96 research outputs found
Ages and Metallicities of Young Globular Clusters in the Merger Remnant NGC 7252
UV-to-visual spectra of eight young star clusters in the merger remnant and
protoelliptical galaxy NGC 7252, obtained with the Blanco 4-m telescope on
Cerro Tololo, are presented. These clusters lie at projected distances of 3-15
kpc from the center and move with a velocity dispersion of 140+/-35 km/s in the
line of sight. Seven of the clusters show strong Balmer absorption lines in
their spectra [EW(H-beta)= 6-13 Angstrom], while the eighth lies in a giant HII
region and shows no detectable absorption features.
Based on comparisons with model-cluster spectra by Bruzual & Charlot (1996)
and Bressan, Chiosi, & Tantalo (1996), six of the absorption-line clusters have
ages in the range of 400-600 Myr, indicating that they formed early on during
the recent merger. These clusters are globular clusters as judged by their
small effective radii and ages corresponding to ~100 core crossing times. The
one emission-line object is <10 Myr old and may be a nascent globular cluster
or an OB association.
The mean metallicities measured for three clusters are solar to within
+/-0.15 dex, suggesting that the merger of two likely Sc galaxies in NGC 7252
formed a globular-cluster system with a bimodal metallicity distribution. Since
NGC 7252 itself shows the characteristics of a 0.5-1 Gyr old protoelliptical,
its second-generation solar-metallicity globulars provide direct evidence that
giant ellipticals with bimodal globular-cluster systems can form through major
mergers of gas-rich disk galaxies.Comment: 34 pages, incl. 6 figures in EPS format, AAS LaTeX, to be published
in AJ, Vol. 116, Nov. 199
An Attempt to Observe Debris from the Breakup of a Titan 3C-4 Transtage
In February 2007 dedicated observations were made of the orbital space predicted to contain debris from the breakup of the Titan 3C-4 transtage back on February 21, 1992. These observations were carried out on the Michigan Orbital DEbris Survey Telescope (MODEST) in Chile with its 1.3deg field of view. The search region or orbital space (inclination and right ascension of the ascending node (RAAN) was predicted using NASA#s LEGEND (LEO-to-GEO Environment Debris) code to generate a Titan debris cloud. Breakup fragments are created based on the NASA Standard Breakup Model (including fragment size, area-to-mass (A/M), and delta-V distributions). Once fragments are created, they are propagated forward in time with a subroutine GEOPROP. Perturbations included in GEOPROP are those due to solar/lunar gravity, radiation pressure, and major geopotential terms. Barker, et. al, (AMOS Conference Proceedings, 2006, pp. 596-604) used similar LEGEND predictions to correlate survey observations made by MODEST (February 2002) and found several possible night-to-night correlations in the limited survey dataset. One conc lusion of the survey search was to dedicate a MODEST run to observing a GEO region predicted to contain debris fragments and actual Titan debris objects (SSN 25000, 25001 and 30000). Such a dedicated run was undertaken with MODEST between February 17 and 23, 2007 (UT dates). MODEST#s limiting magnitude of 18.0 (S\N approx.10) corresponds to a size of 22cm assuming a diffuse Lambertian albedo of 0.2. However, based on observed break-up data, we expect most debris fragments to be smaller than 22cm which implies a need to increase the effective sensitivity of MODEST for smaller objects. MODEST#s limiting size can be lowered by increasing the exposure time (20 instead of 5 seconds) and applying special image processing. The special processing combines individual CCD images to detect faint objects that are invisible on a single CCD image. Sub-images are cropped from six consecutive CCD images with pixel shifts between images being consistent with the predicted movement of a Titan object. A median image of all the sub-images is then created leaving only those objects with the proper Titan motion. Limiting the median image in this manner brings the needed computer time to process all images taken on one night down to about 50 hours of CPU time
Usage of Light Emitting Diodes (LEDs) for improved satellite tracking
With the increasing number of satellite launches, especially in Low Earth Orbit (LEO), optical tracking can offer a convenient enhancement of tracking precision and availability. Spaceborne active illumination devices, such as LED payloads, can offer a significant improvement to optical observations, extending the observability interval to the whole eclipse time and performing optimized flash sequences for identification, orbit determination, attitude reconstruction or low data rate communication. The main features of LED panels for optical tracking mounted on small satellites platforms (and with particular regards to nano-satellite platforms) are outlined in this paper, along with the description of the design drivers. The analysis of the performance is referred to Sun-Synchronous (at 700 km of altitude) and International Space Station (400 km) orbits, while the ground segment and the optical link budget reference design relies on a standard university space debris observation station architecture. The paper also outlines the advantages of using different observation techniques and the variety of flashing patterns. The LEDSAT 1U CubeSat, aiming at demonstrating the effectiveness of an LED-based payload for observation and tracking, is used as a study case for examples of the LED payloads and related operations that are reported and described in this paper
HST-NICMOS Observations of M31's Metal Rich Globular Clusters and Their Surrounding Fields: II. Results
We have obtained HST-NICMOS observations of five of M31's most metal rich
globular clusters: G1, G170, G174, G177 & G280. For the two clusters farthest
from the nucleus we statistically subtract the field population and estimate
metallicities using K-(J-K) color-magnitude diagrams (CMDs). Based on the
slopes of their infrared giant branches we estimate [Fe/H]=-1.22+/-0.43 for G1
and -0.15+/-0.37 for G280. We combine our infrared observations of G1 with two
epochs of optical HST-WFPC2 V-band data and identify at least one LPV based on
color and variability. The location of G1's giant branch in the K-(V-K) CMD is
very similar to that of M107, indicating a higher metallicity than our purely
infrared CMD: [Fe/H]=-0.9+/-0.2.
