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Daily reports

New strategy for editing the page: With the log of Saturday it appeared that the ANTI-CHRONOLOGICAL ORDER makes it difficult to follow updates and discussions since the latest entry may answer an older entry possibly difficult to find for someone not following the updates in real time. So we go back to CHRONOLOGICAL ORDER and use the table of content with hyper links TO AVOID ENDLESS SCROLL DOWNS :)

Monday 14-05-2012

Saturday 19-05-2012

Je suis a 490 MHz sur la click FPGA soit un bin de 1.869 MHz je mets 50kHz de deviation modulation sur les 2 bandes matrice A : 1mm : 2.288149 GHz dac 3db HF 0 db sortie 10db - 1 ampli matrice B : 2mm : 1.3013 GHz dac 3db HF 20 db sortie directe - 1 ampli

12h51m11_0001_T scan table xy pas 5mm et 20% (50x50)

13h02m45_0002_B un balayage complet des 2 bandes la 1 mm a beaucoup bouge : je recherche les résonances sur les 2 matrices 13h29m01_B Je relance un balayage 13h31m01_0004_T puis une carte scan table xy pas 5mm et 20% (50x50) 13h48m41_B balayage complet la 1mm est montee en frequence de 110 KHz : je recentre la 1mm et ne touche pas a la 2mm

• petit balayage sur les 2 matrices pour recentrer le bins

13h58m01_0005_T Nouvelle carte avec un pas plus faible (3mm)

• mesures de bruit

14h22m30 balayage complet pour regarder les derives: la 1mm est montee de 140 kHz (on est a 181 mK en train de refroidir lineairement 5mK par heure 14h30m57_0006_T encore une carte pas de 5mm apres un reglage pour voir la stabilite de la photometrie

• Il y a des sauts dus à des erreurs sur la roach A (pas d'erreur sur la roachB) : je fais kill dhclient3 (3304.3)

14h40m20_0007_T Un petit balayage et je refaits une carte : a priori, plus d'erreur et plus de sauts

14h47m50_T 14h50 : corps noir a 12.32 ohm : je chauffe a 20V 1.3A puis 30V 2A

• 14h56 : corps noir a 13.09 ohm puis ca refroidis a nouveau 14h58 : j'enleve le bras et la bille puis je passe 2 fois une feuille de polystyrene mesure de bruit

15h10 : je baisse la puissance de 5db sur la matrice A : dac 3db HF 5 db sortie 5db - 1 ampli

• la frequence monte encore de 250 KHz : je recentre les resonnances qui sont plus belles

15h18m35_B Un balayage complet matrice A 15h20m08_B un petit balayage pour verifier et recentrer 15h22m50 2 passages d'une feuille de polystyrene puis mesure de bruit

Friday 25-05-2012

NIKA was moved into the truck. Early start on Monday for Philippe and Martino.

Monday, 28-05-2012

Alain, Xavier, Samuel and Nico took the plane from Lyon to Granada. Juan picked them up at the aiport and drove all of them up to the observatory. Everybody was happy to be there for dinner and taste Maria-Carmen's special pasta. Poor Philippe and Martino arrived around only around 11pm after a 18 hour road trip. We unloaded the truck and started to plug in computers.

We had the visit of a fox in the evening (photos to come) and from local wild goats. As you can see, the weather is quite nice for now.

Tuesday, 29-05-2012

We only had access to the telescope this morning at 10.30 and started to install all the hardware. It took us until the end of the technical time (16:30) before being ready to cool down; installation a bit longer than we expected with some minor problems to solve (e.g. pressure in the anti-vibration table, the data acquisition computer which died, etc.), but at the end of the day we are nearly there: cooling has started, and the work on the NIKA network is ongoing.

Wednesday 30-05-2012

Cooling down is going according to plan. Better overall cooling speed compared to the last 'critical' run we had in Grenoble. But let's see what happens, Alain is planning to start condensation overnight. To get an idea, below the screenshots of the cooling down so far.

We took a ~1-2h slot in the evening to do the pre-alignment in order to set the final fixed position of M4 for NIKA, and drill holes in the M4 mount in order to screw the locking component. Working on the software, data transfers, and procedures.

