shock structures and momentum transfer in herbig
... profile that varies spatially across the object, it is easy to become overwhelmed by the sheer volume of information. In this section we will consider how to interpret spectra of HH objects and explore what these data tell us about conditions in the flows. A. Structure of Radiative Shocks The high r ...
... profile that varies spatially across the object, it is easy to become overwhelmed by the sheer volume of information. In this section we will consider how to interpret spectra of HH objects and explore what these data tell us about conditions in the flows. A. Structure of Radiative Shocks The high r ...
Observation of the Crab pulsar wind nebula and microquasar Ph.D. Dissertation
... and Major Atmospheric Gamma-ray Imaging Cherenkov (MAGIC) telescopes, have been capable to increase the total number of known VHE emitting sources from a few to almost one hundred in just seven years of operation. This population comprises galactic and extragalactic objects. IACTs have proved to be ...
... and Major Atmospheric Gamma-ray Imaging Cherenkov (MAGIC) telescopes, have been capable to increase the total number of known VHE emitting sources from a few to almost one hundred in just seven years of operation. This population comprises galactic and extragalactic objects. IACTs have proved to be ...
The colour–magnitude relation of early
... redshift estimate. We used the 15 galaxies with spectroscopic redshifts in order to assess the uncertainty of the technique. The agreement between our estimates and the spectroscopic ones is generally good, with redshift errors of jDzj , 0:08. This uncertainty is propagated through to the rest-frame ...
... redshift estimate. We used the 15 galaxies with spectroscopic redshifts in order to assess the uncertainty of the technique. The agreement between our estimates and the spectroscopic ones is generally good, with redshift errors of jDzj , 0:08. This uncertainty is propagated through to the rest-frame ...
Where is the angular momentum in elliptical galaxies?
... • Globular cluster luminosity (mass) – probability of a LMXB scales roughly linearly with GC mass • Globular cluster color (metallicity) – probability of a LMXB roughly 3x larger for red (metal-rich) GCs relative to blue (metal-poor) GCs Statistically marginal correlations with globular cluster size ...
... • Globular cluster luminosity (mass) – probability of a LMXB scales roughly linearly with GC mass • Globular cluster color (metallicity) – probability of a LMXB roughly 3x larger for red (metal-rich) GCs relative to blue (metal-poor) GCs Statistically marginal correlations with globular cluster size ...
Herschel far-infrared observations of the Carina Nebula complex⋆
... complex (CNC) and reveal the population of deeply embedded young stellar objects (YSOs), most of which are not yet visible in the mid- or near-infrared. Methods. We study the properties of the 642 objects that are independently detected as point-like sources in at least two of the five Herschel band ...
... complex (CNC) and reveal the population of deeply embedded young stellar objects (YSOs), most of which are not yet visible in the mid- or near-infrared. Methods. We study the properties of the 642 objects that are independently detected as point-like sources in at least two of the five Herschel band ...
Stellar Evolution - Astrophysics
... these scaling relations relating them to L, M and R are therefore extremely important. Teff is the most important parameter which is immediately apparent from an inspection of stellar energy distributions or spectra; it determines (roughly) the wavelength at which the maximum flux density occurs and ...
... these scaling relations relating them to L, M and R are therefore extremely important. Teff is the most important parameter which is immediately apparent from an inspection of stellar energy distributions or spectra; it determines (roughly) the wavelength at which the maximum flux density occurs and ...
THE NEW GALAXY: Signatures of Its Formation
... density enhancements. The first stars formed after the collapse of the first primordial molecular clouds; these stars produced the epoch of reionization. The earliest recognizable protocloud may have begun to assemble at about this time. Within the context of CDM, the dark halo of the Galaxy assembl ...
... density enhancements. The first stars formed after the collapse of the first primordial molecular clouds; these stars produced the epoch of reionization. The earliest recognizable protocloud may have begun to assemble at about this time. Within the context of CDM, the dark halo of the Galaxy assembl ...
MOLECULAR OUTFLOWS AND A MID
... stellar objects in the filament with a combined stellar mass of 127 27 M. An additional 22 sources were identified as probable cluster members based on the presence of strong 24 m emission. The total star formation efficiency in the G34.4 cloud filament is estimated to be 7%, while the massive ...
... stellar objects in the filament with a combined stellar mass of 127 27 M. An additional 22 sources were identified as probable cluster members based on the presence of strong 24 m emission. The total star formation efficiency in the G34.4 cloud filament is estimated to be 7%, while the massive ...
First DENIS I-band extragalactic catalog
... Fig. 7. Distribution of “distances” dij between DENIS and LEDA galaxies (i and j). This graph is used to chose dlimit in the cross-identification phase (see text) ...
... Fig. 7. Distribution of “distances” dij between DENIS and LEDA galaxies (i and j). This graph is used to chose dlimit in the cross-identification phase (see text) ...
