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\begin{document}
\institution{The University of Wisconsin-Madison}
\department{Department of Astronomy}
\location{Madison, WI 53706}
%\rptauthor{}
\maketitle

During the past year, the Astronomy Department at UW-Madison has been
active in a wide range of observational and theoretical research
program. We initiated instrumentation development for space and ground
based programs, and increased the number of faculty and staff. We have
joined the Southern African Large Telescope (SALT) consortium that
will construct a 10-meter optical telescope located at the Southern
African Astronomical Observatory site in Sutherland, South Africa. The
design will be modified from the Hobby-Eberly Telescope but will have
a larger corrected field of view (8\arcmin) with better image quality,
larger pupil, and an enlarged prime-focus instrument
payload. Ground-breaking occurred September 1, 2000. First light is
expected in 2003.

We are especially pleased that Dr. Amy Barger has accepted a position
as Assistant Professor, to begin her duties in August 2001. She is
currently the Hubble Fellow/Chandra Fellow at Large at the Institute
of Astronomy, University of Hawaii.

WIYN refers to the Wisconsin-Indiana-Yale-NOAO 3.5-m telescope
on Kitt Peak.

\section{Personnel}

The faculty consists of Professors Anderson (Chair), Cassinelli,
Churchwell, Gallagher, Hoessel, Mathieu, Nordsieck, Reynolds, Savage,
and Sparke, Associate Professor Bershady (promoted to the rank during
the year), and Assistant Professors Barger, Lazarian and
Wilcots. Bless, Code, and Mathis are Professors Emeriti who reside
in Madison. Percival is Scientist; Harris and Wakker are Associate
Scientists. Assistant scientists are Barnes (McKinney Assistant
Scientist), Kobulnicky (Hubble Fellow), and Quigley. M. Orio was
appointed Visiting Associate Scientist. Dr. Philipp Richter joined the
staff as Assistant Scientist, following his graduate work in Bonn,
Germany. He will work with Savage on data from the Far Ultraviolet
spectrograph (FUSE) satellite relating to gas in the interstellar and
intergalactic medium. Dr. Jungyeon Cho arrived from the Johns Hopkins
University to work with Lazarian as Assistant Scientist. Dolan,
Haffner, and Stasson are Research Associates. W. Harris, M. Quigley,
and J. Morgenthaler served as Lecturer for a semester during the
academic year. Many scientists visited during the year.

The monograph by H.J.G.L.M. Lamers \& J.P. Cassinelli, {\it
Introduction to Stellar Winds}, was published by Cambridge University
Press. The advanced-undergraduate textbook ``Galaxies in the Universe:
An Introduction'', by L.S. Sparke and J.S. Gallagher, is ready for
publication by the Cambridge University Press in late 2000.

K. Stasson received the PhD for his thesis entitled ``A Test of Star
Formation Theory: The Connection Between Rotation, Accretion, and
Circumstellar Disks Among Low-Mass Pre-Main Sequence Stars.'' C. Dolan
completed his PhD thesis ``The Young Population of the $\lambda$
Orionis Star-Forming Region.'' Both theses were supervised by
Mathieu. P. Erwin received the PhD with a thesis entitled ``Barred
Galaxies and Orbits in Binary Systems'', supervised by Sparke. Erwin
in now at the Astrophysical Institute of the Canares in Tenerife, Spain.

Graduate student C. Conselice is spending the 2000-2001 academic year
as a visitor at the Space Telescope Science Institute where, in
addition to his thesis research, he is investigating the structures of
high redshift galaxies. Graduate student J. Hoffman won first place in
the Ruth and Helen Dickie Graduate Research Seminar Competition,
sponsored by the UW-Madison chapter of Sigma Delta Epsilon, Graduate
Women in Science, for her talk entitled ``Building a Binary Star:
Monte Carlo Modeling of $\beta$ Lyrae." Hoffman continues as observing
coordinator for the Half-wave Polarimeter (HPOL) at Pine Bluff
Observatory.

Bless served on two significant committees: Gemini Observatory Site
Visit Committee (Division of Astronomical Sciences, NSF), and
Portfolio Allocation Review Committee (Division of Astronomical
Sciences, NSF). Churchwell served as Co-chair of Joint Discussion 3 at
the IAU General Assembly in Manchester, England. He continues to serve
on the NAIC Visitors Committee for Arecibo Observatory and on the
Program Advisory Committee for NRAO, advisory to the NRAO director on
long-range programs. Mathieu was Co-Chair of IAU Symposium 200, {\it
The Formation of Binary Stars}, served on the Astronomy and
Astrophysics Survey, ``Ultraviolet, Optical, and Infrared from Space''
Panel, as President of the WIYN Board, as Associate Director of the
National Institute of Science Education, and as Director of its
College Level 1 Institute. Anderson, Nordsieck, Reynolds, Bershady,
and Wilcots have represented Wisconsin on the Interim Board of the
Southern African Large Telescope (SALT). Bershady has been appointed
as the Wisconsin SALT Board representative and Nordsieck to the SALT
Science Working Group. Percival continued his participation in the IAU
Working Group on Astronomical Standard's initiative called SOFA:
``Standards of Fundamental Astronomy." Its goal is to produce a set of
basic software that implement commonly-used formulae and standard
models in fundamental astronomy. Savage continued as a member of the
Committee for Astronomy and Astrophysics of the National Research
Council and of the Space Telescope Institute Council.

\section{Stars, Outflows, and Galactic Structure}%%%%%%

Barnes continued his work on the rotation rates of late-type stars.
His theoretical work with Sofia (Yale) and Pinsonneault (Yale)
suggests that the majority of the stars in young open clusters have
undergone disk interactions with a time-scale of the order of 1 Myr in
their early stages. These models must be compared to observations of
stellar rotation periods in clusters that are a few to several hundred
Myr old. Some data have already been acquired for NGC~2477 at CTIO;
other clusters will be targeted in the winter and spring of 2000-2001.
A large dataset for the younger cluster NGC~2516 and a smaller one for
the open cluster M 34 is being analyzed in order to investigate the
angular momentum distribution and transport in stellar interiors, to
learn about its loss through stellar winds, and to understand aspects
of star-disk interaction on the pre-main-sequence.

Cassinelli and Miller obtained high-resolution X-ray observations of
the early-type stars Zeta Puppis and $\delta$ Ori using the
High-Energy Transmission Grating Spectrometer on the Chandra
spacecraft. The spectra show the line emission from early-type stars
in unprecedented detail. Initial results confirm older shock model
estimates of the temperature of the emitting gas. The high-resolution
capability of the {\it Chandra} satellite makes density diagnostics of
the forbidden, intercombination, and resonance lines of helium-like
ions accessible. Initial analysis indicates the densities of the
emitting gas are much higher than expected. They plan to analyze the
temperature structure of the gas and to search for time
variability. Wayne Waldron (Emergent Information Technologies) and
Cassinelli carried out a study of the properties of the X-ray sources
in Zeta Ori. Cassinelli and John Brown of Glasgow continued
investigating the transfer of angular momentum to the disks around Be
stars. Richard Ignace (U. Iowa), Quigley, Babler and Cassinelli are
analyzing the profiles of recombination and forbidden lines in the
{\it Infrared Space Observatory} spectra of Wolf Rayet stars in order
to derive information about the velocity and ionization structure in
the winds of the stars. The forbidden lines provide the best
information regarding the terminal velocities of the winds; the He II
recombination line profiles provide information about their rate of
acceleration.

