Astronomy Astrophysics Circumstellar emission in Be/X-ray binaries of the Magellanic
... Our main goals are exploring whether previously published relations, valid for isolated Be stars, are applicable to Be/X-ray binaries and computing the distance to these systems after correcting for the effects of the circumstellar contamination. Methods. Simultaneous U BVRI photometry and spectra in ...
... Our main goals are exploring whether previously published relations, valid for isolated Be stars, are applicable to Be/X-ray binaries and computing the distance to these systems after correcting for the effects of the circumstellar contamination. Methods. Simultaneous U BVRI photometry and spectra in ...
A new view of galaxy evolution
... relaxation over a relatively quick timescale. However, the question remains as to how and why these galaxies look the way they do in the distant universe; specifically, we need to understand how they got distorted in the first place. Furthermore, kinematic studies of these galaxies show that they of ...
... relaxation over a relatively quick timescale. However, the question remains as to how and why these galaxies look the way they do in the distant universe; specifically, we need to understand how they got distorted in the first place. Furthermore, kinematic studies of these galaxies show that they of ...
The Jansky Very Large Array – New Capabilities, New Science
... • Three of the four prior examples employed mm (PdBI) interferometer observations as well as VLA. • The rise of ALMA will strengthen this complementarity, with stellar scientific results. • New example – Wagg and Carilli combine VLA and ALMA for early forming galaxies: – Massive galaxies at z~2 must ...
... • Three of the four prior examples employed mm (PdBI) interferometer observations as well as VLA. • The rise of ALMA will strengthen this complementarity, with stellar scientific results. • New example – Wagg and Carilli combine VLA and ALMA for early forming galaxies: – Massive galaxies at z~2 must ...
– 1 – 1. Emission Lines in Nearby Galaxies 1.1.
... All these diagnostics were developed for HII regions and have been under development and use for decades. For z > 1.2 most of the relevant lines have shifted from the optical into the near-IR, where it is much harder to obtain the necessary data for these faint sources. Development of new metrics fo ...
... All these diagnostics were developed for HII regions and have been under development and use for decades. For z > 1.2 most of the relevant lines have shifted from the optical into the near-IR, where it is much harder to obtain the necessary data for these faint sources. Development of new metrics fo ...
The cosmological significance of high
... We have used new and archival infrared and radio observations to search for a dwarf galaxy associated with the high-velocity cloud (HVC) known as Complex H. Complex H is a large (Ω & 400 deg2 ) and probably nearby (d = 27 kpc) HVC whose location in the Galactic plane has hampered previous investigat ...
... We have used new and archival infrared and radio observations to search for a dwarf galaxy associated with the high-velocity cloud (HVC) known as Complex H. Complex H is a large (Ω & 400 deg2 ) and probably nearby (d = 27 kpc) HVC whose location in the Galactic plane has hampered previous investigat ...
Introduction to Observational Cosmology
... – For compact or unresolved objects surveys are flux-limited (separate flux limit in each observational band). – For extended objects surveys are surface brightness limited (i.e. limited by the contrast to the background) ...
... – For compact or unresolved objects surveys are flux-limited (separate flux limit in each observational band). – For extended objects surveys are surface brightness limited (i.e. limited by the contrast to the background) ...
Slide 1
... are close by (because of lower energy scales), hence associated with bright galaxies. 2: SGRs should produce periodic tail following the giant bursts ...
... are close by (because of lower energy scales), hence associated with bright galaxies. 2: SGRs should produce periodic tail following the giant bursts ...
exploring fundamental physics with neutron stars
... neutron stars, broadly distinguished by the source that power they emission (for a review, see Ref. [3-c]): rotational kinetic energy (RPPs), thermal energy (INSs and CCOs), magnetic field energy (magnetars), accretion from a companion star (X-ray binary pulsars). Although the normal RPPs constitute ...