- Isaac Newton Group of Telescopes
... the presence of prominent bands of titanium oxide and, especially, vanadium oxide at 750 nm allowed to derive its spectral classification and an estimate of its effective surface temperature, which turned out to be some 2350 K. The spectrum allowed to infere a velocity measurement of this object in ...
... the presence of prominent bands of titanium oxide and, especially, vanadium oxide at 750 nm allowed to derive its spectral classification and an estimate of its effective surface temperature, which turned out to be some 2350 K. The spectrum allowed to infere a velocity measurement of this object in ...
A numerical study of recent tidal interactions between dwarf galaxies
... has an influence on the evolution of the dwarf galaxies. In all studies tidal stripping and tidal tails were observed. These interactions also led to star formation bursts in the dwarf galaxies. And there was stated by Mayer et al. (2001a) that dwarf galaxies in the Milky Way potential were transfor ...
... has an influence on the evolution of the dwarf galaxies. In all studies tidal stripping and tidal tails were observed. These interactions also led to star formation bursts in the dwarf galaxies. And there was stated by Mayer et al. (2001a) that dwarf galaxies in the Milky Way potential were transfor ...
Catalogs of Hot White Dwarfs in the Milky Way from GALEX`s
... colors are insensitive (see e.g. Bianchi (2007), Bianchi et al. (2007a), Bianchi et al. (2007b)) as well as to their very short lifetimes on the constant-luminosity post-AGB phase. To make matters more difficult, the post-AGB luminosity at a given stellar temperature varies significantly according t ...
... colors are insensitive (see e.g. Bianchi (2007), Bianchi et al. (2007a), Bianchi et al. (2007b)) as well as to their very short lifetimes on the constant-luminosity post-AGB phase. To make matters more difficult, the post-AGB luminosity at a given stellar temperature varies significantly according t ...
The Density Profiles of Massive, Relaxed Galaxy Clusters - HAL-Insu
... and clusters through the imprint of baryons on their halos. For instance, dark and baryonic density profiles can inform us about the relative importance of dissipational and dissipationless assembly processes (e.g., Lackner & Ostriker 2010). The observation from that massive ellipticals have nearly ...
... and clusters through the imprint of baryons on their halos. For instance, dark and baryonic density profiles can inform us about the relative importance of dissipational and dissipationless assembly processes (e.g., Lackner & Ostriker 2010). The observation from that massive ellipticals have nearly ...
High-mass star-forming cloud G0.38+0.04 in the Galactic center dust
... whereas in other H2 CO masers in Sgr B2, the emission is unresolved. While this might normally hint at thermal emission processes, the high brightness temperature (T B ∼ 7300 K) indicates instead that there must be multiple unresolved maser spots within the source. Zapata et al. (2009b) note that th ...
... whereas in other H2 CO masers in Sgr B2, the emission is unresolved. While this might normally hint at thermal emission processes, the high brightness temperature (T B ∼ 7300 K) indicates instead that there must be multiple unresolved maser spots within the source. Zapata et al. (2009b) note that th ...
Post Common Envelope Binaries from SDSS. I: 101 white dwarf
... and Eisenstein et al. (2006), as well as a set of WDMS independently found in the SDSS data by our team. This search resulted in a sample of 130 WDMS with two to seven SDSS spectra. Among those WDMS, 101 systems have a clearly pronounced Na I λλ 8183.27,8194.81 absorption doublet and/or Hα emission ...
... and Eisenstein et al. (2006), as well as a set of WDMS independently found in the SDSS data by our team. This search resulted in a sample of 130 WDMS with two to seven SDSS spectra. Among those WDMS, 101 systems have a clearly pronounced Na I λλ 8183.27,8194.81 absorption doublet and/or Hα emission ...
the density profiles of massive, relaxed galaxy clusters. i. the total
... et al. (2011, N11) presented very extended stellar kinematics in A383 and additionally used X-ray observations to assess the non-spherical geometry of the cluster along the line of sight (l.o.s.). In both A611 and A383 we confirmed a shallow inner density slope β < 1 for the DM. In this paper we pre ...
... et al. (2011, N11) presented very extended stellar kinematics in A383 and additionally used X-ray observations to assess the non-spherical geometry of the cluster along the line of sight (l.o.s.). In both A611 and A383 we confirmed a shallow inner density slope β < 1 for the DM. In this paper we pre ...
On the origin of lopsidedness in galaxies as determined
... inclination is clearly inappropriate. Instead, those studies must determine inclinations using a shape-independent approach, for example using the ratio of the H i line width, which is inclination-dependent, to the expected width calculated from the Tully–Fisher relation and the galaxy’s magnitude. ...
... inclination is clearly inappropriate. Instead, those studies must determine inclinations using a shape-independent approach, for example using the ratio of the H i line width, which is inclination-dependent, to the expected width calculated from the Tully–Fisher relation and the galaxy’s magnitude. ...
Master Thesis - Sterrenkunde RU Nijmegen
... average), which produces the pressure needed to counter gravity. For a derivation see Prialnik [49, appendix:B] Degenerate matter has some interesting properties. One is that the pressure does not depend on temperature. White dwarfs are born with a temperature of ∼100000K and quickly cool down to lo ...
