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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 198551.0, MPI für Astronomie / Publikationen_mpia
Seeing the Unvierse at redshift one with the
AAT and CIRPASS: A multi-object near-infrared
Authors:Parry, I. R.; Dalton, G. B.; Doherty, M.; Sharp, R. G.; Dean, A. J.; Bunker, A. J.; Lewis, I.; MacDonald, E.; Wolf, C.; Hippelein, H.; Meisenheimer, K.; Moustakas, L. A.
Date of Publication (YYYY-MM-DD):2003
Title of Journal:Bulletin of the American Astronomical Society
Journal Abbrev.:Bulletin of the American Astronomical Society
Issue / Number:3
Start Page:716
End Page:– +
Sequence Number of Article:2003AAS...202.1111P
Review Status:not specified
Audience:Experts Only
Abstract / Description:We present preliminary results from the CIRPASS instrument (Parry et al. 2000 SPIE 4008, 1193) -- a near-infrared fiber-fed spectrograph which was successfully commissioned in its multi-object spectroscopy (MOS) mode on the 4-m Anglo Australian Telescope in October 2002. The high resolving power of λ / Δ λ FWHM≈ 5000 enables us to work effectively in the low-background regions between the OH sky lines in the J- and H-bands (1.0-1.7 μ m). CIRPASS-MOS has 150 fibres each of 1.6'' diameter, deployable over a 40'-wide area. A natural project for CIRPASS-MOS is tracing star formation at z ∼ 1 using robust indicators such as Hα , redshifted into the near-infrared. We demonstrated this capability in our AAT observations last October, by observing some galaxies from the Calar Alto Deep Imaging Survey (CADIS) selected from a narrow redshift interval at z=0.88 by their [Oriptsize II] 3727 Å line emission observed in extensive Fabry-Perot observations (Hippelein et al. 2003, astro-ph/0302116). The Hα is found at ≈ 1.247 μ m in a very clean (OH line-free) region of the night-sky spectrum, and we were able to detect Hα for a number of these galaxies. We demonstrated that CIRPASS achieved its design sensitivity: in a stacked 12-hour exposure we detected lines as faint as 4x 10-17 ergs cm-2 s-1 at 10 σ (for Δ vFWHM ∼ 300 km/s). This corresponds to an Hα flux at z ∼ 1 equivalent to an unobscured star formation rate of 2 h70}-2 M{sun yr-1 at z=1 (Ω M=0.3, Ω Λ =0.7), comparable to the star formation rate of the Milky Way today. We also successfully targeted a number of galaxies with photometric redshifts z ∼ 1, and broad-band colours indicating star formation. We are currently installing a 2kx 2k detector on CIRPASS, which will double the wavelength coverage to 2100 Å , and hence our ability to successfully target photometrically-selected galaxies over a range of redshifts will be greatly increased. Bibtex entry for this abstract Preferred format for this abstract (see
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
External Affiliations:AB(Oxford Astrophysics), AC(Institute of
Astronomy, Cambridge), AD(Institute of Astronomy,
Cambridge), AE(Institute of Astronomy,
Cambridge), AF(Institute of Astronomy,
Cambridge), AG(Oxford Astrophysics), AH(Oxford
Astrophysics), AI(Oxford Astrophysics), AJ(MPIA
Heidelberg), AK(MPIA Heidelberg), AL(STScI)
Identifiers:URL: [ID No:1]
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