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\begin{document}

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\carmamemo{44}

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%\almamemo{222} % ALMA Memo number.
%\bimamemo{101} % BIMA Memo number.


\title{CARMA SUMMER SCHOOL 2007}
\author{Melvyn Wright, Marc Pound, Dick Plambeck, Douglas Bock, Katey Alatalo, Amber Baumeister, Peter Williams, Claudia Cyganowski, Danielle Lucero, Ran Wang, Laura Perez, Walter Max-Moerbeck, Colette Salyk, Sidharth Kumar, Kijeong Yim, Hsin-Fang Chiang, Nick Hakobian, Megan DeCesar, Katharine Johnston}
% \affil{Radio Astronomy laboratory, University of California, Berkeley, CA, 94720}

\begin{abstract}
The first CARMA SUMMER SCHOOL  was held at the observatory on Cedar Flat
2007 July 8-14 with 15 students from the Berkeley, Caltech, Illinois,
Maryland, NRAO, and Scotland.  During the school each participant made
observations, and analyzed the results. In this memo we collect together
some of these results from the student projects.

\end{abstract}

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\ChangeRecordBegin
\addrevision{1.0}{2008-Jan-03}{MCHW}{1-6}{Draft memo}
\addrevision{1.1}{2008-Feb-08}{MCHW}{1-13}{added student contributions}
\addrevision{1.2}{2008-Mar-25}{Megan}{7,14}{added student contributions}
\addrevision{1.3}{2008-Mar-25}{MCHW}{1-14}{cleanup TeX}
\addrevision{1.4}{2008-Apr-02}{MCHW}{1-14}{added Danielle Lucero text abd figures}
\addrevision{1.5}{2008-May-08}{MWP}{1-14}{Major cleanup, added Sid Kumar}
\ChangeRecordEnd


\section{INTRODUCTION}

The first CARMA SUMMER SCHOOL was held at the observatory on Cedar Flat
2007 July 8-14 with 15 students from the Berkeley, Caltech, Illinois,
Maryland, NRAO, and Scotland.  During the school each participant made
observations, reduced the data and analyzed the results. Here are some
of the instrumental characteristics to help select a suitable project
and to learn observing and data analysis techniques from it.
Each student received 2 to 4 hours on source.

The CARMA telescope is designed as an aperture synthesis telescope.
There are two receiver bands: 3 mm and 1 mm. A basic aperture synthesis
observation makes an image the size of the primary beam (lambda/diameter
$\sim$ 1 arcmin at 100 GHz; 0.5 arcmin at 230 GHz) with a resolution
corresponding to the maximum separations of the 15 antennas. Students
learn how this works at the school. During the school the telescope was
in the compact D-configuration, which gives an angular resolution
of $\sim$ 3-6 at 100 GHz, and 1.5-3 arcsec at 230 GHz.

The most convenient source size is one which is smaller than the size
of the primary beam. Larger sources can be imaged by time-sharing the
pointing of the antennas (mosaicing), at the cost of lowered sensitivity.

The sensitivity is determined by the system noise (receivers plus
atmosphere), the bandwidth (or velocity resolution), and the observing
time. The atmosphere is usually not so good for 1 mm observations
in the summer, or for sources which are at low declinations and must
be observed through more of the atmosphere, so it's best to select a
bright source which is high in the sky and can be observed at 3 mm,
but don't be discouraged if your favorite source does not satisfy all
these conditions. It's best to observe a strong enough source that you
can make an image during the school, rather than a detection project,
then you can see the effects of different imaging techniques.


\section{LOGISTICS}

Because this is a 'hands-on' school, we held all lectures and
demonstrations in the control building at Cedar Flat, adjacent to
the telescopes.  Breakfast and lunch food were provided. Dinners from
Mon-Fri were cooked communally in the control room kitchen.

Since the dorm and cottage at OVRO can accommodate at most 8, several
students joined Mel, Dick, and Marc in camping out at the 'Nelson' group
campground, about 1.5 miles from the control room.  The campers avoid
the hassle of driving up and down the mountain each day, and have a
wonderful opportunity to star-gaze each night.

