Search

Your search keyword '"Hamilton, J-C."' showing total 280 results
Start Over Author "Hamilton, J-C."

Refine your results

more »

more »

more »

more »
280 results on '"Hamilton, J-C."'

1. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological implications of the large-scale two-point correlation function

Author

Sanchez, Ariel G., Scoccola, C. G., Ross, A. J., Percival, W., Manera, M., Montesano, F., Mazzalay, X., Cuesta, A. J., Eisenstein, D. J., Kazin, E., McBride, C. K., Mehta, K., Montero-Dorta, A. D., Padmanabhan, N., Prada, F., Rubino-Martin, J. A., Tojeiro, R., Xu, X., Magana, M. Vargas, Aubourg, E., Bahcall, N. A., Bailey, S., Bizyaev, D., Bolton, A. S., Brewington, H., Brinkmann, J., Brownstein, J. R., Gott III, J. Richard, Hamilton, J. C., Ho, S., Honscheid, K., Labatie, A., Malanushenko, E., Malanushenko, V., Maraston, C., Muna, D., Nichol, R. C., Oravetz, D., Pan, K., Ross, N. P., Roe, N. A., Reid, B. A., Schlegel, D. J., Shelden, A., Schneider, D. P., Simmons, A., Skibba, R., Snedden, S., Thomas, D., Tinker, J., Wake, D. A., Weaver, B. A., Weinberg, David H., White, Martin, Zehavi, I., and Zhao, G.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We obtain constraints on cosmological parameters from the spherically averaged redshift-space correlation function of the CMASS Data Release 9 (DR9) sample of the Baryonic Oscillation Spectroscopic Survey (BOSS). We combine this information with additional data from recent CMB, SN and BAO measurements. Our results show no significant evidence of deviations from the standard flat-Lambda CDM model, whose basic parameters can be specified by Omega_m = 0.285 +- 0.009, 100 Omega_b = 4.59 +- 0.09, n_s = 0.96 +- 0.009, H_0 = 69.4 +- 0.8 km/s/Mpc and sigma_8 = 0.80 +- 0.02. The CMB+CMASS combination sets tight constraints on the curvature of the Universe, with Omega_k = -0.0043 +- 0.0049, and the tensor-to-scalar amplitude ratio, for which we find r < 0.16 at the 95 per cent confidence level (CL). These data show a clear signature of a deviation from scale-invariance also in the presence of tensor modes, with n_s <1 at the 99.7 per cent CL. We derive constraints on the fraction of massive neutrinos of f_nu < 0.049 (95 per cent CL), implying a limit of sum m_nu < 0.51 eV. We find no signature of a deviation from a cosmological constant from the combination of all datasets, with a constraint of w_DE = -1.033 +- 0.073 when this parameter is assumed time-independent, and no evidence of a departure from this value when it is allowed to evolve as w_DE(a) = w_0 + w_a (1 - a). The achieved accuracy on our cosmological constraints is a clear demonstration of the constraining power of current cosmological observations., Comment: 26 pages, 15 figures. Minor changes to match version accepted by MNRAS

Published
2012
Full Text
View/download PDF

2. Intensity and polarization of the atmospheric emission at millimetric wavelengths at Dome Concordia

Author

Battistelli, E. S., Amico, G., Baù, A., Bergé, L., Bréelle, É., Charlassier, R., Collin, S., Cruciani, A., de Bernardis, P., Dufour, C., Dumoulin, L., Gervasi, M., Giard, M., Giordano, C., Giraud-Héraud, Y., Guglielmi, L., Hamilton, J. -C., Landé, J., Maffei, B., Maiello, M., Marnieros, S., Masi, S., Passerini, A., Piacentini, F., Piat, M., Piccirillo, L., Pisano, G., Polenta, G., Rosset, C., Salatino, M., Schillaci, A., Sordini, R., Spinelli, S., Tartari, A., and Zannoni, M.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Atmospheric and Oceanic Physics
Abstract

Atmospheric emission is a dominant source of disturbance in ground-based astronomy at mm wavelengths. The Antarctic plateau is recognized to be an ideal site for mm and sub-mm observations, and the French/Italian base of Dome C is among the best sites on Earth for these observations. In this paper we present measurements, performed using the BRAIN-pathfinder experiment, at Dome C of the atmospheric emission in intensity and polarization at 150GHz, one of the best observational frequencies for CMB observations when considering cosmic signal intensity, atmospheric transmission, detectors sensitivity, and foreground removal. Careful characterization of the air-mass synchronous emission has been performed, acquiring more that 380 elevation scans (i.e. "skydip") during the third BRAIN-pathfinder summer campaign in December 2009/January 2010. The extremely high transparency of the Antarctic atmosphere over Dome Concordia is proven by the very low measured optical depth: =0.050 \pm 0.003 \pm 0.011 where the first error is statistical and the second is systematic error. Mid term stability, over the summer campaign, of the atmosphere emission has also been studied. Adapting the radiative transfer atmosphere emission model "am" to the particular conditions found at Dome C, we also infer the level of the PWV content of the atmosphere, notoriously the main source of disturbance in millimetric astronomy (=0.77 +/- 0.06 + 0.15 - 0.12 mm). Upper limits on the air-mass correlated polarized signal are also placed for the first time. The degree of circular polarization of atmospheric emission is found to be lower than 0.2% (95%CL), while the degree of linear polarization is found to be lower than 0.1% (95%CL). These limits include signal-correlated instrumental spurious polarization., Comment: MNRAS accepted for publication. Refined analysis

Published
2012
Full Text
View/download PDF

3. Simulations of BAO reconstruction with a quasar Lyman-alpha survey

Author

Goff, J. -M. Le, Magneville, C., Rollinde, E., Peirani, S., Petitjean, P., Pichon, C., Rich, J., Yeche, C., Aubourg, E., Busca, N., Charlassier, R., Delubac, T., Hamilton, J. C., Delabrouille, N. Palanque, Paris, I., and Vargas, M.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The imprint of Baryonic Acoustic Oscillations (BAO) on the matter power spectrum can be constrained using the neutral hydrogen density in the intergalactic medium as a tracer of the matter density. One of the goals of the Baryon Oscillation Spectroscopic Survey (BOSS) of the Sloan Digital Sky Survey (SDSS-III) is to derive the Hubble expansion rate and the angular scale from the BAO signal in the IGM. To this aim, the Lyman-alpha forest of 10^5 quasars will be observed in the redshift range 2.2

Published
2011
Full Text
View/download PDF

4. Aperture calculation of the Pierre Auger Observatory surface detector

Author

Allard, D., Allekotte, I., Armengaud, E., Aublin, J., Bertou, X., Chou, A., Ghia, P. L., Berisso, M. Gómez, Hamilton, J. C., Lhenry-Yvon, I., Medina, C., Navarra, G., Parizot, E., and Tripathi, A.

Subjects
Astrophysics
Abstract

We determine the instantaneous aperture and integrated exposure of the surface detector of the Pierre Auger Observatory, taking into account the trigger efficiency as a function of the energy, arrival direction (with zenith angle lower than 60 degrees) and nature of the primary cosmic-ray. We make use of the so-called Lateral Trigger Probability function (or LTP) associated with an extensive air shower, which summarizes all the relevant information about the physics of the shower, the water tank Cherenkov detector, and the triggers., Comment: Proc. of the 29th ICRC (Pune, India), LaTeX, 4 pages, 5 figures

Published
2005

5. The trigger system of the Pierre Auger Surface Detector: operation, efficiency and stability

Author

Allard, D., Armengaud, E., Allekotte, I., Allison, P., Aublin, J., Ave, M., Bauleo, P., Beatty, J., Beau, T., Bertou, X., Billoir, P., Bonifazi, C., Chou, A., Chye, J., Dagoret-Campagne, S., Dorofeev, A., Ghia, P. L., Berisso, M. Gomez, Gorgi, A., Hamilton, J. C., Harton, J., Knapik, R., Lachaud, C., Lhenry-Yvon, I., Letessier-Selvon, A., Matthews, J., Medina, C., Meyhandan, R., Navarra, G., Nitz, D., Parizot, E., Revenu, B., Szadkowski, Z., and Yamamoto, T.

Subjects
Astrophysics
Abstract

The trigger system of the Surface Detector (SD) of the Pierre Auger Observatory is described, from the identification of candidate showers ($E>1$ EeV) at the level of a single station, among a huge background (mainly single muons), up to the selection of real events and the rejection of random coincidences at a higher central trigger level (including the reconstruction accuracy). Efficiency of a single station trigger is evaluated using real data , and the high performance of event selection hierarchy will be demonstrated., Comment: 4 pages, 2 figures, ICRC2005

Published
2005

6. Asymfast, a method for convolving maps with asymmetric main beams

Author

Tristram, M., Hamilton, J. -C., Macias-Perez, J. F., and Renault, C.

Subjects
Astrophysics
Abstract

We describe a fast and accurate method to perform the convolution of a sky map with a general asymmetric main beam along any given scanning strategy. The method is based on the decomposition of the beam as a sum of circular functions, here Gaussians. It can be easily implemented and is much faster than pixel-by-pixel convolution. In addition, Asymfast can be used to estimate the effective circularized beam transfer functions of CMB instruments with non-symmetric main beam. This is shown using realistic simulations and by comparison to analytical approximations which are available for Gaussian elliptical beams. Finally, the application of this technique to Archeops data is also described. Although developped within the framework of Cosmic Microwave Background observations, our method can be applied to other areas of astrophysics., Comment: 9 pages, 4 figures, Phys. Rev. D, in press

Published
2003
Full Text
View/download PDF

7. Dislocation Emission around Nanoindentations on a (001) fcc Metal Surface Studied by STM and Atomistic Simulations

Author

de la Fuente, O. Rodriguez, Zimmerman, J. A., Gonzalez, M. A., de la Figuera, J., Hamilton, J. C., Pai, Woei Wu, and Rojo, J. M.

Subjects
Condensed Matter - Materials Science
Abstract

We present a combined study by Scanning Tunneling Microscopy and atomistic simulations of the emission of dissociated dislocation loops by nanoindentation on a (001) fcc surface. The latter consist of two stacking-fault ribbons bounded by Shockley partials and a stair-rod dislocation. These dissociated loops, which intersect the surface, are shown to originate from loops of interstitial character emitted along the <110> directions and are usually located at hundreds of angstroms away from the indentation point. Simulations reproduce the nucleation and glide of these dislocation loops., Comment: 10 pages, 4 figures

Published
2002
Full Text
View/download PDF

8. Type Ia supernova rate at $z \sim 0.1$

Author

Hardin, D., Afonso, C., Alard, C., Albert, J. N., Amadon, A., Andersen, J., Ansari, R., Aubourg, É., Bareyre, P., Bauer, F., Beaulieu, J. P., Blanc, G., Bouquet, A., Char, S., Charlot, X., Couchot, F., Coutures, C., Derue, F., Ferlet, R., Glicenstein, J. F., Goldman, B., Gould, A., Graff, D., Gros, M., Haissinski, J., Hamilton, J. C., de Kat, J., Kim, A., Lasserre, T., Lesquoy, É., Loup, C., Magneville, C., Mansoux, B., Marquette, J. B., Maurice, É., Milsztajn, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Prévot, L., Regnault, N., Rich, J., Spiro, M., Vidal-Madjar, A., Vigroux, L., Zylberajch, S., and collaboration, The EROS

Subjects
Astrophysics
Abstract

We present the EROS nearby supernova ($z \sim 0.02 - 0.2$) search and the analysis of the first year of data (1997). A total of 80 square degrees were surveyed. Eight supernov{\ae} were detected, four of which were spectroscopically identified as type Ia supernov{\ae}. The search efficiency was determined with a Monte-Carlo simulation taking into account the efficiencies for both supernova detection and host galaxy identification. Assuming that for a given galaxy the supernova rate is proportional to the galactic luminosity, we compute a type Ia supernova explosion rate of: ${\cal R} = 0.44 {}_{-0.21}^{+0.35} {}_{-0.07}^{+0.13} h^2: / 10^{10} \lbsun / 100 {\rm yrs}$ at an average redshift of $\sim 0.1$ where the errors are respectively statistical and systematic (type misidentification included)., Comment: 8 pages, 6 figures, accepted in A&A

Published
2000

9. Qubic: the q and u bolometric interferometer for cosmology

Author

Zmuidzinas, J, Gao, JR, Piat, M, Battistelli, E, De Bernardis, P, Dalessandro, G, De Petris, M, Grandsire, L, Hamilton, J, Hoang, T, Marnieros, S, Masi, S, Mennella, A, Mousset, L, Osullivan, C, Prele, D, Stankowiak, G, Tartari, A, Thermeau, J, Torchinsky, S, Voisin, F, Zannoni, M, Ade, P, Alberro, J, Almela, A, Amico, G, Arnaldi, L, Auguste, D, Aumont, J, Azzoni, S, Banfi, S, Belier, B, Bau, A, Bennett, D, Berge, L, Bernard, J, Bersanelli, M, Bigot-Sazy, M, Bonaparte, J, Bonis, J, Bunn, E, Burke, D, Buzi, D, Cavaliere, F, Chanial, P, Chapron, C, Charlassier, R, Cobos Cerutti, A, Columbro, F, Coppolecchia, A, De Gasperis, G, De Leo, M, Dheilly, S, Duca, C, Dumoulin, L, Etchegoyen, A, Fasciszewski, A, Ferreyro, L, Fracchia, D, Franceschet, C, Gamboa Lerena, M, Ganga, K, Garcia, B, Garcia Redondo, M, Gaspard, M, Gayer, D, Gervasi, M, Giard, M, Gilles, V, Giraud-Heraud, Y, Gomez Berisso, M, Gonzalez, M, Gradziel, M, Hampel, M, Harari, D, Henrot-Versille, S, Incardona, F, Jules, E, Kaplan, J, Kristukat, C, Lamagna, L, Loucatos, S, Louis, T, Maffei, B, Marty, W, Mattei, A, May, A, Mcculloch, M, Mele, L, Melo, D, Montier, L, Mundo, L, Murphy, J, Nati, F, Olivicri, E, Oriol, C, Paiella, A, Pajot, F, Passerini, A, Pastoriza, H, Pelosi, A, Perbost, C, Perciballi, M, Pezzotta, F, Piacentini, F, Piccirillo, L, Pisano, G, Platino, M, Polenta, G, Puddu, R, Rambaud, D, Rasztocky, E, Ringegni, P, Romero, G, Salum, J, Schillaci, A, Scoccola, C, Scully, S, Spinelli, S, Stolpovskiy, M, Supanitsky, A, Timbie, P, Tomasi, M, Tucker, C, Tucker, G, Vigano, D, Vittorio, N, Wicek, F, Wright, M, Zullo, A, Piat M., Battistelli E. S., De Bernardis P., Dalessandro G., De Petris M., Grandsire L., Hamilton J. -C., Hoang T. D., Marnieros S., Masi S., Mennella A., Mousset L., Osullivan C., Prele D., Stankowiak G., Tartari A., Thermeau J. -P., Torchinsky S. A., Voisin F., Zannoni M., Ade P., Alberro J. G., Almela A., Amico G., Arnaldi L. H., Auguste D., Aumont J., Azzoni S., Banfi S., Belier B., Bau A., Bennett D., Berge L., Bernard J. -Ph., Bersanelli M., Bigot-Sazy M. -A., Bonaparte J., Bonis J., Bunn E., Burke D., Buzi D., Cavaliere F., Chanial P., Chapron C., Charlassier R., Cobos Cerutti A. C., Columbro F., Coppolecchia A., De Gasperis G., De Leo M., Dheilly S., Duca C., Dumoulin L., Etchegoyen A., Fasciszewski A., Ferreyro L. P., Fracchia D., Franceschet C., Gamboa Lerena M. M., Ganga K. M., Garcia B., Garcia Redondo M. E., Gaspard M., Gayer D., Gervasi M., Giard M., Gilles V., Giraud-Heraud Y., Gomez Berisso M., Gonzalez M., Gradziel M., Hampel M. R., Harari D., Henrot-Versille S., Incardona F., Jules E., Kaplan J., Kristukat C., Lamagna L., Loucatos S., Louis T., Maffei B., Marty W., Mattei A., May A., McCulloch M., Mele L., Melo D., Montier L., Mundo L. M., Murphy J. A., Murphy J. D., Nati F., Olivicri E., Oriol C., Paiella A., Pajot F., Passerini A., Pastoriza H., Pelosi A., Perbost C., Perciballi M., Pezzotta F., Piacentini F., Piccirillo L., Pisano G., Platino M., Polenta G., Puddu R., Rambaud D., Rasztocky E., Ringegni P., Romero G. E., Salum J. M., Schillaci A., Scoccola C. G., Scully S., Spinelli S., Stolpovskiy M., Supanitsky A. D., Timbie P., Tomasi M., Tucker C., Tucker G., Vigano D., Vittorio N., Wicek F., Wright M., Zullo A., Zmuidzinas, J, Gao, JR, Piat, M, Battistelli, E, De Bernardis, P, Dalessandro, G, De Petris, M, Grandsire, L, Hamilton, J, Hoang, T, Marnieros, S, Masi, S, Mennella, A, Mousset, L, Osullivan, C, Prele, D, Stankowiak, G, Tartari, A, Thermeau, J, Torchinsky, S, Voisin, F, Zannoni, M, Ade, P, Alberro, J, Almela, A, Amico, G, Arnaldi, L, Auguste, D, Aumont, J, Azzoni, S, Banfi, S, Belier, B, Bau, A, Bennett, D, Berge, L, Bernard, J, Bersanelli, M, Bigot-Sazy, M, Bonaparte, J, Bonis, J, Bunn, E, Burke, D, Buzi, D, Cavaliere, F, Chanial, P, Chapron, C, Charlassier, R, Cobos Cerutti, A, Columbro, F, Coppolecchia, A, De Gasperis, G, De Leo, M, Dheilly, S, Duca, C, Dumoulin, L, Etchegoyen, A, Fasciszewski, A, Ferreyro, L, Fracchia, D, Franceschet, C, Gamboa Lerena, M, Ganga, K, Garcia, B, Garcia Redondo, M, Gaspard, M, Gayer, D, Gervasi, M, Giard, M, Gilles, V, Giraud-Heraud, Y, Gomez Berisso, M, Gonzalez, M, Gradziel, M, Hampel, M, Harari, D, Henrot-Versille, S, Incardona, F, Jules, E, Kaplan, J, Kristukat, C, Lamagna, L, Loucatos, S, Louis, T, Maffei, B, Marty, W, Mattei, A, May, A, Mcculloch, M, Mele, L, Melo, D, Montier, L, Mundo, L, Murphy, J, Nati, F, Olivicri, E, Oriol, C, Paiella, A, Pajot, F, Passerini, A, Pastoriza, H, Pelosi, A, Perbost, C, Perciballi, M, Pezzotta, F, Piacentini, F, Piccirillo, L, Pisano, G, Platino, M, Polenta, G, Puddu, R, Rambaud, D, Rasztocky, E, Ringegni, P, Romero, G, Salum, J, Schillaci, A, Scoccola, C, Scully, S, Spinelli, S, Stolpovskiy, M, Supanitsky, A, Timbie, P, Tomasi, M, Tucker, C, Tucker, G, Vigano, D, Vittorio, N, Wicek, F, Wright, M, Zullo, A, Piat M., Battistelli E. S., De Bernardis P., Dalessandro G., De Petris M., Grandsire L., Hamilton J. -C., Hoang T. D., Marnieros S., Masi S., Mennella A., Mousset L., Osullivan C., Prele D., Stankowiak G., Tartari A., Thermeau J. -P., Torchinsky S. A., Voisin F., Zannoni M., Ade P., Alberro J. G., Almela A., Amico G., Arnaldi L. H., Auguste D., Aumont J., Azzoni S., Banfi S., Belier B., Bau A., Bennett D., Berge L., Bernard J. -Ph., Bersanelli M., Bigot-Sazy M. -A., Bonaparte J., Bonis J., Bunn E., Burke D., Buzi D., Cavaliere F., Chanial P., Chapron C., Charlassier R., Cobos Cerutti A. C., Columbro F., Coppolecchia A., De Gasperis G., De Leo M., Dheilly S., Duca C., Dumoulin L., Etchegoyen A., Fasciszewski A., Ferreyro L. P., Fracchia D., Franceschet C., Gamboa Lerena M. M., Ganga K. M., Garcia B., Garcia Redondo M. E., Gaspard M., Gayer D., Gervasi M., Giard M., Gilles V., Giraud-Heraud Y., Gomez Berisso M., Gonzalez M., Gradziel M., Hampel M. R., Harari D., Henrot-Versille S., Incardona F., Jules E., Kaplan J., Kristukat C., Lamagna L., Loucatos S., Louis T., Maffei B., Marty W., Mattei A., May A., McCulloch M., Mele L., Melo D., Montier L., Mundo L. M., Murphy J. A., Murphy J. D., Nati F., Olivicri E., Oriol C., Paiella A., Pajot F., Passerini A., Pastoriza H., Pelosi A., Perbost C., Perciballi M., Pezzotta F., Piacentini F., Piccirillo L., Pisano G., Platino M., Polenta G., Puddu R., Rambaud D., Rasztocky E., Ringegni P., Romero G. E., Salum J. M., Schillaci A., Scoccola C. G., Scully S., Spinelli S., Stolpovskiy M., Supanitsky A. D., Timbie P., Tomasi M., Tucker C., Tucker G., Vigano D., Vittorio N., Wicek F., Wright M., and Zullo A.

Abstract

QUBIC (Q and U bolometric interferometer for cosmology) is an international ground-based experiment dedicated to the measurement of the polarized fluctuations of the cosmic microwave background (CMB). It is based on bolometric interferometry, an original detection technique which combines the immunity to systematic effects of an interferometer with the sensitivity of low temperature incoherent detectors. QUBIC will be deployed in Argentina, at the Alto Chorrillos mountain site near San Antonio de los Cobres, in the Salta province. The QUBIC detection chain consists of 2048 NbSi transition edge sensors (TESs) cooled to 320 mK. The voltage-biased TESs are read out with time domain multiplexing based on superconducting quantum interference devices (SQUIDs) at 1 K and a novel SiGe application-specific integrated circuit (ASIC) at 60 K allowing an unprecedented multiplexing (MUX) factor equal to 128 to be reached. The current QUBIC version is based on a reduced number of detectors (1/4) in order to validate the detection technique. The QUBIC experiment is currently being validated in the lab in Salta (Argentina) before going to the site for observations. This paper presents the main results of the characterization phase with a focus on the detectors and readout system.

Published
2022

11. QUBIC: the Q&U Bolometric Interferometer for Cosmology

Author

Piat, M., Battistelli, E., Baù, A., Bennett, D., Bergé, L., Bernard, J.-P., de Bernardis, P., Bigot-Sazy, M.-A., Bordier, G., Bounab, A., Bréelle, E., Bunn, E. F., Calvo, M., Charlassier, R., Collin, S., Cruciani, A., Curran, G., Dumoulin, L., Gault, A., Gervasi, M., Ghribi, A., Giard, M., Giordano, C., Giraud-Héraud, Y., Gradziel, M., Guglielmi, L., Hamilton, J.-C., Haynes, V., Kaplan, J., Korotkov, A., Landé, J., Maffei, B., Maiello, M., Malu, S., Marnieros, S., Martino, J., Masi, S., Montier, L., Murphy, A., Nati, F., O’Sullivan, C., Pajot, F., Parisel, C., Passerini, A., Peterzen, S., Piacentini, F., Piccirillo, L., Pisano, G., Polenta, G., Prêle, D., Romano, D., Rosset, C., Salatino, M., Schillaci, A., Sironi, G., Sordini, R., Spinelli, S., Tartari, A., Timbie, P., Tucker, G., Vibert, L., Voisin, F., Watson, R. A., and Zannoni, M.

Published
2012
Full Text
View/download PDF

13. Chemical and Mineralogical Characterization of a Hematite-bearing Ridge on Mauna Kea, Hawaii: A Potential Mineralogical Process Analog for the Mount Sharp Hematite Ridge

Author

Graff, T. G, Morris, R. V, Ming, D. W, Hamilton, J. C, Adams, M, Fraeman, A. A, Arvidson, R. E, Catalano, J. G, and Mertzman, S. A

Subjects
Geosciences (General), Lunar And Planetary Science And Exploration
Abstract

The Mars Science Laboratory (MSL) rover Curiosity landed in Gale Crater in August 2012 and is currently roving towards the layered central mound known as Mount Sharp [1]. Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) hyperspectral data indicate Mount Sharp contains an ~5 km stratigraphic sequence including Fe-Mg smectites, hematite, and hydrated sulfates in the lower layers separated by an unconformity from the overlying anhydrous strata [1,2,3]. Hematite was initially detected in CRISM data to occur in the lower sulfate layers on the north side of the mound [2]. [3] further mapped a distinct hematite detection occurring as part of a ~200 m wide ridge that extends ~6.5 km NE-SW, approximately parallel with the base of Mount Sharp. It is likely a target for in-situ analyses by Curiosity. We document here the occurrence of a stratum of hematite-bearing breccia that is exposed on the Puu Poliahu cinder cone near the summit of Mauna Kea volcano (Hawaii) (Fig.1). The stratum is more resistant to weathering than surrounding material, giving it the appearance of a ridge. The Mauna Kea hematite ridge is thus arguably a potential terrestrial mineralogical and process analog for the Gale Crater hematite ridge. We are acquiring a variety of chemical and mineralogical data on the Mauna Kea samples, with a focus on the chemical and mineralogical information already available or planned for the Gale hematite ridge.

Published
2014

15. TES Bolometer Arrays for the QUBIC B-Mode CMB Experiment

Author

Marnieros, S, Ade, P, Alberro, J, Almela, A, Amico, G, Arnaldi, L, Auguste, D, Aumont, J, Azzoni, S, Banfi, S, Battaglia, P, Battistelli, E, Bau, A, Belier, B, Bennett, D, Berge, L, Bernard, J, Bersanelli, M, Bigot-Sazy, M, Bleurvacq, N, Bonaparte, J, Bonis, J, Bottani, A, Bunn, E, Burke, D, Buzi, D, Cavaliere, F, Chanial, P, Chapron, C, Charlassier, R, Columbro, F, Coppolecchia, A, D'Alessandro, G, de Bernardis, P, De Gasperis, G, De Leo, M, De Petris, M, Dheilly, S, Dumoulin, L, Etchegoyen, A, Fasciszewski, A, Ferreyro, L, Fracchia, D, Franceschet, C, Gamboa Lerena, M, Ganga, K, Garcia, B, Garcia Redondo, M, Gaspard, M, Gayer, D, Gervasi, M, Giard, M, Gilles, V, Giraud-Heraud, Y, Gomez Berisso, M, Gonzalez, M, Gradziel, M, Grandsire, L, Hamilton, J, Harari, D, Henrot-Versille, S, Hoang, D, Incardona, F, Jules, E, Kaplan, J, Kristukat, C, Lamagna, L, Loucatos, S, Louis, T, Maffei, B, Marty, W, Masi, S, Mattei, A, May, A, Mcculloch, M, Mele, L, Melhuish, S, Mennella, A, Montier, L, Mousset, L, Mundo, L, Murphy, J, Nati, F, Olivieri, E, Oriol, C, O'Sullivan, C, Paiella, A, Pajot, F, Passerini, A, Pastoriza, H, Pelosi, A, Perbost, C, Perciballi, M, Pezzotta, F, Piacentini, F, Piat, M, Piccirillo, L, Pisano, G, Platino, M, Polenta, G, Prele, D, Puddu, R, Rambaud, D, Ringegni, P, Romero, G, Salatino, M, Salum, J, Schillaci, A, Scoccola, C, Scully, S, Spinelli, S, Stankowiak, G, Stolpovskiy, M, Tartari, A, Thermeau, J, Timbie, P, Tomasi, M, Torchinsky, S, Tucker, G, Tucker, C, Vigano, D, Vittorio, N, Voisin, F, Wicek, F, Zannoni, M, Zullo, A, Marnieros S., Ade P., Alberro J. G., Almela A., Amico G., Arnaldi L. H., Auguste D., Aumont J., Azzoni S., Banfi S., Battaglia P., Battistelli E. S., Bau A., Belier B., Bennett D., Berge L., Bernard J. -P., Bersanelli M., Bigot-Sazy M. -A., Bleurvacq N., Bonaparte J., Bonis J., Bottani A., Bunn E., Burke D., Buzi D., Cavaliere F., Chanial P., Chapron C., Charlassier R., Columbro F., Coppolecchia A., D'Alessandro G., de Bernardis P., De Gasperis G., De Leo M., De Petris M., Dheilly S., Dumoulin L., Etchegoyen A., Fasciszewski A., Ferreyro L. P., Fracchia D., Franceschet C., Gamboa Lerena M. M., Ganga K., Garcia B., Garcia Redondo M. E., Gaspard M., Gayer D., Gervasi M., Giard M., Gilles V., Giraud-Heraud Y., Gomez Berisso M., Gonzalez M., Gradziel M., Grandsire L., Hamilton J. -C., Harari D., Henrot-Versille S., Hoang D. T., Incardona F., Jules E., Kaplan J., Kristukat C., Lamagna L., Loucatos S., Louis T., Maffei B., Marty W., Masi S., Mattei A., May A., McCulloch M., Mele L., Melhuish S., Mennella A., Montier L., Mousset L., Mundo L. M., Murphy J. A., Murphy J. D., Nati F., Olivieri E., Oriol C., O'Sullivan C., Paiella A., Pajot F., Passerini A., Pastoriza H., Pelosi A., Perbost C., Perciballi M., Pezzotta F., Piacentini F., Piat M., Piccirillo L., Pisano G., Platino M., Polenta G., Prele D., Puddu R., Rambaud D., Ringegni P., Romero G. E., Salatino M., Salum J. M., Schillaci A., Scoccola C., Scully S., Spinelli S., Stankowiak G., Stolpovskiy M., Tartari A., Thermeau J. -P., Timbie P., Tomasi M., Torchinsky S., Tucker G., Tucker C., Vigano D., Vittorio N., Voisin F., Wicek F., Zannoni M., Zullo A., Marnieros, S, Ade, P, Alberro, J, Almela, A, Amico, G, Arnaldi, L, Auguste, D, Aumont, J, Azzoni, S, Banfi, S, Battaglia, P, Battistelli, E, Bau, A, Belier, B, Bennett, D, Berge, L, Bernard, J, Bersanelli, M, Bigot-Sazy, M, Bleurvacq, N, Bonaparte, J, Bonis, J, Bottani, A, Bunn, E, Burke, D, Buzi, D, Cavaliere, F, Chanial, P, Chapron, C, Charlassier, R, Columbro, F, Coppolecchia, A, D'Alessandro, G, de Bernardis, P, De Gasperis, G, De Leo, M, De Petris, M, Dheilly, S, Dumoulin, L, Etchegoyen, A, Fasciszewski, A, Ferreyro, L, Fracchia, D, Franceschet, C, Gamboa Lerena, M, Ganga, K, Garcia, B, Garcia Redondo, M, Gaspard, M, Gayer, D, Gervasi, M, Giard, M, Gilles, V, Giraud-Heraud, Y, Gomez Berisso, M, Gonzalez, M, Gradziel, M, Grandsire, L, Hamilton, J, Harari, D, Henrot-Versille, S, Hoang, D, Incardona, F, Jules, E, Kaplan, J, Kristukat, C, Lamagna, L, Loucatos, S, Louis, T, Maffei, B, Marty, W, Masi, S, Mattei, A, May, A, Mcculloch, M, Mele, L, Melhuish, S, Mennella, A, Montier, L, Mousset, L, Mundo, L, Murphy, J, Nati, F, Olivieri, E, Oriol, C, O'Sullivan, C, Paiella, A, Pajot, F, Passerini, A, Pastoriza, H, Pelosi, A, Perbost, C, Perciballi, M, Pezzotta, F, Piacentini, F, Piat, M, Piccirillo, L, Pisano, G, Platino, M, Polenta, G, Prele, D, Puddu, R, Rambaud, D, Ringegni, P, Romero, G, Salatino, M, Salum, J, Schillaci, A, Scoccola, C, Scully, S, Spinelli, S, Stankowiak, G, Stolpovskiy, M, Tartari, A, Thermeau, J, Timbie, P, Tomasi, M, Torchinsky, S, Tucker, G, Tucker, C, Vigano, D, Vittorio, N, Voisin, F, Wicek, F, Zannoni, M, Zullo, A, Marnieros S., Ade P., Alberro J. G., Almela A., Amico G., Arnaldi L. H., Auguste D., Aumont J., Azzoni S., Banfi S., Battaglia P., Battistelli E. S., Bau A., Belier B., Bennett D., Berge L., Bernard J. -P., Bersanelli M., Bigot-Sazy M. -A., Bleurvacq N., Bonaparte J., Bonis J., Bottani A., Bunn E., Burke D., Buzi D., Cavaliere F., Chanial P., Chapron C., Charlassier R., Columbro F., Coppolecchia A., D'Alessandro G., de Bernardis P., De Gasperis G., De Leo M., De Petris M., Dheilly S., Dumoulin L., Etchegoyen A., Fasciszewski A., Ferreyro L. P., Fracchia D., Franceschet C., Gamboa Lerena M. M., Ganga K., Garcia B., Garcia Redondo M. E., Gaspard M., Gayer D., Gervasi M., Giard M., Gilles V., Giraud-Heraud Y., Gomez Berisso M., Gonzalez M., Gradziel M., Grandsire L., Hamilton J. -C., Harari D., Henrot-Versille S., Hoang D. T., Incardona F., Jules E., Kaplan J., Kristukat C., Lamagna L., Loucatos S., Louis T., Maffei B., Marty W., Masi S., Mattei A., May A., McCulloch M., Mele L., Melhuish S., Mennella A., Montier L., Mousset L., Mundo L. M., Murphy J. A., Murphy J. D., Nati F., Olivieri E., Oriol C., O'Sullivan C., Paiella A., Pajot F., Passerini A., Pastoriza H., Pelosi A., Perbost C., Perciballi M., Pezzotta F., Piacentini F., Piat M., Piccirillo L., Pisano G., Platino M., Polenta G., Prele D., Puddu R., Rambaud D., Ringegni P., Romero G. E., Salatino M., Salum J. M., Schillaci A., Scoccola C., Scully S., Spinelli S., Stankowiak G., Stolpovskiy M., Tartari A., Thermeau J. -P., Timbie P., Tomasi M., Torchinsky S., Tucker G., Tucker C., Vigano D., Vittorio N., Voisin F., Wicek F., Zannoni M., and Zullo A.

