The XXL Survey: X. K -band luminosity - Weak-lensing mass relation for groups and clusters of galaxies

F. Ziparo; G.P. Smith; S.L. Mulroy; M. Lieu; J.P. Willis; P. Hudelot; S.L. McGee; S. Fotopoulou; C. Lidman; S. Lavoie; M. Pierre; C. Adami; L. Chiappetti; N. Clerc; P. Giles; B. Maughan; F. Pacaud; T. Sadibekova

doi:10.1051/0004-6361/201526792

The XXL Survey: X. K -band luminosity - Weak-lensing mass relation for groups and clusters of galaxies

F. Ziparo, G.P. Smith, S.L. Mulroy, M. Lieu, J.P. Willis, P. Hudelot, S.L. McGee, S. Fotopoulou, C. Lidman, S. Lavoie, M. Pierre, C. Adami, L. Chiappetti, N. Clerc, P. Giles, B. Maughan, F. Pacaud, T. Sadibekova

Physics and Astronomy

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

8 Citations (Scopus)

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Abstract

Galaxy clusters and groups are important cosmological probes and giant cosmic laboratories for studying galaxy evolution. Much effort has been devoted to understanding how and when baryonic matter cools at the centre of potential wells. However, a clear picture of the efficiency with which baryons are converted into stars is still missing. We present the K-band luminosity-halo mass relation, LK,500-M500,WL, for a subsample of 20 of the 100 brightest clusters in the XXL Survey observed with WIRCam at the Canada-France-Hawaii Telescope (CFHT). For the first time, we have measured this relation via weak-lensing analysis down to M500,WL = 3.5 × 1013 MȮ. This allows us to investigate whether the slope of the LK-M relation is different for groups and clusters, as seen in other works. The clusters in our sample span a wide range in mass, M500,WL = 0.35-12.10 × 1014 MȮ, at 0 < z < 0.6. The K-band luminosity scales as log 10(LK,500/ 1012 LȮ) ? βlog 10(M500,WL/ 1014 MȮ) with β = 0.85+0.35 -0.27 and an intrinsic scatter of σlnLKM = 0.37+0.19 -0.17. Combining our sample with some clusters in the Local Cluster Substructure Survey (LoCuSS) present in the literature, we obtain a slope of 1.05+0.16 -0.14 and an intrinsic scatter of 0.14+0.09 -0.07. The flattening in the LK-M seen in previous works is not seen here and might be a result of a bias in the mass measurement due to assumptions on the dynamical state of the systems. We also study the richness-mass relation and find that group-sized halos have more galaxies per unit halo mass than massive clusters. However, the brightest cluster galaxy (BCG) in low-mass systems contributes a greater fraction to the total cluster light than BCGs do in massive clusters; the luminosity gap between the two brightest galaxies is more prominent for group-sized halos. This result is a natural outcome of the hierarchical growth of structures, where massive galaxies form and gain mass within low-mass groups and are ultimately accreted into more massive clusters to become either part of the BCG or one of the brighter galaxies. © ESO, 2016.

Original language	English
Journal	Astronomy and Astrophysics
Volume	592
Early online date	15 Jun 2016
DOIs	https://doi.org/10.1051/0004-6361/201526792
Publication status	Published - Aug 2016

Bibliographical note

Export Date: 15 August 2017

CODEN: AAEJA

Funding details: RE 1462-6, DFG, Deutsche Forschungsgemeinschaft

Funding text: F.P. acknowledges support from the BMBF/DLR grant 50 OR 1117, the DFG grant RE 1462-6 and the DFG Transregio Programme TR33.

