The GEEC2 spectroscopic survey of Galaxy groups at 0.8 <z <1

M.L. Balogh; S.L. McGee; A. Mok; D.J. Wilman; A. Finoguenov; R.G. Bower; J.S. Mulchaey; L.C. Parker; M. Tanaka

doi:10.1093/mnras/stu1332

The GEEC2 spectroscopic survey of Galaxy groups at 0.8 <z <1

M.L. Balogh, S.L. McGee, A. Mok, D.J. Wilman, A. Finoguenov, R.G. Bower, J.S. Mulchaey, L.C. Parker, M. Tanaka

Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

31 Citations (Scopus)

Abstract

We present the data release of the Gemini-South GMOS spectroscopy in the fields of 11 galaxy groups at 0.8 < z < 1, within the COSMOS field. This forms the basis of the Galaxy Environment Evolution Collaboration 2 (GEEC2) project to study galaxy evolution in haloes with M ∼ 10¹³M_⊙ across cosmic time. The final sample includes 162 spectroscopically confirmed members with R < 24.75, and is >50 per cent complete for galaxies within the virial radius, and with stellar mass Mstar > 10^10.3 M_⊙. Including galaxies with photometric redshifts, we have an effective sample size of ∼400 galaxies within the virial radii of these groups. We present group velocity dispersions, dynamical and stellar masses. Combining with the GCLASS sample of more massive clusters at the same redshift, we find the total stellar mass is strongly correlated with the dynamical mass, with log M₂₀₀ = 1.20(log M_star − 12) + 14.07. This stellar fraction of ∼1 per cent is lower than predicted by some halo occupation distribution models, though the weak dependence on halo mass is in good agreement. Most groups have an easily identifiable most massive galaxy (MMG) near the centre of the galaxy distribution, and we present the spectroscopic properties and surface brightness fits to these galaxies. The total stellar mass distribution in the groups, excluding the MMG, compares well with an NFW (Navarro Frenk & White) profile with concentration 4, for galaxies beyond ∼0.2R₂₀₀. This is more concentrated than the number density distribution, demonstrating that there is some mass segregation.

Original language	English
Pages (from-to)	2679-2694
Number of pages	16
Journal	Royal Astronomical Society. Monthly Notices
Volume	443
Issue number	3
DOIs	https://doi.org/10.1093/mnras/stu1332
Publication status	Published - 2014

Bibliographical note

Export Date: 15 August 2017

CODEN: MNRAA

Correspondence Address: Balogh, M.L.; Department of Physics and Astronomy, University of Waterloo, Waterloo, Ontario N2L 3G1, Canada; email: mbalogh@uwaterloo.ca

Funding details: LCP, Library Company of Philadelphia

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Mod. Phys., 77, p. 207; Wetzel, A.R., Tinker, J.L., Conroy, C., Bosch F.C.v., d., (2014) MNRAS, 439, p. 2687; White, S.D.M., Navarro, J.F., Evrard, A.E., Frenk, C.S., (1993) Nature, 366, p. 429; Williamson, R., (2011) ApJ, 738, p. 139; Wilman, D.J., Balogh, M.L., Bower, R.G., Mulchaey, J.S., Oemler, A., Carlberg, R.G., Morris, S.L., Whitaker, R.J., (2005) MNRAS, 358, p. 71; Wolf, C., Gray, M.E., Meisenheimer, K., (2005) ÁA, 443, p. 435; Yang, X., Mo, H.J., van den Bosch, F.C., Pasquali, A., Li, C., Barden, M., (2007) ApJ, 671, p. 153; York, D.G., (2000) AJ, 120, p. 1579; Zehavi, I., (2002) ApJ, 571, p. 172; Ziparo, F., (2013) MNRAS, 434, p. 3089

Keywords

Galaxies: evolution
Galaxies: groups: general

Access to Document

10.1093/mnras/stu1332Licence: None: All rights reserved

Birmingham Astrophysics : Consolidated Grant 2013-2016
Vecchio, A., Ponman, T., Freise, A., Smith, G., Speake, C., Mandel, I., Cruise, M., Raychaudhury, S. & Stevens, I.
SCIENCE & TECHNOLOGY FACILITIES COUNCIL
1/04/13 → 30/09/16
Project: Research Councils

