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Article: The dipole anisotropy of the 2 Micron All-Sky Redshift Survey

TitleThe dipole anisotropy of the 2 Micron All-Sky Redshift Survey
Authors
KeywordsCosmology: observations
Infrared: galaxies
Methods: data analysis
Local Group
Large-scale structure of Universe
Issue Date2006
Citation
Monthly Notices of the Royal Astronomical Society, 2006, v. 368, n. 4, p. 1515-1526 How to Cite?
AbstractWe estimate the acceleration on the Local Group (LG) from the 2 Micron All-Sky Redshift Survey (2MRS). The sample used includes about 23 200 galaxies with extinction-corrected magnitudes brighter than and it allows us to calculate the flux-weighted dipole. The near-infrared flux-weighted dipoles are very robust because they closely approximate a mass-weighted dipole, bypassing the effects of redshift distortions and require no preferred reference frame. This is combined with the redshift information to determine the change in dipole with distance. The misalignment angle between the LG and the cosmic microwave background (CMB) dipole drops to at around , but then increases at larger distances, reaching at around . Exclusion of the galaxies Maffei 1, Maffei 2, Dwingeloo 1, IC342 and M87 brings the resultant flux dipole to away from the CMB velocity dipole. In both cases, the dipole seemingly converges by . Assuming convergence, the comparison of the 2MRS flux dipole and the CMB dipole provides a value for the combination of the mass density and luminosity bias parameters. © 2006 RAS.
Persistent Identifierhttp://hdl.handle.net/10722/208850
ISSN
2015 Impact Factor: 4.952
2015 SCImago Journal Rankings: 2.806

 

DC FieldValueLanguage
dc.contributor.authorErdoǧdu, Pirin-
dc.contributor.authorHuchra, John P.-
dc.contributor.authorLahav, Ofer-
dc.contributor.authorColless, Matthew-
dc.contributor.authorCutri, Roc M.-
dc.contributor.authorFalco, Emilio E.-
dc.contributor.authorGeorge, Teddy A.-
dc.contributor.authorJarrett, Thomas H M-
dc.contributor.authorJones, Daniel Heath-
dc.contributor.authorKochanek, Christopher S.-
dc.contributor.authorMacri, Lucas M.-
dc.contributor.authorMader, Jeff A.-
dc.contributor.authorMartimbeau, Nathalie-
dc.contributor.authorPahre, Michael A.-
dc.contributor.authorParker, Quentin A.-
dc.contributor.authorRassat, Anaïs-
dc.contributor.authorSaunders, Will J.-
dc.date.accessioned2015-03-23T02:01:56Z-
dc.date.available2015-03-23T02:01:56Z-
dc.date.issued2006-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2006, v. 368, n. 4, p. 1515-1526-
dc.identifier.issn0035-8711-
dc.identifier.urihttp://hdl.handle.net/10722/208850-
dc.description.abstractWe estimate the acceleration on the Local Group (LG) from the 2 Micron All-Sky Redshift Survey (2MRS). The sample used includes about 23 200 galaxies with extinction-corrected magnitudes brighter than and it allows us to calculate the flux-weighted dipole. The near-infrared flux-weighted dipoles are very robust because they closely approximate a mass-weighted dipole, bypassing the effects of redshift distortions and require no preferred reference frame. This is combined with the redshift information to determine the change in dipole with distance. The misalignment angle between the LG and the cosmic microwave background (CMB) dipole drops to at around , but then increases at larger distances, reaching at around . Exclusion of the galaxies Maffei 1, Maffei 2, Dwingeloo 1, IC342 and M87 brings the resultant flux dipole to away from the CMB velocity dipole. In both cases, the dipole seemingly converges by . Assuming convergence, the comparison of the 2MRS flux dipole and the CMB dipole provides a value for the combination of the mass density and luminosity bias parameters. © 2006 RAS.-
dc.languageeng-
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society-
dc.subjectCosmology: observations-
dc.subjectInfrared: galaxies-
dc.subjectMethods: data analysis-
dc.subjectLocal Group-
dc.subjectLarge-scale structure of Universe-
dc.titleThe dipole anisotropy of the 2 Micron All-Sky Redshift Survey-
dc.typeArticle-
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1111/j.1365-2966.2006.10243.x-
dc.identifier.scopuseid_2-s2.0-33744516911-
dc.identifier.volume368-
dc.identifier.issue4-
dc.identifier.spage1515-
dc.identifier.epage1526-
dc.identifier.eissn1365-2966-

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