One simulation to fit them all – changing the background parameters of a cosmological N-body simulation

We demonstrate that the output of a cosmological N-body simulation can, to remarkable accuracy, be scaled to represent the growth of large-scale structure in a cosmology with parameters similar to but different from those originally assumed. Our algorithm involves three steps: a reassignment of leng...

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Published in:	Monthly notices of the Royal Astronomical Society Vol. 405; no. 1; pp. 143 - 154
Main Authors:	Angulo, R. E., White, S. D. M.
Format:	Journal Article
Language:	English
Published:	Oxford, UK Blackwell Publishing Ltd 11.06.2010 Wiley-Blackwell Oxford University Press
Subjects:	Algorithms Amplitudes Astronomy Computer simulation Cosmology cosmology: theory Earth, ocean, space Errors Exact sciences and technology Halos large-scale structure of Universe Mathematical models Scale (corrosion) Simulation Universe large-scale structure of Universe cosmology: theory Red shift Fluctuations Uncertainty Coupling constants Galaxies Power spectra Digital simulation N body system WMAP satellite Large-scale structure Baryons Algorithms Cosmological parameter Galaxy formation Center of mass Positions Cosmology Models Performance Mass spectra
ISSN:	0035-8711, 1365-2966
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Abstract	We demonstrate that the output of a cosmological N-body simulation can, to remarkable accuracy, be scaled to represent the growth of large-scale structure in a cosmology with parameters similar to but different from those originally assumed. Our algorithm involves three steps: a reassignment of length, mass and velocity units; a relabelling of the time axis and a rescaling of the amplitudes of individual large-scale fluctuation modes. We test it using two matched pairs of simulations. Within each pair, one simulation assumes parameters consistent with analyses of the first-year Wilkinson Microwave Anisotropy Probe (WMAP) data. The other has lower matter and baryon densities and a 15 per cent lower fluctuation amplitude, consistent with analyses of the three-year WMAP data. The pairs differ by a factor of a thousand in mass resolution, enabling performance tests on both linear and non-linear scales. Our scaling reproduces the mass power spectra of the target cosmology to better than 0.5 per cent on large scales (k < 0.1 h Mpc−1) both in real and in redshift space. In particular, the baryonic acoustic oscillation features of the original cosmology are removed and are correctly replaced by those of the target cosmology. Errors are still below 3 per cent for k < 1 h Mpc−1. Power spectra of the dark halo distribution are even more precisely reproduced, with errors below 1 per cent on all scales tested. A halo-by-halo comparison shows that centre-of-mass positions and velocities are reproduced to better than 90 h−1 kpc and 5 per cent, respectively. Halo masses, concentrations and spins are also reproduced at about the 10 per cent level, although with small biases. Halo assembly histories are accurately reproduced, leading to central galaxy magnitudes with errors of about 0.25 mag and a bias of about 0.13 mag for a representative semi-analytic model. This algorithm will enable a systematic exploration of the coupling between cosmological parameter estimates and uncertainties in galaxy formation in future large-scale structure surveys.
