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| = NIKA2 = The New Instrument of Kids Arrays (NIKA2) is the next generation continuum instrument to be placed at the 30m telescope of IRAM, at Pico Veleta (Spain). The instrument is based on Kinetic Inductance Detectors (KIDS). The baseline detector focal plane units consist of 1000 detectors at 2 mm and 4000 detectors at 1.25 mm. The instrument will provide the measurement of the linear polarization at 1.25 mm. |
= NIKA2 Homepage = The New IRAM KID Array 2 (NIKA2) is a dual-band camera operating with three frequency-multiplexed kilopixels arrays of Lumped Element Kinetic Inductance Detectors (LEKID) cooled at 150mK. NIKA2 is designed to observe the intensity and polarisation of the sky at 1.15 and 2.0 mm. NIKA2 was successfully installed in October 2015. Commissioning is ongoing. NIKA2 will become an IRAM resident instrument for the next ten years or more. NIKA2 is built by an international consortium, led by the Institute Neel (Grenoble France). |
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| '''[[ http://www.iram.es/IRAMES/mainWiki/FrontPage | Go to the Front Page ]]''' | NIKA2 in the web: * [[http://ipag.osug.fr/nika2/Welcome.html | NIKA2 website at IPAG ]] * [[http://www.iram.fr/wiki/nika2/index.php/Nika2Wiki | NIKA2-internal wiki at IRAM-FR ]]. |
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| The main characteristics of the latest configuration (05/AUG/2015) are summarized on the following table. || '''Band''' || '''Number of KIDs''' || '''Wavelength''' || '''Bandwidth ''' || '''NEFD''' || '''HPBW''' || '''FoV''' || || NIKA 2 mm || 1000 || 2.0 mm || xxx GHz || 10 mJy*s^1/2^ || 18.5" || 6.5' || || NIKA 1 mm || 2x2000 || 1.2 mm || xxx GHz || 15 mJy*s^1/2^ || 11.0" || 6.5' || * Number of KIDs = number of KIDs which resonance is probed with a tone generated by the electronics (in parenthesis = conservative number of KIDs for which no problem has been found in the data). Physically there's 224 KIDs on the 1mm array and 132 KIDs on the 2mm array. * NEFD = Noise equivalent flux density outside of the atmosphere = sensitivity. * HPBW = Half power beam width = angular resolution. * FoV = effective Field-of-View calculated from area covered by all pixels. * NIKA is a prototype used to test the technologies to be used in the bigger 6.5' FOV [[http://ipag.osug.fr/nika2/Welcome.html | NIKA2 ]] instrument currently in development phase ([[http://www.iram.fr/wiki/nika2/index.php/Nika2Wiki | private Wiki here]]). * Go to the NIKA [[http://www.iram.es/IRAMES/mainWiki/Continuum/NIKA/WishList | wish list]]. ---- == Call for proposals == NIKA is offered for the first time to the community the winter semester 2013/14: * [[http://www.iram-institute.org/EN/content-page-169-7-57-169-0-0.html | Call for observing proposals with the 30m]] * [[http://www.iram.es/IRAMES/mainWiki/Continuum/TimeEstimatorScript | Guidelines to estimate observing times]]. ---- == Reports and Publications == * Reports: * [[attachment:1stNIKApool.pdf | Summary of the 1st NIKA pool (February 2014)]]. * [[ CoolingPTcryostatNIKA | Procedure for cooling down the PT NIKA cryostat]] -- for IRAM staff * Refereed papers: * '''Performance and calibration of the NIKA camera at the IRAM 30 m telescope''' ([[http://arxiv.org/abs/1402.0260 | Catalano et al. 2014, arXiv ]]) * '''First observation of the thermal Sunyaev-Zel'dovich effect with Kinetic Inductance Detectors''' ([[ http://arxiv.org/abs/1310.6237 | Adam et al. 2013, arXiv]]) * '''Improved mm-wave photometry for kinetic inductance detectors''' ([[http://adsabs.harvard.edu/abs/2013A%26A...551L..12C | Calvo et al. 2013, A&A]]) * '''NIKEL: Electronics and data acquisition for kilopixels kinetic inductance camera''' ([[http://arxiv.org/abs/1204.1415 | O. Bourrion et al. 2012, arXiv]]) * '''A Dual-band Millimeter-wave Kinetic Inductance Camera for the IRAM 30 m Telescope''' ([[http://esoads.eso.org/abs/2011ApJS..194...24M | Monfardini et al. 2011, ApJS]]) * '''NIKA: A millimeter-wave kinetic inductance camera''' ([[http://esoads.eso.org/abs/2010A%26A...521A..29M |Monfardini et al. 2010, A&A]]) ---- |
Some prelimiary characteristics of NIKA-2: || '''Band''' || '''Number of KIDs''' || '''Wavelength''' || '''Bandwidth ''' || '''NEFD''' || '''HPBW''' || '''FoV''' || || NIKA2 2 mm/150 GHz || 616 || 2.00 mm || 125-170 GHz || 15 mJy*s^1/2^ || 18" || 6.5' || || NIKA2 1 mm/260 GHz || 2x1140 || 1.15 mm || 240-280 GHz || 30 mJy*s^1/2^ || 12" || 6.5' || Comments: A new 2mm array with 616 pixels was installed mid September 2016. The previously installed array had 1020 pixels. Further changes in September 2016 were a new dichroic frequency splitter, new lenses and a new cryostat window. In addition, several of the 20 readout electronics boards have been replaced with the last version. NIKA2 now has a homogeneous set of boards, plus several spare boards. Commissioning is currently still ongoing, while first science verifications observations have started in April 2017. <3-May-2017> == Call for proposals and time estimator == In the upcoming summer semester running from 1 June to 30 November 2017, a limited amount of time will be available for NIKA2 science projects. See the [[http://www.iram-institute.org/EN/content-page-169-7-57-169-0-0.html | call for proposals ]]. On the following page, we give information on how to estimate total observing times: * [[http://www.iram.es/IRAMES/mainWiki/Continuum/TimeEstimatorScript | Guidelines to estimate observing times for summer semester 2017]]. ---- == Open Time Programs == [[http://www.iram.es/IRAMES/mainWiki/AcceptedProjects | List of open time projects accepted to be observed with NIKA2 at the 30m telescope.]] '''[[ http://www.iram.es/IRAMES/mainWiki/Continuum/NIKA2/Main | Go to the top ]]''' ---- == The five Guaranteed Time Programs == Four Large Programs for NIKA2 in guaranteed time were submitted to the Program Committee for the deadline in September 2016, and one for the March 2017 deadline. All 5 have been rated high by the PC and will be observed. Here, we provide the proposal abstracts together with the list of sources and map sizes. These shall be "fenced" against new continuum 2mm/1mm mapping projects at the 30m or NOEMA. <3-May-2017> === Abstracts === ==== Galactic Star Formation with NIKA2 - GASTON (122-16) ==== Abstract: The IMF is a fundamental global output of the star formation process, and the question of its origin and universality has been a long-standing open issue. While the base of the IMF (0.1 to 1 Msun) may result from Jeans-like fragmentation of interstellar filaments, the problem of how the most extreme stellar objects (brown dwarfs, intermediate- and high-mass stars) build up their masses remains unsettled. The high-sensitivity and fast mapping capability of the NIKA2 camera offer the unique opportunity to detect large populations of low-brightness sources, and probe star-forming regions as never before. We propose to use this new instrument to: i. perform a complete survey of pre-brown-dwarf cores in two nearby star-forming regions, ii. map the intertwined populations of interstellar filaments and intermediate to high-mass cores within rich galactic plane star-forming regions; iii. use the dual band capability of NIKA2 at 1.2mm and 2mm to constrain the dust properties in a broad range of environments and reduce mass uncertainties by a factor of 3. Altogether, these observations will provide new insight on the earliest stages of star formation across both ends of the stellar IMF. PI is Nicolas Peretto. '''[[ http://www.iram.es/IRAMES/mainWiki/Continuum/NIKA2/Main | Go to the top ]]''' ==== Interpreting the Millimetre Emission of Galaxies with IRAM and NIKA (IMEGIN) (160-16) ==== Abstract: The mm part of the spectrum is one of the least explored parts of a galaxy’s spectral energy distribution (SED), yet it contains emission from three fundamentally important physical processes. These processes are thermal emission from dust, free-free emission from ionized gas and synchrotron emission from charged particles moving in the galactic magnetic field. We are proposing to use the NIKA2 camera to observe a sample of 22 nearby galaxies that also have considerable ancillary data across the SED from the radio to the ultra-violet. We will investigate the dust emissivity, the relationship between the three physical processes and their relation to star formation and the gas-to-dust ratio. As the sample galaxies are of large angular size we will be able to carry out this project in a spatially resolved way and hence investigate the different environments found within galaxies. PI is Jonathan Davies '''[[ http://www.iram.es/IRAMES/mainWiki/Continuum/NIKA2/Main | Go to the top ]]''' ==== The NIKA2 Cosmological Legacy Survey (N2CLS) (192-16) ==== Abstract: Using 300h of the NIKA2 Guaranteed Time, we will map the star formation at high redshift in two of the most popular fields. N2CLS will reach for the first time the confusion noise at the 30m, in 160 square arcminutes in GOODS-N. In COSMOS, N2CLS sensitivity will at least match or outperform the sensitivity of the S2CLS survey at 850 microns on 0.5 square degree. N2CLS will detect hundreds of dust-obscured optically-faint galaxies during their major episodes of formation in the early universe. It will fully open a new window on the faint and high-redshift dusty Universe and answer the outstanding issue of whether dusty star-formation contributes to early galaxy evolution. It will uniquely probe the transition at z~3-4 of the cosmic star-formation history between the predominantly unobscured growth in the early Universe and the obscured star formation, driven by the build-up of the most massive galaxies during the peak of cosmic assembly. The availability of this uniquely large sample of mm-selected galaxies with superb supporting multi-wavelength data will provide the opportunity to address the history of star formation, dust production and the growth of large-scale structures. PIs: Guilaine Lagache, Alexandre Beelen, Nicolas Ponthieu '''[[ http://www.iram.es/IRAMES/mainWiki/Continuum/NIKA2/Main | Go to the top ]]''' ==== High-resolution tSZ observations of a large sample of clusters of galaxies (NIKA2SZ) (199-16) ==== Abstract: The development of precision cosmology with clusters of galaxies requires high angular resolution observations to extend the understanding of galaxy clusters towards high redshift. The NIKA2 camera at the IRAM 30 m telescope is the only instrument currently in operation that is suited for this kind of observations, given its resolution, sensitivity and dual-band observation capability. We intend to observe a large sample of clusters of galaxies at high redshift (0.5 < z < 0.9), selected from the Planck and ACT catalogs. We have formed a representative cluster sample for redshift evolution and cosmological studies, with a homogeneous coverage in cluster