References: Andreon, S., (2010) MNRAS, 407, p. 263; Balogh, M.L., Mazzotta, P., Bower, R.G., (2011) MNRAS, 412, p. 947; Balogh, M.L., McGee, S.L., Mok, A., (2014) MNRAS, 443, p. 2679; Behroozi, P.S., Wechsler, R.H., Conroy, C., (2013) ApJ, 770, p. 57; Berrier, J.C., Stewart, K.R., Bullock, J.S., (2009) ApJ, 690, p. 1292; Bertin, E., (2006) ASP Conf. Ser., 351, p. 112; Bertin, E., Arnouts, S., (1996) A&AS, 117, p. 393; Bielby, R.M., Gonzalez-Perez, V., McCracken, H.J., (2014) A&A, 568, p. A24; Biviano, A., Murante, G., Borgani, S., (2006) A&A, 456, p. 23; Bruzual, G., Charlot, S., (2003) MNRAS, 344, p. 1000; Chabrier, G., (2003) PASP, 115, p. 763; Clerc, N., Adami, C., Lieu, M., (2014) MNRAS, 444, p. 2723; Cole, S., Norberg, P., Baugh, C.M., (2001) MNRAS, 326, p. 255; Cortese, L., Gavazzi, G., Boselli, A., (2006) A&A, 453, p. 847; Coupon, J., Ilbert, O., Kilbinger, M., (2009) A&A, 500, p. 981; Cowie, L.L., Gardner, J.P., Hu, E.M., (1994) ApJ, 434, p. 114; Davis, M., Efstathiou, G., Frenk, C.S., White, S.D.M., (1985) ApJ, 292, p. 371; De Lucia, G., Blaizot, J., (2007) MNRAS, 375, p. 2; De Lucia, G., Weinmann, S., Poggianti, B.M., Aragón-Salamanca, A., Zaritsky, D., (2012) MNRAS, 423, p. 1277; Dubinski, J., (1998) ApJ, 502, p. 141; Eckert, D., Molendi, S., Owers, M., (2014) A&A, 570, p. A119; Edge, A.C., (1991) MNRAS, 250, p. 103; Erben, T., (2012) AAS Meeting, 219. , 130.09; Giles, P.A., Maughan, B.J., Pacaud, F., (2016) A&A, 592, p. A3. , XXL Survey, III; Giodini, S., Pierini, D., Finoguenov, A., (2009) ApJ, 703, p. 982; Gonzalez, A.H., Sivanandam, S., Zabludoff, A.I., Zaritsky, D., (2013) ApJ, 778, p. 14; Gwyn, S.D.J., (2012) AJ, 143, p. 38; Heymans, C., Grocutt, E., Heavens, A., (2012) MNRAS, 427, p. 146; Hilton, M., Hasselfield, M., Sifón, C., (2013) MNRAS, 435, p. 3469; Hinshaw, G., Larson, D., Komatsu, E., (2013) ApJS, 208, p. 19; Jarrett, T.H., Chester, T., Cutri, R., (2000) AJ, 119, p. 2498; Kelly, B.C., (2007) ApJ, 665, p. 1489; Kochanek, C.S., Pahre, M.A., Falco, E.E., (2001) ApJ, 560, p. 566; Kravtsov, A.V., Borgani, S., (2012) ARA&A, 50, p. 353; Kravtsov, A., Vikhlinin, A., Meshscheryakov, A., (2014) ApJ, , submitted [arXiv:1401.7329]; Leauthaud, A., Finoguenov, A., Kneib, J.-P., (2010) ApJ, 709, p. 97; Kron, R.G., (1980) ApJS, 43, p. 305; Laporte, C.F.P., White, S.D.M., Naab, T., Gao, L., (2013) MNRAS, 435, p. 901; Lidman, C., Suherli, J., Muzzin, A., (2012) MNRAS, 427, p. 550; Lin, Y.