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Galaxy-induced transformation of dark matter haloes: Transformations of CDM haloes
Open accessAbstract
We use N-body/gasdynamical cosmological simulations to examine the effect of the assembly of a central galaxy on the shape and mass profile of its surrounding dark matter halo. Two series of simulations are compared; one that follows only the evolution of the dark matter component of individual haloes in the proper Λcold dark matter (ΛCDM) cosmological context, and a second series where a baryonic component is added and followed hydrodynamically. The simulations with baryons include radiative cooling but neglect the formation of stars and their feedback. The efficient, unimpeded cooling that results leads most baryons to collect at the halo centre in a centrifugally supported disc which, due to angular momentum losses, is too small and too massive when compared with typical spiral galaxies. This admittedly unrealistic model allows us, nevertheless, to gauge the maximum effect that galaxies may have in transforming their surrounding dark haloes. We find, in agreement with earlier work, that the shape of the halo becomes more axisymmetric: post galaxy assembly, haloes are transformed from triaxial into essentially oblate systems, with well-aligned isopotential contours of roughly constant flattening (〈c/a〉∼ 0.85). Haloes always contract as a result of galaxy assembly, but the effect is substantially less pronounced than predicted by the traditional ‘adiabatic-contraction’ hypothesis. The reduced contraction helps to reconcile ΛCDM haloes with constraints on the dark matter content inside the solar circle and should alleviate the longstanding difficulty of matching simultaneously the scaling properties of galaxy discs and the galaxy luminosity function. The halo contraction we report is also less pronounced than found in earlier simulations, a disagreement which suggests that halo contraction is not solely a function of the initial and final distribution of baryons. Not only how much baryonic mass has been deposited at the centre of a halo matters, but also the mode of its deposition. Although simple formulae might work in particular cases where galaxies form nearly adiabatically, in general it might prove impossible to predict the halo response to galaxy formation without a detailed understanding of a galaxy's detailed assembly history.
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“Nonetheless, individual haloes can deviate from the mean prediction since the size of the contraction is weakly dependent on the assembly history of the system (e.g. Abadi et al. 2010; Artale et al. 2019).”
From The milky way total mass profile as inferred from Gaia DR2 (2020) · cites this paper as Abadi et al. 2010
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“This simplification is unlikely to affect our results since the baryonic distribution leads to a roughly spherical DM distribution in the inner regions, i.e. for r ≲ 20 kpc , which is the region where the best quality rotation curve data exists”
From The milky way total mass profile as inferred from Gaia DR2 (2020) · cites this paper as Abadi et al. 2010
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“Other simpler adiabatic contraction approximations, such as those used by Blumenthal et al. (1986) and Gnedin et al. (2004), tend systematically to under- or overpredict the halo contraction (e.g. Abadi et al. 2010; Duffy et al. 2010; Pedrosa et al. 2010; Dutton et al. 2016; Artale et al. 2019).”
From The milky way total mass profile as inferred from Gaia DR2 (2020) · cites this paper as Abadi et al. 2010
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Citations
Cites
Spergel, D. N., Verde, L., Peiris, H. V., Komatsu, E., Nolta, M. R., Bennett, C. L., Halpern, M., Hinshaw, G., Jarosik, N., Kogut, A., et al. (2003) · The Astrophysical Journal Supplement Series · doi:10.1086/377226 · Cited by 10,976 · cited 1×
“We adopt cosmological parameters consistent with the combined analysis of the 2dfGRS (Colless et al., 2001) and the first-year WMAP data (Spergel et al., 2003): a present day value of the Hubble constant of H0 = 70 km/s/Mpc; a scalefree initial density perturbation spectrum with no tilt and…”
MethodA Universal Density Profile from Hierarchical Clustering
Navarro, J. F., Frenk, C. S., & White, S. D. M. (1997) · The Astrophysical Journal · doi:10.1086/304888 · Cited by 9,917 · cited 4×
“The DMO mass profile is shown by the thick red solid curve and, as expected, it is well approximated by the NFW (Navarro et al., 1996b, 1997) formula (thin solid line).”
BackgroundMethodInfluentialSelf-citationThe Structure of Cold Dark Matter Halos
Navarro, J. F., Frenk, C. S., & White, S. D. M. (1996) · The Astrophysical Journal · doi:10.1086/177173 · Cited by 8,544 · cited 4×
“The DMO mass profile is shown by the thick red solid curve and, as expected, it is well approximated by the NFW (Navarro et al., 1996b, 1997) formula (thin solid line).”
BackgroundMethodInfluentialSelf-citationA Universal Density Profile from Hierarchical ClusteringPreprint
Navarro, J. F., Frenk, C. S., & White, S. D. M. (1996) · Cited by 6,275
Self-citationSimulations of the formation, evolution and clustering of galaxies and quasars
Springel, V., White, S. D. M., Jenkins, A. R., Frenk, C. S., Yoshida, N., Gao, L., Navarro, J. F., Thacker, R. J., Croton, D., Helly, J. C., et al. (2005) · Nature · doi:10.1038/nature03597 · Cited by 5,060 · cited 1×
“Each dot in this panel correspond to an NFW halo with concentration drawn at random from the mass-concentration relation (including scatter) derived by Neto et al. (2007) from the Millennium Simulation (Springel et al., 2005).”
