Colour-magnitude diagrams of the post
... can be considered a member. Goranskii determined a period of 0.5752 days, so that the cluster can be tentatively classified as Oosterhoff type I. 5. Conclusions Cluster parameters based on CCD photometry were derived for NGC 6256 and NGC 6717. They are both located in the bulge, but are not metal-ri ...
... can be considered a member. Goranskii determined a period of 0.5752 days, so that the cluster can be tentatively classified as Oosterhoff type I. 5. Conclusions Cluster parameters based on CCD photometry were derived for NGC 6256 and NGC 6717. They are both located in the bulge, but are not metal-ri ...
A spectroscopic investigation of the O-type star - ORBi
... Results. We confirm the binarity for four objects: HD 193443, HD 228989, HD 229234 and HD 194649. We derive for the first time the orbital solutions of three systems, and we confirm the values of the fourth, showing that these four systems all have orbital periods shorter than 10 days. Besides these ...
... Results. We confirm the binarity for four objects: HD 193443, HD 228989, HD 229234 and HD 194649. We derive for the first time the orbital solutions of three systems, and we confirm the values of the fourth, showing that these four systems all have orbital periods shorter than 10 days. Besides these ...
Conference Abstract Booklet here.
... RCB stars form a class of cool, carbon-rich supergiants that have almost no hydrogen. They undergo extreme, irregular declines in brightness of up to 8 magnitudes due to the formation of thick clouds of carbon dust. Two scenarios have been proposed for the origin of an RCB star: the merger of a CO/H ...
... RCB stars form a class of cool, carbon-rich supergiants that have almost no hydrogen. They undergo extreme, irregular declines in brightness of up to 8 magnitudes due to the formation of thick clouds of carbon dust. Two scenarios have been proposed for the origin of an RCB star: the merger of a CO/H ...
Chemical abundances and winds of massive stars in M31: a B
... et al. (1996a) investigated the extinction in M31 using the HST/FOS data for OB 10-64 and additional M31 OB stars and concluded that the 2175Å bump is weak or absent in M31. The slope of the extinction curve was consistent with the Galactic curve, but the low reddening of their M31 target stars pre ...
... et al. (1996a) investigated the extinction in M31 using the HST/FOS data for OB 10-64 and additional M31 OB stars and concluded that the 2175Å bump is weak or absent in M31. The slope of the extinction curve was consistent with the Galactic curve, but the low reddening of their M31 target stars pre ...
IXO as an observatory in the large telescopes era
... often obscured, remain largely undiscovered. Uncovering such objects at z=6-7 (and even higher redshifts) holds the key to our understanding of this crucial phase in the development of the Universe. It is very likely that SMBHs as massive as 106 M, possibly hosted by vigorously star forming galaxie ...
... often obscured, remain largely undiscovered. Uncovering such objects at z=6-7 (and even higher redshifts) holds the key to our understanding of this crucial phase in the development of the Universe. It is very likely that SMBHs as massive as 106 M, possibly hosted by vigorously star forming galaxie ...
The environment of high-redshift AGN OLIMPIA JUDIT FOGASY
... In order to understand the formation and evolution of local massive galaxies and to reveal the processes that engineered the tight correlations found between their supermassive black hole (SMBH) mass and bulge mass or velocity dispersion, the study of powerful, high-redshift active galactic nuclei ( ...
... In order to understand the formation and evolution of local massive galaxies and to reveal the processes that engineered the tight correlations found between their supermassive black hole (SMBH) mass and bulge mass or velocity dispersion, the study of powerful, high-redshift active galactic nuclei ( ...
Chapter 12
... To observe stellar parallax, astronomers take advantage of the Earth’s motion around the Sun, as shown in figure 12.2A. They observe a star and carefully measure its position against background stars. They then wait 6 months until the Earth has moved to the other side of its orbit, a known distance ...
... To observe stellar parallax, astronomers take advantage of the Earth’s motion around the Sun, as shown in figure 12.2A. They observe a star and carefully measure its position against background stars. They then wait 6 months until the Earth has moved to the other side of its orbit, a known distance ...
Ch. 20 - Astro1010
... the distances to these bright giant stars. • RR Lyrae stars all have about the same luminosity; knowing their apparent magnitude and using the inverse square law allows us to calculate the distance. • Cepheids have a luminosity that is strongly correlated with the period of their oscillations; once ...
... the distances to these bright giant stars. • RR Lyrae stars all have about the same luminosity; knowing their apparent magnitude and using the inverse square law allows us to calculate the distance. • Cepheids have a luminosity that is strongly correlated with the period of their oscillations; once ...
Luminosity, Flux and Magnitudes Outline
... stars according to their apparent brightness. He labeled 1080 stars as class 0, 1,.. 6. 0 was the brightest, 1 the next brightest, etc. ...
... stars according to their apparent brightness. He labeled 1080 stars as class 0, 1,.. 6. 0 was the brightest, 1 the next brightest, etc. ...
