20 pm - Starmap
... As a starting point, face North, holding the map in your eyesight direction, with its North down. As you change the direction, rotate the map accordingly. The objects listed on the first page can be observed with naked eyes, in clear skies, with moderate light pollution. Close your eyes one minute a ...
... As a starting point, face North, holding the map in your eyesight direction, with its North down. As you change the direction, rotate the map accordingly. The objects listed on the first page can be observed with naked eyes, in clear skies, with moderate light pollution. Close your eyes one minute a ...
Powerpoint slides
... Position your first volunteer at the back/far side of the room with a set of building blocks and photographs. (S)he is the Distant Galaxy. Position your second volunteer (along with the second set of blocks and photographs) about halfway between you (the telescope/observer) and Distant Galaxy. (S)he ...
... Position your first volunteer at the back/far side of the room with a set of building blocks and photographs. (S)he is the Distant Galaxy. Position your second volunteer (along with the second set of blocks and photographs) about halfway between you (the telescope/observer) and Distant Galaxy. (S)he ...
Supplementary Information
... respect to the observed one dimensional distributions in total Hα intensity, mean velocity and velocity dispersion along the major axis and also in Hα mean velocity along the minor axis (114 west of north) in the undisturbed and well sampled north-western section of the disk, ~0.69” from the nucleu ...
... respect to the observed one dimensional distributions in total Hα intensity, mean velocity and velocity dispersion along the major axis and also in Hα mean velocity along the minor axis (114 west of north) in the undisturbed and well sampled north-western section of the disk, ~0.69” from the nucleu ...
Less than 15 percent of star formation in massive galaxies is
... …it was believed that the evolution of the merger rate could drive the decrease of the SFR density ...
... …it was believed that the evolution of the merger rate could drive the decrease of the SFR density ...
ONE- AND MULTI- ZONE MODELS: Chemical properties
... Lynden-Bell, 1975 Tinsley, 1980a Chiosi, 1981), i.e. models in which the total mass of the disk is let increase with time at a suitable rate starting from a much lower value. With the current law of star formation (proportional to the gas mass) the competition between gas accretion by infall and g ...
... Lynden-Bell, 1975 Tinsley, 1980a Chiosi, 1981), i.e. models in which the total mass of the disk is let increase with time at a suitable rate starting from a much lower value. With the current law of star formation (proportional to the gas mass) the competition between gas accretion by infall and g ...
As far as - Sangeeta Malhotra
... Hubble observations have taken us back 12.6 billion years. observe. It’s a tricky business, employing many indirect arguments. Next in the HUDF distance scale come small, blue galaxies actively forming stars and bearing a resemblance to nearby dwarf irregular galaxies. The ACS grism (a cross between ...
... Hubble observations have taken us back 12.6 billion years. observe. It’s a tricky business, employing many indirect arguments. Next in the HUDF distance scale come small, blue galaxies actively forming stars and bearing a resemblance to nearby dwarf irregular galaxies. The ACS grism (a cross between ...
8.1 Radio Emission from Solar System objects
... emission arising from the interaction of their magnetic fields. There is also a category of stars that show flare behavior. It is thought that these are very young stars that are ejecting matter in the form of minor jets. Most of the strong radio emission comes from stars that are either very young ...
... emission arising from the interaction of their magnetic fields. There is also a category of stars that show flare behavior. It is thought that these are very young stars that are ejecting matter in the form of minor jets. Most of the strong radio emission comes from stars that are either very young ...
The MAGNUM survey: positive feedback in the nuclear region of
... wavelengths (e.g., Fig. 1, panels, b and c). As we discuss later, this is because of the higher extinction to the W, indicating that the EELR is tilted with respect to the galaxy plane, and it is lying behind the disk of the galaxy to the W, while it is seen mostly above the disk to the E. An [OIII] ...
... wavelengths (e.g., Fig. 1, panels, b and c). As we discuss later, this is because of the higher extinction to the W, indicating that the EELR is tilted with respect to the galaxy plane, and it is lying behind the disk of the galaxy to the W, while it is seen mostly above the disk to the E. An [OIII] ...
