EDP Sciences
Free Access
Issue
A&A
Volume 582, October 2015
Article Number A59
Number of page(s) 90
Section Interstellar and circumstellar matter
DOI https://doi.org/10.1051/0004-6361/201425190
Published online 07 October 2015

Online material

Appendix A: Additional figures

thumbnail Fig. A.1

Example Ca ii H and K spectra towards the seven clusters observed with FLAMES-GIRAFFE.

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thumbnail Fig. A.2

FLAMES-GIRAFFE Ca ii K spectra towards NGC 330 in the SMC. Data are in the LSR and the spectral resolution is ~16 km s-1.

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thumbnail Fig. A.2

continued. NGC 330 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.2

continued. NGC 330 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.2

continued. NGC 330 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.2

continued. NGC 330 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.2

continued. NGC 330 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.2

continued. NGC 330 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.3

FLAMES-GIRAFFE Ca ii K spectra towards NGC 346 in the SMC. Data are in the LSR and the spectral resolution is ~16 km s-1.

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thumbnail Fig. A.3

continued. NGC 346 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.3

continued. NGC 346 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.3

continued. NGC 346 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.3

continued. NGC 346 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.3

continued. NGC 346 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.3

continued. NGC 346 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.4

FLAMES-GIRAFFE Ca ii K spectra towards NGC 1761 (LH 09) in the LMC. Data are in the LSR and the spectral resolution is ~16 km s-1.

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thumbnail Fig. A.4

continued. NGC 1761 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.4

continued. NGC 1761 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.4

continued. NGC 1761 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.4

continued. NGC 1761 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.4

continued. NGC 1761 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.4

continued. NGC 1761 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.5

FLAMES-GIRAFFE Ca ii K spectra towards NGC 2004 in the LMC. Data are in the LSR and the spectral resolution is ~16 km s-1.

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thumbnail Fig. A.5

continued. NGC 2004 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.5

continued. NGC 2004 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.5

continued. NGC 2004 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.5

continued. NGC 2004 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.5

continued. NGC 2004 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.5

continued. NGC 2004 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.6

FLAMES-GIRAFFE Ca ii K spectra towards NGC 3293 in the Milky Way. Data are in the LSR and the spectral resolution is ~16 km s-1.

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thumbnail Fig. A.6

continued. NGC 3293 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.6

continued. NGC 3293 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.6

continued. NGC 3293 Ca ii FLAMES spectra.

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thumbnail Fig. A.6

continued. NGC 3293 Ca ii FLAMES spectra.

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thumbnail Fig. A.7

FLAMES-GIRAFFE Ca ii K spectra towards NGC 4755 in the Milky Way. Data are in the LSR and the spectral resolution is ~16 km s-1.

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thumbnail Fig. A.7

continued. NGC 4755 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.7

continued. NGC 4755 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.7

continued. NGC 4755 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.7

continued. NGC 4755 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.8

FLAMES-GIRAFFE Ca ii K spectra towards NGC 6611 in the Milky Way. Data are in the LSR and the spectral resolution is ~16 km s-1.

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thumbnail Fig. A.8

continued. NGC 6611 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.8

continued. NGC 6611 Ca ii FLAMES-GIRAFFE spectra.

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thumbnail Fig. A.9

Ca ii K spectra towards NGC 330 showing the spectra of 16 star-to-star pairs in which the maximum difference in the equivalent width was detected between a velocity of 35 and +35 km s-1 in the LSR. Each star is only plotted once.

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thumbnail Fig. A.10

Ca ii K spectra towards NGC 346 showing the spectra of 16 star-to-star pairs in which the maximum difference in the equivalent width was detected between a velocity of 35 and +35 km s-1 in the LSR. Each star is only plotted once.

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thumbnail Fig. A.11

Ca ii K spectra towards NGC 1761 showing the spectra of 16 star-to-star pairs in which the maximum difference in the equivalent width was detected between a velocity of 60 and +30 km s-1 in the LSR. Each star is only plotted once.

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thumbnail Fig. A.12

Ca ii K spectra towards NGC 2004 showing the spectra of 16 star-to-star pairs in which the maximum difference in the equivalent width was detected between a velocity of 35 and +35 km s-1 in the LSR. Each star is only plotted once.

