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\begin{document}
\vspace*{\fill}
\title{Further Insights into the Structure of}
\title{30 Doradus from the}
\title{Hubble Space Telescope Instruments\/\altaffilmark{1}}

\author{Nolan R. Walborn and Jes\'us Ma\'{\i}z-Apell\'aniz}
\affil{Space Telescope Science Institute\\
3700 San Martin Drive\\
Baltimore, MD 21218\\
walborn@stsci.edu, jmaiz@stsci.edu}

\author{Rodolfo H. Barb\'a\/\altaffilmark{2}}
\affil{Facultad de Ciencias Astron\'omicas y Geof\'{\i}sicas\\
Universidad Nacional de La Plata\\
Paseo~del~Bosque\\
1900 La~Plata, Argentina\\
rbarba@fcaglp.fcaglp.unlp.edu.ar}
\vspace{1in}
\centerline{\titlelarge To be published in the September 2002 issue of the \emph{Astronomical Journal}}
\received{24 April 2002}
\accepted{22 May 2002}
\sluginfo
\vfill

\altaffiltext{1}{Based on observations with the NASA/ESA 
Hubble Space Telescope obtained at the Space Telescope Science Institute, 
which is operated by the Association of Universities for Research in Astronomy, 
Inc., under NASA contract NAS5-26555.}
\altaffiltext{2}{Member of the Carrera del Investigador Cient\'{\i}fico, CONICET, Argentina.}

\begin{abstract}
New observations with the HST Wide Field Planetary Camera~2, combined
with prior archival data, provide nearly complete coverage of the inner
30~Doradus Nebula in both nebular lines and continuum at 0\farcs1
resolution.  The developing wind-blown cavity surrounding the massive
first-generation, central cluster and its interface with the remanent
molecular clouds, the site of second-generation, triggered star
formation, are imaged in their entirety.  Dithered Planetary Camera 
observations with 0\farcs03 resolution of Knots~1--3 reveal further 
structural details of the large dust pillars oriented toward the central 
cluster and the newborn, massive multiple systems of the second generation 
in those fields.  The new data also provide the first WFPC2 coverage of 
the fields of two interesting, luminous infrared sources observed in
our previous Near Infrared Camera and Multi-Object Spectrometer program;
comparisons of the high-resolution optical and IR images are illuminating.
In addition, we have obtained Space Telescope Imaging Spectrograph optical,
long-slit observations of seven O-type multiple systems in the region,
including those in Knots~1--3 and four representatives of the older
generation.  The spatially resolved spectrograms and classifications of
the close pairs, with separations ranging from 0\farcs09 to 1\farcs18,
are presented, as well as WFPC2 photometry of the individual components 
and the compact clusters of fainter stars associated with them.
These new observations, and planned further analysis of them, offer
significant new information about the intricate structure and evolution 
of the two-stage starburst in 30~Doradus.     
\end{abstract}

\keywords{galaxies: starburst --- H~II regions --- ISM: individual (30~Doradus) 
---  Magellanic Clouds --- stars: early-type --- stars: formation}


\section{Introduction}

The praises of 30~Doradus are often sung and need not be echoed here;
suffice it to recall that it is the largest H~II region in the Local
Group, and the most propitious representative of its age group for 
investigation of the spatial and temporal characteristics of a starburst 
in fine detail.  In recent years, the Hubble Space Telescope (HST) has
contributed qualitative advances in our knowledge of 30~Doradus, because
of its high spatial resolution and ultraviolet sensitivity.  Photometry
in images from the HST cameras of thousands of individual stars in the 
massive central cluster, including its dense core R136, has revealed a
normal initial mass function and a total mass of $\sim2 \times 10^4$~M$_{\sun}$ 
(Hunter et~al.\ 1995a, 1996, 1997; Parker, Heap, \& Malumuth 1995; Sirianni
et~al.\ 2000).  Spatially resolved spectroscopy of dozens of the brighter
members of the inner cluster with the HST spectrographs has found the
richest concentration of the most massive hot stars (spectral types O2--O3)
accessible to such observations (de~Koter, Heap, \& Hubeny 1997, 1998;
Massey \& Hunter 1998; Walborn et~al.\ 2002).  HST nebular imaging has
shown intricate structural details, providing the essential insight that
the brightest nebulosity comprises the narrow interface between the
central cavity being evacuated by the stellar winds, and the surrounding
molecular clouds (Hunter et~al.\ 1995b; Scowen et~al.\ 1998; Rubio et~al.\ 1998).  
Infrared images from HST have discovered surprising characteristics of the 
new stellar generation being triggered at and near that interface (Walborn 
et~al.\ 1999a; Brandner et~al.\ 2001).

In this paper, we present further observations of 30~Doradus with the HST 
Wide Field Planetary Camera~2 (WFPC2) and the Space Telescope Imaging
Spectrograph (STIS), which offer useful additional information about this
unique region.  The new WFPC2 images essentially complete the partial coverage 
of the inner nebula available from previous programs and provide higher 
spatial resolution for three subfields of special interest.  They also include
the fields of two luminous infrared sources observed in our earlier HST 
Near Infrared Camera and Multi-Object Spectrometer (NICMOS) program, 
which are compared with the new optical images here.  The STIS long-slit
spectroscopy resolves several O-type multiple systems outside the cluster
core, including representatives of both the younger, second stellar generation
and the older first generation.  WFPC2 photometry of these objects is also 
presented, based on archival and new images.  Finally, further measurements 
and analyses of these data planned for future papers are previewed. 


\section{Observations}

\subsection{WFPC2}

Previously, only partial HST/WFPC2 coverage of 30~Doradus was available,
comprising the three, asymmetrically located WFC fields when the clusters
R136 (programs Nos.~5114/PI J.~Westphal and 5589/PI J.~Trauger) and
Hodge~301 (No.~6122/PI Y.-H.~Chu) were centered in the PC chip.
Furthermore, program No.~5114 contains only continuum-filter exposures.
We have remedied this situation in our program No.~8163, which performed
two WFPC2 continuum pointings designed to cover the gaps, and three
nebular-line pointings with Knots~1--3 centered in the PC and field
rotations again planned to complete coverage of the inner nebula insofar
as possible.  (The southern continuum field observed the association
surrounding the Luminous Blue Variable R143--Parker et~al.\ 1993; Walborn
\& Blades 1997--and is not discussed in this paper.)

The continuum observations were done in 1999~October and the nebular-line
observations in 2000~March, April, and September.  Table~1 lists details
of the WFPC2 data.  Successive columns identify the fields; the
pointing coordinates for equinox 2000; the dates of the observations; the
filters; and the exposure times.  Each continuum observation consisted of
a short and a long exposure, the latter split in half for cosmic-ray
removal, in order to cover the stellar magnitude range of interest (12--21)
without saturation.  The nebular-line observations were dithered to
increase the resolution, in a 4-point box pattern for F673N and a dual
pattern for the other filters.

\vspace{-6pt}

\subsection{NICMOS}

The NICMOS images in 30~Doradus were obtained under HST program No.~7819
during 1998 February and March.  The data have been described by Walborn
et~al.\ (1999a) and Brandner et~al.\ (2001), so only a few details pertinent 
to those shown here will be repeated.  They were obtained with the NIC2 
camera, which has a 19\arcsec\ square field of view, through broad-band 
filters F110W (approximately $J$), F160W ($H$), and F205W ($K$), with total 
exposure times of 320~s, 384~s, and 448~s, respectively, split equally 
between two dithered positions.  The present images have been processed
through the STScI data pipeline, including subtraction of the thermal
background at $K$ by means of a blank field observation, and they have
not been deconvolved.

\vspace{-6pt}

\subsection{STIS}

During prior work with the WFPC2 and NICMOS images, a number of
interesting close visual binaries or multiple systems were noted among
the 30~Doradus stellar populations outside of R136, including the systems 
in all of Knots~1--3.  In order to understand the content of these
systems, spatially resolved spectroscopy is required.  Such was included 
in our HST program No.~8163, by means of the long-slit capability of STIS.  
The optimum wavelength region for spectral classification and subsequent 
quantitative analysis of OB stars is the blue-violet, 3900--4800~\AA.  
Neither of the two STIS/CCD configurations covering this
region is ideal for these purposes:  although the spectral coverage of
the lower resolution G430L configuration (2900--5700~\AA) is more than
ample, its 2-pixel resolution of 5.5~\AA\ is rather lower than desirable; 
while the higher resolution G430M configuration offers more resolution
(0.56~\AA) than necessary at least for classification, but covers only 
286~\AA\ per observation, which together with the supported central 
wavelengths requires 4 exposures to provide the desired wavelength
coverage (settings at 3936, 4194, 4451, and 4706~\AA).
This situation has been recounted at some length to explain the observing
strategy adopted: for the brighter systems, the optimum 4 G430M
observations were obtained; for the systems of intermediate brightness,
the 3 longest wavelength G430M settings were obtained; while for the
faintest systems, only the single G430M setting covering the crucial He~I
$\lambda\lambda$4387, 4471 and He~II $\lambda$4541 lines, as well as
H$\gamma$, was observed, supplemented by a G430L observation.  In all
cases, the STIS long slit was oriented at the position angle of the
separation between the brightest binary components in the systems.

The STIS observations were performed from 1999~October through 2000~May.
Table~2 lists characteristics of the stellar systems and the observations, 
first for the three young systems in Knots~1--3, followed by four older
systems.  Successive columns give the stellar identification from Parker 
(1993); coordinates for equinox 2000; the separation of the binary components 
in arcsec; the position angle of the fainter component from the brighter in
degrees; the date of the observations; the STIS grating settings observed; 
the exposure times in seconds; and the peak signal-to-noise per 2-pixel
resolution element in each spectrogram.  

For completeness, it is mentioned that an eighth object, Parker~644, was
also observed with the single G430M setting and G430L.  This interesting
faint star is located near the southern end of the western interface and
appears to be very young, similarly to Knots~1--3.  It is an IR source
(Rubio et~al.\ 1998 IRSW-98; the NICMOS field NIC01 is reproduced by 
Brandner et~al.\ 2001) and has associated nebular knots, one of which is
resolved in the STIS spectrograms.  Unfortunately, the higher resolution
STIS observation is too noisy to be useful, and at the lower resolution
the stellar spectrum is nearly featureless, with only some high Balmer
series members detected in absorption.  We are uncertain whether the latter 
results are primarily physical or observational; in any event, these data 
are not discussed further here.

