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1. OLIMPO: A balloon-borne SZE imager to probe ICM dynamics and the WHIM

Author

Sayers J., Avestruz C., Thakur R. Basu, Battistelli E., Bulbul E., Cacciotti F., Columbro F., Coppolecchia A., Cray S., D’Alessandro G., de Bernardis P., De Petris M., Hanany S., Lamagna L., Lau E., Masi S., Paiella A., Pettinari G., Piacentini F., Rapaport E., Rudnick L., Zhuravleva I., and ZuHone J.

Subjects
Physics, QC1-999
Abstract

OLIMPO is a proposed Antarctic balloon-borne Sunyaev-Zel’dovich effect (SZE) imager to study gas dynamics associated with structure formation along with the properties of the warm-hot intergalactic medium (WHIM) residing in the connective filaments. During a 25 day flight OLIMPO will image a total of 10 z∼0.05 galaxy clusters and 8 bridges at 145, 250, 365, and 460 GHz at an angular resolution of 1.0′–3.3′. The maps will be significantly deeper than those planned from CMB-S4 and CCAT-P, and will have excellent fidelity to the large angular scales of our low-z targets, which are difficult to probe from the ground. In combination with X-ray data from eROSITA and XRISM we will transform our current static view of galaxy clusters into a full dynamic picture by measuring the internal intra-cluster medium (ICM) velocity structure with the kinematic SZE, X-ray spectroscopy, and the power spectrum of ICM fluctuations. Radio observations from ASKAP and MeerKAT will be used to better understand the connection between ICM turbulence and shocks with the relativistic plasma. Beyond the cluster boundary, we will combine thermal SZE maps from OLIMPO with X-ray imaging from eROSITA to measure the thermodynamics of the WHIM residing in filaments, providing a better understanding of its properties and its contribution to the total baryon budget.

Published
2024
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2. Archeops in-flight performance, data processing, and map making

Author

Macias-Perez, J.F., Lagache, G., Maffei, B., Ganga, K., Bourrachot, A., Ade, P.A.R., Amblard, A., Ansari, R., Aubourg, É., Aumont, J., Bargot, S., Bartlett, J., Benoit, A., Bernard, J.-P., Bhatia, R., Blanchard, A., Bock, J.J., Boscaleri, A., Bouchet, F.R., Camus, P., Cardoso, J.-F., Couchot, F., De Bernardis, P., Delabrouille, J., Desert, F.-X., Dore, O., Douspis, M., Dumoulin, L., Dupac, X., Filliatre, P., Fosalba, P., Gannaway, F., Gautier, B., Giard, M., Giraud-Héraud, Y., Gispert, R., Guglielmi, L., Hamilton, J.-Ch., Hanany, S., Henrot-Versille, S., Hristov, V.V., Kaplan, J., Lamarre, J.-M., Lange, A.E., Madet, K., Magneville, Ch., Marrone, D.P., Masi, S., Mayet, F., Murphy, J.Anthony, Naraghi, F., Nati, F., Patanchon, G., Perdereau, O., Perrin, G., Plaszczynski, S., Piat, M., Ponthieu, N., Prunet, S., Puget, J.-L., Renault, C., Rosset, C., Santos, D., Starobinsky, Alexei A., Strukov, I., Sudiwala, R., Teyssier, R., Tristram, M., Tucker, C., Vanel, J.-C., Vibert, D., Wakui, E., Yvon, D., Macias-Perez, J.F., Lagache, G., Maffei, B., Ganga, K., Bourrachot, A., Ade, P.A.R., Amblard, A., Ansari, R., Aubourg, É., Aumont, J., Bargot, S., Bartlett, J., Benoit, A., Bernard, J.-P., Bhatia, R., Blanchard, A., Bock, J.J., Boscaleri, A., Bouchet, F.R., Camus, P., Cardoso, J.-F., Couchot, F., De Bernardis, P., Delabrouille, J., Desert, F.-X., Dore, O., Douspis, M., Dumoulin, L., Dupac, X., Filliatre, P., Fosalba, P., Gannaway, F., Gautier, B., Giard, M., Giraud-Héraud, Y., Gispert, R., Guglielmi, L., Hamilton, J.-Ch., Hanany, S., Henrot-Versille, S., Hristov, V.V., Kaplan, J., Lamarre, J.-M., Lange, A.E., Madet, K., Magneville, Ch., Marrone, D.P., Masi, S., Mayet, F., Murphy, J.Anthony, Naraghi, F., Nati, F., Patanchon, G., Perdereau, O., Perrin, G., Plaszczynski, S., Piat, M., Ponthieu, N., Prunet, S., Puget, J.-L., Renault, C., Rosset, C., Santos, D., Starobinsky, Alexei A., Strukov, I., Sudiwala, R., Teyssier, R., Tristram, M., Tucker, C., Vanel, J.-C., Vibert, D., Wakui, E., and Yvon, D.

