Formation of Molecular Clouds and Global Conditions for Star
... or the H2 to 13 CO abundance ratio, both of which can vary within and between clouds in response to local conditions of UV irradiance, density, temperature, and metallicity (Bolatto et al. 2013; Ripple et al. 2013). Millimeter wave interferometers can resolve large GMC complexes in nearby galaxies b ...
... or the H2 to 13 CO abundance ratio, both of which can vary within and between clouds in response to local conditions of UV irradiance, density, temperature, and metallicity (Bolatto et al. 2013; Ripple et al. 2013). Millimeter wave interferometers can resolve large GMC complexes in nearby galaxies b ...
Gamma Ray Bursts
... „p of the Sky” prototype at LCO, July 2004 – July 2005 no GRB optical counterpart observed so far limits 11-12m for 2 GRB before and during g burst several limits ~minutes after GRB several flashes observed neither confirmed nor excluded by others 1 flash identified as CN Leo flare star outburst 100 ...
... „p of the Sky” prototype at LCO, July 2004 – July 2005 no GRB optical counterpart observed so far limits 11-12m for 2 GRB before and during g burst several limits ~minutes after GRB several flashes observed neither confirmed nor excluded by others 1 flash identified as CN Leo flare star outburst 100 ...
The CCD Photometric Calibration Cookbook
... Nearly a century has passed since Prof. Kapteyn made this remark and during the intervening period much effort has been devoted to developing techniques for the proper calibration of astronomical photographs and latterly CCD images. The techniques for calibrating CCD images are now well established. ...
... Nearly a century has passed since Prof. Kapteyn made this remark and during the intervening period much effort has been devoted to developing techniques for the proper calibration of astronomical photographs and latterly CCD images. The techniques for calibrating CCD images are now well established. ...
User`s Manual for DAOPHOT II This manual is intended as a guide
... you may prefer to skip the second or even both automatic star-finding passes, and go directly to interactive star identification. (5) A principal source of photometric error for the faint stars is the difficulty of defining what is meant by the term “sky brightness” in crowded fields. This is not s ...
... you may prefer to skip the second or even both automatic star-finding passes, and go directly to interactive star identification. (5) A principal source of photometric error for the faint stars is the difficulty of defining what is meant by the term “sky brightness” in crowded fields. This is not s ...
constellations - Richmond and Glen Allen Weather
... What is a constellation? Constellation is derived from the Latin "constellatus," set with stars; from "com-," together, and "stellare," to shine; stella, a star. A constellation is a group of stars, which might form a pattern or shape within a specific area of the sky and is often named after people ...
... What is a constellation? Constellation is derived from the Latin "constellatus," set with stars; from "com-," together, and "stellare," to shine; stella, a star. A constellation is a group of stars, which might form a pattern or shape within a specific area of the sky and is often named after people ...
SUB-KILOPARSEC IMAGING OF COOL MOLECULAR GAS IN
... in the literature (e.g., Bolatto et al. 2013). The conversion factor, αCO , varies with the kinematic state of the gas (through the escape fraction of CO photons) and the gas metallicity (through CO formation and destruction processes). A variety of observations suggest that a value of αCO ∼ 3.6 − 4 ...
... in the literature (e.g., Bolatto et al. 2013). The conversion factor, αCO , varies with the kinematic state of the gas (through the escape fraction of CO photons) and the gas metallicity (through CO formation and destruction processes). A variety of observations suggest that a value of αCO ∼ 3.6 − 4 ...
A1 F2015 Seasonal.key
... information: the direction you must face (north, northeast, east, etc.) and how far above the horizon you must look (low, high or directly overhead). If you cannot see the star, state that explicitly. The descriptions for four positions are given as examples a) A1: east, low ...
... information: the direction you must face (north, northeast, east, etc.) and how far above the horizon you must look (low, high or directly overhead). If you cannot see the star, state that explicitly. The descriptions for four positions are given as examples a) A1: east, low ...
