BISPECTRUM OF THE SUNYAEV-ZEL'DOVICH EFFECT

被引：41

作者：

Bhattacharya, Suman ^{[1
,2
]}

Nagai, Daisuke ^{[3
,4
]}

Shaw, Laurie ^{[3
,4
]}

Crawford, Tom ^{[5
]}

Holder, Gilbert P. ^{[6
]}

机构：

[1] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60439 USA

[2] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA

[3] Yale Univ, Dept Phys, New Haven, CT 06520 USA

[4] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA

[5] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA

[6] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada

来源：

ASTROPHYSICAL JOURNAL | 2012年 / 760卷 / 01期

基金：

加拿大自然科学与工程研究理事会; 美国国家科学基金会;

关键词：

cosmic background radiation; cosmology: theory; galaxies: clusters: intracluster medium; large-scale structure of universe; MICROWAVE BACKGROUND ANISOTROPIES; ATACAMA COSMOLOGY TELESCOPE; GALAXY CLUSTERS; POWER SPECTRUM; AGN FEEDBACK; DARK-MATTER; STATISTICAL PROPERTIES; REPRESENTATIVE SAMPLE; MASS FUNCTION; GAS;

D O I：

10.1088/0004-637X/760/1/5

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We perform a detailed study of the bispectrum of the Sunyaev-Zel'dovich (SZ) effect. Using an analytical model for the pressure profiles of the intracluster medium, we demonstrate the SZ bispectrum to be a sensitive probe of the amplitude of the matter power spectrum parameter sigma(8). We find that the bispectrum amplitude scales as B-tSZ proportional to sigma(11-12)(8), compared to that of the power spectrum, which scales as A(tSZ) proportional to sigma(7-9)(8). We show that the SZ bispectrum is principally sourced by massive clusters at redshifts around z similar to 0.4, which have been well studied observationally. This is in contrast to the SZ power spectrum, which receives a significant contribution from less well understood low-mass and high-redshift groups and clusters. Therefore, the amplitude of the bispectrum at l similar to 3000 is less sensitive to astrophysical uncertainties than the SZ power spectrum. We show that current high-resolution cosmic microwave background (CMB) experiments should be able to detect the SZ bispectrum amplitude with high significance, in part due to the low contamination from extragalactic foregrounds. A combination of the SZ bispectrum and the power spectrum can sharpen the measurements of thermal and kinetic SZ components and help distinguish cosmological and astrophysical information from high-resolution CMB maps.

引用

页数：11

共 57 条

[11]

Cooray A, 2000, PHYS REV D, V62, DOI 10.1103/PhysRevD.62.103506

[12] Large-scale Sunyaev-Zeldovich effect: Measuring statistical properties with multifrequency maps [J].

Cooray, A ;

Hu, W ;

Tegmark, M .

ASTROPHYSICAL JOURNAL, 2000, 540 (01) :1-13

[13] Dark matter halo concentrations in the Wilkinson Microwave Anisotropy Probe year 5 cosmology [J].

Duffy, Alan R. ;

Schaye, Joop ;

Kay, Scott T. ;

Dalla Vecchia, Claudio .

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2008, 390 (01) :L64-L68

[14] THE ATACAMA COSMOLOGY TELESCOPE: COSMOLOGICAL PARAMETERS FROM THE 2008 POWER SPECTRUM [J].

Dunkley, J. ;

Hlozek, R. ;

Sievers, J. ;

Acquaviva, V. ;

Ade, P. A. R. ;

Aguirre, P. ;

Amiri, M. ;

Appel, J. W. ;

Barrientos, L. F. ;

Battistelli, E. S. ;

Bond, J. R. ;

Brown, B. ;

Burger, B. ;

Chervenak, J. ;

Das, S. ;

Devlin, M. J. ;

Dicker, S. R. ;

Doriese, W. Bertrand ;

Duenner, R. ;

Essinger-Hileman, T. ;

Fisher, R. P. ;

Fowler, J. W. ;

Hajian, A. ;

Halpern, M. ;

Hasselfield, M. ;

Hernandez-Monteagudo, C. ;

Hilton, G. C. ;

Hilton, M. ;

Hincks, A. D. ;

Huffenberger, K. M. ;

Hughes, D. H. ;

Hughes, J. P. ;

Infante, L. ;

Irwin, K. D. ;

Juin, J. B. ;

Kaul, M. ;

Klein, J. ;

Kosowsky, A. ;

Lau, J. M. ;

Limon, M. ;

Lin, Y-T. ;

Lupton, R. H. ;

Marriage, T. A. ;

Marsden, D. ;

Mauskopf, P. ;

Menanteau, F. ;

Moodley, K. ;

Moseley, H. ;

Netterfield, C. B. ;

Niemack, M. D. .