LSS-GAC – A LAMOST Spectroscopic Survey of the
... simulations, the scenario involves many currently poorly understood and often highly non-linear baryonic physics (e.g. star formation and feedback) that it is compulsory to find out empirically the assemblage history of galaxies via detailed study of large samples of member stars of nearby, well-reso ...
... simulations, the scenario involves many currently poorly understood and often highly non-linear baryonic physics (e.g. star formation and feedback) that it is compulsory to find out empirically the assemblage history of galaxies via detailed study of large samples of member stars of nearby, well-reso ...
The influence of chemical composition on the pulsation properties of
... Sandage (1958): “...the possibility exists that the PL relation is not unique and the scatter real...the existence of an intrinsic scatter in the P=f(L) suggests that a third parameter is involved...in what follows, a semi-theoretical relation is found which indeed involves three parameters [the thi ...
... Sandage (1958): “...the possibility exists that the PL relation is not unique and the scatter real...the existence of an intrinsic scatter in the P=f(L) suggests that a third parameter is involved...in what follows, a semi-theoretical relation is found which indeed involves three parameters [the thi ...
microquasars
... -THE PHYSICS OF RELATIVISTIC JETS FROM BH’s -THE CONNECTION BETWEEN ACCRETION & EJECTION -THE FORMATION OF BLACK HOLES AND NEUTRON STARS: Can stars of >40 Msolar end as neutron stars rather than BHs ? Do BHs of >10 Msolar form promptly rather than in bright SN ? ...
... -THE PHYSICS OF RELATIVISTIC JETS FROM BH’s -THE CONNECTION BETWEEN ACCRETION & EJECTION -THE FORMATION OF BLACK HOLES AND NEUTRON STARS: Can stars of >40 Msolar end as neutron stars rather than BHs ? Do BHs of >10 Msolar form promptly rather than in bright SN ? ...
Tutor Marked Assignment
... We hope you are familiar with the system of evaluation to be followed for the Bachelor’s Degree Programme. At this stage you may probably like to re-read the section on assignments for Elective Courses in the Programme Guide that we sent you after your enrolment. A weightage of 30 per cent, as you a ...
... We hope you are familiar with the system of evaluation to be followed for the Bachelor’s Degree Programme. At this stage you may probably like to re-read the section on assignments for Elective Courses in the Programme Guide that we sent you after your enrolment. A weightage of 30 per cent, as you a ...
and galaxies
... Inside the GMCs are more hot and dense cores with dimensions of 0.05-1 parsec, T~100-200K and densities of 107-109 /cm3. 1000s of GMC are known in our galaxy, mostly in the spiral arms ...
... Inside the GMCs are more hot and dense cores with dimensions of 0.05-1 parsec, T~100-200K and densities of 107-109 /cm3. 1000s of GMC are known in our galaxy, mostly in the spiral arms ...
arXiv:astro-ph/0701792v1 29 Jan 2007
... star-forming feedback which plays an important role in resisting the gravity at large scale; while at small scale, the inward star forming feedback is introduced to connect the starburst region and the nuclear region by virtue of the theoretical and observational considerations. We also show that th ...
... star-forming feedback which plays an important role in resisting the gravity at large scale; while at small scale, the inward star forming feedback is introduced to connect the starburst region and the nuclear region by virtue of the theoretical and observational considerations. We also show that th ...
Physics of Galaxies 2016 Exercises with solutions – Batch II
... Should EW(Hα) be dust corrected before the comparison to models is made? This is where it gets complicated. The naive answer would be “no”, since the emission line and the underlying continuum are sampled at nearly the same wavelength, so even though dust may well have attenuated both the line and t ...
... Should EW(Hα) be dust corrected before the comparison to models is made? This is where it gets complicated. The naive answer would be “no”, since the emission line and the underlying continuum are sampled at nearly the same wavelength, so even though dust may well have attenuated both the line and t ...
Chemical evolution models for the dwarf spheroidal galaxies Leo 1
... Aims. We investigate the chemical evolutionary history of the dwarf spheroidal galaxies Leo 1 and Leo 2 by means of predictions from a detailed chemical evolution model compared to observations. The model adopts up to date nucleosynthesis and takes into account the role played by supernovae of differ ...
... Aims. We investigate the chemical evolutionary history of the dwarf spheroidal galaxies Leo 1 and Leo 2 by means of predictions from a detailed chemical evolution model compared to observations. The model adopts up to date nucleosynthesis and takes into account the role played by supernovae of differ ...