Cite this

@article{807a659e41724cf0b96327a9c4823aea,

title = "The GEEC2 spectroscopic survey of Galaxy groups at 0.8 <z <1",

abstract = "We present the data release of the Gemini-South GMOS spectroscopy in the fields of 11 galaxy groups at 0.8 < z < 1, within the COSMOS field. This forms the basis of the Galaxy Environment Evolution Collaboration 2 (GEEC2) project to study galaxy evolution in haloes with M ∼ 1013 M⊙ across cosmic time. The final sample includes 162 spectroscopically confirmed members with R < 24.75, and is >50 per cent complete for galaxies within the virial radius, and with stellar mass Mstar > 1010.3 M⊙. Including galaxies with photometric redshifts, we have an effective sample size of ∼400 galaxies within the virial radii of these groups. We present group velocity dispersions, dynamical and stellar masses. Combining with the GCLASS sample of more massive clusters at the same redshift, we find the total stellar mass is strongly correlated with the dynamical mass, with log M200 = 1.20(log Mstar − 12) + 14.07. This stellar fraction of ∼1 per cent is lower than predicted by some halo occupation distribution models, though the weak dependence on halo mass is in good agreement. Most groups have an easily identifiable most massive galaxy (MMG) near the centre of the galaxy distribution, and we present the spectroscopic properties and surface brightness fits to these galaxies. The total stellar mass distribution in the groups, excluding the MMG, compares well with an NFW (Navarro Frenk & White) profile with concentration 4, for galaxies beyond ∼0.2R200. This is more concentrated than the number density distribution, demonstrating that there is some mass segregation.",

keywords = "Galaxies: evolution, Galaxies: groups: general",

author = "M.L. Balogh and S.L. McGee and A. Mok and D.J. Wilman and A. Finoguenov and R.G. Bower and J.S. Mulchaey and L.C. Parker and M. Tanaka",

