<i>Spitzer</i>/IRAC‐MIPS Survey of NGC 2244: Protostellar Disk Survival in the Vicinity of Hot Stars

Balog, Z.; Muzerolle, James; Rieke, G. H.; Su, K. Y. L.; Young, E. T.; Megeath, S. T.

doi:10.1086/513311

Cited by 120 publications

(176 citation statements)

References 41 publications

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“…The upper right panel of Fig. 14 also allows a more easy confrontation of our result with that of Balog et al (2007). As explained, these authors studied the spatial variation in the disk frequency with respect to the positions of massive stars in the young cluster NGC 2244.…”

Section: Spatial Distribution Of the Clustermentioning

confidence: 83%

“…The region corresponding to the highest fluxes in Fig. 13 has a radius of 0.6 parsecs, the distance from massive stars at which Balog et al (2007) found a sudden decline in disk frequency in NGC 2244.…”

Section: Spatial Distribution Of the Clustermentioning

confidence: 89%

“…Balog et al (2007) and Guarcello et al (2007), hereafter GPM07, each applied this approach to a young cluster, NGC 2244 and NGC 6611, respectively. In their Spitzer/IRAC-MIPS study of NGC 2244 (at a distance of 1.4−1.7 kpc from the Sun and with an age of about 2−3 Myr), Balog et al (2007) found that the disk frequency drops dramatically at a distance of 0.5 parsec from the massive cluster members. At larger distances, however, stars with disk do not experience effects induced by massive stars, since the disk frequency is not spatially correlated with their positions.…”

Section: Introductionmentioning

confidence: 99%

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Correlation between the spatial distribution of circumstellar disks and massive stars in the young open cluster NGC 6611

Guarcello

Micela

Damiani

et al. 2009

A&A

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Context. The observations of the proplyds in the Orion Nebula Cluster, exhibiting clear evidence of ongoing photoevaporation, have provided clear proof of the role of externally induced photoevaporation in the evolution of circumstellar disks. NGC 6611 is an open cluster suitable for study of disk photoevaporation, due to its significant population of massive members and stars with disk. In a previous paper, we obtained evidence of the influence of the strong UV field generated by the massive cluster members on the evolution of disks around low-mass Pre-Main Sequence members. Our study was based on a multiband BVIJHK and X-ray catalog compiled for the purpose of selecting cluster members with and without disk. Aims. We attempt to complete the list of candidate cluster members, using data at longer wavelengths obtained with Spitzer/IRAC, and we reinvestigate the effects of UV radiation on the evolution of disks in NGC 6611. Methods. In a field of view of 33 × 34 centered on the cluster, we select the candidate members with disks of NGC 6611 using IRAC color-color diagrams and suitable reddening-free color indices. Using the X-ray data to select Class III cluster members, we also estimate disks frequency relative to the intensity of the incident radiation emitted by massive members. Results. We identify 458 candidate members with circumstellar disks, among which 146 had not been discovered previously. By comparing all color indices used to select cluster members with disk, we claim that these indices measure the excess of radiation due to the emission of the same physical region of the disk (i.e. the inner rim at the dust sublimation radius). Our new results confirm that UV radiation from massive stars affects the evolution of nearby circumstellar disks.

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Section: Spatial Distribution Of the Clustermentioning

confidence: 83%

Section: Spatial Distribution Of the Clustermentioning

confidence: 89%

Section: Introductionmentioning

confidence: 99%

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Correlation between the spatial distribution of circumstellar disks and massive stars in the young open cluster NGC 6611

Guarcello

Micela

Damiani

et al. 2009

A&A

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“…Spitzer observations have revealed a clear anti-correlation between the Based on observations performed at ESO's La Silla-Paranal observatory under programme 081.C-0467. Tables 1 and 3 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/539/A119 frequencies of circumstellar disks and the presence of massive stars in these clusters (e.g., NGC 2244, NGC 6611, Balog et al 2007;Guarcello et al 2009). UV irradiation by hot, massive stars causing photoevaporation of disks around neighboring lower mass young stars is a favored mechanism to explain the observed low disk frequencies near massive stars.…”

