1. Andrew Humphrey INAOE Submitted to MNRAS Letters with M. Villar-Martín, S.F. Sánchez, A. Martínez-Sansigre, R. González Delgado, E. Pérez, C. Tadhunter, M.-A. Pérez-Torres Part 1: Integral Field Spectroscopy of moderate redshift, type II quasars

2. Selected from SDSS type II quasar catalogue z = 0.3-0.4 Originally identified by zakamska et al. (2003) SDSS spectra show narrow lines high [OIII] 5007 fluxes (>10 -15 erg s -1 cm -2 ) typical AGN high ionization lines [NeV], HeII 3.5m telescope, Calar Alto, 2008 Jan & July Potsdam Multi-Aperture Spectrograph (PMAS) Total exposure time 7200 s (6x1200) Spatial scale 1”/ lens, FOV 16”x16” Seeing FWHM=1.2”-1.6” V300 grating: 4250-7650 Å and IP = 7.4 Å Individual spectra assembled into a datacube

3. L [OIII]5007 =1.5 x10 43 erg s -1. spatial extent ~40x30 kpc 2. H  and [NeV] also extended. S FIRST =10.6 mJy SDSS J1550+39 (z=0.347) SDSS J0840+38 (z=0.313) L [OIII]5007 =9.8 x10 41 erg s -1. spatial extent ~23x27 kpc 2 S FIRST =1.4 mJy.

4. L [OIII]5007 =1.5 x10 43 erg s -1. spatial extent ~40x30 kpc 2. H  and [NeV] also extended. SDSS J1550+39 (z=0.347) SDSS J0840+38 (z=0.313) L [OIII]5007 =9.8 x10 41 erg s -1. spatial extent ~23x27 kpc 2. 7C and 3CRR complete samples (Willott et al. 1999) 0840 1550

5. SDSS J1550+39 (z=0.347) [OII]/[OIII] significant spatial variation between 0.3 and 1.7. no clear radial trend

6. SDSS J1550+39 (z=0.347) [OII]/[OIII] significant spatial variation between 0.3 and 1.7, suggesting range in excitation no clear radial trend pixels with highest [OII]/[OIII] show an unusual spectrum [NeIII] / [OIII]5007 ~1 In photoionized gas [NeIII]/[OIII] ~0.15, the relative abundance ratio in the ISM. In shocks [NeIII]/[OIII] can reach ~1, due to temperature structure and relative recombination rates (Dopita & Sutherland 1996).

7. SDSS J1550+39 (z=0.347) Kinematic properties high FWHM near centre (~1000 km s -1 ) too high to be gravitational motion at larger radii, the kinematics are relatively quiescent (FWHM~ a few hundred km s -1 ) – consistent with gravitation. M dyn ~10 12 M sol kinematically perturbed regions show blueshift relative to quiescent regions These properties are remarkably similar to those shown by the Ly  haloes of powerful radio galaxies (e.g. Villar-Martin et al. 2003)... However, this galaxy has much lower radio power (L 1.4GHz ~10 30 erg s -1 Hz -1 Sr -1 )

8. <--- Blue wing Suggests outflow About 500 km/s

9. What powers the outflow in SDSS J1550+39? Radio jets? Probably present but too low power... – S NVSS =13.1±0.6 mJy (45”), S FIRST =10.6±0.5 mJy (5”) – Using 3 x10 45 x(L 151 /10 35 ) 6/7 to estimate jet kinetic power (Willott et al. 1999) gives ~2 x10 41 erg s -1. – For a spherical outflow of v=570 km s -1, gas density=1 cm -3, and injection time of 10 Myr, injection rate required would be ~10 45 erg s -1. (A difference of more than 3 orders of magnitude.) – Edit: Brian McNamara told us that Willott et al. Relation underestimates kinetic power by about 2 orders of magnitude

10. What powers the outflow in SDSS J1550+39? Star formation? Maybe... – FIRST flux density 11 mJy would imply high star formation rates (SFR >1000 M sol yr -1) – Further observations, in mid-IR and sub-mm would be useful.

11. What powers the outflow in SDSS J1550+39? AGN radiation? Maybe... – L(OIII) × 1000 ~ L(bol) → 10 46 erg s -1 – A 5% radiative efficiency → M BH ~ 10 8 M sol – Accretion near Eddington limit → 5 M sol yr -1 – Accretion ~ outflow rate (king & Pounds 03)

12. SDSS J0840+38 (z=0.313) [OII]/[OIII] smaller spatial variation between 0.5 and 1.1 higher ratio at larger radii

13. SDSS J0840+38 (z=0.313) Kinematic properties near the AGN,FWHM is high (~1100 km s -1 ) line emission is relatively blueshifted (~80 km s -1 ) in this object, the blueshifted gas is not resolved M dyn ~5 x10 12 M solar. Emission line properties of these type II radio quiet quasars are consistent with the few other type II quasars whose extended nebulae have been examined, e.g. – (AMS05 at z=2.85, Smith et al.2009)

14. Andrew Humphrey INAOE Published in MNRAS 2008, 390, 1505, with M. Villar-Martín, S.F. Sánchez, et al. Part 2: Spatially extended line absorption associated with the z=2.6 BLRG MRC 2025-218

15. Motivation At z>2 many radio galaxies show spatially extended Ly-alpha absorption, detected with the aid of their giant Ly- alpha emission haloes (~10-100 kpc) – Studies have focused on strong resonance lines Ly-alpha and CIV – Enriched in metals and part neutral part ionized Going beyond Ly-alpha and CIV – We need to break degeneracies and reduce dependence on ionization model parameters From Jarvis et al. (2003)

16. Observations VLT with VIMOS – Integral field unit of VIMOS on UT3 – Instrumental profile FWHM=1.7 Angstroms – 4150-6200 A (1140-1700 A restframe) – 10 h total exposure time – FOV=27”x27” Keck II LRIS – Low Resolution Imaging Spectometer – IP FWHM=10 A – 3800-9000 A (1060-2430 A restfame) – 5.1 h exposure – 1” wide slit placed along optical major axis 4.5” X 7” Pentericci et al. (1999)

17. Results LRIS VIMOS Ly-alpha

18. Discussion Rich absorption line spectrum Some species have multiple lines in wavelength range – Good constraints on column density using variant of the Equivalent Width Method (e.g. Spitzer & Jenkins 1975) – CI 1188.8 oscillator strength f=0.013. Nondetection. → N upper limit – CI 1277.2 f=0.11. Saturated detection. → N lower limit – CI 1157.2 f=0.55. Saturated detection. → N lower limit – Applied this method to multiple lines of SiII, SiII*, CIV, NV – SiII / SiII* (excited state) ratio → lower limit n > 10 cm -3 – Overall, the column ratios are consistent with photoionization by a hard AGN-like continuum – the central AGN or AGN-dominated MBR. The presence of NV rules out stellar photoionization. The ratios are inconsistent with predictions of fast shocks. (becomes lower limit on flat part of CoG)