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| ==== Rough fluxes ==== |
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| The fluxes measured at the 30m can be compared with theoretical predictions from planetary models: | ==== Accurate fluxes ==== For accurate fluxes, use the following predictions from recent planetary models: |
Useful information for observations
Back to the NIKA2 Run 1 main page
Contents
List of Astronomical Target for NIKA2 (from NIKA2R1.sou)
Here is the full detailed formatted list Full list with some fluxes. And here is the catalog for Pako has to be RENAMED to NIKA2R1.sou on the pako computer.
LST coverage (created with nika2.astro by CK)
Radio sources from IRAM catalog nika2-radio.pdf.
Planets, Asteroids, and Secondary Calibrators (from Lisenfeld+2000) nika2-secondaries.pdf
Strong Galactic sources nika2-galactic.pdf
Weak Galactic sources nika2-weak-galactic.pdf
Nearby galaxies nika2-nearby-galaxies.pdf
Distant galaxies or faint quasars nika2-distant.pdf
Details on planets and asteroids
Mars and Uranus are well known primary calibrators for photometric calibration and for beam maps. Jupiter, Saturn can be used for the errorbeams or to map the satellites.
Rough fluxes
The following table gives some rough numbers for the fluxes. Note that some are strongly varying.
Name |
Right Ascension |
Declination |
Diam (arcsec) |
Flux @ 1.15 mm Jy |
Flux @ 2.00 mm |
TB K |
MERCURY |
12:04:33.0985 |
00:13:18.988 |
8.25x8.25 |
1156.5 |
387.2 |
450 |
MARS |
10:46:24.9914 |
09:12:15.947 |
4.00x3.98 |
117.08 |
39.50 |
198 |
JUPITER |
10:57:47.6613 |
07:38:57.99 |
31.77x29.71 |
5928.86 |
2004.54 |
170 |
SATURN |
16:00:29.2947 |
-18:50:13.907 |
15.49x13.83 |
1181.45 |
400.29 |
150 |
URANUS |
01:09:34.4370 |
06:39:29.520 |
3.69x3.58 |
44.01 |
18.44 |
93 @1mm, 113 @2mm |
NEPTUNE |
22:37:43.8247 |
-09:32:13.503 |
2.30x2.24 |
17.16 |
7.19 |
93 @1mm, 113 @2mm (yes, same as Uranus) |
Accurate fluxes
For accurate fluxes, use the following predictions from recent planetary models:
- For Uranus and Neptune:
Download the ESA2 templates of the model of Moreno 2010 ("Neptune and Uranus planetary brightness temperature tabulation. Technical report, ESA Herschel Science Center).
Download the ESA4 templates of the models of Moreno and Orton described by Bendo et al. 2013 (Flux calibration of the Herschel-SPIRE photometer, MNRAS 433, 3062, 2013).
- For Mars:
Visit the web page of Emmanuel Lelloche. It will ask for the HPBW at 300 GHz which is ~8" at the 30m.
In addition to that, check the Pointing sources and calibrators wiki page by IH.
Interface with the telescope: Pako
Short manual on useful "Pako for Nika" see on Granada computers on the NIKA directory Pako_helpv??.txt ??? OR IS THERE NOW A PAKO WIKI ???
- Pako scripts are in the Pako subdirectory
- Before starting the pointing session, we may be requested to move the azimuth by 60deg to reset the inclinometer of the az axis.
- Always stay at more that 1 deg from the Sun. There are internal safeties that prevent the antenna to point to the Sun, but we may not get error messages.
- The antenna can point between 60 and 460 degrees in azimuth, between 20 and 80 degrees in elevation.
- If a source is available both at low and high azimuth, use command SET TOPO LOW (or SET TOPO HIGH) to stay on the source without moving.
- The minimum number of sources to observe for the pointing model is 15. 30 is good enough.
- the pointing sources should be observed on 'short' period, e.g. 3-4 hours to avoid daily pointing variations.
Commissioning requirements and observations plan
see private wiki