A Panchromatic View of Galaxies by Alessandro Boselli

By Alessandro Boselli

Content material:
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 gasoline (pages 61–62):
Chapter 7 dirt homes (pages 63–69):
Chapter eight Radio houses (pages 71–75):
Chapter nine The Spectral strength Distribution (pages 77–90):
Chapter 10 Spectral good points (pages 91–106):
Chapter eleven gasoline homes (pages 107–123):
Chapter 12 dirt Extinction (pages 125–142):
Chapter thirteen megastar Formation Tracers (pages 143–159):
Chapter 14 gentle Profiles and Structural Parameters (pages 161–170):
Chapter 15 Stellar and Dynamical plenty (pages 171–191):
Chapter sixteen Statistical instruments (pages 195–213):
Chapter 17 Scaling family (pages 215–233):
Chapter 18 subject Cycle in Galaxies (pages 235–243):
Chapter 19 The position of our environment on Galaxy Evolution (pages 245–254):

Show description

By Alessandro Boselli

Content material:
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 gasoline (pages 61–62):
Chapter 7 dirt homes (pages 63–69):
Chapter eight Radio houses (pages 71–75):
Chapter nine The Spectral strength Distribution (pages 77–90):
Chapter 10 Spectral good points (pages 91–106):
Chapter eleven gasoline homes (pages 107–123):
Chapter 12 dirt Extinction (pages 125–142):
Chapter thirteen megastar Formation Tracers (pages 143–159):
Chapter 14 gentle Profiles and Structural Parameters (pages 161–170):
Chapter 15 Stellar and Dynamical plenty (pages 171–191):
Chapter sixteen Statistical instruments (pages 195–213):
Chapter 17 Scaling family (pages 215–233):
Chapter 18 subject Cycle in Galaxies (pages 235–243):
Chapter 19 The position of our environment on Galaxy Evolution (pages 245–254):

Show description

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Extra info for A Panchromatic View of Galaxies

Sample text

This effect significantly increases the mean free path of Ly α photons within galaxies, thus enormously increasing the chances of dust absorption with respect to continuum photons in dust-rich systems [116, 117]. 1). As a consequence, the Ly α luminosity is not a good tracer of star formation (see Chapter 13). 49 51 5 Millimeter and Centimeter Radio The millimeter and centimeter radio domain is of fundamental importance in the study of galaxies. Here the continuum emission is due to a thermal component originating from HII regions (free–free) and to a nonthermal component due to relativistic electrons spinning around weak magnetic fields (synchrotron), with a contribution to the thermal emission by the coldest dust at short wavelengths.

Alessandro Boselli. © 2012 WILEY-VCH Verlag GmbH & Co. KGaA. Published 2012 by WILEY-VCH Verlag GmbH & Co. KGaA. 1 The submillimeter–radio continuum spectral energy distribution of the starburst galaxy M82, adapted from [119]. The submillimeter domain is dominated by the Rayleigh–Jeans tail of the modified black body emission due to the cold dust (dotted line), the radio continuum at λ 1 cm is due to synchrotron emission (long dashed line), while free–free dominates the 1 mm 1 cm spectral range (dotted dashed line).

As a consequence, the Ly α luminosity is not a good tracer of star formation (see Chapter 13). 49 51 5 Millimeter and Centimeter Radio The millimeter and centimeter radio domain is of fundamental importance in the study of galaxies. Here the continuum emission is due to a thermal component originating from HII regions (free–free) and to a nonthermal component due to relativistic electrons spinning around weak magnetic fields (synchrotron), with a contribution to the thermal emission by the coldest dust at short wavelengths.

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