skip to main content

DOE PAGESDOE PAGES

Title: The density of dark matter in the Galactic bulge and implications for indirect detection

A recent study, making use of the number of horizontal branch stars observed in infrared photometric surveys and kinematic measurements of M-giant stars from the BRAVA survey, combined with N-body simulations of stellar populations, has presented a new determination of the dark matter mass within the bulge-bar region of the Milky Way. That study constrains the total mass within the $$\pm 2.2 \times \pm 1.4 \times \pm 1.2$$ kpc volume of the bulge-bar region to be ($$1.84 \pm 0.07) \times 10^{10} \, M_{\odot}$$, of which 9-30% is made up of dark matter. Here, we use this result to constrain the the Milky Way's dark matter density profile, and discuss the implications for indirect dark matter searches. Furthermore uncertainties remain significant, these results favor dark matter distributions with a cusped density profile. For example, for a scale radius of 20 kpc and a local dark matter density of 0.4 GeV/cm$^3$, density profiles with an inner slope of 0.69 to 1.40 are favored, approximately centered around the standard NFW value. In contrast, profiles with large flat-density cores are disfavored by this information.
Authors:
ORCiD logo [1]
  1. Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States); Univ. of Chicago, Chicago, IL (United States)
Publication Date:
Report Number(s):
FERMILAB-PUB-16-291-A; arXiv:1608.00003
Journal ID: ISSN 2212-6864; 1478730
Grant/Contract Number:
AC02-07CH11359; FG02-13ER41958; SC0009924
Type:
Accepted Manuscript
Journal Name:
Physics of the Dark Universe
Additional Journal Information:
Journal Volume: 15; Journal Issue: C; Journal ID: ISSN 2212-6864
Publisher:
Elsevier
Research Org:
Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)
Sponsoring Org:
USDOE Office of Science (SC), High Energy Physics (HEP) (SC-25)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; 72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS
OSTI Identifier:
1331124
Alternate Identifier(s):
OSTI ID: 1415860

Hooper, Dan. The density of dark matter in the Galactic bulge and implications for indirect detection. United States: N. p., Web. doi:10.1016/j.dark.2016.11.005.
Hooper, Dan. The density of dark matter in the Galactic bulge and implications for indirect detection. United States. doi:10.1016/j.dark.2016.11.005.
Hooper, Dan. 2016. "The density of dark matter in the Galactic bulge and implications for indirect detection". United States. doi:10.1016/j.dark.2016.11.005. https://www.osti.gov/servlets/purl/1331124.
@article{osti_1331124,
title = {The density of dark matter in the Galactic bulge and implications for indirect detection},
author = {Hooper, Dan},
abstractNote = {A recent study, making use of the number of horizontal branch stars observed in infrared photometric surveys and kinematic measurements of M-giant stars from the BRAVA survey, combined with N-body simulations of stellar populations, has presented a new determination of the dark matter mass within the bulge-bar region of the Milky Way. That study constrains the total mass within the $\pm 2.2 \times \pm 1.4 \times \pm 1.2$ kpc volume of the bulge-bar region to be ($1.84 \pm 0.07) \times 10^{10} \, M_{\odot}$, of which 9-30% is made up of dark matter. Here, we use this result to constrain the the Milky Way's dark matter density profile, and discuss the implications for indirect dark matter searches. Furthermore uncertainties remain significant, these results favor dark matter distributions with a cusped density profile. For example, for a scale radius of 20 kpc and a local dark matter density of 0.4 GeV/cm$^3$, density profiles with an inner slope of 0.69 to 1.40 are favored, approximately centered around the standard NFW value. In contrast, profiles with large flat-density cores are disfavored by this information.},
doi = {10.1016/j.dark.2016.11.005},
journal = {Physics of the Dark Universe},
number = C,
volume = 15,
place = {United States},
year = {2016},
month = {11}
}