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51. Frequentist Estimation of Cosmological Parameters from the MAXIMA-1 Cosmic Microwave Background Anisotropy Data

Author: Abroe, M. E., Balbi, A., Borrill, J., Bunn, E. F., Ferreira, P. G., Hanany, S., Jaffe, A. H., Lee, A. T., Olive, K. A., Rabii, B., Richards, P. L., Smoot, G. F., Stompor, R., Winant, C. D., and Wu, J. H. P.
Subjects: Astrophysics
Abstract: We use a frequentist statistical approach to set confidence intervals on the values of cosmological parameters using the MAXIMA-1 and COBE measurements of the angular power spectrum of the cosmic microwave background. We define a $\Delta \chi^{2}$ statistic, simulate the measurements of MAXIMA-1 and COBE, determine the probability distribution of the statistic, and use it and the data to set confidence intervals on several cosmological parameters. We compare the frequentist confidence intervals to Bayesian credible regions. The frequentist and Bayesian approaches give best estimates for the parameters that agree within 15%, and confidence interval-widths that agree within 30%. The results also suggest that a frequentist analysis gives slightly broader confidence intervals than a Bayesian analysis. The frequentist analysis gives values of \Omega=0.89{+0.26\atop -0.19}, \Omega_{\rm B}h^2=0.026{+0.020\atop -0.011} and n=1.02{+0.31\atop -0.10}, and the Bayesian analysis gives values of \Omega=0.98{+0.14\atop -0.19}, \Omega_{\rm B}h^2=0.0.029{+0.015\atop-0.010}, and $n=1.18{+0.10\atop -0.23}$, all at the 95% confidence level., Comment: 10 pages, 9 Postscript figures, changes made to reflect published version
Published: 2001
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52. Estimate of the Cosmological Bispectrum from the MAXIMA-1 Cosmic Microwave Background Map

Author: Santos, M. G., Balbi, A., Borrill, J., Ferreira, P. G., Hanany, S., Jaffe, A. H., Lee, A. T., Magueijo, J., Rabii, B., Richards, P. L., Smoot, G. F., Stompor, R., Winant, C. D., and Wu, J. H. P.
Subjects: Astrophysics, High Energy Physics - Phenomenology
Abstract: We use the measurement of the cosmic microwave background taken during the MAXIMA-1 flight to estimate the bispectrum of cosmological perturbations. We propose an estimator for the bispectrum that is appropriate in the flat sky approximation, apply it to the MAXIMA-1 data and evaluate errors using bootstrap methods. We compare the estimated value with what would be expected if the sky signal were Gaussian and find that it is indeed consistent, with a $\chi^2$ per degree of freedom of approximately unity. This measurement places constraints on models of inflation., Comment: 5 pages, 2 figures. New version to match paper accepted for publication in Phys. Rev. Lett. Non-diagonal terms included leading to new limits on f_NL
Published: 2001
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53. Making Maps Of The Cosmic Microwave Background: The MAXIMA Example

Author: Stompor, R., Balbi, A., Borrill, J. D., Ferreira, P. G., Hanany, S., Jaffe, A. H., Lee, A. T., Oh, S., Rabii, B., Richards, P. L., Smoot, G. F., Winant, C. D., and Wu, J. -H. P.
Subjects: Astrophysics
Abstract: This work describes Cosmic Microwave Background (CMB) data analysis algorithms and their implementations, developed to produce a pixelized map of the sky and a corresponding pixel-pixel noise correlation matrix from time ordered data for a CMB mapping experiment. We discuss in turn algorithms for estimating noise properties from the time ordered data, techniques for manipulating the time ordered data, and a number of variants of the maximum likelihood map-making procedure. We pay particular attention to issues pertinent to real CMB data, and present ways of incorporating them within the framework of maximum likelihood map-making. Making a map of the sky is shown to be not only an intermediate step rendering an image of the sky, but also an important diagnostic stage, when tests for and/or removal of systematic effects can efficiently be performed. The case under study is the MAXIMA data set. However, the methods discussed are expected to be applicable to the analysis of other current and forthcoming CMB experiments., Comment: Replaced to match the published version, only minor changes
Published: 2001
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54. Cosmological implications of the MAXIMA-I high resolution Cosmic Microwave Background anisotropy measurement

Author: Stompor, R., Abroe, M., Ade, P., Balbi, A., Barbosa, D., Bock, J., Borrill, J., Boscaleri, A., De Bernardis, P., Ferreira, P. G., Hanany, S., Hristov, V., Jaffe, A. H., Lee, A. T., Pascale, E., Rabii, B., Richards, P. L., Smoot, G. F., Winant, C. D., and Wu, J. H. P.
Subjects: Astrophysics, High Energy Physics - Phenomenology
Abstract: We discuss the cosmological implications of the new constraints on the power spectrum of the Cosmic Microwave Background Anisotropy derived from a new high resolution analysis of the MAXIMA-1 measurement (Lee et al. 2001). The power spectrum shows excess power at $\ell \sim 860$ over the average level of power at $411 \le\ell \le 785.$ This excess is statistically significant on the 95% confidence level. Such a feature is consistent with the presence of a third acoustic peak, which is a generic prediction of inflation-based models. The height and the position of the excess power match the predictions of a family of inflationary models with cosmological parameters that are fixed to fit the CMB data previously provided by BOOMERANG-LDB and MAXIMA-1 experiments (e.g., Jaffe et al.2001). Our results, therefore, lend support for inflationary models and more generally for the dominance of coherent perturbations in the structure formation of the Universe. At the same time, they seem to disfavor a large variety of the non-standard (but still inflation-based) models that have been proposed to improve the quality of fits to the CMB data and consistency with other cosmological observables. Within standard inflationary models, our results combined with the COBE-DMR data give best fit values and 95% confidence limits for the baryon density, $\Omega_b h^2\simeq 0.033{\pm 0.013}$, and the total density, $\Omega=0.9{+0.18\atop -0.16}$. The primordial spectrum slope ($n_s$) and the optical depth to the last scattering surface ($\tau_c$) are found to be degenerate and to obey the relation $n_s \simeq 0.46 \tau_c + (0.99 \pm 0.14)$, for $\tau_c \le 0.5$ (all 95% c.l.)., Comment: Replaced to match a published version
Published: 2001
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55. A High Spatial Resolution Analysis of the MAXIMA-1 Cosmic Microwave Background Anisotropy Data

Author: Lee, A. T., Ade, P., Balbi, A., Bock, J., Borrill, J., Boscaleri, A., De Bernardis, P., Ferreira, P. G., Hanany, S., Hristov, V. V., Jaffe, A. H., Mauskopf, P. D., Netterfield, C. B., Pascale, E., Rabii, B., Richards, P. L., Smoot, G. F., Stompor, R., Winant, C. D., and Wu, J. H. P.
Subjects: Astrophysics
Abstract: We extend the analysis of the MAXIMA-1 cosmic microwave background (CMB) data to smaller angular scales. MAXIMA, a bolometric balloon experiment, mapped a 124 deg$^2$ region of the sky with 10\arcmin resolution at frequencies of 150, 240 and 410 GHz during its first flight. The original analysis, which covered the multipole range $36 \leq \ell \leq 785$, is extended to $\ell = 1235$ using data from three 150 GHz photometers in the fully cross-linked central 60 deg$^2$ of the map. The main improvement over the original analysis is the use of 3\arcmin square pixels in the calculation of the map. The new analysis is consistent with the original for $\ell < 785$. For $\ell > 785$, where inflationary models predict a third acoustic peak, the new analysis shows power with an amplitude of $56 \pm 7$ \microk at $\ell \simeq 850$ in excess to the average power of $42 \pm 3$ \microk in the range $441 < \ell < 785$.
Published: 2001
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56. Tests for Gaussianity of the MAXIMA-1 CMB Map

Author: Wu, J. H. P., Balbi, A., Borrill, J., Ferreira, P. G., Hanany, S., Jaffe, A. H., Lee, A. T., Rabii, B., Richards, P. L., Smoot, G. F., Stompor, R., and Winant, C. D.
Subjects: Astrophysics
Abstract: Gaussianity of the cosmological perturbations in the universe is one of the key predictions of standard inflation, but it is violated by other models of structure formation such as topological defects. We present the first test of the Gaussianity of the cosmic microwave background (CMB) on sub-degree angular scales, where deviations from Gaussianity are most likely to occur. We apply the methods of moments, cumulants, the Kolmogorov test, the $\chi^2$ test, and Minkowski functionals in eigen, real, Wiener-filtered and signal-whitened spaces, to the MAXIMA-1 CMB anisotropy data. We conclude that the data, which probe angular scales between 10 arcminutes and 5 degrees, are consistent with Gaussianity., Comment: 5 pages, 6 figures, (PRL, in press (2001))
Published: 2001
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57. From the time-ordered data to the Maximum-Likelihood temperature maps of the Cosmic Microwave Backgorund anisotropy

Author: Stompor, R., Balbi, A., Borrill, J., Ferreira, P., Hanany, S., Jaffe, A., Lee, A., Oh, S., Rabii, B., Richards, P., Smoot, G., Winant, C., and Wu, J. -H. P.
Subjects: Astrophysics
Abstract: We review selected methods of the Cosmic Microwave Background data analysis appropriate for the analysis of the largest currently available data sets. We focus on techniques of the time-ordered data manipulation and map making algorithms based on the maximum-likelihood approach. The presented methods have been applied to the MAXIMA data analysis (Hanany et al 2000) and the description of the algorithms is illustrated with the examples drawn from that experience. The more extensive presentation of the here-mentioned issues will be given in the forthcoming paper (Stompor et al 2001)., Comment: 7 pages, no figures, uses eso.sty, to appear in Mining the Sky, ESO Astrophysics Symposia Series
Published: 2000

58. CMB Analysis of Boomerang & Maxima & the Cosmic Parameters {Omega_tot,Omega_b h^2,Omega_cdm h^2,Omega_Lambda,n_s}

Author: Bond, J. R., Ade, P., Balbi, A., Bock, J., Borrill, J., Boscaleri, A., Coble, K., Crill, B., de Bernardis, P., Farese, P., Ferreira, P., Ganga, K., Giacometti, M., Hanany, S., Hivon, E., Hristov, V., Iacoangeli, A., Jaffe, A., Lange, A., Lee, A., Martinis, L., Masi, S., Mauskopf, P., Melchiorri, A., Montroy, T., Netterfield, B., Oh, S., Pascale, E., Piacentini, F., Pogosyan, D., Prunet, S., Rabii, B., Rao, S., Richards, P., Romeo, G., Ruhl, J., Scaramuzzi, F., Sforna, D., Sigurdson, K., Smoot, G., Stompor, R., Winant, C., and Wu, P.
Subjects: Astrophysics
Abstract: We show how estimates of parameters characterizing inflation-based theories of structure formation localized over the past year when large scale structure (LSS) information from galaxy and cluster surveys was combined with the rapidly developing cosmic microwave background (CMB) data, especially from the recent Boomerang and Maxima balloon experiments. All current CMB data plus a relatively weak prior probability on the Hubble constant, age and LSS points to little mean curvature (Omega_{tot} = 1.08\pm 0.06) and nearly scale invariant initial fluctuations (n_s =1.03\pm 0.08), both predictions of (non-baroque) inflation theory. We emphasize the role that degeneracy among parameters in the L_{pk} = 212\pm 7 position of the (first acoustic) peak plays in defining the $\Omega_{tot}$ range upon marginalization over other variables. Though the CDM density is in the expected range (\Omega_{cdm}h^2=0.17\pm 0.02), the baryon density Omega_bh^2=0.030\pm 0.005 is somewhat above the independent 0.019\pm 0.002 nucleosynthesis estimate. CMB+LSS gives independent evidence for dark energy (Omega_\Lambda=0.66\pm 0.06) at the same level as from supernova (SN1) observations, with a phenomenological quintessence equation of state limited by SN1+CMB+LSS to w_Q<-0.7 cf. the w_Q=-1 cosmological constant case., Comment: 11 pages, 3 figs., in Proc. IAU Symposium 201 (PASP), CITA-2000-65
Published: 2000

59. The Cosmic Background Radiation circa nu2K

Author: Bond, J. R., Pogosyan, D., Prunet, S., collaboration, the MaxiBoom, Ade, P., Balbi, A., Bock, J., Borrill, J., Boscaleri, A., Coble, K., Crill, B., de Bernardis, P., Farese, P., Ferreira, P., Ganga, K., Giacometti, M., Hanany, S., Hivon, E., Hristov, V., Iacoangeli, A., Jaffe, A., Lange, A., Lee, A., Martinis, L., Masi, S., Mauskopf, P., Melchiorri, A., Montroy, T., Netterfield, B., Oh, S., Pascale, E., Piacentini, F., Rabii, B., Rao, S., Richards, P., Romeo, G., Ruhl, J., Scaramuzzi, F., Sforna, D., Smoot, G., Stompor, R., Winant, C., and Wu, P.
Subjects: Astrophysics
Abstract: We describe the implications of cosmic microwave background (CMB) observations and galaxy and cluster surveys of large scale structure (LSS) for theories of cosmic structure formation, especially emphasizing the recent Boomerang and Maxima CMB balloon experiments. The inflation-based cosmic structure formation paradigm we have been operating with for two decades has never been in better shape. Here we primarily focus on a simplified inflation parameter set, {omega_b,omega_{cdm},Omega_{tot}, Omega_\Lambda,n_s,\tau_C, \sigma_8}. Combining all of the current CMB+LSS data points to the remarkable conclusion that the local Hubble patch we can access has little mean curvature (Omega_{tot}=1.08\pm 0.06) and the initial fluctuations were nearly scale invariant (n_s=1.03\pm 0.08), both predictions of (non-baroque) inflation theory. The baryon density is found to be slightly larger than that preferred by independent Big Bang Nucleosynthesis estimates (omega_b=0.030\pm 0.005 cf. 0.019\pm 0.002). The CDM density is in the expected range (omega_{cdm}=0.17 \pm 0.02). Even stranger is the CMB+LSS evidence that the density of the universe is dominated by unclustered energy akin to the cosmological constant (Omega_\Lambda=0.66\pm 0.06), at the same level as that inferred from high redshift supernova observations. We also sketch the CMB+LSS implications for massive neutrinos., Comment: 7 pages, 4 figs., in Proc. Neutrino 2000 (Elsevier), CITA-2000-63
Published: 2000
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60. The Quintessential CMB, Past & Future

Author: Bond, J. R., Pogosyan, D., Prunet, S., Sigurdson, K., collaboration, the MaxiBoom, Ade, P., Balbi, A., Bock, J., Borrill, J., Boscaleri, A., Coble, K., Crill, B., de Bernardis, P., Farese, P., Ferreira, P., Ganga, K., Giacometti, M., Hanany, S., Hivon, E., Hristov, V., Iacoangeli, A., Jaffe, A., Lange, A., Lee, A., Martinis, L., Masi, S., Mauskopf, P., Melchiorri, A., Montroy, T., Netterfield, B., Oh, S., Pascale, E., Piacentini, F., Rabii, B., Rao, S., Richards, P., Romeo, G., Ruhl, J., Scaramuzzi, F., Sforna, D., Smoot, G., Stompor, R., Winant, C., and Wu, P.
Subjects: Astrophysics
Abstract: The past, present and future of cosmic microwave background (CMB) anisotropy research is discussed, with emphasis on the Boomerang and Maxima balloon experiments. These data are combined with large scale structure (LSS) information and high redshift supernova (SN1) observations to explore the inflation-based cosmic structure formation paradigm. Here we primarily focus on a simplified inflation parameter set, {omega_b,omega_{cdm},Omega_{tot}, Omega_Q,w_Q, n_s,tau_C, sigma_8}. After marginalizing over the other cosmic and experimental variables, we find the current CMB+LSS+SN1 data gives Omega_{tot}=1.04\pm 0.05, consistent with (non-baroque) inflation theory. Restricting to Omega_{tot}=1, we find a nearly scale invariant spectrum, n_s =1.03 \pm 0.07. The CDM density, omega_{cdm}=0.17\pm 0.02, is in the expected range, but the baryon density, omega_b=0.030\pm 0.004, is slightly larger than the current nucleosynthesis estimate. Substantial dark energy is inferred, Omega_Q\approx 0.68\pm 0.05, and CMB+LSS Omega_Q values are compatible with the independent SN1 estimates. The dark energy equation of state, parameterized by a quintessence-field pressure-to-density ratio w_Q, is not well determined by CMB+LSS (w_Q<-0.3 at 95%CL), but when combined with SN1 the resulting w_Q<-0.7 limit is quite consistent with the w_Q=-1 cosmological constant case. Though forecasts of statistical errors on parameters for current and future experiments are rosy, rooting out systematic errors will define the true progress., Comment: 14 pages, 3 figs., in Proc. CAPP-2000 (AIP), CITA-2000-64
Published: 2000
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61. Cosmology from Maxima-1, Boomerang and COBE/DMR CMB Observations

