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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 is built by an international consortium, led by the Institute Neel (Grenoble France). 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 simultaneously the intensity at 1.15 and 2.0 mm. In addition, it allows for polarisation observations at 1.15 mm. NIKA2 is built by an international consortium, led by the Institute Neel (Grenoble, France).

Since October 2015, NIKA2 is installed at the IRAM 30m telescope. After a phase of upgrades, tests, and commissioning, NIKA2 has been offered to the astronomy community for total power observations since October 2017. Polarimetry at 1mm has been commissioned in 2022 and observations of the B-FUN large polarimetry program have started.

Since October 2019, the PIIC software for the reduction of total-power NIKA2 data is available for download together with an extensive, regularly updated tutorial (see the [[PIIC | PIIC dedicated]] page).
Line 10: Line 14:
 * [[http://ipag.osug.fr/nika2/Welcome.html | NIKA2 website at IPAG ]]  * [[https://nika2.osug.fr | NIKA2 website ]]
Line 19: Line 23:
|| NIKA2 2 mm/150 GHz || 616 || 2.00 mm || 125-170 GHz || 9 mJy*s^1/2^ || 17.7" || 6.5' ||
|| NIKA2 1 mm/260 GHz || 2x1140 || 1.15 mm || 240-280 GHz || 34 mJy*s^1/2^ || 11.2" || 6.5' ||

Comments: The half power beam widths are taken from [[https://arxiv.org/pdf/1707.00908.pdf|Adam et al. (2017)]] presenting results from the commissioning. The NEFDs are preliminary, new values, extrapolated to a sky opacity of 0, from observations in the February 2017 commissioning run. NEFDs given in the last call for proposals were too optimistic. <15-Oct-2017 CK>

== Call for proposals and time estimator for winter 2017/18 ==

In the upcoming winter semester running from 1 December 2017 to 30 May 2018, NIKA2 will be offered to the community. Please check the [[http://www.iram-institute.org/EN/content-page-169-7-57-169-0-0.html | call for proposals ]] when it becomes available in August. The time estimator and an accompanying document has been updated [[http://www.iram.es/IRAMES/mainWiki/Continuum/TimeEstimatorScript_winter | here ]], accounting for the commissioning results described in [[https://arxiv.org/pdf/1707.00908.pdf|Adam et al.]].

----


== Open Time Programs ==

[[http://www.iram.es/IRAMES/mainWiki/AcceptedProjects | Summer semester 2017 ]]

[[http://www.iram.es/IRAMES/mainWiki/AcceptedProjects_1w18 | Summer semester 2018 ]]

'''[[ http://www.iram.es/IRAMES/mainWiki/Continuum/NIKA2/Main | Go to the top ]]'''

----
 || NIKA2 2 mm/150 GHz || 616 || 2.00 mm || 125-170 GHz || 9 ± 1 mJy*s^1/2^ || 17.6" || 6.5' ||
|| NIKA2 1 mm/260 GHz || 2x1140 || 1.15 mm || 240-280 GHz || 30 ± 3 mJy*s^1/2^ || 11.1" || 6.5' ||

Comments: The half-power beam widths and the NEFDs are taken from [[https://arxiv.org/abs/1910.02038|Perotto et al. 2020]]. The NEFDs are extrapolated to a sky opacity of 0 and 90 deg. elevation.

== NIKA2 observing time estimator ==

##A Python script to estimate observing times is available together with a document describing the approach and giving examples. Please find it [[http://www.iram.es/IRAMES/mainWiki/Continuum/TimeEstimatorScriptGuideS2020 | here ]] (2020 version).

A Python script to estimate observing times is available together with a document describing the approach and giving examples. Please find it [[http://www.iram.es/IRAMES/mainWiki/Continuum/TimeEstimatorScriptGuideW2023 | here ]].

----
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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 are "fenced" against new continuum 2mm/1mm mapping projects at the 30m or NOEMA. <5-Jul-2017> 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 are "fenced" against new continuum 2mm/1mm mapping projects at the 30m or NOEMA.

The three large programs in Phase I have started observations in October 2017. The Phase II large program on nearby galaxies, 160-16, has started in the summer semester 2019. The B-Fun NIKA2Pol project has started in the winter semester 2021/22.
<CK 08-Feb-2022>
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   * [[attachment:NIKA2-GT-LPs-21jun2017.pdf|NIKA2-GT-LPs-21jun2017.pdf]]
   * [[attachment:NIKA2-GT-LPs-21jun2017.xls|NIKA2-GT-LPs-21jun2017.xls]]


=== Phase I ===

==== 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 ]]'''



==== 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

Homepage: [[ http://lpsc.in2p3.fr/NIKA2LPSZ/ | NIKA2LPSZ]]

'''[[ http://www.iram.es/IRAMES/mainWiki/Continuum/NIKA2/Main | Go to the top ]]'''

=== Phase II ===

==== 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 ]]'''

==== 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 ]]'''
    * [[attachment:NIKA2-GT-LPs-08feb2022.pdf|NIKA2-GT-LPs-08feb2022.pdf]]
   * [[attachment:NIKA2-GT-LPs-08feb2022.xls|NIKA2-GT-LPs-08feb2022.xls]]


 * Phase I

   * '''Galactic Star Formation with NIKA2 - GASTON (122-16) PI is Nicolas Peretto.''' 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.

   * '''The NIKA2 Cosmological Legacy Survey (N2CLS) (192-16) PIs: Guilaine Lagache, Alexandre Beelen, Nicolas Ponthieu''' 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.

   * '''High-resolution tSZ observations of a large sample of clusters of galaxies (NIKA2SZ) (199-16) PIs: Frédéric Mayet, Laurence Perotto''' Homepage: [[ http://lpsc.in2p3.fr/NIKA2LPSZ/ | NIKA2LPSZ]] 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.

 * Phase II

   * '''Interpreting the Millimetre Emission of Galaxies with IRAM and NIKA (IMEGIN) (160-16) PI is Suzanne Madden''' 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.

