Spectroscopic Atlas for Amateur Astronomers
... which systematically covers the classes O, B, A, F, G, K, M, by commenting most of the lines, visible in a medium resolved spectral profile was still missing. In the Internet we find many professional papers, mostly focused on small sections of a spectral profile. Nevertheless, they often contribute ...
... which systematically covers the classes O, B, A, F, G, K, M, by commenting most of the lines, visible in a medium resolved spectral profile was still missing. In the Internet we find many professional papers, mostly focused on small sections of a spectral profile. Nevertheless, they often contribute ...
On the nature of sn stars. I. A detailed abundance study
... questioned. There is no general agreement about their origin. We aim to derive abundances for a sample of 9 stars, including sn and non-sn stars, to determine the possible relation between sn and CP stars and compare their chemical abundances. That most sn stars belong to open clusters allows us to ...
... questioned. There is no general agreement about their origin. We aim to derive abundances for a sample of 9 stars, including sn and non-sn stars, to determine the possible relation between sn and CP stars and compare their chemical abundances. That most sn stars belong to open clusters allows us to ...
Observational Studies of Interacting Galaxies and the Development
... is to use the integral field spectroscopic technique, capitalizing its intrinsic capability of obtaining 2-D spectra effectively. However, the currently available integral field spectrographs are inadequate to provide the required combination of integral field size and spectral resolution for merger ...
... is to use the integral field spectroscopic technique, capitalizing its intrinsic capability of obtaining 2-D spectra effectively. However, the currently available integral field spectrographs are inadequate to provide the required combination of integral field size and spectral resolution for merger ...
Brightest Stars : Discovering the Universe Through the Sky`s Most
... through direct involvement—in astronomy, through actual observation. This is especially true in today’s world, in which a vast majority of people live under skies significantly degraded by human-made light pollution. In such a world, it is the brightest stars that everybody can see, even people who ...
... through direct involvement—in astronomy, through actual observation. This is especially true in today’s world, in which a vast majority of people live under skies significantly degraded by human-made light pollution. In such a world, it is the brightest stars that everybody can see, even people who ...
Strongly suggested reading: The stellar halo of the Galaxy
... may lead to an article that is rapidly out of date. On the other hand, this of course, is only a sign of the field’s health and its great promise for the young generations of scientists hoping to unravel the formation of the Galaxy. The reader is hereby warned that our understanding of the Galactic ...
... may lead to an article that is rapidly out of date. On the other hand, this of course, is only a sign of the field’s health and its great promise for the young generations of scientists hoping to unravel the formation of the Galaxy. The reader is hereby warned that our understanding of the Galactic ...
Radio Emission Toward Regions of Massive Star Formation
... stars with accretion disks and bipolar outflows have been directly observed (Kraus et al. 2010). Therefore, there must be some other important physics simple models do not take into account. The review by Zinnecker & Yorke (2007) discusses three prevailing theories: monolithic collapse in cores with ...
... stars with accretion disks and bipolar outflows have been directly observed (Kraus et al. 2010). Therefore, there must be some other important physics simple models do not take into account. The review by Zinnecker & Yorke (2007) discusses three prevailing theories: monolithic collapse in cores with ...
High-mass star-forming cloud G0.38+0.04 in the Galactic center dust
... This high detection rate of masers in star-forming regions within the CMZ, despite limited statistical information, suggests that H2 CO masers may be an efficient tracer of high-mass star formation in extreme environments. By contrast, extensive surveys have shown that the occurrence of H2 CO masers ...
... This high detection rate of masers in star-forming regions within the CMZ, despite limited statistical information, suggests that H2 CO masers may be an efficient tracer of high-mass star formation in extreme environments. By contrast, extensive surveys have shown that the occurrence of H2 CO masers ...
The Ages of Stars
... comparisons of the Sun to other stars often rely on the very stellar properties (such as activity, rotation, or lithium abundance) that one is trying to understand; the process is self-referential. • To fully understand the Galaxy’s history of formation, enrichment, and dynamics, we need to be able ...
... comparisons of the Sun to other stars often rely on the very stellar properties (such as activity, rotation, or lithium abundance) that one is trying to understand; the process is self-referential. • To fully understand the Galaxy’s history of formation, enrichment, and dynamics, we need to be able ...
Abstract The Star Formation History of Low Surface Brightness Galaxies
... The star formation histories of low surface brightness galaxies are interesting but poorly constrained. These objects tend to be rather blue, contradicting the initial impression that they may simply be faded remnants of higher surface brightness galaxies whose star formation has finished. Other sce ...
