9 research outputs found
Lumped element kinetic inductance detectors maturity for space-borne instruments in the range between 80 and 180 GHz
This work intends to give the state-of-the-art of our knowledge of the
performance of LEKIDs at millimetre wavelengths (from 80 to 180~GHz). We
evaluate their optical sensitivity under typical background conditions and
their interaction with ionising particles. Two LEKID arrays, originally
designed for ground-based applications and composed of a few hundred pixels
each, operate at a central frequency of 100, and 150~GHz (
about 0.3). Their sensitivities have been characterised in the laboratory using
a dedicated closed-circle 100~mK dilution cryostat and a sky simulator,
allowing for the reproduction of realistic, space-like observation conditions.
The impact of cosmic rays has been evaluated by exposing the LEKID arrays to
alpha particles (Am) and X sources (Cd) with a readout sampling
frequency similar to the ones used for Planck HFI (about 200~Hz), and also with
a high resolution sampling level (up to 2~MHz) in order to better characterise
and interpret the observed glitches. In parallel, we have developed an
analytical model to rescale the results to what would be observed by such a
LEKID array at the second Lagrangian point.Comment: 7 pages, 2 tables, 13 figure
LEKID sensitivity for space applications between 80 and 600 GHz
We report the design, fabrication and testing of Lumped Element Kinetic
Inductance Detectors (LEKID) showing performance in line with the requirements
of the next generation space telescopes operating in the spectral range from 80
to 600 GHz. This range is of particular interest for Cosmic Microwave
Background (CMB) studies. For this purpose we have designed and fabricated
100-pixel arrays covering five distinct bands. These wafers have been measured
via multiplexing, where a full array is read out using a single pair of lines.
We adopted a custom cold black-body installed in front of the detectors and
regulated at temperatures between 1 K and 20 K. We will describe in the present
paper the main design considerations, the fabrication processes, the testing
and the data analysis
Exploring Cosmic Origins with CORE: Cluster Science
We examine the cosmological constraints that can be achieved with a galaxycluster survey with the future CORE space mission. Using realistic simulationsof the millimeter sky, produced with the latest version of the Planck SkyModel, we characterize the CORE cluster catalogues as a function of the mainmission performance parameters. We pay particular attention to telescope size,key to improved angular resolution, and discuss the comparison and thecomplementarity of CORE with ambitious future ground-based CMB experiments thatcould be deployed in the next decade. A possible CORE mission concept with a150 cm diameter primary mirror can detect of the order of 50,000 clustersthrough the thermal Sunyaev-Zeldovich effect (SZE). The total yield increases(decreases) by 25% when increasing (decreasing) the mirror diameter by 30 cm.The 150 cm telescope configuration will detect the most massive clusters() at redshift over the whole sky, although theexact number above this redshift is tied to the uncertain evolution of thecluster SZE flux-mass relation; assuming self-similar evolution, CORE willdetect clusters at redshift . This changes to 800 (200) whenincreasing (decreasing) the mirror size by 30 cm. CORE will be able to measureindividual cluster halo masses through lensing of the cosmic microwavebackground anisotropies with a 1- sensitivity of , for a 120 cm aperture telescope, and for a 180 cmone. [abridged
Exploring cosmic origins with CORE: Survey requirements and mission design
Future observations of cosmic microwave background (CMB) polarisation have
the potential to answer some of the most fundamental questions of modern
physics and cosmology. In this paper, we list the requirements for a future CMB
polarisation survey addressing these scientific objectives, and discuss the
design drivers of the CORE space mission proposed to ESA in answer to the "M5"
call for a medium-sized mission. The rationale and options, and the
methodologies used to assess the mission's performance, are of interest to
other future CMB mission design studies. CORE is designed as a near-ultimate
CMB polarisation mission which, for optimal complementarity with ground-based
observations, will perform the observations that are known to be essential to
CMB polarisation scienceand cannot be obtained by any other means than a
dedicated space mission.Comment: 79 pages, 14 figure
The NIKA2 Instrument at 30-m IRAM Telescope: Performance and Results
The New IRAM KID Arrays 2 (NIKA2) consortium has just finished installing and commissioning a millimetre camera on the IRAM 30-m telescope. It is a dual-band camera operating with three frequency-multiplexed kilo-pixels arrays of lumped element kinetic inductance detectors (LEKID) cooled at 150 mK, designed to observe the intensity and polarisation of the sky at 260 and 150 GHz (1.15 and 2 mm). NIKA2 is today an IRAM resident instrument for millimetre astronomy, such as intracluster medium from intermediate to distant clusters and so for the follow-up of Planck satellite detected clusters, high redshift sources and quasars, early stages of star formation and nearby galaxies emission. We present an overview of the instrument performance as it has been evaluated at the end of the commissioning phase
Exploring cosmic origins with CORE: Cluster science
none121siWe examine the cosmological constraints that can be achieved with a galaxy
cluster survey with the future CORE space mission. Using realistic simulations of the millimeter sky, produced with the latest version of the Planck Sky Model, we characterize the CORE cluster catalogues as a function of the main mission performance parameters. We pay
particular attention to telescope size, key to improved angular resolution, and discuss the
comparison and the complementarity of CORE with ambitious future ground-based CMB
experiments that could be deployed in the next decade.