MethodSelf-citationCroton, D. J., Springel, V., White, S. D. M., Lucia, G. D., Frenk, C. S., Gao, L., Jenkins, A., Kauffmann, G., Navarro, J. F., & Yoshida, N. (2005) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2005.09675.x · Cited by 3,686 · cited 2×
“…formation have adopted this formulation in order to link the (observed) dynamical properties of luminous galaxies to the (predicted) properties of the dark halos that surround them (see, e.g., Mo et al., 1998; Cole et al., 2000; Dutton et al., 2005; Croton et al., 2006; Somerville et al., 2008).”
BackgroundSelf-citationStatistical Properties of X‐Ray Clusters: Analytic and Numerical Comparisons
Bryan, G. L., & Norman, M. L. (1998) · The Astrophysical Journal · doi:10.1086/305262 · Cited by 2,372 · cited 1×
“The virial density contrast, ∆vir(z) is given by ∆vir(z) = 18π 2 + 82f(z) − 39f(z)2, where f(z) = [Ω0(1 + z)3/(Ω0(1 + z)3 + ΩΛ))] − 1 and Ω0 = ΩCDM + Ωb(Bryan & Norman, 1998).”
The 2dF Galaxy Redshift Survey: spectra and redshifts
Colless, M., Dalton, G., Maddox, S., Sutherland, W. J., Norberg, P., Cole, S., Bland‐Hawthorn, J., Bridges, T. J., Cannon, R., Collins, C. A., et al. (2001) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2001.04902.x · Cited by 2,368 · cited 1×
“We adopt cosmological parameters consistent with the combined analysis of the 2dfGRS (Colless et al., 2001) and the first-year WMAP data (Spergel et al., 2003): a present day value of the Hubble constant of H0 = 70 km/s/Mpc; a scalefree initial density perturbation spectrum with no tilt and…”
MethodThe formation of galactic discs
Mo, H. J., Mao, S., & White, S. D. M. (1998) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.1998.01227.x · Cited by 2,166 · cited 2×
“…formation have adopted this formulation in order to link the (observed) dynamical properties of luminous galaxies to the (predicted) properties of the dark halos that surround them (see, e.g., Mo et al., 1998; Cole et al., 2000; Dutton et al., 2005; Croton et al., 2006; Somerville et al., 2008).”
BackgroundCole, S., Lacey, C. G., Baugh, C. M., & Frenk, C. S. (2002) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2000.03879.x · Cited by 1,952
Research works printed but not linked: 1
- Ma, 2004, Phys. Rev. Lett., 93, 1301
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Items 101–200 of 238
Dark matter contraction and stellar-mass-to-light ratio gradients in massive early-type galaxies
Oldham, L., & Auger, M. W. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty065 · Cited by 54
Zhu, K., Lu, S., Cappellari, M., Li, R., Mao, S., & Gao, L. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad1299 · Cited by 54
The Milky Way’s plane of satellites is consistent with ΛCDM
Sawala, T., Cautun, M., Frenk, C. S., Helly, J. C., Jasche, J., Jenkins, A. R., Johansson, P. H., Lavaux, G., McAlpine, S., & Schaller, M. (2022) · Nature Astronomy · doi:10.1038/s41550-022-01856-z · Cited by 65
SELF-SIMILAR DYNAMICAL RELAXATION OF DARK MATTER HALOS IN AN EXPANDING UNIVERSE
Lapi, A., & Cavaliere, A. G. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/743/2/127 · Cited by 50
“However, recent numerical experiments (see Abadi et al. 2010) suggest that the classic treatment of adiabatic contraction is likely to be extreme; actually, in the inner region the contraction may be inefficient and the density slope hardly modified.”
BackgroundnIFTy galaxy cluster simulations – IV. Quantifying the influence of baryons on halo properties
Cui, W., Power, C., Knebe, A., Kay, S. T., Sembolini, F., Elahi, P. J., Yepes, G., Pearce, F. R., Cunnama, D. C., Beck, A. M., et al. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw603 · Cited by 49
“…but an influence on their suite of host haloes, which drives the DM halo to become more spherical especially at the central regions (see also Debattista et al. 2008; Tissera et al. 2010; Abadi et al. 2010; Bryan et al. 2013; Tenneti et al. 2014; Butsky et al. 2015; Tenneti et al. 2015, etc.).”
BackgroundConstraints on the shapes of galaxy dark matter haloes from weak gravitational lensing
van Uitert, E., Hoekstra, H., Schrabback, T., Gilbank, D. G., Gladders, M. D., & Yee, H. K. C. (2012) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201219295/pdf · Cited by 49
Bringing the Galaxy's dark halo to life
Piffl, T., Penoyre, Z., & Binney, J. J. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv938 · Cited by 48
“This is the reverse of what is usually found with N-body simulations, in which generally less contraction is observed than Blumenthal et al. predict (Abadi et al. 2010; Gnedin et al. 2010).”
Resolving the disc–halo degeneracy – I: a look at NGC 628
Aniyan, S., Freeman, K. C., Arnaboldi, M., Gerhard, O., Coccato, L., Fabricius, M., Kuijken, K. H., Merrifield, M. R., & Ponomareva, A. A. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty310 · Cited by 48
Blaña, M., Gerhard, O., Wegg, C., Portail, M., Opitsch, M., Saglia, R. P., Fabricius, M., Erwin, P., & Bender, R. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty2311 · Cited by 48
“2 kpcDM 200=0.97 × 1010 M , as more recent hydrodynamical cosmological simulations show less contraction (Abadi et al. 2010, implemented with ν=0.4 prescription from Dutton et al. 2011).”
