Other Science Areas
The following table shows the contribution that PRVS can make in other areas of science
Science Topic | PRVS Contribution | Requirement |
---|---|---|
Planetary atmospheres | Chemical composition & physics of Solar System planetary atmospheres. | Wide spectral coverage Resolution of few km/s |
Exoplanetary atmospheres | Measurements of exoplanetary atmospheric composition. | Coverage 1-1.8um Accurate flatfield accuracy |
Brown dwarf spectroscopy | Atmospheric spectroscopy to define BD models (mass, gravity, “weather”). Doppler imaging of BD surfaces. | Wide wavelength coverage Resolution ~10km/s |
Low-mass spectroscopic binaries | Fraction of spectroscopic M-L binaries, mass ratios & orbital parameters. | Wide spectral coverage R~50,000 |
Rotational velocities of young stars and low-mass stars | Distribution of vsini in young clusters, and of low mass stars (M, L, T dwarfs). | Wide spectral coverage R~50,000 |
Hot protostellar disks | Use atomic lines (eg [FeII], CI, H2) to probe geometry in disk atmospheres. | Simultaneous coverage from 1.0-1.7µm Resolution ~ few km/s |
Stellar magnetic fields | High sensitivity measurements of magnetic fields using Zeeman splitting. | R~50,000 |
Asteroseismology | Activity of stars across the main sequence. | Wide spectral coverage, R>50,000 |
Jet & shock physics | Use [FeII] lines to measure extinction, excitation, electron density across line profiles. | Simultaneous coverage from 1.0-1.7µm Resolution ~ few km/s |
Masses & ages of nuclear stellar clusters in spiral galaxies | The role of nuclear stellar clusters in defining the properties of the host galaxy. | Wide spectral coverage, R>50,000 |
Fine Structure Constant | Extend measurements z>2.5. | Wide spectral coverage,R~50,000 |
Absorption lines against GRBs | Followup spectroscopy against bright GRBs to measure gas and metallicities at high redshifts. Measure lines of (eg) FeII, MnII, CrII, ZnII for z>2.5. | Rapid time to get on-source. Resolution <10km/s. Wide simultaneous coverage. |