A possible CORE mission concept with a 150 cm diameter primary mirror can detect
of the order of 50,000 clusters through the thermal Sunyaev-Zeldovich effect (SZE). The
total yield increases (decreases) by 25% when increasing (decreasing) the mirror diameter by
30 cm. The 150 cm telescope configuration will detect the most massive clusters (> 1014 M)
at redshift z > 1.5 over the whole sky, although the exact number above this redshift is tied to
the uncertain evolution of the cluster SZE flux-mass relation; assuming self-similar evolution,
CORE will detect ⌠500 clusters at redshift z > 1.5. This changes to 800 (200) when
increasing (decreasing) the mirror size by 30 cm. CORE will be able to measure individual
cluster halo masses through lensing of the cosmic microwave background anisotropies with a
1-Ï sensitivity of 4 Ă10^14M, for a 120 cm aperture telescope, and 10^14M for a 180 cm one.
From the ground, we estimate that, for example, a survey with about 150,000 detectors
at the focus of 350 cm telescopes observing 65% of the sky would be shallower than CORE
and detect about 11,000 clusters, while a survey with the same number of detectors observing
25% of sky with a 10 m telescope is expected to be deeper and to detect about 70,000 clusters.
When combined with the latter, CORE would reach a limiting mass of M500 ⌠2â3Ă10^13M
and detect 220,000 clusters (5 sigma detection limit).
Cosmological constraints from CORE cluster counts alone are competitive with other
scheduled large scale structure surveys in the 2020âs for measuring the dark energy equationof-state parameters w0 and wa (Ï_w0 = 0.28, Ï_wa = 0.31). In combination with primary CMB constraints, CORE cluster counts can further reduce these error bars on w_0 and w_a to 0.05 and
0.13 respectively, and constrain the sum of the neutrino masses, ÎŁmÎœ, to 39 meV (1 sigma).
The wide frequency coverage of CORE, 60â600 GHz, will enable measurement of the
relativistic thermal SZE by stacking clusters. Contamination by dust emission from the
clusters, however, makes constraining the temperature of the intracluster medium difficult.
