Deuterium to hydrogen towards QSO 1009+2956 from a mesoturbulent model

Abstract We present a new analysis of the deuterium absorption at z = 2.504 towards the quasar Q1009+2956 using the mesoturbulent model which accounts for possible correlations in the large-scale velocity field. We obtain a slightly higher deuterium-to-hydrogen ratio D/H ≈ (3.5–5.0) × 10−5 as compared with the recent measurement D/H ≈ (3.3–4.5) × 10−5 (68% C.L.) performed by Burles and Tytler (1998b) using the usual microturbulent approximation which assumes that the velocity field is uncorrelated. Other mesoturbulent calculations of the D-abundances at z = 3.572 towards Q1937–1009 and at z = 0.701 towards Q1718+4807 (the systems showing ‘low’ and possibly ‘high’ D/H values, respectively, in the microturbulent approaches) agree with the present one with the errors of measurements. Thus, the mesoturbulent analysis does not reveal any spatial variations of D/H and supports the standard homogeneous model of big bang nucleosynthesis.

[1]  F. Takahara,et al.  New aspects of absorption‐line formation in intervening turbulent clouds ‐‐ III. The inverse problem in the study of H+D profiles , 1999 .

[2]  F. Takahara,et al.  Measurability of Kinetic Temperature from Metal Absorption-Line Spectra Formed in Chaotic Media , 1998, astro-ph/9809166.

[3]  M. Giavalisco,et al.  Infrared Observations of Nebular Emission Lines from Galaxies at z ≃ 3 , 1998, astro-ph/9806219.

[4]  F. Takahara,et al.  The D/H Ratio at z = 3.57 toward Q1937–1009 , 1998, astro-ph/9802110.

[5]  C. Churchill,et al.  The Kinematic Composition of Mg II Absorbers , 1997, astro-ph/9712235.

[6]  R. Steiger,et al.  Primordial Nuclei and Their Galactic Evolution , 1998 .

[7]  S. Burles,et al.  The Deuterium Abundance Towards Q1937-1009 , 1997, astro-ph/9712108.

[8]  S. Burles,et al.  The Deuterium Abundance toward QSO 1009+2956 , 1997, astro-ph/9712109.

[9]  Toshitaka Kajino,et al.  Origin of Matter and Evolution of Galaxies , 1997 .

[10]  I. Mazets,et al.  New aspects of absorption line formation in intervening turbulent clouds — II. Monte Carlo simulation of interstellar H+D Lyα absorption profiles , 1997 .

[11]  F. Takahara,et al.  New aspects of absorption line formation in intervening turbulent clouds - I. General principles , 1997, astro-ph/9710122.

[12]  H. Kurki-Suonio,et al.  Stochastic Isocurvature Baryon Fluctuations, Baryon Diffusion, and Primordial Nucleosynthesis , 1996, astro-ph/9606011.

[13]  H. Rottgering,et al.  THE GASEOUS ENVIRONMENTS OF RADIO GALAXIES IN THE EARLY UNIVERSE : KINEMATICS OF THE LYMAN ALPHA EMISSION AND SPATIALLY RESOLVED HI ABSORPTION , 1996, astro-ph/9608092.

[14]  E. L. Wright,et al.  The Cosmic Microwave Background Spectrum from the Full COBE FIRAS Data Set , 1996, astro-ph/9605054.

[15]  G. Fuller,et al.  Nucleosynthesis in the presence of primordial isocurvature Baryon fluctuations , 1994, astro-ph/9410027.

[16]  E. Ellingson,et al.  Mg II absorption by previously known galaxies at z≃0.5 , 1992 .

[17]  S. Cristiani,et al.  Discovery of Z of about 1 galaxies causing quasar absorption lines , 1992 .

[18]  M. Donahue,et al.  New photoionization models of intergalactic clouds , 1991 .

[19]  J. Silk,et al.  Birth of Galaxies , 1990 .