Background Picture: Millennium Simulation (MPA); Spectrum-Roentgen-Gamma satellite (P. Predehl 2011)

Transcription

1 By Collaborators Alex Kolodzig (MPA) Marat Gilfanov (MPA,IKI), Gert Hütsi (MPA), Rashid Sunyaev (MPA,IKI) Publications Kolodzig et al. 2013b, A&A, 558, 90 (ArXiv : ) Hüsti et al. 2014, submitted (ArXiv: ) At Clustering Measurements of AGN, ESO, Garching, Germany, Background Picture: Millennium Simulation (MPA); Spectrum-Roentgen-Gamma satellite (P. Predehl 2011)

2 X-ray surveys of the last ~2 decades ROSAT Average XMM-Newton Poles Chandra Figure by Brandt & Hasinger erass: new era of LSS studies - Kolodzig et al. - Clustering with AGN, ESO,

3 Large-scale structure studies in X-rays Krumpe+2012 ROSAT LSS studies: # of AGN Area [deg 2 ] Depth Krumpe+2012 ~3 500 ~5 500 z < 0.5 Allevato+2011 ~600 ~2 z~1 erass ~ z~1.0 Poles erass XMM-Newton Chandra Allevato+2011 Figure by Brandt & Hasinger erass: new era of LSS studies - Kolodzig et al. - Clustering with AGN, ESO,

4 Large-scale structure studies in X-rays Krumpe+2012 ROSAT LSS studies: # of AGN Area [deg 2 ] Depth Krumpe+2012 ~3 500 ~5 500 z < 0.5 Allevato+2011 ~600 ~2 z~1 erass ~ z~1.0 erass XMM-Newton erass: # of AGN Area [deg 2 ] Depth SPIDERS (brightest ~30%) > ~2 500 z~0.8 4MOST (brightest ~60%) Allevato+2011 ~ z~0.9 Chandra Figure by Brandt & Hasinger erass: new era of LSS studies - Kolodzig et al. - Clustering with AGN, ESO,

5 erass: predicted redshift distribution Peak(Median): L * ~ erg/s 10%: >10 45 erg/s Peak: ~0.8 ~0.7 ~0.5 Median ~1.0 ~0.9 ~0.8 XLF of Hasinger erass: new era of LSS studies - Kolodzig et al. - Clustering with AGN, ESO,

6 Tools of erass for LSS studies AGN as phase of galaxy evolution: X-ray Luminosity Function (see Kolodzig et al. 2013a): AGN evolution accretion history of SMBHs Clustering strength (linear bias factor): AGN environment AGN triggering mechanism SMBH co-evolution with dark matter halo AGN as cosmological probe: Baryonic acoustic oscillations (BAOs) independent constrains on cosmological parameters erass: new era of LSS studies - Kolodzig et al. - Clustering with AGN, ESO,

7 Clustering Model

8 Our Clustering Model Based on Hütsi, Gilfanov & Sunyaev 2012: Angular Power Spectrum: Assumptions: Mass of dark matter halo (DMH) of AGN hosts: (e.g. Allevato et al. 2011, Krumpe et al. 2012, Mountrichas et al. 2013) M DMH,eff = M /h -> bias b(z, M DMH,eff ) X-ray Luminosity Function of Hasinger et al ( kev) for flux-cut and redshift-evolution -> selection function (z) (LDDE model, with redshift cutoff of Brusa et al at z>2.7) Cosmology: flat CDM, Ω = 0.7, Ω m = 0.3, Ω b = 0.05, h = 0.7, 8 = 0.8 Assume: redshifts are known! C 2 lin ( ) 2 P k W ( k, z) k dk DM z ( ) ( W ( k, z) j k r( z) g( ) b z z) dz growth factor erass: new era of LSS studies - Kolodzig et al. - Clustering with AGN, ESO,

9 predicted angular power spectrum - C l full erass AGN sample (0 < z < 5) shot noise level C 2 1 C (2 1), fsky N zmin zmax linear regime cut Kolodzig et al. 2013b erass: new era of LSS studies - Kolodzig et al. - Clustering with AGN, ESO,

10 predicted angular power spectrum - C l Kolodzig et al. 2013b erass: new era of LSS studies - Kolodzig et al. - Clustering with AGN, ESO,

11 Clustering Strength (Linear Bias Factor)

12 Clustering Strength vs. redshift Extragal.Sky deg 2 Kolodzig+2013b deg 2 S/N of 7:1 3 high S/N (>10) for wide z-range and small sky fraction erass: new era of LSS studies - Kolodzig et al. - Clustering with AGN, ESO,

13 Clustering Strength vs. redshift Extragal.Sky adopted from Kolodzig+2013b Brightest 60% Brightest 60% deg deg 2 3 brightest 60% (4MOST-case) and deg 2 : good S/N ( 3) up to z~ erass: new era of LSS studies - Kolodzig et al. - Clustering with AGN, ESO,

14 Clustering Strength vs. redshift Extragal.Sky adopted from Kolodzig+2013b Brightest 60% Brightest 60% deg deg 2 3 Brightest 30% (SPIDERS-case) brightest 30% (SPIDERS-case) and deg 2 : good S/N ( 3) up to z~ erass: new era of LSS studies - Kolodzig et al. - Clustering with AGN, ESO,

