The Life Cycle of Stars: Supernovae in Starbursts by Jason Kezwer
... nuclear background and find an absolute magnitude of MK = −22.19 ± 0.16 (nonabsorbed). This exceeds the luminosity of a typical core collapse supernova by roughly 3.5 magnitudes; rather, the observed variations in nuclear brightness are most likely the signature of an active galactic nucleus embedde ...
... nuclear background and find an absolute magnitude of MK = −22.19 ± 0.16 (nonabsorbed). This exceeds the luminosity of a typical core collapse supernova by roughly 3.5 magnitudes; rather, the observed variations in nuclear brightness are most likely the signature of an active galactic nucleus embedde ...
Luminosities and mass-loss rates of SMC and LMC AGB stars and
... of the expansion velocity from future observations from ALMA. The OGLE-III data reveal an O-rich star in the SMC with a period of 1749 days. Its absolute magnitude of Mbol = −8.0 makes it a good candidate for a super-AGB star. Key words. stars: AGB and post-AGB – stars: mass loss – Magellanic Clouds ...
... of the expansion velocity from future observations from ALMA. The OGLE-III data reveal an O-rich star in the SMC with a period of 1749 days. Its absolute magnitude of Mbol = −8.0 makes it a good candidate for a super-AGB star. Key words. stars: AGB and post-AGB – stars: mass loss – Magellanic Clouds ...
Towards the understanding of the deepest layers of solar
... I would like to start by thanking both my supervisors, Dra. Margarida Cunha and Prof. Dr. Jørgen Christensen-Dalsgaard, without whom the realization of this thesis would not have been possible. I would like to give a very special thank to Prof. Dr. Jørgen ChristensenDalsgaard for his hospitality and ...
... I would like to start by thanking both my supervisors, Dra. Margarida Cunha and Prof. Dr. Jørgen Christensen-Dalsgaard, without whom the realization of this thesis would not have been possible. I would like to give a very special thank to Prof. Dr. Jørgen ChristensenDalsgaard for his hospitality and ...
THE PERIOD OF ROTATION OF THE SUN
... catalog from the US Naval Observatory on-line services, which includes positional and photometric data on 1.1 billion point sources, with photometric magnitudes in the B, V, R, J, H, and K passbands. Because it simulates a very large and diverse sample of the observable astronomical sky as seen with ...
... catalog from the US Naval Observatory on-line services, which includes positional and photometric data on 1.1 billion point sources, with photometric magnitudes in the B, V, R, J, H, and K passbands. Because it simulates a very large and diverse sample of the observable astronomical sky as seen with ...
Vireo Manual - Gettysburg College
... catalog from the US Naval Observatory on-line services, which includes positional and photometric data on 1.1 billion point sources, with photometric magnitudes in the B, V, R, J, H, and K passbands. Because it simulates a very large and diverse sample of the observable astronomical sky as seen with ...
... catalog from the US Naval Observatory on-line services, which includes positional and photometric data on 1.1 billion point sources, with photometric magnitudes in the B, V, R, J, H, and K passbands. Because it simulates a very large and diverse sample of the observable astronomical sky as seen with ...
Instruction Manual #11007 / #11008 / #11009 ®
... • Database filter limits for creating custom object lists • Storage for programmable user defined objects; and many other high performance features! The CPC DeluxeHD’s features combined with Celestron’s legendary optical systems give amateur astronomers the most sophisticated and easy to use teles ...
... • Database filter limits for creating custom object lists • Storage for programmable user defined objects; and many other high performance features! The CPC DeluxeHD’s features combined with Celestron’s legendary optical systems give amateur astronomers the most sophisticated and easy to use teles ...
On the elemental abundance and isotopic mixture of mercury in
... In the present paper the optical region mercury lines Hg λ4358, Hg λλ3984, 6149 have been studied, and the wavelength and oscillator strength of the hyperfine and isotopic components for each transition are presented in Table 2 for the case of a terrestrial isotopic mixture (Anders & Grevesse 1 ...
... In the present paper the optical region mercury lines Hg λ4358, Hg λλ3984, 6149 have been studied, and the wavelength and oscillator strength of the hyperfine and isotopic components for each transition are presented in Table 2 for the case of a terrestrial isotopic mixture (Anders & Grevesse 1 ...
SpeX Observing Manual - NASA Infrared Telescope Facility
... the ‘Test Go’ button. This will turn save off, put the telescope beam in position A, set NDRs to one, take an image and then restore the original set up. Finally, measure the rate using the maximum level reported in DV (avoiding hot pixels and scaling to one second), and adjust the itime. Observers ...
... the ‘Test Go’ button. This will turn save off, put the telescope beam in position A, set NDRs to one, take an image and then restore the original set up. Finally, measure the rate using the maximum level reported in DV (avoiding hot pixels and scaling to one second), and adjust the itime. Observers ...
maximum likelihood fitting of tidal streams with application
... star counts often suggested a more spherical spheroid (Bahcall 1986). By early in the 21st century, the spheroid was still thought of as a smooth power-law distribution, but studies were starting to show that the shape of the spheroid depended on the type of star being observed, and it was noted tha ...
... star counts often suggested a more spherical spheroid (Bahcall 1986). By early in the 21st century, the spheroid was still thought of as a smooth power-law distribution, but studies were starting to show that the shape of the spheroid depended on the type of star being observed, and it was noted tha ...
SPIRAL STRUCTURE IN THE OUTER GALACTIC
... According to the age and the places where they are located, clusters present a variety of challenges in deriving their intrinsic parameters. In the case of very young clusters, they are normally close to the Galactic plane where interstellar absorption and crowded stellar fields make membership assi ...