BackgroundInfluentialBaryonic imprints on DM haloes: population statistics from dwarf galaxies to galaxy clusters
Anbajagane, D., EVRARD, A. E., & Farahi, A. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab3177 · Cited by 48
Cattaneo, A., Blaizot, J., Devriendt, J., Mamon, G. A., Tollet, É., Dekel, A., Guiderdoni, B., Kucukbas, M., & Thob, A. C. R. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx1597 · Cited by 47
“Cole et al. (2000)’s model for adiabatic contraction (based on Blumenthal et al. 1986) is partially responsible for this offset because it overestimates the phenomenon (Gnedin et al. 2004; Abadi et al. 2010) and thus the DM mass with the disc.”
BackgroundLi, R., Shu, Y., & Wang, J. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty1813 · Cited by 47
“The former processes lead to a higher baryon densities and steepen the inner density profile (e.g., Gustafsson et al. 2006; Abadi et al. 2010; Velliscig et al. 2014), while the latter processes tend to heat the gas and soften the density profile (e.g., Martizzi et al. 2012; Dubois et al. 2013;…”
BackgroundWang, Y., Vogelsberger, M., Xu, D., Mao, S., Springel, V., Li, H., Barnes, D. J., Hernquist, L., Pillepich, A., Marinacci, F., et al. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz3348 · Cited by 46
“…of gas cooling in hydrodynamical simulations favored less contraction than the prediction of the adiabatic contraction scheme, but still found halos to be contracted and the dark matter profiles in the inner region to be steeper than the standard NFW profile (Gnedin et al. 2004; Abadi et al. 2010).”
BackgroundResultCan multistate dark matter annihilation explain the high-energy cosmic ray lepton anomalies?
Cirelli, M., & Cline, J. M. (2010) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.82.023503 · Cited by 47
Tan, C. Y., Shajib, A. J., Birrer, S., Sonnenfeld, A., Treu, T., Wells, P., Williams, D., Buckley‐Geer, E., Drlica-Wagner, A., & Frieman, J. A. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae884 · Cited by 46
Shajib, A. J., Vernardos, G., Collett, T. E., Motta, V., Sluse, D., Williams, L. L. R., Saha, P., Birrer, S., Spiniello, C., & Treu, T. (2024) · Space Science Reviews · doi:10.1007/s11214-024-01105-x · Cited by 46
“The simulations of Gnedin et al. (2004) point to ν ∼ 0.8, and those of Abadi et al. (2010) to ν ∼ 0.4 (Dutton and Treu, 2014).”
BackgroundInfluentialGrillo, C. (2012) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/747/1/l15 · Cited by 46
“This is in line with the recent findings of high-resolution hydrodynamical simulations which include radiative cooling and feedback processes (e.g., Abadi et al. 2010; Tissera et al. 2010; Duffy et al. 2010).”
ResultON THE DISCREPANCY BETWEEN THEORETICAL AND X-RAY CONCENTRATION-MASS RELATIONS FOR GALAXY CLUSTERS
Rasia, E., Borgani, S., Ettori, S., Mazzotta, P., & Meneghetti, M. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/776/1/39 · Cited by 45
Testing adiabatic contraction of dark matter in fossil group candidates
Démoclès, J., Pratt, G. W., Pierini, D., Arnaud, M., Zibetti, S., & D’Onghia, E. (2010) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201014328 · Cited by 45
“We choose this prescription among others (Blumenthal et al. 1986; Abadi et al. 2009) for consistency with previous investigations (Zappacosta et al. 2006; Humphrey et al. 2006; Gastaldello et al. 2007).”
ResultZasov, A. V., Saburova, A. S., Khoperskov, A. V., & Александрович, Х. С. (2016) · Physics-Uspekhi · doi:10.3367/ufne.2016.03.037751 · Cited by 45
A halo expansion technique for approximating simulated dark matter haloes
Lowing, B., Jenkins, A. R., Eke, V. R., & Frenk, C. S. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.19222.x · Cited by 43
“For example, if a model of a baryon disk is introduced, the associated reduction of the triaxiality at the centre of the dark halo (Debattista et al. 2008; Abadi et al. 2010; Bett et al. 2010) cannot be included in the expansion approximation.”
BackgroundDark matter annihilation radiation in hydrodynamic simulations of Milky Way haloes
Schaller, M., Frenk, C. S., Theuns, T., Calore, F., Bertone, G., Bozorgnia, N., Crain, R. A., Fattahi, A., Navarro, J. F., Sawala, T., et al. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv2667 · Cited by 42
“We can summarize our findings as follows: (i) As seen in previous simulations (e.g. Dubinski 1994; Abadi et al. 2010; Bryan et al. 2013), the central concentration of baryons significantly reduces the asphericity typical of haloes in dark matteronly simulations.”
MethodSelf-citationTHE ElIXr GALAXY SURVEY. II. BARYONS AND DARK MATTER IN AN ISOLATED ELLIPTICAL GALAXY
Humphrey, P. J., Buote, D. A., O’Sullivan, E., & Ponman, T. J. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/755/2/166 · Cited by 40
“A theoretical modification to the DM profile is expected to arise from adiabatic contraction (Blumenthal et al. 1986; Gnedin et al. 2007; Abadi et al. 2010), which causes the halo to become cuspier due to the gravitational influence of the baryons.”