Abstract

Aims. Archeops is a balloon-borne experiment inspired by the Planck satellite and its high frequency instrument (HFI). It is designed to measure the cosmic microwave background (CMB) temperature anisotropies at high angular resolution (~12 arcmin) over a large fraction of the sky (around 30%) at 143, 217, 353, and 545 GHz. The Archeops 353 GHz channel consists of three pairs of polarized sensitive bolometers designed to detect the polarized diffuse emission of Galactic dust. Methods. In this paper we present an update of the instrumental setup, as well as the flight performance for the last Archeops flight campaign (February 2002 from Kiruna, Sweden). We also describe the processing and analysis of the Archeops time-ordered data for that campaign, which led to measurement of the CMB anisotropy power spectrum in the multipole range = 10-700 and to the first measurements of both the polarized emission of dust at large angular scales and its power spectra in the multipole range = 3-70 Results. We present maps covering approximately 30% of the sky. These maps contain Galactic emission, including the Galactic plane, in the four Archeops channels at 143, 217, 353, and 545 GHz and CMB anisotropies at 143 and 217 GHz. These are one of the first sub-degree-resolution maps in the millimeter and submillimeter ranges of the large angular-scale diffuse Galactic dust emission and CMB temperature anisotropies, respectively.

Published
2007

3. Archeops in-flight performance, data processing, and map making

Author

Macias-Perez, J, Lagache, G, Maffei, B, Ade, P, Amblard, A, Ansari, R, Aubourg, E, Aumont, J, Bargot, S, Bartlett, J, Benoit, A, Ph Bernard, J, Bhatia, R, Blanchard, A, Bock, J, Boscaleri, A, Bouchet, F, Bourrachot, A, Camus, P, Cardoso, J, Couchot, F, De Bernardis, P, Delabrouille, J, Desert, F, Dore, O, Douspis, M, Dumoulin, L, Dupac, X, Filliatre, P, Fosalba, P, Ganga, K, Gannaway, F, Gautier, B, Giard, M, Giraud Heraud, Y, Gispert, R, Guglielmi, L, Ch Hamilton, J, Hanany, S, Henrot Versille, S, Hristov, V, Kaplan, J, Lamarre, J, Lange, A, Madet, K, Magneville, C, Marrone, D, Masi, S, Mayet, F, Murphy, J, Naraghi, F, Nati, F, J.F. Macias-Perez, G. Lagache, B. Maffei, P. Ade, A. Amblard, R. Ansari, E. Aubourg, J. Aumont, S. Bargot, J. Bartlett, A. Benoit, J. Ph Bernard, R. Bhatia, A. Blanchard, J.J. Bock, A. Boscaleri, F.R. Bouchet, A. Bourrachot, P. Camus, J.F. Cardoso, F. Couchot, Paolo De Bernardis, J. Delabrouille, F.X. Desert, O. Dore, M. Douspis, L. Dumoulin, X. Dupac, P.H. Filliatre, P. Fosalba, K. Ganga, F. Gannaway, B. Gautier, M. Giard, Y. Giraud Heraud, R. Gispert, L. Guglielmi, J. Ch Hamilton, S. Hanany, S. Henrot Versille, V. Hristov, J. Kaplan, J.M. Lamarre, A.E. Lange, K. Madet, C.H. Magneville, D.P. Marrone, Silvia Masi, F. Mayet, J.A. Murphy, F. Naraghi, Federico Nati, Macias-Perez, J, Lagache, G, Maffei, B, Ade, P, Amblard, A, Ansari, R, Aubourg, E, Aumont, J, Bargot, S, Bartlett, J, Benoit, A, Ph Bernard, J, Bhatia, R, Blanchard, A, Bock, J, Boscaleri, A, Bouchet, F, Bourrachot, A, Camus, P, Cardoso, J, Couchot, F, De Bernardis, P, Delabrouille, J, Desert, F, Dore, O, Douspis, M, Dumoulin, L, Dupac, X, Filliatre, P, Fosalba, P, Ganga, K, Gannaway, F, Gautier, B, Giard, M, Giraud Heraud, Y, Gispert, R, Guglielmi, L, Ch Hamilton, J, Hanany, S, Henrot Versille, S, Hristov, V, Kaplan, J, Lamarre, J, Lange, A, Madet, K, Magneville, C, Marrone, D, Masi, S, Mayet, F, Murphy, J, Naraghi, F, Nati, F, J.F. Macias-Perez, G. Lagache, B. Maffei, P. Ade, A. Amblard, R. Ansari, E. Aubourg, J. Aumont, S. Bargot, J. Bartlett, A. Benoit, J. Ph Bernard, R. Bhatia, A. Blanchard, J.J. Bock, A. Boscaleri, F.R. Bouchet, A. Bourrachot, P. Camus, J.F. Cardoso, F. Couchot, Paolo De Bernardis, J. Delabrouille, F.X. Desert, O. Dore, M. Douspis, L. Dumoulin, X. Dupac, P.H. Filliatre, P. Fosalba, K. Ganga, F. Gannaway, B. Gautier, M. Giard, Y. Giraud Heraud, R. Gispert, L. Guglielmi, J. Ch Hamilton, S. Hanany, S. Henrot Versille, V. Hristov, J. Kaplan, J.M. Lamarre, A.E. Lange, K. Madet, C.H. Magneville, D.P. Marrone, Silvia Masi, F. Mayet, J.A. Murphy, F. Naraghi, and Federico Nati

