ISO far infrared observations of the high latitude cloud L 1642

Lehtinen, K.; Russeil, D.; Juvela, M.; Mattila, K.; Lemke, D.

doi:10.1051/0004-6361:20047087

Cited by 23 publications

(54 citation statements)

References 24 publications

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“…The spatial resolutions of the IRIS maps at 12, 25, 60, and 100 μm are 3.8 , 3.8 , 4.0 , and 4.3 , respectively. We compared our results with the 200 μm observations at 90 resolution (Lehtinen et al 2004), obtained with the ISOPHOT instrument of the ISO satellite (Kessler et al 1996).…”

Section: Other Infrared Datamentioning

confidence: 96%

“…Lehtinen et al (2004) derived virial masses using these equations, and assuming that k = 1.25, a value between the density distributions ρ(r) = r −1 and ρ(r) = r −2 . To compare our results with this, we used the same value for k.…”

Section: Mass Calculationmentioning

confidence: 99%

“…Lehtinen et al (2004) named the dense regions A1, A2, B, and C. We adopt this naming convention and show the regions in Fig. 2 (top left panel).…”

Section: (Left)mentioning

confidence: 99%

“…See Welsh & Shelton (2009) for a description of the Local Bubble. We adopted the distance of 140 pc similarly to Russeil et al (2003) and Lehtinen et al (2004). A&A 563, A125 (2014) L1642 has been studied using several molecules, see Liljestrom (1991) for a review of the early studies.…”

Section: Introductionmentioning

confidence: 99%

“…L1642 has also been widely studied using other methods such as dust emission in mid-and far-infrared (Laureijs et al 1987;Reach et al 1998;Verter & Rickard 1998;Verter et al 2000;Lehtinen et al 2004Lehtinen et al , 2007 and optical (360-600 nm) surface brightness (Laureijs et al 1987;Mattila et al 2012). Mattila et al (2007) studied scattered Hα light in L1642.…”

Section: Introductionmentioning

confidence: 99%

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Multiwavelength study of the high-latitude cloud L1642: chain of star formation

Malinen

Juvela

Zahorecz

et al. 2014

A&A

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Context. L1642 is one of the two high galactic latitude (|b| > 30 • ) clouds confirmed to have active star formation. Aims. We examine the properties of this cloud, especially the large-scale structure, dust properties, and compact sources at different stages of star formation.Methods. We present high-resolution far-infrared and submillimetre observations with the Herschel and AKARI satellites and millimetre observations with the AzTEC/ASTE telescope, which we combined with archive data from near-and mid-infrared (2MASS, WISE) to millimetre wavelength observations (Planck).Results. The Herschel observations, combined with other data, show a sequence of objects from a cold clump to young stellar objects (YSOs) at different evolutionary stages. Source B-3 (2MASS J04351455-1414468) appears to be a YSO forming inside the L1642 cloud, instead of a foreground brown dwarf, as previously classified. Herschel data reveal striation in the diffuse dust emission around the cloud L1642. The western region shows striation towards the NE and has a steeper column density gradient on its southern side. The densest central region has a bow-shock like structure showing compression from the west and has a filamentary tail extending towards the east. The differences suggest that these may be spatially distinct structures, aligned only in projection. We derive values of the dust emission cross-section per H nucleon of σ e (250 μm) = 0.5−1.5 × 10 −25 cm 2 /H for different regions of the cloud. Modified black-body fits to the spectral energy distribution of Herschel and Planck data give emissivity spectral index β values 1.8-2.0 for the different regions. The compact sources have lower β values and show an anticorrelation between T and β. Conclusions. Markov chain Monte Carlo calculations demonstrate the strong anticorrelation between β and T errors and the importance of millimetre wavelength Planck data in constraining the estimates. L1642 reveals a more complex structure and sequence of star formation than previously known.

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Section: Other Infrared Datamentioning

confidence: 96%

Section: Mass Calculationmentioning

confidence: 99%

“…Lehtinen et al (2004) named the dense regions A1, A2, B, and C. We adopt this naming convention and show the regions in Fig. 2 (top left panel).…”

Section: (Left)mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Multiwavelength study of the high-latitude cloud L1642: chain of star formation

Malinen

Juvela

Zahorecz

et al. 2014

A&A

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A study of CO and FIR dust emission of lynds 694/695 dark clouds

Lee

2005

New Astronomy

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High-resolution mapping of interstellar clouds with near-infrared scattered light

Juvela¹,

Pelkonen²,

Padoan

et al. 2006

Proc. IAU

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Abstract. We examine the intensity of scattered near-infrared (NIR) light in the case of interstellar clouds illuminated by the normal interstellar radiation field. We have developed a way to convert the observed surface brightness into estimates of the column density and have estimated the accuracy of the new method. The NIR intensities can be converted into reliable estimates of the column density in regions with A V up to almost 20 magnitudes. The errors can be further reduced with detailed radiative transfer modelling and by using the lower resolution information that is provided by the colour excess data of background stars. Therefore, NIR scattered light is a promising new way to map quiescent interstellar clouds at a high, even sub-arcsecond resolution. Keywords. ISM: clouds, ISM: structure,infrared: ISM, scatteringCurrent wide-field near-infrared (NIR) instruments make it possible to map the scattered light over large cloud areas (e.g., Foster & Goodman 2006). Below A V ∼10 magnitudes the surface brightness should be directly proportional to the column density. At higher column densities the scattered intensity shows signs of saturation that starts at the shortest wavelengths. The resulting changes in the intensity ratios between the NIR bands can be used to estimate the level of saturation. We have developed a way to convert observed near-infrared surface brightness values into estimates of column density . The reliability of this new method has been examined using simulated observations . The studies are based on three-dimensional cloud models obtained from simulations of magnetohydrodynamic turbulence. Maps of near-infrared scattered light are obtained for the model clouds with radiative transfer calculations, and are converted back into column density using the proposed method. We find that NIR intensities can be converted into reliable estimates of the column density in regions with A V up to almost 20 magnitudes. The errors can be further reduced with detailed radiative transfer modelling and, in particular, by using the lower resolution information that is available through the colour excess data of background stars. The NIR scattered light provides a promising new method for the mapping of quiescent interstellar clouds. The main advantage is the high, even sub-arcsecond resolution that can be reached with current instruments. The comparison of surface brightness and extinction data can also serve as a sensitive indicator of changes in dust properties and radiation field within the clouds.

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ISO far infrared observations of the high latitude cloud L 1642

Cited by 23 publications

References 24 publications

Multiwavelength study of the high-latitude cloud L1642: chain of star formation

Multiwavelength study of the high-latitude cloud L1642: chain of star formation

A study of CO and FIR dust emission of lynds 694/695 dark clouds

High-resolution mapping of interstellar clouds with near-infrared scattered light

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