Search

Your search keyword '"Le Brun, A. M. C."' showing total 33 results
Start Over Author "Le Brun, A. M. C."
33 results on '"Le Brun, A. M. C."'

1. Euclid preparation: XXXIX. The effect of baryons on the halo mass function

Author

Castro, T, Borgani, S, Costanzi, M, Dakin, J, Dolag, K, Fumagalli, A, Ragagnin, A, Saro, A, Le Brun, A, Aghanim, N, Amara, A, Andreon, S, Auricchio, N, Baldi, M, Bardelli, S, Bodendorf, C, Bonino, D, Branchini, E, Brescia, M, Brinchmann, J, Camera, S, Capobianco, V, Carbone, C, Carretero, J, Casas, S, Castellano, M, Cavuoti, S, Cimatti, A, Congedo, G, Conselice, C, Conversi, L, Copin, Y, Corcione, L, Courbin, F, Courtois, H, Cropper, M, Da Silva, A, Degaudenzi, H, Di Giorgio, A, Dinis, J, Dubath, F, Duncan, C, Dupac, X, Farina, M, Farrens, S, Ferriol, S, Frailis, M, Franceschi, E, Fumana, M, Galeotta, S, Gillis, B, Giocoli, C, Grazian, A, Grupp, F, Haugan, S, Holmes, W, Hormuth, F, Hornstrup, A, Jahnke, K, Keihanen, E, Kermiche, S, Kiessling, A, Kilbinger, M, Kubik, B, Kunz, M, Kurki-Suonio, H, Ligori, S, Lilje, P, Lindholm, V, Lloro, I, Maiorano, E, Mansutti, O, Marggraf, O, Markovic, K, Martinet, N, Marulli, F, Massey, R, Maurogordato, S, Medinaceli, E, Meneghetti, M, Merlin, E, Meylan, G, Moresco, M, Moscardini, L, Munari, E, Niemi, S, Padilla, C, Paltani, S, Pasian, F, Pettorino, V, Pires, S, Polenta, G, Poncet, M, Popa, L, Pozzetti, L, Raison, F, Rebolo, R, Renzi, A, Rhodes, J, Riccio, G, Romelli, E, Roncarelli, M, Saglia, R, Sapone, D, Sartoris, B, Schneider, P, Schrabback, T, Secroun, A, Seidel, G, Serrano, S, Sirignano, C, Sirri, G, Stanco, L, Starck, J, Tallada-Crespi, P, Taylor, A, Tereno, I, Toledo-Moreo, R, Torradeflot, F, Tutusaus, I, Valentijn, E, Valenziano, L, Vassallo, T, Veropalumbo, A, Wang, Y, Weller, J, Zacchei, A, Zamorani, G, Zoubian, J, Zucca, E, Biviano, A, Bozzo, E, Cerna, C, Colodro-Conde, C, Di Ferdinando, D, Mauri, N, Neissner, C, Sakr, Z, Scottez, V, Tenti, M, Viel, M, Wiesmann, M, Akrami, Y, Anselmi, S, Baccigalupi, C, Ballardini, M, Borlaff, A, Bruton, S, Burigana, C, Cabanac, R, Cappi, A, Carvalho, C, Castignani, G, Canas-Herrera, G, Chambers, K, Cooray, A, Coupon, J, Cucciati, O, Diaz-Sanchez, A, Davini, S, De La Torre, S, De Lucia, G, Desprez, G, Di Domizio, S, Dole, H, Escoffier, S, Ferrero, I, Finelli, F, Gabarra, L, Ganga, K, Garcia-Bellido, J, Giacomini, F, Gozaliasl, G, Hildebrandt, H, Ilic, S, Jimanez Munnoz, A, Kajava, J, Kansal, V, Kirkpatrick, C, Legrand, L, Loureiro, A, MacIas-Perez, J, Magliocchetti, M, Mainetti, G, Maoli, R, Martinelli, M, Martins, C, Matthew, S, Maturi, M, Maurin, L, Metcalf, R, Migliaccio, M, Monaco, P, Morgante, G, Nadathur, S, Patrizii, L, Pezzotta, A, Popa, V, Porciani, C, Potter, D, Pontinen, M, Reimberg, P, Rocci, P, Sanchez, A, Schaye, J, Schneider, A, Sefusatti, E, Sereno, M, Simon, P, Spurio Mancini, A, Stadel, J, Stanford, S, Steinwagner, J, Testera, G, Tewes, M, Teyssier, R, Toft, S, Tosi, S, Troja, A, Tucci, M, Valiviita, J, Vergani, D, Castro T., Borgani S., Costanzi M., Dakin J., Dolag K., Fumagalli A., Ragagnin A., Saro A., Le Brun A. M. C., Aghanim N., Amara A., Andreon S., Auricchio N., Baldi M., Bardelli S., Bodendorf C., Bonino D., Branchini E., Brescia M., Brinchmann J., Camera S., Capobianco V., Carbone C., Carretero J., Casas S., Castellano M., Cavuoti S., Cimatti A., Congedo G., Conselice C. J., Conversi L., Copin Y., Corcione L., Courbin F., Courtois H. M., Cropper M., Da Silva A., Degaudenzi H., Di Giorgio A. M., Dinis J., Dubath F., Duncan C. A. J., Dupac X., Farina M., Farrens S., Ferriol S., Frailis M., Franceschi E., Fumana M., Galeotta S., Gillis B., Giocoli C., Grazian A., Grupp F., Haugan S. V. H., Holmes W., Hormuth F., Hornstrup A., Jahnke K., Keihanen E., Kermiche S., Kiessling A., Kilbinger M., Kubik B., Kunz M., Kurki-Suonio H., Ligori S., Lilje P. B., Lindholm V., Lloro I., Maiorano E., Mansutti O., Marggraf O., Markovic K., Martinet N., Marulli F., Massey R., Maurogordato S., Medinaceli E., Meneghetti M., Merlin E., Meylan G., Moresco M., Moscardini L., Munari E., Niemi S. -M., Padilla C., Paltani S., Pasian F., Pettorino V., Pires S., Polenta G., Poncet M., Popa L. A., Pozzetti L., Raison F., Rebolo R., Renzi A., Rhodes J., Riccio G., Romelli E., Roncarelli M., Saglia R., Sapone D., Sartoris B., Schneider P., Schrabback T., Secroun A., Seidel G., Serrano S., Sirignano C., Sirri G., Stanco L., Starck J. -L., Tallada-Crespi P., Taylor A. N., Tereno I., Toledo-Moreo R., Torradeflot F., Tutusaus I., Valentijn E. A., Valenziano L., Vassallo T., Veropalumbo A., Wang Y., Weller J., Zacchei A., Zamorani G., Zoubian J., Zucca E., Biviano A., Bozzo E., Cerna C., Colodro-Conde C., Di Ferdinando D., Mauri N., Neissner C., Sakr Z., Scottez V., Tenti M., Viel M., Wiesmann M., Akrami Y., Anselmi S., Baccigalupi C., Ballardini M., Borlaff A. S., Bruton S., Burigana C., Cabanac R., Cappi A., Carvalho C. S., Castignani G., Canas-Herrera G., Chambers K. C., Cooray A. R., Coupon J., Cucciati O., Diaz-Sanchez A., Davini S., De La Torre S., De Lucia G., Desprez G., Di Domizio S., Dole H., Escoffier S., Ferrero I., Finelli F., Gabarra L., Ganga K., Garcia-Bellido J., Giacomini F., Gozaliasl G., Hildebrandt H., Ilic S., Jimanez Munnoz A., Kajava J. J. E., Kansal V., Kirkpatrick C. C., Legrand L., Loureiro A., MacIas-Perez J., Magliocchetti M., Mainetti G., Maoli R., Martinelli M., Martins C. J. A. P., Matthew S., Maturi M., Maurin L., Metcalf R. B., Migliaccio M., Monaco P., Morgante G., Nadathur S., Patrizii L., Pezzotta A., Popa V., Porciani C., Potter D., Pontinen M., Reimberg P., Rocci P. -F., Sanchez A. G., Schaye J., Schneider A., Sefusatti E., Sereno M., Simon P., Spurio Mancini A., Stadel J., Stanford