The Primeval Populations of the Ultra
... than that of any globular cluster, the age determination must rely upon theoretical isochrones (see §3.2), but a comparison to M92 is still instructive. In our analysis, the largest uncertainties are the distances of the UFDs relative to the globular cluster calibrators of our isochrone library, wit ...
... than that of any globular cluster, the age determination must rely upon theoretical isochrones (see §3.2), but a comparison to M92 is still instructive. In our analysis, the largest uncertainties are the distances of the UFDs relative to the globular cluster calibrators of our isochrone library, wit ...
Formation of Massive Stars
... UC HII regions are powerful radio beacons of newly formed stars still embedded in their natal molecular clouds • Physical parameters of compact regions of ionized gas are determined mostly from radio data • Radio continuum is modeled as free-free from an isothermal homogeneous region of ionized gas ...
... UC HII regions are powerful radio beacons of newly formed stars still embedded in their natal molecular clouds • Physical parameters of compact regions of ionized gas are determined mostly from radio data • Radio continuum is modeled as free-free from an isothermal homogeneous region of ionized gas ...
Chapter 2 The HRS+ Sample 2.1 The Herschel Reference Survey
... the sample used in this thesis as the HRS+ sample. As such, these criteria produce a sample of 454 galaxies residing within the area of sky between 10h 17m < R.A.(2000) < 14h 43m and -6◦ < Dec. < 60◦ , shown in Figure 2.1. This sample consists of 171 early-type and 283 late-type galaxies inhabiting ...
... the sample used in this thesis as the HRS+ sample. As such, these criteria produce a sample of 454 galaxies residing within the area of sky between 10h 17m < R.A.(2000) < 14h 43m and -6◦ < Dec. < 60◦ , shown in Figure 2.1. This sample consists of 171 early-type and 283 late-type galaxies inhabiting ...
Merger of binary neutron stars with realistic equations of state in full
... realistic equations of state are quite different from those in the -law equation of state with 2 (hereafter referred to as the 2 equation of state) which has been widely adopted so far (e.g., [12]).1 It can be expected that these differences will modify the properties of the merger quantita ...
... realistic equations of state are quite different from those in the -law equation of state with 2 (hereafter referred to as the 2 equation of state) which has been widely adopted so far (e.g., [12]).1 It can be expected that these differences will modify the properties of the merger quantita ...
Article PDF - IOPscience
... analyzed here (NGC 6240 and NGC 6000). We refer the reader to Mattila et al. (2007), Kankare et al. (2008, 2012), Väisänen et al. (2008a, 2008b), and Randriamanakoto et al. (2013) for details of observations and data reduction. 2.1. Photometry and SSC Selection The SSC candidate photometric catalo ...
... analyzed here (NGC 6240 and NGC 6000). We refer the reader to Mattila et al. (2007), Kankare et al. (2008, 2012), Väisänen et al. (2008a, 2008b), and Randriamanakoto et al. (2013) for details of observations and data reduction. 2.1. Photometry and SSC Selection The SSC candidate photometric catalo ...
Feedback in low-mass galaxies in the early Universe
... As exemplified by M82, the archetypal starburst described above, detailed observations of galactic outflows in the local Universe reveal that they are a complex, multi-phase phenomenon, with outflows observed in hot gas traced by X-rays51,52, ionized gas seen via optical emission lines53, neutral ga ...
... As exemplified by M82, the archetypal starburst described above, detailed observations of galactic outflows in the local Universe reveal that they are a complex, multi-phase phenomenon, with outflows observed in hot gas traced by X-rays51,52, ionized gas seen via optical emission lines53, neutral ga ...
Astronomy Astrophysics
... X-3 in quiescence, at orbital phases 0.83 to 1.04. The 2.4–12 µm continuum radiation observed with ISOPHOT-S can be explained by thermal free-free emission in an expanding wind with, above 6.5 µm, a possible additional black-body component with temperature T ∼ 250 K and radius R ∼ 5000 R at 10 kpc, ...
... X-3 in quiescence, at orbital phases 0.83 to 1.04. The 2.4–12 µm continuum radiation observed with ISOPHOT-S can be explained by thermal free-free emission in an expanding wind with, above 6.5 µm, a possible additional black-body component with temperature T ∼ 250 K and radius R ∼ 5000 R at 10 kpc, ...
The age of elliptical galaxies and bulges in a merger model The age
... galaxies using absorption-line index strengths show that the outer parts of elliptical galaxies are both older and more metal-poor than the nuclei, consistent with the merger/starburst picture (Faber et al. 1995). The fact remains, however, that the stellar populations of present-day elliptical gala ...
... galaxies using absorption-line index strengths show that the outer parts of elliptical galaxies are both older and more metal-poor than the nuclei, consistent with the merger/starburst picture (Faber et al. 1995). The fact remains, however, that the stellar populations of present-day elliptical gala ...
