Massive Star Formation in the Galactic Center
... and evolution models. It contains 10% of the present star formation activity in the Galaxy, yet fills only a tiny fraction of a percent of the volume in the Galactic disk†. The initial conditions for star formation in the GC are unique in the Galaxy. The molecular clouds in the region are extraordina ...
... and evolution models. It contains 10% of the present star formation activity in the Galaxy, yet fills only a tiny fraction of a percent of the volume in the Galactic disk†. The initial conditions for star formation in the GC are unique in the Galaxy. The molecular clouds in the region are extraordina ...
Neutron Stars – Cooling and Transport
... 2.8 × 1014 g cm−3 is the nuclear saturation density (the typical density of a heavy atomic nucleus). It is usually several kilometers thick and contains most of the stellar mass. The outer core is mostly composed of neutrons with an admixture of the protons and leptons – electrons and muons (npeµ ma ...
... 2.8 × 1014 g cm−3 is the nuclear saturation density (the typical density of a heavy atomic nucleus). It is usually several kilometers thick and contains most of the stellar mass. The outer core is mostly composed of neutrons with an admixture of the protons and leptons – electrons and muons (npeµ ma ...
Stars, Galaxies, and Beyond
... Pearson/Addison Wesley, hereafter abbreviated IMA2. References herein to chapters refer to that textbook, but a great deal of information I have included under these chapter headings is from the lectures and especially from other sources, so may not have been stated as such in the textbook (nor have ...
... Pearson/Addison Wesley, hereafter abbreviated IMA2. References herein to chapters refer to that textbook, but a great deal of information I have included under these chapter headings is from the lectures and especially from other sources, so may not have been stated as such in the textbook (nor have ...
Insights into thermonuclear supernovae from the incomplete Si
... young SNIa remnants and the metallicity of the WD progenitor, which allowed them to conclude that the metallicity of the progenitor of Tycho’s supernova is supersolar. The same technique has been since applied to other suspected SNIa remnants to determine their progenitors’ metallicity. The picture ...
... young SNIa remnants and the metallicity of the WD progenitor, which allowed them to conclude that the metallicity of the progenitor of Tycho’s supernova is supersolar. The same technique has been since applied to other suspected SNIa remnants to determine their progenitors’ metallicity. The picture ...
distribution and properties of a sample of massive young stars
... of our campaign as without these we cannot accurately calculate source luminosities, and thus, distinguish between nearby low and intermediate-mass YSOs from the more generally more distance MYSOs. As mentioned in the introduction, kinematic distance ambiguities affect a large proportion of our samp ...
... of our campaign as without these we cannot accurately calculate source luminosities, and thus, distinguish between nearby low and intermediate-mass YSOs from the more generally more distance MYSOs. As mentioned in the introduction, kinematic distance ambiguities affect a large proportion of our samp ...
X-ray binaries in the Milky Way and other galaxies
... 5.1.3. Star formation rate estimates . 5.1.4. Contribution of a central AGN 5.1.5. Contribution of LMXBs . . . . ...
... 5.1.3. Star formation rate estimates . 5.1.4. Contribution of a central AGN 5.1.5. Contribution of LMXBs . . . . ...
The Emission Line Spectrum of Active Galactic
... the variability time-scale and the ionization parameter. However, these requirements can also be fulfilled if the lines are emitted by a continuous medium whose thickness is much smaller than its lateral dimension, for instance a thin disk or the atmosphere of a disk. Assuming that the velocity is K ...
... the variability time-scale and the ionization parameter. However, these requirements can also be fulfilled if the lines are emitted by a continuous medium whose thickness is much smaller than its lateral dimension, for instance a thin disk or the atmosphere of a disk. Assuming that the velocity is K ...
DTU Chap 16 Galaxies v2
... Pairs of colliding galaxies often exhibit long “antennae” of stars ejected by the collision. This particular system is known as NGC 4676 or “the Mice” (because of its tails of stars and gas). It is 300 million light-years from Earth in the constellation Coma Berenices. The collision has stimulated a ...
... Pairs of colliding galaxies often exhibit long “antennae” of stars ejected by the collision. This particular system is known as NGC 4676 or “the Mice” (because of its tails of stars and gas). It is 300 million light-years from Earth in the constellation Coma Berenices. The collision has stimulated a ...
Double relics in Abell 2345 and Abell 1240
... The hierarchical model of structure formation predicts that clusters of galaxies form by subsequent merging of smaller structures. A consistent amount of energy (∼1063 −1064 erg) is released in the intra cluster medium (ICM) as result of such merger events. Cosmological numerical simulations have sh ...
