dc.contributor.author | Calzetti, D | |
dc.contributor.author | Lee, JC | |
dc.contributor.author | Sabbi, E | |
dc.contributor.author | Adamo, A | |
dc.contributor.author | Smith, LJ | |
dc.contributor.author | Andrews, JE | |
dc.contributor.author | Ubeda, L | |
dc.contributor.author | Bright, SN | |
dc.contributor.author | Thilker, D | |
dc.contributor.author | Aloisi, A | |
dc.contributor.author | Brown, TM | |
dc.contributor.author | Chandar, R | |
dc.contributor.author | Christian, C | |
dc.contributor.author | Cignoni, M | |
dc.contributor.author | Clayton, GC | |
dc.contributor.author | Da Silva, R | |
dc.contributor.author | De Mink, SE | |
dc.contributor.author | Dobbs, C | |
dc.contributor.author | Elmegreen, BG | |
dc.contributor.author | Elmegreen, DM | |
dc.contributor.author | Evans, AS | |
dc.contributor.author | Fumagalli, M | |
dc.contributor.author | Gallagher, JS | |
dc.contributor.author | Gouliermis, DA | |
dc.contributor.author | Grebel, EK | |
dc.contributor.author | Herrero, A | |
dc.contributor.author | Hunter, DA | |
dc.contributor.author | Johnson, KE | |
dc.contributor.author | Kennicutt, RC | |
dc.contributor.author | Kim, H | |
dc.contributor.author | Krumholz, MR | |
dc.contributor.author | Lennon, D | |
dc.contributor.author | Levay, K | |
dc.contributor.author | Martin, C | |
dc.contributor.author | Nair, P | |
dc.contributor.author | Nota, A | |
dc.contributor.author | Östlin, G | |
dc.contributor.author | Pellerin, A | |
dc.contributor.author | Prieto, J | |
dc.contributor.author | Regan, MW | |
dc.contributor.author | Ryon, JE | |
dc.contributor.author | Schaerer, D | |
dc.contributor.author | Schiminovich, D | |
dc.contributor.author | Tosi, M | |
dc.contributor.author | Van Dyk, SD | |
dc.contributor.author | Walterbos, R | |
dc.contributor.author | Whitmore, BC | |
dc.contributor.author | Wofford, A | |
dc.date.accessioned | 2016-06-08T13:46:45Z | |
dc.date.issued | 2015-02-01 | |
dc.description.abstract | The American Astronomical Society. All rights reserved. The Legacy ExtraGalactic UV Survey (LEGUS) is a Cycle 21 Treasury program on the Hubble Space Telescope aimed at the investigation of star formation and its relation with galactic environment in nearby galaxies, from the scales of individual stars to those of ∼kiloparsec-size clustered structures. Five-band imaging from the nearultraviolet to the I band with the Wide-Field Camera 3 (WFC3), plus parallel optical imaging with the Advanced Camera for Surveys (ACS), is being collected for selected pointings of 50 galaxies within the local 12 Mpc. The filters used for the observations with the WFC3 are F275W (λ2704 A˚), F336W(λ3355 A˚), F438W(λ4325 A˚), F555W(λ5308 A˚), and F814W(ë8024 A˚); the parallel observations with the ACS use the filters F435W (λ4328 A˚), F606W(λ5921 A˚), and F814W(λ8057 A˚). The multiband images are yielding accurate recent (≲50 Myr) star formation histories from resolved massive stars and the extinction-corrected ages and masses of star clusters and associations. The extensive inventories of massive stars and clustered systems will be used to investigate the spatial and temporal evolution of star formation within galaxies. This will, in turn, inform theories of galaxy evolution and improve the understanding of the physical underpinning of the gas-star formation relation and the nature of star formation at high redshift. This paper describes the survey, its goals and observational strategy, and the initial scientific results. Because LEGUS will provide a reference survey and a foundation for future observations with the James Webb Space Telescope and with ALMA, a large number of data products are planned for delivery to the community. | en_GB |
dc.description.sponsorship | Based on observations made with the NASA/ESA Hubble
Space Telescope, obtained at the Space Telescope Science
Institute, which is operated by the Association of Universities
for Research in Astronomy, under NASA Contract NAS
5–26555. These observations are associated with Program
13364. Support for Program 13364 was provided by NASA
through a grant from the Space Telescope Science Institute.
This research has made use of the NASA/IPAC Extragalactic
Database (NED), which is operated by the Jet Propulsion
Laboratory, California Institute of Technology, under contract
with the National Aeronautics and Space Administration.
S.d.M. acknowledges support for this work by NASA
through Einstein Fellowship grant PF3-140105. C.L.D.
acknowledges funding from the European Research Council
for the FP7 ERC starting grant project, LOCALSTAR. D.A.G.
kindly acknowledges financial support by the German
Research Foundation through grant GO 1659/3-1. A.H.
acknowledges support by the Spanish MINECO under Project
Grant AYA2012-39364-C02-1. J.E.R. gratefully acknowledges
the support of the National Space Grant College and
Figure 6. Hierarchical structures traced by the UV-bright stars in NGC
6503 are shown on a three-color image (UV, B, I) of the galaxy. The UVbright
population has been selected from the CMD of the galaxy, using the
region delimited by −2 ⩽ NUV−U ⩽ 2 mag and brighter than
absolute magnitude MNUV −2.5 mag. The four-color contours (blue, cyan,
green, and yellow, in order of increasing physical scale, separated by a factor of
2 in smoothing kernel FWHM) delimit regions having significant difference in
the smoothed surface density of the UV-bright stars between one scale and the
next. The largest regions have sizes ∼700 pc. Our method links together any
spatially associated overdensities detected at arbitrary scale into composite
hierarchical structures. The field of view of the image is ∼3.3 kpc × 1.6 kpc.
Figure 7. Two-point angular correlation function of the young stars (<100
Myr; blue line) and old stars (>500 Myr; red line) for the whole extent of NGC
6503. The horizontal gray dotted line is the expected two-point angular
correlation function of a randomly distributed population. The monotonically
decreasing functions imply that the stellar distributions follow a hierarchical
pattern, with the young stars more strongly clustered than the old stars across
galactic scales up to projected sizes of at least 100″ (equivalent to ∼2.75 kpc).
21
The Astronomical Journal, 149:51 (25pp), 2015 February Calzetti et al.
Fellowship Program and the Wisconsin Space Grant Consortium.
A.W. acknowledges funding from the European
Research Council under the European Communityʼs Seventh
Framework Programme (FP7/2007-2013 Grant Agreement
321323). | en_GB |
dc.identifier.citation | Vol. 149:51 | en_GB |
dc.identifier.doi | 10.1088/0004-6256/149/2/51 | |
dc.identifier.uri | http://hdl.handle.net/10871/21926 | |
dc.language.iso | en | en_GB |
dc.publisher | American Astronomical Society | en_GB |
dc.subject | galaxies | en_GB |
dc.subject | star clusters | en_GB |
dc.subject | star formation | en_GB |
dc.subject | stellar content | en_GB |
dc.subject | ultraviolet | en_GB |
dc.subject | stars | en_GB |
dc.title | Legacy extragalactic UV survey (LEGUS) with the hubble space telescope. I. Survey description | en_GB |
dc.type | Article | en_GB |
dc.date.available | 2016-06-08T13:46:45Z | |
dc.identifier.issn | 0004-6256 | |
dc.description | This is the final version of the article. Available from the publisher via the DOI in this record. | en_GB |
dc.identifier.journal | Astronomical Journal | en_GB |