-T., Mohr, J.J., (2004) ApJ, 617, p. 879; Lin, Y.-T., Mohr, J.J., Stanford, S.A., (2003) ApJ, 591, p. 749; Lin, Y.-T., Mohr, J.J., Stanford, S.A., (2004) ApJ, 610, p. 745; Lin, Y.-T., Mohr, J.J., Gonzalez, A.H., Stanford, S.A., (2006) ApJ, 650, p. L99; Lieu, M., Smith, G.P., Giles, P.A., (2016) A&A, 592, p. A4. , XXL Survey, IV; Marmo, C., Bertin, E., (2008) ASP Conf. Ser., 394, p. 619; McCracken, H.J., Milvang-Jensen, B., Dunlop, J., (2012) A&A, 544, p. A156; McGee, S.L., Balogh, M.L., Bower, R.G., Font, A.S., McCarthy, I.G., (2009) MNRAS, 400, p. 937; Merritt, D., (1985) ApJ, 289, p. 18; Mulroy, S.L., Smith, G.P., Haines, C.P., (2014) MNRAS, 443, p. 3309; Muzzin, A., Yee, H.K.C., Hall, P.B., Lin, H., (2007) ApJ, 663, p. 150; Navarro, J.F., Frenk, C.S., White, S.D.M., (1997) ApJ, 490, p. 493; Okabe, N., Takada, M., Umetsu, K., Futamase, T., Smith, G.P., (2010) PASJ, 62, p. 811; Okabe, N., Smith, G.P., Umetsu, K., Takada, M., Futamase, T., (2013) ApJ, 769, p. LL35; Ostriker, J.P., Hausman, M.A., (1977) ApJ, 217, p. L125; Pacaud, F., Clerc, N., Giles, P.A., (2016) A&A, 592, p. A2. , XXL Survey, II; Patel, S.G., Kelson, D.D., Williams, R.J., (2015) ApJ, 799, p. L17; Pierre, M., Valtchanov, I., Altieri, B., (2004) J. Cosmol. Astropart. Phys., 9, p. 011; Pierre, M., Pacaud, F., Adami, C., (2016) A&A, 592, p. A1. , XXL Survey, I; Poggianti, B.M., (1997) A&AS, 122, p. 399; Poggianti, B.M., De Lucia, G., Varela, J., (2010) MNRAS, 405, p. 995; Ramella, M., Boschin, W., Geller, M., Mahdavi, A., Rines, K., (2004) ApJ, 128, p. 2022; Schlegel, D.J., Finkbeiner, D.P., Davis, M., (1998) ApJ, 500, p. 525; Smith, G.P., Khosroshahi, H.G., Dariush, A., (2010) MNRAS, 409, p. 169; Springel, V., Frenk, C.S., White, S.D.M., (2006) Nature, 440, p. 1137; Šuhada, R., Song, J., Boehringer, H., (2012) A&A, 537, p. A39; Tanaka, M., Kodama, T., Kajisawa, M., (2007) MNRAS, 377, p. 1206; Van Der Burg, R.F.J., Muzzin, A., Hoekstra, H., (2014) A&A, 561, p. A79; White, S.D.M., (1976) MNRAS, 174, p. 19; White, S.D.M., Rees, M.J., (1978) MNRAS, 183, p. 341; Zabludoff, A.I., Mulchaey, J.S., (1998) ApJ, 496, p. 39; Zibetti, S., White, S.D.M., Schneider, D.P., Brinkmann, J., (2005) MNRAS, 358, p. 949; Ziparo, F., Braglia, F.G., Pierini, D., (2012) MNRAS, 420, p. 2480; Ziparo, F., Popesso, P., Biviano, A., (2013) MNRAS, 434, p. 3089

