LEGACY EXTRAGALACTIC UV SURVEY (LEGUS) WITH THE<i>HUBBLE SPACE TELESCOPE</i>. I. SURVEY DESCRIPTION

Calzetti, Daniela; Lee, Janice; Sabbi, E.; Adamo, Angela; Smith, L. J.; Andrews, Jennifer E.; Úbeda, Leonardo; Bright, Stacey N.; Thilker, David A.; Aloisi, Alessandra; Brown, Thomas M.; Chandar, Rupali; Christian, C. A.; Cignoni, M.; Clayton, Geoffrey C.; Silva, R. da; Mink, S. E. de; Dobbs, Clare; Elmegreen, Bruce G.; Elmegreen, D. M.; Evans, A. S.; Fumagalli, Michele; Gallagher, John S.; Gouliermis, D. A.; Grebel, Eva K.; Herrero, A.; Hunter, Deidre A.; Johnson, K. E.; Kennicutt, Robert C.; Kim, Hwi; Krumholz, Mark R.; Lennon, D. J.; Levay, K.; Martin, Christopher; Nair, Preethi; Nota, A.; Östlin, Göran; Pellerin, Anne; Prieto, J. L.; Regan, Michael W.; Ryon, J. E.; Schaerer, D.; Schiminovich, David; Tosi, M.; Dyk, Schuyler D. Van; Walterbos, R. A. M.; Whitmore, Bradley C.; Wofford, Aida

doi:10.1088/0004-6256/149/2/51

Cited by 200 publications

(283 citation statements)

References 251 publications

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“…It is worth noting, however, that some of the galaxies presented in also do not make the distinction between bound and unbound aggregates, though several make age cuts to remove young clusters that likely cause contamination of unbound sources. This lack of uniformity is addressed by the LEGUS survey (Calzetti et al 2015).…”

Section: Results and Limitationsmentioning

confidence: 99%

“…The galaxy is part of the Legacy ExtraGalactic UV Survey (LEGUS, Calzetti et al (2015), HST project number GO-13364) and as such has complete and homogeneous imaging coverage in the UV (F275W), U (F336W), B (F438W), V (F555W) and I (F814W) bands obtained using WFC3. No conversion was made to the Cousins-Johnson filter system, but the central wavelengths of these bands are approximately equal to the WFC3 bands, so we use this nomenclature for simplicity.…”

Section: Data and Photometrymentioning

confidence: 99%

“…Furthermore, UV emission is associated with massive stars within clusters, and so is more reliably representative of the cluster. The potential for using UV to disentangle degeneracies in age dating of clusters is a key aspect of the LEGUS survey (Calzetti et al 2015).…”

Section: Age and Mass Fittingmentioning

confidence: 99%

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Properties of the cluster population of NGC 1566 and their implications

Hollyhead

Adamo

Bastian

et al. 2016

Mon. Not. R. Astron. Soc.

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We present results of a photometric study into the cluster population of NGC 1566, a nearby grand design spiral galaxy, sampled out to a Galactocentric radius of ≈ 5.5 kpc. The shape of the mass-limited age distribution shows negligible variation with radial distance from the centre of the galaxy, and demonstrates three separate sections, with a steep beginning, flat middle and steep end. The luminosity function can be approximated by a power law at lower luminosities with evidence of a truncation at higher luminosity. The power law section of the luminosity function of the galaxy is best fitted by an index ≈ −2, in agreement with other studies, and is found to agree with a model luminosity function, which uses an underlying Schechter mass function. The recovered power law slope of the mass distribution shows a slight steepening as a function of galactocentric distance, but this is within error estimates. It also displays a possible truncation at the high mass end. Additionally, the cluster formation efficiency (Γ) and the specific U-band luminosity of clusters (T L (U )) are calculated for NGC 1566 and are consistent with values for similar galaxies. A difference in NGC 1566, however, is that the fairly high star formation rate is in contrast with a low Σ SF R and Γ, indicating that Γ can only be said to depend strongly on Σ SF R , not the star formation rate.