Author: Jaffe, A. H., Ade, P. A. R., Balbi, A., Bock, J. J, Bond, J. R., Borrill, J., Boscaleri, A., Coble, K., Crill, B. P., de Bernardis, P., Farese, P., Ferreira, P. G., Ganga, K., Giacometti, M., Hanany, S., Hivon, E., Hristov, V. V., Iacoangeli, A., Lange, A. E., Lee, A. T., Martinis, L., Masi, S., Mauskopf, P. D., Melchiorri, A., Montroy, T., Netterfield, C. B., Oh, S., Pascale, E., Piacentini, F., Pogosyan, D., Prunet, S., Rabii, B., Rao, S., Richards, P. L., Romeo, G., Ruhl, J. E., Scaramuzzi, F., Sforna, D., Smoot, G. F., Stompor, R., Winant, C. D., and Wu, J. H. P.
Subjects: Astrophysics
Abstract: Recent results from BOOMERANG-98 and MAXIMA-1, taken together with COBE-DMR, provide consistent and high signal-to-noise measurements of the CMB power spectrum at spherical harmonic multipole bands over $2<\ell\lta800$. Analysis of the combined data yields 68% (95%) confidence limits on the total density, $\Omega_{\rm {tot}}\simeq 1.11 \pm 0.07 (^{+0.13}_{-0.12})$, the baryon density, $\Omega_b h^2\simeq 0.032^{+0.005}_{-0.004} (^{+0.009}_{-0.008})$, and the scalar spectral tilt, $n_s\simeq1.01^{+0.09}_{-0.07} (^{+0.17}_{-0.14})$. These data are consistent with inflationary initial conditions for structure formation. Taken together with other cosmological observations, they imply the existence of both non-baryonic dark matter and dark energy in the universe., Comment: 5 Pages, 2 Figures, Changes to match published version
Published: 2000
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62. Asymmetric Beams in Cosmic Microwave Background Anisotropy Experiments

Author: Wu, J. H. P., Balbi, A., Borrill, J., Ferreira, P. G., Hanany, S., Jaffe, A. H., Lee, A. T., Oh, S., Rabii, B., Richards, P. L., Smoot, G. F., Stompor, R., and Winant, C. D.
Subjects: Astrophysics
Abstract: We propose a new formalism to handle asymmetric beams in the data analysis of cosmic microwave background anisotropy experiments. For any beam shape, the formalism finds the optimal circularly symmetric equivalent and is thus easily adaptable to existing data analysis methods. We demonstrate certain key points by using a simulated highly elliptic beam, and the beams and data of the MAXIMA-1 experiment, where the asymmetry is mild. In particular, we show that in both cases the formalism does not bias the angular power spectrum estimates. We analyze the limitations of the formalism and find that it is well suited for most practical situations., Comment: 41 pages, 13 figures; ApJS in press
Published: 2000
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63. Constraints on Cosmological Parameters from MAXIMA-1

Author: Balbi, A., Ade, P., Bock, J., Borrill, J., Boscaleri, A., de Bernardis, P., Ferreira, P. G., Hanany, S., Hristov, V. V., Jaffe, A. H., Lee, A. T., Oh, S., Pascale, E., Rabii, B., Richards, P. L., Smoot, G. F., Stompor, R., Winant, C. D., and Wu, J. H. P.
Subjects: Astrophysics
Abstract: We set new constraints on a seven-dimensional space of cosmological parameters within the class of inflationary adiabatic models. We use the angular power spectrum of the cosmic microwave background measured over a wide range of \ell in the first flight of the MAXIMA balloon-borne experiment (MAXIMA-1) and the low \ell results from COBE/DMR. We find constraints on the total energy density of the universe, \Omega=1.0^{+0.15}_{-0.30}, the physical density of baryons, \Omega_{b}h^2=0.03 +/- 0.01, the physical density of cold dark matter, \Omega_{cdm}h^2=0.2^{+0.2}_{-0.1}$, and the spectral index of primordial scalar fluctuations, n_s=1.08+/-0.1, all at the 95% confidence level. By combining our results with measurements of high-redshift supernovae we constrain the value of the cosmological constant and the fractional amount of pressureless matter in the universe to 0.45<\Omega_\Lambda<0.75 and 0.25<\Omega_{m}<0.50, at the 95% confidence level. Our results are consistent with a flat universe and the shape parameter deduced from large scale structure, and in marginal agreement with the baryon density from big bang nucleosynthesis., Comment: 4 pages, 4 figures. Reflects version published on ApJ Letters. Includes erratum (1 page, 2 figures) as published on ApJ Letters
Published: 2000
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64. MAXIMA-1: A Measurement of the Cosmic Microwave Background Anisotropy on angular scales of 10 arcminutes to 5 degrees

Author: Hanany, S., Ade, P., Balbi, A., Bock, J., Borrill, J., Boscaleri, A., de Bernardis, P., Ferreira, P. G., Hristov, V. V., Jaffe, A. H., Lange, A. E., Lee, A. T., Mauskopf, P. D., Netterfield, C. B., Oh, S., Pascale, E., Rabii, B., Richards, P. L., Smoot, G. F., Stompor, R., Winant, C. D., and Wu, J. H. P.
Subjects: Astrophysics
Abstract: We present a map and an angular power spectrum of the anisotropy of the cosmic microwave background (CMB) from the first flight of MAXIMA. MAXIMA is a balloon-borne experiment with an array of 16 bolometric photometers operated at 100 mK. MAXIMA observed a 124 square degrees region of the sky with 10 arcminute resolution at frequencies of 150, 240 and 410 GHz. The data were calibrated using in-flight measurements of the CMB dipole anisotropy. A map of the CMB anisotropy was produced from three 150 and one 240 GHz photometer without need for foreground subtractions. Analysis of this CMB map yields a power spectrum for the CMB anisotropy over the range 36 < l < 785. The spectrum shows a peak with an amplitude of 78 +/- 6 micro-Kelvin at l ~ 220 and an amplitude varying between ~40 micro-Kelvin and ~50 micro-Kelvin for 400 < l < 785., Comment: Reflects version accepted for publication in Ap J Letters
Published: 2000
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65. Measurement of a Peak in the Cosmic Microwave Background Power Spectrum from the North American test flight of BOOMERANG

Author: Mauskopf, P. D., Ade, P. A. R., de Bernardis, P., Bock, J. J., Borrill, J., Boscaleri, A., Crill, B. P., DeGasperis, G., De Troia, G., Farese, P., Ferreira, P. G., Ganga, K., Giacometti, M., Hanany, S., Hristov, V. V., Iacoangeli, A., Jaffe, A. H., Lange, A. E., Lee, A. T., Masi, S., Melchiorri, A., Melchiorri, F., Miglio, L., Montroy, T., Netterfield, C. B., Pascale, E., Piacentini, F., Richards, P. L., Romeo, G., Ruhl, J. E., Scannapieco, E., Scaramuzzi, F., Stompor, R., and Vittorio, N.
Subjects: Astrophysics, General Relativity and Quantum Cosmology, High Energy Physics - Experiment
Abstract: We describe a measurement of the angular power spectrum of anisotropies in the Cosmic Microwave Background (CMB) from 0.3 degrees to ~10 degrees from the North American test flight of the BOOMERANG experiment. BOOMERANG is a balloon-borne telescope with a bolometric receiver designed to map CMB anisotropies on a Long Duration Balloon flight. During a 6-hour test flight of a prototype system in 1997, we mapped > 200 square degrees at high galactic latitudes in two bands centered at 90 and 150 GHz with a resolution of 26 and 16.6 arcmin FWHM respectively. Analysis of the maps gives a power spectrum with a peak at angular scales of ~1 degree with an amplitude ~70 uK., Comment: 5 pages, 1 figure LaTeX, emulateapj.sty
Published: 1999
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66. MAXIMA: an experiment to measure temperature anisotropy in the cosmic microwave background

Author: Lee, A. T., Ade, P., Balbi, A., Bock, J., Borrill, J., Boscaleri, A., Crill, B. P., De Bernardis, P., Del Castillo, H., Ferreira, P., Ganga, K., Hanany, S., Hristov, V., Jaffe, A. H., Lange, A. E., Mauskopf, P., Netterfield, C. B., Oh, S., Pascale, E., Rabii, B., Richards, P. L., Ruhl, J., Smoot, G. F., and Winant, C. D.
Subjects: Astrophysics
Abstract: We describe the MAXIMA experiment, a balloon-borne measurement designed to map temperature anisotropy in the Cosmic Microwave Background (CMB) over a wide range of angular scales (multipole range 80 < l < 800). The experiment consists of a 1.3 m diameter off-axis Gregorian telescope and a receiver with a 16 element array of bolometers cooled to 100 mK. The frequency bands are centered at 150, 240, and 410 GHz. The 10' FWHM beam sizes are well matched to the scale of acoustic peaks expected in the angular power spectrum of the CMB. The first flight of the experiment in its full configuration was launched in August 1998. A 122 sq-deg map of the sky was made near the Draco constellation during the 7 hour flight in a region of extremely low galactic dust contamination. This map covers 0.3% of the sky and has 3200 independent beamsize pixels. We describe the MAXIMA instrument and its performance during the recent flight., Comment: To appear in proceedings of `3K Cosmology', ed. F Melchiorri, Conference held Oct 5-10 1998, Rome, 13 pages LaTeX (using aipproc2.sty & aipproc2.cls), Postscript with higher resolution graphics available at http://cfpa.berkeley.edu/group/cmb/gen.html
Published: 1999
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67. Applications of Wavelets to the Analysis of Cosmic Microwave Background Maps

Author: Tenorio, L., Jaffe, A. H., Hanany, S., and Lineweaver, C. H.
Subjects: Astrophysics
Abstract: We consider wavelets as a tool to perform a variety of tasks in the context of analyzing cosmic microwave background (CMB) maps. Using Spherical Haar Wavelets we define a position and angular-scale-dependent measure of power that can be used to assess the existence of spatial structure. We apply planar Daubechies wavelets for the identification and removal of points sources from small sections of sky maps. Our technique can successfully identify virtually all point sources which are above 3 sigma and more than 80% of those above 1 sigma. We discuss the trade-offs between the levels of correct and false detections. We denoise and compress a 100,000 pixel CMB map by a factor of about 10 in 5 seconds achieving a noise reduction of about 35%. In contrast to Wiener filtering the compression process is model independent and very fast. We discuss the usefulness of wavelets for power spectrum and cosmological parameter estimation. We conclude that at present wavelet functions are most suitable for identifying localized sources., Comment: 10 pages, 6 figures. Submitted to MNRAS
Published: 1999
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68. The Effect of the Detector Response Time on Bolometric Cosmic Microwave Background Anisotropy Experiments

Author: Hanany, S., Jaffe, A. H., and Scannapieco, E.
Subjects: Astrophysics
Abstract: We analyze the effects of the detector response time on bolometric measurements of the anisotropy of the cosmic microwave background (CMB). We quantify the effect in terms of a single dimensionless parameter $L$ defined as the ratio between the time the beam sweeps its own size and the bolometer response time. As $L$ decreases below $\sim 2.5$ the point source response of the experiment becomes elongated. We introduce a window function matrix based on the timestream data to assess the effects of the elongated beam. We find that the values of the window function matrix elements decrease slowly as a function $L$. Our analysis and results apply to other cases of beam asymmetry. For the High Frequency Instrument on board the Planck Surveyor satellite we show that for a broad range of $L$ the ability of the experiment to extract the cosmological parameters is not degraded. Our analysis enhances the flexibility in tuning the design parameters of CMB anisotropy experiments., Comment: 9 Pages, 4 Figures, mn.sty; Final version to be published in MNRAS
Published: 1998
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69. The Maxima and Boomerang Experiments

Author: Hanany, S., Collaboration, MAXIMA, and Collaboration, BOOMERANG
Subjects: Astrophysics
Abstract: MAXIMA and BOOMERanG are balloon borne experiments designed to map the cosmic microwave background anisotropy power spectrum from l=10 to l=900 with high resolution. Here we describe the program of observations, the experiments, their capabilities, and their expected performance., Comment: 3 pages, Latex, sprocl.sty file attached, to appear in the Proceedings of the 18th Texas Symposium on Relativistic Astrophysics
Published: 1997

70. The MAX and MAXIMA Experiments

Author: Hanany, S., collaboration, MAX, and collaboration, MAXIMA
Subjects: Astrophysics
Abstract: We summarize the performance of the MAX experiment during its 5 years of operation and present a compilation of the results to date. We describe MAXIMA, a balloon borne experiment employing an array of detectors in the focal plane, that will provide sensitive measurements of the power spectrum between l~60 and l~650., Comment: 6 pages, 1 fig., Latex and additional .sty files attached. To appear in the Proceedings of The XXXI Moriond Meeting "Microwave Background Anisotropies"
Published: 1996

71. The Second Measurement of Anisotropy in the Cosmic Microwave Background Radiation at 0\fdg5 Scales near the Star Mu Pegasi

Author: Lim, M. A., Clapp, A. C., Devlin, M. J., Figueiredo, N., Gundersen, J. O., Hanany, S., Hristov, V. V., Lange, A. E., Lubin, P. M., Meinhold, P. R., Richards, P. L., Staren, J. W., Smoot, G. F., and Tanaka, and S. T.
Subjects: Astrophysics
Abstract: During the fifth flight of the Microwave Anisotropy Experiment (MAX5), we revisited a region with significant dust emission near the star Mu Pegasi. A 3.5 cm$^{-1}$ low frequency channel has been added since the previous measurement (\cite{mei93a}). The data in each channel clearly show structure correlated with IRAS 100 \micron\ dust emission. The spectrum of the structure in the 6, 9 and 14 cm$^{-1}$ channels is described by $I_{\nu}\propto\nu^{\beta}B_{\nu}(T_{dust})$, where $\beta$ = 1.3 and $T_{dust}$ = 19~K and $B_{\nu}$ is the Planck function. However, this model predicts a smaller amplitude in the 3.5 cm$^{-1}$ band than is observed. Considering only linear combinations of the data independent of the best fit foreground spectrum for the three lower channels, we find an upper limit to CMBR fluctuations of $\Delta T/T = \langle \frac{C_l~l(l+1)}{2\pi}\rangle^{\frac{1}{2}} \leq 1.3\times 10^{-5}$ at the 95\% confidence level. The result is for a flat band power spectrum and does not include a 10\% uncertainty in calibration. It is consistent with our previous observation in the region.
Published: 1996
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72. Measurements of Anisotropy in the Cosmic Microwave Background Radiation at 0\fdg5 Scales near the Stars HR5127 and Phi Herculis