Abstract

Aims. Archeops is a balloon-borne experiment inspired by the Planck satellite and its high frequency instrument ( HFI). It is designed to measure the cosmic microwave background ( CMB) temperature anisotropies at high angular resolution (similar to 12 arcmin) over a large fraction of the sky ( around 30%) at 143, 217, 353, and 545 GHz. The Archeops 353 GHz channel consists of three pairs of polarized sensitive bolometers designed to detect the polarized diffuse emission of Galactic dust. Methods. In this paper we present an update of the instrumental setup, as well as the flight performance for the last Archeops flight campaign ( February 2002 from Kiruna, Sweden). We also describe the processing and analysis of the Archeops time-ordered data for that campaign, which led to measurement of the CMB anisotropy power spectrum in the multipole range l = 10-700 and to the first measurements of both the polarized emission of dust at large angular scales and its power spectra in the multipole range l = 3-70 Results. We present maps covering approximately 30% of the sky. These maps contain Galactic emission, including the Galactic plane, in the four Archeops channels at 143, 217, 353, and 545 GHz and CMB anisotropies at 143 and 217 GHz. These are one of the first sub-degree-resolution maps in the millimeter and submillimeter ranges of the large angular-scale diffuse Galactic dust emission and CMB temperature anisotropies, respectively.