BackgroundGalactic tides and the shape and orientation of dwarf galaxy satellites
Barber, C., Starkenburg, E., Navarro, J. F., & McConnachie, A. W. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu2494 · Cited by 40
“…(e.g., Navarro, Eke & Frenk 1996; Read & Gilmore 2005; Mashchenko, Wadsley & Couchman 2008; Knebe et al. 2010; Kazantzidis, Abadi & Navarro 2010; Abadi et al. 2010; Peñarrubia et al. 2012; Pontzen & Governato 2012; Zolotov et al. 2012; Garrison-Kimmel et al. 2013; Arraki et al. 2014; Brooks &…”
BackgroundSelf-citationSchuldt, S., Chirivì, G., Suyu, S. H., Yıldırım, A., Sonnenfeld, A., Halkola, A., & Lewis, G. F. (2019) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201935042 · Cited by 40
“…condense toward the center (e.g., Blumenthal et al. 1986; Gnedin et al. 2004; Sellwood & McGaugh 2005; Gustafsson et al. 2006; Pedrosa et al. 2009; Abadi et al. 2010; Sommer-Larsen & Limousin 2010), active galactic nuclei (AGNs) feedback (e.g., Peirani et al. 2008, 2017; Martizzi et al. 2013; Li…”
BackgroundThe diversity of rotation curves of simulated galaxies with cusps and cores
Roper, F. A., Oman, K. A., Frenk, C. S., Benítez-Llambay, A., Navarro, J. F., & Santos-Santos, I. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad549 · Cited by 40
Self-citationnIFTY galaxy cluster simulations – III. The similarity and diversity of galaxies and subhaloes
Elahi, P. J., Knebe, A., Pearce, F. R., Power, C., Yepes, G., Cui, W., Cunnama, D. C., Kay, S. T., Sembolini, F., Beck, A. M., et al. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw338 · Cited by 39
“…centrally concentrating material and forming galaxies, although this can be MNRAS 458, 1096–1116 (2016) at U niversity of C am bridge on D ecem ber 9, 2016 http://m nras.oxfordjournals.org/ nloaded from completely counteracted by feedback physics (e.g. Abadi et al. 2010; di Cintio et al. 2011).”
BackgroundNIHAO – XXIII. Dark matter density shaped by black hole feedback
Macciò, A. V., Crespi, S., Blank, M., & Kang, X. (2020) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1093/mnrasl/slaa058 · Cited by 43
Dynamical models of elliptical galaxies – II. M87 and its globular clusters
Agnello, A., Evans, N. W., Romanowsky, A. J., & Brodie, J. P. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu960 · Cited by 38
“2012; Hilz et al. 2013), the interplay between luminous and dark components over different timescales (Blumenthal et al. 1986; Abadi et al. 2010; Zubovas & King 2012), as well as the initial conditions (Stiavelli & Bertin 1987; Nipoti et al. 2012; Remus et al. 2013) all leave imprints on the final…”
BackgroundOn the Density profile slope of Clusters of GalaxiesPreprint
Popolo, A. D. (2014) · Cited by 37
Stellar discs in Aquarius dark matter haloes
DeBuhr, J., Ma, C., & White, S. D. M. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.21910.x · Cited by 36
“The presence of a disk in simulations has been shown to wash out the prolateness of the halo and make the inner haloes either more spherical or oblate (e.g., Dubinski 1994; Berentzen & Shlosman 2006; Debattista et al. 2008; Kazantzidis et al. 2010; Tissera et al. 2010; Abadi et al. 2010).”
BackgroundTo be or not to be oblate: the shape of the dark matter halo in polar ring galaxies
Александрович, Х. С., Moiseev, A. V., Khoperskov, A. V., & Saburova, A. S. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu692 · Cited by 36
“…shape is supported, by numerous cosmological simulations which demonstrate the formation of DM halos with different spatial scales a 6= b 6= c at almost any condition (Dubinski & Carlberg 1991; Jing & Suto 2002; Bailin & Steinmetz 2005; Allgood et al. 2006; Kuhlen et al. 2007; Abadi et al. 2010).”
BackgroundDynamical models of elliptical galaxies – I. Simple methods
Agnello, A., Evans, N. W., & Romanowsky, A. J. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu959 · Cited by 36
“When baryonic effects are included in the simulations, these can transfer energy between the luminous and dark components and alter the DM profile through different channels (Abadi et al. 2010; Di Cintio et al. 2013).”
BackgroundIndirect dark matter detection for flattened dwarf galaxies
Sanders, J. L., Evans, N. W., Geringer-Sameth, A., & Dehnen, W. (2016) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.94.063521 · Cited by 34
Prediction of Supernova Rates in Known Galaxy–Galaxy Strong-lens Systems
Shu, Y., Bolton, A. S., Mao, S., Kang, X., Li, G., & Soraisam, M. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aad5ea · Cited by 32
“…important clues to galaxy formation and evolution (e.g., Gnedin et al. 2004; Nipoti et al. 2004; Gustafsson et al. 2006; Romano-Díaz et al. 2008; Abadi et al. 2010; Duffy et al. 2010; Governato et al. 2010; Bolton et al. 2012a; Martizzi et al. 2012; Dubois et al. 2013; Velliscig et al. 2014;…”
BackgroundEmami, R., Genel, S., Hernquist, L., Alcock, C. R., Bose, S., Weinberger, R., Vogelsberger, M., Marinacci, F., Loeb, A., Torrey, P., et al. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/abf147 · Cited by 36
“For example, Abadi et al. (2010) investigated the radial dependence of halo shapes inside their hydrodynamical simulations and found s= a/c∼ 0.85.”
