@article {2014A\&A...572A..38G,
	title = {{Nearby supernova host galaxies from the CALIFA Survey. I. Sample, data analysis, and correlation to star-forming regions}},
	journal = {Astronomy and Astrophysics},
	volume = {572},
	year = {2014},
	month = {dec},
	pages = {A38},
	abstract = {We use optical integral field spectroscopy (IFS) of nearby supernova (SN) host galaxies (0.005 {\l}t}z{\l}t} 0.03) provided by the Calar Alto Legacy Integral Field Area (CALIFA) Survey with the goal of finding correlations in the environmental parameters at the location of different SN types. In this first study of a series we focus on the properties related with star formation (SF). We recover the sequence in association of different SN types to the star-forming regions by using several indicators of the ongoing and recent SF related to both the ionized gas and the stellar populations. While the total ongoing SF is on average the same for the three SN types, SNe Ibc/IIb tend to occur closer to star-forming regions and in higher SF density locations than SNe II and SNe Ia; the latter shows the weakest correlation. SNe Ia host galaxies have masses that are on average \~{}0.3-0.8 dex higher than those of the core collapse (CC) SNe hosts because the SNe Ia hosts contain alarger fraction of old stellar populations. Using the recent SN Ia delay-time distribution and the SFHs of the galaxies, we show that the SN Ia hosts in our sample are expected to produce twice as many SNe Ia as the CC SN hosts. Since both types occur in hosts with a similar SF rate and hence similar CC SN rate, this can explain the mass difference between the SN Ia and CC SN hosts, and reinforces the finding that at least part of the SNe Ia originate from very old progenitors. By comparing the mean SFH of the eight least massive galaxies with that of the massive SF SN Ia hosts, we find that the low-mass galaxies formed their stars during a longer time (0.65\%, 24.46\%, and 74.89\% in the intervals 0-0.42 Gyr, 0.42-2.4 Gyr, and {\gt}2.4 Gyr, respectively) than the massive SN Ia hosts (0.04\%, 2.01\%, and 97.95\% in these intervals). We estimate that the low-mass galaxies produce ten times fewer SNe Ia and three times fewer CC SNe than the high-mass group. Therefore the ratio between the number of CC SNe and SNe Ia is expected to increase with decreasing galaxy mass. CC SNe tend to explode at positions with younger stellar populations than the galaxy average, but the galaxy properties at SNe Ia locations are one average the same as the global galaxy properties. Tables 2, 3, 7-9 are only available in electronic form at <A href={\textquoteright}{\textquoteright}http://www.aanda.org/10.1051/0004-6361/201424717/olm{\textquoteright}{\textquoteright}>http://www.aanda.org</A>},
	keywords = {Galaxy: general, supernovae: general, techniques: spectroscopic},
	doi = {10.1051/0004-6361/201424717},
	url = {http://adsabs.harvard.edu/abs/2014A\%26A...572A..38G},
	author = {Galbany, L. and Stanishev, V. and Mour{\~a}o, A.~M. and Rodrigues, M. and Flores, H. and Garc{\'\i}a-Benito, R. and Mast, D. and Mendoza, M.~A. and S{\'a}nchez, S.~F. and Badenes, C. and Barrera-Ballesteros, J. and Bland-Hawthorn, J. and Falc{\'o}n-Barroso, J. and Garc{\'\i}a-Lorenzo, B. and Gomes, J.~M. and Gonz{\'a}lez Delgado, R.~M. and Kehrig, C. and Lyubenova, M. and L{\'o}pez-S{\'a}nchez, A.~R. and de Lorenzo-C{\'a}ceres, A. and Marino, R.~A. and Meidt, S. and Moll{\'a}, M. and Papaderos, P. and M. A. P{\'e}rez-Torres and Rosales-Ortega, F.~F. and van de Ven, G.}
}
@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.}
}
