Brown dwarfs are objects that form like stars but have insufficient mass to fuse hydrogen in their cores. As such, they cool substantially over time, achieving planet-like atmospheres and physical dimensions. Brown dwarf spectra exhibit complex molecular and atomic absorption features, requiring spectral resolutions of several thousands for abundance and kinematic analyses. These objects are also intrinsically faint, and emit the majority of their luminous flux in the IR. Such properties are ideally suited for FIRE.

Brown Dwarf Infrared Spectrum

Infrared spectrum of a bright brown dwarf, illustrating an abundance atmospheric
features from steam and methane. (A. Burgasser)

Gamma-ray bursts (GRBs) are believed to originate in the catastrophic death of massive stars and are among the most energetic events observed in the universe at all epochs. Most GRBs are accompanied by optical afterglows that can initially be several magnitudes brighter than the brightest quasars known. As many as 20% of all GRBs are estimated to occur at z > 5; GRB 050904 has recently been identified at z = 6.3.

Given their association with massive star formation, GRB afterglows may be a better probe than quasars for studying nascent galaxies at very high redshift. However, heavily obscured GRBs or events occurring at z > 6 have most of their optical light extinguished by local dust or neutral gas in the IGM. Several of these optically dark GRBs have been localized, but never followed up with IR spectroscopy. A high-throughput, high-sensitivity IR spectrometer is essential for studying the host environment that powers the GRB event at high redshift.

Optical and Near-IR Images of GRB050904

Optical (R,I) and near-IR (Y,J,H,K) images of GRB050904, a burst whose
redshift was estimated at 6.28 from its lack of optical flux. (L. Cowie)

Infrared spectroscopy is an important tool for exploring the atmospheres and surface compositions of planets in our own Solar System. In much the same way as with brown dwarf studies, IR spectra can be used to measure absorption from methane and water in the atmospheres of the gas giant planets. Reflected sunlight spectra provide information about the makeup of the outer, cold, icy planets. It also can be used to study the surfaces of icy satellites in the Kuiper Belt, planetary moons, and the debris tails of comets.

Sunlight Spectra (Pluto and 2003UB13)

Spectra of sunlight reflected from the surface of Pluto (red) and 2003UB13,
the so-called "10th planet" beyond Pluto's orbit. Both show signatures of
methane absorption in the near-IR. (M. Brown)