Radio pulsars
... • Optimised for MSPs: tobs = 4 min, tsamp = 125 ms. • 14 pulsars discovered so far, including 4 MSPs ...
... • Optimised for MSPs: tobs = 4 min, tsamp = 125 ms. • 14 pulsars discovered so far, including 4 MSPs ...
21 -26 August University of Exeter
... Title: Theory review Abstract: Molecular clouds condense out of the warm interstellar medium (ISM) on scales of several 100 pc and host filamentary substructures on sub-pc scales. Furthermore, molecular clouds (MCs) consist of molecular hydrogen (H2), which can only be traced indirectly in observati ...
... Title: Theory review Abstract: Molecular clouds condense out of the warm interstellar medium (ISM) on scales of several 100 pc and host filamentary substructures on sub-pc scales. Furthermore, molecular clouds (MCs) consist of molecular hydrogen (H2), which can only be traced indirectly in observati ...
Hunting for Substructure in the Milky Way
... the surrounding stars. This means that the angular momentum is predominantly in the direction of the North Galactic Pole. In order to conserve angular momentum, over time this orbit remains approximately circular. Astronomers measure the velocity and distances of stars to analyse the angular momentu ...
... the surrounding stars. This means that the angular momentum is predominantly in the direction of the North Galactic Pole. In order to conserve angular momentum, over time this orbit remains approximately circular. Astronomers measure the velocity and distances of stars to analyse the angular momentu ...
The Milky Way`s external disc constrained by 2MASS star counts
... with simulated star counts obtained with the simulations from the Galaxy model (middle panel). The difference is shown in the bottom panel. In addition to the overestimate of the warp slope, it appears that the modelled density of stars is too high at |l| 80◦ probably due to the value of the scale ...
... with simulated star counts obtained with the simulations from the Galaxy model (middle panel). The difference is shown in the bottom panel. In addition to the overestimate of the warp slope, it appears that the modelled density of stars is too high at |l| 80◦ probably due to the value of the scale ...
on the pms star hbc 498 and its associated nebulous stars1
... Assigned assuming luminosity class V. b Has an emission reversal in c d its core. Variable, see Fig. 2 and text for details. Spectrogram with low S/N ratio ≤ 9 at 6400 Å. ...
... Assigned assuming luminosity class V. b Has an emission reversal in c d its core. Variable, see Fig. 2 and text for details. Spectrogram with low S/N ratio ≤ 9 at 6400 Å. ...
SPIRAL STRUCTURE IN THE OUTER GALACTIC
... According to the age and the places where they are located, clusters present a variety of challenges in deriving their intrinsic parameters. In the case of very young clusters, they are normally close to the Galactic plane where interstellar absorption and crowded stellar fields make membership assi ...
... According to the age and the places where they are located, clusters present a variety of challenges in deriving their intrinsic parameters. In the case of very young clusters, they are normally close to the Galactic plane where interstellar absorption and crowded stellar fields make membership assi ...
thick disk - asteroSTEP
... disk stars that are the debris of common dispersed star-forming aggregates. Chemical tagging will work if • stars form in large aggregates - believed to be true • aggregates are chemically homogenous • aggregates have unique chemical signatures defined by several elements which do not vary in lockst ...
... disk stars that are the debris of common dispersed star-forming aggregates. Chemical tagging will work if • stars form in large aggregates - believed to be true • aggregates are chemically homogenous • aggregates have unique chemical signatures defined by several elements which do not vary in lockst ...
bode elert johann
... astronomy Johann Elert Bode (1747–1826) had presented them as early as 1776.11 The numbers are contained in the Sammlung Astronomischer Tafeln, a three-volume collection of astronomical tables, made in partnership with Johann Heinrich Lambert and Johann Karl Gottlieb Schulze. Vol. i contains an 89-p ...
... astronomy Johann Elert Bode (1747–1826) had presented them as early as 1776.11 The numbers are contained in the Sammlung Astronomischer Tafeln, a three-volume collection of astronomical tables, made in partnership with Johann Heinrich Lambert and Johann Karl Gottlieb Schulze. Vol. i contains an 89-p ...