S. A., Steinwagner J., Testera G., Tewes M., Teyssier R., Toft S., Tosi S., Troja A., Tucci M., Valiviita J., Vergani D., Castro, T, Borgani, S, Costanzi, M, Dakin, J, Dolag, K, Fumagalli, A, Ragagnin, A, Saro, A, Le Brun, A, Aghanim, N, Amara, A, Andreon, S, Auricchio, N, Baldi, M, Bardelli, S, Bodendorf, C, Bonino, D, Branchini, E, Brescia, M, Brinchmann, J, Camera, S, Capobianco, V, Carbone, C, Carretero, J, Casas, S, Castellano, M, Cavuoti, S, Cimatti, A, Congedo, G, Conselice, C, Conversi, L, Copin, Y, Corcione, L, Courbin, F, Courtois, H, Cropper, M, Da Silva, A, Degaudenzi, H, Di Giorgio, A, Dinis, J, Dubath, F, Duncan, C, Dupac, X, Farina, M, Farrens, S, Ferriol, S, Frailis, M, Franceschi, E, Fumana, M, Galeotta, S, Gillis, B, Giocoli, C, Grazian, A, Grupp, F, Haugan, S, Holmes, W, Hormuth, F, Hornstrup, A, Jahnke, K, Keihanen, E, Kermiche, S, Kiessling, A, Kilbinger, M, Kubik, B, Kunz, M, Kurki-Suonio, H, Ligori, S, Lilje, P, Lindholm, V, Lloro, I, Maiorano, E, Mansutti, O, Marggraf, O, Markovic, K, Martinet, N, Marulli, F, Massey, R, Maurogordato, S, Medinaceli, E, Meneghetti, M, Merlin, E, Meylan, G, Moresco, M, Moscardini, L, Munari, E, Niemi, S, Padilla, C, Paltani, S, Pasian, F, Pettorino, V, Pires, S, Polenta, G, Poncet, M, Popa, L, Pozzetti, L, Raison, F, Rebolo, R, Renzi, A, Rhodes, J, Riccio, G, Romelli, E, Roncarelli, M, Saglia, R, Sapone, D, Sartoris, B, Schneider, P, Schrabback, T, Secroun, A, Seidel, G, Serrano, S, Sirignano, C, Sirri, G, Stanco, L, Starck, J, Tallada-Crespi, P, Taylor, A, Tereno, I, Toledo-Moreo, R, Torradeflot, F, Tutusaus, I, Valentijn, E, Valenziano, L, Vassallo, T, Veropalumbo, A, Wang, Y, Weller, J, Zacchei, A, Zamorani, G, Zoubian, J, Zucca, E, Biviano, A, Bozzo, E, Cerna, C, Colodro-Conde, C, Di Ferdinando, D, Mauri, N, Neissner, C, Sakr, Z, Scottez, V, Tenti, M, Viel, M, Wiesmann, M, Akrami, Y, Anselmi, S, Baccigalupi, C, Ballardini, M, Borlaff, A, Bruton, S, Burigana, C, Cabanac, R, Cappi, A, Carvalho, C, Castignani, G, Canas-Herrera, G, Chambers, K, Cooray, A, Coupon, J, Cucciati, O, Diaz-Sanchez, A, Davini, S, De La Torre, S, De Lucia, G, Desprez, G, Di Domizio, S, Dole, H, Escoffier, S, Ferrero, I, Finelli, F, Gabarra, L, Ganga, K, Garcia-Bellido, J, Giacomini, F, Gozaliasl, G, Hildebrandt, H, Ilic, S, Jimanez Munnoz, A, Kajava, J, Kansal, V, Kirkpatrick, C, Legrand, L, Loureiro, A, MacIas-Perez, J, Magliocchetti, M, Mainetti, G, Maoli, R, Martinelli, M, Martins, C, Matthew, S, Maturi, M, Maurin, L, Metcalf, R, Migliaccio, M, Monaco, P, Morgante, G, Nadathur, S, Patrizii, L, Pezzotta, A, Popa, V, Porciani, C, Potter, D, Pontinen, M, Reimberg, P, Rocci, P, Sanchez, A, Schaye, J, Schneider, A, Sefusatti, E, Sereno, M, Simon, P, Spurio Mancini, A, Stadel, J, Stanford, S, Steinwagner, J, Testera, G, Tewes, M, Teyssier, R, Toft, S, Tosi, S, Troja, A, Tucci, M, Valiviita, J, Vergani, D, Castro T., Borgani S., Costanzi M., Dakin J., Dolag K., Fumagalli A., Ragagnin A., Saro A., Le Brun A. M. C., Aghanim N., Amara A., Andreon S., Auricchio N., Baldi M., Bardelli S., Bodendorf C., Bonino D., Branchini E., Brescia M., Brinchmann J., Camera S., Capobianco V., Carbone C., Carretero J., Casas S., Castellano M., Cavuoti S., Cimatti A., Congedo G., Conselice C. J., Conversi L., Copin Y., Corcione L., Courbin F., Courtois H. M., Cropper M., Da Silva A., Degaudenzi H., Di Giorgio A. M., Dinis J., Dubath F., Duncan C. A. J., Dupac X., Farina M., Farrens S., Ferriol S., Frailis M., Franceschi E., Fumana M., Galeotta S., Gillis B., Giocoli C., Grazian A., Grupp F., Haugan S. V. H., Holmes W., Hormuth F., Hornstrup A., Jahnke K., Keihanen E., Kermiche S., Kiessling A., Kilbinger M., Kubik B., Kunz M., Kurki-Suonio H., Ligori S., Lilje P. B., Lindholm V., Lloro I., Maiorano E., Mansutti O., Marggraf O., Markovic K., Martinet N., Marulli F., Massey R., Maurogordato S., Medinaceli E., Meneghetti M., Merlin E., Meylan G., Moresco M., Moscardini L., Munari E., Niemi S. -M., Padilla C., Paltani S., Pasian F., Pettorino V., Pires S., Polenta G., Poncet M., Popa L. A., Pozzetti L., Raison F., Rebolo R., Renzi A., Rhodes J., Riccio G., Romelli E., Roncarelli M., Saglia R., Sapone D., Sartoris B., Schneider P., Schrabback T., Secroun A., Seidel G., Serrano S., Sirignano C., Sirri G., Stanco L., Starck J. -L., Tallada-Crespi P., Taylor A. N., Tereno I., Toledo-Moreo R., Torradeflot F., Tutusaus I., Valentijn E. A., Valenziano L., Vassallo T., Veropalumbo A., Wang Y., Weller J., Zacchei A., Zamorani G., Zoubian J., Zucca E., Biviano A., Bozzo E., Cerna C., Colodro-Conde C., Di Ferdinando D., Mauri N., Neissner C., Sakr Z., Scottez V., Tenti M., Viel M., Wiesmann M., Akrami Y., Anselmi S., Baccigalupi C., Ballardini M., Borlaff A. S., Bruton S., Burigana C., Cabanac R., Cappi A., Carvalho C. S., Castignani G., Canas-Herrera G., Chambers K. C., Cooray A. R., Coupon J., Cucciati O., Diaz-Sanchez A., Davini S., De La Torre S., De Lucia G., Desprez G., Di Domizio S., Dole H., Escoffier S., Ferrero I., Finelli F., Gabarra L., Ganga K., Garcia-Bellido J., Giacomini F., Gozaliasl G., Hildebrandt H., Ilic S., Jimanez Munnoz A., Kajava J. J. E., Kansal V., Kirkpatrick C. C., Legrand L., Loureiro A., MacIas-Perez J., Magliocchetti M., Mainetti G., Maoli R., Martinelli M., Martins C. J. A. P., Matthew S., Maturi M., Maurin L., Metcalf R. B., Migliaccio M., Monaco P., Morgante G., Nadathur S., Patrizii L., Pezzotta A., Popa V., Porciani C., Potter D., Pontinen M., Reimberg P., Rocci P. -F., Sanchez A. G., Schaye J., Schneider A., Sefusatti E., Sereno M., Simon P., Spurio Mancini A., Stadel J., Stanford S. A., Steinwagner J., Testera G., Tewes M., Teyssier R., Toft S., Tosi S., Troja A., Tucci M., Valiviita J., and Vergani D.