Low radioderived star formation rates in z < 0.5 gammaray burst host
... Radio SFRs in GRB host galaxies SFRs (2.4 and 1.1 M yr−1 , respectively). However, measurements of [O II] emission-line flux have yielded higher estimates of ∼10– 11 M yr−1 (Küpcü Yoldaş, Greiner & Perna 2006; Levesque et al. 2010a). Our upper limit, derived from 6-cm radio flux, is SFRradio < ...
... Radio SFRs in GRB host galaxies SFRs (2.4 and 1.1 M yr−1 , respectively). However, measurements of [O II] emission-line flux have yielded higher estimates of ∼10– 11 M yr−1 (Küpcü Yoldaş, Greiner & Perna 2006; Levesque et al. 2010a). Our upper limit, derived from 6-cm radio flux, is SFRradio < ...
A comparison of the s- and r-process element evolution in local
... galaxies to have a more homogeneous sample with data coming from different authors and to make a more proper comparison with the predictions of the models. In LMC06a, however, we only analysed the elements Ba and Eu. We extend the analysis to Yttrium and Lanthanum, for which there is a new set of dat ...
... galaxies to have a more homogeneous sample with data coming from different authors and to make a more proper comparison with the predictions of the models. In LMC06a, however, we only analysed the elements Ba and Eu. We extend the analysis to Yttrium and Lanthanum, for which there is a new set of dat ...
The Early-time Optical Properties of Gamma
... Gamma Ray Bursts (GRBs) are brief, intense flashes of high energy gamma rays originating at cosmological distances and often associated with subsequent radiation emitted at longer wavelengths from X-ray to radio waves on times scales of minutes to days after the initial gamma ray burst. In the stand ...
... Gamma Ray Bursts (GRBs) are brief, intense flashes of high energy gamma rays originating at cosmological distances and often associated with subsequent radiation emitted at longer wavelengths from X-ray to radio waves on times scales of minutes to days after the initial gamma ray burst. In the stand ...
Recent star formation in local, morphologically disturbed
... In this work, we study the GALEX (UV) and Sloan Digital Sky Survey (SDSS; optical, see Adelman-McCarthy et al. 2006) properties of early-type galaxies on the optical red sequence, originally studied by van Dokkum (2005, hereafter vD05). The novelty of the vD05 study was the unprecedented depth of th ...
... In this work, we study the GALEX (UV) and Sloan Digital Sky Survey (SDSS; optical, see Adelman-McCarthy et al. 2006) properties of early-type galaxies on the optical red sequence, originally studied by van Dokkum (2005, hereafter vD05). The novelty of the vD05 study was the unprecedented depth of th ...
RADIO RELICS AND MAGNETIC FIELDS IN GALAXY CLUSTERS
... of the baryon mass indeed resides in the intra-cluster medium (ICM), a hot and tenuous medium which permeates the whole cluster volume. Its thermal bremsstrahlung emission in the X-rays makes clusters visible in the X-rays and plays an important role in the understanding of cluster physics. In the r ...
... of the baryon mass indeed resides in the intra-cluster medium (ICM), a hot and tenuous medium which permeates the whole cluster volume. Its thermal bremsstrahlung emission in the X-rays makes clusters visible in the X-rays and plays an important role in the understanding of cluster physics. In the r ...
The First Galaxies: Assembly under Radiative Feedback from the
... Radiation in the Lyman-Werner (LW) bands dissociates molecular hydrogen, the main coolant in minihalos (e.g., Haiman et al. 1997). Hydrogen-ionizing radiation heats the gas inside the first halos and the intergalactic medium (IGM). The associated increase in pressure drives the gas outside halos wit ...
... Radiation in the Lyman-Werner (LW) bands dissociates molecular hydrogen, the main coolant in minihalos (e.g., Haiman et al. 1997). Hydrogen-ionizing radiation heats the gas inside the first halos and the intergalactic medium (IGM). The associated increase in pressure drives the gas outside halos wit ...
The VLT LEGA-C Spectroscopic Survey: The Physics of Galaxies at
... star formation history and galaxy structure: among starforming galaxies the instantaneous SFR depends on concentration (Whitaker et al. 2015), and it has been argued that bulge fraction is the driving factor (Abramson et al. 2014; Lang et al. 2014). This explains to some extent, but not fully, the s ...
... star formation history and galaxy structure: among starforming galaxies the instantaneous SFR depends on concentration (Whitaker et al. 2015), and it has been argued that bulge fraction is the driving factor (Abramson et al. 2014; Lang et al. 2014). This explains to some extent, but not fully, the s ...