note = "Export Date: 15 August 2017 CODEN: MNRAA Correspondence Address: Balogh, M.L.; Department of Physics and Astronomy, University of Waterloo, Waterloo, Ontario N2L 3G1, Canada; email: mbalogh@uwaterloo.ca Funding details: LCP, Library Company of Philadelphia References: Balogh, M.L., Navarro, J.F., Morris, S.L., (2000) ApJ, 540, p. 113; Balogh, M.L., Babul, A., Voit, G.M., McCarthy, I.G., Jones, L.R., Lewis, G.F., Ebeling, H., (2006) MNRAS, 366, p. 624; Balogh, M.L., (2007) MNRAS, 374, p. 1169; Balogh, M.L., McCarthy, I.G., Bower, R.G., Eke, V.R., (2008) MNRAS, 385, p. 1003; Balogh, M.L., (2009) MNRAS, 398, p. 754; Balogh, M.L., (2011) MNRAS, 412, p. 2303. , (Paper I); Beers, T.C., Flynn, K., Gebhardt, K., (1990) AJ, 100, p. 32; Behroozi, P.S., Wechsler, R.H., Conroy, C., (2013) ApJ, 770, p. 57; Berlind, A.A., Weinberg, D.H., (2002) ApJ, 575, p. 587; Bǐrzan, L., Rafferty, D.A., McNamara, B.R., Wise, M.W., Nulsen, P.E.J., (2004) ApJ, 607, p. 800; Blanton, M.R., Roweis, S., (2007) AJ, 133, p. 734; B{\"o}hringer, H., (2001) {\'A}A, 369, p. 826; B{\"o}hringer, H., (2007) {\'A}A, 469, p. 363; Bower, R.G., Benson, A.J., Malbon, R., Helly, J.C., Frenk, C.S., Baugh, C.M., Cole, S., Lacey, C.G., (2006) MNRAS, 370, p. 645; Bruzual, G., (2007), Vazdekis A., Peletier R., eds. Proc. IAU Symp. 241, Stellar Populations as Building Blocks of Galaxies. Cambridge Univ. Press, Cambridge; Capak, P., (2007) ApJS, 172, p. 99; Carlberg, R.G., Yee, H.K.C., Ellingson, E., Abraham, R., Gravel, P., Morris, S., Pritchet, C.J., (1996) ApJ, 462, p. 32; Carlberg, R.G., (1997) ApJ, 476, pp. L7; Carlberg, R.G., Yee, H.K.C., Morris, S.L., Lin, H., Hall, P.B., Patton, D.R., Sawicki, M., Shepherd, C.W., (2001) ApJ, 552, p. 427; Chabrier, G., (2003) PASP, 115, p. 763; Colless, M., (2001) MNRAS, 328, p. 1039; Connelly, J.L., (2012) ApJ, 756, p. 139; Conroy, C., Graves, G.J., van Dokkum, P.G., (2014) ApJ, 780, p. 33; Cucciati, O., (2010) {\'A}A, 520, pp. A42; Demarco, R., (2007) ApJ, 663, p. 164; Driver, S.P., (2011) MNRAS, 413, p. 971; Duffy, A.R., Schaye, J., Kay, S.T., Dalla Vecchia, C., (2008) MNRAS, 390, pp. L64; Dutton, A.A., Macci'o, A.V., (2014) MNRAS, 441, p. 3359; Eke, V.R., (2004) MNRAS, 348, p. 866; Ellingson, E., Lin, H., Yee, H.K.C., Carlberg, R.G., (2001) ApJ, 547, p. 609; Elvis, M., (2009) ApJS, 184, p. 158; Erfanianfar, G., (2013) ApJ, 765, p. 117; Fassbender, R., (2011) {\'A}A, 527, pp. A78; Finoguenov, A., (2007) ApJS, 172, p. 182; George, M.R., (2011) ApJ, 742, p. 125; George, M.R., (2012) ApJ, 757, p. 2; Gerke, B.F., (2007) MNRAS, 376, p. 1425; Gerke, B.F., (2012) ApJ, 751, p. 50; Gettings, D.P., (2012) ApJ, 759, pp. L23; Gilbank, D.G., Gladders, M.D., Yee, H.K.C., Hsieh, B.C., (2011) AJ, 141, p. 94; Gillis, B.R., Hudson, M.J., (2011) MNRAS, 410, p. 13; Giodini, S., (2009) ApJ, 703, p. 982; Gladders, M.D., Yee, H.K.C., (2005) ApJS, 157, p. 1; Glazebrook, K., Bland-Hawthorn, J., (2001) PASP, 113, p. 197; Hao, J., (2010) ApJS, 191, p. 254; Hickox, R.C., (2009) ApJ, 696, p. 891; Hinshaw, G., (2013) ApJS, 208, p. 19; Ilbert, O., (2009) ApJ, 690, p. 1236; Ilbert, O., (2010) ApJ, 709, p. 644; Jian, H.-Y., (2014) ApJ, 788, p. 109; Kewley, L.J., Ellison, S.L., (2008) ApJ, 681, p. 1183; Kim, J.