CLUMPY: Jeans analysis, -ray and fluxes from dark matter (sub-)structures

详细信息    查看全文

• 作者：Vincent Bonnivard^a ; ^{bonnivard@lpsc.in2p3.fr" class="auth_mail" title="E-mail the corresponding author} ; Moritz Hü ; tten^b ; ^{moritz.huetten@desy.de" class="auth_mail" title="E-mail the corresponding author} ; Emmanuel Nezri^c ; ^{Emmanuel.Nezri@lam.fr" class="auth_mail" title="E-mail the corresponding author} ; Aldé ; e Charbonnier^d ; Cé ; line Combet^a ; ^{celine.combet@lpsc.in2p3.fr" class="auth_mail" title="E-mail the corresponding author} ; David Maurin^a ; ^{dmaurin@lpsc.in2p3.fr" class="auth_mail" title="E-mail the corresponding author}
• 关键词：Cosmology ; Dark matter ; Indirect detection ; Gamma-rays ; Neutrinos
• 刊名：Computer Physics Communications
• 出版年：2016
• 出版时间：March 2016
• 年：2016
• 卷：200
• 期：Complete
• 页码：336-349
• 全文大小：1554 K

文摘

We present an update of the CLUMPY code for the calculation of the astrophysical class="mathmlsrc">class="formulatext stixSupport mathImg" data-mathURL="/science?_ob=MathURL&_method=retrieve&_eid=1-s2.0-S0010465515004348&_mathId=si4.gif&_user=111111111&_pii=S0010465515004348&_rdoc=1&_issn=00104655&md5=07fba56259e901f254351dfaf119cfa6" title="Click to view the MathML source">Jclass="mathContainer hidden">class="mathCode">$J$-factors (from dark matter annihilation/decay) for any Galactic or extragalactic dark matter halo including substructures: halo-to-halo concentration scatter may now be enabled, boost factors can include several levels of substructures, and triaxiality is a new option for dark matter haloes. This new version takes advantage of the cfitsio and HEALPix libraries to propose fits output maps using the HEALPix pixelisation scheme. Skymaps for class="mathmlsrc">class="formulatext stixSupport mathImg" data-mathURL="/science?_ob=MathURL&_method=retrieve&_eid=1-s2.0-S0010465515004348&_mathId=si5.gif&_user=111111111&_pii=S0010465515004348&_rdoc=1&_issn=00104655&md5=b61114185494c6a92cc3712f9de02423" title="Click to view the MathML source">γclass="mathContainer hidden">class="mathCode">$\gamma$-ray and class="mathmlsrc">class="formulatext stixSupport mathImg" data-mathURL="/science?_ob=MathURL&_method=retrieve&_eid=1-s2.0-S0010465515004348&_mathId=si59.gif&_user=111111111&_pii=S0010465515004348&_rdoc=1&_issn=00104655&md5=9bfed5f2ce390fa030d0cf81feede6f7" title="Click to view the MathML source">νclass="mathContainer hidden">class="mathCode">$\nu$ signals from generic annihilation/decay spectra are now direct outputs of CLUMPY. Making use of HEALPix routines, smoothing by a user-defined instrumental Gaussian beam and computing the angular power spectrum of the maps are now possible. In addition to these improvements, the main novelty is the implementation of a Jeans analysis module, to obtain dark matter density profiles from kinematic data in relaxed spherical systems (e.g., dwarf spheroidal galaxies). The code is also interfaced with the GreAT toolkit designed for Markov Chain Monte Carlo analyses, from which probability density functions and credible intervals can be obtained for velocity dispersions, dark matter profiles, and class="mathmlsrc">class="formulatext stixSupport mathImg" data-mathURL="/science?_ob=MathURL&_method=retrieve&_eid=1-s2.0-S0010465515004348&_mathId=si4.gif&_user=111111111&_pii=S0010465515004348&_rdoc=1&_issn=00104655&md5=07fba56259e901f254351dfaf119cfa6" title="Click to view the MathML source">Jclass="mathContainer hidden">class="mathCode">$J$-factors.

