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Planck Sky Model : User Manual

1. gt PSM_IDEAL 4 gt HFI_IDEAL 4 gt LFI_IDEAL h gt HFI_BLUEBOOK 4 gt LFI_BLUEBOOK 59 gt HFI_RIMO h gt LFI_RIMO gt WMAP gt IRAS_IDEAL gt IRAS_TABLEBANDS gt channel_list is the list of channels to be included gt default all individual detectors or all frequency bands if freqs is set gt version sets the version for HFI_RIMO LFI_RIMO WMAP 18 2 Instrument structures An instrument is represented as a collection of channels with each a symmetric beam a spectral band noise properties polarisation properties pixelisation properties It is represented internally by the PSM as a somewhat complex structure created with the LOAD_INSTRUMENT procedure For instance the following command line in IDL creates a PSM instrument that represents in a simplified way the WMAP instrument 7 year version with here 5 channels only one per frequency band and ideal monochromatic spectral band approximation IDL gt wmap LOAD_INSTRUMENT WMAP version 7yr freqs Information about the corresponding WMAP instrument can be visualised using the PRTSTRUCT utility e g IDL gt prtstruct wmap name WMAP WMAP NAME gt STRING gt WMAP WMAP VERSION gt STRING gt 7yr WMAP NCHANNEL gt INT 5 WMAP CHANNEL_1 INST g
2. ee 32 3 The debug keyword o scemi heb ee HA ES eee ee eee LAA Se ee De es 3 2 4 The carefulness keyword e sars ee sos BE ee ee 3 2 5 The verbosity keyword e 3 3 Outputs f the PSM oo mai a ee a EO ae a ES ee 34 Consecutive PSM runs 2 I Su edo git ee eee ee oe a OE ok eae a Oe e a 3 5 Monte Carlo simulations using the PSM 1 2 0 022 000 0000 000000000 4 Configuration files 4 1 Syntax for editing configuration files 0 0 0 00000000 00000000004 4 2 User ready configuration files 2 ee e 4 3 Global parameters of the PSM runa 4 3 1 QUIPUT DIRECTORY a oo UE SAO Be a a a GE ita 4 3 2 PRECISION nce rd oe PR ee chad dae AE aa Ee Re Pes dd gt sBIELDS 3 8 2 oO Qh ee eo ee Ba a AAN re ek oe A ASA CLEARVAL Lice seit etn ea ee PR a AA MSE ee LOR DS ee a Aios VISU ct i os RR he te Gasca Recta Shae maha see gence Sea A336 QUIPUT VISU ap bits vandre ey id e a dt Soe ee ea al es A SEED us fe tt asc don at OP sees ad Se pias ea By Be ao ee a oe oh on el shoe G ALO eGET DATA 3 gea di net eth aed ne tie SEs at ng Me an ee Eni The sky model 5 1 Global parameters of the sky model pee ee ee Dalsl SKYETASK i isc ia e da GA he ae Sick Gs Be es oe ta Da 51 2 YSKY RESOLUTION 4 Ax E A ee a De Be EO SS Oe PEO ee Bligh OKY LMAX a a AE Riek oh ae ae wb Ge ek BR ae Gh ie eee ee a eta 01 47 SKYEPTRELISATI N cea a e ei ee be Ba eRe Ee Od 5 1 5 HEALPIX NSIDE
3. gt lt PtrHeapVar150 gt STRING co_ampl132 fits l UNIT gt STRING MJy sr INFO gt STRING flux at ref freq NUREF VALUE gt lt PtrHeapVari51 gt DOUBLE E 3 4579600e 11 UNIT gt STRING Hz l INFO gt STRING reference frequency 15 2 4 Emission laws PSM emission laws are parametric functions F v where v is frequency and a set of parameters Imple mented emission laws are listed in Table 28 51 emission law description comments parameters cmb CMB anisotropy emission law derivative of blackbody none w r t temperature at T Tomb blackbody Black body F v T x B T temperature T greybody Modified black body F v a T x v B T Sen powerlaw Power law F v a x v spectral index a spectral index a curvpowerlaw Curved power law F v a de Ve x vot 810 4 ve curv amplitude a curv ref freq Ve freefree Free free emission law electron temp Te spindust Spinning dust emission law see section 10 5 thermalsz Thermal SZ emission law The temperature parameter is electron temp Te optional If present it is used to compute relativistic cor rections up to order 4 in T mc relatszl Spectral dependence of the first order relativistic correction none to thermal SZ relatsz2 Spectral dependence of the second order relativistic correc none tion to t
4. 17 4 Seeds for random number generation 58 18 Some useful PSM software tools The PSM software distribution comprises various tools that can be useful for various purposes besides the generation of simulations using the PSM_MAIN procedure This section describes the most useful of them 18 1 Documentation and online help 18 1 1 Documentation Partial documentation about PSM programs can be generated using the PSMDOCGEN procedure Simply type PSMDOCGEN in the IDL command line and an html document named psm_documentation html will be generated in the doc subdirectory of the PSM software directory Only partial information is available so far however 18 1 2 PSMHELP A complete list of PSM procedures and functions is printed out in the IDL standard output by typing IDL gt psmhelp The output can be limited to programs that contain a particular template in their names as follows e g IDL gt psmhelp instrument will print out all programs that contain instrument in their names The output is 18 1 3 PROHELP For a large fraction of PSM procedures and function short online help can be obtained using the PROHELP procedure e g typing IDL gt prohelp load_instrument will print out LOAD_INSTRUMENT function which returns a structure describing an instrument gt SYNTAX result LOAD_INSTRUMENT instrument_name channel_list version freqs gt Choose instrument_name from the following list
5. 0 ced wea alee ala ee Aw A ee ee oR a a ea 51 6 JSKY PIXWINDOW 3 O O A eee gee a lT WRITE ANCILLARY vk cee ee eed Qe ek a E A A ae he a 5 2 Models tor all components vasc ee Bow Gi pea eee a aoe eae Gee Sew aE Daly Cosmology 6 1 Cosmological parameters ee 6 2 Density fluctuations and cosmic structure ooo ee 6 21 RUNEGAMB a ea k hte eee a 4 46 wre wie dd A Hepes big a ae 6 2 2 gt TRUNZCLASS ci ee ea a a A ee a a De eee ee 6 23 CMBECL SOURCE odai vei hed ed Wn ee a ike ake Mo he ee a td et 2d 6 2 4 COSMOZPK SOURCE es Re ee ga ae beer Ren Bee SE da dad The CMB dipole fA prediction CMB dipoles woe ce z s aos A ae tae ins Gl he ee A a AP ee we haba aie T2 generic CMB dipoles i005 o Pe E erie ee a ee Pk A A See ees Cosmic Microwave Background anisotropies 8 1 prediction CMB Modelo A A a ee a se a 8 2 gaussian MB modelito o sd didi eee a ee ee eo ee AA et ol 8 2 1 CMB CONSTRAINED ui Gece a ee ie doa ARA AA FE ea a ore Wade ae es 82 27 CMBLENSING a m ol a tee eae ae Re a Ge Oe ET Be ek ei ae ee 2S es 8 3 nongaussian_fnl CMB model s ns secceihin pe eaaa pae a b kaaa EE SL NE SIMUSET srg d si ree ace es ls a da ee da ai Wenas we ge Boe ee eS 8 3 2 SHI ELE EXTEND GAUSSIAN 20000000 wee a A A A ee E a 73 0 READJUSE NG SPECTRUM anier i a a cio A Se A Be eS Gat DRAWESNE o dieat 4 A ar Be Bod Peete dl bo bk Bie tet eg ala ane a BS FONDSMIN o e ee eee a Be eae oa eh ce S316 SE ND MAR s
6. CMB anisotropies cmb the thermal and kinetic SZ effects sz Galactic emission from the diffuse inter stellar medium which comprises thermal dust spinning dust synchrotron free free and CO lines galaxy emission from radio sources infrared sources ultra compact H II regions and WMAP unresolved sources collectively denoted as point sources ps and the far infrared background firb For each of these components several different models are available each of which specified with a number of model specific parameters detailed in sections 7 to 12 Table 3 summarises the available models for each of the main components component description comments accepted models default dipole The CMB cosmological dipole due essen no_dipole no_dipole tially to the motion of the solar system prediction generic cmb The CMB anisotropies including lensing no_cmb no_cmb ISW and re ionisation effects prediction gaussian nongaussian_fnl SZ effect The Sunyaev Zel dovich emission including no_sz no_sz thermal and kinetic effect prediction dmb nbody hydro hydro dmb galaxy The emission of the galactic inter stellar no_galaxy no_galaxy medium including thermal dust spinning prediction dust synchrotron free free and CO emis simulation sion lines point sources The emission of galactic and extra galactic no_ps no_ps point sources radio and infrared ultracom prediction pact H II
7. For WMAP WMAP For IRAS IRAS_IDEAL IRAS_RIMO They are described in more detail in the next sections 44 14 2 1 HFI_IDEAL The HFI_IDEAL instrument comprises the 6 HFI channels with 6 monofrequency bands at 100 143 217 353 545 and 857 GHz The resolution of each channel is that of the Planck Blue Book Noise for this instrument is generated if the HFI_IDEAL_NOISE is set to nominal default value is none i e no noise The noise is uncorrelated and uniform over the whole sky The noise level is taken from the Planck blue book but can be scaled from the original nominal mission duration of 14 months using the HFI_IDEAL_DURATION keyword in months Table 24 gives the main characteristics of the HFT channels The last three columns give the multiplicative coefficients that permit to change the units of a map from ysz to Komp SZ Compton parameter to thermody namic temperature in Kelvin from Kgy to Komp antenna temperature to thermodynamic temperature and MJy sr to Kcu The numbers given here are obtained for single precision integration they may vary slightly for double precision simulations typically by a fraction of a per cent See section 17 2 for important precisions about the units used in the PSM channel FWHM YSZ2KCMB KRJ2KCMB MJYSR2KCMB 100GHz 10 4 1091199 1 2867296 0 0041880799 143GHz Tel 2 8341320 1 6539019 0 0026324815 217GHz 5 0 019536398 2 9923766 0 0020683517 353GHz 5 6 1
8. In principle nothing should prevent the PSM to run under any IDL version between 7 1 1 and 8 1 2 1 4 astron The PSM uses the IDL Astronomy User s Library astron downloadable from http idlastro gsfc nasa gov ftp The present version of the PSM has been developed with the dec 2010 version of astron Farlier versions can be the source of problems in the handling of fits headers errors in calls to the SXPAR function of the astron package 2 1 5 HEALPix A fully functional installation of the HEALPix package is required In particular the anafast_cxx and alm2map_cxx binaries should be in the execution path The HEALPix package can be downloaded from http healpix jpl nasa gov The present version of the PSM is compatible with version 2 14 and 2 15a of HEALPix 2 1 6 MPFIT The PSM uses the MPFIT fitting library by Craig Markwardt which can be downloaded from http www physics wisc edu craigm id1 fitting html 2 1 7 CAMB For generating a CMB model using CMB power spectra computed from user specified cosmological parameters a fully functional installation of a Boltzman code is needed The default option is to use the CAMB package which can be downloaded from http camb info The present version of the PSM has been developed and tested with the jan 2010 version of CAMB 2 1 8 CLASS CLASS can be used by the PSM as an alternative to CAMB for computing CMB and matter power spectra For ease of use the proper versio
9. Whether to include polarised SZ effect yes no no Table 12 Parameters used by the dmb SZ emission model 9 4 1 SZ_CONSTRAINED When this parameter is set to yes a catalogue of observed clusters as specified with the SZ_INPUT_CAT parameter is produced Clusters in the simulated catalogue that match best the observed ones same bin of mass and redshift location on the sky as close as possible as that of the real cluster are replaced by the observed ones 9 4 2 SZ_INCLUDE_POLARISED This parameter is used to generate SZ polarisation due to the transverse motion of the cluster This feature needs revision for band integration and should not be used at present but can be reactivated if needed Contact Jacques Delabrouille and or Jean Baptiste Melin 9 5 SZ hydro dmb The SZ hydro dmb model merges a low redshift z lt 0 25 full hydrodynamic simulation containing the constrained local SZ map with a high redshift model based on cluster number counts following the method implemented in the dmb model The high redshift dmb part accepts the same keywords as the corresponding model Note that the catalogue of clusters written by the PSM contains only the high redshift objects no catalogue is available yet for the low redshift objects present in the hydro simulation 9 6 SZ nbody hydro The SZ nbody hydro model uses a combination of hydro N body simulations of the distribution of baryons for redshifts z lt 0 025
10. al 2003 MNRAS 342 163 M T p 3 2 E Q 3 2 A E ay e O he 1015 h t Mo T Ao where T is in keV A is the mean overdensity inside the virial radius in units of the critical density and E the Hubble parameter normalized to its present value Under the assumption of clusters being isothermal we use equation 3 so the T parameter to normalise equation 1 or 2 9 2 SZ Catalogue parameters A few parameters are used for the generation of a cluster catalogue They are used by the dmb hydro dmb and prediction SZ models and are listed below 9 2 1 MASS_FUNCTION This parameter defines the model to use for the number density dN dMdz of clusters of mass M at redshift z The references are e Press W H Schechter P 1974 ApJ 187 425 e Sheth R K Tormen G 1999 MNRAS 308 119 e Evrard A E et al 2002 ApJ 573 7 Jenkins A et al 2001 MNRAS 321 372 Tinker J et al 2008 ApJ 688 709 28 keyword name description comments accepted values default MASS_FUNCTION The mass function used to generate the cata press_schechter tinker logue sheth_tormen evrard jenkins tinker CLUSTER_M_INF Lower mass limit of clusters included in the a number be 0 1 catalogue in units of 10 solar masses tween 0 01 and 1 typically SZ_INPUT_CAT List of catalogues of known clusters to be in a list that can rosat sdss cluded in the model sky emission include rosat sdss SZ_RELATIVISTIC Orde
11. eta Be eee as ae BO eA en ee Ae Fee 11 13 INGLUDE RADTO SOURGES a OL LL BO ee AA a ee a 11 14 INCLUDE WMAP SOURCES asno a ee eed Goes aes Wk ee RE A A OE a 1115 INCLUDE UCHI IT SQURGES 3 028 td a st ae HO ie Se eA ee eS 11 1 67 TNCLUDE TRESOURCES 00 va ies ta ah RI ti ald BoE deh ed eds Dig EGS 11 1 7 MEANZTREPOLAR DEGREE 3 coe ravea aoina an oe ok Boe a Oe we ee a a a TL 2 Radio Sources i a oP ek A A ee OO ee A De EA AY ea ee 113 mtrated SOULCES 66 2 3 4nd Son oh Pore es hes td Ak E Bie ce Bo ee ee tee ae e a 114 WMAP sources a e dd a Be Glee ES Ti be UCH SQUECES A 2c 8 a Be wm as ae Ba es Ee es A Ee lo et Bee The Far Infrared Background Band integration and simulated observations 13 1 General parameters of sky observation ee 13 1 1 STRONG SOUURCES lt TULCAT ar eed eg a Ee Se A Poe A Se oe vee a 13 1 2 STRONG SOURCES TO MAP oss o nsi a Oe ee EA a ee ee 1313 GROUP GALAXY e Se a saat here dae ae See ee ae BOSS a ee Su eG fe eS 13 04 GROUP FATENT PS ois oes wera te alae Bow Apa ee ce Re et Sel e T3 0 5 GROUP STRONG PSr ele oe A OR eee Lo Gee eo BOM a ded oo es 13 1 6 OBS TASK iays fe Ae Be A ee ee a a A A A A A e T Lode WHAT OBS ciha h Ae AP A A E to ao TA OE Ae Be RE ae da 131 8 OBS RES ett 5 a Ble ACR da GR ta e 31 31 31 31 31 32 32 32 32 33 33 33 33 33 33 34 34 34 35 13 2 Goadditi n ules s g dii hiite ehyt a a ee dd ad 14 Instruments 14 1 14 2 The PSM_IDEAL
12. in the PSM to model random deviations of the dipole from its nominal amplitude and direction 22 8 Cosmic Microwave Background anisotropies The PSM provides maps and power spectra of the CMB anisotropies temperature and polarisation The output modelled CMB data are stored in the components cmb subdirectory of the PSM output directory The theoretical Ce of the simulation are stored in the cmb_cl fits file and the CMB map and harmonic coefficients are stored in cmb_map fits and cmb_alm fits respectively 8 1 prediction CMB model The CMB prediction selected in the PSM configuration file by setting CMB_MODEL prediction is derived from a CMB map obtained on WMAP 5 year data using a needlet ILC component separation method The predicted CMB temperature anisotropies estimates best in a least square sense the sky CMB emission at the target sky resolution Note that the actual resolution of the map is set by the required sky resolution the resolution of the available CMB observation and the map signal to noise ratio The prediction CMB is a result of a compromise between CMB error and noise contamination in the Wiener sense The input CMB map is the NILC5 map stored in the PSM input ancillary data in Data ancillary observations WMAP NILC CMB 5yr mapilc5yr fits This map is then Wiener filtered to minimize the total RMS error for the target sky resolution The corresponding assumed CMB power spectrum is a default WM
