110 - Institute for Astronomy
... We explore the infrared M band (4.7 µm) spectrum of the class I protostar L1489 IRS in the Taurus Molecular Cloud. This is the highest resolution wide coverage spectrum at this wavelength of a low mass protostar observed to date (R =25,000; ∆v =12 km s−1 ). A large number of narrow absorption lines ...
... We explore the infrared M band (4.7 µm) spectrum of the class I protostar L1489 IRS in the Taurus Molecular Cloud. This is the highest resolution wide coverage spectrum at this wavelength of a low mass protostar observed to date (R =25,000; ∆v =12 km s−1 ). A large number of narrow absorption lines ...
Observations of gravitational microlensing events with OSIRIS
... This sample can be expected to include 50 ongoing microlensing events at any time. If the time available for observations in the bulge is very limited, then the area to be covered can be reduced, producing correspondingly fewer events. A signal-to-noise ratio higher than 50 was achieved for an obser ...
... This sample can be expected to include 50 ongoing microlensing events at any time. If the time available for observations in the bulge is very limited, then the area to be covered can be reduced, producing correspondingly fewer events. A signal-to-noise ratio higher than 50 was achieved for an obser ...
a High-Mass Protostar with a Rotating Disk.
... The molecular cloud southwest of the H II region NGC 7538 is a well known site of high-mass star formation [6]. However, the OH and H2 O maser source 8000 south of IRS 1, NGC 7538 S, is even younger and more extreme than any of the other known high–mass (proto)stars in this region. It is very deeply ...
... The molecular cloud southwest of the H II region NGC 7538 is a well known site of high-mass star formation [6]. However, the OH and H2 O maser source 8000 south of IRS 1, NGC 7538 S, is even younger and more extreme than any of the other known high–mass (proto)stars in this region. It is very deeply ...
Self-Regulation of Star Formation in Low Metallicity Clouds
... After the recombination era, little information is accessible until z ∼ 5, after that we can observe objects such as galaxies and QSOs. On the other hand, the reionization of the intergalactic medium and the presence of heavy elements at high-z suggest that there are other populations of luminous ob ...
... After the recombination era, little information is accessible until z ∼ 5, after that we can observe objects such as galaxies and QSOs. On the other hand, the reionization of the intergalactic medium and the presence of heavy elements at high-z suggest that there are other populations of luminous ob ...
Gal - University of Rochester
... grow simultaneously with bars (differing from other models). • We don’t know which resonance is dominant, but if we figure it out we may learn about the vertical shapes of galaxy bulges. • We used a symmetrical bar, however warp modes may be important during bar formation. • Formulism can also be us ...
... grow simultaneously with bars (differing from other models). • We don’t know which resonance is dominant, but if we figure it out we may learn about the vertical shapes of galaxy bulges. • We used a symmetrical bar, however warp modes may be important during bar formation. • Formulism can also be us ...
UMich w/s
... CDM predicts many more satellite galaxies than observed, at all masses `Solutions’: warm DM; self-interacting DM; star formation suppression by reionization; self-regulated star formation; very high M/L plus some other variant; predictions `wrong’, count different things; predictions host-dependent ...
... CDM predicts many more satellite galaxies than observed, at all masses `Solutions’: warm DM; self-interacting DM; star formation suppression by reionization; self-regulated star formation; very high M/L plus some other variant; predictions `wrong’, count different things; predictions host-dependent ...
Masers and high mass star formation Claire Chandler
... • Physical properties of clouds undergoing low- and highmass star formation are different: – Massive SF: clouds are warmer, larger, more massive, mainly located in spiral arms; high mass stars form in clusters and ...
... • Physical properties of clouds undergoing low- and highmass star formation are different: – Massive SF: clouds are warmer, larger, more massive, mainly located in spiral arms; high mass stars form in clusters and ...
Chapter 16 Star Birth
... • Without CO molecules to provide cooling, the clouds that formed the first stars had to be considerably warmer than today’s molecular clouds • The first stars must therefore have been more massive than most of today’s stars, for gravity to overcome pressure ...
... • Without CO molecules to provide cooling, the clouds that formed the first stars had to be considerably warmer than today’s molecular clouds • The first stars must therefore have been more massive than most of today’s stars, for gravity to overcome pressure ...
