![The old Nuclear Star Cluster in the Milky Way](http://s1.studyres.com/store/data/017241845_1-b4770ff8bf5e6640792374097eb10f54-300x300.png)
The old Nuclear Star Cluster in the Milky Way
... hole. For this ∼ 10000 proper motions, ∼ 2500 line-of-sight velocities, and star counts from Fritz et al. (2014) obtained with VLT instruments are used. In addition, for the first time a measurement of dust extinction within the Galactic old nuclear star cluster is presented. As a first step, the su ...
... hole. For this ∼ 10000 proper motions, ∼ 2500 line-of-sight velocities, and star counts from Fritz et al. (2014) obtained with VLT instruments are used. In addition, for the first time a measurement of dust extinction within the Galactic old nuclear star cluster is presented. As a first step, the su ...
Manual for Visual Observing of Variable Stars
... Variable stars are stars that change in brightness. Stars often vary in brightness when they are very young or when they are very old. The cause of variability may be intrinsic to the star (expansion, contraction, eruption, etc.), or may be due to extrinsic factors such as eclipses of two or more st ...
... Variable stars are stars that change in brightness. Stars often vary in brightness when they are very young or when they are very old. The cause of variability may be intrinsic to the star (expansion, contraction, eruption, etc.), or may be due to extrinsic factors such as eclipses of two or more st ...
New challenges for adaptive optics: extremely large telescopes
... to obtain the full potential in angular resolution, to avoid source confusion for extragalactic studies at high redshifts, and to reduce the background contribution, dramatically increasing limiting magnitude (the signal-to-noise ratio is then proportional to the square of telescope diameter). Compe ...
... to obtain the full potential in angular resolution, to avoid source confusion for extragalactic studies at high redshifts, and to reduce the background contribution, dramatically increasing limiting magnitude (the signal-to-noise ratio is then proportional to the square of telescope diameter). Compe ...
DOC - IVOA
... star’s entry becomes a group containing as few as one member. There were two general problems that prevented the IUE Object Class system from succeeding and thereby preventing archival data users from conveniently retrieving archival information on groups of stars with common properties. One was tha ...
... star’s entry becomes a group containing as few as one member. There were two general problems that prevented the IUE Object Class system from succeeding and thereby preventing archival data users from conveniently retrieving archival information on groups of stars with common properties. One was tha ...
A large-scale CO survey of the Rosette Molecular Cloud: assessing
... lines. The image also shows that many of the clumps and clouds are limb brightening on their edge facing the O stars. By consideration of the full data cube, we identify three distinct spatiovelocity structures: (1) relatively compact regions with broad line wings, identified as compact or well-coll ...
... lines. The image also shows that many of the clumps and clouds are limb brightening on their edge facing the O stars. By consideration of the full data cube, we identify three distinct spatiovelocity structures: (1) relatively compact regions with broad line wings, identified as compact or well-coll ...
$doc.title
... The lightcurve is characterised by rapid aperiodic ‘flaring’ throughout the 16 years of observations. Changes in the high excitation emission line component of the spectrum imply evolution in the stellar temperature - as expected for luminous blue variables although somewhat surprisingly, spectrosco ...
... The lightcurve is characterised by rapid aperiodic ‘flaring’ throughout the 16 years of observations. Changes in the high excitation emission line component of the spectrum imply evolution in the stellar temperature - as expected for luminous blue variables although somewhat surprisingly, spectrosco ...
Extragalactic background light inferred from AEGIS
... redshifts, and corrections to fit their results to other observational data are applied. Type (iii) models are not directly based on galaxy data. Instead, they are built from some parametrization of the history of the SFR density. This is a quantity derived using several different methods, each of w ...
... redshifts, and corrections to fit their results to other observational data are applied. Type (iii) models are not directly based on galaxy data. Instead, they are built from some parametrization of the history of the SFR density. This is a quantity derived using several different methods, each of w ...
the mass-loss return from evolved stars to the large
... MACHO data (Fraser et al. 2008) for HV 571514 indicate multi-periodic variability, with primary and secondary periods of 415.97 and 211.06 days, respectively, with corresponding peak-to-peak MACHO blue-band amplitudes of 0.8 and 0.66, respectively. On plots of Ks versus log(primary period) by Fraser ...
... MACHO data (Fraser et al. 2008) for HV 571514 indicate multi-periodic variability, with primary and secondary periods of 415.97 and 211.06 days, respectively, with corresponding peak-to-peak MACHO blue-band amplitudes of 0.8 and 0.66, respectively. On plots of Ks versus log(primary period) by Fraser ...
A numerical study of recent tidal interactions between dwarf galaxies
... In the context of dwarf galaxy interactions, mergers of dwarf galaxies have been studied (e.g. Bekki, 2008; Cloet-Osselaer et al., 2014; Starkenburg, Helmi & Sales, 2016). However, the study of tidal interactions without eventual merger has never been done in great detail. Only one numerical study w ...
