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NIKA2, the second generation Neel-IRAM-KID-Array, is a dual band camera operating simultaneously at 150 and 260 GHz. The instrument is based on large arrays of superconducting Kinetic Inductance Detectors (KID) operated at temperatures of 100mK. NIKA2 is built by an international consortium, led by the Institute Neel (Grenoble France).
Successful installation took place in early October 2015. NIKA2's field of view has a 6.5arcmin diameter, with angular resolutions of 12 and 18 arcsec at 1 and 2 mm wavelengths respectively. NIKA2 is designed as a facility instrument which will remain at its present position for at least a decade. The instrument will allow to measure linear polarizations at 1.15 mm.

For September 2016, some important changes to the hardware are currently being prepared: the 150 GHz array, the dichroic frequency
splitter, the lenses, and the cryostat window will be replaced and upgraded. In addition, several of the 20 readout electronics boards
will be replaced with the last version. Commissioning will then continue well into the winter semester and NIKA2 shall be opened to the community in 2017. 		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).
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Some prelimiary characteristics of NIKA-2:
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|| NIKA2 2 mm/150 GHz || 1020 || 2.00 mm || 125-170 GHz || 20 mJy*s^1/2^ || 12" || 6.5' ||
|| NIKA2 1 mm/260 GHz || 2x1140 || 1.15 mm || 240-280 GHz || 30 mJy*s^1/2^ || 18" || 6.5' ||



== Call for proposals and time estimator ==

A limited amount of time will be available in the upcoming winter semester 2016/17. See the call for proposals [[http://www.iram-institute.org/EN/content-page-169-7-57-169-0-0.html | here ]]. The above sensitivities shall be used, together with a factor for overheads (pointing, focus, slewing) of 2.0. A time estimator is in preparation and shall go online in early August.

## * [[http://www.iram.es/IRAMES/mainWiki/Continuum/TimeEstimatorScript | Guidelines to estimate observing times]].

----		 || NIKA2 2 mm/150 GHz || 616 || 2.00 mm || 125-170 GHz || 6 mJy*s^1/2^ || 17.7" || 6.5' ||
|| NIKA2 1 mm/260 GHz || 2x1140 || 1.15 mm || 240-280 GHz || 20 mJy*s^1/2^ || 11.2" || 6.5' ||

Comments: The half power beam widths and NEFDs are taken from [[https://arxiv.org/pdf/1707.00908.pdf|Adam et al. (2017)]] presenting results from the commissioning. The NEFDs are average values, extrapolated to a sky opacity of 0, as measured in the February 2017 commissioning run. <5-July-2017>

== 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/Continuum/NIKA2/Main | Go to the top ]]'''

----


== 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. <5-Jul-2017>

 * Source list
   * [[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

'''[[ 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 ]]'''
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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)
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   * 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]]
Line 53: Line 115:
   * Adam et al. 2017, '''Mapping the hot gas temperature in galaxy clusters using X-ray and Sunyaev-Zel'dovich imaging''', A&A, subm. [[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]]
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   * ''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]]
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'''[[ http://www.iram.es/IRAMES/mainWiki/Continuum/NIKA2/Main | Go to the top ]]'''
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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 ]]
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 * [[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)]]
Line 78: Line 159:
   * [[http://www.iram.es/IRAMES/mainWiki/Continuum/NetworkAccess | Remote network access to NIKA-2 ]]

   * [[http://www.iram.es/IRAMES/mainWiki/Continuum/PoolPreparation | Pool Preparation]] 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/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.
Line 92: Line 173:
## == Open runs ==
##
## === 1st NIKA2 pool (coming soon) ===		 == Open runs ==
##
=== 1st NIKA2 pool (coming soon) ===
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== Technical runs to commission NIKA2 == == Commissioning runs ==

=== Phase I (October 2015 - April 2017) ===
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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]
  * [[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 (degraded during run 5 intervention), 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]]