... According to the age and the places where they are located, clusters present a variety of challenges in deriving their intrinsic parameters. In the case of very young clusters, they are normally close to the Galactic plane where interstellar absorption and crowded stellar fields make membership assi ...
The masses and spins of neutron stars and stellar
... As the remnants of core-collapse supernovae, neutron stars and black holes are also windows into the collapse and explosion processes. The further evolution of these systems in accreting binaries can tell us about the accretion process, e.g., the total amount of mass that is typically deposited on t ...
... As the remnants of core-collapse supernovae, neutron stars and black holes are also windows into the collapse and explosion processes. The further evolution of these systems in accreting binaries can tell us about the accretion process, e.g., the total amount of mass that is typically deposited on t ...
Multiplicity in Early Stellar Evolution
... tree (level 1). Inner pairs associated with primary and secondary components of the outer pair are called levels 11 and 12, respectively, and this notation continues to deeper levels. Triple systems can have inner pairs at level 11 or 12. When both sub-systems are present, we get the so-called 2+2 q ...
... tree (level 1). Inner pairs associated with primary and secondary components of the outer pair are called levels 11 and 12, respectively, and this notation continues to deeper levels. Triple systems can have inner pairs at level 11 or 12. When both sub-systems are present, we get the so-called 2+2 q ...
Astronomy Astrophysics
... The procedure employed for determining the fundamental cluster parameters such as age, reddening, and distance is described in Borissova et al. (2011) and Chené et al. (2012, 2013). As described in Borissova et al. (2011), we used the field-star decontamination algorithm of Bonatto & Bica (2010), wh ...
... The procedure employed for determining the fundamental cluster parameters such as age, reddening, and distance is described in Borissova et al. (2011) and Chené et al. (2012, 2013). As described in Borissova et al. (2011), we used the field-star decontamination algorithm of Bonatto & Bica (2010), wh ...
exploring anticorrelations and light element variations
... of GC color–magnitude diagrams. In fact, while some clusters seem to photometrically comply with the simple stellar population paradigm, a growing number of them are found to be characterized by multiple main sequences and/or subgiant and/or giant branches (Piotto et al. 2007; Milone et al. 2008, e. ...
... of GC color–magnitude diagrams. In fact, while some clusters seem to photometrically comply with the simple stellar population paradigm, a growing number of them are found to be characterized by multiple main sequences and/or subgiant and/or giant branches (Piotto et al. 2007; Milone et al. 2008, e. ...
Annual Report 2006/2007
... supernova remnant Cassiopeia A (Cas A). This object is the brightest radio source in the sky, and has been created by a supernova explosion about 330 year ago. The star itself had a mass of around 20 times the mass of the sun, but by the time it exploded it must have lost most of the outer layers. T ...
... supernova remnant Cassiopeia A (Cas A). This object is the brightest radio source in the sky, and has been created by a supernova explosion about 330 year ago. The star itself had a mass of around 20 times the mass of the sun, but by the time it exploded it must have lost most of the outer layers. T ...
A Spitzer mid-infrared spectral survey of mass
... Bessell & Fox 1983; Feast et al. 1989), and the intermediate-age clusters NGC 419 and 1978, both of which have a known mid-IR source. Targets were selected to span the long sequence of increasing mass-loss in LIMS which stretches from (J − K , M K ) ∼ (2, − 9) to (7, −4) in Fig. 1(a). [The bright ox ...
... Bessell & Fox 1983; Feast et al. 1989), and the intermediate-age clusters NGC 419 and 1978, both of which have a known mid-IR source. Targets were selected to span the long sequence of increasing mass-loss in LIMS which stretches from (J − K , M K ) ∼ (2, − 9) to (7, −4) in Fig. 1(a). [The bright ox ...
OBSERVATIONS OF PHYSICAL PROCESSES IN
... cluster galaxies (BCGs) of those clusters. It has been known for a while that the state of the hot intracluster medium (ICM) gas in the core of a galaxy cluster, quantified as the central entropy of the gas, can be found in two particular states. Galaxy clusters with central entropies greater than 3 ...
... cluster galaxies (BCGs) of those clusters. It has been known for a while that the state of the hot intracluster medium (ICM) gas in the core of a galaxy cluster, quantified as the central entropy of the gas, can be found in two particular states. Galaxy clusters with central entropies greater than 3 ...
Cygnus (constellation)
Cygnus /ˈsɪɡnəs/ is a northern constellation lying on the plane of the Milky Way, deriving its name from the Latinized Greek word for swan. The swan is one of the most recognizable constellations of the northern summer and autumn, it features a prominent asterism known as the Northern Cross (in contrast to the Southern Cross). Cygnus was among the 48 constellations listed by the 2nd century astronomer Ptolemy, and it remains one of the 88 modern constellations.Cygnus contains Deneb, one of the brightest stars in the night sky and one corner of the Summer Triangle, as well as some notable X-ray sources and the giant stellar association of Cygnus OB2. One of the stars of this association, NML Cygni, is one of the largest stars currently known. The constellation is also home to Cygnus X-1, a distant X-ray binary containing a supergiant and unseen massive companion that was the first object widely held to be a black hole. Many star systems in Cygnus have known planets as a result of the Kepler Mission observing one patch of the sky, the patch is the area around Cygnus. In addition, most of the eastern part of Cygnus is dominated by the Hercules–Corona Borealis Great Wall, a giant galaxy filament that is the largest known structure in the observable universe; covering most of the northern sky.