AbstractList	We demonstrate that the output of a cosmological N-body simulation can, to remarkable accuracy, be scaled to represent the growth of large-scale structure in a cosmology with parameters similar to but different from those originally assumed. Our algorithm involves three steps: a reassignment of length, mass and velocity units; a relabelling of the time axis and a rescaling of the amplitudes of individual large-scale fluctuation modes. We test it using two matched pairs of simulations. Within each pair, one simulation assumes parameters consistent with analyses of the first-year Wilkinson Microwave Anisotropy Probe (WMAP) data. The other has lower matter and baryon densities and a 15 per cent lower fluctuation amplitude, consistent with analyses of the three-year WMAP data. The pairs differ by a factor of a thousand in mass resolution, enabling performance tests on both linear and non-linear scales. Our scaling reproduces the mass power spectra of the target cosmology to better than 0.5 per cent on large scales ( k < 0.1 h Mpc-1 ) both in real and in redshift space. In particular, the baryonic acoustic oscillation features of the original cosmology are removed and are correctly replaced by those of the target cosmology. Errors are still below 3 per cent for k < 1 h Mpc-1 . Power spectra of the dark halo distribution are even more precisely reproduced, with errors below 1 per cent on all scales tested. A halo-by-halo comparison shows that centre-of-mass positions and velocities are reproduced to better than 90 h-1 kpc and 5 per cent, respectively. Halo masses, concentrations and spins are also reproduced at about the 10 per cent level, although with small biases. Halo assembly histories are accurately reproduced, leading to central galaxy magnitudes with errors of about 0.25 mag and a bias of about 0.13 mag for a representative semi-analytic model. This algorithm will enable a systematic exploration of the coupling between cosmological parameter estimates and uncertainties in galaxy formation in future large-scale structure surveys. [PUBLICATION ABSTRACT] We demonstrate that the output of a cosmological N-body simulation can, to remarkable accuracy, be scaled to represent the growth of large-scale structure in a cosmology with parameters similar to but different from those originally assumed. Our algorithm involves three steps: a reassignment of length, mass and velocity units; a relabelling of the time axis and a rescaling of the amplitudes of individual large-scale fluctuation modes. We test it using two matched pairs of simulations. Within each pair, one simulation assumes parameters consistent with analyses of the first-year Wilkinson Microwave Anisotropy Probe (WMAP) data. The other has lower matter and baryon densities and a 15 per cent lower fluctuation amplitude, consistent with analyses of the three-year WMAP data. The pairs differ by a factor of a thousand in mass resolution, enabling performance tests on both linear and non-linear scales. Our scaling reproduces the mass power spectra of the target cosmology to better than 0.5 per cent on large scales (k < 0.1 h Mpc-1) both in real and in redshift space. In particular, the baryonic acoustic oscillation features of the original cosmology are removed and are correctly replaced by those of the target cosmology. Errors are still below 3 per cent for k < 1 h Mpc-1. Power spectra of the dark halo distribution are even more precisely reproduced, with errors below 1 per cent on all scales tested. A halo-by-halo comparison shows that centre-of-mass positions and velocities are reproduced to better than 90 h-1 kpc and 5 per cent, respectively. Halo masses, concentrations and spins are also reproduced at about the 10 per cent level, although with small biases. Halo assembly histories are accurately reproduced, leading to central galaxy magnitudes with errors of about 0.25 mag and a bias of about 0.13 mag for a representative semi-analytic model. This algorithm will enable a systematic exploration of the coupling between cosmological parameter estimates and uncertainties in galaxy formation in future large-scale structure surveys. We demonstrate that the output of a cosmological N-body simulation can, to remarkable accuracy, be scaled to represent the growth of large-scale structure in a cosmology with parameters similar to but different from those originally assumed. Our algorithm involves three steps: a reassignment of length, mass and velocity units; a relabelling of the time axis and a rescaling of the amplitudes of individual large-scale fluctuation modes. We test it using two matched pairs of simulations. Within each pair, one simulation assumes parameters consistent with analyses of the first-year Wilkinson Microwave Anisotropy Probe (WMAP) data. The other has lower matter and baryon densities and a 15 per cent lower fluctuation amplitude, consistent with analyses of the three-year WMAP data. The pairs differ by a factor of a thousand in mass resolution, enabling performance tests on both linear and non-linear scales. Our scaling reproduces the mass power spectra of the target cosmology to better than 0.5 per cent on large scales (k < 0.1 