Published
2007

4. The CMB temperature power spectrum from an improved analysis of the Archeops data

Author

Tristram, M, Patanchon, G, Macias-Perez, J, Ade, P, Amblard, A, Ansari, R, Aubourg, E, Benoit, A, Ph Bernard, J, Blanchard, A, Bock, J, Bouchet, F, Bourrachot, A, Camus, P, Cardoso, J, Couchot, F, De Bernardis, P, Delabrouille, J, Desert, F, Douspis, M, Dumoulin, L, Filliatre, P, Fosalba, P, Giard, M, Giraud-Heraud, Y, Gispert, R, Guglielmi, L, Ch Hamilton, J, Hanany, S, Henrot-Versille, S, Kaplan, J, Lagache, G, Lamarre, J, Lange, A, Madet, K, Maffei, B, Magneville, C, Masi, S, Mayet, F, Nati, F, Perdereau, O, Plaszczynski, S, Piat, M, Ponthieu, N, Prunet, S, Renault, C, Rosset, C, Santos, D, Vibert, D, Yvon, D, M. Tristram, G. Patanchon, J.F. Macias-Perez, P. Ade, A. Amblard, R. Ansari, E. Aubourg, A. Benoit, J. Ph Bernard, A. Blanchard, J.J. Bock, F.R. Bouchet, A. Bourrachot, P. Camus, J.F. Cardoso, F. Couchot, Paolo De Bernardis, J. Delabrouille, F.X. Desert, M. Douspis, L. Dumoulin, P.H. Filliatre, P. Fosalba, M. Giard, Y. Giraud-Heraud, R. Gispert, L. Guglielmi, J. Ch Hamilton, S. Hanany, S. Henrot-Versille, J. Kaplan, G. Lagache, J.M. Lamarre, A.E. Lange, K. Madet, B. Maffei, C.H. Magneville, Silvia Masi, F. Mayet, Federico Nati, O. Perdereau, S. Plaszczynski, M. Piat, N. Ponthieu, S. Prunet, C. Renault, C. Rosset, D. Santos, D. Vibert, D. Yvon, Tristram, M, Patanchon, G, Macias-Perez, J, Ade, P, Amblard, A, Ansari, R, Aubourg, E, Benoit, A, Ph Bernard, J, Blanchard, A, Bock, J, Bouchet, F, Bourrachot, A, Camus, P, Cardoso, J, Couchot, F, De Bernardis, P, Delabrouille, J, Desert, F, Douspis, M, Dumoulin, L, Filliatre, P, Fosalba, P, Giard, M, Giraud-Heraud, Y, Gispert, R, Guglielmi, L, Ch Hamilton, J, Hanany, S, Henrot-Versille, S, Kaplan, J, Lagache, G, Lamarre, J, Lange, A, Madet, K, Maffei, B, Magneville, C, Masi, S, Mayet, F, Nati, F, Perdereau, O, Plaszczynski, S, Piat, M, Ponthieu, N, Prunet, S, Renault, C, Rosset, C, Santos, D, Vibert, D, Yvon, D, M. Tristram, G. Patanchon, J.F. Macias-Perez, P. Ade, A. Amblard, R. Ansari, E. Aubourg, A. Benoit, J. Ph Bernard, A. Blanchard, J.J. Bock, F.R. Bouchet, A. Bourrachot, P. Camus, J.F. Cardoso, F. Couchot, Paolo De Bernardis, J. Delabrouille, F.X. Desert, M. Douspis, L. Dumoulin, P.H. Filliatre, P. Fosalba, M. Giard, Y. Giraud-Heraud, R. Gispert, L. Guglielmi, J. Ch Hamilton, S. Hanany, S. Henrot-Versille, J. Kaplan, G. Lagache, J.M. Lamarre, A.E. Lange, K. Madet, B. Maffei, C.H. Magneville, Silvia Masi, F. Mayet, Federico Nati, O. Perdereau, S. Plaszczynski, M. Piat, N. Ponthieu, S. Prunet, C. Renault, C. Rosset, D. Santos, D. Vibert, and D. Yvon

Abstract

We present improved results on the measurement of the angular power spectrum of the Cosmic Microwave Background (CMB) temperature anisotropies using the data from the last ARCHEOPS flight. This refined analysis is obtained by using the 6 most sensitive photometric pixels in the CMB bands centered at 143 and 217 GHz and 20% of the sky, mostly clear of foregrounds. Using two different cross-correlation methods, we obtain very similar results for the angular power spectrum. Consistency checks are performed to test the robustness of these results paying particular attention to the foreground contamination level which remains well below the statistical uncertainties. The multipole range from l = 10 to l = 700 is covered with 25 bins, confirming strong evidence for a plateau at large angular scales (the Sachs-Wolfe plateau) followed by two acoustic peaks centered around l = 220 and l = 550 respectively. These data provide an independent confirmation, obtained at different frequencies, of the WMAP first year results.