... In the context of dwarf galaxy interactions, mergers of dwarf galaxies have been studied (e.g. Bekki, 2008; Cloet-Osselaer et al., 2014; Starkenburg, Helmi & Sales, 2016). However, the study of tidal interactions without eventual merger has never been done in great detail. Only one numerical study w ...
The Evolution of the Mass-Size relation to z = 3.5 in the GOODS
... in narrow mass bins for all galaxies from CDF-S. The UV bright galaxies are in general larger than normal field galaxies at the same mass. ...
... in narrow mass bins for all galaxies from CDF-S. The UV bright galaxies are in general larger than normal field galaxies at the same mass. ...
- SkyServer
... PSF_FLUX_INTERP, SATURATED, or BAD_COUNTS_ERROR, DEBLEND_NOPEAK, or COSMIC_RAY) – Spectra available – In main galaxy sample (primTarget = GALAXY but not GALAXY_RED) ...
... PSF_FLUX_INTERP, SATURATED, or BAD_COUNTS_ERROR, DEBLEND_NOPEAK, or COSMIC_RAY) – Spectra available – In main galaxy sample (primTarget = GALAXY but not GALAXY_RED) ...
astro-ph/9704019 2 Apr 1997 - National Optical Astronomy
... using galaxies as tracers of the cosmic deceleration (Tammann 1984). Evolution was considered primarily as a necessary ‘correction’ to apply in the grander quest for the nature of the world model; the term ‘evolutionary correction’ remains (c.f. Poggianti 1997). Galaxy evolution only rose to promine ...
... using galaxies as tracers of the cosmic deceleration (Tammann 1984). Evolution was considered primarily as a necessary ‘correction’ to apply in the grander quest for the nature of the world model; the term ‘evolutionary correction’ remains (c.f. Poggianti 1997). Galaxy evolution only rose to promine ...
Power Point Presentation
... sources that you know are the same brightness The apparent brightness of the distant source will allow you to calculate its distance, compared to the nearby source This is because the brightness decreases like 1/(distance)2 March 11, 2003 ...
... sources that you know are the same brightness The apparent brightness of the distant source will allow you to calculate its distance, compared to the nearby source This is because the brightness decreases like 1/(distance)2 March 11, 2003 ...
Hints for families of gamma-ray bursts improving the Hubble diagram
... textbook example of the Cepheids variables and the estimate of the Hubble constant H0 . Indeed, the first H0 determinations based on a mixed sample of Cepheids and RR Lyrae variables were grossly wrong because of the use of the same period–luminosity relation for two radically different stellar obje ...
... textbook example of the Cepheids variables and the estimate of the Hubble constant H0 . Indeed, the first H0 determinations based on a mixed sample of Cepheids and RR Lyrae variables were grossly wrong because of the use of the same period–luminosity relation for two radically different stellar obje ...
Gamma Ray Bursts
... • in 3 years, the period of SGR 1806-20 decreases by 0.008s • reason – magnetic field calculated to be 1011 T ! • magnetar – neutron star withmagnetic field of ~1011 T ...
... • in 3 years, the period of SGR 1806-20 decreases by 0.008s • reason – magnetic field calculated to be 1011 T ! • magnetar – neutron star withmagnetic field of ~1011 T ...
Post Common Envelope Binaries from SDSS. I: 101 white dwarf
... and Eisenstein et al. (2006), as well as a set of WDMS independently found in the SDSS data by our team. This search resulted in a sample of 130 WDMS with two to seven SDSS spectra. Among those WDMS, 101 systems have a clearly pronounced Na I λλ 8183.27,8194.81 absorption doublet and/or Hα emission ...
... and Eisenstein et al. (2006), as well as a set of WDMS independently found in the SDSS data by our team. This search resulted in a sample of 130 WDMS with two to seven SDSS spectra. Among those WDMS, 101 systems have a clearly pronounced Na I λλ 8183.27,8194.81 absorption doublet and/or Hα emission ...
Astronomy Astrophysics
... (Becklin et al. 1973), and observed simultaneously at X-ray and near-IR wavelengths by Mason et al. (1986), is believed to be the orbital period of the binary system. Following infrared spectroscopic measurements (van Kerkwijk et al. 1992), where WR-like features have been detected in I and K band s ...
... (Becklin et al. 1973), and observed simultaneously at X-ray and near-IR wavelengths by Mason et al. (1986), is believed to be the orbital period of the binary system. Following infrared spectroscopic measurements (van Kerkwijk et al. 1992), where WR-like features have been detected in I and K band s ...
PPT presentation
... framework, to be compared with future PNe observations AND other dynamical tracers (GCs, Xrays, lensing). Thanks to the PN.S statistical samples of PN radial velocities are reaching the precision which will allow to discriminate the efficiency of the baryon cooling in galaxies. We have shown on a sa ...
... framework, to be compared with future PNe observations AND other dynamical tracers (GCs, Xrays, lensing). Thanks to the PN.S statistical samples of PN radial velocities are reaching the precision which will allow to discriminate the efficiency of the baryon cooling in galaxies. We have shown on a sa ...