Section: Introductionmentioning

confidence: 99%

Star formation and disk properties in Pismis 24

Fang

Boekel

King

et al. 2012

A&A

126

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Context. Circumstellar disks are expected to evolve quickly in massive young clusters harboring many OB-type stars. Two processes have been proposed to drive the disk evolution in such cruel environments: (1) gravitational interaction between circumstellar disks and nearby passing stars (stellar encounters); and (2) photoevaporation by UV photons from massive stars. The relative importance of both mechanisms is not well understood. Studies of massive young star clusters can provide observational constraints on the processes of driving disk evolution. Aims. We investigate the properties of young stars and their disks in the NGC 6357 complex, concentrating on the most massive star cluster within the complex: Pismis 24. Methods. We use infrared data from the 2MASS and Spitzer GLIMPSE surveys, complemented with our own deep Spitzer imaging of the central regions of Pismis 24, in combination with X-ray data to search for young stellar objects (YSOs) in NGC 6357 complex. The infrared data constrain the disk presence and are complemented by optical photometric and spectroscopic observations, obtained with VLT/VIMOS, that constrain the properties of the central stars. For those stars with reliable spectral types we combine spectra and photometry to estimate the mass and age. For cluster members without reliable spectral types we obtain the mass and age probability distributions from R and I-band photometry, assuming these stars have the same extinction distribution as those in the "spectroscopic" sample. We compare the disk properties in the Pismis 24 cluster with those in other clusters/star-forming regions employing infrared color-color diagrams. Results. We discover two new young clusters in the NGC 6357 complex. We give a revised distance estimate for Pismis 24 of 1.7 ± 0.2 kpc. We find that the massive star Pis 24-18 is a binary system, with the secondary being the main X-ray source of the pair. We provide photometry in 9 bands between 0.55 and 9 μm for the members of the Pismis 24 cluster. We derive the cluster mass function and find that up to the completeness limit at low masses it agrees well with the initial mass function of the Trapezium cluster. We derive a median age of 1 Myr for the Pismis 24 cluster members. We find five proplyds in HST archival imaging of the cluster, four of which are newly found. In all cases the proplyd tails are pointing directly away from the massive star system Pis 24-1. One proplyd shows a second tail, pointing away from Pis 24-2, suggesting this object is being photoevaporated from two directions simultaneously. We find that the global disk frequency (∼30%) in Pismis 24 is much lower than some other clusters of similar age, such as the Orion Nebula Cluster. When comparing the disk frequencies in 19 clusters/star-forming regions of various ages and different (massive) star content, we find that the disks in clusters harboring extremely massive stars (typically earlier than O5), like Pismis 24, are dissipated roughly twice as quickly as in clusters/star-forming regions with...

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“…Their conclusion is essentially based on the fact that some clusters are outside the ionization front and that they did not observed any overdensity of very young objects at the front position itself. A more local influence has been investigated by Balog et al (2007). They show that the OB stars in NGC 2244 contribute to the photo-evaporation of a low-mass star circumstellar disk when they are located within 0.5 pc.…”

Section: Introductionmentioning

confidence: 99%

Young stellar clusters in the Rosette molecular cloud

Cambrésy

Márton

Fehér

et al. 2013

A&A

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Aims. We focus on characterizing the young stellar population in the Rosette complex to improve our understanding of the processes that regulate the star formation in this region. Methods. We propose an original method that relies on the joint analysis of the star color and density in the near-infrared. It leads to mapping the molecular cloud spatial distribution and detecting the embedded clusters with their characterization in terms of member number and age estimation. Results. We have identified 13 clusters, 2 of which are new discoveries, and we estimate that the total number of young stellar objects in the Rosette ranges between 4000 and 8000 members. We find that the age distribution of the young clusters is not consistent with a general triggered scenario for the star formation in this molecular cloud. Conclusions. This study proves that the Rosette complex evolution is not governed by the influence of its OB star population. It suggests that the simple morphological appearance of an active region is not sufficient to conclude much about the triggering role in the star formation process. Our method of constraining the cluster properties using UKIDSS and WISE data has proven efficient, and studies of other regions of the Galactic plane would definitely benefit from this approach.

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Spitzer/IRAC‐MIPS Survey of NGC 2244: Protostellar Disk Survival in the Vicinity of Hot Stars

Cited by 120 publications

References 41 publications

Correlation between the spatial distribution of circumstellar disks and massive stars in the young open cluster NGC 6611

Correlation between the spatial distribution of circumstellar disks and massive stars in the young open cluster NGC 6611

Star formation and disk properties in Pismis 24

Young stellar clusters in the Rosette molecular cloud

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