2019
DOI: 10.1093/mnrasl/slz146 View full text |Buy / Rent full text
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Abstract: The universe region obscured by the Milky Way is very large and only future blind large HI redshift, and targeted peculiar surveys on the outer borders will determine how much mass is hidden there. Meanwhile, we apply for the first time two independent techniques to the galaxy peculiar velocity catalog CosmicF lows−3 in order to explore for the kinematic signature of a specific large-scale structure hidden behind this zone : the Vela supercluster at cz ∼ 18, 000,km s −1 . Using the gravitational velocity and d… Show more

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“…The V-web has been employed on observational data for years because the cosmic velocity field can be inferred from accurate measurement of extra-galactic distances, redshifts and peculiar velocities as in the CosmicFlows projects (Tully et al 2016;Kourkchi et al 2020). This method is useful and powerful because a quantification of the peculiar velocity field can lead to the identification of basins of attraction and repulsion (Dupuy et al 2019) as well as the discovery of super clusters like Vela (Kraan-Korteweg et al 2017;Courtois et al 2019) and Laniakea, our home supercluster (Tully et al 2014). This opens the door for COWS to be applied to observational data and verify filamentary structures in our local Universe, that before have only been identified through visual inspection, and perhaps uncover new, undiscovered cosmic filaments.…”
Section: Discussionmentioning
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“…The V-web has been employed on observational data for years because the cosmic velocity field can be inferred from accurate measurement of extra-galactic distances, redshifts and peculiar velocities as in the CosmicFlows projects (Tully et al 2016;Kourkchi et al 2020). This method is useful and powerful because a quantification of the peculiar velocity field can lead to the identification of basins of attraction and repulsion (Dupuy et al 2019) as well as the discovery of super clusters like Vela (Kraan-Korteweg et al 2017;Courtois et al 2019) and Laniakea, our home supercluster (Tully et al 2014). This opens the door for COWS to be applied to observational data and verify filamentary structures in our local Universe, that before have only been identified through visual inspection, and perhaps uncover new, undiscovered cosmic filaments.…”
Section: Discussionmentioning
“…This model has also been successful in constraining group masses (Pivato et al 2006), although we notice relevant departures from this simple picture given that the mass distribution around groups is strongly anisotropic due to the network of filaments, walls, and clusters dominating the largescale Universe. For this reason, the velocity fields surrounding groups exhibit a significant variance that is strongly connected to surrounding large-scale structures (Kashibadze et al 2020;Courtois et al 2019;Tully et al 2019;Libeskind et al 2015). These effects have been reported and analyzed in numerical simulations (Ceccarelli et al 2011), and in this work we aim to obtain observational counterparts of these theoretical results.…”
Section: Velocity Field Anisotropiesmentioning
“…The requirement for such a survey has been highlighted for several decades to fully explain the CMB dipole anisotropy, a well-known signature caused by the peculiar motion of the Milky Way (Lineweaver et al 1996;Rauzy & Gurzadyan 1998). This motion cannot adequately be accounted for due to the obscuration by the ZoA of large mass concentrations such as the Great Attractor (Lynden-Bell et al 1988;Kraan-Korteweg & Lahav 2000) and the recently-discovered Vela Supercluster (Kraan-Korteweg et al 2015, 2017Courtois et al 2019). While a truly whole-sky magnitude-limited redshift survey does not exist, imaging surveys have been made of the entire sky.…”
Section: Introductionmentioning
“…These catalogues can be complementary to dedicated surveys within the ZoA (e.g., Staveley-Smith et al 2016;Ramatsoku et al 2016;Kraan-Korteweg et al 2018). A complete whole-sky local-universe group catalogue is also required to quantify other large-scale structures such as filaments and voids (Alpaslan et al 2014), which are useful in conjunction with other studies of galaxy flows due to large-scale structures in the local Universe (Pomarède et al 2017;Courtois et al 2019;Tully et al 2019). Furthermore, a complete 2MRS group catalogue based on spectroscopic redshifts can be compared to one based on photometric redshift estimates (2MPZ, Bilicki et al 2014), which may improve the accuracy of the latter technique.…”
Section: Introductionmentioning