What do “yellowballs” have to do with the birth of new stars?
... Stars form in the densest and dustiest regions of the interstellar medium, where it is impossible to study the stars using a regular telescope. Fortunately, over the past few decades, astronomers have developed telescopes and detectors that are sensitive to invisible infrared light, which is a type ...
... Stars form in the densest and dustiest regions of the interstellar medium, where it is impossible to study the stars using a regular telescope. Fortunately, over the past few decades, astronomers have developed telescopes and detectors that are sensitive to invisible infrared light, which is a type ...
Stellar Lives (continued). Galaxies.
... In massive stars the core temperature can reach the critical 600 million K to ignite carbon. But carbon burns away in a few hundred years. Each successive stage of nuclear burning proceeds more rapidly than prior stages. Many different reactions may act at the same time. At the end of a massive star ...
... In massive stars the core temperature can reach the critical 600 million K to ignite carbon. But carbon burns away in a few hundred years. Each successive stage of nuclear burning proceeds more rapidly than prior stages. Many different reactions may act at the same time. At the end of a massive star ...
Chapter 16 Star Birth Where do stars form? Star
... • Elements like carbon and oxygen had not yet been made when the first stars formed • Without CO molecules to provide cooling, the clouds that formed the first stars had to be considerably warmer than today’s molecular clouds • The first stars must therefore have been more massive than most of today ...
... • Elements like carbon and oxygen had not yet been made when the first stars formed • Without CO molecules to provide cooling, the clouds that formed the first stars had to be considerably warmer than today’s molecular clouds • The first stars must therefore have been more massive than most of today ...
Infrared Instrumentation & Observing Techniques
... other galaxies at (angular & spectral) resolutions comparable with the work done in our own Galaxy ...
... other galaxies at (angular & spectral) resolutions comparable with the work done in our own Galaxy ...
Formation of elliptical galaxies
... with mass ratios in the range 1:1 - 3:1 •Good agreement of both with intermediate mass giant elliptical galaxies (see also Cox et al. 2006) •Disk merger remnants, as well as ULIRGS, can follow the Fundamental Plane and the MBH-relation (Robertson et al. 2005; Springel et al. 2005) •Mergers trigger ...
... with mass ratios in the range 1:1 - 3:1 •Good agreement of both with intermediate mass giant elliptical galaxies (see also Cox et al. 2006) •Disk merger remnants, as well as ULIRGS, can follow the Fundamental Plane and the MBH-relation (Robertson et al. 2005; Springel et al. 2005) •Mergers trigger ...
Cosmological dynamics with non-minimally coupled scalar field and
... example from the quantum field theory in curved spacetime. f ( R) theories are also widely used as an alternative explanation of the dark energy phenomena which places them amongst the most popular and widely explored alternative theories of gravity. Most of the studies on f ( R) theories though are ...
... example from the quantum field theory in curved spacetime. f ( R) theories are also widely used as an alternative explanation of the dark energy phenomena which places them amongst the most popular and widely explored alternative theories of gravity. Most of the studies on f ( R) theories though are ...
Colliding molecular clouds in head
... Abstract. We present further observations of molecular gas in head-on collisions of spiral galaxies, this time of the CO(J = 1 → 0) and CO(J = 2 → 1) lines in the UGC 813 – UGC 816 system. UGC 813/6 are only the second known example of head-on spiral-spiral collisions, the first example being the UG ...
... Abstract. We present further observations of molecular gas in head-on collisions of spiral galaxies, this time of the CO(J = 1 → 0) and CO(J = 2 → 1) lines in the UGC 813 – UGC 816 system. UGC 813/6 are only the second known example of head-on spiral-spiral collisions, the first example being the UG ...
Astronomy 401 Lecture 8 Spiral Galaxies II 1 The Tully
... The classic spiral galaxy is called a grand design spiral, with two symmetric and well-defined arms. Others have more than two arms, or arms that appear fragmented. Galaxies without well-defined arms that can be traced over a large angular distance are called flocculent spirals. Grand design: ∼ 10% ...
