Stellar populations in the nuclear regions of nearby radio galaxies
... galaxy (DA 240) was observed with this alternative setup. The dichroics 5700 and 6100 were used in 1997 November and 1998 February, and in both runs we used a filter to avoid second-order contamination in the spectra. We obtained flux standards (HZ 44 and G1912 B2B) for the four nights and gratings, ...
... galaxy (DA 240) was observed with this alternative setup. The dichroics 5700 and 6100 were used in 1997 November and 1998 February, and in both runs we used a filter to avoid second-order contamination in the spectra. We obtained flux standards (HZ 44 and G1912 B2B) for the four nights and gratings, ...
CO OBSERVATIONS OF SPIRAL STRUCTURE AND THE LIFETIME
... By virtue of its broad latitude coverage, the survey of Solomon, Scoville, and Sanders (1978) affords an excellent opportunity to trace large scale galactic features such as spiral arms or cloud clusters which do not necessarily maintain a constant latitude over their full longitude extent. Approxim ...
... By virtue of its broad latitude coverage, the survey of Solomon, Scoville, and Sanders (1978) affords an excellent opportunity to trace large scale galactic features such as spiral arms or cloud clusters which do not necessarily maintain a constant latitude over their full longitude extent. Approxim ...
Starburst Galaxies - Beck-Shop
... The young stars, that can now be seen directly, have masses ranging from 0.08 solar masses (the brown dwarf limit) to slightly over 100 solar masses (beyond which stars become unstable). By far the majority of stars though are at the low-mass end of this range – 80% have masses less than that of the ...
... The young stars, that can now be seen directly, have masses ranging from 0.08 solar masses (the brown dwarf limit) to slightly over 100 solar masses (beyond which stars become unstable). By far the majority of stars though are at the low-mass end of this range – 80% have masses less than that of the ...
1 Pau Amaro Seoane - modest 15-s
... of turbulent molecular clouds. The stars are assumed to form in the densest regions in the collapsing cloud after an initial free-fall times of the molecular cloud. The dynamical evolution of these stellar distributions are continued by means of direct N-body simulations. The molecular clouds typica ...
... of turbulent molecular clouds. The stars are assumed to form in the densest regions in the collapsing cloud after an initial free-fall times of the molecular cloud. The dynamical evolution of these stellar distributions are continued by means of direct N-body simulations. The molecular clouds typica ...
Introduction to Observational Cosmology
... Structure (Size, bulge-to-disc ratio, etc..) Dynamical mass Star formation rate Color (or spectral energy distribution) of the stellar population ...
... Structure (Size, bulge-to-disc ratio, etc..) Dynamical mass Star formation rate Color (or spectral energy distribution) of the stellar population ...
Evolution of galaxy morphology - Lecture 1 - NCRA-TIFR
... gravitationally bound agglomerations of stars, dust, gas, dark matter. Mass ratio Gas:Stars:Dark Matter - 1:10:100 they are the basic building blocks of the Universe on large scales they show a broad range in their physical properties Understanding of galaxy formation and evolution is one of the mai ...
... gravitationally bound agglomerations of stars, dust, gas, dark matter. Mass ratio Gas:Stars:Dark Matter - 1:10:100 they are the basic building blocks of the Universe on large scales they show a broad range in their physical properties Understanding of galaxy formation and evolution is one of the mai ...
The Interstellar Medium Not Quite Empty Space Why study the ISM
... The diffuse ISM at longer wavelengths • Diffuse medium with higher column densities best observed at infrared wavelengths • IR spectra of cool bright stars - across the Galaxy • Interstellar absorption lines and bands give columns of atomic or ionic gas, molecules & dust – Dust bands are broader and ...
... The diffuse ISM at longer wavelengths • Diffuse medium with higher column densities best observed at infrared wavelengths • IR spectra of cool bright stars - across the Galaxy • Interstellar absorption lines and bands give columns of atomic or ionic gas, molecules & dust – Dust bands are broader and ...
P - Inaf
... (our final sample consists of 11 296 centrals and 7053 satellites), at least the final sample of model galaxies is biased in a similar way as the real data, thus allowing for a more meaningful comparison.2 Fig. 6 shows the average metallicity and mass-weighted stellar ages of the W08 model galaxies ...
... (our final sample consists of 11 296 centrals and 7053 satellites), at least the final sample of model galaxies is biased in a similar way as the real data, thus allowing for a more meaningful comparison.2 Fig. 6 shows the average metallicity and mass-weighted stellar ages of the W08 model galaxies ...
