Linear and circular spectropolarimetry of diffuse interstellar bands

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Volume 531 (July 2011)

A&A, 531 (2011) A25

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Issue		A&A Volume 531, July 2011


Article Number		A25
Number of page(s)		19
Section		Interstellar and circumstellar matter
DOI		https://doi.org/10.1051/0004-6361/201016365
Published online		06 June 2011

Online material

Appendix A: Polarisation (ΔP) and total intensity I spectra for weak and near-infrared DIBs

	Fig. A.1 ΔP (top) and normalised intensity (bottom) spectra of 16 weak DIBs toward HD 197770. The ΔP spectra are scaled 10 × and displaced vertically for display.
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	Fig. A.2 ΔP (top) and normalised intensity (bottom) spectra of 16 weak DIBs toward HD 194279. The ΔP spectra are scaled 10 × and displaced vertically for display.
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	Fig. A.3 ΔP (top) and normalised intensity (bottom) spectra of 13 near-infrared DIBs toward HD 197770. The ΔP spectra are scaled 10 × and displaced vertically for display.
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	Fig. A.4 ΔP (top) and normalised intensity (bottom) spectra of 13 near-infrared DIBs toward HD 194279. The ΔP spectra are scaled 10 × and displaced vertically for display.
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Appendix B: Atomic, molecular and DIB line profiles, equivalent widths and central depths

	Fig. B.1 Normalised I and P (5 × ) spectra of atomic and molecular transitions as a function of heliocentric velocity (in km s^-1) toward HD 197770. From top left to bottom right Na i D, K i, CH, CH + , Ca i, Ca ii, and CN. The dashed vertical lines indicate the interstellar radial velocity.
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	Fig. B.2 Normalised I and P (5 × ) spectra of atomic and molecular transitions as a function of heliocentric velocity (in km s^-1) toward HD 194279. From top left to bottom right Na i D, K i, CH, CH + , Ca i, Ca ii, and CN. The dashed vertical lines indicate the interstellar radial velocity.
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	Fig. B.3 C₂ (2−0) Phillips band toward both sightlines. Line strengths are given in Table B.1. For HD 194279 the strong Hydrogen Paschen line at 8750.47 Å has been removed (no C₂ lines detectable), and furthermore, the 8764.4 Å DIB is clearly present in this line-of-sight.
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Table B.1

Equivalent widths (mÅ) for interstellar atomic and diatomic lines observed for the two lines-of-sight.

Table B.2

Equivalent widths (in mÅ) for DIBs in Table 2.

Table B.3

Central depths cd (with respect to the normalized continuum) for DIBs in Table 2.

Appendix C: Stokes I, U, Q, and V spectra for the selected DIBs

	Fig. C.1 Stokes V, U, Q and I spectra (top to bottom) of 12 strong DIBs toward HD 197770. The Q,U,V spectra are scaled 5 × and displaced vertically for display.
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	Fig. C.2 Stokes V, U, Q and I spectra (top to bottom) of 12 strong DIBs toward HD 194279. The Q,U,V spectra are scaled 5 × and displaced vertically for display.
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	Fig. C.3 Stokes V, U, Q and I spectra (top to bottom) of 16 weak DIBs toward HD 197770. The Q,U,V spectra are scaled 5 × and displaced vertically for display.
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	Fig. C.4 Stokes V, U, Q and I spectra (top to bottom) of 16 weak DIBs toward HD 194279. The Q,U,V spectra are scaled 5 × and displaced vertically for display.
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	Fig. C.5 Stokes V, U, Q and I spectra (top to bottom) of 13 near-infrared DIBs toward HD 197770. The Q,U,V spectra are scaled 5 × and displaced vertically for display.
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	Fig. C.6 Stokes V, U, Q and I spectra (top to bottom) of 13 near-infrared DIBs toward HD 194279. The Q,U,V spectra are scaled 5 × and displaced vertically for display.
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© ESO, 2011

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