The Molonglo Galactic Plane Survey. I. Overview and Images

Green, Anne; Cram, L. E.; Large, M. I.; Ye, Taisheng

doi:10.1086/313208

Cited by 116 publications

(149 citation statements)

References 26 publications

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“…3). This source is extended (35−40 arcsec) and spatially coincident with the radio source MGPS J150850-621025 (Green et al 1999). The source is detected with an energy flux of (7.0 ± 0.7) × 10 −13 erg cm −2 s −1 in the range 2−10 keV, compatible with the flux measured by ROSAT.…”

Section: X-ray Observations and Data Analysismentioning

confidence: 76%

“…At radio and infrared wavelengths, HESS J1507-622 is offset too far from the Galactic plane to be covered by the Southern Galactic Plane Survey (Haverkorn et al 2006) or by Spitzer GLIMPSE (Benjamin 2005). This region of the sky had been covered by the Midcourse Space Experiment (MSX) in all its wave bands (8.28 μm, 12.13 μm, 14.65 μm, 21.3 μm, Simon et al 2006) and by the MOLONGLO Galactic plane survey (Green et al 1999), yielding no evidence of any plausible counterpart. HESS J1507-622 is located on a radio emission filament shown in Duncan et al (1995) at 2.4 GHz, which was tentatively considered a part of a very large (∼15 • in diameter) and nearby candidate SNR (visible in Fig.…”

Section: Searching For Counterpartsmentioning

confidence: 99%

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Discovery and follow-up studies of the extended, off-plane, VHE gamma-ray source HESS J1507-622

Acero¹,

Aharonian²,

Akhperjanian³

et al. 2010

A&A

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Context. The detection of gamma-rays in the very-high-energy (VHE) range (100 GeV−100 TeV) offers the possibility of studying the parent population of ultrarelativistic particles found in astrophysical sources, so it is useful for understanding the underlying astrophysical processes in nonthermal sources. Aims. The discovery of the VHE gamma-ray source HESS J1507-622 is reported and possibilities regarding its nature are investigated. Methods. The H.E.S.S. array of imaging atmospheric Cherenkov telescopes (IACTs) has a high sensitivity compared with previous instruments (∼1% of the Crab flux in 25 h observation time for a 5σ point-source detection) and has a large field of view (∼5 • in diameter). HESS J1507-622 was discovered within the ongoing H.E.S.S. survey of the inner Galaxy, and the source was also studied by means of dedicated multiwavelength observations. Results. A Galactic gamma-ray source, HESS J1507-622, located ∼3.5 • from the Galactic plane was detected with a statistical significance >9σ. Its energy spectrum is well fitted by a power law with spectral index Γ = 2.24 ± 0.16 stat ± 0.20 sys and a flux above 1 TeV of (1.5 ± 0.4 stat ± 0.3 sys ) × 10 −12 cm −2 s −1 . Possible interpretations (considering both hadronic and leptonic models) of the VHE gamma-ray emission are discussed in the absence of an obvious counterpart.

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Section: X-ray Observations and Data Analysismentioning

confidence: 76%

Section: Searching For Counterpartsmentioning

confidence: 99%

Discovery and follow-up studies of the extended, off-plane, VHE gamma-ray source HESS J1507-622

Acero¹,

Aharonian²,

Akhperjanian³

et al. 2010

A&A

View full text Add to dashboard Cite

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“…We define an association when the object is located within the FWHM size of the core. An association with a source of free-free emission was established by using the 1.4 GHz SGPS survey (Haverkorn et al 2006) and the 843 MHz MOST survey (Green et al 1999), which were both correlated with the NVSS catalog given by Condon et al (1998) and with White (2005) catalog. We cannot check the nature of the detected cm-emission with the current database, but it is probably caused by the emission of H ii regions.…”

Section: Association With Radio Sources and Masersmentioning

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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“…With the aim of finding any possible radio counterpart within the location error box of the X-ray source, we have used the Molonglo Galactic Plane Survey (MGPS) conducted at 843 MHz with the Molonglo Observatory Synthesis Telescope (MOST) (Green et al 1999). Observations of the region of interest were conducted on 1990 June 9 and on 1992 April 16.…”

Section: Multiwavelength Study Of the Ax J16390−4642 Fieldmentioning

confidence: 99%

The dust-enshrouded microquasar candidate AX J1639.0-4642 = IGR J16393-4643

Combi

Ribó

Mirabel

et al. 2004

A&A

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Abstract. We present a multiwavelength study of the field containing the unidentified X-ray source AX J1639.0−4642, discovered with the ASCA observatory and recently detected with the IBIS telescope, onboard the INTEGRAL satellite, dubbed IGR J16393−4643. The huge hydrogen column density towards the source, the hard spectral index in the 0.7-10 keV band and its flux variability suggest that the source is a High Mass X-ray Binary (HMXB) enshrouded by dust. Our search reveals the presence of a non-thermal radio counterpart within the X-ray error box. After a study of the broadband emission from X-rays to the radio domain, we propose that AX J1639.0−4642 is a dust-enshrouded Microquasar (MQ) candidate. In addition, the X-ray source is well within the 95% location contour of the unidentified γ-ray source 3EG J1639−4702. The main properties of AX J1639.0−4642/3EG J1639−4702 are consistent with those of two other MQs previously proposed to display high-energy γ-ray emission.

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The Molonglo Galactic Plane Survey. I. Overview and Images

Cited by 116 publications

References 26 publications

Discovery and follow-up studies of the extended, off-plane, VHE gamma-ray source HESS J1507-622

Discovery and follow-up studies of the extended, off-plane, VHE gamma-ray source HESS J1507-622

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

The dust-enshrouded microquasar candidate AX J1639.0-4642 = IGR J16393-4643

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