Technical
Mode:Line
Back end:ACR800
Back end Mode:1x2, multi-bank
Procedures:OffOn
Receiver:X
Switching Scheme:TotalPwr
|
Proposal Information
PI:Turner
Bands: X
Back ends: S
Support Person: A. Minter
|
Checkout Notes
The spectral baselines are critical to the program's success.
09/12/02 D. Balser
he spectrometer modes have not been checked out by engineering. Only
one of the four modes has been checked out. A hardware change is
required in two places to accommodate the desired observing modes. The
preferred spectrometer mode requires multiple banks which are not yet
available. An alternative spectrometer mode with less spectral
resolution has not been checked out by engineering.
Regardless, we need to understand the instrumental spectral baseline
problems at X-band before scheduling this project. In particular the
2.4 MHz and 20 MHz ripples observed at X-band will significantly
affect this project. The expected linewidths are 30 km/s (1 MHz).
o Observational Setup: - Front End: X-band - Back End: Spectrometer
1. Preferred mode Samplers: 16 (tune to 8 different frequencies) BW: 12.5 MHz Level: 9 Banks: 4 (4096 lags; Resolution = 3.1 kHz (0.10 km/s)) Mode: 1N4-0A-12-9; 1N4-1B-12-9; 1N4-2C-12-9, 1N4-3D-12-9
Notes: (i) In order to tune to 8 different frequencies simultaneously requires a hardware change to the cabling. (ii) In order to accomodate the last two spectrometer modes requires a hardware change to the cabling. (iii) Multiple banks cause M&C reliability problems.
2. Alternative mode Samplers: 8 (tune to 4 different frequencies) BW: 12.5 MHz Level: 9
Banks: 1 (2048 lags; Resolution = 6.1 kHz (0.20 km/s)) Mode: 1N8-0B-12-9
Notes: (i) Our integration time increases by a factor of two. (ii) By using only one bank our resolution is degraded by a factor of four (or only two with just 8 samplers). Although we need to detect narrow C RRL lines which might be blended with the 4He line, I suspect that 0.20 km/s would be sufficient.
- Observing Mode: Position Switching
|
Spectrometer (Autocorrelator) Notes
Preferred: 2W1-40-800; 2W1-54-800; Alternate: 1W2-004-800
|
Technical
Mode:Line
Back end:ACR50
Back end Mode:4x2, 9-level, multi-bank
Procedures:OffOn
Receiver:PF300
Switching Scheme:TotalPwr
|
Proposal Information
PI:Langston
Bands: 3
Back ends: S
Support Person: G. Langston
|
Checkout Notes
RFI will be severe so SP might be superior to ACR. Need cross polarization mode of SP or ACR.
9/6/2 GL
Spectrometer 9-level, 2IF 50 MHz, 1 Quadrant mode, OR Spectrometer 3-level, 2IF 200MHz, 1 Quadrant mode, OR Spectrometer 9-level, 4IF 50 MHz, 2 Quadrant mode
|
Spectrometer (Autocorrelator) Notes
1N2-0A-50-9 or 1W2-001-200 or 2N4-0A-50-9
|
Scheduling Notes
Waiting for PI feedback.
|
Technical
Mode:Line
Back end:ACR50
Back end Mode:4x2, 9-level, multi-bank
Procedures:OffOn
Receiver:34
Switching Scheme:TotalPwr
|
Proposal Information
PI:Briggs
Bands: 34
Back ends: S
Support Person: G. Langston
|
Checkout Notes
GL Comments 08/23/02 follow-
Besides less RFI, the main thing the Briggs and Lane proposals need is support for the 8 IF spectrometer mode. Last year I used this mode and it appeared to work from the M&C point of view. However, the AIPS++ side is missing (I think).
They could and would observe, if they could get a series of late night obseving sessions. (Say from 1 to 6 am) when the RFI seems to be less. They felt the RFI was much
better early saturday morning.
They asked me to make an early morning RFI survey, to confirm the RFI is less in the early morning. I was going to do at 300 MHz next week.
RFI in the 300 MHz band appears to be acceptable during evening and nighttime periods.
