Download FY1995 Q1 Oct-Dec NO.. - National Optical Astronomy Observatory

NATIONAL
OPTICAL
ASTRONOMY
OBSERVATORIES
NATIONAL OPTICAL ASTRONOMY OBSERVATORIES
QUARTERLY REPORT
OCTOBER - DECEMBER 1994
March 6, 1995
TABLE OF CONTENTS
I.
INTRODUCTION
1
II.
SCIENTIFIC HIGHLIGHTS
1
A.
1
Cerro Tololo Inter-American Observatory
1.
B.
C.
CN and CH Abundance Variations in Globular Cluster Turnoff Stars and
Implications for Stellar Evolution and Star Formation
1
2.
Detection of Lens Candidates for the Double Quasar Q2345+007
2
3.
The Lithium Abundance in M67 and Implications for Stellar Evolution and Cosmology
2
Kitt Peak National Observatory
3
1.
Color Evolution of Galaxies
3
2.
Kinematics of Brightest Cluster Galaxies
4
3.
Evolution of the Infrared Spectrum of an ONeMgNova
5
National Solar Observatory
6
1.
High Temperature Coronal Regions Follow Solar Ring Current
6
2.
Scattering of P-Modes by Localized Inhomogeneities
7
3.
Detection of Intrinsically Weak Solar Disk Magnetism
8
III. US GEMINI PROGRAM
IV. PERSONNEL AND BUDGET STATISTICS, NOAO
9
10
A.
Visiting Scientists
10
B.
Hired
10
C.
Completed Employment
10
D.
Changed Status
10
E.
Gemini 8-m Telescopes Project
11
F.
Chilean Economic Statistics
11
G.
NSF Foreign Travel Fund
11
Appendices
Appendix A: Telescope Usage Statistics
Appendix B: Observational Programs
Appendix C: Safety Report
I. INTRODUCTION
This document covers scientific highlights and personnel changes for the period 1 October - 31 December 1994.
Highlights emphasize concluded projects rather than work in progress. The NOAO Newsletter Number 41
(March 1995) contains information on major projects, new instrumentation, and operations. The appendices to
this report summarize telescope usage statistics and observational programs.
H. SCIENTIFIC HIGHLIGHTS
A. Cerro Tololo Inter-American Observatory
1. CN and CH Abundance Variations in Globular Cluster Turnoff Stars
and Implications for Stellar Evolution and Star Formation
Globular clusters are typically characterized by a single abundance of heavy metals: the fraction of heavy
elements compared to hydrogen is constant from star to star. This suggests that the cluster formation was rapid,
occurring in less than the characteristic time for heavy metal enrichment by Type II supernovae. (In fact, the
energetics of these supernovae may have been responsible for clearing the gas from the early clusters, thus
ending the star formation process in these systems.) It has long been known, however, that the abundances of
light elements, such as carbon (C) and nitrogen (N), vary substantially from star to star within a cluster. These
results are based on observations of the bright red giant stars in these clusters. Two scenarios have been put
forward to explain these variations. The first involves deep convection, in which material processed by the
nuclear reactions near the core of a star is dredged up to the star's surface; the activity of this process varies
from star to star, resulting in the light-element abundance variations in stars' spectra. The second possible
explanation invokes a "primordial" cause, such as enrichment of the intra-cluster gas and later-forming stars by
the stellar winds of the earliest-formed, high-mass stars. Enrichment would have occurred before a cluster was
swept clean of gas by supernova detonations.
Aluminum (Al) and sodium (Na) abundances also are observed to vary from star to star in some clusters. This
was taken as strong evidence for a primordial cause until Langer et al. (1993) showed that nuclear reactions
involving Al and Na can take place in the hydrogen-burning shells of some red giant stars. Thus observations of
less-evolved stars are required to determine which of the two processes are responsible for the observed C and N
variations. During the 1980's, several studies were made of the CN and CH features of main sequence turnoff
(MSTO) stars in the nearby globular cluster 47 Tuc. These studies employed single-slit spectrographs, however,
so the numbers of stars in the samples were small. The studies showed that CN and CH variations do appear at
the MSTO, but did not reveal whether the proportions of CN-strong and CN-weak stars mimic those seen among
the red giants.
M.M. Briley (U. of Texas, Austin), J.E. Hesser (Dominion Astrophys. Obs.), R.A. Bell (U. of Maryland), M.
Bolte, and G.H. Smith (UC Santa Cruz) used the Argus multi-fiber spectrograph at the CTIO 4-m telescope to
observe 24 stars near the MSTO in 47 Tuc. The work is published in the December, 1994, issue of the
Astronomical Journal. The observers obtained spectral indices for the CN feature at 3839 A and for the CH
feature at 4300 A. They found a broad range in CN and CH strengths at a given stellar temperature, thus
confirming previous studies of MSTO stars. By comparing their observed indices with those derived from model
atmospheres, they determined that the observed range in CN strengths was larger than could be produced by
dredge-up of processed material with C > N, and that a large fraction of the atmosphere must have undergone
O > N cycling as well. The range of observed CH strengths also mimics that seen in the red giants, and the dwarf
stars show a CN-CH anti-correlation, as do the giants. The observers therefore argue that at least some
component of the abundance variations on the giant branch cannot be explained by processes occurring during
the giant branch evolutionary phase. They were able to rule out several scenarios for explaining the observed
variations: surface accretion of N-rich material ejected from higher-mass cluster members in the past, mass
transfer from other more-massive cluster stars during stellar interactions, and mixing via meridional circulation
in the stellar interior. They conclude that the abundance variations are most easily explained as having existed
from near the time of cluster formation. Perhaps gas enhanced in N and depleted in C was expelled from moremassive stars into the interstellar medium, and then condensed into new stars before the cluster gas was swept
out by the first supernovae.
2. Detection of Lens Candidates for the Double Quasar Q2345+007
The object called Q2345+007 AB is actually a pair of quasars that appear to lie about 7" apart on the sky. The
two components (A and B) have very similar spectra and redshifts (z = 2.15), raising the possibility that the pair
is part of a gravitationally lensed system. Such a system would consist of a single quasar that appears double (or
multiple) because an object between Earth and the quasar causes the light from the quasar to be bent. Deep
searches have failed to detect the object responsible for the lensing of Q2345+007, however. If the system is not
part of a gravitational lens, then the presence of two physically associated quasars at high redshift may indicate
that clustering was occurring at this epoch.
P. Fischer, J.A. Tyson (Bell Labs), G.M. Bernstein (U. of Arizona), and P. Guhathakurta (STScI) combined
images from the CTIO 4-m Prime Focus CCD with images from other telescopes to produce a B-band image of
over 13 hours integration time, and an R-band image of nearly 9 hours integration time. They used point-spreadfunction fitting routines to subtract the light of the quasar pair, and found a faint galaxy (B = 25 mag) about 1.5
arcsec from the B image, nearly on a line between the A and B images. They also detected a large number of
faint galaxies scattered over the rest of the image. There were several enhancements in the surface density
distribution of these galaxies, one of which lay near the quasar pair. The authors suspect that the latter represents
a cluster of galaxies, perhaps at z = 1.5, the redshift at which absorption-line systems are seen in the spectra of
the quasars.
Assuming that Q2345+007 is a lensing system, Fischer et al. constructed lensing models involving the faint
galaxy near component B and the suspected cluster. Though the solution was not uniquely determined, they
found several combinations of parameters which reproduced the positions and relative brightnesses of the two
quasar components. Thus they suggest that Q2345+007 is an example of a gravitationally lensed system. They
further suggest that the slight color difference between components A and B (0.13 mag; a lensing event should
be achromatic) might be due to differential reddening along the lines of sight, or to variability of the quasar
compounded by the time delay along the two different light paths. The authors point out that presence of a large
cluster (the lens models indicate a mass of 1013 solar masses) at z = 1.5 is less likely in dark matter (Q. = 1)
models of the Universe than in open (£2 = 0.2) models. The work is published in the August 20, 1994, issue of
the Astrophysical Journal Letters.
3. The Lithium Abundance in M67 and Implications for Stellar Evolution
and Cosmology
An accurate determination of the primordial abundance of lithium (Li) places important constraints on models of
Big Bang nucleosynthesis and on the baryon density of the Universe. Determinations from meteorites suggest
A(Li) = 3.31 (on a logarithmic scale where A(hydrogen) = 12), yet observations in stars indicate the primordial
value may be lower. Li can be produced or depleted in a variety of ways. In particular, if surface convection in a
star is deep enough, Li will be mixed down to a layer where it is burned, and the surface abundance of Li will
appear low in that star. Studies of star clusters of different age show that Li is conserved in a narrow range of
effective temperatures, thus forming the "Li peak." The Li abundance in stars within the peak slowly drops with
age: A(Li) = 3.1 in the Pleiades (80 Myr), 2.9 in the Hyades (700 Myr), and 2.5 in M67 (5 Gyr). In halo dwarfs,
the Li peak lies at A(Li) = 2.5 as well.
Standard stellar models cannot reproduce this behavior, yet models which include rotationally-induced mixing
are more successful. This mixing is strongly supported during the time when a star is spinning down, during its
late pre-main sequence and early main sequence life. Another way to test the rotationally-mixed models is to
measure Li abundances of stars which are not expected to undergo spin down: short-period, tidally-locked
binaries (SPTLBs).
C.P. Deliyannis (U. of Hawaii), J.R. King (U. of Texas), A.M. Boesgaard (U. of Hawaii), and S.G. Ryan
(Anglo-Australian Observatory) used the CTIO 4-m telescope with the echelle spectrograph to observe the weak
Li line at 6708 A in a SPTLB in M67. Both components of this binary system have temperatures coincident with
the Li peak. The observers find A(Li) = 2.9-3.0 for both components, significantly larger than the Li abundances
of the single stars in the cluster. They take this as strong evidence that the rotationally-mixed stellar models are
on the right track. They note that even SPTLBs may not preserve their initial Li abundances intact. Some spin-up
or spin-down may occur as the stars' orbits are circularized, with the consequent mixing and Li depletion. Thus,
the initial Li abundance for M67 was at least 3.0. Galactic Li enrichment places another roadblock in the path of
determining the primordial Li abundance via stellar Li abundances. The material that later formed M67 might
have been enhanced in Li over its primordial Li abundance. Thus the observers stress the need to find and
measure the Li abundance of SPTLBs in the Galactic halo, where the history of the pre-stellar interstellar
medium is shorter. The work appeared in the October 20, 1994, issue of the Astrophysical Journal Letters.
B. Kitt Peak National Observatory
1. Color Evolution of Galaxies
The color of a galaxy, observed by measuring the galaxy's spectrum, is the sum of the colors of the individual
stars in the galaxy. A recent burst of active star formation produces a subpopulation of massive blue stars that
dominate the blue and near-ultraviolet light of the integrated spectrum. An initial burst of global star formation
followed by a long period of passive evolution of the stellar population produces a spectrum dominated by stars
on the red giantbranch and the main-sequence turn-off. A series of intermediate-age bursts will produce a mixed
stellar population, with properties interpreted through model spectral synthesis. By observing many galaxies at
different redshifts, we can study the history of star formation in galaxies, since looking back to higher redshifts
means observing galaxies as they were in the past. The study of the color evolution of galaxies, or change in
color with time, can also provide information about the ages and metal content of galaxies.
