<i>Spitzer</i>Observations of a 24 μm Shadow: Bok Globule CB 190

Stutz, Amelia M.; Bieging, John H.; Rieke, G. H.; Shirley, Yancy L.; Balog, Z.; Green, Elizabeth M.; Keene, J.; Kelly, Brandon C.; Rubin, M.; Werner, M. W.

doi:10.1086/519488

Cited by 18 publications

(40 citation statements)

References 42 publications

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“…This corresponds to A V = 26 mag, using the Ryter (1996) calibration. A more elaborate modelling of the fore-and background contributions (e.g., Stutz et al 2007) would probably increase the calculated column density, but is beyond the scope of this letter. In addition, the standard (coarse) pixel scale of 2.…”

Section: New Very Cold Source Detectionsmentioning

confidence: 99%

The structured environments of embedded star-forming cores

Linz¹,

Krause²,

Beuther³

et al. 2010

A&A

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The intermediate-mass star-forming core UYSO 1 has previously been found to exhibit intriguing features. While deeply embedded and previously only identified by means of its (sub-)millimeter emission, it drives two powerful, dynamically young, molecular outflows. Although the process of star formation has obviously started, the chemical composition is still pristine. We present Herschel PACS and SPIRE continuum data of this presumably very young region. The now complete coverage of the spectral energy peak allows us to precisely constrain the elevated temperature of 26-28 K for the main bulge of gas associated with UYSO1, which is located at the interface between the hot H ii region Sh 2-297 and the cold dark nebula LDN 1657A. Furthermore, the data identify cooler compact far-infrared sources of just a few solar masses, hidden in this neighbouring dark cloud.

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Section: New Very Cold Source Detectionsmentioning

confidence: 99%

The structured environments of embedded star-forming cores

Linz¹,

Krause²,

Beuther³

et al. 2010

A&A

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“…Data reduction was done with the Data Analysis Tool (DAT; Gordon et al 2005). The data were processed according to Stutz et al (2007). These images are presented here for the first time.…”

Section: Spitzermentioning

confidence: 99%

The Earliest Phases of Star formation (EPoS) observed withHerschel: the dust temperature and density distributions of B68

Nielbock

Launhardt

Steinacker

et al. 2012

A&A

129

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Context. Isolated starless cores within molecular clouds can be used as a testbed to investigate the conditions prior to the onset of fragmentation and gravitational proto-stellar collapse. Aims. We aim to determine the distribution of the dust temperature and the density of the starless core B68. Methods. In the framework of the Herschel guaranteed-time key programme "The Earliest Phases of Star formation" (EPoS), we have imaged B68 between 100 and 500 μm. Ancillary data at (sub)millimetre wavelengths, spectral line maps of the 12 CO (2-1), and 13 CO (2-1) transitions, as well as an NIR extinction map were added to the analysis. We employed a ray-tracing algorithm to derive the 2D mid-plane dust temperature and volume density distribution without suffering from the line-of-sight averaging effects of simple SED fitting procedures. Additional 3D radiative transfer calculations were employed to investigate the connection between the external irradiation and the peculiar crescent-shaped morphology found in the FIR maps. Results. For the first time, we spatially resolve the dust temperature and density distribution of B68, convolved to a beam size of 36. 4. We find a temperature gradient dropping from (16.7 ) × 10 5 cm −3 . B68 has a mass of 3.1 M of material with A K > 0.2 mag for an assumed distance of 150 pc. We detect a compact source in the southeastern trunk, which is also seen in extinction and CO. At 100 and 160 μm, we observe a crescent of enhanced emission to the south. Conclusions. The dust temperature profile of B68 agrees well with previous estimates. We find the radial density distribution from the edge of the inner plateau outward to be n H ∝ r −3.5 . Such a steep profile can arise from either or both of the following: external irradiation with a significant UV contribution or the fragmentation of filamentary structures. Our 3D radiative transfer model of an externally irradiated core by an anisotropic ISRF reproduces the crescent morphology seen at 100 and 160 μm. Our CO observations show that B68 is part of a chain of globules in both space and velocity, which may indicate that it was once part of a filament that dispersed. We also resolve a new compact source in the southeastern trunk and find that it is slightly shifted in centroid velocity from B68, lending qualitative support to core collision scenarios.

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“…Lawrence). The MIPS observations were reduced using the data analysis tool (DAT; Gordon et al 2005) according to steps outlined in Stutz et al (2007). The IRAC frames were processed using the IRAC Pipeline v14.0, and mosaics were created from the basic calibrated data (BCD) frames using a custom IDL program (see Gutermuth et al 2008).…”

Section: Near-ir Datamentioning

confidence: 99%

Dust-temperature of an isolated star-forming cloud:Herschelobservations of the Bok globule CB244

Stutz

Launhardt²,

Linz³

et al. 2010

A&A

109

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We present Herschel observations of the isolated, low-mass star-forming Bok globule CB244. It contains two cold sources, a low-mass Class 0 protostar and a starless core, which is likely to be prestellar in nature, separated by 90 (∼18 000 AU). The Herschel data sample the peak of the Planck spectrum for these sources, and are therefore ideal for dust-temperature and column density modeling. With these data and a near-IR extinction map, the MIPS 70 μm mosaic, the SCUBA 850 μm map, and the IRAM 1.3 mm map, we model the dust-temperature and column density of CB 244 and present the first measured dust-temperature map of an entire starforming molecular cloud. We find that the column-averaged dust-temperature near the protostar is ∼17.7 K, while for the starless core it is ∼10.6 K, and that the effect of external heating causes the cloud dust-temperature to rise to ∼17 K where the hydrogen column density drops below 10 21 cm −2 . The total hydrogen mass of CB 244 (assuming a distance of 200 pc) is 15 ± 5 M . The mass of the protostellar core is 1.6 ± 0.1 M and the mass of the starless core is 5 ± 2 M , indicating that ∼45% of the mass in the globule is participating in the star-formation process.

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SpitzerObservations of a 24 μm Shadow: Bok Globule CB 190

Cited by 18 publications

References 42 publications

The structured environments of embedded star-forming cores

The structured environments of embedded star-forming cores

The Earliest Phases of Star formation (EPoS) observed withHerschel: the dust temperature and density distributions of B68

Dust-temperature of an isolated star-forming cloud:Herschelobservations of the Bok globule CB244

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