ASTROPHYSICAL JOURNAL, 2011, 739 (01)

[15] A simple empirically motivated template for the thermal Sunyaev-Zel'dovich effect [J].

Efstathiou, George ;

Migliaccio, Marina .

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2012, 423 (03) :2492-2497

[16] THE ATACAMA COSMOLOGY TELESCOPE: A MEASUREMENT OF THE 600 < l < 8000 COSMIC MICROWAVE BACKGROUND POWER SPECTRUM AT 148 GHz [J].

Fowler, J. W. ;

Acquaviva, V. ;

Ade, P. A. R. ;

Aguirre, P. ;

Amiri, M. ;

Appel, J. W. ;

Barrientos, L. F. ;

Battistelli, E. S. ;

Bond, J. R. ;

Brown, B. ;

Burger, B. ;

Chervenak, J. ;

Das, S. ;

Devlin, M. J. ;

Dicker, S. R. ;

Doriese, W. B. ;

Dunkley, J. ;

Duenner, R. ;

Essinger-Hileman, T. ;

Fisher, R. P. ;

Hajian, A. ;

Halpern, M. ;

Hasselfield, M. ;

Hernandez-Monteagudo, C. ;

Hilton, G. C. ;

Hilton, M. ;

Hincks, A. D. ;

Hlozek, R. ;

Huffenberger, K. M. ;

Hughes, D. H. ;

Hughes, J. P. ;

Infante, L. ;

Irwin, K. D. ;

Jimenez, R. ;

Juin, J. B. ;

Kaul, M. ;

Klein, J. ;

Kosowsky, A. ;

Lau, J. M. ;

Limon, M. ;

Lin, Y. -T. ;

Lupton, R. H. ;

Marriage, T. A. ;

Marsden, D. ;

Martocci, K. ;

Mauskopf, P. ;

Menanteau, F. ;

Moodley, K. ;

Moseley, H. ;

Netterfield, C. B. .

ASTROPHYSICAL JOURNAL, 2010, 722 (02) :1148-1161

[17] STELLAR AND TOTAL BARYON MASS FRACTIONS IN GROUPS AND CLUSTERS SINCE REDSHIFT 1 [J].

Giodini, S. ;

Pierini, D. ;

Finoguenov, A. ;

Pratt, G. W. ;

Boehringer, H. ;

Leauthaud, A. ;

Guzzo, L. ;

Aussel, H. ;

Bolzonella, M. ;

Capak, P. ;

Elvis, M. ;

Hasinger, G. ;

Ilbert, O. ;

Kartaltepe, J. S. ;

Koekemoer, A. M. ;

Lilly, S. J. ;

Massey, R. ;

McCracken, H. J. ;

Rhodes, J. ;

Salvato, M. ;

Sanders, D. B. ;

Scoville, N. Z. ;

Sasaki, S. ;

Smolcic, V. ;

Taniguchi, Y. ;

Thompson, D. .

ASTROPHYSICAL JOURNAL, 2009, 703 (01) :982-993

[18] Weak lensing of the CMB: A harmonic approach [J].

Hu, W .

PHYSICAL REVIEW D, 2000, 62 (04) :17

[19] Cosmological-parameter determination with microwave background maps [J].

Jungman, G ;

Kamionkowski, M ;

Kosowsky, A ;

Spergel, DN .

PHYSICAL REVIEW D, 1996, 54 (02) :1332-1344

[20] Cosmological simulations of the intracluster medium [J].

Kay, ST ;

Thomas, PA ;

Jenkins, A ;

Pearce, FR .

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 2004, 355 (04) :1091-1104

← 1 2 3 4 5 6 →