Abstract

QUBIC is a ground-based experiment aiming to measure the B-mode polarization of the cosmic microwave background. The developed instrument is an innovative two-frequency band bolometric interferometer that will operate at 300 mK with NbSi TES arrays. In this paper, we describe the fabrication process of the detectors.

Published
2020

16. The QUBIC instrument for CMB polarization measurements

Author

Mele, L, Ade, P, Alberro, J, Almela, A, Amico, G, Arnaldi, L, Auguste, D, Aumont, J, Azzoni, S, Banfi, S, Battistelli, E, Ba, A, B lier, B, Bennett, D, Berge, L, Bernard, J, Bersanelli, M, Bigot-Sazy, M, Bleurvacq, N, Bonaparte, J, Bonis, J, Bottani, A, Bunn, E, Burke, D, Buzi, D, Cavaliere, F, Chanial, P, Chapron, C, Charlassier, R, Columbro, F, Coppolecchia, A, D'Alessandro, G, Bernardis, P, Gasperis, G, Leo, M, Petris, M, Dheilly, S, Dumoulin, L, Etchegoyen, A, Fasciszewski, A, Ferreyro, L, Fracchia, D, Franceschet, C, Lerena, M, Ganga, K, Garcia, B, Redondo, M, Gaspard, M, Gayer, D, Gervasi, M, Giard, M, Gilles, V, Giraud-Heraud, Y, Gomez Berisso, M, Gonzalez, M, Gradziel, M, Grandsire, L, Hamilton, J, Harari, D, Henrot-Versille, S, Hoang, D, Incardona, F, Jules, E, Kaplan, J, Kristukat, C, Lamagna, L, Loucatos, S, Louis, T, Maffei, B, Marnieros, S, Marty, W, Masi, S, Mattei, A, May, A, Mcculloch, M, Melhuish, S, Mennella, A, Montier, L, Mousset, L, Mundo, L, Murphy, J, Nati, F, Olivieri, E, Oriol, C, O'Sullivan, C, Paiella, A, Pajot, F, Passerini, A, Pastoriza, H, Pelosi, A, Perbost, C, Perciballi, M, Pezzotta, F, Piacentini, F, Piat, M, Piccirillo, L, Pisano, G, Platino, M, Polenta, G, Pr le, D, Puddu, R, Rambaud, D, Ringegni, P, Romero, G, Salatino, M, Salum, J, Schillaci, A, Scoccola, C, Scully, S, Spinelli, S, Stankowiak, G, Stolpovskiy, M, Tartari, A, Thermeau, J, Timbie, P, Tomasi, M, Torchinsky, S, Tristram, M, Tucker, G, Tucker, C, Vigan, D, Vittorio, N, Voisin, F, Wicek, F, Zannoni, M, Zullo, A, Mele L., Ade P., Alberro J. G., Almela A., Amico G., Arnaldi L. H., Auguste D., Aumont J., Azzoni S., Banfi S., Battistelli E. S., Ba A., B lier B., Bennett D., Berge L., Bernard J. -P., Bersanelli M., Bigot-Sazy M. -A., Bleurvacq N., Bonaparte J., Bonis J., Bottani A., Bunn E., Burke D., Buzi D., Cavaliere F., Chanial P., Chapron C., Charlassier R., Columbro F., Coppolecchia A., D'Alessandro G., Bernardis P. D., Gasperis G. D., Leo M. D., Petris M. D., Dheilly S., Dumoulin L., Etchegoyen A., Fasciszewski A., Ferreyro L. P., Fracchia D., Franceschet C., Lerena M. M. G., Ganga K., Garcia B., Redondo M. E. G., Gaspard M., Gayer D., Gervasi M., Giard M., Gilles V., Giraud-Heraud Y., Gomez Berisso M., Gonzalez M., Gradziel M., Grandsire L., Hamilton J. -C., Harari D., Henrot-Versille S., Hoang D. T., Incardona F., Jules E., Kaplan J., Kristukat C., Lamagna L., Loucatos S., Louis T., Maffei B., Marnieros S., Marty W., Masi S., Mattei A., May A., McCulloch M., Melhuish S., Mennella A., Montier L., Mousset L., Mundo L. M., Murphy J. A., Murphy J. D., Nati F., Olivieri E., Oriol C., O'Sullivan C., Paiella A., Pajot F., Passerini A., Pastoriza H., Pelosi A., Perbost C., Perciballi M., Pezzotta F., Piacentini F., Piat M., Piccirillo L., Pisano G., Platino M., Polenta G., Pr le D., Puddu R., Rambaud D., Ringegni P., Romero G. E., Salatino M., Salum J. M., Schillaci A., Scoccola C., Scully S., Spinelli S., Stankowiak G., Stolpovskiy M., Tartari A., Thermeau J. -P., Timbie P., Tomasi M., Torchinsky S., Tristram M., Tucker G., Tucker C., Vigan D., Vittorio N., Voisin F., Wicek F., Zannoni M., Zullo A., Mele, L, Ade, P, Alberro, J, Almela, A, Amico, G, Arnaldi, L, Auguste, D, Aumont, J, Azzoni, S, Banfi, S, Battistelli, E, Ba, A, B lier, B, Bennett, D, Berge, L, Bernard, J, Bersanelli, M, Bigot-Sazy, M, Bleurvacq, N, Bonaparte, J, Bonis, J, Bottani, A, Bunn, E, Burke, D, Buzi, D, Cavaliere, F, Chanial, P, Chapron, C, Charlassier, R, Columbro, F, Coppolecchia, A, D'Alessandro, G, Bernardis, P, Gasperis, G, Leo, M, Petris, M, Dheilly, S, Dumoulin, L, Etchegoyen, A, Fasciszewski, A, Ferreyro, L, Fracchia, D, Franceschet, C, Lerena, M, Ganga, K, Garcia, B, Redondo, M, Gaspard, M, Gayer, D, Gervasi, M, Giard, M, Gilles, V, Giraud-Heraud, Y, Gomez Berisso, M, Gonzalez, M, Gradziel, M, Grandsire, L, Hamilton, J, Harari, D, Henrot-Versille, S, Hoang, D, Incardona, F, Jules, E, Kaplan, J, Kristukat, C, Lamagna, L, Loucatos, S, Louis, T, Maffei, B, Marnieros, S, Marty, W, Masi, S, Mattei, A, May, A, Mcculloch, M, Melhuish, S, Mennella, A, Montier, L, Mousset, L, Mundo, L, Murphy, J, Nati, F, Olivieri, E, Oriol, C, O'Sullivan, C, Paiella, A, Pajot, F, Passerini, A, Pastoriza, H, Pelosi, A, Perbost, C, Perciballi, M, Pezzotta, F, Piacentini, F, Piat, M, Piccirillo, L, Pisano, G, Platino, M, Polenta, G, Pr le, D, Puddu, R, Rambaud, D, Ringegni, P, Romero, G, Salatino, M, Salum, J, Schillaci, A, Scoccola, C, Scully, S, Spinelli, S, Stankowiak, G, Stolpovskiy, M, Tartari, A, Thermeau, J, Timbie, P, Tomasi, M, Torchinsky, S, Tristram, M, Tucker, G, Tucker, C, Vigan, D, Vittorio, N, Voisin, F, Wicek, F, Zannoni, M, Zullo, A, Mele L., Ade P., Alberro J. G., Almela A., Amico G., Arnaldi L. H., Auguste D., Aumont J., Azzoni S., Banfi S., Battistelli E. S., Ba A., B lier B., Bennett D., Berge L., Bernard J. -P., Bersanelli M., Bigot-Sazy M. -A., Bleurvacq N., Bonaparte J., Bonis J., Bottani A., Bunn E., Burke D., Buzi D., Cavaliere F., Chanial P., Chapron C., Charlassier R., Columbro F., Coppolecchia A., D'Alessandro G., Bernardis P. D., Gasperis G. D., Leo M. D., Petris M. D., Dheilly S., Dumoulin L., Etchegoyen A., Fasciszewski A., Ferreyro L. P., Fracchia D., Franceschet C., Lerena M. M. G., Ganga K., Garcia B., Redondo M. E. G., Gaspard M., Gayer D., Gervasi M., Giard M., Gilles V., Giraud-Heraud Y., Gomez Berisso M., Gonzalez M., Gradziel M., Grandsire L., Hamilton J. -C., Harari D., Henrot-Versille S., Hoang D. T., Incardona F., Jules E., Kaplan J., Kristukat C., Lamagna L., Loucatos S., Louis T., Maffei B., Marnieros S., Marty W., Masi S., Mattei A., May A., McCulloch M., Melhuish S., Mennella A., Montier L., Mousset L., Mundo L. M., Murphy J. A., Murphy J. D., Nati F., Olivieri E., Oriol C., O'Sullivan C., Paiella A., Pajot F., Passerini A., Pastoriza H., Pelosi A., Perbost C., Perciballi M., Pezzotta F., Piacentini F., Piat M., Piccirillo L., Pisano G., Platino M., Polenta G., Pr le D., Puddu R., Rambaud D., Ringegni P., Romero G. E., Salatino M., Salum J. M., Schillaci A., Scoccola C., Scully S., Spinelli S., Stankowiak G., Stolpovskiy M., Tartari A., Thermeau J. -P., Timbie P., Tomasi M., Torchinsky S., Tristram M., Tucker G., Tucker C., Vigan D., Vittorio N., Voisin F., Wicek F., Zannoni M., and Zullo A.

Abstract

Measurements of cosmic microwave background (CMB) polarization may reveal the presence of a background of gravitational waves produced during cosmic inflation, providing thus a test of inflationary models. The Q&U Bolometric Interferometer for Cosmology (QUBIC) is an experiment designed to measure the CMB polarization. It is based on the novel concept of bolometric interferometry, which combines the sensitivity of bolometric detectors with the properties of beam synthesis and control of calibration offered by interferometers. To modulate and extract the input polarized signal of the CMB, QUBIC exploits Stokes polarimetry based on a rotating half-wave plate (HWP). In this work, we illustrate the design of the QUBIC instrument, focusing on the polarization modulation system, and we present preliminary results of beam calibrations and the performance of the HWP rotator at 300 K.

Published
2020

17. Hydrothermal Precipitation of Sanidine (Adularia) Having Full Al,Si Structural Disorder and Specular Hematite at Maunakea Volcano (Hawai'i) and at Gale Crater (Mars)

Author

Morris, R. V., primary, Rampe, E. B., additional, Vaniman, D. T., additional, Christoffersen, R., additional, Yen, A. S., additional, Morrison, S. M., additional, Ming, D. W., additional, Achilles, C. N., additional, Fraeman, A. A., additional, Le, L., additional, Tu, V. M., additional, Ott, J. P., additional, Treiman, A. H., additional, Hogancamp, J. V., additional, Graff, T. G., additional, Adams, M., additional, Hamilton, J. C., additional, Mertzman, S. A., additional, Bristow, T. F., additional, Blake, D. F., additional, Castle, N., additional, Chipera, S. J., additional, Craig, P. I., additional, Des Marais, D. J., additional, Downs, G., additional, Downs, R. T., additional, Hazen, R. M., additional, Morookian, J.‐M., additional, and Thorpe, M., additional

Published
2020
Full Text
View/download PDF

18. Chemical and Mineralogical Characterization of Acid-Sulfate Alteration of Basaltic Material on Mauna Kea Volcano, Hawaii: Jarosite and Hydrated Halloysite

Author

Graff, Trevor G, Morris, R. V, Archilles C. N, Agresti, D. G, Ming, D. W, Hamilton, J. C, Mertzman, S. A, and Smith, J

Subjects
Geophysics
Abstract

Sulfates have been identified on the martian surface during robotic surface exploration and by orbital remote sensing. Measurements at Meridiani Planum (MP) by the Alpha-Particle X-ray Spectrometer (APXS) and Mossbauer (MB) instruments on the Mars Exploration Rover Opportunity document the presence of a ubiquitous sulfate-rich outcrop (20-40% SO3) that has jarosite as an anhydrous Fe3+-sulfate [1- 3]. The presence of jarosite implies a highly acidic (pH <3) formation environment [4]. Jarosite and other sulfate minerals, including kieserite, gypsum, and alunite have also been identified in several locations in orbital remote sensing data from the MEx OMEGA and MRO CRISM instruments [e.g. 5-8]. Acid sulfate weathering of basaltic materials is an obvious pathway for formation of sulfate-bearing phases on Mars [e.g. 4, 9, 10]. In order to constrain acid-sulfate pathways on Mars, we are studying the mineralogical and chemical manifestations of acid-sulfate alteration of basaltic compositions in terrestrial environments. We have previously shown that acidsulfate alteration of tephra under hydrothermal conditions on the Puu Poliahu cone (summit region of Mauna Kea volcano, Hawaii) resulted in jarosite and alunite as sulfate-bearing alteration products [11-14]. Other, more soluble, sulfates may have formed, but were leached away by rain and melting snow. Acidsulfate processes on Puu Poliahu also formed hematite spherules similar (except in size) to the hematite spherules observed at MP as an alteration product [14]. Phyllosilicates, usually smectite }minor kaolinite are also present as alteration products [13]. We discuss here an occurrence of acid-sulfate alteration on Mauna Kea Volcano (Hawaii). We report VNIR spectra (0.35-2.5 microns ASD spectrometer), Mossbauer spectra (MER-like ESPI backscatter spectrometer), powder XRD (PANalytical), and major element chemical compositions (XRF with LOI and Fe redox) for comparison to similar data acquired or to be acquired by MRO-CRISM and MEx OMEGA, MERMB, MSL-CheMin, and MER and MSL APXS, respectively.

Published
2012

19. Use of Hawaii Analog Sites for Lunar Science and In-Situ Resource Utilization

Author

Sanders, G. B, Larson, W. E, Picard, M, and Hamilton, J. C

Subjects
Man/System Technology And Life Support
Abstract

In-Situ Resource Utilization (ISRU) and lunar science share similar objectives with respect to analyzing and characterizing the physical, mineral, and volatile materials and resources at sites of robotic and human exploration. To help mature and stress instruments, technologies, and hardware and to evaluate operations and procedures, space agencies have utilized demonstrations at analog sites on Earth before use in future missions. The US National Aeronautics and Space Administration (NASA), the Canadian Space Agency (CSA), and the German Space Agency (DLR) have utilized an analog site on the slope of Mauna Kea on the Big Island of Hawaii to test ISRU and lunar science hardware and operations in two previously held analog field tests. NASA and CSA are currently planning on a 3rd analog field test to be held in June, 2012 in Hawaii that will expand upon the successes from the previous two field tests.

Published
2011

20. Mauna Kea, Hawaii as an Analogue Site for Future Planetary Resource Exploration: Results from the 2010 ILSO-ISRU Field-Testing Campaign

Author

ten Kate, I. L, Armstrong, R, Bernhardt, B, Blummers, M, Boucher, D, Caillibot, E, Captain, J, Deleuterio, G, Farmer, J. D, Glavin, D. P, Hamilton, J. C, Klingelhoefer, G, Morris, R. V, Nunez, J. I, Quinn, J. W, Sanders, G. B, Sellar, R. G, Sigurdson, L, Taylor, R, and Zacny, K

Subjects
Lunar And Planetary Science And Exploration
Abstract

Within the framework of the International Lunar Surface Operation - In-Situ Resource Utilization Analogue Test held on January 27 - February 11, 2010 on the Mauna Kea volcano in Hawaii, a number of scientific instrument teams collaborated to characterize the field site and test instrument capabilities outside laboratory environments. In this paper, we provide a geological setting for this new field-test site, a description of the instruments that were tested during the 2010 ILSO-ISRU field campaign, and a short discussion for each instrument about the validity and use of the results obtained during the test. These results will form a catalogue that may serve as reference for future test campaigns. In this paper we provide a description and regional geological setting for a new field analogue test site for lunar resource exploration, and discuss results obtained from the 2010 ILSO-ISRU field campaign as a reference for future field-testing at this site. The following instruments were tested: a multispectral microscopic imager, MMI, a Mossbauer spectrometer, an evolved gas analyzer, VAPoR, and an oxygen and volatile extractor called RESOLVE. Preliminary results show that the sediments change from dry, organic-poor, poorly-sorted volcaniclastic sand on the surface, containing basalt, iron oxides and clays, to more water- and organic-rich, fine grained, well-sorted volcaniclastic sand, primarily consisting of iron oxides and depleted of basalt and clays. Furthermore, drilling experiments showed a very close correlation between drilling on the Moon and drilling at the test site. The ILSO-ISRU test site was an ideal location for testing strategies for in situ resource exploration at the lunar or martian surface.

