text:
\section{Introduction}\label{sec1}
Investigation of the distribution, kinematics, and mass of dense molecular material
in the centers of galaxies plays a key role in studying the evolution of galaxies
because it is the reservoir of fuel for active galactic nuclei (AGNs), and also the site of massive star formation (starburst = SB).
On the other hand, these heating sources significantly affect their surrounding gas in radiative and/or mechanical ways.
For example, intense UV radiation from massive stars forms photodissociation regions (PDRs) around them,
and X-ray dominated regions (XDRs), which can be larger in volume than PDRs, are formed in the vicinity of AGNs
(e.g., \citealt{1996ApJ...466..561M,1999RvMP...71..173H,2005A&A...436..397M,2007A&A...461..793M}).
Cosmic rays from frequent supernovae (SNe) and the injection of mechanical energy due to SNe
or AGN jet/outflow (mechanical heating) are also important for the chemical layout
(e.g., \citealt{2011A&A...525A.119M,2012A&A...542A..65K,2015A&A...574A.127K,2015ApJ...799...26M}).
Thus, the dense molecular gas can provide us critical information on the nature of
the underlying physical processes accompanying the non-thermal radiation in the centers of galaxies.

Millimeter/submillimeter spectroscopic observations are indispensable for such a study
since they can trace dense, cold molecular material with little dust extinction,
which takes the bulk of gas mass in the nuclear regions of galaxies.
This would contrast with observations of warm molecular gas such as H$_2$ 1-0 S(1) in the near-IR (e.g., \citealt{2009ApJ...696..448H}).

Nevertheless, our knowledge on the circumnuclear dense molecular matter has still been limited, especially for AGNs.
This is because there have been only a small number of high resolution (i.e., $\sim$ 100 pc or higher scale)
and sensitive observations of dense molecular gas even in nearby AGNs
(e.g., \citealt{2010A&A...519A...2G,2011ApJ...736...37K,2012MNRAS.424.1963S,2015ApJ...799...26M}),
although several low resolution surveys of dense gas have been conducted
with single dish telescopes to address their global properties (e.g., \citealt{2004ApJS..152...63G,2004ApJ...606..271G}).

This situation is now being improved significantly by the advent of the {\it{Atacama Large Millimeter/submillimeter Array (ALMA)}}.
Indeed, the spatial distribution, kinematics, and the chemistry have been reported in greater detail for,
e.g., NGC 1068 (\citealt{2014A&A...567A.125G,2014A&A...570A..28V,2014PASJ...66...75T,2015PASJ...67....8N})
, NGC 1097 (\citealt{2013PASJ...65..100I,2013ApJ...770L..27F,2015A&A...573A.116M}),
NGC 1433 (\citealt{2013A&A...558A.124C}), and NGC 1566 (\citealt{2014A&A...565A..97C}).
Among these works, \citet{2013PASJ...65..100I} (hereafter \citetalias{2013PASJ...65..100I}) suggested
that HCN(4-3)/HCO$^+$(4-3) and HCN(4-3)/CS(7-6) integrated intensity ratios seem to be
higher in AGNs than in SB galaxies ({\it{submm-HCN enhancement}}),
although the number of the sample galaxies in \citetalias{2013PASJ...65..100I} is few
and the actual cause of the enhancement is not clear.

With the above things in mind, we here present the results of our high resolution
ALMA band 7 observations of submillimeter dense gas tracers towards the central kpc region of NGC 7469.
Because NGC 7469 hosts a luminous type-1 AGN
($L_{\rm{2-10keV}}$ = 1.5 $\times$ 10$^{43}$ erg s$^{-1}$; \citealt{2014ApJ...783..106L}),
we can investigate the effects of AGN luminosity on the surrounding molecular gas
with little uncertainty by directly comparing the results
with those obtained in the type-1 low-luminosity
($L_{\rm{2-10keV}}$ = 6.9 $\times$ 10$^{40}$ erg s$^{-1}$; \citealt{2014ApJ...783..106L})
AGN, NGC 1097 (\citetalias{2013PASJ...65..100I}).

\subsection{The target galaxy NGC 7469}\label{sec1.1}
NGC 7469 is an active galaxy with a large scale (several kpc)
stellar bar detected at near-IR (NIR) wavelength (\citealt{2000ApJ...529...93K}).
This galaxy is located at the distance of 70.1 Mpc
($z$ = 0.0164; \citealt{1990ApJ...354..158M}) thus 1$''$ = 330 pc,
and hosts a luminous type-1 Seyfert nucleus as evidenced by
broad Balmer emission lines (FWHM of H$\beta$ = 4369 km s$^{-1}$; \citealt{2014ApJ...795..149P})
with time variability (e.g., \citealt{1990ApJ...353..445B,1998ApJ...500..162C}).
Time variability is also confirmed by UV and X-ray observations
(e.g., \citealt{2000ApJ...535...58K,2000ApJ...544..734N,2004A&A...413..477P,2005ApJ...634..193S}),
revealing this nucleus is indeed an AGN.
NGC 7469 is also classified as a luminous infrared galaxy (LIRG) due to its high IR luminosity
($L_{\rm {8-1000}}$ $\equiv$ $L_{\rm IR}$ = 10$^{11.7}$ $L_\odot$; \citealt{2003AJ....126.1607S}).

The type-1 AGN is surrounded by a luminous circumnuclear SB ring
with a radius of 1.5$''$--2.5$''$ or 495--825 pc (e.g., \citealt{2003AJ....126..143S,2007ApJ...661..149D}, see also Figure \ref{figure1}a),
which accounts for two thirds of the bolometric luminosity of the galaxy (\citealt{1995ApJ...444..129G}).
Therefore, this galaxy provides us with a nice opportunity to investigate how AGN and SB
influence their surrounding molecular gas when observed at high resolution.

The SB ring is prominent at various wavelengths including centimeter
(\citealt{1991ApJ...378...65C,1991ApJ...381...79W,2010MNRAS.401.2599O}),
far-IR (FIR, \citealt{2000ApJ...537..631P}), mid-IR (MIR, \citealt{2003AJ....126..143S,2004ApJ...605..156G}),
NIR (\citealt{1995ApJ...444..129G}), optical-to-UV (\citealt{1998ApJS..117...25M,2000MNRAS.311..120D,2007ApJ...661..149D}),
and soft X-ray (\citealt{1996ApJ...468..191P}).
A tidal interaction with its neighbor IC 5283 ($\sim$ 1.3$'$ away from NGC 7469) is believed
to have caused the powerful SB activity (e.g., \citealt{1994AJ....108...90M,1995ApJ...444..129G}).
Dusty, young ($<$ 100 Myr), and massive star clusters
(individual typical mass is 10$^{6-7}$ $M_\odot$) exist within the ring (e.g., \citealt{2007ApJ...661..149D}).

As for the central $\sim$ 1$''$ region, multi-wavelength studies including
centimeter, K-band (2.2 $\mu$m), and 3.3 $\mu$m PAH feature indicate
that the AGN is energetically dominant at these wavelengths
(\citealt{2003ApJ...592..804L}; \citealt{1995ApJ...444..129G}; \citealt{2004ApJ...617..214I}),
although one third of the K-band continuum is of stellar origin (\citealt{1995ApJ...444..129G}).
A core jet-like structure (e.g., \citealt{2003ApJ...592..804L,2006ApJ...638..938A}) and ionized outflows
(\citealt{2005ApJ...634..193S,2007A&A...466..107B}) have also been observed in this AGN.
Reverberation mapping revealed the mass of the central supermassive black hole ($M_{\rm BH}$) to be
$\sim$ 1 $\times$ 10$^7$ $M_\odot$ (\citealt{2004ApJ...613..682P,2014ApJ...795..149P}).
This $M_{\rm BH}$ is typical for QSOs at $z$ = 5 on average, which will eventually
grow up to $M_{\rm BH}$ = 10$^9$ $M_\odot$ at $z$ = 0 (\citealt{2009ApJ...690...20S}).
In addition, the Eddington ratio of this AGN ($\sim$ 0.3; \citealt{2004A&A...413..477P}) is also comparable to those of QSOs.
Therefore the obtained spectrum of NGC 7469 could serve as a local template for high redshift QSOs as well.
Other relevant properties of NGC 7469 are summarized in Table \ref{tbl1} with the information shown above.

\begin{table*}
\begin{center}
\caption{Properties of NGC 7469 \label{tbl1}}
\begin{tabular}{ccc}
\tableline\tableline
Parameter & Value$^a$ & Reference$^b$ \\
\tableline
RC3 morphology & (R$'$)SAB(rs)a & (1) \\
Position of the nucleus &  & (1) \\
$\alpha_{\rm J2000.0}$ & 23$^{\rm h}$03$^{\rm m}$15.6$^{\rm s}$ &  \\
$\delta_{\rm J2000.0}$ & +08$^\circ$52$'$26.4$''$ &  \\
Position angle [${}^\circ$] & 128 & (2) \\
Inclination angle [${}^\circ$] & 45 & (2) \\
Recession Velocity [km s$^{-1}$] & 4925 ($z$=0.0164) & (3) \\
Adopted distance [Mpc] & 70.1 &  \\
Linear scale [pc arcsec$^{-1}$] & 330 &  \\
Nuclear activity & Seyfert 1 & (4) \\
$L_{\rm 2-10keV}$ [erg s$^{-1}$] & 1.5 $\times$ 10$^{43}$ & (5) \\
$L_{\rm IR}$ [$L_\odot$] & 2.5 $\times$ 10$^{11}$ & (6) \\
$<$SFR$>$ (CND) [$M_\odot$ yr$^{-1}$ kpc$^{-2}$] & 50--100 & (7) \\
Stellar age (CND) [Myr] & 110--190 & (7) \\
\tableline
\end{tabular}
\tablecomments{$^{(a)}$ The LSR velocity of the center of the galaxy is obtained from the CO(1-0) emission. We use this value to calculate the distance to NGC 7469 and the linear scale,
by assuming $H_0$ = 71 km s$^{-1}$ Mpc$^{-1}$, $\Omega_{\rm M}$ = 0.27, and $\Omega_{\rm \Lambda}$ = 0.73 cosmology.
The $<$SFR$>$ (CND) indicates the averaged star formation rate over the central $\sim$ 1$''$ region (i.e., circumnuclear disk = CND).
The stellar age is also for the CND.
$^{(b)}$ (1) NASA/IPAC Extragalactic Database (NED, \url{http://ned.ipac.caltech.edu}); (2) \citet{2004ApJ...602..148D}; (3) \citet{1990ApJ...354..158M};
(4) \citet{1993ApJ...414..552O}; (5) \citet{2014ApJ...783..106L}; (6) \citet{2003AJ....126.1607S}; (7) \citet{2007ApJ...671.1388D}.
}
\end{center}
\end{table*}

Observations of CO molecules revealed the existence of
a large amount of cold molecular gas (e.g., \citealt{1988ApJ...324L..55S,1990ApJ...354..158M,2009A&A...493..525I}),
as well as warm molecular gas (\citealt{2015ApJ...801...72R}) in the central region of NGC 7469.
The detailed spatial structure and the dynamics of the cold molecular gas were first investigated
by high resolution (0.7$''$) CO(2-1) observations (\citealt{2004ApJ...602..148D}).
Their CO(2-1) map also showed a ring-like structure with a similar radius
seen at other wavelengths, and a bright extended ($\sim$ 1$''$) nuclear region.
Note that we hereafter call this kind of (100 pc scale) central molecular concentration
a {\it{circumnuclear disk (CND)}} in general.
\citet{2004ApJ...602..148D} also found a bar or a pair of spiral arms between the ring and the CND,
which is only visible in the molecular emission, and not prominent at NIR wavelengths.
This configuration is quite unusual (see Section \ref{sec5}).
The total molecular gas mass inside the $r$ $<$ 2.5$''$ (825 pc) region
inferred from their observations is 2.7 $\times$ 10$^9$ $M_\odot$.
The spatial distributions of typical dense gas tracers such as HCN and HCO$^+$, on the other hand,
have not been clear due to the lack of spatial resolution of previous studies.

