Informations useful for the observations: List of astronomical Target, Pako scripts, Observing strategies

List of Astronomical Target for Nika End 2012 run5

FXD: First version for planets (14/06/2012) v2 (2/10/2012) prepare Thursday teleconf

Back to the NIKA run5 page

1. Planets Mars, Uranus, Neptune for photometric calibration (primary calibrators)

Here are the ephemeris for the planets

2. Usual bright quasars

• for image quality and linearity checks

Pointing quasars

3. Strong Galactic sources

• for secondary calibration and science

Strong galactic sources

4. Weak Galactic sources

• for photometric calibration checks (secondary calibrators)

Weak galactic sources

5. External extended galaxies

• for Science demonstration (mapping)

Nearby galaxies

6. High redshift sources

• for Science demonstration (sensitivity)

Distant galaxies

7. Deep survey and SZ sources

• for Science demonstration (sensitivity)

Deep survey and cluster of galaxies

Here is the full detailed formatted list Full list with fluxes

Here is the catalog for Pako NIKA2012N5v1.0.sou.txt has to be RENAMED to NIKA.sou on the pako computer Here is a list of IRAM pointing sources with fluxes at 3mm and 2mm (I miss fluxes at 1mm, SL) FluxForPointingSources

Interface with the telescope: Pako

Here is a short manual on useful "Pako for Nika" commands Pako_helpv10.txt

Here is a collection of Pako scripts to gain time and have a reference on the observations we will do (to use them rename the files without the .txt, 2nd version updated with slower mapping speed to minimize tracking errors, 3rd version include pako line continuation sign (-)):

nini.pako => run the initial series of commands that always have to be run at the beginning of an observing session, updated with choice of receiver and backend allowing to get fits files, updated with correct focus and correct nasmyth offset deduced from pointing model session from 17 to 18/10/2011 night.

ListAstroTargetNika3/OTF_pointing.pako => OTFMAP 100"x84" in 22 subscan x 10 s = 4+1 ~= 5 min (10"/s) with 2.6 samples (subscan step) per convolved 1mm HPBW (for pointing & focus). 10s = minimum subscan time possible (Pako doesn't authorizes less), hence the choice of subscan length. Scan height changed from 60" to 92" to have more margins for the useful pixels.

ListAstroTargetNika3/OTF_geometry.pako => OTFMAP 300"x220" in 56 subscan x 20 s = 19+3 ~= 22 min (15"/s) with 2.6 samples (subscan step) per convolved 1mm HPBW (for the array geometry = pixels map in sky)

ListAstroTargetNika3/OTF_ps.pako => OTFMAP 140"x90" in 19 subscan x 14 s = 4+1 ~= 5 min (10"/s) with 2 sample (subscan step) per convolved 1mm HPBW (for point source observations)

ListAstroTargetNika3/OTF_2x2.pako => OTFMAP 120"x120" in 25 subscan x 12 s = 5+1 ~= 6 min (10"/s) with 2 samples (subscan step) per convolved 1mm HPBW (for extended source < 2')

ListAstroTargetNika3/OTF_5x5.pako => OTFMAP 300"x300" in 51 subscan x 20 s = 17+3 ~= 20 min (15"/s) with 1.7 samples (subscan step) per convolved 1mm HPBW (for extended source < 5')

ListAstroTargetNika3/OTF_10x10.pako => OTFMAP 600"x600" in 41 subscan x 30 s = 20+4 ~= 24 min (20"/s) with 0.7 samples (subscan step) per convolved 1mm HPBW (for very extended source < 10')

ListAstroTargetNika3/OTF_faint_source.pako => OTFMAP 120"x80" in 21 subscan x 12 s = 4.2+0.8 ~= 5 min (10"/s) with 2.6 samples (subscan step) per convolved 1mm HPBW (for faint sources)