Churchwell has continued a broad collaborative observational program
to study the properties of galactic massive star formation regions
(MSFRs). A C$^{17}$O (1-0, 2-1, 3-2) and C$^{18}$O (2-1) survey
towards 16 MSFRs by Hofner, Wyrowski, Walmsley, and Churchwell
indicates that the CO emitting clumps have sizes of $\sim$1 pc,
averaged densities of $\sim$10$^5$ cm$^{-3}$, temperatures of $\sim$25
K, and clump masses from 10$^3$ to 4$\times 10^4$ M\subsun. Most of
the clumps are virialized in the sense that their gravitational energy
is about the same as the bulk kinetic energy inferred from line
widths. The CO temperatures are lower than those inferred from
CH$_3$CN, which is confined to the central cores.

Hunter, Churchwell, Watson, Cox, Benford, and Roelfsema imaged
24 MSFRs at 350 $\mu$m with a resolution of
11$^{\prime\prime}$ using the Caltech Submillimeter Observatory,
mainly to detect precursors of Ultracompact (UC)
HII regions in MSFRs. Of the 28 detected submm components, 10 had
luminosities $>10^{4.3}$ L\subsun\ but no detected ionized gas. Most
of these are maser emitter (either OH, and/or H$_2$O, or CH$_3$OH).
These are precisely the properties expected during the rapid accretion
phase of massive star formation believed to occur prior to the
formation of a UC HII region. Analysis of the 350 $\mu$m sources
indicate average masses of $\sim10^{3.5}$ M\subsun, luminosities of
$\sim10^5$ L\subsun, and H column densities of $10^{23.8}$ cm$^{-2}$.

A program to observe and analyze CH$_3$CN emission toward MSFRs has
been initiated by Churchwell and Watson in collaboration with V.
Pankonin (NSF) and John Bieging (U. Ariz). The single dish observations
using the Heinrich Hertz telescope of the Submillimeter Observatory
have just been submitted for publication (Pankonin et al. 2000, ApJ,
submitted). High resolution observations have been obtained with the
Berkeley Illinois Millimeter Array toward two regions. Sewilo has
analyzed high dynamic range VLA continuum images of G5.89 obtained
over a 10 year period; an angular expansion rate of 4$\pm$1 mas/y was
found, the same as Acord, Churchwell, and Wood (1998) found over a 5
year baseline.

Barnes, Dolan, Meibom, and Mathieu continued their program acquiring
high-precision stellar radial velocities with the WIYN telescope and
Multi-Object Spectrograph. As part of the WIYN Open Cluster Study,
they have obtained 4776 velocity measurements of 509 stars in NGC~188,
2594 measurements of 936 stars in M35, 1795 measurements of 347 stars
in NGC~2264, and 3196 measurements of 861 stars in NGC~6819. Extensive
spectroscopic binary populations are being discovered in all four
clusters. Nearly 50 binaries have orbital solutions in NGC~188, the
most extensively observed cluster. Emphasis this year shifted to
careful error analyses in preparation for publication. Raw data for
bright stars have measurement precisions of 0.4 km s$^{-1}$, due to
variations among fibers and in night-to-night zero-points. Correction
for systematic effects should lower measurement precisions to 0.3 km
s$^{-1}$. Photon errors dominate at the limit of V = 16.5. Using the
Mini-Mosaic imager on WIYN, Barnes obtained deep BVI photometry of the
central region of the open cluster NGC~6819 in order to generate a
color-magnitude diagram for the lower main sequence and to test the
Mini-Mosaic.

Dolan completed his thesis study (with Mathieu) on the
$\lambda$~Orionis star-forming region, which presents a snapshot of a
moderate-mass giant molecular cloud 1--2 Myr after cloud disruption by
OB stars. The OB stars, the low-mass stellar population, remnant
molecular clouds, and the dispersed gas are all still present. Dolan
used optical photometry and multi-object spectroscopy for lithium
absorption to identify 266 PMS stars in an 8 squared degree area. He
also obtained new Str\"omgren photometry for the massive stars, from
which he derived a distance of 450 pc and a turnoff age of 6 -- 7
Myr. Using these parameters and pre-main-sequence evolutionary models,
he mapped the star-formation history of the low-mass stars. He finds
that low-mass star formation started throughout the region at about
the same time as the birth of the massive stars. Thereafter the birth
rate accelerated. Within the last 1--2 Myr star-formation ceased in
the center of the star-forming region, near the concentration of OB
stars, while it continues in dark clouds 20 pc away. He suggested that
a supernova 1--2 Myr ago destroyed the molecular cloud core from which
the OB stars formed, but did not terminate star formation in more
distant reaches of the giant molecular cloud. He found no secure
evidence for triggered or sequential star formation in the outer
molecular clouds. The global star formation of the $\lambda$~Ori
region has generated the field IMF, but local star formation in
sub-regions shows large deviations from the expected ratio of high- to
low-mass stars.

Mathieu, Lattanzi (Torino), and Zinnecker (Potsdam) used relative
astrometric observations of the pre-main-sequence single-lined
spectroscopic binary 045251+3016 obtained with the Fine Guidance
Sensor on the HST. Mathieu and Steffen determined the orbital elements
of this system; the semi-major axis is 0.0352\arcsec. Optical spectra
taken at CfA (with Latham and Torres) provided 58 radial-velocity
measurements of the primary star and IR spectra taken at KPNO (with
Mazeh (Tel Aviv), Prato (UCLA) and Simon (Stony Brook) provided a mass
ratio for the binary system. The derived values for the primary and
secondary masses are 1.44 $\pm$ 0.25 M\subsun\ and 0.78 $\pm$ 0.11
M\subsun, respectively, at a distance of 138 $\pm$ 8 pc. The
theoretical mass derived from the Baraffe et al. (1998) tracks is
closest to the derived mass, deviating by less than one sigma. The
Palla and Stahler (1999) tracks deviate further but remain consistent
with these data. The D'Antona and Mazzitelli (1997) tracks are more
than three sigma away from the derived mass, making them inconsistent
with these measurements.

Mathieu, Carr (NRL) and Najita (NOAO) continued a program of
high-resolution near-infrared spectroscopy (CO fundamental and
overtone transitions) in order to explore the circumstellar gas in
several young binaries. They made the first discoveries of CO
fundamental ro-vibrational emission from PMS stars. The
high-resolution infrared echelle spectra reveal emission lines from
both the v=1 and v=2 vibrational levels with line widths of about 70
km s$^{-1}$. The average CO excitation temperature is about 1200
K. The disk model requires gas with an average surface density of 5
$\times 10^{-4}$ g cm$^{-2}$ that extends outward to 0.5 $\pm$ 0.1 AU and
inward to at least 0.1 AU of the center-of-mass. The radial extent for
the emitting gas is close to the predicted size of the gap in the DQ
Tau accretion disk that is expected to be dynamically cleared by the
binary. They interpret these results, and previous modeling of DQ Tau's
spectral energy distribution, as evidence for a small amount ($\sim$
10$^{-10}$ M\subsun) of diffuse material residing within the
optically-thin disk gap, perhaps connected with accreting material
crossing the disk gap. 

Hoffman and Nordsieck used the Space Telescope Imaging Spectrograph on
the Hubble Space Telescope to search for Doppler signatures of a
bipolar outflow in the interacting eclipsing binary star $\beta$
Lyrae. They seek to confirm their previously-published polarimetric
evidence for such an outflow and to investigate its size and
composition.

