LOGIN TO YOUR ACCOUNT

Username
Password
Remember Me
Or use your Academic/Social account:

CREATE AN ACCOUNT

Or use your Academic/Social account:

Congratulations!

You have just completed your registration at OpenAire.

Before you can login to the site, you will need to activate your account. An e-mail will be sent to you with the proper instructions.

Important!

Please note that this site is currently undergoing Beta testing.
Any new content you create is not guaranteed to be present to the final version of the site upon release.

Thank you for your patience,
OpenAire Dev Team.

Close This Message

CREATE AN ACCOUNT

Name:
Username:
Password:
Verify Password:
E-mail:
Verify E-mail:
*All Fields Are Required.
Please Verify You Are Human:
fbtwitterlinkedinvimeoflicker grey 14rssslideshare1
Schneider, Aurel; Teyssier, Romain; Potter, Doug; Stadel, Joachim; Onions, Julian; Reed, Darren S; Smith, Robert E; Springel, Volker; Pearce, Frazer R; Scoccimarro, Roman (2016)
Publisher: IOP Publishing
Languages: English
Types: Article
Subjects: QB, 530 Physics, Institute for Computational Science, Astrophysics - Cosmology and Nongalactic Astrophysics
Future galaxy surveys require one percent precision in the theoretical knowledge of the power spectrum over a large range including very nonlinear scales. While this level of accuracy is easily obtained in the linear regime with perturbation theory, it represents a serious challenge for small scales where numerical simulations are required. In this paper we quantify the precision of present-day $N$-body methods, identifying main potential error sources from the set-up of initial conditions to the measurement of the final power spectrum. We directly compare three widely used $N$-body codes, Ramses, Pkdgrav3, and Gadget3 which represent three main discretisation techniques: the particle-mesh method, the tree method, and a hybrid combination of the two. For standard run parameters, the codes agree to within one percent at $k\leq1$ $h\,\rm Mpc^{-1}$ and to within three percent at $k\leq10$ $h\,\rm Mpc^{-1}$. We also consider the bispectrum and show that the reduced bispectra agree at the sub-percent level for $k\leq 2$ $h\,\rm Mpc^{-1}$. In a second step, we quantify potential errors due to initial conditions, box size, and resolution using an extended suite of simulations performed with our fastest code Pkdgrav3. We demonstrate that the simulation box size should not be smaller than $L=0.5$ $h^{-1}\rm Gpc$ to avoid systematic finite-volume effects (while much larger boxes are required to beat down the statistical sample variance). Furthermore, a maximum particle mass of $M_{\rm p}=10^{9}$ $h^{-1}\rm M_{\odot}$ is required to conservatively obtain one percent precision of the matter power spectrum. As a consequence, numerical simulations covering large survey volumes of upcoming missions such as DES, LSST, and Euclid will need more than a trillion particles to reproduce clustering properties at the targeted accuracy.
  • The results below are discovered through our pilot algorithms. Let us know how we are doing!

