The COMPLETE Survey of Star-Forming Regions: Phase I Data

Ridge, Naomi A.; Francesco, James Di; Kirk, Helen; Li, Di; Goodman, Alyssa A.; Alves, J.; Arce, Héctor G.; Borkin, Michelle A.; Caselli, P.; Foster, Jonathan B.; Heyer, M. H.; Johnstone, Doug; Kosslyn, David A.; Lombardi, Marco; Pineda, Jaime E.; Schnee, Scott; Tafalla, M.

doi:10.1086/503704

Cited by 273 publications

(369 citation statements)

References 26 publications

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“…The selection criteria for all the clusters analyzed within the GES are summarized in Bragaglia et al (in prep.). In L1688, the targets have been selected among the stars with the following selection criteria: i) they have an estimated I-band magnitude I 17.5 mag for GIRAFFE targets and I 14.0 mag for UVES targets and ii) they are located within the L1688 starforming cloud in Ophiuchus (i.e., 16 h 30 m < RA < 16 h 24 m , −25 • 12 < Dec < −23 • 48 , Ridge et al 2006).…”

Section: Target Selection and Observationsmentioning

confidence: 99%

TheGaia-ESO Survey: Dynamical analysis of the L1688 region in Ophiuchus

Rigliaco

Wilking

Meyer

et al. 2016

A&A

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The Gaia ESO Public Spectroscopic Survey (GES) is providing the astronomical community with high-precision measurements of many stellar parameters including radial velocities (RVs) of stars belonging to several young clusters and star-forming regions. One of the main goals of the young cluster observations is to study their dynamical evolution and provide insight into their future, revealing whether they will eventually disperse to populate the field rather than evolve into bound open clusters. In this paper we report the analysis of the dynamical state of L1688 in the ρ Ophiuchi molecular cloud using the dataset provided by the GES consortium. We performed the membership selection of the more than 300 objects observed. Using the presence of the lithium absorption and the location in the Hertzspung-Russell diagram, we identify 45 already known members and two new association members. We provide accurate RVs for all 47 confirmed members. A dynamical analysis, after accounting for unresolved binaries and errors, shows that the stellar surface population of L1688 has a velocity dispersion σ ∼ 1.14 ± 0.35 km s −1 that is consistent with being in virial equilibrium and is bound with a ∼80% probability. We also find a velocity gradient in the stellar surface population of ∼1.0 km s −1 pc −1 in the northwest-southeast direction, which is consistent with that found for the pre-stellar dense cores, and we discuss the possibility of sequential and triggered star formation in L1688.

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Section: Target Selection and Observationsmentioning

confidence: 99%

TheGaia-ESO Survey: Dynamical analysis of the L1688 region in Ophiuchus

Rigliaco

Wilking

Meyer

et al. 2016

A&A

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“…We used the J = 1-0 spectral lines of 12 CO and 13 CO observed at FCRAO as part of the COMPLETE project (Ridge et al 2006), as well as FCRAO C 18 O J = 1-0 spectral line data toward the central core region of NGC 1333. In Fig.…”

Section: Disfavored On Energetic Grounds (Mac Low and Klessen 2004)mentioning

confidence: 99%

Turbulent driving scales in molecular clouds

Brunt¹,

Heyer²,

Low³

2009

A&A

159

151

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Context. Supersonic turbulence in molecular clouds is a dominant agent that strongly affects the clouds' evolution and star formation activity. Turbulence may be initiated and maintained by a number of processes, acting at a wide range of physical scales. By examining the dynamical state of molecular clouds, it is possible to assess the primary candidates for how the turbulent energy is injected. Aims. The aim of this paper is to constrain the scales at which turbulence is driven in the molecular interstellar medium, by comparing simulated molecular spectral line observations of numerical magnetohydrodynamic models and molecular spectral line observations of real molecular clouds. Methods. We use principal component analysis, applied to both models and observational data, to extract a quantitative measure of the driving scale of turbulence. Results. We find that only models driven at large scales (comparable to, or exceeding, the size of the cloud) are consistent with observations. This result applies also to clouds with little or no internal star formation activity. Conclusions. Astrophysical processes acting on large scales, including supernova-driven turbulence, magneto-rotational instability, or spiral shock forcing, are viable candidates for the generation and maintenance of molecular cloud turbulence. Small-scale driving by sources internal to molecular clouds, such as outflows, can be important on small scales, but cannot replicate the observed large-scale velocity fluctuations in the molecular interstellar medium.

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“…For sources in common, most positions agree within 3 . Figure 1 shows the distribution of the sample as plotted on the SCUBA 850 μm map of L 1688 (Johnstone et al 2000;Ridge et al 2006;Di Francesco et al 2008).…”

Section: Sample Selectionmentioning

confidence: 99%

The nature of the Class I population in Ophiuchus as revealed through gas and dust mapping

Kempen

Dishoeck

Salter

et al. 2009

A&A

112

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Context. The Ophiuchus clouds, in particular L 1688, are an excellent region to study the embedded phases of star formation, due to the relatively large number of protostars. However, the standard method of finding and characterizing embedded young stellar objects (YSOs) through just their infrared spectral slope does not yield a reliable sample. This may affect the age determinations, often derived from the statistics on the total number of embedded YSOs and pre-main sequence stars within a cloud. Aims. Our aim is to characterize the structure of protostellar envelopes on an individual basis and to correctly identify the embedded YSO population of L 1688. Methods. Spectral maps of the HCO + J = 4−3 and C 18 O J = 3−2 lines, using the HARP-B array on the James Clerk Maxwell Telescope and SCUBA 850 μm dust maps, are obtained of all sources in the L 1688 region with infrared spectral slopes consistent with, or close to, that of embedded YSOs. Selected 350 μm maps obtained with the Caltech Submillimeter Observatory are presented as well. The properties, extent and variation of dense gas, column density and dust up to 1 (∼7500 AU) are probed at 15 resolution. Using the spatial variation of the gas and dust, together with the intensity of the HCO + J = 4−3 line, we are able to accurately identify the truly embedded YSOs and determine their properties. Results. The protostellar envelopes range from 0.05 to 0.5 M in mass. The concentration of HCO + emission (∼0.5 to 0.9) is generally higher than that of the dust concentration. Combined with absolute intensities, HCO + proves to be a better tracer of protostellar envelopes than dust, which can contain disk and cloud contributions. Our total sample of 45 sources, including all previously classified Class I sources, several flat-spectrum sources and some known disks, was re-classified using the molecular emission. Of these, only 17 sources are definitely embedded YSOs. Four of these embedded YSOs have little (0.1−0.2 M ) envelope material remaining and are likely at the interesting transitional stage from embedded YSO to T Tauri star. About half of the flat-spectrum sources are found to be embedded YSOs and about half are disks. Conclusions. The presented classification method is successful in separating embedded YSOs from edge-on disks and confused sources. The total embedded population of the Ophiuchus L 1688 cloud is found almost exclusively in Oph-A, Oph-B2 and the Ophiuchus ridge with only three embedded YSOs not related to these regions. The detailed characterization presented will be necessary to interpret deep interferometric ALMA and future Herschel observations.

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The COMPLETE Survey of Star-Forming Regions: Phase I Data

Cited by 273 publications

References 26 publications

TheGaia-ESO Survey: Dynamical analysis of the L1688 region in Ophiuchus

TheGaia-ESO Survey: Dynamical analysis of the L1688 region in Ophiuchus

Turbulent driving scales in molecular clouds

The nature of the Class I population in Ophiuchus as revealed through gas and dust mapping

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