   * '''Probing the B-Field in star-forming Filaments Using NIKA2-Pol (B-FUN) (015-17) PI: Philippe Andre''' 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.
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 * Adam et al. 2017, '''The NIKA2 large field-of-view millimeter continuum camera for the 30-m IRAM telescope''', [[https://arxiv.org/abs/1707.00908|arxiv]] (accepted for publication on A&A, Jul-2017)  * Astronomical papers:
   * NIKA2
     * Several proceedings papers of the mm Universe conference 2023 (Grenoble/France) have appeared on [[https://arxiv.org/search/?query=NIKA2&searchtype=all&abstracts=show&order=-announced_date_first&size=50 | ArXiv]]
     * Bing et al. 2023, '''NIKA2 Cosmological Legacy Survey: Survey Description and Galaxy Number Counts''', accepted by A&A [[https://arxiv.org/abs/2305.07054|ArXiv]]
     * Katsioli et al. 2023, '''NGC891 seen at millimeter wavelengths''', A&A, 679, A7 [[https://arxiv.org/abs/2309.08403 | ArXiv]][[https://ui.adsabs.harvard.edu/abs/2023A%26A...679A...7K/abstract | ADS ]]
     * Scibelli et al. 2023, '''3D Radiative Transfer Modelling and Virial Analysis of Starless Cores in the B10 Region of the Taurus Molecular Cloud''', MNRAS, 521, 4579 [[https://arxiv.org/pdf/2303.09574.pdf|ArXiv]], [[https://ui.adsabs.harvard.edu/abs/2023MNRAS.521.4579S/abstract|ADS]]
     * Sai et al. 2022, '''Which Part of Dense Cores Feeds Material to Protostars? The Case of L1489 IRS''', A&A, 925, 12 [[https://ui.adsabs.harvard.edu/abs/2022ApJ...925...12S/abstract|ADS]]
     * Muñoz-Echeverría et al. 2022, '''Multi-probe analysis of the galaxy cluster CL J1226.9+3332: Hydrostatic mass and hydrostatic-to-lensing bias''',A&A, 671A, 28, [[https://ui.adsabs.harvard.edu/abs/2023A%26A...671A..28M/abstract|ADS]]
     * Rose et al. 2022, '''The variability of brightest cluster galaxies at high radio frequencies''', MNRAS, 509, 2869 [[https://ui.adsabs.harvard.edu/abs/2022MNRAS.509.2869R/abstract|ArXiv]]
     * Lestrade et al. 2022, '''Candidate cosmic filament in the GJ526 field, mapped with the NIKA2 camera''', accepted for A&A [[https://arxiv.org/abs/2209.12904|ArXiv]]
     * Ferragamo et al. 2022, '''Comparison of hydrostatic and lensing cluster mass estimates: A pilot study in MACS J0647.7+7015''', [[https://ui.adsabs.harvard.edu/abs/2022A%26A...661A..65F/abstract|ADS]]
     * Rose et al. 2022, '''The variability of brightest cluster galaxies at high radio frequencies''', [[https://ui.adsabs.harvard.edu/abs/2022MNRAS.509.2869R/abstract|ADS]]
     * Gianfagna et al. 2021, '''Exploring the hydrostatic mass bias in MUSIC clusters: application to the NIKA2 mock sample''', [[https://ui.adsabs.harvard.edu/abs/2021MNRAS.502.5115G/abstract|ADS]]
     * Rigby et al. 2021, '''GASTON: Galactic Star Formation with NIKA2. Evidence for the mass growth of star-forming clumps''', [[https://arxiv.org/abs/2101.08811|ArXiv]] [[https://academic.oup.com/mnras/article/502/3/4576/6119927?guestAccessKey=2f6e188f-554a-4ac6-8548-de90ade99261|MNRAS]], 502, 4576
     * Luppe et al. 2021, '''Observability of dusty debris discs around M-stars''', [[https://ui.adsabs.harvard.edu/abs/2020MNRAS.499.3932L/abstract|ADS]]
     * Ricci et al. 2020, '''The XXL Survey. XLIV. Sunyaev-Zel'dovich mapping of a low-mass cluster at z ∼ 1: a multi-wavelength approach''', [[https://ui.adsabs.harvard.edu/abs/2020A%26A...642A.126R/abstract|ADS]]
     * Keruzore et al. 2020, '''Exploiting NIKA2/XMM-Newton imaging synergy for intermediate-mass high-z galaxy clusters within the NIKA2 SZ large program. Observations of ACT-CL J0215.4+0030 at z ˜ 0.9''', [[https://ui.adsabs.harvard.edu/abs/2020A%26A...644A..93K/abstract|ADS]]
     * Torne et al. 2020, '''Detection of the magnetar XTE J1810-197 at 150 and 260 GHz with the NIKA2 kinetic inductance detector camera''', [[https://ui.adsabs.harvard.edu/abs/2020A%26A...640L...2T/abstract|ADS]]
     * Ruppin et al. 2020, '''Unveiling the Merger Dynamics of the Most Massive MaDCoWS Cluster at z = 1.2 from a Multiwavelength Mapping of Its Intracluster Medium Properties''', [[https://iopscience.iop.org/article/10.3847/1538-4357/ab8007|ApJ]]
     * Ruppin et al. 2018, '''First Sunyaev-Zel'dovich mapping with NIKA2: implication of cluster substructures on the pressure profile and mass estimate''', [[http://cdsads.u-strasbg.fr/abs/2018A%26A...615A.112R|A&A, 2018, 26, 615]], [[https://arxiv.org/abs/1712.09587|astro-ph]]
     * Conference proceedings of [[https://www.epj-conferences.org/articles/epjconf/abs/2022/01/contents/contents.html|mm Universe 2022 @ NIKA2 - Observing the mm Universe with the NIKA2 Camera]]
     * Conference proceedings of [[https://www.epj-conferences.org/articles/epjconf/abs/2020/04/contents/contents.html|mm Universe 2020 @ NIKA2 - Observing the mm Universe with the NIKA2 Camera]]
   * NIKA
     * Sicilia-Aguilar et al. 2019, '''IRAM and Gaia views of multi-episodic star formation in IC 1396A The origin and dynamics of the Class 0 protostar at the edge of an HII region''', A&A (622, 118) [[https://ui.adsabs.harvard.edu/abs/2019A%26A...622A.118S/abstract|ADS]]
     * Adam et al. 2018, '''Sub-structure and merger detection in resolved NIKA Sunyaev-Zel'dovich images of distant clusters''', A&A (614, A118)
     * Romero et al. 2018, '''A multi-instrument non-parametric reconstruction of the electron pressure profile in the galaxy cluster CLJ1226.9+3332''', A&A (613, 39)
     * Rigby, A., Peretto, N., et al. 2018, '''A NIKA view of two star-forming infrared dark clouds: Dust emissivity variations and mass concentration''', [[https://arxiv.org/pdf/1801.09801.pdf|astro-ph]] [[https://www.aanda.org/articles/aa/pdf/2018/07/aa32258-17.pdf|A&A, 615, A18]]
     * Ritacco, A., Macías Pérez, J.-F., Ponthieu, N. et al. 2018, '''NIKA 150 GHz polarization observations of the Crab nebula and its spectral energy distribution''', [[https://www.aanda.org/component/article?access=doi&doi=10.1051/0004-6361/201731551|A&A]], 616, A35
     * Adam et al. 2017, '''Mapping the hot gas temperature in galaxy clusters using X-ray and Sunyaev-Zel'dovich imaging''', A&A, 606, 64 [[http://cdsads.u-strasbg.fr/abs/2017arXiv170610230A|ADS]]
     * Bracco et al. 2017, '''Probing changes of dust properties along a chain of solar-type prestellar and protostellar cores in Taurus with NIKA''', A&A, 604, 52 [[http://cdsads.u-strasbg.fr/abs/2017arXiv170608407B|ADS]]
     * 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]]
     * Chacon-Tanarro et al. 2017, '''Search for grain growth towards the center of L1544''', A&A, 606, A142 [[http://cdsads.u-strasbg.fr/abs/2017A%26A...606A.142C|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, [[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]]