\vspace{-6pt}

\section{Reductions}

\subsection{WFPC2 Images}

The WFPC2 images were reduced with two different procedures.  The four 
continuum and five narrow-band pointings were jointly processed to produce 
$272\arcsec\times179\arcsec$ mosaics at 0\farcs10 resolution, while the three
new narrow-band dithered PC fields were used to produce $33\arcsec\times
33\arcsec$ images at an enhanced 0\farcs032 resolution.  The reductions
were carried out with both standard STSDAS/IRAF\footnote{IRAF 
is distributed by the National Optical Astronomy Observatory, which is 
operated by the Association of Universities for Research in Astronomy, 
Inc., under cooperative agreement with the National Science Foundation.} 
packages and custom-made IDL\/\footnote{IDL is a registered trademark of
Research Systems, Inc.} routines.

The first step was to update the WFPC2 group parameters affected by
plate-scale, shift, and rotation changes due to Project Data Base Updates
with the WFPC2 task {\it uchcoord\/} (Biretta et~al.\ 2000). A correction was
found to be necessary for the data from programs Nos.~5114 and 5589. The 
second step was to eliminate cosmic rays. For the three new narrow-band 
dithered pointings this step was done with a combination of the {\it dither\/} 
package (Koekemoer et~al.\ 2000) and the WFPC2 task {\it crrej\/}.  For the 
rest of the data we simply used {\it crrej\/}.

At this point we were able to produce the final narrow-band, 
high-resolution PC images of the three Knots by using the standard 
{\it dither\/} procedures.  Color images were produced from these data in two 
ways:  with F502N and F656N in the green and red channels, respectively; 
and with F502N and F673N in the green and red channels, respectively 
(note that the blue channel is not used for these images).
On the other hand, the production of the large lower-resolution
mosaics was somewhat more complicated.   We first corrected for geometric
distortions using the WFPC2 task {\it wmosaic\/} and we photometrically
calibrated each field.  The next step was to combine all the continuum and
narrow-band pointings into a single $272\arcsec\times 179\arcsec$ mosaic. 
In order to do that, one has to take into account that the precision of the 
absolute astrometry in the WFPC2 headers is determined by that of the 
Guide Star Catalogue, which is typically 1\arcsec\ (10~WFC pixels). This 
effect is quite large when one combines different WFPC2 pointings and it has 
to be corrected.  To do so, we applied the {\it crossdriz\/} task in the 
{\it dither\/} package in selected regions common to pairs of different 
pointings and we then corrected for the relative displacements which were 
indeed found to be of the order of 1\arcsec.  Finally, we used a procedure 
similar to that outlined in MacKenty et~al.\ (2000) to eliminate the nebular 
contribution to the continuum filters and produce ``pure-continuum'' images. 
We also tried the same procedure to eliminate the continuum contribution to 
the narrow-band filters, but we decided not to use it because of the 
introduction of artifacts due to the existence of uncorrected 
geometrical displacements and distortions at the 0\farcs1 (1~WFC pixel)
level (these distortions are unimportant in the continuum mosaics due to the
point-source nature of the stellar images).

The above procedure was applied to the data to produce three continuum
(WFPC2 $U$, $V$, and $I$) and three narrow-band (F502N, F656N, and F673N) 
multi-pointing mosaics. Along the way we applied several procedures to 
eliminate cosmetic defects such as bad pixels, low-signal interchip regions, 
and saturated stars. We also eliminated by hand the noisy pixels in the 
short-exposure F336W images from program No.~5114.  In order to produce an 
RGB color mosaic of the full field that represented gas excitation and 
intensity as well as star colors and brightnesses, we first discarded the 
F502N mosaic since F673N and F656N contain the required information.  Our 
idea was to show stars in ``near-true'' color by using WFPC2 $I$, $V$, and 
$U$ for the red, green, and blue channels, respectively, and to include the 
information about the gas by adding F673N and F656N to the red and green
channels, respectively.  When we tried to do that, we found that the
contrast between the bright and dim regions in F673N was so large that it 
was not possible to show the structures present at different intensity 
levels.  To reduce the contrast we subtracted from the original mosaic a 
$101\times 101$~pixel median-filtered version of itself multiplied by a 
positive coefficient smaller than one.  We also discovered that the continuum 
contamination in the F673N and F656N filters changed the color of all stars 
into red or orange. This problem was solved by masking the positions of the 
stars in those filters.  With those corrections implemented, the final result 
displayed below was obtained.

\vspace{-6pt}

\subsection{STIS}

The standard procedure for extracting STIS CCD spectra is to obtain a
wavelength calibration (which produces a $\lambda(x)$ function, where $x$
is the horizontal pixel coordinate), and to sum over a range of pixels in 
the spatial direction of the detector ($y$) in order to produce the flux at 
a given $\lambda$ after the background is subtracted.  Such a procedure 
would not work for most of our observations because of the overlapping
spatial profiles produced by the small separations between pairs of stars. 
Therefore, we fitted the data at each $x$ position with a double-peaked 
spatial profile in order to produce the flux as a function of $\lambda$ for 
each of the two stars.  We tested different alternatives for the double-peaked 
function (gaussians, gaussians with additional wings, and gaussians 
integrated over the spatial direction for each pixel), but the results
were nearly independent of the choice made.  The discussion below refers
to the third profile (spatially integrated gaussians), but its modification 
for the other two cases is straightforward.

Our goal is to obtain three parameters for each of the two stars at each
$x$ coordinate:  $I_0(x)$ (the peak intensity), $y_0(x)$ (the spatial
position of the peak), and $\sigma(x)$ (the width of the fitting profile). 
The parameter $y_0(x)$ is not a constant since there is a displacement of a 
few pixels between $x=1$ and $x=1024$ caused by the grating alignment.  In 
principle, one would think that the six parameters at a given $x$ (three for 
each star) could be allowed to vary in a completely independent way to 
produce the final result.  However, there is a numerical problem that impedes 
such a procedure.  As each profile moves from a pixel center (half-integer 
values of $y_0(x)$) to a pixel edge (integer values of $y_0(x)$), the discrete 
nature of the sampled profile shifts flux from one star to the other during 
the fitting procedure by introducing a non-physical oscillation as a function 
of $x$ in the values of $y_0(x)$ and $\sigma(x)$.  We solved this problem 
in three steps. (1)~In a first pass, we fitted all three parameters 
($I_0(x)$, $y_0(x)$, and $\sigma(x)$) for each of the two stars at each
$x$ position.  (2)~From those results, we fitted a straight line to each
$y_0(x)$ and repeated the fitting procedure fixing the value of the two 
$y_0(x)$ to those obtained from the fit.  (3)~From the results of the 
previous step, we now fitted a parabola to each of the $\sigma(x)$.  Then, 
we did a final pass fixing each of the $y_0(x)$ and $\sigma(x)$ (i.e., 
leaving only the two $I_0(x)$ as free parameters) in order to obtain the 
two final values of $I_0(x)$.  The integrated fluxes for each star 
(proportional to $I_0(x)\times\sigma$) were then rectified to produce the 
final spectrograms.

\vspace{-6pt}

\subsection{WFPC2 Photometry}

The photometric results presented here are concentrated in small areas around 
the spectroscopic targets.  These results are extracted from a complete 
photometric analysis of about 20,000 stars down to $V=25$ in the WFPC2 images 
of the 30~Dor Nebula; a more detailed description of the reduction process 
will be presented in subsequent papers (Barb\'a et~al., in preparation). 

All broad-band WFPC2 images were calibrated with standard STSDAS/IRAF 
procedures.  The photometric analysis was performed with two different 
software packages, {\em HSTphot} (Dolphin 2000a) and {\em IRAF/DAOPHOT} 
(Stetson 1987), to provide internal checks.  The results presented here 
are derived mainly from {\em HSTphot}; DAOPHOT was used to recover 
photometric information for several important stars with special 
circumstances, such as those located in vignetted regions of the chips. 

The {\em HSTphot} package (Dolphin 2000a, b) is specifically designed to 
handle the characteristics of the WFPC2 images by means of a library of 
TinyTim (Krist 1995) undersampled PSFs; it also contains a set of 
programs for general reduction procedures such as masking, cleaning, and 
combining WFPC2 images.  Version~1.1 (October 2001) was used here.
The first step was to mask all bad and saturated pixels identified in the
data-quality images with the procedure {\em mask}.  The next step was to 
remove cosmic rays from the images with the procedure {\em crmask}.  This task 
can clean images that are not perfectly aligned, and it can handle images
with different filters, when the individual observations were not split  
(as was the case for the F336W image in program No.~5114). 
For each of five different WFPC2 pointings and three broad-band filters,  
a combined deep image was produced with the procedure {\em coadd}.  The
final required steps {\em getsky} and {\em hotpixels} were applied to the 
combined images to compute sky background and clean hot pixels.
The {\em HSTphot} (named {\em multiphot} in version~1.0 of the package)
routine was run on the images from each of the five pointings.  {\em HSTphot} 
is a powerful task that performs stellar PSF photometry on multiple 
images in a single run, including alignment and aperture corrections, 
PSF modification to compensate geometric distortion (Holtzman et~al.\ 1995) 
and the 34th row error (Shaklan, Sharman, \& Pravdo 1995; Anderson \& King 
1999), and correction of charge-transfer inefficiency (Dolphin 2000b).  
During the run of {\em HSTphot}, the determination of the ``local sky'' 
parameter was enabled because of the very nonuniform nebular background in
the 30~Dor Nebula.  A ``sharpness'' parameter and a measure of 
the quality of the fit (${\chi}^2$) were used to reject false star 
detections in regions with very structured nebulosity or diffraction spikes 
of bright stars, among other artifacts.  Additional star rejections were 
made by visual inspection of the images.  

The photometric results presented in Tables~4--8 correspond to stars  
contained in a  $12''\times12''$ box around the spectroscopic targets, with 
F555W magnitudes brighter than 20.5.  The magnitudes are in the WFPC2 
flight system as defined by Holtzman et~al.\ (1995), but with new
photometric zero-point calibrations derived by Dolphin (2000b).  The X and
Y coordinates are in the chip coordinate systems of the F555W images, with 
the {\em HSTphot} convention (0--799).  

Stars P1304 and P1306 were observed in images from program No.~5114, and they 
are in the vignetted region of chip~2 (Y~$<46$); therefore, some loss of light 
is expected.  We estimate the loss for those stars to be about 30\% from 
linear interpolation between values of 50\% illumination at Y~=~26 and full 
illumination at Y~=~46 (see Table~2.5 of the WFPC2 Instrument Handbook).  
The magnitudes for stars in the vignetted region were obtained with 
{\em IRAF/DAOPHOT}, since {\em HSTphot} is disabled in that region.
However, no accurate correction of the vignetting itself is available,
and further aspects of the {\em IRAF/DAOPHOT} application there will be
discussed in the subsequent papers.
 

