SIMBAD references

2013A&A...550A.128P - Astronomy and Astrophysics, volume 550A, 128-128 (2013/2-1)

Planck intermediate results. II. Comparison of Sunyaev-Zeldovich measurements from Planck and from the Arcminute Microkelvin Imager for 11 galaxy clusters.

PLANCK COLLABORATION (The AMI Collaboration), ADE P.A.R., AGHANIM N., ARNAUD M., ASHDOWN M., AUMONT J., BACCIGALUPI C., BALBI A., BANDAY A.J., BARREIRO R.B., BATTANER E., BATTYE R., BENABED K., BENOIT A., BERNARD J.-P., BERSANELLI M., BHATIA R., BIKMAEV I., BOEHRINGER H., BONALDI A., BOND J.R., BORRILL J., BOUCHET F.R., BOURDIN H., BROWN M.L., BUCHER M., BURENIN R., BURIGANA C., BUTLER R.C., CABELLA P., CARVALHO P., CATALANO A., CAYON L., CHAMBALLU A., CHARY R.-R., CHIANG L.-Y., CHON G., CLEMENTS D.L., COLAFRANCESCO S., COLOMBI S., COULAIS A., CRILL B.P., CUTTAIA F., DA SILVA A., DAHLE H., DAVIES R.D., DAVIS R.J., DE BERNARDIS P., DE GASPERIS G., DE ROSA A., DE ZOTTI G., DELABROUILLE J., DEMOCLES J., DICKINSON C., DIEGO J.M., DOLAG K., DOLE H., DONZELLI S., DORE O., DOUSPIS M., DUPAC X., EFSTATHIOU G., ENSSLIN T.A., ERIKSEN H.K., FEROZ F., FINELLI F., FLORES-CACHO I., FORNI O., FOSALBA P., FRAILIS M., FRANCESCHI E., FROMENTEAU S., GALEOTTA S., GANGA K., GENOVA-SANTOS R.T., GIARD M., GIRAUD-HERAUD Y., GONZALEZ-NUEVO J., GORSKI K.M., GRAINGE K.J.B., GREGORIO A., GRUPPUSO A., HANSEN F.K., HARRISON D., HENROT-VERSILLE S., HERNANDEZ-MONTEAGUDO C., HERRANZ D., HILDEBRANDT S.R., HIVON E., HOBSON M., HOLMES W.A., HUFFENBERGER K.M., HURIER G., HURLEY-WALKER N., JAGEMANN T., JUVELA M., KEIHAENEN E., KHAMITOV I., KNEISSL R., KNOCHE J., KUNZ M., KURKI-SUONIO H., LAGACHE G., LAMARRE J.-M., LASENBY A., LAWRENCE C.R., LE JEUNE M., LEACH S., LEONARDI R., LIDDLE A., LILJE P.B., LINDEN-VORNLE M., LOPEZ-CANIEGO M., LUZZI G., MACIAS-PEREZ J.F., MacTAVISH C.J., MAINO D., MANDOLESI N., MARIS M., MARLEAU F., MARSHALL D.J., MARTINEZ-GONZALEZ E., MASI S., MASSARDI M., MATARRESE S., MATTHAI F., MAZZOTTA P., MEINHOLD P.R., MELCHIORRI A., MELIN J.-B., MENDES L., MENNELLA A., MITRA S., MIVILLE-DESCHENES M.-A., MONTIER L., MORGANTE G., MUNSHI D., NASELSKY P., NATOLI P., NORGAARD-NIELSEN H.U., NOVIELLO F., NOVIKOV D., NOVIKOV I., OLAMAIE M., OSBORNE S., PAJOT F., PAOLETTI D., PASIAN F., PATANCHON G., PEARSON T.J., PERDEREAU O., PERROTT Y.C., PERROTTA F., PIACENTINI F., PIERPAOLI E., PLATANIA P., POINTECOUTEAU E., POLENTA G., POPA L., POUTANEN T., PRATT G.W., PUGET J.-L., RACHEN J.P., REBOLO R., REINECKE M., REMAZEILLES M., RENAULT C., RICCIARDI S., RISTORCELLI I., ROCHA G., RODRIGUEZ-GONZALVEZ C., ROSSET C., ROSSETTI M., RUBINO-MARTIN J.A., RUMSEY C., RUSHOLME B., SANDRI M., SAUNDERS R.D.E., SAVINI G., SCHAMMEL M.P., SCOTT D., SHIMWELL T.W., SMOOT G.F., STARCK J.-L., STIVOLI F., STOLYAROV V., SUDIWALA R., SUNYAEV R., SUTTON D., SUUR-USKI A.-S., SYGNET J.-F., TAUBER J.A., TERENZI L., TOFFOLATTI L., TOMASI M., TRISTRAM M., VALENZIANO L., VAN TENT B., VIELVA P., VILLA F., VITTORIO N., WADE L.A., WANDELT B.D., YVON D., ZACCHEI A. and ZONCA A.

Abstract (from CDS):

A comparison is presented of Sunyaev-Zeldovich measurements for 11 galaxy clusters as obtained by Planck and by the ground-based interferometer, the Arcminute Microkelvin Imager. Assuming a universal spherically-symmetric Generalised Navarro, Frenk and White (GNFW) model for the cluster gas pressure profile, we jointly constrain the integrated Compton-Y parameter (Y₅₀₀) and the scale radius (θ₅₀₀) of each cluster. Our resulting constraints in the Y₅₀₀-θ₅₀₀ 2D parameter space derived from the two instruments overlap significantly for eight of the clusters, although, overall, there is a tendency for AMI to find the Sunyaev-Zeldovich signal to be smaller in angular size and fainter than Planck. Significant discrepancies exist for the three remaining clusters in the sample, namely A1413, A1914, and the newly-discovered Planck cluster PLCKESZ G139.59+24.18. The robustness of the analysis of both the Planck and AMI data is demonstrated through the use of detailed simulations, which also discount confusion from residual point (radio) sources and from diffuse astrophysical foregrounds as possible explanations for the discrepancies found. For a subset of our cluster sample, we have investigated the dependence of our results on the assumed pressure profile by repeating the analysis adopting the best-fitting GNFW profile shape which best matches X-ray observations. Adopting the best-fitting profile shape from the X-ray data does not, in general, resolve the discrepancies found in this subset of five clusters. Though based on a small sample, our results suggest that the adopted GNFW model may not be sufficiently flexible to describe clusters universally.

Abstract Copyright: ∼

Journal keyword(s): cosmology: observations - galaxies: clusters: general - galaxies: clusters: intracluster medium - cosmic background radiation - X-rays: galaxies: clusters

Simbad objects: 47

Full paper

View the references in ADS

To bookmark this query, right click on this link: simbad:2013A&A...550A.128P and select 'bookmark this link' or equivalent in the popup menu