The UvA-LINKER will give you a range of other options to find the full text of a publication (including a direct link to the full-text if it is located on another database on the internet).
De UvA-LINKER biedt mogelijkheden om een publicatie elders te vinden (inclusief een directe link naar de publicatie online als deze beschikbaar is in een database op het internet).


Zoekopdracht: journal id: "astrophysicalxjournal"

AuteursA. Bik, E. Puga, L.B.F.M. Waters, M. Horrobin, T. Henning, T. Vasyunina, H. Beuther, H. Linz, L. Kaper, M. van den Ancker, A. Lenorzer, E. Churchwell, S. Kurtz, M.B.N. Kouwenhoven, A. Stolte, A. de Koter, W.F. Thi, F. ComerĂ³n, C. Waelkens
TitelSequential star formation in RCW 34: a spectroscopic census of the stellar content of high-mass star-forming regions
TijdschriftAstrophysical Journal
FaculteitFaculteit der Natuurwetenschappen, Wiskunde en Informatica
Instituut/afd.FNWI: Astronomical Institute Anton Pannekoek (IAP)
SamenvattingIn this paper, we present VLT/SINFONI integral field spectroscopy of RCW 34 along with Spitzer/IRAC photometry of the surroundings. RCW 34 consists of three different regions. A large bubble has been detected in the IRAC images in which a cluster of intermediate-and low-mass class II objects is found. At the northern edge of this bubble, an Hii region is located, ionized by 3 OB stars, of which the most massive star has spectral type O8.5V. Intermediate-mass stars (2-3M(circle dot)) are detected of G-and K-spectral type. These stars are still in the pre-main-sequence (PMS) phase. North of the Hii region, a photon-dominated region is present, marking the edge of a dense molecular cloud traced by H-2 emission. Several class 0/I objects are associated with this cloud, indicating that star formation is still taking place. The distance to RCW 34 is revised to 2.5 +/- 0.2 kpc and an age estimate of 2 +/- 1 Myr is derived from the properties of the PMS stars inside the Hii region. Between the class II sources in the bubble and the PMS stars in the Hii region, no age difference could be detected with the present data. The presence of the class 0/I sources in the molecular cloud, however, suggests that the objects inside the molecular cloud are significantly younger. The most likely scenario for the formation of the three regions is that star formation propagated from south to north. First the bubble is formed, produced by intermediate-and low-mass stars only, after that, the Hii region is formed from a dense core at the edge of the molecular cloud, resulting in the expansion similar to a champagne flow. More recently, star formation occurred in the rest of the molecular cloud. Two different formation scenarios are possible. (1) The bubble with the cluster of low-and intermediate-mass stars triggered the formation of the O star at the edge of the molecular cloud, which in its turn induces the current star formation in the molecular cloud. (2) An external triggering is responsible for the star formation propagating from south to north.
Soort documentArtikel
Document finderUvA-Linker