In this paper, we present the spatial distribution and line ratios of submillimeter dense gas tracers
based on our high resolution (0.50$''$ $\times$ 0.40$''$, 1$''$ = 330 pc) ALMA observations of
the central kpc region of NGC 7469 involving HCN(4-3), HCO$^+$(4-3), CS(7-6), and partially CO(3-2) lines,
and the underlying continuum emission.
Our new ALMA observations improved this situation;
we clearly separated the CND from the SB ring, and then obtained a spectrum of each component.
The spatial resolution of this study (0.5$''$) is comparable to that of the
CO(2-1) observation (0.7$''$) by \citet{2004ApJ...602..148D},
so that we can directly compare the molecular gas distributions and kinematics.
Note that, however, the spatial resolution of this study ($\sim$ 150 pc) would still be insufficient
to exclusively probe the region where gas heating due to an AGN with NGC 7469-like luminosity dominates (see Appendix-\ref{app-A} for details).

We describe in Section \ref{sec2} the details of our observations.
An 860 $\mu$m continuum map and a nuclear spectral energy distribution are shown in Section \ref{sec3}.
A full band 7 spectrum and some line ratios are presented in Section \ref{sec4},
although we will extensively compare the line ratios with those obtained in other galaxies
and discuss the possible causes of the HCN-enhancement in our succeeding paper (Izumi et al. submitted).
The spatial distributions of the submillimeter dense gas tracers are shown in Section \ref{sec5}.
Finally, our main conclusions are summarized in Section \ref{sec6}.
A kinematic study using our data is presented in \citet{2015ApJ...806L..34F}.

\section{Observation and data reduction}\label{sec2}
\subsection{ALMA band 7 data of NGC 7469}
NGC 7469 was observed with ALMA on 2013 November 3-4
with 28 antennas in C32-2 configuration, as a Cycle 1 early science program (ID = 2012.1.00165.S, PI = T. Izumi).
Baseline lengths range from 15.0 to 1284.3 m (corresponds to the $uv$ distance from 17.4 to 1493.4 k$\lambda$ at 860 $\mu$m).
The observations were conducted in a single pointing with a 18$''$ field of view,
which fully covered the nucleus and the SB ring (total $\sim$ 4$''$ in diameter).
We set the phase tracking center to ($\alpha_{\rm J2000.0}$, $\delta_{\rm J2000.0}$)
= (23$^{\rm h}$03$^{\rm m}$15.64$^{\rm s}$, +08$^\circ$52$'$25.80$''$).
The receiver was tuned to cover the redshifted lines of HCN(4-3) (rest frequency $\nu_{\rm rest}$ = 354.505 GHz),
HCO$^+$(4-3) ($\nu_{\rm rest}$ = 356.734 GHz) in the upper side band,
and CS(7-6) ($\nu_{\rm rest}$ = 342.883 GHz), CO(3-2) ($\nu_{\rm rest}$ = 345.796 GHz) in the lower side band,
both in the 2SB dual-polarization mode.
Each spectral window has a bandwidth of 1.875 GHz,
and two spectral windows were set to each sideband
to achieve a total frequency coverage of $\sim$ 7.5 GHz.
The velocity spacing was originally 0.43 km s$^{-1}$ (488 kHz) per channel,
but 47 channels were binned to improve the signal-to-noise (S/N) ratio,
which resulted in a final velocity resolution of $\sim$ 20 km s$^{-1}$.
In the following, we express velocities in the optical convention.
Note that we could only cover the CO(3-2) line with $V_{\rm LSR}$ $>$ 4900 km s$^{-1}$
due to the limited band width for ALMA Cycle 1 observations,
the recession velocity (4925 km s$^{-1}$, defined by CO(1-0) observations; \citealt{1990ApJ...354..158M}),
and the molecular line width of NGC 7469 (typically full width at half maximum = FWHM $\sim$ 200 km s$^{-1}$ at the nucleus).
The bandpass, phase, and flux were calibrated with
3C454.3, J2257+0743 (this object is 2$^\circ$ away from NGC 7469), and J2232+117, respectively.
Weather conditions were good throughout the observations
with system temperatures of 100--200 K (usually 100--150 K).
The total on-source integration time was $\sim$ 55 min.

The reduction and calibration of the data were done with
CASA version 4.1 (\citealt{2007ASPC..376..127M}) in standard manners,
and the data was delivered to us from the East Asia ALMA Regional Center.
All images of the line and continuum emissions were reconstructed
with the CASA task \verb|CLEAN| (gain = 0.1, threshold = 1.0 mJy, weighting = natural).
These images were further analyzed with MIRIAD (\citealt{1995ASPC...77..433S}).
The achieved synthesized beams were typically 0.50$''$ $\times$ 0.40$''$,
corresponding to 165 pc $\times$ 132 pc ($\sim$ 150 pc
for the geometric mean) at the assumed distance of NGC 7469.
The rms noise in the line channel maps is 0.55--0.58 mJy beam$^{-1}$
at a velocity resolution of 20 km s$^{-1}$ after a primary beam correction,
and measured at areas free of line emission.
However, in channels including CO(3-2) emission,
the rms increases to $\sim$ 2.3 mJy beam$^{-1}$, probably due to remaining sidelobes.
For the continuum emission, the channels free of line emission were averaged,
which resulted in an rms of 0.09 mJy beam$^{-1}$
centered at $\nu_{\rm rest}$ = 349.7 GHz (860 $\mu$m),
after combining both the LSB and USB data.
This continuum emission was subtracted in the $uv$-plane before making line maps.
The conversion factors between Jy beam$^{-1}$ and K are 51.50, 51.60, 50.47, and 51.83 K (Jy beam$^{-1}$)$^{-1}$
for CS(7-6), CO(3-2), HCN(4-3), and HCO$^+$(4-3), respectively.

We used the MIRIAD task \verb|MOMENT| to make the integrated intensity maps presented in Section \ref{sec5},
by computing the zeroth moment of each data cube without any clipping.
The velocity range included for the integration was
$\sim$ 4650--5250 km s$^{-1}$ for CS(7-6), HCN(4-3), and HCO$^+$(4-3),
but the lower limit was 4900 km s$^{-1}$ for CO(3-2) due to our spectral setting restrictions.
These velocity ranges can cover the whole spectral range obtained within our 18$''$ field of view, except for CO(3-2).
Throughout this paper, the pixel scale of ALMA images is set to 0.1$''$,
and the displayed errors indicate only statistical ones unless mentioned otherwise.
We use line intensities corrected for the primary beam attenuation for quantitative discussions.
But this correction is not critical since most of the emission is within $\sim$ 4$''$.
The adopted systematic error of the absolute flux calibration was 10 \%\footnote{\url{https://almascience.eso.org/documents-and-tools/cycle-1/alma-proposers-guide}}.

\subsection{Ancillary data}
We retrieved the {\it{Hubble Space Telescope (HST)}} ACS/HRC image (F550M) of NGC 7469
from the Hubble Legacy Archive (HLA)\footnote{\url{http://hla.stsci.edu}}.
This image was calibrated by the HST pipeline products in a standard manner.
We used the image only to check the positional consistency
or shift between peaks in optical (V-band) and our ALMA band 7 images as shown in Section \ref{sec3}.

\section{860 $\mu$m continuum emission}\label{sec3}
Figure \ref{figure1}a shows the 860 $\mu$m continuum emission
overlaid on the HST V-band (F550M) emission in the central 2 kpc region of NGC 7469.
In this figure, we can see a bright central source,
which corresponds to the CND as defined in Section \ref{sec1.1},
and some knots in the SB ring with a radius of $\sim$ 1.5$''$ ($\sim$ 500 pc).
The peak position of the 860 $\mu$m continuum emission is
($\alpha_{\rm J2000.0}$, $\delta_{\rm J2000.0}$)
= (23$^{\rm h}$ 03$^{\rm m}$ 15$^{\rm s}$.62, +08$^\circ$ 52$'$ 26.04$''$),
which precisely coincides with that of the VLA 8.4 GHz (3.5 cm)
continuum emission (\citealt{1991ApJ...378...65C,2010MNRAS.401.2599O};
their angular resolutions were 0.22$''$--0.25$''$).
This precise match supports the accuracy of the astrometry of ALMA.
We hereafter treat this peak position as the position of the AGN of NGC 7469.
The 860 $\mu$m flux density there (marked as A in Figure \ref{figure1}a)
is 5.19$\pm$0.09 mJy beam$^{-1}$.
The 860 $\mu$m knots in the SB ring (marked as B, C, and D in Figure \ref{figure1}a)
coincide with those visible at centimeter wavelengths
(e.g., 8.4 GHz; \citealt{2010MNRAS.401.2599O}),
and the knots of dense molecular gas tracers such as
CO(3-2), HCN(4-3), and HCO$^+$(4-3) (Section \ref{sec5}).
On the other hand, there is inconsistency between the peak positions
of the 860 $\mu$m and those of the V-band emissions.
The magnitude of this positional shift is $\sim$ 0.5$''$,
which is the same size as our synthesized beam and thus significant.
Similar discrepancy was also reported between the PdBI CO(2-1) emission
and HST J-band maps (\citealt{2004ApJ...602..148D}),
and between centimeter and J, H, K-bands maps (\citealt{1995ApJ...444..129G}), for example.
Although one possible explanation for the discrepancy is
that the absolute astrometry of HST is slightly off,
it is rather likely that the stellar light is obscured by large amounts of dust
traced by the 860 $\mu$m emission as also suggested by \citet{2007ApJ...661..149D}.

We also investigated the origin (thermal or non-thermal) of the 860 $\mu$m continuum at the position-A
by constructing the spectral energy distribution (SED) as shown in Figure \ref{figure1}b.
We used high angular resolution (comparable to, or higher than our ALMA band 7 resolution = 0.5$''$) data of
4.9 GHz from \citet{1991ApJ...381...79W}, 8.4 GHz and 14.9 GHz from \citet{2010MNRAS.401.2599O},
11.8 $\mu$m and 18.7 $\mu$m from \citet{2010MNRAS.402..879R}, and J, H, and K-bands from \citet{1995ApJ...444..129G}.
The systematic flux uncertainty is included.
Although the data is sparse at the submilimeter to FIR range,
the SED indicates that the centimeter continuum emission can be
well reproduced as synchrotron ($\alpha$ = -0.62$\pm$0.02; flux $\propto$ $\nu^\alpha$),
whereas the flux density of the 860 $\mu$m continuum is well beyond the expected value of the synchrotron emission,
i.e., the 860 $\mu$m continuum is dominated by thermal emission.
Note that the percentage of the 860 $\mu$m continuum that is due to synchrotron is $\sim$ 30\% as estimated from the above scaling.
In addition, we used the \verb|CLEAN| algorithm to deconvolve the continuum emission in the LSB and USB of ALMA band 7 separately.
Then, the flux at position-A is 4.66$\pm$0.13 mJy beam$^{-1}$ and 5.00$\pm$0.13 mJy beam$^{-1}$ at 343.7 GHz and 356.0 GHz, respectively
(errors indicate statistical ones only since they were observed simultaneously), suggesting a positive spectral index
($\beta$ = 0$\pm$1; flux $\propto$ $\nu^{(2+\beta)}$, but the number of data points is just two for this fitting).
Therefore, we conclude that the 860 $\mu$m continuum at the position-A mainly originates from thermal dust.

\begin{figure*}
\epsscale{1}
\plotone{f1.eps}
\caption{(a) Continuum map towards the central 2 kpc region of NGC 7469
at 860 $\mu$m (contours) overlaid on the HST-V band (F550M) map (color; the intensity scale only indicates the counts).
Contours are 3, 5, 10, 20, 30, 40, and 50 $\sigma$, where 1 $\sigma$ = 0.09 mJy beam$^{-1}$.
The maximum is 5.19 mJy beam$^{-1}$.
The central cross indicates the peak position of the VLA 8.4 GHz continuum (\citealt{1991ApJ...378...65C}),
which is identical to that of the 860 $\mu$m continuum.
We regard this position as that of the AGN.
The white filled ellipse indicates the synthesized beam at 860 $\mu$m (0.50$''$ $\times$ 0.40$''$, PA = 68.6$^\circ$).
The AGN position and three bright knots in the SB ring are marked as A, B, C, and D, respectively.
(b) The nuclear SED of the continuum emission in NGC 7469.
We used 4.9 GHz data from \citet{1991ApJ...381...79W}, 8.4 GHz and 14.9 GHz data from \citet{2010MNRAS.401.2599O},
our ALMA band 7 data (red square), 18.7 $\mu$m and 11.8 $\mu$m data from \citet{2010MNRAS.402..879R}, and J, H, K-bands data from \citet{1995ApJ...444..129G}.
The solid and dashed lines indicate $\nu^\alpha$ and $\nu^{2+\beta}$ scalings with $\alpha$ = -0.62 and $\beta$ = 1.5, respectively.
The systematic flux errors are included in this plot.
}
\label{figure1}
\end{figure*}

