The Mopra Southern Galactic Plane CO Survey

Burton, M. G.; Braiding, Catherine; Glueck, Christian; Goldsmith, Paul F.; Hawkes, J.; Hollenbach, D. J.; Kulesa, Craig; Martin, Christopher L.; Pineda, J. L.; Rowell, G.; Simon, R.; Stark, A. A.; Stutzki, J.; Tothill, N.; Urquhart, J. S.; Walker, Constance E.; Walsh, A. J.; Wolfire, M. G.

doi:10.1017/pasa.2013.22

Cited by 84 publications

(54 citation statements)

References 61 publications

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“…12 CO in its different excitation states and 13 CO lines have been surveyed over most of the sky and public data are available from the classical survey "The Milky Way in Molecular Clouds" by Dame et al (2001) 2 , the "FCRAO CO Survey of the Outer Galaxy" by Heyer et al (1998) 3 , the "Galactic Ring Survey" by Jackson et al (2006) 4 , or the new "MOPRA Southern Galactic Plane CO Survey" by Burton et al (2013), among others. These public databases are an excellent starting point to search for possible SNR/MC interactions.…”

Section: Molecular Emissionmentioning

confidence: 99%

Supernova Remnants Interacting with Molecular Clouds: X-Ray and Gamma-Ray Signatures

et al. 2014

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The giant molecular clouds (MCs) found in the Milky Way and similar galaxies play a crucial role in the evolution of these systems. The supernova explosions that mark the death of massive stars in these regions often lead to interactions between the supernova remnants (SNRs) and the clouds. These interactions have a profound effect on our understanding of SNRs. Shocks in SNRs should be capable of accelerating particles to cosmic ray (CR) energies with efficiencies high enough to power Galactic CRs. X-ray and γ-ray studies have established the presence of relativistic electrons and protons in some SNRs and provided strong evidence for diffusive shock acceleration as the primary acceleration mechanism, including strongly amplified magnetic fields, temperature and ionization effects on the shock-heated plasmas, and modifications to the dynamical evolution of some systems. Because protons dominate the overall energetics of the CRs, it is crucial to understand this hadronic component even though electrons are much more efficient radiators and it can be difficult to identify the hadronic component. However, near MCs the densities are sufficiently high to allow the γ-ray emission to be dominated by protons. Thus, these interaction sites provide some of our best opportunities to constrain the overall energetics of these particle accelerators. Here we summarize some key properties of interactions between SNRs and MCs, with an emphasis on recent X-ray and γ-ray studies that are providing important constraints on our understanding of cosmic rays in our Galaxy.

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Section: Molecular Emissionmentioning

confidence: 99%

Supernova Remnants Interacting with Molecular Clouds: X-Ray and Gamma-Ray Signatures

et al. 2014

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“…In this paper we present wide-field data from the Mopra telescope in Australia, obtained as part of the Southern Galactic Plane CO survey (Burton et al 2013;Braiding et al 2015) and the High Elevation Antarctic Terahertz (HEAT) telescope at Ridge A in Antarctica of atomic carbon, aimed at pursuing this objective. The data covers roughly 1 square degree along the G328 sightline through the Galactic plane (i.e., =  l 328 ).…”

Section: Introductionmentioning

confidence: 99%

Extended Carbon Line Emission in the Galaxy: Searching for Dark Molecular Gas Along the G328 Sightline

Burton

Ashley

Braiding

et al. 2015

ApJ

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We present spectral data cubes of the [CI] 809 GHz, CO 12 115 GHz, CO 13 110 GHz, and HI 1.4 GHz line emission from a ∼1 square degree region along the =  l 328 (G328) sightline in the Galactic Plane. Emission arises principally from gas in three spiral arm crossings along the sightline. The distribution of emission in the CO and [CI] lines is found to be similar, with the [CI] slightly more extended, and both are enveloped in extensive HI. Spectral line ratios per voxel in the data cubes are found to be similar across the entire extent of the Galaxy. However, toward the edges of the molecular clouds the [CI]/ CO 13 and CO 12 / CO 13 line ratios rise by ∼50%, and the [CI]/HI ratio falls by ∼10%. We attribute this to these sightlines passing predominantly through the surfaces of photodissociation regions (PDRs), where the carbon is found mainly as C or C + , while the H 2 is mostly molecular, and the proportion of atomic gas also increases. We undertake modeling of the PDR emission from low density molecular clouds excited by average interstellar radiation fields and cosmic-ray ionization to quantify this comparison, finding that depletion of sulfur and reduced PAH abundance is needed to match line fluxes and ratios. Roughly one-third of the molecular gas along the sightline is found to be associated with this surface region, where the carbon is largely not to be found in CO. Approximately 10% of the atomic hydrogen along the sightline is cold gas within PDRs.

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“…However, comparable quality data to that of low mass star formation is now becoming available. Major observational spectral line surveys in the millimetre regime are now being carried out of massive star forming regions across the galaxy, for example in NH3 (HOPS, Walsh et al 2011), CO (Burton et al 2013), CS (Jordan et al 2015), and multiple lines MALT90 (Jackson et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Scaled up low-mass star formation in massive star-forming cores in the G333 giant molecular cloud

Wiles

Redman

et al. 2016

Mon. Not. R. Astron. Soc.

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Three bright molecular line sources in G333 have recently been shown to exhibit signatures of infall. We describe a molecular line radiative transfer modelling process which is required to extract the infall signature from Mopra and Nanten2 data. The observed line profiles differ greatly between individual sources but are reproduced well by variations upon a common unified model where the outflow viewing angle is the most significant difference between the sources. The models and data together suggest that the observed properties of the high-mass star-forming regions such as infall, turbulence, and mass are consistent with scaled-up versions of the low-mass case with turbulent velocities that are supersonic and an order of magnitude larger than those found in low-mass star-forming regions. Using detailed radiative transfer modeling, we show that the G333 cores are essentially undergoing a scaled-up version of low mass star formation. This is an extension of earlier work in that the degree of infall and the chemical abundances are constrained by the RT modeling in a way that is not practical with a standard analysis of observational data. We also find high velocity infall and high infall mass rates, possibly suggesting accelerated collapse due to external pressure. Molecular depletion due to freeze-out onto dust grains in central regions of the cores is suggested by low molecular abundances of several species. Strong evidence for a local enhancement of 13 C-bearing species towards the outflow cloud cores is discussed, consistent with the presence of shocks caused by the supersonic motions within them.

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The Mopra Southern Galactic Plane CO Survey

Cited by 84 publications

References 61 publications

Supernova Remnants Interacting with Molecular Clouds: X-Ray and Gamma-Ray Signatures

Supernova Remnants Interacting with Molecular Clouds: X-Ray and Gamma-Ray Signatures

Extended Carbon Line Emission in the Galaxy: Searching for Dark Molecular Gas Along the G328 Sightline

Scaled up low-mass star formation in massive star-forming cores in the G333 giant molecular cloud

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