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 houses of the recent X?Ray Emitting fuel (pages 61–62):
Chapter 7 airborne dirt and dust houses (pages 63–69):
Chapter eight Radio homes (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 airborne dirt and dust Extinction (pages 125–142):
Chapter thirteen superstar 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 kin (pages 215–233):
Chapter 18 subject 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

Sample text

As rare sources, they are probably associated with intermediate mass black holes (IMBH of mass 102 104 Mˇ ; [58]) or extreme high-mass X-ray binaries and are generally found in active starforming, low metallicity environments off-centered with respect to the nucleus of the galaxy [59]. This evidence suggests that, contrary to nuclear massive black holes, they have a stellar origin. 4. Super Soft Sources (SSS), characterized by a black body spectrum of temperature k T 15 80 eV, probably associated with nuclear burning white dwarf binaries.

At the same time, this process is particularly important since, within stars, the primordial gas has been processed to form the heavy elements, generally called metals, now present in the universe. A Panchromatic View of Galaxies, First Edition. Alessandro Boselli. © 2012 WILEY-VCH Verlag GmbH & Co. KGaA. Published 2012 by WILEY-VCH Verlag GmbH & Co. KGaA. 1 Continuum: Stellar Emission Stars are bodies bound by self-gravity which radiate energy supplied by an internal engine [67]. They can be represented by a black body with effective temperature Teff .

Balmer absorption lines are at their maximum in stars with effective temperatures 8000 K Ä Teff Ä 12 000 K (A stars), and decrease for cooler spectral types. The presence of dominant Balmer absorbtion features in the spectra of galaxies, generally measured in terms of equivalent width, indicates recent star formation activity that rapidly ceased [90]. In general, this spectral index can be used to estimate the age of the underlying stellar population, although it should be used with some caution because of the possible degeneracy due to the contribution of the blue horizontal branch population [91].

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