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Section: Results and Limitationsmentioning

confidence: 99%

Section: Data and Photometrymentioning

confidence: 99%

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Properties of the cluster population of NGC 1566 and their implications

Hollyhead

Adamo

Bastian

et al. 2016

Mon. Not. R. Astron. Soc.

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“…High resolution, sensitivity and wide-area coverage are critical for the identification of stars and stellar systems at various length-scales in galaxies in the extended Milky Way neighbourhood, and the Hubble Space Telescope (HST) with its unique UV-sensitivity, is the only telescope that meets all three requirements. In light of these requirements, in the HST Legacy ExtraGalactic UV Survey 1 (LEGUS; Calzetti et al 2015) we performed panchromatic imaging of 50 star-forming Local Volume galaxies. The program focuses on the investigation of star formation and its relation with galactic environment.…”

Section: Introductionmentioning

confidence: 99%

Hierarchical star formation across the grand-design spiral NGC 1566

Gouliermis

Elmegreen²,

Elmegreen

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We investigate how star formation is spatially organized in the grand-design spiral NGC 1566 from deep HST photometry with the Legacy ExtraGalactic UV Survey (LEGUS). Our contour-based clustering analysis reveals 890 distinct stellar conglomerations at various levels of significance. These star-forming complexes are organized in a hierarchical fashion with the larger congregations consisting of smaller structures, which themselves fragment into even smaller and more compact stellar groupings. Their size distribution, covering a wide range in length-scales, shows a power-law as expected from scale-free processes. We explain this shape with a simple "fragmentation and enrichment" model. The hierarchical morphology of the complexes is confirmed by their mass-size relation which can be represented by a powerlaw with a fractional exponent, analogous to that determined for fractal molecular clouds. The surface stellar density distribution of the complexes shows a log-normal shape similar to that for supersonic non-gravitating turbulent gas. Between 50 and 65 per cent of the recentlyformed stars, as well as about 90 per cent of the young star clusters, are found inside the stellar complexes, located along the spiral arms. We find an age-difference between young stars inside the complexes and those in their direct vicinity in the arms of at least 10 Myr. This timescale may relate to the minimum time for stellar evaporation, although we cannot exclude the in situ formation of stars. As expected, star formation preferentially occurs in spiral arms. Our findings reveal turbulent-driven hierarchical star formation along the arms of a grand-design galaxy.

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“…We assess the quality of our catalog by comparing with a catalog of clusters selected manually from more recent HST/ WFC3 images of M51, which were taken as part of the LEGUS project (Calzetti et al 2015). Overall, the cluster catalogs match fairly well at the bright end, but some differences emerge at the faint end.…”

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confidence: 99%

The Age, Mass, and Size Distributions of Star Clusters in M51

Chandar

Whitmore

DiNino

et al. 2016

ApJ

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We present a new catalog of 3816 compact star clusters in the grand design spiral galaxy M51 based on observations taken with the Hubble Space Telescope. The age distribution of the clusters declines starting at very young ages, and can be represented by a power law,, with g = - 0.65 0.15. No significant changes in the shape of the age distribution at different masses is observed. The mass function of the clusters younger than t » 400 Myr can also be described by a power law, µ b dN dM M , with b » - 2.1 0.2. We compare these distributions with the predictions from various cluster disruption models, and find that they are consistent with models where clusters disrupt approximately independent of their initial mass, but not with models where lower mass clusters are disrupted earlier than their higher mass counterparts. We find that the half-light radii of clusters more massive than »´ M M 3 10 4and with ages between 100 and 400 Myr are larger by a factor of ≈3-4 than their counterparts that are younger than 10 7 years old, suggesting that the clusters physically expand during their early life.

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LEGACY EXTRAGALACTIC UV SURVEY (LEGUS) WITH THEHUBBLE SPACE TELESCOPE. I. SURVEY DESCRIPTION

Cited by 200 publications

References 251 publications

Properties of the cluster population of NGC 1566 and their implications

Properties of the cluster population of NGC 1566 and their implications

Hierarchical star formation across the grand-design spiral NGC 1566

The Age, Mass, and Size Distributions of Star Clusters in M51

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