The low dark matter content of the lenticular galaxy NGC 3998
... mergers are one possibility (Querejeta et al. 2015), but simulations of repeated minor mergers have also produced realistic galaxies (Bournaud, Jog & Combes 2007). The star formation rate of starforming galaxies in groups shows no evidence of being globally lower than for star-forming galaxies in th ...
... mergers are one possibility (Querejeta et al. 2015), but simulations of repeated minor mergers have also produced realistic galaxies (Bournaud, Jog & Combes 2007). The star formation rate of starforming galaxies in groups shows no evidence of being globally lower than for star-forming galaxies in th ...
HD 100453: An Evolutionary link between
... Meeus suggested star and disk evolution may be decoupled for this sample We find that the star, accretion rate, and disk evolve together. We conclude that the hypothesis suggesting Meeus Group I sources evolve to Meeus Group II sources does not hold. ...
... Meeus suggested star and disk evolution may be decoupled for this sample We find that the star, accretion rate, and disk evolve together. We conclude that the hypothesis suggesting Meeus Group I sources evolve to Meeus Group II sources does not hold. ...
10-Jets and outflows
... on the opposite side red shifted. This, in itself, does not require the gas to be part of an outflow but other factors leave no other option open. For example, the radial speeds implied by the line shifts are often of the order of tens of km s−1 on scales larger than 0.1 pc. Such speeds can only be ...
... on the opposite side red shifted. This, in itself, does not require the gas to be part of an outflow but other factors leave no other option open. For example, the radial speeds implied by the line shifts are often of the order of tens of km s−1 on scales larger than 0.1 pc. Such speeds can only be ...
Document
... loose energy through gravitational waves • The 2 objects will get closer until tidal forces rip the NS apart and matter falls into a BH. • The process has ms timescale • Evidence for the merger model are less striking: ...
... loose energy through gravitational waves • The 2 objects will get closer until tidal forces rip the NS apart and matter falls into a BH. • The process has ms timescale • Evidence for the merger model are less striking: ...
Abstract book
... Title: Asymptotic Giant Branch stars in intermediate age clusters Abstract. Spectroscopic and photometric observations of AGB stars belonging to intermediate age clusters (1 to 3 Gyrs) represent one of the most challenging test for the theory of AGB evolution and nucleosynthesis. Their masses (1.3 t ...
... Title: Asymptotic Giant Branch stars in intermediate age clusters Abstract. Spectroscopic and photometric observations of AGB stars belonging to intermediate age clusters (1 to 3 Gyrs) represent one of the most challenging test for the theory of AGB evolution and nucleosynthesis. Their masses (1.3 t ...
Chemical composition of 90 F and G disk dwarfs
... provide a powerful way to probe the chemical and dynamical evolution of the Galaxy. As far as the disk stars are concerned, many general trends have been discovered during the past decades. Most notable results are correlations of metallicity with age, Galactocentric distance, and vertical distance ...
... provide a powerful way to probe the chemical and dynamical evolution of the Galaxy. As far as the disk stars are concerned, many general trends have been discovered during the past decades. Most notable results are correlations of metallicity with age, Galactocentric distance, and vertical distance ...
Science with the Constellation
... The high throughput and broad-band response of Constellation-X will allow us to utilize the iron-line diagnostic in an unprecedented manner. Observations of many individual sources will allow us to develop a statistical picture of the material surrounding the central black hole. We will search for a ...
... The high throughput and broad-band response of Constellation-X will allow us to utilize the iron-line diagnostic in an unprecedented manner. Observations of many individual sources will allow us to develop a statistical picture of the material surrounding the central black hole. We will search for a ...
Galaxies
... underlying dark matter. We have started to understand how baryonic gas within the dark matter halos cools and collapses to form stars, and how the energy from star formation can feed back into the surrounding gas and regulate subsequent star formation. However, at a fundamental level we still lack a ...
... underlying dark matter. We have started to understand how baryonic gas within the dark matter halos cools and collapses to form stars, and how the energy from star formation can feed back into the surrounding gas and regulate subsequent star formation. However, at a fundamental level we still lack a ...
STELLAR AGE VERSUS MASS OF EARLY
... performed visually by allowing age steps of 0.05 dex. The age range was then kept fixed for the other colors (middle and bottom panel). We see from the top panel of Fig. 2 that the SSP of HPL07 exceeds the observed color range at intermediate ages. This is no surprise, though: since the reddest colo ...
... performed visually by allowing age steps of 0.05 dex. The age range was then kept fixed for the other colors (middle and bottom panel). We see from the top panel of Fig. 2 that the SSP of HPL07 exceeds the observed color range at intermediate ages. This is no surprise, though: since the reddest colo ...