Keywords

Galaxies: clusters: general
Galaxies: groups: general
Galaxies: photometry
Galaxies: stellar content
Gravitational lensing: weak
X-rays: galaxies: clusters
Cosmology
Luminance
Surveys
Galaxies: clusters: General
Galaxies: groups: generals
X rays: galaxies: clusters
Galaxies

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10.1051/0004-6361/201526792

Ziparo_et_al_The_XXL_survey_X._K-band_luminosity_Astronomy_&_Astrophysics_2016
Checked for eligibility:16/08/2017 Reproduced with permission from Astronomy & Astrophysics, © ESO https://www.aanda.org/articles/aa/pdf/2016/08/aa26792-15.pdf
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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

Ziparo, F., Smith, G. P., Mulroy, S. L., Lieu, M., Willis, J. P., Hudelot, P., McGee, S. L., Fotopoulou, S., Lidman, C., Lavoie, S., Pierre, M., Adami, C., Chiappetti, L., Clerc, N., Giles, P., Maughan, B., Pacaud, F., & Sadibekova, T. (2016). The XXL Survey: X. K -band luminosity - Weak-lensing mass relation for groups and clusters of galaxies. Astronomy and Astrophysics, 592. Advance online publication. https://doi.org/10.1051/0004-6361/201526792

@article{f23192f7ea0d42be9b5a75bc90f4d6cc,

title = "The XXL Survey: X. K -band luminosity - Weak-lensing mass relation for groups and clusters of galaxies",

abstract = "Galaxy clusters and groups are important cosmological probes and giant cosmic laboratories for studying galaxy evolution. Much effort has been devoted to understanding how and when baryonic matter cools at the centre of potential wells. However, a clear picture of the efficiency with which baryons are converted into stars is still missing. We present the K-band luminosity-halo mass relation, LK,500-M500,WL, for a subsample of 20 of the 100 brightest clusters in the XXL Survey observed with WIRCam at the Canada-France-Hawaii Telescope (CFHT). For the first time, we have measured this relation via weak-lensing analysis down to M500,WL = 3.5 × 1013 MȮ. This allows us to investigate whether the slope of the LK-M relation is different for groups and clusters, as seen in other works. The clusters in our sample span a wide range in mass, M500,WL = 0.35-12.10 × 1014 MȮ, at 0 < z < 0.6. The K-band luminosity scales as log 10(LK,500/ 1012 LȮ) ? βlog 10(M500,WL/ 1014 MȮ) with β = 0.85+0.35 -0.27 and an intrinsic scatter of σlnLKM = 0.37+0.19 -0.17. Combining our sample with some clusters in the Local Cluster Substructure Survey (LoCuSS) present in the literature, we obtain a slope of 1.05+0.16 -0.14 and an intrinsic scatter of 0.14+0.09 -0.07. The flattening in the LK-M seen in previous works is not seen here and might be a result of a bias in the mass measurement due to assumptions on the dynamical state of the systems. We also study the richness-mass relation and find that group-sized halos have more galaxies per unit halo mass than massive clusters. However, the brightest cluster galaxy (BCG) in low-mass systems contributes a greater fraction to the total cluster light than BCGs do in massive clusters; the luminosity gap between the two brightest galaxies is more prominent for group-sized halos. This result is a natural outcome of the hierarchical growth of structures, where massive galaxies form and gain mass within low-mass groups and are ultimately accreted into more massive clusters to become either part of the BCG or one of the brighter galaxies. {\textcopyright} ESO, 2016.",

keywords = "Galaxies: clusters: general, Galaxies: groups: general, Galaxies: photometry, Galaxies: stellar content, Gravitational lensing: weak, X-rays: galaxies: clusters, Cosmology, Luminance, Surveys, Galaxies: clusters: General, Galaxies: groups: generals, X rays: galaxies: clusters, Galaxies",

author = "F. Ziparo and G.P. Smith and S.L. Mulroy and M. Lieu and J.P. Willis and P. Hudelot and S.L. McGee and S. Fotopoulou and C. Lidman and S. Lavoie and M. Pierre and C. Adami and L. Chiappetti and N. Clerc and P. Giles and B. Maughan and F. Pacaud and T. Sadibekova",