Abstract

The Euclid photometric survey of galaxy clusters stands as a powerful cosmological tool, with the capacity to significantly propel our understanding of the Universe. Despite being subdominant to dark matter and dark energy, the baryonic component of our Universe holds substantial influence over the structure and mass of galaxy clusters. This paper presents a novel model that can be used to precisely quantify the impact of baryons on the virial halo masses of galaxy clusters using the baryon fraction within a cluster as a proxy for their effect. Constructed on the premise of quasi-adiabaticity, the model includes two parameters, which are calibrated using non-radiative cosmological hydrodynamical simulations, and a single large-scale simulation from the Magneticum set, which includes the physical processes driving galaxy formation. As a main result of our analysis, we demonstrate that this model delivers a remarkable 1% relative accuracy in determining the virial dark matter-only equivalent mass of galaxy clusters starting from the corresponding total cluster mass and baryon fraction measured in hydrodynamical simulations. Furthermore, we demonstrate that this result is robust against changes in cosmological parameters and against variation of the numerical implementation of the subresolution physical processes included in the simulations. Our work substantiates previous claims regarding the impact of baryons on cluster cosmology studies. In particular, we show how neglecting these effects would lead to biased cosmological constraints for a Euclid-like cluster abundance analysis. Importantly, we demonstrate that uncertainties associated with our model arising from baryonic corrections to cluster masses are subdominant when compared to the precision with which mass-observable (i.e. richness) relations will be calibrated using Euclid and to our current understanding of the baryon fraction within galaxy clusters.

Published
2024

2. Galaxy clusters as astrophysical laboratories and probes of cosmology

Author

Le Brun, A. M. C., McCarthy, Ian, and Collins, Chris

Subjects
523.1, QB Astronomy
Abstract

Galaxy clusters are the most recent of cosmological structures to have formed by the present time in the currently favoured hierarchical scenario of structure formation and are widely regarded as powerful probes of cosmology and galaxy formation physics alike. Over the past few years, it became increasingly clear that precision cluster cosmology requires the development of detailed, realistic theoretical models of galaxy clusters and the confrontation of synthetic surveys generated using these models with observations. This motivates a campaign of large cosmological hydrodynamical simulations, with plausible 'sub-grid' prescriptions for the relevant galaxy formation physics. This thesis presents a new suite of large-volume cosmological hydrodynamical simulations called cosmo-OWLS. They form an extension to the Overwhelmingly Large Simulations (OWLS) project, and have been designed to help improve our understanding of cluster astrophysics and the non-linear structure formation, which are now the limiting systematic errors when using clusters as cosmological probes. Starting from identical initial conditions in either the Planck or WMAP7 cosmologies, the most important 'sub-grid' physics, including feedback from supernovae and active galactic nuclei (AGN) has been systematically varied. Via the production of synthetic surveys of the simulations and comparisons with observations, the realism of these state-of-the-art models was explored. At the same time, the simulations were shown to providea valuable tool for interpreting the observational data, as well as powerful means for testing commonly-employed methods for estimating, for example, cluster masses and determining survey selection functions, which are crucial for cluster cosmology. The properties of the simulated galaxy groups and clusters were first compared to a wide range of observational data,such as x-ray luminosity and temperature, gas mass fractions, entropy and density profiles, Sunyaev-Zel'dovich flux, I-band mass-to-light ratio, dominance of the brightest cluster galaxy, and central massive black hole (BH) masses, by producing synthetic observations and mimicking observational analysis techniques. These comparisons demonstrated that some AGN feedback models can produce a realistic population of galaxy groups and clusters, broadly reproducing both the median trend and, for the first time, the scatter in physical properties over approximately two decades in mass (¹³M⊙≲500≲10¹⁵M⊙) and 1.5 decades in radius (0.05≲500≲1.5). However, in other models, the AGN feedback is too violent (even though they reproduce the observed BH scaling relations), implying calibration of the models is required. The production of realistic populations of simulated groups and clusters, as well as models that bracket the observations, opens the door to the creation of synthetic surveys for assisting the astrophysical and cosmological interpretation of cluster surveys, as well as quantifying the impact of selection effects. A study of the scatter and evolution of the hot gas properties of the populations of galaxy groups and clusters, such as X-ray luminosity and temperature, gas mass and Sunyaev-Zel'dovich flux, as a function of the important non-gravitational physics of galaxy formation was then conducted. The median relations and the scatter about them are reasonably well-modelled by evolving broken power-laws. The non-radiative model and the model that neglects AGN feedback are consistent with having selfsimilar mass slopes, whereas the mass slopes of the AGN feedback models deviate significantly from the self-similar expectation. Self-similar evolution, which is widely adopted in current cosmological studies, was also found to break down when efficient feedback is included. The log-normal scatter varies mildly with mass, is relatively insensitive to non-gravitational physics, but shows a moderately strong decreasing trend with increasing redshift. The X-ray luminosity has a significantly larger scatter than all the other hot gas proxies examined. It is thus the poorest one, while the 'best' one is the mean X-ray temperature. Synthetic Sunyaev-Zel'dovich observations, generated using a 'multi-purpose' light cone software package developed during the thesis, were used to check the veracity of some of the results reported by the Planck collaboration at the end of 2012. Taken at face value, their results seem to favour a close to self-similar scaling relation between the Sunyaev-Zel'dovich flux and total mass all the way down to individual galaxy haloes, which is in contradiction with X-ray and absorption lines observation. The matched filter used by the Planck collaboration recovers fluxes which are biased increasingly high as feedback intensity increases. Two likely causes for the bias, i.e. confusion and deviations from the universal pressure profiles were investigated. Confusion was found to have a negligible effect when the signal is averaged over a large number of systems. Instead a shape mismatch (in terms of pressure profiles) was identified as being mostly responsible for the bias. Finally, synthetic X-ray observations, generated using a combination of the developed light cone software and of the XMM-Newton simulator and processed with the detection pipeline of the XXL survey, were used to start quantifying the selection function of the XXL survey. Preliminary results suggest that: (i) XXL is only able to find a very small fraction of the galaxy group population, (ii) the survey is best at finding lowmass clusters (14.0≲log₁₀[M₅₀₀(M⊙)]≲14.5) at z ≲ 0:75, and (iii) the detection pipeline misses a few very massive, very extended, nearby systems.

Published
2014
Full Text
View/download PDF

3. Euclid preparation: XXXIX. The effect of baryons on the halo mass function.

Author

Euclid Collaboration, Castro, T., Borgani, S., Costanzi, M., Dakin, J., Dolag, K., Fumagalli, A., Ragagnin, A., Saro, A., Le Brun, A. M. C., Aghanim, N., Amara, A., Andreon, S., Auricchio, N., Baldi, M., Bardelli, S., Bodendorf, C., Bonino, D., Branchini, E., and Brescia, M.

Subjects
GALAXY clusters, BARYONS, DARK energy, DARK matter, GALAXY formation, HYDRODYNAMICS
Abstract

The Euclid photometric survey of galaxy clusters stands as a powerful cosmological tool, with the capacity to significantly propel our understanding of the Universe. Despite being subdominant to dark matter and dark energy, the baryonic component of our Universe holds substantial influence over the structure and mass of galaxy clusters. This paper presents a novel model that can be used to precisely quantify the impact of baryons on the virial halo masses of galaxy clusters using the baryon fraction within a cluster as a proxy for their effect. Constructed on the premise of quasi-adiabaticity, the model includes two parameters, which are calibrated using non-radiative cosmological hydrodynamical simulations, and a single large-scale simulation from the Magneticum set, which includes the physical processes driving galaxy formation. As a main result of our analysis, we demonstrate that this model delivers a remarkable 1% relative accuracy in determining the virial dark matter-only equivalent mass of galaxy clusters starting from the corresponding total cluster mass and baryon fraction measured in hydrodynamical simulations. Furthermore, we demonstrate that this result is robust against changes in cosmological parameters and against variation of the numerical implementation of the subresolution physical processes included in the simulations. Our work substantiates previous claims regarding the impact of baryons on cluster cosmology studies. In particular, we show how neglecting these effects would lead to biased cosmological constraints for a Euclid-like cluster abundance analysis. Importantly, we demonstrate that uncertainties associated with our model arising from baryonic corrections to cluster masses are subdominant when compared to the precision with which mass–observable (i.e. richness) relations will be calibrated using Euclid and to our current understanding of the baryon fraction within galaxy clusters. [ABSTRACT FROM AUTHOR]

Published
2024
Full Text
View/download PDF

4. Internal dark matter structure of the most massive galaxy clusters since redshift 1

Author

Le Brun Amandine M. C. and Teyssier Romain

Subjects
Physics, QC1-999
Abstract

We investigate the evolution of the dark matter density profiles of the most massive galaxy clusters in the Universe. Using a ‘zoom-in’ procedure on a large suite of cosmological simulations of total comoving volume of 3 (h-1 Gpc)3, we study the 25 most massive clusters in four redshift slices from z ~ 1 to the present. The minimum mass is M500 > 5:5 × 1014 M⊙ at z = 1. Each system has more than two million particles within r500. Once scaled to the critical density at each redshift, the dark matter profiles within r500 are strikingly similar from z ~ 1 to the present day, exhibiting a low dispersion of 0.15 dex, and showing little evolution with redshift in the radial logarithmic slope and scatter. They have the running power law shape typical of the NFW-type profiles, and their inner structure, resolved to 3:8 h-1 comoving kpc at z = 1, shows no signs of converging to an asymptotic slope. Our results suggest that this type of profile is already in place at z > 1 in the highest-mass haloes in the Universe, and that it remains exceptionally robust to merging activity.

