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Large Scale Distribution of Galaxies

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Large Scale Distribution of Galaxies Large scale distribution of galaxies Projections on the sky Pie diagrams Motion of galaxies Constrained simulations Voids Galaxies: effects of environment Projection 1986ApJ...302L...1D 1986ApJ...302L...1D 1986ApJ...302L...1D 1986ApJ...302L...1D 1986ApJ...302L...1D 1986ApJ...302L...1D 168 O. Lahav et al. For comparison, we also apply our analysis to the complete which the density of galaxies is enhanced can be found by IRAS 1.2-Jy sample (Fisher et al. 1995a; Strauss et al. 1992), calculating the covariance matrix: I x^ x^ , where the ij gal i j which includes 5313 galaxies over 87.6 per cent of the sky. The Cartesian axes xÃi i 1; 2; 3 are defined for a unit sphere. The P ZOA in IRAS was interpolated according to the Yahil et al. (1991) matrix Iij can be diagonalized (cf. Section 4.2) and the smallest procedure mentioned above. Hereafter, we refer to this sample as eigenvector indicates the direction of the normal to the great the IRAS sample. We note that the ORS and IRAS samples are not circle. We considered the projected IRAS galaxy distribution out to really independent; roughly 60 per cent of the IRAS 1.2-Jy 40 and 80 h21 Mpc, and found that the great circle is aligned with galaxies out to 80 h21 Mpc are also catalogued in the ORS the standard de Vaucouleurs' SGP to within 198 and 78, magnitude-limited sample. respectively. Can we see the translation of the great circle to a We work purely in Local Group redshift space, except in plane in three dimensions? Fig. 1 shows the distribution of Section 6 on Wiener reconstruction. galaxies projected on the sky in the IRAS and ORS samples. The distribution is highly non-isotropic, and the SGP is clearly the most prominent feature. We note that the structures seen in ORS 3 A B R I E F T O U R O F T H E S G P and IRAS are quite similar, but the ORS map is more densely sampled, and clusters are more prominent. Fig. 2 shows the raw In this section, we first show the distribution of galaxies in the distributions, of ORS and IRAS galaxies, uncorrected for selection samples projected on to the various supergalactic planes. We then effects, in a sphere of radius of 40 h21 Mpc projected on the quantify this by calculating the density field in shells as a function standard (SGX±SGZ ), (SGX±SGY ) and (SGY±SGZ ) planes. The of SGZ. Finally, we quantify the centre of mass of the overdensity. SGP is particularly visible edge-on in the (SGX±SGZ ) and (SGY±SGZ ) projections. Maps of the smoothed density field, after applying the 3.1 Visual impression appropriate weights, are shown elsewhere for the IRAS survey Historically, the SGP was identified in projected 2D maps. We (Saunders et al. 1991; Strauss et al. 1992; Fisher et al. 1995b; used the IRAS data (which is uniformly sampled over the sky) to Strauss & Willick 1995; Webster, Lahav & Fisher 1997) and for revisit the 2D appearance of the SGP by fitting the data to a great ORS (Santiago et al. 1995, 1996; Baker et al. 1998). In Figs 3 circle. For a projected distribution of sources the great circle along and 4 we show histograms of the galaxy density field d, corrected 168 O. Lahav et al. For comparison, we also apply our analysis to the complete which the density of galaxies is enhanced can be found by IRAS 1.2-Jy sample (Fisher et al. 1995a; Strauss et al. 1992), calculating the covariance matrix: I x^ x^ , where the 168 O. Lahav et al. ij gal i j which includes 5313 galaxies over 87.6 per cent of the sky. The Cartesian axes xÃi i 1; 2; 3 are defined for a unit sphere. The P ZOA in IRAS was interpolated according to the YahilForet al.comparison,(1991) matrixwe alsoIij canapplybe diagonalizedour analysis(cf. Sectionto 4.2)the andcompletethe smallest which the density of galaxies is enhanced can be found by procedure mentioned above. Hereafter, we refer to this sample as eigenvector indicates the direction of the normal to the great the IRAS sample. We note that the ORS and IRASIRASsamples1.2-Jyare notsamplecircle.(FisherWe consideredet al.the1995a;projectedStraussIRAS galaxyet distributional. 