note = "Export Date: 15 August 2017 CODEN: AAEJA Funding details: RE 1462-6, DFG, Deutsche Forschungsgemeinschaft Funding text: F.P. acknowledges support from the BMBF/DLR grant 50 OR 1117, the DFG grant RE 1462-6 and the DFG Transregio Programme TR33. References: Andreon, S., (2010) MNRAS, 407, p. 263; Balogh, M.L., Mazzotta, P., Bower, R.G., (2011) MNRAS, 412, p. 947; Balogh, M.L., McGee, S.L., Mok, A., (2014) MNRAS, 443, p. 2679; Behroozi, P.S., Wechsler, R.H., Conroy, C., (2013) ApJ, 770, p. 57; Berrier, J.C., Stewart, K.R., Bullock, J.S., (2009) ApJ, 690, p. 1292; Bertin, E., (2006) ASP Conf. Ser., 351, p. 112; Bertin, E., Arnouts, S., (1996) A&AS, 117, p. 393; Bielby, R.M., Gonzalez-Perez, V., McCracken, H.J., (2014) A&A, 568, p. A24; Biviano, A., Murante, G., Borgani, S., (2006) A&A, 456, p. 23; Bruzual, G., Charlot, S., (2003) MNRAS, 344, p. 1000; Chabrier, G., (2003) PASP, 115, p. 763; Clerc, N., Adami, C., Lieu, M., (2014) MNRAS, 444, p. 2723; Cole, S., Norberg, P., Baugh, C.M., (2001) MNRAS, 326, p. 255; Cortese, L., Gavazzi, G., Boselli, A., (2006) A&A, 453, p. 847; Coupon, J., Ilbert, O., Kilbinger, M., (2009) A&A, 500, p. 981; Cowie, L.L., Gardner, J.P., Hu, E.M., (1994) ApJ, 434, p. 114; Davis, M., Efstathiou, G., Frenk, C.S., White, S.D.M., (1985) ApJ, 292, p. 371; De Lucia, G., Blaizot, J., (2007) MNRAS, 375, p. 2; De Lucia, G., Weinmann, S., Poggianti, B.M., Arag{\'o}n-Salamanca, A., Zaritsky, D., (2012) MNRAS, 423, p. 1277; Dubinski, J., (1998) ApJ, 502, p. 141; Eckert, D., Molendi, S., Owers, M., (2014) A&A, 570, p. A119; Edge, A.C., (1991) MNRAS, 250, p. 103; Erben, T., (2012) AAS Meeting, 219. , 130.09; Giles, P.A., Maughan, B.J., Pacaud, F., (2016) A&A, 592, p. A3. , XXL Survey, III; Giodini, S., Pierini, D., Finoguenov, A., (2009) ApJ, 703, p. 982; Gonzalez, A.H., Sivanandam, S., Zabludoff, A.I., Zaritsky, D., (2013) ApJ, 778, p. 14; Gwyn, S.D.J., (2012) AJ, 143, p. 38; Heymans, C., Grocutt, E., Heavens, A., (2012) MNRAS, 427, p. 146; Hilton, M., Hasselfield, M., Sif{\'o}n, C., (2013) MNRAS, 435, p. 3469; Hinshaw, G., Larson, D., Komatsu, E., (2013) ApJS, 208, p. 19; Jarrett, T.H., Chester, T., Cutri, R., (2000) AJ, 119, p. 2498; Kelly, B.C., (2007) ApJ, 665, p. 1489; Kochanek, C.S., Pahre, M.A., Falco, E.E., (2001) ApJ, 560, p. 566; Kravtsov, A.V., Borgani, S., (2012) ARA&A, 50, p. 353; Kravtsov, A., Vikhlinin, A., Meshscheryakov, A., (2014) ApJ, , submitted [arXiv:1401.7329]; Leauthaud, A., Finoguenov, A., Kneib, J.