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%\documentstyle[11pt,patt2]{article}        % Use if no embedded figs
%\documentstyle[11pt,patt2,epsf]{article}  % Use if embedding figs with epsf
\documentstyle[11pt,patt2,psfig]{article} % Use if embedding figs with psfig
\typeout{This is the PATT2 (Optical/IR) blank LaTeX form}
\begin{document}

\telescope{INT}                     % eg WHT,INT,JKT
\semester {98B}                     % eg 98A

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% PAGE 1 OF PATT2 FORM %
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% PI information

\pisurname     {Ciliegi}                % Surname
\piinitials    {P}                % Initials
\pititle       {Dr}                % Mr/Mrs/Ms/Miss/Dr/Prof
\pistatus      {Research associate}                % Post held
\piaddressone  {Institute of Astronomy}  % Name of Institute
\piaddresstwo  {Madingley Road}          % Postal Address
\piaddressthree{Cambridge CB3 0HA}       % Postal Address
\piphone       {01223 - 337544}                % Phone number
\pifax         {01223 - 337523}                % Facsimile number
\piemail       {ciliegi@ast.cam.ac.uk}  % email address
\piobserver    {Yes}                % Is the PI going to observe? {Yes/No}

% collaborator 1
\collabonename    {R. McMahon}  % Name of first collaborator
\collaboneinst    {Institute of Astronomy, Cambridge} % Name of Institute
\collaboneobserver{Yes}             % Will collaborator observe? {Yes/No}

% collaborator 2
\collabtwoname    {A. Caccianiga}
\collabtwoinst    {Osservatorio di Brera, Milano , Italy}
\collabtwoobserver{Yes}

% collaborator 3
\collabthreename    {T. Maccacaro}
\collabthreeinst    {Osservatorio di Brera, Milano, Italy}
\collabthreeobserver{No}

% collaborator 4

\collabfourname    {}
\collabfourinst    {}
\collabfourobserver{}

% proposal information

\title{A complete sample of X-ray luminous radio sources}   
% Brief title  (12 words only)
\abstract   
{We propose to obtain CCD identifications
of a complete sample of 46 optically unidentified
radio loud X-ray sources.
The parent sample of 395 sources with
F$\rm _x$(0.5-2.0keV)$>5\times10^{-14}$ erg cm$^{-2}$ s$^{-1}$
and S$_{20cm}$ $>$ 10 mJy, 
covers $\sim$500 deg$^{2}$ and 
explores a new regime in multi-wavelength
parameter space, and will provide unparalled constraints
on the numbers of BL Lacs, obscured AGN and high
redshift radio loud quasars. By using UBR colours alone we
shall be able to make a preliminary classification of the optical
counterparts 
without recourse
to an indiscriminate redshift campaign. In addition, as
an important bye-product of the large field of view of the
INT WFC, we shall obtain multi-colour CCD colours over
an area of 9deg$^2$, which contains a few hundred 
faint X-ray and radio sources and $\sim1000$ UVX quasars,
allowing for the first time systematic, unbiased,
statistically significant($N/\sqrt{N}>10$) 
multi-wavelength AGN studies from radio though optical
to X-rays at low X-ray and radio fluxes.
}                % Summary of proposed observations

% Instrument requirements

\focalstation       {Prime}        % eg Prime,Cass,Nasmyth
\instrument         {WFC}        % eg ISIS,WYFFOS,AUX,LDSS,UES,TAURUS,etc
\detector           {EEV}        % eg TEK,EEV,Loral,Own,etc
\gratingsandfilters {U,B,R}        % eg UBVRI,H$\alpha$,R1200R,etc

\timerequested  {2}{}{}{}      % No. of {Dark},{Grey},{Bright}, {Weeks/Nights}
\minuseful      {2}{}{}        % Minimum number of useful {D},{G},{B} 
\lttotaltime    {5}{}{}{}      % For long term proposals only {D},{G},{B},{W/N}

