SKA and VLBI synergies
... a unique tool providing stellar parallax measurements and proper motion determinations as well as the search for planets via the reflex motion of the star. The addition of SKA to the Global VLBI Arrays will not increase the angular resolution of the arrays. However, it will provide an excellent sens ...
... a unique tool providing stellar parallax measurements and proper motion determinations as well as the search for planets via the reflex motion of the star. The addition of SKA to the Global VLBI Arrays will not increase the angular resolution of the arrays. However, it will provide an excellent sens ...
10:30 Coffee break - Astrometry and Astrophysics in the Gaia sky
... 13:10 Lunch break Astrometry and fundamental physics ...
... 13:10 Lunch break Astrometry and fundamental physics ...
A STRONGLY MAGNETIZED PULSAR WITHIN THE GRASP OF THE MILKY... SUPERMASSIVE BLACK HOLE Rea ,
... (ACIS-S; see Table 1). The HRC-S instrument (timing mode with a 0. 14 pixel size) observed SGR J1745–2900 for about 10 ks. The three ACIS-S observations were performed in faint data mode with the one-eight chip sub-array (the source was positioned in the back-illuminated ACIS-S3 CCD at the nominal ...
... (ACIS-S; see Table 1). The HRC-S instrument (timing mode with a 0. 14 pixel size) observed SGR J1745–2900 for about 10 ks. The three ACIS-S observations were performed in faint data mode with the one-eight chip sub-array (the source was positioned in the back-illuminated ACIS-S3 CCD at the nominal ...
JOA Vol 1 No. 2 - Apr 2011 - RASNZ Occultation Section
... When we realize that an asteroidal occultation has been reasonably well-observed, we inform Brian Warner, [email protected], and he notifies other observers of asteroid lightcurves that observations are desirable soon. It’s also useful to inform Raoul Behrend, [email protected], sin ...
... When we realize that an asteroidal occultation has been reasonably well-observed, we inform Brian Warner, [email protected], and he notifies other observers of asteroid lightcurves that observations are desirable soon. It’s also useful to inform Raoul Behrend, [email protected], sin ...
Astronomy Astrophysics - Max Planck Institut für Radioastronomie
... regime (for four objects) as well as in the spectrally resolved Brγ emission line (for one object). The spectro-interferometric data is supplemented by archival and new VLT/ISAAC spectroscopy. Results. For all objects (except MWC 297), we measure an increase of visibility within the Brγ emission lin ...
... regime (for four objects) as well as in the spectrally resolved Brγ emission line (for one object). The spectro-interferometric data is supplemented by archival and new VLT/ISAAC spectroscopy. Results. For all objects (except MWC 297), we measure an increase of visibility within the Brγ emission lin ...
Supervisors
... Introduction Stellar spectra provide most of the information that is known about the stars, such as their chemical composition, rotation, magnetic fields etc. The light that makes up the spectrum of a star is radiated by its outer layers that are called a stellar atmosphere. Understanding stellar a ...
... Introduction Stellar spectra provide most of the information that is known about the stars, such as their chemical composition, rotation, magnetic fields etc. The light that makes up the spectrum of a star is radiated by its outer layers that are called a stellar atmosphere. Understanding stellar a ...
2 GMT OVERVIEW
... The baseline GMT is designed to allow five observing modes, two in natural seeing and three with adaptive optics. In natural seeing, the GMT’s aplanatic Gregorian design provides a field of view 8′ in diameter with (geometric) image aberrations less than 0.1″ RMS diameter. With a refractive correcto ...
... The baseline GMT is designed to allow five observing modes, two in natural seeing and three with adaptive optics. In natural seeing, the GMT’s aplanatic Gregorian design provides a field of view 8′ in diameter with (geometric) image aberrations less than 0.1″ RMS diameter. With a refractive correcto ...
THE ORIGIN AND EVOLUTION OF PLANETARY NEBULAE
... The first planetary nebula was observed by Charles Messier in 1764 and was given the number 27 in his catalog of nebulous objects. The final version of the Messier catalog of 1784 included four planetary nebulae (PN) together with other nonstarlike objects such as galaxies and star clusters. The nam ...
... The first planetary nebula was observed by Charles Messier in 1764 and was given the number 27 in his catalog of nebulous objects. The final version of the Messier catalog of 1784 included four planetary nebulae (PN) together with other nonstarlike objects such as galaxies and star clusters. The nam ...
The Correlation of Lithium and Beryllium in F and G
... (1) it is more difficult to observe the resonance lines of Be ii near the atmospheric cutoff near 3000 8, (2) there is more line blending in that spectral region, which can blur the spectra of relatively slowly rotating stars, and (3) the spectrum synthesis requires knowledge of the UV opacity sourc ...
