Distribution of Serpens South protostars revealed with ALMA^★

¹ European Southern Observatory, Av. Alonso de Córdova 3107, Vitacura, Santiago, Chile
e-mail: aplunket@eso.org
² Instituto Argentino de Radioastronomía, CCT-La Plata (CONICET), C.C.5, 1894 Villa Elisa, Argentina
³ Department of Astronomy, Yale University, PO Box 208101, New Haven, CT 06520, USA
⁴ Institut de Ciències de l’Espai (IEEC-CSIC), Campus UAB, Carrer de Can Magrans, S/N, 08193 Cerdanyola del Vallès, Catalunya, Spain
⁵ Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile
⁶ Department of Physics, State University of New York at Fredonia, Fredonia, NY 14063, USA
⁷ Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS 78, Cambridge, MA 02138, USA

Received: 28 November 2017
Accepted: 27 March 2018

Abstract

Context. Clusters are common sites of star formation, whose members display varying degrees of mass segregation. The cause may be primordial or dynamical, or a combination both. If mass segregation were to be observed in a very young protostellar cluster, then the primordial case can be assumed more likely for that region.

Aims. We investigated the masses and spatial distributions of pre-stellar and protostellar candidates in the young, low-mass star forming region Serpens South, where active star formation is known to occur along a predominant filamentary structure. Previous observations used to study these distributions have been limited by two important observational factors: (1) sensitivity limits that leave the lowest-mass sources undetected or (2) resolution limits that cannot distinguish binaries and/or cluster members in close proximity.

Methods. Recent millimeter-wavelength interferometry observations can now uncover faint and/or compact sources in order to study a more complete population of protostars, especially in nearby (D < 500 pc) clusters. Here we present ALMA observations of 1 mm (Band 6) continuum in a 3 × 2 arcmin region at the center of Serpens South. Our angular resolution of ~1′′ is equivalent to ~400 au, corresponding to scales of envelopes and/or disks of protostellar sources.

Results. We detect 52 sources with 1 mm continuum, and we measure masses of 0.002–0.9 solar masses corresponding to gas and dust in the disk and/or envelope of the protostellar system. For the deeply embedded (youngest) sources with no IR counterparts, we find evidence of mass segregation and clustering according to: the minimum spanning tree method, distribution of projected separations between unique sources, and concentration of higher-mass sources near to the dense gas at the cluster center.

Conclusions. The mass segregation of the mm sources is likely primordial rather than dynamical given the young age of this cluster, compared with segregation time. This is the first case to show this for mm sources in a low-mass protostellar cluster environment.