M. López-Caniego Cavendish Laboratory University of Cambridge Detection of Point Sources in Maps of the Cosmic Microwave Background Radiation using Linear Filters

Outline M. López-Caniego Cavendish Laboratory University of Cambridge Introduction Study the performance of three different filters detecting point sources at the 9 Planck frequency channels: Matched Filter Mexican Hat Wavelet Mexican Hat Wavelet 2 Application of these results to WMAP data:.- WMAP 3yr Non-Blind Analysis: NEWPS Catalogue of 380 PS.- WMAP 5yr Blind + Non-Blind Analysis: NEWPS-5yr Catalague 516 PS Detection of SZ clusters using the Matched Multifilter Conclusions

INTRODUCTION M. López-Caniego Cavendish Laboratory University of Cambridge INTRO

INTRODUCTION M. López-Caniego Cavendish Laboratory University of Cambridge INTRO One of the main objectives of Planck will be to produce a map of the Cosmic Microwave Background radiation (CMB), a relic radiation from the Big Bang that was produced when the Universe was only years old. In particular, we are interested in the so-called anisotropies of the CMB, fluctuations of 1 part in a million from the mean temperature field of 2.73 Kelvin.

INTRODUCTION M. López-Caniego Cavendish Laboratory University of Cambridge INTRO One of the main objectives of Planck will be to produce a map of the Cosmic Microwave Background radiation (CMB), a relic radiation from the Big Bang that was produced when the Universe was only years old. In particular, we are interested in the so-called anisotropies of the CMB, fluctuations of 1 part in a million from the mean temperature field of 2.73 Kelvin.

The detection of extragalactic point sources in maps of the Cosmic Microwave Background is very important: Our knowledge of the populations of galaxies at frequencies >5 GHz is very poor. In particular, in the range of frequencies observed by Planck. The resolved and unresolved point sources contaminate the data and we need to do something with them (mask, substract,calibrate the effect etc). When Planck is launched and starts sending data, it will yield a wealth of information about EPS, but untill then we have to work with the best all-sky available data, WMAP. Several methods to detect point sources have been proposed:.- Bayesian methods ‏.- Linear filters (Matched Filters, Mexican Hat Wavelets 1 & 2, Scale Adaptive…)‏.- Combination of Linear Filters + Bayesian Detectors We are comparing some these methods with realistic Planck Simulations within the Planck WG2 and CSI (Cambridge-Santander-IPAC (Caltech)) collaboration (G. Rocha) INTRODUCTION M. López-Caniego Cavendish Laboratory University of Cambridge INTRO

INTRODUCTION M. López-Caniego Cavendish Laboratory University of Cambridge INTRO WMAP Science team. 5yr data 390 Point Sources, Wright et al. 2008

Comparison of filters for the detection of point sourceson Planck Simulations M. López-Caniego Cavendish Laboratory University of Cambridge Comparison of filters for the detection of point sources in Planck simulations López-Caniego, M.; Herranz, D.; González-Nuevo, J.; Sanz, J. L.; Barreiro, R. B.; Vielva, P.; Argüeso, F.; Toffolatti, L..2006, MNRAS, 370, 2047L INTRO PLANCK SIMULATIONS

The Simulations: Freq (GHz) # Im Size FWHM (‘) Pix Size (‘)‏ x ’ x x x x x x x x M. López-Caniego Cavendish Laboratory University of Cambridge INTRO PLANCK SIMULATIONS

Simulations: Galactic components and SZ Clusters (Reference Sky)‏ 1.Thermal Dust2.Synchrotron 3. Free-Free4.SZ Clusters M. López-Caniego Cavendish Laboratory University of Cambridge INTRO PLANCK SIMULATIONS

Simulations: Foregrounds patch extraction 70 GHz Foregrounds map We obtained 12 patches that will be used in the simulations M. López-Caniego Cavendish Laboratory University of Cambridge INTRO PLANCK SIMULATIONS

Simulations: noise reduction and large scale structure removal += = M. López-Caniego Cavendish Laboratory University of Cambridge INTRO PLANCK SIMULATIONS