Beyond Our Solar System
... – Human eyes are sensitive to only a narrow range of colors. – As you explore the universe, you will learn to use a wide range of ‘colors’—from X rays to radio waves—to reveal sights invisible to ...
... – Human eyes are sensitive to only a narrow range of colors. – As you explore the universe, you will learn to use a wide range of ‘colors’—from X rays to radio waves—to reveal sights invisible to ...
chapter16StarBirth
... infrared and radio photons that escape the cloud. If there are no molecules, but only H, He, Li, and Bi like right after the big bang only very massive stars could form since there would be no molecular emission line cooling. ...
... infrared and radio photons that escape the cloud. If there are no molecules, but only H, He, Li, and Bi like right after the big bang only very massive stars could form since there would be no molecular emission line cooling. ...
First results of the Herschel key program “Dust, Ice and Gas In Time
... integration ramp linearity, cross-talk and response drift corrections as these were not yet scientifically validated. After level 1 processing, we extracted the spectra for the two nod positions separately from the central spaxel (spatial element). The wavelength–dependent point spread function (PSF ...
... integration ramp linearity, cross-talk and response drift corrections as these were not yet scientifically validated. After level 1 processing, we extracted the spectra for the two nod positions separately from the central spaxel (spatial element). The wavelength–dependent point spread function (PSF ...
LSS-GAC – A LAMOST Spectroscopic Survey of the Galactic Anti
... simulations, the scenario involves many currently poorly understood and often highly non-linear baryonic physics (e.g. star formation and feedback) that it is compulsory to find out empirically the assemblage history of galaxies via detailed study of large samples of member stars of nearby, well-res ...
... simulations, the scenario involves many currently poorly understood and often highly non-linear baryonic physics (e.g. star formation and feedback) that it is compulsory to find out empirically the assemblage history of galaxies via detailed study of large samples of member stars of nearby, well-res ...
SHELL H II REGIONS IN NGC 6334
... • Large proper motions due to large scale motion of region with respect to Sun and agree very well with Jones & Herbig (1979) • However, proper motions not identical for N and S components, indicating relative (orbital) motions ...
... • Large proper motions due to large scale motion of region with respect to Sun and agree very well with Jones & Herbig (1979) • However, proper motions not identical for N and S components, indicating relative (orbital) motions ...
Centimeter and Millimeter Observations of Very Young Binary Systems
... • Large proper motions due to large scale motion of region with respect to Sun and agree very well with Jones & Herbig (1979) • However, proper motions not identical for N and S components, indicating relative (orbital) motions ...
... • Large proper motions due to large scale motion of region with respect to Sun and agree very well with Jones & Herbig (1979) • However, proper motions not identical for N and S components, indicating relative (orbital) motions ...
the summary
... turned into iron, there is no energy source to prevent the core from collapsing under the weight of the star. During the gravitational collapse that follows, a lot of energy is released and the object becomes very bright for a couple of days to weeks. This is the phenomenon we already mentioned: a s ...
... turned into iron, there is no energy source to prevent the core from collapsing under the weight of the star. During the gravitational collapse that follows, a lot of energy is released and the object becomes very bright for a couple of days to weeks. This is the phenomenon we already mentioned: a s ...
150 Million ly - Northern Michigan University
... • Often the colliding galaxies repeatedly collide until they merge and form one new galaxy – Galactic Cannibalism!! ...
... • Often the colliding galaxies repeatedly collide until they merge and form one new galaxy – Galactic Cannibalism!! ...
Determining the Cepheid Period–Luminosity Relation Using
... on the V- and I-band photometry, which has been employed in particular by the Hubble Space Telescope Key Project on the extragalactic distance scale (Freedman et al., 2001). We find a significant effect in the sense that metal-poor stars are fainter than metal-rich stars by 0.23 ± 0.1 mag per dex. T ...
... on the V- and I-band photometry, which has been employed in particular by the Hubble Space Telescope Key Project on the extragalactic distance scale (Freedman et al., 2001). We find a significant effect in the sense that metal-poor stars are fainter than metal-rich stars by 0.23 ± 0.1 mag per dex. T ...