Carbon-enhanced metal-poor stars in dwarf galaxies
... stars in Local Group dwarf galaxies by means of a statistical, data-calibrated cosmological model for the hierarchical build-up of the Milky Way and its dwarf satellites. The model self-consistently explains the variation with dwarf galaxy luminosity of the observed: i) frequency and [Fe/H] range of ...
... stars in Local Group dwarf galaxies by means of a statistical, data-calibrated cosmological model for the hierarchical build-up of the Milky Way and its dwarf satellites. The model self-consistently explains the variation with dwarf galaxy luminosity of the observed: i) frequency and [Fe/H] range of ...
Measuring distances to the edge of the local group
... Scheduling constraints and non-usable dates (up to four lines). ...
... Scheduling constraints and non-usable dates (up to four lines). ...
PDF only - at www.arxiv.org.
... The aim of this work are to find a Kepler’s constant by using polynomial regression of the angular separation = (t) and the position angle = (t). The Kepler’s constant obtained is used to derive the elements of orbit. As a case study the angular separation and the position angle of the WDS 000 ...
... The aim of this work are to find a Kepler’s constant by using polynomial regression of the angular separation = (t) and the position angle = (t). The Kepler’s constant obtained is used to derive the elements of orbit. As a case study the angular separation and the position angle of the WDS 000 ...
Reassessing the formation of the inner Oort cloud
... In a recent publication attempting to solve some of the outstanding problems associated with the Oort cloud as a whole, Levison et al. (2010) investigated the capture by the Sun of comets from other stars. They simulated embedded clusters ranging from 30 to 300 stars with a star formation efficiency ...
... In a recent publication attempting to solve some of the outstanding problems associated with the Oort cloud as a whole, Levison et al. (2010) investigated the capture by the Sun of comets from other stars. They simulated embedded clusters ranging from 30 to 300 stars with a star formation efficiency ...
Chemical abundances and winds of massive stars in M31: a Btype
... following Fitzpatrick (1986) in using other B-type supergiants in the LMC as the comparison stars. We chose Sk-67 108 (B0 Ia) and Sk-69 276 (O9-B0Ia) as the comparison stars on the basis of the morphology of their UV spectra compared to OB 10-64. These two stars have essentially little or no interna ...
... following Fitzpatrick (1986) in using other B-type supergiants in the LMC as the comparison stars. We chose Sk-67 108 (B0 Ia) and Sk-69 276 (O9-B0Ia) as the comparison stars on the basis of the morphology of their UV spectra compared to OB 10-64. These two stars have essentially little or no interna ...
Trapezium Fracture
... trapezoidal grouping of stars within the very heart of its structure. Known to astronomers as “the trapezium” because of their relative spatial arrangement, they are very young supermassive giants, each with over 100,000 times the radiant luminosity of our own Sun. They radiate ultraviolet radiation ...
... trapezoidal grouping of stars within the very heart of its structure. Known to astronomers as “the trapezium” because of their relative spatial arrangement, they are very young supermassive giants, each with over 100,000 times the radiant luminosity of our own Sun. They radiate ultraviolet radiation ...
a wide-field survey for variable stars
... This diploma thesis will focus on the use of wide-field instrumentation and associated analysis methods in order to facilitate the discovery of new variable stars. The thesis has been organised in the following way. In Chapter one I give an introduction to the variable star nomenclature and taxonomy ...
... This diploma thesis will focus on the use of wide-field instrumentation and associated analysis methods in order to facilitate the discovery of new variable stars. The thesis has been organised in the following way. In Chapter one I give an introduction to the variable star nomenclature and taxonomy ...
Program and Abstract Book - European Southern Observatory
... Mike Dunham (SUNY Fredonia, NY, USA) Stars form from the gravitational collapse of dense molecular cloud cores. In the protostellar phase, mass both accretes from the core onto a protostar, likely through an accretion disk, and is ejected in the form of jets and outflows. It is during this protostel ...
... Mike Dunham (SUNY Fredonia, NY, USA) Stars form from the gravitational collapse of dense molecular cloud cores. In the protostellar phase, mass both accretes from the core onto a protostar, likely through an accretion disk, and is ejected in the form of jets and outflows. It is during this protostel ...
OBSERVATIONS OF PHYSICAL PROCESSES IN
... cluster galaxies (BCGs) of those clusters. It has been known for a while that the state of the hot intracluster medium (ICM) gas in the core of a galaxy cluster, quantified as the central entropy of the gas, can be found in two particular states. Galaxy clusters with central entropies greater than 3 ...
... cluster galaxies (BCGs) of those clusters. It has been known for a while that the state of the hot intracluster medium (ICM) gas in the core of a galaxy cluster, quantified as the central entropy of the gas, can be found in two particular states. Galaxy clusters with central entropies greater than 3 ...
Activity III: Calibrating Images
... Counts - The measure of light that each pixel of the CCD receives from the star. This measurement is particular to the equipment used and to the atmospheric conditions during the observation. When we display an image, the grayness or color at each pixel is based on the Counts for that pixel. Appare ...
