Nuclear Activity in UZC Compact Groups of Galaxies M.A. Martinez
... We have inspected three database archives looking for UZC-CG galaxies spectra. The databases are the Z-Machine Spectrograph Archive, the FAST Spectrograph Archive and the Sloan Digital Sky Survey DR4. We have found 652, 246 and 221 spectra respectively. In several cases the spectrum of the same gala ...
... We have inspected three database archives looking for UZC-CG galaxies spectra. The databases are the Z-Machine Spectrograph Archive, the FAST Spectrograph Archive and the Sloan Digital Sky Survey DR4. We have found 652, 246 and 221 spectra respectively. In several cases the spectrum of the same gala ...
Journey through the cosmos
... of our own Galaxy with the naked eye. The darker the skies, the more stars you can see. Of course, there are billions more stars but they are so far away. You can see stars because they are luminous, which means that they give out their own energy as light. Each galaxy is a collection of many millio ...
... of our own Galaxy with the naked eye. The darker the skies, the more stars you can see. Of course, there are billions more stars but they are so far away. You can see stars because they are luminous, which means that they give out their own energy as light. Each galaxy is a collection of many millio ...
Activity : Milky Way
... To investigate spiral arms in our own Galaxy, what do we search for and what difficulties are involved? Taking our clues from other galaxies, what objects (in visible light first) seem to indicate the positions of spiral arms? • Dark dust rift lanes • Bright, clustering, stars • Pink (hydrogen) nebu ...
... To investigate spiral arms in our own Galaxy, what do we search for and what difficulties are involved? Taking our clues from other galaxies, what objects (in visible light first) seem to indicate the positions of spiral arms? • Dark dust rift lanes • Bright, clustering, stars • Pink (hydrogen) nebu ...
More about the game plan:
... • Orbital velocity of stars different than pattern speed • Stars, gas bunch up at position of spiral arms • Causes higher grav. potential • Unclear if self-sustaining or forced. ...
... • Orbital velocity of stars different than pattern speed • Stars, gas bunch up at position of spiral arms • Causes higher grav. potential • Unclear if self-sustaining or forced. ...
The Spectra of Stars
... Colors of Stars Colors of Stars • Stars are made of hot, dense gas Stars are made of hot dense gas – Continuous spectrum from the lowest visible ...
... Colors of Stars Colors of Stars • Stars are made of hot, dense gas Stars are made of hot dense gas – Continuous spectrum from the lowest visible ...
Astronomy Astrophysics
... A suitable object in which mass segregation can be studied is the moderately rich open cluster M 67 (NGC 2682), located at J2000 08h 51m 25s + 11◦ 490 5000 (` = 215.68◦, b = 31.93◦), consequently it is a high-latitude, not heavily contaminated object. Its apparent size can easily be traced visually ...
... A suitable object in which mass segregation can be studied is the moderately rich open cluster M 67 (NGC 2682), located at J2000 08h 51m 25s + 11◦ 490 5000 (` = 215.68◦, b = 31.93◦), consequently it is a high-latitude, not heavily contaminated object. Its apparent size can easily be traced visually ...
Astronomy - Mr. Hill`s Science Website
... that our galaxy is filled with starlight-absorbing dust, or interstellar dust. This means that stars far away from our Sun appear dimmer or are not even visible from Earth. This effect means we preferentially see the stars nearest to our Sun and cannot easily observe the other side of the galaxy. Th ...
... that our galaxy is filled with starlight-absorbing dust, or interstellar dust. This means that stars far away from our Sun appear dimmer or are not even visible from Earth. This effect means we preferentially see the stars nearest to our Sun and cannot easily observe the other side of the galaxy. Th ...
Nebula
... hydrogen) that produces spectral line emission. These emission nebulae are often called HII regions; the term "HII" is used in professional astronomy to refer to ionized hydrogen. In contrast to emission nebulae, reflection nebulae do not produce significant amounts of visible light by themselves bu ...
... hydrogen) that produces spectral line emission. These emission nebulae are often called HII regions; the term "HII" is used in professional astronomy to refer to ionized hydrogen. In contrast to emission nebulae, reflection nebulae do not produce significant amounts of visible light by themselves bu ...
Estimating the Age of Supernova Remnants - Chandra X
... 8. Find the average velocity of the stellar core for this displacement. 9. Using this average velocity, find its kinetic energy. Evidence indicates the core is a neutron star with a mass of approximately 1.4 solar masses. ...