... The classic spiral galaxy is called a grand design spiral, with two symmetric and well-defined arms. Others have more than two arms, or arms that appear fragmented. Galaxies without well-defined arms that can be traced over a large angular distance are called flocculent spirals. Grand design: ∼ 10% ...
CH15.AST1001.S15.EDS
... • Dying stars expel gas and new elements, producing hot bubbles (~106 K). • Hot gas cools, allowing atomic hydrogen clouds to form (~100–10,000 K). • Further cooling permits molecules to form, making molecular clouds (~30 K). • Gravity forms new stars (and planets) in molecular clouds. ...
... • Dying stars expel gas and new elements, producing hot bubbles (~106 K). • Hot gas cools, allowing atomic hydrogen clouds to form (~100–10,000 K). • Further cooling permits molecules to form, making molecular clouds (~30 K). • Gravity forms new stars (and planets) in molecular clouds. ...
The Milky Way
... Which of the following is NOT a good reason for learning more about dark matter? dark matter provides the gravitational force that holds galaxies together the total amount of dark matter determines the fate of our Universe the Earth would be destroyed if it ever ran into a clump of cold dark matter ...
... Which of the following is NOT a good reason for learning more about dark matter? dark matter provides the gravitational force that holds galaxies together the total amount of dark matter determines the fate of our Universe the Earth would be destroyed if it ever ran into a clump of cold dark matter ...
UMich w/s - Royal Observatory, Edinburgh
... Galaxy halo (green), dSph (blue), LMC (cyan), Sgr (red) and dIrr (yellow) element ratios The systematic difference is apparent (from Geisler, Wallerstein, etal 0708.0570) NB Sgr is *very* distinctive: it must be the first such event. ...
... Galaxy halo (green), dSph (blue), LMC (cyan), Sgr (red) and dIrr (yellow) element ratios The systematic difference is apparent (from Geisler, Wallerstein, etal 0708.0570) NB Sgr is *very* distinctive: it must be the first such event. ...
ref evlution of stars
... be hot : perhaps they are collapsing under gravity, or may be excited by ultraviolet radiation from a nearby star. The gas will tend to have a lot of ionised hydrogen in it (H II) and will form an emission nebula. ...
... be hot : perhaps they are collapsing under gravity, or may be excited by ultraviolet radiation from a nearby star. The gas will tend to have a lot of ionised hydrogen in it (H II) and will form an emission nebula. ...
Complex Processes in Simple Ices
... found each other and bonded together long enough to be considered a stable species. The Universe’s first molecule had formed. Other molecules followed, even if the chemistry was rather primitive compared to what we are used to on earth – carbon, oxygen and all other larger elements had yet to form. ...
... found each other and bonded together long enough to be considered a stable species. The Universe’s first molecule had formed. Other molecules followed, even if the chemistry was rather primitive compared to what we are used to on earth – carbon, oxygen and all other larger elements had yet to form. ...
Galaxies
... arms are wound, with “a” being most tightly wound. The Andromeda Galaxy is an Sb. • Elliptical galaxies are denoted by “E”, with a number from 0-7 indicating how circular it appears. An example of this would be M87, which is an E0 galaxy. • Irregulars, such as the Small Magellanic Cloud, are denoted ...
... arms are wound, with “a” being most tightly wound. The Andromeda Galaxy is an Sb. • Elliptical galaxies are denoted by “E”, with a number from 0-7 indicating how circular it appears. An example of this would be M87, which is an E0 galaxy. • Irregulars, such as the Small Magellanic Cloud, are denoted ...
Lyman-α: The Many Applications and Challenges of This Powerful
... parts per million (ppm) in the gas located within about 300 light-years of the Sun. At further distances, the large range in interstellar gas D/H ratios between 4 and 23 ppm can be explained by different amounts of D gas depletion onto dust grains along these lines of sight. This technique has allow ...
... parts per million (ppm) in the gas located within about 300 light-years of the Sun. At further distances, the large range in interstellar gas D/H ratios between 4 and 23 ppm can be explained by different amounts of D gas depletion onto dust grains along these lines of sight. This technique has allow ...
Life Before the Fall: Group Galaxy Evolution Prior to Cluster Assembly
... Ringberg Workshop - October 25, 2005 ...
... Ringberg Workshop - October 25, 2005 ...