mass as reconstructed from the integrated Compton parameter. We will use the SZ-dedicated pipeline that we have developed for the SZ observation with the NIKA camera. Our primary objective is to produce unprecedented high-quality deliverables (tSZ maps and pressure profiles) for all clusters of the sample. NIKA2 data will be complemented with ancillary data including X-ray, optical and radio observations. The full dataset will lead to significant improvements on the use of clusters of galaxies to draw cosmological constraints. PIs: Frédéric Mayet, Barbara Comis '''[[ http://www.iram.es/IRAMES/mainWiki/Continuum/NIKA2/Main | Go to the top ]]''' ==== Probing the B-Field in star-forming Filaments Using NIKA2-Pol (B-FUN) (015-17) ==== Abstract: Recent Herschel and Planck observations of Galactic interstellar clouds support a paradigm of star formation in which magnetized filaments play a central role. Herschel results indicate that most cores/stars form in dense, supercritical filaments of ~0.1 pc width, and Planck polarization data suggest that the formation and evolution of these filaments is largely controlled by magnetic fields. The low resolution of Planck polarization data is however insufficient to probe individual cores along filaments and understand the role of B fields in filament evolution and fragmentation. To make decisive progress in this area, we propose a 1.2 mm polarimetric imaging survey with NIKA2-POL of ~8 nearby star-forming filaments spanning a range of line masses from marginally supercritical to highly supercritical. The proposed observations will constrain the role of magnetic fields in channeling matter from filaments to prestellar cores and will determine whether the B field remains roughly perpendicular to the filaments, as observed by Planck on larger scales, or becomes more parallel to the filaments in their dense interior, which would have profound implications for core formation. PI: Philippe Andre '''[[ http://www.iram.es/IRAMES/mainWiki/Continuum/NIKA2/Main | Go to the top ]]''' === Source list === * [[attachment:NIKA2-GT-LPs-21jun2017.pdf|NIKA2-GT-LPs-21jun2017.pdf]] * [[attachment:NIKA2-GT-LPs-21jun2017.xls|NIKA2-GT-LPs-21jun2017.xls]] == Publications == * Instrument/detectors papers: * Bourrion et al. 2016, '''NIKEL_AMC: Readout electronics for the NIKA2 experiment''', [[https://arxiv.org/abs/1602.01288|arxiv]] * Ritacco et al. 2016, '''First polarised light with the NIKA camera''', JLTP, Volume 184, Issue 3-4, pp. 724-732, 08/2016 [[https://arxiv.org/abs/1508.00747|arxiv]] * Catalano et al. 2016, '''The NIKA2 commissioning campaign: performance and first results''', [[http://arxiv.org/abs/1605.08628|arxiv]] * Calvo et al. 2016, '''The NIKA2 instrument, a dual-band kilopixel KID array for millimetric astronomy''', [[http://arxiv.org/abs/arXiv:1601.02774|arxiv]] * Goupy et al. 2016, '''Microfabrication technology for large LEKID arrays : from NIKA2 to future applications''', [[http://arxiv.org/abs/1601.03969|arxiv]] * Monfardini et al. 2014, '''Latest NIKA Results and the NIKA-2 Project''', JLTP 176, 787, [[http://arxiv.org/abs/arXiv:1310.1230|arxiv]] * Catalano et al. 2014, '''Performance and calibration of the NIKA camera at the IRAM 30 m telescope''', A&A 569, A9, [[http://arxiv.org/abs/arXiv:1402.0260|arxiv]] * Calvo et al. 2013, '''Improved mm-wave photometry for kinetic inductance detectors''', A&A, 551, L12 [[http://adsabs.harvard.edu/abs/2013A%26A...551L..12C|ADS]] * Bourrion et al. 2012, '''NIKEL: Electronics and data acquisition for kilopixels kinetic inductance camera''', Journal of Instrumentation, 7, 07, pp. 7014. [[http://arxiv.org/abs/1204.1415|arXiv]] * Monfardini et al. 2011, '''A Dual-band Millimeter-wave Kinetic Inductance Camera for the IRAM 30 m Telescope''', ApJS, 194, 2, article id. 24. [[http://arxiv.org/abs/1102.0870|arXiv]] * [[http://www.iram.fr/wiki/nika2/index.php/Technical_NIKA_papers_to_be_cited|Internal list of technical papers]] * Astronomical papers: * Ritacco, A., Ponthieu, N, Catalano, A., et al, 2017, '''Polarimetry at millimeter wavelengths with the NIKA camera: calibration and performance''', A&A 599, A34, [[http://adsabs.harvard.edu/abs/2017A%26A...599A..34R|ADS]] * Ruppin, F., Adam, R., Comis, B., et al. 2016, '''Non parametric deprojection of NIKA SZ observations: pressure distribution in the Planck-discovered cluster PSZ1 G045.85+57.71''', A&A, in press [[http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1607.07679|ADS]] * Adam, R., Bartalucci, I., Pratt, G. W., et al. 2016, '''Mapping the kinetic Sunyaev-Zel'dovich effect toward MACS J0717.5+3745 with NIKA''', A&A, in press [[http://esoads.eso.org/abs/2016arXiv160607721A|ADS]] * Adam, R., Comis, B., Bartalucci, I., et al. 2016, '''High angular resolution Sunyaev-Zel'dovich observations of MACS J1423.8+2404 with NIKA: Multiwavelength analysis''', A&A, 586, 122 [[http://esoads.eso.org/abs/2016A%26A...586A.122A|ADS]] * Adam, R., Comis, B., Macias-Perez, J.-F., et al, 2015, '''Pressure distribution of the high-redshift cluster of galaxies CL J1226.9+3332 with NIKA''', A&A, 576, A12 [[http://adsabs.harvard.edu/abs/2015A%26A...576A..12A|ADS]] * Adam, R., Comis, B., Macias-Perez, J.