... 8. Find the average velocity of the stellar core for this displacement. 9. Using this average velocity, find its kinetic energy. Evidence indicates the core is a neutron star with a mass of approximately 1.4 solar masses. ...
A Study of the Nature and Representative Features of Supernova
... closely related (Moore D. 2001). A brief description of each type follows. Type Ia Exhibit no hydrogen or helium lines but show a prominent silicon (Si II) line. Believed to be caused by runaway carbon burning in a white dwarf with a binary companion, from which the required matter to cause the expl ...
... closely related (Moore D. 2001). A brief description of each type follows. Type Ia Exhibit no hydrogen or helium lines but show a prominent silicon (Si II) line. Believed to be caused by runaway carbon burning in a white dwarf with a binary companion, from which the required matter to cause the expl ...
A galaxy rapidly forming stars 700 million years after the Big Bang at
... that a typical galaxy at z < 7 has SFR 5 10 M[ yr21; the measured SFR of z8_GND_5296 is a factor of more than 30 times greater. If this SFR function is accurate, the expected space density per co-moving Mpc3 for this galaxy would be =1025. The implied rarity of this galaxy could indicate that it is ...
... that a typical galaxy at z < 7 has SFR 5 10 M[ yr21; the measured SFR of z8_GND_5296 is a factor of more than 30 times greater. If this SFR function is accurate, the expected space density per co-moving Mpc3 for this galaxy would be =1025. The implied rarity of this galaxy could indicate that it is ...
GALAXY FORMATION AND CLUSTER FORMATION Richard B
... compact than typical present-day irregular or spiral galaxies, since a higher star formation rate requires a higher mean density (Larson 1977). Typical irregular or spiral galaxies also do not make clusters as massive as typical globular clusters, so they cannot serve as suitable prototypes for the ...
... compact than typical present-day irregular or spiral galaxies, since a higher star formation rate requires a higher mean density (Larson 1977). Typical irregular or spiral galaxies also do not make clusters as massive as typical globular clusters, so they cannot serve as suitable prototypes for the ...
Make Your Own Star Bracelet
... telescopes. We must look for them by their heat, looking at their infrared radiation." "The next two beads tell us of two possible endings for stars." (pick up the metallic bead) "Pick up the metallic bead and thread it onto the cord. When some stars grow old, they blow off their outer layers of gas ...
... telescopes. We must look for them by their heat, looking at their infrared radiation." "The next two beads tell us of two possible endings for stars." (pick up the metallic bead) "Pick up the metallic bead and thread it onto the cord. When some stars grow old, they blow off their outer layers of gas ...
Herschel-ATLAS: SDSS cross-correlation induced by weak lensing
... we have estimated the magnification of each background source by the foreground source closest to its line of sight using the formalism by Lapi et al. (2012). The simulations confirms that a statistically significant cross-correlation appeared at the relevant scales, demonstrating that the observed ...
... we have estimated the magnification of each background source by the foreground source closest to its line of sight using the formalism by Lapi et al. (2012). The simulations confirms that a statistically significant cross-correlation appeared at the relevant scales, demonstrating that the observed ...
the magellanic clouds newsletter - Keele University Astrophysics
... Deep photometry of the Small Magellanic Cloud (SMC) stellar periphery (R = 4◦ , 4.2 kpc) is used to study its lineof-sight depth with red clump (RC) stars. The RC luminosity function is affected little by young (< 1 Gyr) blue-loop stars in these regions because their main-sequence counterparts are n ...
... Deep photometry of the Small Magellanic Cloud (SMC) stellar periphery (R = 4◦ , 4.2 kpc) is used to study its lineof-sight depth with red clump (RC) stars. The RC luminosity function is affected little by young (< 1 Gyr) blue-loop stars in these regions because their main-sequence counterparts are n ...
SPITZER/MIPS 24 µm OBSERVATIONS OF GALAXY CLUSTERS
... X-ray luminous galaxy clusters spanning a wide redshift range (0.02 < z < 0.83). Uniform photometry, high resolution HST imaging, and extensive redshift catalogs enable us to measure the fraction of members with strong, dust-obscured star formation. We find that the fraction of cluster galaxies with ...
... X-ray luminous galaxy clusters spanning a wide redshift range (0.02 < z < 0.83). Uniform photometry, high resolution HST imaging, and extensive redshift catalogs enable us to measure the fraction of members with strong, dust-obscured star formation. We find that the fraction of cluster galaxies with ...
