Header

UZH-Logo

Maintenance Infos

Detecting the Milky Way's dark disk


Bruch, T; Read, J; Baudis, L; Lake, G (2009). Detecting the Milky Way's dark disk. Astrophysical Journal, 696(1):920-923.

Abstract

In the standard model of disk galaxy formation, a dark matter disk forms as massive satellites are preferentially dragged into the disk plane and dissolve. Here, we show the importance of the dark disk for direct dark matter detection. The low velocity of the dark disk with respect to the Earth enhances detection rates at low recoil energy. For weakly interacting massive particle (WIMP) masses M WIMP gsim 50 GeV/c 2, the detection rate increases by up to a factor of 3 in the 5-20 keV recoil energy range. Comparing this with rates at higher energy is sensitive to M WIMP, providing stronger mass constraints particularly for M WIMP gsim 100 GeV/c 2. The annual modulation signal is significantly boosted and the modulation phase is shifted by ~3 weeks relative to the dark halo. The variation of the observed phase with recoil energy determines M WIMP, once the dark disk properties are fixed by future astronomical surveys. The constraints on the WIMP interaction cross section from current experiments improve by factors of 1.4-3.5 when a typical contribution from the dark disk is included.

Abstract

In the standard model of disk galaxy formation, a dark matter disk forms as massive satellites are preferentially dragged into the disk plane and dissolve. Here, we show the importance of the dark disk for direct dark matter detection. The low velocity of the dark disk with respect to the Earth enhances detection rates at low recoil energy. For weakly interacting massive particle (WIMP) masses M WIMP gsim 50 GeV/c 2, the detection rate increases by up to a factor of 3 in the 5-20 keV recoil energy range. Comparing this with rates at higher energy is sensitive to M WIMP, providing stronger mass constraints particularly for M WIMP gsim 100 GeV/c 2. The annual modulation signal is significantly boosted and the modulation phase is shifted by ~3 weeks relative to the dark halo. The variation of the observed phase with recoil energy determines M WIMP, once the dark disk properties are fixed by future astronomical surveys. The constraints on the WIMP interaction cross section from current experiments improve by factors of 1.4-3.5 when a typical contribution from the dark disk is included.

Statistics

Citations

60 citations in Web of Science®
59 citations in Scopus®
Google Scholar™

Altmetrics

Downloads

123 downloads since deposited on 25 Feb 2010
22 downloads since 12 months
Detailed statistics

Additional indexing

Item Type:Journal Article, refereed, original work
Communities & Collections:07 Faculty of Science > Institute for Computational Science
07 Faculty of Science > Physics Institute
Dewey Decimal Classification:530 Physics
Language:English
Date:May 2009
Deposited On:25 Feb 2010 17:14
Last Modified:05 Apr 2016 13:56
Publisher:Institute of Physics Publishing
ISSN:0004-637X
Funders:Swiss NSF
Publisher DOI:https://doi.org/10.1088/0004-637X/696/1/920
Related URLs:http://arxiv.org/abs/0804.2896

Download

Preview Icon on Download
Preview
Content: Accepted Version
Filetype: PDF (Accepted manuscript, Version 2)
Size: 1MB
View at publisher
Preview Icon on Download
Preview
Content: Accepted Version
Filetype: PDF (Accepted manuscript, Version 1)
Size: 179kB