Connecting the Scales: Large Area High-resolution Ammonia Mapping of NGC 1333

Abstract

We use NH3 inversion transitions to trace the dense gas in the NGC 1333 region of the Perseus molecular cloud. NH3(1,1) and NH3(2,2) maps covering an area of 102 square arcminutes at an angular resolution of ~3.7" are produced by combining VLA interferometric observations with GBT single dish maps. The combined maps have a spectral resolution of 0.14 km/s and a sensitivity of 4 mJy/beam. We produce integrated intensity maps, peak intensity maps and dispersion maps of NH3(1,1) and NH3(2,2) and a line-of-sight velocity map of NH3(1,1). These are used to derive the optical depth for the NH3(1,1) main component, the excitation temperature of NH3(1,1), and the rotational temperature, kinetic temperature and column density of NH3 over the mapped area. We compare these observations with the CARMA J=1-0 observations of N2H+ and H13CO+ and conclude that they all trace the same material in these dense star forming regions. From the NH3(1,1) velocity map, we find that a velocity gradient ridge extends in an arc across the entire southern part of NGC 1333. We propose that a large scale turbulent cell is colliding with the cloud, which could result in the formation of a layer of compressed gas. This region along the velocity gradient ridge is dotted with Class 0/I YSOs, that could have formed from local overdensities in the compressed gas leading to gravitational instabilities. The NH3(1,1) velocity dispersion map also has relatively high values along this region, thereby substantiating the shock layer argument.

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Cited by in corpus (16)

• PRODIGE -- Envelope to disk with NOEMA I. A 3000 au streamer feeding a Class I protostar
• Velocity-coherent Filaments in NGC 1333: Evidence for Accretion Flow?
• Self-gravitating Filament Formation from Shocked Flows: Velocity Gradients across Filaments
• Probing the physics of star formation (ProPStar): I. First resolved maps of the electron fraction and cosmic-ray ionization rate in NGC 1333
• A train of shocks at 3000 au scale? Exploring the clash of an expanding bubble into the NGC 1333 IRAS 4 region. SOLIS XIV
• Probing the Physics of Star-Formation (ProPStar): II. The first systematic search for streamers toward protostars
• The Infall Motion in the Low-Mass Protostellar Binary NGC 1333 IRAS 4A1/4A2
• Linking the dust and chemical evolution: Taurus and Perseus -- New collisional rates for HCN, HNC, and their C, N, and H isotopologues
• Tracking the ice mantle history in the Solar-type Protostars of NGC 1333 IRAS 4
• Hyperfine Group Ratio: A Recipe for Deriving Kinetic Temperature from Ammonia Inversion Lines
• Probing the Physics of Star-Formation (ProPStar) III. No evidence for dissipation of turbulence down to 20 mpc (4 000 au) scale
• Emergence of high-mass stars in complex fiber networks (EMERGE) III. Fiber networks in Orion
• Emergence of high-mass stars in complex fiber networks (EMERGE) IV. Environmental dependence of the fiber widths
• First Detections of PN, PO, and PO+ toward a Shocked Low-mass Starless Core
• KAgoshima Galactic Object survey with Nobeyama 45-metre telescope by Mapping in Ammonia lines (KAGONMA): Discovery of parsec-scale CO depletion in the Canis Major star-forming region
• The factors that influence protostellar multiplicity II. Gas temperature and mass in Perseus with APEX