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thumbnail Fig. A.13

Ca ii K spectra towards NGC 3293 showing the spectra of 16 star-to-star pairs in which the maximum difference in the equivalent width was detected between a velocity of 80 and +60 km s-1 in the LSR. Each star is only plotted once.

Open with DEXTER

thumbnail Fig. A.14

Ca ii K spectra towards NGC 4755 showing the spectra of 16 star-to-star pairs in which the maximum difference in the equivalent width was detected between a velocity of 80 and +60 km s-1 in the LSR. Each star is only plotted once.

Open with DEXTER

thumbnail Fig. A.15

Ca ii K spectra towards NGC 6611 showing the spectra of 16 star-to-star pairs in which the maximum difference in the equivalent width was detected between a velocity of 80 and +100 km s-1 in the LSR. Each star is only plotted once.

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thumbnail Fig. A.16

Top panels: FEROS or UVES Ca ii K (3933 Å) and Na i D1 (5889 Å) profiles towards Galactic and Magellenic stars, showing the observed spectrum in the LSR, Voigt model fit and data-model residual. Bottom panel: corresponding H i data from the GASS (black line) and LABS (dotted red line) surveys.

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thumbnail Fig. A.16

continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.

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thumbnail Fig. A.16

continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.

Open with DEXTER

thumbnail Fig. A.16

continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.

Open with DEXTER

thumbnail Fig. A.16

continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.

Open with DEXTER

thumbnail Fig. A.16

continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.

Open with DEXTER

thumbnail Fig. A.16

continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.

Open with DEXTER

thumbnail Fig. A.16

continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.

Open with DEXTER

thumbnail Fig. A.16

continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.

Open with DEXTER

thumbnail Fig. A.16

continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.

Open with DEXTER

thumbnail Fig. A.16

continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.

Open with DEXTER

thumbnail Fig. A.16

continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.

Open with DEXTER

thumbnail Fig. A.16

continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.

Open with DEXTER

thumbnail Fig. A.16

continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.

Open with DEXTER

thumbnail Fig. A.16

continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.

Open with DEXTER

thumbnail Fig. A.16

continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.

Open with DEXTER

thumbnail Fig. A.16

continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.

Open with DEXTER

thumbnail Fig. A.16

continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.

Open with DEXTER

thumbnail Fig. A.16

continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.

Open with DEXTER

thumbnail Fig. A.16

continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.

Open with DEXTER

thumbnail Fig. A.17

FEROS Ca ii K spectra towards the Magellanic clouds showing the spectra of 16 star-to-star pairs in which the maximum difference in the equivalent width was detected between a velocity of 35 and +35 km s-1 in the LSR. Each star is only plotted once.

Open with DEXTER

thumbnail Fig. A.18

FEROS Na i D spectra towards the Magellanic clouds showing the spectra of 16 star-to-star pairs in which the maximum difference in the equivalent width was detected between a velocity of 35 and +35 km s-1 in the LSR. Each star is only plotted once.

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thumbnail Fig. A.19

Left panels: variation in total Ca ii K column density between the limits in LSR km s-1 shown on the figures as a function of star-to-star sky separation in degrees as observed by FLAMES-GIRAFFE. Right panels: corresponding percentage variation in observed Ca ii K equivalent width. a), b): NGC 330, c), d): NGC 346, e), f): NGC 1761, g), h): NGC 2004.

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thumbnail Fig. A.19

continued. i), j): NGC 3293, k), l): NGC 4755, m), n): NGC 6611.

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thumbnail Fig. A.20

FLAMES-GIRAFFE NGC 330 (SMC) equivalent width and velocity map for low velocity gas where larger symbol sizes correspond to larger equivalent widths. Sightlines with uncorrected FWHM velocities greater than 20 km s-1 have been excluded from the plot.

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thumbnail Fig. A.21

FLAMES-GIRAFFE NGC 346 (SMC) equivalent width and velocity map for low velocity gas where larger symbol sizes correspond to larger equivalent widths. Sightlines with uncorrected FWHM velocities greater than 20 km s-1 have been excluded from the plot.

Open with DEXTER

thumbnail Fig. A.22

FLAMES-GIRAFFE NGC 1761 (LMC) equivalent width and velocity map for low velocity gas where larger symbol sizes correspond to larger equivalent widths. Sightlines with uncorrected FWHM velocities greater than 20 km s-1 have been excluded from the plot.

