CARMA Large Area Star Formation Survey: Observational Analysis of Filaments in the Serpens South Molecular Cloud
arXiv:1407.0755 · doi:10.1088/2041-8205/790/2/L19
Abstract
We present the N2H+(J=1-0) map of the Serpens South molecular cloud obtained as part of the CARMA Large Area Star Formation Survey (CLASSy). The observations cover 250 square arcminutes and fully sample structures from 3000 AU to 3 pc with a velocity resolution of 0.16 km/s, and they can be used to constrain the origin and evolution of molecular cloud filaments. The spatial distribution of the N2H+ emission is characterized by long filaments that resemble those observed in the dust continuum emission by Herschel. However, the gas filaments are typically narrower such that, in some cases, two or three quasi-parallel N2H+ filaments comprise a single observed dust continuum filament. The difference between the dust and gas filament widths casts doubt on Herschel ability to resolve the Serpens South filaments. Some molecular filaments show velocity gradients along their major axis, and two are characterized by a steep velocity gradient in the direction perpendicular to the filament axis. The observed velocity gradient along one of these filaments was previously postulated as evidence for mass infall toward the central cluster, but these kind of gradients can be interpreted as projection of large-scale turbulence.
12 pages, 4 figures, published in ApJL (July 2014)
References in corpus (3)
Cited by in corpus (53)
- The link between turbulence, magnetic fields, filaments, and star formation in the Central Molecular Zone cloud G0.253+0.016
- ALMA-IMF I -- Investigating the origin of stellar masses: Introduction to the Large Program and first results
- Magnetized filamentary gas flows feeding the young embedded cluster in Serpens South
- A closer look at the "characteristic" width of molecular cloud filaments
- From diffuse gas to dense molecular cloud cores
- CARMA Large Area Star Formation Survey: Structure and Kinematics of Dense Gas in Serpens Main
- Investigating the structure and fragmentation of a highly filamentary IRDC
- Zooming in on Individual Star Formation: Low- and High-mass Stars
- Self-gravitating Filament Formation from Shocked Flows: Velocity Gradients across Filaments
- The Role of Turbulence and Magnetic Fields in Simulated Filamentary Structure
- Widespread Molecular Outflows in the Infrared Dark Cloud G28.37+0.07: Indications of Orthogonal Outflow-Filament Alignment
- CARMA Large Area Star Formation Survey: Project Overview with Analysis of Dense Gas Structure and Kinematics in Barnard 1
- The fragmentation and stability of hierarchical structure in Serpens South
- Formation of the Hub-Filament System G33.92+0.11: Local Interplay between Gravity, Velocity, and Magnetic Field
- Assessing molecular outflows and turbulence in the protostellar cluster Serpens South
- The width of Herschel filaments varies with distance
- Low mass young stars in the Milky Way unveiled by DBSCAN and Gaia EDR3. Mapping the star forming regions within 1.5 Kpc
- A cold accretion flow onto one component of a multiple protostellar system
- ALMA observations reveal no preferred outflow--filament and outflow--magnetic field orientations
- The Gould's Belt Very Large Array Survey II: The Serpens region
- The role of the magnetic field in the fragmentation process: the case of G14.225-0.506
- Flow of gas detected from beyond the filaments to protostellar scales in Barnard 5
- The JCMT BISTRO-2 Survey: Magnetic Fields of the Massive DR21 Filament
- Dissecting the super-critical filaments embedded in the 0.5 pc subsonic region of Barnard 5
- Rotating filament in Orion B: Do cores inherit their angular momentum from their parent filament?
- Fragmentation and kinematics in high-mass star formation: CORE-extension targeting two very young high-mass star-forming regions
- A Novel Survey for Young Substellar Objects with the W-band filter II. The Coolest and Lowest Mass Members of the Serpens-South Star-forming Region
- CARMA Large Area Star Formation Survey: Dense Gas in the Young L1451 Region of Perseus
- Gas kinematics and star formation in the filamentary molecular cloud G47.06+0.26
- Structural and Dynamical Analysis of 0.1pc Cores and Filaments in the 30~Doradus-10 Giant Molecular Cloud
- ALMA-IMF XIII: NH kinematic analysis on the intermediate protocluster G353.41
- Convergent Filaments Contracting Towards an Intermediate-mass Prestellar Core
- Emergence of high-mass stars in complex fiber networks (EMERGE). I. Early ALMA Survey: observations and massive data reduction
- Turbulence and Accretion: a High-resolution Study of the B5 Filaments
- On the evolution of the observed Mass-to-Length relationship for star-forming filaments
- Gas kinematics around filamentary structures in the Orion B cloud
- VLA ammonia observations of L1287: analysis of the "Guitar" core and two filaments
- The distance to the Serpens South Cluster from H2O masers
- Young Stellar Populations in MYStIX Star Forming Regions: Candidate Protostars
- ALMA-IMF XVIII: The assembly of a star cluster: Dense NH (1-0) kinematics in the massive G351.77 protocluster
- The Kinematic Structure of Magnetically Aligned HI Filaments
- On the 3D Curvature and Dynamics of the Musca filament
- Predictions for Observing Protostellar Outflows with ALMA
- Confirming the Explosive Dispersal Outflow in DR21 with ALMA
- Velocity-Coherent Substructure in TMC-1: Inflow and Fragmentation
- Modelling Star Cluster Formation: Gas Accretion
- Different molecular filament widths as tracers of accretion onto filaments
- Core formation via filament fragmentation and the impact of ambient pressure on it
- Emergence of high-mass stars in complex fiber networks (EMERGE) IV. Environmental dependence of the fiber widths
- Random gas motions inside sub-parsec scale supercritical filaments
- Scale-dependent surface and volume density properties of filaments in molecular clouds
- The factors that influence protostellar multiplicity II. Gas temperature and mass in Perseus with APEX
- Unveiling Fiber Networks and Core Formation in the DR21 South Filament