... The hierarchical model of structure formation predicts that clusters of galaxies form by subsequent merging of smaller structures. A consistent amount of energy (∼1063 −1064 erg) is released in the intra cluster medium (ICM) as result of such merger events. Cosmological numerical simulations have sh ...
discovery of four new massive and dense cold cores
... temperature, determined from Gaussian fits to the spectra, are given in columns (6)–(8) of Table 1, respectively. The line widths are broad, typically 4 km s1, much larger than the thermal widths, indicating that these cores are highly turbulent and implying that their mean pressures are very high ...
... temperature, determined from Gaussian fits to the spectra, are given in columns (6)–(8) of Table 1, respectively. The line widths are broad, typically 4 km s1, much larger than the thermal widths, indicating that these cores are highly turbulent and implying that their mean pressures are very high ...
Stars, neutral hydrogen and ionised gas in early
... for the study of the relation between stellar and H i properties in early-type galaxies. We characterised the environment of IC 4200 by looking for extragalactic objects within 100 arcmin (∼1.6 Mpc at this redshift) and 300 km/s from the galaxy; for this search we used the Nasa Extragalactic Databas ...
... for the study of the relation between stellar and H i properties in early-type galaxies. We characterised the environment of IC 4200 by looking for extragalactic objects within 100 arcmin (∼1.6 Mpc at this redshift) and 300 km/s from the galaxy; for this search we used the Nasa Extragalactic Databas ...
... Therefore, any probe of star formation which is insensitive to the obscuring effects of dust will have a tremendous advantage. Such a transparent view of the high z Universe is provided by sub-mm and mm observations, which now have the instrumental sensitivity (e.g., SCUBA, MAMBO) to detect the form ...
How special are brightest group and cluster galaxies?
... candidate(s), this becomes third BCG candidate. If the first=second=third candidate, then it is BCG. (242 obj) Other cases, the candidates are inspected visually on 2.5’’×2.5’’ color images from DR4 CAS. (472) Other cases, inspected visually on color images(only <2Mpc, ...
... candidate(s), this becomes third BCG candidate. If the first=second=third candidate, then it is BCG. (242 obj) Other cases, the candidates are inspected visually on 2.5’’×2.5’’ color images from DR4 CAS. (472) Other cases, inspected visually on color images(only <2Mpc, ...
The Spitzer/GLIMPSE Surveys - UW-Madison Astronomy
... EGOs are located toward IRDCs and, where the coverage of Class II 6.7 GHz CH3 OH maser surveys overlaps that of GLIMPSE I, EGOs and 6.7 GHz CH3 OH masers are strongly correlated (Cyganowski et al. 2008). Class II methanol masers are radiatively excited by IR photons from warm dust heated by the cent ...
... EGOs are located toward IRDCs and, where the coverage of Class II 6.7 GHz CH3 OH maser surveys overlaps that of GLIMPSE I, EGOs and 6.7 GHz CH3 OH masers are strongly correlated (Cyganowski et al. 2008). Class II methanol masers are radiatively excited by IR photons from warm dust heated by the cent ...
Galaxies at High Redshift Encyclopedia of Astronomy & Astrophysics eaa.iop.org Mauro Giavalisco
... of light is that the light emitted from any given galaxy is observed by a remote observer (i.e. one located on a different galaxy, for example the Milky Way) as having a longer wavelength than it had at the emission. This is because the cosmic expansion has caused the space between the two galaxies ...
... of light is that the light emitted from any given galaxy is observed by a remote observer (i.e. one located on a different galaxy, for example the Milky Way) as having a longer wavelength than it had at the emission. This is because the cosmic expansion has caused the space between the two galaxies ...
Crash Galaxies
... occurrence. Yet no galaxies seem to be near enough to have produced that effect through recent gravitational interaction (Ferris 1982, p. 72). Experts suggest that possibly this galaxy has, at some time in her history, taken a massive cloud of intergalactic gas and dust as her dance partner, only to ...
... occurrence. Yet no galaxies seem to be near enough to have produced that effect through recent gravitational interaction (Ferris 1982, p. 72). Experts suggest that possibly this galaxy has, at some time in her history, taken a massive cloud of intergalactic gas and dust as her dance partner, only to ...
New brown dwarfs and giant planets
... ~50% trig/50% photo parallaxes Proper motions for all (U, V, W) velocities ...
... ~50% trig/50% photo parallaxes Proper motions for all (U, V, W) velocities ...
$^{13} $ CO/C $^{18} $ O Gradients Across the Disks of Nearby
... The other two, NGC 2903 and NGC 3184, show only weak emission and we place lower limits on 13 CO/C18 O in these systems. We recover the C18 O line in all four ALMA targets. Table 2 reports our measured 13 CO/C18 O ratios of line-integrated intensities on the Tmb scale. For each target, we quote the ...
... The other two, NGC 2903 and NGC 3184, show only weak emission and we place lower limits on 13 CO/C18 O in these systems. We recover the C18 O line in all four ALMA targets. Table 2 reports our measured 13 CO/C18 O ratios of line-integrated intensities on the Tmb scale. For each target, we quote the ...