Open with DEXTER

thumbnail Fig. A.23

FLAMES-GIRAFFE NGC 2004 (LMC) equivalent width and velocity map for low velocity gas where larger symbol sizes correspond to larger equivalent widths. Sightlines with uncorrected FWHM velocities greater than 20 km s-1 have been excluded from the plot.

Open with DEXTER

thumbnail Fig. A.24

FLAMES-GIRAFFE NGC 3293 (Milky Way) equivalent width and velocity map for low velocity gas where larger symbol sizes correspond to larger equivalent widths. Sightlines with uncorrected FWHM velocities greater than 20 km s-1 have been excluded from the plot.

Open with DEXTER

thumbnail Fig. A.25

FLAMES-GIRAFFE NGC 4755 (LMC) equivalent width and velocity map for low velocity gas where larger symbol sizes correspond to larger equivalent widths. Sightlines with uncorrected FWHM velocities greater than 20 km s-1 have been excluded from the plot.

Open with DEXTER

thumbnail Fig. A.26

FLAMES-GIRAFFE NGC 6611 (LMC) equivalent width and velocity map for low velocity gas where larger symbol sizes correspond to larger equivalent widths. Sightlines with uncorrected FWHM velocities greater than 20 km s-1 have been excluded from the plot.

Open with DEXTER

thumbnail Fig. A.27

The Magellanic Clouds. Equivalent width and velocity map for Low-Velocity gas for Ca ii K where larger symbol sizes correspond to larger equivalent widths. Sightlines with uncorrected FWHM velocities greater than 20 km s-1 have been excluded from the plot.

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thumbnail Fig. A.28

The Magellanic Clouds. Equivalent width and velocity map for Low-Velocity gas for Na i D where larger symbol sizes correspond to larger equivalent widths. Sightlines with uncorrected FWHM velocities greater than 20 km s-1 have been excluded from the plot.

Open with DEXTER

thumbnail Fig. A.29

(a) Parallax vs. column density for Al ii, Al iii, Ar i, C i and C i* with the data being taken from Gudennavar et al. (2012). All available sightlines and sighlines with |b| < 10° are shown.

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thumbnail Fig. A.30

(b) Parallax vs. column density for Cl ii, C iv, C2, Ca i and Ca ii with the data being taken from Gudennavar et al. (2012). All available sightlines and sighlines with |b| < 10° are shown.

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thumbnail Fig. A.31

(c) Parallax vs. column density for Cu ii, D i, F i, Fe ii and Fe iii with the data being taken from Gudennavar et al. (2012). All available sightlines and sighlines with |b| < 10° are shown.

Open with DEXTER

thumbnail Fig. A.32

(d) Parallax vs. column density for Ge ii, H, H i, H2 and HD with the data being taken from Gudennavar et al. (2012). All available sightlines and sighlines with |b| < 10° are shown.

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thumbnail Fig. A.33

(e) Parallax vs. column density for He i, He ii, K .i, Kr i and Mg i with the data being taken from Gudennavar et al. (2012). All available sightlines and sighlines with |b| < 10° are shown.

Open with DEXTER

thumbnail Fig. A.34

(f) Parallax vs. column density for Mg ii, Mn ii, N i, N ii and Na i with the data being taken from Gudennavar et al. (2012). All available sightlines and sighlines with |b| < 10° are shown.

Open with DEXTER

thumbnail Fig. A.35

(g) Parallax vs. column density for Ni ii, O i, O vi, P ii, and S i with the data being taken from Gudennavar et al. (2012). All available sightlines and sighlines with |b| < 10° are shown.

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thumbnail Fig. A.36

(h) Parallax vs. column density for S ii, Si ii, Si iv, Ti ii, Zn i and a combination of Ca ii, Mn ii and P ii with the data being taken from Gudennavar et al. (2012). All available sightlines and sighlines with |b| < 10° are shown.

Open with DEXTER

thumbnail Fig. A.37

(i) Parallax vs. column density for a combination of a combination of Ca ii plus Ti ii and Ca ii, Mn ii and P ii with the data being taken from Gudennavar et al. (2012). All available sightlines and sighlines with |b| < 10° are shown.

Open with DEXTER


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