Published
2010

23. QUBIC: measuring CMB polarization from Argentina

Author

de Bernardis, P., Ade, P., Amico, G., Auguste, D., Aumont, J., Banfi, S., Barbarán, G., Battaglia, P., Battistelli, E., Baù, A., Bélier, B., Bennett, D., Bergé, L., Bernard, J. P., Bersanelli, M., Bigot-Sazy, M. A., Bleurvacq, N., Bonaparte, J., Bonis, J., Bordier, Bréelle, G., Bunn, E., Burke, D., Buzi, D., Buzzelli, A., Cavaliere, F., Chanial, P., Chapron, C., Charlassier, R., Columbro, F., Coppi, G., Coppolecchia, A., Couchot, F., D'Agostino, R., D'Alessandro, G., De Gasperis, G., De Leo, M., De Petris, M., Di Donato, A., Dumoulin, L., Etchegoyen, A., Fasciszewski, A., Franceschet, C., Gamboa Lerena, M. M., García, B., Garrido, X., Gaspard, M., Gault, A., Gayer, D., Gervasi, M., Giard, M., Giraud-Heraud, Y., Gómez Berisso, M., González, M., Gradziel, M., Grandsire, L., Guerrard, E., Hamilton, J. C., Harari, D., Haynes, V., Henrot-Versillé, S., Hoang, D. T., Incardona, F., Jules, E., Kaplan, J., Korotkov, A., Kristukat, C., Lamagna, L., Loucatos, S., Louis, T., Lowitz, A., Lukovic, V., Luterstein, R., Maffei, B., Marnieros, S., Masi, S., Mattei, A., May, A., Mcculloch, M., Medina, M. C., Mele, L., Melhuish, S., Mennella, A., Montier, L., Mundo, L. M., Murphy, J. A., Murphy, J. D., Olivieri, E., O'Sullivan, C., Paiella, A., Pajot, F., Passerini, A., Pastoriza, H., Pelosi, A., Perbost, C., Perdereau, O., Pezzotta, F., Piacentini, F., Piat, M., Piccirillo, L., Pisano, G., Polenta, G., Prêle, D., Puddu, R., Rambaud, D., Ringegni, P., Romero, G. E., Salatino, M., Schillaci, A., Scóccola, C., Scully, S., Spinelli, S., Stolpovskiy, M., Suarez, F., Tartari, A., Thermeau, J. P., Timbie, P., Torchinsky, S., Tristram, M., Truongcanh, V., Tucker, G., Tucker, C., Vanneste, S., Viganò, D., Vittorio, N., Voisin, F., Watson, B., Wicek, F., Zannoni, M., and Zullo, A.

Subjects
cosmic microwave background, polarization, cosmology
Published
2018

24. 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
Full Text
View/download PDF

25. Optical modelling and analysis of the Q and U bolometric interferometer for cosmology

Author

Sadwick L.P.,Yang T., Burke, D, Gayer, D, Kalinauskaite, E, O'Sullivan, C, Murphy, J, Scully, S, De Petris, M, De Leo, M, Mennella, A, Torchinsky, S, Zannoni, M, Amico, G, Auguste, D, Aumont, J, Banfi, S, Barbaran, G, Battaglia, P, Battistelli, E, Bau, A, Belier, B, Bennett, D, Berge, L, Bernard, J, Bersanelli, M, Bigot-Sazy, M, Bleurvac, N, Bonaparte, J, Bonis, J, Bordier, G, Breelle, E, Bunn, E, Buzi, D, Buzzelli, A, Cavaliere, F, Chanial, P, Chapron, C, Charlassier, R, Columbro, F, Coppi, G, Coppolecchia, A, Couchot, F, D'Alessandro, G, D'Agostino, R, De Bernardis, P, De Gasperis, G, Di Donato, A, Drilien, A, Dumoulin, L, Etchegoyen, A, Fasciszewski, A, Franceschet, C, Gamboa-Lerena, M, Garcia, B, Garrido, X, Gaspard, M, Gault, A, Gervasi, M, Giard, M, Giraud-Heraud, Y, Gomez Berisso, M, Gonzalez, M, Gradziel, M, Grandsire, L, Guerrard, E, Hamilton, J, Harari, D, Haynes, V, Henrot-Versille, S, Hoang, D, Holtzer, N, Incardona, F, Jules, E, Kaplan, J, Korotkov, A, Kristukat, C, Lamagna, L, Lande, J, Loucatos, S, Louis, T, Lowitz, A, Lukovic, V, Luterstein, R, Maffei, B, Marnieros, S, Masi, S, Mattei, A, May, A, Mcculloch, M, Medina, M, Mele, L, Melhuish, S, Mundo, L, Montier, L, Neel, D, Olivieri, E, Paiella, A, Pajot, F, Passerini, A, Pastoriza, H, Pelosi, A, Perbost, C, Perdereau, O, Pezzotta, F, Piacentini, F, Piat, M, Piccirillo, L, Pisano, G, Polenta, G, Prele, D, Puddu, R, Rambaud, D, Rigaut, O, Ringegni, P, Romero, G, Salatino, M, Schillaci, A, Scoccola, C, Spinelli, S, Stolpovskiy, M, Suarez, F, Tartari, A, Thermeau, J, Timbie, P, Tristram, M, Truongcanh, V, Tucker, G, Tucker, C, Vigano, D, Vittorio, N, Voisin, F, Watson, B, Wicek, F, Zullo, A, Burke D., Gayer D., Kalinauskaite E., O'Sullivan C., Murphy J. D., Scully S. P., De Petris M., De Leo M., Mennella A., Torchinsky S. A., Zannoni M., Amico G., Auguste D., Aumont J., Banfi S., Barbaran G., Battaglia P., Battistelli E., Bau A., Belier B., Bennett D. G., Berge L., Bernard J. -P., Bersanelli M., Bigot-Sazy M. -A., Bleurvac N., Bonaparte J., Bonis J., Bordier G., Breelle E., Bunn E. F., Buzi D., Buzzelli A., Cavaliere F., Chanial P., Chapron C., Charlassier R., Columbro F., Coppi G., Coppolecchia A., Couchot F., D'Alessandro G., D'Agostino R., De Bernardis P., De Gasperis G., Di Donato A., Drilien A. -A., Dumoulin L., Etchegoyen A., Fasciszewski A., Franceschet C., Gamboa-Lerena M., Garcia B., Garrido X., Gaspard M., Gault A., Gervasi M., Giard M., Giraud-Heraud Y., Gomez Berisso M., Gonzalez M., Gradziel M. L., Grandsire L., Guerrard E., Hamilton J. -C., Harari D., Haynes V., Henrot-Versille S., Hoang D. T., Holtzer N., Incardona F., Jules E., Kaplan J., Korotkov A. L., Kristukat C., Lamagna L., Lande J., Loucatos S., Louis T., Lowitz A., Lukovic V., Luterstein R., Maffei B., Marnieros S., Masi S., Mattei A., May A. J., McCulloch M. A., Medina M. C., Mele L., Melhuish S. J., Mundo L., Montier L., Murphy J. A., Neel D., Olivieri E., Paiella A., Pajot F., Passerini A., Pastoriza H., Pelosi A., Perbost C., Perdereau O., Pezzotta F., Piacentini F., Piat M. R., Piccirillo L., Pisano G., Polenta G., Prele D., Puddu R., Rambaud D., Rigaut O., Ringegni P., Romero G. E., Salatino M., Schillaci A., Scoccola C. G., Spinelli S. M., Stolpovskiy M., Suarez F., Tartari A., Thermeau J. -P., Timbie P. T., Tristram M., Truongcanh V., Tucker G. S., Tucker C. E., Vigano D., Vittorio N., Voisin F., Watson B., Wicek F., Zullo A., Sadwick L.P.,Yang T., Burke, D, Gayer, D, Kalinauskaite, E, O'Sullivan, C, Murphy, J, Scully, S, De Petris, M, De Leo, M, Mennella, A, Torchinsky, S, Zannoni, M, Amico, G, Auguste, D, Aumont, J, Banfi, S, Barbaran, G, Battaglia, P, Battistelli, E, Bau, A, Belier, B, Bennett, D, Berge, L, Bernard, J, Bersanelli, M, Bigot-Sazy, M, Bleurvac, N, Bonaparte, J, Bonis, J, Bordier, G, Breelle, E, Bunn, E, Buzi, D, Buzzelli, A, Cavaliere, F, Chanial, P, Chapron, C, Charlassier, R, Columbro, F, Coppi, G, Coppolecchia, A, Couchot, F, D'Alessandro, G, D'Agostino, R, De Bernardis, P, De Gasperis, G, Di Donato, A, Drilien, A, Dumoulin, L, Etchegoyen, A, Fasciszewski, A, Franceschet, C, Gamboa-Lerena, M, Garcia, B, Garrido, X, Gaspard, M, Gault, A, Gervasi, M, Giard, M, Giraud-Heraud, Y, Gomez Berisso, M, Gonzalez, M, Gradziel, M, Grandsire, L, Guerrard, E, Hamilton, J, Harari, D, Haynes, V, Henrot-Versille, S, Hoang, D, Holtzer, N, Incardona, F, Jules, E, Kaplan, J, Korotkov, A, Kristukat, C, Lamagna, L, Lande, J, Loucatos, S, Louis, T, Lowitz, A, Lukovic, V, Luterstein, R, Maffei, B, Marnieros, S, Masi, S, Mattei, A, May, A, Mcculloch, M, Medina, M, Mele, L, Melhuish, S, Mundo, L, Montier, L, Neel, D, Olivieri, E, Paiella, A, Pajot, F, Passerini, A, Pastoriza, H, Pelosi, A, Perbost, C, Perdereau, O, Pezzotta, F, Piacentini, F, Piat, M, Piccirillo, L, Pisano, G, Polenta, G, Prele, D, Puddu, R, Rambaud, D, Rigaut, O, Ringegni, P, Romero, G, Salatino, M, Schillaci, A, Scoccola, C, Spinelli, S, Stolpovskiy, M, Suarez, F, Tartari, A, Thermeau, J, Timbie, P, Tristram, M, Truongcanh, V, Tucker, G, Tucker, C, Vigano, D, Vittorio, N, Voisin, F, Watson, B, Wicek, F, Zullo, A, Burke D., Gayer D., Kalinauskaite E., O'Sullivan C., Murphy J. D., Scully S. P., De Petris M., De Leo M., Mennella A., Torchinsky S. A., Zannoni M., Amico G., Auguste D., Aumont J., Banfi S., Barbaran G., Battaglia P., Battistelli E., Bau A., Belier B., Bennett D. G., Berge L., Bernard J. -P., Bersanelli M., Bigot-Sazy M. -A., Bleurvac N., Bonaparte J., Bonis J., Bordier G., Breelle E., Bunn E. F., Buzi D., Buzzelli A., Cavaliere F., Chanial P., Chapron C., Charlassier R., Columbro F., Coppi G., Coppolecchia A., Couchot F., D'Alessandro G., D'Agostino R., De Bernardis P., De Gasperis G., Di Donato A., Drilien A. -A., Dumoulin L., Etchegoyen A., Fasciszewski A., Franceschet C., Gamboa-Lerena M., Garcia B., Garrido X., Gaspard M., Gault A., Gervasi M., Giard M., Giraud-Heraud Y., Gomez Berisso M., Gonzalez M., Gradziel M. L., Grandsire L., Guerrard E., Hamilton J. -C., Harari D., Haynes V., Henrot-Versille S., Hoang D. T., Holtzer N., Incardona F., Jules E., Kaplan J., Korotkov A. L., Kristukat C., Lamagna L., Lande J., Loucatos S., Louis T., Lowitz A., Lukovic V., Luterstein R., Maffei B., Marnieros S., Masi S., Mattei A., May A. J., McCulloch M. A., Medina M. C., Mele L., Melhuish S. J., Mundo L., Montier L., Murphy J. A., Neel D., Olivieri E., Paiella A., Pajot F., Passerini A., Pastoriza H., Pelosi A., Perbost C., Perdereau O., Pezzotta F., Piacentini F., Piat M. R., Piccirillo L., Pisano G., Polenta G., Prele D., Puddu R., Rambaud D., Rigaut O., Ringegni P., Romero G. E., Salatino M., Schillaci A., Scoccola C. G., Spinelli S. M., Stolpovskiy M., Suarez F., Tartari A., Thermeau J. -P., Timbie P. T., Tristram M., Truongcanh V., Tucker G. S., Tucker C. E., Vigano D., Vittorio N., Voisin F., Watson B., Wicek F., and Zullo A.

Abstract

Remnant radiation from the early universe, known as the Cosmic Microwave Background (CMB), has been redshifted and cooled, and today has a blackbody spectrum peaking at millimetre wavelengths. The QUBIC (Q&U Bolometric Interferometer for Cosmology) instrument is designed to map the very faint polaristion structure in the CMB. QUBIC is based on the novel concept of bolometric interferometry in conjunction with synthetic imaging. It will have a large array of input feedhorns, which creates a large number of interferometric baselines. The beam from each feedhorn is passed through an optical combiner, with an off-axis compensated Gregorian design, to allow the generation of the synthetic image. The optical-combiner will operate in two frequency bands (150 and 220 GHz with 25% and 18.2 % bandwidth respectively) while cryogenically cooled TES bolometers provide the sensitivity required at the image plane. The QUBIC Technical Demonstrator (TD), a proof of technology instrument that contains 64 input feed-horns, is currently being built and will be installed in the Alto Chorrillos region of Argentina. The plan is then for the full QUBIC instrument (400 feed-horns) to be deployed in Argentina and obtain cosmologically significant results. In this paper we will examine the output of the manufactered feed-horns in comparison to the nominal design. We will show the results of optical modelling that has been performed in anticipation of alignment and calibration of the TD in Paris, in particular testing the validity of real laboratory environments. We show the output of large calibrator sources (50 ° full width haf max Gaussian beams) and the importance of accurate mirror definitions when modelling large beams. Finally we describe the tolerance on errors of the position and orientation of mirrors in the optical combiner.

Published
2018

26. Diffusion mechanisms in Ir-coated Re for high-temperature, radiation-cooled rocket thrusters

Author

Hamilton, J. C, Yang, N. Y. C, Clift, W. M, Boehme, D. R, and Mccarty, K. F

Subjects
Spacecraft Propulsion And Power
Abstract

Materials used for radiation-cooled rocket thrusters must be capable of surviving under extreme conditions of high temperatures and oxidizing environments. Thruster chambers were developed using chemical-vapor-deposited (CVD) Re coated with CVD Ir on the inside surface which is exposed to hot combustion gases. Ir serves as an oxidation barrier protecting the Re which maintains structural integrity at high temperatures. In order to predict and extend the performance limits of these Ir-coated Re thrusters, the diffusion kinetics of CVD materials at temperature are studied. Thruster end ring sections were examined using electron microprobe analysis both before and after exposure to high temperature vacuum environments. The resulting elemental maps for Re, Ir, and Mo in the near-surface region allow identification of diffusion mechanisms operating at these temperatures. Line scans for Ir and Re were fit using a diffusion model to extract relevant diffusion constants. The fastest diffusion process is seen to be grain boundary diffusion with Re diffusing down grain boundaries in the Ir overlayer. The measured dependence of the diffusion rate on temperature will allow prediction of operating lifetimes for these thrusters.

Published
1991

28. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: analysis of potential systematics

Author

{Ross} A.~J., {Percival} W.~J., {Sanchez}} A.~G., {Samushia} L., {Ho} S., {Kazin} E., {Manera} M., {Reid} B., {White} M., {Tojeiro} R., {McBride} C.~K., {Xu} X., {Wake} D.~A., {Strauss} M.~A., {Montesano} F., {Swanson} M.~E.~C., {Bailey} S., {Bolton} A.~S., {Dorta} A.~M., {Eisenstein} D.~J., {Guo} H., {Hamilton} J.-C., {Nichol} R.~C., {Padmanabhan} N., and {Prada} F.

Published
2012
Full Text
View/download PDF

29. The Q U Bolometric Interferometer for Cosmology (QUBIC)

Author

O'Sulivan, C, Scully, S, Gayer, D, Gradziel, M, Murphy, JA, De Petris, M, Buzi,D, Hamilton, J. C, Piat, M, Bigot Sazy, M. A, Brossard, J, Maffei, B., GERVASI, MASSIMO, ZANNONI, MARIO, O'Sulivan, C, Scully, S, Gayer, D, Gradziel, M, Murphy, J, De Petris, M, Buzi, D, Gervasi, M, Zannoni, M, Hamilton, J, Piat, M, Bigot Sazy, M, Brossard, J, and Maffei, B

Subjects
FIS/05 - ASTRONOMIA E ASTROFISICA, FIS/01 - FISICA SPERIMENTALE, Polarization, Cosmic Microwave Background, Instrumentation
Abstract

QUBIC is a novel ground-based instrument that aims to detect the very faint B-mode polarisation pattern in the Cosmic Microwave Background. Since gravitational waves are the only way to produce this type of polarisation at large angular scales, B-modes are a key prediction of Inflation, the leading theory of the very early Universe. No confirmed primordial B-mode detection has ever been made. QUBIC uses bolometric interferometry, a technique that can combine the sensitivity of an imager with the immunity to systematic effects of an interferometer. It will directly observe the sky through an array of entry horns whose signals will be superimposed using a quasi- optical beam combiner. Images of the resulting interference fringes will be formed on two focal planes tiled with TES bolometers. This paper focuses on the design and modelling of the QUBIC beam combiner, including the feedhorn array, optics and shielding. The modelling was carried out using a combination of ray-tracing, a paraxial diffraction analysis and physical optics, with both commercial and in-house software.

