The young stellar population in the Serpens Cloud Core: An ISOCAM survey

Kaas, A. A.; Olofsson, G.; Bontemps, Sylvain; André, Ph.; Nordh, L.; Huldtgren, M.; Prusti, T.; Persi, P.; Delgado, A.; Motte, F.; Abergel, A.; Boulanger, F.; Burgdorf, M.; Casali, M.; Césarsky, C. J.; Davies, J. I.; Falgarone, É.; Montmerle, T.; Pérault, M.; Puget, J.-L.; Sibille, F.

doi:10.1051/0004-6361:20035775

Cited by 82 publications

(239 citation statements)

References 86 publications

(184 reference statements)

Supporting

Mentioning

221

Contrasting

Order By: Relevance

“…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%

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

Dionatos

Nisini

Codella

et al. 2010

A&A

View full text Add to dashboard Cite

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.

show abstract

Section: Overallmentioning

confidence: 99%

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

Dionatos

Nisini

Codella

et al. 2010

A&A

View full text Add to dashboard Cite

show abstract

“…There seem to be no apparent spatial preferences among the optically selected PMS stars. We calculate the distribution of separations of pairs of members within the different sub-groups, a way to quantitatively assess possible clustering properties (Kaas et al 2004), although projected in the plane of the sky. In Fig.…”

Section: Spatial Distributionsmentioning

confidence: 99%

Analysis of the stellar population in the central area of the HII region Sh 2-284 ,

Delgado

Djupvik

Alfaro

2009

A&A

Self Cite

View full text Add to dashboard Cite

Context. There is a lack of state-of-the-art information on very young open clusters with implications for determining the structure of the Galaxy. Aims. Our main objective is to study the timing and location of the star formation processes which yielded the generation of the giant HII region Sh 2-284. This includes the determination of different physical variables of the stars, such as distance, reddening, age and evolutionary stage, including pre-main-sequence (PMS) stars. Methods. The analysis is based on UBVR C I C CCD measurements of a field of 6.5 × 6.5 containing the cluster, and JHK s photometry in the 3.5 × 3.5 subfield, centered in the apparent higher condensation. The determination of cluster distance, reddening and age is carried out through a comparison with ZAMS, post-MS and PMS isochrones. The reference lines used are obtained from theoretical post-MS and PMS isochrones from the Geneva and Yale groups for a metallicity of Z = 0.004, which agrees with the spectroscopic metallicity determination published for several cluster members. Results. The results amount to E(B − V) = 0.78 ± 0.02, DM = 12.8 ± 0.2 (3.6 kpc), Log Age(yr) = 6.51 ± 0.07 (3.2 Myr). The distance result critically depends on the use of low metallicity ZAMS and isochrones. A PMS member sequence is proposed, with an age of Log Age(yr) = 6.7 ± 0.2 (4.7 Myr) which is therefore coeval within the errors with the post-MS cluster age. The mass function for this population in the mass range above 1.3−3.5 M is well fitted by a Salpeter mass function. The presence of a different star generation in the cluster with a distinctly older age of around 40 Myr is suggested. On the other hand, the NIR photometry results indicate a large number of sources with (H − K s ) excess, practically distinct from the optical PMS candidate members. Conclusions. The analysis of our deep UBVRIJHK photometry of Dolidze 25 therefore reveals a young cluster with coeval MS and PMS populations of age 3.2−5 Myr. In addition, a distinctly older cluster member population of the age of 40 Myr is suggested. The distance determined for the cluster from quantitative fits to ZAMS and isochrones is distinctly lower than previously published values. This result originates in the consistent use of low metallicity models for ZAMS fitting, applying published metallicity values for the cluster.

show abstract

“…Thanks to their high sensitivity and good spatial resolution in the midinfrared, ISO and, more recently, Spitzer could perform more complete surveys in all major nearby star-forming regions (e.g. Nordh et al 1996;Bontemps et al 2001;Kaas et al 2004;Allen et al 2007;Evans et al 2009). The population of the youngest protostars, the Class 0 YSOs, can however not be properly surveyed solely in the near and mid-infrared.…”

Section: Introductionmentioning

confidence: 99%

TheHerschelfirst look at protostars in the Aquila rift

Bontemps

André

Könyves

et al. 2010

A&A

Self Cite

123

107

View full text Add to dashboard Cite

As part of the science demonstration phase of the Herschel mission of the Gould Belt key program, the Aquila rift molecular complex has been observed. The complete ∼3.3 • × 3.3 • imaging with SPIRE 250/350/500 μm and PACS 70/160 μm allows a deep investigation of embedded protostellar phases, probing of the dust emission from warm inner regions at 70 and 160 μm to the bulk of the cold envelopes between 250 and 500 μm. We used a systematic detection technique operating simultaneously on all Herschel bands to build a sample of protostars. Spectral energy distributions are derived to measure luminosities and envelope masses, and to place the protostars in an M env −L bol evolutionary diagram. The spatial distribution of protostars indicates three star-forming sites in Aquila, with W40/Sh2-64 HII region by far the richest. Most of the detected protostars are newly discovered. For a reduced area around the Serpens South cluster, we could compare the Herschel census of protostars with Spitzer results. The Herschel protostars are younger than in Spitzer with 7 Class 0 YSOs newly revealed by Herschel. For the entire Aquila field, we find a total of ∼45-60 Class 0 YSOs discovered by Herschel. This confirms the global statistics of several hundred Class 0 YSOs that should be found in the whole Gould Belt Survey.

show abstract

The young stellar population in the Serpens Cloud Core: An ISOCAM survey

Cited by 82 publications

References 86 publications

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

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

Analysis of the stellar population in the central area of the HII region Sh 2-284 ,

TheHerschelfirst look at protostars in the Aquila rift

Contact Info

Product

Resources

About