- Haverford Scholarship
... greater than six, simulations are consistent with optical follow-up that demonstrated this subsample is 100% pure. The simulations further imply that the total sample is 80% complete for clusters with mass in excess of 6 × 1014 solar masses referenced to the cluster volume characterized by 500 times ...
... greater than six, simulations are consistent with optical follow-up that demonstrated this subsample is 100% pure. The simulations further imply that the total sample is 80% complete for clusters with mass in excess of 6 × 1014 solar masses referenced to the cluster volume characterized by 500 times ...
Numerical Star-Formation Studies-
... The formation of stars is a key process in astrophysics. Detailed knowledge of the physical mechanisms that govern stellar birth is a prerequisite for understanding the formation and evolution of our galactic home, the Milky Way. A theory of star formation is an essential part of any model for the o ...
... The formation of stars is a key process in astrophysics. Detailed knowledge of the physical mechanisms that govern stellar birth is a prerequisite for understanding the formation and evolution of our galactic home, the Milky Way. A theory of star formation is an essential part of any model for the o ...
The life-cycle of star formation in distant clusters
... The life-cycle of star formation in distant clusters sequence to the remnant phase. One possible drawback is that the models assume solar metallicity, thereby neglecting chemical evolution effects; however, as we are primarily concerned with testing short-term changes to old wellestablished galaxies ...
... The life-cycle of star formation in distant clusters sequence to the remnant phase. One possible drawback is that the models assume solar metallicity, thereby neglecting chemical evolution effects; however, as we are primarily concerned with testing short-term changes to old wellestablished galaxies ...
ongoing massive star formation in the bulge of m511 hjglm lamers,2
... e.g., Millard et al. 1999). The galaxy was observed through the broadband Ðlters F255W and F336W in 1994 and through the broadband Ðlters F439W, F555W, F675W, and F814W in 1995. We will refer to these Ðlters as the UV, U, B, V , R, and I Ðlters. The observations in the UV, U, and B Ðlters were split ...
... e.g., Millard et al. 1999). The galaxy was observed through the broadband Ðlters F255W and F336W in 1994 and through the broadband Ðlters F439W, F555W, F675W, and F814W in 1995. We will refer to these Ðlters as the UV, U, B, V , R, and I Ðlters. The observations in the UV, U, and B Ðlters were split ...
The effect of the environment on the HI scaling relations
... existence of a ‘gas fraction plane’ linking Hi gas fraction2 to stellar mass surface density and N U V − r colour and proposed to use this plane to isolate interesting outliers that might be in the process of accreting or loosing a significant fraction of their gas content. In this context, the plan ...
... existence of a ‘gas fraction plane’ linking Hi gas fraction2 to stellar mass surface density and N U V − r colour and proposed to use this plane to isolate interesting outliers that might be in the process of accreting or loosing a significant fraction of their gas content. In this context, the plan ...
PowerPoint file - Departament d`Astronomia i Meteorologia
... inside the IRAS ellipsoid error: IRS 1 and IRS 3. With the SMA observations, we have discovered a high-velocity bipolar outflow in the EW direction clearly associated with IRS 1, the most embedded source in the region. Surprisingly, only weak continuum emission is found toward IRS 1, and the stronge ...
... inside the IRAS ellipsoid error: IRS 1 and IRS 3. With the SMA observations, we have discovered a high-velocity bipolar outflow in the EW direction clearly associated with IRS 1, the most embedded source in the region. Surprisingly, only weak continuum emission is found toward IRS 1, and the stronge ...
Astrophysical X-ray source
Astrophysical X-ray sources are astronomical objects with physical properties which result in the emission of X-rays.There are a number of types of astrophysical objects which emit X-rays, from galaxy clusters, through black holes in active galactic nuclei (AGN) to galactic objects such as supernova remnants, stars, and binary stars containing a white dwarf (cataclysmic variable stars and super soft X-ray sources), neutron star or black hole (X-ray binaries). Some solar system bodies emit X-rays, the most notable being the Moon, although most of the X-ray brightness of the Moon arises from reflected solar X-rays. A combination of many unresolved X-ray sources is thought to produce the observed X-ray background. The X-ray continuum can arise from bremsstrahlung, either magnetic or ordinary Coulomb, black-body radiation, synchrotron radiation, inverse Compton scattering of lower-energy photons be relativistic electrons, knock-on collisions of fast protons with atomic electrons, and atomic recombination, with or without additional electron transitions.Furthermore, celestial entities in space are discussed as celestial X-ray sources. The origin of all observed astronomical X-ray sources is in, near to, or associated with a coronal cloud or gas at coronal cloud temperatures for however long or brief a period.