The morphology-density relation in z ∼ 1 clusters

M. Postman, M. Franx, N. J G Cross, B. Holden, H. C. Ford, G. D. Illingworth, T. Goto, R. Demarco, P. Rosati, J. P. Blakeslee, K. V. Tran, N. Benitez, M. Clampin, G. F. Hartig, N. Homeier, D. R. Ardila, F. Bartko, R. J. Bouwens, L. D. Bradley, T. J. BroadhurstR. A. Brown, C. J. Burrows, E. S. Cheng, P. D. Feldman, D. A. Golimowski, C. Gronwall, L. Infante, R. A. Kimble, J. E. Krist, M. P. Lesser, A. R. Martel, S. Mei, F. Menanteau, G. R. Meurer, G. K. Miley, V. Motta, M. Sirianni, W. B. Sparks, H. D. Tran, Zlatan Tsvetanov, R. L. White, W. Zheng

Research output: Contribution to journalReview article

265 Citations (Scopus)

Abstract

We measure the morphology-density relation (MDR) and morphology-radius relation (MRR) for galaxies in seven z ∼ 1 clusters that have been observed with the Advanced Camera for Surveys (ACS) on board the Hubble Space Telescope. Simulations and independent comparisons of our visually derived morphologies indicate that ACS allows one to distinguish between E, S0, and spiral morphologies down to z8550 = 24, corresponding to L/L* = 0.21 and 0.30 at z = 0.83 and 1.24, respectively. We adopt density and radius estimation methods that match those used at lower redshift in order to study the evolution of the MDR and MRR. We detect a change in the MDR between 0.8 < z < 1.2 and that observed at z ∼ 0, consistent with recent work; specifically, the growth in the bulge-dominated galaxy fraction, f E+S0, with increasing density proceeds less rapidly at z ∼ 1 than it does at z ∼ 0. At z ∼ 1 and Σ ≥ 500 galaxies Mpc -2, we find 〈fE+S0〉 = 0-72 ± 0.10. At z ∼ 0, an E+S0 population fraction of this magnitude occurs at densities about 5 times smaller. The evolution in the MDR is confined to densities Σ ≳ 40 galaxies Mpc-2 and appears to be primarily due to a deficit of SO galaxies and an excess of Sp+Irr galaxies relative to the local galaxy population. Theye-density relation exhibits no significant evolution between z = 1 and 0. We find mild evidence to suggest that the MDR is dependent on the bolometric X-ray luminosity of the intracluster medium. Implications for the evolution of the disk galaxy population in dense regions are discussed in the context of these observations.

Original languageEnglish
Pages (from-to)721-741
Number of pages21
JournalAstrophysical Journal
Volume623
Issue number2 I
DOIs
Publication statusPublished - 20 Apr 2005
Externally publishedYes

Fingerprint

galaxies
radii
cameras
disk galaxies
estimation method
Hubble Space Telescope
luminosity
simulation
x rays

Keywords

  • Galaxies: clusters: general
  • Galaxies: evolution
  • Galaxies: formation
  • Galaxies: structure

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Postman, M., Franx, M., Cross, N. J. G., Holden, B., Ford, H. C., Illingworth, G. D., ... Zheng, W. (2005). The morphology-density relation in z ∼ 1 clusters. Astrophysical Journal, 623(2 I), 721-741. https://doi.org/10.1086/428881

The morphology-density relation in z ∼ 1 clusters. / Postman, M.; Franx, M.; Cross, N. J G; Holden, B.; Ford, H. C.; Illingworth, G. D.; Goto, T.; Demarco, R.; Rosati, P.; Blakeslee, J. P.; Tran, K. V.; Benitez, N.; Clampin, M.; Hartig, G. F.; Homeier, N.; Ardila, D. R.; Bartko, F.; Bouwens, R. J.; Bradley, L. D.; Broadhurst, T. J.; Brown, R. A.; Burrows, C. J.; Cheng, E. S.; Feldman, P. D.; Golimowski, D. A.; Gronwall, C.; Infante, L.; Kimble, R. A.; Krist, J. E.; Lesser, M. P.; Martel, A. R.; Mei, S.; Menanteau, F.; Meurer, G. R.; Miley, G. K.; Motta, V.; Sirianni, M.; Sparks, W. B.; Tran, H. D.; Tsvetanov, Zlatan; White, R. L.; Zheng, W.

In: Astrophysical Journal, Vol. 623, No. 2 I, 20.04.2005, p. 721-741.

