![the first simultaneous microlensing observations by two space](http://s1.studyres.com/store/data/021655744_1-bfc0fe02d169bf3cfbc7b98219f1c11f-300x300.png)
the first simultaneous microlensing observations by two space
... is the first microlensing event observed by two space telescopes, Spitzer and Swift, and from the ground. The ground light-curve shows a short anomaly over the peak, due to a companion, and the parallax measurement from Spitzer allows us to determine that it is a BD. This additional BD detection prov ...
... is the first microlensing event observed by two space telescopes, Spitzer and Swift, and from the ground. The ground light-curve shows a short anomaly over the peak, due to a companion, and the parallax measurement from Spitzer allows us to determine that it is a BD. This additional BD detection prov ...
Lecture 3
... • If the filter is 1000Å wide, then the line contributes ~10% of the flux • If half the filter is damped by Ly- forest, the line contributes ~20% of the flux • The exact contribution depends on the transmission of the Ly forest, width of filter and strength of line ...
... • If the filter is 1000Å wide, then the line contributes ~10% of the flux • If half the filter is damped by Ly- forest, the line contributes ~20% of the flux • The exact contribution depends on the transmission of the Ly forest, width of filter and strength of line ...
The extinction map of the OMC-1 molecular cloud behind the Orion
... A number of previous studies provide results relevant to the issue of the galactic reddening in the direction of OMC-1. Schlegel et al. (1998) (SFD98 hereafter) combined the COBE/DIRBE observations (100 μm and 240 μm) and the IRAS/ISSA observations (100 μm) to obtain a full-sky 100 μm map with ∼6 r ...
... A number of previous studies provide results relevant to the issue of the galactic reddening in the direction of OMC-1. Schlegel et al. (1998) (SFD98 hereafter) combined the COBE/DIRBE observations (100 μm and 240 μm) and the IRAS/ISSA observations (100 μm) to obtain a full-sky 100 μm map with ∼6 r ...
The Milky Way`s external disc constrained by 2MASS star counts
... HI warp. At negative longitudes, the disc presents peculiarities that are not reproduced well by any simple model. Finally, comparing with the warp seen in the dust, it seems to follow an intermediate slope between the gas and the stars. Key words. Galaxy: disk – galaxie: structure – surveys ...
... HI warp. At negative longitudes, the disc presents peculiarities that are not reproduced well by any simple model. Finally, comparing with the warp seen in the dust, it seems to follow an intermediate slope between the gas and the stars. Key words. Galaxy: disk – galaxie: structure – surveys ...
A subaru/suprime-cam wide
... (1) Most of the blue GCs are associated with the host galaxy, not the host galaxy cluster, even in central cluster galaxies like M87. (2) Blue GCs may be linked with the dark matter halo of a massive elliptical galaxy: they might have formed in sub-galactic clumps and assembled thereafter, whilst re ...
... (1) Most of the blue GCs are associated with the host galaxy, not the host galaxy cluster, even in central cluster galaxies like M87. (2) Blue GCs may be linked with the dark matter halo of a massive elliptical galaxy: they might have formed in sub-galactic clumps and assembled thereafter, whilst re ...
Astronomy Astrophysics Astrophysical parameters and orbital solution of the peculiar X-ray
... Of course, a clumpy spherical wind can exist together with an eccentric orbit (Blay et al. 2012), and this scenario would also explain the quasi-stable X-ray luminosity of SGXBs, since they have circular orbits. Furthermore, Bozzo et al. (2008) proposed a model that makes use of transitions between ...
... Of course, a clumpy spherical wind can exist together with an eccentric orbit (Blay et al. 2012), and this scenario would also explain the quasi-stable X-ray luminosity of SGXBs, since they have circular orbits. Furthermore, Bozzo et al. (2008) proposed a model that makes use of transitions between ...
Planets and Debris Disks: Results from a Spitzer/MIPS Search for IR
... surveys, some screening is done to maximize the success rate - a companion star orbiting at several AU is assumed to rule out the presence of a planet or disk at a similar location. Nevertheless, despite efforts to cull such systems, there are stars in both sets of data that do in fact have low-mass ...
... surveys, some screening is done to maximize the success rate - a companion star orbiting at several AU is assumed to rule out the presence of a planet or disk at a similar location. Nevertheless, despite efforts to cull such systems, there are stars in both sets of data that do in fact have low-mass ...
Untitled - NMSU Astronomy
... wavelength of spectral lines in nanometers, and measure the sizes of features on the Sun that are larger than 100,000 kilometers. ...
... wavelength of spectral lines in nanometers, and measure the sizes of features on the Sun that are larger than 100,000 kilometers. ...
from z=0 to z=1
... do not overlap with each other very much. SCUBA galaxies have significantly higher SFR, higher attenuation, higher stellar mass, and higher correlation length than LBGs. 7. At intermediate redshifts of z~0.6, UV selected galaxies show moderate evolution in stellar mass in the sense that for a given ...