... neutron stars, broadly distinguished by the source that power they emission (for a review, see Ref. [3-c]): rotational kinetic energy (RPPs), thermal energy (INSs and CCOs), magnetic field energy (magnetars), accretion from a companion star (X-ray binary pulsars). Although the normal RPPs constitute ...
EXPLORING FUNDAMENTAL PHYSICS WITH NEUTRON STARS
... neutron stars, broadly distinguished by the source that power they emission (for a review, see Ref. [3-c]): rotational kinetic energy (RPPs), thermal energy (INSs and CCOs), magnetic field energy (magnetars), accretion from a companion star (X-ray binary pulsars). Although the normal RPPs constitute ...
... neutron stars, broadly distinguished by the source that power they emission (for a review, see Ref. [3-c]): rotational kinetic energy (RPPs), thermal energy (INSs and CCOs), magnetic field energy (magnetars), accretion from a companion star (X-ray binary pulsars). Although the normal RPPs constitute ...
Introduction
... fraction of quenched late-type galaxies are, however, not gas deficient, and form a more heterogeneous class of objects with probably more complex evolutionary histories. In contrast to the case of star formation, the chemical evolution of star-forming galaxies, as traced by the stellar mass-metalli ...
... fraction of quenched late-type galaxies are, however, not gas deficient, and form a more heterogeneous class of objects with probably more complex evolutionary histories. In contrast to the case of star formation, the chemical evolution of star-forming galaxies, as traced by the stellar mass-metalli ...
ROTATION CURVES OF HIGH-LUMINOSITY SPIRAL GALAXIES
... Downloaded from https:/www.cambridge.org/core. IP address: 88.99.165.207, on 16 Jun 2017 at 01:43:40, subject to the Cambridge Core terms of use, available at https:/www.cambridge.org/core/terms. https://doi.org/10.1017/S0074180900014492 ...
... Downloaded from https:/www.cambridge.org/core. IP address: 88.99.165.207, on 16 Jun 2017 at 01:43:40, subject to the Cambridge Core terms of use, available at https:/www.cambridge.org/core/terms. https://doi.org/10.1017/S0074180900014492 ...
ULXs: General Properties and Variability - X
... •evidence against beaming (QPOs, broad Fe Lines, eclipses) •At least one object has a break in the PDS at the frequency predicted for M~1000M objects •Associated extended radio sources •General lack of optical Ids (massive stars would be seen) •they lie near, but not in star forming regions Kyoto me ...
... •evidence against beaming (QPOs, broad Fe Lines, eclipses) •At least one object has a break in the PDS at the frequency predicted for M~1000M objects •Associated extended radio sources •General lack of optical Ids (massive stars would be seen) •they lie near, but not in star forming regions Kyoto me ...
Lab 14 Galaxy Morphology
... appeared similar to comets, but did not move. Others of these nebulae were resolved into clusters of stars as bigger telescopes were constructed, and used to examine them. Some of these fuzzy nebulae, however, did not break-up into stars no matter how big a telescope was used to look at them. While ...
... appeared similar to comets, but did not move. Others of these nebulae were resolved into clusters of stars as bigger telescopes were constructed, and used to examine them. Some of these fuzzy nebulae, however, did not break-up into stars no matter how big a telescope was used to look at them. While ...
Star formation in a galactic outflow
... the spheroidal component of galaxies11,13, and would contribute to the population of highvelocity stars, which could even escape the galaxy13. Such star formation could provide in-situ chemical enrichment of the circumgalactic and intergalactic medium (through supernova explosions of young stars on ...
... the spheroidal component of galaxies11,13, and would contribute to the population of highvelocity stars, which could even escape the galaxy13. Such star formation could provide in-situ chemical enrichment of the circumgalactic and intergalactic medium (through supernova explosions of young stars on ...
Evolution of galaxy morphology - Lecture 1 - NCRA-TIFR
... Where e refers to effective values and n is the Sérsic index. For n=4 it becomes the de Vaucouleurs function; for n=1 an exponential, and when n=0.5, a Gaussian! For values in the range 1-4, approximately, it describes bulges in late-type spiral galaxies (or pseudo-bulges) to bulges in early-type sp ...
