arXiv:1601.01542v1 [astro-ph.GA] 7 Jan 2016
... Roy & Walsh 1997, among others). These features have been theoretically suggested to be motivated, for instance, by the presence of radial migration (Minchev et al. 2011, 2012). Nevertheless, their origin is still unknown. All these spectroscopic studies were limited by statistics, either in the num ...
... Roy & Walsh 1997, among others). These features have been theoretically suggested to be motivated, for instance, by the presence of radial migration (Minchev et al. 2011, 2012). Nevertheless, their origin is still unknown. All these spectroscopic studies were limited by statistics, either in the num ...
Physics of Neutron Star Crusts
... opportunities. The elementary constituents of the matter are neutrons, protons, and electrons – like in the atomic matter around us. The density is “subnuclear”, so that the methods developed and successfully applied in the last decades to terrestrial nuclear physics can be applied to neutron star c ...
... opportunities. The elementary constituents of the matter are neutrons, protons, and electrons – like in the atomic matter around us. The density is “subnuclear”, so that the methods developed and successfully applied in the last decades to terrestrial nuclear physics can be applied to neutron star c ...
The impact of protocluster environments at z = 1.6
... approximately twice the size of the protocluster field. The low photometric redshift uncertainties mean that these three redshift bins are well-separated. The Cl 0218.3−0510 protocluster consists of six galaxy groups surrounded by a dense sea of intergroup galaxies (see Fig. 1). In Hatch et al. (201 ...
... approximately twice the size of the protocluster field. The low photometric redshift uncertainties mean that these three redshift bins are well-separated. The Cl 0218.3−0510 protocluster consists of six galaxy groups surrounded by a dense sea of intergroup galaxies (see Fig. 1). In Hatch et al. (201 ...
Dust in historical Galactic Type Ia supernova remnants with Herschel
... with the Balloon-borne Large Aperture Submillimetre Telescope (BLAST) and the Herschel Space Observatory showed it was difficult to distinguish between cold dust in the remnant and cold dust from intervening interstellar clouds using photometry alone (Barlow et al. 2010; Sibthorpe et al. 2010). Thes ...
... with the Balloon-borne Large Aperture Submillimetre Telescope (BLAST) and the Herschel Space Observatory showed it was difficult to distinguish between cold dust in the remnant and cold dust from intervening interstellar clouds using photometry alone (Barlow et al. 2010; Sibthorpe et al. 2010). Thes ...
A Collimated Jet and an Infalling-Rotating Disk in G192.16−3.84
... H2 O maser spatio–kinematical parameters, we discuss the formation mechanism of the massive young stellar objects and the outflow development in G192.16−3.84. Key words: ISM: jets and outflows — masers — stars: formation — stars: individual (G192.16−3.84) — stars: mass accretion 1. Introduction The ...
... H2 O maser spatio–kinematical parameters, we discuss the formation mechanism of the massive young stellar objects and the outflow development in G192.16−3.84. Key words: ISM: jets and outflows — masers — stars: formation — stars: individual (G192.16−3.84) — stars: mass accretion 1. Introduction The ...
The effects of galaxy interactions on star formation
... using data from the Hubble Space Telescope along with ancillary data from the Spitzer Space Telescope and Galaxy Evolution Explorer to obtain broader wavelength coverage. Combined with starburst99 evolutionary synthesis models, we estimate the ages and masses of the clusters. The mass and luminosity ...
... using data from the Hubble Space Telescope along with ancillary data from the Spitzer Space Telescope and Galaxy Evolution Explorer to obtain broader wavelength coverage. Combined with starburst99 evolutionary synthesis models, we estimate the ages and masses of the clusters. The mass and luminosity ...
The PAH emission spectra of Large Magellanic Cloud H II regions
... spectra, the spline points for this continuum were located at ∼5.8 µm, in the 9–10 µm region, and at the blue base of the [S iv] 10.5 µm line. The wavelength coverage of ISOPHOT (ending at 11.6 µm) hampers the determination of the continuum redwards of the [S iv] 10.5 µm line. Without continuum poin ...
... spectra, the spline points for this continuum were located at ∼5.8 µm, in the 9–10 µm region, and at the blue base of the [S iv] 10.5 µm line. The wavelength coverage of ISOPHOT (ending at 11.6 µm) hampers the determination of the continuum redwards of the [S iv] 10.5 µm line. Without continuum poin ...
The binary fractions in the massive young Large Magellanic Cloud
... yield high detection efficiency, since it only depends on a single set of observations. In principle, one does not need to adopt many physical assumptions either; the approach is only based on our understanding of stellar evolution. This also allows us to simulate artificial observations for compari ...
... yield high detection efficiency, since it only depends on a single set of observations. In principle, one does not need to adopt many physical assumptions either; the approach is only based on our understanding of stellar evolution. This also allows us to simulate artificial observations for compari ...
The KMOS Redshift One Spectroscopic Survey
... at progressively high redshifts, in that galaxies with the same rotation velocity in the distant Universe have lower stellar masses (e.g. Swinbank et al. 2006). This suggests either higher gas fractions as measured directly by Tacconi et al. (2010) or increased dark matter fractions or perhaps even ...