A) The Matched Filter Filters: Matched Filter & Wavelets M. López-Caniego Cavendish Laboratory University of Cambridge INTRO PLANCK SIMULATIONS B) The Mexican Hat Wavelet Family MHW and MHW2 (1 st / 2 nd order Laplacian of the Gaussian)‏ Gaussian, MHW, MHW2 & CMHW in Real and Fourier space:

A) The Mexican Hat Wavelet used as a filter Proportional to the Laplacian of the Gaussian function. In 2D: B) The Mexican Hat Wavelet Family MHW and MHW2 (1 st / 2 nd order Laplacian of the Gaussian) CMHW (such that we have a perfect reconstruction of any function in R 2 at any scale). Gaussian, MHW, MHW2 & CMHW in Real and Fourier space: M. López-Caniego Cavendish Laboratory University of Cambridge Filters: Matched Filter & Wavelets INTRO PLANCK SIMULATIONS

Filters: Comparison of the MHW1 and MHW2 with the MF M. López-Caniego Cavendish Laboratory University of Cambridge INTRO PLANCK SIMULATIONS

Filters: Ringing effects with the Matched FIlterFilters: Ringing effects MF vs. MWH2 M. López-Caniego Cavendish Laboratory University of Cambridge Theoretically the matched filter is optimal (among the class of linear filters) in the sense of signal- to-noise ratio amplification In practice, implementation issues degrade the performance INTRO PLANCK SIMULATIONS

Another example of dramatic border effects introduced by the a very bright source in the edge of the patch after being filtered with a Matched Filter. Further work need to be done to improve the estimation of the P(k). Filters: Ringing effects with the Matched FIlterFilters: Ringing effects MF vs. MWH2 M. López-Caniego Cavendish Laboratory University of Cambridge INTRO PLANCK SIMULATIONS

Results M. López-Caniego Cavendish Laboratory University of Cambridge INTRO PLANCK SIMULATIONS

M. López-Caniego Cavendish Laboratory University of Cambridge INTRO PLANCK SIMULATIONS

M. López-Caniego Cavendish Laboratory University of Cambridge

We have compared the performance of three filters (MHW1, MHW2, MF) when dealing with the detection of point sources in maps of the CMB. We have performed 145 simulations (area: half sky) with the characteristics of the 9 Planck frequencies. We have found that the MHW2 and the MF outperform the MHW1 in several aspects. The MHW2 is comparable to the MF in almost every aspect. The “problematics” with the MF in the plane and in particular on the sphere make this result a very important one. One can deal with most of these problematics on a one-by-one approach. M. López-Caniego Cavendish Laboratory University of Cambridge INTRO PLANCK SIMULATIONS Conclusions :

A new radio source catalogue obtained with the MHW2 from the three-year WMAP data M. López-Caniego Cavendish Laboratory University of Cambridge Non-blind Catalog of Extragalactic Point Sources from the Wilkinson Microwave Anisotropy Probe (WMAP) First 3 Year Survey Data. López-Caniego, M.; González-Nuevo, J.; Herranz, D.; Massardi, M.; Sanz, J. Luis; De Zotti, G.; Toffolatti, L.; Argüeso, F. ApJS, 2007, Volume 170, Issue 1, pp Blind and Non-Blind source detection in WMAP 5-year maps Massardi, M.; López-Caniego, M.; González-Nuevo, J.; Herranz, D.; De Zotti, G.; Sanz, J. L.; Submited to MNRAS. INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND

What are the advantages/disadvantanges of a BLIND and NON-BLIND search: NON-BLIND: - The position of the object is known, and only the flux must be estimated. - Better estimation of the noise in the vicinity of the source - Catalogues produced in this way may be easily be incomplete, depending on the selection criterion used to construct them: –surveys at other frequencies (mostly low frequency). –different angular resolution. –variability, observation at different epochs –Low freq surveys may miss strong inverted sources. –High resolution experiments may miss extended sources, etc. BLIND: 2 additional parameters for the source position must be found, and below a certain flux level the number false objects that appear as point sources increases rapidly, affecting the reliability. Two complementary approaches : BLIND or NON-BLIND M. López-Caniego Cavendish Laboratory University of Cambridge INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND

WMAP Team has produced 3 catalogues of point sources: –(WMAP1) 1 year data: detected 208 sources (Bennett C. L., et al., 2003, ApJS, 148, 97). –(WMAP3) 3 years data: detected 323 sources (Hinshaw et al. ApJS 170, , 2007)‏ –(WMAP5) 5 years data: detected 390 sources (Wright et al ApJS submited). Nie & Zhang 2007: clean the 1st year maps and look for sources in the residual maps. 101 sources, 26 (25) of them new to WMAP1 (WMAP3). Chen & Wright 2008: combine the 61 and 94 maps to cancel the CMB, detected 31 (64 in 3 yrs data) sources, 21 of them new to WMAP3. Wright 2008: using the same method as before, detected 99 sources outside |b|>10, 64 in WMAP5, 17 new, 17 Galactic and 1 unidentified object. Some recent BLIND works detecting Point Sources in WMAP: M. López-Caniego Cavendish Laboratory University of Cambridge INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND

Recent NON-BLIND works detecting Point Sources in WMAP: Lopez-Caniego et al. 2007: NEWPS catalogue using WMAP 3 year data M. López-Caniego Cavendish Laboratory University of Cambridge Our NON-BLIND approach in the WMAP 3 year data: INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND

Recent NON-BLIND works detecting Point Sources in WMAP: Lopez-Caniego et al. 2007: NEWPS catalogue using WMAP 3 year data Non-blind:positions of known sources observed at low frequency surveys. Our NON-BLIND approach in the WMAP 3 year data: M. López-Caniego Cavendish Laboratory University of Cambridge INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND

A complete sample at 5 GHz is generated from other catalogues: 1,980,491 sources at 5 GHz with positions and fluxes above ~5 mJy and spectral indexes A subsample of 4050 objects with flux > 500 mJy 5 GHz is selected as our Initial Catalogue (IC)‏ Our NON-BLIND approach in the WMAP 3 year data: INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND

Recent NON-BLIND works detecting Point Sources in WMAP: Lopez-Caniego et al. 2007: NEWPS catalogue using WMAP 3 year data Non-blind:positions of known sources observed at low frequency surveys. Local approach: filters that are specific for the statistical properties of the neighbourhood of the sources M. López-Caniego Cavendish Laboratory University of Cambridge Our NON-BLIND approach in the WMAP 3 year data: INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND

Filtering with the MHW2 at the optimal scale for each flat patch M. López-Caniego Cavendish Laboratory University of Cambridge Our NON-BLIND approach in the WMAP 3 year data: INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND

Recent NON-BLIND works detecting Point Sources in WMAP: Lopez-Caniego et al. 2007: NEWPS catalogue using WMAP 3 year data Non-blind:positions of known sources observed at low frequency surveys. Local approach: filters that are specific for the statistical properties of the neighbourhood of the sources Better beam modelling: symmetrized radial beam profiles instead of idealized Gaussian beams M. López-Caniego Cavendish Laboratory University of Cambridge Our NON-BLIND approach in the WMAP 3 year data: INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND

WMAP 3rd year symmetrized radial beam profiles M. López-Caniego Cavendish Laboratory University of Cambridge Our NON-BLIND approach in the WMAP 3 year data: INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND

Recent NON-BLIND works detecting Point Sources in WMAP: Lopez-Caniego et al. 2007: NEWPS catalogue using WMAP 3 year data Non-blind:positions of known sources observed at low frequency surveys. Local approach: filters that are specific for the statistical properties of the neighbourhood of the sources Better beam modelling: symmetrized radial beam profiles instead of idealized Gaussian beams Selection criterion: in order to obtain complete sample of extragalactic point sources down to a fixed flux detection threshold M. López-Caniego Cavendish Laboratory University of Cambridge Our NON-BLIND approach in the WMAP 3 year data: INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND

For each position in the initial catalog: * A flat patch centered at such position is obtained * Each patch is filtered with the MHW2: Determination of the optimal scale maximum amplification minimum variance * Local noise estimation in a corona around the center of the patch * Look for peaks above a certain SNR * Estimate the flux density of these peaks NEWPS 3yr Non-Blind: Local filtering and noise estimation M. López-Caniego Cavendish Laboratory University of Cambridge INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND

(4050 Obj.) Initial Catalogue WMAP 3yr 323 obj Catalogue 25 Missed Objs. 297 Common Objs. WMAP 11 5  dets. out non det. 5  Objs. 258 Common 5  dets. 39 non detected 5  If, for example, we look at the 23 GHz 5  SubCatalogue (SC)‏ 80 new 5  detected objects from IC in WMAP Total: 349 ( ) 5  at 23 GHz M. López-Caniego Cavendish Laboratory University of Cambridge The NEWPS 3yr source catalogue: Summary of the results INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND

The NEWPS 3yr source catalogue: Summary of the results Galactic cut | b | < 5 deg & LMC (5 deg). Bright Galactic objects outside the previously introduced cut are removed. Why?: Sources in the WMAP catalogues are not 5  at all frequencies: 5  in at least one and at least >2  in the other NEWPS 5  : all sources are 5  M. López-Caniego Cavendish Laboratory University of Cambridge 98 NEW 5  SOURCES INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND

One Step further: NEWPS 5yr Blind + Non-Blind Approach Combine the power of both techniques, the Blind and Non-Blind approach. Divide the sky into flat patches Filter with the MHW2 Detect objetcs SNR > 5 and estimate S Make histogram of the fluxes of sources Flag area around 5% brightest sources Flag a border around the patch Estimate noise from unflagged pixels Using a list of known positions: For every object, a patch centered in this posiiton is obtained Filter with the MHW2 Detect objetcs SNR > 5 and estimate S Make histogram of the fluxes of sources Flag area around 5% brightest sources Flag a border around the patch Estimate noise from unflagged pixels ONLY in a CORONA around the object M. López-Caniego Cavendish Laboratory University of Cambridge INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND WMAP-5yr BLIND+NON-BLIND Simple Blind Detection (SB):Non-Blind Detection (NB)‏

We have used the BSS (Massardi et al. 2008) to study the flux estimation, completeness and reliability of our blind+non-blind approach, in WMAP 5 year data in the same area covered by AT20G. The BSS:Bright Source Sample is a subsample of 320 objects observed by Australian Telescope 20 GHz Survey (AT20G), 294 of them with |b|>5° and  1 Jy). It is a complete sample down to S20=0.5 Jy, and the observations are contemporary to WMAP. Results from the comparison at 23 GHz channel with SNR > 5: (114)# detected BSS obj (common to NB) ‏ 41 ( ) ‏ SB -New sources NB M. López-Caniego Cavendish Laboratory University of Cambridge The BSS: testing the Blind + Non-Blind Approach INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND WMAP-5yr BLIND+NON-BLIND

Error in the estimation of the flux: good agreement above aprox. 840mJy M. López-Caniego Cavendish Laboratory University of Cambridge The Bright Source Sample: Flux density estimation INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND WMAP-5yr BLIND+NON-BLIND Systematic overestimation of the fluxes in WMAP data below 840 mJy. 840 mJy

M. López-Caniego Cavendish Laboratory University of Cambridge The Bright Source Sample: Reliability Simple Blind: 41 new ps not in BSS: 15 extragalactic 9 Galactic 17 no counterpart (14 |b|<20 deg)‏ INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND WMAP-5yr BLIND+NON-BLIND A cut of |b| > 10 deg will remove most of the contaminated regions, but some valuable regions as well. The usual |b|>5 deg cut is a better compromise between removing contaminated regions and preserving clean ones. We have produced a noise map at 23 GHz corresponding to HEALPix nside=32 using the noise estimations of the individual sources in the SB. We can make a “noise mask”, removing the |b|<5 deg regions. The median of the remaining pixels outside this cut is = 169 mJy.

