Adapted Method for Separating Kinetic SZ Signal from Primary CMB Fluctuations
<p/< <p<In this first attempt to extract a map of the kinetic Sunyaev-Zel'dovich (KSZ) temperature fluctuations from the cosmic microwave background (CMB) anisotropies, we use a method which is based on simple and minimal assumptions. We first focus on the intrinsic limitations of t...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Forni Olivier [verfasserIn] Aghanim Nabila [verfasserIn] |
|---|
| Format: |
E-Artikel |
|---|---|
| Sprache: |
Englisch |
| Erschienen: |
2005 |
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| Schlagwörter: |
|---|
| Übergeordnetes Werk: |
In: EURASIP Journal on Advances in Signal Processing - SpringerOpen, 2008, (2005), 15, p 587370 |
|---|---|
| Übergeordnetes Werk: |
year:2005 ; number:15, p 587370 |
| Links: |
|---|
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DOAJ024930695 |
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| 520 | |a <p/< <p<In this first attempt to extract a map of the kinetic Sunyaev-Zel'dovich (KSZ) temperature fluctuations from the cosmic microwave background (CMB) anisotropies, we use a method which is based on simple and minimal assumptions. We first focus on the intrinsic limitations of the method due to the cosmological signal itself. We demonstrate using simulated maps that the KSZ reconstructed maps are in quite good agreement with the original input signal with a correlation coefficient between original and reconstructed maps of <inline-formula<<graphic file="1687-6180-2005-587370-i1.gif"/<</inline-formula< on average, and an error on the standard deviation of the reconstructed KSZ map of only <inline-formula<<graphic file="1687-6180-2005-587370-i2.gif"/<</inline-formula<% on average. To achieve these results, our method is based on the fact that some first-step component separation provides us with (i) a map of Compton parameters for the thermal Sunyaev-Zel'dovich (TSZ) effect of galaxy clusters, and (ii) a map of temperature fluctuations which is the sum of primary CMB and KSZ signals. Our method takes benefit from the spatial correlation between KSZ and TSZ effects which are both due to the same galaxy clusters. This correlation allows us to use the TSZ map as a spatial template in order to mask, in the <inline-formula<<graphic file="1687-6180-2005-587370-i3.gif"/<</inline-formula< map, the pixels where the clusters must have imprinted an SZ fluctuation. In practice, a series of TSZ thresholds is defined and for each threshold, we estimate the corresponding KSZ signal by interpolating the CMB fluctuations on the masked pixels. The series of estimated KSZ maps is finally used to reconstruct the KSZ map through the minimisation of a criterion taking into account two statistical properties of the KSZ signal (KSZ dominates over primary anisotropies at small scales, KSZ fluctuations are non-Gaussian distributed). We show that the results are quite sensitive to the effect of beam convolution, especially for large beams, and to the corruption by instrumental noise.</p< | ||
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(DE-627)DOAJ024930695 (DE-599)DOAJ88519b1f00954f8e9afd3320524d0ba9 DE-627 ger DE-627 rakwb eng TK5101-6720 TK7800-8360 Forni Olivier verfasserin aut Adapted Method for Separating Kinetic SZ Signal from Primary CMB Fluctuations 2005 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier <p/< <p<In this first attempt to extract a map of the kinetic Sunyaev-Zel'dovich (KSZ) temperature fluctuations from the cosmic microwave background (CMB) anisotropies, we use a method which is based on simple and minimal assumptions. We first focus on the intrinsic limitations of the method due to the cosmological signal itself. We demonstrate using simulated maps that the KSZ reconstructed maps are in quite good agreement with the original input signal with a correlation coefficient between original and reconstructed maps of <inline-formula<<graphic file="1687-6180-2005-587370-i1.gif"/<</inline-formula< on average, and an error on the standard deviation of the reconstructed KSZ map of only <inline-formula<<graphic file="1687-6180-2005-587370-i2.gif"/<</inline-formula<% on