statistical properties of radio galaxies in the local universe
DESCRIPTION
Statistical Properties of Radio Galaxies in the local Universe. Yen-Ting Lin Princeton University Pontificia Universidad Católica de Chile Yue Shen, Michael Strauss, Ragnhild Lunnan (Princeton), Zheng Zheng (IAS). outline. motivations science goals - PowerPoint PPT PresentationTRANSCRIPT
Statistical Properties of Radio Galaxies in the local
Universe
Yen-Ting LinPrinceton University
Pontificia Universidad Católica de ChileYue Shen, Michael Strauss, Ragnhild Lunnan (Princeton), Zheng Zheng (IAS)
outline
• motivations• science goals
– consensus of radio galaxies (RGs) hosted by massive galaxies in the local universe (z0.3)
– formation mechanism of RGs– identification of interesting objects for detailed study
• the sample• several statistics to look at
– relationship with radio-quiet (RQ) population– dependence on the environment
motivation: to make the bright end of the luminosity function
right
Croton et al (2006)
motivation: SZ surveys are happening!
credit: CXO
Carlstrom et al (2002)
Atacama Cosmology Telescope in construction
see Lin et al (0805.1750) for estimation of effects of radio sources on SZ signal
• using NYU-VAGC DR6 LSS galaxy sample as parent sample, containing ~220,000 galaxies down to Mr–20.5 (about M*)
• cross-matched with NVSS and FIRST surveys at 1.4 GHz to generate the largest radio galaxy catalog to date: 10,500 RGs stronger than 3mJy
• improvements over previous studies– construction of several volume-limited subsamples– 90% of RGs have measured redshift– all RGs visually inspected to secure matches and measurement
of fluxes– morphology information of radio sources– high S/N measurement of correlation functions– halo occupation distribution (HOD) modeling
the sample
bivariate luminosity function
whole sample M-20.5 volume-limited M-21.5 volume-limited
optical luminosity function
• 0.02z0.132• 108,873 galaxies• 2,253 RGs• 2.1% of galaxies
more luminous than M* have radio power logP23.12
• fiber collision correction applied
correlation function
• both galaxies and RGs are volume-limited and subject to same optical luminosity cut (Mr–21.5)
• RGs (red) more strongly clustered than galaxies (blue)
• clustering length comparable to groups of galaxies (~10h-1Mpc)
correlation function: HOD modeling
• consider NRG=NRG,cen+NRG,sat
• NRG,cen=1 if(MMmin)• NRG,sat=(M/M1)
• HOD modeling suggests RGs are hosted by halos more massive than 1013 Msun (consistent with lensing results from Mandelbaum et al 2008)
RGs in massive halos: halo occupation number
• count galaxies and RGs at Mr–20.5 in 134 X-ray clusters from ROSAT all-sky survey
• number of galaxies goes as M0.8
• occupation number of RGs not a strong function of cluster mass
• 1435 galaxies, 85 RGs (~6%)• 62/134 (=46%) clusters host
RGs• among these, 34 have RL BCGs• 44 clusters host only 1 RG, 20 of
these are BCG• 25% of BCGs are RL• 3.9% of non-BCG galaxies are
RL• NOTE: 2.1% of galaxies are RL
globally BCGs
clusters w/o RGs
RGs in massive halos: spatial distribution
RGs in dense regions
• excess number of neighbors– 1000 RGs, 1000 RQ
galaxies matched to optical luminosity, apparent magnitude, and redshift
– count nearby objects out to 2 Mpc from SDSS photometric catalog, within –23.5Mr–20.5
– within ~0.5 Mpc, RL galaxies always have higher number of neighbors than RQ ones
Mpc
RGs in dense regions
no RLAGN–SF galaxy pairs atscales<1Mpc!
caution: small number ofSF galaxies in the sample!
summary
• observations:– given optical luminosity and color, RGs are more strongly clustered
than the corresponding RQ galaxy sample
– large scale clustering implies hosts are group or cluster-sized halos
– RGs very centrally concentrated towards halo center
• ingredients for RL AGN phenomenon– dense environment
– presence of intracluster/intragroup gas: confining pressure
– low level supply of gas: what’s the source?
• work in progress– dissection of the bivariate LF
– environment of high and low-excitation RL AGNs (e.g., FRI vs FRII)
– relationship with X-ray and optical AGNs