-F, et al, 2014, '''First observation of the thermal Sunyaev-Zel'dovich effect with kinetic inductance detectors''', A&A, 569, 66 [[http://adsabs.harvard.edu/abs/2014A%26A...569A..66A|ADS]] * Ph.D. thesis: * ''Rémi Adam (2012-2015) - Advisors: J.F. Macías-Pérez and F.X. Désert'' ([[https://tel.archives-ouvertes.fr/tel-01303736 | Observation des amas de galaxies par effet Sunyaev-Zel'dovich et de la polarisation du fond diffus cosmologique : de Planck à NIKA (in French)]]) * ''Alessia Ritacco (2013-2016) - Advisors: J.F. Macías-Pérez, Alessandro Monfardini, Andrea Catalano, Nicolas Ponthieu'' ([[https://tel.archives-ouvertes.fr/tel-01467862|Polarimetry at millimeter wavelengths with the instruments NIKA and NIKA2]]) * Talks: * Alessia Ritacco, November 2016, '''Polarimetry at Millimeter wavelengths with NIKA and NIKA2''' [[attachment:ritacco-seminar-nika2-nov2016.pdf]] * [[http://ipag.osug.fr/nika2/Publications.html|NIKA2 publications list maintained at IPAG]] '''[[ http://www.iram.es/IRAMES/mainWiki/Continuum/NIKA2/Main | Go to the top ]]''' ---- == Technical Documentation == * [[attachment:calvo-12jun2017-NIKA2networkDescription.pdf | Computer Network, M.Calvo, June-2017 ]] * [[attachment:calvo-07apr2017-nika2-PTpositionAdjustment.pdf| Pulse Tube Adjustment, M.Calvo, Apr-2017 ]] * [[attachment:calvo-feb2016-nika2-camadia.pdf | NIKA2 Data Acquisition, Camadia, M.Calvo, Feb-2016 ]] * [[attachment:calvo-docTuning_feb2016.pdf | NIKA2 tuning procedure and data flagging description, M.Calvo, Feb-2016 ]] * [[attachment:garcia-02mar2017-NIKA2_recovery.pdf | NIKA2 recovery of acquisition system, P.Garcia, Mar-2017 (ask AR or CK for TeX file) ]] * [[http://www.iram.es/IRAMES/mainWiki/Continuum/NIKA2/InstrumentalDoc | Instrument-related documentation page ]] * [[https://mrt-lx1.iram.es/FrontendGroupWiki/RxNIKA2 | Documentation on Cryostat, Cooling procedure, etc. by the Granada Receiver Group (internal)]] * Wiki-pages: * [[http://www.iram.es/IRAMES/mainWiki/OffProcNika2Run1Beam | Discussion on beams ]] * [[http://www.iram.es/IRAMES/mainWiki/Spectral%20bands | Spectral bands ]] * [[http://www.iram.es/IRAMES/mainWiki/Continuum/NetworkAccess | Remote network access to nika2-a computer ]] * [[http://www.iram.es/IRAMES/mainWiki/Continuum/PoolPreparation | Pool observations]] provides information on the observing modes offered for NIKA2 and examples of the scripts that you must prepare to observe your project. * [[http://www.iram.es/IRAMES/mainWiki/Continuum/ObservingSession | Observing session]] provides an example of a typical session with NIKA2 at the 30m telescope. * [[http://www.iram.es/IRAMES/mainWiki/Continuum/Calibrators | Pointing sources and calibrators ]] provides a list of pointing sources and calibrators. ## * [[http://www.iram.es/IRAMES/mainWiki/Continuum/TimeEstimatorScript|Time Estimator (UNDER CONSTRUCTION)]] ## * [[http://www.iram.es/IRAMES/mainWiki/Continuum/ObserveGRBs | Observe GRBs]] ## ---- ## ## == Open runs == ## ## === 1st NIKA2 pool (coming soon) === ## ## For information about the accepted projects and the observers at the 30m please go to: ## * [[http://www.iram.es/IRAMES/mainWiki/Continuum/NIKA2/Pool1st | 1st NIKA2 pool organization.]] ## ## The progress of the pool can be followed via: ## ## * [[https://pools.iram.es | Pool data base]] ## ## * [[https://tapas.iram.es/tapas/ | TAPAS]] ## ## Both databases are synchronized and can be used to write/read the logsheet. '''[[ http://www.iram.es/IRAMES/mainWiki/Continuum/NIKA2/Main | Go to the top ]]''' ---- == Technical runs to commission NIKA2 == * '''1^st^ test run of NIKA2''': 29-October-2015 till 10-November-2015. Installation, cool down at the 30m, testing/debugging/developing. [= Run 13 of a NIKA instrument] * [[Nika2Run1|Go to the 1st run Wiki page]] * [[http://www.iram.fr/wiki/nika2/index.php/NIKA2_Run1_30m_CharacterizationPlan | Private Wiki detailing the organization of the run and the instrument characterization plan]] * '''2^nd^ test run of NIKA2''': 24-November-2015 till 02-December-2015. Continue tests started during run 1, in particular Beam maps and NEFD with the 13 NIKEL boards assembled the last days of run 1. [= Run 14 of a NIKA instrument] * [[Nika2Run2|Go to the 2nd run Wiki page]] * '''3^rd^ test run of NIKA2''': 12-January-2016 till 01-February-2016. Implementation of new NIKEL boards; the 20 data lines of NIKA2 are foreseen to be plugged simultaneously. With the 3 arrays fully read, continue and redo tests started with runs 1 & 2, in particular '''Beam maps''' and NEFD. [= Run 15 of a NIKA instrument] * [[Nika2Run3|Go to the 3rd run Wiki page]] * '''4^th^ test run of NIKA2''': 1-March-2016 till 15-March-2016. Continue tests started with previous runs, in particular investigate deeper beam patterns (XY focus, beam maps), synchronization, array 1 & 3 performances vs electronic boards, NEFD, mapping strategies. [= Run 16 of a NIKA instrument] * [[Nika2Run4|Go to the 4th run Wiki page]] * '''Dark run''': 4-May-2016. Test sensitivity of NIKA2 to external electromagnetic perturbations, with the entrance window of the cryostat closed. [= Run 17 of a NIKA instrument] * '''5^th^ test run of NIKA2''': 16-September-2016 till 11-October-2016. Upgrade NIKA2 with new dichroic, new corrugated lenses and window, new 2mm array, new NIKEL boards (get the 20 lines with homogeneous electronics, v3); redo better the tests started with previous runs (mostly beam maps in best weather conditions, but also various types of scan to investigate deeper beams and noise, synchronization, NEFD, skydips, mapping strategies, possibly polarization. [= Run 18 of a NIKA instrument] * [[Nika2Run5|Go to the 5th run Wiki page]] * '''6^th^ test run of NIKA2''': 25-October-2016 till 