1992),out to calculating the covariance matrix: Iij galx^ix^j, where the 21 really independent; roughly 60 per cent of whichthe IRASincludes1.2-Jy 531340 andgalaxies80 h Mpc,overand87.6foundperthatcentthe greatof circlethe skis alignedy. Thewith Cartesian axes xÃi i 1; 2; 3 are defined for a unit sphere. The 21 galaxies out to 80 h Mpc are also cataloguedZOAinintheIRASORSwas interpolatedthe standard deaccordingVaucouleurs'to theSGPYahilto withinet al.19(1991)8 and 78, matrix I can be diagonalized (cf. Section P4.2) and the smallest magnitude-limited sample. respectively. Can we see the translation of the great circle to a ij We work purely in Local Group redshiftprocedurespace, exceptmentionedin planeabovin threee. Hereafterdimensions?, weFig.refer1 shotowsthisthesampledistributionas of eigenvector indicates the direction of the normal to the great Section 6 on Wiener reconstruction. the IRAS sample. Wgalaxiese noteprojectedthat theonORSthe skyandin theIRASIRASsamplesand ORS samples.are notThe circle. We considered the projected IRAS galaxy distribution out to really independent;distributionroughlyis highly60 pernon-isotropic,cent of andthetheIRASSGP is 1.2-Jyclearly the 40 and 80 h21 Mpc, and found that the great circle is aligned with most2prominent1 feature. We note that the structures seen in ORS 3 A B R I E F T O U R O F T H E S G P galaxies out to 80andh IRASMpcare quiteare similaralso , cataloguedbut the ORS mapin isthemoreORSdensely the standard de Vaucouleurs' SGP to within 198 and 78, magnitude-limited sampled,sample.and clusters are more prominent. Fig. 2 shows the raw respectively. Can we see the translation of the great circle to a In this section, we first show the distribution of galaxies in the Mon. Not. R. Astron. Soc. 312, 166±176 (2000) distributions, of ORS and IRAS galaxies, uncorrected for selection samples projected on to the various supergalactic planes.We workWe thenpurely in Local Group redshift space, except in plane in three dimensions? Fig. 1 shows the distribution of effects, in a sphere of radius of 40 h21 Mpc projected on the quantify this by calculating the density field in shells as a function Section 6 on Wienerstandardreconstruction.(SGX±SGZ ), (SGX±SGY ) and (SGY±SGZ ) planes. The galaxies projected on the sky in the IRAS and ORS samples. The of SGZ. Finally, we quantify the centre of mass of the overdensity. The supergalactic plane revisited with theSGPOpticalis particularlyRedshiftvisible edge-onSurveyin the (SGX±SGZ ) and distribution is highly non-isotropic, and the SGP is clearly the (SGY±SGZ ) projections. most prominent feature. We note that the structures seen in ORS Maps of the smoothed density field, after applying the 3.1 Visual impr1,2wession 3 1 4 5 and IRAS are quite similar, but the ORS map is more densely O. Lahav, B. X. Santiago, A.3 M.A WB RebsterI E F, TMichaelappropriateO U R OA.weights,F TStrauss,HareE shoS Gwn²PMelse. whereDavis,for the IRAS survey Historically, the6SGP was identified in projected7 2D maps. We (Saunders et al. 1991; Strauss et al. 1992; Fisher et al. 1995b; sampled, and clusters are more prominent. Fig. 2 shows the raw A.usedDresslerthe IRAS dataand(whichJ.isPuniformly. HuchrasampledInovthiser thesection,sky) to weStraussfirst &shoWwillickthe1995;distributionWebster, Lahavof &galaxiesFisher 1997)in theand for 1Institute of Astronomy, Madingley Road, Cambridge CB3 0HA distributions, of ORS and IRAS galaxies, uncorrected for selection revisit the 2D appearance of the SGP by fittingsamplesthe data to projecteda great onORSto(Santiagothe variouset al. 1995,supergal1996;acticBakerplanes.et al. 1998).We InthenFigs 3 21 2Racah Institute of Physics, The Hebrew University, Jerusalem 91904, Israel circle. For a projected distribution of sources the great circle along and 4 we show histograms of the galaxy density field d, corrected effects, in a sphere of radius of 40 h Mpc projected on the 3Instituto de FõÂsica, Universidade Federal do Rio Grandquantifye do Sul, 91501-970,this byPortocalculatingAlegre, RS, Braztheil density field in shells as a function 4 standard (SGX±SGZ ), (SGX±SGY ) and (SGY±SGZ ) planes. The Princeton University Observatory, Princeton, NJ 08544,ofUSASGZ. Finally, we quantify the centre of mass of the overdensity. 5Physics and Astronomy Departments, University of California, Berkeley, CA 94720, USA SGP is particularly visible edge-on in the (SGX±SGZ ) and 6Observatories of the Carnegie Institution, 813 Santa Barbara St, Pasadena, CA 91101, USA 7Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA (SGY±SGZ ) projections. Maps of the smoothed density field, after applying the 3.1 Visual impression appropriate weights, are shown elsewhere for the IRAS survey Accepted 1999 September 20. ReceiveD 1999 September 6; in original form 1998 October 5 Historically, the SGP was identified in projected 2D maps. We (Saunders et al. 1991; Strauss et al. 1992; Fisher et al. 1995b; used the IRAS data (which is uniformly sampled over the sky) to Strauss & Willick 1995; Webster, Lahav & Fisher 1997) and for A B S T R A CreTvisit the 2D appearance of the SGP by fitting the data to a great ORS (Santiago et al. 1995, 1996; Baker et al. 1998). In Figs 3 We re-examine the existence and extent of the planar structure in the local galaxy density field, the so-calledcircle. supergalacticFor a projectedplanedistrib(SGP).utionThis ofstructuresourcesis studtheiedgreatherecirclein threealong and 4 we show histograms of the galaxy density field d, corrected dimensions using both the new Optical Redshift Survey (ORS) and the IRAS 1.2-Jy redshift survey.
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