13. number of optional keywords which bypass any equivalent definition of the same keywords in the configuration file 3 2 1 The output_dir keyword All products of the PSM run are written in a directory the output directory specified by the user This output directory is created by the PSM process if it does not already exist The name of the PSM output directory can be passed to PSM_MAIN in two ways Either it can be written in the configuration file QUTPUT_DIRECTORY parameter or it can be supplied as a keyword in the call of PSM_MAIN If the keyword is set it overwrites whatever is written in the configuration file The PSM is launched with the output directory supplied by keyword with the command IDL gt PSM_MAIN config psm output_dir path towards output directory 3 2 2 The check param keyword If the check_param keyword is set in the call to PSM_MAIN the PSM simply prints out information about the input parameters without actually running the code to produce PSM outputs This permits one to check easily prior to running the PSM what parameters will actually be used during the run This is achieved by entering at the IDL prompt the command IDL gt PSM_MAIN config psm check_param 11 3 2 3 The debug keyword There is also a debug mode which bypasses the error catch in component pipes The debug mode as the name indicates is useful for debugging as it permits to find where an error actually occurred Th
14. profile 51500 rvir 5r500 CLUSTER_T_STAR Normalisation parameter T to be used if any number 1 48 NORM_PROFILE is set to no Table 10 Parameters used to model cluster profiles and normalise them 9 1 1 CLUSTER_PROFILE This parameter sets the type of profile used to model the cluster The three dimensional beta profile is given by P r z 1 i 2 with the core radius re depending on the cluster mass and 8 being fixed to 2 3 The xmm and chandra profile are Generalized Navarro Frenk and White profile of the form al 2 P r P n AS c5s001 1 c5001 where x r Rso0 Psoo an analytical formula depending on the cluster mass and redshift and a 3 y being fitted on XMM data Arnaud M Pratt G W Piffaretti R et al 2010 A amp A 517 A92 and Chandra data Nagai D Kravtsov A V amp Vikhlinin A 2007 ApJ 668 1 respectively 27 9 1 2 NSTD_PROFILE When set to yes Po C500 y a and 6 for the cluster profile see eq 2 are set to the values of eq 12 in Arnaud M Pratt G W Piffaretti R et al 2010 A amp A 517 A92 If set to no then values are taken from eq B 2 of the same paper NSTD_PROFILE stands for non standard profile because choosing the values from eq 12 leads to a non standard slope of the Y M relation Y M1 78 while choosing the values from eq B 2 leads to a standard slope Y M3 Values from eq 12 are the best fit
15. regions simulation firb The emission of the background of blended no_firb no_firb extra galactic infrared point sources simulation Table 3 Available models for the different components of sky emission included in the PSM 18 6 Cosmology The PSM produces sky simulations on the basis of an underlying assumed ACDM cosmological model The main parameters of the model are listed in 6 1 These parameters are adjustable by the PSM user and are used as input parameters for running CAMB and or CLASS to compute CMB and or matter power spectra as well as to generate shells of density contrast at various redshifts see 6 2 6 1 Cosmological parameters Cosmological parameters are used in various parts of the PSM sky simulation As much as possible the same set of parameters is used everywhere in the simulation The only exception to this is when pre computed maps of some component are used in which case these specific maps use the cosmological model assumed for their generation which can be different from the global cosmological parameters defined by the PSM user Cosmological parameters are used in particular for the computation of a CMB power spectrum with CAMB in the gaussian CMB model and for the computation of cluster mass functions in the dmb and hydro dmb models of SZ emission Table 4 summarizes the cosmological parameters used by the PSM Note that in principle og can and should be computed from the other parameters Th
16. scalar and tensor power spectra are defined SCALAR_AMPLITUDE Amplitude of scalar modes 2 441e 9 Table 4 Cosmological parameters read out from the configuration file by the PSM 19 6 2 Density fluctuations and cosmic structure Perturbations of the spacetime metric along the cosmic history are of major importance for the PSM Perturba tions in the early universe mostly around the epoch of last scattering 2 1100 give rise to CMB anisotropies Late time perturbations z lt 10 are linked to cosmic structure that defines the distribution of galaxies and clusters of galaxies The PSM uses CAMB and or CLASS to compute CMB temperature and polarisation power spectra lensing potential and matter power spectra at late time The following parameters are used to run CAMB and CLASS during the execution of a PSM run to generate CMB and matter power spectra corresponding to the cosmological parameters listed in 6 1 and to select what is used to compute the matter power spectrum used in the PSM run Table 5 lists the options parameter description comments accepted val default ues RUN_CAMB Whether to compute CMB and matter power spectra yes no no using CAMB RUN_CLASS Whether to compute CMB and matter power spectra yes no no using CLASS CMB_CL_SOURCE Source for CMB Ce and lensing potential standard LCDM CAMB CAMB CLASS COSMO_PK_SOURCE Source for computing the matter power spectrum P z EisHu BBKS
17. strongradiops stronguchii strongwmapps strongercscps e Faint point sources faintirps faintradiops faintuchii faintwmapps faintercscps e The Cosmic Infrared Background firb The ID key PSM_CPID is a unique identification key that is given to the particular component when it is created by the PSM run 54 16 3 PSM observation header An example of a PSM observation header is given in the observed map header displayed on page 53 COMMENT PSM observation header PSM_OBID rWfTLUpiDe6RJUEY PSM observation ID key CMIX1 synchrotron Component included in observation CMIX2 freefree Component included in observation CMIX3 thermaldust Component included in observation CMIX4 spindust Component included in observation CMIX5 co 4 Component included in observation The PSM observation header block comprises an ID key and a number of keywords of the form CMIXz where x is a number Each one of the CMIX keywords is used to specify the name of one component present in the observed map 16 4 PSM map header A typical PSM map header block is COMMENT PSM imap Reader 2 27 2223 25 2222 2H a TSS SS SSS PSM_PXTP HEALPIX Pixelisation type PSM_LMAX 2000 Maximum multipole number PXWIN O Pixel window function The PSM map header comprises a keyword that specifies the pixelisation scheme the PSM_PXTP keyword a keyword that
18. to a collection of blended high redshift infrared sources No parameter exists at present for this component 39 13 Band integration and simulated observations Once a model of the sky is generated the PSM performs band integration of the emissions to generate band integrated maps of components at the resolution of the generated model sky These band integrated sky emission maps are then used to generate simulated observations by instruments with noise added resolution changed and possibly map format changed 13 1 General parameters of sky observation The general parameters specific for band integration only are as follows keyword name description comments accepted values default STRONG_SOURCES_TO_CAT Whether a catalogue of strong point sources yes no yes with fluxes integrated in the band is produced STRONG_SOURCES_TO_MAP Whether a map of strong point sources with yes no no fluxes integrated in the band is produced GROUP_GALAXY Whether to co add all diffuse galactic compo yes no yes nents into a single maps of galactic emission GROUP_FAINT_PS Whether to co add all faint point sources ra yes no yes dio infrared and the FIRB into a single map of point source background GROUP_STRONG_PS Whether to co add all strong point sources yes no yes radio infrared ultra compact H11 into a sin gle map of strong sources Table 19 Parameters specifying the rules for b
19. to multiplying the ag coefficients of its spherical harmonic transform by the HEALPix pixel window function Setting SKY_PIXWINDOW to 1 results in PSM maps to be averaged in pixels of the size specified by HEALPIX_NSIDE and multiplying harmonic coefficients by the corresponding HEALPix pixel window function For all PSM maps and harmonic coefficients files the pixel window function applied to the data is written in the fits header s using the parameter PXWIN in the fits header PXWIN gives the value of nside corresponding to the pixel window function applied to the data i e PXWIN 512 for a map at any nside for which the pixel window function applied is that of a nside 512 healpix map see section 16 5 1 7 WRITE_ANCILLARY If the WRITE_ANCILLARY parameter is set to yes the PSM writes in the ancillary subdirectory of the PMS output directory ancillary catalogues of the PSM point sources infrared sources as they would be observed by IRAS at 100 and 60 microns radio sources as they would be observed at 0 84 1 4 and 4 85 GHz and ultracompact H II regions as they would be observed at all these frequencies The measured ancillary fluxes comprise errors with respect to modelled source fluxes which are compatible with the measurement errors in the actual data These ancillary catalogues are written in the format of IDL save sets 17 5 2 Models for all components The main components generated by the PSM are the CMB dipole dipole
20. used to gener SFD SDFnoHIT ate dust emission FFP6 JD Table 16 Parameters used for generating the thermal dust emission model 10 4 1 1100 The 1100 parameter sets the version of the 100 micron dust template used to generate dust emission The SFD option corresponds to the Schlegel Finkebiner Davies map in HEALPix format at native nside 1024 The default option SDFnoHII corresponds to the same map with ultra compact HII regions subtracted note that the former parameter INCLUDE_ H2REGION used in previous versions is now obsolete and is replaced by the use of 1100 The third option FFP6 JD is a template built from an extrapolation at 100 microns of Planck HFI 857 GHz observations filtered to suppress cosmic infrared background anisotropies and with point sources subtracted That third option is restricted to the Planck collaboration 10 5 Spinning dust Spinning dust emission is included in the sky model if the INCLUDE_SPINDUST parameter is set to yes The spinning dust model uses a single template which is scaled in frequency using a specific emission law The spinning dust template map at 23 GHz is stored in the spindust_amp1 fits output file located in the components spindust subdirectory of the PSM output directory Spinning dust emission is not polarised in the present model keyword name description comments accepted values default SPINDUST_EMISSION_LAW Wh
21. yes then all these maps are co added for each frequency band and are are saved in a single file per frequency band 13 1 4 GROUP_FAINT_PS This parameter is similar to tt GROUP_GALAXY except that it co adds all faint source maps including the far infrared background 13 1 5 GROUP_STRONG_PS This parameter is similar to tt GROUP_GALAXY except that it co adds all strong source maps including the far infrared background 13 1 6 OBS_TASK In addition to the default option of not observing the sky i e doing no integration of the sky model into instrumental frequency bands the PSM offers the possibility to generate a new integrated sky emission or to update an existing one This is set using the OBS_TASK parameter If it is set to update then the code checks for existing band integrated sky maps in the relevant directories of the PSM output and checks whether the current instrumental band is the same as the one stored If the instrumental band is the same and the band integrated sky file already exists then the band integration is not redone Otherwise if either the sky or the band have changed then the band integration is re done and the new band integrated sky emission is saved in place of any already existing band integrated sky emission When instead the OBS_TASK parameter is set to new then all existing observations are erased and re done The update mode is particularly useful for generating new observations of an existin
22. 090741 12 915154 0 0033734774 545GHz 5 15 259461 159 98662 0 017531469 857GHz 5 30 229624 15753 256 0 69813007 Table 24 HFI_IDEAL instrument characteristics 14 2 2 LFI_IDEAL The LFI_IDEAL instrument is very similar in spirit to HFI_IDEAL except that it uses the LFI_IDEAL_NOISE and LFI_IDEAL_DURATION parameters instead Table 27 gives the main characteristics of the LFI channels channel FWHM YSZ2KCMB KRJ2KCMB MJYSR2KCMB 30GHz 33 5 3238063 1 0234751 0 037013687 44GHz 24 5 1799698 1 0510483 0 017670341 70GHz 14 4 7766109 1 1332425 0 0075275633 Table 25 LFI_IDEAL instrument characteristics 45 14 2 3 HFI_BLUEBOOK The HFI_BLUEBOOK instrument differs from HFI_IDEAL only through the shape of the frequency bands which are square instead of monofrequency The HFI_BLUEBOOK_NOISE and HFI_BLUEBOOK DURATION parameters are used to specify the noise properties in the same way as for the HFI_IDEAL instrument channel FWHM YSZ2KCMB KRJ2KCMB MJYSR2KCMB 100GHz 10 4 0649414 1 2993981 0 0041912780 143GHz 7 1 2 7749512 1 6818202 0 0026528442 217GHz 5 0 0014196425 3 0654824 0 0020998274 303GHz 5 5 7909145 12 972937 0 0033580961 545GHz 5 14 024523 143 55841 0 015589777 857G Hz 5 26 833689 9832 7070 0 43183285 Table 26 HFI_BLUEBOOK instrument characteristics 14 2 4 LFI_BLUEBOOK The LFI_BLUEBOOK instrument differs from HFI_IDEAL only through the shape of the frequency ban
23. 9 5 OZ hydrotdmbs ida once ail wed ah aL a eee Suh ee o Gre de ae Sete adh Qe ata 9 6 SZimbodythydro r wra v Mb kode A aed Waele a a ae Sa tes YS The Galaxy 10 1 Galactic polarisation ooo a ee ee ee es 10 151 GAL POLAR MODEL sf ieee SR tel AR oo oe eo Ae god es 10 422 DUST INTRINSIC POL uso a a ER A ee ee 10 4 3 GAL BFEELD PLT GH ANGLE caou e 4 he vk Ge Gb ee BP ee ee Be ee a oe Eee ek 10 14 GAL BFIELD TURB AMPL m me Ra sa ee gk AA A ee a ee he a 10 2 Synchrotrones oe a a id hh he AB Ak amp A doe A RA be ee dg Re bd 10 2 1 SYNCHROTRON_EMISSTON LAW ee 10 2 2 SYNCHROTRON_INDEX_MODEL ee 10 2 3 SSYNCHROTRON CURV FREQ oe i 5 300 a e a Ee pe 10 2 4 SYNCHROTRON CURV AMPL lt lt ooo aa BA Bok WA a a wo a 10 3 Freestre tara E AS ele aut 1 AA AAA AAA ADA i tS 10 3 1 FREEFREE TEMPLATE a popor 2 bbe mh ee eA A Ee ee es 10 3 2 FREEFREECE TEMP OS 2 e ob va Gee Sey er Peon Big a Be ee da Ek ae ee a 10 4 Vhermal dust or RE cd tnt et hy A ee ee oe TOs T1000 a HAR ee Sis en RT Be hat Go Ae eb nt PS 1057 Spinning dust 4 4 ah eA See eae eee Se EG we Eb ea ae oe 10 51 SPENDUST EMISSION LAW lt 3 cet a ee atte a Gb he ee ee a aTi 10 6 CO molecular lines ias Seb ed ae Sine ee be Biba te HS eee Gee PS Point sources 11 1 Parameters of the point source model 2 0 0 0000 ee ee TIA STRONGPS LIMIT FREQ GHZ noui Dardo andere eee ie BARK GB ok Mints BG eke ea 11 12 STRONG PS LIMIT FLUXIY eee og
24. AP fit obtained from running CAMB online on the Lambda web site using the following parameter file available in the PSM ancillary data products and if not already available on the user computer read from the PSM data base upon normal PSM execution Data ancillary models cmb standard_1cdm camb_42481064 ini The CMB power spectrum is read from the output of the CAMB run available in the same data directory either in camb_42481064_lensedcls dat or in camb_42481064_scalc1s dat depending on whether the CMB_LENSING parameter is set to cl or something different in the PSM configuration file This parameter is the only one specifically used for the predicted CMB in addition to all global PSM and sky model parameters described in section 4 3 and 5 1 Note that the choice of Ce lensed or not has no impact on the output CMB map It only impacts the model power spectrum written as an output of the PSM run in the component cmb subdirectory of the ouput directory Note also that on the basis of the theoretical correlation between E and T the CMB prediction model produces not only a best guess for CMB temperature but also for CMB E modes of polarisation In the present version of the PSM the B modes vanish 23 8 2 gaussian CMB model The gaussian CMB model is selected in the PSM configuration file by setting CMB_MODEL gaussian The CMB map produced by the PSM is a random generation of CMB harmonic coefficients aem according to Gaussian st