   * NIKA related papers
     *Aumont, J., Macías Pérez, J.-F., Ritacco, A., Ponthieu, N., Mangilli, A., 2018, '''Absolute calibration of the polarisation angle for future CMB B-mode experiments from current and future measurements of the Crab nebula''', (submitted to A&A) [[https://arxiv.org/abs/1805.10475|arxiv]]
     * Chastenet et al., '''SOFIA/HAWC+ observations of the Crab Nebula: dust properties from polarized emission''', MNRAS, 516,[[https://ui.adsabs.harvard.edu/abs/2022MNRAS.516.4229C/abstract|ADS]]
Line 105: Line 108:

   * 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:
   * Adam et al. 2017, '''Mapping the hot gas temperature in galaxy clusters using X-ray and Sunyaev-Zel'dovich imaging''', A&A, 606, 64 (in press) [[http://cdsads.u-strasbg.fr/abs/2017arXiv170610230A|ADS]]
   * Bracco et al. 2017, '''Probing changes of dust properties along a chain of solar-type prestellar and protostellar cores in Taurus with NIKA''', A&A, subm. [[http://cdsads.u-strasbg.fr/abs/2017arXiv170608407B|ADS]]
   * 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]]		    * NIKA2
     * Perotto et al. 2020, '''Calibration and Performance of the NIKA2 camera at the IRAM 30-meter Telescope''', [[https://arxiv.org/abs/1910.02038|arxiv]] [[https://www.aanda.org/articles/aa/pdf/2020/05/aa36220-19.pdf|A&A]]
     * Adam et al. 2018, '''The NIKA2 large field-of-view millimeter continuum camera for the 30-m IRAM telescope''', [[https://arxiv.org/abs/1707.00908|arxiv]] [[https://www.aanda.org/component/article?access=doi&doi=10.1051/0004-6361/201731503|A&A]]
     * 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]]
   * NIKA
     * 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]]
     * 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]]
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   * ''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]])
   * ''Aurélien Bideaud (2007-2010) - NEEL - Supervisors: A. Benoit and F.-X. Desert'' - [[https://https://tel.archives-ouvertes.fr/tel-00589869 | Development of a camera for millimeter-wave radioastronomy]].

   * ''Markus Roesch (2010 - 2013) - IRAM - Supervisors: K. Schuster and M. Siegel'' - [[https://www.ksp.kit.edu/9783731501107 | Development of lumped element kinetic inductance detectors for mm-wave astronomy at the IRAM 30m telescope]].

   * ''Antonio D’Addabbo (2011 - 2014) - NEEL - Supervisors: A. Monfardini and P. de Bernardis'' - [[https://tel.archives-ouvertes.fr/tel-01368000 | Applications of Kinetic Inductance Detectors to Astronomy and Particle Physics]].

   * ''Rémi Adam (2012-2015) - LPSC - Advisors: J.F. Macías-Pérez and F.X. Désert'' - [[https://tel.archives-ouvertes.fr/tel-01303736 | Observation of galaxy clusters via the Sunyaev-Zel'dovich effect and the polarization of the cosmic microwave background]] (in French).

   * ''Grégoire Coiffard (2012 - 2015) - IRAM - Supervisor: K. Schuster'' - [[https://tel.archives-ouvertes.fr/tel-01266429 | Development of kinetic inductance detectors for millimeter astronomy and related problems in material science and process technology]].

   * ''Alessia Ritacco (2013-2016) - LPSC - Advisors: J.F. Macías-Pérez, Alessandro Monfardini, Andrea Catalan and Nicolas Ponthieu'' - [[https://tel.archives-ouvertes.fr/tel-01467862|Polarimetry at millimeter wavelengths with the instruments NIKA and NIKA2]].

   * ''Florian Ruppin (2016 - 2018) - LPSC - Supervisor: F. Mayet'' - [[https://tel.archives-ouvertes.fr/tel-01978797 | Cosmology from Sunyaev-Zel’dovich observations of galaxy clusters with the NIKA2]].

   * ''Shibo Shu (2017 - 2019) - IRAM - Supervisors: K. Schuster and E. Driessen'' - [[https://tel.archives-ouvertes.fr/tel-02493945 | Large format LEKID arrays for millimeter-wave astronomy]].

