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\rhead{Monitoring southern hemisphere \Fermi-detected AGNs}
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\title{\hm\vspace{-8ex} \LARGE\bf Monitoring southern hemisphere \Fermi-detected AGNs with
the Radio Interferometer in New Zealand}

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\vspace{-14ex}\hfill \framebox{\Large\bf Competition sensitive! Draft of \isodate }\vspace{12ex}

\section{Introduction}
  
   Analysis of \Fermi\ LAT data revealed that more than one half of detected 
points sources are active galactic nuclei (AGNs). The intrinsic property of 
AGNs is variability at scales from days to decades at all wavelengths from 
radio to hard $\gamma$-rays. One of major outcomes of \Fermi\ mission is 
monitoring of $\gamma$-ray loud AGNs. High energy light curves together with 
the spectrum in MeV--GeV range and position localisation is the legacy data 
product of the mission. In order to enhance the outcome of the \Fermi\ 
mission, matching monitoring programs at other wavelengths are needed. The 
most comprehensive matching program is the The OVRO 40-Meter Telescope 
Monitoring Program that observes for 10 year a list of 1835 AGNs at 
declinations $>-20^\circ$, including 930 $\gamma$-rays associated sources 
from FL8Y catalogue of point sources with a cadence of 2 times a month.
The SED of AGNs has two distinctive broad peaks: one spanning from radio 
through optic to soft X-ray and another spanning from KeV to TeV. Emission 
mechanism of two peaks is different. Therefore, monitoring in radio does not 
duplicate monitoring in $\gamma$-ray range, but provides additional 
complementary information.

   Radio/$\gamma$-ray monitoring data are used for statistical study of the 
AGN population and for case study of selected sources. The focus of 
statistical studies is on deriving the radio and radio/$\gamma$-ray 
observational properties of the AGN population, including a) the radio 
variability properties of the AGN population, their dependence on redshift, 
spectral classification, luminosity, etc; b) any differences between the 
radio properties of \Fermi\ detected AGNs and AGNs with similar radio 
luminosity which have not been detected by \Fermi; c) the properties of 
cross-correlations between radio and $\gamma$-ray flares. The focus of case 
studies is to derive time delay between $\gamma$-ray and radio flares and 
detect periodicities and peculiarities in light curves.

   The OVRO blazar monitoring program is highly successful: by 2018 over
one hundred peer-reviewed and proceedings papers used the light curves
from that program. But geography sets the limit of the program: sources
with declinations below $-20^\circ$, i.e. 1/3 of the sky are excluded.

\section{New observing capabilities in the southern hemisphere}

  The majority of radio telescopes is located in the northern hemisphere.
Few existing telescopes are over-subscribed. To make things worse, 
budgeting restriction for last 2--5 years reduced the amount of time
existing radiotelecopes at the south are available to work for 
sciences, f.e. Parkes and Mopra. In this situation a large dedicated
program on existing radioastronomical facilities is highly problematic.
Our group spend XXX years for converting a former telecommunication 
32-m dish in Warkworth (latitude: $-36.4^\circ$, 
longitude: $174.7^\circ$), New Zealand, to a working radiotelescope. 
In 2014 first successful results at 6.7 GHz receiver were obtained 
\citet{r:wa15} and in August 2017 first successful observations using 
a 8~GHz receiver were made. There is a smaller 12m radio-telescope 
designed for geodesy also equipped with a 8~GHz receiver at 185.226 
meter distance from the 32m telescope. Since August 2017 both telescopes 
participate in VLBI observations at X-band (8 GHz). Analysis of VLBI 
results at 185m long baseline showed excellent performance: residual 
phase delays over 24 hour period has a scatter of 5~ps, i.e. phase 
is stable with rms of $15^\circ$ and fringe amplitude is also stable.

  This prompts us to propose a program of using a former 
telecommunication dish and the geodetic radio telescope as a radio 
interferometer suitable for source flux density monitoring. We measured
sensitivity of the interferometer and found that we can determine flux 
density of a 50~mJy source with the thermal noise of 5~mJy using 
8~minute integration time.

