DSP-Enabled Radio Astronomy: Towards IIIZW35 Reconquest

Abstract In radio astronomy, the radio spectrum is used to detect weak emission from celestial sources. By spectral averaging, observation noise is reduced and weak sources can be detected. However, more and more observations are polluted by man-made radio frequency interferences (RFI). The impact o...
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Autor*in:	Weber, Rodolphe [verfasserIn] Viou, Cédric [verfasserIn] Coffre, Andrée [verfasserIn] Denis, Laurent [verfasserIn] Zarka, Philippe [verfasserIn] Lecacheux, Alain [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2005

Übergeordnetes Werk:	Enthalten in: EURASIP journal on advances in signal processing - Heidelberg : Springer, 2007, 2005(2005), 16 vom: 21. Sept.
Übergeordnetes Werk:	volume:2005 ; year:2005 ; number:16 ; day:21 ; month:09

Links:	Volltext

DOI / URN:	10.1155/ASP.2005.2686

Katalog-ID:	SPR031978665

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allfields	10.1155/ASP.2005.2686 doi (DE-627)SPR031978665 (SPR)ASP.2005.2686-e DE-627 ger DE-627 rakwb eng 620 ASE 53.73 bkl Weber, Rodolphe verfasserin aut DSP-Enabled Radio Astronomy: Towards IIIZW35 Reconquest 2005 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract In radio astronomy, the radio spectrum is used to detect weak emission from celestial sources. By spectral averaging, observation noise is reduced and weak sources can be detected. However, more and more observations are polluted by man-made radio frequency interferences (RFI). The impact of these RFIs on power spectral measurement ranges from total saturation to subtle distortions of the data. To some extent, elimination of artefacts can be achieved by blanking polluted channels in real time. With this aim in view, a complete real-time digital system has been implemented on a set of FPGA and DSP. The current functionalities of the digital system have high dynamic range of 70 dB, bandwidth selection facilities ranging from 875 kHz to 14 MHz, high spectral resolution through a polyphase filter bank with up to 8192 channels with 49 152 coefficients and real-time time-frequency blanking with a robust threshold detector. This receiver has been used to reobserve the IIIWZ35 astronomical source which has been scrambled by a strong satellite RFI for several years. Viou, Cédric verfasserin aut Coffre, Andrée verfasserin aut Denis, Laurent verfasserin aut Zarka, Philippe verfasserin aut Lecacheux, Alain verfasserin aut Enthalten in EURASIP journal on advances in signal processing Heidelberg : Springer, 2007 2005(2005), 16 vom: 21. Sept. (DE-627)534054277 (DE-600)2364203-8 1687-6180 nnns volume:2005 year:2005 number:16 day:21 month:09 https://dx.doi.org/10.1155/ASP.2005.2686 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER 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 53.73 ASE AR 2005 2005 16 21 09
spelling	10.1155/ASP.2005.2686 doi (DE-627)SPR031978665 (SPR)ASP.2005.2686-e DE-627 ger DE-627 rakwb eng 620 ASE 53.73 bkl Weber, Rodolphe verfasserin aut DSP-Enabled Radio Astronomy: Towards IIIZW35 Reconquest 2005 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract In radio astronomy, the radio spectrum is used to detect weak emission from celestial sources. By spectral averaging, observation noise is reduced and weak sources can be detected. However, more and more observations are polluted by man-made radio frequency interferences (RFI). The impact of these RFIs on power spectral measurement ranges from total saturation to subtle distortions of the data. To some extent, elimination of artefacts can be achieved by blanking polluted channels in real time. With this aim in view, a complete real-time digital system has been implemented on a set of FPGA and DSP. The current functionalities of the digital system have high dynamic range of 70 dB, bandwidth selection facilities ranging from 875 kHz to 14 MHz, high spectral resolution through a polyphase filter bank with up to 8192 channels with 49 152 coefficients and real-time time-frequency blanking with a robust threshold detector. This receiver has been used to reobserve the IIIWZ35 astronomical source which has been scrambled by a strong satellite RFI for several years. Viou, Cédric verfasserin aut Coffre, Andrée verfasserin aut Denis, Laurent verfasserin aut Zarka, Philippe verfasserin aut Lecacheux, Alain verfasserin aut Enthalten in EURASIP journal on advances in signal processing Heidelberg : Springer, 2007 2005(2005), 16 vom: 21. Sept. (DE-627)534054277 (DE-600)2364203-8 1687-6180 nnns volume:2005 year:2005 number:16 day:21 month:09 https://dx.doi.org/10.1155/ASP.2005.2686 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER 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 53.73 ASE AR 2005 2005 16 21 09