\section{Band 7 spectra, line ratios, and dense molecular gas mass}\label{sec4}
Here we show the ALMA band 7 spectra in Figure \ref{figure2}.
These spectra were extracted from a single synthesized beam (150 pc-resolution) placed at the positions A-D in Figure \ref{figure1}a, for comparison.
The strongest line at the position-A is CO(3-2), followed by HCN(4-3), HCO$^+$(4-3), and CS(7-6).
Other lines were not detected (i.e., $<$ 3 $\sigma$) or are blended with other lines,
and their spectral positions are marked by black arrows in Figure \ref{figure2}.
On the other hand, at the SB ring (positions B-D), HCO$^+$(4-3) is brighter than HCN(4-3).
The FWHM of the HCN(4-3) and HCO$^+$(4-3) emissions are
200 and 190 km s$^{-1}$, 66 and 60 km s$^{-1}$, 41 and 42 km s$^{-1}$, and 50 and 50 km s$^{-1}$ at the positions A-D,
respectively (see also Figures \ref{figure4} and \ref{figure5}).
Thus, these values are consistent with each other,
which suggests that they are tracing the same volume.
We list the emission line parameters at these positions in Table \ref{tbl2} with other relevant quantities.

\begin{figure*}
\epsscale{1}
\plotone{f2.eps}
\caption{ALMA band 7 spectra extracted with a single synthesized beam (150 pc-resolution)
placed at positions-A, B, C, and D in Figure \ref{figure1}a.
The flux of the spectral window containing CO(3-2) emission line is reduced by 20 times for a presentation.
At the position-A (= AGN), we detected CO(3-2), HCN(4-3), HCO$^+$(4-3), and CS(7-6) with $>$ 3 $\sigma$ significance.
Other lines were undetected (i.e., $<$ 3 $\sigma$) or blended with other lines.
Their expected locations are marked by black arrows in the top panel.
The redshift of the nucleus assumed in this study is $cz$ = 4925 km s$^{-1}$,
based on CO(1-0) observations (\citealt{1990ApJ...354..158M}).
The Gaussian fit to the observed CS(7-6), CO(3-2), HCN(4-3), and HCO$^+$(4-3)
emissions is represented by the red line.
The fitting parameters can be found in Table \ref{tbl2}.
As for CO(3-2), we could not cover the whole spectral range in our observations.
Thus, we use the peak flux density in the channel map (Figure \ref{figure3})
and the FWHM of HCN(4-3) emission line, to anyhow fit the CO(3-2) emission.
However, we did not fit the CO(3-2) emission line at the positions A and B,
since we could not find a clear turnover feature or blue part of the spectrum there.
The continuum emission has been subtracted.
Note that there is a dip at the lower frequency side of the CO(3-2) emission line
at the position-B, which is due to a negative sidelobe (see also Figure \ref{figure3}).
}
\label{figure2}
\end{figure*}

\subsection{$R_{\rm HCN/HCO^+}$ and $R_{\rm HCN/CS}$}\label{sec4.1}
By inspecting the spectra, one may notice that the HCN(4-3)/HCO$^+$(4-3) integrated intensity ratio
(hereafter $R_{\rm HCN/HCO^+}$) is higher than unity only at the position-A.
To further clarify this, we list the values of $R_{\rm HCN/HCO^+}$, and the HCN(4-3)/CS(7-6) integrated intensity ratio
(hereafter $R_{\rm HCN/CS}$; \citetalias{2013PASJ...65..100I} also proposed this ratio
to be an empirical discriminator of AGN and SB) at the positions A-D in Table \ref{tbl3}.
The integrated intensity of each line emission at each position is given in Table \ref{tbl2}.
They are calculated by the Gaussian fit to the data.
The line ratios in Table \ref{tbl3} are consistent to the submm-HCN enhancement
scenario first proposed by \citetalias{2013PASJ...65..100I},
i.e., AGNs tend to show higher $R_{\rm HCN/HCO^+}$
and/or $R_{\rm HCN/CS}$ compared to SB galaxies,
although the $R_{\rm HCN/HCO^+}$ at the position-A is only slightly larger than unity and totally comparable
to the $R_{\rm HCN/HCO^+}$ of a typical early phase (e.g., \citealt{2009ApJ...694..610M})
SB galaxy NGC 253 (1.1$\pm$0.3; \citetalias{2013PASJ...65..100I}).
But the ratio is significantly higher than that of a typical late phase (e.g., \citealt{2009ApJ...694..610M})
SB galaxy, M82 ($R_{\rm HCN/HCO^+}$ $\sim$ 0.4; \citetalias{2013PASJ...65..100I}).
Note that a mechanical heating due to, e.g., frequent supernovae,
would be responsible in the central region of NGC 253 (\citealt{2014A&A...564A.126R})
for its relatively high $R_{\rm HCN/HCO^+}$, as compared to M82.

By investigating the 8.4 GHz radio flux obtained at 0.2$''$ (\citealt{2001ApJ...553L..19C}) and at 0.03$''$,
\citet{2007ApJ...671.1388D} estimated that a nuclear supernova rate is $\sim$ 0.1 yr$^{-1}$.
This rate corresponds to a star formation rate of $\sim$ 15 $M_\odot$ yr$^{-1}$
assuming the Salpeter initial mass function (\citealt{1955ApJ...121..161S}).
Our relatively large spatial resolution ($\sim$ 150 pc)
would pick up line fluxes emanating from the extended SB activity inside the CND
(see also Appendix-\ref{app-A} for the estimated size of the XDR of NGC 7469),
which would impact the line ratios discussed here.
We can not find any morphological and kinematic signatures of a jet-ISM interaction
in the high resolution maps of H$_2$ and Br$\gamma$ emissions (\citealt{2009ApJ...696..448H,2011ApJ...739...69M}),
although \citet{2003ApJ...592..804L} reported the existence of a core radio jet-like structure.
Therefore, we speculate that the energetics of the CND of NGC 7469
is influenced by both the AGN (XDR) and the SB activity (PDR)
when observed at the rather coarse resolution (150 pc in this work).

In our succeeding paper (Izumi et al. submitted),
we conducted non-local thermodynamic equilibrium (non-LTE) line modelings by the RADEX code (\citealt{2007A&A...468..627V}).
Assuming a one zone cloud, we widely changed gas kinetic temperature,
molecular column density, molecular abundance ratio, and background temperature
(we expect higher background temperature in AGNs than in SB galaxies),
but fixed H$_2$ gas density among the models ($n_{\rm H_2}$ = 10$^5$ cm$^{-3}$).
This treatment was based on the assumption that
there would be no systematic variation in $n_{\rm H_2}$ between AGNs and SB galaxies.
Then, we calculated the resultant line intensity ratio, i.e., $R_{\rm HCN/HCO^+}$ or $R_{\rm HCN/CS}$, in each model case.
As a result, we found that both $X$(HCN)/$X$(HCO$^+$) $\ga$ 10
and $X$(HCN)/$X$(CS) $\ga$ 10 are required to reproduce
$R_{\rm HCN/HCO^+}$ $>$ 1 and $R_{\rm HCN/CS}$ $>$ 10 as are observed in NGC 7469 and NGC 1097.
Furthermore, the line opacity of HCN(4-3) is moderately thick, whereas that of CS(7-6) is thin when $R_{\rm HCN/CS}$ $\ga$ 10.
Here, $X(\rm mol)$ indicates a molecular fractional abundance relative to H$_2$.
The above required abundance ratios are significantly
higher (at least by a factor of a few) than those necessary to reproduce the line ratios in SB galaxies.
Therefore, these results suggest that a chemical abundance variation
between AGNs and SB galaxies would be the key for the HCN-enhancement.

\begin{table*}
\begin{center}
\caption{Parameters of detected lines at the peak positions of the 860 $\mu$m continuum emission \label{tbl2}}
\begin{tabular}{ccccccccc}
\tableline\tableline
Emission & $\nu_{\rm rest}$ & $n_{\rm crit}$ & $E_u/k_{\rm B}$ & Peak flux & $v_{\rm LSR}$ & $\Delta v$ & $S$ & $I$ \\
 & [GHz] & [cm$^{-3}$] & [K] & [mJy beam$^{-1}$] & [km s$^{-1}$] & [km s$^{-1}$] & [Jy beam$^{-1}$ km s$^{-1}$] & [K km s$^{-1}$] \\
 (1) & (2) & (3) & (4) & (5) & (6) & (7) & (8) & (9) \\
\tableline
CS($J$=7-6) & 342.883 & 2.9$\times$10$^6$ & 65.8 & 2.20$\pm$0.58 & 4919.7$\pm$29.3& 196.5$\pm$27.2 & 0.46$\pm$0.14 & 23.7$\pm$7.1 \\
 & & & & $<$1.74$^*$ & - & - & $<$0.12$^\dag$ & $<$6.2$^\dag$ \\
 & & & & 1.87$\pm$0.58 & 5059.9$\pm$60.6 & 59.0$\pm$18.0 & 0.12$\pm$0.05$^\ddag$ & 6.0$\pm$2.6$^\ddag$ \\
 & & & & 1.98$\pm$0.58 & 4982.2$\pm$47.9 & 74.1$\pm$17.0 & 0.16$\pm$0.06$^\ddag$ & 8.0$\pm$3.0$^\ddag$ \\
CO($J$=3-2) & 345.796 & 8.4$\times$10$^3$ & 33.2 & - & - & - & - & - \\
 & & & & 202$\pm$2$^{**}$ & - & - & {\textcolor{magenta}{-}} & {\textcolor{magenta}{-}} \\
 & & & & 232$\pm$2$^{**}$ & - & - & 9.7$\pm$1.2$^{\dag}$ & 498.9$\pm$61.0$^\dag$ \\
 & & & & 235$\pm$2$^{**}$ & - & - & 12.0$\pm$0.4$^{\dag}$ & 617.5$\pm$19.2$^\dag$ \\
HCN($J$=4-3) & 354.505 & 8.5$\times$10$^6$ & 42.5 & 21.00$\pm$0.55 & 4915.8$\pm$7.8 & 199.6$\pm$6.7 & 4.46$\pm$0.19 & 225.1$\pm$9.5 \\
 & & & & 6.41$\pm$0.55 & 4935.0$\pm$17.5 & 65.5$\pm$5.9 & 0.45$\pm$0.06 & 22.6$\pm$2.8 \\
 & & & & 6.84$\pm$0.55 & 5044.2$\pm$26.5 & 41.0$\pm$5.0 & 0.30$\pm$0.04 & 15.0$\pm$2.0 \\
 & & & & 8.98$\pm$0.55 & 4981.3$\pm$16.3 & 50.1$\pm$1.5 & 0.48$\pm$0.03 & 24.2$\pm$1.7 \\
HCO$^+$($J$=4-3) & 356.734 & 1.8$\times$10$^6$ & 42.8 & 19.38$\pm$0.58 & 4914.1$\pm$5.7 & 189.7$\pm$4.8 & 3.91$\pm$0.15 & 202.8$\pm$7.9 \\
 & & & & 9.09$\pm$0.58 & 4936.6$\pm$13.0 & 60.3$\pm$3.9 & 0.58$\pm$0.05 & 30.2$\pm$2.7 \\
 & & & & 14.50$\pm$0.58 & 5045.2$\pm$8.9 & 41.5$\pm$1.9 & 0.64$\pm$0.04 & 33.2$\pm$2.0 \\
 & & & & 18.24$\pm$0.58 & 4984.4$\pm$6.1 & 50.1$\pm$1.5 & 0.97$\pm$0.04 & 50.4$\pm$2.2 \\
860 $\mu$m & 349.7 & - & - & 5.19$\pm$0.09 & - & - & - & - \\
 & & & & 1.04$\pm$0.09 & - & - & - & - \\
 & & & & 1.23$\pm$0.09 & - & - & - & - \\
 & & & & 1.70$\pm$0.09 & - & - & - & - \\
\tableline
\end{tabular}
\tablecomments{Column 1: Full line name. Column 2: Line rest frequency.
Column 3: Critical density of the line, calculated for $T_{\rm kin}$ = 100 K in the optically thin limit (\citealt{2009ApJ...692.1432G}).
Column 4: Upper level energy.
Column 5: Peak flux density of the line and continuum emission determined from the Gaussian fits to the data (Figure \ref{figure2}).
They are extracted with a single synthesized beam (150 pc resolution)
placed at the positions-A (AGN-position), B, C, and D (listed vertically in this order) marked in Figure \ref{figure1}a.
For the lines, errors were estimated from the adjacent emission-free channels except for CO(3-2).
For the continuum, an error was estimated from the emission-free areas in the continuum image.
$^*$The 3 $\sigma$ upper limit is listed.
$^{**}$The peak flux density (i.e., flux density at the turnover feature) in the channel map is listed.
Thus, these are not the results of the Gaussian fit to the data.
The primary beam attenuation is corrected.
Column 6, 7: LSR velocity and full width at half maximum (FWHM) of the line, which is calculated by the Gaussian fit.
Column 8, 9: Velocity-integrated intensity in the unit of [Jy beam$^{-1}$ km s$^{-1}$] and [K km s$^{-1}$]
at the same positions as listed in Column 5, which is estimated by combining the Columns 5 and 7.
$^\dag$The velocity centroid and the FWHM of HCN(4-3)
at the corresponding position are used for the Gaussian fits.
$^\ddag$Although the resultant integrated intensity is $<$ 3 $\sigma$, we list the value.
}
\end{center}
\end{table*}

