Performance and calibration of the NIKA camera at the IRAM 30 m telescope

Catalano, A.; Calvo, M.; Ponthieu, N.; Adam, R.; Adane, A.; Ade, Peter A. R.; André, Ph.; Beelen, A.; Bélier, B.; Benoı̂t, A.; Bideaud, A.; Billot, N.; Boudou, Nicolas; Bourrion, O.; Coiffard, G.; Comis, B.; D'Addabbo, A.; Désert, F.-X.; Doyle, S.; Goupy, J.; Krämer, C.; Leclercq, S.; Macías-Pérez, J. F.; Martino, J. Rodrı́guez; Mauskopf, Philip Daniel; Mayet, F.; Monfardini, A.; Pajot, F.; Pascale, Enzo; Perotto, L.; Revéret, V.; Rodriguez, L.; Savini, G.; Schuster, K.; Sievers, A.; Tucker, C.; Zylka, R.

doi:10.1051/0004-6361/201423557

Cited by 70 publications

(123 citation statements)

References 41 publications

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“…The observations were carried out using the IRAM 30 m telescope, located at Pico Veleta (Spain), during the spring of 2014, using the New IRAM KID Array (NIKA) (Catalano et al 2014;Calvo et al 2013). The project number is 151-13.…”

Section: Nikamentioning

confidence: 99%

Search for grain growth toward the center of L1544

Chacón-Tanarro

Caselli

Bizzocchi

et al. 2017

A&A

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In dense and cold molecular clouds dust grains are surrounded by thick icy mantles. It is however not clear if dust growth and coagulation take place before the switch-on of a protostar. This is an important issue, as the presence of large grains may affect the chemical structure of dense cloud cores, including the dynamically important ionization fraction, and the future evolution of solids in protoplanetary disks. To study this further, we focus on L1544, one of the most centrally concentrated pre-stellar cores on the verge of star formation, and with a well-known physical structure. We observed L1544 at 1.2 and 2 mm using NIKA, a new receiver at the IRAM 30 m telescope, and we used data from the Herschel Space Observatory archive. We find no evidence of grain growth towards the center of L1544 at the available angular resolution. Therefore, we conclude that single dish observations do not allow us to investigate grain growth toward the pre-stellar core L1544 and high sensitivity interferometer observations are needed. We predict that dust grains can grow to 200 µm in size toward the central ∼300 au of L1544. This will imply a dust opacity change by a factor of ∼2.5 at 1.2 mm, which can be detected using the Atacama Large Millimeter and submillimeter Array (ALMA) at different wavelengths and with an angular resolution of 2 .

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Section: Nikamentioning

confidence: 99%

Search for grain growth toward the center of L1544

Chacón-Tanarro

Caselli

Bizzocchi

et al. 2017

A&A

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“…The effective FWHM was measured to be 18.2 and 12.0 arcsec at 150 and 260 GHz, respectively, by fitting a Gaussian model on the planet. The opacity was measured and corrected for by using NIKA total power data as a tau-meter as described in Catalano et al (2014). The Compton y to surface brightness (measured in Jy/beam) conversions were computed by integrating the tSZ spectrum (see Sect.…”

Section: Observations Of CL J12269+3332mentioning

confidence: 99%

“…The details of the NIKA data reduction are available in Adam et al (2014) and Catalano et al (2014). Here, the main procedure is briefly summarized for the reader's convenience.…”

Section: Data Reductionmentioning

confidence: 99%

“…In this paper, we report 150 and 260 GHz tSZ observations of CL J1226.9+3332, using the New IRAM KIDs Array (NIKA, see Monfardini et al 2010Monfardini et al , 2011Bourrion et al 2011;Calvo et al 2013;Adam et al 2014;Catalano et al 2014, for more details on the NIKA camera) at the IRAM (Institut de Radio Astronomie Millimétrique) 30-m telescope. The reconstructed tSZ map of the cluster is used to constrain its pressure distribution, as well as the thermodynamics of the ICM gas by combining it with X-ray data.…”