\makepatttwopageone

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% PAGE 2 OF PATT2 FORM %
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\prefdates            {Aug-Nov}           % Preferred dates, eg Jan,Feb
\impossdates          {Dec-Jan}           % Impossible dates, eg Mar,Apr
\datesjustification   {RA range}           % Why impossible? eg wrong RAs, etc
\simultaneous         {}           % Simultaneous with other tels/satellites?
\othertimeconstraints {}           % eg Moon phase/position,specific dates
\serviceobservingyes  {}           % Observations to be done as Service? {x}
\serviceobservingno   {}           % or not {x}
\serviceobservingmaybe{x}           % or maybe {x}
\supporteverynight    {}           % Support astronomer every night? {x}
\supportnone          {}           % No support astronomer? {x}
\supportfirstnight    {x}           % Support astronomer first night only? {x}
                                   % (This is the only option for ING)

% target info                      % Target RA,Dec,Mags,Colours,Exp Time

\targetinfo{
\footnotesize
\begin{tabular}[t]{p{1.2in}p{1.0in}p{1.0in}p{1.0in}p{1.0in}p{1.0in}}
%name    & ra     & dec    & mag & colour & exposure time \\
REXJ00+13   & 00  29 &   +13 47 & R$>$20     & UBR    & 600 s per band \\
REXJ00$-$12 & 00  25 & $-$12 23 & R$>$20     & UBR    & 600 s \\ 
REXJ01+85   & 01  00 &   +85 07 & R$>$20     & UBR    & 600 s \\
REXJ01+01   & 01  39 &   +01 19 & R$>$20     & UBR    & 600 s \\
REXJ02+15   & 02  08 &   +15 44 & R$>$20     & UBR    & 600 s \\
REXJ02+00   & 02  53 &   +00 06 & R$>$20     & UBR    & 600 s \\
REXJ04$-$08 & 04  35 & $-$08 11 & R$>$20     & UBR    & 600 s \\
REXJ04$-$01 & 04  37 & $-$01 59 & R$>$20     & UBR    & 600 s \\
REXJ04+04   & 04  22 &   +04 51 & R$>$20     & UBR    & 600 s \\
REXJ04+03   & 04  59 &   +03 23 & R$>$20     & UBR    & 600 s \\
REXJ19$-$10 & 19  42 & $-$10 39 & R$>$20     & UBR    & 600 s \\
REXJ20$-$02 & 20  45 & $-$02 18 & R$>$20     & UBR    & 600 s \\
REXJ21+13   & 21  53 &   +13 40 & R$>$20     & UBR    & 600 s \\
REXJ21$-$11 & 21  05 & $-$11 25 & R$>$20     & UBR    & 600 s \\
REXJ22+03   & 22  44 &   +03 12 & R$>$20     & UBR    & 600 s \\
REXJ22+14   & 22  51 &   +14 48 & R$>$20     & UBR    & 600 s \\
REXJ23$-$08 & 23  04 & $-$08 16 & R$>$20     & UBR    & 600 s \\
REXJ23+09   & 23  26 &   +09 08 & R$>$20     & UBR    & 600 s \\
REXJ23+08   & 23  44 &   +08 38 & R$>$20     & UBR    & 600 s \\

\end{tabular}

\normalsize
}

% Other applications this semester for similar programmes (e.g. via CAT, AAT)
\otherapplications{
\begin{tabular}[t]{p{2.0in}p{3.0in}}
%Telescope/Committee & Short title of programme  \\
\end{tabular}
}

\makepatttwopagetwo

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% PAGE 3 OF PATT2 FORM - SCIENTIFIC JUSTIFICATION %
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\sciencecase{