Masses of Dwarf Satellites of the Milky Way
... Fig. 1.— Projected velocity dispersion profiles for eight bright dSphs, from Magellan/MMFS and MMT/Hectochelle data. Over-plotted are profiles calculated from isothermal, power-law, NFW and cored halos considered as prospective “universal” dSph halos (Section 5). For each type of halo we fit only fo ...
... Fig. 1.— Projected velocity dispersion profiles for eight bright dSphs, from Magellan/MMFS and MMT/Hectochelle data. Over-plotted are profiles calculated from isothermal, power-law, NFW and cored halos considered as prospective “universal” dSph halos (Section 5). For each type of halo we fit only fo ...
A Spectroscopically Confirmed Excess of 24 micron Sources in a
... understanding the interplay between galaxy evolution and environment is to study galaxy groups because: 1) most galaxies in the local universe are in groups (e.g. Geller & Huchra 1983); and 2) hierarchical structure formation predicts that galaxy clusters assemble from the merger and accretion of sm ...
... understanding the interplay between galaxy evolution and environment is to study galaxy groups because: 1) most galaxies in the local universe are in groups (e.g. Geller & Huchra 1983); and 2) hierarchical structure formation predicts that galaxy clusters assemble from the merger and accretion of sm ...
Multiwavelength properties of γ-ray loud binary systems.
... The excess variability is not centered at the Galactic Center itself, but traces the part of the Galactic Plane at positive Galactic longitude 0○ < l < 7○ dominated by the diffuse emission, with no clearly isolated bright sources. The end part of the variable region, with the brightest excess at the ...
... The excess variability is not centered at the Galactic Center itself, but traces the part of the Galactic Plane at positive Galactic longitude 0○ < l < 7○ dominated by the diffuse emission, with no clearly isolated bright sources. The end part of the variable region, with the brightest excess at the ...
Astronomy 140 Lecture Notes, Spring 2008 c
... then cools off as the core burning stops. The once again red star then goes to higher luminosity on the asymptotic giant brach (AGB). Finally they eject their envelopes and become planetary nebulae. The gas dissipates and only the central star, which was the core of the star, remains. This just cool ...
... then cools off as the core burning stops. The once again red star then goes to higher luminosity on the asymptotic giant brach (AGB). Finally they eject their envelopes and become planetary nebulae. The gas dissipates and only the central star, which was the core of the star, remains. This just cool ...
P7 Further Physics
... 2x10-18s-1 calculate how fast that galaxy is moving. 2) Another galaxy is 10Mpc from Earth. Taking H to be 75kms-1Mpc-1 calculate its recessional velocity. 3) Another galaxy has a recessional velocity of 500km/s. Calculate the distance to the galaxy in both megaparsecs and kilometres (take H to be 2 ...
... 2x10-18s-1 calculate how fast that galaxy is moving. 2) Another galaxy is 10Mpc from Earth. Taking H to be 75kms-1Mpc-1 calculate its recessional velocity. 3) Another galaxy has a recessional velocity of 500km/s. Calculate the distance to the galaxy in both megaparsecs and kilometres (take H to be 2 ...
The physics and modes of star cluster formation: observations
... their formation and early evolution, are completely embedded in molecular gas and dust. They are thus obscured from view at optical wavelengths, where the traditional astronomical techniques are most effective. Fortunately, molecular clouds are considerably less opaque at infrared wavelengths and th ...
... their formation and early evolution, are completely embedded in molecular gas and dust. They are thus obscured from view at optical wavelengths, where the traditional astronomical techniques are most effective. Fortunately, molecular clouds are considerably less opaque at infrared wavelengths and th ...
The molecular disk surrounding the protostellar binary L1551 IRS5
... Saito et al. (1996). When those data are convolved with our beam the agreement is perfect. The flattened structure can be traced in the position-velocity diagrams of Fig. 2 for at least 10000 , thus indicating a structure larger than what can be discerned from the interferometric observations which ...
... Saito et al. (1996). When those data are convolved with our beam the agreement is perfect. The flattened structure can be traced in the position-velocity diagrams of Fig. 2 for at least 10000 , thus indicating a structure larger than what can be discerned from the interferometric observations which ...
Lives of Stars - Astronomy Outreach
... IANA: To put it another way, the speed of the atoms zipping around increased. But as all the gas moved toward the same central point, the volume of the whole cloud decreased. You would think that as the temperature of the gas increased, the cloud would expand. But because there was so much gas, and ...
... IANA: To put it another way, the speed of the atoms zipping around increased. But as all the gas moved toward the same central point, the volume of the whole cloud decreased. You would think that as the temperature of the gas increased, the cloud would expand. But because there was so much gas, and ...
FLARE SWG theme 3: high
... Other “environment” measures of first quasars with FLARE: Large-scale clustering analyses with respect to galaxies – bias and constraints on BH seed formation? Mpc-scale environment around first quasars using FLARE IFU: co-eval galaxy and other z>6 quasar/AGN connections (multiple growing BHs)? Evid ...