... The star formation histories of low surface brightness galaxies are interesting but poorly constrained. These objects tend to be rather blue, contradicting the initial impression that they may simply be faded remnants of higher surface brightness galaxies whose star formation has finished. Other sce ...
Astronomy Astrophysics
... centered on each candidate cluster were used to construct color–magnitude and color–color diagrams. Follow-up spectroscopy of the brightest members of several cluster candidates was obtained in order to clarify their nature. Results. We report the discovery of 58 new infrared cluster candidates. Fun ...
... centered on each candidate cluster were used to construct color–magnitude and color–color diagrams. Follow-up spectroscopy of the brightest members of several cluster candidates was obtained in order to clarify their nature. Results. We report the discovery of 58 new infrared cluster candidates. Fun ...
LACEwING: A New Moving Group Analysis Code
... kinematic and spatial information. LACEwING works in right-handed Cartesian Galactic coordinates, with UVW space velocities and XYZ space positions, where the U/X axis is toward the Galactic center. The matrices of Johnson & Soderblom (1987) transform observational equatorial coordinates into UVW an ...
... kinematic and spatial information. LACEwING works in right-handed Cartesian Galactic coordinates, with UVW space velocities and XYZ space positions, where the U/X axis is toward the Galactic center. The matrices of Johnson & Soderblom (1987) transform observational equatorial coordinates into UVW an ...
6.7 GHz Methanol Masers and the GBT
... • This makes 6.7 GHz methanol masers unique compared to OH and H2O masers which are also found towards late type stars/low-mass stars. • What makes the 6.7 GHz line even more interesting is that it traces one of the earliest phases of massive star formation. • A sample of 6.7 GHz methanol masers can ...
... • This makes 6.7 GHz methanol masers unique compared to OH and H2O masers which are also found towards late type stars/low-mass stars. • What makes the 6.7 GHz line even more interesting is that it traces one of the earliest phases of massive star formation. • A sample of 6.7 GHz methanol masers can ...
A Spitzer mid-infrared spectral survey of mass
... clusters NGC 419 and 1978, both of which have a known mid-IR source. Targets were selected to span the long sequence of increasing mass-loss in LIMS which stretches from (J − K , M K ) ∼ (2, − 9) to (7, −4) in Fig. 1(a). [The bright oxygen-rich object near (J − K , M K ) ∼ (1, −10.7) in Fig. 1(b) wa ...
... clusters NGC 419 and 1978, both of which have a known mid-IR source. Targets were selected to span the long sequence of increasing mass-loss in LIMS which stretches from (J − K , M K ) ∼ (2, − 9) to (7, −4) in Fig. 1(a). [The bright oxygen-rich object near (J − K , M K ) ∼ (1, −10.7) in Fig. 1(b) wa ...
365 days of SKYWATCHING
... night as the terminator - the line between sunset and shadow - progresses over the surface, revealing new details. Unlike a star chart, Moon feature instructions are based on lunar topography and not our Earthly cardinal directions. While these pages outline what features should be visible on any gi ...
... night as the terminator - the line between sunset and shadow - progresses over the surface, revealing new details. Unlike a star chart, Moon feature instructions are based on lunar topography and not our Earthly cardinal directions. While these pages outline what features should be visible on any gi ...
Abd al-Rahman al-Sufi and his book of the fixed stars: a journey of
... Fixed Stars. It was written in Arabic by the famous Persian author and astronomer ′Abd alRaḥmān al-Ṣūfī around A.D. 964. Ever since I read this comment by Professor Kunitzsch I wondered what prompted one of the foremost experts in the history of Arabic astronomy to write such a comment about a book, ...
... Fixed Stars. It was written in Arabic by the famous Persian author and astronomer ′Abd alRaḥmān al-Ṣūfī around A.D. 964. Ever since I read this comment by Professor Kunitzsch I wondered what prompted one of the foremost experts in the history of Arabic astronomy to write such a comment about a book, ...
The most metal-poor galaxies
... one looks, this quantity may vary substantially. For example in our Galaxy, the bulge, the solar neighbourhood and the halo differ in metallicity. The most metal-poor halo stars have heavy element abundances 10−4 times that of the Sun (Cayrel 1996) while stars in the Galactic centre may be three tim ...
... one looks, this quantity may vary substantially. For example in our Galaxy, the bulge, the solar neighbourhood and the halo differ in metallicity. The most metal-poor halo stars have heavy element abundances 10−4 times that of the Sun (Cayrel 1996) while stars in the Galactic centre may be three tim ...
