Title:	
Radio to X-ray observations of the jet-cloud interaction in PKS2152-699

Authors:
R A E Fosbury, T Bedding, L Binette, S Borelli, A Cimatti, Th 
Courvoisier, S di Serego Alighieri, P Grandi, J Kirk, T Snijders, C 
Tadhunter, W Wilson

Addresses:

Abstract

Introduction

The far-field radiation pattern of an active galactic nucleus is clearly 
anisotropic. The physical origin of this anisotropy can be both intrinsic 
and extrinsic, eg. relativistic beaming or obscuration by an equatorial 
disk or torus respectively, but the structures responsible for forming or 
modifying this power output are generally on spatial scales too small to 
be resolved with any technique other than radio VLBI in nearby objects 
(Nature Jan 95 - masers). In addition to the photon radiation, there is a 
matter outflow which, in the case of the powerful radio sources, can 
take the form of a highly collimated jet moving at relativistic speeds 
over at least part of its length.
The interaction between these forms of power output and material 
within and beyond the host galaxy can provide a rich source of 
information, not only about the AGN itself, but also about the nature 
of the host and its environment. This is particularly pertinent at high 
redshift where a powerful quasar can illuminate its surroundings over a 
large volume and give us a picture of the early evolution of galaxies 
which it complimentary to that which can be gleaned from absorption 
line studies. The result of these interactions is seen clearly in the high 
redshift radio galaxies (HzRG) where there is a close alignment between 
the elongated (rest-frame) ultraviolet images and the radio axis: the 
'alingment effect' (McCarthy et al. 1987; Chambers et al. 1987; see also 
McCarthy 1993 - ARAA)
It is largely because of the importance of being able to understand the 
physical processes which result in the structures visible at early epochs 
that we have continued our detailed study of the nearby radio galaxy 
PKS2152-699 (z=0.0282). This object exhibits a region of energetic 
extranuclear activity which, because of its brightness over a very broad 
waveband, gives us the opportunity to study the effects of a jet/cloud 
interaction in considerable detail (Tadhunter et al. 1987, Tadhunter et 
al. 1988, di Serego Alighieri et al. 1988, Fosbury et al. 1990).
The galaxy identified with the radio source is an E3 with B=14.8 (M_B=-
21.4; H_0=50 km/s/Mpc). The total radio power at 5GHz is 5x10^25 
W/Hz. There is an intense nuclear emission line spectrum which has 
been described in the optical by Marenbach & Appenzeller (1982), 
Whittle (1982), Danziger & Goss (1983) and Tadhunter et al. (1987, 
1988) and in the ultraviolet by Fosbury et al. (1990) and Keel & 
Windhorst (1991). The Highly Ionized Cloud (HIC), at a projected 
distance from the nucleus of around 10 arcsec (8kpc), shows a highly 
excited emission line spectrum with ions extending up to Fe^9+ and a 
very blue optical to near-UV continuum with 10% linear polarization 
with the E-vector perpendicular to the position angle of the nucleus-
HIC axis. The existence of the blue, polarized continuum led di Serego 
Alighieri et al. (1988) to suggest that this resulted from the scattering 
by dust in the cloud of beamed radiation from the nucleus. With a 
typical AGN spectrum extending to higher energies, such a photon beam 
could readily ionize the gas in the HIC although there are very likely to 
be additional local sources of ionization such as high velocity shocks 
(Bicknell ref.). The presence of some gas at high velocities, observed at 
velocities up to 3000 km/s from the systemic velocity of the HIC and 
galaxy, is indicated by weak, broad blue wings on the intense [OIII] lines 
emitted by the HIC (Tadhunter et al. 1988).
Early, low resolution radio maps show an unequal double with an axis 
position angle of 25deg (Tadhunter et al. 1988, cf. 46deg: the PA of the 
HIC) and the first maps made with the Australia Telescope (Norris et al. 
1990; Fosbury et al. 1990) start to reveal the nuclear source distinct 
from the southern lobe. VLBI observations at 2.3GHz show an elliptical 
core with a major axis in PA 40deg (John Reynolds, private 
communication - check publication, email sent).
In this paper we present observations of this galaxy which are designed 
to elucidate in more detail the nature of the physical interaction 
between the nuclear activity and the HIC. Full synthesis observations 
at two frequencies with the Australia Telescope Compact Array show 
radio emission associated --- but not coextensive ---  with the optical 
cloud. IUE spectra are used to measure line and continuum fluxes 
separately from the nucleus and the HIC. The High Resolution Imager 
(HRI, ref)) on the ROSAT satellite reveals X-ray emission coincident 
with both components. In addition, we have new optical line and 
continuum images which show fainter emission line regions extending 
to much larger radial distances close to the PA of the HIC. The 
existence of one of these clouds was already known from the 
spectroscopic observations of Tadhunter et al. (1988). A K-band image 
allows us to place an upper limit on the HIC flux at 2.2 microns. 
Ultraviolet imaging and polarimetry with HST will be described in a 
subsequent paper.
Describe organisation of paper.