average. To achieve these results, our method is based on the fact that some first-step component separation provides us with (i) a map of Compton parameters for the thermal Sunyaev-Zel'dovich (TSZ) effect of galaxy clusters, and (ii) a map of temperature fluctuations which is the sum of primary CMB and KSZ signals. Our method takes benefit from the spatial correlation between KSZ and TSZ effects which are both due to the same galaxy clusters. This correlation allows us to use the TSZ map as a spatial template in order to mask, in the <inline-formula<<graphic file="1687-6180-2005-587370-i3.gif"/<</inline-formula< map, the pixels where the clusters must have imprinted an SZ fluctuation. In practice, a series of TSZ thresholds is defined and for each threshold, we estimate the corresponding KSZ signal by interpolating the CMB fluctuations on the masked pixels. The series of estimated KSZ maps is finally used to reconstruct the KSZ map through the minimisation of a criterion taking into account two statistical properties of the KSZ signal (KSZ dominates over primary anisotropies at small scales, KSZ fluctuations are non-Gaussian distributed). We show that the results are quite sensitive to the effect of beam convolution, especially for large beams, and to the corruption by instrumental noise.</p< cosmic microwave background data analysis Telecommunication Electronics Aghanim Nabila verfasserin aut In EURASIP Journal on Advances in Signal Processing SpringerOpen, 2008 (2005), 15, p 587370 (DE-627)534054277 (DE-600)2364203-8 16876180 nnns year:2005 number:15, p 587370 https://doaj.org/article/88519b1f00954f8e9afd3320524d0ba9 kostenfrei http://dx.doi.org/10.1155/ASP.2005.2413 kostenfrei https://doaj.org/toc/1687-6172 Journal toc kostenfrei https://doaj.org/toc/1687-6180 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_110 GBV_ILN_161 GBV_ILN_170 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2522 AR 2005 15, p 587370 |
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(DE-627)DOAJ024930695 (DE-599)DOAJ88519b1f00954f8e9afd3320524d0ba9 DE-627 ger DE-627 rakwb eng TK5101-6720 TK7800-8360 Forni Olivier verfasserin aut Adapted Method for Separating Kinetic SZ Signal from Primary CMB Fluctuations 2005 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier <p/< <p<In this first attempt to extract a map of the kinetic Sunyaev-Zel'dovich (KSZ) temperature fluctuations from the cosmic microwave background (CMB) anisotropies, we use a method which is based on simple and minimal assumptions. We first focus on the intrinsic limitations of the method due to the cosmological signal itself. We demonstrate using simulated maps that the KSZ reconstructed maps are in quite good agreement with the original input signal with a correlation coefficient between original and reconstructed maps of <inline-formula<<graphic file="1687-6180-2005-587370-i1.gif"/<</inline-formula< on average, and an error on the standard deviation of the reconstructed KSZ map of only <inline-formula<<graphic file="1687-6180-2005-587370-i2.gif"/<</inline-formula<% on average. To achieve these results, our method is based on the fact that some first-step component separation provides us with (i) a map of Compton parameters for the thermal Sunyaev-Zel'dovich (TSZ) effect of galaxy clusters, and (ii) a map of temperature fluctuations which is the sum of primary CMB and KSZ signals. Our method takes benefit from the spatial correlation between KSZ and TSZ effects which are both due to the same galaxy clusters. This correlation allows us to use the TSZ map as a spatial template in order to mask, in the <inline-formula<<graphic file="1687-6180-2005-587370-i3.gif"/<</inline-formula< map, the pixels where the clusters must have imprinted an SZ fluctuation. In practice, a series of TSZ thresholds is defined and for each threshold, we estimate the corresponding KSZ signal by interpolating the CMB fluctuations on the masked pixels. The series of estimated KSZ maps is finally used to reconstruct the KSZ map through the minimisation of a criterion taking into account two statistical properties of the KSZ signal (KSZ dominates over primary anisotropies at small scales, KSZ fluctuations are non-Gaussian distributed). We show that the results are quite sensitive to the effect of beam convolution, especially for large beams, and to the corruption by instrumental noise.