Hostname: page-component-cd9895bd7-7cvxr Total loading time: 0 Render date: 2024-12-23T11:02:13.626Z Has data issue: false hasContentIssue false
  • English
  • Français

Stellar masses calibrated with micro-lensed quasars

Published online by Cambridge University Press:  10 April 2015

Paul L. Schechter ,
Jeffrey A. Blackburne ,
David Pooley  and
Joachim Wambsganss
Paul L. Schechter
Affiliation:
MIT Kavli Institute Cambridge, MA 02139, USA email: [email protected]
Jeffrey A. Blackburne
Affiliation:
Areté Associates, Northridge, CA 91324
David Pooley
Affiliation:
Sam Houston State University, Huntsville, TX 77341
Joachim Wambsganss
Affiliation:
Zentrum für Astronomie der Universität Heidelberg, Germany
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We measure the stellar mass surface densities of early type galaxies by observing the micro-lensing of macro-lensed quasars caused by individual stars, including stellar remnants, brown dwarfs and red dwarfs too faint to produce photometric or spectroscopic signatures. Our method measures the graininess of the gravitational potential, in contrast to methods that decompose a smooth total gravitational potential into two smooth components, one stellar and one dark. We find the median likelihood value for the calibration factor $\cal F$ by which Salpeter stellar masses (with a low mass cutoff of 0.1 M⊙) must be multiplied is 1.23, with a one sigma confidence range of 0.77 < $\cal F$ < 2.10.

Keywords

galaxies: stellar contentgravitational lensing
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S311: Galaxy Masses as Constraints of Formation Models , July 2014 , pp. 96 - 99
Copyright
Copyright © International Astronomical Union 2015 

References

Auger, M. W., Treu, T., Bolton, A. S., et al. 2010, ApJ, 724, 511Google Scholar
Bate, N. F., Floyd, D. J. E., Webster, R. L., & Wyithe, J. S. B. 2011, ApJ, 731, 71CrossRefGoogle Scholar
Blackburne, J. A., Pooley, D., Rappaport, S., & Schechter, P. L. 2011, ApJ, 729, 34Google Scholar
Hyde, J. B. & Bernardi, M. 2009, MNRAS, 396, 1171Google Scholar
Kochanek, C. S. 2004, ApJ, 605, 58Google Scholar
Mosquera, A. M. & Kochanek, C. S. 2011, ApJ, 738, 96Google Scholar
Pooley, D., Blackburne, J. A., Rappaport, S., & Schechter, P. L. 2007, ApJ, 661, 19Google Scholar
Schechter, P. L., Pooley, D., Blackburne, J. A., & Wambsganss, J. 2014, arXiv:1405.0038Google Scholar
Schechter, P. L. & Wambsganss, J. 2004, in IAU Symposium, Vol. 220, Dark Matter in Galaxies, ed. Ryder, S., Pisano, D., Walker, M., & Freeman, K., 103.Google Scholar
Sonnenfeld, A., Gavazzi, R., Suyu, S. H., Treu, T., & Marshall, P. J. 2013, ApJ, 777, 97CrossRefGoogle Scholar