Astronomy Astrophysics - Max Planck Institut für Radioastronomie
... five Herbig Ae/Be stars (HD 163296, HD 104237, HD 98922, MWC 297, V921 Sco) in the Brγ emission line as well as in the adjacent continuum. From the measured wavelength-dependent visibilities, we derive the characteristic size of the continuum and Brγ lineemitting region. Additional information is pr ...
... five Herbig Ae/Be stars (HD 163296, HD 104237, HD 98922, MWC 297, V921 Sco) in the Brγ emission line as well as in the adjacent continuum. From the measured wavelength-dependent visibilities, we derive the characteristic size of the continuum and Brγ lineemitting region. Additional information is pr ...
Pulsars - Arecibo Observatory
... Millisecond Pulsars with white dwarf companions are formed in Low-Mass X-ray Binaries (LMXBs), where mass is being transferred from a low-mass star into a neutron star. This accretion process lasts hundreds of millions of years, and produces very fast rotation. Double neutron stars result from Hig ...
... Millisecond Pulsars with white dwarf companions are formed in Low-Mass X-ray Binaries (LMXBs), where mass is being transferred from a low-mass star into a neutron star. This accretion process lasts hundreds of millions of years, and produces very fast rotation. Double neutron stars result from Hig ...
The Properties of Super Star Clusters in A Sample of
... of small OB-associations to super star clusters) serendipitously detected in nearby galaxies. This sample of objects begins to fill in the continuum of cluster masses between individual UCH II regions and the embedded massive clusters. ...
... of small OB-associations to super star clusters) serendipitously detected in nearby galaxies. This sample of objects begins to fill in the continuum of cluster masses between individual UCH II regions and the embedded massive clusters. ...
The UV properties of E+ A galaxies: constraints on feedback
... near-ultraviolet (N U V ), centred at ∼ 2310Å. This crossmatching produced 38 E+A galaxies which have at least a detection in the N U V filter, 28 of which have photometry in both the F U V and N U V filters. Figure 1 shows the position of our E+A galaxies (filled blue circles) in the (N U V − r) v ...
... near-ultraviolet (N U V ), centred at ∼ 2310Å. This crossmatching produced 38 E+A galaxies which have at least a detection in the N U V filter, 28 of which have photometry in both the F U V and N U V filters. Figure 1 shows the position of our E+A galaxies (filled blue circles) in the (N U V − r) v ...
Stellar Population Effects on the Inferred Photon Density at
... only approximately 25 per cent of binary systems survive the first supernova. The models in use here comprise version 2.0 of the bpass model dataset. We employ stellar evolution and atmosphere models with a metallicity mass fraction ranging from Z = 0.001 to 0.040. These metallicities correspond to o ...
... only approximately 25 per cent of binary systems survive the first supernova. The models in use here comprise version 2.0 of the bpass model dataset. We employ stellar evolution and atmosphere models with a metallicity mass fraction ranging from Z = 0.001 to 0.040. These metallicities correspond to o ...
O stars with weak winds: the Galactic case - Max-Planck
... not affected by winds, plane-parallel models can be used for a preliminary analysis. Hence, we have taken advantage of the recent grid of TLUSTY spectra (OSTAR2002, Lanz & Hubeny 2002). This grid covers the log g - Teff plane for O stars and includes optical synthetic spectra computed with a turbule ...
... not affected by winds, plane-parallel models can be used for a preliminary analysis. Hence, we have taken advantage of the recent grid of TLUSTY spectra (OSTAR2002, Lanz & Hubeny 2002). This grid covers the log g - Teff plane for O stars and includes optical synthetic spectra computed with a turbule ...
the redshift evolution of the mean temperature
... that nongravitational processes (e.g., cooling, AGN feedback) are important in the central region of the cluster while gravity is the dominant force in the outer region. While the aforementioned studies have made significant progress in quantifying the average temperature, entropy, and pressure prof ...
... that nongravitational processes (e.g., cooling, AGN feedback) are important in the central region of the cluster while gravity is the dominant force in the outer region. While the aforementioned studies have made significant progress in quantifying the average temperature, entropy, and pressure prof ...
Chapter 7 in the LSST Science Book
... This is one of the most pressing problems of galaxy formation today, and any formulation of galaxy formation must account for this tension. Indeed there are a number of competing suggestions aimed at explaining how thin disks may survive and/or emerge from the expected bombardment. To first order, t ...
... This is one of the most pressing problems of galaxy formation today, and any formulation of galaxy formation must account for this tension. Indeed there are a number of competing suggestions aimed at explaining how thin disks may survive and/or emerge from the expected bombardment. To first order, t ...
Article PDF - IOPscience
... of molecular gas in late types, it will only make yet more gas-rich galaxies, which are already inferred to be very gas rich. Hence, our qualitative results are very robust, even if the quantitative details are subject to improvement in the CO data. Moreover, it is only the ratio ! /g that matters t ...
... of molecular gas in late types, it will only make yet more gas-rich galaxies, which are already inferred to be very gas rich. Hence, our qualitative results are very robust, even if the quantitative details are subject to improvement in the CO data. Moreover, it is only the ratio ! /g that matters t ...
Multiwavelength Observations of Massive Stellar Cluster Candidates
... cooperative agreement by Associated Universities, Inc. ...
... cooperative agreement by Associated Universities, Inc. ...
The Formation of Massive Stars - Max-Planck
... counterpart in the GLIMPSE data. While this could also indicate a genuine HMSC, they found relatively high temperatures [~33 K from NH3(1,1) and (2,2)], an increasing N2H+(1–0) line width from the core edge to the core center, and so-called “green fuzzy” mid-infrared emission at the edge of the core ...
... counterpart in the GLIMPSE data. While this could also indicate a genuine HMSC, they found relatively high temperatures [~33 K from NH3(1,1) and (2,2)], an increasing N2H+(1–0) line width from the core edge to the core center, and so-called “green fuzzy” mid-infrared emission at the edge of the core ...
THE ORIGIN AND EVOLUTION OF PLANETARY NEBULAE
... At the beginning of the 20th Century, when stars were believed to evolve from high temperatures to low temperatures, PN were thought to be very young stars because of their high temperatures. From his studies of the velocity distribution of PN, Curtis (1918) found that PN are more similar to late-ty ...
... At the beginning of the 20th Century, when stars were believed to evolve from high temperatures to low temperatures, PN were thought to be very young stars because of their high temperatures. From his studies of the velocity distribution of PN, Curtis (1918) found that PN are more similar to late-ty ...
CO emissions from optically selected galaxies at z ∼0.1–0.2: Tight
... the strength of the 4000 Å break, instead of the commonly used far-infrared (FIR) flux. We successfully detected the CO emissions from eight galaxies with signal-to-noise ratio larger than three, demonstrating the effectiveness of the Dn(4000)-based sample selection. For the first time, we find a t ...
... the strength of the 4000 Å break, instead of the commonly used far-infrared (FIR) flux. We successfully detected the CO emissions from eight galaxies with signal-to-noise ratio larger than three, demonstrating the effectiveness of the Dn(4000)-based sample selection. For the first time, we find a t ...
The Space Density of Spiral Galaxies as f(magnitude, size and
... observed trends between stellar ages & metallicities and galaxy surface brightness parameters ...
... observed trends between stellar ages & metallicities and galaxy surface brightness parameters ...
H EMISSION FROM HIGH-VELOCITY CLOUDS AND
... having upper limits on the order of 30–70 mR. The H measurements are discussed in relation to their H i properties, and distance constraints are given to each of the complexes based on f^esc 6% of the ionizing photons escaping normal to the Galactic disk ( fesc 1% 2% when averaged over solid an ...
... having upper limits on the order of 30–70 mR. The H measurements are discussed in relation to their H i properties, and distance constraints are given to each of the complexes based on f^esc 6% of the ionizing photons escaping normal to the Galactic disk ( fesc 1% 2% when averaged over solid an ...
MUSE three-dimensional spectroscopy and kinematics of the
... indicate (e.g. O’Dea, Baum & Stanghellini 1991) that they have become confined (trapped) within the host galaxy nucleus by a very dense (clumpy and dusty) interstellar medium, or simply that they are observed very soon after the radio outburst is triggered (e.g. Morganti et al. 1997). It is now cons ...
... indicate (e.g. O’Dea, Baum & Stanghellini 1991) that they have become confined (trapped) within the host galaxy nucleus by a very dense (clumpy and dusty) interstellar medium, or simply that they are observed very soon after the radio outburst is triggered (e.g. Morganti et al. 1997). It is now cons ...
REVIEW Numerical Star-Formation Studies— A Status Report
... In the past, progress has only been achievable by dividing the problem into smaller bits and pieces and by focusing on few feedback loops. Stars of all ages radiate and will thus heat up physical processes or single scales only. Today, however, algothe gas in their vicinity. By doing so they influenc ...
