Protostellar candidates in a sample of bright far-infrared IRAS sources

McCutcheon, W. H.; Dewdney, P. E.; Purton, C. R.; Sato, T.

doi:10.1086/115776

Cited by 51 publications

(39 citation statements)

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“…The position of this knot is toward the centre of the cloud and west of the bright, diffuse arc-type emission. Indication of this radio knot can also be seen in the map presented by McCutcheon et al (1991) (see their Fig. 1).…”

Section: Emission From Ionized Gassupporting

confidence: 56%

“…We estimate log10(N lyc ) to be 46.79 which translates to a main-sequence spectral type between B0.5 -B0 (see Table 2 of Panagia (1973)). The spectral type determined from this work is within one subclass of the estimates obtained from previous radio continuum studies by Odenwald & Schwartz (1989) and McCutcheon et al (1991) after scaling to the distance and electron temperature used in our study. Verma et al (2003) carried out the radiative transfer modeling of two FIR cores located towards the cloud centre (see Section 3.5) using MIR and FIR data and estimated the spectral type of the sources associated with these cores to be between B0.5 -B0.…”

Section: Emission From Ionized Gassupporting

confidence: 55%

“…The retrieved map has a beam size of 4.07 × 4.01 , field of view of 4.56 and rms level ∼ 100 µJy/beam. Though the date of observation is not explicitly mentioned in their paper, this data is possibly the one which is presented in McCutcheon et al (1991). We have used this data alongwith the data obtained from GMRT maps to study the ionized emission associated with IRAS 20286+4105.…”

Section: Available Datasets From Various Archivesmentioning

confidence: 99%

“…Based on 2MASS data, a Present Affiliation and E-mail: Institute of Physics and Astronomy, University of Potsdam; varsha@astro.physik.uni-potsdam.de resolved cluster/stellar group is also reported to be associated with this region (Dutra & Bica 2001;Kumar, Keto & Clerkin 2006). This complex has been the target of a couple of radio continuum observations (Wendker 1984;Wendker, Higgs & Landecker 1991;McCutcheon et al 1991). In the FIR, this region has been studied in detail by Verma et al (2003) at 150 and 210 µm using the balloon-borne TIFR telescope.…”

Section: Introductionmentioning

confidence: 99%

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Radio and infrared study of the star-forming region IRAS 20286+4105

Ramachandran

Das

Tej

et al. 2016

Mon. Not. R. Astron. Soc.

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A multi-wavelength investigation of the star forming complex IRAS 20286+4105, located in the Cygnus-X region, is presented here. Near-infrared K-band data is used to revisit the cluster / stellar group identified in previous studies. The radio continuum observations, at 610 and 1280 MHz show the presence of a HII region possibly powered by a star of spectral type B0 -B0.5. The cometary morphology of the ionized region is explained by invoking the bow-shock model where the likely association with a nearby supernova remnant is also explored. A compact radio knot with non-thermal spectral index is detected towards the centre of the cloud. Mid-infrared data from the Spitzer Legacy Survey of the Cygnus-X region show the presence of six Class I YSOs inside the cloud. Thermal dust emission in this complex is modelled using Herschel far-infrared data to generate dust temperature and column density maps. Herschel images also show the presence of two clumps in this region, the masses of which are estimated to be ∼ 175 M and 30 M . The mass-radius relation and the surface density of the clumps do not qualify them as massive star forming sites. An overall picture of a runaway star ionizing the cloud and a triggered population of intermediate-mass, Class I sources located toward the cloud centre emerges from this multiwavelength study. Variation in the dust emissivity spectral index is shown to exist in this region and is seen to have an inverse relation with the dust temperature.

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Section: Emission From Ionized Gassupporting

confidence: 56%

Section: Emission From Ionized Gassupporting

confidence: 55%

Section: Available Datasets From Various Archivesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Radio and infrared study of the star-forming region IRAS 20286+4105

Ramachandran

Das

Tej

et al. 2016

Mon. Not. R. Astron. Soc.

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“…The maser position coincides with a bright red source detected with the Spitzer Space Telescope's IRAC camera at 4.5 µm. Although no radio continuum (at 6cm) was detected in IRAS 05168+3634 by McCutcheon et al (1991), Molinari et al (1998) detected a 6cm continuum emission peak of 4.23 mJy at a position ∼ 1.7 ′ toward the northeast of IRAS 05168+3634. In this region, there are several sources at different evolutionary and star-formation phases.…”

Section: Introductionmentioning

confidence: 94%

The outer rotation curve project with VERA: Trigonometric parallax of IRAS 05168+3634

et al. 2012

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Abstract. We present a measurement of the trigonometric parallax of IRAS 05168+3634 with VERA. The parallax is 0.532 ± 0.053 mas, corresponding to a distance of 1.88 +0.21 −0.17 kpc. This is significantly closer than the previous distance estimate of 6 kpc based on a kinematic distance measurement. This drastic change in the source distance implies the need for revised values of not only the physical parameters of IRAS 05168+3634, but it also implies a different location in the Galaxy, placing it in the Perseus arm rather than the Outer arm. We also measured the proper motion of the source. A combination of the distance and proper motion with the systemic velocity yields a rotation velocity Θ = 227 +9 −11 km s −1 at the source position, assuming Θ0 = 240 km s −1 . Our result, combined with previous VLBI results for six sources in the Perseus arm, indicates that the sources rotate systematically more slowly than the Galactic rotation velocity at the local standard of rest. In fact, we derive peculiar motions in the disk averaged over the seven sources in the Perseus arm of (Umean, Vmean) = (11 ± 3, −17 ± 3) km s −1 , which indicates that these seven sources are moving systematically toward the Galactic Center and lag behind the overall Galactic rotation.

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