Observations

Australia Telescope
The radio galaxy PKS2152-699 was the first radio image obtained the 
Australia Telescope (Norris et al. 1990). Further early maps were shown 
by Fosbury et al.  (1990) and it was on the basis of these that we 
decided to obtain full synthesis maps with the Australia Telescope 
Compact Array (ATCA) at both 3 and 6cm wavelength.  Four 
configurations of the 6km ATCA were used on the 19 and 23 January, 
21 March and 1 April 1992 . The derived flux densities for the major 
image components are listed in Table <n>. The flux scale is based on 
the recent compilation of measurements of PKS1934-638 by John 
Reynolds (privat communication, 30 July 1994). This differs from the 
previous calibration in use at the AT by (new-old) -7.9% at 4740MHz 
and +9.8% at 8640MHz. The total fluxes derived from these synthesis 
observations are lower than single dish observations at the same 
frequencies due to missing small spacings. This is particularly apparent 
at 3cm. The total intensity maps are shown in Figure <m> .
The source shows a mixed FR I/II morphology (Fanaroff & Riley 19??) 
with an edge-brightened southern lobe which suggests jet precession. 
The northern lobe, however, is diffuse with a much lower surface 
brightness and a single, centrally placed hot spot. The source is 
asymmetric both in lobe flux ratio and core distance ratio . (add 
numbers). The position of the radio axis (PA25�) is significantly different 
from the position angle of the HIC with respect to the nucleus (45�) 
and, while there is a radio component at a similar radial distance to the 
HIC, its PA is intermediate between these two and it appears to lie on 
the northern edge of the optical and X-ray HIC sources.
A precise position of the nuclear source has been determined from a 
dual S/X-band VLBI observation between Tidbinbilla and Hobart 
(Reynolds et al. 1994?). This is given, along with astrometry at other 
wavelengths, in Table <n>. Comments on structure?
Comments on the polarization structure.
Reduction description
Images at both frequencies
Polarization (mostly at 6cm)
Derive the total flux from the MOST observation - see Gordon



IUE
Ultraviolet spectra have been obtained of PKS2152-699 with both the 
long and short wavelength cameras on the IUE satellite during 1984 
and 1989 (see Table <n>). Although two of these exposures were 
specifically centred on the HIC, the size and orientation of the large 
aperture means that both nucleus and cloud can be present 
simultaneously. During reduction of the cloud spectra, care has been 
taken to exclude the parts of the image contaning by nuclear light.
Since the source is faint by IUE standards, the preceeding exposures 
taken by the cameras were checked to ensure that no bright sources 
contributed remnant images. The spectrum below Geocoronal Ly-a is 
very uncertain, but the SWP is well-exposed at its long wavelength end. 
Both ends of the LWP spectra (1950-2300� and 3100-3300�) are 
unreliable. Our best estimates of the emission line fluxes from the 
nucleus and the HIC are given in Table <n>. The continuum flux was 
first averaged in 100� bins. The most reliable of these, ie. those 
excluding emission lines and in reasonably well exposed regions, were 
combined to give the bands and their associated fluxes in Table <n>. 
The flux for the HIC below 1750� is less than 3s and so should be 
considered an upper limit. Figure <m> shows these continuum points 
together with the optical (emission line free) fluxes from di Sergo 
Alighieri et al. (1988).



