The primary science objectives of the COS Instrument Development
Team (IDT) are to study the
origins of large scale structure in the Universe, the formation and
evolution of galaxies, the origin of stellar and planetary systems,
and the cold interstellar medium.
| ID |
Title & Description |
Orbits |
| ---- |
IGM |
253 |
| 2035 |
Cool, Warm and Hot Gas in the Cosmic Web and in Galaxy Halos:
Observations of 17 QSOs to study the cool,warm and hot gas in the cosmic web and in galaxy halos. The goal of this program is to obtain the information that will allow an assessment of the baryonic content in the IGM.
|
100 |
| 2019 |
Studies of the He II Reionization Epoch:
Observations of He II absorption will be used as diagnostics of the ionizing sources and radiative transport over large (30-50 Mpc) distances through the IGM
|
27 |
| 2045 |
Great Wall Tomography:
Observe several targets behind the Great Wall, a typical galaxy filament in the Universe, to perform a "cosmic tomography".
|
19 |
| 2044 |
QSO Absorbers, Galaxies and Large-Scale Structures in the Local Universe:
Probe the large scale structure of baryons in the universe, including addressing questions of baryon fraction, physical conditions and relationships between absorbers and large-scale structures of galaxies.
|
100 |
| ---- |
Star Forming Galaxies |
20 |
| 2037 |
Star Formation/Lyman-Alpha:
Using a sample of 20 star-forming galaxies, characterize the Lyman-alpha properties and establish correlations with fundamental galaxy properties.
|
20 |
| 2051 |
Observations of I Zwicky 18:
Observations using COS's high sensitivity to surface brightness to detect UV gas emission, especially
HeII 1640, in I Zwicky 18.
|
7 |
| ---- |
Warm-Hot ISM |
61 |
| 2034 |
Warm and Hot ISM in and near the Milky Way:
Observations of 10 AGN's situated beyond Milky Way high velocity clouds will be used to obtain high quality absorption line profiles for C IV, Si IV and N V in the gas.
|
28 |
| 2021 |
STIS high resolution observations of the local ISM:
Observations of bright early-type B stars located within 150pc of the Sun to probe the absorption properties of the interstellar gas associated with the local cavity.
|
4 |
| 2022 |
Sampling the Local ISM with hot white dwarfs:
Observations of hot white dwarfs located within 150pc of the Sun to probe the absorption properties of the interstellar gas associated with the local cavity.
|
6 |
| 2023 |
An Absorption Study of Galactic Intermediate Velocity Clouds Using Hot Stars in Globular Clusters
:
UV bright hot post-AGB stars located within globular clusters to sample the UV absorption properties of the intervening line-of-sight interstellar gas.
|
17 |
| 2024 |
Sampling the Interstellar Gas Between the Milky Way and Triangulum Galaxies
:
Interstellar absorption measurements towards the star UIT-236 located within M33 to sample gas associated with the inner and outer halo of the Milky Way, the intergalactic medium, and gas in the M33 galaxy.
|
6 |
| ---- |
Cold ISM |
65 |
| 2020 |
Cold ISM:
Observations of interstellar spectra, translucent clouds, molecular lines and bands, and extinction curves.
|
65 |
| ---- |
X-Ray Binaries |
26 |
| 2018 |
X-Ray Binaries:
UV Spectra and contemporaneous optical spectra of soft X-ray transients in their quiescent states. The data will be used to establish the broadband spectral energy distribution and measure emission line strengths and widths in the UV.
|
26 |
| ---- |
Cool Stars |
60 |
| 2043 |
Alien Dwarfs:
COS spectra will be used to determine whether metal poverty changes the heating, structure, and the dynamics of the outer layers of these dwarfs.
|
8 |
| 2038 |
Brown Dwarf Activity:
Obtain UV spectra of brown dwarfs to study their outer atmospheres, molecular hydrogen emission, older and younger varieties.
|
29 |
| 2039 |
Activity of Solar Mass Stars from Cradle to Grave:
Study how chromospheric and coronal activity of stars decline as stars lose angular momentum and magnetic fields with age.
|
5 |
| 2041 |
Accretion Flows and Winds of Pre-Main Sequence:
Obtain spectra of T Tauri stars with different inclination angles with respect to the line of sight to determine the temperature distributions, flow velocities, and column densities.
|
16 |
| 2040 |
Metal Deficient Chromospheres of Old Giants:
Study Giants with very low metal abundances to test the mechanisms of their chromospheres.
|
2 |
| ---- |
Planetary Transits |
20 |
| 2042 |
Atmosphere of a Transiting Planet:
Observations at different orbital locations to identify the chemical content, size, temperature, and flows in the atmosphere of the transiting planet.
|
20 |
| ---- |
Solar System |
46 |
2026 |
Deep Search for an Oxygen Atmosphere on Callisto:
Search for 1340 and 1356Å O emission from Callisto, to detect or place strong limits on the presence of a hypothesized O2 atmosphere.
|
4 |
| 2027 |
Sleuthing the Source of Distant Cometary Activity:
Far-UV observations to probe the causes of cometary activity beyond 3 AU. |
6 |
| 2028 |
NUV Spectra of Bright Kuiper Belt Objects:
Obtain NUV spectra of bright Kuiper belt objects to observe NUV KBO reflectance slopes and to compare/contrast different KBO spectra.
|
3 |
| 2031 |
Imaging of Mid-UV Emissions from Io in Eclipse:
First images of Io's 2000-3000Å auroral emissions, to determine whether emission is concentrated over volcanos or over the sub-Jovian point.
|
1 |
| 2030 |
Io's Atmospheric Response to Eclipse:
Study response of Io's SO2 atmosphere to eclipse egress in the NUV, and the FUV auroral response in and after eclipse.
|
6 |
| 2029 |
Spatial Distribution of Io's Atmosphere:
Observe the disk-integrated longitudinal distribution of Io's atmosphere with STIS to provide complementary disk-resolved information at key locations.
|
16 |
| 2032 |
Plutos Mid-UV Reflectance:
Measure Pluto's albedo below 2100Å, to better constrain surface composition. |
5 |
| 2033 |
Search for Hydrocarbons and Nitriles in Pluto's Atmosphere:
Spectra from 2080-2480Å and 2800-3200Å covering absorption bands of the hydrocarbon diacetylene and the nitrile cyanoacetylene.
|
5 |