</p< cosmic microwave background data analysis Telecommunication Electronics Aghanim Nabila verfasserin aut In EURASIP Journal on Advances in Signal Processing SpringerOpen, 2008 (2005), 15, p 587370 (DE-627)534054277 (DE-600)2364203-8 16876180 nnns year:2005 number:15, p 587370 https://doaj.org/article/88519b1f00954f8e9afd3320524d0ba9 kostenfrei http://dx.doi.org/10.1155/ASP.2005.2413 kostenfrei https://doaj.org/toc/1687-6172 Journal toc kostenfrei https://doaj.org/toc/1687-6180 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_110 GBV_ILN_161 GBV_ILN_170 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2522 AR 2005 15, p 587370 |
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(DE-627)DOAJ024930695 (DE-599)DOAJ88519b1f00954f8e9afd3320524d0ba9 DE-627 ger DE-627 rakwb eng TK5101-6720 TK7800-8360 Forni Olivier verfasserin aut Adapted Method for Separating Kinetic SZ Signal from Primary CMB Fluctuations 2005 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier <p/< <p<In this first attempt to extract a map of the kinetic Sunyaev-Zel'dovich (KSZ) temperature fluctuations from the cosmic microwave background (CMB) anisotropies, we use a method which is based on simple and minimal assumptions. We first focus on the intrinsic limitations of the method due to the cosmological signal itself. We demonstrate using simulated maps that the KSZ reconstructed maps are in quite good agreement with the original input signal with a correlation coefficient between original and reconstructed maps of <inline-formula<<graphic file="1687-6180-2005-587370-i1.gif"/<</inline-formula< on average, and an error on the standard deviation of the reconstructed KSZ map of only <inline-formula<<graphic file="1687-6180-2005-587370-i2.gif"/<</inline-formula<% on average. To achieve these results, our method is based on the fact that some first-step component separation provides us with (i) a map of Compton parameters for the thermal Sunyaev-Zel'dovich (TSZ) effect of galaxy clusters, and (ii) a map of temperature fluctuations which is the sum of primary CMB and KSZ signals. Our method takes benefit from the spatial correlation between KSZ and TSZ effects which are both due to the same galaxy clusters. This correlation allows us to use the TSZ map as a spatial template in order to mask, in the <inline-formula<<graphic file="1687-6180-2005-587370-i3.gif"/<</inline-formula< map, the pixels where the clusters must have imprinted an SZ fluctuation. In practice, a series of TSZ thresholds is defined and for each threshold, we estimate the corresponding KSZ signal by interpolating the CMB fluctuations on the masked pixels. The series of estimated KSZ maps is finally used to reconstruct the KSZ map through the minimisation of a criterion taking into account two statistical properties of the KSZ signal (KSZ dominates over primary anisotropies at small scales, KSZ fluctuations are non-Gaussian distributed). We show that the results are quite sensitive to the effect of beam convolution, especially for large beams, and to the corruption by instrumental noise.</p< cosmic microwave background data analysis Telecommunication Electronics Aghanim Nabila verfasserin aut In EURASIP Journal on Advances in Signal Processing SpringerOpen, 2008 (2005), 15, p 587370 (DE-627)534054277 (DE-600)2364203-8 16876180 nnns year:2005 number:15, p 587370 https://doaj.org/article/88519b1f00954f8e9afd3320524d0ba9 kostenfrei http://dx.doi.org/10.1155/ASP.2005.2413 kostenfrei https://doaj.org/toc/1687-6172 Journal toc kostenfrei https://doaj.org/toc/1687-6180 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_110 GBV_ILN_161 GBV_ILN_170 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2522 AR 2005 15, p 587370 |
