A complete ^\mathsf12CO 2-1 map of M 51 with HERA

2006/09/25 by K. F. Schuster, K. Schüster, C. Krämer +5 · 2 citations
Mathematics · Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Star Formation Studies #Context (archaeology) #Face (sociological concept) #Galaxies: Formation, Evolution, Phenomena #Galaxy #Geography #HERA #Linguistics #Mathematical analysis #Mathematics #Particle physics #Philosophy #Physics #Spiral (railway) #Spiral galaxy #Star (game theory) #Star formation #astro-ph

paper · pdf · doi:10.1051/0004-6361:20065579

accepted by A&A

arxiv created 2006/09/25 · openalex publication_date 2006/09/26 · arxiv updated 2009/12/01 · openalex created_date 2022/08/27 · openalex updated_date 2026/07/31

Abstract

Context. The mechanisms governing the star formation rate in spiral galaxies are not yet clear. The nearby, almost face-on, and interacting galaxy M 51 offers an excellent opportunity to study at high spatial resolutions the local star formation laws.

Citations

• CI and CO in the center of M 51
• Formation of Globular Clusters in Galaxy Mergers
• Control of Star Formation in Galaxies by Gravitational Instability
• The galactic infrared/submillimeter dust radiation
• Radio Emission from Normal Galaxies

Cited by

• A simple model for the relationship between star formation and surface density
• THE STAR FORMATION EFFICIENCY IN NEARBY GALAXIES: MEASURING WHERE GAS FORMS STARS EFFECTIVELY