![Determination of the position angle of stellar spin axes](http://s1.studyres.com/store/data/014539615_1-2c70d6793c545b0603fcfac0319ff16f-300x300.png)
Determination of the position angle of stellar spin axes
... cross-section of the star projected on the sky. The absolute stellar position angle PA star is defined from north to east. The slit is represented by the spatial axis YS , which may not be aligned with the northern axis by an angle PA slit . ψ is the angle formed between the slit axis and the stella ...
... cross-section of the star projected on the sky. The absolute stellar position angle PA star is defined from north to east. The slit is represented by the spatial axis YS , which may not be aligned with the northern axis by an angle PA slit . ψ is the angle formed between the slit axis and the stella ...
The Massive Star Population of Cygnus OB2
... stars have secondaries with known spectral types, although it is likely that there still remain a number of undiscovered binary companions in this sample. For objects with known companions it is possible to correct for the light of the secondary when using the observed photometry as long as the spec ...
... stars have secondaries with known spectral types, although it is likely that there still remain a number of undiscovered binary companions in this sample. For objects with known companions it is possible to correct for the light of the secondary when using the observed photometry as long as the spec ...
YELLOW SUPERGIANTS IN THE ANDROMEDA GALAXY (M31)
... is dominated by foreground contamination, requiring membership to somehow be determined. Fortunately, the large negative systemic velocity of M31, coupled to its high rotation rate, provides the means for separating the contaminating foreground dwarfs from the bona fide yellow supergiants within M31 ...
... is dominated by foreground contamination, requiring membership to somehow be determined. Fortunately, the large negative systemic velocity of M31, coupled to its high rotation rate, provides the means for separating the contaminating foreground dwarfs from the bona fide yellow supergiants within M31 ...
A fundamental metallicity relation for galaxies at z = 0.84–1.47 from
... (NBJ and NBH ), along with the H2 S1 filter in the K band, to undertake panoramic, moderate depth surveys of emission line galaxies. HiZELS targets the Hα emission line redshifted into the nearinfrared at z = 0.84, 1.47 and 2.23 using these filters. In addition, the UKIRT data are complemented by de ...
... (NBJ and NBH ), along with the H2 S1 filter in the K band, to undertake panoramic, moderate depth surveys of emission line galaxies. HiZELS targets the Hα emission line redshifted into the nearinfrared at z = 0.84, 1.47 and 2.23 using these filters. In addition, the UKIRT data are complemented by de ...
Mapping the Pathways of Galaxy Transformation Across Time and
... Is “quenching” the termination of star formation or the compression of star formation histories (SFHs)? I discuss the deep implications this reframing has for what we see as and how we study core processes shaping galaxy life-cycles. As a lens, I use two outcomes from the IMACS Cluster-Building Surv ...
... Is “quenching” the termination of star formation or the compression of star formation histories (SFHs)? I discuss the deep implications this reframing has for what we see as and how we study core processes shaping galaxy life-cycles. As a lens, I use two outcomes from the IMACS Cluster-Building Surv ...
Strongly suggested reading: The stellar halo of the Galaxy
... On the other hand, this of course, is only a sign of the field’s health and its great promise for the young generations of scientists hoping to unravel the formation of the Galaxy. The reader is hereby warned that our understanding of the Galactic halo is still evolving significantly. In an attempt ...
... On the other hand, this of course, is only a sign of the field’s health and its great promise for the young generations of scientists hoping to unravel the formation of the Galaxy. The reader is hereby warned that our understanding of the Galactic halo is still evolving significantly. In an attempt ...
Present
... Masses in red stars range from 8x1010 to 6x1011 Mo, if the mean stellar age is below 109 years, and significantly higher masses if the stars are older. They are probably young massive ellipticals in the final stages of star formation, where much of their stellar mass is already in place, yet very ...
... Masses in red stars range from 8x1010 to 6x1011 Mo, if the mean stellar age is below 109 years, and significantly higher masses if the stars are older. They are probably young massive ellipticals in the final stages of star formation, where much of their stellar mass is already in place, yet very ...
2 Justification and benefits in joining TMT
... reveal that the Universe is dominated by dark matter and dark energy. The nature of these two dark components is the most fundamental question in (astro-)physics today. The discovery of more than 400 extrasolar planet systems indicates that our solar system may be the exception rather than the norm; ...
... reveal that the Universe is dominated by dark matter and dark energy. The nature of these two dark components is the most fundamental question in (astro-)physics today. The discovery of more than 400 extrasolar planet systems indicates that our solar system may be the exception rather than the norm; ...
The binary fractions in the massive young Large Magellanic Cloud
... towards binaries with short periods (Milone et al. 2012) and the relatively high orbital inclinations required to observe at least partial eclipses, which cause variability. Both approaches are hampered by low discovery efficiencies, since they require extensive time-domain observations and, hence, ...
... towards binaries with short periods (Milone et al. 2012) and the relatively high orbital inclinations required to observe at least partial eclipses, which cause variability. Both approaches are hampered by low discovery efficiencies, since they require extensive time-domain observations and, hence, ...
