Too Many Parsecs: Star birth in the nests and filaments of Vela-C

Monday, July 16, 2012

Star birth in the nests and filaments of Vela-C

ESA's Herschel Space Observatory has imaged the Vela-C molecular cloud, revealing the cloud's reservoir of gas and dust in unprecedented detail. Vela-C is a rich stellar nursery where stars of low, intermediate and high mass are forming. The image shows how the raw material from which stars form is organised in tangled nests as well as dense, ridge-like filaments, and suggests that the two environments may be responsible for producing different populations of stars.

This image shows Vela-C, a giant molecular cloud where stars are being born, as viewed at far-infrared wavelengths with ESA's Herschel Space Observatory. Vela-C is the most massive component of the Vela Molecular Ridge, a vast star-forming complex in the plane of our Galaxy, the Milky Way.

The Vela Molecular Ridge is a vast star-forming complex in the plane of our Galaxy, the Milky Way. Observing this region at far-infrared wavelengths, ESA's Herschel Space Observatory has obtained an extraordinarily detailed image of the most massive component of this molecular complex, known as Vela-C.

Located roughly 2300 light years away, Vela-C saw the onset of star formation less than a million years ago – relatively recently on astronomical timescales. Massive, as well as low- and intermediate-mass, stars are being born in this region, making it an ideal laboratory to study the birth of different populations of stars.

This image reveals previously unseen detail in the cold mixture of gas and dust that pervades the region. Cosmic dust is a minor but crucial component of the interstellar medium and, due to its low temperature, it shines brightly at the far-infrared wavelengths that Herschel is designed to observe. By detecting emission from cosmic dust, astronomers can unravel the distribution of the raw material out of which stars form.

The coldest and densest portions of the cloud complex release most of their radiation at the longest wavelengths probed by Herschel, shown in red in this image. The cloud material is organised in a highly sub-structured network, with tangled and less organised material alternating with more defined and elongated filaments. Intricate bundles of material can be seen on the left, centre and right of the image. These nest-like structures are linked to one another by dense, ridge-like filaments.

A number of white flecks dot the clouds and, in particular, the prominent ridge-like filaments in Vela-C. These flecks are in fact pre-stellar cores – compact clumps of matter that might eventually give rise to star formation – and proto-stellar cores, whose density is high enough for star formation to have already begun, eventually resulting in fully-fledged stars. As a result of Herschel's unparalleled resolution and sensitivity at these wavelengths, astronomers are able to carry out detailed studies of the properties, such as their mass and temperature, of the different cores across the nests and filaments. From the Herschel image, it appears that the majority of pre- and proto-stellar cores with large masses are found along the two densest filaments, suggesting that these sites are the most likely, in the cloud, to host the formation of massive stars.

Studies done with Herschel data seem to indicate that the ridge-like filaments in star-forming regions such as Vela-C formed from converging flows of matter in the interstellar medium. The high densities in these thick, elongated structures induce massive clumps of matter to collapse under their own gravity, giving rise to high-mass stars. The nest-like structures, on the other hand, appear to be dominated by turbulence rather than by gravity and are likely to form mainly low- and intermediate-mass stars.

Not only does Vela-C host seeds of future stellar generations, it also comprises a handful of objects that have already evolved into young, massive stars. Embedded in the central part of the image is a stellar cluster whose stars are not visible in the Herschel image, but their effects are. The butterfly-shaped structure at the centre of the image, known as RCW 36 (or Gum 20), is a result of winds and radiation released by the hot stars in this cluster. RCW 36 is an HII region – a pocket of gas that is being energised and ionised by the action of nearby young, massive stars. Due to its higher temperature relative to the colder material in the cloud, RCW 36 shines brightly at the shortest wavelengths probed by Herschel, indicated in blue in this image. In the lower right corner of the image is another HII region called RCW 34 (or Gum 19); it is unclear whether RCW 34 and the hot stars that illuminate it are part of the Vela-C molecular cloud or whether they are located farther away.

This image shows the Vela-C molecular cloud region as observed at optical (upper panel) and far-infrared (lower panel) wavelengths. The optical image is dominated by the emission from stars. The eerie orange cloud in the centre-left part of the image is an HII region known as RCW 36 (or Gum 20). Another HII region, called RCW 34 (or Gum 19), can be seen as a small orange fleck in the lower part of the image to the right. The two HII regions RCW 36 and RCW 34 stand out also in the far-infrared image. Due to their higher temperature relative to the colder material in the cloud, they shine brightly at the shortest wavelengths probed by Herschel, indicated in blue in the image. Credit: ESO/Digitized Sky Survey 2 (upper panel); ESA/PACS/SPIRE/Tracey Hill & Frédérique Motte, Laboratoire AIM Paris-Saclay, CEA/Irfu - CNRS/INSU - Univ. Paris Diderot, France (lower panel)