A Cluster of Class 0 Protostars in Serpens: An [ITAL]IRAS[/ITAL] HIRES Study

Hurt, Robert L.; Barsony, M.

doi:10.1086/309969

Cited by 79 publications

(106 citation statements)

References 10 publications

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“…In minimising the χ 2 SED , we also varied the source luminosity from 20 L to 60 L and found the best-fit for a source luminosity equal to 33 L . Note that the estimated value of the bolometric luminosity is much lower than the values derived in previous studies toward this source (Harvey et al 1984;Casali et al 1993;Hurt & Barsony 1996;Larsson et al 2000). This is due to the adopted smaller distance to the source.…”

Section: A52 Analysiscontrasting

confidence: 54%

Physical structure of the envelopes of intermediate-mass protostars

Ceccarelli¹,

Alonso-Albi

Fuente

et al. 2010

A&A

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Context. Intermediate mass protostars provide a bridge between low-and high-mass protostars. Furthermore, they are an important component of the UV interstellar radiation field. Despite their relevance, little is known about their formation process. Aims. We present a systematic study of the physical structure of five intermediate mass, candidate Class 0 protostars. Our two goals are to shed light on the first phase of intermediate mass star formation and to compare these protostars with low-and high-mass sources. Methods. We derived the dust and gas temperature and density profiles of the sample. We analysed all existing continuum data on each source and modelled the resulting SED with the 1D radiative transfer code DUSTY. The gas temperature was then predicted by means of a modified version of the code CHT96. Results. We found that the density profiles of five out of six studied intermediate mass envelopes are consistent with the predictions of the "inside-out" collapse theory. We compared several physical parameters, like the power law index of the density profile, the size, the mass, the average density, the density at 1000 AU and the density at 10 K of the envelopes of low-, intermediate, and high-mass protostars. When considering these various physical parameters, the transition between the three groups appears smooth, suggesting that the formation processes and triggers do not substantially differ.

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Section: A52 Analysiscontrasting

confidence: 54%

Physical structure of the envelopes of intermediate-mass protostars

Ceccarelli¹,

Alonso-Albi

Fuente

et al. 2010

A&A

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“…This shift should not come as a surprise, since bolometric luminosities reported in this work and in Enoch et al (2009) are up to a factor of ∼10 lower than previous estimations (Casali et al 1993;Hurt & Barsony 1996;Larsson et al 2000), this difference being attributed to the better spatial resolution of Spitzer.…”

Section: Outflow Momentum Flux and Mechanical Luminosity Versus Bolomsupporting

confidence: 42%

“…Estimations of the bolometric luminosity for the very young protostars in the Serpens core differ substantially in diverse studies (Casali et al 1993;Hurt & Barsony 1996;Larsson et al 2000). In particular, the large beams of the mid and far-IR facilities deployed (e.g.…”

Section: Bolometric Luminositymentioning

confidence: 99%

“…It has been suggested that the difference in the spatial distribution of YSOs at different evolutionary stages reflects different star-forming episodes in Serpens (Casali et al 1993;Hurt & Barsony 1996;Kaas et al 2004). …”

Section: Overallmentioning

confidence: 99%

“…Again, deeply embedded Class0/I sources are tagged along with the strongest outflow lobes. This area comprises SMM1/FIRS1 and SMM10, with the former the most prominent source in Serpens (Casali et al 1993;Hurt & Barsony 1996;Davis et al 1999), which displays a series of mass-ejection phenomena. It has been associated with a radio jet and OH maser emission (Rodriguez et al 1989;Curiel et al 1993), while strong outflows have been traced in a number of molecular lines.…”

Section: Area Bmentioning

confidence: 99%

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Wide field COJ= 3 → 2 mapping of the Serpens cloud core

Dionatos

Nisini

Codella

et al. 2010

A&A

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Context. Outflows provide indirect means to gain insight into diverse star formation-associated phenomena. At the level of individual protostellar cores, both outflows and the intrinsic core properties can be used to study the mass accretion/ejection process of heavily embedded protostellar sources. Aims. The main objective of the paper is to study the overall outflow distribution and its association with the young population of the Serpens Core cluster. In addition, the paper addresses the correlation of the outflow momentum flux with the bolometric luminosity of their driving sources using this homogeneous dataset for a single star-forming site.Methods. An area comprising 460 × 230 of the Serpens cloud core was mapped in 12 CO J = 3 →2 with the HARP-B heterodyne array at the James Clerk Maxwell Telescope; J = 3 →2 observations are more sensitive tracers of hot outflow gas than lower J CO transitions; combined with the high sensitivity of the HARP-B receptors outflows are sharply outlined, enabling their association with individual protostellar cores. Results. Most of ∼20 observed outflows are found to be associated with known protostellar sources in bipolar or unipolar configurations. All but two outflow/core pairs in our sample tend to have a projected orientation spanning roughly NW-SE. The overall momentum driven by outflows in Serpens lies between 3.2 and 5.1 × 10 −1 M km s −1 , the kinetic energy from 4.3 to 6.7 × 10 43 erg, and momentum flux is between 2.8 and 4.4 × 10 −4 M km s −1 yr −1 . Bolometric luminosities of protostellar cores based on Spitzer photometry are found up to an order of magnitude lower than previous estimations derived with IRAS/ISO data. Conclusions. We confirm the validity of the existing correlations between the momentum flux and bolometric luminosity of Class I sources for the homogenous sample of Serpens, though we suggest that they should be revised by a shift to lower luminosities. All protostars classified as Class 0 sources stand well above the known Class I correlations, indicating a decline in momentum flux between the two classes.

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Unraveling the Initial Conditions of Star Formation in Serpens North

Duarte-Cabral

Peretto

Fuller

et al. 2011

Star Clusters in the Era of Large Surveys

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The Serpens North Cluster is a nearby low mass star forming region which is part of the Gould Belt. It contains a range of young stars thought to correspond to two different bursts of star formation and so provides the opportunity to study different stages of cluster formation. Here we present recent results based on a detailed analysis of molecular line and dust continuum data of this region. By studying the dynamics, column density and dust temperature structure of Serpens we propose that a cloud-cloud collision has been responsible for the trigger of the most recent episode of star formation. This scenario has been explored using SPH simulations. These simulations are able to successfully explain the similarities and differences observed in the two sub-protoclusters composing Serpens North

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A Cluster of Class 0 Protostars in Serpens: An [ITAL]IRAS[/ITAL] HIRES Study

Cited by 79 publications

References 10 publications

Physical structure of the envelopes of intermediate-mass protostars

Physical structure of the envelopes of intermediate-mass protostars

Wide field COJ= 3 → 2 mapping of the Serpens cloud core

Unraveling the Initial Conditions of Star Formation in Serpens North

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