   * ''Aina Andrianasolo (2017 - 2019) - IPAG - Supervisors: F.-X. Desert and N. Ponthieu'' - [[https://theses.hal.science/tel-02936622 | Measuring the sky polarization with KIDS on the ground with NIKA2 and preparing satellite observations]].
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   * Many more [[https://wiki.iram.fr/wiki/nika2/index.php/Conferences | talks in the dedicated private wiki table]]
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 * [[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 ]]
  * Cryostat & Electronics
   * [[attachment:calvo-07jan2017-nika2-PTpositionAdjustment.pdf| Pulse Tube Adjustment, M.Calvo, Jan-2017 ]]
   * [[attachment:replacingElectronicBoxes_1.pdf | Guide to replace electronic boxes for thermometer readout ]]
   * [[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)]]
   * [[SpectralBands | Spectral bands ]]
 * Network
   * [[attachment:calvo-12jun2017-NIKA2networkDescription.pdf | Computer Network, M.Calvo, June-2017 ]]
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 * Acquisition and tuning
   * [[attachment:calvo-feb2016-nika2-camadia.pdf | Data Acquisition: HOWTO, M.Calvo, Feb-2017 ]]
   * [[attachment:NIKA2_recovery13mar2018.pdf | Data Acquisition V1: Recovery, M.Calvo, Mar-2018 ]]
   * [[attachment:NIKA2_V2_IRAM_recovery.pdf | Data Acquisition V2: Recovery, M.Calvo, Oct-2018 ]]
   * [[attachment:calvo-docTuning_feb2016.pdf | Tuning procedure and data flagging description, M.Calvo, Feb-2016 ]]
   * [[attachment:checkingNoiseSpectra_v2.pdf | Checking Noise traces ]]
 * Observations
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## * [[http://www.iram.es/IRAMES/mainWiki/Continuum/TimeEstimatorScript|Time Estimator (UNDER CONSTRUCTION)]]

## * [[http://www.iram.es/IRAMES/mainWiki/Continuum/ObserveGRBs | Observe GRBs]]

## ----
##
== Science runs ==
##
=== s17 pool: 24-31 October 2017 ===
 
 * Accepted [[http://www.iram.es/IRAMES/mainWiki/AcceptedProjects|projects in open time]] and in [[http://www.iram.es/IRAMES/mainWiki/Continuum/NIKA2/Main#Phase_I | guaranteed time]].
 * See the progress of observations in the [[https://pools.iram.es | Pool data base]] and in [[https://tapas.iram.es/tapas/ | TAPAS]]. Both databases are synchronized and can be used to write/read a logsheet. [[D2DLogNika2Pool1 |Day to day logbook]] : Scan types table, Pipeline RTA logbook (Quicklook plots table).
 * [[GoalsPrepStaffNika2Pool1 |Observers and staff at the telescope]]
 * [[http://www.iram.es/IRAMES/mainWiki/Continuum/PoolPreparation | Preparation Page ]]
 * [[http://www.iram.es/IRAMES/mainWiki/Continuum/ObservingSession | Observing session Page ]]
 * [[DailyReportsNika2Pool1| Daily Reports]]
 * [[D2DLogNika2Run12 |Day to day logbook]] : Scan types table, Pipeline RTA logbook (Quicklook plots table)
 * [[attachment:NIKA2_Oct2017_Planning.xlsx | Proposed Technical Observations ]]
 * ~-[= Run 25 of a NIKA instrument]-~		    * [[http://www.iram.es/IRAMES/mainWiki/Continuum/PolarimetricObservations| Polarimetric observations]] provides information for changing from total power to polarimetric observations mode and vice versa, in a checklist form.
 * Data reduction
   * [[PIIC | PIIC]] software.
   * IDL pipeline

----

== Science runs (October 2017 - February 2024) ==

 * See the progress of observations in the [[https://pools.iram.es | Pool data base]] and in [[https://tapas.iram.es/tapas/ | TAPAS]]. Both databases are synchronized and can be used to write/read a logsheet.

 * [[http://www.iram.es/IRAMES/mainWiki/Continuum/ObservingSession | Information on HowTo observe ]]


=== Current Semester: Winter 2023 {{nobold|(no science observations in Summer 2023 due to 30m telescope upgrade)}} ===

   * '''13-20 February 2024 - w23 Pool #1''' ~-[= Cryo Run 77, 65^th^ of NIKA2]-~

     * [[GoalsPrepStaffNika2Pool130224 |Observers and staff at the telescope]]
     * [[DailyReportsNika2Pool130224| Daily Reports]]

   * '''20-27 February 2024 - w23 Pool #2''' ~-[= Cryo Run 77, 65^th^ of NIKA2]-~

     * [[GoalsPrepStaffNika2Pool200224 |Observers and staff at the telescope]]
     * [[DailyReportsNika2Pool200224| Daily Reports]]


=== Previous Semester: Winter 2022 ===

   * '''6-13 December 2022 - w22 Pool #1''' ~-[= Cryo Run 74, 62^nd^ of NIKA2]-~

     * [[GoalsPrepStaffNika2Pool061222 |Observers and staff at the telescope]]
     * [[DailyReportsNika2Pool061222| Daily Reports]]

   * '''10-17 January 2023 - w22 Pool #2''' ~-[= Cryo Run 75, 63^rd^ of NIKA2]-~

     * [[GoalsPrepStaffNika2Pool100123 |Observers and staff at the telescope]]
     * [[DailyReportsNika2Pool100123| Daily Reports]]

   * '''17-24 January 2023 - w22 Pool #3''' ~-[= Cryo Run 75, 63^rd^ of NIKA2]-~

     * [[GoalsPrepStaffNika2Pool170123 |Observers and staff at the telescope]]
     * [[DailyReportsNika2Pool170123| Daily Reports]]

   * '''24-31 January 2023 - w22 Pool #4''' ~-[= Cryo Run 75, 63^rd^ of NIKA2]-~

     * [[GoalsPrepStaffNika2Pool240123 |Observers and staff at the telescope]]
     * [[DailyReportsNika2Pool240123| Daily Reports]]


=== Previous Semesters ===

   * [[SummerPools2022 | Science Runs Summer 2022 ]]
   * [[WinterPools2021 | Science Runs Winter 2021 ]]
   * [[SummerPools2021 | Science Runs Summer 2021 ]]
   * [[WinterPools2020 | Science Runs Winter 2020 ]]
   * [[SummerPools2020 | Science Runs Summer 2020 ]]
   * [[WinterPools2019 | Science Runs Winter 2019 ]]
   * [[SummerPools2019 | Science Runs Summer 2019 ]]
   * [[WinterPools2018 | Science Runs Winter 2018 ]]
   * [[SummerPools2018 | Science Runs Summer 2018 ]]
   * [[WinterPools2017 | Science Runs Winter 2017 ]]