Gamma Ray Bursts (GRB)
... Gamma-ray bursts - short-lived bursts of gamma ray photons, the most energetic form of light. At least some of them are associated with a special type of supernova, the explosions marking the deaths of especially massive stars. ...
... Gamma-ray bursts - short-lived bursts of gamma ray photons, the most energetic form of light. At least some of them are associated with a special type of supernova, the explosions marking the deaths of especially massive stars. ...
IRAM Annual Report 2011
... detection of the [NII] 205 μm. The line shows comparable blue and red components, with a strikingly broad blue component, suggesting strong ionized gas flows. The system, even when the amplification factor is taken into account, is hyper-luminous (>1013 L⊙, or 2-3 orders of magnitude more than the M ...
... detection of the [NII] 205 μm. The line shows comparable blue and red components, with a strikingly broad blue component, suggesting strong ionized gas flows. The system, even when the amplification factor is taken into account, is hyper-luminous (>1013 L⊙, or 2-3 orders of magnitude more than the M ...
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 ...
Classification of Variable Stars
... No hydrogen, metallic anhydrides, alkali metals Methane Neutral metals, carbon Zirconium Oxide, neutral metal lines, Yttrium, Barium ...
... No hydrogen, metallic anhydrides, alkali metals Methane Neutral metals, carbon Zirconium Oxide, neutral metal lines, Yttrium, Barium ...
book_text4
... (ESO) near Munich in Germany, this work benefits greatly from the unique scientific environment that ESO provides. He started doing this in 1985, more than 5 years before launch and so has been involved in this huge project for quite a while. During the latter part of this period, Bob served on NASA ...
... (ESO) near Munich in Germany, this work benefits greatly from the unique scientific environment that ESO provides. He started doing this in 1985, more than 5 years before launch and so has been involved in this huge project for quite a while. During the latter part of this period, Bob served on NASA ...
Mapping of the extinction in giant molecular clouds using optical star
... between m − 1/2 and m + 1/2) in each cell of a regular rectangular grid in an obscured area and to compare the result with the counts obtained in a supposedly unextinguished region. In order to improve the spatial resolution, Bok (1956) proposed to make count up to the completeness limiting magnitud ...
... between m − 1/2 and m + 1/2) in each cell of a regular rectangular grid in an obscured area and to compare the result with the counts obtained in a supposedly unextinguished region. In order to improve the spatial resolution, Bok (1956) proposed to make count up to the completeness limiting magnitud ...
Observations of Jets and Outflows from Young Stars
... into a jet, with a velocity several times the escape-speed from the launch region, which can range from 100 to over 500 km s−1 . Internal shocks form where faster ejecta overrun slower material. The very fastest shocks can sometimes be detected in X-rays. These primary flows often contain molecules ...
... into a jet, with a velocity several times the escape-speed from the launch region, which can range from 100 to over 500 km s−1 . Internal shocks form where faster ejecta overrun slower material. The very fastest shocks can sometimes be detected in X-rays. These primary flows often contain molecules ...
83-98
... The presence of a largescale radial abundance gradient in the disc of our Galaxy is fairly well established from the observations of Η II regions, planetary nebulae and stellar atmospheres. In addition to this global variation, abundance variations across individual spiral features are also observed ...
... The presence of a largescale radial abundance gradient in the disc of our Galaxy is fairly well established from the observations of Η II regions, planetary nebulae and stellar atmospheres. In addition to this global variation, abundance variations across individual spiral features are also observed ...
Binarity in carbon-enhanced metal-poor stars
... CEMP-no stars that additionally have [Fe/H] < −3.0, with one exception (CS 22878−027). We note that 53327-2044-515 will have an upper limit of [Ba/Fe] < +0.34 if the star is on the main sequence and thus might or might not qualify the restrictions for CEMP-no stars. In addition to this sample, we ta ...
