Mapping the Pathways of Galaxy Transformation Across Time and
... activity, stellar mass assembly, and morphology. In this talk, I will illustrate the relation between global properties and kpc-scale substructures of galaxies out to z∼2. Using combined high resolution data from the Hubble Space Telescope and long exposure spectroscopic observations with the Keck t ...
... activity, stellar mass assembly, and morphology. In this talk, I will illustrate the relation between global properties and kpc-scale substructures of galaxies out to z∼2. Using combined high resolution data from the Hubble Space Telescope and long exposure spectroscopic observations with the Keck t ...
The Evolution of Star Formation Activity in . Cory R. Wagner
... IRAC Shallow Cluster Survey, and 25 low-redshift (0.15 < z < 1) clusters from The Cluster Lensing And Supernova survey with Hubble. We compare cluster galaxy star formation to that of the field over 0.15 < z < 1.5 using ∼8000 galaxies from the UltraVISTA survey. Mid-infrared star formation rates are ...
... IRAC Shallow Cluster Survey, and 25 low-redshift (0.15 < z < 1) clusters from The Cluster Lensing And Supernova survey with Hubble. We compare cluster galaxy star formation to that of the field over 0.15 < z < 1.5 using ∼8000 galaxies from the UltraVISTA survey. Mid-infrared star formation rates are ...
365 days of SKYWATCHING
... it’s possible to watch as the Earth overtakes a planet, much like running past an object on a racetrack. As we approach it, it will seem to slow down, stand still, and then move backwards as we go by. Once we have passed, it will then appear to resume forward motion. Since Mercury and Venus are on t ...
... it’s possible to watch as the Earth overtakes a planet, much like running past an object on a racetrack. As we approach it, it will seem to slow down, stand still, and then move backwards as we go by. Once we have passed, it will then appear to resume forward motion. Since Mercury and Venus are on t ...
Chandra News March 2005 Published by the Chandra X-ray Center (CXC)
... reflect the orbital motion of this cone and the plasma flow along the cone modulated by the phase-dependent orientation of the cone to the line of sight (Henley, Stevens & Pittard 2003). Figure 4 shows some of the variation seen. We highlight a few of the important results from these observations be ...
... reflect the orbital motion of this cone and the plasma flow along the cone modulated by the phase-dependent orientation of the cone to the line of sight (Henley, Stevens & Pittard 2003). Figure 4 shows some of the variation seen. We highlight a few of the important results from these observations be ...
introduction to geodetic astronomy
... geodetic astronomy is essential for.the demarcation of astronomically defined boundaries. ...
... geodetic astronomy is essential for.the demarcation of astronomically defined boundaries. ...
1 Globular Cluster Systems - McMaster Physics and Astronomy
... cluster in which the principal CMD sequences are de ned). For metal-poor clusters in which RR Lyrae stars are present, by convention MV (HB ) is identical to the mean luminosity of these RR Lyraes. For metal-richer clusters in which there are only red HB stars and no RR Lyraes, MV (HB ) is equal to ...
... cluster in which the principal CMD sequences are de ned). For metal-poor clusters in which RR Lyrae stars are present, by convention MV (HB ) is identical to the mean luminosity of these RR Lyraes. For metal-richer clusters in which there are only red HB stars and no RR Lyraes, MV (HB ) is equal to ...
- Isaac Newton Group of Telescopes
... should be undergoing gravitational contraction, radiating much more energy than in later stages of their evolution. More massive brown dwarfs in the Pleiades should be detectable in sufficiently deep surveys. After only 0.3% of the clusters area had been explored using IAC80 telescope at Teide Obse ...
... should be undergoing gravitational contraction, radiating much more energy than in later stages of their evolution. More massive brown dwarfs in the Pleiades should be detectable in sufficiently deep surveys. After only 0.3% of the clusters area had been explored using IAC80 telescope at Teide Obse ...
MERCURY In-flight calibration of the PHEBUS UV instrument and
... A unique feature of Mercury’s space environment is its strongly coupled surfaceexosphere-magnetosphere-solar wind system, which can be remotely monitored by space missions such as Mariner 10, MESSENGER and soon BepiColombo and by ground-based observatories. Mercury’s exosphere is a very complex medi ...
... A unique feature of Mercury’s space environment is its strongly coupled surfaceexosphere-magnetosphere-solar wind system, which can be remotely monitored by space missions such as Mariner 10, MESSENGER and soon BepiColombo and by ground-based observatories. Mercury’s exosphere is a very complex medi ...
The visibility of Lyman Alpha Emitters: constraining reionization
... GADGET-2 to obtain the physical properties of z ≃ 5.7 galaxies, (b) a dust model that took into account the entire star formation history of each galaxy to calculate its dust enrichment and, (c) a RT code (CRASH) to obtain the ionization fields to calculate the IGM Lyα transmission for each galaxy, ...
... GADGET-2 to obtain the physical properties of z ≃ 5.7 galaxies, (b) a dust model that took into account the entire star formation history of each galaxy to calculate its dust enrichment and, (c) a RT code (CRASH) to obtain the ionization fields to calculate the IGM Lyα transmission for each galaxy, ...
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 ...
Review of asymmetric dark matter
... required). Many models of asymmetric DM can be tested through direct detection and collider signatures, but the parameters involved typically include some that are independent of the physics behind the cosmological DM abundance. In most ADM models, the number density of DM particles is comparable to ...
... required). Many models of asymmetric DM can be tested through direct detection and collider signatures, but the parameters involved typically include some that are independent of the physics behind the cosmological DM abundance. In most ADM models, the number density of DM particles is comparable to ...