h Mpc−1) both in real and in redshift space. In particular, the baryonic acoustic oscillation features of the original cosmology are removed and are correctly replaced by those of the target cosmology. Errors are still below 3 per cent for k < 1 h Mpc−1. Power spectra of the dark halo distribution are even more precisely reproduced, with errors below 1 per cent on all scales tested. A halo-by-halo comparison shows that centre-of-mass positions and velocities are reproduced to better than 90 h−1 kpc and 5 per cent, respectively. Halo masses, concentrations and spins are also reproduced at about the 10 per cent level, although with small biases. Halo assembly histories are accurately reproduced, leading to central galaxy magnitudes with errors of about 0.25 mag and a bias of about 0.13 mag for a representative semi-analytic model. This algorithm will enable a systematic exploration of the coupling between cosmological parameter estimates and uncertainties in galaxy formation in future large-scale structure surveys. We demonstrate that the output of a cosmological N-body simulation can, to remarkable accuracy, be scaled to represent the growth of large-scale structure in a cosmology with parameters similar to but different from those originally assumed. Our algorithm involves three steps: a reassignment of length, mass and velocity units; a relabelling of the time axis and a rescaling of the amplitudes of individual large-scale fluctuation modes. We test it using two matched pairs of simulations. Within each pair, one simulation assumes parameters consistent with analyses of the first-year Wilkinson Microwave Anisotropy Probe (WMAP) data. The other has lower matter and baryon densities and a 15 per cent lower fluctuation amplitude, consistent with analyses of the three-year WMAP data. The pairs differ by a factor of a thousand in mass resolution, enabling performance tests on both linear and non-linear scales. Our scaling reproduces the mass power spectra of the target cosmology to better than 0.5 per cent on large scales (k < 0.1 h Mpc−1) both in real and in redshift space. In particular, the baryonic acoustic oscillation features of the original cosmology are removed and are correctly replaced by those of the target cosmology. Errors are still below 3 per cent for k < 1 h Mpc−1. Power spectra of the dark halo distribution are even more precisely reproduced, with errors below 1 per cent on all scales tested. A halo-by-halo comparison shows that centre-of-mass positions and velocities are reproduced to better than 90 h −1 kpc and 5 per cent, respectively. Halo masses, concentrations and spins are also reproduced at about the 10 per cent level, although with small biases. Halo assembly histories are accurately reproduced, leading to central galaxy magnitudes with errors of about 0.25 mag and a bias of about 0.13 mag for a representative semi-analytic model. This algorithm will enable a systematic exploration of the coupling between cosmological parameter estimates and uncertainties in galaxy formation in future large-scale structure surveys. ABSTRACT We demonstrate that the output of a cosmological N‐body simulation can, to remarkable accuracy, be scaled to represent the growth of large‐scale structure in a cosmology with parameters similar to but different from those originally assumed. Our algorithm involves three steps: a reassignment of length, mass and velocity units; a relabelling of the time axis and a rescaling of the amplitudes of individual large‐scale fluctuation modes. We test it using two matched pairs of simulations. Within each pair, one simulation assumes parameters consistent with analyses of the first‐year Wilkinson Microwave Anisotropy Probe (WMAP) data. The other has lower matter and baryon densities and a 15 per cent lower fluctuation amplitude, consistent with analyses of the three‐year WMAP data. The pairs differ by a factor of a thousand in mass resolution, enabling performance tests on both linear and non‐linear scales. Our scaling reproduces the mass power spectra of the target cosmology to better than 0.5 per cent on large scales (k < 0.1 h Mpc−1) both in real and in redshift space. In particular, the baryonic acoustic oscillation features of the original cosmology are removed and are correctly replaced by those of the target cosmology. Errors are still below 3 per cent for k < 1 h Mpc−1. Power spectra of the dark halo distribution are even more precisely reproduced, with errors below 1 per cent on all scales tested. A halo‐by‐halo comparison shows that centre‐of‐mass positions and velocities are reproduced to better than 90 h−1 kpc and 5 per cent, respectively. Halo masses, concentrations and spins are also reproduced at about the 10 per cent level, although with small biases. Halo assembly histories are accurately reproduced, leading to central galaxy magnitudes with errors of about 0.25 mag and a bias of about 0.13 mag for a representative semi‐analytic model. This algorithm will enable a systematic exploration of the coupling between cosmological parameter estimates and uncertainties in galaxy formation in future large‐scale structure surveys.
Author	White, S. D. M. Angulo, R. E.