Author: Tanaka, S. T., Clapp, A. C., Devlin, M. J., Figueiredo, N., Gundersen, J. O., Hanany, S., Hristov, V. V., Lange, A. E., Lim, M. A., Lubin, P. M., Meinhold, P. R., Richards, P. L., Smoot, G. F., and Staren, J.
Subjects: Astrophysics
Abstract: We present measurements of cosmic microwave background (CMB) anisotropy near the stars HR5127 and Phi Herculis from the fifth flight of the Millimeter-wave Anisotropy eXperiment (MAX). We scanned 8\arcdeg\ strips of the sky with an approximately Gaussian 0\fdg5 FWHM beam and a 1\fdg4 peak to peak sinusoidal chop. The instrument has four frequency bands centered at 3.5, 6, 9, and 14~cm$^{-1}$. The IRAS 100~\micron\ map predicts that these two region have low interstellar dust contrast. The HR5127 data are consistent with CMB anisotropy. The Phi Herculis data, which were measured at lower flight altitudes, show time variability at 9 and 14~cm$^{-1}$ which we believe to be due to atmospheric emission. However, the Phi Herculis data at 3.5 and 6~cm$^{-1}$ are essentially independent of this atmospheric contribution and are consistent with CMB anisotropy. Confusion from galactic foregrounds is unlikely based on the spectrum and amplitude of the structure at these frequencies. If the observed HR5127 structure and the atmosphere independent Phi Herculis structure are attributed to CMB anisotropy, then we find $\Delta T/T = \langle\frac{l(l+1)C_l}{2\pi}\rangle^{1/2} = 1.2^{+0.4}_{-0.3}\times 10^{-5}$ for HR5127 and $1.9^{+0.7}_{-0.4}\times 10^{-5}$ for Phi Herculis in the flat band approximation. The upper and lower limits represent a 68\% confidence interval added in quadrature with a 10\% calibration uncertainty., Comment: 17 pages, 2 Postscript figures, uses aasms4.sty
Published: 1995
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73. Developments of Highly Multiplexed, Multi-chroic Pixels for Balloon-Borne Platforms

Author: Aubin, F., Hanany, S., Johnson, B. R., Lee, A., Suzuki, A., Westbrook, B., and Young, K.
Published: 2018
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74. The MAXIMA and MAXIPOL experiments

Author: Richards, P.L., Abroe, M., Ade, P., Balbi, A., Bock, J., Borrill, J., Boscaleri, A., de Bernardis, P., Collins, J., Ferreira, P.G., Hanany, S., Hristov, V.V., Jaffe, A.H., Johnson, B., Lee, A.T., Matsumu, T., Mauskopf, P.D., Netterfield, C.B., Pascale, E., Rabii, B., Smoot, G.F., Stompor, R., Winant, C.D., and Wu, J.H.P.
Subjects: Classical and quantum mechanics, general physics
Published: 2001

75. MAXIMA-1: A Measurement of the Cosmic Microwave Background Anisotropy on angular scales of 10' to 5 degrees

Author: Ade, P., Balbi, A., Bock, J., Borrill, J., Boscaleri, A., de Bernardis, P., Ferreira, P.G., Hanany, S., Hristov, V.V., Jaffe, A.H., Lange, A.E., Lee, A.T., Mauskopf, P.D., Netterfield, C.B., Oh, S., Pascale, E., Rabii, B., Richards, P.L., Smoot, G.F., Stompor, R., Winant, C.D., and Wu, J.H.P.
Subjects: General and miscellaneous//mathematics, computing, and information science
Published: 2000

76. Performance of a 200 mm Diameter Achromatic HWP with Laser-Ablated Sub-Wavelength Structures.

Author: Takaku, R., Ghigna, T., Hanany, S., Hoshino, Y., Ishino, H., Katayama, N., Komatsu, K., Konishi, K., Kuwata-Gonokami, M., Matsumura, T., Sakurai, H., Sakurai, Y., Wen, Q., Yamasaki, N. Y., and Yumoto, J.
Subjects: COSMIC background radiation, DIAMETER, ULTRAVIOLET lasers
Abstract: We laser-ablated sub-wavelength structures (SWS) on 200 mm diameter birefringent sapphire disks to produce broadband anti-reflection coating (ARC). The disks were assembled into a stack of five plates making an achromatic half-wave plate (AHWP) suitable for operation between 40 and 140 GHz. We report on the SWS fabrication and transmission measurements of the stack at room temperature. From the measurements, we compute a band average transmission and modulation efficiency for nine spectral bands that correspond to the frequency coverage of the LiteBIRD Low-Frequency Telescope (LFT). We also assess the level of instrumental polarization the AHWP exhibits. We discuss paths for further development to minimize the instrumental polarization from the AHWP. This work is a development milestone toward the implementation of an AHWP for the LiteBIRD satellite. [ABSTRACT FROM AUTHOR]
Published: 2023
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77. Design Evolution of the Spiderweb TES Bolometer for Cosmology Applications

Author: Westbrook, B., Lee, A., Meng, X., Suzuki, A., Arnold, K., Shirokoff, E., George, E., Aubin, F., Dobbs, M., MacDermid, K., Hanany, S., Raach, K., Aboobaker, A., Hubmayr, J., Oshima, T., Kawamura, M., Kohno, K., The EBEX Collaboration, and The ASTE Collaboration
Published: 2012
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78. Digital Frequency Multiplexer for TES Detectors—Path to Flight

Author: Dobbs, M., Aubin, F., de Haan, T., Hanany, S., Harrington, N., Holzapfel, W., Hubmayr, J., Lee, A., Lueker, M., Macdermid, K., and Smecher, G.
Published: 2012
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79. Microwave spectro-polarimetry of matter and radiation across space and time

Author: Delabrouille, J, Delabrouille, J, Abitbol, MH, Aghanim, N, Ali-Haïmoud, Y, Alonso, D, Alvarez, M, Banday, AJ, Bartlett, JG, Baselmans, J, Basu, K, Battaglia, N, Climent, JRB, Bernal, JL, Béthermin, M, Bolliet, B, Bonato, M, Bouchet, FR, Breysse, PC, Burigana, C, Cai, ZY, Chluba, J, Churazov, E, Dannerbauer, H, De Bernardis, P, De Zotti, G, Di Valentino, E, Dimastrogiovanni, E, Endo, A, Erler, J, Ferraro, S, Finelli, F, Fixsen, D, Hanany, S, Hart, L, Hernández-Monteagudo, C, Hill, JC, Hotinli, SC, Karatsu, K, Karkare, K, Keating, GK, Khabibullin, I, Kogut, A, Kohri, K, Kovetz, ED, Lagache, G, Lesgourgues, J, Madhavacheril, M, Maffei, B, Mandolesi, N, Martins, C, Masi, S, Mather, J, Melin, JB, Dizgah, AM, Mroczkowski, T, Mukherjee, S, Nagai, D, Negrello, M, Palanque-Delabrouille, N, Paoletti, D, Patil, SP, Piacentini, F, Raghunathan, S, Ravenni, A, Remazeilles, M, Revéret, V, Rodriguez, L, Rotti, A, Martin, JAR, Sayers, J, Scott, D, Silk, J, Silva, M, Souradeep, T, Sugiyama, N, Sunyaev, R, Switzer, ER, Tartari, A, Trombetti, T, Zubeldia, Í, Delabrouille, J, Delabrouille, J, Abitbol, MH, Aghanim, N, Ali-Haïmoud, Y, Alonso, D, Alvarez, M, Banday, AJ, Bartlett, JG, Baselmans, J, Basu, K, Battaglia, N, Climent, JRB, Bernal, JL, Béthermin, M, Bolliet, B, Bonato, M, Bouchet, FR, Breysse, PC, Burigana, C, Cai, ZY, Chluba, J, Churazov, E, Dannerbauer, H, De Bernardis, P, De Zotti, G, Di Valentino, E, Dimastrogiovanni, E, Endo, A, Erler, J, Ferraro, S, Finelli, F, Fixsen, D, Hanany, S, Hart, L, Hernández-Monteagudo, C, Hill, JC, Hotinli, SC, Karatsu, K, Karkare, K, Keating, GK, Khabibullin, I, Kogut, A, Kohri, K, Kovetz, ED, Lagache, G, Lesgourgues, J, Madhavacheril, M, Maffei, B, Mandolesi, N, Martins, C, Masi, S, Mather, J, Melin, JB, Dizgah, AM, Mroczkowski, T, Mukherjee, S, Nagai, D, Negrello, M, Palanque-Delabrouille, N, Paoletti, D, Patil, SP, Piacentini, F, Raghunathan, S, Ravenni, A, Remazeilles, M, Revéret, V, Rodriguez, L, Rotti, A, Martin, JAR, Sayers, J, Scott, D, Silk, J, Silva, M, Souradeep, T, Sugiyama, N, Sunyaev, R, Switzer, ER, Tartari, A, Trombetti, T, and Zubeldia, Í
Abstract: This paper discusses the science case for a sensitive spectro-polarimetric survey of the microwave sky. Such a survey would provide a tomographic and dynamic census of the three-dimensional distribution of hot gas, velocity flows, early metals, dust, and mass distribution in the entire Hubble volume, exploit CMB temperature and polarisation anisotropies down to fundamental limits, and track energy injection and absorption into the radiation background across cosmic times by measuring spectral distortions of the CMB blackbody emission. In addition to its exceptional capability for cosmology and fundamental physics, such a survey would provide an unprecedented view of microwave emissions at sub-arcminute to few-arcminute angular resolution in hundreds of frequency channels, a data set that would be of immense legacy value for many branches of astrophysics. We propose that this survey be carried out with a large space mission featuring a broad-band polarised imager and a moderate resolution spectro-imager at the focus of a 3.5 m aperture telescope actively cooled to about 8K, complemented with absolutely-calibrated Fourier Transform Spectrometer modules observing at degree-scale angular resolution in the 10–2000 GHz frequency range. We propose two observing modes: a survey mode to map the entire sky as well as a few selected wide fields, and an observatory mode for deeper observations of regions of specific interest.
Published: 2021

80. Broadband, millimeter-wave anti-reflective structures on sapphire ablated with femto-second laser

Author: Takaku, R., primary, Hanany, S., additional, Imada, H., additional, Ishino, H., additional, Katayama, N., additional, Komatsu, K., additional, Konishi, K., additional, Kuwata-Gonokami, M., additional, Matsumura, T., additional, Mitsuda, K., additional, Sakurai, H., additional, Sakurai, Y., additional, Wen, Q., additional, Yamasaki, N. Y., additional, Young, K., additional, and Yumoto, J., additional
Published: 2020
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81. Gravity Wave Breaking and Vortex Ring Formation Observed by PMC Turbo

Author: Geach, C., primary, Hanany, S., additional, Fritts, D. C., additional, Kaifler, B., additional, Kaifler, N., additional, Kjellstrand, C. B., additional, Williams, B. P., additional, Eckermann, S. D., additional, Miller, A. D., additional, Jones, G., additional, and Reimuller, J., additional
Published: 2020
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82. Exploring cosmic origins with CORE: Extragalactic sources in cosmic microwave background maps