\section{Results and Discussion}\nobreak
\subsection{The Structure of the Inner 30 Doradus Nebula}
Figure~1 is a nearly complete mosaic of the inner 30~Doradus Nebula,
based on seven HST/WFPC2 pointings, four from the current program and
three from the archives, as detailed in the preceding sections.  The 
color coding of the filters is as follows: blue is WFPC2 $U$, green is
H$\alpha$ + $V$, and red is [S~II] + $I$.  Thus, the hot stars are blue,
high-excitation gas exposed directly to the hot stars is green, 
low-excitation gas shielded from direct sightlines to the hot 
stars is red, and the interfaces between the high-excitation 
cavity and surrounding molecular clouds show as yellow.  The dense
core of the ionizing cluster, Radcliffe~136, is below center.  The older
cluster with red supergiants at upper right is Hodge~301, analyzed in
these images from their HST program by Grebel \& Chu (2000).  Figure~1
serves double duty as a chart locating seven subfields to be discussed
in subsequent sections: the PC fields of Knots~1--3, NICMOS fields 15 and
16, and two smaller fields containing the older O-type multiple systems
measured spectroscopically and photometrically.

It is now well established that 30~Doradus is (at least) a two-stage
starburst:  the central cluster has an age of about 2~Myr, while there is
a younger, evidently triggered second stellar generation less than 1~Myr
old developing along the surrounding cavity interface (Walborn \& Parker 
1992; Rubio et~al.\ 1992; Hyland et~al.\ 1992; Parker \& Garmany 1993; 
Walborn \& Blades 1997; Rubio et~al.\ 1998; Walborn et~al.\ 1999a; 
Brandner et~al.\ 2001).  Attributes of the new generation include 
massive young stellar systems in dense nebular knots, dust pillars 
oriented toward the central cluster, infrared sources often within or 
near the pillars, and jets associated with several IR sources.  Some of
these features are visible in Fig.~1 and several will be discussed at a 
larger scale below.  The remanent molecular material is concentrated to 
the northeast and southwest of the central cluster (Werner et~al.\ 1978; 
Rubio et~al.\ 1998; Johansson et~al.\ 1998), beyond the bright interfaces 
in those directions. 

Figure~1 reveals the full extent of the 30~Doradus interface.  Its
projected distance from the cluster core ranges from about 10 to 20~pc. 
It is more extended to the north, following the diffuse extension 
of the ionizing cluster in that direction.  On the other hand, the 
east-west asymmetry may be due to a lower ambient density in the 
former direction.  It is noteworthy that the interface and molecular 
material lie predominantly in one hemisphere relative to the cluster 
core.  That morphology is ubiquitous among starbursts on this scale 
(Walborn 2002), suggesting that the initial burst is triggered near
the surface of the original giant molecular cloud by an external event, 
rather than by a collapse of the cloud toward its center.  The next
evolutionary phase of 30~Doradus will be a giant shell H~II region, with
an evolved central association in a completely evacuated cavity, and with 
the nebulosity and early O stars around the periphery, as in Henize~N11, 
the second-ranked H~II region of the Large Magellanic Cloud (Parker et~al.\
1992; Walborn \& Parker 1992; Walborn et~al.\ 1999b; Heydari-Malayeri et~al.\ 
2000).  The projected radius of the N11 cavity is 30 to 40~pc; its
central association is 3.5~Myr old and has produced many supernovae,
whereas there may not have been any yet in the core of 30~Dor, because the 
most massive stars are still there.  The energetics of N11 has been modeled
by Meaburn et~al.\ (1989) and Rosado et~al.\ (1996).  Thus, the 30~Dor
cavity and second stellar generation are still under construction, being
primarily products of the stellar winds from the central cluster;
ultimately they will become substantially more extensive than at present,
once the imminent supernovae have added their contribution.

In further analysis underway with M.~Rubio, the structural information 
from Fig.~1 will be combined with new H$_2$ and CO data, including velocity 
information, to develop an improved three-dimensional physical model of 
30~Doradus. 

\subsection{The Fields of Knots 1--3}

The objects called Knots~1--2 were identified as very young O~stars 
within dense nebular condensations in the filaments northeast of R136 by
Walborn \& Blades (1987); Knot~3 in the filament west of R136 was added
by Walborn (1991).  It was suggested then that these objects represented
ongoing star formation in 30~Doradus.  Of course, it is these ``filaments'' 
in groundbased images that have been revealed by WFPC2 as the interfaces 
between the central cavity and surrounding molecular clouds. 
Figures~2--4 display the dithered PC images with 30~milliarcsec
resolution of Knots~1--3, respectively.  In each of these figures, the
left panel shows [O~III] in green and H$\alpha$ in red, while the right
panel is [O~III] green plus [S~II] red; the two filter combinations
reveal rather different aspects of the nebular structures in these regions.
NICMOS $JHK$ composite images of these fields were compared with lower
resolution WFPC2 data by Walborn et~al.\ (1999a); at that time, only
continuum images of Knots~1--2 were available from WFPC2.

The new images of Knot~1 (Fig.~2) provide higher definition of the nebular
structures and the newborn, massive Trapezium system including the stars
Parker (1993) P1201 and P1222 (which are identified and further discussed
in Section~4.4.1 below).  As discussed by Walborn et~al.\ (1999a), the 
stellar system has just blown off the summit of its natal pillar,
oriented toward R136, creating a celestial facsimile of Mount St.\ Helens.
The [O~III] + H$\alpha$ representation shows clearly that the third
component of the system is redder than the others and appears to have a
red nebular halo, indicating that it is still more deeply embedded in the
dust cloud than its two brighter companions.  The [O~III] + [S~II] frame
shows well which nebular structures in the region are of lower and/or
collisional ionization.  Walborn et~al.\ (1999a) also show a rich cluster
of faint IR stars associated with the Knot~1 Trapezium; two very luminous
IR sources embedded in the adjacent, intact pillar to the east of Knot~1; 
and a faint, very red IR source within the easternmost of the three dark
globules north of Knot~1.  Rubio et~al.\ (1998) and Johansson et~al.\ (1998)
chart massive molecular concentrations just north of these pillars,
opposite to the direction of R136; that is, these structures and the new
stars they contain have likely been formed on the side of the cloud facing 
R136 by the energetic stellar outflows from the latter.

The images of Knot~2 in Fig.~3 again reveal further intricacy of the nebular
structures.  The brightest optical star in the knot is P1429A, just below
and left of center in the frames; it turns out to be of very early
spectral type (Section~4.4.1 below).  A primary motivation of these
observations was to search for optical structures related to a stellar
jet in Knot~2, inferred from two extended IR sources oppositely aligned
across the stellar system (Walborn et~al.\ 1999a).  However, no features
associated with the nonstellar sources or the presumed linear jet appear
in these images.  This field contains an H$_2$O maser for which an
accurate position has recently been determined (Lazendic et~al.\ 2002); it
does not coincide exactly with any of the IR sources, but is nearest to a
faint optical star (cf.\ Rubio et~al.\ 1998).

Fig.~4 displays the new PC images of the field of Knot~3, which contains
a remarkable array of stellar and nebular structures related to current
star formation; they have been discussed in some detail by Walborn et~al.\
(1999a), but are seen with improved clarity here.  Knot~3 is the bright
nebular patch below center, within which the two optical components of
P409 (Section~4.4.1 below) can be seen.  The two pillars above it,
oriented in the general direction of R136, are of outstanding interest.
The bright-rimmed one contains a faint optical star within its head,
which is one of the brightest stellar IR sources in 30~Dor.  The adjacent
dark pillar is highly reminiscent of the Orion Horsehead Nebula at this
resolution.  The characteristics of the 30~Dor pillars and others are
intercompared by Walborn (2002); see also Scowen et~al.\ (1998).  The other 
major molecular concentration in 30~Dor lies beyond these objects with 
respect to R136 (Rubio et~al.\ 1998; Johansson et~al.\ 1998), so the basic 
physical structure of this region is entirely analogous to that of Knot~1.

\subsection{The Fields of NIC15--16}

Hyland et~al.\ (1992) discovered four luminous protostars (P1--4) in 
30~Doradus, which not surprisingly turn out to be the brightest of the 
numerous stellar IR sources found there with subsequent instrumentation.  
Their P1 is located in the pillar adjacent to Knot~1 and was resolved
into two bright sources by Rubio et~al.\ (1998; IRSN-122/126), Walborn et~al.\ 
(1999a), and Brandner et~al.\ (2001).  P3 (IRSW-30 in the subsequent
references) is the source in the head of the bright-rimmed pillar just
north of Knot~3.  P2 (not observed by Rubio et~al.\ 1998) and P4
(IRSN-134/137) were also observed in our NICMOS program and have been 
measured by Brandner et~al.\ (2001; the NICMOS field numbers are defined in 
that paper), but they are located further north of R136 than the other sources 
(Fig.~1) and were not covered by the previous WFPC2 data.  Our new WFPC2 
fields do include them, so they are compared with the NICMOS images here
in Figures 5 and 6, in each of which the left panel displays WFPC2 F336W, 
F555W, and F814W (approximately $U$, $V$, and $I$) as blue, green, and
red, respectively, and the right panel NICMOS $J$, $H$, and $K$ analogously. 

The images of P4 in field NIC15, displayed in Fig.~5, show that it is a
small, heavily embedded cluster, the brighter members of which can be
seen in the optical image.  We have measured an F555W magnitude of 21.12 
and F814W of 19.60 for the brightest star in the cluster, centered in the
NICMOS image.  Brandner et~al.\ (2001) measured NICMOS $J$ of 17.06, $H$
of 15.24, and $K$ of 13.48 for this star, in good agreement with the
groundbased values of Rubio et~al.\ (1998) for IRSN-137.  It will be of
some interest to measure and analyze the entire cluster in these images.  
    
In striking contrast, P2 in NIC16, Fig.~6, is completely unresolved in
the HST images.  It is undetected in WFPC2 F555W, implying an upper limit
of 23--24~mag, but we have measured it at 20.91 in F814W; it is clearly
visible as a very red source in the left panel of Fig.~6.  From the
NICMOS image, Brandner et~al.\ (2001) measured $J$ of 15.38, $H$ of 13.27,
and $K$ of 11.71 for this star, the latter value similar to those for P3
and the brighter component of P1.  It should be recalled that at the distance 
of the LMC, 0\farcs1 subtends 5000~AU, but at face value the HST images of 
P2 and P4 imply two qualitatively different modes of massive star formation: 
fragmentation into a cluster and a monolithic object, respectively.   