Published
2005

5. First detection of polarization of the submillimetre diffuse galactic dust emission by Archeops

Author

Benoit, A., Ade, P.A.R., Amblard, A., Ansari, R., Aubourg, É., Bargot, S., Bartlett, J.G., Bernard, J.-P., Bhatia, R., Blanchard, A., Bock, J.J., Boscaleri, A., Bouchet, F.R., Bourrachot, A., Camus, P., Couchot, F., De Bernardis, P., Delabrouille, J., Desert, F.-X., Dore, O., Douspis, M., Dumoulin, L., Dupac, X., Filliatre, P., Fosalba, P., Ganga, K., Gannaway, F., Gautier, B., Giard, M., Giraud-Héraud, Y., Gispert, R., Guglielmi, L., Hamilton, J.-Ch., Hanany, S., Henrot-Versille, S., Kaplan, J., Lagache, G., Lamarre, J.-M., Lange, A.E., Macias-Perez, J.F., Madet, K., Maffei, B., Magneville, Ch., Marrone, D.P., Masi, S., Mayet, F., Murphy, J.Anthony, Naraghi, F., Nati, F., Patanchon, G., Perrin, G., Piat, M., Ponthieu, N., Prunet, S., Puget, J.-L., Renault, C., Rosset, C., Santos, D., Starobinsky, Alexei A., Strukov, I., Sudiwala, R., Teyssier, R., Tristram, M., Tucker, C., Vanel, J.-C., Vibert, D., Wakui, E., Yvon, D., Benoit, A., Ade, P.A.R., Amblard, A., Ansari, R., Aubourg, É., Bargot, S., Bartlett, J.G., Bernard, J.-P., Bhatia, R., Blanchard, A., Bock, J.J., Boscaleri, A., Bouchet, F.R., Bourrachot, A., Camus, P., Couchot, F., De Bernardis, P., Delabrouille, J., Desert, F.-X., Dore, O., Douspis, M., Dumoulin, L., Dupac, X., Filliatre, P., Fosalba, P., Ganga, K., Gannaway, F., Gautier, B., Giard, M., Giraud-Héraud, Y., Gispert, R., Guglielmi, L., Hamilton, J.-Ch., Hanany, S., Henrot-Versille, S., Kaplan, J., Lagache, G., Lamarre, J.-M., Lange, A.E., Macias-Perez, J.F., Madet, K., Maffei, B., Magneville, Ch., Marrone, D.P., Masi, S., Mayet, F., Murphy, J.Anthony, Naraghi, F., Nati, F., Patanchon, G., Perrin, G., Piat, M., Ponthieu, N., Prunet, S., Puget, J.-L., Renault, C., Rosset, C., Santos, D., Starobinsky, Alexei A., Strukov, I., Sudiwala, R., Teyssier, R., Tristram, M., Tucker, C., Vanel, J.-C., Vibert, D., Wakui, E., and Yvon, D.

Abstract

We present the first determination of the Galactic polarized emission at 353 GHz by Archeops. The data were taken during the Arctic night of February 7, 2002 after the balloon-borne instrument was launched by CNES from the Swedish Esrange base near Kiruna. In addition to the 143 GHz and 217 GHz frequency bands dedicated to CMB studies, Archeops had one 545 GHz and six 353 GHz bolometers mounted in three polarization–sensitive pairs that were used for Galactic foreground studies. We present maps of the Stokes parameters over 17% of the sky and with a 13 arcmin resolution at 353 GHz (). They show a significant Galactic large scale polarized emission coherent on the longitude ranges and deg. with a degree of polarization at the level of 4–5%, in agreement with expectations from starlight polarization measurements. Some regions in the Galactic plane (Gem OB1, Cassiopeia) show an even stronger degree of polarization in the range 10–20%. These findings provide strong evidence for a powerful grain alignment mechanism throughout the interstellar medium and a coherent magnetic field coplanar to the Galactic plane. This magnetic field pervades even some dense clouds. Extrapolated to high Galactic latitude, these results indicate that interstellar dust polarized emission is the major foreground for PLANCK–HFI CMB polarization measurements.