BackgroundInfluentialThe radial acceleration relation in a ΛCDM universe
Paranjape, A., & Sheth, R. K. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab2141 · Cited by 30
The impact of galactic feedback on the shapes of dark matter haloes
Chua, K. T. E., Vogelsberger, M., Pillepich, A., & Hernquist, L. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac1897 · Cited by 30
Dutton, A. A., Macciò, A. V., Stinson, G. S., Gutcke, T. A., Penzo, C., & Buck, T. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv1755 · Cited by 29
“The magenta lines show the formula from Abadi et al. (2010), rf/ri = 1− 0.3(Mi/Mf − 1) 2, which approximately describes our forced quenching simulations at z = 0 (lower right panel).”
BackgroundResultInfluentialON PHYSICAL SCALES OF DARK MATTER HALOS
Zemp, M. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/792/2/124 · Cited by 28
“12 ter distribution on large scales (e.g. Dubinski 1994; Kazantzidis et al. 2004; Stanek et al. 2009; Abadi et al. 2010; Duffy et al. 2010; Kazantzidis et al. 2010; Pedrosa et al. 2010; Tissera et al. 2010; Cui et al. 2012; Zemp et al. 2012; Bryan et al. 2013).”
BackgroundBars in dark-matter-dominated dwarf galaxy discs
Marasco, A., Oman, K. A., Navarro, J. F., Frenk, C. S., & Oosterloo, T. A. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty354 · Cited by 27
Self-citationA two-point correlation function for Galactic halo stars
Cooper, A. P., Cole, S., Frenk, C. S., & Helmi, A. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.19401.x · Cited by 26
Collett, T. E., Buckley-Geer, E., Lin, H., Bacon, D., Nichol, R. C., Nord, B., Morice-Atkinson, X., Amara, A., Birrer, S., Kuropatkin, N., et al. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa76e6 · Cited by 27
“…and contract, dragging DM inwards and increasing the central density, but supernovae, active galactic nuclei and dynamical heating can inject energy into the interstellar medium, causing the halo to expand (Pontzen & Governato 2012; Teyssier et al. 2011; Abadi et al. 2010; Laporte et al. 2012).”
BackgroundExciting dark matter in the Galactic Center
Chen, F., Cline, J. M., Fradette, A., Frey, A. R., & Rabideau, C. (2010) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.81.043523 · Cited by 26
On the relevance of chaos for halo stars in the solar neighbourhood
Maffione, N. P., Gómez, F. A., Cincotta, P. M., Giordano, C. M., Cooper, A. P., & O’Shea, B. W. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv1778 · Cited by 25
Velocity-dependent J-factors for annihilation radiation from cosmological simulations
Erin Board, Bozorgnia, N., Strigari, L. E., Grand, R. J. J., Fattahi, A., Frenk, C. S., Marinacci, F., Navarro, J. F., & Oman, K. A. (2021) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2021/04/070 · Cited by 25
Self-citationMilky Way satellite velocities reveal the dark matter power spectrum at small scales
Esteban, I., Peter, A. H. G., & Kim, S. Y. (2024) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.110.123013 · Cited by 25
Mauro, M. D., Stref, M., & Calore, F. (2022) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.106.123032 · Cited by 24
Schuldt, S., Chirivì, G., Suyu, S. H., Yıldırım, A., Sonnenfeld, A., Halkola, A., & Lewis, G. F. (2019) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201935042/pdf · Cited by 24
Lacroix, T., Núñez-Castiñeyra, A., Stref, M., Lavalle, J., & Nezri, E. (2020) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2020/10/031 · Cited by 23
“baryonic cooling processes, in agreement with other studies [107–112].”
ResultChandra X-ray galaxy clusters at z < 1.4: Constraints on the inner slope of the density profiles
Babyk, Y. V., Popolo, A. D., & Vavilova, I. B. (2014) · Astronomy Reports · doi:10.1134/s1063772914090017 · Cited by 23
Around the Way: Testing ΛCDM with Milky Way Stellar Stream Constraints
Dai, B., Robertson, B. E., & Madau, P. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aabb06 · Cited by 22
“The baryonic dissipation alters the dark matter halo shape from prolate to an oblate halo aligned with the disk, consistent with previous studies (e.g., Kazantzidis et al. 2004; Gustafsson et al. 2006; Abadi et al. 2010).”
BackgroundResultThe orbital phase space of contracted dark matter haloes
Callingham, T. M., Cautun, M., Deason, A. J., Frenk, C. S., Grand, R. J. J., Marinacci, F., & Pakmor, R. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa1089 · Cited by 23
“…on many factors including the mass of the central galaxy, its assembly history and the orbital distribution of DM particles (e.g. Gnedin et al. 2004; Abadi et al. 2010; Duffy et al. 2010; Schaller et al. 2016; Dutton et al. 2016; Artale et al. 2019; Barnes & White 1984a; Blumenthal et al. 1986).”
