Planck intermediate results - XXVIII. Interstellar gas and dust in the Chamaeleon clouds as seen by Fermi LAT and Planck

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Volume 582 (October 2015)

A&A, 582 (2015) A31

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Table E.1

Best-fit coefficients of the γ-ray models (q for each energy band) and of the dust models (y) for the γ + A_VQ (top), γ + τ₃₅₃ (middle), and γ + R (bottom) analyses.

Energy band	q_{HI Cha}	q_{HI IVA}	q_{HI Gal}	q_CO^a	q_DNM^b1	q_IC	q_iso

10^2.6–10^2.8 MeV ..............
10^2.8–10^3.2 MeV..............
10^3.2–10^3.6 MeV..............
10^3.6–10^5.0 MeV..............
10^2.6–10^5.0 MeV..............

	y _{HI Cha} ^c1	y _{HI IVA} ^c1	y _{HI Gal} ^c1	y _CO ^d1	y _DNM ^c1		y _iso ^e1



Energy band	q_{HI Cha}	q_{HI IVA}	q_{HI Gal}	q_CO^a	q_DNM^b2	q_IC	q_iso

10^2.6–10^2.8 MeV..............
10^2.8–10^3.2 MeV..............
10^3.2–10^3.6 MeV..............
10^3.6–10^5.0 MeV..............
10^2.6–10^5.0 MeV..............

	y _{HI Cha} ^c2	y _{HI IVA} ^c2	y _{HI Gal} ^c2	y _CO ^d2	y _DNM ^c2		y _iso ^e2



Energy band	q _{HI Cha}	q _{HI IVA}	q _{HI Gal}	q _CO ^a	q _DNM ^b3	q _IC	q _iso

10^2.6–10^2.8 MeV..............
10^2.8–10^3.2 MeV..............
10^3.2–10^3.6 MeV..............
10^3.6–10^5.0 MeV..............
10^2.6–10^5.0 MeV..............

	y _{HI Cha} ^c3	y _{HI IVA} ^c3	y _{HI Gal} ^c3	y _CO ^d3	y _DNM ^c3		y _iso ^e3

Notes. The first uncertainties are statistical, the second result from changes in H i spin temperature over the 2σ confidence interval from the optically thin case. The latter do not include the 8% systematic uncertainty in the LAT sensitive area for the q parameters. Model uncertainties have been used to optimize the dust fits.

^(a)

In 10²⁰ cm^-2 K^-1 km^-1 s,

^(b1)

In 10²⁰ cm^-2 mag^-1,

^(b2)

In 10²⁵ cm^-2,

^(b3)

In 10³¹ sr W^-1,

^(c1)

In 10^-22 mag cm²,

^(c2)

In 10^-26 cm²,

^(c3)

In 10^-32 W sr^-1,

^(d1)

In 10^-2 mag K^-1 km^-1 s,

^(d2)

In 10^-6 K^-1 km^-1 s,

^(d3)

In 10^-8 W m^-2 sr^-1 K^-1 km^-1,

^(e1)

In 10^-2 mag,

^(e2)

In 10^-6,

^(e3)

In 10^-8 W m^-2 sr^-1.

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