Clustering studies of ROSAT/SDSS AGN through cross-correlation functions with SDSS Galaxies
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1 Clustering studies of ROSAT/SDSS AGN through cross-correlation functions with SDSS Galaxies Mirko Krumpe (ESO, UCSD) Collaborators: Takamitsu Miyaji (UNAM-E, UCSD), Alison L. Coil (UCSD), Hector Aceves (UNAM-E), Bernd Husemann (ESO, AIP)
2 Motivation Status before 2009: bias of broad-line AGN well-known at high z evolution with redshift remains unclear measure bias of BL AGN at low redshifts! use cross-correlation measurements with galaxies in a large volume However: low number density of broad-line AGN at low z 2
3 Outline Use ROSAT/SDSS clustering measurements to precisely constrain M DHM at low z (Krumpe et al. 2010) Expand the method to lower and higher redshifts and optically selected SDSS AGN (Krumpe et al. 2012) Explore clustering dependence in respect to M BH and/or L/L EDD (Krumpe et al. in prep.) 3
4 Method correlation function 4 separation in Mpc ξ ACF(AGN) = ξ 2 CCF(AGN-Gal.) / ξ ACF(Gal.) (Coil et al. 2009)
5 ROSAT All-Sky Survey/SDSS AGN sample still the most sensitive all-sky (soft) X-ray survey, with ~110,000 sources (Voges et al. 1999) 6224 broad-line AGN with spectroscopic redshifts from SDSS Credits: ROSAT mission/mpe (Anderson et al. 2003, 2007) L X ~ erg s -1 5
6 Cross-correlating galaxy sample requirements for tracer set: high number density (>> AGN) & well-defined and replicable selection SDSS luminous red galaxies X-ray AGN 0.16<z<
7 Large-scale bias Clustering strength of low-z AGN red galaxies blue galaxies red luminous galaxies total RASS AGN sample (X-ray selected) low L X RASS AGN sample high L X RASS AGN sample redshift (Krumpe et al. 2010) 7
8 Taking the next steps extend to higher and lower redshifts (z= ) X-ray and optically selected AGN samples AGN sample selection: radio-quiet, optical without X-ray counterparts, radio-quiet and no X-ray AGN, X-ray no optical narrow line X-ray selected AGN Krumpe et al. (2012) 8
9 SDSS AGN sample Credits: SDSS area map of SDSS DR7 spectroscopic footprint ~18 candidates per deg 2 105,783 broad-line AGN fainter than i~15 mag M i brighter than -22 mag (Schneider et al. 2010, Richards et al. 2002) 9
10 Cross-correlating galaxy samples requirements for tracer set: high number density (>> AGN) & well-defined and replicable selection SDSS very luminous red galaxies X-ray/optical AGN 0.36<z<0.50 SDSS luminous red galaxies X-ray/optical AGN 0.16<z<0.36 SDSS main galaxies X-ray/optical AGN 0.07<z<
11 Large-scale bias X-ray vs. optically selected AGN X-ray selected AGN (high z) Optically selected AGN (high z) ROSAT AGN (auto-correlation function) total RASS AGN sample (X-ray) total SDSS AGN sample (optical) narrow-line RASS AGN sample (X-ray) redshift (Krumpe et al. 2012) 11
12 General picture of AGN clustering over cosmic time AGN reside in M DHM ~ M SUN low redshift (z<0.5) broad-line and narrow-line cluster like L galaxies or a small galaxy group of ~L no statistically convincing difference in the clustering of X-ray and optically selected broad-line AGN weak luminosity dependence of the clustering for broad-line AGN (high L X AGN cluster higher similar to red galaxies) high redshift X-ray selected AGN appear to cluster more strongly than optically selected AGN real? why: different populations, different luminosities? 12
13 Origin of the weak L X dependence of the broad-line AGN clustering strengths at low z 13
14 Motivation Krumpe et al. in prep. Galaxy clustering measurements: clustering strength depends on galaxy properties (e.g., luminosity, morphological type, stellar mass) more luminous more clustered more massive dark matter halos (DMHs) AGN clustering measurements: constraints on theoretical models of AGN triggering, AGN host galaxy properties & cosmological parameters Do AGN properties correlate with clustering strength? 14
15 log L X [erg s -1 ] AGN luminosity dependence of the clustering Mirko Krumpe AGN 2014 workshop, ESO, July Krumpe et al. (2010): more X-ray luminous AGN cluster more strongly (larger M DMH ) than lowerluminosity counterparts Cause of the luminosity dependence of the clustering X-ray luminosity depends on: M BH and L/L EDD Krumpe et al. (in prep.): redshift explore physical origin of clustering dependence caused by M BH or/and L/L EDD?
16 What is predicted? 16 Booth & Schaye (2010): cosmological simulations: M BH ~M DMH use AGN clustering measurements to test predictions
17 flux flux Determine M BH for the RASS/SDSS AGN sample Hα bandpass see Denney et al. (2009) Cause of the luminosity dependence of the clustering fit the Hα line profile Mirko Krumpe wavelength determine Hα-FWHM & L Hα convert to Hβ-FWHM & L 5100 (Geene & Ho 2005) AGN 2014 workshop, ESO, July 2014 M BH 17
18 Mirko Krumpe M BH - L/L EDD plane AGN 2014 workshop, ESO, July <z<0.36 L/L EDD = 1.26 x M BH /M SUN erg/s
19 Mirko Krumpe Unbiased split distributions AGN 2014 workshop, ESO, July same L / L EDD distribution only within each L/L EDD bin, split distributions of M BH values
20 HOD slope α 21 Main Result: M BH correlates weakly with M DMH low vs high L X low vs high M BH low vs high L/L EDD minimum DMH mass to host an AGN: log M [h -1 M SUN ] difference is more prominent in 2D parameter space
21 Theory vs. Observation 22 Booth & Schaye (2010) Millennium Sim., Springel et al. (2005) reasonable agreement
22 Consequences At the luminosity and redshift range studied: (BL AGN; L X ~ erg s -1 ; 0.16<z<0.36) NO correlation with L/L EDD : higher densities of galaxies/larger DMH masses do NOT cause more accretion of matter Correlation with M BH : high X-ray luminosity AGN do not require dense environments mergers play only a minor role in the accretion process 23
23 Conclusions we accurately measure the clustering of X-ray and optically selected AGN at low redshift through CCFs (Krumpe et al. 2010, 2012) Broad-line, luminous AGN (z= ): No statistically convincing difference between: X-ray, optically selected, radio-quiet AGN weak L X dependence of the clustering strength L X dependence of the clustering strength is mainly caused by a dependence on M BH more results of the project will be presented in T. Miyaji s talk 24
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