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Some Thoughts on Surveys
Peter Barnes
University of Florida DSET 2 H
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7 7Some background...
1. Timing
We are a bit late to this game! Excluding FIR or shorter-l surveys like GLIMPSE/MSX, we have:
Bolocam Galactic Plane Survey at CSO, 150 deg2, l1.1mm, already done! Public data release by end of year.
ATLASGAL at APEX, 360 deg2, l0.87mm, underway.
...and locally...
CHaMP at Mopra: 120 deg2, first pass (8593 GHz) done! First public data release next year.
HOPS at Mopra: 100 deg2, ~1/3 done?
We still have a window of opportunity, but it is shrinking rapidly. If we are to go ahead with MMWS, we need to get on with it! DSET 2 H
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...background...
2. Direct competition
The ALMA-ISM community is starting to realise that it has a looming problem with field-of-view. They are also agitating for an increased emphasis on long-mm wavelengths, ie 3 and 7mm.
They may come to Mopra for these needs, or they may build their own solution. Compared to the total ALMA budget, buying a 15m-class dish with its own multibeam array, and putting it on an existing good mm-wave site, is not such a big deal. If the Europeans or the (non-Nanten) Japanese decide they need to do this quickly, they will blow Mopra out of the water.
Bottom line: dont kid yourselves that we have this field to ourselves for an arbitrary amount of time. DSET 2 H h
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%$ %Getting it done
Radiometer equation:
per pixel/beam/etc. (1)
Can turn this around to get time required for a particular observation:
(2)
At 3mm with Mopra looking at some typical molecular cloud,
~ 15 sec in zoom mode. (3) DSET 2 H ( > , 6 * ^ ^ G @ @ 8 d xpr CWEE GGrphbj
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(m) 2063 378 sh
( km s) 1379 912 sh
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end MTsave restore
d MATH
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So for a typical 55 OTF map with Nyquist-sampled pixels, we need
tmap ~ 400 tpix = 100 min. (4)
Really, ~2 hr / map including overheads for pointing, etc. But really really, ~34 hr / map including weather outages. This matches the CHaMP experience when mapping dense cores in bright lines (TA* ~ 12 K @ 0.1 km/s resolution).
So if we want to map the fourth quadrant this way, for starters we need to cover (eg) 350 > l > 300, |b| < 1, or about 100 deg2, whence
tsurvey ~ 2122100 tmap = 3 106 min. = 2,000 days (5)
This is not feasible. DSET 2 H t
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Workarounds
All is not lost!
1. The lesson of CHaMP
If you can get finder charts from (eg) a lower-resolution or higher-efficiency survey, you can get to your dense gas maps in a tiny fraction of the time. So, CHaMP uses Nanten 12CO13COC18O to eliminate empty sky and do in 2 short seasons (~10 weeks total) what would have otherwise taken 20 years full-time all winter long!
Of course, you need the finder charts...... Nanten has done this for 300 > l > 280 only! ATLASGAL is not yet ready. Catch-22.
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Workarounds
All is not lost!
1. The lesson of CHaMP
If you can get finder charts from (eg) a lower-resolution or higher-efficiency survey, you can get to your dense gas maps in a tiny fraction of the time. So, CHaMP uses Nanten 12CO13COC18O to eliminate empty sky and do in 2 short seasons (~10 weeks total) what would have otherwise taken 20 years full-time all winter long!
Of course, you need the finder charts...... Nanten has done this for 300 > l > 280 only! ATLASGAL is not yet ready. Catch-22.
Try again! DSET 2 H '
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Workarounds
2a. Lower frequencies
(6)
Time required very sensitive to Tsys . At shorter wavelengths, Tsys is smaller, maybe by factor 24! (~ l1 to first order)
So what about CS J=10 (49 GHz), or NH3 (24 GHz)? In these cases, Trms and V have the same requirements due to the nature of the sources, but l is bigger by the same factor! Effectively cancels out one power of Tsys ~ l1.
Net time gain is about one factor of l1, except.....
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(D) 1437 950 sh
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(Kf) 1352 394 sh
(T) 1810 394 sh
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192 ns
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(rms) 1855 1026 sh
384 /Times-Roman f1
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192 /Times-Roman f1
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end MTsave restore
d MATH {
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2b. Lower frequencies
Its actually worse than this: in an OTF map, you can scan at the Nyquist rate, so if you want the fastest map you can go l2 times faster due to the larger beam. But then your point-source sensitivity gets worse by l! This takes care of the other l1.