\begin{table*}
\begin{center}
\caption{HCN(4-3)/HCO$^+$(4-3), HCN(4-3)/CS(7-6), and HCN(4-3)/CO(3-2) integrated intensity ratios in NGC 7469 \label{tbl3}}
\begin{tabular}{ccccc}
\tableline\tableline
Position  & A & B & C & D \\
\tableline
$R_{\rm HCN/HCO^+}$ & 1.11$\pm$0.06 & 0.75$\pm$0.11 & 0.45$\pm$0.07 & 0.48$\pm$0.04 \\
$R_{\rm HCN/CS}$ & 9.50$\pm$2.87 & $>$3.65 & 2.50$\pm$1.13 & 3.03$\pm$1.15 \\
$R_{\rm HCN/CO}$ & - & -$^*$ & 0.03$\pm$0.01 & 0.04$\pm$0.01 \\
\tableline
\end{tabular}
\tablecomments{Row 1: The positions marked in Figure \ref{figure1}a,
where line ratios are extracted with a single synthesized beam (150 pc-resolution).
Row 2: HCN(4-3)/HCO$^+$(4-3) integrated intensity ratio.
Row 3: HCN(4-3)/CS(7-6) integrated intensity ratio.
Row 4: HCN(4-3)/CO(3-2) integrated intensity ratio (tentative).
$^*$The peak intensity ratio at the position-B is $\sim$ 0.03.
The integrated intensities of these lines are shown in Table \ref{tbl2},
although the values of CO(3-2) are tentative.
The velocity ranges integrated over are shown in Section \ref{sec2}.
The ratios are measured in the brightness temperature scale.}
\end{center}
\end{table*}

In the following, we discuss possible mechanisms to realize the abundance variation in AGNs,
although it is still unclear, since (1) there are various ways to change the chemical compositions significantly
(e.g., {\it{X-ray irradiation, mechanical heating, high temperature chemistry}}),
and (2) the number of high resolution observational data of dense gas tracers is currently insufficient.

In conventional XDR models (\citealt{1996A&A...306L..21L,2005A&A...436..397M}),
we find reproducing a high $X$(HCN)/$X$(HCO$^+$) such as $\ga$ 10 is hard (usually it is less than unity),
since a powerful ionizing capability in XDRs will favor to enhance ionic species such as HCO$^+$.
Nonetheless, according to the steady state, gas phase 1-dimensional XDR models
intensively presented by \citet{2005A&A...436..397M} and \citet{2007A&A...461..793M},
we can expect a high $X$(HCN)/$X$(HCO$^+$) and the resultant
$R_{\rm HCN/HCO^+}$ $>$ 1 in a low-to-moderate gas density ($n_{\rm H_2}$ $\la$ 10$^5$ cm$^{-3}$) cloud
with a low hydrogen column density ($N_{\rm H}$ $\la$ 10$^{22.5}$ cm$^{-2}$)
and a high X-ray flux (e.g., $F_{\rm X}$ $\ga$ 10 erg s$^{-1}$ cm$^{-2}$).
For larger $N_{\rm H}$ where the $F_{\rm X}$ is attenuated, they predicted $R_{\rm HCN/HCO^+}$ $<$ 1.
Following this scenario, we estimate the largest distance from the AGN that can keep $F_{\rm X}$ $>$ 10 erg s$^{-1}$ cm$^{-2}$
is $r$ $\sim$ 18 pc and $\sim$ 35 pc for NGC 1097 and NGC 7469, respectively,
considering their 2-10 keV X-ray luminosities
($L_{\rm 2-10keV}$ = 6.9 $\times$ 10$^{40}$ erg s$^{-1}$ and 1.5 $\times$ 10$^{43}$ erg s$^{-1}$
for NGC 1097 and NGC 7469, respectively; \citealt{2014ApJ...783..106L}).
We here assume that the X-ray emission is isotropic around the AGN itself.
Attenuation due to obscuring material is considered for this estimation (\citealt{1983ApJ...270..119M}; Appendix-\ref{app-B}).
But one critically weak point in this scenario is that the model predicted line intensities are
extremely low (\citealt{2006ApJ...650L.103M,2007A&A...461..793M}),
which is inconsistent to the prominent HCN(4-3) and HCO$^+$(4-3) emission lines in these galaxies.
Furthermore, \citet{2015A&A...573A.116M} argued that HCN(1-0)/HCO$^+$(1-0) integrated intensity ratio
is decreased in NGC 1097 as we approach the very central region
($\sim$ 2 at the edge of the CND\footnote{An upper limit of the image convolved size is $\sim$ 90 pc $\times$ 70 pc (\citetalias{2013PASJ...65..100I})},
but $\sim$ 1.5 at the center),
which seems to be incompatible with the above speculation of the largest distance for a high line ratio in NGC 1097.
Note that, however, \citet{2015A&A...573A.116M} did not fully resolve the CND of NGC 1097,
thus, their argument is a tentative one at this moment.

Another possible scenario is the high temperature gas phase chemistry (\citealt{2010ApJ...721.1570H}),
which significantly enhances $X$(HCN) especially at $T$ $>$ 300 K
due to the activated formation path from CN (see also Figure 17 of \citetalias{2013PASJ...65..100I}).
This mechanisms would be important to make line intensity of HCN(4-3) sufficiently detectable.
Furthermore, $X$(HCO$^+$) will be somewhat decreased in these models since they will react with H$_2$O
(this is also a typical molecule in a high temperature environment) to form H$_3$O$^+$.
This type of chemistry can be complemented to XDRs (\citealt{2013ApJ...765..108H}) where we can expect
much higher gas temperature in such regions due to efficient X-ray heating than in SB environments.
Indeed, some fraction of warm molecular gas exists in NGC 7469,
as evidenced by the detections of near-IR H$_2$ (\citealt{2009ApJ...696..448H})
and high-$J$ CO emission lines (\citealt{2015ApJ...801...72R}).

With these items, we here focus on the notable fact that the $R_{\rm HCN/HCO^+}$ obtained at the position-A of NGC 7469 (1.11$\pm$0.13)
is only as half as that at the CND of NGC 1097 (2.0$\pm$0.2; \citetalias{2013PASJ...65..100I}),
despite the more than two orders of magnitude higher X-ray luminosity of NGC 7469.
Note that NGC 1097 also hosts a nuclear SB activity in the CND ($\sim$ a few $M_\odot$ yr$^{-1}$; \citealt{2007ApJ...671.1388D}),
which would contaminate the line fluxes obtained with the $\sim$ 100 pc resolution beam (\citetalias{2013PASJ...65..100I}).
Furthermore, \citet{2014A&A...567A.125G} found $R_{\rm HCN/HCO^+}$ = 1.5
at the vicinity of the AGN in NGC 1068 ($L_{\rm 2-10 keV}$ = 6.9 $\times$ 10$^{42}$ erg s$^{-1}$; \citealt{2006A&A...455..173P}),
whereas it increases to $\sim$ 3 at the East/West-knots of its CND, which are $\sim$ 100 pc away from the AGN (their spatial resolution was $\sim$ 35 pc).
These results indicate that higher X-ray luminosity does not simply lead to higher $R_{\rm HCN/HCO^+}$.
From the perspective of high temperature chemistry, the results again seem to be controversial,
since the large difference in X-ray luminosity would compensate the $\sim$ 2.5 times larger spatial scale (in area)
sampled in NGC 7469 than in NGC 1097,
leading to a higher X-ray energy deposition rate per particle
(this is an important parameter to determine the thermal structure of XDRs e.g., \citealt{1996ApJ...466..561M}) in NGC 7469,
if the molecular gas distributes uniformly over the CND.
In this case, we can expect a higher $R_{\rm HCN/HCO^+}$
in NGC 7469 than in NGC 1097 by a naive view, but the actual result is totally opposite.

Therefore, we presume that a non-radiative heating, namely mechanical heating
caused by, e.g., AGN jet or outflow, is important to realize the high
$R_{\rm HCN/HCO^+}$ of 2-3 (\citealt{2012A&A...542A..65K,2015A&A...574A.127K}) as is observed in
NGC 1097 and in the East/West knots of the CND of NGC 1068.
Indeed, a large radio jet exists in NGC 1068, which is supposed to cause shocks in the knots (e.g., \citealt{2011ApJ...736...37K}).
Furthermore, a radio core jet has been discovered in NGC 1097 (e.g., \citealt{2014ApJ...787...62M}),
although its intrinsic (deprojected) size is uncertain.
However, we can not discard the possibility such as
the line emitting region of NGC 1097 is extremely centrally-concentrated,
which would result in higher energy deposition rate per particle (i.e., more violent X-ray heating)
than in NGC 7469 and the close vicinity of NGC 1068.
Moreover, we again emphasize that the line fluxes of NGC 7469 would be
contaminated by the emission from the extended SB region inside the CND.
Higher resolution observations of these molecular emissions are necessary to
accurately map the distribution of the line ratios across the CND of NGC 1097 and NGC 7469,
and to search for a signature of shock-ISM interaction.

\subsection{Other line emissions and their ratios}\label{sec4.2}
Table \ref{tbl3} also includes HCN(4-3)/CO(3-2) integrated intensity ratios ($R_{\rm HCN/CO}$) extracted at the positions C and D.
We exclude the ratio at the positions A and B since we could not measure the accurate fluxes there.
Admitting the uncertainty in CO(3-2) integrated intensity (we used the velocity centroid and the FWHM of HCN(4-3) emission line
to fit the Gaussian profile to CO(3-2) line; see also Figure \ref{figure2} and Table \ref{tbl2}),
the tentative $R_{\rm HCN/CO}$ at the SB ring are
well below the value obtained in Ori-KL ($\sim$ 0.32; \citealt{1997ApJS..108..301S}).
Since the line critical density is orders of magnitude different between HCN(4-3) and CO(3-2) (see Table \ref{tbl2}),
we can expect the line emitting region of HCN(4-3) is much smaller than that of CO(3-2).
Hence, this ratio would be highly prone to be affected by the spatial resolution,
which could lead to significantly lower $R_{\rm HCN/CO}$ in NGC 7469 than in Ori-KL.
This is well manifested in the case of NGC 253 (SB galaxy).
When observed at $\sim$ 200-300 pc resolution (comparable to our 150 pc resolution for NGC 7469),
$R_{\rm HCN/CO}$ $\sim$ 0.03 (\citealt{2007ApJ...666..156K,1995A&A...302..343I}), which is quite similar to our result.
However, the ratio increase to $\sim$ 0.08, i.e., increase by a factor of a few, when observed at higher resolution (25-30 pc; \citealt{2011ApJ...735...19S}).
Then, matching the spatial resolution is important to compare line ratios of emission lines with totally different critical densities among objects.