   * Previously accepted [[http://www.iram.es/IRAMES/mainWiki/AcceptedProjectsOpenTime|projects in open time]].
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=== w18 pool weeks ===

==== I: 16-23 January 2018 ====
 
 * Accepted [[http://www.iram.es/IRAMES/mainWiki/AcceptedProjects_1w18|projects in open time]] and in [[http://www.iram.es/IRAMES/mainWiki/Continuum/NIKA2/Main#Phase_I | guaranteed time]].
 * See the progress of observations in the [[https://pools.iram.es | Pool data base]] and in [[https://tapas.iram.es/tapas/ | TAPAS]]. Both databases are synchronized and can be used to write/read a logsheet. [[D2DLogNika2Pool1 |Day to day logbook]] : Scan types table, Pipeline RTA logbook (Quicklook plots table).
 * [[http://www.iram.es/IRAMES/mainWiki/Continuum/PoolPreparation | Preparation Page ]]
 * [[http://www.iram.es/IRAMES/mainWiki/Continuum/ObservingSession | Observing session Page ]]
 * ~-[= Run 27 of a NIKA instrument]-~
 
==== II: 13-20 February 2018 ====

'''[[ http://www.iram.es/IRAMES/mainWiki/Continuum/NIKA2/Main | Go to the top ]]'''

----

== Commissioning runs ==

=== Phase I (October 2015 - April 2017) ===

 * '''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]		 ----

== Commissioning & special test runs ==

 * [[attachment:History_of_optical_and_radio_alignments_of_NIKA2.pdf|History_of_optical_and_radio_alignments_of_NIKA2.pdf]]

=== Phase I [total power] (October 2015 - April 2017) ===

 * '''1^st^ run of NIKA2 (test)''': 29-October-2015 till 10-November-2015. '''Installation''', cool down at the 30m, testing/debugging/developing. Alignment. [= Run 13 of a NIKA instrument ; numbering useful for analysis software, count numbers of cooling down the cryostat <=> Cryo Run]
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 * '''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]  * '''2^nd^ run of NIKA2 (test)''': 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 <=> Cryo Run 14]
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 * '''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]  * '''3^rd^ run of NIKA2 (test)''': 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]
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 * '''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]  * '''4^th^ run of NIKA2 (test)''': 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]
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 * '''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]  * '''5^th^ run of NIKA2 (test)''': 16-September-2016 till 11-October-2016. '''Upgrade NIKA2 with new dichroic, new corrugated lenses, 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. (window not changed due to defects on new one). Alignment. [= Run 18 of a NIKA instrument]
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 * '''6^th^ test run of NIKA2''': 25-October-2016 till 1-November-2016. Continue NIKA2 commissioning. [= Run 19 of a NIKA instrument]  * '''6^th^ run of NIKA2 (test)''': 25-October-2016 till 1-November-2016. Continue NIKA2 commissioning. [= Run 19 of a NIKA instrument]
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 * '''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]  * '''7^th^ run of NIKA2 (test)''': 6-December-2016 till 13-December-2016. Test DRO based external calibrator, continue NIKA2 commissioning. [= Run 20 of a NIKA instrument]
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 * '''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 (degraded during run 5 intervention), short test on sky to see effect of the intervention. [= Run 21 of a NIKA instrument]  * '''8^th^ run of NIKA2 (test)''': 9-January-2017 to 13-January-2017, then 23-January to 27-January. Reverse 1mm bands 0.1K lenses to smooth version + adjust fixation of cold mirrors block (M7-M8) to get better radio alignment of the internal optics (degraded during run 5 intervention), short test on sky to see effect of the intervention. [= Run 21 of a NIKA instrument]
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 * '''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]  * '''9^th^ run of NIKA2 (test)''': 21-February-2017 to 28-February-2017. Resume NIKA2 commissioning after run 8 intervention. [= Run 22 of a NIKA instrument]
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 * '''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]  * '''10^th^ run of NIKA2 (test)''': 18-April-2017 to 25-April-2017. End of commissioning phase 1, science verification. [= Cryo Run 23]
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=== Phase II (June, November 2017) ===

 * '''11^th^ test run of NIKA2''': 8-June-2017 to 13-June-2017. Start commissioning phase 2: polarization. [= Run 24 of a NIKA instrument]		 === Phase II [Polarization, Tests] (June 2017 - November 2021) ===

 * '''11^th^ run of NIKA2 (test)''': 8-June-2017 to 13-June-2017. Start commissioning phase 2: polarization. [= Cryo Run 24]
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 * '''13^th^ test run of NIKA2''': 21-November-2017 to 28-November-2017. Continuation of commissioning in polarization mode. [= Run 26 of a NIKA instrument]  * '''13^th^ run of NIKA2 (test)''': 21-November-2017 to 28-November-2017. (Alignment done in run 12). Continuation of commissioning in polarization mode. [= Cryo Run 26]
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-----  * 16^th^ run of NIKA2 (test): 6 to 13-March-2018. Continuation of commissioning in polarization mode. [= Cryo Run 29] (Run lost due to bad weather)
  * [[Nika2Run16|Go to the 16th run Wiki page]]

 * '''19^th^ run of NIKA2 (test)''': 12 to 17-June-2018. Continuation of commissioning in polarisation mode (redo run 16 lost due to bad weather). '''+ Spectral characterization with a Martin Puplett''' (named PIMP): 18 to 22 June 2018. [= Cryo Run 32]
  * [[Nika2Run19|Go to the 19th run Wiki page]]

 * '''Change of dichroic''' and entrance window: 27 to 29-August-2018. Results of June's PIMP measurement; remove 2nd dichroic and install 3rd dichroic; preparation of PIMP upgrade.
  * [[Nika2DichroicChange|Go to the Wiki page]]

