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P h o t o z z=0.8 z=0.6 z=0.4 z=0.2 I AB <25 1.4Mio galaxies X-ray contours

P h o t o z z=0.8 z=0.6 z=0.4 z=0.2 I AB <25 1.4Mio galaxies X-ray contours. X-ray galaxy groups in zCOSMOS. Alexis Finoguenov MPE/UMBC +zCOSMOS team. X-ray+red sequence: 278 Xray+spectroscopy: 195 z<0.8 152/175 91% 0.8<z<1 37/50 74% z>1 6/53 11%. N(z)=>2.

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P h o t o z z=0.8 z=0.6 z=0.4 z=0.2 I AB <25 1.4Mio galaxies X-ray contours

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  1. Photoz z=0.8 z=0.6 z=0.4 z=0.2 IAB<25 1.4Mio galaxies X-ray contours

  2. X-ray galaxy groups in zCOSMOS Alexis Finoguenov MPE/UMBC +zCOSMOS team

  3. X-ray+red sequence: 278 Xray+spectroscopy: 195 z<0.8 152/175 91% 0.8<z<1 37/50 74% z>1 6/53 11% N(z)=>2 View on baryons from COSMOS

  4. X-ray only groups View on baryons from COSMOS

  5. How X-ray groups are different from spectroscopic groups? Spec. completeness is better at low z But drops faster with redshift

  6. Comparison of a group definition X-ray only Spec-z groups with X-rays Spec-z 3 member groups, no X-rays: stacked X-ray signal @<2.e-16> @z>0.8 X-rays (`a 6.e-16 cgs) are more sensitive group tracer compared to IAB<22.5 galaxies Inside dense LSS Fraction of X-ray groups increases by a factor of 2 View on baryons from COSMOS

  7. Stacked X-ray detection of Knobel groups View on baryons from COSMOS

  8. Stacked detection of spectro-z groups

  9. Lx-sigma relation View on baryons from COSMOS

  10. LSS at 0.12, 0.22, 0.34, 0.37, 0.51, 0.73, 0.89 (Optical groups:0.22,0.36,0.38) K.Kovac

  11. Resolving LSS with X-ray groups View on baryons from COSMOS

  12. Fraction of matter resolved in groups Simulations… A. Faltenbacher, AF, N. Drory 2010 ApJ

  13. Environmental dependence of galaxy mass function View on baryons from COSMOS

  14. No change in HOD! View on baryons from COSMOS

  15. Bump in galaxy mass function:centrals vs sattelites View on baryons from COSMOS

  16. Conclusions • X-ray groups approach the status of being spectroscopically confirmed. • X-ray groups are not a subsample of spectroscopic groups • Groups are tracers of density field and can be used to overcome to sample variance. View on baryons from COSMOS

  17. People involved • Masayuki Tanaka – properties of galaxies in X-ray groups using zCOSMOS • Stefania Giodini– HOD of galaxies, galaxy mass function, fossil groups • Alexie Leauthaud– properties of BCGs • Berian James – conditional mass function – modeling • Andreas Faltenbacher – conditional mass function – simulations • Katarina Kovac – density fields • Angela Iovino, MicholBolzonella, Olga Cucciatti – properties of galaxies • Viola Allevato(my PhD student) – clustering analysis • Michael Ballogh – 10 groups at z~0.9 with Gemini • Masayuki Tanaka – groups at z>1 with Subaru • Mara Salvato – high-z clusters • Simona Mei et al. FORS2 program – already 350 redshifts for groups added (or 30% of total number) • And likely you! (a number of on-going efforts!) View on baryons from COSMOS

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