Advanced camera for surveys observations of young star clusters in the interacting galaxy UGC 10214

H. D. Tran, M. Sirianni, H. C. Ford, G. D. Illingworth, M. Clampin, G. Hartig, R. H. Becker, R. L. White, F. Bartko, N. Benítez, J. P. Blakeslee, R. Bouwens, T. J. Broadhurst, R. Brown, C. Burrows, E. Cheng, N. Cross, P. D. Feldman, M. Franx, D. A. Golimowski & 14 others C. Gronwall, L. Infante, R. A. Kimble, J. Krist, M. Lesser, D. Magee, A. R. Martel, Wm J. McCann, G. R. Meurer, G. Miley, M. Postman, P. Rosati, W. B. Sparks, Z. Tsvetanov

Research output: Contribution to journalArticle

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Abstract

We present the first Advanced Camera for Surveys (ACS) observations of young star clusters in the colliding/merging galaxy UGC 10214. The observations were made as part of the Early Release Observation (ERO) program for the newly installed ACS during service mission SM3B for the Hubble Space Telescope (HST). Many young star clusters can be identified in the tails of UGC 10214, with ages ranging from ∼3 to 10 Myr. The extreme blue V-I(F606W-F814W) colors of the star clusters found in the tail of UGC 10214 can only be explained if strong emission lines are included with a young stellar population. This has been confirmed by our Keck spectroscopy of some of these bright blue stellar knots. The most luminous and largest of these blue knots has an absolute magnitude of Mv = - 14.45, with a half-light radius of 161 pc, and if it is a single star cluster, it would qualify as a super star cluster (SSC). Alternatively, it could be a superposition of multiple scaled OB associations or clusters. With an estimated age of ∼4-5 Myr, its derived mass is less than 1.3 × 106 M. Thus, the young stellar knot is unbound and will not evolve into a normal globular cluster. The bright blue clusters and associations are much younger than the dynamical age of the tail, providing strong evidence that star formation occurs in the tail long after it was ejected. UGC 10214 provides a nearby example of processes that contributed to the formation of halos and intracluster media in the distant and younger universe.

Original languageEnglish
Pages (from-to)750-755
Number of pages6
JournalAstrophysical Journal
Volume585
Issue number2 I
DOIs
Publication statusPublished - 10 Mar 2003
Externally publishedYes

Fingerprint

interacting galaxies
star clusters
cameras
young population
globular clusters
Hubble Space Telescope
star formation
halos
universe
spectroscopy
young
galaxies
color
radii

Keywords

  • Galaxies: individual (Arp 188, UGC 10214, VV 29)
  • Galaxies: star clusters

ASJC Scopus subject areas

  • Space and Planetary Science
  • Nuclear and High Energy Physics

Cite this

Tran, H. D., Sirianni, M., Ford, H. C., Illingworth, G. D., Clampin, M., Hartig, G., ... Tsvetanov, Z. (2003). Advanced camera for surveys observations of young star clusters in the interacting galaxy UGC 10214. Astrophysical Journal, 585(2 I), 750-755. https://doi.org/10.1086/346125

Advanced camera for surveys observations of young star clusters in the interacting galaxy UGC 10214. / Tran, H. D.; Sirianni, M.; Ford, H. C.; Illingworth, G. D.; Clampin, M.; Hartig, G.; Becker, R. H.; White, R. L.; Bartko, F.; Benítez, N.; Blakeslee, J. P.; Bouwens, R.; Broadhurst, T. J.; Brown, R.; Burrows, C.; Cheng, E.; Cross, N.; Feldman, P. D.; Franx, M.; Golimowski, D. A.; Gronwall, C.; Infante, L.; Kimble, R. A.; Krist, J.; Lesser, M.; Magee, D.; Martel, A. R.; McCann, Wm J.; Meurer, G. R.; Miley, G.; Postman, M.; Rosati, P.; Sparks, W. B.; Tsvetanov, Z.

In: Astrophysical Journal, Vol. 585, No. 2 I, 10.03.2003, p. 750-755.