Published
2015

31. Combined analysis of the binary lens caustic-crossing event MACHO 98-SMC-1

Author

Afonso, C, Alard, C, Albert, J N, Andersen, J, Ansari, R, Aubourg, E, Bareyre, P, Bauer, F, Beaulieu, J P, Bouquet, A, Char, S, Charlot, X, Couchot, F, Coutures, C, Derue, F, Ferlet, R, Glicenstein, J F, Goldman, B, Gould, A, Graff, D, Gros, M, Haissinski, J, Hamilton, J C, Hardin, D, de Kat, J, Kim, A, Lasserre, T, Lesquoy, E, Loup, C, Magneville, C, Marquette, J B, Maurice, E, Milsztajn, A, Moniez, M, Palanque-Delabrouille, N, Perdereau, O, Prevot, L, Regnault, N, Rich, J, Spiro, M, Vidal-Madjar, A, Vigroux, L, Zylberajch, S, Alcock, C, Allsman, R A, Alves, D, Axelrod, TS, Becker, A C, Peterson, B A, Szymanski, M, Dominik, Martin, Naber, R M, Sackett, Penny D, Kapteyn Astronomical Institute, and Astronomy

Subjects
Lens (geometry), Physics, Proper motion, MICROLENSING EVENT, 010308 nuclear & particles physics, Astrophysics (astro-ph), gravitational lensing, FOS: Physical sciences, Binary number, Astronomy and Astrophysics, Astrophysics, Mass ratio, Gravitational microlensing, 01 natural sciences, dark matter, Einstein radius, Space and Planetary Science, Limb darkening, 0103 physical sciences, Magellanic Clouds, astrometry, PHOTOMETRY, Small Magellanic Cloud, 010303 astronomy & astrophysics
Abstract

We fit the data for the binary-lens microlensing event MACHO 98-SMC-1 from 5 different microlensing collaborations and find two distinct solutions characterized by binary separation d and mass ratio q: (d,q)=(0.54,0.50) and (d,q)=(3.65,0.36), where d is in units of the Einstein radius. However, the relative proper motion of the lens is very similar in the two solutions, 1.30 km/s/kpc and 1.48 km/s/kpc, thus confirming that the lens is in the Small Magellanic Cloud. The close binary can be either rotating or approximately static but the wide binary must be rotating at close its maximum allowed rate to be consistent with all the data. We measure limb-darkening coefficients for five bands ranging from I to V. As expected, these progressively decrease with rising wavelength. This is the first measurement of limb darkening for a metal-poor A star., 29 pages + 9 figures + 2 tables, submitted to ApJ

Published
2000

32. Optical design and modelling of the QUBIC instrument, a next-generation quasi-optical bolometric interferometer for cosmology

Author

Scully, S., additional, Burke, D., additional, O'Sullivan, C., additional, Gayer, D., additional, Gradziel, M., additional, Murphy, J. A., additional, De Petris, M., additional, Buzi, D., additional, Zannoni, M., additional, Mennella, A, additional, Gervasi, M., additional, Tartari, A., additional, Maffei, B., additional, Aumont, J., additional, Banfi, S., additional, Battaglia, P., additional, Battistelli, E. S., additional, Baù, A., additional, Bélier, B., additional, Bennet, D., additional, Bergé, L., additional, Bernard, J.-Ph., additional, Bersanelli, M., additional, Bigot-Sazy, M.-A., additional, Bleurvacq, N., additional, Bordier, G., additional, Brossard, J., additional, Bunn, E. F., additional, Cammileri, D., additional, Cavaliere, F., additional, Chanial, P., additional, Chapron, C., additional, Coppolecchia, A., additional, Couchot, F., additional, D'Alessandro, G., additional, De Bernardis, P., additional, Decourcelle, T., additional, Del Torto, F., additional, Dumoulin, L., additional, Franceschet, C., additional, Gault, A., additional, Ghribi, A., additional, Giard, M., additional, Giraud-Héraud, Y., additional, Grandsire, L., additional, Hamilton, J. C., additional, Haynes, V., additional, Henrot-Versillé, S., additional, Holtzer, N., additional, Kaplan, J., additional, Korotkov, A., additional, Lande, J., additional, Lowitz, A., additional, Marnieros, S., additional, Martino, J., additional, Masi, S., additional, McCulloch, Mark, additional, Melhuish, Simon, additional, Montier, L., additional, Néel, D., additional, Ng, M. W., additional, Pajot, F., additional, Passerini, A., additional, Perbost, C., additional, Perdereau, O., additional, Piacentini, F., additional, Piat, M., additional, Piccirillo, L., additional, Pisano, G., additional, Prêle, D., additional, Puddu, R., additional, Rambaud, D., additional, Rigaut, O., additional, Salatino, M., additional, Schillaci, A., additional, Stolpovskiy, M., additional, Timbie, P., additional, Tristram, M., additional, Tucker, G., additional, Viganò, D., additional, Voisin, F., additional, and Watson, B., additional

Published
2016
Full Text
View/download PDF

33. Baryon acoustic oscillations in the Ly α forest of BOSS quasars*

Author

Busca, NG, Delubac, T, Rich, J, Bailey, S, Font-Ribera, A, Kirkby, D, Goff, J-ML, Pieri, MM, Slosar, A, Aubourg, É, Bautista, JE, Bizyaev, D, Blomqvist, M, Bolton, AS, Bovy, J, Brewington, H, Borde, A, Brinkmann, J, Carithers, B, Croft, RAC, Dawson, KS, Ebelke, G, Eisenstein, DJ, Hamilton, J-C, Ho, S, Hogg, DW, Honscheid, K, Lee, K-G, Lundgren, B, Malanushenko, E, Malanushenko, V, Margala, D, Maraston, C, Mehta, K, Miralda-Escudé, J, Myers, AD, Nichol, RC, Noterdaeme, P, Olmstead, MD, Oravetz, D, Palanque-Delabrouille, N, Pan, K, Pâris, I, Percival, WJ, Petitjean, P, Roe, NA, Rollinde, E, Ross, NP, Rossi, G, Schlegel, DJ, Schneider, DP, Shelden, A, Sheldon, ES, Simmons, A, Snedden, S, Tinker, JL, Viel, M, Weaver, BA, Weinberg, DH, White, M, Yèche, C, and York, DG

Subjects
Large-scale structure of Universe, Cosmological parameters, Dark energy, Astrophysics::Instrumentation and Methods for Astrophysics, astro-ph.CO, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, observations [Cosmology], Astrophysics::Galaxy Astrophysics, Astronomical and Space Sciences
Abstract

We report a detection of the baryon acoustic oscillation (BAO) feature in the three-dimensional correlation function of the transmitted flux fraction in the \Lya forest of high-redshift quasars. The study uses 48,640 quasars in the redshift range $2.1\le z \le 3.5$ from the Baryon Oscillation Spectroscopic Survey (BOSS) of the third generation of the Sloan Digital Sky Survey (SDSS-III). At a mean redshift $z=2.3$, we measure the monopole and quadrupole components of the correlation function for separations in the range $20\hMpc

Published
2013

34. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Baryon Acoustic Oscillations in the Data Release 9 Spectroscopic Galaxy Sample

Author

Anderson, Lauren, Aubourg, E., Bailey, Stephen, Bizyaev, Dmitry, Blanton, Michael, Bolton, Adam S., Brinkmann, J., Brownstein, Joel R., Burden, Angela, Cuesta, Antonio J., da Costa, Luiz N. A., Dawson, Kyle S., de Putter, Roland, Eisenstein, Daniel J., Gunn, James E., Guo, Hong, Hamilton, J.-C., Harding, Paul, Ho, Shirley, Honscheid, Klaus, Kazin, Eyal, Kirkby, D., Kneib, J.-P., Labatie, Antoine, Loomis, Craig, Lupton, Robert H., Malanushenko, Elena, Malanushenko, Viktor, Mandelbaum, Rachel, Manera, Marc, Maraston, Claudia, Mcbride, Cameron K., Mehta, Kushal T., Mena, Olga, Montesano, Francesco, Muna, Demetri, Nichol, Robert C., Nuza, Sebastian E., Olmstead, Matthew D., Oravetz, Daniel, Padmanabhan, Nikhil, Palanque-Delabrouille, N., Pan, Kaike, Parejko, John, Pâris, I., Percival, Will J., Petitjean, P., Prada, Francisco, Reid, Beth, Roe, Natalie A., Ross, Ashley J., Ross, Nicholas P., Samushia, Lado, Sanchez, Ariel G., Schneider, David J., Schlegel, Donald P., Scoccola, Claudia G., Seo, Hee-Jong, Sheldon, Erin S., Simmons, Audrey, Skibba, Ramin A., Strauss, Michael A., Swanson, Molly E. C., Thomas, Daniel, Tinker, Jeremy L., Tojeiro, Rita, Vargas Magana, M., Verde, Licia, Wagner, Christian, Wake, David A., Weaver, Benjamin A., Weinberg, David H., White, Martin, Xu, Xiaoying, Yèche, C., Zehavi, Idit, Zhao, Gong-Bo, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire d'Astrophysique de Marseille (LAM), 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), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), SDSS-III, 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Universitat de Barcelona, APC - Cosmologie, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-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)), 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)-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), and UAM. Departamento de Física Teórica

Subjects
Astrofísica, Cosmology and Gravitation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Cosmological parameters, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Energia fosca (Astronomia), Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Measurement of distances, Observacions astronòmiques, Dark energy, 0103 physical sciences, observations [Cosmology], Dark energy (Astronomy), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Distance scale, Cosmologia, 010308 nuclear & particles physics, Cosmology: observations, Física, Astronomy and Astrophysics, Cosmology and Extragalactic Astrophysics, Cosmology, Mesurament de les distàncies, Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, Astronomical observations
Abstract

This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2012 RAS © 2012 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved., We present measurements of galaxy clustering from the Baryon Oscillation Spectroscopic Survey (BOSS), which is part of the Sloan Digital Sky Survey III (SDSS-III). These use the Data Release 9 (DR9) CMASS sample, which contains 264 283 massive galaxies covering 3275 square degrees with an effective redshift z = 0.57 and redshift range 0.43 < z < 0.7. Assuming a concordance λCDM cosmological model, this sample covers an effective volume of 2.2 Gpc3, and represents the largest sample of the Universe ever surveyed at this density, n̄ ~3 × 10-4 h-3 Mpc3. We measure the angle-averaged galaxy correlation function and power spectrum, including density-field reconstruction of the baryon acoustic oscillation (BAO) feature. The acoustic features are detected at a significance of 5σ in both the correlation function and power spectrum. Combining with the SDSS-II luminous red galaxy sample, the detection significance increases to 6.7σ. Fitting for the position of the acoustic features measures the distance to z = 0.57 relative to the sound horizon DV/rs = 13.67 ± 0.22 at z = 0.57. Assuming a fiducial sound horizon of 153.19 Mpc, which matches cosmic microwave background constraints, this corresponds to a distance DV (z = 0.57) = 2094 ± 34 Mpc. At 1.7 per cent, this is the most precise distance constraint ever obtained from a galaxy survey. We place this result alongside previous BAO measurements in a cosmological distance ladder and find excellent agreement with the current supernova measurements. We use these distance measurements to constrain various cosmological models, finding continuing support for a flat Universe with a cosmological constant, WJP is grateful for support from the UK Science and Technology Facilities Research Council, the Leverhulme Trust, and the European Research Council.AJR is grateful to theUKScience and Technology Facilities Council for financial support through the grant ST/I001204/1. CGS acknowledges funding from project AYA2010- 21766-C03-02 of the Spanish Ministry of Science and Innovation (MICINN). DJE, XX, and KM were supported by NSF grant AST-0707725 and NASA grant NNX07AH11G. NP and AJC are partially supported by NASA grant NNX11AF43G. FP acknowledges support from the SpanishMICINNs Consolider grantMultiDark CSD2009- 00064. MAS was supported by NSF grant AST-0707266. MECS was supported by the NSF under Award No. AST-0901965. Support for LAMBDA is provided by the NASA Office of Space Science

Published
2012

35. The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Analysis of potential systematics

Author

Ross, A. J., Percival, W. J., Sánchez, A. G., Samushia, L., Ho, S., Kazin, E., Manera, M., Reid, B., White, M., Tojeiro, R., McBride, C. K., Xu, X., Wake, D. A., Strauss, M. A., Montesano, F., Swanson, M. E. C., Bailey, S., Bolton, A. S., Dorta, A. M., Eisenstein, D. J., Guo, H., Hamilton, J.-C., Nichol, R. C., Padmanabhan, N., Prada, F., Schlegel, D. J., Magaña, M. V., Zehavi, I., Blanton, M., Bizyaev, D., Brewington, H., Cuesta, A. J., Malanushenko, E., Malanushenko, V., Oravetz, D., Parejko, J., Pan, K., Schneider, D. P., Shelden, A., Simmons, A., Snedden, S., Zhao, G.-b., 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), SDSS-III, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), APC - Cosmologie, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-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)), 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)-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), and University of St Andrews. School of Physics and Astronomy

Subjects
Cosmology and Gravitation, Distance scale, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmology and Extragalactic Astrophysics, Astrophysics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], QC Physics, QB Astronomy, observations [Cosmology], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], QC, Astrophysics::Galaxy Astrophysics, QB, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We analyze the density field of galaxies observed by the Sloan Digital Sky Survey (SDSS)-III Baryon Oscillation Spectroscopic Survey (BOSS) included in the SDSS Data Release Nine (DR9). DR9 includes spectroscopic redshifts for over 400,000 galaxies spread over a footprint of 3,275 deg^2. We identify, characterize, and mitigate the impact of sources of systematic uncertainty on large-scale clustering measurements, both for angular moments of the redshift-space correlation function and the spherically averaged power spectrum, P(k), in order to ensure that robust cosmological constraints will be obtained from these data. A correlation between the projected density of stars and the higher redshift (0.43 < z < 0.7) galaxy sample (the `CMASS' sample) due to imaging systematics imparts a systematic error that is larger than the statistical error of the clustering measurements at scales s > 120h^-1Mpc or k < 0.01hMpc^-1. We find that these errors can be ameliorated by weighting galaxies based on their surface brightness and the local stellar density. We use mock galaxy catalogs that simulate the CMASS selection function to determine that randomly selecting galaxy redshifts in order to simulate the radial selection function of a random sample imparts the least systematic error on correlation function measurements and that this systematic error is negligible for the spherically averaged correlation function. The methods we recommend for the calculation of clustering measurements using the CMASS sample are adopted in companion papers that locate the position of the baryon acoustic oscillation feature (Anderson et al. 2012), constrain cosmological models using the full shape of the correlation function (Sanchez et al. 2012), and measure the rate of structure growth (Reid et al. 2012). (abridged), Matches version accepted by MNRAS. Clarifications and references have been added. See companion papers that share the "The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey:" title

Published
2012

36. Intensity and polarization of the atmospheric emission at millimetric wavelengths at Dome Concordia

Author

Battistelli, E.S., Amico, G., Baù, A., Bergé, L., Bréelle, É., Charlassier, R., Collin, S., Cruciani, A., de Bernardis, P., Dufour, C., Dumoulin, L., Gervasi, M., Giard, M., Giordano, C., Giraud-Héraud, Y., Guglielmi, L., Hamilton, J.-C., Landé, J., Maffei, B., Maiello, M., Marnieros, S., Masi, S., Passerini, A., Piacentini, F., Piat, M., Piccirillo, L., Pisano, G., Polenta, G., Rosset, C., Salatino, M., Schillaci, A., Sordini, R., Spinelli, S., Tartari, A., Zannoni, M., CSNSM INSTR, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), 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)-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), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), CSNSM PS1, 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)-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)-Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), 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), Centre d'étude spatiale des rayonnements (CESR), 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, BRAIN, 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)-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), 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 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)-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)-Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), APC - Cosmologie, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-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)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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), and 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)

Subjects
polarimeters [Instrumentation], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FOS: Physical sciences, instrumentation: polarimeters, Astronomy and Astrophysics, atmospheric effects, cosmic background radiation, site testing, Atmospheric effects, Cosmic background radiation, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Physics - Atmospheric and Oceanic Physics, Space and Planetary Science, Atmospheric and Oceanic Physics (physics.ao-ph), Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Site testing, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

Atmospheric emission is a dominant source of disturbance in ground-based astronomy at mm wavelengths. The Antarctic plateau is recognized to be an ideal site for mm and sub-mm observations, and the French/Italian base of Dome C is among the best sites on Earth for these observations. In this paper we present measurements, performed using the BRAIN-pathfinder experiment, at Dome C of the atmospheric emission in intensity and polarization at 150GHz, one of the best observational frequencies for CMB observations when considering cosmic signal intensity, atmospheric transmission, detectors sensitivity, and foreground removal. Careful characterization of the air-mass synchronous emission has been performed, acquiring more that 380 elevation scans (i.e. "skydip") during the third BRAIN-pathfinder summer campaign in December 2009/January 2010. The extremely high transparency of the Antarctic atmosphere over Dome Concordia is proven by the very low measured optical depth: =0.050 \pm 0.003 \pm 0.011 where the first error is statistical and the second is systematic error. Mid term stability, over the summer campaign, of the atmosphere emission has also been studied. Adapting the radiative transfer atmosphere emission model "am" to the particular conditions found at Dome C, we also infer the level of the PWV content of the atmosphere, notoriously the main source of disturbance in millimetric astronomy (=0.77 +/- 0.06 + 0.15 - 0.12 mm). Upper limits on the air-mass correlated polarized signal are also placed for the first time. The degree of circular polarization of atmospheric emission is found to be lower than 0.2% (95%CL), while the degree of linear polarization is found to be lower than 0.1% (95%CL). These limits include signal-correlated instrumental spurious polarization., Comment: MNRAS accepted for publication. Refined analysis

Published
2012

37. Sky emission at 0.4 meV and beyond the EeV: cosmology and cosmic rays

Author

Hamilton, J.-C., APC - Cosmologie, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-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)), 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)-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 Paris-Diderot - Paris VII, Pierre Binétruy, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-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 sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), 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)-Université Paris Diderot - Paris 7 (UPD7)-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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and Hamilton, Jean-Christophe

