generally be given higher priority in the use of unallocated time
(d)	The proposers will be responsible for preparation of their own Schedule  files
(e)	The Operations Group will copy the observations onto exabyte tape or CD and send these to the PI of the relevant 'observing' group.


PARKES:
The upgrading prior to Galileo support is expected to begin on 1st October, and the Parkes telescope will be available for observing during August and September only.  Applications may be submitted requesting the use of the SETI front-end receiver, which may still be available for part of this period.


MOPRA:
	*MM-WAVE OPERATION AT MOPRA DURING THE 1995 AUGUST OBSERVING TERM

After the end of the SETI-PHOENIX project in June, the mm-wave receiver system will be reinstalled on the Mopra antenna.  It is intended to offer the system for general observing in the 1995 August term on a 'shared-risk' basis.  Because the system will still be in a commissioning phase, although the ANTF will endeavour to fully support programs that are allocated observing time, there will be no guarantee that the observing will be successful, or even  uninterrupted by system problems.  It is still too early for the available system to be fully defined, but projected features are as follows:

(a)	3-mm SIS receiver with 86-GHz system temperature of about 130 K (double- sideband) at the zenith.  The system temperature will be higher for CO  observations at 115 GHz 
(b)	Dual-channel system with one channel tuned for frequencies near CO (115 GHz), the other tuned to 86 GHz (for pointing observations using SiO Masers)
(c)	Antenna efficiency 30 - 40 % at 86 GHz
(d)	Antenna beamwidth of around 45 arcsec for CO observations
(e)	Pointing accuracy better than 15 arcsec
(f)	Expected optical depth tau for CO observations of around 0.5
(g)	No beam switch; frequency switching may be available for observing narrow spectral lines
(h)	Correlator providing a selection of bandwidth/channels combinations ranging from 4 MHz/8192 channels to at least 256 MHz/256 channels.


VLBI:
It is not expected that VLBI observations will be carried out in the coming term; however, applications for time-critical observing may be submitted for consideration.


***   Publications which reference observations made with the Compact Array or Parkes Telescope should contain the footnote "operated by CSIRO Australia Telescope National Facility".