In order to study the rate and nature of color evolution of distant galaxies, K. Rakos (U. of Vienna) and J.M.
Schombert (IPAC) carried out an imaging program for ten clusters of galaxies using the KPNO 4-meter
telescope and the Prime Focus CCD Camera. Their results are reported in the Astrophysical Journal of Jan. 20,
1995. In order to measure the spectra of galaxies in the clusters, the researchers used an extensive set of filters
constructed to mimic the Stromgren intermediate band system in the rest frame of each redshifted cluster. By
observing the galaxies' colors with the redshifted filters, Rakos and Schombert were able to observe each galaxy
at the same rest wavelengths, so that the spectra of the galaxies could be compared. Those filters measure the
Balmer continuum (uz), the Paschen continuum in blue and green (bz and yz), and the absorption-rich region just
longward of the blanketing break, centered at 4100 A (vz). The filters avoid all strong emission lines. The
sample of galaxy clusters was chosen from the Gunn-Hoessel-Oke catalog of distant clusters, identified from
photographic plates by their surface density contrast, and confirmed by spectroscopic redshifts.
The major phenomenon Rakos and Schombert measured was the Butcher-Oemler effect, the increasing fraction
of blue cluster galaxies with increasing cosmic look-back time, or redshift. That fraction was consistently
defined by application of the bz-yz or vz-yz indices to identify objects bluer than the E/SO restframe colors.
They found that the blue fraction increases from about 20% at z = 0.4 to 80% at z = 0.9. This strong trend
suggests that all galaxies with disks or high gaseous surface densities were involved in star formation at redshifts
around z= 1. The colors of the Butcher-Oemler population suggest ongoing star formation or post-starburst
populations (E+A galaxy spectral type). Interpreting the colors with spectral synthesis models points to a
formation epoch for the blue population around z = 2 or 3.
The interpretation of the blue population is problematic, because the fraction of blue galaxies at high redshift is
much greater than that observed now. The blue galaxies cannot be converted to red galaxy types, such as
ellipticals or SOs, and do not share the latter's morphological properties. The authors propose that the population
of Butcher-Oemler (blue) objects consists of low surface brightness galaxies undergoing episodes of pressureinduced star formation as they undergo infall into their clusters. This population fades with time, and is later
destroyed by the cluster tidal field while the older, more massive systems survive.
The colors of the red galaxies are consistent with initial burst and quiet evolution of ellipticals, including a red
color peak at z~0.4. The vz-yz metallicity index is bluer than the models predict, suggesting the need for
including more metal-poor stars in the old population in galaxy models. The oldest (reddest) galaxies seem to
have formation redshifts of z~10. That early epoch is a challenge to structure formation theories. Since the mean
colors suggest an epoch of formation of z~5, ellipticals in clusters were probably not formed at the same time as
the other galaxies.
The combination of imaging from HST with high angular resolution, intermediate-band imaging as in this paper,
and selected spectroscopy with very large aperture ground-based telescopes holds the promise for progress in
understanding the complex problem of the evolution of galaxies and their stellar populations.
2. Kinematics of Brightest Cluster Galaxies
Many rich clusters of galaxies contain a brightest cluster galaxy (BCG), an elliptical galaxy that is larger and
brighter both than other galaxies within the cluster and any galaxies found outside of clusters. A variety of
formation mechanisms have been proposed for brightest cluster galaxies. One model assumes continuing mergers
that lead to a progressive build-up of the central galaxy in a cluster as smaller galaxies are tidally disrupted. An
alternative involves some merging, but depends primarily on formation during cluster collapse, with little
subsequent evolution. A third possibility is mass accretion from x-ray cooling flows, which are observed to
occur in many clusters; the accumulation in the central potential would build up the mass of the central brightest
cluster galaxy with time.
To discriminate among the formation models, detailed information about the motions of stars in the brightest
cluster galaxies is needed. D. Fisher and G. Illingworth (Lick Obs.) and M. Franx (U. of Groningen) have
obtained and analyzed long-slit spectra of a sample of 13 brightest cluster galaxies, and compared them to a
larger sample of less luminous ellipticals. They reported their results in the 10 January 1995 Astrophysical
Journal. The spectra were obtained mostly with the Cryogenic Camera on the KPNO 4-m telescope. The authors
used a Fourier fitting technique to derive spatially resolved velocity centroids and dispersions by use of a
normalized stellar template.
They found that, with one previously-observed exception, the velocity dispersions decreased outward from the
centers of the galaxies with a shallow gradient, similarly to other bright ellipticals. Taken in conjunction with the
finding that brightest cluster galaxies fit relations among other physical properties for normal ellipticals (the
"fundamental plane"), the authors suggest that BCGs and ellipticals share similar histories.
Only two of the 13 brightest cluster galaxies showed appreciable central rotation. The BCG sample continued a
trend indicated in the larger sample of normal ellipticals: the higher the intrinsic luminosity, the lower the
rotational velocities measured for the galaxy. The two galaxies in the sample with well established rotation were
at the low luminosity end, and fell within the locus of the normal ellipticals. Similarly, the brightest cluster
galaxies with the lowest level of rotational relative to random velocities lie in the clusters with the highest cluster
velocity dispersions. The latter result should not be surprising given the strong correlation between absolute
luminosity of the brightest cluster galaxy and cluster velocity dispersion. In general, the brightest cluster galaxies
were not consistent with being rotationally flattened prolate or oblate spheroids, suggesting that further
investigations of the degree of triaxiality would be profitable.
The unique aspects of these BCGs relative to other ellipticals are therefore their extremely low level of rotational
support, and the extent of their extremely extended stellar envelopes. The derived mass-to-light ratios showed a
large scatter when plotted against quantities such as the dispersion gradient, the degree of rotational support, the
absolute luminosity or the cluster mass accretion rate inferred from x-ray cooling flows. Other studies have
indicated evidence for increasing M/L with increasing mass accretion rate, a trend consistent with but not
confirmed by the data presented in this paper. If verified, that trend would indicate a significant coupling
between mass inflow and the dynamical and physical properties of the brightest central galaxies.
Ongoing mergers in the central potential of a cluster are expected from the density of galaxies in a cluster. The
existence of a counter-rotating core observed in NGC 4073 further supports the idea that mergers play a role in
the development of BCGs. Further work in this area will push the observations of the extended envelopes of
BCGs to determine the dynamical state of the extended stellar component.
3. Evolution of the Infrared Spectrum of an ONeMg Nova
Nova explosions are the result of a thermonuclear runaway reaction on the surface of a white dwarf that is
accreting material from a close companion star. After the detonation, a shell expands from the white dwarf. The
shell is optically thick, and appears as an expanding pseudo-photosphere. As the shell becomes optically thin, the
nova spectrum becomes dominated by free-free continuum emission and recombination lines of hydrogen and
helium, which diminish in intensity as the shell evolves. After this period, many novae exhibit a coronal line
phase, with emission of near-infrared forbidden line features from heavy elements.
The nature of the coronal spectrum depends partially on the composition of the accreted material and partially on
the composition of the white dwarf. The composition of the white dwarf depends on the degree of processing of
material during the helium flash phase of the progenitor star. White dwarfs can therefore be made of helium, if
the processing stops after helium formation, or of iron, if processing continues as far as possible. In the case of
an intermediate stage of processing, the white dwarf will contain a mixture of oxygen (O), neon (Ne), and
magnesium (Mg). The spectra of ONeMg novae are unique in showing strong permitted magnesium emission,
along with forbidden neon lines. Abundance analyses of their ejecta typically show enhancements of oxygen,
neon, aluminum and magnesium over their solar ratios relative to hydrogen. Observational monitoring of novae
is required to identify the thermonuclear processes at work in the explosion, the composition of the white dwarf
primaries, and the physical conditions in the ejecta and the nova environment into which the material expands.
In the 10 January 1995, issue of the Astrophysical Journal, C.E. Woodward (U. of Wyoming) and colleagues,
including R.R.Joyce (KPNO), report on near-infrared spectroscopy of Nova Cygni 1992. The spectra were
obtained primarily with the Cryogenic Spectrometer (CRSP) on the KPNO 2.1-m telescope. The nova outburst
occurred on 19 February 1992; the KPNO spectra were obtained from March 1992, through June 1993. The
nova showed spectral similarities to QU Vulpeculae, the archetype of the ONeMg novae. It faded slowly while
producing little dust, making it suitable for an extended spectral monitoring program.
The spectral lines observed in the nova included hydrogen and helium recombination lines; permitted lines of
oxygen and nitrogen; and infrared coronal lines of [Al VI], [Al VIII], [Ca IV], [Mg VIII], and newly-identified
features of [S FX] and [Ca FX]. By using ratios of strengths of features from successive ionization states in the
same element (for example, forbidden Si VI and VII), the authors determined the temperature and density of the
emitting gas. With ranges for those parameters, abundance ratios were then derived. They found that the Al/Si
ratio is about five times the solar abundance ratio, while the Mg/Si ratio is at least three times solar. At the same
time, there were only upper limits on the strength of certain forbidden sodium (Na) features. The Al-to-Na ratio
is a sensitive function of the peak temperature in the thermonuclear runaway, the white dwarf envelope
composition, and the mass of the white dwarf. The observed chemical abundance pattern deduced from the
coronal spectrum of the ejecta suggests that the ONeMg nova was produced on an intermediate mass (~1 solar
mass) white dwarf, and that the initial accreted envelope of material was close to solar abundance.
The hydrogen recombination lines were used to set limits on the density of the material in the pre-coronal phase.
The line ratios suggest that the density exceeded 109 atoms per cubic cm on day 23.5, and 10 atoms per cubic
cm on day 203. Permitted oxygen lines were observed that were probably excited by Bowen fluorescence
(hydrogen Lyman p pumping). On the other hand, other oxygen line ratios were inconsistent with that
mechanism, and arose within regions where both hydrogen and oxygen were neutral. Higher dispersion spectra
of the line profiles suggested several discrete components contributing to individual lines. The most consistent
model is that of high density clumps embedded in a hottersubstrate. The complexity of the nuclear processes and
the hydrodynamics of the nova explosion can be slowly unraveled through exploitation of relative abundance
diagnostics.
C. National Solar Observatory
1. High-Temperature Coronal Regions Follow Solar Ring Current
R. Altrock (USAF/PL/GPSS and NSO/SP) collaborated with P. Hick and B.V. Jackson (UCSD), J.T. Hoeksema
and X.P. Zhao (Stanford U.) and G. Slater (Lockheed) to study the large-scale structure of the solar corona.
They used large-scale "synoptic" Carrington-rotation maps produced from NSO/SP coronal data, Yohkoh/SXT
(Soft X-ray Telescope) satellite data, and Wilcox Solar Observatory (WSO) "source surface" maps of the largescale solar magnetic field.
They found that the NSO/SP Fe XIV 5303 A data are an excellent proxy for smoothed Yohkoh/SXT data.
Isolated emission features and large-scale structures are nearly identical in SXT and Fe XJV data. In addition,
coronal holes and other low-emission regions are very similar. The two-dimensional cross-correlation
coefficients for such pairs of maps are in the range 0.8 to 0.9. This indicates that the Fe XIV data are sensitive to
the same physical processes as the soft x-ray data and could be very useful in studies of the large-scale structure
of the solar corona during pre- and post-Yohkoh epochs.
