AGN Cosmology. a new perspective for VLTI in the E-ELT and LSST era. Sebastian F. Hoenig School of Physics & Astronomy / University of Southampton

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1 AGN Cosmology a new perspective for VLTI in the E-ELT and LSST era Sebastian F. Hoenig School of Physics & Astronomy / University of Southampton ESO January 2015

2 Extragalactic priorities in the 2020s Nature of Dark Energy v los ( 40/40) [km s 1 ] 0.200/0.200) 1.5 y [arcsec] (LSST and E-ELT primary Onken science et al. goals) σ los (80/130) [km s 1 ] h 4 ( 0.200/0.200) h 3 ( 0.200/0.200) h 4 ( 0.200/0.200) black holes masses / sphere of influence (E-ELT DRM science case) High-Z SN Search Team Supernova Cosmology Project 1.0 Both cases require precise distances Hubble diagram; absolute radii s of line-of-sight velocity (V los ), velocity dispersion (σ los ) and the third and fourth Gauss Hermite (GH) moments (h 3,h 4 )in0. 2 spaxels. The x,y aligned with the major and minor kinematic axes, respectively. The minimum and the maximum values of the color scale are indicated in the title n.5parenthesis (V1.0 los, σ los 1.5 in 1.5 km s ; h 3 0.5,h 4 in 0.0 dimensionless units). 1.5 The top row shows the original kinematical data while the bottom row shows the r it is bi-symmetrized. The Astrophysical Journal, 791:37(20pp),2014August10 Onken et al /0.200) h 4 ( 0.200/0.200) v los ( 40/ 40) v los ( 70/ 70) km/s 1.0 y [arcsec] y [arcsec] km/s parison of stellar velocity fields observed with the NIFS IFU (left) and SAURON IFU (right; Dumas et al. 2007). The AO-assisted NIFS data are ththegauss Hermite larger-scale velocity(gh) map, but dynamical moments probe a spatial (h 3,hregion 4 black )in0. inaccessible 2 spaxels. hole to the mass The optical x,y data measurement because the AGN emission in precludes measurements of the ynamics (the black region in the right panel). In both figures north is up and east is left. nd the maximum values of the color scale are indicated in the title NGC 4151 (Onken+14) hows the original kinematical data while the bottom row shows the in sensible results from an axisymmetric dynamical constraints on the mass-to-light ratio (ϒ). However, we do not de, which assumes such an underlying symmetry. include the SAURON data in our modeling, relying instead tic data were bi-symmetrized in a weighted mean, on the long-slit kinematics obtained from MMT and KPNO dividual uncertainties reported by ppxf to derive to provide the constraints on ϒ at large radii. This is partly a m-m (mag) (m-m) (mag) =0.3, =0.7 =0.3, =0.0 =1.0, = z SN Ia Hubble Diagram (Riess+98)

3 Precise geometric distances to AGN via Dust (and Quasar) Parallaxes

Dust Parallaxes: Idea (1/2) Standard Ruler: Invert the parallactic triangle ness

new base of an long (very o an object, ce given just situation is of ngle and the s

Dquasar Quasar s central source θ dregion Figure 1 Geometric distances.

4 Dust Parallaxes: Idea (1/2) Standard Ruler: Invert the parallactic triangle ness allows 1a he Universe s best-known ver, a better cal distances n this issue trate a new base of an long (very o an object, ce given just situation is of ngle and the s against the om one side other every lthough the a Earth Dstar Sun θ Star Hot dust b Dquasar Quasar s central source θ dregion Figure 1 Geometric distances. a, The distance to a star (D ) from Earth can benature measured by solving an M. Elvis, News & Views

5 Dust Parallaxes: Idea (2/2) Geometric distance: IR survey telescope geometric distance = physical size angular size As reference, one may use: VLTI broad line region of AGN (Elvis & Karovska 02) difficult for VLTI, but potentially possible (Rakshit+15, Petrov+15) have to work out gas physics (models) the hot dusty ring at the inner edge of the torus (Hoenig 2014) successfully shown! (Hoenig+14, Nature, 515, 528)

