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A WFC3 study of globular clusters in NGC 4150: An early-type minor merger

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A WFC3 study of globular clusters in NGC 4150 : An early-type minor merger. / Kaviraj, S.; Mark Crockett, R.; Silk, J.; Whitmore, B.C.; Mutchler, M.; O'Connell, R.W.; Windhorst, R.A.; Rejkuba, M.; Yi, S.; Frogel, J.A.; Calzetti, D.

In: Monthly Notices of the Royal Astronomical Society: Letters, Vol. 422, No. 1, 01.05.2012, p. L96-L100.

Research output: Contribution to journalArticle

Harvard

Kaviraj, S, Mark Crockett, R, Silk, J, Whitmore, BC, Mutchler, M, O'Connell, RW, Windhorst, RA, Rejkuba, M, Yi, S, Frogel, JA & Calzetti, D 2012, 'A WFC3 study of globular clusters in NGC 4150: An early-type minor merger', Monthly Notices of the Royal Astronomical Society: Letters, vol. 422, no. 1, pp. L96-L100. https://doi.org/10.1111/j.1745-3933.2012.01246.x

APA

Kaviraj, S., Mark Crockett, R., Silk, J., Whitmore, B. C., Mutchler, M., O'Connell, R. W., ... Calzetti, D. (2012). A WFC3 study of globular clusters in NGC 4150: An early-type minor merger. Monthly Notices of the Royal Astronomical Society: Letters, 422(1), L96-L100. https://doi.org/10.1111/j.1745-3933.2012.01246.x

Vancouver

Author

Kaviraj, S. ; Mark Crockett, R. ; Silk, J. ; Whitmore, B.C. ; Mutchler, M. ; O'Connell, R.W. ; Windhorst, R.A. ; Rejkuba, M. ; Yi, S. ; Frogel, J.A. ; Calzetti, D. / A WFC3 study of globular clusters in NGC 4150 : An early-type minor merger. In: Monthly Notices of the Royal Astronomical Society: Letters. 2012 ; Vol. 422, No. 1. pp. L96-L100.

Bibtex

@article{b00af0cd509440cabf5b6506286048da,
title = "A WFC3 study of globular clusters in NGC 4150: An early-type minor merger",
abstract = "We combine near-ultraviolet (NUV; 2250 {\AA}) and optical (U, B, V, I) imaging from the Wide Field Camera 3 (WFC3), on-board the Hubble Space Telescope (HST), to study the globular cluster (GC) population in NGC 4150, a sub-L* (M ~-18.48 mag) early-type minor-merger remnant in the Coma I cloud. We use broad-band NUV-optical photometry from the WFC3 to estimate individual ages, metallicities, masses and line-of-sight extinctions [E(B - V)] for 63 bright (M <-5 mag) GCs in this galaxy. In addition to a small GC population with ages greater than 10 Gyr, we find a dominant population of clusters with ages centred around 6 Gyr, consistent with the expected peak of stellar mass assembly in faint early types residing in lowdensity environments. The old and intermediate-age GCs in NGC 4150 are metal poor, with metallicities less than 0.1 Z, and reside in regions of low extinction [E(B - V) <0.05 mag]. We also find a population of young, metal-rich (Z > 0.3 Z) clusters that have formed within the last Gyr and reside in relatively dusty [E(B - V) > 0.3 mag] regions that are coincident with the part of the galaxy core that hosts significant recent star formation. Cluster disruption models (in which ~80-90 per cent of objects younger than a few ×10 yr dissolve every dex in time) suggest that the bulk of these young clusters are a transient population.",
author = "S. Kaviraj and {Mark Crockett}, R. and J. Silk and B.C. Whitmore and M. Mutchler and R.W. O'Connell and R.A. Windhorst and M. Rejkuba and S. Yi and J.A. Frogel and D. Calzetti",
year = "2012",
month = "5",
day = "1",
doi = "10.1111/j.1745-3933.2012.01246.x",
language = "English",
volume = "422",
pages = "L96--L100",
journal = "Monthly Notices of the Royal Astronomical Society: Letters",
issn = "1745-3925",
publisher = "Oxford University Press",
number = "1",

}

RIS

TY - JOUR

T1 - A WFC3 study of globular clusters in NGC 4150

T2 - An early-type minor merger

AU - Kaviraj, S.