BackgroundResultChua, K. T. E., Dibert, K. R., Vogelsberger, M., & Zavala, J. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa3315 · Cited by 21
The GALAH survey: accreted stars also inhabit the Spite plateau
Simpson, J. D., Martell, S. L., Buder, S., Bland‐Hawthorn, J., Casey, A. R., Silva, G. M. D., D’Orazi, V., Freeman, K. C., Hayden, M., Kos, J., et al. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab2012 · Cited by 24
The response of dark matter haloes to gas ejection: CuspCore II
Li, Z., Dekel, A., Mandelker, N., Freundlich, J., & François, T. L. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac3233 · Cited by 21
Effects of baryon mass loss on profiles of large galactic dark matter haloes
Ragone-Figueroa, C., Granato, G. L., & Abadi, M. G. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.21113.x · Cited by 21
“The dependence on the timescale of the mass loss is c© 0000 RAS, MNRAS 000, 000–000 weak.”
BackgroundMethodInfluentialSelf-citationMultiwavelength mock galaxy catalogues of the low-redshift Universe
Paranjape, A., Choudhury, T. R., & Sheth, R. K. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab722 · Cited by 21
“Here we describe the technique for calculating the response of the dark matter profile to presence of baryonic matter through an approximate conservation of angular momentum (Barnes & White 1984; Blumenthal et al. 1986; Gnedin et al. 2004; Abadi et al. 2010; Teyssier et al. 2011; ST15).”
MethodThe Cusp–Core Problem in Gas-Poor Dwarf Spheroidal Galaxies
Boldrini, P. (2021) · Galaxies · doi:10.3390/galaxies10010005 · Cited by 28
“we use the algorithm from [41] adapted to Enzo as de-”
BackgroundMethodDavis, A., Khochfar, S., & Vecchia, C. D. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu1201 · Cited by 20
“Abadi et al. (2010) also found similar results; their haloes with active merger histories were less concentrated than haloes with smooth accretion.”
BackgroundResultDark matter response to galaxy assembly history
Artale, M. C., Pedrosa, S. E., Tissera, P. B., Cataldi, P., & Di Cintio, A. (2019) · Astronomy & Astrophysics · doi:10.1051/0004-6361/201834096 · Cited by 19
“3.6, at z = 0 the models proposed by Abadi et al. (2010) and Pedrosa et al. (2010) are in good agreement with the mass distribution of the SPH haloes.”
BackgroundMethodResultInfluentialThe Effect of Adiabatic Compression on Dark Matter Halos and the Radial Acceleration Relation
Li, P., McGaugh, S., Lelli, F., Tian, Y., Schombert, J. M., & Ko, C. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac52aa · Cited by 19
“They numerically computed the profiles of the stabilized DM halos, finding that initial NFW halos experienced adiabatic contraction due to baryonic compression (see also Abadi et al. 2010).”
MethodDark matter response to galaxy assembly history
Artale, M. C., Pedrosa, S., Tissera, P. B., Cataldi, P., & Cintio, A. D. (2019) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201834096/pdf · Cited by 20
Properties of barred spiral discs in hydrodynamical cosmological simulations
Goz, D., Monaco, P., Murante, G., & Curir, A. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu2557 · Cited by 19
“…from prolate to oblate in the inner part was already studied in isolated systems by Dubinski (1994), Debattistaet al. (2008), in cosmological environment by Kazantzidis et al. (2004), Tissera et al. (2010), Abadi et al. (2010) and more recently by Zemp et al. (2012), Bryan et al. (2013).”
BackgroundA steep slope and small scatter for the high-mass end of the L–σ relation atz∼ 0.55
Montero-Dorta, A. D., Shu, Y., Bolton, A. S., Brownstein, J. R., & Weiner, B. J. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv2871 · Cited by 18
“Gas cooling permits baryons to condense in the central regions of galaxies, and therefore it is believed to make the mass distribution more centrally concentrated (e.g. Gnedin et al. 2004; Gustafsson et al. 2006; Abadi et al. 2010; Velliscig et al. 2014).”
BackgroundConstraining dark matter properties with gamma-rays from the Galactic Center with Fermi–LAT
Bernal, N., & Palomares-Ruiz, S. (2011) · Nuclear Physics B · doi:10.1016/j.nuclphysb.2011.12.016 · Cited by 18
“In principle, it is not yet clear how baryons would affect the profile of the Milky Way, but the picture could be significantly changed [170–180].”
BackgroundCooper, A. P., Cole, S., Frenk, C. S., Bret, T. L., & Pontzen, A. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx955 · Cited by 18
“…orbital evolution of a particular satellite may be differ- ent in simulations from the same initial conditions with and without hydrodynamics, because the host halo potential can also change shape and concentration in response to the motion of baryons (e.g. Abadi et al. 2010; Binney & Piffl 2015).”
BackgroundDark Matter in Elliptical GalaxiesPreprint
Buote, D. A., & Humphrey, P. J. (2016) · Cited by 18
On the relevance of chaos for halo stars in the solar neighbourhood II
Maffione, N. P., Gómez, F. A., Cincotta, P. M., Giordano, C., Grand, R. J. J., Marinacci, F., Pakmor, R., Simpson, C. M., Springel, V., & Frenk, C. S. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty1297 · Cited by 17
“…are taken into account, DM haloes present a significantly more oblate distribution in the inner regions (for instance: Dubinski 1994; Gustafsson, Fairbairn & Sommer-Larsen 2006; Debattista et al. 2008; Abadi et al. 2010), thus enhancing the asymmetry within the inner and the outer galactic regions.”