9/6/2 GL
Spectrometer 9-level, 8IF 50 MHz, 4 Quadrant mode, OR Spectrometer 9-level, 4IF 50 MHz, 2 Quadrant mode OR (???) at 50 % efficiency Spectrometer 3-level, 2IF 200MHz, 1 Quadrant mode, due to RFI.
They cannot efficiently use the Spectral Processor for a blind search.
|
Spectrometer (Autocorrelator) Notes
4N8-0A-50-9 or 2N4-0A-50-9 or 1W2-001-200 (?)
|
Technical
Mode:Line
Back end:ACR50
Back end Mode:ACR: 1x2, 9-level, 12.5 or 50 MHz; SP 2x024, 10 or 40 MHz
Procedures:OffOn
Receiver:3468
Switching Scheme:TotalPwr
|
Proposal Information
PI:Lane
Bands: 3468
Back ends: SP
Support Person: G. Langston
|
Checkout Notes
10/18/03 - G. Langston
The high redshift neutral hydrogen absorption looks good
in the frequency range 380 and 450 MHz. At higher frequencies there
is still a lot of RFI, preventing observing in > 50% of the band above
450 MHz. Project was 01A61. This project could be scheduled
for observing in the lower frequency range. Software is critically
needed for data Flagging, before this project could yield science results.
Setup went fairly well using a CLEO TCF for this observation. Found
that the 240 MHz filter on the PF1 receiver was not passing any
signal, so used the 80 MHz filters for both polarizations. This was
probably OK, as the RFI was so bad towards the higher frequency that
using a wider bandwidth would probably have spoiled the observations
anyway. Used center frequency 405 MHz, and dual polarization mode
of the spectrometer with 200 MHz bandwidth.
Observed a series of high redshift quasars.
Data are in /home/gbtdata/TGBT01A_061
GL Comments 08/23/02 follow-
Besides less RFI, the main thing the Briggs and Lane proposals need is support for the 8 IF spectrometer mode. Last year I used this mode and it appeared to work from the M&C point of view. However, the AIPS++ side is missing (I think). They could and would observe, if they could get a series of late night obseving sessions. (Say from 1 to 6 am) when the RFI seems to be less. They felt the RFI was much better early saturday morning. They asked me to make an early morning RFI survey, to confirm the RFI is less in the early morning. I was going to do at 300 MHz next week.
RFI in the 300 MHz band appears to be acceptable during evening and nighttime periods.
9/6/2 GL
Spectrometer 9-level, 8IF 50 MHz, 4 Quadrant mode, OR Spectrometer 9-level, 4IF 50 MHz, 2 Quadrant mode OR (???) at 50 % efficiency Spectrometer 3-level, 2IF 200MHz, 1 Quadrant mode, due to RFI.
They cannot efficiently use the Spectral Processor for a blind search.
08/29/03 G. Langston
GBT Observing Checkout Summary: RFI and deep integrations at 600 MHz
Short, two hour, checkout was successful in scanning the 475 to 755 MHz
frequency range for RFI. Considerable RFI change since last check in
2002 February. Changes were no 2 MHz spaced interference spikes (good),
much more digital TV and also the analog TV signals seemed stronger (bad).
Observing Summary
=================
Used CLEO and GO to configure the system. Had a larger than usual number
of software problems: 1) PF1 manager was hung at startup. Had to
reboot computer GBTAIO1. 2) BCPM manager appeared to be hung, which
stopped GO. Had to use GO T and remove the BCPM.
Spectrometer was in the "FATAL" state at startup. Had more than usual
Spectrometer failures. Also the software appeared to be doing slightly
different actions. Spectrometer was repeatedly going into FATAL
DMA error state at each scan (in two bank, A1 B1, mode with 50 MHz, 9 level,
2 IFs per bank mode and 10 second integrations). Since OffOn pairs were
running, the spectrometer would appear to clear at the start
of the next scan, but then immediately go into FATAL state.
The M&C configuration file indicated that the 800 MHz feed was in place,
when actually the 600 MHz feed was installed. This caused some M&C
functions to declare no signal present, when signal was present.
