By Alessandro Boselli
Chapter 1 advent (pages 1–13):
Chapter 2 X?Ray (pages 17–23):
Chapter three UV?Optical?NIR (pages 25–40):
Chapter four The Infrared (pages 41–49):
Chapter five Millimeter and Centimeter Radio (pages 51–57):
Chapter 6 homes of the new X?Ray Emitting fuel (pages 61–62):
Chapter 7 dirt homes (pages 63–69):
Chapter eight Radio homes (pages 71–75):
Chapter nine The Spectral strength Distribution (pages 77–90):
Chapter 10 Spectral positive aspects (pages 91–106):
Chapter eleven gasoline homes (pages 107–123):
Chapter 12 airborne dirt and dust Extinction (pages 125–142):
Chapter thirteen famous person Formation Tracers (pages 143–159):
Chapter 14 mild Profiles and Structural Parameters (pages 161–170):
Chapter 15 Stellar and Dynamical lots (pages 171–191):
Chapter sixteen Statistical instruments (pages 195–213):
Chapter 17 Scaling kinfolk (pages 215–233):
Chapter 18 topic Cycle in Galaxies (pages 235–243):
Chapter 19 The position of our surroundings on Galaxy Evolution (pages 245–254):
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Extra resources for A Panchromatic View of Galaxies
In G stars such as the Sun, the most important absorption features are the magnesium triplet MgI at 5167, 5173 and 5184 Å (generally indicated with Mgb), the two sodium NaI lines at 5890 and 5896 Å, the calcium doublet CaII (H and K) at 3969 and 3934 Å and the calcium triplet at 8498, 8542 and 8662 Å. A prominent feature, the so called G band, is present at 4300 Å. This feature results from a combined effect due to a series of lines caused by the absorption of CH molecules and of iron. Other absorption features such as TiO can be detected when late-type stars are present.
PAHs have been found in almost all of the ISM environments where they can be excited by UV or optical photons, in particular in the photodissociation regions between HII regions and giant molecular clouds, while they are rare in those regions with a very intense UV radiation ﬁeld which is able to destroy them. Indeed they are the dominant emission features in the mid-IR spectrum of massive spirals, contributing to . 10% of their total 4 1000 μm far-IR luminosity, while they become less important in low-metallicity systems where a combined effect of the intense UV radiation ﬁeld and the low dust content favor their dissociation [44, 107].
7) where τ l is the optical thickness at 1 GHz and ν g is the frequency in GHz. 27 in NGC 253. , 250, 350, 500 μm 53 54 5 Millimeter and Centimeter Radio for SPIRE on Herschel). 8) Here, the Rayleigh–Jeans spectrum is modiﬁed by the grain emissivity with the same ν β factor given in Eq. 7). 2. 2 Emission Lines The radio domain includes several of the most important lines necessary for the study of galaxy evolution. 6 mm is used to determine the molecular hydrogen content. 25 , the higher level CO transition lines such as 12 CO(3 2) fall into the millimeter bands for high-redshift objects, and the 12 CO(1 0) line becomes observable at high frequencies with centimeter radio telescopes such as the VLA.