We also found that the H${}^{12}$CN(4-3)/H${}^{13}$CN(4-3) isotopic ratio
at the position-A was $\ga$ 11.9 in the brightness temperature scale.
Note this is a peak intensity ratio and we used a 3 $\sigma$ upper limit for H${}^{13}$CN(4-3).
Then, adopting a ${}^{12}$C/${}^{13}$C ratio of $>$ 40 observed in
NGC 253 (\citealt{2014A&A...565A...3H}; \citealt{2010A&A...522A..62M}, $\sim$ 340 pc resolution),
the upper limit to the opacity of the H$^{12}$CN(4-3) is 3.5 at the position.
For this calculation, we assume (1) the gas is in the LTE, (2) H$^{12}$CN is optically thick,
(3) H$^{13}$CN is optically thin, and (4) H$^{12}$CN and H$^{13}$CN emissions are coming from the same volume of gas.
Alternatively, if we adopt a ${}^{12}$C/${}^{13}$C ratio of 100 obtained in
Mrk 231 (\citealt{2014A&A...565A...3H}, $\sim$ 19 kpc resolution), the upper limit of the opacity increases to 8.8.
In either case, the derived optical depth is rather smaller than the values of the Galactic star forming regions
(e.g., $\sim$ 70 in Ori-KL; \citealt{1997ApJS..108..301S}),
likely reflecting the much more turbulent environments in the nuclear regions of galaxies.

Note that vibrationally excited HCN emission, namely HCN($v_2$=1$^{1f}$, $J$=4-3)
at $\nu_{\rm rest}$ = 356.256 GHz, was not detected at the position-A,
despite the fact that NGC 7469 is classified as a LIRG (\citealt{2003AJ....126.1607S}) hosting a luminous AGN.
Considering the above mentioned modest optical depth of H$^{12}$CN(4-3),
we can expect HCN($v_2$=1$^{1f}$, $J$=4-3) is completely optically thin,
which makes itself hard to be detectable.
Therefore, the non-detection of HCN($v_2$=1$^{1f}$, $J$=4-3) emission does not necessarily mean
that IR-pumping has little contribution to the observed line intensities,
although we here simply treat that the HCN(4-3) emission
is the consequence of the purely rotational transition.
We need quantitative modeling of the line excitation to further address this problem.
We also note that the contribution of HC$_3$N(39-38) emission to the HCN(4-3) emission is negligible at the position-A
since HC$_3$N emission is typically much fainter than that of HCN,
and the line profile of the bluer HCN(4-3) is very similar to that of HCO$^+$(4-3), which does not suffer from line blending.
We thus conclude that the contribution of HC$_3$N(38-37) to the CO(3-2) emission is also negligible.

\subsection{Dense molecular gas mass}\label{sec4.3}
In addition to $R_{\rm HCN/HCO^+}$ and $R_{\rm HCN/CS}$,
we list line luminosities of HCN(4-3) and HCO$^+$(4-3)
extracted at the position-A and the whole CND (i.e., central 1$''$ diameter region)
in Table \ref{tbl4} as well since these lines are relatively strong enough to be detectable
even in high redshift galaxies (e.g., \citealt{1997ApJ...484..695B,2011ApJ...726...50R}).
By using this data, we roughly estimate the mass of dense molecular gas ($M_{\rm dense}$) in the CND as follows.
First, we convert $L'_{\rm HCN(4-3)}$ to the corresponding value of HCN(1-0),
assuming HCN(4-3)/HCN(1-0) = 0.6$\pm$0.2 in the brightness temperature unit.
This ratio is an averaged value over the CND of the nearby typical Seyfert-2 galaxy, NGC 1068,
sampled at 100 pc resolution (\citealt{2014A&A...570A..28V}).
Note that NGC 1068 has a quite similar X-ray luminosity and an Eddington ratio to NGC 7469.
Then, we obtain $L'_{\rm HCN(1-0)}$ = (9.3$\pm$3.1) $\times$ 10$^6$ K km s$^{-1}$ pc$^2$.
Finally, assuming a conversion factor from $L'_{\rm HCN(1-0)}$ to $M_{\rm dense}$
to be 10, which is derived for AGNs by \citet{2008ApJ...677..262K} based on IRAM 30m observations,
we estimate $M_{\rm dense}$ = (9.3$\pm$3.1) $\times$ 10$^7$ $M_\odot$.
The dynamical mass ($M_{\rm dyn}$) of the CND, on the other hand, is calculated
assuming a thin disk with Keplerian rotation as,
$M_{\rm dyn}$ = 230 ($r$/pc) [$v(r)^2$/(km s$^{-1}$)] (sin $i$)$^{-2}$ $M_\odot$.
Here, $v(r)$ is a rotation velocity at a radius $r$, and $i$ is an inclination angle of the disk.
Then, putting the FWHM $\sim$ 200 km s$^{-1}$ at the CND (1$''$ = 330 pc diameter)
and $i$ = 45$^\circ$ (\citealt{2004ApJ...602..148D}),
we obtain $M_{\rm dyn}$ = 7.6 $\times$ 10$^8$ $M_\odot$.
This is almost identical to the value derived in \citet{2015ApJ...806L..34F},
who isolated the rotation velocity and the velocity dispersion
based on their harmonic decomposition analysis of the observed velocity field.
Our $M_{\rm dyn}$ is also consistent to those derived for $r$ $<$ 2.5$''$ region,
i.e., including the SB ring (6.5 $\times$ 10$^9$ $M_\odot$; \citealt{2004ApJ...602..148D}).

Taking them together, we can estimate the dense gas mass fraction in the CND of NGC 7469
as $f_{\rm gas}$ $\equiv$ $M_{\rm dense}/M_{\rm dyn}$ $\sim$ 12\%.
Recalling the fact that the above used mass conversion factor
has {\it{a factor of $\sim$ 3 uncertainty}} (\citealt{2008ApJ...677..262K}),
$f_{\rm gas}$ eventually has the same level of uncertainty at this moment.
Therefore, although the value of $f_{\rm gas}$ $\sim$ 12\%
is comparable to those estimated for {\it{low-luminosity}} AGNs (\citealt{2012MNRAS.424.1963S}) using the same conversion factor (i.e., 10),
it is still difficult to speculate whether or not $f_{\rm gas}$ has any relevance with the current mass accretion
onto the central supermassive black hole.
We need an accurate mass conversion factor estimated through multi-transitional analysis
(i.e., estimating an accurate relative abundance of HCN with respect to H$_2$) to further
constrain the $f_{\rm gas}$ and its relevance to the nuclear activity.

\begin{table*}
\begin{center}
\caption{HCN(4-3) and HCO$^+$(4-3) line luminosities both in [$L_\odot$] unit and [K km s$^{-1}$ pc$^2$] unit \label{tbl4}}
\begin{tabular}{ccccc}
\tableline\tableline
 & $L_{\rm HCN(4-3)}$ & $L_{\rm HCO^+(4-3)}$ & $L'_{\rm HCN(4-3)}$ & $L'_{\rm HCO^+(4-3)}$ \\
 & [$L_\odot$] & [$L_\odot$] & [K km s$^{-1}$ pc$^2$] & [K km s$^{-1}$ pc$^2$] \\
\tableline
  AGN position & (7.95$\pm$0.34) $\times$ 10$^3$ & (7.01$\pm$0.27) $\times$ 10$^3$ & (5.58$\pm$0.24) $\times$ 10$^6$ & (4.83$\pm$0.19) $\times$ 10$^6$ \\
  CND & (2.10$\pm$0.09) $\times$ 10$^4$ & (1.86$\pm$0.08) $\times$ 10$^4$ & (1.47$\pm$0.06) $\times$ 10$^7$ & (1.28$\pm$0.06) $\times$ 10$^7$ \\
\tableline
\end{tabular}
\tablecomments{Row 1: Line luminosities within a synthesized beam (150 pc-resolution) placed at the position-A (i.e., AGN position) marked in Figure \ref{figure1}a.
The luminosity was calculated following the formulae by \citet{2005ARA&A..43..677S}.
Row 2: Line luminosities within the CND (i.e., the central $\sim$ 1$''$ = 330 pc diameter region).}
\end{center}
\end{table*}

\section{Spatial distribution of the dense gas tracers}\label{sec5}
We show in Figures \ref{figure3} to \ref{figure5} the channel maps of the CO(3-2), HCN(4-3), and HCO$^+$(4-3) line emissions
from the central 8$''$ $\times$ 8$''$ (2.6 kpc $\times$ 2.6 kpc) region of NGC 7469.
We could not cover the whole CO(3-2) emission line as noted before.
Comparing with CO(2-1) map in \citet{2004ApJ...602..148D},
we conclude that the emission from the south-west region of the map is missing.
The HCN(4-3) and HCO$^+$(4-3) emissions were detected (i.e., $>$ 3 $\sigma$) over velocity ranges of
4744-5165 km s$^{-1}$ and 4752-5150 km s$^{-1}$ at the position-A, respectively,
of which widths (FWZI $\sim$ 400 km s$^{-1}$) are almost consistent with each other.
As for CO(3-2), the covered velocity range corresponds to $\sim$ 70\%
of the total velocity range of HCN(4-3) and HCO$^+$(4-3) at the position-A.
However, we can not see a clear turnover feature in the CO(3-2) spectrum at that position (Figure \ref{figure2}).
Therefore, we conclude that the FWZI of CO(3-2) emission line is significantly wider than those of HCN(4-3) and HCO$^+$(4-3) lines there.
It might be possible that we detected CO(3-2) emission from an outer diffuse, high-velocity component around the CND.
It might also be possible that the high velocity component of HCN(4-3) and HCO$^+$(4-3) emission lines
are too faint to be significantly detectable.
On the other hand, the line widths at the knots of the SB ring are almost consistent
among CO(3-2), HCN(4-3), HCO$^+(4-3)$ emission lines (Figure \ref{figure2}).
The channel maps also show that the CND and the SB ring are bridged by a bar-like,
or several spiral arm-like structures as morphologically discussed later.
A detailed kinematic study of this region is presented in \citet{2015ApJ...806L..34F}.

\begin{figure*}
\epsscale{1}
\plotone{f3.eps}
\caption{Velocity channel maps of the CO(3-2) line emission in the central 8$''$ $\times$ 8$''$ (2.6 kpc $\times$ 2.6 kpc) region of NGC 7469.
The central red cross in each channel indicates the position-A in Figure \ref{figure1}a (i.e., the AGN position).
The velocity width of each channel is $\sim$ 20 km s$^{-1}$, and the central velocity of each channel is shown in the upper left corner.
The synthesized beam (0.50$''$ $\times$ 0.40$''$, PA = 68.5$^\circ$) is also plotted in the bottom left corner.
Contour levels are -5, 3, 5, 10, 30, 50, 70, 90, and 110 $\sigma$, where 1 $\sigma$ = 2.34 mJy beam$^{-1}$.
The negative contour is indicated by the dashed lines.
Note that we could not observe channels with $V_{\rm LSR}$ $<$ 4900 km s$^{-1}$ due to our observational setup.
Attenuation due to the primary beam pattern is corrected.
}
\label{figure3}
\end{figure*}

\begin{figure*}
\epsscale{1}
\plotone{f4.eps}
\caption{Velocity channel maps of the HCN(4-3) line emission in the central 8$''$ $\times$ 8$''$ (2.6 kpc $\times$ 2.6 kpc) region of NGC 7469.
The central red cross in each channel indicates the position-A in Figure \ref{figure1}a (i.e., the AGN position).
The velocity width of each channel is $\sim$ 20 km s$^{-1}$, and the central velocity of each channel is shown in the upper left corner.
The synthesized beam (0.49$''$ $\times$ 0.39$''$, PA = 70.4$^\circ$) is also plotted in the bottom left corner.
Contour levels are -5, 3, 5, 10, 20, and 30 $\sigma$, where 1 $\sigma$ = 0.55 mJy beam$^{-1}$.
Although we set the negative contours to be indicated by the dashed lines, they are not prominent in this figure.
Attenuation due to the primary beam pattern is corrected. }
\label{figure4}
\end{figure*}

\begin{figure*}
\epsscale{1}
\plotone{f5.eps}
\caption{Velocity channel maps of the HCO$^+$(4-3) line emission in the central 8$''$ $\times$ 8$''$ (2.6 kpc $\times$ 2.6 kpc) region of NGC 7469.
The central red cross in each channel indicates the position-A in Figure \ref{figure1}a (i.e., the AGN position).
The velocity width of each channel is $\sim$ 20 km s$^{-1}$, and the central velocity of each channel is shown in the upper left corner.
The synthesized beam (0.48$''$ $\times$ 0.38$''$, PA = 57.9$^\circ$) is also plotted in the bottom left corner.
Contour levels are -5, 3, 5, 10, 20, and 30 $\sigma$, where 1 $\sigma$ = 0.58 mJy beam$^{-1}$.
Although we set the negative contours to be indicated by the dashed lines, they are not prominent in this figure.
Attenuation due to the primary beam pattern is corrected. }
\label{figure5}
\end{figure*}

We also show the maps of the CO(3-2), HCN(4-3), HCO$^+$(4-3), and CS(7-6) velocity-integrated intensities
in the central 2 kpc region of NGC 7469 in Figure \ref{figure6}.
The peak positions of the 860 $\mu$m continuum emission (the positions A-D in Figure \ref{figure1}a)
are again marked by the arrows in the CO(3-2) map.
The dense gas tracers are also bright at these peak positions,
indicating they are the sites of dust-obscured star formation.
Two rather fainter knots are also seen in the CO(3-2) map, which are located northwest to the CND (marked as E and F).

