Direct Mid—IR Images of GL 2591,W51—IRS2 and S140

Persi, P.; Ferrari-Toniolo, M.; Marenzi, Anna; Busso, M.; Corcione, L.; Marengo, Massimo; Tapia, M.

doi:10.1007/978-94-011-0147-9_131

Cited by 12 publications

(23 citation statements)

References 4 publications

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“…We also see the presence of lower mass stars forming a well-defined cluster (e.g., near IRS 5) together with O-B type stars that have recently formed. These results support the hypothesis that the formation of high-mass stars is associated with the formation of dense clusters of lowmass stars (e.g., Persi et al 1994;Tapia et al 1997). The stellar cluster near IRS 5 has a total luminosity of about 2 ; 10 5 L .…”

Section: Mass Estimationsupporting

confidence: 87%

Deep Near‐Infrared Observations of the W3 Main Star‐forming Region

Ojha

Tamura

Nakajima

et al. 2004

ApJ

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We present a deep JHK s -band imaging survey of the W3 Main star-forming region, using the near-infrared camera SIRIUS mounted on the University of Hawaii 2.2 m telescope. The near-infrared survey covers an area of $24 arcmin 2 with 10 limiting magnitudes of $19.0, 18.1, and 17.3 in the J, H, and K s bands, respectively. We construct JHK color-color and J versus JÀH and K versus HÀK color-magnitude diagrams to identify young stellar objects and estimate their masses. Based on these color-color and color-magnitude diagrams, a rich population of young stellar objects is identified that is associated with the W3 Main region. A large number of previously unreported red sources (HÀK > 2) have also been detected around W3 Main. We argue that these red stars are most probably pre-main-sequence stars with intrinsic color excesses. We find that the slope of the K s -band luminosity function (KLF) of W3 Main is lower than the typical values reported for young embedded clusters. The derived slope of the KLF is the same as that found in 1996 by Megeath and coworkers, from which analysis indicated that the W3 Main region has an age in the range of 0.3-1 Myr. Based on the comparison between models of pre-main-sequence stars and the observed color-magnitude diagram, we find that the stellar population in W3 Main is primarily composed of low-mass pre-main-sequence stars. We also report the detection of isolated young stars with large infrared excesses that are most probably in their earliest evolutionary phases.

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Section: Mass Estimationsupporting

confidence: 87%

Deep Near‐Infrared Observations of the W3 Main Star‐forming Region

Ojha

Tamura

Nakajima

et al. 2004

ApJ

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“…1), with the brightest source (IRS 1) located adjacent to the main peak of the radio emission. Further high resolution photometric observations by Persi et al (1994) have revealed the presence of a very young, deeply embedded cluster with 130 members in the same region. Spectra of these sources exhibit deep 9.7 μm silicate absorption features (Moorwood & Salinari 1981), leading to their interpretation as pre-main-sequence objects.…”

Section: Prior Observations Of Ngc 3576mentioning

confidence: 96%

“…The hourglass shaped emission feature running north-south across the centre of the image likely correspond to a bipolar cavity being evacuated by the central embedded cluster. The giant molecular cloud which hosts NGC3576 manifests itself as large extincted areas to the north-east and south-west, and is at a distance of 2.4 kpc (Persi et al 1994). The extent of the H II region is illustrated by the thick black contour, corresponding to the 3-σ (54 mJy/beam) level in the 3.4-cm free-free emission mapped by de Pree et al (1999).…”

Section: Prior Observations Of Ngc 3576mentioning

confidence: 99%

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Multi-generation massive star-formation in NGC 3576