Annual Report 2011 - Max Planck Institute for Astrophysics
... had an internationally-recognized numerical astrophysics program that is unparalleled by any other The Max-Planck-Institut für Astrophysik, called institution of similar size. the MPA for short, was founded in 1958 under the directorship of Ludwig Biermann. It was first established as an offshoot of ...
... had an internationally-recognized numerical astrophysics program that is unparalleled by any other The Max-Planck-Institut für Astrophysik, called institution of similar size. the MPA for short, was founded in 1958 under the directorship of Ludwig Biermann. It was first established as an offshoot of ...
Analysis of Stellar Activity and Orbital Dynamics in Extrasolar
... Nearly four centuries later, as- age can be estimated based on short26 tronomers are much closer to finding lived, extinct radionuclides like Al and ...
... Nearly four centuries later, as- age can be estimated based on short26 tronomers are much closer to finding lived, extinct radionuclides like Al and ...
Differential rotation on both components of the pre-main
... We present the first measurements of surface differential rotation on a pre-main-sequence binary system. Using intensity (Stokes I) and circularly polarized (Stokes V) time-series spectra, taken over 11 nights at the Anglo-Australian Telescope (AAT), we incorporate a solarlike differential rotation ...
... We present the first measurements of surface differential rotation on a pre-main-sequence binary system. Using intensity (Stokes I) and circularly polarized (Stokes V) time-series spectra, taken over 11 nights at the Anglo-Australian Telescope (AAT), we incorporate a solarlike differential rotation ...
IRAM Annual Report 2011
... because of its flux density (~200 mJy at 500 μm) and redshift (z=5.2429). The dominant lens is a foreground z=0.63 galaxy, not the cluster itself. The source has a far-infrared (FIR) luminosity of LFIR= 1.1 1014μ L⊙, where μ~11 is the magnification factor. Combes reported the redshift identification ...
... because of its flux density (~200 mJy at 500 μm) and redshift (z=5.2429). The dominant lens is a foreground z=0.63 galaxy, not the cluster itself. The source has a far-infrared (FIR) luminosity of LFIR= 1.1 1014μ L⊙, where μ~11 is the magnification factor. Combes reported the redshift identification ...
FLARE SWG theme 3: high
... (2) Environments of first massive black holes Other “environment” measures of first quasars with FLARE: 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 quas ...
... (2) Environments of first massive black holes Other “environment” measures of first quasars with FLARE: 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 quas ...
Article PDF - IOPscience
... a major merger of disk galaxies and, concurrently, a merger of their SMBHs. It is now understood on the basis of detailed numerical simulations that the merger of disk galaxies can create a relatively normal elliptical galaxy (Barnes & Hernquist 1992). Since most (if not all) bright disk galaxies co ...
... a major merger of disk galaxies and, concurrently, a merger of their SMBHs. It is now understood on the basis of detailed numerical simulations that the merger of disk galaxies can create a relatively normal elliptical galaxy (Barnes & Hernquist 1992). Since most (if not all) bright disk galaxies co ...
Comprehensive Wide-Band Magnitudes and Albedos for the Planets
... used for brightness references, the optical and sensor hardware employed, the observing procedures and the methods of calibration. The Sloan standard stars of Smith et al. (2002) range from about magnitude r’ = 9 to r’ = 14 and, thus, are generally too faint to serve as references for planetary phot ...
... used for brightness references, the optical and sensor hardware employed, the observing procedures and the methods of calibration. The Sloan standard stars of Smith et al. (2002) range from about magnitude r’ = 9 to r’ = 14 and, thus, are generally too faint to serve as references for planetary phot ...
Carl Sagan - Cosmos (1980) [Full Color Illustrated
... nature. The treatment of toothache with second-rate beer was tied to the deepest cosmological mysteries. Today we have discovered a powerful and elegant way to understand the universe, a method called science; it has revealed to us a universe so ancient and so vast that human affairs seem at first s ...