Published
2022
Full Text
View/download PDF

5. Euclid preparation: XXIV. Calibration of the halo mass function in Λ(ν)CDM cosmologies

Author

Castro, T., Fumagalli, A., Angulo, R. E., Bocquet, S., Borgani, S., Carbone, C., Dakin, J., Dolag, K., Giocoli, C., Monaco, P., Ragagnin, A., Saro, A., Sefusatti, E., Costanzi, M., Le Brun, A. M. C., Corasaniti, P. -S., Amara, A., Amendola, L., Baldi, M., Bender, R., Bodendorf, C., Branchini, E., Brescia, M., Camera, S., Capobianco, V., Carretero, J., Castellano, M., Cavuoti, S., Cimatti, A., Cledassou, R., Congedo, G., Conversi, L., Copin, Y., Corcione, L., Courbin, F., Da Silva, A., Degaudenzi, H., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Farrens, S., Ferriol, S., Fosalba, P., Frailis, M., Franceschi, E., Galeotta, S., Garilli, B., Gillis, B., Grazian, A., Grupp, F., Haugan, S. V. H., Hormuth, F., Hornstrup, A., Hudelot, P., Jahnke, K., Kermiche, S., Kitching, T., Kunz, M., Kurki-Suonio, H., Lilje, P. B., Lloro, I., Mansutti, O., Marggraf, O., Marulli, F., Meneghetti, M., Merlin, E., Meylan, G., Moresco, M., Moscardini, L., Munari, E., Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Pettorino, V., Pires, S., Polenta, G., Poncet, M., Popa, L., Pozzetti, L., Raison, F., Rebolo, R., Renzi, A., Rhodes, J., Riccio, G., Romelli, E., Saglia, R., Sapone, D., Sartoris, B., Schneider, P., Seidel, G., Sirri, G., Stanco, L., Tallada Crespi, P., Taylor, A. N., Toledo-Moreo, R., Torradeflot, F., Tutusaus, I., Valentijn, E. A., Valenziano, L., Vassallo, T., Wang, Y., Weller, J., Zacchei, A., Zamorani, G., Andreon, S., Bardelli, S., Bozzo, E., Colodro-Conde, C., Di Ferdinando, D., Farina, M., Gracia-Carpio, J., Lindholm, V., Neissner, C., Scottez, V., Tenti, M., Zucca, E., Baccigalupi, C., Balaguera-Antolinez, A., Ballardini, M., Bernardeau, F., Biviano, A., Blanchard, A., Borlaff, A. S., Burigana, C., Cabanac, R., Cappi, A., Carvalho, C. S., Casas, S., Castignani, G., Cooray, A., Coupon, J., Courtois, H. M., Davini, S., De Lucia, G., Desprez, G., Dole, H., Escartin, J. A., Escoffier, S., Finelli, F., Ganga, K., Garcia-Bellido, J., George, K., Gozaliasl, G., Hildebrandt, H., Hook, I., Ilic, S., Kansal, V., Keihanen, E., Kirkpatrick, C. C., Loureiro, A., Macias-Perez, J., Magliocchetti, M., Maoli, R., Marcin, S., Martinelli, M., Martinet, N., Matthew, S., Maturi, M., Metcalf, R. B., Morgante, G., Nadathur, S., Nucita, A. A., Patrizii, L., Peel, A., Popa, V., Porciani, C., Potter, D., Pourtsidou, A., Pontinen, M., Sanchez, A. G., Sakr, Z., Schirmer, M., Sereno, M., Spurio Mancini, A., Teyssier, R., Valiviita, J., Veropalumbo, A., and Viel, M.

Subjects
number, x-ray-clusters, Large-scale structure of Universe, Cosmology: theory, Galaxies: clusters: general, universal, initial conditions, NO, general, galaxies, evolution, code, clusters, statistical properties, theory, constraints, cosmology, n-body simulations
Abstract

Euclid's photometric galaxy cluster survey has the potential to be a very competitive cosmological probe. The main cosmological probe with observations of clusters is their number count, within which the halo mass function (HMF) is a key theoretical quantity. We present a new calibration of the analytic HMF, at the level of accuracy and precision required for the uncertainty in this quantity to be subdominant with respect to other sources of uncertainty in recovering cosmological parameters from Euclid cluster counts. Our model is calibrated against a suite of N-body simulations using a Bayesian approach taking into account systematic errors arising from numerical effects in the simulation. First, we test the convergence of HMF predictions from different N-body codes, by using initial conditions generated with different orders of Lagrangian Perturbation theory, and adopting different simulation box sizes and mass resolution. Then, we quantify the effect of using different halo finder algorithms, and how the resulting differences propagate to the cosmological constraints. In order to trace the violation of universality in the HMF, we also analyse simulations based on initial conditions characterised by scale-free power spectra with different spectral indexes, assuming both Einstein-de Sitter and standard λCDM expansion histories. Based on these results, we construct a fitting function for the HMF that we demonstrate to be sub-percent accurate in reproducing results from 9 different variants of the λCDM model including massive neutrinos cosmologies. The calibration systematic uncertainty is largely sub-dominant with respect to the expected precision of future mass-observation relations; with the only notable exception of the effect due to the halo finder, that could lead to biased cosmological inference.

Published
2023

7. Euclid preparation: XXIV. Calibration of the halo mass function in Λ(ν)CDM cosmologies.

Author

Euclid Collaboration, Castro, T., Fumagalli, A., Angulo, R. E., Bocquet, S., Borgani, S., Carbone, C., Dakin, J., Dolag, K., Giocoli, C., Monaco, P., Ragagnin, A., Saro, A., Sefusatti, E., Costanzi, M., Le Brun, A. M. C., Corasaniti, P.-S., Amara, A., Amendola, L., and Baldi, M.

Subjects
N-body simulations (Astronomy), PHYSICAL cosmology, LARGE scale structure (Astronomy), PERTURBATION theory, GALAXY clusters, CALIBRATION
Abstract

Euclid's photometric galaxy cluster survey has the potential to be a very competitive cosmological probe. The main cosmological probe with observations of clusters is their number count, within which the halo mass function (HMF) is a key theoretical quantity. We present a new calibration of the analytic HMF, at the level of accuracy and precision required for the uncertainty in this quantity to be subdominant with respect to other sources of uncertainty in recovering cosmological parameters from Euclid cluster counts. Our model is calibrated against a suite of N-body simulations using a Bayesian approach taking into account systematic errors arising from numerical effects in the simulation. First, we test the convergence of HMF predictions from different N-body codes, by using initial conditions generated with different orders of Lagrangian Perturbation theory, and adopting different simulation box sizes and mass resolution. Then, we quantify the effect of using different halo finder algorithms, and how the resulting differences propagate to the cosmological constraints. In order to trace the violation of universality in the HMF, we also analyse simulations based on initial conditions characterised by scale-free power spectra with different spectral indexes, assuming both Einstein–de Sitter and standard ΛCDM expansion histories. Based on these results, we construct a fitting function for the HMF that we demonstrate to be sub-percent accurate in reproducing results from 9 different variants of the ΛCDM model including massive neutrinos cosmologies. The calibration systematic uncertainty is largely sub-dominant with respect to the expected precision of future mass–observation relations; with the only notable exception of the effect due to the halo finder, that could lead to biased cosmological inference. [ABSTRACT FROM AUTHOR]

Published
2023
Full Text
View/download PDF

9. Sunyaev-Zel'dovich detection of the galaxy cluster Cl J1449+0856 at z=1.99: The pressure profile in uv space

Author

Gobat, R., Daddi, E., Coogan, R. T., Le Brun, A. M. C., Bournaud, F., Melin, J. -B., Riechers, D. A., Sargent, M., Valentino, F., Hwang, H. S., Finoguenov, A., Strazzullo, V., Gobat, R., Daddi, E., Coogan, R. T., Le Brun, A. M. C., Bournaud, F., Melin, J. -B., Riechers, D. A., Sargent, M., Valentino, F., Hwang, H. S., Finoguenov, A., and Strazzullo, V.