The school ran from 9am Monday to Friday night 13 July.  Most students
arrived on Sunday 8 July and departed on Saturday 14 July.  We organized
a hike to Bristlecone Pines on Saturday.


\section{STUDENT PROJECTS}
\subsection{Claudia Cyganowski (U. Wisconsin, Madison)}

I observed HCO+(1-0), HCN(1-0), and N2H+ (1-0) (and continuum) towards
G28.83 (a MYSO outflow candidate identified based on extended 4.5um
emission in GLIMPSE images).  The science goals were to investigate
whether HCO+ traced an outflow coincident with the extended 4.5um emission
(which has been hypothesized to trace shocked H2 in outflows) seen in the
GLIMPSE images, and to determine whether the 4.5um emission was associated
with a single or multiple protostar(s) (using dense gas tracers and dust
continuum emission).  The HCO+ (1-0) velocity structure is complicated,
apparently tracing multiple outflows from at least two protostars.  A
central compact core is observed in HCN and mm continuum (I also observed
at 1mm in bad weather; the continuum was useable).  The mass of this core
(calculated from 1mm continuum) is consistent with it being a massive
protostar.

\subsection{Ran Wang (NRAO)}

The science goal is to detect DCO+, DCN, H2CO absorptions toward the
gravitational lensing BL Lac object B0218+357.  I observed 5.5 hours on
source and detected H2CO (Figure \ref{f-B0218}). 
There is a recent published H2CO absorption result
for the same target (the same line), which was observed in 1997. Compared
to their result, I found that the continuum of the target increased by
a factor of 2, and the optical depth of the line absorption also changed.

The original plan was to search the DCO+ and DCN absorptions in the 
z=0.68547 gravitational lens towards B0218+357 and study the D/H ratios.
However the final rms was not good enough to get these two lines.
The H2CO absorption was detected and the optical depth determined.
I found the optical depth is about 2-3 times smaller compared to the
published measurements ten years ago. I am thinking about high
resolution observations of this source with the VLA to understand this
change.


\begin{figure}
\psfig{figure=B0218.H2CO.7.ps,angle=-90,width=6.0in}
\caption{
H2CO absorption spectra towards B0218+357 at 7 km/s resolution.
}
\label{f-B0218}
\end{figure}

\subsection{Hsin-Fang Chiang (UIUC)}


The source I observed was the Class 0 young stellar object L1157-MM at RA
20:39 and DEC +68:02.  The  correlator configuration was 3mm continuum and
12CO(1-0) line at 115.271GHz.  Bandwidths of both 8MHz and 2MHz were used,
and coincided at the same frequency.  Both 3mm continuum and 12CO(1-0) line
emission were observed and well detected (Figure \ref{f-L1157}).  
The 3mm dust continuum shows
the envelope structure and can help revealing the envelope's collapsing
mechanism, also may suggest the existence of embedded circumstellar disk
after detailed modeling.  The CO line emission traces the bipolar outflows
driven by this young stellar object.  The CO map as in the figure shows the
morphology of the outflows.  In the velocity space it can be seen that the
northern lobe is redshifted and the southern lobe is blueshifted.  What was
observed in this track was only the central part of the long-extended
outflows.  A mosaic will be needed to see the whole outflow structure.

\begin{figure}
\psfig{figure=COoutflow2.ps,angle=-90,width=7.0in}
\caption{
CO outflow in Class 0 young stellar object L1157-MM.
}
\label{f-L1157}
\end{figure}

\subsection{Amber Bauermeister \& Katey Alatalo (UCB)}

Amber Bauermeister observed NGC5005, one of the BIMA SONG galaxies
with the highest CO surface brightness, in HCN. Katey Alatalo observed
another BIMA SONG galaxy in HCN for the same purpose. We wanted to see
if we could detect it in HCN, a tracer for high density gas in the inner
region of the galaxy. Our observations did give a detection of HCN in the
central region of the galaxy.