-P., (2010) ApJ, 709, p. 97; Kron, R.G., (1980) ApJS, 43, p. 305; Laporte, C.F.P., White, S.D.M., Naab, T., Gao, L., (2013) MNRAS, 435, p. 901; Lidman, C., Suherli, J., Muzzin, A., (2012) MNRAS, 427, p. 550; Lin, Y.-T., Mohr, J.J., (2004) ApJ, 617, p. 879; Lin, Y.-T., Mohr, J.J., Stanford, S.A., (2003) ApJ, 591, p. 749; Lin, Y.-T., Mohr, J.J., Stanford, S.A., (2004) ApJ, 610, p. 745; Lin, Y.-T., Mohr, J.J., Gonzalez, A.H., Stanford, S.A., (2006) ApJ, 650, p. L99; Lieu, M., Smith, G.P., Giles, P.A., (2016) A&A, 592, p. A4. , XXL Survey, IV; Marmo, C., Bertin, E., (2008) ASP Conf. Ser., 394, p. 619; McCracken, H.J., Milvang-Jensen, B., Dunlop, J., (2012) A&A, 544, p. A156; McGee, S.L., Balogh, M.L., Bower, R.G., Font, A.S., McCarthy, I.G., (2009) MNRAS, 400, p. 937; Merritt, D., (1985) ApJ, 289, p. 18; Mulroy, S.L., Smith, G.P., Haines, C.P., (2014) MNRAS, 443, p. 3309; Muzzin, A., Yee, H.K.C., Hall, P.B., Lin, H., (2007) ApJ, 663, p. 150; Navarro, J.F., Frenk, C.S., White, S.D.M., (1997) ApJ, 490, p. 493; Okabe, N., Takada, M., Umetsu, K., Futamase, T., Smith, G.P., (2010) PASJ, 62, p. 811; Okabe, N., Smith, G.P., Umetsu, K., Takada, M., Futamase, T., (2013) ApJ, 769, p. LL35; Ostriker, J.P., Hausman, M.A., (1977) ApJ, 217, p. L125; Pacaud, F., Clerc, N., Giles, P.A., (2016) A&A, 592, p. A2. , XXL Survey, II; Patel, S.G., Kelson, D.D., Williams, R.J., (2015) ApJ, 799, p. L17; Pierre, M., Valtchanov, I., Altieri, B., (2004) J. Cosmol. Astropart. Phys., 9, p. 011; Pierre, M., Pacaud, F., Adami, C., (2016) A&A, 592, p. A1. , XXL Survey, I; Poggianti, B.M., (1997) A&AS, 122, p. 399; Poggianti, B.M., De Lucia, G., Varela, J., (2010) MNRAS, 405, p. 995; Ramella, M., Boschin, W., Geller, M., Mahdavi, A., Rines, K., (2004) ApJ, 128, p. 2022; Schlegel, D.J., Finkbeiner, D.P., Davis, M., (1998) ApJ, 500, p. 525; Smith, G.P., Khosroshahi, H.G., Dariush, A., (2010) MNRAS, 409, p. 169; Springel, V., Frenk, C.S., White, S.D.M., (2006) Nature, 440, p. 1137; {\v S}uhada, R., Song, J., Boehringer, H., (2012) A&A, 537, p. A39; Tanaka, M., Kodama, T., Kajisawa, M., (2007) MNRAS, 377, p. 1206; Van Der Burg, R.F.J., Muzzin, A., Hoekstra, H., (2014) A&A, 561, p. A79; White, S.D.M., (1976) MNRAS, 174, p. 19; White, S.D.M., Rees, M.J., (1978) MNRAS, 183, p. 341; Zabludoff, A.I., Mulchaey, J.S., (1998) ApJ, 496, p. 39; Zibetti, S., White, S.D.M., Schneider, D.P., Brinkmann, J., (2005) MNRAS, 358, p. 949; Ziparo, F., Braglia, F.G., Pierini, D., (2012) MNRAS, 420, p. 2480; Ziparo, F., Popesso, P., Biviano, A., (2013) MNRAS, 434, p. 3089",