25. ATA ee ANA A A So ae ee 59 SES PROHEED A A at a Be Begs A A A E es 59 13 2 Instrument structires a aay jaa wena a aa ad Et e De tn 60 18 22 Spectral bands a session Scat ee eee Ee Shoe eR a e a a 61 18212 Detector beams sta ie moe oe beeper Ree Sa eh a EE l A 61 18 2 3 Noise description ias ee ee pane Be Bee eR ee ek a ee SE Dele a 61 18 3 Band integration and color correction o oo a a 61 18 31 Band integration aq d bace kune eta Gow SR ae RS Pay ee ae ee wae 4 61 18 3 2 Color correction coefficients 2 ee 61 1 Foreword 1 1 Overview The Planck Sky Model is a set of programs and data for the simulation or the prediction of sky emission at frequencies ranging from about 3 GHz 10 cm to about 3 THz 100 microns The software is developed mostly in the IDL programming language It uses the HEALPix sky pixellisation package with calls to C and F90 binaries the astron library the CAMB and or CLASS softwares and the MPFIT fitting library The package comes as a collection of component specific simulation codes put together by driver routines automating fastidious tasks like parameter processing and component map coaddition The present document is a user manual that describes some of the PSM features and possibilities The document is regularly updated but is not fully complete as in particular new developments are not documented before their interfaces with the rest of the software have stabilised and be
26. EisHu CAMB CLASS Table 5 Parameters specifying whether CMB and matter power spectra are computed with none either or both of CAMB and CLASS and what is used to compute CMB lensing and matter power spectra in the PSM run The RUN_CAMB and RUN_CLASS parameters are compatible i e it is possible to run both CAMB and CLASS for instance for comparing their outputs or none or one of them only The outputs actually used for generating CMB fluctuations are specified with the CMB_CL_SOURCE parameter The outputs used to compute the matter power spectrum as a function of redshift z are specified with COSMO_PK_SOURCE 6 2 1 RUN_CAMB When the RUN_CAMB parameter is set the PSM run calls the CAMB software to generate CMB and matter power spectra according to the cosmological parameters defined in section 6 1 The PSM generates an input parameter file saved in the cosmo camb subdirectory of the PSM output directory that is used for running CAMB The outputs of CAMB are saved in the same directory They are optionally used for generating the CMB and for computing the matter power spectrum used in some of the models of SZ emission 6 2 2 RUN_CLASS When the RUN_CLASS parameter is set the PSM run calls the CLASS software to generate CMB and matter power spectra according to the cosmological parameters defined in section 6 1 The PSM generates an input parameter file for CLASS saved in the cosmo class subdirectory of the PSM outp
27. MB component The CMB component is saved in the components cmb subdirectory of the PSM output directory The structure produced and used by the PSM code is saved in the cmb sav IDL save set The structure is also printed out in the cmb txt text file for easy checking by PSM users A typical CMB structure print out obtained using the PRTSTRUCT procedure is CMB NAME Was gt STRING cmb CMB TYPE gt STRING comp CMB ID gt STRING MmFsg5TZju6WVbZV CMB CLASS gt STRING diffuse CMB POLARISED 5 53 gt BYTE 1 CMB NLAW Mas gt INT 1 CMB El LAW L gt STRING cmb NUMIN VALUE gt lt PtrHeapVar550 gt FLOAT 0 00000 UNIT gt STRING Hz INFO gt STRING min freq range value NUMAX VALUE gt lt PtrHeapVar551 gt FLOAT Inf UNIT gt STRING Hz INFO gt STRING max freq range value AMPL VALUE gt lt PtrHeapVar552 gt STRING cmb_map fits UNIT gt STRING uK_CMB INFO gt STRING flux at ref freq NUREF VALUE gt lt PtrHeapVar553 gt UNDEFINED lt Undefined gt UNIT gt STRING Hz l INFO gt STRING reference frequency The structure shows that the CMB emission is modelled using one single emission law cmb see section 15 2 4 and stores the name
28. Planck Sky Model User Manual Jacques Delabrouille amp the PSM development team Release version 1 7 8 Contents 1 Foreword VAL WOWEEVIEW A A A A i te rs tes a Ee T AMO ti ha case A RS aby Soak one A aes 4B ee ey e ar a ION By 1 37 About this version s derg a Ra wh we EOP RA EN eek eG ee a Ss 124 Contact elias dl ee Se A he does Tb 26 reditsanid i ask ge Rok BA yah Bate wie Ye ke Ae Sb ee te ae oe 2 Installation Procedure Dil Reqiitenments et Bo a te Be ats ee tee Ren A e a a A ata ee Ae Pc 2 1 Operating System s soria wie ea Aenea Be a we Bee A ee a DNs TWEE Sos Ye ah A AN Ded LDS yet ce eae E ath Ae a Re Ee Be Se Zed ASTON D Aes eh A AA tO Oe ati ay tee oP ee Ae ee oe toe Alb Go a eed Sa a Zo HEALPI Mog 4 ds b Byles ad Ak ahead hat bok EE de tek A a 21 6 MBE o fae sed ode Boek ee ded GMA Sb ek e eG ee BTR eee Di AMB iri Bnd tn O A Stott ETE a pho A EME Nene A hte OOD waite By ARE ANA IGN vlogs ig DES OUASS 48 2 44 eke A A eae wena te Geum eines BD ee eee Oia ert 29 O 2 2 A kb dela bea oo Be OAL ae amp Bete eg bh SER Beene Ee a 2 2 Getting and installing the code 20 Getting PSM data Lt A Sey See ee Ble ee Te ET he a 3 Running the code 3 1 Running the PSM iF fo ae Bed oe ae EE Ee eb ha a ee he gr 3 2 Optional keywords 2 seres soe bose Ae a BG e oe oe GO PR ed apa ew a a2 The output dir keyword aai s wee Gee By ater CY IA EARS AA ie 3 2 2 The check_param keyword
29. SM output directory that are created by the PSM and listed in section 15 1 are emptied and erased unless the carefulness keyword described in section 3 2 is set to 2 4 3 5 VISU The VISU parameter sets whether the PSM run produces output visualisation of the modelled sky components and observed maps It can range from 0 no visualisation to 2 4 3 6 OUTPUT_VISU The OUTPUT_VISU parameter sets the support for visualisation which can be screen png or ps The first two require the X window graphic system device to be operational for your ongoing IDL session png or ps outputs are written in the figures subdirectory of the PSM output directory with self explanatory names Visualisation is useful for checking that the outputs of the PSM run look as expected 4 3 7 SEED The PSM is designed in order to avoid as much as possible unintended correlation between random numbers drawn by different parts of the package while keeping the ability to reproduce simulations The SEED parameter is a long integer which provides the starting point for the random number generator Details on how the seeds are handled by the PSM are given in section 17 4 Note Rerunning the PSM with the same seed but a different set of parameters different nside Imax number of components etc generates a somewhat different sky as the number of random draws depends on the parameters Hence reproducing the same sky requires not only the same seed but the same para
30. UDE_RADIO_SOURCES Set this parameter to include the population of radio sources in the model 11 1 4 INCLUDE_WMAP_SOURCES Set this parameter to include the population of radio sources in the model Note that when this is done a number of sources from the radio catalogue produced from lower frequency data are replaced by sources that match the WMAP measurements Most of these sources however are highly variable so that an experiment observing the sky some years after WMAP is not likely to observe compatible emission from these sources 11 1 5 INCLUDE_UCHII_SOURCES Set this parameter to include a population of galactic ultra compact H I regions 11 1 6 INCLUDE_IR_SOURCES Set this parameter to include a population of infrared sources based on the IRAS observed sources 11 1 7 MEAN_IR_POLAR_DEGREE This parameter sets the level of polarisation of infrared sources for polarised sky simulations 11 2 Radio sources Radio sources faintradiops and strongradiops components in the PSM are modelled as pointlike objects in the sky with a Spectral Energy Distribution SED that depends on frequency as a set of band limited power laws Each radio source is modelled with four distinct power laws that describe their emission below 4 85 GHz between 4 85 and 20 between 20 and 100 and above 100 GHz Each source has its own amplitude and spectral indices Each source has its own polarisation fraction and angle but both are constant for ea
31. _a file to be found in the datafiles spindust directory of the PSM distribution The PSM user can change the spinning dust emission law by modifying the corresponding emit4 jnu extra_a data file and changing the proportion of extra emission recommended only to experimented PSM users The total spinning dust emission law is the sum of the individual emissions of all components in proportions set by the parameters described next The d198 spinning dust emission law default corresponds to 96 2 warm neutral medium and 3 8 reflection nebulae 10 6 CO molecular lines CO molecular line emission is included in the sky model if the INCLUDE_CO parameter is set to yes Currently the model is rather simple one single template part sky coverage only constant line ratio no polarisation The map used for generating CO emission has only part sky coverage 35 11 Point sources Point sources in the PSM are separated into three categories radio sources radiops infrared sources irps and ultra compact HII regions uchii In addition WMAP sources are treated as a special case of radio sources There are two point sources models implemented in the PSM prediction and simulation As many radio sources are variable the prediction model comprises only infrared sources and ultra compact HII regions modelled on the basis of extrapolations of real IRAS sources The simulation model comprises fake faint infrared sources to homogenize the IRAS c
32. alaxy instead of OBS_COADD synchrotron freefree thermaldust spindust co lThe other exception is the INSTRUMENT parameter see section 14 42 14 Instruments The PSM uses for observing the simulated sky simple models of a few relevant instruments Each instrument is described on the basis of a number of channels or detectors with each a specific beam polarisation sensitivity frequency band simplified noise properties and pixelisation scheme Specific instruments implemented in the current version comprise a few different versions of the Planck LFI and HFI of WMAP and of IRAS lowest two frequency channels In addition the software implements a generic simple instrument called PSM_IDEAL which permits the user to define a simplified instrument model Instruments used for band integrating and observing sky emission in the PSM are specified in the PSM configuration file by lines such as INSTRUMENT PSM_IDEAL INSTRUMENT LFI_BLUEBOOK INSTRUMENT HFI_RIMO INSTRUMENT WMAP These keywords specify that in both the skyinbands and observations directories if OBS_TASK is either new or update a subdirectory corresponding to each of these instruments will will contain the catalogues and or maps of emission after band integration if WHAT_OBS is equal to bandinteg or fullobs and as observed by the detectors of the corresponding instrument if WHAT_OBS is equal to fullobs 14 1 The PSM_IDEAL instrument PSM_IDEAL is
33. ameters used for generating the point sources in the PSM 11 1 1 STRONG_PS_LIMIT_FREQ_GHZ Set this parameter to a set of frequencies that will be used to separate between strong and point sources 11 1 2 STRONG_PS_LIMIT_FLUX_JY Set this parameter to a set of limit fluxes in Jy Each of these fluxes corresponds to one of the frequencies set with STRONG_PS_LIMIT_FREQ_GHZ so that the number of specified frequencies and fluxes should be the same Any source that has a flux in excess of the limit at any of the specified frequencies is considered as strong the rest being considered as faint i e those sources that exceed the limit at none of the specified frequencies Maps and catalogues of observed strong sources will contain the same list of sources for all frequencies of observation Note that depending on how these parameters are set there is no guarantee that the sources selected as strong 36 are indeed the strongest ones in all the frequency bands of observation An extreme example would be to set the limit strong vs faint at radio frequencies e g 5 GHz but observing the sky in high frequency bands The PSM would consider as strong some strong radio sources but not any of the strong infrared galaxies that are likely to be the strongest in the observations For safety it is recommended to have at least one radio frequency and one far infrared frequency in the STRONG_PS_LIMIT_FREQ GHZ list as is done by default 11 1 3 INCL
34. an map number used if not drawn at random 26 9 SZ effect The SZ effect due to the inverse Compton interaction of CMB photons with ionised gaz primarily in clusters of galaxies is simulated in the PSM with the superposition of thermal and kinetic SZ effects in a catalogue of galaxy clusters The generation of thermal and kinetic SZ effects in the sky model is turned on by setting to yes the SZ_INCLUDE_THERMAL and SZ_INCLUDE_KINETIC parameters respectively SZ effects are generated in the PSM by two means either by post processing large scale N body and or hydrodynamical simulations of Large Scale Structure to produce catalogues of clusters and maps of thermal and kinetic SZ effects or on the basis of a cluster mass function which provides for a given cosmology as defined by the cosmological parameters described in section 6 the number density dN dMdz of clusters of mass M at redshift z 9 1 SZ Cluster parameters A number of parameters are used to convert mass and redshift into integrated Y parameter or connect X ray observations to Y These are listed below keyword name description comments accepted values default CLUSTER_PROFILE Which type of profile is used to model clusters xmn chandra xmm beta NSTD_PROFILE Whether to use a non standard profile yes no yes NORM_PROF ILE Whether the cluster profile is normalised to yes no yes match the observations PROFILE_BOUNDS Boundary for the
35. and integration Observation parameters that impact the production of coadded maps as seen by the instruments are keyword name description comments accepted values default OBS_TASK Specifies what observation is performed new update none none WHAT_OBS Whether to do only band integration or full bandinteg bandinteg observation fullobs OBS_RES Whether the observations are smoothed or de instr sky sky convolved to put them either at sky resolution or at the resolution of the instrument OBS_COADD Which coadded map s to produce in the see section 13 2 none observations subdirectory Table 20 Parameters specifying the rules for sky observation 13 1 1 STRONG_SOURCES_TO_CAT Strong sources as selected on the basis of the values of the STRONG_PS_LIMIT_FREQ_GHZ and STRONG_PS_LIMIT_FLUX_JY parameters described in section 11 1 can be observed in the format of a catalogue of observed sources Set STRONG_SOURCES_TO_CAT to yes to produce for each instrument channel a catalogue of strong point source observations 40 13 1 2 STRONG_SOURCES_TO_MAP Set this parameter to yes to produce maps of strong point sources for each of the instrument channels 13 1 3 GROUP_GALAXY For the purpose of saving disk space it is possible to avoid writing on disk the maps for individual galactic components synchrotron free free thermal dust spinning dust CO lines If tt GROUP_GALAXY is set to