So (eg) for HOPS with a Tsys ~ 75 K, you can go ~64 times faster for Nyquist-sampled maps, but then your Trms ~ 0.8 K. Or you can go 4 times faster to recover Trms ~ 0.2 K (although really youd want Trms < 0.1 K for ammonia). So HOPS can only detect bright hot cores, and a similar problem holds at 7mm. This is not the kind of MMWS we are talking about.
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Workarounds
2b. Lower frequencies
Its actually worse than this: in an OTF map, you can scan at the Nyquist rate, so if you want the fastest map you can go l2 times faster due to the larger beam. But then your point-source sensitivity gets worse by l! This takes care of the other l1.
So (eg) for HOPS with a Tsys ~ 75 K, you can go ~64 times faster for Nyquist-sampled maps, but then your Trms ~ 0.8 K. Or you can go 4 times faster to recover Trms ~ 0.2 K (although really youd want Trms < 0.1 K for ammonia). So HOPS can only detect bright hot cores, and a similar problem holds at 7mm. This is not the kind of MMWS we are talking about.
Thank you for playing! DSET 2 H 4
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Workarounds
3. The one exception (ok, two exceptions)
Cleverly neglected in previous discussion is any mention of observing 12CO or 13CO at Mopra. Typically for Galactic clouds,
TA*(12CO) ~ 10 TA*(C18O) (7a)
and TA*(13CO) ~ 5 TA*(C18O) (7b)
So to get the same S/N for 12CO or 13CO maps as we usually do for C18O maps, we need only integrate for Trms2 as long:
tsurvey(13CO) = tsurvey(C18O) (4/25) = 320 days (8a)
tsurvey(12CO) = tsurvey(C18O) (4/100) = 80 days (8b)
where we have also allowed for Tsys (110 GHz) ~ 2Tsys (90 GHz).
NOTE: these are S/N requirements only! DSET 2 H 8
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How to get there
The sample time
But how do we get Nyquist-sampled maps so quickly? The key is the MOPS systems data dump rate, currently fixed at 2 sec. This fixes the Nyquist-sampled scan rate as well during an OTF, as in eqs. (35). If we have lines that are bright enough, we could scan much faster with an accelerated dump rate.
Suppose tdump = 0.32 sec, then eq. (4) becomes
tmap(13CO) = 17 min. (9)
for a Nyquist-sampled 55 OTF map with Trms = 1.0 K, which is roughly what we need for 13CO in eq. (8a) (ok, so I cheated).
If we can get this dump rate with even 2 dual-polarisation zoom modes (instead of 16), then we get 12CO at the same sensitivity, for free. DSET 2 H <
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Justification post facto
A real survey
This is exactly what we want: a dual 12CO and 13CO survey at 1K rms per 0.1 km/s channel over 100 deg2, which will take 320 days including overheads(!) of continuous telescope time.
If we allow for smoothing to 0.2 km/s channels, this can be achieved as a Mopra Key Project in just 3 winter seasons assuming it can be run for 16 hours/day over 12 weeks in each season (or some combination of similar numbers). However we can probably do ~2x better if we use the existing Nanten 12CO maps as finder charts for MMWS.
A built-in finder chart
Subsequent deeper integrations can always be added in selected areas, eg to flesh out the 13CO maps, and we have our complete set of finder charts for other 3712 mm tracers. DSET 2 H @
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P Benefit
Maximum downstream applications
The general nature of such a survey will guarantee maximum flexibility and usefulness for subsequent investigations, whether at ATCA, ALMA, or anywhere else.
Prompt availability of data cubes from a pipeline reduction process to the community will be essential, for all imaginable follow-up projects. FITS- and Virtual-Observatory-compatible format will both be desirable.
Besides finder chart generation, extensions to the MMWS in later seasons can be conducted in a number of ways: extending in l and/or b, deeper integrations for 12CO outflows and/or 13CO extents, comparison with ATLASGAL, GRS, GLIMPSE, HI-GAL, etc. These options are limited only by the communitys imagination! DSET 2 H D T
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Final warning
Objects in mirror are closer than they appear, or,
Dont try this at home, kids!
This is a VAST project, way too big for anything less than a community-wide effort. (Eg, CHaMP has ~300 Gb raw data from 10 weeks on the telescope: reduction and analysis is a major logistical challenge.) A data management and publication plan must be devised and agreed beforehand.
Let us be perfectly frank: if we are to use MMWS to stave off repeated attempts to shut Mopra down, we are fighting an uphill battle against the entrenched cm-bias in Australian radio astronomy. Nothing less than a unified mm-community approach will succeed.
We all have to be part of this. DSET 2 H H h 8 {
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