Subjects
[SDU.ASTR.CO] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], fond diffus cosmologique, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], cosmic microwave background, cosmic rays, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], bolometric interferometry, inflation, cosmologie, rayons cosmiques, interférométrie bolométrique, cosmology
Abstract

Cette habilitation a' diriger des recherches de ́crit les travaux de recherche que j'ai effectue ́s depuis ma soute- nance de the'se qui en 1999. Elle s'articule autour de deux parties correspondants aux deux the'mes scientifiques sur lesquels j'ai travaille ́ ces dernie'res anne ́es : les rayons cosmiques d'ultra-haute e ́nergie et l'e ́tude du fond diffus cosmologique. C'est au sein de la collaboration Pierre Auger que j'ai travaille ́ sur la the ́matique des rayons cosmiques ultra- e ́nerge ́tiques entre fin 2002 et fin 2006. Il s'agit la' du plus grand de ́tecteur jamais construit par l'homme destine ́ a' eclaircir un myste're vieux de plus d'un sie'cle : quelle est la nature, ou' sont produits, et comment se propagent lesrayonscosmiquesquel'onobservea'dese ́nergiesdequelques1019eV?enexiste-t-ilau-dela'delafameuse coupure GZK qui, du fait le la perte d'e ́nergie des rayons cosmiques aux plus hautes e ́nergies par inte ́raction avec le fond diffus cosmologique limite l'horizon a' quelques centaines de Mpc a' ces e ́nergies? Je de ́cris dans cette habilitation mes travaux d'analyse de donne ́es concernant d'une part la recherche d'e ́ventuelles aniso- tropies dans la distribution sur le ciel des rayons cosmiques (des anisotrpies aux petites e ́chelles permettant d'identifier les sources, et aux plus grandes e ́chelles pouvant signer divers sce ́narios, par exemple top-down si l'on observe un exce's en provenance du centre Galactique) et d'autre part sur sur la recherche de photons aux plus hautes e ́nergies, une des signatures les plus claires d'une origine top-down pour les rayons cosmques les plus e ́nerge ́tiques. Les re ́sultats ne ́gatifs de cette recherche de photons, ajoute ́s a' l'observation claire de la cou- pure GZK ont permis a' l'Observatoire Pierre Auger de trancher en faveur d'une origine bottom-up, c'est a' dire issue d'acce ́le ́rateurs cosmiques, pour les rayons cosmiques les plus e ́nerge ́tiques. Par ailleurs, aucune aniso- tropien'estpourl'heureobserve ́eauxplusgrandese ́chellesalorsquelesrayonscosmqieslespluse ́nerge ́tiques montrent une autocorre ́lation significative aux petites e ́chelles, en corre ́lation avec un catalogues d'AGN (dont la distribution spatiale est elle-meˆme corre ́le ́e au reste de la matie're, cela' ne signe donc pas les AGN comme sites d'acce ́le ́ration). J'ai commence ́ a' aborder la the ́matique des anisotropies du fond diffus cosmologique au cours de mon post- doctorat et de ma premie're anne ́e au CNRS au sein de l'e ́xperience Archeops, un projet ballon d'observation de latempe ́ratureetdelapolarisationdecerayonnementsavecuneinstrumentationsimilairea'celledePlanck-HFI. J'ai travaille ́ a' l'e ́laboration des cartes du ciel et a' l'extraction du spectre angulaire de puissance des fluctuations de tempe ́rature, permettant l'observation pre ́cise, avant WMAP, du premier pic acoustique, et la de ́termination des parame'tres cosmologiques. J'ai rejoint a' nouveau cette the ́matique fin-2006 au sein de la collaboration QU- BIC dont l'objectif est de ́tecter les modes-B de polarisation du fond diffus cosmologique. Ces derniers sont la signature d'ondes gravitationnelles primordiales, c'est a' dire de modes tenseurs engendre ́s par l'inflation. Leur de ́tection et la mesure de leur spectre est conside ́re ́e comme le Graal de la cosmologie contemporaine tant ont apprendrait sur les processus a' l'oeuvre dans l'Univers primordial : mesure de l'e ́chelle en e ́nergie de l'inflation, de ́termination de la forme du potentiel de l'inflaton, tests de cohe ́rence interne du mode'le inflationnaire. Ces modes-b de polarisation sont d'une amplitude si faible (en dessous du micro-Kelvin) qu'une nouvelle ge ́ne ́rtion d'intrumentsestrequisepourlesobserver:largesmatricesdebolome'tres(limite ́sparlebruitdephotons),design instrumental minimisant l'impact des effets syste ́matiques qui pourraient devenir dominants pour des de ́tecteurs aussi sensibles. Le projet QUBIC est base ́ sur le concept d'interfe ́rome ́trie bolome ́trique, combinant les avan- tages des bolome'tres en terme de sensibilite ́ et ceux des interfe ́rome'tres en terme de faible contamination par les effets syste ́matiques. Depuis pre's de trois ans, je travaille au de ́veloppement du concept instrumental d'un interfe ́rome'tre bolome ́trique : reconstruction des visibilite ́s de manie're optimale graˆce a' des modulateurs de phases, calcul de la sensibilite ́s et comparaison avec un imageur et un interfe ́rome'tre classique (montrant que nous avons en effet un interfe ́rome'tre plus sensible graˆce aux de ́tecteurs bolome ́triques) et enfin de ́termination du design optimal de l'instrument QUBIC afin d'atteindre notre objectif scientifique d'eˆtre en mesure d'exclure un rapport entre les modes tenseurs et scalaires de 0.01 a' 95% de niveau de confiance en un an. L'instrument ne ́cessaire est typiquement un ensemble de 6 modules d'interfe ́rome'tres comprenant chacun 144 cornets, une feneˆtre de 40 cm de diame'tre et un plan focal comprenant 900 bolome'tres avec une largeur de bande de 25%.

Published
2009

38. BRAIN/MBI: a bolometric interferometer dedicated to the CMB polarization

Author

Tartari, A., Bartlett, J. G., Elia Stefano Battistelli, Baù, A., Bennett, D., Bergé, L., Bernard, J. P., Bounab, A., Bréelle, E., Bunn, E., Charlassier, R., Cruciani, A., Collin, S., Curran, G., Paolo de Bernardis, Dumoulin, L., Gault, A., Gervasi, M., Ghribi, A., Giard, M., Giordano, C., Giraud Héraud, Y., Gradziel, M., Guglielmi, L., Hamilton, J. C., Haynes, V., Iacoangeli, A., Kaplan, J., Korotkov, A., Lande, J., Maffei, B., Maiello, M., Malu, S. S., Marnieros, S., Silvia Masi, Murphy, A., Sullivan, C. O., Pajot, F., Passerini, A., Peterzen, S. S., Francesco Piacentini, Piccirillo, L., Piat, M., Giampaolo Pisano, Polenta, G., Prêle, D., Rosset, C., Schillaci, Alessandro, Sironi, G., Spinelli, S., Tucker, G., Timbie, P., Voisin, F., Watson, B., Zannoni, M., Tartari, A, Bartlett, J, Battistelli, E, Bau', A, Bennett, D, Bergè, L, Bernard, J, Bounab, A, Brèelle, E, Bunn, E, Charlassier, R, Cruciani, A, Collin, S, Curran, G, De Bernardis, P, Dumoulin, L, Gault, A, Gervasi, M, Ghribi, A, Giard, M, Giordano, C, Giraud Hèraud, J, Gradziel, M, Guglielmi, L, Hamilton, J, Haynes, V, Iacoangeli, A, Kaplan, J, Korotkov, A, Lande, J, Maffei, B, Maiello, M, Malu, S, Marnieros, S, Masi, S, Murphy, A, O'Sullivan, C, Pajot, F, Passerini, A, Peterzen, S, Piacentini, F, Piccirillo, L, Piat, M, Pisano, G, Polenta, G, Prêle, D, Rosset, C, Schillaci, A, Sironi, G, Spinelli, S, Tucker, G, Timbie, P, Voisin, F, Watson, B, and Zannoni, M

Subjects
QUBIC, CMB, Polarization, CMB, polarimetry, QUBIC, CMB, polarimetry
Abstract

BRAIN/MBI is a mm-wave ground-based experiment dedicated to the study of the B-modes of CMB polarization. It is based on the bolometric interferometry (BI) technique, and it is the result of the merging of two different projects proposed in the last years: BRAIN (France, Italy, UK) and MBI 4 (US, UK). BI is a technique already validated in a laboratory environment using small scale demonstrators employing as detectors standard 4 K bolometers. In fact, both the MBI and BRAIN teams demonstrated that interference fringes are observed once the signals coming from the two antennas of a single baseline are phase-shifted, combined and then detected. Both optical and wave-guided combination schemes have been tested within the collaboration. From the hardware point of view, the simplest unity of BRAIN/MBI is constituted by a feed horn, an OMT, and two independent phase shifters for each polarization. After phase shifting, the two beams coming out from each unity, feed a beam combiner redirecting the signals towards the detectors. Some of the most critical components, that are OMTs, phase-shifters and possibly detectors, will be made using superconducting technologies and are now under development. Moreover, detailed calculations showed that the sensitivity of a bolometric interferometer, if operated with a proper phase modulation-demodulation scheme, can approach that one of an imager with a comparable number of detectors, while exploiting the systematics cleaness of compact interferometers. On one side, BRAIN/MBI will be an instrument with a sensitivity and a polarization purity suitable for the detection of B-modes. On the other side, it will be a benchmark for new and promisings technologies that may be qualified for the CMB science in perspective of a post-Planck space mission. Since BI is prone to different contaminations from systematics with respect to imagers, a cross-check of the results and a comparison of two conceptually orthogonal strategies will finally be possible

Published
2009

39. A demonstrator for bolometric interferometry

Author

Ghribi, A., Tartari, A., Galli, S., Piat, M., Bréelle, E., Hamilton, J.-C., Spinelli, S., Gervasi, M., Zannoni, M., 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Radio Group, Università degli Studi di Milano = University of Milan (UNIMI), APC - Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-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, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Università degli Studi di Milano [Milano] (UNIMI), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, 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), Università degli studi di Milano [Milano], PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-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)-Physique Corpusculaire et Cosmologie - Collège de France (PCC), and Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Bolometric Interferometry (BI) is one of the most promising techniques for precise measurements of the Cosmic Microwave Background polarization. In this paper, we present the results of DIBO (Demonstrateur d'Interferometrie Bolometrique), a single-baseline demonstrator operating at 90 GHz, built to proof the validity of the BI concept applied to a millimeter-wave interferometer. This instrument has been characterized in the laboratory with a detector at room temperature and with a 4 K bolometer. This allowed us to measure interference patterns in a clean way, both (1) rotating the source and (2) varying with time the phase shift among the two interferometer's arms. Detailed modelisation has also been performed and validated with measurements., 15 pages, 14 figures

