Microlensing in dark matter haloes
Using eight dark matter haloes extracted from fully self-consistent cosmological N-body simulations, we perform microlensing experiments. A hypothetical observer is placed at a distance of 8.5 kpc from the centre of the halo measuring optical depths, event durations and event rates towards the direc...
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Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2006-05, Vol.368 (3), p.1209-1222 |
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creator | Holopainen, Janne Flynn, Chris Knebe, Alexander Gill, Stuart P. Gibson, Brad K. |
description | Using eight dark matter haloes extracted from fully self-consistent cosmological N-body simulations, we perform microlensing experiments. A hypothetical observer is placed at a distance of 8.5 kpc from the centre of the halo measuring optical depths, event durations and event rates towards the direction of the Large Magellanic Cloud. We simulate 1600 microlensing experiments for each halo. Assuming that the whole halo consists of massive astronomical compact halo objects (MACHOs), f= 1.0, and a single MACHO mass is mM= 1.0 M⊙, the simulations yield mean values of τ= 4.7+5.0−2.2× 10−7 and Γ= 1.6+1.3−0.6× 10−6 events star−1 yr−1. We find that triaxiality and substructure can have major effects on the measured values so that τ and Γ values of up to three times the mean can be found. If we fit our values of τ and Γ to the MACHO collaboration observations, we find f= 0.23+0.15−0.13 and mM= 0.44+0.24−0.16. Five out of the eight haloes under investigation produce f and mM values mainly concentrated within these bounds. |
doi_str_mv | 10.1111/j.1365-2966.2006.10205.x |
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A hypothetical observer is placed at a distance of 8.5 kpc from the centre of the halo measuring optical depths, event durations and event rates towards the direction of the Large Magellanic Cloud. We simulate 1600 microlensing experiments for each halo. Assuming that the whole halo consists of massive astronomical compact halo objects (MACHOs), f= 1.0, and a single MACHO mass is mM= 1.0 M⊙, the simulations yield mean values of τ= 4.7+5.0−2.2× 10−7 and Γ= 1.6+1.3−0.6× 10−6 events star−1 yr−1. We find that triaxiality and substructure can have major effects on the measured values so that τ and Γ values of up to three times the mean can be found. If we fit our values of τ and Γ to the MACHO collaboration observations, we find f= 0.23+0.15−0.13 and mM= 0.44+0.24−0.16. Five out of the eight haloes under investigation produce f and mM values mainly concentrated within these bounds.</description><subject>Astronomy</subject><subject>Cosmology</subject><subject>Dark matter</subject><subject>Earth, ocean, space</subject><subject>Exact sciences and technology</subject><subject>Galaxy: structure</subject><subject>gravitational lensing</subject><subject>methods: N-body simulations</subject><subject>Simulation</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2006</creationdate><recordtype>article</recordtype><recordid>eNqNkVFL5DAUhcOyCzs7u_-hCO5ba5LbJO2LsIg64riCKMi-XNI00Y6ddkxmcPz3plYUFgXzknDvOYd7vxCSMJqxePYWGQMpUl5KmXFKZcYopyLbfiGT18ZXMqEURFooxr6THyEsKKU5cDkhO2eN8X1ru9B0N0nTJbX2d8lSr9fWJ7e67W34Sb453Qb76-Wekqujw8uDWTo_Pz45-DNPjZBCpBXUVQWVURV1hRNQcilypStVGGMVOGdL0K6oTV3ngjteKVsUpeXMxLJVDKbk95i78v39xoY1LptgbNvqzvabgLwoASSITwjjcqzMo3DnP-Gi3_guLoGcKhA5RCxTUoyiyCEEbx2ufLPU_hEZxQExLnAgiQNJHBDjM2LcRuvuS74ORrfO68404c2vlJAShjn2R91D09rHT-fj2d-L52cMgDGg36w-sKfvjZeOrias7fbVFz8YpQIlcHb9D08h5-x0LvEangC8lKtl</recordid><startdate>20060521</startdate><enddate>20060521</enddate><creator>Holopainen, Janne</creator><creator>Flynn, Chris</creator><creator>Knebe, Alexander</creator><creator>Gill, Stuart P.</creator><creator>Gibson, Brad K.</creator><general>Blackwell Publishing Ltd</general><general>Blackwell Science</general><general>Oxford University Press</general><scope>BSCLL</scope><scope>IQODW</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>7U5</scope></search><sort><creationdate>20060521</creationdate><title>Microlensing in dark matter haloes</title><author>Holopainen, Janne ; Flynn, Chris ; Knebe, Alexander ; Gill, Stuart P. ; Gibson, Brad K.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c5655-b3dbb3bc7b0f8f53926547ab78cce73ffe93af8dcdd452f2b7e889e21c3afe713</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2006</creationdate><topic>Astronomy</topic><topic>Cosmology</topic><topic>Dark matter</topic><topic>Earth, ocean, space</topic><topic>Exact sciences and technology</topic><topic>Galaxy: structure</topic><topic>gravitational lensing</topic><topic>methods: N-body simulations</topic><topic>Simulation</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Holopainen, Janne</creatorcontrib><creatorcontrib>Flynn, Chris</creatorcontrib><creatorcontrib>Knebe, Alexander</creatorcontrib><creatorcontrib>Gill, Stuart P.</creatorcontrib><creatorcontrib>Gibson, Brad K.</creatorcontrib><collection>Istex</collection><collection>Pascal-Francis</collection><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Solid State and Superconductivity Abstracts</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Holopainen, Janne</au><au>Flynn, Chris</au><au>Knebe, Alexander</au><au>Gill, Stuart P.</au><au>Gibson, Brad K.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Microlensing in dark matter haloes</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><stitle>Monthly Notices of the Royal Astronomical Society</stitle><addtitle>Monthly Notices of the Royal Astronomical Society</addtitle><date>2006-05-21</date><risdate>2006</risdate><volume>368</volume><issue>3</issue><spage>1209</spage><epage>1222</epage><pages>1209-1222</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><coden>MNRAA4</coden><abstract>Using eight dark matter haloes extracted from fully self-consistent cosmological N-body simulations, we perform microlensing experiments. A hypothetical observer is placed at a distance of 8.5 kpc from the centre of the halo measuring optical depths, event durations and event rates towards the direction of the Large Magellanic Cloud. We simulate 1600 microlensing experiments for each halo. Assuming that the whole halo consists of massive astronomical compact halo objects (MACHOs), f= 1.0, and a single MACHO mass is mM= 1.0 M⊙, the simulations yield mean values of τ= 4.7+5.0−2.2× 10−7 and Γ= 1.6+1.3−0.6× 10−6 events star−1 yr−1. We find that triaxiality and substructure can have major effects on the measured values so that τ and Γ values of up to three times the mean can be found. If we fit our values of τ and Γ to the MACHO collaboration observations, we find f= 0.23+0.15−0.13 and mM= 0.44+0.24−0.16. Five out of the eight haloes under investigation produce f and mM values mainly concentrated within these bounds.</abstract><cop>Oxford, UK</cop><pub>Blackwell Publishing Ltd</pub><doi>10.1111/j.1365-2966.2006.10205.x</doi><tpages>14</tpages><oa>free_for_read</oa></addata></record> |
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subjects | Astronomy Cosmology Dark matter Earth, ocean, space Exact sciences and technology Galaxy: structure gravitational lensing methods: N-body simulations Simulation |
title | Microlensing in dark matter haloes |
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