\parindent 20pt  
\parskip 5pt  

\noindent{\bf Introduction} 
The systematic optical identification of sources detected at radio
and X-ray wavelengths has been of fundamental importance in
determining our knowledge of the nature and physical processes in
active galaxies. Unlike purely optical surveys for AGN, X-ray and
radio selected sample are much more diverse primarily since such
samples are less prone to orientation and obscuration related
effects. Up until now studies of the properties of AGN have been
primarily based on samples selected at bright radio (eg 3--7C, PKS)
or bright X-ray fluxes(eg Piccinotti et al. 1982, EMSS (Maccacaro et al. 
1994), RASS).  Studies at lower
fluxes have been thwarted by the lack of radio and X-ray data at low
fluxes.
The situation has undergone a radical change in the last
two years with the advent of deep all-sky radio surveys
(e.g. the NVSS, Condon et al. 1998, the FIRST survey, Becker et al. 1995)
and large area coverage to faint X-rays fluxes via serendipitous
sources in ROSAT PSPC images.
These surveys offer a great opportunity
to derive new sizable sample of AGN ie ($N/\sqrt{N}>10$). 

%(see Maccacaro et
%al. 1998 for a detailed description of the REX project). 
Through a positional cross-correlation of sources detected in the NVSS
and ROSAT fields (Caccianiga et al 1998), we have derived a sample of
{\em Radio Emitting X-ray sources (REX) } which are expected to
contain a high fraction of AGN (radio loud QSO, BL Lacs, Seyfert
galaxies) and radio galaxies (Maccacaro et al, 1998). Considering the
X-ray sources with PSPC off-axis angles less than 35$^{\prime}$,
Fx(0.5-2.0keV)$>5\times10^{-14}$ erg cm$^{-2}$ s$^{-1}$, S(20cm)$>$ 10
mJy, $\delta>-$20, the REX sample covers 590 deg$^2$, and contains 395
sources.

The primary goal of the REX project is the selection of a statistically 
complete sample of AGN by using simultaneously the information derived 
from the NVSS survey and from pointed ROSAT PSPC images. The project
complements and extends by a decade lower in both radio and X-ray
fluxes the efforts of Brinkman et al. (1997) who have used the
brighter flux limits of the ROSAT All Sky Survey and GreenBank radio
surveys. In addition, the survey is a factor of $\sim$100 larger 
than the previous most comparable work by 
Ciliegi et al. (1995) who studied the
radio properties of the CRSS survey.
The primary interest of the Milan group is in the properties of
the BL Lac's within the above sample. The Cambridge group are
primarily interested in the evolution of the quasar luminosity function
at low radio and X-ray luminosities and particularly
in the use of the REX sample in the discovery of quasars at high
redshift. In the longer term, such studies will use the much
larger samples that will come available from XMM which shall
the launched in 18months and thus the current proposal is
a cornerstone in long term planning for the exploitation
of XMM. In the context of the search for high
redshift quasars this program is an extension of the work
by Hook \& McMahon(1998) who have discovered two z$>$4 radio
loud, X-ray luminous quasars with z=4.30 and 4.72 (Fabian
et al., 1997) based on the ROSAT All Sky Survey and brighter
radio catalogues. 

%{\bf Related work} \\
%Serendipitous sources detected in the ROSAT PSPC 
%are being used for at least 3 clusters surveys
%(SHARC: ref; WARPS: ref ; Rosati et al)
%and
%two general AGN follow-up programs ie RIXOS(ref) and CRSS(ref).
%The cluster searches have deliberately excluded point sources
%and only CRSS has been combined with a radio data. 
%The REX sample is this 
%The choice of limits is also 
%Whilst there are at least three 


\noindent{\bf Observational status} 
During the last two years we have performed 
optical spectroscopic observations at ESO and Mauna Kea 
of the brighter sources (m(R)$<$20) that were identified on APM
catalogues derived from POSS and UKST plates and have identified
and spectroscopically classified 
154(39\%) of the 395 REX sources.
In total, the identified fraction of the REX sample of 395 sources
(both from literature
and from our own observations) consists of 24 BL Lac's(6\%), 
$\sim$ 75 broad 
line AGN(14\%) and $\sim$55 narrow lined AGN or radio galaxies(19\%). 