From these maps, it is apparent that the HCN(4-3), HCO$^+$(4-3), and CS(7-6) emissions are
significantly concentrated towards the CND.
A two-dimensional Gaussian fit to the HCN(4-3) image shows that the CND has an extent of
(244.2$\pm$9.9) $\times$ (194.7$\pm$6.6) pc$^2$ with PA = 58.8$^\circ$$\pm$6.7$^\circ$,
which is similar to that of HCO$^+$(4-3) emission.
This is the beam-convolved size, thus the actual CND must be smaller.
We derived these uncertainties using Monte Carlo techniques by creating 10$^3$ realizations of the image,
each time adjusting the data by adding the normally-distributed (measured) noise randomly.
Again using Figure \ref{figure6}, we estimate that the CND of NGC 7469 contains $\sim$ 82 \% and 53 \%
of the total emission of HCN(4-3) and HCO$^+$(4-3) within the 18$''$ field of view of ALMA ($\sim$ 6 kpc), respectively,
suggesting their utility to probe the nuclear regions of external galaxies especially about HCN(4-3).

Here, we expect that the missing flux is not significant for the CND,
although we recovered only 54$\pm$16 \% of the HCO$^+$(4-3) flux
measured by APEX (\citealt{2014ApJ...784L..31Z}) within the central 18$''$ region,
since its size ($\sim$ 1$''$) is much smaller than that of the maximum measurable
angular scale of our observations, which was 7.1$''$ (2.3 kpc).
Since the APEX's HCO$^+$(4-3) spectrum of
\citet{2014ApJ...784L..31Z} is somewhat noisy, we can expect
the systematic flux uncertainty would be larger
than the value mentioned in that paper (15\% for absolute flux calibration uncertainty)
additionally due to, e.g., baseline uncertainty.
In other words, we expect the actual recovered rate can be higher than 54\%.
Unfortunately, we can not estimate the percentage
of the recovered flux of HCN(4-3) and CS(7-6) since there are currently
no significant detection of these line emissions with single dish telescopes.

In addition to the CND, we can see a partial circumnuclear SB ring at a radius of 1.5$''$--2.5$''$.
\citet{2004ApJ...602..148D} also reported the existence of a bar or a pair of short,
loosely wound spiral arms at a PA = 56$^\circ$ between the CND and the SB ring
(connecting the positions B-A-D in Figure \ref{figure6}a),
based on their 0.7$''$ CO(2-1) observations.
Interestingly, that structure is only found in molecular emission;
neither K-band (\citealt{1995ApJ...444..129G}; \citealt{2000AJ....119..991S})
nor centimeter continuum (\citealt{1991ApJ...378...65C}; \citealt{2010MNRAS.401.2599O}) image shows such a structure.
This configuration is quite unusual if the structure is a genuine molecular bar,
since a corresponding stellar structure should be easily visible in this scenario.
Indeed, \citet{2004ApJ...602..148D} found no kinematic characteristics expected for a barred potential,
i.e., an S-shaped contours in a isovelocity field (e.g., \citealt{2004A&A...422..865L,1999ApJ...511..157K})
and a tilted-X shape in a position-velocity diagram along the
(hypothesized) bar axis (e.g., \citealt{1999ApJ...511..709L,2000ApJ...533..149S}).
Moreover, Figures \ref{figure4} and \ref{figure5} reveal that there seem to be several connections
between the CND and the SB ring in addition to the above hypothesized bar axis,
e.g., channels at around 4850, 4980, and 5020 km s$^{-1}$.
Although we can not rule out the existence of a faint stellar bar that could not be detected in previous NIR observations,
it might be possible that the nuclear region of NGC 7469 consists of several spiral features
like the case of, e.g., NGC 1097 (\citealt{2005AJ....130.1472P, 2006ApJ...641L..25F, 2009ApJ...702..114D}).
Since the lack of spatial resolution leads to blending several molecular clouds, which would result in an illusional bar,
higher angular resolution and sensitivity observations of both CO and NIR emissions are necessary to settle this issue.

\begin{figure*}
\epsscale{1}
\plotone{f6.eps}
\caption{Integrated intensity maps of (a) CO(3-2), (b) HCN(4-3), (c) HCO$^+$(4-3), and (d) CS(7-6),
in the central $\sim$ 2 kpc region of NGC 7469.
The rms noises (1 $\sigma$) are 0.20, 0.06, 0.06, and 0.06 Jy beam$^{-1}$ km s$^{-1}$ in (a), (b), (c), and (d), respectively.
Note that we could not observe CO(3-2) emission at $V_{\rm LSR}$ $<$ 4900 km s$^{-1}$
due to our observational setting, thus the displayed map is incomplete (south-east part is deficient).
Some bright molecular knots are marked as A-F in the CO(3-2) map (the positions A-D are the same as the ones marked in Figure \ref{figure1}a).
The white filled ellipses indicate the synthesized beams ($\sim$ 0.50$''$ $\times$ 0.40$''$).
The central crosses indicate the AGN position.
Contours are: (a) -5, 3, 5, 10, 20, 30, ..., and 130 $\sigma$, (b) -5, 3, 5, 10, 20, 30, ..., and 70 $\sigma$, (c) -5, 3, 5, 10, 20, 30, 40, and 50 $\sigma$, (d) -5, 3, and 5 $\sigma$, respectively.
Negative contours are indicated by dashed lines.
See also Section \ref{sec2} for the velocity ranges integrated over.
}
\label{figure6}
\end{figure*}

\section{Summary and conclusion}\label{sec6}
In this paper, we present high resolution (0.5$''$ $\times$ 0.4$''$; 1$''$ = 330 pc) ALMA band 7 (350 GHz band)
observations of the submillimeter dense molecular gas tracers such as HCN(4-3), HCO$^+$(4-3),
CS(7-6), and partially CO(3-2), in addition to the underlying 860 $\mu$m continuum emission,
towards the central kpc region of the luminous type-1 Seyfert galaxy, NGC 7469.
The region consists of the CND (central $\sim$ 1$''$)
and the surrounding SB ring with a radius of 1.5$''$-2.5$''$.
We revealed the spatial distribution of these emissions.
Thanks to the high spatial resolution, we can reliably measure the line fluxes at the CND and the SB ring separately.
The obtained line ratios are directly compared with those in NGC 1097 (a low-luminosity type-1 Seyfert galaxy),
to achieve insights of possible effects of AGN luminosity on the surrounding molecular material.
The main results of our observations and conclusions are summarized as follows:

\begin{itemize}
\item[-] The spatial distribution of the 860 $\mu$m continuum emission
resembles well to those of centimeter and MIR continuum emissions, and dense molecular gas tracers.
But their peak positions (including some knots in the SB ring)
are shifted significantly from the optical ones,
suggesting the existence of dust obscured star formation there.
\item[-] The maximum position of the 860 $\mu$m continuum is identical to that of the VLA 8.4 GHz continuum, indicating it is the AGN position.
The SED reveals that the 860 $\mu$m continuum there is dominated by a thermal dust emission.
We detected CO(3-2), HCN(4-3), HCO$^+$(4-3), and CS(7-6) emissions at the same position.
Other lines including the vibrationally excited HCN were not detected, although NGC 7469 is classified as a LIRG.
\item[-]  The high $R_{\rm HCN/HCO^+}$ and $R_{\rm HCN/CS}$ are only found in the CND,
which is consistent to the findings in \citetalias{2013PASJ...65..100I},
i.e., AGNs tend to show higher $R_{\rm HCN/HCO^+}$ ($\ga$ 1)
and/or $R_{\rm HCN/CS}$ ($\ga$ 10) than those in SB galaxies (submm-HCN enhancement).
\item[-] Although the actual physical mechanisms to enhance $R_{\rm HCN/HCO^+}$ in AGNs are still unclear,
we found this ratio is significantly lower in NGC 7469 (1.11$\pm$0.06) than
in NGC 1097 (2.0$\pm$0.2) despite the more than two orders of magnitude
higher X-ray luminosity of NGC 7469 than that of NGC 1097.
The close vicinity of the luminous AGN of NGC 1068 also shows a comparable ratio ($\sim$ 1.5) to NGC 7469.
Some other heating mechanisms than X-ray (e.g., mechanical heating) would
contribute significantly for shaping the chemical composition in NGC 1097.
\item[-] The CO(3-2) emission, which is not fully observed though, is distributed over both the CND and the SB ring,
whereas the HCN(4-3) and the HCO$^+$(4-3) emissions are significantly concentrated toward the CND
($\sim$ 82\% and 53\% of the total flux inside the 18$''$ field of view of ALMA, for HCN and HCO$^+$, respectively),
suggesting their utility to probe the nuclear regions of galaxies.
\item[-] Between the CND and the SB ring, we found several spiral-like structures,
which would be transporting gas from the SB ring to the CND.
This might be a more preferable scenario than a bar.
We should test this tentative view by further high resolution observations and kinematic analysis.
\end{itemize}

From this work, we achieved supportive evidence for the submm-HCN enhancement
in AGNs tentatively proposed by \citetalias{2013PASJ...65..100I}.
We will further investigate this trend by increasing the number of sample galaxies,
and extensively discuss the possible cause of the HCN-enhancement
in our succeeding paper (Izumi et al. submitted).

\acknowledgments
We thank the anonymous referee for very kind and helpful comments for improving the paper.
This paper makes use of the following ALMA data: ADS/JAO.ALMA\#2012.1.00165.S.
ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan),
together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile.
The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ.
The National Radio Astronomy Observatory is a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities, Inc.
We used data based on observations with the NASA/ESA Hubble Space Telescope,
and obtained from the Hubble Legacy Archive,
which is a collaboration between the Space Telescope Science Institute (STScI/NASA),
the Space Telescope European Coordinating Facility (ST-ECF/ESA)
and the Canadian Astronomy Data Centre (CADC/NRC/CSA).
In addition, this research has made use of the NASA/IPAC Extragalactic Database (NED)
which is operated by the Jet Propulsion Laboratory, California Institute of Technology,
under contract with the National Aeronautics and Space Administration.
T. I. was supported by the ALMA Japan Research Grant of NAOJ Chile Observatory, NAOJ-ALMA-0029.
T. I. and H. U. are thankful for the fellowship received from the Japan Society for the Promotion of Science (JSPS).

redpajama_set_name: RedPajamaArXiv


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Die Basilika St. Jakob ist eine gotische Hallenkirche und die größte Hauptkirche der Stadt Straubing.
1581 wurde das Chorherrenstift Pfaffenmünster im Zuge der Gegenreformation nach St. Jakob übertragen. Seither hat die ehemalige Stiftskirche den heiligen Tiburtius als zweiten Kirchenpatron.