Abstract

We present Atacama Large Millimetre Array and Atacama Compact Array observations of the Sunyaev-Zel’dovich effect in the z = 2 galaxy cluster Cl J1449+0856, an X-ray-detected progenitor of typical massive clusters in the present day Universe. While in a cleaned but otherwise untouched 92 GHz map of this cluster little to no negative signal is visible, careful subtraction of known sub-millimetre emitters in the uv plane reveals a decrement at 5σ significance. The total signal is −190 ± 36 μJy, with a peak offset by 5″–9″ (∼50 kpc) from both the X-ray centroid and the still-forming brightest cluster galaxy. A comparison of the recovered uv-amplitude profile of the decrement with different pressure models allows us to derive total mass constraints consistent with the ∼6 × 1013M⊙ estimated from X-ray data. Moreover, we find no strong evidence for a deviation of the pressure profile with respect to local galaxy clusters, although a slight tension at small-to-intermediate spatial scales suggests a flattened central profile, opposite to that seen in a cool core and possibly an AGN-related effect. This analysis of the lowest mass single SZ detection so far illustrates the importance of interferometers when observing the SZ effect in high-redshift clusters, the cores of which cannot be considered quiescent, such that careful subtraction of galaxy emission is necessary.

Published
2019

12. Exploring cosmic origins with CORE : Survey requirements and mission design

Author

Delabrouille, J., de Bernardis, P., Bouchet, F. R., Achucarro, A., Ade, P. A. R., Allison, R., Arroja, F., Artal, E., Ashdown, M., Baccigalupi, C., Ballardini, M., Banday, A. J., Banerji, R., Barbosa, D., Bartlett, J., Bartolo, N., Basak, S., Baselmans, J. J. A., Basu, K., Battistelli, E. S., Battye, R., Baumann, D., Benoit, A., Bersanelli, M., Bideaud, A., Biesiada, M., Bilicki, M., Bonaldi, A., Bonato, M., Borrill, J., Boulanger, F., Brinckmann, T., Brown, M. L., Bucher, M., Burigana, C., Buzzelli, A., Cabass, G., Cai, Z. -Y., Calvo, M., Caputo, A., Carvalho, C. -S., Casas, F. J., Castellano, G., Catalano, A., Challinor, A., Charles, I., Chluba, J., Clements, D. L., Clesse, S., Colafrancesco, S., Colantoni, I., Contreras, D., Coppolecchia, A., Crook, M., D'Alessandro, G., D'Amico, G., da Silva, A., de Avillez, M., de Gasperis, G., De Petris, M., de Zotti, G., Danese, L., Desert, F. -X., Desjacques, V., Di Valentino, E., Dickinson, C., Diego, J. M., Doyle, S., Durrer, R., Dvorkin, C., Eriksen, H. K., Errard, J., Feeney, S., Fernandez-Cobos, R., FineIli, F., Forastieri, F., Franceschet, C., Fuskeland, U., Galli, S., Genova-Santos, R. T., Gerbino, Martina, Giusarma, E., Gomez, A., Gonzalez-Nuevo, J., Grandis, S., Greenslade, J., Goupy, J., Hagstotz, S., Hanany, S., Handley, W., Henrot-Versille, S., Hernandez-Monteagudo, C., Hervias-Caimapo, C., Hills, M., Hindmarsh, M., Hivon, E., Hoang, D. T., Hooper, D. C., Hu, B., Keihanen, E., Keskitalo, R., Kiiveri, K., Kisner, T., Kitching, T., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamagna, L., Lapi, A., Lasenby, A., Lattanzi, M., Le Brun, A. M. C., Lesgourgues, J., Liguori, M., Lindholm, V., Lizarraga, J., Luzzi, G., Macias-Perez, J. F., Maffei, B., Mandolesi, N., Martin, S., Martinez-Gonzalez, E., Martins, C. J. A. P., Masi, S., Massardi, M., Matarrese, S., Mazzotta, P., McCarthy, D., Melchiorri, A., Melin, J. -B., Mennella, A., Mohr, J., Molinari, D., Monfardini, A., Montier, L., Natoli, P., Negrello, M., Notari, A., Noviello, F., Oppizzi, F., O'Sullivan, C., Pagano, L., Paiella, A., Pajer, E., Paoletti, D., Paradiso, S., Partridge, R. B., Patanchon, G., Patil, S. P., Perdereau, O., Piacentini, F., Piat, M., Pisano, G., Polastri, L., Polenta, G., Pollo, A., Ponthieu, N., Poulin, V., Prele, D., Quartin, M., Ravenni, A., Remazeilles, M., Renzi, A., Ringeval, C., Roest, D., Roman, M., Roukema, B. F., Rubino-Martin, J. -A., Salvati, L., Scott, D., Serjeant, S., Signorelli, G., Starobinsky, A. A., Sunyaev, R., Tan, C. Y., Tartari, A., Tasinato, G., Toffolatti, L., Tomasi, M., Torrado, J., Tramonte, D., Trappe, N., Triqueneaux, S., Tristram, M., Trombetti, T., Tucci, M., Tucker, C., Urrestilla, J., Valiviita, J., Van de Weygaert, R., Van Tent, B., Vennin, V., Verde, L., Vermeulen, G., Vielva, P., Vittorio, N., Voisin, F., Wallis, C., Wandelt, B., Wehus, I. K., Weller, J., Young, K., Zannoni, M., Delabrouille, J., de Bernardis, P., Bouchet, F. R., Achucarro, A., Ade, P. A. R., Allison, R., Arroja, F., Artal, E., Ashdown, M., Baccigalupi, C., Ballardini, M., Banday, A. J., Banerji, R., Barbosa, D., Bartlett, J., Bartolo, N., Basak, S., Baselmans, J. J. A., Basu, K., Battistelli, E. S., Battye, R., Baumann, D., Benoit, A., Bersanelli, M., Bideaud, A., Biesiada, M., Bilicki, M., Bonaldi, A., Bonato, M., Borrill, J., Boulanger, F., Brinckmann, T., Brown, M. L., Bucher, M., Burigana, C., Buzzelli, A., Cabass, G., Cai, Z. -Y., Calvo, M., Caputo, A., Carvalho, C. -S., Casas, F. J., Castellano, G., Catalano, A., Challinor, A., Charles, I., Chluba, J., Clements, D. L., Clesse, S., Colafrancesco, S., Colantoni, I., Contreras, D., Coppolecchia, A., Crook, M., D'Alessandro, G., D'Amico, G., da Silva, A., de Avillez, M., de Gasperis, G., De Petris, M., de Zotti, G., Danese, L., Desert, F. -X., Desjacques, V., Di Valentino, E., Dickinson, C., Diego, J. M., Doyle, S., Durrer, R., Dvorkin, C., Eriksen, H. K., Errard, J., Feeney, S., Fernandez-Cobos, R., FineIli, F., Forastieri, F., Franceschet, C., Fuskeland, U., Galli, S., Genova-Santos, R. T., Gerbino, Martina, Giusarma, E., Gomez, A., Gonzalez-Nuevo, J., Grandis, S., Greenslade, J., Goupy, J., Hagstotz, S., Hanany, S., Handley, W., Henrot-Versille, S., Hernandez-Monteagudo, C., Hervias-Caimapo, C., Hills, M., Hindmarsh, M., Hivon, E., Hoang, D. T., Hooper, D. C., Hu, B., Keihanen, E., Keskitalo, R., Kiiveri, K., Kisner, T., Kitching, T., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamagna, L., Lapi, A., Lasenby, A., Lattanzi, M., Le Brun, A. M. C., Lesgourgues, J., Liguori, M., Lindholm, V., Lizarraga, J., Luzzi, G., Macias-Perez, J. F., Maffei, B., Mandolesi, N., Martin, S., Martinez-Gonzalez, E., Martins, C. J. A. P., Masi, S., Massardi, M., Matarrese, S., Mazzotta, P., McCarthy, D., Melchiorri, A., Melin, J. -B., Mennella, A., Mohr, J., Molinari, D., Monfardini, A., Montier, L., Natoli, P., Negrello, M., Notari, A., Noviello, F., Oppizzi, F., O'Sullivan, C., Pagano, L., Paiella, A., Pajer, E., Paoletti, D., Paradiso, S., Partridge, R. B., Patanchon, G., Patil, S. P., Perdereau, O., Piacentini, F., Piat, M., Pisano, G., Polastri, L., Polenta, G., Pollo, A., Ponthieu, N., Poulin, V., Prele, D., Quartin, M., Ravenni, A., Remazeilles, M., Renzi, A., Ringeval, C., Roest, D., Roman, M., Roukema, B. F., Rubino-Martin, J. -A., Salvati, L., Scott, D., Serjeant, S., Signorelli, G., Starobinsky, A. A., Sunyaev, R., Tan, C. Y., Tartari, A., Tasinato, G., Toffolatti, L., Tomasi, M., Torrado, J., Tramonte, D., Trappe, N., Triqueneaux, S., Tristram, M., Trombetti, T., Tucci, M., Tucker, C., Urrestilla, J., Valiviita, J., Van de Weygaert, R., Van Tent, B., Vennin, V., Verde, L., Vermeulen, G., Vielva, P., Vittorio, N., Voisin, F., Wallis, C., Wandelt, B., Wehus, I. K., Weller, J., Young, K., and Zannoni, M.