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(DE-627)DOAJ024930695 (DE-599)DOAJ88519b1f00954f8e9afd3320524d0ba9 DE-627 ger DE-627 rakwb eng TK5101-6720 TK7800-8360 Forni Olivier verfasserin aut Adapted Method for Separating Kinetic SZ Signal from Primary CMB Fluctuations 2005 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier <p/< <p<In this first attempt to extract a map of the kinetic Sunyaev-Zel'dovich (KSZ) temperature fluctuations from the cosmic microwave background (CMB) anisotropies, we use a method which is based on simple and minimal assumptions. We first focus on the intrinsic limitations of the method due to the cosmological signal itself. We demonstrate using simulated maps that the KSZ reconstructed maps are in quite good agreement with the original input signal with a correlation coefficient between original and reconstructed maps of <inline-formula<<graphic file="1687-6180-2005-587370-i1.gif"/<</inline-formula< on average, and an error on the standard deviation of the reconstructed KSZ map of only <inline-formula<<graphic file="1687-6180-2005-587370-i2.gif"/<</inline-formula<% on average. To achieve these results, our method is based on the fact that some first-step component separation provides us with (i) a map of Compton parameters for the thermal Sunyaev-Zel'dovich (TSZ) effect of galaxy clusters, and (ii) a map of temperature fluctuations which is the sum of primary CMB and KSZ signals. Our method takes benefit from the spatial correlation between KSZ and TSZ effects which are both due to the same galaxy clusters. This correlation allows us to use the TSZ map as a spatial template in order to mask, in the <inline-formula<<graphic file="1687-6180-2005-587370-i3.gif"/<</inline-formula< map, the pixels where the clusters must have imprinted an SZ fluctuation. In practice, a series of TSZ thresholds is defined and for each threshold, we estimate the corresponding KSZ signal by interpolating the CMB fluctuations on the masked pixels. The series of estimated KSZ maps is finally used to reconstruct the KSZ map through the minimisation of a criterion taking into account two statistical properties of the KSZ signal (KSZ dominates over primary anisotropies at small scales, KSZ fluctuations are non-Gaussian distributed). We show that the results are quite sensitive to the effect of beam convolution, especially for large beams, and to the corruption by instrumental noise.</p< cosmic microwave background data analysis Telecommunication Electronics Aghanim Nabila verfasserin aut In EURASIP Journal on Advances in Signal Processing SpringerOpen, 2008 (2005), 15, p 587370 (DE-627)534054277 (DE-600)2364203-8 16876180 nnns year:2005 number:15, p 587370 https://doaj.org/article/88519b1f00954f8e9afd3320524d0ba9 kostenfrei http://dx.doi.org/10.1155/ASP.2005.2413 kostenfrei https://doaj.org/toc/1687-6172 Journal toc kostenfrei https://doaj.org/toc/1687-6180 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_110 GBV_ILN_161 GBV_ILN_170 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2522 AR 2005 15, p 587370 |
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(DE-627)DOAJ024930695 (DE-599)DOAJ88519b1f00954f8e9afd3320524d0ba9 DE-627 ger DE-627 rakwb eng TK5101-6720 TK7800-8360 Forni Olivier verfasserin aut Adapted Method for Separating Kinetic SZ Signal from Primary CMB Fluctuations 2005 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier <p/< <p<In this first attempt to extract a map of the kinetic Sunyaev-Zel'dovich (KSZ) temperature fluctuations from the cosmic microwave background (CMB) anisotropies, we use a method which is based on simple and minimal assumptions. We first focus on the intrinsic limitations of the method due to the cosmological signal itself. We demonstrate using simulated maps that the KSZ reconstructed maps are in quite good agreement with the original input signal with a correlation coefficient between original and reconstructed maps of <inline-formula<<graphic file="1687-6180-2005-587370-i1.gif"/<</inline-formula< on average, and an error on the standard deviation of the reconstructed KSZ map of only <inline-formula<<graphic file="1687-6180-2005-587370-i2.gif"/<</inline-formula<% on average. To achieve these results, our method is based on the fact that some first-step component separation provides us with (i) a map of Compton parameters for the thermal Sunyaev-Zel'dovich (TSZ) effect of galaxy