EROs and submm galaxies: Expectations for FMOS in the
... The emission line is identified as Hα at z=1.34. [OII] at z=3.12 is ruled out from the absence of a continuum break and the extreme continuum ...
... The emission line is identified as Hα at z=1.34. [OII] at z=3.12 is ruled out from the absence of a continuum break and the extreme continuum ...
to - NexStar Resource Site
... tunnel shaped clouds we could fly through. But let us keep to the facts. :-). Charles Messier on July 12, 1764 discovered M27. It was the first Planetary Nebula ever discovered. This is one of only 4 planetary nebula in the Messier catalogue. As noted in our Messier discussions, nebula are the tough ...
... tunnel shaped clouds we could fly through. But let us keep to the facts. :-). Charles Messier on July 12, 1764 discovered M27. It was the first Planetary Nebula ever discovered. This is one of only 4 planetary nebula in the Messier catalogue. As noted in our Messier discussions, nebula are the tough ...
FLARE SWG theme 3: high
... Large-scale clustering analyses with respect to galaxies – bias and constraints on BH seed formation? Mpc-scale environment around first quasars using FLARE IFU: co-eval galaxy and other z>6 quasar/AGN connections (multiple growing BHs)? Evidence for quasar outflows (e.g., broad CIV absorption troug ...
... Large-scale clustering analyses with respect to galaxies – bias and constraints on BH seed formation? Mpc-scale environment around first quasars using FLARE IFU: co-eval galaxy and other z>6 quasar/AGN connections (multiple growing BHs)? Evidence for quasar outflows (e.g., broad CIV absorption troug ...
Lab 14 Galaxy Morphology
... seen from an angle. For example, think of a football. If we look at the football from one angle it is long, and pointed at both ends. But if we rotate it by 90o , it appears to be round. This is a “projection effect”, and one that we can never remove since we cannot go out and look at elliptical gal ...
... seen from an angle. For example, think of a football. If we look at the football from one angle it is long, and pointed at both ends. But if we rotate it by 90o , it appears to be round. This is a “projection effect”, and one that we can never remove since we cannot go out and look at elliptical gal ...
THE STAR FORMATION AND NUCLEAR ACCRETION HISTORIES OF NORMAL GALAXIES
... may be most abundant at z < ∼ 1 and, if so, they could produce a substantial fraction of the “normal” galaxy X-ray flux at these redshifts. Given their similar evolution, spectral shapes (e.g., Ptak et al. 1999), and potentially similar luminosities, it may be difficult to disentangle the X-ray emis ...
... may be most abundant at z < ∼ 1 and, if so, they could produce a substantial fraction of the “normal” galaxy X-ray flux at these redshifts. Given their similar evolution, spectral shapes (e.g., Ptak et al. 1999), and potentially similar luminosities, it may be difficult to disentangle the X-ray emis ...
T3-Cosmic Star Formation History
... pace. Multiwavelength imaging surveys with the Hubble (HST) and Spitzer space telescopes and ground-based facilities, together with spectroscopic follow-up with 8-m-class telescopes, have led to the discovery of galaxies with confirmed redshifts as large as z = 7.5 (Finkelstein et al. 2013) as well a ...
... pace. Multiwavelength imaging surveys with the Hubble (HST) and Spitzer space telescopes and ground-based facilities, together with spectroscopic follow-up with 8-m-class telescopes, have led to the discovery of galaxies with confirmed redshifts as large as z = 7.5 (Finkelstein et al. 2013) as well a ...
Markov Chain Monte Carlo Modeling of High-Redshift Quasar
... Quasars, the visible phenomena associated with the active accretion phase of supermassive black holes found in the centers of galaxies, represent one of the most energetic processes in the Universe. As matter falls into the central black hole, it is accelerated and collisionally heated, and the radi ...
... Quasars, the visible phenomena associated with the active accretion phase of supermassive black holes found in the centers of galaxies, represent one of the most energetic processes in the Universe. As matter falls into the central black hole, it is accelerated and collisionally heated, and the radi ...
LACEwING: A New Moving Group Analysis Code
... For each NYMG, we use 100,000 Monte Carlo iterations within the triaxial ellipsoids to generate a realistic spread of UVW velocities. Using inverted matrices from Johnson & Soderblom (1987), we convert the UVW velocities into μα, μδ, and γ for a simulated star at the α and δ of the target, at a stan ...
... For each NYMG, we use 100,000 Monte Carlo iterations within the triaxial ellipsoids to generate a realistic spread of UVW velocities. Using inverted matrices from Johnson & Soderblom (1987), we convert the UVW velocities into μα, μδ, and γ for a simulated star at the α and δ of the target, at a stan ...
CONSTELLATION PERSEUS The constellation
... Located 92.8 light-years from Earth, it varies in apparent magnitude from a minimum of 3.5 to a maximum of 2.3 over a period of 2.867 days. The star system is the prototype of a group of eclipsing binary stars named Algol variables. • Alpha Persei known as Mirfak (Arabic for elbow) is the brightest ...
