Mass and Light distributions in Clusters of Galaxies - Henry A ...

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Mass and Light of A1703, A370 & RXJ1347-11 in the green sample. The total flux of the cluster in the n th radial bin is therefore, F cl (r n ) = ∑ i F (G) i − 〈D(B) 〉/〈D (G) 〉〈g T (r n ) (B) 〉 ∑ i F (G) i g (G) T,i (3.6) and the flux is then translated to luminosity. First we calculate the absolute magnitude, M = m − 5 log d L − K(z) + 5, (3.7) where the K-correction is evaluated for each radial bin according to its color. The luminosity is simply, L = 10 0.4(M ⊙−M) L ⊙ , (3.8) where M ⊙ is the absolute magnitude of the Sun (AB system) in the relevant band. The results for all four clusters, including A1689, are shown in Fig. 3.8. As explained in § 3.3, the green sample comprises mostly of cluster galaxies, therefore the correction is not big for r < 10 ′ , and only present at large radii, increasing the error. The cluster luminosity profiles mostly have a steady linear decline with radius, and are well described by a power-law fit, but with different slopes of d log(L)/d log(r) ∼ −0.95 ± 0.1, −1.4 ± 0.06, −0.9 ± 0.1 for A1703, A370 and RXJ1347-11, respectively. 3.9 M/L profiles We may now derive a radial profile of the differential mass-to-light ratio (often referred to as δM(r)/δL(r)) by dividing the best-fit NFW projected mass density profile by the newly derived luminosity density profile obtained in § 3.8. The four M/L profiles are shown together in Fig. 3.9 to the limit of our data, ∼ 3 h Mpc. The mass profiles for these clusters and their NFW fits were derived in our earlier work, Broadhurst et al. (2005b) for A1689 and in 98
3.9 M/L profiles Broadhurst et al. (2008) for A370, A1703 and RXJ1347 based on the sample selection scheme described in this paper. For A1689, we found previously that the M/L ratio peaks at intermediate radius around r ∼ 100 h −1 kpc and then falls off to larger radius. Here we find a similar behavior for the other clusters, especially evident for A370, where M/L peaks at about r ∼ 350 h −1 kpc with values of M/L R ∼ 300 − 400 h(M/L) ⊙ , and declines to values of M/L R ∼ 100 h(M/L) ⊙ at the outskirts. A decline in M/L is also seen towards the center of the cluster, reaching M/L R ∼ 200 h(M/L) ⊙ below r 200 h −1 kpc. The M/L profile of A1703 also shows a similar trend, where it peaks at a radius of r ∼ 200 − 300 h −1 kpc with values of M/L r ′ ∼ 300 h(M/L) ⊙ and declines gradually to values of M/L r ′ ∼ 100 h(M/L) ⊙ at large radii. The profile of RXJ1347-11 declines from values of M/L R ∼ 400 − 500 h(M/L) ⊙ at r ∼ 200 − 300 h −1 kpc to values of M/L R ∼ 100 h(M/L) ⊙ at large radius. The decrease in M/L values toward the center of the cluster is only really evident for two clusters, A1689 and A370. For these clusters the luminosity profiles are relatively steep, and it this is continuation of a steep power-law towards the center that causes M/L to decline, as the mass profiles are not power-law but have a continuously declining gradient towards the cluster centers (NFW-like), so that the proportion of M/L declines markedly interior to the characteristic radius for these two clusters. The decrease in M/L toward large radius seen for all four clusters is possibly explained by the increasing proportion of later type galaxies at larger radii, a manifestation of the morphology-density relation (Dressler 1980). Similar results have been shown by Rines et al. (2000) and Katgert et al. (2004); in Rines et al. (2000) where the differential M/L profile is similar to ours, with a decreasing M/L with radius, and their outermost value of M/L R ∼ 100 h(M/L) ⊙ is in good agreement with the values we get for all our four clusters. Katgert et al. (2004) show a decrease at small radius, and by removing the brightest cluster members this decrease is shown to disappear. The declining behavior is not simply accounted for by the change of stellar population with distance from the cluster center. The galaxy colors show a 99
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TELAVIVUNIVERSITY SCHOOLOFPHYSICS&A
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To my parents
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1.2.3 Weak Gravitational Lensing .
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Chapter 1 Introduction Clusters of
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Page 163 and 164: REFERENCES Broadhurst, T., Umetsu,
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REFERENCES Gaidos, E. J. 1997, AJ,
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REFERENCES Kaiser, N. 1995, ApJ, 43
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REFERENCES Natarajan, P., Loeb, A.,
Page 171 and 172:
REFERENCES Schrabback, T. et al. 20
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כפי שמתואר בפרק השל
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עבודה זו נעשתה בהנח
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