ROSAT
Observations of the PKS2152-699 field were obtained with all three 
instruments on ROSAT during AO-2. The primary instrument was the 
HRI but a short observation was also made with the PSPC. The WFC 
was run in parallel with HRI. The observation log is given in Table <n>.
The directly summed image of the HRI data shows a source � the 
strongest in the field � which we identify with the galaxy (Figure 
<m>a). In order to realise the full angular resolution of the instrument, 
it is necessary to correct for the well-known spacecraft attitude 'wobble' 
and the secular errors in the star-tracker calibration (eg. Morse 1994). 
Consequently, we  divided the data into time segments whose length, 
typically 1000�1500 sec, was set to enable the determination of a 
centroid position for the galaxy with a precision comparable to the 
width of the point spread function (PSF). After some manipulation of 
the start and finish times of these segments to avoid obvious position 
jumps, the sub-images were shifted and added to give the combined 
photon image shown in Figure <m>b. 
In order to convert the corrected photon image to an intensity map, we 
have made a conservative application of the Lucy-Richardson image 
restoration algorithm (ref) using  the 'instantaneous' on-axis HRI PSF 
(ref) convolved with a gaussian function with a sigma of ?arcsec, 
representing the mean centroiding error. For presentation, the resulting 
intensity model is convolved with a gaussian PSF with a FWHM of 3 
arcsec (Figure <m>c) � which is the approximate resolution of the 
centroided image. Such an application of this algorithm is not intended 
to enhance spatial resolution but rather to filter thos components of 
the noise with spatial frequencies incompatible with the instrumental 
PSF (ref).
Derivations:
HRI flux
Relative positions of the two sources and uncertainty
PSPC flux and spectral fits
Variability?
Rejection of outer HRI energy channels (Cecil et al.) ?



Optical imaging

Images centred on PKS2152-699 were obtained with the ESO NTT using 
interference filters of bandwidth around 70� FWHM chosen to isolate 
the [OII] 3727 and [OIII] 5007 doublets and the nearby continuum 
(Table <n>). 
The data were reduced using the method described by di Serego Alighieri 
(1989). This involved removing cosmic rays during the combination of 
sub-exposures, subtracting the sky using measurements in the region 
surrounding the galaxy and co-aligning the line and continuum frames 
using field stars. The formation of the line image was done using a 
scaling factor derived from a spectrophotometric standard star and 
assuming that the continuum of the host galaxy was typical of an 
elliptical galaxy (Yee & Oke 1978). The [OIII] continuum we used 
contained the Hb line within its band and so the subtraction was done 
taking into account the Hb flux given by Tadhunter et al. (1988). The 
flux errors were calculated  by propagating the poissonian noise from 
object and sky observations in both filters. 
The resulting fluxes are given in Table <n>. The nights were not 
perfectly photometric and so we estimate an additional 10% uncertainty 
due to possible small transparency variations (Andrea ?).
The [OII] and [OIII] line and continuum images of the galaxy and the 
HIC are shown in Figure <m>. Examination of the full field of the [OIII] 
frame reveals additional emission line clouds which were not apparent 
on previous images. These are marked in Figure <m> and the three (?) 
brighter clouds are also visible on the � lower s/n � [OII] image. (note: 
add field size to obs log). The diffuse region at 20 arcsec(?) along the PA 
of the HIC was already seen as a high ionization feature in the 
spectroscopy of Tadhunter et al. (1988). The other clouds show a 
preference for the same axis but fall well outside the region of radio 
emission.



IR imaging

A K-band image was obtained  on the ESO/MPI 2.2m telescope with 
IRAC2  (ref)  (Table <n>). The total integration time of  4095sec 
comprised two identical 3x3 pointing arrays on a 25arcsec grid spacing 
with dwells of 15x13 sec and 20x13 sec at each point. The  calibration 
standard star was HD 223886. The median of all the images was 
calculated to represent the sky and this was subtracted from each sub-
frame which was then divided by the normalized (to the median value) 
differential dome flat. The resulting mosaic of the sub-images is shown 
in Figure <m>.



Results
Astrometry
The most precise position for the radio core is provided by the S/X-band 
VLBI observations reported by Reynolds et al. (1993). This shows an 
elongated structure on a scale of (mas?) with the major axis in PA 
40deg. The reference frame for the ATCA maps is (Warwick ??).  The 
optical and K-band images have been referred to the Guide Star 
Catalogue (Ref) frame using GSC stars which appear in the CCD frames 
(Sperello - we need to measure the new frames). The uncertainty in the 
offset between the radio and the GSC reference frames is ????
The ROSAT HRI attitude solution has an absolute uncertainty of (5-6 
arcsec - check) in addition to the spacecraft wobble of similar 
amplitude. We have therefore assigned the VLBI position to the centroid 
of the X-ray photon map. The effect of uncertainties in the spacecraft 
roll angle are negligible over the relevant field. The uncertainty in the 
relative position of the HIC X-ray source is dominated by photon 
statistical errors and the effective HRI PSF.
Figure <n> shows a montage of the radio, optical and X-ray images of 
the nucleus/HIC region using the reference frames described above. 