Published
2004

6. The cosmic microwave background anisotropy power spectrum measured by Archeops

Author

Benoit, A., Ade, P.A.R., Amblard, A., Ansari, R., Aubourg, É., Bargot, S., Bartlett, J.G., Bernard, J.-P., Bhatia, R., Blanchard, A., Bock, J.J., Boscaleri, A., Bouchet, F.R., Bourrachot, A., Camus, P., Couchot, F., De Bernardis, P., Delabrouille, J., Desert, F.-X., Dore, O., Douspis, M., Dumoulin, L., Dupac, X., Filliatre, P., Fosalba, P., Ganga, K., Guglielmi, L., Hamilton, J.-Ch., Hanany, S., Henrot-Versille, S., Kaplan, J., Lagache, G., Lamarre, J.-M., Lange, A.E., Macias-Perez, J.F., Madet, K., Maffei, B., Magneville, Ch., Marrone, D.P., Masi, S., Mayet, F., Murphy, J.Anthony, Naraghi, F., Nati, F., Patanchon, G., Perrin, G., Piat, M., Ponthieu, N., Prunet, S., Puget, J.-L., Renault, C., Rosset, C., Santos, D., Starobinsky, Alexei A., Strukov, I., Sudiwala, R., Teyssier, R., Tristram, M., Tucker, C., Vanel, J.-C., Vibert, D., Wakui, E., Yvon, D., Benoit, A., Ade, P.A.R., Amblard, A., Ansari, R., Aubourg, É., Bargot, S., Bartlett, J.G., Bernard, J.-P., Bhatia, R., Blanchard, A., Bock, J.J., Boscaleri, A., Bouchet, F.R., Bourrachot, A., Camus, P., Couchot, F., De Bernardis, P., Delabrouille, J., Desert, F.-X., Dore, O., Douspis, M., Dumoulin, L., Dupac, X., Filliatre, P., Fosalba, P., Ganga, K., Guglielmi, L., Hamilton, J.-Ch., Hanany, S., Henrot-Versille, S., Kaplan, J., Lagache, G., Lamarre, J.-M., Lange, A.E., Macias-Perez, J.F., Madet, K., Maffei, B., Magneville, Ch., Marrone, D.P., Masi, S., Mayet, F., Murphy, J.Anthony, Naraghi, F., Nati, F., Patanchon, G., Perrin, G., Piat, M., Ponthieu, N., Prunet, S., Puget, J.-L., Renault, C., Rosset, C., Santos, D., Starobinsky, Alexei A., Strukov, I., Sudiwala, R., Teyssier, R., Tristram, M., Tucker, C., Vanel, J.-C., Vibert, D., Wakui, E., and Yvon, D.

Abstract

We present a determination by the Archeops experiment of the angular power spectrum of the cosmic microwave background anisotropy in 16 bins over the multipole range . Archeops was conceived as a precursor of the Planck HFI instrument by using the same optical design and the same technology for the detectors and their cooling. Archeops is a balloon–borne instrument consisting of a 1.5 m aperture diameter telescope and an array of 21 photometers maintained at mK that are operating in 4 frequency bands centered at 143, 217, 353 and 545 GHz. The data were taken during the Arctic night of February 7, 2002 after the instrument was launched by CNES from Esrange base (Sweden). The entire data cover ~30% of the sky. This first analysis was obtained with a small subset of the dataset using the most sensitive photometer in each CMB band (143 and 217 GHz) and 12.6% of the sky at galactic latitudes above 30 degrees where the foreground contamination is measured to be negligible. The large sky coverage and medium resolution (better than 15 arcmin) provide for the first time a high signal-to-noise ratio determination of the power spectrum over angular scales that include both the first acoustic peak and scales probed by COBE/DMR. With a binning of to 25 the error bars are dominated by sample variance for below 200. A companion paper details the cosmological implications.

Published
2003

7. Archeops in-flight performance, data processing, and map making

Author

Macías-Pérez, J. F., primary, Lagache, G., additional, Maffei, B., additional, Ganga, K., additional, Bourrachot, A., additional, Ade, P., additional, Amblard, A., additional, Ansari, R., additional, Aubourg, E., additional, Aumont, J., additional, Bargot, S., additional, Bartlett, J., additional, Benoît, A., additional, Bernard, J.-Ph., additional, Bhatia, R., additional, Blanchard, A., additional, Bock, J. J., additional, Boscaleri, A., additional, Bouchet, F. R., additional, Camus, P., additional, Cardoso, J.-F., additional, Couchot, F., additional, de Bernardis, P., additional, Delabrouille, J., additional, Désert, F.-X., additional, Doré, O., additional, Douspis, M., additional, Dumoulin, L., additional, Dupac, X., additional, Filliatre, Ph., additional, Fosalba, P., additional, Gannaway, F., additional, Gautier, B., additional, Giard, M., additional, Giraud-Héraud, Y., additional, Gispert, R., additional, Guglielmi, L., additional, Hamilton, J.-Ch., additional, Hanany, S., additional, Henrot-Versillé, S., additional, Hristov, V., additional, Kaplan, J., additional, Lamarre, J.-M., additional, Lange, A. E., additional, Madet, K., additional, Magneville, Ch., additional, Marrone, D. P., additional, Masi, S., additional, Mayet, F., additional, Murphy, J. A., additional, Naraghi, F., additional, Nati, F., additional, Patanchon, G., additional, Perdereau, O., additional, Perrin, G., additional, Plaszczynski, S., additional, Piat, M., additional, Ponthieu, N., additional, Prunet, S., additional, Puget, J.-L., additional, Renault, C., additional, Rosset, C., additional, Santos, D., additional, Starobinsky, A., additional, Strukov, I., additional, Sudiwala, R. V., additional, Teyssier, R., additional, Tristram, M., additional, Tucker, C., additional, Vanel, J.-Ch., additional, Vibert, D., additional, Wakui, E., additional, and Yvon, D., additional

