Star formation in Perseus - Clusters, filaments and the conditions for star formation

By J. Hatchell, J. Richer, G. Fuller, C. Qualtrough, E. Ladd, C. Chandler. 2005

193 citations recorded by the source corpus.

We present a complete survey of current star formation in the Perseus molecular cloud, made at 850 and 450 µm with SCUBA at the JCMT. Covering 3 deg 2 , this submillimetre continuum survey for protostellar act ivity is second in size only to that ofOphiuchus (Johnstone et al. 2004). Complete above 0.4 M⊙ (5� detection in a 14 '' beam), we detect a total of 91 protostars and prestellar cores. Of these, 80% lie in cluste rs, representative of star formation across the Galaxy. Two of the groups of cores are associated with the young stellar clusters IC348 and NGC1333, and are consistent with a steady or reduced star formation rate in the last 0.5 Myr, but not an increasing one. In Perseus, 40-60% of cores are in small clusters (< 50 M⊙) and isolated objects, much more than the 10% suggested from infrared studies. Complementing the dust continuum, we present a C 18 O map of the whole cloud at 1 ' resolution. The gas and dust show filamentary structure of th e dense gas on large and small scales, with the high column density filaments breaking up in to clusters of cores. The filament mass per unit length is 5-11 M⊙ per 0.1 pc. Given these filament masses, there is no requireme nt for substantial large scale flows along or onto the filament s in order to gather suffi cient material for star formation. We find that the probabili ty of finding a submillimetre core is a strongly increasing function of column density, as measured by C 18 O integrated intensity, P(core)∝ I 3.0 . This power law relation holds down to low column density, suggesting that there is no Av threshold for star formation in Perseus, unless all the low- Av submm cores can be demonstrated to be older protostars which have begun to lose their natal molecular cloud.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/757f1940b00ed47c19fdca871567a9ef2fa4214e