M. López-Caniego Cavendish Laboratory University of Cambridge The Bright Source Sample: Reliability INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND WMAP-5yr BLIND+NON-BLIND We can make a “noise mask”, removing the |b|<5 deg regions. The median of the remaining pixels outside this cut is = 169 mJy.

|b|<5° Dropping areas with  > 1.5  median = 253 mJy at 23 GHz removes 17 Objects, 9 of which where doubtful. If the remaining 8 objects where actually spurious, the sample reliability will be 95.5%. M. López-Caniego Cavendish Laboratory University of Cambridge The Bright Source Sample: Reliability INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND WMAP-5yr BLIND+NON-BLIND

M. López-Caniego Cavendish Laboratory University of Cambridge The Bright Source Sample: Reliability INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND WMAP-5yr BLIND+NON-BLIND Threshold at 1.5 = 253 mJy

Considering only SB detections, the completeness is 89% above 1 Jy. Considering the combination of the SB+NB, increases to 91%. Taking these results into account, we propose a recipe to do the PS Detection in the full-sky maps of WMAP 5yr. M. López-Caniego Cavendish Laboratory University of Cambridge The Bright Source Sample: Completeness INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND WMAP-5yr BLIND+NON-BLIND

Blind and Non-Blind detection in WMAP 5-year data: Recipe The analysis of the BSS provides a recipe to study the WMAP 5yr and to update NEWPS-3yr to NEWPS-5yr catalogue –Carry out a Simple Blind detection over the full sky maps –Generate noise maps of the mean noise values per pixel for nside=32 (  pixel ) and compute the median excluding the |b|<5 deg (  median ). –Generate a mask with all the pixels with noise level > 1.5  median –Consider all the sources outside the mask and SNR > 5 as true detections. –Carry out a Non-Blind search on the maps at the positions of the NEWPS-3yr-3  sample. - Combine results from both methods M. López-Caniego Cavendish Laboratory University of Cambridge INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND WMAP-5yr BLIND+NON-BLIND

Areas with  pixel > 1.5  median have been excluded. 516 different sources: 480 EPS, 20 GS, 16 unidentified - at least 96.9% reliable In the region covered by NEWPS, WMAP has 388 PS: 356 SNR >5 and 32 SNR < 5 NEWPS-5yr has 164 new sources not in WMAP-5yr: from em, only 16 may be false We recover the 64 objects of Chen & Wright (08) and the objects by Nie & Zhang (07)‏ Summary of the properties of the NEWPS-5yr 5  catalogue M. López-Caniego Cavendish Laboratory University of Cambridge INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND WMAP-5yr BLIND+NON-BLIND

M. López-Caniego Cavendish Laboratory University of Cambridge NEWPS-5yr Number Counts INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND WMAP-5yr BLIND+NON-BLIND

We have studied the efficiency in source detection and flux density estimation of a Blind+Non-Blind approach based on the MHW2 applied on WMAP 5yr. Using the ATC20G Bright Source Sample (Massardi et al. 2008) we have been able to estimate the completeness, reliability and accuracy of the flux density Determination for the samples obtained with the blind and the non-blind approach. The flux density are unbiased down to 840 mJy where we overestimate the Fluxes (a manfestation of the Eddington bias). This will affect the number counts, but it can be corrected using high resolution surveys that go below WMAP detection limit, AT20G (Massardi 08, Ricci 04) and 9C (Waldram, 03). At higher flux density, most candidates to be spurious are low Galactic |b|<20 deg. Excluding objects in contaminated areas (  > 1.5  median outside |b|>5) the number of dubious objects reduces by half. If all of them are spurious, reliability 95.5% M. López-Caniego Cavendish Laboratory University of Cambridge Conclusions INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND WMAP-5yr BLIND+NON-BLIND

In the full-sky study: Blindfinds 488 sources (|b|>5, noise > 1.5  median )‏ Non-Blind finds 28 additinal sources Total: 516 ( ) sources with SNR > 5 compared with the 388 objects in the WMAP-5yr catalogue. From the 516, since only 16 of them are dubious, then the reliability at least 96.9%. Conclusions M. López-Caniego Cavendish Laboratory University of Cambridge INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND WMAP-5yr BLIND+NON-BLIND

Planck expects to detect aproximately clusters of galaxies in 2/3 of the sky.The SZ effect induces a characteristic spectral distortion in the CMB produced by inverse Compton scattering of CMB photons during their passage through hot ionized gas, mainly in the inner regions of clusters of galaxies. Detection of Sunyaev Zel’dovich clusters on flat patches: M. López-Caniego Cavendish Laboratory University of Cambridge INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND WMAP-5yr BLIND+NON-BLIND SZ CONCLUSIONS