allfields_unstemmed	10.1155/ASP.2005.2686 doi (DE-627)SPR031978665 (SPR)ASP.2005.2686-e DE-627 ger DE-627 rakwb eng 620 ASE 53.73 bkl Weber, Rodolphe verfasserin aut DSP-Enabled Radio Astronomy: Towards IIIZW35 Reconquest 2005 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract In radio astronomy, the radio spectrum is used to detect weak emission from celestial sources. By spectral averaging, observation noise is reduced and weak sources can be detected. However, more and more observations are polluted by man-made radio frequency interferences (RFI). The impact of these RFIs on power spectral measurement ranges from total saturation to subtle distortions of the data. To some extent, elimination of artefacts can be achieved by blanking polluted channels in real time. With this aim in view, a complete real-time digital system has been implemented on a set of FPGA and DSP. The current functionalities of the digital system have high dynamic range of 70 dB, bandwidth selection facilities ranging from 875 kHz to 14 MHz, high spectral resolution through a polyphase filter bank with up to 8192 channels with 49 152 coefficients and real-time time-frequency blanking with a robust threshold detector. This receiver has been used to reobserve the IIIWZ35 astronomical source which has been scrambled by a strong satellite RFI for several years. Viou, Cédric verfasserin aut Coffre, Andrée verfasserin aut Denis, Laurent verfasserin aut Zarka, Philippe verfasserin aut Lecacheux, Alain verfasserin aut Enthalten in EURASIP journal on advances in signal processing Heidelberg : Springer, 2007 2005(2005), 16 vom: 21. Sept. (DE-627)534054277 (DE-600)2364203-8 1687-6180 nnns volume:2005 year:2005 number:16 day:21 month:09 https://dx.doi.org/10.1155/ASP.2005.2686 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER 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 53.73 ASE AR 2005 2005 16 21 09
allfieldsGer	10.1155/ASP.2005.2686 doi (DE-627)SPR031978665 (SPR)ASP.2005.2686-e DE-627 ger DE-627 rakwb eng 620 ASE 53.73 bkl Weber, Rodolphe verfasserin aut DSP-Enabled Radio Astronomy: Towards IIIZW35 Reconquest 2005 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract In radio astronomy, the radio spectrum is used to detect weak emission from celestial sources. By spectral averaging, observation noise is reduced and weak sources can be detected. However, more and more observations are polluted by man-made radio frequency interferences (RFI). The impact of these RFIs on power spectral measurement ranges from total saturation to subtle distortions of the data. To some extent, elimination of artefacts can be achieved by blanking polluted channels in real time. With this aim in view, a complete real-time digital system has been implemented on a set of FPGA and DSP. The current functionalities of the digital system have high dynamic range of 70 dB, bandwidth selection facilities ranging from 875 kHz to 14 MHz, high spectral resolution through a polyphase filter bank with up to 8192 channels with 49 152 coefficients and real-time time-frequency blanking with a robust threshold detector. This receiver has been used to reobserve the IIIWZ35 astronomical source which has been scrambled by a strong satellite RFI for several years. Viou, Cédric verfasserin aut Coffre, Andrée verfasserin aut Denis, Laurent verfasserin aut Zarka, Philippe verfasserin aut Lecacheux, Alain verfasserin aut Enthalten in EURASIP journal on advances in signal processing Heidelberg : Springer, 2007 2005(2005), 16 vom: 21. Sept. (DE-627)534054277 (DE-600)2364203-8 1687-6180 nnns volume:2005 year:2005 number:16 day:21 month:09 https://dx.doi.org/10.1155/ASP.2005.2686 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER 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 53.73 ASE AR 2005 2005 16 21 09
allfieldsSound	10.1155/ASP.2005.2686 doi (DE-627)SPR031978665 (SPR)ASP.2005.2686-e DE-627 ger DE-627 rakwb eng 620 ASE 53.73 bkl Weber, Rodolphe verfasserin aut DSP-Enabled Radio Astronomy: Towards IIIZW35 Reconquest 2005 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract In radio astronomy, the radio spectrum is used to detect weak emission from celestial sources. By spectral averaging, observation noise is reduced and weak sources can be detected. However, more and more observations are polluted by man-made radio frequency interferences (RFI). The impact of these RFIs on power spectral measurement ranges from total saturation to subtle distortions of the data. To some extent, elimination of artefacts can be achieved by blanking polluted channels in real time. With this aim in view, a complete real-time digital system has been implemented on a set of FPGA and DSP. The current functionalities of the digital system have high dynamic range of 70 dB, bandwidth selection facilities ranging from 875 kHz to 14 MHz, high spectral resolution through a polyphase filter bank with up to 8192 channels with 49 152 coefficients and real-time time-frequency blanking with a robust threshold detector. This receiver has been used to reobserve the IIIWZ35 astronomical source which has been scrambled by a strong satellite RFI for several years. Viou, Cédric verfasserin aut Coffre, Andrée verfasserin aut Denis, Laurent verfasserin aut Zarka, Philippe verfasserin aut Lecacheux, Alain verfasserin aut Enthalten in EURASIP journal on advances in signal processing Heidelberg : Springer, 2007 2005(2005), 16 vom: 21. Sept. (DE-627)534054277 (DE-600)2364203-8 1687-6180 nnns volume:2005 year:2005 number:16 day:21 month:09 https://dx.doi.org/10.1155/ASP.2005.2686 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER 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 53.73 ASE AR 2005 2005 16 21 09