... do not overlap with each other very much. SCUBA galaxies have significantly higher SFR, higher attenuation, higher stellar mass, and higher correlation length than LBGs. 7. At intermediate redshifts of z~0.6, UV selected galaxies show moderate evolution in stellar mass in the sense that for a given ...
The Radio Galaxy 3C265 Contains a Hidden Quasar Nucleus
... observations of Jannuzi and Elston (1991). If we assume that the primary scattering mechanism is Thomson scattering within a radiation cone of half opening angle 45 uniformly lled with electrons, then the maximum possible intrinsic polarization of the scattered light is Pmax 53%. Since the obser ...
... observations of Jannuzi and Elston (1991). If we assume that the primary scattering mechanism is Thomson scattering within a radiation cone of half opening angle 45 uniformly lled with electrons, then the maximum possible intrinsic polarization of the scattered light is Pmax 53%. Since the obser ...
Models of red giants in the CoRoT asteroseismology fields
... Solar reference values from M14 are Δν = 135.1 μHz, νmax, = 3090 μHz and T eff, = 5777 K. As the Hipparcos parallax, π, is available for most of the stars studied here, we can derive the stellar luminosity from the apparent magnitude in V-band, and then the stellar radius. The bolometric correctio ...
... Solar reference values from M14 are Δν = 135.1 μHz, νmax, = 3090 μHz and T eff, = 5777 K. As the Hipparcos parallax, π, is available for most of the stars studied here, we can derive the stellar luminosity from the apparent magnitude in V-band, and then the stellar radius. The bolometric correctio ...
The impact of rotation on the line profiles of Wolf
... 1989) were shown to also cause it. Moreover, rotational velocities are very hard to quantify on the basis of polarimetric measurements alone. Recent spectroscopic studies performed with the non-LTE Potsdam Wolf-Rayet (PoWR) model atmosphere code potentially imply the existence of rapidly rotating WR ...
... 1989) were shown to also cause it. Moreover, rotational velocities are very hard to quantify on the basis of polarimetric measurements alone. Recent spectroscopic studies performed with the non-LTE Potsdam Wolf-Rayet (PoWR) model atmosphere code potentially imply the existence of rapidly rotating WR ...
book_text4
... The Hubble Space Telescope has undoubtedly had a greater public impact than any other space astronomy mission ever. The images included in this beautiful volume are quite staggering in what they reveal about the Universe we live in and have already become part of our common scientific and cultural h ...
... The Hubble Space Telescope has undoubtedly had a greater public impact than any other space astronomy mission ever. The images included in this beautiful volume are quite staggering in what they reveal about the Universe we live in and have already become part of our common scientific and cultural h ...
Possibility for albedo estimation of exomoons: Why should we care
... whether next generation telescopes will be capable of albedo estimations for icy exomoons using their occultation light curves. The success of the measurements depends on the depth of the moon’s occultation in the light curve and on the sensitivity of the used instruments. We applied simple calculat ...
... whether next generation telescopes will be capable of albedo estimations for icy exomoons using their occultation light curves. The success of the measurements depends on the depth of the moon’s occultation in the light curve and on the sensitivity of the used instruments. We applied simple calculat ...
The Dwarf Starburst Host Galaxy of a Type Ia SN at z= 1.55 from
... now include over 500 well-studied SNe with a dispersion in peak magnitudes of ∼0.16 magnitudes (e.g., Conley et al. 2011; Suzuki et al. 2012). At this precision, a larger sample size alone will not improve cosmological constraints, so the limiting factor is our understanding of systematic effects. A ...
... now include over 500 well-studied SNe with a dispersion in peak magnitudes of ∼0.16 magnitudes (e.g., Conley et al. 2011; Suzuki et al. 2012). At this precision, a larger sample size alone will not improve cosmological constraints, so the limiting factor is our understanding of systematic effects. A ...
SKA and VLBI synergies
... The technique of very-long-baseline interferometry (VLBI) probes compact objects in the microwave range, at angular scales from 100 millarcseconds (mas) down to fractions of mas. This corresponds to scales of several astronomical units at the distance of few kpc (e.g., microquasars in our Galaxy or ...
... The technique of very-long-baseline interferometry (VLBI) probes compact objects in the microwave range, at angular scales from 100 millarcseconds (mas) down to fractions of mas. This corresponds to scales of several astronomical units at the distance of few kpc (e.g., microquasars in our Galaxy or ...
ellc: A fast, flexible light curve model for detached eclipsing binary
... which includes a modification of the potential to allow for nonsynchronous rotation of the star. The direction of the star’s rotational angular momentum vector, Lrot is assumed to be parallel to Lorb . The values of A−D are set by requiring that the value of this potential is equal at the six points ...
... which includes a modification of the potential to allow for nonsynchronous rotation of the star. The direction of the star’s rotational angular momentum vector, Lrot is assumed to be parallel to Lorb . The values of A−D are set by requiring that the value of this potential is equal at the six points ...
