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VSOP AO2 PROPOSAL COVER SHEETS
DEADLINE : 8 May, 1998
SEND TO : VSOG, ISAS, 3­1­1 Yoshinodai, Sagamihara, Kanagawa 229­8510, JAPAN
(1) Date prepared : 3­May­1998
(2) Proposal title : Imaging of Strong GPS Sources
(3) INVESTIGATORS INSTITUTION
P.I. E.A. King COSSA, Australia
co­I. D. Jauncey, J. Reynolds, A. Tzioumis ATNF, Australia
co­I. P.M. McCulloch, M.E. Costa Univ. of Tasmania, Australia
co­I. J.E.J. Lovell ISAS, Japan
co­I. R. Preston, D. Murphy, D. Meier JPL, USA
co­I. D. Jones, S. Tingay JPL, USA
co­I. G.D. Nicolson CSIR, South Africa
co­I. P.E. Dewdney DRAO, Canada
co­I. W.Canon ISTS, Canada
(4) Principal Investigator (or contact person) details...
Name : Edward King
E­mail : eking@atnf.csiro.au
Fax : 61 2 6216 7222
Phone : 61 2 6216 7197
Address : COSSA
: GPO Box 3023
: Canberra, ACT
: 2601, Australia
:
(5) Proposal Abstract :
We propose high resolution imaging of six strong GPS sources with compact double structure.
Space­ground baselines are needed to achieve the resolution to accurately measure component
sizes at the frequency of the spectral peak, an essential requirement in distinguishing between
free­free and synchrotron self absorption mechanisms. Many of the components of these sources
are only just beginning to show signs of any internal structure on the longest Earth­only base­
lines and space VLBI presents the only possible opportunity to examine their structure at the
frequency of the peak in any detail.
(6) Proposal Category (indicate all that apply):
Object type:
p
AGN, Maser, Stellar, Pulsar, Other :
Observation type:
p
Continuum, Spectral Line, Polarization, Time­critical, Other :

(7) Number of proposed experiments
An `experiment' is one or more observations of one source at a fixed HALCA set­up. A request to observe the same
source at 1.6 GHz and separately at 5 GHz requires two columns to be filled in in item (8) below. A request to observe
the same source with HALCA simultaneously observing at 1.6 GHz and 5 GHz requires one column to be filled in.
Multi­epoch observations of the same source at the same frequency -- a `monitoring experiment' -- requires only one
column to be filled in. Suggested observing dates, especially for for time­critical and monitoring experiments, should
be specified in item (10).
The number of experiments in this proposal is: 6
(8) Details of proposed experiments
Experiment 1 Experiment 2 Experiment 3 Experiment 4
Source name (Jhhmm\Sigmaddmm) J1939­6342 J0024­4202 J0240­2309 J1723­6500
Alternative name PKS 1934­638 PKS 0022­423 PKS 0237­233 PKS 1718­649
RA(J2000) (hh mm ss.ssss) 19 39 25.026 00 24 42.990 02 40 08.1747 17 23 41.029
Dec(J2000) (dd mm ss.ssss) ­63 42 45.63 ­42 02 03.95 ­23 09 15.736 ­65 00 36.61
Observing frequency band (GHz) 1.6 1.6 1.6 5
Continuum observations:
Standard VSOP freq. channels?
p p p p
Channel A range (MHz)
Channel B range (MHz)
Spectral line observations:
Ch.A spectral line rest freq. (MHz)
Ch.A LSR velocity (km/s)
Ch.B spectral line rest freq. (MHz)
Ch.B LSR velocity (km/s)
FWHM of field of view required (mas)
Min. spectral channels per IF channel 128 128 128 128
Correlator averaging time (sec)
No. of correlating passes (if ?1)
Total flux density (Jy) 15.6 3.5 7.2 3.8
Correlated flux (mJy) 800 500 1200 800
Ground Radio Telescopes:
Suggested array given at Item (10)?
p p p p
GRT observing mode:
128Mbps LCP (standard)
p p p p
128Mbps LCP/RCP
256Mbps LCP/RCP
Preferred correlator:
No preference
Mitaka
Penticton
p p p p
Socorro
p
Monitoring programs :
Number of observations
Mean interval (days)
Related AO1 proposal code(s) V101 V101 V101 V101

Experiment 5 Experiment 6 Experiment 7 Experiment 8
Source name (Jhhmm\Sigmaddmm) J1130­1449 J2136+0041
Alternative name PKS 1127­145 PKS 2134+004
RA(J2000) (hh mm ss.ssss) 11 30 07.0524 21 36 38.5866
Dec(J2000) (dd mm ss.ssss) ­14 49 27.386 +00 41 54.217
Observing frequency band (GHz) 1.6 5
Continuum observations:
Standard VSOP freq. channels?
p p
Channel A range (MHz)
Channel B range (MHz)
Spectral line observations:
Ch.A spectral line rest freq. (MHz)
Ch.A LSR velocity (km/s)
Ch.B spectral line rest freq. (MHz)
Ch.B LSR velocity (km/s)
FWHM of field of view required (mas)
Min. spectral channels per IF channel 128 128
Correlator averaging time (sec)
No. of correlating passes (if ?1)
Total flux density (Jy) 7.4 10.7
Correlated flux (mJy) 1500 800
Ground Radio Telescopes:
Suggested array given at Item (10)?
p p
GRT observing mode:
128Mbps LCP (standard)
p p
128Mbps LCP/RCP
256Mbps LCP/RCP
Preferred correlator:
No preference
Mitaka
Penticton
p p
Socorro
p p
Monitoring programs :
Number of observations
Mean interval (days)
Related AO1 proposal code(s) V101 V101

(9) VSOP spacecraft observing mode (see Section 3 and Table 5 of the VSOP Proposer's Guide):
p
2 channel x 16 MHz, 2­bit (Standard mode),
Other:
Phase calibration tones:
p
On (Standard continuum mode),
Off (Standard spectral line mode)
(Include justification of any non­standard choice at (10) below)
(10) Additional notes to the scheduler :
For sources south of ffi \Gamma 25 ffi :
Preferred ground array: ATCA, Mopra, Hobart, Tidbinbilla, Hartebeesthoek,
+ Ceduna(5GHz only)
For sources north of ffi \Gamma 25 ffi :
Preferred ground array: As above + VLBA, Goldstone(1.6GHz only), Shanghai, Usuda.
If the translation VLBA/S2 is not feasible, separate VLBA and S2 correlations are requested
and the two datasets will be combined later with the loss of the transcontinental baselines. To
allievate this we request parallel VLBA & S2 recording in as many stations as practicable.
(11) Attach a scientific and technical justification, not in excess of 2 pages of text and 2 pages of
figures. Up to one page of (u,v) plots per source may optionally be included.
(Refer to the VSOP Announcement of Opportunity for detailed instructions.)
Preprints and reprints will not be forwarded to the Scientific Review Committee.
Send two paper copies of the complete proposal to:
VSOP Observing Proposals
VSOP Science Operations Group
Institute of Space and Astronautical Science
3­1­1 Yoshinodai, Sagamihara
Kanagawa 229­8510 JAPAN
In addition, e­mail the completed L A T E X file to submit@vsop.isas.ac.jp
Information from the Cover Sheets of scheduled proposals will be made available from the VSOP WWW
site.
Proposals must be received at ISAS by 8 May 1998