For the field surrounding G280, we estimate the metallicity to be -1.3 with a
spread of 0.5 from the slope and width of the giant branch. Based on the
numbers and luminosities of the brightest giants, we conclude that only a small
fraction of the stars in this field could be as young as 2 Gyr, while the
majority have ages closer to 10 Gyr.
The K-band luminosity functions (LFs) of the upper few magnitudes of G1 and
G280, as well as for the fields surrounding all clusters, are indistinguishable
from the LF measured in the bulge of our Galaxy. This indicates that these
clusters are very similar to Galactic clusters, and at least in the surrounding
fields observed, there are no significant populations of young luminous stars.Comment: AAS LaTeX v5.0, 17 pages. Submitted to the A
Deviations from the Local Hubble Flow. I. The Tip of the Red Giant Branch as a Distance Indicator
The properties of the velocity field in the local volume (cz < 550 km/s) have
been difficult to constrain due to a lack of a consistent set of galaxy
distances. The sparse observations available to date suggest a remarkably quiet
flow, with little deviation from a pure Hubble law. However, velocity field
models based on the distribution of galaxies in the 1.2 Jy IRAS redshift
survey, predict a quadrupolar flow pattern locally with strong infall at the
poles of the local Supergalactic plane. We probe this velocity field and begin
to establish a consistent set of galactic distances. We have obtained images of
nearby galaxies in the I and V band from the W.M. Keck Observatory and in F814W
and F555W filters from the Hubble Space Telescope. Where these galaxies are
well resolved into stars we may use the Tip of the Red Giant Branch (TRGB) as a
distance indicator. Using a maximum likelihood analysis to quantitatively
measure the I magnitude of the TRGB we determine precise distances to seven
nearby galaxies: Leo I, Sextans B, NGC 1313, NGC 3109, UGC 03755, UGC 06456,
and UGC 07577.Comment: AJ in Press, 54 pages, 30 figures, typos corrected, references added,
postscript version with high resolution figures available at
ftp://deep.berkeley.edu/pub/trgb/trgb.p
BVRI Light Curves for 29 Type Ia Supernovae
BVRI light curves are presented for 27 Type Ia supernovae discovered during
the course of the Calan/Tololo Survey and for two other SNe Ia observed during
the same period. Estimates of the maximum light magnitudes in the B, V, and I
bands and the initial decline rate parameter m15(B) are also given.Comment: 17 pages, figures and tables are not included (contact first author
if needed), to appear in the Astronomical Journa
Optical Light Curves of the Type Ia Supernovae 1990N and 1991T
We present UBVRI light curves for the bright Type Ia supernovae SN 1990N in
NGC 4639 and SN 1991T in NGC 4527 based on photometry gathered in the course of
the Calan/Tololo supernova program. Both objects have well-sampled light curves
starting several days before maximum light and spanning well through the
exponential tail. These data supercede the preliminary photometry published by
Leibundgut et al (1991) and Phillips et al (1992). The host galaxies for these
supernovae have (or will have) accurate distances based on the Cepheid
period-luminosity relationship. The photometric data in this paper provide
template curves for the study of general population of Type Ia supernova and
accurate photometric indices needed for the Cepheid-supernova distance scale.Comment: AAS LaTeX, 30 pages, 10 figures, to appear in the Jan 1998
Astronomical Journal. Figs 1 and 2 (finding charts) not include
Recommended from our members
Catalytic conversion of light alkanes: Quarterly report, January 1-March 31, 1992
The first Quarterly Report of 1992 on the Catalytic Conversion of Light Alkanes reviews the work done between January 1. 1992 and March 31, 1992 on the Cooperative Agreement. The mission of this work is to devise a new catalyst which can be used in a simple economic process to convert the light alkanes in natural gas to oxygenate products which can either be used as clean-burning, high octane liquid fuels, as fuel components or as precursors to liquid hydrocarbon transportation fuel. During the past quarter we have continued to design, prepare, characterize and test novel catalysts for the mild selective reaction of light hydrocarbons with air or oxygen to produce alcohols directly. These catalysts are designed to form active metal oxo (MO) species and to be uniquely active for the homolytic cleavage of the carbon-hydrogen bonds in light alkanes producing intermediates which can form alcohols. We continue to investigate three molecular environments for the active catalytic species that we are trying to generate: electron-deficient porphryinic macrocycles (PHASE I), polyoxometallates (PHASE II), and regular oxidic lattices including zeolites and related structures as well as other molecular surface structures having metal oxo groups (PHASE III)
Dark Matter in the Milky Way's Dwarf Spheroidal Satellites
The Milky Way's dwarf spheroidal satellites include the nearest, smallest and
least luminous galaxies known. They also exhibit the largest discrepancies
between dynamical and luminous masses. This article reviews the development of
empirical constraints on the structure and kinematics of dSph stellar
populations and discusses how this phenomenology translates into constraints on
the amount and distribution of dark matter within dSphs. Some implications for
cosmology and the particle nature of dark matter are discussed, and some
topics/questions for future study are identified.Comment: A version with full-resolution figures is available at
http://www.cfa.harvard.edu/~mwalker/mwdsph_review.pdf; 70 pages, 22 figures;
invited review article to be published in Vol. 5 of the book "Planets, Stars,
and Stellar Systems", published by Springe
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