Cosmic Microwave Background Polarization and Temperature Power Spectra Estimation Using Linear Combination of WMAP 5 Year Maps

We estimate cosmic microwave background (CMB) polarization and temperature power spectra using Wilkinson Microwave Anisotropy Probe (WMAP) 5 year foreground contaminated maps. The power spectrum is estimated by using a model-independent method, which does not utilize directly the diffuse foreground...

Full description

Saved in:
Bibliographic Details
Published in:The Astrophysical journal 2010-05, Vol.714 (1), p.840-851
Main Authors: Samal, Pramoda Kumar, Saha, Rajib, Delabrouille, Jacques, Prunet, Simon, Jain, Pankaj, Souradeep, Tarun
Format: Article
Language:English
Subjects:
ANISOTROPY
Astronomy
Astrophysics
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
BACKGROUND RADIATION
COMPUTERIZED SIMULATION
Cosmology and Extra-Galactic Astrophysics
DATA ANALYSIS
Earth, ocean, space
ELECTROMAGNETIC RADIATION
Exact sciences and technology
MICROWAVE RADIATION
Physics
POINT SOURCES
POLARIZATION
RADIATION SOURCES
RADIATIONS
RELICT RADIATION
Sciences of the Universe
SIMULATION
SPECTRA
Citations: Items that this one cites
Items that cite this one
Online Access:Get full text
Tags: Add Tag
No Tags, Be the first to tag this record!
cited_by cdi_FETCH-LOGICAL-c449t-664c645ea8951f5b8c7f816126e90e81de81634646434d7d39854680990920df3
cites cdi_FETCH-LOGICAL-c449t-664c645ea8951f5b8c7f816126e90e81de81634646434d7d39854680990920df3
container_end_page 851
container_issue 1
container_start_page 840
container_title The Astrophysical journal
container_volume 714
creator Samal, Pramoda Kumar
Saha, Rajib
Delabrouille, Jacques
Prunet, Simon
Jain, Pankaj
Souradeep, Tarun
description We estimate cosmic microwave background (CMB) polarization and temperature power spectra using Wilkinson Microwave Anisotropy Probe (WMAP) 5 year foreground contaminated maps. The power spectrum is estimated by using a model-independent method, which does not utilize directly the diffuse foreground templates nor the detector noise model. The method essentially consists of two steps: (1) removal of diffuse foregrounds contamination by making linear combination of individual maps in harmonic space and (2) cross-correlation of foreground cleaned maps to minimize detector noise bias. For the temperature power spectrum we also estimate and subtract residual unresolved point source contamination in the cross-power spectrum using the point source model provided by the WMAP science team. Our TT, TE, and EE power spectra are in good agreement with the published results of the WMAP science team. We perform detailed numerical simulations to test for bias in our procedure. We find that the bias is small in almost all cases. A negative bias at low l in TT power spectrum has been pointed out in an earlier publication. We find that the bias-corrected quadrupole power (l(l + 1)Cl /2π) is 532 μK2, approximately 2.5 times the estimate (213.4 μK2) made by the WMAP team.
doi_str_mv 10.1088/0004-637X/714/1/840
format article
fullrecord <record><control><sourceid>proquest_osti_</sourceid><recordid>TN_cdi_osti_scitechconnect_21448861</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>849466387</sourcerecordid><originalsourceid>FETCH-LOGICAL-c449t-664c645ea8951f5b8c7f816126e90e81de81634646434d7d39854680990920df3</originalsourceid><addsrcrecordid>eNqNkV9rFDEUxYNYcK1-Al8CIkJlusnkTiZ5XJf-EXaxYIv6FNJMpo3OJGMy22If_OxmmLIv9kFCCMn9ncPNPQi9oeSYEiGWhBAoOKu_LWsKS7oUQJ6hBa2YKIBV9XO02BMv0MuUfkzXUsoF-rMOqXcGb52J4V7fWfxRm583Mex8gy9Cp6N70KMLHuv8cGn7wUY97qLNxXsb8ZfBmjFqfJJG18_gVXL-Bm-ctzrideivnZ8LocVft6sLXOHvU2mrh_QKHbS6S_b143mIrk5PLtfnxebz2af1alMYADkWnIPhUFktZEXb6lqYuhWU05JbSaygTd6cAc-LQVM3TIoKuCBSElmSpmWH6O3sG3KfKhk3WnNrgve5e1VSACE4zdSHmbrVnRpi_lD8rYJ26ny1Uc6XA1OE1JMr3E30-5keYvi1s2lUvUvGdp32NuySEiCBcybqTLKZzDNOKdp2b06JmgJUUx5qikflABXNWpJV7x79dTK6a6P2xqW9tCxrAF5B5o5nzoXhP42P_hU8AaohT-4vZZizwg</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>849466387</pqid></control><display><type>article</type><title>Cosmic Microwave Background Polarization and Temperature Power Spectra Estimation Using Linear Combination of WMAP 5 Year Maps</title><source>EZB Electronic Journals Library</source><creator>Samal, Pramoda Kumar ; Saha, Rajib ; Delabrouille, Jacques ; Prunet, Simon ; Jain, Pankaj ; Souradeep, Tarun</creator><creatorcontrib>Samal, Pramoda Kumar ; Saha, Rajib ; Delabrouille, Jacques ; Prunet, Simon ; Jain, Pankaj ; Souradeep, Tarun</creatorcontrib><description>We estimate cosmic microwave background (CMB) polarization and temperature power spectra using Wilkinson Microwave Anisotropy Probe (WMAP) 5 year foreground contaminated maps. The power spectrum is estimated by using a model-independent method, which does not utilize directly the diffuse foreground templates nor the detector noise model. The method essentially consists of two steps: (1) removal of diffuse foregrounds contamination by making linear combination of individual maps in harmonic space and (2) cross-correlation of foreground cleaned maps to minimize detector noise bias. For the temperature power spectrum we also estimate and subtract residual unresolved point source contamination in the cross-power spectrum using the point source model provided by the WMAP science team. Our TT, TE, and EE power spectra are in good agreement with the published results of the WMAP science team. We perform detailed numerical simulations to test for bias in our procedure. We find that the bias is small in almost all cases. A negative bias at low l in TT power spectrum has been pointed out in an earlier publication. We find that the bias-corrected quadrupole power (l(l + 1)Cl /2π) is 532 μK2, approximately 2.5 times the estimate (213.4 μK2) made by the WMAP team.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.1088/0004-637X/714/1/840</identifier><identifier>CODEN: ASJOAB</identifier><language>eng</language><publisher>Bristol: IOP Publishing</publisher><subject>ANISOTROPY ; Astronomy ; Astrophysics ; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ; BACKGROUND RADIATION ; COMPUTERIZED SIMULATION ; Cosmology and Extra-Galactic Astrophysics ; DATA ANALYSIS ; Earth, ocean, space ; ELECTROMAGNETIC RADIATION ; Exact sciences and technology ; MICROWAVE RADIATION ; Physics ; POINT SOURCES ; POLARIZATION ; RADIATION SOURCES ; RADIATIONS ; RELICT RADIATION ; Sciences of the Universe ; SIMULATION ; SPECTRA</subject><ispartof>The Astrophysical journal, 2010-05, Vol.714 (1), p.840-851</ispartof><rights>2015 INIST-CNRS</rights><rights>Distributed under a Creative Commons Attribution 4.0 International License</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c449t-664c645ea8951f5b8c7f816126e90e81de81634646434d7d39854680990920df3</citedby><cites>FETCH-LOGICAL-c449t-664c645ea8951f5b8c7f816126e90e81de81634646434d7d39854680990920df3</cites><orcidid>0000-0002-1755-4582</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,315,786,790,891,27957,27958</link.rule.ids><backlink>$$Uhttp://pascal-francis.inist.fr/vibad/index.php?action=getRecordDetail&amp;idt=22744654$$DView record in Pascal Francis$$Hfree_for_read</backlink><backlink>$$Uhttps://hal.in2p3.fr/in2p3-00709904$$DView record in HAL$$Hfree_for_read</backlink><backlink>$$Uhttps://www.osti.gov/biblio/21448861$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>Samal, Pramoda Kumar</creatorcontrib><creatorcontrib>Saha, Rajib</creatorcontrib><creatorcontrib>Delabrouille, Jacques</creatorcontrib><creatorcontrib>Prunet, Simon</creatorcontrib><creatorcontrib>Jain, Pankaj</creatorcontrib><creatorcontrib>Souradeep, Tarun</creatorcontrib><title>Cosmic Microwave Background Polarization and Temperature Power Spectra Estimation Using Linear Combination of WMAP 5 Year Maps</title><title>The Astrophysical journal</title><description>We estimate cosmic microwave background (CMB) polarization and temperature power spectra using Wilkinson Microwave Anisotropy Probe (WMAP) 5 year foreground contaminated maps. The power spectrum is estimated by using a model-independent method, which does not utilize directly the diffuse foreground templates nor the detector noise model. The method essentially consists of two steps: (1) removal of diffuse foregrounds contamination by making linear combination of individual maps in harmonic space and (2) cross-correlation of foreground cleaned maps to minimize detector noise bias. For the temperature power spectrum we also estimate and subtract residual unresolved point source contamination in the cross-power spectrum using the point source model provided by the WMAP science team. Our TT, TE, and EE power spectra are in good agreement with the published results of the WMAP science team. We perform detailed numerical simulations to test for bias in our procedure. We find that the bias is small in almost all cases. A negative bias at low l in TT power spectrum has been pointed out in an earlier publication. We find that the bias-corrected quadrupole power (l(l + 1)Cl /2π) is 532 μK2, approximately 2.5 times the estimate (213.4 μK2) made by the WMAP team.