Author: Zotti, G, González-Nuevo, J, Lopez-Caniego, M, Negrello, M, Greenslade, J, Hernández-Monteagudo, C, Delabrouille, J, Cai, Z, Bonato, M, Achúcarro, A, Ade, P, Allison, R, Ashdown, M, Ballardini, M, Banday, A, Banerji, R, Bartlett, J, Bartolo, N, Basak, S, Bersanelli, M, Biesiada, M, Bilicki, M, Bonaldi, A, Bonavera, L, Borrill, J, Bouchet, F, Boulanger, F, Brinckmann, T, Bucher, M, Burigana, C, Buzzelli, A, Calvo, M, Carvalho, C, Castellano, M, Challinor, A, Chluba, J, Clements, D, Clesse, S, Colafrancesco, S, Colantoni, I, Coppolecchia, A, Crook, M, D'Alessandro, G, de Bernardis, P, de Gasperis, G, Diego, J, Valentino, E, Errard, J, Feeney, S, Fernández-Cobos, R, Ferraro, S, Finelli, F, Forastieri, F, Galli, S, Génova-Santos, R, Gerbino, M, Grandis, S, Hagstotz, S, Hanany, S, Handley, W, Hervias-Caimapo, C, Hills, M, Hivon, E, Kiiveri, K, Kisner, T, Kitching, T, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamagna, L, Lasenby, A, Lattanzi, M, Brun, A, Lesgourgues, J, Lewis, A, Liguori, M, Lindholm, V, Luzzi, G, Maffei, B, Mandolesi, N, Martinez-Gonzalez, E, Martins, C, Masi, S, Massardi, M, Matarrese, S, Mccarthy, D, Melchiorri, A, Melin, J, Molinari, D, Monfardini, A, Natoli, P, Notari, A, Paiella, A, Paoletti, D, Partridge, R, Patanchon, G, Piat, M, Pisano, G, Polastri, L, Polenta, G, Pollo, A, Poulin, V, Quartin, M, Remazeilles, M, Roman, M, Rossi, G, Roukema, B, Rubiño-Martín, J, Salvati, L, Scott, D, Serjeant, S, Tartari, A, Toffolatti, L, Tomasi, M, Trappe, N, Triqueneaux, S, Trombetti, T, Tucci, M, Tucker, C, Väliviita, J, de Weygaert, R, Tent, B, Vennin, V, Vielva, P, Vittorio, N, Young, K, Zannoni, M, Zotti, G. De, González-Nuevo, J., Lopez-Caniego, M., Negrello, M., Greenslade, J., Hernández-Monteagudo, C., Delabrouille, J., Cai, Z. -Y., Bonato, M., Achúcarro, A., Ade, P., Allison, R., Ashdown, M., Ballardini, M., Banday, A. J., Banerji, R., Bartlett, J. G., Bartolo, N., Basak, S., Bersanelli, M., Biesiada, M., Bilicki, M., Bonaldi, A., Bonavera, L., Borrill, J., Bouchet, F., Boulanger, F., Brinckmann, T., Bucher, M., Burigana, C., Buzzelli, A., Calvo, M., Carvalho, C. S., Castellano, M. G., Challinor, A., Chluba, J., Clements, D. L., Clesse, S., Colafrancesco, S., Colantoni, I., Coppolecchia, A., Crook, M., D'Alessandro, G., de Bernardis, P., de Gasperis, G., Diego, J. M., Valentino, E. Di, Errard, J., Feeney, S. M., Fernández-Cobos, R., Ferraro, S., Finelli, F., Forastieri, F., Galli, S., Génova-Santos, R. T., Gerbino, M., Grandis, S., Hagstotz, S., Hanany, S., Handley, W., Hervias-Caimapo, C., Hills, M., Hivon, E., Kiiveri, K., Kisner, T., Kitching, T., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamagna, L., Lasenby, A., Lattanzi, M., Brun, A. Le, Lesgourgues, J., Lewis, A., Liguori, M., Lindholm, V., Luzzi, G., Maffei, B., Mandolesi, N., Martinez-Gonzalez, E., Martins, C. J. A. P., Masi, S., Massardi, M., Matarrese, S., McCarthy, D., Melchiorri, A., Melin, J. -B., Molinari, D., Monfardini, A., Natoli, P., Notari, A., Paiella, A., Paoletti, D., Partridge, R. B., Patanchon, G., Piat, M., Pisano, G., Polastri, L., Polenta, G., Pollo, A., Poulin, V., Quartin, M., Remazeilles, M., Roman, M., Rossi, G., Roukema, B. F., Rubiño-Martín, J. -A., Salvati, L., Scott, D., Serjeant, S., Tartari, A., Toffolatti, L., Tomasi, M., Trappe, N., Triqueneaux, S., Trombetti, T., Tucci, M., Tucker, C., Väliviita, J., de Weygaert, R. van, Tent, B. Van, Vennin, V., Vielva, P., Vittorio, N., Young, K., Zannoni, M., Zotti, G, González-Nuevo, J, Lopez-Caniego, M, Negrello, M, Greenslade, J, Hernández-Monteagudo, C, Delabrouille, J, Cai, Z, Bonato, M, Achúcarro, A, Ade, P, Allison, R, Ashdown, M, Ballardini, M, Banday, A, Banerji, R, Bartlett, J, Bartolo, N, Basak, S, Bersanelli, M, Biesiada, M, Bilicki, M, Bonaldi, A, Bonavera, L, Borrill, J, Bouchet, F, Boulanger, F, Brinckmann, T, Bucher, M, Burigana, C, Buzzelli, A, Calvo, M, Carvalho, C, Castellano, M, Challinor, A, Chluba, J, Clements, D, Clesse, S, Colafrancesco, S, Colantoni, I, Coppolecchia, A, Crook, M, D'Alessandro, G, de Bernardis, P, de Gasperis, G, Diego, J, Valentino, E, Errard, J, Feeney, S, Fernández-Cobos, R, Ferraro, S, Finelli, F, Forastieri, F, Galli, S, Génova-Santos, R, Gerbino, M, Grandis, S, Hagstotz, S, Hanany, S, Handley, W, Hervias-Caimapo, C, Hills, M, Hivon, E, Kiiveri, K, Kisner, T, Kitching, T, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamagna, L, Lasenby, A, Lattanzi, M, Brun, A, Lesgourgues, J, Lewis, A, Liguori, M, Lindholm, V, Luzzi, G, Maffei, B, Mandolesi, N, Martinez-Gonzalez, E, Martins, C, Masi, S, Massardi, M, Matarrese, S, Mccarthy, D, Melchiorri, A, Melin, J, Molinari, D, Monfardini, A, Natoli, P, Notari, A, Paiella, A, Paoletti, D, Partridge, R, Patanchon, G, Piat, M, Pisano, G, Polastri, L, Polenta, G, Pollo, A, Poulin, V, Quartin, M, Remazeilles, M, Roman, M, Rossi, G, Roukema, B, Rubiño-Martín, J, Salvati, L, Scott, D, Serjeant, S, Tartari, A, Toffolatti, L, Tomasi, M, Trappe, N, Triqueneaux, S, Trombetti, T, Tucci, M, Tucker, C, Väliviita, J, de Weygaert, R, Tent, B, Vennin, V, Vielva, P, Vittorio, N, Young, K, Zannoni, M, Zotti, G. De, González-Nuevo, J., Lopez-Caniego, M., Negrello, M., Greenslade, J., Hernández-Monteagudo, C., Delabrouille, J., Cai, Z. -Y., Bonato, M., Achúcarro, A., Ade, P., Allison, R., Ashdown, M., Ballardini, M., Banday, A. J., Banerji, R., Bartlett, J. G., Bartolo, N., Basak, S., Bersanelli, M., Biesiada, M., Bilicki, M., Bonaldi, A., Bonavera, L., Borrill, J., Bouchet, F., Boulanger, F., Brinckmann, T., Bucher, M., Burigana, C., Buzzelli, A., Calvo, M., Carvalho, C. S., Castellano, M. G., Challinor, A., Chluba, J., Clements, D. L., Clesse, S., Colafrancesco, S., Colantoni, I., Coppolecchia, A., Crook, M., D'Alessandro, G., de Bernardis, P., de Gasperis, G., Diego, J. M., Valentino, E. Di, Errard, J., Feeney, S. M., Fernández-Cobos, R., Ferraro, S., Finelli, F., Forastieri, F., Galli, S., Génova-Santos, R. T., Gerbino, M., Grandis, S., Hagstotz, S., Hanany, S., Handley, W., Hervias-Caimapo, C., Hills, M., Hivon, E., Kiiveri, K., Kisner, T., Kitching, T., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamagna, L., Lasenby, A., Lattanzi, M., Brun, A. Le, Lesgourgues, J., Lewis, A., Liguori, M., Lindholm, V., Luzzi, G., Maffei, B., Mandolesi, N., Martinez-Gonzalez, E., Martins, C. J. A. P., Masi, S., Massardi, M., Matarrese, S., McCarthy, D., Melchiorri, A., Melin, J. -B., Molinari, D., Monfardini, A., Natoli, P., Notari, A., Paiella, A., Paoletti, D., Partridge, R. B., Patanchon, G., Piat, M., Pisano, G., Polastri, L., Polenta, G., Pollo, A., Poulin, V., Quartin, M., Remazeilles, M., Roman, M., Rossi, G., Roukema, B. F., Rubiño-Martín, J. -A., Salvati, L., Scott, D., Serjeant, S., Tartari, A., Toffolatti, L., Tomasi, M., Trappe, N., Triqueneaux, S., Trombetti, T., Tucci, M., Tucker, C., Väliviita, J., de Weygaert, R. van, Tent, B. Van, Vennin, V., Vielva, P., Vittorio, N., Young, K., and Zannoni, M.
Abstract: We discuss the potential of a next generation space-borne Cosmic Microwave Background (CMB) experiment for studies of extragalactic sources. Our analysis has particular bearing on the definition of the future space project, CORE, that has been submitted in response to ESA's call for a Medium-size mission opportunity as the successor of the Planck satellite. Even though the effective telescope size will be somewhat smaller than that of Planck, CORE will have a considerably better angular resolution at its highest frequencies, since, in contrast with Planck, it will be diffraction limited at all frequencies. The improved resolution implies a considerable decrease of the source confusion, i.e. substantially fainter detection limits. In particular, CORE will detect thousands of strongly lensed high-z galaxies distributed over the full sky. The extreme brightness of these galaxies will make it possible to study them, via follow-up observations, in extraordinary detail. Also, the CORE resolution matches the typical sizes of high-z galaxy proto-clusters much better than the Planck resolution, resulting in a much higher detection efficiency; these objects will be caught in an evolutionary phase beyond the reach of surveys in other wavebands. Furthermore, CORE will provide unique information on the evolution of the star formation in virialized groups and clusters of galaxies up to the highest possible redshifts. Finally, thanks to its very high sensitivity, CORE will detect the polarized emission of thousands of radio sources and, for the first time, of dusty galaxies, at mm and sub-mm wavelengths, respectively.
Published: 2018

83. The polarization dependence of x-ray photoelectron yield of a Au photocathode

Author: Shaw, P.S., Hanany, S., Liu, Y., Novick, R., LaRosa, G., Manzo, G., Santangelo, A., and Bivona, S.
Subjects: Photoelectric devices -- Research, Photoemission -- Analysis, Polarization (Light) -- Analysis, Physics
Abstract: Experimental evaluation of the X-ray photoelectron productivity of an Au photocathode reveals that the modulation factor is below 4% when the polarization state changes. Photocathode excitation is done at a glancing angle between 5 and 50 degrees with 2.7, 2.5 and 4.0 keV of energies. Photoelectron yield does not depend on polarization for all three energies, in contrast with previous reports.
Published: 1994

84. Exploring cosmic origins with CORE: Effects of observer peculiar motion

Author: Burigana, C., Carvalho, C. S., Trombetti, T., Notari, A., Quartin, M., Gasperis, G. D., Buzzelli, A., Vittorio, N., Zotti, G. De, De Bernardis, P., Chluba, J., Bilicki, M., Danese, L., Delabrouille, J., Toffolatti, L., Lapi, A., Negrello, M., Mazzotta, P., Scott, D., Contreras, D., Achúcarro, A., Ade, P., Allison, R., Ashdown, M., Ballardini, M., Banday, A. J., Banerji, R., Bartlett, J., Bartolo, N., Basak, S., Bersanelli, M., Bonaldi, A., Bonato, M., Borrill, J., Bouchet, F., Boulanger, F., Brinckmann, T., Bucher, M., Cabella, P., Cai, Z. -Y., Calvo, M., Castellano, M. G., Challinor, A., Clesse, S., Colantoni, I., Coppolecchia, A., Crook, M., D'Alessandro, G., Diego, J. -M., Marco, A. Di, Valentino, E. Di, Errard, J., Feeney, S., Fernández-Cobos, R., Ferraro, S., Finelli, F., Forastieri, F., Galli, S., Génova-Santos, R., Gerbino, M., González-Nuevo, J., Grandis, S., Greenslade, J., Hagstotz, S., Hanany, S., Handley, W., Hernández-Monteagudo, C., Hervias-Caimapo, C., Hills, M., Hivon, E., Kiiveri, K., Kisner, T., Kitching, T., Kunz, M., Kurki-Suonio, H., Lamagna, L., Lasenby, A., Lattanzi, M., Lesgourgues, J., Liguori, M., Lindholm, V., Lopez-Caniego, M., Luzzi, G., Maffei, B., Mandolesi, N., Martinez-Gonzalez, E., Martins, C. J. A. P., Masi, S., Matarrese, S., Mccarthy, D., Melchiorri, A., Melin, J. -B., Molinari, D., Monfardini, A., Natoli, P., Paiella, Alessandro, Paoletti, D., Patanchon, G., Piat, M., Pisano, G., Polastri, L., Polenta, G., Pollo, A., Poulin, V., Remazeilles, M., Roman, M., Rubiño-Martín, J. -A., Salvati, L., Tartari, A., Tomasi, M., Tramonte, D., Trappe, N., Tucker, C., Väliviita, J., De Weijgaert, R. Van, Tent, B. Van, Vennin, V., Vielva, P., Young, K., Zannoni, M., D'Alessandro, Giuseppe, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut Néel (NEEL), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Institut Lagrange de Paris, Sorbonne Université (SU), Département de Physique des Particules (ex SPP) (DPP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), CORE, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Cryogénie (NEEL - Cryo), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Département de Physique des Particules (ex SPP) (DPhP), Hélium : du fondamental aux applications (NEEL - HELFA), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Universitat de Barcelona, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Sorbonne Universités, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Burigana, C, Carvalho, C, Trombetti, T, Notari, A, Quartin, M, Gasperis, G, Buzzelli, A, Vittorio, N, Zotti, G, de Bernardis, P, Chluba, J, Bilicki, M, Danese, L, Delabrouille, J, Toffolatti, L, Lapi, A, Negrello, M, Mazzotta, P, Scott, D, Contreras, D, Achúcarro, A, Ade, P, Allison, R, Ashdown, M, Ballardini, M, Banday, A, Banerji, R, Bartlett, J, Bartolo, N, Basak, S, Bersanelli, M, Bonaldi, A, Bonato, M, Borrill, J, Bouchet, F, Boulanger, F, Brinckmann, T, Bucher, M, Cabella, P, Cai, Z, Calvo, M, Castellano, M, Challinor, A, Clesse, S, Colantoni, I, Coppolecchia, A, Crook, M, D'Alessandro, G, Diego, J, Marco, A, Valentino, E, Errard, J, Feeney, S, Fernández-Cobos, R, Ferraro, S, Finelli, F, Forastieri, F, Galli, S, Génova-Santos, R, Gerbino, M, González-Nuevo, J, Grandis, S, Greenslade, J, Hagstotz, S, Hanany, S, Handley, W, Hernández-Monteagudo, C, Hervias-Caimapo, C, Hills, M, Hivon, E, Kiiveri, K, Kisner, T, Kitching, T, Kunz, M, Kurki-Suonio, H, Lamagna, L, Lasenby, A, Lattanzi, M, Lesgourgues, J, Liguori, M, Lindholm, V, Lopez-Caniego, M, Luzzi, G, Maffei, B, Mandolesi, N, Martinez-Gonzalez, E, Martins, C, Masi, S, Matarrese, S, Mccarthy, D, Melchiorri, A, Melin, J, Molinari, D, Monfardini, A, Natoli, P, Paiella, A, Paoletti, D, Patanchon, G, Piat, M, Pisano, G, Polastri, L, Polenta, G, Pollo, A, Poulin, V, Remazeilles, M, Roman, M, Rubiño-Martín, J, Salvati, L, Tartari, A, Tomasi, M, Tramonte, D, Trappe, N, Tucker, C, Väliviita, J, de Weijgaert, R, Tent, B, Vennin, V, Vielva, P, Young, K, Zannoni, M, Helsinki Institute of Physics, Department of Physics, Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut d'astrophysique spatiale ( IAS ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut Néel ( NEEL ), Université Grenoble Alpes [Saint Martin d'Hères]-Centre National de la Recherche Scientifique ( CNRS ), Département de Physique des Particules (ex SPP) ( DPP ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Laboratoire d'Annecy-le-Vieux de Physique Théorique ( LAPTH ), Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique Théorique d'Orsay [Orsay] ( LPT ), Université Paris-Sud - Paris 11 ( UP11 ) -Centre National de la Recherche Scientifique ( CNRS ), and Astronomy
Subjects: POLARIZATION, CMBR experiments, CMBR theory, high redshift galaxies, reionization, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], BACKGROUND-RADIATION, Cosmic microwave background, astro-ph.CO, Astrophysics, high redshift galaxie, 01 natural sciences, CMBR experiments, CMBR theory, high redshift galaxies, reionization, Astronomy and Astrophysics, cosmic flows, Infrared astronomy, CMB SPECTRAL DISTORTIONS, Peculiar velocity, ENERGY-RELEASE, CMBR experiments – CMBR theory – reionization – high redshift galaxies, MICROWAVE, 010303 astronomy & astrophysics, QC, QB, Astronomia infraroja, Physics, REDSHIFT SURVEY, COSMIC cancer database, Astrophysics::Instrumentation and Methods for Astrophysics, DIPOLE ANISOTROPY, Cosmology, GALAXIES, Amplitude, symbols, CMBR experiment, LOCAL GROUP, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, NO, symbols.namesake, FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Planck, Reionization, Cosmologia, 010308 nuclear & particles physics, SOLAR MOTION, HOT-MODEL, CONSTRAINTS, 115 Astronomy, Space science, Dipole, PSCZ DIPOLE, CLUSTERS, Multipole expansion, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We discuss the effects on the CMB, CIB, and thermal SZ effect due to the peculiar motion of an observer with respect to the CMB rest frame, which induces boosting effects. We investigate the scientific perspectives opened by future CMB space missions, focussing on the CORE proposal. The improvements in sensitivity offered by a mission like CORE, together with its high resolution over a wide frequency range, will provide a more accurate estimate of the CMB dipole. The extension of boosting effects to polarization and cross-correlations will enable a more robust determination of purely velocity-driven effects that are not degenerate with the intrinsic CMB dipole, allowing us to achieve a S/N ratio of 13; this improves on the Planck detection and essentially equals that of an ideal cosmic-variance-limited experiment up to a multipole l of 2000. Precise inter-frequency calibration will offer the opportunity to constrain or even detect CMB spectral distortions, particularly from the cosmological reionization, because of the frequency dependence of the dipole spectrum, without resorting to precise absolute calibration. The expected improvement with respect to COBE-FIRAS in the recovery of distortion parameters (in principle, a factor of several hundred for an ideal experiment with the CORE configuration) ranges from a factor of several up to about 50, depending on the quality of foreground removal and relative calibration. Even for 1% accuracy in both foreground removal and relative calibration at an angular scale of 1 deg, we find that dipole analyses for a mission like CORE will be able to improve the recovery of the CIB spectrum amplitude by a factor of 17 in comparison with current results based on FIRAS. In addition to the scientific potential of a mission like CORE for these analyses, synergies with other planned and ongoing projects are also discussed., 61+5 pages, 17 figures, 25 tables, 8 sections, 5 appendices. In press on JCAP - Version 3 - Minor changes, affiliations fixed, references updated - version in line with corrected proofs
Published: 2018
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85. Exploring cosmic origins with CORE: B-mode component separation

