Dark Matter Substructure Detection Using Spatially Resolved Spectroscopy of Lensed Dusty Galaxies

• Published in: The Astrophysical Journal
• Main Authors: Hezaveh, Yashar, Dalal, Neal, Holder, Gilbert, Kuhlen, Michael, Marrone, Daniel, Murray, Norman, Vieira, Joaquin
• Format: Article in Journal/Newspaper
• Language: unknown
• Published: American Astronomical Society 2013
• Subjects: dark matter; galaxies: dwarf; galaxies: luminosity function; mass function; galaxies: structure; gravitational lensing: strong; South Pole; South pole
• Online Access: https://doi.org/10.1088/0004-637X/767/1/9

We investigate how strong lensing of dusty, star-forming galaxies (DSFGs) by foreground galaxies can be used as a probe of dark matter halo substructure. We find that spatially resolved spectroscopy of lensed sources allows dramatic improvements to measurements of lens parameters. In particular, we find that modeling of the full, three-dimensional (angular position and radial velocity) data can significantly facilitate substructure detection, increasing the sensitivity of observables to lower mass subhalos. We carry out simulations of lensed dusty sources observed by early ALMA (Cycle 1) and use a Fisher matrix analysis to study the parameter degeneracies and mass detection limits of this method. We find that even with conservative assumptions, it is possible to detect galactic dark matter subhalos of ~10^8 M_☉ with high significance in most lensed DSFGs. Specifically, we find that in typical DSFG lenses, there is a ~55% probability of detecting a substructure with M > 10^8 M_☉ with more than 5σ detection significance in each lens, if the abundance of substructure is consistent with previous lensing results. The full ALMA array, with its significantly enhanced sensitivity and resolution, should improve these estimates considerably. Given the sample of ~100 lenses provided by surveys such as the South Pole Telescope, our understanding of dark matter substructure in typical galaxy halos is poised to improve dramatically over the next few years. © 2013 American Astronomical Society. Received 2012 October 15; accepted 2013 February 15; published 2013 March 19. This work was supported by NASA under grant NNX12AD02G, by NSERC, the CRC program, and CIfAR. Y.D.H. is grateful for useful discussions with C. Fassnacht which considerably improved the uv-plane modeling. Y.D.H. acknowledges the support of FQRNT through International Training Program and Doctoral Research scholarships. N.D. gratefully acknowledges support by a Sloan Research Fellowship from the Alfred P. Sloan Foundation. We thank the SPT team for ...