Nordsieck, Hoffman, and Polidan (GSFC) are continuing in their
spectropolarimetric investigation of active Algols and W Ser eclipsing
interacting binaries. The goal is to obtain spectropolarimetry from
3200 - 10500 \AA\ with a resolution R $\sim$ 800 over the binary
phase, with about 20 points per orbit. This is to be analyzed using
Hoffman's Monte Carlo code. Observations, obtained with HPOL at Pine
Bluff Observatory and WIYN, are now complete for the W Ser stars W
Ser, V367 Cyg, RX Cas, and SX Cas, including interstellar polarization
measurements at WIYN of the very close companions of SX Cas and V367
Cyg. Observations are also complete for the active Algol systems RY
Per, UX Mon, TT Hya and V356 Sgr. The first paper will be for V367
Cyg.

Hoffman and Nordsieck continued their investigation of eclipsing
binary Herbig Ae/Be stars by conducting several more polarimetric
observations of BM Ori and MWC1080 with HPOL at WIYN in September.
They now have nearly complete polarization phase curves for both these
young systems, and plan to model them using Hoffman's Monte Carlo code
in order to compare their geometrical structures with those of the
evolved binary systems previously studied.

Hoffman has completed a Monte Carlo radiative transfer model for
binary star-disk systems. She is currently investigating the
variations in its observable characteristics throughout parameter
space. This model has shown promise in reproducing the observed flux
and polarization curves of $\beta$ Lyrae and should provide insights
into the structure of a wide range of other binary systems. B.
Whitney (Space Science Institute) continues as a mentor and
collaborator in this modeling effort. Hoffman also attended the NASA
Summer School for High-Performance Computing at GSFC in July to
investigate the possibility of parallelizing the Monte Carlo code in
order to construct high-precision wavelength-dependent models.

A new analysis of the visible and ultraviolet continuum polarization
in P Cyg, as observed by HPOL and the Wisconsin Ultraviolet
PhotoPolarimeter (WUPPE), combined with the wind models of Najarro,
has led Nordsieck and collaborators to important new limits on the
location, ionization, density, and density contrast of the wind
inhomogeneities that cause the intrinsic polarization (Nordsieck and
Wisniewski 2000). The lack of a Balmer Jump in polarization indicates
that the clumps must be highly ionized. The polarization decrease into
the infrared is interpreted as due to competition of free-free
absorption with the polarizing electron scattering. The required
density indicates that the polarizing clumps must be at the very base
of the wind, and the density contrast is a factor of $\sim$10.

Orio has continued to study classical novae, low mass X-ray binaries,
and supersoft X-ray sources, especially the optical identification of
X-ray sources. She searched for ionization nebulae around systems with
shell hydrogen burning white dwarfs. With the BeppoSAX satellite, she
has studied a recent nova (V382 Vel) in X-rays immediately after the
outburst. With collaborators, she performed a Target of Opportunity
observation of Nova LMC 2000 with the X-ray satellite XMM. She is
analyzing archival X-ray observations of novae at any stage after the
outburst (even in quiescence). She has participated in an extensive
search for other ionization nebulae around novae, cataclysmic
variables, and supersoft X-ray sources with the WIYN telescope. She is
using it to search for optical counterparts of supersoft X-ray sources
in M31 (one has been identified with a nova) and candidate neutron
stars (anomalous X-ray pulsars in the Galaxy.)

\section{Interstellar Medium \label{ism}}%%%%%%

Lazarian worked with D. Pogosyan (CITA) on obtaining the statistics of
turbulence from observations. They derived relations between the
channel maps and underlying 3D velocity and density statistics. With
E. Vishniac (JHU), Lazarian continued to investigate
turbulent reconnection. They obtained important results for
reconnection in partially ionized gas. Together with De Gouveia Dal
Pino (Univ. of Sao Paolo), Lazarian considered the acceleration of
ultrahigh energy cosmic rays during reconnection events. With
B. Draine (Princeton), Lazarian obtained measures of polarization for
dipole radiation from tiny rotating grains (PAHs), important for the
Galactic contribution in the range of 10-100 GHz. With M. Efroimsky
(Harvard), Lazarian calculated the rate of internal
dissipation within asteroids. These results can be used to measure
the time from the most recent impact on the asteroid.

Nordsieck and Doane are analyzing data from the fourth flight of the
sounding rocket payload Wide-Field Imaging Survey Polarimeter (WISP),
launched on 11 April, 1999. WISP is a 20 cm off-axis Schmidt telescope
with polarimetric optics, obtaining imaging polarimetry over a
3x4\deg\ field with a resolution of 1\arcmin\ through a broadband
filter centered at 1750 \AA. The target for this flight was the
mid-latitude galactic reflection nebulosity near M81 and M82 (the
``Sandage region"), which has strong visible and IR cirrus. It has
been detected in the ultraviolet by the JHU and UCB UVX detectors. The
goal was to obtain photometry and polarimetry of any scattered UV
galactic diffuse light. Surprisingly, no UV cirrus was detected. Using
photometry of stars of known brightness in the field, we find that the
majority of the detected UV diffuse light cannot be scattered light
from galactic cirrus.

Haffner and Reynolds have completed the reduction of the Wisconsin
H-alpha Mapper (WHAM) survey. It provides the first view of the large
scale distribution and kinematics of the diffuse interstellar H$^+$
north of declination $-30$\deg. Haffner and Reynolds have begun a
collaboration with Tufte (Lewis and Clark College) to study optical
emission lines from High Velocity Clouds through remote observing with
the WHAM facility. Reynolds, Haffner, Madsen, Mathis, and Wood (CfA)
have begun to explore absorption and scattering in the diffuse
interstellar medium by comparing radiation transfer models with
observed \ha\ and H$\beta$ intensities and line profiles from WHAM.

Haffner, with Jenkins, Tripp (Princeton), Roesler (Physics Dept), and
Reynolds has begun comparing STIS UV observations of the Si~II$^*$
absorption line with WHAM \ha\ observations to explore the properties
of the warm ionized medium.

Fabian, Savage, Richter, Wakker, Sembach (JHU), Howk (JHU), and Tripp
(Princeton) are studying the galactic ISM absorption lines recorded in
Space Telescope Imaging Spectrograph (STIS) and FUSE spectra of bright
QSOs. The spectra are being used to study the abundances physical
conditions, and kinematics of neutral, warm ionized and hot ionized
gas extending many kiloparsecs away from the Galactic plane. The first
4 sightlines included the warped outer Galaxy and a high H I column
density region of Complex C. Galactic high velocity clouds are found
along all four lines of sight.

Savage, Sembach (JHU), Richter, Wakker, Fabian, and members of the
FUSE science team are studying the distribution of O~VI in the
Galactic halo. The first FUSE halo gas paper revealed the existence
of an extended but irregularly distributed halo of O~VI with an
exponential scale height of 2.7$\pm$0.4 kpc. The FUSE observations
combined with similar observations of other highly ionized species
from the IUE and HST suggest there is a systematic decrease in the
scale heights of Si~IV, C~IV, N~V, to O~VI from 5.1 to 2.7 kpc. Such
a decrease is difficult to explain with a single model for the origin
of the highly ionized gas in the Milky Way halo. Possible hybrid
models include hot gas arising in a fountain flow with a augmentation
to the amount of Si~IV and C~IV at high z from turbulent mixing of hot
and warm gas or by photoionization by hot halo stars or the
extragalactic background. The FUSE halo gas program is being expanded
to include measures of O~VI absorption toward $\sim$50 AGNs. This
larger data set will allow measures of the kinematics of the hot gas
and provide clues for the origin(s) of its irregular distribution.
These new observations will also make it possible to study the
relationships among the gas phases traced by O~VI, Fe~III, and S~III.
O~VI traces the hot ISM while Fe~III and S~III trace the warm ionized
phase of the ISM.