... Where e refers to effective values and n is the Sérsic index. For n=4 it becomes the de Vaucouleurs function; for n=1 an exponential, and when n=0.5, a Gaussian! For values in the range 1-4, approximately, it describes bulges in late-type spiral galaxies (or pseudo-bulges) to bulges in early-type sp ...
3.1 Radio Astronomy Research Results For much of PY 2010, radio
... (Martin et al., 2010, ApJ 723, 1359). Fig. 3.4 compares the HI mass functions derived by ALFALFA (solid blue curve) and HIPASS (dashed red curve: Zwaan et al. 2005 MNRAS 359, L30). Also evident from Fig. 3.3, ALFALFA samples HI masses over a significantly larger dynamic range and a much larger volum ...
... (Martin et al., 2010, ApJ 723, 1359). Fig. 3.4 compares the HI mass functions derived by ALFALFA (solid blue curve) and HIPASS (dashed red curve: Zwaan et al. 2005 MNRAS 359, L30). Also evident from Fig. 3.3, ALFALFA samples HI masses over a significantly larger dynamic range and a much larger volum ...
Gamma-Ray Pulsars - INTEGRAL
... et al.,1975; COS-B, Mayer-Hasselwander et al., 1982) are dominated by the sources now known as the young pulsars Crab, Vela and Geminga. Unlike in any other waveband these young pulsars outshine other sources at energies above 100 MeV. The sky survey performed with the Compton Gamma-Ray Observatory ...
... et al.,1975; COS-B, Mayer-Hasselwander et al., 1982) are dominated by the sources now known as the young pulsars Crab, Vela and Geminga. Unlike in any other waveband these young pulsars outshine other sources at energies above 100 MeV. The sky survey performed with the Compton Gamma-Ray Observatory ...
Ch 11a (Measuring Stars 10-28-10)
... Distance: If you know the parallax “p” (in arcseconds) you can calculate the distance “d” (in parsecs) d=1/p (1parsec= 3.26 lightyears) Apparent brightness: how bright a star looks in the sky The inverse-square Law: light from stars gets fainter as the inverse square of the distance (apparent bri ...
... Distance: If you know the parallax “p” (in arcseconds) you can calculate the distance “d” (in parsecs) d=1/p (1parsec= 3.26 lightyears) Apparent brightness: how bright a star looks in the sky The inverse-square Law: light from stars gets fainter as the inverse square of the distance (apparent bri ...
8-4.9 - S2TEM Centers SC
... ecliptic, they are not normally in alignment with each other because their orbital velocities and orbital periods vary.) Planets cannot be seen with the naked eye. The earth is the center of the solar system. (The planets, sun and moon revolve around the earth.) The solar system contains only ...
... ecliptic, they are not normally in alignment with each other because their orbital velocities and orbital periods vary.) Planets cannot be seen with the naked eye. The earth is the center of the solar system. (The planets, sun and moon revolve around the earth.) The solar system contains only ...
Galaxy Evolution
... masses per year or M yr−1 (this is the total stellar mass, not the number, of new stars). The STELLAR MASSES of freshly produced stars are not all equal, but vary approximately between 100 solar masses to about one tenth of solar mass (i.e. stars whose mass is between one hundred times and one tent ...
... masses per year or M yr−1 (this is the total stellar mass, not the number, of new stars). The STELLAR MASSES of freshly produced stars are not all equal, but vary approximately between 100 solar masses to about one tenth of solar mass (i.e. stars whose mass is between one hundred times and one tent ...
Galaxy Evolution Encyclopedia of Astronomy & Astrophysics eaa.iop.org Mauro Giavalisco
... masses per year or M yr−1 (this is the total stellar mass, not the number, of new stars). The STELLAR MASSES of freshly produced stars are not all equal, but vary approximately between 100 solar masses to about one tenth of solar mass (i.e. stars whose mass is between one hundred times and one tent ...