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Cites_doi	10.1016/S0370-1573(02)00276-4 10.1111/j.1365-2966.2005.09782.x 10.1086/587840 10.1086/163168 10.1111/j.1365-2966.2005.09655.x 10.1103/PhysRevLett.103.091302 10.1111/j.1365-2966.2007.12797.x 10.1086/503249 10.1086/512151 10.1086/309179 10.1086/592020 10.1111/j.1365-2966.2004.07962.x 10.1111/j.1365-2966.2009.15921.x 10.1111/j.1365-2966.2006.11287.x 10.1111/j.1365-2966.2009.15572.x 10.1088/0034-4885/69/12/R02 10.1111/j.1365-2966.2008.14211.x 10.1086/377226 10.1038/nature04805 10.1111/j.1365-2966.2007.12587.x 10.1038/nature03597 10.1086/466512 10.1111/j.1365-2966.2009.15819.x 10.1086/513700 10.1111/j.1365-2966.2005.09833.x 10.1103/PhysRevLett.102.021302 10.1086/321477 10.1046/j.1365-8711.2001.04591.x 10.1111/j.1365-2966.2005.09318.x 10.1086/341434 10.1086/152650 10.1086/178037 10.1111/j.1365-2966.2007.12508.x 10.1086/591439 10.1111/j.1365-2966.2007.12035.x 10.1051/0004-6361:20031757 10.1038/nature06555 10.1086/589636 10.1093/mnras/286.1.38
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References_xml	– year: 2009 – volume: 187 start-page: 425 year: 1974 publication-title: ApJ – volume: 366 start-page: 189 year: 2006 publication-title: MNRAS – volume: 170 start-page: 377 year: 2007 publication-title: ApJS – volume: 326 start-page: 255 year: 2001 publication-title: MNRAS – volume: 372 start-page: 1 year: 2002 publication-title: Phys. Rep. – volume: 375 start-page: 2 year: 2007 publication-title: MNRAS – volume: 364 start-page: 1105 year: 2005 publication-title: MNRAS – volume: 435 start-page: 629 year: 2005 publication-title: Nat – volume: 575 start-page: 617 year: 2002 publication-title: ApJ – volume: 440 start-page: 1137 year: 2006 publication-title: Nat – volume: 538 start-page: 473 year: 2000 publication-title: ApJ – volume: 682 start-page: 737 year: 2008 publication-title: ApJ – volume: 366 start-page: 101 year: 2006 publication-title: MNRAS – volume: 402 start-page: 589 year: 2010 publication-title: MNRAS – volume: 382 start-page: 1503 year: 2007 publication-title: MNRAS – volume: 69 start-page: 3101 year: 2006 publication-title: Rep. Progress Phys. – volume: 684 start-page: L1 year: 2008 publication-title: ApJ – volume: 659 start-page: 1 year: 2007 publication-title: ApJ – volume: 379 start-page: 1562 year: 2007 publication-title: MNRAS – volume: 286 start-page: 38 year: 1997 publication-title: MNRAS – volume: 393 start-page: 297 year: 2009 publication-title: MNRAS – volume: 5 start-page: 84 year: 1970 publication-title: A&A – volume: 351 start-page: L44 year: 2004 publication-title: MNRAS – volume: 103 start-page: 091302 year: 2009 publication-title: Phys. Rev. Lett. – volume: 647 start-page: 116 year: 2006 publication-title: ApJ – volume: 688 start-page: 709 year: 2008 publication-title: ApJ – volume: 472 start-page: 14 year: 1996 publication-title: ApJ – volume: 102 start-page: 021302 year: 2009 publication-title: Phys. Rev. Lett. – volume: 400 start-page: 1643 year: 2009 publication-title: MNRAS – volume: 362 start-page: 505 year: 2005 publication-title: MNRAS – volume: 451 start-page: 541 year: 2008 publication-title: Nat – volume: 416 start-page: 853 year: 2004 publication-title: A&A – volume: 401 start-page: 2181 year: 2010 publication-title: MNRAS – volume: 384 start-page: 1301 year: 2008 publication-title: MNRAS – volume: 555 start-page: 240 year: 2001 publication-title: ApJ – volume: 383 start-page: 755 year: 2008 