Published
2007
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8. Temperature and polarization angular power spectra of Galactic dust radiation at 353 GHz as measured by Archeops

Author

Ponthieu, N., primary, Macías-Pérez, J. F., additional, Tristram, M., additional, Ade, P., additional, Amblard, A., additional, Ansari, R., additional, Aumont, J., additional, Aubourg, É., additional, Benoît, A., additional, Bernard, J.-Ph., additional, Blanchard, A., additional, Bock, J. J., additional, Bouchet, F. R., additional, Bourrachot, A., additional, Camus, P., additional, Cardoso, J.-F., additional, Couchot, F., additional, de Bernardis, P., additional, Delabrouille, J., additional, Désert, F.-X., additional, Douspis, M., additional, Dumoulin, L., additional, Filliatre, Ph., additional, Fosalba, P., additional, Giard, M., additional, Giraud-Héraud, Y., additional, Gispert, R., additional, Grain, J., additional, Guglielmi, L., additional, Hamilton, J.-Ch., additional, Hanany, S., additional, Henrot-Versillé, S., additional, Kaplan, J., additional, Lagache, G., additional, Lange, A. E., additional, Madet, K., additional, Maffei, B., additional, Masi, S., additional, Mayet, F., additional, Nati, F., additional, Patanchon, G., additional, Perdereau, O., additional, Plaszczynski, S., additional, Piat, M., additional, Prunet, S., additional, Puget, J.-L., additional, Renault, C., additional, Rosset, C., additional, Santos, D., additional, Vibert, D., additional, and Yvon, D., additional

Published
2005
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9. The CMB temperature power spectrum from an improved analysis of the Archeops data

Author

Tristram, M., primary, Patanchon, G., additional, Macías-Pérez, J. F., additional, Ade, P., additional, Amblard, A., additional, Ansari, R., additional, Aubourg, É., additional, Benoît, A., additional, Bernard, J.-Ph., additional, Blanchard, A., additional, Bock, J. J., additional, Bouchet, F. R., additional, Bourrachot, A., additional, Camus, P., additional, Cardoso, J.-F., additional, Couchot, F., additional, de Bernardis, P., additional, Delabrouille, J., additional, Désert, F.-X., additional, Douspis, M., additional, Dumoulin, L., additional, Filliatre, Ph., additional, Fosalba, P., additional, Giard, M., additional, Giraud-Héraud, Y., additional, Gispert†, R., additional, Guglielmi, L., additional, Hamilton, J.-Ch., additional, Hanany, S., additional, Henrot-Versillé, S., additional, Kaplan, J., additional, Lagache, G., additional, Lamarre, J.-M., additional, Lange, A. E., additional, Madet, K., additional, Maffei, B., additional, Magneville, Ch., additional, Masi, S., additional, Mayet, F., additional, Nati, F., additional, Perdereau, O., additional, Plaszczynski, S., additional, Piat, M., additional, Ponthieu, N., additional, Prunet, S., additional, Renault, C., additional, Rosset, C., additional, Santos, D., additional, Vibert, D., additional, and Yvon, D., additional

Published
2005
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10. Cosmological constraints from Archeops