ListAstroTargetNika3/OTF_deep_field.pako => OTFMAP 360"x360" in 61 subscan x 20 s = 20+4 ~= 24 min (18"/s) with 1.7 samples (subscan step) per convolved 1mm HPBW (for faint sources)

ListAstroTargetNika3/OTF_sz.pako => OTFMAP 360"x240" in 41 subscan x 20 s = 14+3 ~= 17 min (18"/s) with 1.7 samples (subscan step) per convolved 1mm HPBW (for faint sources)

ListAstroTargetNika3/OTF_moon.pako => OTFMAP 2000x 2000 in 34 subscan x 40 s = 23+3 ~= 26 min with 0.17 samples (subscan step = 60) per convolved 1mm HPBW (to look at the moon in bad weather)

Here's an excel sheet which helps to find the best focus thanks to a 2nd order polynomial line trend fitting on beam width and amplitude (note that amplitude is much more robust):

Full focus Excel only,

Best focus with basic 2nd order polynomial

Status of observations

spread sheet of sources with integrated time

Observing procedures, strategies for performance verification and debugging

• v1 starting from discussions between FXD, RZ, NP & SL on 30/5/2012 v2 2/10/2012 elaborate on results from previous runs =

• Use the NIKA pointing model as the starting reference, setting Nasmyth offsets to 0. (NIKA pointing model is close to EMIR one)
• Do a "classical" POINTING (cross)
• Do a "NIKA type" OTF-POINTING
• Implement Nasmyth correction to point on the central pixel
• Check with POINTING
• 1st crude Focus without Wobbler: FOCUS sequence
• 1st OTF-GEOMETRY (scan width = baseline x 2 + FOV + max pointing error = 1x2 + 2.5 + 1 + 0.5 = 5')

• 1st OTF pointing session (as many quasars as possible in the 8 h slot, probably ~20 ?) => define the NIKA pointing model (20 is not enough stat for a clear determination, but should be OK at 1st order)

• OTF-GEOMETRY for different foci => focus characteristics for all pixels

• OTF pointing session => define a better NIKA pointing model

• test skydip going at high airmass values (at least 3)
• observe typical calibrators 1-20 Jy (e.g. OJ)
• observe known fainter sources (e.g. Tau sources)
• redo this procedure the next day

Note: good focus depend on geometry which depend on focus ==> iterative process.

How to find the elevation axis with the observation ? This is degenerate with the pointing model => Iterative approach => accumulate statistics. Due to the degeneracy one as to make a choice on the strategy for the definition of the center of rotation of the array (rotation with elevation of the sky image). After discussions the next days: at the start of the run we will choose the best of the 4 pixels at the center of the array and define it as the center for the pointing model.

For skydips: for each subscan, a calibration is done in order to find the central frequency of each kid

How to investigate the plateau, beam broadening etc. => gain of amplifiers and power on the tone are the hardware parameters that we will change => write the information in Wiki log pages (this is in the raw data anyway, but discuss with Alain to get all the info in the FITS).

IMBFITS format: keep same structure as before run (e.g. with a fixed number of pixels close to the maximum available, not a varying number of pixels)

Strategy to investigate the Plateau

Since we see the plateau on 31/05/2012 pointing scans with crosses patterns, we will use these fast scans to investigate the plateau, the width should be larger than the plateau itself, that is to say bigger than the array with margins ==> 3 arcmin widths.

So far (01/06/2012) we identify 3 hardware parameters we could play on:

• Limit the total power in the acquisition line: play with 2 different values of the DAC => at least 2 scans

• Limit the number of tones generated (e.g. probe all pixels, or only one which means generating only one tone, or only one part of the array) => at least 2 scans

• Move the tones frequencies by a small amount to place them on a different location on the slope of the resonance => at least 3 scans

• Repeat the procedure at least twice to check repeatability => 14 scans minimum

==> This should allow us to determine whether the plateau is a pure electronic effect, and have ideas on what causes it.

Science demonstration requirement

TBW