Richter worked on FUSE FUV absorption line data in order explore the
nature of the hot Galactic halo gas, the intermediate- and
high-velocity clouds (HVCs/IVCs), and molecular hydrogen in the
diffuse ISM.

Wakker, in collaboration with van Woerden (Groningen), Schwarz
(Nijmegen), and Kalberla (Bonn), continued investigating the distances
and metallicities of HVCs/IVCs. Two large HVCs are distant (d $>$ 4
kpc) and metal poor (Z $<$ 0.1 Z\subsun), while most large IVCs are
nearby (z$\sim$1 kpc) and metal rich (Z $\sim$ 0.5-1
Z\subsun). Combining ion abundances in HVCs and IVCs with those in low
velocity gas, Wakker \& Mathis found strong correlations between the
MgII, CaII, TiII, MnII, FeII abundances and N(HI); the implications of
this for the structure of the ISM were discussed.

Mathis continues to investigate the ionization properties of the
diffuse ionized gas in the Galaxy by means of photoionization models.
He is also interested in the properties of interstellar elemental
depletions and, especially, their rather small dispersions about the
mean value at a particular value of H~I column density. There is
considerable unexpected physical content in the column density, and
grain destruction must not take place in a few hard shocks, but rather
is a continuous function that can be parameterized by the H~I column
density.

\section{Extragalactic Astronomy}%%%%%%

Anderson, Weitenbeck (UW-Baraboo) and undergraduate Halstead continued
polarimetric observations at the Pine Bluff Observatory in the
direction of NGC~1502 in order to investigate the interstellar medium.

Bershady has completed a follow-up imaging survey with WIYN of
intermediate redshift spiral galaxies with optical rotation-curves
obtained at Palomar and Lick (with Haynes and Giovanelli (Cornell),
Mihos (Case Western), and Koo (UC Santa Cruz). The WIYN images suggest
that the outlying galaxies in the Tully-Fisher (rotation
speed-luminosity) correlation are disturbed systems. Some of the most
optically disturbed systems also display evidence for kinematic
asymmetry.

Bershady, Gallagher, Sparke, and Wilcots (alphabetical) have continued
a collaboration to explore the kinematics and evolution of
galaxies. One project bearing results this year is with with
D. Andersen (Penn State), namely to determine the intrinsic
ellipticity of nearby galaxy disks. Preliminary findings are that
disks are non-circular, with a model-dependence measurement of
ellipticity of 5\% (on average). If correct, then disk ellipticity
contributes as much as 50\% of the scatter in the Tully-Fisher
relation.

Bershady, Conselice, Jangren (Penn State), Koo (UCSC), and Guzman
(Yale) completed development of quantitative indices of galaxy
morphology, and have applied them to understanding an enigmatic
population of luminous, compact narrow emission-line galaxies that
appear at intermediate and high redshifts, as well as other distant
galaxy populations. The indices include rotational asymmetry, image
concentration, size, surface-brightness, and multi-band
color. Bershady and Conselice are currently analyzing recent NICMOS
observations with the Hubble Deep Field in collaboration with
Dickinson (STScI).

Hoessel and Bershady have begun a long-term, deep variability survey
pointed at intermediate redshift clusters using the WIYN telescope and
the Mini-Mosaic CCD imager. This project is in collaboration with
A. Saha (NOAO), and S. Majewski (Virginia). First-epoch observations
were achieved for 11 of the 15 targeted fields.

Gallagher and several collaborators continue to study stellar
populations and evolution of galaxies. He, with A. Cole (UMass) and
Smecker-Hane (UC-Irvine), used spectroscopic observations of the Large
Magellanic Cloud from CTIO to focus on abundance determinations as
well as stellar kinematics, while WFPC2 provides quality photometry of
the highly resolved field stars. Currently they are completing an
analysis of the WFPC2 color-magnitude diagrams. A related project
with R. Wyse (Johns Hopkins) and collaborators explores the star
formation history of the Ursa Minoris dwarf spheroidal galaxy using
combined ground and WFPC2 optical observations.

Gallagher is part of a team led by E. Skillman (U. Minnesota) to
obtain deep WFPC2 photometry for the dwarf irregular
galaxy IC~1613. An initial analysis of variable stars by
A. Dolphin and A. Saha (NOAO) confirm the presence of RR Lyrae
variables in a blue horizontal branch. IC~1613 joins the Local Group
dwarfs with old metal-poor stars. Gallagher is a member of a group led
by E. Tolstoy (UK Gemini office) and Cole (UMass) to derive a star
formation history. He also is working with Tolstoy in analyzing deep
photometry of isolated Local Group dwarfs obtained under excellent
seeing conditions with the ESO VLT/UT1 8-m telescope in 1999.

L. J. Smith (Univ. College London) and Gallagher completed a detailed
study of the super star cluster M82-F, for which they measured a
stellar velocity dispersion and derived an age and mass. The cluster
is overluminous for its 60~Myr age. It possibly lacks low mass
stars; it would then dissolve within the next Gyr, despite its 10$^6$
M\subsun\ mass. Gallagher participated in a team led by D. Hunter (Lowell)
completing a WFPC2 study of the structures and evolutionary status
of super star clusters and their surroundings in the starburst region
of NGC~1569.

Gallagher joined de Grijs (Virginia, now Cambridge U.) and O'Connell
(Virginia) in an HST optical/IR study of star clusters in region B of
M82. Large numbers of compact clusters exist covering a range in age
of $>$0.1~Gyr in this post-starburst zone; evidently star formation
preferred to make tightly bound objects in this region. He also
collaborated with the Virginia group in studying optically visible
supernova remnants on WFPC2 images. Gallagher and Homeier are
exploring the super star clusters in luminous clumps in the starburst
galaxies NGC~2403, NGC~7673, and II~Zw~168 with WFPC2 and WIYN optical
and UV images. Gallagher initiated discussions with Lancon
(U. Strasbourg) to better understand the role of stochastic effects in
determining the observed properties of populations of star clusters,
and with de Grijs and Hunter to better understand properties of
starburst cluster luminosity functions.

Working with A. Ferguson (Cambridge U.) and Wyse (JHU), Gallagher
joined a WFPC2 study of And~IV that established it is a background
dwarf irregular galaxy. They obtained WFPC2 images of HII regions far
from the mid-plane of the Magellanic type galaxy NGC~55 to search for
high latitude star formation in this edge on Magellanic system and to
study stellar populations beyond its main disk. Matthews (NRAO) and
Gallagher continued investigating the evolution of pure disk
galaxies. An initial analysis of the archetype superthin galaxy
UGC~7321 based on WIYN imaging is finished. Results from WFPC2
observations are being prepared for publication. Structural studies by
Matthews show that these types of disks experienced slow
evolution. They can be used as laboratories for studying
self-regulation of star formation processes and its implications for
the Tully-Fisher relationship. 

