J/MNRAS/451/4346 Early-type stars in SMC and LMC (Smoker+, 2015)
Large- and small-scale structure of the intermediate- and high-velocity clouds
towards the LMC and SMC.
Smoker J.V., Fox A.J., Keenan F.P.
<Mon. Not. R. Astron. Soc., 451, 4346-4359 (2015)>
=2015MNRAS.451.4346S 2015MNRAS.451.4346S (SIMBAD/NED BibCode)
ADC_Keywords: Magellanic Clouds ; Clusters, open
Keywords: ISM: structure -
open clusters and associations: individual: NGC 330 -
open clusters and associations: individual: NGC 346 -
open clusters and associations: individual: NGC 1761 -
open clusters and associations: individual: NGC 2004 -
Magellanic Clouds
Abstract:
We employ CaII K and NaI D interstellar absorption-line spectroscopy
of early-type stars in the Large and Small Magellanic Clouds (LMC,
SMC) to investigate the large- and small-scale structure in foreground
intermediate- and high-velocity clouds (I/HVCs). Data include
FLAMES-GIRAFFE CaII K observations of 403 stars in four open clusters,
plus FEROS or UVES spectra of 156 stars in the LMC and SMC. The FLAMES
observations are amongst the most extensive probes to date of CaII
structures on ∼20-arcsec scales in Magellanic I/HVCs. From the FLAMES
data within a 0.5° field of view, the CaII K equivalent width in
the I/HVC components towards three clusters varies by factors of ≥10.
There are no detections of molecular gas in absorption at intermediate
or high velocities, although molecular absorption is present at LMC
and Galactic velocities towards some sightlines. The FEROS/UVES data
show CaII K I/HVC absorption in ∼60 per cent of sightlines. The range
in the CaII/NaI ratio in I/HVCs is from -0.45 to +1.5dex, similar to
previous measurements for I/HVCs. In 10 sightlines we find CaII/Oi
ratios in I/HVC gas ranging from 0.2 to 1.5dex below the solar value,
indicating either dust or ionization effects. In nine sightlines I/HVC
gas is detected in both Hi and CaII at similar velocities, implying
that the two elements form part of the same structure.
Description:
FLAMES observations towards four open clusters in the LMC and SMC
were retrieved from the ESO archive and are used to study the I/HVCs
towards these galaxies and their variation on small scales.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 101 154 *FEROS and UVES-observed stars towards the
Magellanic Clouds
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Note on tablea1.dat: Stars with RA<2h are in the SMC and with RA>3h in the LMC.
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- Name Name
16- 27 A12 --- AName Alternative name
30- 31 I2 h RAh Right ascension (J2000)
33- 34 I2 min RAm Right ascension (J2000)
36- 40 F5.2 s RAs Right ascension (J2000)
42 A1 --- DE- Declination sign (J2000)
43- 44 I2 deg DEd Declination (J2000)
46- 47 I2 arcmin DEm Declination (J2000)
49- 52 F4.1 arcsec DEs Declination (J2000)
54- 59 F6.2 deg GLON Galactic longitude
61- 66 F6.2 deg GLAT Galactic latitude
68- 73 F6.3 mag Vmag ?=- V magnitude
75- 80 F6.3 mag Bmag ?=- B magnitude
82- 92 A11 --- SpType MK spectral type
93- 95 I3 pix-1 S/NCaK ?=- CaK signal-to-noise ratio
97- 99 I3 pix-1 S/NNaD ?=- NaD signal-to-noise ratio
101 A1 --- Inst [FU] Instrumet (F)eros or (U)VES.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 16-Jun-2016