Of the unidentified sources, the majority(195) remain 
unidentified because optical
spectra have not been obtained for all likely candidates. However there are
46 REX sources in which there are no optical candidate brighter than 
the APM catalog limits ($\sim$20 mag in $O$ ($\sim B$) band and $\sim$21.5 mag
in $E(\sim R)$ band). On page 4a we describe the technique 
that we used to define a REX source as an optical blank field. 
In figure 3 we show the X-ray and radio flux distributions 
of the REX sample. The filled distributions represent the 46 REX sources
with  optical blank fields. 
As shown in 
Figure 3, they are not primarily the faintest X-ray or radio objects in the 
REX sample. One possibility is that these sources are extremely high 
redshift (z$>$3.5) or obscured AGN.
%The discovery of such 
%objects would have important implications for the origin of the hard 
%X-ray background. 
%The X-ray could also be coming from distant (z$>$0.5) 
%clusters,
%which can have high X-ray to optical luminosity ratio. For example Newsam
%et al. 1997 have recently discovered two possible high redshift (z$\sim$1) 
%galaxy cluster using deep K band image around two ROSAT PSPC X-ray sources 
%with blank optical field ($i.e.$ nothing within 15$^{\prime\prime}$ of the 
%X-ray centroid with R$<$23). 

\noindent{\bf Proposed INT observations} 
We propose to obtain U, B and R CCD observations of
the complete sample of 46 optically unidentified
radio loud X-ray sources.
Using the U-B, B-R colours alone we
shall be be able to make a preliminary classification of the optical
counterparts into BL Lacs, galaxies, low redshift(z$<$2) or
high redshift(z$>$3) quasars, cluster of galaxies or obscured
AGN  and thus we can plan our 
follow-up spectroscopic phase based on more specific scientific goals.
}
\makepatttwopagethree

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% PAGE 4 OF PATT2 FORM - TECHNICAL INFORMATION (I) - FEASIBILITY, S/N, ETC %
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\technicalpage{
%\subsection*{Sample definition} 
\vspace{-0.75cm}
\paragraph*{Optical Identifications}
There are a total of 395 sources with $F_x>5\times10^{-14}$ erg cm$^{-2}$
s$^{-1}$ and $S_\nu$(20cm)$>$10mJy. Of these 349(88\%) have optical 
counterparts(as described below)
detected on APM scans on the UKST(m(B$_J$)$<$22.0) or POSS1 
(E(m$_R$)$<$20.0); O(m$_O$)$<$21.5) plates. In Figure 1 we show the magnitude 
distribution  of these 349 sources (in the case of detections on the UKST
B plates we have converted this to E using a spectral index;$\nu^\alpha$ 
of -0.5).
This fractional identification
rate(88\%) is similar to that of CRSS(91\%; 
Boyle, McMahon, Wilkes, Elvis, 1995, MNRAS, 272, 462) and
RIXOS(90\%; Carrera et al, preprint), which have similar X-ray
flux limits.

