2005A&A...443..525S


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.12CET20:58:41

2005A&A...443..525S - Astronomy and Astrophysics, volume 443, 525-533 (2005/11-4)

CaII K observations of QSOs in the line-of-sight to the Magellanic Bridge.

SMOKER J.V., KEENAN F.P., THOMPSON H.M.A., BRUENS C., MULLER E., LEHNER N., LEE J.-K. and HUNTER I.

Abstract (from CDS):

We describe medium-resolution spectroscopic observations taken with the ESO Multi-Mode Instrument (44Sc emmi) in the Ca44Sc II K line (λair=3933.661Å) towards 7 QSOs located in the line-of-sight to the Magellanic Bridge. At a spectral resolution R=λ/Δλ=6000, five of the sightlines have a signal-to-noise (S/N) ratio of ∼20 or higher. Definite Ca absorption due to Bridge material is detected towards 3 objects, with probable detection towards two other sightlines. Gas-phase Ca44Sc II K Bridge and Milky Way abundances or lower limits for the all sightlines are estimated by the use of Parkes 21-cm H44Sc I emission line data. These data only have a spatial resolution of 14-arcmin compared with the optical observations which have milli-arcsecond resolution. With this caveat, for the three objects with sound Ca44Sc II K detections, we find that the ionic abundance of Ca44Sc II K relative to H44Sc I, A=log(N(CaK)/N(H44Sc I)) for low-velocity Galactic gas ranges from -8.3 to -8.8dex, with H44Sc I column densities varying from 3-6x1020cm–2. For Magellanic Bridge gas, the values of A are ∼0.5dex higher, ranging from ~-7.8 to -8.2dex, with N(H44Sc I)=1-5x1020cm–2. Higher values of A correspond to lower values of N(H44Sc I), although numbers are small. For the sightline towards B0251-675, the Bridge gas has two different velocities, and in only one of these is Ca44Sc II tentatively detected, perhaps indicating gas of a different origin or present-day characteristics (such as dust content), although this conclusion is uncertain and there is the possibility that one of the components could be related to the Magellanic Stream. Higher signal-to-noise Ca44Sc II K data and higher resolution H44Sc I data are required to determine whether A changes with N(H44Sc I) over the Bridge and if the implied difference in the metalicity of the two Bridge components towards B0251-675 is real.

Abstract Copyright:

Journal keyword(s): galaxies: Magellanic Clouds - galaxies: Seyfert - ISM: abundances

Simbad objects: 12

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Number of rows : 12

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9140 1
2 ICRF J020213.6-762003 Sy1 02 02 13.6940093296 -76 20 03.062346923   16.95 16.90     ~ 93 1
3 2MASX J02430962-7216476 Sy1 02 43 09.6128590493 -72 16 48.432281446 15.43 16.34 15.86 16.14   ~ 20 0
4 QSO B0251-675 QSO 02 51 55.9685672696 -67 18 00.352679809     17.5     ~ 19 1
5 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5407 1
6 ESO 31-8 Sy1 03 07 35.3443011815 -72 50 02.595498156   15.11 14.98 14.58   ~ 42 0
7 NAME Magellanic Bridge HI 03 11 -77.5           ~ 307 1
8 QSO J0311-7651 BLL 03 11 55.2500768688 -76 51 50.846014733 15.27 16.09 16.10 15.33   ~ 207 1
9 ESO 55-2 Sy2 03 54 00.8518934644 -72 08 01.689414088   15.67 15.7 14.21   ~ 17 0
10 QSO B0355-669 QSO 03 55 47.8828153036 -66 45 33.814027251   17.3       ~ 26 1
11 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14390 1
12 M 15 GlC 21 29 58.33 +12 10 01.2   3       ~ 2857 0

    Equat.    Gal    SGal    Ecl

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2019.12.12-20:58:41

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