Research output: Contribution to journalReview article

Postman, M, Franx, M, Cross, NJG, Holden, B, Ford, HC, Illingworth, GD, Goto, T, Demarco, R, Rosati, P, Blakeslee, JP, Tran, KV, Benitez, N, Clampin, M, Hartig, GF, Homeier, N, Ardila, DR, Bartko, F, Bouwens, RJ, Bradley, LD, Broadhurst, TJ, Brown, RA, Burrows, CJ, Cheng, ES, Feldman, PD, Golimowski, DA, Gronwall, C, Infante, L, Kimble, RA, Krist, JE, Lesser, MP, Martel, AR, Mei, S, Menanteau, F, Meurer, GR, Miley, GK, Motta, V, Sirianni, M, Sparks, WB, Tran, HD, Tsvetanov, Z, White, RL & Zheng, W 2005, 'The morphology-density relation in z ∼ 1 clusters', Astrophysical Journal, vol. 623, no. 2 I, pp. 721-741. https://doi.org/10.1086/428881
Postman M, Franx M, Cross NJG, Holden B, Ford HC, Illingworth GD et al. The morphology-density relation in z ∼ 1 clusters. Astrophysical Journal. 2005 Apr 20;623(2 I):721-741. https://doi.org/10.1086/428881
Postman, M. ; Franx, M. ; Cross, N. J G ; Holden, B. ; Ford, H. C. ; Illingworth, G. D. ; Goto, T. ; Demarco, R. ; Rosati, P. ; Blakeslee, J. P. ; Tran, K. V. ; Benitez, N. ; Clampin, M. ; Hartig, G. F. ; Homeier, N. ; Ardila, D. R. ; Bartko, F. ; Bouwens, R. J. ; Bradley, L. D. ; Broadhurst, T. J. ; Brown, R. A. ; Burrows, C. J. ; Cheng, E. S. ; Feldman, P. D. ; Golimowski, D. A. ; Gronwall, C. ; Infante, L. ; Kimble, R. A. ; Krist, J. E. ; Lesser, M. P. ; Martel, A. R. ; Mei, S. ; Menanteau, F. ; Meurer, G. R. ; Miley, G. K. ; Motta, V. ; Sirianni, M. ; Sparks, W. B. ; Tran, H. D. ; Tsvetanov, Zlatan ; White, R. L. ; Zheng, W. / The morphology-density relation in z ∼ 1 clusters. In: Astrophysical Journal. 2005 ; Vol. 623, No. 2 I. pp. 721-741.
@article{cfa05e348c3d49e8978cbdfaec591b6d,
title = "The morphology-density relation in z ∼ 1 clusters",
abstract = "We measure the morphology-density relation (MDR) and morphology-radius relation (MRR) for galaxies in seven z ∼ 1 clusters that have been observed with the Advanced Camera for Surveys (ACS) on board the Hubble Space Telescope. Simulations and independent comparisons of our visually derived morphologies indicate that ACS allows one to distinguish between E, S0, and spiral morphologies down to z8550 = 24, corresponding to L/L* = 0.21 and 0.30 at z = 0.83 and 1.24, respectively. We adopt density and radius estimation methods that match those used at lower redshift in order to study the evolution of the MDR and MRR. We detect a change in the MDR between 0.8 < z < 1.2 and that observed at z ∼ 0, consistent with recent work; specifically, the growth in the bulge-dominated galaxy fraction, f E+S0, with increasing density proceeds less rapidly at z ∼ 1 than it does at z ∼ 0. At z ∼ 1 and Σ ≥ 500 galaxies Mpc -2, we find 〈fE+S0〉 = 0-72 ± 0.10. At z ∼ 0, an E+S0 population fraction of this magnitude occurs at densities about 5 times smaller. The evolution in the MDR is confined to densities Σ ≳ 40 galaxies Mpc-2 and appears to be primarily due to a deficit of SO galaxies and an excess of Sp+Irr galaxies relative to the local galaxy population. Theye-density relation exhibits no significant evolution between z = 1 and 0. We find mild evidence to suggest that the MDR is dependent on the bolometric X-ray luminosity of the intracluster medium. Implications for the evolution of the disk galaxy population in dense regions are discussed in the context of these observations.",
keywords = "Galaxies: clusters: general, Galaxies: evolution, Galaxies: formation, Galaxies: structure",
author = "M. Postman and M. Franx and Cross, {N. J G} and B. Holden and Ford, {H. C.} and Illingworth, {G. D.} and T. Goto and R. Demarco and P. Rosati and Blakeslee, {J. P.} and Tran, {K. V.} and N. Benitez and M. Clampin and Hartig, {G. F.} and N. Homeier and Ardila, {D. R.} and F. Bartko and Bouwens, {R. J.} and Bradley, {L. D.} and Broadhurst, {T. J.} and Brown, {R. A.} and Burrows, {C. J.} and Cheng, {E. S.} and Feldman, {P. D.} and Golimowski, {D. A.} and C. Gronwall and L. Infante and Kimble, {R. A.} and Krist, {J. E.} and Lesser, {M. P.} and Martel, {A. R.} and S. Mei and F. Menanteau and Meurer, {G. R.} and Miley, {G. K.} and V. Motta and M. Sirianni and Sparks, {W. B.} and Tran, {H. D.} and Zlatan Tsvetanov and White, {R. L.} and W. Zheng",
year = "2005",
month = "4",
day = "20",
doi = "10.1086/428881",
language = "English",
volume = "623",
pages = "721--741",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "2 I",

}

TY - JOUR

T1 - The morphology-density relation in z ∼ 1 clusters

AU - Postman, M.

