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... PSF fitting for HST does 0.01 pixels, or half a mili-arcsecond so the minimal detections with HST go out to 2-3 kilaparsecs (WFC or HRC) ...
... PSF fitting for HST does 0.01 pixels, or half a mili-arcsecond so the minimal detections with HST go out to 2-3 kilaparsecs (WFC or HRC) ...
3 Gravitational Waves from Binaries
... The low-frequency band is the domain of detectors flown in space (in Earth orbit or in interplanetary orbit). The most important of these are the Doppler tracking o f spacecraft via microwave signals sent from Earth to the spacecraft and there transponded back to Earth (a technique that N A S A has ...
... The low-frequency band is the domain of detectors flown in space (in Earth orbit or in interplanetary orbit). The most important of these are the Doppler tracking o f spacecraft via microwave signals sent from Earth to the spacecraft and there transponded back to Earth (a technique that N A S A has ...
G070666-00 - DCC
... Compact Binary Inspirals: Identifying a possible gravitational wave (2/2) • Second step: Follow up event candidates remaining at end of pipeline Goal: determine our level of confidence in the detection → Each candidate is analyzed through a detection checklist: - Check for data quality at the time ...
... Compact Binary Inspirals: Identifying a possible gravitational wave (2/2) • Second step: Follow up event candidates remaining at end of pipeline Goal: determine our level of confidence in the detection → Each candidate is analyzed through a detection checklist: - Check for data quality at the time ...
The Cosmos in Your Pocket: How Cosmological
... • 1862: Alvan Clark reported the detection of a faint star near Sirius, believed to be a companion of the star[25]. This would explain Bessel’s 1844 observations. • 1896: J. Schaeberle discovered a faint companion of the star Procyon, estimating its mass to be about 1/5 that of Procyon and suspectin ...
... • 1862: Alvan Clark reported the detection of a faint star near Sirius, believed to be a companion of the star[25]. This would explain Bessel’s 1844 observations. • 1896: J. Schaeberle discovered a faint companion of the star Procyon, estimating its mass to be about 1/5 that of Procyon and suspectin ...
The X-shooter Spectral Library (XSL): I. DR1. Near
... spectra may vary substantially during their pulsation cycles. X-shooter offers multiple spectroscopic observation modes; we used the longslit SLIT mode for all observations. Three observing strategies are supported in SLIT mode: classical “staring” observations, A–B “nodding” along the slit for impr ...
... spectra may vary substantially during their pulsation cycles. X-shooter offers multiple spectroscopic observation modes; we used the longslit SLIT mode for all observations. Three observing strategies are supported in SLIT mode: classical “staring” observations, A–B “nodding” along the slit for impr ...
thesis
... occurs a much greater portion of their formation history is hidden from our view compared to the case for low-mass star formation. Finally, massive stars often form in the densest clusters, making the interpretation of the observations much more difficult. Nevertheless, the following sequence of eve ...
... occurs a much greater portion of their formation history is hidden from our view compared to the case for low-mass star formation. Finally, massive stars often form in the densest clusters, making the interpretation of the observations much more difficult. Nevertheless, the following sequence of eve ...
U P C NIVERSITAT
... marked contrast to the case of core-collapse supernovae, whose stellar progenitors are highly-luminous, massive stars. Observational evidence favors the double-degenerate channel, but significant discrepancies exist between observations and theory. There are approximately a few hundred million doubl ...
... marked contrast to the case of core-collapse supernovae, whose stellar progenitors are highly-luminous, massive stars. Observational evidence favors the double-degenerate channel, but significant discrepancies exist between observations and theory. There are approximately a few hundred million doubl ...
THE STAR FORMATION AND NUCLEAR ACCRETION HISTORIES OF NORMAL GALAXIES
... dominated by star formation, while that from early-type galaxies is dominated by a combination of hot gas and active galactic nucleus (AGN) emission. We find that the mean star formation and supermassive black hole accretion rate densities evolve like ∼ (1+z)3±1 , in agreement with the trends found ...