... masses per year or M yr−1 (this is the total stellar mass, not the number, of new stars). The STELLAR MASSES of freshly produced stars are not all equal, but vary approximately between 100 solar masses to about one tenth of solar mass (i.e. stars whose mass is between one hundred times and one tent ...
POSTERS SESSION I: Atmospheres of Massive Stars
... Independently of the possibility of internally generated fields, there are good reasons to believe that massive stars actually harbour significant magnetic fields of fossil origin. As the ISM itself possesses organized, largescale magnetic fields, it is unavoidable because of magnetic flux conservat ...
... Independently of the possibility of internally generated fields, there are good reasons to believe that massive stars actually harbour significant magnetic fields of fossil origin. As the ISM itself possesses organized, largescale magnetic fields, it is unavoidable because of magnetic flux conservat ...
WORD - Astrophysics
... “dark matter”. The only component that directly retains observable information about star formation rates and metal enrichment rates - the evolution of the baryonic component - is the stellar population. This is because low mass stars have extremely long life times, comparable to the age of the Univ ...
... “dark matter”. The only component that directly retains observable information about star formation rates and metal enrichment rates - the evolution of the baryonic component - is the stellar population. This is because low mass stars have extremely long life times, comparable to the age of the Univ ...
Indications for an influence of Hot Jupiters
... is slightly lower than the typical X-ray luminosities found for main sequence field stars of spectral type F and G, (log LX = 28.05[27.12, 28.98] erg s−1 , Schmitt & Liefke (2004)). Its Xray emission therefore suggest an age of ca. 5 Gyr or more. This is consistent with the observation that υ And A ...
... is slightly lower than the typical X-ray luminosities found for main sequence field stars of spectral type F and G, (log LX = 28.05[27.12, 28.98] erg s−1 , Schmitt & Liefke (2004)). Its Xray emission therefore suggest an age of ca. 5 Gyr or more. This is consistent with the observation that υ And A ...
Gamma-ray burst
Gamma-ray bursts (GRBs) are flashes of gamma rays associated with extremely energetic explosions that have been observed in distant galaxies. They are the brightest electromagnetic events known to occur in the universe. Bursts can last from ten milliseconds to several hours. The initial burst is usually followed by a longer-lived ""afterglow"" emitted at longer wavelengths (X-ray, ultraviolet, optical, infrared, microwave and radio).Most observed GRBs are believed to consist of a narrow beam of intense radiation released during a supernova or hypernova as a rapidly rotating, high-mass star collapses to form a neutron star, quark star, or black hole. A subclass of GRBs (the ""short"" bursts) appear to originate from a different process – this may be due to the merger of binary neutron stars. The cause of the precursor burst observed in some of these short events may be due to the development of a resonance between the crust and core of such stars as a result of the massive tidal forces experienced in the seconds leading up to their collision, causing the entire crust of the star to shatter.The sources of most GRBs are billions of light years away from Earth, implying that the explosions are both extremely energetic (a typical burst releases as much energy in a few seconds as the Sun will in its entire 10-billion-year lifetime) and extremely rare (a few per galaxy per million years). All observed GRBs have originated from outside the Milky Way galaxy, although a related class of phenomena, soft gamma repeater flares, are associated with magnetars within the Milky Way. It has been hypothesized that a gamma-ray burst in the Milky Way, pointing directly towards the Earth, could cause a mass extinction event.GRBs were first detected in 1967 by the Vela satellites, a series of satellites designed to detect covert nuclear weapons tests. Hundreds of theoretical models were proposed to explain these bursts in the years following their discovery, such as collisions between comets and neutron stars. Little information was available to verify these models until the 1997 detection of the first X-ray and optical afterglows and direct measurement of their redshifts using optical spectroscopy, and thus their distances and energy outputs. These discoveries, and subsequent studies of the galaxies and supernovae associated with the bursts, clarified the distance and luminosity of GRBs. These facts definitively placed them in distant galaxies and also connected long GRBs with the explosion of massive stars, the only possible source for the energy outputs observed.