SPT 0538−50: PHYSICAL CONDITIONS IN THE ISM OF A STRONGLY... GALAXY AT Z=2.8
... conclude in §5. All magnitudes in this work are given in the Vega system. Throughout this work we adopt a cosmological model with (Ωm , ΩΛ , H0 ) = (0.27, 0.73, 71 km s−1 Mpc−1 ), and a Kroupa (2001) initial mass function. 2. OBSERVATIONS AND RESULTS ...
... conclude in §5. All magnitudes in this work are given in the Vega system. Throughout this work we adopt a cosmological model with (Ωm , ΩΛ , H0 ) = (0.27, 0.73, 71 km s−1 Mpc−1 ), and a Kroupa (2001) initial mass function. 2. OBSERVATIONS AND RESULTS ...
The ionized gas in the central region of NGC 5253
... used for the masterbias creation while six and three continuum lamp exposures were needed for the creation of the L385.7 and L427.2 masterflats, respectively. In order to remove the cosmic rays in the target exposures, we combined all the individual frames for a given grating using imcombine with IR ...
... used for the masterbias creation while six and three continuum lamp exposures were needed for the creation of the L385.7 and L427.2 masterflats, respectively. In order to remove the cosmic rays in the target exposures, we combined all the individual frames for a given grating using imcombine with IR ...
Galaxy Number Counts from the Sloan Digital Sky Survey
... The SDSS survey is carried out using a wide-field 2.5 m telescope, a large format imaging camera (Gunn et al. 1998), two fiber-fed double spectrographs, and an auxiliary 0.5 m telescope for photometric calibration. The sky is imaged in five passbands, u′ , g′ , r ′ , i′ , z ′ covering the entire opt ...
... The SDSS survey is carried out using a wide-field 2.5 m telescope, a large format imaging camera (Gunn et al. 1998), two fiber-fed double spectrographs, and an auxiliary 0.5 m telescope for photometric calibration. The sky is imaged in five passbands, u′ , g′ , r ′ , i′ , z ′ covering the entire opt ...
- National Optical Astronomy Observatory
... Movement of the Iron ions is restricted to the magnetic field lines from within the umbra to the edge of the penumbra. This is supported by the data, which shows an initial outward flow of the ions and then a downward flow near penumbra. Because the nickel particles are not ionized, their velocities ...
... Movement of the Iron ions is restricted to the magnetic field lines from within the umbra to the edge of the penumbra. This is supported by the data, which shows an initial outward flow of the ions and then a downward flow near penumbra. Because the nickel particles are not ionized, their velocities ...
Decoding Galaxy Evolution with Gas
... product of metallicity-dependent core-collapse supernova (CCSN) yields. Applying PCAA to a sample of local disk dwarfs yields a nearly identical PC1, suggesting broadly similar α-enrichment histories. However, the disk PC2 is dominated by a Y–Ba correlation, likely indicating a contribution of s-pro ...
... product of metallicity-dependent core-collapse supernova (CCSN) yields. Applying PCAA to a sample of local disk dwarfs yields a nearly identical PC1, suggesting broadly similar α-enrichment histories. However, the disk PC2 is dominated by a Y–Ba correlation, likely indicating a contribution of s-pro ...
Modeling Spatially and Spectrally Resolved Observations to
... In extragalactic astronomy, a central challenge is that we cannot directly watch what happens to galaxies before and after they are observed. This dissertation focuses on linking predictions of galaxy time-evolution directly with observations, evaluating how interactions, mergers, and other processe ...
... In extragalactic astronomy, a central challenge is that we cannot directly watch what happens to galaxies before and after they are observed. This dissertation focuses on linking predictions of galaxy time-evolution directly with observations, evaluating how interactions, mergers, and other processe ...
Revised physical elements of the astrophysically important O9.5+O9
... the topic. Simon & Sturm (1992, 1994) developed a new technique of spectra disentangling, which permits the separation of the spectra of binary components with a simultaneous determination of the orbital and physical elements. Simon et al. (1994) applied this technique to a study of Y Cyg. Comparing ...
... the topic. Simon & Sturm (1992, 1994) developed a new technique of spectra disentangling, which permits the separation of the spectra of binary components with a simultaneous determination of the orbital and physical elements. Simon et al. (1994) applied this technique to a study of Y Cyg. Comparing ...
TWO NEW LONG-PERIOD GIANT PLANETS FROM THE
... stress the importance of monitoring the magnetic activity level of a target star, as long-term activity cycles can mimic the presence of a Jupiter-analog planet. Key words: planetary systems – stars: activity – techniques: radial velocities Supporting material: machine-readable tables The RV techniq ...
... stress the importance of monitoring the magnetic activity level of a target star, as long-term activity cycles can mimic the presence of a Jupiter-analog planet. Key words: planetary systems – stars: activity – techniques: radial velocities Supporting material: machine-readable tables The RV techniq ...