</description><subject>ANISOTROPY</subject><subject>Astronomy</subject><subject>Astrophysics</subject><subject>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</subject><subject>BACKGROUND RADIATION</subject><subject>COMPUTERIZED SIMULATION</subject><subject>Cosmology and Extra-Galactic Astrophysics</subject><subject>DATA ANALYSIS</subject><subject>Earth, ocean, space</subject><subject>ELECTROMAGNETIC RADIATION</subject><subject>Exact sciences and technology</subject><subject>MICROWAVE RADIATION</subject><subject>Physics</subject><subject>POINT SOURCES</subject><subject>POLARIZATION</subject><subject>RADIATION SOURCES</subject><subject>RADIATIONS</subject><subject>RELICT RADIATION</subject><subject>Sciences of the Universe</subject><subject>SIMULATION</subject><subject>SPECTRA</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2010</creationdate><recordtype>article</recordtype><recordid>eNqNkV9rFDEUxYNYcK1-Al8CIkJlusnkTiZ5XJf-EXaxYIv6FNJMpo3OJGMy22If_OxmmLIv9kFCCMn9ncPNPQi9oeSYEiGWhBAoOKu_LWsKS7oUQJ6hBa2YKIBV9XO02BMv0MuUfkzXUsoF-rMOqXcGb52J4V7fWfxRm583Mex8gy9Cp6N70KMLHuv8cGn7wUY97qLNxXsb8ZfBmjFqfJJG18_gVXL-Bm-ctzrideivnZ8LocVft6sLXOHvU2mrh_QKHbS6S_b143mIrk5PLtfnxebz2af1alMYADkWnIPhUFktZEXb6lqYuhWU05JbSaygTd6cAc-LQVM3TIoKuCBSElmSpmWH6O3sG3KfKhk3WnNrgve5e1VSACE4zdSHmbrVnRpi_lD8rYJ26ny1Uc6XA1OE1JMr3E30-5keYvi1s2lUvUvGdp32NuySEiCBcybqTLKZzDNOKdp2b06JmgJUUx5qikflABXNWpJV7x79dTK6a6P2xqW9tCxrAF5B5o5nzoXhP42P_hU8AaohT-4vZZizwg</recordid><startdate>20100501</startdate><enddate>20100501</enddate><creator>Samal, Pramoda Kumar</creator><creator>Saha, Rajib</creator><creator>Delabrouille, Jacques</creator><creator>Prunet, Simon</creator><creator>Jain, Pankaj</creator><creator>Souradeep, Tarun</creator><general>IOP Publishing</general><general>IOP</general><general>American Astronomical Society</general><scope>IQODW</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>KL.</scope><scope>1XC</scope><scope>OTOTI</scope><orcidid>https://orcid.org/0000-0002-1755-4582</orcidid></search><sort><creationdate>20100501</creationdate><title>Cosmic Microwave Background Polarization and Temperature Power Spectra Estimation Using Linear Combination of WMAP 5 Year Maps</title><author>Samal, Pramoda Kumar ; Saha, Rajib ; Delabrouille, Jacques ; Prunet, Simon ; Jain, Pankaj ; Souradeep, Tarun</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c449t-664c645ea8951f5b8c7f816126e90e81de81634646434d7d39854680990920df3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2010</creationdate><topic>ANISOTROPY</topic><topic>Astronomy</topic><topic>Astrophysics</topic><topic>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</topic><topic>BACKGROUND RADIATION</topic><topic>COMPUTERIZED SIMULATION</topic><topic>Cosmology and Extra-Galactic Astrophysics</topic><topic>DATA ANALYSIS</topic><topic>Earth, ocean, space</topic><topic>ELECTROMAGNETIC RADIATION</topic><topic>Exact sciences and technology</topic><topic>MICROWAVE RADIATION</topic><topic>Physics</topic><topic>POINT SOURCES</topic><topic>POLARIZATION</topic><topic>RADIATION SOURCES</topic><topic>RADIATIONS</topic><topic>RELICT RADIATION</topic><topic>Sciences of the Universe</topic><topic>SIMULATION</topic><topic>SPECTRA</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Samal, Pramoda Kumar</creatorcontrib><creatorcontrib>Saha, Rajib</creatorcontrib><creatorcontrib>Delabrouille, Jacques</creatorcontrib><creatorcontrib>Prunet, Simon</creatorcontrib><creatorcontrib>Jain, Pankaj</creatorcontrib><creatorcontrib>Souradeep, Tarun</creatorcontrib><collection>Pascal-Francis</collection><collection>CrossRef</collection><collection>Meteorological &amp; Geoastrophysical Abstracts</collection><collection>Meteorological &amp; Geoastrophysical Abstracts - Academic</collection><collection>Hyper Article en Ligne (HAL)</collection><collection>OSTI.GOV</collection><jtitle>The Astrophysical journal</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Samal, Pramoda Kumar</au><au>Saha, Rajib</au><au>Delabrouille, Jacques</au><au>Prunet, Simon</au><au>Jain, Pankaj</au><au>Souradeep, Tarun</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Cosmic Microwave Background Polarization and Temperature Power Spectra Estimation Using Linear Combination of WMAP 5 Year Maps</atitle><jtitle>The Astrophysical journal</jtitle><date>2010-05-01</date><risdate>2010</risdate><volume>714</volume><issue>1</issue><spage>840</spage><epage>851</epage><pages>840-851</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><coden>ASJOAB</coden><notes>ObjectType-Article-1</notes><notes>SourceType-Scholarly Journals-1</notes><notes>ObjectType-Feature-2</notes><notes>content type line 23</notes><abstract>We estimate cosmic microwave background (CMB) polarization and temperature power spectra using Wilkinson Microwave Anisotropy Probe (WMAP) 5 year foreground contaminated maps. The power spectrum is estimated by using a model-independent method, which does not utilize directly the diffuse foreground templates nor the detector noise model. The method essentially consists of two steps: (1) removal of diffuse foregrounds contamination by making linear combination of individual maps in harmonic space and (2) cross-correlation of foreground cleaned maps to minimize detector noise bias. For the temperature power spectrum we also estimate and subtract residual unresolved point source contamination in the cross-power spectrum using the point source model provided by the WMAP science team. Our TT, TE, and EE power spectra are in good agreement with the published results of the WMAP science team. We perform detailed numerical simulations to test for bias in our procedure. We find that the bias is small in almost all cases. A negative bias at low l in TT power spectrum has been pointed out in an earlier publication. We find that the bias-corrected quadrupole power (l(l + 1)Cl /2π) is 532 μK2, approximately 2.5 times the estimate (213.4 μK2) made by the WMAP team.</abstract><cop>Bristol</cop><pub>IOP Publishing</pub><doi>10.1088/0004-637X/714/1/840</doi><tpages>12</tpages><orcidid>https://orcid.org/0000-0002-1755-4582</orcidid></addata></record>
fulltext fulltext
identifier ISSN: 0004-637X
ispartof The Astrophysical journal, 2010-05, Vol.714 (1), p.840-851
issn 0004-637X
1538-4357
language eng
recordid cdi_osti_scitechconnect_21448861
source EZB Electronic Journals Library
subjects ANISOTROPY
Astronomy
Astrophysics
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
BACKGROUND RADIATION
COMPUTERIZED SIMULATION
Cosmology and Extra-Galactic Astrophysics
DATA ANALYSIS
Earth, ocean, space
ELECTROMAGNETIC RADIATION
Exact sciences and technology
MICROWAVE RADIATION
Physics
POINT SOURCES
POLARIZATION
RADIATION SOURCES
RADIATIONS
RELICT RADIATION
Sciences of the Universe
SIMULATION
SPECTRA
title Cosmic Microwave Background Polarization and Temperature Power Spectra Estimation Using Linear Combination of WMAP 5 Year Maps
url http://sfxeu10.hosted.exlibrisgroup.com/loughborough?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2024-09-23T03%3A12%3A40IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_osti_&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=Cosmic%20Microwave%20Background%20Polarization%20and%20Temperature%20Power%20Spectra%20Estimation%20Using%20Linear%20Combination%20of%20WMAP%205%20Year%20Maps&rft.jtitle=The%20Astrophysical%20journal&rft.au=Samal,%20Pramoda%20Kumar&rft.date=2010-05-01&rft.volume=714&rft.issue=1&rft.spage=840&rft.epage=851&rft.pages=840-851&rft.issn=0004-637X&rft.eissn=1538-4357&rft.coden=ASJOAB&rft_id=info:doi/10.1088/0004-637X/714/1/840&rft_dat=%3Cproquest_osti_%3E849466387%3C/proquest_osti_%3E%3Cgrp_id%3Ecdi_FETCH-LOGICAL-c449t-664c645ea8951f5b8c7f816126e90e81de81634646434d7d39854680990920df3%3C/grp_id%3E%3Coa%3E%3C/oa%3E%3Curl%3E%3C/url%3E&rft_id=info:oai/&rft_pqid=849466387&rft_id=info:pmid/&rfr_iscdi=true