... Located 92.8 light-years from Earth, it varies in apparent magnitude from a minimum of 3.5 to a maximum of 2.3 over a period of 2.867 days. The star system is the prototype of a group of eclipsing binary stars named Algol variables. • Alpha Persei known as Mirfak (Arabic for elbow) is the brightest ...
83-98
... fine analysis. However, for X Cyg the estimate of HP is higher than the one derived by LL by 0.18 dex which is surprising. The differences in phases can partly account for the discrepancy. The observations of HP were made at a phase at which the assumption of hydrostatic equilibrium holds better tha ...
... fine analysis. However, for X Cyg the estimate of HP is higher than the one derived by LL by 0.18 dex which is surprising. The differences in phases can partly account for the discrepancy. The observations of HP were made at a phase at which the assumption of hydrostatic equilibrium holds better tha ...
Chapter 24
... than possessing a dense central nucleus, they often exhibit little internal structure of any kind. As with spirals, the stellar density increases sharply in the central nucleus. Denoted by the letter E, these systems are subdivided according to how elliptical they appear on the sky. The most circula ...
... than possessing a dense central nucleus, they often exhibit little internal structure of any kind. As with spirals, the stellar density increases sharply in the central nucleus. Denoted by the letter E, these systems are subdivided according to how elliptical they appear on the sky. The most circula ...
LCM SerieS
... computer automated technology. Simple and friendly to use, the LCM telescope is up and running after locating just three bright celestial objects. It’s the perfect combination of power and portability. If you are new to astronomy, you may wish to start off by using the LCM’s built-in Sky Tour featur ...
... computer automated technology. Simple and friendly to use, the LCM telescope is up and running after locating just three bright celestial objects. It’s the perfect combination of power and portability. If you are new to astronomy, you may wish to start off by using the LCM’s built-in Sky Tour featur ...
MPhil Thesis - Final - Suzanne Knight
... A large sample of white dwarfs within the solar neighbourhood has been examined to search for resolved common proper motion companions. The luminosity of these white dwarfs make them ideal candidates for detecting low mass objects such as brown dwarfs and gas giant planets. ! Theoretical predictions ...
... A large sample of white dwarfs within the solar neighbourhood has been examined to search for resolved common proper motion companions. The luminosity of these white dwarfs make them ideal candidates for detecting low mass objects such as brown dwarfs and gas giant planets. ! Theoretical predictions ...
View
... of the most sophisticated and easy to use telescopes available on the market today. Take time to read through this manual before embarking on your journey through the Universe. It may take a few observing sessions to become familiar with your telescope, so you should keep this manual handy until you ...
... of the most sophisticated and easy to use telescopes available on the market today. Take time to read through this manual before embarking on your journey through the Universe. It may take a few observing sessions to become familiar with your telescope, so you should keep this manual handy until you ...
The Circumstellar Environments of Young Stars at AU Scales
... tion for many types of YSOs (e.g., T Tauri, Herbig Ae/Be, FU Orionis). The interferometer data can also can be compared to predictions of specific physical models and this exercise has allowed to rule out certain classes of models, and provided crucial constraints to models that can be made to repro ...
... tion for many types of YSOs (e.g., T Tauri, Herbig Ae/Be, FU Orionis). The interferometer data can also can be compared to predictions of specific physical models and this exercise has allowed to rule out certain classes of models, and provided crucial constraints to models that can be made to repro ...
Planet Formation in the Outer Solar System
... td ∼ 1–10 Myr (Russell et al. 1996; Hartmann et al. 1998; Lada 1999; Brandner et al. 2000; Haisch, Lada, & Lada 2001). The observational timescales place strong constraints on planet formation models. Gas giants must form before the gas disappears. Rocky planets must form before the dust disappears. ...
... td ∼ 1–10 Myr (Russell et al. 1996; Hartmann et al. 1998; Lada 1999; Brandner et al. 2000; Haisch, Lada, & Lada 2001). The observational timescales place strong constraints on planet formation models. Gas giants must form before the gas disappears. Rocky planets must form before the dust disappears. ...
Article PDF - IOPscience
... segments” that cover the overlapping range between the first and second orders in both SL and LL; we used these to verify the flux calibration between the first and second orders. In addition to the spectroscopic modules, the IRS also contains two peakup imaging arrays used to position the target on ...
... segments” that cover the overlapping range between the first and second orders in both SL and LL; we used these to verify the flux calibration between the first and second orders. In addition to the spectroscopic modules, the IRS also contains two peakup imaging arrays used to position the target on ...
Introduction
... to relatively isolated systems. As such, the sample is ideal for disentangling the internal and environmental processes driving evolution. The combination of ultraviolet, optical, near- and far-infrared imaging, nuclear and integrated optical spectroscopy, and atomic hydrogen emission line data, tra ...