Published
2009

40. Upper limit on the cosmic-ray photon flux above 1019 eV using the surface detector of the Pierre Auger Observatory

Author

Abraham, J., Abreu, P., Aglietta, M., Aguirre, C., Allard, D., Allekotte, I., Allen, J., Allison, P., Alvarez Muniz, J., Ambrosio, M., Anchordoqui, L., Andringa, S., Anzalone, A., Aramo, C., Argiro', Stefano, Arisaka, K., Armengaud, E., Arneodo, F., Arqueros, F., Asch, T., Asorey, H., Assis, P., Atulugama, B. S., Aublin, J., Ave, M., Avila, G., Baecker, T., Badagnani, D., Barbosa, A. F., Barnhill, D., Barroso, S. L. C., Bauleo, P., Beatty, J. J., Beau, T., Becker, B. R., Becker, K. H., Bellido, J. A., Benzvi, S., Berat, C., Bergmann, T., Bernardini, P., Bertou, X., Biermann, P. L., Billoir, P., Blanch Bigas, O., Blanco, F., Blasi, P., Bleve, C., Biuemer, H., Bohacova, M., Bonifazi, C., Bonino, Raffaella, Boratav, M., Brack, J., Brogueira, P., Brown, W. C., Buchholz, P., Bueno, A., Burton, R. E., Busca, N. G., Caballero Mora, K. S., Cai, B., Camin, D. V., Caramete, L., Caruso, R., Carvalho, W., Castellina, A., Catalano, O., Cataldi, G., Cazon, L., Cester, Rosanna, Chauvin, J., Chiavassa, Andrea, Chinellato, J. A., Chou, A., Chye, J., Clark, P. D. J., Clay, R. W., Colombo, E., Conceicao, R., Connolly, B., Contreras, F., Coppens, J., Cordier, A., Cotti, U., Coutu, S., Covault, C. E., Creusot, A., Criss, A., Cronin, J., Curutiu, A., Dagoret Campagne, S., Daumiller, K., Dawson, B. R., de Almeida, R. M., Donato, C. D., de Jong, S. J., La Vega, G. D., de Mello, W. J. M., J. r., de Mello Neto, J. R. T., Mitri, I. D., Souza, V. d., Peral, L. d., Deligny, O., Selva, A. D., Fratte, C. D., Dembinski, H., Giulio, C. D., Diaz, J. C., Dobrgkeit, C., D'Olivo, J. C., Dornic, D., Dorofeev, A., dos Anjos, J. C., Dova, M. T., D'Urso, D., Dutan, I., Duvernois, M. A., Engel, R., Epele, L., Erdmann, M., Escobar, C. O., Etchegoyen, A., San Luis, P. F., Falcke, H., Farrar, G., Fauth, A. C., Fazzini, N., Ferrer, F., Ferry, S., Fick, B., Filevich, A., Fllipicic, A., Fleck, I., Fonte, R., Fracchiolla, C. E., Fulgione, W., Garcia, B., Gamez, D. G., Garcia Pinto, D., Garrido, X., Geenen, H., Gelmini, G., Gemmeke, H., Ghia, P. L., Giller, M., Glass, H., Gold, M. S., Golup, G., Albarracin, F. G., Berisso, M. G., Herrero, R. G., Gonqalves, P., do Amaral, M. G., Gonzalez, D., Gonzalez, J. G., Gonzalez, M., Gora, D., Gorgi, Alessio, Gouffon, P., Grassi, V., Grillo, A. F., Grunfeld, C., Guardincerri, Y., Guarino, F., Guedes, G. P., Gutierrez, J., Hague, J. D., Hamilton, J. C., Hansen, P., Harari, D., Harmsma, S., Harton, J. L., Haungs, A., Hauschildt, T., Healy, M. D., Hebbeker, T., Hebrero, G., Heck, D., Hojvat, C., Holmes, V. C., Homola, P., Hoerandel, J., Horneffer, A., Horvat, M., Hrabovsky, M., Huege, T., Hussain, M., Iarlori, M., Insolia, A., Ionita, F., Italiano, A., Kaducak, M., Kampert, K. H., Karova, T., Kegl, B., Keilhauer, B., Kemp, E., Kieckhafer, R. M., Klages, H. O., Kleifges, M., Kleinfeller, J., Knapik, R., Knapp, J., Koang, D. H., Krieger, A., Kroemer, O., Kuempel, D., Kunka, N., Kusenko, A., Rosa, G. L., Lachaud, C., Lago, B. L., Lebrun, D., Lebrun, P., Lee, J., Leigui de Oliveira, M. A., Letessier Selvon, A., Leuthold, M., Lhenry Yvon, I., Lopez, R., Agueera, A. L., Bahilo, J. L., Garcia, R. L., Maccarone, M. C., Macolino, C., Maldera, S., Mancarella, G., Mancenido, M. E., Mandat, D., Mantsch, P., Mariazzi, A. G., Maris, I. C., Marquez Falcon, H. R., Martello, D., Martinez, J., Bravo, O. M., Mathes, H. J., Matthews, J., Matthews, J. A. J., Matthiae, G., Maurizio, D., Mazur, P. O., Mccauley, T., Mcewen, M., Mcneil, R. R., Medina, M. C., Medina Tanco, G., Meli, A., Melo, D., Menichetti, Ezio, Menschikov, A., Meurer, C., Meyhandan, R., Micheletti, M. I., Miele, G., Miller, W., Mollerach, S., Monasor, M., Ragaigne, D. M., Montanet, F., Morales, B., Morello, C., Moreno, J. C., Morris, C., Mostafa, M., Muller, M. A., Mussa, R., Navarra, G., Navarro, J. L., Navas, S., Necesal, P., Nellen, L., Newman Holmes, C., Newton, D., Thao, N. T., Nierstenhoefer, N., Nitz, D., Nosek, D., Nozka, L., Oehlschlaeger, J., Ohnuki, T., Olinto, A., Olmos Gilbaja, V. M., Ortiz, M., Ortolani, F., Ostapchenko, S., Otero, L., Pacheco, N., Selmi Dei, D. P., Palatka, M., Pallotta, J., Parente, G., Parizot, E., Parlati, S., Pastor, S., Patel, M., Paul, T., Pavlidou, V., Payet, K., Pech, M., Pekala, J., Pelayo, R., Pepe, I. M., Perrone, L., Petrera, S., Petrinca, P., Petrov, Y., Diep, P. N., Dong, P. N., Nhung, P. T., Pichel, A., Piegaia, R., Pierog, T., Pimenta, M., Pinto, T., Pirronello, V., Pisanti, O., Platino, M., Pochon, J., Privitera, P., Prouza, M., Quel, E. J., Rautenberg, J., Redondo, A., Reucroft, S., Revenu, B., Rezende, F. A. S., Ridky, J., Riggi, S., Risse, M., Riviere, C., Rizi, V., Roberts, M., Robledo, C., Rodriguez, G., Rodriguez Frias, M. D., Martino, I. R., Rojo, J. R., Rodriguez Cabo, I., Ros, G., Rosado, I., Roth, M., Roucelle, C., Rouille d'Orfeuil, B., Roulet, E., Rovero, A. C., Salamida, F., Salazar, H., Salina, G., Sanchez, F., Santander, M., Santo, C. E., Santos, E. M., Sarazin, F., Sarkar, S., Sato, R., Scherini, V., Schieler, H., Schmidt, A., Schmidt, F., Schmidt, T., Scholten, O., Schovanek, P., Schuessler, F., Sciutto, S. J., Scudeni, M., Segreto, A., Semikoz, D., Settimo, M., Shellard, R. C., Sidelnik, I., Siffert, B. B., Sigl, G., De Grande, N. S., Smialkowski, A., Smida, R., Smith, A. G. K., Smith, B. E., Snow, G. R., Sokolsky, P., Sommers, P., Sorokin, J., Spinka, H., Squartini, R., Strazzeri, E., Stutz, A., Suarez, F., Suomijaervi, T., Supanitsky, A. D., Sutherland, M. S., Swain, J., Szadkowski, Z., Takahashi, J., Tamashiro, A., Tamburro, A., Tascau, O., Tcaciuc, R., Thomas, D., Ticona, R., Tiffenberg, J., Timmermans, C., Tkaczyk, W., Todero Peixoto, C. J., Tome, B., Tonachini, Aurelio Siro, Torres, I., Torresi, D., Travnicek, P., Tripathi, A., Tristram, G., Tscherniakhovski, D., Tueros, M., Tunnicliffe, V., Ulrich, R., Unger, M., Urban, M., Valdes Galicia, J. F., Valino, I., Valore, L., van den Berg, A. M., Elewyck, V. v., Vazquez, R. A., Veberic, D., Veiga, A., Velarde, A., Venters, T., Verzi, V., Videla, M., Villasenor, L., Vorobiov, S., Voyvodic, L., Wahlberg, H., Wainberg, O., Walker, P., Warner, D., Watson, A. A., Westerhoff, S., Wieczorek, G., Wiencke, L., Wilczynska, B., Wilczynski, H., Wileman, C., Winnick, M. G., Wu, H., Wundheiler, B., Yamamoto, T., Younk, P., Zas, E., Zavrtanik, D., Zavrtanik, M., Zech, A., Zepeda, A., Holkowski, M., APC - Astrophysique des Hautes Energies (APC - AHE), AstroParticule et Cosmologie (APC (UMR_7164)), 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)-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)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), 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 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)-Université Grenoble Alpes (UGA), APC - Cosmologie, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-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)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, 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), Institut de Physique Nucléaire d'Orsay (IPNO), APC - THEORIE, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut für theoretische Physik, Universität Hamburg (UHH)-Universität Hamburg (UHH), Laboratory for Astroparticle Physics, University of Nova Gorica, PIERRE AUGER, J., Abraham, P., Abreu, M., Aglietta, C., Aguirre, D., Allard, I., Allekotte, J., Allen, P., Allison, J., Alvarez Muniz, M., Ambrosio, L., Anchordoqui, S., Andringa, A., Anzalone, C., Aramo, S., Argiro', K., Arisaka, E., Armengaud, F., Arneodo, F., Arquero, T., Asch, H., Asorey, P., Assi, B. S., Atulugama, J., Aublin, M., Ave, G., Avila, T., Backer, D., Badagnani, A. F., Barbosa, D., Barnhill, S. L. C., Barroso, P., Bauleo, J. J., Beatty, T., Beau, B. R., Becker, K. H., Becker, J. A., Bellido, S., Benzvi, C., Berat, T., Bergmann, Bernardini, Paolo, X., Bertou, P. L., Biermann, P., Billoir, O., Blanch Biga, F., Blanco, P., Blasi, C., Bleve, H., Blumer, M., Bohacova, C., Bonifazi, R., Bonino, M., Boratav, J., Brack, P., Brogueira, W. C., Brown, P., Buchholz, A., Bueno, R. E., Burton, N. G., Busca, K. S., Caballero Mora, B., Cai, D. V., Camin, L., Caramete, R., Caruso, W., Carvalho, A., Castellina, O., Catalano, G., Cataldi, L., Cazon, R., Cester, J., Chauvin, A., Chiavassa, J. A., Chinellato, A., Chou, J., Chye, P. D. J., Clark, R. W., Clay, E., Colombo, R., Conceicao, B., Connolly, F., Contrera, J., Coppen, A., Cordier, U., Cotti, S., Coutu, C. E., Covault, A., Creusot, A., Cri, J., Cronin, A., Curutiu, S., Dagoret Campagne, K., Daumiller, B. R., Dawson, R. M., de Almeida, C., De Donato, S. J., de Jong, G., De La Vega, W. J. M., de Mello Junior, J. R. T., de Mello Neto, DE MITRI, Ivan, V., de Souza, L., del Peral, O., Deligny, A., Della Selva, C., Delle Fratte, H., Dembinski, C., Di Giulio, J. C., Diaz, C., Dobrigkeit, J. C., D’Olivo, D., Dornic, A., Dorofeev, J. C., dos Anjo, M. T., Dova, D., D’Urso, I., Dutan, M. A., Duvernoi, R., Engel, L., Epele, M., Erdmann, C. O., Escobar, A., Etchegoyen, P., Facal San Lui, H., Falcke, G., Farrar, A. C., Fauth, N., Fazzini, F., Ferrer, S., Ferry, B., Fick, A., Filevich, A., Filipcic, I., Fleck, R., Fonte, C. E., Fracchiolla, W., Fulgione, B., Garcia, D., Garcia Gamez, D., Garcia Pinto, X., Garrido, H., Geenen, G., Gelmini, H., Gemmeke, P. L., Ghia, M., Giller, H., Gla, M. S., Gold, G., Golup, F., Gomez Albarracin, M., Gomez Berisso, R., Gomez Herrero, P., Goncalve, M., Goncalves do Amaral, D., Gonzalez, J. G., Gonzalez, M., Gonzalez, D., Gora, A., Gorgi, P., Gouffon, V., Grassi, A. F., Grillo, C., Grunfeld, Y., Guardincerri, F., Guarino, G. P., Guede, J., Gutierrez, J. D., Hague, J. C., Hamilton, P., Hansen, D., Harari, S., Harmsma, J. L., Harton, A., Haung, T., Hauschildt, M. D., Healy, T., Hebbeker, G., Hebrero, D., Heck, C., Hojvat, V. C., Holme, P., Homola, J., Horandel, A., Horneffer, M., Horvat, M., Hrabovsky, T., Huege, M., Hussain, M., Iarlori, A., Insolia, F., Ionita, A., Italiano, M., Kaducak, K. H., Kampert, T., Karova, B., Kegl, B., Keilhauer, E., Kemp, R. M., Kieckhafer, H. O., Klage, M., Kleifge, J., Kleinfeller, R., Knapik, J., Knapp, D. H., Koang, A., Krieger, O., Kromer, D., Kuempel, N., Kunka, A., Kusenko, G., La Rosa, C., Lachaud, B. L., Lago, D., Lebrun, P., Lebrun, J., Lee, M. A., Leigui de Oliveira, A., Letessier Selvon, M., Leuthold, I., Lhenry Yvon, R., Lopez, A., Lopez Aguera, J., Lozano Bahilo, R., Luna Garcia, M. C., Maccarone, C., Macolino, S., Maldera, Mancarella, Giovanni, M. E., Mancenido, D., Mandat, P., Mantsch, A. G., Mariazzi, I. C., Mari, H. R., Marquez Falcon, Martello, Daniele, J., Martinez, O., Martinez Bravo, H. J., Mathe, J., Matthew, J. A. J., Matthew, G., Matthiae, D., Maurizio, P. O., Mazur, T., Mccauley, M., Mcewen, R. R., Mcneil, M. C., Medina, G., Medina Tanco, A., Meli, D., Melo, E., Menichetti, A., Menschikov, Meurer, C. h. r., R., Meyhandan, M. I., Micheletti, G., Miele, W., Miller, S., Mollerach, M., Monasor, D., Monnier Ragaigne, F., Montanet, B., Morale, C., Morello, J. C., Moreno, C., Morri, M., Mostafa, M. A., Muller, R., Mussa, G., Navarra, J. L., Navarro, S., Nava, P., Necesal, L., Nellen, C., Newman Holme, D., Newton, N. T., Thao, N., Nierstenhoefer, D., Nitz, D., Nosek, L., Nozka, J., Oehlschlager, T., Ohnuki, A., Olinto, V. M., Olmos Gilbaja, M., Ortiz, F., Ortolani, S., Ostapchenko, L., Otero, N., Pacheco, D., Pakk Selmi Dei, M., Palatka, J., Pallotta, G., Parente, E., Parizot, S., Parlati, S., Pastor, M., Patel, T., Paul, V., Pavlidou, K., Payet, M., Pech, J., Pekala, R., Pelayo, I. M., Pepe, Perrone, Lorenzo, S., Petrera, P., Petrinca, Y., Petrov, P. N., Diep, P. N., Dong, P. T., Nhung, A., Pichel, R., Piegaia, T., Pierog, M., Pimenta, T., Pinto, V., Pirronello, O., Pisanti, M., Platino, J., Pochon, P., Privitera, M., Prouza, E. J., Quel, J., Rautenberg, A., Redondo, S., Reucroft, B., Revenu, F. A. S., Rezende, J., Ridky, S., Riggi, M., Risse, C., Riviere, V., Rizi, M., Robert, C., Robledo, G., Rodriguez, M. D., Rodriguez Fria, J., Rodriguezmartino, J., Rodriguez Rojo, I., Rodriguez Cabo, G., Ro, J., Rosado, M., Roth, C., Roucelle, B., Rouille' d’Orfeuil, E., Roulet, A. C., Rovero, F., Salamida, H., Salazar, G., Salina, F., Sanchez, M., Santander, C. E., Santo, E. M., Santo, F., Sarazin, S., Sarkar, R., Sato, V., Scherini, H., Schieler, A., Schmidt, F., Schmidt, T., Schmidt, O., Scholten, P., Schovanek, F., Schussler, S. J., Sciutto, M., Scuderi, A., Segreto, D., Semikoz, M., Settimo, R. C., Shellard, I., Sidelnik, B. B., Siffert, G., Sigl, N., Smetniansky De Grande, A., Smialkowski, R., Smida, A. G. K., Smith, B. E., Smith, G. R., Snow, P., Sokolsky, P., Sommer, J., Sorokin, H., Spinka, R., Squartini, E., Strazzeri, A., Stutz, F., Suarez, T., Suomijarvi, A. D., Supanitsky, M. S., Sutherland, J., Swainc, Z., Szadkowski, J., Takahashi, A., Tamashiro, A., Tamburro, O., Tascau, R., Tcaciuc, D., Thoma, R., Ticon, J., Tiffenberg, C., Timmerman, W., Tkaczyk, C. J., Todero Peixoto, B., Tome', A., Tonachini, I., Torre, D., Torresi, P., Travnicek, A., Tripathi, G., Tristram, D., Tscherniakhovski, M., Tuero, V., Tunnicliffe, R., Ulrich, M., Unger, M., Urbana, J. F., Valdes Galicia, I., Valino, L., Valore, A. M., van den Berg, V., van Elewyck, R. A., Vazquez, D., Veberic, A., Veiga, A., Velarde, T., Ventersc, V., Verzi, M., Videl, L., Villasenor, S., Vorobiov, L., Voyvodic, H., Wahlber, O., Wainber, P., Walker, D., Warner, A. A., Watson, S., Westerhoff, G., Wieczorek, L., Wiencke, B., Wilczynska, H., Wilczynski, C., Wileman, M. G., Winnick, H., Wua, B., Wundheiler, T., Yamamoto, P., Younk, E., Zasb, D., Zavrtanik, M., Zavrtanik, A., Zech, A., Zepeda, M., Ziolkowski, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-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 sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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), 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 sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut für theoretische Physik, 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)-Université Paris Diderot - Paris 7 (UPD7)-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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut für theoretische Physik, Guarino, Fausto, D'Urso, Domenico, Aramo, Carla, Miele, Gennaro, Pisanti, Ofelia, and Valore, Laura

Subjects
Photon, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astronomy, Flux, FOS: Physical sciences, Osservatorio Pierre Auger, Cosmic ray, Fotones, Astrophysics, 7. Clean energy, 01 natural sciences, Auger, Nuclear physics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], High Energy Physics - Phenomenology (hep-ph), Raggi cosmici, ultra high energy photons, Cascada atmosférica, Observatory, 0103 physical sciences, 010306 general physics, Ciencias Exactas, Pierre Auger Observatory, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Física, Astronomy and Astrophysics, Energia ultra alta, High Energy Physics - Phenomenology, Pair production, 13. Climate action, Fotoni, Experimental High Energy Physics, ddc:540, flux upper limit, Neutrino, Sciami atmosferici estesi
Abstract

A method is developed to search for air showers initiated by photons using data recorded by the surface detector of the Auger Observatory. The approach is based on observables sensitive to the longitudinal shower development, the signal risetime and the curvature of the shower front. Applying this method to the data, upper limits on the flux of photons of 3.8 x 10-3, 2.5 x 10-3; and 2.2 x 10-3 km-2 sr-1 yr-1 above 1019 eV, 2 x 1019 eV; and 4 x 1019 eV are derived, with corresponding limits on the fraction of photons being 2.0%, 5.1%, and 31% (all limits at 95% c.l.). These photon limits disfavor certain exotic models of sources of cosmic rays. The results also show that the approach adopted by the Auger Observatory to calibrate the shower energy is not strongly biased by a contamination from photons., Facultad de Ciencias Exactas

Published
2008

41. Erratum to 'Correlation of the highest-energy cosmic rays with the positions of nearby active galactic nuclei' [Astroparticle Physics 29(3) (2008) 188-204]