Barry rebooted the spectrometer and we could scan the band for RFI.
All was OK with the spectrometer for 45 minutes.
Jeff Acree was present and we noted that even the radio astronomy band,
608 to 614 MHz, had some low level RFI in it. This may be due to
aliasing of very bright TV signals into the band.
Next started a deep OffOn pair on blank sky with the same mode, but
1 second averaging. The first 3 minute scan was OK, but in the
next scan the spectrometer croaked with a DMA error.
|
Spectrometer (Autocorrelator) Notes
4N8-0A-50-9 or 2N4-0A-50-9 or 1W2-001-200 (?)
|
Technical
Mode:Line
Back end:ACR12_5
Back end Mode:8x2, 9-level, four-banks or 4x2, 9-level, single-bank
Procedures:OffOn
Receiver:X
Switching Scheme:TotalPwr
|
Proposal Information
PI:Balser
Bands: X
Back ends: SDP
Support Person: D. Balser
|
Checkout Notes
D. Balser comments 08/23/02 follow-
Based on recent tests the project GBT02A-021 (A Search for Recombination Lines from Diffuse Gas in the Galactic Center Region by Lockman, Roshi, and Balser) can be scheduled for time sometime after the first week in September but before October. We will attempt to
use the spectral processor with 8 IFs instead of the spectrometer. We would also require some commissioning time before and/or after our target source observing to make sure the spectral processor baseline problems are not present for these sensitive observations. Also, since we are using only 8 IFs of the desired 16 this will take a factor of two longer integration time to achieve the same sensitivity.
Alternative mode: Integration time increases by a factor of two.; By using only one bank, resolution is degraded by a factor of four (or only two with just 8 samplers). But our lines should be broad and this will not be a problem. The spectral baselines are critical to the program's success.
09/12/02 D. Balser
The spectrometer modes have not been checked out by engineering. Only
one of the four modes has been checked out. A hardware change is
required in two places to accommodate the desired observing modes. The
preferred spectrometer mode requires multiple banks which are not yet
available. An alternative spectrometer mode with less spectral
resolution has not been checked out by engineering.
The spectral baselines are important to this project as the lines are
expected to be very weak and broad (100 km/s). These observers have
agreed to perform test observations. Part of this project is
currently being scheduled with the spectral processor.
o Observational Setup: - Front End: S-band (C-band; L-band) - Back End: Spectrometer
1. Preferred mode Samplers: 16 (tune to 8 different frequencies) BW: 12.5 MHz Level: 9
Banks: 4 (4096 lags; Resolution = 3.1 kHz (0.28 km/s)) Mode: 1N4-0A-12-9; 1N4-1B-12-9; 1N4-2C-12-9; 1N4-3D-12-9
Notes: (i) In order to tune to 8 different frequencies simultaneously requires a hardware change to the cabling. (ii) In order to accomodate the last two spectrometer modes requires a hardware change to the cabling. (iii) Multiple banks cause M&C reliability problems.
2. Alternative mode Samplers: 8 (tune to 4 different frequencies) BW: 12.5 MHz Level: 9
Banks: 1 (2048 lags; Resolution = 6.1 kHz (0.55 km/s)) Mode: 1N8-0B-12-9
Notes: (i) Our integration time increases by a factor of two. (ii) By using only one bank our resolution is degraded by a factor of four (or only two with just 8 samplers). But our lines should be broad and this will not be a problem.
- Alternative Back End: Spectral Processor (L,S bands)
Mode: 8x256 BW: 10 MHz (Resolution = 39 kHz (4.7 km/s))
Notes: (i) Baselines might be problematic with the spectral processor.
- Observing Mode: Position Switching
|
Spectrometer (Autocorrelator) Notes
Preferred: 1N4-0A-12-9; 1N4-1B-12-9; 1N4-2C-12-9, 1N4-3D-12-9, Alternate: 1N8-0B-12-9
|
Technical
Mode:Line
Back end:ACR12_5
Back end Mode:8x2, 9-level, 4-Banks or 4x2, 9-level, single bank
Procedures:OffOn
Receiver:LCS
Switching Scheme:TotalPwr
|
Proposal Information
PI:Lockman
Bands: LSC
Back ends: S
Support Person: D. Balser
|
Checkout Notes
In order to tune to 8 different frequencies simultaneously requires a hardware change to the cabling. Multiple banks cause M&C reliability problems.