Research output: Contribution to journalArticle

Tran, HD, Sirianni, M, Ford, HC, Illingworth, GD, Clampin, M, Hartig, G, Becker, RH, White, RL, Bartko, F, Benítez, N, Blakeslee, JP, Bouwens, R, Broadhurst, TJ, Brown, R, Burrows, C, Cheng, E, Cross, N, Feldman, PD, Franx, M, Golimowski, DA, Gronwall, C, Infante, L, Kimble, RA, Krist, J, Lesser, M, Magee, D, Martel, AR, McCann, WJ, Meurer, GR, Miley, G, Postman, M, Rosati, P, Sparks, WB & Tsvetanov, Z 2003, 'Advanced camera for surveys observations of young star clusters in the interacting galaxy UGC 10214', Astrophysical Journal, vol. 585, no. 2 I, pp. 750-755. https://doi.org/10.1086/346125
Tran HD, Sirianni M, Ford HC, Illingworth GD, Clampin M, Hartig G et al. Advanced camera for surveys observations of young star clusters in the interacting galaxy UGC 10214. Astrophysical Journal. 2003 Mar 10;585(2 I):750-755. https://doi.org/10.1086/346125
Tran, H. D. ; Sirianni, M. ; Ford, H. C. ; Illingworth, G. D. ; Clampin, M. ; Hartig, G. ; Becker, R. H. ; White, R. L. ; Bartko, F. ; Benítez, N. ; Blakeslee, J. P. ; Bouwens, R. ; Broadhurst, T. J. ; Brown, R. ; Burrows, C. ; Cheng, E. ; Cross, N. ; Feldman, P. D. ; Franx, M. ; Golimowski, D. A. ; Gronwall, C. ; Infante, L. ; Kimble, R. A. ; Krist, J. ; Lesser, M. ; Magee, D. ; Martel, A. R. ; McCann, Wm J. ; Meurer, G. R. ; Miley, G. ; Postman, M. ; Rosati, P. ; Sparks, W. B. ; Tsvetanov, Z. / Advanced camera for surveys observations of young star clusters in the interacting galaxy UGC 10214. In: Astrophysical Journal. 2003 ; Vol. 585, No. 2 I. pp. 750-755.
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abstract = "We present the first Advanced Camera for Surveys (ACS) observations of young star clusters in the colliding/merging galaxy UGC 10214. The observations were made as part of the Early Release Observation (ERO) program for the newly installed ACS during service mission SM3B for the Hubble Space Telescope (HST). Many young star clusters can be identified in the tails of UGC 10214, with ages ranging from ∼3 to 10 Myr. The extreme blue V-I(F606W-F814W) colors of the star clusters found in the tail of UGC 10214 can only be explained if strong emission lines are included with a young stellar population. This has been confirmed by our Keck spectroscopy of some of these bright blue stellar knots. The most luminous and largest of these blue knots has an absolute magnitude of Mv = - 14.45, with a half-light radius of 161 pc, and if it is a single star cluster, it would qualify as a super star cluster (SSC). Alternatively, it could be a superposition of multiple scaled OB associations or clusters. With an estimated age of ∼4-5 Myr, its derived mass is less than 1.3 × 106 M⊙. Thus, the young stellar knot is unbound and will not evolve into a normal globular cluster. The bright blue clusters and associations are much younger than the dynamical age of the tail, providing strong evidence that star formation occurs in the tail long after it was ejected. UGC 10214 provides a nearby example of processes that contributed to the formation of halos and intracluster media in the distant and younger universe.",
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T1 - Advanced camera for surveys observations of young star clusters in the interacting galaxy UGC 10214

AU - Tran, H. D.

AU - Sirianni, M.

AU - Ford, H. C.

AU - Illingworth, G. D.

AU - Clampin, M.

AU - Hartig, G.

AU - Becker, R. H.

AU - White, R. L.

AU - Bartko, F.

AU - Benítez, N.

AU - Blakeslee, J. P.

AU - Bouwens, R.

AU - Broadhurst, T. J.

AU - Brown, R.

AU - Burrows, C.

AU - Cheng, E.

AU - Cross, N.

AU - Feldman, P. D.

AU - Franx, M.

AU - Golimowski, D. A.

AU - Gronwall, C.

AU - Infante, L.

AU - Kimble, R. A.

AU - Krist, J.

AU - Lesser, M.

AU - Magee, D.

AU - Martel, A. R.

AU - McCann, Wm J.

AU - Meurer, G. R.

AU - Miley, G.

AU - Postman, M.

AU - Rosati, P.

AU - Sparks, W. B.

AU - Tsvetanov, Z.

PY - 2003/3/10

Y1 - 2003/3/10

N2 - We present the first Advanced Camera for Surveys (ACS) observations of young star clusters in the colliding/merging galaxy UGC 10214. The observations were made as part of the Early Release Observation (ERO) program for the newly installed ACS during service mission SM3B for the Hubble Space Telescope (HST). Many young star clusters can be identified in the tails of UGC 10214, with ages ranging from ∼3 to 10 Myr. The extreme blue V-I(F606W-F814W) colors of the star clusters found in the tail of UGC 10214 can only be explained if strong emission lines are included with a young stellar population. This has been confirmed by our Keck spectroscopy of some of these bright blue stellar knots. The most luminous and largest of these blue knots has an absolute magnitude of Mv = - 14.45, with a half-light radius of 161 pc, and if it is a single star cluster, it would qualify as a super star cluster (SSC). Alternatively, it could be a superposition of multiple scaled OB associations or clusters. With an estimated age of ∼4-5 Myr, its derived mass is less than 1.3 × 106 M⊙. Thus, the young stellar knot is unbound and will not evolve into a normal globular cluster. The bright blue clusters and associations are much younger than the dynamical age of the tail, providing strong evidence that star formation occurs in the tail long after it was ejected. UGC 10214 provides a nearby example of processes that contributed to the formation of halos and intracluster media in the distant and younger universe.

AB - We present the first Advanced Camera for Surveys (ACS) observations of young star clusters in the colliding/merging galaxy UGC 10214. The observations were made as part of the Early Release Observation (ERO) program for the newly installed ACS during service mission SM3B for the Hubble Space Telescope (HST). Many young star clusters can be identified in the tails of UGC 10214, with ages ranging from ∼3 to 10 Myr. The extreme blue V-I(F606W-F814W) colors of the star clusters found in the tail of UGC 10214 can only be explained if strong emission lines are included with a young stellar population. This has been confirmed by our Keck spectroscopy of some of these bright blue stellar knots. The most luminous and largest of these blue knots has an absolute magnitude of Mv = - 14.45, with a half-light radius of 161 pc, and if it is a single star cluster, it would qualify as a super star cluster (SSC). Alternatively, it could be a superposition of multiple scaled OB associations or clusters. With an estimated age of ∼4-5 Myr, its derived mass is less than 1.3 × 106 M⊙. Thus, the young stellar knot is unbound and will not evolve into a normal globular cluster. The bright blue clusters and associations are much younger than the dynamical age of the tail, providing strong evidence that star formation occurs in the tail long after it was ejected. UGC 10214 provides a nearby example of processes that contributed to the formation of halos and intracluster media in the distant and younger universe.

KW - Galaxies: individual (Arp 188, UGC 10214, VV 29)

KW - Galaxies: star clusters

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