\subsection{O-Type Multiple Systems}

The spatially resolved STIS spectrograms of seven close visual binaries
in 30~Doradus are displayed in Figures~7 and~8, the former containing the
systems in Knots~1--3, and the latter four systems believed to correspond
to the somewhat older first stellar generation.  The spectral
classifications of the components derived from these data, and a
photometric analysis of each, are listed in Table~3.  Successive columns
give the stellar identification from Parker (1993); the spectral type;
the WFPC2 F555W magnitude and F336W$-$F555W, F336W$-$F814W colors
measured here; $E_{B-V}$ derived from F336W$-$F555W according to the
intrinsic colors and relation given by Massey \& Hunter (1998);\footnote{The 
color excesses derived similarly from F336W$-$F814W were twice or more as
large and were not used.} the absolute visual magnitude $M_V$ derived 
following Massey \& Hunter, but with $V_0 - M_V = 18.6$ and $R_V = 3.0$;    
the calibration $M_V$ for the spectral type from Walborn (1973); the
difference between the two absolute magnitudes, in the sense observed
minus calibration; and a stellar mass estimated from the evolutionary 
calibration of Vacca, Garmany, \& Shull (1996), by linear scaling according 
to the visual-luminosity difference at the appropriate spectral type.  The 
results for each system will be discussed below in turn, where WFPC2 charts, 
a table of WFPC2 photometry for all stars down to F555W magnitude $\sim20.5$ 
in a 12\arcsec\ square field containing the multiple system (from which the 
values in Table~3 are extracted), and color-magnitude diagrams (CMDs) will 
also be presented for each.  (The CMDs contain fainter stars than the
tables, which will be listed and fully discussed by Barb\'a et~al., in
preparation.)


\subsubsection{Knots 1--3}

The spectroscopic and photometric results for these three very young stellar
systems are listed in the first part of Table~3, where it can be seen that 
most of the components are subluminous relative to the calibration,
consistent with extreme youth.  On the other hand, it is also possible
that an abnormally high value of $R_V$ applies in these regions, in which
case the derived $M_V$'s would become brighter.  This possibility will be
investigated in future analyses combining the optical and IR (Brandner et~al.\ 
2001) photometry.  The very small masses derived for some of these
stars (Table~3) are probably unrealistic, indicating either that the
linear scaling by visual luminosity is inappropriate over such large
ranges, or that in fact $R_V$ is larger than 3.0.  (In addition, the
spectral type of P1429B is uncertain, as further noted below.)

Charts for the field of P409 in Knot~3 are given in Figure~9 (see also
Fig.~4), the photometry in Table~4, and the CMDs in Figure~10.  The two
classified optical components are of similar late-O types, although the
combined light had been given an early-O classification from groundbased
data by Walborn \& Blades (1997); the nebular emission-line contamination is 
of course strongly suppressed by the HST spatial resolution.  P409C (Star~2C 
in Table~4) is the IR component found by Walborn et~al.\ (1999a).  Star~1
is P467; while Star~3 is P454 and Rubio et~al.\ (1998) IRSW-46, another IR 
source.  The CMDs indicate that there is a coeval cluster with three very red 
objects in this field, further analysis of which will likely prove rewarding.

The field of P1201 and P1222 in Knot~1 (Fig.~2; the Mount St.\ Helens
pillar) is shown in Figure~11, the photometry is listed in Table~5, and
CMDs are shown in Figure~12.  Again, both classified components are of
late-O types.  However, the spectrum of P1222 appears peculiar, in that all
observed He lines are of similar intensity; it has been classified as O9
on the basis of He~II~$\lambda4541 \sim$~He~I~$\lambda4387$ and
He~II~$\lambda4200 \sim$~He~I~$\lambda4144$, although He~I~$\lambda4471$
should be relatively much stronger at that type.  But the strengths of the 
weaker He~I lines rule out an earlier type.  This effect is possibly due to 
residual nebular emission-line filling at the stronger He~I lines.  Star~10 
is the third brightest, redder component of the multiple system (Fig.~2).  
Star~3 is P1164 and Star~4 is P1170, classified O3--6~V by Walborn \& Blades 
(1997); note, however, that P1222 had also been given that type from the
groundbased data, similarly to P409 discussed in the previous paragraph.
The CMDs again suggest a physical cluster, without any very red objects
in this case.

P1429 in Knot~2 (Fig.~3) and its surroundings are charted in Figure~13,
photometry is given in Table~6, and the CMDs in Figure~14.  Fortunately,
the early-O spectral type of Walborn \& Blades (1997) is confirmed by the
much higher quality STIS data!  The spectral type of P1429B (Star~4,
which includes the even fainter, red third component shown by Walborn et~al.\ 
1999a) is very uncertain, since it is derived from only a low-resolution 
(G430L), low-S/N observation.  The derived $M_V$ would correspond to a normal 
B2.5~V star on the main sequence (Walborn 1972), which would still have a 
much higher mass than shown in Table~3.  Star~2 is IRSN-138 and Star~3 is
ISRN-133 (Rubio et~al.\ 1998).  The CMDs may correspond to a cluster with 
many red, embedded objects, but further investigation is required.    

\subsubsection{First-Generation Systems}

The spectroscopic and photometric results for these four systems are
listed in the latter part of Table~3.  As expected from their locations,
the derived absolute magnitudes and masses are fairly reasonable for the
spectral types, consistent with first-generation stars, except for the
vignetted stars P1304/P1306, further commented upon below.

P294 and P304 are the brightest members of a small, anonymous cluster at 
the northern fringe of the extended ionizing association (Fig.~1); it lies 
beyond the interface, but must be in front of the molecular cloud from the 
relatively low reddenings (Table~3), the lowest in the present spectroscopic 
sample.  Charts are given in Figure~15, photometry in Table~7, and CMDs in 
Figure~16.  The spectral types are mid- and late-O, respectively; the
relative magnitudes are opposite to what the spectral types predict,
suggesting the possibility that P304 may be composite.  P304, but likely 
the combined light of both stars (separation 0\farcs65; Table~1), was 
classified O8--8.5~V by Walborn \& Blades (1997), which falls nicely between 
the spatially resolved types; such agreement is expected when nebular 
emission-line contamination is low.  Star~4 is P280.  The CMDs show a
very well defined main sequence, as might be expected for a compact,
isolated cluster with little differential extinction.

The multiple systems P1231, P1304/P1306, and P1312 all lie in the same
12\arcsec\ square field (Fig.~1), so they are shown together in the charts
of Figure~17; but an additional, short-exposure UV image is displayed in
Figure~18, to show the very close pairs P1231AB (0\farcs09; Table~1) and 
P1312AB (0\farcs12) resolved.  Photometry for the whole field is listed
in Table~8 and the CMDs are shown in Figure~19.  The spectral types are
in the O5--O8 range; some profiles in the spectrum of P1231A suggest
double lines, but further observations would be required to confirm that
interpretation.  The derived absolute magnitudes of P1304 and P1306 are both 
1.1~mag fainter than the calibration values, which is not expected from 
their spectral types, e.g., a giant luminosity class for P1306 (based on the
apparent weakening of He~II~$\lambda4686$ absorption relative to the other 
He lines; Fig.~8).  However, these two stars are in the vignetted region
of WFPC2 chip~2, as discussed above, and their derived magnitudes are
likely too faint by at least 0.4~mag.  Parker (1993) gives substantially
brighter magnitudes for these stars, but they are denoted as very uncertain 
in his thesis, presumably because of mutual blending.  Walborn \& Blades (1997) 
classified P1306 (actually the combined light with P1304, separation 0\farcs47) 
as O8~III, and P1312AB as O7~V, in fair and excellent agreement with the STIS 
results, respectively.  Star~1 is P1253, classified BN0.5~Ia by Walborn \& 
Blades (1997).  Stars~4--7 are P1320, P1281, P1248, and P1225, respectively, 
and there are a number of fainter Parker stars in this field, but none
has spectroscopic information to date.  The CMDs reveal a perhaps surprisingly 
tight cluster sequence, given that this is an arbitrary subfield of the
ionizing cluster ``halo'' (Fig.~1).  That result is consistent with the
stars being a coeval sample of the first stellar generation, although
P1253 belongs to an older subpopulation in the field according to the
analysis of Walborn \& Blades (1997).  


\section{Summary and Outlook}

New HST observations of 30~Doradus, consisting of WFPC2 images and STIS
long-slit, optical spectroscopy, have been described.  The unifying theme
is the intricacy of both nebular and stellar structures in this region,
at the spatial resolution of HST.  A WFPC2 mosaic of the inner nebula 
reveals its entire structure, including the full extent of the interface 
between the incipient wind-blown, central cavity and the surrounding 
molecular clouds, with 0\farcs1 resolution.  Particular emphasis has been
given to new information about both nebular structures and young stellar 
multiple systems in the fields of Knots~1-3, representative of the second,
triggered generation, obtained from PC images with even higher resolution 
and from STIS spectroscopy, respectively.  New WFPC2 coverage of the fields 
of two luminous IR sources previously observed with NICMOS has been compared 
with the IR images.  Finally, detailed spectroscopic information from STIS 
about four additional stellar multiple systems belonging to the first 
generation has been presented.  These data provide valuable insights into      
both the overall structure of 30~Doradus and several subregions of special 
interest, which will be enhanced by planned further analyses that have been 
mentioned throughout the discussion.  Eventually, complete photometric
studies of both the optical and IR images from HST will be combined with 
available stellar spectroscopic and nebular molecular data to characterize 
the complex stellar populations of 30~Doradus as well as their environment.
The HST data will endow this enterprise with higher precision than would be 
feasible from groundbased observations alone.   


