List of Astronomical Target for Nika Oct 2011 run3

FXD: Final version before run (12/10/2011), SL update Pako help and IRAM pointing sources (14/10/2011)

Back to the NIKA run3 page

1. Planets Mars, Venus (too big, 57 arcsec), Uranus, Neptune for photometric calibration (primary calibrators)

Here are the ephemerides for the planets

and the other objects LST Pointing quasars Strong galactic sources Weak galactic sources External galaxies High-z galaxies Clusters of galaxies

2. Usual bright quasars

• for image quality and linearity checks

3. List of bright ultracompact HII regions

• for photometric calibration checks (secondary calibrators)

4. Extended emission from

• Herschel new sources
• bright galaxies M87 (again), M82, others
• less bright NGC1068 22mJy at 1.3mm rising to 36 at 3mm

• --> Need fast speed scanning to reduce 1/f residual noise

5. Faint quasars in the 10 mJy range at 1mm (use Omont&Cox + Herschel list)

• test detectability in faint source mode: e.g.
• J075618.14+410408.6 z= 5.09 20.15 1.3 mm 5.5 ± 0.5 Wang et al 2008, ApJ, 135, 1201
• J092721.82+200123.7 z= 5.77 19.87g 1.3 mm 5.0 ± 0.8 mJy 3.5 mm: 0.12 ± 0.03 mJy
• IRAS F10214+4724 = SDSS J102434.56+470909.5 1.3mm: 10 mJy
• H1413+517 14h15m46.240s +11d29m43.40s z=2.558 1.3mm 18+-2 mJy

6 Cluster of galaxies:

• Main target MS0451, 04h54m11.0s, -03d00'53", z=0.55, y0=3E-4, rc=60" seen by ; Bolocam, ACT, CARMA
• other targets include
  • RXJ1347-1145 (maybe too close to the sun), A665, A2163 and CL0016+16
  If sensitivity allows demonstrate the ability to map clusters (one of the main scientific goals of this camera).

7. Blind survey

Field coordinates

Aztec1 09h59m42.86s, +02d29'38.2", z=4.65, S1.3mm= 9.4+-1.6 mJy, S850=16mJy, Smolcic 2011, ApJL 731, L27

and/or

GN20 12h37m11.90s, +62d22'12.1", z=4.055, S850um=30mJy, 3.3mm=0.33mJy, Daddi et al 2009, ApJ, 694, 1517

Need 10x10 arcmin field with known faint sources. Hope to achieve 1mJy 1sigma in 1 hour with a 2x2 arcmin field of view (times 25 in 25h) : 25hours total

Here is the full detailed formatted list Source_list_fmt2011v2.2.txt with fluxes (Final version 20111023)

Here is the catalog for Pako NIKA2011v2.2.sou.txt has to be RENAMED to NIKA.sou on the pako computer (Final version 20111023)

Here is a list of IRAM pointing sources with fluxes at 3mm and 2mm (I miss fluxes at 1mm, SL) IRAM_pointing_sources_with_fluxes.xls

Here is a short manual on useful "Pako for Nika" commands Pako_helpv8.txt => updated among few other things with (v3..v5) the correct project name for this run: t21, and warning about the need for the correct project name for NCS, some typos, (v6) information about topology, backend choice, scanning speed, (v7) obligation to choose heterodyne devices in Pako otherwise no fits files in ncsServer !, (v8) command to run Xephem with the telescope position displayed in real time.

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 cession, updated with choice of receiver and backend allowing to get fits files, updated with correct focus and correct nasmyth offset deduced from pointing model cession from 17 to 18/10/2011 night.

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.

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)

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)

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')

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')

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')

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)

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)

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)

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