lecture course
... In most galaxy samples there are roughly equal numbers of elliptical, spiral, and peculiar (irregular) galaxies. Elliptical galaxies come in two types - giant ellipticals, which have high brightnesses at their centres and absolute B magnitudes between about -25 and -15, and dwarf ellipticals, which ...
... In most galaxy samples there are roughly equal numbers of elliptical, spiral, and peculiar (irregular) galaxies. Elliptical galaxies come in two types - giant ellipticals, which have high brightnesses at their centres and absolute B magnitudes between about -25 and -15, and dwarf ellipticals, which ...
Here
... of the currently known sample are presented and discussed. The star formation rates derived from the FIR luminosity range from about 300 to 5000 M⊙ year−1 and the molecular mass from 4 × 109 to 1 × 1011 M⊙ . At the lower end, these star formation rates, gas masses, and diameters are similar to those ...
... of the currently known sample are presented and discussed. The star formation rates derived from the FIR luminosity range from about 300 to 5000 M⊙ year−1 and the molecular mass from 4 × 109 to 1 × 1011 M⊙ . At the lower end, these star formation rates, gas masses, and diameters are similar to those ...
Evolution of galaxy morphology - Lecture 1 - NCRA-TIFR
... Where e refers to effective values and n is the Sérsic index. For n=4 it becomes the de Vaucouleurs function; for n=1 an exponential, and when n=0.5, a Gaussian! For values in the range 1-4, approximately, it describes bulges in late-type spiral galaxies (or pseudo-bulges) to bulges in early-type sp ...
... Where e refers to effective values and n is the Sérsic index. For n=4 it becomes the de Vaucouleurs function; for n=1 an exponential, and when n=0.5, a Gaussian! For values in the range 1-4, approximately, it describes bulges in late-type spiral galaxies (or pseudo-bulges) to bulges in early-type sp ...
The first carbon-enhanced metal-poor star found in the Sculptor
... The origin of carbon-enhanced metal-poor (CEMP) stars and their possible connection with the chemical elements produced by the first stellar generation is still highly debated. In contrast to the Galactic halo, not many CEMP stars have been found in the dwarf spheroidal galaxies around the Milky Way ...
... The origin of carbon-enhanced metal-poor (CEMP) stars and their possible connection with the chemical elements produced by the first stellar generation is still highly debated. In contrast to the Galactic halo, not many CEMP stars have been found in the dwarf spheroidal galaxies around the Milky Way ...
PS1-12SK IS A PECULIAR SUPERNOVA FROM A HE
... 08h 44m 54.86s + 42◦ 58´16.89˝ (J2000), within the galaxy cluster RXC J0844.9+4258. The object was spectroscopically classified as the first Type Ibn SN discovered by Pan-STARRS1 after just ∼ 2 years of survey operation. At z = 0.054, PS1-12sk is more distant than any previously discovered SN Ibn.12 ...
... 08h 44m 54.86s + 42◦ 58´16.89˝ (J2000), within the galaxy cluster RXC J0844.9+4258. The object was spectroscopically classified as the first Type Ibn SN discovered by Pan-STARRS1 after just ∼ 2 years of survey operation. At z = 0.054, PS1-12sk is more distant than any previously discovered SN Ibn.12 ...
Galaxies
... The radiation from these galaxies is called nonstellar radiation Many luminous galaxies are experiencing an outburst of star formation, probably due to interactions with a neighbor These galaxies are called starburst galaxies, and we will discuss them later The galaxies we will discuss now are those ...
... The radiation from these galaxies is called nonstellar radiation Many luminous galaxies are experiencing an outburst of star formation, probably due to interactions with a neighbor These galaxies are called starburst galaxies, and we will discuss them later The galaxies we will discuss now are those ...
SXDS Highlights : Subaru / FOCAS Spectroscopy
... Natural guide star AO system on Subaru telescope with IRCS. 154 hours of observation in total. 13 FoVs with 36 LBGs , 1 RadioG., and 7 DRGs are observed. Typical on-source effective integration is 5 hours. Typical PSF size at the target position is FWHM=0.2” (~1.5kpc@z=3) ...
... Natural guide star AO system on Subaru telescope with IRCS. 154 hours of observation in total. 13 FoVs with 36 LBGs , 1 RadioG., and 7 DRGs are observed. Typical on-source effective integration is 5 hours. Typical PSF size at the target position is FWHM=0.2” (~1.5kpc@z=3) ...
Astronomy Astrophysics Circumstellar emission in Be/X-ray binaries of the Magellanic
... In order to be able to decouple the interstellar reddening and extinction from the circumstellar reddening and brightening1 we need a set of programme stars with well-known distances and interstellar reddenings as well as good determinations of the spectral types. In principle we could choose Be/X-r ...