36. annel of the instrument Less complete but easier to read information can be printed out using the PRINT_INSTRUMENT utility e g IDL gt print_instrument wmap channel FWHM YSZ2KCMB KRJ2KCMB MJYSR2KCMB K N A 5 3756860 1 0137430 0 062373463 Ka N A 5 2974526 1 0284615 0 030738867 Q N A 5 2152334 1 0442069 0 020218388 V N A 4 9356367 1 0999517 0 0096214733 W N A 4 2586475 1 2503038 0 0046056137 Note that for this instrument beams are not Gaussian and hence are not described by a single FWHM per channel hence the N A in the FWHM column of the above printout 18 2 1 Spectral bands 18 2 2 Detector beams 18 2 3 Noise description 18 3 Band integration and color correction The PSM uses several types of emission laws described above in Section 15 2 4 and uses structures that describe spectral bands of instruments such as Planck and IRAS Procedures and functions that combine both types of data for band integration and color correction are implemented in the PSM and are described below 18 3 1 Band integration 18 3 2 Color correction coefficients The COLORCOR function is a very simple tool for computing color correction for POWERLAW and GREYBODY PSM emission laws the call is result COLORCOR band emlaw nuref specind temp double where band is a structure representing a spectral band emlaw is the name of the emission law nuref is the reference frequency for color correction and specind and temp are parame
37. aps will be found in the observations subdirectory of the output in subdirectories corresponding to individual instrument channels Map names will start with group1_map_ group2_map_ etc The list of components included in each map is written in the README file included in each channel subdirectory For instance consider the following lines in the PSM configuration file OBS_COADD allsky OBS_COADD all OBS_COADD synchrotron freefree thermaldust spindust co OBS_COADD synchrotron freefree OBS_COADD faintps strongps OBS_COADD noise These five lines specify that the PSM should produce 5 maps of observed emission for each detector of each instrument For each detector the first map saved in the file named groupi_map_ fits will be the coaddition of all sky emission The second map will be the coaddition of all sky emission and instrumental noise the third the coaddition of the specified galactic components etc Note that coaddition rules will look for the specified sky components in the skyinbands directory If the maps are not present they will not be coadded For instance if the parameter GROUP_GALAXY has been set to yes individual band integrated maps do not exist for synchrotron free free etc Instead there exists a single map of galactic emission It is not possible anymore to make a coadded map of synchrotron and free free only and the coaddition of all galactic components should be specified by OBS_COADD g
38. at emission law should be used to model d198 d198 spinning dust emission d198composition SPD_CNM Proportion of cold neutral medium for spin any number be 0 ning dust emission tween 0 and 1 SPD_WNM Proportion of warm neutral medium for spin any number be 0 962 ning dust emission tween 0 and 1 SPD_WIM Proportion of warm ionised medium for spin any number be 0 ning dust emission tween 0 and 1 SPD_MOL Proportion of molecular clouds for spinning any number be 0 dust emission tween 0 and 1 SPD_DRK Proportion of dark gas for spinning dust emis any number be 0 sion tween 0 and 1 SPD_RN Proportion of reflexion nebulae for spinning any number be 0 038 dust emission tween 0 and 1 SPD_EXTRA Proportion of extra component for spinning any number be 0 dust emission tween 0 and 1 Table 17 Parameters used for generating the spinning dust emission model 10 5 1 SPINDUST_EMISSION_LAW There are two options for the emission law which are selected with the SPINDUST_EMISSION_LAW parameter in the PSM configuration file If this parameter is set to d198composition the average composition of the 34 ISM in terms of cold neutral medium CNM warm neutral medium WNM warm ionised medium WIM molecular clouds MOL dark component DRK reflection nebulae RN are set by the PSM user The d198composition emission law also accepts an extra component EXTRA the emission law of which is tabu lated in the emit4 jnu extra
39. atistics defined by an input CMB power spectrum temperature and polarisation The parameters of the model are specified in table 8 Their impact on the simulated CMB is detailed below keyword name description comments accepted values default CMB_CONSTRAINED Whether the CMB realisation should be con yes no no strained to match the observed CMB CMB_LENSING Method used to do the CMB lensing if any cl ilens none cl Table 8 Parameters used by the gaussian CMB model in the PSM 8 2 1 CMB_CONSTRAINED Setting this parameter to yes amounts to forcing the simulated CMB to match WMAP observations The simulated CMB is then the sum of the predicted CMB described in section 8 1 and of randomly generated missing power On large scales the CMB then essentially matches WMAP observations whereas on small scales it is essentially random Note that in spite of the name of the model the constrained Gaussian CMB map may be detectably non Gaussian since the WMAP map used to constrain the CMB realisation is itself slightly non Gaussian by reason or low level residual foregrounds in the map for instance if nothing else Setting this parameter to no will result in a totally random Gaussian CMB realisation 8 2 2 CMB_LENSING Lensing of the CMB by large scale structure generates small shifts of the CMB temperature and polarisation patterns on the sky This in turn changes the power spectrum of temperatu
40. bed the general parameters that define the global properties of the modelled sky Table 2 summarizes these parameters keyword name description comments accepted values default SKY_TASK Specify the sky modeling task new restore new SKY_RESOLUTION Resolution of sky maps in arc minutes Gaus any positive real 15 sian number SKY_LMAX Maximum value of the modelled sky any positive inte 1536 ger SKY _PIXELISATION Pixelisation used to map the sky HEALPIX HEALPIX HEALPIX_NSIDE nside parameter for sky HEALPix maps 1 2 4 8 16 512 SKY_PIXWINDOW Whether sky maps are sampled at pixel cen 0 1 1 ters 0 or averaged over pixel areas 1 WRITE_ANCILLARY If set to yes some ancillary data is written yes no no in the ancillary subdirectory of the PSM output directory Table 2 Global parameters used by the PSM to model the emission of the sky 5 1 1 SKY_TASK The keyword SKY_TASK sets whether the PSM run should produce a new model of the sky SKY_TASK new or use a model of the sky already existing in the PSM output directory and simply perform the band integration of this pre existing model and its observation with an instrument SKY_TASK restore 5 1 2 SKY_RESOLUTION The keyword SKY_RESOLUTION sets the resolution understood as the size of an hypothetical Gaussian beam at which the component maps should be created Note that the resolution of the map i e an equivalent Ga
41. ber and outputs are stored in single precision 4 3 3 FIELDS The PSM can be run in modes where either only temperature data or both temperature and polarisation data are produced When FIELDS is set to TP the maps of diffuse sky emission are polarised when the corresponding sky emission is polarised and when the relevant parameter is different for T Q and U For instance the map of synchrotron amplitude produced by the PSM will be polarised but the map of thermal SZ effect will not Catalogues of points sources will be polarised When FIELDS is set to T the observations of the sky with instruments output in the observations subdirectory of the PSM output directory will be temperature only irrespective of the polarisation state of the 14 sky model which could have been generated by a previous PSM run in which the FIELDS keyword could have been set to T or of the polarisation capability of the instrument s When FIELDS is set to TP the polarisation state of the observations for each channel depends on both the sky model polarisation and on the polarisation capability of the particular channel However the polarisation state of band integrated sky maps output in the skyinbands subdirectory of the PSM output directory is set by the polarisation state of the sky model irrespective of the polarisation capability of the instrument s 4 3 4 CLEAR_ALL When the CLEAR_ALL keyword is set to yes all the subdirectories of the P
42. ch source across frequencies The model catalogues of radio point sources is stored in the format of an IDL save file in the component ps subdirectory of the PSM output directory There is in general a catalogue for faint radio sources and another one for strong radio sources The total number of modelled radio sources in the PSM is about 2 000 000 11 3 Infrared sources Infrared sources faintirps and strongirps components are modelled as pointlike objects with an SED in the form of a single greybody each Infrared sources are mostly galactic sources and local galaxies Catalogues for strong and faint infrared sources are stored as IDL save sets in the component ps subdirectory of the PSM output directory 37 11 4 WMAP sources WMAP sources are considered as radiosources and treated as such except that they are modelled with an emission al below 4 85 GHz one between 4 85 and 23 one between each of the central frequencies of the WMAP frequency bands 23 33 41 61 and 94 GHz and one above 94 GHz If the parameter INCLUDE _WMAP_SOURCES is set to yes this replaces the modeling of some of the radio sources above 11 5 UCH II sources Ulracompact H II regions are modelled with the sum of two emission laws a greybody for the thermal emission part and a free free emission at radio frequencies 38 12 The Far Infrared Background There is at present one single model of emission for the far infrared background due
43. co ae eA ok Re ee Sa Bae eae O eat ae a aes 2 Oe Soul FONG Se het A A Ae Stink cn a NA we sing Se ey O E A Aya de 8 3 8 DRAW NG MAP NUMBER istiaci qo Pde dee te ee a BR Re ck a eG a a 8 3 9 NG MAP NUMBER MIN 3 0 cack ee a ee we a AA Se ees 8 3 10 NG_MAP_NUMBER MAX ee 3 30 11 NG MAP NUMBER Gu 4 soso A emo be ee Ee AA a Ae eae eS 9 SZ effect 9 1 SZ Cluster parameters sas eased beeen ae eu hea bee ee baad ead a la 9 1 CLUSTER PROF TILE ssf SE AAS A ee he OP ee Be a 9 1 2 NSTD PROFTLE 2 i eae ees PE ae a a A Re aes 97103 NORM PROETEES 26400 ete GR Ree a ane eh Sega he ee es Bee a 9 1 4 PROFILE BOUNDS roa et ok cb che a a ee ee ee 9 1 9 CEUSTER lt TESTAR A a ee ae ted Baw Rata he ee Se A eee 2d aaa 9 2 SZ Catalogue parameters s oe s on E e e a a E E oai a a a O E a EE EEA 9 2 1 MASS FUNCTIONS 5 ot a ea Ge as A Pt a SE ate ne ce ars 9 2 2 CLUSTERMEINE Late ayaa ie Belk ded ada he be he ee ob Eh le EE EG 16 16 16 16 17 17 17 17 17 18 19 19 20 20 20 20 21 22 22 22 10 11 12 13 92 39 SZEINPUTZCAT 2 kai rra ye es id e e A Bop oid dike AT es 5 9 2 4 SZ RELATIVISTIC rta gos Se A ee ee ee ee a 03 OLE prediction sse as rA yere had ly hobs vee oe ea len Be lec ntl he Th a Seok he ten tea ne pets DAY SZ SOMO ds WAN NA ane an eae ae 9 4 SZ CONSTRATINED a Be ae a os Gs A AR ae ee Sa ee a ea Es 9 4 2 SZ INCLUDE POLARISED oia Bow Bowe Bo eS Bee Be eed ee a
44. der The PSM beam header block stores the information about the beam associated with the data stored in the fits file 56 17 Important technical aspects 17 1 Bibliographic information Essential bibliographic information about the model generated is provided in two files which are written at the time of PSM execution in the psminfo subdirectory of the output directory The information about the model used is written in psm_citations txt and the corresponding bibliography in psm bibliography txt Please use the information provided there to give proper credit to the original work that has been used to generate your particular sky model 17 2 Units The PSM uses strict unit conventions that are used in all output data sets Conversion between these units is implemented in a single routine conversion_factor pro in the tools units subdirectory of the PSM software distribution All units can be prefixed by any of the following n u m k M G for nano micro milli kilo Mega Giga and optionally raised to an integer power in which case the unit is in parentheses and postfixed by 2 3 For instance mK_CMB 2 is a valid PSM unit 17 2 1 Brightness units The list of brightness units used by the PSM is Jy sr K_CMB K RJ K KCMB y_sz W m2 sr Hz Conversion from one of these units to another is frequency dependent except f
45. ds which are square instead of monofrequency The LFI_BLUEBOOK NOISE and LFI_BLUEBOOK DURATION parameters are used to specify the noise properties in the same way as for the HFI_IDEAL instrument channel FWHM YSZ2KCMB KRJ2KCMB MJYSR2KCMB 30GHz 33 5 3217640 1 0238649 0 036904771 44GHz 24 5 1757340 1 0518942 0 017625811 70GHz 14 4 7669721 1 1354356 0 0075170747 Table 27 LFI_BLUEBOOK instrument characteristics 46 14 2 5 HFI_RIMO 14 2 6 LFI_RIMO 14 2 7 WMAP 14 2 8 IRAS_IDEAL 14 2 9 IRAS_RIMO 47 15 Description of the PSM outputs 15 1 The PSM output directory All the products of a PSM run are organised in a hierarchy of subdirectories of the PSM output directory A complete PSM output directory comprises the following directory structure OUTPUT_DIRECTORY gt psm gt ancillary gt components gt cosmo gt figures gt observations gt psminfo gt skyinbands cmb co dipole freefree ps spindust synchrotron SZ thermaldust camb class standard HFI_BLUEBOOK HFI_IDEAL HFI_RIMO gt gt gt IRAS_IDEAL IRAS_RIMO LFI_BLUEBOOK LFI_IDEAL LFI_RIMO WMAP gt gt gt HFI_BLUEBOOK HFI_IDEAL HFI_RIMO IRAS_IDEAL IRAS_RIMO The main subdirectories are briefly described above section user s point of view are the components cosmo observations psmin
46. e PSM_MAIN routine is launched in debug mode with the command IDL gt PSM_MAIN config psm debug 3 2 4 The carefulness keyword The PSM_MAIN routine can be run with different levels of carefulness This is done by setting the carefulness keyword By default the PSM is moderately careful overwriting existing files if any and basically trusting the user to know what he she is doing By setting carefulness to 1 moderate care is taken the PSM performs some elementary checks during its execution stopping if an unexpected situation is encountered By setting the carefulness parameter to 2 the PSM is very careful during its execution in particular no existing file is erased Tf carefulness is set to 3 no missing parameter is set to a default value and consistency checks are performed all along the PSM run The carefulness is set by assigning a value to the carefulness keyword e g IDL gt PSM_MAIN config psm carefulness 2 Note At present setting carefulness to a non zero value causes the PSM to crash because of missing information in some file headers This will be fixed ASAP 3 2 5 The verbosity keyword The PSM_MAIN routine can be run with different levels of verbosity This is done by setting the verbosity keyword By default the PSM writes little information on the ongoing processes Set the verbosity keyword to 1 or 2 for increasing amount of information about the run e g IDL gt PSM_MAIN config psm v
47. e among which of these simulation sets the CMB map will be drawn 8 3 2 HI_ELL_EXTEND_GAUSSIAN Set this parameter to yes to extend the CMB to harmonic modes higher than the limit in the original simulation The additional small scales will be Gaussian 8 3 3 READJUST_NG_SPECTRUM Setting this keyword to yes results in scaling the linear scalar modes of the non Gaussian simulation to match the power spectrum corresponding to the cosmology set by the PSM user with the cosmological parameters discussed in section 6 The cosmological parameter set used to generate the non Gaussian simulations is the de fault PSM cosmology corresponding to WMAP 7year BAO H0 The corresponding CMB power spectrum 25 scalar modes is C For a different cosmology we should have instead C If READJUST_NG_SPECTRUM is set to yes then the linear part of the scalar modes of the maps are scaled by lone ie so that the spectrum of the CMB is compatible with the cosmological parameter set used in the simulation If however the keyword READJUST_NG_SPECTRUM is set to no then the cosmological parameters set by the PSM user are overwritten to match those used in the non Gaussian simulation Not also that whether or not READJUST_NG_SPECTRUM is set to yes tensor modes are added to the simulation if the tensor to scalar ratio is non vanishing The CMB_CL_SOURCE parameter see section 6 2 sets the origin of the CMB power spectrum or spectra used to r