\subsection{Kijeong Yim (UIUC)}

The source was NGC 891 taken by 13CO(1-0).  The science goals was
study of vertically extended emission in the edge-on galaxy NGC 891.
My observations were two mosaic tracks, along the major and minor axes
of the galaxy (Figures \ref{f-n891integ-major}, \ref{f-n891integ-minor},
\ref{f-n891pv-major}, \ref{f-n891pv-minor}).  While I did detect 13CO(1-0),
I couldn't see any extended vertical disk.  The tracks have similar
integration time. However since the major axis mosaic contained more
pointings, the S/N in that track is lower.

\begin{figure}
\psfig{figure=n891.vel.ps,angle=-90,width=6.0in}
\caption{
13 CO (1-0) map of NGC 891 from 300 to 740 km/sec.
Mosaic at five points along the disk major axis. (offsets:
[0.667,0.667],[0.33,0.33],[0.0,0.0],[-0.33,-0.33],[-0.667,-0.667])
}
\label{f-n891integ-major}
\end{figure}

\begin{figure}
\psfig{figure=vel.ps,angle=-90,width=6.0in}
\caption{
vel.ps : 13 CO (1-0) map of NGC 891 from 300 to 740 km/sec.
Mosaic at two points along the axis perpendicular to disk.
(offsets in mosaic options: [0.0,0.0],[-0.4,0.167])
}
\label{f-n891integ-minor}
\end{figure}

\begin{figure}
\psfig{figure=n891.pv.ps,angle=-90,width=6.0in}
\caption{
Position-velocity diagram of 13 CO (1-0) from major axis track. The velocity
resolution is 20 km/sec.
}
\label{f-n891pv-major}
\end{figure}

\begin{figure}
\psfig{figure=pv.ps,angle=-90,width=6.5in}
\caption{
Position-velocity diagram of 13 CO (1-0) from minor axis track. The velocity resolution
is 20 km/sec.
}
\label{f-n891pv-minor}
\end{figure}


\subsection{Megan DeCesar (UMD)}

My source was M82, a starburst galaxy in the nearby M81 group that has
been studied extensively.  The starburst is the result of an
interaction between M81 and M82 that occurred $\sim 200$ million years
ago.  Long tails of atomic hydrogen connect the galaxies today,
providing concrete evidence of this past interaction that triggered
star formation in the spiral arms of M81 and inner regions of M82.
The violent deaths of massive stars in M82 have blown gas from its
core, giving it its ragged appearance and classification as a
starburst galaxy.  

I chose this object because it has been observed successfully by BIMA
and would be an easy target for CARMA.  This almost guaranteed that I
would get good data that could be used to learn the data reduction
tools in MIRIAD.

My data turned out well, as expected.  We did have a calibration issue
-- we had not observed a calibration source other than at the
beginning and end of the observation.  In spite of this, M82 showed up
clearly in both the image and the spectra, so although we cannot
obtain a flux measurement we can still glean information like
rotational velocity from the data.

Figure \ref{f-m82} shows the CO(1-0) transition in the central $\sim
400$ pc of M82, assuming a distance of $\sim 3.7$ Mpc.  We have
deconvolved the data using a point source clean routine (blue) and a
maximum entropy routine (red).  The two methods are consistent in
their reproduction of the source structure, and match well with images
made previously of this region of the galaxy.

\begin{figure}
\psfig{figure=m82_megan.cm.ps,angle=-90,width=7.0in}
\caption{CARMA map of the CO J=1-0 transition in M82's center.  The blue contours were derived from a point source deconvolution, the red from maximum entropy.}
\label{f-m82}
\end{figure}

\subsection{Sidharth Kumar (UMD) }

The Eagle Nebula (RA,DEC) = 18:18,--13:47) was observed in
$^{13}$CO$(1-0)$ $(110.2GHz)$, $^{12}$C$^{18}$O$(1-0)$ $(109.78GHz)$
and in the continuum. The bandwidths for the set line frequencies and
the continuum were $8MHz, 8MHz$ and $500MHz$ respectively. The pillars
of the nebula were mapped out in a $19$ point mosaic. The signal to noise
was highest in the $^{13}$CO$(1-0)$ maps as expected. Fig. \ref{f-eagle}
shows the velocity integrated image obtained in the $^{13}$CO$(1-0)$.