Gallagher, Calzetti (STScI), and others (including Conselice) continue
to explore the structure of ionized gas in starburst galaxies.
Following completion of a study of the extended ionized gas in
NGC~5253, new WFPC2 observations have been obtained for the starburst
nuclear region of its interacting companion, M83. These reveal a
complicated relationship between dense gas and stars, indicating that
large local variations in conditions on short timescales within this
region. One low-extinction zone contains the usual starburst structure
of compact star clusters on a bright background, with ionized gas
extending outward from the hole. Gallagher, Conselice, and Homeier are
studying the starburst responses of low mass disk galaxies to mild
perturbations. These are sometimes very strong. A working hypothesis
is that extreme late-type field galaxies that have not been perturbed
live on the edge of stability and can respond dramatically to an
interaction. This mechanism could produce faint blue field galaxies at
moderate redshifts.

Star formation in starbursts often occurs in large ``clumps'' that may
be the characteristic scales of gravitational instabilities in
perturbed, gas-rich disks. Gallagher is exploring the evolution of
this type of system through observations of evolutionary sequences of
starbursts with guidance from theoretical models. A key question is
whether clumps retain their identities and spiral into the centers of
galaxies under dynamical friction to form bulges.

Conselice, with Gallagher and Wyse (JHU) as supervisors, is pursuing a
PhD thesis on populations of dwarf galaxies in clusters of
galaxies. The goal is understanding the origins and astrophysical
implications of large numbers of dwarf elliptical (dE) galaxies in
clusters. Observations with Levine (USNO- Flagstaff) of Virgo dwarfs
yielded photometric and structural information. New radial velocities
were measured for 3 dozen Virgo dE candidates. These results in
combination with earlier measurements indicate dEs are less
dynamically relaxed than galaxies in the cluster cores, suggesting
that many of the dEs joined the cluster somewhat later, probably due
to infall. Side benefits of this program are excellent optical WIYN
images of clusters. These supported a study of ionized filaments
around NGC~1275 in Perseus, suggesting the outer filaments originate
where relativistic plasma or hot gas disturbs the surrounding,
possibly cooling IGM. They also produced a new gravitational lens ring
candidate in the galaxy cluster Abell~611; if confirmed, this will
join the small set of giant lensed arcs in clusters with low
redshifts.

Gallagher, Conselice, and Tolstoy are analyzing properties of faint
Local Group dwarf galaxies with VLT B- and R-band images. These
data complement deep HST imaging projects in reaching similar limiting
magnitudes but with much better surface brightness sensitivity; indeed,
most detected objects are resolved. A comparison of the two samples
yields insights into the role of selection effects in determining our
view of populations of faint galaxies.

As part of her PhD thesis, Otte (working with Gallagher and Reynolds)
is obtaining narrow band filter imaging with WIYN and long slit
spectroscopy with the 2.1m telescope on Kitt Peak to test the
hypothesis of an additional heating mechanism in the diffuse ionized
gas of galaxies. With Wilcots, she is using the DensePak on WIYN to
measure the \ha\ velocities and line widths in several galaxies.

Kobulnicky completed a 21-cm and optical emission line kinematic study
of local spiral and irregular galaxies with Gebhardt (UCSC). This
study provides a calibration of [O~II] emission line kinematics with
Ca H\&K stellar kinematics and 21 cm HI kinematics for assessing the
usefulness of these tracers to measure masses of galaxies in the high
redshift universe. With Koo (UCSD), Kobulnicky conducted near infrared
spectroscopic observations of two high-redshift galaxies near $z$ =
2.9 using the newly-commissioned NIRSPEC spectrograph on the Keck II
telescope. The oxygen abundances and masses of these high-redshift
galaxies studied to date show 2-3 magnitudes more luminosity for their
linewidth and metallicity compared to objects in the local
universe. With Woosley and Fryer at UCSC, Kobulnicki is continuing to
monitor the radial velocities of 140 O and B stars in Cygnus OB2
association in order to detect companion stars and measure their mass
distribution. An initial publication is in preparation and the
long-term survey continues at the Lick and Keck
Observatories. Kobulnicky and Pisano have described Arecibo 21 cm HI
measurements of unusually blue, compact galaxies in the nearby
universe. These may be analogs of compact starbursting galaxies
observed in the Hubble Deep Field. The goal is to infer the gas
properties of these distant galaxies and the potential for future star
formation by studying their local counterparts. With K. Johnson
(U. Colorado), Kobulnicky presented a press conference at the 2000
Winter AAS meeting on their discovery (ApJ December 1999) of extremely
young starburst clusters with ages less than a million years. This
discovery received attention from the Discovery Channel Online, the
ABC news online, and Sky \& Telescope magazine (July 2000).

Madsen and Reynolds have carried out a deep search for \ha\ emission
beyond the outer edge of the H I disk of M~31. No emission was
detected down to a limit of 0.03 Rayleighs, corresponding to an
emission measure of 0.08 cm$^{-6}$~pc.

To determine the physical conditions in the recently detected
intervening O~VI systems found at low redshift, Savage, Richter, Tripp
(Princeton), Jenkins (Princeton), Sembach (JHU), and Howk (JHU) are
studying the intergalactic absorption lines found in FUSE and STIS
spectra of bright low redshift QSOs. These absorption systems may
harbor a major fraction of the baryons existing in the low redshift
universe (Tripp et al. 2000). The FUSE spectra extend from 905 to 1187
\AA; the STIS from 1150 -- 1750 \AA. The first objects in this
program include PG 0953+415 ( $z$ = 0.239), H 1821+643 ($z$ =0.297),
PG 1116+215 ($z$ = 0.177), and PG 1259+593 ($z$ = 0.472). These UV
spectra have been supplemented with WIYN observations of the redshifts
of galaxies brighter than B $\sim$ 19 mag.

Howk and Savage are using the HST to image edge-on galaxies to search
for dusty interstellar clouds in the disk-halo interface of spiral
galaxies. This is a follow-up program to the successful WIYN imaging
program that revealed that spiral galaxies like NGC~891 commonly have
dust structures extending 0.5 to 1.5 kpc into the halos. These halo
dust structures trace 10$^5$ to 10$^6$ solar masses of gas and may be
the sites of ongoing star formation. The HST program involves
obtaining BVI images of five galaxies in the distance range from 17 to
70 Mpc with the WFPC2. The HST results for these galaxies will be
compared to those from the closer sample imaged with WIYN under
sub-arcsecond seeing conditions.

The PhD thesis of Erwin (Sparke, advisor) included a survey of
early-type barred galaxies with the WIYN telescope, searching for
signs of inner bars and other central structures. These turn out to
be surprisingly common; about a quarter of the galaxies have secondary
bars and about the same fraction have inner disks. One, NGC~2681, may
be the clearest example yet of a galaxy with three concentric
bars. NGC~3945, previously thought to be triple-barred, is merely
double, but it also has a large, extremely bright disk inside its
primary bar, with patchy dust lanes, a faint nuclear ring or
pseudo-ring within the disk, and an apparent secondary bar crossing
the ring. The presence of stellar nuclear rings in these and other
galaxies suggests that the centers of these galaxies are dynamically
cool and disklike, rather than being dynamically ``hot'' bulges.