48. eadjust the NG CMB power spectrum when the READJUST_NG_SPECTRUM parameter is set to yes 8 3 4 DRAW_F_NL Set DRAW_F_NL to yes to generate the value of fa at random between F_NL_MIN and F_NL_MAX with a uniform probability distribution If DRAW_F_NL is set to no the value of fy is set with the F_NL parameter 8 3 5 F_NL_MIN Set to minimum allowed value of fan if drawn at random The default value is 30 but this number can also be positive 8 3 6 F_NL_MAX Set to maximum allowed value of fp if drawn at random The default value is 30 Note that just as much as F_NL_MIN this number can be negative if requested 8 3 7 FNL This parameter is used to set fy to a fixed value can be positive negative or zero 8 3 8 DRAW_NG_MAP_NUMBER The PSM uses a number of pre generated non Gaussian simulations If this parameter is set to yes the map used in the simulations is drawn at random among available maps 8 3 9 NG_MAP_NUMBER_MIN The lowest map number used for random selection of the non Gaussian simulation Can be fixed between 1 and 1000 for simulations at Imax 1024 and between 1 and 100 for simulations at lmax 3500 8 3 10 NG_MAP_NUMBER_MAX The highest map number used for random selection of the non Gaussian simulation Can be fixed between NG_MAP_NUMBER_MIN and 1000 for simulations at Ima 1024 and between NG_MAP_NUMBER_MIN and 100 for simulations at lmax 3500 8 3 11 NG_MAP_NUMBER This parameter is used to set the non Gaussi
49. ectory will also contain a Data subdirectory in which PSM input data will be copied Add the routines of the package to your path for example path path expand_path PSMROOT Soft Add the astron HEALPix MPFIT and CGIS IDL routines to your path preferably in that order e Make sure a compiled version executables of HEALPix C and F90 routines are in your unix execution path e Optionally download the CAMB compile it and make sure that the executable is in your unix execution path This is necessary for running a PSM simulation with the RUN_CAMB parameter set to yes see section 6 2 e Optionally compile CLASS and or ilens packages both provided in the Soft libraries subdirectory of the PSM software distribution and make sure that the executables are in your unix execution path This is useful for some of the advanced options in the PSM respectively when you set the RUN_CLASS parameter to yes see section 6 2 and when you set the CMB_LENSING parameter to ilens see section 8 2 3 Getting PSM data The PSM software uses a large set of miscellaneous data observations simulations data files describing in struments etc which must be downloaded to the local machine for proper PSM run By default during program execution the PSM checks for the availability of the PSM data sets needed for the simulation If any required data set is not available a request is made to the PSM data base us
50. ent of this directory is completely independent of the instrument or set of instruments ultimately used to observe the sky This directory is itself organised in several sub directories one per component A description of the component outputs can be found in section 15 2 15 1 4 The cosmo directory The cosmo directory contains the inputs and outputs of CAMB and CLASS runs used by the PSM for generation CMB maps and matter power spectra for upcoming versions of the code It contains also files for the present default CMB power spectrum Cy for the current best fit concordance cosmological model 15 1 5 The figures directory The figures directory contains any figures produced during the process of the PSM run The production of these outputs are activated by setting the VISU parameter in the PSM configuration file to any non zero integer and setting the OUTPUT_VISU parameter to png or ps 15 1 6 The psminfo directory The psminfo directory contains information relative to the PSM run duplicates of any configuration file used to produce the simulations present in the output directory a file giving the bibliography relevant to the modelled sky and its observation log files giving the details of the PSM run The configuration files stored in this directory is directly reusable as input configuration files of the PSM to recompute the same outputs see configuration file description in section 4 15 1 7 The observations directory T
51. erbosity 1 3 3 Outputs of the PSM The outputs of the code are sets of maps catalogues of objects IDL save sets and text files The various outputs are organized in subdirectories of the output directory as described in section 15 1 3 4 Consecutive PSM runs It is possible to run the PSM several times in a row using different configuration files but using the same output directory Each consecutive run then updates the content of the PSM output directory according to the instructions given in the parameter file The history of PSM runs for a given output directory is written in the psminfo subdirectory of the output directory All individual parameter files are copied with a naming of the form config n_xxxxxxxxxxxxxxxx psm where n stands for the order of the run in the consecutive run list and xxxxxxxxxxxxxxxxx is a 16 ASCII character code assigned to each PSM run that helps trace the run that produced any particular data product 3 5 Monte Carlo simulations using the PSM At present there is no standard way to generate Monte Carlo PSM simulations i e make many runs with varying input parameters For doing MC simulations one has to write an external piece of software that writes or modifies PSM configuration files and launches the PSM_MAIN procedure with these different configuration files as inputs 12 4 Configuration files Except for the keywords of the PSM_MAIN procedure described in section 3 2 the PSM
52. fo and skyinbands directories The psm directory contains informations private to the PSM run that are used in consecutive runs of the PSM on that output directory Some of this is obsolete The ancillary directory contains ancillary data produced 48 detector_100_1a detector_100_1b K Ka The most important directories from the during the PSM run not used much for the moment The figures directory contains some figures produced automatically by the PSM but this will probably change in the near future 15 1 1 The psm directory The psm directory contains information that is private to the PSM code and in principle is not useful to the PSM user either duplicates information stored elsewhere or is only useful for technical aspects of software implementation 15 1 2 The ancillary directory The ancillary directory contains ancillary data generated during the PSM run if the WRITE_ANCILLARY pa rameter is set to yes in the PSM configuration file Such ancillary data is meant to mimic existing observables currently available which could be used as ancillary data for analysing PSM outputs They are simulations compatible with the model sky generated during the PSM run This feature of the PSM is not fully operational at present only limited ancillary data is generated if any 15 1 3 The components directory The components directory contains all the information concerning the model sky parameters maps catalogues The cont
53. fore they are tested and validated at a reasonable level The PSM is permanently under development Visit the web site regularly for releases of simulation products and of the software package 1 2 Authors The following people have contributed to the PSM project Mark Ashdown Jonathan Aumont Carlo Bacci galupi Anthony Banday Soumen Basak Jean Philippe Bernard Marc Betoule Francois Bouchet Guillaume Castex David Clements Antonio Da Silva Gianfranco de Zotti Jacques Delabrouille Jean Marc Delouis Clive Dickinson Fabrice Dodu Klaus Dolag Franz Elsner Lauranne Fauvet Gilles Fay Giovanna Giardino Joaquin Gonzalez Nuevo Maude Le Jeune Hugo Jim nez P rez Samuel Leach Julien Lesgourgues Michele Liguori Juan Macias Marcella Massardi Sabino Matarrese Pasquale Mazzotta Jean Baptiste Melin Marc Antoine Miville Desch nes Ludovic Montier Sylvain Mottet Roberta Paladini Bruce Partridge Rocco Piffaretti Gary Prezeau Simon Prunet Sara Ricciardi Matthieu Roman Bjorn Schafer Sibylle T chen Luigi Toffolatti 1 3 About this version The version presented in this document version 1 7 8 is the first public release of the PSM code It is identical to v1 7 7 except for a bug fix in one program read_camb_cl pro and minor changes in the documentation This version has been used to generate part of FFP6 simulations for the Planck collaboration 1 4 Contact For questions about the PSM to report bugs or t
54. ful for data of observation type i e for which the PSM_DTTP keyword in the base header is 0BS A typical header for a tophat band such as those used by the Planck HFI and LFI bluebook instrument is COMMENT PSM band header 2222222222120 ROS BD_SHP TOPHAT Band shape e g DIRAC TOPHAT INSTR BD_LNU 9 00000E 10 Band lower frequency BD_UNU 1 15000E 11 Band upper frequency This header stores the shape of the band in the keyword BD_SHP and the lower and upper bounds of the frequency band Different header blocks are implemented for other types of bands instrumental tabulated bands for which BD SHP INSTR monofrequency bands for which BD SHP DIRAC COMMENT PSM band header 3 25 25325 22 2222022 2 SH Sp SS BD_SHP INSTR 7 Band shape e g DIRAC TOPHAT INSTR BD_INSTR HFI_RIMO Instrument for the specified band BD_VERS 20120124 Version for the specified band BD_CHAN F143 Channel for the specified band COMMENT PSM band header 2sSsSSSsse ss aee BD_SHP DIRAC 7 Band shape e g DIRAC TOPHAT INSTR BD_CNU 1 00000E 11 Band central frequency Software tools are available in the PSM to read this information in the fits file headers and convert it into usable band objects that can be used for unit conversion color correction ad band integration 16 8 PSM beam hea
55. g sky in which case it would be used with the SKY_TASK parameter set to restore see section 5 1 13 1 7 WHAT_OBS The observation of the PSM model sky is performed in two steps 1 First integration in frequency bands at the resolution of the sky model This is the bandinteg step 2 Then smoothing if required to the resolution of instrumental channels or deconvolving if the resolution of the instrument is better than that of the sky model although this is not particularly recommended coaddition generation and addition of instrumental noise and reprojection in the pixelisation schem of each instrumental channel This is the fullobs step Set WHAT_OBS to bandinteg to stop at the end of step 1 and to fullobs to stop at the end of step 2 13 1 8 OBS_RES This parameter offers the possibility to produced final observations at the resolution of the sky model rather than that of the instrument It is useful to generate maps at degraded resolution 41 13 2 Coaddition rules The PSM offers flexibility in the production of co added or partially coadded output maps Rules for coaddition are defined using the special parameter OBS_COADD Unlike most parameters defined in the PSM configuration file there can be several instances of OBS_COADD in the instructions Each one of them will then be used to generate one single map of observation containing the emission of one ore more sky components and or of instrumental noise The m
56. he observations directory contains simulated noisy observations of the PSM sky with an instrument or a set of instruments Each observation is stored in a format and in units which are specific to each channel of the instrument and are set in the PSM configuration file 15 1 8 The skyinbands directory The skyinbands directory contains maps of sky diffuse components and or catalogue of point sources as seen after integration of their emission in instrumental frequency bands 49 15 2 Sky model The first step in a PSM run is the creation of the model sky Each component is represented either using maps or catalogues of emission laws The parameters of these emission laws are stored in the components subdirectory of the PSM output directory in a specific subdirectory for each component Outputs relevant to the cosmological model are written in the cosmo subdirectory of the PSM output directory For each component an IDL save set is written in the corresponding component subdirectory e g for the CMB a file cmb sav This save set contains meta information about the component that is used in the following steps to produce maps of band integrated emission This meta information is saved in the format of a structure that contains in particular information about the number of emission laws used to model the component and about the type and parameter values for instance pointers to ag or map files of each such emission law 15 2 1 The C
57. hermal SZ relatsz3 Spectral dependence of the third order relativistic correc none tion to thermal SZ relatsz4 Spectral dependence of the fourth order relativistic correc none tion to thermal SZ dirac Emission line infinitely thin F v Vret x V Vref reference freq Vref Table 28 PSM emission laws 15 3 Band integrated sky emission After generation of the model sky that stores all parameters of all emission components the PSM integrates those components in frequency bands specified by a list of instruments Band integrated components are stored in the skyinbands directory For each instrument there is a sub directory named after the instrument which contains maps and catalogues obtained after band integration 15 4 Observed sky emission 52 16 PSM headers for fits files Significant effort is made to include in the headers of all fits files produced by the PSM the relevant information about the data stored For this purpose headers of fits files written by the PSM comprise a section that is specific to the PSM and contains most of the information useful for describing what is in the data set Software for manipulating PSM headers can be found in the psm fitshdr subdirectory of the PSM software distribution PSM headers are written between two standard delimiting lines between which PSM header blocks carry each a part of the information connected to one particular feature of the data Base headers bl
58. ile_4iT1lo6c24yvriQZ2 fits If you interrupt the execution of the PSM it is possible that a temporary file has been created but the PSM process has been interrupted before the file has been erased It is recommended to check for forgotten temporary files created during the present PSM run using IDL gt PRINT PSM_TMPFILES If necessary erase any forgotten temporary files with the command IDL gt ERASE_TMPFILES This last command erases only files created during the present PSM run To check for and or erase all temporary PSM files including those created by another run of the PSM set the allpsm keyword in the calls e g IDL gt PRINT PSM_TMPFILES allpsm IDL gt ERASE_TMPFILES allpsm This will erase all files matching the standard PSM temporary file format make sure neither you nor a colleague have any other PSM process es writing useful temporary files in the same IDL_TMPDIR before using this command When not set by the user the IDL_TMPDIR default value is the standard directory used for this purpose by the current operating system This can be changed for instance to a personal temporary directory In bash this is done for instance using a command such as export IDL_TMPDIR scratch USER date s Large parallel computers often provide such dedicated space Check with your system administrator what is the correct place to use On personal computers the default value of IDL_TMPDIR is usually a good choice
59. ing wget The data is copied into a subdirectory of the PSMROOT directory called Data PSM data accumulates there as consecutive PSM runs are made see however the use of the GET_DATA parameter in section 4 3 We recommend that users that normally use the PSM on machines connected to the web use this particular feature to let the PSM download only those files that they need for the type of simulations they are doing An alternate option is to retrieve PSM data before any PSM run This is recommended if you install the PSM with the objective or running many PSM simulations with various configuration files Then use the GET_PSM_DATA procedure as follows IDL gt GET_PSM_DATA This however will download the full PSM data directory which contains several sample simulations made with different seeds and amounts to hundreds of GBytes of data It should be avoided if you have only limited storage on your computer e g avoid using this command on your laptop Under normal operation of the PSM software the PSMROOT directory contains at least the PSM software directory Soft and the PSM data directory Data Note that some PSM data is presently restricted to the Planck collaboration Retrieval of such data limited in the present version to somewhat more detailed description of the Planck instrument for Planck specific simulations requires a username and a password Restricted PSM data is obtained with the command IDL gt GET_PSM_DATA priva
