Publication

Disentangling Baryons and Dark Matter in the Spiral Gravitational Lens B1933+503

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., May-2012, In : Astrophysical Journal. 750, 1, 15 p., 10.

Research output: Contribution to journalArticleAcademicpeer-review

APA

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. (2012). Disentangling Baryons and Dark Matter in the Spiral Gravitational Lens B1933+503. Astrophysical Journal, 750(1), [10]. https://doi.org/10.1088/0004-637X/750/1/10

Author

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. / Disentangling Baryons and Dark Matter in the Spiral Gravitational Lens B1933+503. In: Astrophysical Journal. 2012 ; Vol. 750, No. 1.

Harvard

Suyu, SH, Hensel, SW, McKean, JP, Fassnacht, CD, Treu, T, Halkola, A, Norbury, M, Jackson, N, Schneider, P, Thompson, D, Auger, MW, Koopmans, LVE & Matthews, K 2012, 'Disentangling Baryons and Dark Matter in the Spiral Gravitational Lens B1933+503', Astrophysical Journal, vol. 750, no. 1, 10. https://doi.org/10.1088/0004-637X/750/1/10

Standard

Disentangling Baryons and Dark Matter in the Spiral Gravitational Lens B1933+503. / 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.

In: Astrophysical Journal, Vol. 750, No. 1, 10, 05.2012.

Research output: Contribution to journalArticleAcademicpeer-review

Vancouver

Suyu SH, Hensel SW, McKean JP, Fassnacht CD, Treu T, Halkola A et al. Disentangling Baryons and Dark Matter in the Spiral Gravitational Lens B1933+503. Astrophysical Journal. 2012 May;750(1). 10. https://doi.org/10.1088/0004-637X/750/1/10


BibTeX

@article{050c146340604cf5aa8caa7ef7c5046f,
title = "Disentangling Baryons and Dark Matter in the Spiral Gravitational Lens B1933+503",
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(1) = 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(-0.05)(+0.07) 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 similar to 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(DM, 2.2) = 0.43(-0.09)(+0.10). The contribution of the disk to the total circular velocity at 2.2 disk scale lengths is 0.76(-0.06)(+0.05), suggesting that the disk is marginally submaximal. The stellar mass of the disk from our modeling is log10(M-*/M-circle dot) = 11.06(-0.11)(+0.09) assuming that the cold gas contributes similar to 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.",
keywords = "galaxies: halos, galaxies: individual (B1933+503), galaxies: kinematics and dynamics, galaxies: spiral, gravitational lensing: strong, INITIAL MASS FUNCTION, EARLY-TYPE GALAXIES, ALL-SKY SURVEY, STELLAR POPULATION SYNTHESIS, HALO DENSITY PROFILES, TULLY-FISHER RELATION, SYSTEM B1933+503, ADIABATIC CONTRACTION, COSMOLOGICAL MODEL, ELLIPTIC GALAXIES",
author = "Suyu, {S. H.} and Hensel, {S. W.} and McKean, {J. P.} and Fassnacht, {C. D.} and T. Treu and A. Halkola and M. Norbury and N. Jackson and P. Schneider and D. Thompson and Auger, {M. W.} and Koopmans, {L. V. E.} and K. Matthews",
note = "M1 - Journal Article",
year = "2012",
month = may,
doi = "10.1088/0004-637X/750/1/10",
language = "English",
volume = "750",
journal = "The Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP PUBLISHING LTD",
number = "1",

}

RIS

TY - JOUR

T1 - Disentangling Baryons and Dark Matter in the Spiral Gravitational Lens B1933+503

AU - Suyu, S. H.

AU - Hensel, S. W.

AU - McKean, J. P.

AU - Fassnacht, C. D.

AU - Treu, T.

AU - Halkola, A.

AU - Norbury, M.

AU - Jackson, N.

AU - Schneider, P.

AU - Thompson, D.

AU - Auger, M. W.

AU - Koopmans, L. V. E.

AU - Matthews, K.

N1 - M1 - Journal Article

PY - 2012/5

Y1 - 2012/5

N2 - 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(1) = 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(-0.05)(+0.07) 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 similar to 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(DM, 2.2) = 0.43(-0.09)(+0.10). The contribution of the disk to the total circular velocity at 2.2 disk scale lengths is 0.76(-0.06)(+0.05), suggesting that the disk is marginally submaximal. The stellar mass of the disk from our modeling is log10(M-*/M-circle dot) = 11.06(-0.11)(+0.09) assuming that the cold gas contributes similar to 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.

AB - 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(1) = 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(-0.05)(+0.07) 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 similar to 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(DM, 2.2) = 0.43(-0.09)(+0.10). The contribution of the disk to the total circular velocity at 2.2 disk scale lengths is 0.76(-0.06)(+0.05), suggesting that the disk is marginally submaximal. The stellar mass of the disk from our modeling is log10(M-*/M-circle dot) = 11.06(-0.11)(+0.09) assuming that the cold gas contributes similar to 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.

KW - galaxies: halos

KW - galaxies: individual (B1933+503)

KW - galaxies: kinematics and dynamics

KW - galaxies: spiral

KW - gravitational lensing: strong

KW - INITIAL MASS FUNCTION

KW - EARLY-TYPE GALAXIES

KW - ALL-SKY SURVEY

KW - STELLAR POPULATION SYNTHESIS

KW - HALO DENSITY PROFILES

KW - TULLY-FISHER RELATION

KW - SYSTEM B1933+503

KW - ADIABATIC CONTRACTION

KW - COSMOLOGICAL MODEL

KW - ELLIPTIC GALAXIES

U2 - 10.1088/0004-637X/750/1/10

DO - 10.1088/0004-637X/750/1/10

M3 - Article

VL - 750

JO - The Astrophysical Journal

JF - The Astrophysical Journal

SN - 0004-637X

IS - 1

M1 - 10

ER -

ID: 5549426