PDF
... away from our line of sight. The small number of confirmed AXPs prevents any detailed statistical discussion of beaming. However, the pulsed fraction and pulse shape of the known AXPs can be used to motivate at least a rough characterization. For each AXP, Table 8-2 lists the pulsed fraction f, the ...
... away from our line of sight. The small number of confirmed AXPs prevents any detailed statistical discussion of beaming. However, the pulsed fraction and pulse shape of the known AXPs can be used to motivate at least a rough characterization. For each AXP, Table 8-2 lists the pulsed fraction f, the ...
Link - Max-Planck-Institut für Astronomie
... with F/G supergiant spectral types but broad lines compared to TTS, and little indication of magnetospheric accretion. In contrast, they show K/M supergiant spectral types in the near-infrared. A supergiant spectrum can also be seen in the ultraviolet (Kravtsova et al., 2007). They are associated wi ...
... with F/G supergiant spectral types but broad lines compared to TTS, and little indication of magnetospheric accretion. In contrast, they show K/M supergiant spectral types in the near-infrared. A supergiant spectrum can also be seen in the ultraviolet (Kravtsova et al., 2007). They are associated wi ...
Slide 1
... The only way to provide high spatial and spectral resolution AND high sensitivity is with large collecting area. ALMA. ...
... The only way to provide high spatial and spectral resolution AND high sensitivity is with large collecting area. ALMA. ...
Core formation in giant planets formed through
... the minimal mass of the cloud that will collapse at a given temperature and density. Once the collapse of the cloud has begun, the denser part of this cloud will collapse more quickly. This leads to a fragmentation of the cloud. Each fragment nally forms its own star. During the collapse, the gravi ...
... the minimal mass of the cloud that will collapse at a given temperature and density. Once the collapse of the cloud has begun, the denser part of this cloud will collapse more quickly. This leads to a fragmentation of the cloud. Each fragment nally forms its own star. During the collapse, the gravi ...
Doppler imaging of AB Doradus using the Li I 6708 line
... spread remains a puzzle. Recent theoretical attempts to explain it have focused on the observed tendency of the fastest rotators at any given spectral type to have the greatest abundances of Li (Butler et al. 1987). While this might indicate that rotation in some way inhibits mixing of Li-rich mater ...
... spread remains a puzzle. Recent theoretical attempts to explain it have focused on the observed tendency of the fastest rotators at any given spectral type to have the greatest abundances of Li (Butler et al. 1987). While this might indicate that rotation in some way inhibits mixing of Li-rich mater ...
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... because of its suspected similarity to either a forming or a young planetary system. With the growing realization that planetary systems are not uncommon, we are more than ever motivated to tackle questions such as how similar is the dust around β Pic to the solar system dust? Is there evidence for ...
... because of its suspected similarity to either a forming or a young planetary system. With the growing realization that planetary systems are not uncommon, we are more than ever motivated to tackle questions such as how similar is the dust around β Pic to the solar system dust? Is there evidence for ...
High-resolution radio emission from RCW 49/Westerlund 2
... be confirmed to be caused by synchrotron emission, we propose a scenario where high-energy emission could be produced. Finally, the newly discovered jet-like structure appears to be an intriguing source that deserves a detailed study by itself. Key words. stars: winds, outflows – ISM: individual obj ...
... be confirmed to be caused by synchrotron emission, we propose a scenario where high-energy emission could be produced. Finally, the newly discovered jet-like structure appears to be an intriguing source that deserves a detailed study by itself. Key words. stars: winds, outflows – ISM: individual obj ...
CHARACTERIZING DUST ATTENUATION IN LOCAL STAR FORMING GALAXIES: UV AND... REDDENING ABSTRACT The dust attenuation for a sample of ∼10000 local (z ....
... to which it can vary. However, these studies have used different techniques than those described in Calzetti et al. (1994, 2000), which can introduce different biases and make direct comparison unclear. More specifically, Johnson et al. (2007b) use average SEDs of galaxies separated according to IRX ...
... to which it can vary. However, these studies have used different techniques than those described in Calzetti et al. (1994, 2000), which can introduce different biases and make direct comparison unclear. More specifically, Johnson et al. (2007b) use average SEDs of galaxies separated according to IRX ...
The evolution of low-metallicity massive stars - Argelander
... compact as Wolf–Rayet stars. However, as opposed to Wolf–Rayet stars, their stellar winds are optically thin. As these hot objects emit intense UV radiation, we show that they can explain the unusually high number of ionizing photons of the dwarf galaxy I Zwicky 18, an observational quantity that ca ...
... compact as Wolf–Rayet stars. However, as opposed to Wolf–Rayet stars, their stellar winds are optically thin. As these hot objects emit intense UV radiation, we show that they can explain the unusually high number of ionizing photons of the dwarf galaxy I Zwicky 18, an observational quantity that ca ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.