The Matched Multifilter This filter works with 9 patches of the sky centered in the same position, producing a weighted sum (taking into account the frequency dependance) of the 9 patches. Then the codelooks for candidates above a certain SNR producing a list of objects to be analysed. Then, each of the candidates is analized individually in an iterative procedure trying to estimate its size. This code is being used to detect clusters in Planck simulations produced at the full Planck resolution. Detection of Sunyaev Zel’dovich clusters on flat patches: M. López-Caniego Cavendish Laboratory University of Cambridge Herranz et al., 2002, MNRAS,Vol 336, INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND WMAP-5yr BLIND+NON-BLIND SZ CONCLUSIONS

The Matched Multifilter This filter works with 9 patches of the sky centered in the same position, producing a weighted sum (taking into account the frequency dependance) of the 9 patches. Then the codelooks for candidates above a certain SNR producing a list of objects to be analysed. Then, each of the candidates is analized individually in an iterative procedure trying to estimate its size. This code is being used to detect clusters in Planck simulations produced at the full Planck resolution. Detection of Sunyaev Zel’dovich clusters on flat patches: M. López-Caniego Cavendish Laboratory University of Cambridge Herranz et al., 2002, MNRAS,Vol 336, INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND WMAP-5yr BLIND+NON-BLIND SZ CONCLUSIONS

The Matched Multifilter This filter works with 9 patches of the sky centered in the same position, producing a weighted sum (taking into account the frequency dependance) of the 9 patches. Then the codelooks for candidates above a certain SNR producing a list of objects to be analysed. Then, each of the candidates is analized individually in an iterative procedure trying to estimate its size. This code is being used to detect clusters in Planck simulations produced at the full Planck resolution. Detection of Sunyaev Zel’dovich clusters on flat patches: M. López-Caniego Cavendish Laboratory University of Cambridge Herranz et al., 2002, MNRAS,Vol 336, INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND WMAP-5yr BLIND+NON-BLIND SZ CONCLUSIONS

M. López-Caniego Cavendish Laboratory University of Cambridge Detection of Sunyaev Zel’dovich clusters on flat patches: INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND WMAP-5yr BLIND+NON-BLIND SZ CONCLUSIONS

M. López-Caniego Cavendish Laboratory University of Cambridge Detection of Sunyaev Zel’dovich clusters on flat patches: Weighted sum of the previous nine patches taking into account the frequency dependence of the SZ in the filtering and weighting process INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND WMAP-5yr BLIND+NON-BLIND SZ CONCLUSIONS

In these works we have approached the problem of point source detection in maps of the Cosmic Microwave Background using linear filters : We have tested the MHW1 and MHW2 against the MF in realistic simulations for the 9 Planck frequencies (the Planck Reference Sky and PS based on the lates models)‏ The MHW2 at the optimal scale is comparable to the MF but easier to implement. We have used the MHW2 in real data from WMAP to construct a new catalogue of extragalactic point sources to complement WMAP result. This was a non-blind approach with initial catalogue of 4050 objects already observed at 5 GHz. Estimated their flux at the WMAP frequencies. Constructed a 3  and 5  subcatalogues of objects, 25% of them not included in WMAP M. López-Caniego Cavendish Laboratory University of Cambridge Final Conclusions and General Remarks for Planck INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND WMAP-5yr BLIND+NON-BLIND SZ CONCLUSIONS

Final Conclusions and General Remarks for Planck Using the WMAP 5-years data we have combined the power of a blind + non- blind approach to create a new catalogue of point sources. The result of this combination is a catalogue with 500 sources SNR > 5, 164 of them are new to WMAP 5yr catalogue. A similar strategy could be used for Planck. These studies are preparatory work for Planck. We have shown that the MWH2 code is performing well, we have installed it in the LFI and HFI DPCs and we are now in the process of installing it in the ERCSC pipeline. There is room for improvement in the high Planck frequencies M. López-Caniego Cavendish Laboratory University of Cambridge INTRO PLANCK SIMULATIONS WMAP-3yr NON-BLIND WMAP-5yr BLIND+NON-BLIND SZ CONCLUSIONS