Section: Introductionmentioning

confidence: 99%

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Pressure distribution of the high-redshift cluster of galaxies CL J1226.9+3332 with NIKA

Adam

Comis

Macías-Pérez

et al. 2015

A&A

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The thermal Sunyaev-Zel'dovich (tSZ) effect is expected to provide a low scatter mass proxy for galaxy clusters since it is directly proportional to the cluster thermal energy. The tSZ observations have proven to be a powerful tool for detecting and studying them, but high angular resolution observations are now needed to push their investigation to a higher redshift. In this paper, we report high angular (<20 arcsec) resolution tSZ observations of the high-redshift cluster CL J1226.9+3332 (z = 0.89). It was imaged at 150 and 260 GHz using the NIKA camera at the IRAM 30-m telescope. The 150 GHz map shows that CL J1226.9+3332 is morphologically relaxed on large scales with evidence of a disturbed core, while the 260 GHz channel is used mostly to identify point source contamination. NIKA data are combined with those of Planck and X-ray from Chandra to infer the cluster's radial pressure, density, temperature, and entropy distributions. The total mass profile of the cluster is derived, and we find M 500 = 5.96 +1.02 −0.79 × 10 14 M within the radius R 500 = 930 +50 −43 kpc, at a 68% confidence level. (R 500 is the radius within which the average density is 500 times the critical density at the cluster's redshift.) NIKA is the prototype camera of NIKA2, a KIDs (kinetic inductance detectors) based instrument to be installed at the end of 2015. This work is, therefore, part of a pilot study aiming at optimizing tSZ NIKA2 large programs.

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“…NIKA is a dual-band camera operating with frequency-multiplexed arrays of lumped element kinetic inductance detectors (LEKIDs) that are based on aluminium (Al) films and are cooled at 100 mK (Monfardini et al 2011). The NIKA instrument exhibits very high sensitivity in the 120-300 GHz band range (Catalano et al 2014). A&A 580, A15 (2015) The frequency range below 120 GHz is not accessible using the NIKA Al films because of the superconducting gap cut-off.…”

Section: Introductionmentioning

confidence: 99%

Bi-layer kinetic inductance detectors for space observations between 80–120 GHz

Catalano

Goupy

Sueur

et al. 2015

A&A

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We have developed lumped element kinetic inductance detectors (LEKIDs) that are sensitive in the frequency band from 80 to 120 GHz. In this work, we take advantage of the so-called proximity effect to reduce the superconducting gap of aluminium (Al), otherwise strongly suppressing the LEKID response for frequencies smaller than 100 GHz. We designed, produced, and optically tested various fully multiplexed arrays based on multi-layer combinations of Al and titanium (Ti). Their sensitivities were measured using a dedicated closed-circle 100 mK dilution cryostat and a sky simulator, which allowed us to reproduce realistic observation conditions. The spectral response was characterised with a Martin-Puplett interferometer up to THz frequencies and had a resolution of 3 GHz. We demonstrate that Ti-Al LEKID can reach an optical sensitivity of about 1.4 × 10 −17 W/Hz 0.5 (best pixel), or 2.2 × 10 −17 W/Hz 0.5 when averaged over the whole array. The optical background was set to roughly 0.4 pW per pixel, which is typical for future space observatories in this particular band. The performance is close to a sensitivity of twice the CMB photon noise limit at 100 GHz, which drove the design of the Planck HFI instrument. This figure remains the baseline for the next generation of millimetre-wave space satellites.

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Performance and calibration of the NIKA camera at the IRAM 30 m telescope

Cited by 70 publications

References 41 publications

Search for grain growth toward the center of L1544

Search for grain growth toward the center of L1544

Pressure distribution of the high-redshift cluster of galaxies CL J1226.9+3332 with NIKA

Bi-layer kinetic inductance detectors for space observations between 80–120 GHz

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