... dominated by star formation, while that from early-type galaxies is dominated by a combination of hot gas and active galactic nucleus (AGN) emission. We find that the mean star formation and supermassive black hole accretion rate densities evolve like ∼ (1+z)3±1 , in agreement with the trends found ...
CONNECTING ANGULAR MOMENTUM AND GALACTIC DYNAMICS
... Chen et al. (2003) compared the spin parameter and the misalignment angles between the dark matter and gas angular momentum vectors obtained in simulations, which include radiative cooling. This enables a splitting of the gas into a cold and a hot component. In their non-radiative model they confirm ...
... Chen et al. (2003) compared the spin parameter and the misalignment angles between the dark matter and gas angular momentum vectors obtained in simulations, which include radiative cooling. This enables a splitting of the gas into a cold and a hot component. In their non-radiative model they confirm ...
X-ray sources in the starburst spiral galaxy M 83
... point sources are detected (above 3.5-σ) in the ACIS S3 image, and 15 of them are within the inner 1600 region of the galaxy. A point source with Lx ≈ 3 × 1038 erg s−1 in the 0.3–8.0 keV band is found to coincide with the infra-red nuclear photometric peak, one of the two dynamical nuclei of the gal ...
... point sources are detected (above 3.5-σ) in the ACIS S3 image, and 15 of them are within the inner 1600 region of the galaxy. A point source with Lx ≈ 3 × 1038 erg s−1 in the 0.3–8.0 keV band is found to coincide with the infra-red nuclear photometric peak, one of the two dynamical nuclei of the gal ...
The impact of protocluster environments at z = 1.6
... colour separates passive and dusty galaxies from unobscured starforming galaxies. The z − J colours of the control field galaxies have been K-corrected to z = 1.62. The distributions of control field and intergroup galaxies in colour–mass space are very similar. Galaxies in both samples populate a ...
... colour separates passive and dusty galaxies from unobscured starforming galaxies. The z − J colours of the control field galaxies have been K-corrected to z = 1.62. The distributions of control field and intergroup galaxies in colour–mass space are very similar. Galaxies in both samples populate a ...
Elliptical Galaxies
... Elliptical galaxies are smooth, quiescent star-piles, devoid of any of the spectacular structures found in SPIRAL GALAXIES. They have no disk, no spiral structure and only small amounts of the gas and dust. As a result there are no obvious symptoms of continuing star formation: no H II regions or yo ...
... Elliptical galaxies are smooth, quiescent star-piles, devoid of any of the spectacular structures found in SPIRAL GALAXIES. They have no disk, no spiral structure and only small amounts of the gas and dust. As a result there are no obvious symptoms of continuing star formation: no H II regions or yo ...
A non-LTE analysis of the hot subdwarf O star BD+28°4211
... horizontal branch (EHB) region, which is itself a hot extension of the horizontal branch. The EHB region of the HertzsprungRussell (HR) diagram encompasses stars that span a wide range of effective temperatures, from 22 000 K up to 100 000 K, and these stars are more compact (4.8 < ∼ log g < ∼ 6.4) t ...
... horizontal branch (EHB) region, which is itself a hot extension of the horizontal branch. The EHB region of the HertzsprungRussell (HR) diagram encompasses stars that span a wide range of effective temperatures, from 22 000 K up to 100 000 K, and these stars are more compact (4.8 < ∼ log g < ∼ 6.4) t ...
A Universal Stellar Initial Mass Function? A Critical Look Further
... The second implicit assumption is required due to finite stellar lifetimes. If one counts stars in a population spanning a large range of ages (as in the disk of the Milky Way), one can only construct the present-day mass function (PDMF). In this example, some fraction of the more massive stars with ...
... The second implicit assumption is required due to finite stellar lifetimes. If one counts stars in a population spanning a large range of ages (as in the disk of the Milky Way), one can only construct the present-day mass function (PDMF). In this example, some fraction of the more massive stars with ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.