The star-forming history of the young cluster NGC 2264

Adams, Mark T.; Strom, K. M.; Strom, S. E.

doi:10.1086/190913

Cited by 60 publications

(44 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…The dark-grey one contains only stars with errors <0.10 and was fitted with a Gaussian distribution function over the interval −0.5 < ∆H α < 0.9 with mean value ∆H α = 0.21 and standard deviation σ ∆H α = 0.18. The mean value, which is assumed to correspond to non-emission objects, is close to the values found by Adams et al (1983) in NGC 2264 (0.30) and NGC 7089 (0.23). However, the dispersion among our data is over twice the value 0.08 found in NGC 2264 by them.…”

Section: The Search For Stars With Hα Emissionsupporting

confidence: 80%

“…We examined the point computing individual present-day masses of PMS stars and giving them the corresponding ages interpolating among the Bernasconi & Maeder (1996) models. Following the Iben & Talbot (1966) and Adams et al (1983) definitions and procedures, we estimated the star formation rate (SFR) in the cluster for three different stellar mass bins. The results, shown in Fig.…”

Section: Star Formation Ratementioning

confidence: 99%

“…Is it coeval or sequential (Iben & Talbot 1966;Herbst & Miller 1982;Adams et al 1983)? -Is the IMF slope universal?…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Photometric study of the young open cluster NGC 3293

Baume

Vazquez²,

Carraro³

et al. 2003

A&A

View full text Add to dashboard Cite

Abstract. Deep and extensive CCD photometric observations at UBV(RI) C H α were carried out in the area of the open cluster NGC 3293. The new data set allows to see the entire cluster sequence down to M V ≈ +4.5, revealing that stars with M V < −2 are evolving off the main sequence; stars with −2 < M V < +2 are located on the main sequence and stars with M V > +2 are placed above it. According to our analysis, the cluster distance is d = 2750 ± 250 pc (V 0 − M V = 12.2 ± 0.2) and its nuclear age is 8 ± 1 Myr. NGC 3293 contains an important fraction of pre-main sequence (PMS) stars distributed along a parallel band to the ZAMS with masses from 1 to 2.5 M and a mean contraction age of 10 Myr. This last value does not differ too much from the nuclear age estimate. If we take into account the many factors that may affect the PMS star positions on the colourmagnitude diagram, both ages can be perfectly reconciled. The star formation rate, on the other hand, suggests that NGC 3293 stars formed surely in one single event, therefore favouring a coeval process of star formation. Using the H α data, we detected nineteen stars with signs of H α emission in the region of NGC 3293, another indication that the star formation process is still active in the region. The computed initial mass function for the cluster has a slope of x = 1.2 ± 0.2, a bit flatter than the typical slope for field stars and similar to the values found for other young open clusters.

show abstract

Section: The Search For Stars With Hα Emissionsupporting

confidence: 80%

Section: Star Formation Ratementioning

confidence: 99%

See 1 more Smart Citation

Photometric study of the young open cluster NGC 3293

Baume

Vazquez²,

Carraro³

et al. 2003

A&A

View full text Add to dashboard Cite

show abstract

“…2.1.2. Similar indices were used in previous works (Adams et al 1983;Sung et al 1998;Baume et al 2003). Figure 7 presents the V vs. ΔH α diagram for all stars with measured ΔH α index together with the corresponding ZAMS in this plane.…”