- Isaac Newton Group of Telescopes
... star cluster of the Pleiades, a group of stars which formed about a hundred million years ago at a distance of approximately 400 light years (3780 billion kilometers) from the Sun, is considered to be one of the most suitable astronomical sources for the detection, and the subsequent study of brown ...
... star cluster of the Pleiades, a group of stars which formed about a hundred million years ago at a distance of approximately 400 light years (3780 billion kilometers) from the Sun, is considered to be one of the most suitable astronomical sources for the detection, and the subsequent study of brown ...
The Evolution of Star Formation Activity in . Cory R. Wagner
... 2006; Clemens et al. 2009; Edwards & Fadda 2011). Studies of cluster galaxy populations to z . 1 find that the evolution in the color and scatter of cluster red-sequences is consistent with simple passive evolution models in which the bulk of galaxies’ stars formed in a short, high-redshift starburs ...
... 2006; Clemens et al. 2009; Edwards & Fadda 2011). Studies of cluster galaxy populations to z . 1 find that the evolution in the color and scatter of cluster red-sequences is consistent with simple passive evolution models in which the bulk of galaxies’ stars formed in a short, high-redshift starburs ...
arXiv:1601.01542v1 [astro-ph.GA] 7 Jan 2016
... of these regions across the galaxy surface. The advent of integral field spectroscopy (IFS) techniques offers astronomers the opportunity to overcome these limitations by tracing the distribution of ionised gas and estimating spatially resolved chemical abundances for the gas phase. Its two-dimensio ...
... of these regions across the galaxy surface. The advent of integral field spectroscopy (IFS) techniques offers astronomers the opportunity to overcome these limitations by tracing the distribution of ionised gas and estimating spatially resolved chemical abundances for the gas phase. Its two-dimensio ...
The Physical Origins of The Morphology
... the de Vaucouleurs-derived values, we note that adopting surface brightness models with a free Sérsic (1968) index does not lead to a significantly different b/a distribution. The systematic difference between the two values is only 0.004 in the median, the scatter is 0.075, and for less than 1% of ...
... the de Vaucouleurs-derived values, we note that adopting surface brightness models with a free Sérsic (1968) index does not lead to a significantly different b/a distribution. The systematic difference between the two values is only 0.004 in the median, the scatter is 0.075, and for less than 1% of ...
Chemical Composition of Selected Metal Poor Stars
... by GalaCtic chemical evolution (chemical enrichment history of our galaxy). Theories of Big Bang nucleosynthesis suggest that, it was mainly hydrogen, helium and little amount of elements upto boron which were synthesized primordially. Other metals (elements heavier than lithium) were formed from th ...
... by GalaCtic chemical evolution (chemical enrichment history of our galaxy). Theories of Big Bang nucleosynthesis suggest that, it was mainly hydrogen, helium and little amount of elements upto boron which were synthesized primordially. Other metals (elements heavier than lithium) were formed from th ...
Grand Design and Flocculent Spirals in the Spitzer Survey of Stellar
... Knapen et al. 1995; Block et al. 2004a). Flocculent spirals rarely have underlying stellar waves even in Ks -band. Weak 2-arm spirals were first found in some flocculent galaxies by Block et al. (1994), Thornley (1996), Thornley & Mundy (1997) and Elmegreen et al. (1999), and discussed by Block & Pu ...
... Knapen et al. 1995; Block et al. 2004a). Flocculent spirals rarely have underlying stellar waves even in Ks -band. Weak 2-arm spirals were first found in some flocculent galaxies by Block et al. (1994), Thornley (1996), Thornley & Mundy (1997) and Elmegreen et al. (1999), and discussed by Block & Pu ...
Spiral arm structures revealed in the M31 galaxy
... pattern is observed within the arm region where Beck et al. (1989) detected a strong regular magnetic field with the wavelength twice as large as the spacing between the complexes. Moreover, complexes are located mostly at the extremes of the wavy magnetic field. In this arm, groups of HII regions l ...
... pattern is observed within the arm region where Beck et al. (1989) detected a strong regular magnetic field with the wavelength twice as large as the spacing between the complexes. Moreover, complexes are located mostly at the extremes of the wavy magnetic field. In this arm, groups of HII regions l ...
Cosmic distance ladder
The cosmic distance ladder (also known as the extragalactic distance scale) is the succession of methods by which astronomers determine the distances to celestial objects. A real direct distance measurement of an astronomical object is possible only for those objects that are ""close enough"" (within about a thousand parsecs) to Earth. The techniques for determining distances to more distant objects are all based on various measured correlations between methods that work at close distances and methods that work at larger distances. Several methods rely on a standard candle, which is an astronomical object that has a known luminosity.The ladder analogy arises because no one technique can measure distances at all ranges encountered in astronomy. Instead, one method can be used to measure nearby distances, a second can be used to measure nearby to intermediate distances, and so on. Each rung of the ladder provides information that can be used to determine the distances at the next higher rung.