clusters, and (ii) a map of temperature fluctuations which is the sum of primary CMB and KSZ signals. Our method takes benefit from the spatial correlation between KSZ and TSZ effects which are both due to the same galaxy clusters. This correlation allows us to use the TSZ map as a spatial template in order to mask, in the <inline-formula<<graphic file="1687-6180-2005-587370-i3.gif"/<</inline-formula< map, the pixels where the clusters must have imprinted an SZ fluctuation. In practice, a series of TSZ thresholds is defined and for each threshold, we estimate the corresponding KSZ signal by interpolating the CMB fluctuations on the masked pixels. The series of estimated KSZ maps is finally used to reconstruct the KSZ map through the minimisation of a criterion taking into account two statistical properties of the KSZ signal (KSZ dominates over primary anisotropies at small scales, KSZ fluctuations are non-Gaussian distributed). We show that the results are quite sensitive to the effect of beam convolution, especially for large beams, and to the corruption by instrumental noise.</p< cosmic microwave background data analysis Telecommunication Electronics Aghanim Nabila verfasserin aut In EURASIP Journal on Advances in Signal Processing SpringerOpen, 2008 (2005), 15, p 587370 (DE-627)534054277 (DE-600)2364203-8 16876180 nnns year:2005 number:15, p 587370 https://doaj.org/article/88519b1f00954f8e9afd3320524d0ba9 kostenfrei http://dx.doi.org/10.1155/ASP.2005.2413 kostenfrei https://doaj.org/toc/1687-6172 Journal toc kostenfrei https://doaj.org/toc/1687-6180 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_110 GBV_ILN_161 GBV_ILN_170 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2522 AR 2005 15, p 587370 |
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Adapted Method for Separating Kinetic SZ Signal from Primary CMB Fluctuations |
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<p/< <p<In this first attempt to extract a map of the kinetic Sunyaev-Zel'dovich (KSZ) temperature fluctuations from the cosmic microwave background (CMB) anisotropies, we use a method which is based on simple and minimal assumptions. We first focus on the intrinsic limitations of the method due to the cosmological signal itself. We demonstrate using simulated maps that the KSZ reconstructed maps are in quite good agreement with the original input signal with a correlation coefficient between original and reconstructed maps of <inline-formula<<graphic file="1687-6180-2005-587370-i1.gif"/<</inline-formula< on average, and an error on the standard deviation of the reconstructed KSZ map of only <inline-formula<<graphic file="1687-6180-2005-587370-i2.gif"/<</inline-formula<% on average. To achieve these results, our method is based on the fact that some first-step component separation provides us with (i) a map of Compton parameters for the thermal Sunyaev-Zel'dovich (TSZ) effect of galaxy clusters, and (ii) a map of temperature fluctuations which is the sum of primary CMB and KSZ signals. Our method takes benefit from the spatial correlation between KSZ and TSZ effects which are both due to the same galaxy clusters. This correlation allows us to use the TSZ map as a spatial template in order to mask, in the <inline-formula<<graphic file="1687-6180-2005-587370-i3.gif"/<</inline-formula< map, the pixels where the clusters must have imprinted an SZ fluctuation. In practice, a series of TSZ thresholds is defined and for each threshold, we estimate the corresponding KSZ signal by interpolating the CMB fluctuations on the masked pixels. The series of estimated KSZ maps is finally used to reconstruct the KSZ map through the minimisation of a criterion taking into account two statistical properties of the KSZ signal (KSZ dominates over primary anisotropies at small scales, KSZ fluctuations are non-Gaussian distributed). We show that the results are quite sensitive to the effect of beam convolution, especially for large beams, and to the corruption by instrumental noise.</p< |