Noordermeer and Sparke investigated the kinematics of a model for
lopsided galaxies consisting of a disk lying off-center in a dark halo
and orbiting the halo center. They searched for families of stable,
closed, non-crossing orbits that the gas should follow. Several
models showed strong lopsided gas kinematics, especially those in
which the disk spins around its axis in a retrograde sense compared to
its orbit around the halo center. The asymmetry was most
pronounced when the halo dominated the system. Late-type galaxies,
which are dominated by dark matter, show lopsided gas
more frequently than early-types.

Sparke, with A. Cox (Beloit College), Watson (UNAM), and van Moorsel
(NRAO) discussed optical observations and HI mapping of II~Zw~71, a
polar ring galaxy, and its close companion II~Zw~70. The blue,
star-forming, and very gas-rich ring orbits almost over the pole of
the small central S0 galaxy, which is almost devoid of HI gas. The
ring gas is in orderly rotation, but there is a gas streamer
connecting the ring with the companion, a starbursting dwarf. This
gaseous bridge, plus the \ha\ emission in the polar ring and in 
II~Zw~70, are strong evidence for an ongoing interaction between the two
galaxies.

Gallagher and Sparke participated in the Hubble Heritage Project's
observation of the polar ring galaxy NGC~4650A, chosen by 8,000
Internet voters from a list of candidates. They used the Wide Field
and Planetary Camera2 to take multi-color visible waveband images.
The unusual disk-ring structure of polar ring systems may be the
remnant of a colossal collision between two galaxies, probably at
least 1 billion years ago. What is left of one galaxy has become the
rotating inner disk of old red stars, while gas from another, smaller,
galaxy would have been stripped off and captured to form the polar
ring, which we see almost edge-on. Dr. Magda Arnaboldi (Naples
Observatory) and her graduate student Enricetta Iodice visited Madison
for a month to compare their near-infrared images. Their models
indicate that the polar ring has undergone vigorous star formation
with the past few hundred million years.

\section{Instrumentation and Observatories}%%%%%\%
\subsection{WIYN Instrumentation}

Bershady and Andersen (Penn State; CIC exchange student at UW)
concluded primary construction of an NSF-funded funded fiber integral
field unit (``6-Pak") for WIYN. The cable will be completed and
installed on WIYN during the upcoming year. As part of this
instrumentation effort, Bershady is developing a throughput
enhancement of the WIYN Bench Spectrograph. A second IFU cable
(``Spider") for the Hobby-Eberly Telescope's Medium Resolution
Spectrograph is completed and awaits installation. These instruments
are unique in their high delivered etendue (7-10 m$^2$ arcsec$^2$) and
spectral resolutions (up to R = 10000). They are designed for study
of the dynamics of spiral disks of external galaxies.

\subsection{SALT}

Wisconsin will lead the effort to contribute the first major SALT
facility-class instrument, the Prime Focus Imaging
Spectrograph. Nordsieck (PI) is working on its design. It will
specialize in very high throughput with low and medium spectral
resolution (R = 500 - 13000), plus spectropolarimetry from 3200 to
9000 \AA, using an articulated camera and Volume Phase Holographic
gratings and a double etalon Fabry-Perot system. With a peak
efficiency above 65\% and a 3200 \AA\ efficiency above 30\%, it will
be unique among or superior to existing 8-10m telescopes in the UV, in
medium resolution spectroscopy, in Fabry-Perot spectroscopy, and in
spectropolarimetry. The instrument will be integrated at the
University of Wisconsin - Madison Space Astronomy Lab. The Fabry-Perot
system will be supplied by Rutgers and the detector system by South
African Astronomical Observatory. Commissioning is currently targeted
for late 2003.

\subsection{Other instruments}%%%%%%
Percival released the new Java-based remote observing package that
integrates {\bf Progressive Image Transmission} for large images with
a remote engineering data system targeted for low-bandwidth
connections to the observatory.

Percival, K. Jaehnig, D. Michalski, and S. Gabelt finished the design
of the {\bf advanced star tracker}, the ST5000, that provides pitch,
yaw, and roll control for sounding rockets. It can also do a full
``lost in space" attitude determination without gyros for both
sounding rockets and satellites. The WISP flight of Nordsieck (see
\S\ref{ism}), its first test, was a complete success. The instrument 
is being considered as a replacement for the Ball ``STRAP" star
tracker that has been standard for sounding rockets since the 1970's.

Nordsieck's {\bf halfwave polarimeter (HPOL)} resided on the 0.9m
telescope at Pine Bluff Observatory during most of this time period,
traveling to the 3.5m WIYN telescope in September 2000. HPOL obtained
415 observations of 134 distinct targets (including 7 nights at WIYN)
between Oct 1, 1999 and Sept 30, 2000. Specific areas of interest are:
interacting binaries, Be stars, ISM probes, AG Dra, Ae/Be stars, and
LRV stars. Broadband polarimetric results of HPOL observations are
listed on the HPOL website: www.sal.wisc.edu/HPOL

Nordsieck, Jaehnig, and Harris are continuing development of the {\bf
Far-Ultraviolet SpectroPolarimeter (FUSP)}, a sounding rocket payload
that will obtain the first high-precision spectropolarimetry from 1050
- 1500 \AA, and the first astronomical polarimetry of any kind below
1300 \AA. FUSP will provide measurements of polarization produced by
electron scattering, resonance line scattering, and hydrogen Rayleigh
scattering in the inner circumstellar environment of hot stellar
systems, and thereby quantitatively constrain the geometry and
dynamics of the system. In addition, the strength and geometry of the
magnetic field will be determined from a new diagnostic tool, the
Hanle Effect. The telescope is F/2.5 prime-focus with a 50 cm
primary. At the telescope focus is the polarimetric optics, a stressed
lithium flouride rotating waveplate, followed by a diamond
Brewster-angle mirror. The spectrometer uses an aber\-ration-corrected
spherical holographic grating and a UV-sensitized CCD detector. The
spectral coverage is 1050 - 1500 \AA, the spectral resolution is 0.65
\AA. The net spatial resolution is about 1\arcmin\ perpendicular to
the dispersion. The first flight is planned for late 2001, targeting
the Be star Zeta Tau and the unpolarized standard $\beta$ Tau.

Harlander (St Cloud State), Roesler (Physics Dept), and Reynolds have
continued the development of a {\bf Spatial Heterodyne Spectrometer}
for observations of faint diffuse [O II] 3727 emission from the warm
ionized component of the interstellar medium.

\noindent {\bf Far-Ultraviolet Spectrographic Explorer (FUSE)}. Savage
is a Co-Investigator for the FUSE satellite which was launched in June
1999. FUSE is a dedicated UV spectroscopy mission operating in the 905
to 1187 \AA\ region at a spectral resolution of $\sim$20,000. Savage's
principal observational program with FUSE involves measurements of O
VI absorption produced by the hot interstellar medium of the Milky Way
disk and halo. The goal is to study the distribution and kinematics of
O~VI in order to gain insights about the origin(s) of the hot gas in
the interstellar medium. During its first 16 months of operation, FUSE
has provided a wealth of information about stars, the ISM, the IGM,
and extragalactic sources. The 2000 July 20 issue of ApJ Letters
contains 22 papers reporting initial FUSE results. Although FUSE was
designed to be a three year mission, NASA has recently agreed to
provide the funding that will allow FUSE to be operated for five
years.