The kinetic SZE pairwise momentum will be extracted with S/N = 70 in the foregroundcleaned CMB map. Measurements of TCMB(z) using CORE clusters will establish competitive constraints on the evolution of the CMB temperature: (1 + z)^(1âÎČ)
, with an uncertaintyof Ï_ÎČ <= 2.7 Ă 10^â3 at low redshift (z <=1). The wide frequency coverage also enables
clean extraction of a map of the diffuse SZE signal over the sky, substantially reducing
contamination by foregrounds compared to the Planck SZE map extraction. Our analysis of
JCAP04(2018)019 the one-dimensional distribution of Compton-y values in the simulated map finds an order
of magnitude improvement in constraints on Ï_8 over the Planck result, demonstrating the
potential of this cosmological probe with COREnoneMelin J.-B.; Bonaldi A.; Remazeilles M.; Hagstotz S.; Diego J.M.; Hernandez-Monteagudo C.; Genova-Santos R.T.; Luzzi G.; Martins C.J.A.P.; Grandis S.; Mohr J.J.; Bartlett J.G.; Delabrouille J.; Ferraro S.; Tramonte D.; Rubino-Martin J.A.; Macias-Perez J.F.; Achucarro A.; Ade P.; Allison R.; Ashdown M.; Ballardini M.; Banday A.J.; Banerji R.; Bartolo N.; Basak S.; Basu K.; Battye R.A.; Baumann D.; Bersanelli M.; Bonato M.; Borrill J.; Bouchet F.; Boulanger F.; Brinckmann T.; Bucher M.; Burigana C.; Buzzelli A.; Cai Z.-Y.; Calvo M.; Carvalho C.S.; Castellano M.G.; Challinor A.; Chluba J.; Clesse S.; Colafrancesco S.; Colantoni I.; Coppolecchia A.; Crook M.; D'Alessandro G.; De Bernardis P.; De Gasperis G.; Petris M.D.; Zotti G.D.; Valentino E.D.; Errard J.; Feeney S.M.; Fernandez-Cobos R.; Finelli F.; Forastieri F.; Galli S.; Gerbino M.; Gonzalez-Nuevo J.; Greenslade J.; Hanany S.; Handley W.; Hervias-Caimapo C.; Hills M.; Hivon E.; Kiiveri K.; Kisner T.; Kitching T.; Kunz M.; Kurki-Suonio H.; Lamagna L.; Lasenby A.; Lattanzi M.; Brun A.M.C.L.; Lesgourgues J.; Lewis A.; Liguori M.; Lindholm V.; Lopez-Caniego M.; Maffei B.; Martinez-Gonzalez E.; Masi S.; Mazzotta P.; McCarthy D.; Melchiorri A.; Molinari D.; Monfardini A.; Natoli P.; Negrello M.; Notari A.; Paiella A.; Paoletti D.; Patanchon G.; Piat M.; Pisano G.; Polastri L.; Polenta G.; Pollo A.; Poulin V.; Quartin M.; Roman M.; Salvati L.; Tartari A.; Tomasi M.; Trappe N.; Triqueneaux S.; Trombetti T.; Tucker C.; Valiviita J.; De Weygaert R.V.; Tent B.V.; Vennin V.; Vielva P.; Vittorio N.; Weller J.; Young K.; Zannoni M.Melin, J. -B.; Bonaldi, A.; Remazeilles, M.; Hagstotz, S.; Diego, J. M.; Hernandez-Monteagudo, C.; Genova-Santos, R. T.; Luzzi, G.; Martins, C. J. A. P.; Grandis, S.; Mohr, J. J.; Bartlett, J. G.; Delabrouille, J.; Ferraro, S.; Tramonte, D.; Rubino-Martin, J. A.; Macias-Perez, J. F.; Achucarro, A.; Ade, P.; Allison, R.; Ashdown, M.; Ballardini, M.; Banday, A. J.; Banerji, R.; Bartolo, N.; Basak, S.; Basu, K.; Battye, R. A.; Baumann, D.; Bersanelli, M.; Bonato, M.; Borrill, J.; Bouchet, F.; Boulanger, F.; Brinckmann, T.; Bucher, M.; Burigana, C.; Buzzelli, A.; Cai, Z. -Y.; Calvo, M.; Carvalho, C. S.; Castellano, M. G.; Challinor, A.; Chluba, J.; Clesse, S.; Colafrancesco, S.; Colantoni, I.; Coppolecchia, A.; Crook, M.; D'Alessandro, G.; De Bernardis, P.; De Gasperis, G.; Petris, M. D.; Zotti, G. D.; Valentino, E. D.; Errard, J.; Feeney, S. M.; Fernandez-Cobos, R.; Finelli, F.; Forastieri, F.; Galli, S.; Gerbino, M.; Gonzalez-Nuevo, J.; Greenslade, J.; Hanany, S.; Handley, W.; Hervias-Caimapo, C.; Hills, M.; Hivon, E.; Kiiveri, K.; Kisner, T.; Kitching, T.; Kunz, M.; Kurki-Suonio, H.; Lamagna, L.; Lasenby, A.; Lattanzi, M.; Brun, A. M. C. L.; Lesgourgues, J.; Lewis, A.; Liguori, M.; Lindholm, V.; Lopez-Caniego, M.; Maffei, B.; Martinez-Gonzalez, E.; Masi, S.; Mazzotta, P.; Mccarthy, D.; Melchiorri, A.; Molinari, D.; Monfardini, A.; Natoli, P.; Negrello, M.; Notari, A.; Paiella, A.; Paoletti, D.; Patanchon, G.; Piat, M.; Pisano, G.; Polastri, L.; Polenta, G.; Pollo, A.; Poulin, V.; Quartin, M.; Roman, M.; Salvati, L.; Tartari, A.; Tomasi, M.; Trappe, N.; Triqueneaux, S.; Trombetti, T.; Tucker, C.; Valiviita, J.; De Weygaert, R. V.; Tent, B. V.; Vennin, V.; Vielva, P.; Vittorio, N.; Weller, J.; Young, K.; Zannoni, M
