Trapezium systems containing T tauri stars

Gyulbudaghian, A. L.

doi:10.1007/bf02113954

Cited by 5 publications

(5 citation statements)

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“…The trapezium contains at least five nebulous stars, reminiscent of other similar very young stellar ensembles studied by our group (e.g. Chavarría-K et al 1987Chavarría-K et al , 1989Chavarría-K et al , 2005Moreno-Corral et al 1993, 2002, 2006; see also Gyulbudaghian 1995), its stellar constituents could be medium and low-mass young stars. In support of this and considering that such clusters are loosely bound and hence subject to disruption by gravitational pull, the tightness of IRAS06548-0815 stellar aggregate (angular and linear diámeter φ 1 ′ , d 0.3 pc, respectively, assuming a distance to LDN1655 D = 1.0 kpc, see §4) signalizes us that gravity has not had the time to disperse it.…”

Section: Introductionsupporting

confidence: 67%

PMS and ZAMS stars associated with the dark cloud LDN 1655

et al. 2013

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We give results of a low-resolution optical spectroscopic study of the bright nebulous stars conforming the tight stellar trapezium embedded in IRAS06548-0815, of the exciting star of IRAS06547-0810, and of the stars associated with reflection nebulae (R-or N-stars) NJ065703.0-081421, NJ065714.1-081016, IRAS06548-0815 D and IRAS06548-0815 G, all objects scarcely observed and apparently pertaining to the dark cloud LDN 1655. Our results given here combined with the corresponding 2MASS near infrared photometry enables us to estimate a photometric distance to LDN1655 of 1.9 kpc and to locate the trapezium stars on the (log Lstar/Lsun, logTeff) or HR diagram in an attempt to disclose about their true nature. The spectroscopy of IRAS06548-0815 revealed two classic T Tauri, two Herbig Ae/Be stars, four weak-line T Tauri stars, and two probable lithium-rich stars. Additionally, we found that the R-star IRAS06547-0810 is excited by a single B1(V) star, that IRAS06548-0815 D is excited by a SpT. B2/B3(V) star, NJ065703.0-081421 and NJ065714.1-081016 are excited by a B3/B4(V) emission star and an A6(V) star, respectively. The brightest near infrared source of the trapezium, IRS1, has an infrared luminosity comparable to a highly reddened O8(V) star (Av of 29m). The second brightest near infrared source of the trapezium, IRAS06548-0815 C is, optically, a single classical T Tauri star of spectral type K4/K5, but is a resolved binary in the 2MASSKs band, both components being of about the same brightness.Comment: Submitted to New Astronomy, 18, 42 (2013): 23 pages, 6 Figure

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Section: Introductionsupporting

confidence: 67%

PMS and ZAMS stars associated with the dark cloud LDN 1655

et al. 2013

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“…The optical nebula list was compiled from: Ber (Bernes 1977), BFS (Blitz et al 1982), BRC (Sugitani et al 1991), Ced (Cederblad 1946), DG (von Dorschner & Gurtler 1963), GGD (Gyulbudaghian et al 1978), GM1- (Gyulbudaghian & Maghakian 1977a), GM2- (Gyulbudaghian & Maghakian 1977b), GM3- (Gyulbudaghian & Maghakian 1977c), Gy1- (Gyulbudaghian 1982a), Gy2- (Gyulbudaghian 1984a), Gy3- (Gyulbudaghian 1984b), Gy82- (Gyulbudaghian 1982b), NS (Neckel & Staude 1984), Parsamian (Parsamian 1965), PP (Parsamian & Petrosian 1979), RNO (Cohen 1980), Sh1- (Sharpless 1953), Sh2- (Sharpless 1959) andvdB-RN (van de Bergh 1966).…”

Section: Search Methodsmentioning

confidence: 99%

New infrared star clusters in the Northern and Equatorial Milky Way with 2MASS

Bica

Dutra

Soares

et al. 2003

A&A

202

216

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Abstract. We carried out a survey of infrared star clusters and stellar groups on the 2MASS J, H and K s all-sky release Atlas in the Northern and Equatorial Milky Way (350The search in this zone complements that in the Southern Milky Way (Dutra et al. 2003a). The method concentrates efforts on the directions of known optical and radio nebulae. The present study provides 167 new infrared clusters, stellar groups and candidates. Combining the two studies for the whole Milky Way, 346 infrared clusters, stellar groups and candidates were discovered, whereas 315 objects were previously known. They constitute an important new sample for future detailed studies.

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“…We observed NGC 6334, NGC 6357, and GM 24 (GM 1-24, Gyulbudaghian et al 1977) in U, B, and V bands with the VIMOS camera (ESO-VLT). VIMOS is a visible (360 to 1000 nm) wide field imager and multi-object spectrograph mounted at the Nasmyth focus B of UT3 Melipal.…”

Section: U B and V Vimos Datamentioning

confidence: 99%

Statistical study of OB stars in NGC 6334 and NGC 6357

Russeil

Zavagno

Adami

et al. 2012

A&A

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Context. Star-forming complexes are large structures exhibiting massive star-formation at different stages of evolution, from dense cores to well-developed H ii regions. They are very interesting for the study of the formation and evolution of stars. NGC 6334 and NGC 6357 are two active and relatively nearby star-forming complexes. From the extinction map and the sub-mm cold dust emission, and because they have similar velocities, these regions are most likely connected. However, located in the direction of the Galactic center their radial velocity is not representative of their distance. An alternative is then to determine the distance of NGC 6334 and NGC 6357 from their stellar content. Aims. Our aim is to perform a census of O-B3 ionising stars in NGC 6334 and NGC 6357, to determine the extinction coefficient, and the distance of both regions. A census of O-B3 stars is an essential basis for estimating the statistical lifetime of the earliest massive star-forming phases. Methods. We performed a U, B, V, and R photometric survey of a large area covering NGC 6334 and NGC 6357 with the VIMOS (ESO-VLT) and the MOSAIC (CTIO) instruments. This allows us to have a complete census of O to B3 stars up to V = 22.6 mag. The OB stars are selected based on their U − B and B − V colors. The most robust extinction coefficient is determined from color−color plots before computing the distance of the OB stars. Results. We find a higher value than typical of the diffuse interstellar medium for R V of 3.53 ± 0.08 and 3.56 ± 0.15 for NGC 6357 and NGC 6334, respectively. Adopting these R V values, the distances of NGC 6357 and NGC 6334 are 1.9 ± 0.4 kpc and 1.7 ± 0.3 kpc. We conclude that, within the error bars, both regions are thus at the same distance of 1.75 kpc (weighted mean). We confirm that the value of R V is linked to the large dust grain content. In particular, we found that there are more very small grains in NGC 6357 than in NGC 6334, suggesting that NGC 6357 could be more evolved than NGC 6334. Placed in the Galactic context, the NGC 6334-NGC 6357 complex appears to be located at the inner edge of the Sagittarius-Carina arm. Our census of O to B3 stars leads to a count of ∼230, which allows us to determine the statistical lifetime of the earliest phases of the massive stars. The starless and the protostellar phases have a mean statistical lifetime of ∼1.5 × 10 4 yr and ∼2.2 × 10 5 yr, respectively.

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Trapezium systems containing T tauri stars

Cited by 5 publications

References 1 publication

PMS and ZAMS stars associated with the dark cloud LDN 1655

PMS and ZAMS stars associated with the dark cloud LDN 1655

New infrared star clusters in the Northern and Equatorial Milky Way with 2MASS

Statistical study of OB stars in NGC 6334 and NGC 6357

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