Die Kirche wurde um 1400 nach den Plänen des Baumeisters Hans von Burghausen errichtet. Das dreischiffige Langhaus, umgeben mit einem Kranz aus 20 Seitenkapellen wurde um 1512 vollendet. Besonders auffällig ist der erst Ende des 16. Jahrhunderts fertiggestellte Turm mit seiner schlanken und spitzen Zwiebelhaube.
Mit 89,50 Metern Höhe ist er der höchste Kirchturm im Gäuboden und eines der Wahrzeichen Straubings. Am 23. Juli 1989 erhob Papst Johannes Paul II. die Stiftskirche mit dem Apostolischen Schreiben Sancti profecto zur Basilica minor.
Im Juli 2016 konnten nach 18 Jahren die Generalsanierungarbeiten abgeschlossen werden.

Ausstattung

Hochaltar
Der Hochaltar der Stiftskirche ist aus dem Jahr 1486 und stammt aus dem Kloster St. Veit in Nürnberg. Im Schrein des Altars sind die Figuren Maria mit Kind, die Kirchenpatrone Jakobus und Tiburtius, sowie Maria Magdalena und der heilige Leonhard dargestellt. Der jetzige Altar ist ein neugotischer Altar, der den oben beschriebenen Schrein von 1486 beinhaltet. Er besitzt zwei Flügelpaare mit acht Gemälden. Im geöffneten Zustand (Feiertagsseite) sind die "Auferstehung des Herrn" und die "Krönung Mariens" zu sehen. Bei einfach geschlossenen Flügeln (Werktagsseite) zeigen sich Gemälde mit den Motiven "Darstellung des Kindes im Tempel", "Anbetung der Könige", "Christi Himmelfahrt" und die "Geistsendung". Diese sechs Gemälde werden der Werkstatt Michael Wolgemuts, des Lehrmeisters Dürers, zugeschrieben. Schließt man die Flügel zweifach (Fastenzeit), präsentieren sich zwei Bilder von 1895: "Jesus begegnet den weinenden Frauen" und "Beweinung Christi". Die Rückseite des Schreins ziert ein dreiteiliges Gemälde von 1895: "Verklärung auf dem Berg Tabor".

Kanzel

Das prachtvollste Ausstattungsstück aus der Rokokozeit ist die großartige Kanzel. Geschaffen wurde sie 1752 vom kurfürstlichen Bildhauer Wenzel Myrowsky, der sie aber nicht vollendet hat. Der Straubinger Schreinermeister Johann Heinrich Klembt wurde mit der Herstellung der Stiege beauftragt. Das Rokoko-Gewand hat der Straubinger Stuckateur Mathias Obermayr geschaffen. Unter dem überreichen Schmuck sind besonders hervorzuheben die Figuren des Heiligen Jakob, der mit einem Puto (mit Palme und Blütenkranz) die Kanzel beherrscht, die sieben Engel mit ihren Attributen (Anker, Kerze, Evangelienbuch, Gesetzestafeln und Kreuz, Getreideähren und Weintraube, Schwert und Palmwedel) und die Reliefs am Korb (vier Evangelisten, heiliger Florian) und Stiege (Martertod der heiligen Sebastian und Laurentius, Unsere Liebe Frau von Altötting). Zu betreten ist die mächtige Kanzelanlage durch eine prächtig ausgeführte Pforte, die eine Büste des heiligen Johannes Nepomuk und je ein Engel mit Kreuz und mit Vorhängeschloss, dem Zeichen der Verschwiegenheit, schmücken. An der Türe sind zwei weitere Reliefs angebracht (Beichte der Königin Johanna beim heiligen Johannes Nepomuk und dessen Martyrium).

Sakramentshäuschen
Etwas nordöstlich vom Hochaltar an einer Vorlage wächst das Sakramentshäuschen aus den Boden bis in die lichte Höhe des Gewölbes. Es stammt in der Substanz aus dem Ende des 15. Jahrhunderts, Fuß, Skulpturen und Tabernakelschrein werden um 1900 erneuert. Einmal im Jahr, vom Gründonnerstag bis zum Ostersonntag, ist es in Gebrauch, wenn nach einer feierlichen Prozession durch die Basilika das Allerheiligste dort deponiert und während einer Gebetsnacht angebetet wird.

Kreuzaltar
Nicht erst seit der Liturgiereform im Rahmen des zweiten Vatikanischen Konzils, sondern seit dem Ende des 15. Jahrhunderts dient die Altarmensa zwischen dem vierten Säulenpaar von Osten her als Zelebrationsaltar. Ursprünglich stand auf ihm eine – 1783 vom Straubinger Bildhauer Franz Xaver Keller (1752–1827) geschaffene – Kreuzigungsgruppe.

Hochfenster

Den größten kunsthistorischen Wert dürften die Glasgemälde besitzen. Denn neben dem Regensburger Dom und der Basilika St. Martin in Amberg weist St. Jakob den umfassendsten Bestand mittelalterlicher und neugotischer Fenster auf. In vier Hochfenstern präsentieren sich Glasmalereien aus dem Ende des 15. Jahrhunderts. Eines sei besonders hervorgehoben. Im Hochfenster über der Josefskapelle ist die Übergabe der Gesetzestafeln an Moses durch Gott in solch frischen und kräftigen Farben dargestellt, dass eine Datierung um 1490 überrascht. Den Entwurf schrieb man Wilhelm Pleydenwurff (1450–1494), einem Schüler Michael Wolgemuts, zu. Neuen Erkenntnissen zufolge stammt der Entwurf für das sogenannte Mosesfenster jedoch von Albrecht Dürer. Angefertigt wurde es in der Werkstatt von Veit Hirschvogel. Die anderen verbleibenden Kirchenfenster wurden im Rahmen der Restaurierung von 1895 bis 1908 mit Glasgemälden der Firmen Zettler und Ostermann und Hartwein versehen.

Orgelanlage
St. Jakob hat eine lange Orgeltradition. Bereits vor 1433 war eine Orgel nachweisbar. 1524 erbaute Thomas Altenburger aus Regensburg ein Instrument, welches 1691 durch ein neues Werk eines nicht überlieferten Orgelbauers abgelöst wurde. Diesem folgte ein Neubau um 1785 von Johann Peter Plersch. Der Umfang und die Disposition der Instrumente sind nicht überliefert.

1898 baute Borgias Maerz als sein Opus 357 eine neue Orgel. Sie verfügte über drei Manuale und 37 Register. Die Pfeifen standen auf pneumatischen Kegelladen, ein damals modernes System, was zudem die Einrichtung eines freistehenden Spieltisches, ausgestattet mit zahlreichen Spielhilfen ermöglichte. Das Instrument wurde jeweils durch Michael Weise 1934 umgebaut und 1947 erweitert.

In den Jahren 1964 bzw. 1967 wurde das Werk durch Orgelbaumeister Friedrich Meier abgetragen und aus akustischen Gründen durch eine Orgelanlage, bestehend aus der Hauptorgel mit 60 Registern (4366 Pfeifen) und der Chororgel mit 17 Registern (1482 Pfeifen) ersetzt. Letztere konnte von einem eigenen Spieltisch im Chorraum der Kirche aus gespielt werden oder auch über das fünfte Manual des auf der Empore stehenden Hauptspieltisches. Außerdem konnte sie (auf einem oder zwei anderen Manualen und Pedal gespielt) zusammen mit der Hauptorgel erklingen. Umgekehrt war es möglich, 30 Register der Hauptorgel vom Spieltisch der Chororgel aus zu benutzen. Insgesamt hatten die beiden Orgeln der Basilika 5848 Pfeifen, die sich auf insgesamt 77 Registern verteilten.

Zwanzig Jahre lang bemühte sich der Orgelbauförderverein St. Jakob Straubing, die Pfarrei St. Jakob bei der Finanzierung einer neuen Orgelanlage zu unterstützen. Schließlich konnte die alte Hauptorgel 2018 abgebaut und Platz für die Errichtung eines neuen Orgelwerkes durch die Fa. Eule geschaffen werden. Die neue Orgelanlage wurde am 19. Juli 2020 in einem Festgottesdienst von Pfarrer Johannes Hofmann geweiht. Sie verfügt über einen mechanischen Spieltisch an der Hauptorgel und einen elektrischen im Chorraum sowie über insgesamt 92 Register, zuzüglich sechs Extensionen und fünf Transmissionen, mit insgesamt 6613 Pfeifen. Für eine leichte Spielbarkeit sind Barkerhebel eingebaut. Die Gesamtanlage bildet somit die drittgrößte Orgel der Diözese Regensburg. Drei Gebläse liefern zusammen bis zu 85 m³ Wind pro Minute. Neu eingerichtet wurde auch ein Fernwerk auf dem Dachboden der Kirche. Die Klänge dieses schwellbaren Teilwerks werden über das Heiliggeistloch in das Innere des Kirchenraumes geleitet. Neben dem historischen Gehäuse finden noch erhaltene Pfeifen der Maerz-Orgel von 1898 in acht Registern der neuen Hauptorgel Verwendung. Die Chororgel ist gänzlich neu.

Hauptorgel
Die Hauptorgel hat 77 Register (zusätzlich 7 Transmissionen und Extensionen), verteilt auf vier Manualwerke und Pedal. Die Register des Solowerks und des Fernwerkes können an alle Manuale und das Pedal gekoppelt werden. Die Disposition lautet wie folgt:

 Anmerkung
 (M) = Register von Maerz

Chororgel
Das Instrument hat 15 Register, zusätzlich 2 Transmissionen und 2 extendierte Register auf zwei Manualwerken und Pedal. Die Disposition lautet:

 Koppeln:
 Normalkoppeln: II/I, III/I, III/II, IV/I, IV/II, IV/III, I/P, II/P, III/P, IV/P
 Superoktavkoppeln: III/I, III/III, IV/I, IV/IV, III/P, ChorSW/ChorSW, Solo/Solo, FW/FW;
 Suboktavkoppeln: III/I, III/III, IV/I, IV/III, IV/IV, ChorSW/ChorSW, FW/FW
 Zuschalter: Chororgel/HW, Chororgel/SW, Solowerk und Fernwerk an I, II, III, IV, P
 Spielhilfen: 4 Schwelltritte: III, IV, Chororgel, FernWerk/Clar. mit Koppler; Walze (mit 4 Programmen); Setzeranlage; Zuschalter Tuba sonora für alle Klaviaturen, im P zusätzlich als 4′; Zuschalter für Celesta zu Man. II+III

Glocken
St. Jakob besitzt mit 10 Glocken das größte Geläut im Bistum Regensburg. Die Glocken 2, 4, 5, 7, 8, 9 und 10 wurden im Jahre 1948 von Friedrich Wilhelm Schilling in Apolda gegossen. Die Glocken 1, 3 und 6 (in original Schilling'scher Rippe gefertigt) kamen im Jahre 2001 hinzu. Bei dieser Maßnahme musste der obere der beiden Glockenstühle, bislang aus Eisen, durch einen doppelstöckigen aus Eichenholz ersetzt werden. Der untere, schon 200 Jahre alt, aus Holz und in gutem Zustand, wurde restauriert. Seit diesem Umbau hängen (wie bisher) im fünften Turmgeschoss drei Glocken und – jetzt neu – im sechsten Turmgeschoss sieben Glocken. Die sehr ungewöhnliche Tonfolge – mit einer Ausnahme ausschließlich Ganz- und Halbtonschritte – bietet eine reichhaltige Auswahl an Teilmotiven.