1-November-2016. Continue NIKA2 commissioning. [= Run 19 of a NIKA instrument] * [[Nika2Run6|Go to the 6th run Wiki page]] * '''7^th^ test run of NIKA2''': 6-December-2016 till 13-December-2016. Test DRO based external calibrator, continue NIKA2 commissioning. [= Run 20 of a NIKA instrument] * [[Nika2Run7|Go to the 7th run Wiki page]] * '''8^th^ test run of NIKA2''': 9-January-2017 to 13-January-2017, then 23-January to 27-January. Reverse array 1 lens to smooth version + adjust fixation of cold mirrors block (M7-M8) to get better radio alignment of the internal optics, short test on sky to see effect of the intervention. [= Run 21 of a NIKA instrument] * [[Nika2Run8|Go to the 8th run Wiki page]] * '''9^th^ test run of NIKA2''': 21-February-2017 to 28-February-2017. Resume NIKA2 commissioning after run 8 intervention. [= Run 22 of a NIKA instrument] * [[Nika2Run9|Go to the 9th run Wiki page]] * '''10^th^ test run of NIKA2''': 18-April-2017 to 25-April-2017. End of commissioning phase 1, science verification. [= Run 23 of a NIKA instrument] * [[Nika2Run10|Go to the 10th run Wiki page]] * '''11^th^ test run of NIKA2''':8-June-2017 to 13-June-2017. Start commissioning phase 2: polarization. [= Run 24 of a NIKA instrument] * [[Nika2Run11|Go to the 11th run Wiki page]] ----- |
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| * NIKA team: * '''Alain Benoit''' <alain.benoit@grenoble.cnrs.fr> (PI, IN) * '''Alessandro Monfardini''' <monfardini@grenoble.cnrs.fr> (co-PI, IN) * François-Xavier Désert <francois-xavier.desert@obs.ujf-grenoble.fr> (IPAG) * Martino Calvo <martino.calvo@grenoble.cnrs.fr> (IN) * Antonio D'Addabbo <antonio.d-addabbo@grenoble.cnrs.fr> (IN) * Nicolas Ponthieu (IPAG) |
* NIKA2 team: * '''Alessandro Monfardini''' <monfardini@neel.cnrs.fr> (PI, IN) * Alain Benoit <alain.benoit@grenoble.cnrs.fr> * François-Xavier Désert <francois-xavier.desert@univ-grenoble-alpes.fr> (IPAG) * Martino Calvo <martino.calvo@neel.cnrs.fr> (IN) * Johannes Goupy <johannes.goupy@neel.cnrs.fr> (IN) * Nicolas Ponthieu <nicolas.ponthieu@univ-grenoble-alpes.fr> (IPAG) |
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| * Remi Adam <adam@lpsc.in2p3.fr> (LPSC) * IRAM/Granada support team: * '''Carsten Kramer''' (Station Manager, <kramer@iram.es>) * Israel Hermelo (30m Continuum Pool Manager, <hermelo@iram.es>) * Nicolas Billot (30m Scheduler, <billot@iram.es>) * Claudia Marka (30m Heterodyne Pool Manager, <marka@iram.es>) * Albrecht Sievers (<sievers@iram.es>) * Robert Zylka * Walter Brunswig ---- == How-to's == * [[http://www.iram.es/IRAMES/mainWiki/Continuum/PoolPreparation | Pool Preparation]] provides information on the observing modes offered for the continuum cameras as well as examples of the scripts that you need to prepare to observe your project. * [[http://www.iram.es/IRAMES/mainWiki/Continuum/ObservingSession | Observing Session]] provides an example of a typical session with the continuum cameras at the 30m telescope. * [[http://www.iram.es/IRAMES/mainWiki/Continuum/Calibrators | Pointing sources and calibrators ]] provides a list of pointing sources and calibrators for the IRAM 30m continuum cameras. * For observers: [[attachment:NIKA_status.pdf | Check the staus of NIKA during the observations]]. * For Experts: [[http://www.iram.es/IRAMES/mainWiki/Continuum/NIKA/PointingSession | Alignment and pointing sesion ]] (in prep.) provides a step-by-step procedure to implement a new pointing model with NIKA * [[http://www.iram.es/IRAMES/mainWiki/Continuum/NIKA/DataReduction | Data Reduction]] Quick look analysis and Offline processing products. * [[http://www.iram.es/IRAMES/mainWiki/Continuum/ObserveGRBs | Observe GRBs]] {*} ## * [[attachment:observer_notice_v2.pdf | NIKA data reduction cookbook (N. Ponthieu 2014)]]. ---- == Open runs == === 3rd NIKA pool (Jan-Feb 2015) === The 3rd NIKA open pool will take place from the January 27th to February 10th. For information about the accepted projects and the observers at the 30m please go to: * [[http://www.iram.es/IRAMES/mainWiki/Continuum/PoolOrganization/3rdNIKApool | 3rd NIKA pool organization.]] The progress of the pool can be followed via: * [[https://pools.iram.es | Pool data base]] * [[https://tapas.iram.es/tapas/ | TAPAS]] Both databases are synchronized and can be used to write/read the logsheet. === 2nd NIKA pool (November 2014) === * [[http://www.iram.es/IRAMES/mainWiki/Continuum/PoolOrganization/2ndNIKApool | 2nd NIKA pool organization.]] * [[http://www.iram.es/IRAMES/mainWiki/NikaRun10 | Internal NIKA team page for organisation]] === 1st NIKA pool (February 2014) === * [[http://www.iram.es/IRAMES/mainWiki/Continuum/PoolOrganization/1stNIKApool | 1st NIKA pool organization]] * [[http://www.iram.es/IRAMES/mainWiki/PoolW13 | IRAM 30m pool observers for the Winter 2013 semester]] * [[http://www.iram.es/IRAMES/mainWiki/NikaRun8 | Internal NIKA team page for organisation]] === Available data products === || '''Run''' || '''Date''' || '''v0''' || '''v1''' || '''v2''' || || 1st NIKA pool || Feb 2014 || (./) || (./) || {X} || || 2nd NIKA pool || Nov 2014 || (./) || {X} || {X} || || 3rd NIKA pool || Jan 2015 || (./) || {X} || {X} || To retrive the data please use the following command: {{{ scp xxx-yy@enter.iram.es:~/observationData/nika/v?.tar.gz /path/in/your/computer }}} where '''xxx-yy''' is your project number and '''v?''' is the version of the data to retrieve (options are v0, v1, and v2). ---- == Technical runs == * '''12th test run - Polarisation''' (February 2015) * [[NikaRun12 | Go to the 12th run Wiki page]] * '''9th test run''' (October 2014) * [[NikaRun9 | Go to the 9th run Wiki page]] * '''May 2014 Dry run''' * Two slots of 4 hours scheduled for the NIKA dry run: Wed 7th May 2014 from 11:00 to 15:00 (LT), Mon 12th May 2014 from 12:00 to 16:00 (LT) * See the [[http://www.iram.es/IRAMES/mainWiki/Continuum/PoolOrganization/DryRunNIKA | NIKA dry run]] organization wiki. * '''7th test run''' (January 2014) * [[NikaRun7 | Go to the 7th run Wiki page]] * '''6th test run''' (June 2013) * [[NikaRun6|Go to the 6th run Wiki page]] * '''5th test run''' (November 2012) * [[NikaRun5|Go to the 5th run Wiki page]] * '''4th test run''' (June 2012, final position, final cryostat) * [[NikaRun4|Go to the 4th run Wiki page]] * '''3rd test run''' (October 2011, cryogen free 1^st^ cold stage cryostat) * [[NikaRun3|Go to the 3rd run Wiki page]] * '''2nd test run''' (October 2010, dual band cryostat) * [[NikaRun2|Go to the 2nd run Wiki page]] * '''1st test run''' (October 2009, 1 band cryostat on MAMBO bench, liquid He 1^st^ cold stage) * [[NikaRun1|Go to the 1st run Wiki page]] ----- Author: Israel Hermelo (IRAM 30m continuum pool manager) email: hermelo@iram.es Created: 2013.Dec.16 This page is maintained by IH, CK, SL and the NIKA team Last update: 2014.Dec.17 |
* Laurence Perotto <laurence.perotto@lpsc.in2p3.fr> (LPSC) * IRAM/Granada NIKA2 support team: * Carsten Kramer (Station Manager and Scheduler, <kramer@iram.es>) * Alessia Ritacco (commissioning of polarization capabilities, <ritaccoa@iram.es>) * Albrecht Sievers (IMBfits, <sievers@iram.es>) * Hans Ungerechts (NCS/pako, <ungerechts@iram.es>) * Pablo Mellado (Computers/Network, <mellado@iram.es>) '''[[ http://www.iram.es/IRAMES/mainWiki/Continuum/NIKA2/Main | Go to top ]]''' ------- Created: 2015.AUG.05 by Israel Hermelo. This page is maintained by AR, SL, CK, and the NIKA2 team. |
NIKA2 Homepage
The New IRAM KID Array 2 (NIKA2) is a dual-band camera operating with three frequency-multiplexed kilopixels arrays of Lumped Element Kinetic Inductance Detectors (LEKID) cooled at 150mK. NIKA2 is designed to observe the intensity and polarisation of the sky at 1.15 and 2.0 mm. NIKA2 was successfully installed in October 2015. Commissioning is ongoing. NIKA2 will become an IRAM resident instrument for the next ten years or more. NIKA2 is built by an international consortium, led by the Institute Neel (Grenoble France).
Contents
NIKA2 in the web:
Overview
Some prelimiary characteristics of NIKA-2:
Band |
Number of KIDs |
Wavelength |
Bandwidth |
NEFD |
HPBW |
FoV |
NIKA2 2 mm/150 GHz |
616 |
2.00 mm |
125-170 GHz |
15 mJy*s1/2 |
18" |
6.5' |
NIKA2 1 mm/260 GHz |
2x1140 |
1.15 mm |
240-280 GHz |
30 mJy*s1/2 |
12" |
6.5' |
Comments: A new 2mm array with 616 pixels was installed mid September 2016. The previously installed array had 1020 pixels. Further changes in September 2016 were a new dichroic frequency splitter, new lenses and a new cryostat window. In addition, several of the 20 readout electronics boards have been replaced with the last version. NIKA2 now has a homogeneous set of boards, plus several spare boards. Commissioning is currently still ongoing, while first science verifications observations have started in April 2017. <3-May-2017>
Call for proposals and time estimator
In the upcoming summer semester running from 1 June to 30 November 2017, a limited amount of time will be available for NIKA2 science projects. See the call for proposals. On the following page, we give information on how to estimate total observing times:
Open Time Programs
List of open time projects accepted to be observed with NIKA2 at the 30m telescope.
The five Guaranteed Time Programs
Four Large Programs for NIKA2 in guaranteed time were submitted to the Program Committee for the deadline in September 2016, and one for the March 2017 deadline. All 5 have been rated high by the PC and will be observed. Here, we provide the proposal abstracts together with the list of sources and map sizes. These shall be "fenced" against new continuum 2mm/1mm mapping projects at the 30m or NOEMA. <3-May-2017>
Abstracts
Galactic Star Formation with NIKA2 - GASTON (122-16)
Abstract: The IMF is a fundamental global output of the star formation process, and the question of its origin and universality has been a long-standing open issue. While the base of the IMF (0.1 to 1 Msun) may result from Jeans-like fragmentation of interstellar filaments, the problem of how the most extreme stellar objects (brown dwarfs, intermediate- and high-mass stars) build up their masses remains unsettled. The high-sensitivity and fast mapping capability of the NIKA2 camera offer the unique opportunity to detect large populations of low-brightness sources, and probe star-forming regions as never before. We propose to use this new instrument to: i. perform a complete survey of pre-brown-dwarf cores in two nearby star-forming regions, ii. map the intertwined populations of interstellar filaments and intermediate to high-mass cores within rich galactic plane star-forming regions; iii. use the dual band capability of NIKA2 at 1.2mm and 2mm to constrain the dust properties in a broad range of environments and reduce mass uncertainties by a factor of 3. Altogether, these observations will provide new insight on the earliest stages of star formation across both ends of the stellar IMF.
PI is Nicolas Peretto.
