Superclustering with the Atacama Cosmology Telescope and Dark Energy Survey. I. Evidence for Thermal Energy Anisotropy Using Oriented Stacking

被引:13
|
作者
Lokken, M. [1 ,2 ,3 ]
Hlozek, R. [1 ,2 ]
van Engelen, A. [4 ]
Madhavacheril, M. [5 ,6 ]
Baxter, E. [7 ]
DeRose, J. [8 ]
Doux, C. [9 ]
Pandey, S. [9 ]
Rykoff, E. S. [10 ]
Stein, G. [8 ,11 ]
To, C. [12 ]
Abbott, T. M. C. [13 ]
Adhikari, S. [14 ,15 ]
Aguena, M. [16 ]
Allam, S. [17 ]
Andrade-Oliveira, F. [16 ,18 ]
Annis, J. [17 ]
Battaglia, N. [19 ]
Bernstein, G. M. [9 ]
Bertin, E. [20 ,21 ]
Bond, J. R. [2 ]
Brooks, D. [22 ]
Calabrese, E. [23 ]
Rosell, A. Carnero [16 ,24 ,25 ]
Kind, M. Carrasco [26 ,27 ]
Carretero, J. [28 ]
Cawthon, R. [29 ]
Choi, A. [30 ]
Costanzi, M. [31 ,32 ,33 ]
Crocce, M. [34 ,35 ]
da Costa, L. N. [16 ,36 ]
Pereira, M. E. da Silva [37 ]
De Vicente, J. [38 ]
Desai, S. [39 ]
Dietrich, J. P. [40 ]
Doel, P. [22 ]
Dunkley, J. [41 ,42 ]
Everett, S. [43 ]
Evrard, A. E. [37 ,44 ]
Ferraro, S. [8 ,11 ]
Flaugher, B. [17 ]
Fosalba, P. [34 ,35 ]
Frieman, J. [15 ,17 ]
Gallardo, P. A. [45 ]
Garcia-Bellido, J. [46 ]
Gaztanaga, E. [34 ,35 ]
Gerdes, D. W. [37 ,44 ]
Giannantonio, T. [47 ,48 ]
Gruen, D. [40 ]
Gruendl, R. A. [26 ,27 ]
机构
[1] Univ Toronto, David A Dunlap Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada
[2] Univ Toronto, Canadian Inst Theoret Astrophys, 60 St George St, Toronto, ON M5S 3H4, Canada
[3] Dunlap Inst Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada
[4] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA
[5] Perimeter Inst Theoret Phys, 31 Caroline St N, Waterloo, ON N2L 2Y5, Canada
[6] Univ Southern Calif, Dept Phys & Astron, Los Angeles, CA 90007 USA
[7] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA
[8] Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA
[9] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA
[10] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA
[11] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, 341 Campbell Hall, Berkeley, CA 94720 USA
[12] Stanford Univ, Dept Phys, 382 Via Pueblo Mall, Stanford, CA 94305 USA
[13] Cerro Tololo Interamer Observ, NSFs Natl Opt Infrared Astron Res Lab, Casilla 603, La Serena, Chile
[14] Univ Chicago, Dept Astron & Astrophys, 5640 South Ellis Ave, Chicago, IL 60637 USA
[15] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA
[16] Lab Interinst E Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil
[17] Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA
[18] Univ Estadual Paulista, Inst Fis Teor, Sao Paulo, Brazil
[19] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA
[20] Inst Astrophys Paris, CNRS, UMR 7095, F-75014 Paris, France
[21] Univ Paris 06, Sorbonne Univ, UPMC, Inst Astrophys Paris,UMR 7095, F-75014 Paris, France
[22] UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England
[23] Cardiff Univ, Sch Phys & Astron, Parade, Cardiff CF24 3AA, Wales
[24] Inst Astrofis Canarias, E-38205 Tenerife, Spain
[25] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain
[26] Natl Ctr Supercomp Applicat, Ctr Astrophys Surveys, 1205 West Clark St, Urbana, IL 61801 USA
[27] Univ Illinois, Dept Astron, 1002 West Green St, Urbana, IL 61801 USA
[28] Barcelona Inst Sci & Technol, Inst Fis Altes Energies IFAE, Campus UAB, E-08193 Bellaterra, Barcelona, Spain
[29] Univ Wisconsin, Dept Phys, 2320 Chamberlin Hall,1150 Univ Ave, Madison, WI 53706 USA
[30] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA
[31] Univ Trieste, Dept Phys, Astron Unit, Via Tiepolo 11, I-34131 Trieste, Italy
[32] Osserv Astron Trieste, INAF, Via GB Tiepolo 11, I-34143 Trieste, Italy
[33] Inst Fundamental Phys Universe, Via Beirut 2, I-34014 Trieste, Italy
[34] Inst Estudis Espacials Catalunya IEEC, E-08034 Barcelona, Spain
[35] CSIC, Inst Space Sci ICE, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain
[36] Observ Nacl, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil
[37] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA
[38] Ctr Invest Energet Medioambientales & Tecnol CIEM, Madrid, Spain
[39] IIT Hyderabad, Dept Phys, Kandi 502285, Telangana, India
[40] Ludwig Maximilians Univ Munchen, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany
[41] Princeton Univ, Joseph Henry Labs Phys, Jadwin Hall, Princeton, NJ 08544 USA
[42] Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA
[43] Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA
[44] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA
[45] Cornell Univ, Dept Phys, Ithaca, NY 14850 USA
[46] Univ Autonoma Madrid, CSIC, UAM, Inst Fis Teor, E-28049 Madrid, Spain
[47] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England
[48] Univ Cambridge, Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England
[49] Columbia Univ, Dept Phys, New York, NY 10027 USA
[50] Flatiron Inst, Ctr Computat Astrophys, New York, NY 10010 USA
来源
ASTROPHYSICAL JOURNAL | 2022年 / 933卷 / 02期
基金
英国科学技术设施理事会; 欧洲研究理事会; 美国国家科学基金会; 新加坡国家研究基金会; 加拿大自然科学与工程研究理事会; 加拿大创新基金会;
关键词
GALAXY CLUSTERS; POWER SPECTRUM; AGN FEEDBACK; COSMIC WEB; SIMULATIONS; FILAMENTS; CALIBRATION; ALIGNMENTS; STATISTICS; RADIATION;
D O I
10.3847/1538-4357/ac7043
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The cosmic web contains filamentary structure on a wide range of scales. On the largest scales, superclustering aligns multiple galaxy clusters along intercluster bridges, visible through their thermal Sunyaev-Zel'dovich signal in the cosmic microwave background. We demonstrate a new, flexible method to analyze the hot gas signal from multiscale extended structures. We use a Compton y-map from the Atacama Cosmology Telescope (ACT) stacked on redMaPPer cluster positions from the optical Dark Energy Survey (DES). Cutout images from the y-map are oriented with large-scale structure information from DES galaxy data such that the superclustering signal is aligned before being overlaid. We find evidence of an extended quadrupole moment of the stacked y signal at the 3.5 sigma level, demonstrating that the large-scale thermal energy surrounding galaxy clusters is anisotropically distributed. We compare our ACT x DES results with the Buzzard simulations, finding broad agreement. Using simulations, we highlight the promise of this novel technique for constraining the evolution of anisotropic, non-Gaussian structure using future combinations of microwave and optical surveys.
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页数:28
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