PS1-10jh: The Disruption of a Main-Sequence Star of Near
... Instead, we run two separate simulations that are each wellequipped to describe the behavior of the debris stream at two different epochs. To determine the fate of the debris liberated from a star during a tidal disruption, we used two similar simulation setups, differing only in the mass ratio q. T ...
... Instead, we run two separate simulations that are each wellequipped to describe the behavior of the debris stream at two different epochs. To determine the fate of the debris liberated from a star during a tidal disruption, we used two similar simulation setups, differing only in the mass ratio q. T ...
O stars with weak winds: the Galactic case - Max-Planck
... the broader the profile, the lower the precision of the fit of the line. The typical error on Teff is usually of ± 2000 K but can be reduced when many optical He lines are available. Note that the errors we give are 2σ errors (we have Teff − error < Teff < Teff + error). We also checked that our fin ...
... the broader the profile, the lower the precision of the fit of the line. The typical error on Teff is usually of ± 2000 K but can be reduced when many optical He lines are available. Note that the errors we give are 2σ errors (we have Teff − error < Teff < Teff + error). We also checked that our fin ...
The Panchromatic STARBurst IRregular Dwarf Survey (STARBIRDS
... strength of this HST archival-defined sample is that the dwarf galaxies cover a range in luminosity (−17.94 < MB < −9.80), morphology (SBdm, IAB(s)m, pec, IBm), and metallicity (7.39 ≤ 12+(O/H)≤ 8.38). The majority of the galaxies have high Galactic latitudes and low foreground extinction (i.e., AR ...
... strength of this HST archival-defined sample is that the dwarf galaxies cover a range in luminosity (−17.94 < MB < −9.80), morphology (SBdm, IAB(s)m, pec, IBm), and metallicity (7.39 ≤ 12+(O/H)≤ 8.38). The majority of the galaxies have high Galactic latitudes and low foreground extinction (i.e., AR ...
Imaging and spectroscopy of ejected common envelopes
... abundances in these objects is usually thought to be a late thermal pulse which forced the central star to return to the AGB and a second PN phase (Then et al. 1983). However, there is no clear evidence to support the contention that any of these objects are binaries, and objects such as those hypot ...
... abundances in these objects is usually thought to be a late thermal pulse which forced the central star to return to the AGB and a second PN phase (Then et al. 1983). However, there is no clear evidence to support the contention that any of these objects are binaries, and objects such as those hypot ...
Gamma-Ray Bursts and Puzzles of Core
... The SN 2006aj spectrum (rest wavelength) obtained with BTA in 3.55 days after XRF/GRB 060218 and corrected for galactic extinction. Synthetic spectra are shown by smooth lines. Locations of spectral lines of some ions and blends of their lines are shown in those parts of the spectrum where contribut ...
... The SN 2006aj spectrum (rest wavelength) obtained with BTA in 3.55 days after XRF/GRB 060218 and corrected for galactic extinction. Synthetic spectra are shown by smooth lines. Locations of spectral lines of some ions and blends of their lines are shown in those parts of the spectrum where contribut ...
Galaxy And Mass Assembly (GAMA): Understanding the wavelength
... 2011). They generally have younger stellar populations than classical bulges, and are likely formed by secular processes. Due to their flattened light profiles they are often difficult to detect at high inclination (Carollo et al. 1997; Kormendy et al. 2006; Drory & Fisher 2007; Gadotti 2009). Conve ...
... 2011). They generally have younger stellar populations than classical bulges, and are likely formed by secular processes. Due to their flattened light profiles they are often difficult to detect at high inclination (Carollo et al. 1997; Kormendy et al. 2006; Drory & Fisher 2007; Gadotti 2009). Conve ...
as a PDF
... the inferred circumstellar masses of dust and gas surrounding classical T-Tauri Stars (cTTSs), measured by millimeter continuum observations, preclude a simple spherical distribution of the circumstellar material about such stars (Rydgren et al. 1982). The mass involved would, if spherically distrib ...
... the inferred circumstellar masses of dust and gas surrounding classical T-Tauri Stars (cTTSs), measured by millimeter continuum observations, preclude a simple spherical distribution of the circumstellar material about such stars (Rydgren et al. 1982). The mass involved would, if spherically distrib ...
Observational evidence for AGN feedback in early
... inspection which produces a sample that is not biased against recent star formation and nuclear activity. Based on the nebular emission-line characteristics we separate between star formation activity, black hole activity, the composite of the two and quiescence. We find that emission is mostly LINE ...
... inspection which produces a sample that is not biased against recent star formation and nuclear activity. Based on the nebular emission-line characteristics we separate between star formation activity, black hole activity, the composite of the two and quiescence. We find that emission is mostly LINE ...
IRC −10414: a bow-shock-producing red supergiant star
... through the red supergiant (RSG) phase during their lifetimes. Nonetheless, although many dozens of massive runaways were found to be associated with bow shocks, only two RSG bow-shock-producing stars, Betelgeuse and μ Cep, are known to date. In this paper, we report the discovery of an arc-like neb ...