 * '''20^th^ and 21^st^ run of NIKA2 (test)''': 5-6 September (!N2R20) and 18 to 25-September-2018 (!N2R21). Performance characterization after replacement of the dichroic. [Sep 5-6 dichroic = Cryo Run 33 ; Sep 5-6 polar = Cryo Run 34; Sep 18-25 = Cryo Run 35] '''Because dichroic no.3 showed problems, the 2nd dichroic was re-installed between 5-6 September and 18-25 September. We are continuing with dichroic no.2..'''
  * [[Nika2Run20|Go to the 20th and 21st runs Wiki page]]

 * '''25^th^ run of NIKA2 (test)''': 04 to 11-December-2018. Continuation of polarisation commissioning. [ = Cryo Run 39]
  * [[Nika2Run25|Go to the 25th run Wiki page]]

 * 31^st^ run of NIKA2 (test): 16 and 17-May-2019. Short DAQ v3 tests. Sep 6: Checks and and test in preparation for the IRAM School (Sep 7-10);(not really a test run) [ = Cryo Run 45]
  * [[Nika2Run31|Go to the 31st run Wiki page]]

 * 32^nd^ run of NIKA2 (test): 7 to 10-September-2019. Sep 7-10 use of NIKA2 at the 9th IRAM 30m Summerschool. (not really a test run) [ = Cryo Run 46]
  * [[Nika2Run32|Go to the 32nd run Wiki page]]

 * '''33^rd^ run of NIKA2 (test)''': Sep 11th 2019 tests of DAQ v3 in preparation of commissioning run. 17 to 24-September-2019. Updated DAQ v3 tests, PIMP, external calibrator, polarization. [ = Cryo Run 47]
  * [[Nika2Run33|Go to the 33rd run Wiki page]]

 * '''42^nd^ run of NIKA2 (test)''': Feb 25th - Mar 3rd 2020. (Alignment done just befor run 38, and re-checked here). Polarimetry commissioning [ = Cryo Run 54]
  * [[Nika2Run42|Go to the 42nd run Wiki page]]

 * '''44^th^ run of NIKA2 (test)''': Aug 6th - Aug 29th 2020. Summer testing festival [ = Cryo Run 56]. Telescope stopped.
  * [[Nika2Run44|Go to the 44th run Wiki page]]

 * '''46^th^ run of NIKA2 (test)''': Nov 10-17 2020. Polarimetry commissioning [ = Cryo Run 58].
  * [[Nika2Run46|Go to the 46th run Wiki page]]

 * '''53^rd^ run of NIKA2 (test)''': Jul 9 2021. A2 recent excess noise investigation. [= Cryo Run 65]
  * [[Nika2Run53| Go to the 53th run Wiki page]]

 * '''54^th^ run of NIKA2 (test)''': Sep 21-25 2021. New Sweep, Check up before pool, Polarization tests including external calibrator source [ = Cryo Run 66].
  * [[Nika2Run54|Go to the 54th run Wiki page]]

----
Line 257: Line 334:
 * Overall coordinator:  * Overall coordinators:
  * '''Stefano Berta''' (IRAM/Grenoble, <berta@iram.fr>)
Line 272: Line 350:
  * Carsten Kramer (30m Station Manager and Scheduler, <kramer@iram.es>)    * Miguel Sanchez (30m Station Manager, <msanchez@iram.es>)
Line 274: Line 352:
  * Albrecht Sievers (IMBfits/Data, <sievers@iram.es>)
  * Hans Ungerechts (NCS/pako, <ungerechts@iram.es>)		   * Albrecht Sievers (IMBfits/Data, NCS/pako, <sievers@iram.es>)
Line 277: Line 354:
  * Santiago Navarro, Dave John (Cryostat, <john@ira.es>, <navarro@iram.es>)   * Santiago Navarro, Dave John (Cryostat, <john@iram.es>, <navarro@iram.es>)
  * Angel Bongiovanni, Ioannis Myserlis, Stergios Amarantidis (NIKA2 Pool Managing, <bongio@iram.es>, <imyserlis@iram.es>, <samarant@iram.es>)
  * Bilal Ladjelate (former postdoc of IRAM/Granada and Pool manager until April 2021, <ladjelate@iram.es>)
Line 282: Line 361:
  * Charles Romero (Commissioning, <romero@iram.fr>)   * Stefano Berta (Coordinator, Data processing Software, <berta@iram.fr>)
Line 284: Line 363:
  * Carsten Kramer (Scheduler, <kramer@iram.fr>)

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 simultaneously the intensity at 1.15 and 2.0 mm. In addition, it allows for polarisation observations at 1.15 mm. NIKA2 is built by an international consortium, led by the Institute Neel (Grenoble, France).

Since October 2015, NIKA2 is installed at the IRAM 30m telescope. After a phase of upgrades, tests, and commissioning, NIKA2 has been offered to the astronomy community for total power observations since October 2017. Polarimetry at 1mm has been commissioned in 2022 and observations of the B-FUN large polarimetry program have started.

Since October 2019, the PIIC software for the reduction of total-power NIKA2 data is available for download together with an extensive, regularly updated tutorial (see the PIIC dedicated page).

Contents

  1. NIKA2 Homepage
    1. Overview
    2. NIKA2 observing time estimator
    3. The five Guaranteed Time Large Programs
    4. Publications
    5. Technical Documentation
    6. Science runs (October 2017 - February 2024)
      1. Current Semester: Winter 2023 {{nobold|(no science observations in Summer 2023 due to 30m telescope upgrade)}}
      2. Previous Semester: Winter 2022
      3. Previous Semesters
    7. Commissioning & special test runs
      1. Phase I [total power] (October 2015 - April 2017)
      2. Phase II [Polarization, Tests] (June 2017 - November 2021)
    8. Support teams

NIKA2 in the web:

Overview

Band

Number of KIDs

Wavelength

Bandwidth

NEFD

HPBW

FoV

NIKA2 2 mm/150 GHz

616

2.00 mm

125-170 GHz

9 ± 1 mJy*s1/2

17.6"

6.5'

NIKA2 1 mm/260 GHz

2x1140

1.15 mm

240-280 GHz

30 ± 3 mJy*s1/2

11.1"

6.5'

Comments: The half-power beam widths and the NEFDs are taken from Perotto et al. 2020. The NEFDs are extrapolated to a sky opacity of 0 and 90 deg. elevation.