\paragraph*{Definition of an optical blank field} 
In order to find an optical
counterpart we searched for optical objects in the APM catalog within
a circle of radius 1$^\prime$ centered on the combined ROSAT-NVSS 
position. For
each optical object we have calculated the likelihood ratio which
is the ratio of the probability of finding the correct 
optical counterpart based on the positional uncertainty
relative to that of finding a similar chance background
objects (eg Sutherland and Saunders, 1992, MNRAS, 259, 413).  
In Figure 2 we show the
likelihood ratio of all the optical objects that we found in the APM
catalog (both in within a circle of 1$^\prime$ centered on the REX
position) as function of the distance between the optical object
and the REX source.
As shown in Figure 2, only 
the optical objects within $\sim$10$^{\prime\prime}$ the REX position have a 
likelihood ratio greater than 10 ($i.e.$ have a probability greater that 90
per cent to be the true identification).
Therefore we define as a blank field all the REX sources without 
an APM object within a 
circle of radius 10$^{\prime\prime}$. 
%Finally, to keep low ($ <10 \%$) the number of chance coincidence X-ray/radio 
%associations (i.e. spurious REX), we have considered
%only the REX sources with an off-axis on the ROSAT PSPC image lower than 
%35$^{\prime}$, and therefore with smaller X-ray error circles, not exceeding
%40$^{\prime\prime}$. 
Of the 395 REX sources we find that the number of
empty fields defined in this manner is 46(19 with b(galactic latitude)
$<$-30 and 27 with b$>$30).
%\subsection*{Observational program and strategy} 
\paragraph*{Observational program and strategy} 
We propose to optically identify, classify and derive
optical colours for these 46 unidentified sources
(19 in the SGC region; 27 in the NGC region) to give us
a complete sample of 395 sources. As well as optically identifying
the sources we propose to use colours to make an initial
astrophysical classification so that a follow-up spectroscopic
program can be designed on this basis, rather than
carrying out an indiscriminate redshift campaign. Based on previous
work at brighter radio fluxes (eg  
Hook \& McMahon, 1998),  we might 
expect that 75\% of these optically
unidentified (on photographic sky survey) sources shall be identified
to R=23 giving us a completeness rate of 97\% after
this phase. Of course it may be higher. {\it One purpose of this
proposal is to derive this value}.
Whilst this may be optimistic since we are studying 
radio sources 20 times fainter, in radio flux, we have to start somewhere 
and 
to invest time on longer exposures at this stage would be
unjustified. From Figure 1, one can already see that the 
magnitude distribution is converging so that by R=23
we would expect all the sources to identified.
Expectations from Signal (version 11.2) for WFC, EEV, INT and 
1$^{\prime\prime}$ seeing:
\begin{itemize}
\item 600s exposures in R; S/N=15 at R=23.0
\item 600s exposures in B; S/N=10 at B=24.4
\item 600s exposures in U; S/N=10 at U=22.8
\end{itemize}
Since we need to carry out image classification
we require a S/N$>$10 at the envisaged limit. We need
a colour limit of B$-$R$>$1.5 to identify any z$>$3
quasars.
Good quality colours are required ie 0.1-0.2 magnitudes
so a S/N of 10 is required. Ideally one would like
the U limit to correspond to U$-$B=$-$0.3 at the B band
limit to allow discrimination of z$<$2.2 quasars but  
this would require 4500s. 600s is therefore a
justifiable compromise since we do not actually know the
underlying magnitude distribution. ie for the brighter
identications this will be adequate.


%\subsection*{Observational requirements} 
\paragraph*{Observational requirements} 
We have 19 sources that are observable in semester 98B. Assuming
read out of 120seconds per source gives a total 
observing time of and a typical observing efficiency
of 80\% (ie allowing time for slewing, guide star
acquisition and standards) the total time for UBR
imaging is 14.25 hrs. We therefore request 2 nights in
the Autumn. In the semester 99A we have 27 unidentified
sources and we therefore request 3 nights for this phase of
the program.

}

\makepatttwopagefour

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% PAGE 4a OF PATT2 FORM - TECHNICAL INFORMATION (II) - REFERENCES, FIGS, ETC %
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\figsandrefspage{
\footnotesize
\underline{References:}\\
Becker, R.H., White R.L., and Helfand D.J, 1995, ApJ, 450, 559 \\
Brinkman, W et al, A\&A, 323, 739, 1997. \\
Caccianga et al, AJ, submitted \\
Ciliegi P. et al, 1995, MNRAS, 277, 1463 \\ 
Condon et al. 1998, in preparation \\
Dunlop J. et al, 1996, Nature, 381, 581 \\
Fabian A. C. et al., 1997, MNRAS, 291, L17. \\
Hook \& McMahon, 1998, MNRAS, 294, 7 \\
Maccacaro T., Caccianiga A., Della Ceca R., Wolter A. and Gioia I., 1998, Astron. Nachr, 319, 15 \\
Maccacaro T. et al. , 1994, ApL,29, 267 \\
%Newsam A.M., McHardy I.M., Jones L.R. and Mason K.O., 1997, MNRAS \\
%Rawlings S. et al., 1996, Nature, 383, 502 \\
%Voges et al. 1996, A\&A , 309, 419\\