Interpreting the Millimetre Emission of Galaxies with IRAM and NIKA (IMEGIN) (160-16)
Abstract: The mm part of the spectrum is one of the least explored parts of a galaxy’s spectral energy distribution (SED), yet it contains emission from three fundamentally important physical processes. These processes are thermal emission from dust, free-free emission from ionized gas and synchrotron emission from charged particles moving in the galactic magnetic field. We are proposing to use the NIKA2 camera to observe a sample of 22 nearby galaxies that also have considerable ancillary data across the SED from the radio to the ultra-violet. We will investigate the dust emissivity, the relationship between the three physical processes and their relation to star formation and the gas-to-dust ratio. As the sample galaxies are of large angular size we will be able to carry out this project in a spatially resolved way and hence investigate the different environments found within galaxies.
PI is Jonathan Davies
The NIKA2 Cosmological Legacy Survey (N2CLS) (192-16)
Abstract: Using 300h of the NIKA2 Guaranteed Time, we will map the star formation at high redshift in two of the most popular fields. N2CLS will reach for the first time the confusion noise at the 30m, in 160 square arcminutes in GOODS-N. In COSMOS, N2CLS sensitivity will at least match or outperform the sensitivity of the S2CLS survey at 850 microns on 0.5 square degree. N2CLS will detect hundreds of dust-obscured optically-faint galaxies during their major episodes of formation in the early universe. It will fully open a new window on the faint and high-redshift dusty Universe and answer the outstanding issue of whether dusty star-formation contributes to early galaxy evolution. It will uniquely probe the transition at z~3-4 of the cosmic star-formation history between the predominantly unobscured growth in the early Universe and the obscured star formation, driven by the build-up of the most massive galaxies during the peak of cosmic assembly. The availability of this uniquely large sample of mm-selected galaxies with superb supporting multi-wavelength data will provide the opportunity to address the history of star formation, dust production and the growth of large-scale structures.
PIs: Guilaine Lagache, Alexandre Beelen, Nicolas Ponthieu
High-resolution tSZ observations of a large sample of clusters of galaxies (NIKA2SZ) (199-16)
Abstract: The development of precision cosmology with clusters of galaxies requires high angular resolution observations to extend the understanding of galaxy clusters towards high redshift. The NIKA2 camera at the IRAM 30 m telescope is the only instrument currently in operation that is suited for this kind of observations, given its resolution, sensitivity and dual-band observation capability. We intend to observe a large sample of clusters of galaxies at high redshift (0.5 < z < 0.9), selected from the Planck and ACT catalogs. We have formed a representative cluster sample for redshift evolution and cosmological studies, with a homogeneous coverage in cluster mass as reconstructed from the integrated Compton parameter. We will use the SZ-dedicated pipeline that we have developed for the SZ observation with the NIKA camera. Our primary objective is to produce unprecedented high-quality deliverables (tSZ maps and pressure profiles) for all clusters of the sample. NIKA2 data will be complemented with ancillary data including X-ray, optical and radio observations. The full dataset will lead to significant improvements on the use of clusters of galaxies to draw cosmological constraints.
PIs: Frédéric Mayet, Barbara Comis
Probing the B-Field in star-forming Filaments Using NIKA2-Pol (B-FUN) (015-17)
Abstract: Recent Herschel and Planck observations of Galactic interstellar clouds support a paradigm of star formation in which magnetized filaments play a central role. Herschel results indicate that most cores/stars form in dense, supercritical filaments of ~0.1 pc width, and Planck polarization data suggest that the formation and evolution of these filaments is largely controlled by magnetic fields. The low resolution of Planck polarization data is however insufficient to probe individual cores along filaments and understand the role of B fields in filament evolution and fragmentation. To make decisive progress in this area, we propose a 1.2 mm polarimetric imaging survey with NIKA2-POL of ~8 nearby star-forming filaments spanning a range of line masses from marginally supercritical to highly supercritical. The proposed observations will constrain the role of magnetic fields in channeling matter from filaments to prestellar cores and will determine whether the B field remains roughly perpendicular to the filaments, as observed by Planck on larger scales, or becomes more parallel to the filaments in their dense interior, which would have profound implications for core formation.
PI: Philippe Andre
Source list
Publications
- Instrument/detectors papers:
Bourrion et al. 2016, NIKEL_AMC: Readout electronics for the NIKA2 experiment, arxiv
Ritacco et al. 2016, First polarised light with the NIKA camera, JLTP, Volume 184, Issue 3-4, pp. 724-732, 08/2016 arxiv
Catalano et al. 2016, The NIKA2 commissioning campaign: performance and first results, arxiv
Calvo et al. 2016, The NIKA2 instrument, a dual-band kilopixel KID array for millimetric astronomy, arxiv
Goupy et al. 2016, Microfabrication technology for large LEKID arrays : from NIKA2 to future applications, arxiv
Monfardini et al. 2014, Latest NIKA Results and the NIKA-2 Project, JLTP 176, 787, arxiv
Catalano et al. 2014, Performance and calibration of the NIKA camera at the IRAM 30 m telescope, A&A 569, A9, arxiv
Calvo et al. 2013, Improved mm-wave photometry for kinetic inductance detectors, A&A, 551, L12 ADS
Bourrion et al. 2012, NIKEL: Electronics and data acquisition for kilopixels kinetic inductance camera, Journal of Instrumentation, 7, 07, pp. 7014. arXiv
Monfardini et al. 2011, A Dual-band Millimeter-wave Kinetic Inductance Camera for the IRAM 30 m Telescope, ApJS, 194, 2, article id. 24. arXiv
- Astronomical papers:
Ritacco, A., Ponthieu, N, Catalano, A., et al, 2017, Polarimetry at millimeter wavelengths with the NIKA camera: calibration and performance, A&A 599, A34, ADS
Ruppin, F., Adam, R., Comis, B., et al. 2016, Non parametric deprojection of NIKA SZ observations: pressure distribution in the Planck-discovered cluster PSZ1 G045.85+57.71, A&A, in press ADS
Adam, R., Bartalucci, I., Pratt, G. W., et al. 2016, Mapping the kinetic Sunyaev-Zel'dovich effect toward MACS J0717.5+3745 with NIKA, A&A, in press ADS
Adam, R., Comis, B., Bartalucci, I., et al. 2016, High angular resolution Sunyaev-Zel'dovich observations of MACS J1423.8+2404 with NIKA: Multiwavelength analysis, A&A, 586, 122 ADS
Adam, R., Comis, B., Macias-Perez, J.-F., et al, 2015, Pressure distribution of the high-redshift cluster of galaxies CL J1226.9+3332 with NIKA, A&A, 576, A12 ADS
Adam, R., Comis, B., Macias-Perez, J.-F, et al, 2014, First observation of the thermal Sunyaev-Zel'dovich effect with kinetic inductance detectors, A&A, 569, 66 ADS
- Ph.D. thesis:
Rémi Adam (2012-2015) - Advisors: J.F. Macías-Pérez and F.X. Désert (Observation des amas de galaxies par effet Sunyaev-Zel'dovich et de la polarisation du fond diffus cosmologique : de Planck à NIKA (in French))
Alessia Ritacco (2013-2016) - Advisors: J.F. Macías-Pérez, Alessandro Monfardini, Andrea Catalano, Nicolas Ponthieu (Polarimetry at millimeter wavelengths with the instruments NIKA and NIKA2)
- Talks:
Alessia Ritacco, November 2016, Polarimetry at Millimeter wavelengths with NIKA and NIKA2 ritacco-seminar-nika2-nov2016.pdf
Technical Documentation
NIKA2 tuning procedure and data flagging description, M.Calvo, Feb-2016
NIKA2 recovery of acquisition system, P.Garcia, Mar-2017 (ask AR or CK for TeX file)
Documentation on Cryostat, Cooling procedure, etc. by the Granada Receiver Group (internal)
- Wiki-pages:
Pool observations provides information on the observing modes offered for NIKA2 and examples of the scripts that you must prepare to observe your project.