... In order to be able to decouple the interstellar reddening and extinction from the circumstellar reddening and brightening1 we need a set of programme stars with well-known distances and interstellar reddenings as well as good determinations of the spectral types. In principle we could choose Be/X-r ...
The Formation and Survival of Discs in a Lambda
... spheroids and very small discs, and one is a spheroidal galaxy with no disc at all. The z = 0 spheroids are made of old stars, while discs are younger and formed from the inside-out. Neither the existence of a disc at z = 0 nor the final disc-to-total mass ratio seems to depend on the spin parameter ...
... spheroids and very small discs, and one is a spheroidal galaxy with no disc at all. The z = 0 spheroids are made of old stars, while discs are younger and formed from the inside-out. Neither the existence of a disc at z = 0 nor the final disc-to-total mass ratio seems to depend on the spin parameter ...
transcript.
... and a half billion light years away, with a giant blast of energy spewing from the center. ...
... and a half billion light years away, with a giant blast of energy spewing from the center. ...
2P28.pdf
... 1995). Does this trend tra e the growth of bulges via satellite a retion? And, is satellite infall onsistent with this trend? Aguerri, Bal ells, & Peletier (2001) (ABP01, hereandafter) investigated this question with N-body simulations of the a retion of dense, spheroidal satellites. Here, we exp ...
... 1995). Does this trend tra e the growth of bulges via satellite a retion? And, is satellite infall onsistent with this trend? Aguerri, Bal ells, & Peletier (2001) (ABP01, hereandafter) investigated this question with N-body simulations of the a retion of dense, spheroidal satellites. Here, we exp ...
Ground-Based Astrometry 2010-2020
... • What are the shape, size, and mass of the Milky Way? Recent improvements in radio astrometry with the VLBA have yielded parallaxes and proper motions to star forming regions across a significant portion of the Milky Way with accuracies of ∼10 µas and a ∼1 km/s, respectively (Reid et al. 2008). In ...
... • What are the shape, size, and mass of the Milky Way? Recent improvements in radio astrometry with the VLBA have yielded parallaxes and proper motions to star forming regions across a significant portion of the Milky Way with accuracies of ∼10 µas and a ∼1 km/s, respectively (Reid et al. 2008). In ...
PoS(EVN 2014)058 - Proceeding of science
... Recent results have strongly challenged the current models and it is now recognised that there is significant discord in our understanding of mass-loss results from clumped and/or porous radiation driven winds (e.g. [7, 8]). This has far reaching consequences for the evolution and fate of massive st ...
... Recent results have strongly challenged the current models and it is now recognised that there is significant discord in our understanding of mass-loss results from clumped and/or porous radiation driven winds (e.g. [7, 8]). This has far reaching consequences for the evolution and fate of massive st ...
20_Testbank
... expect them all to have the same luminosity; observations of white-dwarf supernovae for which we can measure distance independently confirm that they all have the same luminosity. Since we can assume we know their luminosity, we can use their apparent brightnesses to determine distance from the lumi ...
... expect them all to have the same luminosity; observations of white-dwarf supernovae for which we can measure distance independently confirm that they all have the same luminosity. Since we can assume we know their luminosity, we can use their apparent brightnesses to determine distance from the lumi ...
Chemical abundances and winds of massive stars in M31: a B
... compared to OB 10-64. These two stars have essentially little or no internal LMC extinction and the E(B-V) values (0.06 and 0.10 respectively) reflect the reddening from intervening Galactic material. This Milky Way extinction is similar to what we expect for the OB 10-64. Using these two stars and ...
... compared to OB 10-64. These two stars have essentially little or no internal LMC extinction and the E(B-V) values (0.06 and 0.10 respectively) reflect the reddening from intervening Galactic material. This Milky Way extinction is similar to what we expect for the OB 10-64. Using these two stars and ...
Physics of the Interstellar and Intergalactic Medium
... 2.1 Consider an electron-proton plasma at temperature T . Let ts (e − e) be the time scale for 90 degree scattering of one electron with kinetic energy ∼ kT by encounters with other electrons. The electron-proton mass ratio mp /me = 1836. The following time scales tx will differ from ts (e − e) by f ...
... 2.1 Consider an electron-proton plasma at temperature T . Let ts (e − e) be the time scale for 90 degree scattering of one electron with kinetic energy ∼ kT by encounters with other electrons. The electron-proton mass ratio mp /me = 1836. The following time scales tx will differ from ts (e − e) by f ...
