Volume 587, March 2016
|Number of page(s)||17|
|Section||Interstellar and circumstellar matter|
|Published online||19 February 2016|
Proper motions of embedded protostellar jets in Serpens⋆
Nordic Optical Telescope, Rambla José Ana Fernández Pérez, 7,
2 Tartu Observatory, 61602 Tõravere, Estonia
3 Institute of Physics, University of Tartu, Ravila 14c, 50411 Tartu, Estonia
4 SOFIA Science Center, NASA Ames Research Center, 94035 Moffett Field, USA
5 Deutsches SOFIA Institut (DSI), University of Stuttgart, 70569 Stuttgart, Germany
6 Institute of Astronomy, University of Latvia, Raina bulv. 19, Riga, LV 1586, Latvia
7 School of Maths & Physics, University of Tasmania, 7001 Hobart, Australia
8 Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen, Denmark
Received: 14 May 2015
Accepted: 18 December 2015
Aims. We determine the proper motion of protostellar jets around Class 0 and Class I sources in an active star forming region in Serpens.
Methods. Multi-epoch deep images in the 2.122 μm line of molecular hydrogen, v = 1−0 S(1), obtained with the near-infrared instrument NOTCam on a timescale of 10 years, are used to determine the proper motion of knots and jets. K-band spectroscopy of the brighter knots is used to supply radial velocities, estimate extinction, excitation temperature, and H2 column densities towards these knots.
Results. We measure the proper motion of 31 knots on different timescales (2, 4, 6, 8, and 10 years). The typical tangential velocity is around 50 km s-1 for the 10-year baseline, but for shorter timescales, a maximum tangential velocity up to 300 km s-1 is found for a few knots. Based on morphology, velocity information, and the locations of known protostars, we argue for the existence of at least three partly overlapping and deeply embedded flows, one Class 0 flow and two Class I flows. The multi-epoch proper motion results indicate time-variable velocities of the knots, for the first time directly measured for a Class 0 jet. We find in general higher velocities for the Class 0 jet than for the two Class I jets. While the bolometric luminosites of the three driving sources are about equal, the derived mass flow rate Ṁout is two orders of magnitude higher in the Class 0 flow than in the two Class I flows.
Key words: stars: formation / ISM: jets and outflows / Herbig-Haro objects / ISM: kinematics and dynamics
© ESO, 2016
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