Lecture 2 Astronomical Distances
... HST sees Cepheids to D = 10-20 Mpc. H0 x D = 70 x 15 ~ 1000 km/s. not really far enough galaxy pecular velocities ~500 km/s. galaxies falling toward Virgo cluster. ...
... HST sees Cepheids to D = 10-20 Mpc. H0 x D = 70 x 15 ~ 1000 km/s. not really far enough galaxy pecular velocities ~500 km/s. galaxies falling toward Virgo cluster. ...
The oxygen abundance deficiency in irregular galaxies
... case will be referred to as a “bursting” star formation history. The case with c = –0.75, τ = 13 Gyr, t0 = 0, and n = 7 is shown in Fig.2. The values 0 < c < 1 corresponds to the opposite case. Following Tosi (1993), this case will be referred to as a “gasping” star formation history. The case with ...
... case will be referred to as a “bursting” star formation history. The case with c = –0.75, τ = 13 Gyr, t0 = 0, and n = 7 is shown in Fig.2. The values 0 < c < 1 corresponds to the opposite case. Following Tosi (1993), this case will be referred to as a “gasping” star formation history. The case with ...
Module 4.1 - The Scale of the Universe [slide 1] We now turn to
... therefore, luminosity must change. If we observe stars spectroscopically, we can observe the velocity of the photo sphere. Come towards us and go away from us. So we can measure stellar temperatures using colors or spectroscopy. We can measure velocity of the pulsating photosphere using spectroscopy ...
... therefore, luminosity must change. If we observe stars spectroscopically, we can observe the velocity of the photo sphere. Come towards us and go away from us. So we can measure stellar temperatures using colors or spectroscopy. We can measure velocity of the pulsating photosphere using spectroscopy ...
ALMA Science Results
... – Aims: mass assembly history and feedback. Why molecular gas--best tracer of circular velocity in galaxies. Best tracer of dynamical mass. – Get masses of supermassive black holes through CO dynamical measurements. NGC4526 high resolution CO imaging. CARMA data. – Fit to CO rotation curve shows a b ...
... – Aims: mass assembly history and feedback. Why molecular gas--best tracer of circular velocity in galaxies. Best tracer of dynamical mass. – Get masses of supermassive black holes through CO dynamical measurements. NGC4526 high resolution CO imaging. CARMA data. – Fit to CO rotation curve shows a b ...
implication on the mass and
... ! Connection between LIRGs and disks (z>0.4) (HST morphologies and color maps) : 40% of LIRGs are large disks (Zheng et al, 2004, A&A) ! Lilly et al (1998) large disk sample (rdisk > 4 h50-1 kpc) at 0.5 < z < 1: 32 (+/-13)% of them are LIRGs ! LIRGs have large stellar masses: 1.4 1010MO
... ! Connection between LIRGs and disks (z>0.4) (HST morphologies and color maps) : 40% of LIRGs are large disks (Zheng et al, 2004, A&A) ! Lilly et al (1998) large disk sample (rdisk > 4 h50-1 kpc) at 0.5 < z < 1: 32 (+/-13)% of them are LIRGs ! LIRGs have large stellar masses: 1.4 1010MO
Messier 87
Messier 87 (also known as Virgo A or NGC 4486, and generally abbreviated to M87) is a supergiant elliptical galaxy in the constellation Virgo. One of the most massive galaxies in the local universe, it is notable for its large population of globular clusters—M87 contains about 12,000 compared to the 150-200 orbiting the Milky Way—and its jet of energetic plasma that originates at the core and extends outward at least 1,500 parsecs (4,900 light-years), travelling at relativistic speed. It is one of the brightest radio sources in the sky, and is a popular target for both amateur astronomy observations and professional astronomy study.French astronomer Charles Messier discovered M87 in 1781, cataloguing it as a nebulous feature while searching for objects that would confuse comet hunters. The second brightest galaxy within the northern Virgo Cluster, M87 is located about 16.4 million parsecs (53.5 million light-years) from Earth. Unlike a disk-shaped spiral galaxy, M87 has no distinctive dust lanes. Instead, it has an almost featureless, ellipsoidal shape typical of most giant elliptical galaxies, diminishing in luminosity with distance from the centre. Forming around one sixth of M87's mass, the stars in this galaxy have a nearly spherically symmetric distribution, their density decreasing with increasing distance from the core. At the core is a supermassive black hole, which forms the primary component of an active galactic nucleus. This object is a strong source of multiwavelength radiation, particularly radio waves. M87's galactic envelope extends out to a radius of about 150 kiloparsecs (490,000 light-years), where it has been truncated—possibly by an encounter with another galaxy. Between the stars is a diffuse interstellar medium of gas that has been chemically enriched by elements emitted from evolved stars.