Stellar Populations of Dwarf Elliptical Galaxies: UBVRI Photometry
... Cluster with previously measured kinematic properties. The global optical colors are red, with median values for the sample of 0.24 ± 0.03 in (U–B), 0.77 ± 0.02 in (B– V), and 1.02 ± 0.03 in (V–I). We recover the well known color-magnitude relation for cluster galaxies, but find no significant diffe ...
... Cluster with previously measured kinematic properties. The global optical colors are red, with median values for the sample of 0.24 ± 0.03 in (U–B), 0.77 ± 0.02 in (B– V), and 1.02 ± 0.03 in (V–I). We recover the well known color-magnitude relation for cluster galaxies, but find no significant diffe ...
Environment and self-regulation in galaxy formation
... Rakos et al. 2007; Annibali et al. 2007; de la Rosa et al. 2007). In summary, early-type galaxies in lower densities appear younger by 1 − 2 Gyr at given galaxy mass. These differences should become even more pronounced when probing earlier epochs. As discussed in the review by Renzini (2006), howev ...
... Rakos et al. 2007; Annibali et al. 2007; de la Rosa et al. 2007). In summary, early-type galaxies in lower densities appear younger by 1 − 2 Gyr at given galaxy mass. These differences should become even more pronounced when probing earlier epochs. As discussed in the review by Renzini (2006), howev ...
Periodic Universal Gravitation Resulting in the Phenomenon of Dark
... quantum space [7]. When observing two galaxies or two stars in one galaxy in the contracting section, their distance is decreasing. According to the research result of NASA, our galaxy will collide into Andromeda Galaxy after 4 billion years, possibly integrating into one galaxy. t = T 0 is the time ...
... quantum space [7]. When observing two galaxies or two stars in one galaxy in the contracting section, their distance is decreasing. According to the research result of NASA, our galaxy will collide into Andromeda Galaxy after 4 billion years, possibly integrating into one galaxy. t = T 0 is the time ...
The CCD Photometric Calibration Cookbook
... photographs and latterly CCD images. The techniques for calibrating CCD images are now well established. However, they must be applied carefully if accurate results are to be obtained. In essence, astronomical photometry is concerned with measuring the brightness of celestial objects. CCD (Charge-Co ...
... photographs and latterly CCD images. The techniques for calibrating CCD images are now well established. However, they must be applied carefully if accurate results are to be obtained. In essence, astronomical photometry is concerned with measuring the brightness of celestial objects. CCD (Charge-Co ...
Astronomy Astrophysics Detailed abundances of a large sample of giant stars in... and in the Sagittarius nucleus
... of the coolest stars (see Fig. 3) in the latter component are heavily affected by titanium oxide (TiO) bands, which severely depress the continuum, in particular in the HR13 spectral range. They were omitted from further analysis. After the first abundance analysis, we found that three stars, attribu ...
... of the coolest stars (see Fig. 3) in the latter component are heavily affected by titanium oxide (TiO) bands, which severely depress the continuum, in particular in the HR13 spectral range. They were omitted from further analysis. After the first abundance analysis, we found that three stars, attribu ...
Sunyaev±Zel'dovich distortion from early galactic winds Subhabrata Majumdar, Biman B. Nath
... simulations assume a disc geometry. However, it is certain that galactic outflows do occur and have important effects on the ambient medium. Recent studies on galactic outflows at high redshift contend that these winds could have suppressed galaxy formation in the vicinity, for masses #109 M( by mas ...
... simulations assume a disc geometry. However, it is certain that galactic outflows do occur and have important effects on the ambient medium. Recent studies on galactic outflows at high redshift contend that these winds could have suppressed galaxy formation in the vicinity, for masses #109 M( by mas ...
The white dwarf cooling sequence of 47 Tucanae
... main-sequence turn-off. Finally, we find that the star formation history of the cluster is compatible with that obtained using main sequence stars, which predict the existence of two distinct populations. Conclusions. We conclude that a correct modeling of the white dwarf population of globular clus ...
... main-sequence turn-off. Finally, we find that the star formation history of the cluster is compatible with that obtained using main sequence stars, which predict the existence of two distinct populations. Conclusions. We conclude that a correct modeling of the white dwarf population of globular clus ...
Chemo-spectrophotometric evolution of spiral galaxies ± II. Main
... popular semi-analytic models of galaxy formation. We compare our results with a large body of observational data on present-day galactic discs, including disc sizes and central surface brightness, Tully±Fisher relations in various wavelength bands, colour±colour and colour± magnitude relations, gas ...
... popular semi-analytic models of galaxy formation. We compare our results with a large body of observational data on present-day galactic discs, including disc sizes and central surface brightness, Tully±Fisher relations in various wavelength bands, colour±colour and colour± magnitude relations, gas ...
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.