NIKA2 observing time estimator

A Python script to estimate observing times is available together with a document describing the approach and giving examples. Please find it here.

The five Guaranteed Time Large 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 are "fenced" against new continuum 2mm/1mm mapping projects at the 30m or NOEMA.

The three large programs in Phase I have started observations in October 2017. The Phase II large program on nearby galaxies, 160-16, has started in the summer semester 2019. The B-Fun NIKA2Pol project has started in the winter semester 2021/22. <CK 08-Feb-2022>

  • Source list
  • Phase I

    • Galactic Star Formation with NIKA2 - GASTON (122-16) PI is Nicolas Peretto. 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.

    • The NIKA2 Cosmological Legacy Survey (N2CLS) (192-16) PIs: Guilaine Lagache, Alexandre Beelen, Nicolas Ponthieu 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.

    • High-resolution tSZ observations of a large sample of clusters of galaxies (NIKA2SZ) (199-16) PIs: Frédéric Mayet, Laurence Perotto Homepage: NIKA2LPSZ 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.

  • Phase II

    • Interpreting the Millimetre Emission of Galaxies with IRAM and NIKA (IMEGIN) (160-16) PI is Suzanne Madden 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.

    • Probing the B-Field in star-forming Filaments Using NIKA2-Pol (B-FUN) (015-17) PI: Philippe Andre 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.

Publications

  • Astronomical papers:
    • NIKA2

      • Several proceedings papers of the mm Universe conference 2023 (Grenoble/France) have appeared on ArXiv

      • Bing et al. 2023, NIKA2 Cosmological Legacy Survey: Survey Description and Galaxy Number Counts, accepted by A&A ArXiv

      • Katsioli et al. 2023, NGC891 seen at millimeter wavelengths, A&A, 679, A7 ArXivADS

      • Scibelli et al. 2023, 3D Radiative Transfer Modelling and Virial Analysis of Starless Cores in the B10 Region of the Taurus Molecular Cloud, MNRAS, 521, 4579 ArXiv, ADS

      • Sai et al. 2022, Which Part of Dense Cores Feeds Material to Protostars? The Case of L1489 IRS, A&A, 925, 12 ADS

      • Muñoz-Echeverría et al. 2022, Multi-probe analysis of the galaxy cluster CL J1226.9+3332: Hydrostatic mass and hydrostatic-to-lensing bias,A&A, 671A, 28, ADS

      • Rose et al. 2022, The variability of brightest cluster galaxies at high radio frequencies, MNRAS, 509, 2869 ArXiv

      • Lestrade et al. 2022, Candidate cosmic filament in the GJ526 field, mapped with the NIKA2 camera, accepted for A&A ArXiv

      • Ferragamo et al. 2022, Comparison of hydrostatic and lensing cluster mass estimates: A pilot study in MACS J0647.7+7015, ADS

      • Rose et al. 2022, The variability of brightest cluster galaxies at high radio frequencies, ADS

      • Gianfagna et al. 2021, Exploring the hydrostatic mass bias in MUSIC clusters: application to the NIKA2 mock sample, ADS

      • Rigby et al. 2021, GASTON: Galactic Star Formation with NIKA2. Evidence for the mass growth of star-forming clumps, ArXiv MNRAS, 502, 4576

      • Luppe et al. 2021, Observability of dusty debris discs around M-stars, ADS

      • Ricci et al. 2020, The XXL Survey. XLIV. Sunyaev-Zel'dovich mapping of a low-mass cluster at z ∼ 1: a multi-wavelength approach, ADS

      • Keruzore et al. 2020, Exploiting NIKA2/XMM-Newton imaging synergy for intermediate-mass high-z galaxy clusters within the NIKA2 SZ large program. Observations of ACT-CL J0215.4+0030 at z ˜ 0.9, ADS

      • Torne et al. 2020, Detection of the magnetar XTE J1810-197 at 150 and 260 GHz with the NIKA2 kinetic inductance detector camera, ADS

      • Ruppin et al. 2020, Unveiling the Merger Dynamics of the Most Massive MaDCoWS Cluster at z = 1.2 from a Multiwavelength Mapping of Its Intracluster Medium Properties, ApJ

      • Ruppin et al. 2018, First Sunyaev-Zel'dovich mapping with NIKA2: implication of cluster substructures on the pressure profile and mass estimate, A&A, 2018, 26, 615, astro-ph

      • Conference proceedings of mm Universe 2022 @ NIKA2 - Observing the mm Universe with the NIKA2 Camera

      • Conference proceedings of mm Universe 2020 @ NIKA2 - Observing the mm Universe with the NIKA2 Camera

    • NIKA

      • Sicilia-Aguilar et al. 2019, IRAM and Gaia views of multi-episodic star formation in IC 1396A The origin and dynamics of the Class 0 protostar at the edge of an HII region, A&A (622, 118) ADS

      • Adam et al. 2018, Sub-structure and merger detection in resolved NIKA Sunyaev-Zel'dovich images of distant clusters, A&A (614, A118)

      • Romero et al. 2018, A multi-instrument non-parametric reconstruction of the electron pressure profile in the galaxy cluster CLJ1226.9+3332, A&A (613, 39)

      • Rigby, A., Peretto, N., et al. 2018, A NIKA view of two star-forming infrared dark clouds: Dust emissivity variations and mass concentration, astro-ph A&A, 615, A18

      • Ritacco, A., Macías Pérez, J.-F., Ponthieu, N. et al. 2018, NIKA 150 GHz polarization observations of the Crab nebula and its spectral energy distribution, A&A, 616, A35

      • Adam et al. 2017, Mapping the hot gas temperature in galaxy clusters using X-ray and Sunyaev-Zel'dovich imaging, A&A, 606, 64 ADS

      • Bracco et al. 2017, Probing changes of dust properties along a chain of solar-type prestellar and protostellar cores in Taurus with NIKA, A&A, 604, 52 ADS

      • 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

      • Chacon-Tanarro et al. 2017, Search for grain growth towards the center of L1544, A&A, 606, A142 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, 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

    • NIKA related papers

      • Aumont, J., Macías Pérez, J.-F., Ritacco, A., Ponthieu, N., Mangilli, A., 2018, Absolute calibration of the polarisation angle for future CMB B-mode experiments from current and future measurements of the Crab nebula, (submitted to A&A) arxiv