... at progressively high redshifts, in that galaxies with the same rotation velocity in the distant Universe have lower stellar masses (e.g. Swinbank et al. 2006). This suggests either higher gas fractions as measured directly by Tacconi et al. (2010) or increased dark matter fractions or perhaps even ...
Galaxy Zoo: Are bars responsible for the feeding
... We present a new study investigating whether active galactic nuclei (AGN) beyond the local universe are preferentially fed via large-scale bars. Our investigation combines data from Chandra and Galaxy Zoo: Hubble (GZH) in the AEGIS (All-wavelength Extended Groth strip International Survey), COSMOS ( ...
... We present a new study investigating whether active galactic nuclei (AGN) beyond the local universe are preferentially fed via large-scale bars. Our investigation combines data from Chandra and Galaxy Zoo: Hubble (GZH) in the AEGIS (All-wavelength Extended Groth strip International Survey), COSMOS ( ...
Universe of Motion - Reciprocal System of theory
... The availability of this accurate new physical theory, developed and verified in other fields where the facts are more readily accessible, now gives us a source of information about astronomical matters that is not subject to the limitations that are inherent in the procedures that the astronomers m ...
... The availability of this accurate new physical theory, developed and verified in other fields where the facts are more readily accessible, now gives us a source of information about astronomical matters that is not subject to the limitations that are inherent in the procedures that the astronomers m ...
Small glitches: the role of strange nuggets?
... spin-frequencies during glitches) ∆Ω/Ω depend on the released energies during glitches, with less released energies corresponding to smaller glitch sizes. On the other hand, as one of the dark matter candidates, our Galaxy might be filled with so called strange nuggets (SNs) which are relics from th ...
... spin-frequencies during glitches) ∆Ω/Ω depend on the released energies during glitches, with less released energies corresponding to smaller glitch sizes. On the other hand, as one of the dark matter candidates, our Galaxy might be filled with so called strange nuggets (SNs) which are relics from th ...
c Copyright by Jonathan C. McKinney, 2004
... per baryon accreted closely follows the thin disk efficiency, so super-efficient accretion does not seem to be a generic property of thick magnetized relativistic disks (McKinney and Gammie, 2004). The Blandford-Znajek (BZ) effect, describing the extraction of spin energy of a rotating black hole b ...
... per baryon accreted closely follows the thin disk efficiency, so super-efficient accretion does not seem to be a generic property of thick magnetized relativistic disks (McKinney and Gammie, 2004). The Blandford-Znajek (BZ) effect, describing the extraction of spin energy of a rotating black hole b ...
The dark matter crisis: falsification of the current standard model of
... ram-pressure-dwarf (type B) galaxies void of DM. Type A dwarfs surround the host approximately spherically, while type B dwarfs are typically correlated in phase-space. Type B dwarfs must exist in any cosmological theory in which galaxies interact. Only one type of dwarf galaxy is observed to exist ...
... ram-pressure-dwarf (type B) galaxies void of DM. Type A dwarfs surround the host approximately spherically, while type B dwarfs are typically correlated in phase-space. Type B dwarfs must exist in any cosmological theory in which galaxies interact. Only one type of dwarf galaxy is observed to exist ...
White dwarfs, black holes and neutron stars in close binaries
... Human and 1 litre water. Lines of constant density are plotted for water (solid), gold (dashed) and air (dotted). The top dotted line gives the density of the ISM and the bottom dashed line the Schwarzschild radius for black holes. ...
... Human and 1 litre water. Lines of constant density are plotted for water (solid), gold (dashed) and air (dotted). The top dotted line gives the density of the ISM and the bottom dashed line the Schwarzschild radius for black holes. ...
H i AND CO IN BLUE COMPACT DWARF GALAXIES: HARO 2 AND
... for primary-beam attenuation elevates the rms by a factor of 5, approximately. The observations have on average an H i mass detection threshold for individual clouds of 4.5 106 M and 1.1 106 M for Haro 2 and Haro 4, respectively. These values correspond to surface brightness sensitivities of 2 ...
... for primary-beam attenuation elevates the rms by a factor of 5, approximately. The observations have on average an H i mass detection threshold for individual clouds of 4.5 106 M and 1.1 106 M for Haro 2 and Haro 4, respectively. These values correspond to surface brightness sensitivities of 2 ...
A deep view on the Virgo cluster core
... Virgo cluster members. The images in both bands were inspected independently from each other. A first pre-selection was based on the following selection criteria. 1. The depth of the observed data revealed many background objects. While their physical size and luminosity would typically be larger th ...
... Virgo cluster members. The images in both bands were inspected independently from each other. A first pre-selection was based on the following selection criteria. 1. The depth of the observed data revealed many background objects. While their physical size and luminosity would typically be larger th ...
