Far-infrared and CO observations of CEP F - Implications for star formation in Cepheus OB3

Sargent, A. I.; Duinen, R. J. van; Nordh, H. L.; Fridlund, C. V. M.; Aalders, J. W. G.; Beintema, D. A.

doi:10.1086/113414

Cited by 13 publications

(13 citation statements)

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“…The peak of CH 3 CCH emission coincide with the IR source IRS1 (Sargent et al 1984) and the continuum sources at 130 and 70 µm (Schreyer et al 1997). The CH 3 CCH source is slightly extended to the southwest from the peak, and approximately coincides with the CS, C 18 O, CO, and CH 3 OH sources (Schreyer et al 1997), but in our map there is no second peak approximately 30 southwest from IRS1, which is present in the C 18 O, CS, and CH 3 OH maps.…”

Section: Comments On Individual Sourcesmentioning

confidence: 64%

Parameters of warm molecular clouds from methyl acetylene observations

et al. 2002

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Abstract. The results of a survey of 63 galactic star-forming regions in the 6K − 5K and 5K − 4K methyl acetylene lines at 102 and 85 GHz, respectively, are presented. Fourty-three sources were detected at 102 GHz, and twentyfive at 85 GHz. Emission was detected towards molecular clouds with kinetic temperatures 20-60 K (so-called "warm clouds"). The CH3CCH abundances in these clouds appeared to be about several units × 10 −9 . Five mapped sources were analyzed using the maximum entropy method. The sizes of the mapped clouds fall within the range between 0.1 and 1.7 pc, virial masses -between 90 -6200 M , and densities -between 6 × 10 4 and 6 × 10 5 cm −3 . The CH3CCH sources spatially coincide with the CO and CS sources. Chemical evolution simulations showed that the typical methyl acetylene abundance in the observed clouds corresponds to an age of ≈ 6 × 10 4 years.

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Section: Comments On Individual Sourcesmentioning

confidence: 64%

Parameters of warm molecular clouds from methyl acetylene observations

et al. 2002

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“…Figure 18 shows the line profiles toward the peaks of the two lobes. The position angle of this well-defined outflow axis Notes.-Cep F( FIR) was discovered by Sargent et al (1983). Units of right ascension are hours, minutes, and seconds, and units of declination are degrees, arcminutes, and arcseconds.…”

Section: Submillimeter Datamentioning

confidence: 99%

“…Sargent et al (1983) discovered an extended far-infrared source, Cep F(FIR), with a luminosity of about 500 L . This source is not unambiguously identified with an IRAS source; instead, several IRAS sources seem to contribute to the Cep F(FIR) object (see Table 2).…”

Section: Star Formation In L1216mentioning

confidence: 99%

V733 Cep (Persson's Star): A New FU Orionis Object in Cepheus

et al. 2007

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Persson recently found that a faint star had appeared in a cloud in Cepheus. A CCD image shows a R $ 17:3 nebulous star, now known as V733 Cep, located in the L1216 = Cep F cloud at the apex of a cavity in the cloud. Infrared photometry indicates a modest infrared excess. Optical spectroscopy shows a well-defined Li i k6707 line, and blueshifted absorption troughs at the H and Na i D lines extending to at least 200 km s À1 , indicative of a massive fast wind. An infrared 1-4 m spectrum of V733 Cep shows the presence of strong water vapor features, and is almost identical to a similar IR spectrum of FU Ori that is reddened by A V ¼ 8 mag. Assuming an intrinsic energy distribution similar to that of FU Ori, V733 Cep has a luminosity of about 135 L at the assumed distance of 800 pc. The star was detected by the Midcourse Space Experiment satellite at 8.3 m, but not by IRAS. Nor is it detected at 850 m, indicating that while the star possesses circumstellar material it is not surrounded by a significant cool envelope. A 12 CO(3-2) map shows what appears to be a small molecular outflow along the same axis as the cavity seen in optical images. There is evidence for a limited amount of other low-and medium-mass star formation in the Cep F cloud. The totality of the evidence strongly indicates that V733 Cep is a new FU Ori-type object that must have erupted sometime between 1953 and 1984.

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“…Other young objects are found in the immediate vicinity of IRS 1 at near-infrared wavelengths (Schreyer et al 1997;Thompson et al 1998;Wang et al 2002) and at submillimeter wavelengths (Ward- Thompson et al 2000). Further to the north, Sargent et al (1984) found a bright far-infrared source, IRS 2. Williams & Garland (2002) mapped the region around IRS 2 at 870 m and found a loose cluster of cold dust cores, IRS 2a-g, which we have also plotted in Figure 9.…”

Section: A Wide-field Survey For Hh Objectsmentioning

confidence: 99%

Deep Imaging Surveys of Star-forming Clouds. I. New Herbig-Haro Flows in NGC 2264

Reipurth

Moriarty‐Schieven

et al. 2004

Astron J

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We have embarked on a major, imaging survey of nearby star-forming regions using wide-field imaging detectors to identify and characterize the full population of Herbig-Haro flows from newborn stars in each region. In this study we present our survey results for the NGC 2264 region in Monoceros, where we have found a number of new Herbig-Haro objects, HH 571-HH 585, including several giant, parsec-scale flows. We discuss the individual flows and attempt to locate their region of origin. In particular, we identify two quadrupolar HH flows emanating from two cloud cores and associated with major molecular outflows. We also draw attention to what appears to be a region of major blowout of gas from a cloud core rich in young stars.

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Far-infrared and CO observations of CEP F - Implications for star formation in Cepheus OB3

Cited by 13 publications

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Parameters of warm molecular clouds from methyl acetylene observations

Parameters of warm molecular clouds from methyl acetylene observations

V733 Cep (Persson's Star): A New FU Orionis Object in Cepheus

Deep Imaging Surveys of Star-forming Clouds. I. New Herbig-Haro Flows in NGC 2264

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