Author: Remazeilles, M., Banday, A. J., Baccigalupi, C., Basak, S., Bonaldi, A., Zotti, G. De, Delabrouille, J., Dickinson, C., Eriksen, H. K., Errard, J., Fernandez-Cobos, R., Fuskeland, U., Hervías-Caimapo, C., López-Caniego, M., Martinez-González, E., Roman, M., Vielva, P., Wehus, I., Achucarro, A., Ade, P., Allison, R., Ashdown, M., Ballardini, M., Banerji, R., Bartlett, J., Bartolo, N., 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, G., Challinor, A., Chluba, J., Clesse, S., Colantoni, I., Coppolecchia, A., Crook, M., D'Alessandro, G., De Bernardis, P., De Gasperis, G., Diego, J. -M., Valentino, E. Di, Feeney, S., Ferraro, S., Finelli, F., Forastieri, F., Galli, S., Genova-Santos, R., Gerbino, M., González-Nuevo, J., Grandis, S., Greenslade, J., Hagstotz, S., Hanany, S., Handley, W., Hernandez-Monteagudo, C., Hills, M., Hivon, E., Kiiveri, K., Kisner, T., Kitching, T., Kunz, M., Kurki-Suonio, H., Lamagna, L., Lasenby, A., Lattanzi, M., Lesgourgues, J., Lewis, A., Liguori, M., Lindholm, V., Luzzi, G., Maffei, B., Martins, C. J. A. P., Masi, S., Matarrese, S., Mccarthy, D., Melin, J. -B., 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., Rubino-Martin, J. -A., Salvati, L., Tartari, A., Tomasi, M., Tramonte, D., Trappe, N., Trombetti, T., Tucker, C., Valiviita, J., De Weijgaert, R. Van, Tent, B. Van, Vennin, V., Vittorio, N., Young, K., Zannoni, M., D'Alessandro, Giuseppe, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut Lagrange de Paris, Sorbonne Universités, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut Néel (NEEL), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Département de Physique des Particules (ex SPP) (DPP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), CORE, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Remazeilles, M, Banday, A, Baccigalupi, C, Basak, S, Bonaldi, A, Zotti, G, Delabrouille, J, Dickinson, C, Eriksen, H, Errard, J, Fernandez-Cobos, R, Fuskeland, U, Hervías-Caimapo, C, López-Caniego, M, Martinez-González, E, Roman, M, Vielva, P, Wehus, I, Achucarro, A, Ade, P, Allison, R, Ashdown, M, Ballardini, M, Banerji, R, Bartlett, J, Bartolo, N, Baumann, D, Bersanelli, M, Bonato, M, Borrill, J, Bouchet, F, Boulanger, F, Brinckmann, T, Bucher, M, Burigana, C, Buzzelli, A, Cai, Z, Calvo, M, Carvalho, C, Castellano, G, Challinor, A, Chluba, J, Clesse, S, Colantoni, I, Coppolecchia, A, Crook, M, D'Alessandro, G, de Bernardis, P, de Gasperis, G, Diego, J, Valentino, E, Feeney, S, Ferraro, S, Finelli, F, Forastieri, F, Galli, S, Genova-Santos, R, Gerbino, M, González-Nuevo, J, Grandis, S, Greenslade, J, Hagstotz, S, Hanany, S, Handley, W, Hernandez-Monteagudo, C, Hills, M, Hivon, E, Kiiveri, K, Kisner, T, Kitching, T, Kunz, M, Kurki-Suonio, H, Lamagna, L, Lasenby, A, Lattanzi, M, Lesgourgues, J, Lewis, A, Liguori, M, Lindholm, V, Luzzi, G, Maffei, B, Martins, C, Masi, S, Matarrese, S, Mccarthy, D, Melin, J, 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, Rubino-Martin, J, Salvati, L, Tartari, A, Tomasi, M, Tramonte, D, Trappe, N, Trombetti, T, Tucker, C, Valiviita, J, de Weijgaert, R, Tent, B, Vennin, V, Vittorio, N, Young, K, Zannoni, M, String Theory (ITFA, IoP, FNWI), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Sorbonne Université (SU), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Helsinki Institute of Physics, Department of Physics, Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Cryogénie (NEEL - Cryo), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Département de Physique des Particules (ex SPP) (DPhP), and Hélium : du fondamental aux applications (NEEL - HELFA)
Subjects: Infrared, Cosmic microwave background, cosmic background radiation: polarization, Astrophysics, cosmic background radiation, 01 natural sciences, B-mode: primordial, thermal, CMBR experiments, cosmological parameters from CMBR, gravitational waves and CMBR polarization, inflation, Astronomy and Astrophysics, gravitational waves and CMBR polarization, CMBR experiments, cosmological parameters from CMBR, inflation, Polarization, CMB POLARIZATION, 010303 astronomy & astrophysics, QC, QB, media_common, Physics, COSMIC cancer database, astro-ph.CO, astro-ph.GA, astro-ph.IM, Cosmology: observations, Astrophysics::Instrumentation and Methods for Astrophysics, Cosmic variance, Polarization (waves), INTERNAL LINEAR COMBINATION, infrared, GALACTIC SYNCHROTRON EMISSION, CMBR experiment, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, RADIO-SOURCES, Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, ANGULAR POWER SPECTRUM, media_common.quotation_subject, FOS: Physical sciences, hydrogen: recombination, Astrophysics::Cosmology and Extragalactic Astrophysics, parametric, NO, cosmic background radiation: B-mode, FIS/05 - ASTRONOMIA E ASTROFISICA, Settore FIS/05 - Astronomia e Astrofisica, gravitation: lens, 0103 physical sciences, ionization, synchrotron, STAR-FORMING GALAXIES, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Reionization, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, POINT-SOURCE DETECTION, methods: data analysis, diffuse radiation, Gravitational lens, Sky, Astrophysics of Galaxies (astro-ph.GA), PROBE WMAP OBSERVATIONS, STATISTICAL PROPERTIES, microwaves: emission, spectral, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], MICROWAVE BACKGROUND POLARIZATION
Abstract: We demonstrate that, for the baseline design of the CORE satellite mission, the polarized foregrounds can be controlled at the level required to allow the detection of the primordial cosmic microwave background (CMB) $B$-mode polarization with the desired accuracy at both reionization and recombination scales, for tensor-to-scalar ratio values of ${r\gtrsim 5\times 10^{-3}}$. We consider detailed sky simulations based on state-of-the-art CMB observations that consist of CMB polarization with $\tau=0.055$ and tensor-to-scalar values ranging from $r=10^{-2}$ to $10^{-3}$, Galactic synchrotron, and thermal dust polarization with variable spectral indices over the sky, polarized anomalous microwave emission, polarized infrared and radio sources, and gravitational lensing effects. Using both parametric and blind approaches, we perform full component separation and likelihood analysis of the simulations, allowing us to quantify both uncertainties and biases on the reconstructed primordial $B$-modes. Under the assumption of perfect control of lensing effects, CORE would measure an unbiased estimate of $r=\left(5 \pm 0.4\right)\times 10^{-3}$ after foreground cleaning. In the presence of both gravitational lensing effects and astrophysical foregrounds, the significance of the detection is lowered, with CORE achieving a $4\sigma$-measurement of $r=5\times 10^{-3}$ after foreground cleaning and $60$% delensing. For lower tensor-to-scalar ratios ($r=10^{-3}$) the overall uncertainty on $r$ is dominated by foreground residuals, not by the 40% residual of lensing cosmic variance. Moreover, the residual contribution of unprocessed polarized point-sources can be the dominant foreground contamination to primordial B-modes at this $r$ level, even on relatively large angular scales, $\ell \sim 50$. Finally, we report two sources of potential bias for the detection of the primordial $B$-modes.[abridged], Comment: 87 pages, 32 figures, 4 tables, expanded abstract. Updated to match version accepted by JCAP
Published: 2018
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86. SOFIA Far-infrared Imaging Polarimetry of M82 and NGC 253: Exploring the Supergalactic Wind

Author: Jones, T., Dowell, C., Lopez Rodriguez, E., Zweibel, E., Berthoud, M., Chuss, D., Goldsmith, P., Hamilton, R., Hanany, S., Harper, D., Lazarian, A., Looney, L., Michail, J., Morris, M., Novak, G., Santos, F., Sheth, K., Stacey, G., Staguhn, J., Stephens, I., Tassis, K., Trinh, C., Volpert, C., Werner, M., Wollack, E., and Team, H.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present far-infrared polarimetry observations of M82 at 53 and 154 Œºm and NGC 253 at 89 Œºm, which were taken with High-resolution Airborne Wideband Camera-plus (HAWC+) in polarimetry mode on the Stratospheric Observatory for Infrared Astronomy. The polarization of M82 at 53 Œºm clearly shows a magnetic field geometry perpendicular to the disk in the hot dust emission. For M82 the polarization at 154 Œºm shows a combination of field geometry perpendicular to the disk in the nuclear region, but closer to parallel to the disk away from the nucleus. The fractional polarization at 53 Œºm (154 Œºm) ranges from 7% (3%) off nucleus to 0.5% (0.3%) near the nucleus. A simple interpretation of the observations of M82 invokes a massive polar outflow, dragging the field along, from a region ~700 pc in diameter that has entrained some of the gas and dust, creating a vertical field geometry seen mostly in the hotter (53 Œºm) dust emission. This outflow sits within a larger disk with a more typical planar geometry that more strongly contributes to the cooler (154 Œºm) dust emission. For NGC 253, the polarization at 89 Œºm is dominated by a planar geometry in the tilted disk, with weak indication of a vertical geometry above and below the plane from the nucleus. The polarization observations of NGC 253 at 53 Œºm were of a insufficient signal-to-noise ratio for a detailed analysis.
Published: 2019

87. The Far-infrared Polarization Spectrum of œÅ Ophiuchi A from HAWC+/SOFIA Observations

Author: Santos, F., Chuss, D., Dowell, C., Houde, M., Looney, L., Lopez Rodriguez, E., Novak, G., Ward-Thompson, D., Berthoud, M., Dale, D., Guerra, J., Hamilton, R., Hanany, S., Harper, D., Henning, T., Jones, T., Lazarian, A., Michail, J., Morris, M., Staguhn, J., Stephens, I., Tassis, K., Trinh, C., Van Camp, E., Volpert, C., and Wollack, E.
Subjects: Astrophysics::Galaxy Astrophysics
Abstract: We report on polarimetric maps made with HAWC+/SOFIA toward œÅ Oph A, the densest portion of the œÅ Ophiuchi molecular complex. We employed HAWC+ bands C (89 Œºm) and D (154 Œºm). The slope of the polarization spectrum was investigated by defining the quantity {{ \mathcal R }}{DC}={p}D/{p}C, where p C and p D represent polarization degrees in bands C and D, respectively. We find a clear correlation between {{ \mathcal R }}{DC} and the molecular hydrogen column density across the cloud. A positive slope ({{ \mathcal R }}{DC} > 1) dominates the lower-density and well-illuminated portions of the cloud, which are heated by the high-mass star Oph S1, whereas a transition to a negative slope ({{ \mathcal R }}{DC} < 1) is observed toward the denser and less evenly illuminated cloud core. We interpret the trends as due to a combination of (1) warm grains at the cloud outskirts, which are efficiently aligned by the abundant exposure to radiation from Oph S1, as proposed in the radiative torques theory; and (2) cold grains deep in the cloud core, which are poorly aligned owing to shielding from external radiation. To assess this interpretation, we developed a very simple toy model using a spherically symmetric cloud core based on Herschel data and verified that the predicted variation of {{ \mathcal R }}{DC} is consistent with the observations. This result introduces a new method that can be used to probe the grain alignment efficiency in molecular clouds, based on the analysis of trends in the far-infrared polarization spectrum.
Published: 2019

88. HAWC+/SOFIA Multiwavelength Polarimetric Observations of OMC-1

Author: Chuss, D., Andersson, B., Bally, J., Dotson, J., Dowell, C., Guerra, J., Harper, D., Houde, M., Jones, T., Lazarian, A., Lopez Rodriguez, E., Michail, J., Morris, M., Novak, G., Siah, J., Staguhn, J., Vaillancourt, J., Volpert, C., Werner, M., Wollack, E., Benford, D., Berthoud, M., Cox, E., Crutcher, R., Dale, D., Fissel, L., Goldsmith, P., Hamilton, R., Hanany, S., Henning, T., Looney, L., Moseley, S., Santos, F., Stephens, I., Tassis, K., Trinh, C., Van Camp, E., Ward-Thompson, D., and Team, H.
Subjects: Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We report new polarimetric and photometric maps of the massive star- forming region OMC-1 using the HAWC+ instrument on the Stratospheric Observatory for Infrared Astronomy. We present continuum polarimetric and photometric measurements of this region at 53, 89, 154, and 214 Œºm at angular resolutions of 5‚Ä≥, 8‚Ä≥, 14‚Ä≥, and 19‚Ä≥ for the four bands, respectively. The photometric maps enable the computation of improved spectral energy distributions for the region. We find that at the longer wavelengths, the inferred magnetic field configuration matches the ‚Äúhourglass‚Äù configuration seen in previous studies, indicating magnetically regulated star formation. The field morphology differs at the shorter wavelengths. The magnetic field inferred at these wavelengths traces the bipolar structure of the explosive Becklin- Neugebauer/Kleinman-Low outflow emerging from OMC-1 behind the Orion Nebula. Using statistical methods to estimate the field strength in the region, we find that the explosion dominates the magnetic field near the center of the feature. Farther out, the magnetic field is close to energetic equilibrium with the ejecta and may be providing confinement to the explosion. The correlation between polarization fraction and the local polarization angle dispersion indicates that the depolarization as a function of unpolarized intensity is a result of intrinsic field geometry as opposed to decreases in grain alignment efficiency in denser regions.
Published: 2019

89. Demonstration of broadband anti-reflection coating on sapphire based on mm-wave sub-wavelength structures

Author: Takaku, R., primary, Katayama, N., additional, Mitsuda, K., additional, Yamasaki, N., additional, Komatsu, K., additional, Ishino, H., additional, Yumoto, J., additional, Kuwata-Gonokami, M., additional, Matsumura, T., additional, Sakurai, H., additional, Konishi, K., additional, Imada, H., additional, Hanany, S., additional, Young, K., additional, Wen, Q., additional, and Sakurai, Y., additional
Published: 2019
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90. Archeops: a high resolution, large sky coverage balloon experiment for mapping cosmic microwave background anisotropies

Author: Benoı̂t, A., Ade, P., Amblard, A., Ansari, R., Aubourg, E., Bartlett, J., Bernard, J.-P., Bhatia, R.S., Blanchard, A., Bock, J.J., Boscaleri, A., Bouchet, F.R., Bourrachot, A., Camus, P., Couchot, F., de Bernardis, P., Delabrouille, J., Désert, F.-X., Doré, O., Douspis, M., Dumoulin, L., Dupac, X., Filliatre, P., Ganga, K., Gannaway, F., Gautier, B., Giard, M., Giraud-Héraud, Y., Gispert, R., Guglielmi, L., Hamilton, J.-C., Hanany, S., Henrot-Versillé, S., Hristov, V.V., Kaplan, J., Lagache, G., Lamarre, J.-M., Lange, A.E., Madet, K., Maffei, B., Marrone, D., Masi, S., Murphy, J.A., Naraghi, F., Nati, F., Perrin, G., Piat, M., Puget, J.-L., Santos, D., Sudiwala, R.V., Vanel, J.-C., Vibert, D., Wakui, E., and Yvon, D.
Published: 2002
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91. Exploring cosmic origins with CORE: $B$-mode component separation

