A Smile in the Sky
... t has just stopped raining. The air is still wet. The late afternoon sun comes out behind you. As you look to the horizon, you see an arc of many colors—a rainbow. Has anything, in the sky or on Earth, captured the human imagination more than a rainbow? Yet you can produce this ethereal phenomenon a ...
... t has just stopped raining. The air is still wet. The late afternoon sun comes out behind you. As you look to the horizon, you see an arc of many colors—a rainbow. Has anything, in the sky or on Earth, captured the human imagination more than a rainbow? Yet you can produce this ethereal phenomenon a ...
Research paper
... Deutsches SOFIA Institut (DSI) University of Stuttgart, Pfaffenwaldring 29, 70569, Germany ...
... Deutsches SOFIA Institut (DSI) University of Stuttgart, Pfaffenwaldring 29, 70569, Germany ...
Pulsars - Arecibo Observatory
... Tests of gravitation... Five Keplerian parameters can normally be measured from fitting the velocity (or, preferably, the delay) curves: orbital period ( Pb), projected size of the orbit, in light seconds (x), eccentricity (e), longitude of periastron (ω) and time of passage through periastron (T0). ...
... Tests of gravitation... Five Keplerian parameters can normally be measured from fitting the velocity (or, preferably, the delay) curves: orbital period ( Pb), projected size of the orbit, in light seconds (x), eccentricity (e), longitude of periastron (ω) and time of passage through periastron (T0). ...
Constraining the Envelope Structure of L1527 IRS
... to the large, bright cavities, the most striking features are the ‘neck’ and absorption lane between the reflection nebulae. The absorption lane is clearly shown in the Ks-band image (Fig. 2), having a width of ∼1000 (1500 AU). The ‘neck’ becomes apparent in the IRAC images as a thin strip of emissi ...
... to the large, bright cavities, the most striking features are the ‘neck’ and absorption lane between the reflection nebulae. The absorption lane is clearly shown in the Ks-band image (Fig. 2), having a width of ∼1000 (1500 AU). The ‘neck’ becomes apparent in the IRAC images as a thin strip of emissi ...
CONTENTS - The Institute of Mathematical Sciences
... This Institute of Mathematical Sciences Report contains the proceedings of the XVIII Conference of the Indian Association for General Relativity and Gravitation (IAGRG), held during February 15-17, 1996. The conference was attended by over 50 participants from all over the country, about half of the ...
... This Institute of Mathematical Sciences Report contains the proceedings of the XVIII Conference of the Indian Association for General Relativity and Gravitation (IAGRG), held during February 15-17, 1996. The conference was attended by over 50 participants from all over the country, about half of the ...
The Properties of Super Star Clusters in A Sample of
... Kobulnicky. With another nod to serendipity, it was my first interaction with Chip (I needed to use one of his published images in a talk) which led us to discover “ultradense HII regions”. These objects form a major part of this thesis and have led to numerous other opportunities for which I am gra ...
... Kobulnicky. With another nod to serendipity, it was my first interaction with Chip (I needed to use one of his published images in a talk) which led us to discover “ultradense HII regions”. These objects form a major part of this thesis and have led to numerous other opportunities for which I am gra ...
distribution and properties of a sample of massive young stars
... the source velocities in conjunction with a Galactic rotation model (e.g. Clemens 1985; Alvarez, May & Bronfman 1990; Brand & Blitz 1993). However, for sources located within the solar circle (Galactocentric radii <8.5 kpc) there are two possible kinematic distances for any given velocity, equally s ...
... the source velocities in conjunction with a Galactic rotation model (e.g. Clemens 1985; Alvarez, May & Bronfman 1990; Brand & Blitz 1993). However, for sources located within the solar circle (Galactocentric radii <8.5 kpc) there are two possible kinematic distances for any given velocity, equally s ...
Current astrometric surveys
... – Ground-based parallax errors can be as low as 0.25 mas, almost as accurate as HST FGS which are about 0.20 mas. • Beware of relying on very large “root n” • N > 100: systematic errors may dominate ...
... – Ground-based parallax errors can be as low as 0.25 mas, almost as accurate as HST FGS which are about 0.20 mas. • Beware of relying on very large “root n” • N > 100: systematic errors may dominate ...
G020007-00 - LIGO dcc - LIGO Scientific Collaboration
... First observed during the solar eclipse of 1919 by Sir Arthur Eddington, when the Sun was silhouetted against the Hyades star cluster ...
... First observed during the solar eclipse of 1919 by Sir Arthur Eddington, when the Sun was silhouetted against the Hyades star cluster ...
A Second Shell in the Fornax dSph Galaxy
... 1998) and proper motion measurements indicate it is on a polar orbit with a small eccentricity (e = 0.27) and is currently at perigalacticon (Dinescu et al. 2004). Moreover, Fornax contains a mass larger than all the other Galactic dSphs combined (excluding Sagittarius), which further precludes the ...
... 1998) and proper motion measurements indicate it is on a polar orbit with a small eccentricity (e = 0.27) and is currently at perigalacticon (Dinescu et al. 2004). Moreover, Fornax contains a mass larger than all the other Galactic dSphs combined (excluding Sagittarius), which further precludes the ...
Investigating the Spectral Energy Distribution TARA JILL PARKIN
... insight into the star formation history of a galaxy. A galaxy with a high metallicity would imply that several generations of stars are present, meaning it is at a later stage in its evolution. A galaxy with a low metallicity would be at a younger stage of evolution, with fewer generations of stars ...
... insight into the star formation history of a galaxy. A galaxy with a high metallicity would imply that several generations of stars are present, meaning it is at a later stage in its evolution. A galaxy with a low metallicity would be at a younger stage of evolution, with fewer generations of stars ...
systems - Research in Astronomy and Astrophysics
... discovered by the UCLA and MPE groups in 2002, when adaptive optics instruments became available. Since the bright short-period star S0-2 was going through closest approach at that time, the two sources were blended and the measurements were somewhat ambiguous. A year later, S0-2 was sufficiently fa ...
... discovered by the UCLA and MPE groups in 2002, when adaptive optics instruments became available. Since the bright short-period star S0-2 was going through closest approach at that time, the two sources were blended and the measurements were somewhat ambiguous. A year later, S0-2 was sufficiently fa ...
Extragalactic Astronomical Masers I
... Maser (Microwave Amplification by Stimulated Emission of Radiation) is a radio wave equivalent of laser at optical wavelength. Laser is an acronym for Light Amplification by Stimulated Emission of Radiation. Laser is an artificial light and it is very different from other lights in that a laser ligh ...
... Maser (Microwave Amplification by Stimulated Emission of Radiation) is a radio wave equivalent of laser at optical wavelength. Laser is an acronym for Light Amplification by Stimulated Emission of Radiation. Laser is an artificial light and it is very different from other lights in that a laser ligh ...
Searching for the Secrets of Massive Star Birth
... molecular lines. Although ALMA will improve our view of protoclusters, even higher resolution will be needed to resolve binary and multiple systems. Proto-binaries with separations similar to 1Ori C in Orion (0.03”) at distances of 1 to 10 kpc require resolution of 10 to 1 milli-arseconds. High-re ...
... molecular lines. Although ALMA will improve our view of protoclusters, even higher resolution will be needed to resolve binary and multiple systems. Proto-binaries with separations similar to 1Ori C in Orion (0.03”) at distances of 1 to 10 kpc require resolution of 10 to 1 milli-arseconds. High-re ...