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Spectroscopy

Citations in the corpus

Physical Processes in the Interstellar Medium (2014, background): “, 2010) or simply a steep dependence of the star formation rate on the column density (Hatchell et al., 2005; Enoch et al., 2008; Heiderman et al., 2010; Gutermuth et al., 2011; Burkert & Hartmann, 2013; Lada et al., 2013; Evans et al., 2014).”
Identifying the Low-Luminosity Population of Embedded Protostars in the c2d Observations of Clouds and Cores (2007, methodology): “The surveys used for Perseus are a 1.1 mm dust continuum survey of 7.5 deg2 with Bolocam at the CSO (Enoch et al. 2006), an 850 µm dust continuum survey of 3.5 deg2 with SCUBA at the JCMT (Kirk et al. 2006), a 450 and 850 µm dust continuum survey of 3.0 deg2 with SCUBA at the JCMT (Hatchell et al. 2”
Spitzer Observations of NGC 1333: A Study of Structure and Evolution in a Nearby Embedded Cluster (2007, background): “The bulk of these observations were originally published and analyzed in Sandell & Knee (2001) with expansion of the original field presented in Hatchell et al. (2005).”
The Global Evolution of Giant Molecular Clouds. I. Model Formulation and Quasi-Equilibrium Behavior (2006, unknown): “…rate were simply following the column density to some power, suggesting that magnetic fields may play a secondary role – Onishi et al. 1998, 1999, 2002; Johnstone et al. 2004 – though see Hatchell et al. 2005 who find that low column densities reduce but do not completely prevent star formation.)”
Cooling, Gravity, and Geometry: Flow-driven Massive Core Formation (2007, background): “Global Collapse and Filament Formation Galactic star formation seems to prefer filamentary – at least elongated – rather than spherical molecular clouds (Schneider & Elmegreen 1979; Chini et al. 1997; Hartmann et al. 2001; Hatchell et al. 2005; Alves et al. 2007).”
A census of dense cores in the Aquila cloud complex: SPIRE/PACS observations from the Herschel Gould Belt survey (2015, methodology): “…of prestellar cores detected below a given background column density by the total surface area imaged by Herschel below the same background column density level (for a related probability function in the case of the submm continuum cores detected by SCUBA in Perseus, see Hatchell et al. 2005).”
Theory of Star Formation (2007, result): “…extent that ambipolar diffusion is essential for forming molecular cores, the absence or near absence of sub-mm cores in the outer layers of Ophiuchus (Johnstone, Di Francesco, & Kirk, 2004) and Perseus (Enoch et al., 2006; Hatchell et al., 2005) is qualitatively consistent with this prediction.”
The Evolution of Outflow-Envelope Interactions in Low-Mass Protostars (2006, background): “Since we do not have separate bolometric temperature measurements for each element of other close ( 5′′) binary systems in our sample (i.e., IRAS3282, HH300, L 1228, RNO129), and since T Tau S and T Tau N should be coeval, we adopt a single Tbol for both stars using flux measurements at different w”
DIRECT OBSERVATION OF A SHARP TRANSITION TO COHERENCE IN DENSE CORES (2010, methodology): “When compared to dust emission maps from BOLOCAM (see contours in Figures 1 and 2) or SCUBA, we find that the NH3(1,1) emission is spatially more extended than its dust continuum counterpart.”
MAMBO Mapping Of Spitzer c2d Small Clouds And Cores (2008, background): “…studied dense cores in large (up to several 10 pc) and massive (up to several 103 M ) complexes of molecular clouds (Motte et al. 1998; Johnstone et al. 2000, 2001, 2004, 2006; Johnstone & Bally 2006; Hatchell et al. 2005; Enoch et al. 2006, 2007; Young K. E. et al. 2006; Stanke et al. 2006).”
A Spitzer Census of the IC 348 Nebula (2007, methodology): “Hatchell et al. (2005) performed a Submillimetre Common-User Bolometer Array (SCUBA, Holland et al. 1999) survey that identified 15 unique dust continuum peaks near the IC 348 nebula, lying mostly in a molecular ridge south of the cluster center.”
THE SPITZER c2d LEGACY RESULTS: STAR-FORMATION RATES AND EFFICIENCIES; EVOLUTION AND LIFETIMES (2008, unknown): “…data are taken from Alcalá et al. (2008), Brede et al. (2008), Davis et al. (1999), Djupvik et al. (2006), Enoch et al. (2006), Enoch et al. (2007), Hatchell et al. (2005), Hatchell et al. (2007), Henning et al. (1993), Johnstone et al. (2000), Kirk et al. (2006), Meŕın et al. (2008a), Stanke et…”
ATLASGAL - The APEX telescope large area survey of the galaxy at 870 μm (2009, methodology): “Using the Submillimetre Common User Bolometer Array (SCUBA) instrument, Johnstone et al. (2004) mapped 4 deg2 of the Ophiuchus star-forming cloud, and Hatchell et al. (2005) covered 3 deg2 of the Perseus molecular cloud.”
HARP/ACSIS: a submillimetre spectral imaging system on the James Clerk Maxwell Telescope (2009, background): “The optically thin C18O traces the velocity structure in and around the dense cores, identified in SCUBA maps (Hatchell et al. 2005, 2007) which can be used to explore the turbulent environment just outside of the cores.”
The Spitzer c2d Survey of Large, Nearby, Interstellar Clouds. III. Perseus Observed with IRAC (2006, background): “L1455-IRS3 is likewise classified as a Class I source but no continuum peak is seen toward this source in the SCUBA maps of Hatchell et al. (2005) (unfortunately it falls just outside the field observed by Enoch et al. (2006)).”
Comparing Star Formation on Large Scales in the c2d Legacy Clouds: Bolocam 1.1 mm Dust Continuum Surveys of Serpens, Perseus, and Ophiuchus (2007, methodology): “Recent advances in millimeter and submillimeter wavelength continuum detectors have enabled a number of large-scale surveys of nearby molecular clouds (e.g. Johnstone et al. 2004; Kirk et al. 2005; Hatchell et al. 2005; Enoch et al. 2006; Stanke et al. 2006; Young et al. 2006).”
The COMPLETE Survey of Star-Forming Regions: Phase I Data (2006, background): “A similar threshold has also been reported by Hatchell et al. (2005) and Enoch et al. (2006).”
Bolocam Survey for 1.1 mm Dust Continuum Emission in the c2d Legacy Clouds. I. Perseus (2005, methodology): “We have used a simple analysis, comparable to that of Hatchell et al. (2005), to study the extinction threshold.”
An Ammonia Spectral Atlas of Dense Cores in Perseus (2007, methodology): “Recently, submillimeter surveys of dense cores have been extended to cover large fractions of molecular clouds (Hatchell et al. 2005; Enoch et al. 2006), making complete surveys of dense cores possible.”