AU - Franx, M.

AU - Cross, N. J G

AU - Holden, B.

AU - Ford, H. C.

AU - Illingworth, G. D.

AU - Goto, T.

AU - Demarco, R.

AU - Rosati, P.

AU - Blakeslee, J. P.

AU - Tran, K. V.

AU - Benitez, N.

AU - Clampin, M.

AU - Hartig, G. F.

AU - Homeier, N.

AU - Ardila, D. R.

AU - Bartko, F.

AU - Bouwens, R. J.

AU - Bradley, L. D.

AU - Broadhurst, T. J.

AU - Brown, R. A.

AU - Burrows, C. J.

AU - Cheng, E. S.

AU - Feldman, P. D.

AU - Golimowski, D. A.

AU - Gronwall, C.

AU - Infante, L.

AU - Kimble, R. A.

AU - Krist, J. E.

AU - Lesser, M. P.

AU - Martel, A. R.

AU - Mei, S.

AU - Menanteau, F.

AU - Meurer, G. R.

AU - Miley, G. K.

AU - Motta, V.

AU - Sirianni, M.

AU - Sparks, W. B.

AU - Tran, H. D.

AU - Tsvetanov, Zlatan

AU - White, R. L.

AU - Zheng, W.

PY - 2005/4/20

Y1 - 2005/4/20

N2 - We measure the morphology-density relation (MDR) and morphology-radius relation (MRR) for galaxies in seven z ∼ 1 clusters that have been observed with the Advanced Camera for Surveys (ACS) on board the Hubble Space Telescope. Simulations and independent comparisons of our visually derived morphologies indicate that ACS allows one to distinguish between E, S0, and spiral morphologies down to z8550 = 24, corresponding to L/L* = 0.21 and 0.30 at z = 0.83 and 1.24, respectively. We adopt density and radius estimation methods that match those used at lower redshift in order to study the evolution of the MDR and MRR. We detect a change in the MDR between 0.8 < z < 1.2 and that observed at z ∼ 0, consistent with recent work; specifically, the growth in the bulge-dominated galaxy fraction, f E+S0, with increasing density proceeds less rapidly at z ∼ 1 than it does at z ∼ 0. At z ∼ 1 and Σ ≥ 500 galaxies Mpc -2, we find 〈fE+S0〉 = 0-72 ± 0.10. At z ∼ 0, an E+S0 population fraction of this magnitude occurs at densities about 5 times smaller. The evolution in the MDR is confined to densities Σ ≳ 40 galaxies Mpc-2 and appears to be primarily due to a deficit of SO galaxies and an excess of Sp+Irr galaxies relative to the local galaxy population. Theye-density relation exhibits no significant evolution between z = 1 and 0. We find mild evidence to suggest that the MDR is dependent on the bolometric X-ray luminosity of the intracluster medium. Implications for the evolution of the disk galaxy population in dense regions are discussed in the context of these observations.

AB - We measure the morphology-density relation (MDR) and morphology-radius relation (MRR) for galaxies in seven z ∼ 1 clusters that have been observed with the Advanced Camera for Surveys (ACS) on board the Hubble Space Telescope. Simulations and independent comparisons of our visually derived morphologies indicate that ACS allows one to distinguish between E, S0, and spiral morphologies down to z8550 = 24, corresponding to L/L* = 0.21 and 0.30 at z = 0.83 and 1.24, respectively. We adopt density and radius estimation methods that match those used at lower redshift in order to study the evolution of the MDR and MRR. We detect a change in the MDR between 0.8 < z < 1.2 and that observed at z ∼ 0, consistent with recent work; specifically, the growth in the bulge-dominated galaxy fraction, f E+S0, with increasing density proceeds less rapidly at z ∼ 1 than it does at z ∼ 0. At z ∼ 1 and Σ ≥ 500 galaxies Mpc -2, we find 〈fE+S0〉 = 0-72 ± 0.10. At z ∼ 0, an E+S0 population fraction of this magnitude occurs at densities about 5 times smaller. The evolution in the MDR is confined to densities Σ ≳ 40 galaxies Mpc-2 and appears to be primarily due to a deficit of SO galaxies and an excess of Sp+Irr galaxies relative to the local galaxy population. Theye-density relation exhibits no significant evolution between z = 1 and 0. We find mild evidence to suggest that the MDR is dependent on the bolometric X-ray luminosity of the intracluster medium. Implications for the evolution of the disk galaxy population in dense regions are discussed in the context of these observations.

KW - Galaxies: clusters: general

KW - Galaxies: evolution

KW - Galaxies: formation

KW - Galaxies: structure

UR - http://www.scopus.com/inward/record.url?scp=20444382104&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=20444382104&partnerID=8YFLogxK

U2 - 10.1086/428881

DO - 10.1086/428881

M3 - Review article

AN - SCOPUS:20444382104

VL - 623

SP - 721

EP - 741

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2 I

ER -