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Galaxy spin as a formation probe: the stellar-to-halo specific angular momentum relation

Posti, Lorenzo; Pezzulli, Gabriele; Fraternali, F; Di Teodoro, Enrico Maria

Description

We derive the stellar-to-halo specific angular momentum relation (SHSAMR) of galaxies at z = 0 by combining (i) the standard Acold dark matter tidal torque theory, (ii) the observed relation between stellar mass and specific angular momentum (the Fall relation), and (iii) various determinations of the stellar-to-halo mass relation (SHMR). We find that the ratio f(j) = j(*)/j(h) of the specific angular momentum of stars to that of the dark matter (i) varies with mass as a double power law, (ii)...[Show more]

dc.contributor.authorPosti, Lorenzo
dc.contributor.authorPezzulli, Gabriele
dc.contributor.authorFraternali, F
dc.contributor.authorDi Teodoro, Enrico Maria
dc.date.accessioned2019-12-17T01:11:19Z
dc.date.available2019-12-17T01:11:19Z
dc.identifier.issn0035-8711
dc.identifier.urihttp://hdl.handle.net/1885/195630
dc.description.abstractWe derive the stellar-to-halo specific angular momentum relation (SHSAMR) of galaxies at z = 0 by combining (i) the standard Acold dark matter tidal torque theory, (ii) the observed relation between stellar mass and specific angular momentum (the Fall relation), and (iii) various determinations of the stellar-to-halo mass relation (SHMR). We find that the ratio f(j) = j(*)/j(h) of the specific angular momentum of stars to that of the dark matter (i) varies with mass as a double power law, (ii) always has a peak in the mass range explored and iii) is three to five times larger for spirals than for ellipticals. The results have some dependence on the adopted SHMR and we provide fitting formulae in each case. For any choice of the SHMR, the peak of f(j) occurs at the same mass where the stellar-to-halo mass ratio f(*) = M-*/M-h has a maximum. This is mostly driven by the straightness and tightness of the Fall relation, which requires f(j) and f(*) to be correlated with each other roughly as f(j) proportional to f(*)(2/3), as expected if the outer and more angular momentum rich parts of a halo failed to accrete on to the central galaxy and form stars (biased collapse). We also confirm that the difference in the angular momentum of spirals and ellipticals at a given mass is too large to be ascribed only to different spins of the parent dark-matter haloes (spin bias).
dc.description.sponsorshipLP acknowledges financial support from a Vici grant from NWO. GP acknowledges support from the Swiss National Foundation grant PP00P2_163824. EDT acknowledges the support of the Australian Research Council (ARC) through grant DP160100723.
dc.format.mimetypeapplication/pdf
dc.language.isoen_AU
dc.publisherOxford University Press on behalf of the Royal Astronomical Society
dc.rights© 2017 The Author(s)
dc.sourceMonthly Notices of the Royal Astronomical Society
dc.subjectgalaxies: elliptical and lenticular
dc.subjectcD
dc.subjectgalaxies: formation
dc.subjectgalaxies: fundamental parameters
dc.subjectgalaxies: haloes, galaxies: spiral
dc.titleGalaxy spin as a formation probe: the stellar-to-halo specific angular momentum relation
dc.typeJournal article
local.description.notesImported from ARIES
local.identifier.citationvolume475
dcterms.dateAccepted2017-12-05
dc.date.issued2018-12-08
local.identifier.absfor020110 - Stellar Astronomy and Planetary Systems
local.identifier.absfor020103 - Cosmology and Extragalactic Astronomy
local.identifier.ariespublicationu4485658xPUB2189
local.publisher.urlhttps://academic.oup.com
local.type.statusPublished Version
local.contributor.affiliationPosti, Lorenzo, University of Groningen
local.contributor.affiliationPezzulli, Gabriele, ETH Zurich
local.contributor.affiliationFraternali, F, University of Bologna
local.contributor.affiliationDi Teodoro, Enrico, College of Science, ANU
dc.relationhttp://purl.org/au-research/grants/arc/DP160100723
local.bibliographicCitation.issue1
local.bibliographicCitation.startpage232
local.bibliographicCitation.lastpage243
local.identifier.doi10.1093/mnras/stx3168
local.identifier.absseo970102 - Expanding Knowledge in the Physical Sciences
dc.date.updated2019-07-28T08:20:09Z
local.identifier.scopusID2-s2.0-85041317491
local.identifier.thomsonID000427144200018
dcterms.accessRightsOpen Access
dc.provenancehttp://sherpa.ac.uk/romeo/issn/0035-8711/..."author can archive publisher's version/PDF" from SHERPA/RoMEO site (as at 17/12/19)
CollectionsANU Research Publications

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