... Other “environment” measures of first quasars with FLARE: Large-scale clustering analyses with respect to galaxies – bias and constraints on BH seed formation? Mpc-scale environment around first quasars using FLARE IFU: co-eval galaxy and other z>6 quasar/AGN connections (multiple growing BHs)? Evid ...
Environmental dependence of bulge
... will further expand on this point in Section 4.4. In Huertas-Company et al. (2013a) we used the above defined sample of z ∼ 0 SDSS early-type galaxies to point out a negligible dependence of the sizes on environment, at fixed stellar mass. More specifically, we were able to demonstrate via detailed ...
... will further expand on this point in Section 4.4. In Huertas-Company et al. (2013a) we used the above defined sample of z ∼ 0 SDSS early-type galaxies to point out a negligible dependence of the sizes on environment, at fixed stellar mass. More specifically, we were able to demonstrate via detailed ...
PPT presentation
... The contamination increases with distance to the galaxy. It is negligible for distances < 10 Mpc, as we just saw. At the distance of the Virgo cluster the luminosity function of the contaminants imitates the PNLF of a low-surfacedensity PN population at that distance. This produced some confusion in ...
... The contamination increases with distance to the galaxy. It is negligible for distances < 10 Mpc, as we just saw. At the distance of the Virgo cluster the luminosity function of the contaminants imitates the PNLF of a low-surfacedensity PN population at that distance. This produced some confusion in ...
Zhu Qualifier Solutions - University of Toronto Astronomy
... 1.4.5. How can the power spectrum be observed? 1.4.6. How can the power spectrum constrain cosmological parameters? 1.4.7. How can we determine the dark matter mass function from perturbation analysis? 1.5. Question 4 1.5.1. What is Olbers’s Paradox? 1.5.2. Are there Big Bang-less cosmologies? 1.6. ...
... 1.4.5. How can the power spectrum be observed? 1.4.6. How can the power spectrum constrain cosmological parameters? 1.4.7. How can we determine the dark matter mass function from perturbation analysis? 1.5. Question 4 1.5.1. What is Olbers’s Paradox? 1.5.2. Are there Big Bang-less cosmologies? 1.6. ...
Distance determination for RAVE stars using stellar models
... used to illuminate a host of substructures in the Galactic halo. The strength of photometric distances is that they can be constructed for a wide range of stellar populations. An important recent study was carried out by Ivezić et al. (2008). In this work they took high-precision multi-band optical ...
... used to illuminate a host of substructures in the Galactic halo. The strength of photometric distances is that they can be constructed for a wide range of stellar populations. An important recent study was carried out by Ivezić et al. (2008). In this work they took high-precision multi-band optical ...
arXiv:astro-ph/9712176v1 15 Dec 1997
... dispersion direction, which depends slightly on the wavelength. Following Gonzales (1993), this effect is only detectable if the variation of the focus’ point spread function (PSF) is dominant compared to the atmospherical seeing (FWHM). For NGC 4816 the focus variation was the dominant effect and w ...
... dispersion direction, which depends slightly on the wavelength. Following Gonzales (1993), this effect is only detectable if the variation of the focus’ point spread function (PSF) is dominant compared to the atmospherical seeing (FWHM). For NGC 4816 the focus variation was the dominant effect and w ...
The dark matter crisis: falsification of the current standard model of
... perhaps gas is a galaxy if its Newtonian median twobody relaxation time is longer than the Hubble time, trel > τH ≈ 104 Myr. This definition of a galaxy (Kroupa 1998, 2008; Forbes & Kroupa 2011) naturally accounts for the dynamical process of energy equipartition not playing a role in galaxies over t ...
... perhaps gas is a galaxy if its Newtonian median twobody relaxation time is longer than the Hubble time, trel > τH ≈ 104 Myr. This definition of a galaxy (Kroupa 1998, 2008; Forbes & Kroupa 2011) naturally accounts for the dynamical process of energy equipartition not playing a role in galaxies over t ...
Farthest Neighbor: The Distant Milky Way Satellite Eridanus II
... star formation (de Jong et al. 2008; Weisz et al. 2012). If this were the case, EriII would be the least luminous star-forming galaxy known. However, Westmeier et al. (2015) measured the H I gas content using HIPASS data (Barnes et al. 2001) and did not detect any H I gas associated with EriII. Cr ...
... star formation (de Jong et al. 2008; Weisz et al. 2012). If this were the case, EriII would be the least luminous star-forming galaxy known. However, Westmeier et al. (2015) measured the H I gas content using HIPASS data (Barnes et al. 2001) and did not detect any H I gas associated with EriII. Cr ...