year = "2016",

month = aug,

doi = "10.1051/0004-6361/201526792",

language = "English",

volume = "592",

journal = "Astronomy and Astrophysics",

issn = "00046361",

publisher = "EDP Sciences",

}

Ziparo, F, Smith, GP, Mulroy, SL, Lieu, M, Willis, JP, Hudelot, P, McGee, SL, Fotopoulou, S, Lidman, C, Lavoie, S, Pierre, M, Adami, C, Chiappetti, L, Clerc, N, Giles, P, Maughan, B, Pacaud, F & Sadibekova, T 2016, 'The XXL Survey: X. K -band luminosity - Weak-lensing mass relation for groups and clusters of galaxies', Astronomy and Astrophysics, vol. 592. https://doi.org/10.1051/0004-6361/201526792

TY - JOUR

T1 - The XXL Survey: X. K -band luminosity - Weak-lensing mass relation for groups and clusters of galaxies

AU - Ziparo, F.

AU - Smith, G.P.

AU - Mulroy, S.L.

AU - Lieu, M.

AU - Willis, J.P.

AU - Hudelot, P.

AU - McGee, S.L.

AU - Fotopoulou, S.

AU - Lidman, C.

AU - Lavoie, S.

AU - Pierre, M.

AU - Adami, C.

AU - Chiappetti, L.

AU - Clerc, N.

AU - Giles, P.

AU - Maughan, B.

AU - Pacaud, F.

AU - Sadibekova, T.

N1 - Export Date: 15 August 2017 CODEN: AAEJA Funding details: RE 1462-6, DFG, Deutsche Forschungsgemeinschaft Funding text: F.P. acknowledges support from the BMBF/DLR grant 50 OR 1117, the DFG grant RE 1462-6 and the DFG Transregio Programme TR33. References: Andreon, S., (2010) MNRAS, 407, p. 263; Balogh, M.L., Mazzotta, P., Bower, R.G., (2011) MNRAS, 412, p. 947; Balogh, M.L., McGee, S.L., Mok, A., (2014) MNRAS, 443, p. 2679; Behroozi, P.S., Wechsler, R.H., Conroy, C., (2013) ApJ, 770, p. 57; Berrier, J.C., Stewart, K.R., Bullock, J.S., (2009) ApJ, 690, p. 1292; Bertin, E., (2006) ASP Conf. Ser., 351, p. 112; Bertin, E., Arnouts, S., (1996) A&AS, 117, p. 393; Bielby, R.M., Gonzalez-Perez, V., McCracken, H.J., (2014) A&A, 568, p. A24; Biviano, A., Murante, G., Borgani, S., (2006) A&A, 456, p. 23; Bruzual, G., Charlot, S., (2003) MNRAS, 344, p. 1000; Chabrier, G., (2003) PASP, 115, p. 763; Clerc, N., Adami, C., Lieu, M., (2014) MNRAS, 444, p. 2723; Cole, S., Norberg, P., Baugh, C.M., (2001) MNRAS, 326, p. 255; Cortese, L., Gavazzi, G., Boselli, A., (2006) A&A, 453, p. 847; Coupon, J., Ilbert, O., Kilbinger, M., (2009) A&A, 500, p. 981; Cowie, L.L., Gardner, J.P., Hu, E.M., (1994) ApJ, 434, p. 114; Davis, M., Efstathiou, G., Frenk, C.S., White, S.D.M., (1985) ApJ, 292, p. 371; De Lucia, G., Blaizot, J., (2007) MNRAS, 375, p. 2; De Lucia, G., Weinmann, S., Poggianti, B.M., Aragón-Salamanca, A., Zaritsky, D., (2012) MNRAS, 423, p. 1277; Dubinski, J., (1998) ApJ, 502, p. 141; Eckert, D., Molendi, S., Owers, M., (2014) A&A, 570, p. A119; Edge, A.C., (1991) MNRAS, 250, p. 103; Erben, T., (2012) AAS Meeting, 219. , 130.09; Giles, P.A., Maughan, B.J., Pacaud, F., (2016) A&A, 592, p. 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PY - 2016/8

