Using X-ray Clusters as Cosmological Probes Hans Bhringer - - PowerPoint PPT Presentation

▶
using x ray clusters as cosmological probes
SMART_READER_LITE
LIVE PREVIEW

Using X-ray Clusters as Cosmological Probes Hans Bhringer - - PowerPoint PPT Presentation

Dec 20, 2022 221 likes •455 views

Using X-ray Clusters as Cosmological Probes Hans Bhringer Max-Planck-Institut fr extraterrestrische Physik (MPE) in collaboration with Gayoung Chon (MPE) Hans Bhringer ICM Conference, MPA

slide-1
SLIDE 1

Hans Böhringer ICM Conference, MPA 15.6. 2015 1

Using X-ray Clusters as Cosmological Probes

Hans Böhringer

  • Max-Planck-Institut für extraterrestrische Physik (MPE)
  • in collaboration with Gayoung Chon (MPE)
slide-2
SLIDE 2

Hans Böhringer ICM Conference, MPA 15.6. 2015 2

Testing cosmological models with the statistics of LSS


Different LSS for different cosmological models SCDM Ωm=1 τCDM Ωm=1 ΛCDM Ωm=0.3 ΩΛ=0.7 OCDM Ωm=0.3

MPA , Garching & Virgo Consortium

slide-3
SLIDE 3

Hans Böhringer ICM Conference, MPA 15.6. 2015 3

Some of the most regular and most structured galaxy clusters

  • f the REXCESS sample
  • a representative sample for X-

ray surveys

  • Böhringer et al. 2007

Morphological variation of clusters

slide-4
SLIDE 4

LX - M relation for REXCESS clusters

  • Hans Böhringer ICM Conference, MPA 15.6. 2015

4

M estimated from YX

  • scatter ~ 40% scatter ~ 18%
  • Pratt, H.B., et al. 2009
slide-5
SLIDE 5

Predicted Cluster Luminosity Function


with parameter dependence

  • Hans Böhringer ICM Conference, MPA 15.6. 2015

5

Sensitive dependence on σ8 and Ωm

  • var. Ωm
  • var. σ8

background cosmology structure formation P(k) mass function (Tinker) LX-mass scaling relation X-ray luminosity function

slide-6
SLIDE 6
  • Combined REFLEX & NORAS Survey
  • LX

redshift

  • Extragal. ALL-SKY RASS Survey

REFLEX II 915 clusters NORAS II 882 clusters F > 1.8 10-12 erg s-1 cm-2

  • REFLEX I: 18 runs La Silla

REFLEX II: 9 runs ESO 3.6m/NTT NORAS 11 runs C.A. 2 runs K.P.

Sample descriptions: Böhringer et al. 2000, 2001, 2004, 2013, 2014, 2015 in prep Chon & Böhringer 2012

6

882 915

slide-7
SLIDE 7

Hans Böhringer ICM Conference, MPA 15.6. 2015 7

Observed and predicted X-ray luminosity function

Prediction from a flat ΛCMD model Ωm = 0.27 , σ8 = 0.80 and REFLEX II XLF

Böhringer et al. 2014

slide-8
SLIDE 8

Hans Böhringer ICM Conference, MPA 15.6. 2015 8

Cosmological constraints for two versions of the scaling relation: slope = 1.51 (solid line) 1.61 (dashed line)

Böhringer et al. 2014

slide-9
SLIDE 9

Hans Böhringer ICM Conference, MPA 15.6. 2015 9

Marginalized Constraints

slope = 1.51 +- 7% normalisation = 0.1175 +- 14%

Böhringer et al. 2014

Ωm σ8

slide-10
SLIDE 10

REFLEX II

Results from REFLEX II, the SDSS MaxBCG sample and from the 400 deg2 survey

Hans Böhringer ICM Conference, MPA 15.6. 2015 10

Rozo et al. 2010 Vikhlinin et al. 2009 local sample: 49 clusters at <z> = 0.05

slide-11
SLIDE 11

REFLEX and PLANCK cluster and PLANCK and WMAP CMB constraints

Hans Böhringer ICM Conference, MPA 15.6. 2015 11

Planck Collaboration 2013 Böhringer et al. 2014 Hinshaw et al. 2013

slide-12
SLIDE 12

Hans Böhringer ICM Conference, MPA 15.6. 2015 12

  • Effect of massive neutrinos
slide-13
SLIDE 13

Hans Böhringer ICM Conference, MPA 15.6. 2015 13

Constraints on As and Ωm for Mν = 0, 0.17, 0.4, 0.6 eV

Böhringer & Chon 2015 Formal consistency for Mν = 0.45 +- 0.28 eV

slide-14
SLIDE 14

Hans Böhringer ICM Conference, MPA 15.6. 2015 14

  • Local Cosmography
slide-15
SLIDE 15

Hans Böhringer ICM Conference, MPA 15.6. 2015 15

REFLEX Cluster Density Distribution as Function of Redshift

Böhringer et al. 2014

slide-16
SLIDE 16

Hans Böhringer ICM Conference, MPA 15.6. 2015 16

REFLEX Cluster Density Distribution at z < 0.06

  • Böhringer et al 2014
slide-17
SLIDE 17

Hans Böhringer ICM Conference, MPA 15.6. 2015 17

Whitbourn & Shanks 2014

  • (see also Keenan et l. 2012)

Local Underdensity in the Galaxy Distribution in the South Galactic Cap

slide-18
SLIDE 18

Hans Böhringer ICM Conference, MPA 15.6. 2015 18

REFLEX Cluster Density Distribution in the North and South Galactic Cap (in the Southern Sky)

  • South galactic cap region North galactic cap region in South

Böhringer et al. 2014

slide-19
SLIDE 19

Hans Böhringer ICM Conference, MPA 15.6. 2015 19

  • Prospects for

Cluster Surveys

slide-20
SLIDE 20

Han 20

Characterization of Clusters in X-rays with RASS

hard image (0.5 – 2 keV ) soft (0.1 – 0.4 keV) smoothed hard image 1’ & 2’ Overlay over DSS image Source extent Growth curve in hard band

slide-21
SLIDE 21

Hans Böhringer ICM Conference, MPA 15.6. 2015 21

Simulated eROSITA Survey Fields

1.9 x 1.2 deg

  • top: 2.2 ks

(mean Survey)

  • bottom: 30 ks

(ecliptic poles)

slide-22
SLIDE 22

22

Results of cluster number forecast for different cosmological models

refer:w=-1 w = -1.3 w = -0.7

  • z > 0.4 41600 42300 43600
  • z > 0.8 4800 3900 6300
  • z > 1.2 490 327 830

fluctuation growth factor

  • w = −1, ±20%, ±50%

eROSITA number counts

Hans Böhringer ICM Conference, MPA 15.6. 2015

Chon & Böhringer 2013

slide-23
SLIDE 23

Hans Böhringer ICM Conference, MPA 15.6. 2015 23

Conclusions

  • Galaxy clusters are good probes for cosmology
  • to test cosmological models
  • to constrain the neutrino mass
  • to map the local LSS matter distribution
  • The success in constraining cosmological parameters

is limted by the imprecise knowledge of scaling relations and mass calibration

  • needs to be improved !!!
  • Ongoing and future surveys (XMM-Newton Surveys

and eROSITA) will add redshift dimension – understanding the high-z ICM will be very important