\section{Proposed work}

  We propose to launch a program of monitoring \underline{\bf{all}}
\Fermi\ associated AGNs with declinations $< 0^\circ$ with flux densities
brighter 50~mJy at 8 GHz with the Radio Interferometer at New Zealand (RINZ) 
that consists of two radio telescopes 185 meter apart. We have identified
773 such sources in the FL8Y catalogue. Each source will be observed from
1 to 8 minutes, depending on flux density, at the interferometer. We plan
to observe two twenty four hour sessions per week, 2500 hours per year.
It will require four days to observe the entire list. Thus, our radio
monitoring program will provide light curves with a cadence $\sim\! 15$ days,
close to that provided by the  OVRO monitoring program. We reserve 
a room for $\sim\! 50$ more sources that will be added to the program upon
a request, for instance, newly detected sources or flaring sources.
We intentionally set the overlap with the OVRO program in the declination
range of -$20^\circ$ to $0^\circ$. The purpose of this overlap is to check 
consistency of our results with respect to the OVRO monitoring results.

\section{Significance of the proposed work}

{\bf We need shhow here why covering remaining 1/3 skay with monitoring
is important for \Fermi\ mission. For instance, we can stress important
of case studies that will allow us to find time delay gamma-radio
for flaring sources. \ldots}


\section{Logistics of the proposed program}

  The data will be recorded at 2 Gbps rate in dual-polarizations and 
transferred via ftp to the computer center of Auckland university 
for correlation. Then the  data will be correlated, fringe-fitted, and 
calibrated. The estimates of flux density including all four Stokes 
parameters will be made publicly available at the project web site 
immediately after completion of analysis, i.e. within 5--15 days after 
observations.

  Calibration will be performed by firing the noise diode of the antenna 
calibration unit before observation of every program source, which is 
a standard procedure in radio interferometry, by observing amplitude 
calibrator radio sources, and by observing common sources with the OVRO 
program. Our goal is to reach 5\% accuracy in calibration and 5~mJy error 
floor. At the moment, only the 30m radiotelescope is equipped with the 
antenna calibration unit. The second 12m radiotelescope designed for geodesy
does not have it. The lack of the antenna calibration unit at the 2nd
antenna adversely affects accuracy of calibration, since antenna gain 
fluctuations at the 12m antenna remain unchecked. Our analysis of VLBI
observations with the 12m antenna provided us the estimate of accuracy of 
the antenna calibration without the noise diode at a level of 20\%. 

  Therefore, we request funds on amount of \$30,000 to purchase the antenna 
calibration unit by the performing organization from the Haystack observatory, 
MIT that manufactures them. The performing organization will loan the unit to 
the Auckland university for the duration of this observing program. Using 
antenna calibration units at both will reduce calibration errors from 20\% 
to 5\%, which is typical for radio interferometers. Calibration accuracy
5\% is required for scientific analysis of light curves. For comparison,
the OVRO program has calibration errors on a level of 2--3\%.

  We request funds at 0.1 FTE level for the PI, Leonid Petrov, for development
of the pipeline of data analysis. No funds are requested for foreign 
co-investigators. Their labor cost as well asoperational cost of running the 
interferometer is covered by Auckland University. The total amount of requested
funds is \$55,000.

  This monutoring progam will be the most valuable if preformed concurrently 
with \Fermi\ observation. Since the \Fermi\ mission will not last forever,
we are hurring up to start observing program as soon as possible, while 
it is operating.

\begin{thebibliography}{3}

   \bibitem[Richards et al.(2011)]{r:ovro}
      Richards, J.~L.,  et al., ApJS, 194. 29, 2011.

   \bibitem[Petrov et al.(2015)]{r:wa15}
      Petrov, L. at al.  PASP, 127, 516--522, 2015.


\end{thebibliography}

\end{document}