\acknowledgments
Support for this work was provided by NASA through grant GO-8163.01-97 
from the Space Telescope Science Institute, which is operated by AURA, 
Inc., under contract NAS5-26555.  RHB also acknowledges hospitality 
and support from the ST~ScI collaborative visitor program, and financial
support from Fundaci\'on Antorchas, Argentina (Project No.~13783-5).


\begin{references}
\reference{} Anderson, J.\ \& King, I.~R. 1999, \pasp, 111, 1095
\reference{} Biretta, J.~A.\ et~al. 2000, WFPC2 Instrument Handbook,
   Version 5.0 (Baltimore: ST~ScI)
\reference{} Brandner, W., Grebel, E.~K., Barb\'a, R.~H., Walborn, N.~R., \&
   Moneti, A. 2001, \aj, 122, 858
\reference{} de Koter, A., Heap, S.~R., \& Hubeny, I. 1997, \apj, 477, 792 
\reference{} ----- 1998, \apj, 509, 879
\reference{} Dolphin, A.~E. 2000a, \pasp, 112, 1383
\reference{} ----- 2000b, \pasp, 112, 1397\newpage
\reference{} Grebel, E.~K., \& Chu, Y.-H. 2000, \aj, 119, 787
\reference{} Heydari-Malayeri, M., Royer, P., Rauw, G., \& Walborn, N.~R. 2000,
   \aap, 361, 877
\reference{} Holtzman, J.~A.\ et~al. 1995, \pasp, 107, 156   
\reference{} Hunter, D.~A., O'Neil, E.~J., Jr., Lynds, R., Shaya, E.~J.,
   Groth, E.~J., \& Holtzman, J.~A. 1996, \apj, 459, L27
\reference{} Hunter, D.~A., Shaya, E.~J., Holtzman, J.~A., Light, R.~M.,
   O'Neil, E.~J., Jr., \& Lynds, R. 1995a, \apj, 448, 179
\reference{} Hunter, D.~A., Shaya, E.~J., Scowen, P., Hester, J.~J.,
   Groth, E.~J., Lynds, R., \& O'Neil, E.~J., Jr. 1995b, \apj, 444, 758
\reference{} Hunter, D.~A., Vacca, W.~D., Massey, P., Lynds, R., \& 
   O'Neil, E.~J. 1997, \aj, 113, 1691
\reference{} Hyland, A.~R., Straw, S., Jones, T.~J., \& Gatley, I. 1992,
   \mnras, 257, 391   
\reference{} Johansson, L.~E.~B.\ et~al. 1998, \aap, 331, 857
\reference{} Koekemoer, A.\ et~al. 2000, HST Dither Handbook, Version 1.0
   (Baltimore: ST~ScI)
\reference{} Krist, J. 1995, in ASP Conf.\ Ser.~77, Astronomical Data
   Analysis Software and Systems IV, eds.\ R.~A.\ Shaw, H.~E.\ Payne, \& 
   J.~J.~E.\ Hayes (San Francisco: ASP), 349   
\reference{} Lazendic, J.~S., Whiteoak, J.~B., Klamer, I., Harbison, P.~D., 
   \& Kuiper, T.~B.~H. 2002, \mnras, 331, 969
\reference{} MacKenty, J.~W., Ma\'{\i}z-Apell\'aniz, J., Pickens, C.~E.,
   Norman, C.~A., \& Walborn, N.~R. 2000, \aj, 120, 3007
\reference{} Massey, P.\ \& Hunter, D.~A. 1998, \apj, 493, 180
\reference{} Meaburn, J., Solomos, N., Laspias, V., \& Goudis, C. 1989, 
   \aap, 225, 497 
\reference{} Parker, J.~Wm. 1993, \aj, 106, 560
\reference{} Parker, J.~Wm., Clayton, G.~C., Winge, C., \& Conti, P.~S. 1993,
   \apj, 409, 770 
\reference{} Parker, J.~Wm.\ \& Garmany, C.~D. 1993, \aj, 106, 1471
\reference{} Parker, J.~Wm., Garmany, C.~D., Massey, P., \& Walborn, N.~R. 1992,
   \aj, 103, 1205
\reference{} Parker, J.~Wm., Heap, S.~R., \& Malumuth, E.~M. 1995, \apj, 448, 705 
\reference{} Rosado, M.\ et al. 1996, \aap, 308, 588
\reference{} Rubio, M., Barb\'a, R.~H., Walborn, N.~R., Probst, R.~G.,
   Garc\'{\i}a, J., \& Roth, M.~R. 1998, \aj, 116, 1708
\reference{} Rubio, M., Roth, M., \& Garc\'{\i}a, J. 1992, \aap, 261, L29
\reference{} Scowen, P.~A. et~al. 1998, \aj, 116, 163
\reference{} Shaklan, S., Sharman, M.~C., \& Pravdo, S.~H. 1995, Appl.\ Opt., 
   34, 6672
\reference{} Sirianni, M., Nota, A., Leitherer, C., De~Marchi, G., \& 
   Clampin, M. 2000, \apj, 533, 203
\reference{} Stetson, P.~B. 1987, \pasp, 99, 191   
\reference{} Vacca, W.~D., Garmany, C.~D., \& Shull, J.~M. 1996, \apj, 460, 914
\reference{} Walborn, N.~R. 1972, \aj, 77, 312
\reference{} ----- 1973, \aj, 78, 1067
\reference{} ----- 1991, in ST~ScI Symp.~5, Massive Stars in Starbursts, 
   eds.\ C.~Leitherer, N.~R.\ Walborn, T.~M.\ Heckman, \& C.~A.\ Norman 
   (Cambridge: CUP), 145
\reference{} ----- 2002, in ASP Conf.\ Ser.~267, Hot Star Workshop III: 
   The Earliest Stages of Massive Star Birth, ed.\ P.~A.\ Crowther 
   (San Francisco: ASP), 111
\reference{} Walborn, N.~R. et~al. 2002, \aj, 123, 2754
\reference{} Walborn, N.~R., Barb\'a, R.~H., Brandner, W., Rubio, M., 
   Grebel, E.~K., \& Probst, R.~G. 1999a, \aj, 117, 225
\reference{} Walborn, N.~R.\ \& Blades, J.~C. 1987, \apj, 323, L65
\reference{} ----- 1997, \apjs, 112, 457
\reference{} Walborn, N.~R., Drissen, L., Parker, J.~Wm., Saha, A.,
   MacKenty, J.~W., \& White, R.~L. 1999b, \aj, 118, 1684
\reference{} Walborn, N.~R.\ \& Parker, J.~Wm. 1992, \apj, 399, L87
\reference{} Werner, M.~W., Becklin, E.~E., Gatley, I., Ellis, M.~J., 
   Hyland, A.~R., Robinson, G., \& Thomas, J.~A. 1978, \mnras, 184, 365
\end{references}

\newpage

\begin{figure}%1 17x26cm
\centering
\includegraphics[height=20.8cm,width=13.6cm]{fig1.ps}
\caption{
Mosaic of WFPC2 images of 30~Doradus.  Blue is WFPC2 $U$, green is
H$\alpha$ + $V$, and red is [S~II] + $I$.  The bright yellow features are
the interfaces between the central cavity and surrounding molecular clouds.  
Pure black spaces are lacking nebular-line or continuum coverage, or both.  
The large white boxes labeled K1--K3 are the 33\arcsec\ square PC fields of 
Knots~1--3.  The intermediate boxes labeled N15, N16 are 19\arcsec\ square 
NICMOS fields.  The two small boxes are 12\arcsec\ square and contain 
multiple stellar systems studied here; the P294/P304 system is to the
north, while the southern field contains P1231, P1304/P1306, and P1312.
\label{fig1}}
\end{figure}

\begin{landscape}
\begin{figure}
\includegraphics[height=9in,angle=90]{fig2.ps}
\caption{
Dithered PC images of Knot~1.  In the left panel, green is [O~III] and
red is H$\alpha$, while at right green is [O~III] and red is [S~II].  
See the text for discussion.
\label{fig2}}
\end{figure}

\begin{figure}%3
\includegraphics[height=9in,angle=90]{fig3.ps}
\caption{
As Fig.~2 for Knot~2.
\label{fig3}}
\end{figure}

\begin{figure}%4
\includegraphics[height=9in,angle=90]{fig4.ps}
\caption{
As Fig.~2 for Knot~3.
\label{fig4}}
\end{figure}

\begin{figure}%5
\includegraphics[height=9in,angle=90]{fig5.ps}
\caption{
Images of the IR cluster P4 in field NIC15.  {\it Left panel\/}, WFPC2 
$U$, $V$, $I$ in blue, green, red, respectively.  {\it Right panel\/},
NICMOS $J$, $H$, $K$, analogously.  See the text for discussion.
\label{fig5}}
\end{figure}

\begin{figure}%6
\includegraphics[height=9in,angle=90]{fig6.ps}
\caption{
As Fig.~5 for the unresolved IR source P2 in field NIC16.
\label{fig6}}
\end{figure}
\end{landscape}

\begin{figure}%7
\includegraphics[width=\textwidth]{fig7.ps}
\caption{
Rectified, blue-violet, spatially resolved STIS spectrograms of the
brightest components in the Knots~1--3 multiple stellar systems.  In the
top three spectrograms, the 4310--4590~\AA\ region in the G430L data has
been replaced by the G430M observations.  The bottom two spectrograms
are entirely G430M data.  The G430L data have been smoothed by 3~pixels,
and the G430M by 11.  The absorption lines identified in the spectrum of
P1429A are Ca~II $\lambda$3933 (interstellar) and He~I~+~II $\lambda$4026,   
while at bottom they are He~I $\lambda\lambda$4121, 4144, 4387, 4471 and
He~II $\lambda\lambda$4200, 4541, 4686.
\label{fig7}}
\end{figure}

\begin{figure}%8
\includegraphics[width=\textwidth]{fig8.ps}
\caption{
As Fig.~7 for the brightest pairs in four older multiple systems.  All data 
are G430M, smoothed by 11~pixels.  The absorption lines identified at bottom 
are as in Fig.~7, with the addition of C~III $\lambda\lambda$4070, 4650 blends 
in P304, and N~III $\lambda\lambda$4634, 4640-42 emission lines in P1304.
\label{fig8}}
\end{figure}

\begin{figure}%9
\includegraphics[width=\textwidth]{fig9.ps}
\caption{
Charts of a 12\arcsec\ square field surrounding P409 in Knot~3; the scales 
are in WFC pixels (0\farcs1~pixel$^{-1}$).  An F555W image from HST 
program No.~5589 is shown at left and the corresponding contour diagram at 
right; a compass in the latter indicates N, E.  Star~2 is P409; the two 
nearly equal optical components are barely resolved in the image.
\label{fig9}}
\end{figure}

\begin{figure}%10  15cm x 22.5cm
\centering
\includegraphics[width=10.5cm,height=15.75cm,angle=-90]{fig10.ps}
\caption{
Color-magnitude diagrams of the Knot~3 field.  The two optical and the
infrared components of P409 are plotted with star symbols.
\label{fig10}}
\end{figure}

\begin{figure}%11
\includegraphics[width=\textwidth]{fig11.ps}
\caption{
Charts of the field of Knot~1 from program No.~5114, as Fig.~9.  Star~1 
is P1222 and Star~2 is P1201.   
\label{fig11}}
\end{figure}

\begin{figure}%12
\centering
\includegraphics[width=10.5cm,height=15.75cm,angle=-90]{fig12.ps}
\caption{
Color-magnitude diagrams of the Knot~1 field.  P1222 and P1201
are plotted with star symbols.  
\label{fig12}}
\end{figure}

\begin{figure}%13
\includegraphics[width=\textwidth]{fig13.ps}
\caption{
Charts of the field of Knot~2 from program No.~5114, as Fig.~9.  Stars~1 
and 4 are P1429A and B, respectively.
\label{fig13}}
\end{figure}

\begin{figure}%14
\centering
\includegraphics[width=10.5cm,height=15.75cm,angle=-90]{fig14.ps}
\caption{
Color-magnitude diagrams of the Knot~2 field.  P1429A and B are plotted
with star symbols.  
\label{fig14}}
\end{figure}

\begin{figure}%15
\includegraphics[width=\textwidth]{fig15.ps}
\caption{
Charts of the field of P304/P294 from program No.~6122, as Fig.~9. Star~1
is P304 and Star~2 is P294.  
\label{fig15}}
\end{figure}

\begin{figure}%16
\centering
\includegraphics[width=10.5cm,height=15.75cm,angle=-90]{fig16.ps}
\caption{
Color-magnitude diagrams of the P304/P294 field.  P304 and P294 are
plotted with star symbols.
\label{fig16}}
\end{figure}