Author

Abraham, J., Abreu, P., Aglietta, M., Aguirre, C., Allard, D., Allekotte, I., Allen, J., Allison, P., Alvarez, C., Alvarez-Muniz, J., Ambrosio, M., Anchordoqui, L., Andringa, S., Anzalone, A., Aramo, C., Argiro, S., Arisaka, K., Armengaud, E., Arneodo, F., Arqueros, F., Asch, T., Asorey, H., Assis, P., Atulugama, B.S., Aublin, J., Ave, M., Avila, G., Bäcker, T., Badagnani, D., Barbosa, A.F., Barnhill, D., Barroso, S.L.C., Bauleo, P., Beatty, J., Beau, T., Becker, B.R., Becker, K.H., Bellido, J.A., Benzvi, S., Bérat, C., Bergmann, T., Bernardini, P., Bertou, X., Biermann, P.L., Billoir, P., Blanch-Bigas, O., Blanco, F., Blasi, P., Bleve, C., Blümer, H., Bohacova, M., Bonifazi, C., Bonino, R., Boratav, M., Brack, J., Brogueira, P., Brown, W.C., Buchholz, P., Bueno, A., Burton, R.E., Busca, N.G., Caballero-Mora, K.S., Cai, B., Camin, D.V., Caramete, L., Caruso, R., Carvalho, W., Castellina, A., Catalano, O., Cataldi, G., Cazon-Boado, L., Cester, R., Chauvin, J., Chiavassa, A., Chinellato, J.A., Chou, A., Chye, J., Clark, P.D.J., Clay, R.W., Colombo, E., Conceiçao, R., Connolly, B., Contreras, F., Coppens, J., Cordier, A., Cotti, U., Coutu, S., Covault, C.E., Creusot, A., Cronin, J., Curutiu, A., Dagoret-Campagne, S., Daumiller, K., Dawson, B.R., de Almeida, R.M., de Donato, C., de Jong, S.J., de La Vega, G., de Mello Junior, W.J.M., de Mello Neto, J.R.T., de Mitri, I., de Souza, V., del Peral, L., Deligny, O., Della Selva, A., Delle Fratte, C., Dembinski, H., Di Giulio, C., Diaz, J.C., Dobrigkeit, C., d'Olivo, J.C., Dornic, D., Dorofeev, A., dos Anjos, J.C., Dova, M.T., d'Urso, D., Dutan, I., Duvernois, M.A., Engel, R., Epele, L., Erdmann, M., Escobar, C.O., Etchegoyen, A., Facal San Luis, P., Falcke, H., Farrar, G., Fauth, A.C., Fazzini, N., Fernandez, Arnaud, Ferrer, F., Ferry, S., Fick, B., Filevich, A., Filipcic, A., Fleck, I., Fonte, R., Fracchiolla, C.E., Fulgione, W., Garc&#305a, B., Garc&#305a Gamez, D., Garcia-Pinto, D., Garrido, X., Geenen, H., Gelmini, G., Gemmeke, H., Ghia, P.L., Giller, M., Glass, H., Gold, M.S., Golup, G., Gomez Albarracin, F., Gomez, M., Gomez Herrero, R., Gonçalves, Paulo, Gonçalves Do Amaral, M., Gonzalez, D., Gonzalez, J.G., Gonzalez, M., Gora, D., Gorgi, A., Gouffon, P., Grassi, V., Grillo, A.F., Grunfeld, C., Guardincerri, Y., Guarino, F., Guedes, G.P., Gutiérrez, J., Hague, J.D., Hamilton, J.-C., Hansen, P., Harari, D., Harmsma, S., Harton, J.L., Haungs, A., Hauschildt, T., Healy, M.D., Hebbeker, T., Heck, D., Hojvat, C., Holmes, V.C., Homola, P., Hörandel, J., Horneffer, A., Horvat, M., Hrabovsky, M., Huege, T., Iarlori, M., Insolia, A., Ionita, F., Italiano, A., Kaducak, M., Kampert, K.H., Karova, T., Kégl, Balázs, Keilhauer, B., Kemp, E., Kieckhafer, R.M., Klages, H.O., Kleifges, M., Kleinfeller, J., Knapik, R., Knapp, J., Koang, D.H., Kopmann, A., Krieger, A., Krömer, O., Kümpel, D., Kunka, N., Kusenko, A., La Rosa, G., Lachaud, C., Lago, B.L., Lebrun, D., Lebrun, P., Lee, J., Leigui, M.A., Oliveira, De, Letessier-Selvon, A., Leuthold, M., Lhenry-Yvon, I., Lopez, R., Lopez, A., Lozano Bahilo, J., Maccarone, M.C., Macolino, C., Maldera, S., Malek, M., Mancarella, G., Mancenido, M.E., Mandat, D., Mantsch, P., Mariazzi, A.G., Maris, I.C., Martello, D., Mart&#305nez, J., Mart&#305nez Bravo, O., Mathes, H.J., Matthews, J., Matthews, J.A.J., Matthiae, G., Maurizio, D., Mazur, P.O., Mccauley, T., Mcewen, M., Mcneil, R.R., Medina, M.C., Medina-Tanco, G., Meli, A., Melo, D., Menichetti, E., Menschikov, A., Meurer, Chr., Meyhandan, R., Micheletti, M.I., Miele, G., Miller, W., Mollerach, S., Monasor, M., Monnier Ragaigne, D., Montanet, F., Morales, B., Morello, C., Moreno, E., Moreno, J.C., Morris, C., Mostafa, M., Muller, M.A., Mussa, R., Navarra, G., Navarro, J.L., Navas, S., Necesal, P., Nellen, L., Newman-Holmes, C., Newton, D., Nguyen Thi, T., Nierstenhöfer, N., Nitz, D., Nosek, D., Nozka, L., Oehlschläger, J., Ohnuki, T., Olinto, A., Olmos-Gilbaja, V.M., Ortiz, M., Ostapchenko, S., Otero, L., Pakk Selmi-Dei, D., Palatka, M., Pallotta, J., Parente, G., Parizot, E., Parlati, S., Pastor, S., Patel, M., Paul, T., Pavlidou, V., Payet, K., Pech, M., Pekala, J., Pelayo, R., Pepe, I.M., Perrone, L., Petrera, S., Petrinca, P., Petrov, Y., Pham Ngoc, Diep, Pham Ngoc, Dong, Pham Thi, T.N., Pichel, A., Piegaia, R., Pierog, T., Pimenta, M., Pinto, T., Pirronello, V., Pisanti, O., Platino, M., Pochon, J., Porter, T.A., Privitera, P., Prouza, M., Quel, E.J., Rautenberg, J., Reucroft, S., Revenu, Benoît, Rezende, F.A.S., R&#305dky, J., Riggi, S., Risse, M., Rivière, C., Rizi, V., Roberts, M., Robledo, C., Rodriguez, G., Rodr&#305guez Fr&#305as, D., Rodriguez Martino, J., Rodriguez, J., Rodriguez-Cabo, I., Ros, G., Rosado, J., Roth, M., Rouillé-d'Orfeuil, B., Roulet, E., Rovero, A.C., Salamida, F., Salazar, H., Salina, G., Sanchez, F., Santander, M., Santo, C.E., Santos, E.M., Sarazin, F., Sarkar, S., Sato, R., Scherini, V., Schieler, H., Schmidt, F., Schmidt, T., Scholten, O., Schovanek, P., Schüssler, F., Sciutto, S.J., Scuderi, M., Segreto, A., Semikoz, D.V., Settimo, M., Shellard, R.C., Sidelnik, I., Siffert, B.B., Sigl, G., Smetniansky de Grande, N., Smia&#322kowski, A., Sm&#305da, R., Smith, A.G.K., Smith, B.E., Snow, G.R., Sokolsky, P., Sommers, P., Sorokin, J., Spinka, H., Squartini, R., Strazzeri, E., Stutz, A., Suarez, F., Suomijärvi, T., Supanitsky, A.D., Sutherland, M.S., Swain, J., Szadkowski, Z., Takahashi, J., Tamashiro, A., Tamburro, A., Tascau, O., Tcaciuc, R., Thomas, D., Ticona, R., Tiffenberg, J., Timmermans, C., Tkaczyk, W., Todero Peixoto, C.J., Tomé, B., Tonachini D. Torresi, A., Travnicek, P., Tripathi, A., Tristram, G., Tscherniakhovski, D., Tueros, M., Tunnicliffe, V., Ulrich, R., Unger, M., Urban, Martin, Valdés Galicia, J.F., Valino, I., Valore, L., van den Berg, A.M., van Elewyck, V., Vazquez, R.A., Veberic, D., Veiga, A., Velarde, A., Venters, T., Verzi, V., Videla, M., Villasenor, L., Vorobiov, S., Voyvodic, L., Wainberg, O., Walker, P., Warner, D., Watson, A.A., Westerhoff, S., Wieczorek, G., Wiencke, L., Wilczynska, B., Wilczynski, H., Wileman, C., Winnick, M.G., Wu, H., Wundheiler, B., Xu, J., Yamamoto, T., Younk, P., Zas, E., Zavrtanik, D., Zavrtanik, M., Zech, A., Zepeda, A., Ziolkowski, M., APC - Astrophysique des Hautes Energies (APC - AHE), 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)-Université Paris Diderot - Paris 7 (UPD7)-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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-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 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), 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), Institut de Physique Nucléaire d'Orsay (IPNO), APC - THEORIE, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut für theoretische Physik, Universität Hamburg (UHH)-Universität Hamburg (UHH), PIERRE AUGER, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-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 sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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), 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 sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut für theoretische Physik, 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)-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)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), 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)-Université Grenoble Alpes (UGA), and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut für theoretische Physik

Subjects
Astroparticle physics, Physics, Active galactic nucleus, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astronomy and Astrophysics, Cosmic ray, Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Ultra-high-energy cosmic ray, 010306 general physics, Energy (signal processing)
Published
2008

42. Evaluation of the Primary Energy of UHE Photon-induced Atmospheric Showers from Ground Array Measurements

Author

Billoir, P., Roucelle, C., Hamilton, J.-C., Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-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 sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), 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 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)-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)-Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-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)-Université Paris Diderot - Paris 7 (UPD7)-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, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics
Abstract

10 pages; A photon induced shower at $E_{prim}\ge 10^{18}$ eV exhibits very specific features and is different from a hadronic one. At such energies, the LPM effect delays in average the first interactions of the photon in the atmosphere and hence slows down the whole shower development. They also have a smaller muonic content than hadronic ones. The response of a surface detector such as that of the Auger Observatory to these specific showers is thus different and has to be accounted for in order to enable potential photon candidates reconstruction correctly. The energy reconstruction in particular has to be adapted to the late development of photon showers. We propose in this article a method for the reconstruction of the energy of photon showers with a surface detector. The key feature of this method is to rely explicitly on the development stage of the shower. This approach leads to very satisfactory results ($\simeq 20%$). At even higher energies ($5.10^{19}$ eV and above) the probability for the photon to convert into a pair of e$^+$e$^-$ in the geomagnetic field becomes non negligible and requires a different function to evaluate the energy with the proposed method. We propose several approaches to deal with this issue in the scope of the establishment of an upper bound on the photon fraction in UHECR.

Published
2007

44. Search for anisotropies in the ultra high energy cosmic rays with the Pierre Auger Observatory

Author

Hamilton, J.-C., 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), and PIERRE AUGER

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present in these proceedings a method developped by the Pierre Auger Collaboration to estimate the background expected number of events in a given direction of the sky in the purpose of anisotropy searches. We also present the first results of the Pierre Auger Observatory regarding the search for excess sources in the regions previously announced for prescriptions, a blind search and a study towards the Galactic Center and Galactic and Super Galactic planes.

Published
2005

45. Bulge Microlensing Optical Depth from EROS 2 observations

Author

Afonso, C., Albert, J N., Alard, C., Andersen, J., Ansari, R., Aubourg, E., Bareyre, P., Bauer, F., Beaulieu, J-P., Blanc, G., Bouquet, A., Char, S., Charlot, X., Couchot, F., Coutures, C., Derue, F., Ferlet, R., Fouque, P., Glicenstein, J-F., Goldman, B., Gould, A., Graff, D., Gros, M., Haissinski, J., Hamache, C., Hamilton, J-C., Hardin, Doug, de Kat, J., Kim, A., Lasserre, T., Le Guillou, L., Lesquoy, E., Loup, C., Magneville, C., Mansoux, B., Marquette, J-B., Maurice, E., Maury, A., Milsztajn, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Prevot, L., Regnault, N., Rich, J., Spiro, M., Tisserand, P., Vidal-Madjar, A., Vogroux, L., Zylberajch, S., 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), 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), Laboratoire de l'Accélérateur Linéaire (LAL), 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), Departement d'Astrophysique Stellaire et Galactique (DASGAL), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-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'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), EROS, 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), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Departement de recherche SPAtiale (DESPA)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present a measurement of the microlensing optical depth toward the Galactic bulge based on the analysis of 15 contiguous1 square degrees fields centered on (l=2.5 deg, b=-4.0 deg) and containing 1.42 million clump-giant stars (belonging to the extended clump area) monitored during almost three bulge seasons by EROS (Experience de Recherche d'Objets Sombres). We find a microlensing optical depth towards the bulge tau_bulge=0.94 +/- 0.29 10^-6 averaged over all fields, based on 16 microlensing events with clump giants as sources. This value is substantially below several other determinations by the MACHO and OGLE groups and is more in agreement with what is expected from axisymmetric and non-axisymmetric bulge models., 18 pages, 15 images, accepted for publication in A&A

Published
2003

46. Photometric constraints on microlens spectroscopy of EROS-BLG-2000-5

Author

Alfonso, C., Albert, J. N., Andersen, J., Ansari, R., Aubourg, É, Bareyre, P., Bauer, F., Blanc, G., Bouquet, A., Char, S., Charlot, X., Couchot, F., Coutures, C., Derue, F., Ferlet, R., Fouqué, P., Glicenstein, J. F., Goldman, B., Gould, A., Graff, D., Gros, M., Haïssinski, J., Hamilton, J. C., Hardin, D., Kat, J., Kim, A., Lasserre, T., Leguillou, L., Lesquoy, É, Loup, C., Magneville, C., Mansoux, B., Marquette, J. B., Maurice, É, Milsztajn, A., Moniez, M., Nathalie Palanque-Delabrouille, Perdereau, O., Prévot, L., Regnault, N., Rich, J., Spiro, M., Vidal-Madjar, A., Vigroux, L., Zylberajch, S., 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), Laboratoire de l'Accélérateur Linéaire (LAL), 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), 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), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Departement de recherche SPAtiale (DESPA), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), 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), EROS, 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), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Fouqué, Pascal

Subjects
Physics, Microlens, Photosphere, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Radius, Atmospheric model, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, Spectral line, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 13. Climate action, Space and Planetary Science, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Absorption (electromagnetic radiation), Spectroscopy, 010303 astronomy & astrophysics, Chromosphere
Abstract

We apply EROS photometric data to interpret previously published Keck and VLT spectra of the binary-microlens caustic-crossing event EROS-BLG-2000-5. We show that the VLT data imply that the outer 4 % of the limb of the K3-giant source is strongly in emission in Halpha, in contradiction to available models of the photosphere. This conflict could be resolved if the integrated Halpha emission from the chromosphere were equal to 8 % of the integrated Halpha absorption from the source as a whole. These conclusions regarding the extreme limb are almost completely model-independent. We also present a general method for using the photometric data to facilitate direct comparison between the atmospheric model and the spectroscopic data. While this method has some model-dependent features, it is fairly robust and can serve to guide the analysis of spectra while more detailed models of the lens geometry are being developed. In addition, we find that the color of the limb of the source (outer 5.5 % by radius) is Delta(V-I) = 0.37 redder than the source as a whole, so that it has the color of a M0 giant., Comment: 7 figures, 1 table

Published
2001

47. Correlation of the South Pole 94 data with 100 $\mu$m and 408 MHz maps

Author

Hamilton, J-C., Ganga, K-M., 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), and Lantz, Simone

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract

We present a correlation between the ACME/SP94 CMB anisotropy data at 25 to 45 GHz with the IRAS/DIRBE data and the Haslam 408 MHz data. We find a marginal correlation between the dust and the Q-band CMB data but none between the CMB data and the Haslam map. While the amplitude of the correlation with the dust is larger than that expected from naive models of dust emission it does not dominate the sky emission.

Published
2001

48. The optical design of the QUBIC beam combiner

Author

Holland, WS, Zmuidzinas, J, Gayer, D, Bennett, D, O'Sullivan, C, Scully, S, Curran, G, Hamilton, J, Bigot Sazy, M, Piat, M, Kaplan, J, Tartari, A, Gervasi, M, Zannoni, M, Hamilton, J. C., Bigot Sazy, M. A, GERVASI, MASSIMO, ZANNONI, MARIO, Holland, WS, Zmuidzinas, J, Gayer, D, Bennett, D, O'Sullivan, C, Scully, S, Curran, G, Hamilton, J, Bigot Sazy, M, Piat, M, Kaplan, J, Tartari, A, Gervasi, M, Zannoni, M, Hamilton, J. C., Bigot Sazy, M. A, GERVASI, MASSIMO, and ZANNONI, MARIO

Abstract

The Q and U Bolometric Interferometer for Cosmology (QUBIC) is a ground-based interferometer that aims to meet one of the major challenges of modern cosmology in the detection of B-mode polarization anisotropies in the Cosmic Microwave Background.B-mode anisotropies originate from tensor fluctuations of the metric produced during the inflationary phase of the early Universe. Their detection would therefore constitute a major step towards understanding the primordial Universe. The expected level of these anisotropies is however so small that detection requires instruments with high sensitivity and extremely good control of systematic effects. The QUBIC instrument is based on the novel concept of bolometric interferometry, and exploits the sensitivity advantages of bolometric detectors along with the greater control of systematics offered by interferometry.The instrument will directly observe the sky through an array of entry horns whose signals will be combined optically onto an array of bolometers cooled to around 300mK. The whole set-up is located inside a cryostat. The sensitivity of the instrument is maximised if equivalent baselines produce identical fringe patterns on the focal plane. This requires the minimization of wavefront aberrations for a wide field-of-view and a fast system.In this poster we present the quasi-optical design and analysis of the dual reflector designed to do this. We report on the loss of sensitivity for different levels of optical aberration in the combiner. The sensitivity of the QUBIC instrument is comparable with that of an imager with the same number of horns but with much greater control over systematics.

Published
2012

49. Observation of Microlensing towards the Galactic Spiral Arms: EROS II 3 year survey

Author

Derue, F, Afonso, C, Alard, C, Albert, J N, Andersen, J, Ansari, R, Aubourg, E, Bareyre, P, Bauer, F, Beaulieu, J P, Blanc, G, Bouquet, A, Char, S, Charlot, X, Couchot, F, Coutures, C, Ferlet, R, Fouqué, P, Glicenstein, J F, Goldman, B, Gould, A, Graff, D, Gros, M H, Haïssinski, J, Hamilton, J C, Hardin, D, De Kat, J, Kim, A, Lasserre, T, Le Guillou, Laurent, Lesquoy, E, Loup, C, Magneville, C, Mansoux, B, Marquette, J B, Maurice, E, Milsztajn, A, Moniez, M, Palanque-Delabrouille, Nathalie, Perdereau, O, Prévot, L, Regnault, N, Rich, J, Spiro, Michel, Vidal-Madjar, A, Vigroux, L, and Zylberajch, S

Subjects
Astrophysics and Astronomy
Published
2000

50. Eros variable stars: A catalog of Cepheids in the Magellanic Clouds

Author

Afonso, C., Hamilton, J.-C., Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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), and EROS-2

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO]
Abstract

17 pages, 4 Eps figures, 17 Gif figures Submitted to A&A Suppl., Report with figures of higher quality (99 Eps figures) + catalog are available at http://www-dapnia.cea.fr/Phys/Spp/Experiences/EROS/Cepheides/catalog_cep.html; We present a catalog containing 290 LMC and 590 SMC Cepheids which have been obtained using the two 4k $\times$ 8k CCD cameras of the EROS~2 microlensing survey. The Cepheids were selected from 1,134,000 and 504,000 stars in the central regions of the LMC and SMC respectively, that were monitored over 150 nights between October 1996 and February 1997, at a rate of one measurement every night. For each Cepheid the light curves, period, magnitudes in the EROS~2 filter system, Fourier coefficients, J2000 coordinates and cross-identifications with objects referenced in the CDS Simbad database are presented. Finding charts of identified Cepheids in clusters NGC 1943, NGC 1958 and Bruck 56 are presented. The catalogue and the individual light--curves will be electronically available through the CDS (Strasbourg).

Published
1999

Catalog

Books, media, physical & digital resources
See catalog results