D. Balser comments 08/23/02 follow-
Based on recent tests the project GBT02A-021 (A S
|
Spectrometer (Autocorrelator) Notes
Preferred: 1N4-0A-12-9; 1N4-1B-12-9; 1N4-2C-12-9; 1N4-3D-12-9, Alternate: 1N8-0B-12-9
|
Technical
Mode:Line
Back end:ACR200
Back end Mode:4x2, multi-bank. Probably SP (2x1024, 40 MHz) is OK
Procedures:DualBeamSwitch
Receiver:UK
Switching Scheme:BeamSw
|
Proposal Information
PI:Hollis
Bands: UK
Back ends: S
Support Person: R. Maddalena
|
Checkout Notes
Not clear why 200 MHz is needed since they need 100 kHz resolution and probably less than 40 MHz badwidth coverage. In this case the SP could be used. In any case, an ACR single bank mode could be substituted for requested multi-bank mode because of requested low resolution. Probably Beam switching better than proposed position switching for some of their sources.
9/5/2 PJ notes
For proposal 02A-025 (Hollis), the program is primarily for K-Band.
Ku-Band may be used as a backup. The Spectrometer mode needed is 200 MHz
with 8 samplers. This mode is possible, but has not been assigned a mode
string in Rich Lacasse's spreadsheet. I'll ask Rich about it. The
observing mode is simple position switching.
I suggest waiting to check this program out until the K-Band Rx goes back
up. I will be willing to test this as soon as the K-Band Rx is available
again (early October?). I am also willing to do a preliminary checkout in
2-IF mode, if the 8-IF mode is not immediately available. I would
probably want to wait until the 200x8 mode is available to do the run,
however.
|
Spectrometer (Autocorrelator) Notes
N/A
|
Technical
Mode:Line
Back end:Mixed
Back end Mode:See notes
Procedures:OffOn
Receiver:X
Switching Scheme:TotalPwr
|
Proposal Information
PI:Rood
Bands: X
Back ends: SDP
Support Person: D. Balser
|
Checkout Notes
|
Spectrometer (Autocorrelator) Notes
Preferred: 1N4-0A-50-9; 1N4-1B-50-9; 1N4-2C-50-9; 1N4-3D-50-9, ALternate: 1W2-001-200; 1W2-123-200; 1W2-245-200; 1W2-367-200
|
Technical
Mode:Line
Back end:S
Back end Mode:4W2---200, 2W2--200, or 1W2---200 single-bank
Procedures:OffOn
Receiver:3468
Switching Scheme:TotalPwr
|
Proposal Information
PI:Carilli
Bands: 3468
Back ends: S
Support Person: G. Langston
|
Checkout Notes
Also requests PF2. Because of large line widths maybe can be done in the 1W2---200 ACFmode. Awaiting checkout of spectrometer modes. RFI will be a problem.
|
Technical
Mode:Line
Back end:S
Back end Mode:Wants 9-level, 200 MHz (not possible!). 4W2--200 single-bank nearest match
Procedures:Track
Receiver:8
Switching Scheme:TotalPwr
|
Proposal Information
PI:Darling
Bands: 8
Back ends: S
Support Person: K. O'Neil
|
Checkout Notes
09/22/03 K. O'Neil
I took some more data for your 02C-008 project. I've attached plots
of some of the observations. As you can see, things aren't great
- lots of RFI and baseline problems. The plots show just the on-source
observation, if that was all that was taken, or the (on-off)/off
in the cases where offs were taken. (The different colors are simply
the different backends)
Unfortunately, I suspect this is as good as the data will get, at least
for the near future. So as you/we look at the data you are going to have
to decide if what you see is acceptable for your project. If there are
more specific tests you;d like me to try, I can try to obtain more telescope
time for that.
