@article {2013PASA...30....3D, title = {{GASKAP-The Galactic ASKAP Survey}}, journal = {Publications of the Astronomical Society of Australia}, volume = {30}, year = {2013}, month = {jan}, pages = {3}, abstract = {A survey of the Milky Way disk and the Magellanic System at the wavelengths of the 21-cm atomic hydrogen (HI) line and three 18-cm lines of the OH molecule will be carried out with the Australian Square Kilometre Array Pathfinder telescope. The survey will study the distribution of HI emission and absorption with unprecedented angular and velocity resolution, as well as molecular line thermal emission, absorption, and maser lines. The area to be covered includes the Galactic plane (|b| {\l}t} 10{\deg}) at all declinations south of {$δ$} = +40{\deg}, spanning longitudes 167{\deg} through 360{\deg}to 79{\deg} at b = 0{\deg}, plus the entire area of the Magellanic Stream and Clouds, a total of 13 020 deg$^{2}$. The brightness temperature sensitivity will be very good, typically {$\sigma$}$_{T}${\sime} 1 K at resolution 30 arcsec and 1 km s$^{-1}$. The survey has a wide spectrum of scientific goals, from studies of galaxy evolution to star formation, with particular contributions to understanding stellar wind kinematics, the thermal phases of the interstellar medium, the interaction between gas in the disk and halo, and the dynamical and thermal states of gas at various positions along the Magellanic Stream.}, keywords = {Galaxy: evolution, Galaxy: general, ISM: clouds, ISM: general, ISM: kinematics and dynamics, ISM: molecules}, doi = {10.1017/pasa.2012.003}, url = {http://adsabs.harvard.edu/abs/2013PASA...30....3D}, author = {Dickey, J.~M. and McClure-Griffiths, N. and Gibson, S.~J. and G{\'o}mez, J.~F. and Imai, H. and Jones, P. and Stanimirovi{\'c}, S. and Van Loon, J.~T. and Walsh, A. and Alberdi, A. and Anglada, G. and Uscanga, L. and Arce, H. and Bailey, M. and Begum, A. and Wakker, B. and Bekhti, N.~B. and Kalberla, P. and Winkel, B. and Bekki, K. and For, B.-Q. and Staveley-Smith, L. and Westmeier, T. and Burton, M. and Cunningham, M. and Dawson, J. and Ellingsen, S. and Diamond, P. and Green, J.~A. and Hill, A.~S. and Koribalski, B. and McConnell, D. and Rathborne, J. and Voronkov, M. and Douglas, K.~A. and English, J. and Ford, H.~A. and Lockman, F.~J. and Foster, T. and Gomez, Y. and Green, A. and Bland-Hawthorn, J. and Gulyaev, S. and Hoare, M. and Joncas, G. and Kang, J.-H. and Kerton, C.~R. and Koo, B.-C. and Leahy, D. and Lo, N. and Migenes, V. and Nakashima, J. and Zhang, Y. and Nidever, D. and Peek, J.~E.~G. and Tafoya, D. and Tian, W. and Wu, D.} } @article {2011A\&A...528A..30C, title = {{Molecules as tracers of galaxy evolution: an EMIR survey. I. Presentation of the data and first results}}, journal = {Astronomy and Astrophysics}, volume = {528}, year = {2011}, month = {apr}, pages = {A30}, abstract = {
Aims: We investigate the molecular gas properties of a sample of 23 galaxies in order to find and test chemical signatures of galaxy evolution and to compare them to IR evolutionary tracers.
Methods: Observation at 3 mm wavelengths were obtained with the EMIR broadband receiver, mounted on the IRAM 30 m telescope on Pico Veleta, Spain. We compare the emission of the main molecular species with existing models of chemical evolution by means of line intensity ratios diagrams and principal component analysis.
Results: We detect molecular emission in 19 galaxies in two 8 GHz-wide bands centred at 88 and 112 GHz. The main detected molecules are CO, $^{13}$CO, HCN, HNC, HCO$^{+}$, CN, and C$_{2}$H. We also detect HC$_{3}$N J = 10-9 in the galaxies IRAS 17208, IC 860, NGC 4418, NGC 7771, and NGC 1068. The only HC$_{3}$N detections are in objects with HCO$^{+}$/HCN {\l}t} 1. Galaxies with the highest HC$_{3}$N/HCN ratios have warm IRAS colours (60/100 {$μ$}m {\gt} 0.8). The brightest HC$_{3}$N emission is found in IC 860, where we also detect the molecule in its vibrationally excited state. We find low HNC/HCN line ratios ({\l}t}0.5), that cannot be explained by existing PDR or XDR chemical models. The intensities of HCO+ and HNC appear anti-correlated. No correlation is found between the HNC/HCN line ratio and dust temperature. All HNC-bright objects are either luminous IR galaxies (LIRG) or Seyferts. Galaxies with bright polycyclic aromatic hydrocarbons (PAH) emission show low HNC/HCO$^{+}$ ratios. The CO/$^{13}$CO ratio is positively correlated with the dust temperature and is generally higher than in our galaxy. The emission of CN and C$^{18}$O is correlated.
Conclusions: Bright HC$_{3}$N emission in HCO$^{+}$-faint objects may imply that these are not dominated by X-ray chemistry. Thus the HCN/HCO$^{+}$ line ratio is not, by itself, a reliable tracer of XDRs. Bright HC$_{3}$N and faint HCO$^{+}$ could be signatures of embedded star-formation, instead of AGN activity. Mechanical heating caused by supernova explosions may be responsible for the low HNC/HCN and high HCO$^{+}$/HCN ratios in some starbursts. We cannot exclude, however, that the discussed trends are largely caused by optical depth effects or excitation. Chemical models alone cannot explain all properties of the observed molecular emission. Better constraints to the gas spacial distribution and excitation are needed to distinguish abundance and excitation effects. Appendices are only available in electronic form http://www.aanda.org}, keywords = {evolution, galaxies: active, galaxies: evolution, galaxies: ISM, ISM: molecules}, doi = {10.1051/0004-6361/201015628}, url = {http://adsabs.harvard.edu/abs/2011A\%26A...528A..30C}, author = {F. Costagliola and Aalto, S. and M. Rodr{\'\i}guez and Muller, S. and Spoon, H.~W.~W. and Mart{\'\i}n, S. and M. A. P{\'e}rez-Torres and Alberdi, A. and Lindberg, J.~E. and Batejat, F. and J{\"u}tte, E. and van der Werf, P. and Lahuis, F.} }