| ID | Name | Coveragea | Areab | Time | Speed |
|---|---|---|---|---|---|
| A | Low Latitudec,d | 167 < l < 360, 0 < l < 79, 0.00 < |b| < 2.75 | 1496 d2 | 2250 hr | 0.66 d2/hr |
| B | Intermediate Latitudec,e | 167 < l < 360, 0 < l < 79, 2.50 < |b| < 10.00 | 4080 d2 | 1700 hr | 2.40 d2/hr |
| C | Magellanic Clouds | 4:45 < RA < 6:10, -72 < Dec < -64 0:30 < RA < 1:30, -74 < Dec < -70 | 64 d2 28 d2 | 700 hr | 0.13 d2/hr |
| D | Magellanic Bridge + Stream | ? | 5000 d2 | 2100 hr | 2.38 d2/hr |
| E | Galactic Center + Bulge | ? | 150 d2 | 1000 hr | 0.15 d2/hr |
| F | High-Latitude Fields | ? | 1100 d2 | 450 hr | 2.44 d2/hr |
| G | Molecular Clouds + H II Regions | ? | 300 d2 | 500 hr | 0.60 d2/hr |
| Total Surveyf | 12,218 d2 | 8700 hr |
| a Mapped with ASKAP composite fields, each a 5.5-degree-wide square containing 30 individual ASKAP fields (1.25-deg primary beam @ 21cm) in a fixed hexagonal lattice (see Simon Johnston diagram, December 2008). |
| b Areas near Galactic plane are Cartesian. |
| c Longitude ranges are consistent with Dec < +40 deg at Galactic equator. |
| d Covered by a single row of ASKAP composite fields at the Galactic equator |
| e Covered by a set of ASKAP composite fields arrayed on either side of the low-lat strip |
| f Simple area sum ignores overlaps. |
| Component | Species | Frequency Range | # Channels | Channel Width | Velocity Range | |
|---|---|---|---|---|---|---|
| A - F (original) | H I | 1416.4 - 1424.4 MHz | 6,900 | 1.16 kHz | 0.245 km/s | |vlsr| < 845 km/s |
| OH | 1610 - 1614 MHz + 1663 - 1669 MHz | 8,650 | 1.16 kHz | 0.216 km/s + 0.209 km/s | |vlsr| < 372 km/s + |vlsr| < 360 km/s | |
| A - F (revised) | H I | 1417.2 - 1423.6 MHz | 6,384 | 1.00 kHz | 0.211 km/s | |vlsr| < 674 km/s |
| OH | 1610 - 1614 MHz + 1663 - 1669 MHz | 10,000 | 1.00 kHz | 0.186 km/s + 0.180 km/s | |vlsr| < 372 km/s + |vlsr| < 360 km/s | |
| G | RRLs + Complex molecules | 16 sub-bands within 1480 - 1780 MHz | 1024 per sub-band | 2.30 kHz | 0.466 km/s to 0.388 km/s | |vlsr| < 238 km/s to |vlsr| < 198 km/s per sub-band |
| Component Groupa | Mapping Speed | Dwell Time (30 d2 field) | Beamb FWHM | Trmsc,d,e [5 kHz] | Srmsd,e [5 kHz] |
|---|---|---|---|---|---|
| Magellanic Clouds Galactic Center Galactic Bulge (C + E) |
0.15 d2/hr | 200 hr | 20'' | 0.76 K | 0.5 mJy |
| 30'' | 0.40 K | 0.6 mJy | |||
| 60'' | 0.14 K | ? | |||
| 90'' | 0.09 K | 1.3 mJy | |||
| 180'' | 0.04 K | 2.3 mJy | |||
| Low Latitude Molecular Clouds H II Regions (A + G) |
0.6 d2/hr | 50 hr | 20'' | 1.51 K | 1.0 mJy |
| 30'' | 0.81 K | 1.2 mJy | |||
| 60'' | 0.28 K | ? | |||
| 90'' | 0.19 K | 2.6 mJy | |||
| 180'' | 0.08 K | 4.6 mJy | |||
| Intermediate Latitude Magellanic Bridge Magellanic Stream High-Latitude Fields (B + D + F) |
2.4 d2/hr | 12.5 hr | 20'' | 3.02 K | 2.0 mJy |
| 30'' | 1.62 K | 2.4 mJy | |||
| 60'' | 0.56 K | ? | |||
| 90'' | 0.37 K | 5.2 mJy | |||
| 180'' | 0.15 K | 9.2 mJy |