Section: H α Photometric Diagramsmentioning

confidence: 78%

The Ara OB1a association

Baume

Carraro²,

Comerón³

et al. 2011

A&A

View full text Add to dashboard Cite

Context. The Ara OB1a association is a nearby complex in the fourth Galactic quadrant where a number of young/embedded star clusters are projected close to more evolved, intermediate age clusters. It is also rich in interstellar matter, and contains evidence of the interplay between massive stars and their surrounding medium, such as the rim HII region NGC 6188. Aims. We provide robust estimates of the fundamental parameters (age and distance) of the two most prominent stellar clusters, NGC 6167 and NGC 6193, that may be used as a basis for studing the star formation history of the region. Methods. The study is based on a photometric optical survey (UBVIH α ) of NGC 6167 and NGC 6193 and their nearby field, complemented with data from 2MASS-VVV, UCAC3, and IRAC-Spitzer in this region. Results. We produce a uniform photometric catalogue and estimate more robustly the fundamental parameters of NGC 6167 and NGC 6193, in addition to the IRAS 16375-4854 source. As a consequence, all of them are located at approximately the same distance from the Sun in the Sagittarius-Carina Galactic arm. However, the ages we estimate differ widely: NGC 6167 is found to be an intermediate-age cluster (20-30 Myr), NGC 6193 a very young one (1-5 Myr) with PMS, H α emitters and class II objects, and the IRAS 16375-4854 source is the youngest of the three containing several YSOs. Conclusions. These results support a picture in which Ara OB1a is a region where star formation has proceeded for several tens of Myr until the present. The difference in the ages of the different stellar groups can be interpreted as a consequence of a triggered star formation process. In the specific case of NGC 6193, we find evidence of possible non-coeval star formation.

show abstract

“…Rebull et al (2002) found systematic differences in model-derived ages of up to half an order in magnitude for a spectroscopically classified sample of variable stars. Sequential star formation has also been suggested (Adams et al 1983), with the peak rate of low-mass (M < 0.5 M ) star formation preceding that of the higher mass population. On the other hand, Baraffe et al (2009Baraffe et al ( , 2012 showed that the broadened cluster sequences observed in a number of star forming regions, which are usually interpreted as arising from an age spread, could also be caused by episodic accretion early on in the star formation process.…”

Section: Comparison To Pre-main Sequence Stellar Evolution Modelsmentioning

confidence: 97%

CoRoT 223992193: A new, low-mass, pre-main sequence eclipsing binary with evidence of a circumbinary disk

Gillen

Aigrain

McQuillan

et al. 2014

A&A

View full text Add to dashboard Cite

We present the discovery of CoRoT 223992193, a double-lined, detached eclipsing binary, comprising two pre-main sequence M dwarfs, discovered by the CoRoT space mission during a 23-day observation of the 3 Myr old NGC 2264 star-forming region. Using multi-epoch optical and near-IR follow-up spectroscopy with FLAMES on the Very Large Telescope and ISIS on the William Herschel Telescope we obtain a full orbital solution and derive the fundamental parameters of both stars by modelling the light curve and radial velocity data. The orbit is circular and has a period of 3.8745745 ± 0.0000014 days. The masses and radii of the two stars are 0.67 ± 0.01 and 0.495 ± 0.007 M and 1.30 ± 0.04 and 1.11 +0.04 −0.05 R , respectively. This system is a useful test of evolutionary models of young low-mass stars, as it lies in a region of parameter space where observational constraints are scarce; comparison with these models indicates an apparent age of ∼3.5-6 Myr. The systemic velocity is within 1σ of the cluster value which, along with the presence of lithium absorption, strongly indicates cluster membership. The CoRoT light curve also contains large-amplitude, rapidly evolving out-of-eclipse variations, which are difficult to explain using starspots alone. The system's spectral energy distribution reveals a mid-infrared excess, which we model as thermal emission from a small amount of dust located in the inner cavity of a circumbinary disk. In turn, this opens up the possibility that some of the out-of-eclipse variability could be due to occultations of the central stars by material located at the inner edge or in the central cavity of the circumbinary disk.

show abstract

The star-forming history of the young cluster NGC 2264

Cited by 60 publications

References 0 publications

Photometric study of the young open cluster NGC 3293

Photometric study of the young open cluster NGC 3293

The Ara OB1a association

CoRoT 223992193: A new, low-mass, pre-main sequence eclipsing binary with evidence of a circumbinary disk

Contact Info

Product

Resources

About