... (1) it is more difficult to observe the resonance lines of Be ii near the atmospheric cutoff near 3000 8, (2) there is more line blending in that spectral region, which can blur the spectra of relatively slowly rotating stars, and (3) the spectrum synthesis requires knowledge of the UV opacity sourc ...
DEPT OF PHYSICS AND ASTRONOMY M.Sc
... e. g. Meteorology, Geological Survey, National Standard organization; in Industrial research Establishment e.g. Astronomical Observations NRAO, NAOJ, ESO, ALMA, FIIRO, PRODA, NASDRA, NASENI, NAEA, SHETSCO; In oil, steel and other industries; and commercial and technical firms needs the services of a ...
... e. g. Meteorology, Geological Survey, National Standard organization; in Industrial research Establishment e.g. Astronomical Observations NRAO, NAOJ, ESO, ALMA, FIIRO, PRODA, NASDRA, NASENI, NAEA, SHETSCO; In oil, steel and other industries; and commercial and technical firms needs the services of a ...
Study of an unbiased sample of B stars observed with Hipparcos
... diagram. The simultaneous detection of these different kinds of modes has never been firmly established in a B-type star. Mathias & Waelkens (1995) have found indications that this might be the case in the star ι Her, but their data set was not sufficiently extensive to unambiguously derive frequenc ...
... diagram. The simultaneous detection of these different kinds of modes has never been firmly established in a B-type star. Mathias & Waelkens (1995) have found indications that this might be the case in the star ι Her, but their data set was not sufficiently extensive to unambiguously derive frequenc ...
First detection of helium emissions in RR Lyrae⋆
... to 0.967). From these figures, nothing was visible (no absorption) before the appearance of He I emission. The maximum He I emission is near 7% at ϕ = 0.911 and occurs at the same time as the maximum Hα emission (I = 27%). It seems (see Fig. 4) that a Schwarzschild’s mechanism (absorption line doubl ...
... to 0.967). From these figures, nothing was visible (no absorption) before the appearance of He I emission. The maximum He I emission is near 7% at ϕ = 0.911 and occurs at the same time as the maximum Hα emission (I = 27%). It seems (see Fig. 4) that a Schwarzschild’s mechanism (absorption line doubl ...
Boron Abundances Across the" Li
... Observations with the STIS instrument on the Hubble Space Telescope were made of vB 14 on 2003 September 9 to determine the B abundance as part of a program to look at B through the Li-Be dip in the Hyades. The four other stars in that program were not observed by the time that STIS died. After the ...
... Observations with the STIS instrument on the Hubble Space Telescope were made of vB 14 on 2003 September 9 to determine the B abundance as part of a program to look at B through the Li-Be dip in the Hyades. The four other stars in that program were not observed by the time that STIS died. After the ...
astronomy and the limits of vision
... Celestial visibility is the study of the limits of observability of objects in the sky, with application to deducing the truth about historical events or to the derivation of astronomical information of modem utility. This study is based on what is seen by ordinary humans, either in their everyday l ...
... Celestial visibility is the study of the limits of observability of objects in the sky, with application to deducing the truth about historical events or to the derivation of astronomical information of modem utility. This study is based on what is seen by ordinary humans, either in their everyday l ...
Numerical models of sunspot formation and fine structure
... promises to resolve many of the challenges that currently restrict the reliable use of helioseismic inversions within and near sunspots. The fine structure of sunspots present at the smallest currently observable scales has puzzled observers for more than a century (see recent reviews [8–12]). In the ...
... promises to resolve many of the challenges that currently restrict the reliable use of helioseismic inversions within and near sunspots. The fine structure of sunspots present at the smallest currently observable scales has puzzled observers for more than a century (see recent reviews [8–12]). In the ...
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... We offer a number of options to achieve these goals. Most of our students seek a Ph.D. in Physics, but we also confer Ph.D.s in Chemical Physics and Physics with formal emphasis in Medica ...
... We offer a number of options to achieve these goals. Most of our students seek a Ph.D. in Physics, but we also confer Ph.D.s in Chemical Physics and Physics with formal emphasis in Medica ...
IR-excesses around nearby Lambda Boo stars are caused by debris
... assisted spectroscopy from large ground-based telescopes would be required to identify a Lambda Boo-like signature in these stars, which has not been done. This could cement the relationship between ISM interactions and surface abundance anomalies. Other metal poor stars have also been searched for ...
... assisted spectroscopy from large ground-based telescopes would be required to identify a Lambda Boo-like signature in these stars, which has not been done. This could cement the relationship between ISM interactions and surface abundance anomalies. Other metal poor stars have also been searched for ...
radial metallicity gradients and age-metallicity relation of stars in the
... solar neighbourhood. The survey selection box was defined using the 2MASS photometry: 12 < J < 14 and 0.23 < J − K < 0.45 +0.5E(B−V); if there were not enough targets, the red edge was extended2. With these criteria, we are predominantly selecting FG stars with magnitudes down to V = 16.5 (Gilmore e ...