Observations in Fe XFV 5303 A and Fe X 6374 A can be used to calculate the temperature of the emitting
plasma. Synoptic temperature maps, calculated from the NSO/SP Fe X/Fe XIV ratio, show a tendency for the
high temperatures to occur where the large-scale solar magnetic fields change polarity at high latitudes. These
regions of enhanced temperature generally follow the heliospheric current sheet (HCS) as defined by the WSO
maps. The HCS is the locus of an inferred large-scale current system circling the Sun at a height of one million
kilometers. The observers hypothesize that this association is due to heating associated with current dissipation
within the HCS. If true, this is an important, previously unknown, source of heating of the solar corona that must
be taken into account by theories of coronal global structure and energy balance, including sources of dynamic
phenomena (e.g., coronal mass ejections). Although this structure appears to overlie the "polar crown"
prominence region, the cause of the excess temperature over those prominences, and not over prominences at
lower latitudes, is not understood. The coronal features associated with all of these lower-lying features are
mostly referred to as "streamers." This study also confirms previous findings that quiet regions in the corona and
"coronal holes" (open-field regions that are the source of the steady-state solar wind) are significantly cooler (by
up to 500,000 K) than the hottest regions. It seems very likely that this phenomenon is revealing properties of the
large-scale distribution of magnetoconvective energy that are not currently accounted for by models of the solar
cycle. Revisions in our concept of how the Sun produces activity appear to be required from these findings. In
particular, it has never been recognized by any accepted model that heating due to current dissipation plays any
role in the temperature structure of the corona.
The group also found that most strong solar active regions have a very complex overlying temperature
distribution, with temperatures ranging from 1 to 6 million K. Temperatures on the low end were previously not
included in models of active regions but must be now.
These results are reported in "Solar Coronal Structure: a Comparison of NSO/SP Ground-Based Coronal
Emission Line Intensities and Temperatures with Yohkoh SXT and WSO Magnetic Data" by R. C. Altrock, P.
Hick, B. V. Jackson, J. T. Hoeksema, X. P. Zhao, G. Slater and T. W. Henry, submitted to Adv. in Space Res.
2. Scattering of P -Modes by Localized Inhomogeneities
Recent observational studies have shown that sunspots scatter intermediate and high-degree p-modes. It is found
that sunspots absorb up to about 50% of the acoustic energy flux that is incident upon them, and furthermore
they produce a shift in phase between the in-going and out-going waves of individual modes. In the past year at
NSO, D. Braun (NSO/SPRC) has discovered that sunspots scatter a measurable amount of incoming p -mode
waves into outgoing modes of the same temporal frequency but different radial orders (a process termed modecoupling). This wealth of observational information on the interaction between p-modes and sunspots offers the
possibility that suitable models of scattering may yield important clues about the subsurface structure and
evolution of solar activity.
A considerable amount of theoretical effort has been devoted to understanding the physical mechanisms of pmode absorption by sunspots, with limited success. Recently, work by Y. Fan, D.-Y. Chou (National Tsing-Hua
U., Taiwan), and Braun has shown that the p-mode phase shifts may be modeled by localized changes in the
acoustic properties of the medium within the volume occupied by the sunspot. Fan, Braun and Chou are carrying
out a study of scattering of p-modes by localized inhomogeneities in wave speed, pressure and density in an
adiabatically stratified polytropic atmosphere. The solution of the scattered waves is obtained by solving the
inhomogeneous wave equation under the simplification of the Born approximation, i.e. in the limit of weak
scattering. It is found that the variation of the observed phase shifts with mode degree, I, and frequency, v, (or
radial order, r\) can be reproduced if the characteristic depth of the inhomogeneity is shallow (-1000 km). The
observed magnitude of the p-mode phase shifts requires an effective wave speed enhancement over this depth
(which is determined largely by the ratio of the magnetic pressure to external gas pressure) within the sunspot of
roughly a factor of two.
The current model is a simplified one which assumes an isotropic increase of wave speed. This represents an
idealized addition of the magnetic pressure to the total restoring force for acoustic waves. Thus, the model does
not include the effect of magnetic tension which introduces anisotropy into the medium. Future research will
incorporate the effects of the Lorentz force into the equation for the scattered waves (following work by
Rosenthal) and hence produce a more realistic model of the magnetic fields. The formalism developed by Fan,
Braun and Chou may also be extended from the simple polytropic atmosphere to a more realistic solar model and
to more complicated sunspot structures. The technique offers a significant step forward in probing acoustic
inhomogeneities produced by sunspots. It is expected that these techniques will play an important role in
interpreting "sunspot seismology" observations planned in the upcoming GONG and SOHO projects.
3. Detection of Intrinsically Weak Solar Disk Magnetism
First, a bit of history: Babcock's 1953 invention of the photoelectric magnetograph revealed non-sunspot fields
down to a few Gauss, but could not discriminate between intrinsically weak fields of, say, 10 G over 2 arcsec,
and 1000 G occupying 0.2 arcsec. Low-resolution observations with the Stenflo line-ratio method (Fe 5250.2 A,
g = 3 vs. Fe 5247.1 A, g = 2), as well as select high-resolution data indicate that plage and network fields
actually have kG field strengths. But what about the intra-network fields which have low values of flux? Until
recently, the field strengths of these regions have not been measurable. Recently in separate studies, S. Martin
(Caltech), C. Keller (NSO/T) and collaborators, and H. Lin (CfA) have suggested that there is an important
component of solar surface magnetism which lies below 500 G in field strength. To explore this question further,
W. Livingston (NSO/T) has put together a single channel Babcock-type system utilizing the favorable g = 3 line
at 15648 A. More sensitive than Fe 5250, the Fe 15648 line allows the deduction of field strengths down to
about 400 G.
The experimental setup is as follows: On the 13.5-m spectrograph of the McMath-Pierce, light input from the
80-cm image feeds a 2 x 2 arcsec image sheer behind the NIM liquid crystal modulator, which is driven at
20Hz. A 0.2 A exit slit can be setto various fixed positions along the line profile (AX = 0.0 A, 0.05 A, 0.10 A,
...) on the 15648 line (0.5A FWHM). Output from the "Babo" InSb diode detector is fed to a lock-in amplifier
set to a time constant of 3 sec. It is possible to scan slowly at 0.1 arcsec/sec along the solar disk N-S meridian.
Seeing-induced Stokes I-V cross-talk is ameliorated by the 20 Hz chopping rate; telescope polarization I-V
cross-talk is eliminated by nulling the lock-in signal with a tilted glass plate in front of the NFM modulator.
Results: Center-to-limb scans are made at exit slit positions from A^= 0.0 to 0.5 A (the last value being
appropriate for strong fields). With the exit slit at 0.1 A from line center we have a noise level of 0.02%
polarization. The scan gives (presumed magnetic) signals of typical amplitude 0.7% which are 3 to 4 arcsec wide
and spaced at an average of 5 arcsec intervals across the entire disk. A comparison with high sensitivity
magnetograms shows that these signals represent mostly intra-network elements. As observed by Martin, they
persist right out to the limb and this needs further study. At a slit position of 0.5 A, the number of signal
elements detected is much less than near line core, as expected if most are weak fields. S. Solanki (ETH) is
modeling signal statistics vs. slit position to deduce field strengths. His preliminary finding is 400 to 500 G as an
upper limit.
Problem: Because our method is statistical, we cannot distinguish in detail between plage (or network) and
intra-network features. An imaging system would be necessary to separate the two.
III. US GEMINI PROGRAM
The US Gemini Program is a division of NOAO which serves as a liaison between the US community and the
international Gemini Project. Personnel in this office include Todd Boroson, the US Gemini Project Scientist,
Fred Gillett, the Associate US Gemini Project Scientist, Kathy Wood, Technical Administrator, and Mark
Trueblood, Project Engineer. During this quarter, Fred Gillett was assigned to the international Gemini Project
to fill in as interim Project Scientist for approximately one year.
This quarter saw the initiation of construction activities at both Gemini sites. The USGP was represented at the
ground-breaking at Gemini North on Mauna Kea, Hawaii, and the laying of the foundation stone at Gemini
South on Cerro Pachon, Chile. The USGP worked with the NSF and AURA on a press announcement for the
two events. The southern ceremony was held immediately after the Gemini Science Committee meeting, which
took place in La Serena, Chile. This meeting saw the beginning of discussions of the scientific aspects of
operations. The USGP held a meeting of its advisory committee, the US SAC, in Tucson in mid-October.
The selection of a supplier for the near-IR Spectrograph was completed during this quarter. This US-allocated
Gemini instrument was the subject of a community-wide competition. As part of a process defined by the USGP
and approved by AURA and the NSF, a panel appointed by the NSF evaluated proposals and made a
recommendation to the international project office. As a result, the international project office has begun
negotiations with NOAO to supply this instrument.
The USGP participated in a number of technical reviews including conceptual review of the coating related
activities, a preliminary design review of the acquisition and guiding assembly, and a meeting to discuss design
tradeoffs for the near-IR imager being built by the University of Hawaii.
Outreach activities of th USGPO this quarter centered on preparations for the American Astronomical Society
meeting in Tucson in January. Work continued on the new version of the Gemini brochure and its translation into
Spanish and French, with printing expected early in the next quarter.