The overall spectrum
Table <m> gives the accumulated flux measurements for the whole 
source, the nucleus and the HIC. This is assembled from the referenced 
literature in addition to the present work. A spectrum, plotted as nu 
f_nu, is given in Figure <n>. While all of the HIC fluxes are free of the 
galaxy background, the distinction between the nuclear and the total 
flux from the galaxy is wavelength and resolution dependent. In 
particular, the optical measurements (di Serego Alighieri et al. 1988) 
were made through a 5.2 arcsec diameter aperture centred on the 
nucleus and include contributions from galactic starlight as well as 
nuclear continuum and emission lines.

Discussion

The spatial structure
At the spatial resolution of the various observations, the optical and X-
ray images of the HIC are at least partially coextensive. The optical 
continuum peak is, as noted by di Serego Alighieri et al. (1988), 
displaced by 1.4�0.2 arcsec towards the nucleus with respect to the 
[OIII] line peak and this has been used as an argument that the two-
photon emission is not a major contributor to the UV continuum. The 
radio contunuum associated with the HIC is closer to the line joining 
the NE and SW radio hot-spots to the nucleus and skirts the NW edge 
of the optical HIC.
The new [OIII] line image shows an extension from the nucleus of the 
galaxy in the general direction of, although not precisely towards, the 
HIC. In fact, in [OIII], the nucleus and the HIC are very similar both in 
total flux and spatial distribution.
An important and significant conclusion is that the HIC radio and X-
ray sources are significantly displaced from one another. The one sigma 
error in the position of the HIC X-ray source, estimated from the 
photon count and the width if the post-centroiding ROSAT/HRI PSF, is 
0.4 arcsec. The separation between this and the 6cm radio peak is 2.1 
arcsec. This 5 sigma difference forms part of the evidence that the X-
rays are not being generated by synchrotron or inverse Compton 
processes, at least by the electrons responsible for the radio emission.
While the HIC radio and optical emission are not coextensive, they are 
clearly physically associated. The other emission line clouds, however, 
have no radio counterparts and are not aligned with the outer radio 
lobe structure. This strongly suggests that they are excited by photon 
radiation from the AGN


The energetics
In this section, we shall attempt to put observational constraints on 
the various components of the AGN power output. There are three 
aspects to the problem which we address:
1) The beamed photon radiation which is seen by the HIC and 
presumably by the other, fainter clouds along the jet axis.
2) The particle jet which fuels the radio lobes and, by inference from the 
existence of the adjacent radio source, has recently interacted, or is 
currently interacting with the HIC.
3) The "isotropic" � although probably obscured along our line-of-sight 
� radiation from the AGN which may be responsible for ionizing the 
low excitation gaseous filaments seen most clearly in Ha images of the 
galaxy.
On the assumption that the line emission and the optical/UV 
continuum radiation from the HIC are dominated by photoioization by, 
and dust scattering of, the blazar beam from the AGN, Magris, Binette 
& Martin (1993) were able to model the power and spectrum of the 
beamed radiation impinging on the cloud. 





References:

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?
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\item Magris C., G., Binette, L.,  \and\ Martin. P. G., 1993,
``A Thick Reflection Nebula Illuminated by a Power Law'', \pro\ {\it
The Nearest Active Galaxies}, ed. J. Beckman,
Astrophysics and Space Science, {\bf 205}, p. 141-148. 



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To: jreynold@atnf.csiro.au
Cc: rfosbury@st9.hq.eso.org
Subject: PKS2152-699
Date: Wed, 30 Nov 1994 11:32:18 +0100
From: Robert Fosbury <rfosbury@eso.org>
Status: O

Dear John, can you give me the latest update on the VLBI measurements
of this object? Tim and I (and others) want to refer to it in a paper 
and
I am not sure if you have published the results yet.
Thanks a lot and regards, Bob...
Observations of the jet-cloud interaction in PKS2152-699

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