uu.seUppsala University Publications
Change search
CiteExportLink to record
Permanent link

Direct link
Cite
Citation style
  • apa
  • ieee
  • modern-language-association
  • vancouver
  • Other style
More styles
Language
  • de-DE
  • en-GB
  • en-US
  • fi-FI
  • nn-NO
  • nn-NB
  • sv-SE
  • Other locale
More languages
Output format
  • html
  • text
  • asciidoc
  • rtf
The GALAH survey: stellar streams and how stellar velocity distributions vary with Galactic longitude, hemisphere, and metallicity
Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA.
Australian Astron Observ, 105 Delhi Rd, N Ryde, NSW 2113, Australia;Univ Sydney, Sch Phys, Sydney Inst Astron, A28, Sydney, NSW 2006, Australia.
Univ Sydney, Sch Phys, Sydney Inst Astron, A28, Sydney, NSW 2006, Australia.
Univ Sydney, Sch Phys, Sydney Inst Astron, A28, Sydney, NSW 2006, Australia;Australian Res Council, Ctr Excellence All Sky Astrophys Dimens 3 ASTRO 3, Canberra, ACT 72611, Australia.
Show others and affiliations
2018 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 478, no 1, p. 228-254Article in journal (Refereed) Published
Abstract [en]

Using GALAH (GALactic Archaeology with HERMES) survey data of nearby stars, we look at how structure in the planar (u, v) velocity distribution depends on metallicity and on viewing direction within the Galaxy. In nearby stars with distance d less than or similar to 1 kpc, the Hercules stream is most strongly seen in higher metallicity stars [Fe/H] > 0.2. The Hercules stream peak v value depends on viewed galactic longitude, which we interpret as due to the gap between the stellar stream and more circular orbits being associated with a specific angular momentum value of about 16.40 km s(-1) kpc. The association of the gap with a particular angular momentum value supports a bar resonant model for the Hercules stream. Moving groups previously identified in Hipparcos (High Precision Parallax COllecting Satellite) observations are easiest to see in stars nearer than 250 pc, and their visibility and peak velocities in the velocity distributions depends on both viewing direction (galactic longitude and hemisphere) and metallicity. We infer that there is fine structure in local velocity distributions that varies over distances of a few hundred pc in the Galaxy.

Place, publisher, year, edition, pages
OXFORD UNIV PRESS , 2018. Vol. 478, no 1, p. 228-254
Keywords [en]
Galaxy: disc, Galaxy: evolution, Galaxy: kinematics and dynamics
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:uu:diva-362163DOI: 10.1093/mnras/sty865ISI: 000439501300017OAI: oai:DiVA.org:uu-362163DiVA, id: diva2:1255552
Available from: 2018-10-12 Created: 2018-10-12 Last updated: 2018-10-12Bibliographically approved

Open Access in DiVA

No full text in DiVA

Other links

Publisher's full text

Authority records BETA

Lind, Karin

Search in DiVA

By author/editor
Buder, SvenLind, KarinSimpson, Jeffrey D.Casagrande, LucaTing, Yuan-Sen
By organisation
Observational Astronomy
In the same journal
Monthly notices of the Royal Astronomical Society
Astronomy, Astrophysics and Cosmology

Search outside of DiVA

GoogleGoogle Scholar

doi
urn-nbn

Altmetric score

doi
urn-nbn
Total: 14 hits
CiteExportLink to record
Permanent link

Direct link
Cite
Citation style
  • apa
  • ieee
  • modern-language-association
  • vancouver
  • Other style
More styles
Language
  • de-DE
  • en-GB
  • en-US
  • fi-FI
  • nn-NO
  • nn-NB
  • sv-SE
  • Other locale
More languages
Output format
  • html
  • text
  • asciidoc
  • rtf