The Midcourse Space Experiment Point Source Catalog Version 2.3 Explanatory Guide

Egan, M. P.; Mizuno, D. R.; Engelke, C. W.; Price, S. D.; Carey, Sean; Cohen, Martin; Kraemer, K. E.; Wright, C. O.; Gugliotti, G. M.

doi:10.21236/ada418993

Cited by 133 publications

(176 citation statements)

References 11 publications

(9 reference statements)

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“…When either of the IRC bands data is saturated, we use the MSX A-band and E-band instead. The resolution of the IRC all-sky survey and MSX is 9.4 and 18.3 (Egan et al 1999), respectively. [O III] 88 μm and the FIR continuum emissions with the radio continuum from the NVSS at 1.4 GHz, and 9 μm and 18 μm emission detected by the IRC all-sky survey.…”

Section: Resultsmentioning

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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Section: Resultsmentioning

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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“…For MSX we used the point-source catalogue (Egan et al 1999), while for Spitzer/MIPSGAL we used aperture photometry from the post-basic calibrated data available at IPAC server 5 . As highmass protostars are expected to form at the center of the dense core and because little Spitzer/MIPSGAL 24 μm or MSX-21 μm emission can be extended, we define a physical association when the source falls within the delimitation of the core but not farther than 23 from the dense core center.…”

Section: Association With 24 μM Sourcesmentioning

confidence: 99%

The earliest phases of high-mass star formation: the NGC 6334-NGC 6357 complex

Russeil¹,

Zavagno²,

Motte

et al. 2010

A&A

135

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Context. Our knowledge of high-mass star formation has been mainly based on follow-up studies of bright sources found by IRAS, and has thus been incomplete for its earliest phases, which are inconspicuous at infrared wavelengths. With a new generation of powerful bolometer arrays, unbiased large-scale surveys of nearby high-mass star-forming complexes now search for the high-mass analog of low-mass cores and class 0 protostars. Aims. Following the pioneering study of Cygnus X, we investigate the star-forming region NGC 6334-NGC 6357 (∼1.7 kpc). Methods. We study the complex NGC 6334-NGC 6357 in an homogeneous way following the previous work of Motte and collaborators. We used the same method to extract the densest cores which are the most likely sites for high-mass star formation. We analyzed the SIMBA/SEST 1.2 mm data presented in Munoz and coworkers, which covers all high-column density areas (A v ≥ 15 mag) of the NGC 6334-NGC 6357 complex and extracted dense cores following the method used for Cygnus X. We constrain the properties of the most massive dense cores (M > 100 M ) using new molecular line observations (as SiO, N 2 H + ,H 13 CO + , HCO + (1-0) and CH 3 CN) with Mopra and a complete cross-correlation with infrared databases (MSX, GLIMPSE, MIPSGAL) and literature. Results. We extracted 163 massive dense cores of which 16 are more massive than 200 M . These high-mass dense cores have a typical FWHM size of 0.37 pc, an average mass of M ∼ 600 M , and a volume-averaged density of ∼1.5 × 10 5 cm −3 . Among these massive dense cores, 6 are good candidates for hosting high-mass infrared-quiet protostars, 9 cores are classified as high-luminosity infrared protostars, and we find only one high-mass starless clump (∼0.3 pc, ∼4 × 10 4 cm −3 ) that is gravitationally bound. Conclusions. Since our sample is derived from a single molecular complex and covers every embedded phase of high-mass star formation, it provides a statistical estimate of the lifetime of massive stars. In contrast to what is found for low-mass class 0 and class I phases, the infrared-quiet protostellar phase of high-mass stars may last as long as their more well known high-luminosity infrared phase. As in Cygnus X, the statistical lifetime of high-mass protostars is shorter than found for nearby, low-mass star-forming regions which implies that high-mass pre-stellar and protostellar cores are in a dynamic state, as expected in a molecular cloud where turbulent and/or dynamical processes dominate.

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“…Finally, to search for star formation activity in the surroundings of WR55, we have inspected available IR point source catalogues: the MSX6C Infrared Point Source Catalogue (Egan et al 1999) in Bands A (8.3 μm), C (12.1 μm), D (14.7 μm), and E (21.3 μm); the IRAS Point Source Catalogue 4 at 12, 25, 60, and 100 μm; and the IRAC point source catalogue, which includes photometry at 3.6, 4.5, 5.8, and 8.0 μm. The CO emission distribution at velocities in the range -67.2 to -61.9 km s −1 shows an elongated cloud extending from E to W, beyond the surveyed area.…”

Section: Complementary Datamentioning

confidence: 99%

Unveiling the molecular environment of the ring nebula RCW 78

Cappa

Rubio

Martín

et al. 2009

A&A

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Aims. We present a study of the ionized, neutral atomic, and molecular gas associated with the ring nebula RCW 78 around the WR star HD 117688 (=WR 55) with the aim of analyzing the distribution of the associated gas and investigating its energetics. Methods. We base our study on 12 CO(1-0) and 12 CO(2-1) observations of the brightest section of the nebula carried out with the SEST telescope with angular resolutions of 45 and 22 , respectively; and on complementary 12 CO(1-0) data of a larger area obtained with the NANTEN telescope with an angular resolution of 2. 7, Hi 21-cm line data taken from the ATCA survey, IRAS HIRES data, and radio continuum data at 4.85 GHz from the Parkes survey. Results. We report the detection of molecular gas having velocities in the range -56 to -33 km s −1 associated with the western region of RCW 78. A few patches of molecular gas possibly linked to the eastern faint section are detected. The CO emission appears concentrated in a region of 23 × 18 in size, with a total molecular mass of (1.3 ± 0.5) × 10 5 M , mainly connected to the western section. The analysis of the neutral atomic gas distribution reveals the H i envelope of the molecular cloud, while the radio continuum emission shows a ring-like structure, which is the radio counterpart of the optical nebula. The gas distribution is compatible with the western section of RCW 78 having originated in the photodissociation and ionization of the molecular gas by the UV photons of the WN7 star HD 117688, and with the action of the stellar winds of the WR star on the surrounding gas. In this scenario, the interstellar bubble expanded more easily towards the east than towards the west due to the lack of dense molecular gas in the eastern section. The proposed scenario also explains the off center location of WR 55. A number of infrared point sources classified as YSO candidates showed that star formation activity is present in the molecular gas linked to the nebula. The possibility that the expansion of the bubble triggered star formation in this region cannot be discarded.

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The Midcourse Space Experiment Point Source Catalog Version 2.3 Explanatory Guide

Cited by 133 publications

References 11 publications

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

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

The earliest phases of high-mass star formation: the NGC 6334-NGC 6357 complex

Unveiling the molecular environment of the ring nebula RCW 78

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