-W., (2014) MNRAS, 438, p. 825; Knobel, C., (2009) ApJ, 697, p. 1842; Knobel, C., (2012) ApJ, 753, p. 121; Knobel, C., (2013) ApJ, 769, p. 24; Koekemoer, A.M., (2007) ApJS, 172, p. 196; Koester, B.P., (2007) ApJ, 660, p. 239; Kovac, K., (2014) MNRAS, 438, p. 717; Labb{\'e}, I., (2005) ApJ, 624, pp. L81; Lacy, M., (2004) ApJS, 154, p. 166; Leauthaud, A., (2010) ApJ, 709, p. 97; Leauthaud, A., (2012) ApJ, 744, p. 159; Leauthaud, A., (2012) ApJ, 746, p. 95; Li, I.H., Yee, H.K.C., (2008) AJ, 135, p. 809; Lidman, C., (2012) MNRAS, 427, p. 550; Lilly, S.J., (2007) ApJS, 172, p. 70; Marulli, F., (2013) {\'A}A, 557, pp. A17; McGee, S.L., Balogh, M.L., Bower, R.G., Font, A.S., McCarthy, I.G., (2009) MNRAS, 400, p. 937; McGee, S.L., Balogh, M.L., Wilman, D.J., Bower, R.G., Mulchaey, J.S., Parker, L.C., Oemler, A., (2011) MNRAS, 413, p. 996; Mok, A., (2013) MNRAS, 431, p. 1090. , (Paper II); Mok, A., (2014) MNRAS, 438, p. 3070. , (Paper III); Mulchaey, J.S., Davis, D.S., Mushotzky, R.F., Burstein, D., (2003) ApJS, 145, p. 39; Muzzin, A., Yee, H.K.C., Hall, P.B., Ellingson, E., Lin, H., (2007) ApJ, 659, p. 1106; Muzzin, A., (2012) ApJ, 746, p. 188; Muzzin, A., Wilson, G., Demarco, R., Lidman, C., Nantais, J., Hoekstra, H., Yee, H.K.C., Rettura, A., (2013) ApJ, 767, p. 39; Navarro, J.F., Frenk, C.S., White, S.D.M., (1997) ApJ, 490, p. 493. , (NFW); Newman, J.A., (2013) ApJS, 208, p. 5; Oman, K.A., Hudson, M.J., Behroozi, P.S., (2013) MNRAS, 431, p. 2307; Omand, C.M.B., Balogh, M.L., Poggianti, B.M., (2014) MNRAS, 440, p. 843; Osmond, J.P.F., Ponman, T.J., (2004) MNRAS, 350, p. 1511; Piffaretti, R., Arnaud, M., Pratt, G.W., Pointecouteau, E., Melin, J.-B., (2011) {\'A}A, 534, pp. A109; (2011) {\'A}A, 536, pp. A8. , Planck Collaboration V.I.I.I; Rosati, P., Borgani, S., Norman, C., (2002) AR{\'A}A, 40, p. 539; Salim, S., (2009) ApJ, 700, p. 161; Sargent, M.T., (2007) ApJS, 172, p. 434; Sawala, T., (2014), preprint (arXiv:1404.3724); Schinnerer, E., (2007) ApJS, 172, p. 46; Scoville, N., (2007) ApJS, 172, p. 1; Simard, L., (2002) ApJS, 142, p. 1; Simard, L., Mendel, J.T., Patton, D.R., Ellison, S.L., McConnachie, A.W., (2011) ApJS, 196, p. 11; Stanford, S.A., Gonzalez, A.H., Brodwin, M., Gettings, D.P., Eisenhardt, P.R.M., Stern, D., Wylezalek, D., (2014), preprint (arXiv:1403.3361); Staniszewski, Z., (2009) ApJ, 701, p. 32; Stern, D., (2005) ApJ, 631, p. 163; Stott, J.P., (2010) ApJ, 718, p. 23; Stott, J.P., Collins, C.A., Burke, C., Hamilton-Morris, V., Smith, G.P., (2011) MNRAS, 414, p. 445; Tanaka, M., (2013) PASJ, 65, p. 17; Tegmark, M., (2004) ApJ, 606, p. 702; van der Burg, R.F.J., Muzzin, A., Hoekstra, H., Wilson, G., Lidman, C., Yee, H.K.C., (2014) {\'A}A, 561, pp. A79; van der Wel, A., (2014) ApJ, 788, p. 28; Vanderlinde, K., (2010) ApJ, 722, p. 1180; Voit, G.M., (2005) Rev. Mod. Phys., 77, p. 207; Wetzel, A.R., Tinker, J.L., Conroy, C., Bosch F.C.v., d., (2014) MNRAS, 439, p. 2687; White, S.D.M., Navarro, J.F., Evrard, A.E., Frenk, C.S., (1993) Nature, 366, p. 429; Williamson, R., (2011) ApJ, 738, p. 139; Wilman, D.J., Balogh, M.L., Bower, R.G., Mulchaey, J.S., Oemler, A., Carlberg, R.G., Morris, S.L., Whitaker, R.J., (2005) MNRAS, 358, p. 71; Wolf, C., Gray, M.E., Meisenheimer, K., (2005) {\'A}A, 443, p. 435; Yang, X., Mo, H.J., van den Bosch, F.C., Pasquali, A., Li, C., Barden, M., (2007) ApJ, 671, p. 153; York, D.G., (2000) AJ, 120, p. 1579; Zehavi, I., (2002) ApJ, 571, p. 172; Ziparo, F., (2013) MNRAS, 434, p. 3089",