Abstract

Future observations of cosmic microwave background (CMB) polarisation have the potential to answer some of the most fundamental questions of modern physics and cosmology, including: what physical process gave birth to the Universe we see today? What are the dark matter and dark energy that seem to constitute 95% of the energy density of the Universe? Do we need extensions to the standard model of particle physics and fundamental interactions? Is the ACDM cosmological scenario correct, or are we missing an essential piece of the puzzle? In this paper, we list the requirements for a future CMB polarisation survey addressing these scientific objectives, and discuss the design drivers of the CORE space mission proposed to ESA in answer to the M5 call for a medium-sized mission. The rationale and options, and the methodologies used to assess the mission's performance, are of interest to other future CMB mission design studies. CORE has 19 frequency channels, distributed over a broad frequency range, spanning the 60-600 GHz interval, to control astrophysical foreground emission. The angular resolution ranges from 2' to 18', and the aggregate CMB sensitivity is about 2 mu K.arcmin. The observations are made with a single integrated focal-plane instrument, consisting of an array of 2100 cryogenically-cooled, linearly-polarised detectors at the focus of a 1.2-m aperture cross-Dragone telescope. The mission is designed to minimise all sources of systematic effects, which must be controlled so that no more than 10(-4) of the intensity leaks into polarisation maps, and no more than about 1% of E-type polarisation leaks into B-type modes. CORE observes the sky from a large Lissajous orbit around the Sun-Earth L2 point on an orbit that offers stable observing conditions and avoids contamination from sidelobe pick-up of stray radiation originating from the Sun, Earth, and Moon. The entire sky is observed repeatedly during four years of continuous scanning, with a combination of th

Published
2018
Full Text
View/download PDF

13. Internal dark matter structure of the most massive galaxy clusters

Author

Le Brun, A M C; https://orcid.org/0000-0002-0936-4594, Arnaud, M, Pratt, G W, Teyssier, R, Le Brun, A M C; https://orcid.org/0000-0002-0936-4594, Arnaud, M, Pratt, G W, and Teyssier, R

Abstract

We investigate the evolution of the dark matter density profiles of the most massive galaxy clusters in the Universe. Using a ‘zoom-in’ procedure on a large suite of cosmological simulations of total comoving volume of 3 (h − 1 Gpc)3, we study the 25 most massive clusters in four redshift slices from z ∼ 1 to the present. The minimum mass is M500 > 5.5 × 1014 M⊙ at z = 1. Each system has more than two million particles within r500. Once scaled to the critical density at each redshift, the dark matter profiles within r500 are strikingly similar from z ∼ 1 to the present day, exhibiting a low dispersion of 0.15 dex, and showing little evolution with redshift in the radial logarithmic slope and scatter. They have the running power-law shape typical of the Navarro–Frenk–White type profiles, and their inner structure, resolved to 3.8 h−1 comoving kpc at z = 1, shows no signs of converging to an asymptotic slope. Our results suggest that this type of profile is already in place at z > 1 in the highest-mass haloes in the Universe, and that it remains exceptionally robust to merging activity.

Published
2018

14. The XXL Survey

Author

Koulouridis, E., primary, Faccioli, L., additional, Le Brun, A. M. C., additional, Plionis, M., additional, McCarthy, I. G., additional, Pierre, M., additional, Akylas, A., additional, Georgantopoulos, I., additional, Paltani, S., additional, Lidman, C., additional, Fotopoulou, S., additional, Vignali, C., additional, Pacaud, F., additional, and Ranalli, P., additional

Published
2018
Full Text
View/download PDF

15. The XXL Survey

Author

Faccioli, L., primary, Pacaud, F., additional, Sauvageot, J.-L., additional, Pierre, M., additional, Chiappetti, L., additional, Clerc, N., additional, Gastaud, R., additional, Koulouridis, E., additional, Le Brun, A. M. C., additional, and Valotti, A., additional

Published
2018
Full Text
View/download PDF

23. The XXL Survey

Author

Eckert, D., primary, Ettori, S., additional, Coupon, J., additional, Gastaldello, F., additional, Pierre, M., additional, Melin, J.-B., additional, Le Brun, A. M. C., additional, McCarthy, I. G., additional, Adami, C., additional, Chiappetti, L., additional, Faccioli, L., additional, Giles, P., additional, Lavoie, S., additional, Lefèvre, J. P., additional, Lieu, M., additional, Mantz, A., additional, Maughan, B., additional, McGee, S., additional, Pacaud, F., additional, Paltani, S., additional, Sadibekova, T., additional, Smith, G. P., additional, and Ziparo, F., additional

Published
2016
Full Text
View/download PDF

24. The XXL Survey

Author

Pierre, M., primary, Pacaud, F., additional, Adami, C., additional, Alis, S., additional, Altieri, B., additional, Baran, N., additional, Benoist, C., additional, Birkinshaw, M., additional, Bongiorno, A., additional, Bremer, M. N., additional, Brusa, M., additional, Butler, A., additional, Ciliegi, P., additional, Chiappetti, L., additional, Clerc, N., additional, Corasaniti, P. S., additional, Coupon, J., additional, De Breuck, C., additional, Democles, J., additional, Desai, S., additional, Delhaize, J., additional, Devriendt, J., additional, Dubois, Y., additional, Eckert, D., additional, Elyiv, A., additional, Ettori, S., additional, Evrard, A., additional, Faccioli, L., additional, Farahi, A., additional, Ferrari, C., additional, Finet, F., additional, Fotopoulou, S., additional, Fourmanoit, N., additional, Gandhi, P., additional, Gastaldello, F., additional, Gastaud, R., additional, Georgantopoulos, I., additional, Giles, P., additional, Guennou, L., additional, Guglielmo, V., additional, Horellou, C., additional, Husband, K., additional, Huynh, M., additional, Iovino, A., additional, Kilbinger, M., additional, Koulouridis, E., additional, Lavoie, S., additional, Le Brun, A. M. C., additional, Le Fevre, J. P., additional, Lidman, C., additional, Lieu, M., additional, Lin, C. A., additional, Mantz, A., additional, Maughan, B. J., additional, Maurogordato, S., additional, McCarthy, I. G., additional, McGee, S., additional, Melin, J. B., additional, Melnyk, O., additional, Menanteau, F., additional, Novak, M., additional, Paltani, S., additional, Plionis, M., additional, Poggianti, B. M., additional, Pomarede, D., additional, Pompei, E., additional, Ponman, T. J., additional, Ramos-Ceja, M. E., additional, Ranalli, P., additional, Rapetti, D., additional, Raychaudury, S., additional, Reiprich, T. H., additional, Rottgering, H., additional, Rozo, E., additional, Rykoff, E., additional, Sadibekova, T., additional, Santos, J., additional, Sauvageot, J. L., additional, Schimd, C., additional, Sereno, M., additional, Smith, G. P., additional, Smolčić, V., additional, Snowden, S., additional, Spergel, D., additional, Stanford, S., additional, Surdej, J., additional, Valageas, P., additional, Valotti, A., additional, Valtchanov, I., additional, Vignali, C., additional, Willis, J., additional, and Ziparo, F., additional

Published
2016
Full Text
View/download PDF

26. The BAHAMAS project: calibrated hydrodynamical simulations for large-scale structure cosmology.

Author

McCarthy, Ian G., Schaye, Joop, Bird, Simeon, and Le Brun, Amandine M. C.