60. input parameters setting the configuration of the run are collected into one single parameter file for a given run For a given version of the PSM the parameter file defines completely the output of the code Simulations are then reproducible one merely has to run the same version of the PSM with the same input parameters As mentioned above for this purpose a special version of the input parameter file config psm with all parameters explicitly set to their used values is stored with the output data 4 1 Syntax for editing configuration files Parameter files consist in a set of couples keyword value separated by the symbol Keyword names are case insensitive but keyword values are not e g mJy sr 4 MJy sr All lines starting with a are considered as comment lines and ignored as well as empty lines when the configuration file is read 4 2 User ready configuration files The file config psm in the Soft psm config can be used as an example to set up user specific configuration files Comments explain the role of most of the keywords and the various options 13 4 3 Global parameters of the PSM run This section describes the global parameter keywords used by the PSM run Table 1 summarizes these param eters dedicated to the general setting keyword name description comments accepted values default OUTPUT DIRECTORY Specify the path to the output directory will any valid pa
61. instrument os eso di a a d ee aA a a a a e e a a E a a E E a Specific instruments ete ceeds e E E a A Ga ee e A o eeta ele es 142 1 HET IDEADL amp 6 8 2 dhie tar e Galo aA ated e aa lil AA aiae A 14227 EETSIDEAL 213 G8 4 atta as aie pad e oTa de nea os Breed e al oat ie 14 2 3 HF T BELUEBOOK 4000 E A A A A A ed AS 42d EBTEBLUEBOOK A i en a a e aa id e tern oh 98 te hanes ane apra 1402207 HE T RIMO 426 a ai eti a e ra ida e de e ll or hh Ls Al a e dd 1426 LETERIMO a ia a ea A a a RO A aa LALDARMA A o AN A eee 14 28 TRAS IDEAL m au i a BO eed e eh ee RE Re da 142 9 SIRAS RIMO 22 ale As ae Ledo daa al at Bad Ea te Ge ey ae ec Ss 15 Description of the PSM outputs 15 1 15 2 15 3 15 4 The PSM output directory 4 eaten 6 oh ee a Ee ee 15 11 Thes psm directory s at 22 de Rupr wt ato ae Ea ek De a ee Se eG 1521 2 Th ancillary directory lt se k ees aid 48 were tae me ok eb e G 15 1 3 The components directory eV e A e 15 1 4 The cosmo directory naas dal dd e ie babos AIA a a 15 10 The Tigures IEC i002 e ei ae e a a ee ER E on ae G 15 160 The psminto directory rro a e a a eS Ee AA 15 1 7 The observations directory soo 000 2 ee 15 1 8 The skyinbands directory e o Skyimodel pia uea ct E A Ore LA le SAR BA AA AE E aA 15 2 The CMB component std aeei a a ae Soe ia deals 15 2 2 The CMB dip le sarro db ta E e ee AA EG 15 2 3 COsemission lines sorone e a ld ew A Oe e e DA e A 15 24 Em
62. ion of the PSM CVS repository was used i e it is not a tagged and released version Data generated with the 1 7 4 release will be tagged with PSM_VERS 1 7 4 e PSM_RNID is the identification key for the PSM run All the data produced by the same run will share the same key which will be written in the PSM headers of the fits files e PSM_DTTP is the data type which can be COMP for a component and OBS for an observation e PSM_DTFM is the data format which can be MAP for a map ALM for spherical harmonics CL for a multivariate power spectrum and CAT for a catalogue of objects e Disregard for the moment the other ID keys PSM_DTID and PSM_FLID They are meant to tag the data object for data objects that have several files associated to them and the file itself for cross reference but they are not handled consistently by the PSM yet 16 2 PSM component header A PSM component header block looks typically as follows COMMENT PSM component header PSM_CPNM kineticsz PSM component name cmb synchrotron PSM_CPID pfF8cQoSlpogDcCs PSM component ID key The PSM component header comprises two keywords PSM_CPNM is the name of the component Valid component names are e CMB components dipole cmb Diffuse galactic components synchrotron freefree thermaldust spindust co SZ effects thermalsz kineticsz polarsz Strong point sources strongirps
63. is is not fully implemented for the moment It is up to the user to make sure that the scalar amplitude used to normalise the CMB scalar anisotropies and og used to generate catalogues of SZ clusters both provided as input are compatible with the same cosmological model parameter description comments default T_CMB CMB temperature Kelvin 2 725 H Hubble parameter at present time 0 704 H h Ho 100 with Ho in km s Mpc OMEGA_M Matter parameter density 0 272 OMEGA _B Baryonic matter parameter density 0 0456 OMEGA_NU Neutrino matter parameter density 0 OMEGA _K Curvature parameter Qx This sets the dark energy density pa 0 rameter as pg 1 Ox Om SIGMA_8 Amplitude of matter perturbations at the scale of 8h Mpc 0 809 N_S Scalar spectral index n of primordial fluctuations 0 963 N_S_RUNNING Running of the scalar spectral index ns 0 N_T Tensor spectral index n of primordial fluctuations 0 N_T_RUNNING Running of the tensor spectral index n 0 R Tensor to scalar ratio primordial power at kpivot 0 05 TAU_REION Reionisation optical depth 0 087 HE_FRACTION Helium fraction by mass 0 24 N_MASSLESS_NU Number of massless i e relativistic neutrino species 3 04 N_MASSIVE_NU Number of massive neutrino species 0 W_DARK_ENERGY w parameter for the equation of state of dark energy 1 K_PIVOT The comoving scale kpivo in Mpc at which the amplitudes of 0 002 initial
64. is used only by the fauvet2011 galactic polarisation model It is used to set the geometry of the regular component of the galactic magnetic field used to produce templates of polarised galactic emission from observations of total intensity 31 10 1 4 GAL_BFIELD_TURB_AMPL This parameter sets the relative strength of the turbulent part of the galactic magnetic field as compared to the regular one used only by the fauvet2011 galactic polarisation model 10 2 Synchrotron Synchrotron emission is included in the sky model if the INCLUDE_SYNCHROTRON parameter is set to yes The synchrotron model in the present PSM is modeled on the basis of a single template at 23 GHz which is scaled in frequency with a pixel dependent emission law either power law or power law with curvature A power law synchrotron emission is implemented as gt Bs 2 3 ra Vref and a curved power law synchrotron emission as V 4 Bs 2 Be logy v Vcur l x Vref where 6 is the synchrotron spectral index Vref is a reference frequency for which the synchrotron template is available currently 23 GHz 6 is the curvature amplitude and Veur is a reference frequency for the curvature of the emission law The synchrotron 23 GHz map is stored in the synchrotron_ampl fits file and the spectral index map in the synchrotron_specind fits file both located in the components synchrotron subdirectory of the PSM output directory Synchrot
65. ission laws i 4 a EE A AR A ee ELA AI es Band integrated sky emission a Observed sky emission s ett bide weg Pie ae Pt Se ee WO Se ee elie hee toe Os 16 PSM headers for fits files 16 1 16 2 16 3 16 4 16 5 16 6 16 7 16 8 PSM base header 20 2 eM eh AS A ee pce bo a ee ee ei A PSM component header eiii hake et ed eg A pee ee RR ee eae dk eed PSM observation header PSM map header e i222 dad tee BS ee ds a o a ea ee ae O es PSMialm header sit Ty dd E E A NE Ri ts EI AS A he tee PSM cl header ra al A be a th ee Ee PSM band header Ta did as ler a ho ae ts See e ae anra Ob ee ale alse amp PSM beam header ida ke en RA Ae Boe ee EB oe ES es 17 Important technical aspects 17 1 17 2 17 3 17 4 Bibliographic information serce t amp 2 yeild a Soa ee we SRO ee el EL ae A US ee ee ae alee BT Se ye ie Bd a o a le aR Bd ste hos a ae ae eG 17 21 Brightnessnits 6 s gue n Hoke a e ta eos Gk Se a ew RR Sy He ee ge a wae G 17 22 Mass Units ra go 6 E ek ee AR Ee a ae A a es es 17 2 3 Angle Units 4 40840 a a Rae amp ee a Se Ba ea So ee ee 12d Denoth Units 7 Se Sock bet ai tae Sess pn tas we Se Boek ATA Macca Bee Tempotary files i dni Mend wy ee ee BW Sa tee Be a ee ees Seeds for random number generation e 18 Some useful PSM software tools 59 18 1 Documentation and online help 59 18 11 DOCUMENTatION lA ad nr dA sd A he at eo a AE Pe EnA 59 18 12 PSMHELD 203 ee Li e A
66. ll the channels and a single parameter list specifies whether the pixelisation for the observations is specific to the instrument or the same as the pixelisation of the sky These parameters are listed in Tables 22 and 23 respectively keyword name description comments accepted values default HFI_UNITS Units for all HFI instruments A list of 6 psmunits K_CMB LFI_UNITS Units for all LFI instruments A list of 3 psmunits K_CMB WMAP_UNITS Units for the WMAP instrument A list of 5 psmunits mK_CMB IRAS_UNITS Units for all IRAS instruments A list of 6 psmunits MJy sr Table 22 Parameters specifying the units for the various specific PSM instruments See section 17 2 for details about PSM units keyword name description comments accepted values default HFI_PIX Pixelisation for all HFI instruments instr sky sky LFI_PIX Pixelisation for all LFI instruments instr sky sky WMAP_PIX Pixelisation for the WMAP instrument instr sky sky IRAS_PIX Pixelisation for all IRAS instruments instr sky sky Table 23 Parameters specifying the pixelisation for the various specific PSM instruments The sky option corresponds to maps in the same pixelisation as sky maps specified with the parameters described in section 5 1 The list of currently implemented specific instruments is For the Planck HFI HFI_IDEAL HFI_BLUEBOOK HFI_RIMO For the Planck LFI LFI_IDEAL LFI_BLUEBOOK LFI_RIMO
67. meter file in general 4 3 8 GET_DATA The input data sets used by the PSM are stored on a central repository For proper operation of the PSM some of these data should be copied onto the machine where the PSM is run see section 2 3 The GET_DATA keyword sets the way the PSM run deals with input data sets during the PSM normal execution A value of 0 means that the PSM run stops or fails if required data is missing on disk A value of 1 means that the PSM run automatically tries to download the required data from the PSM data directory and the PSM run fails only if the data retrieval was unsuccessful this is the default option A value of 2 means that for each input file the PSM is checking the data repository for the date stamp of the data to be used If the data stored on the central repository is more recent than the local copy the latter is updated and the previous version is erased Although in principle no data set in the PSM data repository is replaced new files with different names are created instead avoid using GET_DATA 2 if you wish to maintain traceability of preexisting simulations with one particular version of the PSM software PSM users are advised to use responsibly the options of GET_DATA If you plan to run many simulations of the PSM consider downloading the PSM data directory once and for all as explained in section 2 3 15 5 The sky model 5 1 Global parameters of the sky model This section descri
68. n of CLASS to be used with a particular PSM release is included in the PSM distribution in the libraries class subdirectory of the PSM software directory The CLASS software is required to generate far infrared background fluctuations according to the castex2012 model The appropriate version of the CLASS software for the present PSM release is included in the PSM distribution in the external subdirectory of the psm software directory Further information about CLASS can be found in the CLASS website http class code net 2 1 9 CGIS Some software tools included in the PSM software but not used in normal PSM runs call routines from the CGIS library COBE analysis software For full consistency you may opt to include this library in your IDL path The library can be downloaded from http lambda gsfc nasa gov product cobe cgis cfm 2 2 Getting and installing the code The PSM is made available as version tagged and documented releases available at the following URL http www apc univ paris7 fr delabrou PSM psm html To install the PSM e Retrieve and extract the tarball of the code e Adapt your IDL_STARTUP file as follows Define the PSMROOT IDL system variable to point to the root of the package This can be done for instance with the command line DEFSYSV PSMROOT Path Towards PSMROOT The PSM software itself should be installed in a subdirectory called Soft of this PSM root directory the root dir
69. nd galactic latitude By default these parameters match the measurement of WMAP 7 year data release Default values are listed in table 6 keyword name description comments accepted values default DIPOLE_GLON Dipole galactic longitude degrees angle in 0 360 263 99 DIPOLE_GLAT Dipole galactic latitude degrees angle in 90 90 48 26 AMPLITUDE Dipole amplitude mK_CMB any positive value 3 355 Table 6 Parameters used by the PSM to model the CMB dipole 7 2 generic CMB dipole The generic model draws at random the dipole amplitude and coordinates according to Gaussian laws The default distributions are set using the same parameter names as in the prediction model and centered on the WMAP measurement by default table 6 Standard deviations are set with the parameters listed in table 7 and have default values equal to the WMAP measurement error bars Note that these uncertainties are used to generate a random dipole only if the dipole model is set to generic keyword name description comments accepted values default DIPOLE_GLON_ERROR Uncertainty lo on dipole galactic longitude any positive value 0 14 degrees DIPOLE_GLAT_ERROR Uncertainty lo on dipole galactic latitude any positive value 0 03 degrees AMPLITUDE ERROR Uncertainty lo on dipole amplitude any positive value 0 017 mK CMB Table 7 Parameters used by the generic CMB dipole model
70. o suggest modifications please contact Jacques Delabrouille delabrouille apc univ paris7 fr 1 5 Credits Whenever the PSM software and or simulations are used please acknowledge the usage of the PSM as follows The authors acknowledge the use of the PSM developed by the Component Separation Working Group WG2 of the Planck Collaboration and cite the PSM paper Delabrouille et al Astronomy amp Astrophysics Volume 553 id A96 as well as the papers that describe the particular model you have been using see section 17 1 2 Installation Procedure 2 1 Requirements 2 1 1 Operating System The PSM requires a UNIX or LINUX operating system for running shell commands and scripts The PSM software often calls UNIX line commands in IDL programs using the IDL command SPAWN 2 1 2 wget During software execution the PSM uses wget to download useful data sets from the PSM data repository if such data are not already present on the local machine The present PSM version is compatible with wget version 1 12 which should be installed on the machine used for running the PSM 2 1 3 IDL The PSM is mainly composed of IDL scripts which require an IDL development environment The present PSM version has been developed and tested mostly with IDL v7 1 1 Earlier versions of IDL cause a problem when the VISU keyword is set to anything else than 0 because of the usage of the DECOMPOSED keyword to calls to the IDL DEVICE routine
71. ocks store information about the PSM run that generated the data and the data type and format Specific headers blocks exist for alm bands beams cl components maps observations Some are exclusive i e map header blocks are specific to maps alm header blocks to alm data and cl header blocks to cl data Component headers blocks are for component files i e files that are part of a model of a component while observation headers blocks are for observations in a frequency band or at a frequency For example a PSM header of an observed map contains a base header an observation header a map header a beam header a band header as in the following example COMMENT PSM header eA rR ARO AACA kk alo COMMENT PSM pase header 3 9 2 sss SSeS e SSeS tS See PSM_VERS head 4 PSM version used to create the data PSM_RNID BzkMjSH1WHyW1FzR ID key of PSM run which produced the data PSM_DTTP OBS PSM data type COMP or OBS PSM_DTFM MAP A PSM data format MAP ALM CL or CAT PSM_DTID ID key of PSM data PSM_FLID PCcOEejcpXpXWSoL ID key of this file COMMENT PSM observation header PSM_OBID rWfTLUpiDe6RJUEY PSM observation ID key CMIX1 synchrotron Component included in observation CMIX2 freefree Component included in observation CMIX3 thermaldust Component included in observa