| a Actual component speeds and sensitivities vary slightly from these cases. |
| b Some tabulated 18'' beam sensitivity data has been used here for 20''. |
| c From Westmeier's Surface Brightness Sensitivity Calculator. |
| d Adapted from ASKAP Array Configuration page. |
| e For 1 kHz channels, multiply by 2.24; for 25 kHz channels, divide by 2.24. |
| Paper | Telescope | Beam | Channels | Trms | Tpeak |
|---|---|---|---|---|---|
| Turner (1979) | GB 43m | 25' | 7.5 kHz | ~ 0.18 K | ? |
| Frail et al. (1996) | GB 43m | 25' | 4.9 kHz | ~ 0.03 K | ? |
| Li & Goldsmith (2003) | AO 305m | 3.9' | 0.7 kHz | ~ 0.1 K | 0.5 - 1.5 K |
| Kavars (2006) | GBT 100m | 11' | 1.5 kHz | ~ 0.015 K | 0.07 - 0.37 K |
| Trms | OH Line Detection Regime |
For proper quantity, multiply all these by line FWHM in km/s! | ||||
|---|---|---|---|---|---|---|
| NOH(1667)/dva [cm-2/km/s] |
NH2/dvb [cm-2/km/s] |
AV/dvc [mag/km/s] |
PI(12CO)/dvd [K] |
I(100um)/dve [MJy/sr/km/s] |
||
| 1.0 | -- | 6.66e+14 | 6.66e+21 | 4.00 | 29. | 33. |
| 0.5 | strongest OH? | 3.33e+14 | 3.33e+21 | 2.00 | 14. | 17. |
| 0.2 | bright T79,LG03 | 1.33e+14 | 1.33e+21 | 0.80 | 5.8 | 6.6 |
| 0.1 | faint T79, LG03 | 6.66e+13 | 6.66e+20 | 0.40 | 2.9 | 3.3 |
| 0.05 | F96, strong K06 | 3.33e+13 | 3.33e+20 | 0.20 | 1.5 | 1.7 |
| 0.02 | faint K06 | 1.33e+13 | 1.33e+20 | 0.08 | 0.58 | 0.66 |
| 0.01 | ? | 6.66e+12 | 6.66e+19 | 0.04 | 0.29 | 0.33 |
| a Presuming OH lines with brightness Tb > 3 * Trms |
| b Minimal detectable OH 1667 column is 3 * Trms * 2.22e+14 * dvFWHM (adapted from Li & Goldsmith 2003). |
| c Inferred minimal H2 column is 1.0e+07 * NOH(1667) (from Liszt & Lucas 1999). |
| d Inferred optical exinction AV = NH2(RV=3) / 1.7e+21 (from Snow & McCall 2006). |
| e CO line profile integral PI(12CO) = NH2 / 2.3e+20 (from Strong et al. 1988). Note the CO X-factor is highly variable, and implied CO columns here may be significant overestimates for diffuse cloud envelopes! |
| f Far-infrared dust surface brightness I(100um) = 2 * NH2 / 1.0e+20 (from Reach et al. 1994). |
| Cloud Type | f(H2)b | f(C+)c | f(CO)d | AVe [mag] | nHf [cm-3] | Tkg [K] | NHh [cm-2] |
|---|---|---|---|---|---|---|---|
| Diffuse Atomic | < 0.1 | ? | ? | >~ 0.0 | 10 - 100 | 30 - 100 | |
| Diffuse Molecular | > 0.1 | < 0.5 | ? | >~ 0.2 | 100 - 500i | 30 - 100 | >~ 3.4e+20 |
| Translucent Mol. | ? | > 0.5 | < 0.9 | >~ 1 - 2 | 500 - 5000? | 15 - 50? | >~ 1.7e+21 - 3.4e+21 |
| Dense Molecular | ? | ? | > 0.9 | >~ 5 - 10 | > 10,000 | 10 - 50 | >~ 8.5e+21 - 1.7e+22 |
| a Most data from Snow & McCall (2006, Table 1) |
| b Fraction of total hydrogen gas in H2 |
| c Fraction of total carbon gas in C II |
| d Fraction of total carbon gas in CO |
| e V-band optical extinction |
| f Total hydrogen gas particle volume density |
| g Gas kinetic temperature |
| h Total hydrogen gas particle column density: NH(RV=3) = 1.7e+21*AV |
| i Regime of Perseus shock HISA clouds in Gibson et al. (2000) + Klaassen et al. (2005) |