Program summary

Program title:CLUMPY

Catalogue identifier: AEKS_v2_0

Program summary URL:class="interref" data-locatorType="url" data-locatorKey="http://cpc.cs.qub.ac.uk/summaries/AEKS_v2_0.html">http://cpc.cs.qub.ac.uk/summaries/AEKS_v2_0.html

Program obtainable from: CPC Program Library, Queen’s University, Belfast, N. Ireland

Licensing provisions: Standard CPC licence, class="interref" data-locatorType="url" data-locatorKey="http://cpc.cs.qub.ac.uk/licence/licence.html">http://cpc.cs.qub.ac.uk/licence/licence.html

No. of lines in distributed program, including test data, etc.: 494335

No. of bytes in distributed program, including test data, etc.: 24425968

Distribution format: tar.gz

Programming language: C/C++.

Computer: PC and Mac.

Operating system: UNIX(Linux), MacOS X.

RAM: Between 500MB and 1GB depending on the size of the requested skymap

Catalogue identifier of previous version: AEKS_v1_0

Journal reference of previous version: Comput. Phys. Comm. 183(2012)656

Classification: 1.1, 1.7, 1.9.

External routines: CERN ROOT (class="interref" data-locatorType="url" data-locatorKey="http://root.cern.ch">http://root.cern.ch), GSL (class="interref" data-locatorType="url" data-locatorKey="http://www.gnu.org/software/gsl">http://www.gnu.org/software/gsl), cfitsio (class="interref" data-locatorType="url" data-locatorKey="http://heasarc.gsfc.nasa.gov/fitsio/fitsio.html">http://heasarc.gsfc.nasa.gov/fitsio/fitsio.html), HEALPix C++ and F90 (class="interref" data-locatorType="url" data-locatorKey="http://healpix.sourceforge.net/index.php">http://healpix.sourceforge.net/index.php), GreAT (class="interref" data-locatorType="url" data-locatorKey="http://lpsc.in2p3.fr/great">http://lpsc.in2p3.fr/great) (for MCMC analyses only), and Doxygen (class="interref" data-locatorType="url" data-locatorKey="http://www.doxygen.org">http://www.doxygen.org) (optional)

Does the new version supersede the previous version?: Yes

Nature of problem:   Calculation of dark matter profile from kinematic data, class="mathmlsrc">class="formulatext stixSupport mathImg" data-mathURL="/science?_ob=MathURL&_method=retrieve&_eid=1-s2.0-S0010465515004348&_mathId=si5.gif&_user=111111111&_pii=S0010465515004348&_rdoc=1&_issn=00104655&md5=b61114185494c6a92cc3712f9de02423" title="Click to view the MathML source">γclass="mathContainer hidden">class="mathCode">$\gamma$-ray and class="mathmlsrc">class="formulatext stixSupport mathImg" data-mathURL="/science?_ob=MathURL&_method=retrieve&_eid=1-s2.0-S0010465515004348&_mathId=si59.gif&_user=111111111&_pii=S0010465515004348&_rdoc=1&_issn=00104655&md5=9bfed5f2ce390fa030d0cf81feede6f7" title="Click to view the MathML source">νclass="mathContainer hidden">class="mathCode">$\nu$ signals from dark matter annihilation/decay.