RFI will be an issue. Waiting of Spectrometer mode.
|
Technical
Mode:Line
Back end:S
Back end Mode:1W2---200 4-bank or 2W4---200 two-bank
Procedures:OffOn
Receiver:UK
Switching Scheme:TotalPwr
|
Proposal Information
PI:Hollis
Bands: UK
Back ends: S
Support Person: R. Maddalena/P. Jewell
|
Checkout Notes
Baseline issues. Multi-bank. They say they will smooth to 100 kHz implying that two-bank 4W1-200 might also work
|
Technical
Mode:Line
Back end:S
Back end Mode:Probably 1W2---200 or 2W2---200 single-bank
Procedures:OffOn
Receiver:U
Switching Scheme:TotalPwr
|
Proposal Information
PI:Bolatto
Bands: U
Back ends: S
Support Person: D. Balser
|
Checkout Notes
Baselines. Maybe beam switching better?
|
Technical
Mode:Line
Back end:S
Back end Mode:1W1--800 four-bank
Procedures:DualBeamSwitch
Receiver:K
Switching Scheme:BeamSw
|
Proposal Information
PI:Lo
Bands: K
Back ends: S
Support Person: R. Maddalena
|
Checkout Notes
Baselines. Assuming BeamSw better for them then TotalPwr. Multibank
|
Technical
Mode:Line+Continuum
Back end:SD
Back end Mode:1N2--12-9 single-bank or SpecProc 10 Mz 2x1024
Procedures:OTFMap
Receiver:L4
Switching Scheme:Frequency
|
Proposal Information
PI:Gibson
Bands: L4
Back ends: SD
Support Person: F. Ghigo
|
Checkout Notes
10/08/03 F. Ghigo
The observations last Friday seem to show that things are not linear when scanning
across Cass A. I set the power levels at varioius points in the system according to
what the engineers recommend for providing adequate dynamic range, but there
still seems to be a problem. Last Friday's observing was done at 835 MHz using
the higher cals. The 800 Mhz receiver was
the lowest available frequency just now until the 450 MHz receiver is installed
later in the month. Scanning across a 1 Jy source results in the expected
antenna temperature for that source. But scanning across Cass A indicates
about 800 Jy, whereas the flux of Cass A at 835 Mhz is about 2500 Jy.
So there seems to be some compression. So at the moment I have to admit that
I have no idea how to do these observations properly. We will try some more testing October 21 or 23 with the engineers consulting
to try to figure out what has gone wrong.
You can decide to go ahead with the observations as scheduled for Nov 6,7,10,11 on
the assumption that we will have figured out how to do it properly by then
(of which there is no guarantee), or you can decide to put off the observing
until later.
09/22/03 F. Ghigo
The only problem was at the beginning: the Spectral Processor was in a strange
state and complained of having no 5 MHz reference. Normal re-booting was not
enough. Barry had to cycle the power on the VME computer in the SP, after
which everything ran fine.
The project was to check for dynamic range problems when scanning across
Cass A at 1420 and 835 MHz. (the project calls for 408 MHz, but that is not
available just now). Continuum mapping is done using the SP so that RFI can be
removed. Scans were done across Cass A and calibrators NGC7029 and
3C48 with the power levels set so as not to saturate on Cass A. The initial impression is that the Spectral Processor can handle this big range in power levels without great deviations from linearity. Later analysis will maybe provide more quantitative evaluation.
==
PF part maye be better off done as a specal-line observation since it will have RFI issues.
09/29/02 FG
Spectrometer mode 1N2-0A-12-9 would be used for the
21cm line map. There is no technical need to wait --
this could be scheduled as soon as it can be worked in.
09/30/02 FG
PI desires polarization (must wait till next year) Waiting answer from PI regarding the options.
The only instrument we have that can do polarization measurements
(until the ACS polarization modes have been tested) is the
spectral processor. In polarization mode, the maximum bandwidth
per IF is 20 MHz and maximum number of channels is 512.
I am told that some polarization channels are bad and will
have to be flagged. Some efforts to understand the instrumental
polarization of the GBT have begun, but at the moment you
probably cannot make much sense of polarization measurements.