... nature. The treatment of toothache with second-rate beer was tied to the deepest cosmological mysteries. Today we have discovered a powerful and elegant way to understand the universe, a method called science; it has revealed to us a universe so ancient and so vast that human affairs seem at first s ...
A Further Examination of the Gospel in the Stars
... stars that we call constellations. Astronomers today recognize 88 constellations, and those 88 constellations encompass the entire celestial sphere. About 40 of the constellations are relatively modern, dating back 500 years or less. The modern system was codified by the International Astronomical U ...
... stars that we call constellations. Astronomers today recognize 88 constellations, and those 88 constellations encompass the entire celestial sphere. About 40 of the constellations are relatively modern, dating back 500 years or less. The modern system was codified by the International Astronomical U ...
IRAM Annual Report 2014
... The detector development program has greatly profited from the French LABEX program FOCUS. The wide field of view of NIKA-2 requires important upgrades in the 30-meter telescope Nasmyth optics. During 2014, these upgrades have been thoroughly prepared with work at the telescope foreseen for spring 2 ...
... The detector development program has greatly profited from the French LABEX program FOCUS. The wide field of view of NIKA-2 requires important upgrades in the 30-meter telescope Nasmyth optics. During 2014, these upgrades have been thoroughly prepared with work at the telescope foreseen for spring 2 ...
Document
... Step 2. Assume that the Parallax and Proper Motion of the reference stars are zero Step 3. Choose a “Standard Plate” (typically your first observation) and transform all other images into it using the method of least-squares and simultaneously solve for Parallax and proper motion Xtrans = a*X+b*Y+c ...
... Step 2. Assume that the Parallax and Proper Motion of the reference stars are zero Step 3. Choose a “Standard Plate” (typically your first observation) and transform all other images into it using the method of least-squares and simultaneously solve for Parallax and proper motion Xtrans = a*X+b*Y+c ...
Starspots: A Key to the Stellar Dynamo | SpringerLink
... flares (UV Cet-type stars). Periodic brightness variations were observed in binary systems of red dwarfs (BY Dra-type) as distortions of the light curves outside eclipses. Kron (1947) was seemingly the first who considered the hypothesis that spottedness of the stellar surface was causing these dist ...
... flares (UV Cet-type stars). Periodic brightness variations were observed in binary systems of red dwarfs (BY Dra-type) as distortions of the light curves outside eclipses. Kron (1947) was seemingly the first who considered the hypothesis that spottedness of the stellar surface was causing these dist ...
Stars sensors terminology and performance
... Figure 3-10: Aspect angle to planetary body or sun .............................................................. 25 Figure 4-1: Schematic generalized Star Sensor model ......................................................... 34 ...
... Figure 3-10: Aspect angle to planetary body or sun .............................................................. 25 Figure 4-1: Schematic generalized Star Sensor model ......................................................... 34 ...
Circumstellar dust emission from nearby Solar
... 10−5 (Paper I). Both stars exhibit detectable temperature minima at wavelengths around 100-300 µm due to a chromospheric temperature inversion akin to that of the sun. The resulting flux difference, when compared to stellar photospheric models, is equivalent to dust emission with a fractional lumino ...
... 10−5 (Paper I). Both stars exhibit detectable temperature minima at wavelengths around 100-300 µm due to a chromospheric temperature inversion akin to that of the sun. The resulting flux difference, when compared to stellar photospheric models, is equivalent to dust emission with a fractional lumino ...
Corvus (constellation)
Corvus is a small constellation in the Southern Celestial Hemisphere. Its name comes from the Latin word ""raven"" or ""crow"". It includes only 11 stars with brighter than 4.02 magnitudes. One of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations. The four brightest stars, Gamma, Delta, Epsilon, and Beta Corvi from a distinctive quadrilateral in the night sky. The young star Eta Corvi has been found to have two debris disks.