... Counts - The measure of light that each pixel of the CCD receives from the star. This measurement is particular to the equipment used and to the atmospheric conditions during the observation. When we display an image, the grayness or color at each pixel is based on the Counts for that pixel. Appare ...
SGR 1900+14
... Giant Flares and short GRBs The two previous giant flares could have been detected Up to 8 Mpc; the recent one up to 40 Mpc Taking into account the SFR in our Galaxy, we would expect 80 such events per year to be compared with the 150 BATSE detected The isotropic distribution of short GRBs, the lac ...
... Giant Flares and short GRBs The two previous giant flares could have been detected Up to 8 Mpc; the recent one up to 40 Mpc Taking into account the SFR in our Galaxy, we would expect 80 such events per year to be compared with the 150 BATSE detected The isotropic distribution of short GRBs, the lac ...
EROs and submm galaxies: Expectations for FMOS in the
... Why FMOS is better than OHS Multiplexing Can observe targets for an entire night (or longer) ...
... Why FMOS is better than OHS Multiplexing Can observe targets for an entire night (or longer) ...
The ATLAS3D project-XXII. Low-efficiency star formation in early
... using a universal local law to form stars in the simulations, we find that the earlytype galaxies are offset from the spirals on the large-scale Kennicutt relation, and form stars two to five times less efficiently. This offset is in agreement with previous results on morphological quenching: gas di ...
... using a universal local law to form stars in the simulations, we find that the earlytype galaxies are offset from the spirals on the large-scale Kennicutt relation, and form stars two to five times less efficiently. This offset is in agreement with previous results on morphological quenching: gas di ...
The local spiral structure of the Milky Way
... main arc of the Local Arm. Instead, these sources, as well as G059.78+00.06 and ON 1, branch off and curve inward in the Milky Way. As the dotted line in Fig. 2 suggests, these sources trace what appears to be a high-inclination spur bridging the Local Arm to the Sagittarius Arm near l ≈ 50°. Additi ...
... main arc of the Local Arm. Instead, these sources, as well as G059.78+00.06 and ON 1, branch off and curve inward in the Milky Way. As the dotted line in Fig. 2 suggests, these sources trace what appears to be a high-inclination spur bridging the Local Arm to the Sagittarius Arm near l ≈ 50°. Additi ...
CPW Science Passage
... Two students discuss the evolution of the Algol system – Algol A, a 3.6-solar-mass MS star; Algol B, a 0.8-solar-mass post-MS star; and Algol C, a 1.7-solar-mass MS star. (One solar mass = the Sun’s mass.) The 3 stars orbit a mutual center of mass, with Algol A and Algol B much closer to each other ...
... Two students discuss the evolution of the Algol system – Algol A, a 3.6-solar-mass MS star; Algol B, a 0.8-solar-mass post-MS star; and Algol C, a 1.7-solar-mass MS star. (One solar mass = the Sun’s mass.) The 3 stars orbit a mutual center of mass, with Algol A and Algol B much closer to each other ...
Spectral Line VLBI - Australia Telescope National Facility
... • The maser components are extremely small (mas) and narrow (fractions of a km/s) Measure position and velocity of components with great accuracy ...
... • The maser components are extremely small (mas) and narrow (fractions of a km/s) Measure position and velocity of components with great accuracy ...
Serpens
Serpens (""the Serpent"", Greek Ὄφις) is a constellation of the northern hemisphere. One of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations defined by the International Astronomical Union. It is unique among the modern constellations in being split into two non-contiguous parts, Serpens Caput (Serpent's Head) to the west and Serpens Cauda (Serpent's Tail) to the east. Between these two halves lies the constellation of Ophiuchus, the ""Serpent-Bearer"". In figurative representations, the body of the serpent is represented as passing behind Ophiuchus between Mu Serpentis in Serpens Caput and Nu Serpentis in Serpens Cauda.The brightest star in Serpens is the red giant star Alpha Serpentis, or Unukalhai, in Serpens Caput, with an apparent magnitude of 2.63. Also located in Serpens Caput are the naked-eye globular cluster Messier 5 and the naked-eye variables R Serpentis and Tau4 Serpentis. Notable extragalactic objects include Seyfert's Sextet, one of the densest galaxy clusters known; Arp 220, the prototypical ultraluminous infrared galaxy; and Hoag's Object, the most famous of the very rare class of galaxies known as ring galaxies.Part of the Milky Way's galactic plane passes through Serpens Cauda, which is therefore rich in galactic deep-sky objects, such as the Eagle Nebula (IC 4703) and its associated star cluster Messier 16. The nebula measures 70 light-years by 50 light-years and contains the Pillars of Creation, three dust clouds that became famous for the image taken by the Hubble Space Telescope. Other striking objects include the Red Square Nebula, one of the few objects in astronomy to take on a square shape; and Westerhout 40, a massive nearby star-forming region consisting of a molecular cloud and an H II region.