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DISENTANGLING BARYONS AND DARK MATTER IN THE SPIRAL GRAVITATIONAL LENS B1933+503.

Authors :
SUYU, S. H.
HENSEL, S. W.
MCKEAN, J. P.
FASSNACHT, C. D.
TREU, T.
HALKOLA, A.
NORBURY, M.
JACKSON, N.
SCHNEIDER, P.
THOMPSON, D.
AUGER, M. W.
KOOPMANS, L. V. E.
MATTHEWS, K.
Source :
Astrophysical Journal; May2012, Vol. 750 Issue 1, p1-15, 15p
Publication Year :
2012

Abstract

Measuring the relative mass contributions of luminous and dark matter in spiral galaxies is important for understanding their formation and evolution. The combination of a galaxy rotation curve and strong lensing is a powerful way to break the disk--halo degeneracy that is inherent in each of the methods individually. We present an analysis of the 10 image radio spiral lens B1933+503 at z<subscript>1</subscript> = 0.755, incorporating (1) new global very long baseline interferometry observations, (2) new adaptive-optics-assisted K-band imaging, and (3) new spectroscopic observations for the lens galaxy rotation curve and the source redshift. We construct a three-dimensionally axisymmetric mass distribution with three components: an exponential profile for the disk, a point mass for the bulge, and a Navarro--Frenk--White (NFW) profile for the halo. The mass model is simultaneously fitted to the kinematics and the lensing data. The NFW halo needs to be oblate with a flattening of a/c = 0.33<subscript>-0.05</subscript><superscript>+0.07</superscript> to be consistent with the radio data. This suggests that baryons are effective at making the halos oblate near the center. The lensing and kinematics analysis probe the inner ~10 kpc of the galaxy, and we obtain a lower limit on the halo scale radius of 16 kpc (95% credible intervals). The dark matter mass fraction inside a sphere with a radius of 2.2 disk scale lengths is f<subscript>DM,2.2</subscript> = 0.43<subscript>-0.09</subscript><superscript>+0.10</superscript>. The contribution of the disk to the total circular velocity at 2.2 disk +0.05 scale lengths is 0.76<subscript>-0.06</subscript><superscript>+0.05</superscript>, suggesting that the disk is marginally submaximal. The stellar mass of the disk from our modeling is log<subscript>10</subscript> (M<subscript>*</subscript> /M<subscript>☉</subscript>) = 11.06<subscript>-0.11</subscript><superscript>+0.09</superscript> assuming that the cold gas contributes ~20% to the total disk mass. In comparison to the stellar masses estimated from stellar population synthesis models, the stellar initial mass function of Chabrier is preferred to that of Salpeter by a probability factor of 7.2. [ABSTRACT FROM AUTHOR]

Details

Language :
English
ISSN :
0004637X
Volume :
750
Issue :
1
Database :
Complementary Index
Journal :
Astrophysical Journal
Publication Type :
Academic Journal
Accession number :
89964960
Full Text :
https://doi.org/10.1088/0004-637X/750/1/10