\clearpage

\begin{figure}%17
\includegraphics[width=\textwidth]{fig17.ps}
\caption{
Charts of the field of P1231, P1304/P1306, and P1312 from program No.~5114, 
as Fig.~9.  Star~2 is P1231; Star~3 is P1312; and Stars~8/9 are P1306/P1304, 
respectively.
\label{fig17}}
\end{figure}

\begin{figure}%18
\includegraphics[width=\textwidth]{fig18.ps}
\caption{
Short-exposure (300~s), 3680~\AA\ medium-band continuum images from program 
No.~2886, showing the components of P1231AB (barely) and P1312AB resolved.  
This image is from the aberrated PC~I (filter F368M); it has not been 
deconvolved, but the cores of the PSF reveal the multiple systems.  Here
the pixels are 0\farcs044 and each panel is 2\farcs6 square.
\label{fig18}}
\end{figure}

\begin{figure}%19
\centering
\includegraphics[width=10.5cm,height=15.75cm,angle=-90]{fig19.ps}
\caption{
Color-magnitude diagrams of the P1231, P1304/P1306, P1312 field. 
{\it Stars}, P1231AB; {\it filled triangles}, P1312AB; 
{\it filled circles}, P1304/P1306. 
\label{fig19}}
\end{figure}
\begin{deluxetable}{lrlcc}
\tablewidth{0pt}
\tablenum{1}
\tablecaption{WFPC2 Observations}
\tablehead{
\colhead{Field} &\colhead{RA/Dec} &\colhead{Date} &\colhead{Filters} &\colhead{Exposure}\\
                &\colhead{(2000)} &               &                  &\colhead{Times [s]}
}
\startdata            
Knot 1      &5 38 52    &2000 Sept 21    &F502N    &$2 \times 500$\\
        &$-$69 05 18    &                &F656N    &$2 \times 400$\\
        &               &                &F673N    &$4 \times 500$\\
\\                                       
Knot 2      &5 38 43    &2000 Apr  21    &F502N    &$2 \times 500$\\
        &$-$69 04 24    &                &F656N    &$2 \times 400$\\
        &               &                &F673N    &$4 \times 500$\\
\\                                       
Knot 3      &5 38 28    &2000 Mar  29    &F502N    &$2 \times 500$\\
        &$-$69 05 57    &                &F656N    &$2 \times 400$\\
        &               &                &F673N    &$4 \times 500$\\
\\                                       
North       &5 38 39    &1999 Oct  5     &F336W       &10 + 80\\
        &$-$69 04 39    &                &F555W       &\phn3 + 80\\
        &               &                &F814W       &\phn5 + 80\\
\\                                       
South       &5 38 50    &1999 Oct  4     &F336W       &10 + 80\\
        &$-$69 07 50    &                &F555W       &\phn3 + 80\\
        &               &                &F814W       &\phn5 + 80
\enddata
\end{deluxetable}


\begin{deluxetable}{lrcrlccc}
\tablenum{2}
\tablewidth{0pt}
\tablecaption{STIS Observations}
\tablehead{
\colhead{Star} &\colhead{RA/Dec} &\colhead{Sep} &\colhead{PA} &\colhead{Date} 
&\colhead{Wavelength\tablenotemark{a}} &\colhead{Exposure} &\colhead{S/N}\\               &\colhead{(2000)} &\colhead{[\arcsec]} &\colhead{[$^\circ$]} &&\colhead{[\AA]}
&\colhead{Time [s]}
}
\startdata          
P409AB    &5 38 34    &0.16      &60     &1999 Oct 20   &4300        &2588   &112/100\\ 
      &$-$69 06 04    &          &       &              &4451        &3088    &40/36\\
\\        
P1222     &5 38 45    &1.18     &309     &2000 May 23   &4194        &\phn650  &39/30\\
/1201 &$-$69 05 09    &         &        &              &4451        &\phn650  &39/30\\
      &               &         &        &              &4706        &\phn740  &40/30\\
\\                                                    
P1429AB   &5 38 48    &0.30     &286     &2000 May 21   &4300        &1070   &110/39\phn\\
      &$-$69 04 43    &         &        &              &4451        &1224    &37/15\\
\\        
P304      &5 38 33    &0.65     &301     &2000 May 25   &3936        &\phn428 &48/38\\
/294  &$-$69 04 32    &         &        &              &4194        &\phn432 &48/39\\
      &               &         &        &              &4451        &\phn432 &47/38\\
      &               &         &        &              &4706        &\phn480 &47/37\\
\\
P1231AB   &5 38 45    &0.09      &55     &1999 Oct 13   &3936        &\phn430 &46/45\\
      &$-$69 05 47    &          &       &              &4194        &\phn430 &46/45\\
      &               &          &       &              &4451        &\phn430 &45/44\\
      &               &          &       &              &4706        &\phn482 &46/45\\
\\
P1306     &5 38 46    &0.47     &189     &2000 Feb  2   &4194        &\phn650 &40/38\\
/1304 &$-$69 05 55    &         &        &              &4451        &\phn650 &39/38\\
      &               &         &        &              &4706        &\phn740 &40/39\\
\\
P1312AB   &5 38 46    &0.12     &64      &1999 Oct 13   &3936        &\phn420 &37/37\\
      &$-$69 05 52    &         &        &              &4194        &\phn420 &37/37\\
      &               &         &        &              &4451        &\phn410 &35/35\\
      &               &         &        &              &4706        &\phn520 &38/38
\enddata
\tablenotetext{a}{The central wavelength of G430L is 4300~\AA; other central wavelengths are G430M settings.}
\end{deluxetable}

\begin{landscape}
\begin{deluxetable}{lccccccccc}
\tablenum{3}
\tablewidth{0pt}
\tablecaption{Stellar Parameters}
\tablehead{
\colhead{Star} &\colhead{Spectral} &\colhead{m(F555W)} &\colhead{F336W--F555W} 
&\colhead{F336W--F814W} &\colhead{$E_{B-V}$} &\colhead{$M_V$} &\colhead{$M_{V,cal}$} 
&\colhead{$\Delta M_V$} &\colhead{$M/M_{\sun}$}\\
&\colhead{Type}
}
\startdata
P409A   &O8.5 V      &17.05      &$-$0.70       &$-$0.23      &0.54    &$-$3.3  &$-$4.4       &+1.1         &\phn9\\
P409B   &O9 V        &17.08      &$-$0.91       &$-$0.51      &0.43    &$-$2.9  &$-$4.3       &+1.4         &\phn6\\
\\
P1201   &O9.5 V      &15.83      &$-$1.28       &$-$0.97      &0.25    &$-$3.6  &$-$4.1       &+0.5        &12\\
P1222   &O9 V(n)p    &15.11      &$-$1.13       &$-$0.85      &0.32    &$-$4.5  &$-$4.3     &$-$0.2        &27\\
\\
P1429A  &O3-4 V      &15.88      &$-$1.08       &$-$0.47      &0.39    &$-$4.0  &$-$5.5       &+1.5        &17\\
P1429B  &O8: V:      &18.10      &$-$1.14       &$-$0.60      &0.32    &$-$1.55 &$-$4.4\rlap{:}      &+2.85\rlap{:}       &\phn2\rlap{:}\\
\\
P294    &O7.5 V      &14.90      &$-$1.48       &$-$1.35      &0.19    &$-$4.35 &$-$4.8       &+0.45       &23\\
P304    &O9.5 V      &14.47      &$-$1.51       &$-$1.47      &0.14    &$-$4.6  &$-$4.1     &$-$0.5        &30\\
\\
P1231A  &O6 V sb2?   &14.55      &$-$1.35       &$-$1.08      &0.25    &$-$4.9  &$-$5.3       &+0.4        &37\\ 
P1231B  &O7 V        &14.61      &$-$1.37       &$-$1.08      &0.24    &$-$4.8  &$-$4.8        &0.0        &35\\
\\
P1304\tablenotemark{a}   &O5 V((f))   &15.29      &$-$1.20       &$-$0.88      &0.32    &$-$4.4  &$-$5.5       &+1.1        &24\\
P1306\tablenotemark{a}   &O7 III      &15.15      &$-$1.20       &$-$0.80      &0.32    &$-$4.5  &$-$5.6       &+1.1        &16\\
\\
P1312A  &O6.5 V      &14.72      &$-$1.20       &$-$0.93      &0.32    &$-$4.9  &$-$5.3       &+0.4        &38\\
P1312B  &O8 V        &14.84      &$-$1.12       &$-$0.78      &0.33    &$-$4.8  &$-$4.4     &$-$0.4        &35
\enddata
\tablenotetext{a}{Stars located in vignetted region of WFPC2 chip; the
listed brightnesses and masses are underestimates.}
\end{deluxetable}
\end{landscape}