... solar neighbourhood. The survey selection box was defined using the 2MASS photometry: 12 < J < 14 and 0.23 < J − K < 0.45 +0.5E(B−V); if there were not enough targets, the red edge was extended2. With these criteria, we are predominantly selecting FG stars with magnitudes down to V = 16.5 (Gilmore e ...
Variability of young solar-type stars: Spot cycles, rotation
... of stellar activity and time series analysis all the way back during writing my bachelor’s thesis. I am grateful for their practical support and the insightful discussions I have had with both of them. A third instrumental person in the success of my thesis research has been Gregory Henry from the T ...
... of stellar activity and time series analysis all the way back during writing my bachelor’s thesis. I am grateful for their practical support and the insightful discussions I have had with both of them. A third instrumental person in the success of my thesis research has been Gregory Henry from the T ...
Massive Stars in the Arches Cluster 12
... choices are motivated by the fact that the majority of stars in the Arches cluster have values within these limits, as can be seen in Figure 4 of Figer et al. (1999a); stars with values outside of these limits are likely to be foreground or background stars. The resultant star list is shown in Table ...
... choices are motivated by the fact that the majority of stars in the Arches cluster have values within these limits, as can be seen in Figure 4 of Figer et al. (1999a); stars with values outside of these limits are likely to be foreground or background stars. The resultant star list is shown in Table ...
multiwavelength observations of the gamma-ray
... quiescence during the period 2009 July–December. Four Target-of-Opportunity observations with the XMM-Newton satellite in the 0.2–10 keV range were supplemented with optical observations at the MDM Observatory, radio and optical data from the GLAST-AGILE Support Program of the Whole Earth Blazar Tel ...
... quiescence during the period 2009 July–December. Four Target-of-Opportunity observations with the XMM-Newton satellite in the 0.2–10 keV range were supplemented with optical observations at the MDM Observatory, radio and optical data from the GLAST-AGILE Support Program of the Whole Earth Blazar Tel ...
IGR J18483-0311: a new intermediate supergiant fast X
... function of the duration and the frequency of their outbursts, as well as their Lmax /Lmin ratio, Walter & Zurita Heras (2007) showed the existence of intermediate SFXTs, characterised by a lower ratio and longer flares. Finally, Negueruela et al. (2008) proposed a general scheme to explain the emis ...
... function of the duration and the frequency of their outbursts, as well as their Lmax /Lmin ratio, Walter & Zurita Heras (2007) showed the existence of intermediate SFXTs, characterised by a lower ratio and longer flares. Finally, Negueruela et al. (2008) proposed a general scheme to explain the emis ...
A FUSE Survey of Coronal Forbidden Lines in Late
... We searched for evidence of coronal forbidden lines in the 900–1200 Å region in our sample of stellar spectra. Because of our relatively poor knowledge of the rest wavelengths of these lines, the relatively weak signal of the coronal lines, and the moderate likelihood of coincidental blends with lo ...
... We searched for evidence of coronal forbidden lines in the 900–1200 Å region in our sample of stellar spectra. Because of our relatively poor knowledge of the rest wavelengths of these lines, the relatively weak signal of the coronal lines, and the moderate likelihood of coincidental blends with lo ...
the red supergiant content of m31
... stars lose most of their hydrogen-rich envelopes and exploded instead as type II-L or even type Ib supernovae. The validity of this resolution rests on the assumption that the RSG mass-loss rates have been seriously underestimated. Meynet et al. (2015) and Georgy et al. (2015) proposed a novel way o ...
... stars lose most of their hydrogen-rich envelopes and exploded instead as type II-L or even type Ib supernovae. The validity of this resolution rests on the assumption that the RSG mass-loss rates have been seriously underestimated. Meynet et al. (2015) and Georgy et al. (2015) proposed a novel way o ...
Potassium abundances in nearby metal-poor stars
... of potassium abundances is difficult. Only the resonance doublet (K 7665 and 7699 Å) is available for abundance analyses of metal-poor stars, however, K resonance lines are often blended with very strong telluric O2 lines. There have been only a few studies which attempted to investigate the stell ...
... of potassium abundances is difficult. Only the resonance doublet (K 7665 and 7699 Å) is available for abundance analyses of metal-poor stars, however, K resonance lines are often blended with very strong telluric O2 lines. There have been only a few studies which attempted to investigate the stell ...
Indian Institute of Astrophysics
The Indian Institute of Astrophysics (IIA), with its headquarters in Bangalore (Karnataka state), India, is a premier national institute of India for the study of and research into topics pertaining to astronomy, astrophysics and related subjects.The Institute has a network of laboratories and observatories located in various places in India, including Kodaikanal (the Kodaikanal Solar Observatory), Kavalur (the Vainu Bappu Observatory), Gauribidanur, Hanle (the Indian Astronomical Observatory) and Hosakote.