Author: Remazeilles , M., Banday , A.J., Baccigalupi , C., Basak , S., Bonaldi , A., De Zotti , G., Delabrouille , J., Dickinson , C., Eriksen , H.K., Errard , J., Fernandez-Cobos , R., Fuskeland , U., Hervías-Caimapo , C., López-Caniego , M., Martinez-González , E., Roman , M., Vielva , P., Wehus , I., Achucarro , A., Ade , P., Allison , R., Ashdown , M., Ballardini , M., Banerji , R., Bartolo , N., Bartlett , J., 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 , G., Challinor , A., Chluba , J., Clesse , S., Colantoni , I., Coppolecchia , A., Crook , M., D'Alessandro , G., De Bernardis , P., De Gasperis , G., Diego , J.M., Di Valentino , E., Feeney , S., Ferraro , S., Finelli , F., Forastieri , F., Galli , S., Genova-Santos , R., Gerbino , M., González-Nuevo , J., Grandis , S., Greenslade , J., Hagstotz , S., Hanany , S., Handley , W., Hernandez-Monteagudo , C., Hills , M., Hivon , E., Kiiveri , K., Kisner , T., Kitching , T., Kunz , M., Kurki-Suonio , H., Lamagna , L., Lasenby , A., Lattanzi , M., Lesgourgues , J., Lewis , A., Liguori , M., Lindholm , V., Luzzi , G., Maffei , B., Martins , C.J.A.P., Masi , S., McCarthy , D., Melin , J.B., 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., Rubino-Martin , J.A., Salvati , L., Tartari , A., Tomasi , M., Tramonte , D., Trappe , N., Trombetti , T., Tucker , C., Valiviita , J., Van de Weijgaert , R., Van Tent , B., Vennin , V., Vittorio , N., Young , K., Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Institut Lagrange de Paris, Sorbonne Universités, Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut d'astrophysique spatiale ( IAS ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut Néel ( NEEL ), Université Grenoble Alpes [Saint Martin d'Hères]-Centre National de la Recherche Scientifique ( CNRS ), Département de Physique des Particules (ex SPP) ( DPP ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Laboratoire d'Annecy-le-Vieux de Physique Théorique ( LAPTH ), Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique Théorique d'Orsay [Orsay] ( LPT ), Université Paris-Sud - Paris 11 ( UP11 ) -Centre National de la Recherche Scientifique ( CNRS ), and CORE
Subjects: satellite: Planck, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmology: observations, Astrophysics::Instrumentation and Methods for Astrophysics, hydrogen: recombination, cosmic background radiation: polarization, Astrophysics::Cosmology and Extragalactic Astrophysics, parametric, cosmic background radiation, methods: data analysis, B-mode: primordial, thermal, diffuse radiation, cosmic background radiation: B-mode, gravitation: lens, Polarization, infrared, ionization, synchrotron, microwaves: emission, spectral, galaxy, inflation, [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics::Galaxy Astrophysics
Abstract: International audience; We demonstrate that, for the baseline design of the CORE satellite mission, the polarized foregrounds can be controlled at the level required to allow the detection of the primordial cosmic microwave background (CMB) B-mode polarization with the desired accuracy at both reionization and recombination scales, for tensor-to-scalar ratio values of r 5× 10−3. We consider detailed sky simulations based on state-of-the-art CMB observations that consist of CMB polarization with τ=0.055 and tensor-to-scalar values ranging from r=10−2 to 10−3, Galactic synchrotron, and thermal dust polarization with variable spectral indices over the sky, polarized anomalous microwave emission, polarized infrared and radio sources, and gravitational lensing effects. Using both parametric and blind approaches, we perform full component separation and likelihood analysis of the simulations, allowing us to quantify both uncertainties and biases on the reconstructed primordial B-modes. Under the assumption of perfect control of lensing effects, CORE would measure an unbiased estimate of r=(5 ± 0.4)× 10−3 after foreground cleaning. In the presence of both gravitational lensing effects and astrophysical foregrounds, the significance of the detection is lowered, with CORE achieving a 4σ-measurement of r=5× 10−3 after foreground cleaning and 60% delensing. For lower tensor-to-scalar ratios (r=10−3) the overall uncertainty on r is dominated by foreground residuals, not by the 40% residual of lensing cosmic variance. Moreover, the residual contribution of unprocessed polarized point-sources can be the dominant foreground contamination to primordial B-modes at this r level, even on relatively large angular scales, &ell; ~ 50. Finally, we report two sources of potential bias for the detection of the primordial B-modes by future CMB experiments: (i) the use of incorrect foreground models, e.g. a modelling error of Δβs = 0.02 on the synchrotron spectral indices may result in an excess in the recovered reionization peak corresponding to an effective Δ r > 10−3; (ii) the average of the foreground line-of-sight spectral indices by the combined effects of pixelization and beam convolution, which adds an effective curvature to the foreground spectral energy distribution and may cause spectral degeneracies with the CMB in the frequency range probed by the experiment.
Published: 2018
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92. Exploring Cosmic Origins with CORE: Cluster Science

Author: 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., Achúcarro, A., Ade, P.A.R., Allison, R., Ashdown, M., Ballardini, M., Banday, A.J., Banerji, R., Bartolo, N., Basak, S., Baselmans, J., Basu, K., Battye, R.A., Baumann, D., Bersanelli, M., Bonato, M., Borrill, J., Bouchet, F.R., 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, Giuseppe, De Bernardis, P., de Gasperis, G., De Petris, M., de Zotti, G., Di Valentino, E., Errard, J., 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.S., Kitching, T., Kunz, M., Kurki-Suonio, H., Lamagna, L., Lasenby, A., Lattanzi, M., Le Brun, A.M.C., Lesgourgues, J., Lewis, A., Liguori, M., Lindholm, V., Lopez-Caniego, M., Maffei, B., Martinez-Gonzalez, E., Masi, S., 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, Neil, Triqueneaux, S., Trombetti, T., Tucker, C., Valiviita, J., van de Weygaert, R., Van Tent, B., Vennin, V., Vielva, P., Vittorio, N., Weller, J., Young, K., and Zannoni, M.
Subjects: Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract: We 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-σ sensitivity of 4 × 1014M, for a 120 cm aperture telescope, and 1014M 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 from Atacama would be shallower than CORE and detect about 11,000 clusters, while a survey from the South Pole 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 such a South Pole survey, CORE would reach a limiting mass of M500 ∼ 2 − 3 × 1013Mand 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 (σw0 = 0.28, σwa = 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, Σmν, to 39 meV (1 sigma). The wide frequency coverage of CORE, 60 - 600 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 foreground-cleaned CMB map. Measurements of TCMB(z) using CORE clusters will establish competitive constraints on the evolution of the CMB temperature: (1+z) 1−β , with an uncertainty of σβ . 2.7×10−3 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 σ8 over the Planck result, demonstrating the potential of this cosmological probe with CORE.
Published: 2018

93. Exploring Cosmic Origins with CORE: Extragalactic sources in Cosmic Microwave Background maps

Author: Zotti, G. De, González-Nuevo, J., Lopez-Caniego, M., Negrello, M., Greenslade, J., Hernández-Monteagudo, C., Delabrouille, J., Cai, Z. -Y., Bonato, M., Achúcarro, A., Ade, P., Allison, R., Ashdown, M., Ballardini, M., Banday, A. J., Banerji, R., Bartlett, J. G., Bartolo, N., Basak, S., Bersanelli, M., Biesiada, M., Bilicki, M., Bonaldi, A., Bonavera, L., Borrill, J., Bouchet, F., Boulanger, F., Brinckmann, T., Bucher, M., Burigana, C., Buzzelli, A., Calvo, M., Carvalho, C. S., Castellano, M. G., Challinor, A., Chluba, J., Clements, D. L., Clesse, S., Colafrancesco, S., Colantoni, I., Coppolecchia, A., Crook, M., D'Alessandro, G., De Bernardis, P., De Gasperis, G., Diego, J. M., Valentino, E. Di, Errard, J., Feeney, S. M., Fernández-Cobos, R., Ferraro, S., Finelli, F., Forastieri, F., Galli, S., Génova-Santos, R. T., Gerbino, M., Grandis, S., Hagstotz, S., Hanany, S., Handley, W., Hervias-Caimapo, C., Hills, M., Hivon, E., Kiiveri, K., Kisner, T., Kitching, T., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamagna, L., Lasenby, A., Lattanzi, M., Brun, A. Le, Lesgourgues, J., Lewis, A., Liguori, M., Lindholm, V., Luzzi, G., Maffei, B., Mandolesi, N., Martinez-Gonzalez, E., Martins, C. J. A. P., Masi, S., Massardi, M., Matarrese, S., Mccarthy, D., Melchiorri, A., Melin, J. -B., Molinari, D., Monfardini, A., Natoli, P., Notari, A., Paiella, A., Paoletti, D., Partridge, R. B., Patanchon, G., Piat, M., Pisano, G., Polastri, L., Polenta, G., Pollo, A., Poulin, V., Quartin, M., Remazeilles, M., Roman, M., Rossi, G., Roukema, B. F., Rubiño-Martín, J. -A., Salvati, L., Scott, D., Serjeant, S., Tartari, A., Toffolatti, L., Tomasi, M., Trappe, N., Triqueneaux, S., Trombetti, T., Tucci, M., Tucker, C., Väliviita, J., De Weygaert, R. Van, Tent, B. Van, Vennin, V., Vielva, P., Vittorio, N., Young, K., Zannoni, M., D'Alessandro, Giuseppe, AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut d'astrophysique spatiale ( IAS ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut Néel ( NEEL ), Université Grenoble Alpes [Saint Martin d'Hères]-Centre National de la Recherche Scientifique ( CNRS ), Institut Lagrange de Paris, Sorbonne Universités, Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Astrophysique de Marseille ( LAM ), Aix Marseille Université ( AMU ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National d'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire AIM, Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay, Département de Physique des Particules (ex SPP) ( DPP ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Laboratoire d'Annecy-le-Vieux de Physique Théorique ( LAPTH ), Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique Théorique d'Orsay [Orsay] ( LPT ), Université Paris-Sud - Paris 11 ( UP11 ) -Centre National de la Recherche Scientifique ( CNRS ), CORE, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Cryogénie (NEEL - Cryo), Institut Néel (NEEL), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Hélium : du fondamental aux applications (NEEL - HELFA), Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Zotti, G, González-Nuevo, J, Lopez-Caniego, M, Negrello, M, Greenslade, J, Hernández-Monteagudo, C, Delabrouille, J, Cai, Z, Bonato, M, Achúcarro, A, Ade, P, Allison, R, Ashdown, M, Ballardini, M, Banday, A, Banerji, R, Bartlett, J, Bartolo, N, Basak, S, Bersanelli, M, Biesiada, M, Bilicki, M, Bonaldi, A, Bonavera, L, Borrill, J, Bouchet, F, Boulanger, F, Brinckmann, T, Bucher, M, Burigana, C, Buzzelli, A, Calvo, M, Carvalho, C, Castellano, M, Challinor, A, Chluba, J, Clements, D, Clesse, S, Colafrancesco, S, Colantoni, I, Coppolecchia, A, Crook, M, D'Alessandro, G, de Bernardis, P, de Gasperis, G, Diego, J, Valentino, E, Errard, J, Feeney, S, Fernández-Cobos, R, Ferraro, S, Finelli, F, Forastieri, F, Galli, S, Génova-Santos, R, Gerbino, M, Grandis, S, Hagstotz, S, Hanany, S, Handley, W, Hervias-Caimapo, C, Hills, M, Hivon, E, Kiiveri, K, Kisner, T, Kitching, T, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamagna, L, Lasenby, A, Lattanzi, M, Brun, A, Lesgourgues, J, Lewis, A, Liguori, M, Lindholm, V, Luzzi, G, Maffei, B, Mandolesi, N, Martinez-Gonzalez, E, Martins, C, Masi, S, Massardi, M, Matarrese, S, Mccarthy, D, Melchiorri, A, Melin, J, Molinari, D, Monfardini, A, Natoli, P, Notari, A, Paiella, A, Paoletti, D, Partridge, R, Patanchon, G, Piat, M, Pisano, G, Polastri, L, Polenta, G, Pollo, A, Poulin, V, Quartin, M, Remazeilles, M, Roman, M, Rossi, G, Roukema, B, Rubiño-Martín, J, Salvati, L, Scott, D, Serjeant, S, Tartari, A, Toffolatti, L, Tomasi, M, Trappe, N, Triqueneaux, S, Trombetti, T, Tucci, M, Tucker, C, Väliviita, J, de Weygaert, R, Tent, B, Vennin, V, Vielva, P, Vittorio, N, Young, K, Zannoni, M, Astronomy, Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Département de Physique des Particules (ex SPP) (DPP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Sorbonne Université (SU), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Science and Technology Facilities Council (STFC), Science and Technology Facilities Council, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Helsinki Institute of Physics, and Department of Physics
Subjects: LENSED GALAXIES, Brightness, POLARIZATION, active galactic nuclei, CMBR experiments, galaxy evolution, galaxy surveys, POINT SOURCES, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmic microwave background, galaxy evolution, Astrophysics, CMB, 01 natural sciences, Physics, Particles & Fields, law.invention, law, CMBR experiments, galaxy surveys, 010303 astronomy & astrophysics, QC, QB, Physics, COSMIC cancer database, Nuclear & Particles Physics, PLANCK, COMPACT SOURCE CATALOG, ALL-SKY SURVEY, Physical Sciences, astro-ph.CO, symbols, GALAXY FORMATION, CMBR experiment, Astrophysics - Cosmology and Nongalactic Astrophysics, RADIO-SOURCES, Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxy survey, astro-ph.GA, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, NO, Telescope, symbols.namesake, FIS/05 - ASTRONOMIA E ASTROFISICA, 0202 Atomic, Molecular, Nuclear, Particle And Plasma Physics, Settore FIS/05 - Astronomia e Astrofisica, active galactic nuclei, Astronomy and Astrophysics, 0103 physical sciences, Planck, Astrophysics::Galaxy Astrophysics, HERSCHEL, Science & Technology, 010308 nuclear & particles physics, Star formation, HERSCHEL-ATLAS, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, EVOLUTION, 0201 Astronomical And Space Sciences, LUMINOSITY FUNCTION, Astrophysics of Galaxies (astro-ph.GA), SKY, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Work supported in part by ASI/INAF agreement n. 2014-024-R.1 and by PRIN–INAF 2014 “Probing the AGN/galaxy co-evolution through ultra-deep and ultra-high resolution radio surveys”. JGN acknowledges financial support from the Spanish MINECO for a “Ramon y Cajal” fellowship (RYC-2013-13256) and the I+D 2015 project AYA2015-65887-P (MINECO/FEDER). CH-M acknowledges the financial support of the Spanish MINECO through I+D project AYA-2015-66211-C2-2-P. MB is supported by the Netherlands Organization for Scientific Research, NWO, through grant number 614.001.451, and by the Polish National Science Centre under contract UMO-2012/07/D/ST9/02785. CJM is supported by an FCT Research Professorship, contract reference IF/00064/2012, funded by FCT/MCTES (Portugal) and POPH/FSE (EC). GR acknowledges support from the National Research Foundation of Korea (NRF) through NRF-SGER 2014055950 funded by the Korean Ministry of Education, Science and Technology (MoEST), and from the faculty research fund of Sejong University in 2016., Zotti, G.D., González-Nuevo, J., Lopez-Caniego, M., Negrello, M., Greenslade, J., Hernández-Monteagudo, C., Delabrouille, J., Cai, Z.-Y., Bonato, M., Achúcarro, A., Ade, P., Allison, R., Ashdown, M., Ballardini, M., Banday, A.J., Banerji, R., Bartlett, J.G., Bartolo, N., Basak, S., Bersanelli, M., Biesiada, M., Bilicki, M., Bonaldi, A., Bonavera, L., Borrill, J., Bouchet, F., Boulanger, F., Brinckmann, T., Bucher, M., Burigana, C., Buzzelli, A., Calvo, M., Carvalho, C.S., Castellano, M.G., Challinor, A., Chluba, J., Clements, D.L., Clesse, S., Colafrancesco, S., Colantoni, I., Coppolecchia, A., Crook, M., D'Alessandro, G., De Bernardis, P., De Gasperis, G., Diego, J.M., Valentino, E.D., Errard, J., Feeney, S.M., Fernández-Cobos, R., Ferraro, S., Finelli, F., Forastieri, F., Galli, S., Génova-Santos, R.T., Gerbino, M., Grandis, S., Hagstotz, S., Hanany, S., Handley, W., Hervias-Caimapo, C., Hills, M., Hivon, E., Kiiveri, K., Kisner, T., Kitching, T., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamagna, L., Lasenby, A., Lattanzi, M., Brun, A.L., Lesgourgues, J., Lewis, A., Liguori, M., Lindholm, V., Luzzi, G., Maffei, B., Mandolesi, N., Martinez-Gonzalez, E., Martins, C.J.A.P., Masi, S., Massardi, M., Matarrese, S., McCarthy, D., Melchiorri, A., Melin, J.-B., Molinari, D., Monfardini, A., Natoli, P., Notari, A., Paiella, A., Paoletti, D., Partridge, R.B., Patanchon, G., Piat, M., Pisano, G., Polastri, L., Polenta, G., Pollo, A., Poulin, V., Quartin, M., Remazeilles, M., Roman, M., Rossi, G., Roukema, B.F., Rubiño-Martín, J.-A., Salvati, L., Scott, D., Serjeant, S., Tartari, A., Toffolatti, L., Tomasi, M., Trappe, N., Triqueneaux, S., Trombetti, T., Tucci, M., Tucker, C., Väliviita, J., De Weygaert, R.V., Tent, B.V., Vennin, V., Vielva, P., Vittorio, N., Young, K., Zannoni, M.
Published: 2016
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94. On the vectorial photoelectric effect at 2.69 keV