Solution method:   Solve the integro-differential Jeans equation (optimised for speed) for several generic distributions (dark matter profile, light profile, velocity anisotropy). Integration of the DM density (squared) along a line-of-sight for generic dark matter haloes with substructures (spatial, mass, concentration distributions). Draw full skymaps of class="mathmlsrc">class="formulatext stixSupport mathImg" data-mathURL="/science?_ob=MathURL&_method=retrieve&_eid=1-s2.0-S0010465515004348&_mathId=si5.gif&_user=111111111&_pii=S0010465515004348&_rdoc=1&_issn=00104655&md5=b61114185494c6a92cc3712f9de02423" title="Click to view the MathML source">γclass="mathContainer hidden">class="mathCode">$\gamma$-ray and class="mathmlsrc">class="formulatext stixSupport mathImg" data-mathURL="/science?_ob=MathURL&_method=retrieve&_eid=1-s2.0-S0010465515004348&_mathId=si59.gif&_user=111111111&_pii=S0010465515004348&_rdoc=1&_issn=00104655&md5=9bfed5f2ce390fa030d0cf81feede6f7" title="Click to view the MathML source">νclass="mathContainer hidden">class="mathCode">$\nu$ emission from dark matter structures, smoothed by an instrument PSF using HEALPix tools.

Reasons for new version: Many more functionalities and options have been added to the code.

Summary of revisions: Inclusion of the PPPC4DMID spectra for gamma-ray and neutrino fluxes; HEALPix pixelisation for skymaps and angular power spectrum; DM profile triaxiality enabled; More mass–concentration options; Multi-level substructure boost; Jeans analysis module to compute dark matter profiles for stellar kinematic data; Improved ROOT and FITS output.

Restrictions:   The diffuse extragalactic contribution to the signal (and class="mathmlsrc">class="formulatext stixSupport mathImg" data-mathURL="/science?_ob=MathURL&_method=retrieve&_eid=1-s2.0-S0010465515004348&_mathId=si5.gif&_user=111111111&_pii=S0010465515004348&_rdoc=1&_issn=00104655&md5=b61114185494c6a92cc3712f9de02423" title="Click to view the MathML source">γclass="mathContainer hidden">class="mathCode">$\gamma$-ray attenuation) as well as secondary radiation from dark matter remains to be included in order to provide a comprehensive description of the expected signal.

Running time:   This is highly dependent of the user-defined choices of DM profiles, precision class="mathmlsrc">class="formulatext stixSupport mathImg" data-mathURL="/science?_ob=MathURL&_method=retrieve&_eid=1-s2.0-S0010465515004348&_mathId=si84.gif&_user=111111111&_pii=S0010465515004348&_rdoc=1&_issn=00104655&md5=bdd81b460b90ff40202e61a855edc844" title="Click to view the MathML source">εclass="mathContainer hidden">class="mathCode">$\epsilon$ and integration angle class="mathmlsrc">title="View the MathML source" class="mathImg" data-mathURL="/science?_ob=MathURL&_method=retrieve&_eid=1-s2.0-S0010465515004348&_mathId=si64.gif&_user=111111111&_pii=S0010465515004348&_rdoc=1&_issn=00104655&md5=df43c064e135b7371cff67779b051ee7">class="imgLazyJSB inlineImage" height="11" width="24" alt="View the MathML source" style="margin-top: -5px; vertical-align: middle" title="View the MathML source" src="/sd/grey_pxl.gif" data-inlimgeid="1-s2.0-S0010465515004348-si64.gif">class="mathContainer hidden">class="mathCode">${\alpha }_{\mathrm{int}}$:

