ASTE Calibrator List
Observers are strongly recommended to make observing tables for observations of standard sources and pointing sources in their own group/project.
You can use device tables and source tables in group/project of aste10/calib10. However, if you copy the observing tables(***.start) to in the following group/project to your group/project, the observed data will be store in aste10/calib10, and the data delivery will be delayed.
Please do not copy observing tables with the extension of .start or .tune in aste10/calib10 to your group/project.
- Group: aste10
- Project: calib10
Standard sources
- We recommend to observe a standard source once per two to three hours.
- The standard chopper wheel calibration technique with a radio absorber at ambient temperature is used to derive the antenna temperature of a source corrected for atmospheric extinction.
- The main bean efficiency can be derived by comparing the integrated intensity of the observed source with that by a telescope with the same aperture diameter as ASTE corrected for SSB obtained. Please see the following references for spectra to be compared.
- [1]Wang et al. 1994, ApJS, 95, 503 (CSO 10m CO(3-2), CS(7-6) observations of e.g., IRC+10216 and M17SW)
- [2]Schilke et al. 1997, ApJS, 108, 301 (CSO 10m line survey of OriKL at 350GHz)
| Standard source | R.A. (B1950) | Dec. (B1950) | VLSR (km/s) | Off position (offset, RA-Dec) |
|---|---|---|---|---|
| IRC10216 (CW Leo) | 09:45:14.8 | +13:30:40.0 | -26 | (-00:06:00.0, +00:00:00.0) |
| M17SW | 18:17:30.0 | -16:13:06.0 | +20 | (+00:12:35.0, +00:03:11.0) |
| Orion KL | 05:32:46.7 | -05:24:17.0 | +9 | (+00:30:00.0, +00:00:00.0) |
| W28 | 17:57:26.8 | -24:03:54.0 | +4 | (-00:10:00.0, +00:00:00.0) |
| W44 | 18:50:46.1 | +01:11:11.0 | +45 | (-00:25:00.0, +00:00:00.0) |
| W51D | 19:21:22.2 | +14:25:17.0 | +55 | (-00:25:00.0, +00:00:00.0) |
| Molecular Line | Frest (GHz) |
|---|---|
| C18O(3-2) | 329.330546 |
| 13CO(3-2) | 330.587960 |
| CS(7-6) | 342.882866 |
| 12CO(3-2) | 345.795991 |
| HCN(4-3) | 354.505480 |
| HCO+(4-3) | 356.734242 |
| Source name | Molecular line | Preview |
|---|---|---|
| IRC10216 (CW Leo) | 12CO(3-2) | view spectra |
| Orion KL | 12CO(3-2) | view spectra |
Pointing sources
- Cross-scan continuum observations of a planet, or 5-point line observations of a compact CO source will achieve an rms pointing accuracy of ~2 arcsec.
- We recommend to use a pointing source close to the target source as much as possible. Please use a pointing source in the northern (southern) sky for a target in the northern (southern) sky. Otherwise it is possible that a pointing error of ~5 arcsec will occur.
- We recommend to conduct pointing observations one per two hours. Please pay attention to the pointing accuracy especially for about an hour after sunset or sunrise by increasing the frequency of pointing observations.
| Source name | J2000 Coordinate | VLSR (km/s) |
Ta*
#1 (K) |
|
|---|---|---|---|---|
| R.A. (h m s) | Dec. (d ' ") | |||
| WX Psc | 01 06 26.04 | +12 35 52.7 | 9 | 0.8 |
| R Scl | 01 26 58.089 | -32 32 35.67 | -19 | 1.0 |
| O Cet | 02 19 20.797 | -02 58 41.07 | 46 | 7.5 |
| R Hor | 02 53 52.779 | -49 53 22.49 | 38 | 2.1 |
| NML Tau | 03 53 28.86 | +11 24 22.4 | 34 | 1.9 |
| R Dor | 04 36 45.529 | -62 04 38.22 | 7 | 3 |
| GX Mon | 06 52 47.04 | +08 25 18.8 | -9 | 1.0 |
| L2 Pup | 07 13 32.383 | -44 38 20.95 | 33 | 0.9 |
| VY CMa | 07 22 58.336 | -25 46 03.17 | 20 | 1.2 |
| RAFGL 4078 | 07 45 02.41 | -71 19 45.7 | -39 | 1.5 |
| RS Cnc | 09 10 38.794 | +30 57 47.09 | 7 | (1.5) |
| RAFGL 5254 | 09 13 53.94 | -24 51 25.1 | 0 | (2.0) |
| R Leo | 09 47 33.490 | +11 25 43.37 | 0 | (1.0) |
| IRC+10216 | 09 47 57.40 | +13 16 43.5 | -26 | (20) |
| RW LMi | 10 16 02.28 | +30 34 19.0 | -2 | (2.5) |
| U Hya | 10 37 33.291 | -13 23 04.60 | -31 | (1.0) |
| V Hya | 10 51 37.248 | -21 15 00.30 | -16 | (1.8) |
| SW Vir | 13 14 04.370 | -02 48 25.17 | -11 | (0.9) |
| R Hya | 13 29 42.752 | -23 16 52.72 | -10 | (0.5) |
| W Hya | 13 49 01.974 | -28 22 03.88 | 41 | (1.0) |
| RX Boo | 14 24 11.637 | +25 42 13.08 | -10 | (1.1) |
| RAFGL 4202 | 14 52 23.82 | -62 04 19.2 | 23 | 1.0 |
| RAFGL 4211 | 15 11 41.44 | -48 19 59.0 | -4 | 1.8 |
| II Lup | 15 23 05.07 | -51 25 58.7 | -15 | 2.1 |
| IRAS 16594-4656 |
17 03 10.027 | -47 00 27.68 | -25 | 1.4 |
| V2548 Oph | 17 07 58.10 | -24 44 31.1 | -3 | 1.0 |
| V833 Her | 17 31 55.29 | +17 45 20.9 | -3 | 1.0 |
| RAFGL 5379 | 17 44 23.930 | -31 55 39.14 | -23 | 0.9 |
| V5104 Sgr | 18 22 34.68 | -27 06 29.3 | 50 | 0.65 |
| V821 Her | 18 41 54.53 | +17 41 08.4 | 0 | 1.25 |
| V1418 Aql | 19 03 18.44 | +07 30 45.3 | 17 | 0.7 |
| R Aql | 19 06 22.254 | +08 13 47.57 | 47 | 1.5 |
| V1427 Aql | 19 13 58.610 | +00 07 31.90 | 90 | 0.6 |
| W Aql | 19 15 23.35 | -07 02 50.3 | -25 | 2.0 |
| χ Cyg | 19 50 33.910 | +32 54 50.36 | 10 | 2.5 |
| EP Aqr | 21 46 31.850 | -02 12 45.79 | -33 | 2.5 |
| π1 Gru | 22 22 44.222 | -45 56 52.67 | -12 | 2.0 |
| RAFGL 3068 | 23 19 12.60 | +17 11 33.1 | -31 | 1.5 |
- Note #1: 12CO(3-2) antenna temperature.