\noindent The {\bf Cosmic Origins Spectrograph (COS)} will be installed
on the Hubble Space Telescope in 2003. Savage is a Co-Investigator on
the COS science team with J. Green ( U. Colorado) serving as the
Principal Investigator. COS is a very high efficiency spectrograph
designed to operate from 1150 to 3200 \AA\ at a spectral resolution of
22,000. In the Far-UV COS is approximately 15 times more efficient
than STIS and will be used for a wide range of spectroscopic studies
of faint galactic and extragalactic objects. Savage's observational
studies with COS will involve the origin of hot gas associated with
galaxy groups and galaxy halos. These studies will be pursued through
absorption line observations of highly ionized ions in the UV spectra
of QSOs. Species to be studied include O~IV, O~V, O~VI, Ne~V, Ne~VI,
Ne~VIII, Mg~X and Si~XII.



\section{Teaching and Outreach}%%%%%%

The College Level-1 Institute (Mathieu, Director) within the National
Institute of Science Education (Mathieu, Associate Director) completed
the Learning Through Technology website. All of the CL-1 products can
be found at the website www.wcer.wisc.edu/nise/cl1/.

The ``Universe in the Park" program (Wilcots, director), now in its
fifth year, is predicated on the idea that the best environment in
which to introduce the general public to astronomy is outside, under
dark skies. The program takes place in state parks throughout
Wisconsin during the summer and fall camping seasons. It consists of
talks and slide shows, question sessions, and providing the general
public a view astronomical objects through one of the program's
telescopes. During the 2000 season there were 43 sessions in 27 state
parks from the end of May to the middle of October, as well as Scout
camps and Camp MASH, a summer camp for arthritic children. We have
involved several members of the faculty, staff, and students, both
graduate and undergraduate.

Hoffman was named a Teaching Fellow by the UW-Madison College of
Letters and Science, and conducted workshops at a college-wide
teaching assistant training session.

\section{Publications}%%%%%%

Andersen, D.R., Bershady, M.A., Sparke, L.S., Gallagher~III, J.S.,
Wilcots, E.M. 2000, ``The Measurement of Disk Elongation in Nearby
Disk Galaxies," submitted to ApJ Lett

Barnes, S. A., 2000, ``Rotation periods of cluster stars'', in
``Stellar Clusters and Associations: Convection, Rotation and
Dynamos'', ed. R. Pallavicini, G. Micela and S. Sciortino, ASP
Conf. Series, vol 198 (San Francisco: ASP Press), 319

Barnes, S. A., Sofia, S., \& Pinsonneault, M. H., 2001,
``Disk-locking and the presence of Slow Rotators among Solar-Type
Stars in Young Star Clusters'', ApJ, 20 Feb2001 issue

Bershady, M. A., Jangren, A., Conselice, C. J. 2000, ``Structural and
Photometric Classification of Galaxies -- I. Calibration Based on a
Nearby Galaxy Sample," AJ, 119, 2645

Bershady, M. A. 2000, ``Galaxy Form and Spectral-Type: A Physical
Framework for Measuring Evolution," Astrophysics \& Space Science,
269-270, 183

Bland-Hawthorn, J. and Reynolds, R. J., ``Gas in Galaxies", in {\it
Encyclopedia of Astronomy and astrophysics}, ed. P. G. Murden (IOP
Publishing and Macmillan), in press

Bouche, N., Lowenthal, J.D., Charlton, J.C., Bershady, M.A.,
Churchill, C.W., Steidel, C.C., 2000,``H-alpha Imaging with HST +
NICMOS of an Elusive Damped Ly-alpha Cloud at z = 0.6'', ApJ,
submitted

Brandt, J.C. et al. (incl. B. D. Savage) 2000, ``Goddard High
Resolution Spectrograph Observations of NGC~4151", AJ, in press

Brandt, W.N., \& Gallagher, J.S. 2000, ``Observational Similarities
and Potential Connections Between Luminous Ultrasoft NLS1s and
BALQSOs'', New Astronomy Reviews, in press

Brown, J.C., Ignace, R. and Cassinelli, J.P. 2000, ``Hot Star
Polarimetric Variability and the Nature of Wind Inhomogeneities",
A\&A, 356, 619

Callaway, M.B., Savage, B.D., Benjamin, R.A., Haffner, L.M., \& Tufte,
S. L. 2000, ``Observational Evidence of Supershell Blowout in GS
018-04+44", ApJ, 532, 943.

Cassinelli, J. P. \& MacGregor, K. B. 2000, ``The Dynamics of Flux
Tubes in the Radiative Interiors of Hot Stars", in IAU Coll. 175, {\it
The Be Phenomenon in Early Type Stars}, eds. M.A. Smith, H.F. Henrichs,
J. Fabregat (San Francisco, ASP), 337

Churchwell, E. 2000, ``Massive Star Formation: New Results", in
{\it Proc. IAU General Assembly, Joint Discussion 3}, in press

Cohen, D.H., Cassinelli, J.P., MacFarlane, J.J., \& Owocki, S.P.
2000, ``EUV/X-ray Emission and the Thermal and Ionization Structure of
B star Winds'', in {\it Thermal and Ionization Aspects of Flows from
Hot Stars: Observations and Theory}, ASP Conf Ser. 204, ed. H.J.G.L.M.
Lamers \& A. Sapar (San Francisco, ASP), 65

Cole A.A., Smecker-Hane, T.A., \& Gallagher, J.S. 2000, `` The
Metallicity Distribution Function of Red Giants in the LMC'',
AJ, 120, 1808

Conselice, C. J., Bershady, M. A., \& Jangren, A. 2000, ``The Symmetry
of Galaxies: Physical Morphology for nearby and High Redshift
Galaxies,'' ApJ, 529, 886

Conselice, C. J., Bershady, M. A., \& Gallagher, J. S., III. 2000,
``Physical morphology and triggers of starburst galaxies", A\&A,
354, L21

Conselice, C.J., Gallagher, J.S., Calzetti, D., Homeier, N., \&
Kinney, A. 2000, ``Panchromatic Study of Nearby Ultraviolet-bright
Starburst Galaxies: Implications for Massive Star Formation and
High-Redshift Galaxies'', AJ, 119, 79

Cox, A.L., Sparke, L.S., Watson, A.M., \& van Moorsel, G. 2001,
``Stars and Gas in the Galaxy Pair II Zw 70/71", AJ, in press

Dayal, A., et al. (incl. J.S. Gallagher). 2000, AJ, 119, 315

de Grijs, R., O'Connell, R. W., Becker, G.D., Chevalier, R.A., \&
Gallagher, J.S. 2000, ``Supernova Remnants in the Fossil Starburst in
M82''. AJ, 119, 681

De Gouveia Dal Pino, E. \& Lazarian, A. 2000,
``Ultra-high-Energy Cosmic-Ray Acceleration by magnetic reconnection
in newborn ac\-cretion-induced collapse pulsars'', ApJ, 536, L31

de Oliveira-Costa, A., Tegmark, M., Devlin, M.J., Haffner, L.M.,
Herbig, T., Miller, A.D., Page, L.A., Reynolds, R.J., and Tufte, S.L.,
``Galactic Contamination in the QMAP Experiment", ApJ(Lett), in press

Dickinson, M. plus 9 co-authors,
Bershady, M. A., Conselice, C., Ferguson, H., Fruchter, A. 2000,
``The Unusual Infrared Object HDF-N J123656.3+621322,'' ApJ, 531, 624

Dolan, C.J., \& Mathieu, R.D. 1999, ``A WIYN Lithium Survey for Young
Stars in the $\lambda$ Orionis Star-Forming Region'', AJ, 118, 2409