class="listitem" id="list_l000005">

class="label">•

class="mathmlsrc">class="formulatext stixSupport mathImg" data-mathURL="/science?_ob=MathURL&_method=retrieve&_eid=1-s2.0-S0010465515004348&_mathId=si86.gif&_user=111111111&_pii=S0010465515004348&_rdoc=1&_issn=00104655&md5=352834ea8b8107c864dff68af9dc3cc5" title="Click to view the MathML source">∼1class="mathContainer hidden">class="mathCode">$\sim 1$ hour for a full skymap (including substructures) with class="mathmlsrc">title="View the MathML source" class="mathImg" data-mathURL="/science?_ob=MathURL&_method=retrieve&_eid=1-s2.0-S0010465515004348&_mathId=si87.gif&_user=111111111&_pii=S0010465515004348&_rdoc=1&_issn=00104655&md5=dc4daa5a4e1b27e37795930eb883c15b">class="imgLazyJSB inlineImage" height="14" width="73" alt="View the MathML source" style="margin-top: -5px; vertical-align: middle" title="View the MathML source" src="/sd/grey_pxl.gif" data-inlimgeid="1-s2.0-S0010465515004348-si87.gif">class="mathContainer hidden">class="mathCode">${\alpha }_{\mathrm{int}}=0.1°$ and class="mathmlsrc">class="formulatext stixSupport mathImg" data-mathURL="/science?_ob=MathURL&_method=retrieve&_eid=1-s2.0-S0010465515004348&_mathId=si88.gif&_user=111111111&_pii=S0010465515004348&_rdoc=1&_issn=00104655&md5=f196be146fa6dabfd4bdc86976e1cf79" title="Click to view the MathML source">ε=0.01class="mathContainer hidden">class="mathCode">$\epsilon =0.01$;

class="label">•

class="mathmlsrc">class="formulatext stixSupport mathImg" data-mathURL="/science?_ob=MathURL&_method=retrieve&_eid=1-s2.0-S0010465515004348&_mathId=si89.gif&_user=111111111&_pii=S0010465515004348&_rdoc=1&_issn=00104655&md5=3c3ff2df61ef73e35a107145cc369648" title="Click to view the MathML source">∼=1class="mathContainer hidden">class="mathCode">$\sim =1$ mn for a class="mathmlsrc">class="formulatext stixSupport mathImg" data-mathURL="/science?_ob=MathURL&_method=retrieve&_eid=1-s2.0-S0010465515004348&_mathId=si24.gif&_user=111111111&_pii=S0010465515004348&_rdoc=1&_issn=00104655&md5=f89a28ab95052d8182d6a663b71d4949" title="Click to view the MathML source">5°×5°class="mathContainer hidden">class="mathCode">$5°\times 5°$ skymap (including substructures) with class="mathmlsrc">title="View the MathML source" class="mathImg" data-mathURL="/science?_ob=MathURL&_method=retrieve&_eid=1-s2.0-S0010465515004348&_mathId=si87.gif&_user=111111111&_pii=S0010465515004348&_rdoc=1&_issn=00104655&md5=dc4daa5a4e1b27e37795930eb883c15b">class="imgLazyJSB inlineImage" height="14" width="73" alt="View the MathML source" style="margin-top: -5px; vertical-align: middle" title="View the MathML source" src="/sd/grey_pxl.gif" data-inlimgeid="1-s2.0-S0010465515004348-si87.gif">class="mathContainer hidden">class="mathCode">${\alpha }_{\mathrm{int}}=0.1°$ and class="mathmlsrc">class="formulatext stixSupport mathImg" data-mathURL="/science?_ob=MathURL&_method=retrieve&_eid=1-s2.0-S0010465515004348&_mathId=si88.gif&_user=111111111&_pii=S0010465515004348&_rdoc=1&_issn=00104655&md5=f196be146fa6dabfd4bdc86976e1cf79" title="Click to view the MathML source">ε=0.01class="mathContainer hidden">class="mathCode">$\epsilon =0.01$;

class="label">•

class="mathmlsrc">class="formulatext stixSupport mathImg" data-mathURL="/science?_ob=MathURL&_method=retrieve&_eid=1-s2.0-S0010465515004348&_mathId=si93.gif&_user=111111111&_pii=S0010465515004348&_rdoc=1&_issn=00104655&md5=767a24e4a1fe0cc535b910599b83af30" title="Click to view the MathML source">∼5class="mathContainer hidden">class="mathCode">$\sim 5$ mn for a typical Jeans/MCMC analysis (on a ‘ultrafaint’-like dwarf spheroidal galaxy) using a constant anisotropy profile.