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title	DSP-Enabled Radio Astronomy: Towards IIIZW35 Reconquest
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title_full	DSP-Enabled Radio Astronomy: Towards IIIZW35 Reconquest
author_sort	Weber, Rodolphe
journal	EURASIP journal on advances in signal processing
journalStr	EURASIP journal on advances in signal processing
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author_browse	Weber, Rodolphe Viou, Cédric Coffre, Andrée Denis, Laurent Zarka, Philippe Lecacheux, Alain
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class	620 ASE 53.73 bkl
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author-letter	Weber, Rodolphe
doi_str_mv	10.1155/ASP.2005.2686
dewey-full	620
author2-role	verfasserin
title_sort	dsp-enabled radio astronomy: towards iiizw35 reconquest
title_auth	DSP-Enabled Radio Astronomy: Towards IIIZW35 Reconquest
abstract	Abstract In radio astronomy, the radio spectrum is used to detect weak emission from celestial sources. By spectral averaging, observation noise is reduced and weak sources can be detected. However, more and more observations are polluted by man-made radio frequency interferences (RFI). The impact of these RFIs on power spectral measurement ranges from total saturation to subtle distortions of the data. To some extent, elimination of artefacts can be achieved by blanking polluted channels in real time. With this aim in view, a complete real-time digital system has been implemented on a set of FPGA and DSP. The current functionalities of the digital system have high dynamic range of 70 dB, bandwidth selection facilities ranging from 875 kHz to 14 MHz, high spectral resolution through a polyphase filter bank with up to 8192 channels with 49 152 coefficients and real-time time-frequency blanking with a robust threshold detector. This receiver has been used to reobserve the IIIWZ35 astronomical source which has been scrambled by a strong satellite RFI for several years.
abstractGer	Abstract In radio astronomy, the radio spectrum is used to detect weak emission from celestial sources. By spectral averaging, observation noise is reduced and weak sources can be detected. However, more and more observations are polluted by man-made radio frequency interferences (RFI). The impact of these RFIs on power spectral measurement ranges from total saturation to subtle distortions of the data. To some extent, elimination of artefacts can be achieved by blanking polluted channels in real time. With this aim in view, a complete real-time digital system has been implemented on a set of FPGA and DSP. The current functionalities of the digital system have high dynamic range of 70 dB, bandwidth selection facilities ranging from 875 kHz to 14 MHz, high spectral resolution through a polyphase filter bank with up to 8192 channels with 49 152 coefficients and real-time time-frequency blanking with a robust threshold detector. This receiver has been used to reobserve the IIIWZ35 astronomical source which has been scrambled by a strong satellite RFI for several years.
abstract_unstemmed	Abstract In radio astronomy, the radio spectrum is used to detect weak emission from celestial sources. By spectral averaging, observation noise is reduced and weak sources can be detected. However, more and more observations are polluted by man-made radio frequency interferences (RFI). The impact of these RFIs on power spectral measurement ranges from total saturation to subtle distortions of the data. To some extent, elimination of artefacts can be achieved by blanking polluted channels in real time. With this aim in view, a complete real-time digital system has been implemented on a set of FPGA and DSP. The current functionalities of the digital system have high dynamic range of 70 dB, bandwidth selection facilities ranging from 875 kHz to 14 MHz, high spectral resolution through a polyphase filter bank with up to 8192 channels with 49 152 coefficients and real-time time-frequency blanking with a robust threshold detector. This receiver has been used to reobserve the IIIWZ35 astronomical source which has been scrambled by a strong satellite RFI for several years.
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container_issue	16
title_short	DSP-Enabled Radio Astronomy: Towards IIIZW35 Reconquest
url	https://dx.doi.org/10.1155/ASP.2005.2686
remote_bool	true
author2	Viou, Cédric Coffre, Andrée Denis, Laurent Zarka, Philippe Lecacheux, Alain
author2Str	Viou, Cédric Coffre, Andrée Denis, Laurent Zarka, Philippe Lecacheux, Alain
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doi_str	10.1155/ASP.2005.2686
up_date	2024-07-04T02:02:36.009Z
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