Deep Near‐Infrared Survey toward the M17 Region

Jiang, Zengjie; Yao, Yongqiang; Yang, Ji; Ando, Moriaki; Kato, Daisuke; Kawai, Takeshi; Kurita, Mikio; Nagata, T.; Nagayama, Takahiro; Nagashima, Chie; Sato, Shuji; Tamura, Motohide; Nakaya, Hidehiko; Sugitani, Koji

doi:10.1086/342157

Cited by 57 publications

(89 citation statements)

References 26 publications

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“…Compared to, e.g., the Orion Nebula (O'Dell 2001) and M17 (Jiang et al 2002) regions, one of the prominent features of the star formation in W3 Main is the absence of dominant OB stars.…”

Section: Star Formation Toward W3 Mainmentioning

confidence: 99%

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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“…Compared to, e.g., the Orion Nebula (O'Dell 2001) and M17 (Jiang et al 2002) regions, one of the prominent features of the star formation in W3 Main is the absence of dominant OB stars.…”

Section: Star Formation Toward W3 Mainmentioning

confidence: 99%

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

Ojha

Tamura

Nakajima

et al. 2004

ApJ

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“…It contains a dozen of O-or early B-type stars (Hanson et al 1997) and the age of the central cluster is <3 Myr (Hanson et al 1997;Jiang et al 2002). Felli et al (1984) presented radio maps of M 17 and discussed the structures and nature of the ISM.…”

Section: Targetsmentioning

confidence: 99%

Properties of active galactic star-forming regions probed by imaging spectroscopy with the Fourier transform spectrometer (FTS) onboard AKARI

Okada

Kawada

Murakami

et al. 2010

A&A

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Aims. We investigate the structure of the interstellar medium (ISM) and identify the location of possible embedded excitation sources from far-infrared (FIR) line and mid-infrared continuum emission maps. Methods. We carried out imaging spectroscopic observations of four giant Galactic star-forming regions with the Fourier transform spectrometer (FTS) onboard AKARI. We obtained [O III] 88 μm and [C II] 158 μm line intensity maps of all the regions: G3.270-0.101, G333.6-0.2, NGC 3603, and M 17. Results. For G3.270-0.101, we obtained high-spatial-resolution [O III] 88 μm line-emission maps and a FIR continuum map for the first time, which imply that [O III] 88 μm emission identifies the excitation sources more clearly than the radio continuum emission. In G333.6-0.2, we found a local [O III] 88 μm emission peak, which is indicative of an excitation source. This is supported by the 18 μm continuum emission, which is considered to trace the hot dust distribution. For all regions, the [C II] 158 μm emission is distributed widely as suggested by previous observations of star-forming regions. Conclusions. We conclude that [O III] 88 μm emission traces the excitation sources more accurately than the radio continuum emission, especially where there is a high density and/or column density gradient. The FIR spectroscopy provides a promising means of understanding the nature of star-forming regions.

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“…M17 is 4 times more distant from the Sun than Orion and considerably more energetic. The M17 H ii region is ionized by the open cluster NGC 6618, which contains over 100 OB stars ( Lada et al 1991) and has an age of less than 3 Myr (Jiang et al 2002). The center of the cluster is dominated by a ring of seven O stars 1 0 in diameter ( Hanson et al 1997).…”

Section: Introductionmentioning

confidence: 99%

A Multiwavelength Study of M17: The Spectral Energy Distribution and PAH Emission Morphology of a Massive Star Formation Region

Povich

Stone

Churchwell

et al. 2007

ApJ

176

199

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We combine diffuse emission photometry from GLIMPSE and several other Galactic plane surveys covering near-IR through radio wavelengths to synthesize a global spectral energy distribution (SED) for the M17 complex. By balancing the integrated flux in the SED with the total bolometric luminosity of all known O and early B stars in the ionizing cluster, we estimate a distance to M17 of 1:6 þ0:3 À0:1 kpc. At this distance, the observed total flux in the SED corresponds to a luminosity of 2:4 AE 0:3 ; 10 6 L . We find that the SED from the H ii region peaks at shorter wavelengths and has a qualitatively different shape than the SED from the photodissociation region ( PDR). We find that polycyclic aromatic hydrocarbons ( PAHs) are destroyed over a short distance or edge at the boundary of the H ii region. We demonstrate that this PAH destruction edge can be located easily using GLIMPSE band-ratio images and confirm this using Spitzer IRS spectra. We investigate the relative roles of extreme ultraviolet (EUV ) and X-ray photons in the destruction of PAHs, concluding that X-rays are not an important PAH destruction mechanism in M17 or, by extension, in any other Galactic H ii region. Our results support the hypothesis that PAHs are destroyed by EUV photons within H ii regions. PAHs dominate the mid-IR emission in the neutral PDR beyond the ionized gas.

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Deep Near‐Infrared Survey toward the M17 Region

Cited by 57 publications

References 26 publications

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

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

Properties of active galactic star-forming regions probed by imaging spectroscopy with the Fourier transform spectrometer (FTS) onboard AKARI

A Multiwavelength Study of M17: The Spectral Energy Distribution and PAH Emission Morphology of a Massive Star Formation Region

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