6 Dust Parallaxes: Angular Size (Instrinsic) angular size from near-ir interferometry Weigelt+12, Hoenig+13 Important: De-projection using geometric constraints from well-covered uv-plane gas dynamics on 10+pc scales E-ELT, ALMA (spectro-)polarimety E-ELT radio jet Dust distribution from multi-band interferometry or see next slide

7 Dust Parallaxes: Physical Size (Instrinsic) physical size from optical/near-ir photometric monitoring Idea: dust reprocesses UV-optical emission optical-ir time-lag = physical size optical near-ir P. Lira, priv. comm. Dust distribution from near-ir transfer function in principle also useable for inclination (high cadence, photometric quality) NB: In favour of a near-ir photometric survey telescope

8 Dust Parallaxes: Precision How well can we do? 14 Mpc 16 Mpc 18 Mpc 20 Mpc 0.5 D A = Mpc 2.6 (68% confidence interval) 22 Mpc 24 Mpc Angular size of the inner boundary, ρ in (mas) Time lag of the inner boundary, τ in (d) NGC 4151 non-optimised data: 12-13% including all systematics!!! better uv-coverage and photometric monitoring: <10% Probability distribution Distance (Mpc) combining constraints from multiple objects: 3% (11 AGN); 1.5% (44 AGN) Marginal posterior

9 How to connect to LSST? Dust and candles (1/2) Hoenig 2014 AB magnitude Epoch (days) Table 1 Relative Contributions of Hot Dust to Wavebands at Different Redshifts Redshift z = 0 z = 0.05 z = 0.1 z = 0.2 z = 0.3 i band z band y band (y3) y band (y4) = cross correlation function time lag (days) Figure 3. Six-day-smoothed cross-correlation function (CCF) of an AGN

10 Dust and candles (2/2) Dust is also standard candle!!! (e.g. Oknyanskij & Horne 01; Yoshi+04,14) 0 log (radius [pc]) near-ir time lag -1-2 distance (Mpc) -3 Koshida AGN luminosity log (L kev [erg s -1 ]) Hoenig redshift With LSST: suitable AGN to z<0.2 AGN = Standard candle + standard ruler

The broad-line region Similar combination possible for BLR!!! (Elvis & Karovska 01; Watson+11; Haas+11) Ω m = 0.27, Ω Λ = 0.73 Ω m = 0.3, Ω Λ = 0.0 Ω m = 1.0, Ω Λ = 0.

11 The broad-line region Similar combination possible for BLR!!! (Elvis & Karovska 01; Watson+11; Haas+11) Ω m = 0.27, Ω Λ = 0.73 Ω m = 0.3, Ω Λ = 0.0 Ω m = 1.0, Ω Λ = τ / (λf λ ) ½ [day (10 15 erg cm 2 s 1 ) ½ ] NGC 4051 NGC 3516 NGC 3227 NGC 5548 NGC 7469 Watson+11 m M D L (Mpc) log(ratio) Redshift (z) log 2.5 (ratio) (mag) Courtesy of Romain Petrov (OCA) Again: the BLR monitoring by LSST (Chellouche+14) alternatively: spectroscopic survey telescope

12 Summary: AGN Cosmology VLTI can be used to measure accurate geometric distances to extragalactic objects from 10 Mpc to ~1000 Mpc Useful for: high-precision H0 in the local universe testing universality of cosmological parameters establishment of AGN as independent branch of distance ladder precise dynamical black hole mass measurements constrain peculiar velocities Complementary approach to BAO Direct connection to LSST (dust reverberation mapping), E-ELT (black hole masses) Wishlist: (1) sensitivity, (2) simple IR imaging instrument, (3) near-ir survey not necessarily longer baselines well-performing Fringe Tracker inevitable (4) add optical and spectral resolution VLTI a one-stop shop of cosmology and BH masses

13 Summary: AGN Cosmology This opens up the prospect of extending AGN size and distance measurements out to the earliest cosmic times, and thus of measuring cosmological properties at distances far beyond where supernovae can take us. [ ] [W]e may now have to consider whether some of our resources should soon be put into building a next generation of optical interferometers. Martin Elvis, Harvard CfA, Nature News & Views, 2014 Dust parallax Hubble diagram based on 1st gen. instruments

The cosmic distance scale

The cosmic distance scale Distance information is often crucial to understand the physics of astrophysical objects. This requires knowing the basic properties of such an object, like its size, its environment,