... through the red supergiant (RSG) phase during their lifetimes. Nonetheless, although many dozens of massive runaways were found to be associated with bow shocks, only two RSG bow-shock-producing stars, Betelgeuse and μ Cep, are known to date. In this paper, we report the discovery of an arc-like neb ...
A CHANDRA X-RAY STUDY OF THE DENSE GLOBULAR CLUSTER TERZAN... C. O. Heinke, P. D. Edmonds, J. E. Grindlay, and...
... merged the two observations. No periods of high background flaring were observed. The X-ray halo of EXO 1745248 displays an X-ray color (defined here as 2:5 log½ð0:5 1:5 keV countsÞ=ð1:5 6 keV countsÞ, following Grindlay et al. 2001a) of 2.9, harder than most known faint globular cluster sources. T ...
... merged the two observations. No periods of high background flaring were observed. The X-ray halo of EXO 1745248 displays an X-ray color (defined here as 2:5 log½ð0:5 1:5 keV countsÞ=ð1:5 6 keV countsÞ, following Grindlay et al. 2001a) of 2.9, harder than most known faint globular cluster sources. T ...
Gas giants in hot water: inhibiting giant planet
... In Section 2, I estimate the temperature of embedded star clusters, and in Section 3 I estimate their protoplanetary disc temperatures. I then compare the relative importance of cluster irradiation and (1) host star irradiation in passive discs, and (2) accretion power in active discs. Generically, ...
... In Section 2, I estimate the temperature of embedded star clusters, and in Section 3 I estimate their protoplanetary disc temperatures. I then compare the relative importance of cluster irradiation and (1) host star irradiation in passive discs, and (2) accretion power in active discs. Generically, ...
L. Zampieri - Astrophysics Group of the University of Crete
... Possible evidences of preferential location of ULXs in low metallicity environments Metallicity of the nebula around NGC 1313 X-2 Results of the statistical analysis of a sample of 66 galaxies observed in X-rays with SFR and metallicities measurements A fraction of ULXs may originate from massive st ...
... Possible evidences of preferential location of ULXs in low metallicity environments Metallicity of the nebula around NGC 1313 X-2 Results of the statistical analysis of a sample of 66 galaxies observed in X-rays with SFR and metallicities measurements A fraction of ULXs may originate from massive st ...
ON THE ORIGIN OF THE SALPETER SLOPE FOR THE INITIAL
... limiting masses that are on the order of the largest clump masses, this should cause an analogous steepening of the cluster mass function under these circumstances. As described above, the ICMF generally has a slope β = 2, but it would be interesting to evaluate any trends. We also note that our mod ...
... limiting masses that are on the order of the largest clump masses, this should cause an analogous steepening of the cluster mass function under these circumstances. As described above, the ICMF generally has a slope β = 2, but it would be interesting to evaluate any trends. We also note that our mod ...
properties and evolution of disks around pre-main
... Mannings et al. 1997). The detection of compact millimeter emission on scales of 1–2 arcsec is considered reliable evidence that the emitting dust is in a disk, rather than in a spherical envelope around the star, since the optical depth of such an envelope would have to be far larger than observed ...
... Mannings et al. 1997). The detection of compact millimeter emission on scales of 1–2 arcsec is considered reliable evidence that the emitting dust is in a disk, rather than in a spherical envelope around the star, since the optical depth of such an envelope would have to be far larger than observed ...
First Results from the WISE Enhanced Resolution Galaxy Atlas
... the table also specifies the primary reference for the distance measurements. The neutral hydrogen mass (with references given in the table) were rescaled to the adopted distance listed in the table. Finally, the Hubble-type morphologies are taken from NED and T-Types (e.g., RC3 of de Vaucouleurs et ...
... the table also specifies the primary reference for the distance measurements. The neutral hydrogen mass (with references given in the table) were rescaled to the adopted distance listed in the table. Finally, the Hubble-type morphologies are taken from NED and T-Types (e.g., RC3 of de Vaucouleurs et ...
Science Case for the Chinese Participation of TMT
... reveal that the Universe is dominated by dark matter and dark energy. The nature of these two dark components is the most fundamental question in (astro-)physics today. The discovery of more than 400 extrasolar planet systems indicates that our solar system may be the exception rather than the norm; ...
... reveal that the Universe is dominated by dark matter and dark energy. The nature of these two dark components is the most fundamental question in (astro-)physics today. The discovery of more than 400 extrasolar planet systems indicates that our solar system may be the exception rather than the norm; ...
Cosmic distance ladder
The cosmic distance ladder (also known as the extragalactic distance scale) is the succession of methods by which astronomers determine the distances to celestial objects. A real direct distance measurement of an astronomical object is possible only for those objects that are ""close enough"" (within about a thousand parsecs) to Earth. The techniques for determining distances to more distant objects are all based on various measured correlations between methods that work at close distances and methods that work at larger distances. Several methods rely on a standard candle, which is an astronomical object that has a known luminosity.The ladder analogy arises because no one technique can measure distances at all ranges encountered in astronomy. Instead, one method can be used to measure nearby distances, a second can be used to measure nearby to intermediate distances, and so on. Each rung of the ladder provides information that can be used to determine the distances at the next higher rung.