UMich w/s - Royal Observatory, Edinburgh
... A minimum half-light size for galaxies, ~100pc mass scale similar, or a little larger Probably cored mass profiles, with similar mean mass densities ~0.1M/pc3, ~5GeV/cc An apparent characteristic (minimum) mass dark halo at dSph, ...
... A minimum half-light size for galaxies, ~100pc mass scale similar, or a little larger Probably cored mass profiles, with similar mean mass densities ~0.1M/pc3, ~5GeV/cc An apparent characteristic (minimum) mass dark halo at dSph, ...
the galaxy-halo connection from abundance matching: simplicity
... Results to date: matching stellar mass/or luminosity to the maximum mass/vmax its halo ever had (current mass(vmax) for central galaxies; mass at accretion for satellites), with a small amount of scatter, works very well. excellent agreement with a wide range of galaxy statistics, including two-poin ...
... Results to date: matching stellar mass/or luminosity to the maximum mass/vmax its halo ever had (current mass(vmax) for central galaxies; mass at accretion for satellites), with a small amount of scatter, works very well. excellent agreement with a wide range of galaxy statistics, including two-poin ...
PDF only - at www.arxiv.org.
... their surroundings act like laboratories, not only for the study of star formation and evolution but also for that of stellar structures and abundance patterns. Open clusters in particular are considered as powerful tools for such studies (Friel 1995; Frinchaboy & Majewski 2008). The first step in e ...
... their surroundings act like laboratories, not only for the study of star formation and evolution but also for that of stellar structures and abundance patterns. Open clusters in particular are considered as powerful tools for such studies (Friel 1995; Frinchaboy & Majewski 2008). The first step in e ...
The Radio and X-ray Jet
... The ground-based experiment reported that p had its normal, expected value with a precision of 15 decimal places. The space-based experiment measured p on a scale of 1012m, and once again found that it has its normal expected value, to an accuracy this time of 10 decimal places. ...
... The ground-based experiment reported that p had its normal, expected value with a precision of 15 decimal places. The space-based experiment measured p on a scale of 1012m, and once again found that it has its normal expected value, to an accuracy this time of 10 decimal places. ...
NEUTRON STARS AND PULSARS Discovery Were it not for
... For centuries astronomers relied on electromagnetic waves, at first, exclusively the visible part of the spectrum using optical telescopes, sometimes built by themselves, such as Herschell’s 48 inch reflecting telescope built with a grant from King George III. Today, the instruments used to search out ...
... For centuries astronomers relied on electromagnetic waves, at first, exclusively the visible part of the spectrum using optical telescopes, sometimes built by themselves, such as Herschell’s 48 inch reflecting telescope built with a grant from King George III. Today, the instruments used to search out ...
PHY104 - Introduction to Astrophysics
... Generally speaking the flux is a perfectly useful measure of how much light we receive on Earth. There are some practical difficulties in measuring the flux of course; our detectors are not 100% efficient, and we have to correct for the amount of light absorbed by the atmosphere. Nevertheless, once ...
... Generally speaking the flux is a perfectly useful measure of how much light we receive on Earth. There are some practical difficulties in measuring the flux of course; our detectors are not 100% efficient, and we have to correct for the amount of light absorbed by the atmosphere. Nevertheless, once ...
Young Stellar Objects in the Orion B Cloud
... NGC 2068 and NGC 2071, which each contain more than 35 YSOs, as clusters and HH 24-26 as a stellar group. More than half of all YSO candidates identified in our study belong to NGC 2068 or NGC 2071, hence the majority of star formation in this part of Orion B appears to occur in a clustered mode, w ...
... NGC 2068 and NGC 2071, which each contain more than 35 YSOs, as clusters and HH 24-26 as a stellar group. More than half of all YSO candidates identified in our study belong to NGC 2068 or NGC 2071, hence the majority of star formation in this part of Orion B appears to occur in a clustered mode, w ...
Penn State Astronomy 11 Laboratory
... which will help you to locate stars and constellations this semester. You will also need a calculator capable of scientific notation, and a small flashlight with some type of red filter on it (i.e., covered with red cellophane, a red balloon, red nail polish, etc.). B. Students will be required to p ...
... which will help you to locate stars and constellations this semester. You will also need a calculator capable of scientific notation, and a small flashlight with some type of red filter on it (i.e., covered with red cellophane, a red balloon, red nail polish, etc.). B. Students will be required to p ...
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.