ALFALFA H-alpha: The Star-Formation-Rate Density
... For astronomers studying past star-formation rates (SFRs), distances play the role of a time machine. Light travels at a finite speed; it travels slowly enough that astronomers can still view light from the Big Bang. Light emitted by the Sun takes more than eight minutes to reach Earth, roughly five ...
... For astronomers studying past star-formation rates (SFRs), distances play the role of a time machine. Light travels at a finite speed; it travels slowly enough that astronomers can still view light from the Big Bang. Light emitted by the Sun takes more than eight minutes to reach Earth, roughly five ...
M sun
... Pistol star: initial mass ~ 200 Msun (but too metal rich to collapse into a BH) R145 in 30 Dor: M sin3i = (140 +/- 37) Msun ...
... Pistol star: initial mass ~ 200 Msun (but too metal rich to collapse into a BH) R145 in 30 Dor: M sin3i = (140 +/- 37) Msun ...
F P US R
... 2.1.1 Measuring H0 directly from observations of H2O masers orbiting active galactic nuclei The Seyfert 2 galaxy NGC 4258 has a sub-pc scale accretion disk in its nucleus that can be traced by VLBI imaging of its H2O maser emission. Hernstein et al (1999, Nature, 400, 539) determined a highly accura ...
... 2.1.1 Measuring H0 directly from observations of H2O masers orbiting active galactic nuclei The Seyfert 2 galaxy NGC 4258 has a sub-pc scale accretion disk in its nucleus that can be traced by VLBI imaging of its H2O maser emission. Hernstein et al (1999, Nature, 400, 539) determined a highly accura ...
Dust in the Circumgalactic Medium of Low
... cold dust is seen up to 20 kpc from the center of M82. Using UV light scattered by dust grains, Hodges-Kluck & Bregman (2014) reported the detection of dust up to about 20 kpc perpendicular to the disk of edge-on galaxies. With a statistical approach, Ménard et al. (2010, MSFR) measured the cross-c ...
... cold dust is seen up to 20 kpc from the center of M82. Using UV light scattered by dust grains, Hodges-Kluck & Bregman (2014) reported the detection of dust up to about 20 kpc perpendicular to the disk of edge-on galaxies. With a statistical approach, Ménard et al. (2010, MSFR) measured the cross-c ...
How To Find Newborn Black Holes Kazumi Kashiyama (UCB)
... Mass loss was included in the calculation, but due to the low metallicity, only 0.05 M⊙ and 0.15 M⊙ was lost in V24 and V36, respectively. Note that, if all the surface material accreted here, the black hole would rotate at nearly its maximum allowed value (i.e., the red line intersects the green on ...
... Mass loss was included in the calculation, but due to the low metallicity, only 0.05 M⊙ and 0.15 M⊙ was lost in V24 and V36, respectively. Note that, if all the surface material accreted here, the black hole would rotate at nearly its maximum allowed value (i.e., the red line intersects the green on ...
What Gaia can reveal about the matter distribution in the Milky Way
... understood. A clue towards better understanding in these fields could be found by more accurately probing the current Galactic structure and matter distribution. This because knowledge of the matter distribution is a prerequisite for analysing all sorts of dynamical phenomena (that depend on the Gal ...
... understood. A clue towards better understanding in these fields could be found by more accurately probing the current Galactic structure and matter distribution. This because knowledge of the matter distribution is a prerequisite for analysing all sorts of dynamical phenomena (that depend on the Gal ...
Stars and Galaxies - Red Hook Central Schools
... http://hubblesite.org/newscenter/archive/releases/star/supernova/2004/09/results/50/ http://hubblesite.org/newscenter/archive/releases/nebula/supernova-remnant/2005/37/results/50/ http://chandra.harvard.edu/photo/2009/casa/ ...
... http://hubblesite.org/newscenter/archive/releases/star/supernova/2004/09/results/50/ http://hubblesite.org/newscenter/archive/releases/nebula/supernova-remnant/2005/37/results/50/ http://chandra.harvard.edu/photo/2009/casa/ ...
outer-disk populations in ngc 7793: evidence for stellar
... a dependence on environment is to be expected. This was further demonstrated by Gogarten et al. (2010), who note that the comparably massive M 33, which is interacting with M31, does show signs of radial diffusion (Williams et al. 2009). We extend this analysis by observing that the K-band absolute ...
... a dependence on environment is to be expected. This was further demonstrated by Gogarten et al. (2010), who note that the comparably massive M 33, which is interacting with M31, does show signs of radial diffusion (Williams et al. 2009). We extend this analysis by observing that the K-band absolute ...
Can we account for the dust
... Mid- and far-IR emission of galaxies ◦ Thermal emission from dust grains ...
... Mid- and far-IR emission of galaxies ◦ Thermal emission from dust grains ...