White dwarf binary
... Stellar death Supernova remnant Role of Mass White dwarfs White dwarf limit White dwarf binary Accretion disks Thought question Nova Thought question 2 types of SN Nova or supernova? Standard candles Neutron stars Discovery Crab pulsar Pulsars Pulsars are NS! Magnetic fields Thought question Binarie ...
... Stellar death Supernova remnant Role of Mass White dwarfs White dwarf limit White dwarf binary Accretion disks Thought question Nova Thought question 2 types of SN Nova or supernova? Standard candles Neutron stars Discovery Crab pulsar Pulsars Pulsars are NS! Magnetic fields Thought question Binarie ...
IR-excesses around nearby Lambda Boo stars are caused by debris
... bow waves have been referred to as “bow shocks” in the literature, but this implies that the gas is being shocked, which is not what is being modelled, so we will not refer to it as such. Since the gas density can be low and dust does not shock like a fluid, the dust is rather pushed around a cone o ...
... bow waves have been referred to as “bow shocks” in the literature, but this implies that the gas is being shocked, which is not what is being modelled, so we will not refer to it as such. Since the gas density can be low and dust does not shock like a fluid, the dust is rather pushed around a cone o ...
Fraction of the X-ray selected AGNs with optical emission lines in
... that the AGN fraction in clusters is 3.0+2.4 −1.4 %, suggesting the rising tendency of AGN fraction in clusters with redshift from 0.05 to 1.5. With the Chandra Multiwavelength Project (ChaMP) and SDSS data, using L0.5−8keV > 1042 erg s−1 to select AGNs, Haggard et al. (2010) found that the AGN frac ...
... that the AGN fraction in clusters is 3.0+2.4 −1.4 %, suggesting the rising tendency of AGN fraction in clusters with redshift from 0.05 to 1.5. With the Chandra Multiwavelength Project (ChaMP) and SDSS data, using L0.5−8keV > 1042 erg s−1 to select AGNs, Haggard et al. (2010) found that the AGN frac ...
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 ...
Early Star-Forming Galaxies and the Reionisation of the Universe
... the universe was ~1 billion years old, and the transition from a neutral medium is popularly interpreted as arising from ionising photons with energies greater than 13.6eV (wavelength λ<91.2 nm) generated by primitive stars and galaxies4 (Fig. 1). Astronomers wish to confirm the connection between e ...
... the universe was ~1 billion years old, and the transition from a neutral medium is popularly interpreted as arising from ionising photons with energies greater than 13.6eV (wavelength λ<91.2 nm) generated by primitive stars and galaxies4 (Fig. 1). Astronomers wish to confirm the connection between e ...
MAXI J1659-152 - UvA-DARE
... 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 ...
![The P Cygni supergiant [OMN2000] LS1](http://s1.studyres.com/store/data/014882705_1-5f78b60dc5267f0c5ad35fc8d810ae0e-300x300.png)
The P Cygni supergiant [OMN2000] LS1
... To derive the stellar parameters for [OMN2000] LS1 one must adopt a distance to it and, by extension, the W51 complex. Figueruedo et al. (2008) provides a summary of the results of previous studies. These show that the kinematic estimate of the distance - utilising radio recombination lines - of 5.5 ...
... To derive the stellar parameters for [OMN2000] LS1 one must adopt a distance to it and, by extension, the W51 complex. Figueruedo et al. (2008) provides a summary of the results of previous studies. These show that the kinematic estimate of the distance - utilising radio recombination lines - of 5.5 ...
Massive Disruptions in the Cool Core of MACS J1931.8-2634 Steven Ehlert
... The AGN jet power is sufficient to overcome radiative losses in the cool core. It appears that the AGN jets and large N-S oscillatory motion did considerably more than simply suppress the cooling flow. Some fraction of the original cool core now resides 30 kpc to the north of the central AGN with ev ...
... The AGN jet power is sufficient to overcome radiative losses in the cool core. It appears that the AGN jets and large N-S oscillatory motion did considerably more than simply suppress the cooling flow. Some fraction of the original cool core now resides 30 kpc to the north of the central AGN with ev ...
The asymmetric nuclear region of M83 and its off
... The barred spiral galaxy M83 is one of the closest galaxies hosting a nuclear starburst. It is almost face-on (i=24◦ Comte 1981), and at a distance of 4.5 Mpc (Thim et al. 2003) it allows excellent spatial resolution (1′′ =22 pc) over the active region. The nuclear region has been studied in detail ...
... The barred spiral galaxy M83 is one of the closest galaxies hosting a nuclear starburst. It is almost face-on (i=24◦ Comte 1981), and at a distance of 4.5 Mpc (Thim et al. 2003) it allows excellent spatial resolution (1′′ =22 pc) over the active region. The nuclear region has been studied in detail ...
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.