\normalsize

\begin{minipage}{8cm}
\hspace*{0.5cm}
\psfig{file=e_histo_limit.ps,width=6cm}
\end{minipage}\hfill
\begin{minipage}{8cm} 
Figure 1. The E mag distribution of the APM objects with a likelihood ratio
greater than 10 within a circle of 10$^{\prime\prime}$ around the REX position.
\end{minipage}\hfill

\begin{minipage}{8cm}
\hspace*{0.5cm}
\psfig{file=like_20.ps,width=8cm}
\end{minipage}\hfill
\begin{minipage}{8cm} 
Figure 2. The Likelihood ratio of the APM sources within a circle 
of 1$^{\prime}$ centered on the REX (NVSS) position as function of the 
distance between the optical object and the REX source.
\end{minipage}\hfill
\begin{minipage}{8cm}
\psfig{file=flux_histo_limit.ps,width=8cm}
\end{minipage}\hfill
\begin{minipage}{8cm} 
Figure 3. The X-ray (upper panel) and radio (lower panel) 
distributions of the REX sample. The 
filled distributions represent the 46 REX sources with optical blank
field
\end{minipage}\hfill

}                     

\makepatttwopagefoura

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% PAGE 5 OF PATT2 FORM %
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\backupprogram{We will concentrate on R band imaging.
}                      % Summary of backup programme

\previous{                            % Previous applications (last 4 Sems)
\begin{tabular}[t]{p{1.5in}p{0.7in}p{0.8in}p{3.2in}}
%Patt No. & Award & clear nights & comments \\
\end{tabular}
}

\publications{
\footnotesize
%{\bf (i)}
{'The APM z$>$4 QSO Survey: Spectra and Intervening Absorption Systems'}
Storrie-Lombardi, L.J., McMahon, R.G., Irwin, M., Hazard, C., 1996,
ApJ, 468, 121--138.
\newline
%{\bf (ii)}
 {'The APM z$>$4 QSO survey for Damped Lyman alpha systems'}
 Storrie-Lombardi, L.J., McMahon, R.G., Irwin, M., 1996,
MNRAS, 282, 1330-1342.
\newline
%{\bf (iii)}
 {'Evolution of Neutral Gas at High Redshift --
 Implications for the Epoch of Galaxy Formation'}
 Storrie-Lombardi, L.J., McMahon, R.G., Irwin, M. , 1996,
 MNRAS, {283}, L79-L83.
\newline
% {\bf (iv)}
 {'A survey for high redshift radio loud quasars II Optical
 spectroscopy of a complete sample of radio sources'}
 Hook, I.M., McMahon, R.G., Irwin, M.J, Hazard, C., 1996,
 MNRAS, 282, 1274--1298.
\newline
% {\bf (v)}
{'Discovery of radio-loud quasars with z=4.72 and z=4.01'}
Hook, I.M., R. G. McMahon, R.G., 1998,
MNRAS, 294, L7-L12.

}         % List pubs with data from patt time (last 4 Sems)
\experience       {}         % Experience of observers on other telescopes
\graduatestudent  {}{}       % Research student {Name of student}{Project}
\grant {Dr P C Hewett}{PATT Travel for the IoA}{GR/J33319}
\nonstandardtravel{}         % Justify T&S for more than one UK oberver
\otherexpenditure {}         % eg for freight etc.

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\shorttitle {}               % Ignore if you are an ING applicant.

%\makepatttwopagesix         % If you are an ING applicant - leave the '%' in!
                             % If you want this page (e.g. if you are using
                             % this file to create a paper copy for UKIRT),
                             % then edit out the '%'

%\formloadfile{formload.dat} % If you are an ING applicant - leave the '%' in!
%\writeformloadfile          % If you are an ING applicant - leave the '%' in!
                             % These last two lines can be used to write a
                             % FORMLOAD (.dat) file (e.g. for AAT electronic
                             % submission).

\end{document}
                                                  