IV. PERSONNEL AND BUDGET STATISTICS, NOAO
A. Visiting Scientists (visitors who arrived thisquarter for a stay of one month or more).
NOAO Facility
Arrived
Name
Institution
10/4/94
University of Sydney
Beijing Normal University
Beijing Normal University
Nanjing Normal University
NSO/Tucson
10/4/94
Damien Burtonclay
Xiang-Tao He
Xiaojun Jiang
Keliang Huang
10/17/94
Olivier Bouchard
Paris, France
NSO/SP
11/15/94
R. Kariyappa
Indian Institute of Astrophysics
NSO/SP
11/28/94
Vincent Foresto
Max-Planck-Institut fur Astronomie
KPNO
11/28/94
Guy Perrin
Observatorie de Paris-Section de
10/4/94
10/4/94
Visited
Meudon - France
NOAO
NOAO
NOAO
KPNO
B. Hired
Date
Name
Position
NOAO Division
10/5/94
Brian Pohl
GONG
NOAO/CCS
KPNO
10/10/94
Carole Leiker
Data Reduction Specialist
Scientific Programmer II
10/12/94
Stephane Chariot
Research Associate
10/12/94
Paola Sartoretti
Research Associate
KPNO
10/27/94
Marguerite Rodriquez
Neil Gaughan
Data Reduction Specialist
Engineering Manager
GONG
10/31/94
ETS
C. Completed Employment
Date
Name
Position
NOAO Division
10/27/94
Rudolf Komm
Research Associate
NSO
11/1/94
John Hughes
Scientific Programmer I
NOAO/CCS
12/30/94
Douglas Geisler
Assistant Scientist
CTIO
Name
Position
NOAO Division
10/1 /94
Wendy Erdwurm
10/1/94
Jeff Vernon
10/3/94
Daniel Bass
Promotion from Scientific Programmer II
to Sr. Scientific Programmer
Promotion from Scientific Programmer I
to Scientific Programmer II
Department transfer from ETS
D. Changed Status
Date
10
GONG
GONG
to GONG
11/1/94
Jean Goodrich
12/1/94
Fred Gillett
12/19/94
Mark Trueblood
GONG
Promotion from Data Reduction Specialist
to Scientific Programmer I
Temporary appointment Acting 8-M
Project Scientist
Promotion Sr. Scientific Programmer
to Sr. Engineer
GONG
NOAO/USGPO
NOAO/USGPO
E. Gemini 8-m Telescopes Project
Changed Status
Date
Name
Position
12/1/94
Matt Mountain
Promotion from 8-M Project Scientist to Director, Gemini
F. Chilean Economic Statistics FY 1995
%Change
Month
inCPI
Cum. Change
Avr. monthly
Pesos/Dollars
inCPI
October
0.6
0.6
414.92
November
0.6
1.2
415.19
December
0.3
1.5
403.03
G. NSF Foreign Travel Fund
For the quarter 1 October through 31 December 1994, a total of $1,374.95 was paid out of the NSF Foreign
Travel account for visits to the following site and institutions:
Las Campanas Observatory, La Serena, Chile,
11
APPENDIX A
Telescope Usage Statistics
October - December 1994
Scheduled Maintenance,
Instrument Tests,
Astronomical Observations
Hours Used
Hours
Telescope
CTIO
Scheduled
NSO
Visitors
Staff
Weather
Equipment
911.5
591.1
116.7
43.5
48.3
111.9
1.5-m
857.6
556.0
99.2
109.4
22.5
70.5
1-m
432.4
295.6
17.0
67.5
12.8
39.5
0.9-m
874.1
548.0
153.5
59.6
14.3
98.7
*0.6/0.9-m
416.6
337.3
9.5
49.3
2.5
18.0
0.6-m
182.5
161.5
0.0
19.5
1.5
0.0
4-m
1061.6
571.72
109.28
338.1
19.0
23.5
1041.25
535.89
75.61
329.25
32.5
68.0
Gourde Feed
963.6
519.45
64.5
303.9
14.25
61.5
1.3-m
1033.5
128.5
433.6
28.8
6.5
0.9-m
916.5
450.37
60.13
325.0
13.5
67.5
Schmidt
392.5
217.88
13.62
140.5
13.5
7.0
Hilltop Dome
1703.0
0.0
1135.0
551.0
17.0
0.0
Vac. Tower/SP
791.0
218.0
177.0
315.0
10.0
71.0
Evans Facility
1191.0
287.0
467.0
414.0
23.0
0.0
**FTSLab
520.0
216.0
224.0
0.0
0.0
80.0
**McMath-Pierce
2000.0
921.0
401.0
573.0
75.0
30.0
Vacuum/KP
592.0
31.0
315.0
231.0
15.0
0.0
436.1
Note: Scheduled hours are calculated according to the ephemerides for CTIO:
October
November
December
*
Equipment Changes,
Engineering, etc.
4-m
2.1-m
KPNO
Hours Lost
9.9 hours/night;
8.9 hours/night;
8.2 hours/night.
Use restricted to dark of the moon.
** Totals include both day and night hours. All others are day only.
APPENDIX B
October - November - December 1994: Individual Telescope Assignments are listed
below. Graduate students are indicated by an asterisk after their names. Nights assigned
(hours worked), and telescope used are indicated. Service Observing programs are denoted by
S.O. instead of nights assigned. A total of 68 programs were carried out during this quarter.
G. Alcaino, W. Liller, E. Wenderoth, F. Alvarado (Instituto Isaac Newton): "Photometry of
Globular Cluster Standards". 9(66) 1-m
E. Albert (U.S. Naval Academy), K. Roth, J. Blades (STScI): "Interstellar Titanium in the
Galactic Halo and the Large Magellanic Cloud". 4(30)4-m
C. Anguita, M.T. Ruiz, P. Loyola (U. de Chile): "CCD Parallaxes for Faint Proper Motion
Stars". 2(18)1.5-m
J. Baldwin (CTIO), B. Wills, D. Wills (U. of Texas), R. Carswell (U. of Cambridge, UK), G.
Ferland (U. of Kentucky), A. Cooke (Cambridge U., England): "The Inner Regions of
Quasars". 3(28)4-m, l(10)0.9-m
T. Barnes III (U. of Texas), T. Moffett (Purdue U.), W. Gieren, M. Gomez* (U. Catolica de
Chile): "Independent Distances to LMC/SMC Cepheids". ll(89)0.9-m
C. Beauvais*, G Bothun (U. of Oregon), R. Schommer (CTIO): "Reducing Tully-Fisher
Scatter Kinematic Observations". 4(34)1.5-m, 1(6)0.9-m
T. Beers, R. Wilhelm* (Michigan State U.), A. Layden (CTIO): "uUBV Photometry of Halo
and Thick-Disk FHB and A-Type Stars". 4(19)1.5-m, 9(51)l-m
L. Campusano (U. de Chile), R. Clowes, M. Graham* (U. Central Lancashire, UK): "Search
for Quasar Groups in SGP and ESO/SERC 345 Fields". 4(28)4-m
E. Colbert* (U. of Maryland), J. Mulchaey*, A. Wilson (STScI), T. Storchi-Bergmann
(UFRGS, Brazil): "Extended Emission-Line Gas as a Probe of the Nuclear Ionizing Continuum
in Active Galaxies". 3(26)4-m
K. Cook (Lawrence Livermore Nat. Lab.), C. Stubbs, M. Pratt (U. of California, Santa
Barbara): "Spectroscopy and Photometry of Candidate Lensed Stars and Other Interesting
Objects from the MACHO Project". 3(27)4-m
A. Cowley, P. Schmidtke (Arizona State U.), J. Hutchings, D. Crampton (Dominion
Astrophys. Obs., Canada): "Spectroscopy of X-Ray Sources in the Magellanic Clouds".
5(50)4-m
A. Crotts, J. Xu* (Columbia U.), S. Heathcote (CTIO): "The Dynamics and Morphology of the
Emission-Line Nebula Surrounding SN 1987A". 3(35)4-m
S. Djorgovski, R. de Carvalho, L. Yan* (California Inst, of Tech.): "Surface Photometry of
Rich Clusters of Galaxies". 9(79)CS
A. Ferguson*, R. Wyse (Johns Hopkins U.), J. Gallagher (U. of Wisconsin-Madison): "Star
Formation in the Outer Regions of Disk Galaxies". 2(10)1.5-m
J. Frogel, D. DePoy, R. Pogge, A. Quillen, K. Sellgren, D. Terndrup (Ohio State U.), R.
Davies (U. of Oxford, UK): "An Atlas of Galaxies in the Near-Infrared: A Study of Structure
and Stellar Content I. Infrared Observations of Spiral Galaxies". 7(45) 1.5-m
J. Frogel, D. DePoy, R. Pogge, A. Quillen, D. Terndrup (Ohio State U.), R. Davies (U. of
Oxford): "An Atlas of Galaxies in the Near-Infrared: A Study of Structure and Stellar Content
II. Optical Surface Photometry". 6(45)0.9-m
A. Fruchter (STScI), B. Moore (U. of California, Berkeley), C. Steidel (Massachusetts Inst, of
Tech.): "Do We All Go Together When We Flow?". 7(46)1.5-m
J. Gardner (U. of Durham, UK), J. Annis (Fermilab): "The Optical and Near-Infrared
Luminosity Function of the Rich X-Ray Cluster Abell 496". 5(50)1.5-m
D. Geisler (CTIO), A. Cooke (Cambridge U., England): "Standard Branches in the Washington
System: A New Method for Metallicity Determination and its Application to the Sculptor and
Fornax dSphs". 5(38)0.9-m
S. Gibson*, K. Nordsieck (U. of Wisconsin): "Faint Reflection Nebulosity Imaging Survey in
the Large Magellanic Cloud". 4(24)CS
M. Gregg (Lawrence Livermore Nat. Lab.), M. Drinkwater (Anglo-Australian Obs.):
"Multicolor Imaging Survey of the Fornax Cluster of Galaxies". 7(64)CS
S. Hawley (Michigan State U.), I. Reid, J. Gizis (California Inst, of Tech.): "Basic Data for
Nearby Stars". 4(37) 1.5-m
M. Irwin (Royal Greenwich Obs.), S. Demers (U. de Montreal), W. Kunkel (Las Campanas
Obs.): "The Absolute Proper Motion of the Small Magellanic Cloud". 2(19)4-m
K. Johnston, N. Zacharias, M. Zacharias (US Naval Observatory), J. Russell (Naval Research
Lab.), Chr. de Vegt (U. of Hamburg, Germany): "Structure Analysis and Precise Positions of
Extragalactic Reference Frame Sources". 8(83)0.9-m
C. Joseph, J. Gallagher (U. of Wisconsin), M. Phillips (CTIO): "Spectroscopic Studies of
Gravitational Microlenses".
2(22)4-m
K. Krisciunas (Joint Astronomy Centre, Hawaii): "Multi-Site Photometry of yDoradus
(Continuation)". 10(80)0.6-m
C. Lacy (U. of Arkansas): "Apsidal Motion in Eccentric Eclipsing Binary Stars". 2(15)0.6-m
A. Landolt (Louisiana State U.): "UBVRI Photoelectric Photometric Sequences (Proposal I)".
7(51)1.5-m
A. Landolt (Louisiana State U.): "Intercomparison of UBVRI Photometric Filter Sets".
5(23) 1-m
T. Lauer (KPNO), M. Postman (STScI), M. Strauss (Inst, of Advanced Study): "Motion of the
Local Group with Respect to Distant Abell Clusters". 4(32) 1.5-m
A. Layden (CTIO): "The Kinematics and Metallicities of Field RR Lyraes at |Z| > 5 kpc
from the Galactic Plane". 3(27)4-m, 5(53)0.9-m
J. Loveday (Fermi Nat. Accelerator Lab.), S. Cote, T. Broadhurst (Johns Hopkins U.): "CCD
Imaging of Parkes-APM Low Surface-Brightness Galaxies". 4(39)1.5-m
P. Lu (Western Connecticut State U.): "Continuing the Spectral and Photometry Studies for F
and G Stars at the SGP". 6(54) 1-m, 6(56)0.9-m
M. Luhman*, D. Jaffe, S. Pak* (U. of Texas): "Uv-Excited H2: A New Tool for Forging
Molecular Clouds". 4(37) 1.5-m
G Mackie (Harvard-Smithsonian), A. Stanford (Infrared Processing & Analysis Center): "A
Dynamical Study of Advanced Merger Galaxies: The Fundamental Plane". 3(30)4-m
G. Mackie, P. Fabbiano (Harvard-Smithsonian): "Optical Panoramic Studies of ROSAT/IRAS
Observed Large Spirals: Local vs. Global Correlations in FIR, X-Ray, Ha
and B, I Emission". 5(42)CS
J. Maza, M. Wischnjewsky, X. Gomez* (U. de Chile): "UBVRI Photometry of Calan-Tololo
Seyfert Galaxies".
l(10)4-m, 6(51)0.9-m
J. Maza, P. Ortiz, M. Wischnjewsky (U. de Chile): "Spectroscopy of Calan-Tololo Quasar
Candidates".
