Mid-IR Spectroscopy of Submm Galaxies: Extended Star Formation in High-z Galaxies

Mid-Infrared Spectroscopy of Submillimeter Galaxies: Extended Star Formation in Massive High-Redshift Galaxies

WaFIRS, a Waveguide Far-IR Spectrometer: Enabling Space-Borne Spectroscopy of High-z Galaxies in the Far-IR and Submm

The discovery of galaxies beyond z~1 which emit the bulk of their luminosity at long wavelengths has demonstrated the need for highsensitivity, broadband spectroscopy in the far-IR/submm/mm bands. Because many of these sources are not detectable in the optical, longwavelength spectroscopy is key to measuring their redshifts and ISM conditions. The continuum source list will increase in the next...

Infrared Spectroscopy of Star Formation in Galaxies

We have observed the Brackett a (4.05 #m) and Brackett "7 (2.17 _m) lines with 7.2" angular and 350 km s -1 velocity resolution in 11 infrared-bright galaxies. From these measurements we derive extinctions, Lyman continuum fluxes, and luminosities due to OB stars. The galaxies observed to date are NGC 3690, M83, NGC 5195, Arp 220, NGC 520, NGC 660, NGC 1614, NGC 3079, NGC 6946, NGC 7714, and Ma...

ALMA resolves extended star formation in high-z AGN host galaxies

We present high-resolution (0.3 arcsec) Atacama Large Millimeter Array (ALMA) 870 μm imaging of five z≈ 1.5–4.5 X-ray detected AGN (with luminosities of L2–8keV > 1042 erg s−1). These data provide a 20 times improvement in spatial resolution over single-dish restframe far-infrared (FIR) measurements. The sub-millimetre emission is extended on scales of FWHM ≈ 0.2 arcsec–0.5 arcsec, correspondin...

Probing Star Formation in Interacting Galaxies Using UV and Mid - IR : The Case of Arp 82

To help understand the effects of galaxy interactions on star formation , we analyze Spitzer infrared and GALEX ultraviolet images of the interacting galaxy pair Arp 82 (NGC 2535/6), and compare to a numerical simulation of the interaction. We investigate the UV and IR properties of several star forming regions (clumps). Using the FUV/NUV colors of the clumps we constrain the ages. The 8 µm and...