The Chamaeleon dark cloud complex. II - A deep survey around HD 97300

Jones, T. J.; Hyland, A. R.; Harvey, P. M.; Wilking, B. A.; Joy, M.

doi:10.1086/113826

Cited by 25 publications

(23 citation statements)

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“…A single field was observed in the Cha I cloud, with the 6 pfov, centred on 11 h 09 m 39. s 4, −76 • 35 2 . The corresponds (approximately) to a previously observed dense core lying to the north of HD97300 (Jones et al 1985;Persi et al 1999). …”

Section: Chamaeleon Isupporting

confidence: 81%

ISOCAM-CVF spectroscopy of the circumstellar environment of young stellar objects

Alexander

Casali

André

et al. 2003

A&A

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Abstract. We present the results of a mid-infrared (5-16.5 µm) imaging spectroscopy survey of Young Stellar Objects (YSOs) and their surrounding environment in four low-mass star formation regions: RCrA, ρ Ophiuchi, Serpens and Chamaeleon I. This survey was performed using ISOCAM and its Circular Variable Filters (CVF) and observed 42 YSO candidates: we were able to obtain complete 5-16.5 µm spectra for 40 of these with a spectral resolving power of λ/∆λ 40. A number of spectral features were measured, most notably the 9.7 µm silicate feature, the bending modes of both water and CO 2 ices at 6.0 and 15.2 µm respectively and the well-known unidentified feature at 6.8 µm. The strength of the unidentified feature was observed to correlate very well with that of the water ice bending mode and far less strongly with the CO 2 ice bending mode. This suggests, in a manner consistent with previous observations, that the carrier of the unidentified feature is a strongly polar ice. Absorption profiles of the bending mode of CO 2 ice are observed to show a significant long wavelength wing, which suggests that a significant fraction of the CO 2 ice observed exists in a polar (H 2 O-rich) phase. The sources observed in RCrA, ρ Oph and Serpens show similar spectral characteristics, whilst the sources observed in Cha I are somewhat anomalous, predominantly showing silicate emission and little or no absorption due to volatile ices. However this is consistent with previous studies of this region of the Cha I cloud, which contains an unusual cluster of YSOs. From comparisons of the strengths of the water ice and silicate bands we detect an apparent under-abundance of water ice towards the sources in ρ Oph, relative to both RCrA and Serpens. This may be indicative of differences in chemical composition between the different clouds, or may be due to evaporation. Finally the CO 2 :H 2 O ice ratios observed towards the sources in ρ Oph show significantly greater scatter than in the other regions, possibly due to varying local conditions around the YSOs in ρ Oph.

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Section: Chamaeleon Isupporting

confidence: 81%

ISOCAM-CVF spectroscopy of the circumstellar environment of young stellar objects

Alexander

Casali

André

et al. 2003

A&A

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“…1. In terms of the large-scale structure, our opacity maps are remarkably similar to the τ 130 map of Jones et al (1985). The opacity is lower around HD 97300 and towards the south (τ 100 ≈ 0.8 × 10 −3 ), and higher farther from the star and to the north (up to τ 100 ≈ 1.8 × 10 −3 in the studied 2 × 2 area).…”

Section: Density Structuresupporting

confidence: 69%

“…Excess emission with respect to a B9-type stellar photosphere was detected at infrared wavelengths towards HD 97300, and was first attributed to an M-type companion or a circumstellar dust shell (Hyland et al 1982;Wesselius et al 1984;Thé et al 1986). On the basis of maps of both optical extinction and 130 μm optical depth, Jones et al (1985) found This work is based on observations made with the Herschel Space Observatory and with the Spitzer Space Telescope. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.…”

Section: Introductionmentioning

confidence: 99%

The dusty environment of HD 97300 as seen byHerschelandSpitzer

Kóspál

Prusti

Cox

et al. 2012

A&A

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Aims. We analyze the surroundings of HD 97300, one of two intermediate-mass stars in the Chamaeleon I star-forming region. The star is known to be surrounded by a conspicuous ring of polycyclic aromatic hydrocarbons (PAHs). Methods. We present infrared images taken with Herschel and Spitzer using 11 different broad-band filters between 3.6 μm and 500 μm. We compare the morphology of the emission using cuts along different position angles. We construct spectral energy distributions, which we compare to different dust models, and calculate dust temperatures. We also derive opacity maps and analyze the density structure of the environment of HD 97300. Results. We find that HD 97300 has no infrared excess at or below 24 μm, confirming its zero-age main-sequence nature. The morphology of the ring is very similar between 3.6 μm and 24 μm. The emission at these wavelengths is dominated by either PAH features or PAH continuum. At longer wavelengths, only the northwestern part of the ring is visible. A fit to the 100-500 μm observations suggests that the emission is due to relatively warm (≈26 K) dust. The temperature gradually decreases with increasing distance from the ring. We find a general decrease in the density from north to south, and an approximate 10% density increase in the northeastern part of the ring. Conclusions. Our results are consistent with the theory that the ring around HD 97300 is essentially a bubble blown into the surrounding interstellar matter and heated by the star.

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“…The first region, located in the northern part, corresponds to the densest zone of the cloud (A V ∼ 17, Jones et al 1985). It harbors a group of about eight previously known pre-main sequence stars in addition to about six non-classified Note: Units of right ascension are hours, minutes, and seconds, and units of declination are degrees, arcminutes, and arcseconds.…”

Section: Introductionmentioning

confidence: 99%

A search for shock-excited molecular hydrogen knots in Chamaeleon I very low mass YSOs

Gómez¹,

Persi

Marenzi

et al. 2004

A&A

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Abstract.We have obtained narrow-band images of three selected areas of the Chamaeleon I dark cloud which harbor very low mass young stars, centered on the H 2 and Brγ lines and neighboring continuum as well as on the broad band K s . One region is located in the northern part of the cloud, roughly coinciding with the densest area. The other two regions are in the southern section of the cloud. Our aim is to search for H 2 outflows associated with these objects. In the northern region, we found seven new H 2 knots, five of which are aligned in the direction of a previously known 12 CO molecular bipolar outflow. Further evidence that the class I low mass stellar object ISO-ChaI 192 is the driving source of the molecular flow is given by the presence of a 960 AU long elongated structure at 2.2 µm emanating from this star and oriented parallel to the bipolar structure. Another pair of H 2 knots, although lying relatively nearby, is not aligned with the outflow direction. They are located on opposite sides of C1-6, a low mass class II object in the northern part of the Chamaeleon I dark cloud. In contrast, we fail to detect any H 2 emission object brighter than our sensitivity limit (∼6 × 10 −32 W/m 2 Hz arcsec 2 ) in the two southern areas of the cloud that also harbor several very low mass stars, including two transition stellar/sub-stellar objects. This negative result is probably not surprising in view of the extremely low accretion rates measured for brown dwarfs (Ṁ ∼ 10 −12 −10 −9 M yr −1 ). Deeper H 2 observations are required to better constraint the outflow event in sub-stellar objects.

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The Chamaeleon dark cloud complex. II - A deep survey around HD 97300

Cited by 25 publications

References 0 publications

ISOCAM-CVF spectroscopy of the circumstellar environment of young stellar objects

ISOCAM-CVF spectroscopy of the circumstellar environment of young stellar objects

The dusty environment of HD 97300 as seen byHerschelandSpitzer

A search for shock-excited molecular hydrogen knots in Chamaeleon I very low mass YSOs

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