    • [1] Ivezic, Z. et al. 2008, arXiv:0805.2366
    • [2] Laureijs, R. et al. 2011, arXiv:1110.3193L
    • [3] Carlson, J., White, M., Padmanabhan, N. 2009, PRD, 80, 043531
    • [4] Fosalba, P., Crocce, M., Gaztañaga, E., Castander, F. J. 2015, MNRAS, 448, 2987F
    • [5] van Daalen, M. P., Schaye, J., Booth, C. M., Dalla Vecchia, C. 2011, MNRAS, 415, 3649V
    • [6] Schneider, A., Teyssier, R. 2015, JCAP, 12, 049S
    • [7] Mohammed, I., Martizzi, D., Teyssier, R., Amara, A. 2014, arXiv:1410.6826
    • [8] Efstathiou, G., Davis, M., White, S. D. M., Frenk, C. S. 1985, ApJS, 57, 241E
    • [9] O'Shea, B. W. Nagamine, K., Springel, V., Hernquist, L., Norman, M. L. 2005, ApJ, 160, 1O
    • [10] Heitmann, K., Ricker, P. M., Warren, M. S., Habib, S. 2005, ApJ, 160, 28H
    • [11] Heitmann, K. et al. 2008, CS&D, 1a5003H
    • [12] Heitmann, K., White, M., Wagner, C., Habib, S., Higdon, D. 2010, ApJ, 715, 104H
    • [13] Crocce, M., Pueblas, S., Scoccimarro, R. 2006, MNRAS, 373, 369C
    • [14] Scoccimarro, R., Hui, L., Manera, M., Chan, K. C. 2012, PRD, 85, 083002
    • [15] Ade, P. A. R, et al. 2014, A&A, 571A, 16P
    • [17] Agertz, O., Teyssier, R., Moore, B. 2011, MNRAS, 410, 1391A
    • [18] Ocvirk, P., Pichon, C., Teyssier, R. 2008, MNRAS, 390, 1326O
    • [19] Rasera, Y., Corasaniti, P.-S., Alimi, J.-M., Bouillot, V., Reverdy, V., Balmès, I. 2014, MNRAS, 440, 1420R
    • [20] Teyssier, R., Pires, S., Prunet, S., Aubert, D., Pichon, C., Amara, A., Benabed, K., Colombi, S., Refregier, A., Starck, J.-L. 2009, A&A, 497, 335T
    • [21] Stadel, J. G. 2001, Thesis (PhD), University of Washington.
    • [22] Diemand, J., Kuhlen, M., Madau, P. 2007, ApJ, 657, 262D
    • [23] Stadel, J., Potter, D., Moore, B., Diemand, J., Madau, P., Zemp, M., Kuhlen, M., Quilis, V. 2009, MNRAS, 398L, 21S
    • [24] Springel, V. 2005, MNRAS, 364, 1105S
    • [25] Springel, V. et al., 2005, Nature, 435, 629S
    • [26] Springel, V., Wang, J., Vogelsberger, M., Ludlow, A., Jenkins, A., Helmi, A., Navarro, J. F., Frenk, C. S., White, S. D. M. 2008, MNRAS, 391, 1685S
    • [27] Bernardeau, F.; Colombi, S.; Gaztañaga, E.; Scoccimarro, R. 2002, Phys. Rep., 367, 1B
    • [28] Pen, U.-L. 1998, ApJ, 504, 601
    • [29] Seljak U., Warren M. S., 2004, MNRAS 355, 129
    • [30] Tegmark, M., Bromley, B. C. 1998, ApJ 518, L69
    • [31] Chiang, L.-Y., Coles, P. 2000, MNRAS, 311, 809
    • [32] Jing, Y. P. 2005, ApJ, 620, 559J
    • [33] Cui, W. Liu, L. Yang, X. Wang Y. Feng, L. Springel, V. 2008, ApJ, 687, 738C
    • [34] Colombi, S., Jaffe, A., Novikov, D., Pichon, C. 2009, MNRAS, 393, 511
    • [35] Jenkins, A. 2010, MNRAS, 403, 1859J
    • [36] Reed, D. S., Smith, R. E., Potter, D., Schneider, A., Stadel, J., Moore, B 2013, MNRAS, 431, 1866R
    • [37] Scoccimarro, R. 1998, MNRAS, 299, 1097
    • [38] Hahn, O., Abel, T. 2011, MNRAS, 415, 2101H
    • [39] Knebe, A., Wagner, C., Knollmann, S., Diekershoff, T., Krause, F. 2009, ApJ, 698, 266K
    • [40] L'Huillier, B., Park, C., Kim, J. 2014, NewAst. 30, 79L
    • [41] McBride, J., Fakhouri, O., Ma, C.-P. 2009, MNRAS, 398, 1858M
    • [42] Gnedin, N. Y., Kravtsov, A. V., Rudd, D. H. 2011, ApJ, 194, 46G
    • [43] Mohammed, I. & Seljak, U. 2014, MNRAS, 445, 3382M
    • [44] Joyce M., Marcos B., Baertschiger, T. 2009, MNRAS, 394, 751J
    • [45] Schneider, A., Smith, R. E., Macciò, A. V. Moore, B. 2012, MNRAS, 424, 684S
    • [46] van Daalen, M. P., Schaye, J. 2015, arXiv:1501.05950
    • [47] Takahashi, R., Sato, M., Nishimichi, T., Taruya, A., Oguri, M. 2012, ApJ, 761, 152T
    • [48] Smith, R. E., Peacock, J. A., Jenkins, A., White, S. D. M., Frenk, C. S., Pearce, F. R., Thomas, P. A., Efstathiou, G., Couchman, H. M. P., 2003, MNRAS, 341, 1311S
    • [49] Heitmann, K., Lawrence, E., Kwan, J., Habib, S., Higdon, D. 2014, ApJ, 780, 111H
    • [50] Skillman, S. W., Warren, M. S., Turk, M. J., Wechsler, R. H., Holz, D. E., Sutter, P. M. 2014, arXiv:1407.2600
    • [51] Angulo, R. E., Hahn, O., Abel, T. 2013, MNRAS, 434, 1756A
    • [52] Smith, R. E., Reed, D. S., Potter, D., Marian, L., Crocce, M., Moore, B., 2014, MNRAS, 440, 249S
    • [53] Crocce, M., Scoccimarro, R. 2006, Phys.Rev.D, 73, 063520
    • [54] Bernardeau, F.; Crocce, M.; Scoccimarro, R. 2012, Phys.Rev.D 85, 123519
    • [55] Sefusatti, E., Crocce, M., Scoccimarro, R., Couchman, H.M.P. 2015, arXiv:1512.07295
  • No related research data.
  • No similar publications.