The large- and small-scale Ca II K structure of the Milky Way from observations of Galactic and Magellanic sightlines

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Volume 582 (October 2015)

A&A, 582 (2015) A59

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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

	Fig. A.1 Example Ca ii H and K spectra towards the seven clusters observed with FLAMES-GIRAFFE.
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	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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	Fig. A.2 continued. NGC 330 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.2 continued. NGC 330 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.2 continued. NGC 330 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.2 continued. NGC 330 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.2 continued. NGC 330 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.2 continued. NGC 330 Ca ii FLAMES-GIRAFFE spectra.
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	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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	Fig. A.3 continued. NGC 346 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.3 continued. NGC 346 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.3 continued. NGC 346 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.3 continued. NGC 346 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.3 continued. NGC 346 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.3 continued. NGC 346 Ca ii FLAMES-GIRAFFE spectra.
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	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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	Fig. A.4 continued. NGC 1761 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.4 continued. NGC 1761 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.4 continued. NGC 1761 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.4 continued. NGC 1761 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.4 continued. NGC 1761 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.4 continued. NGC 1761 Ca ii FLAMES-GIRAFFE spectra.
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	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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	Fig. A.5 continued. NGC 2004 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.5 continued. NGC 2004 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.5 continued. NGC 2004 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.5 continued. NGC 2004 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.5 continued. NGC 2004 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.5 continued. NGC 2004 Ca ii FLAMES-GIRAFFE spectra.
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	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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	Fig. A.6 continued. NGC 3293 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.6 continued. NGC 3293 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.6 continued. NGC 3293 Ca ii FLAMES spectra.
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	Fig. A.6 continued. NGC 3293 Ca ii FLAMES spectra.
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	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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	Fig. A.7 continued. NGC 4755 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.7 continued. NGC 4755 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.7 continued. NGC 4755 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.7 continued. NGC 4755 Ca ii FLAMES-GIRAFFE spectra.
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	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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	Fig. A.8 continued. NGC 6611 Ca ii FLAMES-GIRAFFE spectra.
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	Fig. A.8 continued. NGC 6611 Ca ii FLAMES-GIRAFFE spectra.
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	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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	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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	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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	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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	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.
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	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.
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	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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	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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	Fig. A.16 continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.
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	Fig. A.16 continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.
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	Fig. A.16 continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.
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	Fig. A.16 continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.
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	Fig. A.16 continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.
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	Fig. A.16 continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.
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	Fig. A.16 continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.
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	Fig. A.16 continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.
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	Fig. A.16 continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.
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	Fig. A.16 continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.
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	Fig. A.16 continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.
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	Fig. A.16 continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.
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	Fig. A.16 continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.
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	Fig. A.16 continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.
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	Fig. A.16 continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.
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	Fig. A.16 continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.
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	Fig. A.16 continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.
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	Fig. A.16 continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.
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	Fig. A.16 continued. FEROS or UVES Ca ii K, Na i D and GASS or LABS H i spectra.
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	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.
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	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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	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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	Fig. A.19 continued. i), j): NGC 3293, k), l): NGC 4755, m), n): NGC 6611.
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	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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	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.
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	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.
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	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.
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	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.
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	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.
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	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.
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	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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	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.
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	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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	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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	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.
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	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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	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.
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	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.
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	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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	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.
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	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.
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