15 Clustering Strength vs. redshift 4MOST-case: brightest 60% of erass AGN, deg 2 3 adopted from Kolodzig+2013b 1 st time: accurate luminosity and redshift resolved studies studies of dark-matter-halo mass of AGN to unprecedented detail 1 st time: statistically meaningful sample of AGN with L X > erg/s comparison with optical quasar-studies possible erass: new era of LSS studies - Kolodzig et al. - Clustering with AGN, ESO,

16 Clustering Strength Measurements - state of the art Fanidakis et al erass: new era of LSS studies - Kolodzig et al. - Clustering with AGN, ESO,

17 Small scales: HOD modeling possible 100 deg 2 Extragal.Sky Average: ~80 AGN/deg 2 Ecliptic Poles: >400 AGN/deg 2 Richardson et al erass: new era of LSS studies - Kolodzig et al. - Clustering with AGN, ESO,

18 Baryonic Acoustic Oscillations (BAOs)

19 BAOs beyond z>0.8 Redshift-Range: 0.8 < z < 2.0 so far no detection best tracers: AGN, QSOs and emission line galaxies (ELGs) planned galaxy surveys: Weinberg et al erass ( ): AGN ~34 kdeg 2 (4MOST: 14 kdeg 2 ) Dedicated optical BAO surveys: eboss ( ): ELGs ~1.5 kdeg 2, QSOs ~7.5 kdeg 2 DESI (BigBOSS) (>2020): ELGs ~14 kdeg erass: new era of LSS studies - Kolodzig et al. - Clustering with AGN, ESO,

20 BAOs with erass AGN sample Extragal.Sky 0.0<z<3.0 CL~14 (full erass AGN sample) 0.8<z<2.0 CL~11 (uncharted z-range) deg 2 0.8<z<2.0 CL~5 Brightest 60% 0.8<z<2.0 CL~4 (4MOST-case) 1 st convincing detection with X-ray selected AGN Kolodzig+2013b, Hüsti+2014 (submitted) erass: new era of LSS studies - Kolodzig et al. - Clustering with AGN, ESO,

21 Comparison with dedicated BAO surveys 4MOST 0.8<z<2.0 20kdeg 2 (erass AGN, brightest 60%) eboss QSO 1.0<z< kdeg 2 BOSS LRG 0.4<z<0.7 10kdeg 2 HETDEX L E 1.9<z< deg 2 eboss ELG 0.6<z< kdeg 2 adopted from Kolodzig+2013b 1 st peak 2 nd peak comparable with dedicated BAO surveys due to large sky coverage of erass (spec-z for Extragal.Sky) erass: new era of LSS studies - Kolodzig et al. - Clustering with AGN, ESO,

22 We need redshifts! For clustering strength & XLF: Required Accuracy: z ~ 0.10 at z~1 photo-z sufficient Required photometry: ugrizyjhk-bands or more (Salvato et al. 2011) Or narrow bands as for J-PAS Optimal photo-z suppliers: J-PAS ( ): ~8.5 kdeg 2, ~ counterparts (I AB = 22.5 mag) Current/future photo-z suppliers: SDSS: ~14 kdeg 2, ~10 6 counterparts (I AB = 21.3 mag), ugriz-bands Pan-STARRS PS1: ~30 kdeg 2, > counterparts, griz-bands Euclid ( ): ~15 kdeg 2 ( b >30 ), YJH-Bands LSST (>2019): ~20 kdeg 2, ugrizy-bands Problems with reliability of photo-z (Salvato et al. 2011) Spec-z suppliers: SPIDERS: ~2.5 kdeg 2, ~ spectra 4MOST (>2020): ~14 kdeg 2, ~ spectra erass: new era of LSS studies - Kolodzig et al. - Clustering with AGN, ESO,

23 We need redshifts! Accuracy requirements for BAO detection fraction of catastrophic failures: f fail ~5 ~14 ~8 Full Sky 0.8 < z < 2.0 Photo-z Accuracy: 0 = z /(1+z) Hüsti et al. 2014, submitted, ArXiv: see for other X-ray survey strategies erass: new era of LSS studies - Kolodzig et al. - Clustering with AGN, ESO,

24 We need redshifts! For 3 detection of BAOs with erass AGN: Required Accuracy (Extragal.Sky): Required Size (for spec-z): deg 2 Potential suppliers: J-PAS ( ): ~8.5 kdeg 2, ~ counterparts ~3 with 0 ~ 0.01 (f fail = 0.0) 4MOST (>2020): ~14 kdeg 2, ~ spectra ~ erass: new era of LSS studies - Kolodzig et al. - Clustering with AGN, ESO,

25 Summary AGN sample of erosita/srg All-Sky Survey: New era of large-scale structure studies with AGN Clustering strength: >10% accuracy for wide z-range for deg 2 ; SPIDERS: >30% up to z~2 1 st time: Luminosity & redshift resolved studies of dark-matter-halo mass of AGN up to z~3 1 st time: comparison with optical quasar studies (for L X > erg/s) Baryonic Acoustic Oscillations: 1 st time: convincing detection with X-ray selected AGN possible ~11 for extragalactic sky & uncharted region: 0.8<z<2.0 ; 4MOST ~4 Comparable with dedicated optical surveys Remarks: We rely on large & deep photometric & spectroscopic follow-up surveys Cross-correlation with other galaxy types (e.g. ELGs) might have even better statistics For details see: Kolodzig et al. 2013b, A&A 558, 90 (ArXiv: ) Hüsti et al. 2014, submitted (ArXiv: ) alex@mpa-garching.mpg.de erass: new era of LSS studies - Kolodzig et al. - Clustering with AGN, ESO,