Observing session provides an example of a typical session with NIKA2 at the 30m telescope.
Pointing sources and calibrators provides a list of pointing sources and calibrators.
Technical runs to commission NIKA2
1st test run of NIKA2: 29-October-2015 till 10-November-2015. Installation, cool down at the 30m, testing/debugging/developing. [= Run 13 of a NIKA instrument]
2nd test run of NIKA2: 24-November-2015 till 02-December-2015. Continue tests started during run 1, in particular Beam maps and NEFD with the 13 NIKEL boards assembled the last days of run 1. [= Run 14 of a NIKA instrument]
3rd test run of NIKA2: 12-January-2016 till 01-February-2016. Implementation of new NIKEL boards; the 20 data lines of NIKA2 are foreseen to be plugged simultaneously. With the 3 arrays fully read, continue and redo tests started with runs 1 & 2, in particular Beam maps and NEFD. [= Run 15 of a NIKA instrument]
4th test run of NIKA2: 1-March-2016 till 15-March-2016. Continue tests started with previous runs, in particular investigate deeper beam patterns (XY focus, beam maps), synchronization, array 1 & 3 performances vs electronic boards, NEFD, mapping strategies. [= Run 16 of a NIKA instrument]
Dark run: 4-May-2016. Test sensitivity of NIKA2 to external electromagnetic perturbations, with the entrance window of the cryostat closed. [= Run 17 of a NIKA instrument]
5th test run of NIKA2: 16-September-2016 till 11-October-2016. Upgrade NIKA2 with new dichroic, new corrugated lenses and window, new 2mm array, new NIKEL boards (get the 20 lines with homogeneous electronics, v3); redo better the tests started with previous runs (mostly beam maps in best weather conditions, but also various types of scan to investigate deeper beams and noise, synchronization, NEFD, skydips, mapping strategies, possibly polarization. [= Run 18 of a NIKA instrument]
6th test run of NIKA2: 25-October-2016 till 1-November-2016. Continue NIKA2 commissioning. [= Run 19 of a NIKA instrument]
7th test run of NIKA2: 6-December-2016 till 13-December-2016. Test DRO based external calibrator, continue NIKA2 commissioning. [= Run 20 of a NIKA instrument]
8th test run of NIKA2: 9-January-2017 to 13-January-2017, then 23-January to 27-January. Reverse array 1 lens to smooth version + adjust fixation of cold mirrors block (M7-M8) to get better radio alignment of the internal optics, short test on sky to see effect of the intervention. [= Run 21 of a NIKA instrument]
9th test run of NIKA2: 21-February-2017 to 28-February-2017. Resume NIKA2 commissioning after run 8 intervention. [= Run 22 of a NIKA instrument]
10th test run of NIKA2: 18-April-2017 to 25-April-2017. End of commissioning phase 1, science verification. [= Run 23 of a NIKA instrument]
11th test run of NIKA2:8-June-2017 to 13-June-2017. Start commissioning phase 2: polarization. [= Run 24 of a NIKA instrument]
Support teams
- Overall coordinator:
Samuel Leclercq (IRAM/Grenoble, <leclercq@iram.fr>)
- NIKA2 team:
Alessandro Monfardini <monfardini@neel.cnrs.fr> (PI, IN)
Alain Benoit <alain.benoit@grenoble.cnrs.fr>
François-Xavier Désert <francois-xavier.desert@univ-grenoble-alpes.fr> (IPAG)
Martino Calvo <martino.calvo@neel.cnrs.fr> (IN)
Johannes Goupy <johannes.goupy@neel.cnrs.fr> (IN)
Nicolas Ponthieu <nicolas.ponthieu@univ-grenoble-alpes.fr> (IPAG)
Juan Macias-Perez <macias@lpsc.in2p3.fr> (LPSC)
Andrea Catalano <catalano@lpsc.in2p3.fr> (LPSC)
Laurence Perotto <laurence.perotto@lpsc.in2p3.fr> (LPSC)
- IRAM/Granada NIKA2 support team:
Carsten Kramer (Station Manager and Scheduler, <kramer@iram.es>)
Alessia Ritacco (commissioning of polarization capabilities, <ritaccoa@iram.es>)
Albrecht Sievers (IMBfits, <sievers@iram.es>)
Hans Ungerechts (NCS/pako, <ungerechts@iram.es>)
Pablo Mellado (Computers/Network, <mellado@iram.es>)
Created: 2015.AUG.05 by Israel Hermelo. This page is maintained by AR, SL, CK, and the NIKA2 team.