If you really want polarization, it's best to wait a few months.
10/04/02 FG
PI indicated hewould wait for polarization capability.
|
Technical
Mode:Line+Polarizatio
Back end:S
Back end Mode:1W2---800 single-bank
Procedures:OTFMap
Receiver:XUK
Switching Scheme:TotalPwr
|
Proposal Information
PI:Finkbeiner
Bands: XUK
Back ends: S
Support Person: K. O'Neil
|
Checkout Notes
Novel data reduction. Will reuire more interaction with observer than most proposals. Parts can be scheduled. RFI may be an issue.
06/13/03 K. O'Neil
Doug Finkbeiner, the PI on GBT proposal 02C-043, would like to
postpone his observations until the baseline issues get sorted out
a bit more. So, as things improve i will remain in touch with
him until the baselines reach a point that he feels he can get good
science. So at least for now his porposed should be put back on the
shelf.
Just as a note - he did say he's willing to go ahead with the observations
without cross-polarization modes on the spectrometer.
|
Scheduling Notes
Would like to schedule January 03 or shortly there after (to follw the public release of MAP data at the AAS in 01/03).
|
Technical
Mode:Line
Back end:P
Back end Mode:
Procedures:
Receiver:3468
Switching Scheme:Position
|
Proposal Information
PI:Lane
Bands: 3468
Back ends: P
Support Person: G. Langston
|
Checkout Notes
05/18/03 G. Langston
The High Redshift Neutral hydrogen Absorption experiment
of Lane (03A-015) can be scheduled for the 800 MHz part. There
is relatively little RFI at the 3 redshifts of interest,
for z = 0.860, z = .6819 and z = .656. Note that there is
alot of RFI in this band, but not near these redshifts.
Test observations in /home/gbtdata/TGBT03A_015_01 clearly show neutral
hydrogen absorption at 839.4 MHz towards 3C286.
|
Technical
Mode:Line
Back end:SP
Back end Mode:
Procedures:
Receiver:QK
Switching Scheme:Position
|
Proposal Information
PI:Widicus
Bands: QK
Back ends: SP
Support Person: F. Ghigo
|
Checkout Notes
06/10/03 F. Ghigo
Project checkouts for projects 02C_052, 03B_011, and 03B_027
were done on May 20th. All of these use the K-band receiver
with 4 IFs of 50 MHz bandwidth. All these projects can be
scheduled (with some slight worries as mentioned below).
Observations were done at 4 frequencies of NH3 transitions,
in source LDN134N. Position switching, nodding, and on-the-fly
mapping was done. Two of the proposals will probably
benefit from double beam-switching (3B_011 and 3B_027).
The other requests mapping.
All of this seems to be working reasonably well. The spectrometer produces reasonable looking spectra both in
single beam (8 samplers) and double beam (16 samplers)
observations. The noise levels were somewhat higher than
theoretical, but the weather was bad and system temperatures
were varying in the range 90-130K, so this is perhaps not
a problem with the spectrometer.
It was not possible to balance the power levels from all IFs at once,
but we put one spectral window at 25.06 GHz, and the
other three in the 23.6 - 23.9 range. It may just not be
possible to balance all windows over that wide a range.
This would be a problem for project 02C_052, which
wants to observe these NH3 transitions. For the other
proposals, the exact transitions were not specified, so we
do not know exactly whether this would be a problem.
So given that the K-band receiver will be undergoing some
improvements over the summer, and that the beam switches
will be working properly, and hoping for improvements in
the dish software for handling multi-IF data, I think
we can go ahead and schedule these projects.
|
Technical
Mode:Line
Back end:S
Back end Mode:
Procedures:
Receiver:L
Switching Scheme:
|
Proposal Information
PI:Li
Bands: L
Back ends: S
Support Person: K. O'Neil
|
Technical
Mode:Other
Back end:O
Back end Mode:
Procedures:Maybe 'other'
Receiver:4LX
Switching Scheme:Position
|
Proposal Information
PI:Coster
Bands: 4LX
Back ends: O
Support Person: F. Ghigo
|
Checkout Notes
9/5/03 Maddalena - They may need a 'home' spun GO observing procedure. IF and backend details need to be worked out.
