Andrew HumphreyINAOE

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

•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

L[OIII]5007

=1.5 x1043 erg s-1.spatial extent ~40x30 kpc2.

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 x1041 erg s-1.spatial extent ~23x27 kpc2

SFIRST

=1.4 mJy.

L[OIII]5007

=1.5 x1043 erg s-1.spatial extent ~40x30 kpc2.

H and [NeV] also extended.SDSS J1550+39 (z=0.347)

SDSS J0840+38 (z=0.313)L

[OIII]5007=9.8 x1041 erg s-1.

spatial extent ~23x27 kpc2.

7C and 3CRR complete samples (Willott et al. 1999)

0840 1550

SDSS J1550+39 (z=0.347)

[OII]/[OIII]significant spatial variation between 0.3 and 1.7.

no clear radial trend

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).

SDSS J1550+39 (z=0.347)

Kinematic propertieshigh FWHM near centre (~1000 km s-1)

too high to be gravitational motionat larger radii, the kinematics are relatively quiescent (FWHM~ a few hundred km s-1)– consistent with gravitation. M

dyn~10

12 M

solkinematically perturbed regions show blueshift relative to quiescent regionsThese 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 ~1030 erg s-1 Hz-1 Sr-1)

<--- Blue wing

•Suggests outflow

•About 500 km/s

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 x1045 x(L151

/1035)6/7 to estimate jet kinetic power (Willott et al. 1999) gives ~2 x1041 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 ~1045 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

What powers the outflow in SDSS J1550+39?

• Star formation? Maybe...– FIRST flux density 11 mJy would imply

high star formation rates (SFR >1000 Msol yr-1)

– Further observations, in mid-IR and sub-mm would be useful.

What powers the outflow in SDSS J1550+39?

• AGN radiation? Maybe...– L(OIII) × 1000 ~ L(bol) → 1046 erg s-1

– A 5% radiative efficiency → MBH

~ 108 Msol

– Accretion near Eddington limit → 5 Msol yr-1

– Accretion ~ outflow rate (king & Pounds 03)

SDSS J0840+38 (z=0.313)

[OII]/[OIII]smaller spatial variation between 0.5 and 1.1

higher ratio at larger radii

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 x1012 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)

Andrew HumphreyINAOE

Published in MNRAS 2008, 390, 1505, with M. Villar-Martín, S.F. Sánchez, et al.

Part 2: Spatially extended lineabsorption associated with thez=2.6 BLRG MRC 2025-218

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)

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)

Results

• LRIS

• VIMOS

Ly-alpha

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)