\begin{deluxetable}{lrrcccccc}
\tablenum{4}
\tablewidth{0pt}
\tablecaption{Photometry of stars around P409 (Knot 3)}
\tablehead{
\colhead{Star} &\colhead{X\tablenotemark{a}} &\colhead{Y\tablenotemark{a}} 
& \colhead{F555W} & \colhead{$\sigma$}
& \colhead{F336W--F555W} & \colhead{$\sigma$} &\colhead{F555W--F814W} &
 \colhead{$\sigma$}\\
}
\startdata
\phn1  & 229.2 & 342.0 & 14.66 & 0.01 & $-1.18$    & 0.02    &  0.32 &  0.01\\
\phn2A & 273.0 & 373.2 & 17.05 & 0.05 & $-0.70$    & 0.09    &  0.47 &  0.07\\  
\phn2B & 271.4 & 373.2 & 17.08 & 0.05 & $-0.91$    & 0.08    &  0.40 &  0.07\\
\phn2C & 272.9 & 376.5 & 20.64 & 0.11 & \nodata    & \nodata &  2.07 &  0.11\\
\phn3  & 255.1 & 330.3 & 17.06 & 0.01 &\hphantom{$-$}3.36 & 0.12    &  1.82 &  0.01\\
\phn4  & 254.4 & 434.7 & 18.11 & 0.01 & $-1.01$    & 0.03    &  0.44 &  0.01\\
\phn5  & 309.3 & 374.9 & 18.82 & 0.04 & $-0.81$    & 0.06    &  0.83 &  0.05\\
\phn6  & 273.1 & 331.4 & 18.93 & 0.01 & $-0.63$    & 0.04    &  0.46 &  0.02\\
\phn7  & 219.6 & 367.6 & 19.23 & 0.01 & $-0.81$    & 0.03    &  0.49 &  0.02\\
\phn8  & 332.5 & 320.8 & 19.43 & 0.05 & $-0.58$    & 0.07    &  0.45 &  0.06\\
\phn9  & 309.1 & 326.8 & 19.60 & 0.01 & \nodata    & \nodata &  0.25 &  0.02\\
10  & 227.7 & 367.7 & 19.69 & 0.01 &\hphantom{$-$}0.39 & 0.10    &  0.20 &  0.03\\
11  & 301.9 & 430.7 & 20.03 & 0.04 & $-0.57$    & 0.07    &  0.52 &  0.05\\
12  & 271.4 & 342.2 & 20.18 & 0.02 & $-0.38$    & 0.09    &  0.33 &  0.05\\
13  & 223.9 & 370.4 & 20.34 & 0.05 &\hphantom{$-$}0.04    & 0.16    &  0.13 &  0.09
\enddata
\tablenotetext{a}{Program No.~5589, chip 4}
\end{deluxetable}

\begin{deluxetable}{lrrcccccc}
\tablenum{5}
\tablewidth{0pt}
\tablecaption{Photometry of stars around P1201/P1222 (Knot 1)}
\tablehead{
\colhead{Star} &\colhead{X\tablenotemark{a}} &\colhead{Y\tablenotemark{a}} 
& \colhead{F555W} & \colhead{$\sigma$} 
& \colhead{F336W--F555W} & \colhead{$\sigma$} &\colhead{F555W--F814W} & \colhead{$\sigma$}\\
}
\startdata
\phn1 &  603.3  &	284.1  & 15.11 & 0.01 & $-1.13$ &  0.01 &  0.28  & 0.01\\
\phn2 &  614.7  &	281.2  & 15.83 & 0.01 & $-1.28$ &  0.01 &  0.31  & 0.01\\
\phn3 &  591.7  &	234.4  & 16.20 & 0.01 & $-1.17$ &  0.01 &  0.27  & 0.01\\
\phn4 &  575.7  &	229.4  & 16.27 & 0.01 & $-1.22$ &  0.02 &  0.21  & 0.01\\
\phn5 &  590.8  &	308.1  & 17.06 & 0.01 & $-1.11$ &  0.02 &  0.27  & 0.01\\
\phn6 &  596.6  &	327.3  & 17.40 & 0.01 & $-1.07$ &  0.03 &  0.43  & 0.01\\
\phn7 &  583.3  &	264.2  & 17.65 & 0.01 & $-1.01$ &  0.03 &  0.28  & 0.01\\
\phn8 &  578.7  &	273.0  & 17.82 & 0.01 & $-1.19$ &  0.03 &  0.20  & 0.01\\
\phn9 &  594.7  &	258.3  & 17.88 & 0.01 & $-1.16$ &  0.03 &  0.27  & 0.01\\
10 &  618.5  &	277.6  & 18.04 & 0.01 & $-0.99$ &  0.04 &  0.66  & 0.01\\
11 &  612.9  &	260.9  & 18.43 & 0.01 & $-0.91$ &  0.06 &  0.34  & 0.01\\
12 &  605.7  &	266.6  & 18.43 & 0.01 & $-0.59$ &  0.07 &  0.55  & 0.01\\
13 &  608.1  &	288.0  & 18.53 & 0.01 &\hphantom{$-$}0.04 &  0.02 &  0.12  & 0.01\\
14 &  597.1  &	282.2  & 18.84 & 0.01 & $-1.06$ &  0.06 &  0.23  & 0.01\\
15 &  587.5  &	240.9  & 19.00 & 0.01 & $-0.83$ &  0.07 &  0.33  & 0.01\\
16 &  595.7  &	272.1  & 19.00 & 0.01 & $-0.07$ &  0.15 &  0.26  & 0.01\\
17 &  604.8  &	290.8  & 19.09 & 0.01 & $-0.21$ &  0.03 &  0.17  & 0.01\\
18 &  551.9  &	265.8  & 19.19 & 0.02 & $-0.70$ &  0.07 &  0.37  & 0.03\\
19 &  599.6  &	273.4  & 19.24 & 0.01 & $-0.77$ &  0.07 &  0.30  & 0.01\\
20 &  591.0  &	273.1  & 19.36 & 0.05 &\hphantom{$-$}0.24 &  0.07 &\llap{$-$}0.01 & 0.06\\
21 &  608.0  &	273.8  & 19.37 & 0.01 & $-0.36$ &  0.04 &  0.14  & 0.01\\
22 &  609.9  &	307.1  & 19.44 & 0.01 & $-0.78$ &  0.10 &  0.24  & 0.01\\
23 &  616.4  &	273.8  & 19.70 & 0.01 & $-0.86$ &  0.04 &  0.67  & 0.01\\
24 &  624.7  &	266.0  & 19.77 & 0.01 &\hphantom{$-$}0.01 &  0.04 &  0.05  & 0.01\\
25 &  628.1  &	260.4  & 19.82 & 0.01 & $-0.16$ &  0.07 &  0.28  & 0.01\\
26 &  581.6  &	242.1  & 19.82 & 0.02 & $-0.13$ &  0.20 &  0.44  & 0.02\\
27 &  660.6  &	220.0  & 20.07 & 0.02 & $-0.17$ &  0.25 &  0.60  & 0.03\\
28 &  592.6  &	268.8  & 20.12 & 0.06 &\hphantom{$-$}0.18 &  0.07 &  0.07  & 0.07\\
29 &  664.5  &	331.1  & 20.14 & 0.02 & $-0.27$ &  0.27 &  0.74  & 0.03\\
30 &  555.8  &	250.1  & 20.16 & 0.02 &\hphantom{$-$}0.06 &  0.29 &  0.58  & 0.02\\
31 &  606.3  &	303.6  & 20.34 & 0.04 & \nodata & \nodata & 0.85 & 0.05\\
32 &  556.8  &	224.1  & 20.46 & 0.02 & \nodata & \nodata & 0.41 & 0.02
\enddata
\tablenotetext{a}{Program No.~5114, chip 2}
\end{deluxetable}

\begin{deluxetable}{lrrcccccc}
\tablenum{6}
\tablewidth{0pt}
\tablecaption{Photometry of stars around P1429 (Knot 2)}
\tablehead{
\colhead{Star} &\colhead{X\tablenotemark{a}} &\colhead{Y\tablenotemark{a}} 
& \colhead{F555W} & \colhead{$\sigma$}
& \colhead{F336W--F555W} & \colhead{$\sigma$} &\colhead{F555W--F814W} &
 \colhead{$\sigma$}\\
}
\startdata
1  & 712.0 & 572.4 & 15.88  & 0.02 & $-1.08$  & 0.05    &  0.61 & 0.05 \\
2  & 684.4 & 564.4 & 17.78  & 0.01 & \nodata  & \nodata &  2.13 & 0.01 \\
3  & 763.8 & 578.1 & 17.96  & 0.01 & \nodata  & \nodata &  1.45 & 0.01 \\
4  & 714.2 & 570.1 & 18.10  & 0.03 & $-1.14$  & 0.15    &  0.54 & 0.07 \\
5  & 710.1 & 588.2 & 19.08  & 0.01 & $-0.55$  & 0.06    &  1.04 & 0.02 \\
6  & 754.9 & 556.1 & 19.64  & 0.02 & \nodata  & \nodata &  1.39 & 0.02 \\
7  & 718.1 & 589.1 & 19.73  & 0.01 & $-0.53$  & 0.08    &  0.65 & 0.02 \\
8  & 707.6 & 580.9 & 20.14  & 0.01 & $-0.78$  & 0.04    &  0.25 & 0.02 \\
9  & 698.0 & 580.7 & 20.45  & 0.01 & $-0.47$  & 0.05    &  0.24 & 0.02 
\enddata
\tablenotetext{a}{Program No.~5114, chip 2}
\end{deluxetable}