Dolan, C.J., \& Mathieu, R.D. 2000, ``The Spatial Distribution of the
$\lambda$ Orionis Pre-Main-Sequence Population'', AJ, in press

Efroimsky, M., Lazarian, A. 2000, ``Inelastic relaxation in tumbling
asteroids and comets'', {\it MNRAS}, 311, 269-278

Ferguson, A.M.N., Gallagher, J. S., \& Wyse, R.F.G. 2000, ``On the
Nature of Andromeda~IV'', AJ, 120, 821

Greiner,J.,Schwarz, R., Zharikov, S., \& Orio, M. 2000, ``RX
J1420+5334 -- another tidal disruption event?'', A\&A (Lett.), in
press (astro-ph 0009430)

Greiner, J., Orio, M., \& Schwarz, R. 1999, ``The shortest-period
supersoft X-ray source'', A\&A, 355, 1041

Haffner, L.M. "The Wisconsin H-Alpha Mapper Northern Sky Survey", ASP
Conference Series, in press

Haffner, L.M., Reynolds, R.J., and Tufte, S.L., 2000, ``The Wisconsin
H-alpha Mapper: A New Look at the Warm Ionized Medium", Rev. Mex. A\&A
(Conf. Proceedings), 9, 335, 2000.

Harries, T.J., Babler, B.L., \& Fox, G. K. 2000, ``The polarized
spectrum of the dust producing Wolf-Rayet+O-star binary WR137" A\&A,
361, 273.

Heiles, C., Haffner, L.M., Reynolds, R.J., and Tufte, S.L. 2000,
``Physical Conditions, Grain Temperatures, and Enhanced Very Small
Grains in the Barnard Loop", ApJ 536, 335

Hoffman, J.L., Whitney, B.A. \& Nordsieck, K.H. 2000, ``The Be
Phenomenon in Early-Type Stars'', in IAU Colloq. 175, ed. M. Smith,
H. Henrichs \& J. Fabregat, ASP Conf 214 (San Francisco: ASP)

Hofner, P., Wyrowski, F., Walmsley, C. M., \& Churchwell, E. 2000,
``A C17O Survey toward Ultracompact HII Regions", Ap. J., 536, 393

Holtzman, J.A., Gallagher, J.S., et al. 1999, ``Observations and
Implications of the Star Formation History of the Large Magellanic
Cloud'', AJ, 118, 2262

Howk, J., Cassinelli, J.P., Bjorkman, J.E., \& Lamers,
H.J.G.L.M. 2000, ``Stagnation and Infall of Dense Clumps in the
Stellar Wind of $\tau$ Scorpii", ApJ, 534, 348

Howk, J.C., \& Savage, B.D. 2000, ``The Multiphase Halo of NGC~891: WIYN
H-alpha and BVI Imaging", AJ, 119, 644

Howk, J.C., Savage, B.D., \& Fabian, D. 1999, ``Abundances and Physical
Conditions in the Warm Neutral Medium Towards Mu Columbae", ApJ,
525, 253

Howk, J.C., Sembach, K. R., \& Savage, B. D. 2000, ``The Abundance of
Interstellar Boron", ApJ, in press

Hunter, D.A.,O'Connell, R.W., Gallagher, J.S., \& Smecker-Hane, T.A.
2000, ``The Star Clusters in the Starburst Irregular Galaxy \\
NGC~1569'', AJ, November.

Hunter, T., Churchwell, E., Watson, C., Cox, P., Benford, D.J., \&
Roelfsema, P.R. 2000, ``350 $\mu$m Images of Massive Star Formation
Regions", AJ, 119, 2711.

Jangren, A., Bershady, M. A., Conselice, C., Koo, D. C., Guzman,
R. 1999, ``Structural and Photometric Classification of Galaxies --
II. Application to Luminous Blue Compact Galaxies at Intermediate
Redshift," submitted to AJ

Lagache, G., Haffner, L.M., Reynolds, R.J., \& Tufte, S.L. 2000,
``Evidence for Dust Emission in the Warm Ionised Medium Using WHAM
Data", A\&A, 354, 247

Lagache, G., Puget, J.-L., et al. (incl. Rey\-nolds, R.J.) 2000, ``The
Extragalactic Background and its Fluctuations in the Far-Infrared
Wavelengths", in proceedings of the Ringberg Castle Conference {\it
ISO Surveys of a Dusty Universe}, in press

Lazarian, A., \& Pogosyan, D. 2000, ``Velocity modification of HI
power spectrum'', ApJ, 537, 720

Lazarian, A. \& Draine, B.T. 2000, ``Resonance paramagnetic relaxation
and alignment of small grains'', ApJ, 536, L15

Lazarian, A. 2000, ``Physics of Grain Alignment'', in {\it Cosmic
Evolution and Galaxy Formation}, ed. J. Franco, ASP, in press

Lazarian, A. \& Vishniac, E. 2000, ``Fast Reconnection of Magnetic
Fields in Turbulent Fluids'', Rev. Mex. Astr. Astrofis.,
9, 55-62

Lazarian, A. 1999, ``Statistics of Turbulence from Spectral-Line Data
Cubes'', in ``Plasma Turbulence and Energetic particles", eds. Michal
Ostrowski \& Reinhard Schlickeiser, Cracow, p. 28-47

Li, Q., Brown, J.C., Ignace, R., Cassinelli, J.P., \& Oskinova, L.M.
2000, ``Wolf-Rayet wind structure and optical variability'', A\&A,
357, 233.

Maciejewski, W., \& Sparke, L.S. 2000, `` Orbits supporting bars
within bars'', MNRAS, 313, 745

Magalh\~{a}es, A.M. \& Nordsieck, K.H. 2000, ``Asymmetries
around Luminous Red Variables", in {\it The Carbon Star
Phenomenon}, ed. R.F.Wing, (Dordrecht:Kluwer), 433

Matheson, T., 4 co-authors, Bershady, M. A., et al. 2000, ``Optical
Spectroscopy of Supernova 1993J During Its First 2500 Days," AJ, 120,
1487

Mathieu, R.D., 2000, ``Assessment Tools to Drive Learning: FLAG, SALG,
and Other Proven Assessments Available Online'', in {\it Targeting
Curricular Change: Reform in Undergraduate Education in Science, Math,
Engineering, and Technology}, Annals Amer. Higher Education, in press

Mathieu, R.D. 2000, ``Pre-Main Sequence Binary Stars'', in {\it
Encyclopedia of Astronomy and Astrophysics}, ed. Emerson, in press

Mathieu, R.D., 2000, ``The WIYN Open Cluster Study'', in {\it Stellar
Clusters and Associations: Convection, Rotation and Dynamos}, ed. R.
Pallavicini, G. Micela \& S. Sciortino (San Francisco: ASP Press), 517

Mathieu, R.D., Ghez, A., Jensen, E.L.N., \& Simon, M., 2000, ``Pre-Main
Sequence Binary Stars'', in {\it Protostars and Planets IV}, ed. V.
Mannings, A.P. Boss and S.S. Russell (Tucson: U. of Ariz. Press), 703

Mathis, J. S. 2000, ``Properties of interstellar dust'',
J. Geophys. Res., 105, 10269

Mathis, J. S. 2000, ``The Warm Ionized Medium in the Milky Way and Other
Galaxies'', ApJ, in press

Matthews, L.D., Gallagher, J.S., \& van Driel, W. 1999, ``The
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