2(17)4-m, 6(40)CS
P. McCarthy (Carnegie Obs.), W. van Breugel (Lawrence Livermore Nat. Lab.), V. Kapahi
(Poone U., India): "Spectroscopy of Southern Hemisphere Radio Galaxies". 4(33)4-m
R. McMillan*, R. Ciardullo (Pennsylvania State U.): "Extragalactic Observations of Supernova
Age Indicators".
8(64)0.9-m
R.H. Mendez (Univ. Observatory, Munich), M. Breger, G Hardier (Inst, for Astronomy,
Vienna), E. Costa (U. de Chile): "On the Variability of the Central Star of the PN IC 418".
5(32)l-m
P. Ortiz, J. Maza (U. de Chile): "Search for Quasars with Redshift z > 4.0". 3(29)CS
S. Pak*, D. Jaffe, M. Luhman* (U. of Texas): " Extended Molecular Hydrogen Emission
from the LMC". 6(45) 1.5-m
J. Patterson, A. Shambrook*, J. Kemp, C. Haswell, J. Zimmerman* (Columbia U.):
"Superhumps in Cataclysmic Variables". 5(28) 1-m
E. Paunzen, M. Gelbmann (Inst, fuer Astronomie, Austria): "Survey to Detect Pulsation in X
Bootis Stars". ll(67)0.6-m
A. Phillips (U. of California, Sta Cruz): "Na D Search for Superwinds in Hotspot Galaxies".
l(7)4-m
M. Phillips, N. Suntzeff, A. Walker, J. Elias, M. Navarrete, M. Hamuy (CTIO), D. DePoy
(Ohio State U.): "Observations of SN 1987A at Late Epochs". 5(40)4-m, l(10)0.9-m
M. Regan*, S. Vogel, R. Gruendl, P. Teuben (U. of Maryland): "The Gas Kinematics of
Barred Spiral Galaxies". 4(40)1.5-m
M. Regan*, S. Vogel, P. Teuben, M. Thornley (U. of Maryland): "The Near Infrared Structure
and Extinction in Barred Spiral Galaxies". 3(30)1.5-m
B. Reipurth, (ESO, Chile), J. Bally, D. Devine (U. of Colorado): "Herbig-Haro Objects in
LI641 in Orion". 3(27)CS
M.T. Ruiz (U. de Chile), M. Peiia, S. Torres-Peimbert (U. Nac. de Mexico): "A Spectroscopic
Study of MC Planetary Nebulae with WR Features and the Changes of N66". 2(19)4-m
M.T. Ruiz (U. de Chile), P. Bergeron (U. de Montreal, Canada), S. Leggett (JAC, Hawaii):
"Study of Carbon White Dwarfs". 4(36)4-m, 4(31)0.9-m
D. Schlegel*, M. Davis (U. of California, Berkeley), J. Roth (California Inst, of Tech.), M.
Strauss (Inst, for Advanced Study): "Tully-Fisher Observations of IRAS Galaxies". 3(31)4-m,
l(6)0.9-m, 2(13)CS
P. Schmidtke, A. Cowley, T. McGrath* (Arizona State U.), J. Hutchings, D. Crampton
(Dominion Astrophys. Obs., Canada): "Photometry of X-Ray Sources in the Magellanic
Clouds".
8(63)0.9-m
F. Schweizer (Dept. of Terrestrial Magnetism), P. Seitzer (U. of Michigan): "Spectroscopy of
Young Globular Clusters in the Merger Remnants NGC 7252 and 1316". 2(14)4-m
T. Smecker-Hane, P. Stetson, J. Hesser (Dominion Astrophys. Obs., Canada), D. Geisler
(CTIO): "The Stellar Populations of Dwarf Spheroidal Galaxies: III. Photometry of Fornax".
3(24)4-m
H.A. Smith, N. Silbermann (Michigan State U.), A. Walker (CTIO): "CCD Photometry of
SMC Variable Stars". 5(25)CS
R.C. Smith (CTIO), F. Winkler (Middlebury College), Y.-H. Chu (U. of Illinois): "An
Emission-Line Survey of [Selected Regions of] the Magellanic Clouds". 1(4)CS
R.C. Smith, R. Elston (CTIO): "IR Imaging & Spectroscopy of Supernova Remnants".
7(63)1.5-m
V. Smith, D. Lambert (U. of Texas), N. Suntzeff (CTIO), K. Cuhna (Observatorio Nacional,
Brazil): "Chemical Evolution and Globular Clusters". 5(49)4-m
C. Sneden (U. of Texas), G. Preston, A. McWilliam (Carnegie Observatories), J. Cowan (U. of
Oklahoma): "An Extremely Metal-Poor Giant with Large Neutron Capture Element Excesses".
4(35)4-m
M. Strauss (Inst, for Advanced Study), T. Lauer (KPNO), M. Postman (STScI): "Velocity
Dispersions and Redshifts of Brightest Cluster Galaxies: Bulk Flows to 240 h-1 Mpc".
4(39)4-m
A. Walker (CTIO): "Horizontal Branch Evolution and Pulsation Study". 5(49)0.9-m
F. Walter (State U. of New York), D. Duncan (U. of Chicago), A. Collier-Cameron (U. of
Sussex, UK), M. Kuerster (MPE, Germany): "The Atmosphere of AB Dor from the
Photosphere through the Corona". 3(32)4-m
T. Williams (Rutgers U.), D. Schiminovich*, J. van Gorkom (Columbia U.), T. van der Hulst
(Kapteyn Astron. Inst., The Netherlands): "Sharp Edges in Neutral Hydrogen in Elliptical Shell
Galaxies and Spirals: the Result of Photoionization?". 3(27)1.5-m
R. Wing (Ohio State U.), D. MacConnell (STScI): "A Photometric Search for Dwarf Carbon
Stars". 8(59) 1-m
P. Winkler (Middlebury College), R.C. Smith (CTIO), R. Petre (NASA/GSFC), Y.-H. Chu (U.
of Illinois): "New Supernova Remnants in the Magellanic Clouds". 4(32)1.5-m
MACHO (Massive Compact Halo Object) Program: S. Marshall (U. of California, Santa
Barbara), D. Bennett (L. Livermore National Lab.), D. Reiss* (U. of Washington): "Real-Time
Follow-up of Candidate Microlensing Events". 6(47)0.9-m
Executed Proposals
1525
H Abt,
0
10/01/94 - 12/31/94
Page 1
Tue Jan 31 14:02:33 1995
Nights
Hours
Days
Hours
4.00
32.50
0.00
0.00
3.00
11.95
0.00
0.00
7.00
37.00
0.00
0.00
7.00
50.00
0.00
0.00
5.00
34.00
0.00
0.00
5.00
30.00
0.00
0.00
3.90
3.00
26.00
33.50
0.00
0.00
0.00
0.00
f94
D Willmarth,
National Optical Astronomy Observatories
Binary Search Among Sharp Lined A Stars
Coude Feed
1447
0
S Adelman,
f94
The Citadel
A Philip, Van Vleck Observatory
Elemental Abundances of Field Horizontal Branch
Stars IV
1490
2
Coude Feed
f94
G Albright, M Richards, University of Virginia
P Koubsky, Astronomical Institute
Simultaneous Balmer Line IUE and Radio Continuum
Observ
1609
Coude Feed
0
f94
B Andersson,
P Wannier,
Jet Propulsion Laboratory
S Federman, University of Toledo
The Envelope of Molecular Cloud B5 II, K I and Na
I Lines
Coude Feed
1595
0
f94
J Annis, Fermi National Accelerator Laboratory
J Gardner, Durham University
K Band Imaging of Low Redshift X-Ray Selected
Clusters
1.3 meter
1622
0
S Baggett,
f94
J MacKenty,
Space Telescope Science Institute
Near-IR Imaging of Edge-On Disk Galaxies
1.3 meter
1486
2
f94
C Bailyn, J Orosz, Yale University
Observations of Black Hole Candidate Nova Per
1992
2.1 meter
4
meter
Executed Proposals
10/01/94 - 12/31/94
Page 2
Tue Jan 31 14:02:33 1995
Nights
Hours
Days
Hours
2.1 meter
5.00
51.50
0.00
0.00
J Bally, D Devine, R Sutherland,
University of Colorado
Kinematics & Excitation of Herbig-Haro Objects &
Jets....
4 meter
3.00
31.00
0.00
0.00
8.00
44.00
0.00
0.00
3.00
25.00
0.00
0.00
3.00
23.50
0.00
0.00
4.00
40.00
0.00
0.00
1446
0
f94
J Baldwin,
National Optical Astronomy Observatories
B Wills,
D Wills,
M Brotherton,
University of Texas, Austin
H Netzer, Tel Aviv University
The Inner Regions of Quasars
1562
1455
0
f94
0
f94
T Beers, Michigan State University
A Search for Extremely Low Metallicity Stars and
FHB/A Star
Burrell Schmidt
1630
0
f94
M Bershady,
C Gronwall,
University of California, Santa Cruz
A Stanford, California Institute of Technology
Are Faint Blue Galaxies Exploding Dwarfs?
4
1605
0
H Bond,
meter
f94
A Saha,
Space Telescope Science Institute
Testing Post-AGB A-F Supergiants as Standard
Candles in
1570
0
G Bothun,
4 meter
f94
University of Oregon
D Silva,
National Optical Astronomy Observatories
Age Dating Suspected Mergers via AGB Light: Part
III
1.3 meter
Executed Proposals
1448
0
10/01/94 - 12/31/94
Page 3
Tue Jan 31 14:02:33 1995
Nights
Hours
Days
Hours
4.00
22.00
0.00
0.00
5.00
3.00
20.50
4.50
0.00
0.00
0.00
0.00
5.00
24.50
0.00
0.00
3.00
10.50
0.00
0.00
f94
M Brotherton, B Wills,
University of Texas, Austin
The Intermediate Line Region of QSOs
2.1 meter
1516
0
f94
D Calzetti, A Kinney,
K McQuade,
Space Telescope Science Institute
T Storchi-Bergmann, Instituto di Fisica
Dust Extinction and Initial Mass Function in
Starburst....