High-mass star-forming cloud G0.38+0.04 in the Galactic center dust
... Sgr B2 (M): there is only one SiO maser spot in Sgr B2, located near Mehringer et al. (1994) H2 CO Source C (not to be confused with Cloud C, the topic of this paper). The Sgr B2 H2 CO maser C is peculiar even among the Sgr B2 masers in that the emission appears to be spatially and spectrally resolv ...
... Sgr B2 (M): there is only one SiO maser spot in Sgr B2, located near Mehringer et al. (1994) H2 CO Source C (not to be confused with Cloud C, the topic of this paper). The Sgr B2 H2 CO maser C is peculiar even among the Sgr B2 masers in that the emission appears to be spatially and spectrally resolv ...
Time Variation of Kepler Transits Induced By Stellar Rotating Spots
... close to zero, while others were found to be misaligned, including systems in retrograde motion where the spin-orbit angle is close to 180◦ (e.g., Hébrard et al. 2011; Winn et al. ...
... close to zero, while others were found to be misaligned, including systems in retrograde motion where the spin-orbit angle is close to 180◦ (e.g., Hébrard et al. 2011; Winn et al. ...
X-ray astronomy of stellar coronae (Review)
... While this review is entirely devoted to (non-solar) stellar studies, an important anchor point would be missing if the success of the Skylab mission in the early seventies were not mentioned. The high-quality images of the full-disk Sun in X-rays formed, together with data from previous rocket flig ...
... While this review is entirely devoted to (non-solar) stellar studies, an important anchor point would be missing if the success of the Skylab mission in the early seventies were not mentioned. The high-quality images of the full-disk Sun in X-rays formed, together with data from previous rocket flig ...
Neutrino Astrophysics
... in which a nucleus containing N neutrons and Z protons decays to a lighter nucleus by converting a neutron to a proton, with the emission of an electron and an electron antineutrino. Indeed, it was the apparent absence of energy conservation in nuclear β decay that first lead Wolfgang Pauli, more th ...
... in which a nucleus containing N neutrons and Z protons decays to a lighter nucleus by converting a neutron to a proton, with the emission of an electron and an electron antineutrino. Indeed, it was the apparent absence of energy conservation in nuclear β decay that first lead Wolfgang Pauli, more th ...
the PDF - Montana State University
... the nature of its well-ordered generation of magnetic field in 11-year activity cycles remains a mystery. In this work, we place the solar cycle in a broader context by examining the long-term variability of solar analog stars within 5% of the solar effective temperature, but varied in rotation rate ...
... the nature of its well-ordered generation of magnetic field in 11-year activity cycles remains a mystery. In this work, we place the solar cycle in a broader context by examining the long-term variability of solar analog stars within 5% of the solar effective temperature, but varied in rotation rate ...
Chapter 5 The Evolutionary Paths Of Nearby Galaxies
... Figure 5.5: The morphological type distribution of galaxies in the HRS+ sample (dotted histogram). The filled histogram represents galaxies in the transition region, while red and blue sequence galaxies are shown with the empty and dashed histogram, respectively. ...
... Figure 5.5: The morphological type distribution of galaxies in the HRS+ sample (dotted histogram). The filled histogram represents galaxies in the transition region, while red and blue sequence galaxies are shown with the empty and dashed histogram, respectively. ...
My Thesis - Uppsala Astronomical Observatory
... Strong evidence exists showing that stellar evolution models are unable to accurately predict the fundamental properties of low-mass stars. Observations of low-mass stars in detached eclipsing binaries (DEBs) indicate that stellar models under-predict real stellar radii by 5 – 10% and predict effect ...
... Strong evidence exists showing that stellar evolution models are unable to accurately predict the fundamental properties of low-mass stars. Observations of low-mass stars in detached eclipsing binaries (DEBs) indicate that stellar models under-predict real stellar radii by 5 – 10% and predict effect ...
SkyWatcher2017.5 1.3 Mb - Boise Astronomical Society
... luminosity distance of DL = 749 mega-parsecs may be calculated from z. It is also one of the most luminous quasars known, with an absolute magnitude of −26.7, meaning that if it were only as distant as Pollux it would appear nearly as bright in the sky as the Sun. Since the sun's absolute magnitude ...
... luminosity distance of DL = 749 mega-parsecs may be calculated from z. It is also one of the most luminous quasars known, with an absolute magnitude of −26.7, meaning that if it were only as distant as Pollux it would appear nearly as bright in the sky as the Sun. Since the sun's absolute magnitude ...
Stellar Intensity Interferometry: The Background John Davis Sydney Institute for Astronomy
... stars”. Robert Hanbury Brown (RHB) was determined to measure them • If these sources were galaxies their angular sizes would be of the order of a minute of arc and easy to measure with a conventional interferometer but, if they were stars, extremely long baselines would be needed and RHB concluded ...
... stars”. Robert Hanbury Brown (RHB) was determined to measure them • If these sources were galaxies their angular sizes would be of the order of a minute of arc and easy to measure with a conventional interferometer but, if they were stars, extremely long baselines would be needed and RHB concluded ...
R136a1
RMC 136a1 (usually abbreviated to R136a1) is a Wolf-Rayet star located at the center of R136, the central condensation of stars of the large NGC 2070 open cluster in the Tarantula Nebula. It lies at a distance of about 50 kiloparsecs (163,000 light-years) in the Large Magellanic Cloud. It has the highest mass and luminosity of any known star, at 265 M☉ and 8.7 million L☉, and also one of the hottest at over 50,000 K.