publication-title: MNRAS – volume: 633 start-page: 560 year: 2005 publication-title: ApJ – volume: 292 start-page: 371 year: 1985 publication-title: ApJ – volume: 148 start-page: 175 year: 2003 publication-title: ApJS – volume: 677 start-page: L77 year: 2008 publication-title: ApJ – volume: 372 start-page: 1 year: 2002 ident: 10.1111/j.1365-2966.2010.16459.x-BIB10 publication-title: Phys. Rep. doi: 10.1016/S0370-1573(02)00276-4 – volume: 366 start-page: 101 year: 2006 ident: 10.1111/j.1365-2966.2010.16459.x-BIB21 publication-title: MNRAS doi: 10.1111/j.1365-2966.2005.09782.x – volume: 5 start-page: 84 year: 1970 ident: 10.1111/j.1365-2966.2010.16459.x-BIB42 publication-title: A&A – volume: 677 start-page: L77 year: 2008 ident: 10.1111/j.1365-2966.2010.16459.x-BIB25 publication-title: ApJ doi: 10.1086/587840 – volume: 292 start-page: 371 year: 1985 ident: 10.1111/j.1365-2966.2010.16459.x-BIB12 publication-title: ApJ doi: 10.1086/163168 – volume: 364 start-page: 1105 year: 2005 ident: 10.1111/j.1365-2966.2010.16459.x-BIB35 publication-title: MNRAS doi: 10.1111/j.1365-2966.2005.09655.x – volume: 103 start-page: 091302 year: 2009 ident: 10.1111/j.1365-2966.2010.16459.x-BIB17 publication-title: Phys. Rev. Lett. doi: 10.1103/PhysRevLett.103.091302 – volume: 384 start-page: 1301 year: 2008 ident: 10.1111/j.1365-2966.2010.16459.x-BIB41 publication-title: MNRAS doi: 10.1111/j.1365-2966.2007.12797.x – volume: 647 start-page: 116 year: 2006 ident: 10.1111/j.1365-2966.2010.16459.x-BIB64 publication-title: ApJ doi: 10.1086/503249 – volume: 659 start-page: 1 year: 2007 ident: 10.1111/j.1365-2966.2010.16459.x-BIB43 publication-title: ApJ doi: 10.1086/512151 – volume: 538 start-page: 473 year: 2000 ident: 10.1111/j.1365-2966.2010.16459.x-BIB23 publication-title: ApJ doi: 10.1086/309179 – volume: 684 start-page: L1 year: 2008 ident: 10.1111/j.1365-2966.2010.16459.x-BIB6 publication-title: ApJ doi: 10.1086/592020 – ident: 10.1111/j.1365-2966.2010.16459.x-BIB26 – ident: 10.1111/j.1365-2966.2010.16459.x-BIB38 – volume: 351 start-page: L44 year: 2004 ident: 10.1111/j.1365-2966.2010.16459.x-BIB3 publication-title: MNRAS doi: 10.1111/j.1365-2966.2004.07962.x – volume: 402 start-page: 589 year: 2010 ident: 10.1111/j.1365-2966.2010.16459.x-BIB24 publication-title: MNRAS doi: 10.1111/j.1365-2966.2009.15921.x – volume: 375 start-page: 2 year: 2007 ident: 10.1111/j.1365-2966.2010.16459.x-BIB13 publication-title: MNRAS doi: 10.1111/j.1365-2966.2006.11287.x – volume: 400 start-page: 1643 year: 2009 ident: 10.1111/j.1365-2966.2010.16459.x-BIB31 publication-title: MNRAS doi: 10.1111/j.1365-2966.2009.15572.x – volume: 69 start-page: 3101 year: 2006 ident: 10.1111/j.1365-2966.2010.16459.x-BIB2 publication-title: Rep. Progress Phys. doi: 10.1088/0034-4885/69/12/R02 – volume: 393 start-page: 297 year: 2009 ident: 10.1111/j.1365-2966.2010.16459.x-BIB27 publication-title: MNRAS doi: 10.1111/j.1365-2966.2008.14211.x – volume: 148 start-page: 175 year: 2003 ident: 10.1111/j.1365-2966.2010.16459.x-BIB33 publication-title: ApJS doi: 10.1086/377226 – volume: 440 start-page: 1137 year: 2006 ident: 10.1111/j.1365-2966.2010.16459.x-BIB37 publication-title: Nat doi: 10.1038/nature04805 – volume: 383 start-page: 755 year: 2008 ident: 10.1111/j.1365-2966.2010.16459.x-BIB1 publication-title: MNRAS doi: 10.1111/j.1365-2966.2007.12587.x – volume: 435 start-page: 629 year: 2005 ident: 10.1111/j.1365-2966.2010.16459.x-BIB36 publication-title: Nat doi: 10.1038/nature03597 – volume: 633 start-page: 560 year: 2005 ident: 10.1111/j.1365-2966.2010.16459.x-BIB16 publication-title: ApJ doi: 10.1086/466512 – volume: 401 start-page: 2181 year: 2010 ident: 10.1111/j.1365-2966.2010.16459.x-BIB22 publication-title: MNRAS doi: 10.1111/j.1365-2966.2009.15819.x – volume: 170 start-page: 377 year: 2007 ident: 10.1111/j.1365-2966.2010.16459.x-BIB34 publication-title: ApJS doi: 10.1086/513700 – ident: 10.1111/j.1365-2966.2010.16459.x-BIB14 – volume: 366 start-page: 189 year: 2006 ident: 10.1111/j.1365-2966.2010.16459.x-BIB30 publication-title: MNRAS doi: 10.1111/j.1365-2966.2005.09833.x – volume: 102 start-page: 021302 year: 2009 ident: 10.1111/j.1365-2966.2010.16459.x-BIB32 publication-title: Phys. Rev. Lett. doi: 10.1103/PhysRevLett.102.021302 – volume: 555 start-page: 240 year: 2001 ident: 10.1111/j.1365-2966.2010.16459.x-BIB5 publication-title: ApJ doi: 10.1086/321477 – volume: 326 start-page: 255 year: 2001 ident: 10.1111/j.1365-2966.2010.16459.x-BIB8 publication-title: MNRAS doi: 10.1046/j.1365-8711.2001.04591.x – volume: 362 start-page: 505 year: 2005 ident: 10.1111/j.1365-2966.2010.16459.x-BIB9 publication-title: MNRAS doi: 10.1111/j.1365-2966.2005.09318.x – volume: 575 start-page: 617 year: 2002 ident: 10.1111/j.1365-2966.2010.16459.x-BIB44 publication-title: ApJ doi: 10.1086/341434 – volume: 187 start-page: 425 year: 1974 ident: 10.1111/j.1365-2966.2010.16459.x-BIB28 publication-title: ApJ doi: 10.1086/152650 – volume: 472 start-page: 14 year: 1996 ident: 10.1111/j.1365-2966.2010.16459.x-BIB40 publication-title: ApJ doi: 10.1086/178037 – volume: 382 start-page: 1503 year: 2007 ident: 10.1111/j.1365-2966.2010.16459.x-BIB19 publication-title: MNRAS doi: 10.1111/j.1365-2966.2007.12508.x – volume: 688 start-page: 709 year: 2008 ident: 10.1111/j.1365-2966.2010.16459.x-BIB39 publication-title: ApJ doi: 10.1086/591439 – volume: 379 start-page: 1562 year: 2007 ident: 10.1111/j.1365-2966.2010.16459.x-BIB11 publication-title: MNRAS doi: 10.1111/j.1365-2966.2007.12035.x – volume: 416 start-page: 853 year: 2004 ident: 10.1111/j.1365-2966.2010.16459.x-BIB15 publication-title: A&A doi: 10.1051/0004-6361:20031757 – volume: 451 start-page: 541 year: 2008 ident: 10.1111/j.1365-2966.2010.16459.x-BIB18 publication-title: Nat doi: 10.1038/nature06555 – volume: 682 start-page: 737 year: 2008 ident: 10.1111/j.1365-2966.2010.16459.x-BIB29 publication-title: ApJ doi: 10.1086/589636 – volume: 286 start-page: 38 year: 1997 ident: 10.1111/j.1365-2966.2010.16459.x-BIB7 publication-title: MNRAS doi: 10.1093/mnras/286.1.38 – ident: 10.1111/j.1365-2966.2010.16459.x-BIB4
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Snippet	We demonstrate that the output of a cosmological N-body simulation can, to remarkable accuracy, be scaled to represent the growth of large-scale structure in a... ABSTRACT We demonstrate that the output of a cosmological N‐body simulation can, to remarkable accuracy, be scaled to represent the growth of large‐scale...
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SubjectTerms	Algorithms Amplitudes Astronomy Computer simulation Cosmology cosmology: theory Earth, ocean, space Errors Exact sciences and technology Halos large-scale structure of Universe Mathematical models Scale (corrosion) Simulation Universe
Title	One simulation to fit them all – changing the background parameters of a cosmological N-body simulation
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