1618
0
1.3 meter
0.9 meter
f94
A Connolly, T Broadhurst, G Szokoly,
Johns Hopkins University
B Mobasher, Imperial College
The Local Infrared Luminosity Function of Field
Galaxies
1454
N
P
N
H
5
1.3 meter
f94
Devereux, New Mexico State University
Scowen, Arizona State University
Duric, University of New Mexico
Alpha Imaging of Large Nearby Galaxies
Burrell
1665
0
Schmidt
f94
M Dickinson, Space Telescope Science Institute
P Eisenhardt, Jet Propulsion Laboratory
Using Radio Galaxies to Find Clusters at z > 1
1477
0
4
meter
3.80
11.00
0.00
0.00
4
meter
2.65
31.00
0.00
0.00
0.9 meter
5.00
41.50
0.00
0.00
f94
E Ellingson, University of Colorado
H Yee, University of Toronto
Quasars in Clusters at Z - 1
1566
0
f94
D Elmegreen,
Vassar College
J Salzer, Wesleyan University
Star Forming Complexes in Spiral Galaxies
Executed Proposals
1585
0
10/01/94 - 12/31/94
Page 4
Tue Jan 31 14:02:33 1995
Nights
Hours
Days
Hours
5.00
42.50
0.00
0.00
4.00
42.00
0.00
0.00
5.00
41.50
0.00
0.00
3.00
24.00
0.00
0.00
6.00
6.00
44.50
26.50
0.00
0.00
0.00
5.50
33.00
0.00
0.00
f94
D Elmegreen, F Chromey, Vassar College
B Elmegreen,
IBM
Near-Infrared Imaging of Barred Galaxies
1.3 meter
1608
0
f94
R Elston,
National Optical Astronomy Observatories
P Eisenhardt, Jet Propulsion Laboratory
The Evolution of Early Type Galaxies at Z=l
4 meter
1459
0
f94
F Fekel, NASA Marshall Space Flight Center
J Marshall, Villanova University
Spectroscopy of Close Multiple Stars and Speckle
Binaries
Coude Feed
1583
0
f94
A Ferguson, R Wyse, Johns Hopkins University
J Gallagher, University of Wisconsin, Madison
Chemical Abundances in Outer Disks of Galaxies
4 meter
1590
0
f94
A Fry, B Carney, University of North Carolina
T Kinman,
National Optical Astronomy Observatories
Infrared Photometry and the Cepheid and RR Lyrae
Distance..
2.1 meter
0.9
1629
0
G Fuller,
meter
0.00
f94
National Radio Astronomy Observatory
E Lada, University of Maryland at College Park
P Myers,
Harvard-Smithsonian Center for Astrophysics
The Structure of the Extinction in the Dense Core
in L1400G
2.1 meter
Executed Proposals
10/01/94 - 12/31/94
Page 5
Tue Jan 31 14:02:33 1995
Nights
1637
0
M Garcia,
Hours
Days
Hours
3.00
25.00
0.00
0.00
3.00
0.00
0.00
0.00
7.00
59.00
0.00
0.00
12.00
74.50
0.00
0.00
6.00
34.50
0.00
0.00
4.00
42.00
0.00
0.00
f94
J McClintock,
P Callanan,
P Zhao,
Harvard-Smithsonian Center for Astrophysics
Searching for Black Holes: Mass Function of X-Ray
Nova....
1634
4
0
meter
f94
M Giavalisco, F Macchetto,
Space Telescope Science Institute
P Rosati,
Johns Hopkins University
C Steidel,
Massachusetts Institute of Technology
A Broad-Band Multi-Color Search for 3
Galaxies
1495
0
<
z
<
4
3.5
meter
f94
S Gibson, K Nordsieck,
University of Wisconsin,
Madison
Interstellar Absorption Associated with Pleiades
Reflection
1510
0
Coude Feed
f94
R Giovanelli, M Haynes, Cornell University
Measurement of Peculiar Velocities of Spiral
Galaxies
1599
0
0.9 meter
f94
R Gonzalez, J Graham, J Najita, A Dey,
University of California, Berkeley
Deep IR Imaging of Nearby Spirals: Global
Morphology and...
1670
0
R Green,
1.3 meter
f94
National Optical Astronomy Observatories
R Griffiths, Johns Hopkins University
V Sarajedini, University of Arizona
The Morphological Evolution of Distant Galaxies
4
meter
Executed Proposals
1632
0
10/01/94 - 12/31/94
Page 6
Tue Jan 31 14:02:33 1995
Nights
Hours
Days
Hours
3.00
5.50
0.00
0.00
4.00
50.00
0.00
0.00
2.00
17.00
0.00
0.00
2.90
32.00
0.00
0.00
meter
4.00
25.50
0.00
0.00
meter
0.00
0.00
7.00
28.00
f94
M Gregg,
Lawrence Livermore Laboratory
A Spectral Atlas of M32
Coude Feed
1671
0
P Hall,
R
f94
University of Arizona
Green,
National Optical Astronomy Observatories
Associated CIV Absorption and Environments of
Radio-Loud...
1661
0
4 meter
f94
P Harding, A Nelson, University of Arizona
A Sarajedini,
National Optical Astronomy Observatories
I Ferrin, University of the Andes
E Alvarez,
The M33 Cluster System
0.9 meter
1606
0
f94
T Heckman, G Meurer, Johns Hopkins University
A
Galactic Wind from the Nucleus
of M31
4
1658
0
meter
f94
L Hillenbrand, L Allen, S Strom,
University of Massachusetts
Age Spreads & Mass Functions in Isolated High
Mass
1548
Star....
0
4
f94
K Hinkle, L Wallace, E Hardesty, D Little,
D
Branston,
National Optical Astronomy Observatories
M Meyer, University of Massachusetts
S Edwards, Smith College
V Sarajedini, University of Arizona
L and K Band Infrared Spectral Standards
4
Executed Proposals
1580
0
10/01/94 - 12/31/94
Page 7
Tue Jan 31 14:02:33 1995
Nights
Hours
Days
Hours
1.00
0.00
0.00
0.00
6.00
1.50
54.50
5.50
0.00
0.00
0.00
0.00
6.50
52.00
0.00
0.00
5.00
32.50
0.00
0.00
4.00
17.50
0.00
0.00
7.50
51.50
0.00
0.00
f94
K Janes,
E Friel,
Boston University
Maria Mitchell Observatory
P Seitzer, University of Michigan
Integrated Properties of Galactic Open Clusters
Burrell
1616
0
f94
B Jannuzi,
Institute for Advanced Study
R
Lowe,
Green,
Schmidt
C
National Optical Astronomy Observatories
R Weymann, Carnegie Observatories, (OCIW)
5 Morris, Dominion Astrophysical Observatory
V Sarajedini, University of Arizona
Connection Between Low Redshift Lyman-a Absorbers
6 Large..
Burrell Schmidt
2.1
1470
0
meter
f94
K Johnston, N Zacharias, U. S. Naval Observatory
J Russell, M Zacharias,
Naval Research Laboratory
C de Vegt,
Universitat Hamburg
Structure Analysis and Precise Positions of
Extragalactic.
1507
0
0.9 meter
£94
S Kenyon, R Marzke, M Geller,
Harvard-Smithsonian Center for Astrophysics
The H-Band Luminosity Function of Nearby
Galaxies
1535
0
1.3 meter
f94
S Kenyon, C Lada, J Alves,
Harvard-Smithsonian Center for Astrophysics
The Luminosity Function of Nearby Protostars
1.3
1523
0
meter
f94
T Kinman,
National Optical Astronomy Observatories
Blue Horizontal Branch & RR Lyrae Stars in the
Outer Halo
1.3
meter
Executed Proposals
1487
0
10/01/94 - 12/31/94
Page 8
Tue Jan 31 14:02:33 1995
Nights
Hours
Days
Hours
1.50
5.50
0.00
0.00
5.00
33.00
0.00
0.00
8.70
41.10
0.00
0.00
6.00
51.00
0.00
0.00
5.00
37.50
0.00
0.00
6.00
49.50
0.00
0.00
f94
R Kirshner, B Schmidt, A Riess,
Harvard-Smithsonian Center for Astrophysics
D Mcintosh, M Walters, University of Arizona
L Wells,
National Optical Astronomy Observatories
P Garnavich, Dominion Astrophysical Observatory
Supernova Light Curves
2.1 meter
1534
0
E Lada,
f94
University of Maryland at College Park
C Lada,
Harvard-Smithsonian Center for Astrophysics
R Phelps, Phillips Laboratory
Investigations of the Nature of Young Stellar
Clusters
1469
1.3 meter
0
f94
A Landolt, Louisiana State University
Broad-Band Standards at Declination +45 Degrees
1.3 meter
1578
0
T Lanz,
f94
NASA Goddard Space Flight Center
J Landstreet, University of Western Ontario
G Mathys, European Southern Observatory
Ap Stars with Magnetically Resolved Lines
Coude Feed
1574
0
T Lauer,
f94
National Optical Astronomy Observatories
M Postman, Space Telescope Science Institute
M Strauss,
Institute for Advanced Study
Motion of the Local Group with Respect to Distant
Abell
1517
S Lee,
2.1 meter
0
f94
Seoul National University
B Carney, M Corwin, University of North Carolina
The Luminosity/Mass Function for Halo Stars
1.3 meter
Executed Proposals
1572
0
M Lehnert,
T Heckman,
10/01/94 - 12/31/94
Page 9
Nights
Hours
Days
Hours
5.00
32.00
0.00
0.00
0.9 meter
4.00
14.00
0.00
0.00
4 meter
2.00
6.00
0.00
0.00
Burrell Schmidt
2.00
24.00
0.00
0.00
4.00
23.00
0.00
0.00
f94
IGPP\Lawrence Livermore Natl. Lab
Johns Hopkins University
Shock-Heated Gas in Halos of Starburst Galaxies
2.1 meter
1573
0
Tue Jan 31 14:02:33 1995
f94
M Lehnert, IGPPXLawrence Livermore Natl. Lab
T Heckman, Johns Hopkins University
Determining the Nature of Diffuse Interstellar
Medium in...
1503
0
C Martin,
f94
R Kennicutt,
Jr.,
University of Arizona
Galactic Winds
9149
0
from Dwarf Galaxies
f94
P Mason, Case Western Reserve University
CCD Photometry of the Unusual Magnetic
Cataclysmic Binary..
1440
0
f94
P Massey,
National Optical Astronomy Observatories
Are There Massive Stars in the Andromeda Galaxy?
4 meter
1496
0
P Massey,
f94
C Corson,
National Optical Astronomy Observatories
S Strom, L Hillenbrand,
University of Massachusetts
The Star Forming History of h and x Persei
Modern Study...
4
meter
0.9
meter
2.00
1.50
9.00
20.00
0.00
0.00
0.00
0.00
R Mathieu, University of Wisconsin, Madison
A Search for Pre-Main Sequence Eclipsing
Binaries
0.9 meter
5.00
56.00
0.00
0.00
1554
0
f94
Executed Proposals
1556
0
10/01/94 - 12/31/94
Page 10
Tue Jan 31 14:02:33 1995
Nights
Hours
Days
Hours
6.00
53.00
0.00
0.00
3.00
3.00
0.00
0.00
6.00
57.00
0.00
0.00
6.00
42.00
0.00
0.00
4.50
52.50
0.00
0.00
3.00
24.00
0.00
0.00
f94
R McMillan,
R Ciardullo,
Pennsylvania State University
Extragalactic Observations of Supernova Age
Indicators
0.9 meter
1504
0
f94
B McNamara,
Harvard-Smithsonian Center for Astrophysics
R Elston, M Wise,
National Optical Astronomy Observatories
B Jannuzi, Institute for Advanced Study
C Sarazin, University of Virginia
U-Band Polarimetry of Active Central Cluster
Galaxies
1614
0
K Merrill,
4 meter
f94
I Gatley,
National Optical Astronomy Observatories
Ontogeny of the NGC 2024 Nascent Cluster: Near IR
Solution
1450
0
1.3 meter
f94
D Meyer, Northwestern University
The Interstellar Lithium Isotope Ratio Toward
Omicron Perse
1651
0
Coude Feed
f94
M Meyer, S Strom, L Allen, K Strom,
University of Massachusetts
S Edwards, Smith College
Infrared Spectroscopy of Deeply Embedded Young
Clusters
9148
0
2.1 meter
f94
B Mueller,
National Optical Astronomy Observatories
I Ferrin,
University of
the Andes
E Alvarez,
Activity of Tempel 2
0.9 meter
Executed Proposals
10/01/94 - 12/31/94
Page 11
Tue Jan 31 14:02:33 1995
Nights
Hours
Days
Hours
8.00
60.00
0.00
0.00
4 meter
2.80
21.00
0.00
0.00
Physical Properties in the Orion Nebula Near
Proplyds....