Läuteordnung

 Hauptgottesdienst an Weihnachten/OsternPfingsten/ Tedeum an Fronleichnam, Patrozinium Hl. Jakobus/ Jahreswechsel: 10 – 9 - 8 - 7 - 6 - 5 - 4 - 3 - 2 - 1.
 Messen an Weihnachten, Ostern und Pfingsten: 10 - 9 - 8 - 6 - 5 - 4 - 2  - 1
 Besondere Anlässe: 6 - 5 - 4 - 3 -2 - 1
 Jahresschluss, Hl. Tiburtius (Zweiter Kirchenpatron): 5 - 4 - 3 - 2 - 1
 Gründonnerstag: 5 - 3 - 2 - 1
 Kreuzweg: 7 - 6 - 5
 Kreuzweg durch die Stadt: 3 - 2
 Hauptgottesdienst an Dreikönig, Palmsonntag, Dreifaltigkeitssonntag, Mariä Himmelfahrt, Christkönig/ Sonntage in der Weihnachts- und Osterzeit: 10 - 9 - 8 - 6 - 5 - 4 - 2
 Messen Dreikönig, Palmsonntag, Dreifaltigkeitssonntag, Mariä Himmelfahrt, Christkönig/ Sonntage in der Weihnachts- und Osterzeit: 9 - 8 - 6 - 5 - 4 - 2
 Hauptgottesdienst an Christi Himmelfahrt, Fronleichnam, Kirchweih, Allerheiligen: 10 - 9 - 8 - 7 - 5 - 4 - 3 - 1
 Messen an Christi Himmelfahrt, Fronleichnam, Kirchweih, Allerheiligen: 9 - 8 -6 - 5 - 4 - 1
 Hauptgottesdienst an Sonntagen in der Adventszeit: 8 - 7 - 5 - 4 - 3
 Messen an Sonntagen in der Adventszeit: 7 - 5 - 4 - 3
 Hauptgottesdienst an Sonntagen in der Fastenzeit: 9 - 7 - 5 - 4 - 3
 Messen an Sonntagen in der Fastenzeit: 9 - 7 - 4 - 3
 Hauptgottesdienst an Sonntagen im Jahreskreis: 9 - 8 - 6 - 5 - 4
 Messen an Sonntagen im Jahreskreis: 8 - 7 - 5 - 4
 Hochfeste an normale Werktagen: 9 - 8 - 7 - 4
 Feste an normalen Werktagen: 9 - 8 - 7 - 5
 Fatimarosenkranz: 9 - 8 - 6
 Fatimagottesdienst, Maiandacht: 9 - 8 - 6 - 4
 Taufe: 8 - 6 - 5
 Trauung: 8 - 7 - 5
 Reguiem: 10 - 8 - 7 - 5
 Aschermittwoch und Allerseelen:
5 - 4 -3
 Normale Werktage: 9 - 8 - 7
 Andachten an Werktagen: 9 - 8
 Angelus: 7:00:  8, 12:00: 4, Abends: (Je nach Dunkelheit):  8, 10,
 Freitag um 15:00 zum Gedächtnis an die Sterbestunde Christi: 3
 Sonntageinläuten und Hochfesteinläuten jeweils um 15:00
Jeweils als Reihenmotivläuten mit anschließenden Zusammenläuten der Geläute der jeweiligen Sonntage und Hochfeste

Weitere Anlässe werden je nach Rang und Bedeutung variabel geläutet.

Maße
 Länge: Außen: 89 m
 Breite: 28 m
 Höhe Gewölbe: 21 m
 Grundfläche: 2132 m2
 Turmhöhe: 89,50 m

Literatur

Weblinks

 Homepage der Pfarrei St. Jakob
 Homepage des Orgelbaufördervereins St. Jakob Straubing
 Die Glocken der Basilika St. Jakob in Straubing (Video)
 Das Vollgeläut von der Basilika St. Jakob in Straubing

Einzelnachweise

Kirchengebäude in Europa
Pfarrkirche des Bistums Regensburg
Kirchengebäude im Gäuboden
Jakob
Jakob
Basilica minor
Kollegiatstift
Kollegiatstiftskirche in Deutschland
Erbaut in den 1510er Jahren
Gotisches Bauwerk in Bayern
Gotische Kirche
Hallenkirche
Backsteinkirche
Jakobus-der-Ältere-Kirche
Rokoko-Kanzel

redpajama_set_name: RedPajamaWikipedia


text:
W-B Boscov's Update
i Jun 5th 2014
By Bill O'Boyle, Wilkes-Barre Times Leader
Al Boscov, principal owner of the Boscov Department Store chain, said the previously announced $1 million renovation of the downtown Wilkes-Barre store should begin within 60 days. He said a similar project was recently completed at the Boscov's store in Binghamton, N.Y.
Last month, Gary Boyer, Boscov's senior executive vice president/chief stores officer, said brighter lights, new carpeting and flooring, freshly painted walls, some new features, expanded departments and maybe a few new shops will be part of the renovations.
Boyer said $1 million will be more than enough to make a significant change to the appearance of the store that Boscov purchased in 1980. Boyer said a similar amount was spent on Boscov's Binghamton downtown store and the result was "dramatic."
One major change/expansion will be in the athletic footwear department. He said the new-look area will feature many more brands to give shoppers a lot of quality choices.
He said they intend to go through all five levels of the store, concentrating at first on the areas that need most attention.
Boscov's employs 141 full- and part-time people. The building contains approximately 230,000 square feet, which includes sales areas, offices and storage. Boscov's also has a multi-level parkade.


text:
Missouri – 2016 – HB1928 – SB 638 – Legislative Task Force on Dyslexia
March 13, 2016 at 11:07 pm April 26, 2017 at 1:19 am
Defines dyslexia, creates a "Legislative Task Force on Dyslexia" and requires the Department of Elementary and Secondary Education to employ a dyslexia specialist and develop professional development programs for school staff
This bill changes the laws regarding dyslexia. In its main provisions, the bill:
(1) Requires, by July 1, 2017, the Department of Elementary and Secondary Education to employ a dyslexia therapist, licensed psychometrist, licensed speech-language pathologist, certified academic language therapist, or certified training specialist to serve as the department's dyslexia specialist who has a minimum of three years of field experience in screening, identifying, and treating dyslexia and related disorders;
(2) Requires the department to ensure that the dyslexia specialist has completed specified training and received specified certification;
(3) Specifies the qualifications the dyslexia specialist must possess and the responsibilities he or she will have, including assisting the department with developing and administering specified programs for school districts no later than the 2017-18 school year;
(4) Establishes the Legislative Task Force on Dyslexia and requires the Joint Committee on Education to provide technical and administrative support as required by the task force to fulfill its duties;
(5) Requires the task force to meet at least quarterly and to advise and make recommendations to the Governor, General Assembly, and relevant state agencies regarding matters concerning individuals with dyslexia, including education and other adult and adolescent services. The meetings may be held via telephone or video conference;
(6) Requires the task force to consist of 18 members who will serve without compensation. Two must be members of the House of Representatives appointed by the Speaker of the House. The remaining membership is specified in the bill;
(7) Requires the task force to make recommendations for a statewide system for identification, intervention, and delivery of supports for students with dyslexia including the development of resource materials and professional development activities, which must be included in a report to the Governor and legislature and must include findings and proposed legislation. The report must be made available no longer than 12 months from the task force's first meeting; and
(8) Specifies what should be included in the recommendations and resource materials developed by the task force.
As Passed in SB 638:
By December 31, 2017, this act requires the Department of Elementary and Secondary Education to develop guidelines for the appropriate screening of students for dyslexia and related disorders and to develop the necessary classroom support for such students. Beginning in the 2018-19 school year, each public school, including charter schools, shall conduct dyslexia screenings and provide reasonable classroom support consistent with the guidelines developed by the Department of Elementary and Secondary Education.
Additionally, practicing teacher assistance programs shall include two hours of in-service training regarding dyslexia and related disorders provided by each school district for all practicing teachers. Such training shall count as two contact hours of professional development. (Section 167.950)
This provision is substantially similar to a provision contained in SCS/HCS/HB 2379 (2016), HCS/SB 711 (2016), SB 809 (2016), and SCS/SB 468 (2015), and is similar to HB 731 (2015).
This act also creates the Legislative Task Force on Dyslexia. The Task Force will advise and make recommendations to the Governor, Joint Committee on Education, and relevant state agencies. The Task Force will consist of twenty members, as described in the act. Except for four legislative members and the Commissioner of Education, the members will be appointed by the President Pro Tempore of the Senate and the Speaker of the House of Representatives. The task force will make recommendations for a statewide system for identification, intervention, and delivery of supports for students with dyslexia, as described in the act.
The Task Force will hire or contract for hire specialist services to support the work of the Task Force as necessary with appropriations or from other available funding.
The Task Force will terminate on August 31, 2018. (Section 633.420)
This provision is identical to a provision in HCS/SB 827 (2016) and HCS/SCS/SB 904 (2016), and is substantially similar to provisions contained in CCS/HCS/SB 635 (2016), HCS/SB 711 (2016), HCS/HB 1928 (2016), SCS/HCS/HB 2379 (2016), SB 548 (2015) and HCS/HB 921 (2015).
Categories Enacted Tags Missouri
US – 2015-2016 – HR 3033 READ Act
Connecticut – 2016 – SB 317 – Concerning Dyslexia
Status: Incorporated into SB 638, passed and signed into law 6/22/16, Bill History - HB 1928, Actions, SB 638
Bill Text: As Introduced; House Committee, Final Bill as Passed (Section 167.950 at pages 46-49)
History - House: 12/22/2015 Prefiled (H); 1/28/2016 Referred: Elementary and Secondary Education(H); 2/08/2016 Public Hearing Completed; 2/15/2016 Executive Session Completed; 2/15/2016 Voted Do Pass; 2/16/2016 Referred: Select Committee on Education; 3/03/2016 Executive Session Completed; 3/03/2016 HCS Voted Do Pass; 3/07/2016 HCS Reported Do Pass; 4/18/2016 H 1877 HCS Adopted (H), 4/18/2016 H 1877 Perfected with Amendments (H) - HA 1, HA 2, HA 3, and HA 4 adopted 4/19/2016 H 1935 Referred: Fiscal Review(H), 4/25/2016 H 2150 Reported Do Pass (H), 4/25/2016 H 2156 - 2157 Third Read and Passed (H) - AYES: 144 NOES: 5 PRESENT: 0, 4/25/2016 S 1045 Reported to the Senate and First Read (S), 4/28/2016 S 1396 Second read and referred: Senate Education(S)


Breath-taking lake views, rolling countryside hills – Wimbleball Lake is nestled in Exmoor National Park and offers the ultimate camping holiday.
Camp in luxury or pitch up your own tent – Wimbleball Lake is an AA graded 3 star campsite with a choice of belle tents, wooden pods, hard standings, electric and non-electric grass pitches for tents, motorhomes and caravans.
Enjoy a camping holiday with all of the home comforts, book a night's stay in one of Wimbleball Lake's brand new belle tents. Glamp on Exmoor, the three belle tents include a double bed and two campsite beds – sleeping 4-6 people comfortably. You can hire a fire pit and enjoy toasting marshmallows with the kids, try a spot of outdoor cooking on a barbeque (raised off the ground) or hire a telescope and do a spot of stargazing.


text:
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The Nanyang Business School, Nanyang Technological University invites applications for faculty positions in Finance at the Assistant/Associate/Full Professor...
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The School of Computer Science and Engineering (SCSE) is proud to have established an international reputation as one of the top Computer Science and Computer E
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Assistant/Associate Professor in Geometry, Dynamics, and Learning (tenure-track/tenured) The College of Science seeks a diverse and inclusive workforce and...
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Initially there are 10 places for 12th modified, 30 for 12th 13.5 and GT12 and 20 for WGTR but this may change depending on entry levels.
Saturday 8th and Sunday 9th September, this is a grand prix style meeting with the Saturday optional, but recommended.
In Bob's honour there will be a raffle in aid of Weston Park Hospital in Sheffield. This will be drawn at the end of the final meeting. If the ticket holder is not present when drawn the ticket will be redrawn, so make sure you are at the last meeting if you want a prize. Donations of prizes are welcome.
Entry is via this web site only. Verbal, email etc. entries will not be accepted. Entries will be accepted on a first come, first served basis. Reserve lists will be kept if necessary. Entry Fee £12.00 per class, per day. It is only possible to enter a single class (except WGTR). We may allow you to run a second class on the day if there are places available but this will also cost £12.00. Note the grand prix meeting is £12 per day, so £24 in total per class if you decide to race on both Saturday and Sunday.


Bristol Ageing Better and The Reader, a national charity building stronger communities through their Shared Reading programs, have announced a new programme. This new programme aims to create meaningful shared experiences and strong social networks for over 50s across Bristol.
Over the next two years, The Reader will work with organisations across the area to establish 30 new Shared Reading groups and train 60 new volunteers from the community and partner organisations to bring Shared Reading groups into sheltered housing sites, care homes, libraries and community centres.
The project has been developed in partnership with Bristol City Council Sheltered Housing, Brunelcare, Fresh Arts at Southmead hospital and Bristol City Council Libraries, who will each host reading groups across the city.