72. of the file in which the CMB map is written note that only the base name of the file is stored rather than the full file name including the path The emission law is valid over the full frequency range from 0 to infinity the map is in uK thermodynamic redundant information as this is also written in the header of the fits file The reference frequency for the emission law nuref is not needed here and is not defined in this specific example 15 2 2 The CMB dipole The dipole is saved in the components dipole subdirectory of the PSM output directory The dipole structure is similar to that of the CMB 50 15 2 3 CO emission lines The CO emission is modelled using one map of emission intensity for each one of the J 1 0 J 2 1 and J 3 2 transitions A typical CO line emission structure print out is as follows CO NAME J Se gt STRING co CO TYPE gt STRING comp co ID SS gt STRING 2cKZ9hv53SasHb8L CO CLASS ie gt STRING diffuse CO POLARISED See gt BYTE 0 CO NLAW eee See gt INT 3 co El LAW 0 gt STRING dirac NUMIN VALUE gt lt PtrHeapVari40 gt DOUBLE E 1 1520000e 11 UNIT gt STRING Hz INFO gt STRING min freq range value NUMAX VALUE gt lt PtrHeapVari41 gt DOUBLE 1 1530000e 11 UNIT gt STRING Hz INFO gt STRING max f
73. on XMM data while values from eq B 2 are obtained when forcing the standard dependance of the scaling laws 9 1 3 NORM_PROFILE When set to yes this parameter imposes a normalisation that matches the observations and this irrespective of the fact that the cosmological model used in the PSM simulation may be different from the real one If in contrast NORM_PROFILE is set to no then the normalisation is made according to a theoretical model and uses the normalisation parameter CLUSTER_T_STAR The normalisation is computed from the pressure profiles derived from X ray observations i e using the Po parameter in the equation 2 If NORM_PROFILE is set to no then Po is ignored The NORM_PROFILE parameter is not active if the CLUSTER_PROFILE parameter is set to beta 9 1 4 PROFILE BOUNDS Distance from the cluster center at which it is assumed all the cluster mass is included This also sets the angular distance from the cluster center at which the SZ emission of a single cluster will vanish in the SZ maps The value 5r500 is 5 times the distance at which in the xmm or chandra model of the cluster profile the density of the cluster is 500 times the critical density The value rvir is the virial radius used for the beta model of cluster profile 9 1 5 CLUSTER_T_STAR Normalisation parameter to be used if NORM_PROFILE is set to no or CLUSTER_PROFILE is set to beta CLUSTER_T_STAR is the value of the T parameter in equation 4 of Perpaoli et
74. or the conversion between Jy sr and W m2 sr Hz The conversion_factor pro program provides this conversion for any frequency or for any frequency band Note that the MJy sr units used in the PSM do not assume any spectral shape contrarily to the IRAS convention sometimes used among members of the Planck consortium In the PSM 1MJy sr equals 10720 W m sr Hz with no convention assumed usual definition of units as can be found on wikipedia or elsewhere 17 2 2 Mass units The list of mass units used by the PSM is gram Msun 17 2 3 Angle units The list of angle units used by the PSM is rad deg arcmin arcsec 17 2 4 Length units The list of length units used by the PSM is meter parsec Hence kmeter is a valid PSM unit but kilometer or km are not at least for this release 97 17 3 Temporary files The PSM requires writing and reading temporary files during its execution The directory used for this is set by the environment variable IDL_TMPDIR Temporary files can be large and the execution time of the PSM can depend significantly on the I O rate to write and read them Names for temporary files are generated automatically during the PSM run and are of the form psm_tmpfile_ key ext where key is a randomly generated key comprising 16 characters and ext is the file extension A typical temporary file name can be for instance psm_tmpf
75. orm over the sky and equal to 3 in Kgy units 32 10 2 3 SYNCHROTRON_CURV_FREQ Frequency Veur in GHz for the steepening of the emission law used only if SYNCHROTRON_EMISSION_LAW is set to curvpowerlaw 10 2 4 SYNCHROTRON_CURV_AMPL Amplitude unitless for the steepening of the emission law also used only if SYNCHROTRON_EMISSION_LAW is set to curvpowerlaw 10 3 Free free Free free emission is included in the sky model if the INCLUDE_FREEFREE parameter is set to yes The free free model uses a single free free template which is scaled in frequency using a specific emission law close to a power law with spectral index 0 15 The free free template map at 23 GHz is stored in the freefree_ampl fits output file located in the components freefree subdirectory of the PSM output directory Free free emission is not polarised in the present model The free free model accepts the following additional parameters keyword name description comments accepted values default FREEFREE_TEMPLATE Template free free map dickinson_h alpha mamd2008 wmap_mem mamd2008 FREEFREE_E_TEMP Temperature of free free electrons in K any positive num 7000 ber typically between 4000 and 10000 Table 15 Parameters used for generating the free free emission model 10 3 1 FREEFREE_TEMPLATE Set this parameter to dickinson_h_alpha to use as a free free template a map of Ha emission corrected for dust extinnc
76. overage and extrapolations of radio sources observed at frequencies ranging from 850 MHz to 4 85 GHz All PSM sources are divided in two additional categories strong sources and faint sources Strong source observed maps are created directly at the sky resolution by drawing individual sources in pixel space while faint point source maps are based on distributing the faint sources on single pixels and then convolving the maps with the appropriate gaussian beam in harmonic space 11 1 Parameters of the point source model keyword name description comments accepted values default STRONG_PS_LIMIT_FREQ GHZ Set of frequencies used to separate between a list of frequen 20 1000 strong and faint sources cies in GHz STRONG_PS_LIMIT_FLUX_JY Flux limits in Jy above which sources are con a list of fluxes in 0 1 0 5 sidered as strong must be a list of same size Jy as the list of corresponding frequencies above INCLUDE_RADIO_SOURCES Whether to include radio sources in the sky yes no yes model INCLUDE_WMAP_SOURCES Whether to include WMAP sources in the sky yes no no model INCLUDE_UCHII_SOURCES Whether to include ultira compact H II re yes no yes gions in the sky model INCLUDE_IR_SOURCES Whether to include infrared sources in the sky yes no yes model MEAN_IR_POLAR_DEGREE Mean degree of polarisation of infrared sources any number be 0 01 tween 0 and 1 Table 18 Par
77. phs keyword name description comments accepted values default NG_SIMUSET What set of input simulations to use elsner1024 elsner3500 elsner3500 HI_ELL_EXTEND_GAUSSIAN Whether to add gaussian fluctuations at gt yes no no 3500 READJUST_NG_SPECTRUM Whether the power spectrum of the simulated yes no no non gaussian template should be readjusted to match the expectation for the input cosmolog ical parameters DRAW_F_NL Whether the value of fa is drawn at random yes no no F_NL_MIN Minimum value of fn if DRAW_F_NL yes any number 30 F_NL_MAX Maximum value of fp if DRAW_F_NL yes any number 30 F_NL Fixed value of fn if DRAW_F_NL no any number 10 DRAW_NG_MAP_NUMBER Whether the number of the precomputed non yes no no Gaussian CMB map used is drawn at random NG_MAP_NUMBER_MIN lowest map number if the map number is ran positive integer 1 domly drawn NG_MAP_NUMBER_MAX highest map number if the map number is ran positive integer 1 domly drawn NG_MAP_NUMBER map number used if the map number is not positive integer 1 randomly drawn Table 9 Parameters used by the nongaussian_fn1 CMB model in the PSM 8 3 1 NG_SIMUSET The non Gaussian simulations available in the PSM comprise two sets of maps The first one comprises 1000 maps at maximum harmonic of 1024 and the other one 100 maps at maximum harmonic of 3500 The NG_SIMUSET parameter is used to decid
78. pted values default GAL_POLAR_MODEL What model should be used for galactic po mamd2008 mamd2008 larised emission fauvet2011 DUST_INTRINSIC_POL Intrinsic polarisation fraction of the thermal any number be 0 15 dust emission tween 0 and 1 GAL_BFIELD_PITCH_ANGLE Pitch angle of the galactic spiral arms any angle in degrees 30 GAL_BFIELD_TURB_AMPL Amplitude of the turbulent component of any positive num 0 2 the galactic magnetic field relative to the ber regular component Table 13 Parameters used for generating the model of galactic polarisation 10 1 1 GAL_POLAR_MODEL This parameter sets which model is used to generate the galactic polarised emission The two possible options are based on a 3 D model of the galactic magnetic field If GAL_POLAR_MODEL is set to mamd2008 polarisation templates have been constrained to match WMAP observations and are fixed except for the dust intrinsic polarisation level Tf it is set to fauvet2011 two additional parameters the galactic pitch angle and the relative amplitude of the turbulent to regular part of the magnetic field can be set by the PSM user 10 1 2 DUST_INTRINSIC_POL Intinsic polarisation fraction of thermal dust emission This parameter will scale the dust polarisation templates for both the mamd2008 and the fauvet2011 galactic polarisation models The default value corresponds to 15 intrinsic dust polarisation 10 1 3 GAL_BFIELD_PITCH_ANGLE This parameter
79. r of relativistic corrections to the thermal 0 1 2 3 4 0 SZ effect Table 11 Parameters used to produce the cluster catalogue 9 2 2 CLUSTER_M_INF This parameter sets the lower mass limit of clusters included in the catalogue in units of 1015 solar masses The number of clusters included increases rapidly with decreasing lower mass This impacts the time for generating the SZ maps and the size of the cluster catalogue 9 2 3 SZ_INPUT_CAT This parameter is used to define the catalogues of known clusters that should be included in the simulation It is used by the prediction model in all cases as well as in the dmb model if the SZ_CONSTRAINED parameter of that model is set to yes The rosat catalogue comprises 1743 galaxy clusters with the ROSAT X ray satellite The sdss catalog comprises 13 823 optically selected clusters extracted from the SDSS galaxy survey 215 clusters are common to these two independent catalogues and their emission is modeled on the basis of the ROSAT observations if both catalogues are used 9 2 4 SZ_RELATIVISTIC This parameter sets whether relativistic corrections are taken into account in the model of thermal SZ and at which order The default is 0 non relativistic limit The relativistic SZ effect is currently fully implemented only for the prediction and dmb SZ models In the hydro dmb model high redshift clusters which are generated from number counts with the dmb model are modelled
80. re and polarisation anisotropies CMB lensing can be made in two ways with the PSM either at the level of the theoretical power spectrum or at the level of the maps In the first case the generated CMB will still be Gaussian but the CMB power will be modified to take into account the impact of lensing In the second case unlensed CMB maps are generated first and are subsequently lensed by shifting the temperature and polarisation patterns of the CMB anisotropies Set CMB_LENSING to cl to generate Gaussian CMB maps with a lensed power spectrum and to ilens to generate CMB maps with lensing effect implemented on maps The second option makes use of a map of lensing potential generated on the basis of CAMB power spectra It requires significant memory of order 40 GBytes for lensing polarised maps at HEALPix nside 2048 and for SKY_LMAX 4300 24 8 3 nongaussian fnl CMB model The PSM can produce simulated CMB maps with non gaussianity of the local type Such CMB realisations have been precomputed and are stored in the PSM data repository both at 1max 1024 1000 realisations or at lmax 3500 100 realisations The non Gaussian CMB model assumes a linear plus quadratic model for Bardeen s gauge invariant curvature potential where the contribution of the quadratic term is given by a single parameter fn The parameters of the non Gaussian CMB model are specified in table 8 Their impact on the simulated CMB is detailed in the following paragra
81. req range value l AMPL VALUE gt lt PtrHeapVar142 gt STRING co_ampl10 fits l l UNIT gt STRING MJy sr INFO gt STRING flux at ref freq NUREF VALUE gt lt PtrHeapVari43 gt DOUBLE a 1 1527100e 11 UNIT gt STRING Hz INFO gt STRING reference frequency CO E2 LAW li Sao nea gt STRING dirac NUMIN VALUE gt lt PtrHeapVari44 gt DOUBLE E 2 3050000e 11 UNIT gt STRING Hz INFO gt STRING min freq range value l NUMAX VALUE gt lt PtrHeapVar145 gt DOUBLE 2 3060000e 11 UNIT gt STRING Hz INFO gt STRING max freq range value l AMPL VALUE gt lt PtrHeapVar146 gt STRING co_ampl21 fits l l UNIT gt STRING MJy sr INFO gt STRING flux at ref freq NUREF VALUE gt lt PtrHeapVari47 gt DOUBLE E 2 3053800e 11 UNIT gt STRING Hz INFO gt STRING reference frequency CO E3 LAW lip SaaS oS gt STRING dirac NUMIN VALUE gt lt PtrHeapVari48 gt DOUBLE SS 3 4570000e 11 UNIT gt STRING Hz INFO gt STRING min freq range value l NUMAX VALUE gt lt PtrHeapVar149 gt DOUBLE 3 4590000e 11 UNIT gt STRING Hz INFO gt STRING max freq range value AMPL VALUE
82. rmonic coefficients files the maximum value of the data is written in the fits header s using the fits parameter PSM_LMAX see section 16 5 1 4 SKY_PIXELISATION This parameter sets the pixelisation scheme used to represent the sky model At present only HEALPIX is implemented 5 1 5 HEALPIX_NSIDE Set this parameter to the nside parameter of the HEALPix pixelisation See the SKY_RESOLUTION parameter for a rule of thumb for an appropriate choice of HEALPIX_NSIDE as a function of the sky resolution and of the harmonic band limit SKY_LMAX of the sky model 5 1 6 SKY_PIXWINDOW Maps of the sky can be viewed as a sampled version of the underlying sky emission in the usual sense of the sampling theorem In this case the map value assigned to a given pixel is the sky emission at the center of that pixel Alternatively a map can be viewed as a tiled approximation of the underlying sky in which case each pixel contains the integral of the sky emission in the pixel area On flat 2 dimensional images with equally spaced samples or pixels for properly sampled band limited images the tiled version of the image is obtained by sampling the image convolved with the pixel shaped square kernel The Fourier transform of the tiled image is obtained from the Fourier transform of the sampled image by simple multiplication by the Fourier transform of the kernel On the sphere the integration of sky emission in HEALPix pixels is approximately equivalent
83. ron emission is polarised if the FIELDS global parameter is set to TP keyword name description comments accepted values default SYNCHROTRON_EMISSION LAW What emission law should be used to model powerlaw powerlaw synchrotron emission curvpowerlaw SYNCHROTRON_INDEX_MODEL Model used for the variablility of the syn giardino2002 mamd2008 chrotron spectral index over the sky mamd2008 uniform SYNCHROTRON_CURV_FREQ Reference frequency for synchrotron curva any positive num 23 ture if any in GHz ber typically be tween 20 and 100 SYNCHROTRON_CURV_AMPL Amplitude of the curvature of the syn any number typi 0 3 chrotron emission law cally negative for steepening Table 14 Parameters used for generating the synchrotron emission model 10 2 1 SYNCHROTRON_EMISSION_LAW If this is set to powerlaw then the synchrotron map template is extrapolated using a power law that can be pixel dependent Set to curvpowerlaw for modelling synchrotron with an emission law that steepens at higher frequency 10 2 2 SYNCHROTRON_INDEX_MODEL Two different templates giardino2002 and mamd2008 can be used for modeling a space varying synchrotron spectral index The first model is based on Giardino et al A amp A 387 82 2002 The second is based on Miville Desch nes et al A amp A 490 1093 2008 Finally if SYNCHROTRON_INDEX MODEL is set to uniform the synchrotron spectral index is assumed to be unif