Y1 - 2016/8

N2 - Galaxy clusters and groups are important cosmological probes and giant cosmic laboratories for studying galaxy evolution. Much effort has been devoted to understanding how and when baryonic matter cools at the centre of potential wells. However, a clear picture of the efficiency with which baryons are converted into stars is still missing. We present the K-band luminosity-halo mass relation, LK,500-M500,WL, for a subsample of 20 of the 100 brightest clusters in the XXL Survey observed with WIRCam at the Canada-France-Hawaii Telescope (CFHT). For the first time, we have measured this relation via weak-lensing analysis down to M500,WL = 3.5 × 1013 MȮ. This allows us to investigate whether the slope of the LK-M relation is different for groups and clusters, as seen in other works. The clusters in our sample span a wide range in mass, M500,WL = 0.35-12.10 × 1014 MȮ, at 0 < z < 0.6. The K-band luminosity scales as log 10(LK,500/ 1012 LȮ) ? βlog 10(M500,WL/ 1014 MȮ) with β = 0.85+0.35 -0.27 and an intrinsic scatter of σlnLKM = 0.37+0.19 -0.17. Combining our sample with some clusters in the Local Cluster Substructure Survey (LoCuSS) present in the literature, we obtain a slope of 1.05+0.16 -0.14 and an intrinsic scatter of 0.14+0.09 -0.07. The flattening in the LK-M seen in previous works is not seen here and might be a result of a bias in the mass measurement due to assumptions on the dynamical state of the systems. We also study the richness-mass relation and find that group-sized halos have more galaxies per unit halo mass than massive clusters. However, the brightest cluster galaxy (BCG) in low-mass systems contributes a greater fraction to the total cluster light than BCGs do in massive clusters; the luminosity gap between the two brightest galaxies is more prominent for group-sized halos. This result is a natural outcome of the hierarchical growth of structures, where massive galaxies form and gain mass within low-mass groups and are ultimately accreted into more massive clusters to become either part of the BCG or one of the brighter galaxies. © ESO, 2016.

AB - Galaxy clusters and groups are important cosmological probes and giant cosmic laboratories for studying galaxy evolution. Much effort has been devoted to understanding how and when baryonic matter cools at the centre of potential wells. However, a clear picture of the efficiency with which baryons are converted into stars is still missing. We present the K-band luminosity-halo mass relation, LK,500-M500,WL, for a subsample of 20 of the 100 brightest clusters in the XXL Survey observed with WIRCam at the Canada-France-Hawaii Telescope (CFHT). For the first time, we have measured this relation via weak-lensing analysis down to M500,WL = 3.5 × 1013 MȮ. This allows us to investigate whether the slope of the LK-M relation is different for groups and clusters, as seen in other works. The clusters in our sample span a wide range in mass, M500,WL = 0.35-12.10 × 1014 MȮ, at 0 < z < 0.6. The K-band luminosity scales as log 10(LK,500/ 1012 LȮ) ? βlog 10(M500,WL/ 1014 MȮ) with β = 0.85+0.35 -0.27 and an intrinsic scatter of σlnLKM = 0.37+0.19 -0.17. Combining our sample with some clusters in the Local Cluster Substructure Survey (LoCuSS) present in the literature, we obtain a slope of 1.05+0.16 -0.14 and an intrinsic scatter of 0.14+0.09 -0.07. The flattening in the LK-M seen in previous works is not seen here and might be a result of a bias in the mass measurement due to assumptions on the dynamical state of the systems. We also study the richness-mass relation and find that group-sized halos have more galaxies per unit halo mass than massive clusters. However, the brightest cluster galaxy (BCG) in low-mass systems contributes a greater fraction to the total cluster light than BCGs do in massive clusters; the luminosity gap between the two brightest galaxies is more prominent for group-sized halos. This result is a natural outcome of the hierarchical growth of structures, where massive galaxies form and gain mass within low-mass groups and are ultimately accreted into more massive clusters to become either part of the BCG or one of the brighter galaxies. © ESO, 2016.

KW - Galaxies: clusters: general

KW - Galaxies: groups: general

KW - Galaxies: photometry

KW - Galaxies: stellar content

KW - Gravitational lensing: weak

KW - X-rays: galaxies: clusters

KW - Cosmology

KW - Luminance

KW - Surveys

KW - Galaxies: clusters: General

KW - Galaxies: groups: generals

KW - X rays: galaxies: clusters

KW - Galaxies

U2 - 10.1051/0004-6361/201526792

DO - 10.1051/0004-6361/201526792

M3 - Article

SN - 00046361

VL - 592

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

ER -

The XXL Survey: X. K -band luminosity - Weak-lensing mass relation for groups and clusters of galaxies

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Birmingham Astrophysics : Consolidated Grant 2013-2016

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