Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· arXiv e-print (arXiv:astro-ph/0509779)
· On-line Data
· References in the article
· Citations to the Article (8) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (6)
· NED Objects (4)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Predictions and Strategies for Integral-Field Spectroscopy of High-Redshift Galaxies
Authors:
Law, David R.; Steidel, Charles C.; Erb, Dawn K.
Affiliation:
AA(Department of Astronomy, California Institute of Technology, MS 105-24, Pasadena, CA 91125; ) AB(Department of Astronomy, California Institute of Technology, MS 105-24, Pasadena, CA 91125; ), AC(Department of Astronomy, California Institute of Technology, MS 105-24, Pasadena, CA 91125; )
Publication:
The Astronomical Journal, Volume 131, Issue 1, pp. 70-83. (AJ Homepage)
Publication Date:
01/2006
Origin:
UCP
AJ Keywords:
Galaxies: High-Redshift, Galaxies: Kinematics and Dynamics, Instrumentation: Spectrographs
DOI:
10.1086/498683
Bibliographic Code:
2006AJ....131...70L

Abstract

We investigate the ability of infrared integral-field spectrographs to map the velocity fields of high-redshift galaxies, presenting a formalism that can be applied to any telescope and imaging spectrograph system. We discuss the 5 σ limiting line fluxes that current integral-field spectrographs reach and extend this discussion to consider future large-aperture telescopes with cryogenically cooled adaptive reimaging optics. In particular, we simulate observations of spectral line emission from star-forming regions at redshifts z=0.5-2.6 using a variety of spatial sampling scales and give predictions for the signal-to-noise ratio expected as a function of redshift. Using values characteristic of the Keck II telescope and the new OSIRIS spectrograph, we calculate integral-field signal-to-noise ratio maps for a sample of UnGR color-selected star-forming galaxies at redshift z~2-2.6 and demonstrate that OSIRIS will be able to reconstruct the two-dimensional projected velocity fields of these galaxies on scales of 100 mas (~1 kpc at redshift z~2). With signal-to-noise ratios per spatial sample up to ~20, OSIRIS will in some cases be able to distinguish between merger activity and ordered disk rotation. Structures on scales smaller than 1 kpc may be detected by OSIRIS for particularly bright sources and will be easy targets for future 30 m class telescopes.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints