Probing nuclear activity versus star formation at z ∼ 0.8 using near
... The latter authors found that the period of moderately luminous AGN activity does not seem to have strong influence on the star formation activity of the galaxies, in contradiction with the results found at low redshift (e.g. Ho 2005). For example, based on FIR data from the Herschel Space Observato ...
... The latter authors found that the period of moderately luminous AGN activity does not seem to have strong influence on the star formation activity of the galaxies, in contradiction with the results found at low redshift (e.g. Ho 2005). For example, based on FIR data from the Herschel Space Observato ...
MAXI J1659−152: the shortest orbital period black
... weeks into the outbursts, again drops in intensity are seen. These dips have, however, a spectral behaviour opposite to that of the absorption dips, and are related to fast spectral state changes (hence referred to as transition dips). The absorption dips recur with a period of 2.414 ± 0.005 h, whic ...
... weeks into the outbursts, again drops in intensity are seen. These dips have, however, a spectral behaviour opposite to that of the absorption dips, and are related to fast spectral state changes (hence referred to as transition dips). The absorption dips recur with a period of 2.414 ± 0.005 h, whic ...
PS1-10jh: The Disruption of a Main-Sequence Star of Near
... Instead, we run two separate simulations that are each wellequipped to describe the behavior of the debris stream at two different epochs. To determine the fate of the debris liberated from a star during a tidal disruption, we used two similar simulation setups, differing only in the mass ratio q. T ...
... Instead, we run two separate simulations that are each wellequipped to describe the behavior of the debris stream at two different epochs. To determine the fate of the debris liberated from a star during a tidal disruption, we used two similar simulation setups, differing only in the mass ratio q. T ...
Z - STScI
... HST ToO : ACS post-explosion (F555W) Star detected in I-band only (J. Maund PhD thesis) ...
... HST ToO : ACS post-explosion (F555W) Star detected in I-band only (J. Maund PhD thesis) ...
FLARE SWG theme 3: high
... Phot-z/Spec-z of X-ray AGN, including obscured systems (cannot be ID’d from FLARE photometry); host measurements from photometry/spectroscopy ...
... Phot-z/Spec-z of X-ray AGN, including obscured systems (cannot be ID’d from FLARE photometry); host measurements from photometry/spectroscopy ...
STELLAR MASSES AND STAR FORMATION RATES OF LENSED DUSTY STAR-FORMING... FROM THE SPT SURVEY
... ∼100 high redshift, strongly gravitationally lensed DSFGs (Vieira et al. 2010; Mocanu et al. 2013). The lensing origin of the SPT DSFGs was confirmed by the Atacama Large Millimeter/submillimeter Array (ALMA) (Hezaveh et al. 2013; Vieira et al. 2013). The ALMA submillimeter imaging is used to model ...
... ∼100 high redshift, strongly gravitationally lensed DSFGs (Vieira et al. 2010; Mocanu et al. 2013). The lensing origin of the SPT DSFGs was confirmed by the Atacama Large Millimeter/submillimeter Array (ALMA) (Hezaveh et al. 2013; Vieira et al. 2013). The ALMA submillimeter imaging is used to model ...
Revising the census of low luminosity AGN
... WHY AN AGN CENSUS? • A PROPER AGN CENSUS IS NEEDED FOR A VARIETY OF STUDIES, SUCH AS, E.G. , THE AGN/HOST GALAXY CONNECTION, THE PROPERTIES OF THE CENTRAL ENGINE, THE AGN LUMINOSITY FUNCTION … • THE CENSUS SHOULD BE COMPLETE (OR AT LEAST WITH WELL DEFINED BIASES) AND INCLUDE THE LEAST NUMBER OF INT ...
... WHY AN AGN CENSUS? • A PROPER AGN CENSUS IS NEEDED FOR A VARIETY OF STUDIES, SUCH AS, E.G. , THE AGN/HOST GALAXY CONNECTION, THE PROPERTIES OF THE CENTRAL ENGINE, THE AGN LUMINOSITY FUNCTION … • THE CENSUS SHOULD BE COMPLETE (OR AT LEAST WITH WELL DEFINED BIASES) AND INCLUDE THE LEAST NUMBER OF INT ...
the inclination of the dwarf irregular galaxy
... galaxy (Meurer et al. 2013; Zheng et al. 2013), lending support to the phenomenon of self-regulation by star formation, as suggested by Quirk (1972). However, although the value of the Qg -parameter is approximately constant across a galaxy, it varies from galaxy to galaxy, indicating that the ‘ther ...
... galaxy (Meurer et al. 2013; Zheng et al. 2013), lending support to the phenomenon of self-regulation by star formation, as suggested by Quirk (1972). However, although the value of the Qg -parameter is approximately constant across a galaxy, it varies from galaxy to galaxy, indicating that the ‘ther ...
White dwarfmain sequence binaries identified within SDSS DR7 and
... [Fe/H] = −2.5–0.5 and M = 0.08–0.8 M . Fig. 1 shows the location of the combined WDMS binaries in four different colour–colour diagrams. Each track is formed by a white dwarf with fixed effective temperature and surface gravity combined with a K or M dwarf of a certain metallicity. Six effective te ...
... [Fe/H] = −2.5–0.5 and M = 0.08–0.8 M . Fig. 1 shows the location of the combined WDMS binaries in four different colour–colour diagrams. Each track is formed by a white dwarf with fixed effective temperature and surface gravity combined with a K or M dwarf of a certain metallicity. Six effective te ...
Cold Gas and Star Formation in Elliptical Galaxies
... than a few µm. Long wavelength emission is also detected towards a significant fraction of early-type galaxies by IRAS (12µm, 25µm, 60µm and 100µm), ISO (between about 5µm and 200 µm; Malhotra et al. 1998, S. Madden, this conference) and at submillimeter wavelengths. The largest sample available is ...
... than a few µm. Long wavelength emission is also detected towards a significant fraction of early-type galaxies by IRAS (12µm, 25µm, 60µm and 100µm), ISO (between about 5µm and 200 µm; Malhotra et al. 1998, S. Madden, this conference) and at submillimeter wavelengths. The largest sample available is ...
Structure of the hot object in the symbiotic prototype Z And during its
... Z And is considered a prototype of the class of symbiotic stars. The binary is composed of a late-type, M4.5 III, giant and a white dwarf accreting from the giant’s wind on a 758-day orbit (e.g. Nussbaumer & Vogel 1989; Mikolajewska & Kenyon 1996). More than 100 years of monitoring Z And (first reco ...
... Z And is considered a prototype of the class of symbiotic stars. The binary is composed of a late-type, M4.5 III, giant and a white dwarf accreting from the giant’s wind on a 758-day orbit (e.g. Nussbaumer & Vogel 1989; Mikolajewska & Kenyon 1996). More than 100 years of monitoring Z And (first reco ...
GALAXY FORMATION AND CLUSTER FORMATION Richard B
... μ is its surface density, and κ is the epicyclic frequency. In a thin disk, violent instability occurs when Q < 1; limited growth of spiral density perturbations occurs for 1 < Q < ^2 (Larson 1984); and stability occurs for Q > ^ 2 . Numerical simulations of disks containing gas (e.g. Sellwood and C ...
... μ is its surface density, and κ is the epicyclic frequency. In a thin disk, violent instability occurs when Q < 1; limited growth of spiral density perturbations occurs for 1 < Q < ^2 (Larson 1984); and stability occurs for Q > ^ 2 . Numerical simulations of disks containing gas (e.g. Sellwood and C ...
the discovery of a massive cluster of red supergiants with glimpse
... in the diffuse emission, possibly a cavity sculpted by the winds and energetic photons from young massive stars. Infrared dark clouds (IRDCs) and dark filaments appear superimposed on the bright diffuse background at many locations across this field, indicating the presence of opaque, cold clouds in ...
... in the diffuse emission, possibly a cavity sculpted by the winds and energetic photons from young massive stars. Infrared dark clouds (IRDCs) and dark filaments appear superimposed on the bright diffuse background at many locations across this field, indicating the presence of opaque, cold clouds in ...
ASTRONOMY AND ASTROPHYSICS Elemental abundances of
... km s−1 ). The achieved spectral resolution of the spectra obtained at McDonald Observatory was determined for the entire observed spectral range to be ∆λ '5.4 Å. The quasars observed with FORS 1 were recorded with two different spectral resolutions which were determinated from the FWHM of several s ...
... km s−1 ). The achieved spectral resolution of the spectra obtained at McDonald Observatory was determined for the entire observed spectral range to be ∆λ '5.4 Å. The quasars observed with FORS 1 were recorded with two different spectral resolutions which were determinated from the FWHM of several s ...
Construction and Operation of an Axion Helioscope
... ·2. The Sun as an axion source a) The arion spectrum If we confine our attention to hadronic axion models where these particles do not interact with electrons at tree level, they can be efficiently produced in the Sun only by processes involving their two photon coupling Eq. (4). In the interior of ...
... ·2. The Sun as an axion source a) The arion spectrum If we confine our attention to hadronic axion models where these particles do not interact with electrons at tree level, they can be efficiently produced in the Sun only by processes involving their two photon coupling Eq. (4). In the interior of ...
The environment of high-redshift AGN OLIMPIA JUDIT FOGASY
... amount of X-ray gas in their halo, while disky ellipticals tend to be smaller in size and lack the hot X-ray gas component. Spiral galaxies have more structure, they contain a thin rotating disk, a central, dense region of stars called bulge and in some cases bars. Bulges can be divided into two gro ...
... amount of X-ray gas in their halo, while disky ellipticals tend to be smaller in size and lack the hot X-ray gas component. Spiral galaxies have more structure, they contain a thin rotating disk, a central, dense region of stars called bulge and in some cases bars. Bulges can be divided into two gro ...
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... high-energy cutoff and an additional black body at lower energies. The photon index of the power law and the black-body flux only depend on the 15–50 keV source flux. No apparent hysteresis effects are seen. These correlations allow us to predict the evolution of the pulsar’s X-ray spectral shape ov ...
... high-energy cutoff and an additional black body at lower energies. The photon index of the power law and the black-body flux only depend on the 15–50 keV source flux. No apparent hysteresis effects are seen. These correlations allow us to predict the evolution of the pulsar’s X-ray spectral shape ov ...
Three Binary Millisecond Pulsars in NGC 6266
... (minimum masses of 0.12 and 0.07 M, respectively). The pulsar in the closest system is the fifth member of an emerging class of millisecond pulsars displaying irregular radio eclipses and having a relatively massive companion. This system is a good candidate for optical identification of the companio ...
... (minimum masses of 0.12 and 0.07 M, respectively). The pulsar in the closest system is the fifth member of an emerging class of millisecond pulsars displaying irregular radio eclipses and having a relatively massive companion. This system is a good candidate for optical identification of the companio ...
PRESENT-DAY CLUSTER FORMATION
... Information about the youngest systems of stars has been obtained from classical optical studies of nearby OB and T associations (Blaauw 1964, 1991; Herbig 1962; Cohen & Kuhi 1979; Herbig & Terndrup 1986), and more recently from infrared observations of newly formed stars and clusters that are still ...
... Information about the youngest systems of stars has been obtained from classical optical studies of nearby OB and T associations (Blaauw 1964, 1991; Herbig 1962; Cohen & Kuhi 1979; Herbig & Terndrup 1986), and more recently from infrared observations of newly formed stars and clusters that are still ...
Hot Gas In and Around Elliptical Galaxies William G. Mathews
... Recent Chandra and XMM X-ray observations of the hot gas in elliptical galaxies and galaxy clusters have radically upset the traditional concept of cooling flows. On the other hand, these same observations may reveal new ways of understanding the origin and evolution of this gas. The most unexpected ...
... Recent Chandra and XMM X-ray observations of the hot gas in elliptical galaxies and galaxy clusters have radically upset the traditional concept of cooling flows. On the other hand, these same observations may reveal new ways of understanding the origin and evolution of this gas. The most unexpected ...
The Dwarf Starburst Host Galaxy of a Type Ia SN at z= 1.55 from
... discovery of the accelerating expansion of the universe, based on just a few dozen objects (Perlmutter et al. 1999; Riess et al. 1998). Nearly 15 years later, modern SNIa samples can now include over 500 well-studied SNe with a dispersion in peak magnitudes of ∼0.16 magnitudes (e.g., Conley et al. 2 ...
... discovery of the accelerating expansion of the universe, based on just a few dozen objects (Perlmutter et al. 1999; Riess et al. 1998). Nearly 15 years later, modern SNIa samples can now include over 500 well-studied SNe with a dispersion in peak magnitudes of ∼0.16 magnitudes (e.g., Conley et al. 2 ...
INFRARED DUST BUBBLES: PROBING THE DETAILED
... Each of the four Spitzer Infrared Array Camera (IRAC ) bandpasses are dominated by different emission processes in the neighborhood of a hot star (see Draine 2003 and Peeters et al. 2003). The brightest objects in the 3.6 m band are stars, but this band also has contributions from a weak, diffuse P ...
... Each of the four Spitzer Infrared Array Camera (IRAC ) bandpasses are dominated by different emission processes in the neighborhood of a hot star (see Draine 2003 and Peeters et al. 2003). The brightest objects in the 3.6 m band are stars, but this band also has contributions from a weak, diffuse P ...
Document
... clusters: gas stripping, star stripping, galaxy-galaxy encounters, interaction with the general tidal field. There’s a correlation between outer rotation-velocity gradients and distance from the cluster centre: inner-cluster galaxies show shallower rotation curves than do outer- cluster galaxies. (R ...
... clusters: gas stripping, star stripping, galaxy-galaxy encounters, interaction with the general tidal field. There’s a correlation between outer rotation-velocity gradients and distance from the cluster centre: inner-cluster galaxies show shallower rotation curves than do outer- cluster galaxies. (R ...
A dozen new galaxies caught in the act: Gas stripping and extended
... One critical clue for understanding the gas removal is detection of the stripped gas. Recent deep Hα imaging observations revealed that some of the galaxies in clusters are accompanied by Hα clouds. In the nearby cluster Abell 1367, Gavazzi et al. (2001) found extended ionized gas regions associated ...
... One critical clue for understanding the gas removal is detection of the stripped gas. Recent deep Hα imaging observations revealed that some of the galaxies in clusters are accompanied by Hα clouds. In the nearby cluster Abell 1367, Gavazzi et al. (2001) found extended ionized gas regions associated ...
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.