Author: Shaw, P. S, Hanany, S, Liu, Y, Church, E. D, Fleischman, J, Kaaret, P, Novick, R, and Santangelo, A
Subjects: Electronics And Electrical Engineering
Abstract: Recent experiments conducted to study the vectorial photoelectric effect with CsI, Al2O3 and Si photocathodes at 2.69 keV indicate null results. Detailed analysis shows that previously measured modulation can be well explained by geometrical misalignment and a combination of the asymmetric shape of the incident X-ray beam and a small detection area of the photoelectron detector. After the elimination of the sources of spurious modulation, we observed a modulation factor of less than 3 percent for a grazing incidence angle as small as 5 deg. There is no observable difference in the pulse height distribution between s and p states.
Published: 1991

95. Status of the Stellar X-Ray Polarimeter for the Spectrum-X-Gamma mission

Author: Kaaret, P, Novick, R, Shaw, P, Hanany, S, Liu, Y, Fleischman, J. R, Siuniaev, R, Lapshov, I, Weisskopf, M. C, and Elsner, R. F
Subjects: Spacecraft Instrumentation
Abstract: The Stellar X-Ray Polarimeter (SXRP) uses the polarization sensitivity of a graphite Bragg crystal and a lithium Thomsom scattering target to measure the polarization of X-rays from astrophysical sources. The SXRP is a focal plane detector for the Soviet-Danish SODART telescopes which will be launched on the Soviet Spectrum-X-Gamma mission. The SXRP will be the third orbiting stellar X-ray polarimeter, and should provide an order of magnitude increase in polarization sensitivity over its predecessors.
Published: 1991

96. Exploring cosmic origins with CORE:B-mode component separation

Author: Remazeilles, M., primary, Banday, A.J., additional, Baccigalupi, C., additional, Basak, S., additional, Bonaldi, A., additional, Zotti, G. De, additional, Delabrouille, J., additional, Dickinson, C., additional, Eriksen, H. K., additional, Errard, J., additional, Fernandez-Cobos, R., additional, Fuskeland, U., additional, Hervías-Caimapo, C., additional, López-Caniego, M., additional, Martinez-González, E., additional, Roman, M., additional, Vielva, P., additional, Wehus, I., additional, Achucarro, A., additional, Ade, P., additional, Allison, R., additional, Ashdown, M., additional, Ballardini, M., additional, Banerji, R., additional, Bartlett, J., additional, Bartolo, N., additional, Baumann, D., additional, Bersanelli, M., additional, Bonato, M., additional, Borrill, J., additional, Bouchet, F., additional, Boulanger, F., additional, Brinckmann, T., additional, Bucher, M., additional, Burigana, C., additional, Buzzelli, A., additional, Cai, Z.-Y., additional, Calvo, M., additional, Carvalho, C.-S., additional, Castellano, G., additional, Challinor, A., additional, Chluba, J., additional, Clesse, S., additional, Colantoni, I., additional, Coppolecchia, A., additional, Crook, M., additional, D'Alessandro, G., additional, de Bernardis, P., additional, de Gasperis, G., additional, Diego, J.-M., additional, Valentino, E. Di, additional, Feeney, S., additional, Ferraro, S., additional, Finelli, F., additional, Forastieri, F., additional, Galli, S., additional, Genova-Santos, R., additional, Gerbino, M., additional, González-Nuevo, J., additional, Grandis, S., additional, Greenslade, J., additional, Hagstotz, S., additional, Hanany, S., additional, Handley, W., additional, Hernandez-Monteagudo, C., additional, Hills, M., additional, Hivon, E., additional, Kiiveri, K., additional, Kisner, T., additional, Kitching, T., additional, Kunz, M., additional, Kurki-Suonio, H., additional, Lamagna, L., additional, Lasenby, A., additional, Lattanzi, M., additional, Lesgourgues, J., additional, Lewis, A., additional, Liguori, M., additional, Lindholm, V., additional, Luzzi, G., additional, Maffei, B., additional, Martins, C.J.A.P., additional, Masi, S., additional, Matarrese, S., additional, McCarthy, D., additional, Melin, J.-B., additional, Melchiorri, A., additional, Molinari, D., additional, Monfardini, A., additional, Natoli, P., additional, Negrello, M., additional, Notari, A., additional, Paiella, A., additional, Paoletti, D., additional, Patanchon, G., additional, Piat, M., additional, Pisano, G., additional, Polastri, L., additional, Polenta, G., additional, Pollo, A., additional, Poulin, V., additional, Quartin, M., additional, Rubino-Martin, J.-A., additional, Salvati, L., additional, Tartari, A., additional, Tomasi, M., additional, Tramonte, D., additional, Trappe, N., additional, Trombetti, T., additional, Tucker, C., additional, Valiviita, J., additional, de Weijgaert, R. Van, additional, Tent, B. van, additional, Vennin, V., additional, Vittorio, N., additional, Young, K., additional, and Zannoni, M., additional
Published: 2018
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97. Exploring cosmic origins with CORE: Cosmological parameters

Author: Valentino, E. Di, primary, Brinckmann, T., additional, Gerbino, M., additional, Poulin, V., additional, Bouchet, F.R., additional, Lesgourgues, J., additional, Melchiorri, A., additional, Chluba, J., additional, Clesse, S., additional, Delabrouille, J., additional, Dvorkin, C., additional, Forastieri, F., additional, Galli, S., additional, Hooper, D.C., additional, Lattanzi, M., additional, Martins, C.J.A.P., additional, Salvati, L., additional, Cabass, G., additional, Caputo, A., additional, Giusarma, E., additional, Hivon, E., additional, Natoli, P., additional, Pagano, L., additional, Paradiso, S., additional, Rubiño-Martin, J.A., additional, Achúcarro, A., additional, Ade, P., additional, Allison, R., additional, Arroja, F., additional, Ashdown, M., additional, Ballardini, M., additional, Banday, A.J., additional, Banerji, R., additional, Bartolo, N., additional, Bartlett, J.G., additional, Basak, S., additional, Baumann, D., additional, de Bernardis, P., additional, Bersanelli, M., additional, Bonaldi, A., additional, Bonato, M., additional, Borrill, J., additional, Boulanger, F., additional, Bucher, M., additional, Burigana, C., additional, Buzzelli, A., additional, Cai, Z.-Y., additional, Calvo, M., additional, Carvalho, C.S., additional, Castellano, G., additional, Challinor, A., additional, Charles, I., additional, Colantoni, I., additional, Coppolecchia, A., additional, Crook, M., additional, D'Alessandro, G., additional, Petris, M. De, additional, Zotti, G. De, additional, Diego, J.M., additional, Errard, J., additional, Feeney, S., additional, Fernandez-Cobos, R., additional, Ferraro, S., additional, Finelli, F., additional, de Gasperis, G., additional, Génova-Santos, R.T., additional, González-Nuevo, J., additional, Grandis, S., additional, Greenslade, J., additional, Hagstotz, S., additional, Hanany, S., additional, Handley, W., additional, Hazra, D.K., additional, Hernández-Monteagudo, C., additional, Hervias-Caimapo, C., additional, Hills, M., additional, Kiiveri, K., additional, Kisner, T., additional, Kitching, T., additional, Kunz, M., additional, Kurki-Suonio, H., additional, Lamagna, L., additional, Lasenby, A., additional, Lewis, A., additional, Liguori, M., additional, Lindholm, V., additional, Lopez-Caniego, M., additional, Luzzi, G., additional, Maffei, B., additional, Martin, S., additional, Martinez-Gonzalez, E., additional, Masi, S., additional, Matarrese, S., additional, McCarthy, D., additional, Melin, J.-B., additional, Mohr, J.J., additional, Molinari, D., additional, Monfardini, A., additional, Negrello, M., additional, Notari, A., additional, Paiella, A., additional, Paoletti, D., additional, Patanchon, G., additional, Piacentini, F., additional, Piat, M., additional, Pisano, G., additional, Polastri, L., additional, Polenta, G., additional, Pollo, A., additional, Quartin, M., additional, Remazeilles, M., additional, Roman, M., additional, Ringeval, C., additional, Tartari, A., additional, Tomasi, M., additional, Tramonte, D., additional, Trappe, N., additional, Trombetti, T., additional, Tucker, C., additional, Väliviita, J., additional, de Weygaert, R. van, additional, Tent, B. Van, additional, Vennin, V., additional, Vermeulen, G., additional, Vielva, P., additional, Vittorio, N., additional, Young, K., additional, and Zannoni, M., additional
Published: 2018
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98. Exploring cosmic origins with CORE : Extragalactic sources in cosmic microwave background maps

Author: De Zotti, G., Gonzalez-Nuevo, J., Lopez-Caniego, M., Negrello, M., Greenslade, J., Hernandez-Monteagudo, C., Delabrouille, J., Cai, Z-Y., Bonato, M., Achucarro, A., Ade, P., Allison, R., Ashdown, M., Ballardini, M., Banday, A. J., Banerji, R., Bartlett, J. G., Bartolo, N., Basak, S., Bersanelli, M., Biesiada, M., Bilicki, M., Bonaldi, A., Bonavera, L., Borrill, J., Bouchet, F., Boulanger, F., Brinckmann, T., Bucher, M., Burigana, C., Buzzelli, A., Calvo, M., Carvalho, C. S., Castellano, M. G., Challinor, A., Chluba, J., Clements, D. L., Clesse, S., Colafrancesco, S., Colantoni, I., Coppolecchia, A., Crook, M., D'Alessandro, G., de Bernardis, P., de Gasperis, G., Diego, J. M., Di Valentino, E., Errard, J., Feeney, S. M., Fernandez-Cobos, R., Ferraro, S., Finelli, F., Forastieri, F., Galli, S., Genova-Santos, R. T., Gerbino, Martina, Grandis, S., Hagstotz, S., Hanany, S., Handley, W., Hervias-Caimapo, C., Hills, M., Hivon, E., Kiiveri, K., Kisner, T., Kitching, T., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamagna, L., Lasenby, A., Lattanzi, M., Le Brun, A., Lesgourgues, J., Lewis, A., Liguori, M., Lindholm, V., Luzzi, G., Maffei, B., Mandolesi, N., Martinez-Gonzalez, E., Martins, C. J. A. P., Masi, S., Massardi, M., Matarrese, S., McCarthy, D., Melchiorri, A., Melin, J-B., Molinari, D., Monfardini, A., Natoli, P., Notari, A., Paiella, A., Paoletti, D., Partridge, R. B., Patanchon, G., Piat, M., Pisano, G., Polastri, L., Polenta, G., Pollo, A., Poulin, V., Quartin, M., Remazeilles, M., Roman, M., Rossi, G., Roukema, B. F., Rubino-Martin, J-A., Salvati, L., Scott, D., Serjeant, S., Tartari, A., Toffolatti, L., Tomasi, M., Trappe, N., Triqueneaux, S., Trombetti, T., Tucci, M., Tucker, C., Valiviita, J., van de Weygaert, R., Van Tent, B., Vennin, V., Vielva, P., Vittorio, N., Young, K., Zannoni, M., De Zotti, G., Gonzalez-Nuevo, J., Lopez-Caniego, M., Negrello, M., Greenslade, J., Hernandez-Monteagudo, C., Delabrouille, J., Cai, Z-Y., Bonato, M., Achucarro, A., Ade, P., Allison, R., Ashdown, M., Ballardini, M., Banday, A. J., Banerji, R., Bartlett, J. G., Bartolo, N., Basak, S., Bersanelli, M., Biesiada, M., Bilicki, M., Bonaldi, A., Bonavera, L., Borrill, J., Bouchet, F., Boulanger, F., Brinckmann, T., Bucher, M., Burigana, C., Buzzelli, A., Calvo, M., Carvalho, C. S., Castellano, M. G., Challinor, A., Chluba, J., Clements, D. L., Clesse, S., Colafrancesco, S., Colantoni, I., Coppolecchia, A., Crook, M., D'Alessandro, G., de Bernardis, P., de Gasperis, G., Diego, J. M., Di Valentino, E., Errard, J., Feeney, S. M., Fernandez-Cobos, R., Ferraro, S., Finelli, F., Forastieri, F., Galli, S., Genova-Santos, R. T., Gerbino, Martina, Grandis, S., Hagstotz, S., Hanany, S., Handley, W., Hervias-Caimapo, C., Hills, M., Hivon, E., Kiiveri, K., Kisner, T., Kitching, T., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamagna, L., Lasenby, A., Lattanzi, M., Le Brun, A., Lesgourgues, J., Lewis, A., Liguori, M., Lindholm, V., Luzzi, G., Maffei, B., Mandolesi, N., Martinez-Gonzalez, E., Martins, C. J. A. P., Masi, S., Massardi, M., Matarrese, S., McCarthy, D., Melchiorri, A., Melin, J-B., Molinari, D., Monfardini, A., Natoli, P., Notari, A., Paiella, A., Paoletti, D., Partridge, R. B., Patanchon, G., Piat, M., Pisano, G., Polastri, L., Polenta, G., Pollo, A., Poulin, V., Quartin, M., Remazeilles, M., Roman, M., Rossi, G., Roukema, B. F., Rubino-Martin, J-A., Salvati, L., Scott, D., Serjeant, S., Tartari, A., Toffolatti, L., Tomasi, M., Trappe, N., Triqueneaux, S., Trombetti, T., Tucci, M., Tucker, C., Valiviita, J., van de Weygaert, R., Van Tent, B., Vennin, V., Vielva, P., Vittorio, N., Young, K., and Zannoni, M.
Abstract: We discuss the potential of a next generation space-borne Cosmic Microwave Background (CMB) experiment for studies of extragalactic sources. Our analysis has particular bearing on the definition of the future space project, CORE, that has been submitted in response to ESA's call for a Medium-size mission opportunity as the successor of the Planck satellite. Even though the effective telescope size will be somewhat smaller than that of Planck, CORE will have a considerably better angular resolution at its highest frequencies, since, in contrast with Planck, it will be diffraction limited at all frequencies. The improved resolution implies a considerable decrease of the source confusion, i.e. substantially fainter detection limits. In particular, CORE will detect thousands of strongly lensed high-z galaxies distributed over the full sky. The extreme brightness of these galaxies will make it possible to study them, via follow-up observations, in extraordinary detail. Also, the CORE resolution matches the typical sizes of high-z galaxy proto-clusters much better than the Planck resolution, resulting in a much higher detection efficiency; these objects will be caught in an evolutionary phase beyond the reach of surveys in other wavebands. Furthermore, CORE will provide unique information on the evolution of the star formation in virialized groups and clusters of galaxies up to the highest possible redshifts. Finally, thanks to its very high sensitivity, CORE will detect the polarized emission of thousands of radio sources and, for the first time, of dusty galaxies, at mm and sub-mm wavelengths, respectively.
Published: 2018
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99. Exploring cosmic origins with CORE : Cosmological parameters