Purcell

Minier

Longmore

et al. 2009

A&A

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Context. Recent 1.2-mm continuum observations have shown the giant H II region NGC 3576 to be embedded in the centre of an extended filamentary dust-cloud. The bulk of the filament away from the H II region contains a number of clumps seen only at (sub-)millimetre wavelengths. Infrared and radio observations of the central star cluster have uncovered evidence of sequential starformation leading us to believe that the adjacent clumps may host massive protostellar objects at a very early stage of evolution. Aims. We have investigated the physical and chemical conditions in the dusty clumps with the goal of characterising their star-forming content. Methods. We have used the Australia Telescope Compact Array (ATCA) to image the cloud for the NH 3 (1,1), (2,2) and (4,4) transitions, 22 GHz H 2 O masers, and 23 GHz continuum emission. The 70-m Tidbinbilla dish was used to estimate the total integrated intensity of NH 3 . We also utilised the 22-m Mopra antenna to map the region for the molecular lines 13 CO (1 -0), C 18 O (1 -0), HCO + (1 -0), H 13 CO + (1 -0), CS (1 -0) and N 2 H + (1 -0). Results. Emission from dense molecular gas follows the morphology of the 1.2-mm dust emission, except towards the central ionised region. The H II region is observed to be expanding into the molecular cloud, sweeping up a clumpy shell of gas, while the central star cluster is dispersing the molecular gas to the east. Analysis of the NH 3 data indicates that temperature and linewidth gradients exist in the western arm of the filament. Temperatures are highest adjacent to the central H II region, indicating that the embedded cluster of young stars there is heating the gas. Six new H 2 O masers were detected in the arms of the filament, all associated with NH 3 emission peaks, confirming that star-formation has begun within these cores. Core masses range from 5 to 516 M and most appear to be gravitationally bound. Complementary results by André et al. (2008) imply that seven cores will go on to form massive stars between 15 and 50 M . The large scale velocity structure of the filament is smooth, but at least one clump shows the signature of inward gas motions via asymmetries in the NH 3 (1,1) line profiles. The same clump exhibits an enhanced abundance of N 2 H + , which coupled with an absence of CO indicates depletion onto the dust grain surface. Conclusions. The HII region at the heart of NGC 3576 is potentially triggering the formation of massive stars in the bulk of the associated cloud.

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“…In conjugation with deep optical photometric data the identified PMS can be better characterized (e.g., mass, age) by comparing their positions on the HR digram with the theoretical evolutionary models. The characterization PMS stars are essential to derive the cluster properties and to understand its star formation history (e.g., Lada & Lada 1991;Persi et al 1994;Tapia et al 1997;Ojha et al 2004). We therefore studied the cluster with multiwavelength photometric data to have a better picture on the cluster properties and star formation activity.…”

Section: Introductionmentioning

confidence: 99%

The young cluster NGC 2282: a multiwavelength perspective

Dutta¹,

Mondal²,

Jose³

et al. 2015

Mon. Not. R. Astron. Soc.

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We present the analysis of the stellar content of NGC 2282, a young cluster in the Monoceros constellation, using deep optical BV I and IPHAS photometry along with infrared (IR) data from UKIDSS and Spitzer-IRAC. Based on the stellar surface density analysis using nearest neighborhood method, the radius of the cluster is estimated as ∼ 3.15 ′ . From optical spectroscopic analysis of 8 bright sources, we have classified three early B-type members in the cluster, which includes, HD 289120, a previously known B2V type star, a Herbig Ae/Be star (B0.5 Ve) and a B5 V star. From spectrophotometric analyses, the distance to the cluster has been estimated as ∼ 1.65 kpc. The K-band extinction map is estimated using nearest neighborhood technique, and the mean extinction within the cluster area is found to be A V ∼ 3.9 mag. Using IR colour-colour criteria and H α -emission properties, we have identified a total of 152 candidate young stellar objects (YSOs) in the region, of which, 75 are classified as Class II, 9 are Class I YSOs. Our YSO catalog also includes 50 H α -emission line sources, identified using slitless spectroscopy and IPHAS photometry data. Based on the optical and near-IR colour-magnitude diagram analyses, the cluster age has been estimated to be in the range of 2 − 5 Myr, which is in agreement with the estimated age from disc fraction (∼ 58%). Masses of these YSOs are found to be ∼ 0.1−2.0 M ⊙ . Spatial distribution of the candidate YSOs shows spherical morphology, more or less similar to the surface density map.

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Direct Mid—IR Images of GL 2591,W51—IRS2 and S140

Cited by 12 publications

References 4 publications

Deep Near‐Infrared Observations of the W3 Main Star‐forming Region

Deep Near‐Infrared Observations of the W3 Main Star‐forming Region

Multi-generation massive star-formation in NGC 3576

The young cluster NGC 2282: a multiwavelength perspective

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