Exploring Cosmic Origins with CORE: Cluster Science
International audienceWe examine the cosmological constraints that can be achieved with a galaxy cluster survey with the future CORE space mission. Using realistic simulations of the millimeter sky, produced with the latest version of the Planck Sky Model, we characterize the CORE cluster catalogues as a function of the main mission performance parameters. We pay particular attention to telescope size, key to improved angular resolution, and discuss the comparison and the complementarity of CORE with ambitious future ground-based CMB experiments that could be deployed in the next decade. A possible CORE mission concept with a 150 cm diameter primary mirror can detect of the order of 50,000 clusters through the thermal Sunyaev-Zeldovich effect (SZE). The total yield increases (decreases) by 25% when increasing (decreasing) the mirror diameter by 30 cm. The 150 cm telescope configuration will detect the most massive clusters (>1014 M⊙) at redshift z>1.5 over the whole sky, although the exact number above this redshift is tied to the uncertain evolution of the cluster SZE flux-mass relation; assuming self-similar evolution, CORE will detect 0~ 50 clusters at redshift z>1.5. This changes to 800 (200) when increasing (decreasing) the mirror size by 30 cm. CORE will be able to measure individual cluster halo masses through lensing of the cosmic microwave background anisotropies with a 1-Ï sensitivity of 4Ă1014 M⊙, for a 120 cm aperture telescope, and 1014 M⊙ for a 180 cm one. From the ground, we estimate that, for example, a survey with about 150,000 detectors at the focus of 350 cm telescopes observing 65% of the sky would be shallower than CORE and detect about 11,000 clusters, while a survey with the same number of detectors observing 25% of sky with a 10 m telescope is expected to be deeper and to detect about 70,000 clusters. When combined with the latter, CORE would reach a limiting mass of M500 ~ 2â3 Ă 1013 M⊙ and detect 220,000 clusters (5 sigma detection limit). Cosmological constraints from CORE cluster counts alone are competitive with other scheduled large scale structure surveys in the 2020's for measuring the dark energy equation-of-state parameters w0 and wa (Ïw0=0.28, Ïwa=0.31). In combination with primary CMB constraints, CORE cluster counts can further reduce these error bars on w0 and wa to 0.05 and 0.13 respectively, and constrain the sum of the neutrino masses, ÎŁÂ mÎœ, to 39 meV (1 sigma). The wide frequency coverage of CORE, 60â600 GHz, will enable measurement of the relativistic thermal SZE by stacking clusters. Contamination by dust emission from the clusters, however, makes constraining the temperature of the intracluster medium difficult. The kinetic SZE pairwise momentum will be extracted with 0S/N=7 in the foreground-cleaned CMB map. Measurements of TCMB(z) using CORE clusters will establish competitive constraints on the evolution of the CMB temperature: (1+z)1âÎČ, with an uncertainty of ÏÎČ  2.7Ă 10â3 at low redshift (z  1). The wide frequency coverage also enables clean extraction of a map of the diffuse SZE signal over the sky, substantially reducing contamination by foregrounds compared to the Planck SZE map extraction. Our analysis of the one-dimensional distribution of Compton-y values in the simulated map finds an order of magnitude improvement in constraints on Ï8 over the Planck result, demonstrating the potential of this cosmological probe with CORE