Photos: The 3He gas stock for the dilutions stored in the cabin between the elevation motors box and an electric box, the NIKA electronics on top of the cryostat and the dilution circulation unit, laser alignment to define the definitive fixed position of M4 matching the best position of NIKA in the cabin, marking the place for the locking component on M4, drilling holes for the locking component, and Alain doing acrobatics to help blocking M4 at the right position.

Thursday 31-05-2012

Still cooling down. 1.5K at 15h00; looks a bit slower than expected, maybe due to cooling power necessary for the extra black stuff that was added to mitigate further stray light ?

Now that M4 is locked on its NIKA position, put back in place the new M6 (it was removed yesterday so that Gregorio could access the mount of M4 on EMIR side to drill holes for wheel lock), and perform the final laser alignment => extremely fast.

For our observation slot the dilution had not started yet; so we gave away 1h, and took the rest of the slot to test the Pako procedures and correct and finalize the merging of the telescope data with NIKA FITS data. We also improved the ELVIN broadcast. Note that the weather was not suitable for observations anyway (opacity > 1.5).

Dilution started in the evening. 1h (Friday): ~300 mK.

Friday 1-06-2012

T detectors = 200mK at 8h00. AM 12h. 200mK and stable or cooling slowly ? Which steepness ?

Though the temperature was still around 200mK and the weather not great (tau ~1), the 1st 6h session was very useful, with many things to do; here's the main facts:

• First light: we saw Mars nicely on the 2mm array, nothing on the 1mm array
• Many debugging in the acquisition software to get the data and merging with the telescope correctly (the soft has been significantly changed w.r.t last run)
• Visibly the ROACH board of the 1mm channel (acquisition electronics) had a problem; a IQ mixer was suspected; get one from IRAM (thanks to Santiago and Salvador)

• Do observation trying to follow at best the procedure strategy defined on the general observation information page; note we report all the scans general information on dedicated logbook pages, and on another page Offline Processing results

At the end of the session we had enough observations to check IMBFITs format, start and test offline processing, and get first crude information on the array characteristics, e.g. pointing, geometry, focus, response.

At night the temperature was continuing to go down on a gentle slope; we entered the sub-200mK region !

We dismounted the dis-functioning ROACH board, and used a RF-generator and spectrum analyzer from the workshop to investigate the problem: when moving the tones frequencies we saw a very significant attenuation every 50GHz. Visibly the problem was not the mixer.

Saturday 2-06-2012

Good news from the cryostat. Tbm is now 120mK, and it keeps cooling (overnight, the rate was about 2mK/h). So maybe the loooong cooling time is a consequence of all the extra added material (black varnish to prevent straylight) that gives us a huge added thermal capacity, and not to some fundamental issue in the dilution system. We'll see where we get.

Good news also from RoachB. We had been experiencing strange issues (the output of the downconverting IQ mixer changed depending on the LO frequency, sometimes very rapidly, so that the variations due to the resonators were effectively hidden by this effect). Apparently though it was just the consequence of one of the cables of the FPGA I/Q outputs used to generate the tones that was making a false contact (though tightly screwed...). Taking out the cables and putting them back in place solved everything. We are going to take everything up to the cabin again so that we can install it again as soon as possible.

Important note concerning the Roaches! In the end we decided, for the joy of Xavier, to use Roach A for the 2mm array and Roach B for the 1mm array!

Hopefully this afternoon we'll be able to observe using both channels.

AM 12h30. OK, if we are below 150mK not a problem in any case. I am not sure it's the new added material because we have already seen this behaviour with the same old optics and before touching anything. But it is reproducible (last 3-4 runs): 48 hours to start the condensation, 12h to condense and then in another 12 hours below 200mK and cooling very slowly. If don't get worse each time that's already good. Luckly as I said less than 150mK shouldn't make any difference (if we're not planning to use TiN soon, and I think that's not the case). I see the sky is still bad, but there's a number of issues already interesting that are not mentioned in the WIKI. In particular my three more urgent questions are: 1) the plateau is still there or not ? 2) what about the glitches ? 3) is the baseline frequency noise the same we had in lab for these arrays ?

RZ, 13:02 the plateau is there, glitches did not check

AM 13h30. Thanks for the first feedback on the plateau. Uhhmm. If it is the very same plateau (same intensity as in 2011 ?) the simplest 'non-linear electronics' explanation loses points. If on the other hand it's at least weaker .. it would be an indication of something at least. In 2010 we didn't have it; that's the more shocking point. OK, we'll have time later for deeper discussions. Now I wish you all good (at least decent) weather !