Subjects
DARK matter, DARK energy, CALIBRATION, HYDRODYNAMICS, METAPHYSICAL cosmology
Abstract

The evolution of the large-scale distribution of matter is sensitive to a variety of fundamental parameters that characterize the dark matter, dark energy, and other aspects of our cosmological framework. Since the majority of the mass density is in the form of dark matter that cannot be directly observed, to do cosmology with large-scale structure, one must use observable (baryonic) quantities that trace the underlying matter distribution in a (hopefully) predictable way. However, recent numerical studies have demonstrated that the mapping between observable and total mass, as well as the total mass itself, are sensitive to unresolved feedback processes associated with galaxy formation, motivating explicit calibration of the feedback efficiencies. Here, we construct a new suite of large-volume cosmological hydrodynamical simulations (called BAHAMAS, for BAryons and HAloes of MAssive Systems), where subgrid models of stellar and active galactic nucleus feedback have been calibrated to reproduce the present-day galaxy stellar mass function and the hot gas mass fractions of groups and clusters in order to ensure the effects of feedback on the overall matter distribution are broadly correct. We show that the calibrated simulations reproduce an unprecedentedly wide range of properties of massive systems, including the various observed mappings between galaxies, hot gas, total mass, and black holes, and represent a significant advance in our ability to mitigate the primary systematic uncertainty in most present large-scale structure tests. [ABSTRACT FROM AUTHOR]

Published
2017
Full Text
View/download PDF

30. XIII. Baryon content of the bright cluster sample.

Author

Eckert, D., Ettori, S., Coupon, J., Gastaldello, F., Pierre, M., Melin, J. -B., Le Brun, A. M. C., McCarthy, I. G., Adami, C., Chiappetti, L., Faccioli, L., Giles, P., Lavoie, S., Lefèvre, J. P., Lieu, M., Mantz, A., Maughan, B., McGee, S., Pacaud, F., and Paltani, S.

Subjects
BARYONS, GALAXY clusters, SUPERCLUSTERS, UNIVERSE, METAPHYSICAL cosmology
Abstract

Traditionally, galaxy clusters have been expected to retain all the material accreted since their formation epoch. For this reason, their matter content should be representative of the Universe as a whole, and thus their baryon fraction should be close to the Universal baryon fraction b= m. We make use of the sample of the 100 brightest galaxy clusters discovered in the XXL Survey to investigate the fraction of baryons in the form of hot gas and stars in the cluster population. Since it spans a wide range of mass (1013-1015 M⊙) and redshift (0:05-1:1) and benefits from a large set of multiwavelength data, the XXL-100-GC sample is ideal for measuring the global baryon budget of massive halos. We measure the gas masses of the detected halos and use a mass-temperature relation directly calibrated using weak-lensing measurements for a subset of XXL clusters to estimate the halo mass. We find that the weak-lensing calibrated gas fraction of XXL-100-GC clusters is substantially lower than was found in previous studies using hydrostatic masses. Our best-fit relation between gas fraction and mass reads fgas;500 = 0:055+0:007 -0:006 M500=1014 M⊙ 0:21+0:11 -0:10. The baryon budget of galaxy clusters therefore falls short of the Universal baryon fraction by about a factor of two at r500;MT. Our measurements require a hydrostatic bias 1-b = MX=MWL = 0:72+0:08 -0:07 to match the gas fraction obtained using lensing and hydrostatic equilibrium, which holds independently of the instrument considered. Comparing our gas fraction measurements with the expectations from numerical simulations, we find that our results favour an extreme feedback scheme in which a significant fraction of the baryons are expelled from the cores of halos. This model is, however, in contrast with the thermodynamical properties of observed halos, which might suggest that weak-lensing masses are overestimated. In light of these results, we note that a mass bias 1 - b = 0:58 as required to reconcile Planck cosmic microwave background and cluster counts should translate into an even lower baryon fraction, which poses a major challenge to our current understanding of galaxy clusters. [ABSTRACT FROM AUTHOR]

Published
2016
Full Text
View/download PDF

31. Exploring Cosmic Origins with CORE: Cluster Science

Author

Melin, J. -B, Bonaldi, A., Remazeilles, M., Hagstotz, S., Diego, J. M., Hernández-Monteagudo, C., Génova-Santos, R. T., Luzzi, G., Martins, C. J. A. P., Grandis, S., Mohr, J. J., Bartlett, J. G., Delabrouille, J., Ferraro, S., Tramonte, D., Rubiño-Martín, J. A., Macìas-Pérez, J. F., Achúcarro, A., Ade, P., Allison, R., Ashdown, M., Ballardini, M., Banday, A. J., Banerji, R., Bartolo, N., Basak, S., Baselmans, J., Basu, K., Battye, R. A., Baumann, D., Bersanelli, M., Bonato, M., Borrill, J., Bouchet, F., Boulanger, F., Brinckmann, T., Bucher, M., Burigana, C., Buzzelli, A., Cai, Z. -Y, Calvo, M., Carvalho, C. S., Castellano, M. G., Challinor, A., Chluba, J., Clesse, S., Colafrancesco, S., Colantoni, I., Coppolecchia, A., Crook, M., D Alessandro, G., Bernardis, P., Gasperis, G., Petris, M., Zotti, G., Di Valentino, E., Errard, J., Feeney, S. M., Fernández-Cobos, R., Finelli, F., Forastieri, F., Galli, S., Gerbino, M., González-Nuevo, J., Greenslade, J., Hanany, S., Handley, W., Hervias-Caimapo, C., Hills, M., Hivon, E., Kiiveri, K., Kisner, T., Kitching, T., Kunz, M., Kurki-Suonio, H., Lamagna, L., Lasenby, A., Lattanzi, M., Le Brun, A. M. C., Lesgourgues, J., Lewis, A., Liguori, M., Lindholm, V., Lopez-Caniego, M., Maffei, B., Martinez-Gonzalez, E., Masi, S., Mccarthy, D., Melchiorri, A., Molinari, D., Monfardini, A., Natoli, P., Negrello, M., Notari, A., Paiella, A., Paoletti, D., Patanchon, G., Piat, M., Pisano, G., Polastri, L., Polenta, G., Pollo, A., Poulin, V., Quartin, M., Roman, M., Salvati, L., Tartari, A., Tomasi, M., Trappe, N., Triqueneaux, S., Trombetti, T., Carole Tucker, Väliviita, J., Weygaert, R., Tent, B., Vennin, V., Vielva, P., Vittorio, N., Weller, J., Young, K., Zannoni, M., and Core, For The Collaboration

32. The XXL Survey

Author

Koulouridis, E., Faccioli, L., Le Brun, A. M. C., Plionis, M., McCarthy, I. G., Pierre, M., Akylas, A., Georgantopoulos, I., Paltani, S., Lidman, C., Fotopoulou, S., Vignali, C., Pacaud, F., and Ranalli, P.