84. specifies the maximum harmonic mode included in the map For HEALPix maps the only implemented map type in the PSM at present there also is a keyword that specifies the window function The value of the latter can be 0 if the map is sampled at the centers of the HEALPix pixels or any power of 2 i e any value of possible HEALPix nside parameter 16 5 PSM alm header A PSM fits file containing spherical harmonics typically comprises 1 or 3 extensions depending on whether the data is polarised or not The PSM alm header block looks typically as follows COMMENT PSM alm header ALM_FLD T 2 Name of alm field stored in this extension PSM_LMAX 1200 Maximum multipole number PXWIN 512 Pixel window function Fields are typically T E and B for polarised harmonic modes for a polarisation observation Lensing potential alms are labelled with ALM_FLD P The other keywords are the same as those used in map header blocks 16 6 PSM cl header A PSM fits file containing a multivariate power spectrum comprises a cl header block such as COMMENT PSM cl header PSM_LMAX 3500 Maximum multipole number PXWIN O Pixel window function 55 16 7 PSM band header Band headers in the PSM store the information about the frequency band associated with the data stored in the fits file This PSM header block is use
85. t STRING gt WMAP VERSION gt STRING Tyr NAME gt STRING K BAND SHAPE gt STRING gt DIRAC NU_C gt FLOAT 2 30000e 10 INTEG_DNU gt DOUBLE 1 0000000 BEAM TYPE gt STRING gt INSTR INSTR gt STRING gt WMAP VERSION gt STRING 7yr CHANNEL gt STRING 7K PIX PIXTYPE gt STRING gt HEALPIX NSIDE gt LONG 512 NPIX gt LONG 3145728 ORDERING gt STRING NESTED OBJECT gt STRING gt FULLSKY FIRSTPIX gt LONG 0 LASTPIX gt LONG 3145727 INDXSCHM gt STRING IMPLICIT COORDSYS gt STRING 9G STOKES 0 gt STRING TQU OBS_UNITS gt STRING gt mK_CMB CONVERSION YSZ2UNITS gt DOUBLE 5375 6860 KCMB2UNITS gt DOUBLE 1000 0000 KRJ2UNITS gt DOUBLE 1013 7430 MEGAJYSR2UNITS gt DOUBLE 62 373463 60 Here only the first channel information has been reprinted Note that units used for the standard observations in each channel as well as main unit conversion coefficients are included in the description of each ch
86. te Upon this command you will be asked for a username and password available only to members of the Planck collaboration 10 3 Running the code 3 1 Running the PSM All the parameters of the simulation code are set in the single text configuration file specified as an argument to PSM MAIN By default if no argument is present the PSM runs using the config psm configuration file which is found in the PSMROOT Soft psm config directory For using your own configuration file copy config psm to your favorite directory for PSM configuration files rename it if you wish e g myconfig psm edit it to suit your needs and use it as input to PSM_MAIN as specified below To run the simulation within the IDL environment call the PSM_MAIN routine with the name of the parameter file provide either full path or relative path e g IDL gt PSM_MAIN full path towards config file myconfig psm or for instance if the configuration file you wish to use here myconfig psm is in your working directory simply IDL gt PSM_MAIN my_config psm Upon execution the PSM software looks for the specified configuration file on the local disk If a simple filename is provided the configuration file is looked for in the working directory first and if no such file is present the PSM looks for the configuration file in the PSMROOT Soft psm config directory 3 2 Optional keywords The PSM_MAIN routine can be launched with a
87. ters of the emission law For instance first define a band using the GET_BAND_STRUCT procedure band GET_BAND_STRUCT INSTR instr HFI_RIMO version DX9 v1 channel 857 1 then find the color correction at 857 GHz for a greybody modified blackbody with temperature and spectral index T 10K and a 1 6 using PRINT COLORCOR band GREYBODY nuref 857e9 specind 1 6 temp 10 The result is 1 0140338 The brightness in MJy sr or W m sr Hz at the reference frequency 857 GHz here is obtained from the average brightness in the same units within the spectral band of detector 857 1 of version DX9 v1 of the HFI RIMO by multiplication by the output of COLORCOR i e 1 857 GHz 1 0140338 x h w L dv 5 0 where h v is the normalised i e tee h v dv 1 spectral band of interest 61 Acknowledgements The PSM project has benefitted from useful discussions with Karim Benabed Rodney Davis Francois Xavier D sert Hans Kristian Eriksen Frode Hansen Lauro Moscardini Francesca Perrotta Stephen Serjeant Grazia Umana Benjamin Wandelt We thank the PSM users who have been testing the consecutive versions of the package and have helped validating simulation outputs and finding fixing some of the bugs We thank in particular Charmaine Armitage Julian Borrill Jason Dick Joanna Dunkley Maxence Fournier Fr d ric Guilloux Martin Reinecke Mathieu Remazeilles and Gra a Rocha 62
88. th PSM_OUTPUT be created PRECISION Floating point precision of the output maps single double single FIELDS Model and process temperature only or both T TP T temperature and polarisation CLEAR_ALL Erase all existing directories and files in the yes no no PSM output directory VISU Level of visualisation of PSM outputs 0 1 2 0 OUTPUT_VISU On what support is the visualisation made screen png ps screen SEED Specify the seed for random number genera any positive long 1 tion integer GET_DATA Option for getting PSM data during the 0 1 2 1 run 0 no retrieval 1 get data if missing on local disk 2 update data if repository more recent Table 1 Global parameters of the PSM run 4 3 1 OUTPUT_DIRECTORY The following line sets the name of the output directory to be My_PSM_run in your current working directory the directory from which the PSM is launched OUTPUT_DIRECTORY My_PSM_run 4 3 2 PRECISION Setting PRECISION to double results in almost all PSM calculations being done in double precision 8 bytes per real number In addition some approximations are bypassed integrals are computed using more integration points and output data are written in double precision requiring about twice the disk space When PRECISION is set to single some calculations are still made in double precision whenever necessary but overall most of the calculations are performed in single precision 4 bytes per real num
89. the easiest simplest and most flexible instrument implemented in the PSM It is fully described by a set of frequencies and corresponding beams polarisation properties and noise levels Maps are always produced in the same pixelisation as the sky model itself and frequency bands are infinitely thin keyword name description comments accepted values default OBS FREQUENCIES A list of frequencies in GHz Any list of numbers No default value OBS_RESOLUTION A list of beam sizes in arcminutes Any list of numbers No default value OBS_STOKES Specifies whether the observations in that T TQU T band are polarised or not OBS_UNITS Units of the maps See section 17 2 for any PSM brightness mK RJ details about PSM units unit psmunit PSM_IDEAL_NOISE Noise for the PSM_IDEAL instrument nominal none none T_NOISE_LEVEL Noise level for temperature observations Any list of numbers 0 P_NOISE_LEVEL Noise level for polarisation observations Any list of numbers 0 NOISE_UNITS Units for the noise per square degree See String of the form uk RJ deg section 17 2 for details about PSM units psmunit deg Table 21 Parameters specifying the PSM_IDEAL instrument 43 14 2 Specific instruments Specific instruments implemented in the PSM are models of the Planck LFI the Planck HFI WMAP and IRAS For all versions of any of these instruments a single parameter list specifies the observation units for a
90. the local universe and of pure N body simulations of dark matter structures in a Hubble volume The model uses pre generated SZ maps of thermal and kinetic SZ and uses them as templates of SZ emission This model requires no additional parameter 30 10 The Galaxy Emission from the galactic interstellar medium is constituted of 5 main components synchrotron free free thermal dust spinning dust and CO molecular lines Subdirectories named synchrotron freefree thermaldust spindust and co of the component subdirectory of the PSM output directory are created upon PSM execution and contain maps and structures describing each of the emissions individually There are at present two models of galactic emission the prediction and simulation models Both of them are based on the same input galactic templates but the simulation model generates random small scale structure that is added to the synchrotron free free and thermal dust templates if the sky resolution of the PSM run is smaller than the resolution of the available template 10 1 Galactic polarisation The polarisation of galactic diffuse emission can be modelled according to two main prescriptions either fol lowing Miville Desch nes et al 2008 or Fauvet et al 2011 The models are tightly connected Table 13 highlights the parameters that specify the modelling of polarised galactic emission in the PSM keyword name description comments acce
91. tion CMIX4 spindust Component included in observation CMIX5 co Component included in observation COMMENT PSM map header 222290071 eS Se Ae PSM_PXTP HEALPIX Pixelisation type PSM_LMAX 200 Maximum multipole number PXWIN O Pixel window function COMMENT PSM beam header gt eae eon St Se ass BEAMTYPE GAUSSIAN BEAMSIZE 180 000 Beam size in arcminutes COMMENT PSM band header 222999 RI aoe BD_SHP INSTR Band shape e g DIRAC TOPHAT INSTR BD_INSTR HFI_RIMO Instrument for the specified band BD_VERS FFP4_bandpass only Version for the specified band BD_CHAN 100_1la Channel for the specified band COMMENT End of PSM header akooo A AAI kkk k kkk 53 16 1 PSM base header A PSM base header block looks typically as follows COMMENT PSM base header 2 22 2025 2253222 52 2292122922 2 PSM_VERS head 4 PSM version used to create the data PSM_RNID cULvKukO0bFipESwb ID key of PSM run which produced the data PSM_DTTP COMP PSM data type COMP or OBS PSM_DTFM MAP PSM data format MAP ALM CL or CAT PSM_DTID pfF8cQoSlpogDcCs ID key of PSM data PSM_FLID yjYA17A8Arf4hMba ID key of this file The PSM base header comprises 6 keywords e PSM_VERS is the version of the PSM code In the kinetic SZ example above the head vers
92. tion as derived in Dickinson et al MNRAS 341 369 2003 to wmap_mem to use the WMAP MEM free free map from Bennett et al and to mamd2008 to use a composite map that uses the former over most of the sky but uses the latter in regions where the extinction is E B V gt 2 or Ay gt 6 and uses the WMAP MEM map also when it is lower than the free free predicted from the Ha emission 10 3 2 FREEFREE_E_TEMP The free free emission law depends slightly on the temperature of the warm medium Set FREEFREE_E_TEMP to the assumed temperature in Kelvin 7000 K is the default 10 4 Thermal dust Thermal dust emission is included in the sky model if the INCLUDE _THERMALDUST parameter is set to yes It is modeled on the basis of the coaddition of two greybodies with fixed emissivity spectral indices and with each an amplitude template map and a temperature map The amplitude maps are stored in thermaldust_ampl11 fits and thermaldust_amp12 fits and temper ature maps are stored in thermaldust_temp1 fits and thermaldust_temp2 fits All the above maps are written in the components thermaldust subdirectory of the PSM output directory When the FIELDS global 33 parameter is set to TP the dust amplitude maps are polarised but the temperature maps are not the emission laws are assumed the same in temperature and polarisation default SDFnoHII keyword name 1100 description comments accepted values Which 100 micron template is
93. ussian smoothing applied to the full resolution sky is different from the pixel size which is set with HEALPIX_NSIDE and from the resolution of the instrument s observing the sky In the PSM the SKY_RESOLUTION parameter exists for making sure that all maps are properly sampled For a proper simulation pipeline the resolution should be of the order of or smaller than the resolution of the final observations The sky pixel size should then be about 1 3 of the map resolution or smaller For instance a resolution of 5 arcminutes corresponds approximately to 1max 4000 but larger Imax is preferable for accurate simulations and nside 2048 It is possible to set the sky resolution to 0 If this is done it is recommended that you generate the sky model with large HEALPIX_NSIDE and large SKY_LMAX to avoid aliasing due to improper sampling Note that ringing around strong point sources is then be expected in the final observations if strong point sources are co added in the final observation maps 16 5 1 3 SKY_LMAX Many of the PSM maps are generated in the harmonic domain Spherical harmonic transforms are used to change the resolution of the maps whenever necessary The SKY_LMAX keyword sets the harmonic band limit of the PSM simulation For specific components e g the dipole the actual maximum multipole order can be lower but no map of the sky will have non vanishing harmonic coefficients at larger than SKY_LMAX For all PSM maps and ha
94. ut directory The outputs of CLASS are saved in the same directory They are optionally used for generating the CMB and for computing the matter power spectrum used in some of the models of SZ emission 6 2 3 CMB_CL_SOURCE This parameter sets the origin of the CMB power spectrum or spectra used to generate the CMB The standard_LCDM option uses the current best fit model CMB power spectrum described in section 8 1 The CAMB option uses the outputs of CAMB and the CLASS option the outputs of CLASS to generate the CMB and lensing 20 potential C In the last two cases the cosmological parameters described in section 6 are used to generate the CMB temperature and polarisation power spectra 6 2 4 COSMO_PK_SOURCE This parameter sets the origin of the matter power spectrum P k The default value is EisHu in which case the approximation of Eisenstein and Hu is used The other cases are not fully implemented or tested yet 21 7 The CMB dipole The CMB dipole is an important term of sky anisotropies in the millimeter wavelengths range It can been used for absolute or relative calibration of CMB observations Two distinct models of CMB dipole emission are implemented in the PSM prediction and generic The output modelled dipole data are stored in the components dipole subdirectory of the PSM output directory 7 1 prediction CMB dipole The prediction model generates a dipole with user defined amplitude galactic longitude a
95. with relativistic correction included The low redshift map however is computed at first order only non relativistic thermal SZ for the moment 9 3 SZ prediction The SZ prediction model includes only expected signals from the clusters included in the catalogues specified with the SZ_INPUT_CAT parameter The parameters CLUSTER_PROFILE NORM_PROFILE PROFILE_BOUNDS and CLUSTER_T_STAR are active for this model This model generates only thermal SZ effect 9 4 SZ dmb The SZ dmb model generates first a catalogue of galaxy clusters according to the mass function specified by the MASS_FUNCTION parameter For each cluster the expected SZ signal is computed on the basis of a physical model linking mass and redshift to electron density and temperature on the basis of the spherically symmetric profile specified with the CLUSTER_PROFILE parameter Cluster are distributed at random over the 47 of the sky with a uniform probability To each cluster a velocity is assigned as a function of its redshift assuming 29 linear growth of structures The 3 D velocity vector is drawn at random given the variance of the velocity field at that redshift for the given cosmological parameters This model accepts two additional parameters SZ_CONSTRAINED and SZ_INCLUDE_POLARISED keyword name description comments accepted values default SZ_CONSTRAINED Whether the catalogue contains real observed yes no no clusters SZ_INCLUDE_POLARISED

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