BackgroundConstraining the Milky Way dark matter density profile with gamma-rays with Fermi-LAT
Bernal, N., & Palomares-Ruiz, S. (2012) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2012/01/006 · Cited by 17
“Moreover, these simulations do not usually include the effect of baryons, which could significantly change the picture [167–175].”
BackgroundA catalogue of Galactic GEMS: Globular cluster Extra-tidal Mock Stars
Grondin, S., Webb, J. J., Lane, J., Speagle, J. S., & Leigh, N. W. C. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae203 · Cited by 19
Deciphering baryonic feedback with galaxy clusters
To, C., Pandey, S., Krause, E., Dalal, N., Anbajagane, D., & Weinberg, D. H. (2024) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2024/07/037 · Cited by 15
He, J., Wang, W., Li, Z., Han, J., Rodríguez-Gómez, V., Zhao, D., Meng, X. T., Jing, Y., Shao, S., Shi, R., et al. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad8882 · Cited by 16
Humphrey, P. J., Buote, D. A., Brighenti, F., Gebhardt, K., & Mathews, W. G. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sts651 · Cited by 15
“…gravitationally, in particular the interplay between adiabatic contraction and dynamical friction (e.g. Blumenthal et al. 1986; Gnedin et al. 2004; El-Zant et al. 2004; Humphrey et al. 2006; Dutton et al. 2007; Gnedin et al. 2007; Abadi et al. 2010; Napolitano et al. 2010; Macciò et al. 2012).”
BackgroundA two-point correlation function for Galactic halo starsPreprint
Cooper, A. P., Cole, S., Frenk, C. S., & Helmi, A. (2011) · Cited by 19
The Dark Matter Haloes of Chandra X-ray Galaxy Clusters and Baryons EffectPreprint
Babyk, I., Vavilova, I. B., & Popolo, A. D. (2012) · arXiv (Cornell University) · doi:10.13140/rg.2.1.3448.9360 · Cited by 15
Impact of tidal environment on galaxy clustering in GAMA
Alam, S., Paranjape, A., & Peacock, J. A. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad3423 · Cited by 14
Baryonic imprints on DM haloes: the concentration–mass relation in the C amels simulations
Shao, M. (., Anbajagane, D., & Chang, C. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad1620 · Cited by 13
Bolamperti, A., Grillo, C., Cañameras, R., Suyu, S. H., & Christensen, L. (2023) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202244680 · Cited by 12
Diagnostics of baryonic cooling in lensing galaxies
Leier, D., Ferreras, I., & Saha, P. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.21173.x · Cited by 12
“At present, it is not clear whether or not cinit differed from cfinal (e.g. Abadi et al. 2010) and it is conceivable that the impact of AC on dark matter profiles might be overestimated by commonly used recipes for baryonic cooling.”
BackgroundThe Parallelism between Galaxy Clusters and Early-type Galaxies. I. The Light and Mass Profiles
D’Onofrio, M., Sciarratta, M., Cariddi, S., Marziani, P., & Chiosi, C. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab1134 · Cited by 12
Interaction of the dark-matter cusp with the baryonic component in disk galaxies
Александрович, Х. С., Shustov, B. M., & Khoperskov, A. V. (2012) · Astronomy Reports · doi:10.1134/s1063772912090041 · Cited by 11
Baryon-driven decontraction in Milky Way-mass haloes
Moreno, V. J. F., Benítez-Llambay, A., Cole, S., & Frenk, C. S. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac312 · Cited by 13
Zasov, A. V., Saburova, A. S., Khoperskov, A. V., & Александрович, Х. С. (2016) · Uspekhi Fizicheskih Nauk · doi:10.3367/ufnr.2016.03.037751 · Cited by 11
Extremely flat haloes and the shape of the galaxy
Evans, N. W., & Bowden, A. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu1113 · Cited by 10
“The ratio of short to long axis isq ≈ 0.8− 0.9 though with some scatter (see e.g., Abadi et al. 2010; Deasonet al. 2011; Zemp et al. 2012).”
BackgroundInfluentialMiXDM: Cosmic Ray Signals from Multiple States of Dark MatterPreprint
Cholis, I., & Weiner, N. (2009) · arXiv (Cornell University) · doi:10.48550/arxiv.0911.4954 · Cited by 10
“due to the naturally large scattering cross section from the light mediator [8]. Some recent simulations involving baryons show a significant increase of the velocity dispersion in the galactic center [33, 34, 35, 36, 37], which can alleviate these constraints [38, 39], possibly opening the possibility of double-excita…”
BackgroundNIHAO – XXVIII. Collateral effects of AGN on dark matter concentration and stellar kinematics
Waterval, S., Elgamal, S., Nori, M., Pasquato, M., Macciò, A. V., Blank, M., Dixon, K. L., Kang, X., & Ibrayev, T. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac1191 · Cited by 9
Probing the shape of the Milky Way dark matter halo with hypervelocity stars: A new method
Gallo, A., Ostorero, L., Chakrabarty, S. S., Ebagezio, S., & Diaferio, A. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202142679 · Cited by 11
Discy dwarf disruption and the shape of the Galactic halo
Gibbons, S. L. J., Belokurov, V. A., Erkal, D., & Evans, N. W. (2016) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1093/mnrasl/slw018 · Cited by 9
“…history (e.g. Allgood et al. 2006); the interplay between Dark Matter (DM) and baryons (see e.g. Kazantzidis et al. 2004; Debattista et al. 2008; Abadi et al. 2010); the nature of the DM particle (e.g. Dubinski & Carlberg 1991; Davé et al. 2001; Mayer et al. 2002); and even the Cosmology…”
BackgroundMASS ESTIMATORS FOR FLATTENED DISPERSION-SUPPORTED GALAXIES
Sanders, J. L., & Evans, N. W. (2016) · The Astrophysical Journal Letters · doi:10.3847/2041-8205/830/2/l26 · Cited by 9
“This represents a limiting case as simulations indicate the dark matter distribution is in fact rounder than the light (Abadi et al. 2010; Zemp et al. 2012) due to baryonic feedback effects, particularly for the more massive dSphs.”