Coude Feed
7.00
68.50
0.00
0.00
1.00
10.00
0.00
0.00
4.00
44.00
0.00
0.00
2.00
4.00
20.00
21.00
0.00
0.00
0.00
1532
0
f94
S Naoumov,
B
Carney,
J
Rose,
University of North Carolina
J Laird,
Bowling Green State University
The Galaxy's Disk: Two Populations or One?
Burrell
1623
0
C O'Dea,
Schmidt
f94
S Baum,
Space Telescope Science Institute
R Gelderman, NASA Goddard Space Flight Center
Spectroscopy of Mysterious GHz Peaked Spectrum
Radio....
1460
0
f94
C O'Dell,
1520
0
F Owen,
W Keel,
X Hu,
Rice University
f94
National Radio Astronomy Observatory
University of Alabama
Evolution of Radio Galaxies to z=l:
Imaging
1657
0
Optical
2.1 meter
f94
B Penprase, J Lauer, M Zarins, Pomona College
High Resolution Spectroscopy of Absorption Lines
Toward....
1654
0
Coude Feed
f94
S Perlmutter, G Goldhaber, D Groom, R Pain,
University of California, Berkeley
C Pennypacker, A Kim,
Lawrence Berkeley Laboratory
D Zaritsky, J Willick,
Carnegie Observatories, (OCIW)
G Bernstein, University of Arizona
B Grossan, Massachusetts Institute of Technology
R McMahon, University of Cambridge
S Deustua, Lawrence Livermore Laboratory
Homogeneity & Rate of High-Redshift Supernovae
with
....
4 meter
2.1 meter
0.00
Executed Proposals
10/01/94 - 12/31/94
Page 12
Tue Jan 31 14:02:33 1995
Nights
Hours
Days
Hours
3.00
25.50
0.00
0.00
2.65
4.00
17.50
35.50
0.00
0.00
0.00
0.00
6.00
32.00
0.00
0.00
4 meter
5.00
29.50
0.00
0.00
Is There Primordial Gas at Redshift Three?
4 meter
2.85
32.00
0.00
0.00
2.00
9.50
0.00
0.00
1652
0
£94
R Peterson, University of California, Santa Cruz
R Saffer, Space Telescope Science Institute
Rotational Velocities as Population Discriminant
for ....
847
2
M Pierce,
4 meter
f94
G Jacoby,
J Hedden,
S Courteau,
National Optical Astronomy Observatories
D Crabtree, Dominion Astrophysical Observatory
Long-Period Variables: An Alternative to
Cepheids?
2.1 meter
0.9 meter
1643
0
f94
C Pilachowski,
D Rabin,
National Optical Astronomy Observatories
Magnetic Fields in Metal Poor Stars
Coude Feed
1441
0
f94
C Prosser, Jr.,
L
Hartmann,
Harvard-Smithsonian Center for Astrophysics
Rotational Velocity Survey Among Pre-Main
Sequence K & M ..
1546
0
M Rauch,
f94
R Weymann,
Carnegie Observatories,
(OCIW)
R Carswell, University of Cambridge
J Webb, University of New South Wales
1587
0
f94
G Rhee, University of Nevada
J Stocke, M Harvanek, E Ellingson,
University of Colorado
A Study of 3C Radio Galaxy Environments at
Intermediate z
0.9 meter
Executed Proposals
1541
0
10/01/94 - 12/31/94
Page 13
Tue Jan 31 14:02:33 1995
Nights
Hours
Days
Hours
7.00
38.50
0.00
0.00
5.70
40.00
0.00
0.00
6.00
46.00
0.00
0.00
1.85
0.00
0.00
0.00
3.00
4.00
10.00
35.00
0.00
0.00
0.00
0.00
4.90
33.00
0.00
0.00
6.00
59.00
0.00
0.00
f94
D Schade,
S Lilly, University of Toronto
The Local Density of Star-Forming Galaxies
Burrell
1529
0
Schmidt
f94
K Sellgren, T Mailloux, Ohio State University
R Smith,
ADFA
T Brooke, Jet Propulsion Laboratory
Search for Interstellar
Clouds
1628
0
"Diamonds"
in Molecular
2.1 meter
f94
M Skrutskie, M Weinberg, M Meyer,
University of Massachusetts
A 1.6um Spectral Survey of Evolved Stars
Coude Feed
1640
0
f94
V Smith, University of Texas, Austin
K Cunha,
Observatorio Nacional
High-Resolution Spectroscopy of Low-Mass Orion
Association.
1656
0
4
meter
£94
A Stanford,
California Institute of Technology
M Dickinson, Space Telescope Science Institute
P Eisenhardt, Jet Propulsion Laboratory
Galaxy Evolution in High Redshift Clusters
4 meter
2.1 meter
1475
0
f94
C Steidel, Massachusetts Institute of Technology
M Dickinson,
Space Telescope Science Institute
M Pettini, Royal Greenwich Observatory
The nature of Normal Galaxies at z>l
4
1449
0
M Strauss,
T
meter
f94
Institute for Advanced Study
Lauer,
National Optical Astronomy Observatories
M Postman, Space Telescope Science Institute
Velocity Dispersions of Brightest Cluster
Galaxies:
Bulk...
2.1 meter
Executed Proposals
1647
0
10/01/94 - 12/31/94
Tue Jan 31 14:02:33 1995
Nights
Hours
Days
Hours
4.95
12.00
45.50
33.50
0.00
0.00
0.00
0.00
f94
D Terndrup, M Pinsonneault,
A Krishnamurthi,
J
Page 14
S Balachandran,
Ohio State University
Stauffer,
Harvard-Smithsonian Center for Astrophysics
S Wolff,
National Optical Astronomy Observatories
M Gagne, University of Colorado
A Key Project to Constrain Angular Momentum
Evolution of...
4 meter
0.9
1435
0
meter
f94
S Veilleux,
National Optical Astronomy Observatories
D Sanders, University of Hawaii
Optical Spectroscopy of a New High Redshift
Sample of Ultra
1482
0
2.1 meter
2.00
0.00
0.00
6.00
48.50
0.00
0.00
5.00
25.00
0.00
0.00
7.00
68.50
0.00
0.00
8.00
63.00
0.00
0.00
f94
F Walter, L Matthews,
SUNY at Stony Brook
A Brown,
4.00
N Adams,
University of Colorado
The Deep ROSAT Survey of Orion: Identifying Low
Mass Stars
1627
0
A Watson,
2.1 meter
f94
J Gallagher,
T Tripp,
University of Wisconsin, Madison
E de Feijter, Lowell Observatory
NIR Hydrogen Recombination Line Mapping of Nearby
Nuclear..
1536
0
1.3 meter
£94
A Welty, L Ramsey, Pennsylvania State University
A Study of T Tauri Star Winds and Accretion
Streams
1559
2.1 meter
0
R White,
f94
Smith College
B Rachford, University of Wyoming
Titanium Abundances
Toward
in Pre-shock and Shocked Gas
Coude Feed
Executed Proposals
1537
0
10/01/94 - 12/31/94
Page 15
Tue Jan 31 14:02:33 1995
Nights
Hours
Days
Hours
6.00
31.50
0.00
0.00
5.00
49.00
0.00
0.00
f94
B Whitney, S Kenyon,
Harvard-Smithsonian Center for Astrophysics
The Near
Taurus
1545
0
IR Polarization of
the Protostars in
1.3 meter
f94
L van Zee, M Haynes, A Broeils,
Cornell University
J Salzer, Wesleyan University
Imaging of High Hydrogen Mass-to-Luminosity Ratio
Galaxies
Total number of proposals:
0.9 meter
90
Appendix B
NATIONAL SOLAR OBSERVATORY REPORT
Quarter Ended: 12/31/94
Nights
Hours
Days
Hours
1023
R Altrock, PL/GPSS
Coronal Observations
Evans Solar Facility/SP
74
84
6
34
9
50
10
77
12
48
42
80
91
541
91
544
1945
R Altrock, PL/GPSS
Emission Line Photometer Support
Evans Solar Facility/SP
1937
J Beckers, National Optical Astronomy Observatories
T Rimmele, New Jersey Institute of Technology
High Resolution Imaging
Vacuum Tower/SP
1911
P Bernasconi, P Steiner, U Egger,
Institut fur Astronomie, Zurich
C Keller,
National Optical Astronomy Observatories
Solar Vector Polarimetry
McMP
1940
P Bernasconi, Institut fur Astronomie, Zurich
C Keller,
National Optical Astronomy Observatories
Two-dimensional Solar Vector Polarimetry
Vacuum Tower/SP
1026
T Brown, National Optical Astronomy Observatories
Coronagraph Monitor
Evans Solar Facility/SP
1034
T Brown, National Optical Astronomy Observatories
K Strand, High Altitude Observatory
Flare Patrol (monitoring)
Hilltop Dome/SP
1035
T Brown, National Optical Astronomy Observatories
White Light Patrol (monitoring)
Hilltop Dome/SP
2-
Nights
Hours
Days
Hours
1771
J Elrod, B Armstrong, T Brown
National Optical Astronomy Observatories
Sunspot Drawings - Manual Drawings of Sunspots
Evans Solar Facility/SP
91
69
2
16
1706
K Cheng, NASA Goddard Space Flight Center
J Neff, Pennsylvania State University
Search for New Proto-Planetary System Candidates
McMP
6
60
1138
D Deming, NASA Goddard Space Flight Center
Monitoring Apparent Velocity of Integrated
Sunlight
McMP
1741
J Eaton,
Center of Excellence in Information Systems
Ha Variations in t, Aurigae Binaries and
Cool Supergiants
McMP
17
26
28
57
26
68
3
30
3
28
1807
M Giampapa,
National Optical Astronomy Observatories
G Basri, University of California, Berkeley
C Imhoff, Computer Sciences Corporation
Comparative Synoptic Study of Two T Tauri Stars
McMP
1833
M Giampapa, W Livingston,
National Optical Astronomy Observatories
Stellar Cycles and the Wilson-Bappu Effect
McMP
1888
M Giampapa,
National Optical Astronomy Observatories
V Andretta, University of Naples
Contemporaneous Lambda 5876 and Lambda 10830
Spectra of F and G Dwarfs
McMP
1916
M Giampapa, T Tilleman,
National Optical Astronomy Observatories
Sun as a Star: GONG line
McMP
-3
Nights
Hours
Days
Hours
1769
J Harvey,
National Optical Astronomy Observatories
DAWN (RISE Observations)
11
KPVT
3790
J Harvey,
National Optical Astronomy Observatories
Vacuum Synoptic Program: Daily/Community
86
KPVT
272
1692
K Harvey, Solar Physics Research Corp.