|
Technical
Mode:Continuum
Back end:D
Back end Mode:
Procedures:Track
Receiver:CK
Switching Scheme:Position
|
Proposal Information
PI:Arzoumanian
Bands: CK
Back ends: D
Support Person: F. Ghigo
|
Checkout Notes
9/5/03 - Maddalena - Need to look into whether requested bandwidths are practical. Should emphasize the advantage of the K-band's dual beams for removing changes in Total Power from the atmosphere, not jist for RFI monitoring.
|
Technical
Mode:Line
Back end:S
Back end Mode:
Procedures:Track
Receiver:LA8463
Switching Scheme:Position
|
Proposal Information
PI:Darling
Bands: LA8463
Back ends: S
Support Person: A. Minter
|
Checkout Notes
9/5/03 Maddalena - Need RFI checks at some frequqncies prior to the obsreving runs. Complicated observing setup that probably will require a 'practice' session with the observer on-site before committing to the full project. Not enough information to determine backend modes, cabling, etc.
|
Technical
Mode:Line
Back end:S
Back end Mode:
Procedures:Other
Receiver:L
Switching Scheme:Position
|
Proposal Information
PI:Li
Bands: L
Back ends: S
Support Person: K. O'neil
|
Checkout Notes
9/5/03 - Should this use the Spectral Processor?
|
Technical
Mode:Line
Back end:S
Back end Mode:1N2-12-9, 2-bank or 2N4-12-9 1-bank
Procedures:Track or NOD
Receiver:U
Switching Scheme:Position
|
Proposal Information
PI:Fish
Bands: U
Back ends: S
Support Person: G. Langston
|
Checkout Notes
9/5/03 Maddalena - Beam switching might be suitable if the sources were compact enough, else OnOff observing. RMS calculations are either sqrt(2) or 2x more pessimistic than necessary and probably they won't need as much observing time.
|
Technical
Mode:Line
Back end:S
Back end Mode:1W2-800 4-banks
Procedures:NOD
Receiver:Q
Switching Scheme:Position
|
Proposal Information
PI:Walter
Bands: Q
Back ends: S
Support Person: G. Langston
|
Checkout Notes
9/5/03 Maddalena - 1600 MHz bandwidths, 24 hours of observing, and 0.3 mJy sensitivity implies baselines will be the determininbg factor here but not as we would have if this were 22 GHz observing.
|
Technical
Mode:Line
Back end:S
Back end Mode:Probably 1N2-50-9 2 bank or 2N4-50-9 1 bank
Procedures:OffOn
Receiver:8
Switching Scheme:Position
|
Proposal Information
PI:Chengalur
Bands: 8
Back ends: S
Support Person: G. Langston
|
Checkout Notes
9/5/03 Maddalena -- RMS calculation seems a factor of 2 too pessimistic and observers may not need their allotted time.
|
Technical
Mode:Line
Back end:S
Back end Mode:
Procedures:
Receiver:Q
Switching Scheme:Position
|
Proposal Information
PI:Roberts
Bands: Q
Back ends: S
Support Person: R. Maddalena
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Checkout Notes
9/5/03 Maddalena -- Moe info is needed since both observing mode and hadrware configuration are not specified.
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Technical
Mode:Line
Back end:S
Back end Mode:1N2-50.9 1 Bank
Procedures:PointMap
Receiver:Q
Switching Scheme:Position
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Proposal Information
PI:Moore
Bands: Q
Back ends: S
Support Person: K. O'Neil
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Checkout Notes
9/5/03 Maddalena - Lines are narrow enough that frequqncy switched mapping might be plausible. Source is to extended for beam-switching, though observers might take advantage of the other beams for mapping purposes. Assumed efficiency is probably high. Requires better pointing then we currently have since any pointing error will introduce apparent abundance errors and compromise their science. I think they completely blew their rms calculations -- I get 30 mK, not 100 mK per 5 minutes.
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