2018A&A...609A..85G


Query : 2018A&A...609A..85G

2018A&A...609A..85G - Astronomy and Astrophysics, volume 609A, 85-85 (2018/1-1)

Multiple origins for the DLA at zabs = 0.313 toward PKS 1127-145 indicated by a complex dust depletion pattern of Ca, Ti, and Mn.

GUBER C.R., RICHTER P. and WENDT M.

Abstract (from CDS):

Aims. We aim to investigate the dust depletion properties of optically thick gas in and around galaxies and its origin we study in detail the dust depletion patterns of Ti, Mn, and Ca in the multi-component damped Lymanα (DLA) absorber at zabs=0.313 toward the quasar PKS 1127-145.
Methods. We performed a detailed spectral analysis of the absorption profiles of CaII, MnII, TiII, and NaI associated with the DLA toward PKS 1127-145, based on optical high-resolution data obtained with the UVES instrument at the Very Large Telescope. We obtained column densities and Doppler-parameters for the ions listed above and determine their gas-phase abundances, from which we conclude on their dust depletion properties. We compared the Ca and Ti depletion properties of this DLA with that of other DLAs.
Results. One of the six analyzed absorption components (component 3) shows a striking underabundance of Ti and Mn in the gas-phase, indicating the effect of dust depletion for these elements and a locally enhanced dust-to-gas ratio. In this DLA and in other similar absorbers, the MnII abundance follows that of TiII very closely, implying that both ions are equally sensitive to the dust depletion effects.
Conclusions. Our analysis indicates that the DLA toward PKS 1127-145 has multiple origins. With its narrow line width and its strong dust depletion, component 3 points toward the presence of a neutral gas disk from a faint LSB galaxy in front of PKS 1127-145, while the other, more diffuse and dust-poor, absorption components possibly are related to tidal gas features from the interaction between the various, optically confirmed galaxy-group members. In general, the Mn/CaII ratio in sub-DLAs and DLAs possibly serves as an important indicator to discriminate between dust-rich and dust-poor in neutral gas in and around galaxies.

Abstract Copyright: © ESO, 2018

Journal keyword(s): quasars: absorption lines - galaxies: abundances - intergalactic medium - quasars: individual: PKS1127-145 - dust, extinction - ISM: kinematics and dynamics

Simbad objects: 17

goto Full paper

goto View the references in ADS

Number of rows : 17
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 NAME Magellanic Stream HVC 00 32 -30.0           ~ 918 1
2 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 10471 1
3 ICRF J045608.9-215909 Sy1 04 56 08.9237717400 -21 59 09.399816312 15.76 16.16 16.10 15.9   ~ 176 1
4 4C -02.19 QSO 05 01 12.80988538 -01 59 14.2564557   19.1 18.4 19.04   ~ 552 1
5 HE 0515-4414 QSO 05 17 07.6238702856 -44 10 55.579731312 14.74 15.49 15.16     ~ 112 0
6 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16419 1
7 QSO B0952+179 QSO 09 54 56.82361677 +17 43 31.2221518   17.31 17.23     ~ 206 1
8 LBQS 1026-0045B QSO 10 28 37.0180551648 -01 00 27.526300632   18.41 18.22     ~ 66 0
9 PG 1101-264 QSO 11 03 25.2993421704 -26 45 15.808554720   16.08 16.02     ~ 243 0
10 QSO J1130-1449 QSO 11 30 07.0523452128 -14 49 27.388021944   17.17 16.90 16 16.97 ~ 672 1
11 4C -02.55 QSO 12 32 00.0159535440 -02 24 04.793069304   17.41 17.06 16.4   ~ 408 1
12 QSO J1246-2547 QSO 12 46 46.80203943 -25 47 49.2889822   17.65 17.41 16.96 15.5 ~ 255 1
13 QSO J1422-0001 QSO 14 22 53.3124227808 -00 01 48.987825996   19.71 19.25     ~ 40 0
14 QSO B2204-54 QSO 22 07 43.73329058 -53 46 33.8199643   18.45 18.0 18.20   ~ 148 1
15 QSO B2245-128 QSO 22 47 52.64103656 -12 37 19.7216861   18.5 18.5 17.74   ~ 48 1
16 QSO B2311-373 QSO 23 13 59.7082094616 -37 04 46.215225516   19.0 18.5 19.05   ~ 41 1
17 QSO J2328+0022 QSO 23 28 20.3832928800 +00 22 38.176896792   18.39 18.06     ~ 62 0

To bookmark this query, right click on this link: simbad:objects in 2018A&A...609A..85G and select 'bookmark this link' or equivalent in the popup menu


2022.12.08-16:39:40

© Université de Strasbourg/CNRS

    • Contact