Far-infrared image restoration analysis of the protostellar cluster in S140

Lester, D. F.; Harvey, P. M.; Joy, M.; Ellis, H. B.

doi:10.1086/164580

Cited by 26 publications

(22 citation statements)

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“…The brightest source is called IRS 1, and the two other sources IRS 2 and IRS 3 are located ∼17 north and ∼9 east of IRS 1. The infrared spectra of these sources are rising steeply between 10 µm and 50 µm (Lester et al 1986), demonstrating that they are deeply embedded young stellar objects associated with circumstellar material. The luminosities of IRS 1, 2, and 3 were estimated at 5, 3, and 2 ×10 3 L respectively Send offprint requests to: T. Preibisch, e-mail: preib@mpifr-bonn.mpg.de Based on observations obtained at the German-Spanish Astronomical Centre, Calar Alto, operated by the Max-PlanckInstiute for Astronomy, Heidelberg, jointly with the Spanish National Commission for Astronomy.…”

Section: Introductionmentioning

confidence: 95%

“…The luminosities of IRS 1, 2, and 3 were estimated at 5, 3, and 2 ×10 3 L respectively Send offprint requests to: T. Preibisch, e-mail: preib@mpifr-bonn.mpg.de Based on observations obtained at the German-Spanish Astronomical Centre, Calar Alto, operated by the Max-PlanckInstiute for Astronomy, Heidelberg, jointly with the Spanish National Commission for Astronomy. (Lester et al 1986), suggesting stellar masses between ≈6 M and ≈10 M . S140 IRS is the source of a strong molecular outflow.…”

Section: Introductionmentioning

confidence: 99%

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The outflow activity of the protostars in S140 IRS

Preibisch

Smith

2002

A&A

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Abstract. The S140/L1204 cloud contains a deeply embedded region of star formation and a powerful molecular outflow. In this paper, we present images of the S140 region obtained in the light of the 2.12 µm molecular hydrogen emission line and adjacent continuum. Our images reveal several knots of H2 line emission originating from shocked material close to IRS 1 as well as further out. Strong H2 shock emission is found north-east of IRS1 (at position angle of ∼20 • -30 • ), as well as to the south-west of IRS1 (at position angles around ∼190 • -220 • ), clearly demonstrating the presence of outflow activity in the north-east/south-west direction. We also find patches of H2 emission several arcminutes away from IRS1 at a position angles of ∼150 • and 340 • , i.e. in directions consistent with the previously known north-west/south-east molecular outflow. Our results therefore provide evidence for the existence of two distinct bipolar outflow systems originating simultaneously from IRS 1. We also discuss general aspects of the star formation process in the S140 region. An inferred high ratio of stellar to gas mass suggests that the outflows have dispersed most of the cloud mass.

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Section: Introductionmentioning

confidence: 95%

Section: Introductionmentioning

confidence: 99%

The outflow activity of the protostars in S140 IRS

Preibisch

Smith

2002

A&A

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“…The emission at the IRS1-peak is 10 offset from the young stellar object IRS1 and coincident with the locations of the deeply embedded source Submm-2, which was first described by Minchin et al (1995) This drop in [C ii] intensity between the IF-peak and IRS1-peak roughly coincides with a local minimum of the dust temperature, where the heating from neither the internal IRS1 source nor the external star (Lester et al 1986) are efficient.…”

Section: [Cii] Cutmentioning

confidence: 59%

The origin of the [C II] emission in the S140 photon-dominated regions. New insights from HIFI

Dedes

Röllig²,

Mookerjea

et al. 2010

A&A

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Using Herschel's HIFI instrument, we observe [C ii] along a cut through S140, as well as high-J transitions of CO and HCO + at two positions on the cut, corresponding to the externally irradiated ionization front and the embedded massive star-forming core IRS1. The HIFI data were combined with available ground-based observations and modeled using the KOSMA-τ model for photon-dominated regions (PDRs). We derive the physical conditions in S140 and in particular the origin of [C ii] emission around IRS1. We identify three distinct regions of [C ii] emission from the cut, one close to the embedded source IRS1, one associated with the ionization front, and one further into the cloud. The line emission can be understood in terms of a clumpy model of PDRs. At the position of IRS1, we identify at least two distinct components contributing to the [C ii] emission, one of them a small, hot component, which can possibly be identified with the irradiated outflow walls. This is consistent with the [C ii] peak at IRS1 coinciding with shocked H 2 emission at the edges of the outflow cavity. We note that previously available observations of IRS1 can be reproduced well by a single-component KOSMA-τ model. Thus, it is HIFI's unprecedented spatial and spectral resolution, as well as its sensitivity that has allowed us to uncover an additional hot gas component in the S140 region.

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“…We made y-scans of G34.3+0.2 at both wavelengths for this reason. The analysis of slit scans is described by Lester, Harvey, & Joy (1986a) and Lester et al (1986c). Similar treatment of scan data for the eight-channel system was used by Campbell et al (1995) and .…”

Section: Scansmentioning

confidence: 99%

“…A color-temperature map was made from the 47 m map (for points above 10% of the peak value) and a 95 m map that was made with the same 4 00 grid and 10 00 cone average as the 47 m map and using 4 Â 4 bin averages. The Fourier beam-matching technique of Lester et al (1986c) was not applied, since the maps' similarity implies that the emission is well resolved at both wavelengths, except in the peaks where the averaging appears to have smoothed out the resolution at 47 m to be close to that at 95 m. The map shows nearly uniform temperatures of about 58 K, with a value of 59 K at the peak emission. For dust emissivity that varies as k À1:9 (consistent with the dust used in our radiative transfer models), the temperature would be 38 K. This temperature is close to the value of 44 K derived from submillimeter observations by Hunter (1997).…”

Section: Introductionmentioning

confidence: 99%

High‐Resolution Far‐Infrared Observations and Models of the Star Formation Core of G34.3+0.2C

Campbell

Harvey

Lester

et al. 2004

ApJ

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High spatial resolution far-infrared (FIR) maps made on the Kuiper Airborne Observatory are presented of the extremely bright source associated with the ''cometary'' ultracompact H ii region G34.3+0.2C. The maps show sharply peaked emission at G34.3+0.2C, surrounded by extended emission of uniform temperature. Maximum entropy method deconvolutions indicate FIR core source sizes of 12 00 and 20 00 at 47 and 95 m, respectively. Radiative transfer models of centrally heated dust cloud cores are presented that match estimates of the FIR core emission at G34.3+0.2C. The FIR data and models imply that this emission is due to a compact, centrally peaked, massive core separate from the hot molecular core 2 00 east of G34.3+0.2C. In comparison to the hot molecular core, the FIR core represents a separate, more evolved core that contains a group of high-mass stars and protostars.

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Far-infrared image restoration analysis of the protostellar cluster in S140

Cited by 26 publications

References 0 publications

The outflow activity of the protostars in S140 IRS

The outflow activity of the protostars in S140 IRS

The origin of the [C II] emission in the S140 photon-dominated regions. New insights from HIFI

High‐Resolution Far‐Infrared Observations and Models of the Star Formation Core of G34.3+0.2C

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