#acl NikaBolometer:read,write,delete Default
NIKA Run 1 offline processing results (FXD)
--------
In principle, efficiencies due to the filtering method have been taken into account 

|| '''Source'''    || '''Date''' || '''Flux''' || '''Stat. Error''' || '''Comments'''                              || '''Map'''                                              ||  '''Scan info'''||
||   Mars          || 20091024...||     130Jy  || -                 ||       Primary calibrator                    ||{{attachment:AzelMap2_Mars_20091024_60_67.jpg}}         ||       60-67          ||
||   3C273         || 2009102 5 & 7   ||     13.1Jy ||  0.1              ||                                             ||{{attachment:AzelMap2_3C273_20091027_66_67.jpg}}   ||      66-67           ||
||   3C345         || 20091024   ||    5.051Jy ||    0.009          ||                                             ||  {{attachment:AzelMap2_3C345_20091024_69_73.jpg}}      ||           69-72 ||
||   G34.3         || 20091024   ||  4.761Jy   ||          0.024    ||   Peak flux, source is extended,            ||  {{attachment:RadecMap2_G34.3_20091024_106_106.jpg}}   ||            106  ||
||   K3_50A        || 20091024   ||  1.442Jy   ||       0.008       ||    Peak flux, source is extended            ||  {{attachment:RadecMap2_K3-50A_20091024_102_104.jpg}}  ||         102-104 ||
||   MWC349        || 20091024   ||   1.364Jy  ||      0.010        ||                                             ||  {{attachment:AzelMap_MWC349_20091024_94_96.jpg}}     ||          94-96  ||
||   B1418+546     || 20091024   ||  1.18Jy    ||  0.040            ||     Flux decreasing (known reasons)         ||  {{attachment:AzelMap2_B1418+546_20091025_104_126.jpg}} ||      75-82           ||
||   M87           || 20091027   ||     ~0.8Jy ||                   ||      Extended , det. eff decreasing         ||  {{attachment:RadecMap3_M87nowob_20091027_84_95.jpg}}          ||  84-96 ||
||   WR147         || 20091025   ||  263mJy    ||    24             ||     Detected.                               ||  {{attachment:AzelMap2_WR147_20091025_129_148.jpg}}          ||        129-148  ||
||   Arp220=IC4553 || 20091025   ||  114mJy    ||    18mJy          ||                                             ||  {{attachment:AzelMap2_Arp220_20091027_123_165.jpg}}          ||                 ||
||   B1800+440     || 20091024   ||  103mJy    ||    7mJy           ||                                             ||  {{attachment:AzelMap2_B1800+440_20091024_98_99.jpg}}          ||           98-99 ||
||   PCyg          || 20091024   || 28mJy      ||    4mJy           ||                                             ||  {{attachment:AzelMap2_PCyg_20091024_85_92.jpg}}          ||           84-92 ||
||   Pluto         || 20091025   ||     12mJy  ||     23            ||    Not detected                             ||  {{attachment:AzelMap2_Pluto_20091025_93_102.jpg}}          ||  93-102 ||
||   GRB091024     || 20091024   ||  6.6mJy    ||    4.8mJy         ||     Heavy weight on first 2 scans           ||           || 18scans, 115-137     ||
||   M51           || 20091024   ||  1.5mJy    ||     12mJy         ||    PS flux at the center, no detection      ||  {{attachment:AzelMap2_M51_20091024_108_113.jpg}}          ||      108-113    ||


Arp220: Expect 43mJy (from 1 to 3 mm PdB interpolate), result a bit high, One article quote 88+-8

G34.3: Sandell gives 12.5 Jy in 27" photometry

WR147: Expected is 200mJy Altenhoff, 1994, but some variability expected

Pluto: 35K (Stern Science 1993, 261, 5129), expect 4 mJy

Note on sensitivity
--------------------

We neglect atm. opacity effect ( between 5 and 10% at most)

* NEFDscan= 276 mJy s1/2 for 120x120 arcsecond field (eg M51)
   NEFDscan= 200 for 90x90 (eg GRB)

NEFDscan= [ NEFDdet/ sqrt(Ndet) ] * sqrt( Omega/ Airy)
with Omega being the field solid angle (eg 120x120) and Airy is the Airy
solid angle (taken as corresponding to a disk of 19" diameter).

Hence we get NEFDdet=190 mJy s1/2 (compatible with 120 and 90 arcsecond
size field observations)
For 2 GRB scans, we even got 90 mJy s1/2 but we agree that it is
advisable NOT to publish that number as it is not representative of the
campaign.

* NEFDairy= NEFDdet/sqrt(Kovers)
Kovers=1/0.632=2.5 (pessimistic)

NEFDairy= 120 mJy s1/2

that can be compared with a classical single horn bolometer sensitivity.
Let us keep in mind that this is one polarization KID. To really compare
we have to divide by a factor between 2 and sqrt(2). We have also
purposedly used the average sensitivity of all the kids (as obtained from
NEFDscan) and not the best ones. That's another factor 1.5 to 2 if we
could homogeneize the array. So, all in all the NIKA Oct 2009
sensitivity becomes (30 to 60 mJy s1/2) comparable to Mambo2 (35 mJy
s1/2 at zenith) although at different frequencies

* To convert to NET, we use the total beam of 0.15 arcmin2 as obtained
from aperture photometry. This is correct for diffuse extended sources.
Mars at 205K is diluted by the beam by a factor 0.103 so that Mars (167
Jy at 2.1mm) is equivalent to a 21.2K blackbody so that
NETairy= NEFDairy* 21.2/167Jy=

NETairy = 15 mK s1/2

* Going to a more uncertain number the NEP:
Using DeltaNu/Nu=0.3, a total transmission of 0.30 (for example an
instrument transmission of 0.6 and a main beam efficiency of 0.5) and
one polarization, I get, in agreement with Alessandro, that the power
from Mars on the central pixel is 1.4 pW, but I use 0.8 pW to take into
account the larger spread of the beam (factor 1.7=3.6/5*2.3) hence the
NEFDdet converts to (back to Hz1/2)
NEP= sqrt(2) 0.8E-12/167* 190E-3=

NEP = 1.3 E-15 W/sqrt(Hz)

Overall, an increase by a factor 5 in sensitivity is withing reach for
the next campaign, by gaining on
- the homogeneity
- the noise
- the spectral bandpass
- the straylight


For the article, I would quote NEFDairy (useful for astronomers), NET
(useful for cosmology and extended source) and NEP (useful for Kid
makers, no kidding)