... In the past, progress has only been achievable by dividing the problem into smaller bits and pieces and by focusing on few feedback loops. Stars of all ages radiate and will thus heat up physical processes or single scales only. Today, however, algothe gas in their vicinity. By doing so they influenc ...
exploring the universe with the low frequency array a scientific case
... Until now, one of the most important limitations in achieving such long baselines at low radio frequencies has been the complicated structure of the ionosphere and its variation over time. Just as the atmosphere causes stars to twinkle, the irregularities in the ionosphere produce jittering in the r ...
... Until now, one of the most important limitations in achieving such long baselines at low radio frequencies has been the complicated structure of the ionosphere and its variation over time. Just as the atmosphere causes stars to twinkle, the irregularities in the ionosphere produce jittering in the r ...
Cold dark matter heats up
... even so, such simulations were expensive, taking 70 hours on state-ofthe-art 3-MHz facilities. Such calculations would now take a few minutes on a mobile telephone. The growth of computing power and parallel capabilities meant that, by the 1990s, simulations became sufficiently powerful to make deta ...
... even so, such simulations were expensive, taking 70 hours on state-ofthe-art 3-MHz facilities. Such calculations would now take a few minutes on a mobile telephone. The growth of computing power and parallel capabilities meant that, by the 1990s, simulations became sufficiently powerful to make deta ...
Accreting millisecond X-ray pulsars, from accretion disk to magnetic
... 1.2 Observation of neutron stars observations, since it is here that the neutron star spectrum forms and the gravitational potential energy is mainly released in accreting systems. I will discuss the properties of this layer in § 1.2. The outer crust has a thickness of a few hundred meters, and is ...
... 1.2 Observation of neutron stars observations, since it is here that the neutron star spectrum forms and the gravitational potential energy is mainly released in accreting systems. I will discuss the properties of this layer in § 1.2. The outer crust has a thickness of a few hundred meters, and is ...
Discovery of a Dwarf Poststarburst Galaxy near a High Column
... length (z 1 compared with z 3:5 at z 0:3 for the Key Project spectroscopy). The ground-based galaxy survey work of Lanzetta et al. (1995) based on the FOS Key Project absorber sample finds that 30% of these high column density absorbers can be identified with bright galaxies at impact para ...
... length (z 1 compared with z 3:5 at z 0:3 for the Key Project spectroscopy). The ground-based galaxy survey work of Lanzetta et al. (1995) based on the FOS Key Project absorber sample finds that 30% of these high column density absorbers can be identified with bright galaxies at impact para ...
Where stars are born: Javier Blasco-Herrera
... The evolution of galaxies in the past has been dominated by interactions, mergers, episodes of strong star formation followed by long quiescent periods... Currently, we are in the process of changing from that epoch of fast evolution into an epoch where internal, slow processes dominate (Kormendy & ...
... The evolution of galaxies in the past has been dominated by interactions, mergers, episodes of strong star formation followed by long quiescent periods... Currently, we are in the process of changing from that epoch of fast evolution into an epoch where internal, slow processes dominate (Kormendy & ...
Some Constraints on the Effects of Age and Metallicity - UvA-DARE
... 3115 in the 0.5–8 keV band. The bulk of these sources are LMXBs. Only 10–15 of the candidates in each galaxy are expected to be contaminating objects such as background active galactic nuclei (Brandt et al. 2000; Mushotzky et al. 2000). Neither of these galaxies show evidence of significant emission ...
... 3115 in the 0.5–8 keV band. The bulk of these sources are LMXBs. Only 10–15 of the candidates in each galaxy are expected to be contaminating objects such as background active galactic nuclei (Brandt et al. 2000; Mushotzky et al. 2000). Neither of these galaxies show evidence of significant emission ...
A photometrically and spectroscopically confirmed
... photometry here, as a large number of our galaxies do not have significant detections in this band. Galaxy NGC 0015 NGC 0109 PGC 001683 IC 0022 NGC 0345 ...
... photometry here, as a large number of our galaxies do not have significant detections in this band. Galaxy NGC 0015 NGC 0109 PGC 001683 IC 0022 NGC 0345 ...
Infrared identification of high-mass X
... the compact object and could be explained by an eccentric binary orbit (Tomsick et al. 2008). Swift observations analyzed by Rodriguez et al. (2009) finally confirmed the previously suggested association for this object, that it is very likely an HMXB and also the possible substantial variation of t ...
... the compact object and could be explained by an eccentric binary orbit (Tomsick et al. 2008). Swift observations analyzed by Rodriguez et al. (2009) finally confirmed the previously suggested association for this object, that it is very likely an HMXB and also the possible substantial variation of t ...
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.