AU - Mark Crockett, R.

AU - Silk, J.

AU - Whitmore, B.C.

AU - Mutchler, M.

AU - O'Connell, R.W.

AU - Windhorst, R.A.

AU - Rejkuba, M.

AU - Yi, S.

AU - Frogel, J.A.

AU - Calzetti, D.

PY - 2012/5/1

Y1 - 2012/5/1

N2 - We combine near-ultraviolet (NUV; 2250 Å) and optical (U, B, V, I) imaging from the Wide Field Camera 3 (WFC3), on-board the Hubble Space Telescope (HST), to study the globular cluster (GC) population in NGC 4150, a sub-L* (M ~-18.48 mag) early-type minor-merger remnant in the Coma I cloud. We use broad-band NUV-optical photometry from the WFC3 to estimate individual ages, metallicities, masses and line-of-sight extinctions [E(B - V)] for 63 bright (M <-5 mag) GCs in this galaxy. In addition to a small GC population with ages greater than 10 Gyr, we find a dominant population of clusters with ages centred around 6 Gyr, consistent with the expected peak of stellar mass assembly in faint early types residing in lowdensity environments. The old and intermediate-age GCs in NGC 4150 are metal poor, with metallicities less than 0.1 Z, and reside in regions of low extinction [E(B - V) <0.05 mag]. We also find a population of young, metal-rich (Z > 0.3 Z) clusters that have formed within the last Gyr and reside in relatively dusty [E(B - V) > 0.3 mag] regions that are coincident with the part of the galaxy core that hosts significant recent star formation. Cluster disruption models (in which ~80-90 per cent of objects younger than a few ×10 yr dissolve every dex in time) suggest that the bulk of these young clusters are a transient population.

AB - We combine near-ultraviolet (NUV; 2250 Å) and optical (U, B, V, I) imaging from the Wide Field Camera 3 (WFC3), on-board the Hubble Space Telescope (HST), to study the globular cluster (GC) population in NGC 4150, a sub-L* (M ~-18.48 mag) early-type minor-merger remnant in the Coma I cloud. We use broad-band NUV-optical photometry from the WFC3 to estimate individual ages, metallicities, masses and line-of-sight extinctions [E(B - V)] for 63 bright (M <-5 mag) GCs in this galaxy. In addition to a small GC population with ages greater than 10 Gyr, we find a dominant population of clusters with ages centred around 6 Gyr, consistent with the expected peak of stellar mass assembly in faint early types residing in lowdensity environments. The old and intermediate-age GCs in NGC 4150 are metal poor, with metallicities less than 0.1 Z, and reside in regions of low extinction [E(B - V) <0.05 mag]. We also find a population of young, metal-rich (Z > 0.3 Z) clusters that have formed within the last Gyr and reside in relatively dusty [E(B - V) > 0.3 mag] regions that are coincident with the part of the galaxy core that hosts significant recent star formation. Cluster disruption models (in which ~80-90 per cent of objects younger than a few ×10 yr dissolve every dex in time) suggest that the bulk of these young clusters are a transient population.

UR - http://www.scopus.com/inward/record.url?scp=84868100568&partnerID=8YFLogxK

U2 - 10.1111/j.1745-3933.2012.01246.x

DO - 10.1111/j.1745-3933.2012.01246.x

M3 - Article

AN - SCOPUS:84868100568

VL - 422

SP - L96-L100

JO - Monthly Notices of the Royal Astronomical Society: Letters

JF - Monthly Notices of the Royal Astronomical Society: Letters

SN - 1745-3925

IS - 1

ER -