... average), which produces the pressure needed to counter gravity. For a derivation see Prialnik [49, appendix:B] Degenerate matter has some interesting properties. One is that the pressure does not depend on temperature. White dwarfs are born with a temperature of ∼100000K and quickly cool down to lo ...
galaxy formation and evolution - Yale Astronomy
... survived as discrete units (Peebles 1974). The detailed way in which structure develops and galaxies form depends on the nature of the initial density fluctuation spectrum, so it is important to try to constrain the form of this spectrum from observations. Information about the structure of the earl ...
... survived as discrete units (Peebles 1974). The detailed way in which structure develops and galaxies form depends on the nature of the initial density fluctuation spectrum, so it is important to try to constrain the form of this spectrum from observations. Information about the structure of the earl ...
The Westerbork Hydrogen Accretion in LOcal GAlaxieS \(HALOGAS
... 2004). In both the MW and M 31, stellar streams are observed via deep optical observations (Belokurov et al. 2007; Ferguson 2007). The H i filament in the halo of NGC 891 may be the cold gas counterpart of this type of stream. It has been recently recognized that NGC 891 also has a giant stellar str ...
... 2004). In both the MW and M 31, stellar streams are observed via deep optical observations (Belokurov et al. 2007; Ferguson 2007). The H i filament in the halo of NGC 891 may be the cold gas counterpart of this type of stream. It has been recently recognized that NGC 891 also has a giant stellar str ...
Spiral arm structures revealed in the M31 galaxy
... Striking regularities are found in the northwestern arm of the M31 galaxy. Star complexes located in this arm are spaced 1.2 kpc apart and have similar sizes of about 0.6 kpc. This pattern is observed within the arm region where Beck et al. (1989) detected a strong regular magnetic field with the wa ...
... Striking regularities are found in the northwestern arm of the M31 galaxy. Star complexes located in this arm are spaced 1.2 kpc apart and have similar sizes of about 0.6 kpc. This pattern is observed within the arm region where Beck et al. (1989) detected a strong regular magnetic field with the wa ...
Spiral Density Waves in a Young Protoplanetary
... described by a smooth and axisymmetric distribution of material in the disk that extends near the stellar photosphere and decreases monotonically with distance from the star (20,23). To estimate the optical depth of the observed dust continuum emission, we performed radiative transfer calculations u ...
... described by a smooth and axisymmetric distribution of material in the disk that extends near the stellar photosphere and decreases monotonically with distance from the star (20,23). To estimate the optical depth of the observed dust continuum emission, we performed radiative transfer calculations u ...
White dwarf dynamical interactions and fast optical transients
... double white dwarf binary system where the components are brought together by gravitational wave radiation, or it could be triggered by a stellar close encounter, perhaps prompted by Kozai oscillations in a triple system (Thompson 2011; Katz & Dong 2012; Antognini et al. 2014) — see Sect. 2. In eith ...
... double white dwarf binary system where the components are brought together by gravitational wave radiation, or it could be triggered by a stellar close encounter, perhaps prompted by Kozai oscillations in a triple system (Thompson 2011; Katz & Dong 2012; Antognini et al. 2014) — see Sect. 2. In eith ...
LOOKING INTO THE HORSEHEAD Marc W. Pound Bo Reipurth and
... Horsehead got the name B33 by which it is known today. The first indication that the IC 434 and Horsehead region could be related to young stars came with the discovery of H emission line stars in the general area by Haro & Moreno (1953), followed by the detection of variable stars in the same regio ...
... Horsehead got the name B33 by which it is known today. The first indication that the IC 434 and Horsehead region could be related to young stars came with the discovery of H emission line stars in the general area by Haro & Moreno (1953), followed by the detection of variable stars in the same regio ...
Astrophysical X-ray source
Astrophysical X-ray sources are astronomical objects with physical properties which result in the emission of X-rays.There are a number of types of astrophysical objects which emit X-rays, from galaxy clusters, through black holes in active galactic nuclei (AGN) to galactic objects such as supernova remnants, stars, and binary stars containing a white dwarf (cataclysmic variable stars and super soft X-ray sources), neutron star or black hole (X-ray binaries). Some solar system bodies emit X-rays, the most notable being the Moon, although most of the X-ray brightness of the Moon arises from reflected solar X-rays. A combination of many unresolved X-ray sources is thought to produce the observed X-ray background. The X-ray continuum can arise from bremsstrahlung, either magnetic or ordinary Coulomb, black-body radiation, synchrotron radiation, inverse Compton scattering of lower-energy photons be relativistic electrons, knock-on collisions of fast protons with atomic electrons, and atomic recombination, with or without additional electron transitions.Furthermore, celestial entities in space are discussed as celestial X-ray sources. The origin of all observed astronomical X-ray sources is in, near to, or associated with a coronal cloud or gas at coronal cloud temperatures for however long or brief a period.