Element abundances in the Z = 1.920 absorber toward the quasar Q 2206-199 N

Details Element abundances in the Z = 1.920 absorber toward the quasar Q 2206-199 N Element abundances in the Z = 1.920 absorber toward the quasar Q 2206-199 N

Jan 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...241..365b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 241, no. 2, Jan. 1991, p. 365-374.

Astronomy and Astrophysics

Astrophysics

16

Abundance, Galactic Evolution, Interstellar Matter, Metallicity, Quasars, Absorption Spectra, Astronomical Models, Astronomical Spectroscopy, Cosmic Dust, Lyman Alpha Radiation, Zinc, Cosmology, Quasars: General, Galaxies: Evolution, Interstellar Medium: Abundances, Dust

Scientific paper

We present high spectral resolution observations of weak absorption lines from the z = 1.920 damped Lyα system towards Q 2206-199 N with the aim of deriving the metal and dust content in this absorber. We detect absorption lines from Si II, Cr ii and Al III and give an upper limit for Zn II absorption. This metal system is multiple and spans about 135 km s-1. The velocity structure differs for the Si ii and Al III ions which must then originate from different regions. From arguments based on the velocity dispersion, the Si II/Al III ionic ratio and an estimate of the N(Si II)/N(H I) ratio using photoionization models, we find that among the four Si ii components at least two and probably three (spanning about 80 km s-1) are associated with the damped Lyα phase. The Si/H abundance is ˜20 times below solar and our non-detection of Zn ii is consistent with a solar Zn/Si abundance ratio. A low dust content is required to account for the small departure of the Cr/Si from the solar value. Similar low metal and dust contents are found for the other damped Lyα systems at z ˜ 2-3 studied with the same approach. If this remains true for larger samples, this would suggest that most of the heavy elements are formed at lower redshift.
In our observing range, there are also two multiple Mg II systems at z ˜ 1. Both systems span roughly 100 km s-1. The one at lower redshift, z =0.9480, is a new system which has three components of small velocity dispersions b ˜ 8-10 km s-1.

Affiliated with

Also associated with

No associations

Rating

Element abundances in the Z = 1.920 absorber toward the quasar Q 2206-199 N does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Element abundances in the Z = 1.920 absorber toward the quasar Q 2206-199 N, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Element abundances in the Z = 1.920 absorber toward the quasar Q 2206-199 N will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1894603