... CEMP-no stars that additionally have [Fe/H] < −3.0, with one exception (CS 22878−027). We note that 53327-2044-515 will have an upper limit of [Ba/Fe] < +0.34 if the star is on the main sequence and thus might or might not qualify the restrictions for CEMP-no stars. In addition to this sample, we ta ...
Hot subdwarf stars-galactic orbits and distribution perpendicular to
... The hotter subdwarf B (sdB) stars form a well defined group. Their luminosity is of the order of 10 L⊙ and their surface temperatures are roughly between 2 104 and 3 104 K. The age of the sdB stars does not follow from the stellar properties. The abundance of metals in subdwarf star atmospheres is p ...
... The hotter subdwarf B (sdB) stars form a well defined group. Their luminosity is of the order of 10 L⊙ and their surface temperatures are roughly between 2 104 and 3 104 K. The age of the sdB stars does not follow from the stellar properties. The abundance of metals in subdwarf star atmospheres is p ...
Gamma-Ray Bursts and Puzzles of Core
... by other authors (HST, VLT). For the galaxy GRB 991208 first measurement of z = 0.706 and R = 24.35 were made at the BTA. Points show location of HDF galaxies from results of deep observations with the Hubble Space Telescope (HST), i.e. the diagram shows stellar magnitudes in the filter HDF F606W an ...
... by other authors (HST, VLT). For the galaxy GRB 991208 first measurement of z = 0.706 and R = 24.35 were made at the BTA. Points show location of HDF galaxies from results of deep observations with the Hubble Space Telescope (HST), i.e. the diagram shows stellar magnitudes in the filter HDF F606W an ...
Preliminary Talk Abstract Book - MoCA
... galaxy growth. I will present the results of theoretical models for the joint evolution of mass, size and velocity dispersion of ETGs in a LambdaCDM universe, based on cosmological and binary-merging N-body simulations. Models and observations are consistent at 0 < z < 2, while there is tension at z ...
... galaxy growth. I will present the results of theoretical models for the joint evolution of mass, size and velocity dispersion of ETGs in a LambdaCDM universe, based on cosmological and binary-merging N-body simulations. Models and observations are consistent at 0 < z < 2, while there is tension at z ...
Gamma Ray Bursts
... • all in our Galaxy • all at SN remnants ~10 000 years old • X-ray oscillations found with ~8s period Puzzle solved in 1998 • 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 ...
... • all in our Galaxy • all at SN remnants ~10 000 years old • X-ray oscillations found with ~8s period Puzzle solved in 1998 • 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 ...
2. The X-ray-Radio correlation for bulgeless galaxies
... the same regardless of the distance of the objects, so the luminosity limit is defined solely by the redshifts.......................................................................................................43 Table 2: Sensitivity limits for both C-COSMOS and VLA-COSMOS surveys. The flux sensi ...
... the same regardless of the distance of the objects, so the luminosity limit is defined solely by the redshifts.......................................................................................................43 Table 2: Sensitivity limits for both C-COSMOS and VLA-COSMOS surveys. The flux sensi ...
- National Optical Astronomy Observatory
... Because the nickel particles are not ionized, their velocities would not correspond to the magnetic field lines unless there was an indirect mechanism for their flow, namely, other materials that are directed by the magnetic field. The data seems to indicate that the mechanism for the nickel’s movem ...
... Because the nickel particles are not ionized, their velocities would not correspond to the magnetic field lines unless there was an indirect mechanism for their flow, namely, other materials that are directed by the magnetic field. The data seems to indicate that the mechanism for the nickel’s movem ...
Zapartas_deMink_Izzard_AA_2017
... Most massive stars, the progenitors of core-collapse supernovae, are in close binary systems and may interact with their companion through mass transfer or merging. We undertake a population synthesis study to compute the delay-time distribution of core-collapse supernovae, that is, the supernova ra ...
... Most massive stars, the progenitors of core-collapse supernovae, are in close binary systems and may interact with their companion through mass transfer or merging. We undertake a population synthesis study to compute the delay-time distribution of core-collapse supernovae, that is, the supernova ra ...
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.