Observations 16h - 22h

Cryostat cold at 110 mK. Array 1mm repaired! Cloudy, tau = 0.7.

Mainly dedicated to arrays characterization: pointing, focus, FWHM, geometry, response on Mars, and data formating, and processing.

Test of skydips, and automatic frequency sweeps at each airmass steps.

Few sans also on sources fainter than Mars (OJ286, IRC10216). Too soon to give numbers, but from these 1st observation it seems very likely that the sensitivities are better than run 3.

Tomorrow we will investigate the plateau based on a procedure discussed today.

Sunday 3-06-2012

RZ, 23:29 More news concerning the plateau: it might be focus dependent. The figures below show a negative "plateau" @1mm and a ring "plateau" @2mm in a defocused map. The focus was set to -0.6mm, the correct value should be around -1.5mm. The ring structure of the "plateau" @2mm is best visible in the off res. KIDs. It has to be checked whether focus is really the reason.

JFMP Noise measurements 2mm : 4 Hz/sqrt(Hz) 1mm: 4.5 Hz/sqrt(Hz)

Monday 4-06-2012

RZ, 13:07 Update on the plateau: the off. resonance pixels @1mm show a positive plateau (below), the working pixels show in all but 4 cases a negative plateau (fig. "negative plateau @1mm per pixel" on 3-06-2012).

The plateau introduces quite significant ambiguity in calculation of the beam widths. Whereas @2mm the beam profile can be assumed as a sum of 2 Gaussians, @1mm this is not the case (and it was not during run 3). Further ambiguity introduces the variability of the plateau, i.e. its dependance on focus. The figures below show the cross-scan #155 observed on June 3rd. At 2mm the 1-component fit gives FWHM~20.9*20.5arcsec, the 2-component fit gives FWHM~18.7*18.3arcsec. At 1mm the difference between 1- and 2-component fits is of course larger but - because of the shape of the plateau + the error beam - the fits are not reliable.

To give a hint of an answer to AMs question of 2-6-2012: there are gliches, quite different intensity and number per observation; some clearly correlated between the pixels, some not. Just two examples below. Shown are data of all OK pixels.

Synchronization: there is a remaining mismatch between the time of NIKA and the telescope of roughly -0.1sec.

Update: some statistics on the synchronization.

History of the cryostat cooldown summarized in 4 snapshots of the dilution temperature (cold stage = temperature of the detectors): 6 days, last 4 days, last 3 days, last 2 days. Though the cooling down is pretty long, the behavior of the dilution is perfectly normal ==> let the cryostat at the telescope. Current temperature: 90 mK.

Afternoon events before observations, and more pictures of the cryostat, showing the entrance HDPE lens and the final setup of the electronics for run4:

Observations 16h - 24h

• Mainly dedicated to characterization of the instrument: Pointing, pointing, focus, pointing, geometry; 1 tone, all tones; then some relatively faint sources to get the sensitivity; then back to pointing, focus, geometry.

• Weather conditions were again pretty mediocre; NIKA is a wonderful tool to study anomalous refraction ! Hopefully it is also useful for astronomy when the weather allows it. Actually the conditions improved decently the last 2 hours of our observing slot and at first glance probably useful to get the geometry at a satisfactory level, at last ! Below the plots showing one of the best focus we succeed to do: FWHM ~12" @ 1mm and ~20" @ 2mm => 2% from nominal value expected from simulations; so it could be better, but with the conditions we had this looks reasonable, and shows at least that the optics is certainly good, without major default. Note also that the focus procedure without wobbler (we never got the Opera box, thanks to the slowness of DHL delivery) seems to work pretty well.

Effect of focus on the error beam: the figure below shows data of two pointing cross-scans, in red out of focus (-2mm, scan 04s202), in black after focussing (-1.6mm, scan 04s205). The effect on the error beam (getting negative) is not quite as expected. An effect of the electronics ?

A similar (or same) effect shows the plateau: @1mm it is negative in a defocused map (see the figure "negative plateau @1mm per pixel" on 3-06-2012) and positive in a focused map (below). Any further systematics and dependance on other factors (e.g. sky load) are currently not known.

End of the run: switching off NIKA, dismounting the electronics, loading the truck:

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