Andrew Humphrey

1
Part 1 Integral Field Spectroscopy of moderate
redshift, type II quasars
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
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 (gt10-15 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 16x16
• Seeing FWHM1.2-1.6
• V300 grating 4250-7650 Å and IP 7.4 Å
• Individual spectra assembled into a datacube

3
LOIII50071.5 x1043 erg s-1. spatial extent
40x30 kpc2. H? and NeV also extended. SFIRST10
.6 mJy
SDSS J155039 (z0.347)
LOIII50079.8 x1041 erg s-1. spatial extent
23x27 kpc2 SFIRST1.4 mJy.
SDSS J084038 (z0.313)
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LOIII50071.5 x1043 erg s-1. spatial extent
40x30 kpc2. H? and NeV also extended.
SDSS J155039 (z0.347)
7C and 3CRR complete samples (Willott et al. 1999)
0840 1550
LOIII50079.8 x1041 erg s-1. spatial extent
23x27 kpc2.
SDSS J084038 (z0.313)
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SDSS J155039 (z0.347)

• OII/OIII
• significant spatial variation between 0.3 and
  1.7.
• no clear radial trend

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SDSS J155039 (z0.347)

• 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 / OIII5007 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).
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SDSS J155039 (z0.347)

• 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. Mdyn1012 Msol
• 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
  (L1.4GHz 1030 erg s-1 Hz-1 Sr-1)

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lt--- Blue wing

• Suggests outflow
• About 500 km/s

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What powers the outflow in SDSS J155039?

• Radio jets? Probably present but too low
  power...
• SNVSS13.10.6 mJy (45), SFIRST10.60.5 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 v570 km s-1, gas
  density1 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

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What powers the outflow in SDSS J155039?

• Star formation? Maybe...
• FIRST flux density 11 mJy would imply high star
  formation rates (SFR gt1000 Msol yr-1)
• Further observations, in mid-IR and sub-mm would
  be useful.

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What powers the outflow in SDSS J155039?

• 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)

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SDSS J084038 (z0.313)

• OII/OIII
• smaller spatial variation between 0.5 and 1.1
• higher ratio at larger radii

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SDSS J084038 (z0.313)

• 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
• Mdyn5 x1012 Msolar.
• 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 z2.85, Smith et al.2009)

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Part 2 Spatially extended line absorption
associated with the z2.6 BLRG MRC 2025-218
Andrew Humphrey INAOE
Published in MNRAS 2008, 390, 1505, with M.
Villar-Martín, S.F. Sánchez, et al.
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Motivation

• At zgt2 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)
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Observations

• VLT with VIMOS
• Integral field unit of VIMOS on UT3
• Instrumental profile FWHM1.7 Angstroms
• 4150-6200 A (1140-1700 A restframe)
• 10 h total exposure time
• FOV27x27
• Keck II LRIS
• Low Resolution Imaging Spectometer
• IP FWHM10 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)
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Results

• LRIS
• VIMOS

Ly-alpha
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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 f0.013.
  Nondetection. ? N upper limit
• CI 1277.2 f0.11. Saturated detection. ? N lower
  limit
• CI 1157.2 f0.55. Saturated detection. ? N lower
  limit
• Applied this method to multiple lines of SiII,
  SiII, CIV, NV
• SiII / SiII (excited state) ratio ? lower limit
  n gt 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)