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\bfseries\uppercase{%
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The Candidate LLAGN in the Nearby Elliptical Galaxy NGC\,4621
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\section{Scientific Justification}

Dynamical studies have established that supermassive black holes, with
masses $M_\bullet = 10^6 - 10^9 M_\odot$, occur in the nuclei of most
nearby galaxies with stellar bulges.  Yet few of these massive black
holes are observed as luminous active galactic nuclei (AGNs).  Rather,
the Palomar spectroscopic survey [2] showed that the majority have
either no AGN signatures or only the weak AGN signatures that define
them as low-luminosity AGNs (LLAGNs; $L(H\alpha) <
10^{40}$~ergs~s$^{-1}$).  Also, Chandra surveys of selected Palomar
LLAGNs [3,9] commonly find X-ray nuclei with $L(2-10~keV) = 10^{38} -
10^{42}$~ergs~s$^{-1}$, leading to $L(2-10~keV) <
10^{42}$~ergs~s$^{-1}$ as an X-ray definition of a LLAGN.  For the
black hole masses involved, such H$\alpha$ and X-ray luminosities are
highly sub-Eddington.  Understanding the radiative quiescence of these
massive black holes has important implications for accretion physics,
fuelling mechanisms, and black-hole growth over cosmic time [5,8].

Etc ...

We wish to build upon our published and archival studies of the nearby
elliptical NGC\,4621.  Its weak radio nucleus needs to be localized to
subarcsecond scales and separated from any extranuclear radio
emission, to enable Chandra/VLA photometry at matched resolutions of
about 0.3 arcsec.  This requires new VLA data at its most sensitive
frequency (8.5~GHz) and in its most extended configuration (A).

\begin{figure}[tbh]
\includegraphics[scale=0.4]{f1.eps}
\caption{\em{NGC\,4621 at 0.5-8 keV over a field of view of 90 arcsec.
The strongest source is the candidate nucleus and has $L(2-10~keV) =
6.8 \times 10^{37}$~ergs~s$^{-1}$. 1 arcsec = 88~pc.}}
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\section{References}

\noindent [1] Di Matteo et al. 2000, MNRAS, 311, 507
   
\noindent [2] Ho et al. 1997, ApJS, 112, 315

\noindent [3] Ho et al. 2001, ApJ, 549, L51

\noindent [4] Ho et al. 2003, ApJ, 583, 159

\noindent [5] Ho 2004, COAS Volume 1, 292

\noindent [6] Nagar et al. 2005, A\&Ap, 435, 521

\noindent [7] Narayan \& Quataert 2005, Science, 307, 77           

\noindent [8] Pellegrini 2005, ApJ, 624, 155

\noindent [9] Terashima \& Wilson 2003, ApJ, 583, 145

\noindent [10] Terashima et al. 2004, IAUS 222, 61

\noindent [11] Wrobel \& Heeschen 1991, AJ, 101, 148

\noindent [12] Wrobel \& Herrnstein 2000, ApJ, 533, L111

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