=== Phase II (June 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]
  * [[Nika2Run11|Go to the 11th run Wiki page]]
Line 138: Line 242:
  * '''Alain Benoit''' <alain.benoit@grenoble.cnrs.fr> (PI, IN)
 * '''Alessandro Monfardini''' <monfardini@neel.cnrs.fr> (co-PI, IN)
  * François-Xavier Désert <francois-xavier.desert@obs.ujf-grenoble.fr> (IPAG)		   * '''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)
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  * Nicolas Ponthieu (IPAG)   * Nicolas Ponthieu <nicolas.ponthieu@univ-grenoble-alpes.fr> (IPAG)
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  * Remi Adam <adam@lpsc.in2p3.fr> (LPSC)
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  * Carsten Kramer (Station Manager and 30m Scheduler, <kramer@iram.es>)
  * Pablo Garcia (30m Continuum Pool Manager, <pgarcia@iram.es>)
  * Albrecht Sievers (IMBfits, <sievers@iram.es>)
  * Hans Ungerechte (NCS/pako, <ungerechts@iram.es>)
  * Pablo Mellado (Computers/Network, <mellado@iram.es>)		   * Carsten Kramer (30m Station Manager and Scheduler, <kramer@iram.es>)
  * Alessia Ritacco (commissioning of polarization capabilities, <ritaccoa@iram.es>)
  * Albrecht Sievers (IMBfits/Data, <sievers@iram.es>)
  * Hans Ungerechts (NCS/pako, <ungerechts@iram.es>)
  * Pablo Mellado, Francesco Pierfederici (Computers/Network, <mellado@iram.es>, <fpierfed@iram.es>)
  * Santiago Navarro, Dave John (Cryostat, <john@ira.es>, <navarro@iram.es>)

 * IRAM/Grenoble NIKA2 support team:
  * Samuel Leclercq (Coordinator, Optics <leclercq@iram.fr>)
  * Robert Zylka (Data Processing Software, <zylka@iram.fr>)
  * Charles Romero (Commissioning, <romero@iram.fr>)
  * Eduard Driessen (Detectors, <driessen@iram.fr>)
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Author: Israel Hermelo
Created: 2015.AUG.05
This page is maintained by PG, CK, SL and the NIKA team
Last update: 29-Jul-2016
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 is built by an international consortium, led by the Institute Neel (Grenoble France).

Contents

  1. NIKA2 Homepage
    1. Overview
    2. Call for proposals and time estimator for winter 2017/18
    3. Open Time Programs
    4. The five Guaranteed Time Large Programs
      1. Phase I
      2. Phase II
    5. Publications
    6. Technical Documentation
    7. Open runs
      1. 1st NIKA2 pool (coming soon)
    8. Commissioning runs
      1. Phase I (October 2015 - April 2017)
      2. Phase II (June 2017)
    9. 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

6 mJy*s1/2

17.7"

6.5'

NIKA2 1 mm/260 GHz

2x1140

1.15 mm

240-280 GHz

20 mJy*s1/2

11.2"

6.5'

Comments: The half power beam widths and NEFDs are taken from Adam et al. (2017) presenting results from the commissioning. The NEFDs are average values, extrapolated to a sky opacity of 0, as measured in the February 2017 commissioning run. <5-July-2017>

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 call for proposals when it becomes available in August. The time estimator and an accompanying document has been updated here, accounting for the commissioning results described in Adam et al..

Open Time Programs

Summer semester 2017

Go to the top

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. <5-Jul-2017>

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.

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

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

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

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

Go to the top

Publications

  • Adam et al. 2017, The NIKA2 large field-of-view millimeter continuum camera for the 30-m IRAM telescope, arxiv (accepted for publication on A&A, Jul-2017)

  • 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

    • 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, subm. 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. 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

    • 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:
  • Talks:

  • NIKA2 publications list maintained at IPAG

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Technical Documentation

Open runs

1st NIKA2 pool (coming soon)

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Commissioning runs

Phase I (October 2015 - April 2017)

  • 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 (degraded during run 5 intervention), 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]

Phase II (June 2017)

  • 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

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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)