year = "2014",

doi = "10.1093/mnras/stu1332",

language = "English",

volume = "443",

pages = "2679--2694",

journal = "Royal Astronomical Society. Monthly Notices",

issn = "0035-8711",

publisher = "SIPRI/Oxford University Press",

number = "3",

}

TY - JOUR

T1 - The GEEC2 spectroscopic survey of Galaxy groups at 0.8 <z <1

AU - Balogh, M.L.

AU - McGee, S.L.

AU - Mok, A.

AU - Wilman, D.J.

AU - Finoguenov, A.

AU - Bower, R.G.

AU - Mulchaey, J.S.

AU - Parker, L.C.

AU - Tanaka, M.

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PY - 2014

Y1 - 2014

N2 - We present the data release of the Gemini-South GMOS spectroscopy in the fields of 11 galaxy groups at 0.8 < z < 1, within the COSMOS field. This forms the basis of the Galaxy Environment Evolution Collaboration 2 (GEEC2) project to study galaxy evolution in haloes with M ∼ 1013 M⊙ across cosmic time. The final sample includes 162 spectroscopically confirmed members with R < 24.75, and is >50 per cent complete for galaxies within the virial radius, and with stellar mass Mstar > 1010.3 M⊙. Including galaxies with photometric redshifts, we have an effective sample size of ∼400 galaxies within the virial radii of these groups. We present group velocity dispersions, dynamical and stellar masses. Combining with the GCLASS sample of more massive clusters at the same redshift, we find the total stellar mass is strongly correlated with the dynamical mass, with log M200 = 1.20(log Mstar − 12) + 14.07. This stellar fraction of ∼1 per cent is lower than predicted by some halo occupation distribution models, though the weak dependence on halo mass is in good agreement. Most groups have an easily identifiable most massive galaxy (MMG) near the centre of the galaxy distribution, and we present the spectroscopic properties and surface brightness fits to these galaxies. The total stellar mass distribution in the groups, excluding the MMG, compares well with an NFW (Navarro Frenk & White) profile with concentration 4, for galaxies beyond ∼0.2R200. This is more concentrated than the number density distribution, demonstrating that there is some mass segregation.

AB - We present the data release of the Gemini-South GMOS spectroscopy in the fields of 11 galaxy groups at 0.8 < z < 1, within the COSMOS field. This forms the basis of the Galaxy Environment Evolution Collaboration 2 (GEEC2) project to study galaxy evolution in haloes with M ∼ 1013 M⊙ across cosmic time. The final sample includes 162 spectroscopically confirmed members with R < 24.75, and is >50 per cent complete for galaxies within the virial radius, and with stellar mass Mstar > 1010.3 M⊙. Including galaxies with photometric redshifts, we have an effective sample size of ∼400 galaxies within the virial radii of these groups. We present group velocity dispersions, dynamical and stellar masses. Combining with the GCLASS sample of more massive clusters at the same redshift, we find the total stellar mass is strongly correlated with the dynamical mass, with log M200 = 1.20(log Mstar − 12) + 14.07. This stellar fraction of ∼1 per cent is lower than predicted by some halo occupation distribution models, though the weak dependence on halo mass is in good agreement. Most groups have an easily identifiable most massive galaxy (MMG) near the centre of the galaxy distribution, and we present the spectroscopic properties and surface brightness fits to these galaxies. The total stellar mass distribution in the groups, excluding the MMG, compares well with an NFW (Navarro Frenk & White) profile with concentration 4, for galaxies beyond ∼0.2R200. This is more concentrated than the number density distribution, demonstrating that there is some mass segregation.

KW - Galaxies: evolution

KW - Galaxies: groups: general

UR - http://www.scopus.com/inward/record.url?eid=2-s2.0-84906057106&partnerID=MN8TOARS

U2 - 10.1093/mnras/stu1332

DO - 10.1093/mnras/stu1332

M3 - Article

SN - 0035-8711

VL - 443

SP - 2679

EP - 2694

JO - Royal Astronomical Society. Monthly Notices

JF - Royal Astronomical Society. Monthly Notices

IS - 3

ER -

The GEEC2 spectroscopic survey of Galaxy groups at 0.8 <z <1

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Birmingham Astrophysics : Consolidated Grant 2013-2016

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