Author: Di Valentino, E., Brinckmann, T., Gerbino, Martina, Poulin, V., Bouchet, F. R., Lesgourgues, J., Melchiorri, A., Chluba, J., Clesse, S., Delabrouille, J., Dvorkin, C., Forastieri, F., Galli, S., Hooper, D. C., Lattanzi, M., Martins, C. J. A. P., Salvati, L., Cabass, G., Caputo, A., Giusarma, E., Hivon, E., Natoli, P., Pagano, L., Paradiso, S., Rubino-Martin, J. A., Achucarro, A., Ade, P., Allison, R., Arroja, F., Ashdown, M., Ballardini, M., Banday, A. J., Banerji, R., Bartolo, N., Bartlett, J. G., Basak, S., Baumann, D., de Bernardis, P., Bersanelli, M., Bonaldi, A., Bonato, M., Borrill, J., Boulanger, F., Bucher, M., Burigana, C., Buzzelli, A., Cai, Z. -Y., Calvo, M., Carvalho, C. S., Castellano, G., Challinor, A., Charles, I., Colantoni, I., Coppolecchia, A., Crook, M., D'Alessandro, G., De Petris, M., De Zotti, G., Diego, J. M., Errard, J., Feeney, S., Fernandez-Cobos, R., Ferraro, S., Finelli, F., de Gasperis, G., Genova-Santos, R. T., Gonzalez-Nuevo, J., Grandis, S., Greenslade, J., Hagstotz, S., Hanany, S., Handley, W., Hazra, D. K., Hernandez-Monteagudo, C., Hervias-Caimapo, C., Hills, M., Kiiveri, K., Kisner, T., Kitching, T., Kunz, M., Kurki-Suonio, H., Lamagna, L., Lasenby, A., Lewis, A., Liguori, M., Lindholm, V., Lopez-Caniego, M., Luzzi, G., Maffei, B., Martin, S., Martinez-Gonzalez, E., Masi, S., Matarrese, S., McCarthy, D., Melin, J. -B., Mohr, J. J., Molinari, D., Monfardini, A., Negrello, M., Notari, A., Paiella, A., Paoletti, D., Patanchon, G., Piacentini, F., Piat, M., Pisano, G., Polastri, L., Polenta, G., Pollo, A., Quartin, M., Remazeilles, M., Roman, M., Ringeval, C., Tartari, A., Tomasi, M., Tramonte, D., Trappe, N., Trombetti, T., Tucker, C., Valiviita, J., van de Weygaert, R., Van Tent, B., Vennin, V., Vermeulen, G., Vielva, P., Vittorio, N., Young, K., Zannoni, M., Di Valentino, E., Brinckmann, T., Gerbino, Martina, Poulin, V., Bouchet, F. R., Lesgourgues, J., Melchiorri, A., Chluba, J., Clesse, S., Delabrouille, J., Dvorkin, C., Forastieri, F., Galli, S., Hooper, D. C., Lattanzi, M., Martins, C. J. A. P., Salvati, L., Cabass, G., Caputo, A., Giusarma, E., Hivon, E., Natoli, P., Pagano, L., Paradiso, S., Rubino-Martin, J. A., Achucarro, A., Ade, P., Allison, R., Arroja, F., Ashdown, M., Ballardini, M., Banday, A. J., Banerji, R., Bartolo, N., Bartlett, J. G., Basak, S., Baumann, D., de Bernardis, P., Bersanelli, M., Bonaldi, A., Bonato, M., Borrill, J., Boulanger, F., Bucher, M., Burigana, C., Buzzelli, A., Cai, Z. -Y., Calvo, M., Carvalho, C. S., Castellano, G., Challinor, A., Charles, I., Colantoni, I., Coppolecchia, A., Crook, M., D'Alessandro, G., De Petris, M., De Zotti, G., Diego, J. M., Errard, J., Feeney, S., Fernandez-Cobos, R., Ferraro, S., Finelli, F., de Gasperis, G., Genova-Santos, R. T., Gonzalez-Nuevo, J., Grandis, S., Greenslade, J., Hagstotz, S., Hanany, S., Handley, W., Hazra, D. K., Hernandez-Monteagudo, C., Hervias-Caimapo, C., Hills, M., Kiiveri, K., Kisner, T., Kitching, T., Kunz, M., Kurki-Suonio, H., Lamagna, L., Lasenby, A., Lewis, A., Liguori, M., Lindholm, V., Lopez-Caniego, M., Luzzi, G., Maffei, B., Martin, S., Martinez-Gonzalez, E., Masi, S., Matarrese, S., McCarthy, D., Melin, J. -B., Mohr, J. J., Molinari, D., Monfardini, A., Negrello, M., Notari, A., Paiella, A., Paoletti, D., Patanchon, G., Piacentini, F., Piat, M., Pisano, G., Polastri, L., Polenta, G., Pollo, A., Quartin, M., Remazeilles, M., Roman, M., Ringeval, C., Tartari, A., Tomasi, M., Tramonte, D., Trappe, N., Trombetti, T., Tucker, C., Valiviita, J., van de Weygaert, R., Van Tent, B., Vennin, V., Vermeulen, G., Vielva, P., Vittorio, N., Young, K., and Zannoni, M.
Abstract: We forecast the main cosmological parameter constraints achievable with the CORE space mission which is dedicated to mapping the polarisation of the Cosmic Microwave Background (CMB). CORE was recently submitted in response to ESA's fifth call for medium-sized mission proposals (M5). Here we report the results from our pre-submission study of the impact of various instrumental options, in particular the telescope size and sensitivity level, and review the great, transformative potential of the mission as proposed. Specifically, we assess the impact on a broad range of fundamental parameters of our Universe as a function of the expected CMB characteristics, with other papers in the series focusing on controlling astrophysical and instrumental residual systematics. In this paper, we assume that only a few central CORE frequency channels are usable for our purpose, all others being devoted to the cleaning of astrophysical contaminants. On the theoretical side, we assume ACDM as our general framework and quantify the improvement provided by CORE over the current constraints from the Planck 2015 release. We also study the joint sensitivity of CORE and of future Baryon Acoustic Oscillation and Large Scale Structure experiments like DESI and Euclid. Specific constraints on the physics of inflation are presented in another paper of the series. In addition to the six parameters of the base ACDM, which describe the matter content of a spatially flat universe with adiabatic and scalar primordial fluctuations from inflation, we derive the precision achievable on parameters like those describing curvature, neutrino physics, extra light relics, primordial helium abundance, dark matter annihilation, recombination physics, variation of fundamental constants, dark energy, modified gravity, reionization and cosmic birefringence. In addition to assessing the improvement on the precision of individual parameters, we also forecast the post-CORE overall reduction of the allowed parameter
Published: 2018
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100. Exploring cosmic origins with CORE : Survey requirements and mission design

Author: Delabrouille, J., de Bernardis, P., Bouchet, F. R., Achucarro, A., Ade, P. A. R., Allison, R., Arroja, F., Artal, E., Ashdown, M., Baccigalupi, C., Ballardini, M., Banday, A. J., Banerji, R., Barbosa, D., Bartlett, J., Bartolo, N., Basak, S., Baselmans, J. J. A., Basu, K., Battistelli, E. S., Battye, R., Baumann, D., Benoit, A., Bersanelli, M., Bideaud, A., Biesiada, M., Bilicki, M., Bonaldi, A., Bonato, M., Borrill, J., Boulanger, F., Brinckmann, T., Brown, M. L., Bucher, M., Burigana, C., Buzzelli, A., Cabass, G., Cai, Z. -Y., Calvo, M., Caputo, A., Carvalho, C. -S., Casas, F. J., Castellano, G., Catalano, A., Challinor, A., Charles, I., Chluba, J., Clements, D. L., Clesse, S., Colafrancesco, S., Colantoni, I., Contreras, D., Coppolecchia, A., Crook, M., D'Alessandro, G., D'Amico, G., da Silva, A., de Avillez, M., de Gasperis, G., De Petris, M., de Zotti, G., Danese, L., Desert, F. -X., Desjacques, V., Di Valentino, E., Dickinson, C., Diego, J. M., Doyle, S., Durrer, R., Dvorkin, C., Eriksen, H. K., Errard, J., Feeney, S., Fernandez-Cobos, R., FineIli, F., Forastieri, F., Franceschet, C., Fuskeland, U., Galli, S., Genova-Santos, R. T., Gerbino, Martina, Giusarma, E., Gomez, A., Gonzalez-Nuevo, J., Grandis, S., Greenslade, J., Goupy, J., Hagstotz, S., Hanany, S., Handley, W., Henrot-Versille, S., Hernandez-Monteagudo, C., Hervias-Caimapo, C., Hills, M., Hindmarsh, M., Hivon, E., Hoang, D. T., Hooper, D. C., Hu, B., Keihanen, E., Keskitalo, R., Kiiveri, K., Kisner, T., Kitching, T., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamagna, L., Lapi, A., Lasenby, A., Lattanzi, M., Le Brun, A. M. C., Lesgourgues, J., Liguori, M., Lindholm, V., Lizarraga, J., Luzzi, G., Macias-Perez, J. F., Maffei, B., Mandolesi, N., Martin, S., Martinez-Gonzalez, E., Martins, C. J. A. P., Masi, S., Massardi, M., Matarrese, S., Mazzotta, P., McCarthy, D., Melchiorri, A., Melin, J. -B., Mennella, A., Mohr, J., Molinari, D., Monfardini, A., Montier, L., Natoli, P., Negrello, M., Notari, A., Noviello, F., Oppizzi, F., O'Sullivan, C., Pagano, L., Paiella, A., Pajer, E., Paoletti, D., Paradiso, S., Partridge, R. B., Patanchon, G., Patil, S. P., Perdereau, O., Piacentini, F., Piat, M., Pisano, G., Polastri, L., Polenta, G., Pollo, A., Ponthieu, N., Poulin, V., Prele, D., Quartin, M., Ravenni, A., Remazeilles, M., Renzi, A., Ringeval, C., Roest, D., Roman, M., Roukema, B. F., Rubino-Martin, J. -A., Salvati, L., Scott, D., Serjeant, S., Signorelli, G., Starobinsky, A. A., Sunyaev, R., Tan, C. Y., Tartari, A., Tasinato, G., Toffolatti, L., Tomasi, M., Torrado, J., Tramonte, D., Trappe, N., Triqueneaux, S., Tristram, M., Trombetti, T., Tucci, M., Tucker, C., Urrestilla, J., Valiviita, J., Van de Weygaert, R., Van Tent, B., Vennin, V., Verde, L., Vermeulen, G., Vielva, P., Vittorio, N., Voisin, F., Wallis, C., Wandelt, B., Wehus, I. K., Weller, J., Young, K., Zannoni, M., Delabrouille, J., de Bernardis, P., Bouchet, F. R., Achucarro, A., Ade, P. A. R., Allison, R., Arroja, F., Artal, E., Ashdown, M., Baccigalupi, C., Ballardini, M., Banday, A. J., Banerji, R., Barbosa, D., Bartlett, J., Bartolo, N., Basak, S., Baselmans, J. J. A., Basu, K., Battistelli, E. S., Battye, R., Baumann, D., Benoit, A., Bersanelli, M., Bideaud, A., Biesiada, M., Bilicki, M., Bonaldi, A., Bonato, M., Borrill, J., Boulanger, F., Brinckmann, T., Brown, M. L., Bucher, M., Burigana, C., Buzzelli, A., Cabass, G., Cai, Z. -Y., Calvo, M., Caputo, A., Carvalho, C. -S., Casas, F. J., Castellano, G., Catalano, A., Challinor, A., Charles, I., Chluba, J., Clements, D. L., Clesse, S., Colafrancesco, S., Colantoni, I., Contreras, D., Coppolecchia, A., Crook, M., D'Alessandro, G., D'Amico, G., da Silva, A., de Avillez, M., de Gasperis, G., De Petris, M., de Zotti, G., Danese, L., Desert, F. -X., Desjacques, V., Di Valentino, E., Dickinson, C., Diego, J. M., Doyle, S., Durrer, R., Dvorkin, C., Eriksen, H. K., Errard, J., Feeney, S., Fernandez-Cobos, R., FineIli, F., Forastieri, F., Franceschet, C., Fuskeland, U., Galli, S., Genova-Santos, R. T., Gerbino, Martina, Giusarma, E., Gomez, A., Gonzalez-Nuevo, J., Grandis, S., Greenslade, J., Goupy, J., Hagstotz, S., Hanany, S., Handley, W., Henrot-Versille, S., Hernandez-Monteagudo, C., Hervias-Caimapo, C., Hills, M., Hindmarsh, M., Hivon, E., Hoang, D. T., Hooper, D. C., Hu, B., Keihanen, E., Keskitalo, R., Kiiveri, K., Kisner, T., Kitching, T., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamagna, L., Lapi, A., Lasenby, A., Lattanzi, M., Le Brun, A. M. C., Lesgourgues, J., Liguori, M., Lindholm, V., Lizarraga, J., Luzzi, G., Macias-Perez, J. F., Maffei, B., Mandolesi, N., Martin, S., Martinez-Gonzalez, E., Martins, C. J. A. P., Masi, S., Massardi, M., Matarrese, S., Mazzotta, P., McCarthy, D., Melchiorri, A., Melin, J. -B., Mennella, A., Mohr, J., Molinari, D., Monfardini, A., Montier, L., Natoli, P., Negrello, M., Notari, A., Noviello, F., Oppizzi, F., O'Sullivan, C., Pagano, L., Paiella, A., Pajer, E., Paoletti, D., Paradiso, S., Partridge, R. B., Patanchon, G., Patil, S. P., Perdereau, O., Piacentini, F., Piat, M., Pisano, G., Polastri, L., Polenta, G., Pollo, A., Ponthieu, N., Poulin, V., Prele, D., Quartin, M., Ravenni, A., Remazeilles, M., Renzi, A., Ringeval, C., Roest, D., Roman, M., Roukema, B. F., Rubino-Martin, J. -A., Salvati, L., Scott, D., Serjeant, S., Signorelli, G., Starobinsky, A. A., Sunyaev, R., Tan, C. Y., Tartari, A., Tasinato, G., Toffolatti, L., Tomasi, M., Torrado, J., Tramonte, D., Trappe, N., Triqueneaux, S., Tristram, M., Trombetti, T., Tucci, M., Tucker, C., Urrestilla, J., Valiviita, J., Van de Weygaert, R., Van Tent, B., Vennin, V., Verde, L., Vermeulen, G., Vielva, P., Vittorio, N., Voisin, F., Wallis, C., Wandelt, B., Wehus, I. K., Weller, J., Young, K., and Zannoni, M.
Abstract: Future observations of cosmic microwave background (CMB) polarisation have the potential to answer some of the most fundamental questions of modern physics and cosmology, including: what physical process gave birth to the Universe we see today? What are the dark matter and dark energy that seem to constitute 95% of the energy density of the Universe? Do we need extensions to the standard model of particle physics and fundamental interactions? Is the ACDM cosmological scenario correct, or are we missing an essential piece of the puzzle? 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 has 19 frequency channels, distributed over a broad frequency range, spanning the 60-600 GHz interval, to control astrophysical foreground emission. The angular resolution ranges from 2' to 18', and the aggregate CMB sensitivity is about 2 mu K.arcmin. The observations are made with a single integrated focal-plane instrument, consisting of an array of 2100 cryogenically-cooled, linearly-polarised detectors at the focus of a 1.2-m aperture cross-Dragone telescope. The mission is designed to minimise all sources of systematic effects, which must be controlled so that no more than 10(-4) of the intensity leaks into polarisation maps, and no more than about 1% of E-type polarisation leaks into B-type modes. CORE observes the sky from a large Lissajous orbit around the Sun-Earth L2 point on an orbit that offers stable observing conditions and avoids contamination from sidelobe pick-up of stray radiation originating from the Sun, Earth, and Moon. The entire sky is observed repeatedly during four years of continuous scanning, with a combination of th
Published: 2018
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