... to relatively isolated systems. As such, the sample is ideal for disentangling the internal and environmental processes driving evolution. The combination of ultraviolet, optical, near- and far-infrared imaging, nuclear and integrated optical spectroscopy, and atomic hydrogen emission line data, tra ...
Stellarium User Guide - Skolekonsulenterne.dk
... As well as travelling through time, Stellarium lets to look around the sky freely, and zoom in and out. There are several ways to accomplish this listed in table 3.4. Let’s try it. Use the cursors to move around left, right, up and down. Zoom in a little using the Page Up key, and back out again usi ...
... As well as travelling through time, Stellarium lets to look around the sky freely, and zoom in and out. There are several ways to accomplish this listed in table 3.4. Let’s try it. Use the cursors to move around left, right, up and down. Zoom in a little using the Page Up key, and back out again usi ...
Observational evidence for AGN feedback in early
... A major amendment in recent models of hierarchical galaxy formation is the inclusion of socalled active galactic nucleus (AGN) feedback. The energy input from an active central massive black hole is invoked to suppress star formation in early-type galaxies at later epochs. A major problem is that th ...
... A major amendment in recent models of hierarchical galaxy formation is the inclusion of socalled active galactic nucleus (AGN) feedback. The energy input from an active central massive black hole is invoked to suppress star formation in early-type galaxies at later epochs. A major problem is that th ...
Galactic Stellar and Substellar Initial Mass Function Invited Review Gilles Chabrier
... ABSTRACT. We review recent determinations of the present-day mass function (PDMF) and initial mass function (IMF) in various components of the Galaxy—disk, spheroid, young, and globular clusters—and in conditions characteristic of early star formation. As a general feature, the IMF is found to depen ...
... ABSTRACT. We review recent determinations of the present-day mass function (PDMF) and initial mass function (IMF) in various components of the Galaxy—disk, spheroid, young, and globular clusters—and in conditions characteristic of early star formation. As a general feature, the IMF is found to depen ...
Galaxies
... underlying dark matter. We have started to understand how baryonic gas within the dark matter halos cools and collapses to form stars, and how the energy from star formation can feed back into the surrounding gas and regulate subsequent star formation. However, at a fundamental level we still lack a ...
... underlying dark matter. We have started to understand how baryonic gas within the dark matter halos cools and collapses to form stars, and how the energy from star formation can feed back into the surrounding gas and regulate subsequent star formation. However, at a fundamental level we still lack a ...
– 1 – 1. Galaxy Observations 1.1.
... the nature of the field. The major concern in studies based on SDSS spectra is the fixed fiber size of 3 arcsec, which means aperture corrections are important as the spatial sampling varies from “nuclear spectra” to “partial or full disk spectra” depending on the redshift. Given radial gradients in ...
... the nature of the field. The major concern in studies based on SDSS spectra is the fixed fiber size of 3 arcsec, which means aperture corrections are important as the spatial sampling varies from “nuclear spectra” to “partial or full disk spectra” depending on the redshift. Given radial gradients in ...
on the pms star hbc 498 and its associated nebulous stars1
... spectra. We expect the accuracy in the resulting MK classification to be of ±1 sub-class. The three brightest objects, namely HBC 498, HBC 495 and DL Ori/G2 have Li Iλ6708 Å strong in absorption (see Fig. 2 and Table 3), with equivalent widths stronger than the richest Li I stars with similar spect ...
... spectra. We expect the accuracy in the resulting MK classification to be of ±1 sub-class. The three brightest objects, namely HBC 498, HBC 495 and DL Ori/G2 have Li Iλ6708 Å strong in absorption (see Fig. 2 and Table 3), with equivalent widths stronger than the richest Li I stars with similar spect ...
SkyProdigy Series Manual
... For astronomical viewing, out of focus star images are very diffuse, making them difficult to see. If you turn the focus knob too quickly, you can go right through focus without seeing the image. To avoid this problem, your first astronomical target should be a bright object (like the Moon or a plan ...
... For astronomical viewing, out of focus star images are very diffuse, making them difficult to see. If you turn the focus knob too quickly, you can go right through focus without seeing the image. To avoid this problem, your first astronomical target should be a bright object (like the Moon or a plan ...
Malmquist bias
The Malmquist bias is an effect in observational astronomy which leads to the preferential detection of intrinsically bright objects. It was first described in 1922 by Swedish astronomer Gunnar Malmquist (1893–1982), who then greatly elaborated upon this work in 1925. In statistics, this bias is referred to as a selection bias and affects the survey results in a brightness limited survey, where stars below a certain apparent brightness are not included. Since observed stars and galaxies appear dimmer when farther away, the brightness that is measured will fall off with distance until their brightness falls below the observational threshold. Objects which are more luminous, or intrinsically brighter, can be observed at a greater distance, creating a false trend of increasing intrinsic brightness, and other related quantities, with distance. This effect has led to many spurious claims in the field of astronomy. Properly correcting for these effects has become an area of great focus.