\begin{deluxetable}{lrrcccccc}
\tablenum{7}
\tablewidth{0pt}
\tablecaption{Photometry of stars around P294/P304}
\tablehead{
\colhead{Star} &\colhead{X\tablenotemark{a}} &\colhead{Y\tablenotemark{a}} 
& \colhead{F555W} & \colhead{$\sigma$}
& \colhead{F336W--F555W} & \colhead{$\sigma$} &\colhead{F555W--F814W} &
 \colhead{$\sigma$}\\
}
\startdata
\phn1 &  600.5 &  664.4 &	 14.47 &   0.01 &  $-1.51$ &  0.01 & 0.04 & 0.01\\
\phn2 &  599.0 &  658.0 &	 14.90 &   0.01 &  $-1.48$ &  0.01 & 0.13 & 0.01\\
\phn3 &  602.5 &  651.9 &	 16.28 &   0.01 &  $-1.38$ &  0.01 & 0.06 & 0.01\\
\phn4 &  586.4 &  638.5 &	 16.51 &   0.01 &  $-1.21$ &  0.01 & 0.11 & 0.01\\
\phn5 &  580.7 &  640.9 &	 17.57 &   0.01 &  $-1.33$ &  0.01 & 0.08 & 0.01\\
\phn6 &  607.3 &  667.9 &	 17.97 &   0.01 &  $-1.07$ &  0.03 & 0.20 & 0.02\\
\phn7 &  596.1 &  609.2 &	 17.99 &   0.01 &  $-1.21$ &  0.02 & 0.16 & 0.01\\
\phn8 &  622.2 &  619.5 &	 18.40 &   0.01 &  $-0.89$ &  0.02 & 0.19 & 0.01\\
\phn9 &  585.8 &  686.6 &	 18.48 &   0.01 &  $-1.04$ &  0.02 & 0.14 & 0.01\\
10 &  593.2 &  646.9 &	 19.23 &   0.01 &  $-0.81$ &  0.03 & 0.12 & 0.02\\
11 &  603.0 &  605.1 &	 19.43 &   0.01 &  $-0.68$ &  0.03 & 0.21 & 0.02\\
12 &  590.4 &  671.2 &	 19.44 &   0.01 &  $-0.48$ &  0.05 & 0.18 & 0.02\\
13 &  588.2 &  615.9 &	 19.78 &   0.01 &  $-0.53$ &  0.04 & 0.21 & 0.02\\
14 &  651.2 &  618.1 &	 19.78 &   0.01 &  $-0.52$ &  0.04 & 0.35 & 0.02\\ 
15 &  583.8 &  664.7 &	 19.90 &   0.01 &  $-0.61$ &  0.07 & 0.13 & 0.02\\
16 &  545.6 &  633.8 &	 19.94 &   0.01 &  $-0.16$ &  0.06 & 0.27 & 0.02\\
17 &  564.3 &  651.3 &	 20.06 &   0.01 &\hphantom{$-$}0.75 &  0.13 & 0.49 & 0.02\\
18 &  618.0 &  661.7 &	 20.06 &   0.02 &  $-0.49$ &  0.09 & 0.28 & 0.03\\
19 &  617.7 &  663.9 &	 20.07 &   0.02 &\hphantom{$-$}0.04 &  0.09 & 0.39 & 0.03\\
20 &  626.4 &  613.0 &	 20.10 &   0.01 &  $-0.18$ &  0.07 & 0.32 & 0.02\\
21 &  607.4 &  638.7 &	 20.13 &   0.01 &  $-0.32$ &  0.10 & 0.18 & 0.03\\
22 &  617.3 &  651.7 &	 20.16 &   0.04 &  $-0.18$ &  0.08 & 0.28 & 0.08\\
23 &  571.7 &  675.1 &	 20.26 &   0.01 &  $-0.23$ &  0.07 & 0.15 & 0.03\\
24 &  638.6 &  649.2 &	 20.29 &   0.01 &  $-0.41$ &  0.07 & 0.31 & 0.03\\
25 &  540.5 &  651.7 &	 20.29 &   0.02 &  $-0.13$ &  0.08 & 0.21 & 0.05\\
26 &  581.8 &  608.2 &   20.31 &   0.01 &  $-0.21$ &  0.10 & 0.20 & 0.02\\
27 &  629.2 &  665.5 &   20.33 &   0.01 &\hphantom{$-$}0.06 &  0.09 & 0.36 & 0.02\\
28 &  598.3 &  649.5 &   20.49 &   0.08 &  \nodata &  \nodata & 0.60 & 0.09
\enddata
\tablenotetext{a}{Program No.~6122, chip 2}
\end{deluxetable}

\begin{deluxetable}{lrrcccccc}
\tablenum{8}
\tablewidth{0pt}
\tablecaption{Photometry of stars around P1231/P1304/P1306/P1312}
\tablehead{
\colhead{Star} &\colhead{X\tablenotemark{a}} &\colhead{Y\tablenotemark{a}} 
& \colhead{F555W} & \colhead{$\sigma$} 
& \colhead{F336W--F555W} & \colhead{$\sigma$} &\colhead{F555W--F814W} 
& \colhead{$\sigma$}
}
\startdata
\phn1   & 277.9 &   56.1 & 12.85 & 0.05 &  $-$1.32 & 0.06 &  0.32 & 0.07 \\ 
\phn2A  & 298.1 &   50.4 & 14.55 & 0.03 &  $-$1.35 & 0.04 &  0.27 & 0.06 \\
\phn2B  & 298.1 &   51.3 & 14.61 & 0.03 &  $-$1.37 & 0.04 &  0.29 & 0.06 \\
\phn3A  & 230.4 &   57.1 & 14.72 & 0.03 &  $-$1.20 & 0.06 &  0.27 & 0.06 \\
\phn3B  & 230.1 &   58.3 & 14.84 & 0.03 &  $-$1.12 & 0.06 &  0.34 & 0.06 \\
\phn4   & 225.3 &   62.0 & 14.90 & 0.01 &  $-$1.17 & 0.02 &  0.26 & 0.01 \\
\phn5   & 243.1 &   51.3 & 14.99 & 0.01 &  $-$1.20 & 0.02 &  0.30 & 0.01 \\
\phn6   & 310.6 &   76.6 & 15.02 & 0.01 &  $-$1.32 & 0.01 &  0.18 & 0.01 \\
\phn7   & 284.7 &   36.2 & 15.03 & 0.01 &  $-$1.29 & 0.02 &  0.23 & 0.01 \\
\phn8   & 207.3 &   37.2 & 15.15 & 0.01 &  $-$1.20 & 0.02 &  0.40 & 0.01 \\
\phn9   & 204.1 &   33.7 & 15.29 & 0.01 &  $-$1.20 & 0.02 &  0.32 & 0.01 \\
\tablebreak
10  & 291.8 &  129.7 & 15.59 & 0.01 &  $-$1.28 & 0.01 &  0.22 & 0.01 \\
11A & 277.6 &  118.5 & 16.15 & 0.03 &  $-$1.15 & 0.04 &  0.36 & 0.04 \\
11B & 277.3 &  120.5 & 16.17 & 0.03 &  $-$1.04 & 0.04 &  0.30 & 0.04 \\
12  & 297.5 &   74.4 & 16.19 & 0.01 &  $-$1.22 & 0.01 &  0.21 & 0.01 \\
13  & 230.6 &   99.4 & 16.42 & 0.01 &  $-$1.20 & 0.02 &  0.17 & 0.01 \\
14  & 259.9 &   75.2 & 16.66 & 0.01 &  $-$1.09 & 0.02 &  0.23 & 0.01 \\
15  & 250.5 &   68.0 & 16.70 & 0.01 &  $-$0.86 & 0.02 &  0.28 & 0.01 \\
16  & 214.6 &   65.9 & 16.73 & 0.01 &  $-$1.14 & 0.02 &  0.23 & 0.01 \\
17  & 233.6 &   74.2 & 17.05 & 0.01 &  $-$1.06 & 0.03 &  0.24 & 0.01 \\
18  & 248.7 &  108.2 & 17.34 & 0.01 &  $-$1.09 & 0.03 &  0.32 & 0.01 \\
19  & 237.3 &   59.7 & 17.49 & 0.01 &  $-$0.90 & 0.03 &  0.27 & 0.01 \\
20  & 261.4 &   69.8 & 17.96 & 0.01 &  $-$0.86 & 0.04 &  0.27 & 0.01 \\
21  & 247.3 &   56.4 & 18.07 & 0.01 &  $-$0.83 & 0.04 &  0.28 & 0.01 \\
22  & 225.7 &   47.9 & 18.09 & 0.03 &  $-$0.94 & 0.09 &  0.28 & 0.05 \\
23  & 291.8 &  134.2 & 18.20 & 0.01 &  $-$0.99 & 0.04 &  0.36 & 0.01 \\
24  & 205.9 &   48.1 & 18.36 & 0.03 &  $-$0.86 & 0.08 &  0.33 & 0.04 \\
25  & 284.6 &  121.2 & 18.41 & 0.01 &  $-$0.77 & 0.05 &  0.38 & 0.01 \\
26  & 223.1 &   45.2 & 18.50 & 0.03 &  $-$0.83 & 0.08 &  0.29 & 0.04 \\
27  & 275.1 &   44.9 & 18.69 & 0.03 &  $-$1.14 & 0.09 &  0.34 & 0.04 \\
28  & 204.4 &   43.4 & 18.83 & 0.03 &  $-$0.55 & 0.10 &  0.37 & 0.04 \\
29  & 222.0 &   37.8 & 19.12 & 0.03 &  $-$0.57 & 0.10 &  0.40 & 0.04 \\
30  & 290.4 &   69.5 & 19.35 & 0.01 &  $-$0.39 & 0.12 &  0.36 & 0.01 \\
31  & 319.3 &   94.1 & 19.38 & 0.01 &  $-$0.77 & 0.10 &  0.39 & 0.01 \\
32  & 283.8 &  113.3 & 19.39 & 0.01 &\hphantom{$-$}0.90 & 0.29 &  1.07 & 0.01 \\
33  & 240.1 &   66.2 & 19.49 & 0.01 &  $-$0.29 & 0.15 &  0.33 & 0.01 \\
34  & 277.6 &   97.3 & 19.50 & 0.01 &  $-$0.47 & 0.12 &  0.33 & 0.01 \\
35  & 208.1 &   43.5 & 19.52 & 0.05 &  $-$0.63 & 0.13 &  0.50 & 0.06 \\
36  & 312.8 &   80.6 & 19.76 & 0.03 &  $-$0.39 & 0.23 &  0.55 & 0.04 \\
37  & 307.9 &   39.9 & 19.79 & 0.02 &  \nodata & \nodata & 0.29 & 0.03 \\
38  & 309.5 &   57.4 & 19.86 & 0.01 &  $-$0.64 & 0.18 &  0.39 & 0.01 \\
39  & 223.1 &   49.8 & 19.88 & 0.05 &  $-$0.28 & 0.18 &  0.51 & 0.07 \\
40  & 260.5 &  103.4 & 19.91 & 0.01 &  $-$0.15 & 0.20 &  0.40 & 0.01 \\
41  & 319.1 &   50.3 & 19.97 & 0.02 &  \nodata & \nodata & 0.34 & 0.03 \\
42  & 202.6 &   50.6 & 19.99 & 0.02 &  \nodata & \nodata & 0.34 & 0.04 \\
43  & 261.9 &   37.1 & 20.04 & 0.02 &  \nodata & \nodata & 0.42 & 0.03 \\
44  & 242.6 &   74.2 & 20.22 & 0.01 &  $-$0.11 & 0.27 &  0.35 & 0.01 \\
45  & 318.4 &   34.7 & 20.28 & 0.02 &  \nodata & \nodata & 0.47 & 0.04 \\
46  & 306.9 &  147.3 & 20.35 & 0.01 &  $-$0.78 & 0.19 &  0.36 & 0.01 \\
47  & 239.5 &   39.8 & 20.40 & 0.02 &  \nodata & \nodata & 0.44 & 0.03 \\
48  & 220.6 &   70.9 & 20.45 & 0.02 &  \nodata & \nodata & 0.37 & 0.03 \\
49  & 299.5 &  109.1 & 20.49 & 0.02 &  \nodata & \nodata & 0.52 & 0.03
\enddata
\tablenotetext{a}{Program No.~5114, chip 2.  Stars with Y~$<46$ are
vignetted and their listed magnitudes are too faint.}
\end{deluxetable}



\end{document}