Submm Observations of Massive Star Formation in the Giant
... Aims. This dissertation focuses on the detailed study of the region NGC 6334, located in the Galaxy at a distance of 1.7 kpc. It is aimed to trace the gas velocities in the filamentary, massive star-forming region NGC 6334 at several scales and to explain its dynamics. For that purpose, different sc ...
... Aims. This dissertation focuses on the detailed study of the region NGC 6334, located in the Galaxy at a distance of 1.7 kpc. It is aimed to trace the gas velocities in the filamentary, massive star-forming region NGC 6334 at several scales and to explain its dynamics. For that purpose, different sc ...
Globular Cluster Bimodality in Isolated Elliptical Galaxies
... composition and are roughly at the same distance from the earth (differing only in their masses), forming rare astrophysical “laboratories”. A globular cluster (GC) is a roughly spherical group of stars, orbiting a galactic core, tightly bound by gravity with high stellar density towards the center. ...
... composition and are roughly at the same distance from the earth (differing only in their masses), forming rare astrophysical “laboratories”. A globular cluster (GC) is a roughly spherical group of stars, orbiting a galactic core, tightly bound by gravity with high stellar density towards the center. ...
- Max-Planck-Institut für Astronomie
... be detected in our images occur only when the galaxies are very close together—typically between the last close pass prior to coalescence and coalescence itself.15 Orientation plays a role: interactions viewed nearly parallel to the orbital plane are visible as very close pairs for 2–3 times longer ...
... be detected in our images occur only when the galaxies are very close together—typically between the last close pass prior to coalescence and coalescence itself.15 Orientation plays a role: interactions viewed nearly parallel to the orbital plane are visible as very close pairs for 2–3 times longer ...
Radio properties of a complete sample of nearby groups of galaxies
... low-frequency GMRT radio images of the nearby (<80 Mpc) central brightest group ellipticals from the high richness CLoGS sub-sample are presented for the first time at 235 and 610 MHz. Using the sensitivity to older electron populations at 235 MHz and the resolution of 610 MHz as a key to identify p ...
... low-frequency GMRT radio images of the nearby (<80 Mpc) central brightest group ellipticals from the high richness CLoGS sub-sample are presented for the first time at 235 and 610 MHz. Using the sensitivity to older electron populations at 235 MHz and the resolution of 610 MHz as a key to identify p ...
BLANCO CARDENAS
... antigua casera Sharo. A aquellos que se fueron de Granada hace un tiempo, estoy feliz de que sean piezas de este rompecabezas con la Alhambra de fondo: gracias Juliane Serres, Ana Victoria Cuesta, Sebastian “Chingue” Meier, Lucı́a Piñeiro Freire, Lizette Duque, Ana Marı́a Salazar; sigo recordándol ...
... antigua casera Sharo. A aquellos que se fueron de Granada hace un tiempo, estoy feliz de que sean piezas de este rompecabezas con la Alhambra de fondo: gracias Juliane Serres, Ana Victoria Cuesta, Sebastian “Chingue” Meier, Lucı́a Piñeiro Freire, Lizette Duque, Ana Marı́a Salazar; sigo recordándol ...
Dust attenuation up to z ≃ 2 in the AKARI North Ecliptic Pole Deep
... 23 345 sources in common within a tolerance radius of 1 arcsec on the coordinates. MegaCam (u? , g0 , r0 , i0 , z0 ) and WIRCam (Y, J, Ks) data are available for these sources. The 5σ detection limits correspond to u? = 24.6, g0 = 26.5, r0 = 25.7, i0 = 24.9, z0 = 23.9, Y = 23.2, J = 22.8, and Ks = 2 ...
... 23 345 sources in common within a tolerance radius of 1 arcsec on the coordinates. MegaCam (u? , g0 , r0 , i0 , z0 ) and WIRCam (Y, J, Ks) data are available for these sources. The 5σ detection limits correspond to u? = 24.6, g0 = 26.5, r0 = 25.7, i0 = 24.9, z0 = 23.9, Y = 23.2, J = 22.8, and Ks = 2 ...
Link
... earlier type stars trace sites of star birth younger than 40 Myr. OB associations whose most massive members have later spectral types can identify locales where stars formed more than 40 Myr ago. The mass spectra, locations, velocities, and ages of young stars and the properties of gas in nearby as ...
... earlier type stars trace sites of star birth younger than 40 Myr. OB associations whose most massive members have later spectral types can identify locales where stars formed more than 40 Myr ago. The mass spectra, locations, velocities, and ages of young stars and the properties of gas in nearby as ...
The drop in the cosmic star formation rate below redshift 2 is caused
... large (see Booth & Schaye 2009). A fraction of 1.5 per cent of the rest-mass energy of the accreted gas is injected into the surrounding medium in the form of heat, by increasing the temperature of at least one neighbouring gas particle by at least 108 K. The minimum temperature increase ensures tha ...
... large (see Booth & Schaye 2009). A fraction of 1.5 per cent of the rest-mass energy of the accreted gas is injected into the surrounding medium in the form of heat, by increasing the temperature of at least one neighbouring gas particle by at least 108 K. The minimum temperature increase ensures tha ...
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.