000227032 001__ 227032
000227032 005__ 20181203024624.0
000227032 0247_ $$2doi$$a10.1093/mnras/stw2251
000227032 022__ $$a0035-8711
000227032 02470 $$2ISI$$a000393568200034
000227032 037__ $$aARTICLE
000227032 245__ $$aThe extraordinary amount of substructure in the Hubble Frontier Fields cluster Abell 2744
000227032 260__ $$aOxford$$bOxford Univ Press$$c2016
000227032 269__ $$a2016
000227032 300__ $$a18
000227032 336__ $$aJournal Articles
000227032 520__ $$aWe present a joint optical/X-ray analysis of the massive galaxy cluster Abell 2744 (z = 0.308). Our strong- and weak-lensing analysis within the central region of the cluster, i.e. at R < 1 Mpc from the brightest cluster galaxy, reveals eight substructures, including the main core. All of these dark matter haloes are detected with a significance of at least 5 sigma and feature masses ranging from 0.5 to 1.4 x 10(14) M-circle dot within R < 150 kpc. Merten et al. and Medezinski et al. substructures are also detected by us. We measure a slightly higher mass for the main core component than reported previously and attribute the discrepancy to the inclusion of our tightly constrained strong-lensing mass model built on Hubble Frontier Fields data. X-ray data obtained by XMM-Newton reveal four remnant cores, one of them a new detection, and three shocks. Unlike Merten et al., we find all cores to have both dark and luminous counterparts. A comparison with clusters of similar mass in the Millennium XXL simulations yields no objects with as many massive substructures as observed in Abell 2744, confirming that Abell 2744 is an extreme system. We stress that these properties still do not constitute a challenge to Lambda cold dark matter, as caveats apply to both the simulation and the observations: for instance, the projected mass measurements from gravitational lensing and the limited resolution of the subhaloes finders. We discuss implications of Abell 2744 for the plausibility of different dark matter candidates and, finally, measure a new upper limit on the self-interaction cross-section of dark matter of sigma(DM) < 1.28 cm(2) g(-1) (68 per cent CL), in good agreement with previous results from Harvey et al.
000227032 6531_ $$agravitational lensing: strong
000227032 6531_ $$agravitational lensing: weak
000227032 6531_ $$agalaxies: clusters: individual: Abell 2744
000227032 700__ $$aJauzac, M.$$uUniv Durham, Dept Phys, Ctr Extragalact Astron, Durham DH1 3LE, England
000227032 700__ $$aEckert, D.$$uEcole Polytech Fed Lausanne, Astrophys Lab, Observ Sauverny, CH-1290 Versoix, Switzerland
000227032 700__ $$aSchwinn, J.$$uEcole Polytech Fed Lausanne, Astrophys Lab, Observ Sauverny, CH-1290 Versoix, Switzerland
000227032 700__ $$0248429$$aHarvey, D.$$g251165$$uEcole Polytech Fed Lausanne, Astrophys Lab, Observ Sauverny, CH-1290 Versoix, Switzerland
000227032 700__ $$aBaugh, C. M.$$uUniv Durham, Inst Computat Cosmol, South Rd, Durham DH1 3LE, England
000227032 700__ $$aRobertson, A.$$uUniv Durham, Inst Computat Cosmol, South Rd, Durham DH1 3LE, England
000227032 700__ $$aBose, S.$$uUniv Durham, Inst Computat Cosmol, South Rd, Durham DH1 3LE, England
000227032 700__ $$aMassey, R.$$uUniv Durham, Dept Phys, Ctr Extragalact Astron, Durham DH1 3LE, England
000227032 700__ $$aOwers, M.$$uMacquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia
000227032 700__ $$aEbeling, H.$$uUniv Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA
000227032 700__ $$0246615$$aShan, H. Y.$$g228749$$uEcole Polytech Fed Lausanne, Astrophys Lab, Observ Sauverny, CH-1290 Versoix, Switzerland
000227032 700__ $$aJullo, E.$$uUniv Aix Marseille, LAM, 38 Rue Joliot Curie, F-13388 Marseille 13, France
000227032 700__ $$0246614$$aKneib, J. -P.$$g222189$$uEcole Polytech Fed Lausanne, Astrophys Lab, Observ Sauverny, CH-1290 Versoix, Switzerland
000227032 700__ $$aRichard, J.$$uUniv Lyon 1, ENS Lyon, CNRS, Ctr Rech Astrophys Lyon,UMR5574, F-69230 St Genis Laval, France
000227032 700__ $$0246906$$aAtek, H.$$g230964$$uYale Univ, Dept Astron, 260 Whitney Ave, New Haven, CT 06511 USA
000227032 700__ $$aClement, B.$$uUniv Lyon 1, ENS Lyon, CNRS, Ctr Rech Astrophys Lyon,UMR5574, F-69230 St Genis Laval, France
000227032 700__ $$aEgami, E.$$uUniv Arizona, Steward Observ, 933 North Cherry Ave, Tucson, AZ 85721 USA
000227032 700__ $$aIsrael, H.$$uUniv Durham, Dept Phys, Ctr Extragalact Astron, Durham DH1 3LE, England
000227032 700__ $$aKnowles, K.
000227032 700__ $$aLimousin, M.$$uMacquarie Univ, Dept Phys & Astron, N Ryde, NSW 2109, Australia
000227032 700__ $$aNatarajan, P.$$uYale Univ, Dept Astron, 260 Whitney Ave, New Haven, CT 06511 USA
000227032 700__ $$0247877$$aRexroth, M.$$g242413$$uEcole Polytech Fed Lausanne, Astrophys Lab, Observ Sauverny, CH-1290 Versoix, Switzerland
000227032 700__ $$aTaylor, P.$$uUniv Durham, Dept Phys, Ctr Extragalact Astron, Durham DH1 3LE, England
000227032 700__ $$aTchernin, C.$$uHeidelberg Univ, Inst Theoret Astrophys, Zentrum Astron, Philosophenweg 12, D-69120 Heidelberg, Germany
000227032 773__ $$j463$$k4$$q3876-3893$$tMonthly Notices Of The Royal Astronomical Society
000227032 909C0 $$0252365$$pLASTRO$$xU10933
000227032 909CO $$ooai:infoscience.tind.io:227032$$pSB$$particle
000227032 917Z8 $$x103317
000227032 937__ $$aEPFL-ARTICLE-227032
000227032 973__ $$aEPFL$$rREVIEWED$$sPUBLISHED
000227032 980__ $$aARTICLE