S Tsuneta, University of Tokyo
K Strong, Lockheed Missiles & Space Company
L Acton, Montana State University
Coordinated Observations with YOHKOH
31
KPVT
1918
S Hawley, Michigan State University
M Giampapa,
National Optical Astronomy Observatories
Coordinated Satellite and Ground-based
Observations of YZ Cmi
11
McMP
1934
B Jackson, University of California, San Diego
D Gary, California Institute of Technology
D Webb, ASE, Inc.
H Hudson, University of Hawaii
R Altrock, PL/GPSS
Temporal and Spatial coronal Temperature
Determinations with Height
Evans Solar Facility/SP
18
71
14
86
1915
D Jennings, P Sada, G McCabe, D Deming,
G Bjoraker, NASA Goddard Space Flight Center
Continuing Thermal-IR Spectroscopic Observations
of Jupiter and Comet Shoemaker-Levy
9 Fragment Collision Sites
McMP
10
99
1942
P Kaufmann,
Centro de Radio Astronomia e Applications
J Zirker, National Optical Astronomy Observatories
Search for Positions of Millisecond radio Bursts
Evans Solar Facility/SP
30
Nights
Hours
Days
Hours
1910
C Keller,
National Optical Astronomy Observatories
J Stenflo, High Altitude Observatory
Coherence Effects in Spectral Lines Near the
Solar Limb
McMP
42
1912
R Kupke, D Mickey, B Graves, F Roddier,
University of Hawaii
Curvature Sensing-based Wavefront Sensor for Use
with Solar Adaptive Optics
McMath-Pierce West
56
1852
T Leifsen, P Maltby, M Omang, M Carlsson
University of Oslo
Solar Oscillations in Infrared Spectral Lines
McMP
1848
W Livingston, L Wallace,
National Optical Astronomy Observatories
Monitoring of Atmospheric Trace Gases
McMP
11
1858
W Livingston,
National Optical Astronomy Observatories
Cycle Variability of the Solar Spectrum
McMP
10
96
1860
J LoPresto, Edinboro University of Pennsylvania
A Pierce,
National Optical Astronomy Observatories
Solar Gravitational Redshift
McMP
12
1880
S Martin, California Institute of Technology
K Harvey, Solar Physics Research Corp.
J Zirker, National Optical Astronomy Observatories
O Engvold, University of Oslo
V Gaizauskas, Herzberg Institute of Astrophysics
T Forbes, University of New Hampshire
E Priest, University of St. Andrews
Filament Formation
Evans Solar Facility/SP
Vacuum Tower/SP
16
88
2
18
5-
Nights
Hours
Days
Hours
1135
P Mcintosh, NOAA
T Brown, National Optical Astronomy Observatories
W Marquett, California Institute of Technology
NOAA Monitoring Program
Evans Solar Facility/SP
91
55
9
26
11
63
3
24
11
4
7
46
1892
J Neff, Pennsylvania State University
F Walter, SUNY at Stony Brook
Mapping the Chromospheric Structure of AR Lac
Over a Stellar Cycle
McMP
5
38
1935
D Neidig, PL/GPSS
Demonstrate Ground-based Coronagraphic Detection
of Space Debris
Evans Solar Facility/SP
1938
L November, L Wilkins
National Optical Astronomy Observatories
O Bouchard,
ICP-French Military Service
The Magnetic Force-free Condition with Height in
the Solar Atmosphere
Vacuum Tower/SP
1569
L O'Brien, Southern Illinois University
Laboratory Measurements of Metal Hydrides in the
Near-Infrared
FTS
3
24
1863
A Pierce,
National Optical Astronomy Observatories
J LoPresto, Edinboro University of Pennsylvania
The Absolute Value of the Solar Limb Effects for
Different Fraunhofer Lines
McMP
1868
A Potter, NASA Johnson Space Flight Center
T Morgan, Southwest Research Institute
Studies of Exospheric Emission Lines from Mercury
and the Moon
McMP
1
2
6-
Nights
Hours
Days
Hours
1866
D Rabin,
National Optical Astronomy Observatories
True-Field Imaging Magnetometry in the Near
Infrared
McMP
70
1936
R Radick, PL/GPSS
R Dunn, National Optical Astronomy Observatories
T Rimmele, New Jersey Institute of Technology
Characterization and Upgrade of VTT Optical
Performance
Vacuum Tower/SP
16
126
14
40
16
50
1901
T Rimmele, P Goode,
New Jersey Institute of Technology
R Stebbins, University of Colorado
Oscillation Excitation Mechanisms
Vacuum Tower/SP
1939
G Roumeliotis, University of Sydney
S Keil, PL/GPSS
K Balasubramaniam,
National Optical Astronomy Observatories
P Sturrock, Stanford University
The Vector Magnetic Field below and H-alpha
Filament
Vacuum Tower/SP
1426
S Saar,
Harvard-Smithsonian Center for Astrophysics
J Linsky, University of Colorado
M Giampapa,
National Optical Astronomy Observatories
Synoptic Observations of Magnetic Fields on G & K
Stars
McMP
1494
F Scherb, University of Wisconsin, Madison
Observation of [OIJ6300 Emission from Io
McMP
1881
E Seykora, East Carolina University
Solar Photospheric Observations with a New Active
Unsharp Mask Filter
Evans Solar Facility/SP
18
92
Nights
Hours
Days
Hours
1037
R Smartt, National Optical Astronomy Observatories
Coronal One-Shot (monitoring)
Hilltop Dome/SP
16
50
12
84
27
69
1737
M Smith, C Rinsland,
NASA Langley Research Center
V Devi, College of William and Mary
Long-Path Laboratory Measurements of Infrared
Spectra of CO and HO
FTS
12
84
19
24
1822
M Smith, T Teays, R Wasatonic,
Computer Sciences Corp.
E Guinan, Villanova University
S Baliunas, A Dupree,
D Luttermoser, Applied Research Corp.
Harvard-Smithsonian Center for Astrophysics
K Nordsieck, University of Wisconsin, Madison
Radial Velocity Observations of Alpha Ori, Alpha
Sco, and Alpha Her
McMP
1884
M Smith, Computer Sciences Corp.
Rapid Lambda 6678 Line Profile Variability in
Gamma cas
McMP
56
1913
J Stauffer,
Harvard-Smithsonian Center for Astrophysics
H Bond, Space Telescope Science Institute
V471 Tau HST Support
McMP
11
1356
K Strassmeier, University of Vienna
Doppler Imaging of Spotted Chromospherically
Active Stars
McMP
1890
G Tagliaferri, Osservatorio Astronomico di Brera
T Fleming, University of Arizona
R Pallavicini, Osservatorio Astrofisico Arcetri
G Cutispoto, Osservatorio Astrofisico di Catania
Spectroscopic Study of Cool Stars Serendipitously
Discovered in EUV Surveys
McMP
46
Nights
Hours
Days
Hours
1823
I Tuominen, T Hackman, J Huovelin, L Jetsu,
University of Helsinki
N Piskunov, University of Western Ontario
SSaar,
Harvard-Smithsonian Center for Astrophysics
Surface Imaging of Two Active Stars: HD 199178
and HD 82558
McMP
19
59
1862
O White, High Altitude Observatory
W Livingston,
National Optical Astronomy Observatories
The Sun as a Star: Ca II K Variability
McMP
3
19
79
209
1024
S Worden, OSUDRE/ADEW
S Keil, PL/GPSS
Solar Rotation 3898-3954A
Evans Solar Facility/SP
Total number of proposals: 54
APPENDIX C
US Sites Safety Report
Following is the summary of recordable occupational injuries and illnesses for the US sites as reported
on the respective CY 1994 OSHA 200 logs. As required, the respective data will be posted at each site
no later than 1 February.
KPNO
NSO/SP
Tucson
Total
Fatalities
Injuries involving days off
or days of restricted work
activity or both
2
3
2
7
Injuries involving days off
2
3
2
7
Days off from work
6
71
4
8
Days of restricted work
activity
0
0
0
0
Injuries without lost
workdays
2
0
4
6
Illnesses
Total recordable
injuries/illnesses:
14
Mountainwide Fire Alarm Systems: At KPNO, fire alarm systems were installed in all the buildings. A
second phase which includes transmitters and a central station receiver and notification system was started
and is nearing completion. At NSO/SP, a similar mountainwide system comprised of individual fire alarm
systems, transmitters and central station receiver was also started and nearing completion.
LPG Tank Farm: At NSO/SP the LPG tank farm was repiped and brought up to current code.
NSO/SP Volunteer Fire Department: Increased their membership to fifteen persons. Because they are a
county fire district this increasewill enable state funds for additional equipment. The departmentwas also
reclassified from class 10 to class 8 which in effect enable additional state funds for the department.
Permits, Emissions Reports: Various county air pollution permits were renewed and the associated
emissions reports filed for the Tucson and KPNO sites.
Loss Prevention Reviews: Various reviews were conducted and the resultant recommendations furnished
in regards to the following:
8-m telescope at the critical design review state;
electrostatic discharge survey of all the Tucson electronics labs;
handling of domestic and industrial waste at KPNO;
various PC workstations in regards to ergonomically sound principles.
followup review of WIYN building and site;
fire inspection of NSO/SP facilities by the Holloman Air Force Base Fire Marshall's Office;
16" visitor's telescope at KPNO;
GONG instrument, shelters and sites;
4-m building for damaged asbestos containing insulation; and,
NASA hazard analysis of exposure to liquid mercury, relative to the future operation of the NASA-JSC
liquid mercury telescope at NSO Cloudcroft facility.
Training: First responders at the KPNO and NSO/SP site received refresher training in first aid and CPR.
Tucson first responders trained for potential ammonia hydroxide spill.
Maintenance personnel in Tucson were retrained in the proper use of respirators for the protection from
asbestos, paints and solvents; personnel at NSO/SP received refresher training in minor abatement of
asbestos containing materials.
Three Tucson staff attended a seminar on workplace violence.
The NSO/SP site Safety Officer and Maintenance Supervisor attended collateral Safety Officer Training at
White Sands Missile Range.
Hazardous Materials/Chemical Waste Disposal: Several drums of various chemical wastes -mainly nonhazardous - were sampled, analyzed and properly disposed. Approximately 300 pounds of mildly
radioactive mirror polishing compound containing ThO which was discovered in the Optics Shop is
awaiting proper disposal.
Memberships: NSO/SP became a member of the Southwest Federal Safety & Health Council. The NOAO
Safety Officer became a member of the National Fire Protection Association.
APPENDIX C
CTIO Safety Report
CTLO Recordable Occupational Injuries: October 1993 - September 1994 (FY 1994)
Fatalities:
0
Injuries involving days off or days of restrictedwork activities or both:
(<p
Injuries involving days off:
Days off from work:
Days of restricted work activity:
Injuries without lost workdays:
3
360
0
0
CTLO Recordable Occupational Injuries: October - December 1994
Fatalities:
Injuries involving days off or days of restricted work activities or both:
Injuries involving days off:
Days off from work:
Days of restricted work activity:
Injuries without lost workdays:
There were no occupational illness recorded at CTIO.
0 ,„
o
-
(0 -A
2
95
0
1