Full Text
View/download PDF

33. Euclid preparation:XXIV. Calibration of the halo mass function in Λ(ν)CDM cosmologies

Author

Euclid Collaboration, Castro, T., Fumagalli, A., Angulo, R. E., Bocquet, S., Borgani, S., Carbone, C., Dakin, J., Dolag, K., Giocoli, C., Monaco, P., Ragagnin, A., Saro, A., Sefusatti, E., Costanzi, M., Brun, A. M. C. Le, Corasaniti, P. -S., Amara, A., Amendola, L., Baldi, M., Bender, R., Bodendorf, C., Branchini, E., Brescia, M., Camera, S., Capobianco, V., Carretero, J., Castellano, M., Cavuoti, S., Cimatti, A., Cledassou, R., Congedo, G., Conversi, L., Copin, Y., Corcione, L., Courbin, F., Da Silva, A., Degaudenzi, H., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Farrens, S., Ferriol, S., Fosalba, P., Frailis, M., Franceschi, E., Galeotta, S., Garilli, B., Gillis, B., Grazian, A., Grupp, F., Haugan, S. V. H., Hormuth, F., Hornstrup, A., Hudelot, P., Jahnke, K., Kermiche, S., Kitching, T., Kunz, M., Kurki-Suonio, H., Lilje, P. B., Lloro, I., Mansutti, O., Marggraf, O., Marulli, F., Meneghetti, M., Merlin, E., Meylan, G., Moresco, M., Moscardini, L., Munari, E., Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Pettorino, V., Pires, S., Polenta, G., Poncet, M., Popa, L., Pozzetti, L., Raison, F., Rebolo, R., Renzi, A., Rhodes, J., Riccio, G., Romelli, E., Saglia, R., Sapone, D., Sartoris, B., Schneider, P., Seidel, G., Sirri, G., Stanco, L., Crespí, P. Tallada, Taylor, A. N., Toledo-Moreo, R., Torradeflot, F., Tutusaus, I., Valentijn, E. A., Valenziano, L., Vassallo, T., Wang, Y., Weller, J., Zacchei, A., Zamorani, G., Andreon, S., Bardelli, S., Bozzo, E., Colodro-Conde, C., Di Ferdinando, D., Farina, M., Graciá-Carpio, J., Lindholm, V., Neissner, C., Scottez, V., Tenti, M., Zucca, E., Baccigalupi, C., Balaguera-Antolínez, A., Ballardini, M., Bernardeau, F., Biviano, A., Blanchard, A., Borlaff, A. S., Burigana, C., Cabanac, R., Cappi, A., Carvalho, C. S., Casas, S., Castignani, G., Cooray, A., Coupon, J., Courtois, H. M., Davini, S., De Lucia, G., Desprez, G., Dole, H., Escartin, J. A., Escoffier, S., Finelli, F., Ganga, K., Garcia-Bellido, J., George, K., Gozaliasl, G., Hildebrandt, H., Hook, I., Ilić, S., Kansal, V., Keihanen, E., Kirkpatrick, C. C., Loureiro, A., Macias-Perez, J., Magliocchetti, M., Maoli, R., Marcin, S., Martinelli, M., Martinet, N., Matthew, S., Maturi, M., Metcalf, R. B., Morgante, G., Nadathur, S., Nucita, A. A., Patrizii, L., Peel, A., Popa, V., Porciani, C., Potter, D., Pourtsidou, A., Pöntinen, M., Sánchez, A. G., Sakr, Z., Schirmer, M., Sereno, M., Mancini, A. Spurio, Teyssier, R., Valiviita, J., Veropalumbo, A., Viel, M., Euclid, Collaboration, Castro, T., Fumagalli, A., Angulo, R. E., Bocquet, S., Borgani, S., Carbone, C., Dakin, J., Dolag, K., Giocoli, C., Monaco, P., Ragagnin, A., Saro, A., Sefusatti, E., Costanzi, M., Le Brun, A. M. C., Corasaniti, P. -S., Amara, A., Amendola, L., Baldi, M., Bender, R., Bodendorf, C., Branchini, E., Brescia, M., Camera, S., Capobianco, V., Carretero, J., Castellano, M., Cavuoti, S., Cimatti, A., Cledassou, R., Congedo, G., Conversi, L., Copin, Y., Corcione, L., Courbin, F., Da Silva, A., Degaudenzi, H., Douspis, M., Dubath, F., Duncan, C. A. J., Dupac, X., Farrens, S., Ferriol, S., Fosalba, P., Frailis, M., Franceschi, E., Galeotta, S., Garilli, B., Gillis, B., Grazian, A., Grupp, F., Haugan, S. V. H., Hormuth, F., Hornstrup, A., Hudelot, P., Jahnke, K., Kermiche, S., Kitching, T., Kunz, M., Kurki-Suonio, H., Lilje, P. B., Lloro, I., Mansutti, O., Marggraf, O., Marulli, F., Meneghetti, M., Merlin, E., Meylan, G., Moresco, M., Moscardini, L., Munari, E., Niemi, S. M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Pettorino, V., Pires, S., Polenta, G., Poncet, M., Popa, L., Pozzetti, L., Raison, F., Rebolo, R., Renzi, A., Rhodes, J., Riccio, G., Romelli, E., Saglia, R., Sapone, D., Sartoris, B., Schneider, P., Seidel, G., Sirri, G., Stanco, L., Tallada Crespí, P., Taylor, A. N., Toledo-Moreo, R., Torradeflot, F., Tutusaus, I., Valentijn, E. A., Valenziano, L., Vassallo, T., Wang, Y., Weller, J., Zacchei, A., Zamorani, G., Andreon, S., Bardelli, S., Bozzo, E., Colodro-Conde, C., Di Ferdinando, D., Farina, M., Graciá-Carpio, J., Lindholm, V., Neissner, C., Scottez, V., Tenti, M., Zucca, E., Baccigalupi, C., Balaguera-Antolínez, A., Ballardini, M., Bernardeau, F., Biviano, A., Blanchard, A., Borlaff, A. S., Burigana, C., Cabanac, R., Cappi, A., Carvalho, C. S., Casas, S., Castignani, G., Cooray, A., Coupon, J., Courtois, H. M., Davini, S., De Lucia, G., Desprez, G., Dole, H., Escartin, J. A., Escoffier, S., Finelli, F., Ganga, K., Garcia-Bellido, J., George, K., Gozaliasl, G., Hildebrandt, H., Hook, I., Ilić, S., Kansal, V., Keihanen, E., Kirkpatrick, C. C., Loureiro, A., Macias-Perez, J., Magliocchetti, M., Maoli, R., Marcin, S., Martinelli, M., Martinet, N., Matthew, S., Maturi, M., Metcalf, R. B., Morgante, G., Nadathur, S., Nucita, A. A., Patrizii, L., Peel, A., Popa, V., Porciani, C., Potter, D., Pourtsidou, A., Pöntinen, M., Sánchez, A. G., Sakr, Z., Schirmer, M., Sereno, M., Spurio Mancini, A., Teyssier, R., Valiviita, J., Veropalumbo, A., and Viel, M.

Subjects
Astrophysic, cosmology theory, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Large-scale structure of Universe, galaxies clusters general, theory [Cosmology], FOS: Physical sciences, clusters: general [Galaxies], Cosmology and Nongalactic Astrophysics
Abstract

Euclid's photometric galaxy cluster survey has the potential to be a very competitive cosmological probe. The main cosmological probe with observations of clusters is their number count, within which the halo mass function (HMF) is a key theoretical quantity. We present a new calibration of the analytic HMF, at the level of accuracy and precision required for the uncertainty in this quantity to be subdominant with respect to other sources of uncertainty in recovering cosmological parameters from Euclid cluster counts. Our model is calibrated against a suite of N-body simulations using a Bayesian approach taking into account systematic errors arising from numerical effects in the simulation. First, we test the convergence of HMF predictions from different N-body codes, by using initial conditions generated with different orders of Lagrangian Perturbation theory, and adopting different simulation box sizes and mass resolution. Then, we quantify the effect of using different halo-finder algorithms, and how the resulting differences propagate to the cosmological constraints. In order to trace the violation of universality in the HMF, we also analyse simulations based on initial conditions characterised by scale-free power spectra with different spectral indexes, assuming both Einstein--de Sitter and standard $Λ$CDM expansion histories. Based on these results, we construct a fitting function for the HMF that we demonstrate to be sub-percent accurate in reproducing results from 9 different variants of the $Λ$CDM model including massive neutrinos cosmologies. The calibration systematic uncertainty is largely sub-dominant with respect to the expected precision of future mass-observation relations; with the only notable exception of the effect due to the halo finder, that could lead to biased cosmological inference., 25 pages, 21 figures, 5 tables, 3 appendixes; v2 matches published version

Published
2023
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results