Author

Guy Perrin, J. F. Macías-Pérez, Nicolas Ponthieu, Jacques Delabrouille, Peter A. R. Ade, R. Ansari, K. Ganga, James G. Bartlett, Bruno Maffei, M. Tristram, R. S. Bhatia, M. Piat, M. Giard, F. Mayet, J.-Ch. Hamilton, Carole Tucker, L. Dumoulin, Alexandre Amblard, Guilaine Lagache, R. Gispert, J. Kaplan, Andrew E. Lange, K. Madet, Alain Blanchard, F. Couchot, Francois-Xavier Désert, Guillaume Patanchon, Marian Douspis, L. Guglielmi, P. de Bernardis, C. Rosset, A. Boscaleri, Silvia Masi, Jean-Charles Vanel, Alain Benoit, Anthony Murphy, D. Vibert, Pablo Fosalba, Philippe Camus, Federico Nati, François R. Bouchet, B. Gautier, I. Strukov, F. Naraghi, J.-M. Lamarre, D. Santos, James J. Bock, E. Wakui, Jean-Loup Puget, Éric Aubourg, C. Renault, X. Dupac, Ch. Magneville, Alexei A. Starobinsky, D. Yvon, Rashmikant V. Sudiwala, S. Bargot, Simon Prunet, A. Bourrachot, Shaul Hanany, O. Doré, Y. Giraud-Héraud, Fred Gannaway, Romain Teyssier, Sophie Henrot-Versille, Daniel P. Marrone, J.-Ph. Bernard, P. Filliatre, Centre de Recherches sur les Très Basses Températures (CRTBT), Université Joseph Fourier - Grenoble 1 (UJF)-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF (institution))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), 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), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), 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), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Centre d'étude spatiale des rayonnements (CESR), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), ARCHEOPS, Benoit, A, Ade, P, Amblard, A, Ansari, R, Aubourg, E, Bargot, S, Bartlett, J, Bernard, J, Bhatia, R, Blanchard, A, Bock, J, Boscaleri, A, Bouchet, F, Bourrachot, A, Camus, P, Couchot, F, De Bernardis, P, Delabrouille, J, Desert, F, Dore, O, Douspis, M, Dumoulin, L, Dupac, X, Filliatre, P, Fosalba, P, Ganga, K, Gannaway, F, Gautier, B, Giard, M, Giraud-Heraud, Y, Gispert, R, Guglielmi, L, Hamilton, J, Hanany, S, Henrot-Versille, S, Kaplan, J, Lagache, G, Lamarre, J, Lange, A, Macias-Perez, J, Madet, K, Maffei, B, Magneville, C, Marrone, D, Masi, S, Mayet, F, Murphy, A, Naraghi, F, Nati, F, Patanchon, G, Perrin, G, Piat, M, Ponthieu, N, Prunet, S, Puget, J, Renault, C, Rosset, C, Santos, D, Starobinsky, A, Strukov, I, Sudiwala, R, Teyssier, R, Tristram, M, Tucker, C, Vanel, J, Vibert, D, Wakui, E, Yvon, D, Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique de Grenoble (INPG)-Université Joseph Fourier - Grenoble 1 (UJF), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, and Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Cosmological parameter, Cold dark matter, Cosmic microwave background, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Omega, Early Universe, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, 0103 physical sciences, Large-scale structure of the Universe, 010303 astronomy & astrophysics, Reionization, QB, Physics, Inflation (cosmology), Archeops, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, Baryon, Space and Planetary Science, symbols, High Energy Physics::Experiment, Astrophysics::Earth and Planetary Astrophysics, Hubble's law
Abstract

We analyze the cosmological constraints that Archeops places on adiabatic cold dark matter models with passive power-law initial fluctuations. Because its angular power spectrum has small bins in l and large l coverage down to COBE scales, Archeops provides a precise determination of the first acoustic peak in terms of position at multipole l_peak=220 +- 6, height and width. An analysis of Archeops data in combination with other CMB datasets constrains the baryon content of the Universe, Omega(b)h^2 = 0.022 (+0.003,-0.004), compatible with Big-Bang nucleosynthesis and with a similar accuracy. Using cosmological priors obtainedfrom recent non-CMB data leads to yet tighter constraints on the total density, e.g. Omega(tot)=1.00 (+0.03,-0.02) using the HST determination of the Hubble constant. An excellent absolute calibration consistency is found between Archeops and other CMB experiments, as well as with the previously quoted best fit model.The spectral index n is measured to be 1.04 (+0.10,-0.12) when the optical depth to reionization, tau, is allowed to vary as a free parameter, and 0.96 (+0.03,-0.04) when tau is fixed to zero, both in good agreement with inflation., Comment: A&A Letter, in press, 6 pages, 7 figures, see also http://www.archeops.org

Published
2003
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