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<p/< <p<In this first attempt to extract a map of the kinetic Sunyaev-Zel'dovich (KSZ) temperature fluctuations from the cosmic microwave background (CMB) anisotropies, we use a method which is based on simple and minimal assumptions. We first focus on the intrinsic limitations of the method due to the cosmological signal itself. We demonstrate using simulated maps that the KSZ reconstructed maps are in quite good agreement with the original input signal with a correlation coefficient between original and reconstructed maps of <inline-formula<<graphic file="1687-6180-2005-587370-i1.gif"/<</inline-formula< on average, and an error on the standard deviation of the reconstructed KSZ map of only <inline-formula<<graphic file="1687-6180-2005-587370-i2.gif"/<</inline-formula<% on average. To achieve these results, our method is based on the fact that some first-step component separation provides us with (i) a map of Compton parameters for the thermal Sunyaev-Zel'dovich (TSZ) effect of galaxy clusters, and (ii) a map of temperature fluctuations which is the sum of primary CMB and KSZ signals. Our method takes benefit from the spatial correlation between KSZ and TSZ effects which are both due to the same galaxy clusters. This correlation allows us to use the TSZ map as a spatial template in order to mask, in the <inline-formula<<graphic file="1687-6180-2005-587370-i3.gif"/<</inline-formula< map, the pixels where the clusters must have imprinted an SZ fluctuation. In practice, a series of TSZ thresholds is defined and for each threshold, we estimate the corresponding KSZ signal by interpolating the CMB fluctuations on the masked pixels. The series of estimated KSZ maps is finally used to reconstruct the KSZ map through the minimisation of a criterion taking into account two statistical properties of the KSZ signal (KSZ dominates over primary anisotropies at small scales, KSZ fluctuations are non-Gaussian distributed). We show that the results are quite sensitive to the effect of beam convolution, especially for large beams, and to the corruption by instrumental noise.</p< |
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<p/< <p<In this first attempt to extract a map of the kinetic Sunyaev-Zel'dovich (KSZ) temperature fluctuations from the cosmic microwave background (CMB) anisotropies, we use a method which is based on simple and minimal assumptions. We first focus on the intrinsic limitations of the method due to the cosmological signal itself. We demonstrate using simulated maps that the KSZ reconstructed maps are in quite good agreement with the original input signal with a correlation coefficient between original and reconstructed maps of <inline-formula<<graphic file="1687-6180-2005-587370-i1.gif"/<</inline-formula< on average, and an error on the standard deviation of the reconstructed KSZ map of only <inline-formula<<graphic file="1687-6180-2005-587370-i2.gif"/<</inline-formula<% on average. To achieve these results, our method is based on the fact that some first-step component separation provides us with (i) a map of Compton parameters for the thermal Sunyaev-Zel'dovich (TSZ) effect of galaxy clusters, and (ii) a map of temperature fluctuations which is the sum of primary CMB and KSZ signals. Our method takes benefit from the spatial correlation between KSZ and TSZ effects which are both due to the same galaxy clusters. This correlation allows us to use the TSZ map as a spatial template in order to mask, in the <inline-formula<<graphic file="1687-6180-2005-587370-i3.gif"/<</inline-formula< map, the pixels where the clusters must have imprinted an SZ fluctuation. In practice, a series of TSZ thresholds is defined and for each threshold, we estimate the corresponding KSZ signal by interpolating the CMB fluctuations on the masked pixels. The series of estimated KSZ maps is finally used to reconstruct the KSZ map through the minimisation of a criterion taking into account two statistical properties of the KSZ signal (KSZ dominates over primary anisotropies at small scales, KSZ fluctuations are non-Gaussian distributed). We show that the results are quite sensitive to the effect of beam convolution, especially for large beams, and to the corruption by instrumental noise.</p< |
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