THE UV-OPTICAL COLOR MAGNITUDE DIAGRAM. II. PHYSICAL
... quite clearly how the NUV r color covers a much wider magnitude range than g r. In addition, the g r color starts to saturate for red galaxies, while NUV r varies by more than 2 magnitudes. We see indications from these plots that rest-frame UV-optical colors correlate with Sersic index (and ...
... quite clearly how the NUV r color covers a much wider magnitude range than g r. In addition, the g r color starts to saturate for red galaxies, while NUV r varies by more than 2 magnitudes. We see indications from these plots that rest-frame UV-optical colors correlate with Sersic index (and ...
Altair -- the ``hottest`` magnetically active star in X-rays
... Several attempts have been made to measure the magnetic field of Altair, e.g. by circular polarization measurement that traces the longitudinal component, but resulted in its non-detection at an accuracy of about 100 G (Landstreet 1982). The onset of stellar magnetic activity is connected to the dev ...
... Several attempts have been made to measure the magnetic field of Altair, e.g. by circular polarization measurement that traces the longitudinal component, but resulted in its non-detection at an accuracy of about 100 G (Landstreet 1982). The onset of stellar magnetic activity is connected to the dev ...
Legends Night Sky Orion
... - Betelgeuse glows with a dull red. - It is labeled alpha Orionis, even if it is less bright than beta Orionis (Rigel). - It is much larger then Rigel. - It is estimated at around 250 Suns. ...
... - Betelgeuse glows with a dull red. - It is labeled alpha Orionis, even if it is less bright than beta Orionis (Rigel). - It is much larger then Rigel. - It is estimated at around 250 Suns. ...
Educator`s Guide
... - Betelgeuse glows with a dull red. - It is labeled alpha Orionis, even if it is less bright than beta Orionis (Rigel). - It is much larger then Rigel. - It is estimated at around 250 Suns. ...
... - Betelgeuse glows with a dull red. - It is labeled alpha Orionis, even if it is less bright than beta Orionis (Rigel). - It is much larger then Rigel. - It is estimated at around 250 Suns. ...
Mission Possible: Voyage to the Stars
... for millions to trillions of years. Not all stars are the same. There are many different types of stars that vary in size, color, temperature, and life span. TYPES OF STARS All stars are created from a nebula but where they go after that depends on their mass. All aspects of a star including size, t ...
... for millions to trillions of years. Not all stars are the same. There are many different types of stars that vary in size, color, temperature, and life span. TYPES OF STARS All stars are created from a nebula but where they go after that depends on their mass. All aspects of a star including size, t ...
Chemical Evolution of Galactic Systems
... This thesis explores the chemical signatures of galaxy formation and evolution using a software package designed specifically for this investigation. We describe the development of this multi-zone chemical evolution code, which simulates the spacetime evolution of stars, gas and a vast array of chem ...
... This thesis explores the chemical signatures of galaxy formation and evolution using a software package designed specifically for this investigation. We describe the development of this multi-zone chemical evolution code, which simulates the spacetime evolution of stars, gas and a vast array of chem ...
Formation of Molecular Clouds and Global Conditions for Star
... or the H2 to 13 CO abundance ratio, both of which can vary within and between clouds in response to local conditions of UV irradiance, density, temperature, and metallicity (Bolatto et al. 2013; Ripple et al. 2013). Millimeter wave interferometers can resolve large GMC complexes in nearby galaxies b ...
... or the H2 to 13 CO abundance ratio, both of which can vary within and between clouds in response to local conditions of UV irradiance, density, temperature, and metallicity (Bolatto et al. 2013; Ripple et al. 2013). Millimeter wave interferometers can resolve large GMC complexes in nearby galaxies b ...
Spectral Matching for Elemental Abundances of Evolved Stars of Globular Clusters
... for their chemical composition. This is especially true for the complex, multimetallic cluster ω Centauri, with its large range of iron, carbon, nitrogen, oxygen, sodium and barium abundances. In order to accomplish this, an automated spectral matching pipeline was developed to determine these abund ...
... for their chemical composition. This is especially true for the complex, multimetallic cluster ω Centauri, with its large range of iron, carbon, nitrogen, oxygen, sodium and barium abundances. In order to accomplish this, an automated spectral matching pipeline was developed to determine these abund ...
T3-Cosmic Star Formation History
... global history of star formation and heavy element production of the Universe, independently of the complex evolutionary phases of individual galaxy subpopulations. The modern version of this technique relies on some basic properties of stellar populations and dusty starburst galaxies: 1. The UV-con ...
... global history of star formation and heavy element production of the Universe, independently of the complex evolutionary phases of individual galaxy subpopulations. The modern version of this technique relies on some basic properties of stellar populations and dusty starburst galaxies: 1. The UV-con ...
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.