\begin{figure}
\psfig{figure=eagle.ps,width=7.0in,angle=-90}
\label{f-eagle}
\caption{$^{13}$CO$(1-0)$ Eagle Nebula image integrated between $V_{LSR}$ = 20 and 27 km/s}
\end{figure}



\subsection{Danielle Lucero (New Mexico Tech)}

My summer school project is a 0ontinuation of  a project that I
started that aims to map the CO emission in a sample of nine
elliptical galaxies.  Our goal is to measure the direction of rotation
of the gas and to compare that to stellar kinematics. The results
should reveal how much of the molecular gas is may have come from
internal stellar mass loss and how much must have been acquired from
outside.  The key is the angular momenta: if the gas and stars have
misaligned angular momenta, then an internal origin can be ruled out
(for galaxies which are not strongly triaxial).

At the summer school I observed the E/S0 galaxy NGC 6524 in the 12CO
1-0 line which was previously detected with the CSO 10m telescope.  I
used a hybrid mode: I used a correlator setup with three 62MHz bands
slightly overlapped to give a total coverage of 440 km/s.

To date the results are: I detected the CO as expected 
(Figures \ref{f-n6524}, \ref{f-n6524velo}, \ref{f-n6524spec}).  
The CO emission resides in a disk in regular rotation about the center.
There may be some indication that the line was longer than what the
literature quoted so I observed the source again using a different
correlator setup so that I could get any line that may have been missed.
I have not yet reduced this extra data set.  It may not be necessary
since it seems that I got enough of the line to determine the science goals.

The total flux is: $\sim 78.8$ Jy~km/s which is very close to the single
dish detection (82 Jy~km/s)
The total H2 mass is then: $6.3\times 10^9 M_{\odot}$.

I have not yet finished reducing the optical data for this particular source.

\begin{figure}
\psfig{figure=N6524intint.eps,angle=-90,width=6.0in}
\caption{
An CO integrated intensity map of NGC 6524 
overlayed on an SDSS2
Red optical image.
contours are in increments of -15\%, -10\%, 10\%, 15\% 30\% 50\% 90\% of the
peak 32.35 Jy/beam~km/s the beam size is: 3.8"x3.2"
}
\label{f-n6524}
\end{figure}

\begin{figure}
\psfig{figure=N6524velo.eps,angle=-90,width=6.0in}
\caption{
An 1st moment map of NGC 6524  Contours are in increments of 5\%
of the peak.
}
\label{f-n6524velo}
\end{figure}

\begin{figure}
\psfig{figure=N6524spec.ps,angle=-90,width=6.0in}
\caption{
The CO spectrum of NGC 6524 calculated for the central brightest pixel.
}
\label{f-n6524spec}
\end{figure}

\clearpage
\section{Email Addresses of Participants}
\begin{verbatim}
Melvyn Wright <wright@astron.berkeley.edu>, 
Marc Pound <mpound@astro.umd.edu>, 
Douglas Bock <dbock@mmarray.org>, 
Dick Plambeck <plambeck@astro.berkeley.edu>, 
Katey Alatalo <kalatalo@astro.berkeley.edu>, 
Amber Baumeister <ameisteb@astro.berkeley.edu>, 
Peter Williams <pkwill@astro.berkeley.edu>, 
Claudia Cyganowski <ccyganow@astro.wisc.edu>, 
Danielle Lucero <dmr2010@gmail.com>, 
Ran Wang <rwang@nrao.edu>, 
Laura Perez <lperez@astro.caltech.edu>,
Walter Max-Moerbeck <wmax@astro.caltech.edu>, 
Colette Salyk <csalyk@gps.caltech.edu>, 
Sidharth Kumar <skumar@astro.umd.edu>, 
Kijeong Yim <kyim2@astro.uiuc.edu>, 
Hsin-Fang Chiang <hchiang2@astro.uiuc.edu>, 
Nick Hakobian <nhakobi2@astro.uiuc.edu>, 
Megan DeCesar <decesar@astro.umd.edu>, 
Katharine Johnston <kgj1@st-andrews.ac.uk>
\end{verbatim}



\end{document}