BackgroundThe coevolution of the velocity and mass functions of galaxies and dark haloes
Chae, K. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.18181.x · Cited by 9
Baryonification: an alternative to hydrodynamical simulations for cosmological studies
Schneider, A., Kovač, M., Bucko, J., Nicola, A., Reischke, R., Giri, S., Teyssier, R., Tröster, T., Réfrégier, A., Schaller, M., et al. (2025) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2025/12/043 · Cited by 14
“68 and n = 1 (Gnedin04-model), [61] proposed α = 0 .”
Cosmology in the non-linear regime: the small scale miracle
Lacasa, F. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202037512 · Cited by 8
Diagnostics of baryonic cooling in lensing galaxies
Leier, D., Ferreras, I., & Saha, P. (2012) · Zurich Open Repository and Archive (University of Zurich) · doi:10.5167/uzh-70271 · Cited by 8
The quasi-adiabatic relaxation of haloes in the IllustrisTNG and EAGLE cosmological simulations
Velmani, P., & Paranjape, A. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad297 · Cited by 12
Angular momentum evolution in dark-matter haloes
Book, L. G., Brooks, A. M., Peter, A. H. G., Benson, A. J., & Governato, F. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.17824.x · Cited by 8
“…(Treu & Koopmans 2004; Gavazzi et al. 2007; Schulz et al. 2009; Simon et al. 2005; de Blok et al. 2008; Kuzio de Naray et al. 2008; Dutton & van den Bosch 2009; Gustafsson et al. 2006; Romano-Dı́az et al. 2008, 2009; Abadi et al. 2009; Governato et al. 2010; Tissera et al. 2009; Duffy et al. 2010).”
BackgroundThe Correlation Luminosity-Velocity Dispersion of Galaxies and Active Galactic Nuclei
D’Onofrio, M., Marziani, P., Chiosi, C., & Negrete, C. A. (2024) · Universe · doi:10.3390/universe10060254 · Cited by 7
Galan, A., Caminha, G. B., Knollmüller, J., Roth, J., & Suyu, S. H. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202449876 · Cited by 7
Chae, K., Kravtsov, A. V., Frieman, J. A., & Bernardi, M. (2012) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2012/11/004 · Cited by 7
Dark Matter Halos: The Dynamical Basis of Effective Empirical Models
Lapi, A., & Cavaliere, A. G. (2010) · Advances in Astronomy · doi:10.1155/2011/903429 · Cited by 7
“On the other hand, some steepening of the inner density profile may be induced by any ‘adiabatic’ contraction of the diffuse star-forming baryons into a disc-like structure, as proposed by Blumenthal et al. (1986) and Mo et al. (1998) but currently under scrutiny, see Abadi et al. (2010).”
Metadata
- Authors
- Abadi, M. G., Navarro, J. F., Fardal, M., Babul, A., & Steinmetz, M.
- Affiliations
- Consejo Nacional de Investigaciones Científicas y Técnicas (AR)
- University of Victoria (CA)
- University of Massachusetts Amherst (US)
- Leibniz Institute for Astrophysics Potsdam (DE)
- Corresponding author
- Abadi, Mario G.
- Venue
- Monthly Notices of the Royal Astronomical Society
- Publisher
- Oxford University Press (OUP)
- Published
- 2010-08-19
- Volume
- 407
- Issue
- 1
- Pages
- 435-446
- ISSN
- 0035-8711 (ISSN-L)
- OpenAlex
- W2159553024
- Cited by
- 237
- References
- 69
- Citations by year
- 2026: 1 · 2025: 7 · 2024: 15 · 2023: 12 · 2022: 14 · 2021: 11 · 2020: 10 · 2019: 14 · 2018: 12 · 2017: 6 · 2016: 17 · 2015: 11 · 2014: 20 · 2013: 13 · 2012: 31
- FWCI
- 14.30
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- Monthly Notices of the Royal Astronomical Society (publishedVersion)
- Conicet (publishedVersion, cc-by-nc-sa)
- arXiv (Cornell University) (submittedVersion)
- HighWire Press Open Archive (submittedVersion)
- arXiv (Cornell University)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Cosmology and Gravitation Theories
- Physical Sciences › Physics and Astronomy › Nuclear and High Energy Physics › Dark Matter and Cosmic Phenomena
- Keywords
- dark matter halos, galaxy formation, halo shape, halo mass profiles, radiative cooling, adiabatic contraction, galaxy assembly, luminosity function
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