RKV: A catalogue of absorption-line systems in QSO's spectra

Authors: Ryabinkov A.I., Kaminker A.D., Varshalovich D.A.

Created on January 10 2003, and significantly updated on February 02 2006

• Introduction
• Manual
• Query Results
• References

The presented catalog contains a compilation of basic information on absorption-line systems (ALSs) in QSO spectra. The data are taken from publications available to the authors up to January 2003. The catalog consists of Introduction, QSO Data Base, and list of references, which (1th edition) are available also at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/vol/page. The catalog contains data on 874 QSOs whose characteristics of spectral observations are collected in full version of Table 2 Absorption systems. The data on QSOs are based on the catalog of M.-P. Veron-Cetty & P.Veron (2001) [A&A, 374, p.92] "A catalog of quasars and active nuclei (10th edition)" (site: vizier.hia.nrc.ca/cats/Usage.htx). Full version of Table 2 (the Query Results) contains information on 20837 absorption lines detected in the spectra of 784 QSOs. These lines form 11298 absorption systems. The list of references contains all numerated literature sources indicated in table Absorption systems.

Table2 Absorption systems contains the following information on spectral observations of the QSOs and on detected ALSs: the names of QSOs (J2000 and Q1950) whose spectral observations are presented in literature, parameters of spectral observations, and characteristics of absorption lines combined into the systems. The catalog includes absorption line systems consisting of lines of heavy-elements, lines of neutral hydrogen (HI), Lyman limit systems (LLS), damped Lyα absorption systems (DLA), and broad absorption-line systems (BAL). In standard definitions LLSs are optically thick at the HI Lyman limit (912 A ) systems corresponding to HI column densities N(HI) > 2 x 10 ¹⁷ cm ^-2 , DLA are systems corresponding to high HI column densities N(HI) > 2 x 10 ²⁰ cm ^-2 , BAL are systems characterized by wide absorption troughs produced by ions with outflow velocity extending from 0 up to 60,000 km/s relative to the QSO emission redshift. We rule out absorption systems consisting only of one heavy-element absorption line. On the other hand, the catalog includes the systems consisting only of one line of HI. We rule out also Galactic interstellar absorption lines.

Observational data on each QSO are delimited in Table 2 Absorption systems by a pair of horizontal solid lines. First data below upper solid line contain two names of the QSO (J2000 and Q1950). The space between upper and lower solid lines contain a few sets of observational data. Each set begins (from top to bottom) by its own parameters of spectral observations delimited by two horizontal dash lines. They include (from left to right):

• the interval of wavelengths used in the observations (Å),
• spectral resolution R = Δλ_obs (Å),
• the signal-to-noise ratio <S/N>, averaged over whole spectral interval or, in some cases, a threshold (minimal) value of absorption equivalent widths used by authors as a criterion of line detection either in the observer frame W_min or in the rest frame W_rest,min (in Å),
• the emission-line redshift z_em,
• the reference (in square brackets).

Below the lower dash lines the next characteristics of absorption systems and lines are listed:

for HI and heavy-elements

• the absorption-system redshift z _abs,
• name of the ion identified, Ion,
• laboratory wavelength λ_lab in Å, (comprised in braces),
• observed wavelength λ_obs in Å,
• error σ(λ_obs) of the value λ_obs at 1 σ significance level,
• absorption-line equivalent width W _obs(Å) (measured in the observer frame) or column density of the ion log N(cm^-2) in the cases marked by the letter N,
• error σ(W_obs ) of the value W_obs or the value log N (cm^-2), respectively;

for LLS

• the absorption-system redshift z_abs,
• the designation " LLS " instead of "Ion";

for DLA systems

• the absorption-system redshift z_abs,
• the designation "DLA" instead of "Ion",
• the observational equivalent width W_obs(Å) of the damped Lyα absorption line or the column density for HI log N(HI)(cm^-2) in the cases marked by the letter N;

for BAL systems

• averaged value of z_abs,
• the designation "BAL" or "trough" (according to referenced papers) instead of "Ion",
• names of identified ions,
• width of the trough (Δz_abs) (indicated in brackets).

All reported wavelengths are vacuum.

The space between two solid lines in Table Absorption systems may contain a few sets of observational data on spectra of the QSOs registered in different observations and presented by different authors. Each set of observational data begins from its own parameters of spectral observations delimited by the pair of horizontal dash lines as described above.

Notations:

• the letter "B" indicates that the line is blended by non-identified ion(s);
• the sign "?" denotes "possible" and indicates an uncertainty of detection or identification of the absorption line;
• the sign "+" following by a name of additional ion designates that the absorption line may be identified also as a line of another ion and may belong to another absorption system with another z_abs, indicated in brackets after the ion's name. There are cases when a few such additional identifications of one absorption line are presented.
• symbol "nd" designates absence of corresponding data in one of positions described above;
• phrase "no line list" designates absence of all characteristics (excepting z_abs and the ion's name) of an absorption line identified in the referenced paper;
• symbol "abs" instead of an ion's name indicates that only value z_abs is available in the referenced paper;
• words "no line" designate that absorption lines are not detected or not identified in the observational spectrum;
• words "only Galactic interstellar lines" indicate that only absorption lines of interstellar gas of our Galaxy are identified in the spectrum;
• symbol "*" designates comments.

The authors are planning to replenish the catalog regularly. Any remarks and comments would be greatly appreciated.

E-mail addresses for contacts:

Ryabinkov A.I.: calisto@rbcmail.ru
Kaminker A.D.: kam@astro.ioffe.ru
Varshalovich D.A.: varsh@astro.ioffe.ru