Near-Infrared Study of M16: Star Formation in the Elephant Trunks

Sugitani, Koji; Tamura, Motohide; Nakajima, Yasushi; Nagashima, Chie; Nagayama, Takahiro; Nakaya, Hidehiko; Pickles, Andrew; Nagata, T.; Sato, Shuji; Fukuda, Naoya; Ogura, K.

doi:10.1086/339196

Cited by 90 publications

(115 citation statements)

References 11 publications

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“…These dense cores have densities n H 2 > 10 4 cm −3 , roughly a hundred times greater than ambient cloud material. Standard theory predicts that these cores collapse from the inside out (e.g., Shu, 1977;Terebey et al, 1984), in which the center forms first and the outer envelope rains down upon it. The collapse propagates at an effective sound speed of about 0.3 km s −1 , accounting for gas pressure and support due to magnetic fields and turbulence.…”

Section: How Do Protostellar Clouds Collapse?mentioning

confidence: 99%

“…These evaporating gaseous globules may contain young stars about to be revealed as the O and B stars evaporate their birth clouds. Near-IR observations show that about 10-20% contained embedded low-mass stellar and brown dwarf candidates see Figure 14), in addition to the higher-mass young stellar objects (YSOs) in the tips of the ablating columns (see also Sugitani et al, 2002;Thompson et al, 2002).…”

Section: How Does Environment Affect Star Formation and Vice Versa?mentioning

confidence: 99%

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The James Webb Space Telescope

et al. 2006

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Abstract. The James Webb Space Telescope (JWST) is a large (6.6 m), cold (<50 K), infrared (IR)-optimized space observatory that will be launched early in the next decade into orbit around the second Earth-Sun Lagrange point. The observatory will have four instruments: a near-IR camera, a near-IR multiobject spectrograph, and a tunable filter imager will cover the wavelength range, 0.6 < λ < 5.0 μm, while the mid-IR instrument will do both imaging and spectroscopy from 5.0 < λ < 29 μm.The JWST science goals are divided into four themes. The key objective of The End of the Dark Ages: First Light and Reionization theme is to identify the first luminous sources to form and to determine the ionization history of the early universe. The key objective of The Assembly of Galaxies theme is to determine how galaxies and the dark matter, gas, stars, metals, morphological structures, Space Science Reviews (2006) and active nuclei within them evolved from the epoch of reionization to the present day. The key objective of The Birth of Stars and Protoplanetary Systems theme is to unravel the birth and early evolution of stars, from infall on to dust-enshrouded protostars to the genesis of planetary systems. The key objective of the Planetary Systems and the Origins of Life theme is to determine the physical and chemical properties of planetary systems including our own, and investigate the potential for the origins of life in those systems. Within these themes and objectives, we have derived representative astronomical observations. To enable these observations, JWST consists of a telescope, an instrument package, a spacecraft, and a sunshield. The telescope consists of 18 beryllium segments, some of which are deployed. The segments will be brought into optical alignment on-orbit through a process of periodic wavefront sensing and control. The instrument package contains the four science instruments and a fine guidance sensor. The spacecraft provides pointing, orbit maintenance, and communications. The sunshield provides passive thermal control. The JWST operations plan is based on that used for previous space observatories, and the majority of JWST observing time will be allocated to the international astronomical community through annual peer-reviewed proposal opportunities.

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Section: How Do Protostellar Clouds Collapse?mentioning

confidence: 99%

Section: How Does Environment Affect Star Formation and Vice Versa?mentioning

confidence: 99%

The James Webb Space Telescope

et al. 2006

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“…Based on the location of # 331A in the CCD, they might be Class I sources of intermediate mass (e.g. Sugitani et al 2002b).…”

Section: Figmentioning

confidence: 99%

The stellar population and complex structure of the bright-rimmed cloud IC 1396N

Beltrán¹,

Massi

López

et al. 2009

A&A

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Context. IC 1396N is a bright-rimmed cloud associated with an intermediate-mass star-forming region, where a number of HerbigHaro objects, H 2 jet-like features, CO molecular outflows, and millimeter compact sources have been observed. Aims. We study the complex structure of the IC 1396N core and the molecular outflows detected in the region in detail and reveal the presence of additional YSOs inside this globule. Methods. We carried out a deep survey of the IC 1396N region in the J, H, K broadband filters and deep high-angular resolution observations in the H 2 narrowband filter with NICS at the TNG telescope. The completeness limits in the 2MASS standard are K s ∼ 17.5, H ∼ 18.5, and J ∼ 19.5. Results. A total of 736 sources have been detected in all three bands within the area where the JHK images overlap. There are 128 sources detected only in HK , 67 detected only in K , and 79 detected only in JH. We found only a few objects exhibiting a near-infrared excess and no clear signs of clustering of sources towards the southern rim. In the case of triggered star formation in the southern rim of the globule, this could be very recent, because it is not shown through Near-Infrared imaging alone. The H 2 emission is complex and knotty and shows a large number of molecular hydrogen features spread over the region, testifying to recent starformation activity throughout the whole globule. This emission is resolved into several chains or groups of knots that sometimes show a jet-like morphology. The shocked cloudlet model scenario previously proposed to explain the V-shaped morphology of the CO molecular outflow powered by the intermediate-mass YSO BIMA 2 seems to be confirmed by the presence of H 2 emission at the position of the deflecting western clump. New possible flows have been discovered in the globule, and some of them could be very long. In particular, the YSO BIMA 3 could be powering an old and poorly collimated outflow.

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“…3b), which indicates that a large fraction of the observed sources in W3 Main exhibit NIR excess emission. We classified the sources into three regions in the CC diagram (see, e.g., Tamura et al 1998;Sugitani et al 2002). ''F'' sources are located between reddening vectors projected from the intrinsic color of main-sequence stars and giants and are considered to be unreddened and reddened field stars (main-sequence stars, giants), or Class III /Class II sources with small NIR excess.…”

Section: Diagrammentioning

confidence: 99%

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

Ojha

Tamura

Nakajima

et al. 2004

ApJ

Self Cite

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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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Near-Infrared Study of M16: Star Formation in the Elephant Trunks

Cited by 90 publications

References 11 publications

The James Webb Space Telescope

The James Webb Space Telescope

The stellar population and complex structure of the bright-rimmed cloud IC 1396N

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

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