      • Chastenet et al., SOFIA/HAWC+ observations of the Crab Nebula: dust properties from polarized emission, MNRAS, 516,ADS

  • Instrument/detectors papers:
    • NIKA2

      • Perotto et al. 2020, Calibration and Performance of the NIKA2 camera at the IRAM 30-meter Telescope, arxiv A&A

      • Adam et al. 2018, The NIKA2 large field-of-view millimeter continuum camera for the 30-m IRAM telescope, arxiv A&A

      • 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

    • NIKA

      • 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

      • 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

      • Internal list of technical papers

  • Ph.D. thesis:
  • Talks:

  • NIKA2 publications list maintained at IPAG

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Technical Documentation

Science runs (October 2017 - February 2024)

Current Semester: Winter 2023 {{nobold|(no science observations in Summer 2023 due to 30m telescope upgrade)}}

Previous Semester: Winter 2022

Previous Semesters

Go to the top

Commissioning & special test runs

Phase I [total power] (October 2015 - April 2017)

  • 1st run of NIKA2 (test): 29-October-2015 till 10-November-2015. Installation, cool down at the 30m, testing/debugging/developing. Alignment. [= Run 13 of a NIKA instrument ; numbering useful for analysis software, count numbers of cooling down the cryostat <=> Cryo Run]

  • 2nd run of NIKA2 (test): 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 <=> Cryo Run 14]

  • 3rd run of NIKA2 (test): 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 run of NIKA2 (test): 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 run of NIKA2 (test): 16-September-2016 till 11-October-2016. Upgrade NIKA2 with new dichroic, new corrugated lenses, 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. (window not changed due to defects on new one). Alignment. [= Run 18 of a NIKA instrument]

  • 6th run of NIKA2 (test): 25-October-2016 till 1-November-2016. Continue NIKA2 commissioning. [= Run 19 of a NIKA instrument]

  • 7th run of NIKA2 (test): 6-December-2016 till 13-December-2016. Test DRO based external calibrator, continue NIKA2 commissioning. [= Run 20 of a NIKA instrument]

  • 8th run of NIKA2 (test): 9-January-2017 to 13-January-2017, then 23-January to 27-January. Reverse 1mm bands 0.1K lenses to smooth version + adjust fixation of cold mirrors block (M7-M8) to get better radio alignment of the internal optics (degraded during run 5 intervention), short test on sky to see effect of the intervention. [= Run 21 of a NIKA instrument]

  • 9th run of NIKA2 (test): 21-February-2017 to 28-February-2017. Resume NIKA2 commissioning after run 8 intervention. [= Run 22 of a NIKA instrument]

  • 10th run of NIKA2 (test): 18-April-2017 to 25-April-2017. End of commissioning phase 1, science verification. [= Cryo Run 23]

Phase II [Polarization, Tests] (June 2017 - November 2021)

  • 11th run of NIKA2 (test): 8-June-2017 to 13-June-2017. Start commissioning phase 2: polarization. [= Cryo Run 24]

  • 13th run of NIKA2 (test): 21-November-2017 to 28-November-2017. (Alignment done in run 12). Continuation of commissioning in polarization mode. [= Cryo Run 26]

  • 16th run of NIKA2 (test): 6 to 13-March-2018. Continuation of commissioning in polarization mode. [= Cryo Run 29] (Run lost due to bad weather)

  • 19th run of NIKA2 (test): 12 to 17-June-2018. Continuation of commissioning in polarisation mode (redo run 16 lost due to bad weather). + Spectral characterization with a Martin Puplett (named PIMP): 18 to 22 June 2018. [= Cryo Run 32]

  • Change of dichroic and entrance window: 27 to 29-August-2018. Results of June's PIMP measurement; remove 2nd dichroic and install 3rd dichroic; preparation of PIMP upgrade.

  • 20th and 21st run of NIKA2 (test): 5-6 September (N2R20) and 18 to 25-September-2018 (N2R21). Performance characterization after replacement of the dichroic. [Sep 5-6 dichroic = Cryo Run 33 ; Sep 5-6 polar = Cryo Run 34; Sep 18-25 = Cryo Run 35] Because dichroic no.3 showed problems, the 2nd dichroic was re-installed between 5-6 September and 18-25 September. We are continuing with dichroic no.2..

  • 25th run of NIKA2 (test): 04 to 11-December-2018. Continuation of polarisation commissioning. [ = Cryo Run 39]

  • 31st run of NIKA2 (test): 16 and 17-May-2019. Short DAQ v3 tests. Sep 6: Checks and and test in preparation for the IRAM School (Sep 7-10);(not really a test run) [ = Cryo Run 45]

  • 32nd run of NIKA2 (test): 7 to 10-September-2019. Sep 7-10 use of NIKA2 at the 9th IRAM 30m Summerschool. (not really a test run) [ = Cryo Run 46]

  • 33rd run of NIKA2 (test): Sep 11th 2019 tests of DAQ v3 in preparation of commissioning run. 17 to 24-September-2019. Updated DAQ v3 tests, PIMP, external calibrator, polarization. [ = Cryo Run 47]

  • 42nd run of NIKA2 (test): Feb 25th - Mar 3rd 2020. (Alignment done just befor run 38, and re-checked here). Polarimetry commissioning [ = Cryo Run 54]

  • 44th run of NIKA2 (test): Aug 6th - Aug 29th 2020. Summer testing festival [ = Cryo Run 56]. Telescope stopped.

  • 46th run of NIKA2 (test): Nov 10-17 2020. Polarimetry commissioning [ = Cryo Run 58].

  • 53rd run of NIKA2 (test): Jul 9 2021. A2 recent excess noise investigation. [= Cryo Run 65]

  • 54th run of NIKA2 (test): Sep 21-25 2021. New Sweep, Check up before pool, Polarization tests including external calibrator source [ = Cryo Run 66].

Support teams

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Created: 2015.AUG.05 by Israel Hermelo. This page is maintained by AR, SL, CK, and the NIKA2 team.

Continuum/NIKA2/Main (last edited 2024-10-23 12:27:04 by CarstenKramer)